Development of millimeter-wave band MKID
camera for wide-field continuum observations

T. Nitta
University of Tsukuba

Contents✴ Scientific Motivation✴ Operation Principle of MKID
✴ MKID Camera Development for Wide-filed Observation✴ THz band Camera✴ SummarySurvey of Distant Galaxies✴ Distant Galaxy Survey

106

102

101

412MBB
Arp220
M82
HR10Eyelash

100

flux (mJy)rest (GHz)104103(a) HFLS3

101

10105

141618-1

2010-2

22
24
1’

10-5
10-1

total

250 µm10010121010
obs (!m)

350 µm
3500 µm
45Infraredmm to THz2

1z=1281010et al., Nature,
10Riechers496, 329, 2013

22z=168
726-4

Arp220
M82HR10Eyelash

S350 > S250

310-310(b)3S500/S350

102107(~ No. of galaxy)distant galaxy- redshift can be determined from the SEDof the galaxy
・optical wavelength observation is difficult
because the emission is absorbed by dust - to reveal the star formation history at・dust emission can be observed at mm-wave high-redshift, dust emission observation
is importantto THz range
A&AAB mag-✴ Star Formation History

004566875
HFLS3 z=6.34

4HLock102 z=5.29
3 HLS A773 z=5.24
HFLS1 z=4.29
HATLAS ID141 z=4.24
HFLS5 z=4.44

S500 > 1.3 S350
S500 > S350

(in prep.)

OpticalUV

123S350/S250

45Burgarella et al., 2013

Wide-Field Observations✴ Wide-field telescope and multi-pixel superconducting camera¯`{~ 2.5 m çzØ¬öþòýºè ýºæÆó_ã¤-ÊĎu±-ÝČ
observation area

<mm/submm Survey>
 optical  imageb²{ā¦mvr(Ò 1000 km [ā£­:G?vr)Č ( (Ò 60km"Ă+ ,:G?vrå +*N*ĊFig. 2ċĎ +(µĉ 3800m ĉČ¶½č20 ďč80 ²r*Ď$Č{¶L·Ü¶ą  ČùÓ%Vra\Î)Č2<>B»( THz Ivison et al., 2000{¶îõÄ²$ĉĊFig. 3ċĎ (§ÿÉ)ČòÖ»Ą»á¾&¼äá¾%÷*Ď#Č¨Ä 68 %Ċ1994, 95sċČ¨|Ä 85 % Îąĉ Čÿ
ALMA : high-angularresolution interferometer
Fig. 4 A schematic illustration of the 10 m THzsĈð 5.8 m/s Î)Č10 m/s RIĈ→ follow-up
observationsof galaxies
detected by the cameraąĎ +(():G?vr2<telescope>B»ČTHz »á¾rIªĉ®T)ČÃ
 1 THz RIOIrIoHá¾hÛ* -ÍĎH Čb²Ã«pćČk ¿#)t¹*hÛ*$ČĉiI

For distant galaxy survey,• camera development for wide field-of-view observation• good observation site for astronomical observations
are importantWide-Field Continuum Camera✴ 100-GHz band Camera (now developing)・Camera is installed to Nobeyama 45m telescope・Detector : 109 pixel MKID array・frequency band : 90 - 110 GHz
・Field-of-view : ~ 3 arcmin✴ THz band Camera (Future Plan)
・Our group is planning to construct the 10 m
telescope at the Antarctica plateau.
・frequency band : 0.4 / 0.85 / 1.3 THz
・Field-of-view : 1 degree

MKID detector is one of the important technology for realizing wide-field camera

Microwave Kinetic Inductance Detector (MKID)✴ Operation Principle

Day et al., Nature, 2003
MW Readout(3 - 9GHz)
図 2.2:(左)MKID (右)MKID の等価回路

・Superconducting resonators operated in
the microwave range
最初に述べたように MKID とはマイクロ波帯で動作す
photonequilibrium
・Incident photons break Cooper-pair から分かるようにキャパシタンスとインダクタンスが並
absorption→ Kinetic Inductance is changed
MKID では共振器の長さは読み出しに使用するマイクロ→ Resonance frequency of MKID is also
長になっており、片側 short , もう片側が open になっていchanged
クロ波で共振を起こす。この時、共振周波数
ω0 は
δf500um
Signals from the objects are observed bymonitoring the shift of the resonance frequency. Gold：Superconductor(Al)Black：Substrate (Si)

✴ Advantage of MKID

2π
ω0 = !
4l (Lg + Lk )C・High-detector yield is expected because
the MKID fabrication
process is relatively
simpleで表される。ここで、l は共振器の長さ、Lg , Cは超伝導パシタンスである。
MKIDにEのエネルギーを持・Intrinsic frequency multiplexing capability→ ~1000 pixels
can bemeasured
one LNAgap ＜ hν with46を破壊すると力学インダクタンスが変化することから、/ 2 MHz span〜 1000素子程度
MKID1→ 2GHzMKID2
MKID3
MKID1 MKID2 MKID3Readout

S21 [dB]

44424038

2πω0 − ∆ω0 = !
4l (Lg + Lk + ∆36
Low-noiseampliﬁer2.3 に示すように低周波側にシフトする。となり、図6.376 6.378
6.386.382 6.384 6.386 6.388
6.39Frequency [GHz]MKID Camera for the Nobeyama 45m Telescope✴ Millimeter-wave MKID Camera
・Millimeter-wave MKID camera has beendeveloped for the Nobeyama 45m telescope
・Collaboration with National AstronomicalObservatory of Japan
・Optics of the 45 m telescope consists of thefour reflective mirrors→ Two Si lenses are used to connect thetelescope focus to the MKID array.

✴ Camera specifications
Observation Frequency
Field-of-view
Polarization
Detector
Cold Optics
No. of pixels
Bath temperature

100-GHz band（90 − 110 GHz）
〜 3 arcmin
linear single polarizationMicrowave Kinetic Inductance Detector
Refractive optics using Si lens
109 pixels< 200 mK

Cryostat Design

Readout System

Camera Cryostat

ਤ 2.3: μϒϧεϩοτΞϯςφͱ݁߹ͨ͠ MKID2.2

ίϓϨφઢ࿏

MKID ͷ৴߸͸༠ిମ‫ج‬൘ʹ੒ບ͞Εͨ௒఻ಋബບʹΑΓ‫ܗ‬੒͞Ε
(Coplanar Waveguide; CPW) ʹΑͬͯ఻ૹ͞ΕΔɻίϓϨφઢ࿏͸ਤΓ৴߸͕ૹΒΕΔத৺ಋମͱ‫ج‬४ిҐͱͳΔ྆ଆಋମ (άϥϯυϓϨʔϯϓΛִͯͯಉҰฏ໘্ʹ࡞ΒΕ͍ͯΔɻ·ͨਤ 2.4(b) ͸ి࣓քγϛϡϨΔίϓϨφઢ࿏͕࡞Δిք෼෍Λද͓ͯ͠Γɺத৺ಋମ͔Β྆ଆಋମ΁
͍ͯΔ͜ͱ͕Θ͔Δɻ͜ͷి৔ͱத৺ಋମΛғ͏࣓৔ʹΑΓ৴߸Λ఻ૹ

Antarctica Plateau
Showa Station✴ Planning telescope at Antarctica
Dome F・10 m class telescope @ Dome C (France-Italy site)
・30 m class telescope @ New Dome F (Japanese site)✴ Comparison to other sites

SouthPole

Dome C

Altitude (m)0goodDome A

2000 4000

Dome F
200 K, 0.1 mm (25% in winter)）＜e.g. Atacama / Mauna Kea >Dome F
200 K, 0.14 mm (50% in winter）
・very good site for astronomy
Atacama Desert
260 K, 0.6 mm (50% in winter） ・There are a lot of telescope on these sites
Mauna Kea
＜ Antarctica ＞
270 K, 1.5 mm(50% in winter）

・higher transmittance・THz bands are only available at the Antarctica
mm-wave submm-wave

THz

Yang et al., 2010

Antarctica is the best site for millimeter-wave and terahertz astronomical observations

MKID Camera for Antarctica telescope✴ Antarctic 10 m Telescope✴ THz band MKID Camera

・Field-of-View：1 degree

・7 optics tubes with Si lens- based on the NRO 45m MKID camera- Survey of distant galaxy- ~20000 pixels for 0.45, 0.85, 1.3 THz

・Two instruments @ Nasmyth focus- Heterodyne receiver & Camera

・Two types of focal plane arrays
8.3 Design of 850 GHz-bands Camera- Select by changing the third mirror

Subreflector

4 K Si Lens
(dia. = 400telescopefocus@F/6Main Reflector
Third mirror→Si lens array and horn array

CameraHeterodyne receiver
Telescope Focus

145Lens array

1 K Si Lens
(dia. = 110 

Figure 8.8: A module design of 850-GHz band camera. (Left) Green part showed thesilicon substrate, and the bottom space is used for the carbon based absorber. (Right)
The camera module with the 2977 pixel silicon lens array and the springs for fixing thecamera module and the lens array.

dB. These parameters were summarized in chapter 5, Fig. 5.1.

The optimized parameters of the extension thickness, the gap height and the lensCold Optics MKID(< 4 K)(<0.2 K)

diameter were L/R = 0.34, H/R = 0.604 and D = 2.4λ (λ = 353 µm; the wavelength ofHDPE850 GHz), respectively. In thissimulation,equivalentarrayto the lens
coldbaffle the detector spacing was HornwindowSummary✴ Scientific Motivation
・distant galaxy survey- wide-field survey is important to detect the unknown galaxies- redshift can be determined from the spectrum energy distribution✴ MKID camera development
・MKID camera for the Nobeyama 45 m telescope- 109 pixel array using lens-antenna coupled MKID
- dark NEP : ~ 10-16 [W/rHz]- improvement of the sensitivity is needed- Beam pattern measured with planets is comparable with the simulation✴ Future development

・Antarctica is the best site for THz astronomy
・~ 20000 pixel camera is designed for the Antarctic 10 m telescope