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Cover Caption
The image shows the intensity map of the ionised carbon in the galaxy BRI 1335-0417 at 12.4
billion years ago taken by Atacama Large Millimeter/submillimeter Array (ALMA). Spiralarms are seen on both sides of the compact and bright region in the galactic centre. Further
analysis of the gas motion indicates the presence of a compact mass structure and rotating
disk structure in the galaxy.
Credit: ALMA (ESO/NAOJ/NRAO), T.Tsukui & S.Iguchi

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 KOKYUSHA Co., Ltd.
5-1-1 Kamisunacho, Tachikawa-shi, Tokyo 190-0032, Japan
TEX: +81-42-536-3511
FAX: +81-42-536-3898

Annual Report of the
National Astronomical Observatory of Japan

Volume 24, Fiscal 2021

Preface

Saku TSUNETA
Director General

I Scientific Highlights April 2021 – March 2022
II Status Reports of Research Activities
01. Subaru Telescope
02. Nobeyama Radio Observatory
03. Mizusawa VLBI Observatory
04. Solar Science Observatory (SOL)
05. ALMA Project, NAOJ Chile, and ASTE Project
06. Center for Computational Astrophysics (CfCA)
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. Office of International Relations
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

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P R E FA C E
Saku TSUNETA
Director General of NAOJ

Fiscal Year 2021, like Fiscal Year 2020, felt a large impact fromthe novel coronavirus. The National Astronomical Observatoryof Japan (NAOJ) has mindfully continued our efforts while
ensuring the safety of our employees and neighbors through thecontinuation of the dual work style of telework and commuting,and by holding events for the public and research conferences
online.
The big news in the astronomy world was the successful launchof the James Webb Space Telescope (JWST) in December 2021,
after long years of work by the American National Aeronautics
and Space Administration (NASA), the European Space Agency,
and others. Like the epoch-defining Hubble Space Telescope
launched 30 years earlier, JWST is expected to show us neverbefore seen facets of the Universe. Also, the National Academiesof Sciences, Engineering, and Medicine’s Decadal Survey on
Astronomy and Astrophysics 2020 (Astro2020) which sets thetone for the coming decade of astronomy and space science
research was released. In it the US-ELT, including the Thirty
Meter Telescope TMT with participation by Japan, was the
top priority for a frontier ground-based observatory. These
activities are outside of Japan, but some of JWST’s planned
observations are based on results from ALMA and the Subaru
Telescope operated by NAOJ, and the high evaluation of USELT in the Decadal Survey is surely due in part to Japan’s steadyadvancement of the preparation for the telescope structure andproduction of mirror substrates. Astronomy is no longer a fieldthat can be pursued within a single country. Particularly in times
of world instability like the present, we have high expectations
for the advancement of international collaboration to solve manyof the mysteries of the Universe based on peace and humanity’s
intellectual curiosity.
Looking at NAOJ’s activities, there were many research results
published in 2021. The Seimei Telescope at Kyoto University’s
Okayama Observatory, for which the Subaru Telescope
Okayama Branch administrates the open-use, was the first to
observe the eruption of a supermassive gas filament as the resultof a “super flare,” a giant explosive phenomenon, on the surface
of a Sun-like star. This offers hints to the effects the young Sun
had on the early Earth, helping to answer questions about how
the environment for early life evolved.
Approximately 100 free-floating planets were found from
Subaru Telescope observations of a young stellar associationnear the constellation Ophiuchus. It is thought that planets which
originally formed around stars were ejected from their planetarysystems at some point. This result too provides hints about how
the Solar System evolved into its current configuration.
Big news came out of the ALMA archive in the form of the
discovery of a galaxy with spiral morphology 12.4 billion years

ago. This result will help to solve the mystery of how spiralgalaxies like our home Milky Way Galaxy are formed. The factthat this result was obtained from the archived data without
making new observations shows the importance of a wellmaintained data archive. In other ALMA results, many kinds oforganic molecules were detected in the extreme outer edge ofthe Galaxy, where the environment from the beginning of theformation of the Milky Way Galaxy has been preserved up to
the present day; and the spatial distribution of molecules with
deuterium around the site of planet formation was mapped.
Deuterium is the key to searching for the origins of the wateron Earth. As the detections of different materials in different
environments increase, they bring us closer to understanding theorigins of the Solar System and life.
The release of “Uchuu” the world’s largest virtual Universe
courtesy of the supercomputer “ATERUI II” can safely be called
an important contribution to the world astronomy community.
In Uchuu, the dark matter which controls the Universe isrepresented by 2.1 trillion particles. Through calculations of dark
matter mutual gravitational interactions, galaxies of various sizes
are depicted in detail throughout a huge space 9.6 billion lightyears across. Comparing this data to large-scale survey programsfrom the Subaru Telescope and other facilities will advance ourunderstanding of the evolution of galaxies and the large-scale
structure of the Universe.
This fiscal year, the Industry Liaison Office launched in2020 opened a website and established various proceduresfor collaboration with industry, strengthening our ties to thewider society. As a matter of fact, collaboration with industry
is gradually developing. In September 2021, we enteredan agreement with the space start-up corporation ALE forthe development of a small microwave sounder for private
meteorological satellites. Also, a comprehensive cooperationagreement was concluded with IWATE NIPPO CO., LTD. (anews media company) aiming to establish a support venture
for next-generation researchers centered on Mizusawa VLBI
Observatory, where both companies will employ the researchers
as “two-fisted scientists and journalists.” This is an example of a
new approach based on cooperation between a research instituteand media, an innovative approach as a means of securing talent
for the advancement of science.
Here I would like to summarize the status of NAOJ’s various
projects in FY 2021. At the Subaru Telescope, using the
supplemental budget which has been received almost every year
since FY 2018, preventative maintenance in response to theaging of the facility has been undertaken, including repairs to
the mechanical parts of the dome, and complete replacement of
the dome air-conditioning system and the uninterruptible power
supply units. As part of the facility update, open-use observations

have switched almost entirely to remote observations. (Remoteobservation system is scheduled to be completed in 2022.) Thisis expected to lead to more efficient open-use observations andmulti-messenger and gravitational wave astronomy.
The Subaru Strategic Program using the ultra-wide field of view
prime focus camera Hyper Suprime-Cam (HSC) which started in
March 2014 concluded successfully at the end of calendar year
2021 after observing for a total of 330 nights over the course of
8 years. The third public data release occurred in August 2021.
Analysis of the weak gravitational lensing in the first 3 years ofdata enabled a high spatial resolution map of dark matter acrossabout 500 square degrees.
The wide-field, multi-object spectrograph PFS (Prime Focus
Spectrograph) is conducting test observations to assess thetechnical performance of the instrument. Aiming to be ready for
open-use observations in FY 2024, planning of the observation
procedure and data analysis tool development are ongoing.
There were test observations with the prototype laser guide starsystem of the ground layer adaptive optics (GLAO) system
which is necessary for the wide-field, high-resolution infraredobservational instrument ULTIMATE. ULTIMATE together
with HSC and PFS will form the core instrument suite of Subaru
Telescope 2.0. It will enable hitherto impossible wide-field,
high-resolution observations in the infrared wavelength range.
The infrared Doppler instrument (IRD), which searches forterrestrial planets, started Subaru Strategic Program observations
in February 2019. In FY 2021, intensive observations were
performed for 35 nights to search for terrestrial planets aroundnearby M type stars. Measurements of atomic abundances in
the atmospheres of M type stars were published. A line-of-sightvelocity measurement precision of 2 m per second has beenstability achieved. The combination of the extreme adaptive
optics system SCExAO and the near infrared high-contrast
integral field spectrograph CHARIS produced observations
looking for protoplanets in the circumstellar disk around youngstars. The development, maintenance, and operation of these
instruments are proceeding through collaboration between
Subaru Telescope and the Astrobiology Center of the National
Institutes of Natural Sciences.
ALMA was forced to suspend observations for approximately
1 year starting in March 2020 due to the COVID-19 pandemic,
but has been able to incrementally return to normal operations.
Cycle 8, the 9th ALMA open-use observation cycle, started
from October 2021. There were 1,735 observation proposals for
Cycle 8 submitted from all over the world; this is a record forthe number of observation proposals. The number of scientificpapers published based on ALMA data reached 2,752 during
the ten-and-a-half-years ending with FY 2021. Japan continued
to have the second largest share of published papers after theUnited States.
In instrument development, tangible results are coming out of
the collaboration in East Asia centered on NAOJ. First, August2021 saw the successful first light of the Band 1 receivers(bandwidth 35–50 GHz) for which the development was led by
the Academia Sinica Institute of Astronomy and Astrophysics in
Taiwan. NAOJ is responsible for the design and manufacturingof the corrugated horns, one of the vital components for the Band
1 receivers. The 3D metal printer in the Advanced Technology
Center (ATC) has been busy mass-producing the horns. In

February 2022, the new spectrometer, for which development
was led by the Korea Astronomy and Space Science Institute,saw first-light on the Atacama Compact Array (ACA, Morita
Array). On the other hand, preparation is also underway for thestart of the ALMA 2.0 project aiming to drastically improve theperformance specs of the ALMA array, including the design ofhigh-performance parts for the Band 8 receivers (385–500 GHz).
TMT is a project to build an extremely large telescope with a
30 m diameter being advanced through collaboration between 5
countries: Japan, the United States, Canada, India, and China.
Onsite construction is currently on hold due to protests, but
the TMT International Observatory (TIO) Project Manager,
who oversees the entire project, has moved to Hilo, Hawai`iand together with NAOJ employees, first and foremost the
Director of NAOJ TMT, is engaging in a direct dialog withlocal individuals and groups who have been opposed to TMT.
They are also participating in after-school tutoring programs
at local schools and other programs. In these ways they are
working to build trust with the people in the local area, including
the Native Hawaiian community. As each country continues
to make progress on its workshare, in Japan preparations
continue for manufacturing the main body structure of thetelescope. In ATC the detailed design for the Infrared Imaging
Spectrograph (IRIS) and the conceptual design for the Wide
Field Optical Spectrograph (WFOS) are proceeding favorably.
The development of the science operations plan for after thetelescope is completed is being led by the United States, andthere is active discussion within the Japanese community as
well.
In the Division of Science, multi-wavelength observations
and theoretical research are blending together organically.
Fruits of this combination include research combining ALMA
observations of rotating jets with MHD models to understandthe growth of young stars; and research tying multi-wavelength
observations to theoretical predictions of electron capture supernovae to further our understanding of the overall picture ofstellar evolution.
At KAGRA, the Large-scale Cryogenic Gravitational Wave
Telescope, led by the Institute for Cosmic Ray Research of
the University of Tokyo with the participation of NAOJ andthe High Energy Accelerator Research Organization KEK,
the upgrades of the ultra-low-frequency vibration isolators,
and other components for which NAOJ is responsible,
have been completed and the restart and adjustment of themain interferometer have commenced. The goal is to detectgravitational waves as part of the next coordinated international
observing run O4 scheduled to start from March 2023. Also
collaborative research between NAOJ and KASI has found apotential solution to the birefringence problem in the sapphire
mirrors which has been a source of much anxiety in KAGRA.
Preparations are underway to install new mirrors before theO5 coordinated international observing run. Also the prospectof introducing frequency-dependent squeezing technology in
KAGRA is being examined, now that the proof-of-concept
experiments using the interferometric gravitational wave antenna
TAMA300 have successfully demonstrated the techniques.
In March 2022, the 40th anniversary ceremony was held forNobeyama Radio Observatory. Open-use observations with theNobeyama 45-m Radio Telescope ended in FY 2021. But basedon discussion about the operation of the telescope after that, apolicy of charging for observation time has been implemented.
The renewal of the focal-plane instrument has enabled results
such as the completion of the Nobeyama Mapping Survey.
Also in FY 2021, Mizusawa VLBI Observatory ended VERA
astrometry observations. It plans to shift its research activities
to focus on the East Asian VLBI Network (EAVN). EAVN has
been producing results, such as determining the structure of jetsright after ejection from around a black hole.

In the Astronomy Data Center, users’ meetings were held tosolicit opinions from the wider community for the renewalof the large-scale archive and multi-wavelength data analysis
system. The optical-infrared archive SMOKA has started toaccept the giant data from Tomo-eGozen at the University ofTokyo’s Kiso Observatory and TriCCS on Kyoto University’s
Seimei Telescope. We expect future use of this data to aid thedevelopment of time domain astronomy.

Operation of the 188-cm reflector telescope at the Okayama
Branch of the Subaru Telescope is being led by the Tokyo
Institute of Technology. The total number of visitors has
surpassed 2 million since the facility first opened to the public
in 1960. In cooperation with Asakuchi City, programs includingstar-gazing parties with the Okayama 188-cm Reflector
Telescope have been implemented. In recognition of these
activities and its scientific discoveries to date, the Okayama
Branch received the 2021 Okayama prefecture tourism industry
award. Ishigakijima Astronomical Observatory is a uniqueobservatory operated in collaboration with the local government.
In addition to observations of Solar System objects and researchon explosive phenomena, the 105-cm aperture Murikabushi
Telescope is continuing observations of the SpaceX Starlink
satellites as part of research into light-pollution reduction
techniques. The number of visitors to the facility has passed
150,000 since it opened in 2006. To improve the safety andsecurity of the visitors, the facility plans to change to charged
admission starting from FY 2022.

In the Public Relations Center, efforts to share astronomy resultswith the public have been strengthened. Making the best use of
the internet and video streaming services, it has been making
efforts in public information and outreach activities including
the FUREAI (Friendly) Astronomy program which expanded
to include remote lectures for overseas schools starting fromFY 2020; the broadcast of the May 26, 2021 total lunar eclipse
which, including the archive, accumulated over 2 million views;
and the online regular stargazing parties and online open house
which have enabled participation by a wider range of people
beyond just those who can come to campus.

After being selected as the 4th JAXA Small Satellite in FY
2020, the Solar-C (EUVST) satellite to conduct high resolution
spectroscopy of the Sun at extreme ultraviolet wavelengths has
been preparing for the mission definition review. The CLASP
sounding-rocket telescope experiments, which with participation
by NASA and others have blazed trails in high-sensitivity
polarization observations in the ultraviolet regime, executed
their third flight in October 2021. Data analysis was performed
to determine the 3D structure of the magnetic fields from thephotosphere to the chromosphere. SUNRISE-3 is a balloon
experiment to perform high-resolution polarization observations
with a 1-m aperture optical telescope. NAOJ is developing thenear-infrared spectro-polarimeter SCIP for it. Testing at the
Max Plank Institute for Solar System Research has concluded,
and preparations are underway for a flight in 2022. At NAOJ
development is underway for a high-speed CMOS camera forsoft X-rays and an X-ray collimator for the NASA FOXSI-4
sounding rocket experiment.
Thailand has become a new member of the East Asian
Observatory (EAO), joining Japan, China, the Republic ofKorea, and Taiwan. Board meetings were held regularly for the
stable operation of the James Clerk Maxwell Telescope (JCMT),EAO’s primary responsibility.
In ATC, development continued for a space-grade version of
the InGaAs infrared sensors. This sensor will be installed in
the infrared astrometry satellite JASMINE. Making best use ofATC’s expertise with superconducting devices, development
work has started for the super-low-power-consumption, lownoise microwave amplifiers needed for superconducting quantum
computing as part of JST’s Moonshot research and development
program. Also, in order to strengthen ATC’s development
procedures, it was reorganized into a matrix organization
structure.

The “Results of Evaluation of the Current State of Research”
at the end of the 4 year period published in 2021 found that interms of both research activities and research results NAOJ isof “particularly high quality.” 1 The reason for the former wascited as the establishment of the Division of Science to achieve
research results transcending the boundary between theory
and observation; and the reason for the latter was cited as thelarge-scale statistical research enabled by HSC on the Subaru
Telescope, advancing our understanding on the origin of supermassive black holes and the birth and evolution of stars and the
Universe.
The 2,944 papers published during 2017~2021 by members of
NAOJ have had an international collaboration rate of 80.4 %;
also, 16.4 % of the papers have made it into the Top10 % of
papers published worldwide in terms of citations and 3.5 %have made it into the Top1 % (according to InCites as ofAugust 2022). While as of August 2022, Japanese members
account for only 5.5 % of the total members of the International
Astronomical Union (approximately one quarter the number ofUnited States members), Japan achieved a 9.5 % world share in
the number of papers published in astronomy during 2021 with
1,707 papers. This is Japan’s highest world share among the 22
fields of study, surpassing physics (7.0 %). As of April 1, 2022,
women account for 10.5 % of NAOJ researchers (including
Research and Academic Staff and specially appointed teachers)
up from 8.9 % in the previous fiscal year.
The Office of International Relations opened its new homepage,
providing information on living in Japan, accommodations,immigration procedures for foreign nationals, and an overview
of the area around campus; as well as references for NAOJ
researchers who will serve as hosts.
This concludes my overview of NAOJ’s activities in FY 2020.
More details can be found in the full report. I look forward to
your continued cooperation and support.

(Note 1): The four-year period covered 2016-2019. Evaluation was performed in FY 2020 and the results were released in FY 2021.

I Scientific Highlights(April 2021 – March 2022)
01 Neutrinos Transport and Signal in Core-collapse Supernova
02 Search for Rare Objects with Subaru Telescope × Anomaly Detection
03

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). IV.
Rapidly Growing (Super)Massive Black Holes in Extremely Radio-loud Galaxies

NAGAKURA, H. 002
SHIMAKAWA, R., et al. 003
ICHIKAWA, K., et al. 004

04 Development of a Galactic Model Optimized for the Galactic Bulge

KOSHIMOTO, N., et al. 005

05 Orphan Cloud Bigger than Milky Way Discovered in the Leo Cluster

GE, C., et al. 006

06 Age Distribution of Stars in Boxy/Peanut/X-shaped Bulges Formed without Bar Buckling
07 Planetesimal Dynamics in the Presence of a Giant Planet

BABA, J., et al. 007
GUO, K., KOKUBO, E. 008

08 A Dusty Protocluster Discovered by Planck and Subaru Telescope

KOYAMA, Y., et al. 009

09 Polarization of the Corona Observed During the 2017 and 2019 Total Solar Eclipses

HANAOKA, Y., et al. 010

10Luminosity Functions and Clustering Revealed with ~4,000,000 Galaxies at z ~ 2−7 fromthe Subaru/Hyper-Suprime Cam Survey

11 Interrelation of the Environment of Lyα Emitters and Massive Galaxies at 2 < z < 4.5
12 On the Hubble Constant Tension
13 Hyper Suprime-Cam Legacy Archive
EMPRESS. IV. Extremely Metal-poor Galaxies Including Very Low-mass Primordial

14 Systems: High Fe/O Suggestive of Metal Enrichment by Hypernovae/Pair-instability
Supernovae

15

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). VI.
Distant Filamentary Structures Pointed by High-z Radio Galaxies at z ~ 4

16Discovery of a Directly Imaged Planetary-mass Companion to a Young Taurus M Dwarf
Star

17

Ionizing Radiation from z > 3.3 AGNs with the Hyper Suprime-Cam Survey and the
CFHT Large U-band Deep Survey

HARIKANE, Y., et al. 011
ITO, K., et al. 012
DAINOTTI, M. G., et al. 013
TANAKA, M., et al. 014
ISOBE, Y., et al. 015
UCHIYAMA, H., et al. 016
HIRANO, T., et al. 017
IWATA, I., et al. 018

18 Horizontal Velocity Estimation with Neural Network

ISHIKAWA, R. T., et al. 019

19 Chemical Abundances of nearby M Dwarfs Investigated with IRD-SSP Data

ISHIKAWA, H. T., et al. 020

001

Neutrinos Transport and Signal in Core-collapse Supernova
NAGAKURA, Hiroki(NAOJ)

2.4

Orig
SK-NORPNS baryon-mass [M ]2.2⊙

DUNE-NOR

21 M⊙ model2

JUNO-NOR
Ice-NOR
SK-InV

1.8

16 M⊙ model

DUNE-InV
JUNO-InV
Ice-InV

1.6
9 M⊙ model

1.4
1.2
1
0.2

0.5

1
Time [s]2

4Figure 1: The PNS mass as a function of time for three different
progenitor models: 9-, 16-, and 21 solar masses. The black line
represents the PNS mass obtained from our CCSN simulations,and other colored-lines represent the retrieved PNS mass fromour newly proposed method. The line type distinguishes neutrino
oscillation models. The figure is taken from [1].

In [2,3], we have tacked one of the formidable issues
on CCSN theory: collective neutrino oscillations. In[2], we developed a new neutrino transport code that
can handle any types of neutrino oscillations, transport,
and neutrino matter interactions in a self-consistentmanner. We adopt a Monte-Carlo approach in our code;
the design and implementation of the code is describedin detail. We also carried out a suites of code tests that
include fast-pairwise collective neutrino oscillation (orfast flavor conversion, FFC) with momentum-exchanged
neutrino scatterings. We present rigorous demonstrationsof the code performance for a broad range of neutrino
oscillation problems.

002

I Scientific Highlights

Orig

50

16 M⊙ model

SK-NOR
DUNE-NOR
JUNO-NORPNS radius [km]I have worked on the theor y of core-collapse
supernova (CCSN) by using large-scale numericalsimulations. In the last year, I have paid a special
attention to neutrino dynamics during the development of
explosion. In [1], we proposed a new strategy to estimate
proto-neutron star (PNS) mass and radius from neutrinosignals in real observations. We analyzed theoreticalmodels of neutrino signal obtained by a series of multidimensional CCSN simulations. We found some robust
correlations between PNS properties (such as mass andradius) and neutrino signal. We evaluated the correlationand provided useful fitting formulae for which the PNS
mass and radius are retrieved from the total number ofneutrino events at each terrestrial neutrino detector. As
shown in Fig. 1, we demonstrated that PNS mass can be
retrieved only from neutrino signal within ~ 10 % errors.
For PNS radii (see Fig. 2), the error is much smaller thanthe case with PNS mass, which is within percents.

Ice-NOR40

SK-InV
DUNE-InV
JUNO-InV30

Ice-InV

20

10
0.2

0.5

1
Time [s]2

4Figure 2: Same as Fig. 1 but for PNS radius. We only display thecase with 16 solar mass model. The figure is taken from [1].

In [3], we studied a possibility of FFC in CCSN core,
paying particular attention to roles of stellar rotation.
We carried out two-dimensional CCSN simulations withfull Boltzmann neutrino transport. It should be notedthat the multi-angle treatment in neutrino transport
plays a crucial role to analyze the occurrence of FFC.
We found that stellar rotation facilitates the occurrenceof FFC around the equatorial region. This is mainly
due to the expansion of low-electron-fraction region,
which enhances the disparity of neutrino absorption
between electron-type and their anti-partners. This
study motivates further investigation of FFC in CCSN
environment.

References[1] Nagakura, H., Vartanyan, D.: 2022, MNRAS, 512, 2806N.
[2] Kato, C., Nagakura, H., Morinaga, T.: 2021, ApJS, 257, 55K.
[3] Harada, A., Nagakura, H.: 2022, ApJ, 924, 109H.

Search for Rare Objects
with Subaru Telescope × Anomaly Detection
SHIMAKAWA, Rhythm, TANAKA, Masayuki, TOBA, Yoshiki(NAOJ)TANAKA, Takumi, SHIMASAKU, Kazuhiro, KASHIKAWA, Nobunari				(University of Tokyo)				

Astronomy has made great strides through thediscover y of u nexpected and u n k now n physicalphenomena and species, such as the Nobel Prizewinning discovery of giant exoplanets by Mayor andQueloz [1], and the recent discovery of fast radio bursts
by Lorimer et al. [2]. The ultimate goal of this project is
to consciously and thoroughly search for rare phenomena
and astronomical sources in the universe, including
unknown events that may bring innovations fromastronomical big data, by utilizing machine learning.
This report introduces our initial results from the search
for low-redshift rare objects using a deep anomaly
detection based on convolutional neural networks (CNN),
as the first series of our project [3].
There are two ways to rare object searches: (1)science-driven methods that use known information of
specific rare objects as training data, and (2) data-driven
methods that find anomalies by analyzing the overall
data structure without any priors. The former approachhas been adopted in most of previous work such as
surveys of the most distant galaxy and black hole.
However, the data-driven approach has not been used
due to its inefficiency, requiring a huge amount of data
to understand the whole structure, and the lack of proper
methods.
Nowadays, the rapidly developing machine learningand legacy surveys with large telescopes, such as the
Subaru Hyper Suprime-Cam (HSC) strategic survey,
enabled the practical application of data-driven searches.
This work attempted to detect rare objects with outlier
features in the multi-band data (grizy) from Subaru HSC
over ~800 deg 2 using deep anomaly detection, which
has a wide range of applications from industrial use to
medical diagnosis. The deep anomaly detection consistsof an encoder and a decoder that perform complex
nonlinear transformations, each of which is optimized
to compress and reconstruct unlabeled training data.
For the optimized model, if an object has an outlier thatdeviate from the general data, it is detected as a highanomaly score since the model cannot reproduce it well
(Figure 1).
As the first series of the project, this study focusedon evaluating the performance of our anomaly detection
in extracting which components of galaxy images asanomalies from bright galaxies at z = 0.05–0.2 identified
by the Sloan Digital Sky Survey. The results show

INOUE, Akio

(Waseda University)

Figure 1: Schematic illustration of deep anomaly detection [4].
When the optimized model read an image of a rare object like aquasar, its peculiar component (in the case of a quasar, a strong
UV radiation) can be detected.

Figure 2: Anomaly galaxy samples detected by the anomaly
detection. They show blue or purple components by strong UVradiation or star formation.

that the optimized model preferentially detect objects
with peculiar spectra as anomalies, especially extreme
emission line galaxies (XELGs) with strong emission
lines affecting broad-band photometry. This is mainly
due to the fact that XELGs have distinctive features
clear to the human eye (Figure 2) and are moderately
abundant in the universe. Particularly, the recovery ratesof XELGs in the g-band and quasars were 90 % and
70 %, which demonstrate that anomaly detection can beused to find rare objects with high probability without
prior information. In the future, we plan to apply a moreadvanced model to all the data and put it to practical use,

References[1] Mayor, M., Queloz, D.: 1995, Nature, 378, 355.
[2] Lorimer, D. R., et al.: 2007, Science, 318, 777.
[3] Tanaka, T. S., et al.: 2022, PASJ, 74, 1.
[4] “Artificial intelligence swimming in big data from the Subaru
Telescope”, Subaru Telescope, Nov. 23 2021,

https://subarutelescope.org/en/results/2021/11/23/3008.
html,（accessed 2022-05-10).

I Scientific Highlights

003

A Wide and Deep Exploration of Radio Galaxies with Subaru HSC(WERGS). IV. Rapidly Growing (Super)Massive Black Holesin Extremely Radio-loud Galaxies
ICHIKAWA, Kohei1, YAMASHITA, Takuji2, TOBA, Yoshiki3, NAGAO, Tohru4, INAYOSHI, Kohei5,
CHARISI, Maria6, HE, Wanqiu2, WAGNER, Alexander7,
AKIYAMA, Masayuki1, BOVONPRATCH, Vijarnwannaluk1, CHEN, Xiaoyang2, KAJISAWA, Ken4,
KAWAMURO, Taiki2, LEE, Chien-Hsiu8, MATSUOKA, Yoshiki4, SCHRAMM, Malte2, SUH, Hyewon2,
TANAKA, Masayuki2, UCHIYAMA, Hisakazu2, UEDA, Yoshihiro3, PFLUGRADT, Janek1, FUKUCHI, Hikaru1
1: Tohoku University, 2: NAOJ, 3: Kyoto University, 4: Ehime University, 5: Kavli Institute of Astronomy and Astrophysics, 6: California
Institute of Technology, 7: Tsukuba University, 8: National Optical-Infrared Astronomy Research Laboratory

Local radio galaxies have been primary targets forinvestigating the effect of supermassive black holes(SMBHs) on the host galaxies because powerful radiogalaxies or radio-loud active galactic nuclei (AGNs)
mainly reside in massive galaxies whose star formationis quenched, with the presence of strong jets dispersing
the interstellar medium.
However, the situation may be different at z > 1. Using
radio AGNs selected from the Very Large Array (VLA)COSMOS 3 GHz large project, researchers demonstrated
that SMBH accretion in radio-bright AGNs becomes
more radiatively efficient (λ Edd > 10 −2) at z > 1. They
reside in star-forming galaxies, which contain plentyof cold gas. This picture of radio AGNs is completely
different from those seen in the local universe in thesame radio luminosity range. Still, the survey volume of
VLA-COSMOS surveys is small so they may be missing
a rare, but radio-bright population. The FIRST survey isthe best tool for exploring such a radio-bright end since
it covers half the sky with the VLA at 1.4 GHz. However,cross matching the VLA/FIRST sources with the SDSS
survey catalog identified optical counterparts in only
30 % of the radio sources.
A recent Subar u / Hy per Supr i me - Cam ( HSC)
strategic survey shed light on such a situation. We haveconducted a search for optically faint radio galaxies (RGs)
using the Subaru HSC survey catalog and the VLA/FIRST radio continuum catalog, and we have found alarge number of RGs at z ~ 1 and covering > 60 % of the
FIRST radio sources. The project is called the Wide anddeep Exploration of Radio Galaxies with Subaru/HSC(WERGS; [1]).
In this study, we have investigated the propertiesof these unique optically faint RGs and found the two
key results. One is that their starformation rate is high,they are likely in the star-forming or starburst phasereaching a specific star formation rate of sSFR = SFR/
M⊙ ~ 10−8 yr−1, suggesting that some of our RGs might
be in a rapid stellar-mass assembly phase with massdoubling times of ~100 Myr. Besides, their stellar massis relatively small, including the low-mass galaxies with

004

I Scientific Highlights

M⊙ < 1010 M⊙.
The second result is that infrared detected RGs
are in a rapid BH accretion phase with high specificblack hole accretion rate (sBHAR) with the expected
Eddington ratio 〈log λEdd〉 ≈ −0.4 and some RGs may be
experiencing a super-Eddington phase, which is shownin Figure 1. Actually, our RGs tend to show high jet
power as well. This paints a different picture of radiogalaxies compared to conventionally known local radiogalaxies with low λEdd. The RGs in this study represent
a population of unique radio galaxies characterized byboth high λEdd and high radio power.

Figure 1: sBHAR properties for RGs in this study. The colors
and symbols are orange for radio-bright RGs (ERGs) and cyanfor other RGs (NRGs). (Left) The distribution of sBHAR. (Right)
The relation between sBHAR and M. The two straight lines are
the expected Eddington limits λEdd = 1 using Equation by [3] (graydashed line) and using the one by [4] (black dotted–dashed line).

References[1] Yamashita, T., Nagao, T., Akiyama, M., et al.: 2018, ApJ, 866,
140.
[2] Ichikawa, K., Yamashita, T., Toba, Y., et al.: 2021, ApJ, 921, 51.
[3] Kormendy, J., Ho, L. C.: 2013, ARA&A, 51, 511.
[4] Reines, A. E., Volonteri, M.: 2015, ApJ, 813, 82.

Development of a Galactic Model Optimized for the Galactic Bulge
KOSHIMOTO, Naoki1/2, BABA, Junichi3, BENNETT, David P.1/2
1: NASA Goddard Space Flight Center, 2: University of Maryland, 3: NAOJ

Gravitational microlensing toward the Galactic bulge
is randomly caused by the motion of stars in our Galaxy.
Therefore, the distribution of microlensing parameters
can be predicted using the Galactic model, a model of thenumber density distribution, velocity distribution, andmass function of stars in our Galaxy. By comparing thisprediction with the distribution of planetary microlensing
events, we can also investigate the distribution of stars
hosting planets in our Galaxy [1]. The results from thismethod depend on the Galactic model used, so the model
must be chosen carefully. However, Galactic models
used in microlensing studies to date have been simplistic,
based on Han & Gould (1995) [2]. The Besançon Galaxy
Model [3], which is often used as a stellar population
synthesis model in our Galaxy, is also known to beinconsistent with observations toward the Galactic bulge,e.g., the bar angle is too low.
Therefore, we developed a new Galactic model whichis consistent with the latest observations [4]. The data
used for model fitting include data from Gaia on thevelocity distribution of stars in the disk [5], as well as
various data in the Galactic bulge region such as stellar
number density [6,7], radial velocity and proper motion[8,9], and the latest observations of 8000 microlensing
events by the OGLE-IV sur vey [7,10] (Fig ure 1).
Through the modeling, we have measured various
important parameters that characterize our Galaxy, suchas the scale length of the velocity dispersion distributionof the disk, the rotational angular velocity of the bar in
the bulge, and the initial mass function (IMF) in thebulge region. In particular, the universality of the IMF
has been controversial, and the Kroupa (2001)'s IMF[11] measured in solar neighborhood is conventionallyapplied to bulge regions as well. The IMF measured
in this study is significantly different from that ofKroupa (2001) and may suggest that the star formation
process in the bulge region is different from that in
the solar neighborhood. The stellar mass-to-light ratio
was estimated from the measured IMF to be 0.72 +0.05−0.02
M⊙ /L K⊙, which is about 70 % of 1.04 M⊙ /L K⊙ for the
IMF of Kroupa (2001). Since the bulge dynamical massis well-determined, this suggests that the stellar mass ofthe bulge is lighter than previously thought and that thedark matter is more massive.
References[1] Penny, M. T., Henderson, C. B., Clanton, C.: 2016, ApJ, 830,
150.
[2] Han, C., Gould, A.: 1995, ApJ, 447, 53.
[3] Robin, A. C., et al.: 2012, A&A, 538, A106.
[4] Koshimoto, N., Baba, J., Bennett, D. P.: 2021, ApJ, 917, 78.
[5] Gaia Collaboration, Katz, D., et al.: 2018, A&A, 616, A11.
[6] Nataf, D. M., et al.: 2013, ApJ, 769, 88.
[7] Mroz, P., et al.: 2019, ApJS, 244, 29.
[8] Kunder, A., et al.: 2012, AJ, 143, 57.
[9] Clarke, J. P., et al.: 2019, MNRAS, 489, 3519.
[10] Mroz, P., et al.: 2017, Nature, 548, 183.
[11] Kroupa, P.: 2001, MNRAS, 322, 231.

Figure 1: Each data-set used for the model
fitting, compared with the model values (froma slide used in a conference talk).

I Scientific Highlights005

Orphan Cloud Bigger than Milky Way Discovered in the Leo Cluster
GE, Chong1, LUO, Rongxin1, SUN, Ming1, YAGI, Masafumi2, JÁCHYM, Pavel3, BOSELLI, Alessandro4,
FOSSATI, Matteo5, NULSEN, Paul E. J.6, SARAZIN, Craig7, EDGE, Tim1, GAVAZZI, Giuseppe5,
GASPARI, Massimo8/9, KODA, Jin10, KOMIYAMA, Yutaka2, YOSHIDA, Michitoshi2
1: University of Alabama in Huntsville, 2: NAOJ, 3: Academy of Sciences of the Czech Republic, 4: Aix Marseille Université, 5: Universitàdegli Studi di Milano Bicocca, 6: CfA Harvard & Smithsonian, 7: University of Virginia, 8: INAF, 9: Princeton University, 10: Stony Brook
University

Galaxy clusters contain hundreds to thousandsof galaxies. The space between cluster galaxies is
not empty, but instead filled with hot gas known as
intracluster medium (ICM). When galaxies are soaring
in the hot gas with a velocity around one thousand
kilometers per second, their cold gas between the stars
known as interstellar medium (ISM) is removed by theram pressure of hot gas. Once removed from the hostgalaxy, the stripped cold ISM mixes with the hot ICM,
produces multi-temperature tails [1]. In nearly all thecases of stripping, the parent galaxy is obvious, as thegas cloud is connected or points to the parent.
We recently discovered an isolated multi-temperaturecloud (Figure 1) without a parent galaxy in the Leo
Cluster (A1367). The cloud was initially noticed fromits warm gas component by the Subaru Telescope, andnamed as “orphan cloud (OC)” [2]. Our follow-up XMMNewton observation (Figure 2) to study other aspects of
A1367 unexpectedly discovered X-ray emission from the
hot gas of this cloud, revealing that the cloud is actuallybigger than the Milky Way [3]. The optical spectroscopy
from VLT/MUSE confirms that the cloud is in the
A1367. Its about solar metallicity suggests that the OC is
stripped from an evolved giant galaxy, but no such giant
galaxy is found around the cloud [3]. Compared the OC
with the stripped tails [1] still attached to their parent
galaxies, we found OC has higher X-ray temperature andluminosity, which indicates an advanced evolutionary
stage of the OC as it has mixed with the surrounding
ICM with a longer time.
This is the first discovery of such an intracluster
multi-temperature clump glowing both in optical (fromwarm gas) and X-ray (from hot gas). This study paves a
new way for research on intracluster clumps, as future
warm gas optical surveys can be used to search for otherorphan clouds and probe ICM clumping.

References[1] Sun, M., et al.: 2022, Nature Astronomy, 6, 270.
[2] Yagi, M., et al.: 2017, ApJ, 839, 65.
[3] Ge, C., et al.: 2021, MNRAS, 505, 4702.

Figure 1: The orphan cloud blue umbrella-shaped emission isfrom hot gas observed by XMM-Newton, the warm gas in red andthe stellar component in white are from Subaru Telescope.

400 kpc
15 arcmin
Figure 2: The Leo Cluster in X-ray from XMM-Newton. The
white square shows the location of Figure 1.

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Age Distribution of Stars in Boxy/Peanut/X-shaped Bulges
Formed without Bar Buckling
BABA, Junichi1, KAWATA, Daisuke2/3, SCHÖNRICH, Ralph2/3
1: NAOJ, 2: Mullard Space Science Laboratory, 3: University College London

Revealing the formation history and structure of
the bar in the Milky Way is a long-standing challenge
in Galactic astronomy. Recent surveys towards the
Galactic bulge, such as BRAVA and VVV, shows a clear
inner boxy/peanut-shaped bulge connected to the longthinner Galactic bar and the current pattern speed of the
Galactic bar is about 35–40 km s−1 kpc−1 [1]. However,the formation epoch of the Galactic bar is completely
unknown.
In this study [2], we study the observable consequence
bar formation using an N-body/SPH simulation of an
isolated Milky Way-like galaxy. As shown in the upper
panel of Figure 1, we found that a boxy/peanut/X (BPX)shaped bulge built up quickly after bar formation via
vILR heating without buckling [3]. Furthermore, we
found that the BPX-shaped bulge is dominated by stars
born prior to bar formation (middle panel of Figure 1).
By contrast, the NSD forms after the bar formation [4].
From this simulation, we expect that the age distributionsof the NSD and BPX-shaped bulge formed without bar
buckling do not overlap each other. Then, the transition
age between these components betrays the formation
time of the bar. To separate the NSD population
kinematically from the other stellar populations, theaccurate measurements of the transverse velocities ofstars are necessary. The near-infrared space astrometry
mission, JASMINE, would play a crucial role to identify
the formation epoch of the Galactic bar.
Figure 1: Upper: Morphological evolution of the simulated
galactic disk. From [2]. Middle: Expected age distributions ofstars in NSD (black square in the bottom panel) and BPX (orange
squares in the bottom panel). Bottom: Gaia images of the Galactic
bulge region (ESA/Gaia/DPAC).

References[1] Kawata, D., et al.: 2021, MNRAS, 508, 728-736.
[2] Baba, J., Kawata, D., Schönrich, R.: 2022, MNRAS, 513, 28502861.
[3] Raha, N., et al.: 1991, Nature, 354, 411-412.
[4] Baba, J., Kawata, D.: 2020, MNRAS, 492, 4500.

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Planetesimal Dynamics in the Presence of a Giant Planet
GUO, Kangrou, KOKUBO, Eiichiro(NAOJ/The University of Tokyo)

another giant planet core?

Figure 1: A schematic illustration of our model: formation of aplanetary core outside a giant planet perturber.

In our study investigating the impact of a Jupiterlike planet on planetesimal accretion (see Fig. 1 for theschematic illustration of our model), we found that the
coupling effect of secular perturbation and nebula gas
drag can align the orbits of planetesimals in the nonresonance regions of the disk, and thus lead to low
relative velocities of planetesimal swarms there [1]. In
this way, the eccentricity of planetesimals induced by theplanet contribute little to the relative velocities, and thegrowth of another planetary core can be unaffected undercertain conditions (Fig. 2).
These results have some interesting implications on
the formation scenario of Saturn. Since Saturn’s current
semi-major axis is near 9.6 au, with some tolerance
for migration, we can speculate that the growth of
Saturn’s core was enabled by the coupled effect of
secular perturbation from Jupiter and nebula gas dragon the relative velocities of planetesimals in the outerdynamically cooler disk location. Afterwards, during its
run-away gas accretion phase, the growing Saturn could
have migrated inward to its current location due to diskplanet interaction. Our results show that the issue of theformation of Saturn’s core, a long-standing mystery, may
be mitigated.
We also explored the dependence of such an effectof orbital alignment on the planet mass and eccentricity.
We found that, generally speaking, higher planet massand eccentricity both lead to higher relative velocity of008

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comparison of growth timescale at ~12au

1012

time [yr]The accretion of planetesimals during the planetforming stage in a protoplanetary disk can be strongly
affected by the secular perturbation from a massive
body in the system. During this phase of planetesimalaccretion, the nebula gas is still in presence in the
disk. Should there be a massive body (such as a stellar
companion or a planet) perturbing the disk, the coupledeffect of secular perturbation (especially when theperturber is eccentric) and nebula gas drag can lower
the relative velocity of planetesimal by aligning the
pericenters of their orbits under certain conditions.

10

11

10

10

10

9

10

8

107
1013

growth timescale (non-aligned)
growth timescale (aligned case)

1014

1015

1016

m [g]

1017

1018

1019

1020

Figure 2: Distribution of longitudes of pericenter. Alignment seen
at non-resonance locations, e.g., near 12 and 14 au.

planetesimals, which makes accretion more challenging.
According to our results, when a system harbors aplanet sufficiently large or eccentric, it is less likely to
produce other planetary companions due to high relative
velocities of planetesimals.
In the big picture, our studies contribute to improve
the standard models of planet formation in the coreaccretion paradigm. The standard models describe well
how planets form in axisymmetric, smoothly distributed
disks. However, in reality, the disks are often perturbed
by bodies such as large planets or stellar companions.
In such configuration, the formation of planetary bodies
can deviate from the standard scenario. Our results
serve as candidate theories for explaining the diverse
architecutres of planetary systems observed in recent
decades.

Reference[1] Guo, K., and Kokubo, E.: 2021, AJ, 162, 115.

A Dusty Protocluster Discovered by Planck and Subaru Telescopelog(M /M )

10.5

11.0

2.32

10.0

2.34

9.5

Over the last years, there has been a big progressin the search for “protoclusters” at high redshifts. In
particular, the deep and wide-field imaging survey
performed with Subaru Hyper Suprime-Cam (HSC)
successfully discovered a number of protoclusters out toz ~ 6. However, most of the protoclusters known to datewere identified by optical surveys, which correspond to
the rest-frame UV search for high-redshift galaxies, andtherefore it is possible that galaxies heavily obscured by
dust are missing in the existing surveys. An interesting
approach to identify dusty protoclusters is to use the allsky submillimeter map provided by the Planck satellite.
With the limited sensitivity and angular resolution,
it is not possible to detect individual high-z galaxies
with Planck. However, theories suggest that Planck
can detect protoclusters as “point sources” if dusty
galaxies are strongly clustered in a compact region on
the sky. Indeed, by investigating the FIR–submm color
informations, recent studies suggest that there exist >2,000 high-z galaxies/clusters candidates in the Planck
compact sources [1], but multi-wavelength follow-up
observations are required to confirm their redshifts andcluster membership.
In this work, we focus on one of the Planck high-z
candidate sources, PHzG237.01+42.50 (PHzG237).
This source is the only Planck high-z candidate source
situated in the COSMOS field, and the distributions ofspectroscopic sources in the COSMOS field suggests
there is an overdensity of galaxies at z = 2.16 aroundthis Planck source. We performed narrow-band Hαimaging observations of the PHzG237 with NB2071
filter on Subaru/MOIRCS, and successfully identified
38 Hα emitters at z = 2.16 [2] (see Fig. 1). In addition,
our follow-up NIR spectroscopy with Large Binocular
Telescope (LBT) also conf ir ms an overdensity ofspectroscopic members at z = 2.15–2.20 [3].
Our data also suggest that Hα emitters residing inhigher-density environments (protocluster core region)
traced by the Hα emitters tend to have higher stellar
mass [2] (see Fig. 1). Furthermore, with the X-ray andoptical/NIR spectroscopic data available in this field,
we find that ~20 % of the galaxies in the protocluster
core region have AGN activities [3]. This result suggests
a strong link between the galaxy evolution processes
in dense environments in the early universe and AGN
activity.
The total SFR of this protocluster derived byintegrating the Hα star formation rate (SFR) of theHα emitters is ≈1,000 M ⊙ /yr, while the FIR-derived
SFR from Planck/Herschel photometry is ≈4,000–

Dec. [deg]1: NAOJ, 2: Tohoku University

KOYAMA, Yusei1, TANAKA, Ichi1, KODAMA, Tadayuki2

S

S
S

S
P

2.30

S
S

2.28

S

2.26
S

2.24

500 [ph-kpc] = 1 arcmin

150.52150.50150.48R.A. [deg]150.46

Figure 1: The 2-D distribution of galaxies around the PHzG237
protocluster at z = 2.16 discovered by this study. The coloredsquare symbols show the Hα emitters identified with our Subaru/
MOIRCS observations, with the redder symbols indicating higher
M. The green circles and orange circles show MIR-detected Hαemitters and Herschel FIR sources, respectively. The original
Planck source position is shown with the “P” mark. The “S” and“X” marks in the plot show the spectroscopic members and X-ray
sources, respectively. The yellow contours are drawn based on thenumber density of all the cluster members.

10,000 M ⊙ /yr. The reason of this large (a factor of~5–10×) discrepancy between the two SFRs is unclear,but it is possible that we may underestimate the Hα dust
attenuation levels, and perhaps there exist many Hαundetected sources heavily obscured by dust. However,further studies are needed because FIR–submm fluxes
measured with the poor spatial resolution of Planck/
Herschel may be overestimated due to the contaminationfrom sources which are not physically connected to theprotocluster.

References[1] Planck Collaboration: 2016, A&A, 596, 100.
[2] Koyama, Y., et al.: 2021, MNRAS, 503, 1.
[3] Polletta, M., et al.: 2021, A&A, 654, 121.

I Scientific Highlights009

Polarization of the Corona
Observed During the 2017 and 2019 Total Solar Eclipses
HANAOKA, Yoichiro1/2, SAKAI, Yoshiaki3/2, TAKAHASHI, Koichi4
1: NAOJ, 2: SEPnet, 3: Chiba Prefectural Ichihara High School, 4: NPO Kwasan Astro Network

010

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2017 Aug 21

4

10000

2

10-10 Bsun

Y (Rsun)

1000

0

100

-2

-4

-4

-2

0
X (Rsun)2

10

4Figure 1: Polarization map of the K+F corona after the eliminationof the sky background covering 8.2 × 8.2 R⊙ area obtained during
the 2017 eclipse. The grayscale image presents Stokes I signals,
and the degree and orientation of the linear polarization signals
are depicted with orange ticks. The solar north is to the top.
2017 August 21 B K+F

105

2017 August 21 p K+F

this study
LASCO C2
104

Streamer/Equator

103

0.10

Streamer/Equator
10

2

pK+F

BK+F (10-10 Bsun)

The white-light solar corona consists of theK-corona from the million-degree plasma of the Sun
and the F-corona from interplanetary dust. Linearpolarization information enables the separation of theK- and F-corona. Therefore, polarimetry has long been
performed in total eclipse observations as well as incoronagraph observations. Total solar eclipses provide
us very low sky-background down to just above thesolar limb, which cannot be achieved in coronagraphobservations. Therefore, the white-light corona has beena particularly important target for the total solar eclipse
observations.
We carried out polarimetric observations of the whitelight corona during the total solar eclipses on 2017 August
21 and 2019 July 2 by taking advantage of professionalamateur collaborations, and successfully obtained data at
two different sites for both eclipses [1]. After eliminating
the sky background, we obtained the brightness (BK+F)
and polarization (pK+F) of the K+F corona, as presented
in Figure 1.
In Figure 2, comparison of the derived brightness andpolarization with other measument results is presented.
For the B K+F , the results of the Large Angle
Spectrometric Coronagraph (LASCO) C2 of the Solarand Heliospheric Observatory [2] show good coincidencewith ours, but for the p K+F , the LASCO results are
systematically smaller than our results and those by
Vorobiev et al. [3], which were also taken at the eclipse.
The discrepancy among the results for pK+F, which
actually corresponds to the brightness of the K-coronaalone, leads the error in the estimated amount of the
hot plasma. The correct amount of the hot plasma of
the corona is important to study the coronal plasmaproducing mechanism and to the study on the coronalvariation according to the solar activity cycle. Wellcalibrated eclipse data, which were taken with a wide
field-of-view, enable intercomparison among various
data and contribute to the correction of the systematic
error in the results from other observations. The eclipse
observations provide a standard to study the amount of
the hot corona quantitatively.

Pole

Pole
this study

101

Vorobiev et al.
LASCO C2

100
1

2

3
Elongation (Rsun)

4

5

0.01
1

2

3
Elongation (Rsun)

4

5

Figure 2: Comparison of the brightness of the K+F corona (BK+F;
left) and the degree of polarization (pK+F; right) among the eclipse
observation, LASCO C2 observation, and the results by Vorobiev
et al. (only pK+F).

References[1] Hanaoka, Y., Sakai, Y., Takahashi, K.: 2021, Solar Phys. 226,
1421.
[2] MEDOC data archive, https://idoc-medoc.ias.u-psud.fr/sitools/
client-user/index.html?project=Medoc-Solar-Portal (accessed2022-5-24).
[3] Vorobiev, D., et al.: 2020, Pub. Astron. Soc. Pac., 132, 024202.

Luminosity Functions and Clustering Revealed with ~4,000,000 Galaxies
at z ~ 2–7 from the Subaru/Hyper-Suprime Cam Survey
HARIKANE, Yuichi1/2, ONO, Yoshiaki1, OUCHI, Masami3/4/1, LIU, Chengze5, SAWICKI, Marcin6,
SHIBUYA, Takatoshi7, BEHROOZI, Peter S.8, HE, Wanqiu3, SHIMASAKU, Kazuhiro1, ARNOUTS, Stephane9,
COUPON, Jean10, FUJIMOTO, Seiji11, GWYN, Stephen12, HUANG, Jiasheng13/14, INOUE, Akio K.15,
KASHIKAWA, Nobunari1, KOMIYAMA, Yutaka3/4 MATSUOKA, Yoshiki16, WILLOTT, Chris J.12
1: The University of Tokyo, 2: University College London, 3: NAOJ, 4: SOKENDAI, 5: Shanghai Jiao Tong University, 6: Saint Mary’s
University, 7: Kitami Institute of Technology, 8: University of Arizona, 9: Laboratoire d’Astrophysique de Marseille, 10: University of Geneva,
11: University of Copenhagen, 12: NRC Herzberg, 13: National Astronomical Observatories of China, 14: Harvard-Smithsonian Centre for
Astrophysics, 15: Waseda University, 16: Ehime University

In this study [1], we present measurements of rest-UV
luminosity functions and angular correlation functions
from 4,100,221 galaxies at z ~ 2–7 identified in the
Subaru/Hyper Suprime-Cam survey and CFHT LargeArea U-band Survey. The obtained luminosity functions
at z ~ 4–7 cover a very wide UV luminosity range of~0.002–2000 L *UV combined with previous studies (Figure1), confirming that the dropout luminosity function is asuperposition of the AGN luminosity function dominant
at M UV < −24 mag and the galaxy luminosity function
dominant at M UV > −22 mag, consistent with galaxy
fractions based on 1037 spectroscopically-identified
sources. Galaxy luminosity functions estimated fromthe spectroscopic galaxy fractions show the bright end
excess beyond the Schechter function at > 2σ levels.
By analyzing the correlation functions at z ~ 2–6 withhalo occupation distribution models, we find a weak
redshift evolution (within 0.3 dex) of the ratio of thestar formation rate (SFR) to the dark matter accretionrate, SFR/M۬ h (Figure 2), indicating the almost constantstar formation efficiency at z ~ 2–6, as suggested by ourearlier work at z ~ 4–7 [2]. Meanwhile, the ratio gradually
increases with decreasing redshift at z < 5 within 0.3 dex,
which quantitatively reproduces the cosmic SFR density
evolution, suggesting that the redshift evolution is
primarily driven by the increase of the halo number
density due to the structure formation, and the decreaseof the accretion rate due to the cosmic expansion.

Galaxy+AGN

GalaxyAGN

Figure 1: The bottom panel shows rest-frame UV luminosity
functions of dropout sources (including galaxies and AGNs) atz ~ 4. The red circles show our results based on the HSC-SSP
survey data, and other symbols are previous results. The top
panel shows a fraction of galaxies in our dropout sample based on
spectroscopic results.

Figure 2: SFR/ M۬ h and baryon conversion efficiency (SFR/(fb M۬ h))
as a function of the halo mass (filled diamonds: this work, circles:[3]). The black solid curve is the fitting formulae, and the grayshaded region represents the 2σ typical scatter of the data points
compared to the relation.

References[1] Harikane, Y., et al.: 2022, ApJS, 259, 20.
[2] Harikane, Y., et al.: 2018, PASJ, 70, S11.
[3] Harikane, Y., et al.: 2016, ApJ, 821, 123.

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Interrelation of the Environment of
Lyα Emitters and Massive Galaxies at 2 < z < 4.5
ITO, Kei*1, KASHIKAWA, Nobunari1, TANAKA, Masayuki2, KUBO, Mariko3, UCHIYAMA, Hisakazu3,
TOSHIKAWA, Jun4, LIANG, Yongming5/2, ISHIMOTO, Rikako1, YOSHIOKA, Takehiro1, TAKEDA, Yoshihiro1
1: University of Tokyo, 2: NAOJ, 3: Ehime University, 4: University of Bath, 5: SOKENDAI

11.0

1.75

10.9

1.25

10.8

log(M,lim/ M )2
ξSFG−LAE/ξ SFG ξLAE

1.50

1.00

10.7

0.75

10.6

0.50
0.25

10.5

0.00
2.0

2.5

3.0

z

3.5

4.0

012

I Scientific Highlights

10.4

2.4 < z < 3.5
QG
SFG
LAE

1.50
1.25
1.00
0.75
0.50
0.25
0.00
− 1.0

− 0.5

0.0

SFG δ

0.5

1.0

Figure 2: Overdensity distribution at the position of three
populations measured by the distribution of SFG. The verticallines show the median of each distribution.

References[1] Shimakawa, R., et al.: 2017, MNRAS, 468, L21.
[2] Ito, K., et al.: 2021, ApJ, 916, 35.
[3] Sobral, D., et al.: 2018, MNRAS, 476, 4725.
[4] Laigle, C., et al.: 2016, ApJS, 224, 24.

* In SOKENDAI/NAOJ when paper was published.

4.5

Figure 1: Ratio between cross- and autocorrelation function.
Colors represent the lower limit of stellar mass of SFGs.

PDF

Recently, the large-scale structure in the distantuniverse has been explored through the distribution ofvarious galaxy populations. On the other hand, it is notnecessarily trivial that different populations trace thesame structure. Indeed, some protoclusters have different
distributions between Lyα emitters and other galaxies [1].
We have not known whether the same trend is seen evenin general.
This work [2] evaluates the distribution differencesof Lyα emitters (LAEs), massive star-forming galaxies(SFGs), and massive quiescent galaxies (QGs) at
2 < z < 4.5 located in the COSMOS field. LAEs samples
are taken from [3], and SFGs and QGs are selected fromthe multi-band data [4].
Firstly, we compare the cross-correlation signal
with the autocorrelation signal between two galaxy
populations. The cross-correlation between SFGs and
QGs is as expected from their autocorrelation. However,that between SFGs and LAEs is significantly smaller
than expected from their autocorrelation, suggesting thatthese two populations locate more differently than the
difference in halo masses (Figure 1).
In addition, the overdensity distributions at theposition of each galaxy population are derived. Thoseof SFGs and QGs do not have a significant difference.
However, those of SFGs and LAEs differ, and LAEs
are found to be located in lower-dense environments(Figure 2).
These results suggest that LAEs are typically locatedin different environments than SFGs and QGs. Thisdifference can be due to the formation time differenceof their host halos or the absorption of Lyα emission by
Intergalactic Medium. This work implies that surveys for
multiple galaxy populations are necessary to understandthe actual large-scale structure at high redshift.

On the Hubble Constant Tension
DAINOTTI, Maria Giovanna1/2/3, DE SIMONE, Biagio4, SCHIAVONE, Tiziano5/6,
MONTANI, Giovanni7/8, RINALDI, Enrico9/10, LAMBIASE, Gaetano11
1: NAOJ, 2: SOKENDAI, 3: Space Science Institute, 4: University of Salerno, 5: University of Pisa, 6: INFN, 7: ENEA, 8: Sapienza University, 9:
University of Michigan, 10: RIKENThe Hubble constant tension problem is thediscrepancy in more than 4σ between the value of the
Hubble constant (H0) measured with local probes suchas Supernovae Ia (SNe Ia) and its value inferred by
the Cosmic Microwave Background data. This open
issue represents a challenge for both astrophysics andcosmology.
We have shown how H0 undergoes an evolution ofits value with the redshift through a statistical analysis
applied to the so-called Pantheon sample which contains
1048 spectroscopically confirmed SNe Ia with a redshift
range 0 ≤ z ≤ 2.26. As a first step, we divided thePantheon sample into 3, 4, 20, and 40 equally populatedbins of SNe Ia ordered in redshift and we estimated H0for each bin through the Monte Carlo Markov Chain
approach. As a second step, we fitted such values of H0
for all the bins with the model H0(z) = H̃0/(1+z)α, where z
is the redshift, H̃0 is the local value of the Hubble constant(H0 at z = 0) and α is the evolutionary parameter.
The results of this analysis in 4 bins show that the
α = 0.008 ± 0.006 and is compatible with zero in 1.5σ
(namely, ασα = 1.5 in the cases of ΛCDM and w0waCDM
model, where w(z) = w0 + wa*z/(1+z) (the so-called CPL
parametrization).
We have repeated the same analysis in 3, 20, and 40
bins, and the values of the α parameters are all compatible
with the 4 bins case in 1σ. This shows that our results arereliable and independent of the particular choice of thebins division.
If the H 0 evolution is not due to the statisticalfluctuations of the division in redshift bins and otherhidden selection biases of SNe Ia parameters, we show
how H0(z) could affect the definition of the luminosity
distance itself. The evolved H0(z) when substituted in the
distance luminosity formula induces an overestimation by≈ 2 % at z = 11.09 in the ΛCDM model.
We extended this analysis [2] by deriving the valuesof H 0, but this time we left free to vary H 0 together
with the total matter density parameter (Ω 0m) in theΛCDM model and together with the coefficient wa in the
w0waCDM model. Further, we added the Baryon Acoustic
Oscillations (BAOs) to the aforementioned 3 bins of SNe
Ia. We confirmed the decreasing trend of H0(z) with α =0.008 ± 0.006 (ασα = 1.2) in the ΛCDM model and α =0.033 ± 0.005 (ασα = 5.8) for the w0waCDM model.
To understand if this trend can be due to modified
gravity theories, we tested one of the most studied dark

Figure 1: H0 vs. z in 4 bins of SNe Ia [1] for the ΛCDM (upper
panel) and the w0waCDM (lower panel) models.

energy models in the f(R) framework, the Hu-Sawicki
model, in 3 bins. However, this model is not able toexplain the H0 tension. Nevertheless, we inferred thescalar field potential in the Jordan frame that could still
reproduce the decreasing trend of H0.
If we exclude the modified gravity scenario, anotherplausible interpretation of this tension is that the observed
evolution is due to selection biases induced by the stretchof the SNe Ia, a problem that has been recently pointed
out by [3].

References[1] Dainotti, M. G., et al.: 2021, ApJ, 912, 150.
[2] Dainotti, M. G., et al.: 2022, Galaxies, 10, 24.
[3] Nicolas, N., et al.: 2021, A&A, 649, A74.

I Scientific Highlights

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Hyper Suprime-Cam Legacy Archive
TANAKA, Masayuki1, MURATA, Kazumi1, MINEO, Sogo1, KOIKE, Michitaro1, OKURA, Yuki1,
HARASAWA, Sumiko1, IKEDA, Hiroyuki2, TAKITA, Satoshi3
1: NAOJ, 2: Wakayama KOSEN, 3: University of Tokyo

About one-third of observing time of Hyper SuprimeCam (HSC) installed at the prime focus of the Subaru
Telescope has been used for the Subaru Strategic
Program (SSP) [1]. Data from HSC-SSP are processedwith a dedicated reduction pipeline and the processeddata are routinely released to the world-wide community[2,3,4]. The reminder of the observing time is used for
PI programs. Processed data from PI programs are notalways released to the public, but the scientific value ofthe data is high. The Subaru Telescope has launched HSC
Legacy Archive (HSCLA), where pipeline-processed,science-ready data from PI programs are available.
The first release of HSCLA occurred in January
2021 (Figure 1) [5]. The release includes data taken in
the first year of science operation of HSC, 2014, andcovers about 580 square degrees of the sky (Figure 2).
Five broad-band filters (grizy) and two narrow-band
filters (NB515 and NB656) are used in this release, andthe data reach down to 24–27th magnitudes (5σ for point
sources). We have performed extensive quality assurance(QA) tests and all the QA plots are made available atthe data release site. Overall, the quality of the data ishigh; we reach 2–3 % photometric accuracy and 0.01
arcsec astrometric accuracy. While the data are ready for
scientific explorations, there are known issues, which aresummarized at the data release site.
The total data volume of HSCLA is very large. In
order to efficiently exploit the data, we offer online/offline
data access tools to the user. They are the same tools
as used for HSC-SSP. The image data can be accessed
through online tools and the catalog data can be retrieved
from a custom-designed database with user-friendly
interface.
We plan to process and release more data in the
future to increase the scientific value of HSCLA. We
hope HSCLA will become a useful resource for scientificresearch and it contributes to solve the mysteries of the
Universe.

014

I Scientific Highlights

Figure 1: HSCLA website (https://hscla.mtk.nao.ac.jp/). The site
offers not just HSC data, but all quality assurance plots as well as
links to data access tools.

Figure 2: Sky area covered by HSCLA2014 is indicated in blue.
The red contours in the background show the Galactic extinction.

References[1] Aihara, H., et al.: 2018a, PASJ, 70, S4.
[2] Aihara, H., et al.: 2018b, PASJ, 70, S8.
[3] Aihara, H., et al.: 2019, PASJ, 71, 114.
[4] Aihara, H., et al.: 2022, PASJ, 74, 247.
[5] Tanaka, M., et al.: 2021, PASJ, 73, 735.

EMPRESS. IV. Extremely Metal-poor Galaxies Including Very
Low-massPrimordial Systems: High Fe/O Suggestive of Metal
Enrichment by Hypernovae/Pair-instability Supernovae
ISOBE, Yuki1/2, OUCHI, Masami1/3/4, SUZUKI, Akihiro3, MORIYA, Takashi J.3/5, NAKAJIMA, Kimihiko3,
NOMOTO, Ken’ichi4, RAUCH, Michael6, HARIKANE, Yuichi1/7, KOJIMA, Takashi1/2, ONO, Yoshiaki1,
FUJIMOTO, Seiji1/3/8/9/10, INOUE, Akio K.10, KIM, Ji Hoon11, KOMIYAMA, Yutaka12, KUSAKABE, Haruka13,
LEE, Chien-Hsiu14, MASEDA, Michael V.15, MATTHEE, Jorryt16, MICHEL-DANSAC, Leo17, NAGAO, Tohru18,
NANAYAKKARA, Themiya19, NISHIGAKI, Moka20, ONODERA, Masato1/20, SUGAHARA, Yuma3/10, XU, Yi1/2
1: Institute for Cosmic Ray Research, University of Tokyo, 2: Faculty of Science, University of Tokyo, 3: NAOJ, 4: Kavli Institute for the Physics andMathematics of the Universe, 5: Monash University, 6: Carnegie Observatories, 7: University College London, 8: Cosmic DAWN Center, 9: Niels Bohr
Institute, 10: Waseda University, 11: Seoul National University, 12: Hosei University, 13: Université de Genéve, 14: National Optical-Infrared Astronomy
Research Laboratory, 15: University of Wisconsin-Madison, 16: ETH Zürich, 17: Centre de Recherche Astrophysique de Lyon, 18: Ehime University, 19:
Swinburne University, 20: SOKENDAIAge (Myr)
1000 100 50 20 10 2

–1.5
–2.0
10

J0811
(Fe/O)⊙J1631

No HN/PISN

10

300 10
300
30
100
100
30

1000
1000

(N/O)⊙–1.0

log(Fe/O)

Primordial galaxies characterized by low gasphase metallicities and low stellar masses (Z <~ 0.01
6
and M* <~ 10 M⊙; e.g., [1]) are important to understandgalaxy formation, while it is hard to observe primordial
galaxies at high redshifts due to their faintness (e.g.,[2]). Complementarily, various studies have actively
investigated local extremely metal-poor galaxies(EMPGs). Although characteristics and formation
processes of EMPGs would not be completely the sameas those of high-z galaxies [3], EMPGs are expected to begood local analogs of high-z primordial galaxies because
EMPGs have low metallicities, low stellar masses, andhigh specific star-formation rates. [4] have launched a
project “Extremely Metal-Poor Representatives Exploredby the Subaru Survey (EMPRESS)”, selecting faint
EMPG candidates from Subaru/Hyper Suprime-Cam(HSC) deep optical images (~26 AB mag). Remarkably,
EMPRESS has pinpointed J1631+4426 having the lowest
metallicity identified so far (0.016 Z⊙) with a low stellar
mass (~106 M⊙) [4].
We have conducted Keck/LRIS deep optical
spectroscopy of 13 EMPG photometric candidates
selected from the HSC deep images [4]. We find that nineout of the 13 candidates are EMPGs with metallicities
less than ~0.1 Z⊙ (Figure 1 top), and four sources arecontaminants of moderately metal-rich galaxies or noemission-line objects. Notably, two out of the nine
EMPGs have extremely-low stellar masses (5 × 104 – 7 ×
105 M⊙) and metallicities (0.02–0.03 Z⊙). With a sampleof five EMPGs with Fe/O measurements, two (three) of
which are taken from this study (the literature; [5,6]), we
confirm that two EMPGs (J1631+4426 and J0811+4730)
with the lowest metallicities (~0.02 Z⊙) show high Fe/
O ratios (~0.1) comparable to the solar abundance ratio.
Comparing galaxy chemical enrichment models, we findthat the two EMPGs cannot be explained by a scenario of
metal-poor gas accretion/episodic star-formation history
due to their low N/O ratios (Figure 1 bottom right).
We conclude that the two EMPGs can be reproduced
by an inclusion of bright hypernovae (BrHNe) and/or
hypothetical pair-instability supernovae (PISNe; Figure30
100 300 –2.0 –1.5 –1.0 –0.5
EW0(Hβ) (Å)
log(N/O)

Figure 1: (Top) HSC gri images of 9 EMPGs identified by [2].
(Bottom left) Fe/O ratio as a function of Hβ equivalent widthand galaxy age. The points (curves) represent EMPGs (galaxy
chemical enrichment model). (Bottom right) Fe/O ratio as afunction of N/O.

1 bottom left) preferentially produced in a metal-poor
environment. This conclusion implies that primordial
galaxies at z ~ 10 could have a high abundance of Fe
that is not originated from Type Ia SNe with delays, andthat Fe may not serve as a cosmic clock for primordial
galaxies. This finding sheds light onto the early processof galaxy formation, providing a sneak peek of high-z
primordial galaxy surveys in the forthcoming era ofJames Webb Space Telescope. This paper is publishedfrom ApJ [2].
References[1] Wise, J. H., et al.: 2012, ApJ, 745, 50.
[2] Isobe, Y., et al.: 2022, ApJ, 925, 111.
[3] Isobe, Y., et al.: 2021, ApJ, 918, 54.
[4] Kojima, T., et al.: 2020, ApJ, 898, 142.
[5] Kojima, T., et al.: 2021, ApJ, 913, 22.
[6] Izotov, Y. I., et al.: 2018, MNRAS, 478, 4851.

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A Wide and Deep Exploration of Radio Galaxies with Subaru HSC(WERGS). VI. Distant Filamentary Structures
Pointed by High-z Radio Galaxies at z ~ 4
UCHIYAMA, Hisakazu1, YAMASHITA, Takuji2/1, TOSHIKAWA, Jun3, KASHIKAWA, Nobunari4,
ICHIKAWA, Kohei5, KUBO, Mariko1, ITO, Kei4, KAWAKATU, Nozomu6, NAGAO, Tohru1,
TOBA, Yoshiki2/7/8/1, ONO, Yoshiaki4, HARIKANE, Yuichi4/9, IMANISHI, Masatoshi2/10,
KAJISAWA, Masaru1, LEE, Chien-Hsiu11, LIANG, Yongming10
1: Ehime University, 2: NAOJ, 3: Bath University, 4: Tokyo University, 5: Tohoku University, 6: Kure College, 7: Kyoto University, 8: ASIAA,
9: University College London, 10: SOKENDAI, 11: NSF’s NOIRLab

4.5

3.5
overdensity significance(σ)

3.0
2.5
2.0
1.5
1.0
0.5
0.0
− 0.5
− 1.0
25.8

101

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26.0

26.2 26.4 26.6 26.8
log L1.4GHz (W Hz 1)

27.0

27.2

faintHzRGs
brightHzRGs
Bornancini+06

100

0.0

References[1] Uchiyama, H., et al.: 2022, ApJ, 926, 76.
[2] Overzier, R. A., et al.: 2006, ApJ, 637, 58.
[3] Venemans, B. P., et al.: 2007, A&A, 461, 823.
[4] Kikuta, S., et al.: 2017, ApJ, 841, 128.

g-dropouts
HzRGs

4.0

isotropyf

In this study [1], we have revealed that high-z radiogalaxies (HzRGs) at z ~ 4 tend to reside in the filamentlike overdense regions based on Hyper Suprime-Cam
Subaru Strategic Program (HSC-SSP) and Faint Imagesof the Radio Sky at Twenty-cm (FIRST).
Radio galaxies eject a huge amount of energy aroundthemselves, which gives a non-negligible influence on thehost/surrounding galaxy evolution and formation. Thus,in order to understand galaxy formation and evolution, it
is key to understand where radio galaxies appear, that is,what the surrounding environments of radio galaxies are.
However, the HzRG environments at z > 4 are not yet
completely grasped due to the rarity of HzRGs and thelack of observations deep and wide enough to capture thesurrounding galaxies, although there are some previous
studies [2,3,4].
We characterize the HzRG environments statisticallyby embracing the largest samples of HzRGs andg-dropout galaxies at z ~ 4 constructed from radio andoptical large survey data of HSC-SSP and FIRST. We
find that the overdensities around the faint HzRGs
with L1.4 GHz ~ 1026.0–26.5 W Hz−1 tend to be higher thanthat of the g-dropout galaxies, while no significant
difference in density environments is found between theluminous HzRGs with L1.4 GHz ~ 1026.5–27.0 W Hz−1 andthe g-dropout galaxies (upper panel of Figure 1). These
results are consistent with a scenario where HzRGs
get older and more massive as the radio-luminosity
decreases. We also find that the surrounding galaxies tend
to distribute along the radio-jet major axis of the HzRGs
at angular distances less than <~ 500 physical kpc (lower
panel of Figure 1). Our findings imply the onset of thefilamentary structures around the HzRGs at z ~ 4.

0.2
0.4
0.6
0.8
1.0
projecteddistancefrom HzRGs (pMpc)

Figure 1: (upper panel) The overdensities around the HzRGs(black points) as a function of their rest-frame 1.4 GHz radio
luminosities. The dashed line and the gray shaded region indicate
the median and standard deviation of the overdensity significancesof the g-dropout galaxies. galaxies, respectively. (lower panel)
Isotropy as a function of the projected distance from the bright(black points) and faint (red points) HzRGs.

Discovery of a Directly Imaged Planetary-mass Companion
to a Young Taurus M Dwarf StarHIRANO, Teruyuki1/2, KUZUHARA, Masayuki1/2, HARAKAWA, Hiroki1, KOTANI, Takayuki1/2,
KUDO, Tomoyuki1, KUROKAWA, Takashi1/2, MISHIKAWA, Jun1/2, OMIYA, Masashi1/2, TAMURA, Motohide1/2,
UEDA, Akitoshi1/2, VIEVARD, Sebastien1, GAIDOS, Eric3, LEE, Rena3, SALAMA, Maissa3, BERGER, Travis3,
LIU, Michael3, HODAPP, Claus3, JACOBSON, Shane3, KRAUS, Adam4, ZHANG, Zhoujian4,
GRUNBLATT, Samuel5, ANSDELL, Megan6, KONISHI, Mihoko7, SERIZAWA, Takuma8
1: NAOJ, 2: Astrobiology Center, 3: University of Hawaii, 4: University of Texas, 5: American Museum of Natural History, 6: NASA, 7: Oita
University, 8: Tokyo University of Agriculture and Technology

a giant planet around a low-mass star at a large orbital
distance (~ 100 au) challenges the classical formation
theories such as the core-accretion model (which requirestime) and disk-instability model (which requires mass) [3].
Future observations for the atmospheric characterizationsof 2M0437b such as by JWST would shed some light on
the formation mechanism of such giant planets aroundlow-mass stars.








      

Young exoplanets are thought to be important targets
to test planet formation theories. Comparison between
the properties of young and old exoplanets also allows us
to observationally constrain the formation and evolutionof exoplanet atmospheres as well as trace the long-term
dynamical evolution of close-in exoplanets. However,young stars generally have higher surface activity andlarge rotational velocities, which in turn complicate
the detection of exoplanets around them using classicalmethods such as radial-velocity measurements. On
the other hand, young exoplanets are thought to retain
the initial heat acquired through the gas accretion attheir formation, and thus often luminous in the nearinfrared. Therefore, one can probe the presence of young
exoplanets by direct imaging with high spatial resolution
at near-infrared wavelengths [1].
We searched for planetary-mass companions
around 2M0437, which is a young M dwarf in the
Taurus star-forming region. Using IRCS and AO188
on the Subaru telescope, we performed high-resolution
H-band imaging for 2M0437. Our first AO imaging in2018 March revealed three “companion candidates” asshown in Figure 1 (named “b”, “SW”, and “E” in orderof increasing distance from 2M0437). To check for thecommon proper motions for those companion candidates,
we performed astrometric observations using Subaru/
IRCS as well as the NIRC2 camera on Keck II. After
three years of astrometric monitoring, we found that thecandidate “b” is physically bound to 2M0437 (i.e., has acommon proper motion), while the other sources (“SW”
and “E”) turned out to be heavily reddened backgroundstars [2].
Isochrone fitting for 2M0437 suggests that it is a 2–5
million-year-old M dwarf with the mass of 0.15–0.17 M⊙.
The companion “b”, located at ≈ 0.9 arcsecond (≈ 100
au in the projected distance) away from 2M0437, had aninferred mass of 3–5 MJup from its luminosity, by which
we concluded that it is a “planet” (rather than a browndwarf). Given that 2M0437b orbits a low-mass star andis one of the least massive, and youngest exoplanets
ever discovered by direct imaging, it is an importantbenchmark to test planet formation and evolution
scenarios around low-mass stars. The existence of such



























     







Figure 1: High-resolution image of 2M0437 capt ured by
IRCS+AO188 with a field-of-view of 16° × 16° [2].

References[1] Marois, C., et al.: 2008, Science, 322, 1348.
[2] Gaidos, E., et al.: 2022, MNRAS, 512, 583.
[3] D’Angelo, G., Lissauer, J. J.: 2018, in Deeg H. J., Belmonte J.
A., eds, Handbook of Exoplanets. Springer, Cham, p. 140.

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Ionizing Radiation from z > 3.3 AGNs
with the Hyper Suprime-Cam Survey
and the CFHT Large U-band Deep Survey
IWATA, Ikuru1/2, SAWICKI, Marcin2, INOUE, Akio K.3, AKIYAMA, Masayuki4, MICHEVA, Genoveva5,
KAWAGUCHI, Toshihiro6, KASHIKAWA, Nobunari7, GWYN, Stephen8, ARNOUTS, Stephane9,
COUPON, Jean10, DESPREZ, Guillaume10
1: NAOJ, 2: Saint Mary’s University, 3: Waseda University, 4: Tohoku University, 5: Leibniz-Institute for Astrophysics Potsdam, 6: Onomichi
City University, 7: University of Tokyo, 8: NRC-Herzberg, 9: Laboratoire d’Astrophysique de Marseille, 10: University of Geneva

In order to comprehend the process of cosmic
reionization which is suggested to be completed by z ~6, it is essential to understand the sources of hydrogenionizing radiation (Lyman Continuum; LyC). Because
LyC is easily absorbed by the intervening H I gas, thedirect measurement of LyC emission from objects atz > 5 is practically impossible, and we need to rely on
observations at lower redshifts to assess how different
galaxy populations contribute to the ionizing radiationbudget. Studies of LyC escape fraction (fesc) for starforming galaxies at z ~ 2–4 have revealed that the average
fesc is lower than 10 % while observed UV luminosity
function (LF) of star-forming galaxies at z > 6 suggests
10–20 % f esc is required to keep intergalactic spaceionized. Although this apparent tension could be resolved
in several ways (e.g., luminosity dependence of fesc or
its evolution), it is important to evaluate the contribution
to ionizing photon budget by Active Galactic Nuclei(AGNs), another population which could be significant
sources of LyC.
We use deep and wide imaging data from the CFHT
Large Area U-band Deep Survey (CLAUDS) and theHyper Suprime-Cam Subaru Strategic Program (HSCSSP) to constrain LyC fesc from AGNs at z ~ 3–4 ([1]).
The unique combination of area, depths and wavelength
coverage achieved by these two surveys enabled us to
examine LyC from 94 AGNs with a wide UV luminosity
range (−27 < M 1450 < −19 in absolute magnitude) at
spectroscopic redshift between 3.3 and 4.0. We use theirU-band / i-band flux ratios to estimate LyC transmission(a ratio of observed ionizing photon flux density to theflux density expected from the fiducial intrinsic quasar
spectrum) of individual AGNs. The distribution of their
LyC transmission shows values lower than the range of
LyC transmission values for IGM of the same redshift
range (Figure 1), which suggests that LyC fesc of AGNs
at z > 3.3 is considerably lower than unity in mostcases. We do not find any trend in LyC transmission
values depending on their UV luminosities. By using
the photometry of stacked images and assuming average
IGM attenuation degrees at the redshifts and a fiducial
intrinsic SED of AGN, we estimate the average LyC
escape fraction fesc = 0.303 ± 0.072 for AGNs at 3.3 < z< 3.6. Based on the estimated LyC escape fraction and018

I Scientific Highlights

the UV LF of AGNs, we argue that UV-selected AGNs’contribution to the LyC emissivity at the epoch is minor,
although the size of their contribution largely depends on
the shape of the UV LF.

Figure 1: LyC transmission for the sample AGNs, plotted against
their redshifts. Blue circles are the values estimated using
u-band photometry, and green squares are those using u*-band
photometry. These two filters used in the CLAUDS have slightly
different transmission curves against wavelength. Downward
triangles are 3σ upper limits for the AGNs without detectionin u-band or u*-band. The blue and green solid lines show theaverage IGM transmission for u-band and u*-band, respectively,from the Monte Carlo simulations, and shaded areas represent
their 68 %-ile fluctuations.

Reference[1] Iwata, I., et al.: 2022, MNRAS, 509, 1820.

Horizontal Velocity Estimation with Neural Network
ISHIKAWA, Ryohtaroh T.1, NAKATA, Motoki2, KATSUKAWA, Yukio1,
MASADA, Youhei3, RIETHMÜLLER, Tino L.4
1: NAOJ, 2: National Institute for Fusion Science, 3: Fukuoka University, 4: Max-Planck Institute for solar system research

Observablevertical motion

Hiddenhorizontal motion

Turbulencein the Sun

Surfacetemperature

Inference by the neural network©NASA/SDO (AIA)

Figure 1: Conceptual diagram of this study using deep learning.
Based on the vertical motion and surface temperature that can beobserved on the solar surface, we estimate the horizontal motionthat is difficult to observe. We use a neural network model taht is
one of the deep learning methods.

Simulated velocity

Estimated velocity

Estimation accuracy at each scale

1.0

Accuracy

Observation of the solar surface reveals cellularpatterns, termed granules, created by thermal convection.
Each convection cell is not stable and causes the turbulent
dynamics of the solar surface. Turbulent flows on thesolar surface is thought to play a role in supplying heatingenergy to the solar corona by amplifying and shaking themagnetic field. Therefore, it is necessary to measure thevelocity of turbulence and its spatial distribution.
Vertical velocity can be measured by the Doppler
effect, but horizontal motion cannot be measured directly.
Traditionally, local correlation tracking methods havebeen used to measure the horizontal velocity from thetime variation of the granular patterns. This method islimited to estimating convective motion on spatial scales
equal to or larger than the size of the granular spots. Theinteraction between the magnetic field and flow field that
occurs at smaller scales has been attracting attention,and estimation accuracy at smaller scales has become
an issue. In recent years, attempts have been made toestimate horizontal velocities by utilizing deep learning.
However, the accuracy of the estimation remains limited.
We constructed a deep learning model that takes
multi-scale nature into account, since there is a varietyof spatial scales of granules. In this model, kernels of
various sizes were used for convolution. Data fromseveral numerical simulations simulating solar thermal
convection were used for training. The network was
constructed to learn the relationship between thetemperature and vertical velocity structures that areeasy to observe and the horizontal motion (Figure 1).
Each of the simulations used has a different physicalprocess to produce the thermal convection, which yields
a different convective pattern. The characteristics of the
deep learning model can be examined by comparing
the difference in estimation accuracy for each of thesimulations.
To evaluate the performance in detail, we developed amethod to evaluate the estimation accuracy at each spatial
scale. It shows that our model achieves higher accuracy
than the existing method for all simulations at all scales.
While achieving high accuracy at large spatial scales,
the accuracy ie still limited at scales smaller than the
typical scale of convection (Figure 2). The clarificationof the validity and estimation accuracy provides clues forfurther improvement of the method.

0.0

10-1

large scale

10⁰

small scale

Figure 2: (left panel) Horizontal motion in different simulations
and horizontal motion estimated with the neural network model.
The light and dark colors correspond to upward and downward
flow, respectively. (Right panel) Estimation accuracy at different
spatial scales. The different colors of the lines indicate theestimation accuracy for horizontal motions in the different
simulations.

Reference[1] Ishikawa, R.T., et al.: 2022, A&A, 658, A142.

I Scientific Highlights

019

Chemical Abundances of nearby M Dwarfs
Investigated with IRD-SSP Data
ISHIKAWA, Hiroyuki Tako1/2, AOKI, Wako2/3, HIRANO, Teruyuki1/2, KOTANI, Takayuki1/2/3,
KUZUHARA, Masayuki1/2, OMIYA, Masashi1/2, HORI, Yasunori1/2, KOKUBO, Eiichiro2, KUDO, Tomoyuki4,
KUROKAWA, Takashi1/5, KUSAKABE, Nobuhiko1/2, NARITA, Norio1/6/7/8, NISHIKAWA, Jun1/2/3,
OGIHARA, Masahiro2/9, UEDA, Akitoshi2, CURRIE, Thayne4/10/11, HENNING, Thomas12, KASAGI, Yui2/3,
KOLECKI, Jared R.13, KWON, Jungmi14, MACHIDA, Masahiro N.15, MCELWAIN, Michael W.16,
NAKAGAWA, Takao17, VIEVARD, Sebastien1/4, WANG, Ji13, TAMURA, Motohide1/2/14, SATO, Bun’ei9
1: Astrobiology Center, 2: NAOJ, 3: SOKENDAI, 4: Subaru Telescope, 5: Tokyo University of Agriculture and Technology, 6: Komabat Canarias,
p a _ 9: Tokyo
al_ Institutegh gh _202_yInstitute for Science/The Univ. of Tokyo, 7: JST/PRESTO, 8: Instituto de Astrofísica deof Technology,
10:_NASAtemp ate für
annua
highl
ht Ohio
2 21
verle
Ames Research Center, 11: Eureka Scientific, 12: Max-Planck-Institut
Astronomie,
13: TheStateIshikaw
University, 14: op
The UniversityofTokyo, 15: Kyushu University, 16: NASA Goddard Space Flight Center, 17: ISAS/JAXA

M dwarfs are the ubiquitous stars in our Galaxy
and have been the main targets for exoplanet search
programs. However, due to their faintness in visible lightand the difficulties associated with low temperatures, theabundance ratios of individual elements have rarely been
investigated. We have developed a method to investigate
the individual elemental(abundanceoftemplateabundances
annual highlight
202 ratios
Ishikaw
Na, Mg, K, Ti, Cr, Mn, Fe, and Sr to H) of M dwarfs inthe solar neighborhood using data from high-resolutiongienear-infraredE
spectroscopy[1].
This study [2] uses high-resolution spectra in 9800–
17500 Å obtained by the IRD Subaru Telescope Strategicw星Program (IRD-SSP), which searches for terrestrial Sun
planets
M dwa fs
around nearby M dwarfs, to determine the elemental
abundances of 13 M dwarfs (2900 < Teff < 3500 K).
The results show
the majority of the stars
B thatard s whiletar
have a composition
similartothatof the Sun, there are
Four o ects w th hemos metallicities.
di fe ent
also stars with low
The correlations
between
A undance
distr
o
was
enera
ly si
different abundance
ratiosofthe13
targetsaresimilar
S (S
t
)
G
e
to those of FGK-type stars in the solar neighborhood(upper panel of Fig. 1). In addition, the kinematics of the
13 stars in the Galaxy was investigated by combining
data from the Gaia. It was found that M dwarfs withlower metallicities tend to have kinematics different
図 is左は元素
from the Sun (lower panel of Fig. 1). This trend
also
同
known for FGK-type stars and is interpreted to reflectthechemical evolution of the Galaxy. A well-known M dwarf“Barnard’s star” is included in the targets. Many previous一
図 1：左は元 量比 Fe/H と[M Fe の関係、右は銀 中心座標にお る 次元速studies have reported
evidence indicatingの that this starはhas a relatively old origin, and the individual elemental
abundances obtained for the first time by this study are
consistent with this.
These results suggest that while most of the nearby
M dwarfs studied here are of Galactic thin disk origin,some are of older origin, given their lower metallicity anddifferent kinematics than the Sun.

020

I Scientific Highlights

FGK dwarfsSun} M dwarfs
Barnard’s Star
Four objects with thedifferentrmosteaf（年次kinematics from theSun (See bottom panel)

Abundance distribution
was generally similar to
FGK-type stars

Barnard’s Star

Sun

Figure 1: The upper panel shows the abundance ratios ofmagnesium to iron as a function of the abundance ratios of ironto hydrogen. The lower panel shows the Galactocentric spaceと g e] 関
心
にお
3 元速
さ た
velocities.
In both panels,
red
stars
indicateした
the 13 星
M dwarfs
treated in this study, and red triangles indicate the results for the
M dwarfs treated in our previous study [1]. For comparison, the
星は、太陽と似
組成や運 を示
天体が多い
literature values
for about
1000 FGK-type stars [3] are shown as
black dots.

References[1] Ishikawa, H. T., et al.: 2020, PASJ, 72, 102.
[2] Ishikawa, H. T., et al.: 2022, AJ, 163, 72.
[3] Adibekyan V. Z., et al.: 2012, A&A, 545, A32.

II Status Reports of Research Activities
01. Subaru Telescope
1. Subaru Telescope Staff
As of the end of FY 2021, the Subaru Telescope staff
consisted of 21 dedicated faculty members including fivestationed at Mitaka and two stationed at Okayama, fiveengineers, one project associate professor, five senior specialist,
and three administrative staff members. Additional staff
members include one project professor, one project associate
professor, two project assistant professors, ten project researchstaff, 11 senior specialist, six administration associates, one
public outreach staff member, and one research supporter, allof whom are stationed at Mitaka. Additional staff members
include one project associate professor, and three administration
associates, all of whom are stationed at Okayama. Moreover,
16 research/teaching staff members, 13 of whom are stationed
at Mitaka and three of whom are stationed at Pasadena, andthree engineers, one of whom is stationed at Mitaka, one ofwhom is stationed at Nobeyama, and one of whom is stationed
at Mizusawa, are posted concurrently. The project also has 67
local staff members dispatched from the Research Corporationof the University of Hawai`i (RCUH), including scientificassistants; engineers in charge of software and observational
instruments; technicians for facilities, machinery, vehicles, andlaboratories; telescope/instrument operators; administrative staff;
researchers employed for Grant-in-Aid for Scientific Research;
Post-Doctoral 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 2021, Subaru Telescope produced many outstanding
scientific outcomes which were published in major international
journals. Below are some examples:(1) A group of astronomers discovered two rocky super-Earthexoplanets lacking thick primordial atmospheres in very close
orbits around two different red dwarf stars. The two planetcandidates (TOI-1634b and TOI-1685b, originally identified
by NASA’s TESS spacecraft) around red dwarf stars wereconfirmed as rocky super-Earths in ultra-short-period orbits byusing the Subaru Telescope and other telescopes. The InfraRed
Doppler (IRD) spectrograph revealed that the planets are “bare,”meaning that they lack primordial thick hydrogen-helium
atmospheres, possibly due to interactions with the extremely
close host stars. The results also show that TOI-1634b is one of
the largest (1.8 Earth radii) and most massive (10 Earth masses)
planets among the known ultra-short period rocky planets. These

new planets offer excellent opportunities to study what kinds
of atmospheres, if any, can develop on ultra-short-period rocky
planets, and provide clues to help understand how such unusual
planets are formed.
(2) One of the youngest planets ever found around a distantinfant star has been discovered using the Infrared Camera andSpectrograph (IRCS) on the Subaru Telescope. The researchers
estimate that the planet, named 2M0437b, is a few times more
massive than Jupiter, and that it formed with its star several
million years ago, around the time the main Hawaiian Islands
first emerged above the ocean. It joins a handful of objects
advancing our understanding of how planets form and changewith time, helping to shed new light on the origin of the Solar
System and Earth.
(3) Using the High Dispersion Spectrograph (HDS), a new studyof lithium production in a classical nova V5669 Sgr found a
production rate of only a couple of percent that seen in otherexamples. This shows that there is a large diversity withinclassical novae and implies that nova explosions alone cannot
explain the amount of lithium seen in the current Universe.
This is an important result for understanding both the explosion
mechanism of classical novae and the overall chemical evolutionof the Universe.
(4) Astronomers have found tails of gas and/or stars trailingbehind a sample of young galaxies without current starformation using Hyper Suprime-Cam and Suprime-Cam data in
the archive. Based on this result, the team concludes that about
half of the ultra-diffuse galaxies in the Coma cluster are likely
to have evolved through collisions with external gas. Ultradiffuse galaxies, together with similar dwarf elliptical galaxies,
account for about 80 % of the members of galaxy clusters, so
understanding their evolution is an important part of modelingthe evolution of the Universe.

3. Open-use
In S21A, 34 programs (58.3 nights including 2.5 nights for
ToO programs) were accepted out of 138 submitted proposals,requesting 286.9 nights in total. In S21B, 37 proposals (60.3nights including 1.5 nights for ToO programs) were acceptedout of 135 submitted proposals, requesting 307.8 nights in total.
In S21A and S21B, 25.5 nights (5 programs) and 13 nights(4 programs) were allocated respectively for the continuous
intensive programs. Service observations were allocatedfor 2.5 nights in each semester. In S21A and S21B, 1 and 2
programs accepted as open-use proposals were by foreign
principal investigators, excluding the University of Hawai`i.

II Status Reports of Research Activities

021

The number of applicants in submitted proposals was 2315 forJapanese researchers (Japanese astronomers at any institute andnon-Japanese astronomers belonging to Japanese institutes)
and 951 for foreign researchers. The number of researchersin accepted proposals was 712 for Japanese astronomers and306 for foreign astronomers. In S21A and S21B, the numberof open-use visiting observers was 490, and 71 were foreign
astronomers. 84 astronomers observed remotely from Mitaka.
In S21A and S21B, 92.29 % of the open use time (including
University of Hawai`i time) was used for actual astronomical
observations after excluding weather factors and scheduled
maintenance downtime. About 1.39 %, 0.11 %, 6.14 %, and0.07 % of observing time was lost due to instrument trouble,
communication trouble, telescope trouble, and operation trouble,
respectively. In S21A and S21B, remote observations from Hilowere conducted for 11 programs with 13 nights. On the other
hand, remote observations from Mitaka were conducted for 17.5
nights with 6 programs including HSC SSP. The numbers oftelescope time exchange nights between Subaru Telescope andKeck were 5.0 nights in S21A and 8.0 nights in S21B. For thosebetween Subaru Telescope and Gemini, Subaru Telescope users
used Gemini time 4.5 nights in S21A and 2.5 nights in S21B (notincluding Fast Track programs) while Gemini users used Subaru
Telescope time 5.3 nights in S21A and 4.1 nights in S21B.

4. Telescope Maintenance and Performance
Improvement
The following major repairs, maintenance, and changes were
implemented in FY 2021.
(1) Replacement of the primary UPS at the Summit facility:
As part of the preventive maintenance work for stable
operation of the telescope, the primary UPS were replaced.
(2) Top Unit Exchange system maintenance:
Maintenance and inspection of the Top Unit Exchangesystem, which had been postponed due to COVID 19, wasperformed. However, due to the coronavirus, the replacement ofsome large equipment was postponed until next year or later.
(3) 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 to renew the dome air
conditioning system, prepare for the recoating of the primary
mirror, and to upgrade the telescope software to improveobservation efficiency.
The other hand, we started the “Telescope MaintenanceGroup collaboration of NAOJ”. The purpose of this activity
is to share know-how and maintenance plans for maintenanceof telescopes owned by NAOJ, and to carry out, evaluate, andimprove maintenance activities through cooperation amongobservatories.

022

II Status Reports of Research Activities

5. Instrumentation
The following five facility instruments were provided forthe open-use observations in FY 2021: Hyper Suprime-Cam(HSC), Faint Object Camera And Spectrograph (FOCAS),High Dispersion Spectrograph (HDS), Infrared Camera andSpectrograph (IRCS), and the 188-elements Adaptive Optics
and Laser Guide Star system (AO188/LGS). As for the carryin instruments, the Simultaneous-color Wide-field Infrared
Multi-object Spectrograph (SWIMS), Fast Near-Infrared
Polarization Differential Imaging (FastPDI), and MKID
Exoplanet Camera (MEC) were newly opened for the openuse programs, in addition to the existing carry-in instrumentsof Subaru Coronagraphic Extreme Adaptive Optics (SCExAO),
Coronagraphic High Angular Resolution Imaging Spectrograph(CHARIS), and Visible Aperture Masking Polarimetric Imager
for Resolved Exoplanetary Structures (VAMPIRES).
The operation of the Multi-Object Infrared Camera andSpectrograph (MOIRCS), one of the facility instruments, hasbeen hibernated since February, 2021 to facilitate the science
operation of the carry-in instrument SWIMS which has a similarcapability to MOIRCS. In addition, the operation of LGS has
been temporarily suspended for its upgrading project.
Among the upgrade projects of the facility instruments, theinstallation of the new LGS system was completed in FY 2021
and it successfully achieved the engineering first light in March
2022. Its integration and test are still ongoing and it will be
opened for open-use programs from S23A. For HSC, fabricationof new filters is still ongoing by HSC users and we received
a narrow-band filter “NB506” and extremely wide-band filter“EB-gri” in FY 2021. They passed the acceptance test and havebeen approved to be opened from S22B. For the Nasmyth Beam
Switcher, we completed the final design, which was done incollaboration with Australian Astronomical Optics, Macquarie
University, and fabricated the optical and mechanical parts in FY
2021. Its assembly, integration, and test are planned in FY 2022.

6. Computer and Network
The Subaru Telescope computing and network systems
core system remained stable with remote work being a key
component. CDM(Computer and Data Management) continued
to operate necessary network services. CDM worked on-site
periodically to assist with users’ needs, install new equipment,
and perform regular housekeeping of working areas. CDM
is working with other groups to become the managers of
network and server equipment, allowing different groups tobe released from those responsibilities. CDM is planning to
implement a new network layout for the GEN2 base and summit
environment. The primary goal is to replace the aging network
equipment for OCS (Software Division), and implement new
fail-over technology with 25/40/100 Gbps uplinks to maximize
the bandwidth between data transfer sub-systems. CDM
continues on-site monitoring and maintenance for the HSC andPFS analysis environment; and installation and configuration of
new servers.

Major improvements came from the Fully-Remote Project.
CDM assisted in the procurement of servers and 100 Gbps
network equipment for a high-speed data transfer network from
the Maunakea summit region to Hilo and Mitaka Campus.
The equipment was installed during February by Mitaka ITSO(Information Technology Security Office) engineers, assisted
by a CDM technician. The University of Hawai`i – Information
Technology and Network Department played a key role inconfiguring the network infrastructure for this project. In
early May, an initial test of the 100 Gbps network during HSC
observations, provided a glimpse of the great potential that thehigh-speed network will provide. Between the efforts of ITSO,
CDM, OCS, and HSC Mitaka Teams, network connections
between Maunakea and Mitaka were successful in transferring
near real-time HSC observation data. Other parts of this project
include Zoom PC based systems, which replaced physical Video
Conferencing equipment; new GERS (GEN2 Remote Users
Observation Portal); Mitaka Data Analysis server; and an on-site
HSCA (Hypersuprime Cam Analysis Cluster) storage array witha 40 Gbps interface.
CDM with the guidance of Associate Director Hideki
Takami, started the process to replace STN5 contract equipment
by February 2023. The next computer and network system,
basically called STN6 will be considerably smaller in physicalsize, but CDM is committed to continue all services necessary
for users. CDM will reduce not only the servers, but also the
network core switches. CDM will leverage 100 G network
switches to maintain the necessary number of network
connections. Our goal with STN6 is to run as efficiently as
possible in power, heating, and processing. Specifications arebeing decided, and the contract process will begin in June 2022.

CDM at this moment is working to virtualize and update to along-term supported OS of all services currently running. The
hope is to have the new virtual systems run STN5 until the endof the contract, and easily migrate to new servers.

7. Education (Under-graduate and Graduate Courses)
The number of Subaru Telescope staff members in Hilo whowere concurrently appointed by SOKENDAI (graduate school)
was ten. The number of SOKENDAI students who had primarysupervisors affiliated with Subaru Telescope (including those
concurrently belonging to Subaru Telescope) was 11, whichconstituted more than one-third of the total 30 SOKENDAI
students hosted in NAOJ. Of those, six had supervisors who
belonged primarily to Subaru Telescope.
In FY 2021, Subaru Telescope hosted 1 graduate student
for a long stay in Hilo (there were no SOKENDAI students).
On top of that, intensive education activities were seen also in
the Subaru Telescope Mitaka Office. The numbers of graduate
course students in all of Japan who obtained master’s degrees
and PhDs based on Subaru Telescope data were 16 and eight,
respectively, of which two and two were related to the Subaru
Telescope Mitaka Office.
We also regularly hosted a series of educational programs
at Subaru Telescope. We hosted a Subaru Telescope observation
training course for three new SOKENDAI students held inJanuary 2022. This was done remotely from Mitaka, due to theworldwide COVID-19 pandemic. In the Hilo and Mitaka offices,
we had many official and informal seminars (remotely this year),many of which were jointly organized with other divisions in
NAOJ and/or neighboring universities.

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
2021.

1. Seimei Telescope(1) Open-use (calendar year)
In the first half of 2021 (January-June), 70 nights were
provided. The number of applications was 20 (Classical: 12,
Classical + ToO: 1, ToO: 7) and the number of nights requested

was 115.2 (Classical: 95, ToO: 20.2), while the number of
accepted applications was 16 (8, 1, 7) and the number ofawarded nights was 81.4 (62.5, 18.9). 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 indicatedby the proposer. The total lost time during this period was 1.0
night. In the second half of 2021 (August-December) 62 nights
were provided. The number of applications was 24 (13, 1, 10)
and the number of nights requested was 114.77 (84, 30.77),
while the number of accepted applications was 21 (10, 1, 10)
and the number of awarded nights was 79.1 (52, 27.1). Total losttime during this period was 3.0 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

II Status Reports of Research Activities

023

In the first half of 2021, only the Kyoto-Okayama Optical
Low-dispersion Spectrograph with the optical-fiber Integral
Field Unit (KOOLS-IFU) was available. In the second halfof 2021, the imaging mode (< 10 fps) of the TriColor CMOS
Camera and Spectrograph (TriCCS) was newly available.
Activities also included management and operation ofenvironmental monitors, storage of acquired data, maintenanceof computers and networks, and maintenance of facilities.
(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 (within
FY 2021).
(4) Research results
The following example of important research results fromobservations with the Seimei Telescope was published in a paper
in FY 2021.
(a) Continuous spectroscopic observations of the young solartype star EK Draconis by several telescopes, the mainstay ofwhich is the Seimei Telescope, and photometric observations
with NASA’s TESS satellite detected an Hα line brightening
phenomenon by spectroscopic observations at the same time
as a white light brightening in photometric observations. This
was the first successful spectroscopic observation of a superflare in visible light for a solar-type star. The Doppler shift of
the Hα line caused by the super-flare was also observed, and the
motion of material with a temperature of about 10,000 K was
captured as it approached along the line of sight. They foundthat this is very similar to filamentary ejections in the Sun, anddiscovered for the first time in the world that a super-flare in asolar-type star is accompanied by a supermassive filamentary
ejection. This is a very important achievement in understanding
the motion of matter associated with super-flares in solar-typestars, their effects on the surrounding interplanetary space, andthe impact of the young Sun or other young solar-type stars on
the atmosphere of the young Earth or young exoplanets orbiting
other stars.

2022. The second term committee was dissolved at the end of
September 2021, and the third term committee was establishedin October.
(c) Kyoto University 3.8-m Telescope Council
On September 24, 2021, the Kyoto University Graduate Schoolof Science and the National Astronomical Observatory ofJapan (NAOJ) held online the fourth meeting of the Kyoto
University 3.8-m Telescope Council regarding the operation of
the Seimei Telescope. The meeting was attended by the Dean of
the Graduate School of Science, Kyoto University, the Director
General of NAOJ, and many others. The status of the operation
was reviewed and research results were reported.

2. Telescopes of the former Okayama
Astrophysical Observatory(1) 188-cm reflecting telescope(a) On July 27, 2021 and March 14, 2022, the National
Astronomical Observatory of Japan (NAOJ), the Exoplanet
Observation Research Center at the School of Science of theTokyo Institute of Technology (TITech), and Asakuchi City held
online the operational council meetings to discuss the use of the
188-cm reflecting telescope.
(b) The revenue from the 188-cm telescope fee enabled us torepair the slit door guide rail, replace the slit door drive wirerope, install a safety fence on the upper deck access ladder,renew the safety fence for the elevating floors, install a storage
room for observing instruments, conduct an annual inspection of
the crane, renew the air conditioners, install LED lighting, repair
the restrooms, renew some interior doors, replace furniture, dowest entrance stage renovation, implement west entrance door
renewal, exterior tile repair, and eave painting. In addition,
the 188-cm primary mirror cover was repaired; the vacuum
evaporation chamber was inspected and maintained; the small
vacuum evaporator was upgraded; the remote observation
environment on the second floor of the Main Building was
prepared; Wonder Eye for viewing parties was maintained; and adrone was introduced for dome maintenance inspections.

(5) Meetings

024(a) Seimei Users Meeting
The third Users’ Meeting was held online on August
11–12, 2021. Meeting Managers: Akito Tajitsu (NAOJ)(Representative), Mikio Kurita (Kyoto Univ.), Masaaki Otsuka(Kyoto Univ.), Masayuki Akiyama (Tohoku Univ.), Shigeyuki
Sako (Univ. Tokyo), Satoshi Honda (Univ. Hyogo). The
maximum number of simultaneous connections was about 90,
and the total number of participants was 117.

(c) We cooperated with the Tokyo Institute of Technologyled aluminization work on the primary mirror of the 188cm reflecting telescope from November 8 to 10, and saw thecompletion of all work without incident. We then accepted thealuminization work on the 1.5-m primary mirror of the Kiso
Schmidt Telescope of the University of Tokyo from November
10 to 11, and on the 1.5-m primary mirror of the Kanata
Telescope of Hiroshima University from November 11 to 12,
and saw the completion of all the work successfully.

(b) Seimei Subcommittee
The Subcommittee met eight times in FY 2021. Two of thesemeetings were for the time allocation to the open-use observing
proposals for the second half of 2021 and the first half of(2) Other telescopes
We also cooperated in the operation of the 91-cm reflecting
telescope, the 50-cm reflecting telescope (MITSuME), and theThirty Milli-Meter Telescope (TMMT).

II Status Reports of Research Activities

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 June 2021, the Okayama Branch received an award fromthe Okayama Prefectural Tourism Federation for its contribution
to Okayama Prefecture's tourism and industry in Fiscal Year
2021, in recognition of the more than 2 million visitors to the
publicly accessible portions of the observatory campus since its
opening in 1960.
(2) In July 2021, the Okayama Branch opened a webpage, inJapanese (http://okayama.mtk.nao.ac.jp/index.html).
(3) In December 2021, “Fiery Dragon’s Breath May Scorch
Young Planets” was released on the web as a result ofcooperative observations by multiple telescopes including the
Seimei Telescope.

II Status Reports of Research Activities025

02. Nobeyama Radio Observatory
1. Nobeyama 45-m Radio Telescope(1) Open Use Observations
The 40th open use observations term started on December
1, 2021. The statistics of the successful proposals are as follows.
“General Programs”: 10 programs were accepted out of 26
submitted proposals including three programs from abroad(out of 10 submitted), “GTO (Guaranteed Time Observation)
Programs”: one submitted proposal was accepted, VLBI open
use observations including the 45-m telescope: five proposals
were accepted out of six submitted.
Remote observations were conducted from Mitaka, Iriki,
Mizusawa, Kagoshima University, Osaka Prefecture University,
University of Tokyo, Keio University, Shibaura Institute ofTechnology, and ASIAA (Taiwan).
(2) Improvements and Developments(a) New Developments
The observatory started the design and fabrication of a new
focal plane array receiver system for observations at 72–116
GHz. It employs seven beam elements, and allows observationsof two polarizations and three bands. This development was
supported by JSPS grant-in-aid KAKENHI Kiban S (PI: K.
Tatematsu).
(b) Approved Development Programs
A total of five programs are in progress as follows. The
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.
Simultaneous observations of H22 and Z45 receivers wererealized by developing and installing a frequency selective
filter.
- Frequency-modulation local oscillation FMLO.
- Band 1 (30–50 GHz) receiver (named “eQ”) developed in
Taiwan was installed on the 45-m telescope and commissioned
to carry out performance evaluations as well as test
observations.
- Millimetric Adaptive Optics (MAO): Development of a Wavefront Sensor.
- 100-GHz, 109-element MKID camera.
(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 were
performed.
- Corrective maintenance due to some malfunctions in thefollowing systems.
- The sub-reflector controller unit of the antenna- The FFT board of the SAM45 spectrometer026

II Status Reports of Research Activities- The power supply unit of the NTP server- The compressor of the refrigerator for FOREST- The replacement of the computer-control system of the M5
mirror, in the older beam transmission optics, was completed.
- Development of the observation preparation tool for overseas
observers is underway.
(3) Scientific Results
A total of 35 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
Amada et al. observed an evolved star IRAS16552-3050 andfound that SiO maser emissions are emitted from this object.
This is the second object for which the SiO maser emissions
were found in evolved stars accompanying a high-velocity
outflow in the H 2 O line, and the paper concludes that themassive outflow that appeared at the end of the asymptotic giant
branch phase drives the emission of the SiO maser. Kohno, M.
et al. observed CO lines toward the Vulpecula OB associationin the Local Spur and found the evidence of cloud collisions
from observations of the gas around the OB association.
Yamada et al. observed the Orion B giant molecular cloud toinvestigate gas kinematics around the high-mass star-forming
region. Sofue et al. showed that the drastic feedback from thehigh-mass star cluster in M17 created an unusual high velocity
component in surrounding gas. Murase et al. observed the NH3line to investigate gas heating around high-mass stars. Sato et al.
investigated a star forming ring in a bared spiral galaxy NGC613
and concluded that the difference of star formation activity in thering is related to the velocity difference between the ring and thebar. Xu et al. applied a deep learning technique to detect outflow
objects in the molecular gas data of nearby molecular clouds andfound the outflows can provide sufficient energy to sustain the
turbulence in the clouds. Dewangan et al. used CO data observedwith the 45-m telescope and archival data for other wavelengths
to investigate the galactic HII region G25.4-0.14 and concluded
that the formation of the stellar cluster located in the central
region of the hub-filament is explainable with the global nonisotropic collapse scenario.

2. Research Support(1) 1.85-m Radio Telescope (Osaka Prefecture University)
With the 1.85-m radio telescope, we 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, we started a new project
supported by JSPS (Grant-in-Aid for Scientific Research on
Innovative Areas). In this project, we will relocate the telescopeto the Atacama site in Chile at an altitude of 2400 m, equippedwith an ultra-wideband receiver (230–345 GHz), and carry out

an extensive survey of molecular clouds along the Galactic
plane and in the Magellanic Clouds in the southern sky. In FY
2019–2021, in preparation for this relocation, we renewed thetelescope system and radome, and developed and tested an ultrawideband receiver in cooperation with ATC in NAOJ Mitaka
Campus. We have successfully developed a wideband receiversystem using superconducting receivers at 230 and 345 GHz,a horn covering the frequency band (210–375 GHz), and anintermediate frequency (IF) band circuit covering 4–21 GHz.
The system can observe six spectra (12CO, 13CO, and C18O)
simultaneously across the two frequency bands. It was mounted
on the 1.85-m telescope, and we succeeded in the commissioning
observations; we successfully mapped the molecular clouds inthe six emission lines toward several star-forming regions. In FY
2021, one peer-reviewed paper (Gregorio-Hetem et al. 2021),
which used the archive data obtained by the telescope for the
analysis and, three papers on the commissioning observations(Nishimura et al. 2021, Masui et al. 2021, Yamazaki et al. 2021)
were published.

held and we supported them.
Moreover, the “Nagano Prefecture is Astro-Prefecture”
liaison council, which was founded in 2016 through cooperation
with Kiso Observatory and other organizations promoted
the activities such as monitoring night sky condition in theprefecture. The sixth meeting was held online and on-site at
Syogaigakushu-center in Chino on November 13 with about 60
participants. Some activity reports and a discussion on future
activities were presented.

3. Public OutreachThree master’s course students from Osaka Prefecture
University were accepted for education.

(1) PR activities at Nobeyama Campus
Nobeyama Campus received a cumulative total of 30,371
visitors throughout the year. The open area for visitors islimited to outdoor areas as a precaution against the spread of
COVID-19. During the COVID-19 situation, staff members
conducted only two guided tours for local schools and granted
12 requests for on-site filming and interviews. One workplace
visit by local junior-high schools was conducted. There was norequest for Super Science High School (SSH) student visits.
The filming and interview requests were mainly about research
activities, cooperation with the local government, promotion of
the “Nagano Prefecture is Astro-Prefecture,” introducing NRO,
and the new operation scheme of NRO starting in April 2022.
In the visitors' open area, the NINS Nobeyama Exhibition
Room has been forced to close during the COVID-19 situation.
The annual Nobeyama Special Open House was held as an
online event. The total number of connections for live streaming
was about 6,700 and the total number of views for all content
was about 130,000 in one month after the event.
Moreover, we received and answered about 162 phone
calls this year from the public regarding the regular openingof the observatory, observatory events, and general astronomy(including 10 interviews).
(2) Cooperation with Local Communities
The annual Nobeyama Special Open House was held
online with contributions by Nagano Prefecture as well as
Minamimaki Village. However, “Jimoto Kansha Day (Thanks
Day for the Locals)” for local communities (Minamimaki and
Kawakami Villages) by 3 Nobeyama institutes was cancelled.
The sora-girl event “Tebura de Hoshizora Kansho-kai (Dropby Star Gazing Event),” hosted by the Minamimaki Tourism
Association and the photography event for the Nobeyama
starry sky in Nobeyama Campus by Minamimaki Village were

(3) NINS Nobeyama Exhibition Room
Although the NINS Nobeyama Exhibition Room had been
opened throughout the year in cooperation with NINS and otherinstitutes, it was forced to close during the COVID-19 situation.
Furthermore, the 4D2U theater could not be presented during
this year. However, the 4D2U theater was presented online 24
times, mainly on holidays.

4. Education

5. Misc. Activities(1) Activities related to the Agreement on Mutual Cooperation
between NAOJ and Minamimaki Village
In 2018, NAOJ and Minamimaki Village signed 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 the promotion
corporation of Minamimaki Village. They had 28 paid group
tours and filmings.
(2) Hiring, Transfer (incoming)
Nishimura, Atsushi: Project Associate Professor,New recruit(3) Retirement, Transfer (outgoing)
Uchiyama, Yoshifumi: Senior Staff of Accounting Section,
moved to Shinshu University
Kinugasa, Kenzo: Senior Specialist, retired
Ide, Hidemi: Technical Expert, retired
Hayashi, Mitsuru: Technical Expert, retired
Inoe, Norio: Technical Expert, retired
Kodaira, Toshiko: Administrative Supporter, retired(4) NRO Conference Workshops and Users Meeting- December 14, 16, and 21, 2022, On-line
FY 2021 ALMA/45-m/ASTE Users Meeting (Organizing
Committee: Hiroshi Nagai, Misato Fukagawa, Daisuke Iono,
Alvaro Gonzalez, Ken Tatematsu, Takeshi Kamazaki (NAOJ))

II Status Reports of Research Activities027

03. 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. The observatory also operates the
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. Furthermore, KaVA (KVN and VERA Array),which combines VERA and KVN (Korean VLBI Network)in Korea, and the East Asian VLBI Network (EAVN), which
consists of Japanese, Chinese, and Korean radio telescopes,
are also being operated and opened to the international
community. As a member organization of the Event Horizon
Telescope project, the observatory contributes to the promotionof millimeter-wave VLBI as well.
In addition to these VLBI-related activities, the observatory
plays a wide range of roles beyond astronomy, such as operationof the Timekeeping Office, which determines the official timein Japan, and also 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 control
from AOC (Array Operation Center) at NAOJ Mizusawa
Campus. In FY 2021, due to long-term maintenance work from
November 2021 to February 2022, the regular VLBI operations
except for EAVN Common Use were suspended, and theannual observation time has decreased by about 30% from theusual year. A total of 188 (1,814 hours) VLBI observations wereconducted with VERA; such as VERA project observations;fringe detection observations for maser and reference sources;
geodetic observations; and JVN (Japanese VLBI Network)observations. In addition to these, 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 processedat the Mizusawa Correlation Center in NAOJ Mizusawa
Campus. The correlated data were sent to each researcher
for the case of common-use and JVN observations and to
persons in charge of data analyses in the case of project dataand geodesy data. VERA common-use calls-for-proposals in
FY 2021 were not conducted by VERA alone. This is because
almost all observing 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 2021, Mizusawa VLBI Observatory published a028

II Status Reports of Research Activities

total of 37 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 SOKENDAI and University of Tokyo as a PI. Using
the facilities operated by Mizusawa VLBI Observatory, one
paper was published to report the VERA astrometry results forthe structure of the Milky Way Galaxy, one for the pulsar study
using the VERA 20-m antennas as single-dish telescopes,
one for an active galactic nuclei (AGN) using the Korea-Japan
international collaboration project KaVA (KVN and VERA
Array), and three for the performance evaluation, variability
study, and high-sensitivity imaging of AGNs with the East
Asian VLBI Network (EAVN). In addition, five papers were
published on the AGN studies from the international project
Event Horizon Telescope (EHT) in which Mizusawa VLBI
Observatory is participating. Instead of observational studies
on the Milky Way Galaxy, star-formation, and stellar evolution
through maser astrometry with VERA, multi-wavelength
studies from radio to optical, X-ray, and gamma-ray for
AGNs and pulsars are newly developing under international
collaborations with EAVN and EHT. Consequently, 6 related
papers were published in FY 2021. Furthermore, results fromthe precursors and pathfinders of the Square Kilometre Array(SKA), which is being planned in Mizusawa VLBI Observatory
by the SK A1 Study Group, were published, including 2
papers from VERA as introduced above. There were 4 papers
for cosmology (Epoch of Reionization) from the Murchison
Widefield Array (MWA) in Australia, 2 for a radio galaxy andgalaxy cluster from MeerKAT in South Africa, and 1 for maser
variability in a star-forming region from VLA (Very Large
Array) in the US.

2. The Japanese VLBI Network (JVN)The University VLBI Collaboration Observation projectis carried out as a joint research project between NAOJ andsix universities. We organize the radio telescopes of VERA,
universities, and research institutes (JAXA/ISAS) to makethe Japanese VLBI Network (JVN), which is operated at threebands of 6.7 GHz, 8 GHz, and 22 GHz. VLBI observations
were carried out for 225 hours in total in FY 2021. The main
research subjects are compact objects toward the galactic
center, gamma-ray active galactic nuclei, and methanol masers.
In addition, over 4000 hours of single-dish observations werecarried out as research related to JVN by Ibaraki University.
In FY 2021, JVN was in the last year of being an A-projectof NAOJ. The term of this project is three years, and the
purpose of this project is to promote time-domain VLBI
astronomy with three research targets as follows: (1) CH 3OH
masers with periodic flux variations, (2) extremely compact
HII regions just after the onset of nuclear burning, and (3)time domain VLBI astronomy of high-energy astrophysicalevents. The high-sensitivity telescopes larger than 30 m of JVN

constitute the key baseline. A survey of extremely compact
HII regions and gamma-ray emitting AGN candidates were
examples of the JVN observations in 2021.
In this year, some papers, such as Imazato et al. (2021) and
Huda et al. (2021), led by JVN researchers were published.
The activities of JVN were presented in some workshops andconferences. A joint research seminar, Ibaraki-Yamaguchi Joint
Seminar, was held for students of these two universities.
For development study, Imai (Kagoshima University),
Niinuma (Yamaguchi University), and Yonekura (Ibaraki
University) led the upgrading the VLBI observation system at
the Nobeyama 45-m Radio Telescope and Ibaraki Station byobtaining Grants-in-Aid for Scientific Research. Some studentsof Ibaraki and Yamaguchi Universities were supervised byProfessor Ogawa in Osaka Prefecture 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 0, E AV N ( E a s t A si a n V L BI Ne t wo r k)observations, utilizing KaVA, the Tianma 65-m, Sheshan 25m, Nanshan 26-m, Nobeyama 45-m, and Yamguchi/Hitachi/
Takahagi 32-m radio telescopes, were conducted for a totalof 186 observations (1,395 hours), including common use
observation, test, and verification observations. The total
observation time has increased by 20 % from last year. Mostof the scheduled observations were successfully conductedwithout any major issues despite the global COVID-19
pandemic.
EAVN open-use calls for proposals for semesters 2021B
and 2022A were released in April and October of 2021,
respectively. In total, 36 proposals requesting a total time of
1,290 hours were submitted from Japan, Korea, China, UK,
Italy, and Thailand. Through the evaluations by 60 referees
nominated from scientists in related fields and the subsequentdecision made by the EAV N combined Time Allocation
Committee, a total of 29 proposals (1,051 hours) were acceptedin 2021B and 2022A.
Regarding global mm-VLBI, EHT observations werecarried out remotely in March 2022 due to the outbreak of
COVID-19.
(2) Results of Research
In FY 2021, 3 papers based on KaVA (2 on active galactic
nuclei, 1 on massive star forming regions), and 3 papers basedon EAVN (1 on array performance evaluation, 2 on active
galactic nuclei) were published in peer-reviewed journals. Fiveof them include significant contributions from members ofMizusawa VLBI Observatory as the lead author or co-authors.
Here some works are highlighted. Kino et al. (2021) monitored
the jet motion of the radio galaxy 3C84 over several years
using KaVA. They captured the moment when the jet collided
with a high-density gas cloud in the circumnuclear region. This
provides evidence that the gravitational energy of the central
black hole is fed back into the galaxy through a jet. EHT Multi-

wavelength Science WG et al. (2021) reported the results fromthe 2017 M87 multi-wavelength observing campaign including
EHT and EAVN, and the study revealed a historically low
activity state of the M87 black hole in 2017. Members ofMizusawa VLBI Observatory played a leading role in paper
coordination, and a press release was also made. As for EAVN
papers two studies, Cui et al. (2021) and Cho et al. (2022), were
led by graduate students. Cho et al. (2022) analyzed in detail
the EAVN SgrA* 22/43 GHz data acquired near in time to
EHT2017, and evaluated the influence of interstellar scattering,which is a necessary piece of information for successful
imaging of SgrA* with EHT. In addition, one M87 paper basedon the KaVA Large Program was submitted to a refereed
journal during FY 2021.
Regarding mmVLBI/EHT, 5 papers (including the abovementioned multi-wavelength paper) were published in peerreviewed journals. In particular, Janssen et al. (2021) obtained
an EHT image of the core of the nearest radio galaxy Centaurus
A based on 2017 observations, and provided important insights
into the formation mechanisms of black hole jets. In addition,
SgrA * papers (6 main papers and 4 official papers) based on2017 EHT observations were compiled and submitted to a peerreviewed journal (some of which were accepted during 2021).

4. Future Planning for SKA
The SKA1 Study Group (SKA1SG) was organized underMizusawa VLBI Observatory for a three-year period since
FY 2019 to conduct preparation studies aimed at project
proposals and in-kind contributions to the SKA1 construction
according to the charge from NAOJ HQ. The project plan ofJapanese participation for SKA1 was proposed in October 2021
by SKA1SG which describes a 2 % contribution to the total
SKA program. For the contribution to SKA1 construction, theJapanese contribution is planned to be mainly Assembling,
Integration, and Verification (AIV) along with other partsof the SKA Observatory Development Program. Japan will
also contribute 2 % to the construction of the SKA Science
Reginal Center (SRC), which is assumed as the same ratio as
the construction contribution. On the scientific side, the project
proposed the plan to focus on promoting major Japanesescientif ic themes and providing user suppor t including
stimulating joint-use observation proposals and supporting
data analysis and archival data use for not only focused themes
but also wider SKA scientific research. At first, this agreement
was to be for the period 2022–2028, during the constructionof SKA1, but in the course of deliberations by the Project
Review Committee, it was requested that the project period be
extended to 2033, when initial research results are expected.
The proposal was revised accordingly.
An SKA science strategy workshop was held on July
12–14, 2021, to discuss Japan’s research strategy in cooperation
with SKA-JP, a Japanese SKA user community organization.
We have a consensus that a strategic Japanese science planis important to promote the research by setting up research
themes that Japan should focus on, while participating in the

II Status Reports of Research Activities029

wide range of scientific research expected to be conducted by
the SKA. The meeting discussed scientific impact, expected
results, and fostering work by young researchers on possible
themes; and selected cosmic reionization, cosmic magnetic
fields, and pulsars as priority research areas.
In addition, SKA-JP proposed participation in the SKA
as a priority large-scale plan to the Science Council of Japan
Master Plan 2023. As requested from the SCJ astronomy andastrophysics subcommittee, SKA-JP presented a scientificresearch plan and Japanese participation plan at the Japan
Radio Astronomy Forum Symposium on the Future Plan ofRadio Astronomy 2021. And the SKA participation plan wasrecommended as one of prioritized plans by the Japan Radio
Astronomy Forum. In response, SK A1SG and the SK AJP made a joint proposal at the Science Council of Japan’s“Symposium on Large and Medium-Sized Future Plans in
Astronomy and Astrophysics” (held on August 10, 2021), but
the Master Plan 2023 itself was subsequently cancelled.
We continued to employ a project research staff member
based on the agreement with the SKA Observatory to planscientific research, and also to develop a testing machinefor the network-type data analysis and archiving system forJapanese SRC, which we started to study jointly with the SKA
consortium in FY 2020. A group of networked data analysis
servers was constructed and tested at NAOJ, Kumamoto
University, and Nagoya University. We also continued ourcommitment in the Australian MWA to develop methods foranalyzing and calibrating cosmic reionization observation dataand other data. On March 7–8, 2022, a data analysis workshop
for cosmic reionization, cosmic magnetism, and pulsar data
was held with the participation of a large number of young
researchers, mainly from Japan.
The MoU on the Japanese AIV commitment was signedwith the SKA Observatory, agreeing on a 1.5 FTE contribution
for 3 years starting from 2022. Based on this MoU, we areparticipating in the AIV of SKA LOW and preparing a test
plan. We have also started to discuss with SKAO the detailed
plan for SKA MID AIV participation.
We are working closely with SKA-JP. We are jointly
sharing the cost of participation in the MWA, the SK A
precursor, and preserving the right of Japanese researchers toaccess observations and achieved data at the MWA. SKA1SG
helped SK A-JP prepare the SK A-JP Engineering Book,
which outlines plans for Japanese technical participation andthe publication of the SKA-JP Science Book in an academic
journal, which was published in FY 2021. In addition, theEast Asian SKA WS was jointly held on May 26–28, 2021, to
promote collaboration and activate research activities using the
SKA and pathfinders in East Asia.
In the area of VLBI research, we have been preparing
for the development of a VLBI system in the SKA. The
preparation for the development of a VLBI system in the SKA
was carried out in cooperation with JIVE and was discussed
at global activities like an international symposium ‘VLBI in
the Era of SKA’ which was held during February 14–18, 2022.
We are also participating in discussions at the Global VLBI

030

II Status Reports of Research Activities

Consortium as a key member. We are also working with India
on preliminary VLBI observations in the SKA LOW frequency
band below 320 MHz. We succeeded in detecting fringes at
320 MHz between the Tohoku University Iitate Station and theIndian NCRA’s Ooty Station.

5. Geodesy and Geophysics
In order to monitor the position and shape of the VERA
network, regular geodetic observations were conducted 1–2
times a month. VERA internal geodetic observation sessions
using K band were conducted once or twice a month. Mizusawa
Station conducted IVS sessions (IVS-T2P and AOV) using Sand X-bands once every one or two months. In AOV and IVST2P, wideband observations using OCTAD-OCTADISK2 havebeen routinely operated. In FY 2021, VERA internal geodetic
observation was conducted 12 times and we participated in IVS
sessions 6 times. The final estimates of the station positions of
VERA were reconstructed based on ITRF2014 and supplied tothe astrometric analysis performed by VERA.
We carried out continuous GNSS (GPS) observationsat VERA stations in order to monitor short term coordinate
variations and to estimate atmospheric propagation delays.
The propagation delays (excess pass delays) vary irregularly intime. We produce essential correction data for VERA accurate
astrometry through GNSS observations. The positioning resultof GNSS at Mizusawa shows the viscosity relaxation process ofthe 2011 off the Pacific coast of Tohoku Earthquake. Mizusawa
is moving to the East-Southeast direction even though 11
years have passed since the occurrence of the earthquake. The
gravity observation at Mizusawa also shows the process ofviscosity relaxation. The gravity change observation at Ishigaki
Island, which was the joint work with the Earthquake ResearchInstitute of the University of Tokyo and the Geological Surveyof Japan, AIST, terminated in February 2022. The strain andtilt observation data obtained at the Esashi Earth Tides Station
are distributed in real time to 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 systemwith a rate of 32 Gbps for VERA in accordance with the next
EAVN broad-band observing mode. In 2021, we modified(redesigned and adjusted) the RF and IF integrated switcheswith 16 inputs and 4 outputs for dual polarizations of five bands(Q, K, C, S, L) to improve the temperature characteristics
and reinstalled them at all stations. We have also identified aproblem in the design of the input clock alignment section of
OCTAD, which had been causing a degradation in SNR sincelast year, and have corrected the problem, completing the AIVof this new observing system together with the integrated
switch. After that, as a CSV (Commissioning and Science
Verification), we conducted VLBI test observations using a RF
direct A/D system at K-band left polarization, which is one

of the features of this system and achieved agreement within
2–3 % SNR compared to the fringe results in the normal IF
band. The above results have enabled the ultra-wideband, dualpolarization observations at a rate of 16 Gbps (all stations) andin addition to that, simultaneous K and Q-band observation
using the world’s first K-band RF A/D system at Iriki station.
As a CSV, we have started some test observations in various
observing modes.
As an extension of the observable frequency band, we
improved the method of the patch antenna array synthesis of the
L-band receiver system installed in 2020. We modified and reinstalled it at Mizusawa and Ishigaki-jima Stations, measured
RFI and EMI, and examined the observable frequency range to
conduct VLBI observations.

7. Timekeeping Office Operations
The Time Keeping Office operates four cesium atomic
clocks together with a hydrogen maser atomic clock at
Mizusawa VERA Station, and sets the “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 7 million daily visits
have been recorded.

8. Public Relations (PR) and AwarenessPromotion Activities(1) Open House Events
The following open house events are held every year ateach telescope site operated by Mizusawa VLBI Observatory.
In 2021, we canceled all open house events to prevent the
spread of the novel coronavirus.
• The Open Observatory Event held by the Ibaraki University
C e nt e r for A st ronomy, a nd NAOJ M i z u s awa V LBI
Observatory, Ibaraki Station.
• The special open house event at VERA Ishigaki-jima Station
held together with “The Southern Island Star Festival.”• The special open house of VERA Iriki Station jointly heldwith “The Yaeyama Highland Star Festival.”• “Iwate Galaxy Festival” is the open house event held at NAOJ
Mizusawa Campus.
• “Star Island” is the open house event held at V ER A
Ogasawara Station.
The Southern Island Star Festival was held on January 29(Saturday) and 30 (Sunday), 2022 at the Ishigaki Civic Hall,and the VERA Ishigaki-jima Station exhibited panels anddistributed goods.
(2) Regular Public Visits
Throughout the year, the following stations are open to the
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)
7,991
The campus is regularly open to the general public with thecooperation of the Oshu Uchu Yugakukan (OSAM: Oshu
Space & Astronomy Museum) located in the campus.
b) VERA Iriki Station 1,338c) VERA Ogasawara Station 4,090d) VERA Ishigakijima Station 1,698
At Mizusawa VLBI Obser vator y, the Oshu Space &Astronomy Museum was closed from August 14, 2021 toSeptember 22, and from January 30, 2022 to February 28, toprevent the spread of the novel coronavirus infections. The
number of visitors during that period is not included. The
Kimura Hisashi Memorial Museum was closed.
(3) Cooperation with Local Communities
Various events were held in cooperation with Iwate
Prefecture and Oshu City. Here are some of the most notable
events.
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 7, 2021(Wed)-Jul 18, 2021(Sun) Hiraizumi Municipal
Library
Jul 24, 2021(Wed)-Aug 22, 2021(Sun) Kanegasaki Municipal
Library
Aug 6, 2021(Fri)-Aug 11, 2021(Wed) Tono City Library
Aug 27, 2021(Fri)-Sep 23, 2021(Thu) Ichinoseki Library of
Ichinoseki Public Libraries
Sep 1, 2021(Wed)-Sep 26, 2021(Sun) Nishiwaga Town Culture
Creation Hall (Galaxy Hall)
Nov 5, 2021(Fri)-Nov 17, 2021(Ewd) Mizusawa Library ofOshu City Libraries
Nov 27, 2021(Sat)-Dec 23, 2021(Thu) Higashiyama Library of
Ichinoseki Public Libraries
Jan 20, 2022(Thu)-Feb 2, 2022(Thu) Hanamaki Library ofHanamaki City Libraries• Lectures and Workshops
Jul 17, 2021 (Sat) Kanegasaki Municipal Library / Prof.
Honma talk event “How to walk in space”
Jul 29, 2021 (Thu) Ohta Library (Nishiwaga town) / Workshop“Let’s make a jack-in-the-box of jets that jump out of theblack hole!”
Aug 8, 2021(Sun) Tono City Library / Summer Vacation
Workshop “Let’s make a spinning top like galaxy!”Sep 22, 2021 (Wed) Kitakami District Fire Association
Nishiwaga Fire Department / 5th Townspeople culture school“Get familiar with the Universe in the Milky Way town of
Nishiwaga”
Jan 22, 2022 (Sat) Hanamaki City Culture Hall / Hanamaki

II Status Reports of Research Activities

031

Library Lecture “Forefront of black hole research”
The Iwate Marugoto Science Museum will be held under
the initiative of Iwate Prefecture. It is held every year at two
locations, in Morioka City and the coastal area, but this year it
was held online to prevent the spread of the novel coronavirus.
In 2021, we held a “Kirari
Oshu City Astronomical Class”
for elementary and junior high schools in Oshu City.
Jul 19, 2021 (Mon) Kuroishi Elementary School 5th and 6th
grade / What is a black hole?
Sep 7, 2021 (Tue) Mizusawa Minami Elementary School 5th
grade joint / What is a black hole?
Sep 13, 2021 (Mon) Ide Elementary School 6th grade / Earth,Moon, and Solar System
Sep 17, 2021 (Fri) Mizusawa Minami Elementary School 6th
grade joint / Earth, Moon, and Solar System
Oct 7, 2021 (Thu) Maesawa Junior High School 3rd grade joint/ Hayabusa2 challenge
Oct 12, 2021 (Tue) Higashimizusawa Junior High School 3rd
grade 1st to 4th joint / What is a black hole?
Nov 19, 2021 (Fri) Maesawa Elementary School 5th grade joint/ What is a black hole?
Dec 20, 2021 (Mon) Tamasato Elementary School 6th grade /Earth, Moon, and Solar System

9. Education(1) University and Post-Graduate Education
Regarding postgraduate education, Mizusawa VLBI
Obser vator y assisted 1 doctor cou rse st udent f rom
SOKENDAI, and 3 doctor and 3 master’s course graduate
students from the University of Tokyo with their research.
Three of them were from foreign countries. The SOKENDI
student got her Ph.D. degree and graduated in December 2021.
One of the students in the university got his master's degreein March 2022. In addition, staff members of Mizusawa VLBI
Observatory give lectures at the University of Tokyo, Tohoku
University, and Niigata University as visiting professors.
(2) Research Experience for High School Students
Although the educational program for high school students
in Ishigaki Island, “The Churaboshi Research Team Workshop”
with the support of JSPS, was held during summer vacationin the past, the Mizusawa VLBI Observatory organized theevent in March 2022 this time due to the serious COVID-19
situation. The event was co-organized with the Public Relations
Center of NAOJ on-site at the VERA Ishigaki-jima Station and
Ishigakijima Astronomical Observatory, while it was reduced
to two days’ sessions. Including participants from outside
Ishigaki Island, a total 9 high school students experienced thelectures on astronomy, observatory tours, and observational
studies with the VERA 20-m antenna. In order to complement
The Churaboshi Research Team Workshop, an on-line event“The VERA-Star Challenge” was held in 2022 January for the
first time, through broadcasting from Mizusawa Observatory.

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The first half of the event was aimed at junior-high school touniversity students, providing lectures and virtual tours of
VERA; and the second half was held for high school students toexperience remote observations with the VERA 20-m antenna.
There were 46 and 24 participants for the first and second halfof the event, respectively.

04. 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. Sekii for SOT and T. Watanabe, professor emeritus, forEIS) join the SSC activity. The SSC serves as a contact point
for observation proposals from world solar physics researchers
to use 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 2021 is about 60.
The Hinode science payload had been steadily observing
the Sun from space, except for the SOT filtergraph instrument
which was terminated in February 2016. Near the end of
December 2021, an anomaly occurred in the attitude control
around the Sun-directed axis, and the satellite entered a safehold state leading to the suspension of observations. The
attitude around the Sun-directed axis had been controlled by
the star tracker, but we established an operational procedure tocontrol the attitude using a geomagnetic sensor and gyro andwere able to resume normal observations from the beginning ofMarch 2022.
ISAS/JA X A approved the four th mission extension
for the period from FY 2021 to FY 2023. The scientificmotivation in the coming period is to continuously observerising activity toward the solar maximum using techniquessuch as observations of magnetic fields in the polar regions
and full-disk mosaic observations, as well as to promote joint
observations with rocket and balloon experiments conductedby the SOL project and with inner heliosphere observations by
new satellites such as Solar Orbiter. Another aim is to conductcollaborative observations with DKIST, a large aperture
ground-based telescope described below.
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 maintainedsuch as a flare catalog, model of magnetic fields above active
regions, and magnetic field data in the solar polar regions. Joint
research is ongoing for a comparative study between radiative
magnetohydrodynamic numerical simulations and Hinodeobservations.

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, and 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.
The observation data are available at a data analysis
server of ADC and on the web page of the SOL project. The
data storage server is continuously upgraded to accommodate
the increasing amount of data. In FY 2021, we replaced a

II Status Reports of Research Activities033

file server and prepared the data format for accommodating
data retrieval from outside as part of the promotion of data
use. Some of the most advanced data accumulated are thosefor magnetic field. The magnetic field observations that wereconducted with SFT starting from 1992 have provided vector
magnetic fields in the photosphere with a field of view covering
active regions by observing an absorption line in the visible
wavelength range. These observations have now been replacedwith near-infrared Stokes polarimetric observations since 2010
for higher precision measurements of magnetic fields both in
the photosphere and in the chromosphere. NAOJ has long-term
solar observation data in the form of films, photographic plates,and sketches acquired since the time of its predecessor, theTokyo Astronomical Observatory. The data are being digitizedfor the study of long-term variations in solar activity. The
sunspot observations that started in 1929 continue, although
they were upgraded to imaging observation using a digital
camera in 1998.
In addition, the SOL project continues to observe total
solar eclipses and has recently achieved success in polarimetricmea su re me nt s of t he corona . We a re developi ng key
technologies required in future solar observing instruments,
such as an infrared camera with an H2RG detector.

3. Nobeyama Solar Radio Polarimeters
The Nobeyama Radio Polarimeters (NoR P) monitor
the microwave radiation from the Sun, especially 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). Before the increase in solar activity, the 35 and 80
GHz antennas, which had previously suspended observations
due to problems caused by a gear failure, were repaired, andobservations at all the frequencies were able to resume in
October 2021. Since then, stable observations have been made,and we have succeeded in acquiring 1-80 GHz microwave
spectra during several solar flares that occurred in April 2022.

4. Rocket and Balloon Experiments
The SOL project is working to carry out the development ofadvanced technology for next-generation solar observations bysounding-rocket and stratospheric balloon experiments.
The CLASP ser ies of sounding rocket exper iments
aim to measure solar magnetic fields in the chromosphereand transition region through high-precision polarization
obser vations in the ultraviolet wavelengths. Following
CLASP2 (flight in 2019, the world’s first successful polarization

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spectroscopic observation of ionized magnesium lines [Mg II
h&k lines, wavelength 280 nm]), the CLASP2 re-flight project(CLASP2.1, Japanese PI: Ishikawa) was led by the SOL project.
Preparations were made with the cooperation of the Advanced
Technology Center (ATC), and after a month and a half oflaunch-site testing at the White Sands Missile Range in the
United States, CLASP2.1 was launched on October 8, 2021
(local time). Slit-scan observations of an active region weresuccessfully made for about 6 minutes, and polarized spectraof the Mg II h&k lines induced by the Zeeman effect wereobtained with high quality. By applying the method constructedby Ishikawa et al. (2021) to these data and combining them with
the Hinode satellite data obtained jointly with CLASP2.1, we
expect to be able to reveal the three-dimensional (two spatial
dimensions plus height) structure of the magnetic field fromthe photosphere to the upper chromosphere. Currently, datacalibration is underway in cooperation with the US team.
SUNRISE-3 is the third flight of the international balloon
project Sunrise, in which Germany, Japan, the United States,
and Spain are participating, and is scheduled to f ly in thesummer of 2022. The SOL project is in charge of the nearinfrared spectro-polarimeter SCIP (Japanese PI: Katsukawa),
which will be installed on the 1-meter aperture telescope of
SUNRISE-3 and will simultaneously observe many spectral
lines with a resolution higher than that of the Hinode satellite.
These obser vations will allow us to obser ve the threedimensional magnetic field structure and its time evolution
from the photosphere to the chromosphere and clarify thetransport and dissipation processes of magnetic energies. In
cooperation with the ATC and ISAS/JAXA, the SCIP opticalunit has been developed to achieve high imaging, spectral, andpolarization performance. After the completion of assemblyand performance evaluation in air, we confirmed the optical
performance and thermal control of the instrument under
the low pressure and thermal environment expected duringballoon flight using a large vacuum chamber at ATC. After thecompletion of the development at NAOJ, SCIP was shippedto Germany in August 2021, where it was integrated into the
1-meter telescope. We conducted verification and calibration of
combined performance with other instruments, and evaluationof performance with natural sunlight. The final test at theballoon launch site in Kiruna, Sweden, has been underway
since April 2022. We are preparing refereed papers on thetechnology development for high-precision spectro-polarimetry
as well as opto-mechanical design and analysis obtained
through the development of SCIP. Methods for analyzing highprecision polarimetric data of the chromosphere are studied
through international collaboration, which is beneficial not
only for the SUNRISE-3 balloon observations but also forobservations with the large solar telescope DKIST.
The Focusing Optics X-ray Solar Imager (FOXSI) is a
joint Japan-US sounding rocket experiment 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; FOXSI-1 and FOXSI-2 (launchedin 2012 and 2014) made focusing X-ray imaging spectroscopic
observations in the hard X-ray band (5 keV to 15 keV), and
FOXSI-3 (launched in 2018) succeeded in imaging spectroscopy
observations in the soft X-ray band (0.5 keV to 5 keV). The
fourth flight, FOXSI-4, aiming to observe solar flares, wasproposed to NASA and was approved with the highest rank
in 2019. In 2021, the budget for FOXSI-4 was adopted by
the ISAS/JAXA small-scale program and the Grant-in-Aid
for Scientific Research, International Cooperative Research
Acceleration Fund (B) (Japanse PI: Narukage). FOXSI-4 isscheduled for launch in 2024 and aims to understand plasma
heating, energy transport, and particle acceleration in a solar
flare. The Japanese group led by the project is developing key
components such as a high-speed camera for X-rays, a highprecision X-ray mirror, a pre-collimator, and an X-ray filter.
These developments are being carried out in collaboration with
the ATC and the CMOS camera team of the Subaru Telescope.
The team is also working on the data calibration of the last
three FOXSI experiments as well as on the creation of scientificresults.

5. Cooperation with SOLAR-C Project
To refine the observation plan for Solar-C (EUVST), weare running research on how the key processes of atmosphericheating are observed spectroscopically using numericalsimulations in the framework of the Hinode Science Center,
which is jointly operated with Nagoya University. The researchis being conducted not only in the visible and near-infrared
spectra targeted by SUNRISE-3 balloon observations but
also in the ultraviolet spectra to be observed by CLASP and
Solar-C. The SOL project contributes to realizing Solar-C,
especially in the development of critical technologies, basedon the technical assets accumulated through the rocket andballoon experiments.

6. Education
The SOL project accepted and supervised three Ph.D.
students from SOKENDAI and three contract graduate students
from the University of Tokyo. One received a Ph.D. degree at
SOKENDAI. One undergraduate student was accepted into asummer student program of SOKENDAI and was supervised
online. The SOL project participated in the Tour of Solar
Research Frontiers (March 2022, online) 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 scientific researchof the Sun to the public: web releases, homepage, social
media, cooperation for exhibitions at science museums, media
appearances in response to requests for media interviews, andproviding materials to the media, etc.

8. Science and Community Meetings
The international Hinode Science Meetings have been
regularly held to advance the solar physics research with
the Hinode satellite. The 14th Hinode Science Meeting
was originally scheduled in 2020 but was postponed due to
COVID-19 and held in October 2021. A meeting of the Hinode
Science Working Group was held online on October 29, 2021,
to discuss ways to continuously generate scientific resultsfrom Hinode and to share the status of mission extension inparticipating countries. The Japan Solar Physics Community
Symposium was held online on February 14–15, 2022, where
the latest research results from domestic instruments andforeign space- and ground-based observations were presented,
and future plans for Solar-C and beyond were introduced anddiscussed.

9. Others
The Daniel K. Inouye Solar Telescope (DK IST) on
Haleakala in Hawai`i, a 4-meter aperture solar telescope ledby the US, obtained its first-light images in January 2020. One
member of SOL (Y. Katsukawa) is a member of the Science
Working Group and helped to develop the Critical Science Planfor the initial observations of DKIST, which was published asa paper. In the first call for observation proposals for DKIST(Operation Commissioning Phase 1, OCP1) issued in 2020, fiveproposals submitted by Japanese researchers were accepted.
The observations of OCP1 were delayed by COVID-19 but
began in February 2022. Based on a grant for enhancing
collaborative research with DKIST (co-I: M. Kubo), we areconducting numerical simulation studies until we obtain
DKIST observation data. A study for the next-generation focal
plane instrument for DKIST has begun in cooperation with
Kyoto University. For the European Solar Telescope (EST, 4m) the SOL project is participating in the SOLARNET project(January 2019 to December 2022) of the European solar
community to develop a prototype IFU (Integral Field Unit) for
the EST-prototype GREGOR solar telescope. An image slicer
unit for the IFU was designed and fabricated with a Grantin-Aid for Scientific Research. 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 tocooperate with NSO for its realization based on the scientificand technological heritage obtained through near-infrared
spectro-polarimetry with SFT at Mitaka Campus.
The 10 cm coronagraph from the former Norikura Corona
Obser vator y has been relocated to Yunnan, China, anddiscussions have started to move the new coronagraph (10 cm
aperture) from the former Norikura Corona Observatory to
Peru. The University of Ica, Peru, has instruments for solar
observations that were jointly developed by SOL and Kyoto
University, and we will resume our cooperation to use themfor education and research after the COVID-19 pandemic has
ended.

II Status Reports of Research Activities035

05. 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. This fiscal year marks the10th anniversary of ALMA observations. This report describes
the progress of the ALMA project, which includes the resultsof the open-use scientific observations and public outreachactivities.
The ASTE telescope is a single-dish 10-m submillimeter (aradio wave with a wavelength of 1 mm or less) telescope locatedat Pampa la Bola in the Atacama highlands where ALMA is
also located. It has been operated in the Southern Hemisphereto make headway into submillimeter astronomy that explores
the spectrum invisible to the human eye, providing various
possibilities and future prospects for research and developmentof ALMA. This report describes the progress of 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 ProjectDue to the outbreak of the novel coronavirus (COVID-19)

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in Chile, ALMA temporarily closed the Array Operations Site
(AOS) and Operations Support Facility (OSF) on March 22,
2020. After one year of careful monitoring, planning, andreturn to operation efforts, scientific observations resumed
as best-effort on March 17, 2021. The support on site by theEngineering team was critical in the recovery of Atacama
Compact Array (ACA) antennas. About 75 % of the originallyoffered 12 m array time was completed by the end of Cycle 7 (endof September 2021). Cycle 8 observations started on October 1,
2021. The ALMA Management Team made important progressin the definition of the framework to upgrade the bandwidth of
ALMA receivers by at least a factor of 2 (goal: a factor of 4)
and upgrade the associated electronics, such as the correlatorsand data transmission system. In terms of development of new
instrumentation, the Band 1 receivers, covering the frequency
range between 35 and 50 GHz, were installed for the first timein the ALMA antennas and successfully achieved their first lightin August 2021. After a successful internal ALMA review inDecember 2021, it was decided that 3D printed horns fabricatedat NAOJ would be integrated into the final Band 1 receivers.
On February 22, 2022, the newly developed spectrometerfor the Total Power Array successfully acquired its first radio
spectra towards Orion KL. As the ALMA system hardware andsoftware ages, efforts have been devoted in the preparation of
a comprehensive obsolescence and aging management plan
towards sustainable operations. The publication rate slowed
down in 2020 possibly due to the pandemic, but it has recoveredin 2021 and recorded the highest number of ALMA publications
in a single year.

2. ALMA Open-Use and Scientific Observations
The 9th round of ALMA open-use observations commencedin October 2021 as Cycle 8. A total of 1,735 proposals were
submitted for Cycle 8. The total required observation hours for
all proposals was the most every requested in a single cycle.
The main capabilities of Cycle 8 include: interferometricobservations using at least forty-three 12-m antennas; ACA
observations (interferometric observation with at least ten 7-m
antennas and single-dish observation with at least three 12-m
antennas); eight frequency bands (Bands 3, 4, 5, 6, 7, 8, 9 and
10); and maximum baselines of 8.5 km. From Cycle 8, Band
5 is available for solar observations, and Bands 9 and 10 are
available for stand-alone 7-m Array observations. In addition tothese, Cycle 8 provides spectral scan observations with the 7-m
Array, mosaicking of continuum linear polarization observations
in Bands 3 to 7 with the 12-m Array, and new VLBI observation
modes.
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.
Dr. Xing Lu (NAOJ) used ALMA Band 6 to observe theCentral Molecular Zone (CMZ) of our Milky Way. The 2000
au resolution observations identified 834 dense cores and 43
protostellar outflows associated with the cores. However, theyfound no significant evidence of outflow for the remaining 800
or so cores. The outflow is unambiguous evidence of ongoingstar formation. Therefore, the ubiquitous presence of the dense
cores without outflow may suggest that these clouds in the CMZ
are at a very early phase of star formation, and there can be a
future burst of star formation, despite the harsh conditions withstrong tidal force, magnetic field, high energy particles, andfrequent supernova explosions.
S O K E N D A I g r a d u a t e s t u d e n t Ta k a f u m i Ts u k u i(SOKENDAI/NAOJ) and NAOJ Professor Dr. Satoru Iguchi
investigated the archival ALMA Band 7 data of a z = 4.4 galaxy
called BRI 1335-0417, finding convincing evidence of spiralstructure in a galaxy which is located only 1.4 billion years
after the Big Bang. The [CII] distribution and kinematics show
evidence of a rising rotation curve toward the galactic center,suggesting a central mass distribution which could be explainedby the presence of a galactic bulge. The Toomre Q parameter
provides evidence of an extended dynamically cold outer disk,suggesting large-scale cosmological inflow or minor mergers as
possible mechanisms to explain the spiral structure.
A team led by Dr. Takuma Izumi (NAOJ/SOKENDAI)
observed the redshifted [CII] line in a z = 7.07 quasar
J1243+0100 using ALMA. This is the only low-luminosity
quasar at z > 7 known to date, and it offers an exciting possibility
to study the detailed gas dynamics when the Universe was lessthan a billion years old. They find that the gas dynamics in thecentral region are dominated by rotation, with a possibility toform a compact bulge with a mass of ~3×1010 Msun. In addition,
the presence of broad wings of ~1000 km/s suggests a stronggalactic-scale quasar-driven outflow that will likely quench thestar formation activity in the host galaxy within a relatively short
time.
Drs. Hiroshi Nagai (NAOJ/SOKENDAI) and Nozomu
Kawakatsu (Kure College) used data from ALMA and VLBI toinvestigate the physical conditions of the central region of NGC
1275, a galaxy 70 Mpc away that harbors an active galactic
nucleus. Their analysis found solid evidence of the coexistenceof supernovae explosions (traced by synchrotron radiation)and the circumnuclear molecular disk (traced by CO), whichsuggests that star formation can occur in the circumnuclear
disk. They further indicate that the supernova explosions canefficiently remove the angular momentum of the rotating gas,
accelerating the mass accretion process to the central AGN.
A team led by Dr. Patricio Sanhueza (NAOJ) used 700
au resolution ALMA data of IRAS 18089-1732, a high-massstar-forming region in the Milky Way Galaxy, finding a wellorganized magnetic field that resembles a spiral “whirlpool”.
Their analysis of the energy balance suggests that gravity inthis system overwhelms all other physical mechanisms such as
turbulence, rotation, and magnetic field. The minor contributionof the magnetic field caught them by surprise since previous
studies found evidence of a strong magnetic field in a similarstar-forming environment. This work suggests that high-massstar formation can occur in weakly magnetized environments,
with gravity taking the dominant role.
A team led by Dr. Takanori Ichikawa (a former graduate
student at Kagoshima University) and Dr. Shigehisa Takakuwa(Kagoshima University), used ALMA archival data to analyzea Class II binary system XZ Tau at Bands 3, 4, and 6. They
found that the CO emission associated with the circum-stellar
disk is consistent with Keplerian rotation, and that the rotationalaxes are misaligned with each other. From the multi-epoch
ALMA data, they have identified the relative orbital motion of
the binary, leading to the conclusion that the two disks and theorbital plane of the XZ Tau system are all misaligned with eachother.
An international team led by Gianni Cataldi (Universityof Tokyo/NAOJ) and Dr. Yuri Aikawa (University of Tokyo)
analyzed DCN/HCN and N 2D +/N 2H + column density ratios
toward five protoplanetary disks observed by the “Moleculeswith ALMA at Planet-forming scales (MAPS)” Large Program.
They found that the DCN/HCN varies considerably for different
parts of the disks, ranging from 10−3 to 10−1. The inner-disk
regions generally show significantly lower HCN deuterationcompared with the outer disk. In addition, they found N2D+ in
the cold outer regions beyond ~50 au from the central star, andN2D+/N2H+ ranges between 10−2 and 1 across the disk sample.
This finding is consistent with the theoretical models which
predicts that N2H+ deuteration proceeds via the low-temperaturechannel only.
A team lead by Dr. Takashi Shimonishi (Niigata University)used ALMA to observe a star forming region in the outer galaxy
called WB89-789, detecting a variety of species that containcarbon, oxygen, nitrogen, sulfur, and silicon. Their detection
includes complex organic molecules and deuterated species.
For the first time, they detected a hot molecular core in theouter galaxy, which is known as an excellent laboratory to study
star formation in a low-metallicity environment. The ALMA
observations reveal that various kinds of complex organic
molecules, such as methanol (CH3OH), ethanol (C 2H 5OH),
methyl formate (HCOOCH 3 ), dimethyl ether (CH 3 OCH 3 ),formamide (NH 2CHO), propanenitrile (C 2H 5CN), etc., arepresent even in the primordial environment of the extreme outer
Galaxy. From their detailed comparison between the inner andouter disk, they conclude that organic molecules form withsimilar efficiency even at the edge of our Galaxy, where theenvironment is very different from the solar neighborhood.

3. Educational Activities and Internships
The NAOJ ALMA Project continues to collaborate with
the Joint ALMA Observatory to create and maintain a Japaneseversion of “ALMA Kids,” a website for children, with the aimof providing opportunities for more people to learn about themechanism of the ALMA telescope 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. In addition, the Project has developed
educational content, mainly targeting elementary school

II Status Reports of Research Activities037

students, called “Why ALMA Workshop” which explains thebasics of radio astronomy by combining videos and worksheets.
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. Three new posters were released in FY 2021.
In addition, the Project now provides short anime (“manga”)
explaining the basics of radio astronomy and interferometry. All
posters and manga are available on the NAOJ ALMA website.
The NAOJ ALMA Project initiated the radio astronomy/
interferometry summer school for university students with
SOKENDAI, which was organized and held on September 16,
17, 21, 22, 24 in 2021 in collaboration with Nobeyama Radio
Observatory, Mizusawa VLBI Observatory, and the ALMA
and VLBI Science Advisory Committees. Of the total 185
participants, 65 were undergraduates, 93 were graduate students,
12 were faculty, and 2 were high school students.

4. Public Outreach Activities
In FY 2021, ALMA scientific observation results werecovered by 75 newspaper/journal articles, and the ALMA
telescope was featured by two television/radio programs. The
NAOJ ALMA website posted 38 news articles and 11 press
releases. Mailing-list-based newsletters have been issued on amonthly basis with approximately 2,200 subscribers. Day-to-day
information is posted in a timely manner on Twitter (@ALMA_
Japan) with nearly 64,300 followers as of the end of FY 2021.
In FY 2021, 14 lectures were given for the general public
and most of them were held online to prevent the spread of
COVID-19 infections. In May-June 2021, the NAOJ ALMA
Project exhibited a booth for the ALMA telescope at theJapan Geoscience Union Meeting (held online). Six new
short educational movies (“Why ALMA?”) were released on
YouTube. In June and July, the NAOJ ALMA Project hosted
special Twitter and online events related to Tanabata. The main
lectures at the NAOJ open house held online in October were
given by NAOJ ALMA Project Manager Alvaro Gonzalez andthe head of the ALMA Department of Engineering Norikazu
Mizuno. In December 2021 – January 2022, a special ALMA
exhibition was held at the Mitaka Information Space ofAstronomy and Science. A webpage dedicated to promoting the
10 year anniversary of ALMA was launched in March 2022.
This website highlights a subset of the key scientific results
achieved over the past 10 years as well as the development
activities of new instruments and components for the future of
ALMA. The website also features interviews with artists. Three
new science promotion movies “Progress in Planet Formation
Research”, “Seeds of Life: Exploration of Organic Molecules”,
and “Tracing Back the History of the Universe” were released
to celebrate the 10-year anniversary. The NAOJ ALMA Projectcontinues to release quarterly online newsletters for scientists.
From mid-March 2015, ALMA began accepting public
visitors to the ALMA Operations Support Facility (OSF) at analtitude of 2,900 meters, but due to the outbreak of COVID-19
in Chile, it stopped accepting public visits in March 2020. As of038

II Status Reports of Research Activities

the end of FY 2021, public visits remain suspended.

5. International Collaboration (Committees, etc.)
For the international ALMA project, meetings are held
frequently by various committees. In FY 2021, all face-toface meetings were replaced by online meetings, affected by
the COVID-19 pandemic. The ALMA Board and the ALMA
Scientific Advisory Committee (ASAC) held online meetings
when necessary, while the ALMA East Asian Science Advisory
Committee (EASAC) held online meetings twice. Meetings
were held more frequently by groups in charge of specific tasks
to implement the international project in close cooperation.

6. Workshops• June 15–16, 2021: ALMA Data reduction tutorial (introductory
level), held with the Astronomy Data Center, held online• Jul. 15–16, 2021: ngVLA Development Days 2021 held online• Nov. 1 and 2: Cold outflows near and far: crossroad of ourcurrent understandings held online• Nov. 2 and 5, 2021: ALMA Data reduction tutorial(intermediate level), held with the Astronomy Data Center,
held online• Nov. 30–Dec 1, 2021: Linking the Science of Large
Interferometers in the 2030s held online• Dec. 6 and 13, 2021: ALMA Grant Fellow Symposium held
online• Dec. 14, 16, and 21, 2021: ALMA/45m/ASTE Users Meeting
2021 held online• Dec. 20 and 22, 2021: Millimeter/submillimeter VLBI scienceswith ALMA• Jan. 18–21, 2022: East Asian ALMA Science Workshop 2022
held online• Mar. 9–10, 2022: East Asian ALMA Development Workshop
2022 held online• Mar. 29–30, 2022: ALMA Cycle 9 Proposal Preparation
Meeting held online

7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research, including
Industry–University Collaboration Expenses• Yusuke Miyamoto: funded by the National Institutes of Natural
Sciences (NINS) research support project (Interdisciplinary
Research by Young Researchers Project)

8. Changes in Project Researchers(1) Hired• Yu Cheng: Project Researcher• Tomonari Michiyama: Project Researcher (secondment toOsaka University)• Toshiki Saito: Project Researcher (secondment to Nihon
University)• Hiddo Algera: Project Researcher (secondment to Hiroshima

University)• Mitsuyoshi Yamagishi: Project Researcher (secondment toUniversity of Tokyo)(2) Departed or transferred• Toshiki Saito: Project Researcher• Mitsuyoshi Yamagishi: Project Researcher• Sarolta Zahorecz: Project Researcher• Kazuki Tokuda: Project Researcher• Yuri Nishimura: Project Researcher• Kohei Kurahara: Project Researcher• Tomoko Suzuki: Project Researcher• Seokho Lee: Project Researcher• Shigeki Inoue: Project Researcher• Yang Yi: Project Researcher

errors, and it was confirmed that the newly deployed instruments
and their control software basically work as designed. The Band
10 receiver (787–950 GHz band) developed with Grants-inAid for Scientific Research also continued to be evaluated. We
continued performance evaluation and data reduction of thereceiver using data taken in FY 2019. The resultant images ofdemo science data obtained toward Orion KL with [CI](3P2-3P1)
and CO(J = 7–6) were released to the public.
In FY 2021, four peer-reviewed papers were published,including two papers written by domestic researchers (outside
NAOJ) and one by overseas researchers. The decrease in
the number of papers published was unavoidable due to thesuspension of scientific observations due to the COVID-19
pandemic between FY 2020 and FY 2021.

9. Main Visitors• Apr. 12, 2021
Hinako Takahashi, Vice Minister of Education, Culture,
Sports, Science and Technology (MEXT) visited NAOJ Mitaka
Campus

10. Progress of the ASTE Telescope
In FY 2021, the ASTE telescope operation started inlate May, which was about a month behind schedule due tothe continuing outbreak of COVID-19 that began to spreadworldwide from February 2020. However, the telescope
operation was suspended by heavy snowfall shortly after thestart, and furthermore, hardware failures occurred at the driving
mechanism of the sub-reflector during the snowfall. A close
investigation into the sub-reflector was prevented by bad weather
conditions of weekly snowfall and strong wind, and a manlift
malfunction caused by low temperature, and we could not
expect to allocate appropriate time slots to the open-use program
observations planned in FY 2021. Thus, we cancelled all the
open-use program observations. The investigation was finallydone in October, and based on it, a possibly malfunctioning
motor for the driving mechanism was replaced in March 2022.
However, the sub-reflector is still out of commission due todifferent hardware alarms. Its recovery work will continue in FY
2022.
As for new observation instruments, two development
projects were carried out with Grants-in-Aid for Scientific
Research: (1) the development of a wide intermediate-frequency
bandwidth for the Band 8 (385–500 GHz band) receiver, and(2) the development of a new spectrometer together with afrequency converter that converts the receiver signal for the
spectrometer. The Band 8 receiver, the new spectrometer,
and the frequency converter were assembled and evaluatedin Mitaka. Then, they were shipped to the ASTE site andsuccessfully installed in the telescope on schedule between
November and December. The Commissioning and Science
Verification was not available due to the sub-reflector problem
mentioned above, but test observations using them ran without

II Status Reports of Research Activities039

06. 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, the specialpurpose computer for gravitational many-body problems/
general-purpose graphic processing units (GPGPU), and ageneral-purpose PC cluster for small-scale calculations, carryingout research and development for computational astrophysics,
and performing astronomical research with simulations. The
new main 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. This fiscal year, CfCA discontinued operation of
GRAPE-DR and GRAPE-9 dedicated to gravitational manybody problems, and augmented the GPGPU and generalpurpose PC cluster. Efforts in visualizing astronomical data also
continue.

2. Open Use of Computers(1) General status
This year marked the fourth year of the upgradedastronomical simulation system, which includes the new openuse supercomputer Cray XC50. This computer is installed andunder operation at Mizusawa VLBI Observatory. The users havebeen 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: aseries of dedicated computers for gravitational N-body problems(known as GRAPE’s) together with several GPU nodes; PCclusters for small to medium-scale computation; large-scale
file servers; a group of servers for processing computational
output data; and an instrument network to encompass the overall
computer system. These components are central to numericalsimulations by researchers in Japan and overseas.
Computational resources of the XC50, GRAPE’s including
GPU, and smaller PC clusters are allocated in accordance witha formal review process. The statistics of applications andapprovals for this year are listed in the next subsection. Ourcenter conducted a survey on the number of peer-reviewed
papers published in English in this fiscal year on studies thatinvolved the project's open-use computers. It turned out that 150
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

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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
Cray XC50● Operating hours
Annual operating hours: 8639.8
Annual core operation ratio by users' PBS jobs: 93.43 %● Number of users
Category S: 0 adopted in the first term, 0 in the second term;
total 0Category A: 13 adopted at the beginning of the year, 0 in thesecond term; total 13
Category B+: 20 adopted at the beginning of the year, 2 in thesecond term; total 22
Category B: 127 adopted at the beginning of the year, 9 in thesecond term; total 136
Category MD: 34 adopted at the beginning of the year, 6 in thesecond term; total 40
Category Trial: 41 (year total)
GRAPE/GPU system● Number of users
18 (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: 547,026
Annual core operation ratio by users’ PBS jobs: 98% (aballpark figure)● Number of users
62 (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 11 - July 9, 2021
7 attendees● Cray XC50 workshop for novice users (zoom)
Introduction to the basic usage of XC50 for novice users
September 29, 2020
13 attendees

● Cray XC50 workshop for intermediate users (zoom)
Introduction to debugging, performance analysis, andoptimization of XC50 for intermediate users
September 30, 2020
15 attendees● CfCA Users’ Meeting (zoom + Slack)
Presentation of research results using the open-use facilities
in this department, and discussion of the operation of theequipment
January 19–20, 2021
95 attendees (January 19), 70 attendees (January 20)● Early spring school for N-body numerical simulations (zoom+ Slack)
Lectures on N-body simulations, and programming practiceusing GPU and GRAPE-Library
February 14–17, 2022
16 attendees (for hands-on training and lectures), 2 attendees(for lectures only)● GPU Workshop (zoom + Slack)
Lectures on CUDA programming basics and optimization
technics for CUDA programming
February 28, 2022
45 attendees● Numerical simulation school for hydrodynamics (zoom +Slack)
Lecture and practice for MHD numerical simulations using the
public code Athena++
March 10–12 and 22–23, 2021
65 attendees

3. PR Activity
In FY 2021, the following press releases were issued fromthe center:● “Telescopes Unite in Unprecedented Observations of FamousBlack Hole”
April 14, 2021, Event Horizon Telescope Science MultiWavelength Science Working Group et al.
● “A New Window to See Hidden Side of the Magnetized
Universe”
May 6, 2021, Takumi Ohmura (The University of Tokyo),
Mami Machida (NAOJ/CfCA) et al.
● “Observation, Simulation, and AI Join Forces to Reveal a
Clear Universe”
July 2, 2021, Masato Shirasaki (NAOJ/the Institute of
Statistical Mathematics)● “Largest Virtual Universe Free for Anyone to Explore”
September 10, 2021, Tomoaki Ishiyama (Chiba University)● “Simulations Provide Clue to Missing Planets Mystery”
November 13, 2021, Kazuhiro Kanagawa (Ibaraki University)
et al.
● “Stellar ‘Ashfall’ Could Help Distant Planets Grow”
December 14, 2021, Yusuke Tsukamoto (Kagoshima
University)
In addition, the following research results and news
appeared on the CfCA website:● “A New Type of Supernova Illuminates an Old Mystery”
June 29, 2021, Takashi Moriya, Nozomu Tominaga (NAOJ/
CfCA)● “Assistant Professor Akimasa Kataoka wins the JSPS
Outstanding Young Scientist Award 2020”
October 29, 2021, Akimasa Kataoka (NAOJ/CfCA)
In December 2021, “Galileo X” (produced by WAC
Corporation) broadcast on BS Fuji featured a Japanesepress release entitled “World’s Largest ‘Simulated Universe’
Unveiled,” which reported on the role of ATERUI II in Japanese
astronomy and the current state of astronomical research using
simulations.
During the Mitaka Open House Day 2021 held online on
October 23, 2021, a video and an interview with CfCA staff
members were made available on the CfCA website. The movie
features CfCA staff introducing the group of computers operated
by the Mitaka CfCA Computer Room, and explains the roleof each computer and the activities of CfCA. In addition to
the Japanese version shown at the event, an English subtitledversion was also created to communicate CfCA's activities to awider audience. Interview articles were created and published
as content to introduce the activities of CfCA and familiarize
people with the staff members by introducing their daily workand personal backgrounds, focusing on individual staff members
who cannot be introduced at the annual Mitaka Open HouseDay.
A Twitter account @CfCA_NAOJ and YouTube channel
have been operated to provide the information on CfCA.

4. 4D2U ProjectIn FY 2021, the 4D2U project continued to develop andprovide movie content and software.
The visualization of simulations was mainly the productionof images and videos published in the CfCA press releases.
In May 2021, “A New Window to See Hidden Side of theMagnetized Universe” (Simulation: Takumi Ohmura/The
University of Tokyo, Visualization: Hirotaka Nakayama/4D2U),
and in September 2021, “Largest Virtual Universe Free forAnyone to Explore” (Simulation: Tomoaki Ishiyama/Chiba
University, Visualization: Hirotaka Nakayama/4D2U) werereleased in image and movie format as visual materials of press
releases.
Version 1.7.0 of the four-dimensional digital universe
viewer “Mitaka” was released in June 2021, and upgradedto version 1.7.2 by January 2022. These versions can now
display asterisms such as the Summer Triangle, display in theequirectangular cylinder method, and display interstellar objects.
Online workshops on how to use the latest version of Mitaka
were held by the Mitaka Working Group of the Japan Society for
the Promotion of Astronomy Education in May 2021.
4D2U content was provided both domestically andinternationally for TV programs, planetarium programs, lecture
presentations, books, and so on. In February and March 2022,
NHK educational TV broadcasted “Space Taxi” (produced byPlanet film), a comedy program about space travel using Mitaka

II Status Reports of Research Activities041

and 4D2U video contents.
For the 2021 Mitaka Open House Day, 4D2U staff andresearchers produced a video explaining the contents and madeit available on the CfCA website. In the introduction of the video
content “Chariklo’s Double Rings,” Shugo Michikoshi (Kyoto
Women’s University), who performed the simulation, introduces
his research and explains the video, and Hirotaka Nakayama(NAOJ/4D2U), who performed the visualization, gives a behindthe-scenes introduction of the video production. In the Mitaka
introductory video, “A ‘special’ space tour by the developer,”developer Tsunehiko Kato (NAOJ/4D2U) gives a demonstrationof Mitaka and introduces some of its highlights.
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
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

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Machida and Tomoya Takiwaki conducted research on “blackhole accretion disks and relativistic jets,” and “Elucidation of
the mechanism of 3D supernova explosions by first-principles
calculations of neutrino radiation transport” using a mesh-type
fluid code, respectivelty. These four projects are still in theprocess of tuning the code in preparation for the large scale run
at Fugaku. In addition, the budget was mainly used to increase
the storage capacity in order to store the huge amount of datathat will be generated in future large-scale calculations.
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
Associate Professor: Takiwaki, Tomoya
Project Research Staff: Matsumoto, Yuji
Research Supporter: Ideguchi, Shinsuke(2) Staff members who departed in this FY
Project Research Staff: Ishikawa, Shogo
Research Supporter: Ban, Makiko

07. Gravitational Wave Science ProjectIn FY 2021, the updated event catalog GWTC-2.1 for the
first half of the 3rd international gravitational wave observations(O3) (April 1 – October 1, 2019) and the second half (November
1, 2019 – March 27, 2022) event catalog GWTC-3 werereleased. In total, 90 gravitational wave events have beenreported to date. In addition, the results of joint observations
made by KAGRA and GEO600 in Germany in April 2020 werereleased. Thus, gravitational wave astronomy is making steadyprogress.
The NAOJ Gravitational Wave Science Project (GWSP)
is leading gravitational wave research in Japan by promoting
gravitational wave observations using KAGRA, and thedevelopment of advanced gravitational wave detector technology
using TAMA300 at Mitaka Campus.

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” with the Institute for
Cosmic Ray Research of the University of Tokyo and the HighEnergy Accelerator Research Organization. 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 manymembers for the Executive Office, System Engineering Office,etc.
In FY 2021, KAGRA equipment was refurbished in
preparation for the 4th international gravitational wave
observations (O4, scheduled to begin mid-December 2022).
Specifically, the following has been carried out.
(1) Vibration Isolation Systems
A total of 19 vibration isolators of 4 types (Type-A, Type-B,
Type-Bp, and Type-C) were retrofitted; problems found in O3
were corrected and new high-sensitivity accelerometers wereintroduced. Operational testing of all the vibration isolators is
ongoing.
(2) Auxiliary Optics
In conjunction with the laser-axis adjustment, installationof mid-size optical baffles has begun in the vacuum chambersof the central laboratory to prevent stray light. These are being
implemented in cooperation with the Advanced Technology
Center (ATC).
(3) Main Interferometer
The Output Mode Cleaner was taken out of KAGRA
and improved in a clean booth at Mitaka ATC, and will bereinstalled in 2022. The GWSP also played a central role in thereconstruction of the main interferometer.

(4) Mirror Evaluation
To replace the two KAGRA input-test-mass mirrors(ITMs) with higher performance ones before the start of O5,
ITM specifications were formulated, test polishing was done,
and sapphire mirror base materials were evaluated in order. In
particular, we found a correlation between the optical absorption
and birefringence distributions, which paved the way for theselection of a high-performance mirror substrate. In addition, theY-end mirror that was contaminated was cleaned and reinstalled.
These activities were conducted at the TAMA300 and ATClaboratories in Mitaka Campus.
(5) Others
An environmental monitoring system was developed byinstalling various sensors in KAGRA. These sensors detectedvarious signals from a large volcanic eruption in Tonga, andthe results were published in the press. The noise reduction
for PCAL, a photon-pressure calibrator for gravitaional wave
signals, was successfully achieved, and preparations were madefor signal calibration during O4. The GWSP also contributed
to the reinstallation of KAGRA’s cryogenic mirror suspension
system.
The above renovation work is scheduled to continue throughFY 2022.

2. R&D in TAMA300 and ATC
The TAMA300, a first-generation interferometricgravitational wave antenna constructed in the 1990s, is being
effectively utilized to develop next-generation gravitational
wave telescope technology. In addition, table-top technology
development and assembly of KAGRA instruments are also
being conducted at the ATC laboratory.
(1) Development of frequency-dependent squeezing
technology in TAMA300
In TAMA300, developing a quantum optics technology
called FDS (Frequency-Dependent Squeezing) to improve
the sensitivity of gravitational wave telescopes over a wide
bandwidth is ongoing. In FY 2021, improvements were madein alignment control, and two research papers were published.
In addition, we started detailed design of FDS for KAGRA inorder to introduce this FDS technology in KAGRA to achieve
higher sensitivity; FDS for KAGRA is being conducted throughcollaboration between NAOJ, National Tsing Hua University in
Taiwan, and the Korea Astronomy and Space Science Institute(KASI).

3. Education
A master student in the Astronomy Department of the
University of Tokyo was admitted. A student in the Tokyo

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043

Institute of Technology received a master’s degree for researchon mirrors for KAGRA at the TAMA300 facility. As forgraduate school and university education, lectures were given at
the University of Tokyo Graduate School and Hosei University.
In addition, we actively engaged in social education activities
such as “FUREAI (Friendly) Astronomy” and visiting lectures athigh schools.

4. OutreachA publicity video produced jointly by the Public Relations
Center and the Gravitational Wave Science Project won
the Science Museum Director’s Award at the Science andTechnology Film/Video Festival. In addition, a virtual tourof TAMA300 was conducted at an open house held online.
In addition, the GWSP cooperated with NAOJ in introducing
KAGRA’s vacuum technology at the Vacuum Exhibition.

5. International Collaboration and Visitors
Under the restrictions of the COVID-19 situation, we had
fewer visitors than normal, actually no visitors. On the other
hand, international cooperation has been actively carried out,
and joint research with CNRS / APC (France), iLM (France),
National Tsing Hua University (Taiwan), Myongji University(Republic of Korea), KASI (Republic of Korea), etc. hasprogressed.

6. Publications, Presentations, and Workshop
Organization
The GWSP members were authors of 37 refereed
publications in international journals. There were 11 nonrefereed publications in European languages and 2 in Japanese.
There were 12 presentations at international conferences and
49 presentations in domestic conferences. There were no otherreports printed in either European languages or Japanese.

7. Acquisition of External Funds
In FY 2021, no external funds other than scientific researchfunds were obtained.

8. Staff
Transfer / Retirement● Hideharu Ishizaki: Research engineer (Retired)● Atsumi Sawagaki: Administrative Supporter (Retired)● Naoatsu Hirata: Senior Specialist (transferred to engineer inATC)● Dan Chen: Project Research Staff (transferred to assistantprofessor in GWSP)● Tasuki Washimi: JSPS PD (transferred to project assistantprofessor in GWSP)

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08. Thirty Meter Telescope Project
The Thirty Meter Telescope (TMT) Project is a project
to build an extremely large 30-meter telescope under thecollaboration of research institutes in five countries: Japan,
the United States, Canada, China, and India (Figure 1). For
Japan’s part, the National Institutes of Natural Sciences(NINS) is the ultimately responsible body, and NAOJ is theexecuting institute. In 2014, an agreement was executed
among the participating organizations to found the TMTInter national Obser vator y (TIO) for the pur pose of theconstruction and operation of the observatory; the construction
was subsequently commenced. Japan is responsible for the
production of the telescope primary mirror, the design andproduction of the telescope structure as well as its on-site
installation and adjustment, and the design and production ofscience instruments. Heading the project for Japan is the TMT
Project established 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, as a TIO
member, NAOJ provides assistance for TIO’s continued
efforts for building trust in Hawai‘i through direct dialogue,
educational suppor t, and other community engagement
activities together with relevant organizations. In the Hawai‘iState Legislature, a bill was submitted and deliberated
to rev iew Mau na kea ma nagement i n considerat ion ofrecommendations by a working group which involved Native
Hawaiian members. In the U.S., the Decadal Survey, which
is a report of the research community that identifies priorities
for the coming decade, ranked a joint program called the U.S.
Extremely Large Telescope Program (the US-ELT Program),including the TMT project, as a top priority for groundbased astronomy. Discussion with the U.S. National Science
Foundation (NSF) began for its possible participation in the
project. Seeing major progress in the situation in Hawai‘i and
NSF’s possible participation in the project, TIO, NAOJ, and theother members are focused on essential activities in the overall
process, including those that will lead the way to full-fledged
construction once on-site efforts restart, while minimizing theirexpenditures.

the National Astronomical Observatories of the Chinese
Academy of Sciences, as well as the U.S. Association of
Universities for Research in Astronomy (AURA) participating
as an Associate Member which envisages future participationof the NSF.
TIO, operated according to deliberations and decisions
made at meetings of the TMT Board of Gover nors, isoverseeing the construction work performed in each country as
well as developing the on-site infrastructure. For the purposeof discussing activities for the official participation of NSF,
the on-site construction issues, and other matters, the Boardof Governors was convened 11 times in FY 2021, including
regular meetings on a quarterly basis. The board meetings wereattended by three representatives from Japan, Director General
Tsuneta, Vice-Director General Iguchi, and NAOJ TMT
Project Manager Usuda. Different working groups were createdunder the board to consider efforts for construction in Hawai‘i,
as well as issues of the project operation, by holding meetings
frequently. One of them is the Business Plan Working Groupchaired by the NAOJ Director General. Convened seven times
in FY 2021, this working group focused on discussion of thestatus of the members’ in-kind contributions and the valuation
method. These meetings were held online due to COVID-19
restrictions.
In the U.S., the Decadal Sur vey, which decenniallyevaluates and identifies the most compelling challenges in
the field of astronomy, started in 2019, and the report wasannounced in November 2021. The US-ELT Program, which
will allow all-sky observation by working in concert with TMT
and the Giant Magellan Telescope (GMT, a telescope with anaperture of 24 m currently under construction in Chile), wasranked as a top priority of the Decadal Survey for ground-based
astronomy. In response to the release by the Decadal Survey,
discussion began with NSF toward a review of design proposals

1. TMT Project Progress and Status of theConstruction Site
The construction of TMT is led by the participating
countries and organizations under TIO established in 2014.
The current officially participating countries and organizations
are NINS (Japan), the University of California, the California
Institute of Technology, the National Research Council of
Canada, the Department of Science and Technology of India,

Figure 1: Conceptual image of TMT (provided by TIO).

II Status Reports of Research Activities045

for the US-ELT Program submitted by TIO along with NSF’s
National Optical-Infrared Astronomy Research Laboratory(NSF’s NOIRLab) and GMT. Considering that the U.S. federal
investment in the TMT project through NSF is essential forthe project’s success, TIO is presently working for NSF’s
preliminary design review (PDR) scheduled for the near future.
In November 2021, as part of the preparation for the NSF PDR,a panel of independent, internationally recognized experts
comprehensively reviewed the TMT project for its technicalmaturity, scheduling, budgeting, risks, etc., and concluded thatthe project is ready for the PDR. The NAOJ TMT Project fully
cooperated with TIO for this independent review.
T he f i nal de cision on t he fede r al f u nd i ng for t heconstruction of TMT through NSF participation will be madeby the U.S. Congress. Prior to the decision to participate, NSF
made informal outreach efforts with stakeholders in Hawai‘i in
FY 2020 in a move to lay the groundwork for an environmental
impact assessment and a consensus-building process inaccordance with the National Historic Preservation Act. In
addition, TIO worked on a proposal for NSF’s development
funding of the primary mirror control system, the secondary
mirror, and other components for an interval before NSF
participation.
As for the situation in Hawai‘i, a CDUP was approved for
the TMT planned site on Maunakea in September 2017, butseveral parties appealed this decision. In October 2018, theState Supreme Court found that due process was followed forissuance of the CDUP, which completed all the legal process
for TMT. However, those opposed to TMT on Maunakea staged
demonstrations, including some sit-ins on the access road tothe summit region, preventing the full-fledged construction in
July 2019. The Board of Governors recognized they had neither
well understood the social issues behind the demonstration nor
engaged in dialogue with the broader communities in Hawai‘i,
which had led to the failure to fully build trust with the
Hawai‘i community. The Board decided to implement phased
relocation of the TIO headquarters to Hawai‘i, with the firststep being to relocate the Project Manager to start communitybased activities. Both the NAOJ TMT Project Manager who
moved to Hawai‘i Island in July 2021 and a Senior Specialist
based in Hawai‘i f ully cont ribute to TIO’s com munit yengagement activities. Through dialogue with the community,
the strong need was expressed for educational support forchildren, in particular, those from low-income families. TIO
started tutoring activities at schools (Figure 2) that Maunakea
observatories had not engaged, which generated a greatinterest among local communities. TIO further developed an
educational support program for the broader communities,
and incorporated it in the development proposal which was
submitted to NSF.
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 wasdeveloped and deliberated at the state legislature for creation

046

II Status Reports of Research Activities

Figure 2: Educational support program at Hilo Intermediate School(after-school tutoring).

of a new management structure for Maunakea that particularly
engages with the Native Hawaiian community. Since thismay affect the TMT Project, its development is being closely
monitored (as of March 2022).
As for the alternative site on the island of La Palma of the
Canary Islands in Spain selected in 2016, the process for all
permits needed for construction was completed in November
2019, including an environment impact assessment. In an
administrative appeal against one of the permits, a court
determined in July 2021 there was a procedural problem,
against which TIO appealed together with a local government
and a local research institute. NAOJ expresses its support forrelocation to La Palma in the case that construction in Hawai‘i
becomes infeasible, as long as the project is expected to receive
the U.S. federal funding.

2. Japan’s Progress on Its Work Share –Development of the Telescope Structure, thePrimary Mirror, and the Science Instruments
For the const r uction of TMT, Japan is responsible
for essential components of the telescope: the design andproduction of the telescope structure and its control system;and the manufacturing of the primary mirror, in accordancewith the executed agreements. It also takes part in productionof a portion of the science instruments which are developed
through international partnerships. While the restart of onsite
construction is halted, Japan worked on designs and preparation
for production in FY 2021, concentrating its efforts on essential
work for the overall process instead of production. In FY 2021,
the following progress was made.
(1) Manufacturing of the Primary Mirror Segments
The TMT primary mirror, comprised of 492 segment
mirrors, requires the manufacturing of 574 segment mirrors
in all with the replacements to be used during mirror coating
included. The processes of manufacturing mirror segments
are: fabrication of the mirror blanks, spherical grinding of thefront and back surfaces, aspherical grinding and polishingof the front surface, hexagonal shaping, and mounting of themirror segments onto support assemblies. These processes arefollowed by final surface finish to be completed in the U.S. andcoating with reflective metal to be performed on site, before themirror segments are finally installed on the telescope.
Of these processes, 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
beginning from aspherical grinding and polishing and ending
with mounting of the mirror segment on a support assembly
distributed among four countries, Japan is leading this workfor 175 of the mirror segments. In FY 2021, the primary mirror
team identified and examined a measure to protect the mirror
surface during the hexagonal shaping as necessary work in aneffort to facilitate production of the primary mirror when fullf ledged manufacturing of the mirror segments is resumed,
without affecting the entire schedule. The team investigatedlow-alkaline and other grinding f luids used for grinding
work that may have little effect on the protection coating. The
highlights of FY 2021 included completion and successful
passage of TIO’s review of 13 segments that were asphericallypolished by FY 2019 to confirm that they meet the technicalconformance criteria before being cut into their hexagonal
shape. (Figure 3)(2) Design and Production of the 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 optics systems, such as theprimary mirror, and the science instruments, and points themin the direction of a target astronomical object. Following
the baseline and detailed designs developed by FY 2016 andpreparation for fabrication in FY 2017, FY 2018 saw the launchof the fabrication process for the telescope structure. In FY
2021, continuing on from the previous fiscal year, with aneye toward a production readiness review scheduled before
full-scale production, the work was focused on completion ofinterface documents and development of production drawingsof a cryo-platform, instrument support structures, etc., as well
as refinement of production drawings of the elevation journal
and the Nasmyth structure, which will pave the way for future
production. As for the examination and determination of theinterfaces, the structure team provided TIO with assistancein definitions of interfaces from the telescope to the support
facility, with a focus on the piping and wiring subsystems thatwere reviewed for the final designs.

Figure 3: Polishing and measuring processes of mirror segments inJapan. In April 2021, the quality review was conducted for mirror
segments that underwent the aspherical polishing process. A total of 13
segments passed the review, which will be followed by the next step of
the process, hexagonal shaping.

(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 that stands for an InfraRed Imaging
Spectrograph. Being in charge of its imager, the NAOJ TMT
Project cur rently engages in development that includes
designing and prototyping in cooperation with the Advanced
Technology Center. IRIS has been in the detailed designphase since FY 2017. In FY 2021, as part of the first detailed
design review held from April to June, the imager which Japanis responsible for was reviewed. The IRIS team provided
documents related to systems engineering (such as requirement
documents, interface documents, risk management, andassembly adjustment plans), and reported designs and analysis
of optical, mechanical, and electric systems, and results ofprototype tests. In response to the review, the team identified
action items to address, and performed thermal analysis of
the entire system, vibration analysis, prototype tests (such as
repeatability of the slicer pickoff mirror’s position, and theposition sensor’s thermal cycle test). Progress was also madein other areas, including development of software engineering
documents, the surface figure measurement of a large mirror ina cryogenic environment, and detailed analysis of stray light.
A Wide Field Optical Spect rometer or W FOS is in
the conceptual design phase. The WFOS team engaged indevelopment of concepts for the slitmask exchanger, theslitmask fabrication facility, and the Integral Field Unit, as
well as setting a code for the slitmask exchanger, followed bydevelopment of the mechanical design. In response to changes
from the original WFOS design, revisions were made to theconcept for the Integral Field Unit, along with examinationof a concept for a case where a physically narrow slicer is
employed. Hoping to verify the technology for devolvementof the WFOS Integral Field Unit, the team made headway on
an optical design of an Integral Field Unit demonstrator to be
mounted on the Subaru Telescope’s visible spectrophotometer
called the Faint Object Camera and Spectrograph. In February2022, a conceptual design review of WFOS, including Japan’s
parts, was successfully completed, and ushered the instrument
into the preliminary design phase.
A Multi-Objective Diffraction-limited High-Resolution
Infrared Spectrograph (MODHIS) is expected to pioneer
the field of exoplanets, which was emphasized in the U.S.
Decadal Survey. With its project management led by an NAOJ
faculty member, MODHIS officially kicked off the first phaseof a conceptual design in August 2021 in partnership with
the California Institute of Technology and the University ofCalifornia, Los Angeles and San Diego. This phase aims toclarify the concept of an adaptive optics to be combined with
the instrument and develop a conceptual design of the interface
to TMT adaptive optics. The team’s effort also went into
defining scientific and technical requirements to be satisfied by
MODHIS. With the sights set on establishing an international
development team, a role for the Astrobiology Center in the

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047

MODHIS development is currently under consideration.
TIO’s development efforts are also contributed to by
NAOJ staff who are based at the NAOJ California Office inPasadena. Their contributions are a considerable asset for TIO
work, including a major role in developing a conceptual designof a coating facility for the secondary and tertiary mirrors
and its review by another NAOJ member. One of the staff
members in Pasadena served on a preliminary design review ofmaintenance and operation of mirror segments.

3. Planning of TMT Science, Instrumentation,
and Operation with Communities of Researchers
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 2021, 7 meetings were held online, attended
by 4 university researchers and NAOJ TMT Project Manager
Usuda 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 developmentof i n st r u me nt s t h roug h i nt e r nat ional pa r t ne r sh ips, a
subcommittee on observation of exoplanets with TMT, chairedby Professor Norio Narita of the University of Tokyo, discussed
research themes based on results of surveys conducted in eachcountry. A sub-working group, created to work on developmentof a science operations plan once the telescope is completed,
was attended by Associate Professor Wako Aoki of NAOJ.
The TMT Science Advisor y Committee, which is adomestic com mittee consisting of 12 researchers f rom
universities and other institutes, reviewed issues of science
programs, instrumentation, and operations. NAOJ’s funding
program for research and development of TMT science
instr uments, which did not call for applications due tobudgetary restrictions in FY 2020, resumed in FY 2021, withadoption of 6 proposals to carry out research for developmentby 26 researchers of 12 universities and research institutions.
Seeing a science operations plan being developed in the U.S.
as part of planning by the US-ELT Program toward possible
participation by NSF, a working group was created under the
TMT Science Advisory Committee to continue examination ofscience operations, and submitted Japan’s opinion to TIO.
More meetings for larger communities of astronomy inJapan were actively organized to explain the status of the
project and engage in discussions. The NAOJ TMT Project
held an online meeting to explain about the results of the
U.S. Decadal Survey in December, as well as a workshop
for the instrument development, and another for the science
operation in June 2021. A series of meetings were held withparticipation by researcher communities representing a broader
range of fields, such as radio astronomy, theoretical astronomy,
and solar research, as well as the community of optical andinfrared astronomy. The NAOJ Director General provided thelatest information on the TMT project for the astronomy andastrophysics subcommittee of the Science Council of Japan.
For the purpose of facilitating communication with the Earth048

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and planetary science community, the NAOJ TMT Project
presented a talk at the fall session of the Japanese Society for
Planetary Sciences in September 2021 to introduce the project,
as well as a lecture on research on the Solar System andobservation of exoplanets envisioned with TMT.

4. Public Relations, Outreach, and Education
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.70
through 73 were delivered.
The outreach activities, which mostly shifted from inperson to online lectures and classes in FY 2020 due to the
COVID-19 pandemic, continued to capitalize on online
opportunities in FY 2021, 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. At the same time, some of theevents returned to an in-person format. There was a total of 30
sessions of lectures for the public and classes on demand.
In Hawai‘i as well, where TMT is to be constructed, eventswere held online. The NAOJ TMT Project participated as ondemand lecturers in a science/technology education and PR
event called “Journey Through the Universe” in March 2022.

5. Organization
By the end of the fiscal year, three Professors, six Associate
Professors, two Assistant Professors, two Research Engineers,
and a Senior Specialist held full-time positions for the NAOJ
TMT Project. In addition, two Professors, an Associate
Professor, a Senior Lecturer, an Assistant Professor, and a
Senior Engineer from the Advanced Technology Center,
the Subaru Telescope, and the NAOJ Chile Observatory
have concurrent positions in the TMT Project, and take partin activities that include the development of TMT science
instruments at the Advanced Technology Center.
With the aim of strengthening the close partnership with
TIO, five members are assigned to the NAOJ California Officein Pasadena. There are three members in Hawai‘i working
for TMT, one of whom is from the Office of International
Relations.
In light of integrated operation of the Subaru Telescope and
TMT in the future, schedules and staffing allocation models
were formulated in line with the long-term plan for operation
with the Subaru Telescope. As part of the efforts, the domestic
administration and the public relations are integrated with the
Subaru Telescope.

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 Small-JASMINE missionof ISAS/JAXA (Institute of Space and Astronautical Science/
the Japan Aerospace Exploration Agency), aiming to realize theworld’s first near-infrared high-precision astrometry and timeseries photometry.
We will perform the following missions to achieve the above
purpose of the JASMINE Project.
1) To contribute to scientific verification and development of
the instruments and the data analysis software for the SmallJASMINE mission of ISAS/JAXA.
2) To provide the scientific community with a catalogue ofphysical information, including parallaxes, proper motions,and light curves, for stars in the Galactic Center, through aninternational framework under the leadership of ISAS/JAXA.
Small-JASMINE (hereafter, referred to as JASMINE. In the
future, JAXA will officially change the name to JASMINE) was
selected by ISAS/JAXA in May 2019 as the unique candidate
for the JAXA Competitive Middle-Class Science Missions
No.3. At the present, according to the progress schedule in theSpace Basic Plan established by the Cabinet Office in Japan, thelaunch of JASMINE is scheduled for 2028. We are promoting
JASMINE with the aim of gradually improving the development
stage at JAXA. JASMINE has the following three primaryscientific goals.
1) To reveal the Milky Way’s central core structure andformation history by measuring the distances and the motionsof stars located as far as 26 thousand light-years away withhigh-precision astrometry observations in the near-infraredband.
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 30 cm toperform infrared astrometric observations (Hw band: 1.1–1.6
μm (TBD)) (to be determined in detail). A mission goal is tomeasure as the highest precision annual parallaxes at a precisionof less than or equal to 25 μas and proper motions, or transverse
angular velocities across the celestial sphere, at a precisionof less than or equal to 25 μas/year in the direction of an areaof a few square degrees of the Galactic nuclear bulge and in
the directions of a number of specific astronomical objectsof interest in order to create a catalogue of the positions andmovements of stars within these regions. The project 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 theeffect of absorption by dust is weak. This project will help toachieve revolutionary breakthroughs in astronomy and basic
physics, including the formation history of the Galactic nuclear
bulge (Galactic Center Archeology); Galacto-seismology; thesupermassive black hole at the Galactic Center; the gravitational
field in the Galactic Nuclear Bulge; the activity around theGalactic Center; formation of star clusters; the orbital elementsof X-ray binary stars and the identification of the compact object
in an X-ray binary; the physics of fixed stars; star formation;planetary systems; and gravitational lensing. Such data willallow for the compilation of a more meaningful catalog whencombined with data from ground based observations of the lineof-sight velocities and chemical compositions of stars in thebulge.
Due to satellite operations, there are periods whenastrometric observations towards the Galactic center direction
are not possible. In such a period, in order to utilize the uniquefeatures of the JASMINE satellite (its capability of highprecision photometric and highly frequent observations in thenear-infrared region), we can plan to observe a few specificastronomical objects in the Galaxy. Therefore, JASMINE
will carry out transit observations utilizing the continuous
photometric observations. It is possible to search for Earth-type
planets that are expected to be in the habitable zones aroundM-type stars, which are low mass red stars belonging to themain sequence. JASMINE dominates the other missions for
explorations of this type of exo-planet. Furthermore, JASMINE
will be Japan’s first satellite mission for the exploration of exoplanets.
The JASMINE Project has also been promoting the plan ofa micro-satellite project, Nano-JASMINE, with a primary mirror
aperture of 5 cm. Nano-JASMINE aims to produce scientificresults based on the astrometric information for bright objects inthe vicinity of the Solar System. Despite its small aperture, thesatellite is capable of observational precision comparable to the
Hipparcos satellite. The combination of observational data from
Nano-JASMINE and the Hipparcos Catalogue is expected to
produce data on proper motions for very bright stars which will
be more precise than those of Gaia. Launch opportunities for the
Nano-JASMINE satellite are under consideration.

II Status Reports of Research Activities049

(2) Major Progress in FY 2021
1) Organization of the office
The JASMINE Project is composed of eight full-time staff
members, one technical supporter, and two graduate students.
Significant contributions were also made by members of thefollowing organizations: Kyoto University’s Graduate Schoolof Science; ISAS/JAXA; the University of Tokyo; and the
University College London.
2) Overview of planning and developing the JASMINE Project
The JASMINE Project established a JASMINE consortium
consisting of researchers. The purposes of the consortium areto 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 December 2021, aconsortium meeting was held online, which also served as anopen science workshop for JASMINE.
Regarding the development of observation instruments, aninfrared detector developed by the NAOJ Advanced Technology
Center for ground based astronomy, is now being adapted forspace use. The development progressed smoothly, such as
passing some radiation resistance tests, completing prototypes,
completing designs for large formatting of a detector, andexamining concepts on the thermal structure of a detector box. In
addition, the specifications of the observation instruments havebeen examined with satellite manufacturer company candidates.
For the satellite system as a whole, the risks that should be
resolved at this point were examined in cooperation withmultiple satellite manufacturer company candidates. Regarding
data analysis, a data-analysis group has been developing andcarrying out simulations of stellar image creation and a series of
end-to-end simulations from estimations of stellar image centers
to deriving astrometric parameters such as annual parallaxes.
After the proof of principle, the group started development
considering more realistic and complex noise. In international
cooperation, we proceeded with preparations for analysis ofastrometric data with researchers at Heidelberg University.
3) Progress of the Nano-JASMINE Project
Assembly of the ﬂight model of Nano-JASMINE that will
be actually launched into space was completed in FY 2010.
However, it is difficult to get a launch service, and coordination
with the launch company is still ongoing.

050

II Status Reports of Research Activities10. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project
1. Project Overview
In FY 2021, the RISE Project first and foremost worked as
the Martian Moons eXploration (MMX) Geodesy sub-scienceteam (G-SST) to continuously investigate the operation plansof MMX, introduce new software, and support designingand manufacturing an onboard instrument. (i) To prepare forsimulation studies of the internal structure of Phobos after
the data acquisition, we examined the accuracy and spatial
resolution of the Phobos gravity field that is expected to be
retrieved from two- and three-dimensional Quasi-Satellite Orbits(2D-QSO/3D-QSO) at the various altitudes. We investigated
how the gravity field model estimated only from the spacecraft
tracking range-rate data would be improved by incorporating
laser altimeter (LIDAR) data and image data. A paper describing
science requirements and an observation plan for geodetic studyof MMX was accepted in the Earth, Planets, and Space journal.
(ii) We selected the orbit/gravity field estimation software
produced by CNES in France as the one to be nominally usedin MMX and regularly had meetings online to train expected
users. (iii) To activate international collaborations of G-SST,
we attended domestic and international Science Board meetingsand discussed possible achievements of scientific research. All
meetings were held online to prevent COVID-19 infections.
(iv) Regarding utilization of the stereophotoclinometry shapemodeling software (SPC), we negotiated with the Planetary
Science Institute (PSI), which developed the SPC and confirmed
consistency with NASA Participating Scientist Program. Oncethe prospect of introducing SPC software was attained, we could
make a detailed plan for imaging Phobos to produce the shapemodel. (v) To support the development of the Flight Model(FM) of LIDAR, we attended development meetings and thefield test and contributed to the development and performance
evaluation of the Engineering Model (EM). (vi) We continued
regular seminars to review recent research on Phobos’s internal
structure and discussed relationships between orbit evolution,
shape changes, and internal physical properties (Love number,
k2 and energy attenuation, Q) of Phobos. In addition, (vii) we
contributed to long-term operation planning in the Mission
Operation Working Team (MOWT) and made a list of expected
data products of G-SST and LIDAR in ground Data Processing
WT (DPWT) to organize the data processing flow.
Second, we produced Level 0 data of the Hayabusa2
LIDAR to be included in the opened data archive and added a
description of how to calculate Level 1 data from Level 0 data
to the Software Interface Specification (SIS) document. We
continuously arranged with the Hayabusa2 data archive team for
publication. An international board reviewed our production. On
the other hand, we studied the slope stability of the top-shapeof the asteroid Ryugu considering the deceleration of its spin
rate and began writing a paper. Also, in March we submitted apaper as coauthors on the surface albedo of Ryugu, which used
LIDAR data. Regarding the laser-link experiment conductedduring the return to Earth of Hayabusa2 with the Institute ofSpace and Astronautical Science (ISAS) and National Instituteof Information and Communications Technology (NICT), one of
the RISE Project members led writing a paper and submitted itas the first author in March.
Third, we held team meetings of the Planetary Science
Working Group under the Science Strategy Committee andconsidered the role of planetary explorations in the National
Astronomical Observatory of Japan. We had online meetingson April 19, June 28, August 17, October 18, December 27, andFebruary 28 to discuss research on exoplanets and the Solar
System in the Division of Science, visible and near-infraredobservation of exoplanets, observation of protoplanetary disks
by radio telescopes, and observation of trans-Neptunian objects.

2. Educational Activities
One RISE member educated a third-year graduate student of
the University of Tokyo as an assistant advisor.

3. Outreach/PRIn FY 2021, the Project members volunteered two times
for Kirari Oshu City Astronomy School as well as six times
for FUREAI (Friendly) Astronomy classes. In addition, RISE
members provided five special lectures for the public.

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11. SOLAR-C Project
1. SOLAR-C Project Overview
SOLAR-C is a planned satellite project and may become
Japan's fourth solar observation satellite mission after Hinotori,
Yohkoh, and Hinode. The plan is to realize the launch in the
mid-to-late 2020s. Through observations from the satellite, thisproject 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
an order of magnitude compared with the similar instrumenton the Hinode satellite. It also has the feature of being able toobserve the hot solar plasma with temperatures ranging fromtwenty thousand to twenty million degrees nearly seamlessly.
Since its establishment, the JAXA SOLAR-C project WG has
involved many non-Japanese specialists in addition to Japanese
researchers. Japan will be responsible for the launch vehicle,
satellite bus, and telescope section of the science instrument. The
spectrograph section will be developed through international
collaborations with the U.S. and European space agencies andinstitutions. NAOJ will play a leading 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 has moved to the Mission
Definition Phase (Pre-Phase-A2) in FY2019. After the preproject candidate down-selection pre-screening in February
2020, this project was selected as the JAXA Small Satellite
4 project in May 2020. In terms of international cooperation,NASA’s participation in this project was decided in December
2020 based on NASA’s Phase A study that had been underway
since 2019, followed by the participation of European space
agencies. In FY 2021, we prepared for the mission definition
review while proceeding with feasibility studies with overseas
partner organizations.

2. Progress of the SOLAR-C Project Activity in FY2021
In FY 2021, the following aspects of the telescope section andsatellite bus, for which Japan is responsible, were studied using
the JAXA front-loading expenses: (1) The design study of the
primary mirror assembly with tip-tilt and focusing mechanisms,(2) the redesign and refinement of the structure model, (3)the on-orbit temperature prediction and thermal deformation
prediction by the thermal mathematical model, (4) the study ofmechanical interface conditions between the satellite and theobservation equipment and those within the science payload, (5)052

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the examination of requirements for the small satellite standard
bus, (6) the performance evaluation of the prototype model of the
Ultra Fine Sun Sensor, and (7) the investigation of outgassing
characteristics of candidate adhesives. Through these design
studies, the validity of the design has been confirmed for somecritical items, while some issues in the initial design have beenclarified. For the primary mirror, it was decided to increase thethickness of the primary mirror to prevent degradation of spatial
resolution due to deformation caused by coating stress, andthe actuator and sensor to be used in the scanning mechanism
were selected. In addition, outgassing data were obtained forcandidate adhesives to be used in the primary mirror support
points, which are expected to reach a high temperature of
approximately 110 degrees C. To accommodate the increased
weight of the primary mirror assembly, we have updated thedesign of the focus adjustment mechanism while utilizing thedeveloped model. From the latter half of the fiscal year, we havebeen focusing on preparation for the mission definition review
and interface coordination with overseas components.

3. SUNRISE-3 Project Support
While the Solar Science Observatory (SSO) has handled
the short-term experiment projects since this fiscal year, most
SOLAR-C project members continue to contribute to developing
the science payload for the Balloon Project SUNRISE-3. In FY
2021, the project completed its development activities in Japanand proceeded to assembly and testing in Germany. Refer to thereport of the Solar Science Observatory for details.

4. Educational and Publicity Outreach Activity
Two SOKENDAI graduate students and one contracted
graduate student (University of Tokyo) were supervised. The
project also participated in the Tour of the Solar Research
Frontline to introduce domestic solar research to undergraduate
students and introduced the project activities in research anddevelopment through the web.

5. Others
While NAOJ reimbursed the SOLAR-C project for its
general operation and contingencies, a large part of the expenses
for supporting the project preparation was funded by otherexternal sources such as the JAXA’s study-acceleration andbasic development fund. From the viewpoint of smoothing out
the administrative work volume of SOLAR-C and SSO projects,
the expense processes for the short-term experiment projects
were conducted by this project.
T. Oba, Project Research Staff, was appointed in April 2021,
and T. Okamoto, Assistant Professor, in November 2021. Y.
Kawabata, Project Research Staff, moves to the Solar Science
Observatory in April 2022.

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 us to obtain spectra of ~2400 objects simultaneously at
wavelengths ranging from 0.38 µm to 1.26 µm with a spectral
resolution of R ~ 2000 – 4000. 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 (6 institutions, USA), Brazilian consortium,
LAM (France), MPE/MPA (Germany), and Chinese PFS
Participation Consortium (6 institutions, China). The subsystemsof the PFS instrument have been developed at designatedinstitutions, and NAOJ is responsible for modifying thetelescope/dome, preparing a temperature-controlled clean room
for the spectrograph system, and operation of the instrument.
NAOJ is also committed to its commissioning, its data pipeline
and science database.
NAOJ approved these activities as an A-project from FY
2019. The mission of the A-project is to complete on-site
assembly and installation into the Subaru Telescope, verify its
system requirements, then perform science commissioning andperformance verification. The A-project work will lead to thestart of PFS operation, at which point PFS will transition to a
Subaru facility instrument, and the A-project will be dissolved.

During testing, the auxiliary electronics of PFI were foundto be unstable and necessitated extensive work to fix. We now
finished stabilizing the electronics, for PFI to be used during
the scheduled engineering run in mid. June, but further work isneeded to improve its long-term reliability.
The fit test of PFI on the telescope also revealed a design
flow of PFI rotator which required the modification of the rotator
limit switches.

2. PFS A-project Leadership Changes
In May 2021, while working in Taiwan for PFS, Takatosan, the PFS A-project leader at NAOJ, passed away. This was aterrible loss for everyone at NAOJ and Subaru.
Following this dramatic event, a period of transition started
to reorganize the PFS A-project leadership. The new PFS
A-project leadership was assigned to Julien Rousselle (leader)and Shintaro Koshida (co-leader).

Figure 1: PFI installed on the telescope for fit test.

3. Progress in FY 2021
(1) Subsystems delivery and assembly
SuNSS (Subaru Night-Sky Spectrograph) was installed on
the Subaru telescope spider arm in Feb. 2021 and successfully
tested on sky in March 2021. This instrument uses two small
optics, the first PFS fiber cable, and the first PFS spectrograph,to take spectra of the night sky background when PFS is not
used. This data will be very valuable for PFS data processing, as
well as for other Subaru instruments.
In June 2021, the Prime Focus Instrument (PFI) was
delivered from ASIAA (Taiwan) and we have performed AIT(Assembly, Integration and Test) activities since then, including
on-sky engineering observation.

Figure 2: PFI focal plane with ~2400 optical fibers, their positioners and
6 auto-guiding cameras.

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053

In April, the second fiber cable (out of 4) was successfully
installed on the telescope and passed our initial performancetest.
(2) On-telescope test and Engineering run
In Sept. PFI was successfully installed on the telescope
prime focus for a fit test, as well as an “end-to-end” test
involving all PFS subsystems already installed (the metrology
camera, PFI, the first spectrograph and the first fiber cable). This
test was also successful and the first sky spectra were taken (seeFig. 3–4).

Figure 3: First sky spectra in Blue camera taken on 2021.09.26

Figure 4: First sky spectra in Red camera taken on 2021.09.26

In Nov. PFS had its first engineering run for 3 nights.
Unfortunately, a design flow of PFI limit switches prevented
us from using the rotator during this run, but we were still able
to take images with the auto-guiding cameras and close theautoguiding loop on the telescope. We also successfully tested
the fiber positioners using the Metrology Camera System (MCS)
installed on the Cassegrain focus.
(3) Science operation updates
During FY 2021 a lot of software development has been
done in both Mitaka and Hilo groups to develop the PFS science
operation. This includes the development of the science andtarget databases and data format, as well as the flux calibration,
object selection, pointing planner and fiber allocation.
We also started to work on the data access policy for open
use, as well as the archiving policy needed to store the large
amount of data created by PFS.

054

II Status Reports of Research Activities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 partof ULTIMATE, which will uniformly improve the seeing
by a factor of 2 over a wide field of view up to ~20 arcmin indiameter. A primary science goal of ULTIMATE is to reveal thehistory of galaxy formation and evolution by an unprecedented
near-infrared survey of the distant Universe.
The GLAO project successfully completed the conceptual
design phase in FY 2018. In FY 2019, the GLAO project was
accepted for the NAOJ’s call for A project proposals and has
started the preliminary design phase. In the A-project period,
the GLAO project aims to complete the preliminary design of
the GLAO system and the prototyping of the key subsystems
within 3 years, followed by final design, production, assembly,
integration, and test phases. The GLAO project is planning to
implement the GLAO system at the Subaru 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 2021 there was one associate
professor dedicated for the GLAO project. There were also
1 project associated professor, 1 senior specialist, 4 assistantprofessors, and 7 RCUH employees (4 research staff and 3
engineering staff ) appointed concurrently. 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 2021
The ULTIMATE science team, consisting of domestic
and international scientists, has been conducting studies ofscience cases for ULTIMATE, in alignment with the strategyof the Japanese optical/infrared astronomy community looking
ahead to the 2030s (TMT era). In FY 2021, the ULTIAMTE
science team has published an “ULTIMATE Science White
Paper,” which summarized the past studies on the main andextended science cases for ULTIAMTE and top-level science
requirements drawn from the science cases. The ULTIMATEdevelopment team has also summarized the technical studies on
the science instruments that will satisfy the science requirements
when used with the GLAO system. The technical studies forthe relocation of MOIRCS to the Nasmyth IR focus to provide a
multi-object spectroscopic capability and for the wide-field nearinfrared imager (WFI) that covers 20 arcmin field of view indiameter at the Cassegrain focus were compiled in a conceptual

design report. A conceptual design review for the ULTIMATE
science cases and the science instruments to realize them washeld in June 2021 by inviting external reviewers. The review
committee highly evaluated the science cases and the instrument
development plan and endorsed the project to move forward
to the next design phase with some suggestions to improve theproject.
The GLAO design has been conducted for its main
subsystems. In FY 2021, the final design of the adaptive
secondary mirror (ASM) has been completed and we are readyto proceed with the production phase. In addition, we continued
the preliminary design of the wavefront sensor (WFS), the laser
guide star facility (LGSF), and the real-time control system(RTC) based on their system requirements. The optical andmechanical interface designs have been completed to use WFS
at the Cassegrain focus with the wide-field imager (WFI). The
preliminary design of the other subsystem will be completed in
the first half of FY 2022. We are planning to hold a preliminary
design review of the GLAO system in October 2022.
The GLAO project has been conduction prototyping
instruments for the GLAO system. We have been upgrading thelaser system for the existing AO system at the Subaru Telescope
to demonstrate the technology for the LGSF. We have also
been developing a Laser Tomography AO (LTAO) system todemonstrate the technology for Shack-Hartman WFSs with four
laser guide stars. In FY 2021, the upgrade of the laser system forthe existing AO system was completed. We have conducted afirst launch of the laser from the Subaru Telescope and conducted
the performance evaluation of the upgraded laser system. The
performance of the GLAO system highly depends on the fractionof the atmospheric turbulence in the ground layer. We havebeen developing an atmospheric turbulence profiler to directly
measure the ground-layer turbulence from the Subaru Telescope.
The profiler has been assembled and tested in a laboratory in
FY 2021. In FY 2022, we will install the profiler on the Subaru
Telescope to measure the ground-layer turbulence.

4. Outreach
To inform the astronomical community and general public
about the Subaru GLAO project and its scientific motivationand goals, we released news articles from the project on a public
website (https://ultimate.naoj.org/english/index.html). In FY
2021, the GLAO project wrote a web release on the first laser
launch from the upgraded laser guide star facility.

5. International Collaboration
The GLAO project has been closely collaborating with
the Australian National University (ANU) and the Academia
Sinica Institute of Astronomy and Astrophysics (ASIAA) forthe preliminary study of the GLAO system. In FY 2021, we
continued the collaboration with ANU for the preliminary

II Status Reports of Research Activities055

design study of the WFS and the LGSF and with ASIAA forthe conceptual design studies of the ULTIMATE science
instruments.
In FY 2021, the Japan Society for the Promotion of Science(JSPS) core-to-core program “International research network
toward the era of deep and wide near-infrared survey of the
Universe with space and ground-based telescopes”, led by the
ULTIMATE science team, has started its activities. We regularly
held seminars to introduce wide-field survey projects plannedin each country and discussed them with participants from theUSA, France, Australia, Taiwan, and Japan.

056

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14. Astronomy Data Center
1. Introduction
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. These activities are supported by the DB/
DA project team, the JVO project team, the HSC data analysis
and archiving software development project team, and theopen-use services team.

2. DB/DA Project
The DB/DA project conducts research and development
on astronomical Databases and Data Analysis. SMOK A(https://smoka.nao.ac.jp/) is the core of the DB/DA project andopens archival data of Subaru Telescope, Okayama 188-cm
telescope, Kiso 105-cm Schmidt telescope (the University ofTokyo), two MITSuME 50-cm telescopes (Tokyo Institute ofTechnology), Kanata 150-cm telescope (Hiroshima University),
NAYUTA 2-m telescope (University of Hyogo), and Seimei
3.8-m Telescope (Kyoto University). The total amount ofopened raw observation data in SMOKA is about 34 million
frames (328 TB) as of May 2022. SMOKA contributes to many
astronomical publications. The total number of refereed papers
using SMOKA data is 270 including 8 new publications as ofMarch 2022.
Data taken with the observing instruments VAMPIRES
and REACH attached to the Subaru Telescope and OBJECT
frames of KOOLS-IFS on the Seimei Telescope were newly
opened in FY 2021. Development of new functions requested
by users and improvements for efficient operation were also
conducted. The information on astrometric calibration of Kiso
KWFC was also opened to the public.
We are operating a system that makes original all-sky
monitor images at Higashi-Hiroshima, Okayama, Akeno,
and Kiso available to the public (https://ozskymon.nao.ac.jp/; 28 TB as of May 2022). A system to publish digitized datafrom photographic plates taken at the Kiso Observatory several
decades ago was developed and operated (https://pplate.nao.
ac.jp/ ; 4 TB). A new data service of Tomo-e Gozen (Kiso
Observatory) stacked data was opened in November 2021
(https://archive.nao.ac.jp/tomoe ; 80 TB as of May 2022).

3. JVO Project
Detection of atomic and molecular emission lines was
perfor med on the published ALMA FITS data, and theinformation on the detected lines was compiled into a databasethat can be searched on the JVO ALMA FITS archive. This
makes it possible to search for FITS data based on the emission
line information of target objects in the large amount of dataacquired by ALMA.
ALMA’s data size per file now exceeds 300 GB, withplans to deliver 1 TB of data in the future. 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 total of seven computers read FITS data in parallel andsynthesize 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
plotted in real time. The development status of FITS WebQL
was presented at ADASS 2021 and the 2022 Spring Meeting of
the Astronomical Society of Japan.
Two achievements made in the last fiscal year, the release of
the processed data obtained with the Subaru Telescope’s former
observing instrument Suprime-Cam, and the development of
the Gaia EDR3 visualization system, were reported at the 2021
Fall Meeting of the Astronomical Society of Japan. AGN survey
data from JAXA’s scientific satellite HALCA was registered in
the JVO system and was opened to the public through the VO
interface. Updates to the VO Crawler DB, a system for highspeed search of metadata for observational data collected fromVO services around the world, were implemented.
The total access count for all JVO services in FY 2021 was
7.6 million and the total download volume was 14 TB.

4. HSC Data Analysis/Archiving Software
Development ProjectThis project, started in January 2009, primarily develops
the data analysis pipeline and data archiving software for Hyper
Suprime-Cam (HSC). Our main subject is to implement thesoftware for efficient and accurate data analysis and archiving.
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 forresearchers. We made the 10th data release (S21A) to the SSP
team collaborators in June 2021, which covers roughly 740
degree2 on the sky with sufficient quality, with a total of 700
TB of files. The catalog database includes about 920 million
objects.
We have continued developing various user interface
software for providing images and catalog products. This fiscal
year, we have finished all of the originally scheduled HSCSSP observations. The next internal data release is planned
to include all data sets from the entire SSP period. We are
updating and carefully testing the pipeline for production. We
have also been supporting the on-site data evaluation for HSC
observations. We have continued development of a fast catalog
query system with a next-generation database for huge HSC
catalogs as well.
In the course of PFS commissioning, we have been
involved in discussions of data formats based on engineering

II Status Reports of Research Activities057

data, and development of science data archives in cooperation
with Subaru Telescope.

5. Open-use computer systems and services“National Astronomical Observator y of Japan: Data
analysis, archive and service system,” which is the open-use
computer system procured under a rental contract, has been in
operation since March 2018. The system plays a leading role aspart of the Inter-University Research Institute.
The system consists of “Multi-Wavelength data analysis
subsystem (M DAS)”, “Large dat a archive and ser vicesubsystem (MASTARS, SMOKA, HSC science, ALMA,
VERA, NRO, Okayama, and Solar data archives)”, “JVO
subsystem”, “Data analysis subsystem in Mizusawa Campus”,“Development subsystem”, and “Open-use terminals andprinters in Mitaka Campus”. The current system will be
replaced by a new one by the end of Feburay 2023, and we arepreparing for the replacement.
We have been constructing the “Large-scale data analysis
system (LSC)” for analyzing the big astronomical observational
data such as HSC. The LSC system has been in operation forgeneral HSC observers since September 2019. A major upgradeof the LSC system to add several computing nodes with another1,500 CPU cores was completed in 2020. A small system
upgrade continues. Starting in October 2020, the LSC systembecame available for researchers wishing to use HSC archival
data, and further expansion has been made since January2022 for those who want to use the LSC system for analyzing
observation data taken with instruments other than HSC.
As part of the tasks as an Inter-University ResearchInstitute, several workshops and hands-on tutorials were
held to demonstrate to users how to use the specific software,
applications, and the open-use systems. All workshops in FY
2021 were held online due to the COVID-19 situation. The
dates and numbers of participants in FY 2021 were as follows.
1. ALMA data analysis school (1st, Co-host), June 15–16, 2021,
12 users
2. PyRAF mini school, July 14–15, 2021, 10 users
3. SOKENDAI summer student program (provided analysis
computers), August – October 2021, 12 users
4. IDL school for beginners, September 29-30 and October 6–7,
2021, 9 users
5. ALMA data analysis school (2nd, Co-host), November 2 and5, 2021, 10 users
6. Subaru Telescope data analysis school (Co-host), November
16–18, 2021, 12 users
7. Database school for beginners, December 21–22, 2021, 12
users.
The total number of participants in the workshops andtutorials in FY 2021 was 77 users. The number of workshops
held in FY 2021 more than doubled compared to last year.

6. Others
ADC user’s meetings were held online on May 19 and058

II Status Reports of Research Activities

June 24, 2021. Since it was time to consider a replacementof the ADC open-use computer system, those meetings weregood opportunities to collect opinions from the astronomy
community on the expected role of ADC; the evaluation andissues for the current system; and requests and expectations forthe next system.
As part of outreach and promotion activities, 151 issues of“ADC News” were published from No. 1055 to No. 1206 and 28
announcements for LSC users were published from No. 40 to
No. 67 in FY 2021. These articles were distributed to users by
E-mail and posted on the ADC public web pages.

15. Advanced Technology Center
1. Summary of Activities in ATC
The Advanced Technology Center (ATC) is the core researchorganization of the technological development at the National
Astronomical Observatory of Japan (NAOJ), and is the researchand development (R&D) center for advanced astronomical
observation instruments, from radio waves to visible andultraviolet light, both on the ground and in space. In FY 2021,
as in the previous fiscal year, many ATC staff members wereforced to work from home due to the declaration of a stateof emergency in relation to COVID-19 and the subsequentissuance of priority measures to prevent the spread of the virus.
Since some staff members are required to come to work due toon-site work, as in the previous fiscal year, ATC continued tomaintain an environment where staff members can work safely
and obeyed our own COVID-19 control manual developed by
ATC last fiscal year. By sharing the manual with ATC staff, users
inside and outside NAOJ, and visitors, the measures against
COVID-19 have been thoroughly implemented. Through these
efforts, we successfully minimized delays in work in the “OpenFacility Program, Joint Research and Development Program”,
NAOJ project work such as “Prioritized Area Developments,”
and the development/manufacturing of other instruments andrelated technology for projects inside and outside of NAOJ.
The restructuring of the current organization to develop the
instruments more systematically, which has been consideredsince FY 2019, officially began operating under the neworganizational structure this fiscal year (refer to Figure 1).
In the process, several issues have been clarified, such as theestablishment of a process to determine whether or not to accept
jobs requested by external projects, and it is necessary to solve
the issues for the management of the matrix organization toestablish the new scheme.
Although the number of visitors was significantly smaller
than usual due to the COVID-19 situation, we were able to stressthe importance of ATC in NAOJ for visitors from MEXT suchas the Vice Minister, the Deputy Director-General, the Directorof the Space Utilization Division, and so on. We also provided
ATC tours for visitors from private companies and online tours
for students.
One of the most notable events in FY 2021 was theimplementation of an independent international external
evaluation of ATC. This was the first international external
evaluation conducted in six years since 2015 (the previous
evaluation was conducted as part of the international external
evaluation of NAOJ as a whole).
Details of the activities in FY 2021 are described below.

2. Prioritized Area Developments(1) TMT Instruments
1) Infrared Imaging Spectrograph (IRIS)
IRIS was in the 4th year of its final design phase, and mostFigure 1: Matrix organization structure of ATC.

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059

IRIS subsystems, including the IRIS Imager which ATC has
been developing, had their final design review. The final design
review for the IRIS Imager was held online on June 2021 with
optical design, mechanical design, thermal design, vibration,
prototyping, and systems engineering (requirements, interfaces,
verifications, integration plan) included in the scope of thereview. The review follows the TMT standard, i.e., after deliveryof the review documents, in-depth pre-review discussions using
an online discussion tool were organized, and the 3-day review
was focused on topics that were not settled in the pre-review
discussion. While our quality deliverables were highly creditedby the review committee, we also received some honest criticalcomments. The review was an invaluable opportunity to collectfeedback from experts for designs that were nourished and built
up throughout the final design phase. The remainder of this year
was devoted to closing action items that were pointed out in thereview panel report such as vibration analysis, opto-mechanicalthermal analysis, and stray light analysis.
2) Wide Field Optical Spectrometer (WFOS)WFOS successfully passed the conceptual design review in
February 2022 and is going to the preliminary design phase from
April 2022. NAOJ conducted the design studies on the slit mask
exchanger, the slit mask fabrication system, and the integral field
unit (IFU). Details are as follows.
i) In terms of the slit mask exchanger, we developed several
exchange methods and selected the most suitable method
based on a trade study considering their exchange times andmechanical complexities. In addition, we modified the design
considering safety for operators.
ii) There are two possible locations for the slit mask fabrication
system: the summit and the base facilities. A trade study about
the location was conducted. The final decision will be made in
the next phase.
iii) The IFU optical design was modified in response to the
WFOS design modification. A new IFU mode with a narrower
slicer was studied. We proceeded with optical design of atechnology validation IFU which will be installed into theoptical spectrograph, FOCAS, on the Subaru Telescope.
iv) We summarized the conceptual study reports on the slit mask
exchanger, the slit mask fabrication system, and the IFU, andestimated their costs and development schedules.
(2) ALMA
1) ALMA Receiver Maintenance of Bands 4, 8, and 10
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

060

II Status Reports of Research Activities

2014. In FY 2021, one Band 4 receiver was repaired anddelivered to the ALMA Operations Support Facility (OSF) in
Chile. Currently, one Band 4 receiver and one Band 10 receiver
have been sent back from Chile for repair, and are in the processof being repaired, which will be completed in the next fiscal
year. The receivers installed in antennas and scheduled to be
repaired are one Band 4 and two Band 10 receivers. They will
be removed from the receiver systems in the course of regular
maintenance, and will be returned for repair in the next fiscal
year or later.
Although the frequency of repairs caused by aging failure
is currently kept low, an increase of the failure rate cannot
be denied when the wear failure period begins according to
the bathtub curve. In order to continue the stable operation of
ALMA, it is important to maintain a maintenance system in ATCthat can quickly respond to ALMA receiver failures.
To address the issue of long-term maintenance work,
multiple persons were assigned to disassemble/ assemble
receivers and conduct comprehensive evaluation tests forrepaired Band 4 receivers to increase the number of experienced
persons, record videos, improve procedures, and updateprocedure manuals. In addition, a remote conference system andremote operation of measuring equipment were used to provide
instructions for key tasks and to discuss interpretation of the test
results from receiver maintenance specialists working in remotelocations.
The ALMA receiver maintenance team in ATC worked
together with a 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 upgrade
For development and upgrade of heterodyne receivers,
we focus on two main activities in close coordination with the
NAOJ ALMA Project. Firstly, we are involved in international
collaboration for the development of ALMA receivers for thefrequency bands not implemented in the array yet: Band 1 andBand 2. Secondly, we have engaged in receiver development to
upgrade the ALMA telescope system in three main directions:wideband, terahertz, and multibeam receivers based on
microfabrication technologies.
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 a contribution to East Asia ALMA is in the middle of the
production phase. We have been contributing to the testingand production of corrugated horns, the support for cryogenic
maintenance of cryocoolers at ASIAA, support for procurement
and shipping of several important components, and support for
shipment of receivers in cooperation with the NAOJ ALMA
project. To ensure the smooth logistics from ASIAA to Chile,
NAOJ has lent out 14 shipping containers in addition to twothat had been already used. As of the end of FY 2021, ASIAA
has completed production and in-house testing of more than

50 receivers, and the receiver acceptance in the ALMA OSF,
and Assembly, Integration and Verification (AIV) activities areaccordingly proceeded with the Joint ALMA Observatory.
Following from last FY, corrugated horns have been
fabricated with the metal 3D printer and evaluated in close
collaboration with the Manufacturing Design Group at ATC.
In this FY, thanks to investigation of the 3D printed metal
properties for the purpose of practical use in a cryogenic
receiver, optimization of the fabrication method and process,and the detailed characterization of the corrugated horn, we
have successfully manufactured the 3D printed corrugated horn
products that meet the ALMA Band 1 receiver requirements.
Accordingly, NAOJ held an internal review with ALMA partners
about the 3D printed corrugated horn to be implemented into
the ALMA Band 1 receivers. We have completed the RF testingat ATC and shipment of the 3D printed corrugated horns. They
are being integrated on the Band 1 cartridge receivers and thefinal cryogenic performance test in-house will be conducted
in ASIAA in FY 2022. NAOJ will also be in charge of Band 1
receiver maintenance in the operation phase, and therefore, theorganization and facility for the maintenance will be establishedtaking over from ASIAA from the end of FY 2022.
We have contributed to the Band 2 project (67–116 GHz)
led by the European Organization for Astronomical Researchin the Southern Hemisphere (ESO) with the design, fabrication,and testing of waveguide components and receiver optics basedon a dielectric lens. For the Band 2 receiver preproduction (first
6 receivers) initiated in April 2019, NAOJ has manufactured
optics and waveguide components including a corrugated horn,
circular-square waveguide transition, and waveguide orthogonalmode transducer (OMT). Their RF characterizations have been
performed at room temperature, and 4 Feed-OMT assemblies
have been initially delivered to ESO for preproduction receivers.
For the remaining assemblies, detailed verification has been
conducted with respect to the RF evaluation. For the dielectriclens development, we have investigated the materials interms of low loss properties and stability for machining andoperation. The material candidates have been verified to checkthe influence of ultra-violet irradiation on the mechanical andelectric properties. For the material properties, we have used thematerial characterization system established at ATC based on
the free-space method and have obtained repeatable and reliablemeasurements. In close collaboration with the Manufacturing
Design Group, the precision test pieces could be fabricatedby a combination of normal and ultra-precision machining
equipment. Thanks to these activities, we could obtain accurate
and useful evaluation results for the material selection. The Band
2 project plans to hold the critical design review in April 2022.
NAOJ has created the reports for detailed design verification of
optics components and optics design based on evaluation resultof the lens material.
2-2) Development for the next generation projects
Wideband receivers are being developed for ALMA Band 8
receiver upgrades. In this FY, we have designed and fabricated a
corrugated horn and OMT implementing the recent technology

development in collaboration with NICT. We also have designed
a sideband separating mixer module that integrates waveguidecircuits, mixer chips, and IF cryogenic amplifiers into asingle block in collaboration with the University of ElectroCommunications. Besides, for practical use of double sideband(DSB) mixers in this frequency band which has been developed
until last fiscal year, we have provided the DSB mixers todomestic universities and institutes such as Keio University/
ASTE project, the University of Tsukuba/Kwansei Gakuin
Universities, and the University of Electro-Communications/
RIKEN, and supported their installation and experiments in theirlaboratories. NAOJ has also collaborated with Osaka Prefecture
University on the development of Band 6+7 (211–373 GHz)
receivers. In this FY, we have successfully demonstrated thequantum limited performance over the IF 4–20 GHz across the
RF range. This is the first demonstration of the wide IF mixer
in this RF range, building on our success in the Band 7+8 (275–500 GHz) mixers reported in past years.
As for the terahertz technologies, we have designed andfabricated a two-layer anti-reflection structure on a silicon
substrate in collaboration with the Microfabrication Laboratory.
The fabricated one showed low-loss transmission characteristics
across the Band 10 frequencies. This development will be
continued towards practical use as a vacuum window forcryogenic receiver installation.
The multibeam heterodyne receiver technology basedon monolithic microwave integrated circuits (MMIC) was
further investigated in terms of transmission loss and its
impact to sensitivity. An innovative method based on on-chipresonators was applied to accurately measure the transmission
loss of superconducting thin film transmission lines adopted
in the MMICs. The results showed reasonably low loss andprovided favorable evidence that justifies the application ofsuperconducting MMIC technology at millimeter frequencies.
In the Microfabrication group, we maintained the fabrication
capability for Nb/Al/AlN x/Al/Nb junctions with unusuallyhigh critical current density, which is the crucial requirement
for broadband SIS receivers. We also proceeded with theinvestigation into fabrication of MMIC-type SIS mixers andanti-reflection surfaces based on the silicon micromachining
technique. With these activities, the foundation is now in place
for the stable production of high-quality devices for future
ALMA development.
(3) KAGRA
In collaboration with the Gravitational Wave Project, we aredeveloping vibration isolation systems (VIS) and auxiliary optics
systems (AOS) of the KAGRA interferometer, and preparing
instruments for evaluating the performance of its mirrors. Herethe AOS includes optical devices or elements required forcompleting the interferometer, such as optical baffles to mitigate
stray light effects, optical angle sensors, beam reduction optics(BRT), cameras for beam monitoring, and viewport windows. At
the Kamioka site, overhauling the interferometer has continued
since the last fiscal year as quickly as possible in order to beready by the start of the 4th international gravitational-wave

II Status Reports of Research Activities

061

observation run (O4; to start December 2022 or later). ATCcontributed to this activity by assembling and delivering some
AOS instruments such as a balancer for the vibration-isolation
stage of the BRT, mechanical covers for the optical angularsensors, and their optical filters. We also responded quickly to
one of the unexpected issues in the VIS instruments during theoverhaul work. In addition, we continued to develop the mirror
performance evaluation system.
(4) Next-generation Solar-observing Satellite: Solar-C (EUVST)
ATC has supported the SOLAR-C project in completing thedesign study of the EUVST spectrometer and contributed to theinterface coordination between the main instrument structure
and the components being provided by overseas partners. In
addition, ATC has helped to prepare cleanroom facilities with acoelostat system that introduces the sunlight into the cleanroom
for instrument calibration, vacuum chambers of various
volumes, and contamination monitoring systems planned 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 (DBA) for holding and cooling the detector.
The detector is a near-infrared detector using an InGaAs
device and is being developed by the Optical Infrared Mission
Instrument Team of the Advanced Mission Instrumentation
Group. The status of the development in FY 2021 is described in
section 3(2).
The DBA is being developed by the Thermal and Mechanical
Design Team of the System Design Group, and in FY 2021, theteam was able to demonstrate a feasible architectural design, andthermal and structural analysis in a conceptual study.

3. Advanced Technology Development(1) Terahertz Technology
The terahertz experiment group supports development ofsuperconducting detectors, cryogenic electronics, and cryogenic
systems. Development of SIS photon detectors in collaboration
with the National Institute of Advanced Industrial Scienceand Technology (AIST) continued to improve the quantum
efficiency of detectors with electromagnetic simulations
using HFSS and FEKO software. A new development
program for 1.5-THz SIS photon detectors was initiated using
superconducting thin film facilities in ATC. Construction andimprovement of two cryostats, one for photon statistics anotherfor intensity interferometry, resulted in the good cryogenic
performance required for optical experiments in the following
year. Development of an MKID camera in collaboration with
the University of Tsukuba has advanced by evaluation of test
observation data followed by scientific observation of a starforming region using the Nobeyama 45-m Radio Telescope.
Evaluation of anti-reflection coating of silicon opticalcomponents using subwavelength structure was performed using
the submillimeter-wave Fourier transform spectrometer, theresults of which were published in Hasebe et al. (2021).

062

II Status Reports of Research Activities(2) Near-infrared Image Sensor
Image sensors for astronomical observation need extremely
high performance, such as low noise, to detect faint objects.
Near infrared image sensors for astronomy were only available
from one company in the US until now. Since an image sensor isthe heart of a scientific instrument, image sensors manufactured
by a domestic company are highly desired especially for a space
application to be able to proceed independent of foreign groups.
We have successfully developed a near infrared image sensor incooperation with a domestic company for a Subaru Telescope
instrument proposed by us. In this year, we worked for fixing
the specifications and design of a new domestic image sensor to
be widely applicable for space use funded by the Front Loading
program of JAXA’s Institute of Space and Astronautical Science.
The sensor will also achieve several performance improvements
such as better sensitivity at the same time. The first prototype
is planned to be manufactured next year. The new sensor has
already been adopted by the JASMINE project instead of the
US sensor. We also evaluated the effect of proton radiation on
an InGaAs sensor in cooperation with the JASMINE group,and found it was within an acceptable range for the JASMINE
project.
(3) Near-infrared Multi-object Spectrograph: SWIMS-IFU
ATC, in cooperation with RIKEN and Institute of
Astronomy, the University of Tokyo has been developing anear-infrared integral-field spectroscopy unit (IFU) using ultraprecision cutting technology.
It is designed to be installed on the near-infrared multiobject spectrograph SWIMS, which is operated at the Subaru
Telescope as a PI instrument since 2021. Its optics consists ofmore than 70 small mirrorlets of a few mm square. It divides
the 14 x 10.4 arcsec field of view into 26 slitlets of 0.4 arcsec
width, and spectra in the wavelength range of 0.9–2.5 μm can beobtained with a single exposure.
The problems in its development are how to suppress theeffect of thermal deformation when cooling the whole systembelow 150 K to suppress thermal radiation, and how to align theaxes of the many mirror surfaces. We are trying to solve these
problems by making the entire structure out of aluminum alloy
and using ultra-precision machining technology to cut and form
all the mirror surfaces directly from the aluminum base material.
In FY 2021, we completed all of the mirror processing using
RIKEN's ultra-precision machine. After assembly and testing at
ATC, the IFU were transported to Subaru Telescope, installed on
SWIMS, and successfully saw first light at the end of March. As
a result, it was confirmed that the performance of the IFU mostly
complies with the requirements.
(4) Sounding Rocket Experiment: CLASP2.1
The CLASP 2.1 project began full-scale preparations forthe launch, which was scheduled for the fall of 2021, andATC supported the planning of operations at the launch site.
Particular attention was paid to the risk assessment for the reflight of the instrument and the investigations of measures
to be taken at the launch site. With these and other carefulpreparations, the month-and-a-half long activities at the launchsite went generally smoothly, and CLASP2.1 was launched on
October 8, 2021 (local time) at the White Sands Missile Rangein the United States. Both the sounding rocket and instruments
performed flawlessly and successfully scanned the active region
for approximately 6 minutes.
(5) US-Japan Solar Flare X-ray Focusing Imaging-spectroscopic
Sounding Rocket Experiment: FOXSI-4
FOXSI-4 is being prepared for the launch in the spring of
2024. ATC is supporting the development and evaluation ofhigh-speed cameras for soft X-rays using back-illuminated
CMOS image sensors and a pre-collimator fabricated by themetal 3D printer. In FY 2021, a reflective type light reduction
system using mirrors was developed for evaluation of CMOS
sensors using a synchrotron radiation beam. This system
overcomes the weakness of the conventional transmissiontype attenuation method using filters (where contamination byhigher-order wavelengths is inevitable) and enables us to easily
obtain monochromatic X-rays with an appropriate flux, thus
establishing an ideal evaluation method for CMOS sensors. In
addition, FOXSI-4’s camera system was started to be developedby the Optics Engineering Team of the System DesignGroup. In the development of the pre-collimator, the Additive
Manufacturing Engineering Team of the Manufacturing
Design Group started to take a development policy thatwould contribute to the advancement of the metal 3D printertechnology.
(6) Balloon-borne Solar Observatory: SUNRISE-3/SCIP
For the SUNRISE-3 balloon experiment, NAOJ leads thedevelopment of a near-infrared spectro-polarimeter called
SCIP. The optical unit of SCIP was designed and developedat ATC to achieve high imaging, spectral, and polarization
performance in the thermal vacuum environment during theballoon f light. To repair a problem with the CMOS camera
installed inside, the SCIP optical unit was reassembled andtested for imaging and polarization performance at the ATC
clean-room, and the thermal, electrical, and optical functions
were verified in vacuum using the ATC large space chamber.
The SCIP development at NAOJ was completed in August
2021, and tests combined with the SUNRISE--3 1-meter
aperture telescope were conducted in Germany. A paper isunder preparation on the results of opto-mechanical design andanalysis obtained in the development of SCIP.

4. System Design GroupT h e Sy s t e m D e sig n G r ou p d e sig n s a n d d e velo p s
instruments for various astronomical projects and supports
the planning and implementation of instrument performanceverification. The System Design Group consists of three teams:
thermal and mechanical engineering, optics engineering, andsensor engineering. From this year, the teams for instrument
development have been organized into one group, enabling
closer cooperation. In particular, thermal and mechanicalengineering and optical engineering are inseparable in
instrument development, and we have taken the first step
toward optomechanical design that handles them in a unified
manner.
(1) Thermal and Mechanical Engineering TeamThe team continued the mechanical design and related
tests of TMT/IRIS, TMT/WFOS, TMT/STR, KAGRA, Solar-C(EUVST), SUNRISE-3, and CLASP2.1 from the previous fiscal
year. In addition, the design study of JASMINE was newly
started this year.
The TMT/IRIS Imager team successfully passed the final
design review in June after a two-year final design phase andcontinued to address the issues raised by the review board.
Specifically, we created an FE (Finite Element) model of theentire Imager for vibration and thermal analysis, optimized thedesign of the ADC prism support mechanism, took measuresagainst thermal stress in the Imager mounting bracket, andconducted a lifetime test of the slicer pick-off mechanism.
Conceptual design of the slit mask exchanger and slitmask
fabrication facility was conducted for TMT/WFOS. Afterdeveloping multiple concepts and discussing their tradeoffs, the functional and physical designs were completed
and reported in the WFOS conceptual design review held in
February 2022. In addition, a cost evaluation of the future
design phase was provided for TMT internal reviews.
TMT/STR finalized the interface documentation, drew theISS and cooling system platforms, and supported the design
review board for the piping and wiring subsystem (TUS) forthe manufacturing readiness review scheduled before the startof the manufacturing process. In addition, an interim review
meeting for the primary mirror replacement system (SHS) was
held to prepare for the pre-production review meeting.
At KAGRA, a movable mass balancer was installed on thetransmission monitor system on the vibration isolation stage
and its performance was confirmed. Functional improvements
were also made through the design of various hardware andmodification of the control program. In addition to the above,
improvements and modifications were made to the antivibration system and auxiliary optics for O4 observation at thesite. Reinstallation of the Type-A (Y-end) vibration isolator
was almost completed, and adjustment of Type-B (BS and SR
systems) and Type-Bp (PR system) was also completed. In
addition, an earthquake and other problems were addressed.
Our contribution has also advanced the conceptual studyof the Solar-C(EUVST) mission payload, particularly for thetelescope structure including analytical estimation of opticalelement deformation and mechanical interface control withcomponents which will be provided by international partners.
For the solar sounding rocket and balloon-borne experiments,
we supported the shipping of SUNRISE -3/SCIP and the range
operation planning for CLASP2.1.
In JASMINE, we were in charge of the thermal andstructural design and analysis of the detector box (DBA) during
the conceptual phase and confirmed its feasibility. In addition,
we developed test equipment to investigate the performance

II Status Reports of Research Activities

063

characteristics under the operational environment (around200 K) of the TEC, which is being considered as one of theelements.
(2) Optics Engineering TeamThe Optics Engineering Team is responsible for the developmentof optical systems and coating for astronomical instruments.
1) Development of optical systems
The team has been involved in numerous astronomical
instr ument projects in NAOJ, universities and research
institutes, and has contributed to their development through its
optical design to its performance verification. In FY 2021, theteam contributed to NAOJ projects such as Solar-C(EUVST),KAGRA, SUNRISE-3, and TMT/WFOS. In addition, the teamcontributed to the following collaborative research projects: (1)development for the focal plane instrument for the Antarctic
submillimeter-wave telescope, (2) development of the IFU
for a Seimei Telescope instrument, (3) feasibility study of alarge space telescope using a group of microsatellites, and (4)performance evaluation of the Gregorian reflecting telescopebuilt in the Edo period. In addition to developments, theteam collects development needs from several projects andconducts activities to introduce the optical equipment neededin the future. In FY 2021, we procured the parallel plane-platemeasurement option and the ultra-high-precision reflective/
transmissive flat for the high-precision Fizeau interferometer.
2) Development of coating
Fundamental experiments continued for improving coatings
using inhomogeneous multilayers. The coating process monitor
was renewed and improved, and various data as to the relation
between the status of the coater and the film characteristics
were obtained for longer processes in detail. A number ofexperiments modifying the ion-source electrodes to improve
long-time stability of the beam current and its profile have been
undertaken. And improvements of the control software havecontinued.
(3) Sensor Engineering TeamThe Sensor Engineering Team consists of engineers
who have been involved in the development of detectors andreceivers for both domestic and international astronomical
instruments. Specifically, the team has contributed to thedesign, development, and manufacturing of ALMA Band 1 andBand 2 receiver components; maintenance of ALMA receivers(Band 4, Band 8, and Band 10); micro-fabrication based onsuperconducting SIS devices; and the IPMU PFS project at the
University of Tokyo. The development of detectors requires
not only a single technology, but also the ability to deal withvarious technological areas such as electronics, mechanics,
vacuum, and cryogenics. We will contribute to the developmentof astronomy with these comprehensive capabilities.

5. Manufacturing Design Group
The Manufacturing Design Group engages in a064

II Status Reports of Research Activities

comprehensive 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 this fiscal year, the AM Engineering Team,now in its second year of operation, responded to several
requests. And the whole group had the opportunity to study andimplement the process from additive manufacturing to finishingkey parts such as interfaces by machining. We also work with
the Thermal and Mechanical Engineering Team of the System
Design Group on fabrication work.
One engineer was assigned to the project (June 2021).
(1) Machining Engineering TeamThe Machining Engineering Team has responded tofabrication consultations and fabrication requests ranging frommajor NAOJ projects, groups at ATC, and open-use users.
And, for users who wanted to work on their own, we provided
guidance as needed. In addition, the 5-axis machining center
is now in regular operation, and an ultra-high-precision wire
electrical discharge machine was newly introduced and put into
operation (March 2022).
The main requests are as follows:i) Regarding TMT/IRIS, fabrication of parts for element tests isbeing conducted by the Thermal and Mechanical Engineering
Team of the System Design Group.
ii) The fabrication of the mask frame for the near-infrared multiobject spectrograph SWIMS, to be mounted on the Subaru
Telescope, was completed (continued from the previous fiscal
year).
iii) Post-processing of metal 3D printer modeling for corrugatedhorns for ALMA Band 1 receiver, and KAGRA QPD circuit
covers.
iv) Fabrication of a folding pendulum for KAGRA was started (tobe continued in the following fiscal year).
As for fabrication by the Ultra-Precision Section, we havebegun processing thin polyethylene sheets to be used as samples
for material property tests in the ALMA radio frequency range.
The work will be carried over to the next fiscal year since thenumber of samples is too many for ultra-precision processing,but some completed samples have already been delivered.
(2) Additive Manufacturing (AM) Engineering TeamAs in the previous fiscal year, the AM Engineering Team has
continued to learn about AM techniques including operation of
the 3D printer and peripheral equipment, and modeling design.
FY 2021 was the second year of operation phase for
AM Engineering Team, and we proceeded to develop andmanufacture ALMA Band 1 corrugated horns which are set
as the first item for the NAOJ AM Team. In this fiscal year,
the detailed material property verification and fine-tuning of
manufacturing parameters were conducted, and finally, we
succeeded in making a component that completely meetsspecifications. This Fiscal Year, 32 horns were manufactured

as production components, and delivered to the NAOJ ALMABand 1 team. Of particular note, in the material property
verification we checked the effect of the thermal stress in the
production component and annealing as a post process of the
manufacturing for releasing the thermal stress, and reported theresults in the 41st Symposium on Engineering in Astronomy.
The electric board case for KAGRA, which like the ALMABand 1 components is also a continuing item, proceeded to makea trial for checking the design and fitting for mounting. Then,
18 of the cover were manufactured and delivered. Through thismanufacturing, we considered the design which allows onetouch assembly and disassembly despite being made of metal,
and surface treatment which is suitable for putting inside of
KAGRA.
As for new items, consideration and manufacturing of
the first trial for some of the waveguide components werestarted, drawing on the experience gained through ALMA horndevelopment. In addition, R&D collaboration was started with
JAXA, the University of Tokyo, and Cybernet Systems Co., Ltd.,in order to get deeper knowledge and apply it to astronomical
observation devices. These new items will be continued to thenext fiscal year.
(3) Measurement and Evaluation TeamThe Measurement and Evaluation Team makes full use
of various measurement instruments to verify and confirm
the accuracy of products by the Machining Engineering Teamand AM Engineering Team. In addition, LEGEX910, a large
3D measurement machine managed by the Management
and Administration Group, is used to respond to requests
for measurements for open use. In FY 2021, in addition to
the usual evaluation, verification, and response to requests
for measurement, to augment the team, our staff attended
a measurement workshop for LEGEX910 arranged by theManagement and Administration Group and started on-the-job
training
The request for fabrication and measurement in FY 2021 arelisted in Table 1.

6. Management and Administration GroupAs part of the reorganization of ATC, the Management
and Administration Group has been established. The groupconsists of the Facility Management and Operation Team, theAdministration Team, and the IT Support Team. The Facility
Management and Operation team was reorganized fromthe former Facility Management Unit, Space Chamber andSpace Optics Shop, and Optical Shop. The Management andAdministration Group will support the smooth progress ofprojects from within ATC and NAOJ as well as for open-use
research.
Facilities for open-use research are currently managed withthe minimal personnel. ATC will discuss how much personnel
will be allocated in the future.
Operation of the facilities for Fiscal Year 2021 are as
follows:

Table 1: The requests for fabrication and measurement in FY 2021.
From FY 2020

5

FY 2021
Advanced Technology Center
ALMA, ASTE
TMT/IRIS, Subaru Telescope
KAGRA
Solar science, SOLAR-C, FOXSI-4
RISE
JASMINE
Public Relations Center
Astrobiology Center/Exoplanets
Others

16
12
8
4
5
3
1
1
2
2

External Organizations
University of Tokyo (TAO, SWIMS)Osaka Prefectural University
Oita University
Total
To FY 2022

7
1
1
63
5

(1) Optical shop
1) Management
At the Optical shop, measurement equipment suchas non-contact and contact 3D measurement machines,
spectrophotometers, and microscopes are available for open use.
The equipment maintenance, including daily inspections, andtechnical consultations for measurement were provided, andthis fiscal year, we arranged a workshop at the request of the
Measurement and Evaluation Team of the Manufacturing DesignGroup.
2) Repairing and upgrading for measurement systems• Replacement of Spectrophotometer (UV-3600iPlus)
3) Arrangement of workshop• LEGEX910 measurement workshop (December 2021),
attendance: 34) Open use• The number of annual users: 199
NAOJ: 132 (including 114 from ATC)
External organizations: 67• Use of LEGEX910 (large 3D measurement machine): 37(including 19 from the Measurement and Evaluation Team of
the Manufacturing Design Group.)
Number of operating days: 43• Technical consultation and troubleshooting: 21(2) Space Chamber
As project support, we have participated in development
activities of the balloon experiment Sunrise-3. We contributed
to the preparation and operation of equipment for a thermal
vacuum optical test of the SUNRISE-3/SCIP using a large
space chamber in a clean room. We have also assisted the Solar-

II Status Reports of Research Activities

065

C(EUVST) and the JASMINE Projects to conduct experiments
using vacuum chambers in ATC.
In terms of equipment management, a dry vacuum pumpfor a large space chamber was overhauled in preparation for
future environmental tests of a satellite telescope. In addition,a new high/low temperature bath circulator used for thermal
vacuum tests was introduced due to the failure of the previous
one. Software for the measuring instruments was continuously
developed and operated, and new functions were added in
response to user requests.
(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 the overall
repair plan, including construction and hazardous materials
for laboratories including clean rooms (CR). In addition, CE
practical skills training was conducted as appropriate among thesafety training courses. To correct the concentration of inspection
workload on certain members of the team, we promoted theacquisition 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. In
addition, we gave a talk about COVID-19 preparedness at the17th NIFS Workshop on Industrial Safety and Health.
After the renovation of the SIS CR two years ago, we have
had problems such as temperature anomalies in the CR and fan
filter unit (FFU) stoppage. The temperature anomaly in the CR
was improved by modifying the temperature control parameters.
And we tried to reduce the load on the FFU, such as changing
the air supply position by root change, to improve the FFU
stoppage. However, the FFU stoppage problem was not solved,
so we will continue to investigate the cause of the FFU stoppage.
In addition, the circulating cooling water pipelines in particularbuildings were inspected and cleaned to reduce deterioration ofwater quality.
To accommodate the increase in the number of staff in ATC,a CR and the electronics shop were converted into office rooms,
and the facilities in the previous rooms were relocated to otherrooms.
Promoting the ALMA 2 project, we planned to expand
the existing SIS CR. Since the conventional vertical laminarflow CR could not provide the necessary ceiling height for the
installation of process machines after the renovation, we planneda side laminar flow CR in this facility.

7. Open-Facility Program, Joint Research andDevelopment Program
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 developmentwith ATC members.
In FY 2021 we made calls for these programs twice, then066

II Status Reports of Research Activities

accepted 20/3 Joint Research Development programs in thefirst/last calls, and 13 Open Facility programs.
Due to COVID-19, visits of external researchers to ATC
were significantly restricted since FY 2020, however, we
resumed the use of the facility with high urgency by taking
countermeasures against infection.

8. International External Evaluation
The international external evaluation was conducted as
an online meeting in March 2022. The evaluation committee
consisted of six reviewers from four countries (Japan, the U.S.,
Italy, and Australia), including two women. In this evaluation,
ATC’s activities over the past five years were assessed from thefollowing five perspectives and evaluation criteria.
1) Are the goals of ATC appropriately defined in line with thethird mid-term goals of NAOJ, and is the organization being
managed in an appropriate manner?
2) Does ATC produce internationally outstanding results,
especially when compared to the size of the center?
3) Does ATC contribute to the creation of results in accordancewith NAOJ’s third mid-term plans?
4) As an Inter-University Research Institute, does ATC
cooperate with universities and other organizations tocontribute to their achievements and the development ofyoung researchers?
5) Does ATC respond appropriately to the evaluation results?
The review meeting was held online due to the COVID-19
disaster. However, since the participating members werelocated in multiple time zones (Japan, the U.S., Europe, andAustralia), it was not possible to hold a long meeting in one
day, so the meeting was held over three days in short sessions.
The virtual lab tour was also very well received, as it allowed
for a real-time question-and-answer session to be conducted as
appropriate, with an explainer guiding the participants throughthe interior of ATC with a camera.
As a result of the review, we received ‘Excellent’ for criteria(2) and (3), and ‘Excellent/Good’ for (1), (4), and (5). The mostimportant thing was that we ourselves objectively recognized
the achievements of our activities. We will work earnestly toresolve the issues that were pointed out by the review board.

16. Public Relations Center
1. Overview
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 7 offices,
1 unit, and 1 observatory: the Public Relations Office, theOutreach and Education Office, the Spectrum Management
Office, the Ephemeris Computation Office, the Library Unit,
the Publications Office, the IAU Office for Astronomy Outreach(OAO), Ishigakijima Astronomical Observatory, and theGeneral Affairs Office.

2. Personnel
In FY 2021, the Public Relations Center was composed of
Director Hitoshi Yamaoka and the following staff members: 2
project professors, 2 associate professors, 2 assistant professors(each holds concurrent posts), 1 research engineer, 1 engineer,
1 unit leader, 6 senior specialists, 3 project research staff
members, 2 research experts, 2 administrative experts, 2
research supporters, 14 public outreach staff members, and 3
re-employment staff members.
On April 1, research supporter Shizuka Nakajima arrived
in the IAU Office for Astronomy Outreach.
On May 1, project researcher Takashi Shibata arrived in the
Ephemeris Computation Office.
On June 1, senior lecturer Masaaki Hiramatsu arrived in
the Spectrum Management Office.
On August 31, senior specialist Kumiko Usuda-Sato (Public
Relations Office) and senior specialist Hansen, Izumi Ka Hoku
Hula O Kekai (IAU Office for Astronomy Outreach), resigned.
On September 1, senior specialist Hiroko Komiyama
arrived in the Public Relations Office.
On September 11, senior specialist Hiroko Tsuzuki (Public
Relations Office) resigned.
On November 1, senior specialist Filipecki Martins Suzanaarrived in the IAU Office for Astronomy Outreach.
On February 28, project research staff Member Takashi

Horiuchi (Ishigakijima Astronomical Observatory) resigned.
On March 1, senior specialist Blumenthal Kelly arrived in
the IAU Office for Astronomy Outreach and project researchstaff member Hidekazu Hanayama (Ishigakijima Astronomical
Observatory) advanced to senior lecturer.
On March 31, unit leader Mizuho Tamefusa (Library)
resigned.

3. Public Relations OfficeThrough press conferences and web releases, the Public
Relations Office actively developed public outreach activities
focused around the results of each research project, first andforemost ALMA and Subaru Telescope, including open-use
and collaborative results with other universities and research
institutes. In addition, our office hosted lectures to publicize
cutting-edge astronomy. In cooperation with the Outreachand Education Office, the Public Relations Office also created
content that explains various astronomical phenomena.
We conduct not only public outreach activities using social
media and video streaming services, but also 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.
(1) Online-Based Information Sharing
The Public Relations Office runs the NAOJ website (https://www.nao.ac.jp/en/), disseminating information via the internet.
Table 1 shows the access counts for the website.
The Office opened Twitter, Facebook, and Instagram
accounts in both Japanese and English sequentially from2010, actively disseminating information on social networking
services. Our office disseminates information on the status ofvarious NAOJ projects such as public visits, regular stargazing
parties at Mitaka Campus, and position openings, both inEnglish and Japanese. As of the end of March 2022, we haveover 240,000 followers on our Japanese Twitter accountand over 8,800 followers on our English Twitter account.
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.227–236 were issued,
introducing research results and NAOJ hosted events. A total ofMonth

Access counts

MonthAccess counts

MonthAccess counts

April 2021

534,726

August 2021

1,042,804

December 2021

1,280,021

May 2021

1,184,064

September 2021

1,088,705

January 2022

897,306

June 2021

605,150

October 2021

877,586

February 2022

549,401

July 2021

762,820

November 2021

1,457,828

March 2022

423,532

Total: 10,703,943
Table 1: Monthly website access statistics for the Public Relations Office website, NAOJ Public Relations Center (April 2021–March 2022).

II Status Reports of Research Activities067

10,967 subscription addresses have been registered as of March
31, 2022.
We continued to produce videos explaining astronomical
phenomena and research results, and videos introducing
outreach activities. Including English versions, 23 originalvideos were produced (Table 2). The videos are uploaded
mainly on YouTube. During FY 2021 these videos accumulated
a total of 5.92 million hours of play time (2.39 million hours
in FY 2020) and 9.24 million views (3.75 million views in FY2020). Both figures represented an approximately 2.5-foldincrease compared to those of the previous fiscal year.
“Gravitational Wave Telescope K AGR A―Revealing
the Universe Through the Cur vat ure of Space-time,” avideo created this fiscal year, received the Science Museum
Director’s Award at the 63rd Science and Technology Film/
Video Festival. We also focused on livestreaming. We received
positive feedback for our live stream of celestial bodies with the
50-cm Telescope for Public Outreach, and of a lunar eclipse,
which was observed simultaneously from three locations:
Mitaka Campus, Ishigakijima Astronomical Observatory,
and the Subaru Telescope. In addition to uploading videos on
our YouTube channel, we have been approved as an official
program by DWANGO Co., Ltd., which manages niconico
Live, a video streaming service, and our viewers are increasing.
The livestream of the total lunar eclipse on May 26, 2021,
attracted 425,128 viewers and the recorded video achieved over
2.20 million views. The recorded video of the partial lunar
eclipse livestream from November 19, 2021, also garnered
nearly 300,000 views. These high numbers of views are likely
due to people staying at home during the lingering novel
coronavirus (COVID-19) pandemic. From November 2020 to
December 2021, an online mini-lecture for elementary school
students was delivered once a month. In addition, explainer
videos were created before the lunar eclipses. Nobeyama Radio
Observatory Special Open House Day and Mitaka Open House
Day were both held online and livestreamed.
(2) Research Result PR
There were 23 research result announcements (compared to

30 in FY 2020 and 33 in FY 2019). We released all the researchreleases in both English and Japanese. For domestic audiences,
we have continued to organize press conferences, as well as
mail press releases to an original media list. For press releases
aimed towards overseas audiences, we have continued to use
the delivery services of AlphaGalileo, and EurekAlert! from
AAAS, and mail press releases to an original media list.
This fiscal year, no sessions of “Astronomy Lecture for
Science Journalists” were held.
(3) Activities as NAOJ’s Public Relations Center
The following activities were pursued in addition to theCenter’s regular task of aiding research result releases.
We have started a Public Relations blog since May toprovide various information related to astronomy and NAOJ.
By March 31, 45 articles were posted and viewed a total of
450,000 times.
The Public Relations Office organized the 33rd National
Institutes of Natural Sciences Symposium “The Universe,
Molecules, and Us.” The lectures by 4 speakers were held
online on NAOJ’s official YouTube channel on March 13, 2022.
The live event was viewed by up to 393 simultaneous viewers,
and its video archive was viewed over 20,000 times by April
21. To raise NAOJ’s international profile, we regularly holdbooths at international meetings where the press, researchers,
and educational officials gather. This fiscal year, we held thesponsored session “KAGRA, Japan’s Large Gravitational Wave
Telescope” at the European Astronomical Society Annual
Meeting 2021 (EAS 2021) on June 28, 2021, and this session
was attended by over 70 people. We also hosted an online
exhibition booth at the 2022 AAAS Annual Meeting (AAAS
2022, held online from February 17 to 20). This booth featured
the English versions of videos we have produced so far anddownloadable content, such as the Four-Dimensional Digital
Universe Viewer Mitaka, in addition to materials describing
NAOJ’s projects.
We also worked to enrich the existing web content by
creating interview articles for four staff members; revamping
NAOJ VR, a 360-degree panorama viewer that enables users

Astronomical Event Information Movies (April 2021 to March 2022, uploaded monthly, totaling 12 videos) Japanese Version
Let’s Watch the Total Lunar Eclipse on May 26, 2021

Japanese Version

Gravitational Wave Telescope KAGRA―Revealing the Universe Through the Curvature of Space-time

Japanese Version

NINS Young Researcher Award Lecture

Japanese Versions

How to Use the NAOJ Telescope Kit

Japanese Version

GALAXY CRUISE: Report by the Captain - A new picture of the galaxy

Japanese/English Versions

Let’s Watch the Partial Lunar Eclipse on November 19, 2021

Japanese Version

Venus Occultation (November 8, 2021)

Japanese Version

Mars Occultation (December 2, 2021)

Japanese Version

Asteroid 7482 (1994 PC1)

Japanese Version

30-Second NAOJ Introduction Video for NINS Symposium

Japanese Version

Table 2: Summary of Produced Videos.

068

II Status Reports of Research Activities

April 6, 2021

Exploring Comet Thermal History: Burnt-out Comet Covered with Talcum Powder

April 16, 2021

Surprise Twist Suggests Stars Grow Competitively

April 22, 2021

ALMA Discovers Rotating Infant Galaxy with Help of Natural Cosmic Telescope

May 6, 2021

A New Window to See Hidden Side of Magnetized Universe

May 10, 2021

Star Formation Triggered by Cloud–Cloud Collisions

May 14, 2021

Charting the Expansion History of the Universe with Supernovae

June 11, 2021

ALMA Discovers Earliest Gigantic Black Hole Storm

June 29, 2021

A New Type of Supernova Illuminates an Old One

July 2, 2021

Observation, Simulation, and AI Join Forces to Reveal a Clear Universe

July 7, 2021

Small Amount of Lithium Production in Classical Nova

July 8, 2021

New Radio Receiver Opens Wider Window to Radio Universe

September 8, 2021

First Light with the ALMA Band 1 Receiver

September 10, 2021

Largest Virtual Universe Free for Anyone to Explore

September 15, 2021

Untangling the Formation of Planetary Systems with Deuterium

October 7, 2021

First ALMA Animation of Circling Twin Young Stars

November 13, 2021

Simulations Provide Clue to Missing Planets Mystery

December 2, 2021

Stellar Cocoon with Organic Molecules at the Edge of our Galaxy

December 14, 2021

Stellar “Ashfall” Could Help Distant Planets Grow

December 23, 2021

Billions of Starless Planets Haunt Dark Cloud Cradles

February 25, 2022

Deep Neural Network to Find Hidden Turbulent Motion on the Sun
Table 3: Web Releases.

April 14, 2021

Telescopes Unite in Unprecedented Observations of Famous Black HoleMay 19, 2021

ALMA Discovers the Most Ancient Galaxy with Spiral Morphology

September 21, 2021

Unveiling Galaxies at Cosmic Dawn That Were Hiding

December 9, 2021

Fiery Dragon's Breath May Scorch Young Planets
Table 4: Press Conferences.

to virtually visit popular places in Mitaka Campus; and adding
information on notable astronomical phenomena (Venus andMars occultations) and images and videos of celestial objects(M45 and M37).
The website terms of use were revised to improve theusability, particularly in the secondary use of copyrighted
material. To suppor t outreach effor ts of other projects,
we contributed to revamping the website for the Office ofInternational Relations (website creation and translation).
(4) New Astronomical Objects
Four staff members, including one full-time and threecontract employees, handled reports of new astronomical
objects and other communications submitted to NAOJ. In
this fiscal year, there were a total of 34 reports including
confirmation requests for new celestial object candidates andother reports. The contents were: 27 novae/supernovae, 4comets/cometary objects, 1 luminous object, and 2 moving
objects. Although no new astronomical objects (novae,
supernovae, or comets) were confirmed in these reports, 10 ofthem were confirmed to be dwarf novae or flare stars.

(5) Citizen Astronomy (Shimin Tenmongaku)
The GALAXY CRUISE website, through which citizens
participate in galaxy classification, was developed and launchedin 2019 as a joint effort with Subaru Telescope. As in last
fiscal year, we implemented campaigns in August and the endof the year, striving to boost the number of both participants
and classified galaxies. As of April 1, 2022, a total of 9,742
people (of which 6,854 are from Japan) from 92 countries andregions have registered, and the total number of classification
results has exceeded 2.5 million. Sufficient classification results
have already been obtained to allow a statistical analysis ofeach one of the classified galaxies. The initial analysis of theresults has confirmed that galactic structures and collisional
remnants are more visible in GALAXY CRUISE than in any
preceding similar projects. We also advanced the planningand development for launching GALAXY CRUISE Season
2, in which fainter galaxies are to be classified, in the next
fiscal year. The GALAXY CRUISE project appeared in news
coverage on TV and in newspapers repeatedly, and we received
many invitations to speak at international conferences andseminars.
“Citizen Astronomy” (“Shimin Tenmongaku” in Japanese)

II Status Reports of Research Activities

069

April–June
July–September
October–December
January–March
Total

Solar
Lunar
Ephemeris Ephemeris
111
176
77
53
125
151
89
70
402
450

Ephemeris

Time

36
41
25
28
130

10
4
3
8
25

Solar System Universe
129
173
315
111
728

66
108
91
66
331

Astronomy

Other

Total

46
56
48
39
189

255
178
332
207
972

829
690
1,090
618
3,227

Table 5: Telephone inquiries made to the Outreach and Education Office of the NAOJ Public Relations Center (April 2021–March 2022).

conducted at NAOJ is an example of “Citizen Science” in which
researchers / research institutes and the public collaborate on
scientific activities.

4. Outreach and Education Office
In FY 2021, 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 6,750 people participated in Mitaka Campus
Public Visits (former name was Visitors’ Area) in FY 2021.
In addition, the group tours in 2021 consisted of 15 general
tours (436 guests), for a total of 7,186 guests visiting Mitaka
Campus. Public visits scheduled for April 25–June 20, 2021,
and July 12–September 30, 2021, were all canceled to preventthe potential spread of COVID-19. Even after the public visits
program resumed, we implemented preventive measures,
restricting public access to within the outdoor areas, andcanceling the acceptance of general group tours.
Regular stargazing parties, which are usually held twice amonth (the day before the 2nd Saturday and the 4th Saturday)
with the 50-cm Telescope for Public Outreach, were canceledin FY 2021 due to the COVID-19 pandemic as they werelast fiscal year. Instead of on-site stargazing parties, “online
stargazing parties” were held on YouTube Live every fourth
Saturday from April 2021 to January 2022 (excluding Octoberdue to Mitaka Open House Day), and on every Friday before
the second Saturday and every fourth Saturday from February
to March 2022. These online events have taken place 13 times
and accumulated 15,178 views as of April 7, 2021. Using the
50-cm telescope, we also photographed an asteroid making aclose approach to Earth and shared the photos and information
on social media.
Regular public screenings at the 4D2U Dome Theater wereoriginally scheduled to be held three times a month (1st, 3rd
Saturday, and the day before the 2nd Saturday) on a reservationbasis. However, the reduced event days (35 days to 9 days)
and capacity (from 40 seats to 14 seats) due to the COVID-19
pandemic resulted in only 340 visitors. “Ast ronomers’
Talks” mini-lectures and public screenings for groups wereboth canceled. In addition, 22 group tours (141 people)
were organized and a total of 481 guests watched the 4D2U
stereoscopic movies.

070

II Status Reports of Research Activities(2) Telephone Inquiries
Since this fiscal year, the starting hours for telephoneinquiries have been changed from 9:00 a.m. to 9:30 a.m. toensure sufficient time for preparation.
Since last fiscal year, our inquiry service has continued
to operate on a rotating shift basis with one person assigned
to each shift, except for seasons in which many inquiries are
expected. This fiscal year, two people were assigned to eachshift during the seasons around the Perseids (August) anda partial solar eclipse (November 19). As they did last year,
inquiries operators worked on-site or from home at theirdiscretion to prevent the spread of COVID-19.
The number of telephone inquiries to which we responded
this fiscal year totaled 3,227, of which 457 were from the media(Table 5), whereas the number of letter inquiries totaled 72, of
which 28 were official documents.
(3) Media Reception
We received 110 interview and filming requests fromvarious media. Among these, we dealt with 101 requests. The
contents were: 29 newspaper articles; 36 TV programs (11news programs, 2 science programs, 23 others); 19 publications(7 magazines, 3 books, 9 others); 9 websites and contents;
4 radio programs; 4 others (2 private location shootings, 1commercial, 1 event). From FY 2019, we started to charge a fee
for commercial filming and photography in the campus. Thisfiscal year, we received filming requests for 1 TV program and1 Web TV program.
(4) Educational and Outreach Activities
The “FUREAI (Friendly) Astronomy” project, now in its
12th year, continued to provide the online lectures introduced
last fiscal year in addition to conventional on-site lectures.
These lectures were delivered at 118 schools, 75 in Japan and43 overseas, by 65 instructors and attended by 9,480 pupils,
with the number of attendees per lecture ranging from 3 to 996.
In 12 years, 82,678 students in total have attended the lecturesin 872 schools inside and outside Japan.
“Mitaka Open House Day” was held online this year as
it was last year, and we participated as part of the secretariat
under the direction of the steering committee, and contributed
to some pieces of the content. This year’s event was heldon October 23 (Saturday) with the theme “Looking back on
the 10 years ALMA's research findings.” It was co-hosted
by the Astrobiology Center, National Institutes of Natural
Sciences; the Institute of Astronomy, the School of Science,the University of Tokyo; and the Department of Astronomical
Science at the School of Physical Sciences of the Graduate
University of Advanced Studies. Unlike last year’s event, wherea single live program was created, this year’s event consisted of
3 main online lectures, livestreams by NAOJ’s projects, video
contents, and web contents. The number of event contents
totaled 103, including 21 livestreams (including YouTube
Premiere events), 45 video contents, and 37 other web contents.
The total number of simultaneous connections reached 2,054,
and the video garnered 60,300 views in the first month of its
release.
(5) Community Activities
The “Mitaka Picture Book House in the Astronomical
Observatory Forest” welcomed 17,472 visitors in FY 2021.
T he Off ice super vised an ex hibition, “T he Unfoldi ng
Universe—Past, Present, and Future.” (July 2021 to June 2022).
Unfortunately, the COVID-19 pandemic forced this year’s
traditional Tanabata and moon viewing events to be canceled.
In addition, through the “Mitaka Picture Book House in 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 7 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 insteadof 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 sixth anniversary since its openingin September 2015. In FY 2021, a total of seven exhibitions
were held at this facility, of which the one titled “Exploring
Our Origin in the Universe —Ten Years of ALMA” wasplanned and held by NAOJ. This event ran from December
3 (Friday), 2021 to January 30 (Sunday), 2022, and attracted
1,279 visitors. At the facility, the Office played videos onlarge displays to publicize NAOJ and provide information
about the night sky and distributed NAOJ News bulletins andmonthly guide materials about the night sky. This fiscal year
saw a total of 9,945 visitors. Although the number dropped byabout 5,300 compared to an average year before 2019 due toan entry restriction implemented in response to the COVID-19
pandemic, the facility has received over 94,000 visitors since

its opening. It is now recognized as a place where the public
can get to know more about science in an urban environment.
(6) Merchandizing Business
The NAOJ Telescope Kit has been on the market since FY
2019. In Japan, this kit goes by the name “NAOJ Telescope
Kit,” whereas the IAU calls it “Kaifu-NAOJ Telescope Kit.”
This 5-cm aperture telescope kit, with eyepieces of 16x and 66x
magnification, started to be sold and distributed in July 2019.
A total of 3,249 kits were sold this fiscal year, with the total
cumulative sales reaching 7,644 kits.
We run “Astronomical Events Information” on the NAOJ
website to provide monthly star charts and information onplanetary and other remarkable astronomical phenomena.
This fiscal year, intended particularly for the media,
articles detailing the remarkable astronomical phenomena of
the year (the Perseids in August and a partial lunar eclipse
on November 19) were created and posted on “Astronomical
Events Information.”

5. Spectrum Management OfficeThis is the third year since the establishment of theSpectrum Management Office (SMO) in 2019. With a newassociate professor (senior lecturer) appointed on June 1, 2021,
the SMO currently consists of four members, of which three
are dedicated members (Head, an associate professor, anda research supporter) and one holds a concurrent post. The
SMO handles a broad range of operations, both domestic andinternational. At the time of establishment, we focused mainlyon the protection of the radio astronomy environment, but since
the rise of mega-constellations issues we have been acting onlight pollution as well.
In fiscal year 2021, the SMO participated in 18 international
meetings and 28 domestic meetings. In addition to these,
the SMO also participated in e-mail 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 forradio astronomy issues, and contributed to the discussion.
This year’s WP7D meetings were held online from April
12 to 16, 2021, and from September 16 to 23, 2021, because the
ITU headquarters were temporarily closed and travel to andfrom Europe was restricted due to the COVID-19 pandemic.
Both meetings focused on topics such as the compatibility
between mobile phone use and radio astronomy in the 6–7
GHz and 43 GHz bands, issues to be studied for realizing radio
astronomy observations in lunar surface radio quiet zones, andsharing of the frequency bands above 71 GHz between active
services and radio astronomy. These meetings also discussed a
new draft report to emphasize the importance of geodetic VLBI
and a new draft report on radio observations with distributed
antennas in the millimeter and submillimeter bands, as well as

II Status Reports of Research Activities

071

revising a report on radio quiet zones.
The SMO also held 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: Although wireless LAN systems currently operate in
the 2.5/5 GHz bands, these frequency bands are increasinglycongested. Given this situation, the possible allocation of the
6 GHz band (5.925–7.125 GHz) to the wireless LAN service
was discussed. In this frequency band, frequencies ranging
from 6.665 to 6.66752 GHz, where CH 3OH maser emissions
exist, are reserved for the radio astronomy service. Sharing
studies with the radio astronomy service found that Low Power
Indoor and other even lower power modes were likely to causesignificant interference and thus concluded that the sharingof this frequency band is not feasible. It was also found thatfor some other services, sharing of the band is not feasible,
and thus the 5.925–6.425 GHz band was newly selected to beallocated to the wireless LAN service. No harmful interferencewith CH3OH maser observations are therefore to be expected
for the time being.
2) Studies on the 76–77 GHz Band Sharing with Vehicle-Borne
Millimeter Wave Radar: To ensure a wide angle and a sufficient
range, studies to improve vehicle-borne radar have beenongoing. In this frequency band, both radar (radiolocation) andradio 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
with vehicle millimeter-wave radar manufact urers anddiscussions in the MIC 76 GHz Low Power Millimeter-Wave
Radar Working Group. The SMO reviewed the acceptableinterference level described in the ITU’s recommendationand exchanged opinions about the calculation method forinterference estimation. These studies are expected to continue
into FY 2022.
3) Outdoor Use of UWB Systems: To avoid CH 3 OH maser
observations at 6.7 GHz being adversely affected, it was agreed
that operational manuals for UWB systems must instruct theusers not to use the systems around radio observatories.
4) Wireless Power Transmission (WPT) Systems: WPTsystems use the 920 MHz, 2.4 GHz, and 5.7 GHz bands totransfer electric power, and thus they should adversely affectnot only ratio astronomy observations but also various radio
communication systems. To prevent any interference fromoccurring, it was decided to register radio observatories
in a database and avoid using WPT systems around theseobservatories. When the MIC later called for public comments

072

II Status Reports of Research Activities

on this matter, the descriptions on the setting of operation
coordination areas included a factual error, which the SMO
pointed out and requested correction in its public comment.
5) Space Cellular: Space Cellular allows existing mobile
phones to communicate directly with satellites, thereby
enabling the devices to connect to the internet even in groundareas with no base stations. Japanese cell phone companies
are considering introducing Space Cellular. Because thefrequencies used for communications between the satellites andthe ground base stations were expected to affect the 42.5–43.5
GHz and 49 GHz radio astronomy bands (SiO and CS), theSMO carried out studies evaluating potential interference tothe radio astronomy service. These studies found that the main
beams from the satellites must not be directed towards radio
astronomy antennas, and that the 42.0–42.5 GHz band needs tobe excluded from the emission bands. Bringing Space Cellular
into practical use needs not only technological evaluations,but also changes to the Radio Law and the Radio Regulations.
Many issues remain to be discussed.
(3) Application for Receiving Equipment Desig nation:
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. In Fiscal
Year 2021, we submitted no applications for designating or
renewing facilities.
(4) Light Pollution
1) Light Pollution Caused by Mega-constellations (such as
Starlink): The IAU and NAOJ issued statements in 2019that express concerns over the possible impacts of megaconstellations, such as Starlink and OneWeb, which aim to
deploy large swarms of satellites to provide internet accessaround the world. SpaceX, which operates the Starlink
satellites, has committed to reducing the satellites’ reflectivity
by developing a dark-painted satellite called “DarkSat” and avisor-equipped satellite called “VisorSat.” In response to these
efforts, Ishigakijima Astronomical Observatory observed thesesatellites in the U, B, gʼ, Rc, Ic, J, H, and K bands, working
together with the Optical and Infrared Synergetic Telescopesfor Education and Research (OISTER). The SMO assisted inanalyzing and interpreting the data obtained by Ishigakijima
Astronomical Observatory.
The IAU Office for Astronomy Outreach (OAO) recently
launched a new project, “Dark and Quiet Sky,” to raiseinternational public awareness about light pollution. The SMO
supports this project and helped the OAO create an interview
video. An SMO member served as part of the Scientific
Organizing Committee of the IAU co-sponsored Dark andQuiet Skies Workshop 2 and contributed to making theworkshop successful.

(5) Activities for Raising Awareness of Frequency Resource
Management
To make more people aware of f requency resou rce
management, the SMO created a brochure explaining the
SMO’s activities and the importance of frequency resource
management, particularly in radio frequencies. This brochureis to be distributed at Mitaka Campus, Nobeyama Campus, the
VERA stations, and Ishigakijima Astronomical Observatory.
The SMO informed domestic radio observatory operators of
our intention to provide the brochure as needed and sent it to
14 of them, including MIC, MEXT, and local communication
stations.
The SMO website has been updated on a continual basis.
This fiscal year, in addition to enriching the glossary of radio
astronomy terms, we launched the English website to provide
information to international audiences.

6. Ephemeris Computation Office
The Ephemeris Computation Office (ECO) estimatesannual astronomical phenomena including the apparent placesof the Sun, Moon, and planets based on international standards
and publishes the “Calendar and Ephemeris” as part of thecompilation of almanacs, which is one of NAOJ’s raisons d’être.
Project researcher Takashi Shibata has joined ECO since
May 2021.
(1) ECO published the “Calendar and Ephemeris 2022”
and compiled the ephemer is section and several par tsof the astronomy section from the “Rika Nenpyo 2022”(Chronological Scientific Tables). ECO also posted the “RekiYoko 2023” in the official gazette on February 1, 2022. 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 “RekiFigure 1: Pageviews for ECO Website.

Yoko.” In the “Calendar and Ephemeris 2022,” ECO revised thevisual magnitude of planets for the first time in over 30 years
and explained the details in its topics page. As for the “Rika
Nenpyo,” ECO has taken responsibility for several pages in theephemeris and astronomy section since FY 2020.
(2) ECO featured lunar eclipses and the 1st sunrise of the year
on its website. Despite the end of the astronomical phenomena
awareness campaigns by OEO, ECO displayed the radiantpoints of the Perseid, Geminid, and Quadrantid meteor showers
and the place of Comet Leonard in the Sky Viewer. In FY 2021,
there were over 36 million page views for the ECO website.
https://eco.mtk.nao.ac.jp/koyomi/index.html.en(3) T he Japa n Associat ion for Calend a rs a nd Cult u re
Promotion, hereafter JACCP, held a mini forum and its 11th
General Meeting via remote conference service. JACCP
also held the annual Calendar Presentation Ceremony with alimited number of people and delivered its lecture via a remote
conference service. The update of the Yoshiro Okada collection
site which holds the research materials collected by the late Dr.
Yoshiro Okada, the Supreme Academic Advisor of JACCP, isstill under way.
https://library.nao.ac.jp/kichou/okada.html(4) ECO holds a reg ular exhibition presenting NAOJ’s
invaluable collection of historical archives of Japanese andChinese books in collaboration with the library. ECO started
the 59th exhibition “Promotional Calendars from the Yoshiro
Okada Collection” which was delayed due to the COVID-19
pandemic. Past exhibitions are available 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. In recent years, withthe continuing digitalization of scientific materials, the portionof the materials in electronic format has increased.
Mitaka Library was originally open to non-NAOJ affiliatedusers on weekdays, but the COVID-19 pandemic has forced thelibrary to close public access 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, 29
materials were provided this fiscal year.
The library also offered a remote service to NAOJ members
off-campus.
The library holds many important documents, the mostprominent of which are those written by the Tenmonkata,

II Status Reports of Research Activities

073

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 and have appeared in multiple
publications outside NAOJ.
For the 2021 Special Open House Day, held online in
October, the Library Unit created special web pages listingbooks related to this year’s theme and other materials housed in
the library. The unit also launched a web page for tips on how
to search in the online public access catalog.
The number of books and journals owned by Mitaka
Library and 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 PR andpromotions. The following periodicals were also published thisyear:
• Annual Report of the National Astronomical Observatory ofJapan Volume 33 Fiscal 2020 (Japanese)• Annual Report of the National Astronomical Observatory ofJapan Volume 23 Fiscal 2020 (English)• 22nd Report of the National Astronomical Observatory ofJapan• Publications of the National Astronomical Observatory ofJapan Volume 16• NAOJ 2021 Pamphlet (Japanese)• NAOJ News, No. 333 – No. 336 (April 2020 – March 2021)• NAOJ Calendar (The 17th in the series)
In FY 2021, the off ice revised the NAOJ pamphlet(Japanese), and published the Annual Report of the NAOJ
(Japanese/English versions), the 22nd Report of the National
Astronomical Observatory of Japan, and Publications of the
National Astronomical Observatory of Japan Volume 16. In
preparation for a shift to digital publication, we changed NAOJ
News to a quarterly format while increasing the page count. In
the systematic production of NAOJ News special editions withthe goal of developing project outreach support, we produced
the issues “VERA and Mizusawa VLBI Observatory” (Summer2021), “ALMA 10th Anniversary” (Autumn-Winter 2021), and“Ishigakijima Astronomical Observatory 150,000 Visitors –A report on the activities of the past 5 years” (Spring 2022).
Other than periodicals, the 2021 calendar “The Universe Seenby the Subaru Telescope Ultra-Wide Field-of-View PrimeFocus Camera HSC (Hyper Suprime-Cam) 2022” (the 17th
since 2005, this time produced taking universal design andaccessibility into consideration) was created. As in other years,
editing support was also given to the publication of the “Rika
Nenpyo 2022 (Chronological Scientific Tables, Astronomy
section).” In addition, the office continued to support the
English production and editing of releases, publications, and074

II Status Reports of Research Activities

web content both inside and outside of NAOJ.
In relation to the shift to digital publication, digital versionsof the past 18 years of Publication Office publications (Annual
Report Highlights, NAOJ Pamphlets, NAOJ News, NAOJ
Calendar, posters of the various NAOJ branches, etc.) werecompiled into a library, and preparation is ongoing for the
release of original (electronic) publications.
Also, in an attempt at research development in the new
field of “Cultural Astronomy” we are creating “arcAstroVR” aprecise astronomical simulator for archeoastronomy research.

9. IAU Office for Astronomy Outreach (OAO)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 125 countries.
During Fiscal Year 2021, we highlight the successful
renewal of the IAU-NAOJ Agreement for the OAO until 2024,
the increase of the OAO core team to three full-time members,
the NOCs Funding Scheme being officially attributed to OAO’s
annual fixed budget by the IAU and the establishment of the
OAO Steering Committee, composed of 4 members, moving
towards a structure more similar to the other IAU sister offices.
Among the key activities carried out by the office during
the period of this report, we highlight the NOC’s management
and engagement, leading to an increase in representation of the
network, nominating representatives in nearly 130 countries
and territories. We concluded the NOCs Funding Scheme 2021
with three projects funded and implemented the 2022 edition
that received 12 proposals.
During FY 2021 we also implemented the IAU OutreachGlobal Projects highlighting Telescopes for All 2021 thatreceived over 225 submissions from 54 countries; 100 Hours of
Astronomy 2021 which was implemented in over 60 countries;
and Women and Girls in Astronomy 2022 with 782 entries forthe Draw an Astronaut competition and a total of 251 events in
39 countries.
We highlight the co-organization with IAU Commission C2
for the CAP conference in May 2022 with over 1200 registeredparticipants from 84 countries. The OAO and NAOJ are also
the publishers of the conference proceedings. Issue #30 of theCommunicating Astronomy with the Public (CAP) Journal was
published. Issue #30 was a special 30th edition in November
2021 (Astronomy Communication in a Time of Confinement)with 7 articles in total (2 peer-reviewed) from a total of 58
submissions.
Rega rdi ng I AU com mu n icat ion cha n nels, we havesuccessfully generated a 15 % growth in our IAU Facebook
channel with 21,400+ Followers. On IAU Twitter we had a 13 %growth rate, reaching 14,700+ followers. In our OAO channels,
we have successfully generated a 26 % growth in our OAO
Facebook channel with 10,200+ Followers. On OAO Twitter wehad a 5 % growth rate, reaching 3,700+ followers. The officealso delivered 220+ astronomy outreach/education news items
through 24 issues of the IAU Astronomy Outreach Newsletter
to 4,368+ subscribers worldwide, and translated into 6 different
languages by volunteers.

10. Ishigakijima Astronomical Observatory
In the first half of FY 2021, public access was almost
entirely canceled due to the COV ID -19 pandemic andthe closure of Maesedake Rindo, the road leading to theobservatory. In public outreach, the facilities were gradually
reopened to the public from October. The total cumulative
number of visitors since opening passed 150,000 in January
and the annual total reached approximately 1,400 visitors.
Moreover, the observatory was involved in many online
activities, such as broadcasts of astronomical events. In
education, we welcomed group tours and gave visiting lecturesand online lectures for the public. In research, 1 refereed paper
was published on observation of small celestial bodies in the
Solar System, bringing the total number of papers publishedbased on data from Ishigakijima Astronomical Observatory to30.
(1) Public Outreach Activities(2) Educational Activities
After October, the public access road reopened and webegan accepting educational group tours again. In November,
we welcomed an Ishigaki City Council inspection. Also,
we worked for local education activities such as providing avisiting lecture at “Ishigaki City Senior University” hosted
by the Ishigaki City Board of Education. In February, an
introductory program was broadcast as a collaboration between
NAOJ and “Hamagin Space Science Center,” and the Churaboshi Research Team Workshop for high school students washeld in March with 9 participants from across Japan.
(3) Research Activities
One refereed paper in a western journal was publishedin FY 2021, on the topic of small celestial bodies in the Solar
System. The total number of papers including results basedon Ishigakijima Astronomical Observatory observational
data reached 30. There were 5 presentations at domestic andinternational conferences. In particular, project research staff
member Horiuchi is leading efforts to compile the results forobserving Starlink satellites through collaborative OISTER
obser vations. We obser ved 46 objects over 101 nights.
Collaborative observations with OISTER, etc. observed 14
objects over 53 nights. Research fellow observations consistedof 20 objects over 69 nights. Public outreach observations
consisted of 12 objects over 49 nights.

[Guided Tours, 4D2U Theater, Stargazing Sessions]
The facilities closed entirely to the public, including
guided tours, screenings at the 4D2U theater, and stargazing
sessions because of the closure of Maesedake Rindo whichis the only road leading to the observatory, from July, 2020
until the end of repair work in September, 2021. In October,
2021, we re-opened to the public, limited to walking aroundthe outside of the facilities, and from November restarted
inside activities including guided tours, the 4D2U Theater,and Stargazing sessions. We limit the number of visitors,
hours, and the number of times, and disinfects thoroughly as
preventative measures against the COVID-19 pandemic. The
total cumulative number of visitors passed 150,000 in January,
and the annual total was approximately 1,400 visitors.
[Special Events, Co-sponsorships, Cooperative Events, etc.]
In May, we participated in the total lunar eclipse broadcast(anchored at Mitaka Campus) by providing a live image feed,
etc. Moreover, we observed Asteroid Kushiike, Supernova
2021qvv, and so on for public outreach, and released the results
through web news.
The Southern Cross Monitor that started in 2020 held anobserving season from December to June, and was active asa Milky Way monitor from July to November. For the thirdyear in a row, entries from observatory employees received
Excellence Awards in the “‘Local’ Star View Photo Contest(GOTO INC.).” In addition, together with Nayoro Observatory,
we conducted an alternative stamp rally from December toMarch.

II Status Reports of Research Activities075

17. Division of Science
1. Overview
We will report the FY 2021 research activities in the
Division of Science based on the following vision andphilosophy of the division:- Achieve fruitful results of research based on liberal ideas
of individuals, 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, 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 education of young researchers, including
students at graduate schools, to attract both Japanese andoversea researchers in the next generation who will leadworld-wide research activities. Become a career path center
for astronomical research in the world.
- Strengthen the astronomical field in Japan by creating newscience by collaboration with domestic and international
researchers, including other Projects in NAOJ. Play animpor tant role to promote inter nationalization 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 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 advantages of the facilities of NAOJ,
such as super-computers of CfCA, the Subaru Telescope,
A LM A, and the Nobeyama 45-m Radio Telescope, we
stimulate collaborations among theoretical and observational
astronomers working on various wavelength ranges. Also, we
advance 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
ground-based and space-based 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. However, due
to COVID-19, visitors from abroad are severely restricted in
FY 2021, following FY 2020. Domestic visitors came backgradually in FY 2021. To compensate for the decrease ofvisitors, the division has been actively inviting internationaland domestic researchers to the division’s online colloquia and076

II Status Reports of Research Activities

seminars to promote discussions. The division also provides
the online opportunities to facilitate the communication among
the division members, including lunch meetings, informal
gatherings, and internal workshops. In addition, the division
actively organizes international and domestic workshops forthe fields of theoretical and observational astronomy, as well as
the cross-disciplinary field between astronomy and planetaryscience, leading research activities in various related fields ofastronomical science.

2. Current Members and Transfers
In FY 2021, the dedicated faculty of the Division of Science
included five professors, three associate professors, and sevenassistant professors in addition to one adjunct professor, one
adjunct associate professor (from February 1), and one adjunctassistant professor who concurrently held a primary position at
the Center for Computation Astrophysics (CfCA). Professors
Masahiro Ikoma and Nozomu Tominaga have newly arrived in
FY 2021 while Professors Kohji Tomisaka and Toshiki Kajino
retired in FY 2020. Accordingly, the research activities on
exoplanets; formation and evolution of planets; supernovae;
time domain astronomy; and multi-messenger astronomy
have been strengthened. Also Dr. Tomoya Takiwaki waspromoted from Assistant Professor in the Division of Scienceto Associate Professor with a primary position at CfCA. In
addition to these faculty members, the division was served byten project assistant professors (including NAOJ fellows), fiveproject research fellows, four special postdoctoral researchersof the Japan Society for the Promotion of Science (JSPS), one
research supporter, and three administrative supporters (onestarted from February 1) who gave full support to all activitiesof the division.

3. Research Results
The refereed research papers published by the division
members as authors are more than 190 in number. Some of theresearch results are presented as the research highlights listed
at the beginning of this report. The following includes researchin which the division members took leading roles:- Planetesimal dynamics in the presence of a giant planet(Kangrou Guo, Eiichiro Kokubo)- On the Hubble Constant Tension (Dainotti, M.G. et al.)- High Spatial Resolution Observations of Molecular Lines
toward the Protoplanetar y Disk around TW Hya with
ALMA Revealing Detailed Physical and Chemical Structure(Nomura, Tsukagoshi, Kawabe et al.)- Observation of hydrogen line emission from a young gas giant
planet and constraints of planetary accretion process (Uyama,
Ikoma)

The following research results are released on the division’s
website (https://sci.nao.ac.jp/main/articles-en/) as researchhighlights:- Surprise Twist Suggests Stars Grow Competitively (Takemura,
Nakamura, Tsukagoshi, Kawabe et al.)
- A New Window to See Hidden Side of Magnetized Universe(Machida et al.)- Char ting the Expansion Histor y of the Universe with
Supernovae (Dainotti et al.)
- A New Type of Supernova Illuminates an Old Mystery(Moriya, Tominaga et al.)- Planetesimal Dynamics in the Presence of a Giant Planet (Guo,
Kokubo)- A LM A Finds Super-Fast Rotation of Baby Star’s Jet(Matsushita, Tomisaka et al.)- Unveiling a century-old mystery: Where the Milky Way’s
cosmic rays come from (Sano et al.)- The ultra-wideband, high sensitivity 7 mm radio receiverinstalled on the 45 m! (Nakamura, Kawabe, Taniguchi et al.)

4. International and Domestic Collaborations
and Cooperation(1) International and Domestic Workshops
Due to COVID-19, international conferences continued
to be severely limited in FY 2021. The members of thedivision organized or co-organized the following internationaland domestic workshops, as a hub of science activities,
collaborating with international and domestic colleagues,
which contributed to stimulating research activities in thefield of astronomy and the cross-disciplinary fields. All thefollowing meetings were held online.
International Meetings- The Isotopic Link from the Planet Forming Region to the
Solar System (July 27–29, 2021)- Mini workshop on GRBs correlations and machine learning
for GRBs and AGN (July 29–30, 2021)- SAZERAC SIPS Early Galaxy Formation Near and Far —Preparing for a Long Journey with JWST — (November 29–
December 3, 2021)
Domestic meetings- W50/SS433 workshop (May 18, 2021)- Workshop on Galactic Star Formation (November 16 –December 2, 2021)- The 10th observational cosmology workshop (November
17–19, 2021)- SNR workshop 2022 (March 28–29, 2022)(2) International Organization Committees and Reviews ofInternational Funds- “Forming and Exploring Habitable Worlds” scientific steeringcommittee (Kokubo)- National Fund for Scientific and Technological Research,
Chile (Ouchi, Ikoma)- The Dutch Research Council (NWO) funds, Netherland(Ouchi)- National Research Agency (ANR), France (Ikoma)- Research Projects of National Relevance (PRIN), Italy (Ikoma)(3) International and Domestic Observation Projects
In order to advance 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 toastronomy, including the plans for large telescopes in NAOJ,
from a scientific perspective.
- Subaru Intensive Program: EMPRESS 3D (PI)(Ouchi)- Subaru Intensive Program: IRD TESS Follow-up Project II.
(Ikoma)- HSC SSP transient working group (Chair)(Moriya)- Subaru IRD SSP (Kokubo)- Hyper SuprimeCam Survey weak lensing science researchgroup (Hamana)- Subaru SAC (Ikoma, Moriya)- Subaru proposal review (Nomura, Tsukagoshi)- Subaru PFS Galaxy Evolution Group (Ouchi)- ULTIMATE-Subaru Science Study Group (Moriya)- NINJA project (Moriya, Ouchi)- TMT-J SAC (Tominaga)- Nobeyama 45-m KAGONMA project (Kobayashi)- Nobeyama proposal review (Sano, Furuya)- JCMT BISTRO-J, JCMT CLOGS survey (Kobayashi)- JCMT proposal review (Arzoumanian)- ngVLA Japan Science Study group (Kobayashi)- SKA-JP Science Study group (Fujii, Machida)- LST Science Study group (Kobayashi, Sano, Tsukagoshi,
Nomura, Harada, Furuya)- Seimei Telescope proposal review (Tominaga)- Hubble Space Telescope proposal review (Moriya)- Swift Senior review (Dainotti)- Fermi-LAT member (Dainotti)- Theseus member (Dainotti)- JOVIAL (JP Co-PI) (Ikoma)- Ariel Consortium (Co-PI), Ariel-JP Science Study group (PI)(Ikoma)- WSO-UV Science Study group (Ikoma)- Roman Science Investigation Team (Ouchi, Moriya)- Euclid Consortium (Moriya)- GREX-PLUS Science Study group (Ouchi, Nomura, Moriya,
Fujii)- GOPIRA 2030s Future Study Working Group (Ouchi)- GOPIRA Future Plan Study Advisory Committee (Ouchi)- IAU Commission F2 Exoplanets and the Solar systemorganization committee (Kokubo)

II Status Reports of Research Activities077

5. Educational and Outreach Activities
The division actively promotes education of young
researchers, including students at graduate schools, to become acareer path center for astronomical research in the world. In FY
2021 the graduate students in the Division of Science included
ten SOKENDAI students (five doctoral and five master’s course
students) and fourteen students in the University of Tokyo(ten doctoral and four master’s course students). The numberof students was twenty-four in total. In addition, the membersin the division engaged in the education of graduate andundergraduate students in the following universities and alsohigh school students.
- Graduate students: U. of Tokyo (Ikoma), Tokyo Tech.
(Nomura), Konan U. (Tominaga), U. of Tokyo/ Nanjing
Normal U. (Harada), Nagoya U. (Sano), [Italy] Salerno U.,
Naples U., Pisa U., [Poland] Jagiellonian U., AGH U., [USA]Maryland U., UC Davis, Cornell U, MU Amherst (Dainotti)- Undergraduate students: [Poland] Jagiellonian U. [India]
Mithibai U., IIT K harag pu r U., [USA] Mar yland U.,
Pennsylvania U., Arizona State U., New York U., Carnegie
Mellon U., Michigan U., Los Angeles U., Tufts U., Purdue U.
(Dainotti)- High school students: [USA] Caribbean Education Foundation(Dainotti)
The members of the division actively engaged in both
graduate and undergraduate lectures at the University of Tokyoand many other institutes and universities. including classes
at Super Science High Schools. In addition, the online open
house (admission guidance) of the Division of Science forundergraduate and master course students was organized in
March 2022. The members also engaged in outreach activities
by offering lectures to the public.

6. Awards
The members in the division were awarded in recognitionof their excellent research achievements in this year as follows.
- The 51th Summer School Oral Awards for Young Astronomy
and Astrophysics (Kiyoaki Doi)
- 2020 ASJ Young Astronomer Award (Akimasa Kataoka,
Kimihiko Nakajima, Takashi Moriya)- The Best Researcher Award 2020 of the Japanese Society ofPlanetary Science (Akimasa Kataoka)- FY 2021 NAOJ Young Researchers Award (Akimasa Kataoka)- 2021 ASJ PASJ Excellent Paper Award“Big Three Dragons: Az = 7.15 Lyman-break galaxy detectedin [O III] 88 μm, [C II] 158 μm, and dust continuum with
ALMA” (Masami Ouchi is coauthor)“The formation of massive molecular filaments and massive
stars triggered by a magnetohydrodynamic shock wave”(Kazunari Iwasaki is coauthor)- The University of Tokyo, The School of Science, Encouragement

078

II Status Reports of Research Activities

Award AY2021 (Misako Tatsuuma)- Highly Cited Researchers 2021 (Clarivate Analytics, USA)
(Masami Ouchi)

18. 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 multi-culturalresearchers 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
2021, some of our activities had to be reduced because of thedecrease in the number of incoming international visitors andthe cancellation or postponement of scheduled events due tothe spread of COVID-19. Despite the circumstances, we took
advantage of this time to focus on activities that were notaffected by the pandemic.

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). The EACOA consists of four coreobservatories representing the East Asian regions: the NAOJ
(Japan), the National Astronomical Observatories of China(China), the Korea Astronomy and Space Science Institute(South Korea), and the Academia Sinica Institute of Astronomy
and Astrophysics (Taiwan), and the EAO is operated by theseEACOA members and the National Astronomical ResearchInstitute of Thailand. During FY 2021, the OIR assisted the
Director General of NAOJ in each of the EACOA/EAO
online board meetings and supported one post-doctoral young
researcher who was hosted by NAOJ 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
and overseas institutions. In FY 2021, we reviewed a totalof 33 new or renewed international agreements and drafted
revisions as needed. One such document was the Memorandumof Understanding (MOU) with the Institute of Astronomy andAstrophysics, Academia Sinica (ASIAA), concerning the joint
development of new instruments for the Subaru Telescope. The
OIR worked in close collaboration with the National Institutesof Natural Sciences (NINS) to organize a virtual signingceremony for this MOU, and in August 2021, the Presidentof NINS and the Director General of NAOJ, as well as the
President of Academia Sinica and the Acting Director of the
ASIAA met online to conclude the MOU. This ceremony createdan opportunity for the parties to confirm their willingness todeepen their ties and cooperation between Japan and Taiwan in
astronomical research.

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 2021, to preventthe spread of COVID-19, the SD staff worked remotely where
possible by providing consultation services over the phone,e-mail, and online conference systems. However, in someinstances where on-site assistance was necessary or requested,
the SD staff accompanied international researchers and students
to municipal offices and other places to complete various
procedures. In addition, as part of an effort to strengthen support
by the SD, the “NAOJ Support Desk Registration Form” wasdeveloped and put into operation. By having international
researchers and students submit this form before their visit, theSD staff can obtain accurate information in a timely mannerand be prepared to provide appropriate support for facilitating
the relocation process to help establish an environment inwhich incomers can concentrate on their research as quickly as
possible.
Furthermore, in July 2021, the OIR launched its newly
redesigned website to provide information to international
researchers and students both inside and outside NAOJ. The
website contains information on immigration procedures,
accommodations, campus neighborhoods, and daily life, as
well as reference information for NAOJ host researchers andstaff. Although all information is provided in both Japanese andEnglish, according to the current statistics, one-fourth of thewebsite visitors have read the English version, indicating that it
is widely used among non-Japanese speakers.
In parallel with these services, the OIR continues tocollaborate with a specialized company to offer beginner-level
Japanese language classes to help international researchersand students quickly adjust to life in Japan. In FY 2021, a
new intermediate course was established. Both courses offer
lessons that have been tailored in response to the requests offormer 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
at their convenience. The courses were well received by thestudents, who remained highly motivated to learn and were able
to acquire more practical Japanese language skills.

3. Information Dissemination at International
Conferences
The OIR has been exhibiting booths at international
conferences to recruit international researchers by providing
information about NAOJ’s research activities and invitational
programs. Although the 239th AAS Meeting was canceled
due to the spread of COVID-19, we have already started our

II Status Reports of Research Activities079

preparations for setting up a booth at the IAU GA 2022, which
will be held in Busan, Republic of Korea, in August 2022.
Furthermore, the OIR supports other NAOJ departments thatplan to have an exhibition booth at international conferences.
During FY 2021, the OIR assisted the Public Relations Center in
exhibiting a virtual booth at the European Astronomical Society(EAS) 2021 Annual Meeting held in June and July 2021. Also,
as a member of the local organizing committee, the OIR has
started preparations to support visa procedures for participantsin the Asia-Pacific Regional IAU Meeting (APRIM 2023), to beheld in August 2023 in Aizu, Fukushima Prefecture.

080

II Status Reports of Research Activities

III Organization
Projects

1. Organization(C Projects)

Subaru Telescope
Nobeyama Radio Observatory
Mizusawa VLBI Observatory
Solar Science Observatory
NAOJ Chile
Advisory Committee for Research and Management

ALMA ProjectCenter for Computational Astrophysics(B Projects)

Gravitational Wave Science Project
Thirty Meter Telescope (TMT) Project

Director General(A Projects)

Vice-Director General (on General Affairs)
Vice-Director General (on Finance)

JASMINE Project
RISE Project
SOLAR-C Project
Subaru Prime Focus Spectrograph (PFS) Project

Director of Engineering
Director of Research Coordination
Executive Advisors to the Director General

Subaru Ground Layer Adaptive Optics (GLAO) Project
ASTE ProjectCenters
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)
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
IT Security Office
Administration Department
III Organization

081

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(2022/3/31)
1
147
28
1
35
10
6
2
53
0
12
39
57
6
152
1
1
33
2
74

18

3. Executives

082

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

III Organization

Watanabe, Junichi
Iguchi, Satoru
Mitsuda, Kazuhisa
Saito, Masao

4. Research Departments
Projects
C Projects

Subaru Telescope
Director
Yoshida, Michitoshi
Vice-Director
Hayano, Yutaka
Professor
Hayano, Yutaka
Professor
Yoshida, Michitoshi
Project Professor
Takami, Hideki
Project Professor *Tamura, Motohide
Associate Professor
Minowa, Yosuke
Associate Professor
Tanaka, Masayuki
Project Associate
Kambe, Eiji
Professor
Project Associate
Oya, Shin
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
Komiyama, Yutaka
Assistant Professor *Kotani, Takayuki
Assistant Professor
Koyama, Yusei
Assistant Professor
Moritani, Yuki
Assistant Professor *Nakajima, Tadashi
Assistant Professor
Okamoto, Sakurako
Assistant Professor
Okita, Hirofumi
Assistant Professor
Onodera, Masato
Assistant Professor
Oono, Yoshito
Assistant Professor
Pyo, Tae-Soo
Assistant Professor *Suto, Hiroshi
Assistant Professor
Yanagisawa, Kenshi
Project Assistant
Hashimoto, Jun
Professor *Project AssistantHori, Yasunori
Professor *Project AssistantIzumi, Takuma
Professor
Project AssistantKuzuhara, Masayuki
Professor *Project Assistant
Livingston, John Henry
Professor *Project Assistant
Shimakawa, Rhythm
Professor
Research Engineer
Bando, Takamasa
Research Engineer
Omiya, Jun
Senior Engineer
Namikawa, Kazuhito
Engineer
Sato, Tatsuhiro(Shunin Gijutsuin)Engineer
Tsutsui, Hironori(Shunin Gijutsuin)Engineer (Gijutsuin)Engineer (Gijutsuin)
Project Research Staff
Project Research Staff
Project Research Staff *Project Research Staff
Project Research Staff *Project Research Staff *Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff *Project Research Staff *Project Research Staff *Project Research Staff *Project Research Staff *Project Research Staff
Project Research Staff
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)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Re-employment Staff

Hirano, Ken
Sawatari, Koichi
Hamano, Satoshi
He, Wanqiu
Ishikawa, Hiroyuki
Kawanomoto, Satoshi
Komatsu, Yu
Krishnamurthy,
Vigneshwaran
Mawatari, Ken
Murata, Kazumi
Nakata, Fumiaki
Nashimoto, Masashi
Nugroho, Stevanus
Kristianto
Omiya, Masashi
Suzuki, Taiki
Takahashi, Aoi
Takarada, Takuya
Wong, Kenneth
Christopher
Yamashita, Takuji
Fujinawa, Toshiyuki
Harasawa, Sumiko
Ishizuka, Yuki
Ishii, Miki
Katakura, Junichi
Kobayakawa, Naoki
Koike, Michitaro
Kusakabe, Nobuhiko
Mineo, Sogo
Morishima, Takahiro
Nakajima, Masayo
Oka, Shinji
Okura, Yuki
Shindo, Miwa
Tanaka, Mitsuhiro
3

III Organization

083

Research Supporter
1
Public Outreach Staff
1
Administrative Supporters 3
Research Assistant Staff 1*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
Izumiura, Hideyuki
Associate Professor
Izumiura, Hideyuki
Project Associate
Tajitsu, Akito
Professor
Assistant Professor
Research Assistant Staff

Maehara, Hiroyuki
3

Nobeyama Radio Observatory
Director
Tatematsu, Ken'Ichi
Professor
Tatematsu, Ken'Ichi
Project Associate
Nishimura, Atsushi
Professor
Assistant Professor
Umemoto, Tomofumi
Engineer (Gishi)
Handa, Kazuyuki
Engineer (Gishi)
Kurakami, TomioEngineer (Gishi)
Miyazawa, Chieko
Engineer (Gishi)
Takahashi, Toshikazu
Senior Specialist
Kinugasa, Kenzou(Tokuninsenmonin)
Senior Specialist
Takahashi, Shigeru(Tokuninsenmonin)
Re-employment Staff
1
Technical Experts
1
Research Supporter
1
Administration Office
General Affairs Unit
Re-employment Staff
1
Administrative Supporters 2
Accounting Unit
LeaderTakami, Masaki
Administrative Supporters 2
Mizusawa VLBI Observatory
Director
Professor
Project Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor

084

III Organization

Honma, Mareki
Honma, Mareki
Kobayashi, Hideyuki
Hada, Kazuhiro
Hirota, Tomoya
Jike, Takaaki
Kameya, Osamu
Kouno, Yusuke
Sunada, Kazuyoshi

Assistant Professor
Tamura, Yoshiaki
Engineer (Gishi)
Ueno, Yuji
Engineer (Gijutsuin)Sato, Gen
Engineer (Gijutsuin)
Takahashi, Ken
Project Research Staff
Akahori, Takuya
Project Research Staff
Kurahara, Kohei
Senior Specialist
Hachisuka, Kazuya(Tokuninsenmonin)
Senior Specialist
Oyama, Tomoaki(Tokuninsenmonin)
Senior Specialist
Ozawa, Tomohiko(Tokuninsenmonin)
Technical Experts
4
Research Supporter
1
Technical Supporter
1
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
Administrative Supporters 2
Time Keeping OfficeDirector
Tamura, Yoshiaki
Solar Science Observatory
Director
Katsukawa, Yukio
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Ishikawa, Ryoko
Associate Professor
Katsukawa, Yukio
Associate Professor
Sekii, Takashi
Assistant Professor
Narukage, Noriyuki
Project Assistant
Benomar, Othman Michel
Professor
Engineer (Gishi)
Shinohara, Noriyuki
Project Research Staff
Matsumoto, Takuma
Senior Specialist
Iju, Tomoya(Tokuninsenmonin)
Senior Specialist
Morita, Satoshi(Tokuninsenmonin)
Research Supporter2
Administrative Supporter 1
Research Assistant Staff 1
NAOJ Chile
Vice-Director
Associate Professor
Engineer (Gishi)
Chile Employees
Chile Employees
Administration Department
Manager

Mizuno, Norikazu
Minamidani, Tetsuhiro
Kobiki, Toshihiko
6
Watanabe, Teruyuki

General Affairs Unit
Staff
Accounting Unit
Senior Staff

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
Iono, Daisuke
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, Koichiro
Professor
Project Associate
Shimajiri, Yoshito
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
Kamazaki, Takeshi
Assistant Professor
Matsuda, Yuichi
Project Assistant
Hull, Charles Lindsay
Professor
Hopkins
Project Assistant
Imada, Hiroaki
Professor
Project AssistantMiyamoto, Yusuke
Professor
Project Assistant
Sanhueza, Nunez Patricio
Professor
Andres
Project Assistant
Tadaki, Kenichi
Professor
Project AssistantUeda, Junko
Professor
Project Assistant
Zavala Sorano, Jorge
Professor
ArmandoResearch Engineer
Nakazato, Takeshi
Research Engineer
Yamada, Masumi
Engineer (Gishi)
Kato, Yoshihiro
Engineer (Gishi)
Nakamura, Kyoko
EngineerIto, Tetsuya(Shunin Gijyutuin)

Engineer(Shunin Gijyutuin)
Engineer(Shunin Gijyutuin)
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
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)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)
Senior Specialist(Tokuninsenmonin)

Nishitani, Hiroyuki
Shizugami, Makoto
Algera, Hiddo SunnyBouwe
Bakx, Tom Johannes
Lucinde Cyrillus
Cataldi, Gianni
Chen, Xiaoyang
Cheng, Yu
Fudamoto, Yoshinobu
Kaneko, Hiroyuki
Kudo, Yuki
Michiyama, Tomonari
Miley, James Maxwell
Nishimura, Yuri
Saito, Toshiki
Sorahana, Satoko
Sugahara, Yuma
Wu, Yu-Ting
Yamagishi, Mitsuyoshi
Yan, Yi
Curotto, Molina Franco
AndreasFujimoto, Yasuhiro
Fukui, Hideharu
Funakawa, Takashi
Hayashi, Yohei
Ikeda, Emi
Kawasaki, Wataru
Konuma, Mika
Miel, Renaud
Nakanishi, Takashi
Nakayama, Susumu
Ohtawara, Kazushige
Shimada, KazuhikoSo, Ryoken
Uemizu, Kazunori
Yoshino, Akira

III Organization

085

Senior Specialist
Zahorecz, Sarolta(Tokuninsenmonin)
Technical Expert
1
Administrative Expert
1
Re-employment Staff
1
Research Supporter
1
Administrative Supporters 3
Research Assistant Staff 1
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 Research Staff
Ishikawa, Shogo
Project Research Staff
Matsumoto, Yuji
Project Research Staff
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

B Projects

Gravitational Wave Science Project
Director
Tomaru, Takayuki
Professor
Tomaru, Takayuki
Associate Professor
Aso, Yoichi
Assistant Professor
Akutsu, Tomotada
Assistant Professor
Leonardi, Matteo
Assistant Professor
Takahashi, Ryutaro
Research Engineer
Ishizaki, Hideharu
Engineer
Tanaka, Nobuyuki(Shunin Gijyutuin)
Project Research Staff
Aritomi, Naoki
Administrative Expert
1
Administrative Supporter 1
Kamioka Branch
Director
Tomaru, Takayuki
Project Research Staff
Chen, Dan
Senior Specialist
Ikeda, Satoru(Tokuninsenmonin)
Administrative Supporter 1
Thirty Meter Telescope (TMT) Project
Director
Usuda, Tomonori
Vice-Director
Aoki, Wako
Professor
Saito, Masao
Professor
Yamashita, Takuya

086

III Organization

Associate Professor
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Research Engineer
Senior Specialist(Tokuninsenmonin)
NAOJ California Office
Professor
Associate Professor
Associate Professor
Assistant Professor
Research Engineer

Aoki, Wako
Noumaru, Junichi
Sugimoto, Masahiro
Terada, Hiroshi
Nishikawa, Jun
Tazawa, Seiichi
Kishimoto, Mayumi

Usuda, Tomonori
Hayashi, Saeko
Suzuki, Ryuji
Yasui, Chikako
Nakamoto, Takashi

A Projects

JASMINE Project
Director
Professor
Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Project AssistantProfessor
Technical Supporter
RISE Project
Director
Professor
Associate Professor
Assistant Professor
Assistant Professor
Research Engineer
Project Research Staff
Administrative Expert

Goda, Naoteru
Goda, Naoteru
Kano, Ryohei
Miyoshi, Makoto
Tatsumi, Daisuke
Tsujimoto, Takuji
Ueda, Akitoshi
Yano, Taihei
Baba, Junichi
1

Namiki, Noriyuki
Namiki, Noriyuki
Matsumoto, Koji
Araki, Hiroshi
Noda, Hirotomo
Asari, Kazuyoshi
Yamamoto, Keiko1

SOLAR-C Project
DirectorHara, Hirohisa
Professor
Hara, Hirohisa
Assistant Professor
Kubo, Masahito
Assistant Professor
Okamoto, Takenori
Engineer (Gishi)
Shinoda, Kazuya
Project Research Staff
Kawabata, Yusuke
Project Research Staff
Oba, Takayoshi
Senior Specialist
Nodomi, Yoshifumi(Tokuninsenmonin)
Administrative Supporter 1
Subaru Prime Focus Spectrograph (PFS) Project
Director
Rousselle, Julien

Subaru Ground Layer Adaptive Optics (GLAO) Project
Director
Minowa, Yosuke
ASTE ProjectActing Director

Kamazaki, Takeshi

Centers
Astronomy Data Center
Director
Associate Professor
Associate Professor
Associate Professor
Associate SeniorResearch Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
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
Professor
Professor
Professor
Project Professor
Executive Engineer
Associate Professor
Associate Professor

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

Uzawa, Yoshinori
Motohara, Kentarou
Miyazaki, Satoshi
Motohara, Kentarou
Uzawa, Yoshinori
Mitsuda, Kazuhisa
Hirabayashi, Masayuki
Kojima, Takafumi
Makise, Kazumasa

Associate Professor
Matsuo, Hiroshi
Associate Professor
Shan, Wenlei
Senior Research Engineer Fujii, Yasunori
Senior Research Engineer Fukushima, Mitsuhiro
Senior Research Engineer Kanzawa, Tomio
Senior Research Engineer Okada, Norio
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
Fukuda, Takeo(Shunin Gijyutuin)
Engineer
Hirata, Naoatsu(Shunin Gijyutuin)
Engineer
Hoshino, Masayuki(Shunin Gijyutuin)
Engineer
Ikenoue, Bungo(Shunin Gijyutuin)
Engineer
Inata, Motoko(Shunin Gijyutuin)
Engineer
Iwashita, Hikaru(Shunin Gijyutuin)
Engineer
Mitsui, Kenji(Shunin Gijyutuin)
Engineer
Miyachi, Akihira(Shunin Gijyutuin)
Engineer
Waseda, Koichi(Shunin Gijyutuin)
Engineer (Gijyutsuin)
Sakai, Ryo
Engineer (Gijyutsuin)
Shimizu, Risa
Project Research Staff
Nagai, Makoto
Senior Specialist
Kusumoto, Hiroshi(Tokuninsenmonin)
Senior Specialist
Saito, Sakae(Tokuninsenmonin)
Re-employment Staff
1
Technical Experts
2
Administrative Supporters 3
Research Assistant Staff 1
Senior Specialist
1(Tokuninsenmonin)

III Organization

087

Public Relations Center
Director
Project Professor
Project Professor
Associate Professor
Associate Professor
Associate Professor(Senior Lecturer)
Associate Professor(Senior Lecturer)
Research Engineer
Engineer(Shunin Gijyutuin)
Project Research Staff
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 Supporter
Public Outreach Staff
Public Relations Office

Yamaoka, Hitoshi
Oishi, Masatoshi
Watanabe, Junichi
Agata, Hidehiko
Yamaoka, Hitoshi
Hanayama, Hidekazu
Hiramatsu, Masaaki
Katayama, Masato
Nagayama, Shogo
Shibata, Takashi
Blumenthal, Kelly Anne
Filipecki Martins, Suzana
Ishikawa, Naomi
Komiyama, Hiroko
Lundock, Ramsey Guy
Pires, Canas Lina Isabel
3
2
2
1
14
Yamaoka, Hitoshi

Outreach and Education OfficeDirector
Agata, Hidehiko
Ephemeris Computation OfficeDirector
Katayama, Masato
Spectrum Management OfficeDirector
Oishi, Masatoshi
Library Unit
LeaderTamefusa, Mizuho
Publications OfficeDirector
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

088

III Organization

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 AssistantProfessor
Project AssistantProfessor
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Project Research Staff
Administrative Experts
Research Supporter
Administrative Supporter
Research Assistant Staffs

Nomura, Hideko
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, Jun-Ichi
Moriya, Takashi
Arzoumanian, Doris
Furuya, Kenji
Nagakura, Hiroki
Nakajima, Kimihiko
Sano, Hidetoshi
Sugiyama, Naonori
Suzuki, Akihiro
Takahashi, Sanemichi
Taniguchi, Kotomi
Tsukagoshi, Takashi
Burns, Ross Alexander
Ito, Yuichi
Kobayashi, Masato
Nozawa, Takaya
Ogami, Takayuki
2
1
1
3

5. Research Support Departments
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
Fukui, Hideharu(Tokuninsenmonin)
Senior Specialist
Hori, Kuniko(Tokuninsenmonin)
Senior Specialist
Noda, Noboru(Tokuninsenmonin)
Senior Specialist
Okamoto, Koichi(Tokuninsenmonin)
Senior Specialist
Suzui, Mitsukazu(Tokuninsenmonin)
Research Assessment Support OfficeDirector
Saito, Masao
Assistant Professor
Ishizuki, Sumio
Senior Specialist
Hori, Kuniko(Tokuninsenmonin)
Industry Liaison OfficeDirector
Hayano, Yutaka
Office of International Relations
Director
Sekiguchi, Kazuhiro
Senior Specialist
Chapman, Junko(Tokuninsenmonin)
Senior Specialist
Kakazu, Yuko
(Tokuninsenmonin)
Senior Specialist
Matsumoto, Mizuho(Tokuninsenmonin)
Research Supporters
1
Support Desk
Research Supporters2
Human Resources Planning OfficeDirector
Noda, Noboru
Safety and Health Management OfficeDirector
Okamoto, Koichi
Technical Expert
1
Engineering Promotion OfficeDirector
Senior Specialist(Tokuninsenmonin)
IT Security Office

Mitsuda, Kazuhisa
Suzui, Mitsukazu

Director
Iguchi, Satoru
Vice Director
Oe, Masafumi
Senior Research Engineer Nakamura, Koji
Associate Professor
Oe, Masafumi(Senior Lecturer)
Engineer
Matsushita, Sayaka
Senior Specialist
Shingu, Uken
(Tokuninsenmonin)
Administrative Expert
1
Administration Department
General Manager
Manager forSpecialMissions(International Relations)
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
Re-employment Staff
Administrative Expert
Administrative Supporter
Personnel Unit
Leader
Staff
Staff
Staff
Administrative Expert
Payroll Unit
Leader
Staff
Staff
Staff
Staff
Administrative Supporters
Employee Affairs Unit
LeaderFujita, Hisashi
Seto, Yoji

Harada, Eiichiro

Nagata, Yuki
Onishi, Tomoyuki
Kawashima, Ryota
Yoshimura, Tetsuya
Ito, Yuko
Murakami, Sachiko
Suzuki, Yoshihiro
1
Kawashima, Ryota
Isozaki, Yuka
Saito, Masahiro
2
1
1
Chiba, Yoko
Matsukura, Koji
Okawa, Makoto
Ouchi, Kaori
1
Furukawa, Shinichiro
Fukuhara, Miyuki
Inoue, Wakaho
Takahashi, Sachiko
Yokota, Banri
2
Yamaura, Mari

III Organization

089

StaffManabe, Yuta
Staff
Tanaka, Masashi
Administrative Expert
1
Research Promotion GroupManager
Hosoya, Akio
Senior Specialist
Seto, Yoji
(International Relations)
Specialist
Ihara, Hiroko(External Funding)
Senior Specialist
Baba, Takashi(Tokuninsenmonin)
Research Support Unit
LeaderGoto, Michiru
Administrative Expert
1
Administrative Supporter 1
External Funding Unit
Specialist
Ihara, Yuko
(External Funding)Staff
Kashiwa, Hidekazu
Administrative Supporters 2
Graduate Student Affairs Unit
LeaderKitabayashi, Kaya
Administrative Experts 2
Administrative Supporter 1
International Academic Affairs Unit
LeaderSato, Yoko
Financial Affairs GroupManager
Kawazu, Hironori
Deputy Manager
Iwashita, Kanefumi
Specialist (Audit)
Tsukano, Satomi
General Affairs Unit
LeaderKikkawa, Hiroko
Staff
Naraoka, Aone
Administrative Supporter 1
Budget Unit
LeaderYamamoto, Shinichi
Staff
Sugimoto, Naomi
Administrative Supporter 1
Asset Management Unit
LeaderIshikawa, Junya
Senior Staff
Okubo, Kazuhiko
Receiving Unit
LeaderIshikawa, Junya
Administrative Supporters 5
Accounting GroupManager
Tahara, Yuji
Specialist (Contracts)
Sato, Kanako
Accounting Unit
Leader
Akeno, Aya
Administrative Supporters 2
Procurement Unit
Leader
Miura, Susumu
Senior Staff
Nakagawa, Yukie

090

III Organization

Staff
Administrative Expert
Administrative Supporter
Facilities GroupManager
Deputy Manager
Senior Specialist
General Affairs Unit
LeaderStaff
Administrative Supporter
Facilities Direction Unit
LeaderAdministrative Supporters
Maintenance Unit
Leader
Staff
Staff

Morita, Akitsugu
1
1
Kataoka, Toru
Murakami, Kazuhiro
Yamanouchi, Mika
Yamanouchi, Mika
Hiramatsu, Naoya
1
Murakami, Kazuhiro
2
Watanabe, Tsuyoshi
Hayashi, Yuki
Kawahara, Iori

6. Personnel Change
Research and Academic Staff
Date
Name
2021/4/1
Ikoma, Masahiro
2021/4/1
Tominaga, Nozomu
Hirabayashi,
2021/5/1
Masayuki2021/9/1
Moritani, Yuki
2021/11/1 Okamoto, Takenori
Hanayama,
2022/3/1
Hidekazu

Change
Hired
Hired
Hired
Hired
Hired
Hired

New Affiliated Institute, Position
Division of Science, Professor
Division of Science, Professor
Advanced Technology Center, Executive
Engineer
Subaru Telescope, Assistant Professor
SOLAR-C Project, Assistant Professor
Public Relations Center, Associate
Professor (Senior Lecturer)
Astronomy Data Center, Associate SeniorResearch Engineer

Previous Affiliated Institute, Position(Public Relations Center, Project
Researcher)(ALMA Project, Senior Specialist)

2022/3/1

Morita, Eisuke

Hired2022/1/31

Iwata, Ikuru

Resigned

2022/1/31
2022/3/31

Ashitagawa, Kyoko
Komiyama, Yutaka

Resigned
Resigned

Thirty Meter Telescope Project,
Associate Professor
ALMA Project, Research Engineer
Subaru Telescope, Assistant Professor

2021/5/14

Takato, Naruhisa

Departed

Subaru Telescope, Professor

2022/3/31

Okada, Norio

RetiredAdvanced Technology Center, SeniorResearch Engineer2022/3/31

Kameya, Osamu

RetiredMizusawa VLBI Observatory,
Assistant Professor

2022/3/31

Tamura, Yoshiaki

RetiredMizusawa VLBI Observatory,
Assistant Professor

2022/3/31

Ishizaki, Hideharu

Retired2022/3/31

Asari, Kazuyoshi

Retired2021/6/1

Hara, Hirohisa

Promoted

SOLAR-C Project, Professor

SOLAR-C Project, Associate
Professor

2021/6/1

Hiramatsu, Masaaki

Promoted

Public Relations Center, Associate
Professor (Senior Lecturer)

ALMA Project, Assistant Professor

2021/6/21

Ishikawa, Ryoko

Promoted

Solar Science Observatory, Associate
Professor

SOLAR-C Project, Asistant Professor

2021/10/1

Hayano, Yutaka

Promoted

Subaru Telescope, Professor

Advanced Technology Center,
Associate Professor

2021/11/1

Gonzalez Garcia,
AlvaroPromoted

ALMA Project, Professor

ALMA Project, Associate Professor

2022/2/1

Takiwaki, Tomoya

Promoted

Center for Computational Astrophysics,
Associate Professor

Division of Science, AssistantProfessor

2022/2/1

Suzuki, Ryuji

Promoted

Thirty Meter Telescope Project, Associate
Professor

Thirty Meter Telescope Project,
Assistant Professor

ChangeNew Affiliated Institute, Position

Gravitational Wave Science Project,
Research Engineer
RISE Project, Research Engineer

Engineering Staff
Date

Name

2021/6/1
2021/7/1
2021/10/1
2021/11/1

Hoshino, Masayuki
Sawatari, Koichi
Takahashi, Ken
Sato, Gen

Hired
Hired
Hired
Hired

Advanced Technology Center, Engineer
Subaru Telescope, Engineer
Mizusawa VLBI Observatory, Engineer
Mizusawa VLBI Observatory, Engineer

2021/12/1

Hirata, Naoatsu

Hired

Advanced Technology Center, Engineer

Previous Affiliated Institute,
Position(Gravitational Wave Science Project,
Senior Specialist)

III Organization

091

2021/4/30

Miura, Takuya

Resigned

Subaru Telescope, Engineer

2021/4/1

Namikawa, Kazuhito Promoted

Subaru Telescope, Senior Engineer

2021/4/1

Ueno, Yuji

Promoted

Mizusawa VLBI Observatory, Engineer

2021/4/1

Kaneko, Keiko

Promoted

Advanced Technology Center, Engineer

2021/10/1
2021/10/1

Tsutsui, Hironori
Shizugami, Makoto

Promoted
Promoted

Subaru Telescope, Engineer
ALMA Project, Engineer

Administrative Staff

092

Previous Affiliated Institute,
Position(Tokai National Higher Education andResearch System)(Japan Society for the Promotion of
Science)Name

2021/4/1

Fujita, Hisashi

Hired2021/4/1

Kawazu, Hironori

Hired2021/4/1

Kataoka, Toru

Hired

2021/4/1

Watanabe, Tsuyoshi

Hired2021/4/1

Inoue, Wakaho

Hired2021/7/1

Kogawa, Hiroshi

Hired2021/10/1

Kawahara, Iori

Hired

2021/11/1

Kashiwa, Hidekazu

Hired2021/6/30

Yamaguchi,
Shin'ichi

Resigned(Iwate University)

Mizusawa VLBI Observatory
Administration Office Accounting
Unit, Leader

2021/7/31

Uchiyama,
Yoshifumi

Resigned(Shinshu University)

Nobeyama Radio Observatory
Administration Office Accounting
Unit, Senior Staff

2021/9/30

Kayamori, Shinji

Resigned

2022/3/31

Nagata, Yuki

Resigned(National Institution For Youth Education)

Administration Department General
Affairs Group, Manager

2022/3/31

Iwashita, Kanefumi

Resigned(The University of Tokyo)

Administration Department Financial
Affairs Group, Deputy Manager

2022/3/31

Tamefusa, Mizuho

Resigned(The University of Tokyo)

Public Relations Center
Administration Office Library, Leader

2022/3/31

Akeno, Aya

Resigned(Tokyo Medical and Dental University)

Administration Department
Accounting Group Accounting Unit,
Leader2022/3/31

Tsukano, Satomi

Resigned(Tokyo Medical and Dental University)

Administration Department Financial
Affairs Group, Specialist (Audit)

PromotedNational Institutes of Natural Sciences
Administrative Bureau General Affairs
Division, Senior Staff (Ministry of
Education, Culture, Sports, Science andTechnology-Japan, Administrative Intern
Trainee)

Administration Department General
Affairs Group Personnel Unit, Staff

Sakamoto, Misato

III Organization

New Affiliated Institute, Position

Advanced Technology Center,
Engineer
Subaru Telescope, Engineer
ALMA Project, EngineerDate2021/4/1

ChangeSubaru Telescope, Engineer
Mizusawa VLBI Observatory,
Engineer

Administration Department, General
Manager
Administration Department Financial
Affairs Group, Manager
Administration Department Facilities
Group, Manager
Administration Department Facilities
Group Maintenance Unit, Leader
Administration Department General
Affairs Group Payroll Unit, Staff
Mizusawa VLBI Observatory
Administration Office Accounting Unit,
LeaderAdministration Department Facilities
Group Maintenance Unit, Staff
Administration Department Research
Promotion Group Resaerch Support Unit
(External Funding), Staff(The University of Tokyo)(Japan Aerospace Exploration
Agency)(Iwate University)

Administration Department General
Affairs Group Payroll Unit, Staff

2021/4/1

Yamafuji, Yasuto

Promoted

NAOJ Chile Administration Office
Accounting Unit, Senior Staff

NAOJ Chile Administration Office
Accounting Unit, Staff

2021/4/1

Okubo, Kazuhiko

Promoted

Administration Department Financial
Affairs Group Asset Management Unit,
Senior Staff

Administration Department Financial
Affairs Group Asset Management
Unit, Staff

2021/4/1

Nakagawa, Yukie

Promoted

Administration Department Accounting
Group Procurement Unit, Senior Staff

Administration Department Research
Promotion Group Research Support
Unit, Staff

2021/7/1

Yoshimura, Tetsuya

Promoted

Administration Department General
Affairs Group, Specialist (Personnel)

2021/8/1

Furuhata, Tomoyuki

Promoted

Subaru Telescope Administration
Department, Manager

Administration Department Financial
Affairs Group Budget Unit, Senior
Staff
Administration Department General
Affairs Group, Deputy Manager

2021/4/1

Yokota, Banri

Reassigned

Administration Department Research
Promotion Group, Staff

National Institutes of Natural
Sciences Administrative Bureau
General Affairs Division, Staff(Ministry of Education, Culture,
Sports, Science and TechnologyJapan, Administrative Intern Trainee)2021/8/1

Seto, Yoji

Reassigned

Administration Department, Manager forSpecial Missions (International Relations)

Subaru Telescope Administration
Department, Manager

ChangeNew Affiliated Institute, Position

Employee on Annual Salary System
Date

Name

2021/4/1

Watanabe, Junichi

Hired2021/4/1

Taniguchi, Kotomi

Hired2021/4/1
2021/4/1
2021/4/1
2021/4/1

Mawatari, Ken
Saito, Toshiki
Michiyama, Tomonari
Yamagishi, Mitsuyoshi

Hired
Hired
Hired
Hired

2021/4/1

Aritomi, Naoki

Hired2021/4/1
2021/4/1
2021/4/1

Yamamoto, KeikoOba, Takayoshi
Ohgami, Takayuki

Hired
Hired
Hired

2021/4/1

Hachisuka, Kazuya

Hired2021/4/1
2021/4/1

Kobayakawa, Naoki
Funakawa, Takashi

Hired
Hired

Public Relations Center, Project Professor(Distinguished Professor)
Division of Science, Project AssistantProfessor
Subaru Telescope, Project Researcher
ALMA Project, Project Researcher
ALMA Project, Project Researcher
ALMA Project, Project Researcher
Gravitational Wave Science Project,
Project Researcher
RISE Project, Project Researcher
SOLAR-C Project, Project Researcher
Division of Science, Project Researcher
Mizusawa VLBI Observatory, Senior
Specialist
Subaru Telescope, Senior Specialist
ALMA Project, Senior Specialist

2021/4/1

Ozawa, Takeaki

HiredAstronomy Data Center, Senior Specialist

2021/4/1

Kitada, Chihiro
Makiuchi,Shin'ichiro

HiredAstronomy Data Center, Senior Specialist

Hired

Astronomy Data Center, Senior Specialist

2021/4/1

Kusumoto, Hiroshi

Hired2021/4/1

Toukoku, Chihiro

Hired2021/4/1

Watanebe, Yoichi

Hired2021/5/1

Matsumoto, Yuji

Hired2021/5/1

Kurahara, Kohei

Hired2021/4/1

Advanced Technology Center, Senior
Specialist
Advanced Technology Center, Senior
Specialist
Administration Department General
Affairs Group, Senior Specialist
Center for Computational Astrophysics,
Project Researcher
ALMA Project, Project Researcher

Previous Affiliated Institute,
Position(Public Relations Center, Professor)(RISE Project, Project Researcher)(Astronomy Data Center, Senior
Specialist)(Astronomy Data Center, Senior
Specialist)(Advanced Technology Center, Senior
Specialist)

III Organization

093

2021/5/1

Onozato, Hiroki

Hired2021/5/1

Shibata, Takashi

Hired2021/5/1
2021/5/1

Hired
Hired
Hired

ALMA Project, Project Assistant Professor

Hired

Subaru Telescope, Project Researcher

2021/7/1
2021/9/1

Shimada, KazuhikoLo, Yu Hsian
Zavala Solano, Jorge
ArmandoWong, Kenneth
Christopher
Ito, Yuichi
Komiyama, Hiroko

Astronomy Data Center, Project
Researcher
Public Relations Center, Project
Researcher
ALMA Project, Senior Specialist
IT Security Office, Senior Specialist

Hired
Hired

2021/9/1

Nagakura, Hiroki

Hired2021/9/27

Arzoumanian, Doris

Hired

2021/9/30

Kobayashi, Masato

Hired2021/10/1

Nishimura, Atsushi

Hired2021/10/1

Kurahara, Kohei

Hired2021/10/1

Cheng, Yu
Algera, Hiddo
Sunny Bouwe
Zahorecz, Sarolta
Konuma, Mika
Filipecki Martins,
Suzana

Hired

Division of Science, Project Researcher
Public Relations Center, Senior Specialist
Division of Science, Project AssistantProfessor
Division of Science, Project AssistantProfessor
Division of Science, Project Researcher
Nobeyama Radio Observatory, Project
Associate Professor
Mizusawa VLBI Observatory, Project
Researcher
ALMA Project, Project Researcher

Hired

ALMA Project, Project Researcher

Hired
Hired

ALMA Project, Senior Specialist
ALMA Project, Senior Specialist

Hired

Public Relations Center, Senior Specialist

2021/11/1

Suzuki, Yoshihiro

Hired

Administration Department General Affairs
Group, Senior Specialist

2021/12/1

Burns, Ross
Alexander

Hired

Division of Science, Project Researcher

2022/2/1

Tokoku, Chihiro

Hired

Advanced Technology Center, Project
Assistant Professor

2022/3/1

Blumenthal, Kelly
Anne

Hired

Public Relations Center, Senior Specialist

2021/6/30

Watanebe, Yoichi

Resigned

2021/7/31

Song, Donguk

Resigned

2021/8/31

Nishikawa, Tomoko

Resigned

2021/8/31

Usuda, Kumiko

Resigned

2021/6/10
2021/7/1

2021/11/1
2021/11/1
2021/11/1
2021/11/1

2021/9/30

Hansen, Izumi Ka
Hoku Hula O Kekai
Inoue, Shigeki

2021/9/30

Kurahara, Kohei

Resigned

2021/9/30 Lu, Xing
2021/10/31 Lee, Seokho
2021/10/31 Zahorecz, Sarolta

2021/8/31

094(ALMA Project, Project Researcher)(ALMA Project, Project Researcher)(Subaru Telescope, Senior Specialist)

Administration Department General
Affairs Group, Senior Specialist
Solar Science Observatory, Project
Researcher
ALMA Project, Senior Specialist
Public Relations Center, Senior
Specialist
Public Relations Center, Senior
Specialist
ALMA Project, Project Researcher

Resigned
Resigned(Mizusawa VLBI Observatory, Project
Researcher)

ALMA Project, Project Researcher

Resigned
Resigned
Resigned(ALMA Project, Senior Specialist)

2021/11/30 Hirata, Naoatsu

Resigned(Advanced Technology Center, Engineer)

ALMA Project, Project Researcher
ALMA Project, Project Researcher
ALMA Project, Project Researcher
Gravitational Wave Science Project,
Senior Specialist

2022/1/31

Resigned(Advanced Technology Center, Project
Assistant Professor)

Tokoku, Chihiro

III Organization

Subaru Telescope, Senior Specialist2022/2/28

Hanayama,
Hidekazu

Resigned

2022/2/28

Horiuchi, Takashi

Resigned

2022/2/28

Morita, Eisuke

Resigned

2022/3/31

Shimajiri, Yoshito

Resigned

2022/3/31

Miyamoto, Yusuke

Resigned

2022/3/31

Sano, Hidetoshi

Resigned

2022/3/31

Suzuki, Akihiro

Resigned

2022/3/31

Ishikawa, Shogo

Resigned

2022/3/31

Saito, Toshiki

Resigned

2022/3/31

Kawabata, Yusuke

Resigned

2022/3/31

Kakuwa, Jun

Resigned

2021/4/30

Nishie, Suminori

2021/6/13

Guzman Fernandez,
Andres Ernesto

2021/8/31

Saigo, Kazuya

2021/9/11

Tsuzuki, Hiroko

2022/1/31

Tokuda, Kazuki

2022/3/30

Kurasaki, Takaaki

2022/3/31

Izumi, Takuma

2022/3/31

Matsumoto, Takuma

2022/3/31

Nashimoto, Masashi

2022/3/31

Nishimura, Yuri

2022/3/31

Yamagishi,
Mitsuyoshi

2022/3/31

Yang, Yi

2022/3/31

Chen, Dan

2022/3/31

Ohgami, Takayuki

2022/3/31

Nozawa, Takaya

2022/3/31

Kinugasa, Kenzo

2022/3/31

Takahashi, Shigeru

Contract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
ExpiredContract
Expired(Public Relations Center, Associate
Professor (Senior Lecturer))(Astronomy Data Center, Associate SeniorResearch Engineer)

Public Relations Center, Project
Researcher
Public Relations Center, Project
Researcher
ALMA Project, Senior Specialist
ALMA Project, Project Associate
Professor
ALMA Project, Project AssistantProfessor
Division of Science, Project AssistantProfessor
Division of Science, Project AssistantProfessor
Center for Computational
Astrophysics, Project Researcher(ALMA Project, Project AssistantProfessor)

ALMA Project, Project Researcher
SOLAR-C Project, Project Researcher
Astronomy Data Center, Project
Researcher
ALMA Project, Senior Specialist
ALMA Project, Project Researcher
ALMA Project, Project AssistantProfessor
Public Relations Center, Senior
Specialist
ALMA Project, Project Researcher
Project Professor(ALMA Project, Project Researcher)

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

Gravitational Wave Science Project,
Project Researcher
Division of Science, Project
Researcher
Division of Science, Project
Researcher
Nobeyama Radio Observatory, Senior
Specialist
Nobeyama Radio Observatory, Senior
Specialist

III Organization

095

2022/3/31

Morita, Satoshi

2022/3/31

Fujimoto, Yasuhiro

2022/3/31

Kishimoto, Mayumi

2022/3/31

Saito, Sakae

Contract
ExpiredContract
ExpiredContract
ExpiredContract
Expired(Solar Science Observatory, Senior
Specialist)

Solar Science Observatory, Senior
Specialist
ALMA Project, Senior Specialist
Thirty Meter Telescope Project, Senior
Specialist
Advanced Techonology Center, Senior
Specialist

Research Administrator Staff
Date

Name

Change2022/3/31

Okamoto, Koichi

Contract
Expired2022/3/31

Fukui, Hideharu

Contract
ExpiredNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Research Enhancement Strategy
Office (Safety and HealthManagement Office),
Senior Specialist(ALMA Project, Senior Specialist of
Employee on Annual Salary System )Research Enhancement Strategy
Office (ALMA Project), Senior
Specialist

Foreign Visiting Researcher
There were no Foreign Visiting Researchers this Fiscal Year, due to the effects of the novel coronavirus.

096

III Organization

7. Advisory Committee for Research and Management
Members
From universities and related institutes○ Doi, Mamoru
Professor at the Graduate School of Science, University of Tokyo
Fujisawa, Kenta
Professor at the Research Institute for Time Studies, Yamagichi University
Inutsuka, Shuichiro
Professor at the Graduate School of Science, Nagoya University
Kawakita, Hideyo
Professor at the Faculty of Science, Kyoto Sangyo University
Kodama, Tadayuki
Professor at the Graduate School of Science, Tohoku University
Kusano, Kanya
Professor at the Institute for Space-Earth Environmental Research, Nagoya University
Ohashi, Masatake
Professor at the Institute for Cosmic Ray Research, University of Tokyo
Sakai, Nami
Chief Scientist at the RIKEN
Takada, Masahito
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
From NAOJ
Fukagawa, Misato
Iguchi, Satoru
Kobayashi, Hideyuki
Kokubo, Eiichiro
Mituda, Kazuhisa
Nomura, Hideko
Saito, Masao
Uzawa, Yoshinori● Watanabe, Junichi
Yoshida, Michitoshi

Professor in ALMA ProjectVice-Director General (on Finance)
Project Professor in the Mizusawa VLBI Observatory
Professor in the Center for Computational Astrophyscis
Director of Engineering
Professor in the Division of Science
Director of Research Coordination
Professor in the Advanced Technology Center
Vice-Director General (on General Affairs)
Professor in Subaru Telescope● Chairperson ○ Vise-Chairperson
Period: June 18, 2020 – March 31, 2022

III Organization

097

8. Professors Emeriti
Professors Emeriti (NAOJ)

098

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
Miyamoto, Masanori
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 2021)
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
9,962,017
1,444,111
1,535,146
27,666464,864
013,433,804
Budget9,989,683
3,767,678
6,222,005
1,444,111
1,535,146
464,864
13,433,804
Budget0

Final Account10,753,314
834,8031,445,146
139,839448,798
5,635
13,627,535
Final Account10,763,788
3,572,220
7,191,568
834,8031,445,146
339,693
13,383,430
Final Account244,105(Unit: ¥1,000)
Budget − Final Account−791,297
609,308
90,000−112,173
16,066−5,635−193,731
Budget − Final Account−774,105
195,458−969,563
609,308
90,000125,171
50,374
Budget − Final Account−244,105

IV Finance099

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2021
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

11

73,80022,14095,940

2
4
9
16
8
2
2
54

59,900101,700
68,60051,600
9,200
1,900
1,190
367,890

17,97030,51020,580
15,4802,520
0
0109,200

77,870132,210
89,18067,08011,7201,900
1,190
477,090

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding
23,1006,930
17,800
5,340
1,900
570
2,200
660
8,300
2,490
53,30015,990Total
30,03023,1402,470
2,860
10,79069,2902. Series of Multi-year Funds for FY 2021
Research Categories
Scientific Research (C)Early-Career Scientists
Challenging Research (Pioneering)Research Activity Start-up
Promotion of Joint International Research
Total

100

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

Number of Selected Projects
27
23
1
2
3
56

VI Research Collaboration
1. Open Use
TypeOpen Use at
Project/Center

Project/Center

Category

Number of
Total
Accepted Number of
Proposals Researchers

Notes

Subaru Telescope
Subaru Telescope
Okayama Branch

Subaru Telescope

71

490 (94)59 Institutes, 12 Countries

SEIMEI Telescope37

152 (2)

9 Institutes, 1 Country

Solar Science
Observatory
Nobeyama Radio
Observatory
Mizusawa VLBI
Observatory

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

*
**

*
**

*
**

45-m telescope (Regular Program)

16

120 (55)

49 Institutes, 17 Countries

VERA

29

141 (110)

46 Institutes, 19 Countries

Astronomy Data Center

336

336 (23)

81 Institutes, 14 Countries

Center for Computational Astrophysics
Facility Use
Advanced
Technology Center Joint Research and Development

330
13
22

330 (19)
63 Institutes, 6 Countries
46
5 Institutes
81
12 Institutes
4429(3858) 397 Institutes, 44 Countries

ALMA Project

ALMA (Cycle 7)

398

ASTE
***
***
***
RISE Project000
Joint Development Research
8
7 Institutes, 0 Countries
Research Assembly
12
8 Institutes, 0 Countries
NAOJ Symposium0
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 7) is from October 2019 to September 2021 due to a period of interruption caused by the spread of
COVID-19.
* The observation data is open to the public on the web. No application is needed to use the data.
** Since the functions of the Hinode Science Center have shifted to the Astronomy Data Center, there is no procedure of application
and adoption as “Hinode.”***ASTE has cancelled the joint-use observations scheduled for FY 2021 due to the spread of the COVID-19 and malfunctions. The
possibility of postponing adopted observation proposals to the following fiscal year or later is being considered.

VI Research Collaboration1012. Commissioned Research Fellows
Visiting Scholars (Domestic)
Host Project/Center/
Division

Name

Position at NAOJ

Affiliated Institute

PeriodTakahashi,
KeitaroVisiting Professor

Faculty of Advanced Science and Technology,
Kumamoto University

2021/4/1–2022/3/31

Kawaguchi,
Toshihiro

Visiting Associate
Professor

Faculty of Economics, Management and2021/4/1–2022/3/31
Information Science, Onomichi City University

Advanced Technology
CenterNishimura,NobuyaVisiting Research
Fellow

RIKEN

Division of Science

2021/4/1–2022/3/31

Mizusawa VLBI
Observatory

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

Acceptance Period

Impacts of astrophysical magnetized plasma on the related
nucleosynthesis

2021/10/1–2022/3/31

Nakamura,
Fumitaka

2021/4/1–2024/3/31

Shimojo, Masumi

2021/4/1–2024/3/31

Honma, Mareki

2021/4/1–2024/3/31

Fujii, Yuka

2021/4/1–2021/9/30

Nagai, Hiroshi

2021/4/1–2022/3/31

Sekii, Takashi

2020/4/1–2022/3/31

Kokubo, Eiichiro

NameLuo, Yudong
Namekata, Kosuke
Yoshiura, Shintaro
Uyama, Taichi
Sakemi, Haruka
Hatta, Yoshiki
Arakawa, Sota

Observational and numerical studies of solar and stellar
magnetic activities
Analysing the 21cm line at the Epoch of Reionisation using
the sparse modelling
Developing exoplanetary science by high-contrast imaging
Analysis of magnetic fields and feedback of a jet terminal
region through radio observation
Mixed-mode asteroseismology of stellar rotation
The birth environment of the Solar System unraveled by thethermal history of small bodies

Host Researcher

Shoda, Munehito

Simulation and observation study of the solar wind
acceleration

2019/4/1–2022/2/28

Katsukawa, Yukio

Baba, Shunsuke

Study of a link between AGN torus formation and circumnuclear starbursts

2019/4/1–2021/9/30

Imanishi, Masatoshi

Ueda, Takashiro

Probing rocky and icy planetesimal formation through twodimensional simulations of gas and dust co-evolution

2019/4/1–2022/3/31

Kataoka, Akimasa

Washimi, Tatsuki

Evaluation of the glitch noise for burst gravitational wave
detection

2019/4/1–2022/3/31

Tomaru, Takayuki

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

102

VI Research Collaboration

Period2020/11/30–2022/11/29
2020/11/30–2022/11/29

Host Researcher
Aso, Yoichi
Leonardi, Matteo

VII Graduate Education
1. Department of Astronomical Science, School of Physical Sciences,
SOKENDAI (The Graduate University for Advanced Studies)
SOKENDAI (The Graduate University for Advanced
Studies) was established in 1988 as an independent graduate
university without undergraduate courses via partnerships withinter-university research institutes for the purpose of advancing
graduate education.
There used to be four schools – Cultural and Social
Studies, Mathematical and Physical Sciences, Life Science,and Advanced Sciences before the reorganization of Schoolof Mathematical and Physical Sciences into the schools ofPhysical Sciences, High Energy Accelerator Science, andMultidisciplinary Sciences in April 2004. Now the total ofsix schools are 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.
(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 and 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 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 the economical basis
upon which they can develop into young researchers skilledin conducting research effectively, the department has set
up the Associate Researcher program in addition to the
Research Assistant system. In addition, the department has
introduced the ‘NAOJ Junior Fellow’ system from FY 2020
to create an environment in which outstanding students candevote themselves more to their studies and research, and tofurther improve the standards of researchers produced by thedepartment.
In FY 2021 there were 8 NAOJ Junior Fellows, 19 Associate
Researchers, and 2 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 Education

103

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

In FY 2021, 26 students participated in the SOKENDAI
Summer Students program. The Asian Winter School, conducted
online, received 499 applications from 15 countries, and ofthese, 257 students participated in the program. In addition,
45 students participated in the Spring School, which was also
conducted online.

(7) Number of Affiliated Staff (2022/3/31)
Chair of the Department of Astronomical Science
Optical and Infrared Astronomy Course
Professors
Associate Professors
Assistant Professors
Radio Astronomy Course
Professors
Associate Professors
Associate Professor (Senior Lecturer)
Assistant Professors
General Astronomy and Astrophysics Course
Professors
Associate Professors
Associate Professors (Senior Lecturers)
Assistant Professors
Total

1
10
8
10
10
11
1
18
9
16
2
19
115

(8) Graduate Students (30 students)

104

1st year (5 student)
Name
Ikeda, Ryota
Ishigami, Shun

Principal Supervisor
Supervisor
Iono, Daisuke
Tadaki, KenichiHara, Hirohisa
Katsukawa, Yukio

Koshisaka, Shiori

Kotani, Takayuki

Fukagawa, Misato

Nishigaki, Moka

Ouchi, Masami

Takata, Tadafumi

Statistical Study for Galaxies at the Early Formation Stage
Identified by Machine-Learning Technique

Yoshida, Tomohiro

Nomura, Hideko

Fukagawa, Misato

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

2nd year (6 students)
Name

Principal Supervisor

Ishihara, Kousuke

Saito, Masao

Sasaki, Shunsuke

Takiwaki, Tomoya

Supervisor
Nakamura,
Fumitaka
Machida, Mami

Sugimori, Kanako

Tanaka, Masayuki

Iwata, Ikuru

Tada, Shotaro

Kotani, Takayuki

Hayano, Yutaka
Minowa, Yosuke

Development of a single-mode fiber spectrometer andcharacterization of exoplanet atmospheres

Doi, Kiyoaki

Kataoka, Akimasa

Nomura, Hideko
Fukagawa, Misato

Unveiling planet formation via protoplanetary disk observations

Naufal,Abdurrahman

Tanaka, Masayuki

Koyama, Yusei

Morphological Evolution of Galaxies across Cosmic
Environment

VII Graduate Course Education

Title of Research Project
Observational Studies of Submillimeter 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

Title of Research Project
The study of high-mass star formation process focusing on thehierarchical fragmentation
Explosion Mechanism of Core-Collapse Supernovae
Evolution of spectral energy distributions of galaxies overcosmic time

3rd year (9 students)
Name

Principal Supervisor

Omae, Rikuto

Machida, Mami

Ouchi, Masami

Kasagi,Yui

Kotani, Takayuki

Hayashi, Saeko
Aoki, Wako

Kashiwagi, Raiga

Iwasaki, Kazunari

Takiwaki, Tomoya

Kobayashi, Umi

Tanaka, Masayuki

Tashima, Yuta

Machida, Mami

Nakanishi, Koichiro
Nakamura,
Fumitaka

Nakano, Suzuka

Nakanishi, Koichiro

Sekii, Takashi

The interplay and co-evolution between galaxies and active
supermassive blackholes

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

Masai, Takaho

Gonzalez, Alvaro

Uzawa, Yoshinori
Kojima, Takafumi

Development of (sub-)mm-wave optics and waveguidecomponents for radio astronomy receivers

Seo, Chanoul

Fujii, Yuka

Nomura, Hideko
Ikoma, Masahiro

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

4th year (2 students)
Name
Takemura, Hideaki

Principal Supervisor
Nakamura, Fumitaka

Nishiumi, Taku

Hori, Yasunori

Supervisor
Hirota, Tomoya
Aoki, Wako
Izumiura, Hideyuki

Title of Research Project
Study of the star formation processes focusing on the CMF
Characterization of exoplanets with MuSCAT series telescopesand MuSCAT series

5th year (8 students)
Name

Principal Supervisor

Supervisor

Ito, Kei

Tanaka, Masayuki

Matsuda, Yuichi

Title of Research Project
The systematical study of a protocluster based on the Subaru
Telescope wide field survey

Isikawa, Ryohtaro

Sekii, Takashi

Katsukawa, Yukio

Study of interactions between turbulence and magnetic fields
with spectro-polarimetric observations

Kambara, Nagaaki

Hara, Hirohisa

Murakami, Izumi(NIFS)

Spectroscopic diagnostics of highly ionised astrophysicalplasmaTsukui, Takafumi

Iguchi, Satoru

Nagai, Hiroshi

Formation and evolution of galactic structures using gas andstellar kinematics

Namiki, Shigeru

Koyama, Yusei

Tanaka, Masayuki

What determines the galaxy morphology? A detailed
comparison between the visual smoothness and various
morphological indicators

Fukagawa, Nao

Aoki, Wako

Iono, Daisuke

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

Cui, Yuzhu

Honma, Mareki

Nagai, Hiroshi

Observational study of jets in active galactic nuclei with theEast Asian VLBI Network

Liang, Yongming

Tanaka, Masayuki

Matsuda, Yuichi

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

Supervisor

Title of Research Project
Study of galactic magnetic field evolution using the polarization
properties of intervening galaxies
Search for extra-solar planets around young to late stars, andbrown dwarfs for understandings planet formation at various
evolutionary stages
A Study on Star Formation Processes in Filamentary Molecular
Clouds by Numerical Simulations
Influence of galaxy interactions and mergers on AGN activities
Study of the galactic magnetic field using the MHD simulationand observational visualization

VII Graduate Course Education

1052. Education and Research Collaboration with Graduate Schools

106

Name
Ikebe, Souta
Nishino, Yohei

Affiliated InstituteSupervisor
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

Development of a camera unit for Y-band high dispersion
spectrograph TARdYS for TAO telescope and evaluation of
NIR array detectors.

Mizutani, Yohsuke
Yano, Yuta
Fariyanto, Elika
Prameswari

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

Theoretical study of formation of planetary systems
Numerical Simulations of Star Formation Process

The University of Tokyo Honma, Mareki

Study of AGN Jets with VLBI observations

Adachi, Hiroaki

The University of Tokyo Fukagawa, Misato

Ogawa, Takuma
Ono, Kyohei
Kofuji, Yutaro

The University of Tokyo Kano, Ryohei
The University of Tokyo Kokubo, Eiichiro
The University of Tokyo Honma, Mareki

Chen, Nuo

The University of Tokyo Motohara, Kentaro

Honda, Yuichi

The University of Tokyo Sakamoto, Seiichi

The study of star formation region by new analysis of
FUGIN data

Morii, Kaho

The University of Tokyo Nakamura, Fumitaka

Testing and Constructing High-mass Star Formation Theories
by ALMA Observations

Moritsuka, Akie

The University of Tokyo Katsukawa, Yukio

Kinoshita, Shinichi

The University of Tokyo Nakamura, Fumitaka

Takamura, Mieko

The University of Tokyo Honma, Mareki

Nakatsuno, Naoki

The University of Tokyo Kano, Ryohei

Mitsuhashi, Ikki

The University of Tokyo Sakamoto, Seiichi

Yoshida, Yuki

The University of Tokyo Kokubo, Eiichiro

Guo, Kangrou

The University of Tokyo Kokubo, Eiichiro

Lee, Sujin
Okino, Hiroki

The University of Tokyo Honma, Mareki
The University of Tokyo Honma, Mareki

Kushibiki, Kosuke

The University of Tokyo Motohara, Kentaro

Hoshino, Haruka

The University of Tokyo Kokubo, Eiichiro

Yamazaki, Yuta

The University of Tokyo Nakamura, Fumitaka

Tatsuuma, Misako

The University of Tokyo Kokubo, Eiichiro

Formation Process of Planetesimals Investigated with
Numerical Calculation of Material Strength of Small Solar
System Bodies

Yamaguchi,
Masayuki

The University of Tokyo Nakamura, Fumitaka

The Statistical Properties of the Detailed Structures of theProtoplanetary Disks in the Taurus Star-forming Region with
ALMA Super-resolution Imaging TechniqueIshizuka, Noriyoshi
Luo, Yudong

The University of Tokyo Katsukawa, Yukio
The University of Tokyo Nakamura, Fumitaka

Study on Magnetic Reconnection Site in Solar Flares
Cosmic time Evolution of r-process isotopic abundances

VII Graduate Course Education

Title of Research Project
Observational research of Fast Radio Bursts
Studies for Gravitational Wave Telescope, KAGRA
Study on an image restoration technique for high-resolution
solar images

Observational Research on Planetary-system Formation
around Young Stars
Study on the Galactic dynamics by the use of astrometric data
Theoritical Study on Formation of Planetary Systems
Imaging super-massive black holes with mm VLBI
Observational Study of Galaxy Formation and Evolution in
the ZFOURGE-COSMOS Field

Study of magneto-convection on the solar surface with
spectro-polarimetric observations
Investigation of triggered star formation by using numericalsimulation
Exploration of the environment of the Narrow-line Seyfert 1
galaxies' core with VLBI
The mechanical effect of central mass concentration on the
double bar structure
Exploration of the star-formation process in high-redshift
galaxies using observations of submillimeter galaxies.
Theoretical Study on Formation of Planetary Systems
Planetesimal Dynamics in the Presence of a Massive
Companion
Observational study of pulsars/magnetars in the radio band
Observational study of AGN jets with Global VLBI
Development of an Integral Field Unit SWIMS-IFU and an
Observational Study of Nearby LIRGs
Theoretical Study on Formation of Planetary Systems
The Evolution of Heavy Elements in the Universe and the
Galaxy3. Commissioned Graduate Students
Doctoral Course

Affiliated Institute

Period2020/10/1–
2021/9/30

Supervisor

Kang, Haoran

The University of Tokyo

Yamasaki, Yasumasa

Osaka Prefecture
University

2021/4/1–
2022/3/31

Kojima, Takafumi

Development of multi-beam and wideband optics
for radio telescope

Huang, Shuo

The University of Tokyo

2021/4/1–
2022/3/31

Kawabe, Ryohei

Multiwavelength Study of Bright Submillimeter
Galaxies

Masui, Sho

Osaka Prefecture
University

2021/4/1–
2022/3/31

Kojima, Takafumi

Development of superconductive circuits

Chin, Kah-wuy

The University of Tokyo

2021/4/1–
2022/3/31

Kawabe, Ryohei

Development of multi-chroic detector for
millimeter/submillimeter multi-chroic camera

Kozuki, Yuto

The University ofElectro-Communications

2021/9/1–
2022/3/31

Uzawa, Yoshinori

Study of Frequency Up-Conversion by SIS
MixersNarita, Kanako

The University of Tokyo

2021/11/1–
2022/3/31

Sakamoto, Seiichi

Observational Study of Material Evolution inInterstellar Space

Master’s Course

Affiliated Institute

Period2020/10/1–
2021/9/30

Gonzalez, Alvaro

Title of Research Project
Study of array receivers in millimeter/
submillimeter waves

Supervisor
Aoki, Wako

Title of Research Project
The Structure of the Andromeda Galaxy’s Stellar
Halo using Subaru/Hyper Suprime-Cam NB515

Ogami, Itsuki

Hosei University

Ishida, Mizuki

Tokyo City University

2021/4/1–
2022/3/31

Agata, HidehikoDevelopment of teaching materials for easy useof astronomical image data in educational fields

Naganuma, Toyo

The University ofElectro-Communications

2021/4/1–
2022/3/31

Uzawa, Yoshinori

Development of the multi-chroic mm/submm
wave camera

Niwa, Ayako

University of Tsukuba

2021/4/1–
2022/3/31

Matsuo, Hiroshi

Development of photon counting THz intensity
interferometry

Noji, Ryohei

University of Tsukuba

2021/4/1–
2022/3/31

Shan, Wenlei

Development of dual-polarization MKIDs forsurface measurements of radio telescopes

Miyazawa, Hiromu

University of Tsukuba

2021/4/1–
2022/3/31

Shan, Wenlei

Development of 1000 pixel MKID arrays for
submillimeter-wave band wide-field observations

Le Ngoc Uyen

The University ofElectro-Communications

2021/6/1–
2022/3/31

Tamura, Motohide

Hydrodynamic Simulations of Giant Impact
between Protoplanets

Katsuki, Riku

The University ofElectro-Communications

2021/8/1–
2022/3/31

Aso, Yoichi

Characterization of the absorption andbirefringence of sapphire substrates used forcryogenic test mass mirrors of interferometricgravitational wave detectors

Kizaki, Taiga

The University ofElectro-Communications

2021/10/1–
2022/3/31

Makise, Kazumasa

Fabrication and characterization of Nb/CuNi/Nb
Josephson junction arrays

Ouchi, Shu

Tokyo University of
Science

2021/10/1–
2022/3/31

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

Abe, Homare

Tokyo Institute ofTechnology

2021/10/1–
2022/3/31

Aso, Yoichi

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

Kawashita, Sana

Osaka Prefecture
University

2021/10/1–
2022/3/31

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

Chinen, Tsubasa

Osaka Prefecture
University

2021/10/1–
2022/3/31

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

Yoneyama, Sho

Osaka Prefecture
University

2021/10/1–
2022/3/31

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

Masukura, Akihiro

Nagoya University

2022/1/1–
2022/12/31

Shan, Wenlei

Research on the superconducting planar circuitfor MMIC SIS receiver

VII Graduate Course Education107

4. Degrees Achieved with NAOJ Facilities
Name

108

DegreeTitle of Research Project
Probing the formation region of relativistic jet in nearby active
galactic nucleus M87 with the East Asian VLBI Network

Cui, Yuzhu

Doctor of Philosophy, SOKENDAI

Ito, Kei

Doctor of Philosophy, SOKENDAIStar Formation Activity of Galaxies and its Relationship toEnvironment in Distant Universe

Tsukui, Takafumi

Doctor of Philosophy, SOKENDAIFormation and Evolution of Galactic Structures Using Gas and Stellar
Kinematics

Namiki, Shigeru

Doctor of Philosophy, SOKENDAI

Origin of the Relation between Galaxy Morphology and its Gas
Content

Isikawa,Ryohtaro

Doctor of Philosophy, SOKENDAI

Observational Studies on Turbulent Convection in the Solar
Photosphere

VII Graduate Course Education

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 (145 days in total): April 25–June 20 and July
12–September 30 (due to COVID-19), November 13(due to equipment inspection), and February 10–14(due to snowfalls)
Visitors: 7,186 (of which 436 were in groups)
As a measure against the COVID-19 pandemic, allgroup activities were suspended, except for thoserecognized as school activities.
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 November 26 to January 16, public access tosolar observation parties and inside the Observatory
History Museum were allowed mainly on Saturdays
and Sundays (but suspended again from January 17
because of a declared state of quasi-emergency).
[Regular Star Gazing Party]
Dates: (On-site) Friday before second Saturday; fourth
Saturday(Online) April–January, fourth Saturday; February–
March, Friday before second Saturday and fourth
Saturday
Visitors: 0 (23 events planned and 0 events held)
Viewers: (On-site) 0 (23 events planned and 0 events held)(Online) Held 13 times, with the total number ofmaximum simultaneous connections reaching 1,359
Total Views: 15,178 (As of March 31, 2022)
All on-site events were canceled due to the
C OV I D -19 p a n d e m i c. O n l i n e e ve n t s we r ebroadcasted via Zoom to YouTube Live.
[4D2U Theater Showings]
Dates: Friday before second Saturday; first and third
Saturdays
Capacity: 42 people per day (reduced due to the COVID-19
pandemic)
Visitors: 340 (35 events planned and 9 events held)
The events scheduled for April to September, October
2 and 8, and February to March (26 events in total)

were canceled as a measure against COVID-19.
[Special Open-House Event] Mitaka Open House Day
Dates: October 22 (Fri.), 2021, 14:00–19:00 (Canceled)
October 23 (Sat.), 2021, 10:00–19:00 (Held online)
Topic: Looking back on the 10 years ALMA's researchfindings
Number of Contents:
Live streams and YouTube Premier events: 21
Video Contents: 45
Others: 37
Total Contents: 103
Total Maximum Simultaneous Connections: 2054
Total Views in the First Month after the Release: 60,300
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).
*As a measure against COVID-19, we had to reduce publicaccess to Mitaka Campus during this fiscal year.

Ishigaki Island: Ishigakijima Astronomical Observatory[Open year-round]
Dates: April to March (except for April 1–September 30*1
and October 1–31*2)
Open Hours: Wednesdays through Saturdays, 10:00–16:30;
Sundays and Holidays, 13:00–16:30 (except for
the New Year’s season; when Monday is a national
holiday, the facility is closed on the following
Tuesday/Wednesday)
Stargazing Sessions: Evenings on Saturdays, Sundays, andHolidays, (19:00–21:00), one 30-minute session perevening
4D2U Theater: 15:30–16:00, from Wednesdays to Sundays
and on Holidays
Visitors: 1,400
Open Facilities: Murikabushi 105-cm optical/infrared
telescope, Hoshizora Manabi no Heya (Starry Sky
Study Room) (featuring the 4D2U “four-dimensional
digital universe” and stargazing sessions with the
40-cm telescope), interior of observation dome, andcorridors (including exhibits of astronomical images)*1 Closed from April 1–September 30 due to a partial closure of
the road leading to the observatory (Maesedake Rindo).
*2 Public access was limited to the outdoor areas due to the
COVID-19 pandemic.

VIII Public Access to Facilities

109

[Special Open Day]
[Southern Island Star Festival 2021] (co-sponsored and held
partially online)
Dates: January 29 (Sat.)–February 6 (Sun.), 2021
Star Festival Live & the Ishigaki Island Starry Sky and Star
Culture Lecture:
Held on January 29 (Sat.) at Ishigaki City Hall, live
streamed with no audience on-site, and viewed 5,290
times on YouTube
Star Festival Memorial Lecture: Held on January 30 (Sun.)
at Ishigaki City Hall with 45 visitors
Star Festival Week Events: Held from January 29 (Sat.)to February 6 (Sun.) at Ishigakijima Astronomical
Observatory with 52 visitors

110

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: 7,991
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.
However, in order to prevent the spread of the novel coronavirus
infection, the Kimura Hisashi Memorial Museum has been
temporarily closed during the following periods: From April 1,
2021 to present[Special Open Day]
In light of the fact that novel coronavirus infections have notyet ended, we consulted with Oshu City and the Oshu Spaceand Astronomy Museum (OSAM: Yugakukan), and decided tocancel this event in consideration of the health and safety of theparticipants and related people, and to prevent the spread of theinfection.

Ishigaki Island: VERA Ishigaki-jima Station[Open year-round]
Dates: April to March (except for 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: 1,698[Special Open day] The Special Open Day was held as a part of
the Southern Island Star Festival.
Dates: January 29 (Sat.), 2022, 18:00–21:00
January 30 (Sun.), 2022, 13:30–16:00
In view of the fact that novel coronavirus infections have notyet ended, this was the first time the event was held in winter,in order to protect the health and safety of the participants andrelated people and to prevent the spread of the infection.
A “Star Festival Commemorative Lecture” was held on thesecond day, and a panel booth was set up at the venue to
distribute VERA goods to participants.

Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for New Year’s season)
Visitors: 1,338[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 torequire that events be cancelled, or at least infection prevention
measures would be needed 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 maincommittee 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: 4,090[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 Facilities1113. Nobeyama Campus[Regular Open Facilities]
Open Time: 8:30–17:00 (every day except around New
Year’s Day (December 29 to January 3))
Visitors: 30,371
Open Facilities: 45-m Radio Telescope, Nobeyama Millimeter
Array, Nobeyama Radioheliograph, etc. (just viewing)[Open House Day] (held online only)
Date: August 28 (Saturday), 2021, 10:00–15:30 (available
for access after the day)Participants: 6715 (total number of views for live stream)
about 130,000 (total number of views for all content
in about the first 30 days)
Nobeyama Open Campus Day 2021 was held online as aprecaution against the spread of COVID-19. The theme was“People who support the science.” We had a special lecture,
which attracts a large audience every year. It was held online
with the title “Developing, repairing, and using observation
instruments: case for radio astronomy” by Associate Prof.
Minamidani, Tetsuhiro (Chile Observatory, NAOJ). The numberof views for this live streaming reached over 3500. Moreover,
the total number of views in the first 30 days was more than
15 thousand. We also proceeded with online streaming content
such as a 4D2U theater, mini lectures led by the ALMA project,demonstration of the 45-m radio telescope, and a live broadcast
from Nobeyama Campus. We prepared many movie contents
including an introduction to our research, a tour inside the 45-m
radio telescope, antenna origami, and so on. Moreover, we had
a “quiz rally,” event for communicating with participants. The
participants look for and collect quiz answers in some movies
and write the answers in a form 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.

112

VIII Public Access to Facilities

4. Subaru Telescope[Summit Facility Tour]
Public tours have been suspended due to various factors
Special tours resumed in September 2021 in a limited way:
2 groups, 8 visitors[Base Facility Tour]Special tours resumed in March 2022 in a limited way:
1 group, 7 visitors[Public information]○ Primary means of public information is posting at the official
website https://subarutelescope.org• Science results from the Subaru Telescope – 15
Japanese and 14 English articles• Depicting special activities or making announcements
on Call for Proposals, recruitment – 34 Japanese and 29
English articles.
○ Web postings are supplemented by social media via official
accounts• Twitter accounts – SubaruTelescope (for Japanese),
SubaruTel_Eng (for English)• Facebook pages – 国立天文台 (for Japanese), National
Astronomical Observatory of Japan, and Subaru
Telescope Hawaii Outreach (for English)• YouTube channels – SubaruTelescopeNAOJ (forJapanese), SubaruTelescopeNAOJe (for English)[Outreach]
1. Lectures, workshops, etc. at nearby facilities:
3 cases, 200 people in total(Breakdown as follows)• Mentorship for high school robotics teams• Judges at 2022 Hawai`i VEX IQ Elementary School State
Championship, in-person tournament• Internal Citizen Science Project “PANOPTES” helped highschool and undergraduate students build a PANOPTES unit.
2. Others1) In person Activities:
4 events, able to interact with about 2,300 people(Breakdown as follows)• AstroDay• AstroDay West• Lili`uokalani Gardens Christmas Light Show (as member of
Maunakea Observatories volunteer group Na Hoku Huihui)• Maunakea Coin Contest (as members of Maunakea Astronomy
Outreach Committee)(Breakdown as follows)• Girl Scout STEM Fest• Hawai`i Island Virtual Career Expo
• Judges at 2022 Hawai`i VEX IQ Elementary School State
Championship, pre-interview• Journey Through The Universe: 8 staff members gave an
online lecture or spoke on a career panel
3. YouTube Live Streaming:
4 cases, about 3,081, 500 views(Breakdown as follows)• Live broadcast of the total lunar eclipse• Live broadcast of the partial lunar eclipse• Live broadcast from the summit facility to the live viewing
event of Akashi Municipal Planetarium for the partial lunar
eclipse• Live Talk event hosted by Hamagin Space Science Center*In April 2021, the Subaru Telescope started a 24/7 live
stream from Maunakea with the Subaru-Asahi Star Camera incollaboration with The Asahi Shimbun Company.
4. Volunteer Activities: 8 cases
In addition to traditional outreach activities, staff members
participated in volunteer activities to contribute to the local
community of Hawai`i.
(Main Activities)• 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
The following local annual events were canceled due to the
COVID-19 pandemic:• The Mary Monarch Parade• The Tanabata Hoshimatsuri Festival• Hawaii Explorations Expo
• Onizuka Science Day
5. Media Interview/Filming: 5 cases (4 Japanese, 1 English), 35
articles were featured in Japanese newspapers*Due to the COVID-19 pandemic, the in-person events were
held by minimizing the close contact.
2) Online Activities:
4 events, able to interact remotely with about 2,200 people

VIII Public Access to Facilities113

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

0
0
0
0
0
0
0
0
0
14
5
1
1
1
1
0
0
4
2
0
0
0
11
40

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

0
0
0
0
0
0
0
0
0
14
5
1
1
1
1
0
0
4
2
0
0
0
11
40

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

114

IX Overseas Travel

X Award Winners
Award Recipients

Affiliated Division

Job Title
RCUH; Associate
Professor ; Senior
Specialist; Public
Outreach Staff

Award
Date
FY 2021 The Commendation for Science andTechnology by the Minister of Education,
Culture, Sports, Science and Technology,
2021/4/14
Awards for Science and Technology (Public
Understanding Promotion Category)

Usuda-Sato, Kumiko;
Tanaka, Masayuki; Koike,
Michitaro; Shibata, Junko

Subaru Telescope

Kojima, Takafumi

Advanced
Technology Center

Associate Professor

Kataoka, Akimasa

Division of Science

Assistant Professor

Okayama Branch Office,Subaru TelescopeMoriya, Takashi

Division of Science

Nakajima, Kimihiko

Division of Science

Kataoka, Akimasa
Nugroho, Stevanus
Kristianto

Division of Science

Assistant Professor
Project AssistantProfessor
Assistant Professor

Subaru Telescope

Project Researcher

The 13th Senshu-kai Award

2021/10/30

Public Relations
Center

Associate Professor

Letter of Appreciation for the 70th
Anniversary of Mitaka City (Sports andCulture Division)

2021/11/3

Agata, Hidehiko
Iguchi, Satoru; Saito,
Masao et al.
Ouchi, Masami
Hanayama, Hidekazu
Miyazaki, Satoshi
The SEIMEI Telescope
Kameno, Seiji
Hanayama, Hidekazu
Ishigakijima Astronomical
Observatory, Public
Relations Center
Kataoka, Akimasa

FY 2021 The Commendation for Science andTechnology by the Minister of Education,
2021/4/14
Culture, Sports, Science and Technology,
The Young Scientists’ Award
FY2020 JSPS Outstanding Young Scientist
2021/6/3
Award
Commendation for Meritorious Service to2021/6/17
Tourism and Product Business
FY 2020 The ASJ Young Astronomer Award 2021/9/14
FY 2020 The ASJ Young Astronomer Award 2021/9/14
FY 2020 The ASJ Young Astronomer Award 2021/9/14

FY 2021 Award of Invention and Innovation
ALMA Project; TMTProfessor; Professor in Kinki Region, Invention Encouragement
Project
Award
Division of Science
Professor
Highly Cited Researcher 2021
Public Relations
Associate Professor 2021 Photo Contest of Local LandscapeCenter(Senior Lecturer)
with Starry Sky
Advanced
Professor
FY2021 The 67th Nishina Memorial Prize
Technology Center
The Society of Instrument and Control
Engineers System Integration Department,
Technical Achievement Award
ALMA-JAO Fundamental Statements
ALMA Project
Professor
Awards (Curiosity)
Public Relations
Associate Professor
Letter of Appreciation from Hayabusa 2
Center(Senior Lecturer)

2021/12/17
2021/12/17
2021/12/19

2022/1/5

Nagai, Hiroshi; Nakanishi,
Koichiro; Hull, Charles;
Kameno, Seiji

ALMA Project

Wong, Kenneth
Christopher

Subaru Telescope

Project Researcher

Project Researcher

2021/12/6

FY 2021 NAOJ Young Researchers Award

Project Associate
Professor; Project
FY 2021 Shoichiro Yoshida Memorial/
Associate Professor;
Nikon Astronomy Achievement Award
Project AssistantProfessor; Professor

Gravitational Wave
Science Project2021/11/26

2021/12/19

Assistant Professor

Aritomi, Naoki

2021/11/16

Letter of Appreciation from Hayabusa 2
Division of Science

National Astronomical
Observatory of Japan

2021/11/4

2022/1/31

FY 2021 The ASJ Young AstronomerAward
The 63rd Science and Technology Film/
Video Festival Science Museum Director
Award
The 16th Young Scientist Award of the
Physical Society of Japan

2022/3/4
2022/3/11
2022/3/16

X Award Winners

115

XI Library, Publications
1. Library
Number of books in each library (2022/3/31)
Japanese Books
Mitaka18,452
Nobeyama
1,128
Mizusawa
4,986
Hawai`i
1,699
Total
26,265

Foreign Books
49,227
5,891
18,113
4,683
77,914

Total
67,6797,019
23,0996,382
104,179

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
12
Total
1,061
2,597

Total
2,046
98
1,487
27
3,658

2. Publication
Here we list continuing publications produced by NAOJ in FY 2021.
(Mitaka)01) Report of the National Astronomical Observatory of Japan, Vol. 22: 1 issue (Digital Publication Only).
02) Annual Report of the National Astronomical Observatory of Japan (Japanese), no. 33, Fiscal Year 2020: 1 issue03) Annual Report of the National Astronomical Observatory of Japan (English), vol. 23 Fiscal Year 2020: 1 issue04) Calendar and Ephemeris, 2022: 1 issue05) NAOJ News, No. 333–336: 4 issues06) NAOJ Pamphlet 2021 (Japanese): 1 issue07) Rika Nenpyo (Chronological Scientific Tables), 2022: 1 issue08) Publication of the National Astronomical Observatory of Japan Volume16: 1 issue (Digital Publication Only)

3. Publication Support
In FY 2021, the NAOJ Reprints were replaced by publication support.
National Astronomical Observatory publication support, No. 3479–3580: 101 issues.
(No. 3537 is missing.)

116

XI Library, Publications

XII Important Dates
April 1, 2021 – March 31, 2022
2021
April 3
April 12The Subaru Telescope started the 24/7 live streaming from Maunakea with the Subaru-Asahi Star Camera incollaboration with The Asahi Shimbun Company.
Vice Minister of Education, Culture, Sports, Science and Technology Hinako Takahashi visited Mitaka Campus.

April 14

A press conference “Telescopes Unite in Unprecedented Observations of Famous Black Hole” was held online,with satellite venues at Mizusawa VLBI Observatory and Kagoshima University connected. The conference was
jointly hosted with the University of Tokyo ICRR, Kogakuin University, Hiroshima University, the Graduate
University for Advanced Studies, Ibaraki University, Yamaguchi University, and other institutes, attended by 27
representatives from 23 media organizations.

April 14GALAXY CRUISE members Kumiko Usuda-Sato, Masayuki Tanaka, Michitaro Koike, and Junko Shibata wereawarded The 2021 Commendation for Science and Technology (Public Understanding Promotion Category) by
the Minister of Education, Culture, Sports, Science and Technology.

April 14

Associate professor Takafumi Kojima received the Young Scientists’ Award, 2021 Commendation for Scienceand Technology by the Minister of Education, Culture, Sports, Science and Technology (MEXT) for his study on
the improvement of sensitivity and bandwidth of receivers for radio astronomy.

April 22

Event Horizon Telescope’s research released new learning content, a poster titled “What have we learned? The
Frontiers of Black Hole Research.”

April 30~May 2

Subaru Telescope participated in the AstroDay event at a shopping mall in Hilo on the Island of Hawai`i withminimum contact and distributed bags containing hands-on astronomy kits.

May 6

Radio interferometric observations captured in detail the jets emanating from the center of a galaxy as they bent
within the galaxy cluster.

May 19A press conference “ALMA Discovers the Most Ancient Galaxy with Spiral Morphology” was held online
jointly with SOKENDAI, attended by 15 representatives from 12 media organizations.

May 20Using images of the M87 giant black hole released in 2019 by the Event Horizon Telescope research team to test
various theories of gravity, including general relativity, the team presented that general relativity agrees very
well with the observed data and that there is still room for other theories of gravity to describe the observed
black hole.

May 24

Based on donations from many people to the National Astronomical Observatory of Japan’s Mizusawa VLBI
Observatory, the exterior of the Kimura Hisashi Memorial Hall was repainted between May 27 and June 30,
2021.

May 25~May 26
May 28June 15~June 16
July 7
July 7
July 7
July 9July 19
July 15~July 16
August 3
August 9
August 17
August 18

Subaru Telescope and its internal citizen science project PANOPTES live-broadcasted the total lunar eclipse
from the Island of Hawai`i.
Subaru Telescope's website for children, “Subaru Kids” relaunched in Japanese.
ALMA Data Analysis Workshop (Beginner Level) was held jointly with the Astronomy Data Center online.
In cooperation with the Iwate Prefectural Kenan Regional Promotion Bureau, an exhibition was planned andexhibited at libraries and other venues in the Kenan area through February 2, 2022.
Associate professor Yoshiharu Asaki gave a lecture at Santiago Japanese School in Chile.
Associate Professor (Senior Lecturer) Masaaki Hiramatsu gave an online lecture at a Star Festival Event.
Vice Minister of MEXT Hinako Takahashi visited the National Astronomical Observatory of Japan Mizusawa
VLBI Observatory, in Oshu City, Iwate Prefecture, and listened to presentaions on a wide range of topics fromthe latest astronomical research techniques and results, to the history of this site where astronomical observation
has been conducted since the Meiji Era.
Event Horizon Telescope’s research team took unprecedented high-resolution images of the root of the Centaurus
A jet, pinpointing the location of the giant black hole and revealing how the massive jet is born.
ngVLA Development Days 2021 was held online.
An undergraduate intern of the Akamai Workforce Initiative program, supervised by Subaru Telescope mentors,presented at the Akamai Internship Symposium.
Minister of Education, Culture, Sports, Science and Technology, Koichi Hagiuda, visited the Subaru Telescope.
Professor Seiichi Sakamoto gave an online lecture at the Camara monthly meeting.
Professor Seiichi Sakamoto participated as lecturers in the online event organized by “Hoshi-tsumugi no mura,”a general incorporated association, for children hospitalaized for a long time or home care, their families andhealthcare professionals.
XII Important Dates

117

August 28
August 31
September 17

The third public data set of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) was released.
Undergraduate students of the SOKENDAI Summer Student program, supervised by Subaru Telescope
scientists, gave online presentations about their study results.

September 21

A press conference “Unveiling Galaxies at Cosmic Dawn That Were Hiding Behind the Dust” was held online.
The conference was jointly hosted with Waseda University, Hiroshima University, the University of Geneva, andthe Joint ALMA Observatory, attended by 11 representatives from 10 media organizations.

October 7

Nour Skaf at Subaru Telescope received the “L’Oréal-UNESCO for Women in Science - Rising Talents - France
2021” award.

October 12

An international research team consisting of Kogakuin University, Yamaguchi University, Go National College
of Technology, National Astronomical Observatory of Japan, National Astrophysical Institute of Italy, Korean
Astronomical Institute, and Harvard University has conducted detailed radio observations using the JapanKorea Joint VLBI Observation Network (KaVA: KVN and VERA Array). The team succeeded for the firsttime in capturing the dramatic phenomenon of an active galactic nuclear jet, which has just been ejected from asupermassive black hole, colliding with a high-density gas cloud and being intercepted by it.

October 23

The Mitaka Open House Day event consisted of 3 main lectures and a total of 103 contents, including 21 live
streams (including YouTube Premiere events) by NAOJ’s projects, 45 video contents, 37 other web contents. The
maximum number of simultaneous connections was 2,054. The archived video garnered 60,300 views in the firstmonth of its release.

November 1~November2“Cold outflows near and far: crossroad of our current understandings” was held online.

November 2,
November 5

ALMA Data Analysis Workshop (Intermediate Level) was held jointly with the astronomy data center online.

November 11

The National Astronomical Observatory of Japan (NAOJ) and Iwate Nippo held a signing ceremony for acomprehensive collaboration agreement at the National Astronomical Observatory of Japan's Mizusawa VLBI
Observatory. This agreement was planned as a “Next Generation Researcher Support Project” with the aim ofcreating a path to secure excellent doctoral human resources. This agreement began with a pleasant conversation
between Dr. Azumane, President of Iwate Nippo, and NAOJ Director General Tsuneta, and came to fruition after
Dr. Azumane made a proposal after attending a lecture by Homma, Director of Mizusawa VLBI Observatory.
We are looking forward to its further development as a powerful means of securing human resources for thepromotion of science.

November 11

Subaru Telescope and NAOJ TMT Project members gave an online presentation at Girl Scout STEM Fest in
Hawai`i.

November 13

The Sixth “Nagano Prefecture is Astro-Prefecture” meeting was held online at Syogaigakushu-center in Chinoby “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 60 participants in the meeting.

November 14

Subaru Telescope, Project PANOPTES, and TMT Project participated in the AstroDay West event at a shopping
center in Kailua-Kona on the Island of Hawai`i.

November 18

Subaru Telescope and Project PANOPTES participated in the online Hawai`i Island Virtual Career Expo andchatted lively with students.

November 18~November 19

Subaru Telescope and Project PANOPTES live-broadcasted the partial lunar eclipse from the Island of Hawai`i.

November 30~December 1

Linking the Science of Large Interferometers in the 2030s was held online.

December
December 4
December 6,
December 13

118Open House day of Nobeyama Radio Observatory was held online. The total number of viewers for live
streaming reached about 6700, and total number of views for all content in about the first 30 days was about
130,000.

Subaru Telescope received a letter of appreciation from the Japan Aerospace Exploration Agency (JAXA) tocommemorate the success of the asteroid explorer Hayabusa2.
Subaru Telescope scientists presented at the online live talk event hosted by Hamagin Space Science Center.
ALMA Grant Fellow Symposium 2021 was held online.

December 9

A press conference “Fiery Dragon’s Breath May Scorch Young Planets” was held online. The conference was
jointly hosted with Kyoto University and the University of Hyogo, attended by 15 representatives from 14 media
organizations.

December 14, 16
and 21

FY 2021 ALMA/45m/ASTE Users Meeting was held online.

XII Important Dates

December 20,
December 22

Millimeter/submillimeter VLBI sciences with ALMA was held online.

December 23~December 25

Subaru Telescope 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.

2022
January
January 5
January 11~January 13

Observations of the Hyper Surpime-Cam Subaru Strategic Program (HSC-SSP) since 2014 completed.
Ishigakijima Astronomical Observatory welcomed the 150,000th visitor to its public facilities.
The annual Subaru Users Meeting FY 2021 was held in a hybrid style of on-site and online.

January 17~March 21

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 18~January 21

East Asian ALMA Science Workshop 2022 was held online.

January 29~February 6

Southern Island Star Festival 2021 was held partially online. The Star Festival Live & the Ishigaki Island Starry
Sky and Star Culture Lecture on January 29 were viewed 5290 times on YouTube. The memorial lecture on
January 30 was attended by 45 people.

February~AprilFebruary 5
February 8

As a part of the NAOJ’s FY2021 Project Review, the international external evaluation of the Subaru Telescope
was conducted online.
Professor Seiichi Sakamoto participated as lecturers in the event organized by Japan Space Forum.
Ceremony for the 40th anniversary of Nobeyama Radio Observatory was held online. About 120 people
participated in it. A memorial magazine was created and distributed.

February 22

Radio observations in the 1.3 cm and 7 mm wavelength bands by the East Asian VLBI network revealed thedetailed structure of the giant black hole object Sagittarius A (ASTER), which lies at the center of the Milky Way
Galaxy. The size of the emitting region suggests that the gas flow accreting onto the giant black hole contains
non-thermal electrons accelerated to extremely high energies, and the nearly circular shape of the emitting
region suggests that the accretion disk's axis of rotation (or the direction of the weak jet) may point almost
exactly in the direction of the Earth.

February 27,
March 5

A total of seven Subaru Telescope and NAOJ TMT Project staff members contributed to the 2022 Hawai`i
VEX IQ Elementary School State Championship as judges at online interviews (February 27) and in-person
tournament (March 5).

February 28~March 4

A total of 13 Subaru Telescope and NAOJ TMT Project staff members participated in the 2022 online Journey
Through the Universe and provided presentations and participated in a career panel.

March

As a part of the NAOJ’s FY2021 Project Review, the international external evaluations of the Advanced
Technology Center, Optical and Infrared Synergetic Telescopes for Education and Research (OISTER), andJapanese VLBI Network (JVN) were each conducted online.

March 3The Subaru Telescope achieved the first launch of a new laser guide star system, upgraded and used for the
Subaru Telescope’s adaptive optics system.

March 5

Kenneth Wong, a Project Research Fellow at the Subaru Telescope, was selected to receive the 2021 ASJ Young
Astronomer Award.

March 9~March 10

East Asian ALMA Development Workshop 2022 was held online.

March 20
~March 21

Chura-boshi Research Team workshop for high school students was held at VERA Ishigaki-jima Station and
Ishigakijima Astronomical Observatory for the first time in two years. Although it was postponed from theoriginal schedule due to the decision to continue a state of emergency, it was successfully held while taking
precautions against novel coronavirus infection.

March 24
~March 25

Workshop on “Astronomy investigated with data science approaches” was held as part of the project“Understanding the 3-D structure of the Milky Way Galaxy based on a machine learning method applied onlarge-scale data of molecular clouds” which is one of the projects of the “Interdisciplinary research by young
researchers Project” by NINS. About 80 researchers in fields of astronomy and informatics including young
researchers participated in it.

March 24
March 28
March 29
~March 30

Subaru Telescope’s website for “Subaru Telescope 2.0” launched in Japanese.
There was an exhibition booth at the Reception for the Emperor's Birthday held in the Embassy of Japan in
Chile.
ALMA Cycle 9 2022 Proposal Preparation Meeting was held online.

XII Important Dates

119

XIII Publications, Presentations
1. Refereed Publications
Abbas, M., Grebel, E. K., Simunovic, M.: 2021, RR Lyrae Stars in
Stellar Streams with Gaia: The Escapers, ApJ, 915, 49.
Abbott, R., et al. including Akutsu, T., Ando, M., 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., LIGO Sci
Collaboration, Virgo Collaboration, KAGRA Collaboration: 2021,
Diving below the Spin-down Limit: Constraints on Gravitational
Waves from the Energetic Young Pulsar PSR J0537-6910, ApJL, 913,
L27.
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 Martin, E.
N., Tomaru, T., Tsuzuki, T., Uraguchi, F., Washimi, T., Zhao,
Y. H., LIGO Sci Collaboration, Virgo Collaboration, KAGRA
Collaboration: 2021, Upper limits on the isotropic gravitationalwave background from Advanced LIGO and Advanced Virgo’s thirdobserving run, Phys. Rev. D, 104, 022004.
Abbott, R., et al. including Akutsu, T., Barton, M. A., Capocasa, E.,
Flaminio, R., Guo, H.-K., Hirata, N., Leonardi, M., Marchio, M.,
Nakamura, K., Shams, B., Shoda, A., Takahashi, R., Tanioka,
S., Tapia San Martin, E. N., Tomaru, T., Washimi, T., Yang, F.
W., Zhao, Y., Fukushima, M., Ikenoue, B., Obuchi, Y., Saito,
S., Shimizu, R., Tsuzuki, T., Uraguchi, F., Aso, Y., Kozakai, C.,
Ohishi, N., LIGO Sci Collaboration, Virgo Collaboration, KAGRA
Collaboration: 2022, Search for intermediate-mass black hole binaries
in the third observing run of Advanced LIGO and Advanced Virgo,
A&A, 659, A84.
Abbott, R., et al. including Akutsu, T., Barton, M. A., Capocasa, E.,
Flaminio, R., Hirata, N., Leonardi, M., Marchesoni, F., Marchio,M., Nakamura, K., Shoda, A., Takahashi, R., Tanioka, S., Tapia
San Martin, E. N., Tomaru, T., Washimi, T., Zhao, Y., Aso, Y.,
Kozakai, C., Ohishi, N., Fukushima, M., Ikenoue, B., Obuchi, Y.,
Saito, S., Shimizu, R., Tsuzuki, T., Uraguchi, F.: 2021, Constraints
from LIGO O3 Data on Gravitational-wave Emission Due toR-modes in the Glitching Pulsar PSR J0537-6910, ApJ, 922, 71.
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., Aso, Y., Kozakai, C., Ohishi,N., Fukushima, M., Ikenoue, B., Obuchi, Y., Saito, S., Shimizu,
R., Tsuzuki, T., Uraguchi, F.: 2021, Searches for Continuous
Gravitational Waves from Young Supernova Remnants in the Early
Third Observing Run of Advanced LIGO and Virgo, ApJ, 921, 80.
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.,

120

XIII Publications, Presentations

Tomaru, T., Washimi, T., Zhao, Y., Aso, Y., Kozakai, C., Ohishi,N., Fukushima, M., Ikenoue, B., Obuchi, Y., Saito, S., Shimizu,
R., Tsuzuki, T., Uraguchi, F., LIGO Sci Collaboration, Virgo
Collaboration, KAGRA Collaboration: 2021, Search for anisotropic
gravitational-wave backgrounds using data from Advanced LIGO
and Advanced Virgo’s first three observing runs, Phys. Rev. D, 104,022005.
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., Aso, Y., Kozakai, C., Ohishi,N., Fukushima, M., Ikenoue, B., Obuchi, Y., Saito, S., Shimizu,
R., Tsuzuki, T., Uraguchi, F.: 2021, All-sky search for long-duration
gravitational-wave bursts in the third Advanced LIGO and Advanced
Virgo run, Phys. Rev. D, 104, 102001.
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., Aso, Y., Kozakai, C., Ohishi,N., Fukushima, M., Ikenoue, B., Obuchi, Y., Saito, S., Shimizu,
R., Tsuzuki, T., Uraguchi, F.: 2021, All-sky search for shortgravitational-wave bursts in the third Advanced LIGO and Advanced
Virgo run, Phys. Rev. D, 104, 122004.
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., LIGO Sci Collaboration,
Virgo Collaboration, KAGRA Collaboration: 2021, Observationof Gravitational Waves from Two Neutron Star-Black Hole
Coalescences, ApJL, 915, L5.
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.: 2021, All-sky search for continuous
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Zapart, C., Shirasaki, Y., Ohishi, M., Mizumoto, Y.: 2022, JVO
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ivoa.net/newsletter/025/index.html

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5. Publications in English
Canas, L., Agata H.: 2021, Communicating Astronomy with the Public
Journal #30, IAU/OAO, Japan.
Tinetti, G., et al. including Ikoma, M., Skaf, N.: 2021, Ariel Atmospheric Remote-sensing Infrared Exoplanet Large-survey
Enabling planetary science across light-years, European space
agency, Europe.

6. Conference Presentations
Agata, H., Canas, L., Hansen, I., González, J., Russo, P.: 2021,
Kaifu-NAOJ Telescope Kit: A Legacy of the IAU100 Celebrations,
Communicating Astronomy with the Public Conference 2021,(Online, May 24–27, 2021).
Agata, H., Fujita, T.: 2021, Scaffolding from Astronomers: Delivering
Lessons to Schools and STEAM Education, 3rd Shaw-IAU Workshop
on Astronomy for Education, (Online, Oct. 12–15, 2021).
Agata, H., Nakajima, S.: 2021, A Study on the Use of an Assembling
Astronomical Telescope for School’s Tasks at Home, Global HandsOn Universe Conference, (Online, Aug. 25–28, 2021).
Agata, H., Okamura, S., Handa, T.: 2021, Considerations for Maintaining
and Updating Academic Terminology -The Internet Encyclopediaof Astronomy as a Case Study, Communicating Astronomy with the
Public Conference 2021, (Online, May 24–27, 2021).
Agata, H.: 2021, On the Possibilities of Astrotourism Japan “SoraTourism” as an attempt to share “Under One Sky”, IAU Astrotourism
Workshop, (Online, Jun. 28, 2021).
Agata, H.: 2021, The Potential of Travel to Mongolia and Astro-tourism
in Japan, “Astronomy and Art for Environmental Protection in Gobi
desert” Workshop, (Online, Jul. 1–4, 2021).
Ahn, K., et al. including Guyon, O., Lozi, J., Vievard, S., Deo, V.,
Skaf, N., Currie, T.: 2021, SCExAO: a testbed for developing highcontrast imaging technologies for ELTs, SPIE Optics and Photonics,(San Diego, Aug. 2–5, 2021).
Ahn, K., Guyon, O., Lozi, J., Vievard, S., Deo, V., Skaf, N., Bragg, J.,
Norris, B., Tuthill, P.: 2021, Laboratory Demonstration of MachineLearning-Based Focal Plane Wavefront Sensing on Subaru/SCExAO,
Wavefront sensing in the VLT/ELT era VII, (Online + Valparaiso,
Chile, Dec. 1–3, 2021).
Ali, S. S., Propris R/D., Chung, C., Bremer, M. N., Phillipps, S.: 2021,
Evolution of early-type galaxies in the UV, NUVA e-meeting “Status
and new UV results from HST, Astrosat and LUT”, (Online, Oct.
26–27, 2021).
Ali, S. S., Propris R/D., Chung, C., Bremer, M. N., Phillipps, S.: 2021,
Unveiling Uv-bright stellar populations in red and dead galaxies with
CUBES, Science with UV-efficient ground-based spectrographs,(Online, Feb. 3–5, 2021).
Aoki, W.: 2021, Stellar elemental abundances constraining
nucleosynthesis and chemical evolution of the universe, The 16th
International Symposium on Nuclei in the Cosmos (NIC-XVI),(Online + Chengdu, China, Sept. 21–25, 2021).
Arai, T., et al. including DESTINY+ science team: 2021, Current status
and science of DESTINY+, JpGU 2021, (Online, May 30–Jun. 6,2021).
Arai, T., et al. including Ito, T.: 2021, Overview and Science of
DESTINY+, Europlanet Science Congress 2021 (EPSC2021),(Online, Sep. 13–24, 2021).
Aritomi, N.: 2021, Demonstration of length control for a filter cavity
with coherent control sidebands, GWADW 2021, (Online, May
17–21, 2021).
Aritomi, N.: 2021, Demonstration of length control for a filter cavity
with coherent control sidebands, The 28th KAGRA Face-to-Facemeeting, (Online, Dec. 20–21, 2021).
Aso, Y., Yamaoka, H.: 2021, Sponsor Session: Gravitational Wave

Telescope KAGRA in Japan, European Astronomical Society Annual
Meeting 2021, (Online, June 28–July 2, 2021).
Baba, S., Imanishi, M., Izumi, T., Kawamuro, T., Nguyen, D. D.,
Nakagawa, T., Isobe, N., Onishi, S., Matsumoto, K.: 2021, Extremely
Buried Nucleus of IRAS 17208−0014 Observed at Sub-Millimeterand Near-Infrared Wavelengths, East-Asia AGN workshop, (Online +Chongqing, China, Oct. 11–13, 2021).
Belikov, R., Sirbu, D., Jewell, J. B., Guyon, O., Stark, C. C.: 2021,
Theoretical performance limits for coronagraphs on obstructed andunobstructed apertures: how much can current designs be improved?,
SPIE Optics and Photonics, (San Diego, Aug. 2–5, 2021).
Beniyama, J., Sekiguchi, T., Kuroda, D., Arai, T., Ishibashi, K., Ishiguro,
M., Ohsawa, R., Ootsubo, T., Sako, S., Senshu, H., Takita, S.,
Yoshida, F.: 2022, Multicolor simultaneous photometry of (3200)
Phaethon with Seimei/TriCCS, PERC Int’l Symposium on Dust &Parent Bodies 2022 (IDP2022), (Online, Feb. 21–22, 2022).
Buitrago-Casas, J. C., et al. including Narukage, N.: 2021, Hard X-ray
upper limits of the quiet Sun with new FOXSI observations, AGU
Fall Meeting 2021, (New Orleans, US, Dec. 13–17, 2021).
Buitrago-Casas, J. C., the FOXSI team: 2021, Assessing quiet Sun
hard X-rays using observations from the FOXSI-2 Sounding Rocket,
RHESSI-20 Workshop: Preparing for the Next Decade in HighEnergy Solar Physics Research, (Online, Jul. 6–9, 2021).
Canas, L.: 2021, IAU Office for Astronomy Outreach: Access,Communication, and International Cooperation, Virtual Conferenceof the African Astronomical Society (AFAS2021), (Online, Mar. 9,2021).
Canas, L.: 2021, Acções em prol da equidade, diversidade e inclusão
em Astronomia: o caso da União Astronómica Internacional (UAI),
Brazilian Astronomical Association Annual Meeting, (Online, Sept.
13–17, 2021).
Canas, L.: 2021, The IAU Office for Astronomy Outreach, Forum on
Astronomy in Africa, (Online, Oct. 27–29, 2021).
Chen, D., on behalf of the KAGRA collaboration.: 2021, Status of
KAGRA Calibration System Upgrade Toward O4, The 8th KAGRAInternational Workshop, (Online, Sep. 7, 2021).
Chen, D., on behalf of the KAGRA collaboration.: 2021, Status of
KAGRA Calibration Toward O4, The 27th KAGRA face to facemeeting, (Online, Aug. 28, 2021).
Chen, D., on behalf of the KAGRA collaboration.: 2021, Report from
Calibration, The 28th KAGRA Face-to-Face meeting, (Online, Dec.
20–21, 2021).
Chen, D., Sawada, T.: 2021, Status of CAL toward O4 observing run,
The 27th KAGRA face to face meeting, (Online, Aug. 28, 2021).
Currie, T. M., Brandt, T., Kuzuhara, M., Chilcote, J., Liu, R. Y.,
Cashman, Ed., Tobin, T., Guyon, O., Lozi, J., Deo, V., Vievard, S.:
2021, A new type of exoplanet direct imaging search: a SCExAO/CHARIS survey of accelerating stars, SPIE Optics and Photonics,(San Diego, Aug. 2–5, 2021).
Dainotti, M. G., De Simone, B., Lambiase, B., Schiavone, T., Montani,G., Rinaldi, E.: 2021, Machine learning analysis for the Hubble
constant computation, Applications of Statistical Methods andMachine Learning in the Space Sciences, (Online, May 21, 2021).
Dainotti, M. G., De Simone, B., Levine, D., Lenart, A., Young, S.: 2021,
GRB observational correlations, 16th Marcel Grossmann Meeting,(Online, Jul. 5–10, 2021).

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145

Dainotti, M. G., Fraija, N., Levine, D., Warren, D.: 2022, The closure
relationships in High Energy, Fermi Collaboration Meeting, (Online,
Mar. 23, 2022).
Dainotti, M. G., Fraija, N., Levine, L., Warren, D., Lenart, A., Young,S.: 2021, The 2D and 3D Dainotti correlations in optical, 17th ItalianKorean Symposium on Relativistic Astrophysics 2021, (Online, Aug.
1, 2021).
Dainotti, M. G., the RATIR collaboration: 2021, The 3D opticalfundamental plane as a further step of the luminosity-time correlationand future perspective with the KISO observatory, AAS 238 Meetingin-a-Meeting “An Exploration of Thorne-Zytkow Objects”, (Online,
Jun. 7–9, 2021).
D’Amore, M., et al. including Matsumoto, K.: 2021, Unsupervised
Learning of NIRS3 Data: Ryugu Spectral Surface Regions
Classification, JpGU 2021, (Online, May 30–Jun. 6, 2021).
De Simone, B., Dainotti, M. G., Lambiase, B., Schiavone, T., Montani,G., Rinaldi, E.: 2021, On the Hubble constant tension in the SNe Ia
Pantheon Sample, 16th Marcel Grossmann Meeting, (Online, Jul.
5–10, 2021).
De Simone, B., Dainotti, M. G., Lambiase, B., Schiavone, T., Montani,G., Rinaldi, E.: 2021, A new perspective on cosmology throughSupernovae Ia and Gamma Ray Bursts, SeMPowisko 2021, (Online,
May 14, 2021).
Deo, V., Vievard, S., Cvetojevic, N., Ahn, K., Barjot, K., Guyon, O.,
Huby, E., Kotani, T., Lacour, S., Lallement, M., Lapereyre, V., Lozi,J., Marchis, F., Martin, G., Martinache, F., Norris, B., Perrin, G.,
Rouan, D., Skaf, N., Tuthill, P.: 2021, Interferometric wavefront
sensing at Subaru/SCExAO: fibered pupil-remapping spectroscopy
and non-redundant masking, Wavefront sensing in the VLT/ELT era
VII, (Online + Valparaiso, Chile, Dec. 1–3, 2021).
Deo, V., Vievard, S., Cvetojevic, N., Norris, B., Guyon, O., Lozi, J.,
Ahn, K., Huby, E., Lacour, S., Martinache, F., Skaf, N., Tuthill,P.: 2021, Wavefront sensing using non-redundant aperture masking
interferometry: tests and validation on subaru/scexao, SPIE Optics
and Photonics, (San Diego, Aug. 2–5, 2021).
Eie, S.: 2021, Multi-frequency observations of a radio magnetar withJapanese radio telescopes, East Asia SKA Workshop 2021, (Online,
May 26–28, 2021).
Eie, S.: 2022, Multifrequency view of energetic pulsar emissions:prospects of multi-telescope observations for magnetars/fast radio
bursts, Black Hole Astrophysics with VLBI 2022, (Online, Feb, 7–9,2022).
Ezaki. S., Nagai M., Sakai R., Kaneko K., Imada H., Kojima T., Shan
W., Uzawa Y., Asayama S.: 2021, Development of silicon vacuum
windows, ALMA Front End Development (Virtual) Conference 2021,(Online, Sept. 27–30, 2021).
Ezawa, H., Matsuo, H., Ukibe, M., Fujii, G., Shiki, S., Niwa, A.: 2021,
Properties of SIS Devices for Terahertz Photon Detection, 19thInternational Workshop on Low Temperature Detectors, (Online, Jul.
19–29, 2021).
Fraser, W. C., et al. including Ito, T.: 2021, A machine learning approachto detecting Kuiper Belt Objects for NASA’s New Horizons Extended
Mission, CASCA 2021 AGM, (Online, May 10–14, 2021).
Fraser, W. C., et al. including Ito, T.: 2022, A successful machinelearning approach to detecting Kuiper Belt Objects for NASA’s
New Horizons Extended Mission, 53rd Lunar and Planetary Science

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Conference (LPSC), (Online + The Woodlands, Texas, USA, Mar.
7–11, 2022).
Fraser, W. C., et al. including Ito, T.: 2022, A machine learning approachto detecting Kuiper Belt Objects for NASA’s New Horizons Extended
Mission, Subaru Users Meeting FY 2021, (Online + Mitaka, Jan.
11–13, 2022).
Fujita,T., Agata, H.: 2021, Delivering lessons to schools from NAOJ
-Scaffolding from Astronomers to STEAM education- Fureai
Astronomy, Global Hands-On Universe Conference, (Online, Aug.
25–28, 2021).
Furusawa, H.: 2022, Report from Data Center, Subaru Users Meeting
FY 2021, (Online + Mitaka, Jan. 11–13, 2022).
Furuya, K., Oba, Y., Shimonishi, T.: 2022, Quantifying the chemicaldesorption of H2S and PH3 from water ice surface, Workshop on ISM
2021, (Hokkaido, Japan, Nov. 17–19, 2021).
Furuya, K., Tsukagoshi, T., Qi, C., Nomura, H., Cleeves, I., Lee, S.,
Yoshida, C. T.: 2022, Detection of HC18O+ in a Protoplanetary Disk:
Exploring Oxygen Isotope Fractionation of CO, East Asian ALMA
Science Workshop 2022, (Online, Jan. 18–21, 2022).
Gibson, S., Dainotti, M. G.: 2021, AGN as classifier with ML regression
methods using SLOPE, NAOJ mini-workshop, (Mitaka, Jul. 30,2021).
Glesener, L., et al. including Narukage, N., The FOXSI Collaboration:
2021, The FOXSI-4 Sounding Rocket: High Resolution Focused
X-ray Observations of the Sun, AGU Fall Meeting 2021, (New
Orleans, US, Dec. 13–17, 2021).
Guyon, O., et al. including Ahn, K., Skaf, N., Currie, T., Lozi, J., Deo,
V., Vievard, S.: 2021, High contrast imaging at the photon noise limit
with self-calibrating WFS/C systems, SPIE Optics and Photonics, (San
Diego, Aug. 2–5, 2021).
Guyon, O., Martinod, M.-A., Ahn, K., Norris, B., Deo, V., Lozi, J.,
Vievard, S., Skaf, N., Tuthill, P., Males, J., Haffert, S.: 2021, HighContrast Imaging at the Photon Noise Limit with WFS-based PSF
calibration, Wavefront sensing in the VLT/ELT era VII, (Online +Valparaiso, Chile, Dec. 1–3, 2021).
Hada, K., Haggard, D., Markoff, S.: 2021, Plans for next MWL papers
and 2022 campaign, EHT Collaboration Meeting 2021 winter,(Online, Dec, 6–10, 2021).
Hada, K.: 2021, High-resolution view of collimaiton and acceleration
regions of nearby AGN jets, Extragalactic jets on all scales - launching,propagation, terminanion (Jets2021), (Onlune, Jun. 14–18, 2021).
Hada, K.: 2022, Event Horizon Telescope Observations of Supermassive
Black Holes, East Asian ALMA Science Workshop 2022, (Online,
Jan. 18–21, 2022).
Haffert, S. Y., Males, J. R., Close, L., Long, J., Schatz, L., van Gorkom, K.,
Hedglen, A., Lumbres, J., Rodack, A., Guyon, O., Knight, J., Kautz,
M., Pearce, L.: 2021, Data-driven subspace predictive control: lab
demonstration and future outlook, SPIE Optics and Photonics, (San
Diego, Aug. 2–5, 2021).
Hamano, S., PFS team: 2022, Persistence characterization of the PFS
H4RG detector (2), PFS 13th collaboration meeting, (Online, Mar.
22–24, 2022).
Handa,T., Okamura, S., Agata, H.: 2021, An online dictionary on
astronomy by ASJ; status report in 2021, Global Hands-On Universe
Conference, (Online, Aug. 25–28, 2021).
Hansen, I., Agata, H., Canas, L., Lindberg, C. L.: 2021, What PeopleWant to Know about Astronomy — Letters to the International
Astronomical Union, Communicating Astronomy with the Public
Conference 2021, (Online, May 24–27, 2021).
Hart, J. G. J. 't., Van Holstein, R. G., Bos, S. P., Ruigrok, J., Snik, F.,
Lozi, J., Guyon, O., Kudo, T., Zhang, J., Jovanovic, N., Norris, B.,
Martinod, M.-A., Groff, T. D., Chilcote, J., Currie, T., Tamura, M.,
Vievard, S., Sahoo, A., Deo, V., Ahn, K., Martinache, F., Kasdin, J.:
2021, Full characterization of the instrumental polarization effects ofthe spectropolarimetric mode of SCExAO/CHARIS, SPIE Optics andPhotonics, (San Diego, Aug. 2–5, 2021).
Hatta, Y.: 2021, Asteroseismology of a possible blue straggler star, KIC
11145123, The Good Vibrations Seminars Series, (Online, Apr. 7,2021).
Hatta, Y.: 2021, Error Propagations in inverse problems, PLATO
Working Package 124 Hands-On Workshop #2 (HOW#2 Meeting),(Online, Apr. 14, 2021).
He, W., Ichikawa, K., Yamashita , T.: 2022, WERGs: Spectroscopic
observations of optically-faint radio galaxies at z~3 in the SubaruHSC Wide field, Quasars and Galaxies through Cosmic Time, (Online,
Jan. 24–27, 2022).
He, W., Ichikawa, K., Yamashita , T.: 2021, WERGs: Spectroscopic
observations of optically-faint powerful radio galaxies at z~3 inthe Subaru-HSC Wide field, East-Asia AGN workshop, (Online +Chongqing, China, Oct. 11–13, 2021).
He, W., Tanaka, M., Ishigaki, M. N., Onodera, M.: 2022, Optimalalgorithm to determine pointing centers for PFS open-use programs,
Subaru Users Meeting FY 2021, (Online + Mitaka, Jan. 11–13, 2022).
He, W., Tanaka, M., Ishigaki, M. N., Onodera, M.: 2022, PFS Pointing
Planner: optimal algorithm to determine pointing centers for PFS
open-use programs, PFS 13th collaboration meeting, (Online, Mar.
22–24, 2022).
Hirabayashi, M., et al. including Noda, H., Matsumoto, K.: 2021,
Hayabusa2 Extended Mission to rendezvous with Asteroid 1998
KY26: Investigations of an extremely small fast rotator for planetary
defense, JpGU 2021, (Online, May 30–June 6, 2021).
Hiramatsu, M., Takanashi, N., Asagiri, S., Kawagoe, S. K., Amano, S.
G., Kamegai, K.: 2021, Virtual ALMA Tour in VRChat – Immersive
Experience in a User-Generated World, Communicating Astronomy
with the Public Conference 2021, (Online, May 24–27, 2021).
Huang, H., on behalf of the KAGRA collaboration: 2021, Improvementof error estimation method for calibration uncertainty with gravity
field calibrator, The 27th KAGRA face to face meeting, (Online, Aug.
28, 2021).
Ikoma, M., Kikuchi, K., Kimura, T., Nakayama, A., Shibata, S.: 2021,
On the Origin of Metal-rich Close-in Gas Giants, Japan Geoscience
Union Meeting 2021, (Online, May 31–Jun. 6, 2021).
Ikoma, M.: 2021, Planetary Population Synthesis Models for Earths
and Super-Earths, Ariel Planetary Interior Meeting, (Online, Nov. 16,2021).
Ikoma, M.: 2022, Formation, Evolution and Detectability of Diverse
Aqua Planets, 10th ELSI Symposium: ELSI Past & Future, (Online,
Jan. 13, 2022).
Imanishi, M.: 2022, ALMA 183 GHz H2O and dense molecular line
observations of nearby (ultra)luminous infrared galaxies, CONquest
workshop 2022, (Online, Jan. 17–20, 2022).
Imanishi, M.: 2022, ALMA high-spatial-resolution dense molecularline observations of the nearby well-studied AGN NGC 1068:
Implications for mass-accreting mechanism onto supermassive black
holes in AGNs, Black Hole Astrophysics with VLBI 2022, (Online,
Feb, 7–9, 2022).
Inoue, S., Chin, K., Uno, S., Kohno, K., Oshima, T., Niwa, Y.,
Takekoshi, T., Naganuma, T.: 2021, Development of planar Magic-T
for wideband millimeter/submillimeter wave detectors, ALMA/45m/
ASTE Users Meeting 2021, (Online, Dec. 14, 16, and 21, 2021).
Ishigaki, M. N., Tanaka, M., Onodera, M., He, W., Moritani, Y.,
Yabe, K., Tamura, N., PFS obsproc working group, PFS-GA Science
working group: 2022, Selection of spectrophotometric and chemical
abundance calibration stars for the PFS observations, PFS 13th
collaboration meeting, (Online, Mar. 22–24, 2022).
Ishikawa, H. T.: 2022, Abundance analysis of individual elements fornearby M dwarfs based on high-resolution near-infrared spectra ofSubaru/IRD, Subaru Users Meeting FY 2021, (Online + Mitaka, Jan.
11–13, 2022).
Ishikawa, H., Takada, S., Matsumoto, Y.: 2021, Rheology of twodimensional crushable granular materials, Powders & Grains 2021,(Online, July 5, 13, 21, 29 and Aug 6,. 2021).
Ishikawa, R. T., Katsukawa, Y., Oba, T., Orozco Suarez, D., Kubo,
M., Suematsu, Y.: 2021, Contribution of microturbulence to spectralline broadening in granular convection studied with Hinode SP, Asia
Oceania Geosciences Society (AOGS) 2021 18th Annual Meeting,(Online, Aug. 1–6, 2021).
Ishikawa, R., Masada, Y., Katsukawa, Y., Nakata, M., Riethmüller, T.:
2021, Multi-Scale Deep Learning for Estimating Horizontal Velocity
Fields on the Solar Surface, Hinode 14/IRIS 11 Joint Science
Meeting, (Online, Oct. 25–28, 2021).
Ishikawa, R., Trujillo Bueno, J., del Pino Aleman, T., Okamoto, T. J.,
McKenzie, D. E., Auchère, F., Kano, R., Song, D., Rachmeler, L.
A., Kobayashi, K., Bethge, C., De Pontieu, B., CLASP2 team: 2021,
Mapping solar magnetic fields from the photosphere to the top of thechromosphere by the CLASP2 sounding rocket experiment, 5th AsiaPacific Conference on Plasma Physics, Division of Plasma Physics,
Association of Asia-Pacific Physical Societies, (Online, Sep. 26–Oct.
1, 2021).
Ito, T.: 2021, Comparison of original orbits of Oort Cloud new comets
given in various catalogues II. Different solutions from different
observations, JpGU 2021, (Online, May 30–June 6, 2021).
Izumi, T.: 2021, Star formation, feedback, and co-evolution in distantquasar host galaxies at z > 6, East-Asia AGN workshop, (Online +Chongqing, China, Oct. 11–13, 2021).
Izumi, T.: 2021, Less-biased view of the early co-evolution ofsupermassive black holes and galaxies, ALMA/45m/ASTE Users
Meeting 2021, (Online, Dec. 14, 16, and 21, 2021).
Izumi, T.: 2021, Parsec-scale view on the multiphase dynamical natureof AGN torus, CONquest workshop 2022, (Online, Jan. 17–20, 2022).
Izumi, T.: 2021, ALMA observations of z > 6 low-luminosity quasars:
unbiased view on the early co-evolution and feedback, SWIFAR
colloquium, (Online, May 13, 2021).
Izumi, T.: 2021, Challenge of Subaru and ALMA: early co-evolutionof supermassive black holes and host galaxies, Osaka University
Theoretical Astrophysics Colloquium, (Online, Oct. 20, 2021).
Izumi, T.: 2021, Challenge of Subaru and ALMA: early co-evolution ofsupermassive black holes and host galaxies, ISAS/JAXA Astrophysics

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Colloquium, (Online, Oct. 28, 2021).
Izumi, T.: 2022, Challenge of Subaru and ALMA: early co-evolution ofsupermassive black holes and host galaxies, Quasars and Galaxies
through Cosmic Time, (Online, Jan. 24–27, 2022).
Jensen-Clem, R., Hinz, P., von Kooten, M., Fitzgerald, M. P., Sallum,S., Mazin, B., Chun, M., Max, C., Millar-Blanchaer, M., Guyon,O., Skemer, A., Stelter, R. D., Wang, J.: 2021, The Planetary
Systems Imager adaptive optics system: an initial optical design andperformance analysis tool for the PSI-Red AO system, SPIE Optics
and Photonics, (San Diego, Aug. 2–5, 2021).
Kaneko, K., Sakai, R., Kanzawa, T., Mitsui, K., Fukushima, M.,
Kojima, T., Uzawa, Y., Gonzalez, A.: 2021, Development ofreceiver optics components using AM technology, ALMA Front End
Development (Virtual) Conference 2021, (Online, Sept. 27–30, 2021).
Kang, H.: 2021, Preliminary Optics Investigation for ALMA Multibeam
Receiver, ALMA Front End Development (Virtual) Conference 2021,(Online, Sept. 27–30, 2021).
Katsukawa, Y., HINODE SOT team: 2021, Coordination with
HINODE with emphasis on the Spectro-Polarimeter, SO/PHI science
preparation meeting, (Oneline, Sep. 28–30, 2021).
Katsukawa, Y., Oba, T., Tsuzuki, T., Fumihiro, U., Tomonori, T.,
Andreas, L., Sami, S., Quintero Noda, C., Matsumoto, T., Hara, H.,
Shimizu, T., Kubo, M., Orozco Suarez, D., del Toro Iniesta, J. C.,
Piqueras Carreno, J., Nodomi, Y., Shinoda, K.: 2021, Near-Infrared
Spectro-Polarimeter SCIP for the SUNRISE-III Balloon-Borne Solar
Observatory, Hinode 14/IRIS 11 Joint Science Meeting, (Online, Oct.
25–28, 2021).
Kavelaars, J. J., et al. including Ito, T.: 2022, The New Horizons searchfor distant KBOs, Subaru Users Meeting FY 2021, (Online + Mitaka,Jan. 11–13, 2022).
Kawamuro, T.: 2021, Circumnuclear Scale Gas around Nearby AGN
Studied with Chandra and ALMA CO(J=2–1), European Astronomical
Society Annual Meeting 2021, (Online, June 28–July 2, 2021).
Kobayashi, H.: 2021, SKA Japan, East Asia SKA Workshop 2021,(Online, May 26–28, 2021).
Kobayashi, H.: 2021, Low frequency VLBI toward SKA1 LOW, East
Asia SKA Workshop 2021, (Online, May 26–28, 2021).
Koike, M., Yabe, K., Loomis, C., Lupton, R., Moritani, Y., Le Fur,A., Yoshida, H., Tanaka, M., Tamura, N.: 2022, OBSLOG (WebApplication for monitoring PFS observation), PFS 13th collaboration
meeting, (Online, Mar. 22–24, 2022).
Kojima, T., Uemizu, K., Kiuchi, H., Tamura, T., Sakai, R., Kaneko,
K., Imada, H., Miyachi, A., Shan, W., Makise, K., Ezaki, S.,
Uzawa, Y., Gonzalez, A., Kroug, M., Sakai, T., Ono, S., Onishi, T.,
Ogawa, H., Masui, S.: 2021, Wideband Technology development for
ALMA receiver upgrades at NAOJ, ALMA Front End Development(Virtual) Conference 2021, (Online, Sept. 27–30, 2021).
Kokubo, E.: 2021, Orbital Architecture of Self-Organized Planetary
Systems, IAU Symposia 364 Multi-scale (time and mass) Dynamics
of Space Objects, (Oneline, Oct. 18–22, 2021).
Koseki, T., Matsuo, H., Terui, A., Noji, R.: 2021, Development ofcryogenic readout circuit for Photon Counting THz Interferometry,
22nd East Asia Submillimeter-wave Receiver Technology Workshop,(Online, Nov. 25–26, 2021).
Lallement, M., Huby, E., Lacour, S., Barjot, K., Vievard, S., Cvetojevic,N., Deo, V., Guyon, O., Kotani, T., Marchis, F., Martin, G., Perrin, G.:

148

XIII Publications, Presentations

2021, H\alpha imaging of protoplanets with the spectro-interferometer
FIRST at the Subaru Telescope, SPIE Optics and Photonics, (San
Diego, Aug. 2–5, 2021).
Lawson, K., Currie, T., Wisniewski, J. P., Hashimoto, J., Guyon, O.,
Groff, T. D., Lozi, J., Brandt, T. D., Chilcote, J., Deo, V., Uyama, T.,
Vievard, S.: 2021, High-contrast integral field spectropolarimetryof planet-forming disks with SCExAO/CHARIS, SPIE Optics andPhotonics, (San Diego, Aug. 2–5, 2021).
Lee, J. W., Kojima, T., Gonzalez, A., Lee, B. W., Kaneko, K., Je, D. H.,
Kim, S.: 2021, Development of Band 7+8 Cartridge Receiver, ALMA
Front End Development (Virtual) Conference 2021, (Online, Sep.
27–30, 2021).
Lenart, A., Dainotti, M. G.: 2021, GRB cosmology, SeMPowisko 2021,(Online, May 14, 2021).
Levine, D., Dainotti, M. G., Zvonarek, K. J.: 2021, Examining the 2D
luminosity-time correlation for gamma-ray burst radio afterglows,
16th Marcel Grossmann Meeting, (Online, Jul. 5–10, 2021).
Longobardo, A., et al. including Matsumoto, K.: 2021, Spectrophotometricbehavior of Ryugu’s surface as inferred from the Hayabusa2/NIRS3
data, JpGU 2021, (Online, May 30–Jun. 6, 2021).
Lozi, J., Ahn, K., Deo, K., Guyon, O., Jovanovic, N., Minowa, Y.,
Nishiyama, S., Ono, Y., Skaf, N., Vievard, S.: 2021, Design andintegration of a new NIR wavefront sensor for the Nasmyth IR
instruments of Subaru, Wavefront sensing in the VLT/ELT era VII,
(Online + Valparaiso, Chile, Dec. 1–3, 2021).
Maeda, N., Terai, T., Ohtsuki, K., Yoshida, F., Ishihara, K., Deyama, T.:
2021, Color and size distributions of main belt asteroids obtained by
the Subaru/Hyper Suprime-Cam, Japan Geoscience Union Meeting
2021, (Online, May 31–Jun. 6, 2021).
Maehara, H., et al. including Namekata, K.: 2021, Time-resolved
spectroscopy and photometry of an M dwarf flare star YZ Canis
Minoris with OISTER and TESS: Blue asymmetry in H-alpha line
during the non-white light flare, TESS Science Conference II, (Online,
Aug. 2–6, 2021).
Maehara, H., et al. including Namekata, K.: 2021, Time-resolved
spectroscopy and photometry of an M dwarf flare star YZ Canis
Minoris with OISTER and TESS: Blue asymmetry in H-alpha line
during the non-white light flare, Asia Oceania Geosciences Society(AOGS) 2021 18th Annual Meeting, (Online, Aug. 1–6, 2021).
Masui, S., Kojima, T., Uzawa, Y., Ogawa, H., Onishi, T.: 2021, Proofof-concept experiment on a novel microwave circulator, 22nd East
Asia Submillimeter-wave Receiver Technology Workshop, (Online,
Nov. 25–26, 2021).
Masui, S., Yamasaki, Y., Hasegawa, Y., Ogawa, H., Onishi, T.,
Kojima, T., Gonzalez, A.: 2021, Development of 230 and 345
GHz simultaneous observation receiver with dual-polarization,
From Vision to Instrument: Designing the Next-Generation EHT toTransform Black Hole Science, (Online, Nov. 1–5, 2021).
Matsumoto, K.: 2021, MMX geodesy investigations: science
requirements and observation strateg, Symposium on Asteroids andComets Gravity and Interiors, (Online, Dec. 8–10, 2021).
Matsuo, H., Ezawa, H., Noji, R., Koseki, T., Niwa, A.: 2021, Cryogenic
Readout Electronics for SIS Photon Detectors, 19th International
Workshop on Low Temperature Detectors, (Online, Jul. 19–29, 2021).
Matsuo, H.: 2021, Prospects of Space Terahertz Intensity Interferometry,
Summit on Astrophysics and Space Research, (Online, Apr. 15, 2021).

Matsuo, H.: 2021, Space Terahertz Intensity Interferometry, URSIGASS 2021, (Online, Aug. 28–Sep. 4, 2021).
Matsuo, H.: 2021, Developments toward Photon Counting Terahertz
Interferometry, Tsukuba Global Science Week 2021, (Online, Sep. 11,2021).
McKenzie, D., et al. including Kano, R., Ishikawa, R.: 2021,
Demonstration of Chromospheric Magnetic Mapping with
CLASP2.1, Hinode 14/IRIS 11 Joint Science Meeting, (Online, Oct.
25–28, 2021).
Miyazaki, S.: 2021, Japanese (Subaru) Perspectives of Ground-Space
Cooperation, ISSI FORUM on “Ground and Space Astronomy:
Challenges and Synergies”, (ISSI, Bern, Switzerland, Nov. 18–19,
2021).
Moritani, Y.: 2022, Commissioning updates, PFS 13th collaboration
meeting, (Online, Mar. 22–24, 2022).
Moritsuka, A., Katsukawa, Y., Ishikawa, R. T., Oba, T.: 2021, Doppler
velocities of the solar photosphere very close to the limb observedwith Hinode SOT, The 16 th European Solar Physics Meeting,(Online, Sep. 6–10, 2021).
Moritsuka, A., Katsukawa, Y., Ishikawa, R. T., Oba, T.: 2021,
Variation of the Doppler velocities in the solar photosphere toward
the limb observed with Hinode SOT, Hinode 14/IRIS 11 Joint Science
Meeting, (Online, Oct. 25–28, 2021).
Moriya, T.: 2021, Possible explosions of Thorne-Zytkow objects andtheir observational properties, AAS 238 Meeting-in-a-Meeting “AnExploration of Thorne-Zytkow Objects”, (Online, Jun. 7–9, 2021).
Moriya, T.: 2021, Diversity in supernovae associated with gamma-ray
bursts, 16th Marcel Grossmann Meeting, (Online, Jul. 5–10, 2021).
Moriya, T.: 2021, Discovering Supernovae at Epoch of Reionization
with Roman, Roman Science Team Community Briefing, (Online,
Nov. 15–19, 2021).
Moriya, T.: 2022, Discovering Supernovae at Epoch of Reionization
with Nancy Grace Roman Space Telescope, Exploring the Transient
Universe with the Nancy Grace Roman Space Telescope, (Online,
Feb. 8–10, 2022).
Murata, K., Ogawa, K.: 2021, Spectral distortion correction of photoncounting CT with machine learning, 2021 IEEE Nuclear Science
Symposium and Medical Imaging Conference (NSS/MIC), (Online,
Oct. 16–23, 2021).
Murata, K.: 2022, Sky-fibre selection, PFS 13th collaboration meeting,(Online, Mar. 22–24, 2022).
Nagai, H., Kawakatu, N.: 2021, Imaging Diffuse Synchrotron Emission
Associated with Supernova Explosions in the Circumnuclear Disk of
NGC 1275, East-Asia AGN workshop, (Online + Chongqing, China,
Oct. 11–13, 2021).
Nagai, M., Murayama, Y., Nitta, T., Suzuki, R., Hikawa, R., Miyazawa,
H., Noji, R., Kiuchi, H., Sekimoto, Y., Matsuo, H., Shan, W., Naruse,
M., Noguchi, T., Kuno, N., Monfardini, A., Macias-Perez, J., Goupy,J., Calvo, M., Catalano, A.: 2021, Configuration of Probe Tones for
MKID Readout with Frequency Sweeping Scheme, 19th International
Workshop on Low Temperature Detectors, (Online, Jul. 19–29, 2021).
Nagai, M.: 2021, MKID Camera for Nobeyama 45-m Radio Telescope,
Tsukuba Global Science Week 2021, (Online, Sep. 11, 2021).
Nagasawa, S., Kawate, T., Narukage, N., Takahashi, T., Caspi, A.,
Woods, T.: 2021, Time Evolution of Thermal and Non-thermal
Emission from M7.6 Class Flare Observed with MinXSS andRHESSI, RHESSI-20 Workshop: Preparing for the Next Decade inHigh-Energy Solar Physics Research, (Online, Jul. 6–9, 2021).
Nagasawa, S., Kawate, T., Narukage, N., Takahashi, T., Caspi, A.,
Woods, T.: 2021, Study of Time Evolution of Thermal and NonThermal Emission from the M-Class Solar Flare, SolFER Spring
2021 Meeting, (Online, May 24–26, 2021).
Nakajima, K.: 2022, Extremely metal-poor galaxies as local probesof Early galaxy evolution: Preparing for JWST spectroscopy, Sesto
workshop 2022: I2I: Linking galaxy physics from ISM to IGM scales,(Sexten, Italy, Mar 21–25, 2022).
Nakamura, K.: 2021, Proposal of a gauge-invariant treatment of thel=0,1-mode perturbations on Schwarzschild Background Spacetime,
The 30th workshop on General Relativity and Gravitation in Japan,(Online, Dec. 6–10, 2021).
Nakamura, K.: 2021, Proposal of a gauge-invariant treatment of thel=0,1-mode perturbations on Schwarzschild Background Spacetime,
Nagoya Univ. QG-lab. Invited Seminar, (Online, Jun. 28, 2021).
Namiki, N., et al. including Noda, H., Matsumoto, K., Araki, H.,
Yamamoto, K.: 2022, Slope Stability Analysis of Top-Shaped
RYUGU, 53rd Lunar and Planetary Science Conference (LPSC),(Online + The Woodlands, Texas, USA, Mar. 7–11, 2022).
Namiki, N.: 2021, Shallow and superficial consideration on top-shape of
Ryugu, Symposium on Asteroids and Comets Gravity and Interiors,(Online, Dec. 8–10, 2021).
Narendra, A., Gibson, S., Dainotti, M. G., Bogdan, M., Pollo, A.,
Liodakis, Y., Poliszczuk, A., Rinaldi, E.: 2021, Predicting the redshiftof gamma-ray loud AGNs using machine learning, The Polish
Astronomical Society Meeting, (Online, Sep. 13–17, 2021).
Narendra, A., Gibson, S., Dainotti, M. G., Bogdan, M., Pollo, A.,
Liodakis, Y., Poliszczuk, A., Rinaldi, E.: 2021, Predicting the redshiftof gamma-ray loud AGNs using machine learning, Applications of
Statistical Methods and Machine Learning in the Space Sciences,(Online, May 21, 2021).
Narendra, A., Gibson, S., Dainotti, M. G., Bogdan, M., Pollo, A.,
Liodakis, Y., Poliszczuk, A., Rinaldi, E.: 2021, AGN as ML regression
to predict redshifts, NAOJ mini-workshop, (Mitaka, Jul. 29, 2021).
Narukage, N., et al. including Shimojo, M.: 2021, Satellite mission:
PhoENiX (Physics of Energetic and Non-thermal plasmas in the X (=magnetic reconnection) region), Particle Acceleration in Solar Flares
and the Plasma Universe - Deciphering its features under magnetic
reconnection, (Online, Nov. 15–19, 2021).
Narukage, N., et al. including Shimojo, M.: 2021, Satellite mission:
PhoENiX (Physics of Energetic and Non-thermal plasmas in the X (=magnetic reconnection) region), JpGU 2021, (Online, May 30–June 6,2021).
Narukage, N., et al. including Shimojo, M.: 2021, Satellite mission:
PhoENiX (Physics of Energetic and Non-thermal plasmas in the X(= magnetic reconnection) region), SolFER Spring 2021 Meeting,(Online, May 24–26, 2021).
Nashimoto, M., Tanaka, M., Chiba, M., Hayashi, K., Komiyama,
Y.: 2022, Statistical Verification of the Missing Satellites Problem
Outside of the Local Group with Subaru/HSC, Subaru Users Meeting
FY2021, (Online + Mitaka, Jan. 11–13, 2022).
Nashimoto, M., Tanaka, M., Chiba, M., Hayashi, K., Komiyama, Y.:
2022, Statistical Verification of the Missing Satellites Problem outside
the Local Group, Galaxy Evolution Workshop 2021, (Online, Feb.

XIII Publications, Presentations149

7–10, 2022).
Nearhood, L., Dainotti, M. G.: 2021, Reconstructing GRB lightcurves
for cosmology, NAOJ mini-workshop, (Mitaka, Jul. 30, 2021).
Nielson, V., Dainotti, M. G.: 2021, GRBs as cosmological tools, NAOJ
mini-workshop, (Mitaka, Jul. 30, 2021).
Nishiyama, G., Namiki, N., Sugita, S.: 2021, Structures and formation
age of lunar linear gravity anomalies estimated from impact
simulations: Implication to the lunar ancient expansion, AGU Fall
Meeting 2021, (New Orleans, US, Dec. 13–17, 2021).
Niwa, A., Matsuo, H., Ezawa, H., Tamura, T.: 2021, SIS photon
detector for THz observation beyond gap energy, 22nd East Asia
Submillimeter-wave Receiver Technology Workshop, (Online, Nov.
25–26, 2021).
Niwa, A., Matsuo, H., Ezawa, H., Tamura, T.: 2022, 1.5 THz photon
counting detectors for Antarctic THz Intensity Interferometry,
TCHoU Workshop, Photon & Particle Detectors Division, (Online,
Mar. 22, 2022).
Nomura, H.: 2021, Isotopic Ratios as Indicators of Physical andChemical Properties of Protoplanetary Disks, Core 2 Disk 2, (Online,
May 17–28, 2021).
Nugroho, S. K., Kawahara, H., Gibson, N. P., de Mooij, E. J. W.,
Hirano, T., Kotani, T., Kawashima, Y., Masuda, K., Brogi, M.,
Birkby, J. L., Watson, C. A., Tamura, M., Zwintz, K., Harakawa,
H., Kudo, T., Kuzuhara, M., Hodapp, K., Ishizuka, M., Jacobson, S.,
Konishi, M., Kurokawa, T., Nishikawa, J., Omiya, M., Serizawa,T., Ueda, A., Vievard, S.: 2021, Detection of Hydroxyl Radical in
the Day-side of an Exoplanet Atmosphere, European Astronomical
Society Annual Meeting 2021, (Online, June 28–July 2, 2021).
Nugroho, S. K., Kawahara, H., Gibson, N. P., de Mooij, E. J. W.,
Hirano, T., Kotani, T., Kawashima, Y., Masuda, K., Brogi, M.,
Birkby, J. L., Watson, C. A., Tamura, M., Zwintz, K., Harakawa,
H., Kudo, T., Kuzuhara, M., Hodapp, K., Ishizuka, M., Jacobson, S.,
Konishi, M., Kurokawa, T., Nishikawa, J., Omiya, M., Serizawa,T., Ueda, A., Vievard, S.: 2021, OH on the day-side of an ultra hot
Jupiter, WASP-33b, Atmospheres, Atmospheres! Do I look like I careabout atmospheres?, (Online, Aug. 23–27, 2021).
Nugroho, S. K., Kawahara, H., Gibson, N. P., de Mooij, E. J. W.,
Hirano, T., Kotani, T., Kawashima, Y., Masuda, K., Brogi, M.,
Birkby, J. L., Watson, C. A., Tamura, M., Zwintz, K., Harakawa,
H., Kudo, T., Kuzuhara, M., Hodapp, K., Ishizuka, M., Jacobson, S.,
Konishi, M., Kurokawa, T., Nishikawa, J., Omiya, M., Serizawa,T., Ueda, A., Vievard, S.: 2021, Detection of Hydroxyl Radical on
the Day-side Atmosphere of an Exoplanet, STScI Symposium 2021,(Online, Apr. 19–23, 2021).
Oba, T., Iida, Y., Shimizu, T.: 2021, Horizontal flow structure and its
dynamics in the photosphere, Hinode 14/IRIS 11 Joint Science
Meeting, (Online, Oct. 25–28, 2021).
Oba, T., Shimizu, T., Iida, Y.: 2021, Horizontal flow structure andits dynamics in the granulation, Hinode 14/IRIS 11 Joint Science
Meeting, (Online, Oct. 25–28, 2021).
Oba, T.: 2021, SO/PHI and Hinode/SP: Multiple line-of-sight Doppler
velocity, SO/PHI Science Meeting, (Göttingen, Germany, Sep. 28–30,
2021).
Ogihara, M., Hori, Y., Kunitomo, M., Kunimoto, M., Kurosaki, K.:
2021, Giant planets with large metal masses and metal fractions suchas HD 149026b and TOI-849b form via giant impacts in a rapidly

150

XIII Publications, Presentations

dissipating disk by photoevaporation, DPS/AAS (AAS Division forPlanetary Sciences) 53rd Annual Meeting, (Online, Oct. 3–8, 2021).
Ohishi, M.: 2021, The Beautful Skies for All, 14th UNISEC-Global
Meeting, (Online, Oct. 16, 2021).
Ohishi, M.: 2021, Protection of Radio Astronomy Observations in the
Era of ngVLA, ngVLA Workshop 2021, (Online, Jul. 15, 2021).
Ohmura, T., Akamatsu, H., Machida, M.: 2022, Simulations of twotemperature jets in galaxy clusters: The X-ray property of the cocoon
shock, Black Hole Astrophysics with VLBI 2022, (Online, Feb, 7–9,2022).
Ohmura, T., Chibueze, J. O., Sakemi, H., Machida, M., Akamatsu, H.,
Akahori, T., Nakanishi, H., Parekh, V., van Rooyen, R., Takeuchi,
T. T.: 2021, Magnetohydrodynamic simulations of the interaction
between the jet and the intra-cluster, Extragalactic jets on all scales launching, propagation, terminanion (Jets2021), (Onlune, Jun. 14–18,
2021).
Ohmura, T., Ono, K., Sakemi, H., Tashima, Y., Omae, R., Machida, M.:
2021, Magnetohydrodynamics modeling of W 50/SS 433: Continuous
jets and backflow model, 9th microquasar workshop: celebrating over
50 pears of discovery, (Online + Cagliari, Italy, Sep. 20–24, 2021).
Oka, M., Glesener, L., Caspi, A., Narukage, N., the PhoENiX team:
2021, Solar Flares as the Key Toward Understanding Particle
Acceleration in the Plasma Universe, Heliophysics 2050 Workshop,(Online, May 3–7, 2021).
Okamoto, S.: 2022, Subaru Near Field Cosmology Survey, Subaru Users
Meeting FY2021, (Online + Mitaka, Jan. 11–13, 2022).
Okino, H., Akiyama, K., Asada, K., Gomez, J., Hada, K., Krichbaum,T., Kino, M., Nagai, H., Nakamura, M., Honma, M., GMVA 3C273
Collaboration: 2022, The collimation structure of the 3C 273 jet withmulti-frequency VLBI observations, Black Hole Astrophysics withVLBI 2022, (Online, Feb, 7–9, 2022).
Okino, H., Akiyama, K., Asada, K., Gomez, J., Hada, K., Krichbaum,T., Kino, M., Nagai, H., Nakamura, M., Honma, M., GMVA 3C273
Collaboration: 2021, Jet collimation in 3C 273 revealed by multifrequency VLBI observations, EHT Collaboration Meeting 2021
winter, (Online, Dec, 6–10, 2021).
Okosh, M., Murata, K., Ogawa, K.: 2021, Improvement of the spatial
resolution with a deconvolution method for a multi-pinhole SPECT
system, 2021 IEEE Nuclear Science Symposium and Medical
Imaging Conference (NSS/MIC), (Online, Oct. 16–23, 2021).
Omae, R., Akahori, T., Machida, M.: 2021, Effects of Depolarizing
Intervening Galaxies on Background Radio Emission I. Global Disk
Magnetic Field, SPARCS X Capturing Science from the Pathfinder
Survey Data, (Online, Nov. 15–19, 2021).
Onishi, T., et al. including Kojima, T., Uemizu, K., Kaneko, K., Sakai,R., Gonzalez, A., Uzawa, Y.: 2021, Development of a new wideband
heterodyne receiver system (RF: 210–375 GHz, IF: 4–21 GHz) for the
Osaka 1.85-mm mm-submm telescope, ALMA Front End Development(Virtual) Conference 2021, (Online, Sept. 27–30, 2021).
Onodera, M., He W., Ishigaki M. N., Jeschke, E., Moritani Y.,
Tanaka M., Yabe, K., Tamura, N., Reinecke M., Fabricius, M., PFS
obsproc working group: 2022, Development of PFS target database,
PFS 13th collaboration meeting, (Online, Mar. 22–24, 2022).
Onozato, H.: 2022, Current Status and Future Plans of SMOKA, Subaru
Users Meeting FY 2021, (Online + Mitaka, Jan. 11–13, 2022).
Ootsubo, T.: 2022, Infrared ground-based observations of small solarsystem bodies in the JWST era, IR2022: An Infrared Bright Future
for Ground-based IR Observatories in the Era of JWST, (Online, Feb.
14–18, 2022).
Osborne, N., Dainotti, M. G.: 2021, The Scavenger hunt in the optical
data and the 3D optical correlation, NAOJ mini-workshop, (Mitaka,Jul. 29, 2021).
Oshe, N., Dainotti, M. G., Moriya, T., Takiwaki, T., Tominaga, N.,
De Simone, B.: 2021, The GRB-SNe Ib/c connection: search forcorrelations, NAOJ mini-workshop, (Mitaka, Jul. 30, 2021).
Ozaki, S., Uraguchi, F., Shimizu, R., Tsuzuki, T., Miyazaki, S.: 2021,
WFOS IFU: a possible upgrade of Wide Field Optical Spectrometer(WFOS) on TMT, Spatially Resolved Spectroscopy with Extremely
Large Telescopes, (Online, Sep. 20–24, 2021).
Page, M.: 2021, Status of Frequency Dependent Squeezing at TAMA,
LIGO/Virgo/KAGRA collaboration meeting, (Online, Sept. 6–10,
2021).
Pavolotsky, A., Kojima, T., Belitsky, V., Masui, S.: 2021, The status of
SIS Process Development at GARD, ALMA Front End Development(Virtual) Conference 2021, (Online, Sept. 27–30, 2021).
Penteado, E. M., Mamajek, E., des Etangs, A. L., Christensen, L. L.,
Yamaoka, H., Canas, L., Gonzalez, J. R., William, G., AngladaEscude, G., Elmegreen, D.: 2021, IAU100NameExoWorlds:
Projecting Cultural Diversity in the Sky, Communicating Astronomy
with the Public Conference 2021, (Online, May 24–27, 2021).
Pluzhnik, E., Lozi, J., Belikov, R., Sirbu, D., Bendek, E., Guyon, O.,
Fogarty, K.: 2021, Multi-star wavefront control with SCExAO
instrument: demonstration with an internal source, SPIE Optics andPhotonics, (San Diego, Aug. 2–5, 2021).
Richardson, P., Dainotti, M. G., Levine, L.: 2021, The closure relationshipin Fermi-LAT, NAOJ mini-workshop, (Mitaka, Jul. 29, 2021).
Rollins, J., Sun, L., Rolland, L., Estevez, D., Chen, D., Sawada, T., onbehalf of the LVK Calibration groups: 2021, LIGO-Virgo-KAGRA
Calibration O4 Plan & Status, LVK Meeting - March 2022, (Online,
Mar. 14–23, 2022).
Sakai, R., Gonzalez, A., Kaneko, K., Imada, H., Ohtawara, K., Kojima,T., Uzawa, Y., Hirose N., Matsui, T.: 2021, Development of complex
permittivity measurement system, ALMA Front End Development(Virtual) Conference 2021, (Online, Sept. 27–30, 2021).
Sano, H.: 2021, Interstellar Hydrogen in Gamma-Ray Supernova
Remnants as a Key to Understanding the Origin of Cosmic Rays,
Linking the science of large interferometers in the 2030s, (Online,
Nov. 30–Dec. 1, 2021).
Sano, H.: 2021, ASTE science I: Supernova Remnants, ALMA/45m/
ASTE Users Meeting 2021, (Online, Dec. 14, 16, and 21, 2021).
Sarracino, G., Dainotti, M. G., Capozziello, S.: 2021, The X-ray
fundamental plane for X-ray afterglow, NAOJ mini-workshop,(Mitaka, Jul. 29, 2021).
Schiavone, T., Montani, G., Dainotti, M. G., De Simone, B., Lambiase,
G., Rinaldi, E.: 2021, Running Hubble constant from the SNe Ia
Pantheon sample?, International Conference of Physics Student(ICPS), (Online, Aug. 5–8, 2021).
Schiavone, T., Montani, G., Dainotti, M. G., De Simone, B., Lambiase,
G., Rinaldi, E.: 2021, Running Hubble constant from the SNe Ia
Pantheon sample?, 17th Italian-Korean Symposium on Relativistic
Astrophysics 2021, (Online, Aug. 1, 2021).
Schiavone, T., Montani, G., Dainotti, M. G., De Simone, B., Lambiase,

G., Rinaldi, E.: 2021, An inconstant Hubble sample?, ENEA plus,(Online, Jun. 24, 2021).
Sezai, S., Murata, K., Nyui, Y., Ogawa, K.: 2021, Development of a
GPU-based Fast Computational Simulation Code for Quantitative
Evaluation of Scattered Radiation, 2021 IEEE Nuclear Science
Symposium and Medical Imaging Conference (NSS/MIC), (Online,
Oct. 16–23, 2021).
Shan, W., Ezaki, S., Kaneko, K., Miyachi, A., Kojima, T., Uzawa, Y.,
Kang, H., Gonzalez, A.: 2021, Demonstration of a Millimeter-wave
Multibeam Receiver Implemented with Superconducting MMICs,
ALMA Front End Development (Virtual) Conference 2021, (Online,
Sept. 27–30, 2021).
Shan, W., Miyachi, A., Ezaki, S., Makise, K.: 2021, 4K Cryogenic
Nitrogen-deficient NbTiN Thin Film Resistors Fabricated by Using
Reactive Sputtering, 22nd East Asia Submillimeter-wave ReceiverTechnology Workshop, (Online, Nov. 25–26, 2021).
Shimada., R., Murata, K., Ogawa, K.: 2021, Comparison of Scatter
Correction Methods in a Multi-pinhole SPECT, 2021 IEEE Nuclear
Science Symposium and Medical Imaging Conference (NSS/MIC),(Online, Oct. 16–23, 2021).
Shirasaki, Y.: 2021, JVO update, ALMA/45m/ASTE Users Meeting
2021, (Online, Dec. 14, 16, and 21, 2021).
Shirasaki, Y.: 2022, Current status of VO and prospects for improvementof ALMA science archive by VO, East Asian ALMA Development
Workshop 2022, (Online, Mar. 9–10, 2022).
Shoda, M.: 2021, Direct numerical simulations of MHD turbulence inthe solar wind, High-Energy Density Sciences (HEDS) 2021, (Online,
Apr. 19–21, 2021).
Shoda, M.: 2021, Direct numerical simulation of the Alfvénic solar
wind: a theoretical origin of magnetic switchback, JpGU 2021,(Online, May 30–June 6, 2021).
Shoda, M.: 2021, Compressional MHD simulation of the solar wind
turbulence, Lorentz Center workshop “Growth of small scales in thecorona and solar wind 2021”, (Online, Jun. 14–18, 2021).
Shoda, M.: 2021, Turbulent generation of magnetic switchbacks in the
Alfvénic solar wind, Parker One conference, (Online, Jun. 14–18,
2021).
Shoda, M.: 2021, Parametric decay instability of Alfvén wave and its
role in the solar wind acceleration, The Royal Astronomical Society’s
National Astronomy Meeting (NAM) 2021, (Online, Jul. 19–23,
2021).
Shoda, M.: 2021, Solar wind in time: rotation dependence of the stellar
wind properties, Asia Oceania Geosciences Society (AOGS) 2021
18th Annual Meeting, (Online, Aug. 1–6, 2021).
Shoda, M.: 2021, Turbulent generation of magnetic switchbacks in the
Alfvénic solar wind, Joint Scientific Assembly IAGA-IASPEI 2021,(Online, Aug. 21–27, 2021).
Shoda, M.: 2021, Seeking the origin of magnetic switchbacks and theacceleration mechanism of the solar wind, AAPPS Division of Plasma
Physics (DPP) conference 2021, (Online, Sep. 26–Oct. 1, 2021).
Shoda, M.: 2021, Direct numerical simulation of the solar wind & its
application to stellar wind, The 30th International Toki Conference on
Plasma & Fusion Research, (Online, Nov. 16–19, 2021).
Shoda, M.: 2021, Modeling the corona and XUV emission of the Sun
and Sun-like stars, AGU Fall Meeting 2021, (New Orleans, US, Dec.
13–17, 2021).

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Sirbu, D., Marx, D., Belikov, R., Bendek, E., Fogarty, K. W., Kern, B.,
Guyon, O., Pluzhnyk, E. E., Wilson, D. W.: 2021, Model validationof phase-induced amplitude apodization complex mask coronagraphfor LUVOIR-A in vacuum, SPIE Optics and Photonics, (San Diego,
Aug. 2–5, 2021).
Skaf, N., Guyon, O., Boccaletti, A., Deo, V., Lozi, J., Vievard, S., Currie,T., Norris, B., Ahn, K., Gendron, E., Vidal, F., Ferreira, F., Sevin, A.,
Bertrou-Cantou, A.: 2021, High contrast imaging wavefront sensor
referencing from coronagraphic images, SPIE Optics and Photonics,(San Diego, Aug. 2–5, 2021).
Skaf, N., Guyon, O., Deo, V., Lozi, J., Vievard, S., Ahn, K., Boccaletti,
A., Gendron, E., Currie, T.: 2021, High contrast imaging wavefront
sensor referencing from coronagraphic images, Wavefront sensing inthe VLT/ELT era VII, (Online + Valparaiso, Chile, Dec. 1–3, 2021).
Steiger, S., et al. including Currie, T., Guyon, O., Kuzuhara, M., Lozi,J., Vievard, S., Sahoo, A., Deo, V., Tamura, M.: 2021, On-sky
demonstration of stochastic speckle discrimination for companion
detection with the MKID Exoplanet Camera (MEC), SPIE Optics andPhotonics, (San Diego, Aug. 2–5, 2021).
Tadaki, K.: 2022, Formation and evolution of massive galaxies, East
Asian ALMA Science Workshop 2022, (Online, Jan. 18–21, 2022).
Takahashi, S., Tsukamoto, Y., Inutsuka, S., Kokubo, E.: 2022, A
Criterion for Self-Gravitational Fragmentation of Protoplanetary
Disks, Modelling of Disc Fragmentation, Planet Migration andEpisodic Accretion, (Online, Jan. 5–7, 2022).
Takamura, M.: 2022, Measurement of Faraday rotation of NLSy1s
using ultra-wideband VERA polarimetry, Black Hole Astrophysics
with VLBI 2022, (Online, Feb, 7–9, 2022).
Takekoshi, T., Lee, K., Chin, K., Uno, S., Naganuma, T., Inoue, S.,
Niwa, Y., Fujita, K., Kouchi, A., Nakatsubo, S., Mima, S., Oshima,T.: 2021, Material properties of a low contraction and resistivity
silicon—aluminum alloy for cryogenic detectors, 19th International
Workshop on Low Temperature Detectors, (Online, Jul. 19–29, 2021).
Tanaka, M.: 2021, Updates on HSC-SSP, 17th eROSITA-DE
Consortium Meeting, (Online, Jun. 21–24, 2021).
Tanaka, M.: 2021, GALAXY CRUISE, 3rd Shaw-IAU Workshop on
Astronomy for Education, (Online, Oct. 12–15, 2021).
Tanaka, M.: 2022, GALAXY CRUISE, Galaxy Evolution Workshop
2021, (Online, Feb. 7–10, 2022).
Tanaka, M.: 2022, HSC+PFS Science Platform, East Asian ALMA
Development Workshop 2022, (Online, Mar. 9–10, 2022).
Tanaka, M.: 2022, Science Database Updates, PFS 13th collaboration
meeting, (Online, Mar. 22–24, 2022).
Tei, A., Yokoyama, T., Toriumi, S., Hara, H., Imada, S.: 2021, EUV
synthesis project for the Solar-C (EUVST) mission, Japan Geoscience
Union Meeting 2021, (Online, May 31–Jun. 6, 2021).
Tomita, A., Ayani, K., Yamaoka, H., Rokni, M., Baghbani, H.: 2021,
Nowruz, the spring equinox ceremony for the 21st century versionof the Silk Road, Communicating Astronomy with the Public
Conference 2021, (Online, May 24–27, 2021).
Tsukagoshi, T., Nomura, H., Shimajiri, Y., Kawabe, R., Saito, M.,
Momose, M.: 2022, ALMA [CI](1–0) survey for protoplanetary disks,
East Asian ALMA Science Workshop 2022, (Online, Jan. 18–21,2022).
Tsuzuki, H., Hansen, I., Canas, L., Agata, H.: 2021, Women and Girlsin Astronomy 2021: Inspiring Aspiring Girls and Women Through152

XIII Publications, Presentations

Videos and Events from All Over the World, Communicating
Astronomy with the Public Conference 2021, (Online, May 24–27,2021).
Tuyenbayev, D., on behalf of the KAGRA collaboration: 2021,
Introduction of a web-based tool for accessing NDS data, The 27th
KAGRA face to face meeting, (Online, Aug. 28, 2021).
Ueda, T.: 2022, Compact massive dust disk with a gap around CW
Tau revealed by ALMA multi-band observation, East Asian ALMA
Science Workshop 2022, (Online, Jan. 18–21, 2022).
Umurhan, O. M., et al. including the New Horizons Science Team:
2022, Arrokoth’s New Horizons measured brightness temperatureprovides consistent evidence for 0.1–10 mm near subsurface grain
sizes: Possible implications for planetesimal formation models, 53rd
Lunar and Planetary Science Conference (LPSC), (Online + The
Woodlands, Texas, USA, Mar. 7–11, 2022).
Usuda-Sato, K., Suzuki, Y., Kawashima, S., Goko, Y., Inoue, T.:
2021, “Touch the Universe” Tactile Exhibition Anywhere in Japan,
Communicating Astronomy with the Public Conference 2021,(Online, May 24–27, 2021).
Usuda-Sato, K.: 2021, Enjoy the Universe with Diverse People:
Inclusive Astronomy and Citizen Science, Southeast Asia-Regional
Astronomy Seminar (SARAS), (Online, Sep. 21–22, 2021).
Usuda-Sato, K.: 2021, GALAXY CRUISE Engages Citizen Astronomers
to Explore Galaxies, Astronomical Data Analysis Software andSystems (ADASS) XXXI, (Online + Cape Town, South Africa, Oct.
24–28, 2021).
Usuda-Sato, K.: 2021, Dissemination of the “Touch the Universe” Tactile
Exhibition, Second Workshop on Astronomy Beyond the Common
Senses for Accessibility and Inclusion, (Online, Nov. 17–18, 2021).
Uzawa, Y., Kojima, T., Makise, K., Kawakami, A., Kozuki, Y., Masui,
S., Shan, W.: 2021, Development status of an SIS-mixer-based
amplifier, 22nd East Asia Submillimeter-wave Receiver Technology
Workshop, (Online, Nov. 25–26, 2021).
Uzawa, Y., Kojima, T., Makise, K., Kawakami, A., Kozuki, Y., Masui,
S., Shan, W.: 2022, Research and Development toward ALMA
Upgrades, International Symposium on Future Trends of Terahertz
Semiconductor Technologies 2022, (Online, Mar. 5–6, 2022).
Verbiscer, A. J., et al. including the New Horizons Science Team: 2022,
Putting (486958) Arrokoth in context: New Horizons observationsof other small cold classical Kuiper Belt Objects, 53rd Lunar andPlanetary Science Conference (LPSC), (Online + The Woodlands,
Texas, USA, Mar. 7–11, 2022).
Vievard, S., Bonnefois, A., Cassaing, F., Mugnier, L., Sauvage, J.-F.,
Guyon, O., Lozi, J., Deo, V., Ahn, K., Skaf, N.: 2021, Focal Plane
Wavefront Sensing for Fragmented Apertures using Linearized Phase
Diversity, Wavefront sensing in the VLT/ELT era VII, (Online +Valparaiso, Chile, Dec. 1–3, 2021).
Vievard, S., et al. including Ahn, K., Deo, V., Guyon, O., Lozi, J.,
Skaf, N.: 2021, Very high resolution spectro-interferometry withwavefront sensing capabilities on Subaru/SCExAO using photonics,
SPIE Optics and Photonics, (San Diego, Aug. 2–5, 2021).
Wagner, K., Ertel, S., Stone, J., Leisenring, J., Apai, D., Kasper, M.,
Absil, O., Close, L., Defrère, D., Guyon, O., Males, J.: 2021,
Imaging low-mass planets within the habitable zones of nearby stars
with ground-based mid-infrared imaging, SPIE Optics and Photonics,(San Diego, Aug. 2–5, 2021).

Weaver, H. A., et al. including the New Horizons Science Team: 2021,
Discovery of Tight Binaries in the Kuiper Belt by New Horizons
LORRI, DPS/AAS (AAS Division for Planetary Sciences) 53rd
Annual Meeting, (Online, Oct. 3–8, 2021).
Wei, C.-E., Nomura, H., Theule, P., Walsh, C.: 2021, Formationof Complex Organic Molecules through Ice Mantle Reactions,
Workshop on ISM 2021, (Hokkaido, Japan, Nov. 17–19, 2021).
Wozniak, K., Dainotti, M. G.: 2021, GRB estimator and optimization tofollow-up high redshift GRBs, NAOJ mini-workshop, (Mitaka, Jul.
30, 2021).
Yamamoto, K.: 2021, Simulation of Phobos internal density structure
estimation by MMX orbit determination, Symposium on Asteroids
and Comets Gravity and Interiors, (Online, Dec. 8–10, 2021).
Yamamoto, K.: 2022, Simulation of Phobos internal density structure
estimation by MMX orbit determination, MMX Science Working
Team meeting, (Online, Mar. 14–16, 2022).
Yamaoka, H.: 2022, NAOJ’s Challenge in Protecting the Sky, NOC
sharing Session #1, (Online, Mar. 1, 2022).
Yamasaki, Y., Hasegawa, Y., Masui, S., Yoneyama, S., Kawashita, S.,
Chinen, T., Onishi, T., Ogawa, O., Tatematsu, K., Miyazawa, C.,
Takahashi, T., Maekawa, J., Gonzalez, A., Kojima, T., Imada, H.,
Kaneko, K., Sakai, R., Sakai, T.: 2021, Development of new optics
for a 7-beam receiver in 72–116 GHz band onboard the Nobeyama
45-m telescope, ALMA Front End Development (Virtual) Conference
2021, (Online, Sept. 27–30, 2021).
Yamasaki, Y., Hasegawa, Y., Masui, S., Yoneyama, S., Kawashita, S.,
Chinen, T., Onishi, T., Ogawa, O., Tatematsu, K., Miyazawa, C.,
Takahashi, T., Maekawa, J., Gonzalez, A., Kojima, T., Imada,H., Kaneko, K., Sakai, R., Sakai T.: 2021, Investigation of optimal
dielectric lens for a new 7-beam receiver in 72–116 GHz on the
Nobeyama 45-m telescope, 22nd East Asia Submillimeter-wave
Receiver Technology Workshop, (Online, Nov. 25–26, 2021).
Yamashita, T., Mineno, S., Tanaka M., the PFS 2D DRP development
team: 2022, Flux calibration development in 2D data reduction
pipeline, PFS 13th collaboration meeting, (Online, Mar. 22–24, 2022).
Yoshida, M.: 2021, Subaru Telescope Update 2021, Keck Science
Meeting 2021, (Online, Sep. 9 2021).
Yoshida, M.: 2021, Overview of Subaru Telescope, SUPER-IRNET
Symposium, (Online, Aug. 25 2021).
Yoshida, M.: 2022, Annual Report of Subaru Telescope, Subaru Users
Meeting FY2021, (Online + Mitaka, Jan. 11–13, 2022).
Yoshiura, S.: 2021, Detecting the 21cm power spectrum from the Epochof Reionization and Cosmic Dawn, East Asia SKA Workshop 2021,(Online, May 26–28, 2021).
Young, S., Dainotti, M. G.: 2021, The 2D optical luminosity correlationand the SUBARU data, NAOJ mini-workshop, (Mitaka, Jul. 29, 2021).
Zapart, C.: 2021, Julia meets BIG DATA: JVO experience with
distributed computing, Astronomical Data Analysis Software andSystems (ADASS) XXXI, (Online + Cape Town, South Africa, Oct.
24–28, 2021).
Zavala, J. A.: 2022, Dust and gas properties in high-z galaxies fromfuture submm surveys, East Asian ALMA Science Workshop 2022,(Online, Jan. 18–21, 2022).
Zavala, J. A.: 2022, Galaxy evolution with the new COSMOS’ surveys,
Galaxy Evolution Workshop 2021, (Online, Feb. 7–10, 2022).
Zemaitis, R., Ferguson, A., Okamoto, S., Arimoto, A., Irwin, M.,

Utsumi, Y.: 2021, The Unseen Side of F8D1 through the Lens ofHyper Suprime-Cam, The Royal Astronomical Society’s National
Astronomy Meeting (NAM) 2021, (Online, Jul. 19–23, 2021).
Zhou, D., Dainotti, M. G., Narendra, A., Pollo, A., Bogdan, M.: 2021,
GRB redshift determination with ML regression models, NAOJ miniworkshop, (Mitaka, Jul. 30, 2021).
Zvonarek, K., Dainotti, M. G., Levine, L.: 2021, The closure
relationship in radio afterglows, NAOJ mini-workshop, (Mitaka, Jul.
29, 2021).

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