– ABSTRACT BOOK –17th International Workshop on Low Temperature Detectors
Kurume, Fukuoka, Japan
June 28, 2017

Preface
The International Workshop on Low Temperature Detectors (LTD) is the biennial meeting to present and discuss
latest results on research and development of cryogenic detectors for radiation and particles, and on applications of
those detectors. The 17-th workshop will be held at Kurume City Plaza in Kurume city, Fukuoka Japan from 17th of
July through 21st.
The workshop will be organized with the following six sessions:
1. Keynote talks
2. Sensor Physics & Developments,• TES, MMC, MKIDS, STJ, Semiconductors, Novel detectors, others
3. Readout Techniques & Signal processing• Electronics, Multiplexing, Filtering, Imaging, Microwave circuit, Data analysis, others
4. Fabrication & Implementation Techniques• Fabrication process, MEMS, Pixel array, Microwave wirings, others
5. Cryogenics and Components• Refrigerators, Window techniques, Optical Blocking Filters, others
6. Applications• Electromagnetic wave & photon (mm-wave, THZ, IR, Visible, X-ray, Gamma-ray), Particles, Neutrons,
CMB, Dark Matter, Neutrinos, Particle & Nuclear Physics, Rare Event Search, Material Analysis & Life
Science
Kurume is a fabulous location for the workshop. It is known by good local foods and good Sake (Japanese rice wine),
and also for traditional fabric called Kurume Gasuri. The LTD17 workshop provides you a wonderful opportunity to
exchange your ideas and extend your experience on the low temperature detectors. We hope you will join and enjoy.

LOC of 17th International Workshop on Low Temperature Detectors

iiContents
Oral presentations

1

Keynote talks
O-1 Low Temperature Detectors (for Dark matter and Neutrinos) 30 Years ago. The Start of a newexperimental Technology. (Franz von Feilitzsch) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-2 X-Ray Microcalorimeters in Space - Today and Tomorrow (Richard L Kelley) . . . . . . . . . . . . . .
O-3 CMB B-mode polarization - Probe the era before the Big Bang (Hitoshi Murayama) . . . . . . . . . .

2

MKIDS 1O-4 Performance of a 961 pixel Kinetic Inductance Detector system for future space borne observatories(Jochem Baselmans, Juan Bueno, Stephen Yates, Ozan Yurduseven, Nuria Llombart, Kenichi Karatsu,
Andrey Baryshev, Lorenza Ferrari, Akira Endo, David Thoen, Pieter de Visser, Reinier Janssen, Vignesh Murugesan, Eduard Driessen, Gregoire Coiﬀard, Jesus Martin-Pintado, Peter Hargrave, Matt
Griﬃn) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-5 The sub-gap KID (SKID): on-chip spectroscopy at centimetric wavelengths (Alessandro Monfardini,
Olivier Dupre, Alain Benoit, Martino Calvo, Andrea Catalano, Johannes Goupy, Christophe Hoarau,
Thierry Klein, Kevin Le Calvez, Benjamin Sacepe, Florence Levy-Bertrand, Alicia Gomez ) . . . . . .
O-6 Moving optical MKIDs to lower temperature: preliminary characterization of Hafnium resonators (Giulia
Collura, Gregoire Coiﬀard, Bruce Bumble, Paul Szypryt, Benjamin A. Mazin) . . . . . . . . . . . . . .
O-7 Suppression of in-detector-chip stray radiation for large arrays of lens-antenna coupled microwave kinetic inductance detectors (Stephen J.C. Yates, Andrey M. Baryshev, Ozan Yurduseven, Juan Bueno,
Kristina K. Davis, Lorenza Ferrari, Willem Jellema, Nuria Llombart, Vignesh Murugesan, David
Thoen, Jochem J.A. Baselmans) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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MKIDS 2
O-8 Counting Near Infrared Photons with Microwave Kinetic Inductance Detectors (Lianfu Wei ) . . . . .
O-9 Characterizing millimeter wave Thermal Kinetic Inductance Detectors with a novel readout system(Roger O’Brient, Bryan Steinbach, Hien Nguyen, Anthony Turner, Jonas Zmuidzinas, James Bock ) .
O-10 Photon Counting Kinetic Inductance Detectors for THz/Submillimeter Space Spectroscopy (Omid
Noroozian, Emily M Barrentine, Thomas R Stevenson, Ari D Brown, Vilem Mikula, Edward J Wollack,
Kongpop U-Yen, Samuel H Moseley) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-11 Low-Loss, Low-Noise, Crystalline Silicon Dielectric for Superconducting Microstriplines and Kinetic
Inductance Detector Capacitors (Fabien Defrance, Andrew D. Beyer, Jack Sayers, Sunil Golwala) . .
O-12 Kalliope-based High-Speed Neutron imager by a delay-line current biased kinetic inductance detector(Hiroaki Shishido, Yuya Miki, Hiroyuki Yamaguchi, Yuki Iizawa, Kenji M Kojima, Kenichi Oikawa,
Masahide Harada, Takayuki Oku, Kazuhiko Soyama, Shigeyuki Miyajima, Mutsuo Hidaka, Takekazu
Ishida) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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Application - Astronomy
O-13 First light of DARKNESS: a pathfinder for exoplanet imaging with Microwave Kinetic Inductance
Detectors (Seth R. Meeker, Benjamin A. Mazin, Alex B. Walter, Matthew J. Strader, Neelay Fruitwala,
Clint Bockstiegel, Paul Szypryt, Gerhard Ulbricht, Gregoire Coiﬀard, Bruce Bumble, Giulia Collura,
Rupert Dodkins, Isabel Lipartito, Michael Bottom, J. Chris Shelton, Dimitri Mawet, Gautam Vasisht,
Eugene Serabyn) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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O-14 Development of ’DESHIMA on ASTE’: towards a field test of a submillimeter wave superconducting onchip filterbank spectrometer based on kinetic inductance detectors (Akira Endo, David Thoen, Kenichi
Karatsu, Nuri van Marrewijk, Sjoerd Bosma, Ozan Yurduseven, Nuria Llombart, Masato Naruse, Nozomu Tomita, Junya Suzuki, Akio Taniguchi, Kotaro Kohno, Shun Ishii, Jun Maekawa, Ryohei Kawabe,
Tai Oshima, Kaui Chin, Yoichi Tamura, Tatsuya Takekoshi, Kazuyuki Fujita, Akira Kouchi, Shunichi
Nakatsubo, Teun Klapwijk, Paul van der Werf, Stephen Yates, Andrey Baryshev, Vignesh Murugesan,
Robert Huiting, Jochem Baselmans) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-15 The NIKA2 instrument at 30-m IRAM telescope: performance and results (Andrea Catalano, NIKA
Core Team) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-16 Sensitivity, Dynamic Range, and Multiplexing Requirements of FIR Detectors for the Origins Space
Telescope (OST) (Johannes G Staguhn) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-17 The Athena X-ray Integral Field Unit (X-IFU) (Francois Pajot, Thien Lam Trong, Jan-Willem den
Herder, Luigi Piro, Massimo Cappi ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-18 Design and status of TIME, a mm-wavelength spectrometer array for [CII] intensity mapping (Jonathon
Hunacek, James Bock, C. Matt Bradford, Tzu-Ching Chang, Yun-Ting Cheng, Asantha Cooray, Abigail
Crites, Steve Hailey-Dunsheath, Daewook Kim, Chao-Te Li, Daniel Marrone, Lorenzo Moncelsi, Erik
Shirokoﬀ, Guochao Sun, Isaac Trumper, Anthony Turner, Bade Uzgil, Michael Zemcov ) . . . . . . . .

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MKIDS 3O-19 Modelling the Performance of Single-Photon Counting Kinetic Inductance Detectors (Josie Dzifa Akua
Parrianen, Simon Doyle, Enzo Pascale) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-20 Ultrasensitive kilo-pixel imaging array of photon noise limited Kinetic Inductance Detectors over anoctave of bandwidth for THz astronomy (Juan Bueno, Ozan Yurduseven, Stephen J. C. Yates, Nuria
Llombart, Vignesh Murugesan, Kenichi Karatsu, David J. Thoen, Andrey M. Baryshev, Andrea Neto,
Jochem J. A. Baselmans) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-21 Development of Multi-Chroic MKIDs for Next-Generation CMB Polarization Studies (Bradley R.
Johnson, Daniel Flanigan, Maximilian H. Abitbol, Peter A. R. Ade, Sean Bryan, Hsiao-Mei Cho,
Rahul Datta, Peter Day, Simon Doyle, Kent Irwin, Glenn Jones, Sarah Kernasovskiy, Dale Li, Phil
Mauskopf, Heather McCarrick, Jeﬀ McMahon, Amber Miller, Yanru Song, Carole Tucker ) . . . . . .
O-22 Millimeter-Wave Polarimeters Using Kinetic Inductance Detectors for TolTEC and Beyond (Jason
Edward Austermann, Jiansong Gao, Johannes Hubmayr, Michael Vissers, James Beall, Bradley Dober,
Shannon Duﬀ, Weijie Guo, Gene Hilton, Christopher McKenney, Joel Ullom, Jeﬀ Van Lanen) . . . .

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TES 1
O-23 Quantitatively characterizing sources of energy resolution degradation in TES microcalorimeters ACbiased at MHz frequencies. (Christine Goodwin Pappas, Dan Becker, Douglas Bennett, Johnathon
Gard, John Mates, Dan Schmidt, Daniel Swetz, Joel Ullom) . . . . . . . . . . . . . . . . . . . . . . . .
O-24 Josephson eﬀects in frequency domain multiplexed TES microcalorimeters and bolometers (Luciano
Gottardi, Stephen J. Smith, Hiroki Akamatsu, Jan van der Kuur, Simon R. Bandler, Marcel P. Bruijn,
James A. Chervenak, Jan R. Gao, Roland den Hartog, Brian D. Jackson, Pourya Khosropanah, Antoine
R. Miniussi, Kenichiro Nagayoshi, Marcel Ridder, Jack Sadleir, Kazuhiro Sakai, Nick Wakeham) . . .
O-25 Development of TES microcalorimeters for 10-50 keV using a gold absorber (Haruka Muramatsu,
Tasuku Hayashi, Keisei Maehisa, Yuki Nakashima, Takehiro Kuroiwa, Takahiro Nakayama, Kazuhisa
Mitsuda, Noriko Y Yamasaki ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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TES 2/BolometerO-26 Noise equivalent power and energy resolution of transition-edge sensors with complex thermal models(Ilari Maasilta) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-27 Exploring the eﬀects of size and geometry of normal metal features on the transition shapes andperformance of transition-edge sensor microcalorimeters (Nicholas Wakeham, Joseph S Adams, Simon
R Bandler, James A Chervenak, Aaron M Datesman, Megan E Eckart, Fred M Finkbeiner, Richard L
Kelly, Caroline A Kilbourne, Antoine R Miniussi, Frederick S Porter, John E Sadleir, Kazuhiro Sakai,
Stephen J Smith, Edward J Wassell, Wonsik Yoon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-28 Dependence of transition width on current and critical current in transition-edge sensors (Kelsey M
Morgan, Christine G Pappas, Douglas A Bennett, Johnathon D Gard, James P Hays-Wehle, Gene C
Hilton, Carl D Reintsema, Daniel R Schmidt, Joel N Ullom, Daniel S Swetz ) . . . . . . . . . . . . . .
O-29 Characterization of Mid-Frequency Arrays for Advanced ACTPol (Steve K. Choi ) . . . . . . . . . . .

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O-30 Characterization of Si-membrane TES bolometer arrays for the HIRMES instrument (Emily M. Barrentine, Karwan Rostem, Ari D. Brown, Regis P. Brekosky, Felipe A. Colazo, Nicholas P. Costen, Vorachai
Kluengpho, Stephen F. Maher, Vilem Mikula, Timothy M. Miller, Joseph B. Oxborrow, Elmer H. Sharp,
Tomomi Watanabe, Edward J. Wollack, Wen-Ting Hsieh, S. Harvey Moseley) . . . . . . . . . . . . .
O-31 Characterization of optical transition-edge sensors (Kaori Hattori, Ryo Kobayashi, Shuichiro Inoue,
Daiji Fukuda) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-32 Eliminating anomalous low energy tails in hard X-ray TES microcalorimeters using electroplated
bismuth (Daikang Yan, Ralu Divan, Lisa M. Gades, Timothy J. Madden, Antonino Miceli, Umeshkumar
M. Patel, Orlando Quaranta, Daniel Becker, Douglas A. Bennett, James P. Hays-Wehle, Gene C.
Hilton, Johnathon Gard, John A. B. Mates, Kelsey M. Morgan, Carl D. Reintsema, Daniel R. Schmidt,
Daniel S. Swetz, Joel N. Ullom, Leila Vale) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-33 A Static and Dynamic Physical Model for Deposition of Energy via Cosmic Rays into Sub-Kelvin
Bolometric Detectors (Samantha Lynn Stever, Francois Couchot, Noel Coron, Bruno Maﬀei ) . . . . .

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Application - Dark matter, neutrino and related physics 1
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O-34 New-generation cryogenic detectors for dark matter and coherent neutrino scattering (Raimund Strauss) 46
O-35 Using defect creation to discriminate dark matter signal in phonon-mediated detectors (Fedja Kadribasic, Nader Mirabolfathi, Kai Nordlund, Eero Holmstrom, Flyura Djurabekova) . . . . . . . . . . . . . 47
O-36 The CUORE and CUORE 0 experiments at LNGS: detector performance and physics results (Francesco
Terranova) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 48
O-37 Status and Prospects of the EDELWEISS-III Direct WIMP Search Experiment (Alexandre Juillard,
Edelweiss Collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 49
O-38 XMASS; A Dark Matter Search Experiment with Liquid Xenon (Hiroyuki Sekiya, XMASS collaboration) 50
Application - Dark matter, neutrino and related physics 2
O-39 Low temperature detectors for neutrinoless double beta decay experiments (Yong-Hamb Kim) . . . .
O-40 Search for hidden photon cold dark matter using radio telescopes (Shugo Oguri, Nozomu Tomita,
Taketo Nagasaki, Osamu Tajima, Junya Suzuki, Yoshizumi Inoue, Makoto Minowa) . . . . . . . . . .
O-41 Enhanced Calorimetry Using Helium Evaporation and Field Ionization (George M Seidel, Derek Stein,
Humphrey J Maris) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-42 Status of the HOLMES experiment to directly measure the electron neutrino mass (Angelo Nucciotti, Bradley Alpert, Daniel Becker, Douglas Bennett, Michele Biasotti, Valentina Ceriale, Matteo De
Gerone, Rugard Dressler, Marco Faverzani, Elena Ferri, Joseph Fowler, Giovanni Gallucci, John Gard,
Flavio Gatti, Andrea Giachero, James Hays-Wehle, Stephan Heinitz, Gene Hilton, Ulli Koester, Maurizio Lusignoli, John Mates, Stefano Nisi, Angiola Orlando, Gianluigi Pessina, Andrei Puiu, Stefano
Ragazzi, Carl Reintsema, Maria Ribeiro-Gomes, Dan Schmidt, Dorothea Schumann, Daniel Swetz, Joel
Ullom, Leila Vale) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-43 The Electron Capture in 163 Ho experiment (Clemens Hassel, ECHo-Collaboration) . . . . . . . . . .

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SSPD and related detectors
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O-44 A distributed superconducting nanowire single photon detector for imaging (Qing-Yuan Zhao, Di Zhu,
Niccolo Calandri, Andrew E. Dane, Adam N. McCaughan, Francesco Bellei, Haozhu Wang, Daniel F.
Santavicca, Berggren K. Karl ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 59
O-45 Four-Lead Superconducting Detector Developed for Neutron Radiography (Takekazu Ishida, Hiroaki
Shishido, Hiroyuki Yamaguchi, Yuya Miki, Yuki Iizawa, Kenji M. Kojima, Shigeyuki Miyajima, Mutsuo
Hidaka, Tomio Koyama, Masahide Harada, Kenichi Oikawa, Takayuki Oku, Kazuhiko Soyama) . . . . 60
O-46 Electrothermal modeling of amorphous WSi nanowires (Jason P Allmaras, Alexander G Kozorezov,Andrew D Beyer, Francesco Marsili, Ryan M Briggs, Boris Korzh, Matthew D Shaw ) . . . . . . . . . 61
O-47 High eﬃciency and low dark-count-rate superconducting nanowire single-photon detectors (Lixing You) 62
O-48 Electron-phonon relaxation time in ultrathin tungsten silicon film (Maria Sidorova, A Kozorezov, A
Semenov, A Korneev, Yu Korneeva, M Mikhailov, A Devizenko, G Chulkova , G Goltsman) . . . . . . 63
O-49 Single microwave-photon detector based on superconducting quantum circuits (Kunihiro Inomata, Zhirong Lin, Kazuki Koshino, William D Oliver, Jaw-Shen Tsai, Tsuyoshi Yamamoto, Yasunobu Nakamura) 64
Other low-temperature detectors
O-50 Physics and Applications of Metallic Magnetic Calorimeters (Sebastian Kempf ) . . . . . . . . . . . .
O-51 Single Photon Detection of 1.5THz Radiation with the Quantum Capacitance Detector (Pierre M.
Echternach, Brian J. Pepper, Theodore Reck, C. Matt Bradford ) . . . . . . . . . . . . . . . . . . . . .
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O-52 Development of STJ with FD-SOI cryogenic amplifier as a far-infrared single photon detector for
COBAND experiment (Yuji Takeuchi, Shin-Hong Kim, Takashi Iida, Kenichi Takemasa, Kazuki Nagata, Chisa Asano, Shunsuke Yagi, Rena Wakasa, Hirokazu Ikeda, Takehiko Wada, Koichi Nagase ,Shuji Matsuura , Yasuo Arai, Ikuo Kurachi, Masashi Hazumi , Takuo Yoshida, Takahiro Nakamura,
Makoto Sakai, Wataru Nishimura , Satoshi Mima, Kenji Kiuchi , Hirokazu Ishino, Atsuko Kibayashi ,Yukihiro Kato , Go Fujii, Shigetomo Shiki, Masahiro Ukibe, Masataka Ohkubo , Shoji Kawahito , Erik
Ramberg, Paul Rubinov, Dmitri Sergatskov , Soo-Bong Kim) . . . . . . . . . . . . . . . . . . . . . . .

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Readout Techniques & Signal processing 1
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O-53 Progress in microwave SQUID readout for calorimetric and bolometric sensors (J.A.B. Mates) . . . . 71
O-54 A large-scale demonstration of microwave SQUID multiplexing: the SLEDGEHAMMER TES gammaray microcalorimeter instrument (Dan Becker, D A Bennet, M P Croce, J W Fowler, J D Gard, J P
Hays-Wehle, G C Hilton, A S Hoover, J A B Mates, M W Rabin, C D Reintsema, D R Schmidt, D S
Swetz, L R Vale, J N Ullom) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72
O-55 Microwave SQUID Multiplexing for TES micro-Calorimeters in the High-Speed Limit (James P HaysWehle, Daniel Becker, Douglas A Bennett, John D Gard, Joseph W Fowler, Gene C Hilton, J. A.
Benson Mates, Carl D Reinstema, Daniel R Schmidt, Daniel S Swetz, Leila R Vale, Joel N Ullom) . . 73
O-56 Optimized Readout Electronics for Microwave SQUID Multiplexed MMC Arrays (Oliver Sander,
Sebastian Kempf, Nick Karcher, Oliver Kromer, Mathias Wegner, Matthias Balzer, Thomas Kuhner,
Christian Enss, Marc Weber ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 74
O-57 64 pixel metallic magnetic calorimeter based detector array with integrated microwave SQUID multiplexer (Mathias Wegner, Andreas Fleischmann, Loredana Gastaldo, Daniel Richter, Sebastian Kempf,
Christian Enss) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 75
O-58 Advanced Time- and Code-Division Multiplexers for X-Ray Spectrometer Arrays (Kent D Irwin,
Saptarshi Chaudhuri, Hsiao-Mei Cho, Carl Dawson, Ed Denison, William ”Randy” Doriese, Malcolm
Durkin, Joseph Fowler, John Gard, Gene C Hilton, Young Il Joe, Stephen Kuenstner, Dale Li, Kelsey
Morgan, Carl Reinstema, Robert Stevens, Daniel Swetz, Charles ”Jamie” Titus, Joel Ullom, Betty Young) 76
Readout Techniques & Signal processing 2
O-59 SiGe Integrated Circuit Developments for SQUID/TES Readout (Damien PRELE, Fabrice VOISIN,
Cyril BEILLIMAZ, Si CHEN, Michel PIAT, Andrea GOLDWURM ) . . . . . . . . . . . . . . . . . . .
O-60 Frequency domain multiplexed readout of TES X-ray microcalorimeters for X-IFU on board of Athena(HIROKI AKAMATSU, L. Gottardi, J. van der Kuur, C.P. de Vries, M.P. Bruijn, J.A. Chervenak,
M. Kiviranta, A.J. van den Linden, B.D. Jackson, S.J. Smith) . . . . . . . . . . . . . . . . . . . . . .
O-61 Traveling-wave, lumped-element kinetic inductance parametric amplifier for detector readout (Saptarshi
Chaudhuri, Dale Li, Kent Irwin, Clint Bockstiegel, Johannes Hubmayr, Joel Ullom, Michael Vissers,
Jiansong Gao) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-62 Lithographed superconducting resonator development for next generation frequency multiplexing readout of transition-edge sensors (Farzad Faramarzi, Tijmen de Haan, Akito Kuaka, Adrian Lee, Barbara
Neuhauser, Richard Plambeck, Christopher Raum, Aritoki Suzuki, Ben Westbrook ) . . . . . . . . . . .

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Fabrication & Implementation Techniques 1
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O-63 Design and Fabrication of Large-Area Transition Edge Sensor Detector Arrays for Cosmic Microwave
Background Polarimetry (Shannon M Duﬀ, AdvACT Collaboration, SPIDER Collaboration) . . . . . . 84
O-64 Superconducting Ti/TiN thin films for mm wave absorption (Abdelkader ALIANE, Mathias SOLANA,
Valerie GOUDON, Claire VIALLE, Elaura BAGHE, Laurent CARLE, Wilfried RABAUD, Laurent
SAMINADAYAR, Laurent DUSSOPT, Patrick AGNESE, Nicolas LIO SOON SHUN, Sebastien BECKER,
Pierre RODIERE, Vincent REVERET, Louis RODRIGUEZ ) . . . . . . . . . . . . . . . . . . . . . . . 85
O-65 Parallel plate resonators for kinetic inductance detectors (Gregoire Coiﬀard, Miguel Daal, Paul Szypryt,
Gerhard Ulbricht, Nicholas Zobrist, Benjamin A. Mazin) . . . . . . . . . . . . . . . . . . . . . . . . . 86
Application - CMB 1
O-66 Low Temperature Detectors For Cosmic Microwave Background Research (Johannes Hubmayr ) . . .
O-67 The Advanced ACTPol 27/39 GHz Array (Sara Michelle Simon) . . . . . . . . . . . . . . . . . . . .
O-68 BICEP3 performance overview and design for BICEP Array (Howard Hui ) . . . . . . . . . . . . . . .
O-69 SPT3G: A Multichroic Receiver for the South Pole Telescope (Adam Jonathan Anderson, SPT3G
collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
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O-70 GroundBIRD - observation of CMB polarization with a high-speed scanning and MKIDs (Taketo Nagasaki, Jihoon Choi, Ricardo Tanausu Genova-Santos, Makoto Hattori, Masashi Hazumi, Hikaru Ishitsuka, Kenichi Karatsu, Kenji Kiuchi, Ryo Koyano, Hiroki Kutsuma, Kyoungmin Lee, Satoru Mima,
Makoto Minowa, Makoto Nagai, Masato Naruse, Shugo Oguri, Chiko Otani, Rafael Rebolo, Jose Alberto Rubino-Martin, Yutaro Sekimoto, Munehisa Semoto, Junya Suzuki, Tohru Taino, Osamu Tajima,
Nozomu Tomita, Tomohisa Uchida, Eunil Won, Mitsuhiro Yoshida) . . . . . . . . . . . . . . . . . . .

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Application - CMB 2
O-71 Design, construction, and characterization of the 280 GHz focal plane units for the second flight of theSpider polarimeter (Amanda Stevie Bergman, Spider collaboration) . . . . . . . . . . . . . . . . . . .
O-72 The LiteBIRD Space Mission - Sub-Kelvin Instrument (Aritoki Suzuki, LiteBIRD Collaboration) . .
O-73 Measuring Reionization, Neutrino Mass, and Cosmic Inflation with BFORE (Sean Alan Bryan, Philip
Mauskopf, Mark Devlin, Christopher Groppi, Johannes Hubmayr, Jeﬀ McMahon, John Ruhl, Joaquin
Viera, Calvin Netterfield, Peter Ade, John Bond, Francois Boulanger, Jeﬀrey Filippini, Laura Fissel,
Gilbert Holder, Michael Niemack, Giles Novak, Giampaolo Pisano, Douglass Scott, Juan Soler, Carole
Tucker ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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Fabrication & Implementation Techniques 2
O-74 Progress of Superconducting Electronics in Clean Room for Analog and Digital Superconductivity:
CRAVITY (Masahiro Ukibe, Go Fujii, Nobuyuki Zen, Shigetomo Shiki, Hiroyuki Yamamori, Shuichi
Nagasawa, Mutsuo Hidaka, Satoshi Kohjiro, Masataka Ohkubo) . . . . . . . . . . . . . . . . . . . . . .
O-75 LC filters for FDM readout of the X-IFU TES calorimeter instrument on Athena (Marcel P. Bruijn,
Anton J. van der Linden, Lorenza Ferrari, Luciano Gottardi, Jan van der Kuur, Roland H. den Hartog,
Brian D. Jackson) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-76 The DARKNESS Array: A 10,000 Pixel PtSi MKID Array (Paul Szypryt, Seth R. Meeker, Bruce
Bumble, Gregoire Coiﬀard, Gerhard Ulbricht, Neelay Fruitwala, Alex B. Walter, Miguel Daal, Clint
Bockstiegel, Giulia Collura, Benjamin A. Mazin) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-77 Magnetic Calorimeter Arrays with High Sensor Inductance and Dense Wiring (Thomas R. Stevenson,
Simon R. Bandler, Manuel A. Balvin, Archana M. Devasia, Peter C. Nagler, Stephen J. Smith, Wonsik
Yoon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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Cryogenics and Components 1
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O-78 CUORE, a large cryogenic system for LTDs (Carlo Bucci ) . . . . . . . . . . . . . . . . . . . . . . . . 105
O-79 A continuous 100-mK helium-light cooling system for MUSCAT on the LMT (Thomas L R Brien,
Edgar Castillo-Dominguez, Simon Chase, Simon Doyle) . . . . . . . . . . . . . . . . . . . . . . . . . . 106
Cryogenics and Components 2
O-80 Vibration measurement and mitigation for cryogen-free dilution refrigerators (Chang Lee) . . . . . .
O-81 Electromagnetic Design of a Magnetically-Coupled Spatial Power Combiner (Berhanu T Bulcha,
Cataldo Giuseppe, Stevenson Thomas, U-yen Kongpop, Moseley Samuel, Wollack Edward ) . . . . . .
O-82 A temperature dependent x-ray absorption characterization of test filters for the ATHENA mission
X-IFU instrument (Luisa Sciortino, Ugo Lo Cicero, Salvartore Ferruggia Bonura, Elena Magnano,Stefano Nannarone, Konstantin Koshmak, Antonella Balerna, Marco Barbera) . . . . . . . . . . . . .

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Application - Material analysis and others 1
O-83 Analytical Transmission Electron Microscope using a Transition Edge Sensor for X-ray Microanalysis (Toru Hara, Keiichi Tanaka, Keisuke Maehata, Kazuhisa Mitsuda, Yoshihiro Yamanaka, Mutsuo
Hidaka, Kuniyasu Nakamura) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-84 Ultrafast X-ray Spectroscopies using TES Microcalorimeter Sensors: Recent Table-top Demonstrations
and Current Work (Joel N Ullom, B. K. Alpert, M. Balasubramanian, N. Chen, N. H. Damrauer, W.
B. Doriese, S. M. Fatur, J. W. Fowler, W. K. Fullagar, G. C. Hilton, Y. I. Joe, R. Jimenez, L. MiajaAvila, G. C. O’Neil, B. Ravel, C. D. Reintsema, D. M. Sagar, D. R. Schmidt, K. L. Silverman, D. S.
Swetz, H. Tatsuno, J. Uhlig) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-85 An ultra-sensitive probe of local electronic structures using transition-edge sensor X-ray microcalorimeters at the Stanford Synchrotron Radiation Lightsource (Sang Jun Lee) . . . . . . . . . . . . . . . . .

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Application - Material analysis and others 2
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O-86 A Search for the Decay of Metastable Th-229m with Superconducting Tunnel Junctions (Francisco
Ponce, Erik L. Swanberg, Jason T. Burke, Stephan Friedrich) . . . . . . . . . . . . . . . . . . . . . . . 117
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O-87 TES application to kaonic atom X-ray spectroscopy in a charged-particle beamline (Tadashi Hashimoto,
HEATES collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-88 Calorimetry of Heavy Charged Particle by superconducting transition edge sensor (Masashi Ohno,
Tomoya Irimatsugawa, Yoshitaka Miura, Hiroyuki Takahashi, Tokihiro Ikeda, Chiko Otani, Makoto
Sakama, Naruhiro Matsufuji ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
O-89 A few photon spectral imaging with photon microscope based on optical transition edge sensor (Daiji
Fukuda, Kazuki Niwa, Kaori Hattori, Ryo Kobayashi, Takayuki Numata, Shuichiro Inoue) . . . . . . .
O-90 2d MMC arrays for high resolution x-ray spectroscopy (Andreas Fleischmann, Christian Enss, Loredana
Gastaldo, Jeschua Geist, Daniel Hengstler, Sebastian Kempf, Mattheaus Krantz, Christian Schoetz,
Tobias Gassner, Marc Oliver Herdrich, Renate Maertin, Thomas Stoehlker, Guenter Weber ) . . . . .

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Poster presentations

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Category A : Sensor Physics & Developments
PA-1 Development of Thermal Kinetic Inductance Detectors suitable for X-ray spectroscopy (Andrea Giachero, Angelo Cruciani, Antonello D’Addabbo, Peter K. Day, Sergio Di Domizio, Marco Faverzani,
Elena Ferri, Benno Margesin, Maria Martinez, Renato Mezzena, Lorenzo Minutolo, Angelo Nucciotti,
Andrei Puiu, Marco Vignati ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-2 Fabrication of antenna-coupled KID array for Cosmic Microwave Background detection (Qing Yang
Tang, Peter S. Barry, Vasish Baungally, Amy Lowitz, Ryan McGeehan, Evan Mayer, Rong Nie, Ritoban
Basu Thakur, Erik Shirokoﬀ ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-3 A dual polarization, 1.4 to 2.8 THz Kinetic Inductance Detector, with background limited sensitivity for
future spaced-based far-infrared observatories (Juan Bueno, Ozan Yurduseven, Nuria Llombart, Stephen
J. C. Yates, Vignesh Murugesan, Lorenza Ferrari, David J. Thoen, Andrey M. Baryshev, Andrea Neto,
Jochem J. A. Baselmans) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-4 Study on the electronic properties of Al thin-film superconducting resonators at low temperatures(Takashi Noguchi, Agnes Dominjon, Yutaro Sekimoto) . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-5 Dual-polarization LEKIDs for CMB Polarimetry (Heather McCarrick, Maximilian H. Abitbol, Peter
A.R. Ade, Sean Bryan, Peter Day, Thomas Essinger-Hileman, Daniel Flanigan, Glenn Jones, Henry
G. Leduc, Michele Limon, Bradley R. Johnson, Philip Mauskopf, Amber Miller, Suzanne Staggs, Carole
Tucker ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-6 CALDER: Phonon-mediated Kinetic Inductance light detectors (Marco Vignati, Fabio Bellini, Martino
Calvo, Laura Cardani, Nicola Casali, Maria Gabriella Castellano, Ivan Colantoni, Carlo Cosmelli,Angelo Cruciani, Antonio D’Addabbo, Sergio Di Domizio, Johannes Goupy, Helene Le Sueur, Maria
Martinez, Lorenzo Minutolo, Alessandro Monfardini ) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-7 Mitigation of cosmic ray eﬀect on Microwave Kinetic Inductance Detectors (Kenichi Karatsu, Akira
Endo, Juan Bueno, David J. Thoen, Vignesh Murugesan, Nozomu Tomita, Eduard F.C. Driessen,
Gregoire Coiﬀard, Jochem J.A. Baselmans) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-8 Development of an MKIDs-Based THz Superconducting Imaging Array (TeSIA) at 0.85 THz (ShengCai SHI, Jing Li, Zhen-Hui Lin, Jin-Ping Yang, Dong Liu, Wen-Ying Duan, Zheng Lou, Qing Shi, Zhi
Li, Wei Miao, Wen Zhang, Qi-Jun Yao) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-9 Titanium nitride for kinetic-inductance detectors: a problematic material or an engineering opportunity? (Eduard F.C. Driessen) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-10 Update on TKIDs: Thermal Kinetic Inductance Detectors for X-ray imaging spectroscopy (Gerhard
Ulbricht, Miguel Daal, Paul Szypryt, Alex B. Walter, Clint Bockstiegel, Benjamin A, Mazin) . . . . .
PA-11 Projection of Cosmic Microwave Background anisotropy measurements for Microwave Kinetic Inductance Devices (Ritoban Basu Thakur ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-12 AlMn LEKIDs for millimeter-wave astronomy below 100 GHz (Hsiao-Mei Cho, Glenn Jones, Max
H. Abitbol, Peter A. R. Ade, Sean Bryan, Peter Day, Daniel Flanigan, Kent D. Irwin, Bradley R.
Johnson, Dale Li, Philip Mauskopf , Heather McCarrick , Amber Miller, Yanru Song, Carole Tucker )PA-13 Antenna-coupled lumped-element kinetic inductance detectors for CMB observations (Erik Shirokoﬀ,
Peter S. Barry, Evan Mayer, Amy Qing Yang Tang, Simon Doyle) . . . . . . . . . . . . . . . . . . . .
PA-14 Coherent excited states in superconductors due to a microwave field - microscopic perspective on
microwave nonlinearity (A.V. Semenov, I.A. Devyatov, P.J. de Visser, T.M. Klapwijk ) . . . . . . . .
PA-15 Operation of a superconducting nanowire in two detection modes: KID and SPD (Edward Schroeder,
Philip Mauskopf, Hamdi Mani, Karl Berggren, Di Zhu) . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-16 A Superconducting Phase Shifter and On-Chip Fourier Transform Spectrometer for W-Band Astronomy (George Che, Samuel Gordon, Philip Mauskopf, Harshad Surdi, Georgios Trichopoulos) . . . . . .

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PA-17 A broadband antenna for on-chip integrated spectrometers at 300-900 GHz (Sebastian Hahnle, Ozan
Yurduseven, Nuria Llombart, Juan Bueno, Vignesh Murugesan, David Thoen, Jochem Baselmans) . . 144
PA-18 Development of the Kinetic Inductance Detector Spectrograph (KIDSpec) prototype (Sumedh Mahashabde, Kieran O’Brien, Rupert Dodkins, Ghassan Yassin, Ian Hepburn, Jo Bartlett, Graham Hardy,
Ben Mazin) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145
PA-19 MoBiKID - Kinetic Inductance Detectors for upcoming B-mode satellite missions (Angelo Cruciani ) 146
PA-20 Electron-phonon coupling in Ti/TiN MKIDs multilayer microresonator (Marco Faverzani, Angelo
Cruciani, Antonio D’Addabbo, Sergio Di Domizio, Peter Kenneth Day, Elena Ferri, Andrea Giachero,
Benno Margesin, Maria Martinez, Renato Mezzena, Lorenzo Minutolo, Angelo Nucciotti, Andrei Puiu,
Marco Vignati ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 147
PA-21 Prototype high angular resolution LEKIDs for NIKA2 (Shibo Shu, Samuel Leclercq, Alessandro
Monfardini, Eduard Driessen) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 148
PA-22 Polarization filter for microstrip lumped-element kinetic inductance detectors (Alicia Gomez, Martino
Calvo, Johannes Goupy, Aurelien Bideaud, Florence Levy-Bertrand, Andrea Catalano, Alain Benoit,
Andrea Tartari, Alessandro Monfardini ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 149
PA-23 Dual-color antenna-coupled LEKID for next generation CMB focal planes (Alessandro Traini, Andrea
Tartari, Guillaume Bordier, Faouzi Boussaha, Christine Chaumont, Samir Beldi, Florent Reix, Michel
Piat) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 150
PA-24 Optimisation of an antenna-coupled LEKID for future ground-based CMB experiments (Amber Loren
Hornsby, Peter Stuart Barry, Simon Doyle, Erik Shirokoﬀ ) . . . . . . . . . . . . . . . . . . . . . . . . 151
PA-25 Investigation of Single Crystal Niobium for Microwave Kinetic Inductance Detectors (Agnes Dominjon,
Shibo Shu, Matthias Kroug, Takashi Noguchi, Yutaro Sekimoto, Tom Nitta, Shigeyuki Sekiguchi, Wenlei
Shan) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 152
PA-26 Design of Near Infrared and Visible Kinetic Inductance Detectors using MIM Capacitors (Samir
Beldi, Faouzi Boussaha, Christine Chaumont, Shan Mignot, Florent Reix, Andrea Tartari, Michel Piat,
Piercarlo Bonifacio) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 153
PA-27 A TiN/Ti/TiN Trilayer Lumped Element KID Array for CMB Polarimetry at 100 GHz (Amy E
Lowitz, Ari D Brown, Vilem Mikula, Thomas R Stevenson, Peter T Timbie, Edward J Wollack ) . . . 154
PA-28 Ultra Low-NEP FIR LEKIDs: a Three-Pronged Approach (Adalyn Fyhrie, Jason Glenn, Henry
Leduc, Peter Day, Byeong Ho Eom, Jonas Zmuidzinas, Christopher McKenney) . . . . . . . . . . . . 155
PA-29 Optimization of geomagnetic shielding for MKIDs mounted on rotating cryostat (Hiroki Kutsuma,
Makoto Hattori, Kenji Kiuchi, Satoru Mima, Taketo Nagasaki, Shugo Oguri, Junya Suzuki, Osamu
Tajima) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 156
PA-30 Proposal of a kinetic inductance current amplifier with coplanar waveguide input structure for magnetic flux focusing (Gensheng Wang, Clarence Chang, Thomas Cecil, Valentine Novosad, Steve Padin,
Volodymyr Yefremenko) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 157
PA-31 Disk Resonator Format for Kinetic Inductance Detectors (Nicholas Zobrist, Miguel Daal, Bernard
Sadoulet, Ben Mazin) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 158
PA-32 Design and characterization of titanium nitride subarrays of Kinetic Inductance Detectors for passive
terahertz imaging (Dmitry Morozov, Simon Doyle, Archan Banerjee, Thomas Brien, Robert H Hadfield,
Dilini Hemakumara, Iain Thayne) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 159
PA-33 Multilayer Readout Wiring for Transition Edge Sensor Calorimeter Arrays Using Chemical Mechanical
Polishing (Kengo Kosaka, Yuichiro Ezoe, Seiichi Kitazawa, Ryota Hayakawa, Koji Nunomura, Takaya
Ohashi, Yshitaka Ishisaki, Shinya Yamada, Mutsuo Hidaka, Tetsuro Satoh, Kazuhisa Mitsuda) . . . . 160
PA-34 An on-chip filter bank spectrometer based on Transition Edge Sensors for meteorology and climatology(Ben Flatman, Peter Hargrave, Staﬀord Withington, Stefan Buhler, Lukas Kluft, Prateek Kumar Dongre)161
PA-35 Advanced ACTPol TES Device Parameters and Noise Performance in Three Fielded Arrays (Kevin
T. Crowley, AdvACT Collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 162
PA-36 Development of gamma-ray position-sensitive transition-edge-sensor microcalorimeters (Naoko Iyomoto, Yuki Shuto, Takehiro Kuroiwa, Yuta Kurume, Yu Kiguchi, Keisuke Maehata, Tasuku Hayashi,
Haruka Muramatsu, Kazuhisa Mitsuda, Shota Yoshimoto, Akira Takano) . . . . . . . . . . . . . . . . 163
PA-37 Dark characterization and comparison of various Mo/Au based TESs (Carlos Pobes, Lourdes Fabrega, Agustin Camon, Nieves Casan-Pastor, Pavel Strichopanec, Javier Sese, Javier Moral-Vico, Rosa
Jaudenes) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 164
PA-38 Twin-slot antenna coupled superconducting Ti transition edge sensor at 350 GHz (Wen Zhang, Wei
Miao, Zheng Wang, Xiao-Hui Guo, Dong Liu, Jia-Qiang Zhong, Qi-Jun Yao, Sheng-Cai Shi ) . . . . . 165
PA-39 Magnetic Sensitivity of AlMn TESes and Shielding Considerations for Next Generation CMB Surveys(Eve Marie Vavagiakis, Shawn Wesley Henderson, Michael D Niemack, Kaiwen Zheng) . . . . . . . . 166
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PA-40 Study of Dissipative Losses in AC-Biased Mo/Au Bilayer Transition-Edge Sensors (Kazuhiro Sakai,Joseph S Adam, Simon R Bandler, James A Chervenak, Aaron M Datesman, Megan E Eckart, Fred M
Finkbeiner, Richard L Kelly, Antoine R Miniussi, Frederick S Porter, Caroline A Kilbourne, John E
Sadleir, Stephen J Smith, Nicholas A Wakeham, Edward J Wassell, Wonsik Yoon, Hiroki Aakamatsu,
M P Brujin, Luciano Gottardi, Brian D Jackson, Jan van der Kuur, Bert-Joost van Leeuven, A J van
der Linden, Henk J van Weers, Mikko Kiviranta) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-41 Development of TiAu TES X-ray calorimeters for the X-IFU on ATHENA space observatory (Pourya
Khosropanah, L. Gottardi, C. P. de Vries, K. Nagayoshi, M. L. Ridder, H. Akamatsu, M. P. Bruijn,
J. R. Gao) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-42 The succesfull readout of the 176 TES FDM system for SAFARI (Richard Arnold Hijmering, Damian
Audley, Roland den Hartog, Marcel Ridder, Anthony J. van der Linden, Brian Jackson, Jan van derKuur, Marcel Bruijn, Jian-Rong Gao) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-43 Design of the EBEX-IDS Instrument and Detectors (Francois Aubin, Shaul Hanany, Bradley Johnson,
Adrian Lee, Aritoki Suzuki, Benjamin Westbrook, Karl Young) . . . . . . . . . . . . . . . . . . . . . .
PA-44 Does membrane strain impact the TES transition surface? (Felix T Jaeckel, C V Ambarish, Megan
Eckart, Rachel Gruenke, Kari L Kripps, Dan McCammon, Dallas Wulf, Shuo Zhang, Yu Zhou) . . . .
PA-45 Optical Characterization of the SPT-3G Focal Plane (Zhaodi Pan, SPT-3G collaboration SPT-3G
collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-46 Spectroscopic measurements of L X-rays with a TES microcalorimeter for a non-destructive assay oftransuranium elements (Keisuke Nakamura, Keisuke Maehata, Tetsuya Sugimoto, Yu Kiguchi, Naoko
Iyomoto, Yuki Morishita, Koji Takasaki, Kazuhisa Mitsuda) . . . . . . . . . . . . . . . . . . . . . . . .
PA-47 Performance of an X-ray absorber on a transition edge sensor for Athena/X-IFU (Kenichiro Nagayoshi,
Marcel Ridder, Marcel Bruijn, Pourya Khosropanah, Cor de Vries, Luciano Gottardi, Jian-Rong Gao)
PA-48 Development of cryogenic single photon TES detectors for an Investigation of the VUV region.
(Valentina Ceriale, Flavio Gatti, Matteo De Gerone, Michele Biasotti, Giovanni Gallucci, Daniele
Grosso) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-49 Mapping the TES Temperature and Current Sensitivities as a Function of Current, Magnetic Field
and Temperature with IV Curve and Complex Impedance (Yu Zhou, Felix T Jaeckel, C V Ambarish,
Megan Eckart, Rachel Gruenke, Kari L Kripps, Dan McCammon, Dallas Wulf, Shuo Zhang) . . . . .
PA-50 Performance of an X-ray microcalorimeter with a 0.24 mm absorber and a 50 um TES bilayer (Antoine
R. Miniussi, Joseph S. Adam, Simon R. Bandler, James A. Chervenak, Aaron M. Datesman, Megan
E. Eckart, Audrey J. Ewin, Fred M. Finkbeiner, Richard L. Kelley, Caroline A. Kilbourne, Frederick S.
Porter, John E. Sadleir, Kazuhiro Sakai, Stephen J. Smith, Nicholas A. Wakeham, Edward J. Wassell,
Wonsik Yoon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-51 Exploration of alternative Transition Edge Sensor materials for the SPT-3G experiment (Clarence L
Chang, SPT-3G collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-52 Transition edge sensor (TES) array for astrophysical observations (Guanhua Gao, Kamal Ahmad,
Zhengwei Li, Jie Liu, Qichun Liu, Jianshe Liu, Wei Chen) . . . . . . . . . . . . . . . . . . . . . . . .
PA-53 Fabrication and Characterization of Al/Ti bilayer Transition Edge Sensor Bolometer Array (Kamal
Ahmad, Guanhua Gao) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-54 Development of a small pixel Ir-TES for optical applications (Yoshitaka Miura, Tomoya Irimatsugawa,Yuya Ishii, Masashi Ohno, Hiroyuki Takahashi ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-55 Understanding and Manipulating the Thermal Conductance of SiN Membranes in Sub-Kelvin Refrigerators and Sensors (Xiaohang Zhang, Peter Lowell, Joel Ullom) . . . . . . . . . . . . . . . . . . .
PA-56 A low nuclear recoil energy threshold for dark matter search with CRESST-III detectors (Michele
Mancuso, on behalf of the CRESST collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-57 Two-Dimensional Spatial Imaging of Charge Transport in Silicon at Low Temperature (Robert A
Moﬀatt, Blas Cabrera, Noah Kurinsky, James Allen, Peter Redl, Brendan Corcoran, Fedja Kadribasic, Benjamin Shank, Betty Young, Matthew Cherry, John Mark Kreikebaum, Astrid Tomada, Kyle
Sundqvist, Bernard Sadoulet, Daniel Brandt, Paul Brink ) . . . . . . . . . . . . . . . . . . . . . . . . .
PA-58 Progress on SuperSpec (Jordan Wheeler, Steve Hailey-Dunsheath, Erik Shirokoﬀ, Peter Barry,
Charles M Bradford, Scott Chapman, George Che, Jason Glenn, Matthew Hollister, Attila Kovacs,
Henry G Leduc, Philip Mauskopf, Ryan McGeehan, Christopher M McKenney, Roger O’Brient, Stephen
Padin, Theodore Reck, Colin Ross, Corwin Shiu, Carole Tucker, Ross Williamson, Jonas Zmuidzinas)
PA-59 MgB2 hot-electron bolometer mixers for sub-mm wave astronomy (Evgenii Novoselov, Sergey Cherednichenko) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PA-60 Integrated SQUID/sensor designs for metallic magnetic microcalorimetry (Stephen T. P. Boyd, Ruslan
Hummatov, Geon Bo Kim, John Ad Hall, Robin C Cantor, Stephan Friedrich) . . . . . . . . . . . . .
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PA-61 Metallic magnetic calorimeter optimization for large-area light detectors (Seung-Yoon Oh, Yong-Hamb
Kim, Hyelim Kim, Inwook Kim, Sora Kim, Hyejin Lee, Minkyu Lee) . . . . . . . . . . . . . . . . . . . 188
PA-62 BRAHMS: POLARIZATION SENSITIVE BOLOMETER ARRAYS FOR THE SPICA IMAGING
POLARIMETER (Louis R Rodriguez, Albrecht Poglitsch, Vincent Reveret, Didier Dubreuil, Abdelkader
Aliane, Olivier Gevin, Bruno Maﬀei, Xavier De la Broise, Jerome Martignac, Lionel Duband, Valerie Goudon, Wilfried Rabaud, Ivan Charles, Christophe Cara, Cyrille Delisle, Obaid Adami, Sophie
Bounissou, Agnes Arnaud, Laurent Dussopt, Amin Rhouni, Jean-Luc Sauvageot) . . . . . . . . . . . . 189
PA-63 Wavelength dependence of intrinsic detection eﬃciency for NbN superconducting nanowire singlephoton detector (Hao Li, Lixing You, Yong Wang, Zhen Wang) . . . . . . . . . . . . . . . . . . . . . 190
PA-64 A model on heat signal of crystal detector at low temperature (Jin Li, Inwook Kim) . . . . . . . . . 191
PA-65 Characteristics of IF bandwidth of NbN Superconducting Tunneling Junction Mixers (Dong Liu, Jie
Hu, Wei Tao Lv, Jing Li, Sheng Cai Shi ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 192
PA-66 NTLE cryogenic light detectors with planar electrode geometry - latest results (Elizabeth Mondragon,
Xavier Defay, Angelina Kinast, Alexander Langenkamper, Jean-Come Lanfranchi, Erik Lindner, Andrea Munster, Tobias Ortmann, Walter Potzel, Stefan Schonert, Andreas Ulrich, Stephan Wawoczny,Michael Willers) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 193
PA-67 Design and fabrication of mid-infrared superconducting hot-electron bolometers (Akira Kawakami,
Hisashi Shimakage, Junsei Horikawa, Masaharu Hyodo, Shingo Saito, Shukichi Tanaka, Yoshinori Uzawa)194
PA-68 Progress towards Photon Counting Detectors for Terahertz Astronomy (Hajime Ezawa, Hiroshi
Matsuo, Masahiro Ukibe, Go Fujii, Shigetomo Shiki ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . 195
PA-69 A Graphene Based Terahertz Hot Electron Bolometer with Johnson Noise Readout (Wei Miao, Hao
GAO, Zheng WANG, Wen ZHANG, Yuan REN, Kangmin ZHOU, Shengcai SHI, Cui YU, Zezhao HE,
Qinbing LIU, Zhihong FENG) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 196
PA-70 HIGH-PRECISION X-RAY SPECTROSCOPY OF HIGHLY-CHARGED IONS AT STORAGERINGS USING SILICON MICROCALORIMETERS (Pascal A. Scholz, Victor Andrianov, Alexander
Bleile, Artur Echler, Peter Egelhof, Oleg Kiselev, Saskia Kraft-Bermuth, Damian Mull ) . . . . . . . . 197
PA-71 Temperature Study of the DC IV curves of NbN Superconducting Nanowire Single Photon Detectors(Andrew Dane, Di Zhu, Emily Toomey, Marco Colangelo, Qingyuan Zhao, Karl Berggren) . . . . . . . 198
PA-72 Axion search experiment by using Josephson-Junction device (Atsushi Tokiyasu, Kennichi Karatsu,
Kenji Kiuchi, Satoru Mima, Katsuro Nakamura) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 199
PA-73 The DM Radio Pathfinder experiment: searching for dark matter from 500 peV to 50 neV (Stephen
Erwin Kuenstner, Saptarshi Chaudhuri, Hsaio-Mei Cho, Carl Dawson, Peter Graham, Kent D. Irwin,
Dale Li, Harvey Moselely, Arran Phipps, Maximiliano Silva-Feaver, Betty Young) . . . . . . . . . . . 200
PA-74 Characterization of doped silicon thermometers for cryogenic bolometers ( Obaid Adami, Louis Rodriguez, Abdelkader Aliane, Albrecht Poglitsch, Jean-Luc Sauvageot, Valerie Goudon, Laurent Dussopt,
Vincent Reveret) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 201
PA-75 Electromagnetic Simulations of newly designed semiconductor bolometers for submillimeter observations (Sophie Bounissou, Vincent Reveret, Louis Rodriguez, Albrecht Poglitsch, Abdelkader Aliane,
Obaid Adami, Valerie Goudon, Laurent Dussopt, Wilfried Rabaud ) . . . . . . . . . . . . . . . . . . . . 202
PA-76 Development of a Dielectric Microcalorimeter with Quantum Ferroelectric Materials (Shota YOSHIMOTO, Keisuke MAEHATA, Naoko IYOMOTO, Kazuhisa MITSUDA, Noriko YAMASAKI ) . . . . . 203
PA-77 Accurate Measurement of Gain Saturation of Superconductor-Insulator-Superconductor (Wenlei
Shan, ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 204
PA-78 Study for the Operating Principle of Superconducting Strip Photon Detectors (SSPDs) (Nobuyuki
Zen, Yutaka Abe, Go Fujii, Yuma Tomitsuka, Yuki Yamanashi, Yasunori Mawatari, Nobuyuki Yoshikawa)205
PA-79 MOCCA: A 4k-pixel molecule camera for the position and energy resolving detection of neutral
molecular fragments at the Cryogenic Storage Ring CSR (Lisa Elena Gamer, Steﬀen Allgeier, Klaus
Blaum, Christian Enss, Andreas Fleischmann, Loredana Gastaldo, Sebastian Kempf, Oldrich Novotny,
Dennis Schulz, Andreas Wolf ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 206
PA-80 Tantalum STJ X-ray Detectors with an Energy Resolution Limited by Charge Statistics (Matthew
Hollis Carpenter, Francisco Ponce, Stephan Friedrich, Robin Cantor ) . . . . . . . . . . . . . . . . . . 207
PA-81 Development of metallic magnetic calorimeters with critical temperature switch for AMoRE experiment (Sora Kim, Yong-Hamb Kim, Hyonsuk Jo, JinA Jeon, Chan Seok Kang, Hyelim Kim, Inwook
Kim, Heyjin Lee, Minkyu Lee, Sung Hoon Lee, Seung-Yoon Oh) . . . . . . . . . . . . . . . . . . . . . . 208
PA-82 Thermal modelling and experimental results on NTD heat signals for Ge macro-bolometers (Julien
Billard, Dimitri Misiak, Romain Maisonobe, Alexandre Juillard, Maryvonne De Jesus, Claudia Nones,
Anastasiia Zolotarova, Stefanos Marnieros, Louis Dumoulin) . . . . . . . . . . . . . . . . . . . . . . . 209
xiPA-83 Statistical approach to the investigation of dark counts in Superconducting Nanostrip Single Photon
Detectors (Mikkel Ejrnaes, Lapo Lolli, Emanuele Taralli, Mauro Rajteri, Eugenio Monticone, Loredana
Parlato, Giampiero Pepe, Alessandro Casaburi, Robert H Hadfield, Roberto Cristiano) . . . . . . . . . 210
PA-84 Low loss submillimeter wave coplanar waveguide made of superconducting NbTiN on sapphire substrate (Nuri van Marrewijk, Akira Endo, Kenichi Karatsu, Stephen Yates, Masato Naruse, Junya
Suzuki, David Thoen, Vignesh Murugesan, Jochem Baselmans) . . . . . . . . . . . . . . . . . . . . . . 211
PA-85 NTD-Ge production in the LUMINEU experiment using cryogenic detectors for Rare Events searches
and other applications (Xavier Francois Navick, Cyril Bachelet, Stephane Bouillaguet, David Bouville,
Noel Coron, Laurent Devoyon, Antoine Egele, Andrea Giuliani, Mathieu Lemaitre, Martin Loidl, Pierrede Marcillac, Claudia Nones, Yves Penichot, Matias Rodrigues) . . . . . . . . . . . . . . . . . . . . . . 212
Category B : Readout Techniques & Signal processing
PB-1 Development of a data acquisition system for kinetic inductance detectors: wide dynamic range andhigh sampling rate for astronomical observation (Junya Suzuki, Hikaru Ishitsuka, Kyungmin Lee, Shugo
Oguri, Osamu Tajima, Nozomu Tomita, Mitsuhiro Yoshida, Eunil Won) . . . . . . . . . . . . . . . . .
PB-2 In-orbit performance of the pulse shape processor of ASTRO-H SXS (Masahiro Tsujimoto, Makoto
S. Tashiro, Yoshitaka Ishisaki, Shinya Yamada, Hiromi Seta, Kazuhisa Mitsuda, Megan E. Eckart,
Maurice A. Leutenegger, Caroline A. Kilbourne, Frederick Scott Porter, Richard L. Kelley, Takashi
Okajima) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-3 Crosstalk in an FDM laboratory set-up and the Athena X-IFU science performance (Roland den
Hartog, Christian Kirsch, Cor de Vries, Hiroki Akamatsu, Thomas Dauser, Philippe Peille, Eduardo
Cucchetti, Brian Jackson, Jorn Wilms, Simon Bandler ) . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-4 Evaluation and Improvement of Nb and NbN Microwave SQUID multiplexers for a gamma-ray TES
with a Sn Absorber linked by Au Post (Tomoya Irimatsugawa, Fuminori Hirayama, Hirotake Yamamori,
Satoshi Kohjiro, Akira Sato, Shuichi Nagasawa, Daiji Fukuda, Mutsuo Hidaka, Yasushi Sato, Masashi
Ohno, Hiroyuki Takahashi ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-5 Toward a 2000-channel Microwave SQUID Multiplexed Unit for Transition-Edge Sensor Bolometer
Arrays (Bradley Jerald Dober, Jason Austermann, James Beall, Dan Becker, Douglas Bennett, Shannon
Duﬀ, Jiansong Gao, Jonathon Gard, James Hays-Wehle, Gene Hilton, Johannes Hubmayr, John A. B.
Mates, Christopher McKenney, Joel Ullom, Jeﬀ Van Lanen, Michael Vissers) . . . . . . . . . . . . . .
PB-6 Development of a cryogenic capacitive trans-impedance amplifier based on FD-SOI CMOS (Koichi
Nagase, Takehiko Wada, Yasuo Arai, Hirokazu Ikeda, Shunsuke Baba, Toyoaki Suzuki, Morifumi Ohno,
Takahiro Ishimaru) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-7 A Second Generation Digital Readout for Large Photon Counting UVOIR MKID Arrays (Neelay H
Fruitwala, Matthew J Strader, Alex B Walter, Gustavo I Cancelo, Ted J Zmuda, Kenneth R Treptow,
Neal G Wilcer, Benjamin A Mazin) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-8 Series SQUID Array Amplifiers Optimized for MHz Frequency-Domain Multiplexed Detector Readout(Stephan T. P. Boyd, John Ad Hall, Robin C Cantor ) . . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-9 SLAC Microresonator Radio Frequency (SMuRF) Electronics for read out of Frequency-DivisionMultiplexed Cryogenic Sensors (Zeeshan Ahmed, SMuRF collaboration) . . . . . . . . . . . . . . . . .
PB-10 Firmware Development for Microwave SQUID Multiplexer Readout (Johnathon D Gard, Dan Becker,
Douglas A Bennett, Joseph W Fowler, Gene C Hilton, John A. B. Mates, Carl D Reintsema, Dan
Schmidt, Dan Swetz, Joel N Ullom, Leila R Vale, Jim P Hays-Wehle) . . . . . . . . . . . . . . . . . .
PB-11 Development of Microwave Multiplexer Readout System Based on SQUIDs Directly Coupled toResonators for TES X-ray Microcalorimeter (Yuki Nakashima, Fuminori Hirayama, Satoshi Kohjiro,
Hirotake Yamamori, Shuichi Nagasawa, Akira Sato, Noriko Yamasaki, Kazuhisa Mitsuda) . . . . . . .
PB-12 Investigation of SIS up-converter for use in multi-pixel receivers (Yoshinori Uzawa, Takafumi Kojima,
Wenlei Shan, Alvaro Gonzalez, Matthias Kroug) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-13 Active tuning of the resonance frequencies of LC bandpass filters for frequency domain multiplexed
readout of TES detector arrays (Jan van der Kuur, L.G. Gottardi, H.A. Akamatsu, B.J. van Leeuwen,
A.C.T. Nieuwenhuizen, R.H. den Hartog, M.P. Bruijn, A.J. van der Linden, B.D. Jackson) . . . . . .
PB-14 Development of semi-rigid superconducting coaxial cables with normal-conductor-clad center conductor (Akihiro Kushino, Tetsuya Okuyama, Soichi Kasai ) . . . . . . . . . . . . . . . . . . . . . . . . . .
PB-15 Superconducting multilayer high density flexible PCB for very high thermal resistance interconnection(Xavier de la Broise, Alain Le Coguie, Jean-Luc Sauvageot, Vincent Moreau, Samuel d’Hollosy) . . .
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PB-16 Acquisition System of Nobeyama MKID Camera (Makoto Nagai, Shunsuke Hisamatsu, Guangyuan
Zhai, Tom Nitta, Naomasa Nakai, Nario Kuno, Yousuke Murayama, Shogo Hattori, Pranshu Mandal,
Yutaro Sekimoto, Hitoshi Kiuchi, Takashi Noguchi, Hiroshi Matsuo, Agnes Dominjon, S Sekiguchi,
Masato Naruse, Jun Maekawa, Tetsuhiro Minamidani, Masao Saito) . . . . . . . . . . . . . . . . . . . 232
PB-17 Frequency Domain Multiplexing Readout with a Self-Trigger System for Kinetic Inductance Detector
Pulse Signals (Yousuke Yamada, Hirokazu Ishino, Atsuko Kibayashi, Yosuke Kida, Naoto Hidehira,
Kunimoto Komatsu, Masashi Hazumi, Nobuaki Sato, Kazuhiro Sakai, Hirotake Yamamori, Fuminori
Hirayama, Sasoshi Kohjiro) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 233
PB-18 Design and Assembly of SPT-3G Cold Readout Hardware (Jessica Avva, SPT-3G Collaboration ,DfMux Collaboration ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 234
PB-19 Automated Measurements for the Characterization of SQUID-Based Time-Division Multiplexing
Chips (C.S. Dawson, S. Chaudhury, H.-M. Cho, J. Gard, G. Hilton, K. Irwin, S. Kuenstner, D. Li, C.
Reintsema, C.J. Titus, B.A. Young) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 235
PB-20 Development of cross-talk suppression algorithm for MKID readout (Kyungmin Lee, Jihoon Choi,
Makoto Hattori, Masashi Hazumi, Hikaru Ishitsuka, Kenichi Karatsu, Kenji Kiuchi, Ryo Koyano,Hiroki Kutsuma, Jose Alberto Rubino Martin, Satoru Mima, Makoto Minowa, Makoto Nagai, Taketo
Nagasaki, Masato Naruse, Shugo Oguri, Chiko Otani, Rafael Rebolo, Ricardo T. Genova Santos, Yutaro
Sekimoto, Munehisa Semoto, Junya Suzuki, Tohru Taino, Osamu Tajima, Nozomu Tomita, Tomohisa
Uchida, Eunil Won, Mitsuhiro Yoshida) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 236
PB-21 Evaluating and Understanding Crosstalk in Microwave SQUID Multiplexers (Douglas A. Bennett,
Dan Becker, Joseph W. Fowler, Johnathon D. Gard, James P. Hays-Wehle, Gene C. Hilton, John A.
B. Mates, Carl D. Reintsema, Daniel R. Schmidt, Daniel S. Swetz, Leila R. Vale, Joel N. Ullom) . . . 238
PB-22 Error Correcting Codes for code-division multiplexed TES detectors (Charles James Titus, Saptarshi
Chaudhuri, Hsiao-Mei Cho, Carl Dawson, W. Bertrand Doriese, Joe W. Fowler, Gene C. Hilton, Kent
D. Irwin, Stephen Kuenstner, Dale Li, Kelsey Morgan, Carl Reintsema, Dan Swetz, Joel Ullom, Betty
Young) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 239
PB-23 SQUID Characterization for Next Generation Digital Frequency Domain Multiplexing (Maximiliano
Silva-Feaver, Kam Arnold ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 240
PB-24 Combined operation of two TESs for front-end signal processing and amplification (Hiroyuki Takahashi, Yoshitaka Miura, Masashi Ohno) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 241
PB-25 Framework for Analyzing Events at High Rates in TES Microcalorimeters (Bradley K Alpert, W.
Bertrand Doriese, Joseph W. Fowler, Young I. Joe, Kelsey M. Morgan, Galen C. O’Neil, Joel N. Ullom,
Daniel S. Swetz ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 243
PB-26 Thermal conductance and high frequency properties of cryogenic normal or superconucting semi-rigid
coaxial cables in a range of 1 and 8 K (Akihiro Kushino, Soichi Kasai, Masahiro Ukibe, Masataka Ohkubo)244
PB-27 High count-rate study of TES X-ray microcalorimeters with two diﬀerent Tc’s (Sang Jun Lee ) . . . 245
PB-28 Toward large FOV high-resolution x-ray imaging spectrometers: microwave multiplexed readout of
32 TES microcalorimeters (Wonsik Yoon, Joseph S. Adams, Simon R. Bandler, James A. Chervenak,
Aaron Datesman, Megan E. Eckart, Fred M. Finkbeiner, Richard Kelly, Caroline A. Kilnourne, Antoine
R. Miniussi, Frederick S. Porter, John E. Sadleir, Kazuhiro Sakai, Stephen J. Smith, Nicholas A.
Wakeham, Edward Wassell, Samuel H. Moseley, Omid Noroozian, Thomas R. Stevenson, Edward J.
Wollack, Douglas A. Bennett, Dan Becker, Joseph D. Fowler, Johnathon D. Gard, Gene C. Hilton,
John A.B. Mates, Carl D. Reintsema, Daniel S. Swetz, Joel N. Ullom, Leila R. Vale) . . . . . . . . . 246
PB-29 A high-throughput automated test system for dc parametric evaluation and quality assurance of TDM
and CDM SQUID multiplexers (Carl D Reintsema, Doug A Bennett, Ed Dennison, Malcolm Durkin,
William B Doriese, Joseph D Fowler, Johnathan D Gard, Arpi Grigorian, Jim Hays-Wehle, Gene C
Hilton, Johannes Hubmayr, Galen C O’Neil, John A B Mates, Kelsey M Morgan, Dan Schmidt, Robert
Stevens, Leila R Vale, Joel N Ullom, Kent D Irwin, Saptarshi Chaudhuri, Carl Dawson, C J Titus) . 247
PB-30 Cryotron Switches for Current-Summed Code-Division Multiplexing in TES Arrays (Joel Weber,Peter Lowell, Malcolm Durkin, John Mates, Carl Reintsema, Gene Hilton, Daniel Schmidt, Daniel
Swetz, Kent Irwin, Joel Ullom) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 248
PB-31 Measurements of Improved TDM and Prototype TDM+ Multiplexing Circuits (Malcolm Durkin,
Carl D Reintsema, Edward V Denison, William B Doriese, Johnathon D Gard, Gene C Hilton, Kent D
Irwin, Kelsey M Morgan, Galen C O’Neil, Robert Stevens, Daniel S Swetz, Leila R Vale, Joel N Ullom) 249
PB-32 Intrinsic losses and noise of high-Q lithographic MHz LC resonators for frequency division multiplexing(Luciano Gottardi, Jan van der Kuur, Marcel P. Bruijn, Anton van der Linden, Mikko Kiviranta, Hiroki
Akamatsu, K. Ravensberg) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 250
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Category C : Fabrication & Implementation Techniques
PC-1 Microfabrication Developments for future Instruments using KID Detectors (J. GOUPY, A. BENOIT,
A. BIDEAUD, O. BOURRION, M. CALVO, A. CATALANO, E.F.C. DRIESSEN, A. GOMEZ, S.
LECLERCQ, F. LEVY-BERTRAND, J.F. MACIAS-PEREZ, A. MONFARDINI, K.F. SCHUSTER)
PC-2 Electrical contacts on germanium at cryogenic temperatures (¡ 300 mK) (Ugo Lo Cicero, Flavio
Nuzzo, Jean-Luc Sauvageot, Francesca Chiodi, Dominique Debarre, Salvatore Ferruggia Bonura, Luisa
Sciortino, Alfonso Collura, Marco Barbera) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-3 Hierarchical sinuous phased array for increased mapping speed of multichroic focal planes (Ari Cukierman, Adrian T. Lee, Christopher Raum, Aritoki Suzuki, Benjamin Westbrook ) . . . . . . . . . . . . .
PC-4 Design and fabrication techniques used to optimize MKID arrays for BLAST-TNG (Christopher M
McKenney, Johannes Hubmayr, Michael R Vissers, Jiansong Gao, Bradley Dober, Gene C Hilton,
Jason E Austerman, Dale Li ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-5 Low-Tc superconducting TES for a Cuore UPgrade with Particle IDentification (CUPID) (Raul
Hennings-Yeomans) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-6 Commercialization of micro-fabrication of antenna-coupled Transition Edge Sensor bolometer detectors
for studies of the Cosmic Microwave Background (Aritoki Suzuki, Chris Bebek, Maurice Garcia-Sciveres,
Stephen Holland, Akito Kusaka, Adrian T Lee, Nicholas Palaio, Natalie Roe, Leo Steinmetz ) . . . . .
PC-7 The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status (Benjamin Westbrook ) . . .
PC-8 Development of dual-polarization sensitive KIDs for CMB measurements (Kenji Kiuchi, Jihoon Choi,
Ryo Koyano, Satoru Mima, Shugo Oguri, Chiko Otani, Munehisa Semoto, Tohru Taino) . . . . . . .
PC-9 TiN-Al MKID Polarimeter Arrays Optimized for Balloon-borne Submillimeter Imaging on BLASTTNG (Michael R Vissers, The BLAST ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-10 A calibration target for cm-range instruments. (Tommaso Ghigna) . . . . . . . . . . . . . . . . . .
PC-11 Design and Fabrication of Multichroic Feedhorn-Coupled MKID Arrays (Yanru Song, Maximilian H.
Abitbol, Peter A. R. Ade, Sean Bryan, Hsiao-Mei Cho, Rahul Datta, Peter Day, Simon Doyle, Daniel
Flanigan, Kent Irwin, Bradley R. Johnson, Glenn Jones, Sarah Kernasovskiy, Dale Li, Phil Mauskopf,
Heather McCarrick, Jeﬀ McMahon, Amber Miller, Giampaolo Pisano, Carole Tucker ) . . . . . . . . .
PC-12 Fabrication and Characterization of (100) Silicon Membranes for a Multi-beam Superconducting
Heterodyne Receiver (Shohei Ezaki, Wenlei Shan, Matthias Kroug, Takafumi Kojima, Alvaro Gonzalez,
Shin’ichiro Asayama, Takashi Nogchi ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-13 Investigating the Eﬀect of Fabrication Processes and Material Properties to the Large Transition
Edge Sensor Array Performance for the South Pole Telescope 3G Experiment (Junjia Ding, SPT-3G
collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-14 Fabrication of Flexible Superconducting Wiring with High Current Carrying Capacity Indium Interconnects (Natalie S DeNigris, James A Chervenak, Meng-Ping Chang, Jong Yoon Ha, Nicholas P
Costen, Simon R Bandler, Megan E Eckart, Caroline A Kilbourne, Stephen J Smith) . . . . . . . . .
PC-15 Growth and Post Treatment of AlMn Film for X-ray Microcalorimeter Based on Transition Edge
Sensor (Wentao Wu, Yue Lv, Bo Gao, Zhen Wang) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-16 Tuning SPT-3G transition-edge-sensor electrical properties with a trilayer Au-Ti-Au thin-film stack(Faustin W Carter, SPT3G SPT3G) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-17 Fabrication of Absorbers with Dry Film Photoresist for Gamma Ray Spectroscopy with Metallic
Magnetic Calorimeters (Ruslan Hummatov, John Ad Hall, Geon Bo Kim, Stephan Friedrich, Robin C
Cantor, Stephen T. P. Boyd ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-18 Fabrication of ultrasensitive transition edge sensor bolometric detectors for HIRMES (Ari D Brown,
Regis Brekosky, Vilem Mikula, Timothy M Miller, Joseph Oxborrow ) . . . . . . . . . . . . . . . . . . .
PC-19 Absorber Materials for the transition edge sensor bolometric detectors on HIRMES (Ari D Brown,
Edward J Wollack, Kevin H Miller, Joseph Oxborrow, Vilem Mikula) . . . . . . . . . . . . . . . . . .
PC-20 Flexible Cryogenic Microwave Wiring for the MKID Exoplanet Camera (Alex B Walter, Clint Bockstiegel, Miguel Daal, Seth R Meeker, Benjamin A Mazin) . . . . . . . . . . . . . . . . . . . . . . . . .
PC-21 TiNx KIDs for the second phase of CALDER (Ivan Colantoni, Laura Cardani, Nicola Casali, Angelo
Cruciani, Fabio Bellini, Maria Gabriella Castellano, Carlo Cosmelli, Antonio d’Addabbo, Sergio di
Domizio, Maria Martinez, Claudia Tomei, Marco Vignati ) . . . . . . . . . . . . . . . . . . . . . . . . .
PC-22 Fabrication of a uniform large scale array of X-ray microcalorimeters for the X-IFU instrument onAthena (Marcel Ridder, Kenichiro Nagayoshi, Marcel Bruijn, Pourya Khosropanah, Luciano Gottardi,
Jiang Rong Gao) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PC-23 Fabrication of the arrays of detectors deployed with the SPT-3G receiver (Chrystian M Posada,SPT-3G Collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
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PC-24 Impact of electrical contacts design and materials on the stability of titanium film superconducting
transition shape (Volodymyr G Yefremenko, SPT-3G collaboration) . . . . . . . . . . . . . . . . . . . . 278
PC-25 Microfabrication of transition-edge sensor arrays of microcalorimeters with Ho-163 for direct neutrinomass measurements with HOLMES (Angiola Orlando, Giancarlo Ceruti, Marco Faverzani, Elena Ferri,Andrea Giachero, Angelo Nucciotti, Andrei Puiu, Dan Schmidt, Dan Swetz, Joel Ullom) . . . . . . . . 280
PC-26 Characterizing Atomic Layer Deposition Titanium Nitride Kinetic Inductance Detectors (Rong Nie,
Peter S. Barry, Erik Shirokoﬀ ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 281
Category D : Cryogenics and Components
282
PD-1 Metamaterial Achromatic Half-Wave Plates for Cosmic Microwave Background Observation (Kevin P
Coughlin, Jeﬀ McMahon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 283
PD-2 Development of a cylindrical magnetic refrigerant with polycrystaline GdLiF4 for Adiabatic Demagnetization Refrigerator (Akio Hoshino, Shunji Kitamoto, Hadi Razavi, Yuki Nakajima, Masayoshi Fuji,
Sadakazu Takayama, Osamu Takagi, Katsukiyo Furukawa, Ryuji Higashinaka, Yuji Aoki, Tatsuma D.
Matsuda, Shin’ya Yamada, Yoshitaka Ishisaki, Yuichiro Ezoe, Takaya Ohashi ) . . . . . . . . . . . . . . 284
PD-3 Development of a half-wave plate based polarization modulator unit for LiteBIRD (Tomotake Matsumura, LiteBIRD collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 285
PD-4 The CUORE cryostat (Antonio D’Addabbo) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 287
PD-5 Stacked Wafer Gradient Index Silicon Optics with Integral Antireflection Layers (Fabien Defrance,
Goutam Chattopadhyay, Jake Connors, Sunil Golwala, Matt I. Hollister, Cecile Jung-Kubiak, Simon
Radford, Jack Sayers, Edward C. Tong, Hiroshige Yoshida) . . . . . . . . . . . . . . . . . . . . . . . . 288
PD-6 Superconducting Flex Cables for CMB Detector Readouts (Robin Cantor, John A Hall ) . . . . . . . 289
PD-7 Improved Automated Control System for ADR Cryostats (Robin Cantor ) . . . . . . . . . . . . . . . 290
PD-8 Compact 0.8 K Helium-4 Sorption Cooler (Hiroshi Matsuo, Hajime Ezawa, Yuta Kawamura, Daiki
Kubo, Norio Okada, Reiho Shimomukai ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 291
PD-9 Improvements of our TES microcalorimeter operation system with a compact adiabatic demagnetization refrigerator cryostat (Keigo Tanaka, Ryuichi Fujimoto, Kenta Nakayama, Yuya Kinoshita, Yu
Kai, Tomohiro Nakano, Ayumi Tsuji ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 292
PD-10 Large Angle Optical Access in a sub-Kelvin Cryostat for the Development of a Beam Steering Antenna(Sebastian Hahnle, Juan Bueno, Robert Huiting, Jochem Baselmans) . . . . . . . . . . . . . . . . . . . 293
PD-11 Feasibility Study for an IR-LED Based Calibration System for SuperCDMS Detectors (Muad M Ghaith)294
PD-12 A cryogenic detector characterisation facility in the shallow underground laboratory at the Technical
University of Munich (Alexander Langenkamper, Xavier Defay, Nahuel Ferreiro, Angelina Kinast, JeanCome Lanfranchi, Erik Lindner, Michele Mancuso, Elizabeth Mondragon, Andrea Munster, Tobias
Ortmann, Walter Potzel, Stefan Schonert, Andreas Ulrich, Stephan Wawoczny, Michael Willers) . . . 295
PD-13 Concept Design of High Frequency Telescope for LiteBIRD (Takashi Hasebe, LiteBIRD Collaboration)296
PD-14 CUTE - A low noise facility for testing cryogenic dark matter detectors (philippe camus, Gilles
Gerbier, Wolfgang Rau, Koby Dering, Antoine Caze, Ali Dastgheibi-Fard, Silvia Scorza) . . . . . . . . 297
PD-15 Optimization of detector arrays and the cryogenic platform for the ECHo experiment (Clemens
Hassel, Steﬀen Allgeier, Christian Enss, Anna Ferring, Andreas Fleischmann, Dorothea Fonnesu, Lisa
Gamer, Loredana Gastaldo, Daniel Hengstler, Sebastian Kempf, Federica Mantegazzini, Dennis Schulz,
Mathias Wegner ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 298
PD-16 Impact of a cryogenic half-wave plate polarization modulator on the detector array sensitivity of
the POLARBEAR-2 CMB experiment (Charles Alexander Hill, Akito Kusaka, Paul Barton, Alex G
Droster, Mael Flament, Suhas Ganjam, Arian Jadbabaie, Oliver Jeong, Brian Keating, Adrian T Lee,
Alex Madurowicz, Frederick T Matsuda, Tomotake Matsumura, Adam Rutkowski, Yuki Sakurai, Danielle
R Sponseller, Aritoki Suzuki, Raymond Tat) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 299
PD-17 International Development of Detector Cooling System Down to 50 mK in Space without Cryogens(Noriko Y. Yamasaki, Kazuhisa Mitsuda, Takao Nakagawa, Keisuke Shinozaki, Chihiro Tokoku, Ryo
Yamamoto, Yuto Minami, Ivan Charles, Jean-Marc Duval, Thomas Prouve, Jerome Andre, Christophe
Daniel, Michel Ledu, Irwin Maussang, Alice Pralines) . . . . . . . . . . . . . . . . . . . . . . . . . . . 300
PD-18 Experimental study and modeling of cryogenic detectors decoupling within dry cryostat (Romain
Maisonobe, Julien Billard, Maryvonne De Jesus, Louis Dumoulin, Alexandre Juillard, Stefanos Marnieros,
Dimitri Misiak, Sayah Sihem, Lionel Vagneron) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 301
PD-19 A 300 mK Testbed for Rapid Characterization of Microwave SQUID Multiplexing Circuits (Abigail
L. Wessels, John A.B. Mates, Vincent Kotsubo, Norman Jarosik, Johnathon D. Gard, Douglas A.
Bennett, Daniel T. Becker, Johannes Hubmayr, Joel N. Ullom) . . . . . . . . . . . . . . . . . . . . . . 302
xv

PD-20 A micro-vibration acoustic attenuator for low temperature detectors. (Luciano Gottardi, J. Dercksen,
H. van Weers, H. Akamatsu, J. van der Kuur, B. Jackson, K. Ravensberg, J. R. Gao, P. Khosropanah) 303
PD-21 Magnetic field shielding for a Rydberg-atom single-photon detector: basic approach and measurements(Masahiro Shibata, Tomohito Haseyama, Kentaro Kominato, Satoru Yamada, Masaru Tada, Yasuhiro
Kishimoto, Izumi Ogawa, Haruhiko Funahashi, Seishi Matsuki ) . . . . . . . . . . . . . . . . . . . . . . 304
PD-22 Design of magnetic shielding and field coils for a TES X-ray microcalorimeter test platform (Antoine
R. Miniussi, Joseph S. Adams, Simon R. Bandler, James A. Chervenak, Aaron M. Datesman, Megan
E. Eckart, Fred M. Finkbeiner, Richard L. Kelley, Caroline A. Kilbourne, Frederick S. Porter, John E.
Sadleir, Kazuhiro Sakai, Stephen J. Smith, Nicholas A. Wakeham, Edward J. Wassell, Wonsik Yoon,
Willam B. Doriese, Henk J. van Weers) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 305
Category E : Applications
306
PE-1 A Review of Packaging and Integration Techniques for Large Superconducting Detector Arrays for
Cosmic Microwave Background Observations (Shuay-Pwu Patty Ho, ACT Collaboration) . . . . . . . . 307
PE-2 Polarization Sensitive Microwave Detectors for a Satellite CMB Mission (Kyle R Helson, Aamir
Ali, John Appel, Charles L Bennett, Berhanu Bulcha, Meng-ping Chang, David T Chuss, Nicholas
Costen, Kevin L Denis, Thomas Essinger-Hileman, Ron Hu, Tobias A Marriage, Karwan Rostem,
Marco Sagliocca, Kongpop U-Yen, Edward J Wollack ) . . . . . . . . . . . . . . . . . . . . . . . . . . . 308
PE-3 Advanced ACTPol 27/39 GHz Detector Array Calibration with Fourier Transform Spectroscopy:
Foreground Removal in CMB Maps (Taylor Baildon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . 309
PE-4 SPIDER: CMB polarimetry from the edge of space (Jeﬀrey P. Filippini, Spider collaboration) . . . 310
PE-5 Advanced ACTPol Low Frequency Array: Readout and Characterization of Prototype 27 and 39 GHz
Transition Edge Sensors (Brian J Koopman, AdvACT Collaboration) . . . . . . . . . . . . . . . . . . . 311
PE-6 POLARBEAR-2: Development of a receiver system for CMB measurements (Haruki Nishino, POLARBEAR Collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 312
PE-7 LiteBIRD: a satellite for the study of B-mode polarization and inflation from cosmic microwave
background radiation detection (Masashi Hazumi, LiteBIRD collaboration) . . . . . . . . . . . . . . . 314
PE-8 The POLARBEAR and Simons Array Cosmic Microwave Background Experiments (Adrian T. Lee,
POLARBEAR collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 317
PE-9 Simons Observatory: Next Generation Telescopes Featuring Large Detector Arrays for Observationsof the Cosmic Microwave Background (Jeﬀ McMahon) . . . . . . . . . . . . . . . . . . . . . . . . . . . 319
PE-10 Design and Performance of the SPT3G First-year Focal Plane (Wendeline Bray Everett, SPT3G
Collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 320
PE-11 Design, Characterization, and Assembly of the POLARBEAR-2A Cryogenic Readout System(Tucker Elleflot, POLARBEAR collaboration) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 321
PE-12 TC tuning of Titanium thin films for CMB detectors on the SWIPE/LSPE experiment (D. Vaccaro,
B. Siri, A.M. Baldini, M. Biasotti, F. Cei, V. Ceriale, M. de Gerone, L. Galli, G. Gallucci, F. Gatti,
M. Grassi, D. Grosso, D. Nicoló, M. Piendibene, G. Signorelli, and F. Spinella) . . . . . . . . . . . . 323
PE-13 Development of a Massive, Highly Multiplexible, Phonon-Mediated Particle Detector using Kinetic
Inductance Detectors (Yen-Yung Chang, Brett Cornell, Taylor Aralis, Bruce Bumble, Sunil R. Golwala) 324
PE-14 A NaI-based cryogenic scintillating calorimeter: status and results from the first COSINUS prototype detectors (Karoline Schaeﬀner, Godehard Angloher, Paolo Carniti, Lorenzo Cassina, Luca Gironi,
Claudio Gotti, Achim Guetlein, Michele Mancuso, Lorenzo Pagnanini, Gianluigi Pessina, Federica Petricca, Stefano Pirro, Rafael Puig, Franz Proebst, Florian Reindl, Jochen Schieck, Wolfgang Seidel ) . . 325
PE-15 The DM Radio: Searching for Ultra-Light-Field Dark Matter (Arran Phipps, S. Chaudhuri, S.
Kuenstner, C. Dawson, H.-M. Cho, D. Li, H. Moseley, B.A. Young, S. Rajendran, J. Mardon, L.
Page, J.A. Tyson, B. Godfrey, S. Hillbrand, P.W. Graham, K.D. Irwin) . . . . . . . . . . . . . . . . . 326
PE-16 Directional sensitivity in single-electron resolution phonon-mediated detectors (Fedja Kadribasic,
Nader Mirabolfathi, Kai Nordlund, Eero Holmstrom, Flyura Djurabekova) . . . . . . . . . . . . . . . . 327
PE-17 Solid xenon bolometers for anti-correlation studies (Michelle Jean Dolinski, Erin V. Hansen) . . . . 328
PE-18 The MINER Experiment: Coherent Neutrino-Nucleus Scattering Measurement With Cryogenic Semiconductor Detectors (Andrew Jastram) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 329
PE-19 A Systematic Study of the Theoretical Calorimetric Electron Capture Spectrum (Katrina E. Koehler,Mark P. Croce, Christopher J. Fontes, Michael W. Rabin, Michael A. Famiano, Thomas W. Gorczyca) 330
xvi

PE-20 Updates on the Transition Edge Sensors and multiplexed readout for HOLMES (andrei puiu, Dan
Becker, Douglas Bennet, Valentina Ceriale, Matteo De Gerone, Marco Faverzani, Elena Ferri, joseph
fowler, john gard, andrea giachero, james hays-wehle, gene hilton, biasotti michele, john mates, angelo
nucciotti, angiola orlando, gianluigi pessina, dan schmidt, dan swetz, joel ullom, bradley alpert, carlreintsema) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 331
PE-21 193 Pt Electron Capture Spectra with Microcalorimeters (Katrina E. Koehler, Mark P. Croce, Christopher J. Fontes, Michael W. Rabin, Michael A. Famiano, Thomas A. Gorczyca) . . . . . . . . . . . . . 332
PE-22 Data processing and analysis for AMoRE-Pilot (I. Kim, S. Choi, F.A. Danevich, A. Fleischmann,
J.A. Jeon, H.S. Jo, C.S. Kang, W.G. Kang, G.B. Kim, H.J. Kim, H.L. Kim, S.K. Kim, S.R. Kim,
Y.H. Kim, Y.D. Kim, V. Kornoukhov, D.H. Kwon, C. Lee, H.J. Lee, M.K. Lee 3, S.H. Lee, S.Y. Oh,
J.H. So, Y.S. Yoon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 333
PE-23 Characterisation of CRESST-III target crystals in the shallow underground laboratory at the Technical
University of Munich (Michael Willers, Xavier Defay, Nahuel Ferreiro, Angelina Kinast, Jean-Come
Lanfranchi, Alexander Langenkamper, Erik Lindner, Michele Mancuso, Elizabeth Mondragon, Andrea
Munster, Tobias Ortmann, Walter Potzel, Stefan Schonert, Raimund Strauss, Andreas Ulrich, Stephan
Wawoczny) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 334
PE-24 Quantum-limited scan strategies: Optimizing resonant axion and hidden photon dark matter detection(Saptarshi Chaudhuri, Kent Irwin, Peter Graham, Jeremy Mardon, Arran Phipps, Stephen Kuenstner,
Hsiao-Mei Cho, Dale Li ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 335
PE-25 TES-based light detectors for the CRESST direct dark matter search (Johannes F. Rothe) . . . . . 336
PE-26 Development of Lumped Element Kinetic Inductance Detectors for Light Dark Matter Searches using
Liquid Helium (Yosuke Kida, Masashi Hazumi, Naoto Hidehira, Fuminori Hirayama, Hirokazu Ishino,
Atsuko Kibayashi, Satoshi Kohjiro, Kunimoto Komatsu, Nobuaki Sato, Yosuke Yamada, Hirotake Yamamori ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 337
PE-27 Current Status of the Detector Developement for the CRESST Dark Matter search (Marc Wuestrich, )338
PE-28 163Ho distillation and implantation for Holmes experiment (Giovanni Gallucci ) . . . . . . . . . . . 339
PE-29 A low-energy electron detector from photoionization process with Rydberg atoms at low temperature to search for dark matter axions (Seishi Matsuki, Haruhiko Funahashi, Akira Matsubara, Kyohei
Nakajima, Izumi Ogawa) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 340
PE-30 Sensitivity of TES Microcalorimeter Arrays for Solar-Axion Line Emission (Kazuhisa Mitsuda, Keisei
Maehisa) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 341
PE-31 Status of the AMoRE experiment searching for neutrinoless double beta decay using low-temperaturedetectors (H.S. Jo, S. Choi, F.A. Danevich, A. Fleischmann, J.A. Jeon, C.S. Kang, W.G. Kang, G.B.
Kim, H.J. Kim, H.L. Kim, I. Kim , S.K. Kim, S.R. Kim, Y.H. Kim, Y.D. Kim , V. Kornoukhov, D.H.
Kwon , C. Lee , H.J. Lee , M.K. Lee, S.H. Lee , S.Y. Oh, J.H. So, Y.S. Yoon) . . . . . . . . . . . . . 342
PE-32 Development of patchable light detectors for the AMoRE project (Hyejin Lee, Hyon-Suk Jo, Chan
Seok Kang, Hyelim Kim, So-Ra Kim, Geon-Bo Kim, Inwook Kim, Yong-Hamb Kim, Minkyu Lee,
Seung-Yoon Oh, Jungho So) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 343
PE-33 Signal stabilization study for AMoRE detectors (Dohyung Kwon, Yong-Hamb Kim, Sora Kim, Chan
Seok Kang, Inwook Kim, Hyon-Suk Jo, Hye Lim Kim, Chang Lee, Hyejin Lee, SeungHoon Lee, SeungYoon Oh, Jin-A Jeon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 344
PE-34 Development of phonon and photon detectors for rare events searches using scintillating crystals(Andreas Fleischmann, Felix Ahrens, Christian Enss, Loredana Gastaldo, Clemens Hassel, SebastianKempf, Yong-Hamb Kim, Martin Loidl, Xavier Francois Navick, Mathias Rodrigues, Won Sik Yoon) . 345
PE-35 Fabrication and characterization of MMCs with enclosed 163 Ho (Loredana Gastaldo, Holger Dorrer, Christoph Emanuel Duellmann, Klaus Eberhardt, Christian Enss, Andreas Fleischmann, Dorothea
Fonnesu, Lisa Gamer, Loredana Gastaldo, Clemens Hassel, Daniel Hengstler, Sebastian Kempf, Tom
Kieck, Federica Mantegazini, Fabian Schneider, Mathias Wegner, Klaus Wendt) . . . . . . . . . . . . 346
PE-36 The ν-cleus experiment: Gram-scale cryogenic calorimeters for a rapid discovery of coherent neutrino
scattering. (Raimund Strauss, Johannes Rothe, Franz Probst, Wolfgang Seidel, Federica Petricca, Stefan
Schonert, Lothar Oberauer, Jochen Schiek ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 347
PE-37 Trigger study on AMoRE-pilot detector (I. Kim, S. Choi, F.A. Danevich, A. Fleischmann, J.A.
Jeon, H.S. Jo, C.S. Kang, W.G. Kang, G.B. Kim, H.J. Kim, H.L. Kim, S.K. Kim, S.R. Kim, Y.H.
Kim, Y.D. Kim, V. Kornoukhov, D.H. Kwon, C. Lee, H.J. Lee, M.K. Lee 3, S.H. Lee, S.Y. Oh, J.H.
So, Y.S. Yoon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 348
PE-38 Directionality study of phonon-scintillation signals from a zinc tungstate crystal (Jeon JA, Kim HL,
Kim IW, Kim SR, Kim YH, Kwon DH, Lee HJ, Lee SH, Oh SY, Sekiya H ) . . . . . . . . . . . . . . . 349
xvii

PE-39 Development of Aluminum LEKIDs for Balloon-Borne Far-IR Spectroscopy (Steven Hailey-Dunsheath,
Alyssa Barlis, James Aguirre, C. Matt Bradford, Henry G. LeDuc, Christopher M. McKenney, Tashalee
Billings) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 350
PE-40 The Mexico-UK Sub-millimetre Camera for Astronomy (Edgar Castillo Dominguez, Peter Ade,
Peter Barry, Tom Brien, Simon Doyle, Abel Perez-Fajardo, Daniel Ferrusca, Victor Gomez, Amber Hornsby, David Hughes, Phil Mauskopf, Paul Moseley, Enzo Pascale, Giampaolo Pisano, Ivan
Rodriguez-Montoya, Sam Rowe, Carole Tucker, Miguel Velazquez ) . . . . . . . . . . . . . . . . . . . . 351
PE-41 Second-generation design of Micro-Spec: a medium-resolution, submillimeter-wavelength spectrometeron-a-chip (Giuseppe Cataldo, Emily M. Barrentine, Berhanu T. Bulcha, Negar Ehsan, Larry A. Hess,
Omid Noroozian, Thomas R. Stevenson, Kongpop U-Yen, Edward J. Wollack, Samuel H. Moseley) . . 352
PE-42 CCAT-prime: An Extreme Field-of-View Submillimeter Telescope on Cerro Chajnantor (Michael D
Niemack ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 353
PE-43 On-Sky Performance of MUSTANG-2: the Multiplexed SQUID TES Array at Ninety GHz (SaraM. Stanchfield, Peter A.R. Ade, James Aguirre, Justus A. Brevik, Hsiao-Mei Cho, Rahul Datta, MarkJ. Devlin, Simon R. Dicker, Bradley Dober, Shannon M. Duﬀ, Dennis Egan, Pam Ford, Gene Hilton,
Johannes Hubmayr, Kent D. Irwin, Paul Marganian, Brian S. Mason, John A.B. Mates, Jeﬀ McMahon,
Melinda Mello, Tony Mroczkowski, Charles Romero, Carole Tucker, Joel Ullom, Leila R. Vale, SteveWhite, Mark Whitehead, Alexander H. Young) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 354
PE-44 The KIDS project (Ivan Colantoni, Elia Battistelli, Maria Gabriella Castellano, Alessandro Coppolecchia, Paolo de Bernardis, Cristian Franceschet, Luca Lamagna, Stefano Mandelli, Jacopo Martelli,Silvia Masi, Aniello Mennella, Alessandro Paiella, Mario Zannoni ) . . . . . . . . . . . . . . . . . . . . 355
PE-45 The performance of the Athena X-ray Integral Field Unit at very high count rates (Philippe Peille,
Thomas Dauser, Christian Kirsch, Roland den Hartog, Edoardo Cucchetti, Joern Wilms, Didier Barret,
Jan-Willem den Herder, Luigi Piro) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 356
PE-46 The Design of Whiskers, the Lynx X-ray Microcalorimeter (Simon Richard Bandler, Michael Dipirro,
Megan E. Eckart, Kazuhiro Sakai, Stephen J. Smith, Douglas Bennett, Vincent Kotsubo, Benjamin
Mates, Daniel Swetz, Joel N. Ullom, Kent D. Irwin, Stephen E. Kuenster, Daniel McCammon, Enectali
Figueroa-Feliciano, Kevin Ryu, Ben Zeiger, Jeﬀrey Olson, Douglas Swartz, Wonsik Yoon) . . . . . . . 357
PE-47 The Demonstration model of the Cryogenic AntiCoincidence detector for the ATHENA X-IFU(Michele Biasotti, Andrea Argan, Valentina Ceriale, Dario Corsini, Matteo D’Andrea, Matteo De
Gerone, Flavio Gatti, Simone Lotti, Claudio Macculi, Gabriele Minervini, Guido Torrioli, Luigi Piro) 358
PE-48 Detector Calibration of the Micro-X Sounding Rocket Telescope (David C. Goldfinger, Joseph S.
Adams, Robert Baker, Simon R. Bandler, Meredith Danowski, Walter B. Doriese, Megan E. Eckart,
Enectali Figueroa-Feliciano, Sarah N.T. Heine, Gene C. Hilton, Antonia J.F. Hubbard, Richard L.
Kelley, Caroline A. Kilbourne, Renee Manzagol, Dan McCammon, Takashi Okajima, F. Scott Porter,
Carl D. Reintsema, Peter Serlemitsos, Stephen J. Smith, Patrick Wikus) . . . . . . . . . . . . . . . . 359
PE-49 Multi-parameter gain drift correction of X-ray micro-calorimeters for the X-ray Integral Field Unit
(Edoardo Cucchetti, Megan E Eckart, Philippe Peille, Francois Pajot, Frederick Scott Porter ) . . . . . 360
PE-50 Development of Multi-temperature Calibrator for the TES Bolometer Camera: System Design (Tatsuya Takekoshi, Kazushige Ohtawara, Tai Oshima, Shun Ishii, Natsuko Izumi, Takuma Izumi, Masayuki
Yamaguchi, Shunta Suzuki, Kazuyuki Muraoka, Akihiko Hirota, Fumiaki Saito, Shunichi Nakatsubo,
Akira Kouchi, Tetsuya Ito, Kazunori Uemizu, Yasunori Fujii, Yoichi Tamura, Kotaro Kohno, Ryohei
Kawabe) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 361
PE-51 Pyramid-type Antireflective Structures on Silicon Lenses for Millimeter-wave Observations (TomNitta, Yutaro Sekimoto, Kazufusa Noda, Takashi Hasebe, Shigeyuki Sekiguchi, Hiroshi Matsuo, Makoto
Nagai, Agnes Dominjon, Wenlei Shan, Yosuke Murayama, Shogo Hattori, Masato Naruse, Nario Kuno,
Naomasa Nakai ) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 362
PE-52 The Cryogenic AntiCoincidence detector for ATHENA X-IFU: characterization of the last generation
single pixel prototype (AC-S8). (Matteo D’Andrea, Claudio Macculi, Andrea Argan, Simone Lotti,
Gabriele Minervini, Luigi Piro, Michele Biasotti, Dario Corsini, Flavio Gatti, Guido Torrioli) . . . . 364
PE-53 The Cryogenic AntiCoincidence detector for ATHENA X-IFU: improvement of the test setup towards
the Demonstration Model (Matteo D’Andrea, Claudio Macculi, Andrea Argan, Simone Lotti, Gabriele
Minervini, Luigi Piro, Michele Biasotti, Dario Corsini, Flavio Gatti, Guido Torrioli, Angela Volpe) . 365
PE-54 Optical Response of TES Bolometer Arrays for SAFARI (Michael Damian Audley, Gert de Lange,
Jian-Rong Gao, Richard Hijmering, Pourya Khosropanah, Marcel Ridder, Neil Trappe) . . . . . . . . 366
PE-55 Vector Beam Pattern Measurements of a large field of view Microwave Kinetic Inductance Detector
camera at 350GHz (Stephen J.C. Yates, Kristina K. Davis, Willem Jellema, Jochem J.A. Baselmans,
Lorenza Ferrari, Ronald Hesper, Kotaro Kohno, Vignesh Murugesan, David Thoen, Andrey M. Baryshev )367
xviii

PE-56 PICTURE-C: A Balloon-borne Optical MKID Camera (Clinton Bockstiegel, Benjamin A. Mazin,
Seth R. Meeker, Paul Szypryt, Alex B. Walter, Gerhard Ulbricht, Giulia Collura, Neelay Fruitwala,
Matthew J. Strader, Isabel Lipartito, Nicholas Zobrist, Gregoire Coiﬀard, Miguel Daal, Rupert Dodkins,
Timothy Cook, Kerri Cahoy, Supriya Chakrabarti, Ewan Douglas, Susanna C. Finn, Marc Kuchner,
Nikole Lewis, Anne Marinan, Jason Martel, Dimitri Mawet, Christopher Mendillo, Gene Serabyn,
David Stuchlik, Mark Swain) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-57 Development of Multi-temperature Calibrator for the TES Bolometer Camera: Deployment at
ASTE (Tai Oshima, Kazushige Ohtawara, Tatsuya Takekoshi, Shun Ishii, Natsuko Izumi, Takuma
Izumi, Masayuki Yamaguchi, Shunta Suzuki, Kazuyuki Muraoka, Akihiko Hirota, Fumiaki Saito, Shunichi Nakatsubo, Akira Kouchi, Tetsuya Ito, Kazunori Uemizu, Yasunori Fujii, Yoichi Tamura, Kotaro
Kohno, Ryohei Kawabe) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-58 Super DIOS: future X-ray spectroscopic mission to search for dark baryons (Shinya Yamada, andDIOS team) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-59 Design and optimization of multi-pixel transition-edge sensors for X-ray astronomy applications(Stephen J Smith, Joseph S Adams, Simon R Bandler, James A Chervenak, Aaron M Datesman,
Megan E Eckart, Audrey J Ewin, Fred M Finkbeiner, Richard L Kelley, Antoine R Miniussi, Frederick
S Porter, Caroline A Kilbourne, John E Sadleir, Kazuhiro Sakai, Nicholas A Wakeham, Edward J
Wassell, Wonsik Yoon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-60 Resolve instrument on X-ray Astronomy Recovery Mission (XARM) (Yoshitaka Ishisaki, Ryuichi
Fujimoto, Masahiro Tsujimoto, Noriko Y. Yamasaki, Yuichiro Ezoe, Shinya Yamada, Shunji Kitamoto,
Manabu Ishida, Yoshitomo Maeda, Ryo Iizuka, Gregory V. Brown, Megan Eckart, Takayuki Hayashi,
Richard L. Kelley, Caroline A. Kilbourne, Maurice A. Leutenegger, Dan McCammon, Hideyuki Mori,
Takashi Okajima, F. Scott Porter, Yang Soong, Andrew E. Szymkowiak ) . . . . . . . . . . . . . . . . .
PE-61 Noise performance of SuperSpec: an on-chip, TiN KID based mm-wave spectrometer (R. McGeehan,
P. S. Barry, C. M. Bradford, S. Chapman, G. Che, P. Day, J. Glenn, S. Hailey-Dunsheath, M. I.
Hollister, A. Kovacs, H. G. LeDuc, P. Mauskopf, H. Nguyen, R. O’Brient, T. Reck, C. Ross, E.
Shirokoﬀ, C. Shiu, C. E. Tucker, J. Wheeler, R. Williamson, J. Zmuidzinas) . . . . . . . . . . . . . .
PE-62 Characterization Tests of Thermal Filters for the ATHENA mission X-IFU Low Temperature Detector(Marco Barbera, Ugo Lo Cicero, Luisa Sciortino, Giancarlo Parodi, Fabio D’Anca, Paolo Giglio, Salvatore Ferruggia Bonura, Flavio Nuzzo, Antonio Jimenez Escobar, Angela Ciaravella, Alfonso Collura,
Salvatore Varisco, Valerie Samain) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-63 MetroBeta: Beta Spectrometry with Metallic Magnetic Calorimeters in the Framework of the European Program of Ionizing Radiation Metrology (Martin Loidl, Jorn Beyer, Lina Bockhorn, Christian
Enss, Daniel Gyori, Sebastian Kempf, Karsten Kossert, Riham Mariam, Ole Nahle, Matias Rodrigues,
Marco Schmidt) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-64 Development of high energy resolution and high throughput SEM-EDS analyzer utilizing 100-pixel
superconducting-tunnel-junction array toward nanometer scale elemental mapping (Go Fujii, Masahiro
Ukibe, Shigetomo Shiki, Masataka Ohkubo) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-65 An X-ray TES detector head assembly for a STEM-EDS system and its performance (Tasuku Hayashi,
Haruka Muramatsu, Keisei Maehisa, Noriko N Yamasaki, Kazuhiro Mitsuda, Akira Takano, Shota
Yoshimoto, Keisuke Maehata, Mutuo Hidaka, Hirotake Yamamori, Toru Hara) . . . . . . . . . . . . .
PE-66 Superconducting microcalorimeters absolutely calibrated?for x-ray spectroscopy (Joseph W Fowler,
Bradley K Alpert, Douglas A Bennett, W Bertrand Doriese, Jonathan D Gard, Gene C Hilton, Lawrence
T Hudson, Young Il Joe, Kelsey M Morgan, Galen C O’Neil, Carl D Reintsema, Daniel R Schmidt,
Daniel S Swetz, Csilla I Szabo, Joel N Ullom) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-67 TES X-Ray Spectrometer for LCLS-II (Dale Li, Bradley K. Alpert, Daniel T. Becker, Douglas A.
Bennett, Gabriella Carini, Hsiao Mei Cho, William B. Doriese, John E. Dusatko, Joseph W. Fowler,
Josef C. Frisch, John D. Gard, Gene C. Hilton, Michael R. Holmes, Kent D. Irwin, Vincent Kotsubo,
Sang Jun Lee, John A.B. Mates, Kelsey M. Morgan, Kazutaka Nakahara, Carl D. Reintsema, Daniel
R. Schmidt, Steve Smith, Daniel S. Swetz, Jana B. Thayer, Charles J. Titus, Joel N. Ullom, Daniel D.
Van Winkle, Abigail Wessels) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-68 Recent advances in broadband, ultrahigh resolution spectroscopy of particle induced x-rays using TES
microcalorimeter arrays (Ilari Maasilta, Mikko Palosaari, Marko Kayhko, Kimmo Kinnunen, Mikko
Laitinen, Kai Arstila, Randy Doriese, Joe Fowler, Carl Reintsema, Dan Swetz, Dan Schmidt, Joel
Ullom, Timo Sajavaara) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-69 Microcalorimeters for Nuclear Material Analysis (Mark P. Croce, Katrina Koehler, Andrew Hoover,Veronika Mocko, Stosh Kozimor, Michael Rabin, Kathryn McIntosh, George Havrilla, Douglas Bennett,
John Mates, Johnathon Gard, Dan Schmidt, Joel Ullom, Matthew Carpenter, Robin Cantor ) . . . . .
xix

368

369
370

371

372

373

374

375

376

378

379

380

381

382

PE-70 Application of Calorimetric Low-Temperature Detectors for the Investigation of Nuclear Charge Distributions of Fission Fragments (Santwana Dubey, Artur Echler, Peter Egelhof, Patrick Grabitz, Manfred
Mutterer, Werner Lauterfeld, Stefan Stolte, Aurelien Blanc, Ulli Koester, Saskia Kraft-Bermuth, Pascal
Scholz, Shawn Bishop, Jose Gomez, Friedrich Goennenwein) . . . . . . . . . . . . . . . . . . . . . . .
PE-71 Development of total decay energy spectrometry of alpha emitters using Metallic Magnetic Calorimeters (Matias Rodrigues, Martin Loidl, Riham Mariam, Xavier-Francois Navick ) . . . . . . . . . . . . .
PE-72 Spectroscopic Measurement of X-rays and γ-rays Emitted by Neptunium Sample Irradiated in theExperimental Fast Reactor Joyo using a TES microcalorimeter (Takashi Yasumune, Koji Takasaki,
Chikara Ito, Masashi Ohno, Tomoya Irimatsukawa, Yuya Ishii, Hiroyuki Takahashi, Satoshi Koujiro)
PE-73 Application of photon number resolving transition edge sensors for the metrology of quantum dot based
light sources (Marco Schmidt, Jorn Beyer, Martin v. Helversen, Fabian Gericke, Elisabeth Schlottmann,
Alexander Thoma, Alexander Schlehahn, Manuel Gschrey, Peter Schnauber, Jan-Henrik Schulze, Andre
Strittmatter, Sven Rodt, Tobias Heindel, Stephan Reitzenstein) . . . . . . . . . . . . . . . . . . . . . .
PE-74 Total eﬃciency calibration of a metallic magnetic calorimeter detector for photon spectrometry below
100 keV. (Riham Mariam, Matias Rodrigues, Martin Loidl ) . . . . . . . . . . . . . . . . . . . . . . . .
PE-75 Calibration of Ge and Si Ionization Yield using Phonon Detectors with Luke-Neganov Amplification(Noemie Bastidon) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-76 A high-resolution x-ray spectrometer for a kaon mass measurement (Ken Suzuki, Kevin Phelan,
Daniele Tortorella, Johann Zmeskal, Matthias Buhler, Theo Hertrich, Andreas Fleischmann) . . . . .
PE-77 Development of hard X-ray TES microcalorimeters using microwave multiplexing for synchrotron
science (Umeshkumar M. Patel, Ralu Divan, Lisa M. Gades, Timothy J. Madden, Antonino Miceli,
Orlando Quaranta, Daikang Yan, Daniel Becker, Doug A. Bennett, James Hays-Wehle, Gene C. Hilton,
Johnathon Gard, John A. B. Mates, Kelsey M. Morgan, Carl D. Reintsema, Daniel R. Schmidt, Daniel
S. Swetz, Joel N. Ullom, Leila Vale) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-78 Low-Energy X-ray Spectroscopy down to 50 eV using a TES microcalorimeter (Keiichi Tanaka,
Atsushi Nagata, Satochi Nakayama, Kazuo Chinone, Kazuhisa Mitsuda, Toru Hara) . . . . . . . . . .
PE-79 Using a TES microcalorimeter spectrometer as a novel probe of heterogeneous quantum materials(Daniel Swetz, Peter Abbamonte, Gilberto de la Pena, William Doriese, Yizhi Fang, Joseph Fowler,
Gene Hilton, Young Il Joe, Sangjun Lee, Jessica McChesney, Kelsey Morgan, Carl Reintsema, Fanny
Rodolakis, Daniel Schmidt, Xiaolan Sun, Joel Ullom) . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-80 TES x-ray detectors for high eﬃciency spectroscopy of hemoglobin and other proteins (Charles
James Titus, Sang Jun Lee, Michael Baker, Brad Alpert, Doug Bennett, W. Bertrand Doriese, Joe
Fowler, Kelly Gaﬀney, Johnathan Gard, Gene Hilton, Kent Irwin, Young Joe, Chris Kenney, Dale
Li, Kelsey Morgan, Dennis Nordlund, Hirohito Ogasawara, Galen C. O’Neil, Carl Reintsema, Dan
Schmidt, Dimosthenis Sorakas, Dan Swetz, Joel Ullom, Tsu-Chien Weng, Christopher Williams, Betty
Young) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-81 Development of Polycapillary Optics for STEM?TES?EDS (Akira Takano, Keiichi Tanaka, Keisuke
Maehata, Tasuku Hayashi, Kazuhisa Mitsuda, Toru Hara) . . . . . . . . . . . . . . . . . . . . . . . . .
PE-82 Development of MMC gamma detectors for precise measurements of uranium isotopes (Geon-Bo Kim,
Sebastian Kempf, Loredana Gastaldo, Andreas Fleischmann, Christian Enss, Stephan Friedrich) . . .
PE-83 Compact measurement system to study scintillation and phononic properties of scintillating crystals
at low temperatures (Hyelim Kim, J.A. Jeon, H.S. Jo, C.S. Kang, G.B. Kim, H.J. Kim, I. Kim, S.R.
Kim, Y.H. Kim, D.H. Kwon, C. Lee, H.J. Lee, S.H. Lee, S.Y. Oh, J.H. So) . . . . . . . . . . . . . . .
PE-84 Transition-edge-sensor microcalorimeters for mass spectrometric identification of neutral molecules(Shinji Okada, Toshiyuki Azuma, Douglas Alan Bennett, William Bertrand Doriese, Joseph W. Fowler,
Tadashi Hashimoto, Ryota Hayakawa, James Hays-Wehle, Gene Hilton, Yuto Ichinohe, Yoshitaka
Ishisaki, Susumu Kuma, Toshio Nakano, Yuji Nakano, Hirofumi Noda, Galen C. O’Neil, Carl D.
Reintsema, Daniel R. Schmidt, Daniel S. Swetz, Hideyuki Tatsuno, Shutaro Ueda, Joel N. Ullom,
Shinya Yamada) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
PE-85 New frontier in TES application: X-ray spectroscopy of hadronic-atoms at Japan Proton Accelerator
Research Complex (J-PARC) (Ryota Hayakawa, HEATES collaboration) . . . . . . . . . . . . . . . . .
Author Index

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390

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397

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Oral presentations

1

Keynote talks2

O-1 Low Temperature Detectors (for Dark matter and Neutrinos) 30 Years ago. The
Start of a new experimental Technology.
Franz von Feilitzsch1
1

Technical University Munich

The beginning of a new exciting development in fundamental and applied physics is reviewed. With the first LTD
Workshop at the Ringberg Castle in Bavaria, a new conference sequence was started in march 1987 and reached with
LTD17 30th anniversary. In this presentation we try to remember some of the exiting new ideas presented at the time,
which by now reached unprecedented results and perspectives.
category : Keynote talk3

O-2 X-Ray Microcalorimeters in Space - Today and Tomorrow
Richard L Kelley1
1

NASA/Goddard Space Flight Center

The application of X-ray calorimeters for high-resolution spectroscopy of individual celestial x-ray sources finallyreached its fulfillment in early 2016 with the launch of the Soft-X-Ray Spectrometer (SXS) on the Hitomi observatory.
The instrument was used to obtain the first ever x-ray spectrum of a cluster of galaxies with a resolution suﬃcient todetect turbulence in the intracluster medium, and demonstrated the power of the technology for measuring velocity
structure with extraordinary precision. It was found that the velocity dispersion corresponding to the turbulent
motion of the gas in the Perseus Cluster is only 160 km/sec with an overall uncertainty of just 12 km/sec down toa physical scale approaching the size of our own galaxy. In my talk, I will present the overall design and performanceof the Hitomi Soft X-Ray Spectrometer (SXS). The instrument used a 36-pixel array of x-ray microcalorimeters at
the focus of a grazing-incidence Soft X-Ray Telescope (SXT). The instrument was designed to achieve an energy
resolution better than 7 eV over the 0.3-12 keV energy range and operate for more than 3 years in orbit. The actualenergy resolution of the overall instrument was 4-5 eV as demonstrated during extensive ground testing prior tolaunch and in orbit. This is consistent with the predicted detector resolution allowing for spectral broadening due
to instrument- and observatory-level terms. The in-orbit measured mass flow rate of the liquid helium cryogen andfill level at launch predicted a lifetime of over 3 years assuming steady mechanical cooler performance. Cryogen-free
operation was successfully demonstrated prior to launch. The successful operation of the SXS in orbit, including thefirst observations of the velocity structure of the Perseus cluster of galaxies, demonstrated the viability and power ofthis technology as a tool for astrophysics.
category : Keynote talk4

O-3 CMB B-mode polarization - Probe the era before the Big Bang
Hitoshi Murayama1
1

Kavli IPMU, University of Tokyo

How did the Universe begin? It is believed that the whole Universe we see today was born much smaller than the sizeof an atom. Then it was stretched to a macroscopic size by a period of accelerated expansion called cosmic inflation.
The hot Big Bang came after the inflation. We do know the Universe was hot because we can see it using thecosmic microwave background. How do we see the inflationary period? The rapid stretching of the Universe musthave caused the space to wobble, namely it let out gravitational waves. These gravitational waves can be indirectly
detected through the polarization of the cosmic microwave background.
In this talk, I will review what we can learn about the Universe from CMB observations, and then talk about
observations with emphasis on the space project, LiteBIRD. Uniform all sky coverage and the low temperature detectors
are crucial for this project.
category : Keynote talk5

MKIDS 1

6

O-4 Performance of a 961 pixel Kinetic Inductance Detector system for future spaceborne observatories
Jochem Baselmans1 , Juan Bueno2 , Stephen Yates3 , Ozan Yurduseven4 , Nuria Llombart5 , Kenichi Karatsu6 , Andrey
Baryshev7 , Lorenza Ferrari8 , Akira Endo9 , David Thoen10 , Pieter de Visser11 , Reinier Janssen12 , Vignesh
Murugesan13 , Eduard Driessen14 , Gregoire Coiﬀard15 , Jesus Martin-Pintado16 , Peter Hargrave17 , Matt Griﬃn18
1

SRON Netherlands Institute for Space research, 2 SRON - Netherlands Institute for Space Research, Sorbonnelaan 2, 3584
CA - Utrecht, The Netherlands , 3 SRON - Netherlands Institute for Space Research, Landleven 12, 9747AD - Groningen, The
Netherlands , 4 Terahertz Sensing Group, Delft University of Technology, Mekelweg 1, 2628 CD - Delft, The Netherlands ,5
Terahertz Sensing Group, Delft University of Technology, Mekelweg 1, 2628 CD - Delft, The Netherlands , 6 Terahertz
Sensing Group, Delft University of Technology, Mekelweg 1, 2628 CD - Delft, The Netherlands , 7 SRON - Netherlands
Institute for Space Research, Landleven 12, 9747AD - Groningen, The Netherlands / Kapteyn Astronomical Institute,
University of Groningen, Landleven 12, 9747 AD - Groningen, The Netherlands , 8 SRON - Netherlands Institute for Space
Research, Landleven 12, 9747AD - Groningen, The Netherlands , 9 Terahertz Sensing Group, Delft University of Technology,
Mekelweg 1, 2628 CD - Delft, The Netherlands , 10 Terahertz Sensing Group, Delft University of Technology, Mekelweg 1, 2628
CD - Delft, The Netherlands , 11 SRON - Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA - Utrecht, The
Netherlands , 12 Kavli Institute of Nanoscience, Faculty of Applied Sciences, Delft University of Technology, Lorentzweg 1,2628 CJ Delft, The Netherlands / Leiden Observatory, University of Leiden, PO Box 9513, 2300 RA Leiden, The Netherlands, 13 SRON - Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA - Utrecht, The Netherlands , 14 Institut deRadioAstronomie Millimetrique (IRAM), 300 Rue de la Piscine, 38406 Saint-Martin-d’Heres, Grenoble, France , 15 Institut deRadioAstronomie Millimetrique (IRAM), 300 Rue de la Piscine, 38406 Saint-Martin-d’Heres, Grenoble, France , 16 Centro de
Astrobiologia, Ctra de Torrejon a Ajalvir, km 4 28850 Torrejon de Ardoz (Madrid), Spain , 17 Cardiﬀ school of Physics andAstronomy, The Parade, Cardi CF24 3AA, UK , 18 Cardiﬀ school of Physics and Astronomy, The Parade, Cardi CF24 3AA,
UK

Future astrophysics and cosmic microwave background space missions operating in the far-infrared to millimeter partof the spectrum will require very large arrays of ultra-sensitive detectors in combination with high multiplexing factors
and eﬃcient low-noise and low-power readout systems. We have developed a demonstrator system suitable for suchapplications. The system combines a 961-pixel imaging array based upon Microwave Kinetic Inductance Detectors(MKIDs) with a readout system capable of reading out all pixels simultaneously with only one readout cable pair and asingle cryogenic amplifier. A microscope image of part of the array chip is given in panel a) of the figure, showing someof the MKID pixels coupled to the feedline used for read-out. An image of the assembled detector package is given inpanel b). We evaluate, in a representative environment, the full system performance in terms of sensitivity, dynamic
range, optical eﬃciency, cosmic ray rejection, pixel-pixel crosstalk and overall yield at an observation center frequencyof 850 GHz and 20% fractional bandwidth. The overall system has an excellent sensitivity, with an average detector
sensitivity NEPdet = 3x10−19 W/rt(Hz) measured for the central pixels of the array using a thermal calibration
source. Additionally, the optical coupling eﬃciency matches the calculated value, as shown in panel c) of the figure.
The electrical NEP can be obtained for all pixels and is identical to the value obtained using the thermal calibration
source. The histogram of the measured sensitivity is given in panel d) of the figure. At a loading power per pixel of
50 fW we demonstrate white, photon noise limited detector noise down to 300 mHz. The dynamic range allows thedetection of 1 Jy bright sources within the field of view without tuning the readout of the detectors. The expecteddead time due to cosmic ray interactions, when operated in an L2 or a similar far-Earth orbit, is found to be <4%.
Additionally, the achieved pixel yield is 83% and the crosstalk between the pixels is <-30dB. This demonstrates that
MKID technology can provide multiplexing ratios on the order of a 1000 with state-of-the-art single pixel performance,
and that the technology is now mature enough to be considered for future space based observatories and experiments.
category : Sensor Physics & Developments7

8

O-5 The sub-gap KID (SKID): on-chip spectroscopy at centimetric wavelengths
Alessandro Monfardini1 , Olivier Dupre2 , Alain Benoit3 , Martino Calvo4 , Andrea Catalano5 , Johannes Goupy6 ,Christophe Hoarau7 , Thierry Klein8 , Kevin Le Calvez9 , Benjamin Sacepe10 , Florence Levy-Bertrand11 , Alicia
Gomez121

6Institut Neel - CNRS, 2 Institut Neel Grenoble , 3 Institut Neel Grenoble , 4 Institut Neel Grenoble , 5 LPSC Grenoble ,Institut Neel Grenoble , 7 Institut Neel Grenoble , 8 Institut Neel Grenoble , 9 Institut Neel Grenoble , 10 Institut Neel Grenoble, 11 Institut Neel Grenoble , 12 INTA-CSIC Madrid

We have fabricated planar indium oxide superconducting resonators (Tc around 3 K) that are sensitive to frequencyselective radiation in the range 7?10 GHz. Those values lay more than 20 times below the equivalent superconducting
gap that is worth about 200 GHz. We show that the detected frequency can be adjusted by modulating the total
length of the superconducting resonator. The measured spectral resolution is of the order of thousands. We attribute
those observations to the excitation of higher-order resonance modes. The coupling between the fundamental (lumped)
and the higher order (distributed) resonances is related to the kinetic inductance non-linearity. These devices, that
we have called Sub-gap Kinetic Inductance Detectors (SKID), are to be distinguished from the standard kinetic
inductance detectors in which quasi-particles are generated when incident light breaks down Cooper pairs. We present
our preliminary results in the band 7-10 GHz and the plans for developing an instrument to monitor the water vapour
line at 22GHz.
category : Sensor Physics & Developments

9O-6 Moving optical MKIDs to lower temperature: preliminary characterization ofHafnium resonators
Giulia Collura1 , Gregoire Coiﬀard2 , Bruce Bumble3 , Paul Szypryt4 , Benjamin A. Mazin5
1

University of California Santa Barbara, 2 University of California Santa Barbara , 3 Jet Propulsion Laboratory , 4 University ofCalifornia Santa Barbara , 5 University of California Santa Barbara

We have fabricated hafnium MKID test arrays with 15 resonators on A-plane sapphire wafers. Hafnium is an elemental
type I superconductor. It has a bulk Tc of 128 mK, lower than Tc 800mK of sub-stoichiometric TiN and PtSi or Tc 1K
of Al used in current MKID instruments, corresponding to a smaller Cooper Pair binding energy. This should leadto increased sensitivity and spectral resolution. Our Hafnium films transition around 460 mK and we have measured
quasiparticle lifetimes of about 50 us at 20 mK. We observe Hafnium resonators with internal quality factors up to
500k that are photosensitive to 800-1350 nm light, exhibiting a spectral resolution R 9 at 808nm. The internal quality
factors and energy resolution observed are comparable to those of optimized PtSi MKID resonators, making Hf a very
promising material for MKID development. We also expect Hf films to have a more uniform surface inductance thanfilms made of compound materials, and we will report on uniformity measurements.
category : Sensor Physics & Developments10O-7 Suppression of in-detector-chip stray radiation for large arrays of lens-antenna
coupled microwave kinetic inductance detectors
Stephen J.C. Yates1 , Andrey M. Baryshev2 , Ozan Yurduseven3 , Juan Bueno4 , Kristina K. Davis5 , Lorenza Ferrari6 ,Willem Jellema7 , Nuria Llombart8 , Vignesh Murugesan9 , David Thoen10 , Jochem J.A. Baselmans11
1

SRON, 2 SRON, Landleven 12, 9747 AD Groningen, The Netherlands / Kapteyn Astronomical Institute, University ofGroningen, P.O. Box 800, 9700 AV Groningen, The Netherlands , 3 Terahertz Sensing Group, Faculty of ElectricalEngineering, Mathematics and Computer Science, Delft University of Technology, Mekelweg 4, 2628 CD Delft, The
Netherlands , 4 SRON, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands. , 5 Arizona State University, 781 Terrace Rd.,
Tempe, AZ, U.S.A , 6 SRON, Landleven 12, 9747 AD Groningen, The Netherlands , 7 SRON, Landleven 12, 9747 AD
Groningen, The Netherlands / Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen,
The Netherlands , 8 Terahertz Sensing Group, Faculty of Electrical Engineering, Mathematics and Computer Science, Delft
University of Technology, Mekelweg 4, 2628 CD Delft, The Netherlands , 9 SRON, Sorbonnelaan 2, 3584 CA Utrecht, The
Netherlands. , 10 Terahertz Sensing Group, Faculty of Electrical Engineering, Mathematics and Computer Science, Delft
University of Technology, Mekelweg 4, 2628 CD Delft, The Netherlands , 11 Terahertz Sensing Group, Faculty of ElectricalEngineering, Mathematics and Computer Science, Delft University of Technology, Mekelweg 4, 2628 CD Delft, The
Netherlands / SRON, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands.

With increasing detector array size, it becomes more important to control stray radiation inside the detector chips
themselves. We show that such stray light is a problem in focal plane arrays of 880 lens-antenna coupled Microwave
Kinetic Inductance Detectors (MKIDs). The arrays are measured with reimaging optics, allowing near field measurements of the optical response versus the position on the array of a reimaged optical source. We demonstrate thatthe optical response of a detector in these arrays saturates oﬀ-pixel at the -30 dB level compared to the peak pixel
response. The result is that the power detected from a point source at the pixel position is almost identical to the stray
response integrated over the chip area. If used on sky with such a stray light contribution, it would be impossible
to measure extended sources; while the point source response is degraded due to an increase of the stray loading.
However, we show that by incorporating an on-chip stray light absorber this eﬀect is reduced at least a factor 10, withthe optical response now limited by the fore-optics and not the detector chip.
category : Sensor Physics & Developments

11

MKIDS 2

12

O-8 Counting Near Infrared Photons with Microwave Kinetic Inductance Detectors
Lianfu Wei1
1

School of information science and technology, Southwest Jiaotong University

We demonstrate photon counting at 1550 nm wavelength using microwave kinetic inductance detectors (MKIDs)
made from TiN/Ti/TiN trilayer films with superconducting transition temperature Tc ? 1.4 K. The detectors havea lumped-element design with a large interdigitated capacitor covered by aluminum and inductive photon absorbers
whose volume ranges from 0.4 μ m3 to 20 μ m3 . The energy resolution improves as the absorber volume is reduced.
We achieved an energy resolution of 0.22 eV and resolved up to 7 photons per optical pulse, both greatly improved frompreviously reported results at 1550 nm wavelength using MKIDs. Further improvements are possible by optimizing
the optical coupling to maximize photon absorption into the inductive absorber.
category : Sensor Physics & Developments13O-9 Characterizing millimeter wave Thermal Kinetic Inductance Detectors with anovel readout system
Roger O’Brient1 , Bryan Steinbach2 , Hien Nguyen3 , Anthony Turner4 , Jonas Zmuidzinas5 , James Bock6
1

NASA Jet Propulsion Laboratory, California Institute of Technology, 2 California Institute of Technology , 3 Jet Propulsion
Laboratory , 4 Jet Propulsion Laboratory , 5 Jet Propulsion Laboratory / California Institute of Technology , 6 Jet Propulsion
Laboratory / California Institute of Technology

We are developing Thermal Kinetic Inductance Detectors (TKIDs) at Caltech/JPL for Cosmic Microwave Backgroundobservations, targeting deployment of a 250GHz BICEP Array camera. TKIDs inherit the scalability of traditional
KIDs via radio frequency domain multiplexing with passive cold electronics, but oﬀer design flexibility similar to what
has allowed TES bolometers to be so highly sensitive. In particular, our design allows us to independently optimize
the absorbing eﬃciency and resonator sensitivity in a manner that is drop-in compatible to existing antenna-coupledarchitectures. In this talk, we will describe detailed noise studies of several island released prototype devices that
contain integrated DC heaters in close thermal contact with KID inductor/thermistors. These heaters allow for astraightforward calibration of eﬃciency and noise spectra. We will describe contributions of leg phonon (G), quasiparticle gr, amplifier and TLS noise and explain how these can be controlled for background limited performance for ourplanned application. We will also describe a novel general-use readout system we are using for these measurements
and will use for characterization of other resonator-based detectors under development at JPL. Our warm readout
electronics uses a thin FPGA layer for generic data acquisition, but implements data processing and reduction in our
computer s GPU. This system can be easily reconfigured without the need for detailed HDL code, facilitating thevariety of measurements we have performed on our TKIDs.
category : Sensor Physics & Developments

14O-10 Photon Counting Kinetic Inductance Detectors for THz/Submillimeter Space
Spectroscopy
Omid Noroozian1 , Emily M Barrentine2 , Thomas R Stevenson3 , Ari D Brown4 , Vilem Mikula5 , Edward J Wollack6 ,Kongpop U-Yen7 , Samuel H Moseley8
1

NRAO, UVA, NASA/GSFC, 2 NASA Goddard Space Flight Center (NASA/GSFC) , 3 NASA Goddard Space Flight Center(NASA/GSFC) , 4 NASA Goddard Space Flight Center (NASA/GSFC) , 5 NASA Goddard Space Flight Center(NASA/GSFC) , 6 NASA Goddard Space Flight Center (NASA/GSFC) , 7 NASA Goddard Space Flight Center(NASA/GSFC) , 8 NASA Goddard Space Flight Center (NASA/GSFC)

Photon-counting direct detectors are highly desirable for reaching the ∼ 10−20 W/rt Hz power sensitivity enabled by
the Origins Space Telescope (OST), a notional cryogenic facility inspired by NASA s Astrophysics Roadmap. We aredeveloping Kinetic Inductance Detectors (KIDs) with photon counting capability in the far-infrared/THz combinedwith integrated spectrometers suitable for the OST facility. To reach the required sensitivity we are experimenting
with single-layer superconducting resonators made from aluminum films that are 10 nm thick on single-crystal Si
substrates. Small-volume inductors made from such thin Al films have the potential to become ultra-sensitive to single
pair-braking far-IR photons (¿90 GHz) under the right conditions. Understanding the physics of these superconducting
films and superconductor-dielectric systems is critical to achieving detector performance with ultra low-loss and lownoise substrates.
In our measurements of these resonators, we have achieved very high internal quality factors (Qi ∼ 7 × 106 for
25 nm Al, and 1.1 × 106 for 10 nm Al) at ∼106 microwave photon drive power. At single-photon drive powers bothfilms remarkably maintain a very high Qi ∼ 0.5 × 106 , by far the highest known value for such thin films reported
in literature. For our 10-nm films we have measured a residual QP density of < 0.2 /µm3 , which is suﬃcient for ourapplication. We have obtained quasi-particle (QP) lifetimes of 1.0 ms for 100 nm Al on Si resonators, another criticalparameter for reaching photon-counting sensitivity. Our testbed was optimized for ultra-low stray radiation, which was
confirmed by measurements. To realize a practical device, we are integrating these films with our Silicon-on-Insulator(SOI) process to form microstrip-style elements on single-crystal dielectric. Our analysis shows that two-level system
noise is not a limiting factor to sensitivity in our design. Based on a detailed physical model, where we simulated
the detector output time stream when illuminated with random photon events, our results show that photon counting
with > 95% eﬃciency at 0.5 THz and 1.0 THz is indeed possible.
We report on these developments and discuss our plans to implement these devices into optically coupled ultrasensitive KIDs suitable for photon counting in space.
category : Sensor Physics & Developments15

O-11 Low-Loss, Low-Noise, Crystalline Silicon Dielectric for Superconducting
Microstriplines and Kinetic Inductance Detector Capacitors
Fabien Defrance1 , Andrew D. Beyer2 , Jack Sayers3 , Sunil Golwala4
1

Division of Physics, Mathematics, and Astronomy, California Institute of Technology, 2 Jet Propulsion Laboratory , 3 Divisionof Physics, Mathematics, and Astronomy, California Institute of Technology , 4 Division of Physics, Mathematics, andAstronomy, California Institute of Technology

A number of technology developments in superconducting sensors for mm/submm astronomy require low-loss dielectricthin films with loss tangents well below the 1e-3 level seen in SiO2 and SiNx conventionally used. To this end, weare pursuing the development of crystalline silicon and hydrogenated amorphous silicon dielectrics, which promise loss
tangents 10 to 1000 times better.
Examples of mm/submm technologies that use low-loss dielectric films include:* Microstrip-coupled superconducting mm/submm detectors, which rely on superconductor-dielectric-superconductor
microstrip transmission line to transmit optical power from a coherent reception element (feedhorn, lens coupled antenna, phased-array antenna) to detectors;* Superconducting spectrometers (SuperSpec, TIME, MicroSpec), which use such microstrip to route optical power
to detectors and to define spectral channels;* Kinetic inductance detectors (KIDs), which use capacitors.
Dielectric loss, quantified by the loss tangent, is critical to these technologies: it determines the optical loss inthe microstrip, the resolution of spectral channels, and the two-level-system (TLS) dielectric fluctuation noise of the
KID capacitor. Currently, the amorphous dielectrics SiO2 and SiNx are used for the first two because they are mostconvenient for fabrication. These amorphous dielectrics have tan delta 1e-3. This loss tangent is acceptable formicrostripline but severely limits the possible architectures and spectral resolving power, and it is too large for KID
capacitors (necessitating the use of interdigitated capacitors on crystalline substrates). Lower loss dielectric would
result in a quantum leap in capability, specifically enabling new architectures incorporating microstripline (such as
remote detectors and multiscale antennas), higher-resolution superconducting spectrometers, and KIDs using compact
parallel-plate capacitors.
We are pursuing hydrogenated amorphous silicon (a-Si:H) and crystalline silicon (cSi) (from silicon-on-insulator
wafers) for low-loss films. Crystalline silicon intrinsically has tan delta ¡5e-6, 200 times lower than SiO2 and SiNx.
a-Si:H has been demonstrated with tan delta ¡ 5e-5, not as good as cSi but still 20 times better than SiO2 and
SiNx. Improvement in loss tangent to 1e-4 would provide significant gains, and further improvements would open new
possibilities, especially for KID noise. We are pursuing the both materials due to their complementary advantages
and challenges.
We use niobium parallel-plate LC resonators to measure the microwave (1-3 GHz) loss tangent and noise. We havedemonstrated that 1 um, 2 um, and 5 um crystalline silicon on SOI wafers have high-power loss tangents of 3e-6 to
3e-5, ¡ 1e-6, and 2 to 5e-6, respectively, and that the 5 um material has low-power loss tangent of 1 to 3e-5. To be usedin microstrip geometries, crystalline silicon must undergo a wafer-bonding process that may degrade the material. We
have thus made measurements for wafer-bonded 5 um crystalline silicon, obtaining low and high power loss tangentsof 6 to 12e-5 and 1 to 3e-5, respectively. We will report on measurements of the properties of wafer-bonded 1 um
and 2 um silicon and also on TLS noise measurements for virgin and wafer-bonded material. We will also report on
progress toward a-Si:H RF test devices and cSi and a-Si:H mm-wave test devices.
category : Sensor Physics & Developments

16O-12 Kalliope-based High-Speed Neutron imager by a delay-line current biased
kinetic inductance detector
Hiroaki Shishido1 , Yuya Miki2 , Hiroyuki Yamaguchi3 , Yuki Iizawa4 , Kenji M Kojima5 , Kenichi Oikawa6 , Masahide
Harada7 , Takayuki Oku8 , Kazuhiko Soyama9 , Shigeyuki Miyajima10 , Mutsuo Hidaka11 , Takekazu Ishida121

Department of Physics and Electronics, Graduate School of Engineering, Osaka Prefecture University, 2 Department of
Physics and Electronics, Graduate School of Engineering, Osaka Prefecture University, Sakai, Osaka 599-8531, Japan ,3
Department of Physics and Electronics, Graduate School of Engineering, Osaka Prefecture University, Sakai, Osaka 599-8531,
Japan , 4 Department of Physics and Electronics, Graduate School of Engineering, Osaka Prefecture University, Sakai, Osaka
599-8531, Japan , 5 Muon Science Laboratory and Condensed Matter Research Center, Institute of Materials Structure
Science, High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan / Department ofMaterials Structure Science, The Graduate Univer, 6 Materials and Life Science Division, J-PARC Center, Japan Atomic
Energy Agency, Tokai, Ibaraki 319-1195, Japan , 7 Materials and Life Science Division, J-PARC Center, Japan Atomic Energy
Agency, Tokai, Ibaraki 319-1195, Japan , 8 Materials and Life Science Division, J-PARC Center, Japan Atomic Energy Agency,
Tokai, Ibaraki 319-1195, Japan , 9 Materials and Life Science Division, J-PARC Center, Japan Atomic Energy Agency, Tokai,
Ibaraki 319-1195, Japan , 10 NanoSquare Research Institute, Osaka Prefecture University, Sakai, Osaka 599-8531, Japan /Advanced ICT Research Institute, National Institute of Information and Communications Technology, 588-2 Iwaoka, Nishi-ku,
Kobe, Hyogo 651-2492, Japan , 11 Advanced Industrial Science and Technology, Tsukuba, Ibaraki 305-8568, Japan ,12
Department of Physics and Electronics, Graduate School of Engineering, Osaka Prefecture University, Sakai, Osaka
599-8531, Japan / NanoSquare Research Institute, Osaka Prefecture University, Sakai, Osaka 599-8531, Japan

Neutron imaging is crucial for non-destructive examination because of the high penetrating capability in mostmaterials, and has been developed to date[1]. The recent progress in high intensity pulsed spallation neutron sources
allows us to perform a high spatial resolution neutron imaging. We have been developed the superconducting sensor
based neutron detectors aiming for a novel neutron imager[2, 3, 4]. The present detector consists of stacking layersof a superconducting Nb ground plane, orthogonal x and y Nb meanderlines and 10 B neutron absorption layer. The
nuclear reaction between an incident neutron and 10 B induces the transient change of the kinetic inductance of Cooper
pairs in x and y meanderlines. It excites voltage pulses under a DC-bias current and the excited signals propagate aselectromagnetic wave toward both sides with opposite polarity along the meanderline. The signals are detected by aKalliope-DC, which is a high time and temporal resolution multichannel detector concomitant with wide time window.
We successfully obtained energy dispersive high spatial resolution neutron images from quartets of signal detection
times by applying the delay-line method. We call this detector the delay-line current biased kinetic inductance detector(CB-KID). The delay-line CB-KIDs
allow us to obtain a neutron imaging by using only four lead wires. It has
definitive advantage in reducing the heat leak to the low temperature stage through the lead wires. The delay-line
CB-KID is one of a superconducting 3 He-free neutron detector, and has capability to enhance the spatial resolution
without any discontinuity by using a high-speed time to digital converter based on the Kalliope-DC systems even withthe present sensor chip.
This work is supported by a Grant-in-Aid for Scientific Research (No. 23226019, No.16H02450) from JSPS, thefoundation fabricator (CRAVITY) and a Cadence software of VDEC at the University of Tokyo.
[1] N. Kardjilov et al., Mater. Today 14, 248 (2011).
[2] K. Takahashi et al., Physica C 392-396, 1501 (2003).
[3] H. Shishido et al., Appl. Phys. Lett. 107, 232601 (2015).
[4] S. Miyajima et al., Nucl. Instrum. Methods. Phys. Res. A 842, 71 (2017).
category : Sensor Physics & Developments

17

Application - Astronomy

18

O-13 First light of DARKNESS: a pathfinder for exoplanet imaging with Microwave
Kinetic Inductance Detectors
Seth R. Meeker1 , Benjamin A. Mazin2 , Alex B. Walter3 , Matthew J. Strader4 , Neelay Fruitwala5 , Clint Bockstiegel6 ,Paul Szypryt7 , Gerhard Ulbricht8 , Gregoire Coiﬀard9 , Bruce Bumble10 , Giulia Collura11 , Rupert Dodkins12 , Isabel
Lipartito13 , Michael Bottom14 , J. Chris Shelton15 , Dimitri Mawet16 , Gautam Vasisht17 , Eugene Serabyn18
1

Department of Physics, University of California Santa Barbara, 2 Department of Physics, University of California Santa
Barbara , 3 Department of Physics, University of California Santa Barbara , 4 Department of Physics, University of California
Santa Barbara , 5 Department of Physics, University of California Santa Barbara , 6 Department of Physics, University ofCalifornia Santa Barbara , 7 Department of Physics, University of California Santa Barbara , 8 Department of Physics,
University of California Santa Barbara , 9 Department of Physics, University of California Santa Barbara , 10 Jet Propulsion
Laboratory, California Institute of Technology , 11 Department of Physics, University of California Santa Barbara ,12
Department of Physics, University of Oxford , 13 Department of Physics, University of California Santa Barbara , 14 Jet
Propulsion Laboratory, California Institute of Technology , 15 Jet Propulsion Laboratory, California Institute of Technology ,16
Department of Astronomy, California Institute of Technology , 17 Jet Propulsion Laboratory, California Institute ofTechnology , 18 Jet Propulsion Laboratory, California Institute of Technology

High-contrast imaging is a powerful technique for the study of extrasolar systems, allowing the direct observation of
exoplanets and circumstellar disks by using a combination of extreme Adaptive Optics and coronagraphy to suppress
the light from their host star. The primary obstacle to imaging faint planets and disks is bright speckles in
the focal plane caused by unsensed and uncorrected optical errors. While techniques exist to reliably correct static
speckles from diﬀraction and instrumental aberrations, speckles resulting from residual atmospheric aberrations areespecially troublesome - with decorrelation times on the order of 1s, they average slowly over long exposures andimpose the current state-of-the-art contrast limits of ∼ 10−6 from the ground (roughly corresponding to detectable
planet masses ¿ 1MJup ). Optical and near-infrared Microwave Kinetic Inductance Detectors (MKIDs) oﬀer great
potential for overcoming this limitation: read-noise free photon counting enables real-time focal plane wavefront
control at frame rates much faster than the atmospheric speckle decorrelation time, and intrinsic energy resolution
enables wavefront correction over a broad bandwidth. DARKNESS (the DARK-speckle Near-infrared Energy-resolving
Superconducting Spectrophotometer) is the first of several planned integral field spectrographs to demonstrate theuse of optical/near-infrared MKIDs for high-contrast astronomy. DARKNESS saw first-light in July 2016 at Palomar
Observatory, and has subsequently travelled to Palomar in November 2016 and April 2017 for ongoing commissioning
and science verification. Here we present an overview of the instrument and early science results, including a study of
temporospatial speckle correlations across millisecond to hour timescales, with implications for using these statistics
to discriminate speckles from true faint companions.
category : Applications

19

O-14 Development of ’DESHIMA on ASTE’: towards a field test of a submillimeterwave superconducting on-chip filterbank spectrometer based on kinetic inductancedetectors
Akira Endo1 , David Thoen2 , Kenichi Karatsu3 , Nuri van Marrewijk4 , Sjoerd Bosma5 , Ozan Yurduseven6 , Nuria
Llombart7 , Masato Naruse8 , Nozomu Tomita9 , Junya Suzuki10 , Akio Taniguchi11 , Kotaro Kohno12 , Shun Ishii13 ,Jun Maekawa14 , Ryohei Kawabe15 , Tai Oshima16 , Kaui Chin17 , Yoichi Tamura18 , Tatsuya Takekoshi19 , Kazuyuki
Fujita20 , Akira Kouchi21 , Shunichi Nakatsubo22 , Teun Klapwijk23 , Paul van der Werf24 , Stephen Yates25 , Andrey
Baryshev26 , Vignesh Murugesan27 , Robert Huiting28 , Jochem Baselmans29
1

Faculty of Electrical Engineeing, Mathematics and Computer Science, Delft University of Technology, 2 Department ofElectrical Engineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628 CD Delft, The
Netherlands. / Kavli Institute of NanoScience, Faculty of Applied Sciences, Delft University of Technology, Lorentzweg 1,
3
Department of Electrical Engineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628
CD Delft, The Netherlands. , 4 Department of Electrical Engineering, Faculty of Mathematics and Computer Science, Delft
University of Technology, 2628 CD Delft, The Netherlands. , 5 Department of Electrical Engineering, Faculty of Mathematics
and Computer Science, Delft University of Technology, 2628 CD Delft, The Netherlands. , 6 Department of ElectricalEngineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628 CD Delft, The Netherlands.
, 7 Department of Electrical Engineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628
CD Delft, The Netherlands. , 8 Department of Electrical Engineering, Faculty of Mathematics and Computer Science, Delft
University of Technology, 2628 CD Delft, The Netherlands. / Saitama Univ. Graduate School of Science and Engineering,
Saitama University, 255, Shimo-okubo, Sakura, S, 9 Department of Physics, Faculty of Science, University of Tokyo, Tokyo
113-0033, Japan. , 10 Department of Physics, Faculty of Science, University of Tokyo, Tokyo 113-0033, Japan. / High Energy
Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki, 305-0801, Japan. , 11 Institute of Astronomy,
University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan. , 12 Institute of Astronomy, University of Tokyo, 2-21-1
Osawa, Mitaka, Tokyo 181-0015, Japan. , 13 National Astronomical Observatory of Japan (NAOJ), National Institutes of
Natural Sciences (NINS), 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan , 14 National Astronomical Observatory of Japan(NAOJ), National Institutes of Natural Sciences (NINS), 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan , 15 National
Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences (NINS), 2-21-1, Osawa, Mitaka, Tokyo
181-8588, Japan , 16 National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences (NINS),
2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan , 17 Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo
181-0015, Japan. / National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences (NINS),
2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan , 18 Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya,
Aichi 464-8062, Japan. , 19 Department of Communication Engineering and Informatics, Graduate School of Informatics andEngineering, The University of Electro-Communications, Chofugaoka, Chofu, Tokyo 182-8585, Japan. , 20 Institute of Low
Temperature Science, Hokkaido University, Kita-19, Nishi-8, Kita-ku, Sapporo 060-0819, Japan. , 21 Institute of Low
Temperature Science, Hokkaido University, Kita-19, Nishi-8, Kita-ku, Sapporo 060-0819, Japan. , 22 Institute of Space andAstronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 252-5210, Japan. , 23 Kavli Institute of
NanoScience, Faculty of Applied Sciences, Delft University of Technology, Lorentzweg 1, 2628 CJ Delft, The Netherlands. /Physics Department, Moscow State Pedagogical University, 119991 Moscow, Russia. , 24 Leiden Observatory, Leiden
University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands. , 25 SRON Netherlands Institute for Space Research, 9747
AD Groningen, The Netherlands.. , 26 SRON Netherlands Institute for Space Research, 9747 AD Groningen, The
Netherlands.. , 27 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands. ,28
SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands. , 29 SRON
Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands.

The redshift distribution and physical evolution of dusty star forming galaxies is an essential ingredient to the historyof cosmic star formation and galaxy evolution, yet large redshift surveys of such submillimeter galaxies havebeen hampered by the narrow bandwidth of widely-used heterodyne spectrometers in the millimeter-submillimeterband. DESHIMA (Deep Spectroscopic High-redshift Mapper) is a project to develop a multi-pixel on-chip filterbank
spectrometer with an instantaneous bandwidth of 240-720 GHz and a frequency resolution of F/∆F = 500, using
kinetic inductance detectors. Here we report on the recent development of a 326-368 GHz, single pixel prototype
DESHIMA system for the first field test on the ASTE (Atacama Submillimeter Telescope Experiment). Locatednear the ALMA site in Chile, the 10 m single dish ASTE telescope combines excellent atmospheric transmission andsuﬃcient collecting area for detecting even high-redshift galaxies. In the conference, we will report on the developmentof the DESHIMA-on-ASTE system, consisting of the filterbank chip, the ADR-based 100 mK cryostat, the optical
chain, readout electronics, control software, calibration strategy, and operation plans.
Figure: (Left) Cross section of the DESHIMA cryostat. (Right) Micrograph of the prototype superconducting
on-chip spectrometer. With 64 channels, the filterbank covers the frequency range of 326-368 GHz, in which theatmospheric transparency is high.
category : Applications

20

300 K scatter filter (two-in-one)

2 THz (66 cm-1) Low Pass Filter

50 K thermal filters

4 K thermal filters
1.5 THz (58 cm-1) Low Pass Filter
1.1 THz (36 cm-1) Low Pass Filter
polarizer
1THz (33 cm-1) LPF + 390 GHz (13 cm-1) LPF

field lensbaﬄe

Parabolic
Mirrors

Nb shield
Cryoperm shieldfilterbank chip & lens
(at 100 mK)

1 mm

x64 spectroscopic channels

326-368 GHz signal from Antenna

21

5-7 GHz readout signal

22

O-15 The NIKA2 instrument at 30-m IRAM telescope: performance and results
Andrea Catalano1 , NIKA Core Team2
1

CNRS, 2 No aﬃliation

The New IRAM KID Array 2 (NIKA 2) is a dual-band camera operating with three frequency multiplexed kilo-pixels
arrays of Lumped Element Kinetic Inductance Detectors (LEKID) cooled at 100 mK. NIKA is designed to observe
the intensity and polarisation of the sky at 250 and 150 GHz from the IRAM 30 m telescope. It represents one
step further with respect the NIKA pathfinder instrument which has already shown state-of-the-art detectors andphotometric performance. NIKA 2 is an IRAM resident instrument for studies of the Intra Cluster Medium fromintermediate to distant clusters and so for the follow-up of Planck satellite detected clusters, high redshift sourcesand quasars, early stages of star formation and nearby galaxies emission. We present an overview of the instrument
performance and the first scientific results.
category : Applications

23

O-16 Sensitivity, Dynamic Range, and Multiplexing Requirements of FIR Detectors
for the Origins Space Telescope (OST)Johannes G Staguhn1
1

Johns Hopkins University & NASA/Goddard Space Flight Center

The Origins Space Telescope is the mission concept for the Far-Infrared Surveyor, one of the four science and technology
definition studies to be submitted by NASA Headquarters to the 2020 Astronomy and Astrophysics Decadal survey.
The observatory will provide orders of magnitude improvements in sensitivity over prior missions, in particular forspectroscopy, enabling breakthrough science across astrophysics. The observatory will cover a wavelength range
between 6 μ m and 600 μ m in order to enable the study of the formation of proto-planetary disks, detection of
bio-signatures from extra-solar planet’s atmospheres, characterization of the first galaxies in the universe, and manymore.
Key technologies enabling the mission include large cryogenic optics (the 10 m telescope will be cooled to 4 K)
and the associated cryo-coolers, plus sub-Kelvin coolers for the science instruments using superconducting detectors
for the incoherent far-infrared imager/polarimeter and spectrometers. The five instruments that are currently studied
are two imaging far-infrared spectrometers using incoherent detectors, providing up to R ∼ 105 spectral resolution,
one far-infrared heterodyne instrument for even higher spectral resolving powers, one far-infrared continuum imager
and polarimeter, plus a mid-infrared coronograph with imaging and spectroscopy mode. In particular, current superconducting detector technologies will need to be matured significantly in terms of sensitivity, dynamic range andmultiplexability while the warm readout electronics will need to operate within the low power constraints provided by
the observatory.
After a brief summary of the anticipated OST scientific capabilities, I will provide an overview of the technologicaldevelopments needed for the far-infrared instruments with focus on the detectors and readout.
category : Applications24

O-17 The Athena X-ray Integral Field Unit (X-IFU)
Francois Pajot1 , Thien Lam Trong2 , Jan-Willem den Herder3 , Luigi Piro4 , Massimo Cappi5
1Institut de Recherche en Astrophysique et Planetologie, CNRS, Universite Paul Sabatier, 2 Centre National d’Etudes
Spatiales , 3 Space Research Of Netherlands , 4 INAF/Istituto di Astrofisica et Planetologia Spaziali , 5 INAF/Istituto di
Astrofisica et Planetologia Spaziali

The X-ray Integral Field Unit (X-IFU) on board the Advanced Telescope for High-ENergy Astrophysics (Athena)
will provide spatially resolved high-resolution X-ray spectroscopy from 0.2 to 12 keV, with 5 arcsec pixels over a fieldof view of 5 arcmin equivalent diameter and a spectral resolution of 2.5 eV up to 7 keV. We will first present how
the core scientific objectives of Athena drive the main performance parameters of the X-IFU, namely the spectral
resolution, the field of view, the eﬀective area, the count rate capabilities, and the instrumental background. Then we
will describe how the performance can be met using a 3840 microcalorimeters array operated at 50 mK and present
the key system issues driving the design of the instrument.
The X-IFU will be provided by an international consortium led by France, The Netherlands and Italy, with further
ESA member state contributions from Belgium, Finland, Germany, Poland, Spain, Switzerland and two international
partners from the United States and Japan.
category : Applications25

O-18 Design and status of TIME, a mm-wavelength spectrometer array for [CII]
intensity mapping
Jonathon Hunacek1 , James Bock2 , C. Matt Bradford3 , Tzu-Ching Chang4 , Yun-Ting Cheng5 , Asantha Cooray6 ,Abigail Crites7 , Steve Hailey-Dunsheath8 , Daewook Kim9 , Chao-Te Li10 , Daniel Marrone11 , Lorenzo Moncelsi12 ,Erik Shirokoﬀ13 , Guochao Sun14 , Isaac Trumper15 , Anthony Turner16 , Bade Uzgil17 , Michael Zemcov18
1

9

California Institute of Technology, 2 Caltech / JPL , 3 Caltech / JPL , 4 JPL , 5 Caltech , 6 UC Irvine , 7 Caltech , 8 Caltech ,University of Arizona , 10 ASIAA , 11 University of Arizona , 12 Caltech , 13 University of Chicago , 14 Caltech , 15 University of
Arizona , 16 JPL , 17 UC Irvine , 18 RIT

TIME is a mm-wavelength spectrometer array that will map fluctuations of the 157.7 μ m emission line of singly
ionized carbon ([CII]) during the Epoch of Reionization (redshift z 5 to 9). A 14 x 0.43 arcmin instantaneous
field of view corresponding to 16 x 1 spatial pixels is sampled by two banks single-polarization grating spectrometers(32 spectrometers total). Each spectrometer consists of an input feedhorn, a parallel-plate waveguide, and a curved
diﬀraction grating (similar to that used in Z-Spec) with resolving power R = 170 and spectral range 183 to 326 GHz.
The output arc of each spectrometer is sampled at R 100 with 60 TES bolometers, of which 16 on the band edges areused for atmospheric monitoring and removal. The TESs (1920 total) are designed in close-packed buttable arrays of
8 spatial x 12 spectral (high frequency) or 8 spatial x 8 spectral (low frequency) pixels, and will be operated from a
250 mK base temperature with a photon-noise-dominated NEP 1e-17 W/sqrt(Hz). Each bolometer consists of gold
absorber on a 3 x 3 mm silicon nitride micro-mesh suspended near the corners by 1 x 1 x 500 um silicon nitride legs.
Absorbed radiation is thermally coupled to elemental Al and Ti TESs connected in series (Al is used in higher-loading
lab conditions). Detector readout uses SQUIDs and time-domain multiplexing.
This talk will briefly motivate the science objectives of TIME and will detail the design and status of the TIME
instrument. The optical and mechanical design of the spectrometer and detector arrays will be highlighted, including
results from laboratory tests of prototypes. Additionally, the detector magnetic shielding design and the operation ofa pair of 3He sorption fridges for continuous 350 mK cooling will be discussed.
category : Applications

26

MKIDS 327

O-19 Modelling the Performance of Single-Photon Counting Kinetic Inductance
Detectors
Josie Dzifa Akua Parrianen1 , Simon Doyle2 , Enzo Pascale3
1

School of Physics and Astronomy, Cardiﬀ University, 2 School of Physics and Astronomy, Cardiﬀ University , 3 School ofPhysics and Astronomy, Cardiﬀ University / Dipartimento di Fisica, Sapienza Universita Di Roma

A principal goal of the next generation of space-based astronomy will be dedicated to the characterisation of extrasolar planets (exoplanets). Of the 1000s discovered only a handful have been characterised beyond their size and mass,
thus there is increasing interest in new exoplanet missions aiming to carry out spectroscopy on very low intensity lightand shallow transit light curves. Energy-resolving, single-photon counting detectors provide an elegant solution forcarrying out spectroscopy without the need for gratings, prisms or combinations thereof.
The Lumped Element Kinetic Inductance Detector (LEKID) is a proven technology capable of counting and energyresolving single-photon events at optical and near infra-red wavelengths. Furthermore, LEKIDs can be multiplexed
into large format arrays with over a 1000 detectors being read out on a single pair of coaxial cables. The combinationof exquisite sensitivity and high multiplexing ratios makes spectroscopic imaging possible, using a LEKID focal planeand simple imaging optics.
While sensitivities yielding noise equivalent powers (NEPs) of order 10−19 W− 1 have been demonstrated in arraysHz2of order 103 pixels at sub-mm wavelengths, the corresponding theoretical energy resolution due to single-photon
events has yet to be met. Using conventional superconductor theory we discuss and validate a model that describes
the energy-resolving performance of an Aluminum LEKID to single-photon absorption events. While Aluminium is
not the optimum material to use in single-photon counting applications, this material is well understood and is used
to understand the underlying device physics of these detectors. We conclude by discussing how we can apply the steps
required to adapt this model for use with more suitable materials; such as Titanium Nitride or bi-layer superconducting
films.
category : Sensor Physics & Developments

28

O-20 Ultrasensitive kilo-pixel imaging array of photon noise limited Kinetic
Inductance Detectors over an octave of bandwidth for THz astronomy
Juan Bueno1 , Ozan Yurduseven2 , Stephen J. C. Yates3 , Nuria Llombart4 , Vignesh Murugesan5 , Kenichi Karatsu6 ,David J. Thoen7 , Andrey M. Baryshev8 , Andrea Neto9 , Jochem J. A. Baselmans10
1

SRON, 2 Terahertz Sensing Group, Delft University of Technology , 3 SRON Netherlands Institute for Space Research,Groningen , 4 Terahertz Sensing Group, Delft University of Technology , 5 SRON ? Netherlands Institute for Space Research,
Utrecht , 6 Terahertz Sensing Group, Delft University of Technology , 7 Terahertz Sensing Group, Delft University ofTechnology , 8 SRON Netherlands Institute for Space Research, Groningen / Kapteyn Astronomical Institute, University ofGroningen , 9 Terahertz Sensing Group, Delft University of Technology , 10 SRON Netherlands Institute for Space Research,
Utrecht / Terahertz Sensing Group, Delft University of Technology

We present the development of an ultra-sensitive kilo-pixel imaging array of ultra-wide bandwidth, background limited
kinetic inductance detectors (KIDs) suitable for THz astronomy applications to be used in space based observatories.
The array consists of 989 KIDs, in which the THz radiation is coupled via a leaky lens antenna, covering the frequency
range between 1.4 and 2.8 THz. The single pixel performance is fully characterised using a representative small
array in terms of sensitivity, optical eﬃciency, beam pattern and frequency response, matching very well its expected
performance. These results have been submitted to Applied Physics Letters. The kilo-pixel array is characterised
electrically, with a very good overall performance. It has a yield larger than 90% and an averaged noise-equivalent
power lower than 3x10−19 W/Hz1/2 . The expected dead time due cosmic ray interactions, when operated in an L2 ora similar far-Earth orbit, is found to be lower than 0.5%. The figure shows an ultrasensitive kilo-pixel imaging array:A) Photograph of the kilo-pixel array in its holder; B) Back illuminated optical image of the centre area of the array.
The light goes through the membrane, where both the antenna and the Al section of the KID are fabricated; C) Backand front illuminated optical image of a single pixel. The bright square indicates the area of the membrane, where
illumination from the chip backside brightens the image. The NbTiN section of the KID and the transmission line
are fabricated on the solid substrate; D) SEM image of the centre of the antenna where the narrow Al line can be
resolved. This work demonstrates that KID technology can provide mature enough technology to be considered for
future space based observatories.

category : Sensor Physics & Developments

29

O-21 Development of Multi-Chroic MKIDs for Next-Generation CMB Polarization
Studies
Bradley R. Johnson1 , Daniel Flanigan2 , Maximilian H. Abitbol3 , Peter A. R. Ade4 , Sean Bryan5 , Hsiao-Mei Cho6 ,Rahul Datta7 , Peter Day8 , Simon Doyle9 , Kent Irwin10 , Glenn Jones11 , Sarah Kernasovskiy12 , Dale Li13 , Phil
Mauskopf14 , Heather McCarrick15 , Jeﬀ McMahon16 , Amber Miller17 , Yanru Song18 , Carole Tucker19
1

Department of Physics, Columbia University, 2 Columbia University , 3 Columbia University , 4 Cardiﬀ University , 5 ArizonaState University , 6 SLAC National Accelerator Laboratory , 7 NASA/GSFC , 8 NASA/JPL , 9 Cardiﬀ University , 10 Stanford
University / SLAC National Accelerator Laboratory , 11 Columbia University , 12 Stanford University , 13 SLAC National
Accelerator Laboratory , 14 Arizona State University , 15 Columbia University , 16 University of Michigan , 17 University ofSouthern California , 18 Stanford University , 19 Cardiﬀ University

We report on the status of an ongoing eﬀort to develop 23-element prototype arrays of horn-coupled, polarizationsensitive microwave kinetic inductance detectors (MKIDs) that are each sensitive to two spectral bands between 130 and
280 GHz. These multi-chroic MKID arrays are tailored for the next-generation, large-detector-count experiments thatare being designed to simultaneously characterize the polarization properties of both the cosmic microwave background(CMB) and Galactic dust emission. Our horn-coupled device design builds from the successful transition edge sensor(TES) bolometer architecture that is now being used in Advanced ACTPol. Our research program has focused on (i)developing and testing the required microstrip-to-CPW coupling between the on-chip polarimeter circuit and the CPW
MKID, (ii) transferring the design to a SOI-based construction to minimize TLS noise, and (iii) demonstrating thatthe performance of theses arrays is competitive with arrays of similar TES-based devices. We present our device designand show results from laboratory-based characterization measurements of our first array. The 23-element prototype
arrays we are building contain 92 MKIDs, so we are currently demonstrating a multiplexing factor of 92. However,the bandwidth of our ROACH-2-based readout system should ultimately allow multiplexing factors of approximately
1000 or more, so as part of this program we are pushing forward the multiplexing capabilities that will be needed in
next-generation experiments. Finally, we will discuss our plans for scaling up our prototype arrays. The prototype
array design in hand is directly scalable to 331 elements, so for example, seven of these future arrays could be tiled
into a 9268 detector array.

category : Sensor Physics & Developments30

O-22 Millimeter-Wave Polarimeters Using Kinetic Inductance Detectors for TolTEC
and Beyond
Jason Edward Austermann1 , Jiansong Gao2 , Johannes Hubmayr3 , Michael Vissers4 , James Beall5 , Bradley Dober6 ,Shannon Duﬀ7 , Weijie Guo8 , Gene Hilton9 , Christopher McKenney10 , Joel Ullom11 , Jeﬀ Van Lanen121

National Institute of Standards and Technology (NIST), 2 National Institute of Standards and Technology , 3 National
Institute of Standards and Technology , 4 National Institute of Standards and Technology , 5 National Institute of Standards
and Technology , 6 National Institute of Standards and Technology , 7 National Institute of Standards and Technology ,8National Institute of Standards and Technology , 9 National Institute of Standards and Technology , 10 National Institute ofStandards and Technology , 11 National Institute of Standards and Technology , 12 National Institute of Standards andTechnology

Microwave Kinetic Inductance Detectors (MKIDs) provide a compelling path forward to the large-format polarimeter,
imaging, and spectrometer arrays needed for next-generation experiments in millimeter-wave cosmology and astronomy.
In this presentation, we describe the development and lab measurement of feedhorn-coupled, background-limited MKID
polarimeters for the TolTEC millimeter-wave imager being constructed for the 50-meter Large Millimeter Telescope(LMT) and beginning observations in late 2018. TolTEC will comprise over 6,000 polarization sensitive MKIDs andwill represent the first MKIDs fabricated and deployed on monolithic 150 mm diameter silicon wafers – a criticaldevelopment towards future large-scale experiments with O(105 ) detectors. TolTEC will operate in observational
bands of 1.1, 1.4, and 2.1 mm and will use dichroics to define a physically independent focal plane for each passband,
thus allowing the polarimeters to use simple, direct-absorption inductive structures that are impedance matched toincoming radiation. This work is part of a larger program headed by NIST-Boulder in the development of MKIDbased detector technologies for use at a wide range of photon energies, from millimeter wavelengths to X-rays. We
describe the detailed pixel design and the results of a large array of simulations used to optimize the polarimeter
performance. We present measurements of prototype devices and compare the measured optical performance to thesimulated predictions of absorption and polarization eﬃciency. We also present characterization of the detector noise
performance, bandpass response, responsivity, and properties of the superconducting materials used in these devices.
Additionally, we discuss our fabrication processes and the resulting uniformity of material properties and detector
characteristics across 150 mm diameter wafers.
category : Sensor Physics & Developments

31

TES 132

O-23 Quantitatively characterizing sources of energy resolution degradation in TES
microcalorimeters AC-biased at MHz frequencies.
Christine Goodwin Pappas1 , Dan Becker2 , Douglas Bennett3 , Johnathon Gard4 , John Mates5 , Dan Schmidt6 , Daniel
Swetz7 , Joel Ullom81National Institute of Standards and Technology (NIST), 2 National Institute of Standards and Technology (NIST) , 3 National
Institute of Standards and Technology (NIST) , 4 National Institute of Standards and Technology (NIST) , 5 National Instituteof Standards and Technology (NIST) , 6 National Institute of Standards and Technology (NIST) , 7 National Institute ofStandards and Technology (NIST) , 8 National Institute of Standards and Technology (NIST)MHz frequency-domain SQUID multiplexing (FDM) is potentially an attractive readout architecture to increase themultiplexing factor and reduce wiring complexity to large arrays of TES microcalorimeters. This readout concept,
currently baselined as the readout for the ATEHNA XIFU, requires the TESs to be AC-biased. However, multiple
groups have reported that devices tested under AC bias exhibit poorer energy resolution than similar sensors under
DC bias. Currently, it is not thoroughly understood why the energy resolution degrades under AC bias, and whether
this observed degradation is inherent to the technique. In this presentation, we describe two factors that are believed
to contribute to the energy resolution degradation: AC loss in the TES s superconducting state and AC weak-link
Josephson Junction eﬀects. We present results from a recent study of the importance of these two eﬀects to device
resolution and describe eﬀorts to mitigate them.
The dissipation observed in the superconducting state of the TES under AC bias is thought to reduce alpha (thelogarithmic derivative of the TES resistance with respect to temperature) and therefore degrade energy resolution. It
has been suggested that this superconducting loss is caused by inductive coupling between the bias leads and normal
metal structures on the TES. The data so far is qualitatively consistent with this hypothesis, but the complex TES
designs under consideration for ATHENA XIFU are diﬃcult to model and compare quantitatively with the theory.
We have fabricated a variety of simple devices to quantitatively test this hypothesis without the need for numericalmodels. In addition, we explore some proposed routes towards reducing the AC superconducting loss in TES devices:using higher resistivity materials for the normal metal structures, positioning the leads further away from the TES,
and adjusting the geometry of the normal metal structures.
AC weak link eﬀects arising from the interaction between the TES and the higher Tc leads create non-linear featuresin the current-voltage relation of the TES. This non-linear structure makes pulse shapes diﬃcult to analyze and may
be an additional source of noise. A TES is in the two-fluid/phase-slip line regime when its transition is dominated byphysics in the TES itself and not interaction with the leads. Because the TES is operated near its critical temperature,long range weak link eﬀects may persist even as the TES length is increased beyond the geometries that have beenmeasured so far. To explore the regime of negligible weak link eﬀects, we have characterized TESs with normal metal
structures designed to completely decouple the TES from the leads. We will discuss whether these devices exhibit theundesirable non-linearities observed in strongly weak link devices.
While previous studies of TES calorimeter performance under MHz frequency AC bias have used MHz FDM
readout, here we read out the TESs with high-bandwidth microwave SQUID readout circuits.?This will allow us toseparate for the first time the intrinsic performance of the TES under AC bias from any eﬀects due to the MHz FDM
readout.
category : Sensor Physics & Developments

33

O-24 Josephson eﬀects in frequency domain multiplexed TES microcalorimeters andbolometers
Luciano Gottardi1 , Stephen J. Smith2 , Hiroki Akamatsu3 , Jan van der Kuur4 , Simon R. Bandler5 , Marcel P.
Bruijn6 , James A. Chervenak7 , Jan R. Gao8 , Roland den Hartog9 , Brian D. Jackson10 , Pourya Khosropanah11 ,Antoine R. Miniussi12 , Kenichiro Nagayoshi13 , Marcel Ridder14 , Jack Sadleir15 , Kazuhiro Sakai16 , Nick Wakeham17
1

SRON - Netherlands Institute for Space Research, 2 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA /CRESST and University of Maryland, Baltimore County, MD 21250, USA , 3 SRON Netherlands Institute for Space Research,
Utrecht, the Netherlands , 4 SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The
Netherlands , 5 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA , 6 SRON Netherlands Institute for Space
Research, Utrecht, the Netherlands , 7 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA , 8 SRON Netherlands
Institute for Space Research, Utrecht, the Netherlands / Kavli Institute of NanoScience, Delft University of Technology, Delft,
the Netherlands , 9 SRON Netherlands Institute for Space Research, Utrecht, the Netherlands , 10 SRON Netherlands Institutefor Space Research, Landleven 12, 9747 AD Groningen, The Netherlands , 11 SRON Netherlands Institute for Space Research,
Utrecht, the Netherlands , 12 NASA Postdoctoral Program, Universities Space Research Assoc., Greenbelt, MD 20771, USA ,13
SRON Netherlands Institute for Space Research, Utrecht, the Netherlands , 14 SRON Netherlands Institute for Space
Research, Utrecht, the Netherlands , 15 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA , 16 CRESST and
USRA, 7178 Columbia Gateway Drive, Columbia, Maryland 21046, USA , 17 NASA Postdoctoral Program, Universities Space
Research Assoc., Greenbelt, MD 20771, USA

Frequency-division multiplexing (FDM) is the baseline readout system for large array of superconducting transitionedge sensors (TES’s) under development for the X-ray and infrared instruments like X-IFU (Athena) and SAFARI(SPICA), respectively. In this multiplexing scheme, the sensors are AC biased at diﬀerent frequencies from 1 to 5 MHz
and operate as amplitude modulator. Weak superconductivity is responsible of the complex TES resistive transition,
experimentally explored in the very details so far, both with DC and AC biased read-out schemes. In this paper we will
review the current status of our understanding of the physics of the TES’s and their interaction with the FDM circuit.
In the past, we have shown that an AC biased TES can be described by non-linear, first order diﬀerential equations
derived from the resistively shunted junction model. The analytical solution of these equations have been used todescribe the experimental observations in TiAu TES bolometers biased at MHz frequencies. We have recently shown
from the numerical solutions of the same equations that we can obtain a qualitative explanation of the phenomena
observed in the I-V characteristic of AC biased TES microcalorimeters.
We are studying the behavior of the TES non-linear impedance, along the superconducting transition, for several detector families, namely: high normal resistance TiAu TES bolometers, low normal resistance MoAu TES
microcalorimeters and high normal resistance TiAu TES microcalorimeters. In this paper we will report on the
progress of this comparison. In particular we will focus on the influence of the FDM read-out circuit on the single
pixel impedance.
category : Sensor Physics & Developments34

O-25 Development of TES microcalorimeters for 10-50 keV using a gold absorber
Haruka Muramatsu1 , Tasuku Hayashi2 , Keisei Maehisa3 , Yuki Nakashima4 , Takehiro Kuroiwa5 , Takahiro
Nakayama6 , Kazuhisa Mitsuda7 , Noriko Y Yamasaki8
1

ISAS, 2 ISAS/JAXA , 3 ISAS/JAXA , 4 ISAS/JAXA , 5 Kyushu University , 6 ISAS/JAXA , 7 ISAS/JAXA , 8 ISAS/JAXA

TES microcalorimeter are high-energy-resolution spectrometers not only in soft X-ray energy range (0.3-10 keV),
but also in hard X- ray energy range (up to ∼ 100 keV). We have developed TES microcalorimeters with gold absorberas a soft X-ray spectrometer for a scanning transmission electron microscope to determine the emission lines from mostof low-Z atoms (H.Muramatsu et al., 2016). On the other hand, in the energy range of 10 to 50 keV there are some Klines of high Z atoms and some nuclear transition lines of interest (K.Maehata et al., 2015). TES microcalorimeters
can be useful to resolve fine structure of lines and to detect weak lines in this range. We studied whether we can simply
extend our microcalorimeters to this energy range. We first studied the energy resolution in 10 to 50 keV energy range
using the present detectors. Although the detection eﬃciency is low, it may not be a problem in some of applications.
The small heat capacity of soft X-ray TES has an advantage in intrinsic energy resolution, i.e. energy resolution at 0
eV. However, the energy resolution will be degraded by two reasons; energy-dependent of pulse shape and non-linear
response in energy to pulse height. We can avoid those eﬀect by using larger heat capacity device. We compered
the performances of a TES microcalorimeter (A) with 0.6 pJ/K heat capacity whose design value of intrinsic energy
resolution is 4.3 eV, and a TES microcalorimeter (B) with 3.7 pJ/K heat capacity whose intrinsic energy resolution
is 14 eV. As expected, device (A) strongly suﬀered from signal saturation and nonlinear response above ∼ 10 keV,
while device (B) did not. After correcting for the pulse saturation and non- linear response, we obtained 16 eV and
25 eV energy resolutions at 18 keV and 26 keV for device (A), while it was constant at 22 eV for device (B). We
consider that it is worth using TES microcalorimeters in the energy rage where it starts to saturates, depending on
the application and the energy range.
category : Sensor Physics & Developments

35

TES 2/Bolometer36

O-26 Noise equivalent power and energy resolution of transition-edge sensors withcomplex thermal models
Ilari Maasilta1
1

Department of Physics, University of Jyvaskyla

Sometimes transition-edge sensors (TES) have thermal circuits with more than one heat capacity, I call those thermal models complex. In previous publications, I have discussed analytical equations and numerical examples for thecomplex impedance, responsivity and noise of such devices [1]. Here, I continue that work and calculate the noise
equivalent power and energy resolution for such complex devices, arguably the most interesting parameters for detectors. The implications of the diﬀerences of the models are discussed, concentrating on the following questions: How
do we get optimal performance out of such devices? Can there be any benefits of complex thermal circuits? The focus
will be kept mostly on the simplest complex models with two heat capacities.
[1] I. J. Maasilta, AIP Advances 2, 042110 (2012)
category : Sensor Physics & Developments37

O-27 Exploring the eﬀects of size and geometry of normal metal features on thetransition shapes and performance of transition-edge sensor microcalorimeters
Nicholas Wakeham1 , Joseph S Adams2 , Simon R Bandler3 , James A Chervenak4 , Aaron M Datesman5 , Megan E
Eckart6 , Fred M Finkbeiner7 , Richard L Kelly8 , Caroline A Kilbourne9 , Antoine R Miniussi10 , Frederick S Porter11 ,John E Sadleir12 , Kazuhiro Sakai13 , Stephen J Smith14 , Edward J Wassell15 , Wonsik Yoon16
1

NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore
County , 3 NASA Goddard Space Flight Center , 4 NASA Goddard Space Flight Center , 5 NASA Goddard Space Flight Center/ SGT, Inc. , 6 NASA Goddard Space Flight Center , 7 NASA Goddard Space Flight Center / Wyle Information Systems ,8NASA Goddard Space Flight Center , 9 NASA Goddard Space Flight Center , 10 NASA Goddard Space Flight Center /CRESST II - University of Maryland Baltimore County , 11 NASA Goddard Space Flight Center , 12 NASA Goddard Space
Flight Center , 13 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 14 NASA
Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 15 NASA Goddard Space Flight
Center / SGT, Inc. , 16 NASA Goddard Space Flight Center / NPP - Universities Space Research Association

The spectral resolution of transition-edge sensor (TES) microcalorimeters is very sensitive to the specific dependenciesof the resistance R in the superconducting transition on the current I, magnetic field B, and temperature T. In
particular, it has been shown that transitions that are very steep in (R,T) space lead to a significant noise term, inexcess of conventional expectations. This so-called unexplained noise is known to be reduced by the additionof normal metal stripes across the TES perpendicular to the direction of current flow. These normal metal stripes
have been shown to drastically alter the oscillatory patterns seen in measurements of the critical current as a functionof magnetic field. However, there are many remaining questions about the exact impact of the stripes on current
distributions within the TES, the oscillatory field pattern and, therefore, the shape of the R(I, B, T) surface.
Through measurements of the resistance under DC bias of TES devices of various sizes, with diﬀerent stripe patterns
and dimensions, we will discuss how these stripes can aﬀect the R(I, B, T) surface. In addition, using measurements
and analysis of the noise spectra of various devices we will present how these changes to the stripe pattern may aﬀect
the performance of the TES. In particular, we will discuss strategies to reduce the presence of localized discontinuities
in the derivative of R, associated with increased noise, while maintaining the globally low levels of unexplained noise
currently achieved with conventional metal stripe patterns. Implementing these strategies is a path towards producing
large arrays with highly uniform transitions and high spectral resolution. These large uniform arrays will be required
for future x-ray astronomy applications, such as the X-IFU on ATHENA.
category : Sensor Physics & Developments38

O-28 Dependence of transition width on current and critical current intransition-edge sensors
Kelsey M Morgan1 , Christine G Pappas2 , Douglas A Bennett3 , Johnathon D Gard4 , James P Hays-Wehle5 , Gene C
Hilton6 , Carl D Reintsema7 , Daniel R Schmidt8 , Joel N Ullom9 , Daniel S Swetz10
1

National Institute of Science and Technology, 2 National Institute of Standards and Technology , 3 National Institute ofStandards and Technology , 4 National Institute of Standards and Technology / University of Colorado Boulder , 5 National
Institute of Standards and Technology / University of Colorado Boulder , 6 National Institute of Standards and Technology ,7
National Institute of Standards and Technology , 8 National Institute of Standards and Technology , 9 National Institute ofStandards and Technology / University of Colorado Boulder , 10 National Institute of Standards and Technology

In transition-edge sensor (TES) X-ray detectors we observe that as we increase the thermal conductance (G) to the heatbath, α (T/R ∂R/∂T at constant I) decreases, indicating that the resistive transition has broadened. Consequently,
the energy resolution for single-photon detection worsens. Using a two-fluid model for the superconducting-to-normaltransition and the Ginsburg-Landau expression for Ic (T ) in a thin film, we show that α can be written as a function of(I0 /Ic0 )2/3 , where I0 is the TES bias current, and Ic0 is the film s critical current at zero temperature. Therefore, thebroadening observed as G increases can be attributed to the larger current (I0 ) necessary to bias the TES at a given
point in the transition. To recover a sharper transition, we fabricated rectangular devices with varying numbers ofnormal-metal bars while keeping G constant. Increasing the normal resistance reduces I0 , and increasing the spacing
between normal-metal bars increases Ic0 . By independently varying both I0 and Ic0 , we show that it is possible tomanipulate the transition width and G independently, thus enabling fast sensors with excellent energy resolution. We
also show that the eﬀects on the transition shape of commonly used normal-metal features such as bars across the
TES bilayer can be well predicted from their eﬀect on Ic0 .
Using this new theoretical understanding, we have demonstrated sensors with thermal time constants below 100µs while maintaining 1.05 eV resolution at 1.25 keV. We will present characterization data, including fits to noise andcomplex impedance, that predict resolution of 0.7 eV when operating in the linear regime below 1 keV. This level of
performance is required for the TES array for the recently approved soft x-ray microcalorimeter spectrometer for the
Linac Coherent Light Source upgrade (LCLS-II) x-ray free electron laser at SLAC National Accelerator Laboratory.
This instrument, being jointly developed by SLAC and Stanford University, aims to maintain approximately 1 eV
resolution while operating with photon fluxes generated from the 10 kHz repetition rate of LCLS-II. Building on theseresults, we will discuss techniques for designing sensors that optimize resolution and throughput collecting at a given
photon rate.
category : Sensor Physics & Developments39

O-29 Characterization of Mid-Frequency Arrays for Advanced ACTPol
Steve K. Choi11

Department of Physics, Princeton University

The Advanced ACTPol upgrade on the Atacama Cosmology Telescope aims to improve the measurement of the cosmic
microwave background polarization anisotropies, using four new dicroic detector arrays fabricated on 150 mm Si wafers.
These bolometric cameras use AlMn transition edge sensors coupled to feedhorn with orthomode transducers. The
first camera, sensitive to both 150 GHz and 230 GHz, has been deployed and in operation. Here we present the lab
characterization of the dark thermal parameters and optical eﬃciencies on the two newest fielded arrays, each sensitive
to both 90 GHz and 150 GHz. The level of systematic uncertainties is evaluated to assess the parameter uniformity
across each array. Lastly, we show their initial optical performances in the field.
category : Sensor Physics & Developments40

O-30 Characterization of Si-membrane TES bolometer arrays for the HIRMES
instrument
Emily M. Barrentine1 , Karwan Rostem2 , Ari D. Brown3 , Regis P. Brekosky4 , Felipe A. Colazo5 , Nicholas P. Costen6 ,Vorachai Kluengpho7 , Stephen F. Maher8 , Vilem Mikula9 , Timothy M. Miller10 , Joseph B. Oxborrow11 , Elmer H.
Sharp12 , Tomomi Watanabe13 , Edward J. Wollack14 , Wen-Ting Hsieh15 , S. Harvey Moseley16
1

NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center , 3 NASA Goddard Space Flight Center , 4 NASA
Goddard Space Flight Center , 5 NASA Goddard Space Flight Center , 6 NASA Goddard Space Flight Center , 7 NASA
Goddard Space Flight Center , 8 NASA Goddard Space Flight Center , 9 NASA Goddard Space Flight Center , 10 NASA
Goddard Space Flight Center , 11 NASA Goddard Space Flight Center , 12 NASA Goddard Space Flight Center , 13 NASA
Goddard Space Flight Center , 14 NASA Goddard Space Flight Center , 15 NASA Goddard Space Flight Center , 16 NASA
Goddard Space Flight Center

The High Resolution Mid-Infrared Spectrometer (HIRMES) instrument will fly onboard NASA’s airborne Stratospheric
Observatory for Infrared Astronomy (SOFIA) in 2019. HIRMES will provide astronomers with a unique observing
window (25-122 µm) for exploring the evolution of protoplanetary disks into young solar systems, and the composition
λ= 100,000)
of our Solar System. There are two focal plane detector arrays for the instrument: a high-resolution ( ∆λ√λ−18
8×16 detector array, with a target noise-equivalent power, NEP ≤ 3 × 10
W/ Hz; and a low-resolution ( ∆λ=√−172,000-19,000) 16×64 detector array with a target NEP ≤ 2 × 10 W/ Hz. The detectors for both of these arrays
are superconducting Mo/Au bilayer transition edge sensor (TES) bolometers on thin suspended single-crystal silicon
membranes. Here we present our characterization results for the detectors in both arrays, including measurements ofthermal conductance with comparison to phonon transport models, saturation power, noise, and array uniformity.
category : Sensor Physics & Developments41

O-31 Characterization of optical transition-edge sensors
Kaori Hattori1 , Ryo Kobayashi2 , Shuichiro Inoue3 , Daiji Fukuda4
1

Quantum optical measurement group National Metrology Institute of Japan , 2 Nihon Univ. , 3 Nihon Univ. , 4 AIST

Optical transition edge sensor (TES) detectors which can resolve an energy of a single optical photon have provendesirable in quantum information and biological imaging. We have developed a gold-titanium bilayer TES embedded
in cavity structure designed to detect photons in a few eV range and lower than this. The TES is formed on a mirror,
covered by an anti-reflection coating. The detector has achieved high detection eﬃciency, nearly 100 % at 1,550 nm(0.8 eV), and an energy resolution of 0.2 eV for 0.8-eV photons. Higher energy resolution is required for an applicationof the TES in multicolor fluorescence microscopy. To improve the energy resolution, understanding the physics ofthe optical TES is necessary. Because of unique features of the optical TES, the underlying physics may be diﬀerent
from that of TESes designed to be used in other applications. The optical TES is characterized by: (1) its small size
(typically 5 to 10 µm) to be sensitive to the low-energy photons and (2) a fast response time (τ ∼ 200 ns) determinedby the heat capacity and weak thermal coupling between electrons and phonons in the detector. Measurements ofa complex impedance (response to a small voltage signal) of the TES can reveal a thermal model of the TES andprovides an expected energy resolution based on the measured parameters of the detectors. We have measured thecomplex impedance up to 20 MHz to examine the fast detector response. We will show the results and discuss theproperties of the TES.
category : Sensor Physics & Developments42

O-32 Eliminating anomalous low energy tails in hard X-ray TES microcalorimeters
using electroplated bismuth
Daikang Yan1 , Ralu Divan2 , Lisa M. Gades3 , Timothy J. Madden4 , Antonino Miceli5 , Umeshkumar M. Patel6 ,Orlando Quaranta7 , Daniel Becker8 , Douglas A. Bennett9 , James P. Hays-Wehle10 , Gene C. Hilton11 , Johnathon
Gard12 , John A. B. Mates13 , Kelsey M. Morgan14 , Carl D. Reintsema15 , Daniel R. Schmidt16 , Daniel S. Swetz17 ,Joel N. Ullom18 , Leila Vale19
1

Applied Physics, Northwestern University, 2 Argonne National Laboratory - USA , 3 Argonne National Laboratory - USA ,4
Argonne National Laboratory - USA , 5 Argonne National Laboratory - USA , 6 Argonne National Laboratory - USA ,7
Argonne National Laboratory - USA , 8 National Institute of Standards and Technology - USA / University of Colorado,
Boulder - USA , 9 National Institute of Standards and Technology - USA , 10 National Institute of Standards and Technology USA , 11 National Institute of Standards and Technology - USA , 12 University of Colorado, Boulder - USA , 13 University ofColorado, Boulder - USA , 14 National Institute of Standards and Technology - USA , 15 National Institute of Standards andTechnology - USA , 16 National Institute of Standards and Technology - USA , 17 National Institute of Standards andTechnology - USA , 18 National Institute of Standards and Technology - USA / University of Colorado, Boulder - USA ,19
National Institute of Standards and Technology - USA

The theoretical energy resolution achievable with a transition edge sensor (TES) microcalorimeter is proportional
to the square root of heat capacity. Since the eﬃcient detection of hard X-rays generally requires thick absorbers,
high-Z and low heat capacity materials are desirable. Bismuth (Bi) is one such material for X-ray TES absorbers.
In particular, evaporated Bi has been extensively used for X-ray TES spectrometers. However, many TESs with
evaporated Bi absorbers exhibit low energy tails in their spectral response, which complicates X-ray line shape analysis
and degrades the detectability of weak emission lines at lower energies relative to stronger emission lines. While theprecise mechanism is uncertain, it is clear that thermalization eﬀects in the evaporated Bi are responsible for the low
energy tailing. In order to eliminate the tails from Bi absorbers, we have developed a Bi electroplating process. In
order to facilitate the comparison, we fabricated TESs with absorbers composed of gold (Au), Au with evaporated Bi
and Au with electroplated Bi from the same wafer. Here we present heat capacity and energy spectra measurements
for these devices. The evaporated and electroplated Bi devices exhibit comparable heat capacities and no measurable
addition to the total heat capacity budget with respect to the devices with Au only absorbers. Yet, our results confirm
the presence of a low energy tail in the evaporated Bi devices, while both the Au and electroplated Bi devices show
little evidence of such tails. This work definitively demonstrates the superiority of electroplated Bi over evaporated Bi.
Microscopy on the Bi films shows that the grain size of electroplated Bi films is significantly larger than for evaporated
films, which may contribute to improved x-ray thermalization.
category : Sensor Physics & Developments43

O-33 A Static and Dynamic Physical Model for Deposition of Energy via Cosmic
Rays into Sub-Kelvin Bolometric Detectors
Samantha Lynn Stever1 , Francois Couchot2 , Noel Coron3 , Bruno Maﬀei4
1

Institut d’Astrophysique Spatiale / CNRS, 2 Laboratoire de l’Accelerateur Lineaire , 3 Institut d’Astrophysique Spatiale ,4Institut d’Astrophysique Spatiale

Cosmology space missions are particularly sensitive to systematic eﬀects resulting from interaction between cosmic
rays and their highly sensitive bolometric detectors. This cosmic ray signal is superimposed to the signal of interest
resulting from CMB mapping and from the much larger foreground components in the sky. To remove this signal,
one must first understand the deposition of energy into these detectors. Since Planck, empirical study, resulting fromlaboratory measurements on spare bolometers, has been made to remove the cosmic ray signal, or glitch , fromscience data. However, a complete physical model for the energy deposition by cosmic rays into these detectors hasremained unrealised. Using a well-known NTD germanium bolometer from the ground-based DIABOLO experiment,
we simulate the eﬀect of cosmic rays using a radioactive source in the laboratory, and develop in parallel a physicallymotivated model which reproduces the signal of a cosmic ray glitch . Through analysis of experimental data, wefind that the glitch signal shape is a function of incoming particle position and angle, as well as the incoming particle
energy. We report also on nonlinear eﬀects in the detector and their origin, as well as their reproducibility in a dynamic
physical model of the bolometer. Once such a physical model is established, we intend to apply it to new generationsof detectors in candidates for future CMB missions such as PIXIE and LiteBIRD.
category : Sensor Physics & Developments

44

Application - Dark matter, neutrino andrelated physics 1

45

O-34 New-generation cryogenic detectors for dark matter and coherent neutrino
scattering
Raimund Strauss1
1

Max-Planck-Institut for Physics, Munich

Cryogenic particle detectors have been constantly improved over the last decades and nowadays find broad applicationin rare-event searches. In recent years, there was significant progress in lowering the energy threshold for nuclear recoils
to the 100eV-regime and below. These detectors enable new experimental approaches, in particular the detection of
sub-GeV dark matter particles and coherent neutrino-nucleus scattering. In the talk, I discuss the current and nextgeneration detector technology of cryogenic dark matter experiments and review recent results. Furthermore, I would
like to point out the high potential of cryogenic devices for a discovery of coherent neutrino-nucleus scattering.
category : Applications46

O-35 Using defect creation to discriminate dark matter signal in phonon-mediateddetectors
Fedja Kadribasic1 , Nader Mirabolfathi2 , Kai Nordlund3 , Eero Holmstrom4 , Flyura Djurabekova51

Department of Physics, Texas A&M University, 2 Department of Physics and Astronomy, Texas A&M University , 3 Helsinki
Institute of Physics and Department of Physics, University of Helsinki , 4 Helsinki Institute of Physics and Department of
Physics, University of Helsinki , 5 Helsinki Institute of Physics and Department of Physics, University of Helsinki

Rare event experiments strive to develop detector technologies with the potential to discriminate signals from theradioactive backgrounds to significantly boost sensitivity. Experiments seeking to detect dark matter or Coherent
Elastic Neutrino Nucleus Scattering (CENNS) are particularly interested in discriminating nuclear recoils originatingfrom signal and electron recoils due to the radioactive background. So far, dual measurement methods such as thosedeveloped by the Cryogenic Dark Matter Search (CDMS) or the Cryogenic Rare Event Search with Superconducting
Thermometers (CRESST) have been the dominant techniques to provide this discrimination. Those methods generally
fail at very low energies, wherein second measurement fundamental noise prevents experiments from reaching therequired thresholds. We examine commonly used material response to low energy nuclear recoils using numericalsimulations of their respective classical interatomic potentials. These simulations, alongside more precise density
functional theory simulations and experiments, predict a nonisotropic, nonlinear energy loss that never produces
phonons due to the nonzero energy required to form defects. Experiments such as the Cryogenic Dark Matter Search(CDMS) and the Mitchell Institute Neutrino Experiment at Reactor (MINER) are actively developing detectors toreach the resolutions necessary to observe this eﬀect. We argue that defect creation from nuclear recoil interactions
distorts the expected spectra in such a way that, statistically, one can discriminate nuclear recoils from electron recoilswith only phonon measurements, especially in the mass range below 10 GeV/c2 .
category : Applications

47

O-36 The CUORE and CUORE 0 experiments at LNGS: detector performance andphysics results
Francesco Terranova1
1

Department of Physics Univ. of Milano Bicocca

The Cryogenic Underground Observatory for Rare Events (CUORE) is the first bolometric experiment searching forneutrinoless double beta decay that has been able to reach the 1-ton scale. The detector consists of an array of 988
TeO2 crystals arranged in a cylindrical compact structure of 19 towers. The construction of the experiment and, inparticular, the installation of all towers in the cryostat was completed in August 2016 and commissioning started in fall2016. The experiment has just completed the pre-operation phase and data taking is commencing. In this talk we will
present the achievements of the CUORE construction phase and the performance of the detector during pre-operation.
Special emphasis will be given on the operation of the CUORE large mass macrobolometers, their characterizationand the performance of the low noise readout system. Physics results from CUORE-0, the first CUORE-style tower
operated in 2013-2015, will also be updated.
IMPORTANT NOTE: The Abstract is submitted by the Speakers Board of the CUORE Collaboration on behalfof the Collaboration. The speaker will be selected as soon as the talk is confirmed.
category : Applications48

O-37 Status and Prospects of the EDELWEISS-III Direct WIMP Search ExperimentAlexandre Juillard1 , Edelweiss Collaboration2
1

Institut de Physique Nucleaire de Lyon, 2 Edelweiss Collaboration

The EDELWEISS collaboration is performing a direct search for WIMP dark matter using an array of up to twentyfour 860g cryogenic germanium detectors equipped with a full charge and thermal signal readout. The experimentis located in the ultra-low radioactivity background of the Modane underground laboratory, in the French-Italian
Frejus tunnel. We present the analysis of data obtained in extended data taking periods. WIMP limits, backgroundrejection factors and measurements of cosmogenic activation are used to assess the performance of the third generationof EDELWEISS detectors in view of the search for WIMPs in the mass range from 1 to 20 GeV/c2. The developments
in progress to pursue this goal in the coming years are also presented.
category : Applications

49

O-38 XMASS; A Dark Matter Search Experiment with Liquid Xenon
Hiroyuki Sekiya1 , XMASS collaboration
1

ICRR, the University of Tokyo

Recently many dark matter direct search experiments have been conducted. Among them, the detectors with noble
liquids, especially liquid Xe detectors, gave the best limits on the dark matter-nucleus cross section so far. First, I
would like to review the principle of direct searches with noble liquid technologies. Then, I will explain the recent
results of XMASS-I. XMASS is a multi-purpose experiment using a single-phase liquid xenon technology locatedunderground at Kamioka Observatory in Japan. XMASS-I detector aims at direct detection of dark matter particles
with 832 kg of liquid xenon. The key concept of XMASS is to use liquid xenon itself for shielding. The detector has
been performed stable operation over 3 years with a very high light yield of 15 photoelectron/keVee. A new result by
annual modulation with 1 keVee energy threshold will be shown with 800 live days x 832 kg exposure in total.
category : Applications

50

Application - Dark matter, neutrino andrelated physics 251

O-39 Low temperature detectors for neutrinoless double beta decay experiments
Yong-Hamb Kim1
1

Center for Underground Physics, Institute for Basic Science

Search for neutrinoless double beta decay (0 νββ) is a key experiment to answer unresolved properties of neutrino.
Experimental observation of 0 νββ will provide a direct answer to the particle type of neutrino (i.e., the Dirac-orMajorana question), validate lepton number violation in the field of particle physics, and confine the absolute massscale of neutrino. A number of large scale experiments have been searching, and are planned to search for 0 νββ.
Low temperature detectors (LTDs) based on thermal calorimetric measurement have been playing a major role in theeﬀort to probe the rare event. In the presentation, current 0 νββ search experiments are introduced with their main
detection technologies. Advantages and challenges using LTD technologies are discussed in comparison with othertechnologies used for 0 νββ. In this review, we summarize past, present and future experiments of LTDs to searchfor 0 νββ.
category : Applications

52

O-40 Search for hidden photon cold dark matter using radio telescopes
Shugo Oguri1 , Nozomu Tomita2 , Taketo Nagasaki3 , Osamu Tajima4 , Junya Suzuki5 , Yoshizumi Inoue6 , Makoto
Minowa7
1

RIKEN Center for Advanced Photonics (RAP), RIKEN, 2 Department of Physics, Faculty of Science, University of Tokyo,
Tokyo 113-0033, Japan , 3 High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan.
, 4 High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan. / The Graduate Univ.
for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193, Japan , 5 High Energy Accelerator Research
Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan. , 6 Department of Physics, Faculty of Science, University ofTokyo, Tokyo 113-0033, Japan , 7 Department of Physics, Faculty of Science, University of Tokyo, Tokyo 113-0033, Japan

Hidden photon (HP) is a candidate for dark matter (DM). DM plays an essential role in forming galaxies in Cosmology.
Most popular candidate of DM is weakly interactive massive particles (WIMPs). Many experiments have attempted
to detect signal from an interaction between WIMPs and atomic nuclei. But there is no evidence for the presence of
WIMP. We focus on alternative candidates of DM, hidden photon cold dark matter (HPCDM). HP is a gauge boson
which arises by introducing extra U(1) gauge field. HPs and ordinary photons have kinetic mixing. As a result, HPs
induce emission of ordinary photons at a reflecting surface. According to Snell’s law, the induced photons are emitted
almost perpendicularly to the mirror. The direction is indiﬀerent of the incoming direction of HPs because the velocity
is small for CDM (v/c ∼ 10−3 ). Some groups have attempted to detect the HPCDM to measure light from sphericalmirrors or combination of plane mirrors and focusing systems.
We suggest a novel method of searching for HPCDM using radio telescopes and low-temperature detectors. Telescopes are designed to concentrate parallel light on detectors in general. All we have to do is to put a plane mirror
in front of the telescope s window and we can realize the HPCDM search experiment. Diversion of telescopes havean advantage in addition to shortening of development time: the telescopes have abilities to change the direction of
the mirrors using pointing system. The direction of the induced photons propagation has a slight deviation fromperpendicular to the mirrors depending on the incident angle to the surface, which provides a way to discriminate
the HPCDM signal from background noise. The wavelength of the induced photon corresponds to the HP mass. It
is meaningful for the expansion of HP mass range to use various detectors which have the sensitivity to the diﬀerent
wavelengths.
We already searched for HPCDM with the mass of around 10−4 eV. We used a millimeter wave spectrometer forsensing of the atmospheric water vapor, KUMODeS. Its sensitivity to the mixing parameter will be five times stronger
than the current limit. In the conference, we report the status of the analysis and show a future plan to use a telescope
developed for observation of CMB polarization, GroundBIRD.
category : Applications

53

O-41 Enhanced Calorimetry Using Helium Evaporation and Field Ionization
George M Seidel1 , Derek Stein2 , Humphrey J Maris3
1

Physics Department, Brown University, 2 Physics Department, Brown University, Providence, RI 02912 USA , 3 Physics
Department, Brown University, Providence, RI 02912 USA

The measurement of small energy deposits in calorimeters having large heat capacities is a challenge faced in a numberof diﬀerent low temperature experiments. For example, the observation of rare events in searches for low-mass dark
matter by direct detection is limited by the threshold energy that can be measured. As an alternative to methods
presently used, we propose a technology for dark matter detection based on the evaporation of helium atoms either
from superfluid helium or from an adsorbed layer of atoms on crystalline solids in which the phonon mean free path islong. It is well known that thermal excitations in liquid helium (phonons and rotons) that have energy greater than thebinding energy of an atom to the liquid (0.62 meV) can evaporate a helium atom from a free surface in a 1 to 1 process
called quantum evaporation. The same is true in a solid with phonons having energies greater than the adsorptionenergy of helium to the surface. The evaporation process transfers energy deposited as thermal excitations in a massive
calorimeter into free helium atoms in vacuum. Presently, evaporated atoms can be detected calorimetrically upon theiradsorption to a low mass wafer.
A more sensitive detection technique is to employ field ionization. Helium atoms can be ionized in a strong electricfield in the vicinity of an anode array of sharp tips, whereupon the released positive ions can impinge on a cathodewith an energy per ion of several keV. In this way an energy deposit of less than 1 meV can be amplified to more than
1 keV. This detection scheme opens up new possibilities for the direct detection of dark matter particles of mass down
to about 1 MeV/c2 . The detection eﬃciency of field ionization depends on the collection of atoms in the high fieldregion of a large array of tips and is dependent in part on the polarization of the atoms and their resulting attraction
to high field regions. Recent developments in nanotechnology for the fabrication of tip arrays provide a method for
obtaining high collection eﬃciency of atoms in the high field region of the tip array, upon which the overall detection
eﬃciency for sensing evaporated atoms depends. Whether or not helium evaporation together with field ionization
can be used with other calorimetric experiments that require large masses, such as searches for neutrinoless double
beta decay or gamma ray spectroscopy, depends on properties of helium atom detection not discussed here, namely,
the achievable energy resolution. This is a property that must be investigated experimentally.
The technique of evaporation and field ionization for detection of small energy depositions in large calorimeters
is not limited to helium. Other atoms or molecules with relatively low binding energies to surfaces, and which havelower ionization potentials and larger polarizabilities than helium may have utility in certain applications.
category : Applications

54

O-42 Status of the HOLMES experiment to directly measure the electron neutrino
mass
Angelo Nucciotti1 , Bradley Alpert2 , Daniel Becker3 , Douglas Bennett4 , Michele Biasotti5 , Valentina Ceriale6 ,Matteo De Gerone7 , Rugard Dressler8 , Marco Faverzani9 , Elena Ferri10 , Joseph Fowler11 , Giovanni Gallucci12 , John
Gard13 , Flavio Gatti14 , Andrea Giachero15 , James Hays-Wehle16 , Stephan Heinitz17 , Gene Hilton18 , Ulli Koester19 ,Maurizio Lusignoli20 , John Mates21 , Stefano Nisi22 , Angiola Orlando23 , Gianluigi Pessina24 , Andrei Puiu25 , Stefano
Ragazzi26 , Carl Reintsema27 , Maria Ribeiro-Gomes28 , Dan Schmidt29 , Dorothea Schumann30 , Daniel Swetz31 , Joel
Ullom32 , Leila Vale33
1

Dipartimento di Fisica, Universita di Milano-Biocca / INFN Sezione di Milano-Bicocca, 2 National Institute of Standards andTechnology (NIST), Boulder, Colorado, USA , 3 National Institute of Standards and Technology (NIST), Boulder, Colorado,
USA , 4 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 5 Istituto Nazionale di Fisica
Nucleare (INFN), Sezione di Genova, Genova, Italy , 6 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Genova,
Genova, Italy , 7 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Genova, Genova, Italy , 8 Paul Scherrer Institut(PSI), Villigen, Switzerland , 9 Dipartimento di Fisica, Universita di Milano-Bicocca, Milano, Italy / Istituto Nazionale di
Fisica Nucleare (INFN), Sezione di Milano-Bicocca, Milano, Italy , 10 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di
Milano-Bicocca, Milano, Italy , 11 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 12 Istituto
Nazionale di Fisica Nucleare (INFN), Sezione di Genova, Genova, Italy , 13 National Institute of Standards and Technology(NIST), Boulder, Colorado, USA , 14 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Genova, Genova, Italy ,15
Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Milano-Bicocca, Milano, Italy , 16 Istituto Nazionale di Fisica
Nucleare (INFN), Sezione di Milano-Bicocca, Milano, Italy / National Institute of Standards and Technology (NIST),
Boulder, Colorado, USA , 17 Paul Scherrer Institut (PSI), Villigen, Switzerland , 18 National Institute of Standards andTechnology (NIST), Boulder, Colorado, USA , 19 Institut Laue-Langevin (ILL), Grenoble, France , 20 Istituto Nazionale di
Fisica Nucleare (INFN), Sezione di Roma 1, Roma, Italy , 21 National Institute of Standards and Technology (NIST), Boulder,
Colorado, USA , 22 Laboratori Nazionali del Gran Sasso (LNGS), INFN, Assergi (AQ), Italy , 23 Istituto Nazionale di Fisica
Nucleare (INFN), Sezione di Milano-Bicocca, Milano, Italy , 24 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di
Milano-Bicocca, Milano, Italy , 25 Dipartimento di Fisica, Universita di Milano-Bicocca, Milano, Italy / Istituto Nazionale di
Fisica Nucleare (INFN), Sezione di Milano-Bicocca, Milano, Italy , 26 Dipartimento di Fisica, Universita di Milano-Bicocca,
Milano, Italy / Laboratori Nazionali del Gran Sasso (LNGS), INFN, Assergi (AQ), Italy , 27 National Institute of Standards
and Technology (NIST), Boulder, Colorado, USA , 28 Multidisciplinary Centre for Astrophysics (CENTRA-IST), University of
Lisbon, Lisbon, Portugal , 29 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 30 Paul
Scherrer Institut (PSI), Villigen, Switzerland , 31 National Institute of Standards and Technology (NIST), Boulder, Colorado,
USA , 32 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 33 National Institute of Standards
and Technology (NIST), Boulder, Colorado, USA

The assessment of neutrino absolute mass scale is still a crucial challenge in today particle physics and cosmology.
Beta or electron capture spectrum end-point study is currently the only experimental method which can provide amodel independent measurement of the absolute scale of neutrino mass. HOLMES is an experiment funded by theEuropean Research Council to directly measure the neutrino mass. HOLMES will perform a calorimetric measurementof the energy released in the electron capture decay of the artificial isotope 163 Ho.
In a calorimetric measurement the energy released in the decay process is entirely contained into the detector,
except for the fraction taken away by the neutrino. This approach eliminates both the issues related to the use ofan external source and the systematic uncertainties arising from decays on excited final states. The most suitabledetectors for this type of measurement are low temperature thermal detectors, where all the energy released into anabsorber is converted into a temperature increase that can be measured by a sensitive thermometer directly coupledwith the absorber. This measurement was originally proposed in 1982 by A. De Rujula and M. Lusignoli, but only inthe last decade the technological progress in detectors development allowed to design a sensitive experiment.
HOLMES plans to deploy a large array of low temperature microcalorimeters with implanted 163 Ho nuclei. The
resulting neutrino mass statistical sensitivity will be as low as 0.4 eV, thereby making HOLMES an important step
forward in the direct neutrino mass measurement with a calorimetric approach as an alternative to spectrometry.
HOLMES will also establish the potential of this approach to extend the sensitivity down to 0.1 eV and lower. In
order to reach a sub-eV sensitivity HOLMES must collect about 3×1013 decays with an instrumental energy resolutionof about 1 eV FWHM and a time resolution of about 1µs. To achieve this in three years of measuring time, HOLMES
is going to deploy 16 sub-arrays of TES microcalorimeters. Each sub-array is composed by 64 pixels and each pixel has
an activity of 300 Bq due to ion implanted 163 Ho nuclei. The TES arrays are read out using microwave multiplexed
rf-SQUIDs in combination with a ROACH2 based digital acquisition system.
The commissioning of the first implanted sub-array is scheduled for the end of 2017 and it will provide precious
data about the EC decay of 163 Ho together with a first limit on the neutrino mass.
In this contribution we outline the HOLMES project with its physics reach and technical challenges, along with its
status and perspectives. In particular we will present the status of the HOLMES activities concerning the 163 Ho isotope
55

production and purification, the TES pixel design and optimization, the multiplexed array read-out characterization,
the cryogenic set-up installation, and the setting up of the system for the isotope embedding in the TES absorbers.
category : Applications

56

O-43 The Electron Capture in 163 Ho experiment
Clemens Hassel1 , ECHo-Collaboration
1

Kirchhoﬀ-Institute for Physics, Heidelberg University,

The Electron Capture in 163 Ho (ECHo) experiment is designed to investigate the electron neutrino mass with
sub-eV sensitivity by the analysis of the electron capture energy spectrum of 163 Ho. The sensitivity on the electron
neutrino mass is crucially related to the energy available for the decay which has been precisely determined by the ECHo
collaboration. The first phase of the experiment, ECHo-1k, for 1 kBq of high purity 163 Ho source will be implanted in
multiplexed arrays of low temperature metallic magnetic calorimeters are presently running. The goals of the current
phase are the precise characterization of the parameters describing the spectrum, optimizing the implantation processof the 163 Ho into the detector arrays as well as the optimization of the detectors production and the identification andreduction of the background. Within 1 year of measuring time, a limit on the electron neutrino mass below 10 eV will
be reached. The results achieved in ECHo-1k will pave the way to the next phase of the experiment addressed to reacha sub-eV sensitivity on the electron neutrino mass. Furthermore, the high statistics and high resolution measurementof the 163Ho electron capture spectrum will allow to investigate the existence of eV sterile neutrinos and keV-scalesterile neutrinos. In this contribution, a general overview of the ECHo will be given as well as a description of thecurrent status and of the future perspectives.
ECHo-Collaboration : Clemens Hassel, K. Blaum2 , K. Chrysalidis3 , T. Day Goodacre4 , A. Domula5 , M. Door2 ,H. Dorrer6,7,8 , Ch. E. Düllmann6,9,10 , K. Eberhardt6,10 , S. Eliseev2 , C. Enss1 , Amand Faessler11 , P. Filianin2 , A.
Fleischmann1 , D. Fonnesu1 , L. Gamer1 , R. Haas3 , C. Hassel1 , D. Hengstler1 , J. Jochum12 , K. Johnston4 , U. Kebschull13, S. Kempf1 , T. Kieck3,6 , U. Köster14 , S. Lahiri15 , M. Maiti16 , F. Mantegazzini1 , B. Marsh4 , P. Neroutsos13 , Yu. N.
Novikov2,17,18 , P. C. O. Ranitzsch1 , S. Rothe4 , A. Rischka2 , A. Saenz19 , O. Sander20 , F. Schneider3,6 , S. Scholl12 , R. X.
Schüssler2 , Ch. Schweiger2 , F. Simkovic21 , T. Stora4 , Z. Szücs22 , A. Türler7,8 , M. Veinhard4 , M. Weber20 , M. Wegner1 ,K. Wendt3 , K. Zuber5
1 Kirchhoﬀ textsuperscript for Physics, Heidelberg University, Heidelberg, Germany 2 Max-Planck textsuperscript for Nuclear Physics,

Heidelberg, Germany 3 textsuperscript for Physics, Johannes Gutenberg-University, Mainz, Germany 4 ISOLDE, CERN, Geneve,
Switzerland/France 5 textsuperscript for Nuclear and Particle Physics, TU Dresden, Germany 6 textsuperscript for Nuclear Chemistry,
Johannes Gutenberg University, Mainz, Germany 7 Laboratory of Radiochemistry and Environmental Chemistry, Department Biology
and Chemistry, Paul Scherrer textsuperscript, CH-5232 Villigen PSI, Switzerland 8 Laboratory of Radiochemistry and Environmental
Chemistry, Department of Chemistry and Biochemistry, University of Bern, Freiestrasse 3, CH-3012 Bern, Switzerland 9 GSI
Helmholtzzentrum für Schwerionenforschung, Darmstadt, Germany 10 Helmholtz textsuperscript Mainz, Mainz, Germany 11
textsuperscript for Theoretical Physics, University of Tübingen, Tübingen, Germany 12 Physics textsuperscript, University of Tübingen,Germany 13 Goethe-Universität, Frankfurt am Main 14 textsuperscriptitut Laue-Langevin, Grenoble, France 15 Chemical Sciences
Division, Saha textsuperscript of Nuclear Physics, 1/AF Bidhannagar, Kolkata 700064, India 16 Department of Physics, Indian
textsuperscript of Technology Roorkee, Roorkee 247667, India 17 Petersburg Nuclear Physics textsuperscript, Gatchina, Russia 18
St.Petersburg State University, St. Petersburg, Russia 19 Karlsruhe textsuperscript of Technology, textsuperscript for Data Processing
and Electronics, Karlsruhe, Germany 20 Department of Nuclear Physics and Biophysics, Comenius University, Bratislava, Slovakia 21
textsuperscript of Nuclear Research of the H.A.S., Bem ter 18/C, 4026 Debrecen, Hungary

category : Applications

57

SSPD and related detectors

58

O-44 A distributed superconducting nanowire single photon detector for imaging
Qing-Yuan Zhao1 , Di Zhu2 , Niccolo Calandri3 , Andrew E. Dane4 , Adam N. McCaughan5 , Francesco Bellei6 , Haozhu
Wang7 , Daniel F. Santavicca8 , Berggren K. Karl91

Department of Electrical Engineering and Computer Science, Massachusetts Institute of Technology, 2 Massachusetts Instituteof Technology, Department of Electrical Engineering and Computer Science, Cambridge, MA, 02139 , 3 Massachusetts Instituteof Technology, Department of Electrical Engineering and Computer Science, Cambridge, MA, 02139 / Politecnico di Milano,
Department of Electronics, Information and Bioengineering, Milano, ITA, 22020 , 4 Massachusetts Institute of Technology,
Department of Electrical Engineering and Computer Science, Cambridge, MA, 02139 , 5 Massachusetts Institute of Technology,
Department of Electrical Engineering and Computer Science, Cambridge, MA, 02139 , 6 Massachusetts Institute of Technology,
Department of Electrical Engineering and Computer Science, Cambridge, MA, 02139 , 7 Massachusetts Institute of Technology,
Department of Electrical Engineering and Computer Science, Cambridge, MA, 02139 , 8 University of North Florida,
Department of Physics, Jacksonville, FL 32224 , 9 Massachusetts Institute of Technology, Department of Electrical Engineeringand Computer Science, Cambridge, MA, 02139

Superconducting nanowire single-photon detectors (SNSPDs) can have near unity detection eﬃciency, sub 20 ps
timing jitter, low dark counts and wide response spectrum. Modified nanowire architectures can further improve theperformance of an SNSPD. For instance, arranging nanowires in parallel can increase the output signals and thus
reduce jitter and simplify readout. These modifications of an SNSPD usually use a lumped electrical model of an
SNSPDs, which is taken as a simple inductor in series with a photon-triggered nonlinear resistor. This treatment isvalid because conventional SNSPDs have short lengths and strong coupling between adjacent wires. However, with
our recent experimental results we found that the eﬀective electrical length of a superconducting nanowire was a few
percent of the vacuum wavelength at microwave frequencies and electromagnetic waves propagated along it with avelocity of a few percent of the speed of light in vacuum. This strange behavior is a consequence of the large kinetic
inductance of the wire. Therefore, in this circumstance one should use a transmission line and treat the nanowire asa distributed element.
I will report our recent results in which we used the distributed features of a nanowire to detect photon absorption
positions and arrival times simultaneously. We slowed down the velocity of pulse propagation to ∼ 2% of the speedof light. Therefore, photon detection pulses were guided in the nanowire, enabling the readout of position and timeof photon absorption from the arrival times of the detection pulses at the nanowire s two ends. In a 19.7-mmlong nanowire meandered across an area of 286 μ m × 193 μ m, we resolved ∼ 590 eﬀective pixels with sub-20
μ m spatial resolution while simultaneously having a temporal resolution of 50 ps full-width-at-half-magnitude. A
distributed electrothermal model will be introduced to analyze our experimental results.
category : Sensor Physics & Developments

59

O-45 Four-Lead Superconducting Detector Developed for Neutron Radiography
Takekazu Ishida1 , Hiroaki Shishido2 , Hiroyuki Yamaguchi3 , Yuya Miki4 , Yuki Iizawa5 , Kenji M. Kojima6 , Shigeyuki
Miyajima7 , Mutsuo Hidaka8 , Tomio Koyama9 , Masahide Harada10 , Kenichi Oikawa11 , Takayuki Oku12 , Kazuhiko
Soyama13
1

Osaka Prefecture University, 2 Department of Physics and Electronics, Osaka Prefecture University, Sakai, Osaka 599-8531,
Japan / NanoSquare Research Institute, Osaka Prefecture University, Sakai, Osaka 599-8531, Japan , 3 Department of Physics
and Electronics, Osaka Prefecture University, Sakai, Osaka 599-8531, Japan , 4 Department of Physics and Electronics, Osaka
Prefecture University, Sakai, Osaka 599-8531, Japan , 5 Department of Physics and Electronics, Osaka Prefecture University,
Sakai, Osaka 599-8531, Japan , 6 Institute of Materials Structure Science, High Energy Accelerator Research Organization(KEK), Tsukuba, Ibaraki 305-0801, Japan , 7 Advanced ICT Research Institute, National Institute of Information andCommunications Technology (NICT), Kobe, Hyogo 651-2492, Japan , 8 National Institute of Advanced Industrial Science andTechnology (AIST), Tsukuba, Ibaraki 305-8568, Japan , 9 Institute for Materials Research, Tohoku University, 2-1-1 Katahira,Aoba-ku, Sendai 980-8577, Japan , 10 Materials and Life Science Division, J-PARC Center, Japan Atomic Energy Agency(JAEA), Tokai, Ibaraki 319-1195, Japan , 11 Materials and Life Science Division, J-PARC Center, Japan Atomic Energy
Agency (JAEA), Tokai, Ibaraki 319-1195, Japan , 12 Materials and Life Science Division, J-PARC Center, Japan Atomic
Energy Agency (JAEA), Tokai, Ibaraki 319-1195, Japan , 13 Materials and Life Science Division, J-PARC Center, Japan
Atomic Energy Agency (JAEA), Tokai, Ibaraki 319-1195, Japan

A superconducting Nb nanowire detector biased by a constant DC current Ib works in the wide temperature and the bias
current range by probing an abrupt change in local kinetic inductance. The nanowire has a magnetic inductance Lmand a kinetic inductance Lk , but we only sense a voltage as Ib d∆Lk /dt generating by a time-dependent ∆Lk (t)(≪ Lk )originating from a mesoscopic excitation (hot spot) [1,2,3,4,5]. A hot spot generates not only a positive pulse travelingtoward one electrode but also a negative pulse traveling toward another electrode at a certain fraction of the light
velocity. The sign of each pulse depends on the direction of DC bias current fed to the detector. We observed the four
complete signal shapes at the four electrodes to know the XY position of the hot spot appeared in the orthogonallysuperimposed meanderlines by using a 4-channel 400-ps-clock digital oscilloscope. We confirm the validity of ourdelay-line imaging technique by two demonstrations after analyzing the four signals from the superconducting detector.
First, we succeeded in recovering the University emblem written by a focused laser spot (20ps, 1.55 µm, 15.8
MeV/pulse) on our XY delay-line detector biased by a DC current at 4K [6]. Second, we were able to observe theneutron absorption image of the 10 B dot (100µm in diameter, 50µm in thickness) array by superimposing a 10 B
conversion layer on top of our detector. This is because the reaction of 10 B(n,α)7 Li dominantly releases the energyof 0.84-MeV 7 Li ion and 1.47-MeV 4 He ion to create a hot-spot of restricted geometry in the eﬀective area 10 mm
× 10 mm. Actually, we obtained clear recovery of 100-µm 10 B dots by irradiating pulsed neutrons at J-PARC [6].
We also give a theoretical explanation of signal generation and transmission in our delay-line detector by means of asuperconducting waveguide of S-I-S structure model [6]. We derive a basic equation for the superconducting phase
diﬀerence defined between the two superconducting layers in the waveguide to explain the voltage pulse propagationsin the directions opposite to each other at the Swihart velocity [6]. This successfully gives us a sound theoretical basisof the operation principle of the delay-line detector.
This work is supported by a Grant-in-Aid for Scientific Research (No. 23226019, No.16H02450) from JSPS, thesuperconductive foundation fabricator (CRAVITY) and a Cadence software of VDEC at the University of Tokyo.
References[1] T. Ishida et al., J. Low Temp. Phys. 167, 447 (2012).
[2] N. Yoshioka et al., IEEE Trans. Appl. Supercond. 23, 2400604 (2013).
[3] Y. Narukami et al., IEEE. Trans. Appl. Supercond. 25, 2400904 (2015).
[4] H. Shishido et al., Appl. Phys. Lett. 107, 232601 (2015).
[5] S. Miyajima et al., Nucl. Instrum. Meth. A842, 71 (2017).
[6] T. Koyama and T. Ishida, to be published.
category : Applications60

O-46 Electrothermal modeling of amorphous WSi nanowires
Jason P Allmaras1 , Alexander G Kozorezov2 , Andrew D Beyer3 , Francesco Marsili4 , Ryan M Briggs5 , Boris Korzh6 ,Matthew D Shaw7
1

Department of Applied Physics, California Institute of Technology, 2 Department of Physics, Lancaster University, Lancaster,
United Kingdom , 3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States , 4 Jet
Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States , 5 Jet Propulsion Laboratory,
California Institute of Technology, Pasadena, CA, United States , 6 Jet Propulsion Laboratory, California Institute ofTechnology, Pasadena, CA, United States , 7 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA,
United States

Superconducting nanowire single photon detectors (SNSPDs) made from amorphous WSi are an emerging technology for fabricating large area, high eﬃciency single photon counting detectors in the near infrared. Despite theirsuccessful demonstration in both the laboratory and field, a complete electrothermal model describing energy flow inamorphous WSi nanowires has not been developed. We describe our eﬀorts in modeling the behavior of WSi nanowires
and compare simulated results to experimental measurements.
Electrothermal models for superconducting nanowires have been developed for polycrystalline NbN [1] and Nb[2]. In these formulations, an energy balance approach couples electron and phonon systems. Published SNSPD
electrothermal models use linearized formulations which are only rigorous in the limit of small temperature deviations
between the electrons, phonons, and the substrate. Based on these models, the temperatures of the electrons andphonons can reach temperatures exceeding the substrate temperature by more than 5 K during a detection event [1],which violates this assumption. Our model corrects this simplification by using the appropriate nonlinear coupling
between systems. In addition, the model explores the two-phonon approach [3] where the phonons are divided into
escaping and bottlenecked populations. The escaping phonons lie within the critical escape cone of the nanowiresubstrate interface leading to rapid thermalization with the substrate. Conversely, the bottlenecked phonons must
scatter into the critical cone before thermalizing. The expanded model also considers the influence of thermal transport
in the substrate and the impact of the amorphous structure of WSi on the phonon system.
Three experimental metrics are used to evaluate the performance of the electrothermal model. WSi nanowires were
fabricated from a 5 nm thick film on 240 nm of thermally oxidized silicon and capped with 110 nm of passivating SiO2 .
The latching behavior of these nanowires was studied as the primary mechanism for determining the dynamic responseof the system. In this experiment, devices of diﬀerent kinetic inductance were fabricated and the switching current
measured under illumination. Suppression of the switching current at low device inductance was due to latching.
Despite the strong temperature dependences of phonon scattering mechanisms, we measure that the latching behavior
is independent of bath temperature. This result suggests that fast WSi devices that typically latch at low temperature
could be operated at high temperature without experiencing any reduction in critical current compared to slow devices.
The hotspot current at various bath temperatures provides a measure of the steady state performance of the model.
Finally, a thermometry scheme was used to estimate the temperature profile and thermal conductivity of the SiO2
substrate. Comparison to simulations suggests the importance of excess heat capacity in the phonon system due tothe amorphous structure.

References[1] J. K. W. Yang et al., IEEE Transactions on Applied Superconductivity, Vol. 17, No. 2, (2007).
[2] A. Annunziata et al., Journal of Applied Physics, Vol. 108, No. 084507 (2010).
[3] M. Sidorova et al., arXiv :1607.07321 (2016).
category : Sensor Physics & Developments

61

O-47 High eﬃciency and low dark-count-rate superconducting nanowire single-photon
detectors
Lixing You1
1

SIMIT, CAS, China

Superconducting nanowire single-photon detectors(SNSPDs) with both high system detection eﬃciency (SDE) andlow dark count rate (DCR) have significant implements in quantum communication and many other applications. The
background dark counts of the SNSPD are generally caused by the black-body radiation and stray light transmitted
through the fiber coupled to the device. As a result, a cold filter with minimal insert-loss will be necessary to suppress
the background DCR. We designed and fabricated a low-loss bandpass filter (BPF) integrated on a single-mode fiber
end-face, with a typical passband from 1540 to 1579 nm and a transmittance of over 0.98 at 1567-nm wavelength.
SNSPD with high SDE was fabricated on a distributed Bragg reflector. Coupled with the fiber integrated with the
BPF on the fiber end-face, the device showed a SDE of 80% with DCR of 0.5 Hz. Compared with the normal fiber
without BPF, the DCR was reduced over 13 dB with SDE decrease of less than 2%.
category : Sensor Physics & Developments

62

O-48 Electron-phonon relaxation time in ultrathin tungsten silicon film
Maria Sidorova1 , A Kozorezov2 , A Semenov3 , A Korneev4 , Yu Korneeva5 , M Mikhailov6 , A Devizenko7 , G Chulkova
8, G Goltsman9
Department of Physics, Lancaster University, 2 Department of Physics, Lancaster University, LA1 4YB, UK , 3 Physics
Department, Moscow State Pedagogical University, Russia / Moscow Institute of Physics and Technology, Russia , 4 Physics
Department, Moscow State Pedagogical University, Russia / Moscow Institute of Physics and Technology, Russia , 5 Physics
Department, Moscow State Pedagogical University, Russia , 6 B. Verkin Institute for Low Temperature Physics andEngineering of the National Academy of Sciences of Ukraine, Kharkiv, Ukraine , 7 National Technical University ”Kharkiv
Polytechnic Institute”, Ukraine , 8 Physics Department, Moscow State Pedagogical University, Russia / National Research
University Higher School of Economics, Russia , 9 Physics Department, Moscow State Pedagogical University, Russia /National Research University Higher School of Economics, Russia
1

We have shown that conventional two-temperature model becomes inadequate for description of energy exchange
between thin metal film and acoustically rigid substrate. We found that the rate of energy exchange in this situation
may substantially slow down as a result of internal phonon bottle-neck eﬀect. This eﬀect is important for both 3D
and 2D phonon systems and originates from splitting of phonon spectrum into sets of non-escaping and escaping
modes. The electrons and non-escaping phonons may form a unified subsystem, which is cooled down only due tointeractions with subsystem of escaping phonons either due to direct phonon conversion as a result of elastic scatteringor indirect sequential interaction with electronic system. The identified regime is qualitatively diﬀerent both fromthe electron heating and the bolometric regime. In contrast with pure electron heating, the energy relaxation time
is not the electron-phonon time but is enlarged compared to the former, due to the fact that only escaping phonons
provide the eﬃcient pathway for energy relaxation. In contrast with bolometric regime, the energy relaxation timein not set by heat conductance of film-substrate interface and, in particular, should be independent on thickness
for suﬃciently thin films. Using amplitude-modulated absorption of sub-THz radiation we studied electron-phonon
interaction in amorphous WSi by measuring the response signal vs modulation frequency in the temperature range
1.8-3.4 K. We observed the specific change of slope on the signal tail indicating split of phonon sustem into two subsystems. We found that experimental data can only be simulated under assumption of lattice heat capacity in WSi
being substantially increased compared to Debye model at low temperature. We show that the excess phonon densityof states in amorphous WSi together with eﬀects of phonon quantization in thin film are likely to be responsible for theobserved ∼ T−3 dependence of electron-phonon relaxation time versus temperature. We demonstrate good agreement
between experiment and simulations.
category : Sensor Physics & Developments

63

O-49 Single microwave-photon detector based on superconducting quantum circuits
Kunihiro Inomata1 , Zhirong Lin2 , Kazuki Koshino3 , William D Oliver4 , Jaw-Shen Tsai5 , Tsuyoshi Yamamoto6 ,Yasunobu Nakamura7
1

The National Institute of Advanced Industrial Science and Technology (AIST), 2 RIKEN, Center for Emergent Matter
Science , 3 College of Liberal Arts and Science, Tokyo Medical and Dental University , 4 MIT Lincoln Laboratory , 5 RIKEN,
Center for Emergent Matter Science / Department of Physics, Tokyo University of Science , 6 NEC IoT Device ResearchLaboratories , 7 RIKEN, Center for Emergent Matter Science / Research Center for Advanced Science and Technology, The
University of Tokyo

Single-photon detection is essential to many quantum-optics experiments, enabling photon counting and its statisticaland correlational analyses [1]. It is also an indispensable tool in many protocols for quantum communication andquantum information processing [2]. In the optical domain, various kinds of single-photon detectors are commerciallyavailable and commonly used [1,3]. However, the detection of a single microwave photon in an itinerant mode remainsa challenging task due to its correspondingly small energy.
In this presentation, we demonstrate an eﬃcient and practical single microwave-photon detector based on thedeterministic switching in an artificial Λ-type three-level system implemented using the dressed states of a driven
circuit-quantum electrodynamics system [4]. The detector features a high quantum eﬃciency 0.66 ± 0.06, a low darkcount probability 0.014 ± 0.001, a bandwidth ∼ 2π × 16 MHz, and a fast reset time ∼ 400 ns. The eﬃciency limited
by a relaxation time (T1 ) of the qubit can readily exceed 0.9 by improving T1 [5]. Although the detector operates in atime-gated mode, we demonstrate “continuous” or “real-time” detection of itinerant microwave photons by coupling
two microwave resonators to a flux qubit.
[1] R. H. Hadfield, Nat. Photon. 3, 696 (2009).
[2] For example, N. Gisin, G. Ribordy, W. Tittel, and H. Zbinden, Rev. Mod. Phys. 74, 145 (2002)[3] M.D. Eisaman, J. Fan, A. Migdall, and S. V. Polyakov, Rev. Sci. Instrum. 82, 071101 (2011).
[4] K. Inomata, Z.R. Lin, K. Koshino, W.D. Oliver, J.S. Tsai, T. Yamamoto, and Y. Nakamura, Nature Communications 7, 12303 (2016).
[5] K. Koshino, K. Inomata, Z.R. Lin, Y. Nakamura, and T. Yamamoto, Phys. Rev. A 91, 04805 (2015).
category : Sensor Physics & Developments

64

Other low-temperature detectors

65

O-50 Physics and Applications of Metallic Magnetic Calorimeters
Sebastian Kempf1
1

Kirchhoﬀ-Institute for Physics, Heidelberg University

Metallic magnetic calorimeters (MMCs) are calorimetric low-temperature particle detectors that are currently strongly
advancing the state-of-the-art in energy-dispersive single particle detection. MMCs are typically operated at temperatures well below 100 mK and make use of a metallic, paramagnetic temperature sensor to transduce the temperaturerise of the detector upon the absorption of an energetic particle into a change of magnetic flux. The latter can be
precisely measured using a superconducting quantum interference device (SQUID). This outstanding interplay between a high-sensitivity magnetic thermometer and a near quantum-limited amplifier results in a very fast signal risetime reaching values well below 100 ns, an excellent energy resolution which is competitive to the resolving power ofwavelength-dispersive crystal spectrometers, a large energy dynamic range, a high quantum eﬃciency as well as analmost ideal linear detector response. For this reason, a growing number of groups located all over the world is developing MMC arrays of various sizes which range from a few to several thousand pixels. These arrays are routinely used
in a variety of applications and often appear to be a key technology for measurements that require high-resolution andwideband energy-resolving detectors. Famous examples are the investigation of the X-ray emission of highly-charged
ions, the search for the neutrinoless double beta decay, the investigation of the electron neutrino mass, metrology,
nuclear safeguards or mass spectrometry.
In this overview talk, we give an introduction into the physics of MMCs and summarize existing detector geometries, detector microfabrication as well as readout schemes for single-channel detectors as well as large-scale MMC
arrays. We discuss the performance of state-of-the-art MMCs and point out strategies to increase the energy resolving
power E/∆EFWHM to values well beyond 10,000. Finally, we highlight the use of micro-fabricated MMCs in several
applications in the fields of atomic, molecular and particle physics where it was shown that MMCs yield a wealth of
new information that are hardly accessible with conventional detector systems.
category : Sensor Physics & Developments66

O-51 Single Photon Detection of 1.5THz Radiation with the Quantum Capacitance
Detector
Pierre M. Echternach1 , Brian J. Pepper2 , Theodore Reck3 , C. Matt Bradford4
1

Jet Propulsion Laboratory, 2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 90089 , 3 Jet
Propulsion Laboratory, California Institute of Technology, Pasadena, CA 90089 , 4 Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, CA 90089

The Quantum Capacitance Detector (QCD) is a new high-sensitivity direct detector under development for low
background applications such as far-infrared spectroscopy from a cold space telescope. The QCD has demonstrated
an optically-measured noise equivalent power of 2x10−20 W Hz1/2 at 1.5THz, making it among the most sensitive
far-IR detectors systems ever demonstrated, and meeting the requirements for spaceborne spectroscopy. Under theselow-background conditions, the photon arrival rate is of the order of 100Hz making it possible to detect individual
photons, provided the detector has enough speed. In this work we describe a new fast readout technique for the
QCD that enabled single photon detection and counting at 1.5THz. Single photon detection and counting of single
photons was demonstrated between 100Hz and 10 kHz. The QCD also demonstrates high absorption eﬃciency: boththe photon arrival rate in counting mode, and the statistics of the shot noise in the non-counting mode indicate a
total photon absorption and detection rate which is within a few percent of that expected for the experimental setup.
Our measurements provide further confidence in the QCD as a detector approach for future ultrasensitive far-IR
instrumentation.
category : Sensor Physics & Developments67

O-52 Development of STJ with FD-SOI cryogenic amplifier as a far-infrared single
photon detector for COBAND experiment
Yuji Takeuchi1 , Shin-Hong Kim2 , Takashi Iida3 , Kenichi Takemasa4 , Kazuki Nagata5 , Chisa Asano6 , Shunsuke
Yagi7 , Rena Wakasa8 , Hirokazu Ikeda9 , Takehiko Wada10 , Koichi Nagase 11 , Shuji Matsuura 12 , Yasuo Arai13 , Ikuo
Kurachi14 , Masashi Hazumi 15 , Takuo Yoshida16 , Takahiro Nakamura17 , Makoto Sakai18 , Wataru Nishimura 19 ,Satoshi Mima20 , Kenji Kiuchi 21 , Hirokazu Ishino22 , Atsuko Kibayashi 23 , Yukihiro Kato 24 , Go Fujii25 , Shigetomo
Shiki26 , Masahiro Ukibe27 , Masataka Ohkubo 28 , Shoji Kawahito 29 , Erik Ramberg30 , Paul Rubinov31 , Dmitri
Sergatskov 32 , Soo-Bong Kim33
1

Division of Physics, University of Tsukuba, 2 University of Tsukuba , 3 University of Tsukuba , 4 University of Tsukuba ,University of Tsukuba , 6 University of Tsukuba , 7 University of Tsukuba , 8 University of Tsukuba , 9 Institute of Space andAstronautical Science, JAXA , 10 Institute of Space and Astronautical Science, JAXA , 11 Institute of Space and Astronautical
Science, JAXA , 12 Kwansei gakuin University , 13 High Energy Accelerator Research Organization, KEK , 14 High Energy
Accelerator Research Organization, KEK , 15 High Energy Accelerator Research Organization, KEK , 16 University of Fukui ,17
University of Fukui , 18 University of Fukui , 19 University of Fukui , 20 RIKEN , 21 RIKEN , 22 Okayama University ,23
Okayama University , 24 Kindai University , 25 Advanced Industrial Science and Technology (AIST) , 26 Advanced Industrial
Science and Technology (AIST) , 27 Advanced Industrial Science and Technology (AIST) , 28 Advanced Industrial Science andTechnology (AIST) , 29 Shizuoka University , 30 Fermi National Accelerator Laboratory , 31 Fermi National Accelerator
Laboratory , 32 Fermi National Accelerator Laboratory , 33 Seoul National University
5

The COBAND collaboration has proposed an experimental search for the COsmic BAckground Neutrino Decay, andhas been developing far-infrared (FIR) photo-detectors. The cosmic background neutrino is predicted as a relic of
the big bang in the standard cosmology, and a heavier neutrino is possible to decay to a lighter neutrino with a FIR
photon, even though its lifetime is expected to be much longer than the age of the universe. Neither the cosmic
background neutrino nor the neutrino decay is, however, established experimentally yet. Only a lower limit in theorder of 1012 years is given on the neutrino lifetime. We, thus, search for photons coming from the cosmic backgroundneutrino decays. The photon spectrum from the cosmic background neutrino decays is expected to have a uniquesignature with a sharp edge at a wavelength of around 50µm depending on the heaviest neutrino mass. To identify
the signature against the overwhelming zodiacal emission (ZE) foreground as well as the cosmic infrared background(CIB), the candidate photo-detectors are required to have an ability to measure the FIR spectrum around 50µm with
suﬃcient precision.
There are several FIR photo-detectors around 50µm already used in practical astronomical measurements, which√ arebased on photoconductors such as Ge:Ga and typically have noise-equivalent-powers (NEPs) of around 10−17 W/√ Hz.
In this collaboration, however, we aim at developing a photo-detector with a NEP better than 10−19 W/ Hz toachieve a sensitivity to the neutrino lifetime in the order of 1014 years for a 200-second measurement with a telescopeof 15cm-diameter in a sounding rocket experiment. Thus, we employ superconductor based detectors and low noise
cryogenic amplifiers for their signal readouts to attain a FIR photon-by-photon spectrometry for the improvement of
the photo-detector NEP.
One of the promising choices for the photo-detector is a combination of a diﬀraction grating and an array of
niobium-aluminum superconducting tunneling junction (Nb/Al-STJ) pixels, where each STJ pixel is capable of thedetection of a FIR single-photon delivered to each pixel per its wavelength by the grating. Also, the cryogenic amplifier
which can be deployed in close proximity to the STJ are expected to reduce the readout noise drastically. We employ
an amplifier circuit using MOSFETs based on the Fully-depleted Silicon-On-Insulator (FD-SOI) technology that havebeen proven to function below 3K.
In the development, we use Nb/Al-STJs which are fabricated at a facility dedicated for fabrications of superconductorbased devices, Clean Room for Analog & Digital superconductiVITY (CRAVITY) at AIST, and we found the Nb/AlSTJs to have a suﬃciently high quality to fulfill our requirements. In this presentation, we mainly focus on the statusof the developments of FD-SOI proto-type cryogenic amplifiers and their tests with practical input signals from the
STJ illuminated by laser pulses.
category : Sensor Physics & Developments

68✁✂✄ ☎✆ ✝✞✟ ✠✡☛☎☞✁✌✍✠ ✎✏✑✒✍✆✍✁✡ ✎✄ ✓✔✕✏✖

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Readout Techniques & Signal processing
170

O-53 Progress in microwave SQUID readout for calorimetric and bolometric sensors
J.A.B. Mates1, 2
1

University of Colorado, 2 NISTThe Microwave SQUID Multiplexer uses rf-SQUIDs to modulate superconducting microwave resonators, encoding thesignal from each input channel in its own microwave tone, summing many tones onto a common output channel.
Compared to existing multiplexing technologies, it provides much larger available output bandwidth (∼ 4 GHz) per
cable. This increased bandwidth allows the multiplexed readout of large numbers of low-temperature detectors, andalso of faster detectors than could be practically multiplexed before.
This talk will review the basic theory and the design considerations of a microwave SQUID multiplexer. It willsurvey the state of the art in terms of parameters like readout noise, speed, crosstalk, and channel density. Finally, it
will discuss current challenges and future directions. It will also showcase results from various experiments using thetechnology, such as the readout of 128 gamma-ray TES microcalorimeters on a single coaxial cable.
category : Readout Techniques & Signal processing71

O-54 A large-scale demonstration of microwave SQUID multiplexing: theSLEDGEHAMMER TES gamma-ray microcalorimeter instrument
Dan Becker1 , D A Bennet2 , M P Croce3 , J W Fowler4 , J D Gard5 , J P Hays-Wehle6 , G C Hilton7 , A S Hoover8 , J A
B Mates9 , M W Rabin10 , C D Reintsema11 , D R Schmidt12 , D S Swetz13 , L R Vale14 , J N Ullom15
1

NIST, 2 National Institute of Standards and Technology , 3 Los Alamos National Laboratory , 4 National Institute ofStandards and Technology , 5 University of Colorado , 6 National Institute of Standards and Technology , 7 National Institute ofStandards and Technology , 8 Los Alamos National Laboratory , 9 University of Colorado , 10 Los Alamos National Laboratory ,11
National Institute of Standards and Technology , 12 National Institute of Standards and Technology , 13 National Institute ofStandards and Technology , 14 National Institute of Standards and Technology , 15 University of Colorado / National Instituteof Standards and Technology

Steady progress has been made over the last 10 years developing large-format arrays of Transition-Edge Sensor (TES)
microcalorimeters to perform gamma-ray spectroscopy [1,2]. These arrays have significantly better energy resolution than state-of-the-art High-Purity Germanium (HPGe) detectors and therefore could become tools for analyzing
complex mixtures of actinide isotopes found in the nuclear fuel cycle. Previous gamma-ray measurements with TES
arrays have demonstrated lower statistical errors than HPGe [3,4]. However, TES arrays with much higher countrate capability are needed to (1) match the measurement speed of HPGe, and (2) assess and minimize the systematic
errors in deduced material composition. To address the need for higher count rate capability, we are developing the
SLEDGEHAMMER pathfinder instrument, which will consist of an array of 512 TES microcalorimeters read out using
microwave SQUID multiplexers. This instrument will be taken to Los Alamos National Laboratory and SavannahRiver National Laboratory, where it will be used to measure the isotopic content of a wide variety of samples relevant
to actinide accounting during the nuclear fuel cycle. We describe the development of this instrument, including its
assembly and a recently completed demonstration of undegraded, simultaneous readout of 128 channels using a single
HEMT amplifier and widely available ROACH2 electronics. The average TES resolution during this demonstration was
55 eV FWHM at 97 keV. This is the first large-scale demonstration of microwave SQUID readout using calorimetricsensors. We also present a detailed characterization of prototype TES microcalorimeters with bulk superconducting
absorbers covering a wide range of thermal response times.
[1] D. A. Bennett et al, Review of Scientific Instruments 83, 093113 (2012),[2] J. N. Ullom and D. A. Bennett, Superconductor Science and Technology 28, 084003 (2015)[3] A. S. Hoover et al, IEEE Transactions on Nuclear Science 60, 681(2013)[4] A. S. Hoover et al, IEEE Transactions on Nuclear Science 61, 2365(2014)
category : Readout Techniques & Signal processing

72

O-55 Microwave SQUID Multiplexing for TES micro-Calorimeters in the High-Speed
Limit
James P Hays-Wehle1 , Daniel Becker2 , Douglas A Bennett3 , John D Gard4 , Joseph W Fowler5 , Gene C Hilton6 , J.
A. Benson Mates7 , Carl D Reinstema8 , Daniel R Schmidt9 , Daniel S Swetz10 , Leila R Vale11 , Joel N Ullom12
1

National Institute of Standards and Technology, 2 University of Colorado , 3 National Institute of Standards and Technology ,University of Colorado , 5 National Institute of Standards and Technology , 6 National Institute of Standards and Technology ,7
University of Colorado , 8 National Institute of Standards and Technology , 9 National Institute of Standards and Technology ,10
National Institute of Standards and Technology , 11 National Institute of Standards and Technology , 12 National Institute ofStandards and Technology
4

Future TES microcalorimeter arrays are being developed for high event rate environments. The requirements of theseexperiments push the technology in two directions: larger multiplexing factors, and faster pixels that can handle highper-pixel event rates. Experiments such as HOLMES for neutrino mass measurement and x-ray spectrometers at highintensity facilities such as LCLS-II are targeting kilopixel arrays and 100 microsecond pulse decay times. Multiplexing
techniques that provide high bandwidth help with both goals because fundamentally both are demands on the same
readout bandwidth. Microwave SQUID multiplexing is a particularly attractive readout technique because it provides
several GHz of bandwidth per amplifier chain. In an optimized experiment, pixel speeds are pushed right up to thelimits imposed by the multiplexing system.
For microwave SQUID multiplexing, this optimization entails the careful matching of the resonator bandwidth,
the resonator spacing, the flux ramp modulation rate, and the frequency content of the detector signal. Each stage ofthis process is a balance between wasted bandwidth and loss of signal fidelity. For example, a detector that is too fast
for its ramp rate will exhibit non-linear distortions, while a ramp rate that is too fast for the resonator bandwidth will
increase noise levels. And finally, a resonator with too much bandwidth for its spacing may cause crosstalk.
This presentation will detail the mechanisms that cause various speed limits, as well as the results of experiments
performed to explore the parameter space near these limits. It describes microwave SQUID readout circuits developedat NIST with resonator bandwidths of 300 kHz, 2 MHz, and 30 MHz, in particular highlighting recent measurementsof TES pulses with 20 microsecond peaking times in a configuration that allows for 33 channels per 512 MHz of room
temperature bandwidth. We will also discuss future readout and analysis techniques meant to enable even faster pixels
without sacrificing multiplexing factor.
category : Readout Techniques & Signal processing73

O-56 Optimized Readout Electronics for Microwave SQUID Multiplexed MMC
ArraysOliver Sander1 , Sebastian Kempf2 , Nick Karcher3 , Oliver Kromer4 , Mathias Wegner5 , Matthias Balzer6 , Thomas
Kuhner7 , Christian Enss8 , Marc Weber9
1Karlsruhe Institute of Technology, 2 Kirchhoﬀ-Institute for Physics, Heidelberg University, Im Neuenheimer Feld 227, 69120
Heidelberg, Germany , 3 Institute for Data Processing and Electronics, Karlsruhe Institute of Technology,
Hermann-von-Helmholtz-Platz 1, 76344 Eggenstein-Leopoldshafen, Germany , 4 Institute for Data Processing and Electronics,
Karlsruhe Institute of Technology, Hermann-von-Helmholtz-Platz 1, 76344 Eggenstein-Leopoldshafen, Germany ,5
Kirchhoﬀ-Institute for Physics, Heidelberg University, Im Neuenheimer Feld 227, 69120 Heidelberg, Germany , 6 Institute for
Data Processing and Electronics, Karlsruhe Institute of Technology, Hermann-von-Helmholtz-Platz 1, 76344
Eggenstein-Leopoldshafen, Germany , 7 Institute for Data Processing and Electronics, Karlsruhe Institute of Technology,
Hermann-von-Helmholtz-Platz 1, 76344 Eggenstein-Leopoldshafen, Germany , 8 Kirchhoﬀ-Institute for Physics, Heidelberg
University, Im Neuenheimer Feld 227, 69120 Heidelberg, Germany , 9 Institute for Data Processing and Electronics, Karlsruhe
Institute of Technology, Hermann-von-Helmholtz-Platz 1, 76344 Eggenstein-Leopoldshafen, Germany

Detection of single particles with energies of a few eV up to several MeV plays a prominent role in many areas ofphysics. Conventional detectors such as semiconductor detectors or crystal spectrometers either oﬀer a high dynamic
range with limited resolution or vice-versa. In contrast, cryogenic detectors such as metallic magnetic calorimeters(MMCs) combine high spectral and temporal resolution while covering a broad energy range at the same time. Modern
magnetic calorimeters as used for soft X-ray spectroscopy oﬀer an energy resolution of 1.6 eV at 6 keV particle energy,
a signal rise time below 100 ns, an energy bandwidth of several 10 keV and an almost ideal linear detector response.
For the readout of MMCs, superconducting quantum interference devices (SQUIDs) are used since they provide a highsystem bandwidth and low noise. The latter two properties are mandatory for detectors with a high temporal andspectral resolution.
In addition to these, many experiments require spatial resolution to determine the location of an event or tocollect a lot of events for high statistics. Both requirements can be fulfilled by using multi-channel detector systems,
which contain a lot of independent pixels. But at the same time, the readout of such multi-channel detector systems
turns out to be challenging. Microwave SQUID multiplexing as previously introduced by Irwin et al. for reading out
arrays of superconducting transition edge sensors turns out to be a very promising approach. Here, non-hysteretic
rf-SQUIDs are used to modulate the pixels information on diﬀerent carrier frequencies in the GHz range. However,
the requirement of processing of the readout electronics imposed by MMC arrays is more demanding as compared toreading out transition edge sensor arrays due to the fast signal rise time of MMCs.
For this reason, a customized readout system for microwave SQUID multiplexed MMC arrays will be presented inthis contribution. The readout system is based on software defined radio. All digital processing is implemented on an
FPGA. Fast Digital-to-Analog-Converters (DAC) and Analog-to-Digital-Converters (ADC) are used for creating anddigitizing the MHz frequency comb which is sent to the multiplexer and modulated according to the actual state ofthe detectors. A customized high-frequency front-end electronics performs the up- and down-mixing of the frequency
comb to the targeted frequency range of 4-8 GHz. Each of the three parts has been developed, implemented, integrated
and evaluated. The first version of the system was successfully used to interface a 64 pixel MMC detector array. Thissolution allowed for the very first true multiplexed readout of a metallic magnetic calorimeters, i.e. to record events on
various independent channels in parallel, by just using one pair of coaxial cables into the cryostat. Moreover, we willshow, how this system architecture can be extended to the readout of thousands of channels in parallel. Eventually,
we target the simultaneous readout of up to 100 k channels with this approach.
category : Readout Techniques & Signal processing74

O-57 64 pixel metallic magnetic calorimeter based detector array with integrated
microwave SQUID multiplexer
Mathias Wegner1 , Andreas Fleischmann2 , Loredana Gastaldo3 , Daniel Richter4 , Sebastian Kempf5 , Christian Enss6
1

Kirchhoﬀ-Institute for Physics, 2 Kirchhoﬀ-Institute for Physics, Heidelberg University , 3 Kirchhoﬀ-Institute for Physics,
Heidelberg University , 4 Kirchhoﬀ-Institute for Physics, Heidelberg University , 5 Kirchhoﬀ-Institute for Physics, Heidelberg
University , 6 Kirchhoﬀ-Institute for Physics, Heidelberg University

Microwave SQUID multiplexing (μ MUXing) appears to be the most promising readout technique for large arrays of
low-temperature microcalorimeters requiring a large bandwidth per pixel. It is therefore highly suited for reading out
metallic magnetic calorimeters (MMCs) that combine an intrinsic fast signal rise time, an excellent energy resolution,a large dynamic range, a quantum eﬃciency close to 100% as well as a highly linear detector response. Each channel ofa microwave SQUID multiplexer consists of an unshunted, non-hysteretic rf-SQUID which is used for detector readout
and which is inductively coupled to a superconducting microwave λ/4 resonator with a unique resonance frequency.
Due to the magnetic flux dependence of the SQUID inductance as well as the mutual interaction between SQUID andresonator, the detector signal is transduced into a resonance frequency shift of the related resonator. Consequently, by
coupling many channels capacitively to a common transmission line and using software defined radio, it is possible tomonitor the resonance frequency shifts of all resonators simultaneously and therefore the actual states of the detectors.
In this contribution we present the successful demonstration of a μ MUXing based MMC readout. The tested
device consists of two 32 pixel detector arrays that are optimized for soft X-ray spectroscopy and are each read out by
an integrated, on-chip multiplexer. Each MMC consists of two meander-shaped pickup-coils which are connected inparallel and form a first order gradiometer. Each coil is equipped with a AgEr300ppm sensor and a 5 ??m thick gold
absorber on top. Both coils are connected in parallel to the current-sensing rf-SQUID which is a second-order parallel
gradiometer. The multiplexer features a common flux modulation coil which is coupled to all SQUIDs and allows
for static flux biasing or flux modulation of all SQUIDs. The resonance frequencies of the superconducting coplanar
waveguide resonators range from 4 GHz to 8 GHz and provide a bandwidth of about 1 MHz per channel which allows
resolving signal rise times well below 1 μ s. According to our detector and multiplexer models, the expected energy
resolution for all pixels within this array is ∆EFWHM ≈ 5 eV at an operating temperature of 20 mK.
We present a detailed characterization of the device. In particular, we show that its performance is as expected
when considering the geometry of the detector, the thermodynamical properties of the sensor material as well as ourmultiplexer model. In addition, we summarize the status of the development of a software defined radio based readout
electronics as well as our advances concerning flux ramp modulation which we will use for linearizing the multiplexer
output signal. Finally, we present our recently developed next-generation multiplexer which will allow reading out 32
channels with one room temperature readout electronics and discuss first experimental results.
category : Readout Techniques & Signal processing75O-58 Advanced Time- and Code-Division Multiplexers for X-Ray Spectrometer
ArraysKent D Irwin1 , Saptarshi Chaudhuri2 , Hsiao-Mei Cho3 , Carl Dawson4 , Ed Denison5 , William ”Randy” Doriese6 ,Malcolm Durkin7 , Joseph Fowler8 , John Gard9 , Gene C Hilton10 , Young Il Joe11 , Stephen Kuenstner12 , Dale Li13 ,Kelsey Morgan14 , Carl Reinstema15 , Robert Stevens16 , Daniel Swetz17 , Charles ”Jamie” Titus18 , Joel Ullom19 ,Betty Young20
1

Stanford University, 2 Stanford University , 3 SLAC National Accelerator Laboratory , 4 Stanford University , 5 National
Institute of Standards and Technology , 6 National Institute of Standards and Technology , 7 National Institute of Standards
and Technology , 8 National Institute of Standards and Technology , 9 National Institute of Standards and Technology ,10
National Institute of Standards and Technology , 11 National Institute of Standards and Technology , 12 Stanford University ,13
SLAC National Accelerator Laboratory , 14 National Institute of Standards and Technology , 15 National Institute ofStandards and Technology , 16 National Institute of Standards and Technology , 17 National Institute of Standards andTechnology , 18 Stanford University , 19 National Institute of Standards and Technology , 20 Stanford University

We present a new generation of advanced SQUID-based time-division multiplexers (TDM) and code-division multiplexers (CDM) for superconducting x-ray spectrometer arrays including the Athena X-IFU. TDM and CDM x-ray
microcalorimeter arrays are presently the most mature x-ray TES multiplexers, with excellent performance with multiplex factors up to 40 pixels and progress towards larger multiplex factors. We describe a new generation of designs
implementing advanced features for cross-talk reduction, robustness for flight instruments, and increased multiplex
factors. These advances include the implementation of error correction codes (ECC) for CDM multiplexers to eliminate the risk of single-point failure for flux-trapping in first-stage SQUIDs, active Josephson circuits to mitigate small
inductive crosstalk sources from flux feedback, and improvements to reduce noise and switching times for larger multiplex factors. We describe designs, fabricated devices, and experimental results including successful error correctionof CDM in TES calorimeter spectra.
category : Readout Techniques & Signal processing76

Readout Techniques & Signal processing
277

O-59 SiGe Integrated Circuit Developments for SQUID/TES Readout
Damien PRELE1 , Fabrice VOISIN2 , Cyril BEILLIMAZ3 , Si CHEN4 , Michel PIAT5 , Andrea GOLDWURM61

APC CNRS/Univ. Paris Diderot , 2 APC CNRS/Univ. Paris Diderot , 3 APC CNRS/Univ. Paris Diderot , 4 APC
CNRS/Univ. Paris Diderot , 5 APC CNRS/Univ. Paris Diderot , 6 APC CNRS/Univ. Paris Diderot

Since more than 10 years, APC develops SiGe integrated circuit dedicated to the readout of superconducting bolometer
arrays for astrophysics. Whether for Cosmic Microwave Background observations with the QUBIC ground based
instrument or to implement the Hot and Energetic Universe science theme with the X-IFU instrument on-board of
the ATHENA space mission, lot of Transition Edge Sensor (TES) arrays are investigated and deployed.
Such superconducting detector array currently implements readout schemes mainly based on Time and Frequency
Domain Multiplexers (TDM and FDM) using SQUID technology. In addition to SQUID devices and deep cryogenic
filter devices, SQUID multiplexers need low noise biasing and amplifications. A smart integration of these last functions
can be obtained using BiCMOS SiGe technology in an Application Specific Integrated Circuit (ASIC).
Indeed, ASIC technology allows integration of very optimized circuit specifically designed for a unique application.
Moreover, SiGe bipolar transistor can be used to reach very low noise and wide band amplifications for operations
both at room and cryogenic temperatures. We propose to present in the LTD17, a short review of the use of SiGe
integrated circuit for SQUID/TES readout and give an update of the last developments done for the QUBIC telescope
and for the X-IFU instrument.
QU Bolometric Interferometer for Cosmology (QUBIC) uses 2 TES focal plans (one for 150 GHz and one for 220
GHz) of 1?k pixels each. A TDM cryogenic readout has been realized for these TES arrays. 3 generations of cryogenic
SiGe ASIC (down to 2 K) has been successfully used to readout the QUBIC TESs. The most recent SQmux128 evo
provides a 128-multiplexing factor in cryogenic environment and is actually implemented in the QUBIC cryostat. A
5MHz 0.2nV/√ Hz low noise amplifier, a sequentially addressed SQUID current sources and a digital clocking of thefull multiplexer is operating for the QUBIC experiment.
The X-ray Integral Field Unit (X-IFU) instrument build for the ATHENA ESA space mission (to be launched in2028) uses a micro-calorimeter/TES focal plan of 4 k pixels. A FDM cryogenic readout based of LC filters and 2
SQUID stages is biased and low-noise amplified by a warm ASIC (named AwaXe) placed outside the cryostat. This
warm front-end electronic uses BiCMOS SiGe technology for the SQUID biasing, the adjustment of the biasing of each
SQUID stage and for the 10MHz 1nV/√ Hz amplification tacking into account challenging gain stability and linearity
constraints.
Both Integrated circuits SQmux128 and AwaXe will be described showing the interest of such SiGe technology for
SQUID multiplexer controls.
category : Readout Techniques & Signal processing

78

79

O-60 Frequency domain multiplexed readout of TES X-ray microcalorimeters for
X-IFU on board of Athena
HIROKI AKAMATSU1 , L. Gottardi2 , J. van der Kuur3 , C.P. de Vries4 , M.P. Bruijn5 , J.A. Chervenak6 , M.
Kiviranta7 , A.J. van den Linden8 , B.D. Jackson9 , S.J. Smith10
1

SRON the Netherlands institute for Space Research, 2 SRON , 3 SRON , 4 SRON , 5 SRON , 6 NASA/GSFC , 7 VTT , 8 SRON ,9
SRON , 10 NASA/GSFC

We are developing frequency domain multiplexing (FDM) readout of TES X-ray microcalorimeter for X-IFU instrument
on board of the X-ray astronomical satellite Athena. FDM is currently baseline readout system for the X-IFU
instrument. In FDM, TESs are biased with alternating current (AC bias) at MHz frequencies and their signal fromeach TESs are distributed by high-quality passive LC filters. Due to strong limitations of electrical and cooling poweron the satellite, a multiplexing factor of 40 pixels/channel in a frequency range from 1 to 5 MHz is required.
Utilizing SRON in-house manufactured LC filters and room-temperature electronics, and a low-noise SQUID systemprovided by VTT, we have demonstrated 5 pixel FDM readout of Mo/Au TES calorimeters with Au/Bi absorbers.
The current technical limitation to realizing multiplexing for the X-IFU instrument on the scale of 40 pixels/channel
is the so-called AC-losses in the TES pixels. This additional resistive loss acts as a temperature insensitive resistancewithin the TES, which suppresses the detector responsivity. The losses are presumably generated by Eddy currents
induced in the Au/Bi absorber by the bias currents flowing in the Nb bias leads. Due to the nature of the eddy
currents, the impact on the performance is getting larger at higher bias frequencies. Recently, we also have started
developing a new setup for the demonstration of 40x2 pixels FDM readout, which matches with the requirement of ademonstration model of the X-IFU instrument. The mechanical construction was just finalized, and first cool downwith dry dilution cooler. After several cooling downs, a 1000-pixels TES array will be installed and characterised
under FDM configuration.
In this contribution, we report on the recent progresses of FDM readout at SRON including single pixel characterizations, the performance of these pixels under FDM configuration and the current status of 40-pixel readoutdemonstrator.
category : Readout Techniques & Signal processing80O-61 Traveling-wave, lumped-element kinetic inductance parametric amplifier for
detector readout
Saptarshi Chaudhuri1 , Dale Li2 , Kent Irwin3 , Clint Bockstiegel4 , Johannes Hubmayr5 , Joel Ullom6 , Michael
Vissers7 , Jiansong Gao81

Department of Physics, Stanford University, 2 SLAC National Accelerator Laboratory , 3 Department of Physics, Stanford
University / SLAC National Accelerator Laboratory , 4 Department of Physics, University of California, Santa Barbara ,5
National Institute of Standards and Technology, Boulder , 6 National Institute of Standards and Technology, Boulder ,7
National Institute of Standards and Technology, Boulder , 8 National Institute of Standards and Technology, Boulder

We describe the development of a broadband, high-dynamic-range, and near-quantum-limited parametric amplifier
based on the nonlinear kinetic inductance of superconducting NbTiN thin films. We show artificial (lumped-element)
transmission-line architectures with two separate phase-matching implementations: periodic impedance loading andresonator phase shifters embedded periodically along the line. The lumped-element designs possess several advantages
over previous CPW-based designs, including intrinsic 50 ohm characteristic impedance, natural suppression of higher
harmonics from a low-pass cutoﬀ, a factor of 3 reduction in required pump power, a factor of 10 reduction in center
trace length, and improved fabrication yield [1]. For both designs, we demonstrate 15 dB gain over a few GHz of
bandwidth. We discuss preliminary noise measurements and implications for the readout of MKIDs and microwave
SQUID multiplexers.
[1] S. Chaudhuri, D. Li, K.D. Irwin, C. Bockstiegel, J. Hubmayr, J.N. Ullom, M.R. Vissers, and J. Gao, Appl.
Phys. Lett. 110(15), 152601 (2017).
category : Readout Techniques & Signal processing81O-62 Lithographed superconducting resonator development for next generation
frequency multiplexing readout of transition-edge sensors
Farzad Faramarzi1 , Tijmen de Haan2 , Akito Kuaka3 , Adrian Lee4 , Barbara Neuhauser5 , Richard Plambeck6 ,Christopher Raum7 , Aritoki Suzuki8 , Ben Westbrook9
1

Department of Physics, University of California Berkeley, 2 University of California Berkeley / Lawrence Berkeley National
Laboratory , 3 University of California Berkeley / Lawrence Berkeley National Laboratory , 4 University of California Berkeley/ Lawrence Berkeley National Laboratory , 5 San Francisco State University , 6 University of California Berkeley / Radio
Astronomy Laboratory, University of California Berkeley , 7 University of California Berkeley / Radio Astronomy Laboratory,
University of California Berkeley , 8 University of California Berkeley / Lawrence Berkeley National Laboratory / Radio
Astronomy Laboratory, University of California Berkeley , 9 University of California Berkeley / Radio Astronomy Laboratory,
University of California Berkeley

Ground-based Cosmic Microwave Background (CMB) experiments are currently undergoing a period of exponential
growth. Current experiments are observing with 1,000-10,000 detectors, and the next generation experiment (CMB
stage 4) is proposing to deploy approximately 500,000 detectors. This order of magnitude increase in detector countwill require a new approach for readout electronics. We have developed superconducting resonators for next generation
frequency domain multiplexing (fMUX) readout architecture. Our goal is to reduce the physical size of resonators, suchthat resonators and detectors can eventually be integrated on a single wafer. To reduce the size of these resonators, wehave designed spiral inductors and interdigitated capacitors that resonate around 10-100 MHz, an order of magnitude
higher frequency compared to current fMUX readout systems. This would also enable higher multiplexity than thecurrent 50 detectors per readout channel. We will report on the simulation, fabrication method, characterization
technique, and measurement of quality factor of these resonators.
category : Readout Techniques & Signal processing

82

Fabrication & Implementation
Techniques 183

O-63 Design and Fabrication of Large-Area Transition Edge Sensor Detector Arrays
for Cosmic Microwave Background Polarimetry
Shannon M Duﬀ1 , AdvACT Collaboration2 , SPIDER Collaboration3
1

National Institute of Standards and Technology, 2 National Institute of Standards and Technology / Princeton University /Cornell University / University of Michigan / University of Pennsylvania , 3 National Institute of Standards and Technology /Princeton University

Mapping the polarization of the Cosmic Microwave Background (CMB) to constrain inflationary physics and the sumof the neutrino masses requires ever larger arrays of highly uniform low-temperature detectors with increased packing
density. To address this need, we are developing 150-mm-diameter feedhorn-coupled superconducting microwave
polarimeter arrays based on AlMn Transition-Edge Sensor (TES) bolometers. We present an improved design andfabrication process and report results from the application of this process for two CMB experiments which havevery diﬀerent constraints ? Advanced ACTPol (AdvACT) and SPIDER. AdvACT is a ground-based CMB telescopeobserving from the Atacama Desert in Chile in which the detectors are operated at 100 mK. We have delivered one
high frequency (HF) 150/230 GHz multichroic array, two mid-frequency (MF) 90/150 GHz multichroic arrays, anda low frequency (LF) 27/39 GHz multichroic array is under development. In contrast, SPIDER is a balloon-borne
experiment optimized to take advantage of the low photon loading conditions of a space-like environment. We haveproduced three 280 GHz arrays, to be operated at 300 mK, in which the thermally isolating legs of the bolometer havean extreme cross-sectional area-to-length aspect ratio to achieve 3 pW saturation powers. Our design and fabrication
process has the versatility to satisfy the diverse constraints of both experiments without altering the process flow, allwhile producing highly uniform arrays. Together, these arrays comprise a total of 5784 TES detectors for AdvACT and
1536 TES detectors for SPIDER. All arrays exhibit ¿ 99% device yield with unprecedented device parameter uniformity
and low-loss microwave performance. We present histograms of superconducting transition temperature, bolometersaturation power, and thermal conductance for these arrays, showing a ¡ 2% variation in transition temperature acrossthe AdvACT HF array and a 5% spread in saturation power across the 512-TES element SPIDER array. In addition
to updates on these arrays, details will be given on current process developments as we continue to improve uniformity
and perform further material characterization to achieve state-of-the-art arrays applicable for 4th generation CMB
experiments and beyond.
category : Fabrication & Implementation Techniques84O-64 Superconducting Ti/TiN thin films for mm wave absorption
Abdelkader ALIANE1 , Mathias SOLANA2 , Valerie GOUDON3 , Claire VIALLE4 , Elaura BAGHE5 , Laurent
CARLE6 , Wilfried RABAUD7 , Laurent SAMINADAYAR8 , Laurent DUSSOPT9 , Patrick AGNESE10 , Nicolas LIO
SOON SHUN11 , Sebastien BECKER12 , Pierre RODIERE13 , Vincent REVERET14 , Louis RODRIGUEZ15
1

CEA tech LETI, Grenoble, 2 Institut Neel, CNRS and Universite Joseph Fourier Grenoble , 3 CEA Tech LETI , 4 CEA Tech
LETI , 5 CEA Tech LETI , 6 CEA Tech LETI , 7 CEA Tech LETI , 8 Institut Neel, CNRS and Universite Joseph Fourier
Grenoble , 9 CEA Tech LETI , 10 CEA Tech LETI , 11 CEA Tech LETI , 12 CEA Tech LETI , 13 Institut Neel, CNRS andUniversite Joseph Fourier Grenoble , 14 CEA/Irfu/SAp , 15 CEA/Irfu/SAp

Superconductors based on thin films are of common issue for many applications at low temperature, mainly in thefield of polarization detection. We focus on the development of polarization sensitive detectors in the range 120 to 500
GHz. In this paper, we have developed and studied superconducting thin films based on Ti/TiN bilayers in order to be
integrated as electromagnetic wave absorbers in suspended silicon bolometers. These silicon bolometers are working
between 50 and 100 mK. The aim is to adapt the critical temperature (Tc) in order to absorb the incident power
and to reduce the heat capacity of the system at low temperature. The Tc of absorbers should be in the range of
600-800 mK. To obtain this adapted Tc, we applied the superconductivity proximity eﬀect between the Ti and TiNlayers. We have also studied the eﬀect of thermal stress (20 - 250 °C) on the Tc and the critical magnetic field (Hc).
Samples are fabricated with two diﬀerent thicknesses of bilayers: Ti: 100nm/TiN: 5nm and Ti: 300nm/TiN: 5nm andare deposited by PVD technique on oxidized silicon substrates. The electrical characterization of the Tc and the Hc
has been performed at low temperature. We observed that the thermal stress has an obvious influence on the criticaltransition temperature (Tc) behavior. To explain this influence, we performed diﬀerent morphological and physicalcharacterizations such as X-rays diﬀraction analysis (XRD), X-ray photoelectron spectroscopy (XPS) and secondary
ion mass spectrometry (SIMS). On the basis of the results, we have suggested that the appearance of an oxidized statein the Ti/TiN films modifies the proximity eﬀect.
Keywords: superconductors, thin films, low temperature, bilayer Ti/TiN
category : Fabrication & Implementation Techniques85

O-65 Parallel plate resonators for kinetic inductance detectors
Gregoire Coiﬀard1 , Miguel Daal2 , Paul Szypryt3 , Gerhard Ulbricht4 , Nicholas Zobrist5 , Benjamin A. Mazin6
1

Department of Physics, University of California Santa Barbara, 2 Department of Physics, University of California, Santa
Barbara CA 93106, USA , 3 Department of Physics, University of California, Santa Barbara CA 93106, USA , 4 School of
Cosmic Physics, Dublin Institute of Advanced Studies, Dublin 4, Ireland , 5 Department of Physics, University of California,
Santa Barbara CA 93106, USA , 6 Department of Physics, University of California, Santa Barbara CA 93106, USA

Microwave kinetic inductance detectors (MKIDs) are superconducting devices that are lithographically patterned into
microscopic resonant circuits. The resonator geometry is typically a lumped element geometry with an interdigitatedcapacitors and a meandered wire inductor. We report on our work to design and fabricate a parallel plate resonator,
which has two parallel plate capacitors connected by a narrower trace. The trace is the sensitive element of this MKID
geometry which we intend to use for optical photon detection. The main goal behind this geometry is to increase
microwave readout power by making a low inductance and high capacitance, unlike the lumped element design thathas high L and low C. From the parallel plate design, we expect: (1) the ability to increase sensitivity by increasing
microwave drive power, (2) a concomitant significant improvement in signal-to-noise ratio due to the saturation of TLS
noise resulting from high microwave drive power and (3) decreased energy resolution degradation due to geometriceﬀects due to the more uniform current passing through the trace.
We will present results from electromagnetic simulations as well as fabricated parallel plate MKIDs. We will discuss
the fabrication, which is challenging due to requiring a 10 nm thick dielectric between the two plates of the capacitor.
With these results we demonstrate the feasibility of the parallel plate MKID design. We will also show that these
MKIDs can be driven at readout powers at least 100 times larger than conventional lumped element designs of similarsensitivity.
category : Fabrication & Implementation Techniques

86

Application - CMB 1

87

O-66 Low Temperature Detectors For Cosmic Microwave Background Research
Johannes Hubmayr1
1

NIST

The Cosmic Microwave Background (CMB) is a gift to cosmologists, providing a basic picture of how the universe
began and evolved. Details of this picture, including what drove the bang of the Big Bang, may be clarified throughprecision measurements of the CMB. As such, enthusiasm for CMB experiment is not lacking.
More than 10 sub-orbital instruments are either observing or in active development, and satellite missions haverecently been proposed in Japan, the US, and Europe. The CMB imager LiteBIRD is in fact a formal candidate
under study for JAXA s strategic large mission. Key components to all of these instruments are the arrays of low
temperature detectors that populate the focal planes. In this presentation, I review the tremendous innovation in
CMB detectors which has transpired in the past decade. A current state-of-the-art array consists of multi-hundreds ofspatial pixels, each dual-polarization sensitive, multi-chroic, and printed on a 150 mm diameter substrate. I present
a hypothetical ideal CMB imaging array, which would be sensitive over 10:1 bandwidth, fabricated on a flexible
circuit to match a non-telecentric focal plane, and possess variable aperture size as a function of wavelength. Several
groups are developing aspects of such a detector array, and these ideas will be presented. I will compare and contrast
implementation of transition-edge-sensor (TES) bolometers with microwave kinetic inductance detectors (MKIDs) for
CMB studies. Lastly, I conclude with the outlook of developing detector arrays to meet the needs of CMB Stage IV,
an experiment to commence in the next decade which aims to map half of the sky to 1 microKelvin-arcminute depths
by use of multiple telescopes sprinkled throughout the globe.
category : Sensor Physics & Developments

88O-67 The Advanced ACTPol 27/39 GHz Array
Sara Michelle Simon1
1

University of Michigan

Advanced ACTPol (AdvACT) is an upgraded camera for the Atacama Cosmology Telescope that will measure theCosmic Microwave Background in both temperature and polarization over a wide range of angular scales and fivefrequency bands from 27-230 GHz. AdvACT s sensitivity, resolution, wide frequency coverage, and large sky coverage
will enable it to simultaneously probe inflation at large angular scales while using small angular scale measurements
to constrain the mass and number of neutrinos, dark energy, and dark matter. Measurements are currently limited
by foreground contamination from galactic dust and synchrotron emission, so wide frequency coverage is required tocharacterize and remove these signals. AdvACT will sequentially deploy four arrays of feedhorn-coupled, polarizationsensitive multichroic pixels in its three optics tubes: one 150/230 GHz array, two 90/150 GHz arrays, and one 27/39
GHz array. The AdvACT 27/39 GHz array will consist of 75 multichroic pixels that will measure the synchrotron
foregrounds, which are dominant at lower frequencies, with unprecedented sensitivity and resolution, making it singularin the field. To maximize the sensitivity of the 27/39 GHz array, the spacing between pixels was minimized to increase
the number of pixels and thus the sensitivity. Light from each feedhorn is waveguide-coupled to a planar orthomodetransducer that splits the radiation into two orthogonal polarizations. The signal is then sent down superconducting
Nb microstrip lines, through a diplexer of quarter-wave stub filters that define the bandpasses, through a hybrid-T,
and onto a transition-edge sensor (TES) bolometer. Each multichroic pixel has four TES bolometers, one for eachfrequency and polarization. I will present the design of the pixels and feedhorns for the AdvACT 27/39 GHz array,
which will be deployed in January 2018.
category : Applications89O-68 BICEP3 performance overview and design for BICEP Array
Howard Hui1
1

Department of Physics, California Institute of Technology

BICEP3 is the latest telescope in the BICEP/Keck program, deployed to the South Pole Station in 2015. It isa 550mm aperture refractive telescope observing the polarization of the cosmic microwave background at 95 GHz.
BICEP3 started the second season of science observation in 2017.
This paper will show the latest BICEP3 performance, including detector spectral response, optical eﬃciency andtelescope sensitivity. We will also present the design for our next generation telescope, BICEP Array, consisting ofmultiple BICEP3-like receivers spanning from 35 GHz to 270 GHz with total detector count in the tens of thousands.
category : Applications

90

O-69 SPT3G: A Multichroic Receiver for the South Pole Telescope
Adam Jonathan Anderson1 , SPT3G collaboration2
1

Fermi National Accelerator Laboratory, 2 Fermi National Accelerator Laboratory

The third-generation camera for the South Pole Telescope, SPT3G, was deployed in early 2017 to map the cosmic
microwave background at 90, 150, and 220 GHz with 16,000 detectors, 10 times more than the previous-generation
receiver on the SPT. The increase in detector count is made possible by lenslet-coupled trichroic polarization-sensitive
pixels fabricated at Argonne National Laboratory, a new optical design with higher throughput, and new multiplexing
readout electronics. The enhanced sensitivity of SPT3G will enable a diverse set of measurements on primordial
B-mode polarization, gravitational lensing of the CMB, and the E-mode damping tail. The instrument is currently
deployed and taking engineering observations during its first year of operation at the South Pole. Here we willsummarize the scientific motivation for SPT3G and present an overview of the instrument and design considerationsof its major subsystems, including detectors, optics, and readout electronics. We will also highlight the on-sky
performance and status of the fully integrated camera as it begins its 4-year 2500 sq-deg survey.
category : Applications91

O-70 GroundBIRD - observation of CMB polarization with a high-speed scanningand MKIDs
Taketo Nagasaki1 , Jihoon Choi2 , Ricardo Tanausu Genova-Santos3 , Makoto Hattori4 , Masashi Hazumi5 , Hikaru
Ishitsuka6 , Kenichi Karatsu7 , Kenji Kiuchi8 , Ryo Koyano9 , Hiroki Kutsuma10 , Kyoungmin Lee11 , Satoru Mima12 ,Makoto Minowa13 , Makoto Nagai14 , Masato Naruse15 , Shugo Oguri16 , Chiko Otani17 , Rafael Rebolo18 , Jose Alberto
Rubino-Martin19 , Yutaro Sekimoto20 , Munehisa Semoto21 , Junya Suzuki22 , Tohru Taino23 , Osamu Tajima24 ,Nozomu Tomita25 , Tomohisa Uchida26 , Eunil Won27 , Mitsuhiro Yoshida28
1
IPNS, KEK, 2 Institute for Basic Science, 70, Yuseong-daero 1689-gil, Yuseong-gu, Daejeon 305-811 Korea , 3 Instituto de
Astrofisica de Canarias, 38200 La Laguna, Tenerife, Canary Islands, Spain / Departamento de Astrofisica, Universidad de La
Laguna (ULL), 38206 La Laguna, Tenerife, Spain , 4 Astronomical Institute, Tohoku University, 6-3 Aramaki, Aoba-ku Sendai
980-8578 Japan , 5 Institute of Particle and Nuclear Studies, High Energy Research Organization, Oho 1-1, Tsukuba-shi,
Ibaraki 305-0801 Japan / The Graduate Univ. for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193 Japan ,6
The Graduate Univ. for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193 Japan , 7 Department of ElectricalEngineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628 CD Delft The Netherlands ,8
RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198 Japa , 9 Saitama University, 255 Shimo-Okubo, Sakura-ku, Saitama-shi
338-8570 Japan , 10 Astronomical Institute, Tohoku University, 6-3 Aramaki, Aoba-ku Sendai 980-8578 Japan , 11 Departmentof Physics, Korea University, 145, Anam-ro Seongbuk-gu, Seoul 136-713 Korea , 12 RIKEN, 2-1 Hirosawa, Wako, Saitama
351-0198 Japa , 13 Department of Physics, Faculty of Science, University of Tokyo, Tokyo 113-0033 Japan , 14 National
Astronomical Observatory of Japan(NAOJ), 2-21-1 Osawa, Mitaka, Tokyo 181-8588 Japan , 15 Saitama University, 255
Shimo-Okubo, Sakura-ku, Saitama-shi 338-8570 Japan , 16 RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198 Japa , 17 RIKEN,
2-1 Hirosawa, Wako, Saitama 351-0198 Japa , 18 Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, CanaryIslands, Spain / Departamento de Astrofisica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain / Consejo
Superior de Investigaciones Cientificas, Spain , 19 Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, CanaryIslands, Spain / Departamento de Astrofisica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain ,20
National Astronomical Observatory of Japan(NAOJ), 2-21-1 Osawa, Mitaka, Tokyo 181-8588 Japan / Department of
Physics, Faculty of Science, University of Tokyo, Tokyo 113-0033 Japan , 21 Saitama University, 255 Shimo-Okubo, Sakura-ku,
Saitama-shi 338-8570 Japan , 22 Institute of Particle and Nuclear Studies, High Energy Research Organization, Oho 1-1,
Tsukuba-shi, Ibaraki 305-0801 Japan , 23 Saitama University, 255 Shimo-Okubo, Sakura-ku, Saitama-shi 338-8570 Japan ,24
Institute of Particle and Nuclear Studies, High Energy Research Organization, Oho 1-1, Tsukuba-shi, Ibaraki 305-0801
Japan / The Graduate Univ. for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193 Japan , 25 Department of
Physics, Faculty of Science, University of Tokyo, Tokyo 113-0033 Japan , 26 Institute of Particle and Nuclear Studies, HighEnergy Research Organization, Oho 1-1, Tsukuba-shi, Ibaraki 305-0801 Japan / The Graduate Univ. for Advanced Studies,
Shonan Village, Hayama, Kanagawa 240-0193 Japan , 27 Department of Physics, Korea University, 145, Anam-ro Seongbuk-gu,
Seoul 136-713 Korea , 28 Institute of Particle and Nuclear Studies, High Energy Research Organization, Oho 1-1, Tsukuba-shi,
Ibaraki 305-0801 Japan / The Graduate Univ. for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193 JapanThe Cosmic Microwave Background radiation (CMB) polarization contains information about of early universe. In
particular, the odd-parity patterns (B-mode) at large angular scale is strong evidence for the inflationary universe.
GroundBIRD is designed to detect the B-mode with high-speed rotation scan system, cold optics, and microwave
kinetic inductance detectors (MKIDs). We plan to start commissioning of GroudBIRD in the Canary Islands in early
2018.
The high-speed scanning is one of the key features in our telescope. The most ground-based experiments haveadopted periodic (i.e., forward and backward) swing in azimuth for their scan strategy. In this way, atmosphericfluctuation (1/f noise) degrades the sensitivity at degree scale observation because the swing scan does not achieve
fast modulation to mitigate the 1/f noise eﬀects. We employed rotation scan allowing continuous high-speed motion
without any deceleration. This scan mitigates the eﬀect of 1/f noise with multiple ranges at 6 ¡ l ¡ 300. We developed
rotary joints for high-pressure helium gas and electricity lines to realize the operation of the cryocooler on a rotatingtable. We confirmed that cold condition can be maintained with rotation at 20 rpm. We set optical mirrors in thecryostat at 4K to reduce radiation from the mirror surfaces. We employ novel approach for blocking thermal radiations
from the receiver aperture, a combination of metal mesh filters (QMC Instruments Ltd.) and radio-transparent multilayer insulations (RT-MLI) at 300 K, 50 K, 4K, and 350 mK. We adopted a focal plane with 350 mK and 250 mKstage connected with Kevlar strings. We achieved to maintain the mirrors at 3.4 K on the optical configuration. We
also achieved 0.25 K temperature for the focal plane stage with a hold time of more than 24 hours. We chose MKID
for the focal plane detector array of the GroundBIRD telescope. MKID has an advantage of multiplicity with a single
readout line. We plan to observe at 220 GHz (112 pixels) as one readout system and at 145 GHz (330 pixels) as six
readout systems. The 220 GHz band observes thermal emission from foreground dust and the 145 GHz observes the
CMB signal. In addition to that, the fast time response (order of 100 us) of MKID is suitable for our high-speed
scan. 120-ch responses of MKID are measured by analog readout system at once. We developed two outputs/inputs
of DAC/ADC analogue board for measurement of phase and amplitude responses. Our prototype detector has one
corrugated horn and ten MKIDs at 145 GHz band (fig). We measured polarization characteristic with a rotation ofhalf-wave plate and confirmed a couple of detectors response in directions orthogonal to each other.
92

In this conference, we will present our status, achievements, and prospects of the GroundBIRD experiment.

category : Applications

93

Application - CMB 2

94

O-71 Design, construction, and characterization of the 280 GHz focal plane units forthe second flight of the Spider polarimeter
Amanda Stevie Bergman1 , Spider collaboration
1

Department of Physics, Princeton University,

We describe the construction and characterization of the 280 GHz bolometric focal plane units (FPUs) to be deployedon the second flight of the balloon-borne Spider instrument. These FPUs are vital to Spider’s primary science goalof detecting or placing an upper limit on the amplitude of the primordial gravitational-wave signature in the cosmic
microwave background (CMB) by constraining the B-mode contamination in the CMB from galactic dust emission.
Each 280 GHz focal plane contains a 16 × 16 grid of corrugated silicon feedhorns coupled to an array of aluminum
manganese transition-edge sensor bolometers, fabricated on 150 mm diameter substrates. In total, the three 280 GHz
FPUs contain 1,530 polarization sensitive bolometers (765 spatial pixels) optimized for the low loading environment
in flight and read out by time-division SQUID multiplexing. In this paper we describe the architecture of the focal
planes, which includes several layers of magnetic shielding, and present cryogenic measurements characterizing theirperformance. The FPUs have near 90% end-to-end yield (including read-out) and an 80% band-averaged optical
Typeset using LAThighstyle in AASTeX61
eﬃciency. We demonstrateuniformity
in device parameters, finding the mean saturation power to be 2.80 pW
EX twocolumn
at 300 mK with a 5% variation across the array at one standard deviation. These focal planes will be deployed
DESIGN,AND inCHARACTERIZATION
THE 280 GHZ FOCAL
UNITS
FORMcMurdo
THE SECONDBase in Antarctica
alongside the 95 and
145CONSTRUCTION,
GHz telescopes
the Spider-2 OF
instrument,
slatedPLANE
to flyfrom
FLIGHT OF THE SPIDER POLARIMETER
in December 2018.
A. S. B ERGMAN , 1 P. A. R. A DE , 2 M. A MIRI , 3 J. A. AUSTERMANN , 4 J. A. B EALL , 4 D. T. B ECKER , 4 S. J. B ENTON , 1 J. J. B OCK , 5, 6
J. R. B OND , 7 S. A. B RYAN , 8 H. C. C HIANG , 9, 10 C. R. C ONTALDI , 11 O. D ORÉ , 5, 6 S. M. D UFF , 4 A. J. D UIVENVOORDEN , 12
H. K. E RIKSEN , 13 M. FARHANG , 7, 14 J. P. F ILIPPINI , 15, 16 L. M. F ISSEL , 17, 14 A. A. F RAISSE , 1 K. F REESE , 18, 12 M. G ALLOWAY , 19
A. E. G AMBREL , 1 N. N. G ANDILO , 20, 21 K. G ANGA , 22 A. G RIGORIAN , 4 J. E. G UDMUNDSSON , 12 M. H ALPERN , 3 J. H ARTLEY , 19
M. H ASSELFIELD , 23 G. H ILTON , 4 W. H OLMES , 6 V. V. H RISTOV , 5 Z. H UANG , 7 J. H UBMAYR , 4 K. D. I RWIN , 24, 25 W. C. J ONES , 1
C. L. K UO , 24 Z. D. K ERMISH , 1 S. L I , 14, 1, 26 P. V. M ASON , 5 K. M EGERIAN , 6 L. M ONCELSI , 5 T. A. M ORFORD , 5 J. M. NAGY , 27
C. B. N ETTERFIELD , 14, 19 M. N OLTA , 7 I. L. PADILLA , 14 B. R ACINE , 13 A. S. R AHLIN , 28, 29 C. R EINTSEMA , 4 J. E. RUHL , 27
M. C. RUNYAN , 6 T. M. RUUD , 13 J. A. S HARIFF , 7 J. D. S OLER , 30 X. S ONG , 1 A. T RANGSRUD , 5, 6 C. T UCKER , 2 R. S. T UCKER , 5
A. D. T URNER , 6 J. U LLOM , 4 J. F. VAN DER L IST , 1 J. VAN L ANEN , 4 M. R. V ISSERS , 4 A. C. W EBER , 6 I. K. W EHUS , 13
D. V. W IEBE , 3 AND E. Y. YOUNG 1
1 Department of Physics, Princeton University, Princeton, NJ, USA

2 School of Physics and Astronomy, Cardiff University, CF24 3AA, UK

3 Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada
4 National Institute of Standards and Technology, Boulder, CO, USA

5 Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
6 Jet Propulsion Laboratory, Pasadena, CA, USA

7 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada
8 School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA

9 School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Durban, South Africa
10 National Institute for Theoretical Physics (NITheP), KwaZulu-Natal, South Africa
11 Blackett Laboratory, Imperial College London, SW7 2AZ, London, UK

12 The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
13 Institute of Theoretical Astrophysics, University of Oslo, Oslo, Norway

14 Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON, Canada
15 Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL, USA

16 Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
17 National Radio Astronomy Observatory, Charlottesville, NC, USA

18 Department of Physics, University of Michigan, Ann Arbor, MI, USA
19 Department of Physics, University of Toronto, Toronto, ON, Canada

20 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
21 NASA Goddard Space Flight Center, Greenbelt, MD, USA

22 APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
23 Pennsylvania State University, University Park, PA, USA

24 Department of Physics, Stanford University, Stanford, CA, USA
25 SLAC National Accelerator Laboratory, Menlo Park, CA, USA

26 Department of Mechanical and Aerospace Engineering, Princeton University, Princeton, NJ, USA

27 Physics Department, Center for Education and Research in Cosmology and Astrophysics, Case Western Reserve University, Cleveland, OH, USA
28 Fermi National Accelerator Laboratory, Batavia, IL, USA

29 Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL, USA
30 Institut d’Astrophysique Spatiale, Orsay, France

ABSTRACT

Figure and1: characterization
The top author
AmandaStevieWe describe the constructionof the 280isGHz
bolometric focal
planeBergman.
units (FPUs) to be deployed on thesecond flight of the balloon-borne S PIDER instrument. These FPUs are vital to S PIDER’s primary science goal of detecting or
placing an upper limit on the amplitude of the primordial gravitational-wave signature in the cosmic microwave background(CMB) by constraining the B-mode contamination in the CMB from galactic dust emission. Each 280 GHz focal plane contains
a 16 ⇥ 16 grid of corrugated silicon feedhorns coupled to an array of aluminum manganese transition-edge sensor bolometers,
category : Applications
fabricated on 150 mm diameter substrates. In total, the three 280 GHz FPUs contain 1,530 polarization sensitive bolometers (765stevie@princeton.edu

95O-72 The LiteBIRD Space Mission - Sub-Kelvin Instrument
Aritoki Suzuki1 , LiteBIRD Collaboration2
1

Radio Astronomy Laboratory, University of California, Berkeley, 2 LiteBIRD Collaborating Institutions

Inflation is the leading theory to explain the first instant of the universe. Inflation, which postulates that the universe
underwent a period of rapid expansion an instant after its birth, beautifully explains cosmological observations.
Recent advancements in detection technology have opened opportunities to explore primordial gravitational waves
generated by the inflation through “B-mode” (divergent-free) polarization pattern embedded in the Cosmic Microwave
Background anisotropies. If detected, these signals would confirm inflation, point to the correct model for inflation,and open a window to physics at ultra-high energies.
LiteBIRD is a satellite mission with a goal of detecting degree-and-large- angular-scale B-mode polarization. The
LiteBIRD team is an international collaboration between Japan, the U.S., Canada, and Europe. LiteBIRD will observeat the second Lagrange point with a 500 mm diameter telescope and ∼2,000 detectors. It will survey the entire sky
with ∼2 microK arcmin noise equivalent CMB temperature (150 GHz) and characterize in 15 bands from 40 to 400
GHz to measure and subtract foregrounds.
The U.S. LiteBIRD team is proposing to deliver milli-Kelvin instruments that include detectors and readout
electronics.A lenslet-coupled sinuous antenna array will cover low-frequency bands (40 GHz to 235 GHz) with four
frequency arrangements of triplexer pixels. Orthomode-transducer-coupled corrugated horn array will cover highfrequency bands (280 GHz to 402 GHz) with three types of single frequency detectors.
Detection will be made with Transition Edge Sensor (TES) bolometers cooled to a 100 milli-Kelvin base temperatureby an adiabatic demagnetization refrigerator. The TES bolometers will be read out using digital frequency multiplexing
readout with Superconducting QUantum Interference Device (SQUID) amplifiers.
Up to 78 bolometers will be multiplexed with a single SQUID amplifer. A collaborative simulation-based study is
being conducted by an international team to optimize the instrument for foreground removal, including the eﬀects of
instrumental systematics. We will report on the milli-Kelvin instrument design and development plan.
category : Applications96

A. Suzuki,15, 45 P. A. R. Ade,48 Y. Akiba,50, 19 D. Alonso,42 K. Arnold,16 J. Aumont,20 C. Baccigalupi,25
D. Barron,49 S. Basak,11, 25 J. Borrill,6, 49 F. Boulanger,20 M. Bucher,3 E. Calabrese,48 Y. Chinone,15, 30 S.
Cho,13 B. Crill,26 A. Cukierman,15 D. W. Curtis,49 T. de Haan,44 M. Dobbs,43 A. Dominjon,35 T. Dotani,22
L. Duband,18 A. Ducout,30 J. Dunkley,10, 42 J. M. Duval,18 T. Elleflot,16 H. K. Eriksen,24 J. Errard,3 J.
Fischer,49 T. Fujino,54 T. Funaki,12 U. Fuskeland,24 K. Ganga,3 N. Goeckner-Wald,15 J. Grain,20 N. W.
Halverson,4, 9, 17 T. Hamada,2, 19 T. Hasebe,35 M. Hasegawa,19, 50 K. Hattori,37 M. Hattori,2 L. Hayes,49
M. Hazumi,19, 30, 50, 22 N. Hidehira,12 C. A. Hill,15, 44 G. Hilton,39 J. Hubmayr,39 K. Ichiki,32 T. Iida,30 H.
Imada,22 M. Inoue,40 Y. Inoue,21, 19 K. D. Irwin,13, 29 H. Ishino,12 O. Jeong,15 H. Kanai,54 D. Kaneko,30 S.
Kashima,35 N. Katayama,30 T. Kawasaki,31 S. A. Kernasovskiy,13 R. Keskitalo,6, 49 A. Kibayashi,12 Y. Kida,12 K.
Kimura,40 T. Kisner,6, 49 K. Kohri,19 E. Komatsu,34 K. Komatsu,12 C. L. Kuo,13, 29 N. A. Kurinsky,13, 29 A.
Kusaka,44, 14 A. Lazarian,53 A. T. Lee,15, 44, 45 D. Li,13 E. Linder,44, 49 B. Maﬀei,20 A. Mangilli,20 M. Maki,19 T.
Matsumura,30 S. Matsuura,27 D. Meilhan,49 S. Mima,46 Y. Minami,19 K. Mitsuda,22 L. Montier,5 M. Nagai,35
T. Nagasaki,19 R. Nagata,19 M. Nakajima,40 S. Nakamura,54 T. Namikawa,13 M. Naruse,47 H. Nishino,19
T. Nitta,52 T. Noguchi,35 H. Ogawa,40 S. Oguri,46 N. Okada,23 A. Okamoto,23 T. Okamura,19 C. Otani,46
G. Patanchon,3 G. Pisano,48 G. Rebeiz,16 M. Remazeilles,51 P. L. Richards,15 S. Sakai,22 Y. Sakurai,30 Y.
Sato,23 N. Sato,19 M. Sawada,1 Y. Segawa,50, 19 Y. Sekimoto,35, 8, 50 U. Seljak,15 B. D. Sherwin,7, 28, 44 T.
Shimizu,8 K. Shinozaki,23 R. Stompor,3 H. Sugai,30 H. Sugita,23 A. Suzuki,15, 45 J. Suzuki,19 O. Tajima,19, 50 S.
Takada,36 R. Takaku,54 S. Takakura,41, 19 S. Takatori,50, 19 D. Tanabe,50, 19 E. Taylor,49 K. L. Thompson,13, 29 B.
Thorne,42, 30 T. Tomaru,19 T. Tomida,22 N. Tomita,1 M. Tristram,33 C. Tucker,16 P. Turin,49 M. Tsujimoto,22
S. Uozumi,12 S. Utsunomiya,30 Y. Uzawa,38 F. Vansyngel,20 I. K. Wehus,24 B. Westbrook,15 M. Willer,49
N. Whitehorn,15 Y. Yamada,12 R. Yamamoto,22 N. Yamasaki,22 T. Yamashita,54 and M. Yoshida19(The LiteBIRD Joint Study Group)
1
Aoyama Gakuin University, Sagamihara, Kanagawa 252-5258, Japan
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, 980-8578, Japan
3
AstroParticule et Cosmologie (APC), Univ Paris Diderot,
CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
4
Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA
5
CNRS, IRAP, F-31028 Toulouse cedex 4, France
6
Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
7
DAMTP, University of Cambridge, Cambridge CB3 0WA, UK
8
Department of Astronomy, The University of Tokyo, Tokyo 113-0033, Japan
9
Department of Astrophysical and Planetary Sciences,
University of Colorado, Boulder, CO 80309, USA
10
Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
11
Department of Physics, Amrita University, Kerala 690525 India
12
Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
13
Department of Physics, Stanford University, Stanford, CA 94305-4060, USA
14
Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
15
Department of Physics, University of California, Berkeley, CA 94720, USA
16
Department of Physics, University of California, San Diego, CA 92093-0424, USA
17
Department of Physics, University of Colorado, Boulder, CO 80309, USA
18
French Alternative Energies and Atomic Energy Commission (CEA), Grenoble, France
19
High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
20
Institut d’Astrophysique Spatiale (IAS), CNRS, UMR 8617,
Université Paris-Sud 11, Bâtiment 121, 91405 Orsay, France
21
Institute of Physics, Academia Sinica, 128, Sec.2, Academia Road, Nankang, Taiwan
22
Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 252-0222, Japan
23
Research and Development Directorate, Japan Aerospace Exploration Agency (JAXA), Tsukuba, Ibaraki 305-8505, Japan
24
Institute of Theoretical Astrophysics, University of Oslo, NO-0315 Oslo, Norway
25
International School for Advanced Studies (SISSA), Via Bonomea 265, 34136, Trieste, Italy
26
Jet Propulsion Laboratory, Pasadena, CA 91109, USA
27
Kansei Gakuin University, Nishinomiya, Hyogo 662-8501, Japan
28
Kavli Institute for Cosmology Cambridge, Cambridge CB3 OHA, UK
29
Kavli Institute for Particle Astrophysics and Cosmology (KIPAC),SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
30
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,
WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
31
Kitazato University, Sagamihara, Kanagawa 252-0373, Japan
2

2
32

Kobayashi-Maskawa Institute for the Origin of Particle and the Universe,
Nagoya University, Nagoya, Aichi 464-8602, Japan
33
Laboratoire de l’Accélérateur Linéaire (LAL), Univ. Paris-Sud,
CNRS/IN2P3, Université Paris-Saclay, Orsay, France
34
Max-Planck-Institut for Astrophysics, D-85741 Garching, Germany
35
National Astronomical Observatory of Japan (NAOJ), Mitaka, Tokyo 181-8588, Japan36
National Institute for Fusion Science (NIFS), Toki, Gifu 509-5202, Japan37
National Institute of Advanced Industrial Science and Technology (AIST), Tsukuba, Ibaraki 305-8563, Japan38
National Institute of Information and Communications Technology (NICT), Kobe, Hyogo 651-2492, Japan
39
National Institute of Standards and Technology (NIST), Boulder, Colorado 80305, USA
40
Osaka Prefecture University, Sakai, Osaka 599-8531, Japan
41
Osaka University, Toyonaka, Osaka 560-0043, Japan
42
Oxford Astrophysics, Oxford, OX1 3RH, United Kingdom
43
Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
44
Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
45
Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA
46
RIKEN, Wako, Saitama 351-0198, Japan47
Saitama University, Saitama, Saitama 338-8570, Japan48
School of Physics and Astronomy, Cardiﬀ University, Cardiﬀ CF10 3XQ, United Kingdom
49
Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
50
The Graduate University for Advanced Studies (SOKENDAI),
Miura District, Kanagawa 240-0115, Hayama, Japan
51
The University of Manchester, Manchester M13 9PL, United Kingdom
52
Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, Ibaraki 305-8571, Japan
53
University of Wisconsin-Madison, Madison, Wisconsin 53706, USA
54
Yokohama National University, Yokohama, Kanagawa 240-8501, Japan97

O-73 Measuring Reionization, Neutrino Mass, and Cosmic Inflation with BFORE
Sean Alan Bryan1 , Philip Mauskopf2 , Mark Devlin3 , Christopher Groppi4 , Johannes Hubmayr5 , Jeﬀ McMahon6 ,John Ruhl7 , Joaquin Viera8 , Calvin Netterfield9 , Peter Ade10 , John Bond11 , Francois Boulanger12 , Jeﬀrey
Filippini13 , Laura Fissel14 , Gilbert Holder15 , Michael Niemack16 , Giles Novak17 , Giampaolo Pisano18 , Douglass
Scott19 , Juan Soler20 , Carole Tucker21
1

School of Earth and Space Exploration, Arizona State University, 2 Arizona State University , 3 University of Pennsylvania ,4
Arizona State University , 5 National Institute of Standards and Technology , 6 University of Michigan , 7 Case Western
Reserve University , 8 University of Illinois, Urbana-Champaign , 9 University of Toronto , 10 Cardiﬀ University , 11 University ofToronto , 12 Centre National de la Recherche Scientifique , 13 University of Illinois, Urbana-Champaign , 14 National Radio
Astronomy Observatory , 15 University of Illinois, Urbana-Champaign , 16 Cornell University , 17 Northwestern University ,18
Cardiﬀ University , 19 University of British Columbia , 20 Max Planck Institute for Astronomy , 21 Cardiﬀ University

BFORE is a NASA high-altitude ultra-long-duration balloon mission proposed to measure the cosmic microwave
background (CMB) across half the sky in a single 28-day mid-latitude flight launched from Wanaka, New Zealand.
With the unique access to large angular scales and high frequencies provided by the balloon platform, BFORE will
significantly improve measurements of the optical depth to reionization tau, breaking parameter degeneracies needed
for a measurement of neutrino mass with the CMB. The large angular scale data will enable BFORE to hunt for
the large-scale gravitational wave B-mode signal, as well as the degree-scale signal, each at the r 0.01 level. The
balloon platform allows BFORE to map Galactic dust foregrounds at frequencies where they dominate, in order torobustly separate them from CMB signals measured by BFORE, in addition to complementing data from ground-based
telescopes. The combination of frequencies will also lead to velocity measurements for thousands of galaxy clusters,
as well as probing how star-forming galaxies populate dark matter halos. The mission will be the first near-space useof TES multichroic detectors (150/217 GHz and 280/353 GHz bands) using highly-multiplexed mSQUID microwave
readout, raising the technical readiness level of both technologies.
category : Applications

98

Fabrication & Implementation
Techniques 299

O-74 Progress of Superconducting Electronics in Clean Room for Analog and Digital
Superconductivity: CRAVITY
Masahiro Ukibe1 , Go Fujii1 , Nobuyuki Zen1 , Shigetomo Shiki1 , Hiroyuki Yamamori1 , Shuichi Nagasawa1 , Mutsuo
Hidaka1 , Satoshi Kohjiro1 , Masataka Ohkubo1
1

National Institute of Advanced Industrial Science and Technology, 1-1-1, Umezono, Tsukuba, Ibaraki, 305-8568, JAPANIn recent years, superconducting array detectors with quite a large number of pixels ( 1000) have been developed
to satisfy demands for high throughput measurement or imaging capability in many applications such as astronomy,material analysis in synchrotron radiation facilities and laboratories. In order to realize such a large-scaled array,
it is necessary to solve three technological diﬃculties: a uniform performance of all pixels, an integration of signal
readout, and cryogenics. For the readout of large scale array detectors, superconducting signal processors are promisingand eﬀective to reduce the number of wires between a cryogenic temperature and a room-temperature environment.
The combination of a superconducting analog detector device and a superconducting digital circuit makes the total
measurement system compact and more practical.
Significant progresses in the above technological diﬃculties has been achieved by a facility called CRAVITY (Clean
room for analog and digital superconductivity) at AIST. First of all, the uniformity of superconducting tunnel junctions(STJs) was significantly improved. For example, a 100-pixel array X-ray detectors with 100 µm-square Nb/Al
STJs has a mean energy resolution (∆E) of 6.7 eV for 400 eV X-ray [1]. The pixel-to-pixel variation is less than ±1.0 eV. Moreover, the quality of the 1000 STJs is extremely uniform: a leakage current variation of ± 1.5 nA at 12.2 nA
in the subgap region. The leakage current uniformity ensures stable biasing for the 1000 pixels simultaneously [2].
Second is the integration of superconducting detectors and signal processors. A high-resolution time-of-flight mass
spectrometry (TOF-MS) was developed by combining a superconducting strip ion detector (SSID) and a single-fluxquantum (SFQ) time-to-digital converters (TDCs) [3, 4]. The signal processing with the SFQ-TDC at 4 K allows alarge reduction of the number of the wirings between a future SSID array detector and a room temperature electronics.
This is necessary for a practical TOF-MS system with a superconducting detector of which detection area is comparable
to those of widely used microchannel plate (MCP) detectors.
The above-mentioned high-performance superconducting devices can be produced in CRAVITY. One of the uniquefeatures of CRAVITY is multilayer superconducting device fabrication based on a planarization technique using chemical mechanical polishing (CMP). In order to achieve a high productivity of complicated analog/digital superconducting
devices and circuits, almost all installed process machines are fully automated. Now, the CRAVITY plays an important role as an innovation hub in the superconducting electronics research.
[1] M. ukibe et al., J. Low Temp. Phys. 184, 200 (2016).
[2] G. Fujii et al., To be published.
[3] N Zen et al., Appl. Phys. Lett. 104, 012601 (2014).
[4] Sano et al., Physica C 540, 97 (2014).

Acknowledgment
The authors thank to clean room members of CRAVITY for their assistance in superconducting device fabrication.
category : Fabrication & Implementation Techniques100

O-75 LC filters for FDM readout of the X-IFU TES calorimeter instrument on AthenaMarcel P. Bruijn1 , Anton J. van der Linden2 , Lorenza Ferrari3 , Luciano Gottardi4 , Jan van der Kuur5 , Roland H.
den Hartog6 , Brian D. Jackson7
1

Instrument Science Group, SRON Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space
Research , 3 SRON Netherlands Institute for Space Research , 4 SRON Netherlands Institute for Space Research , 5 SRON
Netherlands Institute for Space Research , 6 SRON Netherlands Institute for Space Research , 7 SRON Netherlands Institutefor Space Research

The X-ray Integral Field Unit (X-IFU) will be a cryogenic X-ray spectrometer on board of the Athena space telescope(ESA, launch in 2028). A large array ( 4000) of Transition Edge Sensors (TES) will be read out, using a Frequency
Division Multiplexing (FDM) technique. Key part of this read out circuit forms a set of chips with high quality factor
superconducting resonators (LCR) where the TES, biased in its transition, forms the resistive element. The chips
serve to deliver the bias power, through reactive voltage division, filter wide band noise from each TES, and sum all
signals with diﬀerent bias frequency to the SQUID based amplification circuit. SRON is developing this technique formany years already for bolometers and calorimeters [1, 2] and has shown that the energy resolution of calorimeters inthis mode is very close to that under DC bias
Heading towards the Demonstration Model for X-IFU, we have fabricated chips for multiplexing of 40 TES pixels
into one SQUID channel. We will present the fabrication and characterization results in FDM development setups
for this DM. Important quality issues are fabrication yield, resonator quality (eﬀective series resistance), cross talk,accuracy of resonance frequency distribution and packing density.
We will present results of an optimization study of these quality issues, where Finite Element Modeling (FEM) is
used in aiding the design. The FEM models are being validated by direct measurements of mutual- and self inductanceof representative test cases.
For the a-Si:H based capacitors and Nb-based coils, presently the component fabrication yield is about 99 % and
the Q-factor at 50 mK is higher than 100.000 at 5 MHz resonance frequency.
[1] Bruijn, M.P., Gottardi, L., Hartog den, R.H., Kuur van der, J., Linden van der, A.J., Jackson, B.D., ”Tailoring
the High-Q LC Filter Arrays for Readout of Kilo-Pixel TES Arrays in the SPICA-SAFARI Instrument”, Journal of
Low Temperature Physics: Volume 176, Issue 3, p. 421-425, 2014, doi:10.1007/s10909-013-1003-6[2] Gottardi, L. , Akamatsu, H, Bruijn, M.P. Hartog, den R, Herder den, J.W., Jackson, J., Kiviranta, M., Kuur
van der, J., Weers van, H., ”Development of the superconducting detectors and read-out for the X-IFU instrument
on board of the X-ray observatory Athena”, Nuclear Instruments and Methods in Physics Research 824, p. 622-625,
2016, doi:10.1016/j.nima.2015.09.072
category : Fabrication & Implementation Techniques101

O-76 The DARKNESS Array: A 10,000 Pixel PtSi MKID Array
Paul Szypryt1 , Seth R. Meeker2 , Bruce Bumble3 , Gregoire Coiﬀard4 , Gerhard Ulbricht5 , Neelay Fruitwala6 , Alex B.
Walter7 , Miguel Daal8 , Clint Bockstiegel9 , Giulia Collura10 , Benjamin A. Mazin11
1

Department of Physics, University of California, Santa Barbara, 2 University of California, Santa Barbara , 3 NASA Jet
Propulsion Laboratory , 4 University of California, Santa Barbara , 5 University of California, Santa Barbara , 6 University ofCalifornia, Santa Barbara , 7 University of California, Santa Barbara , 8 University of California, Santa Barbara , 9 University ofCalifornia, Santa Barbara , 10 University of California, Santa Barbara , 11 University of California, Santa Barbara

We have fabricated and characterized 10,000 pixel MKID arrays for the Dark-speckle Near-IR Energy-resolved Superconducting Spectrophotometer (DARKNESS). DARKNESS is a new MKID instrument designed to sit behind an
adaptive optics system with the goal of directly imaging extrasolar planets in a 700-1400 nm band. The array contains
10,000 (80x125) pixels divided evenly between 5 coplanar waveguide microwave transmission lines. These MKIDs aredesigned with a readout band of 4-8 GHz, with 2 MHz spacing between resonators. In the past, the DARKNESS
detector arrays were fabricated using titanium nitride on a silicon substrate. These arrays, however, suﬀered fromsevere non-uniformities in the TiN critical temperature, causing resonances to shift away from their designed values
and lowering usable detector yield. More recently, we have instead fabricated DARKNESS arrays using platinum
silicide on sapphire. Not only do these arrays have much higher uniformity than the TiN arrays, resulting in higher
pixel yields, they also display improved sensitivity to photons within DARKNESS’s band of operation. PtSi MKIDs
also do not display the hot pixel eﬀects seen when illuminating TiN on silicon MKIDs with photons shorter than 1
micron. Finally, the PtSi detectors have energy resolution similar to that seen in the TiN devices, but this is expected
to improve as the quality factor of the resonators is increased. In the near future, we will be fabricating 20,000 pixel
versions of these arrays to be used in the MKID Exoplanet Camera (MEC).
category : Fabrication & Implementation Techniques102

O-77 Magnetic Calorimeter Arrays with High Sensor Inductance and Dense WiringThomas R. Stevenson1 , Simon R. Bandler2 , Manuel A. Balvin3 , Archana M. Devasia4 , Peter C. Nagler5 , Stephen J.
Smith6 , Wonsik Yoon7
1

NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center , 3 NASA Goddard Space Flight Center , 4 NASA
Goddard Space Flight Center / CRESST, University of Maryland, Baltimore County , 5 NASA Goddard Space Flight Center ,6
NASA Goddard Space Flight Center / CRESST, University of Maryland, Baltimore County , 7 NASA Goddard Space Flight
CenterWe describe prototype arrays of Magnetically-Coupled Microcalorimeters fabricated with an approach scalable to verylarge format arrays. The superconducting interconnections and sensor field coils have suﬃciently low inductance inthe wiring and suﬃciently high inductance in the field coils in each pixel, to enable arrays containing greater than
4000 sensors and 100,000 x-ray absorbers to be used in future astrophysics missions such as Lynx. We have usedprojection lithography to create submicron patterns (e.g. 400 nm lines and spaces) in our niobium sensor meanders
and wiring, integrated with gold-erbium sensor films and gold x-ray absorbers. Our prototype devices will explore thedevice physics of Metallic Magnetic Calorimeters as feature sizes are reduced to nanoscale.
category : Fabrication & Implementation Techniques

103

Cryogenics and Components 1104

O-78 CUORE, a large cryogenic system for LTDs
Carlo Bucci1
1

INFN - Laboratori Nazionali del Gran Sasso

In recent years, large mass cryogenic detectors have achieved excellent performances and are widely used in neutrinoless double beta decay and dark matter searches. In such types of experiments a sizable detector mass is a key
issues and requires special cryogenic systems.
The Cryogenic Underground Observatory for Rare Events (CUORE) is searching for neutrinoless double beta decay
in 130Te. CUORE must operate a ton-scale array of 988 TeO2 cryogenic detectors at 10 mK providing exceptionally
low background and low vibration conditions. In order to meet this unprecedented challenge, the CUORE detector
array is cooled down by a multistage cryogen-free cryostat. The base temperature is delivered by a custom made3He-4He dilution refrigerator. Strict material selection and cleaning procedures are applied to all the structures facing
the detector. Seven tons of low-temperature lead shielding protect the inner cubic meter scale experimental volume
from the residual background contamination of the cryostat. Vibration-induced noise is minimized by means of special
suspensions that mechanically decouple the detector from the cryostat. In 2017 the CUORE cryostat successfully
cooled down the ton-scale detector at 7mK, delivering an uniform and constant base temperature over few months.
In this talk the CUORE cryogenic setup, the results of the commissioning runs and the performance of the system
during the first CUORE physics run will be presented.
category : Cryogenics and Components

105O-79 A continuous 100-mK helium-light cooling system for MUSCAT on the LMT
Thomas L R Brien1 , Edgar Castillo-Dominguez2 , Simon Chase3 , Simon Doyle4
1

School of Physics & Astronomy, Cardiﬀ University, 2 Instituto Nacional de Astrofisica, Optica y Electronica (Mexico) ,3
Chase Research Cryogenics Ltd. , 4 School of Physics & Astronomy, Cardiﬀ University

The MUSCAT instrument is a large-format camera planned for installation on the Large Millimeter Telescope (LMT)in early 2018. MUSCAT requires continuous cooling of several large-volume stages to sub-Kelvin temperatures, withthe focal plane cooled to 100 mK. Through the use of continuous sorption pumps and a miniature dilution refrigerator,
the MUSCAT project can fulfil its cryogenic requirements at a fraction of the cost and space required from conventional
dilution systems. Our design is a helium-light system, using a total of only 9 litres of helium-3 across several continuous
cooling systems, cooling from 4 K to 100 mK. Here we describe the operation of both the continuous sorption and theminiature dilution refrigerator systems along with the overall thermal design and budgeting of MUSCAT to enable
this large-format camera to be compatible with our proposed compact continuous cooler. MUSCAT will represent thefirst deployment of this new technology in a science-grade instrument and will prove the concept as a viable option
for future large-scale experiments such as CMB-S4.
category : Cryogenics and Components

106Cryogenics and Components 2107

O-80 Vibration measurement and mitigation for cryogen-free dilution refrigerators
Chang Lee1
1

Center for Underground Physics, Institute of Basic Science

While cryogen-free dilution refrigerators are getting more popular for operation of low temperature detectors, mechanical vibration originating from its pulse tube refrigerator can aﬀect experiments in various ways. We present thedisplacement, velocity, and acceleration measurement results at diﬀerent stages of a commercial dilution refrigerator
in vertical and horizontal directions. The same measurements are repeated after installing mechanical filters at two
diﬀerent stages. The eﬀects of the filters on the sensor waveform, energy resolution, and particle discriminations are
discussed as well.
category : Cryogenics and Components

108O-81 Electromagnetic Design of a Magnetically-Coupled Spatial Power Combiner
Berhanu T Bulcha1 , Cataldo Giuseppe2 , Stevenson Thomas3 , U-yen Kongpop4 , Moseley Samuel5 , Wollack Edward6
1

NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center , 3 NASA Goddard Space Flight Center , 4 NASA
Goddard Space Flight Center , 5 NASA Goddard Space Flight Center , 6 NASA Goddard Space Flight Center

Bulcha, B., Cataldo, G, Stevenson, T.R., U-Yen, K., Moseley, S.H., Wollack, E.J.
NASA Goddard Space Flight Center
Abstract ? The design of a two-dimensional spatial beam-combining network employing a parallel-plate superconducting waveguide with a mono-crystalline silicon dielectric is presented. This novel component employs arraysof magnetically coupled antenna elements to achieve high coupling eﬃciency and full sampling of the intensity distribution while avoiding diﬀractive losses in the multi-mode region defined by the guide. These attributes enable thestructure s use in realizing compact far-infrared spectrometers for astrophysical and instrumentation applications.
If unterminated, reflections within a finite-sized spatial beam combiner can potentially lead to spurious couplings.
A meta-material electromagnetic absorber is implemented to control this response in the device. This broadband
termination absorbs greater than 99% of the power over the 1.7:1 operational band at angles ranging from normal
to near parallel incidence. The design approach, simulations, and applications of the spatial power combiner will bepresented.
category : Cryogenics and Components

109O-82 A temperature dependent x-ray absorption characterization of test filters for
the ATHENA mission X-IFU instrument
Luisa Sciortino1 , Ugo Lo Cicero2 , Salvartore Ferruggia Bonura3 , Elena Magnano4 , Stefano Nannarone5 , Konstantin
Koshmak6 , Antonella Balerna7 , Marco Barbera8
1

Dipartimento di Fisica e Chimica, Universita degli Studi di Palermo, 2 INAF, Osservatorio Astronomico di Palermo G.S.
Vaiana, Palermo, Italy , 3 Universita degli Studi di Palermo, Dipartimento di Fisica e Chimica, Palermo, Italy , 4 IOM-CNR,
Laboratorio TASC, Trieste, Italy , 5 IOM-CNR, Laboratorio TASC, Trieste, Italy , 6 IOM-CNR, Laboratorio TASC, Trieste,
Italy , 7 INFN, Frascati National Laboratory, Frascati, Italy , 8 Universita degli Studi di Palermo, Dipartimento di Fisica e
Chimica, Palermo, Italy / INAF, Osservatorio Astronomico di Palermo G.S. Vaiana, Palermo, Italy

The ATHENA mission, that provides the demanded capabilities to address the ESA science theme ”Hot and Energetic
Universe”, will be equipped with an high spectral resolution energy dispersive instrument named X-ray Integral Field
Unit (X-IFU).
The X-IFU detector is an array of Transition-Edge Sensor microcalorimeters that will be sensitive in the 0.2
keV - 12 keV energy range, with 2.5 eV energy resolution at 7 keV. Such a detector operates at 50 mK and thus
requires a sophisticated multistage cryostat. Thermal filters will be used to close the X-rays entrance aperture in thecryostat thermal shields. These filters, highly transparent in X-rays, will attenuate the Infrared (IR) radiative heatload onto the microcalorimeters and will avoid energy resolution degradation due to photon shot noise. Polyimide
and aluminum have been currently selected as suitable filter materials in order to achieve high X-ray transmission andgood IR reflection, respectively. In the current design five filters are expected to be used at five diﬀerent temperatures
corresponding to the cryostat shields temperatures. Each filter consists of a bilayer of thin polyimide membrane (45nm - 100 nm thick) coated with aluminum film ( ∼ 30 nm thick).
The chemical elements (C, N, O, and Al) that make up the filters show absorption X-rays edges in the energetic
range of interest of the X-IFU. The oscillations above the edges are known to be sensitive to the changes of temperatures.
Since the X-IFU will have an high spectroscopic resolution, an accurate knowledge of the X-ray response of the filters
is mandatory to sort out a reliable calibration plan. Here, we present the X-ray absorption characterization of test
filters in the soft X-rays (40 eV - 1750 eV) range at diﬀerent temperatures (80 K - 300 K) to investigate the eﬀect oftemperature on the selected materials and its impact on the calibration of the flight filters.
category : Cryogenics and Components

110Application - Material analysis andothers 1111

O-83 Analytical Transmission Electron Microscope using a Transition Edge Sensor for
X-ray Microanalysis
Toru Hara1 , Keiichi Tanaka2 , Keisuke Maehata3 , Kazuhisa Mitsuda4 , Yoshihiro Yamanaka5 , Mutsuo Hidaka6 ,Kuniyasu Nakamura7
1

Research Center for Structural Materials, National Institute for Materials Science, 2 Hitachi High-Tech Science Corporation /Hitachi High-Technologies Corporation , 3 Kyushu University , 4 Japan Aerospace Exploration Agency , 5 Taiyo Nippon Sanso
Corporation , 6 National Institute of Advanced Industrial Science and Technology , 7 Hitachi High-Technologies Corporation

Microstructure evaluation is essentially important to develop new materials. Electron microscopes, such as scanningtransmission electron microscope (STEM), plays an important role for such purpose. A function of compositional
analysis in nano-scale, in addition to microstructure morphological observation, is very important for current electron
microscopy analysis. In order to measure the composition in electron microscopes, x-ray spectroscopy, which is inducedby the incident electron beam is now widely applied. However, accuracy and/or sensitivity of a semiconductor based
x-ray detector is not suﬃcient for the current required level: for example, advanced heat-resistant steel contains morethan 10 elements with their amount of ¡0.1% each. They have been added empirically to improve mechanical property.
However, at present, we do not understand where and how these trace elements work. In order to realize precise x-ray
analysis in electron microscopes, we have been trying to apply transition-edge sensor (TES) microcalorimeter. With
using this detector, it is expected that most of all elements can be measured without any peak overlaps, it leads highaccuracy and sensitivity. To ensure high spatial resolution, less than 1nm, we adopt the TES detector onto a STEM.
Our target specs of the developed x-ray detector are as follows: i) x-ray energy resolution: ¡10eV, ii) detecting
x-ray energy range: 0.5-10keV or wider, iii) x-ray counting rate: ¿5kcps. Applying this x-ray detector with a STEM
whose accelerating voltage of 200kV, we will be able to realize the elemental mapping with a spatial resolution of lessthan 10nm. In order to realize the specs listed above, we developed a new detector system. The developed TES-STEM
system is shown in figure 1. The characteristic points of the detector are as follows: i) detector device is 64 pixel
TES to increase countrate more than 5kcps, ii) multicapillary x-ray lens is applied to increase detecting solid-angle,iii) compact Liq.He free cooling system has been developed for high stability. Newly developed cooling system, basedon a dilution refrigerator, can keep low temperature more than half a year, so that we can measure anytime with thesame condition. By the end of 2016, we have assembled the new analytical STEM with the multipixel TES detector
and succeeded to obtain x-ray spectra with high energy-resolution, less than 10eV, for the range from 0.5-15keV.
In this report, I will briefly review the recent progress of development on the analytical STEM applied with themultipixel TES detector system.

STEM Column
STEM Console

SampleDilutionrefrigerator

Detector

category : Applications

112

113

O-84 Ultrafast X-ray Spectroscopies using TES Microcalorimeter Sensors: Recent
Table-top Demonstrations and Current Work
Joel N Ullom1 , B. K. Alpert2 , M. Balasubramanian3 , N. Chen4 , N. H. Damrauer5 , W. B. Doriese6 , S. M. Fatur7 , J.
W. Fowler8 , W. K. Fullagar9 , G. C. Hilton10 , Y. I. Joe11 , R. Jimenez12 , L. Miaja-Avila13 , G. C. O’Neil14 , B. Ravel15 ,C. D. Reintsema16 , D. M. Sagar17 , D. R. Schmidt18 , K. L. Silverman19 , D. S. Swetz20 , H. Tatsuno21 , J. Uhlig22
1

NIST and University of Colorado, 2 NIST, Boulder, Colorado 80305, USA , 3 Advanced Photon Source, Argonne National
Laboratory, Lemont, Illinois 60439, USA , 4 Canadian Light Source, Saskatoon, Saskatchewan S7N 2V3, Canada , 5 Departmentof Chemistry and Biochemistry, University of Colorado Boulder, Boulder, Colorado 80309, USA , 6 NIST, Boulder, Colorado
80305, USA , 7 Department of Chemistry and Biochemistry, University of Colorado Boulder, Boulder, Colorado 80309, USA ,8
NIST, Boulder, Colorado 80305, USA , 9 Department of Chemical Physics, Lund University, Lund 223 62, Sweden , 10 NIST,
Boulder, Colorado 80305, USA , 11 NIST, Boulder, Colorado 80305, USA , 12 JILA, NIST and University of Colorado Boulder,
Boulder, Colorado 80309, USA / Department of Chemistry and Biochemistry, University of Colorado Boulder, Boulder,
Colorado 80309, USA , 13 NIST, Boulder, Colorado 80305, USA , 14 NIST, Boulder, Colorado 80305, USA , 15 NIST,
Gaithersburg, Maryland 20899, USA , 16 NIST, Boulder, Colorado 80305, USA , 17 JILA, NIST and University of Colorado
Boulder, Boulder, Colorado 80309, USA , 18 NIST, Boulder, Colorado 80305, USA , 19 NIST, Boulder, Colorado 80305, USA ,20
NIST, Boulder, Colorado 80305, USA , 21 NIST, Boulder, Colorado 80305, USA / Department of Chemical Physics, Lund
University, Lund 223 62, Sweden , 22 Department of Chemical Physics, Lund University, Lund 223 62, Sweden

This presentation on the use of Transition-Edge Sensor (TES) x-ray detectors for ultrafast materials analysis will
cover three topics. First, we describe a recent successful demonstration of table-top Time-Resolved X-ray Absorption
Spectroscopy (TR-XAS) using a laser plasma x-ray source to produce picosecond (ps) duration x-ray pulses and a 240
element TES array read out using time-division SQUID multiplexing for x-ray detection. This apparatus allows opticalpump, x-ray probe experiments with ultrafast temporal resolution. Using TR-XAS, we studied the photoreduction of
ferrioxalate, a reaction that has been the subject of a long-running debate in the literature, including contradictory
x-ray measurements. Our results [1] strongly support a picture in which reduction of the central iron is complete by
100 ps and contradict a theory in which the photoreduction occurs on much longer timescales.
Second, after making a small geometrical change to our apparatus, we were able to demonstrate Time-Resolved Xray Emission Spectroscopy (TR-XES). Using TR-XES, we studied spin cross-over in photoexcited iron tris-bipyridine
and accurately measured the lifetime of the quintet state from simultaneous observations of the iron Kalpha and Kbeta
features. We also determined the time resolution of our apparatus to be better than 6 ps. Better time resolution in
TR-XES has only been demonstrated at two x-ray free electron lasers. These results [2] are the first laboratoryscale demonstration of ultrafast TR-XES and they were enabled by the unique combination of spectral resolution andcollecting eﬃciency provided by TES sensors. In particular, the collecting eﬃciency of these devices allowed the quintet
lifetime to be measured using 100-1,000 × fewer x-rays delivered to the sample than comparable work performed ata synchrotron.
Our TR-XAS and TR-XES results are the first use of TES sensors for ultrafast x-ray science. The execution ofthese complicated experiments has provided valuable lessons with regard to calibration, cross-talk, time stamping, andlarge-scale pulse processing. In the final part of the presentation, we discuss some of these lessons. We also discusscurrent work that includes (1) a TES spectrometer for time-resolved x-ray science at the Linac Coherent Light Source
under development with SLAC and Stanford University, and (2) a significant upgrade to the table-top time-resolved
x-ray apparatus located at NIST.
[1] G. C. O Neil et al, Journal of Physical Chemistry Letters 8, 1099 (2017)[2] L. Miaja-Avila et al, Physical Review X 6, 031047 (2016)
category : Applications

114

O-85 An ultra-sensitive probe of local electronic structures using transition-edge
sensor X-ray microcalorimeters at the Stanford Synchrotron Radiation Lightsource
Sang Jun Lee1
1

SLAC National Accelerator Laboratory

Transition-edge sensor (TES) microcalorimeters provide a unique combination of good energy resolution and higheﬃciency, enabling a two-order-of-magnitude improvement over existing technology in sensitivity to defects, dopants,
thin surface layers, and dilute solutes. We have developed an X-ray spectrometer based on an array of 240-pixel
TESs using time-division multiplexed readout, and commissioned the spectrometer at the Stanford Synchrotron Radiation Lightsource (SSRL). This system is a powerful new tool to probe the local electronic structure of ultra-low
concentration sites in biology, chemistry and materials science in the soft X-ray regime that are currently inaccessible
due to the limited sensitivity of existing technology. We have performed a number of experiments to explore newparadigms in soft X-ray spectroscopy enabled by the TES spectrometer, achieving an extremely high sensitivity of
sub-mM concentrations in aqueous/organic solvents, sub-percent sensitivity for monolayer films, and sensitivity toconcentrations < 1019 /cm3 for defect and dopants. We present an introduction to our TES spectrometer and recent scientific results with dopants/defects in N-doped carbon and semiconductors, and measurements of active metal
centers in bio-enzymes. We further describe our eﬀorts towards seamless integration of the TES with X-ray science
experiments in a synchrotron environment.
category : Applications

115

Application - Material analysis andothers 2116O-86 A Search for the Decay of Metastable Th-229m with Superconducting Tunnel
JunctionsFrancisco Ponce1 , Erik L. Swanberg2 , Jason T. Burke3 , Stephan Friedrich4
1

Lawrence Livermore National Laboratory, 2 Lawrence Livermore National Laboratory , 3 Lawrence Livermore National
Laboratory , 4 Lawrence Livermore National Laboratory

The desire to build ultra-precise nuclear clocks is currently driving the interest in accurate measurements of low-energy
metastable nuclear states. The approach to embed the radioactive nucleus of interest inside the Superconducting
Tunnel Junction (STJ) detector is particularly promising, because the measured decay energy does not depend on
chemical eﬀects. We have demonstrated this approach by implanting recoiling U-235m nuclei from the alpha decayof Pu-239 inside a STJ, and measuring the decay of the U-235m to the ground state. The STJ response is calibrated
with an energy comb of photons from a pulsed 355 nm laser, and corrected for drift and oﬀsets. An energy resolutionof 2 eV FWHM and maximum count rates above 5000 counts/s allow calibration of the STJ to a precision of better
than 10 meV. With the method proven, we began a search for the decay of metastable Th-229m, whose first excitednuclear state lies at only 7.6 ± 0.5 eV above the ground state. We show that high-resolution STJ photon detectors
can reduce the uncertainty of the decay energy of U-235m by an order of magnitude, and discuss the first results fromthe search for the decay of Th-229m.
category : Applications

117

O-87 TES application to kaonic atom X-ray spectroscopy in a charged-particle
beamline
Tadashi Hashimoto1 , HEATES collaboration2
1
Advanced Science Research Center, Japan Atomic Energy Agency, 2 Advanced Science Research Center, Japan Atomic
Energy Agency / RIKEN Nishina Center, RIKEN / National Institute of Standards and Technology (NIST) / Department of
Physics, Tokyo Metropolitan University

We are developing a new technique to study the strong interaction between a hadron and an atomic nucleus:
high-resolution TES-based X-ray spectroscopy of hadronic atoms. A hadronic atom is a Coulomb-bound system of
a nucleus, electrons, and a negatively charged hadron, such as a π − , K − , or anti-proton. It is formed when thenegatively charged hadron beam produced at an accelerator is stopped in a target sample. The hadron is initially in ahighly excited state, which then cascades by emitting electrons and X-rays. The hadron s mass is much larger thanthe electron s mass, so the atomic transitions of the hadronic atom are shifted to much higher energies than thoseof the corresponding standard atom. In addition, the strong interaction induces a shift and broadening of the atomic
energy levels from their purely electromagnetic values. Thus, precise measurements of the X-ray-emission lines of a
hadronic atom can reveal the hadron-nucleus strong interaction at zero kinetic energy.
In recent years, anti-kaonic nuclear states have been proposed and are attracting great interest as a new form ofmatter and a possible unique testing ground of dense nuclear matter. However, the existence of these states is still
controversial, primarily due to the lack of precise enough measurements of the antikaon-nucleus strong interaction.
Presently, we are preparing to measure the 3d-2p X-ray lines of kaonic helium-3 and helium-4 (6.2 keV and 6.4 keV,
respectively) at the Japan Proton Accelerator Research Complex (J-PARC; Tokai, Japan). If we determined thestrong-force shift in the helium 2p orbital to a precision of 0.2 eV, we could distinguish between the two leading
antikaon-nucleus strong-interaction models. Semiconductor X-ray detectors have been used in previous experiments.
Here, we plan to use a 240-pixel TES array of about 23 mm2 collecting area with 4 µm thick Bi absorbers.
Our project represents the first attempt to use a TES-based X-ray spectrometer in a charged-particle beamline, andwe have identified some challenges: 1) energy resolution is deteriorated by charged-particle passages; 2) a continuum
background in the X-ray spectrum is generated by charged particles; 3) the science X-ray yield is expected to be very
low, at 200 counts per week for the kaonic-helium-atom experiment.
Here we present the status of our project. In 2014, we performed a demonstration experiment at a pion beamlineof the Paul Scherrer Institute (PSI; Villigen, Switzerland). We successfully measured the pionic-carbon 4-3 X-ray line
at 6.4 keV with average energy resolution of 7 eV (FWHM). In June 2016, we tested the spectrometer under realistic
experimental conditions at J-PARC K1.8BR beamline. Our two promising results were achieved energy resolution
close to 6 eV and confirmation that the continuum background intensity caused by charged particles was low enoughto allow observation of the dim kaonic-atom emission lines.
Finally, we describe the technical details of our scientific kaonic-atom X-ray spectroscopy campaign that is plannedfor early 2018.
HEATES collaboration
T. Hashimoto1 , M. Bazzi2 , D.A. Bennett3 , C. Berucci4 , D. Bosnar5 , C. Curceanu2 , W.B. Doriese3 , J.W. Fowler3 , H. Fujioka6 ,C. Guaraldo2 , F. Parnefjord Gustafsson7 , R. Hayakawa8 , R.S. Hayano9 , J.P. Hays-Wehle3 , G.C. Hilton3 , T. Hiraiwa10 ,Y. Ichinohe8 , M. Iio11 , M. Iliescu2 , S. Ishimoto11 , Y. Ishisaki8 , K. Itahashi12 , M. Iwasaki12,13 , Y. Ma12 , H. Noda14 ,H. Noumi10 , G.C. O’Neil3 , H. Ohnishi15 , S. Okada12 , H. Outa12 , K. Piscicchia2 , C.D. Reintsema3 , Y. Sada10 , F. Sakuma12 ,M. Sato11 , D.R. Schmidt3 , A. Scordo2 , M. Sekimoto11 , H. Shi2 , D. Sirghi2 , F. Sirghi2 , K. Suzuki4 , D.S. Swetz3 , K. Tanida1 ,H. Tatsuno7 , M. Tokuda13 , J. Uhlig7 , J.N. Ullom3,17 , S. Yamada8 ,T. Yamazaki9 and J. Zmeskal4
1 Japan Atomic Energy Agency (JAEA)
2 Laboratori Nazionali di Frascati dell’ INFN
3 National Institute of Standards and Technology (NIST)
4 Stefan-Meyer-Institut für subatomare Physik
5 Department of Physics, University of Zagreb
6 Department of Physics, Kyoto University
7 Department of Chemical Physics, Lund University
8 Department of Physics, Tokyo Metropolitan University
9 Department of Physics, The University of Tokyo
10 Research Center for Nuclear Physics (RCNP), Osaka University
11 High Energy Accelerator Research Organization (KEK)
12 RIKEN Nishina Center, RIKEN

118

13 Department of Physics, Tokyo Institute of Technology
14 Frontier Research Institute for Interdisciplinary Sciences, Tohoku University
15 Research Center for Electron Photon Science, Tohoku University
16 AMO physics laboratory, RIKEN
17 Department of Physics, University of Colorado at Boulder

category : Applications

119O-88 Calorimetry of Heavy Charged Particle by superconducting transition edge
sensorMasashi Ohno1 , Tomoya Irimatsugawa2 , Yoshitaka Miura3 , Hiroyuki Takahashi4 , Tokihiro Ikeda5 , Chiko Otani6 ,Makoto Sakama7 , Naruhiro Matsufuji81

Nuclear Professional School, School of Engineering, The University of Tokyo, 2 The University of Tokyo , 3 The University ofTokyo , 4 The University of Tokyo , 5 RIKEN , 6 RIKEN , 7 National Institute of Radiological Sciences , 8 National Institute ofRadiological Sciences

Precision measurement of the absorbed dose in heavy ion beam is required to realize the eﬀective heavy ion cancer
therapy. Calorimetry of the absorbed energy in heavy ion is very eﬀective for minimizing of the uncertainty in dose
rate measurement. Therefore we suggest the superconducting transition edge sensor (TES) for the precision heavycharged particle detector. Using the Ir/Au-TES coupled to a tin absorber, we have succeeded to detect the helium
ions and the carbon ions which were injected from HIMAC (Heavy Ion Medical Accelerator in Chiba) in National
Institute of Radiological Sciences. In the experiment of the helium ions beam injection (100 MeV/u), LET (Linier
Energy Transfer) inside the tin absorber which is 0.3 mm thick, was adjusted by changing attenuation length of thealuminum attenuator. Although the incident signals are fully saturated because the temperature change is beyond
the transition region, the saturation time of the signal is reflected the incident energy of the injected heavy ions. As aresult we confirmed that the saturation time of the observed incident signal depends on the loss energy inside the tin
absorber, which is calculated from the integral of LET. Based on these results, we consider that TES is the promisingdetector for precision calorimetry of heavy charged particle.

Al : 35 mm
Al : 34 mm

Saturation time

Al : 36 mm

Al : 0 mm

Al

0.3mm

Sn
absorberIr/Authermometer

category : Applications120

O-89 A few photon spectral imaging with photon microscope based on opticaltransition edge sensor
Daiji Fukuda1 , Kazuki Niwa2 , Kaori Hattori3 , Ryo Kobayashi4 , Takayuki Numata5 , Shuichiro Inoue6
1

NMIJ/AIST, 2 NMIJ/AIST , 3 NMIJ/AIST , 4 NMIJ/AIST / Nihon University , 5 NMIJ/AIST , 6 Nihon University

We report on the development of a photon microscope , which can measure single photon spectra from an object andconstruct two dimensional red-green-blue (RGB) and infrared images[1]. The photon microscope contains an opticalsystem coupled to an optical fiber and a single pixel optical transition edge sensor (TES). The TES is fabricated with a
Titanium-Gold bilayer embedded in an optical cavity structure to enhance detection eﬃciency[2]. Its eﬀective spectral
range is from the visible to the infrared (IR), up to 2800 nm, which is beyond the capabilities of other photodetectors.
We have performed a demonstration of the photon microscope with a test sample of a three-color ink pattern. The
test sample is illuminated by a heavily attenuated white light source from a halogen lump. The reflected photons aremeasured with the optical fiber coupled TES in the microscope. A spectrum of photons at each focus point on thesample is determined by measuring the energy of reflected photons from the sample with the TES. By scanning thesample, a RGB color image is constructed from the spectra. The attached figure shows an example of the obtained
image for the test sample with 200 × 200 pixels, 1 µ m in the scan step and 50 ms/pixel in exposure time. The average
photon number in the experiment is 20 photons/pixel, which corresponds to optical power of 0.15 fW. As shown in
the figure, a high contrast RGB image was successfully obtained in the few photon regime, whereas only a black andwhite image could be obtained with a photon multiplier tube. This is a great advantage of the energy-dispersive TES
photon detectors.
In life science research and industry, multiple biomolecules labeled with color, fluorescence, and/or chromic dye
probes are observed in spectral imaging to determine the dynamic molecular mechanisms behind the biological phenomena. The results of the photon microscope show that TES is a very powerful tool for use in these spectral imaging
applications.
References:[1] K. Niwa and et al., Sci. Rep. 7, 45660; doi:10.1038/srep45660 (2017).
[2] D. Fukuda et al., Opt. Express 19, 870-875 (2011).

121

category : Applications

122

O-90 2d MMC arrays for high resolution x-ray spectroscopy
Andreas Fleischmann1 , Christian Enss2 , Loredana Gastaldo3 , Jeschua Geist4 , Daniel Hengstler5 , Sebastian Kempf6 ,Mattheaus Krantz7 , Christian Schoetz8 , Tobias Gassner9 , Marc Oliver Herdrich10 , Renate Maertin11 , Thomas
Stoehlker12 , Guenter Weber13
1

Kirchhoﬀ Institute for Physics, Heidelberg University, 2 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120
Heidelberg, Germany , 3 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany ,4
Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 5 Kirchhoﬀ Institute for Physics,
Heidelberg University, INF 227, 69120 Heidelberg, Germany , 6 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227,
69120 Heidelberg, Germany , 7 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany ,8
Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 9 Helmholtz-Institute Jena,
Froebelstieg 3, 07743 Jena, Germany , 10 Helmholtz-Institute Jena, Froebelstieg 3, 07743 Jena, Germany ,11Helmholtz-Institute Jena, Froebelstieg 3, 07743 Jena, Germany , 12 Helmholtz-Institute Jena, Froebelstieg 3, 07743 Jena,
Germany , 13 Helmholtz-Institute Jena, Froebelstieg 3, 07743 Jena, Germany

The study of x-ray transition energies of highly charged ions allows for high precision tests of quantum electrodynamics(QED) in the presence of very strong electric and magnetic fields. These high precision measurements would greatly
benefit from x-ray detectors characterized by high energy resolution, large dynamic range as well as high quantum
eﬃciency over a large energy range to study precise positions and branching ratios of several atomic transitions. Low
temperature metallic magnetic calorimeters (MMCs) are energy dispersive particle detectors, operated at temperatures
below 50 mK, which fulfill all these requirements. MMCs use a paramagnetic temperature sensor to convert thetemperature upon the absorption of a single x-ray photon into a change of magnetic flux in a SQUID.
We have developed a mobile and flexible platform to operate MMCs arrays in order to perform experiments at
diﬀerent facilities as the Experimental Storage Ring at GSI-Darmstadt or EBITs as the one at Max-Planck Institutefor Nuclear Physics in Heidelberg. This system is based on a dry dilution refrigerator with a 40 cm long copper sidearm, as extension of the mixing chamber experimental plate, suitable to locate the detectors as close as possible tothe x-ray sources. The front of this long arm is equipped with an experimental platform which can host one 64-pixel
array with the corresponding 8 SQUID chips, each carrying four front-end SQUIDs whose input coils are coupled to
the 64 MMCs. The SQUIDs for the amplification of the front-end SQUIDs signals are located along the arm. This
platform design was optimized for the use of the 2d array of the series maXs. The maXs design is flexible to be
applied for detectors optimized for x-ray energies up to 20/30/200 keV, defining the name of the single designs to bemaXs-20/30/200. Each array consists of 64 absorbers positioned in a square of 8*8 pixels covering a surface of 2*2
mm2 / 4*4 mm2 /8*8 mm2 for maXs-20/30/200 respectively with a filling factor for the detection area of >90%. In
this talk the challenges of the fabrication of the maXs arrays will be discussed and the performance achieved by thesearrays will be presented.
A new large array covering 1 cm2 has been developed to study the polarization of photon emitted in heavy ionsatomic transitions which is suitable to be readout using a similar platform as for the maXs arrays. This detector
chip features a 6x6 mm2 large hole, in correspondence of the position of the Reyleigh scatterer consisting of a 20 µm
thick copper foil, positioned in the center of silicon chip of about 1.7 cm2 and surrounded by 64 pixels read out by 32
two-stage dc-SQUIDs. A first prototype of this design has been recently fabricated and preliminary tests are on-going.
In this talk the design concept as well as the results from the first characterizations will be discussed.
Results obtained in proof of concept experiments will be discussed and an overview of the planned high precision
measurements will be given.
category : Applications

123

Poster presentations

124

Category A : Sensor Physics &Developments

125PA-1 Development of Thermal Kinetic Inductance Detectors suitable for X-ray
spectroscopy
Andrea Giachero1 , Angelo Cruciani2 , Antonello D’Addabbo3 , Peter K. Day4 , Sergio Di Domizio5 , Marco Faverzani6 ,Elena Ferri7 , Benno Margesin8 , Maria Martinez9 , Renato Mezzena10 , Lorenzo Minutolo11 , Angelo Nucciotti12 ,Andrei Puiu13 , Marco Vignati14
1

INFN and University of Milano Bicocca, Department of Physics, 2 INFN - Sezione di Roma1, Roma, Italy , 3 INFN Laboratori Nazionali del Gran Sasso (LNGS), Assergi (AQ), Italy , 4 Jet Propulsion Laboratory, Pasadena, CA, U.S.A. ,5
Dipartimento di Fisica - Universita degli Studi di Genova, Genova, Italy / INFN - Sezione di Genova, Genova, Italy , 6 INFN
- Sezione di Milano-Bicocca, Milano, Italy / Universita di Milano-Bicocca, Milano, Italy , 7 INFN - Sezione di Milano-Bicocca,
Milano, Italy , 8 Fondazione Bruno Kessler (FBK), Trento, Italy / INFN - Trento Institute for Fundamental Physics andApplications (TIPFA), Trento, Italy , 9 INFN - Sezione di Roma1, Roma, Italy / Dipartimento di Fisica - Sapienza Universita
di Roma, Roma, Italy, , 10 INFN - Trento Institute for Fundamental Physics and Applications (TIPFA), Trento, Italy /Dipartimento di Fisica, Univerista di Trento, Povo, Trento, Italy , 11 INFN - Sezione di Roma1, Roma, Italy / Dipartimento di
Fisica - Sapienza Universita di Roma, Roma, Italy, , 12 INFN - Sezione di Milano-Bicocca, Milano, Italy / Universita di
Milano-Bicocca, Milano, Italy , 13 INFN - Sezione di Milano-Bicocca, Milano, Italy / Universita di Milano-Bicocca, Milano,
Italy , 14 INFN - Sezione di Roma1, Roma, Italy

We report on the development of Thermal Kinetic Inductance Detectors (TKIDs) suitable to perform X-ray spectroscopy measurements. The aim is to implement MKIDs sensors working in thermal quasi-equilibrium mode to
detect X-ray photons as pure calorimeters. The thermal mode is a variation on the MKID classical way of operationthat has generated interest in recent years. TKIDs can oﬀer the MKIDs inherent multiplexibility in the frequency
domain, a high spatial resolution comparable with CCDs, and an energy resolution theoretically limited only bythermodynamic fluctuations across the thermal weak links.
Microresonators are built in Ti/TiN multilayer technology with the inductive part thermally coupled with a metal
absorber on a suspended SiN membrane, to avoid escape of phonons from the film to the substrate. The mid-term goal
is to optimize the single pixel design in term of superconducting critical temperatures, internal quality factors, kinetic
inductance and spectral energy resolution. The final goal is to realize a demonstrator array for a next generation
thousand pixels X-ray spectrometer.
In this contribution, the status of the project after one year of developments is reported, with detailed reference tothe microresonators design and simulations, to the fabrication process, and to the obtained preliminary characterization
results.
category : Sensor Physics & Developments

126

PA-2 Fabrication of antenna-coupled KID array for Cosmic Microwave Backgrounddetection
Qing Yang Tang1 , Peter S. Barry2 , Vasish Baungally3 , Amy Lowitz4 , Ryan McGeehan5 , Evan Mayer6 , Rong Nie7 ,Ritoban Basu Thakur8 , Erik Shirokoﬀ9
1

Department of Astronomy & Astrophysics, University of Chicago, 2 Kavli Institute of Cosmological Physics, University of
Chicago , 3 Kavli Institute of Cosmological Physics, University of Chicago , 4 Kavli Institute of Cosmological Physics,
University of Chicago , 5 Kavli Institute of Cosmological Physics, University of Chicago / Department of Physics, University of
Chicago , 6 Kavli Institute of Cosmological Physics, University of Chicago , 7 Department of Astronomy and Astrophysics,
University of Chicago , 8 Kavli Institute of Cosmological Physics, University of Chicago , 9 Department of Astronomy andAstrophysics, University of Chicago / Kavli Institute of Cosmological Physics, University of Chicago

Microwave Kinetic Inductance Detectors (MKIDs) have become an attractive alternative to traditional Transition
Edge Sensor (TES) bolometers in the sub-mm and mm observing community due to its innate frequency multiplexing
capabilities and simple lithographic processes. These advantages make MKIDs a viable option for the O(100,000)
detectors needed for the upcoming Cosmic Microwave Background - Stage 4 (CMB-S4) experiment. We have fabricateddual polarization antenna-coupled MKID array in the 100GHz band optimized for CMB detection. The Al KIDs
are made from evaporating Al on a high resistivity silicon substrate. The microstrip coupling the antenna and KID
consists of growing Si3N4 between two layers of evaporated Nb. We present details of the fabrication process as well
as a preliminary characterization of these devices with a cryogenic blackbody load.
category : Sensor Physics & Developments

127

PA-3 A dual polarization, 1.4 to 2.8 THz Kinetic Inductance Detector, withbackground limited sensitivity for future spaced-based far-infrared observatories
Juan Bueno1 , Ozan Yurduseven2 , Nuria Llombart3 , Stephen J. C. Yates4 , Vignesh Murugesan5 , Lorenza Ferrari6 ,David J. Thoen7 , Andrey M. Baryshev8 , Andrea Neto9 , Jochem J. A. Baselmans10
1

SRON, 2 Terahertz Sensing Group, Delft University of Technology , 3 Terahertz Sensing Group, Delft University of Technology, 4 SRON? Netherlands Institute for Space Research, Groningen , 5 SRON ? Netherlands Institute for Space Research, Utrecht ,6
SRON? Netherlands Institute for Space Research, Groningen , 7 Terahertz Sensing Group, Delft University of Technology ,8
SRON? Netherlands Institute for Space Research, Groningen / Kapteyn Astronomical Institute, University of Groningen ,9Terahertz Sensing Group, Delft University of Technology , 10 SRON ? Netherlands Institute for Space Research, Utrecht /Terahertz Sensing Group, Delft University of Technology

Future space based observatories for the far infrared, such as SPICA and the far infrared surveyor, will use actively
cooled optics to reach the background flux of the universe. An imaging spectrometer for such an observatory requires
large detector arrays that combine high optical eﬃciency, broad band and dual polarization radiation coupling at THz
frequencies. We have developed a kinetic inductance detector (KID) coupled to a leaky lens antenna operating at alarge bandwidth of 1.4 - 2.8 THz to fulfill these requirements. The device shows photon noise limited performanceboth in the phase and amplitude readout simultaneously, with a noise-equivalent power below 3x10−19 W/Hz1/2 andgood agreement between the measured and expected optical eﬃciency. The beam pattern and frequency response of
the device are also measured, showing a good match with the simulations. The figure shows the dual polarisation leaky
lens antenna coupled KID: A) Back and front illuminated optical image of a small detector array; B) Optical imageof a single pixel. The bright square indicates the area of the membrane, where illumination from the chip backsidebrightens the image. The NbTiN section of the KID and the transmission line are fabricated on the solid substrate;C) SEM image of the centre of the antenna where the narrow Al line (1.2 – 0.8 – 1.2 µ m) can be resolved.

category : Sensor Physics & Developments

128PA-4 Study on the electronic properties of Al thin-film superconducting resonators at
low temperatures
Takashi Noguchi1 , Agnes Dominjon2 , Yutaro Sekimoto3
1

Advanced Technology Center, National Astronomical Observatory, 2 National Astronomical Observatory of Japan , 3 National
Astronomical Observatory of Japan

We have been studying the influence of quasiparticles in the electronic states broadened into the superconducting gap
to the response of a superconducting resonator, which is a key element of the microwave kinetic inductance detector(MKID). We have derived the analytic expressions of the Mattis-Bardeen equations, which are valid for the complex
conductivity, σs = σ1 + iσ2 at both the microwave frequency (hf << 2∆1 ) and low temperature (kB T << 2∆1 ), usingwith a gap parameter which has a small imaginary part, i.e. ∆ = ∆1 + i∆2 , where ∆2 /∆1 << 1. We found that the σ1
is dominated by the contribution of quasiparticles in the broadened states in the gap and shows saturation in decrease
with decreasing temperature at low temperature. It was predicted that the conductivity quality factor defined by
Qs = σ2 /σ1 saturates in increase with decreasing temperature at low temperature and reaches asymptotically ∆1 /∆2
at T = 0, since σ2 does not strongly depend either on temperature or on the magnitude of ∆2 .
To verify the validity of the above-mentioned hypothesis, we prepared two types of Al thin-film superconducting
resonators; one is made by dc magnetron sputtering and the other is made by thermal evaporation, and then thequality factor, Qi , and resonance frequency, fr , were measured in detail as function of temperature. The temperaturedependence of the Qi and fr of the Al thin-film resonator made by thermal evaporation were very similar to those
ever reported and well fitted by the analytic expressions of Mattis-Bardeen equations with the α and ∆ as adjustableparameters, where α is a ratio of kinetic inductance to total inductance of the resonator.
On the other hand, it was found that Qi of Al thin-film resonator made by sputtering reaches a peak and thendecreases when the temperature is lowered at well below Tc , although its fr is very similar to those observed in thethermally evaporated Al thin-film resonators. From the plot of 1/Qi as a function of temperature, it was found that
1/Qi increases in proportion to − log(T ) as the temperature goes down below the temperature where Qi reaches thepeak. Since it is supposed that 1/Qi ≈ α(Rres /ωr L), where Rres and L are a residual resistance and inductance ofthe resonator at low temperature, respectively, and ωr = 2πfr , it is indicated that the Rres has a log(T )-temperaturedependence, suggesting of the Kondo eﬀect.
According to the results above mentioned, we confirmed that the electronic properties of the Al resonators at thetemperature far below Tc are governed by residual quasiparticles occupying the broadened quasiparticle states at thebottom of the superconducting energy gap, not by the two level systems (TLS).
category : Sensor Physics & Developments

129

5

× 10

-4

× 10

3.943 GHz

0.0

1.0

αγ = 0.122-5
δ = 7.10x104.480 GHzQr

-0.5

αγ = 0.142-4
δ = 1.14x10

0.6

-1.0

αγ = 0.131-4
δ = 3.88x10
αγ = 0.125-4δ = 9.10x10

0.4

δ fr /fr

0.8

-1.5

Tc = 1.25 K( Δ1=0.190 meV)4.579 GHz

-2.0

0.2

3.525 GHz
0
0.05

0.1

0.15

0.2

0.25

Temperature T (K)0.3

0.35 0.05

0.1

0.15

0.2

0.25

Temperature T (K)

0.3

0.35

-2.5

(a)
10.0

5

× 10

3.370 GHz3.399 GHz
3.408 GHz

Quaity factor Qi

2.0

3.399 GHz
3.408 GHz
3.370 GHz

-6

× 10

} Fitted

1/Qi

8.0

1.0

6.0

Al film (Sputtered)
0.0

4.0
0.1

0.2

Temperature (K)0.3

Al film (Sputtered)
0.08

0.1

0.12
0.15
Temperature (K)

0.2

(b)
(a) Quality factor and fractional frequency change of the e-beam deposited
Al thin-film resonator as a function of temperature(b) Intrinsic quality factor and inverse of the intrinsic quality factor of
the sputtered Al thin-film resonator as a function of temperature

130PA-5 Dual-polarization LEKIDs for CMB Polarimetry
Heather McCarrick1 , Maximilian H. Abitbol2 , Peter A.R. Ade3 , Sean Bryan4 , Peter Day5 , Thomas
Essinger-Hileman6 , Daniel Flanigan7 , Glenn Jones8 , Henry G. Leduc9 , Michele Limon10 , Bradley R. Johnson11 ,Philip Mauskopf12 , Amber Miller13 , Suzanne Staggs14 , Carole Tucker15
1

Department of Physics, Columbia University, 2 Columbia University, New York, NY 10027, USA , 3 Cardiﬀ University, Cardiﬀ,
Wales, CF24 3AA, UK , 4 Arizona State University, Tempe, AZ 85287, USA , 5 Jet Propulsion Laboratory, Pasadena, CA
91109, USA , 6 Goddard Space Flight Center, Greenbelt, MD 20771, USA , 7 Columbia University, New York, NY 10027, USA ,8
Columbia University, New York, NY 10027, USA , 9 Jet Propulsion Laboratory, Pasadena, CA 91109, USA , 10 Columbia
University, New York, NY 10027, USA , 11 Columbia University, New York, NY 10027, USA , 12 Arizona State University,
Tempe, AZ 85287, USA , 13 University of Southern California, Los Angeles, CA 90089, USA , 14 Princeton University,
Princeton, NJ 08544, USA , 15 Cardiﬀ University, Cardiﬀ, Wales, CF24 3AA, UK

We report on the development of dual-polarization, lumped-element kinetic inductance detectors (LEKIDs) optimized
for cosmic microwave background (CMB) polarization studies. We have designed, fabricated, and tested 64-element
modules where each element contains a profiled horn and two resonators sensitive to orthogonal polarizations. Therefore, there are 128 single-polarization detectors per module. The front-illuminated devices are fabricated on 160 µm
thick silicon wafers, which are diced into square arrays and mounted inside the aluminum modules containing the horn
arrays. The thickness of the wafer sets the distance to the backshort, which is used to optimize millimeter-wave radiation absorption. We will present the constraints and motivations behind the detector design and array architecture,and discuss solutions to problems encountered, such as methods for reducing the cross-polarization response and mitigating the eﬀect of mechanical vibrations. We will present measured results from these arrays including responsivity,
noise, and polarization selectivity. Finally, we will outline our work towards integrating a LEKID array comprised offour dual-polarization LEKID modules into the Atacama B-mode Search (ABS) instrument. This ABS project willallow us to demonstrate LEKIDs in a CMB polarimeter with on-sky measurements and test a multiplexing factor of
512.
category : Sensor Physics & Developments131PA-6 CALDER: Phonon-mediated Kinetic Inductance light detectors
Marco Vignati1 , Fabio Bellini2 , Martino Calvo3 , Laura Cardani4 , Nicola Casali5 , Maria Gabriella Castellano6 , Ivan
Colantoni7 , Carlo Cosmelli8 , Angelo Cruciani9 , Antonio D’Addabbo10 , Sergio Di Domizio11 , Johannes Goupy12 ,Helene Le Sueur13 , Maria Martinez14 , Lorenzo Minutolo15 , Alessandro Monfardini16
1

INFN Sezione di Roma, 2 INFN Sezione di Roma, 00185 Roma, Italy / Dipartimento di Fisica, Sapienza Universita di Roma,
00185 Roma, Italy , 3 Institut Neel, CNRS and Universite Grenoble Alpes, 38042 Grenoble, France , 4 INFN Sezione di Roma,
00185 Roma, Italy , 5 INFN Sezione di Roma, 00185 Roma, Italy , 6 Istituto di Fotonica e Nanotecnologie-CNR, 00156 Roma,
Italy , 7 Istituto di Fotonica e Nanotecnologie-CNR, 00156 Roma, Italy , 8 INFN Sezione di Roma, 00185 Roma, Italy /Dipartimento di Fisica, Sapienza Universita di Roma, 00185 Roma, Italy , 9 INFN Sezione di Roma, 00185 Roma, Italy ,10
INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy , 11 INFN Sezione di Genova and Dipartimento di
Fisica Universita degli Studi di Genova, 16146 Genova, Italy , 12 Institut Neel, CNRS and Universite Grenoble Alpes, 38042
Grenoble, France , 13 Centre de Sciences Nucle ?aires et de Sciences de la Matiere, 91405 Orsay, France , 14 INFN Sezione diRoma, 00185 Roma, Italy / Dipartimento di Fisica, Sapienza Universita di Roma, 00185 Roma, Italy , 15 INFN Sezione diRoma, 00185 Roma, Italy / Dipartimento di Fisica, Sapienza Universita di Roma, 00185 Roma, Italy , 16 Institut Neel, CNRS
and Universite Grenoble Alpes, 38042 Grenoble, France

The development of large area cryogenic light detectors is one of the priorities of next generation bolometric experiments
searching for neutrinoless double beta decay. The simultaneous read-out of the heat and light signals enables particle
identification, provided that the energy resolution and the light collection are suﬃciently high. CALDER (Cryogenic
wide-Area Light Detectors with Excellent Resolution) is developing phonon-mediated silicon light detectors using
KIDs, with the goal of sensing an area of 5x5 cm2 with a resolution of 20 eV RMS. We present the latest results
obtained with aluminum chips and with newly developed multilayer titanium-aluminum chips featuring a remarkablesensitivity.
http://www.roma1.infn.it/exp/caldercategory : Sensor Physics & Developments132

PA-7 Mitigation of cosmic ray eﬀect on Microwave Kinetic Inductance Detectors
Kenichi Karatsu1 , Akira Endo2 , Juan Bueno3 , David J. Thoen4 , Vignesh Murugesan5 , Nozomu Tomita6 , Eduard
F.C. Driessen7 , Gregoire Coiﬀard8 , Jochem J.A. Baselmans9
1

Delft University of Technology, 2 Delft University of Technology , 3 SRON - Netherlands Institute for Space Research , 4 Delft
University of Technology , 5 SRON - Netherlands Institute for Space Research , 6 The University of Tokyo , 7 Institut de Radio
Astronomie Millimetrique (IRAM) , 8 Institut de Radio Astronomie Millimetrique (IRAM) , 9 Delft University of Technology /SRON - Netherlands Institute for Space Research

One of the main issues for space borne observatories is the interaction between radiation detectors and cosmic ray
particles. Approximately 90 % of the cosmic rays in space consist of protons produced by solar activity or other galactic
sources. The energy spectrum of the cosmic rays has a peak at around 200 MeV with quite a broad energy distribution.
Therefore, the cosmic rays can easily penetrate the satellite structure and reach the detectors. The incident particles
interact with the detectors and deposit a fraction of their energy through ionization. The energy deposition in a 350µm Sapphire / Si substrate, which is usually used for the detectors, is simulated to have a peak at around 100-200
keV. The deposited energy causes a cascade of high-energy phonons that spread inside of the detectors, trigger thedetectors response, and create glitches in the data stream. These glitches lead to dead time of the detectors duringobservation.
We investigate possible solutions to mitigate the dead time caused by cosmic ray events for Microwave Kinetic
Inductance Detector (MKID) arrays. We prepared 4 types of Al-NbTiN hybrid MKID arrays: 1), 2) Arrays with acapacitive mesh of TiN on backside (Tc = 3.2 K and 0.8-1.2 K, respectively); 3) Array with SiN membrane structureand no backside TiN mesh layer; and 4) Reference array without any back side layer or membrane structure. All
arrays are made on a 55 mm x 55 mm x 350 µm chip and consist of 961 MKIDs. For arrays type 1 and 2, the idea isthat high-energy of phonons are down-converted eﬃciently in the TiN layer to phonon energies below the gap energyof aluminium, which makes them impossible to be detected by the MKIDs. For type 3, the aluminium of the MKID
is on top of SiN membranes and physically isolated from the substrate.
We measured cosmic ray events with those arrays in the laboratory, where cosmic rays consist mainly of muons.
Cosmic ray events were extracted from 30 minutes of data by a 2-step iterative procedure based upon the second
derivative of the time ordered data of the phase response of MKIDs. As a result, the array dead time caused by cosmic
rays was reduced to 80 %, 20 %, and 3 % of the dead time with respect to the reference array (4) for type 1, 2 and3, respectively. We estimated the dead time fraction of the MKIDs arrays when operating them in an L2 or similar
far-Earth orbit by simply scaling cosmic ray event rates on the arrays to the measured rate of 5 /s/cm2 by Plancksatellite at L2 orbit: they are 13 %, 4 % and 0.5 % for type 1, 2, and 3, respectively.
category : Sensor Physics & Developments133

PA-8 Development of an MKIDs-Based THz Superconducting Imaging Array(TeSIA) at 0.85 THz
Sheng-Cai SHI1 , Jing Li2 , Zhen-Hui Lin3 , Jin-Ping Yang4 , Dong Liu5 , Wen-Ying Duan6 , Zheng Lou7 , Qing Shi8 , Zhi
Li9 , Wei Miao10 , Wen Zhang11 , Qi-Jun Yao12
1

Purple Mountain Observatory, CAS, 2 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 3 Purple
Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 4 Purple Mountain Observatory, CAS / Key Lab of Radio
Astronomy, CAS , 5 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 6 Purple Mountain
Observatory, CAS / Key Lab of Radio Astronomy, CAS , 7 Purple Mountain Observatory, CAS / Key Lab of Radio
Astronomy, CAS , 8 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS / Shanghai Normal University ,9
Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS / University of Science and Technology of China ,10
Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 11 Purple Mountain Observatory, CAS / Key Lab
of Radio Astronomy, CAS , 12 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS

Dome A, the highest point of the cold and dry Antarctic ice sheet, oﬀers the best access to atmospheric windows
at THz/FIR wavelengths on Earth. China is planning to build a 5-m THz telescope (DATE5) at Dome A. To fulfill
the DATE5 s scientific objectives, we are developing a THz superconducting imaging array (TeSIA). The TeSIA,
based on Aluminum MKIDs, will be operating at 0.85 THz (350-micron window) with a pixel number of 32 × 32 andback-ground limited sensitivity (NEP) of 10-16W/Hz0.5. Detailed system design and performance of TeSIA will bepresented.
category : Sensor Physics & Developments134

PA-9 Titanium nitride for kinetic-inductance detectors: a problematic material or anengineering opportunity?
Eduard F.C. Driessen1
1Institut de Radioastronomie Millimetrique (IRAM)

Titanium nitride and related materials with a large normal-state resistivity have been proposed and used for kinetic
inductance detectors at various wavelengths from near-IR to millimeter. The expected advantages of these materials
are manifold, e.g. a tunable critical temperature, a large kinetic inductance fraction, and better matching to theincident radiation due to the large resistivity. However, whereas even large (2 diameter) telescope-ready detector
arrays have come into sight, the detailed behavior of TiN detectors still shows many puzzling features, at odds withthe perfectly understood behavior of conventional aluminum KIDs.
In this contribution I will give an overview of the diﬀerent studies that have been performed on TiN resonators.
In this overview, I will emphasize the unconventional behavior of the material, and the diﬀerences with aluminum.
Among these diﬀerences are a smooth detection gap edge, an increasing sensitivity with optical power, and a quality
factor that does not change with loading. I will argue that these diﬀerences are unavoidably linked to the large
normal-state resistivity of the material and its accompanying intrinsic electronic inhomogeneity, and that they should
be fully taken into account when considering this material for detectors.
Finally, I will discuss the status of TiN for use in (sub)-mm instruments and I will argue that some of the observed
unconventional behavior might in fact prove an engineering opportunity for ground-based observation.
category : Sensor Physics & Developments

135

PA-10 Update on TKIDs: Thermal Kinetic Inductance Detectors for X-ray imaging
spectroscopy
Gerhard Ulbricht1 , Miguel Daal2 , Paul Szypryt3 , Alex B. Walter4 , Clint Bockstiegel5 , Benjamin A, Mazin6
1School of Cosmic Physics, Dublin Institute of Advanced Studies, 2 Department of Physics, University of California, Santa
Barbara CA 93106, USA , 3 Department of Physics, University of California, Santa Barbara CA 93106, USA , 4 Department of
Physics, University of California, Santa Barbara CA 93106, USA , 5 Department of Physics, University of California, Santa
Barbara CA 93106, USA , 6 Department of Physics, University of California, Santa Barbara CA 93106, USA

Thermal Kinetic Inductance Detectors (TKIDs) are MKIDs that operate as microcalorimeters by suspending theirinductor and a separate photon or particle absorber on a freestanding Si3N4 membrane. They allow the kinetic
inductance detector principle to be extended to detect and characterize X-rays and higher energies while retaining theunique multiplexibility MKIDs oﬀer, promising the potential to scale up to kilo- or even mega-pixel detector arrays.
We will present our recent progress with improving and optimizing our TKID prototype design and characteristics.
We investigated both sub-stoichiometric TiNx and co-sputtered WSix for TKIDs and will compare their respective
advantages and disadvantages in respect to detector performance and fabrication. We will also discuss our firstexperiments varying the TKID readout frequency in order to utilize smallest possible heat capacities to allow tofurther increase energy resolution in tighter energy bands.
category : Sensor Physics & Developments136PA-11 Projection of Cosmic Microwave Background anisotropy measurements for
Microwave Kinetic Inductance Devices
Ritoban Basu Thakur1
1

Kavli Institute for Cosmological Physics, University of Chicago

The Stage 4 Cosmic Microwave Background (CMB-S4) collaboration will bring together tens of telescopes, each with
1E5 low-temperature low-noise detectors, to measure the CMB with sub-nK sensitivity across decades of angular scales(1E-1 to 1E2 degrees). These measurements will enable deriving extremely precise constraints on the matter-energy
budget and dynamics of the universe, and probe several interesting early universe inflationary theories. Microwave
Kinetic Inductance Devices (MKIDs) are poised to allow for massively and natively multiplexed detectors arrays,
improving the current multiplexing factor by over an order of magnitude, thus enabling for 1E5 detectors required
for CMB-S4. In this proceeding we forecast what the status of the present generation of MKIDs implies for CMB
measurements. We use various MKID noise spectra and simulate a telescope scan strategy which projects the detector
noise onto the CMB sky. We then analyze the simulated CMB + MKID noise to understand how MKID properties,
such as responsivity, low frequency and white noise levels, aﬀect the various features of the CMB, such as the acoustic
peaks and the damping tail. Based on this we develop a framework connecting the MKID characteristics with scanstrategies, to the type of CMB signals we may probe with such detectors.
category : Sensor Physics & Developments137PA-12 AlMn LEKIDs for millimeter-wave astronomy below 100 GHz
Hsiao-Mei Cho1 , Glenn Jones2 , Max H. Abitbol3 , Peter A. R. Ade4 , Sean Bryan5 , Peter Day6 , Daniel Flanigan7 ,Kent D. Irwin8 , Bradley R. Johnson9 , Dale Li10 , Philip Mauskopf 11 , Heather McCarrick 12 , Amber Miller13 , Yanru
Song14 , Carole Tucker15
1

SLAC national accelerator laboratory , 2 Department of Physics, Columbia University, New York, NY 10027, USA ,Department of Physics, Columbia University, New York, NY 10027, USA , 4 School of Physics and Astronomy, Cardiﬀ
University, Cardiﬀ, Wales CF24 3AA, UK , 5 School of Earth and Space Exploration, Arizona State University, Tempe, AZ
85287, USA , 6 NASA, Jet Propulsion Laboratory, Pasadena, CA 91109, USA , 7 Department of Physics, Columbia University,
New York, NY 10027, USA , 8 SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA / Department of Physics,
Stanford University, Stanford, CA, 94305-4085, USA , 9 Department of Physics, Columbia University, New York, NY 10027,
USA , 10 SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA , 11 School of Earth and Space Exploration,
Arizona State University, Tempe, AZ 85287, USA , 12 Department of Physics, Columbia University, New York, NY 10027, USA, 13 Department of Physics and Astronomy, University of Southern California, Los Angeles, CA 90089, USA , 14 Department of
Physics, Stanford University, Stanford, CA, 94305-4085, USA , 15 School of Physics and Astronomy, Cardiﬀ University, Cardiﬀ,
Wales CF24 3AA, UK
3

We report the development of manganese-doped aluminum lumped-element MKIDs (LEKIDs) with high internal quality factor, high uniformity, and tunable critical temperature for millimeter-wave astronomy below the gap of aluminum.
Manganese-doped aluminum (Al-Mn) has a critical temperature that can be tuned by varying the manganese concentration. It is an attractive material for MKIDs if the internal quality factor remains suﬃciently high. Manganese loses
its magnetic character in lightly doped Al-Mn, and the resulting films have been shown to retain a relatively sharp
density of states, with only a small broadening of the superconducting gap, as expected for non-magnetic impurities.
We have fabricated and tested a prototype eight-element array of Al-Mn LEKIDs. The manganese concentration of
900 ppm results in a measured critical temperature of 694 mK. We measure a quasiparticle lifetime of 60 microseconds
using light pulses from a 1550 nm light-emitting diode. The internal quality factor of this prototype array is greaterthan 2 × 105 , which is high enough for millimeter-wave astrophysical observations. We also measure deviations of
microwave surface impedance from the Mattis-Bardeen theory, suggesting that a small smearing of the gap needs tobe taken into account in the theory.
category : Sensor Physics & Developments138PA-13 Antenna-coupled lumped-element kinetic inductance detectors for CMB
observations
Erik Shirokoﬀ1 , Peter S. Barry2 , Evan Mayer3 , Amy Qing Yang Tang4 , Simon Doyle5
1

Department of Astronomy & Astrophysics, University of Chicago, 2 University of Chicago , 3 University of Chicago ,4
University of Chicago , 5 Cardiﬀ University

Focal plane arrays consisting of low-noise, polarization-sensitive detectors have made possible the pioneering advancesin the study of the cosmic microwave background (CMB), and have provided exquisite constraints on the origin,content and evolution of the Universe. To make further advances, the next generation of CMB experiments will
require a substantial increase in the number of detectors compared to current instruments. Arrays of kinetic inductancedetectors (KIDs) provide a possible path to realizing such large format arrays owing to their inherent multiplexing
advantage and relative simplicity. In this proceedings, we report on the design and performance of a novel variant of
the traditional KID design; the antenna-coupled lumped-element KID. This design employs a polarization-sensitive
twin-slot antenna behind an anti-reflection coated hemispherical alumina lens, and incident power couples into a
niobium microstrip line that guides the power into the inductive section of an aluminum KID. The optical signal
then breaks Cooper pairs in the Al inductor, and modifies the resonant frequency and quality factor of the KID. We
will present preliminary results from dark and optical characterization of a small seven-element prototype array andcompare to the expected modeled performance, and discuss ongoing progress toward a field-ready kilo-pixel array.
category : Sensor Physics & Developments

139PA-14 Coherent excited states in superconductors due to a microwave field microscopic perspective on microwave nonlinearity
A.V. Semenov1 , I.A. Devyatov2 , P.J. de Visser3 , T.M. Klapwijk4
1

SRON, Netherlands Institute for Space Research, 2 Moscow Institute of Physics and Technology, Dolgoprudny, Moscow
141700, Russia / Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics, 1(2), Leninskie gory, GSP-1,
Moscow 119991, Russia , 3 Kavli Institute of NanoScience, Faculty of Applied Sciences, Delft University of Technology,
Lorentzweg 1, 2628 CJ Delft, The Netherlands / SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA
Utrecht, The Netherlands , 4 Moscow State Pedagogical University, 1 Malaya Pirogovskaya Street, Moscow 119992, Russia /Kavli Institute of NanoScience, Faculty of Applied Sciences, Delft University of Technology, Lorentzweg 1, 2628 CJ Delft, The
Netherlands

How is the superconducting state modified by a current, i.e., when the condensate is moving? Working with superconductors in strong microwave fields (MKIDs, parametric amplifiers), we often ask ourselves this question, either explicit
or unknowingly.
The answer is well known for the case of a dc current flowing in a superconducting wire. For a dc current, theCooper pairs gain a finite momentum, which leads to the suppression of the superconducting properties of the wire.
The superconducting order parameter |∆| is reduced and the sharp BCS singularity near the gap is smeared. This eﬀect
leads to the well-known I 2 nonlinearity of the inductance. For microwave frequencies, the dc-derived I 2 nonlinearity
is usually assumed, which is a reasonable approximation for some practical cases. However it does not address what
happens on a microscopic level to the superconductor when exposed to a microwave field, which is, in contrast to adc field, quantised by the microwave photon energy.
We describe theoretically the depairing eﬀect of a microwave field with frequency ω0 on diﬀusive s-wave superconductors [1]. In contrast to dc depairing, the density of states acquires, steps at multiples of the photon energy∆ ± nh̄ω0 . Fig. a compares the density of states as a function of energy (E) for dc and rf fields. Fig. b shows thedensity of states for diﬀerent field strengths and microwave energies. On top of that, the density of states shows an
exponential-like tail in the subgap regime (clearly seen on log-scale in Fig. c). We show that this ac depairing explains
the measured frequency shift of an aluminium superconducting resonator with microwave power at low temperatures[2].
For MKIDs this shows that not only the distribution function of the resonator is aﬀected by the microwave field[2], but also the density of states changes, which becomes apparent especially at low temperatures. The exponential
tail in the density of states provides a clue what triggers the microwave absorption (leading to excess quasiparticles)
at low temperatures. For parametric amplifiers this work does not only give a rigorous basis for understanding thenonlinearity, but may also lead to new functionality or exotic phenomena due to the acquired steps in the density ofstates of the superconductor.
[1] A. V. Semenov, I. A. Devyatov, P. J. de Visser, and T. M. Klapwijk, Phys. Rev. Lett. 117, 047002 (2016)[2] P. J. de Visser, D. J. Goldie, P. Diener, S. Withington, J. J. A. Baselmans, and T. M. Klapwijk, Phys. Rev.
Lett. 112, 047004 (2014)
category : Sensor Physics & Developments

140

141

PA-15 Operation of a superconducting nanowire in two detection modes: KID andSPD
Edward Schroeder1 , Philip Mauskopf2 , Hamdi Mani3 , Karl Berggren4 , Di Zhu5
1

Department of Physics, Arizona State University, 2 Arizona State University, Department of Physics, Tempe, AZ, UnitedStates / Arizona State University, School of Earth and Space Exploration, Tempe, AZ, United States , 3 Arizona State
University, School of Earth and Space Exploration, Tempe, AZ, United States , 4 Massachusetts Institute of Technology,
Department of Electrical Engineering and Computer Science, Cambridge, MA, United States , 5 Massachusetts Institute ofTechnology, Department of Electrical Engineering and Computer Science, Cambridge, MA, United States

We present the characterization of a superconducting nanowire that can be operated in two detection modes: i)
as a kinetic inductance detector (KID) or ii) as a single-photon detector (SPD). Two superconducting nanowires
developed for use as single-photon detectors (SNSPDs) are embedded as the inductive (L) component in resonant
inductor/capacitor (LC) circuits coupled to a microwave transmission line. The capacitors are low loss commercial
chip capacitors and limit the internal quality factor of the resonators to approximately Qi = 200. The resonator quality
factor, Qr ≃ 25 is dominated by the coupling to the feed line and limits the detection bandwidth to on the order of 1
MHz. When operated in KID mode, the detectors are AC biased with tones at their resonant frequencies of 46 and 93
MHz. In this mode, a single photon produces a hot spot that does not turn an entire section of the line normal but only
increases the kinetic inductance. The optical response of this detector, or superconducting nanowire resonator (SNR),in linear-mode to 1.3 µm photons is characterized by a noise equivalent power (NEP) of approximately 10−14 W/rtHzat an operating temperature of 2.8 K. At low optical loading levels, the noise is dominated by the cryogenic low noise
amplifier (LNA) with a noise temperature of 4 K. The noise was characterized with a homodyne system by recording
the tone and transmitted signals on an oscilloscope and mixing the results in software. When operated as an SPD in
Geiger-mode, the resonators are DC biased through cryogenic bias tees and each photon produces a sharp voltage step
followed by a ringdown signal at the resonant frequency of the detector which is converted to a standard pulse withan envelop detector. The internal quantum eﬃciency (IQE) in Geiger mode is obtained by determining the numberof photons that are counted for a given LED current bias at a given device current bias and comparing that with theabsorbed power estimated from the frequency shift and the excess photon noise in linear-mode.
category : Sensor Physics & Developments142PA-16 A Superconducting Phase Shifter and On-Chip Fourier Transform
Spectrometer for W-Band Astronomy
George Che1 , Samuel Gordon2 , Philip Mauskopf3 , Harshad Surdi4 , Georgios Trichopoulos5
1

School of Earth & Space Exploration, Arizona State University, 2 Arizona State University , 3 Arizona State University ,4
Arizona State University , 5 Arizona State University

Accessible from the ground, W-Band (75-110 GHz) contains a plethora of information about star formation, galaxy
evolution, and the cosmic microwave background. We present the design, fabrication, and characterization of adual purpose superconducting microstrip circuit that facilitates the next generation of high sensitivity astronomical
observations in this regime. Signal amplification is a universal need for all astronomical instruments. In phaseshifter mode, our device provides the means to measure the relative phase shift between two signals propagating
down two identical NbTiN microstrip lines subject to diﬀerent DC bias. Measurement of the current-dependent nonlinear phase shift due to non-linear kinetic inductance provides the upper limit to the achievable gain of a NbTiN
kinetic inductance parametric amplifier (KIP). Compared to current transistor-based low noise amplifiers, KIPs provide
significant improvements in bandwidth, dynamic range, and noise performance. Applying this new amplifier technology
would greatly increase both the scanning eﬃciency and sensitivity of W-Band receivers. In addition, our device canalso operate as an on-chip Fourier Transform Spectrometer (FTS) that provides continuous phase shift and parametricgain.
To deliver W-Band signals into our cryogenic testbed for circuit characterization, we have developed a custom
high frequency waveguide feedthrough which minimizes conductive heat load on the cooling system, delivers suﬃcientsignal power to our device under test, and avoids stray light issues that complicate free-space propagation solutions.
Our feedthrough is comprised of copper circular waveguide sections, thin Mylar vacuum windows, and conical horn
thermal breaks. Measurements at room temperature indicate electromagnetic losses well within our loss budget of 30
dB. We will integrate this feedthrough into our cryostat and perform full system calibration at 4 K before using it tocharacterize the optical response of our W-Band phase shifter and FTS circuit.
category : Sensor Physics & Developments143PA-17 A broadband antenna for on-chip integrated spectrometers at 300-900 GHz
Sebastian Hahnle1 , Ozan Yurduseven2 , Nuria Llombart3 , Juan Bueno4 , Vignesh Murugesan5 , David Thoen6 , Jochem
Baselmans7
1

SRON Netherlands Institute for Space Research, 2 Delft University of Technology , 3 Delft University of Technology , 4 SRON
Netherlands Institute for Space Research , 5 SRON Netherlands Institute for Space Research , 6 Delft University of Technology, 7 SRON Netherlands Institute for Space Research / Delft University of Technology

The redshift mapping of sub-mm galaxies requires broad band spectrometers. Highly integrated on-chip spectrometers
based on KIDs (Kinetic Inductance Detectors) are a prime candidate for this type of experiment and diﬀerent designs
have been shown to work using narrow band prototypes. One of the challenges in the step from a narrow band toa broad band spectrometer is the eﬃcient coupling of incoming radiation to the detectors over the whole frequency
range.
We designed an antenna based on the leaky-wave principle with a high eﬃciency over a bandwidth of 300 - 900 GHz.
In a spectrometer, the antenna is coupled to a superconducting transmission line (co-planar waveguide or microstrip)
which is connected to an on-chip filterbank. The whole spectrometer is therefore fully integrated on a single chip. We
fabricated a prototype of the antenna and characterized it using a single MKID directly coupled to the Antenna.

category : Sensor Physics & Developments

144

PA-18 Development of the Kinetic Inductance Detector Spectrograph (KIDSpec)
prototype
Sumedh Mahashabde1 , Kieran O’Brien2 , Rupert Dodkins3 , Ghassan Yassin4 , Ian Hepburn5 , Jo Bartlett6 , Graham
Hardy7 , Ben Mazin8
1
3

Astrophysics, Department of Physics, University of Oxford, 2 Astrophysics, Department of Physics, University of Oxford ,Astrophysics, Department of Physics, University of Oxford , 4 Astrophysics, Department of Physics, University of Oxford ,5
Mullard Space Science Laboratory, University College London , 6 Mullard Space Science Laboratory, University College
London , 7 Mullard Space Science Laboratory, University College London , 8 University of California Santa Barbara

KIDSpec is a proposed medium-resolution Visible/NIR spectrograph using an array of Microwave Kinetic Inductance
Detectors (MKIDs). The intrinsic energy resolution of the MKIDs (R 10-20) is used to distinguish photons frommultiple orders to obtain a higher final spectral resolution (R ¿ 1000). We present the design and current build status of
the KIDSpec prototype which will be used to demonstrate the order sorting capabilities of the MKIDs. The detectors
are PtSi devices cooled to ¡100mK using an Adiabatic Demagnetisation Refrigerator. Using a benchtop setup with areflective diﬀraction grating and a broadband light source, we illuminate the MKID pixels with light from multiple
diﬀraction orders. An optical fibre couples the dispersed light to the detectors in the cryostat. The readout is based on
a Reconfigurable Open Architecture Computing Hardware (ROACH) board. We also present numerical simulationsof the spectral reconstruction capability of KIDSpec which has been simulated using Python.
category : Applications

145PA-19 MoBiKID - Kinetic Inductance Detectors for upcoming B-mode satellite
missions
Angelo Cruciani1
1

INFN - Sezione di Roma 1

Our comprehension of the dawn of universe grew incredibly during last years, pointing to the existence of the cosmic
inflation. The primordial B-mode polarization of the Cosmic Microwave Background (CMB) represents a unique probe
to confirm this hypothesis. The detection of such small perturbations of the CMB is a challenge that will be faced in
the near future by a new dedicated satellite mission.
MoBiKID is a new project, funded by INFN, to develop an array of Kinetic Inductance Detectors able to matchthe requirements of a next-generation experiment. The goal of the project is to reach a Noise Equivalent Power better
than 5 aW/Hz0.5 . The detectors will be designed to minimize the background induced by cosmic rays, which could be
the main limit to the sensitivity.
I will present the current status of detectors development and the next planned steps to reach the goal of thisproject.
category : Sensor Physics & Developments

146

PA-20 Electron-phonon coupling in Ti/TiN MKIDs multilayer microresonator
Marco Faverzani1 , Angelo Cruciani2 , Antonio D’Addabbo3 , Sergio Di Domizio4 , Peter Kenneth Day5 , Elena Ferri6 ,Andrea Giachero7 , Benno Margesin8 , Maria Martinez9 , Renato Mezzena10 , Lorenzo Minutolo11 , Angelo Nucciotti12 ,Andrei Puiu13 , Marco Vignati14
1

University and INFN of Milano Bicocca, 2 Dipartimento di Fisica, Universita di Roma ”La Sapienza”, Roma, Italy / Istituto
Nazionale di Fisica Nucleare, Sezione di Roma, Roma, Italy , 3 Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali delGran Sasso, Assergi (AQ), Italy , 4 Dipartimento di Fisica, Universita di Genova, Genova, Italy / Istituto Nazionale di Fisica
Nucleare, Sezione di Genova, Genova, Italy , 5 Jet Propulsion Laboratory, Pasadena, CA, U.S.A. , 6 Istituto Nazionale di Fisica
Nucleare, Sezione di Milano-Bicocca, Milano, Italy , 7 Istituto Nazionale di Fisica Nucleare, Sezione di Milano-Bicocca, Milano,
Italy , 8 Fondazione Bruno Kessler, Trento, Italy , 9 Dipartimento di Fisica, Universita di Roma ”La Sapienza”, Roma, Italy /Istituto Nazionale di Fisica Nucleare, Sezione di Roma, Roma, Italy , 10 Istituto Nazionale di Fisica Nucleare, Trento Institutefor Fundamental Physics and Applications (TIPFA), Trento, Italy / Dipartimento di Fisica, Universita di Trento, Povo (TN),
Italy , 11 Dipartimento di Fisica, Universita di Roma ”La Sapienza”, Roma, Italy / Istituto Nazionale di Fisica Nucleare,
Sezione di Roma, Roma, Italy , 12 Dipartimento di Fisica, Universita di Milano-Bicocca, Milano, Italy / Istituto Nazionale di
Fisica Nucleare, Sezione di Milano-Bicocca, Milano, Italy , 13 Dipartimento di Fisica, Universita di Milano-Bicocca, Milano,
Italy / Istituto Nazionale di Fisica Nucleare, Sezione di Milano-Bicocca, Milano, Italy , 14 Istituto Nazionale di Fisica
Nucleare, Sezione di Roma, Roma, Italy

Over the last few years there has been a growing interest toward the use of superconducting microwave microresonators
operated in quasi-thermal equilibrium mode, especially applied to single particle detection. Indeed, previous devices
designed and tested by our group with X-ray sources in the keV range evidenced
that several issues arise from the attempt of detection through athermal quasiparticles produced within direct
strikes of X-rays in the superconductor material of the resonator.
In order to prevent issues related to quasiparticles self-recombination and to avoid exchange of athermal phonons
with the substrate, our group focused on the development of thermal superconducting microresonators. In thisconfiguration resonators composed of multilayer films of Ti/TiN sense the temperature of an absorbing material. To
maximize the thermal response, low critical temperature films are
preferable. By lowering the critical temperature, though, the maximum probing power bearable by the resonators
decrease abruptly because of the weakening of the electron-phonon coupling. A proper compromise has to be foundin order to avoid signal to noise ratio degradation. In this contribution we report the latest measurement of theelectron-phonon coupling and the latest designs of our thermal devices.
category : Sensor Physics & Developments

147

PA-21 Prototype high angular resolution LEKIDs for NIKA2
Shibo Shu1 , Samuel Leclercq2 , Alessandro Monfardini3 , Eduard Driessen4
1

Institut de Radioastronomie Millimetrique, 2 Institut de RadioAstronomie Millimetrique , 3 Institut Neel, CNRS & Universite
Joseph Fourier , 4 Institut de RadioAstronomie Millimetrique

The resolution of a detector is determined by the size of the eﬀective beam resulting from the convolution of thediﬀraction pattern created by the instrument optics with the pixel transfer function. This resolution is expected
to approach the telescope diﬀraction limited resolution with small pixels. The current 1 mm arrays of the NIKA2
instrument consist of 1140 lumped element kinetic inductance detector (LEKID) pixels for each polarization. In
current design, an inductor size of 1.6 mm, which is equivalent to 10.4 angular resolution when projected on the sky,
is chosen to cover the full 6.5 field-of-view. During commissioning, the angular resolution of the instrument has been
demonstrated to be very close to this designed value. To further approach the diﬀraction limit of the IRAM 30-m
telescope (8.5 in the 1.2 mm band), a compact Hilbert-type LEKID array is designed with a 1 mm inductor size. The
array is fabricated with 20 nm thick aluminum and contains 1312 LEKIDs covering a 60 mm diameter circle on the
NIKA2 focal plane, which corresponds to a field-of-view of 4.9 . We present the design and characterization of thisarray, and compare it to the performance of the current NIKA2 1 mm arrays. The design could easily be expanded tocover the full field-of-view with 2400 pixels once the readout bandwidth will be doubled.
category : Sensor Physics & Developments

148

PA-22 Polarization filter for microstrip lumped-element kinetic inductance detectors
Alicia Gomez1 , Martino Calvo2 , Johannes Goupy3 , Aurelien Bideaud4 , Florence Levy-Bertrand5 , Andrea Catalano6 ,Alain Benoit7 , Andrea Tartari8 , Alessandro Monfardini91

Centro de Astrobiologia (INTA-CSIC), 2 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France , 3 Institut Neel
& Universite Joseph Fourier, CNRS, Grenoble, France , 4 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France ,5
Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France , 6 LPSC, Universite Grenoble-Alpes, CNRS/IN2P3,
Grenoble, France , 7 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France , 8 APC, Astroparticule et
Cosmologie, Universite Paris Diderot, Paris, France , 9 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France

Lumped Element Kinetic Inductance Detectors (LEKIDs) have a broad potential for their future use in Cosmic
Microwave Background radiation (CMB) experiments. However, for these experiments, polarization sensitivity is amajor requirement and LEKIDs based on meander inductors exhibit a cross polarization around 30%.
LEKIDs consist of series inductance-capacitance resonators coupled to a feed line. Coplanar waveguide (CPW),
coplanar striplines (CPS) and microstrip (MS) have been tested for the feed line configuration in order to decrease
coupling dispersion and avoid parasitic propagating modes. MS configuration, which consists on shield loops aroundeach resonator and a ground plane on the bottom side of the wafer, has already shown good performance and is, forinstance, the configuration integrated in NIKA 2 arrays [1].
In this work, continuous ground plane of the MS has been replaced with parallel lines in order to be used as apolarizer. Microwave simulations show that if the spacing between lines is small enough compared to the resonant
frequency wavelength, it acts as an eﬀective ground plane with no influence on the electromagnetic performance.
Several devices have been fabricated in order to test the polarizer-ground plane and preliminary experiments show amitigation of the cross polarization to 2 %.
[1] Calvo, M. et al.
The NIKA2 instrument, a dual-band kilopixel KID array for millimetric astronomy , J.
Low Temp. Phys, 184: 816 (2016).
category : Sensor Physics & Developments149

PA-23 Dual-color antenna-coupled LEKID for next generation CMB focal planes
Alessandro Traini1 , Andrea Tartari2 , Guillaume Bordier3 , Faouzi Boussaha4 , Christine Chaumont5 , Samir Beldi6 ,Florent Reix7 , Michel Piat8
1

CNRS / APC Universite Paris Diderot, 2 APC, Universite Paris Diderot , 3 APC, Universite Paris Diderot , 4 GEPI,
Observatoire de Paris , 5 GEPI, Observatoire de Paris , 6 GEPI, Observatoire de Paris , 7 GEPI, Observatoire de Paris , 8 APC,
Universite Paris Diderot

We present an antenna coupled Kinetic Inductance Detector for millimeter wave astronomy. Next generation telescopes
for observing the Cosmic Microwave Background are demanding in terms of number of detectors and focal plane area
filling eﬃciency. Moreover, foreground reduction in B- Mode polarimetry requires sky observation with multiple
frequency bands. In this context KIDs are promising technology because of their large multiplexing rate, while
antenna coupling can provide multi-band and dual-polarization solutions in compact design.
We have developed polarization sensitive dual band pixel at 140 GHz and 160 GHz with a bandwidth of almost 10
We will present performance estimations with numerical simulation software (CST, Sonnet) and preliminary measurements of sample devices.
category : Sensor Physics & Developments150PA-24 Optimisation of an antenna-coupled LEKID for future ground-based CMB
experiments
Amber Loren Hornsby1 , Peter Stuart Barry2 , Simon Doyle3 , Erik Shirokoﬀ4
1

School of Physics and Astronomy, Cardiﬀ University, 2 School of Physics and Astronomy, Cardiﬀ University / Department of
Astronomy & Astrophysics, University of Chicago , 3 School of Physics and Astronomy, Cardiﬀ University , 4 Department of
Astronomy & Astrophysics, University of Chicago

Optical coupling to a lumped-element kinetic inductance detector (LEKID) via an antenna and transmission line
structure enables compact, polarisation sensitive multichroic pixels to be realised in an architecture easily optimised forsensitivity and multiplexing performance. Here we present a robust study into the optimisation of an antenna-coupled
LEKID for applications in cosmic microwave background (CMB) experiments. Future ground-based B-mode studies
will require thousands of detectors performing at the photon noise limit under typical optical sky loading. We combine
electrodynamics of type-I superconductors and transmission line theory to investigate the pair breaking eﬃciency ofan optical signal coupled to a LEKID meander via a microstrip transmission line to yield the optimum length ofmeander required for full absorption. We then consider the performance of a LEKID under optical load, exploring therelationship between quality factor, quasiparticle lifetime and other limitations allowing for ideal detector parameters
to be determined when incorporated into a large array with high multiplexing ratios. We discuss the experimental
data acquired to corroborate our model and the steps required to extend this model to support to bi-layer materials
with reduced band-gaps to enable detection at wavelengths beyond 3mm.
category : Sensor Physics & Developments151

PA-25 Investigation of Single Crystal Niobium for Microwave Kinetic Inductance
Detectors
Agnes Dominjon1 , Shibo Shu2 , Matthias Kroug3 , Takashi Noguchi4 , Yutaro Sekimoto5 , Tom Nitta6 , Shigeyuki
Sekiguchi7 , Wenlei Shan814National Astronomical Observatory of Japan, 2 University of Tokyo , 3 National Astronomical Observatory of Japan ,National Astronomical Observatory of Japan , 5 National Astronomical Observatory of Japan , 6 University of Tsukuba ,7
University of Tokyo , 8 National Astronomical Observatory of Japan

During last decade, Microwave Kinetic Inductance Detectors (MKIDs) have been increasingly investigated in the fieldof astrophysical observations. The Advanced Technology Centre (ATC) of National Astronomical Observatory ofJapan is developing MKIDs for future wide field-of-view observations.
In this contribution, we present our study on MKIDs made of single crystal niobium with 150 nm of thickness.
The entire fabrication of the detector is carried out in the ATC clean room. The Nb layers have been sputtered on
sapphire wafer with a large 4′′ target and a high speed of 1.7 nm/s. The chamber vacuum was maintained to 10−6 Pa
and the substrates were heated up to 800 degC during the deposition.
First, the DC properties of the single crystal Nb layer (Tc, rho and RRR) have been characterized using a helium
bath (T = 4.2 K). A critical temperature of 9.4 K and a resistivity of 15.8 µOhm.cm have been measured for a thicknessof 150 nm. The residual resistivity ratio has reached values ranging from 40 to 80.
Then, the MKIDs made with this single crystal Nb have been characterized in a 0.1 K dilution refrigerator. An
internal quality factor Qi was measured up to 106 and the two level system eﬀects are found in the shift of resonancefrequency with increasing temperature up to 1.9 K. The Qi reaches its maximum value under -70 dBm readout power
at 800 mK. The measurement of the noise power spectral density of these MKIDs gives a low value of -95 dBc/Hz
from 100 Hz to 100 kHz.
This study on MKID made of single crystal Nb has been compared to a similar device made of polycrystalline Nb
in order to show the interest of using a single crystal structure material for superconducting micro-resonators.
category : Sensor Physics & Developments152

PA-26 Design of Near Infrared and Visible Kinetic Inductance Detectors using MIM
Capacitors
Samir Beldi1 , Faouzi Boussaha2 , Christine Chaumont3 , Shan Mignot4 , Florent Reix5 , Andrea Tartari6 , Michel Piat7 ,Piercarlo Bonifacio8
1

GEPI,GEPI, Observatoire de Paris, 2 GEPI, Observatoire de Paris , 3 GEPI, Observatoire de Paris , 4 GEPI, Observatoire deParis , 5 GEPI, Observatoire de Paris , 6 APC, Universite de Paris , 7 APC, Universite de Paris , 8 GEPI, Observatoire de Paris

Abstract
We are developing superconducting microwave kinetic Inductance detectors (MKIDs) to operate at near infraredand optical wavelengths for astronomy applications. In order to eﬃciently meet with the requirements of someastronomical applications, the KID size should be diminished typically from hundreds to a few tens of μ m. Successful
titanium nitride (TiN) optical Lumped-element KID using an inductive meander with an interdigital capacitance havebeen developed [1]. These pixels feature, for example, a size of 130 × 130 μ m and are coupled to coplanar transmission
line (CPW) to operate at around 4 GHz. For operation in the band 1-2 GHz where the readout electronics system
is easier to implement, the pixel can easily reach a size of 300 × 300 μ m. In this case, the interdigital capacitancesize can represent up to 90 % of the overall pixel size. We propose to replace the interdigital capacitor by a MIM(Metal-Insulator-Metal) capacitor which has the advantage of presenting a larger capacitance value within a muchsmaller space, which can also be adjusted by choosing dielectrics with high permittivity (ε r).
In this paper, we will present designs and simulation results of the reduced TiN-based LEKID using MIM. The
pixel will occupy a space of typically 100x85 μ m which is 9 times less than a typical pixel size using the interdigital
capacitor for frequency operation below 2 GHz.
[1] Meeker, S.R., Mazin, B.A., Jensen-Clem, R., Walter, A.B., Szypryt, P., Strader, M.J., and Bockstiegel, C.Design
and Development Status of MKID Integral Field Spectrographs for High Contrast Imaging. Proc.
AO4ELT 4, 2015.
category : Sensor Physics & Developments

153

PA-27 A TiN/Ti/TiN Trilayer Lumped Element KID Array for CMB Polarimetry at
100 GHzAmy E Lowitz1 , Ari D Brown2 , Vilem Mikula3 , Thomas R Stevenson4 , Peter T Timbie5 , Edward J Wollack6
1

KICP, University of Chicago, 2 NASA Goddard Space Flight Center , 3 Catholic University of America , 4 NASA Goddard
Space Flight Center , 5 University of Wisconsin - Madison , 6 NASA Goddard Space Flight Center

Kinetic inductance detectors (KIDs) are a promising technology for astronomical observations overa wide range of wavelengths in the mm to submm regime and beyond. Simple fabrication, with as little
as a single lithographic layer, and passive frequency-domain multiplexing, with readout of up to 1000
detectors on a single line with a single cold amplifier, make KIDs an attractive solution for high pixel-countdetector arrays. In this presentation we describe the design, fabrication, and testing of a 20-pixel
prototype array of TiN/Ti/TiN trilayer kinetic inductance detectors intended for cosmic microwave
background (CMB) polarimetry in a band centered at 3 mm (100 GHz), which is an important band for
CMB observations from the ground. We discuss the theoretical performance of idealized KIDs
compared to idealized superconducting transition edge sensors (TESs), describe the lumped-element,
integrated groundplane resonator design, and present measurements of dark performance and opticalresponse.
category : Sensor Physics & Developments154

PA-28 Ultra Low-NEP FIR LEKIDs: a Three-Pronged Approach
Adalyn Fyhrie1 , Jason Glenn2 , Henry Leduc3 , Peter Day4 , Byeong Ho Eom5 , Jonas Zmuidzinas6 , Christopher
McKenney7
1

University of Colorado Boulder, 2 University of Colorado Boulder , 3 Jet Propulsion Laboratory , 4 Jet Propulsion Laboratory ,5
Jet Propulsion Laboratory , 6 Jet Propulsion Laboratory / Caltech , 7 National Institute of Standards and Technology

Future generations of far-infrared (FIR) telescopes such as the Origins Space Telescope will need detectors with NEPs
on the order of 5x10−20 W/sqrt(Hz) in order to be limited by astrophysical backgrounds only. FIR detectors thatcan robustly reach this limit have not yet been demonstrated. We present updates on three arrays of around 100
kinetic inductance detectors (KIDs) that use a variety of techniques for achieving these low NEPs. Our first arrays(presented at LTD 2015) are low-volume Al/TiN bilayer devices that reached an NEP of 2x10−17 W/sqrt(Hz) at 350
um and showed evidence for excess photon loading and significant 1/f noise. Our second arrays (presented at SPIE
2016) are low-volume Al-only devices and are of a similar design to the bilayer devices. These devices reached an
NEP of 10−17 W/sqrt(Hz) at 350 um and also showed evidence of excess photon loading, but no 1/f noise. Our third
array (simulations of which were presented at SPIE 2016) use phonon recycling, the process of trapping recombination
phonons below the detector active area, to increase sensitivity. We present strategies to reduce the excess photon
loading seen in arrays one and two, and preliminary tests on the phonon recycling arrays.
category : Sensor Physics & Developments155

PA-29 Optimization of geomagnetic shielding for MKIDs mounted on rotating
cryostat
Hiroki Kutsuma1 , Makoto Hattori2 , Kenji Kiuchi3 , Satoru Mima4 , Taketo Nagasaki5 , Shugo Oguri6 , Junya Suzuki7 ,Osamu Tajima8
1

Tohoku University Astronomical Institute, Tohoku University, 2 Tohoku University , 3 RIKEN , 4 RIKEN , 5 RIKEN , 6 RIKEN, 7 KEK , 8 KEK / SOKENDAI

Observational confirmation of the cosmic inflation theory is one of the most important subjects in the modern cosmology. Existence of a period of exponential expansion of the space-time metric in the very early universe, inflation period,
provides solutions for problems left in the standard Big Bang model of the cosmology. One of the consequences of theinflation is an emergence of the primordial gravitational waves, which imprint characteristic spiral patterns (B-modes)on the polarization map of the Cosmic Microwave Background (CMB) radiation.
GroundBIRD is a ground based CMB experiment which aims to detect the CMB B-modes polarization imprinted
by the gravitational waves. One of the key features of the GroundBIRD telescope is the rotating scan in azimuth
direction at 20 rpm to suppress the baseline drift of the detector response caused by 1/f atmospheric fluctuation. We
employ Microwave Kinetic Impedance Detectors (MKIDs). MKID is a high sensitive superconductive direct detector.
Its extremely fast time response direct detectors makes possible to realize this high-speed scan.
Shielding of MKIDs from geomagnetism is an important subject. If the detector traps magnetic field in a processof the phase transition from normal to superconducting state, the sensitivity of the detector is dramatically reduced.
To solve this problem significant reduction of the magnetic field at the focal plane by using magnetic shield with highpermeability is designed. Our cryostat is composed by cavity at 4 Kelvin, 40 Kelvin, and 300 Kelvin. We set magnetic
shields on each cavity.
We used MS-FR made by Hitachi-material as high permeability magnetic shield. First, we measured shielding powerusing a cylinder of MS-FR seat with a Gaussmeter. Based on this consistency check, we estimate required shielding
power using a prototype MKIDs array installed in cryostat which also has three layers of cavity and shield similes toGroundBIRD. We also estimated how time required for cooling down response to number of shield. We confirm that
our strategy of magnetic shields satisfies our requirements. In order to design magnetic shield for GroundBIRD, weevaluated the shielding power by ANSYS Maxwell, which employs finite element method to simulate electromagnetic
field. Dealing with thin film with high permeability or a large volume causes systematic bias in the simulation. By
increasing the thickness of the shield as keeping a value multiplied by the thickness of the shield and the permeabilityof the shield material constant, times required for simulations are dramatically reduced. From measurement andsimulation we conclude that the sensitivity of MKIDs is not aﬀected by geomagnetism if five sheets of MS-FR set
on each cavity of the cryostat. We also simulate the eﬀect of gap between the side and top shields and the eﬀect ofrotation of the cryostat due to scanning observations.
category : Sensor Physics & Developments156

PA-30 Proposal of a kinetic inductance current amplifier with coplanar waveguide
input structure for magnetic flux focusing
Gensheng Wang1 , Clarence Chang2 , Thomas Cecil3 , Valentine Novosad4 , Steve Padin5 , Volodymyr Yefremenko6
1

Argonne National Laboratory, 2 Argonne National Laboratory , 3 Argonne National Laboratory , 4 Argonne National
Laboratory , 5 Argonne National Laboratory , 6 Argonne National Laboratory

We propose a multiplexable kinetic inductance current amplifier which has a high-quality-factor, superconducting,lumped-element kinetic inductance resonator for readout and a short, superconducting coplanar waveguide (CPW)for input. The resonator consists of an interdigitated capacitor and a narrow strip that inductively couples to the
CPW. The input current running through the central line of the CPW generates magnetic fields. These magnetic
fields are focused into the CPW gaps where the inductive superconducting strip of the resonator sits. Because thekinetic inductance of the superconducting strip depends on the strength of the magnetic fields, the input current isconverted to a change of the resonance frequency of the high-quality factor resonator. With appropriate geometricalparameters, and high-resistivity superconducting films, the amplifier is expected to have a low input impedance anda high current readout sensitivity. We present a preliminary analysis of the amplifier’s response to an input current,and discuss its noise.
category : Sensor Physics & Developments157

PA-31 Disk Resonator Format for Kinetic Inductance Detectors
Nicholas Zobrist1 , Miguel Daal2 , Bernard Sadoulet3 , Ben Mazin4
1

Department of Physics, University of California, Santa Barbara, 2 University of California, Santa Barbara , 3 University ofCalifornia, Berkeley , 4 University of California, Santa Barbara

We propose disk format resonators for use as kinetic inductance detectors. Pros and cons of this design are discussedwith consideration for potential detector applications. We have conducted electromagnetic simulations of the resonatorgeometry and will use them to discuss the disk resonator properties. We will compare several schemes for couplingthese resonators to feed lines and discuss the eﬀect of a large kinetic inductance on the design equations for the
resonant frequency and coupling quality factor. Additionally, a strategy to reduce the resonator metal volume bymeshing is considered and its eﬀects on the resonator s current distribution are shown. We find that meshing cansignificantly alter the resonant frequency of the disk.
category : Sensor Physics & Developments158

PA-32 Design and characterization of titanium nitride subarrays of Kinetic
Inductance Detectors for passive terahertz imaging
Dmitry Morozov1 , Simon Doyle2 , Archan Banerjee3 , Thomas Brien4 , Robert H Hadfield5 , Dilini Hemakumara6 , Iain
Thayne71School of Engineering, University of Glasgow, 2 School of Physics and Astronomy, Cardiﬀ University, Cardiﬀ, UK , 3 School ofEngineering, University of Glasgow, Glasgow, UK , 4 School of Physics and Astronomy, Cardiﬀ University, Cardiﬀ, UK ,5
School of Engineering, University of Glasgow, Glasgow, UK , 6 School of Engineering, University of Glasgow, Glasgow, UK ,7
School of Engineering, University of Glasgow, Glasgow, UK

Terahertz (THz) imaging for security applications attracts increasing interest in both research community and industrial sector. As THz radiation can be transmitted through many non-metallic materials, passive imaging camera can
detect thermal radiation from room temperature objects and allow to identify the presence of concealed dangerous
objects. During the last few years several passive imagers have been built utilising diﬀerent types of superconducting
bolometers and semiconducting detectors [1, 2]. Kinetic Inductance Detectors have an advantage of relatively simple
fabrication and scalability, which makes them a technology of choice for building an imager with large number ofpixels. Recently, arrays of KIDs, predominately used in astronomical instruments, were successfully utilized in THz
camera built by Cardiﬀ University [3, 4]. With Lumped Element design of KIDs (LEKIDs) based on aluminium film
demonstration camera achieved quasi-video frame rate of 2 Hz and noise equivalent temperature of 0.1 K at 0.35
THz. At the same time usage of Al based chips requires sub ¡300mK cryogenic setup, which adds complexity to theoverall design. On the other hand, titanium nitride (TiN) film based LEKIDs with sheet impedance of the order of
100-300 μ Ohm*cm and transition temperature (Tc) of 3.5-4 K can be operated at ¿1K bath temperature, which iseasily achievable with modern compact cryogenic systems. Also varying the thickness of the TiN film, one can adjust
its Tc and sheet impedance for the optimal optical coupling in LEKID configuration.
Here we report on development and characterization of a prototype subarrays based on Atomic Layer Deposition(ALD) TiN films. We present results on growth and characterization of ALD TiN films with thickness ranging from15 to 60 nm and Tc ranging up to 3.5 K and compare the results with sputtered TiN films. We also present theresults of LEKID subarray design, fabrication and optical characterization with internal black body source and 0.35
THz band pass filter.
References:
1. E. Heinz, et al., Proc. SPIE 8544, 2012
2. E. Grossman, et al., Appl. Opt. 49, E106 (2010)
3. K. Wood, et al., Infrared, Millimeter and Terahertz Waves, 2011
4. S. Rowe, et al., Rev. Sci. Instrum. 87, 033105 (2016)
category : Sensor Physics & Developments

159

PA-33 Multilayer Readout Wiring for Transition Edge Sensor Calorimeter Arrays
Using Chemical Mechanical Polishing
Kengo Kosaka1 , Yuichiro Ezoe2 , Seiichi Kitazawa3 , Ryota Hayakawa4 , Koji Nunomura5 , Takaya Ohashi6 , Yshitaka
Ishisaki7 , Shinya Yamada8 , Mutsuo Hidaka9 , Tetsuro Satoh10 , Kazuhisa Mitsuda11
1

Department of Physics, Tokyo Metropolitan University, 2 Tokyo Metropolitan University , 3 Tokyo Metropolitan University ,Tokyo Metropolitan University , 5 Tokyo Metropolitan University , 6 Tokyo Metropolitan University , 7 Tokyo Metropolitan
University , 8 Tokyo Metropolitan University , 9 AIST , 10 AIST , 11 JAXA / ISAS

4

We report on fabrication and evaluation of a 20 ×20 pixel array of TES (Transition Edge Sensor) microcalorimeters
based on multilayer readout wiring for future X-ray astronomy missions (e.g., DIOS, Ohashi et al. 2016 SPIE). We
have achieved 2.8 eV at 5.9 keV with a 4×4 pixel TES array (Akamatsu et al., 2009 AICP) and 4.4 eV at 5.9 keVwith a 16×16 pixel TES array (Ezoe et al., 2009 AICP). For a larger format TES array required in future missions like
DIOS,superconducting readout wiring becomes important. In the multilayer readout wiring, signal and return lines
are vertically stacked via insulation layer to reduce mutual inductance between readout lines and also self inductance.
It also reduces wiring space.
We thus have been developing the multilayer readout wiring TES arrays (Ezoe et al. IEEE JQE 2015, Kuromaru
et al. J. Low Temp Detector 2016). However, surface roughness of the upper readout wiring on which a TES film isdeposited hindered a proper super-normal transition, resulting in a large residual resistance. Therefore, we introduced
chemical mechanical polishing process. In this new fabrication process, we pattern the upper and lower readout wiring
made of Nb as before. Then, we put a thick SiO2 layer on the wafer (∼800 nm thick) and polish the wafer until theupper wiring is exposed to the surface. We achieved about 2.5 times better roughness than before (∼0.4 nm rms at 1
micro meter scale). We then put a TES film (Ti 100 nm/Au 20 nm) on the wafer. To minimize damage of the layer
underneath TES, we lowered the inverse sputtering power and time from 150 W, 3 min to 100 W, 1 min.
We characterized RT curves of the new TES array and confirmed a proper super-normal transition at 360 mK
with a small residual resistance of ∼1 mOhms. The transition temperature is near that of bulk Ti (390 mK), which isconsistent with the fact that the thick Ti and thin Au make proximity eﬀect weaker and the TES transition temperatureapproach that of Ti. We will proceed to complete fabrication of the 20×20 multilayer wiring TES array by depositing
Au absorbers and etching the silicon substrate for membrane structures to evaluate the energy resolution of pixels in
the array.
category : Sensor Physics & Developments160

PA-34 An on-chip filter bank spectrometer based on Transition Edge Sensors formeteorology and climatology
Ben Flatman1 , Peter Hargrave2 , Staﬀord Withington3 , Stefan Buhler4 , Lukas Kluft5 , Prateek Kumar Dongre6
1

School of Physics and Astronomy, Cardiﬀ University, 2 Cardiﬀ University, School of Physics & Astronomy , 3 University ofCambridge, Cavendish Laboratory , 4 Universitat Hamburg, Geowissenschaften, Meteorologisches Institut , 5 Universitat
Hamburg, Geowissenschaften, Meteorologisches Institut , 6 Cardiﬀ University, School of Physics & Astronomy

We propose a new superconducting on-chip filter bank spectrometer, based on novel few-mode ballistic Transition
Edge Sensors (TES s). This is a key enabling technology for a novel hyperspectral microwave instrument for use insatellite-based meteorology and climatology applications. The instrument is currently in its design and implementation
phase. TES s are still the leading technology in astronomy due to their reliability, low-noise and high dynamic
range. A filter bank spectrometer based on TES s has a significant advantage over similar systems based on Kinetic
Inductance Detectors (KIDs), as, unlike KIDs, they can easily reach frequencies below 140GHz. Importantly TES s
will allow access to critical atmospheric temperature sounding lines in the 50-60GHz region. While demonstration oflower frequency response is the initial goal, the final satellite concept will take advantage of the wide responsivity of
TES s to allow the coverage of significant absorption features across the 50-850GHz region. Current meteorologicalsatellite technology does not employ active cooling to sub-kelvin operating temperatures. Therefore in conjunction
with industry partners we are initiating a parallel study to investigate solutions to cooling an instrument of this typein low earth orbit. This instrument will be a disruptive technology for use in improving numerical weather prediction
and in constraining global climate models. Here we report on the current design and predicted performance of our
instrument concept.
category : Sensor Physics & Developments161

PA-35 Advanced ACTPol TES Device Parameters and Noise Performance in Three
Fielded Arrays
Kevin T. Crowley1 , AdvACT Collaboration2
1

Department of Physics, Princeton University, 2 Advanced ACTPol Collaboration

The Advanced ACTPol (AdvACT) upgrade to the Atacama Cosmology Telescope features arrays of aluminum manganese transition-edge sensors (TESes) optimized for ground-based observations. These arrays are central to AdvACTs science goals, which include measuring B-mode polarization patterns in the cosmic microwave background (CMB).
Tests of these arrays reveal highly responsive detectors with uniform thermal parameters across the array and thermal
conductance-dominated noise at low frequencies. We report on parameters acquired from swept-sine impedance datataken on a small subset of TESes using simple and extended bolometer electrothermal models. We then compare
expected noise spectral densities based on these parameters to measured noise. These tests indicate excess noise at
frequencies around 100 Hz, outside of the nominal band of temporal frequencies used in CMB measurements. However,
we investigate this excess in order to shed light on the mechanism of excess noise in TESes. In addition, we describe
full-array noise measurements in the laboratory and in the field for two new AdvACT mid-frequency arrays, sensitiveat bands centered on 90 and 150 GHz, as well as achieved noise performance during observations of the previously
installed high-frequency array (150 and 230 GHz).
category : Sensor Physics & Developments

162

PA-36 Development of gamma-ray position-sensitive transition-edge-sensor
microcalorimeters
Naoko Iyomoto1 , Yuki Shuto2 , Takehiro Kuroiwa3 , Yuta Kurume4 , Yu Kiguchi5 , Keisuke Maehata6 , Tasuku
Hayashi7 , Haruka Muramatsu8 , Kazuhisa Mitsuda9 , Shota Yoshimoto10 , Akira Takano11
1

Kyushu University, 2 Kyushu University , 3 Kyushu University , 4 Kyushu University , 5 Kyushu University , 6 Kyushu
University , 7 ISAS/JAXA , 8 ISAS/JAXA , 9 ISAS/JAXA , 10 Kyushu University , 11 Kyushu University

We are developing Transition-edge sensor (TES) microcalorimeters to detect gamma-rays up to a few MeV. The
photoelectric attenuation length in the energy range is several tens of mm. Energy resolutions of such thick-absorbermicrocalorimeters tends to suﬀer from degradation due to dependence of pulse shape on gamma-ray interaction positions in the absorber. In order to avoid such a degradation of energy resolution due to the position dependence, weare proposing Position-Sensitive TESs (PoSTs) for gamma rays. We fabricated a PoST with a long lead absorber anda TES on each end of the absorber. The length, width and thickness of the absorber are 20 mm, 0.5 mm and 0.5 mm,
respectively. We report on the results of gamma-ray irradiation on the device.
category : Sensor Physics & Developments

163

PA-37 Dark characterization and comparison of various Mo/Au based TESs
Carlos Pobes1 , Lourdes Fabrega2 , Agustin Camon3 , Nieves Casan-Pastor4 , Pavel Strichopanec5 , Javier Sese6 , Javier
Moral-Vico7 , Rosa Jaudenes8
1Institute of Material Science of Aragon (ICMA), CSIC-University of Zaragoza, 2 ICMAB-CSIC , 3 ICMA-CSIC ,4
ICMAB-CSIC , 5 ICMA-CSIC / ICMAB-CSIC , 6 INA , 7 ICMAB-CSIC , 8 ICMA-CSIC / ICMAB-CSIC

Transition Edge Sensors (TESs) are among the best devices for radiation detection in a wide range of energies. They arevery sensitive thermometers that, when coupled to suitable absorbers or antennas, exhibit excellent energy resolution
for a specific energy range (microcalorimeters) or excellent signal to noise ratio (bolometers). This explains theirincreasingly widespread use in several instruments for fundamental and applied science.
We report here on the DC dark characterization and comparison of parameters of diﬀerent TESs based on Mo/Au
proximity bilayers, aimed at soft X-ray detection, with Bi absorbers. A refinement of the fabrication process has
improved reproducibility and allowed fabrication of devices with Tc, G and power dissipation in the range of interestfor the X-IFU instrument onboard Athena. Thanks to the achieved control of both Tc, G and Rn, we can also tune
our designs towards other wavelengths of interest as new applications of TESs emerge.
TESs with two diﬀerent designs and several geometries of bare sensors, with and without lateral banks, have beencharacterized, with critical temperatures on the order of 100 mK and normal resistances between 10 m? and 20 m?.
Various sizes and thicknesses of SiN membranes have been used to control the thermal link of the bilayer to the thermalbath. First TESs with a few microns of electrodeposited Bi have also been characterized. A good understanding of
the thermal conductance, capacitance and noise levels of our devices has been achieved through IVs, Z(w) and noise
measurements. For all the tested devices, G scales perfectly with the radiant area of the TES-membrane system
irrespective of the membrane size. Detailed analysis of key parameters like logarithmic sensitivities, eﬀective time
constants, capacitance and excess noise has also been performed as a function of bath temperature and TES operation
point for these bare devices.
A reasonable understanding of TES performances through complex model fitting of our data is also the starting
point for further optimizations. We show that even for simple devices without absorber, banks or metal structures,
two thermal block models are not in general enough to reproduce the experimental data.
category : Sensor Physics & Developments164PA-38 Twin-slot antenna coupled superconducting Ti transition edge sensor at 350
GHz
Wen Zhang1 , Wei Miao2 , Zheng Wang3 , Xiao-Hui Guo4 , Dong Liu5 , Jia-Qiang Zhong6 , Qi-Jun Yao7 , Sheng-Cai Shi8
1

Purple Mountain Observatory, 2 Purple Mountain Observatory / Key Lab of Radio Astronomy , 3 Purple Mountain
Observatory / Key Lab of Radio Astronomy , 4 Purple Mountain Observatory / Key Lab of Radio Astronomy , 5 Purple
Mountain Observatory / Key Lab of Radio Astronomy , 6 Purple Mountain Observatory / Key Lab of Radio Astronomy ,7
Purple Mountain Observatory / Key Lab of Radio Astronomy , 8 Purple Mountain Observatory / Key Lab of Radio
Astronomy

Superconducting transition edge sensors (TES) based on a Ti microbridge on Si substrate have demonstrated a very
low noise equivalent power. Their eﬀective response time, however, is in the order of microseconds due to its relatively
high transition temperature of 400 mK, making it diﬃcult to read out the signal of a large Ti TES array with a
SQUID-based multiplexer. We have reported on a free-standing membrane supported superconducting Ti TES with
an eﬀective response time of 5 μ s. In order to further increase the eﬀective response time, we etch the supported
SiN membrane before KOH wet etching, and then the Ti TES microbridge is suspended only by the left four legs
after removing the silicon substrate. The current-voltage (I-V) curves are measured at diﬀerent bath temperatures
before and after KOH wet etching. The thermal conductance is reduced to 500 pW/K from 9000 pW/K. The eﬀective
response time measured with a light emitting diode (LED) is about 100 μ s, about 20 times larger. In addition, we
have studied the optical noise equivalent power (NEP) with a cryogenic blackbody in combination with metal-meshfilters to define the radiation bandwidth. The obtained optical NEP is 6x10−16 W/Hz0.5 at a bath temperature of 350
mK. The achieved optical sensitivity is suitable for ground-based astronomical applications.
category : Sensor Physics & Developments165

PA-39 Magnetic Sensitivity of AlMn TESes and Shielding Considerations for Next
Generation CMB Surveys
Eve Marie Vavagiakis1 , Shawn Wesley Henderson2 , Michael D Niemack3 , Kaiwen Zheng4
1

Department of Physics, Cornell University, 2 Cornell University , 3 Cornell University , 4 Cornell University

In the next decade, new ground-based Cosmic Microwave Background (CMB) experiments such as Simons Observatory (SO), CCAT-prime, and CMB-S4 will increase the number of detectors observing the CMB by an order ofmagnitude or more, dramatically improving our understanding of cosmology and astrophysics. These eﬀorts will likely
deploy receivers utilizing large arrays of (tens of thousands) transition edge sensor (TES) bolometers coupled to Superconducting Quantum Interference Device (SQUID)-based readout systems. It is well known that superconducting
devices such as TESes and SQUIDs are sensitive to magnetic fields. Understanding the magnetic field sensitivity of
TESes is particularly important for upcoming CMB surveys because changes in the TES responsivity could mimic
faint CMB signals. The eﬀects of magnetic fields on the superconducting transition of these devices are not easily
predicted due to the lack of a complete physical model of the TES transition. This motivates direct measurements ofthe magnetic sensitivity of these devices to inform magnetic shielding requirements for upcoming CMB surveys. AlMn
TESes are becoming widely used due to their simple single layer film manufacturing process yielding highly uniform
arrays over large detector wafers, and will likely be used for upcoming experiments such as SO and CCAT-prime. We
present measurements of the critical temperature versus applied magnetic field, which may be the first of this type
for AlMn TESes, on devices varying in both geometry and manganese concentration, including ACTPol, Advanced
ACT (AdvACT), and POLARBEAR bolometers, using four-lead measurements. We discuss the observed eﬀects ofexternally applied magnetic fields on detector parameters and their implications. We also compare measurements ofmagnetic sensitivity for time division multiplexing SQUIDs used in AdvACT to that of frequency division multiplexing
microwave rf-SQUIDs currently under consideration for use in SO and CCAT-prime. We discuss the implications ofour measurements on the magnetic shielding required for upcoming CMB experiments, which may field hundreds ofthousands of TESes and SQUIDs in order to map the CMB to near-fundamental limits.
category : Sensor Physics & Developments

166

PA-40 Study of Dissipative Losses in AC-Biased Mo/Au Bilayer Transition-Edge
Sensors
Kazuhiro Sakai1 , Joseph S Adam2 , Simon R Bandler3 , James A Chervenak4 , Aaron M Datesman5 , Megan E
Eckart6 , Fred M Finkbeiner7 , Richard L Kelly8 , Antoine R Miniussi9 , Frederick S Porter10 , Caroline A Kilbourne11 ,John E Sadleir12 , Stephen J Smith13 , Nicholas A Wakeham14 , Edward J Wassell15 , Wonsik Yoon16 , Hiroki
Aakamatsu17 , M P Brujin18 , Luciano Gottardi19 , Brian D Jackson20 , Jan van der Kuur21 , Bert-Joost van Leeuven22 ,A J van der Linden23 , Henk J van Weers24 , Mikko Kiviranta25
1

NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore
County , 3 NASA Goddard Space Flight Center , 4 NASA Goddard Space Flight Center , 5 NASA Goddard Space Flight Center/ SGT, Inc. , 6 NASA Goddard Space Flight Center , 7 NASA Goddard Space Flight Center / Wyle Information Systems ,8NASA Goddard Space Flight Center , 9 NASA Goddard Space Flight Center / CRESST II - University of Maryland
Baltimore County , 10 NASA Goddard Space Flight Center , 11 NASA Goddard Space Flight Center , 12 NASA Goddard Space
Flight Center , 13 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 14 NASA
Goddard Space Flight Center / NPP - Universities Space Research Association , 15 NASA Goddard Space Flight Center /SGT, Inc. , 16 NASA Goddard Space Flight Center / NPP - Universities Space Research Association , 17 SRON National
Institute for Space Research , 18 SRON National Institute for Space Research , 19 SRON National Institute for Space Research ,20
SRON National Institute for Space Research , 21 SRON National Institute for Space Research , 22 SRON National Institutefor Space Research , 23 SRON National Institute for Space Research , 24 SRON National Institute for Space Research , 25 VTT

We are developing a kilo-pixel array of transition-edge sensor (TES) microcalorimeters for the X-Ray Integral Field
Unit of the future European X-Ray Observatory Athena. Recent measurements of AC-biased Mo/Au bilayer TESs
imply a dissipative loss at the TES. These measurements are made using a resonant circuit in the frequency range of
1-5 MHz. In this paper, we present the results of our measurements and discuss the cause of the AC losses. The ACbias currents used in these measurements are so low that under DC-bias, with the same nominal Joule power heating,
the TESs would remain in the superconducting state. However under AC bias there is loss at MHz frequencies,
which is frequency dependent and can be non-negligible even when biasing within the TES transition. The dissipation
behaves as a series resistance within the TES, and therefore alters the transition shape, lowering the steepness of thetransition, particularly low in the transition. This will aﬀect the key properties that determine the microcalorimeterenergy resolution. We measured AC losses and transition properties on various TES geometries. We looked at TESs
with diﬀerent sizes, TESs with diﬀerent numbers of stripes, TESs with diﬀerent sheet resistances, and TESs with
diﬀerent geometries for the contact area between the TES and the absorber. We also modeled the TES using a finite
element method (FEM) and simulated the AC loss. The loss measurements on various TES devices and the FEM
simulation results indicate a causal relationship between the loss and the normal metal area exposed to the self-induced
magnetic field, implying that the loss is due to Eddy current heating.
category : Sensor Physics & Developments

167

PA-41 Development of TiAu TES X-ray calorimeters for the X-IFU on ATHENA
space observatory
Pourya Khosropanah1 , L. Gottardi2 , C. P. de Vries3 , K. Nagayoshi4 , M. L. Ridder5 , H. Akamatsu6 , M. P. Bruijn7 , J.
R. Gao8
1

SRON Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research , 3 SRON Netherlands
Institute for Space Research , 4 SRON Netherlands Institute for Space Research , 5 SRON Netherlands Institute for Space
Research , 6 SRON Netherlands Institute for Space Research , 7 SRON Netherlands Institute for Space Research , 8 SRON
Netherlands Institute for Space Research / Kavli Institute of NanoScience, Delft University of Technology, Delft, theNetherlands

SRON is developing X-ray calorimeters with a goal to meet the detector requirements for X-IFU instrument on the
ATHENA space observatory. ATHENA is the second ’Large mission’ of ESA’s Cosmic Vision-programme and has aplanned launch date in 2028. This X-ray telescope will study spectacular astrophysical phenomena near black holes
and neutron stars. The X-ray Integral Field Unit (X-IFU) is one of the instruments on board to deliver spatiallyresolved high-resolution X-ray spectroscopy over a limited field of view.
Our calorimeters are based on a superconducting TiAu bilayer TES (transition edge sensor) with critical temperature of around 100 mK on a 1 um thick SiN membrane with gold or gold and bismuth absorbers. Quite a few devices
have been successfully fabricated with a large variety of design parameters that includes:• TESes with or without metallic bars and dots of diﬀerent sizes.
• TESes with or without slots in the SiN membrane for low and high thermal conductance.
• Variety of absorbers and absorber coupling schemes.
• Variety in wiring.
We are currently characterizing these calorimeters under AC bias (1-5 MHz bias frequency) using an FDM readout,
also developed at SRON. This system is a small version of what is considered as the baseline for X-IFU instrument
readout and enables us to measure up to 18 devices in each run.
Characterization is done by measuring the IV curves, critical temperature, thermal conductance, noise and baseline
resolution. We also measure the X-ray energy resolution using Fe-55 source at 6 keV at selected bias points. By looking
at the shape and the statistics of the rise/fall time of the pulses, we are able to determine the quality of our absorberand absorber coupling. So far our best calorimeter shows a 2.9 eV baseline resolution and a 3.6 eV X-ray resolution at
6 keV. We will present all the key results and report the latest status of development of X-ray calorimeters at SRON.
Acknowledgement: This work is partly funded by European Space Agency (ESA) and coordinated with other
European eﬀorts under ESA CTP contract ITT AO/1-7947/14/NL/BW.
category : Sensor Physics & Developments

168

PA-42 The succesfull readout of the 176 TES FDM system for SAFARI
Richard Arnold Hijmering1 , Damian Audley2 , Roland den Hartog3 , Marcel Ridder4 , Anthony J. van der Linden5 ,Brian Jackson6 , Jan van der Kuur7 , Marcel Bruijn8 , Jian-Rong Gao9
1

SRON Netherlands institute for Space Research, 2 SRON Netherlands institute for Space Research, Groningen, The
Netherlands , 3 SRON Netherlands institute for Space Research, Utrecht, The Netherlands , 4 SRON Netherlands institute forSpace Research, Utrecht, The Netherlands , 5 SRON Netherlands institute for Space Research, Utrecht, The Netherlands ,6
SRON Netherlands institute for Space Research, Groningen, The Netherlands , 7 SRON Netherlands institute for Space
Research, Groningen, The Netherlands , 8 SRON Netherlands institute for Space Research, Utrecht, The Netherlands , 9 SRON
Netherlands institute for Space Research, Utrecht, The Netherlands / Kavli Institute of NanoScience, Delft University ofTechnology, Delft, the Netherlands

At SRON we are developing Frequency Domain Multiplexing (FDM) for read out of large AC biased TES arrays forboth the SAFARI instrument, for the far-IR SPICA mission, and XIFU instrument, for the X-ray Athena mission.
In this paper we focus on the development of a FDM demonstration model for the SAFARI instrument. SAFARI is
one of the focal-plane instruments for the Japanese/European far-IR SPICA mission proposed earlier this year for
the ESA M5 selection. It is a high sensitive grating spectrometer with a resolving power of 300 operating in the
wavelength range of 34-210 μ m. The instrument is based on four arrays with in total 3550 TES-based bolometerswith noise-equivalent powers (NEP) in the range of 2?10-19 W/?Hz having background-limited sensitivity and higheﬃciency. In FDM the TES bolometers are AC biased and readout using in total 24 channels. Each channel contains
160 pixels of which the resonance frequencies are defined by in house developed cryogenic lithographic LC filters. To
overcome the dynamic range limitations of the SQUID pre-amplifier, a special technique named baseband feedback(BBFB) is applied. FDM is based on the amplitude modulation of a carrier signal, which also provides the AC voltage
bias, with the signal detected by the TES. BBFB attempts to cancel the error signal in the sum-point (located at
the input coil of the SQUID), by feeding back a remodulated signal to the sum-point, and therefore improving the
dynamic range of the SQUID pre-amplifier.
Previously we reported on the results of our first iteration of a prototype 160 pixel FDM system with which we
performed a detailed study on the eﬀects of electrical crosstalk. The knowledge obtained we used to develop a second
generation full 176 pixel FDM experiment in which the electrical crosstalk elements are minimized. The cold part ofthe experiment consists of a detector chip with 176 bolometers with a design NEP of 7?10-19 W/?Hz. On either sideof the bolometer chip two LC filter chips are placed of which each contain 88 carefully placed high-Q superconducting
resonators with in total 176 diﬀerent resonance frequencies. The pixels are read out using a single-stage SQUID. The
warm electronics consist of a low-noise amplifier (LNA) and in-house developed digital board which performs; thegeneration of the bias carriers, the demodulation of the signal and remodulation of the feedback signal.
In the new prototype the electrical crosstalk has been drastically lowered by reducing the carrier leakage by a factor
two and removing the eﬀects of mutual inductance by careful design. The common impedance has been reduced to
4nH, including the 3nH input coil of the SQUID. By implementing screening of the input coil this has successfully
been further reduced to below 1nH. Connecting the pixels in stages; a quarter, half and the full array resulted in
detecting and solving remaining issues. Using this set-up we successfully simultaneously locked and read-out morethan 130 pixels. In this paper we will report on the results obtain with this 176 pixel FDM experiment.
category : Sensor Physics & Developments

169

PA-43 Design of the EBEX-IDS Instrument and Detectors
Francois Aubin1 , Shaul Hanany2 , Bradley Johnson3 , Adrian Lee4 , Aritoki Suzuki5 , Benjamin Westbrook6 , Karl
Young71School of Physics and Astronomy, University of Minnesota, 2 University of Minnesota , 3 Columbia University , 4 University ofCalifornia, Berkeley , 5 University of California, Berkeley , 6 University of California, Berkeley , 7 University of Minnesota

EBEX-IDS is a balloon-borne polarimeter designed to characterize the polarization of foregrounds and to detect
the primordial gravity waves through their B-mode signature on the polarization of the cosmic microwave background(CMB). EBEX-IDS will operate 20,562 transition edge sensor (TES) bolometers spread over 7 frequency bands between
150 and 360 GHz with resolution higher than 7.2’ for all bands. EBEX-IDS will use sinuous antenna multichroic pixels(SAMP) with TES bolometers which have been developed for ground-based CMB telescopes such as POLARBEAR-2,
Simons Array and SPT-3G. Balloon and satellite platforms enable observations at frequencies inaccessible from theground and with higher instantaneous sensitivity. Both advantages are due to the lower atmospheric emission. But
to realize these advantages the instrument must be optimized for a significantly lower optical loading.
We introduce the instrument design of the EBEX-IDS CMB polarization balloon-borne payload to take advantage ofhigh altitude balloon flight. We also present our work to develop and characterize low thermal conductance bolometersthat are part of SAMPs to be used with the EBEX-IDS payload. We use longer and thinner bolometer legs to decrease
the bolometer thermal conductance. We consequently modify the heat capacity in contact with the transition edge
sensor to tune the time-constant of the detector. We finally discuss cold inductor-capacitor chips operated at 4 K toread out the detectors with frequency domain multiplexing electronics that has a multiplexing factor of 105, which is
60% larger than the highest factor used to date with this readout system.
category : Sensor Physics & Developments170

PA-44 Does membrane strain impact the TES transition surface?
Felix T Jaeckel1 , C V Ambarish2 , Megan Eckart3 , Rachel Gruenke4 , Kari L Kripps5 , Dan McCammon6 , Dallas
Wulf7 , Shuo Zhang8 , Yu Zhou9
1

University of Wisconsin - Madison, 2 University of Wisconsin - Madison , 3 NASA Goddard Space Flight Center , 4 Universityof Wisconsin - Madison , 5 University of Wisconsin - Madison , 6 University of Wisconsin - Madison , 7 University of Wisconsin Madison , 8 Institute for High Energy Physics , 9 University of Wisconsin - Madison

Recently, we have shown that uniaxial strain can shift the transition temperature of Mo by about 0.3K/(unit strain).
Additionally, we have observed small strain induced changes in critical current. The implications of this finding onpractical transition edge sensor devices depend on two questions: 1) How big are the strains encountered in real world
devices, and 2) how does a strain induced change in Tc or Ic impact the resistive transition surface and thus device
operation?
To answer the first question we use an optical technique to measure the curvature of TES fabricated on membranes
and estimate the magnitude of the strains present in such devices.
The second question, however, is more diﬃcult to address: the transition surface of typical devices shows asignificant amount of structure commonly attributed to weak-leak eﬀects. It is conceivable that local modulation ofstrain and Tc may lead to substantial qualitative changes in these important details of the transition surface. Since nodetailed physical model has been proposed to predict these features, we attempt to tackle this problem experimentally.
To this end, we are investigating methods to systematically modulate the strain field on a membrane.
category : Sensor Physics & Developments

171

PA-45 Optical Characterization of the SPT-3G Focal Plane
Zhaodi Pan1 , SPT-3G collaboration SPT-3G collaboration2
1

Department of Physics, Kavli Institute for Cosmological Physics, The University of Chicago, 2 The institutions thatcollaborate for SPT-3G

The third-generation South Pole Telescope camera (SPT-3G) is designed to measure the Cosmic Microwave Background(CMB) across three frequency bands (90, 150 and 220 GHz) with 16,000 transition-edge sensor (TES) bolometers.
Each multichroic pixel on a detector wafer has a broadband sinuous antenna that couples power to six TESs, one foreach of the three observing bands and each polarization, via lumped element filters. Ten detector wafers populate thefocal plane, which is coupled to the sky via a large-aperture optical system. Here we present optical characterization of
the cryogenic detectors and outline our testing set up. In particular we focus on frequency band characterization done
via Fourier Transform Spectrometry, optical time constant, beam properties, and optical and polarization eﬃcienciesof these detectors.
category : Sensor Physics & Developments

172

PA-46 Spectroscopic measurements of L X-rays with a TES microcalorimeter for a
non-destructive assay of transuranium elements
Keisuke Nakamura1 , Keisuke Maehata2 , Tetsuya Sugimoto3 , Yu Kiguchi4 , Naoko Iyomoto5 , Yuki Morishita6 , Koji
Takasaki7 , Kazuhisa Mitsuda8
1

Nuclear Fuel Cycle Engineering Laboratories, Japan Atomic Energy Agency , 2 Kyushu University , 3 Kyushu University ,4
Kyushu University , 5 Kyushu University , 6 Japan Atomic Energy Agency , 7 Japan Atomic Energy Agency , 8 Japan
Aerospace Exploration Agency

Because L X-rays of the energy ranging from 10 keV to 25 keV are emitted following internal conversion after the
α-decay of TRU elements, spectroscopic measurement of L X-ray is one of important techniques for a non-destructive
assay of transuranium (TRU) elements. High purity germanium (HPGe) semiconductor detectors have been used inspectroscopic measurement of L X-rays emitted from TRU elements so far. However, the accurate identification of L
X-ray peaks is diﬃcult due to the insuﬃcient energy resolution of the HPGe detector. For identification of L X-ray
peaks of TRU elements, the energy resolution of the detector is required to be better than 100 eV of the full width at
half maximum (FWHM).
In this work, a transition-edge-sensor (TES) microcalorimeter was operated for spectroscopic measurements of L
X-rays emitted from a Np-237 and Cm-244 sources. The Au absorber of 5 µm thick was deposited on the TES toprovide absorption eﬃciency from 35 to 80 % for incident X-ray photons with the energy from 10 to 30 keV. Energy
spectra of L X-rays were obtained by processing detection signal pulses with using an optimal filtering method. Typical
L X-ray peaks of Pa, U and Pu elements were clearly identified in the obtained energy spectra. In peak fittings, naturalline width of L X-ray emission and an impulse response of the detector was approximated by Lorentzian distribution
and Gaussian distribution, respectively. The FWHM energy resolution of the TES microcalorimeter was obtained to
be 32.7 eV at Pu L α1 X-ray peak of 14.28 keV with natural line width of 12.20 eV. We considered a feasibility of anon-destructive assay of TRU elements with experimental L X-ray spectra obtained by the TES microcalorimeter.
Acknowledgement
This work was financially supported by a Grant-in-Aid for Scientific Research (B) (24360397) from the Japan
Society for the Promotion of Science.
category : Sensor Physics & Developments

173

PA-47 Performance of an X-ray absorber on a transition edge sensor for
Athena/X-IFU
Kenichiro Nagayoshi1 , Marcel Ridder2 , Marcel Bruijn3 , Pourya Khosropanah4 , Cor de Vries5 , Luciano Gottardi6 ,Jian-Rong Gao7
1

SRON, 2 SRON , 3 SRON , 4 SRON , 5 SRON , 6 SRON , 7 Delft University of Technology

Cryogenic calorimetric sensors using a transition edge (TES) given by a super conducting film are known as one ofthe promising devices for future satellite missions thanks to their major breakthrough in sensitivities. Athena is an
ESA-driven X-ray observatory to be launched in 2028, with the aim of high resolution spectroscopy enabling us to
explore new horizons of science themes on the hot and energetic universe. X-ray Integral Field Unit (X-IFU) is an
instrument consisting a large array of the TES calorimeter designed to be oﬀering 2.5 eV spectral resolution with a
5 image pixel, corresponding to the pixel size of 250 µm square.
Thermal properties of the X-ray absorber coupled on a part of the TES thermometer play important roles to achieverequirements for the X-IFU. We have improved electroplating techniques for a few microns thick gold and bismuth,which can be used as heat thermalization and X-ray stopping layers in the absorber respectively. The typical resistivityof 1 micron thick gold at 4 Kelvin is 0.1 µΩ cm, corresponding to the residual resistance ratio of 24 which is limited bysurface scattering. The bismuth films are well dense and flat with the crystalline structure. We have integrated theseprocesses into the X-ray TES device fabrication with optimization of photolithography and demonstrated free-standing
full-size absorbers with a pixel gap of a few microns, which meet requirements for the X-IFU such as high filling factor
and quantum eﬃciency above 95 %.
We will present details of fabrication and discuss performances of X-ray absorbers based on the X-ray pulse analysis.
Acknowledgement: This work is partly funded by European Space Agency (ESA) and coordinated with other
European eﬀorts under ESA CTP contract ITT AO/1-7947/14/NL/BW.

category : Sensor Physics & Developments

174

PA-48 Development of cryogenic single photon TES detectors for an Investigation of
the VUV region.
Valentina Ceriale1 , Flavio Gatti2 , Matteo De Gerone3 , Michele Biasotti4 , Giovanni Gallucci5 , Daniele Grosso6
1

Physics Department University of Genoa, 2 Universita degli studi di Genova / INFN Sez. di Genova , 3 INFN Sez. di Genova ,4
Universita degli studi di Genova , 5 INFN Sez. di Genova , 6 Universita degli studi di Genova / INFN Sez. di Genova

Deep UV energy range (10 eV-30 eV) is very interesting for astrophysics spectrometry and quantum information.
In our work we want to investigate the possibility to use cryogenic TES-microcalorimeters for single photon detection in the VUV range. Small and quick detectors should be developed in order to increase the VUV photon peaks
resolution.
TES microcalorimeters are fully fabricated with photolithographic techniques in the clean room facility inside the
Low Temperature Detector Laboratory of the University of Genova. The TESs are 100 nm Ir films deposited by Pulsed
Laser Deposition (PLD). The absorbers are made of gold and are directly set on the TES.
The Ir TES detectors are tested in our 3He-4He dilution refrigerator Oxford Kelvinox-25, on high temperaturestability cold finger whose base temperature is 50 mK. The working temperature of Ir TES is around 100 mK. The
signal readout is performed by a VTT SQUID with Magnicon electronics for I-V curves. A lock-in amplifier with 4probe measurement is used for ancillary R(T) transition measurements.
We excite the microcalorimeter with a UV pulsed laser light source, by using an optical fiber. The pulse response intime is registered. Fast microcalorimeters have been developed, realized and tested in the Low Temperature Laboratoryof the University of Genoa. The latest results are shown.
category : Sensor Physics & Developments

175

PA-49 Mapping the TES Temperature and Current Sensitivities as a Function of
Current, Magnetic Field and Temperature with IV Curve and Complex Impedance
Yu Zhou1 , Felix T Jaeckel2 , C V Ambarish3 , Megan Eckart4 , Rachel Gruenke5 , Kari L Kripps6 , Dan McCammon7 ,Dallas Wulf8 , Shuo Zhang914

Physics Department, University of UW-Madison, 2 University of Wisconsin-Madison , 3 University of Wisconsin-Madison ,University of Wisconsin-Madison , 5 University of Wisconsin-Madison , 6 University of Wisconsin-Madison , 7 University of
Wisconsin-Madison , 8 University of Wisconsin-Madison , 9 Institute for High Energy Physics

To resolve the spectra of the astronomical diﬀuse X-ray background in the 0.1-0.5 keV energy range, we need large
area pixels (∼1mm2 ) with excellent energy resolution (1–2 eV). The energy resolution of a micro-calorimeter with a√√resistive thermometer is ideally ∼ 7 (kB T2 C (1+2β)/α). For TES pixels with large absorbers that have relatively
high heat capacity, high α and low β are needed to achieve the required energy resolution. But most work in thefield has found high α to be correlated with high β and also with excess noise, with the cause of this correlation
remaining not understood.
To investigate this correlation, we have been mapping the resistance R(T, I, Bext) surface of TES devices over theentire transition region, calculaing α and β from the derivatives of the IV curves.Admittance (A(f)) measurements
could provide a more eﬃcient way to map α and β that would allow characterization of a large number of devices.
We are currently performing this complementary measurement to see if the results agree with those obtained from IV
curves. We have also begun measuring noise spectra at promising operating points on the R(T, I, Bext) surface todetermine weather excess noise is an unavoidable accompaniment of high α.
category : Sensor Physics & Developments176

PA-50 Performance of an X-ray microcalorimeter with a 0.24 mm absorber and a 50
um TES bilayer
Antoine R. Miniussi1 , Joseph S. Adam2 , Simon R. Bandler3 , James A. Chervenak4 , Aaron M. Datesman5 , Megan E.
Eckart6 , Audrey J. Ewin7 , Fred M. Finkbeiner8 , Richard L. Kelley9 , Caroline A. Kilbourne10 , Frederick S. Porter11 ,John E. Sadleir12 , Kazuhiro Sakai13 , Stephen J. Smith14 , Nicholas A. Wakeham15 , Edward J. Wassell16 , Wonsik
Yoon171

NASA/GSFC, 2 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 3 NASA
Goddard Space Flight Center , 4 NASA Goddard Space Flight Center , 5 NASA Goddard Space Flight Center / SGT, Inc. ,6NASA Goddard Space Flight Center , 7 NASA Goddard Space Flight Center , 8 NASA Goddard Space Flight Center / Wyle
Information Systems , 9 NASA Goddard Space Flight Center , 10 NASA Goddard Space Flight Center , 11 NASA Goddard Space
Flight Center , 12 NASA Goddard Space Flight Center , 13 NASA Goddard Space Flight Center / CRESST II - University of
Maryland Baltimore County , 14 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore
County , 15 NASA Goddard Space Flight Center / NPP - Universities Space Research Association , 16 NASA Goddard Space
Flight Center / SGT, Inc. , 17 NASA Goddard Space Flight Center / NPP - Universities Space Research Association

We have been developing superconducting transition-edge sensor (TES) microcalorimeters for a variety of potential
astrophysics missions, including Athena. The X-ray Integral Field Unit (X-IFU) instrument on this mission requires
close-packed pixels on a 0.25 mm pitch, and high quantum eﬃciency between 0.2 and 12 keV. The traditional approachwithin our group has been to use square TES bilayers of molybdenum and gold that are between 100 and 140 microns in
size, deposited on silicon nitride membranes to provide a weak thermal conductance to a 50 mK heat bath temperature.
It has been shown that normal metal stripes on top of the bilayer are needed to keep the noise consistent with thespectrum expected from the electrothermal model and estimates of the near-equilibrium non-linear Johnson noise.
In this work we describe a new approach in which we use a square TES bilayer that is 50 microns in size. While thesuperconducting weak link eﬀect is much stronger in this size of TES, we have found that excellent spectral performancecan be achieved without the need for any normal metal stripes on top of the TES. A spectral performance of 1.58
eV at 6 keV has been achieved, the best resolution seen in any of our devices with this pixel size. The absence of
normal metal stripes has lead to more uniform transition shapes, and more reliable excellent spectral performance.
The smaller TES size has meant that that the thermal conductance to the heat bath, determined by the perimeter
length of the TES and the membrane thickness, is lower than on previous devices, and thus has a lower count ratecapability. This is an advantage for low count-rate applications where the slower speed enables easier multiplexing
in the read-out, thus potentially higher multiplexing factors. In order to recover the higher count rate capabilities, apotential path exits using thicker silicon nitride membranes to increase the thermal conductance to the heat bath.
category : Sensor Physics & Developments

177

PA-51 Exploration of alternative Transition Edge Sensor materials for the SPT-3G
experiment
Clarence L Chang1 , SPT-3G collaboration2
1

Argonne National Lab/KICP University of Chicago, 2 multi-institution collaboration

The SPT-3G focal plane targets detector saturation powers in the range of 10-20 pW, which can be achieved withTransition Edge Sensors (TES) having Tc in the range of 400-500 mK. The baseline TES material for the SPT-3G
focal plane are bilayers and multi-layers using Ti and Au. In addition to the Ti/Au materials, we have also exploredalternative TES materials including ion-implanted materials like Al-Mn and Mo-Cu. For Al-Mn, we have investigatedfabrication techniques using either lift-oﬀ and a dry etch processing. In this work, we present some results from ourstudies of these alternative TES materials.
category : Sensor Physics & Developments

178

PA-52 Transition edge sensor (TES) array for astrophysical observations
Guanhua Gao1 , Kamal Ahmad2 , Zhengwei Li3 , Jie Liu4 , Qichun Liu5 , Jianshe Liu6 , Wei Chen7
1

Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, 2 Tsinghua National Laboratory for Information
Science and Technology, Department of Microelectronics and Nanoelectronics; Institute of Micro electronics, Tsinghua
University , 3 Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences ,4
Tsinghua National Laboratory for Information Science and Technology, Department of Microelectronics and Nanoelectronics;
Institute of Micro electronics, Tsinghua University , 5 Tsinghua National Laboratory for Information Science and Technology,
Department of Microelectronics and Nanoelectronics; Institute of Micro electronics, Tsinghua University , 6 Tsinghua National
Laboratory for Information Science and Technology, Department of Microelectronics and Nanoelectronics; Institute of Microelectronics, Tsinghua University , 7 Tsinghua National Laboratory for Information Science and Technology, Department ofMicroelectronics and Nanoelectronics; Institute of Micro electronics, Tsinghua University

We present a design and fabrication process of transition edge sensor (TES) array for astrophysical observations.
The fabricated prototypes contain Al TES array with transition temperature at 1.2K, in which the TES islands aresupported by Si3N4 holders. The low temperature performance of the TES array is measured in a He3 sorption
refrigerator, such as the resistance -temperature curve. We designed diﬀerent structure for connecting TES andantenna to detect the irradiation from the optical window.
category : Sensor Physics & Developments179

PA-53 Fabrication and Characterization of Al/Ti bilayer Transition Edge Sensor
Bolometer Array
Kamal Ahmad1 , Guanhua Gao2
1

Institute of Microelectronics,Tsinghua University Beijing China, 2 Institute of High Energy Physics

We present design and development of transition edge sensor (TES) bolometer array for astrophysical observations
and the low noise, low impedance and low power of superconductor quantum inference device (SQUID) make it more
ideal amplifier signal condition. We have fabricated 4x4 TES bolometer array that based on Al/Ti bilayer withtransition temperature at most 1.2 K the layout design is given in figure1. Our bolometers are established on Si3N4
membrane technology for the thermal link as shown in figure3(c). A TES is described, that should enable the readoutof the bolometer operated at 4.2 K using a room temperature amplifier without a significant degradation in noise
performance. We also focus on the voltage-biased TES, which is feasible in strong negative electrothermal feedback(ETF) for improved linearity.
Keywords: TES, SQUID, ETF.
category : Sensor Physics & Developments

180PA-54 Development of a small pixel Ir-TES for optical applications
Yoshitaka Miura1 , Tomoya Irimatsugawa2 , Yuya Ishii3 , Masashi Ohno4 , Hiroyuki Takahashi5
1

University of Tokyo, 2 University of Tokyo , 3 University of Tokyo , 4 University of Tokyo , 5 University of Tokyo

We aim to realize a single-photon detector which greatly improves its sensitivity and response speed by minimizing of
the thermometer volume using a single superconducting Ir thin film. Iridium has a sharp superconducting transitionat 112 mK in bulk, therefore, even if it is used as a single superconducting thin film for the thermometer of TES,
excellent energy resolution is expected.
Under this concept, we fabricated 5 to 25 μ m size small pixel Ir-TES for single-photon detector. In this presentation, we will introduce the result in our first small pixel Ir-TES device (10 μ m size, 20 nm thickness, Fig.1). In the
I-V characterization, two transition regions and two normal regions were observed. Resistance of each normal region
was estimated at approximately 3 and 6 ohms respectively. We consider that it is because the contact area between
Ir-TES and niobium electrode is wide, but this is under investigation. Also, now we plant to perform the photon
irradiation experiment using this small pixel Ir-TES.

category : Sensor Physics & Developments

181

PA-55 Understanding and Manipulating the Thermal Conductance of SiN
Membranes in Sub-Kelvin Refrigerators and Sensors
Xiaohang Zhang1 , Peter Lowell2 , Joel Ullom3
1

NIST, 2 NIST , 3 NIST / University of Colorado, Boulder

Ultra-sensitive cryogenic detectors, like Transition-Edge Sensors (TESs), that operate at sub-Kevin temperatures
are critical for understanding the structure and origins of the universe. Refrigeration to sub-Kelvin temperatures
remains costly, bulky, and complex. A new refrigeration technique using Normal-Insulator-Superconductor (NIS)
tunnel junctions has been developed to provide an economical, light, and compact solution to reach temperatures near
100 mK. In previous work, we demonstrated a copper platform with over 150 g of mass and 28 cm2 of area for attachinguser-supplied devices cooled by NIS tunnel junction refrigerators from 291 mK to 233 mK and infer cooling to 228
mK [1]. The thermal isolation provided by micromachined SiN membranes plays an important role in a variety ofdevices including these tunnel junction refrigerators and TES bolometers. To improve the performance of NIS tunnel
junction refrigerators and TESs, a better understanding of the SiN membranes thermal conductance is desirable.
The design of SiN membranes often balances the level of thermal isolation against mechanical robustness. To achieve
greater thermal isolation while preserving robustness, we are exploring the impact of surface roughness and additional
patterned features on the thermal conductivity of SiN membranes. We are conducting this study as a functionof membrane thickness and temperature. Techniques to suppress the thermal conductivity of SiN membranes haveobvious applications for TES bolometers whose Noise-Equivalent-Powers (NEPs) depend sensitively on this parameter.
The base temperature of refrigerators based on NIS tunnel junctions designed to cool the phonons of a payload also
depends on membrane conductance. We have demonstrated that the thermal conductance of SiN membranes can be
reducing using several techniques including: (1) depositing normal metal islands on the membrane; (2) cutting holes
in the membrane; (3) using meandering legs. We attempt to explain our results using contemporary theory for phonontransport [2].
[1] X. Zhang, P. J. Lowell, B. L. Wilson, G. C. O’Neil, J. N. Ullom ? Phys. Rev. Applied, 4, 024006 (2015).
[2] T. Kuhn, Phononic Transport in Dielectric Membranes, doctoral thesis, University of Jyvaskyla (2007)
category : Sensor Physics & Developments

182

PA-56 A low nuclear recoil energy threshold for dark matter search with CRESST-III
detectors
Michele Mancuso1 , on behalf of the CRESST collaboration2
1

Max-Planck-Institut fur Physik, 2 Max-Planck-Institut fur Physik, D-80805 Munchen, Germany / INFN, Laboratori Nazionali
del Gran Sasso, I-67010 Assergi, Italy / Physik-Department and Excellence Cluster Universe, Technische Universitat
Munchen, D-85747 Garching, Germany / Institut fur H

The CRESST-III experiment (Cryogenic Rare Events Search with Superconducting Thermometers), located at theunderground facility Laboratori Nazionali del Gran Sasso in Italy, uses scintillating CaWO4 crystals as cryogenic
calorimeter to search for direct dark matter interaction in detectors.
Detecting dark matter particles is one of the most exciting experimental challenges of modern astroparticle physics.
A large part of the parameter space for spin-independent scattering oﬀ nuclei remains untested for dark matter particles
with masses below few GeV, despite many naturally motivated theoretical models for light dark matter.
The CRESST-III detectors are designed to achieve the performance required to probe the low mass region of theparameter space with a sensitivity never reached before.
Each detector consists of a scintillating crystal of ∼ 25 g and a second smaller nearby cryogenic calorimeter madeof Silicon-On-Sapphire for the detection of the scintillating light. Both calorimeters are equipped with Transition Edge
Sensors (TES) for read-out, designed to provide thresholds of the order of 50-100 eV for the CaWO4 crystals and 10-20
eV for the Silicon-On-Sapphire detectors. The double channel read-out allows event-by-event particle identification
which is used for background suppression. In addition, the CRESST-III detectors are also equipped with a fully
scintillating housing and instrumented holders to veto a possible background originating from surrounding surfaces.
This innovative active holding system allows to suppress induced thermal signals from particle interaction in theholding material.
In this talk, new results on the performance and a complete overview of the CRESST-III detectors will be presented,
emphasizing the current status and future perspectives of Phase 1 that started taking data in August 2016.
category : Sensor Physics & Developments

183

PA-57 Two-Dimensional Spatial Imaging of Charge Transport in Silicon at Low
Temperature
Robert A Moﬀatt1 , Blas Cabrera2 , Noah Kurinsky3 , James Allen4 , Peter Redl5 , Brendan Corcoran6 , Fedja
Kadribasic7 , Benjamin Shank8 , Betty Young9 , Matthew Cherry10 , John Mark Kreikebaum11 , Astrid Tomada12 , Kyle
Sundqvist13 , Bernard Sadoulet14 , Daniel Brandt15 , Paul Brink16
1

Department of Physics, Stanford University, 2 Stanford University , 3 Stanford University / SLAC National Accelerator
Laboratory , 4 Stanford University , 5 Stanford University , 6 Stanford University , 7 Stanford University , 8 Stanford University ,9
Stanford University / Santa Clara University , 10 SLAC National Accelerator Laboratory , 11 Stanford University , 12 SLAC
National Accelerator Laboratory , 13 University of California, Berkeley , 14 University of California, Berkeley , 15 SLAC National
Accelerator Laboratory , 16 SLAC National Accelerator Laboratory

The Cryogenic Dark Matter Search (CDMS) is a direct-detection dark matter experiment which employs high-purity
silicon and germanium crystals as dark matter detectors. Accurate modeling of charge transport in these materials isessential for improving our data analysis and detector design.
This experiment produces a two-dimensional image of charge density, which allows electron and hole transport insilicon and germanium to be studied in detail at sub-kelvin temperatures and in electric fields of strength between
0.5 and 6 V/cm. We have demonstrated anisotropic behavior in both electron and hole propagation, which varies asa function of temperature and applied electric field. We present these experimental results, along with Monte Carlosimulations which reproduce the observed behavior.
category : Sensor Physics & Developments

184

PA-58 Progress on SuperSpec
Jordan Wheeler1 , Steve Hailey-Dunsheath2 , Erik Shirokoﬀ3 , Peter Barry4 , Charles M Bradford5 , Scott Chapman6 ,George Che7 , Jason Glenn8 , Matthew Hollister9 , Attila Kovacs10 , Henry G Leduc11 , Philip Mauskopf12 , Ryan
McGeehan13 , Christopher M McKenney14 , Roger O’Brient15 , Stephen Padin16 , Theodore Reck17 , Colin Ross18 ,Corwin Shiu19 , Carole Tucker20 , Ross Williamson21 , Jonas Zmuidzinas22
1

CASA University of Colorado Boulder, 2 California Institute of Technology, 1200 E. California Blvd, Mail Code 301-17,
Pasadena 91125, USA , 3 Department of Astronomy & Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago,
IL 60637, USA , 4 Department of Astronomy & Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL
60637, USA , 5 California Institute of Technology, 1200 E. California Blvd, Mail Code 301-17, Pasadena 91125, USA / Jet
Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA , 6 Department of Physics and Atmospheric Science,
Dalhousie University, Coburg Road, Halifax NS B3H 1A6, Canada , 7 School of Earth and Space Exploration and Departmentof Physics, Arizona State University, Tempe, AZ 85287, USA , 8 Center for Astrophysics and Space Astronomy, University ofColorado Boulder, 2000 Colorado Avenue, Boulder 80309, USA , 9 California Institute of Technology, 1200 E. California Blvd,
Mail Code 301-17, Pasadena 91125, USA , 10 California Institute of Technology, 1200 E. California Blvd, Mail Code 301-17,
Pasadena 91125, USA / Institute for Astrophysics, University of Minnesota, 116 Church St SE, Minneapolis, MN 55455, USA, 11 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA , 12 School of Earth and Space Exploration
and Department of Physics, Arizona State University, Tempe, AZ 85287, USA , 13 Department of Astronomy & Astrophysics,
University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA , 14 National Institute of Standards and Technology,
325 Broadway, Boulder, CO 80305, USA , 15 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA ,16
California Institute of Technology, 1200 E. California Blvd, Mail Code 301-17, Pasadena 91125, USA , 17 Jet Propulsion
Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA , 18 Department of Physics and Atmospheric Science, Dalhousie
University, Coburg Road, Halifax NS B3H 1A6, Canada , 19 California Institute of Technology, 1200 E. California Blvd, Mail
Code 301-17, Pasadena 91125, USA , 20 School of Physics & Astronomy, Cardiﬀ University, 5 The Parade, Cardiﬀ CF24 3AA,
UK , 21 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA , 22 California Institute of Technology,
1200 E. California Blvd, Mail Code 301-17, Pasadena 91125, USA

SuperSpec is an exciting new technology for millimeter and submillimeter spectroscopy. It is an on-chip spectrometer
being developed for multi-object, moderate resolution (R = 100?500), large bandwidth survey spectroscopy of highredshift galaxies for the 1 mm atmospheric window. In particular it targets the CO ladder in the redshift range ofz = 0 to 4 and the [CII] 158 um line from redshift z = 5 to 9. SuperSpec employs a novel architecture in which
detectors are coupled to a series of resonant filters along a single microwave feedline instead of using dispersive optics.
This construction allows for the creation of a full spectrometer occupying only 10 cm squared of silicon. This is areduction in size of several orders of magnitude when compared to standard grating spectrometers. This small profile
enables the production of future multi-object spectroscopic instruments required as the millimeter-wave spectroscopy
field matures.
SuperSpec receives astrophysical radiation via a lens-coupled antenna. This radiation then propagates down amicrostrip transmission line where specific frequencies of radiation are picked oﬀ by proximity coupled half wavelength
microstrip resonators. Careful tuning of the proximity of the resonators to the feedline dials in the desired resolving
power of the SuperSpec filterbank by tuning the coupling quality factor. The half wavelength resonators are then inturn coupled to the inductive meander of kinetic inductance detectors (KIDs), which serve as the power detectors for
the SuperSpec filterbank. Each SuperSpec filter bank contains hundreds of KIDs and the natural multiplexibility ofthese detectors allow for readout of the large numbers of required detectors. SuperSpec employs titanium nitride TiN
KIDs. The unique coupling scheme employed by SuperSpec allows for the creation of incredibly low volume, highresponsivity, TiN KIDs. Current inductor volumes are of order 2 cubic microns. Since responsivity is proportional
to the inverse of quasiparticle-occupied volume this allows SuperSpec to reach the low NEPs required by moderate
resolution spectroscopy to be photon limited from the best ground-based observing sites.
We will present the latest results from SuperSpec prototype devices and ongoing progress toward the deploymentof a SuperSpec demonstration instrument covering the full 1 mm atmospheric band in Spring 2018. In particular
NEPs, measured filter bank eﬃciency, and spectral profiles for a 50-channel filterbank prototype will be presented.
This includes the results of new detector design changes. Such as, detector NEP values for newly reduced inductor
volumes of 2 cubic microns from 9 cubic microns of the previous generation prototype devices. In addition we havetested capping the interdigitated capacitor of the kinetic inductance detectors with niobium to reduce the parasitic
inductance in the capacitor rails. Also the optical properties of our new wide band dual slot bowtie antenna will bepresented. Finally, we will report on our system end to end eﬃciency and total system NEP.
category : Sensor Physics & Developments

185

PA-59 MgB2 hot-electron bolometer mixers for sub-mm wave astronomy
Evgenii Novoselov1 , Sergey Cherednichenko2
1

Department of Microtechnology and Nanoscience, Chalmers University of Technology, 2 Chalmers University of Technology

The terahertz range (0.1-10THz) of electromagnetic spectrum is of the great interest for astronomical observations dueto the presence of large amount of various emission lines. The study of these lines allows for investigation of physics,
chemistry and dynamics of various remote space objects. Heterodyne receivers with their high spectral resolution(106-107) are required in order to benefit from astronomical observations in THz range. For frequencies above 1THz
phonon-cooled hot-electron bolometers (HEBs) are devices of the first choose for heterodyne instrument s mixers.
The currently used NbN and NbTiN HEB mixers are suﬀering from a relatively small noise bandwidth (NBW) of
about 4GHz. It sets the limitation on study of some extra-galactic objects which Doppler-shifted emission lines could
be as few GHz wide. Such wide lines could be then observed only been divided into two scans, which doubles required
observation time.
We have managed to improve the bandwidth of HEB mixers without sensitivity sacrificial by using MgB2 superconducting ultrathin films grown by hybrid physical chemical vapor deposition (HPCVD) technique. Both a highTc (short electron-phonon interaction time) and a small thickness (short phonon escape time) are crucial for large
bandwidth achievement. Using this deposition method films as thin as 5-10nm with a critical temperature (Tc) above
30K were grown. A NBW of 11GHz was measured for HEBs with a Tc of 30K fabricated from an 8nm thick film,
and a NBW of 13GHz was measured for HEBs with a Tc of 33K fabricated from a 5nm thick film. The DSB receivernoise temperature of such devices measured at a 5K bath temperature is about 1000K at 0.69THz and 1.69THz local
oscillators (LOs). The HEBs can operate at bath temperatures up to 20-25K without significant increase of the noise
temperature. The main reason for the noise temperature increase at higher temperatures is a reduction of the mixer
gain, which occurs proportionally to the LO power reduction while the mixer output noise remains constant. Device
current-voltage (IV) characteristics are identical when pumped with LOs from 0.69 THz to 2.56 THz, and match wellwith IV curves at elevated temperatures. Therefore, the eﬀect of the THz waves on the mixer is totally thermal, due toabsorption in the π conduction band of MgB2. The MgB2 HEB mixer noise temperature was found to be proportional
to the device width, and we expect it to be further decreased if HEBs wider than 1 μ m would be fabricated andanti-reflection coating would be applied.
Fig. 1. The receiver noise (at 1.63 THz LO) as a function of the IF recorded at 5K, 15K, and 20K operation
temperatures.
category : Sensor Physics & Developments

1.2(Broadband Channel After)/(Broadband Channel Before Filter Bank)(Spectral Channels)/(Broadband Channel Before Filter Bank)

1.0

Normalized Power

0.8
0.6
0.4
0.2
0.0
220

230

240

250
Frequency (GHz)

186

260

270

280

PA-60 Integrated SQUID/sensor designs for metallic magnetic microcalorimetry
Stephen T. P. Boyd1 , Ruslan Hummatov2 , Geon Bo Kim3 , John Ad Hall4 , Robin C Cantor5 , Stephan Friedrich6
1

Department of Physics and Astronomy, University of New Mexico, 2 Department of Physics and Astronomy, University of
New Mexico , 3 Lawrence Livermore National Laboratory , 4 STAR Cryoelectronics , 5 STAR Cryoelectronics , 6 Lawrence
Livermore National Laboratory

Metallic magnetic microcalorimeters (MMCs) achieve energy resolution performance comparable to transition-edge
sensors (TESs) while relying on very diﬀerent measurement physics. One consequence of MMC physics of current interest is the improved linearity of MMC pixels over a wide energy range compared to TES. We have recently completed
fabrication of new low-pixel-count (14 pixels, 7 SQUIDs) MMC gamma-ray detector arrays using several exploratory
integrated SQUID/sensor designs. Integration of the SQUID and sensing coil on the same chip allows optimal inductance matching and control of stray reactances. These designs use diﬀerent combinations of one-layer/two-layer
sensing coils and direct/flux-transformer coupling of the input circuits. All designs use the superconducting cap
geometry to keep the magnetizing field in-plane and lower sensing coil inductance. Passive Nb:Ta alloy (Tc = 5.3 K)
persistent-current shunts, described in a previous report, are used throughout the chip both for trapping persistentmagnetizing currents as well as for blocking unwanted induced persistent currents. We describe the motivations,tradeoﬀs, and measured performance of these exploratory designs.
category : Sensor Physics & Developments

187

PA-61 Metallic magnetic calorimeter optimization for large-area light detectors
Seung-Yoon Oh1 , Yong-Hamb Kim2 , Hyelim Kim3 , Inwook Kim4 , Sora Kim5 , Hyejin Lee6 , Minkyu Lee7
1

Dept. of Physics and Astronomy, Sejong University, 2 Center for Underground Physics (CUP), Institute for Basic Science(IBS) / Korea Research Institute of Standards and Science (KRISS) , 3 Center for Underground Physics (CUP), Institute for
Basic Science (IBS) , 4 Center for Underground Physics (CUP), Institute for Basic Science (IBS) , 5 Center for UndergroundPhysics (CUP), Institute for Basic Science (IBS) , 6 Center for Underground Physics (CUP), Institute for Basic Science (IBS) ,7
Korea Research Institute of Standards and Science (KRISS)We report on an optimization study for large-area light detectors using metallic magnetic calorimeters (MMCs). The
detectors are to be used for light detection in simultaneous phonon-scintillation measurement for rare event searchexperiments.
The present detectors are composed of a 2-inch Ge wafer as an absorber and an MMC as a temperature sensor.
We studied the dependence of signal amplitudes to MMC and SQUID parameters. The erbium concentration, size ofmeander-shaped pick-up coil, field current, SQUID input and mutual inductances were subjected to change maximizing
the signal size. Measured results are compared with calculation.
category : Sensor Physics & Developments

188

PA-62 BRAHMS: POLARIZATION SENSITIVE BOLOMETER ARRAYS FOR
THE SPICA IMAGING POLARIMETERLouis R Rodriguez1 , Albrecht Poglitsch2 , Vincent Reveret3 , Didier Dubreuil4 , Abdelkader Aliane5 , Olivier Gevin6 ,Bruno Maﬀei7 , Xavier De la Broise8 , Jerome Martignac9 , Lionel Duband10 , Valerie Goudon11 , Wilfried Rabaud12 ,Ivan Charles13 , Christophe Cara14 , Cyrille Delisle15 , Obaid Adami16 , Sophie Bounissou17 , Agnes Arnaud18 , Laurent
Dussopt19 , Amin Rhouni20 , Jean-Luc Sauvageot21
1

Departement d’Astrophysique IRFU/CEA- Universite Paris Sacalay, France, 2 Departement d’Astrophysique
UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France / Max-Planck-Institut fur extraterrestrische Physik, Garching bei
Munchen, Germany , 3 Departement d’Astrophysique UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France , 4 Departementd’Astrophysique UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France , 5 Laboratoire d’Electronique et de Technologie del’Information/DOPT/CEA-Grenoble, France , 6 Service d’Electronique des detecteurs et d’Informatique/IRFU-CEA/Universite
Paris-Saclay, France , 7 Institut d’Astrophysique Spatiale Universite Paris-Saclay, France , 8 Service d’Electronique desdetecteurs et d’Informatique/IRFU-CEA/Universite Paris-Saclay, France , 9 Departement d’Astrophysique
UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France , 10 Service des Basses Temperatures INAC/CEA-Grenoble, France ,11
Laboratoire d’Electronique et de Technologie de l’Information/DOPT/CEA-Grenoble, France , 12 Laboratoire d’Electronique
et de Technologie de l’Information/DOPT/CEA-Grenoble, France , 13 Service des Basses Temperatures INAC/CEA-Grenoble,
France , 14 Departement d’Astrophysique UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France , 15 Departementd’Astrophysique UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France , 16 Departement d’Astrophysique
UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France , 17 Departement d’Astrophysique UMR-AIM/IRFU-CEA/Universite
Paris-Saclay, France , 18 Laboratoire d’Electronique et de Technologie de l’Information/DOPT/CEA-Grenoble, France ,19
Laboratoire d’Electronique et de Technologie de l’Information/DOPT/CEA-Grenoble, France , 20 Service d’Electronique desdetecteurs et d’Informatique/IRFU-CEA/Universite Paris-Saclay, France , 21 Departement d’Astrophysique
UMR-AIM/IRFU-CEA/Universite Paris-Saclay, France

We develop bolometer arrays, with pixel polarimetric capability, to be used in the polarization sensitive camera for the
SPICA Space Observatory, a joint JAXA/ESA mission. The detectors are based on the resistive all silicon technology
initially elaborated for the Herschel/PACS photometer. With our new design, each pixel will output total flux andfully diﬀerential polarization signals. The camera covers a 2.6 arcmin FOV simultaneously at three wavelengths (100,200 and 350 μ m) with Nyqvist sampling. The 1334 pixels (5336 bolometers) are operated around 50 mK to achievea sensitivity of few aW/√ Hz. The three Stokes parameters I, Q and U are retrieved by the specific arrangement of
the focal plane and a rotating half wave plate located near the Camera optical input.
category : Sensor Physics & Developments

189

PA-63 Wavelength dependence of intrinsic detection eﬃciency for NbN
superconducting nanowire single-photon detector
Hao Li1 , Lixing You2 , Yong Wang3 , Zhen Wang4
1

Shanghai Institute of Microsystem and Information Technology, Chinese Academy of Sciences , 2 Shanghai Institute ofMicrosystem and Information Technology, Chinese Academy of Sciences , 3 Shanghai Institute of Microsystem and Information
Technology, Chinese Academy of Sciences , 4 Shanghai Institute of Microsystem and Information Technology, Chinese
Academy of Sciences

Superconducting nanowire single photon detectors (SNSPDs) have been demonstrated as a key-enabling technology forvarious applications such as quantum key distribution, space-ground laser communication and depth imaging. Nevertheless, the working mechanisms of SNSPD have not been well understood though many theoretical and experimental
studies were reported in recent years. By tuning the wavelength of the incident photons, one can study the detection
eﬃciency (DE) dependence on the bias current (Ib) for the photon energies, which provides an interesting method
to probe the intrinsic detection eﬃciency (IDE). Renema et al first systematically studied the DE-Ib (bias current)
relations at diﬀerent photon energy[1] and found a linear relation between the photon energy and triggering current
for NbN-based bow-tie nanodetector, where the triggering current is defined as the point leading to the detection
probability of 1%. Later, similar studies were carried out on WSi [2] and MoSi [3] SNSPDs, while the nonlinear
relations were reported.
In this work, we carried out the study on NbN-SNSPDs. We designed and fabricated NbN-SNSPDs with diﬀerent
linewidths. In our measurement polarized photons from 450 to 2000 nm were prepared using a supercontinuum laser
and an acousto-optic tunable filter. By tuning the wavelength and polarization, the DE- Ib relations were obtained atvarious wavelengths for both parallel and perpendicular polarizations. Diﬀerent with reported work on NbN detectors[1], nonlinear relations between photon energy and current were concluded. Detailed wavelength dependence of intrinsic
detection eﬃciency and energy-current relations will be presented in our report.
Reference[1] J. J. Renema, R. Gaudio, Q. Wang, Z. Zhou, A. Gaggero, F. Mattioli, et al., ”Experimental Test of Theoriesof the Detection Mechanism in a Nanowire Superconducting Single Photon Detector,” Physical Review Letters, vol.
112, 2014.
[2] D. Y. Vodolazov, Y. P. Korneeva, A. V. Semenov, A. A. Korneev, and G. N. Goltsman, ”Vortex-assisted
mechanism of photon counting in a superconducting nanowire single-photon detector revealed by external magnetic
field,” Physical Review B, vol. 92, 2015.
[3] M. Caloz, B. Korzh, N. Timoney, M. Weiss, S. Gariglio, R. J. Warburton, et al., ”Optically probing the detection
mechanism in a molybdenum silicide superconducting nanowire single-photon detector,” Applied Physics Letters, vol.
110, p. 083106, 2017.
category : Sensor Physics & Developments

190

PA-64 A model on heat signal of crystal detector at low temperature
Jin Li1 , Inwook Kim2
1

IBS Center for Underground Physics, 2 Seoul National University

We present a model to calculate heat signal shapes from low temperature bolometer attached to a crystal. It can beused to understand and predict signals of real detectors, e.g., in the AMoRE double beta decay experiment. This modelis based on the elementary acoustic wave theory at low temperature, and has been developed using modern Monte
Carlo techniques. Physical processes in phonon propagation, such as scattering, decay and reflection are considered.
Finally, the calculated time dependence of signal is compared against real experimental data to test our model.
category : Applications

191

PA-65 Characteristics of IF bandwidth of NbN Superconducting Tunneling Junction
MixersDong Liu1 , Jie Hu2 , Wei Tao Lv3 , Jing Li4 , Sheng Cai Shi5
1

Purple Mountain Observatory, 2 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 3 Purple
Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 4 Purple Mountain Observatory, CAS / Key Lab of Radio
Astronomy, CAS , 5 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS

Besides the sensitivity nearly approaching the quantum limit, the intermediate-frequency (IF) bandwidth is of particular interesting for Superconductor-insulator-superconductor (SIS) mixers for radio astronomy research. In this paper,
we are going to present the characteristic of IF bandwidth of two type of NbN SIS mixers, long distributed junctions
and two distributed junctions. Firstly, the relative mixers’ gain are measured with 50 Ω IF load impedance for both
two SIS mixers. And also the relative mixers’ gain with diﬀerent IF load impedance are simulated to get the optimum
IF load impedance over a relative large IF bandwidth (2-15GHz). Finally, an IF matching circuit are designed andmeasured associating with SIS mixers, the measurement results show that the mixers gain are flatter over a large IF
bandwidth than with 50 Ω IF load impedance.
category : Sensor Physics & Developments

192

PA-66 NTLE cryogenic light detectors with planar electrode geometry - latest results
Elizabeth Mondragon1 , Xavier Defay2 , Angelina Kinast3 , Alexander Langenkamper4 , Jean-Come Lanfranchi5 , Erik
Lindner6 , Andrea Munster7 , Tobias Ortmann8 , Walter Potzel9 , Stefan Schonert10 , Andreas Ulrich11 , Stephan
Wawoczny12 , Michael Willers13
1

Physics Department and Excellence Cluster Universe, Technical University of Munich, 2 Physics Department and Excellence
Cluster Universe, Technical University of Munich , 3 Physics Department and Excellence Cluster Universe, Technical
University of Munich , 4 Physics Department and Excellence Cluster Universe, Technical University of Munich , 5 Physics
Department and Excellence Cluster Universe, Technical University of Munich , 6 Physics Department and Excellence Cluster
Universe, Technical University of Munich , 7 Physics Department and Excellence Cluster Universe, Technical University of
Munich , 8 Physics Department and Excellence Cluster Universe, Technical University of Munich , 9 Physics Department andExcellence Cluster Universe, Technical University of Munich , 10 Physics Department and Excellence Cluster Universe,
Technical University of Munich , 11 Physics Department and Excellence Cluster Universe, Technical University of Munich ,12
Physics Department and Excellence Cluster Universe, Technical University of Munich , 13 Physics Department andExcellence Cluster Universe, Technical University of Munich

The Neganov-Trofimov-Luke eﬀect (NTLE) is a promising way to improve the sensitivity of cryogenic light detectors byenhancing the thermal signal in a semiconductor. This eﬀect in the semiconductor is caused by drifting photo-generated
electron-hole pairs while under an electric field and at mK temperatures. Such cryogenic light detectors are of highimportance for direct dark matter searches (such as CRESST), cryogenic neutrinoless double-beta decay searches, andexperiments searching for coherent neutrino nucleus scattering (CNNS); experiments where excellent sensitivity andenergy resolution are required. A novel approach to NTLE light detectors is the use of a planar electrode geometry
based on very thin implanted contacts on silicon absorber crystals. The main diﬀerence to previous approaches is thatthe photo-generated charge carriers are drifted through the bulk of the absorber instead of being drifted across thefree surfaces of the absorber, leading to an improved signal-amplification, signal-to-noise ratio, and charge collection.
In this contribution we will present an update on the development of these detectors at the Technical University of
Munich.
category : Sensor Physics & Developments

193

PA-67 Design and fabrication of mid-infrared superconducting hot-electronbolometers
Akira Kawakami1 , Hisashi Shimakage2 , Junsei Horikawa3 , Masaharu Hyodo4 , Shingo Saito5 , Shukichi Tanaka6 ,Yoshinori Uzawa7
1

NICT, 2 Ibaraki University , 3 Fukui College , 4 Kanazawa University , 5 National Institute of Information and Communications
Technology , 6 National Institute of Information and Communications Technology , 7 National Institute of Information andCommunications Technology

To design antennas for mid-infrared superconducting hot-electron bolometer (HEB), the surface reactance of Au thinfilm at cryogenic temperatures was evaluated using Fourier transform infrared spectroscopy with a sample coolingsystem. We fabricated mid-infrared resonator arrays that were constructed by gold thin film strips, and found thatthe resonant frequency was shifted to the low frequency side as the temperature was lowered. By fitting the resonant
frequency to simulated results, the corrected surface reactance was established. Prototypes of a mid-infrared HEB
formed by a twin-slot antenna with a niobium nitride strip were fabricated. When the HEB was biased close to thecritical current under mid-infrared pulsed light (λ=4.89 μ m) irradiation, the detector output synchronized with thetrigger signal was observed. The output waveforms comprised voltage pulse trains, and the full width at half maximumof the pulse was evaluated to be approximately 0.25 ns.
category : Sensor Physics & Developments

194

PA-68 Progress towards Photon Counting Detectors for Terahertz Astronomy
Hajime Ezawa1 , Hiroshi Matsuo2 , Masahiro Ukibe3 , Go Fujii4 , Shigetomo Shiki51

National Astronomical Observatory of Japan, 2 National Astronomical Observatory of Japan , 3 National Institute ofAdvanced Industrial Science and Technology , 4 National Institute of Advanced Industrial Science and Technology , 5 National
Institute of Advanced Industrial Science and Technology

High resolution imaging plays an important role in modern astronomy and astrophysics. ALMA or VLTI are successfully serving their high angular resolution capability in radio or optical wavelengths, respectively, while high resolution
imaging technology for terahertz frequency is yet to be explored. Intensity interferometry will be a powerful method
for next generation interferometric instruments, where direct detectors can be used to realize high sensitivity andwide bandwidth. We have introduced a new concept to determine the ‘delay’ to synthesize images with intensity
interferometry by making use of the photon bunches of thermal radiation, even with the absence of electromagnetic
phase information. This idea was demonstrated by observing the sun with the Nobeyama Radioheliograph, where thekey to the success was to sample the signal in high speed (Ezawa et al. 2015, ISSTT 2015, W2-2)
Following this success, we are discussing to introduce a photon counting concept to intensity interferometry (PCTI;
Matsuo 2012, JLTP 167, 840), aiming for high angular resolution and high sensitivity with future space terahertz interferometers. Various developments are ongoing to realize photon counting detectors in terahertz region. Consideringa typical case of observing an 1 Jy source using a 10-m telescope at 1 THz with 100 GHz bandwidth, photon rate
√ of
100 Mphotons/s is expected. Therefore the detector should respond as fast as 1 GHz, and realize NEP< 10−17 W/ Hz(Matsuo & Ezawa 2016, JLTP 184, 718).
Our design involves SIS junctions (or STJs) to be used as photon detectors. The key to realize the required
specification is to develop an SIS junction with low leakage current of 1 pA at cryogenic temperature of 0.8 K. We arefabricating small junctions with Nb/Al/AlOx/Al/Nb using CRAVITY facility at AIST to meet this requirement. Keyparameters including junction area, thickness of aluminum layer, and current density are optimized. The cryogenic
properties of the junctions are investigated at NAOJ, especially to ensure the low leakage current to operate them as
photon counting devices.
Photoelectrons produced by the SIS junction, will be read out through cryogenic FETs and wide-bandwidth
amplifiers. GaAs-JFET or Junction pHEMT are considered as candidates for the first-stage FET of the readout circuit,which show good performance under cryogenic temperatures, such as low noise and low gate leakage. Currently we areworking with the prototype of each component. Various properties including NEP, spectral and time responses of thedetector measured with a cryogenic calibration source, as well as the design of the detection system will be discussed
in the presentation.
category : Sensor Physics & Developments

195

PA-69 A Graphene Based Terahertz Hot Electron Bolometer with Johnson Noise
Readout
Wei Miao1 , Hao GAO2 , Zheng WANG3 , Wen ZHANG4 , Yuan REN5 , Kangmin ZHOU6 , Shengcai SHI7 , Cui YU8 ,Zezhao HE9 , Qinbing LIU10 , Zhihong FENG11
1

Purple Mountain Observatory, 2 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 3 Purple
Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 4 Purple Mountain Observatory, CAS / Key Lab of Radio
Astronomy, CAS , 5 Purple Mountain Observatory, CAS / Key Lab of Radio Astronomy, CAS , 6 Purple Mountain
Observatory, CAS / Key Lab of Radio Astronomy, CAS , 7 Purple Mountain Observatory, CAS / Key Lab of Radio
Astronomy, CAS , 8 Hebei Semiconductor Research Institute , 9 Hebei Semiconductor Research Institute , 10 Hebei
Semiconductor Research Institute , 11 Hebei Semiconductor Research Institute

Graphene is a very attractive material for hot electron bolometers due to its weak electron phonon coupling and small
electronic heat capacity. Here we present the development of a graphene based hot electron bolometer at terahertz(THz) frequencies. The bolometer is a 2 um long and 10 um wide graphene microbridge connected to a log spiralantenna by Au contact pads. The Fourier transform spectrometer (FTS) measurement shows that the bolometerhas high coupling eﬃciency in the frequency range from 0.3 to 1.6 THz. During the measurement, the electronic
temperature of graphene is measured by means of noise thermometry. Using 300 K/77 K blackbody loads, we measure
an optical noise equivalent power (NEP) of 5.7 × 10-12 W/Hz0.5 at 3 K. To understand the thermal transport inside
the graphene microbridge, we also measure the bolometers with diﬀerent microbridge lengths (varying from 0.6 to 8um) at diﬀerent bath temperatures. The measurements show that the thermal conductance caused by the electron
diﬀusion to the Au contact pads is significant in our bolometers. Therefore, the bolometer performance can be further
improved if the electron diﬀusion is eliminated (e.g., using superconducting contact pads).
category : Sensor Physics & Developments

196

PA-70 HIGH-PRECISION X-RAY SPECTROSCOPY OF HIGHLY-CHARGED
IONS AT STORAGE RINGS USING SILICON MICROCALORIMETERS
Pascal A. Scholz1 , Victor Andrianov2 , Alexander Bleile3 , Artur Echler4 , Peter Egelhof5 , Oleg Kiselev6 , Saskia
Kraft-Bermuth7 , Damian Mull8
1

Justus Liebig University Giessen, 2 Institute of Nuclear Physics, Lomonosov Moscow State University, Russia , 3 GSI
Helmholtz Centre for Heavy Ion Research, Germany / Institute of Physics, Johannes-Gutenberg University Mainz, Germany ,4
1. Physics Institute, Justus-Liebig-University Giessen, Germany / GSI Helmholtz Centre for Heavy Ion Research, Germany /Institute of Physics, Johannes-Gutenberg University Mainz, Germany , 5 GSI Helmholtz Centre for Heavy Ion Research,
Germany / Institute of Physics, Johannes-Gutenberg University Mainz, Germany , 6 GSI Helmholtz Centre for Heavy Ion
Research, Germany , 7 1. Physics Institute, Justus-Liebig-University Giessen, Germany , 8 1. Physics Institute,Justus-Liebig-University Giessen, Germany

High precision X-ray spectroscopy of hydrogen-like heavy ions provides a sensitive test of quantum electrodynamics in very strong Coulomb fields. However, one limitation of the current accuracy of such experiments is the energy
resolution of available X-ray detectors [1]. To improve this accuracy, a novel detector concept, namely the concept of
microcalorimeters, is now exploited for such measurements. With this kind of detectors and aﬃxed X-ray absorbers
appropriate to the desired energy range, a relative energy resolution of about 1 per mille is obtained in the energy
regime of 1 - 100 keV [2].
The application of microcalorimeters for hard X-rays, based on silicon thermistors and tin absorbers, for the determination of the 1s Lamb Shift in hydrogen-like heavy ions has been pursued by our collaborating groups for more than
two decades. Two detector arrays have been successfully applied in two experiments at the Experimental Storage Ring
(ESR) of the GSI Helmholtz Center for Heavy Ion Research to determine the 1s Lamb Shift of hydrogen-like lead andgold [3]. An excellent agreement with theory has been obtained.
In order to improve the statistical uncertainty and lateral sensitivity, a larger detector array with three times the active
detector area in a new, cryogen-free cryostat is currently in preparation. Due to space limitations within the sidearmof the cryostat, a re-design of the detector was necessary for the next generation detector. The new detector design
is a more compact version of the design of Bleile et al. [2]. In 2016 this new design was tested at the ESR storage
ring of the GSI facility using a hydrogen-like Xenon and a lithium-like Uranium beam. This test was an importantbenchmark on the way to the larger detector array.
In this contribution, we will present the design of the new experimental setup and the results of the recent experiment. In addition to the current developments for experiments at the future FAIR facility, perspectives for otherhigh-precision experiments, i.e. spectroscopy of inner-shell transitions, will be discussed.
References:[1] Th. Stohlker et al., Lecture Notes in Physics 745, 151, Springer-Verlag Berlin, Heidelberg(2008)[2] A. Bleile et al., AIP Conference Proceedings 605 (2002) 409-412[3] S. Kraft-Bermuth et al., Journal of Physics B: Atomic, Molecular and Optical Physics 50(2017) 055603
category : Sensor Physics & Developments197

PA-71 Temperature Study of the DC IV curves of NbN Superconducting Nanowire
Single Photon Detectors
Andrew Dane1 , Di Zhu2 , Emily Toomey3 , Marco Colangelo4 , Qingyuan Zhao5 , Karl Berggren6
1

Electrical Engineering and Computer Science, MIT, 2 Massachusetts Institute of Technology , 3 Massachusetts Institute ofTechnology , 4 Massachusetts Institute of Technology , 5 Massachusetts Institute of Technology , 6 Massachusetts Institute ofTechnology

Superconducting nanowire single photon detectors (SNSPDs) are the leading technology for eﬃcient high-speeddetection of single telecommunications wavelength photons. SNSPDs are attractive because they combine 100s of
MHz count rates, with close to 100% detection eﬃciency and 10s of picoseconds of timing jitter. A range of applications and basic measurements have employed SNSPDs or are being developed to take advantage of the SNSPD s
superior performance, including: low power space-based optical communication, quantum photonic integrated circuits,
and tests of quantum mechanics.
Despite the SNSPD s attractive features and demonstrated performance, the fundamental limits to performanceas well as a large number of sample and material dependent properties which strongly influence device performance
are unknown or infrequently measured. For instance, the thermal boundary conductance to the substrate, whichremoves the heat generated in an SNSPD by an absorbed photon or proceeding detection event, has no definitive
measurements, despite our understanding that it may be the determinant of maximum non-latching detector speed.
Additionally, constrictions remain an important issue for SNSPDs but compared to switching currents and photon
count rates, constriction factor is not typically measured.
We measured the temperature dependence of a NbN SNSPD s current-voltage (IV) relationship in order to better
understand the thermal properties of the nanowire system. As the current bias through the SNSPD is varied at 3.2 K,
the nanowire IV curve shows pronounced hysteresis, switching into a voltage state when the bias exceeds the switchingcurrent (Isw ), but only switching back once the bias is reduced below a current less than half of Isw . This lower
current is known as the retrapping current (Ir ) and its magnitude can be related to the thermal parameters of thesystem. As the system temperature was raised, Isw dropped rapidly, while Ir reduced more gradually. At a crossover
temperature (T ∗ ) 9 K, the switching and retrapping currents became equal, and between T ∗ and Tc the IV curve of
the wire was non-hysteretic.
Figure 1 shows our fit of the non-hysteretic IV curve data at 9.4 K with the Ambegoakar and Halperin model forthermal noise in an overdamped Josephson junction. The wire critical current and the normal state resistance wereboth used as fitting parameters. This fit suggests a temperature regime where flux flow across the wire is prominentand the available cooling power is larger than the dissipated electrical power. The critical currents used to fit the IV
curves in this regime are significantly higher than the switching currents obtained using a 1 mV voltage threshold todefine the switching current of the wire. A comparison between the critical current obtained by modelling the wire
this way and the experimentally determined switching currents may give us insight into premature switching of thewire due to vortex motion at lower temperatures.
Lastly, the non-hysteretic regime may represent an opportunity for a fundamentally diﬀerent type of device operation where the absorption of a photon modulates flux flow across the nanowire. We comment on the feasibility ofdetecting photons while operating in this regime.
category : Sensor Physics & Developments

198

PA-72 Axion search experiment by using Josephson-Junction device
Atsushi Tokiyasu1 , Kennichi Karatsu2 , Kenji Kiuchi3 , Satoru Mima4 , Katsuro Nakamura5
1

Tohoku University, 2 TU Delft , 3 RIKEN , 4 RIKEN , 5 KEK

Cosmic dark matter is the main component of the universe, and its detail has not been identified. Axion is known as
one of the leading candidates of cosmic dark matter. Axion was theoretically proposed by Peccei and Quinn in 1970s,
to solve the so-called strong CP problem in Quantum-chromo dynamics. However, the existence of axion has not been
confirmed, because it hardly interact with the ordinal matter.
We are planning a new search experiment of axion by using a unique technique which was proposed by C. Beck et
al. in 2013 (Phys. Rev. Lett. 111, 231801).
They focused on the analogy between the equation of motion of axion and the equation of the phase of JosephsonJunction. In the theoretical model, a quantum interference eﬀect will occur if the voltage corresponding to axion mass
is supplied in the Josephson-Junction.They insist the existence of axion field explains some steps which were observed
around 0.55 meV in the I-V curves.
However, there are some critical opinion for their model. There is a possibility that observed steps were createdby the external radiation. The situation is still controversial, and a systematic study of Josephson-Junction in the low
background conditions is awaited.
We are planning an new experiment to search for axion by using the same method. In our Josephson-Junction
device, Nb and Al was used for the superconducting,and normal conducting material, respectively. The gap distance
was set to 120 nm to maximize the probability to observe axion.
The device was produced at RIKEN, and the property was measured. The electro-magnetic shield was also designed
and the was shielding power was tested by using FEM software. We need to measure extraordinarily small current,
and the experimental design was determined.
In this contribution, the experimental overview and the current situation will be explained. The plan will be also
shown.
category : Sensor Physics & Developments

199

PA-73 The DM Radio Pathfinder experiment: searching for dark matter from 500
peV to 50 neV
Stephen Erwin Kuenstner1 , Saptarshi Chaudhuri2 , Hsaio-Mei Cho3 , Carl Dawson4 , Peter Graham5 , Kent D. Irwin6 ,Dale Li7 , Harvey Moselely8 , Arran Phipps9 , Maximiliano Silva-Feaver10 , Betty Young11
1

Department of Physics, Stanford University, 2 Stanford University, Stanford, CA, USA , 3 SLAC National Accelerator
Laboratory, Menlo Park, CA, USA , 4 Stanford University, Stanford, CA, USA , 5 Stanford University, Stanford, CA, USA ,6
Stanford University, Stanford, CA, USA , 7 SLAC National Accelerator Laboratory, Menlo Park, CA, USA , 8 NASA Goddard
Space Flight Center, Greenbelt, MD, USA , 9 Stanford University, Stanford, CA, USA , 10 University of California San Diego,
San Diego, CA, USA , 11 Stanford University, Stanford, CA, USA / Santa Clara University, Santa Clara, CA, USA

In this work we describe the DM Radio Pathfinder, a dark matter search based on a superconducting lumpedelement LC resonator. While WIMP searches have been conducted for several decades, very little is known about thefundamental properties of dark matter, motivating the search for a broad range of dark matter candidates. Light-fielddark matter candidates, including the spin-0 axion and the spin-1 hidden photon, can be detected with coherent
amplifiers. DM Radio is an experimental campaign using tunable, lumped element LC resonators and SQUID-based
amplifiers to probe many orders of magnitude of hidden photon and axion mass and coupling strength. In this work, wereport on progress on the detector for the DM Radio Pathfinder experiment, a liquid-helium-cooled, niobium lumped
element detector. We perform in situ measurements to demonstrate the lumped element resonator, and measurecoupling to the SQUID amplifiers and isolation from the environment.
category : Sensor Physics & Developments

200

PA-74 Characterization of doped silicon thermometers for cryogenic bolometers
Obaid Adami1 , Louis Rodriguez2 , Abdelkader Aliane3 , Albrecht Poglitsch4 , Jean-Luc Sauvageot5 , Valerie Goudon6 ,Laurent Dussopt7 , Vincent Reveret8
1Institut de recherche sur les lois fondamentales de l’Univers, 2 Institut de recherche sur les lois fondamentales de l’Univers,
Service d’Astrophysique, CEA/Saclay , 3 MINATEC, CEA/Grenoble , 4 Institut de recherche sur les lois fondamentales del’Univers, Service d’Astrophysique, CEA/Saclay , 5 Institut de recherche sur les lois fondamentales de l’Univers, Serviced’Astrophysique, CEA/Saclay , 6 MINATEC, CEA/Grenoble , 7 MINATEC, CEA/Grenoble , 8 Institut de recherche sur les lois
fondamentales de l’Univers, Service d’Astrophysique, CEA/Saclay

Doped silicon has long been used as thermometers for X-ray micro-calorimeters and in far-infrared bolometers. In
the course of developing cooled semiconductor thermometers for submillimeter wave detection, typically 100 μ m ?
λ ? 1.5 mm, we have investigated several phosphorus and boron ion-implanted Si (Si:P,B) thin layers with diﬀerent
doping densities at temperatures between 50 and 300 mK. The aim was to get suﬃcient understanding of thermometer
behavior for optimizing the design of cryogenic detectors. The first step of this work, presented as part of this congress,
is to obtain a square thermometer of 1 Mohm impedance around 50-100mK with high sensitivity to build 1 Gohm
sensor (thanks to an aspect ratio around 1000). This leads to an important increase of the readout signal.
The obtained results showed that, at low supplied power, the electrical conductivity is approximated over a wide
range of doping densities and temperature by the variable range hoping (VRH). However, at high supplied power, thenon-Ohmic eﬀects become dominant and the so-called ”hot electron model”, where the resistance is a function of theelectrons temperature, provides a good fit to our data over a wide range of doping densities and temperature. These
non-Ohmic eﬀects may cause additional noise but mainly decrease the net sensitivity of the thermometers.
category : Sensor Physics & Developments201

PA-75 Electromagnetic Simulations of newly designed semiconductor bolometers for
submillimeter observations
Sophie Bounissou1 , Vincent Reveret2 , Louis Rodriguez3 , Albrecht Poglitsch4 , Abdelkader Aliane5 , Obaid Adami6 ,Valerie Goudon7 , Laurent Dussopt8 , Wilfried Rabaud91

Department of Astrophysics, CEA Paris-Saclay, France, 2 AIM Paris Saclay, CEA/Irfu/DAp, Bat 709, Orme des Merisiers,
91191 Gif-sur-Yvette, France , 3 AIM Paris Saclay, CEA/Irfu/DAp, Bat 709, Orme des Merisiers, 91191 Gif-sur-Yvette, France, 4 AIM Paris Saclay, CEA/Irfu/DAp, Bat 709, Orme des Merisiers, 91191 Gif-sur-Yvette, France / MPE, Giessenbachstr.,
85748 Garching, Germany , 5 CEA/LETI, MINATEC, 17 avenue des Martyrs, 38054 Grenoble, France , 6 AIM Paris Saclay,
CEA/Irfu/DAp, Bat 709, Orme des Merisiers, 91191 Gif-sur-Yvette, France , 7 CEA/LETI, MINATEC, 17 avenue desMartyrs, 38054 Grenoble, France , 8 CEA/LETI, MINATEC, 17 avenue des Martyrs, 38054 Grenoble, France , 9 CEA/LETI,MINATEC, 17 avenue des Martyrs, 38054 Grenoble, France

In the frame of the SPICA mission, new semiconductor bolometers have been designed for the SAFARI/POL instrument which are directly part of the HERSCHEL/PACS legacy. These detectors are cooled down to 50 mK and are
sensitive to the polarization for the 100, 200 and 350 um wavelength bands. In this paper, preliminary simulations
have been carried out using thin film theory to check the reliability of the first 3D simulations with a multiphysics
software. The detector is broadly modelled by absorbers deposited on a silicon substrate suspended at the top of aresonant cavity (created by a reflector). This work shows that we can accurately recover the theoretical absorption
curves by simulating a 3D structure within a short computation time. Then the whole bolometer structure has been
designed with the two suspended interlaced silicon-spirals which support the vertical and horizontal absorbers (sensitive to the two orthogonal polarizations) of the SAFARI/POL detectors. These simulations allow to quantify thecross-polarization potentially induced by the layout of the absorbers. From this study we can conclude that crosspolarization has a really small eﬀect on the electromagnetic absorption of the detector, which should be confirmed byforthcoming measurements.
category : Sensor Physics & Developments202

PA-76 Development of a Dielectric Microcalorimeter with Quantum FerroelectricMaterials
Shota YOSHIMOTO1 , Keisuke MAEHATA2 , Naoko IYOMOTO3 , Kazuhisa MITSUDA4 , Noriko YAMASAKI5
1

Department of Applied Quantum Physics and Nuclear Engineering, Kyushu University, 2 Kyushu University , 3 Kyushu
University , 4 Japan Aerospace Exploration Agency , 5 Japan Aerospace Exploration Agency

The dielectric constant of quantum paraelectric materials increases with temperature decreasing and holds a constant value at a temperature region of lower than tens K. Quantum paraelectric materials transit into a quantum
ferroelectric phase by employing appropriate impurity doping. The dielectric constant of some kinds of the quantum
ferroelectric materials has temperature dependence below 1K, and the change of the dielectric constant can be utilized
as a thermosensor of microcalorimeters. The following are an operating principal of a dielectric microcalorimeter(DMC): By applying a constant DC voltage to facing surfaces across the dielectric capacitor, a change in the electric
capacitance alters the amount of the electric charge stored in a dielectric capacitor. The temperature rise induced by
the incident radiation is converted into electric charge proportional to the change in dielectric constant of the material.
This electric charge is collected by the feedback capacitance of a conventional charge sensitive preamplifier. Because
there is no DC-current through the dielectric device, the DMC has advantage of the suppression of the Johnson noise
and the Joule heat generation in the device. Furthermore, the DMC is insensitive to magnetic fields. In this work,
we fabricated prototype of DMC using KTa(1−x) Nbx O3 (KTN) dielectric material, whose quantum ferroelectrics has
been reported on D. Rytz et al. : Phys. Rev. B 27, 6830 (1983) . Geometrical dimensions of the KTN chip are
surface area of 2 mm X 1 mm and 0.2 mm thick. Au electrodes of 0.1 μ m thick were deposited on the upper andlower surfaces. Electric capacitance of the KTN with x = 0.01 was found to have temperature dependence of 3 pF/K
at temperatures below 1 K by electric capacitance measurement with using the 4 terminal pair method. The DMC
using KTN with x=0.01 was irradiated with alpha rays emitted by a Am-241 source at a temperature of 100 mK.
Although signal pulses were observed with applying a DC bias voltage of 10 V, the number of the observed pulse wasextremely small. The number of the observed signal pulse was found to increase by applying an AC bias voltage withthe amplitude of 10 V and the frequency of 0.01 Hz. Signal pulses corresponding to alpha particle detection wereselected with analyzing the rise time constant of the signal pulses. In this presentation, we report details of sensitivityof the dielectric thermosensor and alpha ray response of the DMC using the KTN with x=0.01.
category : Sensor Physics & Developments203

PA-77 Accurate Measurement of Gain Saturation ofSuperconductor-Insulator-Superconductor
Wenlei Shan1 ,1

National Astronomical Observatory of Japan,

Superconductor-Insulator-Superconductor (SIS) tunnel junction mixers and direct detectors are very sensitive detectors
in millimeter and submillimeter waves. However, they can be significantly saturated by a room temperature blackbody
radiation, which results in uncertainties in calibration of radio telescopes. Astronomical observation, on the other hand,requires high fidelity in order to accurately derive physical parameters of celestial bodies. Besides eﬀorts in improving
the linearity of SIS mixers in circuit design, accurate measurement of the gain saturation up to an uncertainty of 1
Experimentally the gain saturation measurement is implemented by introducing a weak cw (continue wave) signal
together with a broadband blackbody radiation into the input port of the mixer and measuring the diﬀerence of cw
power at the output with switching the blackbody temperature from liquid nitrogen to room temperature. For an
ideal linear mixer, the cw output power is indiﬀerent to the broadband noise level. But in practice, a certain reductionin the cw output power can be detected when the input noise level is switched from low (liquid nitrogen) to high (roomtemperature). Although the principle is simple, the measurement result is found to be diﬀerent with diﬀerent power
measurement instruments, specifically a standard spectrometer and a diode powermeter. Both of them are verified toshow good linear responses to a cw source. This discrepancy is found to be dependent on the power level of the cw
signal that is injected. The lower signal-to-noise level, the bigger discrepancy was found. Besides the uncertainty inmeasure gain saturation, the noise temperature of the mixer is also found to vary with output power level.
The above mentioned uncertainties were found to be caused by the diﬀerence in the response of power detectors
between cw signal, noise-like signal and the mixture of cw and noise-like signal with small signal-to-noise ratio. Powerdetectors that are widely used are diode-based detectors because they are fast in response, stable, sensitive andeconomical. However, because they are not based on thermal eﬀect in the measurement of signals, they may response
diﬀerently to cw signals of diﬀerent frequencies and between cw signals and noise-like signals. While the former one
is often noticed in the calibration manual, the later one is in general not been paid attention to. In this work, we will
analyze the detection error, the calibration method and an example of characterization of a SIS mixer.
category : Sensor Physics & Developments

204

PA-78 Study for the Operating Principle of Superconducting Strip Photon Detectors(SSPDs)Nobuyuki Zen1 , Yutaka Abe2 , Go Fujii3 , Yuma Tomitsuka4 , Yuki Yamanashi5 , Yasunori Mawatari6 , Nobuyuki
Yoshikawa7
1

Nanoelectronics Research Institute, AIST, 2 Yokohama National University , 3 AIST , 4 Yokohama National University ,5
Yokohama National University , 6 AIST , 7 Yokohama National University

Superconducting strip photon detectors (SSPDs) are promising single photon detectors for realizing practical quantum
cryptography; their high quantum eﬃciencies, low timing jitters, and low dark count rates overcome those of avalanche
photo diodes or other single photon detectors. Recently, some research groups have established testbeds for quantum
cryptography and succeeded in field tests of quantum key distribution at a speed of sub Mbps using practical opticalfibers in the length of tens of km.
However, the detecting mechanism of the SSPD is still under investigation. The most probable hypothesis is thefollowings: (1) an incident photon fluctuates the order parameter of a superconducting strip resulting in the nucleationof vortex-antivortex pairs; (2) vortex pairs are unbound and forced out of the strip in the perpendicular direction ofbias current; (3) kinetics of vortices forms a normal band across the strip and a current pulse outputs. Conventional
SSPDs utilize the current pulse as a photon detection signal and its response characteristics such as a response timeof several ns regulate the quantum communication speed of sub Mbps as mentioned above.
On the other hand, the numerical simulations have shown that the time scale of kinetics of vortices is in the rangeof ps. Therefore, by detecting the extruded vortices instead of current pulse, we could expect the communication
speed faster than several orders of magnitude of that realized by conventional SSPDs. In this study, we have directly
connected a superconducting strip with single flux quantum (SFQ) circuits to capture the extruded vortices out of the
strip. Since the information carriers of SFQ circuits are also vortices, not only capturing the vortices but also counting
the number of them or other logical operations are possible.
category : Sensor Physics & Developments

205

PA-79 MOCCA: A 4k-pixel molecule camera for the position and energy resolving
detection of neutral molecular fragments at the Cryogenic Storage Ring CSR
Lisa Elena Gamer1 , Steﬀen Allgeier2 , Klaus Blaum3 , Christian Enss4 , Andreas Fleischmann5 , Loredana Gastaldo6 ,Sebastian Kempf7 , Oldrich Novotny8 , Dennis Schulz9 , Andreas Wolf10
1

Kirchhoﬀ-Institute for Physics, 2 Kirchhoﬀ-Institute for Physics, Heidelberg University , 3 Max Planck Institute for Nuclear
Physics, Heidelberg , 4 Kirchhoﬀ-Institute for Physics, Heidelberg University , 5 Kirchhoﬀ-Institute for Physics, Heidelberg
University , 6 Kirchhoﬀ-Institute for Physics, Heidelberg University , 7 Kirchhoﬀ-Institute for Physics, Heidelberg University ,8
Max Planck Institute for Nuclear Physics, Heidelberg , 9 Kirchhoﬀ-Institute for Physics, Heidelberg University , 10 Max Planck
Institute for Nuclear Physics, Heidelberg

The Cryogenic Storage Ring CSR at the Max Planck Institute for Nuclear Physics in Heidelberg is designed to prepare
and store molecular ions in their rotational and vibrational ground state. A key requirement for the study of electronion interactions within CSR is the identification of reaction products. The use of metallic magnetic calorimeters(MMCs) allows for identifying all neutral products since the deposited kinetic energy of incident particles into MMC
absorbers can be used as a measure of the particle mass. To actually resolve the full reaction kinematics, a position
sensitive coincident detection of multiple reaction products is necessary.
For these measurements we designed MOCCA, a 4k-pixel molecule camera based on MMCs with a detection areaof 45mm × 45mm, which is segmented into 64 × 64 absorbers and read out using only 32 SQUIDs. We discuss thedetector design and its microfabrication as well as its multi-hit capability, cross-talk and expected energy resolution
for photons and massive particles. In addition, we present first proof-of-principle measurements with photons as wellas our plans for integrating MOCCA and its 3He/4He dilution refrigerator into CSR.
category : Sensor Physics & Developments

206

PA-80 Tantalum STJ X-ray Detectors with an Energy Resolution Limited by Charge
Statistics
Matthew Hollis Carpenter1 , Francisco Ponce2 , Stephan Friedrich3 , Robin Cantor4
1

STAR Cryoelectronics, 2 Lawrence Livermore National Laboratory, 7000 East Ave., L-188, Livermore, CA 94550 , 3 Lawrence
Livermore National Laboratory, 7000 East Ave., L-188, Livermore, CA 94550 , 4 STAR Cryoelectronics, 25-A Bisbee Ct.,
Santa Fe, NM 87508

We are developing superconducting tunnel junction (STJ) detectors for high-resolution soft X-ray spectroscopy atsynchrotron light sources. The sensor consists of 36- or 112-pixel arrays of Ta-Al-AlOx-Al-Ta STJs, and each pixel has
an area of (208 µm)2 . When illuminated directly with a monochromatic X-ray beam at a synchrotron, the STJs havean energy resolution between ≈2 and ≈5 eV FWHM in the energy range below 1 keV, and can be operated at several
1000 counts/s per pixel. The STJ line width is much narrower than the width of X-ray fluorescence lines in the sameenergy range, indicating that the STJ energy resolution is higher than the natural line width of the fluorescence. In
fact, at low energies the resolution is set by the statistics of charge generation and tunneling, plus an electronic noise
contribution of ≈2 eV. We discuss STJ detector performance and their use in synchrotron science.
category : Sensor Physics & Developments

207

PA-81 Development of metallic magnetic calorimeters with critical temperatureswitch for AMoRE experiment
Sora Kim1 , Yong-Hamb Kim2 , Hyonsuk Jo3 , JinA Jeon4 , Chan Seok Kang5 , Hyelim Kim6 , Inwook Kim7 , Heyjin
Lee8 , Minkyu Lee9 , Sung Hoon Lee10 , Seung-Yoon Oh11
1

Institute for Basic Science, 2 Center for Underground Physics (CUP), Institute for Basic Science (IBS) / Korea ResearchInstitute of Standards and Science(KRISS) , 3 Center for Underground Physics (CUP), Institute for Basic Science (IBS) ,4
Center for Underground Physics (CUP), Institute for Basic Science (IBS) , 5 Center for Underground Physics (CUP),
Institute for Basic Science (IBS) , 6 Center for Underground Physics (CUP), Institute for Basic Science (IBS) , 7 Center for
Underground Physics (CUP), Institute for Basic Science (IBS) / Korea Research Institute of Standards and Science(KRISS) ,8
Center for Underground Physics (CUP), Institute for Basic Science (IBS) , 9 Korea Research Institute of Standards andScience(KRISS) , 10 Center for Underground Physics (CUP), Institute for Basic Science (IBS) , 11 Korea Research Institute ofStandards and Science(KRISS)We report the recent progress on MMC development of a critical temperature switch. A meander-shaped coil in the
MMC should form a superconducting loop to measure the magnetic signal and to apply a persistent field current
to magnetize the paramagnetic sensor material. In this work, a part of the superconducting loop is fabricated withanother superconducting material with its transition temperature (Tc) lower than that of niobium. A persistentcurrent can be injected in the loop while reducing the temperature from above to below Tc. A part of the loop is
made of an alloy of Nb and Ta (NbTa) with its Tc between 2.7 K to 5 K. In this method, the number of MMC wirings
can be reduced, and the field current injection procedure can be simplified. The MMCs with a critical temperatureswitch are to be used for future AMoRE detector that requires about 1000 MMC channels.
category : Sensor Physics & Developments

208

PA-82 Thermal modelling and experimental results on NTD heat signals for Ge
macro-bolometers
Julien Billard1 , Dimitri Misiak2 , Romain Maisonobe3 , Alexandre Juillard4 , Maryvonne De Jesus5 , Claudia Nones6 ,Anastasiia Zolotarova7 , Stefanos Marnieros8 , Louis Dumoulin9
1

CNRS, 2 Univ Lyon, Universite Lyon 1, CNRS/IN2P3, IPN-Lyon, F-69622, Villeurbanne, France , 3 Univ Lyon, Universite
Lyon 1, CNRS/IN2P3, IPN-Lyon, F-69622, Villeurbanne, France , 4 Univ Lyon, Universite Lyon 1, CNRS/IN2P3, IPN-Lyon,
F-69622, Villeurbanne, France , 5 Univ Lyon, Universite Lyon 1, CNRS/IN2P3, IPN-Lyon, F-69622, Villeurbanne, France ,6
CEA Saclay, DSM/IRFU, 91191 Gif-sur-Yvette Cedex, France , 7 CEA Saclay, DSM/IRFU, 91191 Gif-sur-Yvette Cedex,
France , 8 Centre de Sciences Nucleaires et de Sciences de la Matiere, Universite Paris Sud, CNRS/IN2P3, Universite
Paris-Saclay, Bat 108, 91405 Orsay, France , 9 Centre de Sciences Nucleaires et de Sciences de la Matiere, Universite Paris Sud,
CNRS/IN2P3, Universite Paris-Saclay, Bat 108, 91405 Orsay, FranceThis work describes the methodology and results from a dedicated study of the heat signals from germanium Neutron
Transmutations Doped (Ge-NTD) used for Ge macro-bolometers as in the EDELWEISS experiment. We show how,with a combined set of measurements with diﬀerent detector configurations, we construct a coherent thermal model,
including the eﬀect of Aluminum electrodes on the heat signals. Eventually, from the set of detector configurations
studied, we define a pathway at improving the energy resolution for 200 (800) gram-scale Ge bolometers down to 100
eV (RMS) which would provide great sensitivity to low-mass dark matter down to 0.5 GeV.
category : Sensor Physics & Developments

209

PA-83 Statistical approach to the investigation of dark counts in Superconducting
Nanostrip Single Photon Detectors
Mikkel Ejrnaes1 , Lapo Lolli2 , Emanuele Taralli3 , Mauro Rajteri4 , Eugenio Monticone5 , Loredana Parlato6 ,Giampiero Pepe7 , Alessandro Casaburi8 , Robert H Hadfield9 , Roberto Cristiano10
1

CNR - SPIN, 2 INRIM-Istituto Nazionale di Ricerca Metrologica, 10135 Torino, Italy , 3 INRIM-Istituto Nazionale di Ricerca
Metrologica, 10135 Torino, Italy , 4 INRIM-Istituto Nazionale di Ricerca Metrologica, 10135 Torino, Italy , 5 INRIM-Istituto
Nazionale di Ricerca Metrologica, 10135 Torino, Italy , 6 CNR - Istituto SPIN Napoli, 80125 Napoli, Italy and Universita
Federico II di Napoli, 80125 Napoli, Italy , 7 CNR - Istituto SPIN Napoli, 80125 Napoli, Italy and Universita Federico II di
Napoli, 80125 Napoli, Italy , 8 School of Engineering, University of Glasgow, Glasgow G12 8LT, UK , 9 School of Engineering,
University of Glasgow, Glasgow G12 8LT, UK , 10 CNR - Istituto SPIN Pozzuoli, 80078 Pozzuoli (Napoli), Italy

Superconducting Nanostrip Single Photon Detectors (SSPDs or SNSPDs) are typically based on thin and narrownanowires patterned out of NbN or NbTiN superconducting films that operates at a temperature of about 2 K andbiased close their critical current value. They can detect single photons in the wavelength range between visible
and near infrared with unprecedented performance in terms of high detection eﬃciency, excellent timing jitter, freerunning operation and especially very low dark count rate [1-3]. In particular, the investigation of the dark countgeneration phenomenon will reveal important aspects of the intrinsic mechanisms underlying the SNSPD operationand signal-to-noise in practical photon counting applications. In addition, this understanding will guide optimizationof improved SNSPD device based on meandered nanostrips like, through mitigation of eﬀects due to current crowding
eﬀects, inhomogeneities and constrictions along the nanostrips and so on [4].
We present measurements of NbN SNSPD performed in the range from 4.2K to 60 mK. At 4.2 K we characterized
current bias dependence of the dark count rate using an innovative statistical approach. From the measurements, we
can reconstruct the dark count rate of the detector along with its statistical distribution and compare this to mathematical models. The detector was subsequently cooled in a dilution refrigerator and measurements were performed in
the range 60 - 650 mK but no dark count events were observed. A follow up optical characterization in the presenceof 1550 nm laser light was performed using the same statistical approach.
References:[1] G.N. Gol tsman, O. Okunev, G. Chulkova, A. Lipatov, A. Semenov, K. Smirnov, B. Voronov and A. Dzardanov,Appl. Phys. Lett, 79, 705 (2001).
[2] C. M. Natarajan, M. G. Tanner and R. H. Hadfield, Supercond. Sci. Technol. 25, 063001 (2012).
[3] M. D. Eisaman, J. Fan, A. Migdall and S. V. Polyakov, Rev. Sci. Instrum. 82, 071101 (2011).
[4] A. Engel, J. J. Renema, K. Il in and A. Semenov, Supercond. Sci. Technol. 28 (2015) 114003 and references
therein.
category : Sensor Physics & Developments

210

PA-84 Low loss submillimeter wave coplanar waveguide made of superconducting
NbTiN on sapphire substrate
Nuri van Marrewijk1 , Akira Endo2 , Kenichi Karatsu3 , Stephen Yates4 , Masato Naruse5 , Junya Suzuki6 , David
Thoen7 , Vignesh Murugesan8 , Jochem Baselmans9
1

Faculty of Electrical Engineering, Mathematics and Computer Science, Delft University of Technology, 2 Department ofElectrical Engineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628 CD Delft, The
Netherlands. / Kavli Institute of NanoScience, Faculty of Applied Sciences, Delft University of Technology, Lorentzweg 1,
3
Department of Electrical Engineering, Faculty of Mathematics and Computer Science, Delft University of Technology, 2628
CD Delft, The Netherlands. , 4 SRON Netherlands Institute for Space Research, 9747 AD Groningen, The Netherlands. ,5
Graduate School of Science and Engineering, Saitama University, Saitama, 338-8570, Japan. , 6 High Energy Accelerator
Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki, 305-0801, Japan. , 7 Department of Electrical Engineering, Facultyof Mathematics and Computer Science, Delft University of Technology, 2628 CD Delft, The Netherlands. / Kavli Institute of
NanoScience, Faculty of Applied Sciences, Delft University of Technology, Lorentzweg 1, 8 SRON Netherlands Institute forSpace Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands. , 9 SRON Netherlands Institute for Space Research,
Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands.

Low loss submillimeter wave coplanar waveguide made of superconducting NbTiN on sapphire Recent advances insubmillimeter technology have enabled on-chip superconducting components such as on-chip spectrometers, parametric amplifiers, multi-color pixels, phased array antennas, and delay lines. Many of these components, and theirinterconnections, require transmission lines with very low losses of the order of tan δ ≪ 10−2 -10−4 , or Q ≫ 102 -104 ,depending on the application. In this study we measured the loss of a superconducting coplanar waveguide (CPW)using an on-chip CPW Fabry Perot (FP) interferometer. The CPW-FP is fabricated from a 100 nm thick NbTiN film,
sputter deposited on a C-plane sapphire substrate, and has an equal slot width and strip width of 2 µm. To minimize
the eﬀects of coupling ends of the FP, we drive the resonator at high order modes (n = 95-100). We measure in the360-380 GHz range Q ∼13 000-16 000, setting lower limits to the intrinsic CPW losses at each resonance frequency.
This shows that 100 nm NbTiN CPW lines are potential building blocks for on-chip components and devices.
category : Sensor Physics & Developments

211

PA-85 NTD-Ge production in the LUMINEU experiment using cryogenic detectors
for Rare Events searches and other applications
Xavier Francois Navick1 , Cyril Bachelet2 , Stephane Bouillaguet3 , David Bouville4 , Noel Coron5 , Laurent Devoyon6 ,Antoine Egele7 , Andrea Giuliani8 , Mathieu Lemaitre9 , Martin Loidl10 , Pierre de Marcillac11 , Claudia Nones12 , Yves
Penichot13 , Matias Rodrigues14
1

CEA, 2 CSNSM, CNRS & Univ. Orsay, France , 3 CEA, DEN/DANS/Orphee, Gif sur Yvette, France , 4 C2N, CNRS & Univ.
Orsay, France , 5 IAS, CNRS & Univ. Orsay, France , 6 CEA, DEN/DANS/Orphee, Gif sur Yvette, France , 7 CEA,
DSM/IRFU, Gif sur Yvette, France , 8 CSNSM, CNRS & Univ. Orsay, France , 9 CEA, DEN/DANS/Orphee, Gif sur Yvette,
France , 10 CEA, DRT/LIST/LNHB, Gif sur Yvette, France , 11 CSNSM, CNRS & Univ. Orsay, France , 12 CEA, DSM/IRFU,
Gif sur Yvette, France , 13 CEA, DSM/IRFU, Gif sur Yvette, France , 14 CEA, DRT/LIST/LNHB, Gif sur Yvette, France

Experiments such as Cupid-Mo and Edelweiss-3 plan to use Neutron Transmutation Doped Germanium sensors (NTD)
as thermistors on their detectors for Neutrinoless Double Beta Decay and light-mass-WIMP search respectively. Sucha choice is motivated by their robustness, reliability, ease of use over a large range of temperature and large dynamic
range in energy. To cope this future large demand on NTDs, our groups in LUMINEU started a new production line
for Ge-NTDs.
In this poster, we present the synthesis of irradiation dose of the diﬀerent irradiations of HPGe wafers and parameters of metallization. Some wafers have been selected on the basis of their R(T) at very low temperature and firstsignals obtained from LUMINEU s detectors equipped with sensors made from these wafers. The performance interm of noise and signal to noise ratio are equivalent to the best previously available NTD sensors. This demonstrates
our ability to produce performant NTD sensors for the desired range of working temperature.
category : Sensor Physics & Developments

212

D S B r e c e iv e r n o is e te m p e r a tu r e ( K )2 5 0 02 0 0 0
2 0 K
1 5 0 0
1 5 K
fit 1 3 G H z
1 0 0 0

5 K

5 0 0

0

T r( f) = T ( 0 ) ( 1 + ( f/fN ) 2 )
2

3

4

5

6

In te r m e d ia te fr e q u e n c y ( G H z )

213

7

8

Figure 1. Non-hysteretic current-voltage (IV) curve measured for a 100 nm wide NbN SNSPD on silicon at
9.4K. A fit line based on Ambegaokar and Halperin’s model of the effect of thermal noise on a resistively
shunted Josephson junction is shown in red. The critical current (Ic) and normal state resistance (Rn) wereused as fitting parameters, with Ic = 4.2 µA and Rn = 6 MΩ.

3214

Category B : Readout Techniques &Signal processing215

PB-1 Development of a data acquisition system for kinetic inductance detectors: wide
dynamic range and high sampling rate for astronomical observation
Junya Suzuki1 , Hikaru Ishitsuka2 , Kyungmin Lee3 , Shugo Oguri4 , Osamu Tajima5 , Nozomu Tomita6 , Mitsuhiro
Yoshida7 , Eunil Won8
1

Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, 2 Graduate Univ. for Advanced
Studies, Shonan Village, Hayama, Kanagawa 240-0193, Japan , 3 Department of Physics, Korea University, 145, Anam-ro
Seongbuk-gu, Seoul 136-713, Korea , 4 RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198 Japan , 5 High Energy Accelerator
Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan / Graduate Univ. for Advanced Studies, Shonan
Village, Hayama, Kanagawa 240-0193, Japan , 6 Department of Physics, Faculty of Science, University of Tokyo, Tokyo
113-0033, Japan , 7 High Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan /Graduate Univ. for Advanced Studies, Shonan Village, Hayama, Kanagawa 240-0193, Japan , 8 Department of Physics, Korea
University, 145, Anam-ro Seongbuk-gu, Seoul 136-713, Korea

Microwave Kinetic Inductance Detectors (MKIDs) have a potential for a variety of applications to astronomical
observation. One of these applications is observation of cosmic microwave background radiation (CMB), and theGroundBIRD telescope for CMB polarization measurement adopts MKIDs arrays as its focal plane detectors.
In order to achieve high sensitivity for large angular scale, the GroundBIRD telescope utilizes a novel circularscanning system employing rotary joints for gas and electricity. MKIDs well match with this high-speed scan for theirprompt time responses. The observation requires high sampling rate (over 1 kSpS), wide dynamic range, and stable
operation for the read-out system.
We built a data acquisition system combining a dedicated analog board and a commercially available digital board.
The analog board RHEA has two pairs of 14-bit ADC and 16-bit DAC operating at 200 MSPS, whose high bit
resolution enables wide dynamic range without losing sensitivity. RHEA also achieves low power consumption andlow heat emission in comparison with a commercially available analog board, enabling stable operation at least over amonth. The digital board is an evaluation board for an FPGA Xilinx KCU105, which calculates the output multi-tone
wave and processes the input waves deformed by detectors to extract the signal. After the process, the data is sent to
a computer via gigabit Ethernet.
In this conference, we will present the status of the development of the data acquisition system. We have alreadyachieved 120 channel simultaneous readout using the direct down-conversion method to decode the signal. Using thefunctionalities of the system, a variety of software, e.g., VNA-like sweep, time-ordered data acquisition, and real-timemonitoring, were developed and tested. We also performed measurements with a test array of MKIDs fabricated in
RIKEN, and confirmed that the system properly works.
Although the data acquisition system was developed for the GroundBIRD experiment, it can be generally used
for readout of MKIDs, in particular when the measurement requires high sampling rate and wide dynamic range. In
addition, the analog board RHEA has a potential for a wide variety of applications beyond MKIDs readout.
Figure: Schematic view of the developed readout system. Output with 120 tones measured with a spectrum
analyzer is included in the upper-left panel.

category : Readout Techniques & Signal processing216

PB-2 In-orbit performance of the pulse shape processor of ASTRO-H SXSMasahiro Tsujimoto1 , Makoto S. Tashiro2 , Yoshitaka Ishisaki3 , Shinya Yamada4 , Hiromi Seta5 , Kazuhisa Mitsuda6 ,Megan E. Eckart7 , Maurice A. Leutenegger8 , Caroline A. Kilbourne9 , Frederick Scott Porter10 , Richard L. Kelley11 ,Takashi Okajima121

Department of Astrophysics, ISAS, JAXA, 2 Saitama University , 3 Tokyo Metropolitan University , 4 Tokyo Metropolitan
University , 5 Tokyo Metropolitan University , 6 JAXA ISAS , 7 NASA GSFC , 8 NASA GSFC , 9 NASA GSFC , 10 NASA GSFC
, 11 NASA GSFC , 12 NASA GSFC

The pulse shape processor (PSP) is the onboard digital signal prcessing unit of the X-ray micro-calorimeter mission;
the Soft X-ray Spectrometer (SXS) onboard the Hitomi (ASTRO-H) satellite. We have reporeted its design and
expected performance in the previous LTD meetings. We present the result obtained in the orbit in this meeting.
The PSP continuously recieves the signal, which is sampled at 12.5 kHz, shaped, amplified, and digitized by thepreceding analogue signal processing unit from 36 micro-calorimeter and two anti-coincidence detector channels. It
is responsible for detecting X-ray pulses, deblending them if they are overlapped in time, cross-correlating them with
templates to derive precise arrival time and energy based on the optimum filtering technique, and editing the telemetryfor downlink. Because these calculations are resource-demanding, the CPU processing speed of the PSP determines thetotal throughput of the SXS. When the PSP cannot catch up with the incoming rate, it inserts dead time artificiallyto discard an entire event buﬀere once in a while.
This design was tested in the orbit during the observation of the Crab nebula, which was suﬃciently bright to
hit the PSP limit. Using the data, we show that the maximum processing rate exceeded the required value of 150
Hz/array, and that the dead times were properly recorded so that we can reconstruct the images, spectra, and pulse
shape of the Crab pulsar and its surrounding nebula.
category : Readout Techniques & Signal processing217

PB-3 Crosstalk in an FDM laboratory set-up and the Athena X-IFU science
performance
Roland den Hartog1 , Christian Kirsch2 , Cor de Vries3 , Hiroki Akamatsu4 , Thomas Dauser5 , Philippe Peille6 ,Eduardo Cucchetti7 , Brian Jackson8 , Jorn Wilms9 , Simon Bandler101

5SRON Utrecht, 2 ECAP, Erlangen, Germany , 3 SRON, Utrecht, the Netherlands , 4 SRON, Utrecht, the Netherlands ,ECAP, Erlangen, Germany , 6 CNES, Toulouse, France , 7 IRAP, Toulouse, France , 8 SRON, Groningen, the Netherlands ,9ECAP, Erlangen, Germany , 10 NASA GSFC, Maryland, USA

The detector of the X-ray Integral Field Unit (X-IFU) instrument onboard Athena will consist of 3840 TES pixels
read out with a Frequency Domain Multiplexing system of 96 channels. At various points along the read-out chain
crosstalk may arise, eﬀectively causing oﬀsets in photon energies measured on pixels due to signals received in neighbors.
Neighboring pixels may be adjacent in space, in the case of thermal crosstalk arising on the array, or in frequency, inthe case of crosstalk in the electrical circuit of the FDM readout. The impact of various crosstalk mechanisms on the
instrument performance has been assessed with detailed end-to-end simulations and so far found to be accomodatablewithin the requirements for energy resolution degradation and throughput of high-quality events. For the crosstalk in
the electrical circuit a detailed model has been developed. In this contribution we test this model against measurements
made with an FDM laboratory set-up and discuss the assumption of deterministic crosstalk in the context of the weaklink eﬀect in the detectors. We show that crosstalk levels predicted by the model are conservative with respect to theobserved levels.
category : Readout Techniques & Signal processing218

PB-4 Evaluation and Improvement of Nb and NbN Microwave SQUID multiplexers
for a gamma-ray TES with a Sn Absorber linked by Au Post
Tomoya Irimatsugawa1 , Fuminori Hirayama2 , Hirotake Yamamori3 , Satoshi Kohjiro4 , Akira Sato5 , Shuichi
Nagasawa6 , Daiji Fukuda7 , Mutsuo Hidaka8 , Yasushi Sato9 , Masashi Ohno10 , Hiroyuki Takahashi11
1

School of Engineering, The University of Tokyo, 2 National Institute of Advanced Industrial Science and Technology ,National Institute of Advanced Industrial Science and Technology , 4 National Institute of Advanced Industrial Science andTechnology , 5 National Institute of Advanced Industrial Science and Technology , 6 National Institute of Advanced Industrial
Science and Technology , 7 National Institute of Advanced Industrial Science and Technology , 8 National Institute of Advanced
Industrial Science and Technology , 9 National Institute of Advanced Industrial Science and Technology , 10 National Instituteof Advanced Industrial Science and Technology , 11 National Institute of Advanced Industrial Science and Technology
3

Transition edge sensors arrays based on microwave SQUID multiplexer[1] (MW-MUX) is promising technique to realizea superconducting detector system with high energy resolution and large active area. The MW-MUX takes advantage
of high-Q superconducting thin-film resonators terminated by dissipationless RF-SQUIDs. Then the signals of TESs
are multiplexed into large bandwidth of low noise cryo-HEMT of a few GHz which leads to the number of multiplexing
TES pixels in a cable much higher than conventional multiplexers.
We have been developing MW-MUX based on Nb or NbN quarter wave resonators optimized for gamma-ray TES
consists of Ir/Au bilayers coupled to a tin bulk absorber being developed at the University of Tokyo[2]. Here, wereport the evaluation of our MW-MUX system based on the first readout of single gamma-ray TES signal.
In the experiment, we readout 5 channels in a MW-MUX chip simultaneously, one of them is connected to the
gamma-ray TES and the other channels are open. The input power of microwave is about -85 dBm at the feedline
and the flux ramp modulation[3] of 60 kHz is applied to the SQUIDs. The intrinsic quality factors (Qi ) of MW-MUX
used in this experiment are about 4 × 103 - 1 × 104 at 100 mK, although our short-ended resonator achieved Qi ≈ 105[4]. The TES is irradiated with the gamma-ray from Co-57 positioned outside the cryostat.
The time constant of rising (τrise ) and the decay (τdecay ) are evaluated by fitting the measured pulse to a theoreticalequation. The obtained values are τrise = 260 µs and τdecay = 6.4 ms those are close to the values obtained by theconventional single pixel readout system.Therefore, our multiplexer is fast enough for our gamma-ray TES. Although
the readout noise (RMS) is about 11 times worse than that of the conventional readout system, reduction of 10 dB
white noise is expected by optimizing the microwave power and increasing Qi to 1 × 105 .
We will discuss possible origin that degrades Qi and show the improvement of noise under the optimized microwave
power.
Reference
1. J. A. B. Mates, et al., Appl. Phys. Lett. 92, 023514 (2008).
2. S. Hatakeyama et al., IEEE. Trans. Appl. Supercond., Vol. 25, No.3 (2015).
3. J. A. B. Mates, et al., J. Low Temp. Phys., vol. 167, (2012).
4. T.Irimatsugawa et al., IEEE Trans. Appl. Supercond., Vol. 27, No. 4, (2017).
Acknowledgements
The chip was fabricated in the clean room for analog-digital superconductivity (CRAVITY) in AIST. This work
is partially supported by the program The Initiatives for Atomic Energy Basic and Generic Strategic Researchorganized by Japan Science and Technology Agency and JSPS KAKENHI Grant No. JP15H02251.
category : Readout Techniques & Signal processing

219

PB-5 Toward a 2000-channel Microwave SQUID Multiplexed Unit forTransition-Edge Sensor Bolometer Arrays
Bradley Jerald Dober1 , Jason Austermann2 , James Beall3 , Dan Becker4 , Douglas Bennett5 , Shannon Duﬀ6 , Jiansong
Gao7 , Jonathon Gard8 , James Hays-Wehle9 , Gene Hilton10 , Johannes Hubmayr11 , John A. B. Mates12 , Christopher
McKenney13 , Joel Ullom14 , Jeﬀ Van Lanen15 , Michael Vissers16
1

National Institute of Standards and Technology, 2 National Institute of Standards and Technology , 3 National Institute ofStandards and Technology , 4 University of Colorado Boulder , 5 National Institute of Standards and Technology , 6 National
Institute of Standards and Technology , 7 National Institute of Standards and Technology , 8 University of Colorado Boulder ,9
National Institute of Standards and Technology , 10 National Institute of Standards and Technology , 11 National Institute ofStandards and Technology , 12 University of Colorado Boulder , 13 National Institute of Standards and Technology , 14 National
Institute of Standards and Technology , 15 National Institute of Standards and Technology , 16 National Institute of Standards
and Technology

Next-generation bolometric receivers for future millimeter-wave astrophysics experiments such as Simons Observatory
and CMB-S4 will have focal planes with 50,000 Transition-Edge Sensors (TESs). Focal planes of this size require
both an increase in multiplexing factor as well as a reduction in detector packaging complexity. The microwave
SQUID multiplexer (uMUX) is a readout technology that has the potential to both drastically increase multiplexing
factors while simplifying the detector packaging. In this talk, we will describe recent measurements at NIST of TES
bolometers optimized for ground-based CMB studies using uMUX. These measurements show (1) a broad-band white
noise contribution well below the intrinsic sensor noise, and (2) low-frequency readout noise compatible with proposed
CMB scan strategies. These two results firmly establish the suitability of uMUX readout for future ground-based
CMB studies. In addition, we will review progress made at NIST towards further optimizing the uMUX design toaccommodate 2000 detector channels on a single readout line, which is achieved by decreasing the resonator bandwidthfrom 300 kHz to 100 kHz and the resonator frequency spacing from 6 MHz to 2 MHz. These steps will allow 2000
TES channels to fit on a single 4-8 GHz bandwidth readout card. Finally, we will highlight steps we have been
taking to significantly reduce the complexity of assembling large focal planes. For example, the complexity of wiring
interconnects can be eliminated by utilizing a single interface and bias wafer that is mounted to the back of thedetector array. The uMUX and packaging technologies described here are expected to enable next-generation CMB
experiments.
category : Readout Techniques & Signal processing220

PB-6 Development of a cryogenic capacitive trans-impedance amplifier based on
FD-SOI CMOS
Koichi Nagase1 , Takehiko Wada2 , Yasuo Arai3 , Hirokazu Ikeda4 , Shunsuke Baba5 , Toyoaki Suzuki6 , Morifumi
Ohno7 , Takahiro Ishimaru8
1

Japan Aerospace Exploration Agency (JAXA), 2 Japan Aerospace Exploration Agency (JAXA) , 3 High Energy Accelerator
Research Organization (KEK) , 4 Japan Aerospace Exploration Agency (JAXA) , 5 The University of Tokyo , 6 Nagoya
University , 7 National Institute of Advanced Industrial Science and Technology (AIST) , 8 Japan Aerospace Exploration
Agency (JAXA)

We are developing an image sensor with sensitivity to far-infrared (IR) wavelengths ranging from 30 to 200 µm
for astronomical observations. Our image sensor consists of a cryogenic readout integrated circuit (ROIC) and asemiconductor detector, such as germanium which is often used for a far-IR detector. The detector must be cooled
down below 2 K to reduce thermal noise; the dark current of the detector is reduced to be below 5 fA. To achieve thedetector noise limit, the input leak current of the ROIC should be lower than the detector dark current. The ROIC
based on MOSFETs is advantageous to achieve such very low leak current.
However, conventional bulk-MOSFETs, in particular NMOS FETs, show degradation such as the kink eﬀect andhysteresis in drain current at cryogenic temperatures. These anomalies are caused by instability of the potential
distribution in the MOSFETs under a carrier freezeout condition. In contrast, MOSFETs fabricated by a fully
depleted silicon-on-insulator (FD-SOI) CMOS process show stable characteristics at cryogenic temperatures. Due tovery thin Si bodies and thus full depleted ones, FD-SOI MOSFETs have no neutral region where the anomalies bycarrier freezeout may happen. Thus, their I-V curves are not almost aﬀected by the kink eﬀect and the hysteresis.
We developed an operational amplifier (OPAMP) based on the FD-SOI CMOS and obtained its excellent performance at 4.2 K. For the far-IR image sensor, we designed a capacitive trans-impedance amplifier (CTIA) using
the OPAMP and evaluated the performance of the CTIA at 4.2 K. The schematic circuit diagram to evaluate theperformance of the CTIA is shown in Figure 1. We demonstrated that our CTIA works as designed and that the input
leak current is < 1.4 × 10−17 A. Those results meet our requirements on the CTIA.

category : Readout Techniques & Signal processing

221

PB-7 A Second Generation Digital Readout for Large Photon Counting UVOIRMKID Arrays
Neelay H Fruitwala1 , Matthew J Strader2 , Alex B Walter3 , Gustavo I Cancelo4 , Ted J Zmuda5 , Kenneth R
Treptow6 , Neal G Wilcer7 , Benjamin A Mazin8
1

Department of Physics, University of California at Santa Barbara, 2 University of California at Santa Barbara , 3 University ofCalifornia at Santa Barbara , 4 Fermi National Accelerator Laboratory , 5 Fermi National Accelerator Laboratory , 6 Fermi
National Accelerator Laboratory , 7 Fermi National Accelerator Laboratory , 8 University of California at Santa Barbara

We present the development of a second generation digital readout system for photon counting MKID (Microwave
Kinetic Inductance Detector) arrays, operating in the UVOIR (UV, optical, infrared) regime. Like our first generation
system, the readout utilizes a two stage downconversion/channelization algorithm, and is capable of measuring photon
arrival time to 1 microsecond. IQ modulation and A/D conversion are performed using custom IF and ADC/DAC
boards, and the channelization algorithm is implemented using a CASPER ROACH2 board. Each complete set of
readout electronics is capable of reading out 1000 pixels in a 2 GHz band between 4 and 8 GHz. Ten such units are
combined to read out our 10,000 pixel DARKNESS array; this setup, combined with a 80 TB storage server, canrecord every photon’s arrival time, energy, and absorption location for over 107 photon/second. At a cost of roughly
7/pixel, this system could conceivably be scaled up to read out much larger arrays.
category : Readout Techniques & Signal processing222

PB-8 Series SQUID Array Amplifiers Optimized for MHz Frequency-Domain
Multiplexed Detector Readout
Stephan T. P. Boyd1 , John Ad Hall2 , Robin C Cantor3
1

Department of Physics and Astronomy, University of New Mexico, 2 STAR Cryoelectronics , 3 STAR Cryoelectronics

The CMB-S4 next-generation ground-based cosmic microwave background experimental program aims to provide
definitive measurements of the early universe using telescopes with large focal plane arrays of ?100,000 detectors. In
this report, we describe first results of a project to develop low-noise cryogenic amplifiers based on series SQUID arraysthat are suitable for frequency domain multiplexed readout for large CMB instruments. Designs were optimized using
modeling and simulation tools to meet the requirements for CMB detector readouts. Two generations of prototype
series SQUID array amplifier (SSAA) designs were completed. A large number of devices from each design iteration
were tested and characterized at 4 K. The new SSAA designs exhibit excellent performance characteristics. V Phi
curves are very smooth indicating little or no impact of RF resonances will be seen at higher frequencies. The bestperforming designs transimpedance (400 V/A versus 500 V/A) and current noise (5.9 pA/Hz versus 3.7 pA/Hz) areapproaching those of the benchmark series SQUID array amplifier from NIST. Two features of the new designs are ofparticular interest for future large-pixel-count CMB experiments: 1) input inductance has been lowered substantially(11 nH versus 150nH), which may permit a higher density of channels in frequency space, and 2) power dissipation
has been lowered substantially (18 nW versus ?900 nW at typical bias) that for the first time will enable the SSAAs
to be operated in close proximity to the pixels and filters at the 100mK focal plane array stage.
category : Readout Techniques & Signal processing223

PB-9 SLAC Microresonator Radio Frequency (SMuRF) Electronics for read out of
Frequency-Division-Multiplexed Cryogenic Sensors
Zeeshan Ahmed1 , SMuRF collaboration
1

Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory

Large arrays of low-temperature sensors for various applications ranging from x-ray, gamma-ray, Cosmic Microwave
Background (CMB) and mm/sub-mm imaging to particle detection increasingly rely on superconducting microresonators for high multiplexing factors. These microresonators take the form of microwave SQUIDs that couple toTransition-Edge Sensors (TES) or Microwave Kinetic Inductance Detectors (MKIDs). In principle, such arrays canbe read out with vastly scalable software-defined radio using suitable FPGAs, ADCs and DACs. In this work, weshare plans and show initial results for SLAC Microresonator Radio Frequency (SMuRF) electronics, a next-generation
control and readout system for superconducting microresonators. SMuRF electronics are unique in their implementation of specialized algorithms for closed-loop tone tracking, which consists of fast feedback and feedforward to eachresonator’s excitation parameters based on transmission measurements. Closed-loop tone tracking enables improved
system linearity, a significant increase in sensor count per readout line, and the possibility of overcoupled resonator
designs for enhanced dynamic range. Low-bandwidth prototype electronics were used to demonstrate closed-loop tone
tracking on twelve 300-kHz-wide microwave SQUID resonators, spaced at ∼6 MHz with center frequencies ∼5–6 GHz.
We achieve multi-kHz tracking bandwidth and demonstrate that the noise floor of the electronics is subdominant to
the noise intrinsic in the multiplexer. Finally, we present the status of the high-bandwidth SMuRF electronics forread out of ∼4,000 microwave-SQUID-coupled TES bolometers, or ∼500 fast TES x-ray calorimeters per readout line.
These electronics are designed for high density and scalability to enable systems with ∼105 or more channels.
SMuRF collaboration is• Z. Ahmed, Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, Menlo Park,
USA• S. Kuenstner, Department of Physics, Stanford University, Stanford, USA• S. A. Kernasovskiy, Department of Physics, Stanford University, Stanford, USA• E. Karpel, Department of Physics, Stanford University, Stanford, USA• D.D. Van Winkle, Advanced Instrumentation for Research Division, SLAC National Accelerator Laboratory, Menlo Park,
USA• S. Smith, Advanced Instrumentation for Research Division, SLAC National Accelerator Laboratory, Menlo Park, USA• J. Dusatko, Advanced Instrumentation for Research Division, SLAC National Accelerator Laboratory, Menlo Park, USA• J.C. Frisch, Advanced Instrumentation for Research Division, SLAC National Accelerator Laboratory, Menlo Park, USA• S. Chaudhuri, Department of Physics, Stanford University, Stanford, USA• H. M. Cho, Advanced Instrumentation for Research Division, SLAC National Accelerator Laboratory, Menlo Park, USA• B. Dober, Quantum Devices Group, National Institute of Standards and Technology, Boulder, USA• G. Hilton, Quantum Devices Group, National Institute of Standards and Technology, Boulder, USA• J. Hubmayr, Quantum Devices Group, National Institute of Standards and Technology, Boulder, USA• K. D. Irwin, Department of Physics, Stanford University, Stanford, USA; Kavli Institute for Particle Astrophysics andCosmology SLAC National Accelerator Laboratory, Menlo Park, USA• C. L. Kuo, Department of Physics, Stanford University, Stanford, USA; Kavli Institute for Particle Astrophysics andCosmology, SLAC National Accelerator Laboratory, Menlo Park, USA• D. Li, Advanced Instrumentation for Research Division, SLAC National Accelerator Laboratory, Menlo Park, USA• J. A. B. Mates, Quantum Devices Group, National Institute of Standards and Technology, Boulder, USA• M. H. Nasr, Department of Electrical Engineering, Stanford University, Stanford, USA; RF Accelerator Research Division,
SLAC National Accelerator Laboratory, Menlo Park, USA• S. Tantawi, Particle Physics and Astrophysics, Stanford University, Stanford, USA; RF Accelerator Research Division,
SLAC National Accelerator Laboratory, Menlo Park, USA• J. Ullom, Quantum Devices Group, National Institute of Standards and Technology, Boulder, USA• L. Vale, Quantum Devices Group, National Institute of Standards and Technology, Boulder, USA• B. A. Young, Department of Physics, Santa Clara University, Santa Clara, USA

category : Readout Techniques & Signal processing224

PB-10 Firmware Development for Microwave SQUID Multiplexer Readout
Johnathon D Gard1 , Dan Becker2 , Douglas A Bennett3 , Joseph W Fowler4 , Gene C Hilton5 , John A. B. Mates6 ,Carl D Reintsema7 , Dan Schmidt8 , Dan Swetz9 , Joel N Ullom10 , Leila R Vale11 , Jim P Hays-Wehle12
1

University of Colorado Boulder, 2 University of Colorado Boulder , 3 National Institute of Standards and Technology ,University of Colorado Boulder / National Institute of Standards and Technology , 5 National Institute of Standards andTechnology , 6 University of Colorado Boulder , 7 National Institute of Standards and Technology , 8 National Institute ofStandards and Technology , 9 National Institute of Standards and Technology , 10 University of Colorado Boulder / National
Institute of Standards and Technology , 11 National Institute of Standards and Technology , 12 University of Colorado Boulder/ National Institute of Standards and Technology
4

The readout requirements for instruments based on Transition-Edge Sensors (TESs) have dramatically increased overthe last decade as demand for systems with larger arrays and faster sensors has grown. Emerging systems are expected
to contain many thousands of sensors and/or sensors with time constants as short as 100 us. These requirements mustbe satisfied while maintaining low noise and low crosstalk. A promising readout candidate for future TES arrays is
the microwave SQUID multiplexer, which oﬀers several gigahertz of readout bandwidth per pair of coaxial cables. In
microwave SQUID multiplexing, sensor signals are coupled to RF-SQUIDs embedded in superconducting microwave
resonators, which are probed via a common microwave feedline and read out at room temperature using GHz signals
carried on coaxial cables. This form of SQUID multiplexing moves complexity from the cryogenic stages to room
temperature hardware and digital signal processing firmware which must synthesize the microwave tones and process
the information contained within them.
To demultiplex at room-temperature, we have implemented an FPGA-based solution using the ROACH2 hardware
platform developed by the CASPER consortium. We have successfully developed a flexible firmware architecture that,with few modifications can read out implementations of microwave SQUID multiplexers optimized for bolometric, highcount rate x-ray, and AC-bias TES applications. These implementations have resonator widths of 100 kHz, 2 MHz,and 30 MHz full width at half maximum respectively, with each diﬀerent resonator bandwidth necessitating digital
filter modifications to accommodate the diﬀering channel counts and required sampling rates.
A gamma-ray spectrometer targeted at nuclear materials accounting applications, known as SLEDGEHAMMER,
is an early adopter of microwave SQUID multiplexing and is driving our current firmware development eﬀort. This
instrument utilizes medium-bandwidth (300 kHz) resonators with 256 channels in a one gigahertz band. We haverecently demonstrated undegraded readout of 128 channels using two ROACH2s and a single HEMT amplifier. We
discuss how the electronics and firmware function, the challenges we encountered, and how these early results are
informing our current electronics and firmware development.
category : Readout Techniques & Signal processing225

PB-11 Development of Microwave Multiplexer Readout System Based on SQUIDs
Directly Coupled to Resonators for TES X-ray Microcalorimeter
Yuki Nakashima1 , Fuminori Hirayama2 , Satoshi Kohjiro3 , Hirotake Yamamori4 , Shuichi Nagasawa5 , Akira Sato6 ,Noriko Yamasaki7 , Kazuhisa Mitsuda8
1

ISAS/JAXA, 2 AIST , 3 AIST , 4 AIST , 5 AIST , 6 AIST , 7 ISAS/JAXA , 8 ISAS/JAXA

We are developing a microwave superconducting quantum interference device (SQUID) multiplexer (MW-Mux) readout system aimed to realize more than 104 pixels large format superconducting transition edge sensor (TES) X-ray
microcalorimeter array, which is larger than that of the Athena mission (i.e., 3840 pixels planned to launch around2028) in an order of magnitude, for future space missions such as an advanced version of DIOS (e.g., Yamada et al.
in this workshop). MW-Mux is a multiplexing technique capable of reading out potentially hundreds to thousands of
TES pixels in a single coaxial pair because of that three orders of magnitude larger bandwidth than those of conventional multiplexing methods (i.e., TDM, CDM and FDM) with several MHz bandwidths. It consists of a number ofsuperconducting resonators in the GHz range, each employing a unique resonance frequency, terminated by either an
inductance magnetically coupled to dissipationless rf-SQUID (conventional work) or SQUID itself (this work). Each
SQUID acts as a flux-variable inductor responding to the magnetic flux threading the SQUID loop in a flux-quantum
Φ0 (= 2.07 × 10−15 Wb) cycle. The advantage of our SQUID directly coupled to resonators is the simple design evenwhen the number of pixel becomes quite large. It is because, in our direct-coupled SQUIDs, all pixels with diﬀerent
resonance frequencies can adopt SQUIDs with the same shape, structure, and dimensions, while it is not the case formagnetically coupled SQUIDs.
The developed MW-Mux readout system consists of the MW-Mux optimized for our TES X-ray microcalorimeter,
the input circuit on chip connecting to that microcalorimeter and the readout electronics. To optimize a MW-Mux for
our TES X-ray microcalorimeter under the condition of applying flux ramp modulation for a linearization purpose, we
made an investigation into required MW-Mux bandwidth by numerical and spice simulations. In our case, that was
required larger than 3 MHz to satisfy suﬃcient energy resolution of our TES X-ray microcalorimeter whose signal riseand fall time constants were respectively 5 to 20 and 60 µs. Then, the 16-channel MW-Mux with larger bandwidththan 3 MHz was designed and fabricated based on three Nb electrode layers with SiO2 insulation layers stacked on Si
substrate. Moreover, we experimentally confirmed that all 16 resonances and SQUID responses to the input signal
agreed with the designed ones, and the bandwidths of those resonances were all over 3 MHz. We have also beendeveloping the input circuit including a microwave filter and some of dumping inductors, which are used to control
the TES signal rise time constant, on the purpose of read the TES signals out using this system.
In this presentation, we report optimized designs of our developed MW-Mux readout system for our TES X-ray
microcalorimeter, experimental result of that performances and brief introduction of TES X-ray microcalorimeterfeatures using that system.
category : Readout Techniques & Signal processing

226

PB-12 Investigation of SIS up-converter for use in multi-pixel receivers
Yoshinori Uzawa1 , Takafumi Kojima2 , Wenlei Shan3 , Alvaro Gonzalez4 , Matthias Kroug5
1

National Institute of Information and Communications Technology, 2 National Astronomical Observatory of Japan , 3 National
Astronomical Observatory of Japan , 4 National Astronomical Observatory of Japan , 5 National Astronomical Observatory ofJapan

In radio astronomy, there is a strong interest in large-scale multi-pixel heterodyne receivers, which enable wide fieldof-view observations with high spectral resolutions. So far, multi-pixel heterodyne receivers have been developed byseveral institutes, up to a maximum pixel number of 64. This number of pixels was achieved by SuperCam , which
explored astrophysically important emission and absorption lines within the 850 micron atmospheric window. Further
increase of the pixel number to as many as 1000 is now being considered. In this case, a key problem is the total power
consumption of a large number of cryogenic low noise amplifiers (LNAs). Given that a typical LNA consumes a few
milliwatts of power, refrigerators with several watts of cooling capacity at the 4-K stage are necessary to cool down
thousands of pixels. This is clearly impractical. To overcome this issue, we propose the use of a frequency divisionmultiplexing (FDM) technique to reduce the number of amplifiers at 4 K. The intermediate frequency (IF) outputsof the diﬀerent SIS mixers used for each of the diﬀerent pixels could be up-converted by a local oscillator (LO) signal
composed of diﬀerent frequency tones, a so-called frequency comb signal. The frequency diﬀerence between 2 LO tones
should be larger than the IF bandwidth at the SIS mixer IF output. Doing this, several SIS mixer IF bandwidths
could be allocated in a larger IF bandwidth, as a FDM signal, which could be amplified at once with current wideband
IF amplifiers. One of the key components to implement this concept is the up-converter, which should have a gain
larger than unity to prevent degradation of the receiver performance due to extra losses before amplification in the
LNA. For this reason, we consider SIS mixers with conversion gains greater than unity due to quantum eﬀects aregood candidates for this purpose. For the currently on-going feasibility study, we have calculated the up-conversion
characteristics of SIS mixers based on the quantum mixing theory developed by Tucker. Analytical results show that
it is necessary to select LO frequencies larger than the voltage scale of the dc nonlinearity of the SIS junction in orderto obtain positive conversion gains. First preliminary experimental results using Nb/AlOx/Nb SIS junctions showed
a possible gain in an SIS up-converter at the LO frequency of 85 GHz.
category : Readout Techniques & Signal processing227

PB-13 Active tuning of the resonance frequencies of LC bandpass filters for frequency
domain multiplexed readout of TES detector arrays
Jan van der Kuur1 , L.G. Gottardi2 , H.A. Akamatsu3 , B.J. van Leeuwen4 , A.C.T. Nieuwenhuizen5 , R.H. den
Hartog6 , M.P. Bruijn7 , A.J. van der Linden8 , B.D. Jackson91

SRON Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584CA
Utrecht, the Netherlands , 3 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584CA Utrecht, theNetherlands , 4 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584CA Utrecht, the Netherlands , 5 SRON
Netherlands Institute for Space Research, Sorbonnelaan 2, 3584CA Utrecht, the Netherlands , 6 SRON Netherlands Institutefor Space Research, Sorbonnelaan 2, 3584CA Utrecht, the Netherlands , 7 SRON Netherlands Institute for Space Research,
Sorbonnelaan 2, 3584CA Utrecht, the Netherlands , 8 SRON Netherlands Institute for Space Research, Sorbonnelaan 2,
3584CA Utrecht, the Netherlands , 9 SRON Netherlands Institute for Space Research, Landleven 12, 9747AD Groningen, theNetherlands

Eﬃcient use of the available frequency space for frequency domain multiplexing (FDM) is essential for space-based
TES detector applications such as the X-IFU instrument on the Athena X-ray telescope. For cross talk reasons there
exists a lower limit on the distance between neighbouring pixels in frequency space, so that accurate control of theresonance frequency helps to use the available frequency space. Independently, from the point of view of eﬃcientsinusoidal bias voltage generation, placing the frequencies on a grid with a fixed spacing helps to avoid the eﬀects ofnonlinearity on the detector performance. Inevitable tolerances in the lithographic production of LC bandpass filters,
and margins in the design of stray inductances limit the the relative accuracy of the resonance frequencies to a few
times 10−3 .
In this paper we will propose a new method which uses the active SQUID readout electronics at room temperature
to further fine tune the resonance frequencies of the LC filters beyond the manufacturing limitations. The results ofan experimental demonstration, in which resonance frequencies of 1 - 5 MHz will be changed over a range of few kHz,
will be shown.
category : Readout Techniques & Signal processing228

PB-14 Development of semi-rigid superconducting coaxial cables withnormal-conductor-clad center conductor
Akihiro Kushino1 , Tetsuya Okuyama2 , Soichi Kasai3
1

2

Kurume University, Department of Materials Systems Engineering, National Colleges of Technology, Kurume College ,3
COAX CO., LTD.

Attenuation [dB/m]

Semi-rigid coaxial cables with seamless metal materials as the outer electrical conductors can often been used forthe readout of low temperature detectors realizing low noise measurements. Moreover thin semi-rigid coaxial cables
employing superconductors, such as niobium-titanium (NbTi) at both center and outer conductors, enable very small
attenuation as well as small heat penetration into the cryogenic stages thanks to their almost zero electrical resistivity
and extreme low thermal conductivity.
We developed low-pass-filter-type semi-rigid coaxial cables with an outer diameter of 0.86 mm adopting bilayer
structure in the center conductor with a diameter of 0.20 mm, i.e., the inner superconductor and surficial normal
conductor. By this configuration, high frequency noise component is expected to attenuate in the normal conductor
with high electrical resistivity when it is thicker than the skin depth. We made and evaluated semi-rigid coaxial cable,
the center conductor of which consists of superconducting NbTi and surficial cupro-nickel (CuNi) clad with diﬀerent
thickness from zero to 38 µm, and observed that cutoﬀ frequency goes higher as the clad becomes thinner. In orderto promote filtering performance, we have chosen more electrically resistive alloy, stainless-steel (SUS304) as the cladmaterial. The semi-rigid cable with SUS304/NbTi center and SUS304 outer conductor was made by the conventional
drawing method. Thermal conductance and high frequency performance were measured. Thermal conductance wasreasonably low as expected from each material. However, attenuation of this SUS304/NbTi center - SUS304 outersemi-rigid cable was very large and attenuation and cutoﬀ frequency cannot be controlled as could be done in CuNi
clad case.
We think martensitic transformation might occurred during drawing treatment of commercial SUS304/NbTi wire,
and observed large attenuation was caused by the magnetization surrounding the center conductor. Precise investigation is being performed.

0

3.1-3.4K
NbTi - CuNi

-10

NbTi(13µm CuNi)- CuNi-20-30

NbTi(38µm CuNi)- CuNi-40-50

NbTi(13µm SUS)
- SUS

-60
-70
0.01

0.1

1

Frequency [GHz]category : Readout Techniques & Signal processing

229

10

PB-15 Superconducting multilayer high density flexible PCB for very high thermal
resistance interconnection
Xavier de la Broise1 , Alain Le Coguie2 , Jean-Luc Sauvageot3 , Vincent Moreau4 , Samuel d’Hollosy5
1

CEA Saclay, 2 CEA-Saclay, DRF, IRFU, 91191 Gif-sur-Yvette, France , 3 CEA-Saclay, DRF, IRFU, 91191 Gif-sur-Yvette,
France , 4 CEA-Saclay, DRF, IRFU, 91191 Gif-sur-Yvette, France , 5 Hightec MC AG, Fabrikstrasse 9, CH-5600 Lenzburg,
Switzerland

Lot of ultra-sensitive detectors, such as IR and X-ray detectors, or detectors for searching of dark matter or gravitational
waves, operate at deep cryogenic temperatures. Similarly, the number of space detectors requiring very low temperature
operation increases, and these detectors are increasingly segmented (large number of readout channels). This causes
ever greater diﬃculties in extracting the signals from the detector (typical temperatures from 50 mK to 300 mK) andinterconnecting them with the readout electronics, placed at a higher temperature.
Indeed, each electrical link constitutes a connection generating thermal leaks. When the number of interconnections
multiplies, the thermal leaks increase until it becomes impossible to cool the detector because the power supplied by
the cryo-refrigerator is insuﬃcient, and this is all the more so as the temperature to be generated is low. For example,
space cryogenerators can evacuate only a few microwatts at 50 mK, and in conventional Cu or Manganin technology
thermal leaks generated by electrical links quickly exceed this value, limiting the number of reading paths to a few
hundred at most. It is therefore a very strong constraint to the increase in the number of channels of the detectors.
For this reason we have carried out a development to produce high-density flexible PCB (17 μ m to 34 μ m
depth) with superconducting tracks (15 μ m wide spaced by 15 μ m), because superconductors are excellent thermal
insulators. They combine the advantages of niobium as superconductors (critical temperature around 9 K) andpolyimide as dielectric, which has an intrinsically low thermal conductivity (1.17x10-4 W/K/cm) and remains flexible
even at very low temperatures.
After the very first validation samples, we have successively developed two products, both in the context ofthe X spatial spectro-imagery. The first product is monolayer, includes 552 tracks, 15 μ m wide spaced by 15 μm, and receives 24 integrated circuits glued and wire-bonded directly on the flexible PCB. The second product ismultilayer, with one tracks layer between two shielding layers interconnected by microvias, includes 37 tracks and canbe interconnected at both ends either by wire-bonding or by connectors. We present the first results of our harnesses; the measurements include, among others, the critical temperature of the superconducting tracks and the criticalcurrent density.
The presented technology exhibits good yields and is, to our knowledge, a world-first. It has also a great potential
for many other applications at K- and mK-temperatures, such as some implementations of quantum cryptography or
quantum computing, and superconducting electronics in general.
category : Readout Techniques & Signal processing

230

231

PB-16 Acquisition System of Nobeyama MKID Camera
Makoto Nagai1 , Shunsuke Hisamatsu2 , Guangyuan Zhai3 , Tom Nitta4 , Naomasa Nakai5 , Nario Kuno6 , Yousuke
Murayama7 , Shogo Hattori8 , Pranshu Mandal9 , Yutaro Sekimoto10 , Hitoshi Kiuchi11 , Takashi Noguchi12 , Hiroshi
Matsuo13 , Agnes Dominjon14 , S Sekiguchi15 , Masato Naruse16 , Jun Maekawa17 , Tetsuhiro Minamidani18 , Masao
Saito19
1

Advanced Technology Center, National Astronomical Observatory of Japan, 2 University of Tsukuba , 3 University of Tsukuba, 4 University of Tsukuba , 5 University of Tsukuba , 6 University of Tsukuba , 7 University of Tsukuba , 8 University of Tsukuba, 9 University of Tsukuba , 10 National Astronomical Observatory of Japan , 11 National Astronomical Observatory of Japan ,12
National Astronomical Observatory of Japan , 13 National Astronomical Observatory of Japan , 14 National Astronomical
Observatory of Japan , 15 The University of Tokyo , 16 Saitama University , 17 National Astronomical Observatory of Japan ,18
National Astronomical Observatory of Japan , 19 National Astronomical Observatory of JapanWe are developing a superconducting camera based on microwave kinetic inductance detectors (MKIDs) to observe100/150-GHz bands with the Nobeyama 45 m telescope. An acquisition system for the camera has been designed tooperate the MKIDs with the telescope. This system is required to connect the telescope control system (COSMOS) to
the readout system of the MKIDs (MKID DAQ) which employs the frequency-sweeping probe scheme. The acquisition
system is also required to record the reference signal of the beam switching for the demodulation by the analysis pipeline
in order to suppress the sky fluctuation. The system has to be able to merge and save all data acquired both by thecamera and by the telescope, including the cryostat temperature and pressure and the telescope pointing. In addition,
the system is desired to provide quick-look data that observers would check. A collection of software which implements
these functions and works as a TCP/IP server on a workstation was developed. The server accepts commands andobservation scripts from COSMOS, and then issue commands to MKID DAQ to configure and start data acquisition.
We checked the demodulation algorithm of beam switching by observing celestial continuum sources with a receiver of
the Nobeyama 45 m telescope. We also made a test operation of the MKID camera on the Nobeyama 45 m telescopeand obtained successful scan signals of the atmosphere and of the Moon.

category : Readout Techniques & Signal processing232

PB-17 Frequency Domain Multiplexing Readout with a Self-Trigger System for
Kinetic Inductance Detector Pulse Signals
Yousuke Yamada1 , Hirokazu Ishino2 , Atsuko Kibayashi3 , Yosuke Kida4 , Naoto Hidehira5 , Kunimoto Komatsu6 ,Masashi Hazumi7 , Nobuaki Sato8 , Kazuhiro Sakai9 , Hirotake Yamamori10 , Fuminori Hirayama11 , Sasoshi Kohjiro12
1

Okayama University, 2 Okayama University , 3 Okayama University , 4 Okayama University , 5 Okayama University , 6 Okayama
University , 7 High Energy Accelerator Research Organization , 8 High Energy Accelerator Research Organization , 9 National
Aeronautics and Space Administration , 10 National Institute of Advanced Industrial Science and Technology , 11 National
Institute of Advanced Industrial Science and Technology , 12 National Institute of Advanced Industrial Science and Technology

We present development of a frequency-domain multiplexing readout of Kinetic Inductance Detectors (KIDs) for pulse
signals with a self-trigger system. The KIDs consist of an array of superconducting resonators that have diﬀerent
resonant frequencies individually, allowing us to readout multiple channels in the frequency domain with a single
wire using a microwave frequency comb. The energy deposited to the resonators break Cooper pairs, changing the
kinetic inductance and, hence, the amplitude and the phase of the probing microwaves. For some applications such as
X-ray detection, the deposited energy is detected as a pulse signal shaped by the time constants of the quasi-particle
lifetime, the resonator quality factor and the ballistic phonon lifetime in the substrate, that range from micro-seconds
to milliseconds. A readout system commonly used converts the frequency domain data to the time domain data. For
the short pulse signals, the data rate may exceed the data transfer bandwidth, as the short time constant pulses require
us to have a high sampling rate. In order to overcome the circumstances, we have developed a KID readout system that
contains a self-trigger system to extract relevant signal data, and reduces the total data rate with a commercial oﬀ-theshelf FPGA board. We have demonstrated that the system can readout pulse signals of 15 resonators simultaneouslywith about 10 Hz event rate by irradiating alpha particles from Am-241 to the silicon substrate on whose surface
niobium KID resonators are formed.
category : Readout Techniques & Signal processing233

PB-18 Design and Assembly of SPT-3G Cold Readout Hardware
Jessica Avva1 , SPT-3G Collaboration 2 , DfMux Collaboration 3
1

Department of Physics, UC Berkeley, 2 SPT-3G Collaboration , 3 DfMux Collaboration

The SPT-3G receiver on the South Pole Telescope was commissioned at the South Pole during the 2016-2017 australseason to study polarization of the Cosmic Microwave Background. In increasing the number of detectors by a factorof 10 to 16,000, the design of the cryogenic wiring was constrained by the need for low thermal conductance and theneed for low inductance imposed by the increased multiplexing factor and bandwidth of the frequency-domain readout
electronics. Our cold readout system consists of aluminum inductive capacitive resonators at 300mK connected to
4K SQUIDs by 10 micron thick Niobium-Titanium broadside coupled striplines. Here, we present a general overview
of the cold readout electronics for the SPT-3G receiver, including new applications of ultrasonic soldering for low
resistance Niobium-Titianium connections, performance of the Niobium-Titanium striplines, and characterization of
the cold readout chain.
category : Readout Techniques & Signal processing

234

PB-19 Automated Measurements for the Characterization of SQUID-Based
Time-Division Multiplexing Chips
C.S. Dawson1 , S. Chaudhury2 , H.-M. Cho3 , J. Gard4 , G. Hilton5 , K. Irwin6 , S. Kuenstner7 , D. Li8 , C. Reintsema9 ,C.J. Titus10 , B.A. Young11
1

Stanford University, 2 Stanford University, Department of Physics , 3 SLAC National Accelerator Laboratory , 4 National
Institute of Standards and Technology, Boulder , 5 National Institute of Standards and Technology, Boulder , 6 Stanford
University, Department of Physics / SLAC National Accelerator Laboratory , 7 Stanford University, Department of Physics ,8
SLAC National Accelerator Laboratory , 9 National Institute of Standards and Technology, Boulder , 10 Stanford University,
Department of Physics , 11 Stanford University, Department of Physics / Santa Clara University, Department of Physics

SQUID-based time-division multiplexing (TDM) is a mature and widely implemented technology for the readoutof transition edge sensors. We describe a suite of automated measurements and software algorithms that have beendeveloped for detailed TDM chip characterization as well as high throughput screening. We show how these techniques
may be used to probe the physics of TDM and in particular, the latest generation of multiplexers (TDM+), which
implement feedback switching for reduction in distant pixel crosstalk. We present data from a variety of recent
measurements.
category : Readout Techniques & Signal processing235

PB-20 Development of cross-talk suppression algorithm for MKID readout
Kyungmin Lee1 , Jihoon Choi2 , Makoto Hattori3 , Masashi Hazumi4 , Hikaru Ishitsuka5 , Kenichi Karatsu6 , Kenji
Kiuchi7 , Ryo Koyano8 , Hiroki Kutsuma9 , Jose Alberto Rubino Martin10 , Satoru Mima11 , Makoto Minowa12 , Makoto
Nagai13 , Taketo Nagasaki14 , Masato Naruse15 , Shugo Oguri16 , Chiko Otani17 , Rafael Rebolo18 , Ricardo T. Genova
Santos19 , Yutaro Sekimoto20 , Munehisa Semoto21 , Junya Suzuki22 , Tohru Taino23 , Osamu Tajima24 , Nozomu
Tomita25 , Tomohisa Uchida26 , Eunil Won27 , Mitsuhiro Yoshida28
1

Department of Physics, Korea University, 2 IBS , 3 Tohoku Univ. , 4 KEK / SOKENDAI , 5 SOKENDAI , 6 TU Delft , 7 RIKEN, 8 Saitama Univ. , 9 Tohoku Univ. , 10 IAC , 11 RIKEN , 12 Univ. of Tokyo , 13 NAOJ , 14 KEK , 15 Saitama Univ. , 16 RIKEN ,17
RIKEN , 18 IAC , 19 IAC , 20 NAOJ , 21 Saitama Univ. , 22 KEK , 23 Saitama Univ. , 24 KEK / SOKENDAI , 25 Univ. of Tokyo, 26 KEK / SOKENDAI , 27 Korea Univ. , 28 KEK / SOKENDAIThe Cosmic Microwave Background Radiation (CMB) is a robust evidence of the expanding Universe. It is observed
as homogeneous and isotropic microwave from the sky. To explain its features, the Inflation model is employed.
The model predicts very weak polarized pattern, B-mode, which is an imprint of the primordial gravitational waves
generated by the early inflation. The GroundBIRD telescope is under construction at present, aiming to achieve thesensitivity on the tensor-to-scalar ratio down to 0.01. One of the key elements in this experiment is the Microwave
Kinetic Inductance Detector (MKID) as the photon sensor of the system.
We have developed a readout system for the MKID. The system is consisted of three parts: Digital part (KC705+RHEA
analog board), analog part for up and down-conversions, and a computer for the control and the data acquisition.
KC705 is a commercially available evaluation board for Xilinx Kintex 7 Field Programmable Gate Array (FPGA).
RHEA board is an analog board which contains a digital to analog converter (DAC) and an analog to digital converter(ADC). The FPGA receives frequencies from the computer, and synthesizes In-phase/Quadratic-phase (I/Q)
signals as carriers for each frequency with Direct Digital Synthesizer (DDS) blocks. The I/Q signals are combined
to a single signal, frequency comb, and converted to analog signal by the DAC. This signal is upconverted to RF( 6 GHz), the resonant frequencies of MKIDs, by frequency mixers, and its amplitude and phase are changed while
passing through the MKID. This signal is down-converted, and the ADC receives the modified signal. The FPGA
channelize the signal by mixing it with the reference I/Q signals from DDS.
The channelized data is downsampled to remove the cross-talks, sinusoidal waves at the frequencies of intervals
between the frequency of the target channel and those of other channels. The cross-talks are not eliminated and leave
leakages when the frequency intervals are arbitrary values instead of the divisors of sampling frequency of the ADC.
The leakage degrades the accuracy of the readout, and becomes more significant when the sampling rate of the readoutis higher and the frequency intervals between the channels are small. We applied the Hanning window function to solve
this problem. It makes the boundaries of the downsampling window to be zero, and removes the leakage eﬀectively.
We will discuss the leakage problem; how does it degrade the accuracy and the sensitivity, and the eﬀect of thewindow function. It will become more important for the future applications which need faster sampling and higher
order multiplexing.
Figure 1. The leakage with respect to the frequency interval between the MKID resonances. The leakage is higher
for smaller frequency intervals. The minimum interval is determined by this. The leakage is on the order of 10−4 andsuppressed to 10−8 with the Hanning window.
category : Readout Techniques & Signal processing

236

237

PB-21 Evaluating and Understanding Crosstalk in Microwave SQUID Multiplexers
Douglas A. Bennett1 , Dan Becker2 , Joseph W. Fowler3 , Johnathon D. Gard4 , James P. Hays-Wehle5 , Gene C.
Hilton6 , John A. B. Mates7 , Carl D. Reintsema8 , Daniel R. Schmidt9 , Daniel S. Swetz10 , Leila R. Vale11 , Joel N.
Ullom121

National Institute of Standards and Technology, 2 National Institute of Standards and Technology, Boulder, CO USA /University of Colorado Boulder, Boulder, CO USA , 3 National Institute of Standards and Technology, Boulder, CO USA /University of Colorado Boulder, Boulder, CO USA , 4 University of Colorado Boulder, Boulder, CO USA , 5 National Instituteof Standards and Technology, Boulder, CO USA / University of Colorado Boulder, Boulder, CO USA , 6 National Institute ofStandards and Technology, Boulder, CO USA , 7 University of Colorado Boulder, Boulder, CO USA , 8 National Institute ofStandards and Technology, Boulder, CO USA , 9 National Institute of Standards and Technology, Boulder, CO USA ,10
National Institute of Standards and Technology, Boulder, CO USA , 11 National Institute of Standards and Technology,
Boulder, CO USA , 12 National Institute of Standards and Technology, Boulder, CO USA / University of Colorado Boulder,
Boulder, CO USA

Electrical crosstalk is an important property of multiplexed readout systems for low temperature detector arrays,
particularly as array sizes and event rates grow. Microwave SQUID multiplexing shows significant promise to increaseachievable array sizes. The lack of feedback in microwave SQUID multiplexers eliminates one of the major crosstalkmechanisms observed in conventional SQUID multiplexing, while the use of flux ramp modulation produces crosstalk ofan unusual character. Crosstalk mitigation in this emerging readout architecture needs to be optimized in the context
of limited resources in both physical and frequency space. To properly evaluate the levels of crosstalk, the dominantmechanisms need to be understood and experimentally characterized. We describe the nature of the crosstalk observedin our most recent generation of microwave SQUID multiplexers, present crosstalk measurements taken as part of aworking TES gamma-ray spectrometer, and compare these results to theoretical estimates.
category : Readout Techniques & Signal processing238

PB-22 Error Correcting Codes for code-division multiplexed TES detectors
Charles James Titus1 , Saptarshi Chaudhuri2 , Hsiao-Mei Cho3 , Carl Dawson4 , W. Bertrand Doriese5 , Joe W.
Fowler6 , Gene C. Hilton7 , Kent D. Irwin8 , Stephen Kuenstner9 , Dale Li10 , Kelsey Morgan11 , Carl Reintsema12 , Dan
Swetz13 , Joel Ullom14 , Betty Young15
1

Department of Physics, Stanford University, 2 Stanford University, Stanford, CA, United States , 3 SLAC, Menlo Park, CA,
United States , 4 Stanford University, Stanford, CA, United States , 5 NIST, Boulder, Co, United States , 6 NIST, Boulder, Co,
United States , 7 NIST, Boulder, Co, United States , 8 Stanford University, Stanford, CA, United States / SLAC, Menlo Park,
CA, United States , 9 Stanford University, Stanford, CA, United States , 10 SLAC, Menlo Park, CA, United States , 11 NIST,
Boulder, Co, United States , 12 NIST, Boulder, Co, United States , 13 NIST, Boulder, Co, United States , 14 NIST, Boulder, Co,
United States , 15 Stanford University, Stanford, CA, United States / Santa Clara University, Santa Clara, CA, United States

Transition Edge Sensors (TES) have proven to be highly sensitive and versatile X-ray spectrometers. Upcoming
missions, including Athena X-IFU, will rely on highly multiplexed focal planes where more than 32 TES pixels areread out using a single SQUID amplifier channel. As multiplexing factors increase, error correcting codes can provide
redundancy to failure of one or more SQUID readout devices. We have developed an error correction algorithm forcode division multiplexed TES signals that is both scalable and easily implemented in hardware. We will present thisalgorithm for error correction, as well as the result of laboratory tests to assess algorithm performance at recovering
TES channels after a SQUID failure.
category : Readout Techniques & Signal processing

239

PB-23 SQUID Characterization for Next Generation Digital Frequency Domain
Multiplexing
Maximiliano Silva-Feaver1 , Kam Arnold2
1

Department of Physics, University of California San Diego, 2 University of California San Dieog

Transition edge sensor (TES) bolometer arrays are the highest sensitivity cameras employed for millimeter wave
applications and are currently operating in the photon noise limited regime. In this regime larger arrays leads tooverall higher array sensitivity. One factor limiting array size is cost of readout in terms of thermal loading, cryogenic
complexity, and component cost. Multiplexing is employed to reduce these constraints but currently deployed arrays
have only demonstrated multiplexing factors of O(100). One avenue to increase multiplexing factors is to extend thefrequency range for the Digital Frequency Domain Multiplexing (DfMux) scheme currently used in CMB experiments
such as POLARBEAR-2, and SPT-3G. This readout multiplexing system uses SQUID amplifiers as the first-stage
amplifying element; We present a characterization of SQUID amplifiers as a function of amplifier and multiplexing
circuit design. We present results from tests on 8-turn NIST SQUID Series Arrays (SSAs) currently used by the
POLARBEAR collaboration and on a newer version of SSA s which have gradiometric input coils which are underconsideration for PB2-C, Simons Observatory, and the LiteBIRD satellite projects.
category : Readout Techniques & Signal processing240

PB-24 Combined operation of two TESs for front-end signal processing andamplification
Hiroyuki Takahashi1 , Yoshitaka Miura2 , Masashi Ohno3
1

Institute of Engineering Innovation, The University of Tokyo, 2 Department of Nuclear Engineering and Management / The
University of Tokyo , 3 Nuclear Professional School / The University of Tokyo

Conventionally, TES is used as an independent device although TES arrays are employed for some applications. In thepast, we demonstrated a parallel bias scheme with some weak link between neighboring TESs. This principle ensuresa coupling of two TESs could make it possible to coordinate two TESs operation as an active circuit. We have used asimulation code based on a two-fluid model for the investigation of such a combined operation of two TES electricallycoupled each other. Of course, in some condition the TESs become unstable. However, we could find a operating
condition and the electrical circuit that enables a stable operation. Based on such an idea, we are trying to investigate
a TES circuit mostly for low-energy photon applications. A simple bridge circuit with two TESs showed a current
gain of 3.

Fig.1 Primary TES current and secondary TES current.

241category : Readout Techniques & Signal processing

242

PB-25 Framework for Analyzing Events at High Rates in TES Microcalorimeters
Bradley K Alpert1 , W. Bertrand Doriese2 , Joseph W. Fowler3 , Young I. Joe4 , Kelsey M. Morgan5 , Galen C. O’Neil6 ,Joel N. Ullom7 , Daniel S. Swetz8
1

NIST, 2 NIST, Boulder , 3 NIST, Boulder , 4 NIST, Boulder , 5 NIST, Boulder , 6 NIST, Boulder , 7 NIST, Boulder , 8 NIST,
Boulder

At very high event rates, the exquisite energy resolving power of transition edge sensors is not easily retained due todetector nonlinearity, short averaging duration per event, and heightened sensitivity to lab environmental conditions.
After a number of false starts, we have achieved some success processing TES current pulses from x-ray excitation
rates previously unanalyzable. In particular, we demonstrate 4.5 eV resolution FWHM at 6 keV in a detector witha 1.2 ms decay time constant at a Poisson event rate of 497 /s with 53% pulse utilization. We present our approach
involving continuous system calibration and change-point detection.
In lieu of simple detector models valid to the level of precision of our devices, we develop empirical calibration
models considerably more elaborate than needed for analysis of isolated events. The eﬀort is focused on event eﬃciency
both in building such models and, from ongoing calibration data, detecting spectrometer perturbations and adjusting
the model. The approach relies on an unvarying spectrum of calibration events, and a device state space that is
eﬀectively single-dimensional (current or temperature) following a brief inductance-induced two-dimensional state
space (current and temperature). Continuous monitoring enables updating of calibration parameters for continuouschange in conditions and replacement of those parameters for discontinuous change.
This analysis approach is intended for use in TES spectrometers deployed at intense x-ray light sources such assynchrotrons and free electron lasers. For example, a TES spectrometer is under development for LCLS-II, targetingan initial excitation repetition rate of 10 kHz.
category : Readout Techniques & Signal processing243

PB-26 Thermal conductance and high frequency properties of cryogenic normal orsuperconucting semi-rigid coaxial cables in a range of 1 and 8 K
Akihiro Kushino1 , Soichi Kasai2 , Masahiro Ukibe3 , Masataka Ohkubo4
1

2

Kurume University, COAX, CO., LTD. , 3 National Institute of Advanced Industrial Science and Technology , 4 National
Institute of Advanced Industrial Science and Technology

Recently, the sizes of superconducting array detectors have been enlarging rapidly for practical applications. The
thermal conductance of wires should be reduced with keeping their transmission performance, because the superconducting large-scaled arrays need a large number of wires for those operations, which leads to increasing the heat flowfrom a room temperature environment through the wires.
The semi-rigid cable is a kind of coaxial cable with seamless outer electrical conductor surrounding center one
through insulator. This configuration generally enables low noise measurements compared to twisted pairs or coaxial
using braided wires as outer conductors. Users can bend semi-rigid cables to match their own experimental apparatus.
In order to develop a semi-rigid cable exhibiting small thermal conductance and high frequency transmission performance simultaneously, we evaluated the dependence of thermal conductance between about 1 and 8 K and transmission
characteristics at 3 K on the outer diameter of wires and materials of center and outer electrical conductors. The outer
diameter was changed from 0.86 to 1.19 mm. The electrical conductors were made of alloys, such as beryllium-copper(BeCu), brass, stainless-steel (SUS304), phosphor-bronze (PB), cupro-nickel (CuNi), and niobium-titanium (NbTi).
Thermal conductance of a commercial miniature coaxial cable with braided wires for the outer electrical conductor
was also examined for a comparison. The transmission performance of semi-rigid cables with normal conductor was
improved by plating silver with a thickness of about 3 µm on the CuNi or SUS304 center conductors. The thermal
conductance after the plating was significantly increased .
The superconducting NbTi semi-rigid cable had the smallest thermal conductance of all below 3 K along with verysmall attenuation up to 5 GHz. The NbTi calbes will play an important role for superconducting scientific instruments.
category : Readout Techniques & Signal processing

244

PB-27 High count-rate study of TES X-ray microcalorimeters with two diﬀerent Tc’s
Sang Jun Lee1
1

SLAC National Accelerator Laboratory

We have developed transition-edge sensor (TES) microcalorimeter arrays with high count-rate capability and highenergy resolution to carry out imaging spectroscopy observations of X-rays from various astronomical sources and also
the Sun. We have studied the energy resolution and throughput (fraction of processed pulses) dependency on countrate
for microcalorimeters with two diﬀerent transition temperatures (Tc). Devices with both transition temperatures were
fabricated within a single microcalorimeter array directly on top of a solid substrate where the thermal conductanceof the microcalorimeter is dependent upon the thermal boundary resistance between the TES sensor and the dielectric
substrate beneath. Because the thermal boundary resistance is highly temperature dependent, the two types of device
with diﬀerent Tc’s had very diﬀerent thermal decay times, approximately one order of magnitude diﬀerent. In ourearlier report, we achieved energy resolutions of 1.6 eV and 2.3 eV at 6 keV from lower and higher Tc devices,
respectively, using a standard analysis method based on the optimal filtering in a low flux limit. We measured thesame devices at elevated X-ray fluxes ranging from 50 Hz to 1000 Hz per pixel. In high flux limit, however, thestandard optimal filtering scheme nearly breaks down because of too frequent X-ray pile-ups. To achieve highest
possible energy resolution for a fixed throughput, we have developed an analysis scheme based on the so-called event
grade method. Using the new analysis scheme, we achieved 5.0 eV FWHM with 96% throughput for 6 keV X-rays of1025 Hz per pixel with the higher Tc device, and 5.8 eV FWHM with 97% throughput with the lower Tc device at
722 Hz.
category : Readout Techniques & Signal processing

245

PB-28 Toward large FOV high-resolution x-ray imaging spectrometers: microwave
multiplexed readout of 32 TES microcalorimeters
Wonsik Yoon1 , Joseph S. Adams2 , Simon R. Bandler3 , James A. Chervenak4 , Aaron Datesman5 , Megan E. Eckart6 ,Fred M. Finkbeiner7 , Richard Kelly8 , Caroline A. Kilnourne9 , Antoine R. Miniussi10 , Frederick S. Porter11 , John E.
Sadleir12 , Kazuhiro Sakai13 , Stephen J. Smith14 , Nicholas A. Wakeham15 , Edward Wassell16 , Samuel H. Moseley17 ,Omid Noroozian18 , Thomas R. Stevenson19 , Edward J. Wollack20 , Douglas A. Bennett21 , Dan Becker22 , Joseph D.
Fowler23 , Johnathon D. Gard24 , Gene C. Hilton25 , John A.B. Mates26 , Carl D. Reintsema27 , Daniel S. Swetz28 , Joel
N. Ullom29 , Leila R. Vale30
1NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA / University of
Maryland, Baltimore County, Baltimore, MD 21250 USA , 3 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA ,4
NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA , 5 NASA Goddard Space Flight Center, Greenbelt, MD
20771 USA / SGT, Inc., Greenbelt, MD 20706 USA , 6 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA ,7
NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA / Wyle Information Systems, McLean, VA 22102 USA ,8
NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA , 9 NASA Goddard Space Flight Center, Greenbelt, MD
20771 USA , 10 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA / Universities Space Research Association,
Columbia, MD 21046 USA , 11 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA , 12 NASA Goddard Space
Flight Center, Greenbelt, MD 20771 USA , 13 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA / Universities
Space Research Association, Columbia, MD 21046 USA , 14 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA /University of Maryland, Baltimore County, Baltimore, MD 21250 USA , 15 NASA Goddard Space Flight Center, Greenbelt,
MD 20771 USA / Universities Space Research Association, Columbia, MD 21046 USA , 16 NASA Goddard Space Flight
Center, Greenbelt, MD 20771 USA / SGT, Inc., Greenbelt, MD 20706 USA , 17 NASA Goddard Space Flight Center,Greenbelt, MD 20771 USA , 18 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA , 19 NASA Goddard Space
Flight Center, Greenbelt, MD 20771 USA , 20 NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA , 21 National
Institute of Standards and Technology, Boulder, CO 80305 USA , 22 National Institute of Standards and Technology, Boulder,
CO 80305 USA , 23 National Institute of Standards and Technology, Boulder, CO 80305 USA , 24 National Institute ofStandards and Technology, Boulder, CO 80305 USA , 25 National Institute of Standards and Technology, Boulder, CO 80305
USA , 26 National Institute of Standards and Technology, Boulder, CO 80305 USA , 27 National Institute of Standards andTechnology, Boulder, CO 80305 USA , 28 National Institute of Standards and Technology, Boulder, CO 80305 USA ,29
National Institute of Standards and Technology, Boulder, CO 80305 USA , 30 National Institute of Standards andTechnology, Boulder, CO 80305 USA

We performed a small-scale demonstration at GSFC of high-resolution x-ray TES microcalorimeters read out using a
microwave SQUID multiplexer. This work is part of our eﬀort to develop detector and readout technologies for future
space based x-ray instruments such as the microcalorimeter spectrometer envisaged for Lynx, a large mission concept
under development for the Astro 2020 Decadal Survey. In this paper we describe our experiment, including detailsof a recently designed, microwave-optimized low-temperature setup that is thermally anchored to the 50 mK stageof our laboratory ADR. Using a ROACH2 FPGA at room temperature, we simultaneously read out 32 pixels of a
GSFC-built detector array via a NIST-built multiplexer chip with Nb coplanar waveguide resonators coupled to RF
SQUIDs. The resonators are spaced 6 MHz apart (at 5.9 GHz) and have quality factors of 15,000. Using flux-ramp
modulation frequencies of 160 kHz we have achieved spectral resolutions of ¡ 3 eV FWHM on each pixel at 6 keV. We
will present the measured system-level noise and maximum slew rates, and briefly describe the implications for future
detector and readout design.
category : Readout Techniques & Signal processing246

PB-29 A high-throughput automated test system for dc parametric evaluation andquality assurance of TDM and CDM SQUID multiplexers
Carl D Reintsema1 , Doug A Bennett2 , Ed Dennison3 , Malcolm Durkin4 , William B Doriese5 , Joseph D Fowler6 ,Johnathan D Gard7 , Arpi Grigorian8 , Jim Hays-Wehle9 , Gene C Hilton10 , Johannes Hubmayr11 , Galen C O’Neil12 ,John A B Mates13 , Kelsey M Morgan14 , Dan Schmidt15 , Robert Stevens16 , Leila R Vale17 , Joel N Ullom18 , Kent D
Irwin19 , Saptarshi Chaudhuri20 , Carl Dawson21 , C J Titus22
1

NIST Quantum Sensors Group, 2 NIST , 3 NIST , 4 NIST , 5 NIST , 6 NIST , 7 NIST , 8 University of Colorado , 9 NIST , 10 NIST
, 11 NIST , 12 NIST , 13 NIST , 14 NIST , 15 NIST , 16 University of Colorado , 17 NIST , 18 NIST , 19 Stanford University ,20
Stanford University , 21 Stanford University , 22 Stanford University

The successful realization and broad deployment of TES based detector systems has led to significant demand for timedivision and code-division SQUID multiplexers (TDM and CDM) as essential components of the cryogenic readout
chain. TDM and CDM circuits are produced by the Boulder Microfabrication Facility in large quantities and multiple
varieties to meet the needs of various bolometric and calorimetric applications. In most cases the basic functionalityof these devices must be verified before they are passed along to internal or external collaborators for integration
into scientific instruments. Until recently, these measurements were made by hand in a slow and arduous process thatcreated a bottleneck in our supply and delivery chain. Over the past year, the instrumentation and methodology of themeasurements has been completely revamped resulting in vastly improved throughput and enhanced data products.
We present a full description of the measurement system including results from the application of the test process toflux-activated switch style multiplexers. The utility of this approach for identifying fabrication trends, yield indicators,
and common failure modes will be demonstrated.
category : Readout Techniques & Signal processing

247

PB-30 Cryotron Switches for Current-Summed Code-Division Multiplexing in TES
ArraysJoel Weber1 , Peter Lowell2 , Malcolm Durkin3 , John Mates4 , Carl Reintsema5 , Gene Hilton6 , Daniel Schmidt7 ,Daniel Swetz8 , Kent Irwin9 , Joel Ullom10
1

Quantum Sensors Group, National Institute of Standards and Technology, 2 National Institute of Standards and Technology ,3National Institute of Standards and Technology , 4 National Institute of Standards and Technology , 5 National Institute ofStandards and Technology , 6 National Institute of Standards and Technology , 7 National Institute of Standards andTechnology , 8 National Institute of Standards and Technology , 9 Department of Physics, Stanford University , 10 National
Institute of Standards and Technology

Next-generation applications of TES arrays in x-ray astrophysics and materials analysis will require instrument designs
with 105 to 106 pixels. These large arrays provide an increased collection area and enable higher count rates resulting in
improved imaging resolution, reduced measurement integration time, and expanded capability towards high-flux x-ray
sources. To scale arrays by several orders of magnitude beyond the current state-of-the-art, device readout techniques
will need to be significantly improved. Up to now, several multiplexing strategies, including time-division (TDM) andfrequency-division multiplexing (FDM), have been developed and successfully integrated with TES arrays. In TDM,
individual TESs within a column are read out successively. Consequently, the eﬀective sampling rate is reduced,
resulting in an aliased noise penalty. FDM avoids this pitfall but relies on physically large LC circuitry and potentially
suﬀers sensor resolution degradation from the use of ac sensor biases.
Current-summed code-division multiplexing (I-CDM) [1] is an alternative to TDM and FDM that, in many ways,
combines the attractive features of both. In I-CDM, signals from all TESs in a column are coupled to a common readout
SQUID with controllable polarity. Suitable polarity modulation creates an orthogonal basis set that can be used to
distinguish signals from diﬀerent sensors. I-CDM avoids noise aliasing, can be physically compact, and is compatible
with dc bias. Because switching control currents are implemented on a row by row basis and device readout on acolumn by column basis, wiring schemes are readily scalable. High performance double-pole, double-throw switches
are a critical requirement for I-CDM. Recently, NIST has developed cryotron switches for a variety of applications,
including I-CDM [2]. A cryotron switch consists of a signal element switched between superconducting (closed) andnormal (open) states by a separate magnetic coil. These switches surpassed available measurement bandwidth, yielding
switching times faster than 200 ns. Device currents up to 900 uA were switched using 2 mA of control current. A
notable attraction of I-CDM with cryotron switches is the possibility of in-focal plane multiplexing of TES detectors
where the readout circuitry is located underneath suspended, overhanging absorbers. We present recent experimental
eﬀorts to improve cryotron performance by increasing maximum device currents while reducing control currents. In
addition, we describe ongoing eﬀorts to model and design I-CDM circuitry.
[1] K. Irwin et al, Journal of Low Temperature Physics, 167, 588-594 (2012)[2] P. Lowell et al, Applied Physics Letters, 109, 142601 (2016)
category : Readout Techniques & Signal processing

248

PB-31 Measurements of Improved TDM and Prototype TDM+ Multiplexing Circuits
Malcolm Durkin1 , Carl D Reintsema2 , Edward V Denison3 , William B Doriese4 , Johnathon D Gard5 , Gene C
Hilton6 , Kent D Irwin7 , Kelsey M Morgan8 , Galen C O’Neil9 , Robert Stevens10 , Daniel S Swetz11 , Leila R Vale12 ,Joel N Ullom13
1

University of Colorado Boulder, 2 National Institute of Standards and Technology , 3 National Institute of Standards andTechnology , 4 National Institute of Standards and Technology , 5 National Institute of Standards and Technology , 6 National
Institute of Standards and Technology , 7 Stanford University , 8 National Institute of Standards and Technology , 9 National
Institute of Standards and Technology , 10 National Institute of Standards and Technology , 11 National Institute of Standards
and Technology , 12 National Institute of Standards and Technology , 13 National Institute of Standards and Technology

The successful deployment of detector systems based on Transition Edge Sensors (TESs) at facilities around theworld has led to demand for larger TES detector systems such as the Athena X-IFU and the proposed Lynx X-ray
microcalorimeter array. Eﬀective readout of these large sensor arrays motivates improved multiplexers with large
multiplexing factors. To meet the energy resolution requirements, these multiplexers must combine low levels of
readout noise with low levels of cross talk.
To maximize the multiplexing factor in Time Division Multiplexing (TDM) SQUID circuits, it is desirable that therow time be as short as possible. Rapid switching between rows requires large analog bandwidth and small amplitude,
fast decaying switching transients. We describe recent work to understand and minimize these transients so as toachieve 160 ns row times in large format multiplexing measurements while achieving a total readout noise level of 0.19
μΦ 0/√ Hz .
Distant pixel cross-talk via a shared SQUID feedback line is another issue in existing TDM circuits. In thesearchitectures, a feedback line is shared between the 1st stage SQUID readout amplifiers of every pixel in an arraycolumn. While the amplifiers can be turned oﬀ by setting the SQUID bias to zero, the feedback line remains inductively
coupled to the unbiased SQUID, resulting in cross-talk between on pixels and oﬀ pixels. Previous TDM designs
have sought to reduce this source of cross-talk by canceling the feedback signal applied to oﬀ SQUIDs using
a dummy squid coupled in the opposite direction. However, this geometric mitigation strategy cannot completely
eliminate coupling due to the variable inductance of the Josephson Junctions in SQUIDs.
The TDM+ architecture seeks to eliminate this source of cross talk by using superconducting switches to bypass
the feedback coils not in use. In this presentation, we show measurements of the first prototypes of this new generationof multiplexers and compare these results with TDM circuits currently being produced at NIST.
category : Readout Techniques & Signal processing

249

PB-32 Intrinsic losses and noise of high-Q lithographic MHz LC resonators forfrequency division multiplexing
Luciano Gottardi1 , Jan van der Kuur2 , Marcel P. Bruijn3 , Anton van der Linden4 , Mikko Kiviranta5 , Hiroki
Akamatsu6 , K. Ravensberg7
1

SRON - Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research, Utrecht, The
Netherlands , 3 SRON Netherlands Institute for Space Research, Utrecht, The Netherlands , 4 SRON Netherlands Institute forSpace Research, Utrecht, The Netherlands , 5 VTT, Espoo, Espoo, Finland , 6 SRON Netherlands Institute for Space Research,
Utrecht, The Netherlands, 7 SRON Netherlands Institute for Space Research, Utrecht, The Netherlands

We are developing the frequency division multiplexing (FDM) read-out for the superconducting transition-edge sensors
arrays of the X-IFU instrument on board of Athena and of the SAFARI instrument on board of SPICA.
An essential component of the FDM is the array of narrow band superconducting resonators, each consisting oflithographically made inductors and capacitors. In the standard FDM configuration, the LC resonators are connected
in series with the input coil of a low noise two-stage SQUID amplifier. In this work we have modified the electrical
scheme to decouple the SQUID amplifier from the LC filters in order to measure their intrinsic properties. We reporton the intrinsic losses and on the noise of high-Q superconducting LC resonators, with resonant frequencies ranging
between 1 and 5 MHz, measured at temperature from 70 to 500 mK.
category : Readout Techniques & Signal processing

250Category C : Fabrication &Implementation Techniques251PC-1 Microfabrication Developments for future Instruments using KID Detectors
J. GOUPY1 , A. BENOIT2 , A. BIDEAUD3 , O. BOURRION4 , M. CALVO5 , A. CATALANO6 , E.F.C. DRIESSEN7 ,A. GOMEZ8 , S. LECLERCQ9 , F. LEVY-BERTRAND10 , J.F. MACIAS-PEREZ11 , A. MONFARDINI12 , K.F.
SCHUSTER13
1

CNRS, 2 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France , 3 Institut Neel & Universite Joseph Fourier,
CNRS, Grenoble, France , 4 LPSC, Universite Grenoble-Alpes, CNRS/IN2P3, Grenoble, France , 5 Institut Neel & Universite
Joseph Fourier, CNRS, Grenoble, France , 6 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France / LPSC,
Universite Grenoble-Alpes, CNRS/IN2P3, Grenoble, France , 7 Institut de Radio Astronomie Millimetrique (IRAM), Grenoble,
France , 8 Centro de Astrobiologia, Madrid, Spain , 9 Institut de Radio Astronomie Millimetrique (IRAM), Grenoble, France ,10
Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France , 11 LPSC, Universite Grenoble-Alpes, CNRS/IN2P3,
Grenoble, France , 12 Institut Neel & Universite Joseph Fourier, CNRS, Grenoble, France / LPSC, Universite Grenoble-Alpes,
CNRS/IN2P3, Grenoble, France , 13 Institut de Radio Astronomie Millimetrique (IRAM), Grenoble, France

The NIKA2 instrument, operating at the 30 meters telescope of the IRAM, demonstrates that the aluminum LEKID
technology is a state of the art solution for detectors dedicated to millimeter wave astronomy. Following this path,several instrumental projects envisage today the use of the LEKID technology. For covering the full 60 GHz ? 600 GHz
band, of interest for CMB-oriented experiments, we are exploring new materials and solutions. Bi-layers or tri-layersof titanium and aluminum are used to address the 60 GHz ? 100 GHz range. Tantalum and vanadium are tested withaluminum to optimize the responsivity in the high end of the band. We present our latest results on such multilayers
and materials. Furthermore, we will present an update on our development of silicon optical lenses, to reduce thehigh frequency photons absorption. In order to minimize the boundary reflections at the silicon, we introduce thethermal-compression process to add anti-reflection layers on curved surfaces.
category : Fabrication & Implementation Techniques252

PC-2 Electrical contacts on germanium at cryogenic temperatures (¡ 300 mK)
Ugo Lo Cicero1 , Flavio Nuzzo2 , Jean-Luc Sauvageot3 , Francesca Chiodi4 , Dominique Debarre5 , Salvatore Ferruggia
Bonura6 , Luisa Sciortino7 , Alfonso Collura8 , Marco Barbera9
1

Osservatorio Astronomico di Palermo, INAF, 2 Istituto Nazionale di Astrofisica / OAPA / Universita degli Studi di Palermo /DFC , 3 Commissariat a l’Energie Atomique de Saclay / DRF, IRFU, Departement d’Astrophysique, LSIS , 4 Centre deNanosciences et de Nanotechnologies / CNRS, Univ. Paris-Sud, Universite Paris-Saclay , 5 Centre de Nanosciences et deNanotechnologies / CNRS, Univ. Paris-Sud, Universite Paris-Saclay , 6 Istituto Nazionale di Astrofisica / OAPA / Universita
degli Studi di Palermo / DFC , 7 Universita degli Studi di Palermo / DFC , 8 Istituto Nazionale di Astrofisica / OAPA ,9Istituto Nazionale di Astrofisica / OAPA / Universita degli Studi di Palermo / DFC

Germanium electrical resistivity shows a strong dependency on temperature below 300 mK. The material is thus
suitable to fabricate accurate and reliable cryogenic temperature sensors and has been successfully used to build
high-resolution energy-dispersive microcalorimeter detectors.
The electrical contacts used in a germanium detector to measure its resistance have to show an ohmic behaviour,
since a strong rectifying eﬀect can alter the measurements accuracy. Ion implantation or metal diﬀusion into germanium
are commonly employed in order to obtain ohmic contact, but these techniques generally imply heat treatments athigh temperatures.
Within an eﬀort to develop planar processes to build arrays of germanium cryogenic microcalorimeters, we haveexperimented with two techniques to fabricate electrical contacts on germanium that do not require high temperatureprocesses. The first one is based on a surface localized high doping of germanium by Gas Immersion Laser Doping(GILD), the second one consists of an indium deposition followed by a mild heat treatment. We fabricated GILD
and indium electrical contacts on a set of p-type compensated Neutron Transmutation Doped (NTD) germanium
samples and performed an electrical characterization at temperatures between 30 mK and 300 mK. Here, we show thecomparison between the two contacts fabrication techniques, reporting the data measured at diﬀerent temperaturesand germanium doping levels.
category : Fabrication & Implementation Techniques253

PC-3 Hierarchical sinuous phased array for increased mapping speed of multichroic
focal planes
Ari Cukierman1 , Adrian T. Lee2 , Christopher Raum3 , Aritoki Suzuki4 , Benjamin Westbrook5
1

Department of Physics, University of California, Berkeley, 2 Department of Physics, University of California, Berkeley / Radio
Astronomy Laboratory, University of California, Berkeley / Physics Division, Lawrence Berkeley National Laboratory , 3 Radio
Astronomy Laboratory, University of California, Berkeley , 4 Department of Physics, University of California, Berkeley / Radio
Astronomy Laboratory, University of California, Berkeley , 5 Department of Physics, University of California, Berkeley / Radio
Astronomy Laboratory, University of California, Berkeley

We present the design, fabrication and performance of a hierarchical sinuous-antenna phased array coupled to transitionedge-sensor (TES) bolometers for measurements of the cosmic microwave background (CMB). To eﬃciently cover abroader range of frequencies, many CMB experiments have begun to deploy multichroic pixels. For a given cryogenic
and optical design, the pixel size that optimizes the mapping speed is frequency-dependent and increases with wavelength. If a multichroic pixel is the same size at all frequencies, then the mapping speed will be optimal in at mostone frequency band. To achieve optimal mapping speed at all frequencies, a pixel size that varies with frequency isneeded. This can be accomplished by creating phased arrays from neighboring pixels, where the size of each phasedarray is chosen independently for each frequency band. As the array unit, we choose a lenslet-coupled sinuous antenna
on account of its wide bandwidth, dual polarization and constant beam waist. We find that the array factor tends
to compensate for beam non-idealities, so that the sinuous antenna can be substantially undersized relative to thesingle-element case; this frees up valuable focal-plane area for bolometers, bandpass filters, summing networks, readout circuitry, etc. An additional benefit of a hierarchical phased array is the reduced readout requirement: since thelow frequencies are arrayed to increase their mapping speeds, the detector count scales approximately logarithmicallywith the number of frequency bands. Here we present measurements from a prototype device, in which hierarchicaltriangular arrays are used at 90, 150 and 220 GHz to keep the eﬀective pixel size and, therefore, the beam widthroughly constant across the entire frequency range. The fabrication process is described, and the utility of hierarchicalphased arrays is discussed in the context of upcoming CMB experiments.
category : Fabrication & Implementation Techniques254

PC-4 Design and fabrication techniques used to optimize MKID arrays for
BLAST-TNG
Christopher M McKenney1 , Johannes Hubmayr2 , Michael R Vissers3 , Jiansong Gao4 , Bradley Dober5 , Gene C
Hilton6 , Jason E Austerman7 , Dale Li8
1

National Institute of Science and Technology, 2 National Institute of Science and Technology , 3 National Institute of Scienceand Technology , 4 National Institute of Science and Technology , 5 National Institute of Science and Technology , 6 National
Institute of Science and Technology , 7 National Institute of Science and Technology , 8 SLAC National Accelerator Laboratory

We report on the layout and fabrication techniques developed for the focal planes of the Balloon-borne Large Angular
Scale Telescope (BLAST-TNG), scheduled to be the first balloon payload to utilize arrays of microwave kinetic
inductance detectors (MKIDs). Implementation of ∼ 3000 resonators in the presence of readout constraints set
by limitations in power, cryogenic cabling, and electronic bandwidth of a balloon mission required an improved
understanding of the sources of frequency scatter in TiN/Ti multilayer films and ultimately the development of a
stepper compliant tiling scheme. This scheme allows thousands of unique pixels to be laid out in a semi-automatedmanner using a small number of reticles with minimal lithographic uncertainty. We detail the layout approach andshow its eﬃcacy through dedicated test structures that map out the intrinsic TiN/Ti multilayer transition temperature
variations as well as lithographic uncertainties which contribute to frequency scatter. We find that percent-level
wafer-scale variations exist. However since the frequency scatter is less than 10−3 on the size scale of near neighborpixels, careful engineering allows low instances of frequency collisions. With this knowledge, we designed the 3,244
superconducting resonators of BLAST-TNG to be read out using five ROACH2-based readout modules, which eachhave 500 MHz of readout bandwidth. A balance between single pixel sensitivity, which in our pixel architecture scales
as 1/Q, and high multiplexed density was considered. Ultimately our material choice and tiling scheme enables 85%of the detectors to be separated by more than 5 linewidths from its nearest neighbors, when operated from a 275 mK
bath. Based on these results, we make performance predictions for future arrays fabricated on 150 mm wafers toacheive ∼104 – 105 pixel counts for next-generation astronomical focal planes.
category : Fabrication & Implementation Techniques255

PC-5 Low-Tc superconducting TES for a Cuore UPgrade with Particle IDentification(CUPID)
Raul Hennings-Yeomans1
1

UC Berkeley

We present measurements of the Tc suppression in superconducting Iridium films, in the range of ∼18-100 mK. We
demonstrate a simple and eﬀective way to suppress Tc of superconducting Iridium, through the proximity eﬀect, byusing Ir/Au and Ir/Pt bilayers as well as Au/Ir/Au trilayers. We study Tc suppression of Ir/Au and Ir/Pt as afunction of Iridium deposition temperature between 100-600 ◦ C. We also present results of Tc suppression on Iridiumby deposition at room temperature in Au/Ir/Au trilayers and Ir/Pt bilayers. Measurements of the relative impedance
between the Ir/Pt bilayers and Au/Ir/Au trilayers fabricated at room temperature show factor of ∼10 higher in
the Ir/Pt case. These new, room temperature-deposited films, could play a key role in the development of scalable
superconducting transition edge sensors that require low-Tc films to minimize heat-capacity and maximize energy
resolution, while keeping high-yield fabrication methods. This work was done in the context of R&D for a futurebolometric experiment in search for neutrinoless double beta decay called CUPID (Cuore UPgrade with Particle
IDentification).
category : Fabrication & Implementation Techniques256PC-6 Commercialization of micro-fabrication of antenna-coupled Transition Edge
Sensor bolometer detectors for studies of the Cosmic Microwave BackgroundAritoki Suzuki1 , Chris Bebek2 , Maurice Garcia-Sciveres3 , Stephen Holland4 , Akito Kusaka5 , Adrian T Lee6 ,Nicholas Palaio7 , Natalie Roe8 , Leo Steinmetz91

Radio Astronomy Laboratory, University of California, Berkeley, 2 Physics Division, Lawrence Berkeley National Laboratory ,3Physics Division, Lawrence Berkeley National Laboratory , 4 Physics Division, Lawrence Berkeley National Laboratory ,5Physics Division, Lawrence Berkeley National Laboratory / Department of Physics, University of Tokyo , 6 Department of
Physics, University of California, Berkeley / Physics Division, Lawrence Berkeley National Laboratory , 7 Engineering
Division, Lawrence Berkeley National Laboratory , 8 Physics Division, Lawrence Berkeley National Laboratory , 9 Departmentof Physics, University of California, Berkeley

We report on the development of commercially fabricated multi-chroic antenna coupled Transition Edge Sensor(TES) bolometer arrays for Cosmic Microwave Background (CMB) polarimetry experiments. CMB polarimetry experiments have deployed instruments in stages. Stage-II experiments deployed with O(1,000) detectors that reported
successful detection of B-mode (divergent free) polarization pattern in the CMB. Stage-III experiments have recently
started observing with O(10,000) detectors with wider frequency coverage.
A concept for a Stage-IV experiment, CMB-S4, is emerging to make a definitive measurement of CMB polarizationfrom the ground with O(500,000) detectors. The orders of magnitude increase in detector count for CMB-S4 requires
a new approach in detector fabrication to increase fabrication throughput. We report on collaborative eﬀorts with twocommercial micro-fabrication foundries to fabricate antenna coupled TES bolometer detectors.
The detector design is based on the sinuous antenna coupled dichroic detector from the POLARBEAR-2 experiment. The TES bolometers showed the expected I-V response and the RF performance agrees with simulation. We will
discuss the motivation, design consideration, fabrication processes, test results, and how industrial detector fabrication
could be a path to fabricate hundreds of detector wafers for future CMB polarimetry experiments.
category : Fabrication & Implementation Techniques257

PC-7 The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status
Benjamin Westbrook1
1

UC Berkeley

We present on the status of POLARBEAR-2 and Simons Array detector fabrication. The Simons Array is an arrayof three Cosmic Microwave Background (CMB) polarization sensitive telescopes located at the POLARBEAR (PB)
site in Northern Chile. As the successor PB experiment each telescope and receiver combination is named as PB-2A,
PB-2B, and PB-2C. PB-2A and -2B will have identical receivers operating at 90 and 150 GHz while PB2-C will housea receiver operating at 220 and 270 GHz. Each receiver will have 1,897 polarization sensitive pixels with 2 transitionedge sensor (TES) bolometers per band and polarization (for a total of 7,588 TES bolometers per telescope). We haveproduced 7 candidate wafers for PB2-A wafers which are undergoing detailed characterization prior to deployment in
the Fall of 2017. Characterization from a witness pixel co-fabricated with these wafers indicates that these wafers meet
our original specifications for the PB2-A receiver. Production of the PB-2B focal plane is ongoing and is expected
to be completed by the end of 2017 for deployment in summer of 2018. Initial designs and prototype devices havealready been fabricated for PB2-C which will also deploy in 2018.
category : Fabrication & Implementation Techniques258

PC-8 Development of dual-polarization sensitive KIDs for CMB measurements
Kenji Kiuchi1 , Jihoon Choi2 , Ryo Koyano3 , Satoru Mima4 , Shugo Oguri5 , Chiko Otani6 , Munehisa Semoto7 , Tohru
Taino81

RIKEN Center for Advanced Photonics, 2 IBS , 3 Saitama University , 4 RIKEN , 5 RIKEN , 6 RIKEN , 7 Saitama University ,8
Saitama University

KIDs are very sensitive millimeter wave detector suitable for CMB measurements. Some group already reported thatthe sensitivities of their detectors are limited by photon noise under the loading power comparable to the typicalground based CMB experiment. Once the detector achieved photon noise limited sensitivity, increasing the number ofdetectors is the straightforward way to improve the measurement sensitivity. KIDs are promising detector to develop
a large number of detector arrays thanks to the intrinsic capability of frequency division multiplexing.
Very characteristic polarization patterns called B-modes on the CMB anisotropy map are a next biggest target
of CMB experiments. The polarization sensitive antennas and millimeter wave circuit to transmit an energy absorbed
at antennas to KIDs are required to measure the B-modes. We designed the horn coupled dual-polarization sensitive
KIDs array. And fabricated a first prototype of our detector.
Each pixel of our detector consists of KIDs part and millimeter wave circuit part. Each part is evaluated separately.
A Hybrid Nb-Al KIDs structure is employed to improve the responsivity. The quality factor of our detector required to
be greater than 50,000 and our fabricated KIDs already satisfied it. And responsivity of our device is also reasonablelevel. The characteristics of the millimeter wave circuit components are measured using the test device. In thisconference, we will report the status of our development.
category : Fabrication & Implementation Techniques259

PC-9 TiN-Al MKID Polarimeter Arrays Optimized for Balloon-borne Submillimeter
Imaging on BLAST-TNG
Michael R Vissers1 , The BLAST2
1National Institute of Standards and Technology - Boulder, 2 Collaboration

Microwave Kinetic Inductance Detectors (MKIDs) have held promise as the focal plane sensing elements in large-format
imaging arrays for over a decade and have found application in several ground-based instruments. In this presentation,
we discuss the first implementation of MKIDs for a balloon-borne instrument. We have built three, large-format MKID
arrays for the Balloon-borne Large-Aperture Submillimeter Telescope ? The Next Generation (BLAST-TNG), whichis scheduled for Antarctic launch in December 2017. Each monolithic 100mm diameter array is sensitive to a diﬀerent
waveband centered at 250 micron, 350 micron, or 500 micron; and a each microwave feedline addresses between
466 and 938 resonators depending on the array. Designing for space-like low photon loads, polarization-sensitivity,
diﬀerent frequency bands, and 275 mK operation all pose unique challenges. We address these challenges by employing
feedhorn-coupled, dual-polarization sensitive pixels fabricated from TiN/Ti multilayers that combine high responsivity,
high uniformity, low loss, and a tunable superconducting Tc. Here, we present the detailed design and fabrication ofthese arrays, which includes an optimized quarter wavelength silicon backshort realized by use of a silicon on insulator(SOI) wafer; aluminum patching of the TiN/Ti absorbing inductor to increase response and tune the eﬀective optical
coupling impedance; and a semi-automated layout scheme to make a stepper-compliant lithography process that tiles
identical stepper images across the array and then trims them individually to minimize their frequency scatter. This
results in high quality, easily reconfigurable, and uniform arrays of MKIDs. We show measurements that demonstratehigh pixel yield, ¿ 98% polarization isolation, and a noise equivalent power (NEP) limited by photon noise at the
expected in-flight photon load.
category : Fabrication & Implementation Techniques260PC-10 A calibration target for cm-range instruments.
Tommaso Ghigna11

Physics Department, Oxford University

High precision measurements in radio astronomy require a good knowledge of noise properties of the receiver in use.
For this purpose we are working on the design, fabrication and test of a pyramidal dry cold load to characterize
receivers in the 4-20 GHz frequency range. At this frequencies, receivers make use of low noise amplifiers with typicalnoise temperature below 5 K. From simulations and experience the overall receiver noise temperature doesn t exceed
10-15 K, therefore, to be able to measure a similar noise level with a 5% accuracy, we need to design a target with abrightness temperature uncertainty smaller than 0.1 K.
The main aim of this work is to test the performances and characterize the noise properties of SKA Band 5 receiver(4.6-15.3 GHz) and NextBASS prototype receiver (6-20 GHz), both under development.
I will present the analysis conducted to design the load to meet the required thermal and electromagnetic specifications.
category : Fabrication & Implementation Techniques261

PC-11 Design and Fabrication of Multichroic Feedhorn-Coupled MKID Arrays
Yanru Song1 , Maximilian H. Abitbol2 , Peter A. R. Ade3 , Sean Bryan4 , Hsiao-Mei Cho5 , Rahul Datta6 , Peter Day7 ,Simon Doyle8 , Daniel Flanigan9 , Kent Irwin10 , Bradley R. Johnson11 , Glenn Jones12 , Sarah Kernasovskiy13 , Dale
Li14 , Phil Mauskopf15 , Heather McCarrick16 , Jeﬀ McMahon17 , Amber Miller18 , Giampaolo Pisano19 , Carole Tucker20
1

School of Physical Science and Technology, Shanghai Tech University, 2 Department of Physics, Columbia University, New
York, NY, 10027, USA , 3 School of Physics & Astronomy, Cardiﬀ University, Cardiﬀ, CF, 243AA, UK , 4 School of Earth andSpace Exploration, Arizona State University, Tempe, AZ, 85287, USA , 5 SLAC National Accelerator Laboratory, Menlo Park,CA, 94025, USA , 6 NASA, Goddard Space Flight Center, Greenbelt, MD, 20771, USA , 7 NASA, Jet Propulsion Lab,
Pasadena, CA, 91109, USA , 8 School of Physics & Astronomy, Cardiﬀ University, Cardiﬀ, CF, 243AA, UK , 9 Department of
Physics, Columbia University, New York, NY, 10027, USA , 10 Department of Physics, Stanford University, Stanford, CA,94305-4085, USA / SLAC National Accelerator Laboratory, Menlo Park, CA, 94025, USA , 11 Department of Physics,
Columbia University, New York, NY, 10027, USA , 12 Department of Physics, Columbia University, New York, NY, 10027,
USA , 13 Department of Physics, Stanford University, Stanford, CA, 94305-4085, USA , 14 SLAC National Accelerator
Laboratory, Menlo Park, CA, 94025, USA , 15 School of Earth and Space Exploration, Arizona State University, Tempe, AZ,
85287, USA , 16 Department of Physics, Columbia University, New York, NY, 10027, USA , 17 Department of Physics,
University of Michigan, Ann Arbor, MI, 48103, USA , 18 College of Letters, Arts and Sciences, University of Southern
California, Los Angeles, CA, 90089, USA , 19 School of Physics & Astronomy, Cardiﬀ University, Cardiﬀ, CF, 243AA, UK ,20
School of Physics & Astronomy, Cardiﬀ University, Cardiﬀ, CF, 243AA, UK

Utilizing the advantageous combination of a high optical eﬃciency feedhorn-coupled architecture and the easy readout
scheme with high multiplexing factors from microwave kinetic inductance detectors (MKIDs), we developed a novel
hybrid design: feedhorn-coupled polarization-sensitive MKID arrays. The incoming radiation is coupled from feedhorns to planar orthomode transducers (OMTs). Each polarization is read out by an MKID. The prototype MKID
array contains 23 multichroic polarization-sensitive pixels resulting in 92 MKIDs which are coupled to only one feedline. We designed the dual frequency bands to be 125-170 GHz and 190-280 GHz for simultaneous observation ofpolarization from both the cosmic microwave background (CMB) and Galactic dust emission. These OMT-coulpled
MKID arrays are fabricated on ultra-high purity (UHP) silicon substrates to achieve high internal quality factors withthin membranes under each OMT for high optical eﬃciency. We start with a bonded silicon-on-insulator (SOI) wafer,
which is a composed of 5 microns of UHP silicon, 500 nanometer silicon dioxide, and a 350 micron silicon handle wafer.
Aluminum is used for the sensing region of the resonators, in which Cooper pair breaking alters the kinetic inductanceof the film. All other microwave elements are made of niobium films and silicon nitride as the dielectric material.
Prototype all-niobium resonators reach internal quality factors of 400,000 in dark conditions, and the coupling quality
factors are 30,000-100,000. In this paper, we present the design and fabrication of prototype arrays as well as somepreliminary results.
category : Fabrication & Implementation Techniques262

PC-12 Fabrication and Characterization of (100) Silicon Membranes for a Multi-beam
Superconducting Heterodyne Receiver
Shohei Ezaki1 , Wenlei Shan2 , Matthias Kroug3 , Takafumi Kojima4 , Alvaro Gonzalez5 , Shin’ichiro Asayama6 ,Takashi Nogchi7
1

National Astronomical Observatory of Japan, 2 National Astronomical Observatory of Japan , 3 National Astronomical
Observatory of Japan , 4 National Astronomical Observatory of Japan , 5 National Astronomical Observatory of Japan ,6
National Astronomical Observatory of Japan , 7 National Astronomical Observatory of Japan

Narrow field of view (FOV) is one of the significant limitations of a radio telescope for large area surveys. Aiming to extend the FOV of the radio telescopes, we started to develop multi-beam superconducting heterodyne receiver which is highly compact and can accommodate more pixels than before. The concept for the multi-beamsuperconducting heterodyne receiver is implementing planar orthomode transducers (OMTs) and SuperconductorInsulator-Superconductor (SIS) circuits into an integrated circuit (IC). The fabrication of membranes is one of themost important techniques for these ICs, because the planar OMTs and wave probes that couples local oscillator
power in the IC are fabricated on the membranes. As a prestudy before the IC fabrication, we fabricated (100) silicon
membranes of 3 mm in diameter on the surface of silicon on insulator (SOI) substrates, and the characteristics of themembranes were investigated.
Two pieces of 15 mm square SOI substrates were used for the membrane fabrication. The SOI substrates consistof a 6 μ m thick (100) silicon device layer on a 1 μ m thick buried oxide (BOX) layer of amorphous SiO2 followed by
a 400 μ m thick (100) silicon handle layer. The handle layer of one SOI substrate was etched using deep reactive ion
etching process with the BOX layer remained together with the device membrane. The BOX layer of the other SOI
substrate, however, was removed using C4F8 based plasma etching after the handle layer etching. Both (100) silicon
membranes are 3 mm in diameter.
The surfaces of both (100) silicon membranes were observed at room temperature using the scanning white lightinterferometer system. Figure (a) and (b) show the 3 dimensional profiles of the (100) silicon membranes with BOX
layer and without BOX layer, respectively. We found that the degrees of curving of the membrane caused by stressare pronounced. The (100) silicon membranes with BOX layer and without BOX layer have the arc-like deformation
with maximum height of 30.7 μ m and 5.7 μ m, respectively. It shows the (100) silicon membranes of SOI substrates
are eﬀectively flattened by etching BOX layers under the (100) silicon device layers.
Both (100) silicon membranes were cooled from room temperature to 4 K by the Giﬀord-McMahon refrigerator
to inspect how the deformation may change at low temperature. The surfaces of the (100) silicon membranes wereobserved using the optical microscopy. Both (100) silicon membranes survived at 4 K. The deformation of both (100)silicon membranes were observed to become more significant near 200 K as shown figure (c). However the wrinkles
of both (100) silicon membranes disappeared below about 180 K as shown figure (d). This phenomenon indicates thedeformation of the (100) silicon membranes at low temperature depends on the properties of the (100) silicon of thedevice layers and independent of BOX layers under the (100) silicon membranes.

263

category : Fabrication & Implementation Techniques264PC-13 Investigating the Eﬀect of Fabrication Processes and Material Properties tothe Large Transition Edge Sensor Array Performance for the South Pole Telescope 3G
Experiment
Junjia Ding1 , SPT-3G collaboration
1

Argonne National Laboratory - Materials Science Division

The cosmic microwave background (CMB) is remnant radiation from the early universe that provides a wealthof information leading to many breakthroughs in our theory of cosmology. Current and future CMB experiments
aim to measure the CMB polarization precisely with the goal of exploring inflation physics and neutrino mass. In
order to precisely measure the CMB polarization, especially the parity violating B-mode polarization pattern, a focal
plane with approximately 2690 pixels (6 transition-edge sensor (TES) bolometers per pixel) has been designed andfabricated. The focal plane contains 10 wafers of detector arrays and it has been installed in the South Pole Telescopeat the end of 2016 for the latest generation of CMB experiment (SPT-3G). In order to further improve the detector
performance, it is critical to understand the eﬀect of fabrication process and material properties to such a large TES
detector array. In this work, we will discuss how the properties of the detector key components, i. e. the dielectric
layer, the microstrip in-line filters, the TES film configurations and the thermal links of the TES bolometers can beextracted and investigated basing on the full detector array testing results.
This work was supported in part by the Oﬃce of Science and the Oﬃce of Basic Energy Sciences of the US
Department of Energy under Contract DE-AC02- 06CH11357; by the National Science Foundation (NSF) underGrant ANT- 0638937; by the NSF Physics Frontiers Center under Grant PHY-1125897; by The Kavli Foundation; by
the Gordon and Betty Moore Foundation; and by the NSF under Grants AST- 0956135 and AST-1402161. Use of theCenter for Nanoscale Materials, an Oﬃce of Science user facility, was supported by the U. S. Department of Energy,Oﬃce of Science, Oﬃce of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357.
category : Fabrication & Implementation Techniques

265

Investigating the E↵ect of Fabrication Processes and Material
Properties to the Large Transition Edge Sensor Array
Performance for the South Pole Telescope 3G Experiment
J. Dinga , P. A. R. Adeb , A. J. Andersonc,d , J. Avvae , Z. Ahmedf,g,h , K. Arnoldi ,J. E. Austermannj , A. N. Benderl,d , B. A. Bensonc,d,k , L. E. Bleeml, d , K. Byruml ,J. E. Carlstromd,m,n,l,k , F. W. Carterl,d , C. L. Changl,d,k , H. M. Choh , J. F. Clicheo ,T. M. Crawfordd,k , A. Cukiermane , D. Czaplewskip , R. Divanp , T. de Haane , M. A. Dobbso,q ,D. Dutcherd,n , W. Everettr , A. Gilberto , R. Gannona , R. Guysers , N. W. Halversonr,t ,N. L. Harringtone , K. Hattoriu , J. W. Henningd , G. C. Hiltonj , W. L. Holzapfele , J. Hubmayrj ,N. Huange , K. D. Irwinf,g,h , O. Jeonge , T. Khairea , D. Kubikc , C. L. Kuof,g,h , A. T. Leee,w ,E. M. Leitchd,k , S. S. Meyerd,m,n,k , C. S. Millerp , J. Montgomeryo , A. Nadolskis , T. Natolicc ,H. Nguyenc , V. Novosada , S. Padind , Z. Pand,n , J. Pearsona , C. M. Posadaa , A. Rahlinc,C. L. Reichardty , J. E. Ruhlz , B. R. Saliwanchikz , J. T. Sayrer , J. A. Shari↵z , I. Shirleye ,E. Shiroko↵d,k , G. Smecheraa , J. Sobrind,n , L. Stanp , A. A. Starkbb , K. Storyf,g , A. Suzukie ,Q Y. Tangd,k , R. B. Thakurd , K. L. Thompsonf,g,h , C. Tuckerb , K. Vanderlindecc,x ,J. D. Vieiras,dd , G. Wangl , N. Whitehorne , W. L. K. Wue , V. Yefremenkol , K. W. Yoonf,g,ha Argonne National Laboratory, Material Science Division, 9700 S. Cass Avenue, Argonne, IL, USA 60439
b School of Physics and Astronomy, Cardi↵ University, Cardi↵ CF24 3YB, United Kingdom
c Fermi National Accelerator Laboratory, MS209, P.O. Box 500, Batavia, IL 60510-0500
d Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
e Department of Physics, University of California, Berkeley, CA 94720
f Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305
g Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305
h SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025
i Department of Physics, University of Wisconsin, Madison, WI 53706
j NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO, USA 80305
k Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
l Argonne National Laboratory, High-Energy Physics Division, 9700 S. Cass Avenue, Argonne, IL, USA 60439
m Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
n Department of Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
o Department of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, Canadap Argonne National Laboratory, Center for Nanoscale Materials, 9700 S. Cass Avenue, Argonne, IL, USA 60439

q Canadian Institute for Advanced Research, CIFAR Program in Cosmology and Gravity, Toronto, ON, M5G 1Z8, Canadar CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
s Astronomy Department, University of Illinois, 1002 W. Green Street, Urbana, IL 61801 USAt Department of Physics, University of Colorado, Boulder, CO 80309
u High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japanv Department of Physics, University of California, One Shields Avenue, Davis, CA 95616
w Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720
x Department of Astronomy & Astrophysics, University of Toronto, 50 St George St, Toronto, ON, M5S 3H4, Canaday School of Physics, University of Melbourne, Parkville, 3010 VIC, Australia
z Physics Department, Case Western Reserve University, Cleveland, OH 44106
aa Three-Speed Logic, Inc., Vancouver, B.C., V6A 2J8, Canada
bb Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138
cc Dunlap Institute for Astronomy & Astrophysics, University of Toronto, 50 St George St, Toronto, ON, M5S 3H4, Canada
dd Department of Physics,University of Illinois, 1110 W. Green Street, Urbana, IL 61801 USA266

PC-14 Fabrication of Flexible Superconducting Wiring with High Current Carrying
Capacity Indium Interconnects
Natalie S DeNigris1 , James A Chervenak2 , Meng-Ping Chang3 , Jong Yoon Ha4 , Nicholas P Costen5 , Simon R
Bandler6 , Megan E Eckart7 , Caroline A Kilbourne8 , Stephen J Smith91

Detector Systems Branch, NASA Goddard Space Flight Center, 2 Detector Systems Branch, NASA Goddard Space Flight
Center , 3 SGT, NASA Goddard Space Flight Center , 4 SB MIcrosystems, NASA Goddard Space Flight Center , 5 SGT, NASA
Goddard Space Flight Center , 6 X-ray Astrophysics Branch, NASA Goddard Space Flight Center , 7 X-ray Astrophysics
Branch, NASA Goddard Space Flight Center , 8 X-ray Astrophysics Branch, NASA Goddard Space Flight Center , 9 NASA
Goddard Space Flight Center / University of Maryland, Baltimore County

The X-ray Integral Field Unit (X-IFU) is a cryogenic spectrometer for the Advanced Telescope for High Energy
Astrophysics (ATHENA). ATHENA is a planned next generation space-based X-ray observatory with capabilities
that surpass the spectral resolution of prior missions. Proposed device designs contain up to 3840 transition edge
sensors (TES), each acting as an individual pixel on the detector, presenting a unique challenge for wiring 8000
superconducting leads to the remaining parts of the instrument. In prototypes, the edges of the focal plane on
the instrument hosted aluminum wire bonding pads; however, indium bumps deposited on molybdenum nitride(MoN) can instead be used as an array of superconducting interconnects. We investigated bumped MoN:In structureswith diﬀerent process cleans and layer thicknesses. Measurements of the resistive transitions showed variation oftransition temperature TC as a function of bias and generally diﬀered from the expected bulk TC of In (3.4 K).
Observed resistance of the In bump structures at temperatures below the MoN transition also depended on the varied
parameters. For our proposed X-IFU geometry (10 microns of In mated to a 1 micron In pad), we measured a TC of
3.1 K at a bias current of 3 mA and a normal resistance of 0.55 m Ω per interconnect. Along with characterizing In
interconnects, the design and fabrication of flexible superconducting niobium (Nb) microstrip atop flexible polyimide
was also investigated. We present a process for combining In bumps with Nb on polyimide to enable high density
wiring for the ATHENA X-IFU focal plane.
category : Fabrication & Implementation Techniques267

PC-15 Growth and Post Treatment of AlMn Film for X-ray Microcalorimeter Basedon Transition Edge Sensor
Wentao Wu1 , Yue Lv2 , Bo Gao3 , Zhen Wang4
1

Shanghai Institute of Microsystem and Information Technology, 2 CAS Center for ExcelleNce in Superconducting Electronics(CENSE) / State Key Laboratory of Functional Materials for Informatics,Shanghai Institute of Microsystem and Information
Technology,Chinese Academy of Sciences / University of Chinese Academy of S, 3 CAS Center for ExcelleNce inSuperconducting Electronics (CENSE) / State Key Laboratory of Functional Materials for Informatics,Shanghai Institute ofMicrosystem and Information Technology,Chinese Academy of Sciences , 4 CAS Center for ExcelleNce in Superconducting
Electronics (CENSE) / State Key Laboratory of Functional Materials for Informatics,Shanghai Institute of Microsystem andInformation Technology,Chinese Academy of Sciences

Magnetically doped superconducting films are promising materials for transition edge sensors because it reduces
the complexity in the design and fabrication of the sensors. We report our recent progress in the DC magnetron
sputtering growth of AlMn superconducting films. We investigated the influence of various film-growth and posttreatment conditions on the superconducting properties of the AlMn films. We found that the power of DC magnetron
sputtering and the temperature of heat treatment are crucial parameters for obtaining high quality films.
category : Fabrication & Implementation Techniques268

PC-16 Tuning SPT-3G transition-edge-sensor electrical properties with a trilayer
Au-Ti-Au thin-film stack
Faustin W Carter1 , SPT3G SPT3G2
1

Argonne National Laboratory, 2 SPT3G Collaboration

The allowed electrical properties of the transition-edge-sensors in the South Pole Telescope’s third generation receiver(a CMB polarimeter, installed at the South Pole this January of 2017) are constrained by several diﬀerent physicalconsiderations. These considerations include various sources of noise, detector stability, impedance matching to electronics, detector saturation power, cryostat base temperature, and fabrication repeatability. Here we discuss tuning thetransition temperature and normal resistance of our gold-titanium-gold tri-layer sensors to satisfy the aforementioned
criteria by varying the relative thicknesses of the tri-layer stack.
category : Fabrication & Implementation Techniques269

PC-17 Fabrication of Absorbers with Dry Film Photoresist for Gamma Ray
Spectroscopy with Metallic Magnetic Calorimeters
Ruslan Hummatov1 , John Ad Hall2 , Geon Bo Kim3 , Stephan Friedrich4 , Robin C Cantor5 , Stephen T. P. Boyd6
1

Department of Physics and Astronomy, University of New Mexico, 2 STAR Cryoelectronics , 3 Lawrence Livermore National
Laboratory , 4 Lawrence Livermore National Laboratory , 5 STAR Cryoelectronics , 6 Department of Physics and Astronomy,
University of New Mexico

We are developing metallic magnetic calorimeters (MMCs) for high resolution gamma-ray spectroscopy for nondestructive assay of nuclear materials. Absorbers for these higher-energy photons can require substantial thickness?100 um to achieve adequate stopping power. We have previously reported successful electroforming of gold absorbers
for these devices using a sacrificial Cu layer as the mask for the posts and Az125nXT photoresist to pattern the tops.
In this report, we describe a new absorber fabrication process using dry film photoresist for both posts and tops. As
with the copper process, the dry-film process is completely compatible with the STARCryo Delta 1000 SQUID
microfabrication process, enabling future commercial deployment of our integrated SQUID/sensor detector designs.
The dry film approach produces well-defined absorbers with fewer and much-simpler process steps and improved yield(100% to date). Absorber adhesion is excellent, with 100% survival to date against vigorous ultrasound and repeated
rapid immersion in liquid nitrogen. Using this approach we have completed fabrication of 14-pixel arrays of integrated
SQUID/sensor MMCs with attached absorbers. At present the absorber thickness is limited to ¡ 50 um with the dryfilm approach. Process development is ongoing to increase the maximum thickness by layering the film. In this report
we describe the post- Delta 1000 fabrication steps used to complete the new MMC devices and initial performance
results.
category : Fabrication & Implementation Techniques270

PC-18 Fabrication of ultrasensitive transition edge sensor bolometric detectors for
HIRMESAri D Brown1 , Regis Brekosky2 , Vilem Mikula3 , Timothy M Miller4 , Joseph Oxborrow5
1

Detector Systems Branch, NASA Goddard Space Flight Center, 2 NASA GSFC / SGT Inc , 3 NASA GSFC / Catholic
University of America , 4 NASA GSFC , 5 NASA GSFC / SB Microsystems

The high resolution mid-infrared spectrometer (HIRMES) is a high resolving power (R 100,000) instrument operatingin the 25-122 micron spectral range and will fly on board the Stratospheric Observatory for Far-Infrared Astronomy(SOFIA) in 2019. Central to HIRMES are its two transition edge sensor (TES) bolometric cameras, an 8x16 detector
high resolution array and a 64x16 detector low resolution array. Both types of detectors consist of Mo/Au TES
fabricated on leg-isolated Si membranes. Whereas the high resolution detectors, with NEP 2 aW/rt(Hz), are fabricatedon 0.45 micron Si substrates, the low resolution detectors, with NEP 10 aW/rt(Hz), are fabricated on 1.45 micron
Si. Here we discuss the similarities and diﬀerences in the fabrication methodologies used to realize the two types ofdetectors.
category : Fabrication & Implementation Techniques271

PC-19 Absorber Materials for the transition edge sensor bolometric detectors on
HIRMESAri D Brown1 , Edward J Wollack2 , Kevin H Miller3 , Joseph Oxborrow4 , Vilem Mikula5
1

Detector Systems Branch, NASA Goddard Space Flight Center, 2 NASA GSFC , 3 NASA GSFC , 4 NASA GSFC / SB
Microsystems , 5 NASA GSFC / Catholic University of America

The high resolution mid-infrared spectrometer (HIRMES) is a high resolving power (R 100,000) instrument operatingin the 25-122 micron spectral range and has two absorber-coupled transition edge sensor (TES) bolometric detector
cameras. The detector pixels on one camera, the high resolution detector array, will be optically coupled to a quarterwave backshort. Consequently, in order to achieve high optical eﬃciency, the absorber-coupled detector pixels need
to be flat to within lambda/10. We have developed novel NbTiN low stress coatings and have demonstrated thatthe 1.4 mm x 1.7 mm optically active region on the 450 nm thick Si high resolution detector pixels is flat to within
5 microns, and these coatings have the required optical impedance across HIRMES operating band. Furthermore,these coatings have a superconducting transition temperature 10 K, which allows them to simultaneously act as highpass filters. This attribute makes these coatings especially attractive for ultrasensitive absorber-coupled bolometricdetector applications, because it decreases optical loading from out-of-band radiation.
category : Fabrication & Implementation Techniques272

PC-20 Flexible Cryogenic Microwave Wiring for the MKID Exoplanet Camera
Alex B Walter1 , Clint Bockstiegel2 , Miguel Daal3 , Seth R Meeker4 , Benjamin A Mazin5
1

Department of Physics & Astronomy, University of California Santa Barbara, 2 Department of Physics & Astronomy,
University of California, Santa Barbara CA 93106, USA , 3 Department of Physics & Astronomy, University of California,
Santa Barbara CA 93106, USA , 4 Department of Physics & Astronomy, University of California, Santa Barbara CA 93106,
USA , 5 Department of Physics & Astronomy, University of California, Santa Barbara CA 93106, USA

We present the microwave and thermal properties of custom made flexible cryogenic microwave cabling for the MKID
Exoplanet Camera (MEC) on the Subaru Telescope. MEC cools a 20,000 pixel MKID array to 100 mK and requires
10 microwave feedlines (20 connections) with signals from 4–8 GHz. Between 300 K and 4 K we use the Rogers Corp.
LCP dielectric film Ultralam with 1/4 oz Cu cladding to make a 10 trace stripline flexible cable. The ends have G3PO
push-on coax connectors. The input side has an integrated 30 dB Pi attenuator at the 4 K end. Between 4 K and 100
mK we use superconducting 53% Nb - 47% Ti alloy laminated onto DuPont’s Kapton/epoxy dielectric film Nikaflex
to make a 10 trace microstrip flexible cable. The ends are glued with silver epoxy to a copper transition board with
G3PO connectors. Our newest design uses 10 micron thick Nb-47Ti and a 76 micron dielectric stackup. The thermalload on the 100 mK stage, assuming thermalization at an intermediate 800 mK stage such as in a two stage ADR, isabout 0.7 uW-cm and is dominated by the dielectric.
category : Fabrication & Implementation Techniques273

PC-21 TiNx KIDs for the second phase of CALDER
Ivan Colantoni1 , Laura Cardani2 , Nicola Casali3 , Angelo Cruciani4 , Fabio Bellini5 , Maria Gabriella Castellano6 ,Carlo Cosmelli7 , Antonio d’Addabbo8 , Sergio di Domizio9 , Maria Martinez10 , Claudia Tomei11 , Marco Vignati121

Institute for Photonics and Nanotechnologies, National Research Council (CNR - IFN), 2 INFN sezione di Roma, Roma
(Italy) , 3 INFN sezione di Roma, Roma (Italy) , 4 INFN sezione di Roma, Roma (Italy) , 5 INFN sezione di Roma, Roma
(Italy) / Dipartimento di Fisica Sapienza Universita di Roma, Roma (Italy) , 6 CNR Istituto di Fotonica e Nanotecnologie(CNR-IFN), Roma (Italy) , 7 INFN sezione di Roma, Roma (Italy) / Dipartimento di Fisica Sapienza Universita di Roma,
Roma (Italy) , 8 LNGS INFN, Assergi (Italy) , 9 Dipartimento di Fisica Universita di Genova, Genova (Italy) / INFN sezione di
Genova, Genova (Italy) , 10 INFN sezione di Roma, Roma (Italy) / Dipartimento di Fisica Sapienza Universita di Roma, Roma
(Italy) , 11 INFN sezione di Roma, Roma (Italy) , 12 INFN sezione di Roma, Roma (Italy)

The goal of the CALDER (Cryogenic wide-Area Light Detectors with Excellent Resolution) project is the developmentof light detectors with large active area and noise energy resolution smaller than 20 eV RMS using phonon-mediatedKinetic Inductance Detectors (KIDs).
Background suppression plays a key role for experiments searching for rare events, like neutrinoless double beta
decay and dark matter interactions. Next generation experiments based on the technology of cryogenic calorimeters
can improve the background rejection exploiting the diﬀerent light emission of diﬀerent particles. CALDER is focussed
on the development of sensitive light detectors that can be easily scaled up to?1000 devices without increasing theheat load for the cryogenic apparatus.
The ?rst phase of the project allow us to reach a baseline resolution of 80 eV using 60 nm Al device. To increase theenergy resolution of our detectors we are considering to use sub-stoichiometric TiN (TiNx) as an alternative material
and we are optimizing its deposition by means of DC-magnetron reactive sputtering. We used a 4-point scheme tomeasure the critical temperature from the IV curves, putting the sample in an Oxford HELIOX cryostat. First results
show that the critical temperature changes consistently with the nitrogen content, as determined by changing thecomposition of the sputtering gas. Furthermore a first KID prototype was designed, entirely made of TiNx, paying
attention to impedance match of the feedline to the external electrical connection.
category : Fabrication & Implementation Techniques274

PC-22 Fabrication of a uniform large scale array of X-ray microcalorimeters for the
X-IFU instrument on AthenaMarcel Ridder1 , Kenichiro Nagayoshi2 , Marcel Bruijn3 , Pourya Khosropanah4 , Luciano Gottardi5 , Jiang Rong Gao6
1

SRON Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research , 3 SRON Netherlands
Institute for Space Research , 4 SRON Netherlands Institute for Space Research , 5 SRON Netherlands Institute for Space
Research , 6 SRON Netherlands Institute for Space Research

Future spaced-based imaging X-ray spectrometers, such as the X-IFU (X-ray Integral Field Unit) instrument on ESA
s Athena mission, will be based on large format arrays consisting of more than 3800 Transition Edge Sensor (TES)
microcalorimeters. We present an optimized lithographic fabrication route that enables the realization of such large
format arrays of microcalorimeters. We improved on process steps concerning the X-ray absorber, the stripline wiring
system and the silicon grid support structure.
We have developed an electroplating process for the fabrication of free standing cantilevered X-ray, which leads toa uniform absorber film thicknesses over the large array. The thickness uniformity obtained across the array is better
than 5% for Au/Bi absorbers with thicknesses of 2/7 μ m.
We developed and fabricated high density Nb/SiO2/Nb striplines to wire a 4000 pixel array with yield of morethan 98%. We designed a fan-out scheme for the stripline wiring system that allows the study on the integrity of thewiring in the array area of the large format array.
We report on the optimization of the deep reactive ion etching step to form the silicon grid structure, which allows
the production of uniform silicon grids accommodating an array of 4000 TES pixels.
Acknowledgement: ESA CTP contract ITT AO/1-7947/14/NL/BW
category : Fabrication & Implementation Techniques

275

276

PC-23 Fabrication of the arrays of detectors deployed with the SPT-3G receiver
Chrystian M Posada1 , SPT-3G Collaboration2
1

Materials Science Division, Argonne National Laboratory, 2 SPT-3G Collaboration

The South Pole Telescope third-generation (SPT-3G) receiver was installed during the austral summer of 2016-7. It
is designed to measure the Cosmic Microwave Background (CMB) across three frequency bands centered at 95 GHz,
150 GHz and 220 GHz. The SPT-3G receiver is composed of ten modules of 271 pixels each. Each pixel featuresa broad-band sinuous antenna coupled to a niobium microstrip transmission line. In-line filters define the desired
band-passes before the millimeter-wavelength signal captured by the antenna is coupled to the six individual Ti/Au
based transition edge sensors (TESs) located within each of the pixels in the arrays. In total, the SPT-3G receiver iscomposed of 16000 detectors, which are readout using a 64x frequency domain multiplexing (fMux) scheme. Here, we
present the process employed in the fabrication of the arrays of detectors currently installed in the SPT-3G receiver.
In addition, we discuss changes being implemented for the fabrication of a second set of detectors with improved yieldand fine-tuned performance. These new set of detectors will be installed at the end of 2017 for the second observationseason of the SPT-3G receiver.
category : Fabrication & Implementation Techniques277

PC-24 Impact of electrical contacts design and materials on the stability of titanium
film superconducting transition shape
Volodymyr G Yefremenko1 , SPT-3G collaboration2
1

Argonne National Laboratory, High Energy Physics Division, 2 SPT-3G collaboration

The South Pole Telescope’s SPT-3G camera,currently deployed, utilizes (Ti/Au)- based Transition Edge Sensors(TES). One of the key requirements for these sensors was reproducibility and long-term stability of the superconducting transitions. Here we will discuss the impact of electrical contacts design and materials on the superconducting
transition shape of Ti-based TESs. Using SEM, AFM and DIC optical microscopy we observed the presence of unexpected defects of morphological nature on the titanium surface and their evolution in time in proximity to Nb contacts.
Furthermore, we found direct correlation between the variations of the morphology and the superconducting transition characteristics. Model experiments with diﬀerent diﬀusion barriers between TES and Nb leads were performed toclarify the origin of this problem. We have demonstrated that the reproducibility of superconducting transition canbe significantly improved by preventing diﬀusion processes in the TES-leads contact areas.
Acknowledgments : This work was supported in part by the Oﬃce of Science and the Oﬃce of Basic Energy
Sciences of the US Department of Energy under Contract DE-AC02- 06CH11357; by the National Science Foundation(NSF) under Grant ANT- 0638937; by the NSF Physics Frontiers Center under Grant PHY-1125897; by The Kavli
Foundation; by the Gordon and Betty Moore Foundation; and by the NSF under Grants AST- 0956135 and AST1402161. Use of the Center for Nanoscale Materials, an Oﬃce of Science user facility, was supported by the U. S.
Department of Energy, Oﬃce of Science, Oﬃce of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357.
category : Fabrication & Implementation Techniques

278

SPT-3G Collaboration
V. Yefremenkoa , P. A. R. Adeb , A. Andersonc,d , J. Avvae , Z. Ahmedf,g,h , K. Arnoldi ,J. E. Austermannj , A. N. Bendera,d , B. A. Bensonc,d,k , L. E. Bleema, d , K. Byruma ,J. E. Carlstromd,l,m,a,k , F. W. Cartera,d , C. L. Changa,d,k , H. M. Choh , J. F. Clichen ,T. M. Crawfordd,k , A. Cukiermane , D. Czaplewskio , J. Dingp , R. Divano , T. de Haane ,M. A. Dobbsn,q , D. Dutcherd,m , W. Everettr , A. Gilbertn , R. Gannonp , R. Guysers ,N. W. Halversonr,t , N. L. Harringtone , K. Hattoriu , J. W. Henningd , G. C. Hiltonj ,G. P. Holdern,q , W. L. Holzapfele , J. Hubmayrj , N. Huange , K. D. Irwinf,g,h , O. Jeonge ,T. Khairep , L. Knoxv , D. Kubikc , C. L. Kuof,g,h , A. T. Leee,w , E. M. Leitchd,k ,S. S. Meyerd,l,m,k , C. S. Millero , J. Montgomeryn , A. Nadolskis , T. Natolicc , H. Nguyenc ,V. Novosadp , S. Padind , Z. Pand,m , J. Pearsonp , C. M. Posadap , A. Rahlinc ,C. L. Reichardty ,J. E. Ruhlz , B. R. Saliwanchikz , I. Shirleye , G. Simardn , G. Smecheraa , J. T. Sayrer ,J. A. Shari↵z , E. Shiroko↵d,k , L. Stano , A. A. Starkbb , J. Sobrind,m , K. Storyf,g , A. Suzukie ,Q Y. Tangd,k , K. L. Thompsonf,g,h , C. Tuckerb , K. Vanderlindecc,x , J. D. Vieiras,dd , G. Wanga ,N. Whitehorne , K. W. Yoonf,g,ha Argonne National Laboratory, High-Energy Physics Division, 9700 S. Cass Avenue, Argonne, IL, USA 60439
b School of Physics and Astronomy, Cardi↵ University, Cardi↵ CF24 3YB, United Kingdom
c Fermi National Accelerator Laboratory, MS209, P.O. Box 500, Batavia, IL 60510-0500
d Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
e Department of Physics, University of California, Berkeley, CA 94720
f Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305
g Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305
h SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025
i Department of Physics, University of Wisconsin, Madison, WI 53706
j NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO, USA 80305
k Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
l Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
m Department of Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
n Department of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, Canadao Argonne National Laboratory, Center for Nanoscale Materials, 9700 S. Cass Avenue, Argonne, IL, USA 60439
p Argonne National Laboratory, Material Science Division, 9700 S. Cass Avenue, Argonne, IL, USA 60439

q Canadian Institute for Advanced Research, CIFAR Program in Cosmology and Gravity, Toronto, ON, M5G 1Z8, Canadar CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
s Astronomy Department, University of Illinois, 1002 W. Green Street, Urbana, IL 61801 USAt Department of Physics, University of Colorado, Boulder, CO 80309
u High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japanv Department of Physics, University of California, One Shields Avenue, Davis, CA 95616
w Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720
x Department of Astronomy & Astrophysics, University of Toronto, 50 St George St, Toronto, ON, M5S 3H4, Canaday School of Physics, University of Melbourne, Parkville, 3010 VIC, Australia
z Physics Department, Case Western Reserve University, Cleveland, OH 44106
aa Three-Speed Logic, Inc., Vancouver, B.C., V6A 2J8, Canada
bb Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138
cc Dunlap Institute for Astronomy & Astrophysics, University of Toronto, 50 St George St, Toronto, ON, M5S 3H4, Canada
dd Department of Physics,University of Illinois, 1110 W. Green Street, Urbana, IL 61801 USA279

PC-25 Microfabrication of transition-edge sensor arrays of microcalorimeters with
Ho-163 for direct neutrino mass measurements with HOLMES
Angiola Orlando1 , Giancarlo Ceruti2 , Marco Faverzani3 , Elena Ferri4 , Andrea Giachero5 , Angelo Nucciotti6 , Andrei
Puiu7 , Dan Schmidt8 , Dan Swetz9 , Joel Ullom10
1

INFN Milano Bicocca, 2 INFN Milano Bicocca , 3 Universita’ di Milano Bicocca , 4 INFN Milano Bicocca , 5 INFN Milano
Bicocca , 6 INFN Milano Bicocca / Universita’ di Milano Bicocca , 7 Universita’ di Milano Bicocca , 8 National Institute ofStandards and Technologies (NIST) , 9 National Institute of Standards and Technologies (NIST) , 10 National Institute ofStandards and Technologies (NIST)

Measuring the neutrino mass is one of the major challenges in today’s particle physics and astrophysics. There areseveral methods to determine the neutrino mass: cosmological observations, neutrinoless double beta decay and beta
or electron capture spectrum end-point study. The latter is currently the only one capable of providing a model
independent measurement of the absolute scale of neutrino mass.
The HOLMES experiment will provide an important step forward in direct neutrino mass measurements with acalorimetric approach as an alternative to spectrometry. In such approach the beta source is embedded in the detector
and the energy emitted in the decay is entirely measured by the detector, except for the fraction taken away by theneutrino. HOLMES plans to deploy a large array of transition-edge sensor (TES) microcalorimeters with implanted
Ho163 nuclei. The detectors will be Mo/Cu TES on a solid Si3N4 membrane and a gold absorber. While good
progress has been made in optimizing single pixel design and fabrication to achieve the target resolution, a major
challenge is the fabrication of arrays of such microcalorimeters with the required amount of Ho163 nuclei embedded in
the gold absorber. Fabrication needs to be compatible with ion implantation, while preserving detectors performance.
Specifically, the gold absorbers will need to be fabricated in more than one step, before and after ion implantation, inorder to fully embed the isotope.
In this contribution we describe the multi-step microfabrication process implemented to produce the final detector
arrays for HOLMES, its challenges and our progress in assessing the feasibility of each step. One crucial part of suchprocess is the ability to perform deposition of gold simultaneous to the Ho163 implantation in the detectors absorber.
We describe the UHV target chamber, with integrated gold deposition system, we have built to achieve this goal andthe first fabrication tests on prototype arrays, prior to integration with the ion implanter.
category : Fabrication & Implementation Techniques280

PC-26 Characterizing Atomic Layer Deposition Titanium Nitride Kinetic Inductance
Detectors
Rong Nie1 , Peter S. Barry2 , Erik Shirokoﬀ3
1

Kavli Institute for Cosmological Physics, University of Chicago, 2 Kavli Institute for Cosmological Physics, University of
Chicago , 3 Kavli Institute for Cosmological Physics, University of Chicago / Department of Astronomy and Astrophysics,
University of Chicago

Kinetic Inductance Detectors (KIDs) oﬀer simple fabrication and low cost multiplexing, and are a compelling candidate
for future astronomical instruments, which require arrays containing thousands of detecting elements. One of themain obstacles that needs to be overcome when scaling to large-format arrays is tight control of uniformity andrepeatability of detector performance across entire wafer. Hence in this work, a novel deposition method - Atomic Layer
Deposition (ALD) is implemented. We outline preliminary results of single-layer lumped-element Titanium Nitride(TiN) resonators coupled to a coplanar waveguide feedline. We demonstrate the eﬀect on the critical temperature
variation with thickness, wafer-scale uniformity, and present detailed modelled fits to frequency and internal quality
factor as a function of temperature. In particular, we demonstrate that films grown by ALD enables us to achievethin films with good repeatability with internal Q factors approaching 106 . We also discuss the measured frequency
noise of these devices and will present preliminary results of the optical responsivity of these films when coupled to a
microstrip fed mm-wavelength antenna.
category : Fabrication & Implementation Techniques

281

Category D : Cryogenics andComponents282

PD-1 Metamaterial Achromatic Half-Wave Plates for Cosmic Microwave Background
Observation
Kevin P Coughlin1 , Jeﬀ McMahon2
1

Physics Department, University of Michigan, 2 University of Michigan

The Advanced ACTPol instrument on the Atacama Cosmology Telescope is one of the latest generation of groundbased Cosmic Microwave Background (CMB) experiments, and incorporates new detector and optical technologies tomake improved measurements of the polarization of the CMB. One of the major issues facing ground based CMB
measurements is noise introduced by the turbulent, unpolarized atmosphere. The constant fluctuations of the air in the
beam of the telescope show up in the data as low frequency noise. To mitigate this eﬀect, ACT will deploy continuously
rotating, ambient-temperature half-wave plates (HWPs) to modulate the incident polarization. The HWPs are madefrom metamaterial silicon. A custom 3-axis dicing saw was used to machine subwavelength features into the silicon.
Breaking 90 degree rotation symmetry in the features induces birefringence in the metamaterial, and allows a HWP
to be made. The HWPs use a 3-stack Pancharatnam geometry with three layers of metamaterial antireflection (AR)coating. Three such HWPs have been made for act; two for the 90/150 GHz band, and one for the 150/220 GHz
band. These HWPs have a number of advantages over the standard sapphire HWPs. With a tunable birefringence,these plates can be made thinner, reducing the thermal loading on the telescope. The metamaterial AR coating isbirefringent, allowing better reflection mitigation than a standard AR coating. This supporting technology will havesignificant implications for the requirements on detectors, superconducting readout, and ability to make large angularscale CMB measruements from the ground. Here, laboratory data from these HWPs will be presented, including thereflection, polarization modulation eﬃciency, and thermal loading. This will be compared with numeric simulations
for the HWPs and preliminary data from field observations.
category : Cryogenics and Components283

PD-2 Development of a cylindrical magnetic refrigerant with polycrystaline GdLiF4
for Adiabatic Demagnetization Refrigerator
Akio Hoshino1 , Shunji Kitamoto2 , Hadi Razavi3 , Yuki Nakajima4 , Masayoshi Fuji5 , Sadakazu Takayama6 , Osamu
Takagi7 , Katsukiyo Furukawa8 , Ryuji Higashinaka9 , Yuji Aoki10 , Tatsuma D. Matsuda11 , Shin’ya Yamada12 ,Yoshitaka Ishisaki13 , Yuichiro Ezoe14 , Takaya Ohashi15
1

Rikkyo University, 2 Department of Physics, Rikkyo University , 3 Advanced Ceramics Research Center, Nagoya Institute ofTechnology , 4 Advanced Ceramics Research Center, Nagoya Institute of Technology , 5 Advanced Ceramics Research Center,
Nagoya Institute of Technology , 6 TYK Corporation , 7 TYK Corporation , 8 TYK Corporation , 9 Department of Physics,
Tokyo Metropolitan University , 10 Department of Physics, Tokyo Metropolitan University , 11 Department of Physics, Tokyo
Metropolitan University , 12 Department of Physics, Tokyo Metropolitan University , 13 Department of Physics, Tokyo
Metropolitan University , 14 Department of Physics, Tokyo Metropolitan University , 15 Department of Physics, Tokyo
Metropolitan University

Adiabatic Demagnetization Refrigerator (ADR) is one of the most promising tool for realizing 0.1 K. The lowest
temperature and holding time are determined by the magnetic characters of refrigerant materials, starting temperatureof demagnetizing, strength of the magnetic field and thermal inflow to the refrigerant. Because recent mechanicalcooler, like pulse-tube cooler, can easily achieve a thermal bath with 2.7- K, designing as a cryogen-free system with
ADRs is a big advantage.
We have designed double refrigerant ADR with a superconducting magnet, chrome potassium alum (CPA) andpolycrystalline GdLiF4 in order to prepare a 0.1 K stage, on which we operate TES x-ray microcalorimeters on 0.1 K
stage. To reduce the thermal inflow from 2.7 K of the thermal bath by pulse-tube cooler to CPA, we are developing
the cylindrical polycrystalline GdLiF4 for utilizing as a thermal buﬀer between CPA and magnet. GdLiF4 has been
investigated as magnetic material by Numazawa. GdLiF4 has larger entropy change at ¿ 2T than that of a typicalmagnetic refrigerant GGG. This cylindrical GdLiF4 cut the radiation to CPA and 5µW of thermal inflow in our coolingsystem. And we estimate that GdLiF4 can keep about 17 hours on 0.5 K.
The GdLiF4 polycrystalline sample was prepared by one axis-pressing powders of GdF3 and LiF with 0.4 g binder
in 50 ± 5 kPa, molded it and calcinating it for 10 hours in 973 K in Ar atmosphere and sinking it to graphite powder
for avoiding reduction reaction by oxygen and evaporation of LiF. In the case that calcinating temperature is 1073 K
for 1.5 hours, LiF is evaporated locally and porous are formed. The optimal calcinating temperature and holding timedepend on the shape and size.
We measured magnetization with MPMS, specific heat capacity with PPMS, crystal structure by XRD, anduniformity by SEM to evaluate our samples. Though we detect existence of GdF3 , Gd4 O3 F6 and Gd2 O3 , magnetic
moment was well consistent with Brillouin function. Our samples were also well consistent to Gd3+ characters between
2-10K. GdF3 , Gd4 O3 F6 were identified by XRD, but other evaluation did not detect them. Small λ-type peak appears
at 3.8 K due to the Gd2 O3 inclusion, of which abundance ratio was partially several percent on entropy comparedwith GdLiF4 . We think these contaminants exist locally on samples.
We are preparing for fabricating cylindrical structure of 10 cm length, 43mmϕ and 3mm thickness with gel casting
method. In the gel casting method, we press slurry with high-pressure water and mold it. It is useful for this method
to fabricate large and unique shapes. We report the status of the development.
category : Cryogenics and Components284

PD-3 Development of a half-wave plate based polarization modulator unit for
LiteBIRD
Tomotake Matsumura1 , LiteBIRD collaboration
1

Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU) The University of Tokyo,

We report our development of a half-wave plate (HWP) based polarization modulator unit (PMU) for a cosmic
microwave background (CMB) polarization experiment. Inflationary signal appears at a large angular scale on the sky
and this large spatially fluctuating signal tends to appear as a long-time scale fluctuating signal in time domain afterscanning by a telescope. This requires for the end-to-end low temperature instruments including detector system toachieve typical stability in time below 0.1 Hz or less.
An increasing interest toward the physics of early universe drives rapid progress in low temperature detector andits surrounding technologies. A HWP based PMU modulates the incident polarized signal in a telescope. This enables
to up-convert an incident polarization signal frequency above typical detector 1/f knee, and thus we achieve a required
stability at the signal band eﬀectively. In addition to achieve the stability, a single polarization sensitive detector canoperate as an independent polarimeter. There is no need for diﬀerencing between the orthogonally polarized detectors,
and correspondingly it does not require a high precision matching of the detector properties, e.g. beam, gain andbandpass, in the detector pair.
LiteBIRD is a candidate of JAXA strategic large satellite projects and currently in Phase-A1 within the JAXA/ISAS
program. The baseline mission design of LiteBIRD is to employ a kilo-pixel transition edge sensor (TES) bolometer array with a HWP based PMU. A current development goal is to demonstrate the feasibility, i.e. experimental
demonstration of a continuously rotating 450 mm diameter HWP operating at about 1 Hz below 10 K.
In this presentation, we report our design of PMU for LiteBRD and the experiment demonstration of our prototype.
We develop a Pancharatnam half-wave plate using a sapphire crystal that covers from 40 to 235 GHz bands. We employ
a superconducting magnetic bearing to support the continuous rotation of the HWP at below 10 K to minimize the heatdissipation. We discuss the requirement of the PMU and impact using HWP which can relax some of the requirements
to TES specifications. We also address the potential systematics and its mitigation that is introduced with use of
PMU.

T. Matsumura,1 Y. Sakurai,1 H. Imada,2 K. Arnold,3 T. Dotani,2 N. Halverson,4 T. Hasebe,5 M. Hazumi,6C. A. Hill,7 M. Bucher,10 J. Borrill,7, 8 T. Iida,11, 1 H. Ishino,12 H. Kanai,13 S. Kashima,5 N. Katayama,1
H. Kataza,2 R. Keskitalo,8 T. Kisner,8 Y. Kobayashi,9 K. Komatsu,12 K. Konishi,15 A. Kusaka,7, 8, 14 M.
Kuwata-Gonokami,14 A. T. Lee,7, 8 M. Maki,6 Y. Minami,6 K. Mitsuda,2 S. Nakamura,13 R. Nagata,6 H.
Ohsaki,16 G. Patanchon,10 H. Sakurai,14 Y. Sekimoto,5 T. Shimomura,16 J. Suzuki,6 A. Suzuki,7, 8 H. Sugai,1
R. Takaku,13 Y. Terao,16 H. Tomida,2 S. Uozumi,12 S. Utsunomiya,1 R. Yamamoto,2 and J. Yumoto15, 14
1

Kavli Institute for The Physics and Mathematics of The Universe (WPI),The University of Tokyo, Kashiwa, Chiba, Japan
2
Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa, Japan3
Department of Physics, University of California, San Diego, CA, USA
4
Department of Physics, University of Colorado, Boulder, CO, USA
5
National Astronomical Observatory of Japan (NAOJ), Mitaka, Tokyo, Japan
6
High Energy Accelerator Research Organization (KEK), Ibaraki, Japan
7
Department of Physics, University of California, Berkeley, CA, USA
8
Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
9
The Institute for Solid State Physics, The University of Tokyo, Kashiwa, Chiba, Japan
10
AstroParticule et Cosmologie, Universit Paris Diderot, CNRS/IN2P3,
CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cit, Paris, France
11
PTI, Inc.,Yokohama, Kanagawa, Japan
12
Okayama University, Okayama, Okayama, Japan
13
Yokohama National University, Yokohama, Kanagawa, Japan
14
Department of Physics, The University of Tokyo, Tokyo, Japan
15
Institute for Photon Science and Technology, The University of Tokyo, Tokyo, Japan
16
Graduate School of Frontier Sciences, The University of Tokyo, Kashiwa, Chiba, Japan

category : Cryogenics and Components
285

286

PD-4 The CUORE cryostat
Antonio D’Addabbo1
1

Laboratori Nazionali del Gran Sasso - INFNThe Cryogenic Underground Observatory for Rare Events (CUORE) is an experiment searching for neutrinolessdouble beta decay in 130 Te. CUORE must operate an ton-scale array of 988 TeO2 bolometers at ∼10 mK providing
exceptionally low background and low vibration conditions. In order to meet this unprecedented challenge, theCUORE detector array is cooled down by a multistage cryogen-free cryostat unique of its kind. Due to the large
mass, a custom made precooling system brings the whole cryostat to a temperature of 35 K using LHe vapours. Laterthe Inner Vacuum Chamber (IVC) is cooled down to 4K by five Pulse Tubes (PTs). Finally the base temperature isdelivered by a custom designed continuous-cycle 3 He/4 He dilution refrigerator. Strict material selection and cleaning
procedures are applied to all the structures facing the detector. Seven tonnes of low-temperature lead shielding protect
the inner cubic meter scale experimental volume from the residual background contamination of the cryostat. Special
suspensions mechanically decouple the detector from the cryostat. Vibration-induced thermal noise on the bolometers
is minimized by means of a dedicated software that optimizes and control the working frequencies and phases of thefive PTs. The cooling power, the total mass and the experimental volume make the CUORE cryostat the biggest andmost powerful dilution cryostat in the world.
CUORE is currently in its final detector commissioning phase at the Laboratori Nazionali del Gran Sasso. The
CUORE cryostat successfully cooled down the ton-scale detector at ∼7 mK, delivering an uniform and constant basetemperature. This result marks a fundamental milestone in low temperature detectors techniques, opening the pathfor future ton-scale bolometric experiments searching for rare events.
category : Cryogenics and Components

287

PD-5 Stacked Wafer Gradient Index Silicon Optics with Integral Antireflection Layers
Fabien Defrance1 , Goutam Chattopadhyay2 , Jake Connors3 , Sunil Golwala4 , Matt I. Hollister5 , Cecile
Jung-Kubiak6 , Simon Radford7 , Jack Sayers8 , Edward C. Tong9 , Hiroshige Yoshida10
1

Division of Physics, Mathematics, and Astronomy, California Institute of Technology, 2 Jet Propulsion Laboratory ,Harvard-Smithsonian Center for Astrophysics , 4 Division of Physics, Mathematics, and Astronomy, California Institute ofTechnology , 5 Division of Physics, Mathematics, and Astronomy, California Institute of Technology / Fermi National
Accelerator Laboratory , 6 Jet Propulsion Laboratory , 7 Harvard-Smithsonian Center for Astrophysics , 8 Division of Physics,
Mathematics, and Astronomy, California Institute of Technology , 9 Harvard-Smithsonian Center for Astrophysics , 10 Divisionof Physics, Mathematics, and Astronomy, California Institute of Technology
3

A wide range of applications in astronomy from tens of GHz to THz frequencies, on the ground and in space, would
benefit from silicon optics because silicon’s high refractive index and low loss make it an ideal optical material atthese frequencies. It is even possible to use silicon for ambient temperature vacuum windows. Silicon’s large refractive
index, however, necessitates antireflection coating. Moreover, multilayer antireflection treatments are necessary forwide spectral bandwidths, with wider bandwidths requiring more layers. To this end, we are developing multilayer
coatings for silicon by bonding together wafers individually patterned with deep reactive ion etching (DRIE).
While a standard approach to antireflection coating is to deposit or laminate dielectric layers of appropriate
refractive index, it is diﬃcult (but not impossible) to find low loss dielectrics with the correct refractive index andother properties to match silicon well, especially if more than one layer is required, operation up to THz frequencies
is desired, and/or the optic will be used cryogenically. Textured surfaces are an attractive alternative to dielectric
antireflection coatings. For millimeter wavelengths, multi-layer antireflection textures with up to 4:1 bandwidths havebeen cut successfully into silicon lens surfaces with a dicing saw, but this technique becomes unusable at frequenciesof 300 GHz and higher given the saw dimensions. Laser machining is being explored but demonstrations are not yet
available. DRIE works well on flat surfaces (and has been demonstrated for narrowband windows to THz frequencies),
but there are limits to the depth and aspect ratio of the features it can create. Furthermore etching has not been
adapted to large, curved optics.
We are pursuing a hybrid approach to this problem: construct a silicon optic by stacking flat patterned wafers.
The starting point is a multilayer optical design incorporating both an axial gradient in the refractive index for
antireflection and a radial index gradient for focusing. For each optical layer, a hole or post pattern is used to achieve
the required eﬀective index of refraction. Using a novel multilayer etching procedure, several layers of the opticalstructure are fabricated on a flat wafer. Several individually patterned wafers are stacked and bonded together toproduce the completed optic. This approach can thus address the aspect ratio limitations of DRIE, and it obviates
etching on curved surfaces.
We present our results to date, which include measurements at 210-330 GHz (and 75-115 GHz) of single-layerand double-layer coatings before and after wafer-bonding. These measurements indicate the basic technique is sound.
We will also report on explorations of the maximum etchable hole aspect ratio, which will define the minimum andmaximum refractive index that can be used for gradient index lens and antireflection designs. We are also beginningto design 4- and 6-layer structures. Our near-term goal is to produce a 10-cm lens with a 6-layer coating providing
5.5:1 bandwidth from 85 to 420 GHz, eventually scaling up to 15-cm, 30-cm, and larger elements.
category : Cryogenics and Components

288

PD-6 Superconducting Flex Cables for CMB Detector Readouts
Robin Cantor1 , John A Hall2
1

STAR Cryoelectronics, 2 STAR Cryoelectronics LLC

Next-generation instruments for astrophysical surveys will have large focal plane arrays of detectors with 100,000 or
more superconducting pixels and thousands or tens of thousands of low-noise cryogenic amplifiers. High-frequency,
high-density superconducting flex cables are needed to read out these arrays using frequency domain multiplexing.
We describe a process we have developed for the fabrication of robust superconducting flex cables to meet theserequirements and to simplify cryogenic system integration. The flex circuits are fabricated using superconducting
NbTi traces (Tc 9 K) sandwiched between a 6-μ m thick polyimide base layer and a 6-μ m thick top layer on a
100-mm diameter Si wafer. The NbTi superconducting traces are sputter deposited onto the base polyimide andpatterned using a lift-oﬀ process, and transition to wire bond pads patterned directly on the Si wafer to improve wirebond reliability. After applying the top polyimide layer, the Si under the traces is removed using a deep reactive ion
etch process, leaving just the thin polyimide/superconductor/polyimide flex with a total thickness of 12.4 μ m. We
discuss preliminary test and characterization measurements carried out at 4 K and future development plans.
This work supported by the U. S. Department of Energy under Contract No. DE-SC0015805.
category : Cryogenics and Components289

PD-7 Improved Automated Control System for ADR Cryostats
Robin Cantor1
1

STAR Cryoelectronics

We have developed an improved control system for ADR cryostats. The LabVIEW-based ACS3 ADR Control Software enables fully automated ADR cryostat operation in conjunction with a STAR Cryoelectronics MC-20 Magnet
Controller and PA-10 Power Amplifier, and a Lake Shore 372 Resistance Bridge and 218 Temperature Monitor. The
application allows the user to monitor up to ten thermometers, and automatically or manually regenerate the ADR,
automatically or manually operate the ADR heat switch, regulate the ADR temperature (using local or remote control), and log all ADR temperatures and cryostat data for further processing or diagnostic purposes. Dual configurable
graphical displays can be used to plot versus time any of the ten thermometer values, the superconducting magnet
parameters (e.g., voltage, current), cryostat pressure, or compressor parameters. The application monitors key systemtemperatures and magnet parameters in real time. If temperature or magnet thresholds are exceeded due to a loss ofcooling or a magnet quench, or there is a power outage, the system is automatically shut down to reduce the risk ofdamage to the ADR or cryostat. We report recent results for temperature control stability and temperature regulation
range.
This work supported in part by the U. S. Department of Energy under Contract No. DE-SC0006214.
category : Cryogenics and Components

290PD-8 Compact 0.8 K Helium-4 Sorption Cooler
Hiroshi Matsuo1 , Hajime Ezawa2 , Yuta Kawamura3 , Daiki Kubo4 , Norio Okada5 , Reiho Shimomukai6
1

National Astronomical Observatory of Japan, 2 National Astronomical Observatory of Japan , 3 The Graduate University for
Advanced Studies (SOKENDAI) , 4 Department of Physics, Toho University , 5 National Astronomical Observatory of Japan ,6
Department of Physics, Toho University

Cryocooler is one of the crucial component for cryogenic detectors, where the cooling power limits the detector
performance, such as pixel numbers or operation speed. Our goal is to realize photon counting terahertz interferometry(PCTI; Matsuo 2012, JLTP 167, 840) by implementing fast terahertz detectors, which count incoming photons of
100 Mphoton/s. Readout electronics as fast as 1 GHz is required, which causes relatively high heat dissipation of
100 µW. Furthermore, we aim to realize a multi-pixel array of these detectors, which requires higher cooling power.
Niobium based devices are preferred for terahertz detectors, such as superconducting tunnel junctions, since theirenergy gap stays within the terahertz frequency range. By cooling niobium device to less than 0.8 K, the quasiparticle
density reduces and the device behaves as an ideal superconductor. We are developing a compact 0.8 K 4 He sorption
cooler which can operate continuously with base temperature of 4 K. 4 He sorption cooler provides relatively highcooling capacity and simple operation as demonstrated by Lau et al. 2006 (Cryogenics 46, 809), where the orifice size
is one of the key parameter to achieve appropriate cooling temperature and power. Our new design aims to realize
the required cooling power with minimum physical size. Altering two sorption coolers will make continuous operation
possible when the 0.8 K hold time is designed to be longer than the fridge-cycle time.
Prototype sorption cooler using 4 ℓ (STP) of 4 He was fabricated in order to evaluate the optimum amount ofactivated charcoal, which dominates the physical size of the cooler. The relation between cool down temperature andheat load was evaluated with an orifice of 1 mm in diameter. With no heat load, the hold time was about 5 hours,
whereas the fridge-cycle time was about 30 minutes. Even with 400 µW heat load, the hold time was more than 2hours, which is still much longer than the fridge-cycle time. Then we designed another sorption cooler with 2 ℓ (STP)of 4 He, and the fridge-cycle time becomes even shorter. Altering operation of two coolers can provide continuous 0.8 K
cooling under heat load of 400 µW. Experimental results of the compact sorption coolers, and the ultimate design ofthe compact sorption cooler will be discussed in the presentation.
category : Cryogenics and Components

291

PD-9 Improvements of our TES microcalorimeter operation system with a compact
adiabatic demagnetization refrigerator cryostat
Keigo Tanaka1 , Ryuichi Fujimoto2 , Kenta Nakayama3 , Yuya Kinoshita4 , Yu Kai5 , Tomohiro Nakano6 , Ayumi Tsuji71

Department of Mathematics and Physics, Kanazawa University, 2 Faculty of Mathematics and Physics, Kanazawa University,
Kakuma-machi, Kanazawa, Ishikawa 920-1192, Japan. , 3 Faculty of Mathematics and Physics, Kanazawa University,
Kakuma-machi, Kanazawa, Ishikawa 920-1192, Japan. , 4 Faculty of Mathematics and Physics, Kanazawa University,
Kakuma-machi, Kanazawa, Ishikawa 920-1192, Japan. , 5 Faculty of Mathematics and Physics, Kanazawa University,
Kakuma-machi, Kanazawa, Ishikawa 920-1192, Japan. , 6 Faculty of Mathematics and Physics, Kanazawa University,
Kakuma-machi, Kanazawa, Ishikawa 920-1192, Japan. , 7 Faculty of Mathematics and Physics, Kanazawa University,
Kakuma-machi, Kanazawa, Ishikawa 920-1192, Japan.

We are developing a TES microcalorimeter operation system using a compact adiabatic demagnetization refrigerator(ADR) of our own making, keeping ground application and future missions in mind. Our ADR cryostat is composedof an FAA salt pill fabricated in-house, a superconducting magnet with a passive magnetic shield around it, anda mechanical heat switch, with a liquid helium tank as a heat sink. In LTD16, we reported the energy resolutionof 3.8 ± 0.2 eV (FWHM), when the detector was operated at 80 mK. Among the noise terms, the readout noise
had the largest contribution (∼ 3.0 eV). It turned out that the noise level of the SQUID we were using became
gradually higher below 3 kHz, while the signal-to-noise ratio of the TES microcalorimeter was the highest at arounda few 100 Hz. Thus, we evaluated the noise level of SQUIDs in our cryostat and adopted a gradiometer-type SQUID
developed by ISAS/JAXA for TES microcalorimeter operation. When it was operated in our cryostat, the noise level
was about 14 pA/sqrtHz in the 1–10 kHz range, and 26 pA/sqrtHz at 100 Hz. An advantage of this SQUID is thatthe heat dissipation is low, and hence, it can be operated at the detector stage. We also improved the SQUID drive
circuit, and removed noise of certain frequencies other than 60 Hz and its harmonics. We are now evaluating the
TES microcalorimeter performance using the new SQUID and the improved circuit. In the poster, we will present theresults.
category : Cryogenics and Components292

PD-10 Large Angle Optical Access in a sub-Kelvin Cryostat for the Development of a
Beam Steering Antenna
Sebastian Hahnle1 , Juan Bueno2 , Robert Huiting3 , Jochem Baselmans4
1

SRON Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research , 3 SRON Netherlands
Institute for Space Research , 4 SRON Netherlands Institute for Space Research / Delft University of Technology

Imaging arrays of antenna coupled MKIDs (Microwave Kinetic Inductance Detectors) use antennas with fast beams
in order to increase the pixel density for a given throughput of the telescope optics, therefore reducing the size of thearray and the cryostat optics. The beam width of these antennas at −10 dB taper is in the order of ±20◦ , whichmakes measurements of the antennas full beam pattern, including side lobes, challenging to implement. However,these measurements are necessary to fully understand the performance of the imaging array. As the operation of
hybrid MKIDs also requires temperatures of T < 270 mK, a low-temperature setup with optical access to an external
hot source at extremely large opening angles is needed.
We present the design of a cryostat based on a He-7 sorption cooler in a dry pulse-tube system with a total
opening angle of θ = 75.6◦ transparent up to fc ≈ 950 GHz. The cryostat was succesfully tested, reaching a loaded
base temperature of Tb = 264 mK with a holdtime of th > 24 h for a single recharge of the sorption cooler.

category : Cryogenics and Components

293PD-11 Feasibility Study for an IR-LED Based Calibration System for SuperCDMS
Detectors
Muad M Ghaith1
1

Department of Physics, Engineering Physics & Astronomy, Queen’s University

The Super Cryogenic Dark Matter Search (SuperCDMS) is one of the leading experiments in the direct search for the
Weakly Interacting Massive Particles (WIMPs) at the low mass scale (below 10 GeV/c2). The experiment operates
cryogenic germanium detectors at a few tens of mK in a well-shielded environment, measuring both phonon and charge
signals to identify elastic scatters of WIMPs oﬀ atomic nuclei. The experiment now is in transition to the new location
at SNOLAB near Sudbury, Canada, and the plan is to lower the energy threshold of the detectors down to a few
tens of eV by reducing the noise in the readout circuit and improving the design of the TES based phonon sensors.
Traditionally radioactive sources are used to calibrate the energy scale and to check the detector stability. However,in most cases, it takes a long time to accumulate enough events to identify peaks in the energy spectrum. Moreover,gammas at low energy as would be desired for the lower threshold detectors cannot penetrate the cryostat. In thisposter, I am presenting a study investigating the possibility of using pulsed infrared LEDs (1650 nm) as alternative
calibration sources.
category : Cryogenics and Components294PD-12 A cryogenic detector characterisation facility in the shallow undergroundlaboratory at the Technical University of Munich
Alexander Langenkamper1 , Xavier Defay2 , Nahuel Ferreiro3 , Angelina Kinast4 , Jean-Come Lanfranchi5 , Erik
Lindner6 , Michele Mancuso7 , Elizabeth Mondragon8 , Andrea Munster9 , Tobias Ortmann10 , Walter Potzel11 , Stefan
Schonert12 , Andreas Ulrich13 , Stephan Wawoczny14 , Michael Willers15
1

Physics Department and Excellence Cluster Universe, Technical University of Munich, 2 Physics Department and Excellence
Cluster Universe, Technical University of Munich , 3 Max-Plack-Institut fur Physik , 4 Physics Department and Excellence
Cluster Universe, Technical University of Munich , 5 Physics Department and Excellence Cluster Universe, Technical Universityof Munich , 6 Physics Department and Excellence Cluster Universe, Technical University of Munich , 7 Max-Plack-Institut fur
Physik , 8 Physics Department and Excellence Cluster Universe, Technical University of Munich , 9 Physics Department andExcellence Cluster Universe, Technical University of Munich , 10 Physics Department and Excellence Cluster Universe,
Technical University of Munich , 11 Physics Department and Excellence Cluster Universe, Technical University of Munich ,12
Physics Department and Excellence Cluster Universe, Technical University of Munich , 13 Physics Department andExcellence Cluster Universe, Technical University of Munich , 14 Physics Department and Excellence Cluster Universe,
Technical University of Munich , 15 Physics Department and Excellence Cluster Universe, Technical University of Munich

The Physics Department of the Technical University of Munich operates a shallow underground detector laboratory(overburden 15 m.w.e.) featuring approximately 180m2 of laboratory space at the campus in Garching, Germany.
One of the main applications of this laboratory is the development and characterisation of cryogenic detectors in theframework of the CRESST-III experiment and next-generation cryogenic neutrinoless double beta decay experiments.
To this end, a dedicated 3He/4He dilution refrigerator (Oxford Kelvinox 100) is operated. The experimental setup is
instrumented with a 4-channel SQUID readout system together with a readout system for NTD sensors, enabling theoperation of a wide range of cryogenic detectors. The experimental setup, furthermore, features a CRESST compatible
data acquisition system as well as an active muon veto system. Passive shielding against external radiation is provided
by 10-15 cm of lead completely surrounding the cryostat dewar.
The laboratory has also recently (2016) been extended to include a 25m2 cleanroom (class ISO 7) which will be
used for the fabrication and assembly of cryogenic detectors for the CRESST-III experiment. In this contribution, we
will present the current status of the shallow underground laboratory, and of the experimental setup.
category : Cryogenics and Components295

PD-13 Concept Design of High Frequency Telescope for LiteBIRD
Takashi Hasebe1 , LiteBIRD Collaboration2
1

National Astronomical Observatory of Japan, 2 see attached list

LiteBIRD is a satellite mission which is planned to be lunched by JAXA in middle of 2020’s for verification of
inflation at the beginning of the universe via the B-mode polarization of the cosmic microwave background. The
precise measurement of the B-mode signal with the sensitivity of σr < 0.001 requires the removal of contaminating
polarized emissions, mainly from synchrotron and thermal dust. In order to separate these foreground emissions, theobservations of the broad frequency spectrum of them are necessary. For the purpose of the broadband and wide filed
observations of the all sky, LiteBIRD receives frequency bands of 40 - 402 GHz with two telescopes, which are the low
frequency telescope (LFT) and the high frequency telescope (HFT).
The HFT consists of a continuous-rotating half wave plate, two silicon lenses and focal plane detectors. In orderto suppress thermal emissions from the optical elements, all components are cooled down to less than 5 Kelvin.
Superconducting detectors at the focal plane operate at 100 mK for extremely low-noise detection.
The baseline design of the HFT has an aperture diameter of 200 mm for 280 - 402 GHz.
The optical design has been optimized to the field-of-view of 10 deg × 10 deg. The mechanical structure andthermal design has been studied to derive requirements and specifications of the components. A possibility to an
expanded option of the HFT with an aperture diameter of 300 mm for 166 - 402 GHz is discussed.
category : Cryogenics and Components296

PD-14 CUTE - A low noise facility for testing cryogenic dark matter detectors
philippe camus1 , Gilles Gerbier2 , Wolfgang Rau3 , Koby Dering4 , Antoine Caze5 , Ali Dastgheibi-Fard6 , Silvia Scorza7
1

Department of Physics, 2 Queen’s University, Kingston (Canada) , 3 Queen’s University, Kingston (Canada) , 4 Queen’s
University, Kingston (Canada) , 5 IPNL, Domaine de la Doua, Villeurbanne (France) , 6 LSM, Carre des Sciences, Modane(France) , 7 SNOLAB, Cregithon Mine 9, Lively (Canada)

CUTE is a new cryogenic facility for testing cryogenic dark matter detectors. It is under construction at SNOLAB,
a laboratory for particle research located 2 km underground near Sudbury (Ontario, Canada). Close to the future
SuperCDMS experiment, this facility will be used to validate the detector towers before installation in the main
experiment. Being in a low background environment, the CUTE facility has a sensitivity competitive with other dark
matter experiment and will be able to produce several advanced results in the search for low-mass WIMPS.
We report the design choices made to control the local background around the detectors and the mechanicalarchitecture in order to limit the vibrations transmission. The low temperature required to operate the cryogenic
detector is obtained by an advanced pulse-tube based dilution refrigerator from CyroConcept (France). The so-called
Ultra Quiet Technique ? UQT, reduces the vibration transmission by using an original gas-coupled thermal link
between the 2-stages pulse tube and the cryostat. In order to install the cryostat into a shielding water tank, we havedeveloped an advanced suspension system which de-couples the cryostat from his environment with a low stiﬀness
support, making a mechanical low-pass filter below 2 Hz for the vertical attenuation.
category : Cryogenics and Components297

PD-15 Optimization of detector arrays and the cryogenic platform for the ECHo
experiment
Clemens Hassel1 , Steﬀen Allgeier2 , Christian Enss3 , Anna Ferring4 , Andreas Fleischmann5 , Dorothea Fonnesu6 , Lisa
Gamer7 , Loredana Gastaldo8 , Daniel Hengstler9 , Sebastian Kempf10 , Federica Mantegazzini11 , Dennis Schulz12 ,Mathias Wegner13
1

Kirchhoﬀ-Institute for Physics, Heidelberg University, 2 Kirchhoﬀ Institute for Physics, Heidelberg University , 3 Kirchhoﬀ
Institute for Physics, Heidelberg University , 4 Kirchhoﬀ Institute for Physics, Heidelberg University , 5 Kirchhoﬀ Institute forPhysics, Heidelberg University , 6 Kirchhoﬀ Institute for Physics, Heidelberg University , 7 Kirchhoﬀ Institute for Physics,
Heidelberg University , 8 Kirchhoﬀ Institute for Physics, Heidelberg University , 9 Kirchhoﬀ Institute for Physics, Heidelberg
University , 10 Kirchhoﬀ Institute for Physics, Heidelberg University , 11 Kirchhoﬀ Institute for Physics, Heidelberg University ,12
Kirchhoﬀ Institute for Physics, Heidelberg University , 13 Kirchhoﬀ Institute for Physics, Heidelberg University

The Electron Capture in 163 Ho experiment ECHo aims to probe the electron neutrino mass on a sub-eV level via
the analysis of the calorimetrically measured high statistics electron capture spectrum of 163 Ho. For this, metallic
magnetic calorimeter arrays (MMC) will be used, which are operated at millikelvin temperatures. The performanceachieved by first prototypes of MMC detectors show that an energy resolution of ∆EFWHM ¡ 5 eV and a signal risetime of τr ¡ 1 µs can be reached. These values, obtained with single channel read out, fulfill the requirements for the
first phase of ECHo, ECHo-1k. The challenge is to keep the same performance using the multiplexed read out. We
present the current status of the new design for the detector arrays to be used in ECHo-1k. This array design allows
for parallel read out as well as for multiplexed read out. We discuss results obtained during the first characterizationof these detectors. The first phase of ECHo will be performed in a new dedicated cryostat. The future plans for
mounting read out cables and the design for the installation of the array on the experimental platform will be shown.
Finally we discuss the present status of the ECHo-1k experimental set-up and present first results obtained with the
new arrays operated in the new cryostat.
category : Cryogenics and Components298PD-16 Impact of a cryogenic half-wave plate polarization modulator on the detector
array sensitivity of the POLARBEAR-2 CMB experimentCharles Alexander Hill1 , Akito Kusaka2 , Paul Barton3 , Alex G Droster4 , Mael Flament5 , Suhas Ganjam6 , Arian
Jadbabaie7 , Oliver Jeong8 , Brian Keating9 , Adrian T Lee10 , Alex Madurowicz11 , Frederick T Matsuda12 , Tomotake
Matsumura13 , Adam Rutkowski14 , Yuki Sakurai15 , Danielle R Sponseller16 , Aritoki Suzuki17 , Raymond Tat18
1

University of California, Berkeley, 2 Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA /Department of Physics, University of Tokyo, Tokyo 113-0033, Japan , 3 Physics Division, Lawrence Berkeley National
Laboratory, Berkeley, CA 94720, USA , 4 Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA, 5 Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA , 6 Department of Physics, Universityof California, Berkeley, CA 94720, USA / Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA, 7 Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA , 8 Department of Physics, Universityof California, Berkeley, CA 94720, USA , 9 Department of Physics, University of California, San Diego, CA 92093-0424, USA ,10
Department of Physics, University of California, Berkeley, CA 94720, USA / Physics Division, Lawrence Berkeley National
Laboratory, Berkeley, CA 94720, USA / Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA ,11
Department of Physics, University of California, Berkeley, CA 94720, USA / Physics Division, Lawrence Berkeley National
Laboratory, Berkeley, CA 94720, USA , 12 Department of Physics, University of California, San Diego, CA 92093-0424, USA ,13
Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan , 14 Physics Division, Lawrence
Berkeley National Laboratory, Berkeley, CA 94720, USA , 15 Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa,
Chiba 277-8583, Japan , 16 Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA ,17
Department of Physics, University of California, Berkeley, CA 94720, USA / Radio Astronomy Laboratory, University ofCalifornia, Berkeley, CA 94720, USA , 18 Department of Physics, University of California, Berkeley, CA 94720, USA / Physics
Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA

Polarization modulation using a continuously-rotating half-wave plate (HWP) is a promising technique to mitigate
the impact of low-frequency noise and systematic error on the performance of Cosmic Microwave Background (CMB)
polarization experiments. However, thermal emission from an ambient-temperature HWP adds significant opticalloading onto the focal plane and thus decreases detector sensitivity to the CMB signal. Therefore, we present thedesign and testing of a cryogenic HWP (CHWP) for implementation on POLARBEAR-2 (PB-2), an upcoming CMB
camera consisting of 7,588 Transition Edge Sensor (TES) bolometers observing at 95 and 150 GHz via dichroic,dual-polarized pixels. The CHWP is comprised of a broadband Pancharatnam sapphire stack on a superconducting
magnetic bearing. It will operate at 50 K, 460 mm diameter, and 2 Hz continuous rotation, modulating the Stokes
Q/U sky signal input to all 1,897 pixels at 8 Hz simultaneously. We discuss CHWP performance from the perspectiveof detector sensitivity, with an emphasis on photon noise, bolometer thermal carrier noise, and instrument mapping
speed.
category : Cryogenics and Components299

PD-17 International Development of Detector Cooling System Down to 50 mK inSpace without Cryogens
Noriko Y. Yamasaki1 , Kazuhisa Mitsuda2 , Takao Nakagawa3 , Keisuke Shinozaki4 , Chihiro Tokoku5 , Ryo
Yamamoto6 , Yuto Minami7 , Ivan Charles8 , Jean-Marc Duval9 , Thomas Prouve10 , Jerome Andre11 , Christophe
Daniel12 , Michel Ledu13 , Irwin Maussang14 , Alice Pralines15
1

ISAS/JAXA, 2 ISAS/JAXA , 3 ISAS/JAXA , 4 ARD/JAXA , 5 ISAS/JAXA , 6 ISAS/JAXA , 7 KEK , 8 CEA , 9 CEA , 10 CEA ,11
CNES , 12 CNES , 13 CNES , 14 CNES , 15 CNES

Low temperature detectors with supreme sensitivity are often expected to be cutting-edge instruments for spaceastronomy missions. The Athena mission has been selected by European Space Agency (ESA) , as a large X-ray
observatory launched in 2028 to implement the Hot and Energetic Universe. One of its instrument is X-IFU, acryogenic X-ray spectrometer based on a large array of TES microcalorimeter with 3840 pixels and 2.5 eV energy
resolution. There also several proposed missions like infrared mission SPICA, cosmic microwave background (CMB)
polarization mission Core+/LiteBIRD to be operated below 100 mK.
ESA called a Core Technology Program (CTP) for design, development, assembling, and functional verification of adetector cooling chain including cryostat and coolers down to 50 mK . The goal of this CC-CTP (Cooling Chain CTP)
is to develop a feasible cryogenic chain in space without exhausting cryogen and/or operating fluid to achieve ¿5 years
working life. It requires a technical jump from Plank and Astro-H. CNES (Centre National d Etudes Spatiales) and
X-IFU pre consortium members for cryogenic system, ALAT (Air Liquid Advanced Technologies), CEA(Commissariat
a l Energie Atomic et aux Energies Alternatives), INTA(Instituto Nacional de Tecnica Aeroespacial), JAXA (Japan
Aerospace eXploration Agency), SRON (SRON Netherlands Institute for Space Research) and RAL (Rutherford
Appleton Laboratory) , participate in this project.
As a first step of CC-CTP, CNES, CEA, and JAXA is fabricating and testing a cryostat with a combination of
4K Joule-Thomson (JT), 2K JT, pre-coolers and sub-K coolers, an adiabatic demagnetization refrigerator (ADR) as
sub-K cooler. Test campaign at CEA premise with Japanese 4K/2K JT and French sub-K coolers to obtain the coolingpower as a function of interface temperatures, power consumption etc., has started from 2017 April. We will present
these activities , as a key technology for future applications of low temperature detectors.
category : Cryogenics and Components

300

PD-18 Experimental study and modeling of cryogenic detectors decoupling within
dry cryostat
Romain Maisonobe1 , Julien Billard2 , Maryvonne De Jesus3 , Louis Dumoulin4 , Alexandre Juillard5 , StefanosMarnieros6 , Dimitri Misiak7 , Sayah Sihem8 , Lionel Vagneron9
1Institut de Physique Nucleaire de Lyon, 2 Institut de Physique Nucleaire de Lyon , 3 Institut de Physique Nucleaire de Lyon ,Centre des Sciences Nucleaires et des Sciences de la Matiere, Orsay , 5 Institut de Physique Nucleaire de Lyon , 6 Centre desSciences Nucleaires et des Sciences de la Matiere, Orsay , 7 Institut de Physique Nucleaire de Lyon , 8 Institut de Physique
Nucleaire de Lyon , 9 Institut de Physique Nucleaire de Lyon

4

The dry cryostat technology is based on pulse tube cryo-coolers and oﬀers a good alternative to wet dilution cryostats.
However, the main drawback is the production of vibrations from the pulse tube. These vibrations can be transmitted
to the cryogenic detectors mounted in the cryostat and cause extra-noises dramatically aﬀecting their performances.
A solution to mitigate the impact of these vibrations is to mount the detectors on a suspended tower.
For this purpose, vibrations in a dry cryostat were modelled and preliminary prototypes were investigated in thescope of detectors R&D for the EDELWEISS-III experiment.
First results and future prospects are discussed in this presentation.
category : Cryogenics and Components301PD-19 A 300 mK Testbed for Rapid Characterization of Microwave SQUID
Multiplexing Circuits
Abigail L. Wessels1 , John A.B. Mates2 , Vincent Kotsubo3 , Norman Jarosik4 , Johnathon D. Gard5 , Douglas A.
Bennett6 , Daniel T. Becker7 , Johannes Hubmayr8 , Joel N. Ullom91

Department of Physics, University of Colorado Boulder, 2 University of Colorado, Boulder , 3 National Institute of Standards
and Technology , 4 Princeton University , 5 University of Colorado, Boulder , 6 National Institute of Standards and Technology ,7
University of Colorado, Boulder / National Institute of Standards and Technology , 8 National Institute of Standards andTechnology , 9 National Institute of Standards and Technology

A significant challenge in the development of arrays of low-temperature detectors has been the development of simple,
low-power, multiplexed readout schemes. This challenge has been heightened as demand grows for arrays of tens of
thousands of pixels and large arrays of high-speed pixels. To meet this demand, a new multiplexing method, microwave
SQUID multiplexing, has been developed that is capable of providing the bandwidth necessary for large arrays of fast
TESs. These multiplexers consist of RF-SQUIDs coupled to superconducting microwave resonators, which are probed
via a common microwave feedline and read out at room temperature using GHz signals carried on coaxial cables.
For both the development of microwave SQUID circuits and quality assurance before circuits are integrated into
instruments, we need a high-throughput testbed for characterization and testing. This will allow us to rapidly screen devices and develop useful statistics describing them. Because the microwave properties of our lithographically-patterned
niobium resonators change substantially above 500 mK, any characterization testbed must reach temperatures below
this critical value to provide relevant data.
We have therefore assembled a testbed for measurement of microwave SQUIDs consisting of a helium-3 sorption
refrigerator, backed by a pumped helium-4 stage, in a compact liquid helium dip probe. The probe enables us tocool microwave devices to 300 mK in roughly three hours. This system will substantially accelerate our ability to test
and characterize microwave SQUID multiplexing circuits. In addition to describing the probe, we show representative microwave SQUID test data, including the dependence of resonator frequency locations and quality factors on
temperature.
category : Cryogenics and Components302

PD-20 A micro-vibration acoustic attenuator for low temperature detectors.
Luciano Gottardi1 , J. Dercksen2 , H. van Weers3 , H. Akamatsu4 , J. van der Kuur5 , B. Jackson6 , K. Ravensberg7 , J.
R. Gao8 , P. Khosropanah91

SRON - Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research, Utrecht, The
Netherlands , 3 SRON Netherlands Institute for Space Research, Utrecht, The Netherlands , 4 SRON Netherlands Institute forSpace Research, Utrecht, The Netherlands , 5 SRON Netherlands Institute for Space Research, Utrecht, The Netherlands ,6
SRON Netherlands Institute for Space Research, Utrecht, The Netherlands , 7 SRON Netherlands Institute for Space
Research, Utrecht, The Netherlands , 8 SRON Netherlands Institute for Space Research, Utrecht, The Netherlands / Kavli
Institute of NanoScience, Delft University of Technology, Delft, The Netherlands , 9 SRON Netherlands Institute for Space
Research, Utrecht, The Netherlands

Most of the low temperature detectors are nowadays operated in dilution or adiabatic demagnetization refrigerator
are based on pulse tube cryocoolers. The main disadvantage of a cryogeen-free cooler is the potential high level ofmechanical vibrations at the warm and cold interfaces that could aﬀect the sensitivity of low temperature instruments.
We describe the performance of a very simple acoustic attenuation system used to eliminate the pulse-tube-induced
low frequency noise of the superconducting transition-edge sensors under development for the instruments of the next
generation of infra-red and X-ray space observatories. The attenuator consists of a multi-stage passive mass-spring
system designed to reduce the level of micro-vibration at the detector site for all the six rotational and translationalmodes. Attenuation of more than 60dB in the noise equivalent power of TES bolometers has been demonstrated witha two-stage acoustic isolator.
.
category : Cryogenics and Components303

PD-21 Magnetic field shielding for a Rydberg-atom single-photon detector: basic
approach and measurements
Masahiro Shibata1 , Tomohito Haseyama2 , Kentaro Kominato3 , Satoru Yamada4 , Masaru Tada5 , Yasuhiro
Kishimoto6 , Izumi Ogawa7 , Haruhiko Funahashi8 , Seishi Matsuki91

Research Center for Nuclear Physics, Osaka Univerisity, 2 Japan Laser Corporation, Inc, Shinjuku, Tokyo 169-0051, Japan ,3
JASTEC, Inc., Kobe 651-2271, Japan , 4 KEK, Tsukuba 305-0801, Japan , 5 KEK, Tsukuba 305-0801, Japan , 6 Kamioka
Observatory, Institute for Cosmic Ray Research, The University of Tokyo, Gifu 506-1205, Japan , 7 Faculty of Engineering,
University of Fukui, Fukui, 910-8507, Japan , 8 Institute for Liberal Arts and Sciences, Kyoto University, Kyoto
606-8501,Japan , 9 Research Center for Nuclear Physics, Osaka University, Ibaraki, Osaka 567-0047, JapanThe Rydberg-atom single-photon detector developed by the CARRACK group in Kyoto is expected to be one of themost sensitive methods to search for dark matter axions[1]. In order for the detector to be successful enough, it isessential to shield a microwave-detection cavity and the following selective field ionization (SFI) region from the highmagnetic field inevitably present closely to convert axions to microwave photons. It is because without the magnetic
field, the energy level structure of the relevant Rydberg atoms becomes simpler and thus easier to handle theoreticallyand also experimentally. Moreover, the eﬀect of motional Stark eﬀect can be reduced by the magnetic field shielding
for an Rydberg atomic beam with its velocity of around 300 m/s suitable for the sensitive photon detection.
We developed an eﬃcient way to shield the magnetic field of 7 T maximum for the axion-photon conversion situatedvery closely from the microwave-photon detection region. Basic approach to this is firstly to reduce the magnetic field
to less than 0.1 T at the photon detection region by using a superconducting cancellation coils and then to cover
the region with Nb metals in which the magnetic field is below the lower critical field Bc1 of Nb. By reducing themagnetic field below the lower critical field of the type II superconductor Nb, it is possible to utilize eﬃciently theperfect diamagnetic (Meissner) eﬀect for the shielding.
Here we report our basic approach to the subject and its related measurements for the magnetic field shielding in
the Rydberg-atom single-photon detector. Specifically we analyzed in detail the eﬀect of the demagnetizing factor in
the shape of the Nb metals on reducing the magnetic field below Bc1 of Nb. We also studied the eﬀect of additional
Nb metal rings and commercially available NbTi/Nb/Cu multilayer-alloy sheets placed above the Nb metal cover. [1]
R. Bradley, S. Matsuki et al., Rev. Mod. Phys. 75(2003)777.
category : Cryogenics and Components

304

PD-22 Design of magnetic shielding and field coils for a TES X-ray microcalorimeter
test platform
Antoine R. Miniussi1 , Joseph S. Adams2 , Simon R. Bandler3 , James A. Chervenak4 , Aaron M. Datesman5 , Megan
E. Eckart6 , Fred M. Finkbeiner7 , Richard L. Kelley8 , Caroline A. Kilbourne9 , Frederick S. Porter10 , John E.
Sadleir11 , Kazuhiro Sakai12 , Stephen J. Smith13 , Nicholas A. Wakeham14 , Edward J. Wassell15 , Wonsik Yoon16 ,Willam B. Doriese17 , Henk J. van Weers18
1

NASA/GSFC, 2 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 3 NASA
Goddard Space Flight Center , 4 NASA Goddard Space Flight Center , 5 NASA Goddard Space Flight Center / SGT, Inc. ,6NASA Goddard Space Flight Center , 7 NASA Goddard Space Flight Center / Wyle Information Systems , 8 NASA Goddard
Space Flight Center , 9 NASA Goddard Space Flight Center , 10 NASA Goddard Space Flight Center , 11 NASA Goddard Space
Flight Center , 12 NASA Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 13 NASA
Goddard Space Flight Center / CRESST II - University of Maryland Baltimore County , 14 NASA Goddard Space Flight
Center / NPP - Universities Space Research Association , 15 NASA Goddard Space Flight Center / SGT, Inc. , 16 NASA
Goddard Space Flight Center / NPP - Universities Space Research Association , 17 NIST - National Institute of Standards andTechnology , 18 SRON - National Institute for Space Research

The performance of transition-edge sensors (TES) and their SQUID multiplexed read-outs are very sensitive to theambient magnetic field and fluctuations that can arise due to fluctuating magnetic fields outside of the focal planeassembly. In order to run ground experiments on thousands of X-ray TES microcalorimeters within a low ambient anduniform magnetic field (¡ 1 uGauss, with a uniformity ¡ 0.1 uGauss) we need a very low field to be trapped into out
superconducting magnetic shields. In addition, we require very stringent magnetic field shielding factors, ideally lessthan a part in 10?5 for field components normal to the surface of the thin-film TES sensors and read-out amplifiers.
This level of shielding is highly beneficial in enabling the detectors and read-out to be immune to external field
variations that can arise due to, for instance, fluctuations in the fields from the adiabatic demagnetization refrigerator,
as well to be immune to AC fluctuations in the external fields.
We have designed a sub-kelvin test platform to reach these specifications. For this purpose, we modeled a new
design for the shielding consisting of a series of diﬀerent mu-metal and superconducting shields, including a niobium
shield at 50 mK, a cryoperm (A4K) shield at 3 K and a mu-metal shield at 300 K. Our study included comparisonsof diﬀerent shield geometries and material thicknesses, which is presented. The status of measurements that confirm
these models will also be presented.
It is often desirable to be able to apply a DC magnetic field across an array to help optimize the performance of
the TESs. We have studied a number of diﬀerent field -coil designs, and the impact of the diﬀerent shield geometries,
in order to reach the required field uniformity. The uniformity desired for the TES array is less than one part in 1000
across a 15 mm array. The variation in fields seen by the read-out SQUID electronics has also been considered, andhas been designed to be kept suﬃciently low to avoid having such fields aﬀect to the read-out performance.
category : Cryogenics and Components

305

Category E : Applications306

PE-1 A Review of Packaging and Integration Techniques for Large Superconducting
Detector Arrays for Cosmic Microwave Background Observations
Shuay-Pwu Patty Ho1 , ACT Collaboration2
1

Department of Physics, Princeton University, 2 ACT Collaboration

The cosmic microwave background (CMB) continues to reveal new aspects of the large scale universe. For example,
current projects are searching for evidence of primordial gravitational waves, for signatures sensitive to the sum of theneutrino masses, and for further understanding of the formation and growth of large structures under the influenceof gravity in the accelerating universe. Technologies for ground-based and balloon-borne instruments measuring thepolarization of the CMB have been well established and advanced in the last decade. Experience from the current
generation of CMB projects indicates that the integration of the cryogenic detector array package, including its
multiplexing and readout elements, is critical to the performance of the CMB instrument. The next generation of
instruments needed to fully explore the potential of the CMB will require many more detectors than have currently
been deployed. As the number of detectors per focal plane scales up, improvements and new technologies for large
array packaging will be required. In this proceedings, we review the integration of Transition-Edge Sensors withreadout components and optical coupling structures for the current array package assembly processes of multiple
telescopes. We present the concept from Advanced ACTPol for the assembly of large bolometer arrays, and compare
to the successes from other CMB projects. We will summarize the possible improvements and limitations anticipatedin driving towards large numbers of even higher density detector arrays, keeping in mind the need for faster production
rates while maintaining good performance and high yield.
category : Applications

307

PE-2 Polarization Sensitive Microwave Detectors for a Satellite CMB Mission
Kyle R Helson1 , Aamir Ali2 , John Appel3 , Charles L Bennett4 , Berhanu Bulcha5 , Meng-ping Chang6 , David T
Chuss7 , Nicholas Costen8 , Kevin L Denis9 , Thomas Essinger-Hileman10 , Ron Hu11 , Tobias A Marriage12 , Karwan
Rostem13 , Marco Sagliocca14 , Kongpop U-Yen15 , Edward J Wollack16
1

NASA/GSFC, 2 Johns Hopkins University , 3 Johns Hopkins University , 4 Johns Hopkins University , 5 NASA/Goddard Space
Flight Center , 6 NASA/Goddard Space Flight Center , 7 Villanova University , 8 NASA/Goddard Space Flight Center ,9NASA/Goddard Space Flight Center , 10 Johns Hopkins University , 11 NASA/Goddard Space Flight Center , 12 Johns
Hopkins University , 13 NASA/Goddard Space Flight Center / Johns Hopkins University , 14 NASA/Goddard Space Flight
Center , 15 NASA/Goddard Space Flight Center , 16 NASA/Goddard Space Flight Center

The detailed characterization of the intensity and polarization of the Cosmic Microwave Background (CMB) radiation
provides a powerful tool to constrain the properties of the early Universe. The polarization induced by a stochastic
gravitational wave background in this epoch produces a distinctive and measurable signature of primordial inflationary
processes. Here we report on the status and development of polarization-sensitive detectors for a satellite CMB
polarization mission and their application in ground based instrument settings. The sensor architecture features anantenna-coupled detector with an integrated orthomode transducer (OMT), on-chip band defining filters, and features
to control spurious radiometric coupling. The detectors are based on a Transition-Edge Sensor (TES) design and thesuperconducting circuitry is defined via thin film coatings on a single-crystal silicon substrate. The sensor design isreadily scalable in both frequency coverage, 30-300 GHz, and in number of detectors.
category : Applications308

PE-3 Advanced ACTPol 27/39 GHz Detector Array Calibration with Fourier
Transform Spectroscopy: Foreground Removal in CMB Maps
Taylor Baildon1
1

University of Michigan

Advanced ACTPol (AdvACT) is an upgrade to the Atacama Cosmology Telescope that oﬀers a unique combinationof sensitivity, resolution, spectral channels, and sky coverage for mapping the polarization of the Cosmic Microwave
Background (CMB). Detection of?B-mode polarization in the CMB could provide the first measurements of?quantum
gravity, determine the energy scale of inflation,?constrain dark matter, and allow us to measure the sum of the neutrino
masses.?To obtain a precise?measurement of the primordial B-mode power spectrum, polarized?galactic?foregroundemission from synchrotron radiation and dust?must be?characterized and?removed with high accuracy. Accurate
subtraction of this foreground emission is contingent upon precise knowledge of the spectral responses of the AdvACT
detectors over AdvACT s five frequency bands, which requires state of the art calibration. A Fourier Transform
Spectrometer (FTS) is an interferometer?with a known source?that can be used to measure the spectral responses of
the AdvACT detectors. Polarizers within the FTS split orthogonal polarizations and allow us probe the detectors fullpolarized responses, and a set of coupling optics couple the FTS beam to the detectors housed in a cryostat.?The?FTS
used to perform detector calibration?for?ACTPol achieved 2-GHz accuracy on the 150 GHz band centers, but thisaccuracy must be improved?by?at least a factor of 4 to obtain?suﬃcient polarization measurements for foregroundcleaning. A new FTS with larger etendue is required to calibrate the low-frequency channels of AdvACT and toenable?fast?calibration of the full focal plane.?To improve the?calibration accuracy in the low frequency range, thetransmission and polarization properties of all optical elements in the new FTS and coupling optics must be precisely
characterized. I will present optical measurements of the AdvACT low frequency 27/39 GHz detector bands obtainedusing the new FTS, and?an overview of the design, characterization, and implementation of the new FTS technology.
category : Applications309

PE-4 SPIDER: CMB polarimetry from the edge of space
Jeﬀrey P. Filippini1 , Spider collaboration
1

Department of Physics, University of Illinois at Urbana-Champaign,

SPIDER is a powerful balloon-borne instrument to map the polarization of the millimeter-wave sky at large angularscales. SPIDER targets the B-mode signature of primordial gravitational waves in the cosmic microwave background(CMB), with a focus on mapping a large sky area with high fidelity at multiple frequencies. SPIDER’s first longduration balloon flight in January 2015 deployed a total of 2400 antenna-coupled TESs at 94 GHz and 145 GHz. I
will review the designof the SPIDER instrument, as well as the current status of science
Typesetandusing LAin-flight
TEX twocolumn performancestyle in AASTeX61
analysis and technology developments toward SPIDER s second flight in 2018. I will also discuss the optimization of
the TESs and receivers
take full advantage
of a space-likeobserving
platform,
includingthecharacterization of the
DESIGN,to
CONSTRUCTION,
AND CHARACTERIZATION
OF THE
280 GHZ FOCALPLANE UNITSFOR THESECOND
FLIGHT
OF THE SPIDERin
POLARIMETER
response of these detectors to particle radiationencounteredspace.
A. S. B ERGMAN , 1 P. A. R. A DE , 2 M. A MIRI , 3 J. A. AUSTERMANN , 4 J. A. B EALL , 4 D. T. B ECKER , 4 S. J. B ENTON , 1 J. J. B OCK , 5, 6
J. R. B OND , 7 S. A. B RYAN , 8 H. C. C HIANG , 9, 10 C. R. C ONTALDI , 11 O. D ORÉ , 5, 6 S. M. D UFF , 4 A. J. D UIVENVOORDEN , 12
H. K. E RIKSEN , 13 M. FARHANG , 7, 14 J. P. F ILIPPINI , 15, 16 L. M. F ISSEL , 17, 14 A. A. F RAISSE , 1 K. F REESE , 18, 12 M. G ALLOWAY , 19
A. E. G AMBREL , 1 N. N. G ANDILO , 20, 21 K. G ANGA , 22 A. G RIGORIAN , 4 J. E. G UDMUNDSSON , 12 M. H ALPERN , 3 J. H ARTLEY , 19
M. H ASSELFIELD , 23 G. H ILTON , 4 W. H OLMES , 6 V. V. H RISTOV , 5 Z. H UANG , 7 J. H UBMAYR , 4 K. D. I RWIN , 24, 25 W. C. J ONES , 1
C. L. K UO , 24 Z. D. K ERMISH , 1 S. L I , 14, 1, 26 P. V. M ASON , 5 K. M EGERIAN , 6 L. M ONCELSI , 5 T. A. M ORFORD , 5 J. M. NAGY , 27
C. B. N ETTERFIELD , 14, 19 M. N OLTA , 7 I. L. PADILLA , 14 B. R ACINE , 13 A. S. R AHLIN , 28, 29 C. R EINTSEMA , 4 J. E. RUHL , 27
M. C. RUNYAN , 6 T. M. RUUD , 13 J. A. S HARIFF , 7 J. D. S OLER , 30 X. S ONG , 1 A. T RANGSRUD , 5, 6 C. T UCKER , 2 R. S. T UCKER , 5
A. D. T URNER , 6 J. U LLOM , 4 J. F. VAN DER L IST , 1 J. VAN L ANEN , 4 M. R. V ISSERS , 4 A. C. W EBER , 6 I. K. W EHUS , 13
D. V. W IEBE , 3 AND E. Y. YOUNG 1
1 Department of Physics, Princeton University, Princeton, NJ, USA

2 School of Physics and Astronomy, Cardiff University, CF24 3AA, UK

3 Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada
4 National Institute of Standards and Technology, Boulder, CO, USA

5 Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
6 Jet Propulsion Laboratory, Pasadena, CA, USA

7 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada
8 School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA

9 School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Durban, South Africa
10 National Institute for Theoretical Physics (NITheP), KwaZulu-Natal, South Africa
11 Blackett Laboratory, Imperial College London, SW7 2AZ, London, UK

12 The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
13 Institute of Theoretical Astrophysics, University of Oslo, Oslo, Norway

14 Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON, Canada
15 Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL, USA

16 Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
17 National Radio Astronomy Observatory, Charlottesville, NC, USA

18 Department of Physics, University of Michigan, Ann Arbor, MI, USA
19 Department of Physics, University of Toronto, Toronto, ON, Canada

20 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
21 NASA Goddard Space Flight Center, Greenbelt, MD, USA

22 APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
23 Pennsylvania State University, University Park, PA, USA

24 Department of Physics, Stanford University, Stanford, CA, USA
25 SLAC National Accelerator Laboratory, Menlo Park, CA, USA

26 Department of Mechanical and Aerospace Engineering, Princeton University, Princeton, NJ, USA

27 Physics Department, Center for Education and Research in Cosmology and Astrophysics, Case Western Reserve University, Cleveland, OH, USA
28 Fermi National Accelerator Laboratory, Batavia, IL, USA

29 Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL, USA
30 Institut d’Astrophysique Spatiale, Orsay, France

ABSTRACT

Figure2: The top
authorJeﬀreyfocal
P. plane
Filippini.
We describe the construction
and characterizationof the280 GHzisbolometricunits (FPUs) to be deployed on thesecond flight of the balloon-borne S PIDER instrument. These FPUs are vital to S PIDER’s primary science goal of detecting or
placing an upper limit on the amplitude of the primordial gravitational-wave signature in the cosmic microwave background(CMB) by constraining the B-mode contamination in the CMB from galactic dust emission. Each 280 GHz focal plane contains
a 16 ⇥ 16 grid of corrugated silicon feedhorns coupled to an array of aluminum manganese transition-edge sensor bolometers,
category : Applications
fabricated on 150 mm diameter substrates. In total, the three 280 GHz FPUs contain 1,530 polarization sensitive bolometers (765stevie@princeton.edu

310

PE-5 Advanced ACTPol Low Frequency Array: Readout and Characterization ofPrototype 27 and 39 GHz Transition Edge Sensors
Brian J Koopman1 , AdvACT Collaboration2
1

Department of Physics, Cornell University, 2 AdvACT Collaboration

Advanced ACTPol (AdvACT) is a third generation polarization sensitive upgrade to the Atacama Cosmology
Telescope (ACT). AdvACT expands on the ACT Polarimeter’s mid frequency (MF, 90/150 GHz) transition edge
sensor (TES) bolometer arrays and adds both high frequency (HF, 220/270 GHz) and low frequency (LF, 27/39
GHz) multichroic arrays. The addition of the high and low frequency detectors allows for the removal of synchrotron
and spinning dust emission at the low frequencies and foreground emission from galactic dust and dusty star forming
galaxies at the high frequencies. The increased spectral coverage of AdvACT will enable improvements in a wide rangeof science, such as improving constraints on dark energy, the sum of the neutrino masses, inflationary parameters andpotentially the energy scale of inflation. The HF array was deployed for the 2016 season and two MF arrays are being
deployed for the 2017 season. The LF array will be the final AdvACT array, with deployment planned for the 2018season. Prior to fabrication of the final LF detector array we designed and characterized prototype TES bolometers.
Detector geometries in these prototypes are varied in order to inform and optimize the bolometer designs for the LF
array, which requires significantly lower noise levels and saturation powers than the higher frequency detectors. Here
we present the design and characterization of the first LF prototype detectors for AdvACT, including measurementsof the saturation power, critical temperature, thermal conductance, time constants and noise properties. We also
describe the modifications to the time-division SQUID readout architecture compared to the MF and HF arrays.
category : Applications311

PE-6 POLARBEAR-2: Development of a receiver system for CMB measurements
Haruki Nishino1 , POLARBEAR Collaboration2
1

KEK, 2 POLARBEAR Collaboration

POLARBEAR-2 is a newly developed receiver system for improving the measurement of Cosmic Microwave Background (CMB) polarization, in particular odd-parity pattern called B-mode, to achieve both the detection of degreescale inflationary signatures and the precise measurement of gravitational lensing eﬀects induced by the cosmologicallarge-scale structure observed in sub-degree angular scales. This receiver system is planned to be installed on the
Simons Array experiment in the Atacama desert in Chile. The 365mm-diameter focal plane of the receiver is cooled
to 0.27 K by a three-stage Helium sorption refrigerator and will have 7600 dichroic super-conducting transition-edge
sensor (TES) bolometers with the broadband antennas. We plan to start deploying the first POLARBEAR-2 receiver,√which is sensitive to 90 and 150 GHz, in Chile in 2017. The expected array sensitivity of POLARBEAR-2 is 4.1 µK s.
The initial Simons Array sensitivity with three-year observation using the first POLARBEAR-2 receiver is expectedto achieve significantly better sensitivities on the measurement of the inflationary B-mode (sigma(r: tensor-to-scalarratio)=0.01) and the gravitational lensing B-mode (resulting in 90 meV (1-sigma) for the sum of neutrino mass) thanthe current limits. Before the deployment in Chile, we are performing the end-to-end tests of the first receiver in ourlaboratory to characterize the integrated performances of the instruments with the observation quality optics, readout
hardware, detectors, and cryogenics, using various types of calibration equipment. In this talk, we report the current
status of the end-to-end test and initial characterization results of the integrated receiver.
category : Applications

312

H. Nishino,1 P. A. R. Ade,2 M. Aguilar,3 Y. Akiba,4, 1 K. Arnold,5 C. Baccigalupi,6 D. Barron,7 D. Beck,8
S. Beckman,9 A. N. Bender,10, 11 F. Bianchini,12 D. Boettger,13 J. Borrill,14, 7 S. Chapman,15 Y. Chinone,9, 16
G. Coppi,17 K. Crowley,5 A. Cukierman,9 R. Dünner,13 M. Dobbs,18 T. Elleflot,5 J. Errard,8 G. Fabbian,19
S. M. Feeney,20 C. Feng,21 G. Fuller,5 N. Galitzki,5 A. Gilbert,18 N. Goeckner-Wald,9 J. Groh,9N. W. Halverson,22, 23, 24 T. Hamada,25, 1 M. Hasegawa,1, 4 M. Hazumi,1, 16, 4, 26 C. A. Hill,9, 27 W. Holzapfel,9L. Howe,5 Y. Inoue,28, 1 G. Jaehnig,22, 24 A. Ja↵e,29 O. Jeong,9 D. Kaneko,16 N. Katayama,16 B. Keating,5
R. Keskitalo,14, 7 T. Kisner,14, 7 N. Krachmalnico↵,6 A. Kusaka,27, 30 M. Le Jeune,8 A. T. Lee,9, 27, 31 D. Leon,5
E. Linder,27, 7 L. Lowry,5 A. Madurowicz,9, 27 D. Mak,29 F. Matsuda,5 A. May,17 N. J. Miller,32 Y. Minami,1J. Montgomery,18 M. Navaroli,5 J. Peloton,33 A. Pham,12 L. Piccirillo,17 D. Plambeck,31 D. Poletti,6G. Puglisi,6 C. Raum,9 G. Rebeiz,5 C. L. Reichardt,12 P. L. Richards,9 H. Roberts,22, 23 C. Ross,15
K. M. Rotermund,15 Y. Segawa,4, 1 B. Sherwin,34, 35, 27 M. Silva-Feaver,5 P. Siritanasak,5 R. Stompor,8
A. Suzuki,9, 31 O. Tajima,1, 4 S. Takakura,36, 1 S. Takatori,4, 1 D. Tanabe,4, 1 R. Tat,9, 27 G. P. Teply,5
A. Tikhomirov,15 T. Tomaru,1 C. Tsai,5 B. Westbrook,9 N. Whitehorn,9 A. Zahn,5 and T. de Haan27(The POLARBEAR Collaboration)
1

High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
School of Physics and Astronomy, Cardi↵ University, Cardi↵ CF10 3XQ, United Kingdom
Departamento de Fı́sica, FCFM, Universidad de Chile, Blanco Encalada 2008, Santiago, Chile
4
The Graduate University for Advanced Studies (SOKENDAI),
Miura District, Kanagawa 240-0115, Hayama, Japan
5
Department of Physics, University of California, San Diego, CA 92093-0424, USA
6International School for Advanced Studies (SISSA), Via Bonomea 265, 34136, Trieste, Italy
7
Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
8
AstroParticule et Cosmologie (APC), Univ Paris Diderot,
CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
9
Department of Physics, University of California, Berkeley, CA 94720, USA
10
Argonne National Laboratory, High-Energy Physics Division,
9700 S. Cass Avenue, Argonne, IL, USA 60439
11
Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
12
School of Physics, University of Melbourne, Parkville, VIC 3010, Australia
13
Instituto de Astrofı́sica and Centro de Astro-Ingenierı́a,
Facultad de Fı́sica, Pontificia Universidad Católica de Chile,
Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
14
Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
15
Department of Physics and Atmospheric Science,
Dalhousie University, Halifax, NS, B3H 4R2, Canada
16
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,
WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
17
The University of Manchester, Manchester M13 9PL, United Kingdom
18
Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
19Institut d’Astrophysique Spatiale, CNRS (UMR 8617), Univ. Paris-Sud,
Université Paris-Saclay, bât. 121, 91405 Orsay, France
20
Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, New York, NY 10010, USA
21
Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, USA
22
Center for Astrophysics and Space Astronomy,
University of Colorado, Boulder, CO 80309, USA
23
Department of Astrophysical and Planetary Sciences,
University of Colorado, Boulder, CO 80309, USA
24
Department of Physics, University of Colorado, Boulder, CO 80309, USA
25
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, 980-8578, Japan
26
Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 252-0222, Japan27
Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
28
Institute of Physics, Academia Sinica, 128, Sec.2, Academia Road, Nankang, Taiwan
29
Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
30
Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
31
Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA
32
Observational Cosmology Laboratory, Code 665,
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
33
Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK
34
DAMTP, University of Cambridge, Cambridge CB3 0WA, UK
35
Kavli Institute for Cosmology Cambridge, Cambridge CB3 OHA, UK
2

3

36

Osaka University, Toyonaka, Osaka 560-0043, Japan

313

2

PE-7 LiteBIRD: a satellite for the study of B-mode polarization and inflation fromcosmic microwave background radiation detection
Masashi Hazumi1 , LiteBIRD collaboration
1

Institute of Particle and Nuclear Studies (IPNS), High Energy Accelerator Research Organization (KEK,

LiteBIRD is a candidate for JAXA s strategic large mission to map the polarization of the cosmic microwave background (CMB) radiation over the full sky at large angular scales with unprecedented precision. It is currently inthe stage of concept design (Phase-A) at ISAS/JAXA. A global joint study group has been formed with researchers
from Japan, U.S., Canada and Europe. We plan a launch in mid 2020 s with a H3 rocket of JAXA for three-year
observations at a Lagrangian point L2. Cosmological inflation is the leading hypothesis to resolve the problems in the
Big Bang theory. It predicts that primordial gravitational waves were created during the inflationary era, which thenimprinted large-scale curl patterns in the CMB polarization map, called the B-modes. Measurements of the CMB
B-mode signals are known as the best probe to detect the primordial gravitational waves. The scientific objective of
LiteBIRD is to test well-motivated inflation models that satisfy single-field slow-roll conditions and lie in the large-fieldregime. The power of the B-mode is proportional to the cosmological parameter tensor-to-scalar, r. The requirementfor LiteBIRD is to measure r with the precision of δr < 0.001, which will oﬀer us a crucial test of cosmic inflation.
The required angular coverage is 2 ≥ ℓ ≥ 200, where ℓ is the multipole moment. LiteBIRD is also expected to produce
various scientific results in cosmology and astronomy. The design and operation of the LiteBIRD system are driven
by the requirements mentioned above. A 3-year full sky survey will be carried out for 15 frequency bands between 40
and 400 GHz to achieve the total sensitivity of 2.5 µK with a typical angular resolution of ∼30 at 150 GHz. The
key components of the mission payload include a half-wave plate system for polarization signal modulation, a lowfrequency telescope with two reflective mirrors with an aperture of ∼40 cm, a high-frequency refractive telescope with
an aperture of ∼20 cm, an array of polarization-sensitive multi-chroic TES bolometers read out with high multiplexing
factors in the frequency domain, and the cryogenic system to provide the 100 mK base temperature.
category : Applications

314

M. Hazumi,19, 30, 50, 22 P. A. R. Ade,48 Y. Akiba,50, 19 D. Alonso,42 K. Arnold,16 J. Aumont,20 C. Baccigalupi,25 D.
Barron,49 S. Basak,11, 25 J. Borrill,6, 49 F. Boulanger,20 M. Bucher,3 E. Calabrese,48 Y. Chinone,15, 30 S. Cho,13 B.
Crill,26 A. Cukierman,15 D. W. Curtis,49 T. de Haan,44 M. Dobbs,43 A. Dominjon,35 T. Dotani,22 L. Duband,18 A.
Ducout,30 J. Dunkley,10, 42 J. M. Duval,18 T. Elleflot,16 H. K. Eriksen,24 J. Errard,3 J. Fischer,49 T. Fujino,54 T.
Funaki,12 U. Fuskeland,24 K. Ganga,3 N. Goeckner-Wald,15 J. Grain,20 N. W. Halverson,4, 9, 17 T. Hamada,2, 19 T.
Hasebe,35 M. Hasegawa,19, 50 K. Hattori,37 M. Hattori,2 L. Hayes,49 N. Hidehira,12 C. A. Hill,15, 44 G. Hilton,39 J.
Hubmayr,39 K. Ichiki,32 T. Iida,30 H. Imada,22 M. Inoue,40 Y. Inoue,21, 19 K. D. Irwin,13, 29 H. Ishino,12 O. Jeong,15
H. Kanai,54 D. Kaneko,30 S. Kashima,35 N. Katayama,30 T. Kawasaki,31 S. A. Kernasovskiy,13 R. Keskitalo,6, 49 A.
Kibayashi,12 Y. Kida,12 K. Kimura,40 T. Kisner,6, 49 K. Kohri,19 E. Komatsu,34 K. Komatsu,12 C. L. Kuo,13, 29 N.
A. Kurinsky,13, 29 A. Kusaka,44, 14 A. Lazarian,53 A. T. Lee,15, 44, 45 D. Li,13 E. Linder,44, 49 B. Maﬀei,20 A.
Mangilli,20 M. Maki,19 T. Matsumura,30 S. Matsuura,27 D. Meilhan,49 S. Mima,46 Y. Minami,19 K. Mitsuda,22 L.
Montier,5 M. Nagai,35 T. Nagasaki,19 R. Nagata,19 M. Nakajima,40 S. Nakamura,54 T. Namikawa,13 M.
Naruse,47 H. Nishino,19 T. Nitta,52 T. Noguchi,35 H. Ogawa,40 S. Oguri,46 N. Okada,23 A. Okamoto,23 T.
Okamura,19 C. Otani,46 G. Patanchon,3 G. Pisano,48 G. Rebeiz,16 M. Remazeilles,51 P. L. Richards,15 S.
Sakai,22 Y. Sakurai,30 Y. Sato,23 N. Sato,19 M. Sawada,1 Y. Segawa,50, 19 Y. Sekimoto,35, 8, 50 U. Seljak,15 B. D.
Sherwin,7, 28, 44 T. Shimizu,8 K. Shinozaki,23 R. Stompor,3 H. Sugai,30 H. Sugita,23 A. Suzuki,15, 45 J. Suzuki,19 O.
Tajima,19, 50 S. Takada,36 R. Takaku,54 S. Takakura,41, 19 S. Takatori,50, 19 D. Tanabe,50, 19 E. Taylor,49 K. L.
Thompson,13, 29 B. Thorne,42, 30 T. Tomaru,19 T. Tomida,22 N. Tomita,1 M. Tristram,33 C. Tucker,16 P. Turin,49 M.
Tsujimoto,22 S. Uozumi,12 S. Utsunomiya,30 Y. Uzawa,38 F. Vansyngel,20 I. K. Wehus,24 B. Westbrook,15 M.
Willer,49 N. Whitehorn,15 Y. Yamada,12 R. Yamamoto,22 N. Yamasaki,22 T. Yamashita,54 and M. Yoshida19(The LiteBIRD Joint Study Group)
1
Aoyama Gakuin University, Sagamihara, Kanagawa 252-5258, Japan
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, 980-8578, Japan
3
AstroParticule et Cosmologie (APC), Univ Paris Diderot,
CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
4
Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA
5
CNRS, IRAP, F-31028 Toulouse cedex 4, France
6
Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
7
DAMTP, University of Cambridge, Cambridge CB3 0WA, UK
8
Department of Astronomy, The University of Tokyo, Tokyo 113-0033, Japan
9
Department of Astrophysical and Planetary Sciences,
University of Colorado, Boulder, CO 80309, USA
10
Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
11
Department of Physics, Amrita University, Kerala 690525 India
12
Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
13
Department of Physics, Stanford University, Stanford, CA 94305-4060, USA
14
Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
15
Department of Physics, University of California, Berkeley, CA 94720, USA
16
Department of Physics, University of California, San Diego, CA 92093-0424, USA
17
Department of Physics, University of Colorado, Boulder, CO 80309, USA
18
French Alternative Energies and Atomic Energy Commission (CEA), Grenoble, France
19
High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
20
Institut d’Astrophysique Spatiale (IAS), CNRS, UMR 8617,
Université Paris-Sud 11, Bâtiment 121, 91405 Orsay, France
21
Institute of Physics, Academia Sinica, 128, Sec.2, Academia Road, Nankang, Taiwan
22
Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 252-0222, Japan
23
Research and Development Directorate, Japan Aerospace Exploration Agency (JAXA), Tsukuba, Ibaraki 305-8505, Japan
24
Institute of Theoretical Astrophysics, University of Oslo, NO-0315 Oslo, Norway
25
International School for Advanced Studies (SISSA), Via Bonomea 265, 34136, Trieste, Italy
26
Jet Propulsion Laboratory, Pasadena, CA 91109, USA
27
Kansei Gakuin University, Nishinomiya, Hyogo 662-8501, Japan
28
Kavli Institute for Cosmology Cambridge, Cambridge CB3 OHA, UK
29
Kavli Institute for Particle Astrophysics and Cosmology (KIPAC),SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
30
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,
WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
31
Kitazato University, Sagamihara, Kanagawa 252-0373, Japan
2

315

2
32

Kobayashi-Maskawa Institute for the Origin of Particle and the Universe,
Nagoya University, Nagoya, Aichi 464-8602, Japan
33
Laboratoire de l’Accélérateur Linéaire (LAL), Univ. Paris-Sud,
CNRS/IN2P3, Université Paris-Saclay, Orsay, France
34
Max-Planck-Institut for Astrophysics, D-85741 Garching, Germany
35
National Astronomical Observatory of Japan (NAOJ), Mitaka, Tokyo 181-8588, Japan36
National Institute for Fusion Science (NIFS), Toki, Gifu 509-5202, Japan37
National Institute of Advanced Industrial Science and Technology (AIST), Tsukuba, Ibaraki 305-8563, Japan38
National Institute of Information and Communications Technology (NICT), Kobe, Hyogo 651-2492, Japan
39
National Institute of Standards and Technology (NIST), Boulder, Colorado 80305, USA
40
Osaka Prefecture University, Sakai, Osaka 599-8531, Japan
41
Osaka University, Toyonaka, Osaka 560-0043, Japan
42
Oxford Astrophysics, Oxford, OX1 3RH, United Kingdom
43
Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
44
Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
45
Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA
46
RIKEN, Wako, Saitama 351-0198, Japan47
Saitama University, Saitama, Saitama 338-8570, Japan48
School of Physics and Astronomy, Cardiﬀ University, Cardiﬀ CF10 3XQ, United Kingdom
49
Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
50
The Graduate University for Advanced Studies (SOKENDAI),
Miura District, Kanagawa 240-0115, Hayama, Japan
51
The University of Manchester, Manchester M13 9PL, United Kingdom
52
Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, Ibaraki 305-8571, Japan
53
University of Wisconsin-Madison, Madison, Wisconsin 53706, USA
54
Yokohama National University, Yokohama, Kanagawa 240-8501, Japan

316

PE-8 The POLARBEAR and Simons Array Cosmic Microwave BackgroundExperiments
Adrian T. Lee1 , POLARBEAR collaboration
1

Physics Department, University of California, Berkeley,

The POLARBEAR and Simons Array Cosmic Microwave Background experiments are pathfinders in both scienceand low-temperature detector development. POLARBEAR-1 has used a 1,274 detector antenna-coupled TES array tomake a 5 sigma detection of gravitational lensing of the polarized CMB, set an upper limit of 3.9 nG on a primordial
magnetic field, and set an upper limit on cosmic birefringence of 93 nG equivalent magnetic field. We will present new
results from an analysis of the first two years of POLARBEAR observations which increase the significance of the thegravitational lensing detection.
POLARBEAR-1 has observed the BICEP/KECK patch using a continuously rotating half-wave plate during thethird and fourth years of observations. This data set will be used to measure degree angular scales to constrain
inflation, and we will present the status of the analysis.
We will also present the development of the three POLARBEAR-2 receivers which will be installed in the Simons
Array. The POLARBEAR-2 receivers will each have focal-plane arrays with two-band Sinuous-Antenna-Coupled TES
bolometers. Two of the receivers will have 95 and 150 GHz bands and one will have 220 and 280 GHz bands. Each
receiver will have 7,588 bolometers, and the Simons Array will have a total of 22,764 detectors. The detectors will bereadout with a 40x Frequency-Domain Multiplexer (FDM). We will report on the construction status of the experimentand give science forecasts for an inflation search and a measurement of the sum of neutrino masses and the eﬀective
number of relativistic species in the early universe.
category : Applications

317

A. T. Lee,1, 2, 3 P. A. R. Ade,4 M. Aguilar,5 Y. Akiba,6, 7 K. Arnold,8 C. Baccigalupi,9 D. Barron,10
D. Beck,11 S. Beckman,1 A. N. Bender,12, 13 F. Bianchini,14 D. Boettger,15 J. Borrill,16, 10 S. Chapman,17
Y. Chinone,1, 18 G. Coppi,19 K. Crowley,8 A. Cukierman,1 R. Dünner,15 M. Dobbs,20 T. Elleflot,8 J. Errard,11
G. Fabbian,21 S. M. Feeney,22 C. Feng,23 G. Fuller,8 N. Galitzki,8 A. Gilbert,20 N. Goeckner-Wald,1J. Groh,1 N. W. Halverson,24, 25, 26 T. Hamada,27, 7 M. Hasegawa,7, 6 M. Hazumi,7, 18, 6, 28 C. A. Hill,1, 2
W. Holzapfel,1 L. Howe,8 Y. Inoue,29, 7 G. Jaehnig,24, 26 A. Ja↵e,30 O. Jeong,1 D. Kaneko,18 N. Katayama,18
B. Keating,8 R. Keskitalo,16, 10 T. Kisner,16, 10 N. Krachmalnico↵,9 A. Kusaka,2, 31 M. Le Jeune,11 D. Leon,8
E. Linder,2, 10 L. Lowry,8 A. Madurowicz,1, 2 D. Mak,30 F. Matsuda,8 A. May,19 N. J. Miller,32 Y. Minami,7J. Montgomery,20 M. Navaroli,8 H. Nishino,7 J. Peloton,33 A. Pham,14 L. Piccirillo,19 D. Plambeck,3 D. Poletti,9G. Puglisi,9 C. Raum,1 G. Rebeiz,8 C. L. Reichardt,14 P. L. Richards,1 H. Roberts,24, 25 C. Ross,17
K. M. Rotermund,17 Y. Segawa,6, 7 B. Sherwin,34, 35, 2 M. Silva-Feaver,8 P. Siritanasak,8 R. Stompor,11
A. Suzuki,1, 3 O. Tajima,7, 6 S. Takakura,36, 7 S. Takatori,6, 7 D. Tanabe,6, 7 R. Tat,1, 2 G. P. Teply,8A. Tikhomirov,17 T. Tomaru,7 C. Tsai,8 B. Westbrook,1 N. Whitehorn,1 A. Zahn,8 and T. de Haan2(The POLARBEAR Collaboration)
1
Department of Physics, University of California, Berkeley, CA 94720, USA
Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
3
Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA
4
School of Physics and Astronomy, Cardi↵ University, Cardi↵ CF10 3XQ, United Kingdom
5Departamento de Fı́sica, FCFM, Universidad de Chile, Blanco Encalada 2008, Santiago, Chile
6
The Graduate University for Advanced Studies (SOKENDAI),
Miura District, Kanagawa 240-0115, Hayama, Japan
7
High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
8
Department of Physics, University of California, San Diego, CA 92093-0424, USA
9International School for Advanced Studies (SISSA), Via Bonomea 265, 34136, Trieste, Italy
10Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
11
AstroParticule et Cosmologie (APC), Univ Paris Diderot,
CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
12
Argonne National Laboratory, High-Energy Physics Division,
9700 S. Cass Avenue, Argonne, IL, USA 60439
13
Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
14
School of Physics, University of Melbourne, Parkville, VIC 3010, Australia
15
Instituto de Astrofı́sica and Centro de Astro-Ingenierı́a,
Facultad de Fı́sica, Pontificia Universidad Católica de Chile,
Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
16
Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
17
Department of Physics and Atmospheric Science,
Dalhousie University, Halifax, NS, B3H 4R2, Canada
18
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,
WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
19
The University of Manchester, Manchester M13 9PL, United Kingdom
20
Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
21
Institut d’Astrophysique Spatiale, CNRS (UMR 8617), Univ. Paris-Sud,
Université Paris-Saclay, bât. 121, 91405 Orsay, France
22
Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, New York, NY 10010, USA
23
Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, USA
24
Center for Astrophysics and Space Astronomy,
University of Colorado, Boulder, CO 80309, USA
25
Department of Astrophysical and Planetary Sciences,
University of Colorado, Boulder, CO 80309, USA
26
Department of Physics, University of Colorado, Boulder, CO 80309, USA
27
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, 980-8578, Japan
28
Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 252-0222, Japan
29
Institute of Physics, Academia Sinica, 128, Sec.2, Academia Road, Nankang, Taiwan
30
Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
31
Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
32
Observational Cosmology Laboratory, Code 665,
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
33
Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK
34
DAMTP, University of Cambridge, Cambridge CB3 0WA, UK
35
Kavli Institute for Cosmology Cambridge, Cambridge CB3 OHA, UK
36
2Osaka University, Toyonaka, Osaka 560-0043, Japan

318

2

PE-9 Simons Observatory: Next Generation Telescopes Featuring Large Detector
Arrays for Observations of the Cosmic Microwave BackgroundJeﬀ McMahon1
1

University of Michigan, dept. of physics

The Simons Observatory is a next generation observatory comprised of large and small telescopes optimized to makeprecise measurements of the comic microwave background (CMB) over frequencies spanning 30-300 GHz. These data
will be used to detect or place stringent limits on gravitational waves from inflation, new light relativistic species,
neutrino properties, and to make many other astrophysical and cosmological measurements. The SO instrument will
pave the way for CMB-S4 which will field hundreds of thousands of CMB detectors across multiple plaftorms. Here we
present an overview of the SO large and small telescopes, the cryogenic receivers, cold optical elements, and our planfor fielding and reading out tens of thousands of multichroic, superconducting detectors on the SO large and small
telescopes.
category : Applications319

PE-10 Design and Performance of the SPT3G First-year Focal Plane
Wendeline Bray Everett1 , SPT3G Collaboration2
1

University of Colorado at Boulder, Center for Astrophysics and Space Astronomy, 2 University of Colorado at Boulder, Center
for Astrophysics and Space Astronomy

During the austral summer of 2016-7, the third-generation camera, SPT3G, was installed on the South Pole Telescope,increasing the number of detectors in the focal plane by an order of magnitude relative to the previous generation.
Designed to map polarization of the Cosmic Microwave Background, SPT3G utilizes ten 6 -hexagonal modules ofdetectors, each with 271 trichroic and polarization-sensitive pixels coupled to the sky using broadband sinuous antennaeand hemispherical alumina lenslets. Each pixel contains six transition-edge-sensor (TES) bolometers, which are readout using 64x frequency-domain multiplexing (fMUX). Here we will discuss design and assembly of the detector
modules, as well as the layout of the first-year focal plane. We ll also discuss early performance characterizationof the full array, including yield and detector properties across the array: TES properties of transition temperature,normal resistance, saturation powers, and loopgain, and readout properties such as stray resistance and stability.
category : Applications320PE-11 Design, Characterization, and Assembly of the POLARBEAR-2A Cryogenic
Readout System
Tucker Elleflot1 , POLARBEAR collaboration
1

Department of Physics, University of California San Diego

The Simons Array (SA) is a Cosmic Microwave Background (CMB) experiment comprised of three telescopes thataims to characterize the B-mode polarization signal from inflationary gravitational waves and gravitational lensing bylarge scale structure. The first Simons Array instrument, POLARBEAR-2A (PB-2A) will have 7,600 polarization
sensitive Transition Edge Sensor (TES) bolometers mutliplexed and read out by 300 mK channel defining aluminum
LC filters and 4 K SQUID amplifiers. This represents a factor of 6 increase in detector count compared to its
predecessor, POLARBEAR-1 (PB-1). The improved array sensitivity that comes with an increased number ofdetectors is accompanied by the challenge of improving the thermal performance of the readout system. To this end,
we have expanded our carrier frequency range from 1 MHz to 4.5 MHz and increased our multiplexing factor fromeight to forty. The higher multiplexing factor allows us to increase the detector count without dramatically increasing
the thermal load on the detector stage. This also imposes stringent constraints on stray impedances in the biasing
circuit since these can cause bolometer nonlinearity and crosstalk between readout channels. We use a NbTi broadsidecoupled stripline to minimize thermal loading and stray impedance in the wiring between SQUIDs and LC filters.
Here we describe the details of the design, assembly, and characterization of the readout system in the PB-2A receiver
and a dark test cryostat.
category : Applications

321

T. Elleflot,1 P. A. R. Ade,2 M. Aguilar,3 Y. Akiba,4, 5 K. Arnold,1 C. Baccigalupi,6 D. Barron,7 D. Beck,8
S. Beckman,9 A. N. Bender,10, 11 F. Bianchini,12 D. Boettger,13 J. Borrill,14, 7 S. Chapman,15 Y. Chinone,9, 16
G. Coppi,17 K. Crowley,1 A. Cukierman,9 R. Dünner,13 M. Dobbs,18 J. Errard,8 G. Fabbian,19 S. M. Feeney,20
C. Feng,21 G. Fuller,1 N. Galitzki,1 A. Gilbert,18 N. Goeckner-Wald,9 J. Groh,9 N. W. Halverson,22, 23, 24
T. Hamada,25, 5 M. Hasegawa,5, 4 M. Hazumi,5, 16, 4, 26 C. A. Hill,9, 27 W. Holzapfel,9 L. Howe,1 Y. Inoue,28, 5
G. Jaehnig,22, 24 A. Ja↵e,29 O. Jeong,9 D. Kaneko,16 N. Katayama,16 B. Keating,1 R. Keskitalo,14, 7 T. Kisner,14, 7
N. Krachmalnico↵,6 A. Kusaka,27, 30 M. Le Jeune,8 A. T. Lee,9, 27, 31 D. Leon,1 E. Linder,27, 7 L. Lowry,1
A. Madurowicz,9, 27 D. Mak,29 F. Matsuda,1 A. May,17 N. J. Miller,32 Y. Minami,5 J. Montgomery,18
M. Navaroli,1 H. Nishino,5 J. Peloton,33 A. Pham,12 L. Piccirillo,17 D. Plambeck,31 D. Poletti,6G. Puglisi,6 C. Raum,9 G. Rebeiz,1 C. L. Reichardt,12 P. L. Richards,9 H. Roberts,22, 23 C. Ross,15
K. M. Rotermund,15 Y. Segawa,4, 5 B. Sherwin,34, 35, 27 M. Silva-Feaver,1 P. Siritanasak,1 R. Stompor,8
A. Suzuki,9, 31 O. Tajima,5, 4 S. Takakura,36, 5 S. Takatori,4, 5 D. Tanabe,4, 5 R. Tat,9, 27 G. P. Teply,1
A. Tikhomirov,15 T. Tomaru,5 C. Tsai,1 B. Westbrook,9 N. Whitehorn,9 A. Zahn,1 and T. de Haan27(The POLARBEAR Collaboration)
1
Department of Physics, University of California, San Diego, CA 92093-0424, USA
School of Physics and Astronomy, Cardi↵ University, Cardi↵ CF10 3XQ, United Kingdom
3
Departamento de Fı́sica, FCFM, Universidad de Chile, Blanco Encalada 2008, Santiago, Chile
4
The Graduate University for Advanced Studies (SOKENDAI),
Miura District, Kanagawa 240-0115, Hayama, Japan
5
High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
6
International School for Advanced Studies (SISSA), Via Bonomea 265, 34136, Trieste, Italy
7
Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
8
AstroParticule et Cosmologie (APC), Univ Paris Diderot,
CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
9
Department of Physics, University of California, Berkeley, CA 94720, USA
10
Argonne National Laboratory, High-Energy Physics Division,
9700 S. Cass Avenue, Argonne, IL, USA 60439
11
Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637
12
School of Physics, University of Melbourne, Parkville, VIC 3010, Australia
13
Instituto de Astrofı́sica and Centro de Astro-Ingenierı́a,
Facultad de Fı́sica, Pontificia Universidad Católica de Chile,
Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
14
Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
15
Department of Physics and Atmospheric Science,
Dalhousie University, Halifax, NS, B3H 4R2, Canada
16
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,
WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
17
The University of Manchester, Manchester M13 9PL, United Kingdom
18
Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
19Institut d’Astrophysique Spatiale, CNRS (UMR 8617), Univ. Paris-Sud,
Université Paris-Saclay, bât. 121, 91405 Orsay, France
20
Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, New York, NY 10010, USA
21
Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, USA
22
Center for Astrophysics and Space Astronomy,
University of Colorado, Boulder, CO 80309, USA
23
Department of Astrophysical and Planetary Sciences,
University of Colorado, Boulder, CO 80309, USA
24
Department of Physics, University of Colorado, Boulder, CO 80309, USA
25
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, 980-8578, Japan
26
Institute of Space and Astronautical Science (ISAS),
Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 252-0222, Japan27
Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
28
Institute of Physics, Academia Sinica, 128, Sec.2, Academia Road, Nankang, Taiwan
29
Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
30
Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
31
Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA
32
Observational Cosmology Laboratory, Code 665,
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
33
Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK
34
DAMTP, University of Cambridge, Cambridge CB3 0WA, UK
35
Kavli Institute for Cosmology Cambridge, Cambridge CB3 OHA, UK
36
Osaka University, Toyonaka, Osaka 560-0043, Japan
2

322

2

PE-12 TC tuning of Titanium thin films for CMB detectors on the SWIPE/LSPE
experiment
D. Vaccaro1, 4 , B. Siri2, 5 , A.M. Baldini1 , M. Biasotti5 , F. Cei1, 3 , V. Ceriale2, 5 , M. de Gerone2 , L. Galli1 , G.
Gallucci2 , F. Gatti2, 5 , M. Grassi1 , D. Grosso2, 5 , D. Nicoló1, 3 , M. Piendibene1 , G. Signorelli1 , and F. Spinella1
1

INFN Sezione di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy, 2 INFN Sezione di Genova, Via Dodecaneso 33, 16146
Genova, Italy, 3 Dipartimento di Fisica, Universitá di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy, 4 Dipartimento di Fisica,
Universitá di Siena, Strada Laterina 8, 53100 Siena, Italy, 5 Dipartimento di Fisica, Universitá di Genova, Via Dodecaneso 33,
16146, Genova, Italy

Cosmic microwave background (CMB) B-mode polarization detection is a major challenge in modern cosmology,
which future experiments are going to undertake either from the ground, on balloons or on satellites. Among these,
the SWIPE/LSPE balloon-borne experiment aims at searching for B-modes exploiting the re-ionization peak at large
angular scales. Detectors in SWIPE are Transition Edge Sensor (TES) spider-web bolometers, with required TC ≃500 mK. We found evidence that temperature control during deposition and post annealing of Titanium thin films
allows the tuning of critical temperature. Titanium is a Type I superconductor with TC ≃ 380 mK. In this paper we
present a systematic study done on thermal treated Titanium films, showing that higher TC can be achieved, in arange suitable for SWIPE.
category : Applications323

PE-13 Development of a Massive, Highly Multiplexible, Phonon-Mediated Particle
Detector using Kinetic Inductance Detectors
Yen-Yung Chang1 , Brett Cornell2 , Taylor Aralis3 , Bruce Bumble4 , Sunil R. Golwala51

3

California Institute of Technology, 2 Division of Physics, Mathematics, & Astronomy, California Institute of Technology ,Division of Physics, Mathematics, & Astronomy, California Institute of Technology , 4 Jet Propulsion Laboraroty , 5 Divisionof Physics, Mathematics, & Astronomy, California Institute of Technology

We present a status update on the development of an phonon-mediated particle detector using Kinetic Inductance
Detectors (KIDs). The design is intended for O(1) kg substrate, using tens to hundreds of KIDs on a single readoutline, to image athermal phonon distribution.
The fine-scale position information provided by the highly multiplexed KIDs, combined with their excellent energy
sensitivity, will provide competitive energy resolution and threshold below 1 keV, as well as precise, robust position
reconstruction. The primary goal is to use the fine-scale position information to make significant gains in defining thesubstrate’s fiducial volume, excluding surfaces and edges that are subject to higher backgrounds and, in the case of
joint detection of ionization production, incomplete ionization collection. In rare-event searches, mis-reconstruction of
the surface event positions and/or incomplete ionization collection can be the dominant background.
Prior work successfully demonstrated the concept on a 20 mm × 22 mm × 1 mm Si substrate with 20 KIDs (Moore
et. al. APL 2012) but met substantial challenges with feedline quality when scaling up to larger substrate. We wereable to overcome it with new feedline design combined with thicker films, resulting in robust feedline characteristics.
We have also developed a new KID design based on improved simulation, and the end product shows much higher
current density uniformity and negligible crosstalk. We will report on the design, fabrication, and performance of
demonstration devices on 76 mm × 1 mm Si substrate, with 40, 80, 140, 256 Nb KIDs, for assessing resonanceplacement accuracy, and with 40 Al KIDs to demonstrate responsivity, noise performance, and particle detection withenergy and position reconstruction.
category : Applications324

PE-14 A NaI-based cryogenic scintillating calorimeter: status and results from thefirst COSINUS prototype detectors
Karoline Schaeﬀner1 , Godehard Angloher2 , Paolo Carniti3 , Lorenzo Cassina4 , Luca Gironi5 , Claudio Gotti6 , Achim
Guetlein7 , Michele Mancuso8 , Lorenzo Pagnanini9 , Gianluigi Pessina10 , Federica Petricca11 , Stefano Pirro12 , Rafael
Puig13 , Franz Proebst14 , Florian Reindl15 , Jochen Schieck16 , Wolfgang Seidel17
1

GSSI - Gran Sasso Science Institute, 2 Max-Planck-Institute for Physics , 3 INFN - Sezione die Milano Bicocca , 4 INFN Sezione die Milano Bicocca , 5 INFN - Sezione die Milano Bicocca / Universita’ Milano Bicocca , 6 INFN - Sezione die Milano
Bicocca , 7 HEPHY / Vienna University of Technology , 8 Max-Planck-Institute for Physics , 9 GSSI - Gran Sasso Science
Institute , 10 INFN - Sezione die Milano Bicocca , 11 Max-Planck-Institute for Physics , 12 INFN - Laboratory Nazionali delGran Sasso , 13 HEPHY / Vienna University of Technology , 14 Max-Planck-Institute for Physics , 15 INFN - Sezione di Roma ,16
HEPHY / Vienna University of Technology , 17 Max-Planck-Institute for Physics

The COSINUS (Cryogenic Observatory for SIgnals seen in Next-generation Underground Searches) project aims toprovide a model independent cross-check of the long-standing DAMA/LIBRA claim on the observation of dark matterby using the same target material, but in a diﬀerent experimental approach.
Operating undoped sodium iodide (NaI) scintillating crystals as low temperature scintillating calorimeters has thedistinguished advantage of providing a lower energy threshold for nuclear recoil events as expected from dark matterparticle interactions combined with particle discrimination. Infact, the dual read-out of phonon and light allows us
to provide background rejection on an event-by-event basis, a unique feature in comparison to other NaI-based dark
matter searches.
In this talk we will discuss in detail the COSINUS detector concept and present the results and performanceparameters from our first prototype measurements.
category : Applications

325

PE-15 The DM Radio: Searching for Ultra-Light-Field Dark Matter
Arran Phipps1 , S. Chaudhuri2 , S. Kuenstner3 , C. Dawson4 , H.-M. Cho5 , D. Li6 , H. Moseley7 , B.A. Young8 , S.
Rajendran9 , J. Mardon10 , L. Page11 , J.A. Tyson12 , B. Godfrey13 , S. Hillbrand14 , P.W. Graham15 , K.D. Irwin16
1

Department of Physics, Stanford University, 2 Stanford University , 3 Stanford University , 4 Santa Clara University ,Stanford University / SLAC National Accelerator Laboratory , 6 Stanford University / SLAC National Accelerator
Laboratory , 7 NASA Goddard Space Flight Center , 8 Santa Clara University , 9 University of California, Berkeley , 10 Stanford
University , 11 Princeton University , 12 University of California, Davis , 13 University of California, Davis , 14 University ofCalifornia, Davis , 15 Stanford University , 16 Stanford University / SLAC National Accelerator Laboratory
5

The Dark Matter Radio (DM Radio) is a sensitive search for sub-eV axion and hidden photon dark matter over a widemass range. While Weakly Interacting Massive Particles (WIMPs) have been the primary focus of direct detection forseveral decades, there has been growing interest in searching for ultra-light-field candidates such as the hidden photon(spin 1 boson) and axion (spin 0 boson). DM Radio uses a superconducting, tunable lumped-element LC resonatorwith SQUID-based readout. The DM Radio Pathfinder is now in operation, and the DM Radio program has been
funded for Stage 2, in which it will set important new limits on hidden photon and axion dark matter. In this talk, I
will discuss the motivation, detection strategy, status, and prospects for the DM Radio experiment and show the dark
matter phase space that DM Radio will search over the next several years.
category : Applications326

PE-16 Directional sensitivity in single-electron resolution phonon-mediated detectors
Fedja Kadribasic1 , Nader Mirabolfathi2 , Kai Nordlund3 , Eero Holmstrom4 , Flyura Djurabekova51

Department of Physics, Texas A&M University, 2 Department of Physics and Astronomy, Texas A&M University , 3 Helsinki
Institute of Physics and Department of Physics, University of Helsinki , 4 Helsinki Institute of Physics and Department of
Physics, University of Helsinki , 5 Helsinki Institute of Physics and Department of Physics, University of Helsinki

A large body of astrophysical observations indicate that around 85 percent of the matter in the universe is not madeof recognized standard model particles. Understanding the nature of this so-called dark matter is of fundamental
importance to cosmology, astrophysics, and high energy particle physics. We present a method for using solid state
detectors with directional sensitivity to dark matter interactions to detect low-mass Weakly Interacting Massive
Particles (WIMPs), the main dark matter candidate, originating from galactic sources. In spite of a plethora ofliterature for high-mass WIMP detectors with directional sensitivity, there is no available technique to cover WIMPs
in the mass range ¡1 GeV/c2 . We make the reasonable assumption that single electron-hole pair creation is caused
by defect formation, which is in sharp contrast to the well-established, but physically incorrect, Lindhard model atenergies below about 100 eV. We examine commonly used semiconductor material response to these low-mass WIMP
interactions using numerical simulations of classical interatomic potentials in these materials. These simulations,backed up by more precise density functional theory simulations and experiments, predict an angular dependence inthe defect formation energy threshold that varies by around 20 eV from minimum to maximum. Experiments suchas the Cryogenic Dark Matter Search (CDMS) and the Mitchell Institute Neutrino Experiment at Reactor (MINER)
are actively developing detectors to reach the resolutions necessary to observe this eﬀect. Once these detectors arecalibrated at these low recoil energies, we argue that the anisotropy in defect formation in single-electron resolution
semiconductor detectors allows for very eﬀective directional sensitivity to dark matter signals for masses below 1
GeV/c2 .
category : Applications327

PE-17 Solid xenon bolometers for anti-correlation studies
Michelle Jean Dolinski1 , Erin V. Hansen2
1

Department of Physics, Drexel University, 2 Drexel University

Cryogenic liquid xenon detectors have become a popular technology in the search for rare events, such as dark
matter interactions and neutrinoless double beta decay. The power of the liquid xenon detector technology is in
the combination of the ionization and scintillation signals, resulting in particle discrimination and improved energy
resolution over the ionization-only signal. The improved energy resolution results from a strong microscopic anticorrelation phenomenon that has not been described from first principles. Solid xenon bolometers, under development
at Drexel University, would oﬀer an opportunity to study scintillation, ionization, and phonon signals simultaneously.
This additional energy channel may oﬀer the final piece of the puzzle in understanding the microscopic anti-correlation
phenomenon in detector energy response.
category : Applications328

PE-18 The MINER Experiment: Coherent Neutrino-Nucleus Scattering
Measurement With Cryogenic Semiconductor Detectors
Andrew Jastram1
1

Department of Physics and Astronomy, Texas A&M University

The proposed Mitchell Institute Neutrino Experiment at Reactor (MINER) experiment at the Nuclear Science Centerat Texas A/&M University will search for coherent elastic neutrino-nucleus scattering within close proximity (about
2 m) of a 1 MW TRIGA nuclear reactor core using low threshold, cryogenic germanium and silicon detectors. Given
the Standard Model cross section of the scattering process and the proposed experimental proximity to the reactor,
as many as 5?20 events/kg/day are expected. We discuss the status of preliminary measurements to characterize themain backgrounds for the proposed experiment. Both in situ measurements at the experimental site and simulations
using the MCNP and GEANT4 codes are described. A strategy for monitoring backgrounds during data taking isbriefly discussed.
category : Applications329

PE-19 A Systematic Study of the Theoretical Calorimetric Electron Capture
Spectrum
Katrina E. Koehler1 , Mark P. Croce2 , Christopher J. Fontes3 , Michael W. Rabin4 , Michael A. Famiano5 , Thomas
W. Gorczyca6
1

Los Alamos National Laboratory, 2 Los Alamos National Laboratory , 3 Los Alamos National Laboratory , 4 Los Alamos
National Laboratory , 5 Western Michigan University , 6 Western Michigan University

A high statistics, high resolution calorimetric spectrum of electron capture in 163 Ho yields the neutrino mass provided the degree of fidelity in the atomic description high enough. By systematically assessing the contributions
from increasingly detailed descriptions of the atomic theory, it is possible to determine the statistical requirements
for experimentally measuring each contribution. Given a theoretical description of high enough fidelity, additional
components will be unmeasurable even in the high-statistics regime of a neutrino mass measurement, indicating thelevel to which a theoretical model must be calculated. We will show this systematic assessment for the calorimetricelectron capture spectrum of 163 Ho.
category : Applications330

PE-20 Updates on the Transition Edge Sensors and multiplexed readout for HOLMES
andrei puiu1 , Dan Becker2 , Douglas Bennet3 , Valentina Ceriale4 , Matteo De Gerone5 , Marco Faverzani6 , Elena
Ferri7 , joseph fowler8 , john gard9 , andrea giachero10 , james hays-wehle11 , gene hilton12 , biasotti michele13 , johnmates14 , angelo nucciotti15 , angiola orlando16 , gianluigi pessina17 , dan schmidt18 , dan swetz19 , joel ullom20 , bradleyalpert21 , carl reintsema22
1

Universita and INFN Milano-Bicocca, 2 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA ,3
National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 4 INFN Genova , 5 INFN Genova ,6
Universita Milano-Bicocca and INFN Milano-Bicocca , 7 INFN Milano Bicocca , 8 National Institute of Standards andTechnology (NIST), Boulder, Colorado, USA , 9 National Institute of Standards and Technology (NIST), Boulder, Colorado,
USA , 10 INFN Milano Bicocca , 11 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA ,12
National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 13 INFN Genova , 14 National Institute ofStandards and Technology (NIST), Boulder, Colorado, USA , 15 Universita Milano-Bicocca and INFN Milano-Bicocca ,16
INFN Milano Bicocca , 17 INFN Milano Bicocca , 18 National Institute of Standards and Technology (NIST), Boulder,
Colorado, USA , 19 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA , 20 National Institute ofStandards and Technology (NIST), Boulder, Colorado, USA , 21 National Institute of Standards and Technology (NIST),
Boulder, Colorado, USA , 22 National Institute of Standards and Technology (NIST), Boulder, Colorado, USA

Measuring the neutrino mass is one the most compelling issues in particle physics. HOLMES is an experiment for a
direct measurement of neutrino mass. HOLMES will perform a precise measurement of the end point of the Electron
Capture decay spectrum of 163 Ho in order to extract information on neutrinomass with a sensitivity as low as 1 eV.
HOLMES, in its final configuration will deploy a 1000 pixel array of low temperature microcalorimeters: eachcalorimeter is made of an absorber, where the Ho atoms will be implanted, coupled to a Transition Edge Sensor
thermometer.
The detectors will be kept at the working temperature of 70 mK in a dilution refrigerator. In order to easily readout the 1000 detectors array of HOLMES, a multiplexing system is necessary: the choice is to couple the Transition
Edge Sensors to a multiplexed rf-SQUID. The rf-SQUIDs are operated in flux ramp modulation
for linearisation purpouses. The rf-SQUID is then coupled to a superconducting quarter wavelength LC resonatorin the GHz range, from which the modulated signal is finally recovered using the homodyne technique.
In this contribution we outline the progress made towards the final configuration of HOLMES regarding both theperformances of the TES detectors and the characteristics of the multiplexing system. We reached the target timeand energy resolution and we are about to finalise the detector array design before starting to
implant Ho in the absorbers. By the end of 2017 we plan to start measuring the first 64 detectors array withimplanted 163 Ho. From this first measurements crucial information will be extracted, such as the importance of
shake-up and shake-oﬀ second order processes, which need to be taken into account in the calculation of
the theoretical spectral shape used for the evaluation of the neutrino mass. With 64 active detectors, a two monthlong exposure time will allow us to set a limit of 7 eV on the neutrino mass.
category : Applications

331

PE-21

193

Pt Electron Capture Spectra with Microcalorimeters

Katrina E. Koehler1 , Mark P. Croce2 , Christopher J. Fontes3 , Michael W. Rabin4 , Michael A. Famiano5 , Thomas A.
Gorczyca6
1

Los Alamos National Laboratory, 2 Los Alamos National Laboratory , 3 Los Alamos National Laboratory , 4 Los Alamos
National Laboratory , 5 Western Michigan University , 6 Western Michigan University

A neutrino mass can be extracted from a high statistics, high resolution calorimetric spectrum of electron capture in163
Ho. In order to understand the resolution degradation seen in embedded sources as measured by microcalorimeterTransition Edge Sensors, a platinum absorber with embedded 193 Pt was created by irradiating a 192 Pt-enriched
platinum foil in the 6-MW MIT reactor. This absorber provides the opportunity to determine the sample preparationand deposition contributions to resolution degradation. Additionally, the 193 Pt electron capture spectrum provides
another independent check on the theoretical calculation for the electron capture spectrum, which has thus far been
compared only to 163 Ho. Experimental and theoretical spectra from this 193 Pt-in-Pt absorber are presented anddiscussed.
category : Applications332

PE-22 Data processing and analysis for AMoRE-Pilot
I. Kim1,2,3 , S. Choi2 , F.A. Danevich4 , A. Fleischmann5 , J.A. Jeon, H.S. Jo1 , C.S. Kang1 , W.G. Kang1 , G.B. Kim1 ,H.J. Kim6 , H.L. Kim1 , S.K. Kim2 , S.R. Kim1 , Y.H. Kim1,3 , Y.D. Kim1 , V. Kornoukhov7 , D.H. Kwon1 , C. Lee1 , H.J.
Lee1 , M.K. Lee 3, S.H. Lee1 , S.Y. Oh1,3 , J.H. So1 , Y.S. Yoon1
1

Center for Underground Physics, Institute for Basic Science (IBS), Daejeon 34047, Korea 2 Department of Physics andAstronomy, Seoul National University, Seoul 08826, Korea 3 Korea Research Institute of Standards and Science (KRISS),
Daejeon 34113, Korea 4 Institute for Nuclear Research, MSP 03680 Kyiv, Ukraine 5 Kirchhoﬀ-Institute for Physics, D-69120
Heidelberg, Germany 6 Department of Physics, Kyungpook National University, Daegu 41566, Korea 7 Institute of Theoreticaland Experimental Physics, Moscow 117218, Russia

AMoRE (Advanced Mo-based Rare process Experiment) is an international collaboration searching for neutrinolessdouble beta decay (0 νββ) of 100Mo by using 40Ca100MoO4 scintillating crystals equipped with metallic magnetic
calorimeters (MMCs) operating at millikelvin temperatures. AMoRE utilizes the phonon (heat) ? photon (scintillation light) simultaneous-measurement technique to achieve excellent particle discrimination, thus reducing alphabackground events. The pilot phase of the experiment has been running in the 700-m-deep Yangyang undergroundlaboratory in Korea, with about 1.5 kg of 40Ca100MoO4 scintillating crystals at temperatures as low as 10 mK.
We present the techniques used for the data analysis of the AMoRE-Pilot experiment. These include optimal signal
filtering to maximize the signal-to-noise ratio and coincidence analysis to reject muon backgrounds.
category : Applications333

PE-23 Characterisation of CRESST-III target crystals in the shallow undergroundlaboratory at the Technical University of Munich
Michael Willers1 , Xavier Defay2 , Nahuel Ferreiro3 , Angelina Kinast4 , Jean-Come Lanfranchi5 , Alexander
Langenkamper6 , Erik Lindner7 , Michele Mancuso8 , Elizabeth Mondragon9 , Andrea Munster10 , Tobias Ortmann11 ,Walter Potzel12 , Stefan Schonert13 , Raimund Strauss14 , Andreas Ulrich15 , Stephan Wawoczny16
1

Technical University of Munich, 2 Physics Department and Excellence Cluster Universe, Technical University of Munich ,Max Planck Institut f. Physics , 4 Physics Department and Excellence Cluster Universe, Technical University of Munich ,5
Physics Department and Excellence Cluster Universe, Technical University of Munich , 6 Physics Department and Excellence
Cluster Universe, Technical University of Munich , 7 Physics Department and Excellence Cluster Universe, Technical
University of Munich , 8 Max Planck Institut f. Physics , 9 Physics Department and Excellence Cluster Universe, Technical
University of Munich , 10 Physics Department and Excellence Cluster Universe, Technical University of Munich , 11 Physics
Department and Excellence Cluster Universe, Technical University of Munich , 12 Physics Department and Excellence Cluster
Universe, Technical University of Munich , 13 Physics Department and Excellence Cluster Universe, Technical University of
Munich , 14 Max Planck Institut f. Physics , 15 Physics Department and Excellence Cluster Universe, Technical University of
Munich , 16 Physics Department and Excellence Cluster Universe, Technical University of Munich
3

The Technical University of Munich (TUM) produces scintillating CaWO4 target crystals with high radiopurity forthe direct dark matter search experiment CRESST-III (Cryogenic Rare Event Search with Superconducting Thermometers). The full production process from the raw materials to the final target crystals is performed in-house at
TUM.
Phase 2 of the CRESST-III experiment plans an increment of the target mass, therefore, the growth of several
CaWO4 ingots (raw crystals used to produce the target crystals) is required. To ensure the high radiopurity of the
produced crystals, TUM is investigating new diagnostic techniques that enable a fast feedback to the production
process. One of the investigated methods is the measurement of the internal alpha-contamination of CaWO4 crystals
operated as scintillating cryogenic detectors. In order to avoid the time-consuming production of W-TES (transitionedge sensors) on the crystals and underground
operation, we study the readout of the alpha-induced phonon signal with the TES based active holding scheme of
CRESST and by means of NTD thermistors in the shallow underground laboratory at TUM.
In this contribution we will present first results on the radiopurity of TUM-grown CaWO4 crystals investigated bythese new methods.
category : Applications334

PE-24 Quantum-limited scan strategies: Optimizing resonant axion and hidden
photon dark matter detection
Saptarshi Chaudhuri1 , Kent Irwin2 , Peter Graham3 , Jeremy Mardon4 , Arran Phipps5 , Stephen Kuenstner6 ,Hsiao-Mei Cho7 , Dale Li81

Department of Physics, Stanford University, 2 Department of Physics, Stanford University / SLAC National Accelerator
Laboratory , 3 Department of Physics, Stanford University , 4 Department of Physics, Stanford University , 5 Department of
Physics, Stanford University , 6 Department of Physics, Stanford University , 7 SLAC National Accelerator Laboratory , 8 SLAC
National Accelerator Laboratory

Tunable electromagnetic resonators read out with a sensitive amplifier provide a promising approach for probing
axion and hidden photon dark matter over a large mass range. For example, DM Radio is a search using a tunable,
lumped-element superconducting resonator read out by a SQUID which will scan for axion and hidden photon dark
matter over frequencies between 100 Hz and 100 MHz (masses between 0.5 peV and 500 neV). In this work, we
discuss the optimization of scanning resonant searches in the broader context of impedance matching and amplifier
noise matching. We show that an optimized scan strategy uses a resonant circuit which is not noise-matched to theamplifier. We explain this result in terms of measurement backaction, which results in a tradeoﬀ between the onresonance signal-to-noise and the bandwidth over which appreciable sensitivity may be obtained. We also determine
the optimal time allocation over resonant frequency scan steps. With these results in hand, we derive a quantum
limit on the sensitivity of scanning resonant searches. We show, contrary to previous results, that there is a gain
in sensitivity for resonator quality factors above one million and that the bandwidth set by virialization does notfundamentally set an optimal Q for a search. We also show that a scanning resonant search is superior to a purely
broadband search at all frequencies at which a resonator can be made. We present progress toward a fundamental
limit on all electromagnetic searches (regardless of pole structure) based on criteria similar to the Bode-Fano limit.
We discuss the implications of these results for resonant searches, in particular, for DM Radio. The application of an
optimized scan strategy may lead to a reduction in scan time, especially at the lower frequencies, where it promises a
few orders of magnitude improvement.
category : Applications335

PE-25 TES-based light detectors for the CRESST direct dark matter search
Johannes F. Rothe1
1Max-Planck-Institute for Physics

The CRESST (Cryogenic Rare Event Search with Superconducting Thermometers) experiment uses TES-based cryogenic detectors, namely scintillating CaWO4 crystals and silicon-on-sapphire (SOS) light detectors, to search for dark
matter interactions with the phonon-light technique. The ?40mm SOS plates of the most recent data taking phase typically reached absolute baseline energy resolutions of σ = 4-7 eV. This is the best performance reported for cryogenic
light detectors of this size. First results of further improved light detectors developed for the ongoing low-threshold
CRESST-III experiment and new developments for large-area visible light detectors are presented.
category : Applications336

PE-26 Development of Lumped Element Kinetic Inductance Detectors for Light Dark
Matter Searches using Liquid Helium
Yosuke Kida1 , Masashi Hazumi2 , Naoto Hidehira3 , Fuminori Hirayama4 , Hirokazu Ishino5 , Atsuko Kibayashi6 ,Satoshi Kohjiro7 , Kunimoto Komatsu8 , Nobuaki Sato9 , Yosuke Yamada10 , Hirotake Yamamori11
1

Graduate School of Natural Science and Technology, Okayama University, 2 Institute of Particle and Nuclear Studies, HighEnergy Accelerator Research Organization (KEK) / Kavli Institute for the Physics and Mathematics of the Universe (IPMU), 3 Graduate School of Natural Science and Technology, Okayama University , 4 Nanoelectronics Research Institute, National
Institute of Advanced Industrial Science and Technology (AIST) , 5 Graduate School of Natural Science and Technology,
Okayama University , 6 Graduate School of Natural Science and Technology, Okayama University , 7 Nanoelectronics ResearchInstitute, National Institute of Advanced Industrial Science and Technology (AIST) , 8 Graduate School of Natural Scienceand Technology, Okayama University , 9 Institute of Particle and Nuclear Studies, High Energy Accelerator Research
Organization (KEK) , 10 Graduate School of Natural Science and Technology, Okayama University , 11 Nanoelectronics
Research Institute, National Institute of Advanced Industrial Science and Technology (AIST)

We have developed the superconducting detector LEKIDs (Lumped Element Kinetic Inductance Detectors) for a dark
matter search using liquid He. It has been supposed that the dark matter is composed of Weakly Interacting Massive
Particles (WIMPs). Direct searches for the WIMPs have been conducted using Xe, Ge, Si and NaI as targets. Theseexperiments have sensitivities for WIMP mass down to about 10 GeV/c2 . In 2013, W. Guo and D. N. McKinsey
proposed to use liquid He as a target to obtain a sensitivity beyond 10 GeV/c2 in WIMP mass. Recoiled helium atoms
produce scintillation light photons with the wavelength of 80 nm (16 eV in energy). Those photons can be detectedwith the superconducting detector LEKID surrounding the target liquid He. The LEKIDs oﬀer us a frequency domain
multiplexing readout that reduces the number of readout cables, decreasing the heat load from the outside. In thiswork, we present the overview concept of the dark matter detector using liquid He and the current status of thedevelopment of LEKIDs.
The LEKIDs are fabricated with photolithographic techniques in clean rooms: CRAVITY in AIST and another at
KEK. We use Nb or NbN for superconducting materials. For the proper operation of LEKIDs, its resonant frequencies
should be as close as designed ones. We have found that the over-etching of the substrate surface during the fabricationaﬀects the resonant frequencies and AlN etching stopper underneath the electrode relaxes this problem. We will discussin detail this improvement as well as other several topics.
category : Applications337

PE-27 Current Status of the Detector Developement for the CRESST Dark MattersearchMarc Wuestrich1 ,1

Max-Planck-Institute f. Physics,

The cryogenic dark matter experiment CRESST aims at the direct detection of dark matter via elastic scattering oﬀ
nuclei in scintillating CaWO4 crystals. Operated as cryogenic calorimeters, the required sensitivity is achieved readingthem out with transition edge sensors (TES). This combination provides excellent energy resolution and allows the
CRESST experiment to achieve one of the lowest detection thresholds in the field. Particle identification is achievedby the simultaneous measurement of phonon and scintillation signal. By exploiting the reduced scintillation output of
nuclear recoils in CaWO4 , the dominant β/γ-backgrounds are vetoed eﬃciently on a event-by event level.
To probe the low mass parameter space of dark matter, a new generation of detectors was developed to be
deployed in the CRESST setup at LNGS Gran Sasso. By significantly reducing the mass of the target crystals andby using improved TES structures, the currently used detector modules (CRESST-III (Phase 1)) aim to lower thethreshold of the phonon channel below ∼ 100 eV and of the light channel below ∼ 20 eV. Furthermore, a new detector
housing and holding concept was developed which establishes a measurement environment able to identify backgroundoriginating from surrounding surfaces. The poster will give a review of the currently achieved detector performancewithin CRESST-III (Phase 1) and an overview of the ongoing R&D eﬀorts to improve the currently achieved detector
performance.
category : Applications338

PE-28 163Ho distillation and implantation for Holmes experiment
Giovanni Gallucci1
1

National Institute of Nuclear Physics - Genova’s Section

HOLMES is an experiment to directly measure the neutrino mass with a calorimetric approach. The calorimetrictechnique eliminates several systematic uncertainties usually present in spectrom- eters where the external source andthe decays to excited states aﬀect the measurement. 163Ho is chosen as source for its very low Q-value (2.8 keV), theproximity of the end-point to resonance M1 and its half life (4570y). These features are optimal to reach simultaneously
a good activity to have suﬃcient statistics in the end-point and a small quantity of 163Ho embedded in the de- tector to
not alter significantly its heat capacity. 163Ho will be produced with neutron irradiation of enriched 162Er2O3 at theInstitute Laue-Langevin (Grenoble, France), and chemical separated at Paul Scherrer Institute (Villigen, Switzerland).
It will arrive at INFN laboratory of Genova in oxide form (Ho2O3) with traces of others Ho isotopes and contaminants
not removeable using chemical methods. In particular the metastable 166mHo has a beta decay with half life ofabout 1200y which can induce background below 5 keV. The removal of these contaminants is critical for Holmes so
a dedicated system is being set up by our group from the Genova INFN section. The system is designed to achieve
an optimal mass separation for 163Ho and consists of two main components: an evaproation chamber and an ion
implanter. In the evaporation chamber Holmium will be reduced in metallic form, using the reaction 2Y+Ho2O3 →Y2O3+2Ho and used to produce a metallic target for the ion implanter source. The ion implanter consists of fivemain components. A Penning sputter ion source, an acceleration section, a magnetic/electrostatic mass analyzer, amagnetic scanning stage and a focusing electrostatic triplet. In this contribution we describe the procedures, undercontinuous refinement, for the Holmium evaporation process, the metallic target production and the status of the ion
implanter.
category : Applications339

PE-29 A low-energy electron detector from photoionization process with Rydberg
atoms at low temperature to search for dark matter axions
Seishi Matsuki1 , Haruhiko Funahashi2 , Akira Matsubara3 , Kyohei Nakajima4 , Izumi Ogawa5
1

Research Center for Nuclear Physics, Osaka Univerisity, 2 Institute for Liberal Arts and Sciences, Kyoto University, Kyoto
606, Japan , 3 Department of Physics, Kyoto University, Kyoto 606, Japan , 4 School of Engineering, University of Fukui, Fukui
910, Japan , 5 School of Engineering, University of Fukui, Fukui 910, JapanThe axion, originally invoked to recover from a serious defect of QCD theory on the CP (Time reversal) invariancein the strong interactions, so-called “strong CP problem”, is one of the most plausible candidates of dark matterparticles. It is usual to search for axions by firstly converting axions into photons in a high magnetic field and thenthe photons are detected with a photon detector in a high-Q resonant cavity [1,2]. In this scheme, we can search foraxions in a very limited range of its mass in one run, although the detection eﬃciency is increased due to the eﬀect ofhigh-Q cavity.
We recently proposed to apply the direct photoionization process with Rydberg atoms to search for axions over awide range of its mass simultaneously without degrading the sensitivity at low temperature[3]: In this new scheme,
axion-converted microwave photons are absorbed to highly excited Rydberg atoms, thereby ionized directly in a metal
container instead of a resonant high-Q cavity. Then the electrons from this photoionization process are guided tooutside the container and accelerated and detected with an electron detector.
Since the final states in the photoionization process distribute continuously, microwave frequencies of photons
absorbed and detected in this process are also continuous, thus enabling us to search for axions in a wide range of its
mass simultaneously. It should also be mentioned that by changing the initially prepared state of the Rydberg atoms
and/or by varying the electric field strength applied to the Rydberg atoms, it is possible to know the mass of axions
once some definite signals of axions are observed.
In order to realize such scheme actually for axion search, it is essential to develop a sensitive low-energy electron
detector from the direct photoionization process at low temperature. We studied possible configuration of the detector
system in which electrons produced over a wide spatial region in a metal container are collected and transported to a
scintillation detector while keeping the temperature of the container and detector system low enough (less than 100mK) to avoid increasing the background from blackbody radiations.
Here we present an electron detector system, which fulfills the above requirement by fully designing the wholesystem with an ion and an optical simulation calculations. Some results of the obtained performance of the detector
system are also presented and discussed.
References:[1] R. Bradley, S. Matsuki, et al., Rev. Mod. Phys. 75(2003)777.
[2] M. Shibata, et a., Rev. Sci. Instr. 74(2003)3317, and references cited therein.
[3] S. Matsuki, et al., to be published.
category : Applications340

PE-30 Sensitivity of TES Microcalorimeter Arrays for Solar-Axion Line Emission
Kazuhisa Mitsuda1 , Keisei Maehisa21ISAS, JAXA, 2 ISAS, JAXA

Axion is a hypothetical elementary particle proposed to solve the strong CP problem in QCD. It is suggested that thesun is a strong axion emitter through Primakoﬀ eﬀect, and that the emission has an energy spectrum with a shapeof a blackbody spectrum with kT ∼ 1.3 keV, reflecting the photon temperature at the center pf the sun. Moriyama(1995) first suggested that monochromatic lines will be also emitted by M1 transition of nuclei. He also suggested
that such axion lines could be detected by using a proper conversion material at the Earth. Several experiments havebeen done so far, however, the upper limit is still high compared to estimations basing on axion models. In this paper,
we will investigate methods to detect solar-axion line emission using TES microcalorimeter arrays and estimate thesensitivities. We consider that by using TES array of a size discussed for future X-ray astronomy mission, such as
Athena X-IFU, we can reach a meaningful sensitivity.
category : Applications341

PE-31 Status of the AMoRE experiment searching for neutrinoless double beta decay
using low-temperature detectors
H.S. Jo1 , S. Choi2 , F.A. Danevich3 , A. Fleischmann4 , J.A. Jeon1 , C.S. Kang1 , W.G. Kang1 , G.B. Kim1 , H.J. Kim5 ,H.L. Kim1 , I. Kim 1,6 , S.K. Kim2 , S.R. Kim1 , Y.H. Kim1,6 , Y.D. Kim 1 , V. Kornoukhov7 , D.H. Kwon 1 , C. Lee 1 ,H.J. Lee 1 , M.K. Lee6 , S.H. Lee 1 , S.Y. Oh1,6 , J.H. So1 , Y.S. Yoon1
1

Center for Underground Physics, Institute for Basic Science (IBS), Daejeon 34047, Korea 2 Department of Physics andAstronomy, Seoul National University, Seoul 08826, Korea 3 Institute for Nuclear Research, MSP 03680 Kyiv, Ukraine
4
Kirchhoﬀ-Institute for Physics, D-69120 Heidelberg, Germany 5 Department of Physics, Kyungpook National University,
Daegu 41566, Korea 6 Korea Research Institute of Standards and Science (KRISS), Daejeon 34113, Korea 7 Institute ofTheoretical and Experimental Physics, Moscow 117218, Russia

The goal of the Advanced Mo-based Rare process Experiment (AMoRE) is to search for neutrinoless double beta decayof 100 Mo using low-temperature detectors consisting of Mo-based scintillating crystals read out via metallic magnetic
calorimeters (MMCs). Simultaneous measurements of heat and light signals are performed at millikelvin temperatures,
which are reached using a dilution refrigerator. The AMoRE-Pilot experiment, using five 100 Mo-enriched, 48 Cadepleted calcium molybdate crystals with a total mass of about 1.5 kg, has been running in the 700-m-deep Yangyang
underground Laboratory as the pilot phase of the AMoRE project. Several setup improvements through diﬀerent runs
allowed us to achieve high energy resolution and eﬃcient particle discrimination. The current status of the AMoRE
experiment, as well as the plans for the next, higher-scale, experimental stages, will be presented.
category : Applications342

PE-32 Development of patchable light detectors for the AMoRE project
Hyejin Lee1 , Hyon-Suk Jo2 , Chan Seok Kang3 , Hyelim Kim4 , So-Ra Kim5 , Geon-Bo Kim6 , Inwook Kim7 ,Yong-Hamb Kim8 , Minkyu Lee9 , Seung-Yoon Oh10 , Jungho So11
1

Institute for Basic Science(IBS), 2 Institute for Basic Science, Daejeon , 3 Institute for Basic Science, Daejeon , 4 Institute for
Basic Science, Daejeon / Kyungpook National University , 5 Institute for Basic Science, Daejeon , 6 Institute for Basic Science,
Daejeon , 7 Institute for Basic Science, Daejeon / Seoul National University, Seoul / Korea Research Institute of Standards andScience, Daejeon , 8 Institute for Basic Science, Daejeon / Korea Research Institute of Standards and Science, Daejeon ,9
Korea Research Institute of Standards and Science, Daejeon , 10 Institute for Basic Science, Daejeon / Korea ResearchInstitute of Standards and Science, Daejeon / Sejong University, Seoul , 11 Institute for Basic Science, Daejeon

We describe light detector development to be used for AMoRE neutrinoless double beta decay experiment. The lightdetectors used in the present stage of the project is composed of a Ge wafer as an absorber for scintillation light andan MMC sensor to read the temperature change by the light absorption. Each MMC sensor is tested individually
and assembled with an absorber wafer. In this patchable design of light detectors, it is relatively easy to replace
the absorber material with better phononic properties. We investigate the absorber dependence of the light signals
employing Ge, Si and Si-on-sapphire wafers. Moreover, the phonon collector films are heat treated in various conditions
to make an eﬃcient heat transfer to the MMC sensor from the wafer.
category : Applications343

PE-33 Signal stabilization study for AMoRE detectors
Dohyung Kwon1 , Yong-Hamb Kim2 , Sora Kim3 , Chan Seok Kang4 , Inwook Kim5 , Hyon-Suk Jo6 , Hye Lim Kim7 ,Chang Lee8 , Hyejin Lee9 , SeungHoon Lee10 , Seung-Yoon Oh11 , Jin-A Jeon121

Center for Underground Physics, Institute for Basic Science, 2 Institute for Basic Science / University of Science andTechnology / Korea Research Institute of Standards and Science , 3 Institute for Basic Science , 4 Institute for Basic Science ,5
Institute for Basic Science / Korea Research Institute of Standards and Science / Seoul National University , 6 Institute for
Basic Science , 7 Institute for Basic Science / Kyungpook National University , 8 Institute for Basic Science , 9 Institute for
Basic Science , 10 Institute for Basic Science , 11 Institute for Basic Science / Korea Research Institute of Standards and Science/ Sejong University , 12 Institute for Basic Science

AMoRE (Advanced Mo-based Rare process Experiment) is an international project to search for neutrinoless double
beta decay (0 νββ) of 100Mo. The project employs simultaneous phonon-scintillation detection from scintillating
crystals containing 100Mo elements based on MMC readouts. As the heat capacities of a crystal absorber and an
MMC sensor varies with temperature together with MMC sensitivity, signal amplitudes may drift over a long time
constant as the base temperature fluctuates. This eﬀect degrades the energy resolution of the calorimetric detection
at low temperatures. By installing a Joule heater on the detector to periodically inject controlled amount of heat, we
can produce reference signals that can be used for gain stabilization. We present the characterization of Joule heaters
for future AMoRE runs, and test results using a molybdate crystal.
category : Applications344

PE-34 Development of phonon and photon detectors for rare events searches using
scintillating crystals
Andreas Fleischmann1 , Felix Ahrens2 , Christian Enss3 , Loredana Gastaldo4 , Clemens Hassel5 , Sebastian Kempf6 ,Yong-Hamb Kim7 , Martin Loidl8 , Xavier Francois Navick9 , Mathias Rodrigues10 , Won Sik Yoon11
1

Kirchhoﬀ Institute for Physics, Heidelberg University, 2 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120
Heidelberg, Germany , 3 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany ,4
Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 5 Kirchhoﬀ Institute for Physics,
Heidelberg University, INF 227, 69120 Heidelberg, Germany , 6 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227,
69120 Heidelberg, Germany , 7 Korean Research Institute of Standards and Science, Daejeon, Rep. of Korea , 8 Commissariat al’energie atomique, Saclay, France , 9 Commissariat a l’energie atomique, Saclay, France , 10 Commissariat a l’energie atomique,
Saclay, France , 11 Korean Research Institute of Standards and Science, Daejeon, Rep. of Korea

The use of scintillating crystals in cryogenic experiments searching for rare events as neutrinoless double beta decay or
the interaction of a Dark Matter particle allows for an eﬃcient background reduction thanks to particle discrimination.
We have developed phonon and photon detectors based on metallic magnetic calorimeters (MMCs) for the simultaneous
measurement of heat and light generated upon the interaction of a particle in a scintillating crystal. The aimed values
for the energy resolution and signal rise-time expected for the phonon detector are ∆EFWHM < 100 eV and τ < 200µs
while for the photon detector we expect ∆EFWHM < 10 eV and < 10µs. The achievement of these time and energy
resolutions will pave the way for a more selective particle discrimination which is of utmost importance for next
generation experiments searching for neutrinoless double beta decays and dark matter direct detection aiming fortarget material of the order of 1 ton.
We present the concepts for the development of the P2 detector, a combined photon and phonon detector, which isfabricated on a 3” Si or Ge wafer. We discuss the challenges to fabricate the P2 detector, in particular the segmented
temperature sensor for the photon detector and the decoupling of the two readout channels. We present the results
obtained with the first experimental characterizations.
category : Applications345

PE-35 Fabrication and characterization of MMCs with enclosed 163 Ho
Loredana Gastaldo1 , Holger Dorrer2 , Christoph Emanuel Duellmann3 , Klaus Eberhardt4 , Christian Enss5 , Andreas
Fleischmann6 , Dorothea Fonnesu7 , Lisa Gamer8 , Loredana Gastaldo9 , Clemens Hassel10 , Daniel Hengstler11 ,Sebastian Kempf12 , Tom Kieck13 , Federica Mantegazini14 , Fabian Schneider15 , Mathias Wegner16 , Klaus Wendt17
1

Kirchhoﬀ Institute for Physics, Heidelberg University, 2 Institute for Nuclear Chemistry, Johannes Gutenberg University, Fritz
Strassmann Weg 2, D- 55128, Mainz, Germany, , 3 Institute for Nuclear Chemistry, Johannes Gutenberg University, Fritz
Strassmann Weg 2, D- 55128, Mainz, Germany, , 4 Institute for Nuclear Chemistry, Johannes Gutenberg University, Fritz
Strassmann Weg 2, D- 55128, Mainz, Germany, , 5 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120
Heidelberg, Germany , 6 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany ,7
Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 8 Kirchhoﬀ Institute for Physics,
Heidelberg University, INF 227, 69120 Heidelberg, Germany , 9 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227,
69120 Heidelberg, Germany , 10 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany ,11
Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 12 Kirchhoﬀ Institute forPhysics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 13 Institute for Nuclear Chemistry, Johannes Gutenberg
University, Fritz Strassmann Weg 2, D- 55128, Mainz, Germany, / Institut fuer Physik, Johannes Gutenberg-Universitaet
Mainz, Staudingerweg 7, D - 55128 Mainz , 14 Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120
Heidelberg, Germany , 15 Institut fuer Physik, Johannes Gutenberg-Universitaet Mainz, Staudingerweg 7, D - 55128 Mainz ,16
Kirchhoﬀ Institute for Physics, Heidelberg University, INF 227, 69120 Heidelberg, Germany , 17 Institut fuer Physik,
Johannes Gutenberg-Universitaet Mainz, Staudingerweg 7, D - 55128 Mainz

The Electron Capture in 163 Ho experiment ECHo aims to probe the electron neutrino mass on a sub-eV level via theanalysis of the calorimetrically measured electron capture spectrum of 163 Ho. For this, metallic magnetic calorimeters(MMC) operated at temperatures in the mK range will be used. The first prototypes of MMC detector arrays withembedded 163 Ho showed so far an excellent performance, with an energy resolution of ∆EFWHM ¡ 5 eV and a signal
rise time of τ ¡ 1 µ??. We present the current status of the detector developments for ECHo-1k, the first phase of theexperiment characterized by a source activity of 1 kBq and an expected sensitivity on the neutrino mass below 10 eV.
We discuss the optimization of the design and fabrication of the ECHo-1k detector arrays including their single
channel to multiplexed readout, and the necessary not standard fabrication processes to prepare the detector for the ion
implantation of 163 Ho. For this, the RISIKO facility at Mainz University underwent several modifications to improve
the reliability and the eﬃciency of the diﬀerent steps as resonant laser ionization, mass separation and implantationin the array. We also present simulations and experimental studies concerning the implantation process itself.
We discuss the results of measurements of the expected additional heat capacity of the detector due to the implantation of 163 Ho, which is a crucial parameter for the detector performance.
category : Applications346

PE-36 The ν-cleus experiment: Gram-scale cryogenic calorimeters for a rapid
discovery of coherent neutrino scattering.
Raimund Strauss1 , Johannes Rothe2 , Franz Probst3 , Wolfgang Seidel4 , Federica Petricca5 , Stefan Schonert6 , Lothar
Oberauer7 , Jochen Schiek8
1

Max-Planck-Institut for Physics, Munich, 2 Max-Planck-Institut fur Physik, Munich , 3 Max-Planck-Institut fur Physik,
Munich , 4 *deceased, Max-Planck-Institut fur Physik, Munich , 5 Max-Planck-Institut fur Physik, Munich , 6 Physik
Department E15, Technical University Munich , 7 Physik Department E15, Technical University Munich , 8 Institut fur
Hochenergiephysik der Osterreichischen Akademie der Wissenschaften, Vienna and Technical University of Vienna

We investigate new gram-scale cryogenic detectors, 1-2 orders of magnitude smaller in size than previous devices. Theseare expected to reach unprecedentedly low energy thresholds, in the 10 eV-regime and below. This technology allows
new approaches in rare-event searches, including the search for MeV-scale dark matter, detection of solar neutrinos
and a rapid discovery of coherent neutrino-nucleus scattering (CNNS) at a nuclear reactor. We show a simple scaling
law for the energy threshold of cryogenic calorimeters, allowing to extrapolate the performance of existing devices
to smaller sizes. Results from a measurement with a 0.5 g sapphire detector are presented. This prototype reacheda threshold of 20 eV, one order of magnitude lower than previous results with massive calorimeters. We discuss anexperiment, called ν-cleus, which enables a 5-σ discovery of CNNS within about 2 weeks of measuring time at 40
m distance from a power reactor. In a second stage, this experiment enables precision measurements of the CNNS
cross-section and spectral shape for new physics beyond the Standard Model.
category : Applications347

PE-37 Trigger study on AMoRE-pilot detector
I. Kim1,2,3 , S. Choi2 , F.A. Danevich4 , A. Fleischmann5 , J.A. Jeon, H.S. Jo1 , C.S. Kang1 , W.G. Kang1 , G.B. Kim1 ,H.J. Kim6 , H.L. Kim1 , S.K. Kim2 , S.R. Kim1 , Y.H. Kim1,3 , Y.D. Kim1 , V. Kornoukhov7 , D.H. Kwon1 , C. Lee1 , H.J.
Lee1 , M.K. Lee 3, S.H. Lee1 , S.Y. Oh1,3 , J.H. So1 , Y.S. Yoon1
1

Center for Underground Physics, Institute for Basic Science (IBS), Daejeon 34047, Korea 2 Department of Physics andAstronomy, Seoul National University, Seoul 08826, Korea 3 Korea Research Institute of Standards and Science (KRISS),
Daejeon 34113, Korea 4 Institute for Nuclear Research, MSP 03680 Kyiv, Ukraine 5 Kirchhoﬀ-Institute for Physics, D-69120
Heidelberg, Germany 6 Department of Physics, Kyungpook National University, Daegu 41566, Korea 7 Institute of Theoreticaland Experimental Physics, Moscow 117218, Russia

Advanced Mo-based Rare process Experiment (AMoRE) is a search for neutrinoless double beta decay of Mo-100 at
millikelvin temperatures using metallic magnetic calorimeters (MMCs). The crystal based detectors that are used forthe experiment have a high energy resolution and a low baseline fluctuation, as well as a low background level thatis acquired by installing the detectors in the underground laboratory. Therefore, the detector setup used for AMoRE
experiment can also be used for a low energy dark matter search experiment given that a crystal with suitable nuclear
mass number is used. As the recoil energy of matter-dark matter collision is thought to be very low, a method toeﬀectively trigger low energy events is required. In this presentation, we discuss the triggering method and the energy
threshold of the AMoRE-pilot detector with 40Ca100MoO4 crystals.
category : Applications348

PE-38 Directionality study of phonon-scintillation signals from a zinc tungstate
crystalJeon JA1 , Kim HL2 , Kim IW3 , Kim SR4 , Kim YH5 , Kwon DH6 , Lee HJ7 , Lee SH8 , Oh SY9 , Sekiya H10
1

Center for Underground Physics, Institute for Basic Science, 2 Center for Underground Physics, Institute for Basic Science,
Daejeon, Republic of Korea , 3 Center for Underground Physics, Institute for Basic Science, Daejeon, Republic of Korea ,4Center for Underground Physics, Institute for Basic Science, Daejeon, Republic of Korea , 5 Center for Underground Physics,
Institute for Basic Science, Daejeon, Republic of Korea / Korea Research Institute of Standards and Science, Daejeon,
Republic of Korea , 6 Center for Underground Physics, Institute for Basic Science, Daejeon, Republic of Korea , 7 Center for
Underground Physics, Institute for Basic Science, Daejeon, Republic of Korea , 8 Center for Underground Physics, Institute for
Basic Science, Daejeon, Republic of Korea , 9 Center for Underground Physics, Institute for Basic Science, Daejeon, Republicof Korea , 10 Kamioka Observatory, ICRR, The University of Tokyo, Hida, Gifu, Japan

Direct dark matter searches for weakly interacting massive particles (WIMPs) are confronted by a firm backgroundfrom coherent neutrino-nucleus scatterings. Introduction of directional dependence of detector response can be one ofthe possibilities for WIMP searches to break the neutrino background floor. We report a directionality study of phononand scintillation signals from a zinc tungstate crystal at low temperature. The simultaneous detection of the heatand light signals with MMC readouts is realized for alphas and low-energy gammas incident in diﬀerent directions.
We present the progress on directional dependence study of the phonon and scintillation signals in comparison with aroom temperature PMT measurement.
category : Applications349

PE-39 Development of Aluminum LEKIDs for Balloon-Borne Far-IR Spectroscopy
Steven Hailey-Dunsheath1 , Alyssa Barlis2 , James Aguirre3 , C. Matt Bradford4 , Henry G. LeDuc5 , Christopher M.
McKenney6 , Tashalee Billings7
1

California Institute of Technology, 2 The University of Pennsylvania , 3 The University of Pennsylvania , 4 Jet Propulsion Lab ,5
Jet Propulsion Lab , 6 National Institute of Standards and Technology , 7 The University of Pennsylvania

We are developing lumped-element kinetic inductance detectors (LEKIDs) designed to achieve background-limited
sensitivity for far-infrared (FIR) spectroscopy on a stratospheric balloon. The Spectroscopic Terahertz Airborne
Receiver for Far-InfraRed Exploration (STARFIRE) will study the evolution of dusty galaxies with observations of
the [CII] 158µm fine-structure transition at z = 0.5 − 1.5, both through direct observations of individual luminous
infrared galaxies, and in blind surveys using the technique of line intensity mapping. The spectrometer will requirelarge format (∼1600 detectors) arrays of dual-polarization sensitive detectors with a targeted NEP of ∼ 4 × 10−18
W Hz−0.5 .
We are developing low-volume LEKIDs fabricated with a single layer of aluminum (20nm thick) patterned ona crystalline silicon wafer, with resonance frequencies of 100 − 250 MHz. The inductor is a single meander with alinewidth of 0.7µm, patterned in a grid to absorb optical power in both polarizations. The meander is coupled to acircular waveguide, fed by a profiled feedhorn. A backshort is produced by backside etching, then depositing gold.
Initial testing of a small array prototype has demonstrated good yield, and an NEP of ∼ 2 × 10−17 W Hz−0.5 . We will
present our ongoing characterization of prototype arrays, and discuss the prospects for achieving our targeted NEP
and scaling up to large format arrays.
category : Applications350

PE-40 The Mexico-UK Sub-millimetre Camera for Astronomy
Edgar Castillo Dominguez1 , Peter Ade2 , Peter Barry3 , Tom Brien4 , Simon Doyle5 , Abel Perez-Fajardo6 , Daniel
Ferrusca7 , Victor Gomez8 , Amber Hornsby9 , David Hughes10 , Phil Mauskopf11 , Paul Moseley12 , Enzo Pascale13 ,Giampaolo Pisano14 , Ivan Rodriguez-Montoya15 , Sam Rowe16 , Carole Tucker17 , Miguel Velazquez18
1

CONACYT-INAOE / Large Millimeter Telescope, 2 School of Physics and Astronomy, Cardiﬀ University , 3 School of Physics
and Astronomy, Cardiﬀ University / Kavli Institute For Cosmological Physics at The University of Chicago , 4 School ofPhysics and Astronomy, Cardiﬀ University , 5 School of Physics and Astronomy, Cardiﬀ University , 6 Instituto Nacional de
Astrofisica Optica y Electronica , 7 Instituto Nacional de Astrofisica Optica y Electronica , 8 Instituto Nacional de Astrofisica
Optica y Electronica , 9 School of Physics and Astronomy, Cardiﬀ University , 10 Instituto Nacional de Astrofisica Optica yElectronica , 11 School Of Earth and Space Exploration, Arizona State University , 12 School of Physics and Astronomy, Cardiﬀ
University , 13 School of Physics and Astronomy, Cardiﬀ University / Sapienza Universita di Roma , 14 School of Physics andAstronomy, Cardiﬀ University , 15 Instituto Nacional de Astrofisica Optica y Electronica , 16 School of Physics and Astronomy,
Cardiﬀ University , 17 School of Physics and Astronomy, Cardiﬀ University , 18 Instituto Nacional de Astrofisica Optica yElectronica

The Mexico-UK Sub-millimetre Camera for Astronomy (MUSCAT) is a large format camera scheduled for installationon the Large Millimetre Telescope (LMT) in 2018. MUSCAT will employ a horn coupled LEKID architecture incorporating a novel meta-material anti-reflection layer to provide a low cost, background limited focal plane operating
at 1.1mm that fills the field of view of the telescope. The easily accessible focal plane will be continuously cooled to
100mK with a novel closed cycle miniature dilution refrigerator and is fed with fully baﬄed reflective optics providing a platform that can be used to demonstrate a range of detector technologies such as on-chip spectrometers andmulti-chroic polarisation sensitive pixels. The MUSCAT project will demonstrate the science capability of such an
instrument on the LMT through two relatively short science programmes to provide high resolution follow up surveys
of galactic and extra-galactics sources previously observed with the Herschel space observatory. In this presentation
we will provide and overview of the detector architecture and the overall instrument design as well as updating on
progress and scheduled installation on the LMT.
category : Applications351

PE-41 Second-generation design of Micro-Spec: a medium-resolution,
submillimeter-wavelength spectrometer-on-a-chip
Giuseppe Cataldo1 , Emily M. Barrentine2 , Berhanu T. Bulcha3 , Negar Ehsan4 , Larry A. Hess5 , Omid Noroozian6 ,Thomas R. Stevenson7 , Kongpop U-Yen8 , Edward J. Wollack9 , Samuel H. Moseley10
1

NASA Goddard Space Flight Center, 2 NASA Goddard Space Flight Center , 3 NASA Goddard Space Flight Center , 4 NASA
Goddard Space Flight Center , 5 NASA Goddard Space Flight Center , 6 NASA Goddard Space Flight Center , 7 NASA
Goddard Space Flight Center , 8 NASA Goddard Space Flight Center , 9 NASA Goddard Space Flight Center , 10 NASA
Goddard Space Flight Center

Micro-Spec (µ-Spec) is a direct-detection spectrometer which integrates all the components of a diﬀraction-grating
spectrometer onto a ∼ 10-cm2 chip through the use of superconducting microstrip transmission lines on a single-crystal
silicon substrate. The second generation of µ-Spec is being designed to operate with a spectral resolution of 512 in thesubmillimeter (500-1000 µm, 300-600 GHz) wavelength range, a band of interest for several spectroscopic applicationsin astrophysics and Earth science. High-altitude balloon missions will provide the first testbed to demonstrate the µSpec technology in a space-like environment and also an economically viable venue for multiple observation campaigns.
This work reports on the current status of the instrument design and will provide a brief overview of each instrument
subsystem. Particular emphasis will be given to the design of the spectrometer s two-dimensional diﬀractive region,
through which the light of diﬀerent wavelengths is focused on the kinetic inductance detectors along the focal plane.
An optimization process is employed to generate geometrical configurations of the diﬀractive region that satisfy specificrequirements on spectrometer size, operating spectral range and performance. An optical design optimized for balloon
missions will be presented in terms of geometric layout, spectral purity and eﬃciency.
category : Applications352

PE-42 CCAT-prime: An Extreme Field-of-View Submillimeter Telescope on Cerro
Chajnantor
Michael D Niemack1
1

Department of Physics, Cornell University

CCAT-prime is a six meter aperture oﬀ-axis submillimeter telescope that will be located at 5600m elevation on Cerro
Chajnantor in Chile with operations beginning in 2021. The science priorities for CCAT-prime span from cosmology
and inflation in the first fraction of a second after the Big Bang to probing the epoch of reionization and galactic ecology
studies of the dynamic interstellar medium. Advances in all these areas are enabled by the combination of the large
field-of-view (FOV) and accessible atmospheric windows between 200 microns and 3 millimeter wavelengths. We aredeveloping: broadband superconducting detector technologies optimized to measure the cosmic microwave background(CMB) and Sunyaev-Zel dovich (SZ) eﬀects and modest resolution spectroscopic imagers to measure fine structureline emission from ionized carbon ([CII] 158 micron) during reionization. In addition, heterodyne spectrometers will
be built to measure galactic emission lines. The crossed-Dragone optics design provides an eight degree diameter FOV,
enabling CCAT-prime to host a next generation CMB instrument with as many as ∼105 superconducting detectors
for a Stage-IV -scale CMB survey and many more detectors at sub-millimeter wavelengths. Here we present a
brief overview of the project and describe the superconducting detector, readout, and instrument technologies thatare being developed and studied for CMB/SZ and [CII] intensity mapping observations.
category : Applications353

PE-43 On-Sky Performance of MUSTANG-2: the Multiplexed SQUID TES Array at
Ninety GHz
Sara M. Stanchfield1 , Peter A.R. Ade2 , James Aguirre3 , Justus A. Brevik4 , Hsiao-Mei Cho5 , Rahul Datta6 , Mark J.
Devlin7 , Simon R. Dicker8 , Bradley Dober9 , Shannon M. Duﬀ10 , Dennis Egan11 , Pam Ford12 , Gene Hilton13 ,Johannes Hubmayr14 , Kent D. Irwin15 , Paul Marganian16 , Brian S. Mason17 , John A.B. Mates18 , Jeﬀ McMahon19 ,Melinda Mello20 , Tony Mroczkowski21 , Charles Romero22 , Carole Tucker23 , Joel Ullom24 , Leila R. Vale25 , SteveWhite26 , Mark Whitehead27 , Alexander H. Young28
1Department of Physics and Astronomy, University of Pennsylvania, 2 Cardiﬀ University , 3 University of Pennsylvania ,National Institute of Standards and Technology Boulder Laboratories , 5 Standford University , 6 University of Michigan ,7
University of Pennsylvania , 8 University of Pennsylvania , 9 National Institute of Standards and Technology Boulder
Laboratories , 10 National Institute of Standards and Technology Boulder Laboratories , 11 Green Bank Observatory , 12 GreenBank Observatory , 13 National Institute of Standards and Technology Boulder Laboratories , 14 National Institute ofStandards and Technology Boulder Laboratories , 15 Standford University , 16 Green Bank Observatory , 17 National Radio
Astronomy Observatory , 18 National Institute of Standards and Technology Boulder Laboratories , 19 University of Michigan ,20
Green Bank Observatory , 21 European Southern Observatory , 22 Institut de Radioastronomie Millimetrique , 23 Cardiﬀ
University , 24 National Institute of Standards and Technology Boulder Laboratories , 25 National Institute of Standards andTechnology Boulder Laboratories , 26 Green Bank Observatory , 27 Green Bank Observatory , 28 University of Pennsylvania
4

We present the array performance and astronomical images from early science results from MUSTANG-2, a 90 GHz
feedhorn-coupled, microwave SQUID-multiplexed TES bolometer array operating on the Robert C. Byrd Green Bank
Telescope (GBT). MUSTANG-2 was installed on the GBT on December 2, 2016 and immediately began commissioning
eﬀorts, followed by science observations. The feedhorn and waveguide-probe-coupled detector technology is a maturetechnology, which has been used on instruments such as the South Pole Telescope, the Atacama Cosmology Telescope,and the Atacama B-mode Search telescope. The microwave SQUID multiplexer-based readout system developed for
MUSTANG-2 currently reads out 66 detectors with a single coaxial cable and will eventually allow thousands ofdetectors to be multiplexed. This microwave SQUID multiplexer combines the proven abilities of millimeter wave
TES detectors with the multiplexing capabilities of KIDs with no degradation in noise performance of the detectors.
Each multiplexing device is read out using warm electronics consisting of a commercially available ROACH board,a DAC/ADC card, and an Intermediate Frequency mixer circuit. The hardware was originally developed by the
Collaboration for Astronomy Signal Processing and Electronic Research (CASPER) group, whose primary goal is
to develop scalable FPGA-based hardware with the flexibility to be used in a wide range of radio signal processing
applications. MUSTANG-2 is the first on-sky instrument to use microwave SQUID multiplexing and is available as ashared-risk/PI instrument on the GBT. In MUSTANG-2’s first season 7 separate proposals were awarded a total of
230 hours of telescope time.
category : Applications354

PE-44 The KIDS project
Ivan Colantoni1 , Elia Battistelli2 , Maria Gabriella Castellano3 , Alessandro Coppolecchia4 , Paolo de Bernardis5 ,Cristian Franceschet6 , Luca Lamagna7 , Stefano Mandelli8 , Jacopo Martelli9 , Silvia Masi10 , Aniello Mennella11 ,Alessandro Paiella12 , Mario Zannoni13
1

Institute for Photonics and Nanotechnologies, National Research Council (CNR - IFN), 2 Dipartimento di Fisica Sapienza
Universita di Roma, Roma (Italy) , 3 CNR Istituto di Fotonica e Nanotecnologie (CNR-IFN), Roma (Italy) , 4 Dipartimento di
Fisica Sapienza Universita di Roma, Roma (Italy) , 5 Dipartimento di Fisica Sapienza Universita di Roma, Roma (Italy) ,6
Dipartimento di Fisica Universita di Milano, Milano (Italy) , 7 Dipartimento di Fisica Sapienza Universita di Roma, Roma
(Italy) , 8 Dipartimento di Fisica Universita di Milano, Milano (Italy) , 9 Dipartimento di Fisica Universita di Milano, Milano(Italy) , 10 Dipartimento di Fisica Sapienza Universita di Roma, Roma (Italy) , 11 Dipartimento di Fisica Universita di Milano,
Milano (Italy) , 12 Dipartimento di Fisica Sapienza Universita di Roma, Roma (Italy) , 13 Dipartimento di Fisica Universita di
Milano Bicocca, Milano (Italy)

The aim of Kinetic Inductance Detectors for Space (KIDS) experiment is the optimization of KIDs for low-energy
photons (IR to mm-waves). Future space missions devoted to the cosmology of the early universe, to molecularand plasma astrophysics and to the observation of the earth and its atmosphere can benefit significantly from theavailability of ultra-sensitive detectors like KIDs.
The goal of the project is the development and characterization of two KIDs array, completed by their corrugatedfeedhorns, test-bed cryogenic setup and custom readout electronics.
The first prototype will be an Al LEKID resonators, sensitive to the total power, and coupled directly to the exit
aperture of the corrugated feedhorns. The second prototype will be an OMT at the output of each feedhorn, withthe outputs of the two OMTs feeding two independent Al LEKIDs on the wafer. Corrugated, dual-profile feed hornantennas and waveguide ortho-mode transducers (OMTs) represent, nowadays, the best devices to couple microwave
signals.
An important problem of KIDs in space is their sensitivity to cosmic rays (CR). CR crossing the Si wafer produce
ioniziation, this is converted into phonon, producing large glitches in the detected signals. One possible solution
is a phonon-absorbing superconductor layer deposited on a face of the wafer, which reduces very significantly the
propagation and energy of phonons towards the resonators. Another possible solution is micromaching of siliconwafer, this technique could be used to minimize silicon volume below the resonator.
category : Applications355

PE-45 The performance of the Athena X-ray Integral Field Unit at very high count
rates
Philippe Peille1 , Thomas Dauser2 , Christian Kirsch3 , Roland den Hartog4 , Edoardo Cucchetti5 , Joern Wilms6 ,Didier Barret7 , Jan-Willem den Herder8 , Luigi Piro9
1

Centre National d’Etudes Spatiales, 2 ECAP, University of Erlangen-Nuremberg , 3 ECAP, University of Erlangen-Nuremberg, 4 SRON, Netherlands Institute for Space Research , 5 IRAP CNRS / Universite Toulouse III Paul Sabatier , 6 ECAP,
University of Erlangen-Nuremberg , 7 IRAP CNRS / Universite Toulouse III Paul Sabatier , 8 SRON, Netherlands Institute forSpace Research , 9 Istituto di Astrofisica e Planetologia Spaziali

The Athena X-ray Integral Field Unit (X-IFU) will operate at 90 mK a matrix of 3840 Transition-Edge Sensor pixels
providing spatially resolved high resolution spectroscopy (2.5 eV FWHM up to 7 keV) between 0.2 and 12 keV. During
the observation of very bright X-ray sources, the X-IFU detectors will receive high photon rates going up to several
tens of counts per second per pixel and hundreds per readout channel, well above the normal operating mode of the
instrument. In this contribution, we investigate through detailed End-to-End simulations the performance achieved by
the X-IFU up to Crab-like fluxes. Special care is notably taken to model and characterize pulse processing limitations
assuming diﬀerent reconstruction methods, readout-chain saturation eﬀects, as well as the non-Gaussian degradationof the energy redistribution from crosstalk at the focal plane level (both thermal and electrical). Overall we showthat more than 50 % throughput at 1 Crab in the 5 to 8 keV band can be achieved with better than 10 eV average
resolution with the inclusion of a Beryllium filter, enabling breakthrough science in the field of bright sources, as
illustrated by the simulation of representative science cases.
category : Applications356

PE-46 The Design of Whiskers, the Lynx X-ray Microcalorimeter
Simon Richard Bandler1 , Michael Dipirro2 , Megan E. Eckart3 , Kazuhiro Sakai4 , Stephen J. Smith5 , Douglas
Bennett6 , Vincent Kotsubo7 , Benjamin Mates8 , Daniel Swetz9 , Joel N. Ullom10 , Kent D. Irwin11 , Stephen E.
Kuenster12 , Daniel McCammon13 , Enectali Figueroa-Feliciano14 , Kevin Ryu15 , Ben Zeiger16 , Jeﬀrey Olson17 ,Douglas Swartz18 , Wonsik Yoon19
1

X-ray Astrophysics Laboratory, NASA - Goddard Space Flight Center, 2 NASA - Goddard Space Flight Center , 3 NASA Goddard Space Flight Center , 4 NASA - Goddard Space Flight Center / University of Maryland - Baltimore County , 5 NASA
- Goddard Space Flight Center / University of Maryland - Baltimore County , 6 National Institute of Standards andTechnology , 7 National Institute of Standards and Technology , 8 National Institute of Standards and Technology , 9 National
Institute of Standards and Technology , 10 National Institute of Standards and Technology , 11 Stanford University , 12 Stanford
University , 13 University of Wisconsin , 14 Northwestern University , 15 Massachusetts Institute of Technology - Lincoln
Laboratories , 16 Luxel , 17 Lockheed Martin Space Systems , 18 NASA - Marshall Space Flight Center , 19 NASA - Goddard
Space Flight Center

Lynx is an x-ray telescope, one of four large satellite mission concepts currently being studied by NASA to be thenext flagship mission after WFIRST. One of Lynx s three instruments is an imaging spectrometer named Whiskers,
an x-ray microcalorimeter behind an X-ray optic with an angular resolution of 0.5 arc-seconds and approximately 3
m2 of area at 1 keV. Whiskers will provide unparalleled diagnostics of distant extended structures and in particularwill allow the detailed study of the role of cosmic feedback in the evolution of the Universe.
We discuss the design of the baseline configuration and a number of options for increasing the capabilities tomaximize the scientific return of the Lynx observatory. We discuss the design of Whiskers, including transition-edge
sensors (TES) versus metallic magnetic calorimeters (MMC), pixel layout, and readout options relative to the four
key instrument requirements: energy resolution, energy range, pixel size, and count-rate. Each option is assessed interms of read-out complexity, cryogenic cooling requirements, technical readiness of the approach, and ultimate mass,
power, and cost of the instrument. In particular we will discuss the use of microwave SQUIDs, HEMT amplifiers, andparametric amplifiers for the read-out.
The baseline configuration utilizes a central 5 arc-minute region consisting multi-absorber devices known as ”hydras”. In each hydra the temperature sensor being read out (TES or MMC) is attached to up to twenty-five 1
arc-second absorbers (pixels), 50 microns in size. Discrimination between absorbers from an x-ray event is possible
because the diﬀerent thermal links to each absorber cause characteristic pulse shapes that can be discriminated. We
will also discuss the possibility of having additional enhancements to the baseline configuration. These include: (1) asub-region of the array with pixel sizes as small as 0.5 arc-seconds to provide better angular resolution; (2) a sub-region
with energy resolution as good as 0.3 eV for energies up 1 keV, allowing the measurement of turbulence in winds
of individual galaxies; and (3) a field-of-view extension that could be as large as 20 arc-minutes using 5 arc-second
pixels, optimized for low-energy X-rays to 2 keV with an energy resolution of approximately 1 eV, allowing the studyof velocities of winds in the outer regions of groups of galaxies.
category : Applications357

PE-47 The Demonstration model of the Cryogenic AntiCoincidence detector for the
ATHENA X-IFU
Michele Biasotti1 , Andrea Argan2 , Valentina Ceriale3 , Dario Corsini4 , Matteo D’Andrea5 , Matteo De Gerone6 ,Flavio Gatti7 , Simone Lotti8 , Claudio Macculi9 , Gabriele Minervini10 , Guido Torrioli11 , Luigi Piro12
1

University of Genoa, 2 INAF-IAPS Roma , 3 Universtity of Genoa / INFN sez. Genova , 4 Universtity of Genoa / INFN sez.
Genova , 5 INAF-IAPS Roma , 6 INFN sez. Genova , 7 Universtity of Genoa / INFN sez. Genova , 8 INAF-IAPS Roma ,9INAF-IAPS Roma , 10 INAF-IAPS Roma , 11 CNR-IFN Roma , 12 INAF-IAPS RomaThe present path toward the X-IFU Flight Model (FM) foresees, as first step, a Demonstration Model (DM) necessary
to solve for technological critical aspects before the mission adoption (2020). This path is also applied to the Cryogenic
AntiCoincidence (CryoAC) detector, whose planning is to deliver its DM to the Focal Plane Assembly team (SRON),
for a subsequent integration with the TES array, by end 2017.
The CryoAC DM is constituted by one single pixel as representative model of the CryoAC Flight Model. It isa microcalorimeter based on 96 parallel connected iridium/gold TES, in which the silicon substrate is used also as
absorber. The silicon substrate has been etched, in order to control the thermal conductance, obtaining a free-standing
pixel connected to the thermal bath with silicon beams.
The main aspects to be solved for the CryoAC DM are: verification of the suspended silicon absorber at cold;
operation at 50mK bath temperature; energy threshold of 20 keV.
In this paper, we present the CryoAC DM development status, and we will show its complete design with also thestudy of silicon beam thermal conductance at low temperature. The first prototype will be presented and a preliminary
device characterization, including transition and load curves will be reported.
category : Applications358

PE-48 Detector Calibration of the Micro-X Sounding Rocket TelescopeDavid C. Goldfinger1 , Joseph S. Adams2 , Robert Baker3 , Simon R. Bandler4 , Meredith Danowski5 , Walter B.
Doriese6 , Megan E. Eckart7 , Enectali Figueroa-Feliciano8 , Sarah N.T. Heine9 , Gene C. Hilton10 , Antonia J.F.
Hubbard11 , Richard L. Kelley12 , Caroline A. Kilbourne13 , Renee Manzagol14 , Dan McCammon15 , Takashi
Okajima16 , F. Scott Porter17 , Carl D. Reintsema18 , Peter Serlemitsos19 , Stephen J. Smith20 , Patrick Wikus21
1

8

Massachusetts Institute of Technology, 2 NASA / University of Maryland , 3 NASA , 4 NASA , 5 L-3 , 6 NIST , 7 NASA ,Northwestern University , 9 Massachusetts Institute of Technology , 10 NIST , 11 Northwestern University , 12 NASA , 13 NASA
, 14 Northwestern University , 15 University of Wisconsin , 16 NASA , 17 NASA , 18 NIST , 19 NASA , 20 NASA / University of
Maryland , 21 Bruker BioSpin AG

Micro-X is a sounding rocket borne X-ray telescope that uses a Transition Edge Sensor microcalorimeter array toprovide superior energy resolution. Micro-X is a versatile instrument with plans to observe the Puppis A supernova
remnant during its first flight, as well as future observations of the Milky Way to search for X-ray signals from decaying
dark matter. Commissioning and functionality testing are complete and the thermal performance of the system has
been validated. We are currently evaluating the detector performance in the flight cryostat with the flight multiplexing
electronics. Operating in this setup has allowed us to characterize sources of detector and readout noise, as well as
to implement mitigation techniques to improve performance in anticipation of the upcoming flight. We present an
overview of important noise considerations in addition to updating the latest detector performance.
category : Applications359

PE-49 Multi-parameter gain drift correction of X-ray micro-calorimeters for the
X-ray Integral Field Unit
Edoardo Cucchetti1 , Megan E Eckart2 , Philippe Peille3 , Francois Pajot4 , Frederick Scott Porter5
1

CNRS-IRAP, 2 NASA/Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, United States , 3 CNES, 18,
avenue Edouard Belin, 31401 Toulouse Cedex 9, France , 4 IRAP CNRS, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse
Cedex 4, France / Universite de Toulouse, UPS-OMP, IRAP; Toulouse, France , 5 NASA/Goddard Space Flight Center, 8800
Greenbelt Rd, Greenbelt, MD 20771, United States

With its array of 3840 Transition Edge Sensors (TESs), the X-Ray Integral Field Unit (X-IFU) onboard Athena(2028) will provide spatially resolved high-resolution spectroscopy (2.5eV FWHM up to 7keV) from 0.2 to 12keV, with
an absolute energy scale accuracy of 0.4eV. Slight changes in the TES operating environment can cause significant
variations in its energy response function, which may result in systematic errors in the absolute energy scale. We plan
to monitor such changes via onboard X-ray calibration sources and correct the energy scale accordingly using a linear
or quadratic interpolation of gain curves obtained during ground calibration. However, this may not be suﬃcient
to meet the 0.4eV accuracy required for the X-IFU. In this contribution, we introduce a new two-parameter gain
correction technique, based on the pulse-height estimate of a calibration line and the baseline value of the pulses.
From simulated gain functions, we show that this technique can accurately correct gain drifts over the instrument
bandpass despite significant deviations in heat sink temperature, bias voltage, thermal radiation loading and linear
amplifier gain. We also address potential optimizations of the onboard calibration source and compare the performanceof this new technique with those previously used.
category : Applications360

PE-50 Development of Multi-temperature Calibrator for the TES Bolometer Camera:
System Design
Tatsuya Takekoshi1 , Kazushige Ohtawara2 , Tai Oshima3 , Shun Ishii4 , Natsuko Izumi5 , Takuma Izumi6 , Masayuki
Yamaguchi7 , Shunta Suzuki8 , Kazuyuki Muraoka9 , Akihiko Hirota10 , Fumiaki Saito11 , Shunichi Nakatsubo12 , Akira
Kouchi13 , Tetsuya Ito14 , Kazunori Uemizu15 , Yasunori Fujii16 , Yoichi Tamura17 , Kotaro Kohno18 , Ryohei Kawabe19
1

Graduate School of Informatics and Engineering, The University of Electro-Communications, 2 National Astronomical
Observatory of Japan , 3 National Astronomical Observatory of Japan , 4 National Astronomical Observatory of Japan ,5
National Astronomical Observatory of Japan , 6 National Astronomical Observatory of Japan , 7 Institute of Astronomy,
University of Tokyo , 8 Graduate School of Science, Osaka Prefecture University , 9 Graduate School of Science, Osaka
Prefecture University , 10 National Astronomical Observatory of Japan , 11 Institute of Low Temperature Science, Hokkaido
University , 12 Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency , 13 Institute of Low
Temperature Science, Hokkaido University , 14 National Astronomical Observatory of Japan , 15 National Astronomical
Observatory of Japan , 16 National Astronomical Observatory of Japan , 17 Department of Astrophysics, Nagoya University ,18
Institute of Astronomy, University of Tokyo , 19 National Astronomical Observatory of JapanWe developed a simple add-on, cryogen-free, and low power consumption calibrator for a new Transition Edge Sensor(TES) bolometer camera for the ASTE 10-m telescope. To accurately correct for the non-linearity and atmospheric
extinction, we designed a motor-driven rotating filter wheel system installed in front of the cryostat window. Thiscalibrator is required to cover the loading power under various atmospheric conditions, corresponding to precipitablewater vapor (pwv) of 0.5–4 mm. For this range of pwv, we imitated 10–150 K blackbody using the 300 K semitransparent filters. Bolometers in the cryostat were optically-coupled to the low temperature stage (4 K) inside thecryostat by spherical mirrors. In addition, moderately absorbing polystyrene plates were placed in between a sphericalmirror and the cryostat window. Various combinations of filters result in eight diﬀerent temperature, and simulate
the atmospheric emission under various weather conditions at the ASTE site.
category : Applications361

PE-51 Pyramid-type Antireflective Structures on Silicon Lenses for Millimeter-wave
Observations
Tom Nitta1 , Yutaro Sekimoto2 , Kazufusa Noda3 , Takashi Hasebe4 , Shigeyuki Sekiguchi5 , Hiroshi Matsuo6 , Makoto
Nagai7 , Agnes Dominjon8 , Wenlei Shan9 , Yosuke Murayama10 , Shogo Hattori11 , Masato Naruse12 , Nario Kuno13 ,Naomasa Nakai14
1

Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 2 National Astronomical Observatory ofJapan , 3 Oshima Prototype Engineering Co. , 4 National Astronomical Observatory of Japan , 5 National Astronomical
Observatory of Japan / the University of Tokyo , 6 National Astronomical Observatory of Japan , 7 National Astronomical
Observatory of Japan , 8 National Astronomical Observatory of Japan , 9 National Astronomical Observatory of Japan ,10
University of Tsukuba , 11 University of Tsukuba , 12 Saitama University , 13 University of Tsukuba , 14 University of Tsukuba

We are developing a 100-GHz band superconducting camera with microwave kinetic inductance detectors (MKID) for
the Nobeyama 45-m telescope. A cold optics of the camera is based on a refractive-type optics and is composed of acold baﬄe, a cold stop, IR blocking filters and two silicon lenses with 300-mm-diameter at 4 K and 154-mm-diameterat 1 K. A columnar crystal silicon manufactured by Mitsubishi Materials Electronic Chemicals Co., Ltd. is a promisingmaterial for large-diameter lenses because it is available up to 100 cm × 100 cm base material. The refractive index andthe dielectric loss tangent in the sub-millimeter frequencies were measured to be ∼ 3.42 and 1 – 5 × 10−4 , respectively,
at around 30 K.
For a silicon lens, almost 30% reflection loss is caused at the lens surface. To reduce this reflection loss, a pyramidtype antireflective subwavelength structure was designed. The structure, which has 600-µm-depth and 265-µm-period,
was simulated using an electromagnetic field simulator (Ansoft HFSS) in order to obtain the reflectance. The simulated
result shows that the reflectance from 140 to 335 GHz is less than 9%. This structure was fabricated on both sides ofa 100 mm diameter plane-convex lens with a 150 mm radius of curvature. A metal bonded V-shaped dicing blade anda homemade three-axis machine were used for the fabrication. The reflectance of the pyramid-type structures on thesilicon lens was measured by vector network analyzer. The measured result from 110 to 170 GHz was −8 to −17 dB.
category : Applications

362

363

PE-52 The Cryogenic AntiCoincidence detector for ATHENA X-IFU:
characterization of the last generation single pixel prototype (AC-S8).
Matteo D’Andrea1 , Claudio Macculi2 , Andrea Argan3 , Simone Lotti4 , Gabriele Minervini5 , Luigi Piro6 , Michele
Biasotti7 , Dario Corsini8 , Flavio Gatti9 , Guido Torrioli10
1INAF/IAPS Roma, 2 INAF/IAPS Roma , 3 INAF/IAPS Roma , 4 INAF/IAPS Roma , 5 INAF/IAPS Roma , 6 INAF/IAPS
Roma , 7 Dept. of Physics, University of Genoa , 8 Dept. of Physics, University of Genoa , 9 Dept. of Physics, University of
Genoa , 10 CNR/IFN Roma

The Advanced Telescope for High ENergy Astrophysics (ATHENA) is the second large-class mission selected in ESA
Cosmic Vision 2015-2025, with a launch foreseen in 2028 towards an L2 orbit. One of the two instruments that willalternately operate at the focal plane is the X-ray Integral Field Unit (X-IFU). The X-IFU is a cryogenic spectrometerbased on a large array of Transition Edge Sensor (TES) microcalorimeters, which will operate at a base temperatureof 50 mK, providing spatially resolved high-resolution spectroscopy (2.5 eV at 6 keV) over a 5 arcmin diameter FoV.
The X-IFU sensitivity is highly degraded by the particle background expected in L2 orbit, which is induced byprimary proton (of both galactic and solar origin) and secondary electrons. To eﬃciently veto these particles and enable
the observation of faint and diﬀuse X-ray sources, the X-IFU incorporates a TES-based Cryogenic Anticoincidence
detector (CryoAC), placed less than 1 mm below the main array.
The baseline CryoAC design foresees 4 identical pixels, each one having an active area of 1.2 cm2 , a bandpass of
20 keV - 750 keV and a separated readout chain. Each pixel is made of a suspended Silicon absorber (500 µm thick)sensed by a network of a hundred Ir:Au TESes. The TESes are uniformly distributed over the absorber surface andconnected in parallel to each other. This design takes advantage of the athermal pulse to be used as fast anticoincidence
trigger: the higher the athermal phonons collection eﬃciency, the better is the detector response.
Here we will report the characterization measurements performed on the last generation CryoAC single pixel
prototype, namely AC-S8. This sample, 1 cm2 area, incorporates 65 Ir TESes connected to an additional network of
Aluminum fingers. We will focus on the role of these Aluminum collector fins, investigating the eﬃciency improvementin the athermal phonons collection.
category : Applications364

PE-53 The Cryogenic AntiCoincidence detector for ATHENA X-IFU: improvement of
the test setup towards the Demonstration Model
Matteo D’Andrea1 , Claudio Macculi2 , Andrea Argan3 , Simone Lotti4 , Gabriele Minervini5 , Luigi Piro6 , Michele
Biasotti7 , Dario Corsini8 , Flavio Gatti9 , Guido Torrioli10 , Angela Volpe111INAF/IAPS Roma, 2 INAF/IAPS Roma , 3 INAF/IAPS Roma , 4 INAF/IAPS Roma , 5 INAF/IAPS Roma , 6 INAF/IAPS
Roma , 7 Dept. of Physics, University of Genoa , 8 Dept. of Physics, University of Genoa , 9 Dept. of Physics, University of
Genoa , 10 CNR/IFN Roma , 11 ASIThe Advanced Telescope for High ENergy Astrophysics (ATHENA) is the second large-class mission selected in ESA
Cosmic Vision 2015-2025, with a launch foreseen in 2028 towards an L2 orbit. One of the two instruments that willalternately operate at the focal plane is the X-ray Integral Field Unit (X-IFU). The X-IFU is a cryogenic spectrometerbased on a large array of Transition Edge Sensor (TES) microcalorimeters, which will operate at a base temperatureof 50 mK, providing spatially resolved high-resolution spectroscopy (2.5 eV at 6 keV) over a 5 arcmin diameter FoV.
The X-IFU sensitivity is highly degraded by the particle background expected in L2 orbit, which is induced byprimary proton (of both galactic and solar origin) and secondary electrons. To eﬃciently veto these particles and enable
the observation of faint and diﬀuse X-ray sources, the X-IFU incorporates a TES-based Cryogenic Anticoincidence
detector (CryoAC), placed less than 1 mm below the main array.
The CryoAC development schedule foresees by the end of 2017 the delivery of a Demonstration Model (DM) to
the X-IFU Focal Plane Assembly development team. The DM is a single-pixel detector based on Silicon suspended
absorber, which will address the final design of the CryoAC. It will verify some representative requirements at singlepixel level, in particular the detector operation with a 50 mK thermal bath and the threshold energy at 20 keV.
Before the delivery, test and characterization activities of the CryoAC DM prototype will be performed in the
cryogenic system at INAF/IAPS. To improve the quality of these measurements, the test facility has been recently
upgraded inserting a magnetic shielding system at the 2.5 K stage of the cryostat.
Here we will describe this cryogenic magnetic shielding system and the preliminary measurements carried out totest its performances. Furthermore, we will report the study of the noise environment, focusing on the impact of thePulse Tube Cooler operations on the detector noise spectra.
category : Applications365

PE-54 Optical Response of TES Bolometer Arrays for SAFARI
Michael Damian Audley1 , Gert de Lange2 , Jian-Rong Gao3 , Richard Hijmering4 , Pourya Khosropanah5 , Marcel
Ridder6 , Neil Trappe7
1

SRON Netherlands Institute for Space Research, 2 SRON Netherlands Institute for Space Research , 3 SRON Netherlands
Institute for Space Research / Kavli Institute of Nanoscience, Delft University of Technology , 4 SRON Netherlands Institutefor Space Research , 5 SRON Netherlands Institute for Space Research , 6 SRON Netherlands Institute for Space Research ,7
Maynooth University

We report on the optical testing of ultra-sensitive prototype horn-coupled bolmeter arrays for SAFARI, the grating
spectrometer on board the proposed SPICA satellite. SAFARI’s four bolometer arrays, coupled with a diﬀraction
grating and Martin-Puplett Fourier Transform Spectrometer (FTS), will make spectroscopic observations of the cold,
dusty Universe over the wavelength range 34 − −230 µm.
Each of SAFARI’s prototype bolometers consists of a Ti/Au transition edge sensor (TES), with a transition
temperature close to 100 mK, and a tantalum absorber on a thermally-isolated silicon nitride membrane. The nitride
membrane sits behind a few-moded feedhorn√ and in front of a hemispherical backshort. SAFARI requires extremely
sensitive detectors (N EP < 2 × 10−19 W/ Hz), with correspondingly low saturation powers, to take advantage of
SPICA’s 6-K cooled optics.
We have measured the optical eﬃciency of prototype detectors for SAFARI’s short-wave band (34 − −60 µm) andused an external FTS to explore the eﬀects of non-linearity and saturation on their spectral response. We present ourlatest measurements of the optical response of prototype arrays, compare them with simulations, and discuss them interms of the instrument performance.
category : Applications366

PE-55 Vector Beam Pattern Measurements of a large field of view Microwave Kinetic
Inductance Detector camera at 350GHz
Stephen J.C. Yates1 , Kristina K. Davis2 , Willem Jellema3 , Jochem J.A. Baselmans4 , Lorenza Ferrari5 , Ronald
Hesper6 , Kotaro Kohno7 , Vignesh Murugesan8 , David Thoen9 , Andrey M. Baryshev10
1

SRON, 2 Arizona State University, 781 Terrace Rd., Tempe, AZ, U.S.A , 3 SRON, Landleven 12, 9747 AD Groningen, The
Netherlands / Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands, 4 SRON, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands / Terahertz Sensing Group, Faculty of Electrical Engineering,
Mathematics and Computer Science, Delft University of Technology, Mekelweg 4, 2628 CD Delft, The Netherlands. , 5 SRON,
Landleven 12, 9747 AD Groningen, The Netherlands , 6 Kapteyn Astronomical Institute, University of Groningen, P.O. Box
800, 9700 AV Groningen, The Netherlands , 7 Institute of Astronomy, University of Tokyo, Tokyo 181-0015, Japan, and alsowith the Research Centre for the Early Universe, University of Tokyo, Tokyo 113-0033, Japan , 8 Institute of Astronomy,
University of Tokyo, Tokyo 181-0015, Japan, and also with the Research Centre for the Early Universe, University of Tokyo,
Tokyo 113-0033, Japan , 9 Terahertz Sensing Group, Faculty of Electrical Engineering, Mathematics and Computer Science,
Delft University of Technology, Mekelweg 4, 2628 CD Delft, The Netherlands. , 10 SRON, Landleven 12, 9747 AD Groningen,
The Netherlands / Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The
Netherlands

We present vector beam pattern measurements of a large field of view Microwave Kinetic Inductance Detector camera
at 350GHz. The angular and position dependent optical response of a receiver, its beam pattern, is given by the Efield of the detected radiation and as such is a vector with both amplitude and phase. Amplitude only measurements,
even if taken in multiple optical planes, will be an incomplete description of the optical response. As such they
will miss subtle phase errors and so not describe how a full instrument will operate in its final scientific operation
configuration on sky. With the phase information the full E-field is described, allowing the beam to be numerically
propagated in either direction to investigate the optics or optical coupling between components. This allows testing at
sub-component level or in the near field of the full instrument, which can then be used to determine and understandthe final deployed far field on sky performance. The power of this technique is widely recognised and as such the phaseand amplitude measurements are now standard procedure in phase sensitive heterodyne instruments, such as used in
ALMA. However, vector beam pattern measurements have only recently been shown to be possible with direct, power
sensitive, detector arrays: the lack of an intrinsic phase response, high pixel count and low detector speed make it morediﬃcult. Additionally, with large field of view cameras the optics become more complex so making this technique more
relevant. Measurements are presented from a large field of view camera with an array of 880 lens-antenna coupled
Kinetic Inductance Detectors. The vector beam patterns are measured using a dual optical source modulation scheme,
using multiplexing electronics allowing around 400 pixels to be simultaneously characterized. Properties across thefield of view are investigated, including defocus and Gaussian beam coupling, that would not otherwise be available
from an amplitude only beam pattern. An added advantage of the technique is that standing waves oﬀ the source canbe corrected for, important for single frequency. Finally, the dual source modulation scheme means the dynamic range
for a given modulation depth is the square of that given by a single source amplitude only measurement. This has
opened up much weaker features on the beam pattern for investigation, placing a limit on the residual in-detector-chipstray light.
category : Applications367

PE-56 PICTURE-C: A Balloon-borne Optical MKID Camera
Clinton Bockstiegel1 , Benjamin A. Mazin2 , Seth R. Meeker3 , Paul Szypryt4 , Alex B. Walter5 , Gerhard Ulbricht6 ,Giulia Collura7 , Neelay Fruitwala8 , Matthew J. Strader9 , Isabel Lipartito10 , Nicholas Zobrist11 , Gregoire Coiﬀard12 ,Miguel Daal13 , Rupert Dodkins14 , Timothy Cook15 , Kerri Cahoy16 , Supriya Chakrabarti17 , Ewan Douglas18 ,Susanna C. Finn19 , Marc Kuchner20 , Nikole Lewis21 , Anne Marinan22 , Jason Martel23 , Dimitri Mawet24 ,Christopher Mendillo25 , Gene Serabyn26 , David Stuchlik27 , Mark Swain28
1

University of California Santa Barbara, 2 University of California Santa Barbara , 3 University of California Santa Barbara ,University of California Santa Barbara , 5 University of California Santa Barbara , 6 University of California Santa Barbara /School of Cosmic Physics, Dublin Institute of Advanced Studies , 7 University of California Santa Barbara , 8 University ofCalifornia Santa Barbara , 9 University of California Santa Barbara , 10 University of California Santa Barbara , 11 University ofCalifornia Santa Barbara , 12 University of California Santa Barbara , 13 University of California Santa Barbara , 14 Universityof Oxford , 15 University of Massachusetts Lowell , 16 Massachusetts Institute of Technology , 17 University of Massachusetts
Lowell , 18 Boston University , 19 University of Massachusetts Lowell , 20 NASA Goddard Flight Center , 21 Space Telescope
Science Institute , 22 Massachusetts Institute of Technology , 23 University of Massachusetts Lowell , 24 California Institute ofTechnology , 25 University of Massachusetts Lowell , 26 Jet Propulsion Laboratory , 27 NASA Wallops Flight Facility , 28 Jet
Propulsion Laboratory
4

We present PICTURE-C, a NASA-funded mission to fly optical MKIDs on a balloon to observe circumstellar debris
disks of three nearby systems in scattered optical light in 2019. UC Santa Barbara is developing the 10,000 pixel
MKID array, cryostat, and readout electronics. The PtSi MKIDs will be optimized for 600nm with a 20% bandpass,
and will be read out with five feedlines by ten ROACH2 and custom ADC/DAC boards. The balloon will launchfrom Fort Sumner NM and fly for 24 hours, carrying the MKIDs for one night at an altitude of 40 km. The Wallops
Arc-Second Pointing system on the gondola will support a 0.6 meter primary mirror and the MKID cryostat, as well
as deformable mirrors for wavefront correction and a Vector Vortex Coronagraph to suppress the on-axis starlight.
category : Applications368

PE-57 Development of Multi-temperature Calibrator for the TES Bolometer Camera:
Deployment at ASTE
Tai Oshima1 , Kazushige Ohtawara2 , Tatsuya Takekoshi3 , Shun Ishii4 , Natsuko Izumi5 , Takuma Izumi6 , Masayuki
Yamaguchi7 , Shunta Suzuki8 , Kazuyuki Muraoka9 , Akihiko Hirota10 , Fumiaki Saito11 , Shunichi Nakatsubo12 , Akira
Kouchi13 , Tetsuya Ito14 , Kazunori Uemizu15 , Yasunori Fujii16 , Yoichi Tamura17 , Kotaro Kohno18 , Ryohei Kawabe19
1

Advanced Technology Center, National Astronomical Observatory of Japan, 2 National Astronomical Observatory of Japan ,3
Graduate School of Informatics and Engineering, The University of Electro-Communications , 4 National Astronomical
Observatory of Japan , 5 National Astronomical Observatory of Japan , 6 National Astronomical Observatory of Japan ,7
Institute of Astronomy, University of Tokyo , 8 Graduate School of Science, Osaka Prefecture University , 9 Graduate School of
Science, Osaka Prefecture University , 10 National Astronomical Observatory of Japan , 11 Institute of Low Temperature
Science, Hokkaido University , 12 Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency ,13
Institute of Low Temperature Science, Hokkaido University , 14 National Astronomical Observatory of Japan , 15 National
Astronomical Observatory of Japan , 16 National Astronomical Observatory of Japan , 17 Department of Astrophysics, Nagoya
University , 18 Institute of Astronomy, University of Tokyo , 19 National Astronomical Observatory of Japan

Extensive large-scale sky survey in the millimeter/submillimeter bands with multi color continuum camera is indispensable for eﬃciently estimating the redshift of submillimeter galaxies, studying the internal structure of hot plasma
in clusters of galaxies using the Sunyaev-Zel’dovich eﬀect, and constraining physical properties of the dust in starforming regions and the spectral index of the initial submillimeter afterglow of gamma ray bursts (GRBs). In orderfor these sensitive scientific observations, reduction of the measurement error induced by the calibration, such as the
non-linearity correction and atmospheric extinction correction, plays an important role. Therefore, we developed anddeployed a simple add-on multi temperature calibrator for our multicolor Transition Edge Sensor (TES) bolometer
camera for the ASTE (Atacama Submillimeter Telescope Experiment) aimed for simultaneous observation at observing
frequencies of 270 GHz and 350 GHz. To cover the power loading level from the atmospheric emission corresponding
to precipitable water vapor (pwv) of 0.5 mm to 4 mm, the calibrator consists of spherical mirrors to show the lowtemperature stages of the cryostat and filters with moderate opacity to mimic the eight temperature cold blackbodies.
The loading powers introduced by each filter were self-calibrated by measuring the load curves of the TES bolometerswhen a filter was placed in front of the cryostat window. Each science observation was preceded by the calibration
process, which measures the response of the TES bolometers to the atmosphere and filters of various opacity. Thenthe responsivities of TES bolometers were derived to convert its output signal to the loading power and correct for
the non-linearity inherent in its response. Furthermore, the loading power falling on the TES bolometers from atmospheric emission measured at various pwv were in good correlation with the pwv measured with the line of sightradiometer. Which enables the atmospheric extinction correction by fast and sensitive bolometers compared to theavailable radiometers with the modest sampling speed.
category : Applications369

PE-58 Super DIOS: future X-ray spectroscopic mission to search for dark baryons
Shinya Yamada1 , and DIOS team
1

Tokyo Metropolitan University,

We present an updated program of the future Japanese X-ray satellite mission DIOS (Diﬀuse Intergalactic Oxygen
Surveyor), called as Super DIOS. The goal of the mission is to search for dark baryons in the form of warm-hot intergalactic medium (WHIM) with high-resolution X-ray spectroscopy. The mission will detect redshifted emission lines
from OVII, OVIII and other ions, leading to an overall understanding of the physical nature and spatial distributionof dark baryons as a function of cosmological time scale. Original DIOS was planned as a small satellite mission which
would be launched in early 2020’s with Epsilon rocket of JAXA. Because of the new start of the program of XARM,
we will re-design the DIOS mission and propose it to be launched around 2030 as a larger satellite.
We are starting conceptual design of the satellite and on-board instruments, which should give us original sciencein the era of 2030’s. Major change will be an improved angular resolution of the X-ray telescope. Super DIOS will
have 10 arcsecond resolution, which is an improvement by a factor of about 20 over DIOS. With this resolution, mostof the contaminating X-ray sources will be separated and the level of diﬀuse X-ray background will be much reduced
after subtraction of point sources. This will give us higher sensitivity to map out the WHIM in emission. We will keep
the field of view to be 30 arcmin or larger, which is along the technical extension of the X-ray telescopes employed for
XMM-Newton. Eﬀective area will be around 1000 cm2 .
Harder technical challenge will be a new TES microcalorimeter with a pixel number of a few tens of thousands.
Super DIOS will have about 10 times more pixels than Athena, and a new readout technique such as microwave
mulplexing would be necessary for such an instrument. The mission will clearly map out the filamentary structure of
the universe from redshift 0.3 to present. We are carrying out a simulation study to see how much Super DIOS canconstrain the chemical and structural evolution of the universe, in collaboration with theory groups. Furthermore, toanalyze a plenty of plasma spectra automatically, a plasma diagnosis method using data-driven feature extraction is
being studied.
We will report the status of our study of Super DIOS, including conceptual design of the satellite with its basic
parameters. We also mention possible international collaboration for this program.
category : Applications370

PE-59 Design and optimization of multi-pixel transition-edge sensors for X-ray
astronomy applications
Stephen J Smith1 , Joseph S Adams2 , Simon R Bandler3 , James A Chervenak4 , Aaron M Datesman5 , Megan E
Eckart6 , Audrey J Ewin7 , Fred M Finkbeiner8 , Richard L Kelley9 , Antoine R Miniussi10 , Frederick S Porter11 ,Caroline A Kilbourne12 , John E Sadleir13 , Kazuhiro Sakai14 , Nicholas A Wakeham15 , Edward J Wassell16 , Wonsik
Yoon171

Center for Space Science and Technology, University of Maryland Baltimore County, 2 CRESST and University of Maryland
Baltimore County / NASA Goddard Space Flight Center , 3 NASA Goddard Space Flight Center , 4 NASA Goddard Space
Flight Center , 5 NASA Goddard Space Flight Center / SGT Inc. , 6 NASA Goddard Space Flight Center , 7 NASA Goddard
Space Flight Center , 8 NASA Goddard Space Flight Center / Wyle Information Sytems , 9 NASA Goddard Space Flight
Center , 10 CRESST and University of Maryland Baltimore County / NASA Goddard Space Flight Center , 11 NASA Goddard
Space Flight Center , 12 NASA Goddard Space Flight Center , 13 NASA Goddard Space Flight Center , 14 CRESST and
University of Maryland Baltimore County / NASA Goddard Space Flight Center , 15 NASA Goddard Space Flight Center /NASA Postdoctoral Program Fellow , 16 NASA Goddard Space Flight Center / SGT Inc. , 17 NASA Goddard Space Flight
Center / NASA Postdoctoral Program Fellow

Multi-pixel transition-edge sensors (TESs), commonly referred to as hydras , are a type of position sensitive
microcalorimeter that enables very large format arrays to be designed without commensurate increase in the numberof readout channels and associated wiring. In the hydra design, a single TES is coupled to discrete absorbers via varied
thermal links. The links act as low pass thermal filters that are tuned to give a diﬀerent characteristic pulse shapefor x-ray photons absorbed in each of the hydra sub pixels. The pre-equilibration signal, such as the pulse rise-time,is then used to determine in which pixel the photon was absorbed. The energy of the photon E is determined using a
digital optimal filter, pre-calibrated for each absorber element.
We are developing hydras with up to 25-pixels per TES for proposed future x-ray astronomy applications suchas Lynx , a large mission concept under study by NASA for the Astro-2020 Decadal Survey. The proposed Lynx
concept for the Whiskers instrument combines a sub-arcsecond x-ray optic with a micro-calorimeter spectrometer incorporating 100,000-pixel TES array, with spectral resolution better than 5 eV full-width-at-half-maximum(FWHM) in the energy band 0.2-10 keV.
In this contribution we report on the experimental results from hydras consisting of up to 20 pixels per TES. We
discuss the design trade-oﬀs between energy resolution, position discrimination and number of pixels and investigate
future design optimizations specifically targeted at meeting the readout technology considered for Lynx. We havefabricated and tested hydras with 9 pixels per TES that have demonstrated ¡Δ EFWHM¿ of 2.23 ± 0.14 eV at
1.5 keV and 2.42 ± 0.29 eV at 6 keV. The 4.5 μ m Au absorbers are on a 65 μ m pitch and are connected to a
35 × 35 μ m TES via 480 nm thick Au strips of diﬀerent lengths. We extended these designs to develop the first
prototype 20-pixel hydras. These designs utilize a hierarchical structure using trunks and branches that make it easier
to design and lay out, but require more complex position discrimination algorithms. We present results on the first
design iteration consisting of 5 clusters of 4 absorbers, where each cluster was individu-ally coupled to the TES. The
measured spectral resolution at 5.4 keV showed ¡Δ EFWHM¿ =3.39 ± 0.18 eV for all 20 pixels. For both of thesehydra designs we explore diﬀerent position discrimination algorithms for optimized position determination down toenergies of a few 100 eV. Measurements are compared to simulations using a finite-element model that qualitatively
reproduce the measured pulse shapes and is used to investigate the role of detector non-linearity with energy on theposition sensitivity.
category : Applications371

PE-60 Resolve instrument on X-ray Astronomy Recovery Mission (XARM)
Yoshitaka Ishisaki1 , Ryuichi Fujimoto2 , Masahiro Tsujimoto3 , Noriko Y. Yamasaki4 , Yuichiro Ezoe5 , Shinya
Yamada6 , Shunji Kitamoto7 , Manabu Ishida8 , Yoshitomo Maeda9 , Ryo Iizuka10 , Gregory V. Brown11 , Megan
Eckart12 , Takayuki Hayashi13 , Richard L. Kelley14 , Caroline A. Kilbourne15 , Maurice A. Leutenegger16 , Dan
McCammon17 , Hideyuki Mori18 , Takashi Okajima19 , F. Scott Porter20 , Yang Soong21 , Andrew E. Szymkowiak22
1

Department of Physics, Tokyo Metropolitan University, 2 Kanazawa University , 3 Institute of Space and Astronautical
Science, JAXA , 4 Institute of Space and Astronautical Science, JAXA , 5 Tokyo Metropolitan University , 6 Tokyo
Metropolitan University , 7 Rikkyo University , 8 Institute of Space and Astronautical Science, JAXA , 9 Institute of Space andAstronautical Science, JAXA , 10 Institute of Space and Astronautical Science, JAXA , 11 Lawrence Livermore National
Laboratory , 12 NASA Goddard Space Flight Center , 13 NASA Goddard Space Flight Center , 14 NASA Goddard Space Flight
Center , 15 NASA Goddard Space Flight Center , 16 NASA Goddard Space Flight Center , 17 University of Wisconsin , 18 NASA
Goddard Space Flight Center , 19 NASA Goddard Space Flight Center , 20 NASA Goddard Space Flight Center , 21 NASA
Goddard Space Flight Center , 22 Yale University

The X-ray Astronomy Recovery Mission (XARM) is a recovery mission of ASTRO-H/Hitomi, which is expected to belaunched in Japanese Financial Year of 2020 at the earliest. The Resolve instrument on XARM consists of an array of
6×6 silicon-thermistor microcalorimeters cooled down to 50 mK and a high-throughput X-ray mirror assembly withfocal length of 5.6 m. Hitomi was launched into orbit in February 2016, and observed several celestial objects including
the Perseus cluster and the Crab pulsar, although the operation of Hitomi was terminated in April 2016 due to thebreak-up of spacecraft. Soft X-ray Spectrometer (SXS) on Hitomi demonstrated high resolution X-ray spectroscopy of∼5 eV (FWHM) in orbit for most of pixels. The Resolve instrument is in principle a remake of Hitomi SXS and Soft
X-ray Telescope, several design changes are planned based on the lessons learned of Hitomi. For example, the vibration
isolation system for cryocoolers to have launch lock, and adding baﬄe for possible optical light leak by micrometeoroids
and orbital debris, are investigated. In addition, the gate vale of liquid helium dewar was kept closed for Hitomi, one of
the largest concern is change of detector performance after the gate valve open due to electro-magnetic interference or
optical light leak. We report the developing status of the Resolve instrument and summarize possible design changes.
category : Applications372

PE-61 Noise performance of SuperSpec: an on-chip, TiN KID based mm-wave
spectrometer
R. McGeehan1 , P. S. Barry2 , C. M. Bradford3 , S. Chapman4 , G. Che5 , P. Day6 , J. Glenn7 , S. Hailey-Dunsheath8 ,M. I. Hollister9 , A. Kovacs10 , H. G. LeDuc11 , P. Mauskopf12 , H. Nguyen13 , R. O’Brient14 , T. Reck15 , C. Ross16 , E.
Shirokoﬀ17 , C. Shiu18 , C. E. Tucker19 , J. Wheeler20 , R. Williamson21 , J. Zmuidzinas22
1

University of Chicago, 2 University of Chicago , 3 Caltech / JPL , 4 Dalhousie University , 5 Arizona State University , 6 JPL ,7
University of Colorado Boulder , 8 Caltech , 9 Caltech / JPL , 10 Caltech , 11 JPL , 12 Arizona State University , 13 Caltech ,14
JPL , 15 JPL , 16 Dalhousie University , 17 University of Chicago , 18 Caltech , 19 Cardiﬀ University , 20 University of Colorado
Boulder , 21 JPL , 22 Caltech / JPL

SuperSpec is a compact on-chip spectrometer for mm and sub-mm wave observations of high redshift dusty galaxies.
With moderate resolution (R=100-500) and large bandwidth (1.8:1), this detector s small size and highly multiplexed
readout will enable the construction of powerful multi-beam spectrometers.
The detector employs a filter bank architecture, consisting of lithographically patterned niobium superconducting
microstrip mm-wave resonators. The power admitted by each resonator is detected by a lumped element titanium
nitride (TiN) kinetic inductance detector (KID) with resonant frequencies from 100-200 MHz.
We present the characterization of the KID noise performance. The low frequency noise intrinsic to the resonators
will be critical to the design of future instruments in a range of applications. We present measurements of detector
noise for prototype devices and compare to a multi-component model as a function of temperature and power.
category : Sensor Physics & Developments373

PE-62 Characterization Tests of Thermal Filters for the ATHENA mission X-IFU
Low Temperature Detector
Marco Barbera1,2 , Ugo Lo Cicero2,1 , Luisa Sciortino1 , Giancarlo Parodi3 , Fabio D’Anca4,1 , Paolo Giglio5,4 , Salvatore
Ferruggia Bonura2,1 , Flavio Nuzzo1 , Antonio Jimenez Escobar2 , Angela Ciaravella2 , Alfonso Collura2 , Salvatore
Varisco2 , Valerie Samain6
1

Dipartimento di Fisica e Chimica - Universit degli Studi di Palermo Via Archirafi 36, 90123 Palermo, Italy, 2 Osservatorio
Astronomico di Palermo ′′ G. S. Vaiana′′ - Istituto Nazionale di Astrofisica Piazza del Parlamento 1, 90134 Palermo, Italy,
3
BCV progetti s.r.l. Via S. Orsola 1, 20123 Milano, Italy, 4 Istituto di BioFisica U.O.S. di Palermo - Consiglio Nazionale delle
Ricerche Via Ugo La Malfa 153, 90146 Palermo, Italy, 5 Dipartimento dell’Innovazione Industriale e Digitale - Università degliStudi di Palermo Viale delle Scienze, Edificio 8, 90128 Palermo, Italy, 5 Centre Spatial de Liège - Université de Liège Avenue
du Pré-Aily, B 4031 Angleur, Belgium

The X-Ray Integral Field Unit (X-IFU) is one of the two detectors of the ATHENA astrophysics space mission
approved by ESA in the Cosmic Vision Science Program (launch scheduled in 2028). The X-IFU consists of a large
array of TES micro-calorimeters that will operate at ∼50 mK inside a sophisticated cryostat. A set of thin filters,
highly transparent to the X-rays focused by the telescope, will be mounted on the dewar and the focal plane assembly
thermal/EMI/mechanical shields. These are designed to attenuate the IR radiative load avoiding energy resolution
degradation due to photon shot noise, to attenuate EM interference onto the detector and the read-out electronics,
and to protect the detector from contamination.
The adoption of ATHENA by ESA is expected at the beginning of 2020; by that time the thermal filter design has
to be consolidated, and the Technology Readiness Level 5 must be demonstrated for the selected technology. Here, we
present the current filter design based on aluminum/polyimide thin bilayer membranes supported by stainless steel
meshes. We describe the filter samples developed/procured so far, and present preliminary results from the ongoing
characterization tests.
Keywords: ATHENA mission, X-IFU, X-ray microcalorimeters, thermal filters.
category : Applications374

PE-63 MetroBeta: Beta Spectrometry with Metallic Magnetic Calorimeters in the
Framework of the European Program of Ionizing Radiation Metrology
Martin Loidl1 , Jorn Beyer2 , Lina Bockhorn3 , Christian Enss4 , Daniel Gyori5 , Sebastian Kempf6 , Karsten Kossert7 ,Riham Mariam8 , Ole Nahle9 , Matias Rodrigues10 , Marco Schmidt11
1

CEA Saclay, Laboratoire National Henri Becquerel, 2 Physikalisch-Technische Bundesanstalt (PTB), Abbestrasse 2-12, 10587
Berlin, Germany , 3 Physikalisch-Technische Bundesanstalt (PTB), Bundesallee 100, 38116 Braunschweig, Germany ,4
Kirchhoﬀ-Institute for Physics, Heidelberg University, Im Neuenheimer Feld 227, 69120 Heidelberg, Germany ,5
Kirchhoﬀ-Institute for Physics, Heidelberg University, Im Neuenheimer Feld 227, 69120 Heidelberg, Germany ,6
Kirchhoﬀ-Institute for Physics, Heidelberg University, Im Neuenheimer Feld 227, 69120 Heidelberg, Germany ,7
Physikalisch-Technische Bundesanstalt (PTB), Bundesallee 100, 38116 Braunschweig, Germany , 8 CEA, LIST, Laboratoire
National Henri Becquerel, Bat. 602 - PC111, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France , 9 Physikalisch-Technische
Bundesanstalt (PTB), Bundesallee 100, 38116 Braunschweig, Germany , 10 CEA, LIST, Laboratoire National Henri Becquerel,
Bat. 602 - PC111, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France , 11 Physikalisch-Technische Bundesanstalt (PTB),
Abbestrasse 2-12, 10587 Berlin, Germany

MetroBeta is a European project aiming at the improvement of the knowledge of the shapes of beta spectra, bothin terms of theoretical calculation and measurement. It is part of a common European program of ionizing radiation
metrology. In this context, metallic magnetic calorimeters (MMCs) are being developed for the precise measurementof the shapes of beta spectra. MMCs with the beta emitter embedded in the absorber have in the past proven to beamong the best beta spectrometers, in particular for low energy beta transitions.
New MMC designs have been optimized for five diﬀerent absorber heat capacities, enabling the measurement ofbeta spectra with Q values ranging from few tens of keV up to 1 MeV. In parallel, a new detector module has
been designed. One of the improvements compared to the previously used setups is a thermal decoupling between the
MMC and SQUID chips. This feature was added since the power dissipation in the shunt resistors of the SQUID often
prevented the MMCs to be cooled below 20 mK.
Four spectra from pure beta emitters will be measured within the project: Sm-151 (Q = 76.3 keV), C-14 (Q =156.5 keV), Tc-99 (Q = 293.8 keV) and Cl-36 (Q = 709.5 keV). Intense research and development work is devoted to
the fabrication of high quality sources from each of the nuclides and their integration with the MMC absorbers. Thisis required because in the past it has been observed that the spectra measured with sources composed of a salt can beconsiderably distorted due to the loss of a fraction of the beta energy in the salt which is then not fully converted toheat. Both (electro-) chemical and physical processes are being studied that can help to avoid this problem. Anotherstudy concerns the composition of the absorbers. For low energy spectra, simple gold or silver absorbers can be used.
However, spectra with Q values higher than 500 keV will be distorted by the escape of Bremsstrahlung from theabsorber. Monte Carlo simulations were performed to study the influence of the absorber material and the usefulnessof composite absorbers to minimize this source of spectrum distortion.
The status of the developments within the project and first measured spectra will be presented.
category : Applications375

PE-64 Development of high energy resolution and high throughput SEM-EDS
analyzer utilizing 100-pixel superconducting-tunnel-junction array toward nanometerscale elemental mapping
Go Fujii1 , Masahiro Ukibe2 , Shigetomo Shiki3 , Masataka Ohkubo4
1

National Institute of Advanced Industrial Science and Technogy, 2 National Institute of Advanced Industrial Science andTechnology , 3 National Institute of Advanced Industrial Science and Technology , 4 National Institute of Advanced Industrial
Science and Technology

An energy-dispersive X-ray spectroscopy (EDS) analyzer combined with a scanning electron microscope (SEM) is
suitable to obtain spatial and quantitative information on the elemental composition of a sample non-destructively.
In order to achieve nanometer scale resolution of the elemental analysis, it is necessary to operate a SEM at lower
accelerating voltage less than 1 keV, because electron ranges and interaction volumes in samples become significantly
small (¡ several 10 nm) at accelerating voltage of 1 keV. However, in the above condition, the material analysis byusing energy-dispersive X-ray detectors such as silicon drift detectors (SDDs) or Si(Li) detectors in the conventional
EDS analyzers is quit diﬃcult, because characteristic X-ray from samples are only soft X-ray less than 1 keV andthe energy-resolving power of conventional energy-dispersive X-ray detectors is insuﬃcient to clearly resolve such soft
X-rays.
In contrast, energy-dispersive X-ray detectors based on array of superconducting-tunnel-junctions (STJs) havesimultaneously exhibited excellent energy resolution, relatively large detection area, and high counting rate capability
for soft X-rays less than 1 keV. Our X-ray detector using 100-pixel Nb/Al/AlOx/Al/Nb STJs with 100 μ m square
has already exhibited a maximum energy resolution of about 4 eV for monochromatic 400 eV X-rays, large detection
area of 1 mm2 , and a maximum counting rate of several 100 kcps, simultaneously. The STJ array was fabricated in
the Clean Room for Analog & digital superconductiVITY (CRAVITY). We have been developing an EDS analyzer
equipped 100-pixel Nb/Al STJ array soft X-ray detector to perform the elemental analysis with nanometer scale
resolution.
In this work, as a first step we have developed a typically SEM with a tungsten filament utilizing the STJ arrayas an EDS system, which is abbreviate as SC-SEM hereafter, in order to demonstrate the throughput and the energy
resolution of the STJ array in the EDS analyzer. To improve a collection eﬃciency of the characteristic X-rays, apolycapillary collimating X-ray lens was installed in the analyzer. An X-ray spectrum acquired by using the SC-SEM
for pure BN is displayed in Fig. 1. Separate B-Kα (188 eV), C-Kα (277 eV), N-Kα (393 eV), and O-Kα (525 eV) peaks
were clearly observed. Its counting rate performance for the N-Kα line was 9.4 cps/nA, which performance was almost
the same as that of electron microprobe analyzer (EPMA), which use wavelength-dispersive X-ray spectrometers(WDS) as X-ray detectors. By replacing collimating X-ray lens for a focusing X-ray lens, the counting rate is expected
to be increased more than 600 times. The counting rate of the improved SC-SEM is almost equal to that of conventional
X-ray spectroscopy analyzers employing SSDs. The energy resolution of the SC-SEM was 10 eV for N-Kα. The energy
resolution of the SC-SEM was 7 times higher than that of the SDD, and was almost equal to that of the WDS. These
results indicate that the improved SC-SEM can realize both the high throughputs of SDDs and the high energy
resolution of WDSs.
category : Applications

376

Acceleration
voltage: 3 kV

N-Ka

C-Ka

B-Ka
O-Ka

377

PE-65 An X-ray TES detector head assembly for a STEM-EDS system and its
performance
Tasuku Hayashi1 , Haruka Muramatsu2 , Keisei Maehisa3 , Noriko N Yamasaki4 , Kazuhiro Mitsuda5 , Akira Takano6 ,Shota Yoshimoto7 , Keisuke Maehata8 , Mutuo Hidaka9 , Hirotake Yamamori10 , Toru Hara11
1

ISAS/JAXA, 2 ISAS/JAXA , 3 ISAS/JAXA , 4 ISAS/JAXA , 5 ISAS/JAXA , 6 Kyushu Univ. , 7 Kyushu Univ. , 8 Kyushu
Univ. , 9 AIST , 10 AIST , 11 NIMS

?An energy-dispersive X-ray spectroscopy (EDS) on a scanning transmission electron microscope (STEM) is a useful
tool for material analysis, biotechnology, and other researches.
Conventional semiconductor-based EDS system is sometimes insuﬃcient to resolve emission lines at closely adjacentenergies. ?Transition Edge Sensor (TES) X-ray microcalorimeter is a promising solution to overcome this problem.
?However, the low maximum counting rate of this type of detector is a significant limitation when we adopt TES-based
EDS for material analysis. ?We thus set the requirement of a maximum counting rate at 5 kcps for our STEM-EDS.
?We also set an energy resolution of FWHM < 10 eV, and an energy band of 0.5 - 15 keV as requirements.
In order to satisfy the counting rate requirement, we adopted an 8 × 8 format 64 pixel TES array (Muramatsu etal., 2016). We read the signals from 64-pixel using parallel 64 signal chains with SQUID array amplifier (SAA). We
decided to mount both the TES microcalorimeter array and 64 SAAs on the detector head at the 100 mK cryogenic
state.
?In this paper, we present the design, integration, and performance of the detector head assembly. ?The size andshape of the detector head is strongly constrained by the geometry of STEM and the 100 mK refrigerator. We adopted
a shape consisting of a rod of 12 mm ?× 12 mm × 10 cm and a 3 cm cube connected at the bottom rod. ?The detectorhead body of the mentioned shape was machined from a copper block. The 64-pixel TES array is mounted on the topof rod, while the SAAs are mounted on four surfaces of the cubic part. ?Connectors to room-temperature electronics
are also mounted on the cube surface. ?SAAs and connectors are first mounted on a superconducting sapphire circuitboard and then mounted on detector-head body. Both the SAA chips and the connectors are connected to thecircuit board using superconducting flip-chip-bonding technology. ?The TES and circuit boards are connected withsuperconducting electrodes assembled on the surface of the rod and cube (Sakai et al. 2012). ?We experienced someproblems in flip-chip bonding and the yield rate was 99.3 % at 50 mK. ?Installing the detector head on the STEM-EDS,
we confirmed the energy resolution of about 9 eV at Au Lα at a counting rate of 150 cps/pixel. In the paper we willshow more details of performance tests.
category : Applications378

PE-66 Superconducting microcalorimeters absolutely calibrated?for x-ray
spectroscopy
Joseph W Fowler1 , Bradley K Alpert2 , Douglas A Bennett3 , W Bertrand Doriese4 , Jonathan D Gard5 , Gene C
Hilton6 , Lawrence T Hudson7 , Young Il Joe8 , Kelsey M Morgan9 , Galen C O’Neil10 , Carl D Reintsema11 , Daniel R
Schmidt12 , Daniel S Swetz13 , Csilla I Szabo14 , Joel N Ullom15
1

NIST Boulder Laboratories, Boulder, Colorado, 2 US National Institute of Standards and Technology , 3 US National Instituteof Standards and Technology , 4 US National Institute of Standards and Technology , 5 US National Institute of Standards andTechnology / University of Colorado , 6 US National Institute of Standards and Technology , 7 US National Institute ofStandards and Technology , 8 US National Institute of Standards and Technology , 9 US National Institute of Standards andTechnology / University of Colorado , 10 US National Institute of Standards and Technology , 11 US National Institute ofStandards and Technology , 12 US National Institute of Standards and Technology , 13 US National Institute of Standards andTechnology , 14 US National Institute of Standards and Technology / Theiss Research , 15 US National Institute of Standards
and Technology / University of Colorado

Databases of fundamental parameters for x-ray analysis include fluorescence line energies and relative intensities, aswell as line shape information including line widths and asymmetries. Although these parameters are often consideredwell-established, this is not uniformly true. The fluorescence line energies of some elements come from measurements
made 40 to 60 years ago. Data on the lower-energy lines, such as the M lines of the heavier elements, are incomplete.
Measurements of fundamental parameters can be time consuming and challenging to calibrate reliably. The US
National Institute of Standards and Technology (NIST) is exploring a new program to improve the situation.
At the heart of this new?program are arrays of superconducting microcalorimeters, Transition-Edge Sensors (TESs).
A TES is an energy-resolving detector, which operates at its?superconducting transition temperature. Energy resolutions of 1 eV at 1500 eV and 2 eV at 5900 eV have been demonstrated, and arrays of hundreds of TESs currently
operate with 3 to 4 eV resolution at 5900 eV. Unlike a wavelength-dispersive spectrometer, the TES can cover a verybroad energy range all at once. This ability oﬀers the potential for rapid characterization of multiple emission lines.
We present results from metrological-quality data taken with an array of 100 TESs to study the positions and shapesof the L-line emission from the lanthanide elements neodymium, samarium, terbium,?and holmium. Employing thewell-characterized K lines of some 3d?transition metals as our calibration reference standards, we find that the TESs
can be calibrated to absolute accuracy of approximately 0.2 eV for use in the estimation of unknown line energies,
a level of accuracy already better in some cases than existing published uncertainties. We also discuss the general
problem of absolute calibration of TESs, which is relevant to tabletop, synchrotron, and astronomical uses of thesedevices.
category : Applications379

PE-67 TES X-Ray Spectrometer for LCLS-II
Dale Li1 , Bradley K. Alpert2 , Daniel T. Becker3 , Douglas A. Bennett4 , Gabriella Carini5 , Hsiao Mei Cho6 , William
B. Doriese7 , John E. Dusatko8 , Joseph W. Fowler9 , Josef C. Frisch10 , John D. Gard11 , Gene C. Hilton12 , Michael R.
Holmes13 , Kent D. Irwin14 , Vincent Kotsubo15 , Sang Jun Lee16 , John A.B. Mates17 , Kelsey M. Morgan18 , Kazutaka
Nakahara19 , Carl D. Reintsema20 , Daniel R. Schmidt21 , Steve Smith22 , Daniel S. Swetz23 , Jana B. Thayer24 , Charles
J. Titus25 , Joel N. Ullom26 , Daniel D. Van Winkle27 , Abigail Wessels28
1

SLAC National Accelerator Laboratory, 2 National Institute of Standards and Technology , 3 University of Colorado ,National Institute of Standards and Technology , 5 SLAC National Accelerator Laboratory , 6 SLAC National Accelerator
Laboratory , 7 National Institute of Standards and Technology , 8 SLAC National Accelerator Laboratory , 9 National Instituteof Standards and Technology , 10 SLAC National Accelerator Laboratory , 11 University of Colorado , 12 National Institute ofStandards and Technology , 13 SLAC National Accelerator Laboratory , 14 SLAC National Accelerator Laboratory / Stanford
University , 15 National Institute of Standards and Technology , 16 SLAC National Accelerator Laboratory , 17 University ofColorado , 18 University of Colorado , 19 SLAC National Accelerator Laboratory , 20 National Institute of Standards andTechnology , 21 National Institute of Standards and Technology , 22 SLAC National Accelerator Laboratory , 23 National
Institute of Standards and Technology , 24 SLAC National Accelerator Laboratory , 25 Stanford University , 26 National Instituteof Standards and Technology / University of Colorado , 27 SLAC National Accelerator Laboratory , 28 University of Colorado
4

SLAC National Accelerator Laboratory, as part of the U.S. Department of Energy Oﬃce of Science, is scheduled
to complete upgrades to its Linac Coherent Light Source (LCLS) in 2020. The new LCLS (called LCLS-II) will be
the world s highest average brightness soft x-ray source (10,000 times brighter than LCLS): a free electron laser(FEL) capable of up to one million pulses of x-ray photons per second. With such high x-ray intensities and precise
timing resolution, LCLS-II will open the door to new studies of the ultra-fast and the ultra-small. One of the four
first-light detectors for LCLS-II will be a fast soft x-ray (250-1000 eV) superconducting transition-edge sensor (TES)
spectrometer for LCLS-II designed for x-ray repetition rates of 10 kHz to 100 kHz. This spectrometer will provide an
unprecedented combination of spectral resolution and eﬃciency to the FEL community. The initial array will have
256 pixels, with upgrades planned to 2,000 and 10,000 pixels (and upgrade paths toward megapixels), an initial solid
angle of 6 milli-steradians towards nearly 2 pi steradians, energy resolution of 1 eV with an upgrade planned to 0.5
eV, and a photon eﬃciency of up to 90% for Cu L. These TES arrays will be multiplexed using microwave SQUIDs.
We present an overview of this instrument.
category : Applications380

PE-68 Recent advances in broadband, ultrahigh resolution spectroscopy of particle
induced x-rays using TES microcalorimeter arrays
Ilari Maasilta1 , Mikko Palosaari2 , Marko Kayhko3 , Kimmo Kinnunen4 , Mikko Laitinen5 , Kai Arstila6 , Randy
Doriese7 , Joe Fowler8 , Carl Reintsema9 , Dan Swetz10 , Dan Schmidt11 , Joel Ullom12 , Timo Sajavaara13
1

4Department of Physics, University of Jyvaskyla, 2 University of Jyvaskyla, Finland , 3 University of Jyvaskyla, Finland ,University of Jyvaskyla, Finland , 5 University of Jyvaskyla, Finland , 6 University of Jyvaskyla, Finland , 7 NIST, Boulder, US, 8 NIST, Boulder, US , 9 NIST, Boulder, US , 10 NIST, Boulder, US , 11 NIST, Boulder, US , 12 NIST, Boulder, US ,13
University of Jyvaskyla, Finland

We discuss the latest developments in wide energy range, energy dispersive X-ray emission spectroscopy in the particle
induced mode (PIXE) using high-energy resolution superconducting transition-edge sensor arrays. This techniqueoﬀers great promise in elemental analysis of many types of samples, especially in the diﬃcult cases where tens tohundreds of diﬀerent elements with nearly overlapping emission lines have to be identified down to trace concentrations[1]. Spectroscopy of several complex multi-element samples in the energy range 1 - 10 keV is presented. Some of thesamples have trace amount of impurities not detectable with standard silicon drift detectors (SDD). The ability to
distinguish the chemical environment of an element was also demonstrated by measuring the intensity diﬀerences andchemical shifts of the characteristics X-ray peaks of titanium compounds. We also assess the detection limits of the
new technique and demonstrate a case study of fly ash with overlapping Ti, V, Ba, and Ce peaks, where minimum
detection limits of V, Ba, and Ce were decreased by factor of 620, 400, and 680, respectively, compared to the SDD
detector [2]. Possible applications for TES-PIXE are also discussed.
[1] M. R. J. Palosaari, M. Kayhko, K. M. Kinnunen, M. Laitinen, J. Julin, J. Malm, T. Sajavaara, W. B. Doriese,
J. Fowler, C. Reintsema, D. Swetz, D. Schmidt, J. N. Ullom, and I. J. Maasilta, Phys. Rev. Applied 6, 024002 (2016).
[2] M. Kayhko, M.R.J. Palosaari, M. Laitinen, K. Arstila, I.J. Maasilta, J.W. Fowler, W.B. Doriese, J.N. Ullom,
T. Sajavaara, Nucl. Instrum. Methods Phys. Res. B, in press (2017).
category : Applications381

PE-69 Microcalorimeters for Nuclear Material Analysis
Mark P. Croce1 , Katrina Koehler2 , Andrew Hoover3 , Veronika Mocko4 , Stosh Kozimor5 , Michael Rabin6 , Kathryn
McIntosh7 , George Havrilla8 , Douglas Bennett9 , John Mates10 , Johnathon Gard11 , Dan Schmidt12 , Joel Ullom13 ,Matthew Carpenter14 , Robin Cantor15
1

Los Alamos National Laboratory, 2 Los Alamos National Laboratory , 3 Los Alamos National Laboratory , 4 Los Alamos
National Laboratory , 5 Los Alamos National Laboratory , 6 Los Alamos National Laboratory , 7 Los Alamos National
Laboratory , 8 Los Alamos National Laboratory , 9 National Institute of Standards and Technology , 10 National Institute ofStandards and Technology , 11 National Institute of Standards and Technology , 12 National Institute of Standards andTechnology , 13 National Institute of Standards and Technology , 14 STAR Cryoelectronics , 15 STAR Cryoelectronics

The capabilities of low-temperature microcalorimeters are enabling new possibilities in nuclear material analysis. We
present our recent work to develop superconducting transition-edge sensor microcalorimeters and analytical techniques
for decay energy, x-ray, and gamma-ray spectroscopy of nuclear materials. Decay energy spectroscopy, in which aradioactive sample is embedded within a microcalorimeter absorber, is an emerging technique for determining theisotopic composition of trace-level samples. For each alpha-decaying nuclide, a single peak at its unique total nuclear
decay energy (Q value) is measured. For beta-decaying nuclides, where the neutrino or antineutrino will escape theabsorber, a continuous spectrum ending at the Q value is measured. We are developing sensors and methods to enable
decay energy spectroscopy of a broad range of samples from pure certified reference materials to nuclear detonation
debris. We have demonstrated that microcalorimeter x-ray emission spectroscopy has the resolution to measure subtle
eﬀects of chemical bonding and nondestructively determine chemical speciation in nuclear materials, and are now
evaluating potential applications. Measurements over the past several years with a time-division multiplexed 256pixel microcalorimeter gamma ray spectrometer have demonstrated the advantages of improved energy resolution overhigh-purity germanium detectors. The order-of-magnitude improvement in energy resolution enables more precise andaccurate nondestructive measurement of plutonium isotopic composition, an important goal for nuclear safeguards.
High-bandwidth microwave frequency-division multiplexing will soon enable high-throughput microcalorimeter gamma
spectrometers suitable for deployment in operational nuclear facilities. We discuss the latest developments in thesethree analytical techniques, and present recent results.
category : Applications382

PE-70 Application of Calorimetric Low-Temperature Detectors for the Investigationof Nuclear Charge Distributions of Fission Fragments
Santwana Dubey1 , Artur Echler2 , Peter Egelhof3 , Patrick Grabitz4 , Manfred Mutterer5 , Werner Lauterfeld6 , Stefan
Stolte7 , Aurelien Blanc8 , Ulli Koester9 , Saskia Kraft-Bermuth10 , Pascal Scholz11 , Shawn Bishop12 , Jose Gomez13 ,Friedrich Goennenwein14
1

Institute of Physics, Johannes Gutenberg Univerity, Mainz, 2 GSI, Darmstadt, Germany / Johannes Gutenberg University,
Mainz, Germany , 3 GSI, Darmstadt, Germany / Johannes Gutenberg University, Mainz, Germany , 4 GSI, Darmstadt,
Germany / Johannes Gutenberg University, Mainz, Germany , 5 GSI, Darmstadt, Germany , 6 Johannes Gutenberg University,
Mainz, Germany , 7 Johannes Gutenberg University, Mainz, Germany , 8 ILL, Grenoble, France , 9 ILL, Grenoble, France ,10
Justus Liebig University, Giessen, Germany , 11 Justus Liebig University, Giessen, Germany , 12 Technical University,
Munchen, Germany , 13 Technical University, Munchen, Germany , 14 Eberhard Karls University, Tubingen, Germany

Calorimetric Low-Temperature Detectors (CLTDs) for heavy-ion detection have demonstrated to achieve an excellent
relative FWHM 1-5 × 10-3 and negligible pulse height defect in a wide range of ions and energies from 20 to 700 MeV.
After successful application in accelerator mass spectrometry and stopping power measurements [1,2], these detectors
were recently applied for the investigation of nuclear charge distributions of fission fragments produced by thermal
neutron induced fission, as precise fission fragment yield data are of great interest for better understanding of thefission process and in applied fields.
The experiment was performed at the high neutron flux reactor ILL, Grenoble at the LOHENGRIN mass spectrometer which filters fission fragments with respect to a specific mass, kinetic energy and ionic charge but not to
the nuclear charge. For the nuclear charge separation, we exploit the nuclear charge dependent energy loss of fission
fragments passing through a degrader foil. With the CLTDs, we measure residual energies of the fragments after
spectrometer separation and passage through a stack of SiN foils as a novel type of degrader material. Compared tothe conventional ionization-mediated detectors, the concept of CLTDs provides better or comparable energy resolution
but no pulse-height defect, both being very important for such measurements. The present CLTD array with an active
area of 15x15mm2 consists of 25 independent detector pixels made of sapphire crystals with aluminum transition-edgesensors (TES) operated at 1.5K. The windowless 4He bath cryostat containing the CLTD array was coupled to the
LOHENGRIN. Variation of absorber thickness was achieved by a remotely controlled sample changer operated inside
the cryostat, close to the CLTD array.
Using three fissile targets of 235U, 239Pu and 241Pu, the quality of nuclear-charge separation was studied forselected masses in the region 82 ? A ? 139 as a function of degrader thickness and fission-fragment kinetic energies.
For the light fragment group, the Z resolution attained matches historically best values achieved with Parylene-C
absorbers and ionization chambers, while for mass symmetry and heavy mass region substantial improvement wasobserved with the new set-up. We have gained first LOHENGRIN data on the isotopic yields in the light-mass group,
89 ? A ? 109 for 241Pu fission. Towards mass symmetry, known Z-yield data were supplemented in the range A = 110
to 112 for 241Pu, and A = 111 to 113 for 239Pu. Extended data sets were cumulated for the masses A = 92 and 96 for
235U (and 241Pu) due to special interests in the precise yields of these isotopes for studies on the reactor anti-neutrino
spectrum [3]. Furthermore, an attempt was made to extend isotopic yield measurements to the heavy-mass region,
128 ? A ? 139 to study odd-even staggering, which was hardly accessible until now. Preliminary data will be presented
for the various parts of the investigations.
[1] S. Kraft-Bermuth et al., Rev. Sc. Inst. 80, 103304 (2009)[2] A. Echler et al., J. Low Temp. Phys. 176, 1033 (2014)[3] A. A. Sonzogni et al., Phys. Rev. C 91, 011301(R) (2015)
category : Applications383

PE-71 Development of total decay energy spectrometry of alpha emitters using
Metallic Magnetic Calorimeters
Matias Rodrigues1 , Martin Loidl2 , Riham Mariam3 , Xavier-Francois Navick4
1

Laboratoire National Henri Becquerel, CEA-Saclay, FRANCE, 2 CEA, LIST, Laboratoire National Henri Becquerel, 91191
Gif-sur-Yvette Cedex, France , 3 CEA, LIST, Laboratoire National Henri Becquerel, 91191 Gif-sur-Yvette Cedex, France ,4
CEA, IRFU, SEDI, 91191 Gif-sur-Yvette Cedex, France

Total decay energy spectrometry (Q spectrometry) with cryogenic detectors is a promising technique for radionuclide
analysis of alpha emitters. It consists of embedding the radioactive sample in the detector absorber and measuring
all of the energy from the emitted particles, and the nuclear recoil. Compared with alpha spectrometry, it has theadvantage of simpler energy spectra, since each radionuclide produces a single peak at its Q-value energy, and the
Q-values for diﬀerent radionuclides tend to diﬀer by more than a few tens of keV from each other, making them readily
identifiable. Moreover, Q spectrometry is independent of the emission probabilities of the emitted particles.
We are developing Metallic Magnetic Calorimeters (MMCs) for Q spectrometry, and applying this technique tothe largest number of radionuclides, noting that some are not compatible with this technique due to high-energy
gamma-rays (which would require large absorbers) or due to extremely short or long half-lives. However, MMCs canuse large and thick gold absorbers to provide significant detection eﬃciency for gamma-rays below 100 keV. Basedon Monte Carlo simulations of the absorber detection eﬃciency and based on numerical calculations of the expectedenergy resolution, a feasibility study has identified the radionuclides compatible with a low photon escape probability
and an FWHM energy resolution of 1 keV using MMCs.
Furthermore, the first MMCs have been optimized and tested. The thermal coupling between the absorber andthe sensor was adjusted in order to obtain a rise time and a pulse height that respect the slew rate of the SQUID
electronics. Large pulse heights of 18 Φ 0 were successfully measured. The total decay energy spectrum of a Po-210
source spontaneously deposited on silver and embedded in a silver absorber has been measured. The spectrum showsa FWHM energy resolution of 1.25 keV at 5.4 MeV with a Gaussian broadening at the half maximum of 0.9 keV. The
baseline FWHM energy resolution is 0.2 keV, consistent with the resolution obtained on low energy L X-rays in the
spectrum at 14 keV. Details of this development and the results of the measurements with MMCs will be presented.

Counts / 0.11 keVQ	
  spectrum	
  of	
  Po-­‐210	
  	
  
1.25	
  keV	
  

100
60
10
5377

5382

5387

5392 5397
Energy (keV)

category : Applications

384

5402

5407

PE-72 Spectroscopic Measurement of X-rays and γ-rays Emitted by Neptunium
Sample Irradiated in the Experimental Fast Reactor Joyo using a TES
microcalorimeter
Takashi Yasumune1 , Koji Takasaki2 , Chikara Ito3 , Masashi Ohno4 , Tomoya Irimatsukawa5 , Yuya Ishii6 , Hiroyuki
Takahashi7 , Satoshi Koujiro8
1

Oarai Research and Development Center, Japan Atomic Energy Agency, 2 Japan Atomic Energy Agency , 3 Japan Atomic
Energy Agency , 4 The University of Tokyo , 5 The University of Tokyo , 6 The University of Tokyo , 7 The University of Tokyo ,8National Institute of Advanced Industrial Science and Technology

Nuclide analysis methods are roughly divided into two categories: non-destructive inspection using direct measurements of γ-rays or neutrons emitted by samples, and destructive inspection using chemical analysis technique. The
destructive inspection is more accurate but less rapidity due to its complicated procedure compared to the nondestructive inspection. In other words, the non-destructive inspection applying γ-ray spectroscopy achieve rapid
analysis. However, it is diﬃcult to γ-ray spectroscopy using conventional radiation detectors with insuﬃcient energy
resolution such as scintillation detectors or high-purity Germanium detectors makes it diﬃcult to identify nuclides
since the energies of photons emitted by transuranium elements such as Plutonium and Americium are close to eachother. In order to maintain an eﬀective nuclear safeguards, establishment of non-destructive inspection of the nuclide
elements like the spent fuel with high eﬃciency and more accuracy is necessary. These demands lead us to the precision
gamma-ray spectroscopy using superconducting transition edge sensor (TES) with ultra-high energy resolution.
To demonstrate the precision measurement of nuclear material sample using a TES microcalorimeter, spectroscopic
measurements of X-rays and γ-rays emitted by neptunium (Np) samples were performed. We measured two types
of Np samples: 237 Np irradiated by neutron in the experimental fast reactor Joyo and a non-iradiated 237 Np. The
obtained results are shown in fig.1 (see the attachment). In the energy spectrum obtained from the measurement of
non-irradiated Np sample, several energy peaks of γ-rays and characteristic X-rays emitted by the elements of 237 Np
and 233 Pa daughter of 237 Np are observed. On the other hand, energy peaks of γ-rays and characteristic X-rays
emitted by the elements of 238 Pu and 137 Cs are observed as well as energy peaks derived from 237 Np in the energy
spectrum obtained from the measurement of irradiated Np sample. 238 Pu is created from the 237 Np(n, gamma)238 Np→ 238 Pu + β reaction. 137 Cs is one of long-lived fission product created by nuclear fission.
From these results, we consider that γ-ray spectrometer using a TES microcalorimeter can be applied to theadvanced non-destructed inspection of the nuclide material.

17.7 keV Np Kβ-X

Counts(Irradiated)

50

20.8 keV Np Kγ-X
137Cs(31.817 keV

Ba Kα2-X)

137Cs(32.194 keV

40

137Cs(36.378 keV

Irradiated Np sample

Ba Kα1-X)
Ba Kβ1-X)

238Pu(43.498 keV

30

237Np(86.477 keVγ)γ)

97.069 keV Np Kα2-X
101.059 keV Np Kα1-X

20
10
0

150

237Np(29.374 keVγ)

Non-irradiated Np sample
237Np(92.282 keVγ)233Pa(75.354keV

U Kα2-X)

237Np(95.863 keV

Sn escape120

Pa Kα2-X)

233Pa(94.654keVγ)

90

Pa Kα1-X)

233Pa(98.434 keV

237Np

60

U Kα1-X)(57.1 keV γ)

30
0

20

40

60

80

100

120

Energy(keV)

Fig.1 Energy spectrum of X-rays and γ-rays emitted by an irradiated Np sample (upper) and a nonirradiated Np sample (lower).

category : Applications

385

140

Counts(Non-Irradiated)

237Np(86.477 keV

386

PE-73 Application of photon number resolving transition edge sensors for themetrology of quantum dot based light sources
Marco Schmidt1 , Jorn Beyer2 , Martin v. Helversen3 , Fabian Gericke4 , Elisabeth Schlottmann5 , Alexander Thoma6 ,Alexander Schlehahn7 , Manuel Gschrey8 , Peter Schnauber9 , Jan-Henrik Schulze10 , Andre Strittmatter11 , Sven
Rodt12 , Tobias Heindel13 , Stephan Reitzenstein14
1

Cryosensors, Physikalisch-Technische Bundesanstalt, 2 Physikalisch-Technische Bundesanstalt , 3 Institut fur Festkorperphysik,Technische Universitat Berlin , 4 Institut fur Festkorperphysik, Technische Universitat Berlin , 5 Institut fur Festkorperphysik,Technische Universitat Berlin , 6 Institut fur Festkorperphysik, Technische Universitat Berlin , 7 Institut fur Festkorperphysik,Technische Universitat Berlin , 8 Institut fur Festkorperphysik, Technische Universitat Berlin , 9 Institut fur Festkorperphysik,Technische Universitat Berlin , 10 Institut fur Festkorperphysik, Technische Universitat Berlin , 11 Institut fur Experimentelle
Physik, Otto-von-Guericke Unversitat Magdeburg , 12 Institut fur Festkorperphysik, Technische Universitat Berlin , 13 Institut
fur Festkorperphysik, Technische Universitat Berlin , 14 Institut fur Festkorperphysik, Technische Universitat Berlin

Light emitting devices based on semiconductor quantum dots (QD) are considered as promising candidates for future
photonic technologies. They will pave the way for applications in the fields of quantum information, quantum computation and quantum metrology. Photon number resolving (PNR) detectors are very attractive optical characterization
tools for such quantum devices as they provide direct access to the photon number distribution and the photon statistics, which allows one to gain detailed knowledge about the quantum optical properties of QD-based quantum lightsources.
In this work, we report on setting up and calibrating of a detection system based on fiber-coupled Tungsten
transition-edge sensors (W-TESs) [1]. The stand-alone system comprises two W-TESs read out by two 2-stage-SQUID
current sensors, which are operated in a compact detector unit integrated in an adiabatic demagnetization refrigerator
with a base temperature of 100 mK. Fast low-noise analog amplifiers and digitizers are used for signal acquisition. The
detection eﬃciency of the single-mode fiber-coupled detector system in the relevant wavelength Range (850 -950 nm)
is determined to be larger than 81%. As a first application in QD-metrology, we employ this detector to evaluate theperformance of diﬀerent types of QD-based light sources. For instance, we determine the photon number distributionof single-QD sources emitting triggered single-photon and twin-photon states [2].
This first application of photon number resolving detectors in the field of QD-based quantum metrology opens up
new routes towards applications of quantum light sources in quantum information, quantum-enhanced sensing andquantum metrology.
[1] Lita, Adriana E. et al., Counting near-infrared single-photons with 95% eﬃciency, Optics Express, vol. 16, issue
5, p. 3032 (2008)[2] Heindel, T. et al. A bright triggered twin-photon source in the solid state. Nat. Commun. 8, 14870 doi:
10.1038/ncomms14870 (2017)
category : Applications387

PE-74 Total eﬃciency calibration of a metallic magnetic calorimeter detector forphoton spectrometry below 100 keV.
Riham Mariam1 , Matias Rodrigues2 , Martin Loidl3
1National labotory of henry beacquerel : LNHB CEA-Saclay , 2 CEA, LIST, Laboratoire National Henri Becquerel(LNE-LNHB), CEA-SACLAY 91191 Gif/Yvette cedex, France. , 3 CEA, LIST, Laboratoire National Henri Becquerel(LNE-LNHB), CEA-SACLAY 91191 Gif/Yvette cedex, France.

L X-ray and gamma emission intensities are fundamental parameters for the quantitative assay of radioactive material
by photon spectrometry. However, they are not very well known or even unknown for many actinides below 100 keV.
Due to the numerous L X-ray emissions within a narrow energy range, their separation is not possible using HPGe
detectors. To complete the knowledge of photon emissions of actinides and improve their quantification, an ultrahigh resolution spectrometer is needed. Therefore CEA-LNHB developed a Metallic Magnetic Calorimeter (MMC)
spectrometer with 4 pixels employing silver-gold bilayer absorbers to obtain a constant eﬃciency below 25 keV andan energy resolution about 30 eV.
Absolute determination of L X-ray emission intensities necessitates a good knowledge and accurate calibration of
detection eﬃciency. To cover the energy range below 100 keV, measurements of many standard sources are needed.
However, cooling down the detector with the source for each radionuclide would be time consuming and expensive.
So, we have combined Monte Carlo simulations of the eﬃciency curve with sampling eﬃciency at various energies
by measuring only one standard source. In this work we will show and discuss about the total eﬃciency calibrationof the MMC by combining Monte-Carlo simulation (using PENELOPE 2014) with the measurement of a reference
source of Am-241, one of the best-known radionuclides for photons of low energies. In addition an algorithm based on
the extended dead time has been created to determine the live time required for total eﬃciency calibration. We havesuccessfully measured the total eﬃciency, through the intensities of L-X-ray groups and gamma emission below 100
keV (Np L α L β L γ L η & L ι and gamma emission at 26, 33, 43, and 59 keV).
The accuracy of the Monte Carlo simulations strongly depends on the uncertainties of the simulated geometry.
Dimensional measurements are not precise enough to ensure precise simulations. Therefore the geometry in the MC
simulations (thickness and position of the individual absorbers with respect to the collimator, source position) wasestablished in an iterative way, adapting the results of the initial simulation to the measured intensities of the reference
source. This corrected geometry will be used in future, for measurements of emission intensities for diﬀerent source
dimensions and source-detector distances simply by applying eﬃciency correction by Monte Carlo simulations.
category : Applications

388

PE-75 Calibration of Ge and Si Ionization Yield using Phonon Detectors with
Luke-Neganov Amplification
Noemie Bastidon1
1

Department of Physics and Astronomy, Northwestern University

The SuperCDMS collaboration is currently planning to do a calibration of the ionization yield and nuclear recoil energy
scale of Ge and Si crystals to 100 eVnr. These measurements will be performed using cryogenic phonon detectors
biased at 100V using Luke-Neganov amplification. Two phases of calibration are planned. First, a small-scaledetector (1 cm x 1 cm x 1 mm) will be calibrated at the Triangle Universities Nuclear Laboratory (TUNL) using amonoenergetic neutron beam of 40 keV. In a second phase, a full-scale SuperCDMS SNOLAB HV prototype detector
will be calibrated using a 2.5 MeV DD (deuterium-deuterium) neutron generator and a custom-built backing detector
array at the Northwestern EXperimental Underground Site at Fermilab (NEXUS@FNAL). In this poster we discuss
the simulation and optimization of the calibration campaign, and give an update on the testing of the small-scaledetectors in preparation for the TUNL campaign.
category : Applications

389

PE-76 A high-resolution x-ray spectrometer for a kaon mass measurement
Ken Suzuki1 , Kevin Phelan2 , Daniele Tortorella3 , Johann Zmeskal4 , Matthias Buhler5 , Theo Hertrich6 , Andreas
Fleischmann7
1

Stefan Meyer Institute, Austrian Academy of Sciences, 2 Stefan Meyer Institute, Austrian Academy of Sciences , 3 Payr
Engineering GmbH , 4 Stefan Meyer Institute, Austrian Academy of Sciences , 5 Low Temperature Solutions UG , 6 Low
Temperature Solutions UG , 7 Kirchhoﬀ-Institut fur Physik, Heidelberg

The ASPE!CT consortium (Adaptable Spectrometer Enabled by Cryogenic Technology) is currently constructing
a generalised cryogenic platform for cryogenic detector work which will be able to accommodate a wide range ofsensors. The cryogenics system is based on a small mechanical cooler with a further adiabatic demagnetisation
stage and will work with cryogenic detectors at sub-Kelvin temperatures. The commercial aim of the consortium
is to produce a compact, user-friendly device with an emphasis on reliability and portability which can easily betransported for specialised on-site work, such as beam-lines or telescope facilities. The cryogenic detector platform willaccommodate a specially developed cryogenic sensor, either a metallic magnetic calorimeter or a magnetic penetrationdepth thermometer. The detectors will be designed to work in various temperatures regions with an emphasis on
optimising the various detector resolutions for specific temperatures. One resolution target is of about 10 eV atthe energies range typically created in kaonic atoms experiments (soft x-ray energies). A following step will see theintroduction of continuous, high-power, sub-Kelvin cooling which will bring the cryogenic basis for a high resolution
spectrometer system to the market. The scientific goal of the project will produce an experimental set-up optimised
for kaon-mass measurements performing high-resolution x-ray spectroscopy on a beam line provided foreseeably by
the J-PARC (Tokai, Japan) or DA Φ NE (Frascati, Italy)
category : Applications390

PE-77 Development of hard X-ray TES microcalorimeters using microwave
multiplexing for synchrotron science
Umeshkumar M. Patel1 , Ralu Divan2 , Lisa M. Gades3 , Timothy J. Madden4 , Antonino Miceli5 , Orlando Quaranta6 ,Daikang Yan7 , Daniel Becker8 , Doug A. Bennett9 , James Hays-Wehle10 , Gene C. Hilton11 , Johnathon Gard12 , John
A. B. Mates13 , Kelsey M. Morgan14 , Carl D. Reintsema15 , Daniel R. Schmidt16 , Daniel S. Swetz17 , Joel N. Ullom18 ,Leila Vale19
1

X-ray Science Divison, Argonne National Laboratory, 2 Argonne National Laboratory ? USA , 3 Argonne National Laboratory? USA , 4 Argonne National Laboratory ? USA , 5 Argonne National Laboratory ? USA , 6 Argonne National Laboratory ?
USA , 7 Argonne National Laboratory ? USA / Northwestern University - USA , 8 National Institute of Standards andTechnology ? USA / University of Colorado, Boulder - USA , 9 National Institute of Standards and Technology ? USA ,10
National Institute of Standards and Technology ? USA , 11 National Institute of Standards and Technology ? USA ,12
National Institute of Standards and Technology ? USA / University of Colorado, Boulder - USA , 13 National Institute ofStandards and Technology ? USA / University of Colorado, Boulder - USA , 14 National Institute of Standards andTechnology ? USA , 15 National Institute of Standards and Technology ? USA , 16 National Institute of Standards andTechnology ? USA , 17 National Institute of Standards and Technology ? USA , 18 National Institute of Standards andTechnology ? USA / University of Colorado, Boulder - USA , 19 National Institute of Standards and Technology ? USA

Transition edge sensor (TES) spectrometers oﬀer great potential for applications in hard X-ray science including
chemically sensitive X-ray microscopy at scanning nanoprobes, dilute sample XAFS, energy-dispersive diﬀraction, andCompton scattering. The Advanced Photon Source at Argonne National Laboratory is the premier hard X-ray facility
in the US and is embarking on a major facility upgrade (APS-U). As part of the upgrade, nine new beamlines will be
constructed. Three of these nine flagship beamlines would greatly benefit from hard X-ray TES spectrometers (i.e.,
In-situ Nanoprobe, Ptychoprobe, Polarization Modulation Spectroscopy). To meet the needs of the APS-U, there
are two critical development needs for hard X-ray TESs: 1.) improvements in thick absorber performance and 2.)
improvements in count rate throughput. We describe results of a small-scale TES array with absorbers made of gold
and gold with electroplated or evaporated bismuth to study the influence of film properties on the low energy tails
in energy spectra. Finally, we present results on the use of a new readout technology for TESs, developed at NIST,
based on the use of superconducting microwave resonators in combination with SQUID amplifiers. In particular, we
describe results of its performance when used to read out hard X-ray TESs.
category : Applications

391

PE-78 Low-Energy X-ray Spectroscopy down to 50 eV using a TES microcalorimeter
Keiichi Tanaka1 , Atsushi Nagata2 , Satochi Nakayama3 , Kazuo Chinone4 , Kazuhisa Mitsuda5 , Toru Hara6
1
4

Hitachi High-Technologies Corporation, 2 Hitachi High-Tech Science Corporation , 3 Hitachi High-Tech Science Corporation ,Hitachi High-Tech Science Corporation , 5 Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 6 National Institute for Materials Science

An energy dispersive spectroscopy (EDS) combined with electron microscope is widely used to analyze the elements
contained in a sample because an EDS can detect X-rays in a wide energy range of typically 0.15 to 20 keV witha single detector. However the energy resolution of conventional silicon based detector is limited to 100 to 200 eV
FWHM. A TES (Transition edge sensor) microcalorimeter is a new type of EDS with a high energy resolution (¡ 10eV). The TES enables detecting small peaks generated by minor elements which are buried underneath tails of large
peaks of major elements for Si detectors. The peak separation ability is important especially when we analyze elements
using X-ray peaks under 1 keV because the K lines of light elements and L lines of transition metal and M lines ofheavy metals are closely packed. However, ability to detect such low energy lines are often limited with the entrance
window and optical blocking filters of the cryogenic system, even though the noise level of the detector is much below
the X-ray energy.
In this paper, we report the results of the X-ray detection experiments for lines blow 1 keV with our TES system.
The energy resolution of our TES is 7 eV for Al-K line. We used the metal samples (Mg, Al, Si) excited by electron
bombardment to create low energy lines.
We detected not only K and L emission lines of those elements but also bound-free emission which is caused byvalence band to L shell transitions of electrons. The upper cut-oﬀ energies of the emission appear at 49.6eV、69.1eV、93.8 eV, respectively for Mg, Al, Si.
We will discuss the consistency between the L to K line intensity ratios of the three elements and the X-ray
transmission of the entrance window and blocking filters.
category : Applications392

PE-79 Using a TES microcalorimeter spectrometer as a novel probe of heterogeneousquantum materials
Daniel Swetz1 , Peter Abbamonte2 , Gilberto de la Pena3 , William Doriese4 , Yizhi Fang5 , Joseph Fowler6 , Gene
Hilton7 , Young Il Joe8 , Sangjun Lee9 , Jessica McChesney10 , Kelsey Morgan11 , Carl Reintsema12 , Fanny Rodolakis13 ,Daniel Schmidt14 , Xiaolan Sun15 , Joel Ullom16
1

NIST, 2 University of Illinois, Department of Physics , 3 University of Illinois, Department of Physics , 4 National Institute ofStandards and Technology , 5 University of Illinois, Department of Physics , 6 National Institute of Standards and Technology ,7
National Institute of Standards and Technology , 8 National Institute of Standards and Technology , 9 University of Illinois,
Department of Physics , 10 Argonne National Laboratory, Advanced Photon Source , 11 National Institute of Standards andTechnology , 12 National Institute of Standards and Technology , 13 Argonne National Laboratory, Advanced Photon Source ,14
National Institute of Standards and Technology , 15 University of Illinois, Department of Physics , 16 National Institute ofStandards and Technology

Despite more than 30 years of intense research, the physical mechanism that causes high-temperature superconductivity
remains a mystery. ?One intriguing property of high-temperature superconductors that may be a source of insight
into the pairing mechanism is the presence of spatial variations in the charge density. Progress understanding thesevariations has been limited, in part, by a lack of instrumentation that can readily observe these variations. X-rays
that undergo resonant scattering from the correlated electrons can be used to observe charge density variations, butwork to date has struggled to detect the small scattered x-ray signal above a large incoherent x-ray background fromfluorescence. ?Recently, the NIST Quantum Sensors Group has pioneered a new x-ray spectrometer based on arrays ofsuperconducting TES microcalorimeters that have the sensitivity to separate the scattered signal from the backgroundof fluoresced photons. ?
The QSG, working with researchers at the University of Illinois - Urbana Champaign and Argonne National
Laboratory, have installed a TES spectrometer at the Advanced Photon Source beamline 29. The instrument achievesenergy resolution as good as 1. 0 eV below 1 keV. Here, we present the first resonant scattering measurements with this
instrument from a cooled high-temperature superconducting crystal of La2-xBaxCuO4 (x=0.125). We demonstrate
the detection of the charge density wave (CDW) that arises from the correlated electrons as a function of beam energy
and sample angle. Using the exquisite resolution of the TES detector, we are able to separate the CDW signal from thefluorescent background. We also present a measurement of the d-d excitation that resides 2 eV below the (002) Bragg
scattering peak. Finally, we will compare the capability of TES spectrometers to multi-channel plate area detectors
and grating spectrometers and show that the TES provides roughly 2 orders of magnitude increase in sensitivity. The
increased sensitivity of the TES spectrometer will allow researchers to probe broad classes of correlated electronicmaterial systems for the first time.
category : Applications393

PE-80 TES x-ray detectors for high eﬃciency spectroscopy of hemoglobin and otherproteins
Charles James Titus1 , Sang Jun Lee2 , Michael Baker3 , Brad Alpert4 , Doug Bennett5 , W. Bertrand Doriese6 , Joe
Fowler7 , Kelly Gaﬀney8 , Johnathan Gard9 , Gene Hilton10 , Kent Irwin11 , Young Joe12 , Chris Kenney13 , Dale Li14 ,Kelsey Morgan15 , Dennis Nordlund16 , Hirohito Ogasawara17 , Galen C. O’Neil18 , Carl Reintsema19 , Dan Schmidt20 ,Dimosthenis Sorakas21 , Dan Swetz22 , Joel Ullom23 , Tsu-Chien Weng24 , Christopher Williams25 , Betty Young26
1Department of Physics, Stanford University, 2 Stanford University, Stanford, CA, United States / SLAC, Menlo Park, CA,
United States , 3 Stanford University, Stanford, CA, United States , 4 NIST, Boulder, Co, United States , 5 NIST, Boulder, Co,
United States , 6 NIST, Boulder, Co, United States , 7 NIST, Boulder, Co, United States , 8 SLAC, Menlo Park, CA, UnitedStates , 9 NIST, Boulder, Co, United States , 10 NIST, Boulder, Co, United States , 11 Stanford University, Stanford, CA,
United States / SLAC, Menlo Park, CA, United States , 12 NIST, Boulder, Co, United States , 13 SLAC, Menlo Park, CA,
United States , 14 SLAC, Menlo Park, CA, United States , 15 NIST, Boulder, Co, United States , 16 SLAC, Menlo Park, CA,
United States , 17 SLAC, Menlo Park, CA, United States , 18 NIST, Boulder, Co, United States , 19 NIST, Boulder, Co, UnitedStates , 20 NIST, Boulder, Co, United States , 21 SLAC, Menlo Park, CA, United States , 22 NIST, Boulder, Co, United States ,23
NIST, Boulder, Co, United States , 24 SLAC, Menlo Park, CA, United States , 25 Stanford University, Stanford, CA, UnitedStates , 26 Stanford University, Stanford, CA, United States / Santa Clara University, Santa Clara, CA, United States

Many fundamental questions about metal-centered proteins, including hemoglobin and photosystem-II, can in principle
be addressed with X-ray spectroscopy, but they remain unsolved because of the low eﬃciency of presently available
x-ray spectrometers. TES x-ray spectrometer arrays oﬀer a unique combination of large active area and good energy
resolution, enabling a powerful new probe of these bioinorganic complexes. We present preliminary results from a 240pixel Transition-Edge-Sensor (TES) array that we have deployed at the Stanford Synchrotron Radiation Lightsource(SSRL). For the first time, this spectrometer makes it possible to apply x-ray spectroscopy techniques, including
partial fluorescence yield x-ray absorption spectroscopy (PFY-XAS) and resonant inelastic x-ray scattering (RIXS),
to the transition metal L edges in dilute proteins. In this poster, we demonstrate our ability to measure ultra-dilute
samples and present preliminary data on hemoglobin that have direct relevance to a long-standing debate about thenature of the iron-oxygen bond.
category : Applications394

PE-81 Development of Polycapillary Optics for STEM?TES?EDS
Akira Takano1 , Keiichi Tanaka2 , Keisuke Maehata3 , Tasuku Hayashi4 , Kazuhisa Mitsuda5 , Toru Hara6
1

Hitachi High-Tech Science, 2 Hitachi High-Tech Science , 3 Kyushu Univ. , 4 JAXA , 5 JAXA , 6 NIMS

Scanning transmission electron microscope (STEM) allows direct observation of the nanoscale structure with a highspatial resolution. An energy dispersive spectrometer (EDS) performed on a STEM plays an important role in a wide
range of science. A Si (Li) semiconductor detector (SSD) is used for detecting X-rays in a typical energy dispersive
spectroscopy (EDS). An insuﬃcient energy resolution of SSD results in peak overlaps of closely adjacent peaks andhinders high accuracy analysis. A superconducting transition edge sensor (TES) microcalorimeter system has beendeveloped for improving the energy resolution of an EDS performed on STEM. The objective lens of the STEM
generates a strong magnetic field in the specimen chamber, which makes it diﬃcult to operate the TES microcalorimeter
without degrading the energy resolution. Therefore, the TES microcalorimeter has been placed outside the STEM
column. To increase the eﬀective detection solid angle, we employed polycapillary optics. The X-ray transmission
characteristics of the polycapillary optics such as a focal spot size and an intensity gain depend on geometricalarrangements of the optics and the X-ray energy. The counting rate of the single-pixel TES microcalorimeter was
300 cps when using the polycapillary optics. However, a counting rate of 300 cps is insuﬃcient for practical STEM
operation. To achieve the counting rate larger than 5000 cps, we are now conducting development of a 64-pixel array
TES microcalorimeter.
In this work, the X-ray transmission characteristics of the polycapillary optics were evaluated by analyzing resultsof energy spectrum measurements of X-rays transmitted by the polycapillary optics installed in the STEM. Then
we made a simulation model that reproduces experimental results. Polycapillary optics for a 64-pixel array TES
microcalorimeter was designed with using the simulation model for evaluating X-ray transmission characteristics. We
performed energy spectrum measurements of X-rays transmitted by the fabricated polycapillary optics for a 64-pixel
array TES microcalorimeter.
category : Applications395

PE-82 Development of MMC gamma detectors for precise measurements of uranium
isotopesGeon-Bo Kim1 , Sebastian Kempf2 , Loredana Gastaldo3 , Andreas Fleischmann4 , Christian Enss5 , Stephan Friedrich6
1

Lawrence Livermore National Laboratory, 2 Heidelberg University , 3 Heidelberg University , 4 Heidelberg University ,5
Heidelberg University , 6 Lawrence Livermore National Laboratory

Precise gamma-ray energies and branching ratios from nuclear decays are important for non-destructive assay innuclear safeguards. We are developing high energy resolution gamma detectors using metallic magnetic calorimeters(MMCs) to measure and improve nuclear decay properties of uranium isotopes. We have shown that our MMC gamma
detectors have good linearity and reproducibility, which makes them suitable for safeguards applications. We discuss
the performance of MMC gamma detectors, and present initial measurements from a mixed-isotope uranium source.
category : Applications396

PE-83 Compact measurement system to study scintillation and phononic propertiesof scintillating crystals at low temperatures
Hyelim Kim1 , J.A. Jeon2 , H.S. Jo3 , C.S. Kang4 , G.B. Kim5 , H.J. Kim6 , I. Kim7 , S.R. Kim8 , Y.H. Kim9 , D.H.
Kwon10 , C. Lee11 , H.J. Lee12 , S.H. Lee13 , S.Y. Oh14 , J.H. So15
1

Center for Underground Physics, Institute for basic science, 2 Center for Underground Physics, Institute for Basic Science ,Center for Underground Physics, Institute for Basic Science , 4 Center for Underground Physics, Institute for Basic Science ,5
Center for Underground Physics, Institute for Basic Science , 6 Department of Physics, Kyungpook National University, ,7Center for Underground Physics, Institute for Basic Science , 8 Center for Underground Physics, Institute for Basic Science ,9
Center for Underground Physics, Institute for Basic Science , 10 Center for Underground Physics, Institute for Basic Science ,11
Center for Underground Physics, Institute for Basic Science , 12 Center for Underground Physics, Institute for Basic Science ,13
Center for Underground Physics, Institute for Basic Science , 14 Korea Research Institute of Standards and Science ,15
Center for Underground Physics, Institute for Basic Science3

A metallic magnetic calorimeter (MMC) is one of the most sensitive detector technologies used in low temperaturedetectors (LTDs). On the other hand, the study on absorber crystals is another important subject in the applicationof LTDs to rare event search experiments such as neutrinoless double beta decay searches. We developed a compact
heat and light detection system to investigate various crystals using MMC sensors. The heat measurement channel isdesigned for a cubic crystal in a standard dimension of 1 x 1 x 1 cm3. A Ge wafer in 15 x 15 x 0.5 mm3 is used for theabsorber of the light detection. We will report recent results with the compact measurement system for scintillating
crystals of CaMoO4 and Na2Mo2O7.
category : Applications397

PE-84 Transition-edge-sensor microcalorimeters for mass spectrometric identificationof neutral molecules
Shinji Okada1 , Toshiyuki Azuma2 , Douglas Alan Bennett3 , William Bertrand Doriese4 , Joseph W. Fowler5 , Tadashi
Hashimoto6 , Ryota Hayakawa7 , James Hays-Wehle8 , Gene Hilton9 , Yuto Ichinohe10 , Yoshitaka Ishisaki11 , Susumu
Kuma12 , Toshio Nakano13 , Yuji Nakano14 , Hirofumi Noda15 , Galen C. O’Neil16 , Carl D. Reintsema17 , Daniel R.
Schmidt18 , Daniel S. Swetz19 , Hideyuki Tatsuno20 , Shutaro Ueda21 , Joel N. Ullom22 , Shinya Yamada23
1

AMO Physics Laboratory, RIKEN, 2 RIKEN , 3 NIST , 4 NIST , 5 NIST , 6 JAEA , 7 TMU , 8 NIST , 9 NIST , 10 TMU , 11 TMU ,12
RIKEN , 13 RIKEN , 14 Rikkyo Univ. , 15 Tohoku Univ. , 16 NIST , 17 NIST , 18 NIST , 19 NIST , 20 Lund Univ. , 21 JAXA ,22
NIST , 23 TMU

To explore the quantum collision dynamics of the stored molecular ions by the merging experiments with a beamof the neutral atoms, we are developing a new technique of mass spectroscopy for the neutral molecular fragmentsfrom the collisions using an array of superconducting transition-edge-sensor (TES) microcalorimeters at a brand-new
cryogenic electrostatic ion storage ring in RIKEN (Wako, Japan).
In the cosmic space, more than 100 kinds of various molecules exist despite low temperature and low density which
is disadvantageous environment to the molecule formations. It remains still unknown how to be generated even for thesimple molecules. We have recently developed a cryogenic low-temperature ion storage ring to reproduce such chemical
reactions at a temperature of outer space. A molecular ion beam with a vibration-rotation energy (temperature) of
4 Kelvin is stored in this storage ring; and we conduct experiments by an interflow collision with neutral molecularbeam having the same direction and velocity as the stored ion beam, where low-energy collisions at the center-of-masssystem are realized.
It is important to identify the products by measuring those molecule masses after the collision to study the reaction
mechanism. In the case of neutral fragments, however, it is diﬃcult to apply the ordinary mass spectrometry without
ionization for the neutral fragments. In our storage ring, the neutral products after the collision have almost thesame velocity as initial ions / neutral molecules; thus mass identification can be realized by a measurement of thetranslational energy. However, the energy resolution of Micro Channel Plate (MCP) detector commonly utilized so
far is not enough to identify the mass of molecular fragments.
We aim a direct detection of neutral molecules and molecular fragments (less than 15 keV) generated after thechemical reactions reproduced using an array of TES microcalorimeters developed by NIST. By a measurement of the
kinetic energy, we perform the mass spectrometric identification of those neutral fragments and aim comprehensive
understanding of the chemical reactions from the initial to final stages.
TES is operated at the superconducting critical temperature of less than 100 mK; thus we usually install radiation
shields in front of the TES sensors to avoid infrared background from heat radiation which deteriorates the energy
resolution. Unlike x-rays, the low energy molecules ( 10 keV) easily stop at the radiation shields even for 100-nm-thickaluminum sheet; thus we need to remove the radiation shield window. One of key issue towards this TES application
is how to operate TES system against the radiation background although our storage ring is at 4 K. We just started
the study at RIKEN from this spring.
In this presentation we will give an overview of this project and the recent progress.
category : Applications

398

PE-85 New frontier in TES application: X-ray spectroscopy of hadronic-atoms at
Japan Proton Accelerator Research Complex (J-PARC)
Ryota Hayakawa1 , HEATES collaboration2
1

Department of Physics, Tokyo Metropolitan University

We are opening up new frontiers in TES application: X-ray spectroscopy of kaonic-helium atoms at Japan Proton
Accelerator Research Complex (J-PARC). We will deduce 2p shifts and 2p width in kaonic helium-3 and helium-4, bymeasuring 6 keV X-rays from those transitions from 3d to 2p. Our ultimate goal is to clarify the role of the strange
quark and its composites in the equation of state of a neutron star.
This project is not only the first attempt to apply TESs to a hadron-beam experiment but also improving thetechnical readiness levels (TRL) of TESs for future satellite missions equipped with TESs such as ATHENA and(super) DIOS. These missions will challenge to detect the X-rays from the warm-hot intergalactic medium (WHIM)
to understand large-scale structure on a cosmic time scale. However, X-ray emission from WHIM is quite weak, so
undistinguished with a classical semiconductor detector from other background sources. Therefore, it is necessary toutilize the sensor which has good energy resolution. Knowing the TES performance under the influence of charged
particles gives another important input to future space calorimetry missions.
In October 2014, we performed the first experiment at the Paul Scherrer Institute (PSI) in Switzerland using pion
beam. We succeeded to measuring 6 keV X-rays emitted from pionic-carbon with an energy resolution of 7eV (Tatsuno
et al. 2015, Okada et al. and Hashimoto et al. ?2016). In June 2016, we performed a short commissioning experimentat J-PARC to optimize the shield thickness to stop K- beam in the target sample. In this test, a lithium block wasplaced at the final focus of the K- beam instead of liquid helium target. After optimizing degrader thickness for K- beam
condition, we installed the TES spectrometer to the beamline and evaluated in-beam performance of the TESs underrealistic background conditions by observing X-rays from 55 Fe radioactive source. Our TES spectrometer achievedenergy resolution of 6.7eV FWHM at 6keV for the on-beam resolution and 5eV for the oﬀ-beam resolution. Fromthese tests, we learned the background in the X-rays spectrum induced by charged particles were mostly consistent
with the simulation by Geant4. During beam on, bath temperature was slightly worsen and the background events
increased. The temperature stability was restored to be about 5 uKrms by optimizing the shielding configuration.
Liquid helium-3 and helium-4 to create Kaonic 3He and 4He will be used for the scientific campaign in early 2018.
Microphonics from vacuum pumps could be an additional concern because they are connected mechanically to the
TES system to maximize eﬀective solid angle. We confirmed that the bath-temperature fluctuation was about 5uKrms under the same condition as the real test setup. Thus we are ready to compile our TES application when beamtime is allocated to our mission.
HEATES collaboration
R. Hayakawa8 , T. Hashimoto1 , M. Bazzi2 , D.A. Bennett3 , C. Berucci4 , D. Bosnar5 , C. Curceanu2 , W.B. Doriese3 ,J.W. Fowler3 , H. Fujioka6 , C. Guaraldo2 , F. Parnefjord Gustafsson7 , R.S. Hayano9 , J.P. Hays-Wehle3 , G.C. Hilton3 ,T. Hiraiwa10 , Y. Ichinohe8 , M. Iio11 , M. Iliescu2 , S. Ishimoto11 , Y. Ishisaki8 , K. Itahashi12 , M. Iwasaki12,13 , Y. Ma12 ,H. Noda14 , H. Noumi10 , G.C. O’Neil3 , H. Ohnishi15 , S. Okada12 , H. Outa12 , K. Piscicchia2 , C.D. Reintsema3 , Y. Sada10 ,F. Sakuma12 , M. Sato11 , D.R. Schmidt3 , A. Scordo2 , M. Sekimoto11 , H. Shi2 , D. Sirghi2 , F. Sirghi2 , K. Suzuki4 , D.S. Swetz3 ,K. Tanida1 , H. Tatsuno7 , M. Tokuda13 , J. Uhlig7 , J.N. Ullom3,17 , S. Yamada8 ,T. Yamazaki9 and J. Zmeskal4
1 Japan Atomic Energy Agency (JAEA)
2 Laboratori Nazionali di Frascati dell’ INFN
3 National Institute of Standards and Technology (NIST)
4 Stefan-Meyer-Institut für subatomare Physik
5 Department of Physics, University of Zagreb
6 Department of Physics, Kyoto University
7 Department of Chemical Physics, Lund University
8 Department of Physics, Tokyo Metropolitan University
9 Department of Physics, The University of Tokyo
10 Research Center for Nuclear Physics (RCNP), Osaka University
11 High Energy Accelerator Research Organization (KEK)
12 RIKEN Nishina Center, RIKEN
13 Department of Physics, Tokyo Institute of Technology
14 Frontier Research Institute for Interdisciplinary Sciences, Tohoku University
15 Research Center for Electron Photon Science, Tohoku University
16 AMO physics laboratory, RIKEN
17 Department of Physics, University of Colorado at Boulder

category : Applications

399

400

Author Index
Adami
Obaid, 201
Ahmad
Kamal , 180
Ahmed
Zeeshan, 224
AKAMATSUHIROKI, 80
ALIANE
Abdelkader, 85
Allmaras
Jason P , 61
AlpertBradley K, 243
Anderson
Adam Jonathan, 91
Aubin
Francois, 170
AudleyMichael Damian, 366
Austermann
Jason Edward, 31
Avva
Jessica, 234

Julien, 209
Bockstiegel
Clinton, 368
Bounissou
Sophie, 202
Boyd
Stephan T. P., 223
Stephen T. P. , 187
BrienThomas L R , 106
Brown
Ari D, 271, 272
BruijnMarcel P., 101
Bryan
Sean Alan, 98
Bucci
Carlo, 105
Bueno
Juan, 29, 128
BulchaBerhanu T, 109
Camus
Philippe, 297
CantorRobin, 289, 290
Carpenter
Matthew Hollis, 207
CarterFaustin W, 269
Catalano
Andrea, 23
CataldoGiuseppe, 352
CerialeValentina, 175
Chang
Clarence L, 178
Yen-Yung, 324
Chaudhuri
Saptarshi, 81, 335
CheGeorge, 143
Cho
Hsiao-Mei, 138
Choi
Steve K. , 40

BaildonTaylor, 309
BandlerSimon Richard, 357
BarberaMarco, 374
Barrentine
Emily M. , 41Baselmans
Jochem, 7
BastidonNoemie, 389
Becker
Dan, 72
Beldi
Samir, 153
Bennett
Douglas A., 238
BergmanAmanda Stevie, 95
Biasotti
Michele, 358
Billard401

CiceroUgo Lo, 253
CoiﬀardGregoire, 86
Colantoni
Ivan, 274, 355
ColluraGiulia, 10
Coughlin
Kevin P, 283
CroceMark P. , 382
Crowley
Kevin T. , 162
CrucianiAngelo, 146
Cucchetti
Edoardo, 360
Cukierman
Ari, 254

Mikkel, 210
Elleflot
Tucker, 321
Endo
Akira, 20
Everett
Wendeline Bray, 320
Ezaki
Shohei, 263
Ezawa
Hajime, 195
Faramarzi
Farzad, 82
Faverzani
Marco, 147
FilippiniJeﬀrey P. , 310
Flatman
Ben, 161
FleischmannAndreas, 123, 345
Fowler
Joseph W, 379
Fruitwala
Neelay H, 222
Fujii
Go, 376
FukudaDaiji, 121
FyhrieAdalyn, 155

D’Addabbo
Antonio, 287
D’Andrea
Matteo, 364, 365
DaneAndrew, 198
DawsonC.S., 235
de la Broise
Xavier, 230
Defrance
Fabien, 16, 288
den Hartog
Roland, 218
DeNigris
Natalie S, 267
Ding
Junjia, 265
Dober
Bradley Jerald, 220
DolinskiMichelle Jean, 328
Dominguez
Edgar Castillo, 351
DominjonAgnes, 152
Driessen
Eduard F.C. , 135
Dubey
Santwana, 383
Duﬀ
Shannon M, 84
DurkinMalcolm, 249

Gallucci
Giovanni, 339
Gamer
Lisa Elena, 206
Gao
Guanhua, 179
Gard
Johnathon D, 225
Gastaldo
Loredana, 346
GhaithMuad M, 294
GhignaTommaso, 261
Giachero
Andrea, 126
Goldfinger
David C. , 359
Gomez
Alicia, 149
Gottardi
Luciano, 34, 250, 303
GOUPY
J., 252

Echternach
Pierre M. , 67
Ejrnaes

Hahnle402

Sebastian, 144, 293
Hailey-Dunsheath
Steven, 350
HaraToru, 112
HasebeTakashi, 296
HashimotoTadashi, 118
HasselClemens, 57, 298
Hattori
Kaori, 42
Hayakawa
Ryota, 399
HayashiTasuku, 378
Hays-Wehle
James P, 73
Hazumi
Masashi, 314
HelsonKyle R , 308
Hennings-Yeomans
Raul, 256
HijmeringRichard Arnold, 169
Hill
Charles Alexander, 299
HoShuay-Pwu Patty, 307
HornsbyAmber Loren, 151
HoshinoAkio, 284
Hubmayr
Johannes, 88
HuiHoward, 90
Hummatov
Ruslan, 270
Hunacek
Jonathon, 26

JaeckelFelix T, 171
JastramAndrew, 329
Jo
Hyon-Suk, 342
JohnsonBradley R. , 30
Juillard
Alexandre, 49
Kadribasic
Fedja, 47, 327
Karatsu
Kenichi, 133
Kawakami
Akira, 194
KelleyRichard L , 4
Kempf
Sebastian, 66
Khosropanah
Pourya, 168
Kida
Yosuke, 337
Kim
Geon-Bo, 396
Hyelim, 397
Inwook, 333, 348
Sora, 208
Yong-Hamb, 52
KiuchiKenji, 259
Koehler
Katrina E., 332
Katrina E. , 330
KoopmanBrian J, 311
KosakaKengo, 160
Kuenstner
Stephen Erwin , 200
KushinoAkihiro, 229, 244
Kutsuma
Hiroki, 156
Kwon
Dohyung, 344

InomataKunihiro, 64
Irimatsugawa
Tomoya, 219
Irwin
Kent D, 76
IshidaTakekazu, 60
Ishisaki
Yoshitaka, 372
IyomotoNaoko, 163

Langenkamper
Alexander, 295
Lee
Adrian T. , 317
Chang, 108
Hyejin, 343
Kyungmin, 236
Sang Jun, 115, 245
Li
Dale, 380

JA
Jeon, 349
403

Hao, 190
Jin, 191

Hitoshi, 5Nagai
Makoto, 232
NagasakiTaketo, 92
NagaseKoichi, 221
Nagayoshi
Kenichiro, 174
Nakamura
Keisuke, 173
Nakashima
Yuki, 226
NavickXavier Francois, 212
NieRong, 281
Niemack
Michael D, 353
NishinoHaruki, 312
Nitta
Tom, 362
NoguchiTakashi, 129
NoroozianOmid, 15
Novoselov
Evgenii, 186
Nucciotti
Angelo, 55

LiuDong, 192
Loidl
Martin, 375
LowitzAmy E , 154
Maasilta
Ilari, 37, 381
Mahashabde
Sumedh, 145
Maisonobe
Romain, 301
MancusoMichele, 183
MariamRiham, 388
Mates
J.A.B., 71
MatsukiSeishi, 340
Matsumura
Tomotake, 285
MatsuoHiroshi, 291
McCarrick
Heather, 131
McGeehanR., 373
McKenney
Christopher M, 255
McMahonJeﬀ, 319
MeekerSeth R., 19
Miao
Wei, 196
Miniussi
Antoine R., 305
Antoine R. , 177
MitsudaKazuhisa, 341
Miura
Yoshitaka, 181
MoﬀattRobert A , 184
Mondragon
Elizabeth, 193
Monfardini
Alessandro, 9MorganKelsey M , 39
Morozov
Dmitry, 159
Muramatsu
Haruka, 35
Murayama

O’Brient
Roger, 14
Oguri
Shugo, 53
Oh
Seung-Yoon, 188
Ohno
Masashi, 120
Okada
Shinji, 398
OrlandoAngiola, 280
OshimaTai, 369
Pajot
Francois, 25Pan
Zhaodi, 172
PappasChristine Goodwin, 33
Parrianen
Josie Dzifa Akua , 28
Patel
Umeshkumar M., 391
Peille404

Philippe, 356
PhippsArran, 326
Pobes
Carlos, 164
PonceFrancisco, 117
PosadaChrystian M, 277
PRELE
Damien, 78
Puiu
Andrei, 331

Silva-Feaver
Maximiliano, 240
Simon
Sara Michelle, 89
Smith
Stephen J, 371
Song
Yanru, 262
Staguhn
Johannes G, 24
Stanchfield
Sara M., 354
Stevenson
Thomas R., 103
SteverSamantha Lynn, 44
Strauss
Raimund, 46, 347
SuzukiAritoki, 96, 257
Junya, 216
Ken, 390
Swetz
Daniel, 393
Szypryt
Paul, 102

Reintsema
Carl D, 247
RidderMarcel, 275
Rodrigues
Matias, 384
Rodriguez
Louis R , 189
Rothe
Johannes F. , 336
Sakai
Kazuhiro, 167
SanderOliver, 74
Schaeﬀner
Karoline, 325
Schmidt
Marco, 387
ScholzPascal A. , 197
Schroeder
Edward, 142
Sciortino
Luisa, 110
SeidelGeorge M, 54
SekiyaHiroyuki, 50
Semenov
A.V., 140
Shan
Wenlei, 204
SHI
Sheng-Cai, 134
Shibata
Masahiro, 304
Shirokoﬀ
Erik, 139
Shishido
Hiroaki, 17
Shu
Shibo, 148
Sidorova
Maria, 63

Takahashi
Hiroyuki, 241
TakanoAkira, 395
Takekoshi
Tatsuya, 361
TakeuchiYuji, 68
TanakaKeigo, 292
Keiichi, 392
TangQing Yang, 127
Terranova
Francesco, 48
ThakurRitoban Basu, 137
TitusCharles James, 239, 394
Tokiyasu
Atsushi, 199
TrainiAlessandro, 150
Tsujimoto
Masahiro, 217
Ukibe
Masahiro, 100
Ulbricht
Gerhard, 136
Ullom
Joel N, 114405

UzawaYoshinori, 227

Wu
Wentao, 268
WuestrichMarc, 338

VaccaroD, 323van der Kuur
Jan, 228
van Marrewijk
Nuri, 211
Vavagiakis
Eve Marie , 166
VignatiMarco, 132
Vissers
Michael R, 260
von Feilitzsch
Franz, 3

YamadaShinya , 370
Yousuke, 233
Yamasaki
Noriko Y. , 300
Yan
Daikang, 43
Yasumune
Takashi, 385
YatesStephen J.C., 367
Stephen J.C. , 11
Yefremenko
Volodymyr G, 278
Yoon
Wonsik, 246
YOSHIMOTO
Shota, 203
You
Lixing, 62

WakehamNicholas, 38
WalterAlex B, 273
Wang
Gensheng, 157
Weber
Joel, 248
WegnerMathias, 75
Wei
Lianfu, 13
Wessels
Abigail L., 302
Westbrook
Benjamin, 258
Wheeler
Jordan, 185
Willers
Michael, 334

ZenNobuyuki, 205
Zhang
Wen, 165
Xiaohang, 182
Zhao
Qing-Yuan, 59
Zhou
Yu, 176
ZobristNicholas, 158

406