PRINTISSN13461192
ONLI
NEI
SSN24367214

Annua
lRe
por
toft
he
Na
t
i
ona
lAs
t
r
onomi
c
a
lObs
e
r
v
a
t
or
y
ofJ
a
pa
n
Vol
ume25Fi
s
c
a
l2022

Cover Caption
A superconducting microwave amplifier developed by NAOJ. It is an amplifier based on
a completely new principle that combines two SIS mixers (frequency converters) usedin receivers on radio telescopes. Further research into miniaturizing and integratingsuperconducting circuits will contribute to the realization of multi-pixel radio cameras andlarge-scale quantum computers.
Credit: NAOJ

Postscript
Publisher National Institutes of Natural Sciences
National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan
TEL: +81-422-34-3600
FAX: +81-422-34-3960
https://www.nao.ac.jp/
Printer DAISAN Co., Ltd.
755-1 Oshiage, Sakura City, Tochigi Prefecture 329-1334, Japan
TEX: +81-28-682-1311
FAX: +81-28-682-1384

Annual Report of the
National Astronomical Observatory of Japan

Volume 25, Fiscal 2022

Preface

Saku TSUNETA
Director General

I Scientific Highlights
II Status Reports of Research Activities
01. Mizusawa VLBI Observatory
02. Nobeyama Radio Observatory
03. Solar Science Observatory (SOL)
04. Subaru Telescope
05. Center for Computational Astrophysics (CfCA)
06. ALMA Project, NAOJ Chile, and ASTE Project
07. Gravitational Wave Science Project
08. Thirty Meter Telescope Project
09. JASMINE Project
10. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project
11. Solar-C Project
12. The Subaru Prime Focus Spectrograph (PFS) Project
13. The Subaru Ground Layer Adaptive Optics (GLAO) Project
14. Astronomy Data Center
15. Advanced Technology Center
16. Public Relations Center
17. Division of Science
18. Library
19. IT Security Office
20. Research Enhancement Strategy Office
21. Office of International Relations
22. Human Resources Planning Office
23. Safety and Health Management Office
24. Engineering Promotion Office
25. Graduate Education Office
III Organization
IV Finance
V KAKENHI (Grants-in-Aid for Scientific Research)
VI Research Collaboration
VII Graduate Education
VIII Public Access to Facilities
IX Overseas Travel
X Award Winners
XI Library, Publications
XII Important Dates
XIII Publications, Presentations
1. Refereed Publications
2. Publications of the National Astronomical Observatory of Japan
3. Report of the National Astronomical Observatory of Japan
4. Conference Proceedings
5. Publications in English
6. Conference Presentations

001
035
040
042
045
050
053
057
059
064
066
067
068
070
072
074
082
089
092
093
094
095
097
098
100
101
102
121
122
123
125
131
136
137
138
139
142
162
162
162
167
167

P R E FA C E

Saku TSUNETA
Director General of NAOJ

Fiscal Year 2022 (FY 2022), like Fiscal Year 2021, continued
to feel the effects of the novel coronavirus, and we maintained
a hybrid style of online and face-to-face for various aspects ofour endeavors. I am confident that the National Astronomical
Observatory of Japan (NAOJ) can strongly promote its activities inthis new era by embracing a hybrid workstyle, not just as a decision
forced by the need to prevent infection, but as a new paradigm
that takes the best parts of both to create an efficient and effective
working style.
One of the highlights in the world of astronomy in 2022 was that
the James Webb Space Telescope (JWST) launched on December
25, 2021 began science observations, and reported mind-boggling
results one after another. On July 11, 2022 (local time) UnitedStates President Joe Biden unveiled the first image of a distantgalaxy cluster taken by JWST, demonstrating the United Statesof America’s commitment to continue to lead the next generationof astronomy. In addition to the release of the beautiful, highresolution infrared images, with the first detection of carbon
dioxide in the atmosphere of an extrasolar planet and the detectionof a galaxy candidate in the Universe over 13.5 billion years ago,
JWST can truly be said to be living up to the expectations that it
will deliver results stretching from the Milky Way Galaxy backto the earliest days of the Universe. Science proposals are being
accepted from all over the world, including many proposals inwhich Japanese researchers, particularly young researchers, areplaying leading roles. We expect strong synergy between JWSTand Japan’s leading observation facilities including the Subaru
Telescope and ALMA.
New instruments which will show us new views of the Universe
have been developed for NAOJ telescopes. The Prime Focus
Spectrograph (PFS), which can deliver simultaneous spectral
observations of up to about 2,400 celestial objects, using theapproximately 2,400 fibers arrayed across the wide field ofview offered by the Subaru Telescope, conducted engineeringobservations in September 2022 where it successfully obtained thespectra for the light from many stars at the same time, achieving
engineering first light. This is an important milestone in the
Subaru Telescope 2.0 project launched in FY 2022 to upgrade thecapabilities of the Subaru Telescope. Test observations to confirm
instrument performance have followed, led by KAVLI IPMU at
the University of Tokyo, making progress towards PFS’s ultimate
goal of “revealing the true nature of dark energy through spectral
observations of numerous galaxies.”
In addition to “Subaru Telescope 2.0” the upgrade plan for ALMA,“ALMA 2.0” will start in FY 2023. Various development work is
continuing in hopes of achieving the 3 major stated science goals of
understanding the formation process of planetary systems on scales
equivalent to the size of Earth’s orbit; understanding the nature oforganic material in the formation process of planetary system, andpinpointing the beginning of nucleosynthesis in the Universe.

This development has potential applications beyond the realm of
astronomy research. A research team in the Advanced Technology
Center (ATC) demonstrated a novel microwave amplifier based oncompletely new principles by coupling together superconducting
SIS mixers from ALMA. This opens the possibility for significant
reductions in size and power consumption compared to previous
microwave amplifiers. It can be expected that this result willcontribute to the actualization of authentic quantum supercomputersrequiring many amplifiers.
The Industry Liaison Office was launched in order to give backto society though the development of technologies like this at
NAOJ. One example is the lecture for journalist about “Technology
Development in NAOJ and Collaboration with Industry” conductedin collaboration with the Public Relations Center together with atour of ATC in December of 2022. FY 2022 also saw the realizationof academic consultation and joint research, contracted research,and contracted projects with private companies. The Industry
Liaison Office plans to further extend its reach by hosting exhibits
at conferences and by courting the media.
As always, NAOJ produced many research results in FY 2022.
In the strategic program utilizing the Subaru Telescope’s Infrared
Doppler instrument (IRD), an extrasolar “Super Earth” witha mass 4 times that of the Earth was discovered around a lowtemperature star. The elucidation of the types of planets that canbe found around low temperature stars, which account for threequarters of the stars in the Milky Way Galaxy, provides fodder
for the discussion of the possibility of life in environments very
different from what is found on Earth. An artificial intelligence (AI)trained on simulation results from the supercomputer “ATERUIII” analyzed observational data for real galaxies and successfullymeasured the cosmic parameters (physical constants which govern
the properties of the Universe) with high precision. As AI isproving its usefulness in various aspects of society, the applicationof AI to astronomy dealing with Big Data is also advancing.
A worldclass result contributed in data analysis by Japanese
researchers, the imaging the supermassive black hole “Tau A*”(pronounced Tau A Star) at the center of the Milky Way Galaxy,
had large impact on society. This is a result of the “Event Horizon
Telescope” which creates a global scale telescope by combining
data taken by 8 radio telescopes at 6 locations, first and foremost
ALMA operated by NAOJ together with international partners.
One of the bases of research like this is the Division of Science,
which had its first international review since its founding where
its research activities combining theory and research were praised.
Further developments are expected through activities occurring
across the traditional boundaries between NAOJ projects andbeyond the Division of Science, such as regularly held joint
seminars and calls for researcher positions conducted together with
Projects including Subaru Telescope and ALMA. Observational
results on extrasolar planets, cosmic parameters, and black holes
are all themes that provide important hints about the appearance
and structure of the Universe in which we live and provide a basis
to think about our own roots. These are themes which NAOJ needs
to pursue.
Here I would like to summarize the status of NAOJ’s various
projects in FY 2022.
New observational instruments have been introduced sequentiallyat the Subaru Telescope since it started observations in 1999,
maintaining its high level of international competitiveness. There
were 192 refereed papers in FY 2022. This is at the highest world

level for a single 8-10 m class ground-based optical/infrared
telescope. This happens against a backdrop where researchers
unaffiliated with NAOJ are actively using the data releases from theultra-wide field of view prime focus camera Hyper Suprime-Cam(HSC) to write papers.
On the other hand, the mechanical components of the telescopeand dome continue to age. Since 2018, the Ministry of Education,
Culture, Sports, Science and Technology (MEXT) has been
providing a budget for countermeasures against the aging of theequipment. In FY 2022, the telescope drive mechanism, which isvital to the operation of the telescope, was repaired and the dome
air conditioning system was renewed.
“Subaru Telescope 2.0” was accepted as a Large-scale Academic
Frontiers Project in FY 2022 and integration and assembly is
continuing for the facility instrument PFS. The Ground Layer
Adaptive Optics (GLAO) to improve the resolution over a wide
field of view, which is required for another facility instrument,
the Ultra-wide Laser Tomographic Imager and MOS with AO forTranscendent Exploration (ULTIMATE), has passed the preliminary
design review and has now moved on to the detailed design phase.
It has been decided to conduct synergetic observations between
the Subaru Telescope and Roman Space Telescope (scheduled forlaunch in 2026). Now we are fleshing out the plan together with
the United States National Aeronautics and Space Administration(NASA) and Institute of Space and Astronautical Science (ISAS)of the Japan Aerospace Exploration Agency (JAXA). Also,in preparation for cooperative research with the Euclid spacetelescope of the European Space Agency (ESA) and the American
Rubin Observatory, a framework for collaboration is being erectedbased on discussions with the astronomy community.
ALMA started its 10th open-use observation cycle, Cycle 9, from
October 2022. A record-setting 1,769 observation proposals werereceived from all over the world. At the end of October, ALMA
observatory in Chile suffered a cyberattack on its computer
systems, forcing the suspension of astronomical observations.
But through the dedicated efforts of everyone involved, open-use
observations resumed in mid-December. The number of scientificpapers published based on ALMA data reached 3,238 during theeleven-and-a-half-years ending with FY 2022. Japan continues to
do well, in terms of primary authors, we had the second largest
number of papers, following the United States of America.
New instrument development and production is proceeding under
the framework for collaboration in East Asia being led by NAOJ.
The Band 1 receivers (observational bandwidth 35-50 GHz)
led by the Institute of Astronomy and Astrophysics, Academia
Sinica (ASIAA) and the new spectrometer led by the Korea
Astronomy and Space Science Institute (KASI) for the Atacama
Compact Array (ACA/Morita Array) will be offered for open-use
observations starting with Cycle 10 in October 2023. Corrugatedhorns developed and manufactured using a 3D metal printer in ATC
are installed in the Band 1 receivers.
Preparation for the “ALMA 2.0” plan aiming for performance
improvements including angular resolution two times better
than ALMA, continued with the project transition evaluationand preliminary review for the Large-scale Academic Frontiers
Projects of the Council for Science and Technology, Subdivision on
Technology, Subcommittee on Research Environment conducted
in 2022. The preliminary review found that “this plan needs to be
actively pursued, and work should start as soon as possible,” thus
the ALMA 2.0 plan will start from FY 2023.

Construction of TMT, an extremely large telescope with a 30 m
diameter being advanced through international collaboration,is on hold due to opposition movements in Hawai`i. NAOJ in
cooperation with TMT International Observatory (TIO) is pursuinga direct dialog with local residents and education support to fostera relationship of mutual trust. The Mauna Kea Stewardship andOversight Authority (MKSOA) with participation by Native
Hawaiian representatives was established in 2022, for the firsttime creating a mechanism to reflect the opinions of indigenous
people in the management of the operation and construction oftelescopes on Maunakea. Also, to achieve the reduction in thenumber of telescopes desired by the Native Hawaiians, progress
is being made on the decommissioning of the 10.4 m diameter
Caltech Submillimeter Observatory (CSO) and decommissioning
preparations for the University of Hawai`i educational telescope
Hoku Kea. The situation in Hawai`i is improving thanks to these
efforts.
The preliminary design review by the United States National
Science Foundation (NSF), which is vital for securing the TMT
construction budget, was held and deemed TMT ready to proceed
to the Final Design Phase. The high level of engineering for thetelescope main structure for which Japan is responsible and theoutreach efforts in Hawai’i led by NAOJ members were both
highly evaluated. In these ways, the TMT plan is advancing bothat the local level in Hawai`i and the US federal government level.
In Japan, while continuing to minimize budgetary expenditures,
preparation is proceeding with the Japanese community for the
manufacturing of Japan’s work share, including a Production
Readiness Review of the main telescope structure conducted by
TIO.
KAGRA, the Large-scale Cryogenic Gravitational Wave Telescope,developed through collaboration between the Institute for Cosmic
Ray Research of the University of Tokyo, NAOJ, and the HighEnergy Accelerator Research Organization KEK, has completed
upgrades to participate in the fourth international gravitational
observing run O4 scheduled to start from May 2023. The PowerRecycled Fabry-Perot Michelson interferometer can now be stably
locked for over 2 hours. NAOJ contributes to various aspects of
KAGRA including interferometer commissioning, noise hunting,and calibration. The sapphire mirrors developed in collaboration
with KASI in Korea and ASIAA in Taiwan are scheduled to beinstalled in KAGRA before the O5 run. In addition, the KAGRA
satellite control room established in Mitaka Campus in FY 2021
has increased work efficiency and reduced costs.
At Nobeyama Radio Observatory, while a new policy of charging
for observation time has been implemented from FY 2022,
observational research is still being actively conducted as before.
Through the use of artificial intelligence (AI) the distances
to interstellar molecular clouds have been determined fromobservational data, creating the first 3D map of molecular gas
distribution in the Milky Way Galaxy.
At Mizusawa VLBI Observatory, collaborative observation
programs have started in addition to open use of the East AsianVLBI Network (EAVN). Results are being produced, such as a
scenario to explain the detailed velocity structure of the M87 jetrevealed by Japan-Korea VLBI observations. Additionally, efforts
to diversify in funding sources are ongoing, including crowd
funding and the employment of project assistant professors throughcooperation with a media company.
The Okayama Branch of Subaru Telescope facilitates the open
use of Kyoto University’s 3.8-m Seimei Telescope, contributing

to the creation of scientific results. Under the leadership of Tokyo
Institute of Technology, the Branch’s 188-cm Reflector Telescope
was used as a dedicated extrasolar planet survey telescope. Since
FY 2018, the city of Asakuchi has used it to offer paid chartered
telescope time and stargazing parties. A problem developed in thedome slit in September 2022, and investigations towards recovery
are underway.
Ishigakijima Astronomical Observatory, taking advantage of thewide observable area of the sky thanks to being located at thesouthern tip of Japan, is using the 105 cm aperture “Murikabushi
Telescope” to study Solar System bodies and transient celestialphenomena. Starting from FY 2022 a paid admission system was
implemented to increase safety and security of the guests andimprove employee working conditions.
In the Optical and Infrared Synergetic Telescopes for Education andResearch (OISTER), 9 domestic universities run 1 m class optical/
infrared telescopes arrayed across Japan and overseas to conduct
follow-up observations of transient phenomena. In Japanese VLBI
Network (JVN) activities, 30 m class radio telescopes operated by
6 domestic universities are combined to form a VLBI observation
network, and mazer monitor observations led by Ibaraki University
continue to detect accretion bursts.
The East Asian Observatory (EAO), with its 5 members of Japan,
China, the Republic of Korea, Taiwan, and Thailand, continues tooperate the James Clerk Maxwell Telescope (JCMT).
The SOLAR-C satellite plan to conduct high-spatial resolution
spectroscopy in the extreme ultraviolet is making steady progress.
It passed the JAXA Mission Definition Review in July 2022,
moving to the pre-project phase, and in December completed
the System Requirement Review. The international SUNRISE-3
balloon experiment, which was to conduct high angular resolution
polarimetry using a 1-m aperture optical telescope, launched inJuly 2022, but was unable to collect observational data due to a
malfunction in the gondola. A re-flight is planned for the summerof 2024. Development is underway at NAOJ for flight models for ahigh-speed CMOS camera for soft X-rays and an X-ray collimator
for the NASA FOXSI-4 sounding-rocket experiment. Aiming fora launch in spring of 2024, FOXSI-4 will conduct solar X-ray
spectroscopy with focusing optics.
The lunar and planetary exploration RISE Project, as the Geodesy
Science Strategy Team (GSST) for the Martian Moons eXploration(MMX) sample return mission, worked together with the Centre
National d’Etudes Spatiales (CNES) in France to develop orbit/
gravity field estimation software. The surface evolution and interior
structure research of the asteroid Ryugu cultivated by Hayabusa2 isnow being expanded towards observations of the Martain satellite
Phobos.
In ATC, evaluation tests are underway for a prototype for use insatellites based on an InGaAs infrared imaging sensors developed
for terrestrial use. Good results, including high sensitivity,
have been obtained. A 2k × 2k multielement prototype has
been completed, and is scheduled to be evaluated in FY 2023
in cooperation with the JASMINE Project. This sensor will be
installed on JAXA’s JASMINE infrared astrometry satellite.
Work to expand the ATC microfabrication cleanroom is underway,
laying a foundation for accelerated progress on research anddevelopment for applications including ALMA 2.0 and quantum
computers. From the perspective of economic security, we haveestablished a management system for superconducting devices

and various device manufacturing equipment, including a newly
constructed secure storage area for sensitive items with security in
mind.
Also, a framework is being developed for the application of ultralow power consumption cooled amplifiers and isolators developed
for radio telescopes to error-tolerant quantum computers and therepurposing of adaptive optics technology, which was developed
to compensate for atmospheric fluctuations in order to capture
clear images of celestial objects, for application in biologicalmicroscopy or satellite to ground communications. In order tomake the technology in ATC relevant to society beyond the limitsof astronomy, preparation is proceeding within the center to launch
the “Social Implementation Program.”
In the Astronomy Data Center, the renewal of the large-scalearchive and multi-wavelength data analysis system has been
postponed due to a semiconductor shortage. The Japanese Virtual
Observatory (JVO) released a VO interface for the JAXA infrared
astronomy satellite AKARI data catalog.
In the Public Relations Center, the live coverage internet broadcastof the total lunar eclipse and occultation of Uranus which occurredon November 8, 2022 attracted much attention with approximately
1.85 million views, over 2 million if you include views of thearchive video. In parallel with online information dissemination
like this, face to face events such as Mitaka Campus Special
Open House Day and Regular Stargazing Parties using the 50cm Telescope for Public Outreach are helping to forge a hybrid
approach of in-person and online activities. By offering the genuine
experience of in-person communication and the accessibility of
online content, we are pursuing an outreach and education strategy
catering to the different needs of different segments of society.
The 2,969 refereed papers published during 2018~2022 bymembers of NAOJ have had an international collaboration rate of
81.8 %; also, 17.3 % of the papers have made it into the Top10% of
papers published worldwide in terms of citations and 3.6 % havemade it into the Top1% (according to InCites as of August 2023).
While as of August 1, 2023, Japanese members account for only
5.5 % of the total members of the International Astronomical Union(with 689 Japanese members, approximately 27 % the number ofUnited States members), Japan achieved a 9.1 % world share in thenumber of papers published in space science during 2022 with 1,590
papers. This is Japan’s highest world share among the 22 fields ofstudy, surpassing physics (6.6 % with 7,748 papers). As of April 1,
2023, women account for 10.2 % of NAOJ researchers (including
Research and Academic Staff and specially appointed teachers)compared to 10.5 % in the previous fiscal year.
In addition, the newly created Graduate Education Office canconduct systematic graduate student education and human resource
development, and can also act as a window for communication
with other institutes. The “NAOJ Future Planning Symposium2022: How to decide and promote future plans” (December 7, 8
@ Mitaka Campus) was held based on discussions by the NAOJ
Scientific Advisory Committee. Here researchers from inside andoutside of NAOJ had a lively exchange of opinions.
This concludes my overview of NAOJ’s activities in FY 2022.
More details can be found in the full report. I look forward to yourcontinued cooperation and support.

I Scientific Highlights(April 2022 – March 2023)
Spectral Evolution of 596 Scheila and Dark Asteroids Induced by Space Weatheringover a DecadeOver Seven Decades of Solar Microwave Data Obtained with Toyokawa and Nobeyama
Radio Polarimeters
Survival of Terrestrial N2-O2 Atmospheres in Violent XUV Environments by Efficient
Atomic Line Radiative Cooling
Narrow Fe-Kα Reverberation Mapping Unveils the Deactivated Broad-Line Region ina Changing-Look Active Galactic Nucleus
Millimeter Methanol Emission in the High-mass Star-forming Region G24.33+0.14

HASEGAWA, Sunao, et al. 002
SHIMOJO, Masumi,
003
IWAI, Kazumasa
NAKAYAMA, Akifumi, et al. 004
NODA, Hirofumi, et al. 005
HIROTA, Tomoya,
006
Maser Monitoring Organization (M2O)

The Resolved Feature at the Center of M87 Found from EHT Public Data

MIYOSHI, Makoto, et al. 007

Automated Sunspot Detection as an Alternative to Visual Observations

HANAOKA, Yoichiro 008

Optical IFU Observations of GOALS Sample with KOOLS-IFU on Seimei Telescope:
Initial Results of Nine U/LIRGs at z < 0.04

TOBA, Yoshiki, et al. 009

Exploring Cosmic Dawn and Epoch of Reionization with 21 cm Line
ALMA Lensing Cluster Survey: Properties of Millimeter Galaxies Hosting X-ray
Detected Active Galactic Nuclei
WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids:(3200) Phaethon, 2005 UD, and 1999 YC
Comparison of Size Distributions between L 4 and L5 Jupiter Trojans

SHIMABUKURO, Hayato, et al. 010
UEMATSU, Ryosuke, et al. 011
KASUGA, Toshihiro,
012
MASIERO, Joseph R.
UEHATA, Kotomi, et al. 013

Mass Function of a Young Cluster in a Low-metallicity Environment. Sh 2-209

YASUI, Chikako, et al. 014

Configuration of Probe Tones for MKID Readout with Frequency Sweeping Scheme

NAGAI, Makoto, et al. 015

Correlation Polarimeter for Millimeter-Wave Wavefront Sensing
uGMRT Observation of CIZA J1358.9-4750: Discovery of a New Diffuse Radio Source
Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical
Spectroscopy
The Coherent Differential Imaging on Speckle Area Nulling (CDI-SAN) Method forHigh-contrast Imaging under Speckle Variation

NAGAI, Makoto, et al. 016
KURAHARA, Kohei, et al. 017
NOBORIGUCHI, Akatoki, et al. 018
NISHIKAWA, Jun 019

Passive Spiral Galaxies Deeply Captured by Subaru Hyper Suprime-Cam

SHIMAKAWA, Rhythm, et al. 020

Discovery of the Monster Supercluster in the Universe at z = 0.6

SHIMAKAWA, Rhythm, et al. 021

An Empirical Method for Mitigating an Excess Up-scattering Mass Bias on the Weak
Lensing Mass Estimates for Shear-selected Cluster Samples

HAMANA, Takashi 022

A Tale of a Tail: A Tidally-Disrupting Ultra-Diffuse Galaxy in the M81 GroupŽEMAITIS, Rokas, et al. 023

Discovery of an Earth-sized Planet around an M5 Dwarf Star at 22 pc

HIRANO, Teruyuki, et al. 024

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). VII.
Redshift Evolution of Radio Galaxy Environments at z = 0.3−1.4
A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). IX. The
Most Overdense Region at z ~ 5 Inhabited by a Massive Radio Galaxy
Spectroscopic Characterization of Young Stars Showing Irregular Dimmings to Unveil
Their Mechanisms
Morpho-kinematic Modeling of the Expanding Ejecta of the Extremely Slow Nova
V1280 Scorpii
Statistical Properties of Satellites of Milky Way-like Galaxies

UCHIYAMA, Hisakazu, et al. 025
UCHIYAMA, Hisakazu, et al. 026
KASAGI, Yui, et al. 027
NAITO, Hiroyuki, et al. 028
NASHIMOTO, Masashi, et al. 029

First Identification of a CMB Lensing Signal Produced by 1.5 Million Galaxies at z ~ 4:Constraints on Matter Density Fluctuations at High Redshift

MIYATAKE, Hironao, et al. 030

Discovery of a Super-Earth around the M4.5 Dwarf Ross 508

HARAKAWA, Hiroki, et al. 031

Deep Near-infrared Imaging of the Faint X-ray Point Sources Constituting the Galactic
Bulge X-ray Emission
Direct Imaging Discovery of a Benchmark Brown Dwarf Orbiting the Hyades
Accelerating F5-type Star HIP 21152
Demonstration of a Low-noise Microwave Amplifier Based on SIS Mixers

MORIHANA, Kumiko, et al. 032
KUZUHARA, Masayuki, et al. 033
KOJIMA, Takafumi, et al. 034
001

Spectral Evolution of 596 Scheila and Dark Asteroids
Induced by Space Weathering over a Decade
HASEGAWA, Sunao1, DeMEO, Francesca E.2, MARSSET, Michaël2/3, HANUS, Josef4,
AVDELLIDOU, Chrysa5, DELBO, Marco5, BUS, Schelte J.6, HANAYAMA, Hidekazu7, HORIUCHI, Takashi8,
TAKIR, Driss9, JEHIN, Emmanuël10, FERRAIS, Marin11, GEEM, Jooyeon12, IM, Myungshin12,
SEO, Jinguk12, BACH, Yoonsoo P.12, JIN, Sunho12, ISHIGURO, Masateru12, KURODA, Daisuke13,
Binzel, Richard P.2, NAKAMURA, Akiko M.14, YANG, Bin15, VERNAZZA, Pierre11
1: Japan Aerospace Exploration Agency, 2: MIT, 3: European Southern Observatory (ESO), 4: Charles University, 5: Observatoire de la Côted’Azur, 6: University of Hawaii, 7: NAOJ, 8: University of Tokyo, 9: NASA Johnson Space Center, 10: Universite de Liege, 11: Laboratoired’Astrophysique de Marseille, 12: Seoul National University, 13: Japan Spaceguard Association, 14: Kobe University, 15: Universidad Diego
PortalesThe surface of airless bodies like asteroids in
our Solar System are known to be affected by space
weathering. Experiments simulating space weathering
are essential for studying the effects of this process on
meteorite samples, but the problem is that the time spent
to reproduce space weathering in these experiments isbillions of times shorter than the actual phenomenon. The
T-type asteroid 596 Scheila underwent a collision with a
few-tens-of-meters impactor in December 2010 [1,2] andits surface was covered with fresh material [3]. A decade
later, there is an opportunity to study how the surface
layer of this asteroid is being altered by space weathering
after the impact. To do so, we perfor med visible
spectrophotometric and near-infrared spectroscopic
observations of 596 Scheila [4]. The acquired spectrum
is consistent with those observed shortly after the 2010
impact event within the observational uncertainty range
This indicates that the surface color of dark asteroids is
not noticeably changed by space weathering over a 10year period (Fig. 1). Our study is the first to investigate
color changes due to space weathering on an actual
asteroid surface in our Solar System (Fig. 2). Consideringthat fresh layers are regularly created on asteroid
surfaces by collisions, we suggest a genetic link between
D/T-type and dark (low albedo) X-complex asteroids andvery red objects such as 269 Justitia, 732 Tjilaki (and203 Pompeja). New observations show that 203 Pompeja
has a X-type-like surface, with some local surface areas
exhibiting a very red spectrum.

Figure 1: Spectra of the asteroid 596 Scheila

References[1] Ishiguro, M., et al.: 2011, ApJL, 740, L11.
[2] Ishiguro, M., et al.: 2011, ApJL, 741, L24.
[3] Haseagwa, S., et al.: 2022, ApJL, 924, L9.
[4] Haseagwa, S., et al.: 2022, ApJL, 939, L9.
Figure 2: Spectral slope for 596 Scheila against space weathering
time.

002

I Scientific Highlights

Over Seven Decades of Solar Microwave Data
Obtained with Toyokawa and Nobeyama Radio Polarimeters
SHIMOJO, Masumi1/2, IWAI, Kazumasa3
1: NAOJ, 2: SOKENDAI, 3: ISEE, Nagoya University

In Japan, we have a long history of observing total
solar microwave fluxes. It was started in May 1951 with
3.75 GHz at Research Institute of Atmospherics, Nagoya
University, then the monitoring observations werestarted with 1 GHz started in June 1957, 2 GHz started in
May 1957, and 9.4 GHz started in May 1956 at Toyokawa(Figure 1). In Nobeyama Solar Radio Observatory, Tokyo
Astronomical Observatory, the monitoring observations
with higher frequencies (17, 35, and 80 GHz) were started
in the late 1970s and early 1980s. These monitoring
observations are being continued at the NobeyamaCampus, NAOJ until now (Figure 1).

We summarized the history of the Toyokawa andNobeyama Radio Polarimeters, especially the instrument
history after the 1, 2, 3.75, and 9.4 GHz antennas weremoved from Toyokawa to Nobeyama, and explained thedetails of the solar microwave database (Figures 2&3)
provided by the Solar Data Archive System (SDAS)
operated by the Astronomy Data Center and Solar
Science Observatory, NAOJ.
The long-term solar microwave database is useful forunderstanding not only the long-term variation of thesolar activity but also the microwave emission from latetype stars.

Figure 2: Variations in total solar microwave fluxes over 70 years.
Red: 1 GHz, orange: 2 GHz, green: 3.75 GHz, blue: 9.4 GHz, andblack: Sunspot number.

Figure 3: Solar microwave spectra at solar maxima and minima.
Left panel: solar maxima, and right panel: solar minima. Colors
indicate solar cycles.

Figure 1: Upper panel: Toyokawa Radio Polarimeters (behind.
The antennas in front are the 8-element solar grating array.
Courtesy of the family of H. Tanaka) Lower panel: Nobeyama
Radio Polarimeters.

Reference[1] Shimojo, M., Iwai, K.: 2023, Geoscience Data Journal, 10,
114-129.

I Scientific Highlights003

Survival of Terrestrial N2-O2 Atmospheres in Violent XUVEnvironments by Efficient Atomic Line Radiative Cooling
NAKAYAMA, Akifumi1/2, IKOMA, Masahiro2/3/4, TERADA, Naoki5
1: Rikkyo University, 2: The University of Tokyo, 3: NAOJ, 4: SOKENDAI, 5: Tohoku University004

I Scientific Highlights

Altitude [km]10000

1FXUV,
3FXUV,
5FXUV,

1000

100
0

1000

2000

3000

4000

5000

Temperature [K]

6000

7000

8000

Figure 1: Effects of atomic line cooling on the upper-atmosphericstructure. Temperature profiles simulated with (solid lines) andwithout (dashed lines) atomic line cooling are shown for threedifferent XUV irradiation levels, one times (blue), three times(green), and five times (red) the present-day Earth’s one, FXUV, ⊕.
1000

Erossion timescaleof 1-bar atmosphere [Gyr]Observational efforts have recently been made tofind potentially habitable planets around M dwarfs,
including a radial velocity survey with Subaru-IRD.
In maintaining planetary habitability, meanwhile,atmospheres are known to have a crucial role. AroundM dwarfs and young Sun-like stars, planets receiving
the same insolation as the present-day Earth does are
exposed to intense stellar X-ray and extreme-ultraviolet(XUV) radiation. A fundamental question, then, arises
whether the present Earth's atmosphere could survive
in such harsh XUV environments. Previous theoreticalstudies suggest that the stellar XUV irradiation is intense
enough to remove atmospheres like the present-day
Earth's one completely on short timescales [1].
In this study [2], we develop a new upper-atmospheremodel and re-examine the thermal and hydrodynamic
response of the thermospheric structure of an Earth-like
N2-O2 atmosphere on an Earth-mass planet to increase
in XUV irradiation. The model includes newly theeffects of radiative cooling via electronic transitions in
the atoms (or atomic line cooling), in addition to thermoand photo-chemistry, thermal and chemical diffusion,adiabatic cooling, absorption of stellar IR radiation,and molecular IR radiative cooling, which previous
models already took into account. As shown in Figure 1,
we have found that the atomic line cooling dominates
over the hydrodynamic effect at XUV irradiation levels
higher than several times the present Earth’s level. As aconsequence, the atmosphere’s structure is kept almosthydrostatic, and its escape remains sluggish even at
XUV irradiation levels even up to thousand times thepresent Earth’s one.
The estimated lifetime of the 1~bar N2-O2 atmosphereis shown as a function of the XUV irradiation level in
Figure 2. Our estimates for the Jeans escape rates of
N2-O2 atmospheres suggest that the 1-bar atmospheres
survive in early active phases of Sun-like stars except
for rapid rotators. Even around rapidly rotating Sunlike stars and M dwarfs, the N 2 -O 2 atmospheres ofseveral bars could avoid a significant thermal loss ontimescales of Gyr. Those results give new insights into
the habitability of terrestrial exoplanets and the Earth’s
climate history.

100

10

1

1

10

100

XUV irradiation level [present Earth]

1000

Figure 2: Estimated lifetime of the 1 bar N 2 -O 2 Earth-likeatmosphere. We have estimated the lifetime, dividing the mass ofpresent Earth’s atmosphere by the mass-loss rate calculated fromour model for each XUV irradiation flux.

References[1] Tian, F., et al.: 2008, JGRE, 113, E05008.
[2] Nakayama, A., Ikoma, M., Terada, N.: 2022, ApJ, 937, 72.

Narrow Fe-Kα Reverberation Mapping Unveils the DeactivatedBroad-Line Region in a Changing-Look Active Galactic Nucleus
NODA, Hirofumi1, MINETA, Taisei1, MATSUMOTO, Hironori1, MINEZAKI, Takeo2, SAMESHIMA, Hiroaki2,
HORIUCHI, Takashi2, KOKUBO, Mitsuru3, MORIHANA, Kumiko3, KAWAMURO, Taiki4,
YAMADA, Satoshi4, WATANABE, Makoto5, ITOH, Yoichi6, KAWABATA, Koji S.7, FUKAZAWA, Yasushi7
1: Osaka University, 2: University of Tokyo, 3: NAOJ, 4: RIKEN, 5: Okayama University of Science, 6: University of Hyogo, 7: Hiroshima
University

Kα emission region and its relation to the BLR utilizing
both the temporal and precise line profile information.

Suzaku 2–10 keV continuum
Swift 2–10 keV continuum
Suzaku narrow Fe-Kα line

4

6

3

4

2

2

1

Fe-Kα flux (10-13 erg s-1 cm-2)

2–10 keV continuum flux (10-11 erg s-1 cm-2)

800Flux density (mJy)

Active Galactic Nuclei (AGN) are luminous compact
object powered by mass accretion onto supermassive
black holes (SMBH). The primary X-ray and UV/opticalcontinua (from the central X-ray corona and accretion
disk, respectively) irradiate surrounding gas/dust clouds
that produce secondary emission such as emission linesand dust thermal emission. In the X-ray band, the mostprominent emission line feature commonly observedin AGNs is the Fe-Kα fluorescence line at 6.4 keV. Dueto the observational difficulty of precisely measuring
the narrow (~ 1000–2000 km/s) Fe-Kα line profile withexisting X-ray satellites (e.g., [1,2]), it is still under
debate where this prominent emission line is originatedfrom.
Since the AGN emission shows f lux variability
on time scales of days-to-years, we can expect new
observational constraints on the spatial extent of the FeKα emission region to be obtained from the temporal
information. To this end, we performed multi-epoch
X-ray and optical observations targeting for a Seyfert
galaxy NGC 3516 in 2013-2015 with Suzaku and Japaneseground-based telescopes in the OISTER framework([3,4]). The X-ray and optical B-band light curves, alongwith the archival Swift X-ray continuum data points, areshown in Figure 1.
NGC 3516 showed large f lux variations both in
the X-ray and optical bands over the observing period(NGC 3516 is a Changing-Look AGN; [5]), that enabled
us to measure the time lags between light curves of
the X-ray corona continuum, optical accretion disk
continuum, and the Fe-Kα emission line; the opticalto-X-ray continuum lag was 2.0 +0.7
−0.6 days, and the FeKα line-to-X-ray continuum lag was 10.1 +5.8
−5.6 days.
This is the second detection of the 6.4 keV Fe-Kα lag in
AGNs after the marginal detection in a Seyfert galaxy
NGC 4151 ([6]). The measured time lags are consistent
with the ‘lamp-post picture’ in that the variable X-ray
corona emission drives the flux variations of the disk
optical continuum (Rdisk ~ 2 lt-days) and Fe-Kα (RFe-Kα ~10 lt-days).
The inferred size of the Fe-Kα emission region
coincides with that of the broad-line region (BLR).
Future multi-epoch high-resolution X-ray spectroscopy
with XRISM will enable us to further constrain the Fe-

2

Optical (B band + 0.5 mJy)

1
0
56000

56200

56400

56600
MJD

56800

57000

57200

Figure 1: The X-ray and optical light curves of NGC 3516 ([4]).
Top: Suzaku/XIS and Swift/XRT X-ray 2–10 keV continuum(black) and Suzaku/XIS Fe-Kα emission line (red). Bottom:
optical B-band accretion disk continuum.

References[1] Shu X. W., et al.: 2010, ApJS, 187, 581.
[2] Shu X. W., et al.: 2011, ApJ, 738, 147.
[3] Noda, H., et al.: 2016, ApJ, 828, 78.
[4] Noda, H., et al.: 2023, ApJ, 943, 63.
[5] Shapovalova, A. I., et al.: 2019, MNRAS, 485, 4790.
[6] Zoghbi A., Miller J., Cackett E.: 2019, ApJ, 884, 26.

I Scientific Highlights

005

Millimeter Methanol Emission
in the High-mass Star-forming Region G24.33+0.14
HIROTA, Tomoya

			 (NAOJ)

Maser Monitoring Organization (M2O)

We have been conducting monitoring observationsof astronomical maser sources under international
collaboration with Maser Monitoring Organization(M2O; https://www.masermonitoring.org). One of the
purposes of the M2O is to detect sudden increase of themaser emission (maser flares) by a global network ofradio telescopes.
In the course of the M2O monitoring, a flare of the
6.7 GHz methanol (CH3OH) maser was observed toward
the high-mass star-forming region G24.33+0.14 (7.2 kpc
from the Sun) in September 2019 using the Torun 32-m
radio telescope in Poland [1]. G24.33+0.14 experienced asimilar flare in 2010–2012, suggesting repeating/periodic
flare activity with an 8-year interval. As reported forsome of the methanol maser f lare events, it could betriggered by an episodic mass accretion event (accretion
burst) in a high-mass protostar.
Using the Atacama Large Millimeter/submillimeter
Array (ALMA) in the Director’s Discretionary Time
(DDT), we carried out a Target-of-Opportunity (ToO)
observations of the millimeter continuum and molecularlines toward G24.33+0.14 in mid-September 2019
(ALMA Cycle 6), 20 days after the onset of the maser
f lare [2]. Combined with the ALMA data taken in
the pre-f lare phase in August 2016 (ALMA Cycle 3),
we investigated possible variability of the millimeteremission in G24.33+0.14.
In G24.33+0.14, we identified a massive (~60 M⊙)
and compact (~2000 au) millimeter core C1 associatedwith the 6.7 GHz methanol masers. The continuum flux
density of C1 showed a marginal increase in Cycle 6
with a flux ratio (Cycle 6/Cycle 3) of 1.16 ± 0.01, which iscomparable to the absolute flux calibration uncertainty
of 10 %. Other than methanol, we also compared the
26 molecular line emission identified in G24.33+0.14
between Cycle 3 and Cycle 6, and found almost thesame f lux ratios as that of the continuum emission,
with an average and standard deviation of 1.12 ± 0.15.
On the other hand, we found that 8 identified methanollines including a torsionally excited transition and a 13C
isotopologue showed a slightly larger flux increase withthe average ratio of 1.23 ± 0.13 (Figure 1). Furthermore,
the methanol lines at higher excitation states tend tohave larger flux increases. If this systematic trend of
the flux increase in the methanol lines is significant, it
would suggest radiative heating in the central part of thecontinuum source C1 due to an episodic accretion event.

References[1] Wolak, P., et al.: 2019, The Astronomer's Telegram, 13080, 1.
[2] Hirota, T., et al.: 2022, PASJ, 74, 1234.

Figure 1: (a) Moment 0 map of the CH 3OH 229.589 GHz (154 -163 E) line for the Cycle 3 data. Contour levels are 4, 8, 16, ..., times therms noise level of 18.7 mJy beam−1 km s−1. A magenta cross and gray square indicate positions of the continuum peak C1 and the 6.7 GHz
methanol maser flare, respectively. (b) Same as (a) but for the Cycle 6 data. The rms noise level is 13.4 mJy beam−1 km s−1. (c) Differential
image of the moment 0 maps between Cycle 3 and Cycle 6. The rms noise level is 23.5 mJy beam−1 km s−1. (d) Spectra of the 229.589 GHz
methanol line in Cycle 3 and Cycle 6.

006

I Scientific Highlights

The Resolved Feature at the Center of M87
Found from EHT Public Data
MIYOSHI, Makoto1, KATO Yoshiaki2/3, JUNICHIRO Makino4
1: NAOJ, 2: RIKEN, 3: Japan Meteorological Agency, 4: Kobe University

We also investigated why the EHTC ring image was
acquired. The ring-like structures of the EHTC can becreated not only from the public data but also from thesimulated data of a point image and noise. Also, therings are very sensitive to the field-of-view (FOV) size.
The u-v coverage of EHT for M87 lacks ~ 40 μas fringe
spacings. Combining with a very narrow FOV, it createdthe ~ 40 μas ring structure. One more to note is that the
EHTC performed simulations searching for appropriate
imaging parameters, but there are deficiencies. Because
the EHTC's simulations only take into account the
reproduction of the input image models, and not thoseof the input noise models, their optimal parameters
can enhance the effects of sampling bias and produce
artifacts such as the ~ 40 μas ring structure, rather than
reproducing the correct image.
We conclude that the absence of the jet and thepresence of the ring in the EHTC result are both artifacts

owing to the narrow FOV setting and the u-v data
sampling bias effect of the EHT array 2017.

Relative Declination (Pixel)

We report the result of our independent image
reconstruction of the M87 from the public data of the
Event Horizon Telescope Collaboration (EHTC). Our
result is different from the image published by the EHTC.
Our analysis shows that (a) the structure at 230 GHz
is consistent with those of lower-frequency very long
baseline interferometry observations, (b) the jet structure
is evident at 230 GHz extending from the core to a few
milliarcsecond, although the intensity rapidly decreases
along the axis, and (c) the “unresolved core” is resolved
into three bright features presumably showing an initial
jet with a wide opening angle of ~ 70°.
The EHTC ring image had un-reasonable features,such as the jets not being visible, the maximum
brightness temperature being too low, the flux density
not being reproduced, and obtaining a ring with the same
diameter as the spacing between the main beam and thefirst sidelobes seen in the structure of the point spreadfunction.
On the other hand, our image shows that (d) theimage reproduces the higher brightness temperature(~ 1011 K) and comparable flux density as that indicatedby the observed data (~ 1 Jy), and that (e) comparing
the amount of residuals between the data and thereconstructed image, our results show smaller residuals
about 1/2 to 1/3 times than those of the EHTC ring
image. Therefore, our resulting images (central core-knot
structure and elongated jet structure) are more reliable.

Relative Right Ascension (Pixel)

Figure 1: Image reconstructed from public data of EHT 2017
observations of M87, revealing a jet structure missed in the EHTC
analysis. The inset is an averaged image of M87 from VLBA
43 GHz observations added for comparison.

Figure 2: Core (C) and knots (K, W) structure found at the centerof M87. The directions of the C-K and C-W lines are the same as
those of the ridges found in the 43 GHz observations. The axis of
the average jet direction bisects the angle KCW.

Reference[1] Miyoshi, M., Kato Y., Makino, J.: 2022, ApJ, 933, 36.

I Scientific Highlights

007

Automated Sunspot Detection
as an Alternative to Visual Observations
HANAOKA, Yoichiro(NAOJ)008

I Scientific Highlights

(a)

(b)

(c)

(d)

(e)

(f)

Figure 1: Sunspot detection results for some portions in a whitelight image on 2014 February 28 taken with the Solar Flare
Telescope. Resutls of sunspot detection for regions shown inpanels (a)–(c) are presented in panels (d)–(f). Penumbrae andumbrae are indicated with red and green patches, respectively.

Number of Sunspots(a) 50
40

SST
KO
SFT
KSM
SM

30
20
10
0
0

100

200
Day of Year (2021)

300

100

200
Day of Year (2021)

300

2

(b)
Ratio

Sunspot numbers present the variation in solar
activity for more than 400 years, and it is important
to continue the derivation of the sunspot number. The
sunspot number counts are still based on hand-drawn
sketches obtained by visual observations. Therefore,
automated detection of sunspots on digital white-lightimages, which enables objective sunspot counting withsmall manpower, is required.
For this reason, NAOJ changed the sunspot counting
met hod f rom ha nd- d raw n v isu al obser vat ion toautomated sunspot detection based on digital images
in 1998 [1]. However, the quality of images is not very
high, and detections of false spots and missed detectionsof true spots often occur. Therefore, we have started
higher-quality imaging observation with the Solar Flare
Telescope at Mitaka and developed another method ofwhich the performance is comparable to that of visualobservations [2]. An example of the results of theautomated detection is shown in Figure 1.
To identify small spots correctly, the quiet-disk
component of the Sun, which is used as a reference toidentify sunspots using a threshold, is derived accurately.
This threshold is determined using an adaptive method
to process images obtained under various conditions.
To eliminate the seeing effect, our method can process
multiple images taken within a short time.
We applied the developed method to digital images
captured by three different observers (the Solar Flare
Telescope, Kawaguchi Science Museum, and an amateur
observer Mr. S. Morita) and compared the detection
results with those of visual observations by Specola
Solare Ticinese and Kwasan Observatory of Kyoto
University. Figure 2(a) presents the number of sunspots
detected by these observations during 2021. Because
they show significant scatter, the monthly-mean ratios of
the number of sunspots with respect to that of the Solar
Flare Telescope are shown in Figure 2(b). The numbersof sunspots detected on the digital images are between
two visual observations. We conclude that the proposedsunspot detection method has a similar performance tothat of visual observation. This method can process datataken with various instruments, and therefore, it can be
widely used by public observatories and amateurs as wellas professional observatories as an alternative to handdrawn visual observation for sunspot counting.

1

0.5
0

SST
KO
KSM
SM

Figure 2: Comparison of detection results based on digital whitelight images and visual observations for 2021. (a) Daily numberof sunspots obtained by automated detection for data taken by the
Solar Flare Telescoe (SFT), Kawaguchi Science Museum (KSM),
and Mr. S. Morita (SM) and those by Specola Solare Ticinese (SST)and Kwasan Observatory (KO) visual observations. (b) Ratio of
the number of sunspots detected with KSM, SM, SST, and KO
observations to those by the SFT each month.

References[1] Imai, H., et al.: 1998, Rep. Nat. Astron. Obs. Japan, 4, 1.
[2] Hanaoka, Y.: 2022, Solar Phys., 297, 158.

Optical IFU Observations of GOALS Sample with KOOLS-IFU
on Seimei Telescope: Initial Results of Nine U/LIRGs at z < 0.04
TOBA, Yoshiki1/2/3/4/5, YAMADA, Satoshi6/2, MATSUBAYASHI, Kazuya7/1, TERAO, Koki1/8,
MORIYA, Aoi3, UEDA, Yoshihiro2, OHTA, Kouji2, HASHIGUCHI, Aoi3, HIMOTO, Kazuharu5,
IZUMIURA, Hideyuki1, JOH, Kazuma5, KATO, Nanako5, KOYAMA Shuhei7/5,
MAEHARA, Hiroyuki1, MISATO, Rana3, NOBORIGUCHI, Akatoki9/8/5, OGAWA, Shoji2,
OTA, Naomi3, SHIBATA, Mio3, TAMADA, Nozomu5, YANAGAWA, Anri3, YONEKURA, Naoki5,
NAGAO, Tohru5, AKIYAMA, Masayuki8, KAJISAWA, Masaru5, MATSUOKA, Yoshiki5
1: NAOJ, 2: Kyoto University, 3: Nara Women’s University, 4: ASIAA, 5: Ehime University, 6: RIKEN, 7: University of Tokyo, 8: Tohoku
University, 9: Shinshu University

References[1] Armus, L., et al.: 2009, PASP, 121, 559.
[2] Stierwalt, S., et al.: 2013, ApJS, 206, 1.
[3] Kewley, R., et al.: 2006, MNRAS, 372, 961.
[4] Toba, Y., et al.: 2022, PASJ, 74, 6.

(b) BPT diagram(a) Intensity map

Strength of ionized gas outflow

Figure 1: (a) Intensity maps and (b) 2D BPT diagram for NGC
7674.

Strength of ionized gas outflow

Galaxy mergers are one of the key phenomena
for understanding the co-evolution of galaxies andsupermassive black holes (SMBHs). To understand how
galaxy mergers affect SMBHs and their host galaxies,
spatially resolved observations with IFU are essential.
In particular, ultra/luminous infrared galaxies (U/LIRGs) with L IR > 1011 L ⊙ show disturbed features intheir optical images and are thought to be an important
population to study the relationship between galaxy
mergers and co-evolution, even from the theoretical pointof view. We have performed IFU observations of U/
LIRGs using the KOOLS-IFU on the Seimei Telescope.
The targets were selected from 245 U/LIRGs from theGreat Observatories All-sky LIRG Survey (GOALS;[1]). We picked up a few U/LIRGs from each of the fivegalaxy merger stages visually classified from IRAC/
Spitzer images in [2] and nine objects selected as targets
and observed during 2019–2020.
We have successfully detected various emission
lines for star-forming galaxies (SFGs) and/or active
galactic nuclei (AGNs) (e.g., Hα, Hβ, [O III]λλ4959,5007,[N II]λλ6549,6583, [S II]λλ6716,6731). This allowed for
creating 2D intensity maps of these emission lines and
BPT diagrams (AGN/SFG diagnostics using emission
line ratios: e.g., [3] (Figure 1). We employed a value by
combining velocity shift and the velocity dispersion of
the broad component of [O III] line (σ0) as an indicator of
the strength of the AGN-driven outflow. We investigated
how σ0 depends on the distance from the galactic centerand the merger stage. We found that AGN outf lows
become stronger (1) towards the galactic center and (2)as a sequence of merging stages (Figure 2), suggestingthat galaxy mergers could induce AGN-driven outflows
[4].

(a)

Galaxycentergalaxyoutskirts(b)

Early-stage Mid-stageLate-stage

Figure 2: Dependence of an indicator of the strength of ionizedgas outflow (σ 0) estimated from [O III] emission line profiles on (a)distance from the galactic center and (b) galaxy merger stage.

I Scientific Highlights

009

Exploring Cosmic Dawn and Epoch of Reionization with 21 cm LineSHIMABUKURO, Hayato1, HASEGAWA, Kenji2, KUCHINOMACHI, Akira3,
YAJIMA, Hidenobu4, YOSHIURA, Shintaro5
1: Yunnan University, 2: Nagoya University, 3: Kumamoto University, 4: University of Tsukuba, 5: NAOJ

After the Big Bang, there was a period in the universe
when there were no stars or galaxies. This is called the
Dark Ages. Then the first stars and galaxies formed in
the universe, and the Cosmic dawn began. Ultraviolet
photons emitted from these first objects ionized theintergalactic medium (IGM). This epoch is called theepoch of reionization (EoR) [1]. Through the observationof galaxies at high redshift such as the James Webb Space
Telescope (JWST), galaxies have already been foundin the EoR [2]. The ionization state of the IGM in the
middle to late stage of EoR is gradually being revealed.
However, to better understand the EoR and the cosmic
dawn, it is more effective to study the IGM more directly,
combined with observing galaxies.
To study these periods, we focus on the 21 cm line
signal. The 21 cm line is emitted from neutral hydrogenatoms due to the hyperfine structure, which corresponds
to the transition between two energy levels of neutralhydrogen atoms. The 21 cm signal can be expressed byδTb (x, z) ≈ 27xHI (x, z) [1 + δm (x, z)]][]−1[Tγ (z)
1 dv∥
1+
× 1−
TS (x, z)H(z) dr∥)) 12 ((Ωb h2
1 + z 0.15[mK].
×10 Ωm h2
0.023

(1)

The 21 cm line signal contains useful information such as
the neutral fraction of the IGM, xHI, the spin temperature,
TS, and cosmological parameters.
We review the current progress of the cosmic dawn
and EoR studies, with a focus on the use of the 21 cm
line signal in our paper [3]. The review paper is divided
into six sections. In section 1, we introduce the various
topics of the high-z universe and provide an overview ofour study. In section 2, we review the essential physics
of the 21 cm line, including what physical mechanism
determines the 21 cm line signal. In section 3, we focus
on astrophysics that affects the 21 cm line signal, witha particular emphasis on the impact of the first stars on
the 21 cm signal. Section 4 reviews how astrophysicalinformation can be statistically extracted from the 21 cm
line signal. In section 5, we introduce the synergy of the
21 cm line with extract more information about EoR.
Finally, in section 6, we review the current status of radio
interferometers related to studying cosmic dawn and EoR
using the 21 cm line signal.

010

I Scientific Highlights

Currently, radio telescopes such as MWA, LOFAR,
and HERA, which are designed to observe the 21 cm
line, are in operation and have already begun to constrain
the 21 cm line power spectrum, although they have notdetected it [4]. In addition, the Square Kilometer Array(SKA) is planned to begin the observation in the near
future, and construction has already begun [5]. It is
expected that the research on the EoR and the cosmic
dawn using the 21 cm line will become increasingly
active, and this review paper is expected to be usefulfor a comprehensive understanding of EoR and cosmic
dawn studies using the 21 cm line. It is also useful as areference for those interested in entering the 21 cm line
research.

References[1] Zaroubi S.: 2013, ASSL, 396, 45.
[2] Harikane Y., et al.: 2023, arXiv, arXiv:2304.06658.
[3] Shimabukuro H., et al.: 2023, PASJ, 75, S1.
[4] Barry N., et al.: 2022, JATIS, 8, 011007.
[5] https://www.skao.int/

ALMA Lensing Cluster Survey: Properties of Millimeter Galaxies
Hosting X-ray Detected Active Galactic Nuclei
UEMATSU, Ryosuke1, UEDA, Yoshihiro1, KOHNO, Kotaro2, YAMADA, Satoshi3, TOBA, Yoshiki4/5/6,
FUJIMOTO, Seiji7/8, HATSUKADE, Bunyo2, UMEHATA, Hideki9, ESPADA, Daniel10/11, SUN, Fengwu12,
MAGDIS, Georgios E.7/13/8, KOKOREV, Vasily14/7/8, AO, Yiping15
1: Kyoto University, 2: The University of Tokyo, 3: RIKEN, 4: NAOJ, 5: Academia Sinica Institute of Astronomy and Astrophysics, 6: Ehime
University, 7: Cosmic Dawn Center, 8: University of Copenhagen, 9: Nagoya University, 10: Universidad de Granada, 11: Facultad de Ciencias,
12: University of Arizona, 13: Technical University of Denmark, 14: University of Groningen, 15: Purple Mountain Observatory and Key
Laboratory for Radio Astronomy

The averaged growth rate of galaxies and SMBHs
reached a peak at z = 1–3, which is often referred to as“cosmic noon”. Thus, galaxies hosting active galactic
nuclei (AGNs) at these epochs are a key population toreveal the mechanisms of galaxy-SMBH co-evolution.
Submillimeter and X-ray observations are powerful tools
to study this population. This is because infrared radiationfrom star-formation activity at these redshifts is observedin millimeter bansd (submillimeter galaxies; SMGs),
while X-ray observations can detect the obscured AGNs.
Utilizing ALMA in cycle-6, our team has performed an
extensive survey with ALMA, called the ALMA Lensing
Cluster Survey (ALCS; Project ID: 2018.1.00035.
L; PI: K. Kohno). This survey covers 134 arcmin2 anddetects 180 secure sources at z ~ 0.5–6 with a flux limitof ~0.2 mJy at 1.2 mm [1]. Here we report the multiwavelength properties of millimeter galaxies hosting
X-ray detected AGN in the ALCS sample.
Chandra observed the ALCS fields on multiple
occasions since 1999. We processed all the data obtainedby 2017, and performed source detection. Then, We
cross-matched the Chandra-detected sources with the
ALMA source list. We found three X-ray counterparts inthe cluster fields of Abell370, MACSJ0416.1–2403, and
MACS0329.7–0211, where the total exposure times of
the Chandra observations are 96.3 ks, 328 ks, and 77.5
ks, respectively. The source names are A370-ID110,
M0416-ID117, and M0329-ID11, and the redshifts are
1.06 (spec-z), 2.09 (spec-z), and 2.84 (photo-z); hereafter
we refer to these X-ray AGNs as “ALCS-XAGNs”.
First, we perform an X-ray spectrum analysis. We fit
the observed X-ray spectra with a simple absorbed powerlaw model. We find that M0416-ID117 and M0329ID11 are not significantly absorbed (log NH/cm−2 < 23),
while A370-ID110 shows signs of moderate absorption(log N H /cm −2 ~ 23.5). This suggests that the former
are type-1 AGNs and the latter is a type-2 AGN. After
that, we perform SED modelling of X-ray to millimeterphotometries with CIGALE [2]. We find that all the X-ray
AGNs are classified as ultra-luminous infrared galaxies(ULIRGs; log L IR/L⊙ > 12) and show high star-forming−1
rates (SFR >~ 100 M⊙ yr ).
Figure 1 plots de-absorbed X-ray luminosity versus

SFR. For comparison, we plots other ALMA and Chandra
selected AGN samples (i.e., X-ray detected AGNs in
ALESS, UDF, ASAGAO, and AS2UDS) at z = 1–3. We
also plots the X-ray selected broad line AGNs at z =1.18–
1.68 in the SXDF as a sample with a different selection
method. We find that ALCS-XAGNs show higher X-ray
luminosities (~ mass-accretion rates) than other ALMA
selected X-ray AGN samples. We also confirm that
ALCS-XAGNs show higher SFRs than a purely X-rayselected AGN sample. This can be explained by theselection bias, showing that a wide and deep survey with
ALMA, combined with medium-depth X-ray data, canefficiently detect intense growth stage of both galaxies
and SMBHs in high-redshift universe. According to themerger-driven evolutionary scenario, the galaxies and
SMBHs “co-evolve” during major mergers being deeply
embedded by gas and dust, and then evolved to the AGN
dominant phase with quenched SFRs by AGN feedback.
If this scenario is applicable, our sources may correspondto the transition stage where the merging has finished, but
the star formation is not yet quenched.

Figure 1: de-absorbed X-ray luminosities versus SFRs. The solidand dashed blue lines represent the relation of galaxy-SMBH
simultaneous evolution.

References[1] Fujimoto, S., et al.: 2023, arXiv:2303.01658[2] Yang, G., et al.: 2022, ApJ, 927, 192.

I Scientific Highlights

011

WISE/NEOWISE Multiepoch Imagingof the Potentially Geminid-related Asteroids:(3200) Phaethon, 2005 UD, and 1999 YC
KASUGA, Toshihiro

MASIERO, Joseph R.

				 (NAOJ)			 (Caltech/IPAC)

Recently, the large-scale structure in the distantuniverse has been explored through the distributionof various galaxy populations. On the other hand, it is
not necessarilWe study space-based thermal infraredobservations of the presumably Geminid-associatedasteroids: (3200) Phaethon, 2005 UD, and 1999 YC using
Wide-field Infrared Survey Explorer/Near-Earth Object
WISE. WISE, the full sky survey simultaneously obtained
the infrared data at the four infrared wavelength bands
3.4micron (W1), 4.6micron (W2), 12micron (W3), and22micron (W4) in 2010. The NEOWISE survey started in
December 2013 and is ongoing project taking the shorter
two-bands at W1 and W2.
Here, we note the primary candidate Phaethon.
Phaethon seems to be dynamically associated with theGeminid meteoroid stream. The Geminid meteoroid
stream consists of near millimeter-scale or larger solid
particles, up to tens of centimeters, as measured by radarand lunar impact flushes. The notable orbital feature ofboth is the small perihelion distance, q = 0.14 au, where
repeatedly exposed to intense thermal process which
possibly causes the Phaethon's recurrent activity.
Spectroscopic measurements of sodium (Na) content
of the Geminid meteors have been utilized for studying
the thermal processes on Phaethon. The Geminids exhibit
the extreme variety in their Na content, from depletion(free) of the Na abundance to near solar-like values. The
thermal desorption of Na is unlikely to occur for theGeminid stream phase even at q = 0.14 au. It takes toolong timescale to sublimate Na compared to the stream
age. Therefore the Na-loss observed in the Geminids
must have originated from the thermal process of theparent, Phaethon [1].
The WISE/NEOWISE multiple observing epochs of
the infrared data provide with information about wherein the orbit the object is along with the limits, as wemight expect a strong variation in production at different
points in the orbit. Another motivation is to find an
activity mechanism far from perihelion, which is different
from thermal-driven. This study provides a groundwork
for JAXA DESTINY+, which is planning to flyby at a
distance of 500 km from Phaethon in 2028.
We find no strong variation in the production rate atdifferent epochs, and find no dependency on the locationof the object in the orbit at the time of observation. No
evidence of lasting mass loss found in the W1 image.
The maximum dust production rate is 2 kg s−1, suggesting012

I Scientific Highlights

no strong dependency on heliocentric distance at
1.0–2.3 au. We find neither dust trail (Geminid stream)from Phaethon nor co-moving objects in the W3 and W4
images at the heliocentric distance of 2.3 au. The upper
limit to the optical depth along the trail direction is 7 ×
10−9. Correspondingly, during the DESTINY+ flyby phase(at 500 km distance), a few 500micron-sized particles areto be encountered by the dust analyzer. Those moderately
large particles might be the Gemindis, insensitive to theradiation pressure sweeping. On the other hand, when
DESTINY+ passes at 50,000 km distance from Phaethon,
several 10micron-sized particles are to be captured by the
instrument [2].

Figure 1: Composite W3-band image of Phaethon in 17.6 s
integration (2 × 8.8s) taken by WISE on UT 2010 January 7. The
frame size is 200″ × 200″.

References[1] Kasuga, T., Jewitt, D.: 2019, Chapter 8 in Meteoroids: Sourcesof Meteors on Earth and Beyond (Cambridge Univ. Press), 187− 209.
[2] Kasuga, T., Masiero, J. R.: 2022, AJ, 164, 193.

Comparison of Size Distributions between L4 and L5 Jupiter Trojans
UEHATA, Kotomi1, TERAI, Tsuyoshi2, OHTSUKI, Keiji1, YOSHIDA, Fumi3
1: Kobe University, 2: NAOJ, 3: University of Occupational and Environmental Health

Jupiter Trojans (JTs) are asteroid swarms liberatingaround the L4 and L5 Lagrangian points of Jupiter. They
can provide clues for elucidating the formation processof the solar system, thus NASA is currently conducting aspacecraft mission for flyby exploration of several JTs [1].
As for their origin, models of their capture by Jupiter into
the current Trojan region when giant planets experienced
orbital instability seem to be promising, but further
studies are desirable. One of the clues to clarify their
origin is the size-frequency distribution (object diametervs. number) of the L4 and L 5 swarms. In the case of
capture due to orbital instability, as mentioned above,the shape of both size distributions is expected to be thesame, otherwise different effects should be involved.
Although this should be examined by observational
studies, it was difficult because a sample of small (kmsized) L5 JTs was very limited. A previous studies showedthat the L 4 and L 5 swarms may have different size
distributions, however, the number of the detected objects
were insufficient so that the measurement accuracy was
not very high.
We therefore performed a survey observation over
~15 deg2 of sky in the Jupiter L5 region using Hyper
Suprime-Cam (HSC) mounted on the Subaru Telescope.
As a result of our data analysis similar to the previous
studies for L4 JTs with HSC [2], we detected 189 L5
JT objects from the survey data with a detection limitof 24.1 mag in the r band which corresponds to ~2 kmof diameter assuming a geometric albedo of 0.05. We
found that the size distribution derived from the unbiased
sample consisting of 87 objects in the diameter range of~2–10 km can be approximated by a single-slope powerlaw with an index for the differential absolute magnitude
distribution of α = 0.37 ± 0.01, which well coincides withthat of L4 JTs [3].
By combining our results with the size distribution of
known L5 JTs, we also found that the shapes of the size
distributions of L4 and L5 JTs agree well with each otherover the entire size range of ~2–100 km (see Figure 1).
The ratio of the total number of asteroids larger than 2 km
in diameter between the two swarms was figured out at
NL4/NL5 = 1.40 ± 0.15. The total number of all JTs larger
than 1 km in diameter is estimated to be 2.6 × 105, which
is one digit smaller than that of main-belt asteroids in thesame size range (~2 × 106 [4]).

Figure 1: Size frequency distributions of L 4 (squares) and L5(circles) swarms of Jupiter Trojans combining the measurement
results by Subaru/HSC observations [2,3] with known asteroids
taken f rom the Minor Planet Center catalog, which werenormalized by absolute magnitude of 17.0 mag corresponding to
2 km in diameter assuming a geometric albedo of 0.05.

References[1] Levison, H. F., et al.: 2021, PSJ, 2, 171.
[2] Yoshida, F., Terai, T.: 2017, AJ, 154, 71.
[3] Uehata, K., et al.: 2022, AJ, 163, 213.
[4] Maeda, N., et al.: 2021, AJ, 162, 280.

I Scientific Highlights

013

Mass Function of a Young Cluster
in a Low-metallicity Environment. Sh 2-209
YASUI, Chikako1, KOBAYASHI, Naoto2, SAITO, Masao1, IZUMI, Natsuko3, IKEDA, Yuji4
1: NAOJ, 2: University of Tokyo, 3: Academia Sinica Institute of Astronomy and Astrophysics, 4: Photocoding

The outer part of spiral galaxies, such as our own
Galaxy, and dwarf irregular galaxies are known tohave low metallicity (~ −1 dex) and to be in a different
environment than the solar neighborhood. Amongthem, the outer Galaxy is closest, making them theonly environment suitable for observational studies ofindividual stars spatially resolved, as is the case in thesolar neighborhood. We have already observed about 10
young star-forming clusters in the outer Galaxy using theSubaru Telescope in the near-infrared wavelength range.
However, because the number of stars in these targets has
not been sufficient (Nstars ~ 100), the initial mass function
has not been derived with high accuracy.
In this study, we performed near-infrared imaging
observations of a star-forming region Sh 2-209 in a lowmetal abundance environment ([O/H] = −0.5 dex) using
the Subaru Telescope MOIRCS (Figure 1), and identified
two star-forming clusters in S209. We developed acode for fitting a model luminosity function with threeparameters, the initial mass function, age, and distance,
and fitted the observed clusters to the luminosity function(Figure 2). The results confirm that i) the distanceobtained from the fitting is consistent with those obtainedwith Gaia EDR3 based on parallaxes (2.5 kpc). This is
close enough to enable us to resolve cluster members
clearly (≃1000 au separation) down to a mass-detection
limit of ≃0.1 M⊙, with individual cluster scales (~1 pc).
ii) The initial mass function has a slightly flat highmass slopes (Γ ≃ −1.0) compared to the Salpeter slope(Γ = −1.35), which is generally obtained in the solar
neighborhood. iii) On the other hand, the peak mass of theinitial mass function is suggested to be slightly smaller(≃0.1 M⊙) compared to the masses usually seen in thesolar neighborhood (~0.3 M⊙). In particular, because theS209 main cluster is a star-forming cluster with a larger
number of members (~1500) than the numbers in regions
previously studied in such environments, it is possible
for the first time to derive the IMF in a low-metallicity
environment with high accuracy over the wide mass
range 0.1–20 M⊙ [1].

Reference[1] Yasui, C., et al.: 2023, ApJ, 943, 137.

014

I Scientific Highlights

Figure 1: NIR color image for S209.

Figure 2: The obtained KLF and IMF for the S209 cluster. Left:
Obtained cluster KLF (blue histogram) and model KLF for the
best-fit IMF (red). Right: Best-fit IMF (black line) and IMFs
previously obtained in the field nearby star clusters (colored lines).

Configuration of Probe Tones for MKID Readout
with Frequency Sweeping Scheme
NAGAI, Makoto1, MURAYAMA, Yosuke1/2, NITTA, Tom2/3, SUZUKI, Ryoji2, HIKAWA, Ryotaro2,
MIYAZAWA, Hiromu2, NOJI, Ryohei2, KIUCHI, Hitoshi1, SEKIMOTO, Yutaro4, MATSUO, Hiroshi1,
SHAN, Wenlei1, NARUSE, Masato5, NOGUCHI, Takashi6, KUNO, Nario2/3, MONFARDINI, Alessandro7,
MACIAS-PEREZ, Juan8, GOUPY, Johannes7, CALVO, Martino7, CATALANO, Andrea8
1: NAOJ, 2: University of Tsukuba, 3: Tomonaga Center, 4: ISAS, JAXA, 5: Saitama University, 6: The University of Electro-Communications,
7: Institut Néel, CNRS and Université Grenoble Alpes, 8: Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3

We are developing detector arrays using microwave
kinetic inductance detectors (MKIDs) for astronomical
observations in the 100-GHz band and a readout system
for MKID arrays [1] with frequency sweeping scheme [2].
Probe tones in this scheme are generated and acquiredby a frequency sweep probe (FSP) which is a digital fast
Fourier transform spectrometer (FFTS) while the probe
tones are converted and modulated by an intermediate
frequency (IF) section. Since the values of the resonancefrequencies change under different photon backgrounds,
an appropriate method to configure the probe tones isessential to preserve the dynamic of the detected signals.
We considered a general IF section which is a cascade ofup/down converter pairs and found that its characteristics
can be described with the base band, the target band,the sign of probe tone order, and the sign of frequency
sweep direction [3]. We implemented an algorithm tomake a list of tone frequencies from a list of resonancefrequencies given (Figure 1). Using this configuringmethod, we assembled IF sections for an antenna-coupled
MKID array and for a LEKID array [4] and set up a
prototype FSP. The resonance frequencies of the antennacoupled MKIDs and the LEKIDs are at 4.6–5.1 GHz
and 0.6–1.0 GHz, respectively, and their spectra wereobtained successfully as shown in Figure 2 and Figure 3.
The method enables us to configure the readout systemfor both types of arrays.

Figure 1: Configuring probe tone in the resonator band.

Figure 2: Obtained spectra of antenna-coupled MKID array. Left)
Whole resonator band. The number of PTs is 105 to cover 105
selected resonances. The ranges of two PTs overlap at 23 PTs.
Right) Spectra of the pixel with the lowest resonance frequency.

Figure 3: Obtained spectra of LEK ID ar ray. Left) W holeresonator band. The number of PTs is 119 to cover 126 selectedresonances. The ranges of two PTs overlap at 24 PTs. Right)
Spectra of the pixel with the lowest resonance frequency.

References[1] Nagai, M., et al.:2020, JLTP, 199, 250–257.
[2] Kiuchi, H., et al.: 2015, IEEE TTST, 5, 456.
[3] Nagai, M., et al. : 2022, JLTP, 209, 677.
[4] Catalano, A., et al. : 2020, A&A, 641, A179.

I Scientific Highlights

015

Correlation Polarimeter for Millimeter-Wave Wavefront Sensing
NAGAI, Makoto1, IMADA, Hiroaki1, NITTA, Tom2/3, MURAYAMA, Yosuke1/2,
NOJI Ryohei2, NARUSE Masato4
1: NAOJ, 2: University of Tsukuba, 3: Tomonaga Center, 4: Saitama University

The mirror surface measurement is of great
importance for next-generation radio telescopes witha large single dish for millimeter- and submillimeterwave astronomy. The main cause of mirror deformationis the wind load to the primary mirror whose timescale is typically 10−1 s to 1 s [1]. Wavefront sensing inmillimeter-wave is necessary to realize adaptive optics
which can compensate for mirror deformation with shorttime scales. One proposed solution is aperture-planeinterferometry, which places a transmitter array on the
primary mirror [1]. Another proposed way of wavefront
sensing is the radio point diffraction interferometer(RPDI) [2]. To measure the field distribution of a beam,
we propose a new type of correlation polarimeter arraybased on phase-shifting interferometry [3]. We aredeveloping a correlation polarimeter easy to fabricate alarge-format array. The polarimeter is implemented as asuperconducting film on a silicon wafer, which employsa dual-polarization twin-slot antenna, a delay circuitcomposed of coplanar waveguide (CPW), and microwave
kinetic inductance detectors (MKIDs), as shown in
Figure 1. We developed a pixel design for 100 GHz, madeelectromagnetic simulations of the components (Figure 2,
and are preparing for trial production.

Figure 1: Schematic of a correlation polarimeter pixel. The input
ports of the delay circuit are named as Port 1 and Port 2. The
output ports of the delay circuit are named as Port 3, Port 4, Port 5,
and Port 6.

References[1] Tamura, Y., et al.: 2020, SPIE Conf., 11445, 114451N.
[2] Okumura, T., et al.: 2016, SPIE Conf., 9906, 990641.
[3] Nagai, M., et al.: 2022, URSI Radio Science Letters, 4,10.46620/22-0044.

Figure 2: Simulation result of phase shift induced by the delay
circuit. (Top) From Port 1. (Bottom) From Port 2.

016

I Scientific Highlights

uGMRT Observation of CIZA J1358.9-4750 :Discovery of a New Diffuse Radio Source
KURAHARA, Kohei1, AKAHORI, Takuya1/2, KALE, Ruta3, AKAMATSU, Hiroki4/5,
FUJITA, Yutaka6, GU, Liyi5, INTEMA, Huib7, NAKAZAWA, Kazuhiro8, OKABE, Nobuhiro9,
OMIYA, Yuki8, PAREKH, Viral10/11, SHIMWELL, Timothy7/12, TAKIZAWA, Motokazu13, VAN WEEREN, Reinout7
1: NAOJ, 2: SKAO, 3: NCRA, 4: QUP/KEK, 5: SRON, 6: Tokyo Metropolitan University, 7: Leiden University, 8: Nagoya University, 9:Hiroshima University, 10: Rhodes University, 11: SARAO, 12: ASTRON, 13: Yamagata University

Galaxy clusters grow through merger events andaccretion from the large scale structure of the universe.
Radio relics and halos, which would be made by shockwaves and turbulence of merging event, have been
discovered previously. Recently, a radio bridge, whichis the expected structure within a galaxy cluster pair andnot been detected in GHz band previously, have been
detected in early-stage merging galaxy clusters called
Abell 399/401. Although, there are theoretical challenges
that cannot be explained by simple Fermi acceleration
alone in order to form these radio structures.
CIZA J1358.9-4750 (CIZA1359) is thought tobe one of the early-stage merging galaxy clusterscite[1]. This source is located at (RA, Dec) = (13h58m40s,−47 d 46 m 00 s ) (J2000), and there is no diffuse radio
structure, such as a radio bridge, in and around the clusterfrom previous radio observations [2]. Therefore, in thisstudy, observations were made with the upgraded Giant
Metrewave Radio Telescope (uGMRT) to probe thediffuse radio emissions associated with CIZA1359.
We used the Source Peeling and Atmospheric
Modeling (SPAM) [3] and applied direction-dependentcalibration (DDC) [4]. Figure 1 shows the distribution of
the radio intensity with the uGMRT. The orange labelsfrom M to W were added for the new sources detected inthis study.
The largest radio structure around CIZA1359 in theuGMRT data is a source U. Since the radio source U
contains several radio compact sources, these compact
sources were subtracted and the flux density wasmeasured. As a result, the integrated flux density of theradio source U is 24.04 ± 2.48 mJy, which is significantly
larger than zero with the error. The radio source U is in
the between two sub-structures of ICM shown and isconsistent with the location of the northern shock wave
[5]. The structure is well aligned with the shock front,
and four galaxies are found within the source U. The
radio energy is 2.40 × 1024 W Hz−1, which is consistent
with the value expected from the X-ray luminosity of
CIZA1359. Also, the estimated magnetic field strength is
2.1 μG, which is also consistent with previous studies [6].
In summary, we suggest that the radio source U isa structure made by re-accelerating seed electrons withshock waves from galaxy cluster merging event. Our
result is considered to be the first detection of radio

emission originating from shock waves in early stage
merging galaxy cluster.

Figure 1: Broadband uGMRT radio intensity distribution of
CIZA1359. The background image shows the total intensity
distribution with a center frequency of 400 MHz and a bandwidthof 200 MHz. The resolution is 14.″8 × 5.″2 and is indicated by
the ellipse at the lower left of the figure. The white line shows
the intensity distribution of 0.4 mJy beam−1 when smoothed at
25 arcsec resolution. The green line shows the X-ray surface
brightness distribution of Suzaku [1]. The red line indicates thehigh-temperature region above 6 keV estimated by XMM-Newton[5].

References[1] Kato, Y., et al.: 2015, PASJ, 67, 71.
[2] Akahori, T., et al.: 2018, PASJ, 70, 53.
[3] Intema, H. T.: 2014, Astronomical Society of India Conference
Series, 13, 469.
[4] Intema, H. T., et al.: 2017, A&A, 598, A78.
[5] Omiya, Y., et al.: 2023, PASJ, 75, 37.
[6] Feretti, L., et al.: 2012, A&ARv, 20, 54.

I Scientific Highlights

017

Extreme Nature of Four Blue-excess Dust-obscured Galaxies
Revealed by Optical Spectroscopy
NOBORIGUCHI, Akatoki1, NAGAO, Tohru2, TOBA, Yoshiki3, ICHIKAWA, Kohei4,
KAJISAWA, Masaru2, KATO, Nanako2, KAWAGUCHI, Toshihiro5, MATSUHARA, Hideo6,
MATSUOKA, Yoshiki2, ONISHI, Kyoko7, ONOUE, Masafusa8, TAMADA, Nozomu2,
TERAO, Koki3, TERASHIMA, Yuichi2, UEDA, Yoshihiro9, YAMASHITA, Takuji3
1: Shinshu University, 2: Ehime University, 3: NAOJ, 4: Tohoku University, 5: Onomichi City University, 6: JAXA, 7: Chalmers University ofTechnology, 8: KIAA, 9: Kyoto University

In Noboriguchi et al. (2022) [1], we reported optical
spectroscopic observations of four blue-excess dustobscured galaxies (BluDOGs) identified by the Subaru
Hyper Suprime-Cam. BluDOGs are a subclass of dustobscured galaxies (DOGs; defined with the extremely red
color (i - [22])AB ≥ 7.0; [2]), showing a significant flux
excess in the optical g and r bands over the power-law fits
to the fluxes at the longer wavelengths ([3]). Noboriguchi
et al. (2019) [3] suggested that BluDOGs with such blue
excess may be in the blowing-out phase involved in
the gas-rich major-merger scenario ([4]). However, thedetailed properties of BluDOGs are not well understoodbecause of the lack of spectroscopic information.
We executed the optical spectroscopic observations
for four BluDOGs by using Subaru/FOCAS and VLT/FORS2. The obtained spectra show broad emission
lines with extremely large equivalent widths, and a blue
wing in the C IV line profile (Figure 1). The averaged
rest-frame equivalent widths of the C IV lines are 160± 33 Å, ~7 times higher than the average of a typicaltype 1 quasar (23.8 ± 0.1 Å: [5]). Such strong C IV lines
significantly affect the broadband magnitudes, which
are partly the origin of the blue excess seen in the
spectral energy distribution of BluDOGs. The estimatedsupermassive black hole (SMBH) masses (MBH) are 1.1
× 10 8 < M BH /M⊙ < 5.5 × 10 8 (Figure 2). The inferred
Eddington ratios (λEdd) of the BluDOGs are higher than
1 (1.1 < λEdd < 3.8), suggesting that the BluDOGs are in a
rapidly evolving phase of supermassive black holes.

Figure 1: Reduced spectra of the BluDOGs. The spectra are forJ0907, J1202, J1207, and J1443 from the top to bottom. Detectedlines are marked by arrows and labels.

Figure 2: Diagram of SMBH mass vs. bolometric luminosity. The
filled-red stars and blue contour denote the BluDOGs and SDSS
quasars ([6]), respectively. The orange-dashed lines represent a
constant Eddington ratio of λEdd = 0.01, 0.1, 1.0, and 10.0.

References[1] Noboriguchi, A., et al.: 2022, ApJ, 941, 195.
[2] Toba, Y., et al.: 2015, PASJ, 67, 86.
[3] Noboriguchi, A., et al.: 2019, ApJ, 876, 132.
[4] Hopkins, P. F., et al.: 2008, ApJS, 175, 356.
[5] Vanden Berk, D. E., et al.: 2001, AJ, 122, 549.
[6] Shen, Y., et al.: 2011, ApJS, 194, 45.

018

I Scientific Highlights

The Coherent Differential Imaging on Speckle Area Nulling (CDI-SAN)
Method for High-contrast Imaging under Speckle Variation
NISHIKAWA, Jun(NAOJ / Graduate University for Advanced Studies / Astrobiology Center)Searching for biosignatures in the spectrum ofreflected light from exoplanets is one of the goals of
future large telescope projects. The contrast of the
exoplanet to the host star in reflected light is 10−8 ~ 10−10.
In ground-based telescopes and space telescopes withinsufficient temperature control, speckle noise brighter
than planets remains and changes, being limited planet
detection by the seckle noise even after post-processing.
The coherent differential imaging on speckle area nulling(CDI-SAN) method is an observation algorithm andpost-processing method that detect a faint exoplanet lying
beneath residual speckles of a host star [1].
The SAN method is a kind of real-time dark-hole
control method that does not use a model. The speckle
electric field (Es) of all pixels in the region of interestis calculated using the intensities of the five types offocused images expressed by equation (1) obtainedby adding five types of modulated wavefronts withthe deformable mirror, respectively, and is reduced bymodifyig the wavefront [2].
2I0 = |Es | + Ip



2
+


 I1 = |Es + ∆E1 | + Ip
2

I1− = |Es − ∆E1 | + Ip2
I2+ = |Es + ∆E2 | + Ip



 −
2
I2 = |Es − ∆E2 | + Ip

that showed an improvement in contrast from dataobtained by measuring two sets of five intensities within
the timescale of speckle change, and repeating thismeasurement one million times. Here hidden pseudoplanets appeared. Assuming that the time scale of speckle
change is 36 ms, the exposure time for one image is 3.6
ms, which is the accumulated data for 10 hours. Whenthe initial intensity is 10 −4, planets at 1/1000 of the
speckle level can be detected. The method has potential
implementation in current and future large telescopes on
the ground and in space.

(1)

However, the higher the contrast, the longer the
exposure time, and if the speckle fluctuates during thattime, the reduction of Es stops and the real-time contrast
setteles there.
Therefore, in the CDI-SAN method, data is acquired
for a long period of time while repeating five typesof modulation wavefront addition and focus image
acquisition by the SAN method at a higher speed than
the speckle variation. As shown in Eq. (2), we separate
the planetary light (I p ) from the stellar light with acontrast close to the photon noise limit under appropriate
conditions by using the integral of the focal image
intensity and the integral of the squared Idifference.
1
( +
)
2
⟨ I1 − I1− ⟩()
Ip1 = ⟨I0 ⟩ −8 ⟨I1+ ⟩ + ⟨I1− ⟩ − 2⟨I0 ⟩()2⟨ I2+ − I2− ⟩
),
(
−
(2)
8 ⟨I2+ ⟩ + ⟨I2− ⟩ − 2⟨I0 ⟩Figure 1: Contrast improvement effect by numerical simulationof CDI-SAN. (Top) Assumed speckle level. From the left zone,
the average intensities were 10 −3 , 10 −4 , 10 −5 , 10 −6 , and 10 −7.
(Bottom) Image after processing 2 million sets of data. Hidden
pseudoplanets are 1x, 1/10th, 1/100th, 1/1000th of the speckle
level at each zone, from top to bottom.

References[1] Nishikawa, J.: 2022, ApJ, 930, 163.
[2] Oya, M., Nishikawa, J., et al.: 2015, OptRev, 22, 736.

Figure 1 shows the results of a numerical simulation

I Scientific Highlights

019

Passive Spiral Galaxies
Deeply Captured by Subaru Hyper Suprime-Cam
SHIMAKAWA, Rhythm1, TANAKA, Masayuki1, BOTTRELL, Connor2,
WU, Po-Feng3, CHANG, Yu-Yen3, TOBA, Yoshiki1, ALI, Sadman1
1: NAOJ, 2: University of Tokyo, 3: ASIAA

The fundamental relations between galaxy
morphology and physical properties have been
extensively studied over the past decades, and modern
astronomy is still at the stage of trying to fit the remaining
missing pieces. In this context, this study focused on an“anemic” spiral galaxy with deep learning, which is aunique population but is of great scientific importance.
We hereafter overview the importance of anemic spiralgalaxies for a comprehensive understanding of galaxy
evolution and the results obtained in this study [1].
Anemic spiral galaxies are a generic term for spiralgalaxies with little or no star formation. In general, spiralgalaxies are rich in gas, the fuel for star formation, whichplays a role in forming their spiral arms and hence arerepresentative of “star-forming galaxies”. However,when this fuel tank is lost for some reason, star formationceases and there is a period of time when the spiralarms are present even though no star formation is taking
place. Spiral galaxies in such a special state are calledanemic spiral galaxies. Anemic spirals are essential
for understanding how spiral galaxies lose their spiralstructure as they reach the end of their activity. Still, they
are extremely difficult to survey statistically because
only a few percent of all bright galaxies exist. This study
focused on this problem and conducted a statistical surveyof anemic spiral galaxies using high-quality big data fromthe Subaru telescope and deep learning classification.
This study used high-quality images of 55k brightnearby galaxies with redshifts of 0.01–0.3 taken by Subaru
Hyper Suprime-Cam, which have been spectroscopicallyconfirmed and for which detailed physical information
is available from multi-wavelength data. We classified
the spiral galaxies using deep learning. Then we used
the physical information from the multi-wavelength data
to obtain a sample of more than 1k non-star-forming
anemic spiral galaxies for the first time. Figure 1 showsthe evolution of the color and morphology of selectedspiral galaxies concerning star formation activity, andFigure 2 compares normal and anemic spiral galaxies,
showing that anemic spiral galaxies are composed
entirely of old stars (orange), from the center to the spiralarms, and spiral arms look smooth. In fact, through thisstudy, we found that the bulge structure and propertiesof these anemic spirals are much closer to those of earlytype galaxies than spiral galaxies, despite the presenceof spiral arms. Furthermore, once a sufficient number

020

I Scientific Highlights

of anemic spiral samples were obtained, we tested if
there were any peculiarities in the distribution of anemic
spirals around galaxy clusters with few spiral galaxies
in the center. We found that anemic spiral galaxies are
more than 10 times (40 percent) more common in theouter regions of clusters than usual. This result strongly
supports the ram pressure stripping scenario of the loss ofspiral structure.

Figure 1: Color and morphology of spiral galaxies at different
SFRs–stellar masses [1].

Figure 2: Examples of normal spiral galaxies (upper panel) andanemic spiral galaxies (lower panel).

Reference[1] Shimakawa, R., et al.: 2022, PASJ, 74, 612

Discovery of the Monster Supercluster in the Universe at z = 0.6
SHIMAKAWA, Rhythm1, TANAKA, Masayuki1, SHIRASAKI, Masato1/2, OKABE, Nobuhiro3
1: NAOJ, 2: The Institute of Statistical Mathematics, 3: Hiroshima University

The universe is a complex, large-scale structure ofgalaxy clusters, filaments, and voids. Clusters of galaxies
are known as the largest self-gravitating systems in theuniverse. However, there is a huge structure called agalaxy supercluster, which is composed of more clustersof galaxies. While superclusters extend over about 100
Mpc, their definition itself is still unclear, and manyquestions remain as to their true nature, what is going on
inside them, and whether they are different from ordinary
clusters of galaxies. Milky Way and local galaxy groups
are part of a supercluster called the Virgo supercluster,and together with other nearby clusters and superclusters,
they form the giant Laniakea supercluster. In other words,
many issues related to these superclusters are inseparablefrom understanding the formation of the nearby universethat surrounds us.
This project aims to discover a large number of distantsuperclusters and voids in the universe and to study theenvironmental dependence of galaxies on large scales byanalyzing multicolor data covering about 1000 square
degrees obtained by the Subaru Hyper Suprime-Cam. In
this study, as part of this project, we performed (1) dark
matter mapping by weak gravitational lensing analysis
and (2) derivation and comparison of stellar mass density
maps obtained by SED fitting for the most promising
candidate supercluster at z = 0.55 from the candidates
selected in previous work [1].
As a result, we succeeded in detecting a large-scale
weak gravitational lensing signal centered on three dense
dark matter regions at a scale of 70 Mpc around the target(we named this object the King Ghidorah supercluster).
In addition to the density excess of dark matter, the King
Ghidorah supercluster is composed of at least 19 clustersof galaxies (Figure 1). This is the largest supercluster
ever reported in the same period. This is the first time thatsuch a wide range of density excesses has been observedin both the dark matter and stellar mass distributions at
z > 0.5 [2].
Furthermore, we performed a direct comparison of
the overdensity analysis on mock data from cosmologicalsimulations as well as observational data. The results
suggest that the King Ghidorah supercluster has atotal dark matter mass of about 10 16 times the massof the Sun. On top of that, two more giant structuresequivalent to superclusters were identified just outsideof this supercluster, suggesting that this supercluster andits surrounding region may grow into a supermassive
structure like the Laniakea supercluster, the largest in the
nearby universe, in the future.

6
5

1

2

7

3

19

4
18

8

12
17

13

10

15

9

11

14
16
1

2

3

4

5

6

7

8

9

10

11

12

13

14

15

16

17

18

19

Figure 1: Three-color composite image of a supercluster region.
The white contours in the upper image show the galaxy density
distribution, and the light red-filled area shows the dark matter
density distribution. The numbers appended on the image indicate
the location of the red clusters associated with the supercluster[3], and their respective extended regions are shown in the lower
panels. The full moon in the upper left panel is the apparent sizeof the full moon, corresponding to the supercluster region (seealso the web release in the Subaru Telescope website).

References[1] Shimakawa, R., et al.: 2021, MNRAS, 503, 3896.
[2] Shimakawa, R., et al.: 2023, MNRAS, 519, L45.
[3] Oguri, M., et al.: 2018, PASJ, 70, S20.

I Scientific Highlights

021

An Empirical Method for Mitigating an Excess Up-scattering Mass Biason the Weak Lensing Mass Estimates for Shear-selected Cluster Samples
HAMANA, Takashi(NAOJ)An excess up-scattering mass bias on a weaklensing cluster mass estimate is a statistical bias that an
observed weak lensing mass of a cluster of galaxies is,in a statistical sense, larger than its true mass becauseof a higher chance of up-scattering than that of downscattering due to random noises in a weak lensing cluster
shear profile. This non-symmetric scattering probability
is caused by a monotonically decreasing cluster massfunction with increasing mass. We examine this bias
in weak lensing shear-selected clusters, and present
an empirical method for mitigating it [1]. In so doing,
we perform the standard weak lensing mass estimateof realistic mock clusters generated using the supercomputer system, XC50, at Center for Computational
Astrophysics, NAOJ, and find that the weak lensing massestimate based on the standard chi-square analysis gives

a statistically correct confidence intervals, but resulting
best-fitting masses are biased high on average. Our
correction method uses the framework of the standard
Bayesian statistics with the prior of the probability
distribution of the cluster mass and concentration
parameter from recent empirical models. We test ourcorrection method using mock weak lensing clusters, andfind that the method works well with resulting corrected.
We applied the correction method to weak lensing shearselected cluster samples from Hyper Suprime-Cam
survey S16A and S19A data, and present bias-corrected
weak lensing cluster masses.

Reference[1] Hamana, T.: 2023, PASJ, 75, 14.

Figure 1: A weak lensing shear-selected cluster of galaxies from HSC survey S16A data. Shown is a 10 arcmin-side riz composite image,the yellow contour shows the weak lensing Signal-to-Noise ratio (the contour lines start from SN = 2 with the interval of 1), and the plus
marks show the position of known clusters.

022

I Scientific Highlights

A Tale of a Tail:
A Tidally-Disrupting Ultra-Diffuse Galaxy in the M81 GroupŽEMAITIS, Rokas1, FERGUSON, Annette M. N.1, OKAMOTO, Sakurako2/3,
CUILLANDRE, Jean-Charles4, ARIMOTO, Nobuo2/3
1: University of Edinburgh, 2: Graduate University for Advanced Studies, 3: NAOJ, 4: Université Paris-Saclay

As the only UDG that is close enough to allow studies
at extremely low surface brightness, and the first to beunambiguously linked to tidal stripping, our results for
F8D1 are of particular importance. It leaves open thepossibility that many other UDGs could be the result ofsimilar processes, with the most telling signatures of thislurking below current detection limits.
 


 







   





 

 

 





 

Ultra-diffuse galaxies (UDGs) are distinguished bytheir low central surface brightnesses and large sizes. A
commonly-used definition is that they have effective radii
Reff ≥ 1.5 kpc and central surface brightnesses fainterthan μg(0) ≥ 24 mag arcsec−2 [1]. Although systems withthese properties have been known to exist for decades,
there has been a recent resurgence in interest in them dueto the sheer abundance of such objects being discoveredin modern deep imaging surveys [2]. They appear
particularly common in dense environments [1], but arealso found in low density groups and in the field [3].
Several explanations for the origin of UDGs haveappeared in the literature, such as, they may be rapidly
rotating normal dwarf galaxies, resulting in a very
extended profile for their stellar mass. Or, their large sizes
may result from tidal stripping and heating experienced
through interactions with massive neighbouring galaxies.
Other possible scenarios are that they are puffed-up
dwarf galaxies that have experienced gas loss due tostar formation-driven outflows or that they are ‘failed’
galaxies that did not manage to build-up their expected
stellar mass. Ram-pressure stripping may play a furtherrole in transforming gas-rich blue UDGs into red ones.
While it is likely that the present-day UDG population
results from a variety of these formation channels, thequestion of which is the dominant channel remains open.
We investigate the deep map of resolved red giant
branch stars constructed using data from our Subaru
Hyper Suprime-Cam survey of the M81 Group [4] anddiscover a giant tidal tail of stars associated with F8D1,
the closest known example of an UDG (see Figure 1).
F8D1 sits in a region of the sky heavily contaminatedby Galactic cirrus and has been poorly studied since its
discovery two decades ago. It has an average surface
brightness of μ g ~ 32 mag arcsec −2 and can be traced
for over a degree on the sky (60 kpc at the distance of
F8D1) with our current imagery. We revisit the main
body properties of F8D1 using deep multiband imagery
acquired with MegaCam on CFHT and measure effective
radii of 1.7–1.9 kpc, central surface brightnesses of 24.7–
25.7 mag and a stellar mass of ~7 × 107 M⊙. Assuming
a symmetric feature on the other side of the galaxy, we
calculate that 30–36 % of F8D1's present-day luminosity
is contained in the tail. We argue that the most likely
origin of F8D1's disruption is a recent close passage toM81, which would have stripped its gas and quenched its
star formation.





 



 














 









Figure 1: Top: Our M81 Group Survey footprint (seven HSC
pointings) overlaid on an SDSS image. Each HSC pointing has adiameter of 1.5 deg and the known galaxies within this area aremarked. The red circle indicates the pointing containing F8D1,
which is the focus of this paper. Bottom: The RGB star countdensity across our HSC pointing. A giant tidal stream can be seen
emanating from F8D1, which is located at the south-western edge.
A DSS image of NGC 2976 is superposed for scale and the hollow
centres of the galaxies indicate regions where the pipeline failed
to return photometry.
References[1] van Dokkum P. G., et al.: 2015, ApJ, 798, L45.
[2] Koda J., et al.: 2015, ApJ, 807, L2.
[3] Merritt, A., et al.: 2016, ApJ, 833, 168.
[4] Okamoto, S., et al.: 2015, ApJ, 809, L1.

I Scientific Highlights

023

Discovery of an Earth-sized Planet around an M5 Dwarf Star at 22 pc
HIRANO, Teruyuki1/2, LIVINGSTON, John1/2, KASAGI, Yui1, ISHIKAWA, Hiroyuki1/2, MIYAKAWA, Kohei1, MATSUMOTO, Yuji1,
KOKUBO, Eiichiro1, IKOMA, Masahiro1, HARAKAWA, Hiroki1, HORI, Yasunori1/2, KOTANI, Takayuki1/2,
KRISHNAMURTHY, Vigneshwaran1/2, KUDO, Tomoyuki1, KUROKAWA, Takashi2, KUZUHARA, Masayuki1/2, NISHIKAWA, Jun1/2,
OMIYA, Masashi1/2, TAKAHASHI, Aoi1/2, TAKARADA, Takuya1/2, UEDA, Akitoshi1, VIEVARD, Sebastien1, DAI, Fei3,
SERABYN, Eugene3, GRZIWA, Sascha4, LAM, Kristine5, SMITH, Alexis5, NARITA, Norio6, KIMURA, Tadahiro6,
FUKUI, Akihiko6, IKUTA, Kai6, KAWAUCHI, Kiyoe6, MORI, Mayuko6, TAMURA, Motohide6, SERRANO, Luisa7,
GANDOLFI, Davide 7, WINN, Joshua 8, WISNIEWSKI, John 9, TENG, Huan-Yu 10, SATO, Bun'ei 10, COCHRAN, William 11,
GUENTHER, Eike12, KNUDSTRUP, Emil13, KORTH, Judith14, PERSSON, Carina14, LUQUE, Rafael15,
ORELL-MIQUEL, Jaume16, PALLE, Enric16, REDFIELD, Seth17, VAN EYLEN, Vincent18
1: NAOJ, 2: Astrobiology Center, 3: California Institute of Technology, 4: University of Cologne, 5: DLR, 6: University of Tokyo, 7: University of Turin, 8: Princeton
University, 9: George Mason University, 10: Tokyo Institute of Technology, 11: University of Texas, 12: Karl Schwarzschild Observatory, 13: Aarhus University, 14:
Chalmers University of Technology, 15: University of Chicago, 16: IAC, 17: Wesleyan University, 18: University College London

Recently, a number of exoplanets have been
discovered around M dwarfs, which are much lessmassive and cooler than the Sun. Transiting planets
around very low-mass stars are particularly importantsince their small radii make the transits deeper, whichallows us to better characterize small-sized exoplanets.
However, the number of “nearby” M dwarfs hostingtransiting planets, which are amenable to futureatmospheric characterization is very limited at thispoint; for instance, there are only ≈ 30 M dwarfs within
30 pc from the Earth, which are known to host transiting
planets (most of which are relatively massive “early-M”
dwarfs)1.
In order to find more low-mass planets that aresuitable for future atmospheric characterization by e.g.,
30m-class telescopes, we have led an effort to detect andvalidate transiting planets around M dwarfs. We analyzed
public data delivered by the Kepler spacecraft's secondary
mission, known as “K2” [1], and identified a transitingplanet candidate around EPIC211414619 (Figure 1),
an M5 dwarf star at 22 pc from the Earth. Since planetcandidates reported by space-based transit surveys
often include false positives, mostly originating from
eclipsing binaries, we conducted follow-up observations
for EPIC211414619 using ground-based telescopes. As aresult of performing high-contrast imaging with IRCS andhigh-resolution spectroscopy with IRD, both mounted on
the Subaru telescope, we ruled out false positive scenarios
for EPIC211414619, and confirmed that the candidate
is a bona fide planet with an orbital period of 4.02 days,
which is now named “K2-415b”. The host star, K2-415,
was also observed by the Transiting Exoplanet Survey
Satellite (TESS) in 2021, and by analyzing both light
curves provided by K2 and TESS missions, we measured
the radius of K2-415b as 1.015±0.051 R⊕. Based on theradial-velocity measurements by Subaru/IRD, we also
obtained an upper limit of 7.5 M⊕ (at 95 % confidence)for the mass of K2-415b [2].
At 22 pc, K2-415 is one of the closest M dwarfs
1 https://exoplanetarchive.ipac.caltech.edu/index.html

024

I Scientific Highlights

known to host an Earth-sized transiting planet; it iscurrently the closest planet-hosting star from the Earthidentified by the Kepler spacecraft. K2-415 is also oneof the lowest-mass (coolest) stars with known transiting
planets. The only M dwarfs cooler than K2-415, hosting
Earth-like transiting planets, are TRAPPIST-1 (12 pc), LP
791-18 (26 pc), LHS 1140 (15 pc), and Kepler-42 (40 pc).
Moreover, as of today, there are only ten transiting-planet(of any size) hosting stars cooler than K2-415, sevenof which are more distant stars than K2-415. Given its
proximity (thus brightness) and small size of the host star,K2-415b is a very unique target for future atmosphericcharacterization.

Figure 1: Light curve of EPIC211414619 (K2-415) around theplanetary transit obtained by the K2 mission. It is folded with K2415b's period (4.02 days). The red solid line indicates the best-fit
theoretical model of the transit.

References[1] Howell, S. B., et al.: 2014, PASP, 126, 398.
[2] Hirano, T., et al.: 2023, AJ, 165, 131.

A Wide and Deep Exploration of Radio Galaxies
with Subaru HSC (WERGS). VII.
Redshift Evolution of Radio Galaxy Environments at z = 0.3−1.4
UCHIYAMA, Hisakazu1/2, YAMASHITA, Takuji1/3, NAGAO, Tohru3, ICHIKAWA, Kohei4/5, TOBA, Yoshiki1/6/7/3,
ISHIKAWA, Shogo6/1, KUBO, Mariko4, KAJISAWA, Masaru3, KAWAGUCHI, Toshihiro8,
KAWAKATU, Nozomu9, LEE, Chien-Hsiu10, NOBORIGUCHI, Akatoki11
1: NAOJ, 2: Kanagawa University, 3: Ehime University, 4: Tohoku University, 5: MPE, 6: Kyoto University, 7: ASIAA, 8: Onomichi City
University, 9: Kure College, 10: NSF’s NOIRLab, 11: Shinshu University

In this study [1], we have examined the redshift
evolution of density environments around 2,163 radiogalaxies with the stellar masses of ~109–1012 M⊙ between
redshifts of z = 0.3–1.4, based on the Hyper SuprimeCam Subaru Strategic Program (HSC-SSP) and Faint
Images of the Radio Sky at Twenty-cm (FIRST). We
use the k-nearest neighbor method to measure the local
galaxy number density around our radio galaxy sample.
We find that the overdensities of the radio galaxies are
weakly but significantly anti-correlated with redshift.
This is consistent with the known result that the relative
abundance of less-massive radio galaxies increases with
redshift [2], because less-massive radio galaxies residein relatively low density regions. Massive radio galaxies
with stellar mass of M * > 10 11 M ⊙ are found in highdensity environments compared with the control sample
galaxies with radio-non-detection and matched-stellarmass. Less-massive radio galaxies with M* < 1011 M⊙
reside in average density environments. The fractionof the radio galaxies associated with the neighbors
within a typical major merger scale, < 70 kpc, is higher
than (comparable to) that of the control galaxies at M*> 1011 M⊙ (M* < 1011 M⊙). We also find that the local
densities around the radio galaxies are anti-correlatedwith the radio luminosities and black hole mass accretion
rates at fixed stellar mass. These findings suggest thatmassive radio galaxies have matured through galaxy
mergers in the past, and have supermassive black holes
whose mass accretion almost ceased at z > 1.4, while lessmassive radio galaxies undergo active accretion just at
this epoch, as they have avoided such merger events.

References[1] Uchiyama, H., et al.: 2022, ApJ, 934, 68.
[2] Donoso, E., et al.: 2009, MNRAS, 392, 617.
Figure 1: (upper panel) The overdensities around the radiogalaxies (black points) as a function of redshifts. The red and blue
open circles indicate the median of the overdensities of the radio
and control galaxies, respectively. The black dashed line shows
the average density. (lower panel) The projected distances fromthe radio galaxies and control galaxies to the nearest neighbors(dk = 1) and their pair fractions ( fpair) as a function of stellar mass.

I Scientific Highlights

025

A Wide and Deep Exploration of Radio Galaxies
with Subaru HSC (WERGS). IX.
The Most Overdense Region at z ~ 5 Inhabited by a Massive Radio Galaxy
UCHIYAMA, Hisakazu1/2, YAMASHITA, Takuji1/3, NAGAO, Tohru3, ONO, Yoshiaki4,
TOSHIKAWA, Jun5, ICHIKAWA, Kohei6/7, KAWAKATU, Nozomu8, KAJISAWA, Masaru3,
TOBA, Yoshiki1/9/10/3, MATSUOKA, Yoshiki3, KUBO, Mariko6, IMANISHI, Masatoshi1/11, ITO, Kei12,
KAWAGUCHI, Toshihiro13, LEE, Chien-Hsiu14, SAITO, Tomoki15
1: NAOJ, 2: Kanagawa University, 3: Ehime University, 4: ICRR, 5: Bath University, 6: Tohoku University, 7: MPE, 8: Kure College, 9: Kyoto
University, 10: ASIAA, 11: SOKENDAI, 12: Tokyo University, 13: Onomichi City University, 14: NSF’s NOIRLab, 15: Hyogo University

In this study [1], we have revealed that a high-z radiogalaxy (HzRG) at z = 4.72, HSC J083913.17+011308.1(HSC J0839+0113) [2], associates with the most
overdense region, by using the data of the Hyper
Suprime-Cam Subaru Strategic Program (HSC-SSP) and
Faint Images of the Radio Sky at Twenty-cm (FIRST).
We use an r-dropout Lyman break galaxy (LBG)
sample from the HSC-SSP data to measure theoverdensities around the HzRG. As a result, we find that
HSC J0839+0113 resides in the outskirt of an overdense
region identified by the r-dropout galaxies at a 4.7σ
significance level (upper panel of Figure 1). The projecteddistance between HSC J0839+0113 and the peak positionof the overdense region is 0.4 physical Mpc which isshorter than the typical protocluster radius in this epoch.
According to the extended Press Schechter and the lightcone models, the HSC J0839+0113-hosted overdense
region is expected to evolve into a halo > 1014 M⊙ at z = 0
with a high probability of > 80 %. These findings suggestthat HSC J0839+0113 is associated with a protocluster.
The HSC J0839+0113 rich-system is the most overdense
region of LBGs among the known protoclusters with
LBGs in the same cosmic epoch. We also find that there
are no r-dropout galaxies with blue color of i-z <~ 0.3 inthe HSC J0839+0113 overdense region (lower panel of
Figure 1). This result implies that the HSC J0839+0113
overdense region predominantly includes galaxies withan old stellar population and/or large amounts of dust.

References[1] Uchiyama, H. et al.: 2022, ApJ, 934, 68.
[2] Yamashita, T., et al.: 2020, AJ, 160, 60.

026

I Scientific Highlights

Figure 1: (upper panel) The overdensity significance map around
HSC J0839+0113 (black star). The peak position is indicatedby the black open circle. The black dots denote the r-dropout
galaxies. The gray shades indicate the masked regions. (lower
panel) The UV absolute magnitudes and i-z colors of ther-dropout galaxies in the HSC J0839+0113 field (blue) and generalfields (gray).

Spectroscopic Characterization of Young Stars
Showing Irregular Dimmings to Unveil Their Mechanisms
KASAGI, Yui1, KOTANI, Takayuki1/2/3, KAWAHARA, Hajime4/5, TAJIRI, Tomoyuki5,
MUTO, Takayuki6, AIZAWA, Masataka7, FUJII, S. Michiko5, HATTORI, Kohei8,
MASUDA, Kento9, MOMOSE, Munetake10, OHSAWA, Ryou3, TAKITA, Satoshi5
1: The Graduate University for Advanced Studies, 2: Astrobiology Center, 3: NAOJ, 4: JAXA, 5: The University of Tokyo, 6: Kogakuin
University, 7: Shanghai Jiao Tong University, 8: Institute of Statistical Mathematics, 9: Osaka University, 10: Ibaraki University

Among young stellar objects, there is a population
called “dippers” that exhibit episodic or quasi-periodic
dimming in their light curves. The photometric variability
is attributed to a shadow by circumstellar materials, but
the detailed mechanisms are not yet fully understood.
Observations of dippers can provide important clues forstudying planet formation processes by revealing theregion close to the star in protoplanetary disks.
In this study [1], we observed four newly discovered
dippers from the Transiting Exoplanet Survey Satellite(TESS) data [2]. We confirmed that all of the targets
exhibit the Hα emission line in the spectra observed using
the High-Dispersion Spectrograph (HDS) installed on the
Subaru telescope (Figure 1). This emission line indicatesongoing accretion of materials onto the surface of a starfrom a protoplanetary disk. We were able to estimate
the accretion in more detail from the line profiles [3]. In
addition, additional observations conducted with otherspectrographs, CAHA/CAFE and Okayama/HIDES,
revealed variability in the Hα line profiles for two targets.
The appearance of blue-shifted or red-shifted absorption
in the Hα emission lines indicates the presence of a disk
wind or the accretion flow around a star, supporting
the dimming mechanisms for each target. Based on the
results, we concluded that the dips in the light curves of
those dippers are attributed to a dusty disk wind or dust
in an accretion-driven disk warp (Figure 2).
This study was the first to characterize these four
dippers and identify the cause of their dimming,suggesting the diversity of planet-forming environments.
We also discovered that one of our targets is a binary
system, as indicated by the large radial velocity variations
observed. Interestingly, the orbital period of this binary
is almost the same as the period of the dips seen in the
TESS light curve. This suggests a strong relationshipbetween the dipper phenomenon and the binary motion.
Such dippers in close binary systems have rarely been
discovered so far, making this target an important sample
for further investigation.

Figure 1: Observed Hα emission lines for our four targets. The
vertical dashed line is at the rest wavelength (6562.8 Å).

(a)

(a)

(b)

(c)

Figure 2: Upper four panels show TESS FFI light curves for ourtargets. The lower three images represent the plausible scenarios
based on our observation.: (a) disk wind, (b) accretion warp,(c) binary and accretion warp. The labels in the light curves
correspond to each scenario.

References[1] Kasagi, Y., et al.: 2022, ApJS, 259, 40.
[2] Tajiri, T., et al.: 2020, ApJS, 251, 18.
[3] Kurosawa, R., et al.: 2006, MNRAS, 370, 580.

I Scientific Highlights

027

Morpho-kinematic Modeling of the Expanding Ejectaof the Extremely Slow Nova V1280 Scorpii
NAITO, Hiroyuki1/2, TAJITSU, Akito3, RIBEIRO, Valério A. R. M.4/5/6, ARAI, Akira3/7, MAEHARA, Hiroyuki3,
KOUZUMA, Shinjirou8, IIJIMA, Takashi9, OKAZAKI, Atsuo T.10, WATANABE, Makoto11,
TAKAGI, Seiko12, WATANABE, Fumitake1, SAKON, Itsuki13, SADAKANE, Kozo14
1: Nayoro Observatory, 2: Nagoya University, 3: NAOJ, 4: Campus Universitário de Santiago, 5: Radboud University, 6: University of CapeTown, 7: Kyoto Sangyo University, 8: Chukyo University, 9: Astronomical Observatory of Padova, 10: Hokkai-Gakuen University, 11:
Okayama University of Science, 12: Hokkaido University, 13: University of Tokyo, 14: Osaka Kyoiku University

evolution is extremely slow; the transition to the nebularphase occurred 50 months after the explosion. Synthetic
line profile spectra were compared to the observed [O III]λλ4959, 5007 and [N II] λ5755 line profiles in order to findthe best-fit morphology, inclination angle, and expansion
velocity of the ejected shell. We find that the observed
spectra were reproduced well for high inclination
angles of ~80 deg (Figure 1). A high inclination angle
is consistent with the observational results showing
multiple absorption lines originating from clumpy gases[3], which are produced in dense and slow equatorially
focused outflows (Figure 2). Increasing the sample sizeof novae whose morphology is studied will be helpful inelucidating the mechanism of the nova explosion.

Figure 1: Top: contour plot showing goodness of fit (reduced χ 2)
of model fits. Bottom: comparison between the observed ([O III]λλ4959, 5007) and model spectra. The figure is taken from Fig. 5of [2].

A classical nova is caused by a thermonuclear
runaway on the surface of a white dwarf following theaccretion of hydrogen-rich material from a companion
star in a close binary system. However, the nova
explosion model is not fully understood. Recently, γ-rays
were detected during nova explosions, and an idea ofcollisions between slow gas ejected on the orbital planeof binary systems and fast nova ejecta has been proposed(e.g., [1]). The morphology of the ejecta, which isoften not taken into account as a parameter, should be
an important key to elucidating the mechanism of the
explosion.
In this study [2], we analyzed high dispersion spectraof V1280 Sco taken with the Subaru Telescope's HDS
between 2009 and 2019, and discussed the morphologyof the nova remnant and the explosion model. V1280
Sco is a classical nova that exploded in 2007 and its

028

I Scientific Highlights

Figure 2: A schematic of V1280 Sco, illustrating fast wind ([O III]and [N II] regions) extended in the polar direction and slow
clumpy absorption components ejected in the equatorial direction.
The figure is taken from Fig. 8 of [2].

References[1] Chomiuk, L., et al.: 2014, Nature, 514, 339.
[2] Naito, H., et al.: 2022, ApJ, 932, 39.
[3] Naito, H., et al.: 2013, PASJ, 65, 37.

Statistical Properties of Satellites of Milky Way–like Galaxies
NASHIMOTO, Masashi1*, TANAKA, Masayuki2, CHIBA, Masashi3,
HAYASHI, Kohei4/3/5, KOMIYAMA, Yutaka6, OKAMOTO, Takashi7
1: University of Tokyo, 2: NAOJ, 3: Tohoku University, 4: National Institute of Technology, Sendai College, 5: Institute for Cosmic Ray
Research, 6: Hosei University, 7: Hokkaido University

Although the ΛCDM model has established itself
as a standard theory in modern cosmology, it is known
that there are some inconsistencies between theory andobservation in small-scale structures. One such problem
is the discrepancy between the observed number andspatial distribution of satellite galaxies around the Milky
Way (MW) and Andromeda galaxies and the simulation
results based on the ΛCDM model. It is essential toclarify whether these problems related to satellite
galaxies are limited to galaxies in the Local Group (LG)or whether they are universal problems in the universe inorder to achieve a fair test of cosmology.
This study [1] focuses on nine galaxies with masses
similar to the MW outside the LG (at a distance ofapproximately 20 Mpc). We observed these galaxies
using Subaru/Hyper Suprime-Cam (HSC) to search forsatellite galaxies. The identification of satellite galaxies
followed the method used in the precursor study [2] tothis study, and the candidates were narrowed down using
the physical quantities of satellite galaxies estimated bymodel fitting to candidate objects.
Figure 1 shows some images of satellite galaxies
detected in this study. A total of 93 faint satellite galaxy
candidates were detected using HSC's high-sensitivity
data. Figure 2a shows the luminosity function of thesatellite galaxies. Compared with observations of MW
and galaxies outside the LG, the average luminosity
function of the nine galaxies observed in this study is
consistent within a standard deviation, indicating thateach galaxies have a similar number of satellite galaxies.
On the other hand, we show that the projected radial
distribution from the host galaxy does not indicate acentrally concentrated distribution as in the MW. It isconsistent with the one expected from simulations forgalaxies with similar mass to the MW (Figure 2b). We
detected no indication of anisotropy in the directional
distribution of satellite galaxies. These comparisons
imply that the characteristics of satellite galaxies insideand outside the LG are different and that the MW maynever be typical galaxies in the universe.

Figure 1: Some images of detected satellite galaxies.

(a) luminosity function.

(b) radial distribution.

Figure 2: Comparison with the average of satellite galaxies
detected in nine galaxies. The red, blue, and green represent
obser vation for MW [3], galaxies outside the LG [4], andsimulation results for MW-like galaxies [5], respectively.

References[1] Nashimoto, M., et al.: 2022, ApJ, 936, 38.
[2] Tanaka, M., et al.: 2018, ApJ, 865, 125.
[3] McConnachie, A. W.: 2012, AJ, 144, 4.
[4] Wang, W., et al.: 2021, MNRAS, 500, 3776.
[5] Carlsten, S. G., et al.: 2020, ApJ, 902, 124.

* In NAOJ when paper was published.

I Scientific Highlights

029

First Identification of a CMB Lensing Signal
Produced by 1.5 Million Galaxies at z ~ 4:Constraints on Matter Density Fluctuations at High Redshift
MIYATAKE, Hironao1, HARIKANE, Yuichi2, OUCHI, Masami3/2, ONO, Yoshiaki2, YAMAMOTO, Nanaka1,
NISHIZAWA, Atsushi J.4, BAHCALL, Neta5, MIYAZAKI, Satoshi3, PLAZAS MALAG´ON, Andr´es A.5
1: Nagoya University, 2: ICRR, University of Tokyo, 3: NAOJ, 4: Gifu Shotoku Gakuen University, 5: Princeton University

The discovery of the accelerated expansion of theuniverse through the observation of Type Ia supernovae
in the late 1990s and the precise measurement of thecosmic microwave background (CMB) and the detectionof baryonic acoustic oscillations in the 2000s haveestablished the so-called ΛCDM standard model. Here, Λis the cosmological constant (more generally, dark energy)
that causes the cosmic acceleration, and CDM stands forcold dark matter required as a gravitational source for theformation of astronomical objects. Although the ΛCDM
model can explain cosmological observations quite well,
the nature of these dark components is unknown. In order
to identify the dark components, it is necessary to first
thoroughly examine the ΛCDM Standard Model.
In the late 2010s, it was suggested that the clumpinessof the Universe S8 obtained from measurements of largescale structure of the universe using weak gravitational
lensing is systematically smaller than that predicted fromthe CMB fluctuation measurements by the Planck satellite[1]. This could be an indication of a breakdown of theΛCDM model and is referred to as the S8 tension.
A method for measuring the large-scale structureof the redshift z < 2 using weak lensing has alreadybeen established, and reducing the statistical error of
weak lensing signals by increasing the statistics andimproving the accuracy of the S8 measurement will be
the focus of the next-generation galaxy imaging surveys,
such as Legacy Survey of Space Time (LSST), Euclid
Space Telescope, and Roman Space Telescope. On theother hand, a method to measure S 8 from large-scale
structures at z > 2 has not been established. A discovery
that S8 varies as a function of the redshift of the largescale structure would suggest the existence of a theory
beyond the ΛCDM Standard Model. In this study, we
have developed a method to measure S8 from large-scale
structures at z > 2 and succeeded in measuring S8 fromlarge-scale structures at z ~ 4 for the first time. The details
are described below.
In the measurement of large-scale structure with weaklensing, it is necessary to use tens to hundreds of millionsof galaxy shapes in order to measure the slight distortionof light coming from the background galaxies. For z > 2,
weak lensing cannot be used because a sufficient numberof background galaxies cannot be detected. On the other
hand, light coming from CMB is also distorted by theforeground structure. Since the CMB lensing is sensitive
to the structure of all redshifts from the recombination
period of the universe to the present, the CMB lensing by030

I Scientific Highlights

itself cannot extract only the z > 2 structure. Therefore,
we have used cross-correlations between a large sample
of distant galaxies consisting of about 1.5 million LymanBreak galaxies detected with the Subaru Hyper SuprimeCam (HSC) using the dropout technique [2] and the
CMB lens map measured with the Planck satellite todetermine the z ~ 4, we have successfully measured thedark matter distribution around the galaxies (Figure 1) [3].
This is the first detection of the dark matter distribution
around galaxies at such a high redshift in the world. In
addition, S8 was measured from the large-scale structureof z ~ 4 by combining it with the clustering signal of thez ~ 4 galaxies [2]. As a result, we obtained S8 smaller
than S8 predicted from the Planck CMB measurement,
but we could not conclude that the difference in S8 wassignificant due to the large statistical error.
Our results are the first example of the new method
for measuring S 8 from large-scale structure at z > 2
applied to real data. We used a galaxy sample based on
HSC data of about 305 square degrees, but the number ofgalaxies in the final HSC data is about three times larger
than the sample used in this study, and LSST, Euclid
Space Telescope, and Roman Space Telescope provide
with us with the much more number of distant galaxies.
In addition, there is already a low-noise CMB lens map
by the Atacama Cosmology Telescope (ACT) and theSimons Observatory and CMB-S4 will provide a CMBlens map wich a much lower noise level. Thus, it will bepossible to measure S8 from large-scale structures at z > 2
with higher accuracy in the future.

Figure 1: CMB lensing signal of a z ~ 4 galaxy sample. The
horizontal axis denotes the angular separation from the galaxies,
and the vertical axis denotes the convergence field of the CMB
lensing. The points with error bars denote data points and thesolid line denotes the best-fit curve. This figure is adopted from [3]with modifications.
References[1] Abdalla, E., et al.: 2022, JHEAp, 34, 49.
[2] Harikane, Y., et al.: 2022, ApJS, 259, 20.
[3] Miyatake, H., et al., 2022, PRL, 129, 061301.

Discovery of a Super-Earth around the M4.5 Dwarf Ross 508
HARAKAWA, Hiroki1, TAKARADA, Takuya2/3, KASAGI, Yui3/4, HIRANO, Teruyuki2/3/4, KOTANI, Takayuki2/3/4,
KUZUHARA, Masayuki2/3, OMIYA, Masashi2/3, KAWAHARA, Hajime5/6, FUKUI, Akihiko6, HORI, Yasunori2/3,
ISHIKAWA, Hiroyuki T.7, OGIHARA, Masahiro8, LIVINGSTON, John2/3, BRANDT, Timothy D.9,
CURRIE, Thayne1/10, AOKI, Wako3/4, BEICHMAN, Charles A.11/12, HENNING, Thomas13, HODAPP, Klaus14,
ISHIZUKA, Masato6, IZUMIURA, Hideyuki15, JACOBSON, Shane14, JANSON, Markus16, KAMBE, Eiji1,
KODAMA, Takanori6, KOKUBO, Eiichiro3/4, KONISHI, Mihoko17, KRISHNAMURTHY, Vigneshwaran18,
KUDO, Tomoyuki1, KUROKAWA, Takashi19, KUSAKABE, Nobuhiko2/3, KWON, Jungmi6, MATSUMOTO, Yuji3,
MCELWAIN, Michael W.20, MITSUI, Koyu6, NAKAGAWA, Takao5, NARITA, Norio6, NISHIKAWA, Jun3/4,
NUGROHO, Stevanus K.2/3, SERABYN, Eugene11, SERIZAWA, Takuma3/19, TAKAHASHI, Aoi2/3,
UEDA, Akitoshi3/4, UYAMA, Taichi3/11/12, VIEVARD, Sébastien1, WANG, Ji21, WISNIEWSKI, John22,
TAMURA, Motohide2/3/6, SATO, Bun’ei23
1: Subaru Telescope, 2: Astrobiology Center, 3: NAOJ, 4: SOKENDAI, 5: ISAS/JAXA, 6: University of Tokyo, 7: University of Western
Ontario, 8: Shanghai Jiao Tong University, 9: University of California Santa Barbara, 10: NASA / Ames Research Center, 11: California
Institute of Technology, 12: NASA Exoplanet Science Institute, 13: Max Planck Institute, 14: University of Hawaii, 15: Subaru Telescope
Okayama Branch, 16: Stockholm University, 17: Oita University, 18: McGill University, 19: Tokyo University of Agriculture and Technology,
20: NASA Goddard Space Flight Center, 21: Ohio State University, 22: University of Oklahoma, 23: Tokyo Institute of Technology

the inner boundary of the habitable zone (the distancefrom the central star where liquid water can exist), but theplanet would enter the habitable zone near the aphelion.
The detailed characterization of Ross 508 b helps
understand the habitability of a super-Earth.
The discovered planet Ross 508 b is the first exampleof the successful detection of a super-Earth using only
the near-infrared Doppler method, demonstrating that the
IRD is capable of detecting planets independently whileachieving the highest precision as a near-infrared Doppler
method. In the future, we plan to report new planet
discoveries from IRD-SSP and findings on the indicatorsof stellar activity, which have not yet been established in
the near-infrared wavelength region.

RV [m s 1]

Search for exoplanets around late M-type dwarfs
is one of the frontiers because of the difficulty ofefficient survey using CCD cameras due to theirfaintness in the visible wavelength. The IRD (InfraRed
Doppler instrument) is a high dispersion near-infrared
spectrograph mounted on the Subaru Telescope in 2018that enables highly accurate exoplanet searches by the
Doppler method. We started the Subaru Strategic Programusing IRD (IRD-SSP) in 2019 and have been conductinga systematic exoplanet search mainly targeting lateM-type stars as a pioneering survey using an 8+ meterclass telescope.
Ross 508 is an M4.5 main-sequence star at a distanceof about 11.2 pc [1] and has been observed 102 times in aframework of IRD-SSP [2]. The spectroscopic abundance
analysis [3] determined its metallicity to be [Fe/H] =−0.20. From the analysis of spectral energy distribution
and photometric data, the effective temperature isestimated to be Teff = 3071 +34−22 K and the mass is estimatedto be M* = 0.177 ± 0.005 M⊙. The periodogram analysisof the radial-velocity (RV) variations indicates that themost significant periodicity was detected around period
10.7 days and that there is no periodicity of stellar
activity that synchronizes with this period, confirmingthat this is not a pseudo variation of the RV but theactual motion of the star by the planet. We estimated theorbital parameters of the planet for the detected period.
We found that the orbital period is 10.77 ± 0.01 days, the−1semi-amplitude of RV is 3.92 +0.60−0.58 m s , the orbit length
radius is about 0.054 au. The estimated minimum mass ofthe planet is approximately 4.0 M⊕ (Figure 1). Although
the orbital eccentricity was not constrained by theaccuracy of the RV measurements and the limited numberof data, the best-fit value was e ~ 0.33, suggesting that theeccentricity may be high. Assuming this orbit, the mean
orbital radius of the planet would be further inward thanMp = 4.00M
P = 10.77 d
e = 0.33

15
b
10
5
0
5
10
15
0.0

0.5
Orbital Phase

1.0

Figure 1: Phase-folded RV variations (yellow and green circles).
Green circles are the same as yellow ones but obtained in 2021
August and September (See HH+2022 for details). The red line
represents the best-fitting RV model. Gray lines represent 100
RV model curves randomly selected from the posterior. The
white circles indicate repeated placement of the same dataset forvisibility.
References[1] Koizumi, Y., et al.: 2021, PASJ, 73, 154.
[2] Harakawa, H., et al.: 2022, PASJ, 74, 904.
[3] Ishikawa, H. T., et al.: 2022, AJ, 163, 72.

I Scientific Highlights

031

Deep Near-infrared Imaging of the Faint X-ray Point Sources
Constituting the Galactic Bulge X-ray Emission
MORIHANA, Kumiko1, TSUJIMOTO, Masahiro2, EBISAWA, Ken2, GANDHI, Poshak3
1: NAOJ, 2: JAXA/ISAS, 3: University of Southampton

The presence of the apparently extended hard (≥2 keV) X-ray emission along the Galactic plane has been
known since the early 1980s [1], which is called theGalactic Diffuse X-ray Emission (GDXE). The emission
has an integrated luminosity of ~1×1038 erg s−1 at 2–10
keV with a spectrum described by two-temperaturethermal plasma (k BT~1 and 5–10 keV). A remarkablefeature in the X-ray spectrum is the strong Fe K emission
line complex (e.g., [2]) comprising neutral or low
ionization state line at 6.4 keV (Fe I) and highly-ionized
ion lines at 6.7 (Fe XXV) and 7.0 keV (Fe XXVI).
With the advent of the Chandra X-ray Observatory,a large fraction of the GDXE at the Galactic bulge (l= 0 °. 08, b = −1 °. 42; the Chandra Bulge Field or CBF,
hereafter) was resolved into 2,002 faint discrete sources[3,4]. The major constituents of these sources have long
been considered to be X-ray active stars and magnetic
cataclysmic variables (CVs). However, recent works
including our NIR imaging and spectroscopic studies
argue that other populations should be more dominant[4,5]. We conducted a much deeper NIR imaging
observation at the CBF to investigate this further.
We carried out a deep J H Ks imaging observation at
the CBF using the MOIRCS on the Subaru telescope,reaching the limiting magnitude of ~18 mag in the J, H,
and Ks bands, and identified ~50 % of the X-ray sources
with NIR counterpart candidates. We classified all the
X-ray sources into three groups (A, B, and C) based on
their X-ray color-color diagram (Figure 1 xy-axis). Since
most of the X-ray sources have poor photon statistics, weused the method based on the color quantiles developedby [6], which was also adopted in our previous work[4] (details are shown in the caption of Figure 1). We
generated three-dimensional plots (Figure 1; X-ray
color–color and the ratio of the X-ray to the NIR flux) todisentangle the overlap among the groups. The ratio of
the X-ray flux to the NIR flux is expected to be relatively
high for the binaries containing compact objects and low
for stellar sources (Figure 1 z-axis). We further made acomposite 0.5–8 keV spectrum of all the X-ray sourcesin each group and carried out spectral fittings. Then, wecharacterized their features based on the X-ray and NIR
features of each group.
We argue that the major population of the GroupA and C are, respectively, CVs (binaries containing
a magnetic and non-magnetic white dwarf with ahigh accretion rate) and X-ray active stars. The major
population of the Group B sources is presumably WD

032

I Scientific Highlights

binaries with low mass accretion rates (“quiet” WDbinaries). The Fe K equivalent width in the composite
X-ray spectrum of the Group B sources is the largest
among the three and comparable to that of the Galactic
bulge X-ray emission. This leads us to speculate that
there are numerous WD binaries with low mass accretion
rates, which are not recognized as CVs, but are the major
contributor to the apparently extended X-ray emission.
“quiet” WD binaris

magnetic-CVs andnon-mag CVs with high accretion rates

-1

10

ABC

10-2
-3

10

FX,h/F K 10-4
10-5
10-6

X-ray active stars-1.4 -1.2 -1.0 -0.8 -0.6

-0.4 -0.2 0.0 0.2
0.4
q1=log 10 Q50/(1-Q50)

3.0
2.5
2.0
1.5 q2=3*Q25/Q75
1.0
0.5

Figure 1: Three-dimensional plot of q1, q2, and the ratio of X-ray
to NIR f lux. Here, the quantile E x (keV) is the energy below
which x % of X-ray photons reside in the energy-sorted list ofx − Eminphotons and Qx = EEmax− Emin , in which Emin and Emax are the lower
and upper bounds of the energy (0.5 and 8 keV), respectively. The
metric q1 reflects the degree of photon spectrum being biased
toward the harder (q1 is large) or softer (q1 is small) end, andthe metric q2 reflects the degree of photon spectrum being less(q2 is large) or more (q2 is small) concentrated around the peak.
Different colors are used for the three groups [7].

References[1] Worrall, D. M., et al.: 1982, ApJ, 255, 111W.
[2] Koyama, K., et al.: 1996, PASJ, 48, 249.
[3] Revnivtsev, M., et al.: 2009, Nature, 7242, 1142.
[4] Morihana, K., et al.: 2013, ApJ, 766, 14.
[5] Morihana, K., et al.: 2016, PASJ, 68, 57.
[6] Hong, J., Schlegel, E. M., Grindlay, J. E.: 2004, ApJ, 614, 508.
[7] Morihana, K., et al.: 2022, PASJ, 74, 283.

Direct Imaging Discovery of a Benchmark Brown Dwarf
Orbiting the Hyades Accelerating F5-type Star HIP 21152 [1]KUZUHARA, M.1/2, CURRIE, T.3/4/5, TAKARADA, T.1/2, BRANDT, T. D.6, SATO, B.7, UYAMA, T.8,
JANSON, M.9, CHILCOTE, J.10, TOBIN, T.10, LAWSON, K.11, HORI, Y.1/2/12, GUYON, O.13/3/1,
GROFF, T. D.14, LOZI, J.3, VIEVARD, S.3, SAHOO, A.3/15, DEO, V.3, JOVANOVIC, N.8, AHN, K.3,
MARTINACHE, F.16, SKAF, N.3/17, AKIYAMA, E.18, NORRIS, B. R.19, BONNEFOY, M.16,
HEŁMINIAK, K. G.20, KUDO, T.3, McELWAIN, M. W.14, SAMLAND, M.21, WAGNER, K.13,
WISNIEWSKI, J.11, KNAPP, G. R.22, KWON, J.23, NISHIKAWA, J.2/1/12, SERABYN, E.24,
HAYASHI, M.2, TAMURA, M.23/1/2
1: Astrobiology Center of NINS, 2: NAOJ, 3: Subaru Telescope, 4: NASA-Ames, 5: Eureka Scientific, 6: UCSB, 7: Tokyo Institute ofTechnology, 8: Caltech, 9: Stockholm University, 10: University of Notre Dame, 11: University of Oklahoma, 12: SOKENDAI, 13: Universityof Arizona, 14: NASA-Goddard, 15: STScI, 16: CNRS, 17: LESIA, 18: Niigata Institute of Technology, 19: University of Sydney, 20: NCAC,
21: MPIA, 22: Princeton University, 23: University of Tokyo, 24: NASA-JPL

The astrometry measurements from the Gaia
space telescope can be combined with those from the
Hipparcos to calculate the proper motion accelerationsof nearby stars [2], which are available to predict whichstars host companion objects. We used the catalog of
the accelerations [2] in target selection to search for
giant planet and brown dwarf (BD) companions. The
selected targets were observed with SCExAO andCHARIS, extreme adaptive optics high-contrast imaging
instruments of the Subaru Telescope. As a result, wediscovered a BD companion around the F5-type star
HIP 21152 [1]. HIP 21152 is a member of the Hyades
open cluster (OC) consisting of a lot of stars as young
as 750 ± 100 Myr [3,4]. We obtained four high-contrast
images with the Subaru and Keck telescopes to confirm
that the companion (HIP 21152B) orbits the star. We
also measured radial velocity (RV) measurements of HIP
21152 using the HIDES on Okayama 188 cm telescope.
The CHARIS observations provide spectra of HIP
21152B, placing the spectral type among L/T typetransition. We applied the orbit analysis software, orvara[5], to the data of direct imaging, RV, and the propermotion accelerations from [2]. As a result, the mass andsemi-major axis of HIP 21152B was estimated to be+7.2
27.8 +8.4−5.4 times higher than that of Jupiter and 17.5 −3.8 au,
respectively. The dynamical mass estimation is slightly
lower than that from a mass estimation dependent on theevolutionary models of [6] and age of HIP 21152B.
The discovery of HIP 21152B corresponds to thefirst direct imaging of a substellar object orbiting a
main-sequence star in the Hyades OC. In addition, its
mass is the closest to a planetary-mass regime among
all the directly-imaged BD companions whose masses
have been dynamically constrained (see a sample listin [7]). Thus, HIP 21152B is a great benchmark to
calibrate the techniques used to infer the properties ofsubstellar objects, including giant planets. Our SCExAO/CHARIS survey continues to observe nearby stars having
accelerations in their proper motions, enabling morediscoveries of intriguing substellar companions withestimations of their dynamical masses.

Figure 1: An image of the HIP 21152 system observed with
SCExAO/CHARIS. Credit: Astrobilogy center

References[1] Kuzuhara, M., et al.: 2022, ApJL, 934, L18.
[2] Brandt, T. D.: 2021, ApJS, 254, 42.
[3] Gagné, J., et al.: 2018, ApJ, 856, 23.
[4] Brandt, T. D., Huang, C. X.: 2015, ApJ, 807, 58.
[5] Brandt, T. D., et al.: 2021, AJ, 162, 186.
[6] Baraffe, I., et al.: 2003, A&A, 402, 701.
[7] Franson, K., et al.: 2022, AJ, 163, 50.

I Scientific Highlights

033

Demonstration of a Low-noise Microwave Amplifier
Based on SIS Mixers
KOJIMA, Takafumi, MASUI, Sho, SHAN, Wenlei, UZAWA, Yoshinori(NAOJ)The development of a large-scale array of heterodyne
receivers is expected for future radio astronomy.
One of the technical challenges in the array receiverdevelopment is the cryogenic low-noise amplifier
operated at a physical temperature of 4 K used in the firststage of the intermediate frequency chain. The typical DC
power consumption of cryogenic semiconductor-based
amplifiers is about 1–10 mW, which makes it difficult todevelop large-scale arrays considering the thermal load
on a typical refrigerator.
We have devised a microwave low-noise amplifier
based on two Superconductor-Insulator-Superconductor(SIS) mixers [1]. The first SIS mixer is used as afrequency converter to up-convert the input microwave
signal to the millimeter-wave by a local oscillator (LO)source, and the subsequent SIS mixer is to down-convert
the signal with the identical LO source. As a result, theinput and output signals have the same frequency, andthus, this configuration can be a very simple microwave
amplifier if both frequency converters provide conversion
gain. It has the potential to become a versatile amplifier
with power consumption in the order of μW, wide
bandwidth, high gain, and low noise.
To demonstrate and characterize this superconducting
amplifier concept, we configured it with two 100-GHzband SIS mixers, two signal/LO couplers, and amillimeter-wave isolator (Figure 1). The bias voltage
and current of the SIS up- and down-converters were
set to the minimum noise temperature of the amplifier.
As a result of characterization, low-noise performance
was obtained, typically with a gain of 6–8 dB and anoise temperature of 11 K below the signal frequencyof 5 GHz [2]. Using a network analyzer, we also
confirmed reasonable gain linearity within the range ofthe measurements. Based on the breakdown of the SIS
amplifier performance at a signal frequency of 1 GHz,
the gain and noise temperatures of the SIS up-converter
and SIS down-converter were found to operate at 2.7
dB and 4.0 K, and 6.4 dB and 7.8 K, respectively. This
result indicates that the lower noise of the respective SIS
converters, and the higher gain of the SIS up converter
can also be expected to further improve the performanceof the SIS amplifiers.
This SIS amplifier concept demonstrated in thisstudy can be regarded as a single amplifying element
like a transistor, and its microwave characteristics arecomparable to those of cryogenic semiconductor devices
such as High Electron Mobility Transistors. If the circuit

034

I Scientific Highlights

can be integrated to be more compact, it is expected tobe applied to array receivers and other array systems.
In addition, we found that the concept of using two
frequency mixers can work as nonreciprocal devices suchas an isolator [3] and gyrator [4]. This also means that
this SIS amplifier can have directivity, which recalls theirrealization as compact general-purpose amplification
devices. This may contribute to the challenges ofdeveloping large-scale systems for radio astronomy andquantum computers.
This work was supported in part by JST Moonshot
R&D Grant Number JPMJMS2067 and JSPS KAKENHI
Grant Numbers JP19H02205, JP21H01134, andJP22H04955.

Figure 1: Photograph of the SIS-based amplifier used in thisdemonstration.

References[1] Kojima, T., Shan, W., Uzawa, Y.: 2018, AIP Advances, 8,025206.
[2] Kojima, T., et al.: 2023, Applied Physics Letters, 122, 072601.
[3] Masui, S., et al.: 2023, IEEE Microwave and Wireless
Technology Letters, 33, 1051.
[4] Masui, S., et al.: 2023, IEEE Appliled Superconductivity, 33, 1.

II Status Reports of Research Activities
01. Mizusawa VLBI Observatory
Mizusawa VLBI Observatory operates VLBI (Very Long
Baseline Interferometry) arrays to provide their machine time
for open use, and conduct observational studies of Galactic
structure, maser sources, active galaxy nuclei, and so on. As
its main facility, the observatory operates the VERA arrayconsisting of four 20 m radio telescopes in cooperation with
Kagoshima University. KaVA (KVN and VERA Array), which
combines the VERA and KVN (Korean VLBI Network) in
Korea, and East Asian VLBI Network (EAVN: East AsianVLBI Network), which consists of Japanese, Chinese, andKorean radio telescopes, are being operated and opened tothe international community. The observatory also operates
Yamaguchi 32-m Radio Telescope and Hitachi / Takahagi 32-m
radio telescopes in collaboration with Yamaguchi and Ibaraki
University, respectively, contributing to research in Japanese
VLBI Networks. As a member organization of the Event
Horizon Telescope project, the observatory contributes to thepromotion of millimeter-wave VLBI as well. The observatory
also plans to participate in SKA (Square Kilometre Array) as
a future project. In addition to these VLBI-related activities,
the observatory plays a wide range of roles beyond astronomy,such as operation of the Esashi Earth Tide Observation Facility,
which is used for research in geophysics.

1. VERA(1) Observations and Common-Use Observations
The four stations of VERA were operated by remote
cont rol f rom AOC (A r ray O peration Center) at NAOJ
Mizusawa Campus. In FY 2022, excluding EAVN commonuse, 159 sessions (1459 hours) of regular VLBI observations
were conducted by VERA, which is a decrease of 20 % fromthe previous year. The main reasons for this decrease are theextension of the maintenance period until September 2022,
the suspension of operations at the Mizusawa station due tosnowfall in winter, and Ishigaki-jima station has suspended
operations from January 2023 due to electrical and drive
system failures. For the regular scientific operation for VERA,a new observational mode “VERA Large-scale Collaborative
Program (VLCOP)” has been initiated since September 2022.
In FY 2022, VLBI observations carried over from FY 2021
were conducted for a total of 63 sessions (515 hours) until
August 2022. After starting VLCOP in September 2022, a
total of 78 observations (693 hours) were conducted via theautomatic remote operation from the Mizusawa AOC. In
addition, single-dish observations were carried out at the AOC
and local sites. These observations were done as part of the
VLCOP programs after September 2022. In the FY 2022, theobserving time for the single-dish operation for all stations was1815 hours.

As for the types of VLBI observations, regular annual
parallax measurements, astrophysical observations, andgeodetic observations were carried out as continuations fromthe previous project. Furthermore, during the period when thefour stations could not operate simultaneously, observations
newly adopted from the second half of this fiscal year, such as
SETI-related observations, installation tests of new observationequipment and fringe tests, were carried out. In addition tothese, we conducted KaVA (KVN and VERA Array) and
EAVN (East Asian VLBI Network) observations, which will
be described in the following sections. These VLBI data,
except for KaVA and EAVN, were processed at the Mizusawa
Correlation Center in NAOJ Mizusawa Campus. The correlated
data were sent to each observation proposer and to persons incharge of data analyses in the case of project data and geodesy
data. VERA common-use calls-for-proposals in FY 2022 were
not conducted by VERA alone. This is because almost allobserving modes became available in the EAVN common-use,
which was released at the same time, and hence, all proposals
were submitted to EAVN.
(2) Science Research
In FY 2022, Mizusawa VLBI Observatory published atotal of 47 refereed journal papers for scientific achievements.
Among them, 4 papers were published by the Observatory
members as a PI and 2 of them were published by graduate
students in the University of Tokyo as a PI. Using the facilities
operated by Mizusawa VLBI Observatory, 10 papers were
published to report scientific results from the East Asian VLBI
Network (EAVN). These are VLBI imaging of AGNs andmaser astrometry, as well as theoretical works related to theobservational results and development works such as VLBI
experiments between East Asia and Italy, new instruments forpolarization measurements, and the multi-frequency receiving
system installed on the Nobeyama 45-m telescope. As followup studies for the EAVN large program, two refereed journal
papers were published to report maser variability and chemical
properties in high-mass star-forming regions using ALMA
observational data. Using radio telescopes in the Japanese
VLBI Network (JVN), two papers were published to report
the first FRB observation in Japan and development of aninterferometer. Furthermore 16 papers were published on the
AGN studies, mostly for the first imaging of the super-massive
black hole at the Galactic center Sgr A*, from the international
project Event Horizon Telescope (EHT) in which Mizusawa
VLBI Observatory is participating. For the preparatory studies
for the future project Square Kilometre Array (SKA) which isunder discussion in Mizusawa VLBI Observatory, there wereseveral refereed journal papers from the SKA precursors andpathfinders, such as two papers for the maser variability studies

II Status Reports of Research Activities

035

using the European VLBI Network (EVN), one paper each forstudies on galaxy clusters from MeerKAT in South Africa,uGMRT in India, and detailed imaging of outf low of highmass star-forming region from JVLA in US and e-MERLIN
in UK through synergy with ALMA. An IAU symposium on
masers (#380) was held in Kagoshima, and there were many
presentations reporting VERA’s results.

2. The Japanese VLBI Network (JVN)The University VLBI Collaboration Observation projects
were conducted jointly by NAOJ and six universities. We
organized the radio telescopes of VERA, universities, andresearch institutes (JAXA/ISAS) to establish the Japanese
VLBI Network (JVN). The JVN operates at three frequency
bands: 6.7 GHz, 8 GHz, and 22 GHz. In FY 2022, a total of
360 hours were dedicated to VLBI observations. The primaryresearch areas included active galactic nuclei, methanol masers,
and X-ray binary systems. Additionally, Ibaraki University
and Yamaguchi University each conducted over 1000 hours of
single-dish observations related to JVN research.
During FY 2022, JVN focused on three research targets
for time-domain VLBI astronomy: (1) (periodic) flux variationsin CH 3 OH masers, (2) ext remely compact HII regions
immediately after the onset of nuclear burning, and (3) timedomain VLBI astronomy of high-energy astrophysical events.
The key baselines for these studies involved high-sensitivity
telescopes larger than 30 m within JVN. One example of JVN
observations in 2022 was a survey of gamma-ray emitting
AGN candidates.
Throughout the year, more than 10 papers were published,including Fujisawa et al. (2022) and Tanabe et al. (2023).
Among them were eight papers on the accretion burst of protohigh-mass stars which was found by the Ibaraki group, as
well as two short reports. A joint research seminar called theIbaraki-Yamaguchi Joint Seminar was held for students fromthese two universities. Yonekura from Ibaraki University
led the development study, focusing on upgrading the VLBI
observation system at the Ibaraki station through Grants-inAid for Scientific Research. Several students from Ibaraki
and Yamaguchi Universities were under the supervision ofProfessor Ogawa at Osaka Metropolitan University.

3. International observations with Korea-Japan
VLBI, East Asian VLBI and mm-VLBI(1) Observations and Common Use Observations of EAVN
I n F Y 2 0 2 2 , E AV N ( E a s t A si a n V L BI Ne t wo r k)observations, utilizing KVN and VERA Array (KaVA), Sejong
22-m in Korea, the Tianma 65-m, Sheshan 25-m, Nanshan
26-m, Kunming 40-m, Nobeyama 45-m, and Yamguchi/
Hitachi/Takahagi 32-m radio telescopes, were conducted fora total of 127 observations (918 hours), including common use
observation, test, and verification observations. Most of thescheduled observations were successfully conducted without
any major issues despite the global COVID-19 pandemic.

036

II Status Reports of Research Activities

EAVN open-use calls for proposals for semesters 2022B
and 2023A were released in June and November of 2022,
respectively. In total, 26 proposals requesting a total time of876 hours were submitted from Japan, Korea, China, Italy,
Spain, Thailand, and Chile. Through the evaluations by 49
referees nominated from scientists in related fields and thesubsequent decision made by the EAVN combined Time
Allocation Committee, a total of 25 proposals (854 hours) were
accepted. Regarding global mm-VLBI, EHT observations werecarried out remotely in March 2023 due to the outbreak of
COVID-19.
(2) Results of Research
In FY 2022, 4 papers based on KaVA (3 on active galactic
nuclei, 1 on massive star forming regions), and 9 papers basedon EAVN (1 on array review, 6 on active galactic nuclei,
2 on galactic astrometry) were published in peer-reviewed
journals. Nine out of them include significant contributions
from members of Mizusawa VLBI Observatory as co-authors.
Here some works are highlighted. Tazaki et al. (2022) applied
the sparse modeling imaging technique to M87 EAVN 22 GHz
data, and they demonstrated that low frequency wave VLBI
images also allow us to accurately constrain the structure of
the formation regions of relativistic jets. EHT Collaboration
et al. (2022) reported the results from the 2017 SgrA* multiwavelength observing campaign including EHT and EAVN,
and EAVN data greatly helped to constrain the interstellar
scattering properties towards the source, which was crucial for
successfully imaging of the black hole shadow with the EHT. In
Asanok et al. (2022), they monitored water vapor masers in themassive star forming region W49N, and revealed the detailed
structure such as bipolar outf lows together with accurate
proper motion measurements. Sakai et al. (2023) performed
KaVA/EAVN astrometry observations towards G034.84-00.95
that is located in the extreme outer galaxy, and they estimatedthe kinematic distance to the source to be 18.6 kpc (±1.0kpc), demonstrating the powerful capability of KaVA/EAVN
astrometry. Other than the above publications, a white paper on
the Thailand 40-m radio telescope was also published, in whichtight collaboration with EAVN is highlighted.
Regarding mmVLBI/EHT, 12 papers (including the abovementioned multi-wavelength paper) were published in peerreviewed journals. Especially, 10 of them (6 collaboration
papers and 4 official papers) were about the first EHT results on
the Galactic Center SgrA* based on the 2017 EHT campaign.
The research results were featured in various media. Other
than EHT, one paper on M87 based on 3 mm global VLBI
observations, in which one of the corresponding authors is amember of Mizusawa VLBI Observatory, was accepted in arefereed journal.

4. Future Planning
As for the SKA observatory project, construction of both
SKA MID, to be built in South Africa, and SKA LOW, to bebuilt in Australia, commenced in July 2021, and the production

of subsystems and site infrastructure has started based on theconstruction sharing by the participating Member countries.
NAOJ par ticipated in the Assembling, Integration, andVerification (AIV) as in-kind contributions. NAOJ has observer
status on the SKA Council to understand the construction
status of the SKA and to explain the status of research in Japan.
Japan has participated in the relevant SKA Finance Committee,
SKA Contracts Committee and SKA In-Kind Contribution
Committee as well and took part in their deliberations.
The SKA1 Study Group (SKAJ) was organized underMizusawa VLBI Observatory for a period of three years
from FY 2019 to conduct preliminary research and in-kind
contributions to the SKA1 program. Based on the resultsof three year's activities, an SKA1 project proposal was
submitted, and the results of the review led to the conclusionthat it was appropriate to proceed with activities as a subprojectat this stage. FY 2022 was a transitional period, including
project review, and the group continued its activities as a study
group.
SKAJ mainly focused on the research on the three major
Japanese themes (cosmic reionization, cosmic magnetism, andpulsars) established by the SKA Consortium, which represents
the SKA research community. And SKAJ shared the costof the MWA participation fee with universities in Japan andcontinued the research of cosmic reionization. Moreover,research on cosmic magnetism, pulsars, and active galactic
nuclei using other SKA precursors such as Australia's ASKAP
and South Africa's MeerKat was conducted. Through the grantby the National Institutes of Natural Sciences’ Accelerated
Program for Strategic International Research Exchange, two
researchers from India were invited from February to March2023 for joint research on pulsar timing arrays using the Indian
GMRT and seven researchers from Japan visited India for it.
Two researchers were invited from Australia and two young
researchers were sent to Australia for joint research on cosmic
magnetism by using ASKAP. In addition, three lecturers wereinvited from abroad for a workshop on data analysis of cosmic
reionization, cosmic magnetism, and pulsar timing arraysfrom March 2 to 6, 2023, and 18 young researchers from Japan
participated in the workshop.
On the engineer ing side, SK AJ par ticipated in the
Assembling, Integration and Verification (AIV) activities
based on the MoU with SKA Observatory from January 2022,
and developed test contents and created test procedures for
SKA1 LOW AA0.5 with 1FTE. For SKA MID, we agreed
with the SKA Observatory and the South African Radio
Observatory to participate in DISH AIV activities with 0.5
FTE and started the collaboration for it. Development of a
VLBI recorder was initiated with the aim of being adopted
in the development program at the SKAO. The data rate of
VLBI recording is required to be 100 times faster than theconventional VLBI recording system, and for this purpose,the development of a high-speed protype system based on the
VLBI recorder developed in Japan was started. In addition,
Osaka Metropolitan University initiated the basic design of the
optical system to evaluate the feasibility of 15 GHz to 29 GHz

observations at the SKA MID, and started collaborations with
South Africa, the United Kingdom, Sweden, Switzerland, andother countries.
The employment of a specially-appointed researcher
based on an agreement with SKA Observatory was continued,
and scientific research planning was promoted. In addition,with regard to the development of a data analysis system,
we participated as a member in the SKA Regional Steering
Com mit tee, which was organized by the par ticipating
countries, and actively took part in the conceptual design of thesystem. In Japan, we continued to develop a test system for the
JPSRC, a networked data analysis and archiving system that webegan to study jointly with the SKA Japan consortium in FY
2020 and constructed a test system of networked data analysis
servers. Using this system, we have supported a Japanese team,which participated in the SKA Data Challenge 3 to verify
the feasibility of the data analysis method and the amount ofcomputation for cosmic reionization research by analyzing
simulation data.

5. Geodesy and Geophysics
In order to monitor the position and shape of the VERA
network, regular geodetic observations were conducted once totwice a month. VERA internal geodetic observation sessions
using K-band were conducted once a month. Mizusawa
Station conducted IVS sessions (IVS-T2P and AOV) using Sand X-bands once every two months. In AOV and IVS-T2P,
wideband observations using OCTAD-OCTADISK2, andrecorded data transfers to the IVS correlation center have beenroutinely conducted. In FY 2022, VERA internal geodetic
observation was conducted 10 times and we participated in
IVS sessions 6 times. The final estimates of the VERA station
positions were reconstructed based on ITRF2020, which is
newly released in 2022, and supplied to the astrometric analysis
performed by VERA.
We carried out continuous GNSS(GPS) observations at
VERA stations in order to monitor short term coordinate
variations and to estimate atmospheric propagation delays.
The analysis software GipsyX which is developed by NASA/
JPL and Caltech is used in the analysis. The propagation delays(excess pass delays) vary irregularly in time. We produce
essential correction data for VERA accurate astrometry
through GNSS observations. The positioning result of GNSS
and gravity observation data in Mizusawa show the viscoelastic
relaxation process of the 2011 off the Pacific coast of Tohoku
Earthquake. The strain and tilts observation data obtainedat the Esashi Earth Tides Station are distributed in real timeto several institutes and universities based on the research
agreement among them.

6. System Development
As a development group, we are currently developing thedual-polarization and dual-frequency (K, Q) receiver system
at a rate of 32 Gbps for VERA in accordance with the next

II Status Reports of Research Activities

037

EAVN broad-band observing mode. In 2022, we implemented
EMI countermeasures for RF and IF integrated switches with
16 inputs and 4 outputs for both polarization bands (Q, K, C, S,
L), a down-converter for right polarization, and high-speed A/
D converter (OCTAD), and re-installed (OCTAD) at all VERA
stations. As a result, we could conduct VLBI test observations
simultaneously at K and Q bands with dual-polarization using
the K-band RF direct A/D system at the Mizusawa and Iriki
stations, and get the first fringes. In addition, a simultaneous
two-beam and dual-polarization observing mode is available inthis new system, and we conducted test observations and could
get the first fringe. Various CSV tests including the above newmodes are currently ongoing.
Eight years have passed since the Mizusawa correlation
center was established, and the time for server replacement isapproaching. Therefore, as the next system, we are upgrading
the software correlation system using GPUs and continuing
to reduce the number of servers. In 2022, the development of
the correlator using GPUs compatible with the new OS (rocky
linux 9) was completed, and we started to evaluate it andconducted test correlations. We prioritized the processing of
wideband dual-polarization observations (16 Gbps) that require
high computational load and SETI observations that require
high-dispersion spectroscopy (16M FFT points), and achieved
10-20 times faster processing than conventional processing(CPU).

7. Public Relations (PR) and AwarenessPromotion Activities(1) Open House Events (Numbers in <> are the number ofparticipants)
The following open house events are held every year ateach telescope site operated by Mizusawa VLBI Observatory.
• On April 24, 2022 The 13th Open Observatory Event heldby the Ibaraki University Center for Astronomy, and NAOJ
Mizusawa VLBI Observatory, Ibaraki Station. <Total 702
people>• On August 7, 2022 The special open house event at VERA
Ishigaki-jima Station held together with “The Southern Island
Star Festival”. <66 people>• The special open house of VERA Iriki Station jointly heldwith “The Yaeyama Highland Star Festival.” In 2022, thespecial exhibition was canceled to prevent the spread of the
new coronavirus infections.
• From August 6 to August 28, 2022 Mizusawa district “Iwate
Galaxy Festa”. In 2022, the schedule was dispersed to preventthe spread of new coronavirus infections. <Total 690 people>• “Star Island” is the open house event held at V ER A
Ogasawara Station. In 2022, the special exhibition wascanceled to prevent the spread of the new coronavirus
infections.
(2) Regular Public Visits
Throughout the year, the following stations are open to the038

II Status Reports of Research Activities

public on a regular basis. The four VERA stations are open
to the public approximately every day except during the New
Year’s season.
The numbers of visitors to each facility are as follows.
a) Mizusawa VLBI Observatory (VERA Mizusawa Station)
11,188 The campus is regularly open to the general public withthe cooperation of the Oshu Uchu Yugakukan (OSAM: Oshu
Space & Astronomy Museum) located in the campus.
b) VERA Iriki Station 1,038c) VERA Ogasawara Station 6,640d) VERA Ishigaki-jima Station 2,584(3) Cooperation with Local Communities (Numbers in <> are
the number of participants)
Various events were held in cooperation with Iwate
Prefecture and Oshu City. Here are some of the most notable
events.
a) We cooperated with special exhibitions, lectures, andworkshops at libraries co-sponsored by the Southern Iwate
Regional Development Bureau and the municipalities in thesouthern part of Iwate Prefecture.
• Special Exhibitions
Jul 23, 2022 (Sat)–Aug 25, 2022 (Thu) Higashiyama Library of
Ichinoseki Public Libraries
Aug 2, 2022 (Tue)–Aug 16, 2022 (Tue) Kanegasaki Municipal
Library
Sep 2, 2022 (Fri)–Sep 15, 2022 (Thu) Nishiwaga Town Culture
Creation Hall (Galaxy Hall)
Sep 13, 2022 (Tue)–Sep 26, 2022 (Mon) Hiraizumi Municipal
Library
Sep 23, 2022 (Fri)–Oct 26, 2022 (Wed) Kawasaki Library of
Ichinoseki Public Libraries
Oct 12, 2022 (Wed)–Oct 24, 2022 (Mon) Hanamaki Library ofHanamaki City Libraries
Oct 28, 2022 (Fri)–Nov 23, 2022 (Wed) Senmaya Library of
Ichinoseki Public Libraries
Dec 16, 2022 (Fri)–Dec 23, 2022 (Fri) Tono City Library
Dec 21, 2022 (Wed)–Jan 8, 2023 (Sun) Mizusawa Library ofOshu City Libraries• Lectures and Workshops
Oct 29, 2022 (Sat) Senmaya Library of Ichinoseki Public
Libraries / Workshop “Let's make the planets of the Solar
System” Lecturer: Daisuke Sakai Specially Appointed
Assistant Professor
Dec 12, 2022 (Sun) Tono City Library / Workshop “Let's makea twinkle twinkle galaxy ornament!” Lecturer: Fumie Tazaki
Tokyo Electron Technology Solutions Ltd.
b) The Iwate Mar ugoto Kagak u Johokan (led by Iwate
Prefecture), an IT science event for children and adults in Iwate
Prefecture, is held every year and we participated in 2022 as
well.

Jul 16, 2022 (Sat) Iwate Mar ugoto Kagak u Johokan in
Kamaishi at Kamaishi Civic Hall TETTO <160 people>
Dec 16 (Fri) and 17 (Sat) 2022 Iwate Mar ugoto Kagaku
Johokan at Big Roof Takizawa <400 people>c) In 2022, we held a “Kirari Oshu City Astronomical Class”
for elementary and junior high schools in Oshu City.
Aug 26, 2022 (Fri) Hirose Elementary School 4th, 5th, and6th grade / “Expanse of the Universe” Lecturer: Tomohiko
Ozawa <18 people>
Sep 6, 2022 (Tue) Mizusawa Minami Elementary School
6th grade joint / “What is a black hole?” Lecturer: Mareki
Honma <107 people>
Sep 9, 2022 (Fri) Tokiwa Elementar y School 4th grade/ “Seasonal constellations and movement of the stars”
Lecturer: Daisuke Sakai <115 people>
Sep 13, 2022 (Tue) Tokiwa Elementary School 6th grade /“Earth, Moon, and Solar System” Lecturer: Koji Matsumoto<112 people>
Oct 6, 2022 (Thu) Maesawa Junior High School 3rd grade joint(Class 1st, 2nd) / “What is a black hole?” Lecturer: Kazuhiro
Hada <58 people>
Oct 6, 2022 (Thu) Maesawa Junior High School 3rd grade joint(Class 3rd, 4th) / “What is a black hole?” Lecturer: Kazuhiro
Hada <58 people>
Dec 15, 2022 (Thu) Harikawa Elementary School 4th, 5th
grade / “Seasonal constellations and movement of the stars”
Lecturer: Noriuyki Namiki <11 people>

8. Education(1) University and Post-Graduate Education
Regarding postgraduate education, Mizusawa VLBI
Observatory assisted 3 doctoral and 3 master’s course graduate
students from the University of Tokyo with their research. Oneof the master’s course students is from a foreign country. Eachdoctoral and master’s student got the degree in March 2023. In
addition, a staff member of Mizusawa VLBI Observatory gives
lectures at Tohoku University as a visiting professor.
(2) Research Experience for High School Students
Consider i ng the i mproved sit uat ion of COV I D -19,
Mizusawa VLBI Observatory organized the educational
program for high school students in Ishigaki Island, “The
Churaboshi Research Team Workshop” with the support of
JSPS, during summer vacation as usual. The event was coorganized with the Public Relations Center of NAOJ on-site at
the VERA Ishigaki-jima Station and Ishigakijima Astronomical
Observatory. Including 18 participants from outside Ishigaki
Island, a total of 21 high school students experienced thelectures on astronomy, observatory tours, star watching, andobservational studies with the VERA 20-m antenna.

II Status Reports of Research Activities039

02. Nobeyama Radio Observatory
1. Nobeyama 45-m Radio Telescope(1) Charged Telescope TimeThe 41st term (charged telescope time) started on September
1, 2022. This term was the first fiscal year of the charged
telescope time, which was a newly introduced operation
system, after the open use was terminated. The statistics of the
conducted programs are as follows. “General Programs”: 34
programs including one program from abroad, “CSV Programs”:
four programs, “Observation Tutorial Programs”: threeprograms. The number of the successful proposals for “Students
Programs”, which are reviewed scientifically, is two proposals
out of the three submitted proposals.
Remote observations were conducted from Mitaka,
Kagoshima University, Osaka Metropolitan University, Nagoya
University, University of Tokyo, Kyushu University, Keio
University, ASIAA (Taiwan), etc.
(2) Improvements and Developments(a) New Developments- A new focal plane array receiver system for observations
at 72–116 GHz (named “7BEE”) was installed on the
45-m telescope in August and commissioned to carry out
performance evaluations as well as test observations. It
employs seven beam elements, and allow observations of
two polarizations and three bands. This development was
supported by JSPS grant-in-aid KAKENHI Kiban S (Grant
Number JP20H05645; PI: K. Tatematsu).
(b) Approved Development Programs
A total of five programs are in progress as follows.
Nobeyama Radio Observatory (NRO) supported each program
team in the installation of the instruments, particularly inhardware and software interfaces and in test runs.
- 3-band simultaneous observing system HINOTORI.
- Frequency-modulation local oscillation FMLO.
- eQ (30–50 GHz) receiver: The problems with the refrigerator
and the cooled amplif ier that occur red last year were
repaired and the instrument was commissioned to carry out
performance evaluations as well as test observations.
- Millimetric Adaptive Optics (MAO): A demonstration
experiment was conducted with the wave-front sensor
expanded to 5 elements.
- 10 0 - GH z , 109 - ele me nt M K I D ca me r a: A f t e r a t e stobser vation, the camera was removed f rom the 45-m
telescope for refurbishment.
(c) Maintenance and improvements
Maintenance of the 45-m telescope, the receiver systems,
computing system, etc. were performed as follows.
- Regularly scheduled and preventative maintenance was
performed.

040

II Status Reports of Research Activities- Corrective maintenance due to some malfunctions in thefollowing systems.
- The crack in back structure of the antenna- The power-board of the SAM45 spectrometer- Development of the observation preparation tool for overseas
observers is underway.
- The H22 receiver had its amplifiers replaced with new cooled
low noise amplifiers which improved the receiver sensitivity.
(3) Scientific Results
A total of 34 refereed journal papers were published on thebasis of research using the 45-m radio telescope.
1) Results from the Legacy Programs and Open Use General
Programs with the 45-m Telescope
Kaneko, H., et al. investigated the interstellar medium infour interacting galaxies in the early or middle stages of theinteraction. They found that sSFR and SFE for the galactic
scale are similar to those for the isolated galaxies, whereas the
SFE is enhanced for the local kpc scale. This fact indicates thedense gas is not changed in the earlier stages of the interaction.
Tatematsu et al. studied the velocity structure of 36 cores inOrion and found that inward motions were more dominant thanoutward motions in those targets. In addition, they found thatthe blue-skewed spectra are detected in 10 % of the samples,and one of them shows the core is at the last stage of starlesscores judging from the chemical evolution factor. Enokiya
et al. reanalyzed the high-density gas for the Sgr B region of
the Galactic center and suggested a new scenario where thecontiguous collision of two clouds having a velocity differenceof 20 km/s triggered the formation of the Sgr B1 and Sgr B2
regions. Wu et al. performed a survey of 22 GHz H 2O masersfor 178 O-rich AGBs in Sagittarius stellar stream and detected
21 masers including 20 first detections. They investigatedthe distribution of H 2O and SiO masers, and also they found
an elongated structure toward the (l, b)~(340°, 40°) region.
Kaneko, M., et al. conducted a detailed search of the molecular
gas toward the Galactic center direction and found a cloud
having peculiar velocity structure suggesting an intermediatemass black hole is trapping the gas. Fujita et al. analyzed the
FUGIN data, one of the legacy programs of NRO, using amachine learning technique and inferred the distances of themolecular clouds. They also identified 140 thousand clouds andmade a catalog.

2. Research Support(1) 1.85-m Radio Telescope (Osaka Metropolitan University)
With the 1.85-m radio telescope, they have conducted an
extensive survey of molecular clouds along the Galactic plane
using the molecular lines of carbon monoxide isotopologues
in the 230 GHz band. In FY 2018, they started a new project
supported by JSPS (Grant-in-Aid for Scientific Research

on Innovative Areas). In this project, they will relocate thetelescope to the Atacama site in Chile at an altitude of 2400 m,
equipped with an ultra-wideband receiver (230–345 GHz), andcarry out an extensive survey of molecular clouds along the
Galactic plane and in the Magellanic Clouds in the southernsky. In preparation for the relocation, the development of thereceivers was mostly completed by FY 2021, and for FY 2022,
development of a software system enabling remote observations
was mainly promoted at the Nobeyama site.

3. Public Outreach(1) PR activities at Nobeyama Campus
Nobeyama Campus received a cumulative total of 37,690
visitors throughout the year. The open area for visitors has
been limited to outdoor areas as a precaution against the spreadof COVID-19, while from Feb. 13 2023, the exhibition room
is opened reflecting that the alert level of Nagano Prefecture
was reduced. The NMA observation building was operated by
NINS as the NINS exhibition room until FY 2021, whereas
the building has been operated by NRO as the NAOJ-NRO
exhibition room from FY 2022.
Staff members conducted 11 guided tours and granted 25
requests for filming and interviews. One workplace visit by
local high schools was conducted. The filming and interview
requests were mainly about research activities and introducing
NRO.
The annual Nobeyama Special Open House was held as
an online event. The maximum number of connections for live
streaming was about 500 and the total number of views for allcontent was about 84,000 in the three months after the event.
Moreover, we received and answered about 134 phone calls
this year from the public regarding the regular opening of theobservatory, observatory events, and general astronomy.

were accepted for education.

5. Misc. Activities(1) Activities related to the Agreement on Mutual Cooperation
between NAOJ and Minamimaki Village
In 2018, NAOJ and Minamimaki Village sig ned anagreement on mutual cooperation to support PR activities forscientific results of NAOJ and the utilization of the facilities of
NRO for the tourist and education activities of Minamimaki
Village. Some activities were conducted, such as paid sighseeing tours around Nobeyama Campus by Minamimaki
Village Shinko-kosha. They had 69 paid group tours andfilmings.
(2) Hiring, Transfer (incoming)
None(3) Retirement, Transfer (outgoing)
Takami, Masaki: Leader of Accounting Section, moved to
Shinshu University
Maekawa, Jun: Research Supporter, retired
Takahashi, Shigeru: Research Supporter, retired(4) NRO Conference Workshops and Users Meeting- December 20–21, 2023, Hybrid (in-person and on-line)
FY 2022 ALMA/45-m/ASTE Users Meeting (Organizing
Committee: Misato Fukagawa, Masumi Shimojo, Ken
Tatematsu, Tetsuhiro Minamidani, Takeshi Kamazaki(NAOJ))(2) Cooperation with Local Communities
The annual Nobeyama Special Open House was held
online with contributions by Minamimaki Village Shinkokosha, Minamimaki Village, Minamimaki village societyof commerce and industry, Nagano Prefecture, and Nagano
Prefecture Board of Education. However, “Jimoto Kansha
Day (Thanks Day for the Locals)” for local communities(Minamimaki and Kawakami Villages) by 3 Nobeyama
institutes was cancelled.
Moreover, the “Nagano Prefecture is Astro-Prefecture”
liaison council promoted the activities such as monitoringnight sky condition in the prefecture. The 7th meeting washeld online and on-site at Bunka-hall in Kiso-Bunka-Koen on
December 10 with about 50 participants. Some activity reports
and a discussion on future activities were presented.

4. Education
Five master’s course students and one doctoral course
student from Osaka Metropolitan University and one doctoral
course student from the University of Electro-Communications

II Status Reports of Research Activities041

03. Solar Science Observatory (SOL)The Solar Science Observatory (SOL) project, as a COE ofsolar observations in Japan, operates the Hinode satellite andground-based solar telescopes to pursue the development ofsolar research by acquiring and accumulating multi-wavelength
data. The project also carries out the development of advanced
technology for next-generation solar observations.

1. Hinode Space Observatory
The scientif ic satellite Hinode is an ear th-orbiting
satellite that was launched on September 23, 2006, by ISAS/
JAXA, as Japan’s third solar observational satellite following
Hinotori (1981) and Yohkoh (1991). Hinode is equippedwith three telescopes: the solar optical telescope (SOT), the
X-ray telescope (XRT), and the extreme ultraviolet imaging
spectrometer (EIS). In addition to observations of the detailed
magnetic field and velocity field of the solar photosphere, itcarries out simultaneous observations of the radiance andvelocity field from the chromosphere to the corona. The
telescopes equipped on the Hinode satellite were developed
through international collaboration based on cooperation
between ISAS/JAXA and NAOJ with contributions by the US
NASA and the UK STFC. The European Space Agency ESA,
and the Norwegian Space Center NSC also join in its scientificoperations. NAOJ played a central role in the development of
the science payload in Japan and has been making a significant
contribution to the science operation and data analysis since its
launch. The data acquired with Hinode are released to everyone
as soon as the data are ready for analysis. The Hinode Science
Working Group (SWG), composed of representatives fromthe international teams, offers support in scientific operationand data analysis. It has a total of 17 members, including three
from SOL: Y. Katsukawa as SOT PI, H. Hara as EIS PI, and T.
Sakurai, professor emeritus, as a project scientist. The Science
Schedule Coordinators (SSC) have been organized to leverage
the open-use observation system. Two Japanese members from
SOL (T. Watanabe, professor emeritus, for EIS and T. Sekii
for SOT followed by J. Okamoto in the latter half of the year)
join the SSC activity. The SSC serves as a contact point for
observation proposals from world solar physics researchers touse Hinode and promotes joint observations between Hinodeand the other science satellites and ground-based observatories.
New science results have been obtained via joint observations
with SDO, IRIS, and ALMA as well as long-term standalone
observations by Hinode. The number of Hinode-related
refereed papers published in FY 2022 is about 60. The Hinodescience payload had been steadily observing the Sun fromspace, except for the SOT filtergraph instrument which wasterminated in February 2016. Since March 2022, the spacecraft
operation has continued with the attitude control around theSun-directed axis using a geomagnetic sensor and gyro.
ISAS/JAXA approved the fourth mission extension for theperiod from FY 2021 to FY 2023, and has conducted science

042

II Status Reports of Research Activities

operations to continuously observe rising activity toward
the solar maximum using techniques such as observationsof magnetic fields in the polar regions and full-disk mosaic
observations, as well as to promote joint observations withrocket and balloon experiments conducted by the SOL project.
The JAXA-led Hinode project will be terminated in order tofocus on the next solar mission SOLAR-C, and the results andlessons learned from Hinode will be transferred to SOLAR-C.
After FY 2024, the operation framework will be shifted to one
in which operations will be continued by a late-stage operations
team within ISAS.
Solar Data Archive System (SDAS) in the Astronomy
Data Center (ADC), which developed from the open-use data
analysis system of the Hinode Science Center and NSRO
(Nobeyama Solar Radio Observatory) in addition to the dataarchive/public release system of the former Solar Observatory,
takes the role of archiving and public release of the solar data.
The data analysis functionality has been integrated into the
ADC Multi-wavelength Data Analysis System (MDAS). The
SOL project is jointly operating SDAS and MDAS with ADC.
The SOL project is jointly operating Hinode Science Center at
the Institute for Space-Earth Environmental Research, Nagoya
University, where value-added Hinode data are maintained
and published such as a flare catalog, model of magnetic fields
above active regions, and magnetic field data in the solar polar
regions.

2. Ground-based Observations at Mitaka Campus
The SOL project continues to conduct observations at
Mitaka Campus to obtain basic data for solar research andto help satisfy the public demand for monitoring its possible
influence on the global environment. The primary observations
are infrared spectro-polarimetry for full-disk magnetic fieldmeasurements both in the photosphere at 1.565 microns andin the chromosphere at 1.083 microns with the Solar Flare
Telescope (SFT). The other observations include full-disk
Hα, Ca K, continuum, G-band imaging observations, andrelative sunspot number measurements as a proxy of long-term
solar magnetic activity. The solar activity has been gradually
increasing since 2019 after the solar minimum, and useful datasuch as active regions and flares have been obtained in the newcycle. To ensure stable operation, we are replacing aging partsof the instruments.
Some of the most advanced data accumulated are thosefor magnetic fields in the solar atmosphere. The magnetic
field observations that were conducted with SFT starting from1992 have provided vector magnetic fields in the photospherewith a field of view covering active regions by observing
an absorption line in the visible wavelength range. Theseobservations have now been replaced with near-infrared Stokes
polarimetric observations since 2010 for higher precision
measurements of magnetic fields both in the photosphereand in the chromosphere. In addition, we are developing key
technologies required in future solar observing instruments,
such as an infrared camera with an H2RG detector.
NAOJ has long-term solar observation data in the form offilms, photographic plates, and sketches acquired since the timeof its predecessor, the Tokyo Astronomical Observatory. The
data are being digitized for the study of long-term variations
in solar activity. In particular, the historical data of total solar
eclipses are being digitized intensively. The past and newobservation data are stored in the common server of ADC and
are available on our webpage. In order to promote the use of
the data, we have made the Hα imaging data searchable on the
Virtual Solar Observatory (VSO), a solar data retrieval systemin the US. We are planning to increase the number of data
available on VSO in the future.

3. Nobeyama Solar Radio Polarimeters
The Nobeyama Radio Polarimeters (NoR P) monitor
the microwave radiation from the Sun, specifically at sevenfrequencies (1, 2, 3.75, 9.4, 17, 34, and 80 GHz), and measure its
circular polarization to study solar cycle activity and particle
acceleration phenomena associated with solar flares. Although
the Nobeyama Solar Radio Observatory (NSRO) was closed
at the end of FY 2014, the observation of intensity and circularpolarization at the seven frequencies, conducted over 70 years,
continues because of its importance in monitoring long-term
solar activity. Since FY 2019, the SOL project started to takeresponsibility for the operation and maintenance of the radio
polarimeters in cooperation with Nobeyama Radio Observatory( NRO) and the solar physics community in Japan. The
replacement of critical components since the last fiscal year
has been successful, and stable operation has been maintainedat all frequencies, and multiple radio bursts accompanying
flares have been detected with the increasing solar activity. To
promote the use of NoRP data, we published a paper (Shimojo& Iwai 2023) describing the history of the instrument andobservations over 70 years, especially the evolution of the
instrument since 1994, when observations started at Nobeyama
and the details of the database available at the Solar Data
Archive System.

4. Rocket and Balloon Experiments
T he SOL proje ct is work i ng t o develop a dva nce dtechnology for next-generation solar observations by sounding
rocket and stratospheric balloon experiments.
The CLASP ser ies of sounding rocket exper iments
aims to measure solar magnetic fields in the chromosphereand transition region through high-precision polarization
observations in the ultraviolet wavelengths. The SOL project
has led, in cooperation with research groups in the U.S.
and Europe, CLASP (in 2015, the world’s first successful
spectropolarimetric observation of the hydrogen Lyman alphaline [wavelength: 121.6 nm]), CLASP2 (in 2019, the world’s
first successful spectropolarimetric observation of ionizedmagnesium lines [h&k, wavelength: 280 nm]), and CLASP2
reflight, CLASP2.1, (in 2021, successful scanning observation
using the CLASP2 instrument). In FY 2022, we worked on
scientific outputs that further extend the CLASP2 initial
results, including the detection of the Hanle and magnetooptical effects and the extraction of magnetic field information
along the height by applying an inversion code, and published
two scientific papers and one instrument paper. We havecompleted the calibration of the data acquired by CLASP2.1
in cooperation with the US team, and have started the data
analysis for scientific results.
SUNRISE-3 is the third flight of the international balloon
project Sunrise carrying the 1-meter aperture telescope forsolar observations. in which Germany, Japan, the United States,
and Spain are participating. The SOL project is in chargeof the near-infrared spectro-polarimeter SCIP (Japanese PI:
Katsukawa), which will be installed on SUNRISE-3 and will
simultaneously observe many spectral lines with a resolution
higher than that of the Hinode satellite. These observations
will allow us to observe the three-dimensional magnetic
field structure from the photosphere to the chromosphere andits time evolution and clarify the transport and dissipation
processes of magnetic energies. The balloon gondola, telescope,and instruments were reassembled at the ESRANGE launchsite in Kiruna in April 2022, and final tests for alignment,
image formation performance, etc. were conducted. A timeline
was developed for efficiently coordinating onboard instrumentsin the flight operation. We had a launch opportunity on July
10, delayed one month from the original schedule due to adelay in NASA logistics. However, due to a shock generated
at the launch, a part in the gondola, for which the US teamwas responsible, failed and was unable to point at the Sun.
For the safe recovery of the telescope and the instruments, theoperation was terminated about 5 hours after the release, andthe gondola was descended in Sweden. The SCIP was operated
without any problems during the f light, and post-recovery
tests confirmed that the SCIP was in good health. The resultsof the scan mirror mechanism, high-precision polarization
calibration, and optomechanical design obtained through thedevelopment of SCIP have been published in three refereed
papers in collaboration with the Advanced Technology Center.
Development of onboard image processing and thermal design
have also been drafted in a paper in cooperation with the
Spanish team. In addition, research on methods for analyzing
high-precision polarization data of the chromosphere isongoing.
The Focusing Optics X-ray Solar Imager (FOXSI) is a joint
Japan-US sounding rocket experiment series to observe X-rays
emitted from the solar corona by 2D focusing imaging andspectroscopy. It has successfully flown three times (FOXSI-1
to -3) to make the world’s first observations of the solar corona
during non-flaring periods. Based on these achievements, thefourth flight FOXSI-4 will realize an observation of a solar
f lare. FOXSI-4 is scheduled for launch in Spring 2024 andaims to understand plasma heating, energy transport, andparticle acceleration in a solar flare. The Japanese group led

II Status Reports of Research Activities043

by the project is developing key components such as a highspeed camera for X-rays, a high-precision X-ray mirror, apre-collimator, and an X-ray filter. In FY 2022, these basic
developments were completed, and the fabrication of f light
products was started. These developments are being carriedout in collaboration with ATC and the CMOS camera team of
the Subaru Telescope. The team is also working on the datacalibration of the last three FOXSI experiments as well as on
the creation of scientific results. The FOXSI-4 project wasapproved by NASA with the highest evaluation and, in Japan,
was adopted by ISAS/JAXA as a small-scale program and theGrant-in-Aid for Scientific Research, International Cooperative
Research Acceleration Fund (B). It was newly adopted in
FY 2022 as a Grant-in-Aid for Scientific Research (A). The
Japanese team for FOXSI-4 is led by the National Astronomical
Observatory of Japan (PI: Narukage), with the participation of
the University of Tokyo Kavli IPMU, ISAS/JAXA, and Nagoya
University. Many graduate students are also participating in
the FOXSI-4 project, contributing to the development of young
researchers.

5. Cooperation with SOLAR-C ProjectIn the preliminary design of EUVST, a high-resolution,
high-sensitivity UV telescope to be installed on the next solar
observing satellite SOLAR-C, the SOL project contributes torealizing SOLAR-C by maximum use of the technical expertisein the optomechanical design, UV observation technology, andIF coordination with overseas institutions accumulated throughthe development of the rocket and balloon experiments. To
refine the observation plan for SOLAR-C, we are conducting
research on how the key processes of atmospheric heating are
observed spectroscopically using numerical simulations etc. in
the framework of the Hinode Science Center, which is jointly
operated with Nagoya University.

6. Education
The SOL project accepted and supervised four Ph.D.
students from SOKENDAI and two contract graduate students
from the University of Tokyo. Two received a master’s degree
at SOKENDAI or the University of Tokyo. The SOL project
participated in the Tour of Solar Research Frontiers (March
2023) and introduced solar research at NAOJ to undergraduate
students.

7. Public Outreach (PO) Activity
The SOL project has been conducting various public
outreach activities for education and delivering the latest
solar activity and the results obtained through the scientificresearch of the Sun to the public: web releases, homepage,social media, cooperation for exhibitions at science museums,
media appearances for solar observations and space weather in
response to requests for media interviews, providing materials
to the media, etc.

044

II Status Reports of Research Activities

8. Science and Community Meetings
The international Hinode Science Meetings have been
regularly held to advance solar physics research with the
Hinode satellite. The 15th Hinode Science Meeting washeld September 19–23, 2022 in Prague, Czech Republic. A
meeting of the Hinode Science Working Group was held on
September 23, 2022, to discuss ways to continuously generatescientific results from Hinode and to share the status of mission
extension in participating countries. The Japan Solar Physics
Community Symposium was held February 20–22, 2023 at
Nagoya University, where the latest research results fromdomestic instruments and foreign space- and ground-based
observations were presented, and future plans for SOLAR-C
and beyond were introduced and discussed.

9. Others
For the Daniel K. Inouye Solar Telescope (DKIST) on
Haleakala in Hawai`i, a 4-meter aperture solar telescope led by
the US, one person from SOL (Y. Katsukawa) is a member of
the Science Working Group. In the second call for observation
proposals for DKIST (Operation Commissioning Phase 2,
OCP2) issued in 2022, three proposals submitted by Japanese
researchers were accepted and two of them are from the NAOJ
researchers. Based on a grant for enhancing collaborative
research with DKIST (co-I: M. Kubo), we are conducting
research using the dat a t aken in OCP1 and nu mer ical
simulation studies assuming future DKIST observation data.
For the European Solar Telescope (EST, 4 m) the SOL project
participated in the SOLARNET project of the European solar
community to develop an image slicer for IFU (Integral Field
Unit) for the EST-prototype GREGOR solar telescope. In
the next-generation global network solar observation project(ngGONG), which is led by NSO in the US, the SOL project
has expressed our intention to cooperate with NSO for its
realization based on the scientific and technological heritage
obtained through near-infrared spectro-polarimetry with SFT
at Mitaka Campus. We helped prepare a white paper aboutngGONG submitted to the Heliophysics Decadal Survey in the
US. The 10 cm coronagraph from the former Norikura Corona
Observatory has been relocated to Yunnan, China, and its
observation operations are underway at the site. Discussions
have begun with the Chinese group regarding future scientificcooperation using the coronagraph data.

04. Subaru Telescope
1. Subaru Telescope Staff
As of the end of FY 2022, the Subaru Telescope staff
consisted of 21 dedicated faculty members including fivestationed at Mitaka and two stationed at Okayama, fiveengineers, one specially appointed associate professor, foursenior specialist, and three administrative staff members.
Additional staff members include one specially appointed
assistant professor, six project research staff members, eight
senior specialist, six administration associates, and one researchsupporter, all of whom are stationed at Mitaka; as well as one
specially appointed associate professor, and two administration
associates, all of whom are stationed at Okayama. Moreover, 12
research/teaching staff members, seven of whom are stationed
at Mitaka and two of whom are stationed at Pasadena, and three
engineers, one of whom is stationed at Mitaka, one of whomis stationed at Nobeyama, and one of whom is stationed at
Mizusawa, are posted concurrently. The project also has 61 local
staff members dispatched from the Research Corporation of the
University of Hawai`i (RCUH), including scientific assistants;
engineers in charge of software and observational instruments;
technicians for facilities, machinery, vehicles, and laboratories;
telescope/instrument operators; administrative staff; researchers
employed for Grants-in-Aid for Scientific Research; PostDoctoral fellows; and graduate students. These staff members
work together in operating the telescope, observational
instruments, and observational facilities; and in conducting
open-use observations, R&D, public outreach, and educational
activities.

2. Science Highlights
In FY 2022, Subaru Telescope produced many outstanding
scientific outcomes, which were published in major international
journals. Below are some examples:(1) A brown dwarf orbiting the Sun-like star HIP 21152 was
discovered using the Extreme Adaptive Optics System (SCExAO
and CHARIS). HIP 21152 B was found to be the lightest browndwarf with an accurately determined mass, approaching the massof a giant planet. HIP 21152 B is expected to be a benchmark
object for the study of the evolution of giant planets and browndwarfs and their atmospheres.
(2) A massive supercluster of galaxies about 5.5 billion lightyears away was discovered based on the Hyper Suprime-Cam
data taken under the Subaru Strategic Program. Not only is therea strong concentration of galaxies and dark matter across anarea of the sky roughly the size of 15 full moons, but there are atleast 19 galaxy clusters associated with it, making it the largest
supercluster ever identified in the Universe beyond 5 billion
light years away.

(3) Hyper Suprime-Cam with Big Data techniques has made it
possible to search wide areas, looking for transient phenomena
which change rapidly with time. Astronomers discovered
20 fast-evolving transients in December 2020. One of them,
MUSSES2020J was very dim in the first images but brightened
significantly over the course of the observations, indicatingthat the team caught it at the very beginning of its occurrence.
Follow-up observations confirmed that this event evolved much
faster than normal supernovae and was about 50 times brighter.
The team proposes calling this new class of events “Fast Blue
Ultraluminous Transients” (FBUT).
(4) Using observations with Hyper Suprime-Cam, a giant tidal
tail has been discovered emanating from a dwarf galaxy in
the nearby M81 galaxy group. The galaxy, named F8D1, isremarkable on account of its low luminosity and large size andis now recognized to be one of the closest examples of an “ultradiffuse” galaxy (UDG). This is the first time that such a stellar
stream has been discovered in a UDG. Revealing F8D1 to be agalaxy in an advanced state of tidal disruption has implications
for both the dynamical evolution of the M81 Group and for theorigin of galaxies that exhibit UDG properties.
(5) An exoplanet was discovered by the Subaru Strategic
Program using the infrared spectrograph IRD (IRD-SSP). Thisis the first discovery based on IRD-SSP. This planet, Ross 508b,
is a super-Earth with about four times the mass of the Earth andis located near the habitable zone. Such a planet may be able
to retain water on its surface. It will be an important target for
future observations to verify the possibility of life around lowmass stars.

3. Open-use
The Open Use Program is conducted semiannually byinviting proposals from the public. The observation period
is from February 1 to July 31 (semester A) for the year's first
half, and from August 1 to January 31 (semester B) for the
year's second half. Applications are accepted at the Subaru
Mitaka Office of the National Astronomical Observatory ofJapan. The Subaru Program Time Allocation Committee (TAC)
reviews the proposals and selects which ones to accept basedon domestic and international referee evaluations. In S22A, 46
proposals (65.5 nights including 1 ToO proposal night) {out of
132 proposals (256.56 nights)} were accepted. And in S22B, 35
proposals (46 nights including 2.0 ToO proposals nights) {outof 129 proposals (246.02 nights)} were accepted. For Intensive
Proposals exceeding one semester, we allocated 22.5 nights (4proposals) in S22A and 17.4 nights (4 proposals) in S22B. In
addition, short-time assignment Service Program observations,were also conducted. Of the proposals selected for Open Use in
S22A and S22B (excluding University of Hawai`i time), three(two in S22A and one in S22B) were foreign PI proposals. The

II Status Reports of Research Activities

045total number of applicants, including co-researchers, was 884
foreign researchers compared to 2,256 domestic applicants, andthe total number of researchers in the accepted proposals was
265 foreign researchers compared to 749 domestic researchers.
The total number of Open Use observers in S22A and S22B
was 334 (including 103 foreign and 130 remote observers in
Mitaka Campus). The Mitaka side handled the application
and review of observation proposals, travel procedures fordomestic researchers to observe, and travel expense payment
administration, while the Hawai`i side prepared the observation
schedule and provided support for observers' accommodation,transportation, and observations in Hawai`i. Open Use
observations during S22A and S22B, including University of
Hawai`i time, utilized 91.85 % of available observation time,
excluding weather factors and scheduled downtime due tomaintenance such as the primary mirror coating. About 2.41 %of the observing time was lost due to instrument trouble, 0.29 %due to communications system trouble, 5.27 % due to telescopetrouble, and 0.18 % due to operation trouble.
Remote observations from the Hilo base facility were madeon 16 nights (12 programs) during S22A and S22B. Remoteobservations from NAOJ Mitaka Campus were conducted for
40 nights (20 proposals including HSC/IRD Subaru Strategic
Programs) with the participation of both summit observers andremote side observers, or only Mitaka remote side observers.
In addition, 6.5 nights of service observations were conducted.
Telescope time exchanges with Gemini and W. M. Keckobservatories are conducted to make the best use of the telescope
resources at the summit of Maunakea. Subaru Telescope andW. M. Keck Observatory exchanged 5.5 nights in S22A and 4.5nights in S22B. Subaru Telescope users were able to use Geminifor 11.0 nights in S22A and 2.1 nights in S22B (excluding FastTrack proposals), and from Gemini users were able to use theSubaru Telescope for 13.1 nights in S22A and 5.4 nights in
S22B.

4. Telescope Maintenance and Performance
Improvement
The following major repairs, maintenance, and changes were
implemented in FY 2022.
(1) Primary mirror recoating:
The recoating work for the telescope primary mirror was
performed to recovery the reflectivity of the primary mirror.
(2) Other activities:
We are accepting new observational instruments, repairing
the outer wall of the dome, performing annual maintenance ofthe mechanical and electrical systems of the telescope / dome,
and repairing sudden failures.
In addition, we have been working on the renewal of thedome air conditioning system and an upgrade of the telescope
software to improve observation efficiency.
The other hand, we started the “Telescope MaintenanceGroup collaboration of NAOJ”. The purpose of this activity is to046

II Status Reports of Research Activities

share know-how and maintenance plans for NAOJ telescopes,
and to carry out, evaluate, and improve maintenance activities
through cooperation among observatories.

5. Instrumentation
The following five facility instruments were provided forthe open-use observations in FY 2022: HSC (Hyper SuprimeCam), FOCAS (Faint Object Camera And Spectrograph),
HDS (High Dispersion Spectrograph), IRCS (Infrared
Camera and Spectrograph), MOIRCS (Multi-Object Infrared
Camera and Spectrograph), and the 188-elements Adaptive
Optics and Laser Guide Star system (AO188/LGS). As forthe carry-in instruments, IRD (Infrared Doppler), SCExAO(Subaru Coronagraphic Extreme Adaptive Optics), andSWIMS (Simultaneous-color Wide-field Infrared Multi-object
Spectrograph) were provided for the open-use observations.
In addition, the following instruments/devices have been usedin combination with SCExAO: CHARIS (Coronagraphic
High Angular Resolution Imaging Spectrograph), FastPDI(Fast Near-Infrared Polarization Differential Imaging), MEC(MKID Exoplanet Camera), REACH (Rigorous Exoplanetary
Atmosphere Characterization with High dispersion
coronagraphy), and VAMPIRES (Visible Aperture Masking
Polarimetric Imager for Resolved Exoplanetary Structures).
The operation of MOIRCS was resumed in January 2023,
after its hibernation since February 2021 to facilitate the science
operation of the carry-in instrument SWIMS. MOIRCS was
successfully recovered in January 2023 and offered for openuse observations from February 2023. The upgrade of the LGS
system was mostly completed and it was opened for open-use
observation from February 2023.
The upgrade projects of the Deformable Mirror (DM) and
Near Infrarred Wavefront Sensor (NIRWFS) for AO188 havebeen actively underway. NIRWFS is planned to be operated asa carry-in device, has successfully done multiple engineeringobservations, and is under preparation to be made available in
S24A. For HSC, fabrication of new filters by HSC users is stillongoing and we received and made available a narrow-band
filter “NB872” in FY 2021. In addition, a project to fabricate~20 intermediate-band filters is ongoing. For the Nasmyth Beam
Switcher, which will improve the operation and management of
IR Nasmyth instruments, we completed the procurements of the
optical and mechanical parts, and started the assembly work.

6. Computers and Networks
The Subaru Telescope computing and network systems
core system remained mostly stable with occasional network
issues due to an increased number of powerline events affecting
both the Base and Summit facilities. CDM (Computer and DataManagement division) has worked to mitigate observing timeloss due to network issues by deploying a backup VPN between
the Summit and Hilo. CDM continues to support day workers
with computing requests, and work to implement changes to thecomputing/network environment if it benefits Subaru staff, anddoesn’t compromise the integrity of the STN environment.
As major improvements CDM has finalized the STN6
(Subaru Telescope Network version 6) contract, prepared thecurrent STN5 contract equipment for removal, and converted
all physical servers and virtual machines services to updated
operating systems. This work is necessary to allow for asmoother and faster transition between contract systems. The
highlight of the new STN6 system is a decreased footprint fromthirty (30) servers/storage devices in four (4) full rack enclosuresto twelve (12) servers/storage/network devices in one half-sized
rack at the Base Facility, with a reduction of a one (1) full rack
to one half-sized rack at the summit. CDM has planned, tested
and transitioned the contract network equipment of a single
chassis environment, to a modular environment, reducing the
network footprint, and improving the recovery time in case ofcomponent failure to minimize the observing time loss. With
guidance from Mitaka ITSO (Information Technology Security
Office), the 100 G Hi-speed Summit-Base-Mitaka network was
established and tested during HSC observations. Further normal
Hilo-Mitaka network traffic, Accounting, STARS, phones, and
ADC related traffic were added to this network. As of the endof FY 2022, utilization of the 100 G network is increasing,with support for large data transmissions for other instruments.
With the new network equipment supporting 25, 40, and 100
Gbps connections, CDM has invested in upgrading parts of new
and existing server environments. OCS (Observation Control
System) -GEN2 base and summit clusters have been upgraded to
80 Gbps core uplink, with redundant failover for servers. Current
PFS and HSC Onsite Analysis server clusters have specificservers with 40 or 100 G connections to allow for maximum

data transmission to support observation. CDM still participatesin the Astronomical Community specifically to network andcollaborate on large data transfer projects. Other highlights
include the transfer of 400 TB of observation data and logs
(STARS) from STN5 to the new storage server. This includes,
validating the data using checksum and updating the database toensure the proper storage location is recorded.

7. Education (Under-graduate and Graduate Courses)
In FY 2022, Subaru Telescope had 15 staff members
jointly affiliated to SOKENDAI. Some of these staff members(including those jointly affiliated to other divisions) are theprimary supervisors of eleven students, which comprise 1/3of all the SOKENDAI students. Among these 11 students, 5
are supervised by staff members primarily affiliated to Subaru
Telescope.
Subaru Telescope hosted 4 students through the Akamai
internship program. Separately from the Akamai program,
Subaru Telescope hosted 1 intern student. As part of the
SOKENDAI summer student program, staff members in Hiloand Mitaka supervised 7 undergraduate students.
Turning to Subaru Telescope’s contributions to the larger
Japanese community, 5/16 graduate students defended their
PhD/Master’s theses using data from the Subaru Telescope.
Among them, one SOKENDAI student affiliated to Subaru
Telescope defended his PhD thesis. The HSC data reduction
school was held in Mitaka in an onsite+online format and 33
people participated in the school, of which 11 also joined thehands-on data reduction session.

Subaru Telescope Okayama Branch
The Okayama Branch was established in FY 2018 primarily
to provide open-use observing time to universities nationwide
utilizing half of the observation time of the 3.8-meter New
Technology Optical-Infrared Telescope (now named as“Seimei Telescope”) at Okayama Observatory, Astronomical
Observatory, Graduate School of Science, Kyoto University.
It also cooperates in the use of the telescopes of the former
Okayama Astrophysical Observatory by universities and the
local government. Two research and academic staff members,
one project associate professor, and two administrative
supporters belong to the Okayama Branch as of the end of FY
2022.

1. Seimei Telescope(1) Open use (calendar year)
In the first half of 2022 (January-June), 70 nights were
provided. The number of applications was 22 (Classical: 11,
Classical + ToO: 1, ToO: 10) and the number of nights requested
was 93.37 (Classical: 65.1, ToO: 28.27), while the numberof accepted applications was 19 (8, 1, 10) and the number ofawarded nights was 83.27 (58, 25.27). Note that “Classical”
refers to an observation that will be made on a pre-assigned date,and “ToO” refers to an observation that will be made upon theoccurrence of an event of interest at a date and time indicated by
the proposer. The total lost time during this period was 3.0 night.
In the second half of 2022 (August-December) 63.5 nights were
provided. The number of applications was 29 (13, 3, 13) and thenumber of nights requested was 125.995 (83.9, 28.133), while
the number of accepted applications was 19 (9, 2, 11) and thenumber of awarded nights was 84.333 (56.2, 28.133). Total losttime during this period was 1.75 nights. During these periods,
we provided accommodations for observers to stay onsite while
taking appropriate measures to prevent the spread of novel
coronavirus infections, and we carried out the open use withoutcausing any infection clusters.
(2) Observing instruments
In 2022, the Kyoto-Okayama Optical Low-dispersion
Spectrograph with the optical-fiber Integral Field Unit (KOOLS-II Status Reports of Research Activities

047IFU) and the TriColor CMOS Camera and Spectrograph(TriCCS), which had been opened in 2021, were available.
In the second half of 2022, the fast-imaging mode (10 to 98fps) of TriCCS was newly available. Activities also included
management and operation of environmental monitors, storageof acquired data, maintenance of computers and networks, andmaintenance of facilities. Development and test observationof a high-dispersion spectrograph for precision radial velocity
measurement (GAOES-RV), which is expected to become a newobservatory instrument, were carried out.
(3) Development of remote and queue observations
In cooperation with Okayama Observatory of Kyoto
University, the remote observation environment wasconditionally opened to open use in the first half of 2022.
Development of the queue observation system was started in2022.

of 2023. At the subcommittee meeting held in February 2023,
the new instrument GAOES-RV was reviewed for open use in
the second half of 2023, and it was accepted.
(c) Kyoto University 3.8-m Telescope Council
On September 16, 2022, the fifth meeting of the Kyoto
University 3.8-m Telescope Council regarding the operation of
the Seimei Telescope was held online by the Kyoto University
Graduate School of Science and the National Astronomical
Observatory of Japan (NAOJ). The meeting was attended by the
Dean of the Graduate School of Science, Kyoto University, theDirector General of NAOJ, and many others. The status of theoperation was reviewed, and research results were reported.

2. Telescopes of the former Okayama
Astrophysical Observatory(1) 188-cm reflecting telescope(4) Research results
The following example of important research results fromobservations with the Seimei Telescope was published in a paper
in FY 2022.
(a) Observations of nearby (redshift z < 0.04) ultra-luminous
infrared galaxies (ULIRG) at various stages of galaxy mergers
were made using the KOOLS-IFU at the Seimei Telescope.
Emission lines such as Hβ, [O III ]λ5007, Hβ, [N II ]λλ6549,
6583, [S II]λλ6717, 6731, etc. were observed with a wavelength
resolution of R = 1500 to 2000. These observations yielded
spatially resolved (approximately 200 to 700 pc) moment mapsof the ionized gas of each galaxy and allowed the diagnosisof active galactic nuclei (AGN) within the central ~3–11 kpc
diameter of the sample. The outflow of the [O III] emission
line driven by an AGN tends to be stronger (i) towards thegalactic center and (ii) with the merging stage. In particular,
the outflow strength in the late-stage mergers is about 1.5 times
stronger than that in the early-state mergers, which indicates thatgalaxy mergers could induce AGN-driven outflows and play animportant role in the co-evolution of galaxies and supermassive
black holes.
(5) Meetings(a) Seimei Users Meeting
The fourth Users’ Meeting was held online on July 26–27,
2022. Meeting Managers: Masaaki Otsuka, (Kyoto Univ.)(Representative), Mikio Kurita (Kyoto Univ.), Akito Tajitsu(NAOJ), Masayuki Akiyama (Tohoku Univ.), Shigeyuki Sako
(Univ. Tokyo), Satoshi Honda (Univ. Hyogo). The maximum
number of simultaneous connections was about 80, and the total
number of participants was about 100.
(b) Seimei Subcommittee
The Subcommittee met eight times in FY 2022. Four ofthese meetings were for the time allocation to the open use
observing proposals for the second half of 2022 and the first half048

II Status Reports of Research Activities(a) On August 10, 2022, the operational council meeting todiscuss the use of the 188-cm reflector telescope was held online
by NAOJ, the Exoplanet Observation Research Center at the
School of Science of the Tokyo Institute of Technology (TITech),and Asakuchi City.
(b) On the evening of September 29, 2022, when observers
using the 188-cm telescope tried to open the dome slit for theirobservation, the upper door of the dome slit, which is a vertical
type, fell down and became inoperable. Due to this accident, the188-cm telescope became unusable and remained in that state
until the end of the fiscal year (as of May 2023, discussions areunderway for restoration).
(c) On March 16, 2023, the operation council was held at
Asakuchi City Hall as a hybrid of face-to-face and online. A
discussion was held on the use of the 188-cm reflector telescope,explanation of the situation of the dome accident, and recovery.
(2) Other telescopes
We also cooperated in the operation of the 91-cm reflector
telescope, the 50-cm reflector telescope (MITSuME), and theThirty Milli-Meter Telescope (TMMT).

3. Public Outreach
The Okayama Branch has no staff assigned to public
relations and dissemination activities, so only the minimum
necessary activities are carried out.
(1) In 2022, we started holding television stargazing eventsusing the Seimei Telescope: June 2022 from Asakuchi City,
September from the children's astronomical club at the Asakuchi
City Okayama Astronomical Museum, and in December from
Yakage Town. Each time about 30 people were invited to test
the stargazing party. In March 2023, the Okayama Astronomical
Museum held the first telescopic stargazing event for publicparticipants (approximately 20 people) with the cooperation of
Kyoto University and NAOJ.
(2) In November 2022, the first “Asakuchi Observatory Festa”
was held with the cooperation of the Asakuchi City Okayama
Astronomical Museum and the Kyoto University Okayama
Observatory.

II Status Reports of Research Activities049

05. Center for Computational Astrophysics (CfCA)
1. Overview
The Center for Computational Astrophysics (CfCA) has
been operating a system of open-use computers for simulations
centered around a general-purpose supercomputer, a generalpurpose graphic processing unit (GPGPU) cluster, and a generalpurpose PC cluster for small-scale calculations, carrying out
research and development of computational astrophysics, andperforming astronomical research with simulations. The newmain supercomputer of the present system renewed in 2018,
ATERUI II (Cray XC50), has a theoretical peak performanceof 3 Pflops, which is the world's fastest supercomputer for
astronomy. CfCA augmented the GPGPU cluster and generalpurpose PC cluster in 2022. Efforts in visualizing astronomical
data also continue.

2. Open Use of Computers(1) General status
This year marked the fifth year of the upgraded astronomical
simulation system, which includes the new open-use
supercomputer Cray XC50. This computer is installed and underoperation at Mizusawa VLBI Observatory. The users have been
making academically significant progress as before.
While XC50 is leased for six years from Hewlett-Packard
Enterprise (which acquired Cray), the center has built thefollowing equipment to aid the open-use computer operations:a series of GPU nodes; two sets of PC clusters for small to
medium-scale computation; large-scale file servers; a groupof servers for processing computational output data; and an
instrument network to encompass the overall computer system.
These components are central to numerical simulations byresearchers in Japan and overseas.
Computational resources of the XC50, GPU, and the PC
clusters are allocated in accordance with a formal review
process. The statistics of applications and approvals for this year
are listed in the next subsection. Our center conducted a survey
on the number of peer-reviewed papers published in English
in this fiscal year on studies that involved the project's openuse computers. It turned out that 156 refereed papers (written in
English) were published in this fiscal year.
The center uses Drupal, a content management system
introduced for data exchange with users of open-use computers.
The acceptance of various applications and the management of
the users’ personal information are all handled through Drupal.
The regular CfCA News is an additional channel of information
dissemination. The center leverages this newsletter to inform
people of all useful and necessary information regarding
the computer system. A subsidy system for publishing andadvertising is continuing this year for research papers whose
major results were obtained by using the center's computers.
(2) Operation stats for each of the facilities

050

II Status Reports of Research Activities

Cray XC50• Operating hours
Annual operating hours: 8357.9
Annual core operation ratio by users' PBS jobs: 95.41 %• Number of users
Category S: 0 adopted in the first term, 0 in the second term;
total 0Category A: 15 adopted at the beginning of the year, 0 in thesecond term; total 15
Category B+: 19 adopted at the beginning of the year, 1 in thesecond term; total 20
Category B: 132 adopted at the beginning of the year, 13 in
the second term; total 145
Category MD: 30 adopted at the beginning of the year, 1 in thesecond term; total 31
Category Trial: 28 (year total)
GPU system• Number of users
25 (at the end of the fiscal year)
General-Purpose PC farm
• Operating hours
Annual operating hours: 8688 (a ballpark figure)Total number of submitted PBS jobs: 1331769
Annual core operation ratio by users' PBS jobs: 98 % (aballpark figure)• Number of users
69 (at the end of the fiscal year)(3) Tutorials and Users Meeting
The center organized various lectures and workshops
to provide the users of the open-use computer system witheducational and promotional opportunities, as well as to train
young researchers. The details are shown below. In addition,
the CfCA Users Meeting was held to serve as a forum for direct
information exchange. Many participated in the meeting, anddiscussions were fruitful.
• Tutorial sessions for iSALE (WebEx + Slack)
Lecture and hands-on training on the basics of the iSALE
shock physics code
June 17 - July 15, 2022
10 attendees (+ 2 Associate Professors [Senior Lecturers] fromoutside NAOJ)• Cray XC50 workshop for novice users (zoom)
Introduction to the basic usage of XC50 for novice users
August 22, 2022
12 attendees• Cray XC50 workshop for intermediate users (zoom)
Introduction to debugging, performance analysis, andoptimization of XC50 for intermediate users
August 23, 2022
10 attendees• CfCA Users' Meeting (Onsite + zoom + Slack)
Presentation of research results using the open-use facilities

in this department, and discussion of the operation of theequipment
January 26–27, 2023
January 26: 44 attendees (Onsite) + 62 (Online),
January 27: 36 attendees (Onsite) + 66 attendees (Online)• Early spring school for N-body numerical simulations (zoom +Slack)
Lectures on N-body simulations, and programming practiceusing GPU and GRAPE-Library
February 6–9, 2023
14 attendees (for hands-on training and lectures), 1 attendees(for lectures only)• GPU Workshop1 (zoom + Slack)
Lectures on CUDA programming basics and introduction ofSingularity container
June 29, 2022
19 attendees• GPU Workshop2 (zoom + Slack)
Implementation of fluid dynamics calculations and N-bodysimulations
January 17, 2023
26 attendees• Numerical simulation school for hydrodynamics (Onsite +zoom + Slack)
Lectures on numerical magnetohydrodynamics and practicefor MHD numerical simulations
February 20–23, 2023
15 attendees (Onsite) + 29 attendees (Online)

3. PR Activity
In FY 2022, the following press releases were issued fromthe center:• “Massive Stars Moving around in Star Clusters”
June 8, 2022, Michiko S. Fujii (The University of Tokyo), Kohei
Hattori (NAOJ/the Institute of Statistical Mathematics) et al.
• “Artificial Intelligence Solves the Mysteries of the Universe”
July 21, 2022, Yosuke Kobayashi (The University of Arizona),
Takahiro Nishimichi (Kyoto University) et al.
• “Is Over-Eating to Blame for Bulges in Milky Way Bar?”
September 9, 2022, Junichi Baba (NAOJ)• “Rare Earth Element Synthesis Confirmed in Neutron Star
Mergers”
October 27, 2022, Nanae Domoto, Masaomi Tanaka (Tohoku
University) et al.
• “Gold-rich Stars Came from Ancient Galaxies”
November 14, 2022, Yutaka Hirai (Tohoku University/ theUniversity of Notre Dame) et al.
In addition, the following research results and news
appeared on the CfCA website in Japanese only:• “Chaotic Motions of Jupiter and Saturn are Key to theFormation of the Terrestrial Planets”
March 29, 2023, Patryk Sofia Lykawka (Kindai University),
Takashi Ito (CfCA)
CfCA organized the following three events at the Iwate
Galaxy Festa 2022, which was held from August 20 to 28, 2022.

• “Supercomputer “ATERUI II” Online Tour”
August 27, 2022, Navigator: Tomoya Takiwaki (CfCA), Livestreaming on YouTube.
• Public Lecture “Light and Shadow of a Black Hole Exploredby Simulation”
August 27, 2022, Speaker: Tomohisa Kawashima (ICRR/
UTokyo), Live streaming of the on-site event (Oshu Space
Museum Seminar Room) on YouTube.
• CfCA Research Poster Exhibition and Visualization Video
Screening
August 20–28, 2022, at Oshu Space Museum Seminar Room.
On October 29, 2022, the Mitaka Open House Day 2022 washeld, and two videos were premiered on the YouTube channel incollaboration with 4D2U. (See “4. 4D2U Project”)
A Twitter account @CfCA_NAOJ and YouTube channel
have been operated to provide the information on CfCA.

4. 4D2U ProjectIn FY 2022, the 4D2U project continued to develop andprovide movie content and software.
The following simulation visualization videos were madeavailable.
• “Massive Stars Moving around in Star Clusters”
June 9, 2022, simulation: Michiko S. Fujii (The University ofTokyo), visualization: Takaaki Takeda (NAOJ), visualized forpress release.
• “Is Over-Eating to Blame for Bulges in Milky Way Bar?”
September 9, 2022, simulation: Junichi Baba (NAOJ),
visualization: Hirotaka Nakayama, visualized for press release.
• “Gas Disk around a Black Hole”
January 31, 2023, simulation: Hiroyuki R. Takahashi(Komazawa University) and Ken Ohsuga (University ofTsukuba), visualization: Hirotaka Nakayama, released flat,
fulldome, VR versions as 4D2U movie contents.
• “Formation of a Multiple-Star System”
March 9, 2023, simulation: Tomoaki Matsumoto (Hosei
University), visualization: Hirotaka Nakayama, released
fulldome and VR versions as 4D2U movie contents.
In addition, we continued development of the fourdimensional digital universe viewer “Mitaka” and released thefollowing versions.
• Version 1.7.3
July 6, 2022, This version includes an enhanced planetarium
mode and improved reproduction of planetary visibility andlunar eclipses.
• Version 1.7.4
February 28, 2023, This version adds features such as thedisplay of terrestrial scenery in planetarium mode and theability to specify constellation and asterism lines in three
dimensions.
4D2U contents were provided both domestically andinternationally for TV programs, planetarium programs, lecture
presentations, books, and so on.
For the Mitaka Open House Day 2022, the following
Japanese videos were premiered on YouTube as a joint project

II Status Reports of Research Activities

051

with CfCA.
• 4D2U video introduction by researchers “Asteroid Collisions
and Shape Evolution”
Speaker: Keisuke Sugiura (ELSI, Tokyo Institute ofTechnology), Satoki Hasegawa (4D2U)• Mitaka introductory video, “A 'special' space tour by the
Mitaka developer (part 2): Visualization of the Milky Way”
Speaker: Tsunehiko Kato (4D2U)
In addition, we exhibited at the following events:• “Innovation Japan 2022”
October 4–31, 2022, A visualization technology developed
by Hirotaka Nakayama, “CG rendering method for stressfree stereoscopic viewing on an omnidirectional 3D display,”
exhibited online.
• “Kashiwanoha Innovation Fes 2022”
October 29–30, 2022, Mitaka demonstrations by Satomi Hatano
and Tsunehiko Kato. Held at Kashiwanoha Conference Center.
A Twitter account @4d2u and YouTube channel have been
operated to provide information on 4D2U.

5. External Activities(1) Joint Institute for Computational Fundamental Science
The Joint Institute for Computational Fundamental
Science (JICFuS) is an inter-organizational instituteestablished in February 2009 as a collaboration base between
three organizations including the Center for Computational
Sciences (CCS) of the University of Tsukuba; the High Energy
Accelerator Research Organization, known as KEK; and NAOJ
to provide active support for computational scientific research.
This organization continues to expand: 8 institutions joinedin 2016, and 13 institutions in 2020. CfCA forms the core of
NAOJ’s contribution to JICFuS. In particular, the instituteengages primarily in computer-aided theoretical research into
the fundamental physics in elementary particle physics, nuclear
physics, astrophysics, and planetary science. The scientific goalof the institute is to promote fundamental research based oncomputational science to encourage interdisciplinary research
between these fields. In addition to its ability as a single
organization, a major feature of the institute is the cooperationof each community to provide considerate and rigorous support
to present and future researchers. Another important mission of
the institute is to provide researchers around Japan with advice
regarding efficient supercomputer use and the developmentof novel algorithms for high-performance computing to meet
research goals from the perspective of computer specialists. In
addition, JICFuS was chosen as the organization responsible
for “Priority Issue 9 to be Tackled by Using the Post-K
Computer” in FY 2014. From FY 2020, JICFuS performs
two new programs: Programs for Promoting Research on the
Supercomputer Fugaku. One is “Simulation for basic science:from fundamental laws of particles to creation of nuclei” and theother is “Toward a unified view of the Universe: from large scale
structures to planets.” CfCA mainly joins the second one.
This year, Eiichiro Kokubo conducted research on“Accumulation of Microplanets and Planet Formation in

052

II Status Reports of Research Activities

Protoplanetary Disks” using N-body and SPH codes. Kazunari
Iwasaki conducted research on “Formation of molecular
clouds and molecular cloud cores in the Milky Way and global
magnetohydrodynamic simulation considering solid particles
in protoplanetary disks” using a mesh-type fluid code. Mami
Machida conducted research on “black hole accretion disks andrelativistic jets,” and Tomoya Takiwaki conducted research on“Elucidation of the mechanism of 3D supernova explosions by
first-principles calculations of neutrino radiation transport,” bothusing a mesh-type fluid code. These four projects are still in theprocess of tuning the code in preparation for the large scale run
on Fugaku. In addition, the budget was used to buy GPUs andincrease the storage capacity in order to analyze and store thehuge amount of data that will be generated in future large-scalecalculations.
Representing CfCA, Professor Eiichiro Kokubo and
Associate Professor Tomoya Takiwaki of NAOJ participate
in bimonthly JICFuS steering committee meetings to engage
in deliberations on spurring computational-science-based
developments in astrophysics research through discussions
with other committee members who specialize in nuclear andelementary particle physics.
(2) HPCI Consortium
As a participant in the government-led High-Performance
Computing Infrastructure (HPCI) project since its planning stage
in FY 2010, the center has engaged in the promotion of the HPC
research field in Japan, centering on the use of the national “K”
and “Fugaku” supercomputers. Note that although the center isinvolved with the activity at JICFuS mentioned in Section 5.1,
the activity in the HPCI consortium is basically independent
from it. The HPCI consortium is an incorporated association
established in April 2012, and the center is currently an associate
member that is able to express views, obtain information, andobserve overall trends in the planning, although we are devoid ofvoting rights as well as the obligation to pay membership fees.
Continuing from last year, a number of conferences and WG’shave been held where participants discussed a next-generation
national supercomputing framework. The national HPC flagshipsupercomputer, “Fugaku,” has already been put into full-scaleservice, and there is much scientific discussion on how the user
community should make the best use of this equipment.

6. Staff Transfers(1) Staff members hired in this FY
Project Research Staff: Ideguchi, Shinsuke
Project Research Staff: Nozawa, Takaya
Project Research Staff: Keszthelyi, Zsolt
Research Supporter: Kimura, Chie
(2) Staff members who departed in this FY
Senior Specialist: Kato, Tsunehiko
Project Research Staff: Taki, Tetsuo
Project Research Staff: Nozawa, Takaya
Research Supporter: Ideguchi, Shinsuke

06. ALMA Project, NAOJ Chile, and ASTE Project
The ALMA project is a global partnership of East Asia (ledby Japan), Europe, and North America (led by the United States)in cooperation with the Republic of Chile to operate a gigantic
millimeter/submillimeter radio telescope deploying 66 highprecision parabolic antennas in the 5000-m altitude Atacama
highlands in northern Chile. ALMA achieves a spatial resolution
nearly ten times higher than that of the Subaru Telescope andthe Hubble Space Telescope. Early scientific observations with
ALMA began in FY 2011 with a partial number of antennas andfull operation commenced in FY 2012. The 10th anniversary of
the start of full operation was held in FY 2022, with a formal
ceremony at the ALMA site and participation from all theregions, local authorities, and local communities. The ALMA
2 project will start from FY 2023. By continuing scientificobservations and upgrading its observational capabilities, ALMA
will continue to lead world astronomy in the coming decade.
This report describes the progress of the ALMA project, which
includes the results of the open-use scientific observations andpublic outreach activities.
The ASTE telescope is a single-dish 10-m submillimetertelescope located at Pampa la Bola in the Atacama highlands
where ALMA is also located. It has been operated in theSouthern Hemisphere to make headway into submillimeter
astronomy that explores the spectrum invisible to the human eye,providing various possibilities and future prospects for researchand development of ALMA. This report describes the progressof the ASTE telescope as well.
The mission of the NAOJ ALMA Project is to: implement
the functions of the East Asian ALMA Regional Center, which
provides support for users in East Asia; coordinate international
project activities based on global partnership; formulate future
project plans; and make budget requests. On the other hand,
the mission of NAOJ Chile is to: take appropriate safety andsecurity measures for Chile-based staff members and theirfamilies, and establish an environment where they can engage intheir activities safely and securely; provide the interface in Chile
with the Joint ALMA Observatory (JAO), the other ALMA
Executives, and Chilean institutions; and establish, organize,
and maintain an exchange scheme for scientists and engineers
between NAOJ and Chilean universities and institutes.
Under NAOJ Chile, the ASTE project has been promoting
and pioneering submillimeter astronomy while providing aplatform for new technology development and submillimeter
observation data to the scientific community through theoperation of the ASTE telescope. In addition, NAOJ establisheda Study Group for the Next Generation Very Large Array(ngVLA) in FY 2019, under the umbrella of the ALMA Project.
The ngVLA Study Group has been assessing, together withthe scientific community, scientific opportunities for a possible
future contribution from Japan to ngVLA; and has initiateddevelopment studies which will allow NAOJ to contributetimely to construction if supported by the Japanese scientificcommunity and budget processes.

1. Progress of the ALMA Project
The 9th round of ALMA open-use observations (Cycle8) ended at the end of September 2022, with the 2nd highest
number of observed hours in a Cycle. Cycle 9 observations
started on October 1, 2022, and proceeded smoothly. However,the ALMA observatory in Chile suffered a cyberattack on
its computer system on October 29, and observations weresuspended. Scientific observations restarted around December
17, after the affected computer system servers and services wererebuilt. During 2018–2022, the ALMA Project established theframework to kick off the implementation of the ALMA2030
wideband sensitivity upgrade (WSU). In November 2022, the
ALMA Board approved project proposals for the developmentof a second-generation correlator led by North America anda new data transmission system (DTS) led by East Asia incooperation with North America. Regarding the developmentof new instrumentation, the production of Band 1 receivers
was completed in Taiwan, and the commissioning review inNovember 2022 was successful. The commissioning reviewof the newly developed spectrometer for the Total Power
Array (ACA spectrometer) was passed in November 2022. It
is anticipated that Band 1 receivers and the ACA spectrometer
will be used for PI science starting from Cycle 10, which will
start in October 2023. In March 2023, ALMA celebrated its 10th
anniversary since its inauguration. A ceremony was held at the
OSF/AOS on March 13. The number of refereed publications
with ALMA data has exceeded 3000. The paper on HL Tau has
passed 1000 citations.

2. ALMA Open-Use and Scientific Observations
Cycle 8 observations finished on September 30, 2022.
The number of science data acquisitions on the 12-m Array in
Cycle 8 was the 2nd highest in ALMA’s history. The subsequenttransition to Cycle 9 on October 1 was completed smoothly. For
Cycle 9, a total of 1,769 proposals were submitted requesting
27,912 hours of time on the 12-m Array, which is the most everrequested in a single cycle. The main capabilities of Cycle 9
include: interferometric observations using at least forty-three
12-m antennas; ACA observations (interferometric observation
with at least ten 7-m antennas and single-dish observation withat least three 12-m antennas); eight frequency bands (Bands
3, 4, 5, 6, 7, 8, 9 and 10); and maximum baselines of 16.2 km.
From Cycle 9, longer baseline high-frequency (Band 8, 9, and10) observations are available, providing the highest angularresolution of ALMA at about 10 milliarcsecond. In addition, fast
regional mapping for solar Total Power observations, spectralline VLBI in Band 3, and continuum VLBI capabilities in Band
7 have become newly available from Cycle 9.
During the initial period of Cycle 9, on October 29, theJoint ALMA Observatory in Chile suffered a cyberattack on
its computer systems, forcing the suspension of astronomical

II Status Reports of Research Activities

053

observations. After the recovery efforts, PI science observations
were resumed in mid-December.
ALMA open-use observations have been producing a
number of scientific results. The following paragraphs highlightsome of the scientific achievements made by East Asian
researchers.
An international team of astronomers, led by Yuichi
Harikane, an assistant professor at the University of Tokyo,
and Akio Inoue, a professor at Waseda University discovereda distant galaxy named HD1, which is about 13.5 billion lightyears away. This discovery implies that bright systems like HD1existed as early as 300 million years after the Big Bang. Thisgalaxy is one of the targets of the James Webb Space Telescope.
A team of astronomers, led by Shinya Komugi, an associate
professor at Kogakuin University, discovered for the first timea faint radio emission around a giant galaxy with an energetic
black hole at its center by using ALMA data. The radio emission
is released from gas that is excited directly by strong radiationfrom around the central black hole. The result was obtained
through high dynamic range imaging. The team expects tounderstand how a black hole interacts with its host galaxy byapplying the same technique to other quasars.
A research team led by Tomohiro Yoshida, a graduate
student at the Graduate University for Advanced Studies,
SOKENDAI, and Hideko Nomura, a professor at NAOJ
discovered that the abundances of different molecular species
vary significantly around a site of planet formation by using
ALMA data. Using a newly developed method, the teammeasured the carbon monoxide isotopologue ratio, which canbe used as a new “fingerprint” to trace the origins of materials,
in the protoplanetary disk around the star TW Hydrae. The
team found significant differences in this ratio depending on theregion. This new “fingerprint” will provide a new method forunderstanding where and how the materials of the Solar Systemand exoplanets were created and transported.
An international team led by Kazuki Tokuda, Project
Assistant Professor at Kyushu University/NAOJ, and Toshikazu
Onishi, a professor at Osaka Metropolitan University conducted
ALMA observations toward massive young stellar objects in
the Small Magellanic Cloud, which is characterized by a low
abundance of elements heavier than helium, similar to thegalaxies 10 billion years ago. The target provides a detailed
observational view thanks to its relatively short distance fromthe Earth. In this study, researchers detected a bipolar gas stream
flowing out of the “baby star” Y246 and determined that themolecular flow has a velocity of more than 54,000 km/h inboth directions. In the present Universe, growing “baby stars”
are thought to have their rotational motion suppressed by thismolecular outflow during gravitational contraction, acceleratingstar growth. The discovery of the same phenomenon in the Small
Magellanic Cloud suggests that this process of star formation
has been common throughout the past 10 billion years. The teamalso expects this discovery to bring new perspectives to studying
star and planet formation.
At the heart of nearly every galaxy lurks a supermassive
black hole. But not all supermassive black holes are alike: there054

II Status Reports of Research Activities

are many types. Quasars, or quasi-stellar objects, are one of thebrightest and most active types of supermassive black holes.
An international group of scientists (under lead author Hiroki
Okino, a Ph.D. student at the University of Tokyo and NAOJ)
published new observations of the first quasar ever identified— the one labeled 3C 273, located in the Virgo constellation –that show the innermost, most profound parts of the quasar’s
prominent plasma jet. This ground-breaking work was madepossible by a closely coordinated set of radio antennas aroundthe globe, a combination of ALMA and the Global Millimeter
VLBI Array.
Gamma-ray bursts are the most luminous explosions in
the Universe, allowing astrophysicists to observe intense,
short-duration gamma rays. Gamma-ray bursts are classified
as either short or long, with long gamma-ray bursts being theresult of massive stars dying. Hence they provide clues about
the evolution of the Universe. Gamma-ray bursts emit gamma
rays as well as radio waves, optical light, and X-rays. Whenthe conversion of explosion energy to emitted energy, i.e., theconversion efficiency, is high, the total explosion energy can becalculated by simply summing over all the emitted energy. But
when the conversion efficiency is low or unknown, measuring
the emitted energy alone is not enough. A team of astrophysicists
succeeded in measuring a gamma-ray burst’s hidden energy
by using ALMA and the Very Large Telescope. The team was
led by Dr. Yuji Urata from the National Central University
in Taiwan and MITOS Science CO., LTD, Professor KenjiToma from Tohoku University’s Frontier Research Institute forInterdisciplinary Sciences, and graduate student Asuka Kuwata
from Tohoku University.
The role of the magnetic field in the star-formation process
is an extensively debated topic. How strong is the magnetic
field? Can it guide material on the way to the star? When andwhere can gravity overpower the magnetic field? Recently, aninternational research team led by Patrick Koch at Academia
Sinica Institute of Astronomy and Astrophysics (ASIAA), used
ALMA to resolve the magnetic field structure in the W51 e2
and e8 high-mass star-forming regions with an unprecedented
resolution of 0.1″. Compared to the earliest magnetic fieldobservations in this region with a resolution of 3″, this is an
improvement in resolution by a factor of about 1000 in area.
This only becomes possible with ALMA’s exquisite sensitivity
and resolution which now sharpen our view of the magnetic field
by a factor of 1000, making visible details as small as 500 au forthe first time.
Asako Sato, a graduate student at Kyushu University, andher team used ALMA to reveal fast gas outflows from a baby
star strongly colliding with nearby dense gas where a group of
baby stars is being born. This result suggests that the outflow
collision shakes the cradle of the baby stars and has a significant
impact on the ongoing star formation process. This study
provides insight into the star formation process within clusterforming regions where baby stars are born simultaneously in a
crowded and complex environment.
An international research team led by Keiichi Maeda, aprofessor from the Graduate School of Science at Kyoto University,and Tomonari Michiyama, ALMA Joint Postdoctoral Fellow fromthe Graduate School of Science at Osaka University, discovered
the first example of a supernova, known as SN 2018ivc, showing
an unprecedented rebrightening at millimeter wavelengths about
one year after the explosion by using ALMA. The analysis
revealed that the dying massive star ejected a large amount of
its envelope due to a strong binary interaction with a companion
star that took place about 1500 years before the explosion. In a
paper published in The Astrophysical Journal Letters, the team
posited that this rebrightening event in SN 2018ivc provides
a missing link between supernovae that occur in binary starsystems and those that involve solitary massive stars.

3. Educational Activities
The NAOJ ALMA Project continues to collaborate with
the Joint ALMA Observatory (JAO) to create and maintaina Japanese version of “ALMA Kids,” a website for children,with the aim of providing opportunities for more people tolearn about the mechanisms of ALMA and its scientific results
in a fun way. ALMA Kids provides up-to-date content for the
younger audiences, introducing various results from the latest
ALMA observations. However, the “ALMA Kids” website wasaffected by the cyberattack and it has not been available sincethen. The final update was done in early September. The Project
has developed educational content, mainly targeting elementary
school students, called “Why ALMA Workshop” which
explains the basics of radio astronomy by combining videos andworksheets. This content is available on the Project website.
The Project continues to release science news posters
aimed for the younger generation visiting science centers andplanetariums. Two new posters were released in FY 2022. In
addition, the Project now provides short anime (“manga”)
explaining the basics of radio astronomy and interferometry. In
FY 2022, this effective medium of manga was also adopted toconvey the upgrade of the data transmission system as a part of
the Wideband Sensitivity Upgrade (WSU) which will be carriedout during the ALMA 2 project phase. All posters and manga are
available on the NAOJ ALMA website.

4. Public Outreach Activities
In FY 2022, ALMA scientific observation and development
results were covered by 45 newspaper/journal articles, and
ALMA was featured by one television program. On December
31, 2022, a staff member of the NAOJ ALMA Project appeared
in a web show with an antenna under maintenance at the ALMA
Operations Support Facility (OSF) in Chile. The NAOJ ALMA
website posted 21 news articles and 6 press releases. Mailinglist-based newsletters have been issued on a monthly basis withapproximately 2,000 subscribers. Day-to-day information isposted in a timely manner on Twitter (@ALMA_Japan) withnearly 67,000 followers as of the end of FY 2022. Impressive
images are often posted on Instagram, which achieved 10,000
followers.
In FY 2022, 7 lectures were given for the general public, of

which one was held online and one was held with the speaker
participating remotely. In May-June 2022, the NAOJ ALMA
Project exhibited a joint booth with the NAOJ TMT Projectat the Japan Geoscience Union Meeting (held both onsite andonline). NAOJ ALMA provided video contents for Nobeyama
Open House Day held online due to COVID-19. NAOJ OpenHouse Day in Mitaka was held in hybrid style in October. Onsite
exhibits of the NAOJ ALMA Project were posters, models of anantenna and the Atacama Desert, virtual tour of Chajnantor, andso on. Workshops for children were not held due to COVID-19.
Two lectures were given online.
ALMA’s 2014 ground-breaking HL Tau results exceeded
1,000 citations in 2022. The NAOJ ALMA Project actively
publicized this record, including posting on the website. Public
relations to provide information about JAO’s recovery fromthe cyberattack also played an important role. NAOJ ALMA
supported the public relations activities for the 10th anniversary
ceremony held in Chile in March of 2023. Also, the planningand preparation of novelty goods has progressed for the 10th
anniversary ceremony in Japan scheduled in May of 2023.
From mid-March 2015, ALMA began accepting public
visitors to the OSF at an altitude of 2,900 meters, but due to theoutbreak of COVID-19 in Chile, it stopped accepting public
visits in March 2020. As of the end of FY 2022, public visits
remain suspended except for VIPs, Media, and the staff’s family
and friends.

5. International Collaboration (Committees, etc.)
For the international ALMA project, meetings are held
frequently by various committees. In FY 2022, many of themeetings continued to be held online as during FY 2021, due tothe COVID-19 pandemic, but by the end of the fiscal year, inperson meetings resumed, including the ALMA Board meeting
held face to face in Santiago (Chile) in November. The ALMA
Board and the ALMA Scientific Advisory Committee (ASAC)
held online meetings as necessary, while the ALMA East AsianScience Advisory Committee (EASAC) held online meetings
three times. Meetings were held more frequently by groups incharge of specific tasks to implement the international project inclose cooperation.

6. Workshops• July 5 and 7, 2022: ALMA Data reduction tutorial (introductory
level), in collaboration with the Astronomy Data Center,
held online• December 19, 2022: ALMA Grant Fellow Symposium 2022,
NAOJ Mitaka Campus and online• December 20–21, 2022: ALMA/45m/ASTE Users Meeting
2022, NAOJ Mitaka Campus and online• February 27–28, 2023: ALMA Data reduction tutorial(beginner-intermediate level), held with the Astronomy Data
Center, NAOJ Mitaka Campus• March 7–10, 2023: ALMA BEARS workshop, NAOJ Mitaka
Campus

II Status Reports of Research Activities

055• March 13, 2023: “ALMA 2030: Wideband Sensitivity
Upgrade”, Special session in the ASJ 2023 Sprint Meeting,Rikkyo University and online

7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research, including
Industry–University Collaboration Expenses• Yuichi Matsuda: funded by the research support project of the
Astrobiology Center (ABC), National Institutes of Natural
Sciences (NINS)

8. Changes in Project Researchers(1) Hired• Andrea Silva: Project Researcher• Piyali Saha: Project Researcher• Takuma Izumi: Project Researcher(secondment to Tokyo Metropolitan University)• Anton Feeney-Johansson: Project Researcher(secondment to the University of Tokyo)• Sanemichi Takahashi: Project Researcher(secondment to Kagoshima University)(2) Departed or transferred• Takuma Izumi: Project Resarcher• Hiroyuki Kaneko: Project Resarcher• Yuki Kudoh: Project Resarcher• Tom Bakx: Project Resarcher• Tomonari Michiyama: Project Resarcher

9. Main Visitors• Apr. 13, 2022: Harumi Takahashi, Parliamentary Secretaryfor Education, Culture, Sports, Science and Technology(MEXT), visited NAOJ Mitaka Campus.
• May 24, 2022: Hideyuki Tanaka, Vice Minister of Education,
Culture, Sports, Science and Technology (MEXT), visited
NAOJ Mitaka Campus.
• Dec. 1, 2022: Thomas Zurbuchen, NASA Associate
Administrator, visited NAOJ Mitaka Campus.
• Feb. 3, 2023: Ricardo G. Rojas, Ambassador of the Republicof Chile to Japan, visited NAOJ Mitaka Campus.

10. Progress of the ASTE Telescope
The cause of the antenna sub-reflector failure identified
last fiscal year (FY 2021) was investigated and examined incooperation with the manufacturer of the antenna. As a result,
we concluded that an on-site inspection by the manufacturer's
engineers was necessary. After procuring replacement parts
to solve the failure, the ASTE telescope site was reopened in
November, and the inspection of the sub-reflector was conducted
together with the manufacturer’s engineers. The sub-reflector
was restored at the beginning of December, but another failure
was soon identified, so the investigation continued until mid-

056

II Status Reports of Research Activities

December. Based on the data obtained from the sub-reflector
drive system at that time, we are continuing to investigate thecause and measures together with the manufacturer.
We tried to conduct the scientific commissioning operationof the wide IF band Band 8 receiver, the new spectrometer(XFFTS), and the frequency converter (IFDC), which were
installed on the ASTE telescope last year (FY 2021) under two
Grants-in-Aid for Scientific Research (PI: Oka, Keio University,
and Tosaki, Joetsu University of Education), using actual
celestial signals. However, due to the sub-reflector failure andbad weather conditions, it was decided to reschedule. The final
operation verification test is expected to be conducted in the next
fiscal year (FY 2023) after the sub-reflector is restored.
In FY 2022, three peer-reviewed papers were published,including 1 paper written by domestic researchers and two by
overseas researchers. The decrease in the number of papers
published was unavoidable due to the suspension of scientificobservations due to the COVID-19 pandemic between FY 2020and FY 2021 and the sub-reflector failure in FY 2021.

07. Gravitational Wave Science ProjectThe 4th International Gravitational-Wave Joint Observation(O4) was repeatedly postponed due to COVID-19 and natural
disasters, and will finally be carried out for a net year and ahalf starting on May 24, 2023. The Large-scale Cryogenic
Gravitational Wave Telescope KAGRA, which NAOJ is
promoting with the Institute for Cosmic Ray Research (ICRR)
of the University of Tokyo and the High Energy Accelerator
Research Organization (KEK), aims to participate in O4 at thestart (O4a) with a sensitivity in the binary neutron star merger
range of 1–3 Mpc. In FY 2022, we made large efforts for
instrument modification and interferometer commissioning torealize this goal.
The GWSP also began in earnest discussions on thedevelopment of next-generation gravitational wave telescope
technology utilizing the TAMA300 facility, and launched new
R&D initiatives and a framework for international cooperation.

1. Gravitational Wave Telescope, KAGRANAOJ GWSP plays an important role in the operation andmanagement of KAGRA as one of the promoting organizations
under the “Memorandum of Understanding on Promotion ofGravitational Wave Astronomy Using the Large-scale Cryogenic
Gravitational Wave Telescope, KAGRA”. In particular, the
GWSP is in charge of the Low Frequency Vibration Isolators,
Auxiliary Optics, Mirror Evaluation, and Main Interferometer,
and also contributes to the operation by providing members to
the Executive Office, System Engineering Office, etc.
The main initiatives for FY 2022 were as follows.
(1) Main Interferometer and Commissioning
Overhaul work was completed for O4, including reinstallationof the Output Mode Cleaner and additional monitoring of theinterferometer optical axis. Commissioning then proceeded,
and the Power-Recycled Fabry-Perot Michelson interferometer
was successfully put into operation. The problems of noisecontamination in the vibration isolator and angular stability ofthe mirror, which had limited the sensitivity of the previous
observation, were largely resolved, and the target sensitivity andoperation stability for O4a were achieved.
(2) Vibration Isolation Systems: All of the vibration isolation
systems (4 types, 19 units in total) were tested, their problems
were corrected, and their control was optimized. In addition,a folding pendulum accelerometer was manufactured andevaluated in cooperation with ATC. This will be installed in
KAGRA in the future.
(3) Auxiliary Optics: A total of 14 medium size optical baffles
with vibration isolators were installed in the vacuum chambers
to prevent stray light. In addition, the optical axis and stray lightcountermeasures of various input and output optical systems
were reviewed, and the installation of the necessary steering

mirrors and beam shields was completed.
(4) Mirror Evaluation: In order to replace the input-side sapphire
mirrors (ITMs) of KAGRA with higher performance ones in
O5, we started ITMs remanufacturing. Five Korean sapphire
crystals were evaluated for optical absorption and birefringence,and the two best ones were selected and shaping processing was
conducted. The GWSP also began new work on the developmentof a scattered light measurement system, birefringencemeasurement system, and spectroscopic analysis.
(5) Others: Various sensors installed in KAGRA contributed
to KAGRA's noise hunting. In addition, two units of PCAL,a photon pressure calibrator for GW signals, were put into
operation to enable automatic operation. Calibration of thecalibrator itself is being performed continuously and has greatly
improved stability compared to O3.

2. R&D in TAMA300 and ATC
Development of cutting-edge technologies for gravitational
wave telescopes is underway at the TAMA300 first-generationinterferometric gravitational wave antenna and the ATClaboratory at Mitaka Campus.
(1) Development of frequency-dependent squeezing (FDS)
technology: Using TAMA300, we are developing a quantum
optics technique called FDS to improve the sensitivity ofgravitational wave telescopes over a wide bandwidth; in FY
2022, we specifically studied backscattering and mode mismatch
loss to implement FDS at KAGRA.
(2) Detector R&D: In order to greatly improve the sensitivityof gravitational wave detectors in the future, a control method
for Speedmeter-type interferometers is being studied. The
theoretical analysis of the control has been published as apaper, and a proof-of-principle experiment will be conductedin the future. We are also discussing future applications of
TAMA300, such as construction of a high-frequency specializedinterferometer using Long-SRC, EPR Entanglement Squeezing,and so on.

3. Education
Two students of the Department of Astronomy at the
University of Tokyo, one student commissioned by Tokyo Tech,and one research student from overseas are currently enrolled in
the group and are supervised. With the increase in the numberof students, the introduction of research papers in the group
was renewed for the education of students. In graduate school
and university education, lectures at Hosei University and the
Graduate School of the University of Tokyo were given. In
addition, social education activities such as “FUREAI (Friendly)

II Status Reports of Research Activities

057

Astronomy” and visiting lectures at high schools were provided.

4. Outreach
Virtual tours of TAMA300 and KAGRA were conductedduring the open house, and the KAGRA tour video was madeavailable on YouTube. In addition, with black holes attracting
much attention, a Japanese language article on gravitational
wave black hole observations titled “New Eyes” was publishedin NAOJ News. In addition, a press release on the research on
dwarf novae conducted by one of our master’s students as anundergraduate student and an article in the Wakayama Shimpo
newspaper covering the “FUREAI (Friendly) Astronomy”
lecture were posted as topics on the web page.

5. International Collaboration and Visitors
Due to COVID-19, the number of overseas visitors remainedlow (six), as in the previous year. Collaborations progressedwith CNRS/APC (France), iLM (France), National Tsing Hua
University (Taiwan), Myongji University, and KASI (Korea),
with which international research exchanges have been active
for a while.

6. Publications, Presentations, and Workshop
Organization
The number of peer-reviewed papers published ininternational journals whose authors were members of GWSP
was 24. The number of non-refereed papers was 2 in European
journals and 4 in Japanese journals. There were 24 reportsof lectures given at international conferences and 34 reportsof conference presentations. There were no other reports ofpresentations or other publications in English or Japanese.

7. Acquisition of External Funds
In FY 2022, no external funds other than scientific researchfunds were obtained.

8. Staff Changes● Michael Page (JSPS Foreign Research Fellow → Project
Researcher)● Marc Eisenmann (JSPS Foreign Research Fellow → Project
Researcher)● Rishabh Bajpai (Joined as Research Support Staff (Kakenhi))● Naho Sakaguchi (Joined as Administrative Support Staff at
Kamioka Branch)● Mariko Doi (Joined as Administrative Expert at Mitaka Office(GWSP & JASMINE))● Matteo Leonardi (Retirement → Associate Prof. in Trent
Univ., Italy)● Naoki Aritomi (Retirement from Project Researcher →Researcher at Caltech)● Mie Ueda (Retirement from Administrative Expert in Mitaka office)058

II Status Reports of Research Activities

08. Thirty Meter Telescope Project
The Thirty Meter Telescope (TMT) Project is the workof an international collaboration to build an extremely large
30-meter telescope (Figure 1). For Japan’s part, with the
National Institutes of Natural Sciences (NINS) as an ultimately
responsible body, NAOJ serves as an executing institute.
In 2014, an agreement was concluded among participatingorganizations to found the TMT International Observatory(TIO) for the purpose of the construction and operation of theobservatory; the construction was subsequently commenced.
Japan is responsible for the production of the telescope primary
mirror, the design and production of the telescope structure aswell as its on-site installation and adjustment, and the design
and production of science instruments. Heading the project forJapan is the TMT Project at NAOJ.
In Hawai‘i where TMT is slated to be built, with the Stateof Hawai‘i’s approval of a Conservation District Use Permit(CDUP) for TMT construction on Maunakea in 2017, onsite construction was planned to start in FY 2019. However,demonstrations and a road blockade by those opposed toconstruction of TMT on Maunakea prevented full-f ledged
construction work at the summit region. Currently, TIO
continuously engages with broader communities in Hawai‘i forbuilding trust through direct dialogue, educational programs,
and other com munit y activities together with relevantorganizations. As a TIO member, NAOJ actively takes partin these activities. The Hawai‘i State Legislature passed abill that established a new management body called Mauna
Kea Stewardship and Oversight Authority (MKSOA) with an
overwhelming majority. The U.S., the Decadal Survey released
in FY 2021, which is a report of the research communitythat identifies priorities for the coming decade, ranked a

Figure 1: Rendering of TMT Telescope Structure Image. (Credit: TIO)

joint program called the U.S. Extremely Large Telescope
Program (the US-ELT Program), including the TMT project,
as a top priority for ground-based astronomy. In response tothis outcome, the National Science Foundation (NSF) held aPreliminary Design Review (PDR) in FY 2022, which ended
with favorable feedback from its external panel. As described
below, NSF is currently conducting a review process toevaluate environmental effects, and is also assessing impacts
on historic properties under Section 106 of the National
Historic Preservation Act, in addition to the process towarda Final Design Review (FDR). Seeing major progress in thesituation in Hawai‘i and NSF’s possible investment of the
U.S. federal funding in the project, TIO, NAOJ, and the otherparticipating members are focused on essential activities in theoverall process, including those that will pave the way to fullfledged construction once on-site construction restarts, while
minimizing their expenditures.

1. TMT Project Progress and Status ofConstruction Site
The construction of TMT is led by TIO established in 2014
and the participating countries and organizations (NINS, theUniversity of California, the California Institute of Technology,
the National Research Council of Canada, the Department of
Science and Technology of India, the National Astronomical
Observatories of the Chinese Academy of Sciences). Alongwith them, as the process is underway for NSF’s participationt h roug h t he feder al f u nd i ng, t he U.S. Associat ion of
Universities for Research in Astronomy (AURA) participates
as an Associate Member.
TIO, operated according to deliberations and decisions by
the TIO Board of Governors, is overseeing the construction
work performed at the institutes, as well as developing the onsite infrastructure. The Board of Governors convened a totalof 5 meetings in FY 2022 mainly to discuss activities aimed
at NSF’s investment of the federal funding and issues relating
to resumption of on-site construction, with 3 representatives
from Japan in attendance: Director General Tsuneta, ViceDirector General Yoshida, and NAOJ TMT Project Manager
Usuda. Several working groups were created under the Boardof Governors to consider efforts for construction in Hawai‘i,
as well as issues of the project operation, by holding meetings
as frequently as in the previous fiscal year. One of themis the Business Plan Working Group chaired by the NAOJ
Director General. This working group held 10 meetings toassess in detail the status and evaluation of members’ in-kind
contributions; and proposals to NSF which included TIO’s
funding plan based on that assessment. All the meetings were
held online.
The U.S. Decadal Survey for astronomy and astrophysics
decennially evaluates and identifies the most compellingchallenges in the field of astronomy. According to the report

II Status Reports of Research Activities

059

published in 2021, the US-ELT Program, which will allow
all-sky observation through TMT and the Giant Magellan
Telescope (GMT, a telescope with an aperture of 24 meterscurrently under construction in Chile) working in concert,
was ranked as a top priority for ground-based astronomy. In
response to the survey results, NSF conducted the PDR for the
US-ELT Program proposed by TIO along with NSF’s National
Optical-Infrared Astronomy Research Laboratory (NSF’s
NOIRLab) and GMT. The first part of the review of the TMT
project was carried out in December 2022, focusing on thetechnical and outreach activities, followed by the second partin January 2023 to assess the project’s management, costs, andschedule risks. The NAOJ TMT Project fully worked with TIO
for both parts of the review. The review panel highly evaluatedthe technical por tion, which includes Japan’s telescope
structure and other in-kind work, and the engagement activities
in Hawai‘i. It concluded that the project was all ready foradvancement to the final design phase of development while
indicating that there were some outstanding issues on technicalreadiness, management, and schedule risks to be resolved by
the FDR. Passing the PDR is an important step for inclusion
in a future NSF budget request for construction funding.
The budget request will need to be deliberated and passed by
Congress and will then be signed into law by the President
before NSF can fund the project. NSF will need to complete the
FDR, the environmental review process, and the Section 106
consultation process under NHPA. Then, a Record of Decision
will be published to announce NSF’s decision. In addition to the
proposal for the construction fund, TIO submitted proposals
to NSF for funding the design and development of the primary
mirror control, the secondary mirror, and other systems.
As for the situation in Hawai‘i, a CDUP was approved
for the TMT planned site on Maunakea in September 2017,
but demonstrations staged by those opposed to TMT on
Maunakea, including a road blockade, prevented the fullfledged construction in July 2019. TIO recognized it had neither
well understood the social issues behind the demonstration
nor engaged in dialogue with broader communities in Hawai‘i,
which had led to the failure to fully build trust with the
Hawai‘i community. The Board of Governors decided onphased relocation of the TIO headquarters from Pasadena,
California, to Hawai‘i, with the first step taken to relocate theProject Manager to the Island of Hawai‘i in June 2021 to start
community-based activities. The NAOJ TMT Project Manager
also moved to Hawai‘i Island in July 2021 to fully contribute
to TIO’s community engagement activities with an NAOJ
Senior Specialist based in Hawai‘i who is currently seconded
to TIO. In particular, they played a major role in developing
and implementing a tutoring program for a broader array ofcommunities as part of TIO’s community engagement. Throughdialogue with the communities, a strong need was expressed
for educational support for children, in particular, those from
low-income families. TIO started tutoring activities at schoolsthat Maunakea observatories had not engaged in before,
which generated great interest among local communities.
This tutoring program was incorporated in the design and060

II Status Reports of Research Activities

development proposal submitted to NSF, where the NAOJ staff
were committed to its formulation.
In May 2021, the House of Representatives of the Hawai‘iState Legislature created a working group to discuss a new
management structure for Maunakea, which subsequently
released a report of recommendations in December. Basedon the recommendations of the working group, a bill started
to be deliberated at the state legislature in January 2022 forthe creation of a new management structure that aims toparticularly engage with the Native Hawaiian community.
The bill was signed into law by the Governor in July 2022
(Act 255). In September 2022, 11 members for the new
management structure, called Mauna Kea Stewardship andOversight Authority (MKSOA), were appointed, some ofwhom were recommended by the heads of the Senate andHouse of Representatives, and the Maunakea Observatories.
Their activities started in November to discuss the roles ofthe members, rules, schedules, and other matters by holding amonthly meeting.
In July 2022, NSF published a notice of intent to initiate
the environmental review process and the Section 106 process
under NHPA. Along with this, a draft Community Engagement
Plan was released to help guide meaningful and effective
engagement with the Hawai‘i community and other interested
members of the public. Four public scoping meetings were heldin Hilo, Na‘alehu, Kona, and Kamuela (Waimea) in August, andpublic comments were solicited by September. Reviewing morethan 7,000 comments received, NSF is currently conducting
the environmental review process and the Section 106 process
under NHPA.
As for the alternative site on the island of La Palma of
the Canary Islands in Spain, which was selected in 2016, theprocess for all permits needed for construction was completed
in November 2019, including an environmental impact
assessment. In an administrative appeal against the land
concession, a court determined in July 2021 that there wasa procedural problem, and annulled the concession, against
which TIO appealed together with a local government and alocal research institute. In September 2022, the Superior Courtof Justice of the Canary Islands issued a judgment upholding
TIO’s appeal, declaring that the land concession is legal andvalid. NAOJ expresses its support for relocation to La Palmain the case that construction in Hawai‘i becomes infeasible,
provided that the project is expected to receive U.S. federal
funding.

2. Japan’s Progress on its Work Share– Development of Telescope Structure,
Primary Mirror, and Science Instruments
For the construction of TMT, Japan is responsible for
essential components of the telescope in accordance withthe executed agreements: the design and production of thetelescope structure and its control system; the manufacturingof the primary mirror; and the production of portions of thescience instruments which are developed through international

partnerships. While the restart of on-site construction is halted,
Japan focused on designs and preparation for production in FY
2022, concentrating its efforts on essential work for the overall
process instead of production. In FY 2022, the progress below
was made.
(1) Manufacturing of Primary Mirror Segments
The TMT primary mirror, comprised of 492 segment
mirrors, requires the manufacturing of 574 segment mirrors
in all, with the replacements during mirror coating included.
The process of manufacturing mirror segments is: fabricationof the mirror blanks, spherical grinding of the front and backsurfaces, aspherical grinding and polishing of the front surface,hexagonal shaping, and mounting of the mirror segments onto
support assemblies. It is followed by the final surface finish to
be completed in the U.S. and coating with reflective metal tobe performed on-site, before the mirror segments are finallyinstalled on the telescope.
Of the above process, the plan calls for Japan to fabricate
all the mirror blanks and to perform spherical grinding on all
574 segment mirrors. With the share of work for the processes
begin ning f rom aspherical grinding and polishing andending with the mounting of the mirror segments on support
assemblies distributed to other participating overseas institutes
as well, Japan is leading this work for 175 of the mirror
segments. In FY 2022, NAOJ’s primary mirror team identified
and examined a measure to protect the mirror surface when the
hexagonal shaping work is performed. This is part of the effort
to facilitate production of the primary mirror segments whenfull-fledged manufacturing of the segments is resumed, without
affecting the entire schedule. As a result of their work, they
singled out a possible protection coating to be used for largescale production by choosing candidates and measuring thedegree of deterioration after soaking them in the fluid used forthe grinding process. The team was also devoted to developinga method to overcoat with epoxy resin the protection coatingthat had been stripped in a past trial. The experiment found that
this can be a prospective method to be employed. In addition,a load test was carried out on an adhesive-bonded part tosimulate the transport of segments to the U.S. after support
assemblies were mounted on them, which confirmed no issues
were observed.
(2) Design and Production of Telescope Structure and Its
Control System
Japan is responsible for the design and production of
the telescope structure, as well as its control system, whichfunctions as a mount for the primary mirror, other optics
systems, and science instruments, and points them in the
direction of target astronomical objects. Following the baselineand detailed designs developed by FY 2016 and preparation
for fabrication in FY 2017, FY 2018 saw the launch of thefabrication process for the telescope structure. In FY2022,
continuing on from the previous fiscal year, with an eye
toward production readiness reviews scheduled before fullscale production, the work was focused on the completionof interface documents and the development of production
drawings. Two production readiness reviews (PRR2 and PRR3)
were conducted to examine the main rotating mechanicalstructures that move around the azimuth and elevation axes, aswell as the Nasmyth structure where the science instruments
and other systems will be placed (Figure 2).
(3) Science Instruments
St e a d y p r og r e s s wa s m a d e t h r ou g h i nt e r n at ion a lcollaboration in the design and fabrication of three first-lightscience instruments, which will be commissioned once thetelescope is complete.
One of them is IRIS which stands for an InfraRed Imaging
Spectrograph. Being in charge of its imager, Japan continues toengage in development that includes designing and prototyping
in cooperation with the Advanced Technology Center. In FY
2022, the work was focused on action items indicated by the
final design review of the imager held in FY 2021, and on
preparation for a final design review of the entire instrument
which is scheduled for FY 2024. The action items identified
in the previous year’s review were followed up by the teammainly through: modeling of the vibration analysis for the
combined Narrow Field InfraRed Adaptive Optics System(NFIRAOS) and IRIS system, and the derivation of its transfer
function; thermal analysis of the imager; verification of theposition sensor’s precision, production of a part that will be
used for a mechanical interface to the vacuum chamber and its
strength testing; and establishment of a structure to conduct
experiments in collaboration with Tohoku University forassessing the performance of HAWAII-2 which will function
as a detector used for the pupil optics. In order to prepare
for the upcoming review, the team performed a system-level
failure modes and effects analysis, and defined requirements bysimulation for conceptual and preliminary designs of an opticalsimulator that will be used for performance assessment of theimager and the integral field spectroscope. Also, in June 2022,
as U.S. manufacturer Teledyne may suspend the production
line of an infrared detector that is intended to be used for theimager, NAOJ’s IRIS team played a leading role in a trade
study for alternative detectors in cooperation with the IRIS
international team.
A Wide Field Optical Spectrometer or WFOS began the
preliminary design phase in FY 2022, following the successful
passage of the conceptual design review in FY 2021. Further
progress was made in FY 2022. NAOJ’s WFOS team performed

Figure 2: Two Production Readiness Reviews (PRR 2 and PRR3) for
TMT’s structure, which were held in person, were successfully completed
in February 2023.

II Status Reports of Research Activities061

a trade study for the slitmask exchanger with the California
Institute of Technology, and also explored the feasibility of
manufacturing a large-scale optical glass substrate and a
Volume Binary Grating. Their work also advanced optical andmechanical designs for the integral field unit, which is planned
as future work, and examined where to place the unit within
WFOS.
A Multi-Objective Diffraction-limited High-Resolution
Infrared Spectrograph (MODHIS) is expected to pioneer thefield of exoplanets, on which the U.S. Decadal Survey placed
an emphasis. With its project management led by an NAOJ
Associate Professor, MODHIS kicked off the first phase of aconceptual design in 2021 in partnership with the California
Institute of Technology and the University of California, Los
Angeles and San Diego. This phase aims to clarify the conceptof the adaptive optics to be combined with the instrument anddevelop a conceptual design of the interface to TMT adaptive
optics. The team’s efforts also go into defining scientific andtechnical requirements to be satisfied by MODHIS. With thesights set on establishing an international development team,
the Astrobiology Center’s role in the MODHIS development iscurrently under consideration.
NAOJ staff who are based at the NAOJ California Officein Pasadena engaged in TIO’s development activities. Their
contributions are a considerable asset for TIO’s work, including
development of the control system for the primary mirror’ssegments, and development of user interface software fortesting. They took part in extensive activities; one of the staff
played a major role in developing a conceptual design of acoating facility for the secondary and tertiary mirrors, which
was reviewed by another NAOJ staff member. Also, one ofthem served on a preliminary design review of maintenance,
cleaning, and operation of mirror segments.

The TMT Science Advisor y Committee, which is adomestic com mittee consisting of 13 researchers f rom
universities and other institutes, reviewed issues of science
programs, instrumentation, and operations. In FY 2022,
NAOJ’s funding program for research and development of TMT
science instruments adopted 6 proposals to carry out researchfor development by 28 researchers at 12 universities andresearch institutions. To provide detail on new capabilities thatwill be brought by a suite of TMT next-generation instruments,
the Roadmap to realize TMT next generation instruments
was prepared by committee members and researchers. This
roadmap was released to a wide range of communities. One of
the meetings was convened at the University of Tokyo in March
2023, where a session for sharing information on TMT and theSubaru Telescope was open to anyone, including students.
More meetings were actively organized to explain thestatus of the project and engage in discussions for larger
communities of astronomy in Japan. The NAOJ TMT Project
held a workshop in June 2022 to keep participants informed on
the status of the project and developments in Hawai‘i, as well as
the release of the above-mentioned development roadmap. The
report on the project was provided at the annual meeting of The
Astronomical Society of Japan, as well as a series of meetings
which were attended by researcher communities of a broader
range of fields, such as radio astronomy, theoretical astronomy,
and high-energy astrophysics, in addition to the community of
optical and infrared astronomy. The NAOJ Director General
took a lead in providing an update on the project at all the
meetings for the astronomy and astrophysics subcommitteeof the Science Council of Japan and the Science Advisory
Committee.

3. Planning of TMT Science, Instrumentation,
and Operation with Research Communities

Information on the TMT Project is provided on NAOJ’s
TMT Project website with a focus on updates regarding thesituation at the Maunakea construction site and the work share
progress made by Japan. Additionally, TMT Newsletters No.74
through 78 were delivered.
The outreach activities, which mostly had shifted fromin-person to online lectures and classes in FY 2020 due tothe COVID-19 pandemic, continued to capitalize on online
opportunities in FY 2022, including a program of NAOJ called
FUREAI (Friendly) Astronomy, which offers school children
in Japan and overseas opportunities to learn about astronomy
directly from astronomers. Some of the events took place inperson. There was a total of 48 sessions of lectures for the
public and classes on demand.
Ma ny events i n Hawai‘i, where T MT is slated forconstruction, gradually returned to in-person. The NAOJ TMT
Project provided on-demand lectures in a science/technology
education and PR event called “Journey Through the Universe”
in FY 2022. It also offered hands-on activities at AstroDay, an
event jointly organized with other observatories and sciencerelated organizations in Hawai‘i to invite the local community
to explore the science happening on their home islands. In

TIO’s Science Advisor y Com m it tee, consist i ng ofresearchers from the participating countries and institutions,discusses science programs and instrumentation envisioned
with TMT. In FY 2022, 3 meetings were held online, attended
by 4 university researchers and the NAOJ TMT ProjectManager on behalf of Japan. In view of the preliminary design
review for potential participation by NSF, the committee held
joint science meetings with GMT. As for development of
instruments through international partnerships, a subcommittee
on observation of exoplanets with TMT, chaired by Universityof Tokyo Professor Norio Narita, discussed research themes
based on results of surveys conducted in each country. A subworking group, created for development of a science operations
plan once the telescope is completed, was attended by NAOJ
Professor Wako Aoki. In December 2022 and January 2023,
the TMT webinar was convened to provide information on
the status of the project and the updating work of a document
called the Detailed Science Case that describes the science that
TMT will enable.

062

II Status Reports of Research Activities

4. Public Relations, Outreach, and Education

Figure 3: The Hawaiian Kupuna leads the group of Maunakea
Observatories at the Merrie Monarch parade held on Hawai‘i Island in
April 2022.

addition, through in-person dialogues with wider communities
and in collaboration with community partners such as publicschools and the State Department of Education, an after-school
tutoring program for children, and workforce development
programs for students are now among the core engagement
activities. This partnership further established the after-school
tutoring program, internship opportunities, a cultural exchange
program, and environmental activities in the proposals to NSF.
(Figure 3).

5. Organization
By the end of the fiscal year, three Professors, one Project
Professor, six Associate Professors, two Assistant Professors,
two Research Engineers, and a Senior Specialist, who isseconded to TIO, held positions in the NAOJ TMT Project. In
addition, one Professor, two Associate Professors, one SeniorLecturer, two Assistant Professors, and one Senior Engineer
from the Advanced Technology Center, the Subaru Telescope,and the NAOJ Chile Observatory have concurrent positionsin the TMT Project, and take part in activities that include thedevelopment of TMT science instruments at the Advanced
Technology Center.
With the aim of strengthening the close partnership with
TIO, three members are assigned to the NAOJ California Officein Pasadena. There are three members in Hawai‘i working for
TMT, one of whom is the Senior Specialist seconded to TIO.
In light of integrated operation of the Subaru Telescope
and TMT in the future, schedules and a staffing allocation plan
were continuously discussed and formulated in line with thelong-term plan for operation with the Subaru Telescope. Aspart of the plan, the domestic administration and the public
relations are integrated with the Subaru Telescope.

II Status Reports of Research Activities

063

09. JASMINE Project
1. Planning and Development of the JASMINE(Japan Astrometry Satellite Mission for Infrared Exploration)

Project(1) Overview
The purpose of the JASMINE Project, NAOJ, is as follows.
We participate in and contribute to the JASMINE mission of
the Institute of Space and Astronautical Science/ the Japan
Aerospace Exploration Agency (hereafter, referred to as ISAS/
JAXA), aiming to realize the world’s first near-infrared highprecision astrometry and timeseries photometry. Note that ISAS/JAXA changed the name of “Small JASMINE” to “JASMINE”
in 2021.
We will perform the following missions to achieve the above
purpose of the JASMINE Project.
1) To contribute to scientific verification and developmentof the instruments and the data analysis software for the
JASMINE mission of ISAS/JAXA.
2) To provide the scientific community with a catalog ofphysical information, including parallaxes, proper motions,and light curves, for stars around the Galactic Center,through an international framework under the leadership of
ISAS/JAXA.
JASMINE was selected by ISAS/JAXA in May 2019as the unique candidate for the JAXA Competitive MiddleClass Science Mission No.3. According to the current progress
schedule in the Space Basic Plan established by the Cabinet
Office in Japan, the launch of JASMINE is scheduled for 2028.
We are promoting JASMINE with the aim of improving thedevelopment stage at JAXA step-by-step. JASMINE has thefollowing three primary scientific objectives.

annual parallaxes at a precision of less than or equal to 25 μas
and proper motions, or transverse angular velocities across thecelestial sphere, at a precision of less than or equal to 25 μas/
year in the direction of an area of a few square degrees of the
Galactic nuclear region to create a catalog of the positions andmovements of stars within this region. JASMINE is unique inthat unlike the optical space astrometry mission, “Gaia Project,”
operated by the European Space Agency (ESA), the sameastronomical object can be observed frequently, and observation
will be performed in the near-infrared band, in which the effectof absorption by dust is weak. JASMINE will help to achieve
revolutionary breakthroughs in astronomy and basic physics,
including the formation history of the Galactic nuclear structure(Galactic Center Archeology); the supermassive black hole at the
Galactic Center; the gravitational field in the Galactic nuclear
structure; the activity around the Galactic Center; formationof star clusters; the orbital elements of X-ray binary stars andthe identification of the compact object in an X-ray binary;
the stellar physicis; star formation; planetary systems; andgravitational lensing. Such data will allow for the compilationof a more meaningful catalog when combined with data fromground based observations of the line-of-sight velocities andchemical compositions of stars in the bulge.
Due to satellite operations, there are periods whenastrometric observations towards the Galactic Center direction
are not possible. In such periods, in order to utilize the uniquefeatures of the JASMINE satellite (its capability of highprecision photometric and highly frequent observations in thenear-infrared band), we can plan to carry out transit observations
to search for Earth-type planets that are expected to be in the
habitable zones around M-type stars which are low mass redstars belonging to the main sequence. JASMINE dominates
other missions for explorations of this type of exo-planet.
(2) Major Progress in FY 2022

1) To reveal the Milky Way’s nuclear structure and formation
history by measuring the distances and the motions of stars
located as far as 26 thousand light-years away with highprecision astrometry observations in the near-infrared band.
2) To explore the formation history of the Milky Way related tothe origin of human beings by revealing the evolution of the
Galactic structures, which caused the radial migration of the
Sun and other stars with their planetary systems.
3) To find Earth-like habitable exoplanets, taking advantageof the time-series photometry capability required for the
precision infrared astrometry.
The mission objective of JASMINE is to use an opticaltelescope with a primary mirror aperture of around 36 cm toperform infrared astrometric observations (Hw band: 1.0–1.6μm). A project objective is to measure as the highest precision

064

II Status Reports of Research Activities

1) Organization of the JASMINE Project
The JASMINE Project, NAOJ, is composed of two
Professors, one Project Associate Professor, six AssistantProfessors, one Project Assistant Professor, one Project
Researcher, and one Technical Supporter. Significant
contributions were also made by members of the following
organizations: ISAS/JAXA; Kyoto University; the University ofTokyo; and the University College London, etc.
2) Overview of planning and developing JASMINE
We are establishing a JASMINE consortium consistingof researchers. The purposes of the consortium are to conduct
the science study, and to prepare a data analysis team, data
validation team, and outreach team. At present, about 60
domestic members are participating. In September 2022, we
held a special session for JASMINE at the 2022 Autumn Annual
Meeting of the Astronomical Society of Japan. We were able tolisten to the opinions of many researchers and lectures in a wide
range of fields.
Regarding the development of the satellite and observation
instruments, a comprehensive review of the satellite/instrument
specifications was carried out with the aim of reducing costs andtechnical risks, and then conceptual studies were conducted withsatellite manufacturer company candidates. In addition, we aredeveloping a domestic infrared camera for space in collaboration
with the NAOJ Advanced Technology Center and ISAS/JAXA.
Progress has been made in the implementation of performance
evaluation tests on a prototype detector, the completion of alarge-format prototype detector, the development of an onorbit system for calibrating the sensitivity flatness of pixels on
the detector, and the conceptual study on the structure/thermal
design of the detector box assembly. Regarding data analysis,
we are simulating stellar images in the field to be observed by
JASMINE, using actual stellar observation catalogs covering thearea near the Galactic center, and also we are developing a seriesof end-to-end simulators from estimating stellar image centersin the field to deriving astrometric parameters such as annual
parallaxes. We are proceeding with such analysis consideringvarious realistic and complex noise sources. In international
cooperation, researchers at Heidelberg University visited
NAOJ and deepened discussions on methods of analyzing
astrometric data based on their knowledge of the Gaia data
analysis. Furthermore, discussions on cooperation with the
NAOJ Astronomical Data Center for the creation of an archiveof observational data have started.

utilized in outreach activities in the future.

3) Nano-JASMINEThe JASMINE Project Office, the predecessor of the
JASMINE Project, had also been promoting a plan for a microsatellite project, Nano-JASMINE (with a primary mirror
aperture of 5 cm). Nano-JASMINE aimed to produce scientificresults based on the astrometric information for bright objects inthe vicinity of the Solar System. This plan was terminated dueto the repeated loss of launch opportunities caused by external
factors and the degradation of the flight model (which was tobe actually launched into space) of the satellite (completed in2010). Although the JASMINE Project Office was not able toperform analysis using actual scientific data, we were able toachieve results in the development of a space telescope, thedevelopment of the detector subsystem, the establishment of data
analysis methods, and the development of pipelines for the data
analysis. The original objectives that NAOJ was supposed toachieve were largely achieved. In addition, the Nano-JASMINE
plan also contributed to the promotion of JASMINE because theclose international cooperative relationship with the Gaia teamgained through the development of the Nano-JASMINE data
analysis system has led to the current strong cooperation in thedevelopment of the data analysis system in JASMINE.
The flight model of the Nano-JASMINE satellite will be
exhibited at the Oshu Space & Astronomy Museum, and theengineering model of the satellite, which is almost the same as
the flight model, will be exhibited at the Gifu Kakamigahara
Air and Space Museum. In this way, Nano-JASMINE will be

II Status Reports of Research Activities065

10. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project
1. Project Overview
In FY 2022, the RISE Project first and foremost worked
as the Martian Moons eXploration (MMX) Geodesy Science
Strategy Team (GSST) to continuously investigate theoperation plans of MMX, introduce new software, and support
the manufacture and tests of an onboard instrument. (i) We
regularly had meetings online with the development team ofthe orbit/gravity field estimation software (GINS) produced
by Centre national d'études spatiales (CNES) in France. To
prepare for Landing Site Selection (LSS) training, we jointly
improved GINS by incorporating laser altimeter (LIDAR)
data and landmark data. At the same time, simulations
have been conducted to retrieve the Phobos gravity fieldmodel from the tracking of Quasi-Satellite Orbits (QSO)
at various altitudes. (ii) We attended monthly development
meetings with the manufacturer of LIADR. We also attended
Engineering Model (EM) tests and contributed to the dataacquisition and performance analysis of the response of EM
to various input energies. Further, we contributed to preparing
Spacecraft Information Base version 2 (SIB2) and designing
PI’s Quick Look. (iii) The contract for utilization of thestereophotoclinometry shape-modeling tools (SPC) was attained,
and regular meetings started. In March, the training session
for SPC tools was conducted. (iv) We attended domestic andinternational Science Board meetings and discussed possible
scientific research achievements. (v) We contributed to mid
to long-term operation planning in the Mission Operation
Working Team (MOWT). Also, we incorporated MOWT and
the Mission Operation Preparation Working Team (MOPWT)
to make detailed plans of imaging operations for the shapemodeling considering the spacecraft attitude control, the numberof necessary commands, and the feasibility of MDP processing.
(vi) In the ground Data Processing WT (DPWT), we identified
Level 0 data required for LSS. We investigated interpolation
procedures of the spacecraft attitude data and their accuracy for
LSS. In addition, (vii) we arranged the interface of LSS products
training and confirmed the data processing flow in the Landing
Site Selection Working Team (LSSWT).
Second, we opened the Hayabusa2 LIDAR data to the
public. Regarding scientific achievements, we published a paper
as coauthors on the surface albedo of Ryugu, which used LIDAR
data. On the other hand, the gravitational potential of the column
of uniform density was solved analytically to discuss the topshaped figure of the Ryugu asteroid in view of slope stability
and a change of rotation period. Also, one of the RISE Project
members published a paper as the first author on the laser-link
experiment conducted during the return to Earth of Hayabusa2
with the Institute of Space and Astronautical Science (ISAS)
and National Institute of Information and Communications
Technology (NICT).
Third, we held team meetings of the Planetary Science
Working Group under the Science Strategy Committee and066

II Status Reports of Research Activities

considered the role of planetary explorations in the National
Astronomical Observatory of Japan. We had online meetings
on February 28, May 9, July 4, and September 12 to prepare theWG report and a workshop open to the science community held
in FY 2023. The RISE project was reviewed, and a three-year
extension was approved.

2. Educational Activities
One RISE member educated a fourth-year graduate student
at the University of Tokyo as an advisor. An internship student
at Paris University joined the RISE project for three months tostudy Ryugu crater topography.

3. Outreach/PRIn FY 2022, the Project members volunteered two times
for Kirari Oshu City Astronomy School as well as five times
for FUREAI (Friendly) Astronomy classes. In addition, RISE
members provided four special lectures for the public and one
invited talk in a workshop.

11. SOLAR-C Project
1. SOLAR-C Project Overview
SOLAR-C is a JAXA satellite project under preparation andmay become Japan's fourth solar observation satellite mission
after Hinotori, Yohkoh, and Hinode. The plan is to realize thelaunch in the late 2020s. Through observations from the satellite,
this project aims to elucidate the following mechanisms of solar
magnetic plasma activities, which are significant problems in thefield of solar physics and have an impact on space weather andspace climate around the Earth.
(1) Formation mechanism of the hot solar atmosphere and solar wind(2) Energy release mechanism of solar explosions
The primary science instrument on the satellite has highimaging resolution and sensitivity that are improved by nearly anorder of magnitude compared with the similar instrument on the
Hinode satellite. It also has the feature of being able to observe
the hot solar plasma with temperatures ranging from twenty
thousand to twenty million degrees nearly seamlessly. Japan will
be responsible for the launch vehicle, satellite bus, and telescopesection of the science instrument. The spectrograph section will
be developed through international collaborations with the U.S.
and European space agencies and institutions. NAOJ will play aleading role in the development of the telescope section.
The SOLAR-C project was proposed as the Solar-C_
EUVST small satellite project in the JAXA public small satellite
solicitation opportunity in January 2018. This proposal was
nominated as a candidate for Publicly Offered Small Satellites 3
or 4 in July 2018, and the plan moved to the Mission Definition
Phase (Pre-Phase-A2) in FY 2019. After the pre-project
candidate down-selection pre-screening in February 2020,
this project was selected as the JAXA Small Satellite 4 projectin May 2020. Regarding international cooperation, NASA'sparticipation in this project was decided in December 2020
based on NASA's Phase A study that had been underway since2019, followed by the participation of European space agencies.
After passing the Mission Definition Review in July 2022, theplan became a JAXA Pre-Project and was followed by finishing
the System Requirement Review in December 2022. Afterward,
we have been preparing for the System Definition Review
scheduled in 2023 while proceeding with feasibility studies withoverseas partner organizations.

2. Progress of the NAOJ SOLAR-C Project
Activity in FY 2022
In FY 2022, the feasibility studies of the following aspectsof the telescope section have proceeded using the JAXA frontloading and preliminary design expenses: (1) The design studyof the primary mirror assembly (PMA) with tip-tilt and launchlock mechanisms and development and evaluation of the breadboard model, (2) the selection of an adhesive for use at the
primary mirror support through evaluation, (3) the design ofthe focus adjustment mechanism, (4) a light-weight designof the telescope structure considering equipment layout andintegration, (5) the on-orbit temperature prediction and thermal
deformation prediction of PMA, (6) the design of telescope
control electronics and performance evaluation with the breadboard model of a control process, (7) mechanical interfaceof optical components and optical alignment procedures, (8)the study of optical measurement for the micro-vibration test,(9) the study of mechanical interface conditions between thesatellite and the observation equipment and those within thescience payload, and (10) the investigation of outgassing
characteristics of a candidate skin sheet of CFRP sandwich
panels. Through these design studies, the validity of the design
has been confirmed for some critical items, while some issues in
the initial design have been clarified.
Design meetings with overseas partner institutions wereconducted through internet conferencing, as it was not possible
to hold the design meetings in a conference room due to
COVID-19.

3. SUNRISE-3 Project Support
Most SOLAR-C project members contributed to developing
the science payload and the flight operation of the flight
experiment of the Balloon Project SUNRISE-3 conducted inJuly 2022 in Kiruna, Sweden. Refer to the report of the Solar
Science Observatory (SSO) for details.

4. Educational and Publicity Outreach Activity
The project staff has supervised three SOKENDAI graduate
students. The project also participated in the Tour of the Solar
Research Frontline to introduce domestic solar research toundergraduate students and introduced the project activities in
research and development through the web.

5. Others
While NAOJ reimbursed the NAOJ SOLAR-C project
activity for its general operation and contingencies, the expenses
for the design and development of the telescope section are
funded by JAXA. From the viewpoint of smoothing out theadministrative work volume of SOLAR-C and SSO projects, theexpense processes for the short-term experiment projects wereconducted by this project.
The changes in the project staff are as follows. Y. Kawabata,
Assistant Professor, was appointed in November 2022, and Y.
Nodomi, Senior Specialist, and J. Sugimoto, Administrative
Supporter, left the SOLAR-C project at the end of March 2023.

II Status Reports of Research Activities067

12. The Subaru Prime Focus Spectrograph (PFS) Project
1. Overview of the PFS project
The Prime Focus Spectrograph (PFS) is a next generation
large-scale facility instrument of the Subaru Telescope. PFS
will enable the observation of ~2400 objects simultaneously at
wavelengths ranging from 0.38 µm to 1.26 µm with a spectral
resolution of R ~ 2000–5000. It is expected to start open-use
observation from FY 2024.
PFS has been developed under an international collaboration
led by Kavli IPMU, Tokyo University. The collaborationconsists of Kavli IPMU (Tokyo Univ.), NAOJ, ASIAA (Taiwan),Caltech/JPL, Princeton Univ., Johns Hopkins Univ., North East
Participation Group (8 institutions, USA), Brazilian consortium,
LAM (France), MPE/MPA (Germany), and Chinese PFS
Participation Consortium (6 institutions, China).
The PFS A-project started in FY 2019 at NAOJ. It is
responsible for the design and construction of the telescope
infrastructure needed for PFS, as well as the operation andmaintenance of the instrument. The PFS A-project is also heavily
involved with PFS integration, commissioning, its performanceverification, and the development of the data reduction pipeline
and science database.
The A-project work will lead to the start of PFS operation,
at which point PFS will transition to a Subaru Telescope facility
instrument, and the PFS A-project will be dissolved.

Figure 1: Top view of the spectrograph clean room, hosting 2
spectrograph modules (Jan. 2023).

2. Progress in FY 2022
(1) Subsystems delivery and integration
PFS is composed of several subsystems, starting with
the Prime Focus Instrument (PFI), hosting the ~2400 science
fibers and their individual positioners, at the prime focus of thetelescope. The next subsystem is made of 4 science fiber cables(CableB) running along the telescope. They bring the light to the
4 spectrograph modules (SpS) located in a dedicated clean roomon the upper level of the dome. Each module is composed of 3
cameras, with a blue, red, and near infrared (NIR) channel. The
last PFS subsystem is the Metrology Camera (MCS) located at
the Cassegrain focus of the telescope, imaging and processing
the positions of PFI and each science fiber.
PFS started FY 2022 with PFI and MCS already installed
and tested on the telescope, 2 (out of 4) science fiber cables(CableB) installed, and 1 (out of 4) spectrograph module,
hosting 2 cameras (1 blue and 1 red channel).
In Nov. 2022, the second spectrograph module (with its
2 visible cameras) was delivered from LAM (France) andintegrated (see Fig. 1). It was immediately tested and used onsky during the Nov. 2022 engineering run.
The first NIR camera was installed on the first spectrographmodule in April 2023 and was used on sky that same month.
The last 2 remaining science fiber cables (CableB#3 and#4) were installed in Feb. and May 2023 respectively (see Fig.
2). Both cables passed the initial fiber performance tests, but

068

II Status Reports of Research Activities

Figure 2: All 4 science fiber cables installed on the telescope, holding~2400 optical fibers (May 2023).

long-term stability monitoring is still ongoing to understandthe correlation of optical fiber performance with the telescope
movement, and other environmental conditions such asatmospheric temperature variation.
At the end of FY 2022, ~1200 science fibers (~50 %) werevisible on 5 spectrograph cameras (2 blue, 2 red and 1 NIR
channel).

(2) Engineering observation runs
From May 2022 to April 2023, 49 engineering observationnights were approved for PFS and 33 nights were used. There
were 10 nights lost to bad winter weather and 6 nights lost totechnical issues with the PFS instrument or the telescope itself.
PFS first engineering light was detected in Nov. 2022, withthe successful alignment of the science fibers on stars and thedetection of their spectra using the first spectrograph module. In
April 2023, the first NIR camera took on-sky data for the firsttime (see fig. 3).
Beyond the instrument first light, the engineeringobservations have been crucial to get a better understanding of
the instrument, including among others:• Understanding the MCS and PFI reference frames andalignment.
• Testing and integrating the auto-guiding cameras to thetelescope systems.
• Optimizing the fiber positioners’ convergence speed andaccuracy.
• Verifying the performance of the spectrographs (including thefirst NIR camera).
• Characterizing the PFS instrument.
• Taking calibration and commissioning data and testing theprocessing pipeline.
• Testing and optimizing the nighttime operation in collaboration
with support astronomers.

help the observatory optimize the PFS observation efficiency.
Such software includes, among others, a tool used to create the
PFS fiber configuration files used for each exposure, the Queue
Planner (qplan) for creating the nightly schedule during queue
mode observation, and the PFS pointing planner (PPP), which
optimizes the telescope pointing to efficiently execute multiple
observing programs in the same exposures (fiber-sharing). An
online version of the PPP was also released to assist PIs with
their proposal submission.
(4) Data reduction pipeline
The PFS team at NAOJ has been continuously contributing
to the data reduction pipeline (DRP) in close collaboration with
Princeton University and other PFS collaborators. NAOJ’s
contribution is the flux calibration part of DRP and an earlyversion was integrated into the pipeline. It has been tested using
data from the Nov. 2022 engineering observation. An importantfunction of the pipeline is to check the quality of processeddata and we made progress in this aspect as well. In particular,
quality assurance tests of detectorMap, which describes the fiber
position and wavelength, can now be made routinely. Anothercontribution to the PFS collaboration is the stable operation of
the science database, which was in use throughout FY 2022.

(3) Observation procedures and policies
In FY 2022, a lot of progress has been made on the openuse observation framework, including on various processes
from the PI proposal submission, through the ranking, to thetime allocation; queue vs. classical mode observation; and data
access. The scientific community at large was able to provide
feedback on the observation procedures during the Subaru usermeetings and dedicated community meetings. The resulting
basic observation framework was presented to the Subaru
Science Advisory Committee (SAC) and agreed upon with theobservatory in Nov. 2022.
Several software tools have been successfully developed to

Figure 3: ~1200 night-sky background spectra detected on the first two
spectrograph modules, including the first NIR camera.

II Status Reports of Research Activities069

13. The Subaru Ground Layer Adaptive Optics (GLAO) Project
1. Project Overview
ULTIMATE-Subaru is a survey instrument that will
enable unprecedentedly wide-field and high-sensitivity survey
observations with a high resolution comparable to the Hubble
Space Telescope. The Subaru Ground Layer Adaptive Optics(GLAO) project aims to develop a GLAO system as a part of
ULTIMATE, which will uniformly improve the seeing by afactor of 2 over a wide field of view up to ~20 arcmin in diameter.
A primary science goal of ULTIMATE is to reveal the historyof galaxy formation and evolution by an unprecedented nearinfrared survey of the distant Universe.
In FY 2019, the GLAO project was accepted for the NAOJ
call for A project proposals and has started the preliminary
design phase. In the A-project period, the GLAO project aims tocomplete the preliminary design of the GLAO system and theprototyping of the key subsystems within 3 years, followed by
final design, production, assembly, integration, and test phases.
The GLAO project plans to implement the GLAO system at theSubaru Telescope and start its commissioning run by the end of
FY 2028.

2. Staff
The GLAO project team mainly consists of members ofSubaru Telescope. At the end of FY 2022, there were 1 associate
professor and 1 research fellow dedicated for the GLAO
project. There were also 1 affiliated associate professor, 1 seniorspecialist, 2 assistant professors, 1 research engineer, and 2
RCUH employees (engineering staff) appointed concurrently.
There was also one associate professor at the Advanced
Technology Center who participated in the GLAO development.
In addition, the GLAO project received support from the
instrument division technicians, day crews, and administration
staff at Subaru Telescope.

3. Major Progress in FY 2022
Based on the results from the conceptual design review for
the ULTIMATE science instruments, which was completed in
FY 2021, we decided to concentrate on the preliminary designof the GLAO system at the Cassegrain focus, which will realize
the main science goals by using a near-infrared wide-field
imager (WFI) at the Cassegrain focus covering 20 arcmin FoV
in diameter. The development of GLAO for MOIRCS at the
Nasmyth IR platform will be suspended until future plans for
the Nasmyth IR platform are determined based on community
demands, as the existing instruments on the Nasmyth IR
platform need to be decommissioned.
The GLAO preliminary design has been completed for the
wavefront sensor (WFS), the laser guide star facility (LGSF),
and the control system. Since the final design of the adaptive
secondary mirror (ASM) was completed in FY 2021, we

070

II Status Reports of Research Activities

started production of the thin shell mirror, which is the main
optical component for the ASM. In FY 2022, we established a
production process, procured the material for the shell mirror,
and fabricated a production jig.
There was a preliminary design review for the GLAO system
in November 2022. We received a review report from the review
panels in February 2023 that endorsed the project to move
forward to the next final design phase with some suggestions toimprove the project.
To demonstrate the technology in the GLAO system, we
have been conducting the upgrade of the Laser Guide Star (LGS)
system for the existing AO system at the Subaru Telescope with
the TOPTICA high-power laser. In FY 2022, we completed
the performance evaluation of the laser guide star systemand obtained the wavefront data using the proto-type ShackHartmann wavefront sensor (SH-WFS) developed by Tohoku
University. We also developed an atmospheric turbulence profiler
in collaboration with Tohoku University to measure the groundlayer atmospheric turbulence, which is crucial for the GLAO
performance. We conducted the initial observation with the
turbulence profiler at the Nasmyth OPT platform of the Subaru
Telescope.

4. Education Activities and Internships
In FY 2022, the GLAO project accommodated two internstudents under the supervision of the research and education
staff. As a part of the SOKENDAI summer student program,
we mentored a 3rd-year undergraduate student from Kwansei
Gakuin University to perform research related to instrument
development. We also mentored a student from the Universityof Hawai`i at Hilo for 4 months as an intern through the Hawai`iSpace Grant Consortium (HSGC) program to provide researchexperience on observational studies of galaxies. In addition,
we hosted four graduate students from Tohoku University
and one from Sokendai staying for 1–2 months at the Subaru
Telescope to conduct research related to the turbulence profiler
or observational studies of galaxies.

5. Outreach
To inform the astronomical community and general public
about the Subaru GLAO project and its scientific motivation andgoals, we released news from the project on a public web site(https://ultimate.naoj.org). In FY 2022, the “Subaru Telescope2.0” project was officially launched and a special web page forthe “Subaru Telescope 2.0” project has been released on the
Subaru Telescope official website. ULTIMATE-Subaru was
highlighted on the Subaru Telescope 2.0 web page.

6. International Collaboration
The ULTIMATE science team is playing a central rolein promoting the activities of the JSPS core-to-core program,“International research network toward the era of deep and widenear-infrared survey of the universe with space and groundbased telescopes (as known as SUPER-IRNET)”. This programaims to significantly advance the next-generation near-infraredwide-field observation program, including ULTIMATE, throughthe collaboration of Japan, the United States, France, Australia,
and Taiwan. In FY 2021 and the first half of FY 2022, a seriesof six online seminars was held, despite the fact that face-toface meetings among researchers were largely limited due to
COVID-19. In March 2023, the first face-to-face workshop“Near-Infrared Wide-Field Deep Space Exploration in the
Universe I (SUPER-IRNET 1st Plenary Seminar)” was held withover 100 participants from the five partner countries.

II Status Reports of Research Activities071

14. Astronomy Data Center
The Astronomy Data Center (ADC) collaborates withobservatories and universities to consolidate astronomical
obser vation data. ADC archives them per manently andopens them to the astronomy community in a user-friendly
way together with the data analysis environment to facilitate
scientific research. To sustain and develop these activities andfunctionalities in the future, and to serve as a cross-project
organization that supports various projects and observatories
in NAOJ through the sharing of human, computers, scientific
data assets, experience, and technology, we are restructuring
the organization. As part of this effort, following an associatesenior research engineer in the Data Archive Group hired in FY
2021, a new research engineer was hired in FY 2022 to provide
technical support to the Data Application Infrastructure Group.
The rental computer system installed in March 2018,
which has been used as an open-use data analysis systemand data archiving systems, was to be renewed after five
years of operation, but a contract was not signed because ofhigh computer prices and long delivery times caused by asemiconductor shortage. Therefore, the operation of the current
system has been extended until the end of June 2024, and the
procurement procedure for a replacement is still underway.
The major activities in ADC are described below.

1. SMOKAThe SMOKA team has been conducting research anddevelopment on astronomical Databases, Data Archiving, andData Analysis. SMOKA (https://smoka.nao.ac.jp/) publishes
archival data of Subaru Telescope, Okayama 188-cm telescope,
Kiso 105-cm Schmidt telescope (the University of Tokyo), two
MITSuME 50-cm telescopes (Tokyo Institute of Technology),
Kanata 150-cm telescope (Hiroshima University), NAYUTA
2-m telescope (University of Hyogo), and Seimei 3.8-m
Telescope (Kyoto University).
SMOKA continues to operate stably in cooperation withthe various observatories and has produced many scientificresults. SMOKA is also a research infrastructure that allows forthe revalidation of research results and supports the credibilityof research results.
The total amount of opened raw observation data in
SMOKA is about 38 million frames (397 TB) as of May 2023.
SMOKA contributes to many astronomical publications.
The total number of refereed papers using SMOKA data is
281 including 10 new publications in FY 2022 as of March
2023. The name “SMOKA” is specified as a source of “DataAvailability” on many other papers. Object frames taken withthe observing instruments TriCCS on the Seimei Telescopewere newly opened in FY 2022. Transmission of huge amountsof data produced by Tomo-e Gozen (Kiso Observatory) and
TriCCS were regularized with a combination of hard disk
transfers and internet transfers.
We are operating a system that makes original all-sky

072

II Status Reports of Research Activities

monitor images at Higashi-Hiroshima, Okayama, Akeno, andKiso available to the public (https://ozskymon.nao.ac.jp/ ; 34
TB as of May 2023). A system to publish digitized data fromphotographic plates taken at the Kiso Observatory several
decades ago was developed and operated (https://pplate.
nao.ac.jp/ ; 4 TB). A data service of Tomo-e Gozen (Kiso
Observatory) stacked data was also being operated (https://archive.nao.ac.jp/tomoe ; 95 TB as of May 2023).
Two papers were published in the Report of NAOJ volume
23 on the development of the SMOKA/Tomo-e Gozen archive
system and on the acceleration of astronomical databasesearches.

2. MASTARS
The operation of MASTARS, a data archive system in
Mitaka for Subaru Telescope observers, was transferred to
ADC working closely with the STARS data archive system
in Hawai`i. As the amount of stored data increased, we setup
a new storage server for expanding the data area and started
operation in FY 2022. We also supported the upgrade of thearchive systems due to the renewal of the IT system in the
Subaru Telescope. Software tools (gitlab, redmine, etc.) wereintroduced and operated for use in development and upgrades.
In addition, we are preparing the data backup on acommercial cloud for data preservation in the case of disaster.

3. JVO (Japanese Virtual Observatory)
Detection of atomic and molecular emission lines was
perfor med on the published ALMA FITS data, and theinformation on the detected lines was put into a database andpublished. In FY 2022, radial velocities for individual target
objects were retrieved from the SIMBAD database, and thefrequencies of the detected lines were then converted to the rest
frame of the object. Previously, only the information from the
FITS header was used, but since it is sometimes inaccurate, we
attempted to use the SIMBAD database. The rest frequencies
of detected lines based on both radial velocities were madeavailable to users.
The size of the publicly available ALMA FITS data perfile now exceeds 300 GB, and in the future, over 1 TB of data
will be available. We have developed FITS WebQL, which
implements a distributed processing mechanism to show
the contents of such huge data cubes on the web browser
interactively at high speed without downloading. A totalof five computers read FITS data in parallel and synthesize
images, enabling even 1 TB of data to be displayed within a
few minutes. We also confirmed that the spectrum calculated
at any position on the image plane can be smoothly plottedin real time. For data over 20 GB, this function was madepublicly available for anyone from the JVO portal service. The
development status of the FITS WebQL was presented at the2023 Spring Meeting of the Astronomical Society of Japan.
In addition, several data catalogs of JAXA's scientificsatellite AKARI were registered in the JVO system and started
to be made public through the VO interface.
The number of accesses to all these JVO services in FY
2022 was 7.4 million and the total download volume was 12
TB.

4. HSC Data Analysis/Archiving Software
Development
We continued to develop data analysis pipeline software
to process Hyper Suprime-Cam (HSC) data accurately andefficiently, conducted data analysis, and developed and operated
data archiving systems to make effective use of the processeddata.
In the Subaru Strategic Program (SSP) with HSC (March
2014-), we have been analyzing the data with the developed
pipeline and producing databases to store the processed
results for researchers. The originally scheduled HSC-SSP
observations were completed in December 2021, and the total
full-color full-depth survey footprint has reached over 1000
square degrees. We plan to process all obtained data withan updated pipeline for the next (11th) data release for SSP
collaborators. As the structure of the pipeline has been largely
updated since the last data release, we have spent this fiscal
year on preparation of the processing platform, execution of atest production run, and getting feedback from collaborators'
evaluations. We experienced a relatively large system update.
Nevertheless, we have maintained the data service functions
and continued developing various user interface software forproviding images and catalog products.
In addition, development to apply next-generation
database technology to a high-speed search service for hugeastronomical catalogs such as HSC-SSP is continuing afterminor updates to the collaborative framework.
We have been involved in establishing data formats for PFS
and developing and testing a science archive for PFS linked to
the HSC data products in cooperation with Subaru Telescope.

We have been constructing and upgrading the “Large-scaledata analysis system (LSC)” for analyzing big astronomical
observation data taken with instruments like HSC. The LSC
system has been in operation for general HSC observers
since September 2019, the scope of users was expanded toresearchers who wish to analyze HSC archival data in October
2020, and was further expanded to those who want to analyze
observation data taken with any other instruments in January
2022.
Several workshops and hands-on tutorials were held withNAOJ projects to demonstrate to users how to use the specificsoftware, applications, and the open-use systems. Due to the
spread of COVID-19 from the winter of 2020, all workshops
in FY 2020 and FY 2021 were held online, but in FY 2022,
more workshops were conducted in a hybrid or face-to-faceformat at NAOJ. The dates and numbers of participants for theworkshops in FY 2022 are as follows.
1. ALMA Data Reduction Workshop (1st, Co-host), July 5 and7, 2022, 10 users
2. SOKENDAI Summer Student Program (provided analysis
computers), August 1–31, 2022, 8 users
3. Subaru Telescope Data Analysis Workshop (Co-host),
November 28–30, 2022, 11 users
4. ALMA Data Reduction Workshop (2nd, Co-host), February
27 and 28, 2023, 10 users
5. JAPAN SKA Data Analysis Workshop (Co-host), March
2–6, 2023, 12 users

5. Open-use Computer Systems and Services
Open-use of the data analysis computer system forastronomical research is one of the key services provided
by ADC. The “Multi-Wavelength data analysis subsystem(MDAS)” procured under a rental contract has been in
operation since March 2018. Since MDAS is scheduled to stop
operation at the end of June 2024, we are currently preparing
for the procurement and construction of the next system. A
temporally disk space (1 Petabyte of network file system) was
added to the system so that it can be used as a data storage
space when migrating to the next system.
Open-use terminals and printers installed in two openuse computer rooms (Subaru and ALMA buildings) in Mitaka
Campus were sequentially replaced with new equipment after
March 2023.

II Status Reports of Research Activities073

15. Advanced Technology Center
1. Summary of Activities in ATC
The Advanced Technology Center (ATC) is the coreresearch organization of the technological development at the
National Astronomical Observatory of Japan (NAOJ), andis the research and development (R&D) center for advanced
astronomical observation instruments, from radio waves tovisible and ultraviolet light, both on the ground and in space.
In FY 2022, although no ‘priority measures to prevent the
spread of the virus’ were issued, operations were carried out
while taking thorough measures to prevent infectious diseases,
including telecommuting.
The reorganization into a matrix-type organization (seeFigure 1) entered its second year of operation and has been
substantially put into practice. In the process, for the first time,
we carried out screening for accepting or rejecting job requests
from outside projects.
Even with the corona disaster still continuing, facility
tours have recovered to pre-corona disaster levels. We wereable to stress the importance of ATC in NAOJ for the ItalianAmbassador to Japan; Chilean Ambassador to Japan; Lebanese
A mbassador to Japan, executives of overseas research
institutes; visitors from the Cabinet Office, METI, and MEXT
such as the State Minister, Administrative Vice Minister, andso on; executives of the National Institutes of Natural Sciences;private companies; etc.; and online visits by students.

Notable items in FY 2022 include the completion of
the expansion of the SIS clean room for the development ofsuperconducting devices for ALMA2 development, as well as
the establishment of rules for the security control of electronic
devices produced there and the building of a new storage area.
In addition, we have been actively engaged in industrial
collaboration activities to apply the technologies developedat ATC to industrial applications, including the developmentof a microwave amplifier with ultra-low power consumption
applicable to quantum computers and the study of industrial
applications of adaptive optics technology used in the Subaru
Telescope. In FY 2022, we prepared for the launch of the “Social
Implementation Program” to promote these activities as ATC.
Details of the activities in FY 2022 are described below.

2. Developments for Prioritized Projects(1) TMT Instruments
1) Infrared Imaging Spectrograph (IRIS)
The IRIS Imager team in ATC continued to study theissues raised at the IRIS Imager Final Design Review held in
June 2021, as they did in FY 2021. System-level analysis anddocumentation have been conducted in preparation for the IRIS
system-wide Final Design Review scheduled for FY 2024. The
former involves the creation of an FEA model for vibration

Figure 1: Matrix organization structure of ATC.

074

II Status Reports of Research Activities

analysis integrating NFIRAOS adaptive optics and IRIS andthe derivation of transfer functions, the creation of a model for
opto-mechanical thermal analysis, and the demonstration of a
prototype mechanical I/F with the cryostat; the latter involves
system-level FMEA/reliability analysis, and requirement
definition through simulations towards the preliminary design ofan optical simulator to be used for performance evaluation of the
Imager and IFS.
In June 2022, the IRIS international team was informedthat the H4RG-10 detector from Teledyne, USA, which was tobe used in the IRIS Imager, was discontinued. As the Imager
interfaces with the IFS and cryostat for which the USA is
responsible, the impact of a change in detector would have awide-spread impact on the instrument; the IRIS Imager team in
ATC led a trade study with an alternative detector, the H4RG-15.
2) Wide Field Optical Spectrometer (WFOS)WFOS has moved to a preliminary design phase. In FY
2022, ATC contributed a trade study led by the California
Institute of Technology on the slit mask unit based on our design
study of the slit mask exchange mechanism. In addition, ATCinvestigated the manufacturability of high-quality large glassblanks and volume binary gratings which have high diffraction
efficiency. ATC has studied an integral field unit (IFU) as a
future upgrade. In FY 2022, we carried out the optical andmechanical designing.
(2) ALMA
1) ALMA Receiver Maintenance
NAOJ is in charge of the maintenance of the cold cartridge
assemblies (CCAs) for three receiver bands - Band 4 (observation
frequency: 125–163 GHz), Band 8 (385–500 GHz), and Band
10 (787–950 GHz) - for ALMA. By FY 2013, a total of 219
CCAs which had been developed and manufactured at NAOJ,
or 73 units including 7 spares for each band, were shipped to
the ALMA site. Most of the receivers have been installed andoperated in the ALMA antennas for scientific observation. At
ATC, the ALMA receiver maintenance team has been repairing
the receiver cartridges that failed during operation since FY 2014.
In FY 2022, two Band-4 receivers and one Band-10 receiver
were repaired and delivered to the ALMA Operations Support
Facility (OSF) in Chile. The receivers installed in antennas
and scheduled to be repaired are one Band-4 and one Band-10
receiver. They will be removed from the receiver systems in thecourse of regular maintenance and will be returned for repair in
FY 2023 or later. Although the frequency of repairs caused byaging failure is currently kept low, an increase of the failure ratecannot be denied when the wear failure period begins according
to the bathtub curve. In order to continue the stable operationof ALMA, it is important to maintain a maintenance system in
ATC that can quickly respond to ALMA receiver failures. The
ALMA receiver maintenance team in ATC worked together witha resident engineer in Chile, who experienced the production of
the receivers in Japan, to support the Joint ALMA Observatory
for solving the problems for smooth operation of ALMA.

2) ALMA receiver development and upgrades
Cont i nu i ng f rom F Y 2021, we a re suppor t i ng t hedevelopment of ALMA Band 1 and Band 2 receivers andare studying with the Microfabrication Lab. and the ALMA
project to develop broadband heterodyne receivers for ALMA2,
which will significantly improve the telescope’s performanceand functionality. In addition, a development study of a datatransmission system for future implementation in ALMA2 wasstarted in FY 2022.
2-1) Receiver development for Bands 1 and 2
The Band 1 project (35–50 GHz), led by Academia Sinica
Institute of Astronomy and Astrophysics (ASIAA) as acontribution to East Asia ALMA, completed its production
phase. We have been contributing to the testing and productionof corrugated horns; the support for cryogenic maintenance of
cryocoolers at ASIAA; support for procurement and shippingof several important components; and support for shipment ofreceivers in cooperation with the NAOJ ALMA project. The
production and performance verification of the Band 1 cartridge
receivers in Taiwan has proceeded as planned, and the in-house
testing and shipment of all receivers, including spares, werecompleted within FY 2022. Integration of the receivers in thetelescope in Chile is ongoing.
NAOJ will also take responsibility for the maintenanceof the Band 1 receivers in the operation phase from FY
2023, in parallel with the Band 4, 8, and 10 receivers, andtherefore, the maintenance team for the Band 1 receivers andrebuilding equipment is being established in ATC, taking
over responsibility from ASIAA in the post-production phase.
Three NAOJ staff members have visited the Band 1 facility in
Taiwan to learn the procedures for the inspection, assembly, andverification of the receivers to be shipped and to check the test
equipment for transfer to NAOJ. This visit was helpful to plan for
the transferring and upgrading of the test equipment and storing
the spare cartridges and parts.
For the Band 2 (67–116 GHz) receiver being led by theEuropean Southern Observatory (ESO), NAOJ is contributing to
the design of the optics system and the design, manufacturing,and testing of optics components. The Critical Design Review(CDR) meetings were held in April and November of FY 2022
and were passed. In the evaluation of the pre-production receiver,
two NAOJ staff members participated in the integration of thefirst receiver into the ALMA cryostat, which was conducted
in Chile from February to March 2023. We have verified theinstallation method and procedure of the warm optics, for which
NAOJ is in charge, and witnessed the testing of the receiverto identify risks and improvements toward the production andintegration. In addition, we published a paper on the material
characterization system with a high-precision analysis method
for extracting the physical properties of dielectric materials usedin quasi-optical lenses for Band 2 receiver optics.
2-2) Development for the next generation projects
Development of wideband receiver technology is underway
to improve the performance of receivers. In FY 2022, the optics

II Status Reports of Research Activities075

and waveguide circuits of the currently installed ALMA Band
8 receiver were analyzed in detail to identify improvements anddevelop a conceptual design for the upgrade. We also evaluatedthe performance of the fabricated corrugated horn and waveguide
orthogonal transducer, and obtained results showing a significant
improvement in performance over the currently installed Band
8 components. As for wideband microwave components for use
in the intermediate frequency band, we started development of acryogenic isolator with a company, and also the development ofa hybrid coupler in collaboration with the University of ElectroCommunications.
In the development of the terahertz receiver system, asilicon substrate with an antireflection structure fabricated in
FY 2021 was mounted on a receiver as a vacuum window, andits performance was characterized. As a result, we obtained asimilar performance in terms of beam characteristics and noise
temperature as the vacuum window using a quartz substrate,
which is currently used in ALMA. For the development ofmulti-beam receivers, the research and development of asuperconducting monolithic microwave integrated circuit(MMIC) was continued, and the transmission line loss of thesuperconducting circuit and its effect on the sensitivity were
investigated.
2-3) Data transmission system
The upgrade of the current ALMA data transmission
system, called DTS hereafter, is implemented as part of the
ALMA development roadmap, in particular, as part of the
Wideband Sensitivity Upgrade. Together with the National
Radio Astronomy Observatory (NRAO) and Korea Astronomy
and Space Institute (KASI) we submitted the phase 1 project
proposal to the ALMA board and it was approved in November
2022. The design of the DTS is in progress for the Preliminary
Design Review (PDR) scheduled for Q2 2024. NAOJ has led the
project since then and has developed the design. The interface
meeting was held among the development teams of the DTS,
Digitizer (which delivers the observation data to the DTS), andthe second-generation Correlator (which receives the data fromthe DTS), in February 2023. The essential parameters as thedesign basis for DTS were approved in the meeting: the datatransmission speed of 400 Gbps and the maximum data amountof 1.2 Tbps. A cooperative research agreement was concluded
with the Photonic Network Laboratory and ICT Testbed Researchand Development Promotion Center of the National Institute ofInformation and Communications Technology (NICT). In thiscontext, the experiment for long-range data transmission by 400
Gbps optical transceivers was performed in the optical fiber
link deployed between Koganei and Otemachi, Tokyo. The key
specifications on the loss and length of the optical fiber link wereobtained by the experiment.
(3) KAGRA
In collaboration with the Gravitational Wave Science
Project, we are developing vibration isolation systems (VIS) andauxiliary optics systems (AOS) of the KAGRA interferometerand preparing instruments for evaluating the performance

076

II Status Reports of Research Activitiesof new mirrors. At the Kamioka site, rapid progress is being
made in overhauling KAGRA to enhance the performance ofthe laser interferometer, in preparation for the 4th international
observation run (referred to as O4), which will start in May
2023. For the AOS device, ATC has responded to this bycontributing to the improvement and delivery of the opticalangle sensor covers and optical filter holder mechanism; theimplementation of the middle-size baffle; and the design andinstallation of other stray light mitigation mechanisms. For the
VIS device, emergency measures were taken to address thetraverser malfunction, then finalization and evaluation works
were conducted on various suspensions. Furthermore, ATCcontributed to various commissioning works for the whole
KAGRA interferometer, including the assembly of the piezoequipped steering mirrors, as well as the design and installationof the optical bench windbreak. In addition, towards upgrade
works for the 5th observation run, the production and evaluationof the folded pendulums, a core device for the acceleration
sensors, were also carried out. Also, the conceptual design for a
new compact vibration isolation device is ongoing. Maintenanceand upgrading of the mirror evaluation system has been
continued from FY 2021.
(4) SOLAR-C: satellite for a high-throughput solar EUV
imaging spectroscopy
ATC has assisted in revising the specifications for thetelescope section of the SOLAR-C instrument, coordinating
mechanical and ther mal interfaces for the optical andelectrical assembly provided by foreign partner institutes,
and cooperating to build a baseline optical alignment plan.
In addition, ATC has assisted the preparation of clean room
facilities, including vacuum chambers of various volumes andcontamination monitoring systems, which are to be used during
the development phase of the SOLAR-C project.
(5) Infrared Astrometric Observation Satellite JASMINE
ATC is in charge of developing detectors for imaging
and a detector box assembly (DBA) for holding and coolingthe detectors. The development of near-infrared detectors
using InGaAs devices is being carried out by the Optical
Infrared Mission Instrument Team of the Advanced Mission
Instrumentation Group. The status of the development in FY
2022 is described in section 3(1). The DBA, on the other hand,is being developed by the Thermal and Mechanical Design
Team of the System Design Group. A radiator facing deep
space will cool the DBA detector head down to ~200 K, andthen Peltier devices will cool the detectors down to ~170 K.
In FY 2022, as a conceptual study of the DBA, the teamevaluated the performance of a candidate Peltier device in sucha low-temperature environment (~200 K), and proceed with
DBA thermal and structural design based on the evaluatedperformance. ATC has also supported the conceptual studyof the JASMINE telescope, especially contributing to theclarification of telescope specifications and verification
test plans based on experience acquired in the telescope
development of the Hinode satellite.

3. Advanced Technology Development(1) Near-infrared Image Sensor
Image sensors used at large scale observatories like theSubaru Telescope require extremely high performance such as
high sensitivity, low noise, and large format. For a long time, ouronly choice was to purchase image sensors for astronomy froma company in the USA. Especially, it was more difficult to haveimage sensors for space use, since sensors for space use require
extra specifications such as radiation tolerance and higher
reliability. Image sensors are generally used in all astronomical
instruments, and we cannot continue observational astronomical
projects without high performance image sensors. We havesuccessfully developed near-infrared image sensors for groundbased astronomy in cooperation with a domestic company. FromFY 2021 to FY 2022, we developed an image sensor widely
applicable to astronomical space missions funded by the JAXAISAS’s front loading program based on the sensor we havedeveloped. In FY 2022, we evaluated a small format prototype
sensor made last year with good results as we expected. We also
manufactured the first prototype sensor of the large-format, nearinfrared image sensor as we planned at the project beginning in
FY 2021. We will evaluate the large format sensor in FY 2023.
(2) Technologies for integral field spectroscopy
Integral field spectroscopy (IFS) enables us to obtain
spectra over an entire field of view in one exposure, which issuitable for studies on extended objects such as galaxies. Owing
to this feature, IFS is becoming one of the major observing
methods in optical and infrared astronomy. An integral field
unit (IFU) is a key optical module realizing IFS. Generally, theIFU is a complex optical system requiring high precision, andtherefore there are few institutions developing an IFU. ATC
has developed basic technologies for the IFU and supported
IFU developments in NAOJ and Japanese research institutes.
ATC is now developing an IFU to verify the basic technologies
developed so far, and plans to conduct a test observation using
it. In FY 2022, we carried out optical designing of the IFU.
In parallel, we conducted optical and mechanical designingof the WFOS IFU. In addition, although the University ofTokyo, RIKEN, and NAOJ completed an IFU for the nearinfrared imaging spectrograph, SWIMS, in FY 2021, we foundghost images in the data taken in a commissioning run. In FY
2022, ATC investigated and identified the cause. After an easy
refurbishment, the ghost images were dramatically suppressed.
(3) Adaptive Optics Technology
Adaptive optics, which enhances the accuracy of imaging
or spectroscopy, is recognized as an important technology inastronomy. The basic studies for adaptive optics are in progress
at ATC. In FY 2022, an experimental adaptive optics system
was prepared and investigations on wave front sensing were
newly started on the phase contrast wave-front sensing andphase diversity. The phase contrast wave-front sensor basedon Zernike’s phase-contrast interferometry enables a straightforward way to measure the distribution of optical phase andhas a good accuracy at low light levels. Such enhancements towavefront sensing in adaptive optics down to photon counting
low illumination will expand the ability of astronomical
observations. The phase diversity method is expected to havegood accuracy down to several nanometers of optical phase. The
use of the aforementioned adaptive optics is being considered as
an experimental light source for the quantitative analysis of thephase diversity method by modulating the wave front phase athigh level accuracy.
Recently, the expectations for the various applications ofadaptive optics are increasing with the paradigm of ‘social
implementation.’ The characteristics of the experimental
adaptive optics above are evaluated regarding air turbulence,and the actual dynamic correction by the adaptive optics isdemonstrated for enterprise and forum.
(4) Terahertz Technology
The terahertz experiment group supports development ofsuperconducting detectors, cryogenic electronics, and cryogenic
systems. In FY 2022, an optical cryostat was furnished forlaboratory evaluation of terahertz intensity interferometry. A
0.8-K sorption cooler successfully cooled SIS photon detectors
down to 0.8 K. Superconducting magnets and magnetic shields
enable stable operation of the detectors. Dual-stage sourcefollowers on cryogenic stages reduce the output impedance of thedetector signal for wide bandwidth readout. A room temperature
optical assembly made with the 3D metallic printer enables
optical experiments using terahertz intensity interferometry
with a baseline length of 100–500 mm using a 600-mm aperture
spherical mirror (R = 4800 mm) and a blackbody source. Opticalexperiments with 600-GHz SIS photon detectors started aroundthe end of the fiscal year.
MKID camera development in collaboration with the
University of Tsukuba realized observation of star-forming
regions at 100 GHz with the Nobeyama 45-m telescope, whose
scientific results were presented in the Astronomical Society
meeting and workshops.
The antarctic ast ronomy prog ram was promoted incollaboration with the University of Tsukuba, Kwansei Gakuin
University, and National Institute of Polar Research. An
astronomy observing program of the galactic plane at 500-GHz
and an intensity interferometry experiment were selected in thegeneral observing program during 2023–2027 within the Xth(10th) Polar Campaign of NIPR.
(5) US-Japan Solar Flare X-ray Focusing Imaging-spectroscopic
Sounding Rocket Experiment: FOXSI-4
FOXSI-4 is being prepared for launch in the spring of 2024.
ATC is supporting the development and evaluation of high-speed
cameras for soft X-rays using back-illuminated CMOS image
sensors and a pre-collimator fabricated by the metal 3D printer.
In FY 2022, a box that houses the electric boards of a high-speed
camera for soft X-ray was machined from aluminum. In order todissipate heat generated by the camera, this box is designed sothat the heat sink attached to the electric board is in close contact
with the bottom of the box. Vibration tests were conducted with

II Status Reports of Research Activities077

the electric boards installed in the box, and it was confirmedthat the boards can withstand the vibrations at the time ofrocket launch. For the pre-collimator, jigs for evaluation tests
were fabricated. These items were fabricated by the Additive
Manufacturing Engineering Team of the Manufacturing DesignGroup.
(6) Balloon-borne Solar Observatory: SUNRISE-3
After completion of testing at the Max Planck Institute for
Solar System Research (MPS) in FY 2021, pre-flight imaging
performance, polarization calibration, and solar pointing wereverified in Kiruna, Sweden, from April 2022. On July 10, 2022,
SUNRISE-3 was launched, but we terminated the operation
5 hours after the launch because of the gondola failure. Afterthe retrieval, we confirmed that the instruments were in goodcondition. We plan to repair the defective part of the gondola
and re-fly SUNRISE-3 in 2024. We published a peer-reviewed
paper on the results of optomechanical design and analysis, scan
mirror mechanism, and high-precision polarization calibration
obtained in the development of the SCIP near-infrared spectropolarimeter.

4. System Design GroupThe System Design Group designs and develops instrumentsfor various astronomical projects and supports the planningand implementation of instrument performance verification.
The System Design Group consists of three teams: thermal
and mechanical engineering, optics engineering, and sensor
engineering. In FY 2022, as in the previous fiscal year, we
continued to respond to requests from projects both inside andoutside NAOJ, and worked on instrument development, focusing
on design work. In addition, one experienced engineer wasadded to the optics engineering team to augment the optical
testing capability.
(1) Thermal and Mechanical Engineering TeamThe team continued the mechanical design and related testsof TMT/IRIS, TMT/WFOS, TMT/STR, KAGRA, SOLAR-C(EUVST), SUNRISE-3, and JASMINE from FY 2021. In
addition, the mechanical design of mirror holders for SAND andthe conceptual mechanical design of the field spectrograph for
TriCCS was newly started in FY 2022.
TMT: For TMT/IRIS, we addressed the issues raised at the
final design review meeting (FDR1). In preparation for FDR2,
we conducted thermal and structural analyses using the Imager
finite element model, studied maintenance plans, designed thefirst lens mount for the Pupil-Viewing Optics, and investigated
the impact of detector changes on the mechanical design. For
TMT/WFOS, the conceptual and basic design of the WFOSIFU optical element holders and adjustment mechanisms were
performed, and the space envelope was confirmed. In the SMXCSU trade study, operational costs for mask manufacturing
were calculated and reported. TMT/STR finalized the interface
documentation and updated the structure model and assembly
drawings for the production manufacturing readiness review

078

II Status Reports of Research Activities

meeting. The Production Readiness Pre-Manufacturing Review(2,3) was conducted and passed for the majority of the Nasmythand Elevation structures.
KAGRA: KAGRA added, improved, and installed hardware
for the auxiliary optics and vibration isolators on site, and madefinal adjustments and confirmations for the O4 observations foreach vibration isolator. In addition, a sapphire mirror shipping
container was designed and the container was provided to
KAGRA for overseas transportation of the mirror for polishing.
Space Instrument: For SOLAR-C (EUVST), we supported
the exchange of structural IF information between the Japanesemanufacturer in charge of the telescope for the mission and theoverseas organization in charge of the onboard instruments,
especially the sharing of design progress and mathematicalmodels. In addition, we have collected constraints on the AITV
instrument system and proposed a measurement configuration
for use in the USA. In JASMINE, we have developed a thermal
structure design to meet the requirement of redundant coolingelements (TECs) in the conceptual study of the detector box.
Elemental testing and test planning continued for TECs and thethermal straps were identified as technical risks.
Other projects: For TriCCS, the conceptual design ofthe mirror holders and alignment mechanisms for the field
spectrograph was carried out. For SAND, the basic design of themirror holders that include an alignment plan and adjustment
mechanisms was done.
(2) Optics Engineering TeamThe optics engineer ing team is responsible for thedevelopment of optical systems and specialized coating inastronomical instrument development.
1) Development of optical systems
The team has been actively involved in developing various
astronomical instruments, including their optical design andperformance verification. In Fiscal Year 2022, the team recruiteda specialized engineer with expertise in optical metrology
and optical assembly. Notably, the team has developed opticalsystems for multiple NAOJ projects, such as SOLAR-C (EUVST),KAGRA, and SUNRISE III. Additionally, the team has conductedjoint research and development, including (1) developing integral
field units for TriCCS for the Seimei Telescope, (2) conducting
a feasibility study of a large space telescope with a group of
microsatellites using diffractive optical elements, (3) developing
integral field units for SWIMS for the Subaru Telescope, and (4)developing a wide-field submillimeter camera for the Greenland
Telescope. Besides development, the team is actively engaged inconsolidating the development requirements of multiple projects
while simultaneously introducing necessary optical equipment for
future needs. Specifically, in Fiscal Year 2022, the team procured
ultra-high-precision spherical prototyping elements for the highprecision Fizeau interferometer, along with a corresponding
holding mount.
2) Development of coating
Fundamental experiments are continued to design and todevelop the concrete processes of coating, taking into accountthe applications and expected performance of inhomogeneous
multilayers. A coating thickness monitor was newly installed,and various data as to the relation between the status of the coaterand the film characteristics were obtained for longer processes
in detail. A number of experiments have been undertaken to
improve stability including ion-source electrodes modifications
to improve long-time stability of the beam current and its profile;stabilization of power supply; lowering the ground resistance;
and improvements of the process-gas and its introduction, havebeen undertaken. And improvements and optimization of thecontrol software have continued.
(3) Sensor Engineering TeamThe sensor engineering team has contributed to thedevelopment and maintenance of ALMA receivers and Subaru
Telescope instruments (PFS, HSC).
For ALMA receivers, measurements and analyses ofthe designed and prototyped components were conductedwith a view to upgrading Band 8 receivers for ALMA2, andan evaluation system was built for them. In addition, themaintenance of Band 1 receivers is being transferred fromASIAA to NAOJ.
As for the development of superconducting devices, our team
was in charge of fabricating SIS devices for Band 8 receivers and
NbTiN deposition experiments for Band 10 devices for ALMA2.
The experimental results showed that the current density
control of SIS junctions can be controlled with high accuracy,
which had been an issue. For future development, we succeededin fabricating a device for loss measurement of integrated
circuits and a vacuum window with a double-sided antireflection
structure that achieves terahertz transparency across a wide
bandwidth. We are also developing a through-hole fabrication
technique using superconducting films for integrated circuits.
In the development of a next-generation detector for the
Subaru Telescope, we were responsible for a CMOS evaluationand electronics development, as well as for overall coordination of
the development, and the development is proceeding as planned.

5. Manufacturing Design GroupT he Manufact u r i ng Desig n G roup engages i n acomprehensive manufacturing process to fabricate experimental
and observational instruments, from fabrication to verification.
All three teams (Additive Manufacturing (AM) Engineering
Team, Machining Engineering Team, and Measurement and
Evaluation Team) cooperate with each other to meet the various
needs from NAOJ projects and other institutions throughmanufacturing. In FY 2022, the AM Engineering Team, now in
its third year of operation, responded to several requests. And
the whole group had the opportunity to study and implement theprocess from additive manufacturing to finishing key parts suchas interfaces by machining. We also work with the Thermal andMechanical Engineering Team of the System Design Group on
fabrication work. The number of requests for manufacturing andmeasurement in FY 2022 is shown in table 1.

Table 1: The requests for fabrication and measurement in FY 2022.

3

From FY 2021
FY 2022
Advanced Technology Center
ALMA, ASTE, ngVLA
TMT/IRIS, Subaru Telescope
KAGRA
Solar Science Observatory, SOLAR-C, FOXSI-4
RISE
JASMINE
Astrobiology Center
Foundation for Promotion of Astronomy
External Organizations
The University of Tokyo (TAO, SWIMS)Osaka Metropolitan University
Tokyo Metropolitan University
Total
To FY 2023

18
22
10
4
9
8
1
1
1
8
1
1
84
10

(1) Machining Engineering TeamThe Machining Engineering Team has responded tofabrication consultations and fabrication requests ranging frommajor NAOJ projects to groups at ATC and open-use users.
And, for users who wanted to work on their own, we provided
guidance as needed.
The main requests are as follows:i. Regarding TMT/IRIS, fabrication of parts for element
tests is being conducted by the Thermal and MechanicalEngineering Team of the System Design Group.
ii. Fabrication of lens holder base and cryostat test parts for
ALMA Band 2 receiveriii. Fabrication of a folding pendulum for KAGRA. Afterfabrication, performance tests were conducted and the results
were fed back into the next process. (to be continued in thefollowing fiscal year).
iv. Support for post processing of metal 3D printers
The main products are as follows.
• Corrugated horns for ALMA Band 1 receiver• KAGRA QPD circuit covers• Parts for ngVLA• Mirror Frame for ATC THz Intensity Interferometer• Filter holder for Tomo-e GOZEN camera for Kiso
Schmidt Telescope, University of TokyoAs for fabrication by the Ultra-Precision Section, we
have finished processing thin polyethylene sheets to be usedas samples for material property tests in the ALMA radio
frequency range, and fabricated f lat mirrors for terahertz
intensity interferometer. In addition, we supported other teams
for the fabrication of a processing holder and samples of laser
effects on metal additive manufacturing.
(2) Additive Manufacturing (AM) Engineering TeamFY 2022 was the third year of the operation phasefor the AM Engineering Team, the team is entering theapplication of equipment operation and modeling. Based on
the knowledge and experience acquired from the development

II Status Reports of Research Activities079

and manufacturing of ALMA Band 1 corrugated horns, which
had been intensively pursued until FY 2021, the team triedvarious types of manufacturing with aluminum materials. For
KAGRA QPD circuit covers, which were continued from FY
2021, we designed and manufactured another type of cover. At
the same time, we continued to study surface treatment, which
we had been evaluating since FY 2021, and proposed a designthat would make the surface treatment more effective as wellas the treatment method, and manufactured and delivered 21
pieces. In the manufacturing of the filter holder for the Tomo-eGozen camera, which is installed on the Schmidt Telescope at
the University of Tokyo’s Kiso Observatory, the largest scale
product of the fiscal year, we made a prototype to respond to
the request of the observation operator to place the filter holder,which is installed in front of the detector, on a spherical surface
along the telescope’s focus, by combining the external shape
manufacturing by the metal 3D printer and detail machining.
After confirming the installation on site, we completed theinstalled product. During this fabrication, the team experienced
manufacturing of the largest size of the equipment and learned
the basic information and techniques for the manufacturingof large parts. Based on the experience with the ALMA
receivers, we produced several components for radio astronomy
instr uments. In collaboration with Osaka Metropolitan
University, we evaluated the performance of waveguides in
the 6.5–12.5 GHz band and fabricated prototypes of an Orthomode Transducer. Also, prototypes of horns and an Ortho-mode
Transducer for ngVLA were fabricated.
(3) Measurement and Evaluation TeamThe Measurement and Evaluation Team makes full use ofvarious measurement instruments to verify and confirm theaccuracy of products by the Machining Engineering Teamand AM Engineering Team. In addition, LEGEX910, a large
3D measurement machine managed by the Management andAdministration Group, is used to respond to requests for open
use measurements. In FY 2022, we conducted research on thelatest measurement instruments and shared the information
among the staff.

6. Management and Administration Group
The Management and Administration Group has been
established to promote smooth support for projects both within
ATC and outside the Institute, including open-use, and is now in
its second year of operation. The Administrative Support Teamhas had to be reestablished with the replacement of 2/3 of thestaff, but in addition to its normal duties, the team has renewed
the ATC web page and posted ATC News about once a month.
ATC adapted shoe covers to make the tours more comfortablefor foreign visitors, taking into consideration their lifestyle, etc.
34 tours (290 people in total) were handled, which is back to
the level before COVID-19. The IT Support Team has set up aprocess to register information assets with ATC, and continues
to register existing and new information assets.
Operation of the facilities for Fiscal Year 2022 are as follows.

080

II Status Reports of Research Activities(1) Optical shop
We are providing some optical measurement systems andtechnical consulting about the measurement system for openuse users as usual and doing daily inspections to keep themeasurement systems in good condition.
In FY 2022 the function of the optical shop in Instrument
Development Building (2) was moved from Room 110 toRoom 111 due to the expansion of the SIS clean room, andmaintenance was performed on all equipment. In addition, theUV-Vis-NIR spectrophotometer UV3600 made by SHIMADZUCORPORATION, which was installed at the end of FY 2021, hasbeen started up and is now available for open use. The number ofusers in FY 2022 is as follows.
• The number of users for open use- The number of annual users: 274
NAOJ: 222 (including 178 from ATC),
External organizations: 52- Use of LEGEX910 (large-scale 3-D measurement machine): 10
Number of operating days: 26• Technical consulting for users: 28- Giving lectures on how to use the measurement instruments- Technical support on measurement methods(2) Space chamber
As for experimental development support, we assisted basic
experiments using vacuum chambers for the SOLAR-C project.
In terms of equipment management, a turbo molecular pumpof the large space chamber was overhauled in preparation for
future environmental tests of a satellite telescope. In addition,
safety and improvement plans for work at-heights for the spacechamber are being discussed. We also investigated failures ofa turbo-molecular pump in the other medium-sized vacuum
chamber and prepared for the replacement of the pump. Software
for measuring instruments was continuously developed andoperated as needed.
(3) Facility Management and Operation TeamThe Facility Management and Operation Team conductedperiodic inspections of the buildings, electrical equipment,
cold evaporator (CE), cranes, forklifts, draft chambers, andother equipment according to law; and implemented theoverall repair plan, including construction and hazardous
materials management for laboratories including clean rooms(CR). We were responsible for the supply and managementof frequently used organic solvents and waste treatment. In
addition, we were in charge of a NAOJ safety training course(CE practical training) as needed. Team members got skills
and qualifications, and were able to promote the sharing of
inspection and operational works for each facility. As a result,better load balancing was achieved than in FY 2021. We willcontinue to promote the acquisition of qualifications within
the team. In response to the COVID-19 disaster, we regularly
replenished the alcohol used for disinfection in ATC building
entrances and rooms.
The CR temperature control problem and the fan filter units(FFUs) stoppage were partially corrected. Further improvement

will be considered for temperature inhomogeneity near theequipment where there is a lot of heat generation. We willcontinue to investigate the cause of the FFUs outage problem, as
the frequency of outages has decreased but the issue is not fully
resolved. The circulating cooling water pipelines in particularbuildings were inspected and cleaned to reduce deterioration ofwater quality, and we installed water improvement systems forthem.

7. Open-Facility Program, Joint Research andDevelopment Program

technologies to quantum computers.
(1) Expansion of the SIS clean room
The SIS CR expansion construction has been completed.
As a result, the area of the SIS CR was increased 1.3 times
from 210 m 2 to 270 m 2 to provide space for newly introduced
manufacturing and inspection equipment. At the completion
inspection, the cleanliness of the CR was measured andfound to be ISO Class 1. This is the world's highest level forsuperconducting device CR.

ATC accepts external researchers based on two programs,
one is an Open-Facility program which only uses commonuse facilities of ATC and the other is a Joint Research andDevelopment program which is a collaborative development withATC members.
We made calls for these programs twice every fiscal year.
In FY 2022, we accepted 16/1 Joint Research Development
programs in the first/last calls, and 13 Open Facility programs.
Although we limited entry to ATC due to COVID-19, we
normally operated these programs except for disinfection ofhands, body-temperature measurement upon entry, and wearing
a mask in the building in FY 2022.

(2) Strengthening of electronic device security management
systemSince some of the electronic devices used in the ALMA
receivers are subject to export control, the security control
rules for these electronic devices and related information were
determined, and NAOJ established the “Rules for Managementof Electronic Devices Fabricated in the SIS Clean Room” andthe “Procedure for Transfer of Electronic Devices Fabricatedin the SIS Clean Room.” In accordance with these rules, a new
storage area for device management was built and NAS-based
management of design, fabrication, and test data was started.
The management rules for electronic devices will be graduallyapplied to the management of other sensors.

8. Micro-fabrication Laboratory

9. Industrial collaboration activities

The Micro-fabrication Laboratory has upgraded its film
deposition and exposure systems and other equipment, as wellas the associated utilities, in order to address aging facilities
and equipment. The new equipment has increased the diameterof prototype substrates (from 35 mmΦ to 4 inches), making
it possible to mount approximately eight times as many chips
in terms of area. In addition, the introduction of maskless
lithography equipment will allow the Laboratory to respondflexibly to frequent design changes, and the Laboratory will
maintain the technology and facilities for fabricating Nb/
Al/AlNx/Al/Nb junctions with high critical current density,
which is extremely important for SIS junctions required for
ALMA receivers, as well as the film deposition equipment
for fabricating low-critical-current junctions required for
peripheral circuits. In addition to maintaining the fabrication
technology and equipment for Nb/Al/AlNx/Al/Nb junctions,which have extremely important high critical current density.
Furthermore, for FY 2023, we are expanding analyticalequipment and automating resist coating and development, andare proceeding with utility maintenance and installation workfor this purpose. By automating new processes and improving
technologies, ALMA is preparing a stable manufacturing basefor the development of high-performance devices for future
development. We constructed an expanded new clean room for
the ALMA2 project, a superconducting device storage room,
and an environment for managing design and process recipes
data, all of these works were conducted in collaboration with
the Facility Management and Operation Team. Furthermore,
we are developing devices for the industrial application of theseATC cooperated with the I ndust r ial Collaboration
Office in order to apply the technologies developed at ATC
for astronomical instruments to society. In FY 2022, ATCparticipated in the “Science Photonics Fair” for the first time
as a part of NAOJ. ATC contributed to the fair by preparing
presentation materials to introduce our technologies, exhibiting
processed parts, and serving as a booth attendant.
Supported in part by JST (Moonshot R&D) (Grant No.
JPMJMS2067) and JSPS KAKENHI (Grant Nos. JP18H03881,
JP19H02205, and JP22H04955), we have devised a new conceptof superconducting microwave low-noise amplifiers for use inradio wave detectors for radio astronomy observations, andsuccessfully demonstrated a high-performance cooled amplifier
with power consumption three orders of magnitude lower thanthat of conventional cooled semiconductor amplifiers. This
result is expected to contribute to the realization of largescale multi-element radio cameras and error-tolerant quantum
computers, both of which require a large number of low-noise
microwave amplifiers.
I n t he f ield of a d apt ive opt ics t e ch nolog y, wh ichcompensates for atmospheric turbulence to obtain a clear imageof celestial objects, there is growing interest in its application
to optical instruments for purposes other than astronomical
observation, such as communications, and in FY 2022 we
provided technical consulting services to private companies.
P repa rat ions were made to lau nch t he “Social
Implementation Program” in FY 2023 for ATC as a whole topromote these industrial collaboration activities.

II Status Reports of Research Activities081

16. Public Relations Center
1. Overview

3. Public Relations Office

The Public Relations Center engages in the publication,
promulgation, and promotion of scientific achievements madenot only by NAOJ but also by others in the field of astronomy
in general to raise public awareness; responds to reports of
discoveries of new astronomical objects; and provides theephemeris and other astronomical information directly related
to people’s everyday activities, such as sunrise and sunset
times. The Public Relations Center is comprised of 9 offices(including Ishigakijima Astronomical Observatory) and 1 unit:
the Public Relations Office, the Outreach and Education Office,the Spectrum Management Office, the Ephemeris Computation
Office, the Library Unit, the Publications Office, the IAU Officefor Astronomy Outreach (OAO), the Time Keeping Office,Ishigakijima Astronomical Observatory, and the General
Affairs Office.

The results of NAOJ's research projects and joint researchwith other universities and research institutes were actively
publicized through press conferences and web releases. In
addition, we are producing and posting online videos andnews article to widely disseminate information about topics
at the forefront of astronomy and astronomical phenomena,and promoting the use of SNS. We conduct new forms of
public outreach such as Citizen Astronomy and exhibits atinternational events in response to the mid-term goals andsuggestions from the External Review.

2. Personnel
In FY 2022, the Public Relations Center was composed of
Director Hitoshi Yamaoka and the following staff members: 2
project professors, 2 associate professors, 2 associate professors(senior lecturers), 2 assistant professors (one of whom holds
concurrent posts), 1 research engineer, 1 engineer, 1 unit
leader, 6 senior specialists, 2 project research staff members,
2 research experts, 2 administrative experts, 1 researchsupporter, 14 public outreach staff members, 4 re-employment
staff members, and 1 Senior Specialist.
On April 1, Leader of the Library Unit Iori Koshihara andSenior Specialist Yoshiaki Tamura arrived in the Time Keeping
Office.
On May 31, Administrative Expert Kana Endo (Ishigakijima
Astronomical Observatory) resigned.
On June 1, Administrative Expert Akiko Ishii arrived in
Ishigakijima Astronomical Observatory.
On September 1, Project Research Staff Natsuki Hayatsu
arrived in Ishigakijima Astronomical Observatory.
On October 1, Associate Senior Research Engineer
Tetsuharu Fuse arrived in the Time Keeping Office.
On October 31, Ad minist rative Exper t A kiko Ishii(Ishigakijima Astronomical Observatory) resigned.
On November 1, Administrative Expert Sumiko Mimura
arrived in Ishigakijima Astronomical Observatory.
On December 25, Public Outreach Staff Ryo Sato (Public
Relations Office) resigned.
On March 31, Public Outreach Staff member Yumi Hibino(Outreach and Education Office) and Public Outreach Staff
member Masaharu Ishizaki (Outreach and Education Office)resigned.

082

II Status Reports of Research Activities(1) Online-Based Information Sharing
The Public Relations Office runs the NAOJ website (https://www.nao.ac.jp/en/), disseminating information via the internet.
In Fiscal Year 2022, the total access count for the NAOJ
website was approximately 12.65 million page views.
The Office opened Twitter, Facebook, Instagram, andFlickr accounts in both Japanese and English sequentiallyfrom 2010, actively disseminating information on social
networking services. As of the end of March 2023, the Japanese
Twitter account has nearly 268,000 followers, and the English
version of the Twitter account has more than 9,400 followers.
Information dissemination via the English version of Twitter,as well as the release of visual images on Instagram have been
conducted continuously this year.
NAOJ e-mail newslet ters No.237–243 were issued,
introducing research results and NAOJ hosted events. A total of
about 11,100 subscription addresses have been registered as ofMarch 31, 2023. (almost unchanged from the previous year)
We continued to produce videos explaining astronomical
phenomena and research results, and videos introducing
outreach activities. Including English versions, 18 originalvideos were produced. In addition, a total of 11 livestreams
were held, including astronomical phenomena such as the total
lunar eclipse and occultation of Uranus; and the occultationof Venus; Special Open House Day lectures, and livestreams
of celestial objects using the 50-cm Telescope for Public
Outreach. In particular, the livestream of the total lunar eclipse
and occultation of Uranus attracted a lot of attention, with
1,849,851 live views and a total of 2,016,018 views includingarchive views. The livestreams of celestial objects have beenvery popular, and in addition to distribution via YouTube, they
are an official program by DWANGO Co., Ltd., which manages
niconico Live, a video streaming service, and our viewers are
increasing. In addition, an explanatory video was made before
the lunar eclipse. On May 24, 2022, a collaborative projectwith the Ministry of Education, Culture, Sports, Science andTechnology (MEXT) titled “GIGA School Special Lecture~Let's Look at the Universe to Understand the World~”
was held. The Mitaka Large Seminar Room and the Subaru
Telescope Observation Room were connected online, andlectures and Q&A sessions were conducted in real time. The
event was streamed on YouTube Live, and the archive wasviewed 12,477 times (as of the end of March 2023).
(2) Research Result PR
There were 30 research result announcements (compared to
23 in FY 2022 and 30 in FY 2021). We released all the researchreleases in both English and Japanese. Press conferences(including online conferences) were held in connection with 3of these releases. All presentations were sent to reporters via
e-mail press releases to an original media list in addition to
being published online.
The 28th “Astronomy Lecture for Science Journalists”
was held on December 1, 2022 on the theme of “Technological
Development in NAOJ and Collaboration with Industry,” with18 lecturers and 14 guests of ATC participating.
(3) Activities as NAOJ’s Public Relations CenterIn addition to the Center’s regular task of aiding research
result releases, in order to raise awareness of NAOJ overseas,
NAOJ holds booths at international conferences where thepress, researchers, and educational officials gather. This year,
we exhibited at the American Association for the Advancementof Science Annual Meeting (AAAS2023, March 2–5, 2023,
Washington, DC). To support outreach efforts of other projects,
we contributed to revamping project websites. The Citizens
Astronomy project “GALAXY CRUISE” conducted with thesupport of Subaru Telescope, has received cooperation fromthe Outreach and Education Office since FY 2022. The second
season, which targets fainter galaxies, began on April 18, 2022.
This year, campaigns were held in August and at the end of theyear. As of the end of March 2023, a total of 11,322 people from102 countries and regions (including 7,675 participants fromJapan) had registered to participate.
(4) New Astronomical Objects
In cooperation with the Outreach and Education Office,four staff members handled reports of new astronomical objects
and other communications submitted to NAOJ. In this fiscal
year, there were a total of 48 reports including confirmation
requests for new celestial object candidates and other reports.
The contents were: 39 novae/supernovae, 6 comets/cometary
objects, 1 luminous object, and 2 moving objects. Among many
reports of previously known celestial bodies or observational
errors, a report in January 2023 was reported through NAOJ
to the Transient Name Server operated by the IAU Supernova
Working Group and recognized as the discovery of supernova
2023fu. A report in February 2023 was communicated throughNAOJ to the IAU Central Bureau for Astronomical Telegrams(CBAT) and was recognized as an independent discovery of thenova V6596 Sgr. In addition, a total of 15 dwarf novae and flarestars were reported.

4. Outreach and Education Office
In FY 2022, the COVID-19 pandemic forced us to suspend,scale down, or restructure many of our outreach and education
activities.
(1) Public Visits
A total of 12,684 people participated in Mitaka Campus
Public Visits (former name was Visitors’ Area) in FY 2022.
In addition, the group tours in 2022 consisted of 62 general
tours (1561 guests), for a total of 14,245 guests visiting Mitaka
Campus. Measures were taken to prevent the spread of
COVID-19, such as restrictions on Public Visits and restrictions
on the acceptance of group tours.
Regular stargazing parties, which before COVID-19 wereusually held twice a month (the day before the 2nd Saturday
and the 4th Saturday) with the 50-cm Telescope for Public
Outreach, were held online twice a month until October (the4th Saturday stargazing party in October was canceled due toMitaka Open House Day). Starting from November  was held
online and  was held onsite on a reduced scale. Online eventswere held 18 times and accumulated 1,851 views as of the endof March 2022. Onsite events with a capacity of 60 guests were
held 5 times, and a total of 220 people participated.
Regular public screenings at the 4D2U Dome Theater
were originally scheduled to be held three times a month(1st, 3rd Saturday, and the day before the 2nd Saturday) on areservation basis. As preventative measures against the spreadof COVID-19, the event capacity was reduced (usually 40 seats,
14 seats in April, 20 seats after May), but screenings were heldon 34 days during the year, and 1,781 people participated. In
addition, screenings for school groups resumed in July, and 349
people participated in 15 events. “Astronomers’ Talks” minilectures and public screenings for groups were both canceled.
There were 53 group tours (544 people) organized and a total of
2,674 guests watched the 4D2U stereoscopic movies.
(2) Telephone Inquiries
Telephone inquiries are accepted from 9:30 to 17:00 on
normal business days. Due to personnel reductions, we havecontinued to have only one person on-duty since fiscal 2020,
but had two people on-duty on the day before (November 7)
and the day of the total lunar eclipse and occultation of Uranus(November 8). In addition, to prevent the spread of COVID-19,
we have been working from home or commuting as appropriate
since FY 2020.
The number of telephone inquiries to which we responded
this fiscal year totaled 3,260, of which 488 were from themedia. The topics (and number) of the inquiries were: Solar
Ephemeris (351), Lunar Ephemeris (340), Ephemeris (62), Time(12), Solar System (776), Universe (240), Astronomy (235),
Other (1244). The number of letter inquiries totaled 56, of
which 16 were official documents.
(3) Media Reception
We received 131 interview and filming requests fromvarious media, out of which the following filmings wereconducted: 32 newspaper articles; 37 TV programs (17 news
programs, 6 science programs, 14 others); 22 publications (9II Status Reports of Research Activities

083

magazines, 5 books, 8 others); 14 websites and contents; 4radio programs; 4 others. From FY 2019, we started to charge
a fee for commercial filming and photography in the campus;
this fiscal year, we accepted a request for a shooting for 1
publication.
(4) Educational and Outreach Activities
The “FUREAI (Friendly) Astronomy” project, now in its
13th year, continued to provide classroom visits and online
lectures as in the previous year. These lectures were deliveredat 112 schools, 69 in Japan and 43 overseas, by 70 instructors
and attended by 7,933 pupils, with the number of attendees
per lecture ranging from 4 to 406. In 13 years, 90,611 students
in total have attended the lectures in 1,013 schools inside andoutside Japan.
“Mitaka Open House Day” was held in hybrid format
for the first time, with both online and on-site (advanceregistration, limited capacity) events. We participated as partof the secretariat under the direction of the steering committee,
and contributed to some of the displays and content. This
year’s event was held on October 28 (Friday, live-streamed)and October 29 (Saturday, hybrid events) with the theme“Time and Astronomy.” It was co-hosted by the Astrobiology
Center, National Institutes of Natural Sciences; the Instituteof Astronomy, the School of Science, the University of Tokyo;
and the Department of Astronomical Science at the Schoolof Physical Sciences of the Graduate University of Advanced
Studies. At the onsite event, hands-on exhibits, mini-lectures,
tours of research facilities usually inaccessible to the public,
etc. were restarted and 419 people selected from among theapplicants participated. Although it was a small number ofpeople, it was the first lively Open House Day in a long time.
Online, in addition to the main lecture streaming, minilectures, video content distribution, online puzzles, etc. were
held. The number of video contents distributed was 31, themaximum total number of simultaneous connections was 1,000,
and the total number of views in the first month after release
was 65,480.
(5) Community Activities
The “Mitaka Picture Book House in the Astronomical
Observatory Forest” welcomed 25,165 visitors in FY 2022.
The Office supervised an exhibition, “You Can’t See It But
It’s There; Here and in Space.” (July 2022 to June 2023).
We also cooperated with an opening ceremony, modern andtraditional Tanabata events, moon viewing event, and otherevents. In addition, through the “Mitaka Picture Book Housein the Astronomical Observatory Forest, Picture Book Original
Drawings Hallway Exhibit Contest” which started from FY
2013, the Outreach and Education Office cooperated in theselection of 6 winning books.
“Mitaka TAIYOKEI walk,” a stamp collecting event thattakes place every Fall under the joint auspices of Mitaka Cityand Mitaka NETWORK University Organization, was held in
a contactless way to avoid any potential spread of COVID-19,
with a smartphone application collecting digital stamps instead

084

II Status Reports of Research Activitiesof physical ones. During the event, lectures on the Solar
System, a stargazing party, and a workshop for building an
actual telescope were held as “Mitaka TAIYOKEI walk-related
lectures,” in which NAOJ cooperated.
The Office also provided the venue for “Astronomy Course
for Apprentice Starry Sky Guides, Star Sommelier Mitaka- Let’s Become Apprentice Starry Sky Guides! -” hosted by
Mitaka NETWORK University Organization, and assisted
by providing teachers and workshops. We also contributed to
selecting lecturers for “Astronomy Pub” (currently held online).
The “Information Space of Astronomy and Science,”
which is jointly operated by Mitaka City, Mitaka NETWORK
University Organization, and Mitaka Town Management
Organization, marked the 8th anniversary since its opening in
September 2015. In FY 2022, a total of six exhibitions were
held at this facility, of which the one titled “Exposing the True
Nature of Black Holes” was planned and held by NAOJ. The
total number of visitors was 12,362 in 2022, still about 2,900
less than in 2019 due to the effects of the novel coronavirus.
The total number of visitors since its opening exceeded 100,000
this year, and we helped with an event to commemorate thismilestone.
(6) Merchandizing BusinessWe run “Astronomical Events Information” on the NAOJ
website to provide monthly star charts and information onplanetary and other remarkable astronomical phenomena. We
created a breaking-news page in response to Comet C/2022 E3(ZTF), which appeared bright from January to February 2023.
This fiscal year, intended particularly for the media, anarticle detailing the remarkable astronomical phenomena of
the year (the total lunar eclipse and occultation of Uranus on
November 8) was created and posted on “Astronomical Events
Information.” In addition, two corrections were made to update
the information on the “Frequently Asked Questions” page,
which summarizes the answers to questions the Telephone
Inquiries service frequently received from the public.

5. Spectrum Management Office
The Spectrum Management Office (SMO) is tasked withprotecting the astronomical observation environment fromvisible light to radio waves. The SMO currently consists of four
members, of which three are dedicated members (Head, anassociate professor, and a research supporter) and one holds a
concurrent post. SMO members participated in 5 international
meetings and 26 domestic meetings this year. In addition tothese, the SMO also participated in email discussions and videoconferences and responded to media inquiries.
(1) International Meetings
The SMO participated in Working Party 7D (WP7D)
hosted by ITU-R, the radiocommunication sector of theInternational Telecommunication Union (ITU) responsible
for radio astronomy issues, and contributed to the discussion.
This year’s WP7D meetings were held from April 25 to 29,

and from September 28 to October 5, in a hybrid format online
and at the ITU headquarters. The main topics on the agenda
were the study of compatibility between radio astronomy
and mobile phones in the 43 GHz band, harmonics entering
radio astronomical bands, and the sharing of frequency bands
above 71 GHz between active services and radio astronomy.
In addition, although lunar surface development is attracting
much attention from the Artemis program and private spacedevelopment companies, the radio quiet region on the lunar
surface, where radio emissions from Earth are blocked (theshielded zone of the Moon), is important as a future radio
telescope installation site. For this reason, issues related tomitigation technology in the case that radio astronomical
facilities are established on the lunar surface were also
discussed, and a new ITU-R Question was adopted by the ITU.
The SMO also participated in online meetings as needed to
exchange opinions and strengthen relationships with people
involved in the protection of radio astronomy.
(2) Results and Current Status of Domestic Issues Discussed
Among the issues discussed by the MIC Information andCommunications Council, the major ones related to radio
astronomy are described here.
1) Frequency Expansion for Wireless LAN into the 6 GHz
Band: In response to the congestion of the wireless LAN
bands, the 6 GHz band (5.925–6.425 GHz) was newly allocatedto wireless LAN in September 2022 in addition to theconventional 2.5/5 GHz bands. In FY 2022, with the aim offurther expanding the band, a study on frequency sharing in the
6.425–7.125 GHz band and a technical study of a wireless LAN
system with greater power emission were conducted. In thisfrequency band, 6.665–6.66752 GHz, where the CH3OH maser
emission line is located, radio astronomy is protected. Basedon the results of a study concluded in FY 2021, it has beenconcluded that radio astronomy and wireless LAN cannot share
this band due to the large amount of interference expected toradio astronomy. Although the introduction of a mechanism toprohibit radio emissions or adjust the output power of wirelessLANs only in areas around radio telescopes and other radio
stations was also considered, no conclusion was reached on thetechnical framework from the viewpoint of sharing between
radio astronomy and other radio services. Studies will continue
in FY 2023.
2) Studies on the 76–77 GHz Band Sharing with VehicleBorne Millimeter Wave Radar: To ensure a wide angle and a
sufficient range, studies to improve vehicle-borne radar havebeen ongoing. In this frequency band, both radar and radio
astronomy are supposed to use the same frequency band. To
prevent radar systems from interfering with radio astronomy
observations, the SMO participated in informal meetings withmillimeter-wave radar manufacturers and discussions in the
MIC 76 GHz Low Power Millimeter-Wave Radar Working
Group. Although the results of the joint study conducted by theradar development companies were discussed, it could not be

said that sufficient studies were conducted to prevent harmfulinterference, and the discussion was postponed to FY 2023.
3) Sharing bet ween satellite cellular phones and radio
astronomy in the 1.6 GHz band: When a new service using thesatellite mobile phone system via the Globalstar satellites wasdeveloped, we studied the possibility of sharing radio band
resources with radio astronomy. As a result, restricted areas
were established around NAOJ VERA Mizusawa Station,
Ishigakijima Station, and JAXA Usuda Deep Space Center toprotect radio astronomy. An operation agreement was signed
on March 23, 2023 between the NAOJ Public Relations Centerand IPmotion Inc., which develops Globalstar satellite services
in Japan.
(3) Application for Receiving Equipment Designation:
Designation of receiving equipment should be conductedbased on the Radio Law, Article 56. Once it is approved, aradio station must be operated in such a way as not to causeinterference or any other obstruction that impairs the operationof radio astronomy stations or equipment designated by the
Ministry of Internal Affairs and Communications. This fiscal
year, we applied for continued protection of the Nobeyama
45-m Radio Telescope, and the protection desig nation
procedures were completed on March 10, 2023.
(4) Light Pollution:
There are concer ns about the detrimental effects to
ast ronomy f rom mega- constellat ions such as St arli n k
and OneWeb comprised of a large number of satellites.
SpaceX, which operates the Starlink satellites, launched
VisorSat equipped with a shade to reduce reflected light, andIshigakijima Astronomical Observatory in cooperation with
the Optical and Infrared Synergetic Telescopes for Education
and Research (OISTER) conducted visible and near infraredobservations of the satellite; and prepared a report (published in
April 2023). The SMO assisted with analysis and interpretationof the data obtained at Ishigakijima Astronomical Observatory.
In addition, the SMO committed to ongoing participation in thedigital camera night-sky brightness survey being conducted by
the Ministry of the Environment and we submitted observation
results from Chichijima in the Ogasawara Islands and Mitaka
City.
(5) Activities for Raising Awareness of Frequency Resource
Management
To make more people aware of f requency resou rce
management, the SMO participated in the Special Open House
Day of Nobeyama Radio Observatory and Mitaka OpenHouse Day 2022, explaining our activities to the guests. In
addition to continuous updates to our webpage, an opinion
submission form was created on the website to promote twoway communication with citizens about frequency resource
management. In addition, an overview of light pollution was
introduced in “SANKEI Kid's News” on January 19, 2023,
and distributed to elementary and junior high schools (moreII Status Reports of Research Activities

085

than 6,000 schools) nationwide. In FY 2022, there were 10
media interviews about negative impacts on astronomy by light
pollution from ground-based sources or mega-constellations,and those situations were covered by newspapers, magazines,
web articles, etc.

6. Ephemeris Computation Office(1) ECO published the “Calendar and Ephemeris 2023”
and compiled the ephemer is section and several par tsof the astronomy section from the “Rika Nenpyo 2023”(Chronological Scientific Tables). ECO also posted the “RekiYoko 2024” in the official gazette on February 1, 2023. In
addition to those paper-oriented products, ECO maintains web
versions of the “Calendar and Ephemeris” and the “Reki Yoko”
and updated their data simultaneously with the release of “RekiYoko.” The “Handbook of Scientific Tables” -The international
edition of Rika Nenpyo- was released in May. We promoted
the book through a web release; leaflet distribution and sample
presentations at IAU and AAS Meetings; and advertisements inthe “Astronomical Herald.”(2) ECO featured the total lunar eclipse with the lunar
occultation of Uranus; the 1st sunrise of the year; and thelunar occultation of Venus on its website. In cooperation withthe “Astronomical Events Information” by the Outreach and
Education Office, ECO displayed the radiant points of the
Perseid, Geminid, and Quadrantid meteor showers and thelocation of Comet ZTF in the Sky Viewer. In FY 2022, there
were over 37 million page views for the ECO website.
https://eco.mtk.nao.ac.jp/koyomi/index.html.en(3) The Japan Association for Calendars and Culture Promotion
hosted Mini Forum, its 12th General Meeting, and the Calendar
Presentation Ceremony. These were also delivered via a remote
conference service.

(4) ECO holds regular exhibitions presenting NAOJ's invaluable
collection of historical archives of Japanese and Chinese
books in collaboration with the library. The theme of the 60th
regular exhibition was “The Antikythera mechanism from thecollection of the National Archaeological Museum of Athens.”
In addition, we published a new catalogue featuring pamphlets
from the 41st through the 60th exhibitions. Past exhibitions areavailable at the Rare Materials Exhibition website.
https://eco.mtk.nao.ac.jp/koyomi/exhibition/

7. Library Unit
The Library Unit collects and sorts scientific journals andbooks in order to make them available for the research andstudy of NAOJ researchers and students. With the continuing
digitalization of scientific materials, it has also become our
responsibility to ensure access to electronic media academic
resources.
Before the COVID-19 pandemic, the Mitaka Library was
open to non-NAOJ affiliated users on weekdays, but the libraryhas been closed to the public since March 2020. Even in such asituation, however, the library continues to lend materials thatare not available at any other libraries or provide photocopiesof these materials to non-NAOJ affiliated users. The librarymaterials are provided to the general users through their local
public libraries, and to researchers and students affiliated toother institutions through the libraries of their institutions.
With both original materials and photocopies combined, 50
materials were provided this fiscal year.
The library holds many important documents, the mostprominent of which are those written by the Tenmonkata,
Shogunate Astronomers of the Edo Era. These documents are
stored in a dedicated room where the environment is strictly
controlled. Some of the collections are digitized and available
on the Library Unit website.
For the Mitaka Open House Day 2022, held in October, theLibrary Unit created special web pages listing books related
to this year’s theme and other materials housed in the library.
The number of books and journals owned by Mitaka Libraryand each observatory and the condition of continuing NAOJ
publications are published in Section XI Library, Publications.

8. Publications Office
The Publications Office continued its activities in planning,
editing, and printing NAOJ’s original materials for educationand outreach. The following periodicals were also publishedthis year:

Figure 1: Pageviews for ECO Website.

086

II Status Reports of Research Activities• Annual Report of the National Astronomical Observatory ofJapan Volume 34 Fiscal 2021 (Japanese)• Annual Report of the National Astronomical Observatory ofJapan Volume 24 Fiscal 2021 (English)• 23nd Report of the National Astronomical Observatory ofJapan• NAOJ 2023 Pamphlet (English)• NAOJ News, No. 337–No. 339 (Summer 2022, Autumn 2022,
Winter-Spring 2023)• NAOJ Calendar (The 18th in the series)
NAOJ News underwent a major renewal in FY 2022 tofocus on general-public readers. Copies for distribution weresent to schools and community facilities in Mitaka City, as wellas member institutions of the Japanese Society for Education
and Popularization of Astronomy, planetariums, and publicobservatories nationwide. Web-based surveys were conductedin accordance with each issue, and based on the results wewill develop more effective content for the magazine. Website
development is continuing for the shift to digital publication. In
new publications, the English edition of the Sandcastle TRPG
was released.

countries).
Other OAO Activities in 2022 included: 1,684 Kaifu-NAOJ
Telescope Kits sold; Dark and Quiet Skies Awareness Month inMay, with an art contest (202 submissions from 13 countries),
a seminar (nearly 3,000 views), and a social media campaignthat highlighted 25 events worldwide; and the OAO presenceat the IAU General Assembly (GA) in Busan in August, witha KASI-OAO Special Outreach event, the OAO GA Sessions
and the Press Conference and Press Release for NameExo
Worlds 2022. “Meet the IAU Astronomers!” had 65 meeting
requests in 29 countries, and 220+ IAU members signed up(50 countries). In October, “100 Hours of Astronomy” saw 196
registered activities and events in 55 countries. “Telescopes
for All” concluded with 110 entries from 30 countries and theengagement of 44 NOCs (15 telescopes awarded).

9. IAU Office for Astronomy Outreach (OAO)

10. Timekeeping Office Operations

The IAU Office for Astronomy Outreach (OAO) is a joint
venture between the IAU and the National Astronomical
Obser vator y of Japan ( NAOJ ). T he OAO is pr i ma r ily
responsible for managing the IAU’s communication andaccessibility initiatives and supporting the international
network of IAU National Outreach Coordinators (NOCs) inover 120 countries and with 350+ volunteer representatives.
In the 2022 fiscal year, we have marked an importantmilestone in the lifetime of the Office for Astronomy Outreach(OAO). To commemorate our 10th Anniversary, we focused on
the sustainable growth of the OAO initiatives, consolidated thework assessed in 2021 by the OAO External Review and added
some special projects.
The 10th Anniversary special projects included NameExo
Worlds 2022, bringing together students, educators, amateurs,
and exoplanetary scientists to collaborate in astronomy
outreach in their communities and put forward names for one of
20 available exoworlds. The program received 603 submissions
from 91 countries, engaging 52 National Panels formed by
NOCs. Under One Sky funded five projects (2000€ per project)that connected indigenous with non-indigenous knowledge,
spanned from remote communities to urban centers, andbuilt multidisciplinary resources for the public to further
engage with their astronomical traditions. The call received 33
proposals from 24 countries.
We also highlight the Communicating Astronomy with the
Public Triptych, including the CAP Conference held in hybrid
format from 12–16 September 2022, hosted by Macquarie
University in Sydney, under the theme: Communicating
Astronomy for a Better World. There were 111 participants
in-person in Sydney and a further 133 online participants, intotal representing 43 countries. Issue #31 of the CAP Journal
was published in October 2022. And CAP Trainings hosted
five editions: abstract writing (66 registrants), OAO-JWST on
First Images (100+ registrants from 60 countries), Relationship
Building at IAU GA XXXI (10+ participants), OAO-JWSTon Image Processing (96 registrants from 50+ countries), andOAO-CXC on Image Accessibility (100+ registrants from 25+

The Time Keeping Office operates four cesium atomic
clocks together with a hydrogen maser atomic clock at
Mizusawa VERA Station, and constructs “Central Standard
Time” of Japan. The facilities contribute to the determinationof UTC (Coordinated Universal Time) by BIPM (Bureau
International des Poids et Mesures) through international timecomparison. The NTP (Network Time Protocol) server at theTime Keeping Office provides standard time on a network. This
service has been in great demand; about 3 million daily visits
have been recorded.

11. Ishigakijima Astronomical Observatory
FY 2022 became the year that we implemented a paid
admission system. In public outreach, the facilities were open
to the public throughout the year, and the total number ofguests was 3,477. Moreover, the observatory was involved inbroadcasts of astronomical events. In education, we welcomedgroup tours and inspections. In research, 1 refereed paper was
published, bringing the total number of papers published basedon data from Ishigakijima Astronomical Observatory to 31.
(1) Public Outreach Activities[Guided Tours, 4D2U Theater, Stargazing Sessions]
The facility was opened to the public through cooperation
with Ishigaki City, Ishigaki City Education Committee,
and Specified Nonprofit Corporation Yaeyama Hoshinokai.
In fiscal 2022, paid admission began for the purposes of
expanding services and improving safety and security. We
limit the number of visitors, hours, and the number of times,
and disinfect thoroughly as preventative measures against the
COVID-19 pandemic. The annual number of visitors was 3,477,
and the cumulative number of visitors was 154,163. Lightning
strikes around the observatory in June damaged the telescope
dome and water supply facilities. It took several months torestore each facility, with the telescope dome finally being
restored in March 2023. During that time, the 40-cm telescope

II Status Reports of Research Activities087

on the roof of the Hoshizora Manabi no Heya (Starry Sky Study
Room) was utilized.
[Special Events, Co-sponsorships, Cooperative Events, etc.]
We were involved in photography for public outreach
including a moonbow and Comet ZTF; photography andstreaming videos with the “Southern Cross Monitor” and“Milky Way Monitor;” support for the broadcast of theNovember total lunar eclipse (based in Mitaka Campus,
2,010,000 views); and the live broadcast of the Marchoccultation of Venus (270,000 views). The “Southern Island
Star Festival” we co-hosted in August had 894 live viewers and6,875 views including archive views. And 250 people attended
the star festival held in Yonaguni Island which we also cosponsored. There were 16 articles in newspapers and othermedia including Mynavi Gakumado, and there were 25 casesof assistance with news gathering. In March, a member of theobservatory received the Yoshihide Kozai Award presented by
the Nonprofit Public Organization: Foundation for Promotionof Astronomy. The 3,200 km “Stamp Rally” held with Nayoro
Observatory KITASUBARU had 20 people complete it.
(2) Educational Activities
There were 18 inspections and educational group tours
held in cooperation with Ishigaki City, Ishigaki City Education
Committee, Specif ied Nonprof it Cor poration Yaeyama
Hoshinokai, and the Ishigaki Youth House with a total of 212
guests. Particularly noteworthy, we received an inspection tourby 12 members of the House of Representatives in July, and an
inspection tour by Liberal Democratic Party Policy ResearchCouncil Chairperson Koichi Hagiuda and 16 other membersof Parliament in December. The Chura-boshi Research Team
Workshop for high school students was held in August with
20 participants from across Japan. We also worked for local
education activities, including classroom visits for local
elementary students and lectures for the local citizens.
(3) Research Activities
One refereed paper in a western journal was published in
FY 2022, on the topic of small celestial bodies in the Solar
System. The total number of papers including results basedon Ishigakijima Astronomical Observatory observational datareached 31. Project Research Staff Member Natsuki Hayatsu
arrived in September. There were 4 presentations at domestic
and international conferences, and two papers were submitted
to peer-reviewed journals. Observations with the Murikabushi
Telescope were suspended long-term from June through theend of the fiscal year due to a lightning strike.

088

II Status Reports of Research Activities

17. Division of Science
1. Overview
We will report the FY 2022 research activities in the
Division of Science based on the following vision andphilosophy of the division:- Achieve fruitful research results based on liberal ideas ofindividuals, and achieve world-leading scientific results.
Expa nd t he hor i zons of ast ronom ical k nowledge bydeveloping new fields such as efficient collaborations between
theory and observations, multi-wavelength astronomy,
and multi-messenger astronomy. In addition to developing
important research, we nurture creative ideas to develop new
fields.
- Utilize large telescopes and supercomputers in NAOJ toachieve top-level research results as a world-leading researchdivision. Contribute to the promotion of future plans of NAOJ
from a scientific perspective.
- Actively promote the education of young researchers,
including students in graduate schools, to attract both
Japanese and oversea researchers in the next generation who
will lead world-wide research activities. Become a career
path center for astronomical researchers worldwide.
- Strengthen astronomy research in Japan by creating newscience through collaboration with domestic and international
researchers, including other Projects in NAOJ. Play animportant role in promoting internationalization in theastronomical field in Japan.
The members of the Division of Science cover a wide
variety of themes in astronomy research from the early
Universe to the formation and evolution of galaxies, stars, andplanets, activities of compact objects, and plasma phenomena
in astronomy and astrophysics – from various aspects of theastronomical hierarchical structure, such as dynamics andmaterial evolution. Taking advantage of the facilities of NAOJ,
such as the super-computers of NAOJ, the Subaru Telescope,
ALMA, and the Nobeyama radio telescope, we stimulate
collaborations among theoretical and observational astronomers
working on various wavelength ranges. Also, we proceedwith interdisciplinary research on the physics of neutrinos,
gravitational waves, elementary particles, and atomic nuclei
as well as planetary science. The division members are also
actively participating in developing the science for future
observational projects.
In order to facilitate highly competitive world-leading
research activities, the Division of Science offers a superb
research environment as a base for astronomy researchaccessible to researchers in Japan and overseas. We are
beginning to see a return to direct domestic and international
interaction even with continuing concerns about COVID-19,
and visitors from other universities and research institutionsin Japan are increasing. We have gradually begun to arrange
opportunities for interaction among members. In addition to theregular lunch meetings of educational staff conducted online,
we have held workshops and social events with all members ina hybrid format. The division actively organizes internationaland domestic workshops for the fields of theoretical andobservational astronomy, as well as a cross-disciplinary field
between astronomy and planetary science, to promote research
activities in various related fields of astronomical science.
To maintain and further develop our high-level researchcapabilities and research environment, we underwent aninternational external review this year during March 1–2 forthe first time since the Division of Science was set up. The
review committee members were invited to Mitaka Campus fortwo days to interview staff, post-doctoral fellows, and graduate
students. Committee members praised the high quality andquantity of research, incorporating theory and observation
since its beginning.

2. Current Members and Transfers
In FY 2022, the dedicated faculties of the Division of
Science included five professors, three associate professors,
one project associate professor, and six assistant professors,in addition to one adjunct professor, one adjunct associate
professor, one adjunct assistant professor, and one adjunctsenior specialist who concurrently held a primary position at
the Center for Computation Astrophysics (CfCA). Accordingly,
the research activities on exoplanets, the formation andevolution of planets, supernovae, time domain astronomy,
and multi-messenger astronomy have been strengthened. In
addition to these faculty members, the division was servedby ten project assistant professors (including NAOJ fellows),
nine project researchers, two special postdoctoral researchersof Japan Society for the Promotion of Science (JSPS), two
research supporters, as well as two administrative supporters(one is from Feb. 1) who gave full support to all activities of thedivision.

3. Output of Our Research
There were 173 refereed research papers published by thedivision members as authors. Some of the research results arepresented as the research highlights listed at the beginningof this report. The following includes research in which thedivision members took leading roles:• Top-heavy stellar mass distribution in galactic nuclei inferredfrom the universally high abundance ratio of [Fe/Mg] (D.
Toyouchi, K. Inayoshi, M. N. Ishigaki, and N. Tominaga)[Japanese Language]• Radio VLBI: still leading advancements in understanding theformation of high-mass stars at high resolution (R. A. Burns,
et. al., + many more)• Na r row Fe -K α Reve rbe r at ion Mappi ng Unvei ls t heDeactivated Broad-Line Region in a Changing-Look Active

II Status Reports of Research Activities

089

Galactic Nucleus (H. Noda, M. Kokubo, K. Morihata, et al.)
• A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ~12 Galaxy in Early JWST CEERS Imaging (S. L. Finkelstein,
et al., including P. Behroozi)
The following research results are released on the division’s
website (https://sci.nao.ac.jp/main/articles-en/) as researchhighlights:• Exploring Atmospheric Properties from Eclipse Data for 25
Hot Jupiters: New Phase in Exoplanet Atmosphere Research(Ikoma, et al.)• Brief Encounter with Mysterious Heavenly Event (Jiang,
Tominaga, Moriya, et al.)• Measuring the Universe with Star-Shattering Explosions(Dainotti, et al.)• Scientists Reveal Distribution of Dark Matter around Galaxies
12 billion Years Ago – Further Back than Ever Before (Ouchi,
et al.)• New Material “Fingerprint” to Understand Planetary System
Formation with ALMA (Yoshida, Nomuira, Furuya, et al.)• Discovery of Two Temperate Super-Earths, the Outer One
Orbits in the Habitable Zone (Ikoma, et al.)• New theory predicts Earth-like aqua planets exist around red
dwarfs (Ikoma, et al.)
• Machine Learning Reveals How Black Holes Grow (Behroozi
et al.)• Model-Independent Method to Weigh Protoplanetary Disks(Yoshida, et al.)• Crisis in Cosmology: Statistics on the rescue. (Dainotti, et al.)• An empirical method for mitigating an excess up-scattering
mass bias on the weak lensing mass estimates for shearselected cluster samples (Hamana, et al.)• Spiral arm high-mass protostellar accretion disk revealed byradio telescopes (Burns, et al.)• Magnetism in High-Mass Stars (Keszthelyi, et al.)

4. International and Domestic Collaborations
and Cooperations(1) International and Domestic Workshops
Restrictions on international meetings due to COVID-19
were relaxed this year. The division members organized or coorganized the following international and domestic workshops
as a hub of science activities, collaborating with internationaland domestic colleagues. This contributed to stimulating
research activities in astronomy and cross-disciplinary fields.
International Meetings• IRCC-AFP Meeting 2022 (Oct. 24–28, 2022 at Mitaka)• France-Japan Galaxy Formation Workshop (Nov. 16–17, at
The University of Tokyo)• Molecules in Extreme Environments: Near and Far (Nov.
23–25, 2022 at Mitaka)• Star Formation in Different Environments 2022 (Aug. 21–27,
2022, Vietnam/Quy Nhon)

090

II Status Reports of Research Activities

Domestic Meetings• Rironkon symposium 2022 (Dec. 21–23, 2022, Fukushima)• 11th Observational Cosmology workshop (Dec. 14–16, 2022,
Mitaka)• SKA-precursor ISM-WS2022 (June 27–28, 2022, Mitaka)• First star/First galaxy workshop 2022 (Nov. 10–12, 2022,
Tokushima University)(2) International and Domestic Observation Projects
In order to proceed with efficient collaborations between
theory and observations, and multi-wavelength astronomy,
the members of the division contributed to the following
observation projects. Also, the members contributed to thepromotion of international and domestic future plans related
to astronomy, including the plans for large telescopes in NAOJ
from a scientific perspective.
• GREX-Plus white paper (Fujii, Nomura)• LST white paper (Kobayashi, Furuya, Nomura)• ULTIMATE-Subaru white paper (Kobayashi)• Subaru SAC (Moriya, Ikoma)• GREX-PLUS science working group (Moriya, Nakajima,
Ouchi, Nomura)• Subaru/NINJA project (Moriya, Tominaga, Ouchi)• ULTIM ATE-Subar u science working group (Moriya,
Nakajima)• HSC SSP transient working group (PI: Moriya, Kokubo)• Euclid Consortium (Moriya)• LAPYUTA Working group (Science goal 4 Chief: Ouchi,
Moriya, Tominaga, Ikoma)• LST whitepaper (Moriya)• Roman-J (Moriya, Nakajima, Ouchi)• CASTOR working group (Moriya)• TMT-J SAC (Tominaga)• TMT WFOS Science Team (Nakajima)• ESA M4 Ariel (co-PI: Ikoma)• WSO-UV (Ikoma)• HSC SSP weak lensing working group (Hamana)• SKA1 study group (Machida)• VLBI SAC (Machida)• POSSUM Astrophysics Group1 (Machida)• POSSUM Astrophysics Group2 (Machida, Omae)• HST Cycle 30 Peer Review (Ouchi)• HSC SSP high-z galaxy working group (Ouchi)• Subaru PFS Collaboration (GE co-chairman: Ouchi, Kokubo)• HETDEX Collaboration (PI: Ouchi)• HSC SSP AGN working group (Kokubo)• ALMA-IMF Management team (Nakamura)• CARMA-NRO Orion Survey Collaboration (Nakamura)• Subaru proposal reviewer (Nomura)• BISTRO (Nakamura, Iwasaki)• NASA Swift Cycle 19 Review (Dainotti)• NASA postdoctoral Program Review (Dainotti)• Fermi-LAT mentors (Dainotti)

5. Educational and Outreach Activities
The division actively promotes the education of young
researchers, including students at graduate schools, to becomea career path center for astronomical researchers worldwide.
In FY 2022 the graduate students in the Division of Science
included thirteen SOKENDAI students (nine doctoral and four
master course students) and nine students in the Universityof Tokyo (six doctoral and three master course students), andone student in Konan University (master course student). In
addition, the members of the division engaged in the educationof graduate and undergraduate students in the following
universities and also high school students.
• Graduate student: Univ. Chinese Academy of Science (Fujii)• Graduate student: University of Salerno (Dainotti)• Graduate student: Scuola Meridionale Superiore of Naples(Dainotti)• Graduate student: Jagiellonian University (Dainotti)
The members of the division actively engaged in lecturesat the University of Tokyo and many other institutes anduniversities. In addition, spring school by the Division of
Science for undergraduate and master course students wasorganized in February 2023. The members also engaged inoutreach activities by offering lectures to the public.

II Status Reports of Research Activities091

18. Library
The purpose of the National Astronomical Observatory ofJapan (NAOJ) Library is to organize and preserve books andother valuable materials, and to make them available to NAOJ
staff, collaborating researchers, and others who wish to conduct
academic research or surveys. The library was established in
1988, taking over the collection of the Tokyo Astronomical
Observatory of the University of Tokyo in the Mitaka, Okayama,
and Nobeyama areas and the Latitude Observatory in the
Mizusawa area. With the incorporation of NAOJ in 2004, theLibrary was established in accordance with Article 20.3 of theGeneral Rules for Organization and Operation of the National
Institutes of Natural Sciences (General Rules No. 1, April 1,
2004). According to the Rules of the Library of the National
Astronomical Observatory of Japan (National Institute of
Natural Sciences Rules No. 41, April 1, 2004), the Director of
the Library is the Director of the Public Relations Center (PRC),
and the administrative work of the Library is handled by the
Library Section of PRC.
The collection includes many Japanese and Chinese books
and documents related to the history of astronomy and calendar
studies, including those originating from the Shogunate's
astronomical office in the Edo period. As part of the storageand management of these materials, we have been microfilming
rare Japanese and Chinese books and documents since 1984,
when the Tokyo Astronomical Observatory started to do it, incooperation with the Calendar Computation Office, and havebeen providing these materials to researchers. From 2009 to
2010, the microfilms were digitized and made publicly available
on the website, and from 2013, digital images of the rare books
themselves are being created.
In order to comply with the new application of theInformation Disclosure Act related to incorporation, a new
entrance for off-premises users was established in FY 2004, andbegan operation in April 2005. On the other hand, a common
MISHOP entry card key system was installed at the existing
entrance for internal users, allowing them to enter and leave thebuilding throughout the day.
See page 086 for details on the activities of the Library
Section in FY 2022, and Chapter XII, 1 (page 138) for the
library collection.

092

II Status Reports of Research Activities19. IT Security Office
IT Security Office (ITSO) has the following missions
to ensure information security at NAOJ while operating andprotecting information assets at NAOJ.
A) Management of servers that are open to the public.
B) Management education for the administrators of servers, etc.,
and matters related to operation rights and licenses.
C) Inspection and measures related to services for the public.
D) Management of accounts and licenses for network usage.
E) Management of recording, storage, and analysis of traffic
data.
F) Management of high-level confidential information
management book.
G) Management of the network.
H) Other matters necessary to ensure information security.
Based on these tasks, ITSO is performing the following six
items.
 Build and operate zero-trust and integrated communications
services based on Microsoft 365 services.
 Build, migrate, and operate network and telephony services.
 Provide information service infrastructure such as
virtualization and bare metal public servers.
 Operate cost-effective external and internal network services
in cooperation with various R&D networks, etc.
 Conduct security-related operations (CSIRT) in cooperation
with the Administrative Division, NINS, and MEXT.
 Collect information and collaborate with other organizations.
The highlights of our activities in FY 2022 are as follows.
(1) Reorganization of Datacenters
The ITSO has international connections to the
Subaru Telescope and NAOJ Chile Observatory throughinterconnections with the academic and educational R&D
networks, ARENA-PAC, and TRANS-PAC for wide-bandwidth
data transmission between the two observatories and Japan.
The NTT.COM Otemachi datacenter served as the core of thesedata transmissions for more than 15 years. In 2022, the building
was closed. ITSO worked the restructuring of the datacentersin Tokyo. In this project, we have deployed a new datacenterand 100 Gbps–400 Gbps transmission network. Now our new
datacenters have interconnections with ARENA-PAC, TRANSPAC, SINET6 of the National Institute of Informatics, and JGNof the National Institute of Information and Communications
Technology.
(2) High bandwidth data transmission with Subaru Telescope
HSC
With the cooperation of the University of Hawai`i and
ARENA-PAC, we constructed a high-bandwidth network
between Subaru Telescope and Tokyo to support HSC's remoteobservation tests.

II Status Reports of Research Activities093

20. Research Enhancement Strategy Office
The Research Enhancement Strategy Office was establishedas part of the functional enhancement program of the
National Institutes of Natural Sciences (NINS) to promote theenhancement of research capabilities in NAOJ. In FY 2022, theDirector of the Human Resources Planning Office, the Research
Assessment Manager, and the Finance Controller worked
as institutional URA staff members through the Research
University Enhancement Promotion Grant, and conducted theirfunctional work using their respective expertise, which should
not be performed by research staff.
In addition, to promote cross-disciplinary research, a
research agreement was concluded with the Institute of
Statistical Mathematics (ISM), and two young researchers(assistant professors) were seconded from NAOJ to ISM todevelop astroinformatics/astrostatics, which attempts to discover
new phenomena from large-scale observational data obtainedwith large telescopes, etc.
Furthermore, the Research Assessment Support Office andthe Industry Liaison Office were established under the Research
Enhancement Strategy Office to contribute to the acceleration of
NAOJ's research capabilities through their respective specialized
work. The activities of each office in FY 2022 are as follows.

1. Research Assessment Support Office(1) Implementation of Project Evaluation
For the international external review of the Division of
Science (March 2–3, 2023), as the secretariat of the NAOJ
Project Review Committee, we supported the external review
committee (two international and five domestic committee
members) from the request for appointment as committee
members to the preparation of the review plan and input
documents by the Division of Science and managed the review
process.
In addition, we supported the preparation of the final
versions of the review reports (4 projects) for FY 20211.
(2) Planning of research evaluation methodology
We prepared a revised draft of the project review procedureand proposed holding an NAOJ overall evaluation, which has
not been conducted since FY 2014.
In addition, to promote the collection and utilization of theresults of open use and research, we drafted a policy for the
NAOJ Repository together with the NAOJ Library and prepared
for its release.
(3) Response to the Evaluation of the Inter-University ResearchInstitute Corporation
Under the leadership of the Director General, together
with the members of the Evaluation Task Force (Vice Director
General Saito, Director of Research Coordination Motohara,
and Associate Professor Machida) and the General Affairs Unit,
General Affairs Group, we prepared materials and confirmed

094

II Status Reports of Research Activities

evaluation results for the “Evaluation of Performance for theThird Mid-term Period” by MEXT, and provided support for
preparations for the Objective of the Fourth Mid-term Period(4) Enhancement of Research InfrastructureWith the cooperation of various groups/projects/offices/
centers within NAOJ, we conducted a literature survey andanalysis, collected information on strengthening researchcapabilities, organized those research achievements, andpresented our report.
In addition, as the LOC for the “NAOJ Future Planning
Symposium 2022: How to decide and promote future plans”(December 7–8, 2022) 2 , we supported the holding of thesymposium together with the Research Support Unit.
In addition, we participated in the NINS Open Use/
Collaborative Research Team and Research and Management
Strategy Analysis Team and exchanged information on efforts
and achievements to contribute to the strengthening of university
research capabilities.

2. Industry Liaison Office(1) Collaboration with private companies
One case each of joint research, entrusted research, andcommissioned business, and two cases of academic consultation
were realized with private companies. There are also several
projects that are still under discussion, and NAOJ's system forhandling industrial collaborations is being put in place.
(2) Participation in exhibitions
In order to promote NAOJ's technologies, we provided
support for participation in exhibitions for the industrial sector.
- Innovation Japan 2022 (October 4–31): Adaptive optics
technology and stereoscopic computer graphics technology- Science Photonics Fair 2022 (November 9–11)(3) Press Lectures
The 28th Astronomy Lecture for Science Journalists“Technological Development in NAOJ and Collaboration
with Industry” was held on December 1, 2022 in cooperation
with the NAOJ Public Relations Center. The lectures
covered an overview of NAOJ's technological development,
superconducting receiver development, and satellite instrument
development, and were attended by 18 participants. This wasfollowed by a tour of the Advanced Technology Center, which
was attended by 14 people. The event received a good response,with articles in Jiji Press, Nikkan Kogyo Shimbun, Yomiuri
KODOMO Shimbun, and other newspapers.

1
2

https://www.nao.ac.jp/en/about-naoj/reports/external-review.html
https://www.nao.ac.jp/for-researchers/naoj-symposium2022/indexE.html

21. Office of International Relations
The Office of International Relations (OIR) strives topromote internationalization at NAOJ by collecting andproviding information on international research exchange andeducation and creating an environment where multiculturalresearchers and students can engage cooperatively in researchand educational activities. Specifically, the main activities of
the OIR include promoting international research collaboration,
supporting visiting international researchers and students, anddisseminating information at international conferences. In FY
2022, despite the continued impact of COVID-19, there was aslight increase in the number of incoming international visitors.
While the office could not fully resume all its scheduled events,
it took advantage of this time to reallocate its efforts to otheractivities.

1. Promoting International Research
Collaboration
The OIR serves as the contact point for the East AsianCore Observatories Association (EACOA) and the East Asian
Observatory (EAO) and manages both the EAO/EACOA budgets
within NAOJ. The EACOA consists of four core observatories
representing the East Asian regions: the NAOJ (Japan), theNational Astronomical Observatories of China (China), the Korea
Astronomy and Space Science Institute (Republic of Korea), and
the Academia Sinica Institute of Astronomy and Astrophysics(Taiwan), and the EAO is operated by these EACOA members
and the National Astronomical Research Institute of Thailand. In
October 2022, the EAO/EACOA Review Meeting of NAOJ wasestablished with the OIR as the secretariat. Since then, the OIR
has been formally in charge of the EAO/EACOA operations at
NAOJ. In November 2022, the EAO held its regular Board of
Directors (BOD) meeting in Chiang Mai, Thailand, as a hybrid
meeting, including the first face-to-face meeting in a long timesince the outbreak of COVID-19. The OIR assisted the NAOJ
representative in this meeting as well as in each of EAO’s online
meetings, such as special BOD meetings, and supported one
post-doctoral young researcher (EACOA Fellow) whom NAOJ
hosted under the EACOA Fellowship Program.
Besides the duties mentioned above, the OIR has been in
charge of reviewing legal documents, such as agreements andmemoranda for international collaboration between NAOJ andoverseas institutions. In FY 2022, the office reviewed a totalof 26 new or renewed international agreements and drafted
revisions as needed. In July 2022, with the expectation of further
advancing the cooperation between Japan and Lebanon in thefield of astronomical research, the Director General of NAOJ
and the President of Notre Dame University in Lebanon (NDU)
signed a Memorandum of Understanding for Research andAcademic Collaboration (MOU) for conducting joint observation
and research on transient celestial bodies, asteroids, and variableobjects. The signing ceremony was held online, with theattendance of the Ambassador of the Lebanese Embassy in Japan.

2. Support Services for International
Researchers and Students
The Support Desk (SD) of the OIR offers a broad range ofservices to help international researchers and students overcome
their difficulties in living in Japan. During FY 2022, to preventthe spread of COVID-19, the SD staff worked mainly remotely byproviding consultation services over the phone, e-mail, and online
conference systems. However, in some instances where on-site
assistance was necessary or requested, the SD staff accompaniedinternational researchers and students to municipal offices andother places to complete various procedures. In addition, the SD
staff made full use of the "NAOJ Support Desk Registration Form,"
which was put into operation in FY 2021 as part of an effort
to strengthen SD services. By having international researchersand students submit this form before their visit, the SD staff canobtain accurate information in a timely manner and be prepared
to provide appropriate support for facilitating the relocation
process to help establish an environment in which incomers canconcentrate on their research as quickly as possible.
Since its launch in July 2021, the OIR has maintained its
website to provide information to international researchersand students both inside and outside NAOJ. The website
contains practical information on immigration procedures,
accommodations, campus neighborhoods, daily life, and reference
information for NAOJ host researchers and staff. Although all
information is provided in both Japanese and English, according
to the current statistics, one-fourth of the website visitors haveread the English version, indicating that it is widely used among
non-Japanese speakers. At the same time, active efforts topublicize the website have helped promote its use among NAOJ
researchers.
In parallel with these services, the OIR continues tocollaborate with a specialized company to offer beginner-level
Japanese language classes to help international researchers andstudents quickly adjust to life in Japan. Starting in FY 2021, a new
curriculum was introduced to provide a program that better suits
the needs of students. Both the beginner and intermediate courses
offer lessons that have been developed in response to the requests
of former students, where a speech-centered method is used toprovide “practical Japanese for daily life.” In addition, by using
supplementary learning tools such as e-learning and enhancing
instructor presence, students are given the freedom to study attheir convenience. The courses were well received by the students,
who remained highly motivated to learn. As a result, in FY 2022,
there were no dropouts aside from those who had to quit due towork-related reasons, and the majority of students were able toacquire more practical Japanese language skills.

3. Information Dissemination at International
Conferences
The OIR has been exhibiting booths at international

II Status Reports of Research Activities095conferences to recruit international researchers by providing
information about NAOJ’s research activities and invitational
programs. In FY 2022, the OIR engaged in the active
dissemination of information to approximately 750 visitors to the
NAOJ booth at the International Astronomical Union General
Assembly (IAUGA 2022) held in Busan, Korea in August 2022,
and approximately 600 visitors to the NAOJ booth at the 241st
American Astronomical Society Meeting (241st AAS Meeting)held in Seattle, USA in January 2023.
Furthermore, the OIR supports other NAOJ departmentsthat plan to host or participate in international conferences.
As a part of this duty, the OIR has been working as a memberof the local organizing committee to provide support forwelcoming participants and to start preparations for setting up
the NAOJ exhibition booth at the Asia-Pacific Regional IAU
Meeting (APRIM 2023) to be held in August 2023 in Koriyama,
Fukushima Prefecture.

096

II Status Reports of Research Activities22. Human Resources Planning Office
The main duties of the “Human Resources Planning Office”
are to plan and implement staff performance management,
talent development, and labor management; and to contributeto the continuity and development of NAOJ's business from apersonnel perspective, while working closely with the Director
General, NAOJ Executives, and the Administration Department.
Specifically, the scope of work of the Human Resources
Planning Office includes operation of the Objective Sharing
and Talent Development System; development of leaders;planning and implementation of training programs; managementof fixed-term employees; creation of a harassment-free work
environment; and handling of individual labor issues.
In FY 2022, due in part to the impact of prevention measuresagainst the spread of the novel coronavirus, face-to-face training
programs could not be implemented, but the following initiatives
were appropriately carried out.

4. Others
The Human Resources Manager participated in the ALMA
HR AG (Human Resource Advisory Group) as a member of
NAOJ's delegation to ALMA's HR Advisory Group and actively
exchanged ideas. The Office continued to coordinate andnegotiate for Joint ALMA Observatory (JAO) staff recruitment
and NAOJ staff seconded to JAO.

1. Objective Sharing and Talent Development
SystemThe “Objective Sharing and Talent Development System”
was properly operated to set annual goals and evaluate thedegree of achievement at the end of the fiscal year for researchand education staff, technical staff, and annual salaried staff.
The evaluation results of the “Objective Sharing and Talent
Development System” were reflected in the diligence allowance(June and December) and January salary increase for researchand education staff and technical staff, and in the annual salaryamount for annual salary system staff.

2. General Employment Management for
Fixed-term Staff
We supported appropriate employment policies for fixedterm staff, including more than 270 salaried staff in a wide
range of employment categories (e.g., operating the Fixed-Term
Employee Review Committee, operating the policy for hiring
staff who are transitioning to the Mandatory Retirement System,etc.).

3. Handling of Harassment, Mental Health, andIndividual Labor Issues
We responded promptly and courteously to consultations
on harassment (consultations with the external consultation
service, with internal counselors, and with the Human Resources
Planning Office), and took appropriate measures, etc., based on
fact-finding.
In addition, the Human Resources Manager worked with
the Employee Affairs Unit of the Administrative Division on
measures to prevent harassment (e.g., conducting training andpreparing leaflets).

II Status Reports of Research Activities097

23. Safety and Health Management Office
The mission of the Safety and Health Management Office
is to prevent accidents through appropriate management andoperation of NAOJ facilities, equipment, and devices and topromote the creation of a comfortable work environment by
maintaining the safety, health, and well-being of employees.
Specifically, the office holds Safety and Health Committee
meetings and promotes information sharing, conducts periodic
safety and health patrols and work environment measurements,
provides safety and health education, implements healthcare
and safety and health training programs, and develops rules andmanuals on workplace safety and health.
Although the director of the office had just been newly
appointed in 2022, the office successfully implemented
preexisting plans, including the continuation of COVID-19
infection prevention measures, the revision of the safety andhealth manuals, and the implementation of voluntary routine
inspections of observatories, including overseas observatories.

1. Holding Safety and Health Committee
Meetings and Promoting Information Sharing
The Safety and Health Committee promotes safety andhealth activities through the committees that are organized ateach work site, namely the Mitaka (including the Okayama
Branch, Kamioka Branch, and Thirty Meter Telescope (TMT)
Project / California Office), Nobeyama, Mizusawa, Hawai`i, andChile districts. The activities of each committee are reported andshared on a monthly basis. In addition to the monthly reports,
committee members and observers from each district and branch
participate in a quarterly all-hands meeting to share information.
The month following a quarterly meeting, important matters arereported at the Project Director Committee, which is attended by
all staff at the management level, including the Director General,
Vice-Director Generals, and Directors of Projects and Centers.
In FY 2022, the committee successfully promoted theplanned activities and achieved the following results.

2. Periodic Patrols and Environmental
Measurements
The health officer (Safety and Health Management Office
Staff) conducted regular weekly patrols at each workplace in
the Mitaka district and left comments for improvement upon
noticing any problems or points of concern.
Alongside the patrols, environmental measurements(illuminance, room temperature, humidity, discomfort index,
Carbon Dioxide concentration, formaldehyde, and suspended
particulate matter PM10) were conducted using a digital
illuminance meter and Air Quality Monitor newly purchased
in FY 2022, and quantitative data were used to check theworkplace environment in more detail, which enabled the office
to gain further insights into the areas for improvement.
In addition, at the end of September 2022, the Subaru

098

II Status Reports of Research Activities

Telescope / Okayama Branch hosted a special joint patrol
program on safety management with the National Institutes of
Natural Sciences. Furthermore, as a part of the voluntary safety
and health routine inspections, the office conducted patrols
at Nobeyama Radio Observatory in early September 2022,
Mizusawa VLBI Observatory in early November 2022, andSubaru Telescope in late February 2023 and identified the statusof maintenance and improvement measures for preventing therecurrence of accidents in each district.

3. Safety and Health Education
As in previous years, a safety and health workshop (special
education for workers who transferred jobs or are engaged inhazardous operations) was held on May 11, 2022.
Course Content:□Physicochemical Hazards of Chemical Substances□Health Hazards of Chemical Substances□Respirators□Protections□New Occupational Safety and Health Laws and Regulations
Participants who completed this course were certified ashazardous materials practitioners for handling “coolants, highpressure gases, cold evaporators (CE), organic solvents, andspecified chemical substances.”
Number of certificates issued: 78 (18 for NAOJ staff, 60 for
students / external staff, etc.)
Other: 1 person participated in CE handling practical training.
The office also worked in cooperation with the Engineering
Promotion Office to hold the “System Safety Training” on
December 9, 2022.
Course Content:□What is System Safety (Overview)□Necessity of System Safety (Examples of Accidents)□System Safety Methodology
Flow of Hazard Analysis, Hazard Countermeasures (Removal,
Fault Tolerance, Risk Minimization, etc.)□Effects of System Safety
Number of Participants: 61 (12 management-level participants,
including Directors of Projects)

4. Healthcare and Safety and Health Training
In fulfilling the responsibilities of a health officer, the officeassisted in promoting the following tasks.
□Health Examination□Influenza Vaccination□Stress Check□Development of “Support Program for Employees Returningfrom Mental Health Leave”□Health Consultation with Occupational Physicians in the
Mitaka district□General Lifesaving Course5. Development of Rules and Manuals
The contents of the safety and health manuals (main andseparate volumes; versions for each branch version) werereviewed. In addition to confirming the necessity of revisions
and issuing revised versions, it was agreed that from now on,
the office will regularly check the need for such revisions atintervals of 1 to 2 years.
□Revised “NAOJ Safety and Health Manual”□Revised “NAOJ Branch Manuals”

II Status Reports of Research Activities099

24. Engineering Promotion Office
1. Outline
The Engineering Promotion Office (EPO) aims to improve
the overall level of NAOJ’s engineering capability and facility
operation by coordinating the skill development of engineering
staff. Specifically, EPO acts mainly on “assigning engineering
staff”, “engineering staff human resource development”, and“other areas needed to improve the engineering capabilities.”

2. Assignment of Engineering Staff
The engineering staff which consists of engineers andresearch engineers, work on NAOJ’s engineering issues withadvanced expertise and a high sense of responsibility.
EPO considers the balance between a long-term plan of
human resource and technological capability development
and the efficient completion of individual technology projects.
Then, EPO prepares and maintains a human resources portfolio
to make medium- and long-term personnel promotion andhiring proposals.
In FY 2022, we cooperated in the recruitment of one
Associate Senior Research Engineer and three ResearchEngineers, and promoted one Senior Engineer, five Engineers,and hired one Engineer.

3. Engineering Staff Human Resource
Development
Human resource development for engineering staff is being
conducted based on the documents compiled for that purpose
in FY 2020. Specifically we are systematizing the line of work
based on the duties of engineering staff. We are also renewing
the human resource development sheet, which had been
simplistic in the past, and communicating the competency foreach line of work and job level with superiors, so that the sheet
can be used as a tool for career path planning.
As for training, 11 engineering staff participated in an
e-learning English training course. In FY 2022, the external
lecturers' training course on systems engineering including
practical exercises, which has been conducted since FY 2020,
was held jointly with the High Energy Accelerator Research
Organization (K EK) with 40 par ticipants f rom NAOJ.
Systems safety training was conducted by NAOJ staff with 61
participants from NAOJ. For some training courses, lectures
were recorded and made available for viewing from NAOJ tocreate an environment where participants can continue to takethe courses.
The 42nd Symposium on Engineering in Astronomy 2022
was held without a hitch, entrusting the management of thesymposium to the engineering staff. The symposium wasattended by more than 90 engineers and researchers fromNAOJ and elsewhere. The symposium aimed to provide aforum for engineers and researchers involved in astronomy to100

II Status Reports of Research Activities

exchange technical information on the design, development,
improvement, and daily operation of astronomical instruments,
and to contribute to technological development in the field ofastronomy.

4. Other areas needed to improve theengineering capabilities
As for the safety and product development assurance in
NAOJ, a standard document of S&PA (Safety and Product
Assurance) for NAOJ is being developed. We have developed
the system to collect and communicate the alert informationsuch as defects and the availability of products and parts
that may be used in NAOJ, and to share the information withconcerned parties. The operation method for this system has
been studied.

25. Graduate Education Office
The Graduate Education Office was established in April 2022
to lay a basis for the sustainable and developing managementof graduate education at NAOJ by systematically managing theefforts for graduate education related to the Graduate University
for Advanced Studies (SOKENDAI), cooperative graduate
schools, NAOJ Special Inter-Institutional Research Fellows, andothers.
With the establishment of the Graduate Education Office,it is expected that the future leaders of graduate education at
NAOJ will have the opportunity to accumulate experience inthe management of graduate education under the auspices ofan organizationally recognized effort. The Graduate Education
Office also acts as a window for cooperation between NAOJ andother universities or research institutions.
The Graduate Education Office also oversees the Graduate
Education Committee and the Committee of the Department of
Astronomical Science, School of Physical Sciences, (reorganized
as Astronomical Science Program, the Graduate Institute forAdvanced Studies from FY 2023) at SOKENDAI. In FY 2022,
in preparation for SOKENDAI's reorganization, the Graduate
Education Office worked on curriculum reorganization; reformulation of educational goals and basic policies; etc. In
addition, the scope of the cooperative graduate school programwith the Graduate School of Science at the University of Tokyo
was expanded to include the Department of Earth and Planetary
Science to further strengthen cooperative graduate school
education at NAOJ. For graduate students, individual meetings
between SOKENDAI students and members of the Graduate
Education Office were arranged for all students to further
enhance support for graduate students.
For further information, refer to section Ⅶ “Graduate
Education.”

Faculty Council of Graduate Schoolof Physical Sciences, SOKENDAI

Director General, NAOJ

Graduate Education Office

Faculty Meeting of the Department of
Astronomical Science

Graduate Education
Committee-Committee of Department of
Astronomical Science, SOKENDAI
Faculty members of the Departmentof Astronomical Science

Faculty members of NAOJ

Figure 1: Organizational chart showing the position of the Graduate Education Office within NAOJ.

II Status Reports of Research Activities

101III Organization
1. Organization

Projects(C Projects)

Mizusawa VLBI Observatory
Nobeyama Radio Observatory
Solar Science Observatory
Subaru Telescope
Center for Computational Astrophysics
Advisory Committee for Research and Management

NAOJ Chile
ALMA Project(B Projects)

Gravitational Wave Science Project
Thirty Meter Telescope (TMT) Project
Director General(A Projects)

JASMINE ProjectVice-Director General (on General Affairs)
Vice-Director General (on Finance)
Director of Engineering

RISE Project
SOLAR-C Project
Subaru Prime Focus Spectrograph (PFS) Project
Subaru Ground Layer Adaptive Optics (GLAO) Project
ASTE Project

Director of Research Coordination
Executive Advisors to the Director General

Centers
Astronomy Data Center
Advanced Technology Center
Public Relations Center
Division of Science
Collaborative Projects
Inter-university Collaboration: Optical and Infrared
Synergetic Telescopes for Education and Research (OISTER)
Inter-university Collaboration: Japanese
VLBI Network (JVN)
Library
IT Security Office
Research Enhancement Strategy Office
Research Assessment Support Office
Industry Liaison Office
Office of International Relations
Human Resources Planning Office
Safety and Health Management Office
Engineering Promotion Office
Graduate Education Office
Administration Department

102

III Organization

2. Number of Staff Members
Director General
Research and Academic Staff
Professor
Executive Engineer
Associate Professor
Senior Research Engineer
Associate Professor (Senior Lecturer)
Associate Senior Research Engineer
Assistant Professor
Research Associate
Research Engineer
Engineering Staff
Administrative Staff
Research Administrator Staff
Employees on Annual Salary System
Research Administrator Staff Transferring to the
Mandatory Retirement System
Employees on Annual Salary System Transferring to the
Mandatory Retirement System
Full-time Contract Employees
Full-time Contract Employees Transferring to the
Mandatory Retirement System
Part-time Contract Employees
Part-time Contract Employees Transferring to the
Mandatory Retirement System(2023/3/31)
1
149
31
1
38
8
6
3
51
0
11
40
58
2
152
1
3
34
2
80

15

3. Executives
Director General
Vice-Director General
on General Affairs
on FinanceDirector of Engineering
Director of Research Coordination

Tsuneta, Saku

Executive Advisor to the Director General
Executive Advisor to the Director General
Executive Advisor to the Director General

Hiramatsu, Masaaki
Kurasaki, Takaaki
Sekiguchi, Kazuhiro

Yoshida, Michitoshi
Saito, Masao
Uzawa, Yoshinori
Motohara, Kentaro

III Organization

1034. Research Departments
Projects
C Projects

Mizusawa VLBI Observatory
Director
Honma, Mareki
Professor
Honma, Mareki
Project Professor
Kobayashi, Hideyuki
Associate Professor
Hirota, Tomoya
Assistant Professor
Hada, Kazuhiro
Assistant Professor
Jike, Takaaki
Assistant Professor
Kouno, Yusuke
Assistant Professor
Sunada, Kazuyoshi
Project Assistant
Sakai, Daisuke
Professor
Engineer (Gishi)
Ueno, Yuji
Engineer
Takahashi, Ken(Shunin Gijutsuin)Engineer (Gijutsuin)Sato, Gen
Project Researcher
Akahori, Takuya
Project Researcher
Kurahara, Kohei
Senior Specialist
Hachisuka, Kazuya(Tokuninsenmonin)
Senior Specialist
Oyama, Tomoaki(Tokuninsenmonin)
Senior Specialist
Ozawa, Tomohiko(Tokuninsenmonin)
Technical Experts
4
Research Supporters
2
Administrative Supporters 2
Administration Office
Head of Administration Onuma, Toru
OfficeGeneral Affairs Unit
LeaderOnuma, Toru
Re-employment Staff
1
Administrative Supporters 3
Accounting Unit
Leader
Kogawa, Hiroshi
Re-employment Staff
1
Administrative Supporter 1
Nobeyama Radio Observatory
Director
Professor
Project Associate
Professor
Engineer (Gishi)
Engineer (Gishi)
Engineer (Gishi)
Engineer (Gishi)
Re-employment Staff
Research Supporters

104

III Organization

Tatematsu, Kenichi
Tatematsu, Kenichi
Nishimura, Atsushi
Handa, Kazuyuki
Kurakami, Tomio
Miyazawa, Chieko
Takahashi, Toshikazu
12Administration Office
Head of Administration Tatematsu, Kenichi
OfficeGeneral Affairs Unit
Re-employment Staff
1
Administrative Supporters 2
Accounting Unit
Administrative Supporters 2
Solar Science Observatory
Director
Katsukawa, Yukio
Professor
Katsukawa, Yukio
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Ishikawa, Ryoko
Assistant Professor
Narukage, Noriyuki
Project Assistant
Benomar, Othman Michel
Professor
Engineer (Gishi)
Shinohara, Noriyuki
Project Researcher
Ishikawa, Ryohtaroh
Senior Specialist
Morita, Satoshi(Tokuninsenmonin)
Research Supporters
2
Administrative Supporter 1
Subaru Telescope
Director
Miyazaki, Satoshi
Vice-Director
Hayano, Yutaka
Professor
Hayano, Yutaka
Professor
Miyazaki, Satoshi
Professor
Yoshida Michitoshi
Project Professor
Takami, Hideki
Project Professor *Tamura, Motohide
Associate Professor
Koyama, Yusei
Associate Professor
Minowa, Yosuke
Associate Professor
Tanaka, Masayuki
Project Associate
Kambe, Eiji
Professor
Senior Research Engineer Iwashita, Hiroyuki
Senior Research Engineer Kumura, Yoshinori
Assistant Professor *Hirano, Teruyuki
Assistant Professor
Imanishi, Masatoshi
Assistant Professor
Ishigaki, Miho
Assistant Professor *Kotani, Takayuki
Assistant Professor
Moritani, Yuki
Assistant Professor *Nakajima, Tadashi
Assistant Professor
Okamoto, Sakurako
Assistant Professor
Okita, Hirofumi
Assistant Professor
Onodera, Masato
Assistant Professor
Ono, Yoshito
Assistant Professor
Pyo, Tae-Soo
Assistant Professor *Suto, Hiroshi
Assistant Professor
Yanagisawa, KenshiProject AssistantProfessor *Project AssistantProfessor *Project AssistantProfessor *Project AssistantProfessor *Project AssistantProfessor
Project AssistantProfessor
Research Engineer
Research Engineer
Senior Engineer
Engineer(Shunin Gijutsuin)Engineer(Shunin Gijutsuin)Engineer(Shunin Gijutsuin)Engineer(Shunin Gijutsuin)
Project Researcher
Project Researcher
Project Researcher *Project Researcher
Project Researcher *Project Researcher
Project Researcher
Project Researcher
Project Researcher *Project Researcher *Project Researcher *Project Researcher *Project Researcher
Project Researcher
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin) *Senior Specialist(Tokuninsenmonin)

Hashimoto, Jun
Hori, Yasunori
Kuzuhara, Masayuki
Livingston, John Henry
Shimakawa, Rhythm
Toba, Yoshiki
Bando, Takamasa
Omiya, Jun
Namikawa, Kazuhito
Hirano, Ken
Sato, Tatsuhiro
Sawatari, Koichi
Tsutsui, Hironori
Hamano, Satoshi
He, Wanqiu
Ishikawa, Hiroyuki
Kawanomoto, Satoshi
Komatsu, Yu
Mawatari, Ken
Murata, Kazumi
Nakata, Fumiaki
Nugroho, Stevanus
Kristianto
Omiya, Masashi
Takahashi, Aoi
Takarada, Takuya
Wong, Kenneth
Christopher
Yamashita, Takuji
Fujinawa, Toshiyuki
Harasawa, SumikoIshii, Miki
Ishizuka, Yuki
Katakura, Junichi
Kobayakawa, Naoki
Kusakabe, Nobuhiko
Mineo, Sogo

Senior Specialist
Morishima, Takahiro(Tokuninsenmonin)
Senior Specialist
Nakajima, Masayo(Tokuninsenmonin)
Senior Specialist
Oka, Shinji(Tokuninsenmonin)
Senior Specialist
Okura, Yuki
(Tokuninsenmonin)
Senior Specialist
Shindo, Miwa
(Tokuninsenmonin)
Senior Specialist
Tanaka, Mitsuhiro(Tokuninsenmonin)
Re-employment Staff
2
Administrative Expert
1
Research Supporters
2
Administrative Supporters 4*concurrently appointed in NINS
Administration Department
Manager
Furuhata, Tomoyuki
General Affairs Unit
Staff
Tamura, Makoto
Accounting Unit
LeaderSugawara, Satoshi
RCUH
RCUH Staff
68
Okayama Branch OfficeDirector
Tajitsu, Akito
Associate Professor
Izumiura, Hideyuki
Project Associate
Tajitsu, Akito
Professor
Assistant Professor
Maehara, Hiroyuki
Administrative Supporters 2
Center for Computational Astrophysics
Director
Kokubo, Eiichiro
Professor
Kokubo, Eiichiro
Associate Professor
Takiwaki, Tomoya
Associate Professor
Ito, Takashi(Senior Lecturer)
Assistant Professor
Iwasaki, Kazunari
Project Researcher
Ideguchi, Shinsuke
Project Researcher
Keszthelyi, Zsolt
Project Researcher
Matsumoto, Yuji
Project Researcher
Nozawa, Takaya
Project Researcher
Taki, Tetsuo
Senior Specialist
Fukushi, Hinako(Tokuninsenmonin)
Senior Specialist
Hohokabe, Hirotaka(Tokuninsenmonin)
Senior Specialist
Kato, Tsunehiko(Tokuninsenmonin)
Research Expert
1
Research Supporters
3
Administrative Supporter 1
NAOJ Chile

III Organization

105Director
Vice-Director
Associate Professor
Engineer (Gishi)
Engineer(Shunin Gijutsuin)Senior Specialist(Tokuninsenmonin)
Chile Employee
Chile Employees
Administration Department
Manager
General Affairs Unit
Staff
Accounting Unit
Senior Staff

Watanabe Teruyuki
Mizuno, Norikazu
Minamidani, Tetsuhiro
Kobiki, Toshihiko
Nishitani, Hiroyuki
Watanabe, Teruyuki

6
Watanabe, Teruyuki
Iwasaki, Yumi
Yamafuji, Yasuto

ALMA Project
Director
Gonzalez Garcia, Alvaro
Professor
Fukagawa, Misato
Professor
Gonzalez Garcia, Alvaro
Professor
Iguchi, Satoru
Professor
Kameno, Seiji
Professor
Mizuno, Norikazu
Professor
Sakamoto, Seiichi
Project Professor
Kiuchi, Hitoshi
Associate Professor
Asaki, Yoshiharu
Associate Professor
Hatsukade, Bunyo
Associate Professor
Okuda, Takeshi
Associate Professor
Sawada, Tsuyoshi
Associate Professor
Shimojo, Masumi
Associate Professor
Takahashi, Satoko
Project Associate
Ishii, Shun
Professor
Project Associate
Nagai, Hiroshi
Professor
Project Associate
Nakanishi, Kouichiro
Professor
Senior Research Engineer Kikuchi, Kenichi
Senior Research Engineer Sugimoto, Kanako
Senior Research Engineer Watanabe, Manabu
Assistant Professor
Ezawa, Hajime
Assistant Professor
Hirota, Akihiko
Assistant Professor
Izumi, Takuma
Assistant Professor
Kamazaki, Takeshi
Assistant Professor
Matsuda, Yuichi
Project AssistantCataldi, Gianni
Professor
Project Assistant
Imada, Hiroaki
Professor
Project Assistant
Saito, Toshiki
Professor
Project Assistant
Sanhueza Nunez, Patricio
Professor
Andres
Project Assistant
Tokuda, Kazuki
Professor

106

III Organization

Project AssistantProfessor
Project AssistantProfessor
Research Engineer
Research Engineer
Engineer (Gishi)
Engineer (Gishi)
Engineer(Shunin Gijutsuin)Engineer(Shunin Gijutsuin)
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)

Wu, Yu-Ting
Zavala Sorano, Jorge
ArmandoNakazato, Takeshi
Yamada, Masumi
Kato, Yoshihiro
Nakamura, Kyoko
Ito, Tetsuya
Shizugami, Makoto
Algera, Hiddo SunnyBouwe
Bakx, Tom Johannes
Lucinde Cyrillus
Chen, Xiaoyang
Cheng, Yu
Feeney-Johansson, Anton
Fiachra George
Fudamoto, Yoshinobu
Kaneko, Hiroyuki
Kudo, Yuki
Michiyama, Tomonari
Miley, James Maxwell
Saha, Piyali
Silva Bustamante,Andrea Ludovina
Sugahara, Yuma
Takahashi, Sanemichi
Asanuma, Masumi
Ebihara, Eiichi
Fukui, Hideharu
Funakawa, Takashi
Ikeda, Emi
Inoue, Naoko
Kawasaki, Wataru
Konuma, Mika
Miel, Renaud Jean
Christphe
Nakayama, Susumu
Otawara, Kazushige
Shakunaga, Takeshi
Shimada, KazuhikoSenior Specialist
So, Ryoken(Tokuninsenmonin)
Senior Specialist
Tagawa, Hiroaki(Tokuninsenmonin)
Senior Specialist
Uemizu, Kazunori(Tokuninsenmonin)
Senior Specialist
Yoshino, Akira(Tokuninsenmonin)
Senior Specialist
Zahorecz, Sarolta(Tokuninsenmonin)
Re-employment Staff
1
Technical Expert
1
Administrative Expert
1
Research Supporter
1
Public Outreach Staff
1
Administrative Supporters 3
Research Assistant Staff 1

B Projects

Gravitational Wave Science Project
Director
Tomaru, Takayuki
Professor
Tomaru, Takayuki
Associate Professor
Aso, Yoichi
Assistant Professor
Akutsu, Tomotada
Assistant Professor
Takahashi, Ryutaro
Engineer
Tanaka, Nobuyuki(Shunin Gijutsuin)
Project Researcher
Eisenmann, Marc
Project Researcher
Page, Michael Anthony
Administrative Expert
1
Research Supporter
1
Administrative Supporter 1
Kamioka Branch OfficeDirector
Tomaru, Takayuki
Assistant Professor
Chen, Dan
Project AssistantWashimi, Tatsuki
Professor
Senior Specialist
Ikeda, Satoru(Tokuninsenmonin)
Administrative Supporter 1
Thirty Meter Telescope (TMT) Project
Director
Usuda, Tomonori
Vice-Director
Aoki, Wako
Professor
Aoki, Wako
Professor
Usuda, Tomonori
Professor
Saito, Masao
Professor
Yamashita, Takuya
Project Professor
Kurasaki, Takaaki
Associate Professor
Iono, Daisuke
Associate Professor
Noumaru, Junichi
Associate Professor
Sugimoto, Masahiro
Associate Professor
Suzuki, Ryuji
Assistant Professor
Nishikawa, Jun
Assistant Professor
Yasui, Chikako

Project AssistantProfessor
Research Engineer
Project Researcher
Senior Specialist(Tokuninsenmonin)
Research Supporter
Senior Specialist(Tokumeisenmonin)
NAOJ California Office
Associate Professor
Associate Professor
Research Engineer

Tadaki, Kenichi
Tazawa, Seiichi
Lee, Kianhong
Kakazu, Yuko
1
1

Hayashi, Saeko
Terada, Hiroshi
Nakamoto, Takashi

A Projects

JASMINE Project
Director
Professor
Professor
Project Associate
Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Project AssistantProfessor
Project Researcher
Technical Supporter
RISE Project
Director
Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Project Researcher
Administrative Expert
Public Outreach Staff

Gouda, Naoteru
Gouda, Naoteru
Kano, Ryouhei
Kataza, Hirokazu
Miyoshi, Makoto
Ohsawa, Ryou
Tatsumi, Daisuke
Tsujimoto, Takuji
Ueda, Akitoshi
Yano, Taihei
Baba, Junichi
Miyakawa, Kohei
1Namiki, Noriyuki
Namiki, Noriyuki
Matsumoto, Koji
Araki, Hiroshi
Kikuchi, Shota
Noda, Hirotomo
Yamamoto, Keiko
1
1

SOLAR-C Project
DirectorHara, Hirohisa
Professor
Hara, Hirohisa
Assistant Professor
Kawabata, Yusuke
Assistant Professor
Kubo, Masahito
Assistant Professor
Okamoto, Takenori
Engineer (Gishi)
Shinoda, Kazuya
Project Researcher
Oba, Takayoshi
Senior Specialist
Nodomi, Yoshifumi(Tokuninsenmonin)
Administrative Supporters 2

III Organization107Subaru Prime Focus Spectrograph (PFS) Project
Director
Rousselle, Julien
Subaru Ground Layer Adaptive Optics (GLAO) Project
Director
Minowa, Yosuke
ASTE Project
Director

Minamidani, Tetsuhiro

Centers
Astronomy Data Center
Director
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate SeniorResearch Engineer
Assistant Professor
Assistant Professor
Research Engineer
Project Researcher
Project Researcher
Project Researcher
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Re-employment Staff
Advanced Technology Center
Director
Vice-Director
Vice-Director
Professor
Professor
Professor
Project Professor
Executive Engineer
Associate Professor

108

III Organization

Kosugi, George
Furusawa, Hisanori
Ichikawa, Shinichi
Kosugi, George
Takata, Tadafumi
Morita, Eisuke
Shirasaki, Yuji
Yagi, Masafumi
Koike, Michitaro
Furusawa, Junko
Onozato, Hiroki
Ootsubo, Takafumi
Isogai, Mizuki
Kitada, Chihiro
Makiuchi, Shinichiro
Nakajima, Yasushi
Ozawa, Takeaki
Tanaka, Nobuhiro
Yamane, Satoru
Zapart, Christopher
Andrew
1

Hirabayashi, Masayuki
Fukushima, Mitsuhiro
Ozaki, Shinobu
Motohara, Kentaro
Ozaki, Masanobu
Uzawa, Yoshinori
Mitsuda, Kazuhisa
Hirabayashi, Masayuki
Fujieda, Miho

Associate Professor
Kojima, Takafumi
Associate Professor
Makise, Kazumasa
Associate Professor
Matsuo, Hiroshi
Associate Professor
Oya, Shin
Associate Professor
Shan, Wenlei
Senior Research Engineer Fukushima, Mitsuhiro
Senior Research Engineer Kanzawa, Tomio
Associate Professor
Nakaya, Hidehiko(Senior Lecturer)
Associate Professor
Ozaki, Shinobu(Senior Lecturer)
Associate Senior
Obuchi, Yoshiyuki
Research Engineer
Assistant Professor
Oshima, Tai
Project Assistant
Hattori, Masayuki
Professor
Project Assistant
Tokoku, Chihiro
Professor
Research Engineer
Ezaki, Shohei
Research Engineer
Sato, Naohisa
Research Engineer
Tsuzuki, Toshihiro
Engineer (Gishi)
Kamata, Yukiko
Engineer (Gishi)
Kaneko, Keiko
Engineer (Gishi)
Omata, Koji
Engineer (Gishi)
Tamura, Tomonori
Engineer (Gishi)
Uraguchi, Fumihiro
Engineer (Shunin
Fukuda, Takeo
Gijutsuin)Engineer (Shunin
Hirata, Naoatsu
Gijutsuin)Engineer (Shunin
Hoshino, Masayuki
Gijutsuin)Engineer (Shunin
Ikenoue, Bungo
Gijutsuin)Engineer (Shunin
Inata, Motoko
Gijutsuin)Engineer (Shunin
Iwashita, Hikaru
Gijutsuin)Engineer (Shunin
Mitsui, Kenji
Gijutsuin)Engineer (Shunin
Miyachi, Akihira
Gijutsuin)Engineer (Shunin
Waseda, Koichi
Gijutsuin)Engineer (Gijutsuin)
Kohara, Naoki
Engineer (Gijutsuin)
Sakai, Ryo
Engineer (Gijutsuin)
Shimizu, Risa
Project Researcher
Kozuki, Yuto
Project Researcher
Murayama, Yosuke
Project Researcher
Nagai, Makoto
Project Researcher
Yoneta, Kenta
Senior Specialist
Kusumoto, Hiroshi(Tokuninsenmonin)
Senior Specialist
Morita, Masaki(Tokuninsenmonin)
Re-employment Staff
1

Technical Experts
2
Administrative Expert
1
Technical Supporter
1
Administrative Supporters 2
Research Assistant Staff 1
Senior Specialist
1(Tokumeisenmonin)
Public Relations Center
Director
Project Professor
Project Professor
Associate Professor
Associate Professor
Associate Professor(Senior Lecturer)
Associate Professor(Senior Lecturer)
Associate SeniorResearch Engineer
Assistant Professor
Research Engineer
Engineer(Shunin Gijutsuin)
Project Researcher
Project Researcher
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Re-employment Staff
Research Experts
Administrative Experts
Research Supporters
Public Outreach Staff
Senior Specialist(Tokumeisenmonin)
Public Relations Office
Outreach and Education OfficeDirector
Ephemeris Computation OfficeDirector
Spectrum Management OfficeDirector
Library
LeaderPublications Office

Yamaoka, Hitoshi
Oishi, Masatoshi
Watanabe, Junichi
Agata, Hidehiko
Yamaoka, Hitoshi
Hanayama, Hidekazu
Hiramatsu, Masaaki
Fuse, Tetsuharu
Umemoto, Tomofumi
Katayama, Masato
Nagayama, Shogo
Hayatsu, Natsuki
Shibata, Takashi
Blumenthal, Kelly Anne
Filipecki Martins, Suzana
Ishikawa, Naomi
Komiyama, Hiroko
Lundock, Ramsey Guy
Pires Canas, Lina Isabel
4
2
2
2
13
1

Yamaoka, Hitoshi
Umemoto, Tomofumi
Katayama, Masato
Oishi, Masatoshi
Koshihara, Iori

Director
Yamaoka, Hitoshi
The Office for Astronomy Outreach of the IAU
Director
Pires, Canas Lina Isabel
Administration OfficeDirector
Matsuda, Ko
Ishigakijima Astronomical Observatory
Director
Hanayama, Hidekazu
Time Keeping OfficeDirector
Watanabe, Junichi

Division of Science
Division Head
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Project AssistantProfessor
Project AssistantProfessor
Project AssistantProfessor
Project AssistantProfessor
Project AssistantProfessor
Project AssistantProfessor
Project AssistantProfessor
Project AssistantProfessor
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Project Researcher
Administrative Experts
Research Supporter
Research Assistant Staff

Ikoma, Masahiro
Ikoma, Masahiro
Kawabe, Ryohei
Nomura, Hideko
Ouchi, Masami
Tominaga, Nozomu
Fujii, Yuka
Machida, Mami
Nakamura, Fumitaka
Dainotti, Maria Giovanna
Hamana, Takashi
Harada, Nanase
Kataoka, Akimasa
Morino, Junichi
Moriya, Takashi
Arzoumanian, Doris
Chiaki, Gen
Furuya, Kenji
Kokubo, Mitsuru
Nagakura, Hiroki
Nakajima, KimihikoSugiyama, Naonori
Taniguchi, Kotomi
Behroozi, Peter Spalding
Ito, Yuichi
Iwata, Yuhei
Jiang, Jian
Kikuta, Satoshi
Ohno, Kazumasa
2
1
3

III Organization

109

5. Research Support Departments
IT Security OfficeDirector
Vice Director
Associate Professor(Senior Lecturer)
Engineer (Gijutsuin)Senior Specialist(Tokuninsenmonin)
Re-employment Staff

Yoshida, MichitoshiOe, Masafumi
Oe, Masafumi
Matsushita, Sayaka
Shingu, Uken
1

Research Enhancement Strategy OfficeDirector
Iguchi, Satoru
Professor
Sekiguchi, Kazuhiro
Assistant Professor
Hattori, Kohei
Assistant Professor
Ishizuki, Sumio
Assistant Professor
Shirasaki, Masato
Senior Specialist
Asaga, Akitaka(Tokuninsenmonin)
Senior Specialist
Chapman, Junko(Tokuninsenmonin)
Senior Specialist
Hori, Kuniko(Tokuninsenmonin)
Research Assessment Support OfficeDirector
Saito, Masao
Assistant Professor
Ishizuki, Sumio
Senior Specialist
Hori, Kuniko(Tokuninsenmonin)
Industry Liaison OfficeDirector
Takami, Hideki
Office of International Relations
Director
Chapman, Junko
Senior Specialist
Chapman, Junko(Tokuninsenmonin)
Senior Specialist
Matsumoto, Mizuho(Tokuninsenmonin)
Research Supporter1
Support Desk
Research Supporters2
Human Resources Planning OfficeDirector
Yoshida, Michitoshi
Senior Specialist
Ishimoto, Tomoko(Tokuninsenmonin)
Safety and Health Management OfficeDirectorMori, Yasushi
Senior Specialist
Mori, Yasushi(Tokuninsenmonin)
Technical Expert
1
Engineering Promotion Office110

III Organization

Director
Uzawa, Yoshinori
Senior Research Engineer Fujii, Yasunori
Graduate Education OfficeDirector
Project Professor
Administration Department
General Manager
Manager forSpecialMissions
Senior Specialist(Tokuninsenmonin)
General Affairs GroupManager
Deputy Manager
Specialist (Information
Technology)
Specialist (Personnel
Relations)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Re-employment Staff
General Affairs Unit
LeaderStaff
Staff
Administrative Expert
Administrative Supporter
Personnel Unit
LeaderSenior Staff
Staff
Staff
Administrative Expert
Payroll Unit
LeaderSenior Staff
Staff
Staff
Staff
Administrative Supporter
Employee Affairs Unit
LeaderSenior Staff
Staff
Administrative Expert
Research Promotion GroupManager

Sekii, Takashi
Sekii, Takashi

Fujita, Hisashi
Seto, Yoji
Harada, Eiichiro

Tanaka, Aiko
Onishi, Tomoyuki
Kawashima, Ryota
Yoshimura, Tetsuya
Ito, Yuko
Murakami, Sachiko
Suzuki, Yoshihiro
1
Kawashima, Ryota
Isozaki, Yuka
Saito, Masahiro
1
1
Chiba, Yoko
Ouchi, Kaori
Okawa, Makoto
Tsuchiya, Sota
1
Furukawa, Shinichiro
Tsuji, Misato
Takahashi, Sachiko
Yamamoto, Kyoko
Yokota, Banri
1
Yamaura, Mari
Tanaka, Masashi
Inoue, Wakaho
1
Hosoya, Akio

Senior Specialist
Seto, Yoji
(International Relations)
Specialist
Iida, Naoto
Senior Specialist
Fujikawa, Hiroaki(Tokuninsenmonin)
Administrative Supporter 1
Research Support Unit
LeaderGoto, Michiru
Administrative Expert
1
Administrative Supporter 1
External Funding Unit
Specialist
Ihara, Yuko
(External Funding)Staff
Kashiwa, Hidekazu
Administrative Expert
1
Graduate Student Affairs Unit
LeaderKitabayashi, Kaya
Administrative Expert
1
Administrative Supporter 1
International Academic Affairs Unit
LeaderSato, Yoko
Financial Affairs GroupManager
Kawazu, Hironori
Deputy Manager
Yamamoto, Futoshi
Specialist (Audit)
Chiba, Satoko
General Affairs Unit
LeaderKikkawa, Hiroko
Staff
Naraoka, Aone
Administrative Supporter 1
Budget Unit
LeaderYamamoto, Shinichi
Senior Staff
Sugimoto, Naomi
Administrative Supporter 1
Asset Management Unit
LeaderIshikawa, Junya
Senior Staff
Okubo, Kazuhiko
Receiving Unit
LeaderIshikawa, Junya
Administrative Supporters 3
Accounting GroupManager
Tahara, Yuji
Specialist (Contracts)
Sato, Kanako
Accounting Unit
LeaderOkazaki, Maya
Administrative Supporters 2
Procurement Unit
Leader
Miura, Susumu
Senior Staff
Nakagawa, Yukie
Staff
Fukuhara, Miyuki
Staff
Manabe, Yuta
Administrative Expert
1
Administrative Supporter 1
Facilities GroupManager
Deputy Manager
Senior Specialist(General Affairs)
General Affairs Unit
LeaderAdministrative Supporter
Facilities Direction Unit
LeaderAdministrative Supporters
Maintenance Unit
Leader
Staff
Staff

Kataoka, Toru
Murakami, Kazuhiro
Yamanouchi, Mika

Tsukano, Satomi
1
Murakami, Kazuhiro
2
Watanabe, Tsuyoshi
Hayashi, Yuki
Kawahara, Iori

III Organization

111

6. Personnel Change
Research and Academic Staff
Date
Name

Change2022/4/1

Fujieda, Miho

Hired2022/4/1

Chen, Dan

Hired

2022/7/1
2022/8/1

Kikuchi, Shota
Osawa, Ryou

Hired
Hired

2022/10/1

Oya, Shin

Hired2022/10/1

Fuse, Tetsuharu

Hired2022/11/1
2023/1/1
2023/1/1
2023/1/1
2023/3/1

Kawabata, Yusuke
Ozaki, Masanobu
Izumi, Takuma
Koike, Michitaro
Hatsukade, Bunyo

Hired
Hired
Hired
Hired
Hired

2022/7/31

Sekii, Takashi

Resigned

2022/11/30

Leonardi, Matteo

Resigned

2023/2/6

Nakamura, Koji

Resigned

2023/3/31

Yoshida, Michitoshi

Resigned

2023/3/31

Kawabe, Ryohei

Retired2023/3/31

Sekiguchi, Kazuhiro Retired

2022/4/1

Koyama, Yusei

Promoted

Subaru Telescope, Associate Professor

2022/5/1

Katsukawa, Yukio

Promoted

Solar Science Observatory, Professor

2022/8/1

Aoki, Wako

Promoted

Thirty Meter Telescope Project, Professor

2022/10/1

Hirota, Tomoya

Promoted

2022/10/1

Furusawa, Hisanori

Promoted

New Affiliated Institute, Position
Advanced Technology Center, Associate
Professor
Gravitational Wave Science Project,
Assistant Professor
RISE Project, Assistant Professor
JASMINE Project, Assistant Professor
Advanced Technology Center, Associate
Professor
Public Relations Center, Associate SeniorResearch Engineer
SOLAR-C Project, Assistant Professor
Advanced Technology Center, Professor
ALMA Project, Assistant Professor
Astronomy Data Center, Research Engineer
ALMA Project, Associate Professor(Graduate Education Office, Project
Professor )(Subaru Telescope, Project Professor(Distinguished Professor))

112(Subaru Telescope, Project Associate
Professor )(ALMA Project, Project Researcher)(Subaru Telescope, Senior Specialist )Solar Science Observatory, Associate
Professor
Gravitational Wave Science Project,
Assistant Professor
IT Security Office, Senior ResearchEngineer
Subaru Telescope, Professor

Research Enhancement Strategy
Office, Professor

Mizusawa VLBI Observatory, Associate
Professor
Astronomy Data Center, Associate
Professor

Date

Name

2022/7/1

Kohara, Naoki

Hired2023/3/31
2023/3/31

Kobiki, Toshihiko
Shinohara, Noriyuki

RetiredRetired2022/11/1

Takahashi, Ken

Promoted

Mizusawa VLBI Observatory, Engineer2022/11/1
2022/11/1

Sawatari Koichi
Hirano, Ken

Promoted
Promoted

Subaru Telescope, Engineer
Subaru Telescope, Engineer

III Organization(Gravitational Wave Science Project,
Project Researcher)

Division of Science, Professor

Engineering Staff
ChangePrevious Affiliated Institute, Position

New Affiliated Institute, Position
Advanced Techonology Center, Engineer

Subaru Telescope, AssistantProfessor
Solar Science Observatory, Associate
Professor
Thirty Meter Telescope Project,
Associate Professor
Mizusawa VLBI Observatory,
Assistant Professor
Astronomy Data Center, AssistantProfessor

Previous Affiliated Institute,
Position
NAOJ Chile, Engineer
Solar Science Observatory, Engineer
Mizusawa VLBI Observatory,
Engineer
Subaru Telescope, Engineer
Subaru Telescope, Engineer

Administrative Staff
Name

2022/4/1

Tanaka, Aiko

Hired2022/4/1

Yamamoto, Futoshi

Hired2022/4/1

Chiba, Satoko

Hired2022/4/1

Okazaki, Maya

Hired

2022/4/1

Koshihara, Iori

Hired

2022/4/1

Tsuchiya, Sota

Hired

2022/4/1

Yamamoto, Kyoko

Hired2022/9/1

Tsukano, Satomi

Hired2022/4/30

Matsukura, Koji

Resigned

2022/7/31

Takami, Masaki

Resigned(Shinshu University)

Nobeyama Radio Observatory
Administration Office Accounting
Unit, Leader

2022/9/30

Hiramatsu, Naoya

Resigned(Tokyo Medical and Dental University)

Administration Department Facilities
Group General Affairs Unit, Staff

2023/3/31

Tahara, Yuji

Resigned(National Institute of Informatics)

Administration Department
Accounting Group, Manager

2023/3/31

Yamaura, Mari

Resigned(Research Organization of Informationand Systems)

Administration Department General
Affairs Group Employee Affairs
Unit, Leader

2022/4/1

Ouchi, Kaori

Promoted

Administration Department General
Affairs Group Personnel Unit, Senior Staff

Administration Department General
Affairs Group Personnel Unit, Staff

2022/4/1

Tanaka, Masashi

Promoted

Administration Department General
Affairs Group Employee Affairs Unit,
Senior Staff

Administration Department General
Affairs Group Employee Affairs
Unit, Staff

2022/4/1

Sugimoto, Naomi

Promoted

Administration Department Financial
Affairs Group Budget Unit, Senior Staff

Administration Department
Financial Affairs Group Budget Unit,
Staff

Administration Department General
Affairs Group Payroll Unit, Senior Staff

National Institutes of Natural
Sciences Administrative Bureau
General Affairs Division, Senior Staff(Ministry of Education, Culture,
Sports, Science and TechnologyJapan, Administrative Intern Trainee)2022/4/1

2022/4/1

2022/7/1

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Date

Administration Department General
Affairs Group, Manager
Administration Department Financial
Affairs Group, Deputy Manager
Administration Department Financial
Affairs Group, Specialist (Audit)
Administration Department Accounting
Group Accounting Unit, Leader
Public Relations Center Administration
Office Library, Leader
Administration Department General
Affairs Group Personnel Unit, Staff
Administration Department General
Affairs Group Payroll Unit, Staff
Administration Department General
Affairs Group, Specialist(Niigata University)(The University of Tokyo)(Tokyo Medical and Dental
University)(Tokyo Medical and Dental
University)(The University of Tokyo)(Tokyo Medical and Dental
University)
Administration Department General
Affairs Group Personnel Unit, Staff

Tsuji, Misato

Reassigned

Morita, Akitsugu

National Institutes of Natural Sciences
Administrative Bureau General Affairs
Reassigned Division, Staff (Ministry of Education,
Culture, Sports, Science and TechnologyJapan, Administrative Intern Trainee)

Administration Department
Accounting Group Procurement
Unit, Staff

Iida, Naoto

Administration Department Research
Reassigned
Promotion Group, Specialist

National Institutes of Natural
Sciences Administrative Bureau
General Affairs Division Personnel
Unit, Leader

III Organization

113

Employee on Annual Salary System

114

Date

Name

Change2022/4/1

Kurasaki, Takaaki

Hired2022/4/1

Toba, Yoshiki

Hired2022/4/1
2022/4/1

Saito, Toshiki
Tokuda, Kazuki

Hired
Hired

2022/4/1

Washimi, Tatsuki

Hired2022/4/1

Chiaki, Gen

Hired2022/4/1

Ishikawa, Ryotaro

Hired2022/4/1

Izumi, Takuma

Hired2022/4/1

Silva Bustamante,Andrea Ludovina

Hired2022/4/1

Nozawa, Takaya

Hired2022/4/1

Miyakawa, Kohei

Hired2022/4/1

Kozuki, Yuto

Hired2022/4/1

Yoneta, Kenta

Hired2022/4/1
2022/4/1

Iwata, Yuhei
Jiang, Jian

Hired
Hired

2022/4/1

Morita, Satoshi

Hired

New Affiliated Institute, Position

Thirty Meter Telescope Project, Project
Professor
Subaru Telescope, Project AssistantProfessor
ALMA Project, Project Assistant Professor (ALMA Project, Project Researcher)
ALMA Project, Project Assistant Professor
Gravitational Wave Science Project,
Project Assistant Professor
Division of Science, Project AssistantProfessor
Solar Science Observatory, Project
Researcher(Subaru Telescope, Project Assistant
ALMA Project, Project Researcher
Professor)
ALMA Project, Project Researcher
Center for Computational Astrophysics,
Project Researcher
JASMINE Project, Project Researcher
Advanced Technology Center, Project
Researcher
Advanced Technology Center, Project
Researcher
Division of Science, Project Researcher
Division of Science, Project Researcher
Solar Science Observatory, Senior
Specialist

2022/4/1

Fukui, Hideharu

Hired2022/4/1

Mori, Yasushi

Hired2022/5/1

Ideguchi, Shinsuke

Hired2022/5/1

Ueda, Junko

Hired

ALMA Project, Senior Specialist

2022/6/1

Kikuta, Satoshi

Hired2022/7/1

Sakai, Daisuke

Hired2022/7/1
2022/7/19

Ebihara, Eiichi
Shakunaga, Takeshi

Hired
Hired

2022/8/1

Sekii, Takashi

Hired2022/8/1

Fujikawa, Hiroaki

Hired2022/9/1

Keszthelyi, Zsolt

Hired

2022/9/1

Hayatsu, Natsuki

Hired2022/9/1
2022/9/1
2022/9/20

Asanuma, Masumi
Tagawa, Hiroaki
Saha, Piyali

Hired
Hired
Hired

Division of Science, Project Researcher
Mizusawa VLBI Observatory, Project
Assistant Professor
ALMA Project, Senior Specialist
ALMA Project, Senior Specialist
Graduate Education Office, Project
Professor
Administration Department Research
Promotion Group, Senior Specialist
Center for Computational Astrophysics,
Project Researcher
Public Relations Center, Project
Researcher
ALMA Project, Senior Specialist
ALMA Project, Senior Specialist
ALMA Project, Project Researcher

III Organization

Previous Affiliated Institute,
Position

ALMA Project, Senior Specialst(Division of Science, Project
Researcher)(Solar Science Observatory, Senior
Specialist)(Research Enhancement Strategy
Office (ALMA Project), Research
Administrator Staff, Senior
Specialist)

Safety and Health Management Office,Senior Specialist
Center for Computational Astrophysics,
Project Researcher(ALMA Project, Project AssistantProfessor)(Solar Science Observatory,
Associate Professor)

2022/9/30

Kokubo, Mitsuru

Hired2022/10/1
2022/11/1

Wu, Yu-Ting
Aso, Yusuke

Hired
Hired

2022/11/1

Murayama, Yosuke

Hired2022/12/1

Eisenmann, Marc

Hired

2022/12/1

Page, Michael
Anthony
Inoue, Naoko

2022/12/1

Ishimoto, Tomoko

Hired2023/1/1

Cataldi, Gianni

Hired2023/1/1

Lee, Kianhong

Hired2022/12/1

Hired
Hired

Division of Science, Project AssistantProfessor
ALMA Project, Project Assistant Professor (ALMA Project, Project Researcher)
ALMA Project, Project Assistant Professor
Advanced Technology Center, Project
Researcher
Gravitational Wave Science Project,
Project Researcher
Gravitational Wave Science Project,
Project Researcher
ALMA Project, Senior Specialist
Human Resources Planning Office, Senior
Specialist
ALMA Project, Project Assistant Professor (ALMA Project, Project Researcher)Thirty Meter Telescope Project, Project
Researcher(Division of Science, Project
ALMA Project, Project Researcher
Assistant Professor)
Division of Science, Project Researcher
Advanced Techonology Center, Senior
Specialist

2023/2/1

Takahashi,
Sanemichi
Ono, Kazumasa

2023/2/1

Morita, Masaki

Hired2023/3/1

Feeney‐Johansson,
Anton Fiachra
George

Hired

ALMA Project, Project Researcher

2022/4/30

Ueda, Junko

Resigned(ALMA Project, Senior Specialist)

2022/4/30

Tsukagoshi, Takashi

Resigned

2022/4/30

Hayashi, Yohei

Resigned

2022/6/30

Baba, Takashi

Resigned

2023/2/1

Hired
Hired

2022/8/31

Hull, Charles
Lindsay Hopkins
Sorahana, Satoko

2022/9/30

Oya, Shin

Resigned

2022/9/30

Aritomi, Naoki

Resigned

2022/10/31

Ueda, Junko
Curotto Molina,
Franco Andreas

Resigned

ALMA Project, Project AssistantProfessor
Division of Science, Project AssistantProfessor
ALMA Project, Senior Specialist
Administration Department Research
Promotion Group, Senior Specialist
ALMA Project, Project AssistantProfessor
ALMA Project, Project Researcher
Subaru Telescope, Project Associate
Professor
Gravitational Wave Science Project,
Project Researcher
ALMA Project, Senior Specialist

Resigned

ALMA Project, Senior Specialist

2022/12/14

Aso, Yusuke

Resigned

2022/12/31

Izumi, Takuma

Resigned

2022/12/31

Cataldi, Gianni

Resigned

2022/12/31

Koike, Michitaro

Resigned

2022/8/14

2022/11/30

2023/1/31
2023/2/28
2023/2/28

Takahashi,
Sanemichi
Burns, Ross
Alexander
Iju, Tomoya

Resigned
Resigned

Resigned
Resigned
Resigned(Advanced Technology Center, Associate
Professor)(ALMA Project, Assistant Professor)(ALMA Project, Project AssistantProfessor)(Astronomy Data Center, ResearchEngineer)(ALMA Project, Project Researcher)

ALMA Project, Project AssistantProfessor
ALMA Project, Project Researcher
ALMA Project, Project Researcher
Subaru Telescope, Senior Specialist
Division of Science, Project AssistantProfessor
Division of Science, Project
Researcher
Solar Science Observatory, Senior
Specialist

III Organization

115

Kobayashi, Masato

Resigned

2023/3/31

Tadaki, Ken'ichi

Resigned

2023/3/31

Baba, Jun'ichi

Resigned

2023/3/31
2023/3/31

Mawatari, Ken
Murata, Kazumi

Resigned
Resigned

2023/3/31

Taki, Tetsuo

Resigned

2023/3/31

Kato, Tsunehiko

Resigned

2022/9/30

Wu, Yu-Ting

Contract
Expired(ALMA Project, Project AssistantProfessor)

2022/9/30

Matsumoto, Mizuho

Contract
Expired(Office of International Relations,
Office of International Relations,
Employee on Annual Salary System
Transferring to the Mandatory Retirement Senior Specialist
System Senior Specialist)

2022/11/30

Nakanishi, Takashi

Contract
ExpiredALMA Project, Senior Specialist

2023/2/28

Shindo, Miwa

Contract
Expired2023/3/31

Takami, Hideki

2023/3/31

Kiuchi, Hitoshi

2023/3/31

Oishi, Masatoshi

2023/3/31

Kambe, Eiji

2023/3/31

Nagai, Hiroshi

2023/3/31

Shimakawa, Rizumu

2023/3/31

Ishikawa, Ryotaro

2023/3/31

Nozawa, Takaya

2023/3/31

Kaneko, Hiroyuki

2023/3/31

Kudo, Yuki

2023/3/31

Chen, Xiaoyang

2023/3/31
2023/3/31
2023/3/31

116

Division of Science, Project
Researcher
Thirty Meter Telescope Project,
Project Assistant Professor
JASMINE Project, Project AssistantProfessor
Subaru Telescope, Project Researcher
Subaru Telescope, Project Researcher
Center for Computational
Astrophysics, Project Researcher
Center for Computational
Astrophysics, Senior Specialist

2023/3/30

Bakx, Tom Johannes
Lucinde Cyrillus
Michiyama,
TomonariLee, Kianhong

III Organization(Subaru Telescope, Employee on Annual
Salary System Transferring to the
Mandatory Retirement System Senior
Specialist)

Contract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredALMA Project, Project Researcher

Subaru Telescope, Senior Specialist
Subaru Telescope, Project Professor(Distinguished Professor)
ALMA Project, Project Professor
Public Relations Center, Project
Professor(Subaru Telescope, Employee on Annual
Salary System Transferring to the
Mandatory Retirement System Project
Associate Professor)(ALMA Project, Associate Professor)

Subaru Telescope, Project Associate
Professor
ALMA Project, Project Associate
Professor
Subaru Telescope, Project AssistantProfessor
Solar Science Observatory, Project
Researcher
Center for Computational
Astrophysics, Project Researcher
ALMA Project, Project Researcher
ALMA Project, Project Researcher(ALMA Project, Project Researcher)

ALMA Project, Project Researcher
ALMA Project, Project Researcher
ALMA Project, Project Researcher(ALMA Project, Project Researcher)Thirty Meter Telescope Project,
Project Researcher

2023/3/31

Otsubo, Takafumi

Contract
Expired2023/3/31

Furusawa, Junko

Contract
Expired2023/3/31

Kozuki, Yuto

2023/3/31

Murayama, Yosuke

2023/3/31

Oyama, Tomoaki

2023/3/31

Morita, Satoshi

2023/3/31

Tanaka, Mitsuhiro

2023/3/31

Mineo, Sogo

2023/3/31

Fukushi, Hinako

Contract
Expired2023/3/31

Uemizu, Kazunori

Contract
Expired2023/3/31

Kawasaki, Wataru

2023/3/31

Nodomi, Yoshifumi

2023/3/31

2023/3/31

Contract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
Expired(Astronomy Data Center, Project
Researcher)(Astoronomy Data Center, Employee on
Annual Salary System Transferring to
the Mandatory Retirement System Senior
Specialist)(Advanced Technology Center, Project
Researcher)(Mizusawa VLBI Observatory, Employee
on Annual Salary System Transferring to
the Mandatory Retirement System Senior
Specialist )Astronomy Data Center, Project
Researcher
Astronomy Data Center, Project
Researcher
Advanced Technology Center, Project
Researcher
Advanced Technology Center, Project
Researcher
Mizusawa VLBI Observatory, Senior
Specialist
Solar Science Observatory, Senior
Specialist
Subaru Telescope, Senior Specialist(Astronomy Data Center, Research
Subaru Telescope, Senior Specialist
Engineer)(Center for Computational Astrophysics,
Center for Computational
Employee on Annual Salary System
Transferring to the Mandatory Retirement Astrophysics, Senior Specialist
System Senior Specialist)(ALMA Project, Employee on Annual
Salary System Transferring to the
Mandatory Retirement System Senior
Specialist)

Contract
ExpiredContract
ExpiredALMA Project, Senior Specialist

ALMA Project, Senior Specialist
SOLAR-C Project, Senior Specialist

Isogai, Mizuki

Contract
Expired(Astoronomy Data Center, Employee on
Annual Salary System Transferring to
the Mandatory Retirement System Senior
Specialist)

Astoronomy Data Center, Senior
Specialist

Tanaka, Nobuhiro

Contract
Expired(Astoronomy Data Center, Employee on
Annual Salary System Transferring to
the Mandatory Retirement System Senior
Specialist)

Astoronomy Data Center, Senior
Specialist

Employees on Annual Salary System Transferring to the Mandatory Retirement System
Date

Name

ChangeNew Affiliated Institute, Position

2022/10/1

Matsumoto, Mizuho

Hired

Office of International Relations, Senior
Specialist

2023/3/1

Shindo, Miwa

Hired

Subaru Telescope, Senior Specialist

Previous Affiliated Institute,
Position(Office of International Relations,
Employee on Annual Salary System
Senior Specialist)(Subaru Telescope, Employee
on Annual Salary System Senior
Specialist)

III Organization

117

Research Administrator Staff
Date

Name

Change2022/9/30

Suzui, Mitsukazu

Contract
Expired2022/12/31

Noda, Noboru

Contract
ExpiredNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Research Enhancement Strategy
Office (Engineering Promotion
Office), Senior Specialist
Research Enhancement Strategy
Office (Human Resources Planning
Office), Senior Specialist

Cross-appointment
Date

Name

Term of
Cross-appointment

2022/4/1

Kataza, Hirokazu

2022/4/1 ~ 2025/3/31

2022/7/1

Behroozi, Peter
Spalding

2022/7/1 ~ 2024/10/15

Foreign Visiting Researchers
Name
PeriodMazzali, Paolo
2022/12/28 ~ 2023/2/2
Pian, Elena118

III Organization

Main Institute, Position

Japan Aerospace Exploration Agency
Institute of Space and Astronautical
Science, Associate Professor
University of Arizona, Associate
Professor

Affiliated in NAOJ,
Position

JASMINE Project, Project
Associate Professor
Division of Science, Project
Researcher

Affiliated Institute
Liverpool John Moores University (UK)
Italian National Institute of Astrophysics, Astrophysics and Space Science
2022/12/28 ~ 2023/2/2
Observatory (Italy)7. Advisory Committee for Research and Management
Members
From universities and related institutes
Arai, Tomoko
Principal Staff Scientist at the Planetary Exploration Research Center, Chiba Institute of Technology○ Kodama, Tadayuki
Professor at the Graduate School of Science, Tohoku University
Ohashi, Masatake
Professor at the Institute for Cosmic Ray Research, University of Tokyo
Omukai, Kazuyuki
Professor at the Graduate School of Science, Tohoku University
Sakai, Nami
Chief Scientist at the RIKEN
Sumi, Takahiro
Professor at the Graduate School of Science, Osaka University
Takada, Masahiro
Professor at the Kavli Institute for the Physics and Mathematics of the Universe, University of Tokyo
Tosaki, Tomoka
Professor at the Graduate School of Education, Joetsu University of Education
Yamasaki, Noriko
Professor at the Institute of Space and Astronautical Science, JAXA
Yokoyama, Takaaki
Professor at the Astronomical Observatory, Graduate School of Science, Kyoto University
Yonekura, Masanori Professor at the Center for Astronomy, Ibaraki University
From NAOJ
Fukagawa, Misato
Kokubo, Eiichiro
Kobayashi, Hideyuki
Miyazaki, Satoshi
Motohara, Kentaro
Nomura, Hideko
Saito, Masao
Uzawa, Yoshinori
Watanabe, Junichi● Yoshida, Michitoshi

Professor in ALMA Project
Professor in the Center for Computational Astrophysics
Project Professor in Mizusawa VLBI Observatory
Professor in Subaru Telescope
Director of Research Coordination
Professor in the Division of Science
Vice-Director General (on Finance)
Director of Engineering
Project Professor in the Public Relations Center
Vice-Director General (on General Affairs)● Chairperson ○ Vise-Chairperson
Period: April 1, 2022 - March 31, 2024

III Organization

1198. Professors Emeriti
Professors Emeriti (NAOJ)

120

III Organization

Ando, Hiroyasu
Arimoto, Nobuo
Chikada, Yoshihiro
Fujimoto, Masakatsu
Fukushima, Toshio
Hasegawa, Tetsuo
Hayashi, Masahiko
Hiei, Eijiro
Hirayama, Tadashi
Inoue, Makoto
Ishiguro, Masato
Iye, Masanori
Karoji, Hiroshi
Kawaguchi, Noriyuki
Kawano, Nobuyuki
Kinoshita, Hiroshi
Kobayashi, Yukiyasu
Kodaira, Keiichi
Manabe, Seiji
Miyama, Shiyoken
Mizumoto, Yoshihiko
Nakano, Takenori
Nariai, Kyoji
Nishimura, Shiro
Nishimura, Tetsuo
Noguchi, Kunio
Noguchi, Takashi
Oe, Masatsugu
Ogasawara, Ryusuke
Okamoto, Isao
Sakurai, Takashi
Shibasaki, Kiyoto
Tomisaka, Koji
Watanabe, Tetsuya
Yamashita, Yasumasa
Yoshida, Haruo

IV Finance
Revenue and Expenses (FY 2022)
RevenueManagement Expenses Grants
Facilities Maintenance Grants
Subsidy Income
Miscellaneous Income
Industry-Academia Research Income and Donation Income
Reversals of Reserves for Specific Purposes
Total
Expenses
Management Expenses
Employee Personnel Expenses
Operating Expenses
Facilities Maintenance Expenses
Subsidy Expenses
Industry-Academia Research Expenses and Donation Expenses
Total
Revenue-Expenses

Budget
8,043,676
2,417,758
1,439,063
14,908422,761
0
12,338,166
Budget8,058,584
3,746,754
4,311,830
2,417,758
1,439,063
422,761
12,338,166
Budget0

Final Account8,648,601
1,204,343
1,445,634
134,692
659,914135,000
12,228,184
Final Account8,338,794
3,625,079
4,713,715
1,204,343
1,445,634
418,908
11,407,679
Final Account820,505(Unit: ¥1,000)
Budget − Final Account−604,925
1,213,415−6,571−119,784−237,153−135,000
109,982
Budget − Final Account−280,210
121,675−401,885
1,213,415−6,571
3,853
930,487
Budget − Final Account−820,505

IV Finance121

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2022
Research Categories
Scientific Research on Innovative Areas(Research in a proposed research area)
Transformative Research Areas (A)Scientific Research (S)Scientific Research (A)Scientific Research (B)JSPS Research Fellows
JSPS International Research Fellows
Publication of Scientific Research Results
Total

Number of Selected Projects

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding

Total

7

41,20012,36053,560

2
5
10
19
6
2
2
53

37,500184,000
104,800
62,200
7,100
1,400
1,190
439,390

11,25055,20031,44018,6602,130
0
0131,040

48,750239,200
136,240
80,860
9,230
1,400
1,190
570,430

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding
16,3004,890
20,600
6,180

Total
21,19026,7802. Series of Multi-year Funds for FY 2022

122

Research Categories

Number of Selected Projects

Scientific Research (C)Early-Career Scientists
Fund for the Promotion of Joint International Research(International Leading Research)
Fund for the Promotion of Joint International Research(Fostering Joint International Research (B))
Total

19
18

V KAKENHI (Grants-in-Aid for Scientific Research)

1

38,30011,49049,790

2

5,200

1,560

6,760

40

80,40024,120104,520

VI Research Collaboration
1. Open Use
TypeProject/Center

Category

Notes

Subaru Telescope
Subaru Telescope
Okayama Branch

Subaru Telescope

81

336 (79)

53 Institutes, 13 Countries

SEIMEI Telescope

41

114

16 Institutes

Solar Science
Observatory

Ground-based Solar Observatory
Sun-observing satellite “Hinode”

Mizusawa VLBI
Observatory

*
**

*
**

*
**

VERA

25

102 (79)

47 Institutes, 15 Countries

339

339 (21)83 Institutes, 11 Countries

355
13
17

355 (26)
42
115

76 Institutes, 8 Countries
10 Institutes
20 Institutes

Open Use at
Project/Center Astronomy Data Center
Center for Computational Astrophysics
Facility Use
Advanced
Technology Center Joint Research and Development
ALMA ProjectCharged
TelescopeTime

Number of
Total
Accepted Number of
Proposals Researchers

Nobeyama Radio
Observatory

Large-scale
Collaborative- Mizusawa VLBI
Observation
Observatory
Program

ALMA (Cycle 8)

253 3418 (2997) 351 Institutes, 39 Countries

ASTE

***

***

***

45-m telescope

46

–

–

VERA

16

80(3)

24 Institutes, 3 Countries

Joint Development Research
5
5 Institutes, 0 Countries
Research Assembly
16
9 Institutes, 0 Countries
NAOJ Symposium
00
The number of researchers at foreign institutes shown in brackets ( ) is included in the total.
The country count does not include Japan.
The period of ALMA (Cycle 8) is from October 2021 to September 2022.
* The observation data is open to the public on the web. No application is needed to use the data.
** Since the function of the Hinode Science Center has shifted to the Astronomy Data Center, there is no procedure of application andadoption as “Hinode”.
*** ASTE has cancelled the joint-use observations scheduled for FY 2022 due to the malfunctions of sub-reflector. The possibility of
postponing adopted observation proposals to the following fiscal year or later is being considered.

VI Research Collaboration

1232. Commissioned Research Fellows
Visiting Scholars (Domestic)
Name

Position at NAOJ

Affiliated Institute

TANAKA,
Yoshiyuki

Visiting Associate
Professor

The University of Tokyo, Graduate School of
Science

PeriodApril 1, 2022 –March 31, 2023

Host Project/Center/
Division
Mizusawa VLBI
Observatory

Visiting Scholars (Foreign)
PeriodHost Project/Center/
Division

Name

Position at NAOJ

Affiliated Institute

Mazzali,
Paolo

Visiting Professor

Liverpool John Moores University

December 28, 2022
– February 2, 2023

Division of Science

Pian, Elena

Visiting Professor

Italian National Institute of Astrophysics,
Astrophysics and Space Science Observatory

December 28, 2022
– February 2, 2023

Division of Science

JSPS (Japan Society for the Promotion of Science) Postdoctoral Research Fellows
Research Subject

Name
Kawabata, Yusuke
Okuya, Ayaka
Uyama, Taichi
Namekata, Kosuke
Yoshiura, Shintaro

Investigation of the evolution of solar active regions withmulti-wavelength observations
Revealing planet formation around intermediate-mass stars
from planetary remnants accreting on white dwarfs
Developing exoplanetary science by high-contrast imaging
Observational and numerical studies of solar and stellar
magnetic activities
Analysing the 21cm line at the Epoch of Reionisation using
the sparse modelling

Acceptance Period

Host Researcher

2022/4/1 – 2022/10/31 Katsukawa, Yukio
2022/4/1 – 2025/3/31

Ikoma, Masahiro

2021/4/1 – 2024/3/31

Fujii, Yuka

2021/4/1 – 2024/3/31

Shimojo, Masumi

2021/4/1 – 2024/3/31

Honma, Mareki

JSPS (Japan Society for the Promotion of Science) Foreign Research Fellows
Name
Page, Michael Anthony
Eisenmann, Marc
Ledger, Blake Steven

124

VI Research Collaboration

Period2020/11/30 – 2022/11/29
2020/11/30 – 2022/11/29
2022/6/9 – 2022/8/8

Host Researcher
Aso, Yoichi
Leonardi, Matteo
Iono, Daisuke

VII Graduate Education
1. Department of Astronomical Science, School of Physical Sciences,
SOKENDAI (The Graduate University for Advanced Studies)
The Graduate University for Advanced Studies, SOKENDAI
was established in 1988 via partnerships with inter-university
research institutes for the purpose of advancing graduate
education.
SOKENDAI currently consists of six schools: Cultural andSocial Studies, Physical Sciences, High Energy Accelerator
Science, Multidisciplinary Sciences, Life Science, and Advanced
Sciences, and is offering doctoral education and research
opportunities.
NAOJ has been accepting three-year doctoral-course
students since FY 1992 and five-year- course students since
FY 2006 for Department of Astronomical Science, School ofPhysical Sciences.
SOKENDAI is reorganizing its six graduate schools
into the Graduate Institute for Advanced Studies to offer a
20-program system starting from April 2023. In accordancewith this reorganization, Department of Astronomical Science isreorganized into Astronomical Science Program.
(1) Objective of Department of Astronomical Science
Department of Astronomical Science aims to train students,
through observational, theoretical, or instrument development
research in astronomy or in related fields, in an environment
with the most advanced observational instruments andsupercomputers, to be researchers who work at the forefrontof world-class research; experts who carry out development ofadvanced technology; and specialists who endeavor in educationand public outreach activities equipped with advanced andspecialized knowledge.
Numbers of students to be admitted annually:
Two (for the five-year doctoral course)
Three (for the three-year doctoral course)
Degree: Doctor of Philosophy (Doctor of Science, or Doctor ofEngineering, depending on the topic of Doctoral thesis)(2) Admission Policy
Department of Astronomical Science seeks students witha strong interest in astronomy and the universe; a passion forunraveling scientific questions through theoretical, observational,
and instrument-development research; and who have not only
basic academic skills, but also the logical and creative aptitude
required for advanced research.
(3) Department Details (Course Offerings)
Optical and Infrared Astronomy[Fields of education and research supervision]
Ground-based astronomy / Optical and infrared telescope
systems / Planets / Sun, stars, and interstellar matter /Galaxies and cosmology
Radio Astronomy[Fields of education and research supervision]
Ground-based astronomy / Radio telescope systems / Sun,stars, and interstellar matter / Galaxies
General Astronomy and Astrophysics[Fields of education and research supervision]
High-precision astronomical measurement / Astronomy
from space / Data analysis and numerical simulation /Earth, planets, and the Sun / Galaxies and cosmology(4) Education and Research Supervision
In observational research with the state-of-the-art opticalIR and radio telescopes, and theoretical research, the research
efforts and the educational efforts are fused together to offer
advanced-level education in astronomy and astrophysics. The
department consists of the Optical Near-Infrared Astronomy
Unit, Radio Astronomy Unit, and General Astronomy andAstrophysics Unit, but all three units cooperate in the education
and research supervision of the students. To ensure that thestudents with a wide variety of backgrounds can perform original
and creative research in the ever-developing field of astronomy,
they are guided to focus on learning the basic astronomy in thefirst year. In order to focus on astronomical research, including
the basis of observational astronomy, instrument development,
and theoretical astronomy, from the second year onwards
students learn subjects ranging from principles to applicationsof advanced technologies that will be the basis of astronomical
observations; how to design, fabricate and test new instruments;
and the forefronts of data acquisition and data analyses.
(5) Financial Supports
In order to provide the students economical basis uponwhich they can develop into young researchers skilled in
conducting research effectively, the department has set up the
Associate Researcher program in addition to Research Assistantsystem. In addition, the department has introduced the ‘NAOJ
Junior Fellow’ system from FY 2020 to create an environment inwhich outstanding students can devote themselves more to theirstudies and research, and to further improve the standards ofresearchers produced by the department.
In FY 2022 there were 9 NAOJ Junior Fellows, 17 Associate
Researchers, and 3 Research Assistants.
To further improve the research environment for the
students, the department provides Oversea Travel Fund, toencourage the students to participate in international conferences
to give English talks, conduct observations at various oversea
observational facilities and so on, and Research Fund to help
them pursue their own original ideas to plan and carry out

VII Graduate Course Education125

research, experiments, etc.
(6) Undergraduate Students
For undergraduate students, and for students abroad, we run
SOKENDAI Summer Students Program, Spring School andAsian Winter School to offer chances to experience research at
the Department of Astronomical Science. Admission Guidance

also targets undergraduate students.
In FY 2022, 22 students participated in the SOKENDAI
Summer Students program. The Asian Winter School, conducted
online, received 211 applications from 9 countries, and of these,
123 students participated in the program. In addition, 37 students
participated in the Spring School, which was held onsite in
Mitaka Campus for the first time in 3 years.

(7) Number of Affiliated Staff (2023/3/31)
Chair of the Department of Astronomical Science
Optical and Infrared Astronomy Course
Professors
Associate Professors
Associate Professors (Senior Lecturers)
Assistant Professors
Radio Astronomy Course
Professors
Associate Professors
Associate Professors (Senior Lecturers)
Assistant Professors
General Astronomy and Astrophysics Course
Professors
Associate Professors
Associate Professors (Senior Lecturers)
Assistant Professors
Total

1
11
8
1
11
10
12
1
14
11
15
1
18
114

(8) Graduate Students (33 students)

126

1st year (5 student)
Name
Kakimoto, Takumi

Principal Supervisor
Supervisor
Tanaka, Masayuki
Iono, daisuke

Sato, Yoshiaki

Sekii, Takashi

Shimojo, Masumi

Naito, YoshihiroHara, Hirohisa

Ishikawa, Ryoko

Spectroscopic study of Alfvenic waves in the source region ofhigh-speed solar winds

Hatano, ShunOuchi, Masami

Koyama, Yusei

Ionizing Sources of Early Galaxies and Cosmic Reionization
Studied by Deep Spectroscopy

Watanabe, Kuria

Ouchi, Masami

Tominaga, Nozomu

Origin of Elements in Early Galaxies Studied by Deep
Spectroscopy

2nd year (5 students)
Name

Principal Supervisor

Ikeda, Ryota

Iono, Daisuke

Ishigami, ShunHara, Hirohisa

Supervisor
Tadaki, Kenichi
Tanaka, Masayuki
Katsukawa, Yukio

Koshisaka, Shiori

Kotani, Takayuki

Fukagawa, Misato

Nishigaki, Moka

Ouchi, Masami

Takata, Tadafumi

Exploring the early phase of galaxy formation with large optical
datasets

Yoshida, Tomohiro

Nomura, Hideko

Fukagawa, Misato

Research on Chemical Structure of Planet-Forming Regions by
ALMA Observations of Molecular Lines

VII Graduate Course Education

Title of Research Project
A bird’s eye view of galaxy evolution across cosmic time
Study of High-Energy Phenomena in the Solar Corona Tackledwith X-ray Imaging-Spectroscopy

Title of Research Project
Observational Studies of Distant Galaxies using ALMA
Spectroscopic study at the site of coronal heating
Study of disks around pre-main sequence stars and extrasolar
planets by high-contrast polarization direct imaging

3rd year (9 students)
Name
Naufal,Abdurrahman

Principal Supervisor

Supervisor

Title of Research Project
Morphological Evolution of Galaxies across Cosmic
Environment

Koyama, Yusei

Tanaka, Masayuki

Ishihara, Kousuke

Saito, Masao

Nakamura, Fumitaka

Sasaki, Shunsuke

Takiwaki, Tomoya

Machida, Mami

Sugimori, Kanako

Tanaka, Masayuki

Onodera, Masato

Tada, Shotaro

Kotani, Takayuki

Hayano, Yutaka
Minowa, Yosuke

Development of a novel method to realize ultra-precision
detector characterization for exoplanet and astrometricobservation in space

Doi, Kiyoaki

Kataoka, Akimasa

Nomura, Hideko
Fukagawa, Misato

Unveiling planet formation by observations of protoplanetary
disks

BHARDWAJ,
ShubhamDainotti, Maria
Giovanna

Tominaga, Nozomu

The Multiwavelength analysis of Gamma-Ray Bursts via
machine learning

Ogami, Itsuki

Aoki, Wako

Furusawa, Hisanori

Sato, Masato

Tominaga, Nozomu

Takiwaki, Tomoya

4th year (9 students)
Name

Principal Supervisor

Supervisor

Study of high-mass star formation processes, focusing on
hierarchical fragmentation
Turbulent-driven mechanism of core-collapse supernovae
Evolution of spectral energy distributions of galaxies overcosmic time

The Nature of the Andromeda Stellar Halo and Substructures
Explored with the Subaru Telescope
Supernova light curve and observation

Title of Research Project
Search for extra-solar planets around young to late stars, andbrown dwarfs for understandings planet formation at various
evolutionary stages

Kasagi,Yui

Kotani, Takayuki

Hayashi, Saeko
Aoki, Wako

Kashiwagi, Raiga

Iwasaki, Kazunari

Takiwaki, Tomoya

Kobayashi,Umi

Tanaka, Masayuki

Nakano, Suzuka

Nakanishi, Koichiro

Nakanishi, Koichiro
Sekii, Takashi
Tanaka, Masayuki

Masai,Takaho

Gonzalez Garcia,
AlvaroUzawa, Yoshinori
Kojima, Takafumi

Study of the effect of aberrations on aperture efficiency in radio
telescopes towards high-performance multi-beam receivers at
sub-mm wavelengths

Omae, Rikuto

Machida, Mami

Ouchi, Masami

Study of galactic magnetic field evolution using the polarization
properties of intervening galaxies

Tashima, Yuta

Machida, Mami

Nakamura, Fumitaka

Study of the galactic magnetic fields using the MHD simulationand observational visualization

Hosokawa, Kou

Kotani, Takayuki

Minowa, Yosuke
Fujii, Yuka

Development of high-contrast and high-spectral resolution
spectrometer for the Subaru telescope and characterization of
exoplanet atmospheres

Seo, Chanoul

Fujii, Yuka

Nomura, Hideko
Ikoma, Masahiro

Atmospheres of sub-Neptune-sized exoplanets in contact withmagma ocean

5th year (5 students)
Name

Principal Supervisor

Supervisor

Takemura, Hideaki

Nakamura, Fumitaka

Hirota, Tomoya

Kambara, Nagaaki

Hara, Hirohisa

Murakami, Izumi(NIFS)

Spectroscopic diagnostics of highly ionised astrophysicalplasmaNishiumi,Taku

Hori,Yasunori

Aoki, Wako
Izumiura, Hideyuki

Characterization of exoplanets with MuSCAT series

Liang, Yongming

Tanaka, Masayuki

Matsuda, Yuichi

Correlation between galaxy and IGM at z≈2 mapped by Subaru/
HSC

Fukagawa, Nao

Aoki, Wako

Iono, Daisuke

Contribution of rotating massive stars to the chemicalenrichment in the low-metallicity environments of dwarf
galaxies

Study on star formation process induced by collisions between
filamentary molecular clouds
Influence of galaxy interactions and mergers on AGN activities
The interplay and co-evolution between galaxies and active
supermassive blackholes

Title of Research Project
Study of star formation process focusing on the core massfunction

VII Graduate Course Education1272. Education and Research Collaboration with Graduate Schools
Name

128

Affiliated InstituteSupervisor

Title of Research Project
Elucidation of the Central Structure of the Phoenix Galaxy
Cluster by VLBI Observations
Observational Study on Exoplanet Formation
Theoretical study on formation of planetary systems
Development of a NIR spectrograph NINJA andobservational study of kilonova

Oki, Aika

The University of Tokyo Honma, Mareki

Ozawa, Yoshiki
Kambara, Yuki

The University of Tokyo Fukagawa, Misato
The University of Tokyo Kokubo, Eiichiro

Cha, Chaenae

The University of Tokyo Motohara, Kentaro

Narita, Kanako

The University of Tokyo Sakamoto, Seiichi

Mitsuhashi, Kohei
Ikebe, Souta
Nishino, Yohei

The University of Tokyo Tomaru, Takayuki
The University of Tokyo Honma, Mareki
The University of Tokyo Tomaru, Takayuki

Fukumitsu, Kakeru

The University of Tokyo Katsukawa, Yukio

Homan, Shogo

The University of Tokyo Motohara, Kentaro

Mizutani, Yohsuke

The University of Tokyo Kokubo, Eiichiro

Yano, Yuta

The University of Tokyo Nakamura, Fumitaka

Fariyanto, Elika
Prameswari

The University of Tokyo Honma, Mareki

The M84 Jet Collimation Profile Analysis

Moritsuka, Akie

The University of Tokyo Katsukawa, Yukio

Study of magneto-convection on the solar surface with
spectro-polarimetric observations

Adachi, Hiroaki

The University of Tokyo Fukagawa, Misato

Kofuji, Yutaro

The University of Tokyo Honma, Mareki

Chen, Nuo

The University of Tokyo Motohara, Kentaro

Morii, Kaho

The University of Tokyo Nakamura, Fumitaka

Kinoshita, Shinichi

The University of Tokyo Nakamura, Fumitaka

Takamura, Mieko

The University of Tokyo Honma, Mareki

Mitsuhashi, Ikki

The University of Tokyo Sakamoto, Seiichi

Yoshida, Yuki

The University of Tokyo Kokubo, Eiichiro

Okino, Hiroki

The University of Tokyo Honma, Mareki

Kushibiki, Kosuke

The University of Tokyo Motohara, Kentaro

Hoshino, Haruka
Yamazaki, Yuta

The University of Tokyo Kokubo, Eiichiro
The University of Tokyo Nakamura, Fumitaka

Guo, Kangrou

The University of Tokyo Kokubo, Eiichiro

Lee, Sujin

The University of Tokyo Honma, Mareki

VII Graduate Course Education

Observational Study of Material Evolution in Interstellar
Space
Gravitational Wave Observation by KAGRA
Analysis of Fast Radio Bursts with GPUs
Studies for Gravitational Wave Telescope, KAGRA
Study on an image restoration technique for high-resolution
solar images
Development of a camera unit for Y-band high dispersion
spectrograph TARdYS for TAO telescope and evaluation of
NIR array detectors.
Planetary system formation from planetesimal rings
Time variation in mass accretion rate on protostars due tomerging molecular cloud cores

Observational Research on Planetary-system Formation
around Young Stars
Imaging super-massive black holes with mm VLBI
Observational Study of Galaxy Formation and Evolution in
the ZFOURGE-COSMOS Field
Testing and Constructing High-mass Star Formation Theories
by ALMA Observations
MHD simulations of star formation
Measurement of Faraday rotation of NLSy1s using ultrawideband VERA polarimetry
Exploration of the star-formation process in high-redshift
galaxies using observations of submillimeter galaxies
Theoretical Study on Formation of Planetary Systems
Observational study of active galactic nuclei jets with global
VLBI network
Development of an Integral Field Unit SWIMS-IFU and an
Observational Study of Nearby LIRGs
Theoretical Study on Formation of Planetary Systems
The Origin and Evolution of Heavy Elements in the Universe
Planetesimal dynamics in the presence of a massive
companion
Radio observations of pulsars/magnetars

3. Commissioned Graduate Students
Doctoral Course

Affiliated Institute

PeriodSupervisor

Title of Research ProjectAbe, Homare

Tokyo Institute ofTechnology

2022/5/1–
2023/3/31

Aso, Yoichi

Measurement of birefringence in a sapphire
mirror for the gravitational-wave telescope
KAGRA

Uno, Shinsuke

The University of Tokyo

2022/4/1–
2023/3/31

Uzawa, Yoshinori

Development of detector circuits for a
submillimeter multichroic camera

Naganuma, Toyo

The University ofElectro-Communications

2022/4/1–
2023/3/31

Uzawa, Yoshinori

Development of the multi-chroic mm/submm wave
cameraNiwa, Ayako

Tsukuba University

2022/6/1–
2023/3/31

Matsuo, Hiroshi

Development of photon counting THz intensity
interferometry

Huang, Shuo

The University of Tokyo

2022/4/1–
2023/3/31

Kawabe, Ryohei

Observational study of submillimeter galaxies
based on the multi-wavelength SED analysis

Masui, Sho

Osaka Prefecture
University

2022/4/1–
2023/3/31

Kojima, Takafumi

Development of superconductive circuits for next
generation radio telescope

Matsumoto, Takeru

Osaka Metropolitan
University

2022/4/1–
2023/3/31

Development of a radio spectrometer with delayNishimura, Atsushi line-based ramp-compare ADC implemented on
FPGA

Miyato, Ken

The University ofElectro-Communications

2022/10/1–
2023/3/31

Nishimura, Atsushi 3D Molecular Cloud Mapping in the Milky Way

Yamasaki, Yasumasa

Osaka Prefecture
University

2022/4/1–
2023/3/31

Kojima, Takafumi

Development of wideband and multi-beam andoptics for radio telescope

Period2022/4/1–
2023/3/31

Supervisor
Tominaga,
NozomuTitle of Research Project
Narrow-band survey and follow-ups of brightmetal-poor star candidates

Master’s Course

Affiliated InstituteOkada, Hiroko

Konan University

Kawashita, Sana

Osaka Prefecture
University

2022/4/1–
2022/9/30

Tatematsu,
Ken'ichiDevelopment and commissioning of new 72–116
GHz 7-beam receiver for 45-m telescope

Koseki, Tomohiro

Tsukuba University

2022/4/1–
2023/3/31

Matsuo, Hiroshi

Development of terahertz photon counting type
intensity interferometer

Chinen, Tsubasa

Osaka Prefecture
University

2022/4/1–
2022/9/30

Tatematsu,
Ken'ichiDevelopment and commissioning of new 72–116
GHz 7-beam receiver for 45-m telescope

Chounan, Yuuta

Tokyo University of
Science2022/4/1–
2023/3/31

Development and evaluation of high-Q
Makise, Kazumasa superconducting resonators for superconducting
quantum computers

Nakao, Yuuka

Osaka Prefecture
University

2022/4/1–
2023/3/31

Nishimura, Atsushi

Development of All-Digital Radio Spectrometer
for wideband radio observation.

Nishimoto, Shinpei

Osaka Prefecture
University

2022/4/1–
2023/3/31

Nishimura, Atsushi

Multiple emission line analysis using machinelearning

Masukura, Akihiro

Nagoya University

2022/1/1–
2022/12/31

Shan, Wenlei

Research on the superconducting planar circuitfor MMIC SIS receiver

Muramatsu, Hiromi

Tokyo Universityof Agriculture andTechnology

2022/5/1–
2023/3/31

Aoki, Wako

Ultra-high contrast imaging for direct
observation of exoplanets

Yanagawa, Anri

Nara Women's
University

2022/10/1–
2022/11/30

Tanaka, Masayuki

Morphological study of member galaxy clusters
viewed with Subaru HSC

Yoneyama, Sho

Osaka Prefecture
University

2022/4/1–
2022/9/30

Tatematsu,
Ken'ichiDevelopment and commissioning of new 72–116
GHz 7-beam receiver for 45-m telescope

VII Graduate Course Education

129

4. Degrees Achieved with NAOJ Facilities
Name

130

DegreeLiang, Yongming

Doctor of Philosophy, SOKENDAI

Takemura, Hideaki

Doctor of Philosophy, SOKENDAIVII Graduate Course Education

Title of Research ProjectCorrelation between Galaxies and IGM at z≈2 Mapped by Subaru/
HSC
Study of Dense Core Property and Core Mass Function with
Simulation and Observation Data to Reveal the Core Growth with
Observations

VIII Public Access to Facilities
1. Mitaka Campus[Open year-round]
Dates: April to March, 10:00–17:00
Every day except for New Year’s season (December
28–January 4) and the following temporary closuredays (4 days in total): October 29 (for Mitaka OpenHouse Day, open to participants only), November 12(due to equipment inspection), and February 11–12(due to snowfall).
Visitors: 14,245 (of which 1,561 were in groups)
Open Facilities: Observatory History Museum (65-cm
Telescope Dome), 20-cm Telescope Dome, Solar
Tower Telescope, Exhibit Room, Repsold Transit
Instrument Building (Transit Instrument Museum),
Astronomical Instruments Museum, Gautier Meridian
Circle Building, Old Library, 6-m Millimeter-Wave
Radio Telescope
As a measure against the COVID-19 pandemic,
only the building exteriors and the areas around theentrances were open to the public.
From April 9, public access to solar observation
parties and inside the Observatory History Museum
were allowed mainly on Saturdays and Sundays.
From June 20 the interior of the Observatory History
Museum was open during normal hours.
[Regular Star Gazing Party]
Dates: (Online)
April–October, Friday before second Saturday;
fourth Saturday
November–March, Friday before second Saturday(On-site) November–March, fourth Saturday(Online) Viewers: Held 18 times, with the total number ofmaximum simultaneous connections reaching 1,851
Total Views: 20,107 (As of March 31, 2023)(On-site) Visitors: Held 5 times, 60 guests each time for a
total of 220 guests.
All on-site events until October were canceled dueto the COVID-19 pandemic. Online events werebroadcasted via Zoom to YouTube Live.
[4D2U Theater Showings]
Dates: Friday before second Saturday; first and third
Saturdays
Capacity: 42 people per day during April, increased to 60
people per day in May(reduced capacity due to the COVID-19 pandemic)
Visitors: 1,781 (36 events planned and 34 events held)
The April 2 event was canceled as a preventative
measure against the COVID-19 pandemic.
The February 10 event was canceled due to snow
fall.

[Special Open-House Event] Mitaka Open House Day
Dates: October 28 (Fri.), 2022, 19:00–20:00 (Online lecture
broadcasts only)
October 29 (Sat.), 2022, 10:00–17:00 (Hybrid Format)
Topic: Time and Astronomy
Onsite Attendees: 419 (advance registration required)
Number of Contents:
Live streams and YouTube Premier events: 9
Video Contents: 22
Total Contents: 31
Total Maximum Simultaneous Connections:approximately 1000
Total Views in the First Month after the Release: 65,480
This event is jointly sponsored by NAOJ, the University ofTokyo Graduate School of Science Institute of Astronomy, the
SOKENDAI Department of Astronomical Science, and the
NINS Astrobiology Center. In FY 2021, instead of being held
on-site at Mitaka Campus, Mitaka Open House Day was held
online only on Saturday (broadcasted on YouTube Live andarchived on our YouTube channel).
This event is jointly sponsored by NAOJ, the University ofTokyo Graduate School of Science Institute of Astronomy, the
SOKENDAI Department of Astronomical Science, and the
NINS Astrobiology Center. In FY 2022, taking preventative
measures against the COVID-19 pandemic into consideration,
the event was held in an onsite (limited capacity, advanced
reservations required) and online hybrid format. The main
lecture on Friday was broadcast over the internet only. On
Saturday, Mitaka Campus facilities were opened, along with
online streaming and web contents.

Ishigaki Island: Ishigakijima Astronomical Observatory[Open year-round]
Dates: April to MarchOpen Hours: Wednesdays through Sundays and Holidays,
10:00–15:30 (except for the New Year’s season;
when Monday or Tuesday is a national holiday, thefacility is closed on the following Wednesday)
Stargazing Sessions: Evenings on Saturdays, Sundays, andHolidays, (20:00–21:00), one 45-minute session perevening
4D2U Theater: 15:30–16:15, from Wednesdays to Sundays
and on Holidays
Visitors: 3,477
Open Facilities: Murikabushi 105-cm optical/infrared
telescope, Hoshizora Manabi no Heya (Starry Sky
Study Room) (featuring exhibits of astronomical
images, the 4D2U “four-dimensional digital
universe,” and stargazing sessions with the 40cm telescope), interior of observation dome, andcorridors (including exhibits of astronomical images)

VIII Public Access to Facilities131

* From June 11 to March 10, due to damage to the dome caused
by lightning strikes around the facility, the 40-cm telescope has
been used for all stargazing sessions.
[Special Open Day]
[Southern Island Star Festival 2022] (co-sponsored)
Dates: July 30 (Sat.)–August 7 (Sun.), 2022
Star Festival Live & the Ishigaki Island Starry Sky and Star
Culture Lecture:
Held on August 6 (Sat.) at Painuhama-machi Green
Park with 600 onsite guests in attendance (livestreamed with the archived video available forviewing)Star Festival Memorial Lecture: Held on August 7 (Sun.) at
Ishigaki City Hall with 50 visitors (archived video
available for viewing)

132

VIII Public Access to Facilities

2. Mizusawa Campus[Open year-round]
Dates: April to March (except for New Year’s season),
9:00–17:00 daily
Visitors: 11,188
Open Facilities: Kimura Hisashi Memorial Museum, VERA
20-m antenna, 10-m VLBI antenna
The open house event is held at the campus with the cooperationof the Oshu Space and Astronomy Museum (OSAM:
Yugakukan) located in the campus.
In addition, in order to prevent the spread of the novel
coronavirus infection, the Kimura Hisashi Memorial Museum
was temporarily closed starting from April 1, but reopened on
July 1.

Ishigaki Island: VERA Ishigaki-jima Station[Open year-round]
Dates: April to March (except for the New Year’s season);premises are open to the public 24 hours/day, andthe observation rooms are open during the hours of
10:00–16:30.
Visitors: 2,584[Special Open day] The Special Open Day was held as a part of
the Southern Island Star Festival.
Dates: August 7 (Sun.), 2022
Visitors: 66
In view of the fact that novel coronavirus infections have not yet
ended, this year’s event was held while prioritizing the healthand safety of the participants and related people.

[Special Open Day] Held as Part of Iwate Galaxy Festival 2022
Dates: August 6 (Sat.), 2022–August 28 (Sun.), 2022
Visitors: 690
In light of the fact that novel coronavirus infections have not yet
ended, we consulted with Oshu City and the Oshu Space andAstronomy Museum (OSAM: Yugakukan), and this year, theevent was scaled down in size and was not concentrated on asingle day, but instead was held over a period of time as several
smaller-scale projects.

Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for New Year’s season)
Visitors: 1,038[Special Open Day]
The special open house is usually held as the "Yaeyama
Highland Star Festival" organized by the executive committee
led by Satsuma-sendai city hall and Kagoshima University. This
year, in light of the measures to prevent the spread of the novel
coronavirus, it was expected that the situation would continue
to require that events be cancelled or infection prevention
measures be taken to avoid crowding during the event period,and even if the event period was postponed, it would be difficult
to implement. After consultation with the main committee
members, it was decided to cancel the conference.

Ogasawara: VERA Ogasawara Station[Open year-round]
Dates: April to March (except for New Year’s season)
Visitors: 6,640[Special Open Day]
In view of the fact that novel coronavirus infections have notyet ended, we decided to cancel this event in order to protect thehealth and safety of the participants and related people and toprevent the spread of the infection.

VIII Public Access to Facilities

1333. Nobeyama Campus[Regular Open]
Open Time: 8:30–17:00 (every day except around New
Year’s Day (December 29 to January 3))
Visitors: 37,690
Open Facilities: 45-m Radio Telescope, Nobeyama Millimeter
Array, Nobeyama Radioheliograph, etc. (just viewing)[Open House Day] (held online only)
Date: August 28 (Saturday), 2022, 9:30–16:00 (available foraccess after the day)Participants:
Public lectures:~500 (am), ~400 (pm) (maximum viewers for live
streaming)~84,000 (total number of views in about the first 90
days)
Virtual space (poster session): ~200
Keyword rally (on-site): ~2500 (held during Aug. 26 – Oct.
30)
Nobeyama Open Campus Day 2022 was held online as aprecaution against the spread of COVID-19. The theme was“40th anniversary and challenge.” We had public lectures
relating to research activities in Nobeyama Campus by 7
researchers such as Associate Prof. Tomomi Shimoikura(Otsuma Women's University) and Project Assistant Prof.
Kotomi Taniguchi (NAOJ). The number of views for this live
streaming reached over 400, and the total number of viewsin the first 90 days was more than 84,000. We also held aposter session in virtual space where researchers gave poster
presentations. Twenty presenters were gathered through an open
call for posters, and about 200 participants gathered to see thepresentations. Moreover, we had a “keywords rally” event onsite. In that event, visitors find and collect keywords distributed
over the entire campus to get NRO original goods.
[Jimoto Kansha Day (Thanks Day for the locals)]This event could not be held due to prevention measures against
the spread of COVID-19.

134

VIII Public Access to Facilities

4. Subaru Telescope[Summit Facility Tour]The public tour program officially ended due tovarious circumstances.
Special tours: 15 groups, 75 visitors[Base Facility Tour]Special tours visitors: 4 groups, 206 visitors*Subaru Telescope initiated a new program, Subaru Stars,
to bring astronomy and STEM education to students andcommunities across the Island of Hawai‘i. This number includes
a school field trip as a part of the Subaru Stars program.
[Public Information]• Primary means of public information is posting at the official
website https://subarutelescope.org• Science results from the Subaru Telescope – 18 Japanese and
18 English articles• Announcements and topics of special activities and events –32 Japanese and 30 English articles.
• Press releases to the local media of Hawai‘i – 4 English
releases• Social media official accounts• Twitter accounts – SubaruTelescope (Japanese),
SubaruTel_Eng (English)• Facebook accounts – 国 立 天 文 台 (Japanese), National
Astronomical Observatory of Japan, and Subaru Telescope
Hawaii Outreach (English)• Instagram account – Subaru_telescope (English)• YouTube channels – SubaruTelescopeNAOJ (Japanese),S u b a r u Te l e s c o p e N A O J e ( E n g l i s h ) , s u b a r u t e l _starcamadmin (bilingual subchannel)*Main targets of the English accounts: Twitter for theinternational community and Facebook and Instagram for the
local community of Hawai‘i.
[Outreach]
1. Lectures, Workshops, etc., at Nearby Facilities:
41 cases, about 1,500 people in total(Main Activities)• School visits as a part of the Subaru Stars program• Judges at a series of VEX robotics competitions for elementary,intermediate, and high school teams• Classroom visits through the annual Journey Through The
Universe program• Support and supervision for A Hua He Inoa high school interns
to propose Hawaiian names for a planet-and-star pair
• Supervision for a science fair project for a intermediate school
student
2. Other Activities, including Outreach Events
1) In person Activities:
15 events, able to interact about 8,900 people.
(Main Activities)• Merrie Monarch Parade• AstroDay• AstroDay West• Career events (Career Fair, Career EXPO) for intermediate andhigh school students• Science events at elementary schools• Lili‘uokalani Gardens Christmas Light Show (as a member of
Maunakea Observatories volunteer group Na Hoku Huihui)• Maunakea Coin Contest (as a members of Maunakea
Astronomy Outreach Committee)2) Online Activities:
1 event, able to interact with about 100 people.
(Activity)• Video message to Tsukimi no Kai event organized by theUnited Japanese Society of Hawai‘i
3. YouTube Live Streaming:
10 cases, about 389,700 views(Main Activities)• MEXT GIGA School, live from the Subaru Telescope summit
facility• Live streaming of the signing ceremony for the agreement on
installation and operation of the Subaru-Asahi Star Camera,
between NAOJ and The Asahi Shimbun Company (*)• Live streaming of the total lunar eclipse (*)• Live streaming of the Mauna Loa eruption (*)• Live streaming of Geminids meteor shower (*)• Live galaxy classification in the NAOJ citizen science project
GALAXY CRUISE(*) Streamed from the Asahi Shimbun Astro LIVE YouTube
Channel. In addition, a 24/7 live stream from the Subaru-Asahi
Star Camera is offered through cooperation with The Asahi
Shimbun Company.
4. Volunteer Activities: 11 cases
In addition to traditional outreach activities, staff members
participated in volunteer activities to contribute to the local
community of Hawai‘i.
(Main Activities)• Tutoring at Hilo High School• Invasive Species Weed Pulls at Halepohaku, the mid-elevation
facilities of Maunakea• Maunakea Forest Restoration Project• The Food Basket (Hawai‘i Island’s Food Bank), packing anddelivery• Cleanup work at Lili‘uokalani Gardens
5. Media Interview/Filming: 24 cases (7 Japanese, 17 English)• 35 articles were published in newspapers in Japan• 25 articles were published in media in Hawai‘i (including
newspapers and online news websites)

VIII Public Access to Facilities135

IX Overseas Travel
Research and Academic Staff Overseas Travel(Including employees on annual salary system.)country/area

category

South Korea
China
ThailandTaiwanHong Kong
Singapore
Indonesia
Philippines
Other areas in Asia
Hawai`i
U.S.A.
Australia
Italy
U.K.
FranceCanadaGuam, Saipan
Germany
Other areas in Europe and Oceania
MexicoBrazilAfricaOther areas in South and Central America *Total

Business Trip

Training

Total

9
0
7
12
0
1
0
0
5
19
12
5
9
4
4
5
0
14
33
1
0
6
26
172

0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0

9
0
7
12
0
1
0
0
5
19
12
5
9
4
4
5
0
14
33
1
0
6
26
172

* In typical years, most travelers to South and Central America go to Chile.

136

IX Overseas Travel

X Award Winners
Award RecipientsHada, Kazuhiro
Okada, Norio
Yoneta, Kenta
Yoneta, Kenta

Affiliated Division
Mizusawa VLBI
Observatory
Advanced
Technology Center
Advanced
Technology Center
Advanced
Technology Center

Job Title

Public Relations
CenterDate

Assistant Professor

The 11th NINS Young Researcher's Prize

2022/7/16

Technical Expert

The 2022 Tokyo Merit Award (Technology
Promotion)

2022/10/1

The 8th OSJ/SPIE Student Award

2022/11/16

The 11th Visible Infrared Scanner Workshop
2022 Young Presenter Gold Prize

2022/12/23

Iwate Nichinichi Culture Award

2023/2/26

2022 Yoshihide Kozai Award

2023/3/15

Project Research
Staff
Project Research
Staff

Mizusawa VLBI
Observatory
Hanayama, Hidekazu

Award

Associate Professor(Lecturer)

X Award Winners

137

XI Library, Publications
1. Library
Number of books in each library (2023/3/31)
Japanese Books
Mitaka18,665
Nobeyama
1,128
Mizusawa
4,986
Hawai`i
1,699
Total
26,478Foreign Books
50,281
5,891
18,113
4,683
78,968

Total
68,946
7,019
23,0996,382
105,446

Number of journal titles in each library (2022/3/31)
Japanese Journals
Foreign Journals
Mitaka371
1,675
Nobeyama
16
82
Mizusawa
659
828
Hawai`i
15
9
Total
1,061
2,594

Total
2,046
98
1,487
24
3,653

2. Publication
Here we list continuing publications produced by NAOJ in FY 2022.
(Mitaka)01) Report of the National Astronomical Observatory of Japan, Vol. 23: 1 issue (Digital Publication Only).
02) Annual Report of the National Astronomical Observatory of Japan (Japanese), no. 34, Fiscal Year 2021: 1 issue03) Annual Report of the National Astronomical Observatory of Japan (English), vol. 24 Fiscal Year 2021: 1 issue04) Calendar and Ephemeris, 2023: 1 issue05) NAOJ News, No. 337–339: 3 issues06) NAOJ Pamphlet 2023 (English): 1 issue07) Rika Nenpyo (Chronological Scientific Tables), 2023: 1 issue

3. Publication Support
In FY 2022, the NAOJ Reprints were replaced by publication support.
National Astronomical Observatory publication support, No. 3581–3684: 104 issues.

138

XI Library, Publications

XII Important Dates
April 1, 2022 – March 31, 2023
2022

April 1Hiroshi Nagai (Project Associate Professor), Koichiro Nakanishi (Project Associate Professor), Charles L.
H. Hull (Project Assistant Professor, NAOJ Fellow) and Seiji Kameno (Professor, Joint ALMA Observatory)
received the 2021 Shoichiro Yoshida Memorial/Nikon Astronomy Achievement Award for the achievement ofrealization of ALMA polarimetry observations and promotion of millimeter and submillimeter polarimetry
science.

April 18

GALAXY CRUISE, NAOJ citizen science project, launched Season 2 with fainter galaxies.

April 19

Mizusawa VLBI Observatory announced that it will be the first National Astronomical Observatory ofJapan (NAOJ) entity to conduct crowdfunding to support young researchers involved in black hole research,disseminate research results, and maintain facilities including telescopes and other research equipment.

April 20
–April 22

TMT Project set up the NAOJ booth at OPIE SPACE & ASTRONOMICAL OPTICS EXPO 2022 held at Pacifico
Yokohama and showcased TMT, the 188-cm Telescope, and the Seimei Telescope in Okayama.

April 23

Subaru Telescope and TMT Project participated in Merrie Monarch Parade held in Hilo, the Island of Hawai‘i, as
Maunakea Observatories members.

April 28

The Churaboshi Research Team Workshop, abbreviated as “Churaken,” called for applications to participate inthis year's event to be held on Ishigaki Island (August 3 (Wed.) to August 5 (Fri.), 2012).

May 14

Subaru Telescope, its internal citizen science project PANOPTES, and TMT Project participated in the annual
AstroDay event, in Hilo, the Island of Hawai‘i, and provided fun science activities at their booths to the local
community.

May 22–May 26

TMT Project and ALMA Project set up the NAOJ booth at the hybrid Japan Geoscience Union (JpGU) Meeting2022 at Makuhari Messe and showcased TMT and ALMA.

May 24June
June 6–July 14Subaru Telescope scientists were in a live streaming of the MEXT GIGA School at the NAOJ YouTube channel
from the summit facility, Maunakea, Hawai‘i.
Subaru Telescope released new data from Hyper Suprime-Cam Legacy Archive (HSCLA).
Led by TMT International Observatory (TIO), TMT Project and Subaru Telescope staff members contributed tothe summer tutoring program at Hilo High School.

June 22

Subaru Telescope started the brand new educational program Subaru Stars at the Na‘alehu Elementary School
summer program in the southern part of the Island of Hawai‘i.

July 11–September 2

Subaru Telescope suspended observations for the aluminum recoating of the primary mirror and telescope
maintenance.

July 12NAOJ and the University of Notre Dame (NDU) in the Republic of Lebanon held an online signing ceremonyof a Memorandum of Understanding for Research and Academic Cooperation with the attendance of H. E. Mr.
Nidal Yahya, Ambassador of the Lebanese Embassy in Tokyo.

July 29

Four Undergraduate interns of the Akamai Workforce Initiative program, supervised by Subaru Telescope
mentors, presented at the Akamai Internship Symposium held at Grand Naniloa Hotel, Hilo, Hawai‘i.

July 30–August 7

The “Southern Island Star Festival” was held for the 21st time this year, featuring evening live performances& star lectures/viewing sessions, commemorative lectures, and a special opening of the VERA Ishigaki-jima
Station.

July 31

Subaru Telescope’s website for “Subaru Telescope 2.0” launched in English.

August 2–August 11

The Office of International Relations, in cooperation with relevant departments at NAOJ, exhibited a NAOJ
booth at the General Assembly of the International Astronomical Union (IAUGA 2022) held in Busan, Republicof Korea.

August 8

NameExoWorlds 2022 campain started.

August 10

It was announced that due to the Corona disaster, rather than being concentrated on a single day, the Special
Open House Day held as part of Iwate Galaxy Festival 2022 (August 20 (Sat.) to August 28 (Sun.)) would be
reduced in scale and held in the form of multiple smaller events over a period of time.

August 20–August 28“The Speical Open House Day held as part of Iwate Galaxy Festival 2022,” announced on August 10, was held
both on-site and online.

August 28

Open House Day of Nobeyama Radio Observatory was held online. The number of viewers for live streaming
reached over 400, and total number of views for all content in about the first 90 days was about 84,000.

September–May (2023)

TMT Project staff members contributed to the afterschool tutoring program every Wednesday at Hilo Intermediate
School.
XII Important Dates

139

September 1

Undergraduate students of the SOKENDAI Summer Student program, supervised by Subaru Telescope
scientists, gave online presentations about their study results.

September 13

NAOJ and The Asahi Shimbun Company held the signing ceremony for the agreement on installing andoperating the Subaru-Asahi Star Camera on the Subaru Telescope, Maunakea, Hawai‘i.

September 21–September 26

During the engineering observations, the Prime Focus Spectrograph (PFS) mounted on the Subaru Telescope
successfully obtained the first spectra from target stars.

October 6

Mizusawa VLBI Observatory received support from a total of 1256 people through crowdfunding from April
to June 2022, and those who agreed to have their names posted on the website are now listed in the manner they
requested at the time of application (honorific titles omitted).

October 11

Satoshi Miyazaki, Director of Subaru Telescope, sent a video message to Tsukimi no Kai event organized by theUnited Japanese Society of Hawai‘i, the Island of Oahu.

October 28–October 29

Mitaka Open House Day held in onsite/online hybrid format.

October 28–May 5A Subaru Telescope scientist helped and supervised A Hua He Inoa high school interns to participate andsuggest Hawaiian names for an exoplanet-and-star pair as part of the International Astronomical Union (IAU)
NameExoWorlds competition.

November 3

Masanori Iye, Professor emeritus of NAOJ and SOKENDAI, received The Order of the Sacred Treasure, Goldand Silver Star at the 2022 Conferment of Decoration.

November 5

Subaru Telescope, its internal citizen science project PANOPTES, and TMT Project participated in the annual
AstroDay West event at a shopping center in Kailua-Kona, the Island of Hawai‘i, and provided fun science
activities at their booths to the local community.

November 7–November 8
November 8
November 14
November 14–November 18

Director General Tsuneta made courtesy visits to Ministry of Foreign Affairs and others in Chile.

November 17

Subaru Telescope and its internal citizen science project PANOPTES participated in Career EXPO for high school
students in Hilo and its vicinity, and introduced various jobs and career paths.

November 19

A Subaru Telescope exoplanet scientist gave a talk at the Exoplanet Revolution event held at ‘Imiloa Astronomy
Center of Hawai‘i.

November 19–February 4
November 21
November 28–November 30

Subaru Telescope and TMT Project staff members contributed to a series of VEX robotics competitions as judges
for elementary, intermediate, and high school teams.
Subaru Telescope released the 3D virtual tour of inside and outside the summit facility's enclosure.
Subaru Telescope (host) and Astronomical Data Center (co-host) held the Subaru Telescope Data Analysis
Workshop in person at the NAOJ Mitaka Campus.

November 29

As a part of the Subaru Stars program, Subaru Telescope invited 3rd and 4th graders of Na‘alehu Elementary
School to the Hilo Base Facility for an immersive field trip.

December 1

The 28th “Astronomy Lecture for Science Journalists” held on the theme of “Technological Development in
NAOJ and Collaboration with Industry.”

December 7–December 8

NAOJ Future Planning Symposium 2022 ― How to decide and promote future plans ―”was held at NAOJ
Mitaka. The total number of participants over the two days was 558 (including online participants, 69% frominside NAOJ).

December 10

The 7th “Nagano Prefecture is Astro-Prefecture” meeting was held online at Bunka-hall in Kiso-Bunka-Koen
by “Nagano Prefecture is Astro-Prefecture” liaison council, which consists of Nobeyama Radio Observatory,
Kiso Observatory of the University of Tokyo, and so on. There were about 50 participants in the meeting.

December 12–December 14
December 19
December 20–December 21

140

Subaru Telescope and its internal citizen science project PANOPTES live-streamed the total lunar eclipse fromthe Island of Hawai‘i.
The Public Relations Center live streamed the lunar eclipse and occultation of Uranus.
Hidehiko Yuzaki, Governor of Hiroshima Prefecture, visited the summit facility of the Subaru Telescope,
Mauakea, Hawai‘i.

Subaru Telescope live streamed the Geminids meteor shower from Maunakea, Hawai‘i, for two consecutive
nights with the cooperation of The Asahi Shimbun Company.
ALMA Grant Fellow Symposium 2022 was held at Mitaka Campus and online.
ALMA/45m/ASTE Users Meeting 2022 was held at Mitaka Campus and online.

December 22

Liberal Democratic Party Policy Research Council Chairperson Koichi Hagiuda toured VERA Ishigaki-jima
Station and Ishigakijima Astronomical Observatory.

December 23–December 24

Subaru Telescope and TMT Project participated in the Lili‘uokalani Gardens Christmas Light Show in Hilo on
the Island of Hawai‘i as a member of Maunakea Observatories volunteer group Na Hoku Huihui.

XII Important Dates

2023
January 8–January 12

The Office of International Relations, in cooperation with the Subaru Telescope and other relevant departments
at NAOJ, exhibited a NAOJ booth at the 241st Meeting of the American Astronomical Society (241st AAS
Meeting) held in Seattle, USA.

January 13–March 15

The Maunakea Coin Contest, open to K-12 students on the Island of Hawai‘i, was held by the Maunakea
Astronomy Outreach Committee. A Subaru Telescope staff member was one of the leaders of the contest.

January 31–February 2
February 3

The annual Subaru Users Meeting FY 2022 was held in a hybrid style of on-site and online.
Ambassador of Chile to Japan visited NAOJ.

February 9

Subaru Telescope (as a member of Maunakea Observatories) and its internal citizen science project PANOPTES
participated in Career EXPO for intermediate school students in Hilo and its vicinity, and introduced various
jobs and career paths.

February 28

The National Astronomical Observatory of Japan, Mizusawa VLBI Observatory was selected for the 40th
Iwate Nichinichi Cultural Award in the academic and research category by the Iwate Nichinichi Shimbun,
which celebrated its 100th anniversary, and the award ceremony was held at Bellino Hotel Ichinoseki (Yamame,
Ichinoseki City).

February 28–March 4

Subaru Telescope and TMT Project staff members participated in the annual educational program Journey
Through the Universe and delivered interactive presentations in classrooms at public elementary, intermediate,and high schools in Hilo, Hawai‘i.

March 2
–March 3

As a part of the FY 2022 Project Review of NAOJ, the international external evaluation of the Division of
Science was conducted at Mitaka Campus.

March 2
–March 5

The Public Relations Center co-Hosted an onsite booth with 4 other organizations at the American Association
for the Advancement of Science Annual Meeting (AAAS2023 held in hybrid format).

March 7
–March 10
March 13
March 24

BEARS ALMA Proposal Workshop was held at Mitaka Campus.
The ALMA 10th anniversary ceremony was held in Chile.
The Public Relations Center live streamed the occultation of Venus.

Throughout the year
Subaru Telescope provides the 24/7 live streaming from Maunakea, Hawai‘i, with the Subaru-Asahi Star Camera
in collaboration with The Asahi Shimbun Company.

XII Important Dates

141

XIII Publications, Presentations
1. Refereed Publications
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, All-sky searchfor gravitational wave emission from scalar boson clouds aroundspinning black holes in LIGO O3 data, Phys. Rev. D, 105, 102001.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
LIGO Sci Collaboration, Virgo Collaboration, Virgo Collaboration,
KAGRA Collaboration: 2022, Searches for Gravitational Waves from
Known Pulsars at Two Harmonics in the Second and Third LIGOVirgo Observing Runs, ApJ, 935, 1.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
LIGO Sci Collaboration, Virgo Collaboration, Virgo Collaboration,
KAGRA Collaboration: 2022, First joint observation by theunderground gravitational-wave detector KAGRA with GEO 600,
Prog. Theor. Exp. Phys., 2022, 063F01.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, Model-based
Cross-correlation Search for Gravitational Waves from the Low-mass
X-Ray Binary Scorpius X-1 in LIGO O3 Data, ApJL, 941, L30.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, All-sky, allfrequency directional search for persistent gravitational waves from
Advanced LIGO's and Advanced Virgo's first three observing runs,
Phys. Rev. D, 105, 122001.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, Search forcontinuous gravitational wave emission from the Milky Way center in
O3 LIGO-Virgo data, Phys. Rev. D, 106, 042003.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, Search for

142

XIII Publications, Presentations

gravitational waves from Scorpius X-1 with a hidden Markov modelin O3 LIGO data, Phys. Rev. D, 106, 062002.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, All-sky searchfor continuous gravitational waves from isolated neutron stars using
Advanced LIGO and Advanced Virgo O3 data, Phys. Rev. D, 106,
102008.
Abbott, R., et al. including Akutsu, T., Aritomi, N., Capocasa,
E., Eisenmann, M., Flaminio, R., Hirata, N., Leonardi, M.,
Nakamura, K., Shoda, A., Takahashi, R., Tomaru, T., Washimi, T.,Zhao, Y., Aso, Y., Chen, D., Kozakai, C., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2022, Search for
Subsolar-Mass Binaries in the First Half of Advanced LIGO's andAdvanced Virgo's Third Observing Run, Phys. Rev. Lett., 129, 061104.
Abbott, R., et al. including Akutsu, T., Barton, M. A., Capocasa, E.,
Flaminio, R., Fukushima, M., Hirata, N., Ikenoue, B., Leonardi,M., Marchio, M., Nakamura, K., Obuchi, Y., Saito, S., Shimizu,
R., Shoda, A., Takahashi, R., Tanioka, S., Tapia San Martín, E.
N., Tomaru, T., Tsuzuki, T., Uraguchi, F., Washimi, T., Zhao,
Y., LIGO Scientific Collaboration, Virgo Collaboration, KAGRA
Collaboration: 2023, Population of Merging Compact Binaries
Inferred Using Gravitational Waves through GWTC-3, Phys. Rev. X,
13, 011048.
Abbott, R., et al. including Akutsu, T., Barton, M. A., Capocasa, E.,
Flaminio, R., Hirata, N., Leonardi, M., Marchio, M., Nakamura,K., Shoda, A., Takahashi, R., Tanioka, S., Tapia San Martin, E. N.,
Tomaru, T., Washimi, T., Zhao, Y., Fukushima, M., Ikenoue, B.,
Obuchi, Y., Saito, S., Shimizu, R., Tsuzuki, T., Uraguchi, F., Aso, Y.,
Kozakai, C., Ohishi, N.: 2022, Narrowband Searches for Continuousand Long-duration Transient Gravitational Waves from Known
Pulsars in the LIGO-Virgo Third Observing Run, ApJ, 932, 133.
Abbott, R., et al. including Akutsu, T., Barton, M. A., Capocasa, E.,
Flaminio, R., Hirata, N., Marchio, M., Nakamura, K., Shoda,A., Takahashi, R., Tanioka, S., Tapia San Martin, E. N., Tomaru,T., Washimi, T., Zhao, Y., Fukushima, M., Ikenoue, B., Obuchi,
Y., Saito, S., Shimizu, R., Tsuzuki, T., Aso, Y., Kozakai, C.,
Ohishi, N., LIGO Sci Collaboration, LIGO Sci Collaboration, Virgo
Collaboration, Virgo Collaboration, KAGRA Collaboration: 2022,
Search for Gravitational Waves Associated with Gamma-Ray Bursts
Detected by Fermi and Swift during the LIGO-Virgo Run O3b, ApJ,
928, 186.
Abbott, R., et al. including Flaminio, R., LIGO Sci Collaboration,
Virgo Collaboration: 2022, Search of the early O3 LIGO data forcontinuous gravitational waves from the Cassiopeia A and Vela Jr.
supernova remnants, Phys. Rev. D, 105, 082005.
Abdalla, E., et al. including Dainotti, M.: 2022, Cosmology intertwined:
A review of the particle physics, astrophysics, and cosmology
associated with the cosmological tensions and anomalies, J. HighEnergy Astrophys., 34, 49–211.

Abe, M., Shimizu, T., Shimojo, M.: 2022, An ALMA Observation ofTime Variations in Chromospheric Temperature of a Solar Plage
Region, Front. Astron. Space Sci., 9, 908249.
Acernese, F., et al. including Flaminio, R.: 2022, The Virgo O3 run and theimpact of the environment, Classical Quantum Gravity, 39, 235009.
Aihara, H., et al. including Furusawa, H., Furusawa, J., Harasawa,
S., Ito, K., Iwata, I., Koike, M., Komiyama, Y., Liang, Y. M.,
Mawatari, K., Mineo, S., Miyazaki, S., Morishima, T., Nakajima,K., Nakata, F., Okura, Y., Ouchi, M., Simunovic, M., Sugimori,K., Takagi, Y., Takata, T., Tanaka, M., Terai, T., Yamada, Y.,
Yamashita, T.: 2022, Third data release of the Hyper Suprime-Cam
Subaru Strategic Program, PASJ, 74, 247–272.
Aizawa, M., et al. including Kasuga, T.: 2022, Fast optical flares from M
dwarfs detected by a one-second-cadence survey with Tomo-e Gozen,
PASJ, 74, 1069–1094.
Akaho, R., Harada, A., Nagakura, H., Iwakami, W., Okawa, H.,
Furusawa, S., Matsufuru, H., Sumiyoshi, K., Yamada, S.: 2023,
Protoneutron Star Convection Simulated with a New General
Relativistic Boltzmann Neutrino Radiation Hydrodynamics Code,ApJ, 944, 60.
Akins, H. B., Fujimoto, S., Finlator, K., Watson, D., Knudsen, K. K.,
Richard, J., Bakx, T. J. L. C., Hashimoto, T., Inoue, A. K., Matsuo,
H., Michalowski, M. J., Tamura, Y.: 2022, ALMA Reveals Extended
Cool Gas and Hot Ionized Outflows in a Typical Star-forming Galaxy
at Z=7.13, ApJ, 934, 64.
Akiyama, K., et al. including Ikeda, S., Kino, M., Nagai, H., Cui,
Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F., Event Horizon Telescope
Collaborat.: 2022, First Sagittarius A* Event Horizon Telescope
Results. I. The Shadow of the Supermassive Black Hole in the Centerof the Milky Way, ApJL, 930, L12.
Akiyama, K., et al. including Ikeda, S., Kino, M., Nagai, H., Cui,
Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F., Event Horizon Telescope
Collaborat.: 2022, First Sagittarius A* Event Horizon Telescope
Results. II. EHT and Multiwavelength Observations, Data Processing,and Calibration, ApJL, 930, L13.
Akiyama, K., et al. including Ikeda, S., Kino, M., Nagai, H., Cui,
Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F., Event Horizon Telescope
Collaborat.: 2022, First Sagittarius A* Event Horizon Telescope
Results. III. Imaging of the Galactic Center Supermassive Black
Hole, ApJL, 930, L14.
Akiyama, K., et al. including Ikeda, S., Kino, M., Nagai, H., Cui,
Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F., Event Horizon Telescope
Collaborat.: 2022, First Sagittarius A* Event Horizon Telescope
Results. IV. Variability, Morphology, and Black Hole Mass, ApJL,
930, L15.
Akiyama, K., et al. including Ikeda, S., Kino, M., Nagai, H., Cui,
Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F., Event Horizon Telescope
Collaborat.: 2022, First Sagittarius A* Event Horizon Telescope
Results. V. Testing Astrophysical Models of the Galactic Center Black
Hole, ApJL, 930, L16.
Akiyama, K., et al. including Ikeda, S., Kino, M., Nagai, H., Cui,

Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F., Event Horizon Telescope
Collaborat.: 2022, First Sagittarius A* Event Horizon Telescope
Results. VI. Testing the Black Hole Metric, ApJL, 930, L17.
Algera, H. S. B., et al. including, Fudamoto, Y.: 2023, The ALMAREBELS survey: the dust-obscured cosmic star formation ratedensity at redshift 7, MNRAS, 518, 6142–6157.
Ali, S. S., De Propris, R.: 2023, Unveiling UV-bright stellar populations
in red and dead galaxies with CUBES, Exp. Astron., 55, 199–207.
Ando, M., Shimasaku, K., Momose, R., Ito, K., Sawicki, M., Shimakawa,
R.: 2022, A systematic search for galaxy protocluster cores at thetransition epoch of their star formation activity, MNRAS, 513, 3252–
3272.
Andre, P. J., Palmeirim, P., Arzoumanian, D.: 2022, The typical widthof Herschel filaments, A&A, 667, L1.
Aoki, W., Beers, T. C., Honda, S., Ishikawa, H. T., Matsuno, T., Placco,
V. M., Yoon, J., Harakawa, H., Hirano, T., Hodapp, K., Ishizuka, M.,
Jacobson, S., Kotani, T., Kudo, T., Kurokawa, T., Kuzuhara, M.,
Nishikawa, J., Omiya, M., Serizawa, T., Tamura, M., Ueda, A.,
Vievard, S.: 2022, Silicon and strontium abundances of very metalpoor stars determined from near-infrared spectra, PASJ, 74, 273-282.
Aoki, W., Li, H. N., Matsuno, T., Xing, Q. F., Chen, Y. Q., Christlieb, N.,
Honda, S., Ishigaki, M. N., Shi, J. R., Suda, T., Tominaga, N., Yan,
H. L., Zhao, J. K., Zhao, G.: 2022, Four-hundred Very Metal-poor
Stars Studied with LAMOST and Subaru. I. Survey Design, Followup Program, and Binary Frequency, ApJ, 931, 146.
Aoki, W., Matsuno, T., Parthasarathy, M.: 2022, Gaia DR2 and EDR3
data and evolutionary status of post-AGB stars with high radial
velocities, PASJ, 74, 1368–1377.
Arakawa, S., Kokubo, E.: 2023, Number of stars in the Sun's birthcluster revisited, A&A, 670, A106.
Arakawa, S., Tanaka, H., Kokubo, E., Nishiura, D., Furuichi, M.:
2023, Threshold velocity for the collisional growth of porous dust
aggregates consisting of cohesive frictionless spheres, A&A, 670,
L21.
Arakawa, S., Tanaka, H., Kokubo, E.: 2022, Impacts of Viscous
Dissipation on Collisional Growth and Fragmentation of Dust
Aggregates, ApJ, 933, 144.
Arakawa, S., Tanaka, H., Kokubo, E.: 2022, Collisional Growth
Efficiency of Dust Aggregates and Its Independence of the Strengthof Interparticle Rolling Friction, ApJ, 939, 100.
Arimatsu, K., Tsumura, K., Usui, F., Watanabe, J.: 2022, Detectionof an Extremely Large Impact Flash on Jupiter by High-cadence
Multiwavelength Observations, ApJL, 933, L5.
Aritomi, N., et al. including Leonardi, M., Eisenmann, M., Page, M.,
Aso, Y., Shoda, A., Takahashi, R.: 2022, Demonstration of length
control for a filter cavity with coherent control sidebands, Phys. Rev.
D, 106, 102003.
Aruga, M., et al. including Sano, H.: 2022, Molecular and Atomic
Clouds Associated with the Gamma-Ray Supernova Remnant Puppis
A, ApJ, 938, 94.
Arzoumanian, D., Russeil, D., Zavagno, A., Chen, M. C. Y., Andre,
P., Inutsuka, S. I., Misugi, Y., Sanchez-Monge, A., Schilke, P.,
Men'shchikov, A., Kohno, M.: 2022, Velocity structure of the 50 pc
long NGC 6334 filamentary cloud Hints of multiple compressions
and their impact on the cloud properties, A&A, 660, A56.

XIII Publications, Presentations

143

Asano, T., Fujii, M. S., Baba, J., Bedorf, J., Sellentin, E., Zwart, S. P.:
2022, Impact of bar resonances in the velocity-space distribution of
the solar neighbourhood stars in a self-consistent N-body Galactic
disc simulation, MNRAS, 514, 460–469.
Asanok, K., Gray, M. D., Hirota, T., Sugiyama, K., Phetra, M., Kramer,
B. H., Liu, T., Kim, K. T., Pimpanuwat, B.: 2023, Proper Motions of
Water Masers in W49 N Measured by KaVA, ApJ, 943, 79.
Asayama, S., Kamazaki, T., Ishii, S., Ito, T., Fujii, Y., Iono, D.,
Gonzalez, A., Inata, M., Sakamoto, S.: 2022, ASTE Band 10 (787–950 GHz) heterodyne receiver: System description, commissioning,and science verification, PASJ, 74, 678–688.
Baba, J., Kawata, D., Schonrich, R.: 2022, Age distribution of stars inboxy/peanut/X-shaped bulges formed without bar buckling, MNRAS,
513, 2850–2861.
Baba, S., Imanishi, M., Izumi, T., Kawamuro, T., Nguyen, D. D.,
Nakagawa, T., Isobe, N., Onishi, S., Matsumoto, K.: 2022, The
Extremely Buried Nucleus of IRAS 17208-0014 Observed at
Submillimeter and Near-infrared Wavelengths, ApJ, 928, 184.
Bae, J., et al. including Cataldi, G.: 2022, Molecules with ALMA at
Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate
in Molecular-line Emission in the AS 209 Disk, ApJL, 934, L20.
Baek, G., et al. including Hirota, T.: 2022, Complex Organic Molecules
Detected in 12 High-mass Star-forming Regions with Atacama Large
Millimeter/submillimeter Array, ApJ, 939, 84.
Bajpai, R., et al. including Tomaru, T.: 2023, Estimation of Newtonian
noise from the KAGRA cooling system, Phys. Rev. D, 107, 042001 .
Bajpai, R., Tomaru, T., Kimura, N., Ushiba, T., Yamamoto, K., Suzuki,T., Honda, T.: 2022, Vibration analysis of KAGRA cryostat at
cryogenic temperature, Classical Quantum Gravity, 39, 165004.
Bajpai, R., Tomaru, T., Yamamoto, K., Ushiba, T., Kimura, N., Suzuki,T., Yamada, T., Honda, T.: 2022, A laser interferometer accelerometerfor vibration sensitive cryogenic experiments, Meas. Sci. Technol.,33, 085902.
Bakx, T. J. L. C., Dannerbauer, H.: 2022, High-z Sudoku: a diagnostic
tool for identifying robust (sub)mm redshifts, MNRAS, 515, 678–686.
Bakx, T. J. L. C., et al. including Zavala, J. A., Mitsuhashi, I., Tadaki,
K. I., Ikeda, R.: 2023, Deep ALMA redshift search of a z ~ 12
GLASS-JWST galaxy candidate, MNRAS, 519, 5076-5085.
Ball, W. H., et al. including Benomar, O.: 2022, Solar-like oscillations
and ellipsoidal variations in TESS observations of the binary 12
Bootis, MNRAS, 516, 3709–3714.
Barnes, A. T., et al. including Saito, T.: 2023, PHANGS-JWST First
Results: Multiwavelength View of Feedback-driven Bubbles (thePhantom Voids) across NGC 628, ApJL, 944, L22.
Barragan, O., et al. including Hirano, T.: 2022, The young HD 73583(TOI-560) planetary system: two 10-M-circle plus mini-Neptunes
transiting a 500-Myr-old, bright, and active K dwarf, MNRAS, 514,
1606–1627.
Bastian, T. S., Shimojo, M., Barta, M., White, S. M., Iwai, K.: 2022,
Solar observing with the Atacama large millimeter-submillimeter
array, Front. Astron. Space Sci., 9, 977368.
Bayandina, O. S., Brogan, C. L., Burns, R. A., Garatti, A. C. O.,
Chibueze, J. O., van den Heever, S. P., Kurtz, S. E., MacLeod, G.
C., Moscadelli, L., Sobolev, A. M., Sugiyama, K., Val'tts, I. E.,
Yonekura, Y.: 2022, The evolution of the H2O maser emission in theaccretion burst source G358.93-0.03, A&A, 664, A44.

144

XIII Publications, Presentations

Bean, B., et al. including Hayashi, Y., Kawasaki, W., Miel, R., Nakazato,
T., Shimada, K., Sugimoto, K., CASA Team: 2022, CASA, Common
Astronomy Software Applications for Radio Astronomy, PASP, 134,
114501.
Behrens, E., et al. including Harada, N., Nakanishi, K., ALMA
Comprehensive High-resolution Extragalactic Molecular Inventory(ALCHEMI) Collaboration: 2022, Tracing Interstellar Heating: An
ALCHEMI Measurement of the HCN Isomers in NGC 253, ApJ, 939,
119.
Beniyama, J., Sako, S., Ohsawa, R., Takita, S., Kobayashi, N., Okumura,S., Urakawa, S., Yoshikawa, M., Usui, F., Yoshida, F., Doi, M, Niino,
Y., Shigeyama, T., Tanaka, M., Tominaga, N., Aoki, T., Arima,N., Arimatsu, K., Kasuga, T., Kondo, S., Mori, Y., Takahashi, H.,
Watanabe, J.: 2022, Video observations of tiny near-Earth objects
with Tomo-e Gozen, PASJ, 74, 877–903.
Berg, D. A., et al. including Ouchi, M., Sugahara, Y., CLASSY Team:
2022, The COS Legacy Archive Spectroscopy Survey (CLASSY)
Treasury Atlas, ApJS, 261, 31.
Berman, D. A., et al. including Zavala, J. A.: 2022, PASSAGES: theLarge Millimeter Telescope and ALMA observations of extremely
luminous high-redshift galaxies identified by the Planck, MNRAS,
515, 3911–3937.
Berne, O., et al. including Naslim, N., PI Team, Core Team, SEPs: 2022,
PDRs4All: A JWST Early Release Science Program on Radiative
Feedback from Massive Stars, PASP, 134, 054301.
Blake, J. S. D., et al. including Fujiyoshi, T.: 2023, Saturn’s seasonalvariability from four decades of ground-based mid-infraredobservations, Icarus, 392, 115347.
Bolin, B. T., Ahumada, T., van Dokkum, P., Fremling, C., Granvik, M.,
Hardegree-Ullman, K. K., Harikane, Y., Purdum, J. N., Serabyn, E.,
Southworth, J., Zhai, C.: 2022, The discovery and characterization of(594913) 'Ayló' chaxnim, a kilometre sized asteroid inside the orbit ofVenus, MNRAS Lett., 517, L49–L54.
Booth, A. S., et al. including Nomura, H.: 2023, Sulphur monoxide
emission tracing an embedded planet in the HD 100546 protoplanetarydisk, A&A, 669, A53.
Bouwens, R. J., et al. including Fudamoto, Y., Algera, H.: 2022,
Reionization Era Bright Emission Line Survey: Selection andCharacterization of Luminous Interstellar Medium Reservoirs in the z> 6.5 Universe, ApJ, 931, 160.
Bouy, H., et al. including Tamura, M., Motohara, K.: 2022, Infrared
spectroscopy of free-floating planet candidates in Upper Scorpius andOphiuchus, A&A, 664, A111.
Brinch, M., et al. including Zavala, J., COSMOS Team: 2023,
COSMOS2020: Identification of High-z Protocluster Candidates in
COSMOS, ApJ, 943, 153.
Broderick, A. E., et al. including Cui, Y.: 2022, The Photon Ring in
M87*, ApJ, 935, 61.
Broderick, A. E., et al. including Moriyama, K., Cui, Y., Hada, K.,
Honma, M., Kofuji, Y., Okino, H., Oyama, T., Sasada, M., Tazaki, F.,
Akiyama, K., Ikeda, S., Kino, M., Nagai, H.: 2022, Characterizing
and Mitigating Intraday Variability: Reconstructing Source Structure
in Accreting Black Holes with mm-VLBI, ApJL, 930, L21.
Brouillet, N., et al. including Sanhueza, P.: 2022, ALMA-IMF IV. A
comparative study of the main hot cores in W43-MM1: Detection,
temperature, and molecular composition, A&A, 665, A140.

Brusa, M., et al. including Schramm, M.: 2022, The eROSITA Final
Equatorial-Depth Survey (eFEDS) The first archetypal quasar in the
feedback phase discovered by eROSITA, A&A, 661, A9.
Buitrago-Casas, J. C., et al. including Narukage, N.: 2022, The faintest
solar coronal hard X-rays observed with FOXSI, A&A, 665, A103.
Burgarella, D., et al. including Bakx, T. J. L. C., Fudamoto, Y., Sugahara,Y., Zavala, J.: 2023, Identification of large equivalent width dusty
galaxies at 4 < z < 6 from sub-millimetre colours, A&A, 671, A123.
Burgarella, D., et al. including Fudamoto, Y., ALPINE Team: 2022, The
ALMA-ALPINE [C II] survey The star formation history and the dust
emission of star-forming galaxies at 4.5 < z < 6.2, A&A, 664, A73.
Cadieux, C., et al. including Hirano, T., Ikoma, M., Kotani, T.,
Tamura, M.: 2022, TOI-1452 b: SPIRou and TESS Reveal a SuperEarth in a Temperate Orbit Transiting an M4 Dwarf, AJ, 164, 96.
Cao, S. L., Dainotti, M., Ratra, B.: 2022, Standardizing Platinum
Dainotti-correlated gamma-ray bursts, and using them withstandardized Amati-correlated gamma-ray bursts to constrain
cosmological model parameters, MNRAS, 512, 439–454.
Cao, S. L., Dainotti, M., Ratra, B.: 2022, Gamma-ray burst data strongly
favour the three-parameter fundamental plane (Dainotti) correlation
over the two-parameter one, MNRAS, 516, 1386–1405.
Cardona-Torres, L., Aretxaga, I., Montana, A., Zavala, J. A., Faber, S. M.:
2023, The SCUBA-2 Cosmology Legacy Survey: the EGS deep field- III. The evolution of faint submillimetre galaxies at z < 4, MNRAS,
520, 5446–5463.
Chakraborty, A., Dainotti, M., Cantrell, O., Lloyd-Ronning, N.: 2023,
Radio-bright versus radio-dark gamma-ray bursts - more evidence for
distinct progenitors, MNRAS, 520, 5764–5782.
Changeat, Q., Edwards, B., Al-Refaie, A. F., Tsiaras, A., Skinner, J. W.,
Cho, J. Y. K., Yip, K. H., Anisman, L., Ikoma, M., Bieger, M. F.,
Venot, O., Shibata, S., Waldmann, I. P., Tinetti, G.: 2022, Five Key
Exoplanet Questions Answered via the Analysis of 25 Hot-JupiterAtmospheres in Eclipse, ApJS, 260, 3.
Chege, J. K., Jordan, C. H., Lynch, C., Trott, C. M., Line, J. L. B.,
Pindor, B., Yoshiura, S.: 2022, Optimising MWA EoR dataprocessing for improved 21-cm power spectrum measurements-finetuning ionospheric corrections, Publ. Astron. Soc. Aust., 39, E047.
Cheng, Y., et al.: 2022, Disks and Outflows in the Intermediate-mass
Star-forming Region NGC 2071 IR, ApJ, 933, 178.
Cheng, Y., Tan, J. C., Tobin, J. J., Fedriani, R., Andersen, M., Wang, J.:
2022, The Disk Population in a Distant Massive Protocluster, ApJ,
940, 124.
Chiaki, G., Wise, J. H.: 2023, Triggered Population III star formation:
the effect of H-2 self-shielding, MNRAS, 520, 5077-5089.
Chibueze, J. O., Akamatsu, H., Parekh, V., Sakemi, H., Ohmura, T., vanRooyen, R., Akahori, T., Nakanishi, H., Machida, M., Takeuchi, T.
T., Smirnov, O., Kleiner, D., Maccagni, F. M.: 2023, MeerKAT's viewof double radio relic galaxy cluster Abell 3376, PASJ, 75, S97–S107.
Ching, T.-C., et al. including Hasegawa, T., Arzoumanian, D., Hull,
C. L. H., Tamura, M., Kataoka, A., Nakamura, F., Shimajiri, Y.,
Tomisaka, K., Hayashi, S., Pyo, T. S.: 2022, The JCMT BISTRO-2
Survey: Magnetic Fields of the Massive DR21 Filament, ApJ, 941,
122.
Choplin, A., Goriely, S., Hirschi, R., Tominaga, N., Meynet, G.: 2022,
The p-process in exploding rotating massive stars, A&A, 661, A86.
Christian, S., et al. including Tamura, M., Narita, N.: 2022, A Possible

Alignment Between the Orbits of Planetary Systems and their Visual
Binary Companions, AJ, 163, 207.
Christiansen, J. L., et al. including Hirano, T., Tamura, M.: 2022,
Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2
Campaigns 2–18, AJ, 163, 244.
Chuang, Y. T., Okumura, T., Shirasaki, M.: 2022, Distinguishing
between ACDM and f(R) gravity models using halo ellipticity
correlations in simulations, MNRAS, 515, 4464–4470.
Colgain, E. O., Sheikh-Jabbari, M. M., Solomon, R., Bargiacchi, G.,
Capozziello, S., Dainotti, M. G., Stojkovic, D.: 2022, Revealing
intrinsic flat Lambda CDM biases with standardizable candles, Phys.
Rev. D, 106, L041301.
Cooper, E. M., et al. including Mawatari, K., Ouchi, M.: 2023,
HETDEX Public Source Catalog 1: 220 K Sources Including Over 50
K Lya Emitters from an Untargeted Wide-area Spectroscopic Survey,
ApJ, 943, 177.
Cooper, O. R., Casey, C. M., Zavala, J. A., Champagne, J. B., da Cunha,
E., Long, A. S., Spilker, J. S., Staguhn, J.: 2022, Searching Far andLong. I. Pilot ALMA 2 mm Follow-up of Bright Dusty Galaxies as aRedshift Filter, ApJ, 930, 32.
Cooray, S., Takeuchi, T. T., Ideguchi, S., Akahori, T., Miyashita, Y.,
Takahashi, K.: 2023, Wavelets and sparsity for Faraday tomography,
PASJ, 75, S85–S96.
Curotto, F., Finger, R., Kojima, T., Uemizu, K., Gonzalez, A., Uzawa,
Y., Bronfman, L.: 2022, Digital calibration test results for Atacama
Large Millimeter/submillimeter Array band 7+8 sideband separatingreceiver, J. Astron. Telesc. Instrum. Syst., 8, 024004.
Currie, T., et al. including Guyon, O., Tamura, M., Kotani, T., Kudo,
T., Hashimoto, J., Fukagawa, M., Lozi, J., Deo, V., Vievard, S.,
Skaf, N.: 2022, Images of embedded Jovian planet formation at awide separation around AB Aurigae, Nat. Astron, 6, 751–759.
Curti, M., et al. including Nakajima, K.: 2023, The chemical enrichment
in the early Universe as probed by JWST via direct metallicity
measurements at z ~ 8, MNRAS, 518, 425–438.
Dainotti, M. G., Bargiacchi, G., Lenart, A. L., Capozziello, S., Colgain,
E. O., Solomon, R., Stojkovic, D., Sheikh-Jabbari, M. M.: 2022,
Quasar Standardization: Overcoming Selection Biases and Redshift
Evolution, ApJ, 931, 106.
Dainotti, M. G., et al. including Moriya, T. J., Takiwaki, T., Tominaga,N.: 2022, The Quest for New Correlations in the Realm of theGamma-Ray Burst-Supernova Connection, ApJ, 938, 41.
Dainotti, M. G., et al.: 2022, The Optical Two- and Three-dimensional
Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst
Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope,
ApJS, 261, 25.
Dainotti, M. G., Lenart, A. L., Chraya, A., Sarracino, G., Nagataki, S.,
Fraija, N., Capozziello, S., Bogdan, M.: 2023, The gamma-ray bursts
fundamental plane correlation as a cosmological tool, MNRAS, 518,
2201–2240.
Dainotti, M. G., Levine, D., Fraija, N., Warren, D., Sourav, S.: 2022,
The Closure Relations in Optical Afterglow of Gamma-Ray Bursts,
ApJ, 940, 169.
Dainotti, M. G., Nielson, V., Sarracino, G., Rinaldi, E., Nagataki, S.,
Capozziello, S., Gnedin, O. Y., Bargiacchi, G.: 2022, Optical and
X-ray GRB Fundamental Planes as cosmological distance indicators,
MNRAS, 514, 1828–1856.

XIII Publications, Presentations

145

Dainotti, M. G., Sarracino, G., Capozziello, S.: 2022, Gamma-ray
bursts, supernovae Ia, and baryon acoustic oscillations: A binned
cosmological analysis, PASJ, 74, 1095–1113.
Delrez, L., et al. including Hirano, T., Hori, Y., Ikoma, M., Kotani, T.,
Krishnamurthy, V., Kusakabe, N., Tamura, M., Harakawa, H.,
Kudo, T., Vievard, S.: 2022, Two temperate super-Earths transiting anearby late-type M dwarf, A&A, 667, A59.
den Brok, J. S., et al. including Saito, T.: 2022, A CO isotopologue LineAtlas within the Whirlpool galaxy Survey (CLAWS), A&A, 662, A89.
Dereli-Begue, H., Pe'er, A., Ryde, F., Oates, S. R., Zhang, B., Dainotti,
M. G.: 2022, A wind environment and Lorentz factors of tens explain
gamma-ray bursts X-ray plateau, Nat. Commun., 13, 5611.
Desprez, G., et al. including Furusawa, H., Tanaka, M.: 2023, Combining
the CLAUDS and HSC-SSP surveys U + grizy(+YJHKs) photometry
and photometric redshifts for 18M galaxies in the 20 deg2 of the
HSC-SSP Deep and ultraDeep fields, A&A, 670, A82.
Dhanpal, S., Benomar, O., Hanasoge, S., Kundu, A., Dhuri, D., Das, D.,
Kaul, B.: 2022, Measuring Frequency and Period Separations in Redgiant Stars Using Machine Learning, ApJ, 928, 188.
Di Mauro, M. P., et al. including Benomar, O.: 2022, On the
Characterization of GJ 504: A Magnetically Active Planet-host Star
Observed by the Transiting Exoplanet Survey Satellite (TESS), ApJ,
940, 93.
Diamond-Lowe, H., et al. including Livingston, J. H.: 2022, The K2-3
System Revisited: Testing Photoevaporation and Core-powered Mass
Loss with Three Small Planets Spanning the Radius Valley, AJ, 164,
172.
Dohi, A., Nishimura, N., Sotani, H., Noda, T., Liu, H.-L., Nagataki, S.,
Hashimoto, M.: 2022, Impacts of the Direct Urca and Superfluidity
inside a Neutron Star on Type I X-Ray Bursts and X-Ray Superbursts,
ApJ, 937, 124.
Doke, Y., Hattori, K.: 2022, Probability of Forming Gaps in the GD-1
Stream by Close Encounters of Globular Clusters, ApJ, 941, 129.
Drimmel, R., et al. including Ramos, P.: 2023, A new resonance-likefeature in the outer disc of the Milky Way, A&A, 670, A10.
Dutta, S., et al. including Tatematsu, K., Sanhueza, P.: 2022, ALMA
Survey of Orion Planck Galactic Cold Clumps (ALMASOP):
Evidence for a Molecular Jet Launched at an Unprecedented Early
Phase of Protostellar Evolution, ApJ, 931, 130.
Esparza-Borges, E., et al. including Kusakabe, N., Livingston, J.,
Ikoma, M., Tamura, M.: 2022, A hot sub-Neptune in the desert anda temperate super-Earth around faint M dwarfs Color validation of
TOI-4479b and TOI-2081b, A&A, 666, A10.
Faisst, A. L., et al. including Fudamoto, Y.: 2022, ALPINE: A Large
Survey to Understand Teenage Galaxies, Universe, 8, 314.
Famiano, M. A., Mathews, G., Balantekin, A. B., Kajino, T., Kusakabe,M., Mori, K.: 2022, Evolution of Urca Pairs in the Crusts of Highly
Magnetized Neutron Stars, ApJ, 940, 108.
Fang, Q. L., Maeda, K., Kuncarayakti, H., Tanaka, M., Kawabata, K. S.,
Hattori, T., Aoki, K., Moriya, T. J., Yamanaka, M.: 2022, Statistical
Properties of the Nebular Spectra of 103 Stripped-envelope Corecollapse Supernovae*, ApJ, 928, 151.
Farah, J., et al. including Honma, M., Kofuji, Y., Moriyama, K., Cui,
Y., Hada, K., Okino, H., Oyama, T., Sasada, M., Tazaki, F., Nagai,
H., Event Horizon Telescope Collaborat.: 2022, Selective Dynamical
Imaging of Interferometric Data, ApJL, 930, L18.

146

XIII Publications, Presentations

Fedriani, R., Tan, J. C., Telkamp, Z., Zhang, Y. C., Yang, Y. L., Liu, M. Y.,
De Buizer, J. M., Law, C. Y., Beltran, M. T., Rosero, V., Tanaka, K. E.
I., Cosentino, G., Gorai, P., Farias, J., Staff, J. E., Whitney, B.: 2023,
The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated
Protostars, ApJ, 942, 7.
Finkelstein, S. L., et al. including Behroozi, P., Zavala, J. A., CEERS
Team: 2022, A Long Time Ago in a Galaxy Far, Far Away: A Candidatez ~ 12 Galaxy in Early JWST CEERS Imaging, ApJL, 940, L55.
Finkelstein, S., et al. including Behroozi, P., Zavala, J. A.: 2023,
CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy
Formation with JWST, ApJL, 946, L13.
Finley, A. J., Brun, A. S., Carlsson, M., Szydlarski, M., Hansteen, V.,
Shoda, M.: 2022, Stirring the base of the solar wind: On heat transfer
and vortex formation, A&A, 665, A118.
Finn, M. K., Indebetouw, R., Johnson, K. E., Costa, A. H., Chen, C. H. R.,
Kawamura, A., Onishi, T., Ott, J., Sewilo, M., Tokuda, K., Wong,
T., Zahorecz, S.: 2022, Structural and Dynamical Analysis of theQuiescent Molecular Ridge in the Large Magellanic Cloud, AJ, 164,
64.
Fraija, N., Dainotti, M. G., Ugale, S., Jyoti, D., Warren, D. C.: 2022,
Synchrotron Self-Compton Afterglow Closure Relations and FermiLAT-detected Gamma-Ray Bursts, ApJ, 934, 188.
Fraija, N., et al. including Dainotti, M. G.: 2022, Modeling Gamma-Ray
Burst Afterglow Observations with an Off-axis Jet Emission, ApJ,
940, 189.
Fraija, N., Kamenetskaia, B. B., Galvan-Gamez, A., Dainotti, M. G.,
Becerra, R. L., Dichiara, S., Veres, P., Pedreira, A. C. C. D. S.:
2022, GRB Afterglow of the Sub-relativistic Materials with Energy
Injection, ApJ, 933, 243.
Francis, L., van der Marel, N., Johnstone, D., Akiyama, E., Bruderer, S.,
Dong, R. B., Hashimoto, J., Liu, H. Y. B., Muto, T., Yang, Y.: 2022,
Gap Opening and Inner Disk Structure in the Strongly Accreting
Transition Disk of DM Tau, AJ, 164, 105.
Franson, K., et al. including Guyon, O., Julien, L.: 2023, Astrometric
Accelerations as Dynamical Beacons: Discovery and Characterizationof HIP 21152 B, the First T-dwarf Companion in the Hyades*, AJ,
165, 39.
Fudamoto, Y., et al. including Algera, H. S. B., Sugahara, Y.: 2022,
The ALMA REBELS Survey: Average [C II] 158 μm Sizes of Starforming Galaxies from z ~ 7 to z ~ 4, ApJ, 934, 144.
Fudamoto, Y., Inoue, A. K., Sugahara, Y.: 2022, Red Spiral Galaxies at
Cosmic Noon Unveiled in the First JWST Image, ApJL, 938, L24.
Fujii, M. S., Hattori, K., Wang, L., Hirai, Y., Kumamoto, J., Shimajiri,Y., Saitoh, T. R.: 2022, SIRIUS Project - V. Formation of off-centre
ionized bubbles associated with Orion Nebula Cluster, MNRAS, 514,
43–54.
Fujii, M. S., Wang, L., Hirai, Y., Shimajiri, Y., Kumamoto, J., Saitoh, T.:
2022, SIRIUS Project - IV. The formation history of the Orion Nebula
Cluster driven by clump mergers, MNRAS, 514, 2513–2526.
Fujimoto, S., Nagakura, H.: 2023, Explosive nucleosynthesis with fastneutrino-flavour conversion in core-collapse supernovae, MNRAS,
519, 2623–2629.
Fujisawa, K., et al. including Honma, M.: 2022, The YamaguchiInterferometer, PASJ, 74, 1415–1420.
Fujita, N., Hori, Y., Sasaki, T.: 2022, Orbital Evolution of Close-in
Super-Earths Driven by Atmospheric Escape, ApJ, 928, 105.

Fujita, S., Ito, A. M., Miyamoto, Y., Kawanishi, Y., Torii, K., Shimajiri,Y., Nishimura, A., Tokuda, K., Ohnishi, T., Kaneko, H., Inoue,T., Takekawa, S., Kohno, M., Ueda, S., Nishimoto, S., Yoneda,
R., Nishikawa, K., Yoshida, D.: 2023, Distance determination ofmolecular clouds in the first quadrant of the Galactic plane using deeplearning: I. Method and results, PASJ, 75, 279–295.
Fukaya, S., Shinnaga, H., Furuya, R. S., Tomisaka, K., Machida, M. N.,
Harada, N.: 2023, Twisted magnetic field in star formation processesof L1521 F revealed by submillimeter dual-band polarimetry using
the James Clerk Maxwell Telescope, PASJ, 75, 120–127.
Fukuchi, H., et al. including Izumi, T.: 2022, H1821+643: The Most
X-Ray and Infrared Luminous Active Galactic Nucleus (AGN) in the
Swift/BAT Survey in the Process of Rapid Stellar and Supermassive
Black Hole Mass Assembly, ApJ, 940, 7.
Fukushima, A., Ishi, D., Ezoe, Y., Ishikawa, K., Numazawa, M., Sakuda,S., Uchino, T., Inagaki, A., Ueda, Y., Morishita, H., Sekiguchi,L., Murakawa, T., Tsuji, Y., Mitsuda, K., Kanamori, Y.: 2022,
Improvement of imaging performance of silicon micropore X-ray
optics by ultra long-term annealing, Opt. Express, 30, 25195–25207.
Furusawa, S., Nagakura, H.: 2023, Nuclei in core-collapse supernovae
engine, Prog. Part. Nucl. Phys., 129, 104018.
Furuta, T., Kaneda, H., Kokusho, T., Nakajima, Y., Fukui, Y., Tsuge, K.:
2022, Three-dimensional geometry and dust/gas ratios in massive
star-forming regions over the entire LMC as revealed by the IRSF/
SIRIUS survey, PASJ, 74, 639–655.
Furuya, K., Hama, T., Oba, Y., Kouchi, A., Watanabe, N., Aikawa, Y.:
2022, Diffusion Activation Energy and Desorption Activation Energy
for Astrochemically Relevant Species on Water Ice Show No Clear
Relation, ApJL, 933, L16.
Furuya, K., Lee, S., Nomura, H.: 2022, Different Degrees of Nitrogenand Carbon Depletion in the Warm Molecular Layers of Protoplanetary
Disks, ApJ, 938, 29.
Gaidos, E., Hirano, T., Lee, R. A., Harakawa, H., Hodapp, K.,
Jacobson, S., Kotani, T., Kudo, T., Kurokawa, T., Kuzuhara, M.,
Nishikawa, J., Omiya, M., Serizawa, T., Tamura, M., Ueda, A.,
Vievard, S.: 2023, Planet(esimal)s around stars with TESS (PAST)
III: A search for triplet He I in the atmospheres of two 200 Myr-old
planets, MNRAS, 518, 3777–3783.
Galiano, A., et al. including Matsumoto, K.: 2022, NIRS3 spectral
analysis of the artificial Omusubi-Kororin crater on Ryugu, MNRAS,
514, 6173–6182.
Garcia-Bernete, I., et al. including Izumi, T., Packham, C.: 2022, A
high angular resolution view of the PAH emission in Seyfert galaxies
using JWST/MRS data, A&A, 666, L5.
Geen, S., et al. including Keszthelyi, Z.: 2023, Bringing Stellar
Evolution and Feedback Together: Summary of Proposals from theLorentz Center Workshop, PASP, 135, 021001.
Georgiev, B., et al. including Akiyama, K., Ikeda, S., Kino, M., Nagai,
H., Cui, Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K.,
Okino, H., Oyama, T., Sasada, M., Tazaki, F.: 2022, A Universal
Power-law Prescription for Variability from Synthetic Images ofBlack Hole Accretion Flows, ApJL, 930, L20.
Giamalaki, K., Beaulieu, C., Prochaska, J. X.: 2022, Assessing
Predictability of Marine Heatwaves With Random Forests, Geophys.
Res. Lett., 49, e2022GL099069.
Ginsburg, A., et al. including Guzman, A., Sanhueza, P., Tatematsu,

K., Nakamura, F., ALMA IMF Consortium: 2022, ALMA-IMF II.
Investigating the origin of stellar masses: Continuum images and dataprocessing, A&A, 662, A9.
Ginsburg, A., McGuire, B. A., Sanhueza, P., Olguin, F., Maud, L. T.,
Tanaka, K. E. I., Zhang, Y. C., Beuther, H., Indriolo, N.: 2023, Saltbearing Disk Candidates around High-mass Young Stellar Objects,
ApJ, 942, 66.
Gjergo, E., Sorokin, A. G., Ruth, A., Spitoni, E., Matteucci, F., Fan, X.
L., Liang, J. N., Limongi, M., Yamazaki, Y., Kusakabe, M., Kajino,
T.: 2023, GalCEM. I. An Open-source Detailed Isotopic Chemical
Evolution Code, ApJS, 264, 44.
Glikman, E., et al. including Rusu, C. E.: 2023, A Highly Magnified
Gravitationally Lensed Red QSO at z=2.5 with a Significant Flux
Ratio Anomaly, ApJ, 943, 25.
Glowacki, M., et al. including Tanaka, M.: 2022, Looking at the Distant
Universe with the MeerKAT Array: Discovery of a Luminous OH
Megamaser at z > 0.5, ApJL, 931, L7.
Greene, J. E., Greco, J. P., Goulding, A. D., Huang, S., Kado-Fong,E., Danieli, S., Li, J. X., Kim, J. H., Komiyama, Y., Leauthaud,A., MacArthur, L. A., Sifon, C.: 2022, The Nature of Low-surfacebrightness Galaxies in the Hyper Suprime-Cam Survey, ApJ, 933, 150.
Guaita, L., Aravena, M., Gurung-Lopez, S., Cantalupo, S., Marino, R.,
Riechers, D., da Cunha, E., Wagg, J., Algera, H. S. B., Dannerbauer,
H., Cox, P.: 2022, Tomography of the environment of the COSMOS/AzTEC-3 submillimeter galaxy at z ~ 5.3 revealed by Lyα and MUSE
observations, A&A, 660, A137.
Guo, K., Kokubo, E.: 2022, Planetesimal Dynamics in the Presence ofa Giant Planet. II. Dependence on Planet Mass and Eccentricity, ApJ,
935, 113.
Guo, Y. C., et al. including Zavala, J. A.: 2023, First Look at z > 1 Barsin the Rest-frame Near-infrared with JWST Early CEERS Imaging,
ApJL, 945, L10.
Gupta, A., Yen, H. W., Koch, P., Bastien, P., Bourke, T. L., Chung, E.
J., Hasegawa, T., Hull, C. L. H., Inutsuka, S., Kwon, J., Kwon,
W., Lai, S. P., Lee, C. W., Lee, C. F., Pattle, K., Qiu, K. P., Tahani,M., Tamura, M., Ward-Thompson, D.: 2022, Effects of Magnetic
Field Orientations in Dense Cores on Gas Kinematics in Protostellar
Envelopes, ApJ, 930, 67.
Haffert, S. Y., et al including Guyon, O.: 2022, Phasing the Giant
Magellan Telescope with the holographic dispersed fringe sensor, J.
Astron. Telesc. Instrum. Syst., 8, 021513.
Hamana, T., Hikage, C., Oguri, M., Shirasaki, M., More, S.: 2022, E/
B mode decomposition of HSC-Y1 cosmic shear using COSEBIs:
Cosmological constraints and comparison with other two-point
statistics, PASJ, 74, 923–945.
Hamana, T.: 2023, An empirical method for mitigating an excess upscattering mass bias on the weak lensing mass estimates for shearselected cluster samples, PASJ, 75, 14–29.
Hamano, S., Kobayashi, N., Kawakita, H., Takenaka, K., Ikeda, Y.,
Matsunaga, N., Kondo, S., Sameshima, H., Fukue, K., Otsubo, S.,
Arai, A., Yasui, C., Kobayashi, H., Bono, G., Saviane, I.: 2022,
Survey of Near-infrared Diffuse Interstellar Bands in Y and J Bands. I.
Newly Identified Bands, ApJS, 262, 2.
Hanaoka, Y.: 2022, Automated Sunspot Detection as an Alternative to
Visual Observations, Sol. Phys., 297, 158.
Harada, N., et al. including Nakanishi, K.: 2022, ALCHEMI Finds a

XIII Publications, Presentations

147

Shocking Carbon Footprint in the Starburst Galaxy NGC 253, ApJ,
938, 80.
Harada, N., Tokuda, K., Yamasaki, H., Sato, A., Omura, M., Hirano, S.,
Onishi, T., Tachihara, K., Machida, M. N.: 2023, Crescent-shaped
Molecular Outflow from the Intermediate-mass Protostar DK Cha
Revealed by ALMA, ApJ, 945, 63.
Harakawa, H., et al. including Takarada, T., Hirano, T., Kotani, H.,
Kuzuhara, M., Omiya, M., Hori, Y., Ishikawa, H. T., Ogihara,
M., Livingston, J., Currie, T., Aoki, W., Izumiura, H., Kambe,
E., Kokubo, E., Krishnamurthy, V., Kudo, T., Kurokawa, T.,
Kusakabe, N., Matsumoto, Y., Nishikawa, J., Nugroho, S. K.,
Serizawa, T., Takahashi, A., Ueda, A., Uyama, T., Vievard, S.,
Tamura, M.: 2022, A super-Earth orbiting near the inner edge of thehabitable zone around the M4.5 dwarf Ross 508, PASJ, 74, 904–922.
Harikane, Y., Inoue, A. K., Mawatari, K., Hashimoto, T., Yamanaka, S.,
Fudamoto, Y., Matsuo, H., Tamura, Y., Dayal, P., Yung, L. Y. A.,
Hutter, A., Pacucci, F., Sugahara, Y., Koekemoer, A. M.: 2022, A
Search for H-Dropout Lyman Break Galaxies at z~12–16, ApJ, 929, 1.
Harikane, Y., Ouchi, M., Oguri, M., Ono, Y., Nakajima, K., Isobe, Y.,
Umeda, H., Mawatari, K., Zhang, Y. C.: 2023, A Comprehensive
Study of Galaxies at z~9–16 Found in the Early JWST Data:
Ultraviolet Luminosity Functions and Cosmic Star Formation History
at the Pre-reionization Epoch, ApJS, 265, 5.
Harra, L., et al. including Sekii, T.: 2022, A journey of exploration to thepolar regions of a star: probing the solar poles and the heliospherefrom high helio-latitude, Exp. Astron., 54, 157–183.
Hartwig, T., Ishigaki, M. N., Kobayashi, C., Tominaga, N., Nomoto,K.: 2023, Machine Learning Detects Multiplicity of the First Stars in
Stellar Archaeology Data, ApJ, 946, 20.
Hasegawa, S., et al. including Hanayama, H.: 2022, Spectral Evolutionof Dark Asteroid Surfaces Induced by Space Weathering over a
Decade, ApJL, 939, L9.
Hashimoto, J., Liu, H. B., Dong, R., Liu, B., Muto, T.: 2022, Grain
Growth in the Dust Ring with a Crescent around the Very Low-mass
Star ZZ Tau IRS with JVLA, ApJ, 941, 66.
Hattori, K., Okuno, A., Roederer, I. U.: 2023, Finding r-II Sibling Stars
in the Milky Way with the Greedy Optimistic Clustering Algorithm,
ApJ, 946, 48.
Hatzes, A. P., et al. including Narita, N.: 2022, A Radial Velocity Studyof the Planetary System of π Mensae: Improved Planet Parameters forπ Mensae c and a Third Planet on a 125 Day Orbit, AJ, 163, 223.
Hayakawa, H., Hattori, K., Soma, M., Iju, T., Besser, B. P., Kosaka, S.:
2022, An Overview of Sunspot Observations in 1727–1748, ApJ, 941,
151.
Hayakawa, H., Murata, K., Soma, M.: 2022, The Variable Earth's
Rotation in the 4th–7th Centuries: New Delta T Constraints from
Byzantine Eclipse Records, PASP, 134, 094401.
Hayakawa, H., Soma, M., Daigo, R.: 2022, Analyses of historical solar
eclipse records in Hokkaido Island in the 18–19th centuries, PASJ,74, 1275–1286.
Hayakawa, H., Suzuki, D., Mathieu, S., Lefevre, L., Takuma, H., Hiei,
E.: 2023, Sunspot observations at Kawaguchi Science Museum:
1972–2013, Geosci. Data J., 10, 87–98.
Hayakawa, R., Yamada, S., Suda, H., Ichinohe, Y., Higurashi, R.,
Sakemi, H., Machida, M., Ohmura, T., Katsuda, S., Uchiyama, H.,
Sato, T., Akamatsu, H., Axelsson, M.: 2022, X-ray hot spots in the148

XIII Publications, Presentations

eastern ear of the supernova remnant W 50 and the microquasar SS
433 system, PASJ, 74, 510–520.
Hedglen, A. D., et al including Guyon, O.: 2022, Lab tests of segment/
petal phasing with a pyramid wavefront sensor and a holographic
dispersed fringe sensor in turbulence with the Giant Magellan
Telescope high contrast adaptive optics phasing testbed, J. Astron.
Telesc. Instrum. Syst., 8, 021515.
Heintz, K. E., et al. including Fudamoto, Y.: 2022, The ALMA REBELS
Survey: The Cosmic H I Gas Mass Density in Galaxies at z ≈ 7, ApJL,
934, L27.
Herman, M. K., de Mooij, E. J. W., Nugroho, S. K., Gibson, N.
P., Jayawardhana, R.: 2022, Dayside Fe I Emission, Day-Night
Brightness Contrast and Phase Offset of the Exoplanet WASP-33b,
AJ, 163, 248.
Herrera-Camus, R., Schreiber, N. M. F., Price, S. H., Ubler, H., Bolatto, A.
D., Davies, R. L., Fisher, D., Genzel, R., Lutz, D., Naab, T., Nestor, A.,
Shimizu, T., Sternberg, A., Tacconi, L., Tadaki, K.: 2022, Kiloparsec
view of a typical star-forming galaxy when the Universe was ~1 Gyr
old II. Regular rotating disk and evidence for baryon dominance ongalactic scales, A&A, 665, L8.
Higashi, S., Susa, H., Chiaki, G.: 2022, Saturation Level of Turbulencein Collapsing Gas Clouds, ApJ, 940, 38.
Hinkley, S., et al. including Kuzuhara, M., Tamura, M.: 2022, The
JWST Early Release Science Program for the Direct Imaging andSpectroscopy of Exoplanetary Systems, PASP, 134, 095003.
Hirai, Y., et al. including Aoki, W.: 2022, Origin of highly r-processenhanced stars in a cosmological zoom-in simulation of a Milky Waylike galaxy, MNRAS, 517, 4856–4874.
Hirano, T., et al. including Livingston, J. H., Kasagi, Y., Ishikawa, H. T.,
Miyakawa, K., Matsumoto, Y., Kokubo, E., Ikoma, M., Harakawa,
H., Hori, Y., Kotani, T., Krishnamurthy, V., Nishikawa, J., Omiya,M., Takahashi, A., Takarada, T., Ueda, A., Tamura, M.: 2023, An
Earth-sized Planet around an M5 Dwarf Star at 22 pc, AJ, 165, 131.
Hirota, T., et al. including Burns, R. A., Sugiyama, K.: 2022,
Millimeter methanol emission in the high-mass young stellar object
G24.33+0.14, PASJ, 74, 1234–1262.
Hisano, S., Crawford, F., Bonidie, V., Alam, M. F., Takahashi, K.,
Lorimer, D. R., Ridley, J. P., McLaughlin, M. M., Perera, B. B. P.:
2022, A Parkes Murriyang Search for Pulsars and Fast Transients in
the Large Magellanic Cloud, ApJ, 928, 161.
Holdship, J., et al. including Harada, N., Sakamoto, K., Nakanishi, K.,
Nishimura, Y., ALMA Comprehensive High-resolution Extragalactic
Molecular Inventory (ALCHEMI) collaboration: 2022, Energizing Star
Formation: The Cosmic-Ray Ionization Rate in NGC 253 Derived from
ALCHEMI Measurements of H3O+ and SO, ApJ, 931, 89.
Honda, M., Tazaki, R., Murakawa, K., Terada, H., Kudo, T., Hattori,
T., Hashimoto, J., Tamura, M., Watanabe, M.: 2022, Subaru/IRCS
L-band spectro-polarimetry of the HD 142527 disk scattered light,
PASJ, 74, 851–856.
Hoshino, H., Kokubo, E.: 2022, Orbital structure of planetary systems
formed by giant impacts: stellar mass dependence, MNRAS, 519,
2838–2847.
Hu, M. K., Hu, L., Jiang, J. A., Xiao, L., Fan, L. L., Wei, J. J., Wu, X.
F.: 2023, Prospects of Searching for Type Ia Supernovae with 2.5-m
Wide Field Survey Telescope, Universe, 9, 7.
Hubmayr, J., et al. including Imada, H., Kashima, S., Mitsuda, K.,

Nagai, M.: 2022, Optical Characterization of OMT-Coupled TES
Bolometers for LiteBIRD, J. Low Temp. Phys., 209, 396–408.
Huijten, E., et al including Chin, K. W.: 2022, TiEMPO: open-source
time-dependent end-to-end model for simulating ground-based
submillimeter astronomical observations, J. Astron. Telesc. Instrum.
Syst., 8, 028005.
Hull, C. L. H., et al.: 2022, Polarization from Aligned Dust Grains in thebeta Pic Debris Disk, ApJ, 930, 49.
Humire, P. K., et al. including Harada, N., Nakanishi, K.: 2022,
Methanol masers in NGC 253 with ALCHEMI, A&A, 663, A33.
Hwang, J., et al including Tomisaka, K., Tamura, M., Hasegawa, T.,
Kataoka, K., Nakamura, F., Shimajiri, Y., Arzoumanian, D.,
Kobayashi, M. I. N., Hayashi, S., Pyo, T. S., Hull, C. L. H., Kim, G.:
2022, The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hubfilament Structure, Monoceros R2, ApJ, 941, 51.
Ideguchi, S., Inoue, T., Akahori, T., Takahashi, K.: 2022, On thepotential of faraday tomography to identify shock structures insupernova remnants, MNRAS, 513, 3289–3301.
Iglesias, D. P., et al. including Miley, J.: 2023, X-shooter survey ofyoung intermediate-mass stars - I. Stellar characterization and discevolution, MNRAS, 519, 3958–3975.
Ikebe, S., Takefuji, K., Terasawa, T., Eie, S., Akahori, T., Murata, Y.,
Hashimoto, T., Kisaka, S., Honma, M., Yoshiura, S., Suzuki, S.,
Oyama, T., Sekido, M., Niinuma, K., Takeuchi, H., Yonekura, Y.,
Enoto, T.: 2023, Detection of a bright burst from the repeating fast
radio burst 20201124A at 2 GHz, PASJ, 75, 199–207.
Ikeda, R., Tadaki, K., Iono, D., Kodama, T., Chan, J. C. C., Hatsukade,B., Hayashi, M., Izumi, T., Kohno, K., Koyama, Y., Shimakawa, R.,
Suzuki, T. L., Tamura, Y., Tanaka, I.: 2022, High-resolution ALMA
Study of CO J=2–1 Line and Dust Continuum Emissions in Cluster
Galaxies at z=1.46, ApJ, 933, 11.
Ilee, J. D., et al. including Tsukagoshi, T., Nomura, H.: 2022, Unveilingthe outer dust disc of TW Hya with deep ALMA observations,
MNRAS Lett., 515, L23–L28.
Imai, M., et al. including Hirota, T., Nomura, H.: 2022, Chemical andPhysical Characterization of the Isolated Protostellar Source CB68:
FAUST IV, ApJ, 934, 70.
Imanishi, Y., Nawa, K., Tamura, Y., Ikeda, H.: 2022, Effects ofvertical nonlinearity on the superconducting gravimeter CT #036 at
Ishigakijima, Japan, Earth Planets Space, 74, 73.
Inami, H., et al. including Algera, H. S. B., Fudamoto, Y.: 2022, The
ALMA REBELS Survey: dust continuum detections at z > 6.5,
MNRAS, 515, 3126–3143.
Inayoshi, K., Onoue, M., Sugahara, Y., Inoue, A. K., Ho, L. C.: 2022,
The Age of Discovery with the James Webb Space Telescope:
Excavating the Spectral Signatures of the First Massive Black Holes,
ApJL, 931, L25.
Inoue, S., Si, X. T., Okamoto, T., Nishigaki, M.: 2022, Classificationof cosmic structures for galaxies with deep learning: connecting
cosmological simulations with observations, MNRAS, 515, 4065–
4081.
Inoue, Y., Hasegawa, M., Hazumi, M., Takada, S., Tomaru, T.: 2023,
Development of an epoxy-based millimeter absorber with expanded
polystyrenes and carbon black for an astronomical telescope, Appl.
Opt., 62, 1419–1427.
Ishiguro, M., Chiba, K., Sakamoto, S.: 2022, From Nobeyama Radio

Observatory to the international project ALMA -Evolution of
millimeter and submillimeter wave astronomy in Japan-, Proc. Jpn.
Acad. Ser. B, Physical Biol. Sci., 98, 439–469.
Ishikawa, R., et al. including Okamoto, T. J., Song, D. G.: 2023,
Evidence for the Operation of the Hanle and Magneto-optical Effects
in the Scattering Polarization Signals Observed by CLASP2 acrossthe Mg II h and k Lines, ApJ, 945, 125.
Ishimoto, R., Kashikawa, N., Kashino, D., Ito, K., Liang, Y. M., Cai,Z., Yoshioka, T., Okoshi, K., Misawa, T., Onoue, M., Takeda, Y.,
Uchiyama, H.: 2022, The physical origin for spatially large scatter of
IGM opacity at the end of reionization: The IGM Lyα opacity-galaxy
density relation, MNRAS, 515, 5914–5926.
Issaoun, S., et al. including Akiyama, K., Hada, K., Honma, M., Ikeda,
S., Kino, M., Kofuji, Y., Nagai, H., Okino, H., Oyama, T., Sasada,M., Tazaki, F.: 2022, Resolving the Inner Parsec of the Blazar J19242914 with the Event Horizon Telescope, ApJ, 934, 145.
Ita, Y., Ichikawa, T., Tsutsui, H., Hanaue, T., Komiyama, T., Onozato,
H., Iwamatsu, A., Morita, R., Habasaki, Y., Amemiya, R., Hanawa,
M., Yanagisawa, K., Izumiura, H., Nakada, Y.: 2022, The Thirty
Millimeter Telescope, PASJ, 74, 578–593.
Ito, K., Tanaka, M., Miyaji, T., Ilbert, O., Kauffmann, O. B.,
Koekemoer, A. M., Marchesi, S., Shuntov, M., Toft, S., Valentino,F., Weaver, J. R.: 2022, COSMOS2020: Ubiquitous AGN Activityof Massive Quiescent Galaxies at 0 < z < 5 Revealed by X-Ray andRadio Stacking, ApJ, 929, 53.
Ito, K., Tanaka, M., Valentino, F., Toft, S., Brammer, G., Gould, K. M. L.,
Ilbert, O., Kashikawa, N., Kubo, M., Liang, Y. M., McCracken, H. J.,
Weaver, J. R.: 2023, COSMOS2020: Discovery of a Protocluster ofMassive Quiescent Galaxies at z=2.77, ApJL, 945, L9.
Ito, M., et al, including Matsumoto, K., Namiki, N., Noda, H.: 2022, A
pristine record of outer Solar System materials from asteroid Ryugu's
returned sample, Nat. Astron, 6, 1163–1171.
Iwakami, W., Harada, A., Nagakura, H., Akaho, R., Okawa, H.,
Furusawa, S., Matsufuru, H., Sumiyoshi, K., Yamada, S.: 2022,
Principal-axis Analysis of the Eddington Tensor for the Early Postbounce Phase of Rotational Core-collapse Supernovae, ApJ, 933, 91.
Iwasaki, K., Tomida, K.: 2022, Universal Properties of Dense Clumps inMagnetized Molecular Clouds Formed through Shock Compressionof Two-phase Atomic Gases, ApJ, 934, 174.
Izumi, N., Kobayashi, N., Yasui, C., Saito, M., Hamano, S., Koch, P. M.:
2022, Star Formation Activity beyond the Outer Arm. II. Distribution
and Properties of Star Formation, ApJ, 936, 181.
James, B. L., et al. including Sugahara, Y., CLASSY Team: 2022,
CLASSY. II. A Technical Overview of the COS Legacy Archive
Spectroscopic Survey*, ApJS, 262, 37.
Jang, H. E., Lee, Y S., Aoki, W., Matsuno, T., Kang, W. S., Lee, H. G.,
Chun, S. H., Jeong, M., Yoon, S. C.: 2023, GRACES Observations of
Mg-Enhanced Metal-Poor Stars in the Milky Way, J. Korean Astron.
Soc., 56, 11–22.
Jhan, K. S., et al. including Tatematsu, K., Sanhueza, P., ALMASOP
Team: 2022, ALMA Survey of Orion Planck Galactic Cold Clumps(ALMASOP): Deriving Inclination Angle and Velocity of theProtostellar Jets from Their SiO Knots, ApJL, 931, L5.
Jiang, J. A., et al. including Tominaga, N., Moriya, T. J., Tanaka, M.,
Furusawa, H., Miyazaki, S.: 2022, MUSSES2020J: The Earliest
Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063,

XIII Publications, Presentations

149

ApJL, 933, L36.
Johns, L., Nagakura, H.: 2022, Self-consistency in models of neutrino
scattering and fast flavor conversion, Phys. Rev. D, 106, 043031.
Jones, G. C., Maiolino, R., Circosta, C., Scholtz, J., Carniani, S.,
Fudamoto, Y.: 2023, Evidence for extended gaseous reservoirs
around AGN at cosmic noon from ALMA CO(3–2) observations,
MNRAS, 518, 691–708.
Jung, P., Kim, Y.-M., Oh, S. H., Son, E. J., Yokozawa, T., Washimi,T., Oh, J. J.: 2022, Identifying multichannel coherent couplings andcausal relationships in gravitational wave detectors, Phys. Rev. D,
106, 042010.
Kalinova, V., Colombo, D., Sanchez, S. F., Rosolowsky, E., Kodaira,K., Garcia-Benito, R., Meidt, S. E., Davis, T. A., Romeo, A. B., Yu,
S. Y., Delgado, R. G., Lacerda, E. A. D.: 2022, Investigating the link
between inner gravitational potential and star-formation quenching in
CALIFA galaxies, A&A, 665, A90.
Kameno, S., Sawada-Satoh, S., Impellizzeri, C. M. V., Kohno, K., Martin,S., Espada, D., Nakai, N., Sugai, H., Terashima, Y., Lee, M. M.,
Kawakatu, N.: 2023, Probing the Jet-Torus Interaction in the Radio
Galaxy NGC 1052 by Sulfur-bearing Molecules, ApJ, 944, 156.
Kaneko, H., Kuno, N., Iono, D., Tamura, Y., Tosaki, T., Nakanishi, K.,
Sawada, T.: 2022, Properties of molecular gas in galaxies in earlyand mid stages of Interaction. III. Resolved Kennicutt-Schmidt law,
PASJ, 74, 343–363.
Kaneko, M., Oka, T., Yokozuka, H., Enokiya, R., Takekawa, S., Iwata, Y.,
Tsujimoto, S.: 2023, Discovery of the Tadpole Molecular Cloud near
the Galactic Nucleus, ApJ, 942, 46.
Kartaltepe, J. S., et al. including Behroozi, P., Zavala, J. A.: 2023,
CEERS Key Paper. III. The Diversity of Galaxy Structure andMorphology at z = 3–9 with JWST, ApJL, 946, L15.
Kasagi, Y., Kotani, T., Kawahara, H., Tajin, T., Muto, T., Aizawa,
M., Fujii, M. S., Hattori, K., Masuda, K., Momose, M., Ohsawa,R., Takita, S.: 2022, Dippers from TESS Full-frame Images. II.
Spectroscopic Characterization of Four Young Dippers, ApJS, 259, 40.
Kasuga, T., Masiero, J. R.: 2022, WISE/NEOWISE Multiepoch Imagingof the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005
UD, and 1999 YC, AJ, 164, 193.
Kato, C., Nagakura, H.: 2022, Effects of energy-dependent scatterings
on fast neutrino flavor conversions, Phys. Rev. D, 106, 123013.
Kawabata, Y., et al. including Katsukawa, Y., Kubo, M., Shinoda, K.,
Tsuzuki, T., Uraguchi, F., Oba, T.: 2022, Polarimetric calibrationof a spectropolarimeter instrument with high precision: Sunrise
chromospheric infrared spectropolarimeter (SCIP) for the SUNRISE
III balloon telescope, Appl. Opt., 61, 9716–9736.
Kawamuro, T., et al. including Imanishi, M., Izumi, T.: 2022, BASSXXXII: Studying the Nuclear Millimeter-wave Continuum Emissionof AGNs with ALMA at Scales <~ 100–200 pc, ApJ, 938, 87.
Kawana, Y., Saito, T., Okumura, S. K., Kawabe, R., Espada, D., Iono, D.,
Kaneko, H., Lee, M. M., Michiyama, T., Motohara, K., Nakanishi,K., Pettitt, A. R., Randriamanakoto, Z., Ueda, J., Yamashita, T.: 2022,
Multiwavelength and Multi-CO View of the Minor Merger Driven
Star Formation in the Nearby LIRG NGC 3110, ApJ, 929, 100.
Kawauchi, K., et al. including Livingston, J. H., Hori, Y., Ikoma, M.,
Kotani, T., Kusakabe, N., Nishikawa, J., Omiya, M., Serizawa, T.,
Tamura, M., Ueda, A., Harakawa, H., Kudo, T., Vievard, S.: 2022,
Validation and atmospheric exploration of the sub-Neptune TOI-

150

XIII Publications, Presentations

2136b around a nearby M3 dwarf, A&A, 666, A4.
Keszthelyi, Z., et al.: 2022, The effects of surface fossil magnetic fields
on massive star evolution: IV. Grids of models at Solar, LMC, and
SMC metallicities, MNRAS, 517, 2028–2055.
Kikuchi, S., et al. including Matsumoto, K., Namiki, N.: 2022, Siteselection for the Hayabusa2 artificial cratering and subsurface
material sampling on Ryug, Planet. Space Sci., 219, 105519.
Kikuchihara, S., et al. including Ouchi, M., Sugahara, Y.: 2022,
SILVERRUSH. XII. Intensity Mapping for Lyα Emission Extending
over 100–1000 Comoving Kpc around z ~ 2–7 LAEs with Subaru
HSC-SSP and CHORUS Data, ApJ, 931, 97.
Kim, C. G., Kim, J. G., Gong, M., Ostriker, E. C.: 2023, Introducing
TIGRESS-NCR. I. Coregulation of the Multiphase Interstellar
Medium and Star Formation Rates, ApJ, 946, 3.
Kim, D.-C., Kim, M., Yoon, I., Momjian, E., Kim, J. H., Letai, J., Evans,
A. S.: 2022, Adaptive optics and VLBA imaging observations ofrecoiling supermassive black hole candidates, MNRAS, 517, 4081–
4091.
Kim, J., et al. including Saito, T.: 2022, Environmental dependence ofthe molecular cloud lifecycle in 54 main-sequence galaxies, MNRAS,
516, 3006–3028.
Kim, J., et al. including Saito, T.: 2023, PHANGS-JWST First Results:
Duration of the Early Phase of Massive Star Formation in NGC 628,
ApJL, 944, L20.
Kim, J.-G., Gong, M., Kim, C.-G., Ostriker, E. C.: 2023, Photochemistryand Heating/Cooling of the Multiphase Interstellar Medium with UVRadiative Transfer for Magnetohydrodynamic Simulations, ApJS,
264, 10.
Kimura, S. S., Toma, K., Noda, H., Hada, K.: 2022, Magnetic
Reconnection in Black Hole Magnetospheres: Lepton Loading into
Jets, Superluminal Radio Blobs, and Multiwavelength Flares, ApJL,
937, L34.
Kimura, T., Fujii, Y., Kita, H., Tsuchiya, F., Sagawa, H., SKA-Japan
Planetary Sci Team: 2023, Revealing the dynamics of magnetosphere,
atmosphere, and interior of solar system objects with the Square
Kilometre Array, PASJ, 75, S196–S216.
Kimura, T., Ikoma, M.: 2022, Predicted diversity in water content ofterrestrial exoplanets orbiting M dwarfs, Nat. Astron, 6, 1296–1307.
Kino, M., et al. including Hada, K.: 2022, Implications from the
Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating
Black Hole Magnetosphere, ApJ, 939, 83.
Kinoshita, S.-W., Nakamura, F.: 2022, MHD Simulations of Dense Core
Collision, ApJ, 937, 69.
Kiuchi, H.: 2022, Bidirectional Optical Carrier Frequency Commonality
Method for Optical Fiber Delay Measurement, IEEE Photonics
Technol. Lett., 34, 887–890.
Klein, M., et al. including Miyazaki, S.: 2022, The eROSITA Final
Equatorial-Depth Survey (eFEDS) Optical confirmation, redshifts,
and properties of the cluster and group catalog, A&A, 661, A4.
Knudstrup, E., et al. including Hirano, T., Livingston, J. H.: 2023, A
puffy polar planet The low density, hot Jupiter TOI-640 b is on apolar orbit, A&A, 671, A164.
Knudstrup, E., et al. including Livingston, J., Hirano, T.: 2023, Radial
velocity confirmation of a hot super-Neptune discovered by TESS
with a warm Saturn-mass companion, MNRAS, 519, 5637–5655.
Ko, H., et al. including Cheoun, M.-K., Kusakabe, M., Sasaki, H.,

Kawano, T., Mathews, G. J.: 2022, Comprehensive Analysis of the
Neutrino Process in Core-collapsing Supernovae, ApJ, 937, 116.
Kobak, A., et al. including Hirota, T., Sobolev, A., Burns, R. A.: 2023,
Multi-frequency VLBI observations of maser lines during the 6.7
GHz maser flare in the high-mass young stellar object G24.33+0.14 ,A&A, 671, A135.
Kobayashi, M. I. N., Inoue, T., Tomida, K., Iwasaki, K., Nakatsugawa,H.: 2022, Nature of Supersonic Turbulence and Density Distribution
Function in the Multiphase Interstellar Medium, ApJ, 930, 76.
Kocevski, D. D., et al. including Zavala, J. A.: 2023, CEERS Key Paper.
II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5with JWST, ApJL, 946, L14.
Koda, J., et al. including Yagi, M., Komiyama, Y.: 2022, First Detectionof the Molecular Cloud Population in the Extended Ultraviolet Diskof M83, ApJ, 941, 3.
Kohno, M., Omodaka, T., Handa, T., Chibueze, J. O., Nagayama, T.,
Burns, R. A., Murase, T., Matsusaka, R., Nakano, M., Sunada, K.,
Yamada, R. I., Bieging, J. H.: 2022, Ammonia mapping observations
toward the Galactic massive star-forming region Sh 2-255 and Sh
2-257, PASJ, 74, 545–556.
Kojima, T., Masui, S., Shan, W., Uzawa, Y.: 2023, Characterization of a
low-noise superconductor-insulator-superconductor-based microwave
amplifier with local oscillator phase-adjusting architecture, Appl.
Phys. Lett., 122, 072601.
Kokorev, V., et al. including Ouchi, M.: 2022, ALMA Lensing Cluster
Survey: Hubble Space Telescope and Spitzer Photometry of 33
Lensed Fields Built with CHArGE, ApJS, 263, 38.
Komatsu, Y., Hori, Y., Kuzuhara, M., Kosugi, M., Takizawa, K.,
Narita, N., Omiya, M., Kim, E., Kusakabe, N., Meadows, V.,
Tamura, M.: 2023, Photosynthetic Fluorescence from Earthlike
Planets around Sunlike and Cool Stars, ApJ, 942, 57.
Komatsu, Y., Suzuki, T.: 2022, Quantum Chemical Study on Interstellar
Synthesis of Cytosine by the Automated Reaction Path Search, ACS
Earth Space Chem., 6, 2491–2498.
Komugi, S., Toba, Y., Matsuoka, Y., Saito, T., Yamashita, T.: 2022,
Detection of Extended Millimeter Emission in the Host Galaxy of 3C
273 and Its Implications for QSO Feedback via High Dynamic Range
ALMA Imaging, ApJ, 930, 3.
Konishi, R., Enokiya, R., Fukui, Y., Muraoka, K., Tokuda, K., Onishi, T.:
2022, Discovery of a Giant Molecular Loop in the Central Region of
NGC 253, ApJ, 929, 63.
Konyves, V., Ward-Thompson, D., Shimajiri, Y., Palmeirim, P., Andre, P.:
2023, A low-mass hub-filament with double centre revealed in NGC
2071-North, MNRAS, 520, 4646–4663.
Koshiba, Y., Uchida, H., Tanaka, T., Amano, Y., Sano, H., Tsuru, T. G.:
2022, High-resolution X-ray study of supernova remnant J0453.66829 with unusually high forbidden-to-resonance ratio, PASJ, 74,
757–766.
Kosugi, M., Kawasaki, M., Shibata, Y., Hara, K., Takaichi, S., Moriya,T., Adachi, N., Kamei, Y., Kashino, Y., Kudoh, S., Koike, H., Senda,
T.: 2023, Uphill energy transfer mechanism for photosynthesis in an
Antarctic alga, Nat. Commun., 14, 730.
Kowalski, A. F., Allred, J. C., Carlsson, M., Kerr, G. S., Tremblay, P. E.,
Namekata, K., Kuridze, D., Uitenbroek, H.: 2022, The Atmospheric
Response to High Nonthermal Electron-beam Fluxes in Solar Flares.
II. Hydrogen-broadening Predictions for Solar Flare Observations

with the Daniel K. Inouye Solar Telescope, ApJ, 928, 190.
Kronrod, E., Matsumoto, K., Kuskov, O. L., Kronrod, V., Yamada, R.,
Kamata, S.: 2022, Towards geochemical alternatives to geophysicalmodels of the internal structure of the lunar mantle and core, Adv.
Space Res., 69, 2798–2824.
Kubo, M., Umehata, H., Matsuda, Y., Kajisawa, M., Steidel, C. C.,
Yamada, T., Tanaka, I., Hatsukade, B., Tamura, Y., Nakanishi, K.,
Kohno, K., Lee, K., Matsuda, K., Ao, Y. P., Nagao, T., Yun, M. S.:
2022, An AGN with an Ionized Gas Outflow in a Massive Quiescent
Galaxy in a Protocluster at z=3.09, ApJ, 935, 89.
Kurahara, K., Akahori, T., Kale, R., Akamatsu, H., Fujita, Y., Gu, L.
Y., Intema, H., Nakazawa, K., Okabe, N., Omiya, Y., Parekh, V.,
Shimwell, T., Takizawa, M., Van Weeren, R. J.: 2023, Diffuse radiosource candidate in CIZA J1358.9-4750, PASJ, 75, S138–S153.
Kurokawa, H., Laneuville, M., Li, Y., Zhang, N., Fujii, Y., Sakuraba,
H., Houser, C., Cleaves, H. J.: 2022, The Origin of Earth's Mantle
Nitrogen: Primordial or Early Biogeochemical Cycling?, Geochem.
Geophys. Geosyst., 23, e2021GC010295.
Kuwata, A., Kawahara, H., Aizawa, M., Kotani, T., Tamura, M.: 2022,
Global Mapping of Surface Composition on an Exo-Earth Using
Sparse Modeling, ApJ, 930, 162.
Kuzuhara, M., et al. including Currie, T., Takarada, T., Hori, Y.,
Guyon, O., Lozi, J., Vievard, S., Sahoo, A., Deo, V., Ahn, K., Skaf,
N., Kudo, T., Nishikawa, J., Hayashi, M., Tamura, M.: 2022, Directimaging Discovery and Dynamical Mass of a Substellar Companion
Orbiting an Accelerating Hyades Sun-like Star with SCExAO/CHARIS, ApJL, 934, L19.
Lammer, H., Scherf, M., Ito, Y., Mura, A., Vorburger, A., Guenther,E., Wurz, P., Erkaev, N. V., Odert, P.: 2022, The Exosphere as a
Boundary: Origin and Evolution of Airless Bodies in the Inner Solar
System and Beyond Including Planets with Silicate Atmospheres,Space Sci. Rev., 218, 15.
Law, C. J., et al. including Tsukagoshi, T.: 2022, CO Line Emission
Surfaces and Vertical Structure in Midinclination Protoplanetary
Disks, ApJ, 932, 114.
Law, C.-Y., et al. including Tanaka, K. E. I.: 2022, Isolated Massive
Star Formation in G28.20-0.05, ApJ, 939, 120.
Lawson, K., Currie, T., Wisniewski, J. P., Groff, T. D., McElwain, M.
W., Schlieder, J. E.: 2022, Constrained Reference Star Differential
Imaging: Enabling High-fidelity Imagery of Highly Structured
Circumstellar Disks *, ApJL, 935, L25.
Le Gouellec, V. J. M., Maury, A. J., Hull, C. L. H.: 2023, Physicalconditions for dust grain alignment in Class 0 protostellar cores I.
Observations of dust polarization and molecular irradiation tracers,
A&A, 671, A167.
Lee, B., et al. including Michiyama, T.: 2022, ALMA/ACA CO Surveyof the IC 1459 and NGC 4636 Groups: Environmental Effects on the
Molecular Gas of Group Galaxies, ApJS, 262, 31.
Lee, J. C., et al. including Saito, T.: 2023, The PHANGS-JWST Treasury
Survey: Star Formation, Feedback, and Dust Physics at High Angular
Resolution in Nearby GalaxieS, ApJL, 944, L17.
Lee, K., Kohno, K., Hatsukade, B., Egusa, F., Yamashita, T., Schramm,M., Ichikawa, K., Imanishi, M., Izumi, T., Nagao, T., Toba, Y.,
Umehata, H.: 2023, Massive Molecular Gas Companions Uncovered
by Very Large Array CO(1–0) Observations of the z=5.2 Radio
Galaxy TN J0924-2201, ApJ, 944, 35.

XIII Publications, Presentations

151

Lenart, A. L., Bargiacchi, G., Dainotti, M. G., Nagataki, S., Capozziello,S.: 2023, A Bias-free Cosmological Analysis with Quasars Alleviating
H0 Tension, ApJS, 264, 46.
Leroy, A. K., et al. including Saito, T.: 2023, PHANGS–JWST First
Results: A Global and Moderately Resolved View of Mid-infrared
and CO Line Emission from Galaxies at the Start of the JWST Era,
ApJL, 944, L10.
Leroy, A. K., et al. including Saito, T.: 2023, PHANGS-JWST First
Results: Mid-infrared Emission Traces Both Gas Column Density andHeating at 100 pc Scales, ApJL, 944, L9.
Levine, D., Dainotti, M., Fraija, N., Warren, D., Chandra, P., LloydRonning, N.: 2023, Interpretation of radio afterglows in theframework of the standard fireball and energy injection models ,MNRAS, 519, 4670–4683.
Li, H. N., Aoki, W., Matsuno, T., Xing, Q. F., Suda, T., Tominaga,N., Chen, Y. Q., Honda, S., Ishigaki, M. N., Shi, J. R., Zhao, J. K.,
Zhao, G.: 2022, Four-hundred Very Metal-poor Stars Studied withLAMOST and Subaru. II. Elemental Abundances, ApJ, 931, 147.
Li, H., Aleman, T. D., Bueno, J. T., Ishikawa, R., Ballester, E. A.,
McKenzie, D. E., Auchere, F., Kobayashi, K., Okamoto, T. J.,
Rachmeler, L. A., Song, D.: 2023, Tomography of a Solar Plage with
the Tenerife Inversion Code, ApJ, 945, 144.
Li, J. Y., Silverman, J. D., Izumi, T., He, W. Q., Akiyama, M., Inayoshi,K., Matsuoka, Y., Onoue, M., Toba, Y.: 2022, On the Connection
between Supermassive Black Holes and Galaxy Growth in theReionization Epoch, ApJL, 931, L11.
Li, S., et al. including Sanhueza, P., Morii, K., Tatematsu, K., Silva, A.:
2022, The ALMA Survey of 70 μm Dark High-mass Clumps in Early
Stages (ASHES). VII. Chemistry of Embedded Dense Cores, ApJ,
939, 102.
Li, X. C., Miyatake, H., Luo, W. T., More, S., Oguri, M., Hamana,T., Mandelbaum, R., Shirasaki, M., Takada, M., Armstrong, R.,
Kannawadi, A., Takita, S., Miyazaki, S., Nishizawa, A. J., Malagon,
A. A. P., Strauss, M. A., Tanaka, M., Yoshida, N.: 2022, The threeyear shear catalog of the Subaru Hyper Suprime-Cam SSP Survey,
PASJ, 74, 421–459.
Li, Z. H., Steidel, C. C., Gronke, M., Chen, Y. G., Matsuda, Y.: 2022,
Where outflows meet inflows: gas kinematics in SSA22 Lyα blob2 decoded by advanced radiative transfer modelling, MNRAS, 513,
3414–3428.
Lin, Z. Y. D., et al. including Hull, C. L. H.: 2023, (Sub)millimetre
dust polarization of protoplanetary discs from scattering by large
millimetre-sized irregular grains, MNRAS, 520, 1210–1223.
Liu, D. Z., et al. including Saito, T.: 2023, PHANGS-JWST First
Results: Stellar-feedback-driven Excitation and Dissociation of
Molecular Gas in the Starburst Ring of NGC 1365?, ApJL, 944, L19.
Liu, D. Z., et al. including Tadaki, K. I.: 2023, An ~ 600 pc View of theStrongly Lensed, Massive Main-sequence Galaxy J0901: A Baryondominated, Thick Turbulent Rotating Disk with a Clumpy Cold Gas
Ring at z=2.259, ApJ, 942, 98.
Liu, L., et al. including Iguchi, S.: 2022, WISDOM Project - XII. Clump
properties and turbulence regulated by clump-clump collisions in thedwarf galaxy NGC 404, MNRAS, 517, 632–656.
Liu, X., et al. including Cheng, Y., Tatematsu, K.: 2022, A Q-band Line
Survey toward Orion KL Using the Tianma Radio Telescope, ApJS,
263, 13.

152

XIII Publications, Presentations

Liu, X., et al. including Cheng, Y., Tatematsu, K.: 2023, First detectionof radio recombination lines of ions heavier than helium, A&A, 671,
L1.
Longobardo, A., et al. including Matsumoto, K.: 2022, Photometricbehavior of Ryugu's NIR spectral parameters, A&A, 666, A185.
Lu, T.-Y., et al. inclduing Toba, Y., SHELLQs Collaboration: 2022,
Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs)- XV. Constraining the cosmic reionization at 5.5 < z < 7, MNRAS,
517, 1264–1281.
Lu, X., Li, G. X., Zhang, Q. Z., Lin, Y. X.: 2022, A massive Keplerian
protostellar disk with flyby-induced spirals in the Central MolecularZone, Nat. Astron, 6, 837–843.
Lu, Y. T., Benomar, O., Kamiaka, S., Suto, Y.: 2022, Meta-analysis of
Photometric and Asteroseismic Measurements of Stellar Rotation
Periods: The Lomb-Scargle Periodogram, Autocorrelation Function,and Wavelet and Rotational Splitting Analysis for 92 Kepler
Asteroseismic Targets, ApJ, 941, 175.
Luo, Q. Y., et al. including Tatematsu, K., Sanhueza, P.: 2022, ALMA
Survey of Orion Planck Galactic Cold Clumps (ALMASOP): How
Do Dense Core Properties Affect the Multiplicity of Protostars?, ApJ,
931, 158.
Luque, R., et al. including Kotani, T., Kudo, T., Kuzuhara, M.,
Livingston, J., Tamura, M.: 2022, Precise mass determination for
the keystone sub-Neptune planet transiting the mid-type M dwarf G
9-40, A&A, 666, A154.
Lustig, P., et al. including Onodera, M.: 2023, Massive quiescentgalaxies at z ~ 3: A comparison of selection, stellar population, andstructural properties with simulation predictions, MNRAS, 518, 5953–
5975.
Lykawka, P. S., Ito, T.: 2023, Terrestrial planet and asteroid belt
formation by Jupiter–Saturn chaotic excitation, Sci. Rep., 13, 4708.
Maas, A. J., et al. including Narita, N.: 2022, Lower-than-expected flare
temperatures for TRAPPIST-1, A&A, 668, A111.
MacLeod, G. C., Yonekura, Y., Tanabe, Y., Baan, W. A., Brogan, C. L.,
Burns, R. A., Chibueze, J. O., Houde, M., Hunter, T. R., Kurtz, S.
E., Rajabi, F., Smits, D. P., Stecklum, B., Sugiyama, K.: 2022, Two
periods instead of one in a single 6.7 GHz methanol maser feature in
G9.62+0.20E, MNRAS Lett., 516, L96–L100.
Maeda, K., et al. including Moriya, T. J., Michiyama, T.: 2023, A
Multiwavelength View of the Rapidly Evolving SN 2018ivc: An
Analog of SN IIb 1993J but Powered Primarily by Circumstellar
Interaction, ApJ, 942, 17.
Maeda, K., Michiyama, T., Chandra, P., Ryder, S., Kuncarayakti,
H., Hiramatsu, D., Imanishi, M.: 2023, Resurrection of Type IIL
Supernova 2018ivc: Implications for a Binary Evolution Sequence
Connecting Hydrogen-rich and Hydrogen-poor Progenitors, ApJL,
945, L3.
Maguire, C., Gibson, N. P., Nugroho, S. K., Ramkumar, S., Fortune,M., Merritt, S. R., de Mooij, E.: 2023, High-resolution atmosphericretrievals of WASP-121b transmission spectroscopy with ESPRESSO:
Consistent relative abundance constraints across multiple epochs andinstruments, MNRAS, 519, 1030–1048.
Maity, A. K., Dewangan, L. K., Sano, H., Tachihara, K., Fukui, Y.,
Bhadari, N. K.: 2022, Unraveling the Observational Signatures of
Cloud-Cloud Collision and Hub-filament Systems in W31, ApJ, 934, 2.
Malhotra, R., Ito, T.: 2022, Pluto near the edge of chaos, Proc. Natl.

Acad. Sci. U.S.A., 119, e2118692119.
Marino, S., Cataldi, G., Jankovic, M. R., Matra, L., Wyatt, M. C.: 2022,
Vertical evolution of exocometary gas - I. How vertical diffusion
shortens the CO lifetime, MNRAS, 515, 507–524.
Masui, S., Hasegawa, Y., Ogawa, H., Kojima, T., Onishi, T.: 2022, 210–365 GHz 90 degrees Differential Phase Shifter for Wideband Circular
Polarizer, IEEE Trans. Terahertz Sci. Technol., 12, 527–534.
Matsukoba, R., Tanaka, K. E. I., Omukai, K., Vorobyov, E. I., Hosokawa,T.: 2022, Protostellar-disc fragmentation across all metallicities,MNRAS, 515, 5506–5522.
Matsumoto, A., et al. including Masami O., Nakajima, K., Motohara,
K., Sugahara, Y., Onodera, M., Moriya, T., Komiyama, Y.,
Fujimoto, S., Hattori, T., Koyama, Y., Lee, C.-H., Mawatari, K.,
Ozaki, S., Suzuki, A.: 2022, EMPRESS. VIII. A New Determinationof Primordial He Abundance with Extremely Metal-poor Galaxies: A
Suggestion of the Lepton Asymmetry and Implications for the Hubble
Tension, ApJ, 941, 167.
Matsumoto, J., Asahina, Y., Takiwaki, T., Kotake, K., Takahashi, H. R.:
2022, Magnetic support for neutrino-driven explosion of 3D nonrotating core-collapse supernova models, MNRAS, 516, 1752–1767.
Matsumoto, K., Nakagawa, T., Wada, K., Baba, S., Onishi, S., Uzuo,
T., Isobe, N., Kudoh, Y.: 2022, Probing Dynamics and Thermal
Properties Inside Molecular Tori with CO Rovibrational Absorption
Lines, ApJ, 934, 25.
Matsuno, T., Dodd, E., Koppelman, H. H., Helmi, A., Ishigaki, M. N.,
Aoki, W., Zhao, J. K., Yuan, Z., Hattori, K.: 2022, High-precisionchemical abundances of Galactic building blocks II. Revisiting thechemical distinctness of the Helmi streams, A&A, 665, A46.
Matsuno, T., Koppelman, H. H., Helmi, A., Aoki, W., Ishigaki, M.
N., Suda, T., Yuan, Z., Hattori, K.: 2022, High-precision chemical
abundances of Galactic building blocks. The distinct chemical
abundance sequence of Sequoia, A&A, 661, A103.
Matsuoka, T., Lee, S. H., Maeda, K., Takiwaki, T., Moriya, T. J.: 2022,
Long-term Evolution of a Supernova Remnant Hosting a Double
Neutron Star Binary, ApJ, 930, 143.
Meidt, S. E., et al. including Saito, T.: 2023, PHANGS-JWST First
Results: Interstellar Medium Structure on the Turbulent Jeans Scalein Four Disk Galaxies Observed by JWST and the Atacama Large
Millimeter/submillimeter Array, ApJL, 944, L18.
Michiyama, T., Inoue, Y., Doi, A., Khangulyan, D.: 2022, ALMA
Detection of Parsec-scale Blobs at the Head of a Kiloparsec-scale Jet
in the Nearby Seyfert Galaxy NGC 1068, ApJL, 936, L1.
Middei, R., et al. including Kameno, S., Nagai, H.: 2023, X-Ray
Polarization Observations of BL Lacertae, ApJL, 942, L10.
Miles, B. E., et al. including Currie, T.: 2023, The JWST Early-release
Science Program for Direct Observations of Exoplanetary Systems
II: A 1 to 20 μm Spectrum of the Planetary-mass Companion VHS
1256–1257 b, ApJL, 946, L6.
Mingozzi, M., et al. including Sugahara, Y.: 2022, CLASSY IV.
Exploring UV Diagnostics of the Interstellar Medium in Local High-z
Analogs at the Dawn of the JWST Era, ApJ, 939, 110.
Minhee., H., et al. including Matsuda, Y.: 2023, The JCMT SCUBA-2
Survey of the James Webb Space Telescope North Ecliptic Pole
Time-Domain Field, ApJS, 264, 19.
Minoda, T., Saga, S., Takahashi, T., Tashiro, H., Yamauchi, D.,
Yokoyama, S., Yoshiura, S.: 2023, Probing the primordial Universe

with 21 cm line from cosmic dawn/epoch of reionization, PASJ, 75,
S154–S180.
Minoda, T., Yoshiura, S., Takahashi, T.: 2022, Probing isocurvature
perturbations with 21-cm global signal in the light of HERA result,
Phys. Rev. D, 105, 083523.
Misugi, Y., Inutsuka, S., Arzoumanian, D.: 2023, Evolution of theAngular Momentum of Molecular Cloud Cores Formed from
Filament Fragmentation, ApJ, 943, 76.
Miyakawa, K., Hirano, T., Sato, B., Okuzumi, S., Gaidos, E.: 2022,
Color Dependence of the Transit Detectability of Young Active M
Dwarfs, AJ, 164, 209.
Miyatake, H., et al. including Shirasaki, M., Komiyama, Y., Miyazaki,S., Tanaka, M.: 2022, Cosmological inference from an emulator
based halo model. II. Joint analysis of galaxy-galaxy weak lensing
and galaxy clustering from HSC-Y1 and SDSS, Phys. Rev. D, 106,083520.
Miyatake, H., et al. including Shirasaki, M.: 2022, Cosmologicalinference from an emulator based halo model. I. Validation tests with
HSC and SDSS mock catalogs, Phys. Rev. D, 106, 083519.
Miyatake, H., Harikane, Y., Ouchi, M., Ono, Y., Yamamoto, N.,
Nishizawa, A. J., Bahcall, N., Miyazaki, S., Malagon, A. A. P.: 2022,
First Identification of a CMB Lensing Signal Produced by 1.5 Million
Galaxies at z ~ 4: Constraints on Matter Density Fluctuations at HighRedshift, Phys. Rev. Lett., 129, 061301.
Miyawaki, R., Hayashi, M., Hasegawa, T.: 2022, W49 N MCN-a: A
disk-accreting massive protostar embedded in an early-phase hotmolecular core, PASJ, 74, 705–737.
Miyawaki, R., Hayashi, M., Hasegawa, T.: 2023, An expanding ring of
the hypercompact H II region W 49 N:A2, PASJ, 75, 225–232.
Miyoshi, M., Kato, Y., Makino, J.: 2022, The Jet and Resolved Featuresof the Central Supermassive Black Hole of M87 Observed with the
Event Horizon Telescope (EHT), ApJ, 933, 36.
Moor, A., et al. including Cataldi, G.: 2022, Mid-infrared time-domain
study of recent dust production events in the extreme debris disc of
TYC 4209-1322-1, MNRAS, 516, 5684–5701.
Mori, K., Moriya, T. J., Takiwaki, T., Kotake, K., Horiuchi, S.,
Blinnikov, S. I.: 2023, Light Curves and Event Rates of Axion
Instability Supernovae, ApJ, 943, 12.
Mori, M., et al. including Livingston, J. H., Hirano, T., Hori,
Y., Ishikawa, H. T., Kuzuhara, M., Ikoma, M., Kotani, T.,
Krishnamurthy, V., Kusakabe, N., Nishikawa, J., Omiya, M., Ueda,
A., Tamura, M.: 2022, TOI-1696: A Nearby M4 Dwarf with a 3R⊕
Planet in the Neptunian Desert, AJ, 163, 298.
Mori, S., Nishida, Y., Iyomoto, N., Yagi, Y., Konno, R., Hayashi, T.,
Tanaka, K., Yamasaki, N. Y., Mitsuda, K., Sato, R., Saito, M.,
Homma, T.: 2022, Simulation of TES X-ray Microcalorimeters
Designed for 14.4 keV Solar Axion Search, J. Low Temp. Phys., 209,
518–524.
Morishima, Y., Sudou, H., Yamauchi, A., Taniguchi, Y., Nakai, N.: 2023,
High-sensitivity VLBI observations of water masers in the Seyfert
galaxy NGC 1068, PASJ, 75, 71–81.
Moriya, T. J., et al., Euclid Consortium: 2022, Euclid: Searching forpair-instability supernovae with the Deep Survey, A&A, 666, A157.
Moriya, T. J., Murase, K., Kashiyama, K., Blinnikov, S. I.: 2022,
Variable thermal energy injection from magnetar spin-down as apossible cause of stripped-envelope supernova light-curve bumps,

XIII Publications, Presentations

153

MNRAS, 513, 6210–6218.
Moriya, T. J., Yoon, S. C.: 2022, Mass-loss of massive helium starsupernova progenitors shortly before explosion constrained bysupernova radio properties, MNRAS, 513, 5606–5610.
Morokuma-Matsui, K., et al. inclduing Koyama, Y., Nakanishi, K.,
Miura, R. E.: 2022, CO(J=1–0) Mapping Survey of 64 Galaxies in
the Fornax Cluster with the ALMA Morita Array, ApJS, 263, 40.
Motte, F., et al. including Nakamura, F., Sanhueza, P., Guzman, A.
E., Izumi, N., Lu, X., Tatematsu, K., Wu, B.: 2022, ALMA-IMF I.
Investigating the origin of stellar masses: Introduction to the Large
Program and first results, A&A, 662, A8.
Murata, K., Takeuchi, T. T.: 2022, Deblurring galaxy images with
Tikhonov regularization on magnitude domain, PASJ, 74, 1329–1343.
Murgas, F., et al. including Livingston, J.: 2022, HD 20329b: An ultrashort-period planet around a solar-type star found by TESS, A&A,
668, A158.
Nagai, M., et al. including Murayama, Y., Miyazawa, H., Noji, R.,
Kiuchi, H., Matsuo, H., Shan, W.: 2022, Configuration of Probe
Tones for MKID Readout with Frequency Sweeping Scheme, J. Low
Temp. Phys., 209, 677–685.
Nagakura, H., Zaizen, M.: 2022, Time-Dependent and QuasisteadyFeatures of Fast Neutrino-Flavor Conversion, Phys. Rev. Lett., 129,
261101.
Nagakura, H., Zaizen, M.: 2023, Connecting small-scale to large-scale
structures of fast neutrino-flavor conversion, Phys. Rev. D, 107,
063033.
Nagakura, H.: 2022, General-relativistic quantum-kinetics neutrinotransport, Phys. Rev. D, 106, 063011.
Nagasawa, S., Kawate, T., Narukage, N., Takahashi, T., Caspi, A.,
Woods, T. N.: 2022, Study of Time Evolution of Thermal andNonthermal Emission from an M-class Solar Flare, ApJ, 933, 173.
Naito, H., Tajitsu, A., Ribeiro, V. A. R. M., Arai, A., Maehara, H.,
Kouzuma, S., Iijima, T., Okazaki, A. T., Watanabe, M., Takagi, S.,
Watanabe, F., Sakon, I., Sadakane, K.: 2022, Morpho-kinematic
Modeling of the Expanding Ejecta of the Extremely Slow Nova
V1280 Scorpii, ApJ, 932, 39.
Nakajima, K., Maiolino, R.: 2022, Diagnostics for PopIII galaxies anddirect collapse black holes in the early universe, MNRAS, 513, 5134–
5147.
Nakajima, K., Ouchi, M., Xu, Y., Rauch, M., Harikane, Y., Nishigaki,
M., Isobe, Y., Kusakabe, H., Nagao, T., Ono, Y., Onodera, M.,
Sugahara, Y., Kim, J. H., Komiyama, Y., Lee, C. H., Zahedy, F.
S.: 2022, EMPRESS. V. Metallicity Diagnostics of Galaxies over
12+log(O/H) ≃ 6.9–8.9 Established by a Local Galaxy Census:
Preparing for JWST Spectroscopy, ApJS, 262, 3.
Nakajima, T.: 2023, Microscopic Quantum Jump: An Interpretation of
Measurement Problem, Int. J. Theor. Phys., 62, 67.
Nakamura, E., et al. including Matsumoto, K., Namiki, N., Noda,
H.: 2022, On the origin and evolution of the asteroid Ryugu: A
comprehensive geochemical perspective, Proc. Jpn. Acad. Ser. B,
Physical Biol. Sci., 98, 227–282.
Nakamura, K., Takiwaki, T., Kotake, K.: 2022, Three-dimensional
simulation of a core-collapse supernova for a binary star progenitorof SN 1987A, MNRAS, 514, 3941–3952.
Nakamura, T., et al. including Noda, H., Namiki, N., Matsumoto, K.,
Kikuchi, S.: 2023, Formation and evolution of carbonaceous asteroid

154

XIII Publications, Presentations

Ryugu: Direct evidence from returned samples, Science, 379, 787.
Nakayama, A., Ikoma, M., Terada, N.: 2022, Survival of Terrestrial N2O2 Atmospheres in Violent XUV Environments through Efficient
Atomic Line Radiative Cooling, ApJ, 937, 72.
Namekata, K., Ichimoto, K., Ishii, T. T., Shibata, K.: 2022, Sun-as-a-starAnalysis of Hα Spectra of a Solar Flare Observed by SMART/SDDI:
Time Evolution of Red Asymmetry and Line Broadening, ApJ, 933,
209.
Namekata, K., Toriumi, S., Airapetian, V. S., Shoda, M., Watanabe, K.,
Notsu, Y.: 2023, Reconstructing the XUV Spectra of Active Sun-likeStars Using Solar Scaling Relations with Magnetic Flux, ApJ, 945,
147.
Namizaki, K., Namekata, K., Maehara, H., Notsu, Y., Honda, S.,
Nogami, D., Shibata, K.: 2023, A Superflare on YZ Canis Minoris
Observed by the Seimei Telescope and TESS: Red Asymmetry of Ha
Emission Associated with White-light Emission, ApJ, 945, 61.
Naraoka, H., et al. including Namiki, N., Matsumoto, K., Noda, H.,
Hirata, N., Shirai, K., Kikuchi, S.: 2023, Soluble organic moleculesin samples of the carbonaceous asteroid (162173) Ryugu, Science,
379, 789.
Narendra, A., Gibson, S. J., Dainotti, M G., Bogdan, M., Pollo, A.,
Liodakis, I., Poliszczuk, A., Rinaldi, E.: 2022, Predicting the Redshiftof Gamma-Ray Loud AGNs Using Supervised Machine Learning. II,
ApJS, 259, 55.
Nashimoto, M., Tanaka, M., Chiba, M., Hayashi, K., Komiyama, Y.,
Okamoto, T.: 2022, The Missing Satellite Problem outside of the
Local Group. II. Statistical Properties of Satellites of Milky Way-like
Galaxies, ApJ, 936, 38.
Nguyen, T., Oba, Y., Sameera, W. M. C., Furuya, K., Kouchi, A.,
Watanabe, N.: 2023, Surface Reaction of Methyl Mercaptan (CH3SH)
with Hydrogen Atoms on Amorphous Solid Water, ApJ, 944, 219.
Niemeyer, M. L., et al. including Ouchi, M.: 2022, Surface Brightness
Profile of Lymanα Halos out to 320 kpc in HETDEX, ApJ, 929, 90.
Niino, Y., et al. including Jiang, J. A., Tominaga, N., Kasuga, T.: 2022,
Deep Simultaneous Limits on Optical Emission from FRB 20190520B
by 24.4 fps Observations with Tomo-e Gozen, ApJ, 931, 109.
Nindos, A., Patsourakos, S., Jafarzadeh, S., Shimojo, M.: 2022, The
dynamic chromosphere at millimeter wavelengths, Front. Astron.
Space Sci., 9, 981205.
Nishikawa, J.: 2022, The Coherent Differential Imaging on Speckle
Area Nulling (CDI-SAN) Method for High-contrast Imaging under
Speckle Variation, ApJ, 930, 163.
Nishiyama, G., Namiki, N., Sugita, S., Uno, S.: 2022, Utilization of ameteorological satellite as a space telescope: the lunar mid-infrared
spectrum as seen by Himawari-8, Earth Planets Space, 74, 105.
Nitta, S., Kondoh, K.: 2022, Effects of Magnetic Shear and
Thermodynamic Asymmetry on Spontaneous Magnetohydrodynamic
Reconnection, ApJ, 936, 125.
Noboriguchi, A., et al. including Toba, Y., Terao, K., Yamashita, T.:
2022, Extreme Nature of Four Blue-excess Dust-obscured Galaxies
Revealed by Optical Spectroscopy, ApJ, 941, 195.
Noda, H., Mineta, T., Minezaki, T., Sameshima, H., Kokubo, M.,
Kawamuro, T., Yamada, S., Horiuchi, T., Matsumoto, H., Watanabe, M.,
Morihana, K., Itoh, Y., Kawabata, K. S., Fukazawa, Y.: 2023, Narrow
Fe-Kα Reverberation Mapping Unveils the Deactivated Broad-line
Region in a Changing-look Active Galactic Nucleus, ApJ, 943, 63.

Noguchi, T., et al. including Matsumoto, K., Namiki, N., Noda, H.:
2023, A dehydrated space-weathered skin cloaking the hydrated
interior of Ryugu, Nat. Astron, 7, 170–181.
Notsu, S., Ohno, K., Ueda, T., Walsh, C., Eistrup, C., Nomura, H.:
2022, The Molecular Composition of Shadowed Proto-solar Disk
Midplanes Beyond the Water Snowline, ApJ, 936, 188.
Nousiainen, J., et al. including Guyon, O.: 2022, Toward on-sky
adaptive optics control using reinforcement learning Model-based
policy optimization for adaptive optics, A&A, 664, A71.
Oba, T., et al. including Katsukawa, Y., Kubo, M., Kawabata, Y.,
Hara, H., Uraguchi, F., Tsuzuki, T., Tamura, T., Shinoda, K.:
2022, Development of Fast and Precise Scan Mirror Mechanism foran Airborne Solar Telescope, Sol. Phys., 297, 114.
Ohkubo, M., Uehara, G., Beyer, J., Mimura, M., Tanaka, H., Ehara, K.,
Tanaka, S., Noguchi, T., Mitchell, E. E., Foley, C. P., Fagaly, R. L.:
2022, Standard measurement method for normal state resistance andcritical current of resistively shunted Josephson junctions, Supercond.
Sci. Technol., 35, 045002.
Ohno, K., Fortney, J. J.: 2023, Nitrogen as a Tracer of Giant Planet
Formation. I. A Universal Deep Adiabatic Profile and Semianalytical
Predictions of Disequilibrium Ammonia Abundances in Warm
Exoplanetary Atmospheres, ApJ, 946, 18.
Okawa, H., Fujisawa, K., Yamamoto, Y., Hirai, R., Yasutake, N.,
Nagakura, H., Yamada, S.: 2023, The W4 method: A new multidimensional root-finding scheme for nonlinear systems of equations,Appl. Numer. Math., 183, 157–172.
Okazaki, R., et al. including Kikuchi, S., Matsumoto, K., Namiki, N.,
Noda, H.: 2022, First asteroid gas sample delivered by the Hayabusa2
mission: A treasure box from Ryugu, Sci. Adv., 8, eabo7239.
Okazaki, R., et al. including Kikuchi, S., Matsumoto, K., Namiki, N.,
Noda, H.: 2023, Noble gases and nitrogen in samples of asteroid
Ryugu record its volatile sources and recent surface evolution,
Science, 379, 788.
Okino, H., et al. including Akiyama, K., Hada, K., Honma, M., Kino,
M., Nagai, H., Moriyama, K., Tazaki, F.: 2022, Collimation of theRelativistic Jet in the Quasar 3C 273, ApJ, 940, 65.
Okura, Y., Futamase, T.: 2022, New highly precise weak gravitational
lensing flexions measurement method based on ERA method,MNRAS, 516, 668–692.
Okuya, A., Ida, S., Hyodo, R., Okuzumi, S.: 2023, Modelling theevolution of silicate/volatile accretion discs around white dwarfs,
MNRAS, 519, 1657–1676.
Okuzumi, S., Ueda, T., Turner, N. J.: 2022, A global two-layer radiativetransfer model for axisymmetric, shadowed protoplanetary disks,
PASJ, 74, 828–850.
Olguin, F. A., Sanhueza, P., Ginsburg, A., Chen, H. R. V., Zhang, Q. Z.,
Li, S. H., Lu, X., Sakai, T.: 2022, Digging into the Interior of Hot
Cores with ALMA (DIHCA). II. Exploring the Inner Binary (Multiple)
System Embedded in G335 MM1 ALMA1, ApJ, 929, 68.
Omae, R., Akahori, T., Machida, M.: 2023, Effects of depolarizing
intervening galaxies on background radio emission. I. Global diskmagnetic field, PASJ, 75, S108–S122.
Omiya, Y., Nakazawa, K., Matsushita, K., Kobayashi, S. B., Okabe, N.,
Sato, K., Tamura, T., Fujita, Y., Gu, L., Kitayama, T., Akahori, T.,
Kurahara, K., Yamaguchi, T.: 2023, XMM-Newton view of theshock heating in an early merging cluster, CIZA J1358.9-4750, PASJ,75, 37–51.
Ono, Y., et al. including Ouchi, M., Imanishi, M., Sugahara, Y.: 2022,
ALMA Observations of CO Emission from Luminous Lyman-break
Galaxies at z = 6.0293–6.2037, ApJ, 941, 74.
Orell-Miquel, J., et al. including Livingston, J.: 2023, HD 191939
revisited: New and refined planet mass determinations, and a newplanet in the habitable zone, A&A, 669, A40.
Orozco Suarez, D., et al. including Ishikawa, R., Katsukawa, Y., Kano,
R.: 2022, CASPER: A mission to study the time-dependent evolutionof the magnetic solar chromosphere and transition regions, Exp.
Astron., 54, 257–276.
Orton, G. S., et al. including Fujiyoshi, T.: 2023, Unexpected long-term
variability in Jupiter’s tropospheric temperatures, Nat. Astron, 7,
190–197.
O'Sullivan, S. P., et al. including Ideguchi, S.: 2023, The Faraday
Rotation Measure Grid of the LOFAR Two-metre Sky Survey: Data
Release 2, MNRAS, 519, 5723–5742.
Ota, N., et al. including Miyazaki, S.: 2023, The eROSITA Final
Equatorial-Depth Survey (eFEDS) X-ray properties of Subaru's
optically selected clusters, A&A, 669, A110.
Otsu, T., Asai, A., Ichimoto, K., Ishii, T. T., Namekata, K.: 2022, Sunas-a-star Analyses of Various Solar Active Events Using Hα Spectral
Images Taken by SMART/SDDI, ApJ, 939, 98.
Pedreira, A. C. C. D. S., Fraija, N., Galvan-Gamez, A., Kamenetskaia,
B. B., Veres, P., Dainotti, M. G., Dichiara, S., Becerra, R. L.: 2023,
Afterglow Polarization from Off-axis Gamma-Ray Burst Jets, ApJ,
942, 81.
Peng, Y., et al. including Tatematsu, K.: 2022, ATOMS: ALMA Threemillimeter Observations of Massive Star-forming regions - X.
Chemical differentiation among the massive cores in G9.62+0.19,
MNRAS, 512, 4419–4440.
Pérez-González, P. G., et al. including Zavala, J. A., Behroozi, P.: 2023,
CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies,
ApJL, 946, L16.
Perez-Martinez, J. M., Dannerbauer, H., Kodama, T., Koyama, Y.,
Shimakawa, R., Suzuki, T. L., Calvi, R., Chen, Z., Daikuhara, K.,
Hatch, N. A., Laza-Ramos, A., Sobral, D., Stott, J. P., Tanaka, I.:
2023, Signs of environmental effects on star-forming galaxies in theSpiderweb protocluster at z=2.16, MNRAS, 518, 1707–1734.
Persson, C. M., et al. including Livingston, J.: 2022, TOI-2196 b: Rareplanet in the hot Neptune desert transiting a G-type star, A&A, 666,
A184.
Pflugradt, J., et al. including Chen, X.: 2022, Finding of a Population of
Active Galactic Nuclei Showing a Significant Luminosity Decline in
the Past ~ 103–104 yr, ApJ, 938, 75.
Plunkett, A., et al. including Miyamoto, Y.: 2023, Data Combination:
Interferometry and Single-dish Imaging in Radio Astronomy, PASP,
135, 034501.
Pouliasis, E., et al. including Toba, Y.: 2022, XXL-HSC: Link between
AGN activity and star formation in the early Universe (z ≥ 3.5), A&A,
667, A56.
Pouteau, Y., et al. including Sanhueza, P.: 2022, ALMA-IMF III.
Investigating the origin of stellar masses: top-heavy core massfunction in the W43-MM2&MM3 mini-starburst, A&A, 664, A26.
Prabhu, D. S., et al. including Simunovic, M.: 2022, Globular Cluster
UVIT Legacy Survey (GlobULeS). III. Omega Centauri in Far-

XIII Publications, Presentations

155

ultraviolet, ApJL, 939, L20.
Quintero Noda, C., et al. including Suematsu, Y.: 2022, The European
Solar Telescope, A&A, 666, A21.
Rachi, S., Sakuma, K., Akahori, T., Sekiya, N.: 2023, Development ofhighly selective compact high-temperature superconducting quadband bandpass filter using interdigital feeding structure for radio
astronomy, Supercond. Sci. Technol., 36, 025006.
Rachmeler, L. A., et al. including Ishikawa, R., Kano, R., Okamoto,T. J., Song, D., Yoshida, M., Narukage, N., Kubo, M., Hara, H.,
Suematsu, Y.: 2022, Quiet Sun Center to Limb Variation of the
Linear Polarization Observed by CLASP2 Across the Mg II h and k
Lines, ApJ, 936, 67.
Ramos-Ceja, M. E., et al. including Miyazaki, S.: 2022, The eROSITA
Final Equatorial-Depth Survey (eFEDS) A complete census of X-ray
properties of Subaru Hyper Suprime-Cam weak lensing shearselected clusters in the eFEDS footprint, A&A, 661, A14.
Redaelli, E., Bovino, S., Sanhueza, P., Morii, K., Sabatini, G., Caselli, P.,
Giannetti, A., Li, S. H.: 2022, The Core Population and Kinematics
of a Massive Clump at Early Stages: An Atacama Large Millimeter/
submillimeter Array View, ApJ, 936, 169.
Ren, Y. W., et al. including Fudamoto, Y., Sugahara, Y., Matsuo, H.:
2023, Updated Measurements of [O III] 88 μm, [C II] 158 μm, andDust Continuum Emission from a z=7.2 Galaxy, ApJ, 945, 69.
Rodriguez, M. J., et al. including Saito, T.: 2023, PHANGS-JWST First
Results: Dust-embedded Star Clusters in NGC 7496 Selected via
3.3 μm PAH Emission, ApJL, 944, L26.
Roederer, I. U., et al. including Hattori, K.: 2022, The R-process
Alliance: A Nearly Complete R-process Abundance Template Derived
from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor
Star HD 222925*, ApJS, 260, 27.
Rybak, M., Bakx, T., Baselmans, J., Karatsu, K., Kohno, K., Takekoshi,T., Tamura, Y., Taniguchi, A., van der Werf, P., Endo, A.: 2022,
Deshima 2.0: Rapid Redshift Surveys and Multi-line Spectroscopy of
Dusty Galaxies, J. Low Temp. Phys., 209, 766–778.
Sabatini, G., Bovino, S., Sanhueza, P., Morii, K., Li, S. H., Redaelli,E., Zhang, Q. Z., Lu, X., Feng, S. Y., Tafoya, D., Izumi, N., Sakai, T.,
Tatematsu, K., Allingham, D.: 2022, The ALMA Survey of 70 μm
Dark High-mass Clumps in Early Stages (ASHES). VI. The Corescale CO Depletion, ApJ, 936, 80.
Sahu, D., et al. including Tatematsu, K., Sanhueza, P.: 2023, ALMA
Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Density
Structure of Centrally Concentrated Prestellar Cores from Multiscale
Observations, ApJ, 945, 156.
Sahu, S., et al. including Simunovic, M.: 2022, Globular Cluster UVIT
Legacy Survey (GlobULeS) - I. FUV-optical colour-magnitude
diagrams for eight globular clusters, MNRAS, 514, 1122–1139.
Saito, S., Tanaka, M., Sawada, R., Moriya, T. J.: 2022, Constraints on
the Explosion Timescale of Core-collapse Supernovae Based on
Systematic Analysis of Light Curves, ApJ, 931, 153.
Saito, T., Takano, S., Harada, N., Nakajima, T., Schinnerer, E., Liu,
D. Z., Taniguchi, A., Izumi, T., Watanabe, Y., Bamba, K., Kohno,K., Nishimura, Y., Stuber, S., Tosaki, T.: 2022, AGN-driven ColdGas Outflow of NGC 1068 Characterized by Dissociation-sensitive
Molecules, ApJ, 935, 155.
Sakai, N., et al. including Sakai, D., Tamura, Y., Jike, T., Kawaguchi,N., Hachisuka, K., Honma, M.: 2023, East Asian VLBI Network

156

XIII Publications, Presentations

astrometry toward the extreme outer Galaxy: Kinematic distance withthe proper motion of G034.84-00.95, PASJ, 75, 208–224.
Sakai, Y., et al. including Kozakai, C.: 2022, Unsupervised learning
architecture for classifying the transient noise of interferometricgravitational-wave detectors, Sci. Rep., 12, 9935.
Sakatani, N., Tanaka, S., Arakawa, S.: 2022, Development of a SmallSized Line Heat Source Apparatus for the Thermal Conductivity
Measurement of Extraterrestrial Soils, Int. J. Thermophys., 43, 89.
Sakaue, H. A., Kato, D., Yamamoto, N., Murakami, I., Hara, H.,
Nakamura, N.: 2023, Energy Dependence of the Line Ratio
I(233.9 Å)/I(243.8 Å) in Fe xv Observed with an Electron Beam Ion
Trap, ApJ, 943, 14.
Sakurai, T., Toriumi, S.: 2023, Probability Distribution Functions ofSunspot Magnetic Flux, ApJ, 943, 10.
Sandstrom, K. M., et al. including Saito, T.: 2023, PHANGS–JWST First
Results: Tracing the Diffuse Interstellar Medium with JWST Imaging
of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies,
ApJL, 944, L8.
Sano, H., Yamaguchi, H., Aruga, M., Fukui, Y., Tachihara, K., Filipovic,
M. D., Rowell, G.: 2022, An Expanding Shell of Neutral Hydrogen
Associated with SN 1006: Hints for the Single-degenerate Origin and
Faint Hadronic Gamma-Rays, ApJ, 933, 157.
Sasaki, H., Takiwaki, T.: 2022, A detailed analysis of the dynamics offast neutrino flavor conversions with scattering effects, Prog. Theor.
Exp. Phys., 2022, 073E01.
Sato, A., Takahashi, S., Ishii, S., Ho, P. T. P., Machida, M. N., Carpenter,
J., Zapata, L. A., Teixeira, P. S., Suri, S.: 2023, ALMA Fragmented
Source Catalog in Orion (FraSCO). I. Outflow Interaction within an
Embedded Cluster in OMC-2/FIR 3, FIR 4, and FIR 5, ApJ, 944, 92.
Sato, K., et al. including Mitsuda, K.: 2022, Super DIOS Project for
Exploring Dark Baryon, J. Low Temp. Phys., 209, 971–979.
Sato, M. T., Aalto, S., Kohno, K., Konig, S., Harada, N., Viti, S.,
Izumi, T., Nishimura, Y., Gorski, M.: 2022, APEX and NOEMA
observations of H2S in nearby luminous galaxies and the ULIRG Mrk
231 A possible relation between dense gas properties and molecular
outflows, A&A, 660, A82.
Sawada-Satoh, S., Kameno, S., Trippe, S.: 2022, Circumnuclear dense
gas disk fuelling the active galactic nucleus in the nearby radio galaxy
NGC 4261, A&A, 664, L11.
Schatz, H., et al. including Aoki, W., Famiano, M. A., Kajino, T.: 2022,
Horizons: nuclear astrophysics in the 2020s and beyond, J. Phys. G:
Nucl. Phys., 49, 110502.
Schatz, L., et al. including Guyon, O.: 2022, Three-sided pyramid
wavefront sensor, part II: preliminary demonstration on the newcomprehensive adaptive optics and coronagraph test instrument
testbed, J. Astron. Telesc. Instrum. Syst., 8, 049001.
Schinnerer, E., et al. including Saito, T.: 2023, PHANGS-JWST First
Results: Rapid Evolution of Star Formation in the Central Molecular
Gas Ring of NGC 1365, ApJL, 944, L15.
Schneider, N., et al. including Arzoumanian, D.: 2022, Understanding
star formation in molecular clouds IV. Column density PDFs fromquiescent to massive molecular clouds, A&A, 666, A165.
Scicluna, P., et al. including Izumiura, H.: 2022, The Nearby Evolved
Stars Survey II: Constructing a volume-limited sample and first resultsfrom the James Clerk Maxwell Telescope, MNRAS, 512, 1091–1110.
Sewilo, M., et al. including Tokuda, K., Zahorecz, S.: 2022, ALMA

Observations of Molecular Complexity in the Large Magellanic
Cloud: The N 105 Star-forming Region, ApJ, 931, 102.
Shajib, A. J., et al. including Wong, K. C., Rusu, C. E.: 2022,
IX. Systematic comparison between lens modelling software
programs:Time-delay prediction for WGD 2038-4008, A&A, 667,
A123.
Shan, W., Ezaki, S.: 2022, Cryogenic NbTiN thin film resistors
fabricated by using reactive magnetron sputtering, Thin Solid Films,
763, 139575.
Sheehan, P. D., et al. including Saigo, K.: 2022, A VLA View of theFlared, Asymmetric Disk around the Class 0 Protostar L1527 IRS,
ApJ, 934, 95.
Shim, H., Hwang, H. S., Jeong, W. S., Toba, Y., Kim, M., Kim, D., Song,H., Hashimoto, T., Nakagawa, T., Nanni, A., Pearson, W. J., Takagi,
T.: 2023, Metallicity-PAH Relation of MIR-selected Star-forming
Galaxies in AKARI North Ecliptic Pole-wide Survey, AJ, 165, 31.
Shimabukuro, H., Hasegawa, K., Kuchinomachi, A., Yajima, H.,
Yoshiura, S.: 2023, Exploring the cosmic dawn and epoch ofreionization with the 21 cm line, PASJ, 75, S1–S32.
Shimakawa, R., Okabe, N., Shirasaki, M., Tanaka, M.: 2023, King
Ghidorah Supercluster: Mapping the light and dark matter in a newsupercluster at z = 0.55 using the subaru hyper suprime-cam, MNRAS
Lett., 519, L45–L50.
Shimakawa, R., Tanaka, M., Bottrell, C., Wu, P. F., Chang, Y. Y., Toba,
Y., Ali, S.: 2022, Passive spiral galaxies deeply captured by Subaru
Hyper Suprime-Cam, PASJ, 74, 612–624.
Shimakawa, R., Tanaka, M., Kikuta, S., Hayashi, M.: 2022, H alphaemission in the outskirts of galaxies at z=0.4, PASJ, 74, 318–325.
Shimakawa, R.: 2022, Search for extended Lymanα emission around 9k
quasars at z=2–3, MNRAS, 514, 3910–3924.
Shimizu, K., Shoda, M., Suzuki, T. K.: 2022, Role of Longitudinal
Waves in Alfven-wave-driven Solar Wind, ApJ, 931, 37.
Shimizu, T., Uyama, T., Hori, Y., Tamura, M., Wallack, N.: 2023,
High-contrast Imaging around a 2 Myr-old CI Tau with a Close-in
Gas Giant, AJ, 165, 20.
Shimojo, M., Iwai, K.: 2023, Over seven decades of solar microwave
data obtained with Toyokawa and Nobeyama Radio Polarimeters,
Geosci. Data J., 10, 114–119.
Shirasaki, M., Okamoto, T., Ando, S.: 2022, Modelling self-interacting
dark matter substructures - I. Calibration with N-body simulations ofa Milky-Way-sized halo and its satellite, MNRAS, 516, 4594–4611.
Shoda, M., Iwai, K., Shiota, D.: 2022, Testing the Alfven-wave Modelof the Solar Wind with Interplanetary Scintillation, ApJ, 928, 130.
Shoji, M., Watanabe, N., Hori, Y., Furuya, K., Umemura, M., Boero,
M., Shigeta, Y.: 2022, Comprehensive Search of Stable Isomers of
Alanine and Alanine Precursors in Prebiotic Syntheses, Astrobiol., 22,1129–1142.
Snellen, I. A. G., et al. including Guyon, O.: 2022, Detecting life outside
our solar system with a large high-contrast-imaging mission, Exp.
Astron., 54, 1237–1274.
Sommovigo, L., et al. including Fudamoto, Y.: 2022, The ALMAREBELS Survey: cosmic dust temperature evolution out to z ~ 7,
MNRAS, 513, 3122–3135.
Song, D., et al, including Ishikawa, R., Kano, R., Okamoto, T. J.,
Yoshida, M., Hara, H., Shinoda, K., Suematsu, Y., Narukage,N., Kubo, M.: 2022, Polarization Accuracy Verification of the

Chromospheric LAyer SpectroPolarimeter, Sol. Phys., 297, 135.
Sotani, H., Nishimura, N., Naito, T.: 2022, New constraints on theneutron-star mass and radius relation from terrestrial nuclear
experiments, Prog. Theor. Exp. Phys., 2022, 041D01.
Stanley, F., et al. including Bakx, T. J. L. C.: 2023, Resolved CO(1–0)
Emission and Gas Properties in Luminous Dusty Star-forming
Galaxies at z=2–4, ApJ, 945, 24.
Stefansson, G., et al. including Hirano, T.: 2022, The Warm Neptune GJ
3470b Has a Polar Orbit, ApJL, 931, L15.
Steiger, S., et al. including Guyon, O., Lozi, J., Deo, V., Vievard, S.,
Skaf, N., Ahn, K.: 2022, Probing Photon Statistics in Adaptive
Optics Images with SCExAO/MEC*, AJ, 164, 186.
Subjak, J., et al. including Livingston, J. H.: 2022, TOI-1268b: The
youngest hot Saturn-mass transiting exoplanet, A&A, 662, A107.
Subrayan, B. M., et al. including Moriya, T. J.: 2023, Inferencing
Progenitor and Explosion Properties of Evolving Core-collapse
Supernovae from Zwicky Transient Facility Light Curves, ApJ, 945,
46.
Sugahara, Y., Inoue, A. K., Fudamoto, Y., Hashimoto, T., Harikane, Y.,
Yamanaka, S.: 2022, Bridging Optical and Far-infrared Emissionline Diagrams of Galaxies from Local to the Epoch of Reionization:
Characteristic High [O III] 88 μm/SFR at z > 6, ApJ, 935, 119.
Sugiyama, S., et al. including Shirasaki, M.: 2022, HSC Year 1
cosmology results with the minimal bias method: HSC ×BOSS
galaxy-galaxy weak lensing and BOSS galaxy clustering, Phys. Rev.
D, 105, 123537.
Suleiman, N., Noboriguchi, A., Toba, Y., Balazs, L. G., Burgarella, D.,
Kovacs, T., Marton, G., Talafha, M., Frey, S., Toth, L. V.: 2022, The
statistical properties of 28 IR-bright dust-obscured galaxies and SED
modelling using CIGALE, PASJ, 74, 1157–1185.
Sumi, M., Takehiro, S. I., Ohfuchi, W., Nomura, H., Fujii, Y.: 2022,
Superrotation of Titan's Stratosphere Driven by the Radiative Heatingof the Haze Layer, ApJ, 928, 149.
Sumiyoshi, K., Furusawa, S., Nagakura, H., Harada, A., Togashi,
H., Nakazato, K., Suzuki, H.: 2023, Effects of nuclear matter andcomposition in core-collapse supernovae and long-term proto-neutronstar cooling, Prog. Theor. Exp. Phys., 2023, 013E02.
Sun, F. W., et al. including Morokuma-Matsui, K.: 2022, ALMA Lensing
Cluster Survey: ALMA-Herschel Joint Study of Lensed Dusty Starforming Galaxies across z ≃ 0.5–6, ApJ, 932, 77.
Sun, J. Y., et al. including Saito, T.: 2022, Molecular Cloud Populations in
the Context of Their Host Galaxy Environments: A Multiwavelength
Perspective, AJ, 164, 43.
Sun, J., et al. including Saito, T.: 2023, Star Formation Laws andEfficiencies across 80 Nearby Galaxies, ApJL, 945, L19.
Sunada, Y., Isobe, N., Tashiro, M. S., Kino, M., Koyama, S., Nakahara,
S.: 2022, Herschel discovery of far-infrared emission from thehotspot D in the radio galaxy Cygnus A, MNRAS, 512, 5995–6006.
Suto, Y., Sasaki, S., Nakagawa, Y., Benomar, O.: 2022, Analytic model
for photometric variation due to starspots on a differentially rotating
star, PASJ, 74, 857–876.
Svetlana J., et al. including Akiyama, K., Ikeda, S., Kino, M., Nagai, H.,
Cui, Y., Hada, K., Honma, M., Kofuji, Y., Moriyama, K., Okino,
H., Oyama, T., Sasada, M., Tazaki, F.: 2023, The Event Horizon
Telescope Image of the Quasar NRAO 530, ApJ, 943, 170.
Swimmer, N., et al. including Currie, T., Guyon, O., Kuzuhara,

XIII Publications, Presentations

157

M., Lozi, J., Vievard, S., Skaf, N., Deo, V., Tamura, M.: 2022,
SCExAO and Keck Direct Imaging Discovery of a Low-mass
Companion Around the Accelerating F5 Star HIP 5319, AJ, 164, 152.
Tadaki, K. I., Tsujita, A., Tamura, Y., Kohno, K., Hatsukade, B., Iono, D.,
Lee, M. M., Matsuda, Y., Michiyama, T., Nagao, T., Nakanishi, K.,
Nishimura, Y., Saito, T., Umehata, H., Zavala, J.: 2022, Detectionof nitrogen and oxygen in a galaxy at the end of reionization, PASJ,
74, L9–L16.
Tahani, M., et al. including Arzoumanian, D., Hasegawa, T., Shimajiri,Y., Tomisaka, K., Kataoka, A., Kusune, T., Nakamura, F., Kim,
G., Hayashi, S. S., Hull, C. L. H., Pyo, T. S.: 2023, JCMT BISTRO
Observations: Magnetic Field Morphology of Bubbles Associatedwith NGC 6334, ApJ, 944, 139.
Takahashi, I., Hamasaki, R., Ueda, N., Tanaka, M., Tominaga, N.,
Sako, S., Ohsawa, R., Yoshida, N.: 2022, Deep-learning real/bogus
classification for the Tomo-e Gozen transient survey, PASJ, 74, 946–
960.
Takahashi, K., Takiwaki, T., Yoshida, T.: 2023, Monotonicity of theCores of Massive Stars, ApJ, 945, 19.
Takahashi, S. Z., Kokubo, E., Inutsuka, S.: 2023, Planetesimal
Formation by the Gravitational Instability of Dust Ring Structures,
ApJ, 945, 120.
Takami, M., et al. including Uyama, T., Fukagawa, M., Pyo, T.-S.:
2023, Time-variable Jet Ejections from RW Aur A, RY Tau, and DG
Tau*, ApJS, 264, 1.
Takamori, Y., Naruko, A., Sakurai, Y., Takahashi, K., Yamauchi, D.,
Yoo, C. M.: 2023, Testing the non-circularity of the spacetime around
Sagittarius A* with orbiting pulsars, PASJ, 75, S217–S231.
Takasao, S., Tomida, K., Iwasaki, K., Suzuki, T. K.: 2022, Threedimensional Simulations of Magnetospheric Accretion in a T Tauri
Star: Accretion and Wind Structures Just Around the Star, ApJ, 941, 73.
Takeda, Y.: 2023, Surface magnetic field of the A-type metallic-line staromicron Pegasi revisited, Astron. Nachr., 344, e220057.
Takekoshi, T., Lee, K., Chin, K. W., Uno, S., Naganuma, T., Inoue, S.,
Niwa, Y., Fujita, K., Kouchi, A., Nakatsubo, S., Mima, S., Oshima,T.: 2022, Material Properties of a Low Contraction and Resistivity
Silicon-Aluminum Composite for Cryogenic Detectors, J. Low Temp.
Phys., 209, 1143–1150.
Takemura, H., et al. including Nakamura, F., Ishii, S., Sanhueza, P.,
Tsukagoshi, T., Shimajiri, Y., Kawabe, R.: 2023, CARMA-NRO
Orion Survey: Unbiased Survey of Dense Cores and Core Mass
Functions in Orion A, ApJS, 264, 35.
Tampo, Y., Isogai, K., Kojiguchi, N., Uemura, M., Kato, T., Tordai,T., Vanmunster, T., Itoh, H., Dubovsky, P. A., Medulka, T., Sano,
Y., Hambsch, F. J., Taguchi, K., Maehara, H., Ito, J., Nogami, D.:
2022, PNV J00444033+4113068: Early superhumps with 0.7 mag
amplitude and non-red color, PASJ, 74, 1287–1294.
Tampo, Y., Nogami, D., Kato, T., Ayani, K., Naito, H., Narita, N.,
Fujii, M., Hashimoto, O., Kinugasa, K., Honda, S., Takahashi,
H., Narusawa, S., Sakamoto, M., Imada, A.: 2022, Spectroscopic
observations of V455 Andromedae superoutburst in 2007: The most
exotic spectral features in dwarf nova outbursts, PASJ, 74, 460–476.
Tan, S., Sekine, Y., Kuzuhara, M.: 2022, Spatially Resolved Observationsof Europa's Surface with Subaru/IRCS at 1.0–1.8 μm: Upper Limits
to the Abundances of Hydrated Cl-bearing Salts, Planet. Sci. J., 3, 70
Tanaka, H., Kogiso, N., Sakano, F., Katsumata, N., Yamazaki, K.,

158

XIII Publications, Presentations

Higuchi, K., Ishimura, K., Iwasa, T., Kishimoto, N., Fujigaki, M.,
Doi, A., Nakahara, S., Hasegawa, Y., Kono, Y.: 2022, Experimental
demonstration of deformable reflector antenna system with highaccuracy deformation measurement, Acta Astronaut., 194, 93–105.
Taniguchi, A., et al, including Bakx, T. J. L. C., Fujii, Y., Ishii, S.,
Kawabe, R., Maekawa, J., Oshima, T.: 2022, DESHIMA 2.0:
Development of an Integrated Superconducting Spectrometer for
Science-Grade Astronomical Observations, J. Low Temp. Phys., 209,
278–286.
Taniguchi, K., Tanaka, K. E. I., Zhang, Y. C., Fedriani, R., Tan, J. C.,
Takakuwa, S., Nakamura, F., Saito, M., Majumdar, L., Herbst,
E.: 2022, Vibrationally Excited Lines of HC3N Associated with the
Molecular Disk around the G24.78+0.08 A1 Hypercompact H II
Region, ApJ, 931, 99.
Tanikawa, A., Chiaki, G., Kinugawa, T., Suwa, Y., Tominaga, N.: 2022,
Can Population III stars be major origins of both merging binary
black holes and extremely metal poor stars?, PASJ, 74, 521–532.
Tanikawa, A., Moriya, T. J., Tominaga, N., Yoshida, N.: 2023, Euclid
detectability of pair instability supernovae in binary population
synthesis models consistent with merging binary black holes, MNRAS
Lett., 519, L32–L38.
Tanikawa, K., Soma, M., Qu, A.: 2022, Short-term variations of Delta
T from Yangdi-eclipse on AD 616 May 21, Suiko eclipse on AD 628
April 10, and neighboring solar eclipses and occultations, PASJ, 74,
665–677.
Tashima, Y., Ohmura, T., Machida, M.: 2023, Pseudo-observation of
spiral galaxies in the radio band to verify depolarization models,
PASJ, 75, S123–S137.
Tatematsu, K., et al. including Sanhueza, P., Kim, G.: 2022, Nobeyama
Survey of Inward Motions toward Cores in Orion Identified by
SCUBA-2, ApJ, 931, 33.
Taylor, L., et al. including Wu, P.-F.: 2022, The Velocity Dispersion
Function for Massive Quiescent and Star-forming Galaxies at 0.6 < z≤ 1.0, ApJ, 939, 90.
Teng, H. Y., Sato, B., Kunitomo, M., Takarada, T., Omiya, M., Harakawa,
H., Xiao, G. Y., Liu, Y. J., Izumiura, H., Kambe, E., Yoshida, M.,
Itoh, Y., Ando, H., Kokubo, E., Ida, S.: 2023, A close-in planet
orbiting giant star HD 167768, PASJ, 75, 169–176.
Teng, H. Y., Sato, B., Takarada, T., Omiya, M., Harakawa, H., Nagasawa,
M., Hasegawa, R., Izumiura, H., Kambe, E., Yoshida, M., Itoh, Y.,
Ando, H., Kokubo, E., Ida, S.: 2022, A trio of giant planets orbiting
evolved star HD 184010, PASJ, 74, 1309–1328.
Terao, K., Nagao, T., Onishi, K., Matsuoka, K., Akiyama, M., Matsuoka,
Y., Yamashita, T.: 2022, Multiline Assessment of Narrow-line
Regions in z ~ 3 Radio Galaxies, ApJ, 929, 51.
Terao, Y., Spitler, L. R., Motohara, K., Chen, N.: 2022, A Selectionof H alpha Emitters at z=2.1–2.5 Using the Ks-band Photometry of
ZFOURGE, ApJ, 941, 70.
Toba, Y., et al. including Imanishi, M.: 2022, The eROSITA Final
Equatorial-Depth Survey (eFEDS) A multiwavelength view of WISE
mid-infrared galaxies/active galactic nuclei, A&A, 661, A15.
Toba, Y., et al. including Terao, K.: 2022, Optical IFU observationsof GOALS sample with KOOLS-IFU on Seimei Telescope: Initial
results of nine U/LIRGs at z < 0.04, PASJ, 74, 1356–1367.
Tobin, J. J., et al. including Furuya, K.: 2023, Deuterium-enrichedwater ties planet-forming disks to comets and protostars, Nature, 615,

227–230.
Tokuda, K., Minami, T., Fukui, Y., Inoue, T., Nishioka, T., Tsuge, K.,
Zahorecz, S., Sano, H., Konishi, A., Chen, C. H. R., Sewilo, M.,
Madden, S. C., Nayak, O., Saigo, K., Nishimura, A., Tanaka, K.
E. I., Sawada, T., Indebetouw, R., Tachihara, K., Kawamura, A.,
Onishi, T.: 2022, An ALMA Study of the Massive Molecular Clump
N159W-North in the Large Magellanic Cloud: A Possible Gas Flow
Penetrating One of the Most Massive Protocluster Systems in the
Local Group, ApJ, 933, 20.
Tokuda, K., Zahorecz, S., Kunitoshi, Y., Higashino, K., Tanaka, K. E.
I., Konishi, A., Suzuki, T., Kitano, N., Harada, N., Shimonishi, T.,
Neelamkodan, N., Fukui, Y., Kawamura, A., Onishi, T., Machida,
M. N.: 2022, The First Detection of a Protostellar CO Outflow in the
Small Magellanic Cloud with ALMA, ApJL, 936, L6.
Tokuoka, T., Inoue, A. K., Hashimoto, T., Ellis, R. S., Laporte, N.,
Sugahara, Y., Matsuo, H., Tamura, Y., Fudamoto, Y., Moriwaki,
K., Roberts-Borsani, G., Shimizu, I., Yamanaka, S., Yoshida, N.,
Zackrisson, E., Zheng, W.: 2022, Possible Systematic Rotation in the
Mature Stellar Population of a z=9.1 Galaxy, ApJL, 933, L19.
Topping, M. W., et al. including Algera, H., Fudamoto, Y.: 2022,
The ALMA REBELS Survey: specific star formation rates in thereionization era, MNRAS, 516, 975–991.
Toriumi, S., Airapetian, V. S., Namekata, K., Notsu, Y.: 2022, Universal
Scaling Laws for Solar and Stellar Atmospheric Heating: Catalog ofPower-law Index between Solar Activity Proxies and Various Spectral
Irradiances, ApJS, 262, 46.
Tran, Q. H., et al. including Livingston, J. H.: 2022, TOI-1670 b and c:
An Inner Sub-Neptune with an Outer Warm Jupiter Unlikely to Have
Originated from High-eccentricity Migration, AJ, 163, 225.
Trump, J. R., et al. including Zavala, J. A.: 2023, The Physical Conditionsof Emission-line Galaxies at Cosmic Dawn from JWST/NIRSpec
Spectroscopy in the SMACS 0723 Early Release Observations, ApJ,
945, 35.
Tsuboi, M., Tsutsumi, T., Miyazaki, A., Miyawaki, R., Miyoshi, M.:
2022, ALMA astrometry of the objects within 0.5 pc of Sagittarius A,
PASJ, 74, 738–756.
Tsuchikawa, T., Kaneda, H., Oyabu, S., Kokusho, T., Kobayashi, H.,
Toba, Y.: 2022, Spitzer/IRS Full Spectral Modeling to Characterize
Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs,
ApJ, 941, 50.
Tsujimoto, M., Hayashi, T., Morihana, K., Moritani, Y.: 2023, X-ray
and optical spectroscopic study of a gamma Cassiopeiae analog
source pi Aquarii, PASJ, 75, 177–186.
Tsujimoto, T.: 2023, From Galactic chemical evolution to cosmic
supernova rates synchronized with core-collapse supernovae limited
to the narrow progenitor mass range, MNRAS, 518, 3475–3481.
Tsujita, A., et al. including Tadaki, K.-i., Zavala, J., Saito, T.: 2022,
Central concentration of warm and dense molecular gas in a strongly
lensed submillimeter galaxy at z=6, PASJ, 74, 1429–1440.
Tsukui, T., Iguchi, S., Mitsuhashi, I., Tadaki, K.: 2023, Estimating
the statistical uncertainty due to spatially correlated noise ininterferometric images, J. Astron. Telesc. Instrum. Syst., 9, 018001.
Tsunetoe, Y., Mineshige, S., Kawashima, T., Ohsuga, K., Akiyama,K., Takahashi, H. R.: 2022, Investigating the Disk-Jet Structure in
M87 through Flux Separation in the Linear and Circular Polarization
Images, ApJ, 931, 25.

Tsuruta, T., Hamamura, Y., Iyomoto, N., Nakamura, Y., Kawaguchi, S.,
Hayashi, T., Yagi, Y., Yamasaki, N., Mitsuda, K.: 2022, Thermal
Conductance of Thick-Membrane TES Microcalorimeters for
Several-MeV Gamma Rays, J. Low Temp. Phys., 209, 449–456.
Uchiyama, H., Yamashita, T., Nagao, T., Ichikawa, K., Toba, Y.,
Ishikawa, S., Kubo, M., Kajisawa, M., Kawaguchi, T., Kawakatu, N.,
Lee, C. H., Noboriguchi, A.: 2022, A Wide and Deep Exploration ofRadio Galaxies with Subaru HSC (WERGS). VII. Redshift Evolutionof Radio Galaxy Environments at z=0.3–1.4, ApJ, 934, 68.
Uchiyama, H., Yamashita, T., Nagao, T., Ono, Y., Toshikawa, J.,
Ichikawa, K., Kawakatu, N., Kajisawa, M., Toba, Y., Matsuoka, Y.,
Kubo, M., Imanishi, M., Ito, K., Kawaguchi, T., Lee, C. H., Saito, T.:
2022, A Wide and Deep Exploration of Radio Galaxies with Subaru
HSC (WERGS). IX. The most overdense region at z ~ 5 inhabited bya massive radio galaxy, PASJ, 74, L27–L32.
Uchiyama, M., Ichikawa, K., Sugiyama, K., Tanabe, Y., Yonekura, Y.:
2022, Mid-infrared and Maser Flux Variability Correlation in Massive
Young Stellar Object G036.70+00.09, ApJ, 936, 31.
Ueda, J., Michiyama, T., Iono, D., Miyamoto, Y., Saito, T.: 2022,
Spatially-resolved relation between [C I] 3P1–3P0 and 12CO (1–0) in
Arp 220, PASJ, 74, 407–420.
Ueda, T., Kataoka, A., Tsukagoshi, T.: 2022, Massive Compact Dust
Disk with a Gap around CW Tau Revealed by ALMA Multiband
Observations, ApJ, 930, 56.
Ueda, T., Ricci, L., Flock, M., Castro, Z.: 2022, Probing the Inner
Edge of Dead Zones in Protoplanetary Disks with ALMA and Next
Generation Very Large Array, ApJ, 928, 110.
Uehata, K., Terai, T., Ohtsuki, K., Yoshida, F.: 2022, Size Distribution of
Small Jupiter Trojans in the L-5 Swarm*, AJ, 163, 213.
Uematsu, R., et al. including Toba, Y.: 2023, ALMA Lensing Cluster
Survey: Properties of Millimeter Galaxies Hosting X-Ray-detected
Active Galactic Nuclei, ApJ, 945, 121.
Umeda, H., Ouchi, M., Nakajima, K., Isobe, Y., Aoyama, S., Harikane,Y., Ono, Y., Matsumoto, A.: 2022, EMPRESS. VII. Ionizing Spectrum
Shapes of Extremely Metal-poor Galaxies: Uncovering the Origins ofStrong He II and the Impact on Cosmic Reionization, ApJ, 930, 37.
Uneme, S., Imada, S., Lee, H., Park, E., Hayakawa, H., Iju, T., Moon,
Y. J.: 2022, Inference of magnetic field during the Dalton minimum:
Case study with recorded sunspot areas, PASJ, 74, 767–776.
Uno, K., et al. including Aoki, K., Tajitsu, A.: 2023, SN 2020uem: aPossible Thermonuclear Explosion within a Dense Circumstellar
Medium (II). The Properties of the CSM from Polarimetry and Lightcurve Modeling, ApJ, 944, 204.
Uno, K., et al. including Motohara, K., Aoki, K., Tajitsu, A.: 2023,
SN 2020uem: a Possible Thermonuclear Explosion within a Dense
Circumstellar Medium. I. The Nature of Type IIn/Ia-CSM SNe from
Photometry and Spectroscopy, ApJ, 944, 203.
Urata, Y., et al. including Nagai, H., Takahashi, S.: 2023, Simultaneousradio and optical polarimetry of GRB 191221B afterglow, Nat.
Astron, 7, 80–87.
Uyama, T., Ruane, G., Lawson, K., Muto, T., Beichman, C., van derMarel, N.: 2022, A Spatially-resolved Large Cavity of the J0337
Protoplanetary Disk in Perseus, AJ, 163, 204.
Uyama, T., Takami, M., Cugno, G., Deo, V., Guyon, O., Hashimoto,J., Lozi, J., Norris, B., Tamura, M., Vievard, S., Gunther, H. M.,
Schneider, P. C., Akiyama, E., Beck, T. L., Currie, T., Hodapp, K.,

XIII Publications, Presentations

159

Kwon, J., Mayama, S., Ohyama, Y., Pyo, T. S., Wisniewski, J. P.:
2022, Monitoring Inner Regions in the RY Tau Jet, AJ, 163, 268.
van der Vlugt, D., et al. including Algera, H. S. B.: 2022, An Ultradeep Multiband Very Large Array (VLA) Survey of the Faint RadioSky (COSMOS-XS): New Constraints on the Cosmic Star Formation
History, ApJ, 941, 10.
Van Reeth, T., et al. including Kambe, E.: 2022, The near-core rotationof HD 112429 A gamma Doradus star with TESS photometry andlegacy spectroscopy, A&A, 662, A58.
Vastel, C., et al. including Hirota, T., Nomura, H.: 2022, FAUST V. Hot
methanol in the [BHB2007] 11 protobinary system; hot corino versus
shock origin, A&A, 664, A171.
Vijarnwannaluk, B., Akiyama, M., Schramm, M., Ueda, Y., Matsuoka, Y.,
Toba, Y., Sawicki, M., Gwyn, S., Pflugradt, J.: 2022, The Obscured
Fraction of Quasars at Cosmic Noon, ApJ, 941, 97.
Vioque, M., et al. including Miley, J.: 2022, Identification and Spectroscopic
Characterization of 128 New Herbig Stars, ApJ, 930, 39.
Vollmer, B., Davies, R. I., Gratier, P., Lizee, T., Imanishi, M., Gallimore,
J. F., Impellizzeri, C. M. V., Garcia-Burillo, S., Le Petit, F.: 2022,
From the Circumnuclear Disk in the Galactic Center to thick,obscuring tori of AGNs Modeling the molecular emission of a parsecscale torus as found in NGC 1068, A&A, 665, A102.
Wang, F., Fujii, Y., He, J. P.: 2022, Unveiling Nongray Surface of Cloudy
Exoplanets: The Influence of Wavelength-dependent Surface Albedo
and Cloud Scattering Properties on Retrieval Solutions, ApJ, 931, 48.
Wang, J. J., Gao, P., Chilcote, J., Lozi, J., Guyon, O., Sahoo, A.,
Vievard, S.: 2022, Atmospheric Monitoring and Precise Spectroscopyof the HR 8799 Planets with SCExAO/CHARIS*, AJ, 164, 143.
Wang, S. L., Kawai, N., Shidatsu, M., Murata, K., Hosokawa, R.,
Hanayama, H., Horiuchi, T., Morihana, K.: 2022, Multi-wavelength
studies of the X-ray binary MAXI J1727-203: constraining systemparameters, MNRAS, 514, 5320–5339.
Wang, W.-H., et al. including Ouchi, M.: 2022, MUSUBI (MegaCam
Ultra-deep Survey: u*-band Imaging) Data for the COSMOS andSXDS Fields, ApJS, 260, 54.
Wang, X. Z., Jiang, W., Shen, Z. Q., Huang, L., Hada, K., Cui, Y. Z., Lu,
R. S.: 2022, Multifrequency VLBI Observations of the M84 Inner Jet/
Counterjet, ApJ, 941, 140.
Washimi, T., et al. including Tomaru, T.: 2022, Response of theunderground environment of the KAGRA observatory against the airpressure disturbance from the Tonga volcanic eruption on January 15,2022, Prog. Theor. Exp. Phys., 2022, 113H02.
Washinoue, H., Shoda, M., Suzuki, T. K.: 2022, The Effect of the
Chromospheric Temperature on Coronal Heating, ApJ, 938, 126.
Watanabe, N., et al. including Kusakabe, N., Nishiumi, T.: 2022, Nodal
precession of WASP-33b for 11 yr by Doppler tomographic andtransit photometric observations, MNRAS, 512, 4404–4418.
Watkins, E. J., et al. including Saito, T.: 2023, PHANGS–JWST First
Results: A Statistical View on Bubble Evolution in NGC 628, ApJL,
944, L24.
Welch, B., et al. including Ouchi, M.: 2022, JWST Imaging of Earendel,
the Extremely Magnified Star at Redshift z=6.2, ApJL, 940, L1.
Wielgus, M., et al. including Akiyama, K., Cui, Y., Hada, K., Honma,
M., Kino, M., Moriyama, K., Nagai, H., Okino, H., Oyama, T.,
Sasada, M., Tazaki, F., Ikeda, S., Kofuji, Y.: 2022, Millimeter Light
Curves of Sagittarius A* Observed during the 2017 Event Horizon

160

XIII Publications, Presentations

Telescope Campaign, ApJL, 930, L19.
Williams, B. A., et al. including Lu, X.: 2022, The initial conditions foryoung massive cluster formation in the Galactic Centre: convergenceof large-scale gas flows, MNRAS, 514, 578–595.
Wisniewski, J. P., et al. including Tamura, M.: 2022, UV spectropolarimetry
with Polstar: protoplanetary disks, Astrophys. Space Sci., 367, 122.
Wong, K. C., Chan, J. H. H., Chao, D. C. Y., Jaelani, A. T., Kayo, I., Lee,C. H., More, A., Oguri, M.: 2022, Survey of Gravitationally lensed
objects in HSC Imaging (SuGOHI). VIII. New galaxy-scale lenses
from the HSC SSP, PASJ, 74, 1209–1219.
Wong, T., et al. including Tokuda, K.: 2022, The 30 Doradus Molecular
Cloud at 0.4 pc Resolution with the Atacama Large Millimeter/
submillimeter Array: Physical Properties and the Boundedness of
CO-emitting Structures, ApJ, 932, 47.
Wright, M., Hirota, T., Forbrich, J., Plambeck, R., Bally, J., Goddi, C.,
Ginsburg, A., McGuire, B.: 2023, An Ionized Outflow in Orion-KL
Source I?, ApJ, 945, 14.
Xiao, M. Y., et al. including Iono, D., Lu, X.: 2022, Starbursts with
suppressed velocity dispersion revealed in a forming cluster at z =2.51, A&A, 664, A63.
Xu, X. F., et al. including Sugahara, Y., Ouchi, M.: 2022, CLASSY III.
The Properties of Starburst-driven Warm Ionized Outflows*, ApJ,
933, 222.
Xu, Y., Ouchi, M., Rauch, M., Nakajima, K., Harikane, Y., Sugahara,Y., Komiyama, Y., Kusakabe, H., Fujimoto, S., Isobe, Y., Kim, J. H.,
Ono, Y., Zahedy, F. S.: 2022, EMPRESS. VI. Outflows Investigatedin Low-mass Galaxies with M* =104–107 M⊙: Weak Feedback in
Low-mass Galaxies?, ApJ, 929, 134.
Yabuta, H., et al. including Namiki, N., Matsumoto, K., Noda, H.,
Kikuchi, S.: 2023, Macromolecular organic matter in samples of theasteroid (162173) Ryugu, Science, 379, 790.
Yamada, R. I., Fukui, Y., Sano, H., Tachihara, K., Bieging, J. H.,
Enokiya, R., Nishimura, A., Fujita, S., Kohno, M., Tsuge, K.:
2022, Evidence for a cloud-cloud collision in Sh2-233 triggering
the formation of the high-mass protostar object IRAS 05358+3543,
MNRAS, 515, 1012–1025.
Yamada, R., Yamamoto, K., Oshigami, S., Araki, H., Senshu, H., Noda,
H., Namiki, N., Matsumoto, K., Yoshida, F.: 2022, Derivation of
1.064 μm normal albedos on the C-type asteroid Ryugu from laser
pulse intensity measurement of the Hayabusa2 LIDAR, Earth Planets
Space, 74, 166.
Yamamoto, H., Okamoto, R., Murata, Y., Nakanishi, H., Imai, H.,
Kurahara, K.: 2022, Physical properties of the molecular cloud, N4,
in SS 433: Evidence for an interaction of molecular cloud with the jetfrom SS 433, PASJ, 74, 493–509.
Yamato, Y., Furuya, K., Aikawa, Y., Persson, M. V., Tobin, J. J.,
Jorgensen, J. K., Kama, M.: 2022, The First InterferometricMeasurements of NH2D/NH3 Ratio in Hot Corinos, ApJ, 941, 75.
Yamazaki, Y., He, Z. Y., Kajino, T., Mathews, G. J., Famiano, M. A.,
Tang, X. D., Shi, J. R.: 2022, Possibility to Identify the Contributions
from Collapsars, Supernovae, and Neutron Star Mergers from the
Evolution of the r-process Mass Abundance Distribution, ApJ, 933,
112.
Yang, H. J., et al. including Koshimoto, N.: 2022, KMT-2021-BLG0171Lb and KMT-2021-BLG-1689Lb: two microlensing planetsin the KMTNet high-cadence fields with followup observations,MNRAS, 516, 1894–1909.
Yang, L., et al. including Yamaguchi, H.: 2022, Breakup of the proton
halo nucleus B-8 near barrier energies, Nat. Commun., 13, 7193.
Yang, Y., et al. including Ishigaki, M. N.: 2022, Existence of tidal tails
for the globular cluster NGC 5824, A&A, 667, A37.
Yang, Y., Zhao, J. K., Ishigaki, M. N., Zhou, J. Z., Yang, C. Q., Xue, X.
X., Ye, X. H., Zhao, G.: 2022, Revisit NGC 5466 tidal stream with
Gaia, SDSS/SEGUE, and LAMOST, MNRAS, 513, 853–863.
Yasui, C., Kobayashi, N., Saito, M., Izumi, N., Ikeda, Y.: 2023, Mass
Function of a Young Cluster in a Low-metallicity Environment. Sh
2-209, ApJ, 943, 137.
Yen, H. W., Koch, P. M., Lee, C. F., Hirano, N., Ohashi, N., Sai, J.,
Takakuwa, S., Tang, Y. W., Tatematsu, K., Zhao, B.: 2023, Increasing
Mass-to-flux Ratio from the Dense Core to the Protostellar Envelope
around the Class 0 Protostar HH 211, ApJ, 942, 32.
Yokoi, N., Masada, Y., Takiwaki, T.: 2022, Modelling stellar convective
transport with plumes - I. Non-equilibrium turbulence effect indouble-averaging formulation, MNRAS, 516, 2718–2735.
Yokoyama, T., et al. including Matsumoto, K., Namiki, N., Noda, H.:
2023, Samples returned from the asteroid Ryugu are similar to Ivunatype carbonaceous meteorites, Science, 379, 786.
Yonekura, N., Kajisawa, M., Hamaguchi, E., Mawatari, K., Yamada, T.:
2022, A Search for Massive Galaxy Population in a Protocluster of
LAEs at z=2.39 near the Radio Galaxy 53W002, ApJ, 930, 102.
Yoneta, K., Murakami, N., Koike, R., Nishikawa, J.: 2022, Binarystar Wave Front Control Based on a Common-path Visible NullingCoronagraph, ApJS, 262, 48.
Yoshida, F., et al. including Noda, H.: 2023, Multi-chord observationof stellar occultation by the near-Earth asteroid (3200) Phaethon on
2021 October 3 (UTC) with very high accuracy, PASJ, 75, 153–168.
Yoshida, T. C., Nomura, H., Furuya, K., Tsukagoshi, T., Lee, S.:
2022, A New Method for Direct Measurement of Isotopologue Ratios
in Protoplanetary Disks: A Case Study of the 12CO/13CO Ratio in the
TW Hya Disk, ApJ, 932, 126.
Yoshida, T. C., Nomura, H., Tsukagoshi, T., Furuya, K., Ueda, T.:
2022, Discovery of Line Pressure Broadening and Direct Constraint
on Gas Surface Density in a Protoplanetary Disk, ApJL, 937, L14.
Yoshida, T., Terada, N., Ikoma, M., Kuramoto, K.: 2022, Less Effective
Hydrodynamic Escape of H2-H2O Atmospheres on Terrestrial Planets
Orbiting Pre-main-sequence M Dwarfs, ApJ, 934, 137.
Yoshii, Y., et al. including Tsujimoto, T.: 2022, Potential Signature ofPopulation III Pair-instability Supernova Ejecta in the BLR Gas of
the Most Distant Quasar at z=7.54*, ApJ, 937, 61.
Yoshitake, T., et al. including Maehara, H., OISTER Collaboration:
2022, Multiwavelength observations of the black hole X-ray binary
MAXI J1820+070 in the rebrightening phase, PASJ, 74, 805–814.
Yuan, C., Liu, M., Shimizu, N., Podolyák, Z., Suzuki, T., Otsuka, T.,
Liu, Z.: 2022, Shell-model study on spectroscopic properties in theregion “south” of Pb 208, Phys. Rev. C, 106, 044314.
Yung, L. Y. A., et al. including Behroozi, P.: 2023, Semi-analytic
forecasts for Roman - the beginning of a new era of deep-wide galaxy
surveys, MNRAS, 519, 1578–1600.
Yutani, N., Toba, Y., Baba, S., Wada, K.: 2022, Origin and Evolution of
Dust-obscured Galaxies in Galaxy Mergers, ApJ, 936, 118.
Zang, W. C., et al. including Koshimoto, N.: 2022, OGLE-2018-BLG0799Lb: a q ~ 2.7 × 10−3 planet with Spitzer parallax, MNRAS, 514,

5952–5968.
Zaritsky, D., Behroozi, P.: 2023, Photometric mass estimation and thestellar mass-halo mass relation for low mass galaxies, MNRAS, 519,
871–883.
Zavagno, A., et al. including Arzoumanian, D.: 2023, Supervisedmachine learning on Galactic filaments Revealing the filamentary
structure of the Galactic interstellar medium, A&A, 669, A120.
Zavala, J. A., Casey, C. M., Spilker, J., Tadaki, K., Tsujita, A.,
Champagne, J., Iono, D., Kohno, K., Manning, S., Montana, A.:
2022, Probing Cold Gas in a Massive, Compact Star-forming Galaxy
at z=6, ApJ, 933, 242.
Zavala, J. A., et al. including Behroozi, P., CEERS Team: 2023, Dusty
Starbursts Masquerading as Ultra-high Redshift Galaxies in JWSTCEERS Observations, ApJL, 943, L9.
Zemaitis, R., et al. including Okamoto, S., Arimoto, N.: 2023, A taleof a tail: a tidally disrupting ultra-diffuse galaxy in the M81 group,
MNRAS, 518, 2497–2510.
Zhang, H. W., Behroozi, P., Volonteri, M., Silk, J., Fan, X. H., Hopkins,
P. F., Yang, J. Y., Aird, J.: 2023, Trinity I: self-consistently modellingthe dark matter halo-galaxy-supermassive black hole connection fromz=0–10, MNRAS, 518, 2123–2163.
Zhang, S. J., et al. including Tatematsu, K.: 2023, ATOMS: ALMA
three-millimeter observations of massive star-forming regions - XIII.
Ongoing triggered star formation within clump-fed scenario found in
the massive (~1500 M⊙) clump, MNRAS, 520, 322–352.
Zhang, Y. C., Tanaka, K. E. I., Tan, J. C., Yang, Y. L., Greco, E.,
Beltran, M. T., Sakai, N., De Buizer, J. M., Rosero, V., Fedriani, R.,
Garay, G.: 2022, Massive Protostars in a Protocluster-A Multi-scale
ALMA View of G35.20-0.74N, ApJ, 936, 68.
Zhao, G. Y., et al. including Akiyama, K.: 2022, Unraveling theInnermost Jet Structure of OJ 287 with the First GMVA plus ALMA
Observations, ApJ, 932, 72.
Zhao, Y. H., et al. including Eisenmann, M., Aritomi, N., Page, M.,
Aso, Y., Shoda, A., Takahashi, R., Leonardi, M., Flaminio, R.:
2022, Improving the stability of frequency-dependent squeezing withbichromatic control of filter cavity length, alignment, and incident
beam pointing, Phys. Rev. D, 105, 082003.
Zhou, J.-W., et al. including Tatematsu, K.: 2022, ATOMS: ALMA
Three-millimeter Observations of Massive Star-forming regions - XI.
From inflow to infall in hub-filament systems, MNRAS, 514, 6038–
6052.
Zhou, Y., Mitsuda, K., Yamasaki, N. Y.: 2022, Spatial Power Spectral
Analysis of the Suzaku X-Ray Background, ApJ, 929, 128.

XIII Publications, Presentations161

2. Publications of the National Astronomical 4. Conference Proceedings
Observatory of Japan
Not Published.

3. Report of the National Astronomical
Observatory of Japan (in Japanese)
Nakajima, Y., Ozawa, T., Onozato, H., Mori, Y., Ichikawa, S.-i.: 2022,
Development of SMOKA / Tomo-e Gozen Data Archive System, Rep.
Nat. Astron. Obs. Japan, 23, 1–15.
Ozawa, T., Onozato, H., Nakajima, Y.: 2022, A Study to Speed Up
Searches in the Optical-Infrared Astronomical Observation Data
Archive System, Rep. Nat. Astron. Obs. Japan, 23, 16–44.

162

XIII Publications, Presentations

Ahn, K., Guyon, O., Lozi, J., Vievard, S., Deo, V., Skaf, N., Bragg,J., Haffert, S. Y., Males, J. R., Currie, T.: 2022, Laboratory
demonstrations of EFC and spatial LDFC on Subaru/SCExAO, Proc.
SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121852B.
Aoki, W.: 2022, Stellar elemental abundances constraining
nucleosynthesis and chemical evolution of the universe, EPJ Web ofConf. 260, Eds. W. Liu, Y. Wang, B. Guo, X. Tang, S. Zeng., 07002.
Belikov, R., Sirbu, D., Marx, D., Mejia Prada, C., Bendek, E., Pluzhnik,E., Bryson, S., Kern, B., Guyon, O., Fogarty, K., Knight, J., Wilson,
D., Hagopian, J.: 2022, Laboratory demonstration of high contrast
with the PIAACMC coronagraph on an obstructed and segmented
aperture, Proc. SPIE, 12180, Eds. L. E. Coyle, S. Matsuura, M. D.
Perrin, 1218025.
Blind, N., Chazelas, B., Kühn, J., Hocimi, E., Lovis, C., Beaulieu,
M., Fusco, T., Genolet, L., Guyon, O., Hagelberg, J., Hughes, I.,
Martinez, P., Sauvage, J. -F., Schnell, R., Sordet, M., Spang, A.: 2022,
RISTRETTO: coronagraph and AO designs enabling High Dispersion
Coronagraphy at 2 λ/D, Proc. SPIE, 12185, Eds. L. Schreiber, D.
Schmidt, E. Vernet, 1218573.
Carpenter, J., Brogan, C., Iono, D., Mroczkowski, T.: 2023, The ALMA
Wideband Sensitivity Upgrade, Proceedings of the 7th ChileCologne-Bonn Symposium, Eds. V. Ossenkopf-Okada, et al., 304.
Chaushev, A., Sallum, S., Lozi, J., Martinache, F., Chilcote, J., Groff,T., Guyon, O., Kasdin, N. J., Norris, B., Skemer, A.: 2022, Spectral
differential imaging using kernel phase with CHARIS/SCExAO:
technique performance and current limitations, Proc. SPIE, 12183,
Eds. A. Merand, S. Sallum, J. Sanchez-Bermudez, 121831L.
Cheng, X., Cho, I., Kawashima, T., Kino, M., Zhao, G.-Y., Algaba, J.C., Kofuji, Y., Lee, S.-S., Lee, J.-W., Cheong, W. Y., Jiang, W., Oh,
J.: 2023, Monitoring the Size and Flux Density of Sgr A* during the
Active State in 2019 with East Asian VLBI Network, Galaxies, 11, 46.
Chiong, C.-C., et al. including Nakamura, F., Nishimura, A., Burns, R.
A., Fujii, Y., Kawabe, R., Kameno, S.: 2022, Extended Q-band (eQ)receiver for Nobeyama 45-m Telescope, Proc. SPIE, 12190, Eds. J.
Zmuidzinas, J. Gao, 121900M.
Clénet, Y., et al. including Deo, V.: 2022, The MICADO first light imager
for the ELT: overview of the SCAO module at its final design, Proc.
SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121854S.
Close, L. M., Males, J. R., Durney, O., Coronado, F., Haffert, S. Y.,
Gasho, V., Hedglen, A., Kautz, M. Y., Connors, T. E., Sullivan, M.,
Guyon, O., Noenickx, J.: 2022, The optical and mechanical design forthe 21,000 actuator ExAO system for the Giant Magellan Telescope:
GMagAO-X, Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E.
Vernet, 1218524.
Dainotti, M. G., et al.: 2023, New insights on the Hubble constanttension through the tomography of the Pantheon Plus and Pantheonsamples of SNe Ia, 16th Marcel Grossmann Meeting, Eds. R. Ruffini,
G. Vereshchagin, 3130–3140.
de Oliveira, A. C., et al. including Moritani, Y., Takato, N.: 2022, Prime
Focus Spectrograqph (PFS): fiber optical cable and connector system(FOCCoS) - intergration, Proc. SPIE, 12184, Eds. C. J. Evans, J. J.
Bryant, K. Motohara, 1218474.
de Oliveira, A. C., Gunn, J. E., de Oliveira, L. S., Marrara, L. S., dosSantos, L. H., Rosa, J. A., Ferreira, D., Loomis, C., Lupton, R.,

Moritani, Y., Takato, N., Tamura, N.: 2022, Subaru Night-Sky
Spectrograph (SuNSS): fiber cable construction, Proc. SPIE, 12184,
Eds. C. J. Evans, J. J. Bryant, K. Motohara, 1218472.
Deo, V., Vievard, S., Cvetojevic, N., Ahn, K., Huby, E., Guyon, O.,
Lacour, S., Lozi, J., Martinache, F., Norris, B., Skaf, N., Tuthill,P.: 2022, Controlling petals using fringes: discontinuous wavefront
sensing through sparse aperture interferometry at Subaru/SCExAO,
Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet,
121850Z.
Emont, B., et al. including Kawasaki, W., Miel, R., Nakazato, T.:
2022, The CASA Software for Radio Astronomy: Status Update fromADASS 2020, ASP Conf. Ser., 532, Eds. R. Enrique, F. Pierfedereci, P.
Teuben, 389.
Farinato, J., et al. including Guyon, O.: 2022, SHARK-NIR, readyto “swim” in the LBT Northern Hemisphere “ocean”, Proc. SPIE,
12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 1218522.
Fujii, H. T., Sakaguchi, N., Ona, K., Uraguchi, F., Hayano, Y.,
Yokoyama, T.: 2022, Low thermal expansion at cryogenic
temperature in Fe39−x Co49+x Cr10 Ni2 alloy used for astronomical
telescopes, Proc. SPIE, 12188, Eds. R. Navarro, R. Geyl, 1218806.
Furusawa, H., Takata, T., Shirasaki, Y.: 2022, Towards Reliable andProductive Astronomical Data Archives, ASP Conf. Ser., 532, Eds. R.
Enrique, F. Pierfedereci, P. Teuben, 163–166.
Giovannini, G., et al. including Hada, K., Takamura, M., Kino, M.,
Hirota, T., Honma, M., Kobayashi, H., Nagai, H.: 2023, The Past
and Future of East Asia to Italy: Nearly Global VLBI, Galaxies, 11, 49.
Guyon, O., Ahn, K., Akiyama, M., Currie, T., Deo, V., Hattori, T.,
Kudo, T., Lozi, J., Minowa, Y., Ono, Y., Tamura. M., Vievard, S.,
Skaf, N.: 2022, High contrast and high angular imaging at Subaru
Telescope, Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E.
Vernet, 121856J.
Guyon, O., Norris, B., Martinod, M.-A., Ahn, K., Deo, V., Skaf, N.,
Lozi, J., Vievard, S., Haffert, S. Y., Currie, T., Males, J. R., Wong, A.,
Tuthill, P.: 2022, High contrast imaging at the photon noise limit with
WFS-based PSF calibration, Proc. SPIE, 12185, Eds. L. Schreiber, D.
Schmidt, E. Vernet, 121850E.
Haffert, S. Y., Males, J. R., Close, L. M., Guyon, O., Hedglen, A., Kautz,
M.: 2022, Visible extreme adaptive optics for GMagAO-X with thetriple-stage AO architecture (TSAO), Proc. SPIE, 12185, Eds. L.
Schreiber, D. Schmidt, E. Vernet, 121853D.
Haffert, S. Y., Males, J. R., Van Gorkom, K., Close, L. M., Long, J.
D., Hedglen, A. D., Ahn, K., Guyon, O., Schatz, L., Kautz, M.,
Lumbres, J., Rodack, A., Knight, J. M., Sun, H., Fogarty, K., Miller,
K.: 2022, Advanced wavefront sensing and control demonstration
with MagAO-X, Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E.
Vernet, 1218581.
Harada, N., Martín, S., Mangum, J., Alchemi Collaboration: 2023,
Chemistry and molecular cloud properties in nearby galaxies, Proc.
7th Chile-Cologne-Bonn Symp., Eds. V. Ossenkopf-Okada et al., 225.
Hatsumi, S., Nakamura, M., Numata, C., Kurokura, T., Kodama, Y.,
Kamei, Y., Yamamoto, H., Hayano, Y., Hattori, M., Tamada, Y.:
2022, Measurement and control of optical disturbance in living cells
and tissues, Optics & Photonics International Congress 2022, Eds. O.
Matoba, S. Gigan, SI-Thru6-04.
Hattori, M., Tamada, Y., Miura, N.: 2022, Chloroplasts as the Guide
Stars; Possibility for the Use of Absorbing Contrast with Scene-

Based Adaptive Optics Microscope, Optics & Photonics International
Congress 2022, Eds. O. Matoba, S. Gigan, SI-Thru6-09.
Hattori, T., Minowa, Y., Okita, H., Rousselle, J., Yoshida, M.: 2022,
Instrumentation at the Subaru Telescope, Proc. SPIE, 12184, Eds. C. J.
Evans, J. J. Bryant, K. Motohara, 1218402.
Hayashi, Y., Nakazato, T., Morita, E., Kosugi, G., Ezawa, H.,
Sugimoto, K.: 2022, Automated System to Generate Calibrated
MeasurementSet in East Asian ALMA Regional Center, ASP Conf.
Ser., 532, Eds. R. Enrique, F. Pierfedereci, P. Teuben, 579.
Hedglen, A. D., et al. including Guyon, O.: 2022, First lab results ofsegment/petal phasing with a pyramid wavefront sensor and a novel
holographic dispersed fringe sensor (HDFS) from the Giant Magellan
Telescope high contrast adaptive optics phasing testbed, Proc. SPIE,
12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 1218516.
Honda, S., Murayama, Y., Nitta, T., Nagai, M., Miyazawa, H., Noji,
R., Mandal, P., Kuno, N., Matsuo, H., Sekimoto, Y., Nakai, N.:
2022, Development and Commissioning of 100 GHz Microwave
Kinetic Inductance Detector (MKID) Camera at the Nobeyama 45 m
Telescope, URSI Radio Sci. Lett., 4, 53.
Iglesias, F. A., et al. including Katsukawa, Y., Kubo, M.: 2022,
Polarimetric calibration of the Sunrise UV Spectropolarimeter andImager, Boletín de la Asociación Argentina de Astronomía, 63, 305–
307.
Inoue, A. K., Kaneda, H., Yamada, T., Harikane, Y., Ishihara, D.,
Kodama, T., Komiyama, Y., Moriya, T., Motohara, K., Nomura,
H., Ouchi, M., Oyabu, S., Suzuki, T., Wada, T., Yamamura, I.: 2022,
GREX-PLUS: galaxy reionization explorer and planetary universe
spectrometer, Proc. SPIE, 12180, Eds. L. E. Coyle, S. Matsuura, M. D.
Perrin, 121801I.
Jensen-Clem, R., Hinz, P. M., van Kooten, M. A. M., Fitzgerald, M. P.,
Sallum, S., Mazin, B. A., Chun, M., Millar-Blanchaer, M. A., Skemer,
A., Wang, J., Stelter, R. D., Guyon, O.: 2022, An updated preliminary
optical design and performance analysis of the Planetary Systems
Imager adaptive optics system, Proc. SPIE, 12185, Eds. L. Schreiber,
D. Schmidt, E. Vernet, 1218546.
Kamizuka, T., et al. including Koshida, S., Motohara, K.: 2022,
Development status of TAO/MIMIZUKU: performance test of thenear-infrared channel, Proc. SPIE, 12184, Eds. C. J. Evans, J. J.
Bryant, K. Motohara, 121845J.
Katsukawa, Y., Hara, H., Kubo, M., Kawabata, Y., Oba, T.,
Piqueras Carreño, J., Pérez Grande, I., Shinoda, K., Tamura, T.,
Uraguchi, F., Tsuzuki, T., Nodomi, Y., Shimizu, T., López Jiménez,A. C., Balaguer Jiménez, M., Álvarez García, D.: 2022, Sunrise
chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III:
thermal-vacuum test of the SCIP optical unit, Proc. SPIE, 12184, Eds.
C. J. Evans, J. J. Bryant, K. Motohara, 121842B.
Kawabata, Y., Katsukawa, Y., Tsuzuki, T., Uraguchi, F., Mitsui,K., Shinoda, K., Tamura, T., Nodomi, Y., Hara, H., Kubo, M.:
2022, Optical alignment and performance evaluation of the Sunrise
Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE
III, Proc. SPIE, 12184, Eds. C. J. Evans, J. J. Bryant, K. Motohara,
1218427.
Keszthelyi, Z.: 2023, Magnetism in High-Mass Stars, Galaxies, 11, 40.
Kim, Y. J., Sallum, S., Lin, J., Xin, Y., Norris, B., Betters, C., LeonSaval, S., Lozi, J., Vievard, S., Gatkine, P., Guyon, O., Jovanovic,
N., Mawet, D., Fitzgerald, M. P.: 2022, Spectroastrometry withXIII Publications, Presentations

163

photonic lanterns, Proc. SPIE, 12184, Eds. C. J. Evans, J. J. Bryant, K.
Motohara, 1218449.
Krishnamoorthy, P., Walawender, J., Gee, W. T., Guyon, O.: 2022,
Project PANOPTES: A Student Led Search for Exoplanets from Your
Backyard, ASP Conf. Ser., 533, Eds. G. Schultz, J. B. Jensen, L.
Shore, 217.
Kushibiki, K., Ozaki, S., Takeda, M., Hosobata, T., Yamagata, Y.,
Morita, S., Nakagawa, K., Saiki, T., Ohtake, Y., Tsuzuki, T., Mitsui,K., Okita, H., Motohara, K., Takahashi, H., Konishi, M., Kato, N.,
Koyama, S., Chen, N., Homan, S., Yasuda, A.: 2022, Development
status of a near-infrared integral field unit SWIMS-IFU, Proc. SPIE,
12188, Eds. R. Navarro, R. Geyl, 121882V.
Lallement, M., Lacour, S., Huby, E., Martin, G., Barjot, K., Perrin, G.,
Rouan, D., Lapeyrere, V., Vievard, S., Guyon, O., Lozi, J., Deo, V.,
Kotani, T., Pham, C., Cassagnettes, C., Billat, A., Cvetojevic, N.,
Marchis, F.: 2022, Photonic chip for visible interferometry: laboratory
characterization and comparison with the theoretical model, Proc.
SPIE, 12188, Eds. R. Navarro, R. Geyl, 121882F.
Lin, J., Vievard, S., Jovanovic, N., Norris, B., Fitzgerald, M. P., Betters,C., Gatkine, P., Guyon, O., Kim, Y. J., Leon-Saval, S., Lozi, J.,
Mawet, D., Sallum, S., Xin, Y.: 2022, Experimental measurementsof AO-fed photonic lantern coupling efficiencies, Proc. SPIE, 12188,
Eds. R. Navarro, R. Geyl, 121882E.
Lin, J., Xin, Y., Norris, B., Kim, Y. J., Sallum, S., Betters, C., LeonSaval, S., Lozi, J., Vievard, S., Guyon, O., Gatkine, P., Jovanovic,
N., Mawet, D., Fitzgerald, M. P.: 2022, Exoplanet detection withphotonic lanterns for focal-plane wavefront sensing and control, Proc.
SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121852G.
Lovis, C., Blind, N., Chazelas, B., Kühn, J. G., Genolet, L., Hughes,
I., Sordet, M., Schnell, R., Turbet, M., Fusco, T., Sauvage, J.-F.,
Bugatti, M., Billot, N., Hagelberg, J., Hocini, E., Guyon, O.: 2022,
RISTRETTO: high-resolution spectroscopy at the diffraction limitof the VLT, Proc. SPIE, 12184, Eds. C. J. Evans, J. J. Bryant, K.
Motohara, 121841Q.
Lozi, J., Ahn, K., Clergeon, C., Deo, V., Guyon, O., Hattori, T.,
Minowa, Y., Nishiyama, S., Ono, Y., Vievard, S.: 2022, AO3000 at
Subaru: combining for the first time a NIR WFS using First Light's
C-RED ONE and ALPAO's 64x64 DM, Proc. SPIE, 12185, Eds. L.
Schreiber, D. Schmidt, E. Vernet, 1218533.
Lucas, M., Bottom, M., Guyon, O., Lozi, J., Norris, B., Deo, V.,
Vievard, S., Ahn, K., Skaf, N., Tuthill, P.: 2022, A visible-light Lyot
coronagraph for SCExAO/VAMPIRES, Proc. SPIE, 12184, Eds. C. J.
Evans, J. J. Bryant, K. Motohara, 121844E.
Maehara, H.: 2023, Spectroscopic classification of PNV
J06245297+0208207 as a helium dwarf nova, The Astronomer's
Telegram, 15849.
Males, J. R., Close, L. M., Haffert, S. Y., Guyon, O., Gasho, V.,
Coronado, F., Durney, O., Hedglen, A., Kautz, M., Noenickx, J.,
Ford, J., Connors, T., Kelly, D.: 2022, The conceptual design of
GMagAO-X: visible wavelength high contrast imaging with GMT,
Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet,
121854J.
Males, J. R., et al. including Guyon, O.: 2022, MagAO-X: current status
and plans for Phase II , Proc. SPIE, 12185, Eds. L. Schreiber, D.
Schmidt, E. Vernet, 1218509.
Martin, G., Foin, M., Phatak, S., Beldjoudi, M., Billat, A., Cassagnettes,

164

XIII Publications, Presentations

C., Coste, A., Courjal, N., Lallement, M., Barjot, K, Cvetojevic,
N., Vievard, S., Huby, E., Lacour, S., Deo, V., Guyon, O.: 2022,
Hybrid electro-optic visible multi-telescope beam combiner for next
generation FIRST/SUBARU instruments, Proc. SPIE, 12188, Eds. R.
Navarro, R. Geyl, 121885Y.
Martin, G., Morand, A., d'Amico, C., Stoian, R., Barjot, K., Lallement,
M., Cvetojevic, N., Vievard, S., Huby, E., Lacour, S., Deo, V.,
Guyon, O., Lv, J., Zhang, G., Cheng, G.: 2022, FIRST 5T 3D: alaser written device for FIRST/SUBARU reducing crosstalk andpropagation losses, Proc. SPIE, 12188, Eds. R. Navarro, R. Geyl,
121882T.
Martinache, F., Cvetojevic, N., Deo, V.: 2022, Fizeau-interferometry
fringe tracking solutions for giant segmented telescope petal modes,
Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet,
121851A.
Martinez, N., Herrald, N., Chandler, D., Haynes, D., Kruse, A.,
Ramasundara, W., Rigaut, F., Bernard, J.T., Travouillon, T., Vaughn, I.,
Minowa, Y., Ono, Y., Tanaka, Y., Terao, K., D'Orgeville, C.: 2022,
Wavefront sensing over a 20-arcmin field in the ULTIMATE-Subaru
Ground Layer Adaptive Optics system, Proc. SPIE, 12185, Eds. L.
Schreiber, D. Schmidt, E. Vernet, 121856K.
Martinez, N., Kruse, A., Herrald, N., Chandler, D., Haynes, D., Rigaut,
F., Bernard, J. T., Travouillon, T., Vaughn, I., Minowa, Y., Ono, Y.,
Tanaka, Y., Terao, K., D'Orgeville, C.: 2022, Preliminary designof the Laser Guide Star Facility for the ULTIMATE-Subaru Ground
Layer Adaptive Optics system, Proc. SPIE, 12185, Eds. L. Schreiber,
D. Schmidt, E. Vernet, 121857G.
Martinod, M.-A., et al. including Guyon, O., Lozi, J.: 2022, Achromaticnulling interferometry and fringe tracking with 3D-photonic
tricouplers with GLINT, Proc. SPIE, 12183, Eds. A. Merand, S.
Sallum, J. Sanchez-Bermudez, 121830K.
Minowa, Y., et al. including Ono, Y., Tanaka, Y., Yoshida, H., Terao,
K., Koyama, Y., Ali, S., Tanaka, I., Hattori, T., Okita, H., Hayano,Y., Oya, S., Motohara, K., Yanagisawa, K., Yoshida, M.: 2022,
ULTIMATE-Subaru: GLAO preliminary design overview, Proc.
SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 1218521.
Miyata, T., et al. including Motohara, K.: 2022, The University of Tokyo
Atacama Observatory 6.5 m telescope: project status 2022, Proc.
SPIE, 12182, Eds. H. K. Marshall, J. Spyromillio, T. Usuda, 1218211.
Nakamura, K.: 2022, Quantum Noise in Balanced Homodyne
Detection by Numbers or Power Counting Multi-Mode Detectors
and Vacuum Fluctuations, The 29th KAGRA face to face meeting,
JGW-G221407-2.
Nakamura, K.: 2022, Gauge-invariant perturbation theory on the
Schwarzschild background spacetime including l=0,1 modes —Realization of exact solutions —, Proc. 31th workshop on General
Relativity and Gravitation in Japan.
Nakano, R., Takakura, H., Sekimoto, Y., Inatani, J., Sugimoto, M.,
Oguri, S., Matsuda, F.: 2022, A holographic phase-retrieval methodof aperture-field evaluation for bolometer-array-equipped radio
telescopes, Proc. SPIE, 12190, Eds. J. Zmuidzinas, J. Gao, 121901S.
Nakazato, T., Sugimoto, K., Yoshino, A., Ezawa, H., Hayashi, Y.,
Kosugi, G., Maekawa, J., Takahashi, S., Tatematsu, K.: 2022,
Pipeline Calibration and Imaging for the Nobeyama 45 m Radio
Telescope, ASP Conf. Ser., 532, Eds. R. Enrique, F. Pierfedereci, P.
Teuben, 397.

Norris, B. R. M., Martinod, M.-A., Tuthill, P., Gross, S., Cvetojevic, N.,
Jovanovic, N., Lagadec, T., Klinner-teo, T., Guyon, O., Lozi, J., Deo,
V., Vievard, S., Arriola, A., Gretzinger, T., Lawrence, J. S., Withford,
M. J.: 2022, Optimal self-calibration and fringe tracking in photonic
nulling interferometers using machine learning, Proc. SPIE, 12183,
Eds. A. Merand, S. Sallum, J. Sanchez-Bermudez, 121831J.
Norris, B. R. M., Wei, J., Betters, C. H., Leon-Saval, S. G., Xin, Y., Lin,J., Kim, Y. J., Sallum, S., Lozi, J., Vievard, S., Guyon, O., Gatkine,P., Jovanovic, N., Mawet, D., Fitzgerald, M. P.: 2022, Demonstrationof a photonic-lantern focal-plane wavefront sensor using fiber mode
conversion and deep learning, Proc. SPIE, 12185, Eds. L. Schreiber,
D. Schmidt, E. Vernet, 1218530.
Ogane, H., Akiyama, M., Cranney, J., Rigaut, F., Martinez Rey, N.,
D'Orgeville, C., Minowa, Y., Ono, Y.: 2022, Aliasing effect of rolling
shutter readout in laser guide star wavefront sensing, Proc. SPIE,
12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121850N.
Olivares, S. R., Lopez, R. L., Collados, M., Dominguez-Tagle, C., PerezGarcia, A., Quintero Noda, C., Suematsu, Y., Barreto, M.: 2022,
Development of a 35-micron slicer-based Integral Field Unit for
high-resolution 2D solar spectroscopy, Proc. SPIE, 12188, Eds. R.
Navarro, R. Geyl, 1218855.
Oya, S., Minowa, Y., Okita, H., Ono, Y., Clergeon, C.: 2022,
ULTIMATE-Subaru: adaptive secondary mirror system, Proc. SPIE,
12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121857T.
Safonov, B., Millar-Blanchaer, M., Zhang, M., Norris, B. R., Guyon,
O., Lozi, J., Sallum, S.: 2022, Differential speckle polarimetry
with SCExAO VAMPIRES, Proc. SPIE, 12183, Eds. A. Merand, S.
Sallum, J. Sanchez-Bermudez, 121832C.
Sakabe, K., Ikeda, Y., Oya, S., Bessho, T., Kojima, R., Komaki, M.,
Jun, T., Kawakita, H.: 2022, The adaptive optics simulation andimprovement plan of CRAO attached to the 1.3m Araki Telescope,Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet,
121853N.
Sakurai, T.: 2022, Probability Distribution Functions of Solar and Stellar
Flares, Physics, 5, 11–23.
Sakurai, T., Hotta, H., Imada, S.: 2023, Eleven-Year Cycle of Solar
Magnetic Activity: Observations, Theories, and Numerical Model
Predictions, Solar-Terrestrial Environmental Prediction, Ed. K.
Kusano, 379–401.
Sallum, S., Millar-Blanchaer, M. A., Batalha, N., Wang, J., Martinez, R.,
Fitzgerald, M. P., Skemer, A., Jensen-Clem, R., Mazin, B. A., Chun,
M., Guyon, O., Hinz, P., Males, J., Max, C.: 2022, The Planetary
Systems Imager for TMT: driving science cases and top level
requirements, Proc. SPIE, 12184, Eds. C. J. Evans, J. J. Bryant, K.
Motohara, 1218446.
Shirasaki, Y., Zapart, C., Ohishi, M., Mizumoto, Y.: 2022, JVO
Subaru Suprime-Cam Mosaic Image Archive DR2, ASP Conf. Ser.,532, Eds. R. Enrique, F. Pierfedereci, P. Teuben, 567–570.
Skaf, N., Guyon, O., Boccaletti, A., Gendron, E., Deo, V., Vievard, S.,
Lozi, J., Ahn, K., Currie, T.: 2022, Imaged-based adaptive optics
wavefront sensor referencing for high contrast imaging, Proc. SPIE,
12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121851U.
Smee, S. A., Gunn, J. E., Barkhouser, R. H., Peebles, J., Loomis, C. P.,
Dohlen, K., Kado-Fong, E., Givans, J. J., Golebiowski, M., Gray, A.,
Hammond, R. P., Hope, S., C., Lupton, R., Moritani, Y., Tamura,N.: 2022, Performance of the near-infrared camera for the Subaru

Prime Focus Spectrograph, Proc. SPIE, 12184, Eds. C. J. Evans, J. J.
Bryant, K. Motohara, 121847L.
Steidel, C., et al. including Uraguchi, F., Ozaki, S.: 2022, Design anddevelopment of WFOS, the Wide-Field Optical Spectrograph for theThirty Meter Telescope, Proc. SPIE, 12184, Eds. C. J. Evans, J. J.
Bryant, K. Motohara, 1218423.
Suda, T., Saitoh, T. R., Moritani, Y., Matsuno, T., Shigeyama, T.: 2022,
Massive first star binaries as new tools for Galactic archaeology, EPJ
Web of Conf. 260, Eds. W. Liu, Y. Wang, B. Guo, X. Tang, S. Zeng.,
11042.
Suematsu, Y., Iju, T., Shinoda, K., Hagino, M., Ueno, S.: 2022,
LiNbO3 Fabry-Perot etalons for solar near-infrared narrow-passband
tunable filtergraph, Proc. SPIE, 12235, Eds. E. J. Ientilucci, C. L.
Bradley, 1223507.
Sugimoto, M., Kato, A., Takaki, J., Tabata, M., Hattori, T., Sadjadpour,A., Espeland, B., Thompson, H., Sofuku, S., Ezaki, Y., Kawaguchi,N., Usuda, T., Kusumoto, H., Saito, M., Terada, H., Tazawa, S.,
Kinoshita, K.: 2022, Seismic isolation system design and performanceof TMT telescope structure, Proc. SPIE, 12182, Eds. H. K. Marshall, J.
Spyromillio, T. Usuda, 1218216.
Takakura, H., Nakano, R., Sekimoto, Y., Inatani, J., Sugimoto, M.,
Matsuda, F., Oguri, S.: 2022, Straylight identification of a crossedDragone telescope by time-gated near-field antenna patternmeasurements, Proc. SPIE, 12180, Eds. L. E. Coyle, S. Matsuura, M.
D. Perrin, 1218052.
Takeda, M., Kushibiki, K., Hosobata, T., Yamagata, Y., Morita, S., Saiki,T., Nakagawa, K., Ohtake, Y., Motohara, K., Ozaki, S., Tsuzuki, T.,
Takahashi, H., Konishi, M.: 2022, Diamond machining of two-in-one
optical element including slice mirror array for near-infrared integralfield spectrograph, Proc. SPIE, 12188, Eds. R. Navarro, R. Geyl,
121882X.
Tamura, N., et al. including Moritani, Y., Ishizuka, Y., Kamata, Y.,
Arai, A., Furusawa, H., Hamano, S., He, W., Ishigaki, M. N.,
Jeschke, E., Kawanomoto, S., Koike, M., Koshida, S., Mineo, S.,
Miyazaki, S., Morishima, T., Murata, K., Okita, H., Onodera,
M., Pyo, T.-S., Ramos, L., Rousselle, J. P., Schubert, K., Takagi,Y., Tanaka, M., Tanaka, Y., Wung, M., Yoshida, H., Yoshida, M.,
Yamashita, T.: 2022, Prime Focus Spectrograph (PFS) for the Subaru
Telescope: its start of the last development phase, Proc. SPIE, 12184,
Eds. C. J. Evans, J. J. Bryant, K. Motohara, 1218410.
Tanaka, Y., Minowa, Y., Ono, Y., Terao, K., Yoshida, H., Akiyama,
M., Rey, N. M., Herrald, N., d'Orgeville, C., Rigaut, F., Vaughn, I.,
Chandler, D., Haynes, D., Schofield, W.: 2022, Optical design of the
wavefront sensing in the ULTIMATE-Subaru Ground Layer Adaptive
Optics system, Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E.
Vernet, 121856M.
Tazaki, F,. et al. including Hada, K., Kino, M., Akiyama, K., Honma,
M.: 2023, Super-Resolved Image of M87 Observed with East AsianVLBI Network, Galaxies, 11, 39.
Terao, K., Akiyama, M., Minowa, Y., Ono, Y., Ogane, H., Akasawa, T.,
Oya, S., Yamamuro, T.: 2022, ULTIMATE-START: current status of
the Subaru Tomography Adaptive optics Research experimenT, Proc.
SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121856L.
Tobin, T. L., Pal, J., Chilcote, J., Brandt, T., Currie, T., Groff, T., Lozi,J., Guyon, O.: 2022, Status of the Automated Data Extraction,
Processing, and Tracking System (ADEPTS) for CHARIS/SCExAO,XIII Publications, Presentations165

Proc. SPIE, 12189, Ed. J. Ibsen, 121892C.
Tokoku, C., Ozaki, S., Moriya, T., Yanagisawa, K., Motohara, K.,
Ouchi, M., Tominaga, N., Tanaka, M., Ono, Y., Minowa, Y.,
Hayano, Y., Koyama, Y., Ali, S., Tanaka, M., Akiyama, M., Nagao,T., Matsuoka, Y., Kushibiki, K., Homan, S., Yasuda, A., Yoshida,M.: 2022, NINJA: an LTAO assisted optical and near-infrared
spectrograph of Subaru Telescope, Proc. SPIE, 12184, Eds. C. J.
Evans, J. J. Bryant, K. Motohara, 121847R.
Tsunetoe, Y., Mineshige, S., Kawashima, T., Ohsuga, K., Akiyama, K.,
Takahashi, H. R.: 2022, Diverse Polarimetric Features of AGN Jets
from Various Viewing Angles: Towards a Unified View, Galaxies, 10,103.
Tsutsumi, T., et al. including Nishimura, A., Miyazawa, C., Oyama,T., Kaneko, H.: 2023, HINOTORI and Its Perspectives in the BlackHole Jet Study, Galaxies, 11, 30.
Tsuzuki, T., Katsukawa, Y., Uraguchi, F., Kawabata, Y., Hara,
H., Kubo, M., Nodomi, Y., Suematsu, Y., Shimizu, T.: 2022,
Development of an optical system for near-infrared spectropolarimeter
onboard SUNRISE balloon-borne solar observatory, 13th Int. Conf.
“Optics-photonics Design & Fabrication”, Eds. Optics Design Groupof The Optical Society of Japan, 108–109. (P-Oth-20)
Uraguchi, F., Hayano, Y., Ikenoue, B., Mukae, S., Saito, S., Tanaka, Y.,
Uchiyama, M., Suzuki, R.: 2022, The Infrared Imaging Spectrograph(IRIS) for TMT: low wavefront error and highly reflective mirror,
Proc. SPIE, 12184, Eds. C. J. Evans, J. J. Bryant, K. Motohara,
121843D.
Usuda-Sato, K., Suzuki, Y., Kawashima, S., Goko, Y., Inoue, T.: 2022,
Dissemination of the “Touch the Universe” Tactile Exhibition,
Proc. 2nd Workshop on Astronomy Beyond the Common Senses
for Accessibility and Inclusion (2WAI) in the Revista Mexicana de
Astronomía y Astrofísica - Serie de Conferencias, Eds. Vargas, S.,
García, B., Hemming, G., Duffau, S., Vázques, N., Pérez, A., 57–60.
Vidal, F., Galland, N., Bertrou-Cantou, A., Gendron, E., Deo, V., Zidi,
A., Ferreira, F., Sevin, A., Kulscar, C., Raynaud, H.-F., Clenet, Y.,
Davies, R.: 2022, The MICADO first light imager for the ELT: FDR
numerical simulations for the SCAO mode, Proc. SPIE, 12185, Eds. L.
Schreiber, D. Schmidt, E. Vernet, 121855O.
Vievard, S. B., Bonnefois, A., Cassaing, F., Mugnier, L. M., Sauvage, J.
F., Guyon, O., Lozi, J., Deo, V., Ahn, K., Skaf, N.: 2022, Linearized
Analytical Phase Diversity: towards lab and on-sky demonstrationon the Subaru Telescope, Proc. SPIE, 12185, Eds. L. Schreiber, D.
Schmidt, E. Vernet, 121850W.
Vievard, S. B., Deo, V., Huby, E., Lacour, S., Guyon, O., Cvetojevic, N.,
Barjot, K., Martin, G., Lallement, M., Lozi, J., Kotani, T., Marchis,F., Rouan, D., Ahn, K., Skaf, N., Perrin, G.: 2022, Interferometricwavefront sensing at FIRST/SCExAO: self-calibrated fibered pupilremapping spectrocopy using a metrology laser source, Proc. SPIE,
12185, Eds. L. Schreiber, D. Schmidt, E. Vernet, 121830R.
Wang, S.-Y., et al. including Moritani, Y., Rousselle, J., Yoshida, H.,
Koshida, S., Takato, N.: 2022, Prime focus spectrograph (PFS) for
the Subaru Telescope: the prime focus instrument, Proc. SPIE, 12184,
Eds. C. J. Evans, J. J. Bryant, K. Motohara, 121846R.
Wong, A. P., Norris, B. R. M., Deo, V., Guyon, O., Tuthill, P. G., Lozi,J., Vievard, S., Ahn, K.: 2022, Machine learning for wavefront
sensing, Proc. SPIE, 12185, Eds. L. Schreiber, D. Schmidt, E. Vernet,
121852I.

166

XIII Publications, Presentations

Yoneta, K., Sudo. S., Hayashi, H., Asano, M., Nishikawa, J., Murakami,
N.: 2022, Recent progress of the facility for coronagraphic elemental
technologies (FACET), Proc. SPIE, 12180, Eds. L. E. Coyle, S.
Matsuura, M. D. Perrin, 1218027.
Zheng, J. R., Binos, N., Gillingham, P., McGregor, H., Smedley, S.,
Lawrence, J., Hattori, T., Minowa, Y., Guyon, O.: 2022, Opticaldesign for Subaru Nasmyth Beam Switcher, Proc. SPIE, 12182, Eds.
H. K. Marshall, J. Spyromillio, T. Usuda, 121823E.

5. Publications in English

6. Conference Presentations

Aoki, W., Ishigaki, M. N.: 2023, Feb, Galactic Chemical Evolution,
Astronomical Observation from Metal-Poor Stars to the Solar
System. In: Tanihata, I., Toki, H., Kajino, T. (eds) Handbook of
Nuclear Physics, Springer, Singapore.
Edited by Virginia Trimble and David A. Weintraub (Hayashi, S. is oneof the 37 contributors, all women astronomers): 2022, The Sky is forEveryone, Princeton University Press, US, UK.
Hanaoka, Y., Watanabe, K., Yashiro, S. (ed. K. Kusano): 2023, Originof Solar Storms, Chapter 9 of “Solar-Terrestrial Environmental
Prediction”, Springer, Singapore.
National Astronomical Observatory of Japan: 2022, Handbook of
Scientific Tables, World Scientific Publishing Co. Pte. Ltd. andMaruzen Publishing Co., Ltd., Singapore.

Agata, H.: 2022, The status of light pollution in Japan and its relation toastrotourism, 31st IAU General Assembly, (Busan, Korea, Aug. 2–11,2022).
Agata, H.: 2022, Astronomy Education for All High School Students Changes in Science Education and Challenges for the Future in Japan,
31st IAU General Assembly, (Busan, Korea, Aug. 2–11, 2022).
Agata, H.: 2022, The Awe Factor in Astronomy, 31st IAU General
Assembly, (Busan, Korea, Aug. 2–11, 2022).
Agata, H.: 2022, Current Status of Starry Sky Protection in Japan,
Workshop of “Educational Psychology and Astronomy for Mental
health and Wellbeing", (Ulaanbaatar, Mongolia, May 19–20, 2022).
Agata, H.: 2022, Starry sky poster to hospitals, Global Hands-On
Universe 2022 Conference, (Online, Aug. 22–25, 2022).
Agata, H.: 2022, Astronomy education for all high school students –challenges for the future, 4th Shaw-IAU Workshop on Astronomy for
Education, (Online, Nov. 15–17, 2022).
Agata, H., Arai M., Akiyama, H., Yamazaki, N.: 2022, The Current Status
and Potential of Astro-tourism - A Case Study of the Movement inJapan, CAP Conference 2022, (Sydney, Australia, Sept. 12–16, 2022).
Ahn, K., Guyon, O., Lozi, J., Vievard, S., Deo, V., Skaf, N., Bragg,J., Haffert, S. Y., Males, J. R., Currie, T.: 2022, Laboratory
demonstrations of EFC and spatial LDFC on Subaru/SCExAO, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Akahori, T.: 2022, Phoenix rising from the ashes; co-existence of violent
cooling and AGN feedback, 31st IAU General Assembly, (Busan,
Korea, Aug. 2–11, 2022).
Ali, S. S.: 2023, Origin of the excess Ultraviolet light in Early-type
Galaxies: A case of Helium-enhanced stellar populations at late stagesof evolution, AAS meeting #241, (Seattle, WA, USA, Jan. 8–12, 2023).
Antuñano, A., Fletcher, L. N., Orton, G. S., Melin, H., Donnelly, P. T.,
Roman, M. T., Sinclair, J. A., Kasaba, Y., Momary, T., Fujiyoshi, T.:
2022, Jupiter's Equatorial Atmosphere Observations, 16th Europlanet
Science Congress 2022, (Palacio de Congresos de Granada, Spain,
Sep. 18–23, 2022).
Antuñano, A., Fletcher, L., Orton, G., Melin, H., Donnelly, P., Roman,
M., Sinclair, J., Kasaba, Y., Momary, T., Fujiyoshi, T.: 2022, Jupiter'sEquatorial Atmosphere Observations, 44th COSPAR Scientific
Assembly, (Athene, Greece, Jul. 16–24, 2022).
Aoki, W.: 2022, Observational studies of r- and s-process elements for
Milky Way stars, Origin of Matter and Evolution of Galaxies, (Hanoi,
Vietnam, Oct. 24–28, 2022).
Arai, T., et al. including Ito, T.: 2022, Current status of DESTINY+
project and science, JpGU Meeting 2022, (Onsite: Chiba, Japan, May
22–27, 2022, Online: May 29–June 3, 2022).
Arai, T., et al. including Ito, T.: 2023, Current status of DESTINY+ andground-based observations of its target asteroid (3200) Phaethon, The
54th Lunar and Planetary Science Conference (LPSC), (Houston,
USA, Mar. 13–17, 2023).
Araki, H.: 2022, Development of Omni-SLR system (1): opticalsubsystem, 22nd International Workshop on Laser Ranging, (Online,
Nov. 7–11, 2022).
Asanok, K., Gray, M. D., Hirota, T., Sugiyama, K., Phetra, M., Kramer,
B. H., Liu, T., Kim, K. T., Pimpanuwat, B.: 2023, The Dynamics

XIII Publications, Presentations

167

of the Outflow Structure in W49 N, IAU Symposium 380: Cosmic
Masers: Proper Motion toward the Next-Generation Large Projects,(Kagoshima, Japan, Mar. 20–24, 2023).
Aso, Y.: 2022, KAGRA Commissioning Activities, Workshop on thedevelopment of innovative tools for new collaborations within
gravitational wave detection experiments, (Online, Apr. 15, 2022).
Bajpai, R., on behalf of KAGRA collaboration: 2023, Cryogenics in
KAGRA:Present and Future Development, Korean Gravitational
Wave Group Annual Assembly Meeting, (Seoul, Korea/Online, Feb.
15, 2023).
Bautista, J. M., Koda, J., Komiyama, Y., Yagi, M., Yamanoi, H., Boissier,S., Madathodika, J.: 2022, Color of Ultra-Diffuse Galaxies in the Coma
Cluster, AAS Meeting #240, (Pasadena, CA, USA, Jun. 12–16, 2022).
Belikov, R., Sirbu, D., Stark, C., Jewell, J., Guyon, O.: 2023,
Theoretical Performance Limits for Coronagraphs onObstructedand Unobstructed Apertures: How Much CanCurrent Designs be
Improved?, AAS meeting #241, (Seattle, WA, USA, Jan. 8–12, 2023).
Bonev, B., et al. including Ootsubo, T.: 2022, Time-sensitive Keck/NIRSPEC observations of the Rosetta target 67P/ChuryumovGerasimenko during its favorable 2021 apparition, AAS Divisionof Planetary Science meeting #54, (London, Ontario, Canada, andVirtual, Oct. 2–7, 2022).
Cataldi, G.: 2022, Studying the C and CO content of debris disks,
Molecules in Extreme Environments: Near and Far, (Mitaka, Japan,
Nov. 23–25, 2022).
Chaushev, A., Sallum, S., Lozi, J., Martinache, F., Chilcote, J., Groff,T., Guyon, O., Kasdin, N. J., Norris, B., Skemer, A.: 2022, Spectral
differential imaging using kernel phase with CHARIS/SCExAO:
technique performance and current limitations, SPIE Astronomical
Telescopes + Instrumentation, (Montréal, QC, Canada, Jul. 17–22,2022).
Chen, D., on behalf of the KAGRA Calibration subgroup: 2022, Statusof KAGRA calibration, KAGRA f2f meeting, (Online, Nov. 30–Dec,
1, 2022).
Chen, D., Sawada, T., on behalf of the KAGRA Calibration subgroup:2022, KAGRA CAL update, LVK meeting, (Online, Sep. 12–15, 2022).
Currie, T., Guyon, O., Brandt, G., Brandt, T., Chilcote, J., Tobin, T.,
Deo, V., Lozi, J., Vievard, S.: 2022, The SCExAO Direct Imaging
Search for Planets Around Accelerating Stars, Exoplanets IV, (Las
Vegas, NV, USA, May 1–6, 2022).
Currie, T., Lozi, J.: 2022, The SCExAO Direct Imaging Search
for Planets Around Accelerating Stars, Spirit of Lyot, (Leiden,
Netherlands, Jun. 27–Jul. 1, 2022).
Dartez, L., Estevez, D., Chen, D., on behalf of the LIGO, Virgo,
KAGRA calibration groups: 2023, Calibration Update, KAGRA f2f
meeting, (Evanston, IL, USA, Mar. 13–16, 2023).
de Oliveira, A. C., et al. including Moritani, Y., Takato, N.: 2022,
Prime Focus Spectrograqph (PFS): fiber optical cable and connector
system (FOCCoS) - intergration, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
de Oliveira, A. C., Gunn, J. E., de Oliveira, L. S., Marrara, L. S., dosSantos, L. H., Rosa, J. A., Ferreira, D., Loomis, C., Lupton, R.,
Moritani, Y., Takato, N., Tamura, N.: 2022, Subaru Night-Sky
Spectrograph (SuNSS): fiber cable construction, SPIE Astronomical
Telescopes + Instrumentation, (Montréal, QC, Canada, Jul. 17–22,2022).

168

XIII Publications, Presentations

Deepshikha, Nakai, N., Yamazaki, M., Yamauchi, A.: 2023, Study of
Active Galactic Nuclei using water vapor masers, IAU Symposium
380: Cosmic Masers: Proper Motion toward the Next-Generation
Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Demidov, M., Hanaoka, Y., Wang, X., Kirichkov, P.: 2022, On the
Differences in the Space Weather Forecasting Caused by Different
Low Boundary Conditions, 44th COSPAR Scientific Assembly,(Athene, Greece, Jul. 16–24, 2022).
Deo, V., Vievard, S., Cvetojevic, N., Ahn, K., Huby, E., Guyon, O.,
Lacour, S., Lozi, J., Martinache, F., Norris, B., Skaf, N., Tuthill,P.: 2022, Controlling petals using fringes: discontinuous wavefront
sensing through sparse aperture interferometry at Subaru/SCExAO,SPIE Astronomical Telescopes + Instrumentation, (Montréal, QC,
Canada, Jul. 17–22, 2022).
Eisenmann, M., Leonardi M., Wang H., Whao Y.: 2022, A heterodyne
WFS for KAGRA, KAGRA f2f meeting, (Online, Nov. 30–Dec, 1,2022).
Eisenmann, M., Leonardi M., Wang H., Whao Y.: 2023, A newalignment scheme for KAGRA and next gen gravitational waves
detectors, ILANCE International Conference on the Physics of theTwo Infinities, (Kyoto, Japan, Mar. 27–30, 2023).
Eisenmann, M., on behalf of KAGRA MIR: 2022, Characterization of
KAGRA nex ITMs substrates, LVK meeting, (Online, Sep. 12–15,
2022).
Eisenmann, M., on behalf of KAGRA MIR: 2022, Preliminary
characterization of substrates for KAGRA new ITMs, The 29th
KAGRA face to face meeting, (Tokyo, Japan, Aug. 1–3. 2022).
Eisenmann, M., on behalf of KAGRA MIR: 2023, Updates on KAGRA
MIR activities, LVK meeting, (Online, Mar. 13–16, 2023).
Ezaki, S., Shan, W.: 2022, Development of Through-Substrate Vias
Process for Silicon Based Monolithic Microwave Integrated Circuits
SIS Mixer, Applied Superconductivity Conference 2022, (Honolulu,
HI, USA, Oct. 23–28, 2022).
Ezawa, H., Matsuo, H., Fujii, G., Shiki, S., Niwa, A., Okada, N.,
Fukushima, M.: 2022, Design and Performance of the Terahertz
Photon Counting System: Detectors and Cryogenics, 32nd
International Symposium on Space Terahertz Technology, (Baeza
Andalusia, Spain, Oct. 16–20, 2022).
Fraser, W. C. et al. including Ito, T.: 2022, A Successful Machine
Learning Approach to Detecting Kuiper Belt Objects for NASA's
New Horizons Extended Mission, ADASS XXXII, (Online, Oct. 31–
Nov. 4, 2022).
Fraser, W. C. et al. including Ito, T.: 2023, Approaches to Detecting
Kuiper Belt Objects for NASA's New Horizons Extended Mission:
Digging Into the Noise, The 54th Lunar and Planetary Science
Conference (LPSC), (Houston, USA, Mar. 13–17, 2023).
Fukumitsu, K., Katsukawa, Y., Ishikawa, R. T., Ichimoto, K.: 2022,
Image Restoration based on Deep Learning for High-Resolution Solar
Images, IAU Symposium 368: Machine Learning in Astronomy:
Possibilities and Pitfalls, (Busan, Korea, Aug. 2–4, 2022).
Fukumitsu, K., Katsukawa, Y., Ishikawa, R. T., Ichimoto, K.: 2022,
Image Restoration Based on Deep Learning for High-Resolution
Solar Images, Hinode-15/IRIS-12 Multi-messenger physics of thesolar atmosphere, (Prague, Czech Republic, Sep. 19–23, 2022).
Furusawa, H.: 2023, Archive and Science Platform, Subaru Users
Meeting FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).

Furusawa, H.: 2023, WISHES data production, The First SUPERIRNET Workshop - Rebooting Our In-Person Collaboration, (Tokyo,
Japan, Mar. 23–24, 2023).
Furuya, K.: 2022, Chemistry in protoplanetary disks: modelingperspective, Molecules in Extreme Environments: Near and Far,
(Mitaka, Japan, Nov. 23–25, 2022).
Furuya, K.: 2022, Chemistry and transport of volatiles in protoplanetarydisks, Dust, Ice, and Gas Astrochemistry, (Online).
Gouda, N., JASMINE team: 2022, Overview and recent progress of
JASMINE: near-infrared space astrometry mission, 31st IAU General
Assembly, (Busan, Korea, Aug. 2–11, 2022).
Guyon, O., Ahn, K., Akiyama, M., Currie, T., Deo, V., Hattori, T.,
Kudo, T., Lozi, J., Minowa, Y., Ono, Y., Tamura. M., Vievard,
S., Skaf, N.: 2022, High contrast and high angular imaging at
Subaru Telescope, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Guyon, O., Norris, B., Martinod, M. A., Ahn, K., Deo, V., Skaf, N.,
Lozi, J., Vievard, S., Haffert, S. Y., Currie, T., Males, J. R.: 2022,
High contrast imaging at the photon noise limit with WFS-based
PSF calibration, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Hada, K., EHT Collaboration: 2022, Event Horizon Telescope
Observations of M87, 31st IAU General Assembly, (Busan, Korea,
Aug. 2–11, 2022).
Haffert, S. Y., Males, J. R., Van Gorkom, K., Close, L. M., Long, J. D.,
Hedglen, A. D., Ahn, K., Guyon, O., Schatz, L., Kautz, M., Lumbres,J.: 2022, Advanced wavefront sensing and control demonstration
with MagAO-X, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Hanaoka, Y., Sakai, Y., Takahashi, K.: 2022, White-Light Brightness
and Polarization of the Corona Observed During Total Solar Eclipses,
44th COSPAR Scientific Assembly, (Athene, Greece, Jul. 16–24,
2022).
Hanaoka, Y., Sakai, Y., Takahashi, K.: 2022, Polarization of the Corona
Observed During the 2017 and 2019 Total Solar Eclipses, Solar
Polarization Workshop 10, (Kyoto, Japan, Nov. 7–11, 2022).
Harada, N.: 2022, Chemistry and molecular cloud properties in nearby
galaxies, Physics and Chemistry of Star Formation: The Dynamical
ISM Across Time and Spatial Scales, (Puerto-Varas, Chile, Sep.
26–30, 2022).
Harada, N.: 2022, Chemical models for extragalactic environments,
Molecules in Extreme Environments: Near and Far, (Mitaka, Japan,
Nov. 23–25, 2022).
Hattori, T.: 2023, Instrument Report, Subaru Users Meeting FY2022,(Tokyo, Japan, Jan. 31-Feb. 2, 2023).
Hayashi, S.: 2022, A New Observatory Is Coming to Your
Neighborhood, Part 3: Group Discussion, Group Voting with 3
Guiding Questions, Report Back, AAS Meeting #240, (Pasadena, CA,
USA, Jun. 12–16, 2022).
Hayashi, S., Skidmore W.: 2022, UV-enhanced coating caveat:
spectrophotometric response, AAS Meeting #240, (Pasadena, CA,
USA, Jun. 12–16, 2022).
Hayatsu, H. N.: 2022, Is CH+ emission real or not? The case of Eyelash
Cy2 (and Cy4) data, A half century of millimeter and submillimeter
astronomy: Impact on astronomy/astrophysics and the future,(Miyakojima, Japan, Dec. 15–18, 2022).

Hayatsu, H. N.: 2023, ALMA Deep Field in SSA22: Reconstracted [CII]Luminosity Function at z = 6, VLTI and ALMA Synthesis Imaging
Workshop, (Garching, Germany, Jan. 9–12, 2023).
He, W., Akiyama, M.: 2022, Cosmic growth of less-luminous quasars
at redshift 4 in the Subaru-HSC Wide field, 44th COSPAR Scientific
Assembly, (Athene, Greece, Jul. 16–24, 2022).
He, W., Akiyama, M.: 2022, Black hole mass and Eddington
ratio distributions of less-luminous quasars at z~4, HSC-AGN
Collaboration Meeting 2022, (Kagoshima, Japan, Nov. 29–Dec. 4,2022).
He, W., Tanaka, M., Ishigaki, M. N., Onodera, M., obsproc member:
2022, PFS Pointing Planner, PFS Community Meeting, (Online, Oct.
4, 2022).
He, W., Tanaka, M., Ishigaki, M. N., Onodera, M., obsproc member:
2023, PFS Pointing Planner (PPP): optimal tiling algorithm for PFS
open-use programs, Subaru Users Meeting FY2022, (Tokyo, Japan,
Jan. 31–Feb. 2, 2023).
Hirano, T.: 2023, RV Jitters in M Dwarfs: Near-Infrared Measurements
and a New Diagnosis, The Extreme Precision Radial Velocity (EPRV)
5 Conference, (Santa Barbara, USA, Mar. 27–30, 2023).
Hirano, T.: 2022, Star-formation studies with VLBI and future prospects
for Southeast Asian VLBI Network, The 2nd Malaysian VLBI
Workshop, (Kuala Lumpur, Malaysia, Sep. 5–8, 2022).
Hirano, T.: 2023, Opening of symposium, IAU Symposium 380: Cosmic
Masers: Proper Motion toward the Next-Generation Large Projects,(Kagoshima, Japan, Mar. 20–24, 2023).
Honda, S., Murayama, Y., Nitta, T., Nagai, M., Miyazawa, H., Noji,
R., Mandal, P., Kuno, K., Matsuo, H., Sekimoto, Y., Nakai, N.:
2022, Development and Commissioning of 100 GHz Microwave
Kinetic Inductance Detector (MKID) Camera at the Nobeyama 45 m
Telescope, 2022 URSI-Japan Radio Science Meeting, (Tokyo, Japan,
Sep. 1–2, 2022).
Honma, M.: 2023, Galactic Maser Astrometry with VERA, IAU
Symposium 380: Cosmic Masers: Proper Motion toward the NextGeneration Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Hori, Y., Fukui, A., Hirano, T., Narita, N., MuSCAT/IRD Team: 2023,
Are Eccentric, Close-in Sub-Neptunes not Rocky?, The Extreme
Precision Radial Velocity (EPRV) 5 Conference, (Santa Barbara,USA, Mar. 27–30, 2023).
Ikoma, M., Enya, K., Ito, Y., Fujii, Y., Kameda, S., Kawashima, Y.,
Narita, N., Fukui, A., Murakami, G.: 2022, Japanese scientificcontribution to Ariel, Japan Geoscience Union Meeting 2022, (Chiba,
Japan, May 22–27, 2022).
Ikoma, M.: 2022, Volatile accumulation, partition, and loss for rocky
planets, Rocky Worlds II, (Oxford, UK, Jul. 4–8, 2023).
Imada, H., Kaneko, K., Sakai, R., Kang, H., Masai, T., Nagai, M.,
Shan, W., Ezaki, S., Uzawa, Y., Kojima, T., Gonzalez, A.: 2023,
An overview of recent research on antennas and feeds for mm-wave
radio astronomy at NAOJ, 17th European Conference on Antennas
and Propagation, (Florence, Italy, Mar. 26–31, 2023).
Imada, H., Kaneko, K., Sakai, R., Kojima, T., Gonzalez, A.: 2022,
Tolerance analysis of a radio- telescope optical system, 23rd East Asia
Submillimeter-Wave Receiver Technology Workshop jointly with the
Riken-NICT Joint Workshop on Terahertz Technology, (Wako, Japan,
Dec. 14–15, 2022).
Imada, H., Kaneko, K., Sakai, R., Kojima, T., Gonzalez, A.: 2022,

XIII Publications, Presentations

169

Study of ALMA Band 2 receiver optical design for ACA 7-m antenna,
32nd International Symposium on Space Terahertz Technology,(Baeza Andalusia, Spain, Oct. 16–20, 2022).
Imanishi, M.: 2023, Dense molecular gas properties of nearby (U)LIRGs' nuclei constrained from HCN and HCO+ three transition line
data, CONquest Workshop 2023, (Gothenberg, Sweden/Online, Jan.
18–19, 2023).
Imanishi, M.: 2023, Supermassive blackhole mass growth in infraredluminous gas-rich galaxy mergers and potential power of millimeter
H2O megamaser observations, IAU Symposium 380: Cosmic
Masers: Proper Motion toward the Next-Generation Large Projects,(Kagoshima, Japan, Mar. 20–24, 2023).
Inoue, A. K., Kaneda, H., Yamada, T., Harikane, Y., Ishihara, D.,
Kodama, T., Komiyama, Y., Moriya, T., Motohara, K., Nomura,
H., Ouchi, M., Oyabu, S., Suzuki, T., Wada, T., Yamamura, I.: 2022,
GREX-PLUS: galaxy reionization explorer and planetary universe
spectrometer, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Inoue, S., Chin, K., Uno, S., Kohno, K., Niwa, Y., Naganuma, T.,
Yamamura, R., Takekoshi, T., Oshima, T.: 2022, Development ofan easy-to-array planar Magic-T for broadband mm/submm wave
detectors, A half century of millimeter and submillimeter astronomy:
Impact on astronomy/astrophysics and the future, (Miyakojima,
Japan, Dec. 15–18, 2022).
Inoue, S., Chin, K., Uno, S., Kohno, K., Niwa, Y., Naganuma, T.,
Yamamura, R., Takekoshi, T., Oshima, T.: 2022, Design method of abroadband planar magic-T: a 6-14GHz scaled model for mm/submm
camera, ALMA/45m/ASTE Users Meeting 2022, (Tokyo, Japan, Dec.
20–21, 2022).
Ishigaki, M. N.: 2023, The selection of spectrophotometric standards
for PFS observations based on PanStarrs1 and Gaia, Subaru Users
Meeting FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).
Ishigaki, M. N.: 2023, Probing the Origin of Metals with Elemental
Abundances in the Oldest Galactic Stars, IAU Symposium 377:
Early Disk-Galaxy Formation from JWST to the Milky Way, (KualaLumpur, Malaysia, Feb. 6–10, 2023).
Ishigami, S., Hara, H., Oba, T.: 2022, Study on the heating distribution
along coronal loops using Hinode/EIS, Hinode-15/IRIS-12 Multimessenger physics of the solar atmosphere, (Prague, Czech Republic,
Sep. 19–23, 2022).
Ishikawa, R. T., Katsukawa, Y.: 2022, Spectral line broadening
associated with the turbulence in fading granules, Solar Polarization
Workshop 10, (Kyoto, Japan, Nov. 7–11, 2022).
Ishikawa, R. T., Nakata, M., Katsukawa, Y., Masada, Y., Riethmuller, T.
L.: 2022, Multi-scale deep learning for estimating horizontal velocity
fields on the solar surface, Hinode-15/IRIS-12 Multi-messenger
physics of the solar atmosphere, (Prague, Czech Republic, Sep.
19–23, 2022).
Ishikawa, R., Trujillo Bueno, J., Alsina Ballester, E., Belluzzi, L., delPino Aleman, T., Kano, R., McKenzie, D., Auchere, F., Kobayashi,K., Okamoto, T. J., Rachmeler, L., Song, D.: 2022, Observational
Evidence for the Hanle and Magneto-Optical Effects in the
Polarization of the Mg II h & k Lines Observed by CLASP2, Solar
Polarization Workshop 10, (Kyoto, Japan, Nov. 7–11, 2022).
Ishikawa, R., Trujillo Bueno, J., del Pino Aleman, T., Okamoto, T. J.,
McKenzie, D. E., Auchère, F., Kano, R., Song, D., Rachmeler, L.

170

XIII Publications, Presentations

A., Kobayashi, K., Bethge, C., De Pontieu, B., CLASP2 team: 2022,
Solar magnetic fields from the photosphere to the top chromosphererevealed by CLASP2 and Hinode, Hinode-15/IRIS-12 Multimessenger physics of the solar atmosphere, (Prague, Czech Republic,
Sep. 19–23, 2022).
Ishikawa, R. T., Nakata, M., Katsukawa, Y., Masada, Y., Riethmuller T.L.: 2022, Multi-scale deep learning for estimating horizontal velocity
fields on the solar surface, IAU Symposium 368: Machine Learningin Astronomy: Possibilities and Pitfalls, (Busan, Korea, Aug. 2–4,2022).
Ishikawa, R. T., Nakata, M., Katsukawa, Y., Masada, Y., Riethmuller
T. L.: 2022, Multi-Scale Deep Learning for Estimating Horizontal
Velocity Fields in the Solar Photosphere, AAS TESS 2022, (Seattle,
USA, Aug. 8–11, 2022).
Ito, T., Malhotra, R.: 2022, Conditions for the long term stability of
Pluto's azimuthal and latitudinal perihelion librations, JpGU Meeting
2022, (Onsite: Chiba, Japan, May 22–27, 2022, Online: May 29–June
3, 2022).
Izumi, T.: 2022, Multiphase Dynamical Gas Fountain that Replaces theClassical Black Hole Obscuration, Behind the Curtain of Dust IV,(Sesto, Italy, Jul. 11–15, 2022).
Izumi, T.: 2022, Resolving supermassive black hole feeding, feedback,and obscuration: multiphase gas flows down to sub-parsec,
TORUS2022, (Leiden, Netherland, Dec. 13–15, 2022).
Izumi, T.: 2022, ALMA Observations of Low-Luminosity Quasars at
Cosmic Dawn, HSC-AGN Collaboration Meeting 2022, (Kagoshima,
Japan, Nov. 29–Dec. 4, 2022).
Izumi, T.: 2022, Multiphase dynamical gas fountain that replaces theclassical black hole obscuration, What drives the growth of black
holes: a decade of reflection, (Reykjavik, Iceland, Sep. 26–30, 2022).
Izumi, T.: 2022, ALMA Observations of Low-Luminosity Quasars at
Cosmic Dawn: Less-biased View on the Early Co-Evolution, 44th
COSPAR Scientific Assembly, (Athene, Greece, Jul. 16–24, 2022).
Izumi, T.: 2023, Resolving supermassive black hole feeding andfeedback down to sub-parsec scales, East-Asian ALMA Science
Workshop 2023, (New Taipei City, Taiwan, Feb., 14–17, 2023).
Jeschke, E., Kackley R., Inagaki, T.: 2022, A Unified Real-Time Sound
Network for Subaru Telescope, ADASS XXXII, (Online, Oct. 31–
Nov. 4, 2022).
Kamizuka, T., et al. including Koshida, S., Motohara, K.: 2022,
Development status of TAO/MIMIZUKU: performance testof the near-infrared channel, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Kaneko, K., Sakai, R., Kanzawa, T., Mitsui, K., Kojima, T., Uzawa, Y.,
Gonzalez, A., Kang, H., Huang, C., Huang, Y.: 2022, Developmentof ALMA Band 1 Corrugated Horns based on Metal 3D Printer, 32nd
International Symposium on Space Terahertz Technology, (Baeza
Andalusia, Spain, Oct. 16–20, 2022).
Kang, H., Kaneko, K., Sakai, R., Gonzalez, A.: 2022, Application of
metal 3D printing technology in high-performance millimeter-wave
corrugated horns, 23rd East Asia Submillimeter-Wave ReceiverTechnology Workshop jointly with the Riken-NICT Joint Workshop
on Terahertz Technology, (Wako, Japan, Dec. 14–15, 2022).
Kang, J., Kim, M. K., Kim, J., Kim, K. T., Hirota, T., Sugiyama, K.,
Chibueze, J. O., Burns, R. A., KaVASF team: 2023, Jet and Outflows
of a High Mass Star Forming Region: G10.34-0.14, IAU Symposium380: Cosmic Masers: Proper Motion toward the Next-Generation
Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Katsuda, S., et al. including Narukage, N.: 2022, Inverse FIP Effects
in Giant Solar Flares Found from Earth X-Ray Albedo with Suzaku/
XIS, 44th COSPAR Scientific Assembly, (Athene, Greece, Jul. 16–24,
2022).
Katsukawa, Y., et al. including Kubo, M., Kawabata, Y., Oba, T.,
Ishikawa, R. T., Hara, H., Uraguchi, F., Tsuzuki, T., Nodomi, Y.,
Shinoda, K., Tamura, T., Suematsu, Y.: 2022, Spectro-polarimetriccapability of SUNRISE III SCIP, Solar Polarization Workshop 10,(Kyoto, Japan, Nov. 7–11, 2022).
Katsukawa, Y., Hara, H., Kubo, M., Kawabata, Y., Oba, T., Piqueras
Carreno, J. , Perez Grande, I., Shinoda, K., Tamura, T., Uraguchi, F.,
Tsuzuki, T., Nodomi, Y., Shimizu, T.: 2022, Sunrise Chromospheric
Infrared spectroPolarimeter (SCIP) for SUNRISE III: Thermalvacuum test of the SCIP optical unit, SPIE Astronomical Telescopes+ Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Katsukawa, Y., et al. including Kubo, M., Kawabata, Y., Oba, T.,
Ishikawa, R. T., Hara, H., Uraguchi, F., Tsuzuki, T., Nodomi, Y.,
Shinoda, K., Tamura, T., Suematsu, Y.: 2022, SUNRISE-III SCIP:
capability and status, Plasma Explosions in the Universe (PEU 2022),(Kyoto, Japan, Sep. 6–8, 2022).
Katsukawa, Y., Morita, S., Hanaoka, Y., Shinoda, K., Iju, T., Nishida,K., Sakurai, T.: 2022, Synoptic acquisition of full-disk magnetic
fields in the photosphere and the chromosphere by an infrared
spectro-polarimeter on the Solar Flare Telescope, IAU Symposium372: The Era of Multi-Messenger Solar Physics, (Busan, Korea, Aug.
2–4, 2022).
Katsukawa, Y., Trujillo Bueno, J., Manso Sainz, R., Ishikawa, R., Stepan,J., Kano, R., Kubo, M., Narukage, N., Bando, T., Winebarger, A.,
Kobayashi, K., Auchere, F.: 2022, Polarization measurement of the
OV 121.83 nm intercombination line with CLASP, Solar Polarization
Workshop 10, (Kyoto, Japan, Nov. 7–11, 2022).
Kawabata, Y.: 2022, Chromospheric magnetic field in active regions,
Solar Polarization Workshop 10, (Kyoto, Japan, Nov. 7–11, 2022).
Kawabata, Y., Katsukawa, Y., Kubo, M., Oba, T., Hara, H., Shimizu, T.,
Matsumoto, T., Ishikawa, R.T., Tsuzuki, T., Uraguchi, F., Nodomi,
Y., Shinoda, K., Tamura, T., Suematsu, Y., Quintero Noda, C.,
del Toro Iniesta, J. C., Sánchez Gómez, A., Hernández Expósito,
D., Orozco Suárez, D., Balaguer Jiménez, M., Bailón Martínez, E.,
Miguel Morales Fernández, J., Moreno Mantas, A., Solanki, S., Lagg
A., Gandorfer, A., Feller, A.: 2022, The pre-flight test and observation
results of the Sunrise Chromospheric Infrared spectroPolarimeter(SCIP), Hinode-15/IRIS-12 Multi-messenger physics of the solar
atmosphere, (Prague, Czech Republic, Sep. 19–23, 2022).
Kawabata, Y., Katsukawa, Y., Tsuzuki, T., Uraguchi, F., Mitsui,K., Shinoda, K., Tamura, T., Nodomi, Y., Hara, H., Kubo, M.:
2022, Optical alignment and performance evaluation of the Sunrise
Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III,SPIE Astronomical Telescopes + Instrumentation, (Montréal, QC,
Canada, Jul. 17–22, 2022).
Kikuchi, S.: 2022, Preliminary Design of the Hayabusa2 Extended
Mission to the Fast-rotating Asteroid 1998 KY26, 73rd International
Astronautical Congress, (Paris, France, Sep. 18–22, 2022).
Kikuchi, S., et al.: 2023, Evolution of impact ejecta produced by the
Hayabusa2 impact experiment on the asteroid Ryugu, PERC Int.

Symposium on Dust & Parent Bodies 2023 (IDP2023), (Chiba, Japan,
Feb. 27, 2023).
Kim, J., Kim, M. K., Hirota, T., Kim, K. T., KaVA Science Working
Group for Star-formation: 2023, Multiple scales of view for outflow
driven by a highmass young stellar object, G25.82-W1, IAU
Symposium 380: Cosmic Masers: Proper Motion toward the NextGeneration Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Kim, M. K., Hirota, T., Kim, K. T., KaVA SFR sub Working Group:2023, A Multiwavelength study towards Galactic H II region G10.320.26, IAU Symposium 380: Cosmic Masers: Proper Motion toward
the Next-Generation Large Projects, (Kagoshima, Japan, Mar. 20–24,
2023).
Kim, Y. J., Sallum, S., Lin, J., Xin, Y., Norris, B., Betters, C., LeonSaval, S., Lozi, J., Vievard, S., Gatkine, P., Guyon, O., Jovanovic,
N., Mawet, D., Fitzgerald, M.: 2023, Imaging and Spectroastrometry
with Photonic Lanterns, AAS meeting #241, (Seattle, WA, USA, Jan.
8–12, 2023).
Kim, Y. J., Sallum, S., Lin, J., Xin, Y., Norris, B., Betters, C., LeonSaval, S., Lozi, J., Vievard, S., Gatkine, P., Guyon, O., Jovanovic, N.,
Mawet, D., Fitzgerald, M. P.: 2022, Spectroastrometry with photonic
lanterns, SPIE Astronomical Telescopes + Instrumentation, (Montréal,
QC, Canada, Jul. 17–22, 2022).
Kojima, T., Masui, S., Makise, K., Shan, W., Uzawa, Y.: 2022, Nonreciprocal microwave circuit based on phase-controlled two-frequencyconverter configuration, 23rd East Asia Submillimeter-Wave ReceiverTechnology Workshop jointly with the Riken-NICT Joint Workshop on
Terahertz Technology, (Wako, Japan, Dec. 14–15, 2022).
Kojima, T., Uzawa, Y., Masui, S., Kozuki, Y., Fujii, Y., Makise, K.,
Shan, W.: 2022, Noise temperature and S-parameter measurementsof an SIS-based microwave amplifier, 32nd International Symposiumon Space Terahertz Technology, (Baeza Andalusia, Spain, Oct. 16–20,
2022).
Kojima, T., Uzawa, Y., Masui, S., Kozuki, Y., Fujii, Y., Makise,K., Shan, W.: 2022, Microwave performance of an SIS-based
amplifier with a millimeter-wave isolator, Applied Superconductivity
Conference 2022, (Honolulu, HI, USA, Oct. 23–28, 2022).
Kokubo, E.: 2022, Dynamical Properties of Planetary Systems Formedby Giant Impacts, NCTS-ASIAA Workshop: Stars, Planets, andFormosa, (Online, Aug. 15–19, 2022).
Kokubo, E., Hoshino, H., Matsumoto, Y.: 2022, Orbital Architecture ofPlanetary Systems Formed by Gravitational Scattering and Collisions,
Forming and Exploring Habitable Worlds , (Edinburgh, UK, Nov.
7–13, 2022).
Kokubo, E., Shibata, T., Ishigaki, M., Makino, J.: 2022, ormationof Protoplanets from Planetesimals under a Realistic Accretion
Condition, The 9th East Asian Numerical Astrophysics Meeting,(Naha, Japan, Sept. 26–30, 2022).
Komatsu, Y., Hori, Y., Kuzuhara, M., Kosugi, M., Takizawa, K., Narita
N., Omiya, M., Kim, E., Kusakabe, N., Meadows, V., Tamura, M.:
2022, Photosynthetic Fluorescence from Earth-like Planets Around
Cool stars, AbSciCon 2022, (Atlanta, GA, USA, May 15–20, 2022).
Koshida, S., Moritani, Y., Tamura, N., Lupton, R., Loomis, C., Le Fur,A., Siddiqui, H., Yan, C.-H., Karr, J., Yoshida, H., Kawanomoto,S., Takagi, Y., Arai, A., Jeschke, E., Onodera, M., Yabe, K., PFS
Collaboration: 2023, Summary of PFS Engineering Observations in
FY 2022, Subaru Users Meeting FY2022, (Tokyo, Japan, Jan. 31–

XIII Publications, Presentations

171Feb. 2, 2023).
Koyama, Y., ULTIMATE-Subaru Science Team: 2023, ULTIMATESubaru Science Overview, The First SUPER-IRNET Workshop Rebooting Our In-Person Collaboration, (Tokyo, Japan, Mar. 23–24,
2023).
Kubo, M., Shiota, D., Katsukawa, Y., Shimojo, M., Orozco Suárez,D., Nitta, N., DeRosa, M., Centeno, R.: 2022, Comparison of polar
magnetic fields derived from MILOS and MERLIN inversion for
Hinode/SOT-SP data, Hinode-15/IRIS-12 Multi-messenger physics ofthe solar atmosphere, (Prague, Czech Republic, Sep. 19–23, 2022).
Kubo, M., Shiota, D., Katsukawa, Y., Shimojo, M., Orozco Suárez,D., Nitta, N., DeRosa, M., Centeno, R.: 2022, Comparison of polar
magnetic fields derived from MILOS and MERLIN inversion for
Hinode/SOT-SP data, Solar Polarization Workshop 10, (Kyoto, Japan,
Nov. 7–11, 2022).
Kudo, T., Lozi, J., Deo, V., Guyon, O., Norris, B., Hashimoto, J.:
2022, Fast NIR Polarimetric Differential Imaging modes on Subaru/
SCExAO, Spirit of Lyot, (Leiden, Netherlands, Jun. 27–Jul. 1, 2022).
Kurahara, K., Akahori, T., Kale, R., Akamatsu, H., Fujita, Y., Gu,
L., Intema, H., Nakazawa, K., Okabe, N., Omiya, Y., Parekh, V.,
Shimwell, T., Takizawa, M., van Weeren, R.: 2022, Diffuse radiosource in CIZA J1358.9-4750, SPARCS XI: The Rise of Sky Surveys,(Online, Nov. 21–25, 2022).
Kushibiki, K., Ozaki, S., Takeda, M., Hosobata, T., Yamagata, Y., Morita,
S., Nakagawa, K., Saiki, T., Ohtake, Y., Tsuzuki, T., Mitsui, K.,
Okita, H., Motohara, K., Takahashi, H., Konishi, M., Kato, N. M.,
Koyama, S., Chen, N., Homan, S., Yasuda, A.: 2022, Development
status of a near-infrared integral field unit SWIMS-IFU, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Lallement, M., Lacour, S., Huby, E., Martin, G., Barjot, K., Perrin, G.,
Rouan, D., Lapeyrere, V., Vievard, S., Guyon, O., Lozi, J., Deo, V.,
Kotani, T., Pham, C., Cassagnettes, C., Billat, A., Cvetojevic, N.,
Marchis, F.: 2022, Photonic chip for visible interferometry: laboratory
characterization and comparison with the theoretical model, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17-22, 2022).
Lin, J., Vievard, S., Jovanovic, N., Norris, B., Fitzgerald, M. P., Betters, C.,
Gatkine, P., Guyon, O., Kim, Y. J., Leon-Saval, S., Lozi, J., Mawet,
D., Sallum, S., Xin, Y.: 2022, Experimental measurements of AO-fed
photonic lantern coupling efficiencies, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Lin, J., Xin, Y., Norris, B., Kim, Y. J., Sallum, S., Betters, C., LeonSaval, S., Lozi, J., Vievard, S., Guyon, O., Gatkine, P., Jovanovic,
N., Mawet, D., Fitzgerald, M. P.: 2022, Exoplanet detection withphotonic lanterns for focal-plane wavefront sensing and control, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Lozi, J.: 2022, AO3000 at Subaru: Combining for the first time a NIR
WFS using First Lights C-RED ONE and ALPAOs 64x64 DM, Spiritof Lyot, (Leiden, Netherlands, Jun. 27–Jul. 1, 2022).
Lozi, J., Ahn, K., Clergeon, C., Deo, V., Guyon, O., Hattori, T.,
Minowa, Y., Nishiyama, S., Ono, Y., Vievard, S.: 2022, AO3000 at
Subaru: combining for the first time a NIR WFS using First Light's
C-RED ONE and ALPAO's 64x64 DM, SPIE Astronomical Telescopes+ Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).

172

XIII Publications, Presentations

Lucas, M., Bottom, M., Guyon, O., Lozi, J., Norris, B., Deo, V.,
Vievard, S., Ahn, K., Skaf, N., Tuthill, P.: 2022, A visible-light Lyot
coronagraph for SCExAO/VAMPIRES, SPIE Astronomical Telescopes+ Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Machida, M., Kawashima, T., Kudoh Y., Matsumoto, Y., Matumoto, R:
2022, Magnetic reconnection in accretion disk spiral arms, IRCCAFP Meeting 2022, (Mitaka, Japan, Oct. 24–28, 2022).
Maeda, N., Terai, T., Ohtsuki, K., Yoshida F., Ishihara, K., Deyama T.:
2022, Size distributions of small main belt asteroids obtained by the
Subaru/Hyper Suprime-Cam, Japan Geoscience Union Meeting 2022,(Chiba, Japan, May 22–27, 2022).
Maehara, H.: 2022, Stellar mass ejections associated with superflareson solar- and late-type stars, Solar Extreme Events: Setting Up a
Paradigm, (Bern, Switzerland/Online, Jun. 7–10, 2022).
Maehara, H.: 2022, Superflares and super-CMEs on solar-type stars,
31st IAU General Assembly, (Busan, Korea, Aug. 2–11, 2022).
Maehara, H., Namekata, K., Notsu, Y., Honda, S., Namizaki, K., Inoue,
S., Ikuta, K., Nogami, D., Shibata, K.: 2022, Hunting for stellar massejections associated with stellar superflares through time-resolved
optical spectroscopy of superflare stars, 44th COSPAR Scientific
Assembly, (Athene, Greece, Jul. 16–24, 2022).
Maehara, H., Namekata, K., Notsu, Y., Honda, S., Namizaki, K., Inoue,
S., Ikuta, K., Nogami, D., Shibata, K.: 2022, Simultaneous TESS
and ground-based spectroscopic observations of stellar superflares:
Exploring the connection between stellar mass ejections andsuperflares, 44th COSPAR Scientific Assembly, (Athene, Greece, Jul.
16–24, 2022).
Malhotra, R., Ito, T.: 2022, Pluto near the edge of chaos, DPS 2022 (54thAnnual Meeting of the Division for Planetary Sciences), (London,
Ontario, Canada, Oct. 2–7, 2022).
Martinache, F., Cvetojevic, N., Deo, V.: 2022, Fizeau-interferometry
fringe tracking solutions for giant segmented telescope petal modes,
SPIE Astronomical Telescopes + Instrumentation, (Montréal, QC,
Canada, Jul. 17–22, 2022).
Martinez, N., Herrald, N., Chandler, D., Haynes, D., Kruse, A.,
Ramasundara, W., Rigaut, F., Bernard, J. T., Travouillon, T., Vaughn,I., Minowa, Y., Ono, Y., Tanaka, Y., Terao, K., D'Orgeville, C.: 2022,
Wavefront sensing over a 20-arcmin field in the ULTIMATE-Subaru
Ground Layer Adaptive Optics system, SPIE Astronomical Telescopes+ Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Martinez, N., Kruse, A., Herrald, N., Chandler, D., Haynes, D., Rigaut,
F., Bernard, J.T., Travouillon, T., Vaughn, I., Minowa, Y., Ono, Y.,
Tanaka, Y., Terao, K., D'Orgeville: 2022, Preliminary design of
the Laser Guide Star Facility for the ULTIMATE-Subaru Ground
Layer Adaptive Optics system, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Martinod, M.-A., et al. including Guyon, O., Lozi, J.: 2022, Achromaticnulling interferometry and fringe tracking with 3D-photonic
tricouplers with GLINT, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Masui, S., Kojima, T., Makise, K., Ogawa, H., Onishi, T., Uzawa, Y.:
2022, Concept of a novel microwave isolator for a large integrated
circuit, Applied Superconductivity Conference 2022, (Honolulu, HI,
USA, Oct. 23–28, 2022).
Masui, S., Ogawa, H., Onishi, T., Makise, K., Kojima, T., Uzawa, Y.:
2022, Proof-of-concept experiment on a novel microwave circulator

based on frequency converters, 32nd International Symposium onSpace Terahertz Technology, (Baeza Andalusia, Spain, Oct. 16–20,
2022).
Masukura, A., Shan, W., Ezaki, S., Kojima, T., Nakajima, T., Mizuno,
A.: 2022, Silicon Membrane Based Superconducting Waveguideto-CPW Transitions at 2 mm Band, Applied Superconductivity
Conference 2022, (Honolulu, HI, USA, Oct. 23–28, 2022).
Matsuo, H., Ezawa, H., Niwa, A., Koseki, T., Enohi, R., Okada, N.:
2022, Progress toward Antarctic Terahertz Intensity Interferometry,
32nd International Symposium on Space Terahertz Technology,(Baeza Andalusia, Spain, Oct. 16–20, 2022).
Matsuo, H., Ezawa, H., Okada, N., Niwa, A., Koseki, T., Enohi, R.:
2022, Laboratory Experiments on THz Intensity Interferometry,
23rd East Asia Submillimeter-Wave Receiver Technology Workshop
jointly with the Riken-NICT Joint Workshop on Terahertz
Technology, (Wako, Japan, Dec. 14–15, 2022).
Matsuo, H., Kuno, N., Seta, M., Nakai, N.: 2022, Proposal of Terahertz
Interferometry from Dome Fuji, SCAR Open Science Conference,(Online, Aug. 1–10, 2022).
Matuura, M., Ezaki, S., Sakai, T., Noguchi, T., Seta, M.: 2022,
Investigation of Nb3Ge Thin Films on Si Substrates, 23rd East Asia
Submillimeter-Wave Receiver Technology Workshop jointly with the
Riken-NICT Joint Workshop on Terahertz Technology, (Wako, Japan,
Dec. 14–15, 2022).
Minowa, Y., et al. including Ono, Y., Tanaka, Y., Yoshida, H., Terao,
K., Koyama, Y., Ali, S., Tanaka, I., Hattori, T., Okita, H., Hayano,Y., Oya, S., Motohara, K., Yanagisawa, K., Yoshida, M.: 2022,
ULTIMATE-Subaru: GLAO preliminary design overview, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Miyata, T., et al. including Motohara, K.: 2022, The University ofTokyo Atacama Observatory 6.5m telescope: project status 2022,
SPIE Astronomical Telescopes + Instrumentation, (Montréal, QC,
Canada, Jul. 17–22, 2022).
Morii, K., Nakamura, F., Sanhueza, P.: 2022, Early fragmentation of
70 μm-dark IRDCs: Observational test for high-mass star formation
scenarios, Star Formation in Different Environments 2022, (QuyNhon, Vietnam, Aug. 22–26, 2022).
Morii, K., Sanhueza, P., Nakamura, F., Zhang, Q.: 2022, Defining theinitial conditions of high-mass star formation with ALMA, EastAsian ALMA Science Workshop 2023, (New Taipei City, Taiwan,
Feb., 14–17, 2023).
Moritani, Y.: 2023, The report of the past commissioning observationand the plans, PFS Science Meeting, (Chiba, Japan, Mar. 2–3, 2023).
Moritsuka, A., Katsukawa, Y., Ishikawa, R. T.: 2022, Doppler velocity
variation toward the solar limb observed with HINODE SOT-SP,
Hinode-15/IRIS-12 Multi-messenger physics of the solar atmosphere,(Prague, Czech Republic, Sep. 19–23, 2022).
Moriya, T.: 2022, Effect of circumstellar matter on Type Ia supernova
early photometric properties, Exploring The Transient Universe,(Tokyo, Japan, Dec. 14–16, 2022).
Moriya, T.: 2022, Supernova model library for the Rubin/LSST era, The
Fourth Chile-Japan Academic Forum 2022, (Los Lagos, Chile, Nov.
28–Dec. 2, 2022).
Moriya, T.: 2022, Massive star mass loss constrained by supernova radio
properties, IAU Symposium 370: Winds of stars and exoplanets,(Busan, South Korea, Aug. 8–11, 2022).
Moriya, T.: 2022, Constraining massive star mass loss throughsupernova radio properties, IAU Symposium 361: Massive Stars Nearand Far, (Ballyconnell, Ireland, May 8–13, 2022).
Moriya, T.: 2023, Discovering Supernovae at Epoch of Reionization
with Nancy Grace Roman Space Telescope, AAS meeting #241,(Seattle, WA, USA, Jan. 8–12, 2023).
Moriya, T.: 2023, Interacting supernovae at cosmological distances,
Interacting Supernovae, (Garching, Germany, Feb. 6–Mar. 3, 2023).
Moriya, T.: 2023, Effects of circumstellar interactions on supernova light
curves, Interacting Supernovae, (Garching, Germany, Feb. 6–Mar. 3,2023).
Moriya, T.: 2023, Environmental dependence of Type IIn supernova
properties, Interacting Supernovae, (Garching, Germany, Feb. 6–Mar.
3, 2023).
Motogi, K., Hirota, T., Machida, M. N., Tanaka, K. E. I., Yonekura, Y.:
2023, The water and methanol masers in the face-on accretion system
around the high-mass protostar G353.273+0.641, IAU Symposium
380: Cosmic Masers: Proper Motion toward the Next-Generation
Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Murayama, Y., Honda, S., Nagai, M., Hosun, L., Ishizaki, Y., Nitta,
T., Noji, R., Miyazawa, H., Kuno, N., Matsuo, H., Shan, W.,
Sekimoto, Y., Noguchi, T., Naruse, M., Nakai, N.: 2022, Responsivity
Evaluation of the 100-GHz Band MKID Camera with Various Optical
Loading Conditions, 23rd East Asia Submillimeter-Wave ReceiverTechnology Workshop jointly with the Riken-NICT Joint Workshop
on Terahertz Technology, (Wako, Japan, Dec. 14–15, 2022).
Nagai, M., Gonzalez, A., Imada, H.: 2022, A Study on the Effect ofAberrations on the Design of High-Aperture Efficiency Optics for(Sub)Millimeter Multibeam Receivers, 23rd East Asia SubmillimeterWave Receiver Technology Workshop jointly with the Riken-NICT
Joint Workshop on Terahertz Technology, (Wako, Japan, Dec. 14–15,
2022).
Nagai, M., Imada, H.: 2022, Aperture Efficiency of Multi-beam
Axisymmetric Dual-reflector Antenna, 23rd East Asia SubmillimeterWave Receiver Technology Workshop jointly with the Riken-NICT
Joint Workshop on Terahertz Technology, (Wako, Japan, Dec. 14–15,
2022).
Nagai, M., Imada, H., Nitta, T., Murayama, Y., Noji, R., Naruse,
M.: 2022, Correlation Polarimeter for Millimeter-wave Wavefront
Sensing, 2022 URSI-Japan Radio Science Meeting, (Tokyo, Japan,
Sep. 1–2, 2022).
Naganuma, T., Yoshioka, K., Yamamura, R., Sakai, T., Oshima, T.,
Takekoshi, T., Niwa, Y., Uno, S., Chin, K., Inoue, S.: 2022, Multioctave anti-reflection coating for mm/submm optics based on adielectric multilayer synthesis approach, A half century of millimeterand submillimeter astronomy: Impact on astronomy/astrophysics andthe future, (Miyakojima, Japan, Dec. 15–18, 2022).
Nakai, N., Yamauchi, A., Yamazaki, M., Harada, R.: 2023, Distanceof the Seyfert 2 galaxy IC 2560 and the Hubble constant, IAU
Symposium 380: Cosmic Masers: Proper Motion toward the NextGeneration Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Nakajima, K.: 2022, Diagnostics for PopIII galaxies and direct collapse
black holes in the early universe, Hot Topics in Astrophysics, (Sesto,
Italy, Jul. 25–29, 2022).
Nakajima, T., Suzuki, K., Kojima, T., Uzawa, Y., Ishino, M., Watanabe,

XIII Publications, Presentations

173

I.: 2022, Propagation in Superconducting Niobium Rectangular
Waveguide in the 100 GHz band, The 35th International Symposiumon Superconductivity (ISS2022), (Nagoya, Japan, Nov. 29–Dec. 1,2022).
Nakamura, F.: 2022, A New Wide-Bandwidth, High-Sensitivity Q-Band
Receiver installed on the NRO 45 m telescope, A half century of
millimeter and submillimeter astronomy: Impact on astronomy/
astrophysics and the future, (Miyakojima, Japan, Dec. 15–18, 2022).
Nakamura, F.: 2022, Ultra-wideband, high-sensitivity Q-band receiver,eQ, Star Formation in Different Environments 2022, (Quy Nhon,
Vietnam, Aug. 22–26, 2022).
Nakamura, F.: 2022, Ultra-wideband, high-sensitivity Q-band receiver,eQ, Molecules in Extreme Environments: Near and Far, (Mitaka,
Japan, Nov. 23–25, 2022).
Nakamura, F.: 2023, Star Formation Triggered by Dense Core Collision
and Some Indirect Evidence of ALMA Observations, East-Asian
ALMA Science Workshop 2023, (New Taipei City, Taiwan, Feb.,
14–17, 2023).
Nakamura, K.: 2022, Gauge-invariant perturbation theory on the
Schwarzschild background spacetime including l=0,1 modes —Realization of exact solutions —, 31th Workshop on General Relativity
and Gravitation in Japan, (Tokyo, Japan, Oct. 24–28, 2022).
Nakamura, K.: 2022, Quantum Noise in Balanced Homodyne Detection
by Numbers or Power Counting Multi-Mode Detectors and Vacuum
Fluctuations, The 29th KAGRA face to face meeting, (Tokyo, Japan,
Aug. 1–3. 2022).
Nakamura, K.: 2022, Proposal of a gauge-invariant treatment of thel=0,1-mode perturbations on Schwarzschild Background Spacetime,The 23rd International conference on General Relativity andGravitation, (Beijin, China, Online, July 4–8, 2022).
Nakamura, K.: 2022, Proposal of a gauge-invariant treatment of thel=0,1-mode perturbations on Schwarzschild Background Spacetime,
Gravity: Current challenges in black hole physics and cosmology,(Kyoto, Japan, Jun. 20–Jul. 1, 2022).
Naknaishi, H., Sakai, N., Kurahara, K., VERA Outer Rotation Curve
project members: 2023, Astrometry of Water Maser sources in
the Outer Galaxy with VERA, IAU Symposium 380: Cosmic
Masers: Proper Motion toward the Next-Generation Large Projects,(Kagoshima, Japan, Mar. 20–24, 2023).
Nishino, Y.: 2022, Speedmeter: advanced technique to reduce quantum
radiation pressure noise, KAGRA Future working group, (Tokyo,
Japan, Nov, 17, 2022).
Niwa, A., Ezawa, H., Tamura, T., Matsuo, H.: 2022, SIS photon
detectors for THz observations beyond the gap energy, 32nd
International Symposium on Space Terahertz Technology, (Baeza
Andalusia, Spain, Oct. 16–20, 2022).
Nomura, H.: 2022, Isotopologue ratios in Protoplanetary Disks: A
Possible Link to Exoplanetary Atmospheres, Flatiron Exoplanet
Symposium, (New York, USA/Online, Aug. 8–12, 2022).
Nomura, H., Hu, B., Dong, R., Tsukagoshi, T., Kawabe, R., Millar,
T. J., Lau, R.: 2022, Infrared and Submillimeter Molecular Linesfrom Circumplanetary Disks, A half century of millimeter andsubmillimeter astronomy: Impact on astronomy/astrophysics and thefuture, (Miyakojima, Japan, Dec. 15–18, 2022).
Norris, B. R. M., Martinod, M.-A., Tuthill, P., Gross, S., Cvetojevic, N.,
Jovanovic, N., Lagadec, T., Klinner-teo, T., Guyon, O., Lozi, J., Deo,

174

XIII Publications, Presentations

V., Vievard, S., Arriola, A., Gretzinger, T., Lawrence, J. S., Withford,
M. J.: 2022, Optimal self-calibration and fringe tracking in photonic
nulling interferometers using machine learning, SPIE Astronomical
Telescopes + Instrumentation, (Montréal, QC, Canada, Jul. 17–22,2022).
Norris, B. R. M., Wei, J., Betters, C. H., Leon-Saval, S. G., Xin, Y., Lin,J., Kim, Y. J., Sallum, S., Lozi, J., Vievard, S., Guyon, O., Gatkine,P., Jovanovic, N., Mawet, D., Fitzgerald, M. P.: 2022, Demonstrationof a photonic-lantern focal-plane wavefront sensor using fiber mode
conversion and deep learning, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Nugroho, S. K., De Mooij, E. J. W., Gibson, N. P., Kawahara, H.,
Parmentier, V., Hirano, T., Kuzuhara, M., Brogi, M., Birkby, J.
L., Tamura, M., Kawashima, Y., Kotani, T., Masuda, K., Watson,
C. A., Zwintz, K., Rafi, S. A., Harakawa, H., Kudo, T., Hodapp,
K., Jacobson, S., Konishi, M., Kurokawa, T., Nishikawa, J.,Omiya, M., Serizawa, T., Ueda, A., Vievard, S.: 2022, Atomic andmolecular species in the near-infrared emission spectrum of WASP33b, Thinkshop 2022: High-resolution spectroscopy for exoplanet
atmospheres and biomarkers, (Potsdam, Germany, Sep. 7–9, 2023).
Oba, T., Cheung, M. C. M., Iida, Y., Shimizu, T.: 2022, Study of therelation between the reversed granulation and the gas compression/
expansion, Hinode-15/IRIS-12 Multi-messenger physics of the solar
atmosphere, (Prague, Czech Republic, Sep. 19–23, 2022).
Odaka, H., et al. including Narukage, N.: 2022, X-ray Imaging
Polarimetry using a Fine Pixel CMOS Imager, NDIP20, (Troyes,
France, July 4–8, 2022).
Ogane, H., Akiyama, M., Cranney, J., Rigaut, F., Martinez Rey, N.,
D'Orgeville, C., Minowa, Y., Ono, Y.: 2022, Aliasing effect ofrolling shutter readout in laser guide star wavefront sensing, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Ohtawara, K., Fujii, Y., Inata, M., Ito, T., Sakamoto, S.: 2022,
ALMA's cryocooler and its maintenance support by NAOJ, The
Fourth Chile-Japan Academic Forum 2022, (Los Lagos, Chile, Nov.
28–Dec. 2, 2022).
Okamoto, J., Sakurai, T.: 2022, The strongest magnetic fields insunspots and their statistical properties, Solar Polarization Workshop
10, (Kyoto, Japan, Nov. 7–11, 2022).
Okamoto, S.: 2023, Subaru Near Field Cosmology Survey, Subaru Users
Meeting FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).
Oki, A., Okino, H., Akahori, T., Kurahara, K., Honma, M., Hada,
K., Nagai, H., Niinuma, K., Kitayama, T., Ueda, S., Ishida, M.: 2023,
Elucidating co-evolutions among AGN, galaxies, and ICM from an
AGN survey with VERA, 9th Galaxy Evolution Workshop, (Kyoto,
Japan, Feb. 20–23, 2023).
Oki, A., Okino, H., Akahori, T., Kurahara, K., Honma, M., Hada,
K., Nagai, H., Niinuma, K., Kitayama, T., Ueda, S., Ishida, M.:
2023, Digging in young jets to elucidate clusters evolution from an
AGN survey with VERA, Black Hole Astrophysics with VLBI 2023,(Mitaka, Japan, Feb. 6–8, 2023).
Omae, R., Akahori, T., Machida, M.: 2023, Polarization Analysis
of Gravitational Lens Galaxies for Future Polarization Surveys,
Scientific Frontiers and Synergies for the DSA-2000 Radio Camera,(Pasadena, CA, USA, Mar. 20–22, 2023).
Ono, S., Narita, T., Masui, S., Kojima, T., Sakai, T.: 2022, Design andFabrication of Stripline Type of a Broadband Quadrature Hybrid
Couplers with Transitions of Coaxial-Microstrip-Stripline, 2022 AsiaPacific Microwave Conference (APMC 2022), (Yokohama, Japan,
Nov. 29–Dec. 2, 2022).
Ono, Y., Akiyama, M., Terao, K., Minowa, Y., Ogane, H., Oya, S.: 2022,
Covariance-based analytical algorithm to predict the performanceof tomographic AO systems, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Ono, Y., Minowa, Y., Tanaka, Y., Martínez, R. N., Herrald, N.,d'Orgeville, C., Rigaut, F., Vaughn, I., Chandler, D., Terao, K.: 2022,
ULTIMATE-Subaru: Requirement analysis of the WFS system for
GLAO, SPIE Astronomical Telescopes + Instrumentation, (Montréal,
QC, Canada, Jul. 17–22, 2022).
Onozato, H.: 2022, Age and metallicity dependence of near-infraredcolor and magnitude of the red clump stars in the Magellanic Clouds,
The Workshop on Infrared Astronomy with Infrared Survey Facility,(Kyoto, Japan, Dec. 1–3, 2022).
Onozato, H.: 2023, Current Status and Future Plans of SMOKA, Subaru
Users Meeting FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).
Ootsubo, T.: 2022, SolSysELTs2022 Part II: Mid-infrared spectroscopic
observation of distant and faint comets with ELT/METIS, Solar
System Science with the ELT, (Garching, Germany, and Virtual, Apr.
28, 2022).
Ootsubo, T.: 2022, Hydrated silicates on evolved cometary nuclei
observed in the mid-infrared, 31st IAU General Assembly, (Busan,
Korea, Aug. 2–11, 2022).
Ootsubo, T., Takata, T., Furusawa, J., Furusawa, H., Terai, T.,
Urakawa, S., Yoshida F.: 2022, Extraction and identification system forsmall solar system bodies in the Hyper Suprime-Cam Subaru Strategic
Program data, ADASS XXXII, (Online, Oct. 31–Nov. 4, 2022).
Orton, G., Sinclair, J., Fletcher, L., Read, P., Flasar, F. M., Achterberg,R., Yanamandra-Fisher, P., Fujiyoshi, T., Fisher, B., Irwin, P.: 2022,
A Survey of Slowly Moving Thermal Waves in Saturn's Atmospherefrom Cassini CIRS and Ground-Based Observations, 44th COSPAR
Scientific Assembly, (Athene, Greece, Jul. 16–24, 2022).
Oshima, T.: 2022, Probing the distant universe with the wide field ofview sub-millimeter camera, Tsukuba Global Science Week 2022,(Online, Sep. 27, 2022).
Oya, S., Minowa, Y., Okita, H., Ono, Y. H., Clergeon, C.: 2022,
ULTIMATE-Subaru: adaptive secondary mirror system, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Page, M.: 2022, Development of the KAGRA filter cavity and frequency
dependent squeezing, KAGRA International Workshop 9, (Online,
June 8, 2022).
Page, M.: 2023, Status of squeezing and quantum enhancement for
gravitational wave detection at NAOJ, ILANCE International
Conference on the Physics of the Two Infinities, (Kyoto, Japan, Mar.
27–30, 2023).
Pyo, T.-S., Okamoto, S., Terai, T.: 2023, The Completeness, Success,and Execution rates in HSC Queue mode, Subaru Users Meeting
FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).
Pyo, T.-S., Okita, H.: 2023, The results of the Telescope Analyses for
23 yrs of the Subaru Telescope (1999-2022), Subaru Users Meeting
FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).
Roman, M. T., Fletcher, L. N., Orton, G. S., Greathouse, T. K., Moses,

J., Rowe-Gurney, N., Irwin, P., G., J., Kasaba, Y., Fujiyoshi, T.,
Hammel, H. B., de Pater, I., Sinclair, J., Antuñano, A.: 2022, MidInfrared Observations of Neptune and Uranus: Recent Discoveries
and Future Opportunities, the 24th EGU General Assembly, (Vienna,
Austria and Online, May 23–27, 2022).
Roman, M. T., Fletcher, L. N., Orton, G. S., Rowe-Gurney, N., Moses, J.,
Greathouse, T. K., Irwin, P. G. J., Kasaba, Y., Fujiyoshi, T., Hammel,
H. B., de Pater, I., Antunano, A., Sinclair, J., Melin, H., Bardet, D.:
2022, Uranus and Neptune in the Mid-Infrared: Recent Findings
from VLT-VISIR and Future Opportunities with JWST-MIRI,
16th Europlanet Science Congress 2022, (Palacio de Congresos deGranada, Spain, Sep. 18–23, 2022).
Roman, M., Fletcher, L., Orton, G., Moses, J., Greathouse, T., RoweGurney, N., Irwin, P., Fujiyoshi, T., Kasaba, Y., Antuñano, A.,
Sinclair, J., De Pater, I., Hammel, H.: 2022, Uranus and Neptune in
the Mid-Infrared: Recent Discoveries and Future Opportunities with
JWST, 44th COSPAR Scientific Assembly, (Athene, Greece, Jul.
16–24, 2022).
Rousselle, J., Gee, W., Koshida, S., Morihana, K., Moritani, Y.,
Okita, H., Ramos, L., Tamura, N., Wung, M., Yoshida, H., thePFS collaboration: 2023, PFS: Status of hardware commissioning at
Subaru, Subaru Users Meeting FY2022, (Tokyo, Japan, Jan. 31–Feb.
2, 2023).
Safonov, B., Millar-Blanchaer, M., Zhang, M., Norris, B. R., Guyon,
O., Lozi, J., Sallum, S.: 2022, Differential speckle polarimetry
with SCExAO VAMPIRES, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Saito, T.: 2022, Negative AGN feedback in the prototypical Seyfert 2galaxy NGC 1068, A half century of millimeter and submillimeter
astronomy: Impact on astronomy/astrophysics and the future,(Miyakojima, Japan, Dec. 15–18, 2022).
Saito, T.: 2023, Molecular Clouds in Nearby Normal and Extreme
Galaxies, East-Asian ALMA Science Workshop 2023, (New Taipei
City, Taiwan, Feb., 14–17, 2023).
Sakabe, K., Ikeda, Y., Oya, S., Bessho, T., Kojima, R., Komaki, M.,
Jun, T., Kawakita, H.: 2022, The adaptive optics simulation andimprovement plan of CRAO attached to the 1.3m Araki Telescope,
SPIE Astronomical Telescopes + Instrumentation, (Montréal, QC,
Canada, Jul. 17–22, 2022).
Sakai, D., Oyama, T., Kobayashi, H., Honma, M.: 2023, Astrometricobservations of water maser sources toward the Galactic Center with
VLBI, IAU Symposium 380: Cosmic Masers: Proper Motion toward
the Next-Generation Large Projects, (Kagoshima, Japan, Mar. 20–24,
2023).
Sakai, N., Nakanishi, H., Kurahara, K., Sakai, D., Hachisuka, K., Kim,
J. S., Kameya, O.: 2023, The origin of the Perseus-arm gap revealedwith VLBI astrometry, IAU Symposium 380: Cosmic Masers: Proper
Motion toward the Next-Generation Large Projects, (Kagoshima,
Japan, Mar. 20–24, 2023).
Sakai, R., Kaneko, K., Imada, H., Kojima, T., Uzawa, Y.: 2022,
Development of Broadband Permittivity Measurement System, 32nd
International Symposium on Space Terahertz Technology, (Baeza
Andalusia, Spain, Oct. 16–20, 2022).
Sakurai, T., IRmag Team: 2022, Calibration and Data Analysis
Pipeline of the Infrared Spectro-Polarimeter at NAOJ/Mitaka, Solar
Polarization Workshop 10, (Kyoto, Japan, Nov. 7–11, 2022).

XIII Publications, Presentations

175

Shan, W.: 2022, Difficulties in RF Noise Measurement of SIS
Mixers, 23rd East Asia Submillimeter-Wave Receiver Technology
Workshop jointly with the Riken-NICT Joint Workshop on Terahertz
Technology, (Wako, Japan, Dec. 14–15, 2022).
Shan, W., Ezaki, S.: 2022, Measurement of Transmission Losses ofSuperconducting Coplanar Waveguide and Microstrip Line with Onchip Resonators at 2 mm Wavelength, 32nd International Symposiumon Space Terahertz Technology, (Baeza Andalusia, Spain, Oct. 16–20,
2022).
Shimakawa, R.: 2022, SWIMMY Survey: The New Age of Data-Driven
Astronomy, HSC-AGN Collaboration Meeting 2022, (Kagoshima,
Japan, Nov. 29–Dec. 4, 2022).
Shimojo, M., Namekata K., Iwai, K., Asai, A., Watanabe, K.: 2022,
Comparing solar and stellar activities via microwave, Plasma
Explosions in the Universe (PEU 2022), (Kyoto, Japan, Sep. 6–8,
2022).
Singh, S., Eisenmann, M., Leonardi, M.: 2023, Fast Birefringencemeasurement and compensation using a pair of identical liquid
crystals, International Conference on the Physics of the two infinites,(Kyoto, Japan, Mar. 27–30, 2023).
Sirbu, D., Belikov, R., Bendek, E., Guyon, O., Kern, B., Lozi, J., Marx,
D., Mendillo, C., Pluzhnik, E., Mejia Prada, C., Riggs, A. E., Ruane,
G.: 2023, Multi-Star Wavefront Control: Update on Technology
Development for Roman Space Telescope and IR/O/UV, AAS
meeting #241, (Seattle, WA, USA, Jan. 8–12, 2023).
Skaf, N., Guyon, O., Boccaletti, A., Gendron, E., Deo, V., Vievard,
S., Lozi, J., Ahn, K., Currie, T.: 2022, Imaged-based adaptive
optics wavefront sensor referencing for high contrast imaging, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Smee, S. A., Gunn, J. E., Barkhouser, R. H., Peebles, J., Loomis, C.
P., Dohlen, K., Kado-Fong, E., Givans, J., J., Golebiowski, M.,
Gray, A., Hammond, R. P., Hope, S. C., Lupton, R., Moritani, Y.,
Tamura, N.: 2022, Performance of the near-infrared camera for the
Subaru Prime Focus Spectrograph, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Song, D., Ishikawa, R., McKenzie, D. E., Trujillo Bueno, J., Auchère, F.,
Kano, R., Rachmeler, L. A., Okamoto, T. J., Kobayashi, K., Bethge,
C.: 2022, The CLASP2 and CLASP2.1 missions for measuring
chromospheric magnetic fields, Solar Polarization Workshop 10,(Kyoto, Japan, Nov. 7–11, 2022).
Steidel, C., et al. including Uraguchi, F., Ozaki, S.: 2022, Designand development of WFOS, the Wide-Field Optical Spectrographfor the Thirty Meter Telescope, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Suematsu, Y., Iju, T., Shinoda, K., Hagino, M., Ueno, S.: 2022,
LiNbO3 Fabry-Perot etalons for solar near-infrared narrow-passband
tunable filtergraph, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Sunada, K., Hirota, T., Kim, M. K., Burns, R. A.: 2023, Intensity
monitor of water maser emission associated with massive YSOs, IAU
Symposium 380: Cosmic Masers: Proper Motion toward the NextGeneration Large Projects, (Kagoshima, Japan, Mar. 20–24, 2023).
Takahashi, R.: 2022, Suspension health check, The 29th KAGRA face
to face meeting, (Tokyo, Japan, Aug. 1–3. 2022).
Takeda, M., Kushibiki, K., Hosobata, T., Yamagata, Y., Morita, S., Saiki,

176

XIII Publications, Presentations

T., Nakagawa, K., Ohtake, Y., Motohara, K., Ozaki, S., Tsuzuki, T.,
Takahashi, H., Konishi, M.: 2022, Diamond machining of two-in-one
optical element including slice mirror array for near-infrared integralfield spectrograph, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Takekoshi, T., Uno, S., Inoue, S., Lee, K., Chin, K., Naganuma, T.,
Niwa, Y., Fujita, K., Kouchi, A., Kimura, Y., Nakatsubo, S., Tsuzuki,T., Kawabe, R., Oshima, T.: 2022, Development of GLTCAM: mm/
submm muti-color camera for the Greenland telescope, A half century
of millimeter and submillimeter astronomy: Impact on astronomy/
astrophysics and the future, (Miyakojima, Japan, Dec. 15–18, 2022).
Takemura, H., Nakamura, F., Benjamin, W.: 2022, Construction of
CMFs with 3D MHD simulation data for future observations, A
half century of millimeter and submillimeter astronomy: Impact on
astronomy/astrophysics and the future, (Miyakojima, Japan, Dec.
15–18, 2022).
Takemura, H., Nakamura, F., CARMA-NRO Orion survey team:2022, Dense core survey and construction of CMF with CARMANRO survey data, Star Formation in Different Environments 2022,(Quy Nhon, Vietnam, Aug. 22–26, 2022).
Tamura, N., et al. including Moritani, Y., Ishizuka, Y., Kamata, Y.,
Arai, A., Furusawa, H., Hamano, S., He, W., Ishigaki, M. N.,
Jeschke, E., Kawanomoto, S., Koike, M., Komatsu, E., Koshida,S., Mineo, S., Miyazaki, S., Morishima, T., Murata, K., Okita, H.,
Onodera, M., Pyo, T.-S., Ramos, L., Rousselle, J. P., Schubert, K.,
Tait, P. J., Takagi, Y., Tanaka, M., Tanaka, Y., Wung, M., Yoshida,
H., Yoshida, M., Yamashita, T.: 2022, Prime Focus Spectrograph(PFS) for the Subaru Telescope: its start of the last development
phase, SPIE Astronomical Telescopes + Instrumentation, (Montréal,
QC, Canada, Jul. 17–22, 2022).
Tanaka, I.: 2022, The Detection of the New Arid Meteor Shower froma Live-Streaming Camera on Maunakea, Hawaii, Meteoroids 2022
Conference, (Online, Jun. 13–17, 2022).
Tanaka, Y., Minowa, Y., Ono, Y., Terao, K., Yoshida, H., Akiyama, M.,
Martínez Rey, N., Herrald, N., d'Orgeville, C., Rigaut, F., Vaughn, I.,
Chandler, D., Haynes, D., Schofield, W.: 2022, Optical design of the
Wavefront sensing in the ULTIMATE-Subaru Ground Layer Adaptive
Optics system, SPIE Astronomical Telescopes + Instrumentation,(Montréal, QC, Canada, Jul. 17–22, 2022).
Tashima, Y., Ohmura, T., Machida, M.: 2022, Pseudo-observation of
spiral galaxies focusing on depolarization based on MHD simulation,
LOFAR Family Meeting 2022, (Cologne, Germany, Jun. 13-17,2022).
Tatematsu, K.: 2022, The establishment of the chemical evolution, theachievement of the Mt. Fuji Submillimeter-wave Telescope, andfuture
prospects, Next Generation Astrochemistry, (Tokyo, Japan, Nov. 29–
Dec. 2, 2022).
Terao, K., Akiyama, M., Minowa, Y., Ono, Y., Ogane, H., Akasawa, T.,
Oya, S., Yamamuro, T.: 2022, ULTIMATE-START: current status of
the Subaru Tomography Adaptive optics Research experimenT, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Toba, T.: 2022, An Introduction of Dust-Obscured AGN Viewed with
Multi-Wavelength Data, 2022 NCHU Astrophysics Symposium,(Online, Sep. 2, 2022).
Toba, Y.: 2022, An overview of the HSC-AGN sciences, Tracingthe SMBH growth: outlook beyond the HSC-SSP, and futurecollaborations, (Kagoshima, Japan, Nov. 30–Dec. 2, 2022).
Toba, Y., Hashiguchi, A., Ota, N., Oguri, M., Okabe, N., Hsieh, B.-C.,
Yanagawa, A., Ueda, Y., HSC Projects 364 and 417 members: 2022,
Dependence of AGN fraction on cluster redshift and the distancefrom the cluster center viewed with Subaru Hyper Suprime-Cam,44th COSPAR Scientific Assembly, (Athene, Greece, Jul. 16–24,
2022).
Toba, Y., Liu, T., Urrutia, T., Salvato, M., Li, J., Ueda, Y., Brusa, M.,
Yutani, N., Wada, K., HSC-eROSITA AGN collaboration: 2022,
ROSITA and WISE view of dust-obscured AGN at z < 4, What drives
the growth of black holes: a decade of reflection, (Reykjavik, Iceland,
Sep. 26–30, 2022).
Toba, Y., PFS-GE AGN subWG: 2023, PFS-SSP preparation: AGN
sciences with cosmology and galaxy evolution surveys, Subaru Users
Meeting FY2022, (Tokyo, Japan, Jan. 31–Feb. 2, 2023).
Toba, Y., Yamada, S., Matsubayashi, K., Terao K., Moriya., A., Ueda, Y.,
GOLAS-KOOLS collaboration: 2023, How do galaxy mergers affectthe ionized gas kinematics of galaxies? ~KOOLS-IFU/Seimei viewof local U/LIRGs~, 9th Galaxy Evolution Workshop, (Kyoto, Japan,
Feb. 20–23, 2023).
Tokoku, C., Ozaki, S., Moriya, T., Yanagisawa, K., Motohara,
K., Ouchi, M., Tominaga, N., Tanaka, M., Ono, Y., Minowa, Y.,
Hayano, Y., Koyama, Y., Ali, S., Tanaka, M., Akiyama, M., Nagao,T., Matsuoka, Y., Kushibiki, K., Homan, S., Yasuda, A., Yoshida,M.: 2022, NINJA : an LTAO assisted optical and near-infrared
spectrograph of Subaru Telescope, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Tokoku, C., Ozaki, S., Moriya, T., Yanagisawa, K., Motohara, K.,
Ouchi, M., Tominaga, N., Tanaka, M., Ono, Y., Minowa, Y.,
Hayano, Y., Koyama, Y., Ali, S., Tanaka, M., Akiyama, M., Nagao,N., Matsuoka, Y., Kushibiki, K., Homan, S., Yasuda, A., Yoshida,M.: 2023, NINJA: Subaru Optical-to-NIR spectrograph optimized
for LTAO, The First SUPER-IRNET Workshop - Rebooting Our InPerson Collaboration, (Tokyo, Japan, Mar. 23–24, 2023).
Tomaru, T., Kimura, N., Hasegawa, K., Saito, Y., on behalf of KAGRA:
2022, Vacuum System in KAGRA Gravitational Wave Telescope, The
22nd International Vacuum Congress, (Sapporo, Japan, Sep. 11–18,
2022).
Tomaru, T., on behalf of KAGRA: 2022, Cryogenics in Gravitational
Wave Telescopes (Half Plenary), 29th Low Temperature Physics,(Sapporo, Japan, Aug. 18–24, 2022).
Tominaga, N.: 2022, Transient survey with Subaru/Hyper Suprime-Cam,
Exploring The Transient Universe, (Tokyo, Japan, Dec. 14–16, 2022).
Torres-Quijano, A. R., Currie, T., Guyon, O., Lozi, J., Groff, T.,
Chilcote, J., Packham, C.: 2022, SCExAO/CHARIS Multi-Epoch
High-Contrast Spectroscopy of HD 1160 B, Exoplanets IV, (Las
Vegas, NV, USA, May 1–6, 2022).
Tsuzuki, T., Katsukawa, Y., Uraguchi, F., Kawabata, Y., Hara,
H., Kubo, M., Nodomi, Y., Suematsu, Y., Shimizu, T.: 2022,
Development of an optical system for near-infrared spectropolarimeter onboard Sunrise balloon-borne solar observatory, 13th
Int. Conf. “Optics-photonics Design & Fabrication”, (Sapporo, Japan,
Aug. 3–5, 2022).
Usuda-Sato, K., Hara, T., Togashi, T., Hiratsuka, Y., Tomita, A.: 2022,
Three High School Teachers Bring the Subaru Telescope's Big Data

to Their Classrooms, 4th Shaw-IAU Workshop on Astronomy for
Education, (Online, Nov. 15–17, 2022).
Usuda-Sato, K., Tanaka, M., Koike, M., Shibata, J., Naito, S.,
Yamaoka, H., Kamegai, K., Umemoto, T.: 2022, GALAXY CRUISE:
What Motivates the General Public in a Citizen Science Project, CAP
Conference 2022, (Sydney, Australia, Sept. 12–16, 2022).
Uzawa, Y., Kojima, T., Makise, K., Kawakami, A., Kozuki, Y.,
Masui, S., Shan, W.: 2022, Development of an SIS-mixer-based
low-noise amplifier with Josephson oscillator pumping, Applied
Superconductivity Conference 2022, (Honolulu, HI, USA, Oct.
23–28, 2022).
Uzawa, Y., Kojima, T., Makise, K., Masui, S., Kozuki, Y., Shan,
W., Kawakami, A., Terai, H.: 2022, Research and Development
toward ALMA Upgrades, 2022 JSPS 146th Committee International
Symposium on Superconductor Electronics, (Kyoto, Japan, Sep.
28–30, 2022).
Verbiscer, A., et al. including Ito, T.: 2022, Searching for New Horizons
Targets in the Distant Kuiper Belt, AGU Fall Meeting 2022, (Chicago,
IL, USA and online, Dec. 12–16, 2022).
Verbiscer, A., et al. including Ito, T.: 2023, Results From the Search for
New Horizons Targets in the Distant Kuiper Belt Using Subaru Hyper
Suprime-Cam, Subaru Users Meeting FY2022, (Tokyo, Japan, Jan.
31–Feb. 2, 2023).
Verbiscer, A., Porter, S., Fraser, W. C., Kavelaars, J. J., Benecchi, S.,
Gerdes, D., Lin, H-W., Buie, M. W., Yoshida, F., Ito, T., Spencer, J.
R., Stern, S. A., Napier, K., Peltier, L., Terai, T.: 2022, Searching for
New Horizons Targets in the Distant Kuiper Belt, AGU Fall Meeting
2022, (Chicago, IL, USA and online, Dec. 12–16, 2022).
Vidal, F., Galland, N., Bertrou-Cantou, A., Gendron, E., Deo, V., Zidi,
A., Ferreira, F., Sevin, A., Kulscar, C., Raynaud, H.-F., Clenet, Y.,
Davies, R.: 2022, The MICADO first light imager for the ELT: FDR
numerical simulations for the SCAO mode, SPIE Astronomical
Telescopes + Instrumentation, (Montréal, QC, Canada, Jul. 17–22,2022).
Vievard, S. B., Bonnefois, A., Cassaing, F., Mugnier, L. M., Sauvage, J.
F., Guyon, O., Lozi, J., Deo, V., Ahn, K., Skaf, N.: 2022, Linearized
Analytical Phase Diversity: towards lab and on-sky demonstrationon the Subaru Telescope, SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Vievard, S. B., Deo, V., Huby, E., Lacour, S., Guyon, O., Cvetojevic, N.,
Barjot, K., Martin, G., Lallement, M., Lozi, J., Kotani, T., Marchis,F., Rouan, D., Ahn, K., Skaf, N., Perrin, G.: 2022, Interferometricwavefront sensing at FIRST/SCExAO: self-calibrated fiberedpupil-remapping spectrocopy using a metrology laser source, SPIE
Astronomical Telescopes + Instrumentation, (Montréal, QC, Canada,Jul. 17–22, 2022).
Vorster, J. M., Chibueze, J. O., Hirota, T.: 2023, Spatio-kinematics
of water masers in the HMSFR NGC 6334I before and during an
accretion burst, IAU Symposium 380: Cosmic Masers: Proper Motion
toward the Next-Generation Large Projects, (Kagoshima, Japan, Mar.
20–24, 2023).
Wang, S.-Y., et al. including Moritani, Y., Rousselle, J., Yoshida, H.,
Koshida, S., Takato, N.: 2022, Prime focus spectrograph (PFS) for
the Subaru Telescope: the prime focus instrument, SPIE Astronomical
Telescopes + Instrumentation, (Montréal, QC, Canada, Jul. 17–22,2022).

XIII Publications, Presentations

177

Washimi, T., on behalf of the KAGRA collaboration: 2022, Underground
Environment KAGRA, Workshop on the development of innovative
tools for new collaborations within gravitational wave detection
experiments, (Online, Apr. 15, 2022).
Washimi, T., on behalf of the KAGRA collaboration: 2022, Tonga's
volcano eruption signals measured by the evironmental monitoring
systems of KAGRA Observatory, GWADW2022 - Approaching the
low-frequency design sensitivity of ground-based detectors, (Online,
May 23–28, 2022).
Washimi, T., on behalf of the KAGRA collaboration: 2022, Kamioka
Lightning&Thundercloud observation and its application for the
astroparticle experiments, Unraveling the History of the Universe andMatter Evolution with Underground Physics 2022, (Tokyo, Japan,
Jun. 13–15, 2022).
Watanabe, K., Maeda, M., Nishimoto, S., Kitajima, S., Shimojo, M.,
Namekata, K., Masuda, S.: 2022, Relationship between Microwave
and EUV Emission in Solar Cycle Variations and Prediction of Solar
EUV Emission Spectrum by Machine Learning Method, AGU Fall
Meeting 2022, (Chicago, IL, USA and online, Dec. 12–16, 2022).
Wei, C.-E., Nomura, H., Theule, P., Walsh, C.: 2022, Formation ofComplex Organic Molecules through Ice Mantle Reactions, Next
Generation Astrochemistry, (Tokyo, Japan, Nov. 29–Dec. 2, 2022).
Wong, A. P., Norris, B. R. M., Deo, V., Guyon, O., Tuthill, P. G., Lozi, J.,
Vievard, S., Ahn, K.: 2022, Machine learning for wavefront sensing,
SPIE Astronomical Telescopes + Instrumentation, (Montréal, QC,
Canada, Jul. 17–22, 2022).
Wong, K. C.: 2022, An Independent Measurement of H0 from Lensed
Quasars, Exploring the Dark Universe, (Blois, France, May 22–27,2022).
Wong, K. C.: 2022, An Independent Measurement of the Hubble
Constant from Lensed Quasars, Gravity: Current challenges in blackhole physics and cosmology, (Kyoto, Japan, Jun. 20–Jul. 1, 2022).
Wong, K. C.: 2022, TDCOSMO: Lens modeling software comparison
and time delay prediction for WGD 2038-4008, 31st IAU General
Assembly, (Busan, Korea, Aug. 2–11, 2022).
Wong, K. C.: 2022, New Strong Gravitational Lens Candidates fromthe HSC SSP, ASJ Fall 2022 Meeting, (Niigata, Japan, Sep. 13–15,2022).
Yagi, M., Iye, M., Fukumoto, H.: 2022, PanSTARRS Spin Catalog of
Galaxies, ADASS XXXII, (Online, Oct. 31–Nov. 4, 2022).
Yamamoto, K.: 2022, Separation of Ice Sheet and GIA Mass Variations
in Antarctica Using Satellite Gravimetry andSatellite Altimetry Data,
AGU Fall Meeting 2022, (Chicago, IL, USA and online, Dec. 12–16,
2022).
Yamasaki, Y., Hasegawa, Y., Onishi, T., Ogawa, H., Nishimura A.,
Tatematsu, K., Gonzalez, A., Imada, H., Kaneko, K., Sakai,R., Kojima, T.: 2022, Study of anti-reflection layer on dielectriclens for the new 72–116 GHz 7-beam receiver of the Nobeyama
45-m telescope, 32nd International Symposium on Space Terahertz
Technology, (Baeza Andalusia, Spain, Oct. 16–20, 2022).
Yamashita, M., Itoh, Y., Takagi, Y., Oasa, Y.: 2022, Measurements of
Dynamo Activity and Spots of Zero-Age Main-Sequence Stars with
TESS, COOL STARS 21, (Toulouse, France, Jul. 4–9, 2022).
Yanagisawa, K.: 2023, Early days of the MITSuME Okayama
Telescope, Transients and variables, (Tokyo, Japan, Mar. 9–10, 2023).
Yano, Y., Nakamura, F.: 2022, Time evolution of accretion gas

178

XIII Publications, Presentations

and circumstellar structure due to core merger, A half century of
millimeter and submillimeter astronomy: Impact on astronomy/
astrophysics and the future, (Miyakojima, Japan, Dec. 15–18, 2022).
Yoneta, K., Murakami, N., Nishikawa, J.: 2022, Halftone wave-front
control and a common-path visible nulling coronagraph toward direct
detection of exoplanets, Sensing and Imaging through Scattering andFluctuating Field in Biology, Telecommunication, and Astronomy,(Kanagawa, Japan, Apr. 18–22, 2022).
Yoneta, K., Sudo. S., Hayashi, H., Asano, M., Nishikawa, J., Murakami,
N.: 2022, Recent progress of the facility for coronagraphic
elemental technologies (FACET), SPIE Astronomical Telescopes +Instrumentation, (Montréal, QC, Canada, Jul. 17–22, 2022).
Yoshida, M.: 2022, Transient Search with Subaru Telescope, 31st IAU
General Assembly, (Busan, Korea, Aug. 2–11, 2022).
Yoshida, M.: 2023, J-GEM: Brief History and Current Status, Transientsand variables, (Tokyo, Japan, Mar. 9–10, 2023).
Yoshida, M.: 2023, Reports from Subaru Telescope, The First SUPERIRNET Workshop - Rebooting Our In-Person Collaboration, (Tokyo,
Japan, Mar. 23–24, 2023).
Yoshida, T., Nomura, H., Furuya K., Tsukagoshi T., Lee S.: 2022,
A New Method for Direct Measurament of Isotopologue Ratios
in Protoplanetary Disks: A Case Study of the 12CO/13CO Ratio in
the TW Hya Disk , NCTS-ASIAA Workshop: Stars, Planets, andFormosa, (Online, Aug. 15–19, 2022).
Yoshida, T., Nomura, H., Tsukagoshi, T., Furuya, K., Ueda, T.: 2022,
Discovery of Line Pressure Broadening in Protoplanetary Disks andConstraint on Gas Surface Density of the TW Hya Disk, Moleculesin Extreme Environments: Near and Far, (Mitaka, Japan, Nov. 23–25,
2022).
Yoshida, T., Nomura, H., Tsukagoshi, T., Furuya, K., Ueda, T.: 2022,
Discovery of Line Pressure Broadening in Protoplanetary Disks
and Constraint on Gas Surface Density of the TW Hya Disk, Next
Generation Astrochemistry, (Tokyo, Japan, Nov. 29–Dec. 2, 2022).
Yoshida, T., Nomura, H., Tsukagoshi, T., Furuya, K., Ueda, T.: 2022,
Discovery of Line Pressure Broadening in Protoplanetary Disks
and Constraint on Gas Surface Density of the TW Hya Disk, A
half century of millimeter and submillimeter astronomy: Impact on
astronomy/astrophysics and the future, (Miyakojima, Japan, Dec.
15–18, 2022).
Yoshida, T., Nomura, H., Tsukagoshi, T., Furuya, K., Ueda, T.: 2023,
Discovery of Line Pressure Broadening in Protoplanetary Disks andConstraint on Gas Surface Density of the TW Hya Disk, East-Asian
ALMA Science Workshop 2023, (New Taipei City, Taiwan, Feb.,
14–17, 2023).
Yoshida, Y., Kokubo, E., Tanaka, H.: 2022, Simulating dust monomer
collisions: expansion of the JKR theory, Forming and Exploring
Habitable Worlds , (Edinburgh, UK, Nov. 7–13, 2022).
Zhou, X., Yokoyama, T., Iijima, H., Matsumoto, T., Toriumi, S.,
Katsukawa, Y., Kubo, M.: 2022, Synthetic Ca II 8542A Stokes
profile of chromospheric magnetic reconnection in emerging flux
region, Solar Polarization Workshop 10, (Kyoto, Japan, Nov. 7–11,2022).

Annua
lRe
por
toft
he
Na
t
i
ona
lAs
t
r
onomi
c
a
lObs
e
r
v
a
t
or
y
ofJ
a
pa
n
Vol
ume25Fiscal2022