Cover Caption
Artist's impression of the explosion phenomenon (kilonova) accompanying the gravitational
wave event GW170817 induced by neutron star merger. The kilonova image detected by
the Subaru Telescope and IRSF is shown in the lower right corner. The kilonova emission
becomes darker and redder with time.
Credit: NAOJ/Nagoya University

Postscript
Editor Publications Committee
HANAOKA, Yoichiro
UEDA, Akitoshi
OE, Masafumi
SÔMA, Mitsuru
NISHIKAWA, Jun
HIROTA, Tomoya
YOSHIDA, Haruo
Publisher

PrinterNational Institutes of Natural Sciences

National Astronomical Observatory of Japan
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TEL: +81-422-34-3600
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Annual Report of the
National Astronomical Observatory of Japan

Volume 20, Fiscal 2017

T A

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Preface

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O F

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O N T

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Saku TSUNETA
Director General
National Astronomical Observatory of JapanI Scientific Highlights April 2017 – March 2018001

II Status Reports of Research Activities
01. Subaru Telescope
02. Okayama Astrophysical Observatory
03. Nobeyama Radio Observatory
04. Mizusawa VLBI Observatory
05. Solar Science Observatory
06. NAOJ Chile Observatory
07. Center for Computational Astrophysics
08. Gravitational Wave Project Office
09. TMT-J Project Office
10. JASMINE Project Office
11. Extra-Solar Planet Detection Project Office
12. RISE Project
13. Solar-C Project Office
14. Astronomy Data Center
15. Advanced Technology Center
16. Public Relations Center
17. Division of Optical and Infrared Astronomy
18. Division of Radio Astronomy
19. Division of Solar and Plasma Astrophysics
20. Division of Theoretical Astronomy
21. Office of International Relations

052
056
061
064
069
071
074
077
079
082
084
086
087
089
091
097
104
107
110
111
114

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III Organization

116

IV Finance

139

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

140

VI Research Collaboration

141

VII Graduate Course Education

143

VIII Public Access to Facilities

148

IX Overseas Travel

152

X Award Winners

153

XI Library, Publications155

XII Important Dates

156

XIII Publications, Presentations
1. Refereed Publications

159

2. Publications of the National Astronomical Observatory of Japan179

3. Report of the National Astronomical Observatory of Japan179

4. Conference Proceedings

180

5. Publications in English

182

6. Conference Presentations

182

Annual Report of the
National Astronomical Observatory of Japan
Volume 20, Fiscal 2017

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

Looking back over the annual report of the National
Astronomical Observatory of Japan (NAOJ) for Fiscal Year2017 (April 2017 – March 2018), we can say that this year
saw many important developments in the field of Astronomy.
I am pleased to say that NAOJ participated in many of theseadvancements and discoveries. This year NAOJ was also
active developing new instruments to ensure that we willcontinue to play a major role in world astronomy in the future.
First of course, this year we saw the dawn of a new age ofmulti-messenger astronomy. The Subaru Telescope detected
the electromagnetic counterpart to GW170817, the firstrecorded gravitational wave produced by the merger of binary
neutron stars, which was initially detected by LIGO (Laser
Interferometer Gravitational-Wave Observatory) in the UnitedStates and Europe’s VIRGO in August 2017. Comparing
observations of the changes in visible and infrared light overtime to numerical simulations helped to finally confirm thatrare earth metals such as gold are formed through the processof rapid neutron capture (r-process) in merging neutron stars.
In Japan, NAOJ and the High Energy Accelerator
Research Organization are participating in the constructionof the Large-scale Cryogenic Gravitational Wave Telescopein Kamioka (Kamioka Gravitational wave detector, KAGRA)
led by the Institute for Cosmic Ray Research of the Universityof Tokyo. KAGRA utilizes the technology and experience
gained from NAOJ’s TAMA300 300-m laser interferometer
gravitational wave detector built in Mitaka Campus in
the 1990’s. NAOJ was responsible for the basic design of
KAGRA, and utilizing the high level engineering skills of theAdvanced Technology Center developed a 14-m multilevel
ultra-high performance vibration isolator, a transmitted lightmonitoring system, and also designed and produced baffles tocounteract all types of scattered light. NAOJ also established
the Kamioka Branch of the Gravitational Wave Project Officeand has played a major role in developing KAGRA.
KAGRA hopes to perform joint observation with LIGO
and Virgo in the second half of 2019. By joining the world
wide gravitational wave detector network, KAGRA will help
to improve the localization of gravitational waves sources,
as well as greatly improving humanity’s gravitational
waves observation capabilities. With coordinated follow-up
observations by electromagnetic telescopes, expectations for
multi-messenger astronomy are very high.
Expectations are also high in radio astronomy. ALMA
started the 5th observation cycle (Cycle 5) from October 2017.
A total of 1,664 observation proposals were received fromall over the world. The total observation time of 4,000 hours
using 12-m antennas during Cycle 5 is a substantial increase
compared to the 3,000 hours during Cycle 4. This is a credit
to the unrelenting efforts of the Joint ALMA Observatory
to improve operations. Additionally, for bands 3, 4, and 6
the maximum baseline of 16 km became available, offering
unprecedented spatial resolution.

The breakdown of ALMA observation papers by subject
is: 23 % “planetary formation”, 22 % “interstellar matter/starformation”, 22 % “active galaxies”, and 33 % miscellaneous
areas. Papers utilizing archived data have also been increasing,and now account for 22 % of the total. If we include papers
that combine new PI data with archive data, the total rises to
27 %. Japan has been very competitive in publishing research
papers using ALMA; it is the nation with the second highest
total of papers after the United States.
In 2017, a large number of papers on protoplanetary disks
and their varieties were published using ALMA observations.
By examining a large number of protoplanetary disks,
astronomers hope to better understand the causes of thevarieties of exoplanets. Additionally, the discovery of rotating
outflows from protostars in Orion has given us a valuable
hint to understand protostars and the transport of angularmomentum in the disks that surround them.
ALMA has also been contributing to the observationof organic molecules. The organic compound acrylonitrile
was discovered in the atmosphere of Saturn’s moon Titan.
This molecule is thought to be capable of naturally forming
membrane-like structures. It is believed that the primeval
Earth had an atmosphere similar to Titan’s, so this is an
important clue to understanding abiogenesis.
Furthermore, observations of a galaxy cluster 9.4 billion
light-years away (z = 1.5) found that the temperature of the gas
in each galaxy decreases for galaxies closer to the peripheryof the cluster. This suggests that cold molecular gas belonging
to the member galaxies is being stripped off by hot gas fromthe cluster. This important discovery betters our understandingof the factors contributing to the gradual decline of starformation throughout the Universe since its peak 10 billion
years ago.
Last year we reported that ALMA had detected theredshifted 88 μm emission line of ionized oxygen in a distantgalaxy discovered by the Subaru Telescope 13.1 billion lightyears away (z = 7.2). This was the most distant confirmationof oxygen in the Universe. ALMA quickly broke this record
with the discovery of oxygen in a galaxy 13.2 billion lightyears away (z = 8.4), drawing us closer to the epoch of cosmic
reionization.
Speaking of the Subaru Telescope, open use at Japan’s
flagship optical-infrared facility is proceeding well. NAOJ
succeeded in creating a wide area three-dimensional mapof dark matter using weak gravitational lensing analysis ondata from the Hyper Suprime-Cam Subaru Strategic Program(HSC SSP). The scope of this HSC dark matter map is morethan 15 times that of previous ones constructed from Hubble
Space Telescope data. It provides a detailed picture of theassembly of matter in the Universe over the past 7.5 billion
years. Other observations utilizing HSC’s ultra-wide field ofview discovered a massive cluster of protogalaxies located
12 billion light-years away. Discoveries such as this bring us

closer to understanding the composition of the early Universe.
The initial results of the HSC SSP observations werecovered in a special edition of the Publications of the
Astronomical Society of Japan (PASJ). The data acquiredat that time was only about a tenth of the total plan, but its
uniqueness enabled the publication of 40 research papers. By
2020, HSC observations are scheduled to cover over 1000
square degrees of the sky with more resolution and depth thanever before. Please watch for future results from HSC.
The Subaru Telescope’s next major instrument after HSC,
the Prime Focus Spectrograph (PFS), is being developedby a collaboration of seven countries led by Kavli IPMU
at the University of Tokyo. PFS is a revolutionary piece ofequipment that has approximately 2,400 optical fibers arrayed
across a field of view comparable to that of HSC. Light
from the sky is directed into four spectrographs, and spectra
ranging from 0.38–1.26 μm can be measured simultaneously.
Development is being carried out across various institutions,aiming to start scientific observations by 2021. Uponcompletion, PFS will allow further inquiry into the distance,
speed, and chemical composition of the multitude of
unidentified celestial bodies captured by HSC. As a result, we
expect major progress towards unveiling the mysteries of darkenergy, as well as gaining a clearer picture of how galaxies
formed throughout the long history of the Universe.
A new exoplanet observation instrument is also underdevelopment at the Subaru Telescope. Final adjustments weremade at the summit in order for the InfraRed Doppler instrument(IRD) to begin open use in 2018. The Subaru Coronagraphic
Extreme Adaptive Optics (SCExAO), which allows for direct
observation of exoplanets, and the Coronagraphic High
Angular Resolution Imaging Spectrograph (CHARIS) arealready available for open use. The development and operationof these instruments are led by the Astrobiology Center,
which was established by the National Institutes of Natural
Sciences in 2015. In December 2017, the NAOJ Extrasolar
Planet Detection Project Office dissolved and relocated to the
Astrobiology Center. Progress in not only exoplanet research,
but also astrobiology, is expected from coordination between
the Astrobiology Center and NAOJ.
At Okayama Astrophysical Observatory, which supported
Japan’s astronomical research for 57 years, open use observations
concluded at the end of 2017. Okayama AstrophysicalObservatory served as the cornerstone to elevate Japanese
astronomy to the world level during the postwar reconstruction
period. It fostered many researchers, and was a driving force
behind the very successful Subaru Telescope. In the future, wewill shift our focus to the open use for Japanese universities
on the Seimei Telescope, Kyoto University’s telescope inOkayama Campus. University researchers will assume
the operation of the Okayama Astrophysical Observatory
telescopes, with support from NAOJ. The Okayama 188-cm
Reflector Telescope has produced outstanding achievements,
such as discovering over 30 exoplanets. We expect even better
results from it in its new role as a dedicated exoplanet telescope.
We also have high hopes for the Thirty Meter Telescope(TMT) Project, a five-nation collaboration between Japan,
the United States, Canada, China, and India to construct an
extremely large telescope with a 30-meter diameter primary
mirror. It is expected to produce groundbreaking results
through exploration of terrestrial exoplanets, tracing of theearly history of the Universe, identification of dark energy, andother research activities. NAOJ is in charge of some of the key
components of TMT, including fabrication of the telescope
structure and the primary mirror. The construction site is

located on Maunakea on the Island of Hawai‘i; however,on-site construction has been suspended for three years,
becoming a cause of concern for all involved. Still, design
and fabrication of the respective work responsibilities haveprogressed steadily in Japan, as well as the other countries,
throughout the delay in on-site construction.
The State of Hawai‘i Board of Land and Natural Resources(BLNR) approved the sublease agreement executed between
the University of Hawai‘i in charge of the management of theMaunakea lands and the TMT International Observatory (TIO)
in July 2014, and in September 2017, granted the Conservation
District Use Permit (CDUP) that is required to build in the
Maunakea summit area. Lawsuits were filed in response to
the BLNR decisions. But the Supreme Court of Hawai‘i
ruled that there are no problems in the sublease agreement
in August 2018, and in October of the same year the court
found the CDUP to be valid. Having continuously engaged
in a number of dialogues with the community of Hawai‘i,
we have obtained its greater support and understanding,and are currently proceeding carefully in discussions withstakeholders in Hawai‘i to prepare for resuming construction
expeditiously.
The scope of astronomy has grown to encompass
fields ranging from basic physics to life sciences, making
cooperation with physicists, chemists, and biologists
vital. University researchers also contribute greatly to the
production of research results, as well as to the developmentof new observational instruments. NAOJ’s large-scaleobservational facilities provide the foundation of an effective
dual support system for university researchers. The facilities
offer the researchers open use observation time to pursue theirown research and also provide a platform for the developmentof major instrumentation with external funding acquired by
the researchers.
There have been concerns about the decline of science inJapan. Eleven of the fourteen fields of natural sciences, which
include physics, chemistry, medical science, and materials
science, have experienced drops in the number of scientificpapers published. And reports have indicated that even thefields that aren’t experiencing drops are falling behind theworld average. However, astronomy is the only field ofstudy experiencing a growth in scientific articles while also
exceeding worldwide averages. Among the fourteen divisionsof natural sciences in Japan, Astronomy also has the highest
share of papers published worldwide. (Refer to “What pricewill science pay for austerity?” Nature 543, S10–S15 (23March 2017), https://dx.doi.org/10.1038/543S10a)
The Subaru Telescope and ALMA have been major
milestones in Japanese science. The rapid developmentof Japanese astronomy, as demonstrated by large-scaleobservational facilities such as these, acted as a catalyst for
new developments and stimulation in Japanese science andresearch facilities. The remarkable scientific returns enabled
by astronomy have increased Japan’s international profile,
while instilling a sense of national pride, and developing aninterest in science among the Japanese people, especiallythe younger generations. In keeping with its duty as part of
the Inter-University Research Institute Corporation, NAOJ
will strive to pioneer new technology while proposing andimplementing large-scale international collaborative projects
dealing with fascinating subjects.

I Scientific Highlights(April 2017 – March 2018)01

Formation of Close-in Super-Earths by Giant Impacts: Effects of Initial Eccentricities andInclinations of Protoplanets

Matsumoto, Y., Kokubo, E.

003

Hanaoka, Y., Sakurai, T.

004

03 ALMA Reveals a Rotating Dense Molecular Torus in NGC 1068

Imanishi, M., et al.

005

04 ALMA Dense Molecular Gas Observations of IRAS 20551−4250

Imanishi, M., et al.

006

Takahashi, H., Ohsuga, K.

007

06 Cyanopolyyne Chemistry in High-Mass Star-Forming Regions

Taniguchi, K., Saito, M.

008

07 Formation Mechanisms of Cyanopolyynes in Low-Mass Starless Cores

Taniguchi, K., Saito, M.

009

Yamauchi, A., et al.

010

09 Evidence for Higher Black Hole Spin in Radio-loud Quasars

Schulze, A., et al.

011

10 Rotating Starburst Cores in Massive Galaxies at z = 2.5

Tadaki, K., et al.

012

11 First ALMA Observation of a Solar Plasmoid Ejection from an X-ray Bright Point

Shimojo, M., et al.

013

12 Variation of Solar Microwave Spectrum in the Last Half Century

Shimojo, M., et al.

014

13 Joint Strong and Weak Lensing Analysis of the Massive Cluster Field J0850+3604

Wong, K. C., et al.

015

14 ALMA Observations of the Gravitational Lens SDP.9

Wong, K. C., et al.

016

02 Statistical Study of the Magnetic Field Orientation in Solar Filaments

05

General Relativistic Radiation MHD Simulations of Supercritical Accretion onto a
Magnetized Neutron Star: Modeling of Ultraluminous X-Ray Pulsars

08 Discovery of H2O Megamasers in Obscured Active Galactic Nuclei

15

Near-infrared Spectroscopic Observations of Comet C/2013 R1 (Lovejoy) by WINERED:CN Red-system Band Emission

Shinnaka, Y., et al.

017

16

Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selectedby Swift/BAT Hard X-Ray Survey

Tanimoto, A., et al.

018

17

Superluminous Transients at AGN Centers from Interaction between Black Hole Disk Winds
and Broad-line Region Clouds

Moriya, T., et al.

019

18 On the Macroturbulence Model for the Solar Photospheric Velocity Field

Takeda, Y., Ueno, S.

020

19 Testing the Planet-engulfment Hypothesis as the Origin of Li-rich Giants

Takeda, Y., Tajitsu, A.

021

Takeda, Y., et al.

022

Suematsu, Y., et al.

023

Komiyama, Y., et al.

024

Yagi, M., et al.

025

Michikoshi, S, Kokubo, E.

026

Baba, J.

027

Shirasaki, Y., et al.

028

Yoshida, F., Terai, T.

029

20 Luminosity Effect of O I 7771-5 Line Strength in Evolved A-F-G Stars
21 Development of Micro-Mirror Slicer Integral Field Unit for Space-borne Solar Spectrographs
22

Stellar Stream and Halo Structure of Andromeda Galaxy revealed by Subaru Hyper
Suprime-Cam

23 Extended Ionized Gas out of Galaxies in the Leo Cluster (Abell 1367)
24 Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk
25 Gaia DR1 Evidence of Disrupting the Perseus Arm
26 Properties of Galaxies around AGNs in the HSC Wide Survey
27 Small Jupiter Trojans Survey with the Subaru/Hyper Suprime-Cam
28

Multi-band Photometry of Trans-Neptunian Objects in the Subaru Hyper Suprime-Cam
SurveyTerai, T., et al.

030

29

Disentangling the Circumnuclear Disk of Centaurus A with ALMA: An Inner MolecularRing, Nuclear Shocks and the CO to Warm H 2 Interface

Espada, D., et al.

031

Sasaki, H., et al.

032

Izumi, T., et al.

033

30 Supernova Nucleosynthesis Enhanced by Collective Neutrino Oscillations
31

On the Disappearance of a Cold Molecular Torus around the Low-luminosity Active Galactic
Nucleus of NGC 1097

001

Molecular Gas Fraction in Interacting Galaxies in Early and Mid Stage Using 12CO(J = 1–0)
Mapping Observations

Kaneko, H., et al.

034

33 Searches for New Milky Way Satellites from the Subaru/HSC Survey: Discovery of Cetus III

Homma, D., et al.

035

Detection of Rotating Outflow Driven by a High-mass Protostar Candidate Orion KL Radio
Source I

Hirota, T., et al.

036

Hayashi, M., et al.

037

Tanaka, I., et al.

038

Koyama, S., et al.

039

Ikeda, H., et al.

040

Hada, K., et al.

041

Sugiyama, K., et al.

042

Giono G., et al.

043

32

34

35 Evolutionary Phases of Gas-rich Galaxies in a Galaxy Cluster at z = 1.46
36 Morphological Evidence for a Past Minor Merger in the Seyfert Galaxy NGC 1068
37

A Universal Correlation between Star Formation Activity and Molecular Gas Properties
across Environments

38

An Optically Faint Quasar Survey at z ~ 5 in the CFHTLS Wide Field: Estimates of the Black
Hole Masses and Eddington Ratios

39 Pilot KaVA (KVN and VERA Array) Monitoring of the M87 Jet
40

The Shortest Periodic and Flaring Activity of the 6.7 GHz Methanol Maser in theIntermediate-mass Protostar G 014.23–00.50

41

Polarization Calibration of the Chromospheric Lyman-Alpha SpectroPolarimeter for a 0.1 %Polarization Sensitivity in the VUV Range

42

Strong Magnetic Field Generated by the Extreme Oxygen-rich Red Supergiant VY Canis
MajorisShinnaga, H., et al.

044

43

Big-Bang Lithium Problem, and Effects of Long-Lived Negatively Charged Massive Particles
on Primordial Nucleosynthesis

Kusakabe, M., et al.

045

Mathews, G. J., et al.

046

Yamazaki, D. G., et al.

047

Iwasawa, M., et al.

048

Boyd, R., et al.

049

Famiano, M., et al.

050

Shin, J.-W., et al.

051

44 Big Bang Nucleosynthesis and Modern Cosmology
45

The New Hybrid BBN Model with the Photon Cooling, X Particle, and the Primordial
Magnetic Field

46 PENTACLE: Parallelized Particle-particle Particle-tree Code for Planet Formation
47

Production of Left-handed Amino Acids in Space in the Supernova Neutrino Amino Acid
Processing (SNAAP) Model

48 Selection of Amino Acid Homochirality in Stellar Environments
49002

Short-baseline Electron Antineutrino Disappearance Study by Using Neutrino Sources from
13C + 9Be Reaction

Formation of Close-in Super-Earths by Giant Impacts:
Effects of Initial Eccentricities and Inclinations of Protoplanets
MATSUMOTO, Yuji

KOKUBO, Eiichiro

Nowadays, dozens super-Earths, which are composedrock or ice, are already found in orbits that are close to
their stars (e.g., [1]). Recent observations have reveled
the orbital eccentricity (e) and orbital inclination (i)distributions of super-Earths [2,3]. We considered how
the eccentricities and inclinations of close-in superEarths are determined in the giant impact stage. These
evolve through gravitational scattering and collisions
between protoplanets in gas-free environments. The
eccentricities are increased by scattering between
protoplanets [4], and they are damped by collisions [5].
The collisions tend to occur at the point where theirorbits initially crossing since the small scattering crosssection of protoplanets in the close-in region. The orbitalcrossing initially occurs around the apocenter of theinner protoplanet and the pericenter of the outer planet.
As a result, the velocity of merged body is about equal to
the Kepler velocity.
We studied the effects of the initial e and i ofprotoplanets on the final orbits of planets formed by
giant impacts [6]. We performed N-body simulationsof the protoplanet accretion over 500 times. Numericalcomputations were carried out on the PC cluster at theCenter for Computational Astrophysics, NAOJ.
We found that the final eccentricities do not depend
on initial eccentricities, when orbits of protoplanets are
initially not crossed. While the eccentricities gradually
increase with each collision if initial e is small, they
gradually decrease when initial e is large. The final
planets become similar due to these relaxations.
On the other hand, the initial inclinations are
not relaxed. When the initial i is small, the velocity
dispersions normal to the disk midplane keep small
through scattering, and the final planets have small i. If
the initial i is large, collisions do not occur immediately
after orbital crossing, since they can collide only inparts of their orbits. Protoplanets experience more
scattering until a collision, which make i larger. This is
why the merged protoplanets have larger i. And, final
inclinations of planets depend on initial inclinations.
The eccentricities In large i cases are larger those insmall i cases due to more scattering. We found that the
inclinations of observed planets are consistent with our
results, if protoplanets initially have ~ 10 −3 –10 −2 radinclinations (Figure 1, [6]).

(d)(Academia Sinica)		

(NAOJ)

10-1

 i M [rad]

				

10

-2

10-3
-4
-3
-2
-1
0
10 10 10 10 102
 i ini 1/2[rad]Figure 1: This figure is from the panel (d) of Figure 9 in [6]. The
mass-weighted inclination (iM) is shown as a functionof the initial inclination dispersion of protoplanets(i 2ini1/2). The error bars indicate the standard deviation.
The filled symbols are the results of models that initial
number of protoplanets is Nini = 16 (models N16), theopen symbols are those of models N8, and crosses
are those of models N32. The initial eccentricity
dispersions are different between red circles and blue
triangles. The solid and dashed lines are the fits by theleast-squares-fit method for models. The dotted lines
shows the mode of the mutual inclination [2,3].

References[1] Mullally, F., et al.: 2015, ApJS, 217, 31.
[2] Fabrycky, D. C., et al.: 2014, ApJ, 790, 146.
[3] Xie, J. W., et al.: 2016, P. Natl. Acad. Sci. USA, 113, 11431.
[4] Kokubo, E., Ida, S.: 2002, ApJ, 581, 666.
[5] Matsumoto, Y., Nagasawa, M., Ida, S.: 2015, ApJ, 810, 106 .
[6] Matsumoto, Y., Kokubo, E.: 2017, AJ, 154, 27.

I Scientific Highlights003

Statistical Study of the Magnetic Field Orientation
in Solar Filaments
HANAOKA, Yoichiro, SAKURAI, Takashi(NAOJ)

Reference[1] Hanaoka, Y., Sakurai, T.: 2017, ApJ, 851, 130.

004

I Scientific Highlights

(a)

(b)

Figure 1: A f ilament (located in the nor ther n hemisphere)
observed on 2014 November 23. The celestial northis to the top. (a) Hα image of the filament and (b) the
linear polarization signals ( > 0.1 %) represented by redlines drawn on the photospheric magnetogram. At thelower-right corner, the approximate direction of theaxis of the filament is shown with a solid line, and theaverage direction of the linear polarization signals isshown with a dashed line.
N-Hemispherecounterclockwise

S-Hemisphere50

0clockwise

Deviation Angle (deg)We have been carrying out full-Sun, full-Stokes
spectropolarimetric observations using the He I 1083.0
nm line since 2010. The He I 1083.0 linear polarization
signals of solar filaments show the magnetic field in
filaments. Figure 1 shows a filament observed in Hα andin He I 1083.0. The linear polarization signals in panel (b)is approximately parallel to the fine structures seen in the
Hα image in panel (a), and they are almost aligned. We
can define the average direction of the magnetic field,
and it deviates clockwise with respect to the filamentaxis.
We have carried out a statistical study of the averageorientation of the magnetic field in filaments with respect
to their axes for 438 samples [1]. Figure 2 shows therelation between the latitude and the deviation of theaverage magnetic field of filament samples. This figure
show a clear hemispheric tendency; most filaments inthe northern (southern) hemisphere show the clockwise(counterclockwise) deviation of the average magnetic
field direction. The deviation angles of the magnetic fieldfrom the axes have the peak around 10–30° (the lightgreen belts in Figure 2). Such a hemispheric tendency
has been studied for the chirality of the fine structuresin filaments and the magnetic field in prominences, andour results are consistent with them. Therefore, ourresults confirm the hemispheric tendency of the filament
magnetic fileds with the direct measurements of themagnetic field in filaments for the first time.
There is an interesting feature in the filaments which
violate the hemispheric tendency; the alignment of the
background magnetic field of such filaments is in manycases opposite to that of active regions following theHale-Nicholson law.
A filament is considered to be located at the bottomof a magnetic f lux rope, which often erupts into theinterplanetary space as a part of a coronal mass ejection(CME). Therefore, our observation of the filament
magnetic field can be used to predict the magnetic fieldof CME flux ropes, which is the key to investigate theirimpact to the geomagnetic field.

-50

-60

-40

-20

0
20
Latitude (deg)40

60

Figure 2: The relation between the latitude of the filaments andtheir average deviation angle. Black symbols represent
filaments in the quiet areas, and red symbols represent
those in the active areas. The cross symbols correspondto the filaments with the preceding positive polarity,and the box symbols correspond to the filaments withthe preceding negative polarity. The dots show thefilaments where the alignment of the polarity cannot be
defined clearly. The vertical lines are error bars.

ALMA Reveals a Rotating Dense Molecular Torus in NGC 1068
IMANISHI, Masatoshi, NAKANISHI, Kouichiro, IZUMI, Takuma

				(NAOJ)					Active galactic nuclei (AGNs) emit strong radiationfrom the compact nuclear regions of galaxies. It is
widely believed that a mass-accreting supermassive
black hole (SMBH) is present at the center, surrounded
by toroidally distributed (torus shaped) gas and dust
which are thought to be rotating under the gravitational
potential of the central SMBH. If this kind of gas anddust torus is present, various observational results of
AGNs can naturally be explained (the so-called AGN
unified model), so that researchers believe that such atorus is present. However, since the torus is spatiallyvery compact, < 10 pc in physical size or < 0.15 arcsec at
the distance of 15 Mpc, its observational understanding is
still highly incomplete. Thanks to the advent of ALMA
with high spatial resolution observing capability, ourunderstanding of the AGN torus is expected to improve alot.
NGC 1068 (z=0.0037, distance ~14 Mpc) is a nearby
well-studied AGN. From previously revealed spatial
distribution of optical ionized gas emission and radio
jet, there is a consensus that the torus should be locatedalong the almost east-west direction. ALMA highspatial-resolution CO J=6–5 observational results werereported, but its dynamical direction is along the almost
north-south direction, rather than the expected east-west
torus direction. The results are largely different from theclassical torus picture.
We have observed NGC 1068, with 0.04 arcsec ×
0.07 arcsec resolution, in the HCN J=3–2 (265.89 GHz)and HCO+ J=3–2 (267.56 GHz) lines, both of which are
known to be good dense gas tracers. We have detected
east-west oriented dense molecular emission androtation (Figure 1), as expected. However, the observed
rotation is slower than that expected from Keplerianmotion dominated by the gravity of the central SMBH.
Dense molecular emission and velocity dispersion areasymmetric. We interpret that the dense molecularemission is brighter at the western part of the central
mass-accreting SMBH, due to higher turbulence andresulting reduced line opacity. We have also found that
dense gas at the eastern (western) part of the torus isredshifted (blueshifted) (Figure 1), while that at thecentral part of the host galaxy outside the torus, along thetorus direction, is counter-rotating (i.e., eastern region isblueshifted and western region is redshifted) (Figure 2),
suggesting that some external process happened in thepast. This may be the result of a minor galaxy merger [1].

WADA, Keiichi(Kagoshima University)

Figure 1: Integrated intensity (Left), intensity-weighted mean
velocity (Middle), and intensity-weighted velocity
dispersion (Right) maps of the HCN J=3–2 (Top) andHCO + J=3–2 (Bottom) emission lines in the torus
region with ~10 pc scale around the mass-accreting
SMBH (denoted as the “+” mark). Gas at the easternpart (left side of the figures) is redshifted, and that at
the western part (right side of the figures) is blueshifted.
At the western part, both lines are brighter and velocity
dispersion is larger.

Figure 2: Integrated intensity (Left) and intensity-weighted mean
velocity (Right) maps of the HCN J=3–2 emission line
at the central ~350 pc region of the host galaxy. The
mark “AGN” (in the left panel) corresponds to the torus
in Figure 1. Dense molecular gas at the eastern (western)part outside the torus along the torus direction (solidline in the right panel) is blueshifted (redshifted),suggesting counter-rotation of dense gas inside andoutside the torus. The HCO+ line also shows virtually
the same properties.

Reference[1] Imanishi, M., et al.: 2018, ApJL, 853, L25.

I Scientific Highlights

005

ALMA Dense Molecular Gas Observations of IRAS 20551−4250
IMANISHI, Masatoshi, NAKANISHI, Kouichiro, IZUMI, Takuma(NAOJ)

Ultraluminous infrared galaxies (ULIRGs; L IR >1012 L) are formed by gas-rich galaxy mergers and areshining brightly in the infrared due to thermal emission
from dust heated by deeply buried starbursts and AGNs(= mass-accreting supermassive black holes; SMBHs).
Distinguishing the hidden energy sources of ULIRGs isimportant to understand the star formation and SMBH
mass growth during galaxy mergers. Since starbursts
and AGNs have different energy generation mechanisms,
physical and chemical effects to the sur rounding
molecular gas should be different. It is expected thatstarbursts and AGNs can be distinguished based onmolecular rotational J-transition line flux ratios at the(almost) dust-extinction-free (sub)millimeter wavelength
range.
It has been argued that HCN rotational J-transitionline fluxes, relative to HCO+, are stronger in AGNs thanin starbursts. Possible reasons include (a) high HCN
abundance in AGNs, and (b) vibrational excitation of
HCN by infrared radiative pumping (by absorbing 14 μm
photons) and the increase of the rotational J-transitionline fluxes at the vibrational ground level due to decay
back. IRAS 20551−4250 (z=0.043) is a ULIRG whichcontains a luminous buried AGN and shows a higher
HCN-to-HCO + f lux ratio than starbursts (Figure 1).
Thanks to small molecular line widths, vibrationallyexcited HCN and HNC emission lines were clearly
detected ([1]), so that this ULIRG is a good target toquantitatively estimate the contribution from (b). We
have observed this ULIRG at multiple J-transition linesof HCN, HCO+, and HNC (Figure 2), and obtained thefollowing results. (1) Main to isotopologue molecularline flux ratios at J=3–2 is smaller for HCN than HCO+
and H NC, due to larger line opacity of HCN. An
enhanced HCN abundance is suggested. The intrinsic
HCN-to-HCO+ flux ratios corrected for line opacity in
IRAS 20551−4250 will increase, further deviating fromstarbursts. (2) High-J to J=1–0 f lux ratios are higher
for HNC than HCN (Figure 3, left), which cannot be
explained by collisional excitation. Inclusion of infrared
radiative pumping, by putting an AGN at 30–100 pc frommolecular gas, can largely explain this result (Figure 3,
right). However, the infrared radiative pumping rate iscomparable for HCN and HCO+, so that this is not a main
mechanism to enhance the HCN-to-HCO+ flux ratios [1].

Reference[1] Imanishi, M., et al.: 2017, ApJ, 849, 29.

006

I Scientific Highlights

Figure 1: Flux ratios of HCN, HCO + , and HNC which probedense molecular gas. In IRAS 20551−4250, the HCN-toHCO+ flux ratios at multiple J-transitions (J=1–0, J=3–2,
J=4–3, and J=8–7) are higher than that of the starburst
galaxy NGC 1614 at J=3–2. For the J=3–2 and J=4–3
lines of IRAS 20551−4250, intrinsic flux ratios corrected
for line opacity are also plotted as open stars (connectedto the observed ratios by dotted lines).

Figure 2: Examples of ALMA spectra. HCN, HCO+, HNC J=1–0
and J=8–7 emission lines are clearly detected.

Figure 3: (Left): High-J to low-J flux ratios. High-J to J=1–0 flux
ratios are higher for HNC than HCN, which cannot be
explained by collisional excitation, based on criticaldensity comparison. (Right): Calculations of molecularline flux ratios in the case of (i) collisional excitation
only and (ii) inclusion of infrared radiative pumping by
putting an AGN at 30–100 pc from molecular gas. In
case (ii), the increase of the high-J to J=1–0 flux ratios
is higher for HNC than HCN, because the infrared
radiative pumping rate for HNC (by absorbing 21.5 μm
photons) is higher than that of HCN.

General Relativistic Radiation MHD Simulations ofSupercritical Accretion onto a Magnetized Neutron Star:
Modeling of Ultraluminous X-Ray Pulsars
TAKAHASHI, Hiroyuki, OHSUGA, Ken(NAOJ)

Gas accretion onto compact objects such as black
holes (BHs) or neutron stars (NSs) is known as one of
the most energetic phenomena in the universe. Thesesystems are powered by liberating the gravitationalenergy th rough mass accretion, so that the massaccretion rate is an important key parameter determining
their activities. In particular, the supercritical accretion,
where the accretion rate exceeds the critical rate M· crit(≡ LEdd /c2, LEdd and c are the Eddington luminosity andlight speed), is of interest since the large amount of gas
falls onto central objects. Such energetic phenomena arethought to happen around the black hole since the blackhole can swallow the gas and energy.
A recent finding of pulsations in ultraluminous
X-ray sources (ULXs) changes the situation. The
X-ray pulsation with a period of P = 1.37 s and its
time derivative P·  −2 × 10−10 s s−1 has been observed
from M82 X-2 [1]. After this notable discovery, X-ray
pulsations have been observed in other two ULXs [2,3].
These observational facts indicate that a supercriticalaccretion happens onto a NS (namely, ULX Pulsar), since
the luminosity of these ULX Pulsars highly exceeds the
Eddington luminosity for the neutron stars.
In this paper, we, for the first time, performed theGeneral Relativistic Radiation Magnetohydrodynamic(GR-RMHD) simulations of supercritical accretion
onto the strongly magnetized neutron star [4]. Figure 1
shows results of GR-RMHD simulations. NS is situatedat the origin. Far from the NS, a geometrically thick,supercritical accretion disk is formed. Close to the NS,
the accretion disk is truncated around r = 3R*, where R*= 10 km is the neutron star radius. Inside this radius, themagnetic energy of NS dominates. The gas accretion
is prohibited by the magnetic pressure. Alternatively,
the angular momentum of the disk gas is efficiently
transported to the NS due to the magnetic torque. Thenthe gas losing angular momentum falls on to the NS
along the magnetic field lines. The gravitational energy
is liberated by the collision of accreting gas with the
NS. Thus, the magnetic pole of NS shines brightly.
The angular momentum transport to the NS resultsin the spin up of NS. The estimated spin up rate inour simulation is about P· = −3 × 10 −11 s s−1, which isquantitatively consistent with the observed value. Thus,
our results support the scenario of supercritical accretion
onto the NS.

Figure 1: Supercritical accretion onto NS using GR-RMHD
simulations. Color shows mass density (left) andradiation energy density (right), and arrows show fluid
velocity (left) and radiation flux (right). Contours show
magnetic field lines.

References[1] Bachetti, M., et al.: 2014, Nature, 514, 202.
[2] Fürst, F., et al.: 2016, ApJL, 831, L14.
[3] Israel, G. L., et al.: 2017, Science, 355, 817.
[4] Takahashi, H. R., Ohsuga, K.: 2017, ApJL, 845, L9.

I Scientific Highlights

007

Cyanopolyyne Chemistry in High-Mass Star-Forming Regions
TANIGUCHI, Kotomi, SAITO, Masao(NAOJ)

Cyanopolyynes (HC2n+1N; n =1, 2, 3, ...) are one of
the representative carbon-chain series. In general, HC3N,
the shortest member of cyanopolyynes, is detectedfrom starless cores and star-forming cores, while longer
cyanopolyynes (i.e., HC5N and HC7N) are abundant instarless cores and deficient in star-forming cores.
The chemical composition around young stellar
objects (YSOs) is key to the initial chemical condition
and/or star formation processes. Figure 1 shows thechemical diversity around YSOs. In low-mass starforming regions, chemically two types have been found:
hot corino (complex organic molecules (COMs)-rich) andwarm carbon chain chemistry (WCCC; carbon-chainrich). The different starless core phases are considered
to be a factor to bring the difference between hot corino
and WCCC; long and short starless core phases lead hot
corino and WCCC, respectively [1]. In high-mass starforming regions, hot core sources, where COMs areabundant as well as hot corino, have been found, while
no counterpart of WCCC source has been confirmed.

cannot be detected if HC5N exists in cold molecular
clouds. Therefore, the detection of these lines means that
HC5N exists in the warm gas around MYSOs. We founda possibility of the chemical diversity among MYSOs;
G28.28−0.36 shows the highest HC 5N abundance
without a thermal CH3OH line observed with the GBT,
while G12.89+0.49 shows the lowest HC5N abundancewith a strong thermal CH 3OH emission line. From theresults, G28.28−0.36 seems to be a good candidate of acounterpart of WCCC source in high-mass star-forming
regions.
In low-mass star-forming regions, cyanopolyynes
are known to be good chemical evolutional indicators(e.g. [3]). On the other hand, the chemical evolution of
cyanopolyynes in high-mass star-forming regions was
not clear. We carried out survey observations of HC3N
and HC5N in the 45 GHz band toward 17 high-mass
starless cores (HMSCs) [4] and 35 high-mass protostellar
objects (HMPOs) [5] with the Nobeyama 45-m radio
telescope [6]. We have detected HC3N from 15 HMSCs
and 28 HMPOs, and HC 5N from 5 HMSCs and 14
HMPOs, respectively. From the Kolmogorov-Smirnov
test, the HC3N column density increases from HMSCs to
HMPOs, which may imply that HC3N is newly formed
at HMPO stage. In addition, the HC3N column density
tends to decrease with increasing the luminosity-tomass ratio, which is a physical evolutional indicator. Thissuggests that HC3N is destroyed by stellar activities (e.g.,
UV radiation).
Our studies are on-going projects. Current ourconclusion is that cyanopolyynes are good candidatesof chemical evolutionary indicators in high-mass starforming regions.

Figure 1: Chemical diversity around YSOs.

We carried out observations of long cyanopolyynes
toward four massive young stellar objects (MYSOs;
G10. 3 0 − 0.15, G12 . 8 9 + 0. 49, G16 . 8 6 −2 .16 , a n d
G28.28−0.36) associated with the 6.7 GHz CH 3 OH
masers with the Nobeyama 45-m radio telescope and theGreen Bank 100-m telescope (GBT) [2]. HC5N has been
detected from all of the four sources and HC7N has been
detected from the three sources except for G10.30−0.15
with the GBT. We also detected the high excitationenergy (E u /k ~ 100 K) lines of HC5N from the threesources, except for G10.30−0.15, with the Nobeyama
45-m radio telescope. Such high excitation energy lines008

I Scientific Highlights

References[1] Sakai, N., Yamamoto, S.: 2013, Chem. Rev., 113, 8981.
[2] Taniguchi, K., et al.: 2017, ApJ, 844, 68.
[3] Suzuki, H., et al.: 1992, ApJ, 392, 551.
[4] Sridharan, T. K., et al.: 2005, ApJL, 634, L57.
[5] Sridharan, T. K., et al.: 2002, ApJ, 566, 931.
[6] Taniguchi, K., et al.: 2018, ApJ, 854, 133.

Formation Mechanisms of Cyanopolyynes
in Low-Mass Starless CoresTANIGUCHI, Kotomi, SAITO, Masao(NAOJ)

Cyanopolyynes (HC2n+1N; n =1, 2, 3, ...) are one of
the representative carbon-chain species. Carbon-chain
molecules tend to be abundant in low-mass starlesscores and deficient in star-forming cores (e.g., [1]). It is
important for understanding of the physical conditions
and evolution in early low-mass starless cores to reveal
formation mechanisms of carbon-chain molecules.
However, the formation mechanisms of carbon-chain
species are unclear due to shor tage of laborator yexperimental data.
One method to investigate formation pathways ofcarbon-chain molecules is 13C isotopic fractionation, i.e.,
differences in abundance among the 13C isotopologues.
At the cyanopolyyne peak in Taurus Molecular Cloud-1(TMC-1 CP), the 13C isotopic fractionation of HC3N wasderived to be [H13CCCN] : [HC13CCN] : [HCC13CN]= 1.0:1.0:1.4, and the neutral-neutral reaction of “C2H 2+ CN” was proposed as the main formation pathway of
HC3N [2]. On the other hand, there is no clear differencein abundance among the five 13C isotopologues of HC5N.
From the results, the ion-molecule reactions of “C5H m++ N” followed by the electron recombination reactions
were proposed as the main formation mechanism of
HC5N at TMC-1 CP [3].
We car r ied out obser vations of the th ree 13 C
isotopologues of HC3N toward two low-mass starlesscores, L1521B and L134N, using the J = 5–4 rotationallines in the 45 GHz band with the Z45 receiver installedon the Nobeyama 45-m radio telescope [4]. T heabundance ratios of the three 13C isotopologues were
derived to be [H13CCCN] : [HC13CCN] : [HCC13CN]= 0.98 (±0.14) : 1.00 : 1.52 (±0.16) and 1.5 (±0.2) : 1.0 :
2.1 (±0.4) (1σ) in L1521B and L134N, respectively. Fromthe 13C isotopic fractionation patterns, the reactionsof “C 2 H 2 + CN” and “CCH + HNC” were proposedas the main formation pathways of HC3N in L1521B
and L134N, respectively. Figure 1 shows the summaryof the main formation pathways of HC3N in low-mass
starless cores. Although these three sources have similar
physical conditions (T ~ 10 K, n ~ 10 4 –10 5 cm−3), theproposed main formation pathway in L134N is different
from those in L1521B and TMC-1. We conducted achemical network simulation and found that the CN/
HNC abundance ratio may be a key factor to produce thedifference in the main formation mechanism of HC3N
among the three cold molecular clouds.
We reported the first detection of HC515N using theJ = 9–8 rotational line in the 20 GHz band from TMC-

Figure 1: Possible formation mechanisms of HC 3 N and the
proposed main formation pathways in three cold
molecular clouds. Expected 13C isotopic fractionation
patterns for each mechanism are shown in red font(discussed in [4] in detail).

1 CP with the Nobeyama 45-m radio telescope [5]. Its
column density was derived to be (1.9 ± 0.5) × 1011 cm−2(1σ). Applying the double isotope method, the 14N/15N
ratio of HC5N was calculated at 344 ± 53. Using theprevious data taken from [6] and [2], we estimated the
14N/15N ratio of HC N at 257 ± 54, which is lower than
3
that of HC5N. The difference in the 14N/15N ratio between
HC5N and HC3N is considered to be produced during
their formation. Since there are possible mechanismsthat 15N concentrates into CN in cold gas, the lower
ratio of HC3N implies that the main formation pathway
involves CN. The higher 14N/15N ratio of HC5N suggeststhat the main formation mechanism involves nitrogenatoms, because the 14N/15N ratio in the local interstellar
medium is ~440. In summary, the suggested main
formation mechanisms from 15N isotopic fractionation
are consistent with those suggested from 13C isotopic
fractionation [2,3].

References[1] Suzuki, H., et al.: 1992, ApJ, 392, 551.
[2] Takano, S., et al.: 1998, A&A, 329, 1156.
[3] Taniguchi, K., et al.: 2016, ApJ, 817, 147.
[4] Taniguchi, K., et al.: 2017, ApJ, 846, 46.
[5] Taniguchi, K., Saito, M.: 2017, PASJ, 69, L7.
[6] Kaifu, N., et al.: 2004, PASJ, 56, 69.

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Discovery of H2O Megamasers in Obscured Active Galactic Nuclei
YAMAUCHI, Aya1/2, MIYAMOTO, Yusuke2, NAKAI, Naomasa3, TERASHIMA, Yuichi4
OKUMURA, Taishi3, ZHOU, Bin3, TANIGUCHI, Kotomi2/5, KANEKO, Hiroyuki2
MATSUMOTO, Naoko2/6, SALAK, Dragan7, NISHIMURA, Atsushi8, UENO, Saeko9
1: JSPS, 2: NAOJ, 3: University of Tsukuba, 4: Ehime University, 5: SOKENDAI, 6: Yamaguchi University, 7: Kwansei Gakuin University, 8:
Nagoya University, 9: Kagoshima University

We carried out a survey of H 2 O maser emission
toward 10 obscured active galactic nuclei (AGNs). The
target galaxies were selected from obscured AGNs foundby Terashima et al. (2015) [1]. They developed a new
method to discover obscured AGNs by utilizing X-ray
and infrared data.
We made observations of H2O maser emission fromFebruary to June and December in 2016 using the 45-m
telescope of the Nobeyama Radio Observatory.
We newly detected maser features from two AGNs,
NGC 1402 and NGC 7738, with a signal-to-noise-ratio(SNR) of above 4, and tentatively detected in NGC 5037
(SNR >3). The isotropic maser luminosities of NGC 1402
and NGC 7738 are 47 L and 468 L, respectively; they
are megamasers (i.e., ≥ 10 L). On the other hand, theisotropic maser luminosity of NGC 5037 is 5 L, which isone order of magnitude smaller than typical luminositiesof megamasers.
NGC 7738 shows maser features redshifted andblueshifted from the systemic velocity of the galaxy(Figure 1). Weak features at VLSR ≈ 6573 km s −1 may
be systemic velocity features, although SNR is nothigh enough. Redshifted and blueshifted features are
symmetrical with respect to the possible systemic
features in velocity. Such symmetrical components are
typically seen as water-vapor masers in AGNs, indicating
a rotating edge-on disk (its inclination angle is ≈ 90°).
Thus the spectrum in NGC 7738 strongly suggests anedge-on maser disk rotating with velocity of ~ 350 km s−1(separation between the systemic and the other two
features).
NGC 1402 and NGC 7738 have an X-ray spectrum
that has a flat continuum and a strong Fe-K emissionline, indicating the presence of Compton-thick AGNs
in these objects. In the case of NGC 6926, classified as
an AGN of the same type by Terashima et al. (2015) [1],H 2 O maser emission has already been detected. This
type of AGNs may tend to have H2O maser emission.
Our detection rate of 20 % (2/10) is higher than thoseof previous surveys (usually several percent). This highdetection rate indicates that the selection method iseffective.

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I Scientific Highlights

Figure 1: Yamauchi et al. (2017) [2]. The H2O maser spectra of
AGNs (marginally) detected with the 45-m telescope. To
make the graph easier to view, the spectra with velocity
resolution of 1 km s−1 are plotted 100 mJy above. Verticaland horizontal lines in the spectra indicate the systemic
velocities of the galaxies and those errors, respectively.

References[1] Terashima, Y., et al.: 2015, ApJ, 814, 11.
[2] Yamauchi, A., et al.: 2017, PASJ, 69, L6.

Evidence for Higher Black Hole Spin in Radio-loud Quasars
SCHULZE, Andreas1, DONE, Chris2, LU, Youjun3/4, ZHANG, Fupeng5, INOUE, Yoshiyuki6
1: NAOJ, 2: University of Durham, 3: National Astronomical Observatories, Chinese Academy of Sciences, 4: University of Chinese Academy of
Sciences, 5: Sun Yat-Sen University, 6: Institute of Space and Astronautical Science JAXA

black hole spin paradigm [2].
100
80

60

Rcrit = 10

50

N

N

30
20

20
0
0.0

Rcrit = 80

40

60
40

10
0.5

1.0

1.5

log EWOIII

2.0

2.5

0
0.0

0.5

1.0

1.5

log EWOIII

2.0

2.5

Figure 1: Histogram of [O III ] equivalent width for the radioloud quasar sample (solid red lines) and the matchedradio-quiet sample (dashed blue lines), in the left panel
for defining radio-loud quasars by a radio loudness
parameter R > 10 and in the right panel using a moreconservative threshold R> 80.

flux fλ

1.2

NeV

NeIII

OII

OIII

1.1

1.0

0.9
5

flux fλOne of the major unsolved questions on theunderstanding of the AGN population is the origin of the
dichotomy between radio-quiet and radio-loud quasars,
i.e. why does the majority of AGN feature only weak core
radio emission, while about 10 % of them have powerfulrelativistic jets with high bulk Lorentz factor. The mostpromising explanation is provided by the spin paradigm,
which suggests radio-loud quasars have higher blackhole spin. However, the measurement of black hole spin
remains extremely challenging.
To address this question, we proposed a novel
approach to probe the mean radiative efficiencies ofboth populations as direct tracers of black hole spin. For
this goal, we used a large well-defined statistical quasar
sample drawn from SDSS [1] at 0.3 < z < 0.8, separated
into radio-loud and radio-quiet quasars. A radio loudquasar is here defined by their radio-to-optical flux
density ratio R either above 10 (or above 80). We used
the [O III] luminosity as an indirect average tracer of theionizing continuum in the extreme-UV regime where
differences in the SED due to black hole spin are mostpronounced. We found that the radio-loud sample showsan enhancement in [O III] line strength by a factor ofat least 1.5 compared to a radio-quiet sample matchedin redshift, black hole mass and optical continuum
luminosity L5100 or accretion rate (see Fig. 1).
We do not see evidence that the observed trend isdriven by star formation or jet-driven outflows (see e.g.
Fig. 2). A remaining uncertainty we cannot fully resolve
given current observations lies in our assumption ofsimilar average NLR structures between radio-loudand radio-quiet quasars. However, we find a similar
enhancement in both narrow and broad high ionizationlines (in particular broad He II λ4686) which suggests that
our result is not driven by NLR physics.
We argue that the most plausible explanation forthe observed [O III] equivalent width enhancement is an
intrinsic difference in ionizing continuum, thus in SED,
meaning higher average bolometric luminosities at fixedaccretion rate in the radio-loud population. This suggeststhat the radio-loud quasar population has on averagesystematically larger radiative efficiencies and therefore
higher black hole spin than the radio-quiet population.
Assuming a standard average radiative efficiency of 0.1
for radio-quiet quasars (a = 0.67), radio-loud quasars
would have an efficiency of 0.15 and thus a = 0.89, which
is high but not yet close to maximum spin.
Our results provide new observational support for the

4
3
2
1
3000

4000

5000

rest wavelength λ [Å]

6000

Figure 2: Composite spectra of the radio-loud (red) and matchedradio-quiet (blue) quasar sample, where the composite
spectra are normalized at 5100 Å, for the full spectrum(lower panel) and several prominent narrow highionization lines (upper panels).

References[1] Shen, Y., et al.: 2011, ApJS, 194, 45.
[2] Schulze, A., et al.: 2017, ApJ, 849, 4.

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Rotating Starburst Cores in Massive Galaxies at z = 2.5
TADAKI, Ken-ichi1/2, KODAMA, Tadayuki2/3, NELSON, Erica J.1, BELLI, Sirio1
FÖRSTER SCHREIBER, Natascha M.1, GENZEL, Reinhard1/4/5, HAYASHI, Masao2
HERRERA-CAMPUS, Rodrigo1, KOYAMS, Yusei2, LANG, Philipp6, LUTZ, Dieter1
SHIMAKAWA, Rhythm3, TACCONI, Linda J.1, ÜBLER, Hannah1, WISNIOSKI, Emily1, WUYTS, Stijn7
HATSUKADE, Bunyo8, LIPPA, Magdalena1, NAKANISHI, Kouichiro2/3, IKARASHI, Soh9
KOHNO, Kotaro8/10, SUZUKI, Tomoko L.3, TAMURA, Yoichi8, TANAKA, Ichi2
1: Max-Planck-Institut für extraterrestrische Physik, 2: NAOJ, 3: Department of Astronomical Science, SOKENDAI (The Graduate University
for Advanced Studies), 4: Department of Physics, Le Conte Hall, University of California, 5: Department of Astronomy, Hearst Field Annex,
University of California, 6: Max-Planck-Institut für Astronomie, 7: Department of Physics, University of Bath, 8: Institute of Astronomy, The
University of Tokyo, 9: Kapteyn Astronomical Institute, University of Groningen, 10: Research Center for the Early Universe, The University ofTokyo

Velocity [km s-1 ]

+500

Data

Model

0
-250

U4-16795

+500
+250
0
-250
-500

U4-16504-0.6

0+0.6 -0.6

0I Scientific Highlights+0.6 -0.6

Positional offset [arcsec]

0

+0.6

Figure 1: Observed position-velocity diagrams of the CO spectra(left). The middle and right panels show the best-fit
dynamical model and the residuals between the data andthe model, respectively.

Reference[1] Tadaki, K. et al.: 2017, ApJ, 841, L25.

012

Residual

+250

-500

Velocity [km s-1 ]We present spatially resolved ALMA observations of
the CO J = 3–2 emission line in two massive galaxies at
z = 2.5 on the star-forming main sequence. Both galaxies
have compact dusty star-forming cores with effective radiiof Re = 1.3 ± 0.1 kpc and Re = 1.2 ± 0.1 kpc in the 870 μm
continuum emission. The spatial extent of star-forming
molecular gas is also compact with R e = 1.9 ± 0.4 kpc
and Re = 2.3 ± 0.4 kpc, but more extended than the dust
emission. Interpreting the observed position-velocity
diagrams with dynamical models, we find the starburst
cores to be rotation-dominated with the ratio of the
maximum rotation velocity to the local velocity dispersion+36−1of vmax/σ0 = 7.0 +2.5
−2.8 (v max=386 −32 km s ) and v max/σ 0 =+1.7+54
4.1 −1.5 (vmax = 391 −41 km s−1). Given that the descendantsof these massive galaxies in the local universe are likely
ellipticals with v/σ nearly an order of magnitude lower,
the rapidly rotating galaxies would lose significant
net angular momentum in the intervening time. The
comparisons among dynamical, stellar, gas, and dust masssuggest that the starburst CO-to-H2 conversion factorof αCO = 0.8 M (K km s−1 pc−2) s−1 is appropriate in thespatially resolved cores. The dense cores are likely to beformed in extreme environments similar to the central
regions of local ultraluminous infrared galaxies. Our
work also demonstrates that a combination of mediumresolution CO and high-resolution dust continuum
observations is a powerful tool for characterizing the
dynamical state of molecular gas in distant galaxies.

First ALMA Observation of a Solar Plasmoid Ejection
from an X-ray Bright PointSHIMOJO, Masumi1/2, HUDSON, Hugh S.3/4, WHITE, Stephen M.5, BASTIAN, Timothy S.6, IWAI, Kazumasa7
1: NAOJ, 2: SOKENDAI, 3: University of Glasgow, 4: UCB, 5: AFRL, 6: NRAO, 7: Nagoya University

Y (arcsecs)

220

200

Y (arcsecs)

240

220

200

Y (arcsecs)

240

220

⇒

Reference[1] Shimojo, M., et al.: 2017, ApJ, 841, L5.

240⇒

Eruptive phenomena such as plasmoid ejections orjets are important features of solar activity and have thepotential to improve our understanding of the dynamics ofthe solar atmosphere. Such ejections are often thought tobe signatures of the outflows expected in regions of fastmagnetic reconnection. The 304 Å EUV line of helium,
formed at around 105 K, is found to be a reliable tracerof such phenomena, but the determination of physicalparameters from such observations is not straightforward.
We have observed a plasmoid ejection from an X-ray
bright point simultaneously at millimeter wavelengths
with ALMA, at EUV wavelengths with SDO/AIA, andin soft X-rays with Hinode/XRT. This paper reports
the physical parameters of the plasmoid obtained by
combining the radio, EUV, and X-ray data. We consider
three basic working hypotheses to consider. (1) The
plasmoid consists of (roughly) isothermal plasma thatis optically thick at 100 GHz. (2) The plasmoid consistsof isothermal plasma that is optically thin at 100 GHz.
(3) The plasmoid consists of multi-thermal plasma. As aresult, we conclude that the plasmoid can consist eitherof (approximately) isothermal ~10 5 K plasma that is
optically thin at 100 GHz, or a ~104 K core with a hot
envelope.
This analysis demonstrates the value of the additionaltemperature and density constraints that ALMA canprovide. In addition, at higher frequencies the spatial
resolution of ALMA is close to that achieved with spaceborne telescopes such as AIA, providing the ability
to spatially resolve the same features at very different
wavelengths, and providing complementary physicalinformation.

200

-260

-240
X (arcsecs)

-220

-200

Figure 1: The leading sunspot of active region NOAA12470
observed with ALMA at Band 3 (100 GHz, upper panel),in ultraviolet continuum from the lower chromosphere(AIA1700, middle panel), and the He II transition-regionline (AIA304, lower panel). The white arrows indicate
an erupted plasmoid.

I Scientific Highlights

013

Variation of Solar Microwave Spectrum in the Last Half Century
SHIMOJO, Masumi1/2, IWAI, Kazumasa3, ASAI, Ayumi4, NOZAWA, Satoshi5
MINAMIDANI, Tetsuhiro1/2, SAITO, Masao1/2
1: NAOJ, 2: SOKENDAI, 3: Nagoya University, 4: Kyoto University, 5: Ibaraki University

Flux & MSD (SFU) / Sunspot Num.

Figure 1: Left: Photos of the antennas at Toyokawa 1957, andNobeyama 2017. Upper Right: Long-term variationof microwave and sunspot number. Lower Right: The
microwave spectra at the solar minima.

Sunspot Num. / AMSD (SFU)

The total solar flux in microwaves, particularly theF10.7 index (total solar flux at 2.8 GHz), is widely used as
an indicator of solar activity in the fields of heliophysics
and geophysics, because the F10.7 index indicatesthe variation of solar UV emission in comparison tosunspot number. The time variation in microwaves is
traditionally classified into three components based on
the timescale of enhancements. The components are abackground component from the quiet-Sun, a slowly
varying component, and a sporadic (burst) component.
The background component is considered to originate
from optically thick thermal bremsstrahlung emission
from the atmosphere above the upper chromosphere, andthe slowly varying component originates in the thermal
bremsstrahlung emission of coronal loops above active
regions and thermal gyro-resonance emission from strong
magnetic field regions, such as sunspots.
In Japan, continuous four-frequency solar microwave
observations (1, 2, 3.75 and 9.4 GHz) began in 1957
at the Toyokawa Branch of the Research Institute ofAtmospherics, Nagoya University. In 1994 the telescopes
were relocated to NAOJ Nobeyama Campus, where
they have continued observations up to the present. We
analyzed the more than 60 years of solar microwave datafrom these telescopes. At first, we determined the monththat solar activity is most minimum in each solar cycle
using the standard deviation of the flux density of thesolar microwave. Then, we investigate the microwave
spectra of the months, and found that microwave
intensities and spectra at the minimums of the latest fivecycles were the same every time. In contrast, during theperiods of maximum solar activity, both the intensity andspectrum varied from cycle to cycle.
These results show that the average atmosphericstructure above the upper chromosphere in the quietSun has not varied for half a century, and suggest thatthe energy input for atmospheric heating from the subphotosphere to the corona have not changed in the quietSun despite significantly differing strengths of magnetic
activity in the last five solar cycles.

Monthly Mean Flux, Monthly Standard Deviation(MSD), Montly Mean Total Sunspot Number

1000.0

100.0
10.0
1.0
0.1

1000.0

50

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89

I Scientific Highlights

15

100.0
10.0
1.0
0.1

50

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76

89

02

15

Figure 2: Upper panel: The monthly mean microwave fluxes, themonthly mean total sunspot number (solid lines), andthe monthly standard deviations (MSD: asterisk). Lower
Panel: The black asterisks indicate the monthly mean
total sunspot number, and the red line is the 13-monthsmoothed monthly total sunspot number. The green
asterisks indicate the Averaged MSD, and the blue lineis the 13-month smoothed AMSD.

Reference[1] Shimojo, M., et al.: 2017, ApJ, 848, 62.

014

02

Monthly Mean Total Sunspot Number, Averaged Monthly Standard Deviation(AMSD)

Joint Strong and Weak Lensing Analysisof the Massive Cluster Field J0850+3604
WONG, Kenneth C.1, RANEY, Catie2, KEETON, Charles R.2, UMETSU, Keiichi3
ZABLUDOFF, Ann I.4, AMMONS, S. Mark5, FRENCH, K. Decker4
1: NAOJ, 2: Rutgers University, 3: ASIAA, 4: Arizona University, 5: Lawrence Livermore National Laboratory

Gravitational lensing by massive galaxy clusters
is a powerful tool to study faint high-redshift galaxies
through lensing magnification. Many orbits of Hubble
Space Telescope (HST) time have been dedicated tocharacterizing such clusters and using them to search forlensed z ≥ 7 galaxies and determine their contribution
to the reionization of the intergalactic medium. The
HST Frontier Fields program [1] has imaged six of themost massive and well-studied lensing clusters for thispurpose. However, cosmic variance is a large source of
uncertainty, and exploring new lines of sight for use ascosmic telescopes will be key to addressing this as wemove into the era of the James Webb Space Telescope(JWST).
Several such fields were identified [2] in the Sloan
Digital Sky Survey (SDSS) based on their large integrated
luminosity density in luminous red galaxies (LRGs),
which are tracers of massive structure. Spectroscopic
follow-up of a subset of these fields reveal massive
structures with large total integrated masses [3]. Oneof these fields, J085007.6+360428 (hereafter J0850),
has archival multi-band imaging from Subaru/SuprimeCam, which shows a multiply-imaged lensed arc witha photometric redshift of z ≈ 5. Spectroscopy of themassive cluster at z =0.38 indicates a dynamical mass of~3 × 1015 M.
Using the Suprime-Cam imaging, we perform a joint
weak and strong lensing analysis of J0850 to constrain
the mass distribution and magnification properties ofthis field. We use a color-color selection to identify
background galaxies, which we use to measure thereduced shear induced by the foreground cluster. We
parameterize the cluster as an elliptical NFW [4] profileand fit it to the shear data. The posterior distributions of
the halo parameters are then used as inputs for a forward
model that reconstructs the multiply-imaged z ≈ 5 galaxy.
This model includes line-of-sight structure, including aforeground group halo identified in the spectroscopy. The
models that reproduce the surface brightness distributionof the arclets are used as our final posterior distribution.
We use the surface brightness distribution of the multiple
images as constraints since this reveals that one of theimages is a rare “fold arc”, a highly-magnified image
that lies across a lensing critical curve, and that would
not be reproduced if only the image positions were used.
Portions of this arc can be magnified by over a factor of
1000, making it promising for high-resolution imaging tostudy features at scales of ≤ 30 pc.
15 M for theWe find a virial mass of 2.93 +0.71
−0.65 × 10
cluster. The concentration is typical of halos of similar
mass and redshift, indicating that there is no bias toward
high concentration as is sometimes seen in lensingselected samples. The cluster has a large ellipticity of
ε = 0.53 +0.09−0.10 , suggesting that it is an efficient lens (i.e. ahigh density of multiple images) [5]. The full results arepresented in [6]. The high mass of this cluster makes it
ideal for future studies of high-z galaxies.

Figure 1: Magnification map for the best mass model of the J0850
field for a source redshift of zS = 5.03, based on our
combined lensing analysis. The region shown is 6′ × 6′.

References[1] Negrello, M., et al.: 2010, Science, 330, 800.
[2] Ealges, S., et al.: 2010, PASP, 122, 499.
[3] Bussmann, R. S., et al.: 2013, ApJ, 779, 25.
[4] Wong, K. C., et al.: 2017, ApJL, 843, L35.
[5] Suyu, S. H., Halkola, A.: 2010, A&A, 524, A94.
[6] Tamura, Y., et al.: 2015, PASJ, 67, 72.
[7] Wong, K. C., et al.: 2015, ApJ, 811, 115.

I Scientific Highlights

015

ALMA Observations of the Gravitational Lens SDP.9
WONG, Kenneth C.1, ISHIDA, Tsuyoshi2, TAMURA, Yoichi3, SUYU, Sherry H.4/5/6
OGURI, Masamune2/7, MATSUSHITA, Satoki6
1: NAOJ, 2: University of Tokyo, 3: Nagoya University, 4: MPA, 5: TUM, 6: ASIAA, 7: IPMU016

I Scientific Highlights

profile slope, and a projected axis ratio of b/a = 0.68 +0.05−0.04.
The lensed image configuration is strikingly different
between the HST and ALMA data. The HST data, whichprobe the rest-frame optical emission from the source,
show a much more symmetric configuration, while the
ALMA submillimeter data has the large bright southernarc and the much smaller northern arc. This difference
suggests a spatial offset between the stellar component
and the gas and dust component of the source galaxy, as
has been seen in other lensed submillimeter galaxies atthis redshift.
Intensity [mJy/beam]
0.00
0.10
0.20

Integrated Intensity [Jy/beam km/s]
0.00
0.10
0.20

40.06
40.02
9:07:39.98
Right Ascention (J2000) [hms]

40.06
40.02
9:07:39.98
Right Ascention (J2000) [hms]-150

Velocity [km/s]
-50
50

150

-0:41:59.0
Declination (J2000) [dms]Recent surveys at submillimeter wavelengths haverevealed a population of gravitationally lensed dusty
star-forming galaxies at z ~ 2–7 [1]. By combining thehigh sensitivity and spatial resolution of the Atacama
Large Millimeter/Submillimeter Array (ALMA) with thenatural magnification of gravitational lensing, the detailed
properties of these galaxies can be studied on spatial
scales of tens to hundreds of parsecs. One such systemis the gravitational lens H-ATLAS J090740.0–004200(hereafter SDP.9). SDP.9 was first identified as one of
the brightest sources in the Science Demonstration Phase(SDP) of the Herschel Astrophysical Terahertz Large
Area Survey (H-ATLAS) [2], and consists of a massive
early-type galaxy at zL = 0.6129 [3] lensing a backgroundsubmillimeter galaxy at zS = 1.5747 into a bright arc andsmall counterimage.
ALMA data on SDP.9 were obtained during Cycle 3(Program 2015.1.00415.S; PI: K. Wong) [4]. The Band 6
continuum was observed, as well as the CO J= 6–5 line.
During the observations, 49 12 m antennas were used,
and baselines ranged from 84.7 m to 16.2 km with the
C36-7 configuration. The total on-source time was 4526 sunder stable weather conditions with precipitable water
vapors ~0.50 mm.
We find that the source is split into two tangentiallyelongated arcs, as is suggested by previous SMA
observations. The northern arc is less extended than thesouthern arc, and some clumpy structures are visible inboth arcs. We measure the peak intensity and total flux
density of each arc in both the continuum and CO maps.
Taking the CO line flux integrated across both arcs ineach velocity bin, we measure an updated source redshift
of zS = 1.5747 ± 0.0002.
We fin d n o clear emis s io n f r o m th e cen traldemagnified image of the lens in the velocity-integrated
CO(6–5) map down to a 3σ rms level of 0.0471 Jy km s−1.
The central image, which is predicted for non-singularmass distributions, offers a unique probe of the innermost
central mass distribution of the lens [5,6], but we areunable to place meaningful constraints for this system.
We model the lens system using constraints from the
ALMA imaging and archival Hubble Space Telescope(HST) imaging with the lens-modeling software G LEE[7]. The velocity gradient in the source galaxy is nearly
orthogonal to the elongation of the lensed arcs, making
a robust identification of multiple-image pair regions
challenging. We find an Einstein radius of θ E = 0.66
± 0.01 arcsec, a slightly steeper than isothermal mass

59.5

42:00.0

00.5
40.06
40.02
9:07:39.98
Right Ascention (J2000) [hms]Figure 1: Left: ALMA Band 6 continuum image with Briggs
weighting and no tapering. Center: velocity-integrated
CO(6–5) intensity map. The black lines indicate theregions used to measure the integrated flux of the arcs.
Right: CO(6–5) velocity map. Small symbols represent
the conjugate points used for our mass modeling, withsymbols of the same shape representing image pairs.

References[1] Negrello, M., et al.: 2010, Science, 330, 800.
[2] Ealges, S., et al.: 2010, PASP, 122, 499.
[3] Bussmann, R. S., et al.: 2013, ApJ, 779, 25.
[4] Wong, K. C., et al.: 2017, ApJL, 843, L35.
[5] Tamura, Y., et al.: 2015, PASJ, 67, 72.
[6] Wong, K. C., et al.: 2015, ApJ, 811, 115.
[7] Suyu, S. H., Halkola, A.: 2010, A&A, 524, A94.

Near-infrared Spectroscopic Observationsof Comet C/2013 R1 (Lovejoy) by WINERED:CN Red-system Band Emission
SHINNAKA, Y.1/2, KAWAKITA, H.2/3, KONDO, S.2/3, IKEDA, Y.2/4, KOBAYASHI, N.2/5/6, HAMANO, S.2
SAMESHIMA, H.2, FUKUE, K.2, MATSUNAGA, N.2/7, YASUI, C.1/2, IZUMI, N.1/2, MIZUMOTO, M.5/7
OTSUBO, S.2/3, TAKENAKA, K.2/3, WATASE, A.2/3, KAWANISHI, T.2/3, NAKANISHI, K.2, NAKAOKA, T.2/3
1: NAOJ, 2: Koyama Astronomical Observatory, 3: Kyoto Sangyo University, 4: Photocoding, 5: University of Tokyo, 6: Kiso Observatory, 7:
ISAS

80
The pure fluorescence
excitation model of 12C14N

70
Relative intensity [arbit. units]

Recently nitrogen isotopic ratios ( 14N/ 15N ratios)in various astrophysical objects have been investigatedby both observational and theoretical studies. From theviewpoint of chemical evolution in molecular cloud andproto-planetary disk, the high 15N-fractionation foundin those environments together with comets in the Solar
System is quite puzzling. Any chemical evolution models
cannot explain the observed high 15N-fractionation ofmolecules in solid-phase quantitatively, so far.
In the case of CN radical of comets, CN B-X
violet band at ~388 nm has been observed (e.g., [1]).
Observational conditions are often not good for a cometwhich becomes brighter as it approaches the Sun because
this band (which is close to UV region) is significantly
affected by telluric extinction. In addition, S/Nratios of CN emission spectra would be worth because of
the extinction by dust grains in cometary coma.
Here we report high-resolution near-infrared spectraof CN red-system band (A-X) at ~1.1 μm [2]. The redsystem band is not severely affected by the telluric
extinction compared to the violet-system band. We
developed the fluorescence excitation model for CN bysolar radiation based on modern spectroscopic studies. We
applied the fluorescence excitation models for CN to theobserved CN spectra of comet C/2013 R1 (Lovejoy). The
spectra were taken by the near-infrared high-resolution
spectrograph WINERED mounted on the 1.3-m Araki
telescope at the Koyama Astronomical Observatory,
Kyoto, Japan on 30 November 2013. Our emission model
could reproduce the observed CN red-system band of thecomet with a linear combination of a pure fluorescence
excitation model for the outer coma region and a fully
collisional fluorescence excitation model for the innercoma region (see Figure 1). The observed spectrum isconsistent within error-bars with the previous estimates ofisotopic ratios in comets; 12C/13C of ~90 [1] and 14N/15N
of ~150 [1,3].
This study was financially supported by JSPS grants(16684001, 20340042, 21840052, 26287028, 13J10504,
15J10864, 16K17669, 16H07323), MEXT Supported
Program for the Strategic Research Foundation at Private
Universities (S0801061, S1411028) and the Japan-India
Science Cooperative Program 2013-2015 and 2016-2018.

60
The fully collisional fluorescence
excitation model of 12C14N(T = 282 K)

50
40

The combination model of 12C14N(Mixing ratio = 0.94 : 0.06)

30
20

Observed spectrum

10
0
10900

10950
11000
11050
Wavelength in vacuum [Å]11100

Figure 1: Comparison between synthesized and observed spectraof comet Lovejoy in the CN red-system (0-0) band [2].
The top three spectra are the synthesized spectrum of
12C14N based on the pure fluorescence excitation model(red), the fully collisional fluorescence excitation modelwith Trot of 282 K (green), and the synthesized spectrumof 12C14N as a linear combination of the fully collisional
fluorescence excitation model and the pure fluorescence
excitation model with a mixing ratio of 0.94:0.06 (blue)
for the observed conditions of comet Lovejoy. The
bottom spectrum (black) is observed emission spectra ofcomet Lovejoy. The gray vertical bars correspond to theregions of OH sky emission lines.

References[1] Manfroid, J., et al.: 2009, A&A, 503, 613-624.
[2] Shinnaka, Y., et al.: 2017, AJ, 154, 45.
[3] Shinnaka, Y., et al.: 2016, MNRAS, 462, S195-S209.

I Scientific Highlights

017

Suzaku Observations of Heavily Obscured (Compton-thick)
Active Galactic Nuclei Selected by Swift/BAT Hard X-Ray Survey
TANIMOTO, Atsushi, UEDA, Yoshihiro

				(Kyoto University)

RICCI, Claudio

KAWAMURO, Taiki(NAOJ)

AWAKI, Hisamitsu, TERASHIMA, Yuichi(Ponticia Universidad Catolica de Chile)		

To reveal the nature of Compton-thick Active Galactic
Nuclei (CTAGNs: log NH/cm−2 ≥ 24) is an important,
yet unresolved issue in modern astronomy. CTAGNs are
key objects to understand the origin of the co-evolutionof Supermassive Black Holes (SMBHs) and their hostgalaxies. According to a galaxy/SMBH evolutionary
scenario, major mergers trigger violent star formation
and rapid growth of SMBHs heavily obscured by gas anddust. This leads to the idea that some CTAGNs may be
distinct populations from less obscured AGNs. However,it remains an open question whether CTAGNs are
intrinsically same objects or not as the rest of AGNs due
to observational difficulties in detecting CTAGNs.
We present a uniform broadband X-ray (0.5–100.0keV) spectral analysis of 12 Swift/BAT selected CTAGNs
observed with Suzaku. We fitted these spectra with theMonte Carlo based AGN torus model [1] (Figure 1). The
main results are as follows. (1) Unabsorbed reflection
components are commonly observed, suggesting thatthe tori are clumpy. (2) Almost CTAGNs show small
scattering fractions implying a buried AGN nature(Figure 2). (3) Comparison with the results obtained
for Compton-thin AGNs [2] (Figure 3) suggests thatthe properties of these CTAGNs can be understood as asmooth extension from Compton-thin AGNs with heavier
obscuration [3].

(Ehime University)

Figure 2: Correlation between hydrogen column density andscattering fraction.

(data−model)/error

keV2 (Photons cm −2 s−1 keV−1)

1

Mrk 3

0.1

Figure 3: Correlation between the X-ray and infrared luminosities.

0.01
10−3
10−4

References[1] Ikeda, S., Awaki, H., Terashima, Y.: 2009, ApJ, 692, 608.
[2] Kawamuro, T., et al.: 2016, ApJS, 225, 14.
[3] Tanimoto, A., et al.: 2018, ApJ, 853, 146.

10−5
5
0
−5
1

10
Energy (keV)

Figure 1: Broadband X-ray spectra. Black and Red: Suzaku/XIS.
Green: Suzaku/PIN. Blue: Swift/BAT.

018

I Scientific Highlights

Superluminous Transients at AGN Centers from Interaction
between Black Hole Disk Winds and Broad-line Region Clouds(NAOJ)		

TANAKA, Masaomi(Tohoku University)

We propose that superluminous transients that appear
at central regions of active galactic nuclei (AGNs) such as
CSS100217:102913+404220 (CSS100217) and PS16dtm,
which reach near or super-Eddington luminosities of
the central black holes, are powered by the interaction
between accretion disk winds and clouds in broad-line
regions (BLRs) surrounding them. Such transients havebeen suggested to be a kind of supernova (SN) explosions
because of their similarities to Type IIn SNe. However,similar transients preferentially appear in AGN central
regions with similar properties. This fact has motivated us
to consider a possibility that these transients are related to
AGN activities rather than SNe.
If the black hole accretion disk luminosity temporary
increases by, e.g., limit-cycle oscillations, leading to a
powerful radiatively driven wind, strong shock waves
propagate in the BLR. Because the dense clouds in the
AGN BLRs typically have similar densities to thosefound in Type IIn SNe, strong radiative shocks emerge
and efficiently convert the ejecta kinetic energy toradiation. As a result, transients similar to Type IIn
supernovae can be observed at AGN central regions.
Since a typical black-hole disk wind velocity is  0.1c
where c is the speed of light, the ejecta kinetic energy is
expected to be  1052 erg when  1 M is ejected. This
kinetic energy is transformed to radiation energy in atimescale for the wind to sweep up a similar mass to itself
in the BLR, which is a few hundred days. Therefore, bothluminosities (~1044 erg s−1) and timescales (~100 days) of
the superluminous transients from AGN central regions
match to those expected in our interaction model. Figure 1
shows a schematic picture of our model to explain the
superluminous transients from AGN activities.
If the superluminous transients from AGN centers
are related to the AGN activities triggered by limitcycle oscillations, we expect that the luminosity of thesuperluminous transients are correlated with the AGN
central BH mass as demonstrated in Figure 2. Also, thelimit-cycle oscillation repeats in the timescale of decades
so the superluminous transients should become bright
repeated in the timescale decades or so.

MOROKUMA, Tomoki(University of Tokyo)		

OHSUGA, Ken(Tsukuba University)

Figure 1: Schematic picture of our BH disk wind model. If the
BH
BH accretion disk ejects a wind with M BH
ej and v ej , it isdecelerated by the dense clouds in the BLRs (red dots)
and its kinetic energy is efficiently converted to radiation
[1].

-30
quasar-28
λL5100 continuum (mag)

MORIYA, Takashi

NLS1

-26
-24

2/3

STACs at peak ∝ MBH

host AGNs ∝ MBH

-22
-20
-18

CSS100217
PS16dtm
678log MBH

910

Figure 2: Luminosity estimates of the superluminous transientsfrom AGN centers (STACs) by the BH disk wind modeland their host AGNs [1].

Reference[1] Moriya, T. J., et al.: 2017, ApJL, 843, L19.

I Scientific Highlights019

On the Macroturbulence Model for the Solar Photospheric Velocity Field

the turbulent velocity dispersion by a factor of ~2. The
classical Gaussian macroturbulence model should be
more reasonable in this respect. See [1] for more detailsof this study.
4(R=1, T=1)

3

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Vlos (km s )I Scientific Highlights

4
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30

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30

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Figure 2: Theoretical Vlos vs. θ diagram corresponding to RTM(solid line) and GM (dashed line).
5

5
weak lines-1

Vlos (km s )

4

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4
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saturated lines

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5
Vlos (km s )With an aim to check whether this RTM model
adequately represents the actual solar photosphericvelocity field, we carried out an extensive study on
the non-thermal velocity dispersion along the line-ofsight (Vlos) at various points of the solar disk based on
locally-averaged spectra obtained by the Domeless Solar
Telescope at Hida Observatory. By comparing two kindsof theoretical Vlos vs. θ relations (θ is the angle between
the surface normal and the line of sight; i.e., θ = 0° at thedisk center and θ = 90° at the limb) predicted from the
RTM model and the Gaussian macroturbulence (GM)model (Figure 2) with the observed trend (Figure 3), thefollowing conclusion was drawn: The center-to-limb runof Vlos is simply monotonic with a slightly increasing
tendency with θ, which contradicts the specific trend (anappreciable peak at θ ~ 45°) predicted from RTM. Thismeans that RTM is not an adequate model at least forsolar-type stars, which would significantly overestimate

3

2

3

Figure 1: Schematic description of the concept of radial–tangential
macroturbulence, which explains why the width of thebroadening function is considerably smaller than theactual velocity dispersion.

4-1

In incorporating the effect of atmospheric turbulencein the broadening of spectral lines, the so-called radialtangential macroturbulence (RTM) model has been
widely used for solar-type stars, which was devised froman intuitive appearance of granular velocity field of theSun. Since this model assumes that turbulent motions are
restricted to only radial and tangential directions, it hasa special broadening function with notably narrow width
due to the projection effect (cf. Figure 1), the validity ofwhich has not yet been confirmed in practice.

UENO, Satoru(Hida Observatory of Kyoto University)

Vlos (km s )(NAOJ)-1

TAKEDA, Yoichi

Vlos (km s )

				

80

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40 60
θ (deg)80

Figure 3: Observed Vlos vs. θ diagram for each of the line-strengthclasses.
Reference[1] Takeda, Y., UeNo, S.: 2017, PASJ, 69, 46.

Testing the Planet-Engulfment Hypothesis as the Origin of Li-rich Giants
TAKEDA, Yoichi, TAJITSU, Akito(NAOJ)

HD 174104

unlikely as the origin of Li-rich giants (at least as the
major mechanism),
See [2] for more details of this study.
4 (a)A 6104(Li)

4

(b)

3

N

3

N

A 6104(Li)It is known that a small fraction (~1 %) of red
giant stars show unusually strong Li line (indicative ofconsiderably large Li abundance in the photosphere), in
marked contrast to normal red giants mostly showing
significant depletion of surface Li because of the dilution
due to evolution-induced envelope mixing. One of thevarious mechanisms proposed so far to explain this Lienhancement is the accretion/swallowing of substellar
companion (planets or brown dwarfs) by the red giant star(see [1] and the references therein). This hypothesis canbe tested by spectroscopically checking 6Li or Be, which
are expected to exist in such cool low-mass companions.
That is, if this is the case, we may as well detect 6Li and/or overabundance of Be.

2

2

6

N(Li6)/N(Li7) = 0.1

1
1

2

3
N
A 6708(Li)7N(Li )/N(Li ) = 0.0

1
1

4

2

3
N
A 6708(Li)4Figure 2: Effect of 6Li/7Li ratio on the A N6104 (Li) vs. A N6708 (Li)correlation.

HD 21018
HD 203136(a)

HD 232862
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HD 203136

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Normalized flux

HD 167304
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(a)

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Ti

Li

Fe

(b)

6706
6708
6710 6100
Wavelength (Å)

Fe

Ti

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6102
6104
Wavelength (Å)

Figure 1: Synthetic spectrum fitting for Li abundance determination.

We recently carried out a compehensive spectroscopic
study on 20 Li-rich giants based on the Subaru/HDS
spectra and compared their observational characteristics
with those of ~300 normal red giants. According to
the resulting Li abundances determined by applying
the spectrum-fitting method to Li I 6708 and Li I 6104
lines (Figure 1), we could not detect any signature forthe existence of 6Li (Figure 2). It was also confirmed
from our analysis of Be II 3131 line that Li-rich giants
are deficient in Be (just like normal giants) without any
sign of enrichment. Consequently, we conclude that the
hypothesis of “engulfment of substellar companions”(accretion of unprocessed gas or solid material) is rather

5000 4500
Teff (K)4000

HD 167304

HD 9746

Ca
Fe

0

HD 183492

HD 214995

Fe

Fe

1

-2

HD 194937

HD 9746
HD 205349(b)A(Be)s.s.

-1

HD 170527

HD 8676
HD 183492

Fe
(+Be)

HD 205349
HD 7873130.5Fe

AL3131(Be)Normalized flux

HD 170527

AL3131(Be)HD 21018

KIC 9821622

Fe

2

(c)

A(Be)s.s.

1
0

-1

0.2

-2

3131
Wavelength (Å)

-1

-0.5

[Fe/H]

00.5

Figure 3: Synthetic spectrum fitting for Be abundance determination,and the resulting Be abundances plotted against Teffand [Fe/H] (small filled circles are normal giants
for comparison, where blue and green symbols
denote established abundances and upper limits forindetermibable cases, respectively).

References[1] Aguilera-Gomez, C., et al.: 2016, ApJ, 829, 127.
[2] Takeda, Y., Tajitsu, A.: 2017, PASJ, 69, 74.

I Scientific Highlights

021

Luminosity Effect of O I 7771–5 Line Strength in Evolved A–F–G Stars(NAOJ)			

JEONG, Gwanghui, HAN, Inwoo

Although the strength of O I 7771–5 triplet feature(W77) is known to show a luminosity effect and may be
usable for empirical evaluation of absolute magnitude(M V ), our understanding on its behavior is stillinsufficient. Especially, the validity and applicability limitof various analytical relations proposed so far (which are
not necessarily consistent with each other) has yet to beclarified.

(KASI, Korea)

to supergiants of −5 > MV > −10, if one wants to safely
make use of the luminosity effect of O I 7771–5 lines.
See [1] for more details of this study.

20 Msun5

15 Msun
12 Msun

4

9 Msun5 Msun4 Msun2

3 Msun2 Msun1

1.5 Msun0
4.1

1 Msun4

3.9
3.8
log Teff (K)

3.7

3.6

Figure 1: Program stars plotted on the theoretical HR diagram.

With an aim to shed light on this situation, weinvestigated how W77 depends on MV and other stellar
parameters for unbiased sample of 75 evolved A-, F-,
and G-type stars of various luminosity classes (subgiants,
giants, and supergiants; cf. Figure 1). Based on the highdispersion spectra obtained with the echelle spectrographof 1.8 m reflector at Bohyunsan Optical Astronomy
Observatory (Korea Astronomy and Space Science
Institute), we measured W77 for each star by applying thespectrum-fitting technique (cf. Figure 2).
Our results are shown in Figure 3, where we canconfirm that W77 tends to increase as MV becomes moreluminous. However, the behavior of W77 for the wholesample is too complicated to be described by a simple
relation. Specifically, distinctly different trends of W77
were found for the lower-gravity (log g < 2.5) groupof supergiants or bright giants and the higher-gravity(log g > 2.5) group of giants or subgiants. That is, thesimple MV vs. W77 formulas proposed by past studies areapplicable only to the former group, but not to the lattergroup showing a totally different tendency. Since these
two groups overlap at 0 > MV > −5 (i.e., F–G supergiantsof the former group and A-type giants of the latter group),
special care should be taken in using W 77 of stars inthis MV range. It is thus recommended to confine only

022

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082210164668006130082543168608006210088759172365007034100418174464008890104452

180583012953111812

185758014489111892

186377020902117566

187982022211

126868188650023230128563

192514025291133002

193370026553141714

194951032188148317

195295032655148743

195324035520149662

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198726038558151070197345039866154319201078045412158170202240050018159026203096050420159877208110057749160365210459059881164136213306072779164507218753077601164613220657

0.2

O OO

7770

Fe

0.2

7780

O OO

7770

Fe
Fe

0.2

O O

O

7780
7770
Wavelength (Å)

7780

Figure 2: Spectrum fitting in the 7765–7785 Å region.

2
W77 (Å)3

Normalized fluxlog (L/Lsun)

7 Msun000571

1

0
5

open symbols: log g < 2.5
filled symbols: log g > 2.5

Trend forlog g > 2.5 starsReby lation
var s reiou pors li ted
tera
ture

TAKEDA, Yoichi

			

0
-5
MV (mag)

Figure 3: W77 vs. MV relation.
Reference[1] Takeda, Y., Jeong, G., Han, I.: 2018, PASJ, 70, 8.

-10Development of Micro-Mirror Slicer Integral Field Unit
for Space-borne Solar Spectrographs
SUEMATSU, Yoshinori(NAOJ)SAITO, Kosuke, KOYAMA, Masatsugu, ENOKIDA, Yukiya, OKURA, Yukinobu
NAKAYASU, Tomoyasu, SUKEGAWA, Takashi(Canon Inc.)

Integral field spectroscopy (IFS) is a two dimensional
spectroscopy, providing spectra for each spatial directionof an extended two-dimensional field simultaneously.
There are three methods to realize the IFS depending on
image slicing devices: micro-lenslet arrays, optical fiber
bundles, and narrow rectangular image slicer arrays.
Basically, the integral field spectroscopy unit (IFU) acts
as a coupler between the telescope and the spectrographby optically reformatting a two-dimensional rectangularfield into a quasi-continuous pseudo-slit located at theentrance focal plane of a spectrograph.
The scientific advantages of IFS for studies of
localized and transient solar surface phenomena
are obvious. From the viewpoint of high-efficiency
spectroscopy, wide wavelength coverage, precision
spectro-polarimetry, and space application, the image
slicer consisting of all reflective optics is the best option
among the three. For space instrumentation, small-sized
IFU units are advantageous; they demand that the widthof the slicing mirrors should be as narrow as an optimal
spectrograph slit width (< 100 μm), which is usuallydifficult to manufacture with glass polishing techniques.
In this study, we could successfully applied a Canon's
novel technique for high optical performance metallic
mirrors of small dimensions.
Keeping in mind a possible application for a future
space-borne spectrograph such as SOLAR-C: a nextplanned Japanese solar space mission, we designed an
IFU that utilizes a micro-mirror slicer of 45 arrayed
30-μm-wide metal mirrors and a pseudo-pupil metal
mirror array of off-axis conic aspheres re-formatting
three pseudo-slits; this design is feasible for opticalconfiguration sharing a spectrograph with a conventional
real slit. We manufactured a prototype IFU for evaluationaccording to the optical design and deposited a protectedsilver coating on both metal mirrors after its successful
space qualification tests.
It demonstrated that the final optical quality of the
IFU is sufficiently high for a visible light spectrograph.
Each slicer micro-mirror is 1.58 mm long and 30 μm widewith the micro-roughness is less than 1 nm rms and edge
sharpness is less than 0.2 μm even after the reflective
coating and mirror tilt errors were less than the required
accuracies. As to the pseudo-pupil mirrors, the microroughness was less than 1.27 nm rms and the surface

figure accuracy was less than 59 nm PV. Tilt errors
around the x-axis of all surfaces were less than 4.6 arcsec
and those around the y-axis of all the surfaces were lessthan 2.3 arcsec, which are less than the requirement(7.7 arcsec). We confirmed that the pseudo pupils were
projected as designed and the re-arranged slicer images
were focused by the pseudo-pupil mirrors as three pseudoslits at a distance 200 mm away (see Figure 1).
We also presented a concept of a field lens placedat the slit plane that changes the diverging beam fromthe pseudo-pupil mirrors to a telecentric beam into aspectrograph. The field lens needs to have a high index
larger than 2. Off-the-shelf ZnSe-made cylindrical lenses
which are close to the optical design were used andsuccessfully verified the optical performance.

Figure 1: Set up of micro-mirror slicer IFU (left), footprint at
pseudo-pupil mirror array of F/24 beams arising fromthe slicer (middle), and image on a camera of the rearranged slicers through the ZnSe cylindrical fieldlens (right), confirming that all the metal mirrors were
fabricated as designed.

Reference[1] Suematsu, Y., et al.: 2017, CEAS Space J., 9, 421-431.

I Scientific Highlights

023

Stellar Stream and Halo Structure of the Andromeda Galaxy
Revealed by Subaru Hyper Suprime-Cam
KOMIYAMA, Yutaka1, CHIBA, Masashi2, TANAKA, Mikito2, TANAKA, Masayuki1, KIRIHARA, Takanobu3
MIKI, Yohei4, MORI, Masao5, LUPTON, R. H.6, GUHATHAKURTA, P.7, KALIRAI, J. S.8, GILBERT, K.8
KIRBY, E.9, LEE, M. G.10, JANG, I. S.10, SHARMA, S.11, HAYASHI, Kohei1
1: NAOJ, 2: Tohoku University, 3: Chiba University, 4: University of Tokyo, 5: Tsukuba University, 6: Princeton University, 7: UCO Lick, 8:
STScI, 9: Caltech, 10: SNU, 11: Sydney

The halos of galaxies preserve fossil records ofgalaxy formation through hierarchical assembly and pastaccretion events. The halo of the Andromeda galaxy(M31) is a complementary target to the Milky Way as
it can be observed in perspective from the center to thehalo. However, the detail of the M31 halo is still vailed
due to its large distance.
We have carried out a wide and deep survey for 9.2
deg2 field in the north-west (NW) halo of the Andromeda
galaxy (M31) using Hyper Suprime-Cam on the Subaru
Telescope. Our survey goes deep enough to probe redclump (RC) stars, which are numerous and make distinct
feature in the color-magnitude diagram, and allows
us to investigate the detailed structure and the stellar
population of the NW Stellar Stream which is known toexist in this field.
From the distance estimate based on the RC
magnitude, it is likely that the NW Stream is located~70 kpc behind the main body of M31. A numericalsimulation incorporating this distance estimate sets a strict
constraint on the orbit of the NW Stream. The detailed
structure of the NW Stream which is traced by the
number density distribution of RC stars is revealed. The
cross-sectional shape of the stream is well represented by
a Gaussian with FWHM of 25 arcmin (5.7 kpc), with aslight skew to the south-west direction. The shape along
the stream is revealed to be complicated: in addition toa significant gap, numbers of bumps and dips are foundalong the stream (see Figure 1). It is expected that future
numerical simulation which reproduces the orbit and theshape of the NW Stream will reveal the nature of the NW
Stream as well as the properties of the halo of M31.
We also found a distinct stellar population other thanthat comprising the NW Stream in the south part of oursurvey field from the analysis of the color-magnitude
diagram. This finding suggests that a substructure which
is more extended and diffuse than the NW Stream do exist
in our survey field. Follow-up observations are necessary
to address the nature of this diffuse substructure.

024

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Figure 1: The number density distribution of RC stars. The
number density decreases from the south-east to thenorth-west and a significant gap is also found. The
diffuse substructure suggested in the text is seen asa diffuse hump of number density at the south-westpart outside the stream. The gray circles represent themasked regions by bright stars and the crosses represent
globular clusters which are suggested to be associatedwith the NW Stream.

Reference[1] Komiyama, Y., et al.: 2018, ApJ, 853, 29.

Extended Ionized Gas out of Galaxies in the Leo Cluster (Abell 1367)
YAGI, Masafumi, YOSHIDA, Michitoshi, KOMIYAMA, Yutaka, KASHIKAWA, Nobunari(NAOJ)		GAVAZZI, Giuseppe(University of Milano-Bicocca) 		

In clusters of galaxies, the relative motion of member
galaxies to the hot gas of the cluster produces a rampressure. The ram pressure strips gas from galaxies,
and sometimes the gas stripped out of the galaxy gets
ionized by some mechanism to be detected as an Hαemitting cloud. We observed a part of the Virgo cluster
and the Coma cluster, in Hα narrow-band, and B, and R
broad-bands of the Subaru Suprime-Cam to study suchintergalactic ionized gas (e.g., [1,2]). We then executed asystematic survey of the Leo cluster (Abell 1367) with anHα filter for redshift z= 0.022 of the Suprime-Cam [3].
By the survey, we detected six new extended ionizedgas clouds in addition to three galaxies with known gas
tails (CGCG 097-073, CGCG 097-079, CGCG 097087; [4]), and one of the new clouds was confirmed tohave much longer tail by a follow-up observation [5].
Remarkable objects compared to the previous studies
were the clouds which show no relation to the galaxies;“Orphan clouds” (Figure 1 top). Other clouds known
so far show the connection to the galaxy from which
the gas came from (parent galaxies). Meanwhile, noparent candidates are found at least within 85 kpc fromthe orphan clouds, and any member galaxies around theregion show no sign of stripping toward the orphans. The
orphan clouds brought to us new mysteries; from where
the gas came, and how the ionization is maintained in~30 kpc.
Another discovery was that the galaxy group whichis infalling onto the cluster (Blue Infalling Group; BIG;[6]) has an ionized gas tail more than 300 kpc long. The
length is about twice longer than known before [7].
The apparence of the tail indicates a helical shape. We
presented a hypothesis that the tail originated not fromthe intragroup gas but from each galaxy, and the helicalshape corresponds to the motion of the galaxy around thebarycenter of the group while the gas had been strippedby the ram-pressure by the cluster gas. We also foundsign of star formation in a limited region of the BIG tail(Figure 1 bottom).
Future spectroscopic observation will enable us toset constraints on the motion, the metallicity, and theionization mechanism of the gas, and to estimate the age
and the mass of the star-forming regions. We will try tounderstand the evolution of the gas in the cluster and theeffect of the stripping on the evolution of the galaxies
deeply and comprehensively.

OKAMURA, Sadanori(Hosei University)

Figure 1: Intergalactic ionized gas clouds in the Leo cluster.
NB671(Hα;red), R(green), B(blue) three color
composite. With the color assignment, ionized clouds
is shown in red, and starforming region is in magenta.
Yellow bars at the bottom-left indicate 10 kpc. (top)Orphan clouds, which show no connection to galaxies.
(bottom) Star-forming regions (green circles) in the tailof the blue infalling group (BIG).
References[1] Yoshida, M., et al.: 2002, ApJ, 567, 118.
[2] Yagi, M., et al.: 2010, AJ, 140, 1814.
[3] Yagi, M., et al.: 2017, ApJ, 839, 65.
[4] Gavazzi, G., et al.: 1995, A&A, 304, 325.
[5] Gavazzi, G., et al.: 2017, A&A, 606, A131.
[6] Gavazzi, G., et al.: 2003, ApJ, 597, 210.
[7] Cortese, L., et al.: 2006, A&A, 453, 847.

I Scientific Highlights

025

Dynamics of Porous Dust Aggregates and Gravitational Instabilityof Their Disk
MICHIKOSHI, Shugo

Planetesimals are building blocks of planets.
The terrestrial planets and the cores of gas giants are
considered to be formed by the collisional accretion ofplanetesimals. In a protoplanetary disk, small dust grains
grow to planetesimals. It is not yet understood how dust
grains grow into planetesimals, because this process mustovercome various obstacles.
Recent studies on the dust growth showed that the icy
dust aggregates formed by coagulation are not compact
but significantly porous. The internal density of dust
aggregates is much smaller than the material density,
which is ~ 10 −5 g cm −3 . A compression mechanism
is necessary to form compact planetesimals. In the
final stage of the dust growth, the dust aggregates arecompressed by the self-gravity [1].
In the previous paper, we considered the final stage ofthe evolution of icy dust aggregates [2]. We investigatedthe dynamics of dust aggregates and obtained theirrandom velocity. We found that, for a reasonable rangeof turbulence strength, the porous dust disk becomes
gravitationally unstable as the dust aggregates evolve
through self-gravity compression. In the previous paper,
we adopted the MMSN model and assumed an isotropic
velocity dispersion and an equilibrium random velocity.
In this work, we extend the previous work and adopt a
more general disk model and a more precise dynamical
model. We considered the self-gravity, mutual collisions,aerodynamic drag, turbulent stirring, and scattering due togas and calculated the eccentricity and inclination. Fromthem we calculated the Toomre’s Q and Roche criterion
to examine the gravitational instability (GI) [3].
In the standard model, we found that the GI conditionis finally satisfied when α <~ 4 × 10−4. Next, we assumed
the general parameters and checked whether GI occurs.
Figure 1 shows the example of the results. The GI is moretend to occur for larger fg, where fg is the normalized disk
mass. Thus, the upper limit of α for the GI exists, and it
depends on the disk parameters.
Considering the simple approximations, we derived
the critical α value analytically(1)
where a is the distance from the central star, CD is thegas drag coefficient, M* is the central star mass, η is thegas pressure gradient parameter, Σd is the dust surface
density, Σg is the dust surface density. Figure 1 shows thisestimate, which well agrees with the numerical result.

026

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KOKUBO, Eiichiro(Kyoto Women's University)		

(NAOJ)

This critical α formula is consistent with that derived in
the previous work.
−3
We found that if the turbulence is not strong (α <~ 10 ),
the GI takes place. The GI accelerates the planetesimalformation significantly.
10−1

10−2
α

			

10−3

10−4
10−1

100

101

fg

Figure 1: Parameter region for the GI on the normalized disk
mass fg and the turbulent strength α plane. The filled
circle points show the cases where the GI takes place.
The triangles show the cases where the GI does not takeplace. The open circles show the cases where the GI
does not take place when the non-equilibrium effect isconsidered. The solid line represents the estimates of thecritical α. The dashed line represents the other estimate.

References[1] Kataoka, A., et al.:2013, A&A, 557, 4.
[2] Michikoshi, S., Kokubo, E.: 2016, ApJ, 825, L28.
[3] Michikoshi, S., Kokubo, E.: 2017, ApJ, 842, 61.

Gaia DR1 Evidence of Disrupting the Perseus Arm
BABA, Junichi(NAOJ)The origin of spiral arms in disk galaxies has been
hotly debated since 1960s. There are two different
theories of spiral arms in terms of lifetimes and rotational
behaviour [1]. The quasi-stationary “density wave”
theory characterises spirals as rigidly rotating, longlived wave patterns (i.e., >~ 1 Gyr) [2]. On the other hand,the “dynamic spiral” theory suggests spiral arms aredifferentially rotating, transient, recurrent patterns on arelatively short time scale (i.e., ~100 Myr) [3].
In this study [4], we investigated kinematics of 77
Cepheid variables around the Perseus arm in the Milky
Way galaxy, taking advantage of the accurately measured
distances of Cepheids and the proper motions from Gaia
Data Release 1. We found that both the Galactocentric
radial (U pec ) and rotation (V pec ) velocities of these
Cepheids are correlated with their distances from thelocus of the Perseus arm (Fig. 1a), as the trailing side isrotating faster (Fig. 1c) and moving inward (Figs. 1b)compared to the leading side. We also found a negative
vertex deviation for the Cepheids on the trailing sidein contrast to the positive vertex deviation in the solar
neighborhood (Fig. 1d).
We compared these observational trends with
our N-body/hydrodynamics simulations based on a
static density-wave spiral scenario and those basedon a transient dynamic spiral scenario. Although
our comparisons are limited to “qualitative” trends,
they favor a conclusion that the Perseus arm is in the
disruption phase of a transient arm. We will further test
the disruption phase scenario of the Perseus arm with the
future Gaia data releases, and compare more sophisticatedsimulations.

References[1] Dobbs, C., Baba, J.: 2014, PASA, 31, 35.
[2] Lin, C. C., Shu, F. H.: 1964, ApJ, 140, 646.
[3] Baba, J., et al.: 2013, ApJ, 763, 46.
[4] Baba, J., et al.: 2018, ApJL, 853, 23.

Figure 1: Comparison between the models and the observed
kinematics of Cepheids in terms of correlations ofdPer–Upec and dPer–Vpec (panel a), mean Upec (panel b),mean Vpec (panel c) and the vertex deviation (panel d).
Horizontal shaded areas in black and red indicate theobserved values. The model results are shown with theopen symbols with error bars. Note that the left side of
the panels shows the “Density Wave” model results fortwo different co-rotation (CR) radius values, whereas
in the right side the “Dynamic Spiral” model results arepresented as a function of time.

I Scientific Highlights

027

Properties of Galaxies around AGNs in the HSC Wide Survey
SHIRASAKI, Yuji

(NAOJ/SOKENDAI)		

HE, Wanqiu

AKIYAMA, Masayuki(Tohoku University)

NAGAO, Tohru

TOBA, Yoshiki(Ehime University)		

(ASIAA)

OHISHI, Masatoshi, MIZUMOTO, Yoshihiko, MIYAZAKI, Satoshi(Tohoku University)				(NAOJ/SOKENDAI)				NISHIZAWA, J. Atsushi(Nagoya University)

The ubiquity of super massive black holes (SMBHs)
at the centers of galaxies has been recognized from theobservation of nearby galaxies. The mechanism of theevolution of SMBHs is however still an open question.
Accretion in a secular mode caused by gravitational
instability inside a galaxy is one of the mechanism todeliver the gas content into the SMBH. The bright quasistellar objects (QSOs) is thought to be maintained by theaccretion induced by external processes such as galaxy
interactions and/or mergers. Different accretion modes
can be the source of feeding SMBH.
We examined the environment of active galactic
nuclei (AGNs) to investigate the relevance of the external
process to the evolution of SMBHs with masses larger
than 108 M [1]. We used the data of the Hyper SuprimeCam Subaru Strategic Program (HSC-SSP, S15b) for
deriving galaxy samples, and the SDSS QSO catalog
from which mass of the SMBHs was obtained using
the empirical formula relating the emission line widthand continuum luminosity to the black hole (BH) mass.
The total number of AGN samples used here is 5,345,
and those samples cover the redshift range of 0.6–3.0
and the BH mass range of 108–1010 M. This is the firstopportunity to investigate the environment of AGNs up
to 3.0, which covers the era of the peak of star formationand mass accretion rate for SMBHs, in unprecedented
statistics.
Figure 1 shows the distribution of over density ofgalaxies with a given absolute magnitude at projecteddistances of 0.2–2.0 Mpc from AGNs relative to those at
7.0–9.8 Mpc. The measured distributions (markers anddashed lines) indicate over density at a bright end against
the expectations calculated from the luminosity function
obtained in literature (solid lines). It is known that moreluminous galaxies tend to be more clustered than lessluminous galaxies. According to the SDSS survey andthe Subaru deep survey, the auto-correlation length ofluminous (< M*: break point of the luminosity function)
galaxies is at most 10 h −1 Mpc. The auto-correlation
length estimated from the over density measured in thiswork amount to 40 h−1 Mpc if we assume that there isno correlation between the distribution of AGNs and theluminous galaxies observed around the AGNs. To resolve
the discrepancy from the previous results, we need tothink of the association between the AGNs and the028

I Scientific Highlights

USUDA, Tomonori(NAOJ/SOKENDAI)

luminous galaxies. This indicates that there is an activity
which induces star formation and feeding SMBHs
beyond > 108 M in multiple galaxies concurrently atseveral Mpc scale. We also obtained the indication thatthe environment of AGNs with larger BH mass has
tendency to have larger red galaxy fraction. Those result
indicate that the mechanism to evolve the SMBH beyond
108 M is related with the large scale phenomena such asa collision between clusters and/or groups of galaxies.

λFigure 1: Absolute magnitude distributions of galaxies measured
by subtracting the distribution at projected distancefrom AGNs rp = 7.0–9.8 Mpc from that at 0.2–2.0 Mpc(markers). Detection efficiency (completeness) ofgalaxies was corrected. Solid lines represents the
distribution expected from the luminosity function
measured in literature. Dashed lines are the Schechter
function fitted to the observation. The arrows indicate
90 % detection limit.

Reference[1] Shirasaki, Y., et al.: 2018, PASJ, 70, S30.

Small Jupiter Trojans Survey with the Subaru/Hyper Suprime-Cam		

YOSHIDA, Fumi

(Chiba Institute of Technology/Kobe University)

Jupiter Trojans (JTs) are asteroids that share theorbits with Jupiter and make swarms near the Lagrangian
points L4 (leading) or L5 (trailing) of Jupiter. They are amajor small-body population located in the middle region
between the main belt asteroids (MBAs) and transNeptunian objects (TNOs). Recent dynamical models
suggest that JTs have formed between/beyond the outerplanet regions and were captured into Jupiter's co-orbital
region during the dynamical instability phase inducedby planetary migration. Investigation of the origin andevolution of JTs is useful for understanding the radial
mixing processes of small bodies in that phase.
Here, we focus on the size frequency distribution(SFD) of JTs as a tracer of their origin, but it remains
uncertain in the small size range. The SFD includes two
kinds of information regarding the accumulation process
and collisional evolution process in the large and small
size ranges, respectively. These are important clues forthe formation region of JTs. Owing to the large apertureof the Subaru Telescope, we detected the smallest sized
JTs obtained by the present ground-based telescopes,
and investigated the detail SFD of small JTs, which ischaracterized by the impact strength properties.
We performed an asteroid survey covering ~26 deg2
of sky area near the Jupiter L4 point using the Hyper
Suprime-Cam attached to the Subaru Telescope anddetected 631 JTs [1]. The detection limit is 24.4 mag
in r band, which is corresponding to ~2 km in diameterassuming a geometric albedo of 0.07 [2]. Considering
the detection limit and heliocentric distance of eachobject, we selected 481 objects as the unbiased sample.
The number of sample is more than three times larger
than that of the previous surveys [3,4]. We found that theSFD exhibits a single-slope power law over the diameter
range of ~2 km to ~10 km and has no feature such as abreak and roll-over, though the previous surveys reported
a broken power-law or double power-law slopes in thesimilar size range. The best-fit power-law index of theabsolute magnitude distribution N(H) ∝ 10αH, where H
is absolute magnitude, is estimated to be α = 0.37 ± 0.01.
This value is consistent with that of the faint end slopepresented by Wong & Brown (2015) [4].
Combining the cataloged L4 JTs and our survey, we
finally show the entire SFD of L4 JTs down to 2 km indiameter (see Figure 1). We confirmed that JTs’ SFD has
a power-law transition at diameter of ~10 km but does notshow a “wavy” structure which is significantly seen inthat of MBAs. This indicates a discrepancy in the impact
strength properties between JTs and MBAs, suggesting

TERAI, Tsuyoshi(NAOJ)

that these two populations have different composition/
collisional evolution. Therefore, it is likely that they
originated from different formation regions.

Figure 1: Cumulative SFDs of L4 JTs combined with the datafrom the Minor Planet Center catalog (squares), Jewitt
et al. (2000) [5] (crosses), and this work (circles). The
dashed line shows the best-fit power law of our data.

References[1] Yoshida, F., Terai, T.: 2017, AJ, 154, 71.
[2] Grav, T., et al.: 2012, ApJ, 759, 49.
[3] Yoshida, F., Nakamura, T.: 2005, AJ, 130, 1900.
[4] Wong, I,. Brown, M. E.: 2015, AJ, 150, 174.
[5] Jewitt, D. C., Trujillo, C. A., Luu, J. X.: 2000, AJ, 120, 1140.

I Scientific Highlights

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Multi-band Photometry of Trans-Neptunian Objects
in the Subaru Hyper Suprime-Cam Survey
TERAI, Tsuyoshi(NAOJ)YOSHIDA, Fumi

(Chiba Institute of Technology/Kobe University)

OHTSUKI, Keiji(Kobe University)

LYKAWKA, Patryk Sofia(Kindai University)

TAKATO, Naruhisa, HIGUCHI, Arika, ITO, Takashi, KOMIYAMA, Yutaka, MIYAZAKI, Satoshi(NAOJ)

WANG, Shiang-Yu(ASIAA)

Trans-Neptunian objects (TNOs), a small body
population orbiting beyond the Neptune, have been
known to exhibit a diversity in visible color, which islikely to reflect their formation environment. The color
distribution of TNOs is helpful to study the formation andevolution of small bodies in the outer region at the earlystage of our solar system.
We performed a visible multi-band photometry of
TNOs [1] using the data acquired by the Subaru Telescopewith Hyper Suprime-Cam (HSC) through the Subaru
Strategic Program survey [2]. From the five broad-band(g, r, i, z, and Y ) imaging data covering ~500 deg2 of sky
within ± 30° of ecliptic latitude, we identified 30 known
TNOs. Based on the dynamical classification scheme
presented by Lykawka and Mukai (2007) [3], theseobjects are classified into the four dynamical groups: 13
cold classical, 6 hot classical, 7 scattered, and 4 resonant
populations. Our color measurements showed that the
hot classical and scattered populations with orbital
inclination (I) of I > 6° (hereinafter, “high-I population”)
share similar color distributions, while the cold classicalpopulation with I < 6° (hereinafter, “low-I population”)
contains a more amount of reddish objects in the shortwavelength range compared to the high-I population.
In addition, we confirmed a significant anti-correlation
between g-r/r-i colors and inclination in the high-I
population as previous studies pointed out.
We also found that the sample objects are separated
into two swarms in the g-i vs. eccentricity (e) plot (seeFigure 1), i.e., the red/low-e and neutral/high-e groups.
Although most of the high-I objects are contained in theneutral/high-e group, four of them are located in the red/
low-e region. This fact suggests that the high-I objects
consist of two sub-populations, which could provide
a useful clue for better understanding the dynamical
evolution history of TNOs in the early solar system.

030

I Scientific Highlights

Figure 1: Top: g-i color vs. eccentricity/inclination of the low-I(circles) and high-I (squares) populations. The dashedlines show the solar color. Bottom: The same plot as the
top panels, but the red high-I objects are marked withtriangles.

References[1] Terai, T., et al.: 2018, PASJ, 70, S40.
[2] Aihara, H., et al.: 2018, PASJ, 70, S4.
[3] Lykawka, P. S., Mukai, T.: 2007, Icarus, 189, 213.

Disentangling the Circumnuclear Disk of Centaurus A with ALMA:An Inner Molecular Ring, Nuclear Shocks and the CO to warm H2 Interface
ESPADA, Daniel1/2, MATSUSHITA, Satoki3, MIURA, Rie E.1, ISRAEL, Frank P.4, NEUMAYER, Nadine5
MARTIN, Sergio6/7, HENKEL, Christian8/9, IZUMI, Takuma10, IONO, Daisuke1/2, AALTO, Susanne11
OTT, Jürgen12, PECK, Alison B.13, QUILLEN, Alice C.14, KOHNO, Kotaro10
1: NAOJ, 2: Graduate University for Advanced Studies, 3: Academia Sinica, Institute of Astronomy & Astrophysics, 4: Sterrewacht Leiden,
Leiden University, 5: Max Planck Institute for Astronomy, 6: Joint ALMA Observatory, 7: European Southern Observatory, 8: Max-PlanckInstitut für Radioastronomie, 9: King Abdulaziz University, Saudi Arabia, 10: The University of Tokyo, 11: Chalmers University, 12: National
Radio Astronomy Observatory, 13: Gemini Observatory, 14: University of Rochester

We present the distribution and kinematics of themolecular gas in the circumnuclear disk (CND, 400 pc ×
200 pc [1]) of Centaurus A with resolutions of ~5 pc (0 ″3).
and shed light onto the mechanism feeding the Active
Galactic Nucleus (AGN) using CO(3–2), HCO +(4–3),
HCN(4–3), and CO(6–5) observations obtained with
ALMA [2]. Multiple filaments or streamers of tens to ahundred parsec scale exist within the CND, which forma ring-like structure with an unprojected diameter of
162 pc × 108 pc and a position angle PA  155°. Inside
the nuclear ring, there are two leading and straight
filamentary structures with lengths of about 30–60 pc
at PA  120° on opposite sides of the AGN, with arotational symmetry of 180° and steeper position-velocity
diagrams, which are interpreted as nuclear shocks due
to non-circular motions. Along the filaments, and unlike
other nearby AGNs, several dense molecular clumps

present low HCN/HCO+(4–3) ratios (< 0.5). The filaments
abruptly end in the probed transitions at r  20 pc fromthe AGN, but previous near-IR H 2(J=1–0)S(1) maps
show that they continue in an even warmer gas phase(T ~ 1000 K), winding up in the form of nuclear spirals,
and forming an inner ring structure with another set ofsymmetric filaments along the N–S direction and withinr  10 pc. The molecular gas is governed primarily by
non-circular motions, being the successive shock fronts at
different scales where loss of angular momentum occurs,a mechanism which may feed efficiently powerful radiogalaxies down to parsec scales.
References[1] Espada, D., et al.: 2009, ApJ, 695, 116.
[2] Espada, D., et al.: 2017, ApJ, 843, 136.
[3] Espada, D., et al.: 2012, ApJL, 756, L10.

Figure 1: Kiloparsec to parsec scale view of the molecular disk of Cen A (NGC 5128): a) Integrated CO(2–1) emission map (green) observed
using the Submillimeter Array (SMA, [1]). The circumnuclear disk is just perpendicular to the X-ray/radio jet (red, Chandra). A
more extended molecular gas component in form of spiral arms [3] is seen. b) Composite image of the CND of Cen A including the
ALMA CO(3–2) (green) and CO(6–5) (blue) integrated intensity maps, as presented in [2]. The distribution of molecular hydrogenas traced by the H2 line (red) is mostly contained within a field of view of 54 pc. The cross sign in the center of the image shows the
AGN position.

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031

Supernova Nucleosynthesis Enhanced
by Collective Neutrino Oscillations
SASAKI, Hirokazu(University of Tokyo)

		

HAYAKAWA, Takehito(QST)			KAJINO, Toshitaka(NAOJ/Beihang University/University of Tokyo)

PHELIVAN, Yamac(Mimar Sinan Fine Arts University)

N e u t r i n o s a r e p r o d u c e d i n s i d e h i g h e n e rg y
astrophysical sites such as core-collapse supernovae,
neutron star mergers and the early universe. Neutrino
spectra can be affected by inner materials and neutrino
themselves. Therefore, we can reveal properties ofastrophysical phenomena by observing emitted neutrinos.
In core-collapse supernovae, energetic neutrinos
are emitted from a proto-neutron star after the corebounce. Non-linear neutrino flavor transitions called“collective neutrino oscillations” [1] are induced bycoherent scatterings of self-interacting neutrinos outside
the proto-neutron star. Collective neutrino oscillationstransform the spectra of all neutrino species. Suchmodified neutrino spectra could change reaction rates ofelectron antineutrino absorptions on free protons, whichis expected to affect νp process nucleosynthesis [2].
However, contributions from neutrino flavor transitions
on such nucleosynthesis are still unknown.
In this work [3], we study the impact of collective
neutrino oscillations on the νp process nucleosynthesis bycombining realistic three flavor multiangle simulations
with network calculations. Fig. 1 shows antineutrino
spectra after collective neutrino oscillations. Theenergetic electron antineutrinos are produced in normal
neutrino mass hierarchy (Fig. 1a). On the other hand,flavor transitions are highly suppressed owing tomultiangle effects in inverted neutrino mass hierarchy(Fig. 1b). As shown in Fig. 2, the abundances of p-nuclei
are enhanced by collective neutrino oscillations up
to 104 times in normal mass hierarchy, which reflects
the increased ν–e flux in Fig. 1a. Our results imply thenecessity of collective neutrino oscillations for the precise
nucleosynthesis in neutrino-driven winds and also help
understand the origin of solar-system isotopic abundancesof molybdenum 92, 94 and ruthenium 96, 98.

TAKIWAKI, Tomoya(NAOJ)BALANTEKIN, Baha

(University of Wisconsin Madison)

Figure 1: Antineutrino spectra after collective neutrino
oscillations. Fig. 1a(b) represents the case of normal(inverted) neutrino mass hierarchy, respectively. The
dotted lines are corresponding to initial spectra.

Figure 2: Nuclear abundances of p-nuclei (74Sr, 78Kr, ..).

References[1] Duan, H., et al.: 2006, Phys. Rev. D, 74, 105014.
[2] Wanajo, S.: 2006, APJ, 647, 1323.
[3] Sasaki, H., et al.: 2017, Phys. Rev. D, 96, 043013.

032

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On the Disappearance of a Cold Molecular Torus
around the Low-luminosity Active Galactic Nucleus of NGC 1097IZUMI, Takuma1, ESPADA, Daniel1, IMANISHI, Masatoshi1, NAKANISHI, Kouichiro1, KOHNO, Kotaro2
FATHI, Kambiz3, HATZIMINAOGLOU, Evanthia4, DAVIES, Ric5, MARTIN, Sergio6/4, MATSUSHITA, Satoki7
SCHINNERER, Eva8, AALTO, Susanne9, ONISHI, Kyoko10, TURNER, Jean L.11, MEIER, David S.12
WADA, Keiichi13, KAWAKATU, Nozomu14, NAKAJIMA, Taku15
1: NAOJ, 2: University of Tokyo, 3: Valhallav, 4: ESO, 5: MPIE, 6: JAO, 7: ASIAA, 8: MPIA, 9: Chalmers University, 10: Ehime University,
11: UCLA, 12: NMIMT, 13: Kagoshima University, 14: Kure National Institute of Technology, 15: Nagoya University

The unified scheme of active galactic nuclei (AGNs)
postulates that the existence (type-1) or absence (type-2)
of a broad line region depends on the viewing angle of an
optically and geometrically thick dusty/molecular torus[1]. However, the physical origin of the high-velocity
dispersion or the vertical height of a torus is still being
debated. At the circumnuclear ~ 10–100 pc scales, energy
feedback from supernova explosions and radiationdriven outflows from the AGN itself can be candidate
mechanisms [2,3].
In order to study the torus properties in more detail,we used the Atacama Large Millimeter/Submillimeter
Array to map the CO(3–2) and the underlying continuum
emissions around the type-1 low-luminosity active
galactic nucleus (LLAGN; bolometric luminosity <1042 erg s−1) of NGC 1097 at ~10 pc resolution [4]. Theseobservations revealed a detailed cold gas distribution
within a ~100 pc of this LLAGN (Figure 1a). In contrast
to the luminous Seyfert galaxy NGC 1068, where a~7 pc cold molecular torus was recently revealed [5], adistinctively dense and compact torus is missing in ourCO(3–2) integrated intensity map of NGC 1097, at its
AGN location. Based on the CO(3–2) flux, the gas massof the torus of NGC 1097 would be a factor of ~ 2–3
less than that found for NGC 1068 by using the same
CO-to-H2 conversion factor, which implies less active
nuclear star formation and/or inflows in NGC 1097, i.e.,
an energy source to support the torus thickness would
be missing in this LLAGN. To better confirm this view,
we performed a dynamical modeling of the CO(3–2)
velocity field to decompose the rotation component (Vrot)
and dispersion component (σ) with tilted-rings (Figure1b). We then found that NGC 1097 hosts a geometricallythinner torus than NGC 1068, indeed, as reflected by theσ/Vrot ratio (a surrogate of the disk aspect ratio; Figure1c). Although the physical origin of the torus thickness
remains unclear, our observations support a theoreticalprediction that geometrically thick tori with high opacity
will become deficient as AGNs evolve from luminous
Seyferts to LLAGNs.

Figure 1: (a) Global spatial distribution of the CO(3–2) integrated
intensity in the central ~130 pc of NGC 1097. The central
star marks the AGN location. No clear gas concentration
was found at the AGN position, indicating the deficit of
the molecular torus. (b) Radial profiles of the rotation
velocity (Vrot; squares) and the velocity dispersion (σ;circles) derived from the CO(3–2) line data with tiltedring models. (c) Radial profiles of the σ/Vrot ratio derived
from the CO(3–2) line of NGC 1097. The ratio of NGC
1097 is well smaller than that of the luminous AGN of
NGC 1068.

References[1] Antonucci, R.: 1993, ARA&A, 31, 473.
[2] Wada, K., Norman, C. A.: 2002, ApJL, 566, L21.
[3] Wada, K.: 2012, ApJ, 758, 66.
[4] Izumi, T., et al.: 2017, ApJL, 845, L5.
[5] Garca-Burillo, S., et al.: 2016, ApJL, 823, L12.

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033

Molecular Gas Fraction in Interacting Galaxies in Early and Mid Stage
Using 12CO(J = 1–0) Mapping Observations
KANEKO, Hiroyuki1, KUNO, Nario2, IONO, Daisuke1/3, TAMURA, Yoichi4
TOSAKI, Tomoka5, NAKANISHI Koichiro1/3, SAWADA Tsuyoshi1/6
1: NAOJ, 2: University of Tsukuba, 3: The Graduate University for Advanced Studies, 4: Nagoya University, 5: Joetsu University of Education,
6: Joint ALMA Observatory

Galaxy interactions play an important role on galaxy
evolution. An enhancement of infrared luminosity has
been observed from interacting galaxies, meaning thatstar formation activity is enhanced during the galaxy
interaction. However, the detailed mechanism of thisphenomena is still unknown. Since molecular gas is afuel of star formation, it is important to understand how
molecular gas is affected through an interaction eventfor revealing the interaction-induced star formation ininteracting galaxies.
We previously have discovered the molecular gas
distributions for four interacting galaxies in early andmid stage by mapping observations of 12CO(J = 1–0)
emission line with the Nobeyama 45-m radio telescope[1]. Molecular gas distributions are different from atomic
gas and stellar distributions: they are not concentrated
to their centre of progenitors compared with isolated
galaxies. This fact suggests that physical properties ofmolecular gas is affected even at the beginning of theinteraction.
In order to inquire detailed effects onto molecular gas
by the interaction, we investigate global molecular gas
fraction, which is defined as

new model successfully explains the observed fmol–Σtotal
relations. We conclude that higher molecular gas fraction
in interacting galaxies is achieved efficient conversion
from atomic gas to molecular gas which is by highexternal pressure. The molecular gas produced throughthis process may be an ingredient of active star formation
in interacting galaxies [3].

(1)
where MH2 and Mtotal are molecular gas and total gas(a sum of molecular gas and atomic gas) mass of thegalaxy, respectively. We find that the global molecular
gas fraction for interacting galaxies is significantly higher
than isolated galaxies, implying the conversion fromatomic gas to molecular gas by the interaction.
We further derive local molecular gas fraction fmol. fmol isexpressed by the following equation:(2)
where ΣH2 and Σtotal are the surface density of molecular
gas and total gas, respectively. Figure 1 shows f mol
distributions for four target interacting galaxies. Allinteracting systems illustrate complex fmol distributions,while an isolated galaxy has a fmol peak at the galactic
centre and fmol decreases with an increase of radius. In
order to investigate how these distributions achieved,
we perform theoretical model fitting based on [2].
Following the failure of the fitting, we include a new term
representing external pressure to the original model. Our034

I Scientific Highlights

Figure 1: Local molecular gas fraction f mol for four target
interacting galaxies.

References[1] Kaneko, H., et al.: 2013, PASJ, 65, 20.
[2] Elmegreen, B. G.: 1993, ApJ, 411, 170.
[3] Kaneko, H., et al.: 2017, PASJ, 69, 66.

Searches for New Milky Way Satellites from the Subaru/HSC Survey:
Discovery of Cetus III
HOMMA, Daisuke(NAOJ)CHIBA, Masashi

OKAMOTO, Sakurako, KOMIYAMA, Yutaka, TANAKA, Masayuki(Tohoku University)				

TANAKA, Mikito(Hosei University)

ISHIGAKI, Miho N.
(Kavli IPMU, WPI)(NAOJ)HAYASHI, Kohei(University of Tokyo)

GARMILLA, Jose A., LUPTON, Robert H., STRAUSS, Michael A.

				
				

(Princeton University)				

WANG, Shiang-Yu(ASIAA)		

The current standard theory of structure formation in
the universe, Λ model, predicts that a Milky Way (MW)sized host halo is surrounded by hundreds to thousands ofsubhalos. However, this prediction is in conflict with theobserved number of only ~50 MW satellites. This is themissing satellites problem, which is one of the unresolved
issues related to ΛCDM models. One of the possible
solutions to the missing satellites problem is that weare still undercounting the population of fainter or moredistant satellites in the MW due to various observationalbiases. Motivated by this, we have started a systematic
search for new MW satellites in the course of the Subaru
Strategic Program (SSP) using Hyper Suprime-Cam(HSC), and have already discovered an extremely faintsatellite candidate, Virgo I, from the early survey data [1].
We report here the discovery of the second new
MW satellite candidate, Cetus III, from the first two
years of HSC-SSP data [2]. It is estimated that an
absolute magnitude of Cetus III is MV ~ −2.4 mag and aheliocentric distance is ~250 kpc in the direction of theconstellation Cetus. The areas where we have discovered
Cetus III and Virgo I have been previously surveyed by
SDSS, but they are beyond the detection limit of SDSS
(Fig. 1), Therefore, the Subaru/HSC is able to discover
yet unidentified faint or distant satellites owing to its
wide and deep survey and is very effective for the searchof missing satellites.
Based on ΛCDM models, we will discover about
10 satellites in the completed HSC-SSP survey over
~1400 deg 2 (Fig. 2). Now we have disovered 2 newsatellites (Cetus III, Virgo I) from first two years data(~300 deg 2 covered), the frequency of discovery (1satellite per 100~200 deg2) is so far consistent with theprediction of ΛCDM models. In the near future, we expect
to find more new satellites, and then the completion of
HSC-SSP survey will provide important insights into thenature of dark matter and galaxy formation theory bycomparing the results of obserbation such as the number
and the spatial distribution of satellites with those of
ΛCDM models.

ARIMOTO, Nobuo(Seoul University)

MIYAZAKI, Satoshi(NAOJ)MURAYAMA, Hitoshi(Kavli IPMU, WPI)

Figure 1: The relation between MV and heliocentric distance forstellar systems. Dots denote globular clusters in the MW
and filled squares denote the MW satellites. The redand blue lines indicate the detection limits of SDSS and
HSC, respectively.

Figure 2: Black solide line denotes the cumulative luminosity
function of visible satellites in the MW-sized halocalculated from ΛCDM models. Blue solid line
considers the correction only for the sky coverage of the
HSC-SSP survey (~1400 deg2). In addition, red solid line
considers the corrections for the detection limit of HSCSSP survey.
References[1] Homma, D., et al.: 2016, ApJ, 832, 21.
[2] Homma, D., et al.: 2018, PASJ, 70, 18.

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035

Detection of Rotating Outflow Driven
by a High-mass Protostar Candidate Orion KL Radio Source I

Reference[1] Hirota, T., et al.: 2017, Nature Astronomy, 1, 146.

I Scientific Highlights

KIM, M. K.

BURNS, R. A.

(NAOJ/KASI)		

(JIVE)(a) Si18O

15

500
10

0

Radial velocity [km s-1]

(Yamaguchi University)			

(Kyushu University)

5

0

-500

100 au
-5

500

0

-500

RA offset [mas](b) H2O

15

500
10

0

Radial velocity [km s-1]

MOTOGI, K., MATSUMOTO, N.

In star-formation processes, in particular for highmass stars, it is still unclear how surrounding matters canaccrete onto central protostars. One of the unresolved
problems is to understand transfer of angular momentum
from the accreting matters, which has been regarded as“angular momentum problem”. From a theoretical pointof view, outflows and jets are predicted to play essential
roles in the transfer of angular momentum. However,observational evidences for this phenomenon are still
limited even for nearby low-mass protostars until very
recent progress, and little quantitative studies have beenpresented for high-mass stars.
We carried out observations of the nearest highmass protostar candidate in Orion KL (420 pc), Radio
Source I using ALMA, and detected a rotating outflow
ejected from a circumstellar disk. Observations weredone in ALMA cycle 2, and the high spatial resolutionof 0.1 arcseconds was achieved at band 8, 400–500 GHz.
A rotational transition of the 18O isotopologue of siliconmonoxide (Si18O) reveals the outflow showing a clear
signature of the velocity gradient perpendicular tothe outflow axis (Figure 1). It is consistent with thatof the circumstellar disk traced by the high excitation(vibrationally excited) water (H2O) line. Considering
the equilibrium of the centrifugal force and gravity, themass of the central object is estimated to be 8.7 M. The
outflow traced by the Si18O line is launched at > 10 au
radii from the central object, and the outward velocity ofthe outflow is estimated to be 10 km s–1 based on a 3Dmodel. These outflow parameters are consistent with thetheoretical model of the magneto-centrifugal disk wind
as a driving mechanism of the outflow observed in thehigh-mass protostar candidate Orion KL Source I. Our
results suggest that the outflow driven by the magnetocentrifugal disk wind would play an essential role forangular momentum transfer in high-mass star-formation
processes.

036

MACHIDA, M. N., MATSUSHITA, Y.

(NAOJ/SOKENDA)				

Dec offset [mas]		

HIROTA, T., HONMA, M.

Dec offset [mas]

		

5

0

-500

100 au
-5

500

0

-500

RA offset [mas]Figure 1: (a) ALMA band 8 continuum emission tracing the disk
(white contours), integrated intensity and radial velocity
maps of the 18O isotopologue of silicon monoxide (Si18O)
line at 484 GHz, showing the outflow driven from thedisk (black contours and color scale, respectively). (b)Same as (a) but for the high excitation (vibrationallyexcited) water (H2O) line at 463 GHz, tracing the hotrotating gas disk.

Evolutionary Phases of Gas-rich Galaxies in a Galaxy Cluster at z=1.46
HAYASHI, Masao

KODAMA, Tadayuki(NAOJ)		

TADAKI, Ken-ichi(NAOJ)		

			

HATSUKADE, Bunyo
TAMURA, Yoichi(Nagoya University)

References[1] Hayashi, M., et al.: 2017, ApJL, 841, L21.
[2] Hayashi, M., et al.: 2014, MNRAS, 439, 2571.
[3] Stanford, S. A., et al.: 2006, ApJL, 646, L13.
[4] Hilton, M., et al.: 2010, ApJ, 718, 133.
[5] Jaffe, Y. L., et al.: 2015, MNRAS, 448, 1715.
[6] Noble, A. G., et al.: 2016, ApJ, 816, 48.

(UCO/Lick Observatory) as of the publication date2 (NAOJ) as of the publication date

(University of Tokyo)

KOYAMA, Yusei, SHIMAKAWA, Rhythm1(University of Tokyo)				

Gas content of galaxies is one of fundamental
quantities directly related to the star-formation activities
in galaxies. Since it is expected that star-forming
galaxies in high-z galaxy clusters grow to massive
early-type galaxies in the local Universe, the cluster
galaxies’ gas content should allow us to better understandthe quenching mechanisms of galaxies in dense
environments.
We conducted a survey of molecular gas in galaxies
in the XMMXCS J2215.9-1738 cluster at z = 1.46 with
ALMA. We have detected emission lines from 17
galaxies within a radius of R 200 from the cluster center,in Band 3 data with a coverage of 2.33 arcmin2. The lines
are all identified as CO J = 2–1 emission lines from cluster
members at z ~ 1.46 by their redshifts and the colors of
their optical and near-infrared counterparts. This is thelargest sample of CO emission-line galaxies associatedwith a z > 1 galaxy cluster to date.
The spatial distribution of galaxies with CO(2–1)
detected suggests that they disappear from the very
center of the cluster (Figure 1). The phase-space diagram
showing relative velocity versus cluster-centric distanceindicates that the gas-rich galaxies have entered thecluster more recently than the gas-poor star-forming
galaxies and passive galaxies located in the virialized
region of this cluster (Figure 2). The results imply that thegalaxies have experienced ram-pressure stripping and/or strangulation during the course of infall towards thecluster center and then the molecular gas in the galaxies
at the cluster center is depleted by star formation. Referto [1] for further discussion.

1

KOHNO, Kotaro, YAMAGUCHI, Yuki

(Tohoku University)			

(NAOJ)SUZUKI, L. Tomoko2(Tohoku University)

Figure 1: Spatial distribution of galaxies with CO(2–1) line
detected which are shown by filled circles. The solid
curve shows a region where the ALMA Band 3 data are
available. The cross symbols show the [O II] emittersassociated with this cluster [2]. A star symbol shows acluster center [3]. The dashed circle shows the clustercentric radius of 0.5R 200 [4].

Figure 2: Phase-space diagram showing the relative line-of-sightvelocities as a function of cluster-centric distance. Red
circles show the CO(2–1) emitters. Blue symbols show
the [O II] emitters without CO(2–1) detection. Greencircles show the other spectroscopically confirmed
cluster members [4,2]. The gray region shows avirialized area defined by [5]. The gray lines show
the curves of constant v × R values [6]. (right panel)
Redshift histograms of spectroscopically confirmed
galaxies. (upper panel) Cumulative fraction of thenumber of galaxies as a function of radius from thecluster center.

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037

Morphological Evidence for a Past Minor Merger
in the Seyfert Galaxy NGC 1068
TANAKA, Ichi, YAGI, Masafumi

TANIGUCHI, Yoshiaki				 (NAOJ)				(The Open University of Japan)

NGC 1068 is one of the archetypical Type-2 Seyfert
galaxies in the local Universe. Thanks to its close
proximity (~15 Mpc) and nearly face-on configuration,
many observational studies have been done about thegalaxy.
There are two major hypotheses on how the Seyferttype Active Galactic Nuclei (AGNs) are triggered. One
mechanism attributes to the internal secular process,where the galactic disk generates the non-axisymmetricstructure (e.g., bars) which efficiently removes theangular momentum of the circulating gas to dump it to
the center. NGC 1068 indeed has the bar structure in thecenter. However, it is also known that the axis of the dust
torus around the central Supermassive Blackhole (SMBH)
is nearly perpendicular to the rotation axis of the galactic
disk. Such misalignment between the central dust torus
and the disk of host galaxy is often observed among
Seyfert galaxies. Explaining the mis-alignment is not soeasy for the triggering scenario by secular evolution.
The other hypothesis is the external trigger such as
mergers. On this standpoint, Taniguchi (1999) proposed
the AGN unification model by mergers. They discussed
that all Seyfert AGN activities were triggered by theminor merger of the nucleated (= with the SMBH at its
center) satellite galaxy [1]. When a satellite is merged tothe main galaxy, most of its body will be destroyed by thetidal field of the main galaxy. However, if it is nucleated,
its core with a SMBH can survive and go into the centerof the main galaxy to merge with the host SMBH.
During the sinking process, the gravitational interaction
can violently disturb the gas near the center of the main
galaxy, which will lead to the AGN activity. As the angleof the dust torus and the narrow line region around the
SMBH is basically determined by the orbit of the sinking
satellite, its correlation with the rotation axis of the main
disk would be weak as observed. However, no previous
studies ever detected the morphological sign of the minor
merger around NGC 1068.
We thought that the sign of minor merger might still
remain at the very outer part of the host galaxy, due to
its longer dynamical timescale. We observed NGC 1068
by Subaru in late 2016. Using the deep optical data byHyper Suprime-Cam (HSC) and Suprime-Cam, we havediscovered the very faint signatures of the past tidal
interaction for the first time [2]. This is shown in the top
panel of the Figure 1. There are two very faint ( > 27 mag
arcsec−2: r band AB) spurs near the north and the south ofthe main disk. Their morphology suggests that they are apart of the loop (see the insets at right of the Fig. 1[top]).

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Such stream structure can be made by the minor merger
occurred several Gyrs ago. And also, there are theintriguing structures on the faint outer disk. The bottom
panel of fig.1 is the contrast-enhanced image of the outerdisk structure. The one-arm structure (“Banana”) as wellas the “ripple” on the other side are clearly visible. Suchstructures are also shown to be made by the past minor
merger event several Gyr ago by the simulations (seediscussions in Tanaka et al. 2017 for more).
Our findings are consistent with the proposed idea by
Taniguchi (1999). We recently started the new imaging
survey for faint tidal signature on Seyferts by HSC. We
will expand the sample size to see how minor merger isimportant to trigger the Seyfert activity.

Figure 1: [Top] The discovered diffuse signatures aroundNGC 1068 by Subaru. Their morphology apparently
resembles a part of a loop which could be the tidal
stream (see the right two panels). The image size is
19′ × 21′. [Bottom] The contrast-enhanced view of the
faint outer disk of NGC 1068. The single-arm structure(“Banana”) and the ripple-like feature (“Ripple”) areseen. See the ref. [2] for more detail.
References[1] Taniguchi, Y.: 1999, ApJ, 524, 65.
[2] Tanaka, I., Yagi, M., Taniguchi, Y.: 2017, PASJ, 69, 90.

A Universal Correlation between Star Formation Activity
and Molecular Gas Properties across Environments
KOYAMA, Shuhei1, KOYAMA, Yusei2, YAMASHITA, Takuji1, MOROKUMA, Kana3, MATSUHARA, Hideo3/4
NAKAGAWA, Takao3, KODAMA, Tadayuki5, HAYASHI, Masao2, SUZUKI, Tomoko5
TADAKI, Kenichi2, TANAKA, Ichi2, SHIMAKAWA, Rhythm2, YAMAMOTO, Moegi4
1: Ehime University, 2: NAOJ, 3: ISAS/JAXA, 4: SOKENDAI, 5: Tohoku University

In the local universe, it is well known that the fractionof early-type galaxies increases with local galaxy density,
while that of late-type galaxies decreases [1]. This strong
correlation between galaxy properties and environment
suggests that the environment plays an important role inshaping the nature of individual galaxies. It is believedthat accelerated galaxy growth and/or efficient quenchingof star formation in high-density environments could
explain the environmental difference, but the physicalcauses (or mechanisms) responsible for the environmental
effects are still unclear.
In this study, we focused on the environmental
impacts on molecular gas properties as the origin ofenvironmental effect, and investigated the environmental
dependence of the relation between star formation
activity and molecular gas content. The galaxy sample
were selected from SDSS DR7 spectroscopic data.
We defined the galaxy environment based on the local
number density of galaxies, which is expressed as(1)(2)
where Dp, 5 is the projected comoving distance to thefifth-nearest neighbor galaxy within a redshift slice ofΔz = ±0.003, and Σ5 is the median density measured
within the same redshift slice. As shown in Figure 1, we
divided the sample into five environmental bins (D1–
D5). We selected six to seven galaxies uniformly from
D1–D5 and estimated the molecular gas mass by theCO(1–0) observations with NRO 45 m telescope. Further,by combining our sample and the COLDGASS data [2],which is the extragalactic CO survey with IRAM 30 m
telescope, we could construct the CO catalog to cover awide range in environment.
This allows us to conduct the first systematic
study of environmental dependence of molecular gas
properties in galaxies from the lowest- to the highestdensity environments in the local universe. As a result,
we confirmed that fH2 have strong positive correlation
with the SFR offset from the star-forming main sequence(ΔMS) and, most importantly, we found that these
correlations are universal across all environments (Figure2). This result demonstrated that star formation activity
within individual galaxies is primarily controlled bytheir molecular gas content, regardless of their global
environment [3].

Figure 1: The distribution of ρ5 for SDSS sample. Our definitionof D1–D5 environment bins are shown with different
color shades.

Figure 2: ΔMS–f H 2 relation for each environmental bin. For
comparison, we show the best-fitting result for D3 bin asgray dotted lines in all of the panels.

References[1] Dressler, A.: 1980, ApJ, 236, 351.
[2] Saintonge, A., et al.: 2011, MNRAS, 415, 32.
[3] Koyama, S., et al.: 2017, ApJ, 847, 137.

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An Optically Faint Quasar Survey at z~5 in the CFHTLS Wide Field:
Estimates of the Black Hole Masses and Eddington Ratios
IKEDA, Hiroyuki(NAOJ)			

KAWAKATU, Nozomu(NIT, Kure College)		

NAGAO, Tohru, KAJISAWA, Masaru(Ehime University)			

AKIYAMA, Masayuki(Tohoku University)		

In order to understand the evolution of supermassive
black holes (SMBHs), many quasars have been
discovered up to z~ 7 by the various quasar surveys (e.g.,[1]). Utilizing these quasar sample, the black hole mass(MBH) and Eddington ratio (L/LEdd) of SMBHs have beenmeasured with a wide range of redshift so far. As for thehigh redshift, MBH of SMBHs have been measured fromthe single-epoch virial estimators [2] and then L/LEdd of
SMBHs also have been measured. Utilizing these physicalparameters, a number of studies for the growth history of
the SMBHs have been investigated so far [3]. However,previous studies have been limited mostly to luminous
quasars which are likely to be high L/LEdd objects and themechanism of SMBH formation is still unclear, due to thelack of the faint quasars at high redshift. Some z~ 5 faintquasar surveys have been carried out and the faint sideof the QLF at z ~ 5 has been derived [4]. While a large
sample of faint quasars at z ~ 5 have been constructed,
the achieved signal-to-noise (S/N) ratio of the spectra
is not sufficient to derive MBH. Therefore we focus on
the public database of CFHT legacy survey (CFHTLS;[5]) to discover faint quasars with high S/N ratio of theirspectra. Among the CFHTLS-Wide fields (~145 deg2), we
specifically focus on a ~6 deg2 area that is covered also by
the United Kingdom Infrared Telescope (UKIRT) Infrared
Deep Sky Survey (UKIDSS; [6])-Deep Extragalactic
Survey (DXS) to select faint quasars effectively. Utilizingthese photometric data, we select nine photometriccandidates and identify three z~ 5 faint quasars, one z ~4
faint quasar, and a late-type star. Since two faint quasar
spectra show C IV emission line without suffering from aheavy atmospheric absorption, we estimate MBH and L/
LEdd of them. The inferred log MBH are 9.04 ± 0.14 and8.53 ± 0.20, respectively. In addition, the inferred log L/
LEdd are −1.00 ± 0.15 and −0.42 ± 0.22, respectively. If
we adopt that L/LEdd = constant or ∝ (1+z)2, the seedblack hole masses (Mseed) of our z ~ 5 faint quasars are
expected to be >105M in most cases (Figure 1). We also
compare the observational results with a mass accretion
model where angular momentum is lost due to supernova
explosions [7]. Accordingly, MBH of the z~5 faint quasars
in our sample can be explained even if Mseed is ~103M.
Since z ~ 6 luminous quasars and our z ~ 5 faint quasars
are not on the same evolutionary track, z ~ 6 luminous
quasars and our z~ 5 quasars are not the same populations
but different populations, due to the difference of a periodof the mass supply from host galaxies [8].

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MATSUOKA, Kenta

MIYAJI, Takamitsu(UNAM)		

(University of Firenze)

MORKUMA Tmoki(University of Tokyo)

Figure 1: Evolutionary tracks of the SMBHs in our sample. Upperand lower panels show MBH vs. t Universe. Solid and dashedlines show the evolutionary tracks for η= 0.1 and η=0.3,
respectively.
References[1] Matsuoka, Y., et al.: 2016, ApJ, 828, 26.
[2] Shen, Y., et al.: 2011, ApJS, 194, 45.
[3] Trakhtenbrot, B., et al.: 2011, ApJ, 730, 7.
[4] McGreer, I. D., et al.: 2013, ApJ, 768, 105.
[5] Gwyn, S. D. J.: 2012, AJ, 143, 38.
[6] Lawrence, A., et al.: 2007, MNRAS, 379, 1599.
[7] Kawakatu, N., Wada, K.: 2008, ApJ, 681, 73.
[8] Ikeda, H., et al.: 2017, ApJ, 846, 57.

Pilot KaVA (KVN and VERA Array) Monitoring of the M87 Jet
HADA, Kazuhiro, KINO, Motoki

		(NAOJ)			

PARK, Jongho(SNU)		KaVA AGN Science Working Group(https://radio.kasi.re.kr/kava/about kava.php)

Very long baseline radio interferometer (VLBI) is a
powerful tool for observing nonthermal radio sourcesin the Universe. In particular, VLBI plays a key role instudying relativistic jets in active galactic nuclei (AGN),
since the high-resolution capability allows us to directly
access the scales of jet formation and acceleration.
The KVN and VERA Array (KaVA) is the first
regularly operated international VLBI network in East
Asia, consisting of a total of 7 radio telescopes. A featureof KaVA is that the array operates for a quasi-full year.
This offers an ideal opportunity to monitor the structural
evolution of relativistic jets via detailed multi-epoch
observations.
In order to promote early science with KaVA, here wefocused on the active galaxy M87. M87 is a giant radiogalaxy located at the center of the Virgo cluster and oneof the nearest AGN jets. Thus we can directly resolve
scales of initial jet formation very close to the black holeby using VLBI.
From December 2013 to June 2014, we performed
KaVA 22 GHz monitoring observations of the M87 jetat intervals of 2–3 weeks. In Figure 1 we show multiepoch KaVA images of M87 obtained by this program.
We successfully acquired high-quality jet images at manyepochs. As a result, we discovered that the jet speed
gradually transitions from subluminal to superluminal
motions around distances of several hundred
Schwarzschild raii (Rs) to thousands of Rs from the black
hole. The observed location of the superluminal motions
is much closer to the jet base than that seen in previous
studies. This suggests that the efficient acceleration of thejet is already started from much closer to the black holethan previously thought.
This initial result demonstrates that KaVA is indeed
a powerful instrument for studying relativistic jets. We
will further continue our monitoring of M87 by KaVA or
EAVN to reveal more detailed velocity fields of this jet.

Figure 1: Multi-epoch KaVA 22 GHz images of the M87 jet
obtained between January 2013 and June 2014 [1].

Reference[1] Hada, K., et al.: 2017, PASJ, 69, 71

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041

The Shortest Periodic and Flaring Activity of the 6.7 GHz Methanol
Maser in the Intermediate-mass Protostar G 014.23–00.50
SUGIYAMA, Koichiro, HONMA, Mareki, UCHIYAMA, Mizuho, HACHISUKA, Kazuya, MATSUMOTO, Naoko(NAOJ)NAGASE, Katsura, YONEKURA, Yoshinori, MOMOSE, Munetake, YASUI, Yasutaka, SAITO, Yu(Ibaraki University)

MOTOGI, Kazuhito, FUJISAWA, Kenta(Yamaguchi University)

To statistically investigate the periodic flux variabilityof methanol masers at 6.7 GHz around protostars [1],we have initiated a single-dish monitor project using
the Hitachi 32-m radio telescope since 30 December
2012 [2]. Target sources consist of 442 methanol masers,
declination of which is upper than −30 deg. Here, wereport the shortest periodic and flaring flux variabilityof the 6.7 GHz methanol maser newly detected in theintermediate-mass protostar G 014.23–00.50 via themonitor until 21 January 2016 [3].
The 6.7 GHz methanol maser in G 014.23–00.50
shows seven spectral components at V lsr = 20.98–
25.30 km s −1. We newly detected characteristic f lux
variability in only one of them at Vlsr = 25.30 km s−1,
those are flaring and periodic one. The flaring activities
were detected via comparing to non-detection durations
below the detection limit (3σ ~ 0.15 Jy in the case of an
integration with all the data in each observational date).
Their time-scale of the flux rising was typically a few
days or shorter (21 hrs at the shortest) and the ratio of thepeak flux density was more than 180 in comparison witha quiescent phase (Figure 1). The periodicity of theseflaring activities was also detected with the period of
23.9 ± 0.1 days, which has persisted in at least 47 cycles(Figure 2). This period is the shortest one observed inmasers at around intermediate-/high-mass protostars so far.
We conclude that the flaring and intermittent periodic(the period of 23.9 days) flux variability detected in only
one spectral component might be explained by a periodic

change in the flux of seed photons or a periodic variationof the dust temperature via an extra heating source ofa shock formed in the colliding-wind binary model [4],in which the orbital semi-major axes of the binary are
0.26–0.34 au.

Figure 1: Example of the flaring activities detected at V lsr =25.30 km s−1. The horizontal axis is observational dates
relative to the reference date of 8 September 2015.
References[1] Goedhart, S., et al.: 2004, MNRAS, 355, 553.
[2] Yonekura, Y., et al.: 2016, PASJ, 68, 74.
[3] Sugiyama, K., et al.: 2017, PASJ, 69, 59.
[4] van der Walt, D. J.: 2011, AJ, 141, 152.

Figure 2: Periodic flux variation detected at Vlsr = 25.30 km s−1. Solid and dashed vertical lines show the expected flaring dates with andwithout observational data.

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Polarization Calibrationof the Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP)
for a 0.1 % Polarization Sensitivity in the VUV Range
GIONO, G., ISHIKAWA, R., NARUKAGE, N., KANO, R., KATSUKAWA, Y., KUBO, M.
BANDO, T., HARA, H., SUEMATSU, Y.
(NAOJ)WINEBARGER, A., KOBAYASHI, K., CIRTAIN, J.

			(MSFC/NASA)			

TRUJILLO BUENO, J., ASENSIO RAMOS, A.

			

MANSO SAINZ, R.

(IAC)				CHAMPEY, P.

(University of Alabama)ŠTĚPÁN, J.
(ASCR)ISHIKAWA, S., TSUNETA, S., SHIMIZU, T., SAKAO, T.

(MPS)					ICHIMOTO, K.

(Kyoto University)AUCHÈRE, F.
(CNRS)BELLUZZI, L.
(IRSL&KIS)(ISAS/JAXA)					CARLSSON, M.

(University of Oslo)

The Chromospheric Lyman-Alpha SpectroPolarimeter(CLASP) is a sounding rocket instrument designed tomeasure for the first time the linear polarization of thehydrogen Lyman-α line at 121.6 nm. The instrument
was successfully launched on 3 September 2015 andobservations were conducted at the solar disc centerand close to the limb during the five-minutes flight. The
disc center observations are used to provide an in-flightcalibration of the instrumental polarization. The derived
in-flight instrumental polarization is consistent with the
spurious polarization levels determined during the preflight calibration (Giono et al., 2016) and a statisticalanalysis of the polarization fluctuations from solar
origin is applied to ensure a 0.014 % precision on the
instrumental polarization (Figure 1). The combination of
the pre-flight with the in-flight polarization calibrations
provides a complete picture of the instrument response
matrix, and a proper error transfer method is used toconfirm the achieved polarization accuracy. As a result,the unprecedented 0.1 % polarization accuracy of the
instrument in the vacuum ultraviolet is ensured by thepolarization calibration.

CASINI, R.

(HAO/NCAR)De PONTIEU, B.
(LMSAL)

GOTO, M.
(NIFS)

Figure 1: Stokes I’, Q’/I’ and U’/I’ profiles obtained at disc center
for a full slit spatially summed and three polarizationmodulator rotations temporal summing, for bothorthogonal polarization channels. Horizontal red solidlines show the expected spurious polarization offsetsfrom the pre-flight calibration, with red dashed lines
showing the ±1σ error. Vertical black solid lines show
the line core (i.e. ±0.02 nm around the line center). Error
bars shown in blue on the polarization signals indicate
the noise (1σ), including the photon noise, the read-out
noise, and the error due to the residual polarization fromthe Sun for the full slit spatially summed. By applying astatistical analysis of the polarization fluctuations fromsolar origin, a 0.014 % precision on the instrumental
polarization is ensured.

References[1] Giono G., et al.: 2016, Solar Phys., 291, 3831-3867.
[2] Giono G., et al.: 2017, Solar Phys., 292, 57.

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Strong Magnetic Field Generated by
the Extreme Oxygen-rich Red Supergiant VY Canis Majoris
						

SHINNAGA, Hiroko

CLAUSSEN, Mark, J.

YAMAMOTO, Satoshi

SHIMOJO, Masumi(Kagoshima University)		
(The University of Tokyo)		

Evolved stars experience high mass-loss rates forming
thick circumstellar envelopes (CSEs). The circumstellar
material is made of the result of stellar nucleosynthesis
and, as such, plays a crucial role in the chemical
evolution of galaxies and the universe. Since asymmetricgeometries of CSEs are common, and with very complex
structures for some cases, radiative pressure from thestars can explain only a small portion of the mass-loss
processes; thus the essential driving mechanism is still
unknown, particularly for high-mass stars. Here we reporton magnetic field measurements associated with the wellknown extreme red supergiant (RSG), VY Canis Majoris(VY CMa). We measured the linear polarization and the
Zeeman splitting of the SiO v= 0, J = 1–0 transition, using
a sensitive radio interferometer. The measured magnetic
field strengths are surprisingly high; their upper limits
range between 150 and 650 Gauss within 530 AU (~80 R*)
of the star. The field strength of lower limit is expected to
be at least ~10 Gauss based on the high degree of linear
polarization. Since the field strengths are very high, themagnetic field must be a key element in understanding
the stellar evolution of VY CMa as well as the dynamical
and chemical evolution of the complex CSE of the star.
M-type supergiants, with large stellar surface, were
thought to be very slow rotators. This would seem tomake a dynamo in operation difficult and would also
dilute any fossil magnetic field. At least for VY CMa,
we expect that powerful dynamo processes must still be
active to generate the intense magnetic field [1].
The CSE of VY CMa has exceptionally strong SiO
lines - most of them are masers - in many rotationaltransitions in multiple vibrational states, along withstrong H2O maser emission [2], over a wide range ofenergy levels, up to ~7,000 K for SiO and ~7,800 K for
H2O. Furthermore, many SiO lines associated with the
CSE are highly polarized, both in circular [3] and linear
polarization ([1] and references therein), from a few
percent up to >~ 60 % in linear polarization. This highdegree of polarization is even detected in low rotationaltransitions in the ground vibrational state [4], which isusually of thermal origin, as the v=0, J= 1–0 and 2 energy
levels are only 2 K and 6 K above ground, respectively.
Zeeman effect in SiO v = 0, J = 1–0 emission was
detected for the first time from an astronomical object.
Along with well-ordered magnetic field pattern measured
with high degree of linear polarization, the observational044

I Scientific Highlights(NRAO)(NAOJ)

Figure 1: Channel maps of SiO v = 0, J = 1–0 emission (contours
drawn at (9, 27, 81, 243, 729) times of 1σ noise levelof 6.8 × 10 −3 Jy/beam; 0 ″. 29 x 0 ″. 12 beam size) withpolarization vectors (black/white bars) measured with
the VLA. Vlsr is written on the top left corner of eachpanel. The polarized intensity unit (grey scale) of the top
left panel and that of the rest panels are in mJy/beam andin Jy/beam, respectively. Polarization vectors are plottedwhen the signal-to-noise ratio for intensity is above 8
sigma. Each clump and the stellar location ([2]; orange
circle, measured with ALMA) are noted.

results presented here strongly indicates that thisenigmatic O-rich RSG VY CMa has a very intense
magnetic field of from 10 Gauss up to 150–650 Gauss.
Future observations will further constrain the magnetic
field strengths to understand the physics of high massloss rate and the stellar evolution of high-mass stars justbefore supernova explosion.

References[1] Shinnaga, H., et al.: 2017, PASJ, 69, L10.
[2] Richards, A. M. S., et al. 2014, A&Ap, 572, L9.
[3] Barvainis, R., McIntosh, G., Predmore, C. R.: 1987, Nature,329, 613.
[4] Shinnaga, H., Tsuboi, M., Kasuga, T.: 1999, PASJ, 51, 175.

Big-Bang Lithium Problem, and Effects of Long-Lived Negatively
Charged Massive Particles on Primordial Nucleosynthesis
KUSAKABE, Motohiko, MATHEWS, Grant J.
(University of Notre Dame)		

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

We reviewed the big bang nucleosynthesis (BBN)
model including a long-lived negatively charged massive
particle, i.e., X − [1]. The mass of the X −, mX, is assumed
to be much larger than the nucleon mass. This model
provides a reason why observed 7Li abundances of metalpoor stars are smaller than that predicted in the standard
BBN (SBBN) model [2]. Since the primordial 9 Be
abundance can be larger than that of the SBBN model,
the existence of the X − particle can be tested by future
observations of 9Be in metal-poor stars [3].
The 7Be nuclei are destroyed via a recombination
with the X − followed by a radiative proton capture, i.e.,
7Be(X −, γ) 7Be (p, γ) 8B [2]. Since the primordial 7Li
X
X
nuclei predominantly originate from 7Be nuclei produced
during BBN, this 7Be destruction reduces the primordial
7Li abundance. Rates for recombination of 7Be and X −were calculated accurately, and the dominant transition isthe d-wave → 2P for mX >~ 100 GeV [3].
Figure 1 shows the energy level diagram of 7Be X
for mX = 1 TeV [1]. Red and blue arrows show the threeimportant transitions in the nonresonant recombination
reaction, while purple and green arrows show decays ofthe two main resonances into bound states of 7BeX* (of thenuclear excited state) in the resonant reaction.
Based on the detailed reaction network calculationsof BBN, the most realistic constraints on the X − particle
were derived [3]. Parameter regions for the solution to the
7Li problem were identified: the X − to baryon ratio is YX
3>
~ 0.04 and the lifetime is τX ~ (0.6–3) × 10 s. Using thisresult, possible candidates of X − particle are considered[1]. One candidate is a slepton, i.e., a supersymmetricpartner of lepton, and the other is a Kaluza-Klein (KK)
leptons, i.e., excited states of leptons realized in extradimensional models [4]. We focus on the situation thatthe slepton can only decay into the gravitino, and the KK
leptons can only decay into the KK graviton.
The thermal relic abundance of the long-lived stau [5]can be consistent with the parameter region for the 7Li
reduction if the stau mass is O(1) TeV. In addition, thelifetime of the sleptons [4] can be close to ~103 s if themasses of sleptons and the gravitino are of order TeV.
The slepton decay induces nonthermal
nucleosynthesis and gravitino production. Constraints
from electromagnetic energy injection at the decay andthe gravitino energy density [5] lead to a very narrow
parameter region. This region for the 7Li problem is

CHEOUN, Myung-Ki(Soongsil University)

available for a selectron and a smuon. However, the stau
has a certain hadronic branching ratio at the decay [4].
Hadronic energy injection is heavily constrained [6], andthe interesting parameter region is excluded in the stau
scenario.
Similarly, a solution to the Li problem exists for thecases of KK electron and muon, while it does not exists
for the case of the KK tau [1].

Figure 1: The energy level diagram of the exotic atom 7BeX form X = 1 TeV [1]. Red and blue arrows show the threeimportant transitions in the nonresonant recombination
reaction. Purple and green arrows show decays of thetwo main resonances into atomic bound states of 7BeX* (ofthe nuclear excited state 7Be*) in the resonant reaction.

References[1] Kusakabe, M., et al.: 2017, Int. J. Mod. Phys. E, 26, 1741004.
[2] Bird, C., et al.: 2008, Phys. Rev. D, 78, 083010.
[3] Kusakabe, M., et al.: 2014, ApJS, 214, 5.
[4] Feng, J. L., et al.: 2003, Phys. Rev. D, 68, 063504.
[5] Asaka, T., et al.: 2000, Phys. Lett. B, 490, 136.
[6] Kawasaki, M., et al.: 2005, Phys. Rev. D, 71, 083502.

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Big Bang Nucleosynthesis and Modern Cosmology
MATHEWS, Grant J., KUSAKABE, Motohiko			(University of Notre Dame)

Big bang nucleosynthesis (BBN) is the testing groundupon which many cosmological models must ultimately
rest [1]. A key quantity for BBN is the baryon-to-photon
number ratio η which is constrained from observations ofcosmic microwave background (CMB) radiation.
A popular explanation for the flat universe and thenear isotropy of CMB comes from an epoch of rapid
inflation in the early universe. In some special kindof inflationary model which involves non-minimal
coupling between matter and gravity, the universe makes
a transition from an inflation driving potential to a darkenergy producing quintessence. BBN study can put asignificant constraint on this model as the nonminimal
couplings lead to an excess energy density in gravity
waves which alter the predicted light element abundances[2].
In addition, a large extra-dimension affects the
dynamics of the universe and BBN. In a RandallSundrum II braneworld cosmology, the cosmic expansion
rate for a 3-space embedded in a higher dimensional
space can be written with a simple equation including
additional terms to that of the 3-space dimensionalcase. The modified term includes the dark radiation
term that scales as a −4 with a the scale factor of theuniverse. Because of this scaling almost similar to that ofnormal radiation, it can significantly alter the fit to BBN
abundances and the CMB, and hence, can be constrained[3].
Figure 1 shows the latest constraint on the darkradiation in the ρDR/ρ vs. η plane [3]. Here, ρDR is theenergy density of the dark radiation, and ρ is the totalenergy density of relativistic particles. Dark and lightshaded region are the allowed region from observationsof the primordial D and He abundances, respectively.
Contour lines show the 1, 2 and 3σ confidence limits fromfits to the CMB power spectrum. Some papers refer toinvisible relativistic particles including neutrinos as darkradiation. However, they are completely different fromextra-dimensional dark radiation. The former clumps in
the universe while the later does not. Their effects on the
CMB temperature fluctuation are then different [3].
Many papers have considered the possibility
that BBN could constrain a first-order quantum
chromodynamics transition. However, a large effect on
BBN from the transition is probably not possible since
results from lattice gauge theory seems to rule out a firstorder transition at low baryon density. Nevertheless, thepossibility of baryon inhomogeneities during BBN arisingfrom other mechanisms remains a viable possibility [4].

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KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

A time dependence of fundamental constants in an
expanding universe appears in theories that attempt tounify gravity and other interactions. BBN is sensitive
to variations in the the average light quark mass. A
re-evaluation of the effects on BBN from the quark
mass variation was performed taking into account an
independent evaluation of the resonant 3He(d,p) 4He
reaction rate based upon the forward and reverse reaction
dependence on the quark mass. The newer abundance
constraints narrow the range of possible variations in thequark mass, and the deduced range is consistent with lessthan a 0.7 % variation in the averaged quark mass [5].

Figure 1: The calculated constraint on the dark radiation in theparameter plane of ρDR/ρ and η [3], where ρDR is theenergy density of the dark radiation, and ρ is the totalenergy density of relativistic particles. Dark and lightshaded region are the allowed regions from observationsof the primordial D and He abundances, respectively.
Contour lines delineate the 1, 2 and 3σ confidence limits
from fits to the CMB power spectrum.

References[1] Mathews, G. J., Kusakabe, M., Kajino, T.: 2017, Int. J. Mod.
Phys. E, 26, 1741001.
[2] Yahiro, M., et al.: 2002, Phys. Rev. D, 65, 063502.
[3] Sasankan, N., et al.: 2017, Phys. Rev. D, 95, 083516.
[4] Nakamura, R., et al.: 2017, Int. J. Mod. Phys. E, 26, 1741003.
[5] Cheoun, M.-K., et al.: 2011, Phys. Rev. D, 84, 043001.

The New Hybrid BBN Model with the Photon Cooling, X Particle,
and the Primordial Magnetic Field
YAMAZAKI, Dai G.

(Ibaraki University/NAOJ)			KUSAKABE, Motohiko(University of Notre Dame)

MATHEWS, Grant J.

(University of Notre Dame)		

The Big bang nucleosynthesis theory accurately
reproduces the abundances of light elements in the
Universes, except for 7Li abundance. Calculated 7Li
abundance with the baryon to photon ratio fixed by theobservations of the cosmic microwave background (CMB)
is inconsistent with the observed lithium abundances on
the surface of metal-poor halo stars, and this problem
is called “7Li problem”. Previous studies proposed toresolve this 7Li problem include photon cooling (possibly
via the Bose-Einstein condensation of a scalar particle),
the decay of a long-lived X particle (possibly the next-tolightest supersymmetric particle), or an energy density ofa primordial magnetic field (PMF) [1,2].
We then used a maximum likelihood analysis toconstrain the parameters of the X particles and the energy
density of the PMF by the observed abundances of lightelements up to Li (Fig. 1) [3].
As a result, we obtained allowed ranges for the
X-particle parameters and find that the new hybrid modelwith a PMF gives the better likelihood than that without a
PMF (Table 1:) [3].
We d i s c u s s e d t h e d e g e n e r a c y b e t w e e n t h eparameters of the X particle and the PMF. Since the X
particle parameters are mainly limited by the D and
7 $Li abundances, while the PMF energy density ismainly limited by the 4He abundance, we found thatthe parameters of the PMF and the X particle have nosignificant degeneracies [3].
We also discussed the effective number of neutrino
species N eff with our new hybrid model. Since theconstraint on Neff from the CMB observations is different
from the N eff value in our hybrid model which isconsistent with the observed light elements, it is difficult
to directly compare these two Neff values. We will report a
new limit on Neff derived by taking into account analyses
of both BBN and the CMB simultaneously in our future
work [3].

KAJINO, Toshitaka(NAOJ/The University of Tokyo/Beihang University)

CHEOUN, Myung-Ki(Soongsil University)

Figure 1: Allowed region in the (τX, ζX) plane by the observational
constraints on the light element abundances for η =4.57 × 10−10 and B = 1.89 μG. The curves denote theallowed regions derived from observational limits
on the primordial elemental abundances. The narrowdark band and the region bounded by the solid curves(color version: blue and aqua regions) show the 2σ(95 %) confidence limits determined from the observed
abundances of D and 7Li, respectively. Dashed, dotdashed and dotted curves (color version: purple, orange
and black curves) are the 2σ (95 %) confidence limits
determined from the upper limits on the 3He, 4He and6
Li abundances.

Table 1: Agreement with observed light element abundances forthe four models considered here.
Model
Nuclide
Yp
D/H
3He/H
7Li/H
6Li/H

γ-cooling

X

PMF












?


(high)γ-cooling+X+PMF
(high)References[1] Yamazaki, D. G., Kusakabe, M.: 2012, Phys. Rev. D, 86,
123006.
[2] Yamazaki, D. G., et al.: 2014, Phys. Rev. D, 90, 023001.
[3] Yamazaki, Dai G., et al.: 2017, Int. J. Mod. Phys. E, 26,1741006.

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PENTACLE: Parallelized Particle-particle Particle-tree Codefor Planet Formation
IWASAWA, Masaki(RIKEN)			

OSHINO, Shoichi(NAOJ)		

Terrestrial planets (Earth and Venus), solid core ofgas planets (Jupiter and Saturn) and ice planets (Uranus
and Neptune) form through collisions and coagulation
between planetesimals (km-sized rocky and icy clumps).
The accumulation process of planets is controlled bygravitational interactions between the celestial bodies.
According to previous studies, planetary accretion has a
two-staged growth mode [1,2]: (i) “runaway growth stage”
in which planetesimals grow rapidly and (ii) “oligarchic
growth stage” in which larger planetesimals, the so-called
protoplanets, continue to slowly grow at orbital separationsof several Hill radii. Today, the theoretical framework ofthese planetary growth process is widely accepted for the
standard formation scenario of not only the solar systembut also extrasolar planetary systems discovered in recent
years. However, past studies on planet formation assumed“extremely large planetesimals” (about 1 / 10th of the planetsize) and planetary embryos at the initial state because of
the limited number of particles used in N-body calculations.
According to previous studies on time evolution of the size
distribution in a swarm of planetesimals, a typical size of aplanetesimal is 1–10 km in radius, which are two orders ofmagnitude larger than ones assumed in previous studies andobserved asteroids such as Itokawa with ~1 km in diameter.
In fact, planetary accretion in a swarm of small planetesimals
can may not follow the conventional oligarchic growth (e.g.
[3]). Thus, it is necessary to develop a new approach that canhandle such small planetesimals, namely, at least 100 millionof particles in N-body simulations for planet formation.
In this research [4], we have newly developed a large
scale N-body simulation code for planet formation. This
code is named PENTACLE, it is freely available on GitHub.
In the past planetary N-body simulations, it was difficult
to calculate such that the number of particles exceeds 100
thousand due to limitation of calculation speed. In the
N-body calculation, the cost of gravity computation of O(N2)per time integral of particle motion occurs (100,000 gravity
calculations / 1 step for 10,000 particles). In a collisionlesssystem which close encounters of particles do not occur, e.g.,a large-scale structure of the universe, N-body calculations
using about 2 trillion particles have been done [5]. This isbecause the computation cost is kept to O(N log N) by thetree method which calculates efficiently gravity forces fromdistant particles and the number of steps required for time
integration of particle motion can be reduced. On the other
hand, in the “collisional system” where close encountersof particles happen, e.g., star cluster and planetary system,
dynamical evolution of the system should be calculated using
short time steps (enormous number of steps). Therefore,

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I Scientific Highlights

FUJII, Michiko

HORI, Yasunori(The University of Tokyo) (Astrobiology Center/NAOJ)

about 100,000 particles in the collisional system are thelimits of the number of particles that can be computed.
Figure 1 shows the computation time per step whenN-body simulations of terrestrial planet formation using
1 million particles is executed with PENTACLE. The
horizontal axis shows the number of cores used for the
calculations, which scales to about 1000 cores. As thenumber of cores increases, the load of data communication
limits the computation speed. We will optimize this partand aim to utilize a larger number of cores in the future.
Figure 2 shows the time evolution of the energy error whenchanging the parameters that determine the calculation
speed and accuracy. It turns out that N-body simulations
using PENTACLE can sufficiently suppress energy errors byadopting appropriate parameters.

Figure 1: The calculation time per Kepler time against the numberof CPU cores.

Figure 2: Relative energy error as a function of time.

References[1] Kokubo, E., Ida, S.: 1998, Icarus, 131, 171.
[2] Kokubo, E., Ida, S., Makino, J.: 2000, Icarus, 148, 419.
[3] Kobayashi, H., et al.: 2010, Icarus, 209, 836.
[4] Iwasawa, M., et al.: 2017, PASJ, 69, 81.
[5] Ishiyama, T., Nitadori, K., Makino, J.: 2012, SC12.

Production of Left-handed Amino Acids in Spacein the Supernova Neutrino Amino Acid Processing (SNAAP) Model
BOYD, Richard			(Ohio State University)			(University of Tokyo)

ONAKA, Takashi

The ability of the Supernova Neutrino Amino Acid
Processing (SNAAP) model to produce enantiomericamino acids in space has been studied in detail [1]. Thismodel uses the magnetic field from a source object suchas a neutron star, along with the Lorentz force electricfield from the motion of objects in the magnetic field, todistinguish between the two chiral states of amino acids.
Then the electron antineutrinos from a neutron star or asupernova selectively destroy one chirality, producing
enantiomeric amino acids in nearby meteoroids.
In the present paper, several possible sites that could
produce the requisite conditions for the SNAAP model
were studied to determine their viability for processing
meteoroids so as to produce left-handed favoring aminoacids. Several sites appear to provide the requisite
magnetic field intensities and electron anti-neutrino
fluxes, although other factors constrain their viability.
Perhaps the most obvious site would be a corecollapse supernova; they produce both a strong magnetic
field and an intense electron antineutrino flux. However,this site alone cannot serve as the SNAAP model source.
The magnetic field from the nascent neutron star when
the supernova occurs was found to be effective out toonly about 1 percent of an A.U., while the star would
expand to about 100 times that radius when it entered its
red giant phase, surely cooking any preexisting aminoacids, and preventing any new ones from being made.
A more likely candidate is a close binary system
consisting of a neutron star and a massive star. The
latter would shed its outer one or two layers to form an
accretion disk around the neutron star, converting themassive star to a Wolf-Rayet star, circumventing the red
giant expansion of the massive star. The dense matter in
the accretion disk is thought to develop into dust grains,meteoroids, and even planets, and amino acids could becreated in these objects as they formed in the outer layersof the disk. The magnetic field necessary for the SNAAP
model would result from the neutron star. Electron
antineutrinos might be provided over long periods oftime from the neutron star, but might also occur from theburst that would be produced when the WR star became
Type Ib or Ic supernova. Other possible candidates, e.g.,
merging neutron stars, were also studied, but have larger
parameter uncertainties.
A recent paper [2] suggests, from the local 26 Al
abundance, that the Solar System was formed from a

FAMIANO, Michael(NAOJ/Western Michigan University)

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

WR star. While this isn't exactly the binary system that
we concluded was necessary for the SNAAP model,
the needs of the SNAAP model do not preclude theWR star that study concludes formed the Solar System.
Furthermore, similarities are sufficiently striking toconclude that this second paper might serve to confirm, atsome level, the SNAAP model.
These results have obvious implications for the originof life on Earth.

References[1] Famiano, M. A., et al.: 2018, Astrobiology, 18, 190.
[2] Dwarkadas, V. V., et al.: 2017, ApJ, 851, 147.

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Selection of Amino Acid Homochirality in Stellar Environments
FAMIANO, Michael		(NAOJ/Western Michigan University)

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

BOYD, Richard(Ohio State University)

ONAKA, Takashi(University of Tokyo)

Because they are asymmetric, amino acids (anexample of which is shown in Figure 1) have two chiralstates - or mirror images - referred to as “left-handed” and“right-handed” forms. With very few notable exceptions,nearly all life on earth utilizes only left-handed aminoacids, a phenomenon referred to as biomolecularhomochirality. Additionally, analyses of inclusions
in meteoritic carbonaceous chondrites have revealed
numerous amino acids. The discovery that meteorites
not only contain amino acids, but can have amino acids
favoring left handed amino acids is a possible indicatorthat amino acid chiral selection may have extra-terrestrial
origins and has led to several hotly contested theories.
Some of the amino acids so synthesized have an excess
of a few percent of the left-handed chirality that isobserved in earthly amino acids. It is generally acceptedthat if some mechanism can introduce an imbalance inthe populations of the left- and right-handed forms of
any amino acid, successive autocatalysis can amplify thisenantiomeric excess to ultimately produce a single form.
What is not well understood is the mechanism by which
the initial imbalance is produced and the means by which
it produces the left-handed chirality observed in theamino acids. The origin of biomolecular homochirality is
one of the top questions in science today [1].

MO, Yirong(Western Michigan University)

A model has been created which predicts the origins
of amino acid homochirality in an emergent stellar
phenomenon involving lepton interactions in magnetic
fields [2]. Multiple sites capable of implementing thismodels have been proposed [3].
The results of an evaluation are shown in Figure 2 forthe amino acid isovaline (in cationic form) for a scenario
representing conditions of a meteoroid in the vicinity of aneutron star. The antineutrino reaction rates are given by
the ratios f = 0, 0, 10−9, 5×10−9, 10−8, 2×10−8, and 5×10−8,
where f is defined as the ratio of the neutrino interaction
rate to the nitrogen nuclear spin relaxation rate.

Figure 2: Enantiomeric excess of isovaline in a high-field,
high flux environment for several different neutrino
interaction rates.

In this figure, the relative amount by which one chiralstate outnumbers another is given by the “enantiomeric
excess,” ee, defined as ee ≡ (NL−ND)/(NL+ND) where
N L and N D represent the number of left- and righthanded amino acids, respectively, of a specific type inan ensemble. The ees computed in this model are similar
to those found in meteorites. It is possible that aminoacid ees have their origin in space, while subsequent
autocatalysis via chemical or biological means canincrease the ee to the homochiral values observed today.

Figure 1: The left-handed enantiomer of the amino acid, alanine,L-alanine. The amine group is indicated by the dashedarrow and the carboxyl group by the solid arrow.

050

I Scientific Highlights

References[1] Kennedy, D., Norman, C.: 2005, Science, 309, 78.
[2] Famiano, M. A., et al.: 2018, Astrobiology, 18, 190.
[3] Boyd, R. N., et al.: 2018, ApJ, 856, 26.

Short-baseline Electron Antineutrino Disappearance Studyby Using Neutrino Sources from 13C + 9Be Reaction
SHIN, Jae Won, CHEOUN, Myung-Ki(Soongsil University)

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)		

Over the past few decades, a considerable numberof studies has been done on the neutrino oscillation witha great success of measuring neutrino mixing angles.
However, some experiments (LSND, MiniBoone, reactor
experiments and gallium experiments) for the neutrino
oscillation revealed more or less disagreements with thethree-flavor neutrino model, which termed as neutrino
anomalies. One of the approaches for explaining theanomalies is to presume the existence of the hypothetical
fourth neutrino (sterile neutrino) because the sterile
neutrino does not interact with other particles except for amixing with active neutrinos.
In our work [1], to investigate the existence of sterile
neutrino, we propose new experimental setup (see figure1) and electron antineutrino source using 13C beams based
IsoDAR concept. The neutrino source is obtained throughβ− decays of unstable isotopes which are generated fromthe 13C + 9Be reaction. Main isotopes (8Li, 9Li, 12Be, 12B,
and 13B) for neutrino production have similar half-lives
and reaction Q values of β− decay, and thus the neutrinoenergy spectrum with a single broad peak is expected.
The production yields of those isotopes arecalculated using three different nucleus-nucleus (AA)reaction models [1]. Even though different yields ofthe isotopes are obtained from the models, the neutrino
spectra are almost identical. This unique feature givesa realistic chance to neutrino oscillation study throughshape analysis, regardless of the theoretical AA models
considered.
Ratios of the expected total event rate for the P3+1
model to that for the P3 model (R3+1-to-R3) at L = 13 m
and L = 21 m show distinguishable features of theevent rates (see Figure 2), and thus it can also give ameaningful signal for the existence of the hypothetical νs.
The expected deviation between the maximum and theminimum values is approximately 17 %, and thus it cangive an effective answer of whether P3+1 models is themost appropriate model for the sterile neutrino.

HAYAKAWA, Takehito(QST / NAOJ)

Figure 1: A schematic view showing proposed short baseline
experiment setup.

Figure 2: Ratios of R3+1-to-R3 with respect to Eν‒e at different L are
shown.

Reference[1] Shin, J. W., et al.: 2017, J. Cosmol. Astropart. Phys., 04, 044.

I Scientific Highlights

051

II Status Reports of Research Activities
1. Subaru Telescope
1. Subaru Telescope Staff
As of the end of FY 2017, the Subaru Telescope staff
consisted of 19 dedicated faculty members including sevenstationed at Mitaka, four engineers, two specially appointed
senior specialist, and three administrative staff members.
Additional staff members include one specially appointed
research staff, seven specially appointed senior specialist, one
research expert, and six administration associates, all of whomare stationed at Mitaka. Moreover, 14 research/teaching staff
members, 13 of whom are stationed at Mitaka and one of whomis stationed at Pasadena, and three engineers, two of whom arestationed at Mitaka and one of whom is stationed at Nobeyama
are posted concurrently. The project also has 70 local staff
members dispatched from the Research Corporation of the
University of Hawaii (RCUH), including scientific assistants;
engineers in charge of software and observational instruments;
technicians for facilities, machinery, vehicles, and laboratories;
telescope/instrument operators; secretaries; librarians;
administrative staff; researchers employed for Grant-in-Aid
for Scientific Research; 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 2017, Subaru Telescope produced many outstanding
scientific outcomes which were published in major international
journals. Below are some examples:(1) The electromagnetic counterpart of a gravitational wave
event was detected for the first time. Based on the time variationof the optical and infrared emission brightness, the firstobservational indication of the “r-process” (one of the processes
to create elements heavier than iron) was obtained.
(2) The light curve of a type Ia supernova discovered with thevery wide field optical camera, Hyper Suprime-Cam (HSC),
soon after the explosion was investigated in detail. The widelybelieved hypothesis that “helium nuclear detonation near thesurface of a white dwarf triggers a stellar explosion” wasstrongly supported.
(3) Using HSC, nearly 200 proto-clusters (ancestors of theclusters of galaxies) were detected at 12 billion light-years away.
This number is ten times larger than have previously been found,enabling systematic investigations of proto-clusters in the distant
Universe for the first time. Unprecedentedly wide and sharp dark

052

II Status Reports of Research Activities

matter maps were also obtained using HSC and the gravitational
lensing technique.
(4) For nearby galaxies, using unprecedentedly deep and sharp
optical images obtained with HSC, clear signs of mergers withsmall galaxies were revealed in M77 which has an actively
mass-accreting supermassive black hole but looks like a normal
quiet spiral galaxy. Using HSC, as many as 11 dwarf galaxies
and 2 tidal streams were detected in a large spiral galaxy (Whale
Galaxy) at the distance of 23 million light-years away from the
Earth.

3. Open-use
In S17A, 42 programs (69 nights) were accepted out of 166
submitted proposals, requesting 418.3 nights in total. In S17B,
37 proposals (55 nights) were accepted out of 135 submitted
proposals, requesting 294 nights in total. Service observations
were made for 9.5 nights. In S17A and S17B, 4 and 2 accepted
open-use proposals were by foreign principal investigators,
excluding University of Hawai`i and East Asian Observatory
observing time. The number of applicants in submitted proposals
was 2278 for Japanese researchers (Japanese astronomers
at any institute and non-Japanese astronomers belonging toJapanese institutes) and 887 for foreign researchers. The numberof researchers in accepted proposals was 751 for Japanese
astronomers and 285 for foreign astronomers. In S17A and
S17B, the number of open-use visiting observers was 271, of
which 61 were foreign astronomers. 113 astronomers observed
remotely from Mitaka. In S17A and S17B, 85.42 % of the
open-use time (including University of Hawai`i time) was used
for actual astronomical observations, after excluding weather
factor and scheduled maintenance downtime. About 1.41 %,0.19 %, 12.92 %, and 0.06 % of observing time was lost due to
instrument trouble, communication trouble, telescope trouble,
and operation trouble, respectively. In S17A and S17B, remoteobservations from Hilo were conducted for 12 programs with
14.5 nights. On the other hand, remote observations from Mitaka
were conducted for 76 nights with 28 programs including HSC
SSP. The number of telescope time exchange nights between
Subaru Telescope and Keck was 8.0 nights in S17A and 8.5nights in S17B. For time exchange between Subaru Telescopeand Gemini, Subaru Telescope users used Gemini time 10.7nights in S17A and 4.7 nights in S17B while Gemini users used
Subaru time 6.0 nights in S17A and 4.5 nights in S17B.

4. Telescope Maintenance and Performance
Improvement
A windscreen incident happened during night operation on

April 10, 2017. The chain to drive the screen panels up and down
and some of the panels of the windscreen fell. Observations forthat night were cancelled immediately. Restoration work wasdone from April 10 to April 17. Observation resumed from April
17. Later, the broken panels and chains were removed. As ofthis writing, science operation has been carried out without awindscreen since the incident.
The mirror hatch, which had an incident in February 2016,
was repaired in June and July. Finally we confirmed the hatch
was fully and safely operational in August.
After the mirror hatch repair, we carried out the primary
mirror recoating work which was originally scheduled forsummer 2016. This was the eighth recoating of the mirror since
its arrival at Maunakea, Hawai`i in 1998 and was about four
years after the previous recoating. The mirror recoating workand telescope related works were performed from October 2 to
December 14. After the recoating work, the reflectivity of the
primary mirror was recovered up to 92 % (at 400 nm).
Other general functions and performances of the telescope
are continuing to be maintained the same as the previous year.
Due to the tight financial situation, the remote maintenancecontract was cancelled, but mass production of the primary
mirror actuator CPU cards was run as scheduled. Some studies
for the Telescope System Computer (TSC) replacement andthe telescope UPS (Uninterruptible Power supply System)
replacement were also run.
To reduce costs, we are developing in-house manufacturing.
A study for a Programmable Logic Controller (PLC), preparation
for full remote control of the telescope, preventive maintenancebased on log data, study for dome-rail flatness measurement, andmodification of a coolant water bottleneck are examples.
However, aging of both the telescope and the dome structure
has been increasing the risk of critical failure. The telescope is ina wear-out failure phase. We should look straight at this severe
reality.

5. Instrumentation
The eight open-use facility instruments of Subaru Telescopewere operated stably in FY 2016. Those instruments are Hyper
Suprime-Cam (HSC), Subaru Prime Focus Camera (SuprimeCam), Faint Object Camera And Spectrograph (FOCAS),High Dispersion Spectrograph (HDS), Infrared Camera andSpectrograph (IRCS), Cooled Mid-infrared Camera andSpectrograph (COMICS), Multi-Object Infrared Camera andSpectrograph (MOIRCS), and the 188-elements Adaptive Optics
and Laser Guide Star system (AO188/LGS).
In these years, there have been discussions on how wemaintain or stop the operation of the facility instruments.
Last year (2016), we decommissioned FMOS. In this year,
Suprime-Cam was decommissioned in May, 2017 and we
shifted completely to HSC for prime-focus wide-field imaging
observations. Thanks to the users’ efforts, we have twelve
narrow-band filters available for open-use observations.
The operation of HSC has been stable similarly to the last
fiscal year, though minor troubles in the filer exchange unit

(FEU) still happened. Tests for replacing filter sets during HSC
observing runs while HSC is on the telescope were completed
and this capability is planned to be in operation from the latter
half of 2018. Preparation of the new monochromatic domeflat system, which enables scanning the wavelength of thelight source for precise photometric accuracy, has also been
conducted in this fiscal year.
The ongoing upgrade projects for the other facility
instruments are the fiber MOS unit for HDS, the polarimetricfunction in thermal infrared for IRCS and in mid-infrared
for COMICS, the integral field unit (IFU) for FOCAS and
MOIRCS, the Transponder-Based Aircraft Detector (TBAD) for
the LGS system, and an upgrade of the real-time control system
and laser guide star system for AO188. Upgrades of the aging
control computers and devices of the first generation instruments
are ongoing. In addition, a design study for a NsIR beamswitcher, which will enable switching NsIR instruments without
physically moving the instruments, has started as a collaboration
with Australian institutes.
In FY 2016, three carry-in (PI-type) instruments HiCIAO(high-contrast coronagraph imager), SCExAO (Subaru
Coronagraphic Extreme Adaptive Optics) and CHARIS (highcontrast integral-field spectrograph) have been offered to the
Subaru open-use program. Operation of HiCIAO at the Subaru
Telescope ended in S17B. Among the instrument modules of
SCExAO, VAMPIRES (visible interferometric imager withdifferential polarimetry) was open for public use.
A new PI-type instrument, IRD (InfraRed Doppler
instrument), has made engineering observations aiming
to start open-use observation in S18B. Two other PI-type
instruments proposed by the University of Tokyo team,
SWIMS (Simultaneous-color Wide-field Infrared Multiobject Spectrograph) and MIMIZUKU (mid-infrared multifield imager and spectrograph), were transferred to the Hilo
Base Facility. Errors in the mechanical dimensions were found,and countermeasures were taken. They will have engineeringobservations starting in S18A.
The Prime-Focus Spectrograph (PFS) is an optical/nearinfrared multi-object spectrograph at the prime focus of the
Subaru Telescope, which will be the next facility instrument
following the successful implementation of HSC. The PFS has
about 2400 optical fibers distributed over the 1.3 degree field ofview of the prime focus which feed the light of the astronomical
objects to four identical spectrographs which will be placedin the telescope dome. The spectrograph modules cover
wavelengths ranging from 0.38 μm to 1.26 μm simultaneously.
There are slight delays in the schedule: the engineering firstlight will be in 2019 and science operation is expected to begin
in 2021. Subaru Telescope is responsible for modifying thetelescope and enclosure to accept PFS. The design works andreinforcement of the spectrograph floor has been conducted. The
data reduction pipeline and the database that combine HSC andPFS data is being developed with US collaborators.
We are conducting a conceptual study of “ULTIMATESubaru,” the Subaru Telescope's next large facility instrument
following HSC and PFS, which will be one of the flagship

II Status Reports of Research Activities

053

instruments at the Subaru Telescope in the 2020’s. We are
studying the concept of a wide-field near-infrared imager, multiobject spectrograph, and multi-object integral field unit (IFU)
spectrograph, assisted by a ground-layer adaptive optics (GLAO)
system. GLAO will allow us to uniformly improve the image
quality over a wide field of view by correcting the turbulence at
the ground layer of the Earth’s atmosphere by using an adaptive
secondary mirror. In FY 2017, with an official (short-term)
agreement established in FY 2016, we have been collaboratingwith Australia on the GLAO feasibility study. We are working
together toward the Conceptual Design Review to be scheduled
in FY 2018. We also had the first ULTIMATE-Subaru“collaboration meeting” in NAOJ (Mitaka) by inviting scientists
in potential partner countries (Australia, Taiwan, Canada) toshare the goals and roles of each partner country. We are pleased
to report that our ULTIMATE-Subaru project has been officiallykicked-off with an external budget (KAKENHI Kiban-S with M.
Akiyama [Tohoku Univ.]).

6. Computer and Network
Subaru Telescope focused on stable operation of the fourthgeneration system of computers and network called STN4
as well as the design, installation, and operation of the fifthgeneration system called STN5. Stable operation was achieved
without serious trouble or attacks/intrusions such as illegal
access.
The observation data archive has been ongoing from theprevious year. The archive is operational without serious
problem. The data archive system in Mitaka also showed stableperformance.
Subaru Telescope has officially offered remote observations
from Mitaka using the Remote Observation Monitor Systemsince 2015. Remote observation is now available for more
instruments than before. An increasing number of observers use
the Remote Observation Monitor System in Mitaka. About 40
observation programs utilized the remote observation monitor
system for 139 nights during May 2017 to March 2018.
Computers for HSC data analysis (HSC On-site Data
Analysis System) were procured in Fiscal Years 2010 and 2011.
We have been replacing and adding hardware as needed. We
replaced a part of the computers in Fiscal Years 2017.
Subaru Telescope has been developing and operating web
applications that support open-use observations. The Proposal
Management System (ProMS) has been updated as the contentsof the calls for proposals change, and has been working well.
Subaru Telescope is planning to develop a web application to
help the referees who score the proposals. Two online visitor
forms are in operation, one for those who visit Subaru Telescopein Hilo for observations and the other for those who visit NAOJ
Mitaka Campus for remote observation monitoring.
Since the rental contract for our computer and network
infrastructure ended in February 2018, we procured thecomputer and network system that started operation in March2018. Subaru Telescope developed the specifications andheld a briefing for bidding in June 2017 and a bidding and054

II Status Reports of Research Activities

technical review of proposals in July 2017. We opened the bids
in August 2017 and signed the contract in September 2017.
Detailed design, installation, and data migration were done withcomputer/network staff at Subaru Telescope and the contractor.
The new system started as scheduled from March 2018.

7. Education (Under-graduate and Graduate
Courses)
The number of Subaru Telescope staff members in Hilo whowere concurrently appointed by SOKENDAI (graduate school)
was eleven. The number of SOKENDAI students who had
primary supervisors affiliated with Subaru Telescope (including
those concurrently belonging to Subaru Telescope) was ten,which constituted about one-third of the total 31 Sokendai
students hosted in NAOJ. Of those, five had supervisors who
belonged primarily to Subaru Telescope.
In FY 2017, Subaru Telescope hosted 3 graduate students
for long stays in Hilo, of which two were SOKENDAI students.
On top of that, intensive education activities were seen alsoin Mitaka in cooperation with the Division of Optical and IR
Astronomy. The numbers of graduate course students in allof Japan who obtained master’s degrees and PhD’s based on
Subaru Telescope data were 17 and eight, respectively, of
which two and three belonged to the Division of Optical and IR
Astronomy.
We also regularly hosted a series of educational programs
at Subaru Telescope. In September 2017, we hosted a Subaru
Autumn School in Mitaka. There were 14 participants. They
learned the reduction and analysis of Subaru Telescope dataand heard a series of lectures. Moreover, we hosted two Subaru
Telescope observation training courses. One was for eightundergraduate students from all over Japan held in January 2018,
and the other for five new SOKENDAI students at NAOJ heldin September 2017. In the Hilo office, we had regular Subaru
Telescope seminars in English 2-3 times per month, where openuse observers, visitors, and Subaru Telescope staff memberspresented their own new research. Also in the Subaru Telescope
Mitaka office, we had many official and informal seminars,
many of which were jointly organized with other divisions in
NAOJ and/or neighboring universities.

8. Public Information and Outreach (PIO)
The goal of the Public Information and Outreach Office (PIO)
is to document, share, and promote the activities and scientificachievements of Subaru Telescope (Subaru) throughout thegeneral population. Raising positive awareness of Subaru
Telescope -- within the local community, in particular -- iscritical for the success of the Subaru project as well as the next
generation telescope project on Maunakea. The PIO has threemajor tasks to achieve its goal.
Task 1: Provide information about activities and scientific resultsfrom Subaru Telescope by effectively using website and social
media platforms. Subaru Telescope provides press releases tothe Japanese, local, and international media and holds press
conferences. During Fiscal Year 2017, there were 12 webpostings (6 in Japanese and 6 in English) about discoveries
from Subaru Telescope. Articles about instrument development,
the work and activities at the Subaru Telescope and otherannouncement totaled 43 (24 in Japanese, 19 in English). For
major scientific discoveries, PIO actively distributes press
release articles to local and Japanese media as well as aninternational network via the American Astronomical Society’s
mailing exploder. As a result, scientific results from Subaru
Telescope often appear in Japanese and local newspapers andweb news.
Social media tools such as Twitter, Facebook, and YouTube
are highly effective nowadays in rapidly disseminating
information. Subaru’s PIO has effectively used these newplatforms by producing and sharing photographs and videos.
Media inquiries and filming requests totaled 22 from Japanese
media and 10 from English media. In addition to media
interaction, PIO also responds to the numerous inquiries andquestions from educational institutions and museums.
Task 2: Provide escorted tours of the summit and base facilities
for the public and special groups. Subaru Telescope started the
public tour program in 2004, providing opportunities for guests
from Hawaiʻi, Japan, and around the world to see the telescope
up-close. Those requesting tours receive prompt responses froma dedicated full-time tour staff. People can sign up for summit
tours via an online form on the Subaru Telescope website.
During Fiscal Year 2017, 307 people visited the summit facility
through the public tour program. This number does not include
tours that were suspended due to poor weather conditions. An
additional 67 groups visited the summit facility via special tour
programs. In total, 677 people visited the summit facility in
Fiscal Year 2017. This includes 8 special tours dedicated for the
residents of Hawaiʻi. All tours are escorted by assigned staff andconducted in either Japanese or English.

Hawaiʻi Island. One of the major outreach events is AstroDay,a family-friendly event held at the local shopping mall. Each
year, more than 2,000 people come to this event. AstroDay iscoordinated by Maunakea observatories, and many astronomy
and scientific institutions such as ‘Imiloa Astronomy Center,
Maunakea Visitor Information Station, and the University of
Hawaiʻi at Hilo participate. This year, AstroDay was also heldin Kona, on the west side of the island, attracting over 3,000
people.
Another major outreach event on Hawaiʻi Island is theannual Onizuka Science Day at the University of Hawaiʻi at
Hilo. Six hundred students between grade 4 and 12 (upper
elementary school to high school) with families and teachers
from all over the island come to this event. Subaru PIO provided
two hands-on astronomy workshops and held an exhibit booth.
Events like these where Subaru Telescope staff meet and directlyinteract with students and members of the local community are
effective for improving the recognition of the Subaru Telescope.
The Subaru PIO has been sharing information about outreachactivities via the website and social media.
It is also important for the staff to have a strong
understanding of the host community. Subaru Telescope started
a new seminar series for the staff to learn Hawaiian culture,
history, and perspectives with lectures from experts in the field.

Tours of the Hilo base facility are often accompanied bya special lecture by staff or a hands-on astronomy workshop.
Some school groups give student presentations and Subaru staff
provide comments and advice. A total of 23 groups (252 people)
visited the base facility this year.
Task 3: Provide on-site and remote lectures for the local
community as well as Japanese schools and museums. During
Fiscal Year 2017, PIO provided/coordinated a total of 84 lecturesat the Subaru Hilo Base Facility or at nearby locations, suchas ʻImiloa Astronomy Center and local schools. This number
includes 45 classroom presentations during the annual Journey
through the Universe program which takes place over the courseof a week. Subaru staff also conducted 31 lectures outside
Hawaiʻi and 10 remote lectures for Japanese schools.
In addition to providing lectures, Subaru Telescope actively
participates in various outreach events and career fairs on

II Status Reports of Research Activities055

2. Okayama Astrophysical Observatory
Okayama Astrophysical Observatory, (hereafter theObservatory) served as the observing and research base of
the optical and infrared astronomy in Japan, and it promoted
open use, primarily of the 188-cm telescope, to universities
throughout the country. It also pursued joint R&D projects with
universities, contributing toward forming stronger foundations
for astronomy research at the universities. Concurrently,
the Observatory pursued its own research activities, taking
advantage of its location and observational environment. In
addition, the Observatory developed activities to realize thenation-wide openuse of the telescope time on Kyoto University’s
Okayama 3.8-m New Technology Optical and Infrared Telescopein FY 2017.
About 230 nights at the 188-cm telescope were exploitedfor observations by researchers from across the country throughthe open use. The Observatory maintained and operated theobserving instruments and provided the observers with support
for observations, travel expenses, accommodations, everyday
needs, etc. It also supported carry-in instruments from otherinstitutions.
Several joint projects with universities were conducted,
including Kyoto University’s Okayama 3.8-m New Technology
Optical and Infrared Telescope Project, the Tokyo Institute ofTechnology’s Gamma-Ray Burst Optical Afterglow Followup Project, and “The Optical & Near-Infrared Astronomy InterUniversity Cooperation Program” supported by MEXT.
The Observatory’s unique research activities included
a comprehensive survey of infrared-variable objects in the
Galactic plane using the 91-cm telescope which has been
converted into an ultra-wide-field near-infrared camera (OAOWFC). The project to automate the 188-cm telescope and to
improve the stability and sensitivity of the high dispersion
spectrograph through a Grant-in-Aid for Scientific Research(Basic Research (A), FY 2016–2020) was continued. This
project aimed at establishing a large sample of exoplanets.
Collaborations with foreign researchers also continued actively.
The personnel breakdown as of March 2018 was five fulltime staff members without term limits, including two associate
professors, one assistant professor, one engineer, and one Chiefof the Administration Office; ten contract employees, including
one specially appointed associate professor, one research expert,
one specially appointed research staff member, one speciallyappointed senior specialist, one research supporter, threeadministrative supporters, and two administrative maintenancestaff members; and one temporary staff member.
NAOJ secured the transfer of the nation-wide open use from
Okayama Astrophysical Observatory to Kyoto University’s 3.8m telescope starting from FY 2018 and dissolved the C Project“Okayama Astrophysical Observatory” on March 31, 2018.

056

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0. Dissolution of the C Project “Okayama
Astrophysical Observatory”
The National Astronomical Observatory of Japan has
positioned Kyoto University’s 3.8-meter telescope as the
successor to the 188-cm telescope, and has placed the promotionof nation-wide open use with the 3.8-meter telescope, insteadof with the 188-cm telescope, at the center of the future planof the Okayama observatory. NAOJ announced its intention todissolve the Okayama observatory, and to apply a considerable
part of its operating expenses and 3 faculty and staff members to
the operation of the 3.8-m telescope, and to provide about halfof the observing time of the 3.8-m telescope for the nation-wide
openuse, as soon as the 3.8-m telescope is ready for scientificobservations. The memorandum of understanding exchanged
between NAOJ and the Graduate School of Science of Kyoto
University on October 12, 2017 guaranteed that NAOJ can
provide about half of the observing time at the 3.8-m telescope
for the nation-wide open use starting from FY 2018, and fixed
the end of the open use of the 188-cm telescope at the end of
Calendar Year (CY) 2017, in line with the discussions between
NAOJ, the optical and infrared astronomy community, andKyoto University. The Observatory submitted a proposal todissolve the C-Project Okayama Astrophysical Observatory at
the end of FY 2017 to the Planning Committee. Having passed
the Executive Committee and the Advisory Committee for
Research and Management, the dissolution was finally approvedat the Board of Directors and Executive Committee of the
National Institutes of Natural Sciences in November, 2017. On
the other hand, NAOJ decided to establish the Okayama Branch
Office of Subaru Telescope as a promotion organization for thenation-wide open use at the 3.8-m telescope.
From the fall of CY 2017, preparations for the dissolutionof OAO and the establishment of the Okayama Branch
Office were carried out at the Observatory. The Observatory
abolished the library, moved about 1,000 books to the Mitaka
Library, and discarded the remaining thousands of books. Two
temporary buildings were abolished and removed. About 15,000
photographic plates of images and spectra of celestial bodies,
stored in one of the two temporary buildings, were moved to the
Mitaka Library. Other valuable materials were also moved to
the Mitaka Library. The Observatory renovated the library room
into two smaller rooms and transferred the computer serverroom and optical laboratory in the solar telescope building to
the renovated rooms. The office kitchenette, women’s changing
room, and ladies room were modernly renovated. The laying
route of the optical network cable was reorganized. A power
meter was installed on each telescope dome. The gateway was
retired and a new gate was installed. Preparation work was done
for transiting to a new security system. The vacuum chamber
for aluminizing the primary of the 1.5 m infrared simulator was
discarded. Through these, the functions that were dispersed in
the telescope domes and temporary buildings were concentrated

in the main building. And as of March 31, the C Project
Okayama Astrophysical Observatory was dissolved.

1. Open Use(1) Overview
The numbers of nights allotted to open use in 2017 were
120 for the first semester (2017A, January to June) and 111 forthe second semester (2017B, July to December). Observing
proposals submitted in response to the calls for proposals werereviewed by the Okayama observatory program subcommittee
and 1 project observation program, 0 academic degree support
programs, 13 general observation proposals, 1 miscellaneous
observation proposal, and 1 ToO observation proposal were
accepted for 2017A, and 1, 0, 13, 0, and 0 were accepted for
2017B. Two proposals, one from each of Chinese Taipei and
Poland, were accepted in 2017A, and two proposals, one fromeach of Chinese Taipei and Poland, were accepted in 2017B. The
Observatory supported their observations with human resources.
There were no major troubles with the telescope or the dome ineither semester. Observing instruments were operated smoothly
in the former semester, but a serious trouble occurred in one of
the three instruments in the latter. Efforts were made in vain torestore the instrument, and its operation was terminated before
the end of the overall open use scheduled at the end of CY
2017. Remaining observing time allotted to this instrument wasredistributed to research subjects using other instruments asmuch as possible and the open use continued.
(2) Observation/Research Results
The majority of objects observed through the open use
in 2017 were stellar sources, exoplanets, and galaxies. The
following primary observation themes were noted: explorationof the physical properties and activities of single and binary stars
via high-dispersion spectroscopy; exoplanet search and binarymass determination via precise radial velocity measurements;
exploration of exoplanet atmospheres by transits observations;and studies of physical processes in galaxies with near-infrared
low-dispersion spectroscopy. As in previous years, a number ofobservational studies were conducted by individual groups ofresearchers within the open-use framework, and their respective
research results were reported in meetings and conferences orwere published in peer-reviewed journals.
(3) Facility and Instrument Maintenance/Management
The 188-cm telescope and its dome had evolved into astable and high-functioning observing system by FY 2014
after the major refurbishment in FY 2012. Efforts were madeto improve the completeness of the automated high dispersion
spectroscopic observations with the fiber-feeding systemdeveloped in FY 2016. The remote observing environment
provided to the open use with no conditions since 2016A wasmaintained and its use greatly increased to over 50 % of the
open-use observations. During the maintenance period in June,
the annual re-aluminization of the primary mirror of the 188cm telescope and lubrication of the telescope and dome werecompleted. The 1.5-m primary of the KANATA Telescope at
Hiroshima University was also accepted for re-aluminizationin the maintenance period. Participants in the aluminization
work from that organization were given NAOJ-mandated
safety and hygiene training as necessary. Utmost efforts weremade to maintain high observing efficiency by conducting
monthly cleaning of the primary mirror of the 188-cm telescopefrom October to December. The dome was checked regularly.
Repair of the worn-down guiding rails for the slit doors andreplacement of the dome rotation drivers were done, in order toachieve smooth open-use operation. Safe storage of the acquired
observing data and appropriate maintenance of the computer andnetwork environment were carried out. Work safety was given
priority in accomplishing the aforementioned maintenance workand observing instrument exchanges. In the total comprehensive
replacement of the computer system of NAOJ at the end of FY
2017, the Observatory successfully completed the updating withthe cooperation of the Astronomical Data Center. As a result,the Observatory continued to share the Okayama data archivefunction of the large-scale data-archive/public-subsystem of the
National Astronomical Observatory Data-Analysis/Archive/
Open System; and the remote backup function of Mizusawa
RISE, Solar, and SMOKA data.
(4) Conferences
In FY 2017, the Observatory cooperated with Kyoto
University and the Okayama Observatory Program
Subcommittee to prepare for transferring the nation-wide open
use from the 188-cm telescope to the 3.8-meter telescope. The
program subcommittee met 13 times during FY 2017.
In early July of 2017, a joint call for proposals was issued on
the first generation open-use observing instruments of the 3.8m telescope by the program subcommittee, Kyoto University,and the Observatory. It was closed in early August and one
application was received. At the program subcommittee in late
September, 2017, it was decided to accept the fiber-type optical
integral field spectrograph “KOOLS-IFU” (PI: Koji Ohta at
Kyoto University).
The Observatory held the Okayama Users Meeting (The28th Optical and Infrared Users Meeting, UM) at the Large
Seminar Room of NAOJ Mitaka Campus on September 4 and5. The present status of the Observatory, including the 188-cm
telescope and dome; current condition of the open-use observing
instruments and remote observation system; execution summaryof the open-use observation programming of semester 2017A
and B; future operation of the 188-cm telescope; development
status of the fully automated observing system for HIDES FiberFeed observation; research results based on openuse of the 188cm telescope; progress situation of the 3.8-m telescope projectand study/preparation of observing instruments; proposals forscientific research using the 3.8-m telescope; status of study andpreparation of the promotion system for nation-wide open use
at the 3.8-m telescope; current situation of the optical infraredobservation facilities such as the Hiroshima University Space
Science Center and their research results; etc. were reported.
Regarding the nation-wide open use at the 3.8-m telescope,

II Status Reports of Research Activities057

the content of the discussion through the previous year wasreconfirmed and shared among the participants, and the changes
due to the change of the newly generated situation was explainedby the Observatory, and the specific policies were discussed
comprehensively by the participants. As a particularly significant
change, it was explained that NAOJ concluded that it would be
difficult for three faculty and staff members to be dispatched
to Kyoto University and planned to establish the Okayama
Branch Office to promote the nation-wide open use at the 3.8-m
telescope and post three faculty and staff members.
The program subcommittee made the draft of the second
report on the nation-wide open use at the 3.8-m telescope titled“The policy for open use in Kyoto University’s Okayama 3.8m New Technology Optical and Infrared Telescope Project.”
The report was expected to be handed to the Director Generalof NAOJ from the Advisory Committee for Optical and Infrared
Astronomy around the end of FY 2017, and the subcommittee
submitted it to the parent Advisory Committee on March 30,
2017 (The first report was titled “Plans for the transfer toand operation of the open use of the Kyoto University 3.8m telescope.”). In the report, the importance of time domain
astronomy and that of student education are emphasized, anda queue observing mode was defined as the main observing
mode at the 3.8-m telescope. It was recommended that in the
future Kyoto University and NAOJ should aim to implement
integrated operation of observations for research subjects with
Kyoto University time and open-use time. It was also suggested
to categorize the observing subjects into “general research”,“ToO”, “degree support”, and “other”, place higher importanceon ToO observations, and implement a system that carries out
ToO observation smoothly.
On October 6, 2017, at the initiative of Okayama Prefecture,
the 18th liaison meeting on the cooperation for preserving theobservational environment for the Okayama AstrophysicalObservatory of the National Astronomical Observatory was heldin Okayama City. Greetings from the Deputy Director of theEnvironment and Culture Department of Okayama Prefectural
government office, greetings by the Director General of NAOJ,
a special lecture by Dr. Takao Doi, a Program-Specific Professor
at Kyoto University and an astronaut at JAXA, and approval of
the regulations were conducted. Then, there were introductions
about recent trends in observational research, the current statusof the 3.8-m telescope of Kyoto University, and measures
to prevent light pollution in Okayama Prefecture. Calls forconservation efforts for the observation environment were madeto various related areas in the prefecture.

2. Developing and Maintaining Open-Use
Observing Instruments(1) HIDES (High-Dispersion Echelle Spectrograph)
The instrument HIDES is a cross-dispersed high-dispersion
echelle spectrograph with two fiber-link systems (HIDES-F).
The high-efficiency (HE) fiber link with approximately 50-K
wavelength resolution offers an improvement in throughput
of nearly one magnitude over the previous value with the058

II Status Reports of Research Activities

Coudé light path and radial velocity measurement precision of
approximately 2 m/s, which is comparable to the case of the
Coudé light path. The high-resolution (HR) link with 100-K
wavelength resolution provides a 4 times better sensitivity at
maximum than the case of the Coudé light path. All functions of
HIDES-F were kept available to the open use in FY 2017. The
HE mode dominated the open use. This year the total numbersof accepted proposals to HIDES were 6 and 7 in 2017A and2017B, including 1 and 1 project observations, respectively.
Regarding the optical comb developed by researchersat the National Institute of Advanced Industrial Science andTechnology (AIST) and others and installed in the 188-cm
telescope dome last year as a next generation high precision
wavelength standard, the collection of experimental data for
astronomical applications was terminated in December. The
optical comb was collected by AIST.
(2) ISLE (Near-Infrared Imager/Spectrograph)
ISLE was a near-infrared imager and low- or mid-dispersion
spectrograph. It was characterized as having the world’s best
low-noise readout capability (less than 10 electrons). Relative
photometry at the one milli-magnitude level was regularly
achievable with its imaging mode for bright sources. A carry-in
YJH-band filter from a user and the HK-band filter as standard
equipment enabled it to obtain a well-connected spectrum from
Y-band to K-band. In FY 2017 as well, the open use of all
functions was continued. A failure occurred and the detector
did not operate properly at the end of July, 2017. Among 13
open-use observing nights using ISLE in July and August, 3
nights were transferred to other equipment and the open-use
observations were carried out. The Observatory cancelled theremaining 10 night open-use observing program and transferred
the 10 nights to observatory time. The Observatory tried
restoration work but concluded that it was not recoverable atthe end of September and decided to terminate the operationof ISLE. The Observatory redistributed 17 nights of open-use
observations scheduled to use ISLE from October to December
to open-use research subjects with other observing instruments.
The numbers of accepted open-use programs using ISLE insemester 2017A was five, three of which were spectroscopy andthe other two of which were imaging photometry. In 2017B,
five were accepted, four of which were spectroscopy and one ofwhich was imaging photometry, but they were not executed dueto the malfunction of the instrument.
(3) MuSCATMuSCAT is a Multicolor Simultaneous Camera for studying
Atmospheres of Transiting exoplanets in three visible colors (g,r, z band). A relative photometric accuracy of 0.05% (0.5 mmag)is achieved in the case of repeating one-minute exposures fora star of 10-th mag in V-band. The Observatory continued tooperate MuSCAT as a PI type open-use instrument in FY 2017.
In the first semester of 2017, five open-use programs (including
one miscellaneous program) were conducted, and three open-use
observing programs were conducted in the second semester of2017.

3. Joint Research with Universities(1) Kyoto University’s Okayama 3.8-m New Technology Opticaland Infrared Telescope Project
The Observatory has participated in a cooperative
implementation framework for the 3.8-m telescope project,which is spearheaded by Kyoto University, together with AstroAerospace, Inc., regarding the 3.8-m telescope project as partof the future plan of the Observatory. Discussions were heldon technological issues regarding the telescope and observing
instruments through weekly TV conferences and in-person
meetings held every three months in FY 2017 also. The 3.8m telescope in the temporary housing was disassembled,
moved to the main dome, reassembled, and continued on toadjustment work in July. In July, a joint call for proposals was
issued on the first generation open-use observing instruments
by the program subcommittee, Kyoto University, and theObservatory. At the program subcommittee in September,
2017, it was decided to accept the fiber-type optical integral
field spectrograph “KOOLS-IFU” (PI: Koji Ohta at Kyoto
University). The Observatory cooperated with researchers at
Kyoto University to further develop and strengthen KOOLSIFU. The Observatory also collaborated with the researchers at
Kyoto University to design the instrument rotator to be installedon the Nasmyth focus platform. Development of a near-infraredfiber-fed spectrometer was continued through a JSPS grant
for scientific research (Basic Research A (General), FY 20162019) applied for and acquired by the Kyoto University side,in which an observatory staff member participated as a coinvestigator. Workshops on high dispersion spectroscopy were
held to reinforce the research groups and enhance the application
activities for external funds.
(2) The Optical & Near-Infrared Astronomy Inter-University
Cooperation Program
The Program entered its second term from FY 2017 as acontinuation of the previous program.
The Observatory decided not to receive budget allocationfrom the program in FY 2017 and contributed to the program bykeeping the 50-cm telescope system operable and available forthe program.
(3) Gamma Ray Burst (GRB) Optical Follow-up Project
Optical follow-up observations of GRBs using the 50cm telescope were conducted in cooperation with the Tokyo
Institute of Technology’s Kawai Laboratory. During FY 2017,
the automatic observation scheduler performed observations on
nearly every possible night; 47 GRBs were observed, with upper
limits for optical afterglows published as 7 GRB Coordinates
Network (GCN) circulars. In addition, follow-up observations ofcandidate gravitational wave sources and monitoring of objects
that include X-ray binaries, active galactic nuclei, and supernovae
were concurrently performed, which resulted in publicationof six peer-reviewed papers. In FY 2017, the Observatory
contributed to the operation through the maintenance of thetelescope, dome, and the electric power supply.

(4) Use of the existing telescopes including the 188-cm reflector
starting from FY 2018
Regarding the use of the existing 188-cm telescope andsmaller ones starting from FY 2018, discussions have been held
repeatedly between NAOJ, researchers at universities, and the
local municipality since FY 2016. For the 188-cm telescope,
the Center for Observation and Research on Exoplanetsof the School of Science of Tokyo Institute of Technology
was established in April, 2017, with an intention to operate
the telescope. Asakuchi City, the local municipality, also
expressed the positive intention to use the 188-cm telescope.
The Observatory cooperated with the executive board andadministrative departments of NAOJ in response to thesedevelopments. The Observatory assisted the preparation for
conclusion of the agreement by the three parties of NAOJ,
Tokyo Institute of Technology, and Asakuchi City on the use of
the 188-cm telescope.
(5) Other
The Observatory welcomed four third-year undergraduate
students and their supervisor from the University of Tokyo
between August 23 and 25 and provided them with anopportunity to conduct high-dispersion spectroscopic
observations using the 188-cm telescope during the early halfnight on August 23.
In collaboration with researchers at Tohoku University, IRTMT, a bright star observing system equipped with Tohoku
University’s 30 mm diameter wide field of view near infrared
camera mounted on the equatorial mounting for 30 cm classtelescopes owned by the Observatory was operated, and dataacquisition continued to create a highly accurate near-infrared
photometric catalog of stars in the solar neighborhood. The
observations were conducted exclusively by remote control fromTohoku University.

4. Unique Research Projects(1) Detection of afterglow from distant GRBs and survey ofvariable stars in the Galactic plane using the ultra-wide-field
infrared camera.
With the 91-cm reflector having been converted into an
infrared camera with an ultra-wide field of view, observationsin the Ks band were conducted to identify infrared counterpartsfor objects such as GRBs and gravitational wave sources. Alongwith them, a comprehensive survey of infrared variable stars
in the Galactic plane was carried out. In FY 2017, frequent
observations were made extending out in the direction of thegalactic longitude from the two zones (centered on 30 and 80
degrees in the galactic longitude) that were monitored last year,
and low frequency (~ every few tens of days) observations of
the two zones were added so that long period variables could be
detected there. Based on preliminary analysis of acquired data,
90 cepheid candidates were detected, and it was confirmed thatmost of them were not detected in visible light due to heavyinterstellar extinction. In addition, automatic monitoring of otherobjects, such as the Orion star forming region and bright blazars

II Status Reports of Research Activities059

were continued.
(2) Development of a far larger scale exoplanet search
Through a Grant-in-Aid for Scientific Research (Basic
Research (A), “Large-scale exoplanet search with a robotic
telescope for high dispersion spectroscopy,” representative:
Hideyuki Izumiura, FY 2016–2020), a project was initiated toestablish an original large-scale sample of exoplanets in theprevious FY. For that purpose, activities were continued todevelop robotic operation of spectroscopic observations withthe 188-cm telescope and to improve the sensitivity and stabilityof the spectrograph. Concerning the robotic operation of theobserving system, once a target list following a certain format
is given to the system by the observer, the system automatically
executes the evaluation of the sunset and weather; opening/closing of the dome slit and mirror covers; telescope focusing;acquisition and tracking of the target; exposure control of thespectrograph; choice of the next target; and the termination
process for the night. The progress of the observations can bechecked with a web browser. Time-based observing efficiency
comparable to those realized by highly experienced observers
has been achieved by tuning through the test observing runs.
On the other hand, the sensitivity of the observing system wasenhanced by applying a new coating to the secondary mirrorof the 188-cm telescope and by introducing a new collimator
mirror and a new cross-disperser grating. The spectrograph wasstabilized by replacing its thermostat equipment.
(3) East Asian Planet Search Network
The Observatory also conducted studies focusing on the
search for exoplanetary systems, involving researchers fromSouth Korea, China, Turkey, and Russia. Efforts were continued
in FY 2017 to secure telescope time on the Korean 1.8-m
telescope, Chinese 2.16-m telescope, Turkish 1.5-m telescope,and the Observatory’s own 188-cm telescope for continued
searches for exoplanetary systems around G-type giant stars.
A meeting on exoplanet searches using precise radial velocity
measurements and astero-seismology was held in Nara City,
welcoming related researchers from Japan, China, South Korea,
and Germany in October 2017. With the above collaborations
two peer-reviewed papers were published and the network wasable to lead the world wide search for exoplanets around G-type
giant stars.

5. PR/Awareness Promotion Activities
In this FY about 30 astronomy-related questions from thepublic were posed irregularly to the Observatory and wereanswered appropriately. The 4D2U screenings, co-hosted with
the Okayama Astronomical Museum, attracted about 2,300
visitors. Fifteen Observatory tours were conducted, including
those for pupils from local elementary schools in Asakuchi
City and Yakage Town. The Observatory also responded to
two lecture requests made by local boards of education andcommunity centers. The Observatory posted one research result
web release and no press releases. A special website “Complete060

II Status Reports of Research Activities

History of Okayama Astrophysical Observatory” (https://www.
nao.ac.jp/study/oao/) was opened upon dissolution of the C
Project Okayama Astrophysical Observatory.

6. Contract Staff Transfers
The following transfers of contract staff members took place
in FY 2017: Hiroyuki Maehara resigned as a research expert on
December 31 and moved out to a Program-Specific Associate
Professor position (The Optical & Near-Infrared Astronomy
Inter-University Cooperation Program) at Kyoto University on
January 1. Nobuharu Ukita retired at mandatory age from NAOJ
as an associate professor on March 31. On March 31, speciallyappointed associate professor Eiji Kambe, research expert
Daisuke Kuroda, specially appointed research staff member
Kazuya Matsubayashi, research supporter Hiroyuki Toda,
administrative supporter Kumiko Katayama, and administrative
maintenance staff member Shoji Koyama all resigned. A worker
dispatch contract for a temporary staff member was terminatedon March 31.

3. Nobeyama Radio Observatory
1. Nobeyama 45-m Radio Telescope(1) Open Use Observations
The 36th open use observations period started on December
8, 2017. The statistics of the successful proposals are as follows,“General Programs”: 26 programs were accepted out of 55
submitted proposals including eleven programs from abroad (outof 20 submitted), “Large Program”: one program was acceptedout of one submitted, “Short Programs”: nine were acceptedout of twelve, “Backup Programs,” which are to be carried out
when weather is not good enough for the main observations: one
program was accepted (out of one submitted), “GTO (Guaranteed
Time Observation) programs”: one program was accepted andanother was treated as a filler program out of two submitted
proposals. “DDT Programs”: no proposals were submitted.
VLBI open use observations including the 45-m telescope: 3
proposals were accepted out of three.
In addition, carry-over programs from the master collimator
driving system failure in the last observing season wereconducted.
Remote observations were conducted from Kagoshima
University, Kyoto University, Nagoya University, Universityof Tsukuba, and ASIAA (Taiwan). A remote operation test was
conducted from KASI (Korea).
(2) Improvements and Developments
Taking into account the reduction of the human andbudgetary resources of Nobeyama Radio Observatory, we
introduced a call for Nobeyama Development Proposals fromthis fiscal year. The main purpose is to concentrate on theenhancement of the capabilities of the open use with the 45-m
telescope rather than general opportunities. The review panel
members were Tomoharu Oka (chair), Kotaro Kohno, Shigehisa
Takakuwa, and Tomoya Hirota. The Director of NRO and
Tetsuhiro Minamidani (as technical assessor) also attended thereview as observers from the observatory side. A total of eight
proposals were received, and three of them (3-band simultaneous
observing system HINOTORI, frequency-modulation local
oscillation FMLO, Band 1 receiver by Taiwan) were accepted.
Maintenance of the 45-m telescope, the receiver systems, thecryogenics, etc. was performed as follows.
- The repair of the master collimator driving system wascompleted during the summer maintenance term. The
observatory investigated the pointing accuracy and confirmedthat the typical pointing accuracy is the same as before.
- A malfunction in the sub-reflector driving system was found,and tentative measures were done.
- Preventive and corrective paint to the antenna main-reflector
structure was done.
- The replacement of a mirror exchange system (new one) wascompleted. The design works for the replacements of the othermirror exchange system (old one) and the beam switchingsystem were started.

- The “On-On” observation mode with the FOREST receiver
was implemented, and was offered to open-use observations.
The TZ receiver was decommissioned.
- Replacing boards of the SAM45 spectrometer reduced thefrequency of trouble occurrences. A test of a GPU spectrometer
was started for the next generation spectrometer.
- New observing-script generator, “nobs,” was developed, andused for open-use observations.
- Nobeyama 45-m Science Data Archive has been opened.
- Development of the data reduction procedure with the
CASA pipeline is continued. These will lead to an automatedobserving system in the future.
- Simultaneous observations of 22 and 43 GHz bands wererealized by installing a frequency selective filter developed by
the HINOTORI program.
(3) Scientific Results
1) 45-m telescope Legacy Projects(a) Star Formation Legacy ProjectIn the Star Formation Legacy Project, we conducted largescale mapping observations toward three nearby star-forming
regions, Orion A, Aquila Rift, and M17 in 12CO (1–0), 13CO
(1–0), C18O (1–0), and N2H+ (1–0). Many cores and clumps
have been identified from structure analysis of these data. In
particular thanks to the high sensitivity, a protostellar molecular
outflow was found that was not in the data taken with BEARS.
(b) Galactic Plane Survey Project (FUGIN: FOREST Unbiased
Galactic plane Imaging survey with the Nobeyama 45-m
telescope)
We conducted a simultaneous survey of the 12CO (1–0),
13CO (1–0), and C18O (1–0) emission lines in the Galactic Plane
at the highest spatial resolution using FOREST aboard the 45-m
telescope. The detailed structure of the molecular gas in our
Galaxy was made clear, from large scales to internal structures(filaments, clumps, and cores) inside giant molecular clouds.
Hints of evidence of the cloud-cloud collision were obtained
toward the massive star forming region W33 (Kohno et al.), thegiant molecular cloud M17 (Nishimura et al.), and others.
(c) Nearby Galaxy Project (COMING: CO Multiline Imaging of
Nearby Galaxies)
The COMING (CO Multiline Imaging of Nearby Galaxies)
project mapped about 140 nearby galaxies in 12 CO (1–0),
13CO (1–0), and C 18O (1–0) emission lines using FOREST,
and analyzed the data automatically. It was found that in thedwarf spiral galaxy NGC 2976 the fraction of the moleculargas depends on the surface density of the total gas (atomic andmolecular) and star formation rate (Hatakeyama et al.)

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2) Results from Open Use Programs with the 45-m telescope- Using also ALMA data, it is found that in the Barred
Spiral Galaxy M83 the CO Integrated Intensity Probability
Distribution Function (PDF) on the bright side in the bar hasa tail, while that in the arm does not (Egusa et al.). Also, it isfound that a large velocity dispersion is responsible for this tailand suppression of star formation.
- By comparing the molecular gas fraction and star formation
efficiency in nearby galaxies, it is found that star formation
activity in individual galaxies depends on molecular gas
content rather than the global environment (Koyama et al.).
- By observing two strong barred galaxies, NGC 1300 and NGC
5383, observational results were obtained supporting the
scenario that high-speed collisions in the bar suppress massive
star formation (Maeda et al.)- The most distant molecular cloud in our Galaxy from us was
discovered (Matsuo et al.).
- In an active star-forming filament G82.65-2.00, it was foundthat the filament is in the process of dispersing, and a region
possibly suggesting accretion onto the main filament throughthe striation was discovered (Saajasto et al.).
- By observing four massive star forming regions, it was foundthat there is HC5N in the warm molecular gas (Taniguchi et al.)
- By observing three 13C isotope molecules of HC3N, it was
found that the formation path differs depending on the region(Taniguchi et al.).
- H(C 5 )( 15 N) was discovered in the interstellar medium(Taniguchi et al.)
- By observing the Cygnus X region, it was shown that the CN/
C18O ratio is enhanced due to photodissociation (Yamagishi etal.).
- Observing 62 LIRG/ULIRG galaxies revealed that themolecular gas mass within several kpc is almost constant(Yamashita et al.).

2. Radio Polarimeters- Operations and maintenance were performed.
- On a monthly basis, the data are examined by solar researchgroups in Kyoto University, Ibaraki University, NICT, and
NAOJ Solar Observatory, and are archived as public data in
the NAOJ Astronomy Data Center so that researchers all over
the world can access them.
- 2 GHz: Data unavailability has continued due to the strong
interference since late June and the malfunction of an origin
sensor since December.
- 9.4 GHz: Data unavailability has continued due to themalfunction of an amplifier since late June and an origin sensor
since January.

3. Research Support(1) SPART (10-m telescope) (Osaka prefecture University)
To better understand the influence of the activities of hoststars on the atmospheric environment of habitable planets, we
continued monitoring observations of the planets in the Solar

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System at 100 and 200 GHz bands with a 10-m telescope, theSolar Planetary Atmosphere Research Telescope (SPART). For
investigations of short-, medium-, and long-term changes of
CO abundance in the Venusian middle atmosphere revealed
by SPART, we carried out synergetic observations with the
Atacama Large Millimeter/Submillimeter Array, and Japanese
Venus Climate Orbiter AKATSUKI (JAXA/ISAS) in May 2017,
and the 1.6-m Pirka Telescope (Nayoro Observatory, Facultyof Science, Hokkaido University) employing a Near Infrared
Echelle Spectrograph (The University of Tokyo) in July 2017.
These studies of the Venusian atmosphere allow us to address
the links between photochemistry and dynamical circulationof materials in the Venusian atmosphere and space weather
environment. In addition, in the NINS Nobeyama Exhibition
Room, we started to show the state of the remote operation and
the SPART observations in the computer display.
(2) Radio Heliograph (Nagoya University)
In FY 2015, an international consortium (ICCON) assumed
operation of the Nobeyama Radioheliograph (NoRH, see https://hinode.isee.nagoya-u.ac.jp/ICCON/). The remote operating
system via internet has functioned very well. About 30
researchers from seven countries (China, Germany, Japan, theRepublic of Korea, Russia, the UK, and the USA) participatedin operation, including the system health check and data
verification. Observational data are automatically transferred to
NAOJ and Nagoya University and are stored/maintained there.
Since the middle of February in 2018, we stopped the operationof NoRH because we found problems in some cables. They will
be exchanged and the operation of NoRH will be resumed inearly April in 2018. Using data of NoRH, one PhD thesis andseventeen refereed papers were published in Fiscal Year 2017.

4. Public Outreach(1) PR activities at Nobeyama Campus
The Nobeyama Campus received a cumulative total of
44,853 visitors throughout the year, including participants in
the Special Open House event. Staff members conducted 49
guided tours, including ones for Super Science High School(SSH) students and the Campus Tour Week, while 4 requests
for lectures and 36 requests for on-site filming and interviews
were granted. These requests, especially those by some local
broadcast stations in Nagano Prefecture, drastically increased
due to efforts to strengthen cooperation with local communities,
especially the “Nagano Prefecture is the Astro-Prefecture”
promotion. The Campus Tour Week for educational institutions
was scheduled during the summer. Six groups took advantageof this opportunity, and many students in the groups enjoyedthe visit. For the workplace visits, 9 students from 4 schools,
primarily local junior-high schools, visited the observatory. For
the SSH initiative, three schools visited NRO and participated in
lectures.
In the area for permanent public access, a controllable
radio-telescope antenna miniature and introduction movies areavailable along with posters and panel displays. In this year, weofficially inaugurated the Nobeyama Exhibition Room of NINS,
and open it every day.
Moreover, we received and answered about 170 phone calls
a year from the public regarding the regular opening of theobservatory, observatory events, and general astronomy.
(2) Cooperation with Local Communities
The annual Nobeyama Special Open House was held with
contributions by Nagano Prefecture as well as Minamimaki
Village, the Minamimaki Chamber of Commerce, and its
youth division. Moreover, Jimoto Kansha Day (Thanks Day
for the Locals) was held as the Special Open House for locals(Minamimaki and Kawakami Village) at NINS Nobeyama
exhibition room by NRO as the main host. Special sponsorshipwas made to the sora-girl event “Tebura de Hoshizora Kanshokai (Drop-by Star Gazing Event),” hosted by the Minamimaki
Tourism Association. The 29th national convention of“Hoshizora-no-machi, Aozora-no-machi (Streets of starry sky
and blue sky)” was held in Minamimaki Village by the Ministryof the Environment with Minamimaki Village as the host,which cooperated with Nobeyama Radio Observatory. The
commemorative lecture and guided tour of NRO facilities were
offered.
Moreover, a “Nagano Prefecture is Astro-Prefecture”
summer stamp-rally event was carried out as the first event by
the “Nagano Prefecture is Astro-Prefecture” liaison council,
which was founded through cooperation with Kiso Observatory
and other organizations last year. The second meeting was heldat the National Institute of Technology, Nagano College on
February 4 with about 80 participants. A lecture, some activity
reports, and discussion on the future activities were presented.
(3) NINS Nobeyama exhibition room
After the improvement work on the building of the
Nobeyama Millimeter Array, NINS Nobeyama exhibition room
was officially opened and started year-round operation. NINS
Nobeyama exhibition room was open to the public at the sametime as the open time of Nobeyama Campus. The opening
ceremony of NINS Nobeyama exhibition room and the press
conference with the President of NINS were held on April 29.
The 4D2U theater was operated during the summer seasonfrom April to September. The exhibition room played a role in
improving awareness of the other institutes of NINS as well as
NAOJ.

5. Education
NRO accepted one third-grade Ph.D. student in SOKENDAI
studying chemical reaction of carbon chain molecules.
SOKENDAI held the workshop on Radio Astronomical
Observation using the Nobeyama 45-m Radio Telescope from
June 5 to 9, with 12 undergraduate students in attendance. While
guiding the students, from observations to presentation of theresults, requires significant efforts, the event offers an invaluable
opportunity for undergraduates to experience observations using
a radio telescope and think of their future careers.

6. Misc. Activities(1) Nobeyama 45-m Radio Telescope was certified as milestonesof IEEE and IEICE
Nobeyama 45-m Radio Telescope was certified as milestonesof IEEE and IEICE. It was nationally and globally recognized
to have significant technical achievements and to have greatly
benefited industrial progress and regional society for a longtime. The commemorative ceremony including presentation of
the IEEE milestone plaque was held at Josui-Kaikan in Tokyo
on June 14. Moreover, the unveiling ceremony of the IEEE
milestone plaque and pedestal was held in NRO on June 16.
In these ceremonies, the telescope was greatly honored by the
local people including the village mayor as well as members
concerned with development and operation. It also seems tohave made great social and cultural contributions to the localarea.
(2) Hiring, Transfer (incoming)
Ken’ichi Tatematsu: Professor from NAOJ Chile Observatory
Masaru Takahashi: Senior Staff from Shinshu University
Hidemi Ide: Technical Expert, hired
Kim Gwanjeong: Specially Appointed Research Staff, hired(3) Retirement, Transfer (outgoing)
Kunio Iijima: Senior Staff, moved to Shinshu University
Yusuke Miyamoto: Specially Appointed Research Staff,
moved to NAOJ Chile Observatory
Hiroko Ide: Administrative Maintenance Staff, retired
Ikuko Koike: Administrative Maintenance Staff, retired
Jyunko Tsuchiya: Administrative Maintenance Staff, retired
Jyunko Kadoshima: Administrative Maintenance Staff,
retiredMichiko Kikuchi: Administrative Maintenance Staff, retired
Eiko Htakeyama: Administrative Supporter, retired
Chisato Tokui: Administrative Supporter, retired
Kotomi Taniguchi: SOKENDAI, obtained PhD(4) NRO Conference Workshops and Users Meeting- August 1–2, 2017, Nobeyama Radio Observatory
NRO45-m/ASTE Single Dish Science Workshop 2017
(Organizing Committee: Tomofumi Umemoto, Ken’ichi
Tatematsu (NRO), Daisuke Iono (Chile Observatory)- December 26–27, 2017, NAOJ Mitaka, Large Seminar Room
ALMA/45-m/ASTE Users Meeting 2017 (Organizing
Committee: Fumi Egusa (NAOJ Chile Observatory) Ken’ichi
Tatematsu, Tomofumi Umemoto (NRO), Daisuke Iono (NAOJ
Chile Observatory))

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4. Mizusawa VLBI Observatory
NAOJ Mizusawa VLBI Obser vator y operates VLBI
(Very Long Baseline Interferometry) facilities such as VERA(VLBI Exploration of Radio Astrometry) and KaVA (KVN
and VERA Array), and provides these unique facilities to theinternational user community to support the research activities
at universities and research institutes. In the meantime,
astronomical research using these VLBI arrays is conducted
mainly on the Galactic structure, celestial masers, AGN’s, andso on. Using the rare dual-beam system which is capable ofphase referencing by observing two sources simultaneously,
VERA conducts high-accuracy astrometry of maser sourcesand determines the detailed structure of the Milky Way. In
addition to the operation of VERA, maintenance and operation
support were provided to the Yamaguchi 32-m Radio Telescope
and two Ibaraki 32-m radio telescopes in collaboration withthe local universities. International collaboration has beenpromoted particularly in the East Asia region through the joint
operation of KaVA and East Asian VLBI Network, the latter ofwhich is a joint VLBI array between the People’s Republic ofChina, Japan, and the Republic of Korea.
In addition to VLBI related activities, “The Central
Standard Time” is kept at the observatory as an obligation of
NAOJ, Esashi Earth Tides Station is operated for geophysicalresearch, and Ishigakijima Astronomical Observatory is
jointly operated with the local city for public outreach andastronomical research.

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 2017, the total of 523 (4,160 hours) VLBI
observations were conducted with VERA, such as common
use observations, VERA project observations, fringe detection
obser vations for maser and reference sources, geodesy
observations, JVN (Japanese VLBI Network) observations,
KaVA (KVN and VERA Array) observations, and others.
These VLBI data, except for KaVA, were processed at theMizusawa Correlation Center in NAOJ Mizusawa Campus.
The correlated data were sent to each researcher for the case ofcommon-use and JVN observations and to persons in charge ofdata analyses in the case of project data and geodesy data.
VERA common-use call-for-proposals with the 43 GHz,
22 GHz, and 6.7 GHz bands for semesters 2017B and 2018A
were released in April and September, respectively. A total of
five proposals, which requested a total time of 112 hours, were
submitted, including one proposal for 30 hours from overseas.
Based on the evaluations by referees elected from scientists inrelated fields, VLBI program committee decided to accept a
total of five proposals (97 hours) in 2017B and 2018A.

064

II Status Reports of Research Activities(2) Science Research
In FY 2017, Mizusawa VLBI Observatory published atotal of 37 refereed journal papers for scientific achievements.
Among them, seven papers were published by the Observatory
staff or students as PI. For those directly related to VERA,
four papers were scientific results from VERA astrometry
obser vations, th ree were the results f rom Korea-Japan
international collaboration, KaVA, and eight were from otherdomestic and international VLBI arrays based on previous
studies with VERA. Representative observational results fromVERA are proper motion measurements of jets and shockedgas associated with water masers in high-mass star-forming
regions, and verification of high accuracy astrometry withmultiple phase calibration sources toward the Galactic Centerregion. In addition, as KaVA has started large programs since2016, verification results for amplitude calibration accuracy
and initial results for monitoring observations of a highvelocity radio jet ejected from an active galactic nucleus (AGN)
M87 were reported. In recent years, high resolution VLBI
observational studies are combined with new instruments,
and discussion on future projects such as ALMA, EHT (Event
Horizon Telescope), and SKA (Square Kilometer Array) has
been carried out. For these new projects, four, three, andone refereed journal papers, respectively, were published.
With ALMA, a rotating outflow was detected in a high-mass
protostar Orion Source I, which has been studied with VERA
for a long time. It provides important information on angularmomentum transfer in star-formation processes. In termsof future plans, a review paper on cosmic magnetism was
published, which will become one of the key sciences with the
future SKA.

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, NICT) to
make the Japanese VLBI Network (JVN), which is operated atthree bands of 6.7 GHz, 8 GHz, and 22 GHz. VLBI observations
were carried out for about 100 hours in total in FY 2017. The
main research subjects are active galactic nuclei and maser/starformation. In addition, single-dish observations of up to 2000
hours were carried out as research related to JVN by Ibaraki
University.
The University Collaborative Workshop was held at
Ibaraki in July 2016, and a white paper entitled “High-SpatialResolution/Time-Domain Astronomy in the centimeter band”
was approved as the baseline of the university collaboration.
Along with this white paper, maser/star formation study is led
mainly by Ibaraki University, while active-galactic-nuclei/
black-hole science is led by Yamaguchi University. In particular,
observations with the Ibaraki-Yamaguchi interferometer arethe key for these studies. Survey observations of 1) Compact
radio sources in the galactic center, 2) High-z AGN’s, 3) Fermi
gamma-ray sources, have been carried out.
Some papers were published in FY 2017 by using JVN,
such as Takefuji et al. (2017) for phase-up technique, Cho etal. (2017) for EAVN calibration, Morokuma et al. (2017) for
peculiar AGN with Optical/Infrared and VLBI collaboration,
and Yoshida et al. (2017) for follow-up observation for thegravitational wave event. Two short reports were issued as ATel
(Sugiyama et al. and Takefuji et al.) for transient events. For
development study, some students of Ibaraki and Yamaguchi
Universities were supervised by Professor Ogawa in Osaka
Prefecture University.

3. Japan-Korea VLBI
(1) Observations and Common Use Observations
In FY 2017, a total of 131 (1138 hours) VLBI observations,common use observations, large program observations, andtest observations, were conducted by KaVA (KVN and VERA
Array) at 43 and 22 GHz bands. The data of the seven VLBI
stations were correlated at the Korea-Japan Correlation Centerat KASI Daejeon campus in Korea.
KaVA common-use call-for-proposals for semester 2017
B and 2018 A were made in April and September of FY 2017,
respectively. In total, 23 proposals requesting a total timeof 888 hours were submitted. Through the evaluations byreferees elected from scientists in related fields and subsequentdecisions made by the VERA and KVN combined Time
Allocation Committee, in total 17 proposals (482 hours) were
accepted in 2017 B and 2018 A.
(2) Results of Research
The number of science results based on KaVA data is
steadily increasing since the opening of the KaVA common
use in FY 2014. In FY 2017, two research papers that made useof KaVA common-use data were published in peer-reviewed
journals, one proceedings of an international conference waspublished, and one paper was submitted to a peer-reviewed
journal. These include a detailed monitoring of the M87 jet(Hada et al. 2017), detailed observations of SgrA* (Cho etal. 2017, Zhao et al. 2017), and the discovery of jet-cloudinteraction in 3C84. These sources are all key sources forstudying AGN activities, and these publications demonstrated
that KaVA is a powerful tool to investigate AGN physics.
The th ree KaVA Large Programs (LP), which werelaunched in late FY 2015, are continuing smoothly, and theanalyses of these data are actively ongoing by each KaVA
Science Working Group (AGN, star-formation regions, latetype stars). An interim review of the LP’s was made at Daejeon
in November. Although there was a comment that the numberof publication for each LP was still relatively small, the review
result was overall positive because a number of interesting
preliminary results have already been obtained. Therefore, thecontinuation of the LP’s was approved expecting that more
publications will be out soon. The LP data are also used formaster/PhD theses of new students.

4. EAVN
To expand the capability of the inter national VLBI
throughout East Asia, the commissioning of the East Asia VLBI
Network (EAVN) is actively ongoing through collaboration
between Japan, the Republic of Korea, and China. In FY 2017,
EAVN commissioning observations were performed for a totalof 13 epochs (and a total of 13 stations joined), which is thelargest EAVN campaign ever made. In particular, the ShanghaiTianma 65-m station joined all of these sessions, and we
succeeded in quasi-regular EAVN operation. Moreover, thesedata allowed detailed performance evaluation of the Tianma
station. As a result, it was officially approved that the commonuse of KaVA+Tianma (plus partially Nobeyama) will open fromthe second semester of FY 2018 (up to 100 hours per semester).
The activities of EAVN were presented at the annual
conference of the Chinese Astronomical Society held in
Urumqi. We also made intensive discussions to accelerate
EAVN commissioning including Urumqi/Nanshan, which
contributes to the longest EAVN baselines. We aim to start the
EAVN common-use including Urumqi from FY 2019.
Along with the com missioning, continuous effor ts
have been made to produce early EAVN science results bycollaborating with the Event Horizon Telescope which observes
nearby supermassive black holes.

5. Future Plans for SKA
The obser vator y has been investigating The Square
Kilometre Array (SKA) Project as one of the possible future
projects of the observatory. In FY 2017, the observatory
released a report on SKA science cases which have beenstudied by the observatory task force for two years. The reportconcludes that, with SKA, we can extend our current research
quantitatively and can evolve our future research qualitatively.
Next, based on a request from the Japan SKA Consortium,
the observatory examined the way to establish the NAOJSKA Promotion Office (NSPO). The observatory provided
opportunities for discussion about SKA at the VERA users
meeting and VLBI Consortium symposium. A consensus forestablishing NSPO has been growing in the VLBI community.
The observatory consulted about NSPO with VLBI and Radioadvisory committees in NAOJ and obtained positive statements
about the NSPO proposal. Through these processes, theobservatory applied to establish NSPO as a new sub-project in
NAOJ.
For the first two years of the project, NSPO will define
the project. NSPO will start preliminary negotiation about
Japanese participation and investigate possible options forscientific and engineering strategies. For the next three years,
NSPO will execute the project, i.e. formal negotiation, funding,and design reviews, and will achieve Japanese participation in
SKA1 as a minor partner.
Finally, the observatory applied to the SKA organization

II Status Reports of Research Activities065

for a SKA pathfinder designation for VERA. This would be
beneficial for enhancing the international presence of VERA,
and for promoting SKA science and technology with VERA.
The application was approved recently.

6. Geodesy and Geophysics
The regular geodetic sessions of VERA are allocated two or
three times per month to maintain the orientation and figure of
the array. VERA internal geodetic observations are performed
once or twice per month using K-band, and Mizusawa station
participates in IVS sessions using S and X-bands on a onceper-month basis. The experimental observations which aimed
at the improvement in accuracy of the solution by wideband
recording were also continued, and a satisfactory result was
obtained.
In FY 2017, we participated in eight IVS sessions andperformed 18 VERA internal geodetic sessions including a
joint VERA and KVN geodetic session. The final estimation ofgeodetic parameters was reconstructed in the ITRF2014 systemand derived by using the software developed by the VERA team.
After “The 2011 Earthquake off the Tohoku Pacific coast”(Mw = 9.0), displacement of Mizusawa station continued bypost-seismic creeping, and the position of Mizusawa station
changed by 6.4 cm during FY 2017. And, in Ogasawara andIshigakijima, f luctuations of the displacement by slow slip
events were detected.
Continuous GPS observations at VERA stations are carriedout in order to detect short term coordinate variations and to
estimate atmospheric propagation delays. The result of GPS
positioning at Mizusawa shows a post-seismic motion to theEast-Southeast direction even though seven years have passed
since the occurrence of the 2011 earthquake. The gravity tide
observation data at VERA stations were analyzed and the tidal
displacements were estimated. The observed displacements
were consistent with the Earth Model which is used in VERA
data reduction. We confirmed that the tidal displacements neveraffect the accuracy of VERA astrometry observations. The
gravity change observation at Ishigakijima continued throughjoint work with other institutes and universities. The strain andtilt observation data obtained at the Esashi Earth Tides Station
are distributed in real time to several institutes based on the
research agreement between the Earthquake Research Institute,
the University of Tokyo, and Mizusawa VLBI Observatory.

7. System Development
In FY 2017, we have developed two down-converters andIF-switches for dual polarization receiving of the Q-band. We
have installed these instruments at Mizusawa and Iriki andperformed a VLBI experiment. As a result, we obtained good
fringes and started scientific test observations with KaVA. We
have installed new RF direct A/D samplers “OCTAD” andhigh-speed recorders “OCTADISK2” developed by NAOJ
at all the VERA stations and performed VLBI experiments
at a recording rate of 8 Gbps. We successfully obtained

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fringes between all the stations. We continued discussion on
the SKA project and high frequency VLBI as future plansof Mizusawa VLBI Observatory. With regard to SKA1, we
considered development of the Band 5C broad-band receiver,AIV (Assembly, Integration, and Verification), and VLBI backend system development as potential items to be contributed
from Japan. With regard to SKA2, we performed various basic
design and development, including a low power consumption
optical transmitter/correlator. With regard to high frequency
VLBI, we performed various development and AIV for aballoon-borne VLBI station. The system was completed andwas ready to be launched in the 2017 summer season. However
due to bad weather, its launch was postponed to next year.

8. Timekeeping Office Operations
The Timekeeping Office operates four cesium atomic
clocks together with a hydrogen maser atomic clock at VERA
Mizusawa Station. The facilities have been operating stably,
contributing to the determination of UTC (Coordinated
Universal Time) through continuous management and operationof the time system. The NTP (Network Time Protocol) serverat the Timekeeping Office provides “Japan Central Standard
Time” on a network. This service has been in great demand;
more than 1,500,000 daily visits were recorded last year.

9. Ishigakijima Astronomical Observatory
FY 2017 was the 12th year of Ishigakijima Astronomical
O b s e r v a t o r y ( I AO). Fo u r r efe r e e d p a p e r s u si n g t h eobservational data of IAO were published, and the total number
has reached 23. The number of visitors was 14,000 people andhas exceeded 10,000 people for the past five years in a row. The
establishment purposes of observational study, public outreach,and regional promotion have been accomplished satisfactorily.
The commemoration ceremony for reaching 120,000
visitors was held in January. The number of foreign tourists has
increased in recent years, from 450 in the previous year to 795
people this year.
In terms of the research, observations of transient objects
were conducted in collaboration with Japanese universities,
and the follow-up observations of Near-Earth Objects werealso carried out in accordance with an invitation from JAXA.
IAO participated in two international projects: JOVIAL for
detection of Jupiter’s oscillation with Japan, France, and theUnited States and GROWTH with Titech, Caltech, and others;
several joint observations were performed. As for the research
results, refereed papers including the study of a binary blackhole V404 Cyg and comet C/2013 US10 were published.
In regards to the education, more than 1,000 people visited
IAO as part of group visits from elementary and junior highschools, and inspections from government offices. The lifelong
study for Okinawa prefectural inhabitants was opened in July.
The Chura-boshi Research Team Workshop for high school
students and the observational experiment for undergraduate
students of the University of the Ryukyus were held inAugust. The lecture for the 179th committee of JSPS photonics
information system was carried out in December.
As for the public outreach, three special events were held.
At the Golden Week event, 610 people attended in five days.
In the “Southern Island Star Festival” event, 1,043 people
visited to IAO in nine days. And 78 people joined in the springvacation event “Urizun Starry Sky Class” in three days. In the
16th year of “the Southern Island Star Festival,” which is hosted
by Ishigaki City and IAO from August 12 to August 20, 11,337
people participated. At “the Star Festival” held in Kohamajima,
which is hosted by IAO and Yaeyama greater metropolitan
area affairs association, 300 people attended. Approximately
200 people joined in the weather class for parents and children
hosted by Ishigakijima local meteorological observatory and
IAO.
On the other hand, IAO cooperated with the international
conference of “the East Asian Young Astronomers Meeting2017” (73 participants) held in November, and many foreign
participants joined in the star party. After the conference,the public lecture “Frontiers of astronomy –two astronomical
discovery stories-” was held, and more than 30 people took partand contributed to the regional development through the two
events.

10. Public Relations (PR) and AwarenessPromotion Activities(1) Open House Events
At each telescope site operated by Mizusawa VLBI
Observatory, we held the following open house events.
On April 16, 2017: the Eighth Open Observatory Eventheld at the Ibaraki University Center for Astronomy, and
NAOJ Mizusawa VLBI Observatory, Ibaraki Station, with acumulative total of 1,141 visitors in attendance.
On July 16: The Star Festival at the site of the 6-m
antenna at Kinko Bay Park in Kagoshima City co-hosted
with Kagoshima Cit y and Kagoshima Universit y, withapproximately 350 visitors.
From August 12 to August 20: “The Southern Island
Star Festival 2017” held together with the special open house
event at the VERA Ishigakijima Station and Ishigakijima
Astronomical Observatory with 11,337 visitors to the whole“Star Festival.” Events included the astronomical observation
party at Ishigakijima Astronomical Observatory, attended by
1,043 visitors; and the special public opening of the VERA
Station attended by 273 visitors.
On August 12: Special open house of VERA Iriki station
held jointly with “The Yaeyama Highland Star Festival 2017,”
with approximately 3,800 visitors in attendance.
On August 19: “Iwate Galaxy Festival 2017,” open houseof NAOJ Mizusawa Campus, held with 1,165 visitors inattendance.
On January 20, 2018: “Star Island 17,” open house event of
VERA Ogasawara Station held, with 167 visitors in attendance.
(2) Regular Public Visiting

Throughout the year, the following stations are open to the
public on a regular basis. The four VERA stations are open to
the public every day, 9 a.m. to 5 p.m., except during the New
Year’s season. Ishigakijima Astronomical Observatory is open
10 a.m. to 5 p.m., Wednesday to Sunday except during the New
Year’s season and other closures.
The numbers of visitors to each facility are as follows,a) VERA Mizusawa Observatory 19,389
The campus is regularly open to the general public with thecooperation of the Oshu Yugakukan (OSAM: Oshu Space &Astronomy Museum) located in the campus.
b) VERA Iriki Station 1,602c) VERA Ogasawara Station 8,340d) VERA Ishigakijima Station 2,577e) Ishigakijima Astronomical Observatory 14,192
Stargazing sessions: Evenings on Saturdays, Sundays.
“The Starry Sky Study Room” (featuring the 4D2U “FourDimensional Digital Universe”), constructed adjacent to theobservatory in FY 2013 by Ishigaki City, was very popular,
welcoming 4,478 guests.

11. Education(1) Under-graduate and Post-graduate Education
Regarding postgraduate education, Mizusawa VLBI
Observatory assisted two doctor and one master students
from the University of Tokyo, and two doctor and one masterstudents from SOKENDAI for their thesis research. One of
the students from the University of Tokyo completed his Ph.D.
thesis. In addition, one master course student from Yamaguchi
University was accepted for education. Two undergraduate
students from Tokyo University of Science and Ochanomizu
University were accepted as summer students of SOKENDAI.
The University of the Ryukyus and NAOJ have offered a joint
course on astronomy from FY 2009. Classroom lectures at
the university took place August 21, 23–25 at the Nishihara
main campus and were opened to the public at the satellite
campuses. Observational workshops were held in Ishigakijima
from August 28–31, with about 33 participants. In addition,
staff members of Mizusawa VLBI Observatory give lecturesat the University of Tokyo, Tohoku University, and Teikyo
University of Science as visiting professors. In 2018 fromJanuary 16 to January 19, NARIT-SOKENDAI Winter School
was co-organized under collaboration with NARIT in Chiang
Mai, Thailand. 21 students, mainly from Thailand and SouthEast Asian countries, attended the school. From Japan, three
students from the University of Tokyo and SOKENDAIat tended , a nd fou r st af f members of Mi z usawa V LBI
Observatory gave lectures in the school.
(2) Research experience for high school students
From August 9 to August 11, the VERA Ishigakijima
station and the Ishigakijima Astronomical Observatory held
“the Churaboshi Research Team Workshop” for 10 local highschool students including three from the Okinawa main island.
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Research Team Event” was held from August 4 to August 6 touse the VERA Mizusawa antenna for observation. A total of
12 high school students from the Tohoku region were accepted
for research experience. From this year, a similar observational
event was started at VERA Ogasawara station and one local
high school student was accepted for this program from July
20 to July 22. Continued from previous years, Mizusawa VLBI
Observatory supported the SSH (Super Science High school)
research activities for Akita Prefectural Yokote Seiryo HighSchool to use the Mizusawa 20-m antenna.

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5. Solar Science Observatory (SSO)
This project started at the beginning of FY 2017 bycombining two projects, the ‘Hinode Science Center’ and‘Solar Observatory,’ to proceed the cutting-edge science fromobservations with the Hinode satellite and ground-based
observatories.

1. Hinode Space Observatory
The scientific satellite Hinode is an artificial satellite that was
launched on September 23, 2006, by the ISAS division of JAXA,
as Japan’s third solar observational satellite following Hinotori(1981) and Yohkoh (1991). Hinode is equipped with threetelescopes: the solar optical telescope (SOT), the X-ray telescope(XRT), and the extreme ultraviolet imaging spectrometer (EIS).
In addition to the detailed magnetic field and velocity field of thesolar photosphere, it carries out simultaneous observations of theradiance and velocity field from the chromosphere to the corona.
The telescopes equipped on the Hinode satellite were developed
through international collaboration with the US NASA and the
UK STFC under the cooperation of ISAS/JAXA and NAOJ,
and the European Space Agency ESA and the Norwegian Space
Center NSC join its scientific operations. NAOJ played a central
role in the development of the science payload in Japan and has
been making a significant contribution to the science operationand the data analysis since the launch. The data acquired with
Hinode is released to everyone as soon as the data for analysis
are ready.
The Hinode Science Working Group (SWG), composedof representatives from the international team, offers support
in scientific operation and data analysis. It has a total of 17
members, including two from SSO: Y. Suematsu for SOT and
T. Watanabe for EIS. The Science Schedule Coordinators (SSC)
have been organized to leverage the open-use observation
system. Two Japanese members from NAOJ (Sekii for SOTand Watanabe for Co-chairman/EIS) join the SSC activity. The
SSC serves as a window observation proposals from world
solar physics researchers to use Hinode and promotes joint
observations between Hinode and the other science satellite or
ground-based observatories.
FY 2017 corresponds to the first year of the third extension
period (FY 2017 to FY 2020) on the Hinode science operation.
During this period; the emphasis is placed on the evolution of
the magnetic field at the site of solar flares, observations of thelocations of magnetic reconnection; long-term observation ofgeneral magnetic fields in the photosphere during the declining
activity phase; and joint observations with the ERG satellite,
ALMA, and new ground-based observatories. The Hinodescience payload has been steadily observing the Sun from space,
except for the SOT imaging instrument which was terminatedin Feb 2016. New science results have been obtained via joint
observations with SDO, IRIS, ALMA as well as long-term
standalone observation by Hinode. The number of Hinoderelated referred papers published in FY 2017 is 87, and further

achievements are expected in the coming years.
The power switch of EIS suddenly turned off on January
21, 2018 and the science operation was suspended for a longtime beyond the end of the fiscal year. The recovery operation is
postponed until May 2018 in order to prepare for the recovery
procedure with careful event analysis and to prioritize joint
observations with ALMA.

2. Ground-based Observations in Mitaka
CampusFull-disk observations of the Sun have been carried out on
the western area of the Mitaka Campus for recording the solar
activity. The primary instrument is a telescope measuring thesolar magnetic fields. The others are an Hα imaging instrumentfor detection of solar flares as sudden phenomena and an opticalimaging instrument observing sunspots and active regions as aproxy of long-term solar magnetic activity.
The magnetic field observation that has been conductedwith the Solar Flare Telescope (SFT) since 1992 has provided
vector magnetic fields in the photosphere with a field of view
covering sunspot regions by observing an absorption line in
the visible wavelength range. It has been replaced with nearinfrared Stokes polarimetric observations since 2010 for higher
precision measurement of magnetic fields in the chromosphereat 1.083 microns and those in the photosphere at 1.565 microns.
Factors that determine the efficiency and precision of magnetic
field measurements are the imaging pixel format of the imaging
camera and the read noise. Toward introduction of a large-format
detector and low-read-noise performance, an imaging camera
with an H2RG sensor is being developed in the Program of the
Solar-Terrestrial Environment Prediction (PSTEP), Grand-inAid for Scientific Research on Innovative Area.
The sunspot observation that started in 1929 continues,
although it was upgraded to imaging observation using a digital
camera in 1998. Full-disk imaging observations in the visible
continuum, the G-band (430 nm), Ca II K line (393 nm), and Hαline (653 nm) are regularly conducted with the SFT to monitor
the photosphere and chromosphere which change according
to the solar magnetic activity. The Hα observation is currently
carried out at multiple wavelength points within the absorption
line with narrow-band filters to enable the measurement of the
Doppler velocity and watch eruptive prominences associatedwith solar flares. These regular observation data including a setof real-time images are available on the SSO website.
NAOJ has long-term solar observation data, the initial
70 years of which were acquired by the Tokyo Astronomical
Observatory, the predecessor of NAOJ. FY 2017 corresponds to
the 100th anniversary since the record keeping began. Full-disk
images, observed in the continuum, Ca II K line, and Hα line,
were recorded on film, photographic plates, and hand-drawn
sketches. SSO proceeds with the digitization of these data forresearch on the long-term variation of the solar activity. While

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these digitized data are opened to the public when ready, highprecision digitization has been applied to the Ca II K line data for
improving the quality as a part of the PSTEP research activity.
Although the Nobeyama Solar Radio Observatory (NSRO)
was closed at the end of FY 2014, the observation of intensity
and circular polarization at seven frequencies, acquired over ahalf century, continues because of its importance in monitoring
long-term solar activity. The Nobeyama Radio Observatory
carries out the operation and maintenance of the automatedtelescope system, and SSO leads the scientific verification andcalibration of the data with the solar researchers in universities
and the National Institute of Information and Communications
Technology.
In addition, members in SSO have observed the total solar
eclipse on August 21, 2017 in Idaho, USA, and imaging andpolarization observations were carried out.

3. SDAS
Solar Data Analysis System (SDAS) in the Astronomy Data
Center (ADC), which developed from the open-use data analysis
system of the Hinode Science Center and NSRO in addition to
the data archive/public release system of the Solar Observatory,
fulfilled the roles of data analysis and data distribution, andit finally completed its task at the end of FY 2017. The data
analysis functionality was integrated into the ADC Multiwavelength Data Analysis System, and the new SDAS, Solar
Data Archive System, has started since the end of FY 2017 forthe archiving and public release of the solar data. SSO operated
SDAS with ADC.

4. Educational Activity
The Project accepted and teaches two Ph.D. course students
and two Master course students, and two postdocs (Specially
Appointed Research Staff) belong to SSO. Two members (T.
Sekii and H. Hara) contributed to the undergraduate course
lectures in astronomy at the University of Tokyo.

5. Public Outreach (PO) Activity
SSO has been conducting various public outreach activities
for education and returning the results obtained through thescientific research of the Sun to the public: exhibition boothat academic conferences and symposiums, press releases, web
releases, cooperation for exhibition activity at science museums,
media appearances by responding to media interviews andproviding materials to the media, etc. The following were createdin the FY 2017 SSO PO activity: explanatory videos for the
10th Hinode anniversary, new Hinode pamphlet revised with thelatest results, and solar VR contents developed for the exhibitionat the FY 2017 NAOJ open house. Since the VR contents were
well-received by visitors, the distribution of the software forsmartphones is planned. In addition, there were many media
interviews on the large solar flares that occurred in September
2017, which shows that it was a subject of social concern.

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6. Science and Community Meetings
The Hinode Science Meeting has been regularly held toadvance the solar physics research with the Hinode satellite. We
co-organized the 11th meeting held May 30 to June 2, 2017 in
Seattle, USA. The number of participants and papers were 130
and 129, respectively.
In cooperation with the DKIST Project, the 4 m diameter
solar telescope scheduled to start its operation in 2019, SSO
co-organized the DKIST workshop for the initial observation
plan at Nagoya University on February 26–29, 2018. The
initial science plan on the research subject of the photosphereand chromosphere has been discussed, and as a result, manyobservation proposals were created during the workshop.
SSO co-organized two solar physics community meetings:‘Research of the Sun from Space in the 2020s’ (July 13, 2017at NAOJ, Mitaka) and ‘JSPC (Japan Solar Physics Community)
Symposium’ (February 20–22, 2018 at Kyoto University).

7. Awards
The following staff in SSO have been awarded for theirresearch activity:
Y. Katsukawa: 6th NINS Young Researcher Award
R. Kano: 4th ISAS Award

8. Others
The Project Review Committee reviewed the SSO research
activity in FY 2015–2017.
Prof. V. Pipin of the Russsian Academy of Sciences andProf. S. Brun of CEA Pris-Saclay stayed as visiting professors
over an extended period (more than a month).
Prof. T. Watanabe and K. Yaji left NAOJ at the end of FY
2017. The personnel transfer of M. Fujiyoshi to another projectis scheduled.

6. NAOJ Chile Observatory
The ALMA Project is a global partnership of East Asia
(led by Japan), Europe, and North America (led by the UnitedStates) in cooperation with the Republic of Chile to operate agigantic millimeter/submillimeter radio telescope deploying
66 high-precision parabolic antennas in the 5000-m altitude
Atacama highlands in northern Chile. ALMA aims to achievea spatial resolution of nearly ten times higher than that of the
Subaru Telescope and the Hubble Space Telescope. Early
scientific observations with ALMA began in FY 2011 with apartial number of antennas and full operation commenced in FY
2012. This report describes the progress of the project, which
includes results of the open-use scientific observations andpublic outreach activities. The ASTE telescope is a single-dish10-m submillimeter telescope located in the Atacama highlands
and has been operated to make headway into submillimeter
observations toward the ALMA Era. This report also describes
the progress of the ASTE telescope.

1. Progress of ALMA Project
ALMA scientific observations and commissioning
observations are currently underway. Commissioning
observations include polarization tests, solar observation tests,
and observation tests using the newly installed Band 5 receiver,which are all making good progress. In these activities, East
Asian researchers have been taking initiatives in international
teams, as demonstrated by Koichiro Nakanishi and Hiroshi
Nagai for polarization, and Masumi Shimojo for solar
observation tests. Also, the sub-components developed by Japansuch as the antennas, correlators, and receivers (Bands 4, 8, and
10) are working properly.

2. ALMA Open-Use and Scientific Observations
The sixth round of ALMA open-use observationscommenced in October 2017 as Cycle 5. The main capabilities
of Cycle 5 include: interferometric observations using fortythree 12-m antennas; Atacama Compact Array (ACA)
observations (interferometric observation with ten 7-m antennas
and single-dish observations with three 12-m antennas);eight frequency bands (Bands 3, 4, 5, 6, 7, 8, 9, and 10); andmaximum baselines extended to 16.2 km (for Bands 3, 4, and 6),
8.5 km (for Band 7), 3.6 km (for Bands 8, 9, and 10) and 1.4 km(for Band 5). In addition to these, Cycle 5 continuously provides
open-use opportunities for large programs that require longobservations over 50 hours, millimeter-wavelength VLBI, ACA
stand-alone mode, solar observations, polarization for spectralline observations, and new Band 5 observations. In response to
the Cycle 5 call for proposals, 1,661 proposals were submitted
from all over the world.
The call for the seventh round of open-use observations
was issued as Cycle 6. The Cycle 6 capabilities will include:interferometric observations using forty-three 12-m antennas;

ACA observations (interferometric observation with ten
7-m antennas and single-dish observations with three 12-m
antennas); eight frequency bands (Bands 3, 4, 5, 6, 7, 8, 9, and10), maximum baselines of 16 km (for Bands 3 to 6), 8.5 km(for Band 7), and 3.6 km (for Bands 8 to 10). Also, Cycle 6 will
provide new circular polarization in Bands 3 to 7, and Band 8
ACA standalone mode. Another remarkable progression is thatthe Band 6 IF bandwidth has been extended to cover 4.5 to 10
GHz. The call for proposals for Cycle 6 is set to be closed at
00:00 JST on April 20, 2018. Cycle 6 is scheduled to start in
October 2018.
Open use of ALMA has already produced a numberof scientific results. This section describes some of theachievements focusing mainly on East Asian projects.
A research team led by Tomoya Hirota observed a massive
baby star called Orion KL Source I with ALMA and imaged
clearly the rotation of outflow ejected from the baby star. The
result shows the outflow carries angular momentum awayfrom the system, which gives us a clue to understanding how
interstellar material dissipates angular momentum in accretion
onto a baby star.
Ryo Ando, a graduate student of the University of Tokyo,
and his colleagues observed the center of the starburst galaxy
NGC 253, an active star forming region, with ALMA highresolution and identified eight clouds of star-forming gas. From
the results, it was found that the eight clouds have evident
diversity in their chemical composition and signal strength,
as the data of one cloud shows an extremely rich chemicalcomposition filled with the signals of various molecules forming
a “molecular forest.” This is the first molecular forest ever foundoutside the Milky Way Galaxy, which indicates that there must
be an enormous diversity among star-forming molecular clouds
in the starburst galaxies.
Masatoshi Imanishi at NAOJ and his colleagues observed an
active galactic nucleus (AGN) at the center of the spiral galaxy
M77 with ALMA high-resolution and imaged a rotating gas
torus around an active supermassive black hole. Such structure
was theoretically suggested as ‘the unified model of AGN’ andthey successfully proved the theory true through observation for
the first time. This is an important step in understanding the coevolution of supermassive black holes and their host galaxies.

3. Educational Activities and Internships
During summer vacation of universities, the NAOJ Chile
Observatory accepted six undergraduate students, four of whichwere involved in research activities in Mitaka and the other two
in Chile. Also, the NAOJ Chile Observatory accepted one postdoctoral fellow as a visiting researcher for a month each fromthe University of Utah (US.), Leibniz Institute for Astrophysics
Potsdam (Germany), and Thai Nguyen University (Vietnam).
On March 9, 2018, the NAOJ Chile Office and the Joint
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Yamagata University as part of the university’s short-term study
program in Chile. The visit includes the introduction of the
ALMA project and a talk session between students and staff
members working at an international institute overseas, which
served as a valuable opportunity for them to reflect on theircareer paths.

4. Public Outreach Activities
Achievements of ALMA scientific observations and test
observations were covered by nearly 110 newspaper/journal
articles and 8 television/radio programs, reporting ALMA
observation results in various fields of astronomy. In particular,
the detection of the rotation of outflow ejected from Orion KL
Source I with ALMA was featured on a news program called“News Shibu Go Ji” on NHK G channel and another news
program called “Your Time” on Fuji Television in June 2017.
The observation results of Orion KL Source I were covered bymore than 180 news websites worldwide, while the detectionof the rotating dusty gaseous donut around a black hole at thecenter of the spiral galaxy M77 was posted on more than 200
news websites. As demonstrated by these figures, the scientificresults by Japanese researchers have been increasingly broadcast
worldwide.
In November 2017, twelve Japanese journalists including
newspaper/magazine writers and freelance writers participated in
the ALMA Site Media Tour that includes the visits to the ALMA
Santiago Central Office (SCO), NAOJ Chile Office, ALMA
Operations Support Facility (OSF), and Array Operations Site
(AOS); photo/movie sessions; and interviews with researchersand engineers. The reports of the tour were covered by many
newspapers and magazines, providing information on the ALMA
site, latest results, and the future development plan of ALMA
widely to the public.
The NAOJ ALMA website was renewed in May 2017.
The new site has an increased number of articles including
review articles that summarize the ALMA research themes andinterviews with ALMA staff members, together with 49 news
articles and eight press releases posted this year. Furthermore,
the contents of the new website (e.g. images) became more
openly available in accordance with the terms of use under theCreative Commons License, which allows easier use of contents.
A mailing-list-based newsletter has been issued on a monthly
basis with approximately 2,500 subscribers. Updated, detailed
information is available on Twitter (@ALMA_Japan), withnearly 38,500 followers as of the end of FY 2017.
In May 2017, the NAOJ Chile Observatory hosted a weeklong ALMA booth at the Japanese Geoscience Union Meeting
held in Makuhari Messe. Public lectures and Science Cafe
events were organized on 15 occasions in FY 2017 to makethe current status and achievements of ALMA widely known
through dialogue with visitors. In particular, the NAOJ Public
Talk / the 23rd ALMA Public Lecture titled “ALMA Telescope
Exploring the Cold Universe – To Solve the Mysteries ofPlanetary Formation with State-of-the-Art Technology”, held at
the Tokyo International Exchange Center (TIEC) on February

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4, 2018, attracted a big audience of over 200, which was a great
opportunity to introduce the latest scientific results of ALMA to
the public.
From mid-March 2015, ALMA started to accept public
visitors to the ALMA Operations Support Facility (OSF) at analtitude of 2900 meters. Every Saturday and Sunday, ALMA
is open to the public up to 40 people/day (advance registrationis required). Visitors to the OSF can have a guided OSF tour
including the control room tour and videos on ALMA. The
registration often reaches the full capacity soon after the startof registration every weekend. Public visits to ALMA are now
becoming a good opportunity to provide many people with live
experience at the workplace of ALMA researchers. The numberof public visitors in FY 2017 amounted to 3,904 people.
On August 25 and 26, a traditional TANABATA event
was held in San Pedro de Atacama, a town at the foot of the
ALMA site. Inviting local residents and tourists to write wishes
on tanzaku (small pieces of colored paper), the TANABATA
star festival was celebrated with tanzaku decorations onbamboo stalks and star gazing. The event served as a public
outreach activity for the ALMA project and NAOJ as well as anopportunity to promote international friendship.

5. International Collaboration (committees, etc.)
In the international ALMA project, meetings are held
frequently by various committees. In FY 2017, the ALMA Board
met face-to-face twice, and the ALMA Scientific Advisory
Committee (ASAC) twice. In addition to these, teleconferences
have been held on a near-monthly basis among the members of
the ALMA Board and ASAC. The ALMA East Asian Science
Advisory Committee (EASAC) had meetings face-to-face or via
teleconferences on a quarterly basis. Each working group holds
meetings and teleconferences more frequently to maintain close
communication in implementing their respective tasks in theinternational project.

6. Workshops and Town Meetings• Aug 1 to 2, 2017 NRO45/ASTE/Single Dish Science Workshop
2017 at NAOJ Nobeyama Radio Observatory (NRO)• October 3 to 5, 2017 ALMA Long Baseline Workshop at
Mielparque Kyoto• December 27 to 28, 2017 ALMA Users Meeting at NAOJ
Mitaka• March 26, 2018 ALMA Town Meeting at Kagoshima
University

7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research including
Industry –University Collaboration Expenses• Hitoshi Kiuchi: Funded externally by the Ministry of Internal
Affairs and Communications (Strategic Information andCommunications R&D Promotion Programme: SCOPE) R&D
for Promotion of Effective Radio Use (Advanced Effective

Radio Use-Phase II)

8. Research Staff Changes(1) Hired• Daniel Walker: Specially Appointed Research Staff• Andres Guzman: Specially Appointed Research Staff• Yu-Ting Wu: Specially Appointed Research Staff• Andrea Silva: Specially Appointed Research Staff• Yuri Nishimura: Specially Appointed Research Staff(secondment to the University of Tokyo)• Tao Wang: Specially Appointed Research Staff (secondment to
the University of Tokyo)• Salinas Nicolas: Specially Appointed Research Staff(secondment to Kagoshima University)• Kei Tanaka: Specially Appointed Research Staff (secondment
to Osaka University)(2) Departed or transferred• Toshiki Saito: Specially Appointed Research Staff• Naslim Neelamkodan: Specially Appointed Research Staff

9. Main Visitors• June 25, 2017
Prof. Kajita Takaaki, Director of the Institute for Cosmic Ray
Research (ICRR) at the University of Tokyo visited the ALMA
site.
• July 29, 2017
Mr. Yoshinobu Hiraishi, Ambassador of Japan to Chile, visited
the ALMA site.
• September 28, 2017
Japan’s Prince Akishino and Princess Kiko visited Chile.
NAOJ Chile Observatory Director Seiichi Sakamoto explained
the NAOJ projects.
• January 12 to 13, 2018
The Japanese State Minister of Education, Culture, Sports,
Science, and Technology, Toshiei Mizuochi visited ALMA.

the future, ASTE will continue to be important for nurturing
young researchers who will play key roles in the equipment
development for the next generation. In the near future, ASTE
will be incorporated into the open-use program for promoting
organic collaboration with the Nobeyama 45-m Telescope.
The open-use program in FY 2017 provided spectroscopic
observations in 345 GHz and 460 GHz bands for a period offour months. To render support for researchers contributing
to the observational performance enhancement of ASTE,
the Guaranteed Time Observation (GTO) scheme has beenoffered since FY 2013, which allows them to exclusively makeproposals for the GTO slots. A total of 25 proposals for open-use
observations were submitted. These proposals were reviewed
by the Millimeter/submillimeter Program Subcommittee and 20
proposals were adopted. Open-use observations were carried out
from the ASTE Mitaka operation room or from other universities
and research institutes from early June to late September, 2017.
Also, the ASTE telescope has been tentatively equipped withDESHIMA (Deep Spectroscopic High-redshift Mapper), a
superconducting on-chip filterbank spectrometer under joint
research and development by Delft University of Technology(Netherlands), SRON (Netherlands), the University of Tokyo,
Nagoya University, and the National Astronomical Observatoryof Japan since October 2017, and successfully detected
astronomical spectra for the first time with this new technology.
On November 21, 2017, the ASTE telescope had a failurein the Azimuth drive that went out of control during a remoteobservation. The result of investigation shows that the cause of
the failure was age deterioration of the AZ reduction gear andthe device must be replaced.

10. Progress of ASTE Telescope
The ASTE telescope has been operated to promote fullfledged submillimeter astronomical research in the southernhemisphere and develop/verify observational equipment andmethods required for submillimeter astronomy. With the ALMA
telescope entering its operation phase in FY 2012, ASTE will be
used mainly to provide observational evidence for strengthening
ALMA observation proposals and promote development for theenhancement of ALMA’s future performance.
Except for ALMA, there are only two large-scale
submillimeter telescopes with a 10-m-class antenna that canobserve the southern sky in the world: one is ASTE and theother is APEX operated by Europe. Therefore, having ASTE
operated by Japan will be a big advantage in strengthening
ALMA proposals and in implementing our strategies for further
extended capabilities with new observing instruments. For

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7. 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 and thespecial-purpose computer for gravitational many-body problems,
carrying out research and development of computational
astrophysics, and performing astronomical research withsimulations. The main supercomputer of the present system,
ATERUI (Cray XC30), has the theoretical peak performanceof 1 Pflops, which is the world's fastest supercomputer for
astronomy. The center also continued operation of othercomputers such as GRAPE-DR and GRAPE-9 that arededicated for gravitational many-body problems, in addition to
general-purpose servers. The center continued to prepare forthe supercomputer replacement in 2018. Efforts in visualizing
astronomical data also continue.

2. Open Use(1) Computer Systems
This year marked the fifth year of the upgraded astronomical
simulation system, which includes the open-use supercomputer
Cray XC30. It is installed and under operation at Mizusawa
VLBI Observatory. The users have been making academicallysignificant progress as before.
While XC30 is leased for five years from Cray Japan Inc.,
the center has built the following equipment to aid the openuse computer operations: a series of dedicated computers forgravitational N-body problems, known as GRAPE’s; PC clusters
for small to medium-scale computation; large-scale file servers;a group of servers for processing computational output data;and networking instruments to encompass the overall computer
system. These components are central to numerical simulations
by researchers in Japan and overseas. In particular, the GRAPE
system is promoted for its effective open use. The center
undertook development, improvement, and maintenance for both
hardware and software for the system this year.
Computational resources are allocated to the XC30,
GRAPE’s, and smaller PC clusters in accordance with a formal
review process. The statistics of applications and approvals
for this year are listed below. Our center conducted a survey
this year on the number of peer-reviewed papers published in
English in this fiscal year on studies that involved the project's
open-use computers. It turned out that 128 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.
(Statistics on the Cray XC30)• Operating hours
Annual operating hours: 8535.7
Annual core operating ratio: 94.46 %• Number of Users
Category S: 0 adopted in the first term, 0 in the second term;
total 0Category A: 11 adopted at the beginning of the year, 0 in thesecond term; total 11
Category B+: 10 adopted at the beginning of the year, 1 in thesecond term; total 11
Category B: 100 adopted at the beginning of the year, 19 in thesecond term; total 119
Category MD: 11 adopted at the beginning of the year, 3 in thesecond term; total 14
Category Trial: 54 (at the end of the fiscal year)(Statistics on the GRAPE system)• Number of Users
10 (at the end of the fiscal year)(Statistics on PC cluster)• Operation stats
Total number of submitted PBS jobs: 225,374
Annual core operation ratio by users' PBS jobs: 72%• Number of Users
51 (at the end of the fiscal year)(2) 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.
• Cray XC30 workshop for intermediate users
August 10, 2017, 6 attendees• Hydrodynamics simulation school
February 13-16, 2018, 22 attendees• N-body simulation Winter School
January 24-26, 2018, 11 attendees• CfCA Users Meeting
November 28-29, 2017, 66 attendees

3. PR Activity
In FY 2017, the following press releases were issued fromthe center:• “First Global Simulation Yields New Insights into Ring
System”
April 28, 2017, Shugo Michikoshi and Eiichiro Kokubo• “Electron surfing and drift accelerations in a Weibel-dominatedhigh-Mach-number shock”
September 25, 2017, Yosuke Matsumoto, Tsunehiko Kato, etal.
• “Supersonic gas streams left over from the Big Bang drive
massive black hole formation”
September 29, 2017, Shingo Hirano, et al.
• “Surface Helium Detonation Spells End for White Dwarf”
October 5, 2017, Ji-an Jiang, Masaomi Tanaka, et al.
• “Astronomers Follow Gravitational Waves to Treasure”
October 16, 2017, Masaomi Tanaka, et al.
• “Rare First Moment of Stellar Explosion Captured by Amateur
Astronomer”
February 22, 2018, Masaomi Tanaka, et al.
The center took part in the special open house of Mizusawa
Campus, Iwate Galaxy Festival 2017, held on August 19, 2017.
About 150 visitors attended the ATERUI guided tours andexperienced a close-up observation of the facility. At the Mitaka
open house held on October 14, 2017, CfCA made the computerroom accessible to the public and introduced simulation
astronomy with GRAPE and the PC cluster. In addition to theopen house, CfCA accepted a group of high school students
to tour the computer room in Mitaka Campus. Moreover, at
OPIE'17, CfCA displayed the GRAPE boards, an ATERUI
blade, and posters to introduce research activities and results ofsimulation astronomy performed by the CfCA system. A Twitter
account @CfCA_NAOJ and YouTube channel have been
operated to provide the information on CfCA.

4. 4D2U ProjectIn FY 2017, the 4D2U project continued to develop andprovide movie contents and software. A simulation movie titled“A Journey Through the Milky Way” was released on the 4D2U
website in June 2017. This movie was also published on the
4D2U YouTube channel with a format for VR on smartphones.
In addition, this movie won the Grand Prix for the VR Categoryof the Lumiere Japan Awards 2017 promoted by the Advanced
Imaging Society of Japan, and the Best VR Science Experienceat the Lumiere Awards promoted by the US Headquarters of theAdvanced Imaging Society.
The updated version of the four-dimensional digital universe
viewer, “Mitaka,” was released in July 2017 (ver.1.4.0). Thisversion of Mitaka included new functions, e.g. displaying thefinal mission of Cassini; and adding the 3D model of Gaia andthe Milky Way texture generated by Gaia's data. Moreover,through calculating the reflection and scattering of light on
Saturn’s rings and the surface of the Moon based on physicalmodels, we are able to draw Saturn and the Moon more
realistically. In March, 2018, the new version, ver.1.4.3 with a
new function for displaying constellation outlines was released.

In FY 2017, demonstrations of Mitaka VR were given
during OPIE'17, the Science Centre World Summit 2017, andthe open campus days of Mizusawa and Mitaka. Many people
were able to enjoy Mitaka outside of the 4D2U Dome Theater.
4D2U contents were provided both domestically andinternationally for TV programs, planetarium programs, lecture
presentations, books, and so on.
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(it has now expanded to include eight institutes). CfCA forms
the core of NAOJ’s contribution to JICFuS. In particular,
the institute engages primarily in computer-aided theoreticalresearch into the fundamental physics in elementary particle
physics, nuclear physics, and astrophysics. The scientificgoal of the institute is to promote fundamental research basedon computational science by encouraging interdisciplinary
research between elementary particle physics and astrophysics.
In addition to its ability as a single organization, a major
feature of the institute is the cooperation of each community toprovide considerate and rigorous support to present and future
researchers. Another important mission of the institute is toprovide researchers around Japan with advice regarding efficient
supercomputer use and the development of novel algorithms
for high-performance computing to meet research goals fromthe perspective of computer specialists. In addition, JICFuS
was chosen as the organization responsible for “Research andDevelopment, Application Development of scientific/social
issues that require particular attention by the use of the Post
K-computer” in FY 2014.
In order to implement research plans, Hiroyuki Takahashi
was engaged as a project assistant professor. Since the central
objects of some ultra-luminous X-ray sources (ULXs) have been
revealed to be neutron stars (NSs), Takahashi investigated thegas dynamics around NSs using general relativistic radiation
magnetohydrodynamics simulations. It was found that, if the
NSs are strongly magnetized, the gas accretes onto the vicinityof the magnetic poles, since inflow around the equatorial
plane is prevented by the strong magnetic fields. In addition,
Takahashi performed high-resolution simulations of the outflows
launched from the black-hole accretion disks. As a result, it
was revealed that the outflow fragments into many clumps
via the hydrodynamical instability in the radiation pressuredominated region. Since such clumps are thought to pass acrossthe observation line of sight, they can account for the observed
time variation of the luminosity. The origin of the luminosity

II Status Reports of Research Activities

075

variations of ULXs is thus revealed by the simulations.
Representing CfCA, Professor Kohji Tomisaka and AssistantProfessors Ken Ohsuga of NAOJ participate in bimonthly
JICFuS steering committee meetings to engage in deliberations
on spurring computational science-based developments inastrophysics research through discussions with other committee
members who specialize in nuclear and elementary particle
physics.
(2) HPCI Consortium
As a participant in the government-led High-Performance
Computing Infrastructure (HPCI) project since its planningstage 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" supercomputer and the “Post-K” plan. Note that although
the center is involved with the JICFuS-led HPCI Strategic
Program Field 5 as well as Priority Issue 9 to be tackled using
the Post-K Computer as mentioned in (1), the activity in the
HPCI consortium is basically independent from them. 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, and observe overall trends
in the planning, although we are devoid of voting rights as wellas the obligation to pay membership fees. Continuing from lastyear, a number of conferences and WG’s have been held whereparticipants discuss a next-generation national supercomputing
framework to follow the “K”. The Post-K project has alreadystarted with some budget from the Ministry of Education,
Culture, Sports, Science, and Technology (MEXT). The primary
institutes and groups responsible for its development have been
established. Now the detailed discussions as to how we can fully
exploit the resources of the post-K system have begun in relevant
communities and organizations. This fiscal year the shutdown
schedule of the current K computer was finally announced. Now
the major subject of the community's discussions has moved
into how we should secure computing resources necessary for
the HPCI program until the flagship Post-K machine becomes
available.

6. Staff Transfers• Staff members hired in this FY(Research expert) n/a(Postdoctoral fellow) n/a(Research associate) Shoko Oshigami, Shogo Ishikawa• Staff members who departed in this FY(Assistant professor) Ken Ohsuga(Research expert) Shigeru Wakita(Postdoctoral fellow) Yuta Asahina(Research associate) Shogo Ishikawa, Tetsuo Taki, Yuki Tanaka(Admin. associate) Yuko Kimura

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8. Gravitational Wave Project Office
In August 2017, gravitational waves from the merger ofbinary neutron stars were detected by LIGO and Virgo. With anextensive campaign of follow up observations, a source object
was identified. The theoretically expected electromagnetic
radiation burst, called a Kilonova, was also observed. This
marks the beginning of multi-messenger astronomy, wheremultiple observation channels are analyzed together to better
understand gravitational wave events. The Gravitational Wave
Project Office (GWPO) is putting most of its resources into theconstruction of KAGRA, a large-scale Japanese gravitational
wave detector, so that Japan can make important contributions to
the emerging field of gravitational wave astronomy.

1. Development of KAGRA
KAGRA is a laser interferometric gravitational wave
detector being constructed in an underground site at Kamioka
in Gifu prefecture Japan. Cryogenic mirrors for the reductionof thermal noise as well as the use of a quiet and stable
underground environment are two unique features of KAGRA
compared with other gravitational wave detectors in the world.
KAGRA’s construction is divided into several phases which
gradually upgrade the interferometer to its final configuration.
In March 2016, KAGRA successfully operated a km-scaleinterferometer in an underground site for the first time in theworld, although the configuration was a simple Michelsoninterferometer. In the Fiscal Year 2017, our effort was focusedon the realization of a cryogenic Michelson interferometer.
NAOJ assembled and installed all the necessary components forwhich we are responsible.
The NAOJ GWPO is contributing to the project in several
aspects. The largest responsibility is for the development andinstallation of ultra-high-performance vibration isolation systems
for the interferometer mirrors. Other technical contributions
include the auxiliary optics, mirror characterization facility, andthe design of the optical configuration and the control strategy
for the main interferometer. NAOJ is also contributing to theproject management through the activities of the executive
office, the systems engineering office, the committee forpublication control, the publication relation committee, and thesafety committee.
(1) Vibration Isolation Systems
In KAGRA, vibration isolation systems are necessary toisolate all the interferometer mirrors and some other opticalcomponents from the ground vibrations. We have developed
four different types of vibration isolation systems, having
different complexities, to meet varied isolation requirementsof different components. In this fiscal year, we assembled andinstalled the isolation systems necessary for the test operation of
the cryogenic Michelson interferometer. We have installed twoof the world’s largest isolation systems, each with a total lengthof 13.5 m for the cryogenic mirrors, and four large isolation

systems for room temperature mirrors. The damping controlof those isolation systems was implemented. They performed
mostly as expected during the test operation of the cryogenic
Michelson interferometer. In order to finish the installation of
the remaining five isolation systems, about 10 members from ouroffice are continuing the hard work in Kamioka.
(2) Auxiliary Optics
The Auxiliary Optics (AOS) subsystem is responsible forproviding optical components for stray light control, opticalangular sensors, beam reducing telescopes (BRT’s), beam
monitoring cameras and optical windows. Highlights of theactivities in FY 2017 involve the BRT’s and the large opticalbaffles for stray light control. A prototype of the baffles forblocking wide angle scattering from cryogenic mirrors was
installed in an actual cryostat, and the cooling test was started
as scheduled. At the same time, the BRT was assembled andinstalled at the Y end of KAGRA. A vibration isolation stage
for the BRT was assembled and the test has been started aswell. For these achievements, ATC provided us great support inmechanical/thermal design, assembly work, and modifications.
(3) Mirror Characterization
We completed a system to measure the optical absorptionof mirrors, which is a critical characteristic for the cryogenic
operation of KAGRA. The system was originally capable ofmeasuring samples of up to 2-inch diameter. Now we are able
to make absorption maps of KAGRA-sized (22-cm diameter)
mirrors. We tested the system with a KAGRA sapphire substrate.
We made calibration checks on sapphire bulk absorption using
different measurement methods in collaboration with LMA(Laboratoire des Matériaux Avancés) in Lyon.

2. R&D(1) R&D for upgrades of KAGRA
Alongside the construction of KAGRA, the GWPO
is actively pursuing the research and development of new
upgrades for KAGRA. One of the targeted upgrades is therealization of frequency dependent squeezed states. Thanks
to the TAMA infrastructure (which is a unique facility in theworld), we had the possibility to realize a 300-meter-long highfinesse filter cavity which in the last year has been extensively
characterized, showing results that exceed the expectations.
The frequency-independent squeezed light source is currently
being finalized. Thanks to this experiment, we establishedlong-term collaborations and got many visitors from abroad.
The absorption measurement bench developed to characterize
the KAGRA mirror is also used to study the performanceof crystalline coatings, a possible solution to reduce coating
thermal noise. The optical performance of crystalline coatings
has been measured in collaboration with LMA. We also directly
measured the thermal noise of such coatings, using a setup

II Status Reports of Research Activities077

developed at MIT, and obtained promising results. Thermal
noise investigation is also the objective of another experimentbeing conducted at ATC to directly measure coating thermal
noise at cryogenic temperatures.
(2) DECIGO
Following on from the conceptual design of the B-DECIGO,
which was compiled in the last fiscal year, the discussion on
how to advance the project is ongoing. Some discussions withnew members for expanding the project collaborators were donein the annual DECIGO workshop.

3. Education
During FY 2017 the GWPO included among its members
two graduate students from the University of Tokyo and two
from SOKENDAI. An additional student joined SOKENDAIfrom China from October. During the same period the office
hosted one master student from Institut d’Optique (France), one
master student from Beijing Normal University (China) andone master student from UEC (Japan). All of them worked at
NAOJ for six months. The office also hosted two undergraduate
students as SOKENDAI summer students. The members of theoffice gave lectures at the University of Tokyo on gravitational
waves and at Hosei University on fluid mechanics.

4. Outreach
Gravitational wave research continued to attract public
interest, partly stimulated by the gravitational-wave-relatedNobel Prize. For outreach purposes, we produced an English
version of the leaflet for our office and helped with the
production of a virtual reality video of TAMA300 and a PR
video for NAOJ. Our office members appeared twice in press
conferences, gave 6 public lectures and wrote articles for anewspaper and a popular scientific magazine. We accepted
visits/interviews by NHK, Nikkei Shinbun, ASCII, and the
Toyota Engineering Society. Our office members took care ofmore than 200 visitors to the KAGRA site. In TAMA300, we
had about 700 visitors on the open day and accepted more than
240 visitors on other occasions.

5. International Collaboration and Visitors
The office continued its collaboration with CNRS/APC
in Paris and with BNU in Beijing on the development of afrequency-dependent squeezed vacuum source at TAMA. In
this context a PhD student from University Paris Diderot visited
NAOJ for two months to complete her PhD work on this topic(she is now a project research fellow at NAOJ). Two morescientists and one research engineer from CNRS/APC visited
NAOJ for a total duration of one and a half month. We started
the EU-funded NEWS project and, in this context, we received
a visit from Dr. Helios Vocca. One of our PhD students visited
CNRS/LAPP (France) for 3 months and another spent two weeks
at MIT (USA) to perform measurements on crystalline mirrors.

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On this topic, we published a paper with our collaborators at
CNRS/LMA (France) and CMS (USA). As usual we received
several visitors at TAMA, among which were the Director
General of SKA, the Dean for Research of Princeton University,and the PI of the LISA project.

6. Publications, Presentations, and Workshop
Organization
The members of the office have authored 36 peer-reviewed
publications including the paper reporting the first detectionof gravitational waves from a merger of binary neutron stars.
Moreover, 11 presentations were given by members of the office
at international conferences. In November 2017, members of
our office organized a commissioning workshop at the KAGRA
site, where active researchers from LIGO and Virgo came to join
KAGRA researchers in commissioning work, to share practicaltechniques and knowledge.

7. Acquisition of External Funds
Our office did not receive external funds apart from 4
Kakenhi grants allocated by JSPS.

8. Staff
During FY 2017 the GWPO hired one assistant professor
and one project research fellow from abroad. As of March 31,2018 the GWPO included 1 professor, 1 associate professor, 4assistant professors, 1 specially appointed assistant professor,
1 researcher, and 3 project research fellows. The team also
included 3 engineers, 2 specialists, 4 administrative staff, and 6
graduate students. Considering 3 affiliated researchers, the total
number of members reached a count of 29 members. A position
to hire a new professor was opened.

9. TMT-J Project Office
The TMT Project is a project to build an extremely large
30-meter telescope under the collaboration of five partnercountries: Japan, the United States, Canada, China, and India.
Heading the project for NAOJ is the TMT-J Project Office.
In 2014, an agreement was executed among the participatingorganizations to found the TMT International Observatory forthe purpose of the construction and operation of the observatory,
and the construction was commenced accordingly. Japan is
responsible for the fabrication of the telescope primary mirror,
the design and fabrication of the telescope structure as well as
performing its onsite installation and adjustment, and the design
and production of science instruments.
The telescope is scheduled to be constructed on Maunakea,
Hawai‘i, with the Conservation District Use Permit issued by
the State of Hawai‘i for the TMT construction in September
2017. Scheduled to commence onsite construction in FY
2018, all the partner countries have engaged in their respective
assigned work; Japan has proceeded with the mass productionof the telescope primary mirror segments, the preparation for
the fabrication of the telescope structure, and the design anddevelopment of the science instruments throughout FY 2017.
As of the end of FY 2017, the TMT-J Project Office wascomprised of three Professors, five Associate Professors, a Chief
Research Engineer, a Specially Appointed Associate Professor, an
Assistant Professor, five Specially Appointed Senior Specialists,
a URA employee, a Special Senior Specialist, a ResearchExpert, a Research Supporter, three Specially Appointed
Research Staff members, four Administrative Supporters, anda RCUH employee for full-time positions, of whom the Chief
Research Engineer, a Specially Appointed Senior Specialist, theResearch Supporter, and an Administrative Supporter resigned
at the end of the fiscal year upon reaching the retirement age or
due to expiration of their respective terms of office. In addition,a Professor, four Associate Professors, two Assistant Professors,
and a Research Engineer primarily assigned to the Advanced
Technology Center, the Subaru Telescope, the NAOJ Chile
Observatory, and the RISE Project have concurrent positions in
the TMT-J Project Office and take part in activities that include
the development of TMT science instruments at the Advanced
Technology Center.

1. TMT Project Progress and Status of the
Hawai‘i Construction Site
The construction of TMT is spearheaded by participating
countries and organizations under the TMT International
Observatory established in 2014. The current officiallyparticipating countries and organizations are the National
Institute of Natural Sciences (Japan), the National Astronomical
Observatories of the Chinese Academy of Sciences, theUniversity of California, the California Institute of Technology,
the Department of Science and Technology of India, andthe National Research Council of Canada. The Association

Figure 1: Conceptual image of the completed TMT.

of Universities for Research in Astronomy (AURA, USA),participating as an Associate Member, is currently taking
steps for the U.S. to eventually become an official participant.
The TMT International Observatory, operated according todeliberations and decisions made in quarterly meetings of
the TMT Board of Governors, is overseeing the construction
work performed in each country as well as developing theonsite infrastructure. The board meetings are attended by three
representatives from Japan.
In December 2015, as the protest movement on Maunakea
continued to gain momentum, the Supreme Court of the Stateof Hawai‘i ruled the permit approval process for the use of theland in the Maunakea Conservation District, the site of planned
construction, to be flawed and consequently invalidated thepermit, although full-fledged construction at the summit of
Maunakea was expected to have commenced by April 2015.
In response to this ruling, the Hawai‘i Board of Land andNatural Resources started a review process in February 2016that included a contested case hearing, and a new Conservation
District Use Permit was subsequently approved in September
2017. During this process, the TMT-J Project Office put in its
own effort as well to garner more understanding by holding
dialogues with local stakeholders.
Although the permit for the construction was issued, a groupof opponents initiated a lawsuit against this approval which ispending before the Hawai‘i Supreme Court as of March 2018.
Additionally, another litigation is in progress at the Supreme
Court against the sublease from the University of Hawai‘i, which
manages the summit of Maunakea, for the TMT construction site
approved by the Board of Land and Natural Resources in 2014.
Under the TMT International Observatory’s plan to resume theonsite construction in FY 2018 while monitoring the progressof these lawsuits, all the partner countries have engaged in theirrespective assigned work.

II Status Reports of Research Activities079

In parallel with this process, the TMT International
Observatory conducted procedures and investigation for
construction at a backup construction site at La Palma in
the Canary Islands, Spain, in case construction at Maunakea
becomes impossible.

2. Japan’s progress on Its Work Share –Fabrication of the Telescope Structure and thePrimary Mirror and Promotion of Developmentof the Science Instruments
For the construction of TMT, Japan is responsible for thedesign and fabrication of the main telescope structure and its
control system and the manufacturing of the primary mirror andportions of the science instruments as according to the executed
agreements. Progress made in FY 2017 is provided below.
(1) Fabrication of the primary mirror segments
The TMT primary mirror, comprised of 492 segment
mirrors, requires the fabrication of 574 segment mirrors in allwith the replacements included. The fabrication processes ofmirror segments are: fabrication of the mirror blanks, spherical
grinding of the front and back surfaces, aspherical grinding andpolishing of the front surface, hexagonal cutting, and mountingof the mirror segments onto support assemblies. These processes
are followed by final surface finish completed in the U.S. andcoating with reflective metal performed onsite before the mirror
segments are finally installed on the telescope.
Of these processes, the plan calls for Japan to fabricate
the mirror blanks and to perform spherical grinding on all 574
segment mirrors. In FY 2017, fifty-two mirror blanks were
fabricated, and spherical grinding was performed on sixty
blanks. The running total rose to 214 blanks that have been
spherically ground by the end of FY 2017.
With the share of work for the processes beginning fromaspherical grinding and polishing and ending with mounting of
the mirror segment on a support assembly distributed amongfour countries, the plan calls for Japan to be leading this workfor 175 of the mirror segments. Aspherical polishing was
performed on eleven blanks in FY 2017. In addition, with the
U.S. scheduled to begin their share of the work to make themirror segments aspherical, shipment of spherical mirror blanks
to the U.S. was commenced.

Figure 2: Mirror segment blanks shipped overseas.

080

II Status Reports of Research Activities(2) Design and preparation for the fabrication of the main
telescope structure and its control system
Japan is leading the design and production of the telescope
structure, as well as its control system, which functions as amount for the optics systems such as the primary mirror andthe science instruments, and points them in the direction ofa target astronomical object. With the baseline and detailed
design developed by FY 2016, work on the telescope structure
in FY 2017 mainly constituted the reduction of technicalrisks involving parts with a high degree of difficulty, theestablishment of a concrete process of performance verification,and the determination of the interface in detail, with an aim tocommence the production. As for the reduction of technicalrisks, a seismic isolation mechanism for the structure and anelevation cable wrap were partly prototyped. The vibration
test, which was performed on the prototype of a reduced-size
seismic isolator model with the use of a vibration test system,
confirmed that a nonlinear analysis result of the detailed design
was mostly reproducible. The elevation-axis motion test wasalso carried out on the prototype of a reduced-size cable wrap toquantitatively assess small-scale vibrations that were produced
externally, and confirmed the current design satisfied thetechnical specifications. A series of these efforts allowed the
production process for the seismic isolation mechanism and theelevation cable wrap to be established. Additionally, FY 2017
saw development in determining the detailed requirements of
the interface between the structure and subsystems, such as thescience instruments, in accordance with the progress of eachsubsystem design. This included the reinforcement of the safety
plan by addressing unconfirmed safety issues in the interface,adjustments of other details, and the implementation of theaccompanying processes.
(3) Science instruments
As part of the international collaboration, Japan is leading
the design and fabrication for a portion of two out of the three
first-light science instruments to be commissioned once thetelescope is complete.
One of them is IRIS (Infrared Imaging Spectrograph).
Being in charge of its imager, Japan currently engages inthe development that includes designing and prototyping incooperation with the Advanced Technology Center. Following
the review regarding the opto-mechanical system in the previous
year, an international review was conducted on the electronics
design, software, and other parts in September 2017, and gave
the green light to enter the final design phase.
With the planned primary role in the camera system of
WFOS (Wide-Field Optical Spectrograph), Japan examined anddeveloped the optical parts in FY 2017. At the same time, studies
of possible architectures for WFOS are currently underway
for a significant change; Japan explores one of the potentialarchitectures, a multi-object spectrometer using an image slicer.

3. Evaluation of Scientific Research by TMT
and Public Relations Activities
The TMT Science Forum, which has been held annually
since 2013, was convened in Mysore, India, in November 2017
to discuss science instruments and the background science goals,
including preparation of white papers (see below) for proposal
and selection of second-generation instrumentation.
The TMT Project plans to implement new instruments
every two to three years subsequent to the first-light instruments
which will be commissioned once the telescope is complete
and operational. The Science Advisory Committee, which
will conduct a review for the selection of second-generation
instrumentation, called for white papers proposing scientificgoals and design concepts for new instruments as the firststep of the selection procedure. White papers on multiple
instruments were submitted by the deadline of March 2018, andJapanese scientists played a leading role in some of those white
papers. The review of the second-generation instrumentation isscheduled to be held in FY 2018, looking into the proposals.
In Japan, continued effort has been made to reflect on the
project opinions of the science community communicatedthrough venues such as the TMT-J Science Advisory Committee.
The committee has engaged in activities such as the designchange of WFOS and the support for the call for second
generation instrumentation. Also, with the continuation of thestrategic fundamental research fund for the purpose of basic
technology research for the development and design of second
generation science instruments, support funding for development
was made available and provided to six universities andinstitutions that applied to the public offering for the funding
support.
Information on the TMT Project is provided in the TMT-J
Project Office website and includes updates particularly
regarding the situation at the Maunakea construction site andthe work share progress made by Japan. Additionally, TMT
Newsletters No. 51 through 56 were delivered. Efforts for public
outreach have been made through lectures and exhibitions
in various regions of Japan. A total of sixty-five lectures andclasses on demand were held for the public.
Contributions were also made through the dispatch of an ondemand lecturer for the science/technology education and PR
event “Journey Through the Universe” (March 2018) held in
Hawai‘i where TMT is to be constructed.
TMT also assembles an international team that includes
Japan to study topics such as education and personnel training,
and as part of this activity, an international workshop was held at
the University of California, Santa Cruz in August 2017 cateringto the young researchers and engineers that will lead the next
generation. About forty graduate students and young researchersthat included seven participants from Japan learned about a wide
range of topics that encompassed not only scientific researchand development, but also international cooperation withpeople of different cultural backgrounds and the management
and operation of large scale projects. At the Communicating
Astronomy with the Public Conference 2018, CAP2018,

organized in Fukuoka City in March 2018, the TMT-J Project
Office reported on its public relations and outreach and, as partof the TMT international team, held a workshop to discuss
activities for an international project.
Donations to the TMT Project have been raised continually;
two corporations and 196 individuals provided donations in2017 (from January to December).

Figure 3: International workshop “Preparing TMT Future Science andTechnology Leaders” held at the University of California, Santa Cruz inAugust 2017 for the young researchers and engineers.

II Status Reports of Research Activities081

10. JASMINE Project Office
1. Planning and Development of the JASMINE(Japan Astrometry Satellite Mission for
Infrared Exploration) Project(1) Overview
The JASMINE mission seeks to survey virtually the entire
20° × 10° Galactic Bulge around the center of the Galaxy andto perform infrared (Kw-band: 1.5–2.5 μm) measurements of
the annual parallaxes, proper motions, and celestial coordinatesof the stars at a high precision of 1/100,000 arcsecond (10 μas)
in order to determine with high reliability the distances andtransverse velocities of stars within approximately 10 kpc
of the Earth in the surveyed direction. Nearly 1 million stars
can be measured with a high precision in the Galactic Bulge
with a relative error for annual parallaxes less than 10 %. Thisis necessary for accurate distance determination. By using
observational data to construct a phase space distribution ofgravitational matter, astrometric surveys of the bulge of the
Milky Way promise to make major scientific breakthroughs in
our understanding of the structure of galactic bulges and thecauses of their formation; the history of star formation withinbulges; and the co-evolution of bulges and supermassive
black holes, which is closely related to the aforementioned
phenomena.
Prior to commencement of the JASMINE mid-sized
scientific satellite project, an ultra-small size project and asmall size project were implemented to progressively build
up scientific results and to accumulate the necessary technicalknowledge and expertise. The Nano-JASMINE micro-satellite
project, with a primary mirror aperture of 5 cm is currently
underway. It aims to test part of the technologies to be used
in JASMINE and to produce scientific results based on theastrometric information for bright objects in the vicinity of
the Solar System. Despite its small aperture, the satellite iscapable of observational precision comparable to the Hipparcos
satellite. The combination of observational data from NanoJASMINE and the Hipparcos Catalogue is expected to produce
more precise data on proper motions and annual parallaxes. The
satellite is scheduled for launch in the near future. An additional
plan is underway to launch a small-scale JASMINE satellite(Small-JASMINE), with a primary mirror aperture of about
30 cm, in FY 2024. This satellite will engage in observationsof a limited area around the nuclear bulge and certain specificastronomical objects. This small-sized version has the goal of
obtaining advanced scientific results at an early stage. The midsized JASMINE satellite, with a main aperture of approximately
80 cm, is designed for surveying the entire bulge and istargeted for launch in the 2030’s. Internationally, Japan shares
responsibilities with ESA. With the Gaia Project, ESA performs
visible-light observation of the entire sky at a precision of
10 μas, while Japan engages in infrared observation of the bulge,which is a method suitable for observations in the direction of
the Galactic Center.

082

II Status Reports of Research Activities(2) Major Progress in FY 20171) Organization of the office
The JASMINE Project Office is composed of four full-time
staff members, six staff members with concurrent posts, two
research associates, one technical associate, and three graduate
students. Significant contributions were made by membersof the following organizations: Kyoto University’s Graduate
School of Science; ISAS at JAXA; the University of Tokyo’s
School of Engineering; Tokyo University of Marine Scienceand Technology; the University of Tsukuba; and the Institute of
Statistical Mathematics.
2) Progress of the Nano-JASMINE Project
The project will engage in spaceborne observations using
an ultra-small satellite to accomplish the following objectives:to make Japan’s first foray into space astrometry; to accumulate
the technical experience in onboard data acquisition, and thelike, necessary for the upcoming JASMINE project; to achievescientific results in the study of dynamical structures in thevicinity of the Solar System; and to analyze star formation basedon stellar motions in star formation regions.
The satellite was scheduled to be launched from a Brazilian
launch site operated by Alcantara Cyclone Space using a
Cyclone-4 rocket built by Yuzhnoye, a Ukrainian rocket
developer. The launch has been impossible due to the adverse
influence of international situations. We now have the possibility
that a foreign company for launch services using small vehicles
can launch the Nano-JASMINE satellite. We are now negotiating
for the launch. Assembly of the flight model that will actually belaunched into space was completed in FY 2010. The extra timeyielded by the launch delay has been used for additional testing
to further ensure project success. Maintenance of the satellite
has also been performed. Steady progress was also made in
the development of the algorithms and software required todetermine astrometric information from raw observational dataat the required level of precision. International cooperation withthe data analysis team for the Gaia Project has been conductedsmoothly.
3) Overview of planning and developing the Small-JASMINE
Project
The objective of the small-sized JASMINE project is to usea three-mirror optical system telescope with a primary mirror
aperture of 30 cm to perform infrared astrometric observations(Hw band: 1.1–1.7 μm). A goal is to measure annual parallaxes
at a precision of less than or equal to 20 μas and proper motions,or transverse angular velocities across the celestial sphere, at a
precision of less than or equal to 20 μas/year in the direction ofan area of a few degrees within the Galactic nuclear bulge andin 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

in that unlike the Gaia Project, the same astronomical object
can be observed frequently and observation will be performedin the near-infrared band, in which the effect of absorption by
dust is weak. This project will help to achieve revolutionary
breakthroughs in astronomy and basic physics, including
the formation histories of the Galactic nuclear bulge and thesuperrmassive black hole at the Galactic Center; the gravitational
field in the Galactic Nuclear Bulge, the activity around theGalactic Center and formations of star clusters; the orbital
elements of X-ray binary stars and the identification of thecompact object in an X-ray binary; the physics of fixed stars; starformation; planetary systems; and gravitational lensing. Suchdata will allow for the compilation of a more meaningful catalog
when combined with data from terrestrial observations of theline-of-sight velocities and chemical compositions of stars in thebulge. Conceptual planning and design of the Small-JASMINE
satellite system and detailed planning of the subsystems beganin November 2008 with cooperation from nearly 10 engineersfrom JAXA’s SE Office (the Systems Engineering Office),
ARD (Aerospace R&D Directorate), and ISAS with a focus on
the satellite’s vital elements such as thermal structure, attitudecontrol, and orbit.
Against this background, in-house discussions andmanufacturers’ propositions, which started in 2009, continued
to consider the design of the satellite bus system to ascertain
the target precision in astrometric measurement as a generalobjective. The SWG, led by Masayuki Umemura of the
University of Tsukuba and including volunteers from diverse
fields in Japan, continued to make scientific considerations.
Other activities such as conceptual planning, design, technicaltesting, and international project collaboration have been
continued.
International partnerships to gain further understanding of
the Galactic Bulge have been formed with multiple overseas
groups engaging in terrestrial high-dispersion spectroscopic
observation to determine the line-of-sight velocities andchemical compositions for bulge stars. In particular, Steven
Majewski of the University of Virginia, the principal
investigator (PI) of the US Apache Point Observatory (APO)
Galactic Evolution Experiment (APOGEE) Project, offered ajoint proposal for the APOGEE-2 project as an extension of theoriginal APOGEE project to engage in bulge observations in thesouthern hemisphere because the project is suitable for bulge
observations. The telescope employed will be equipped with ahigh-dispersion spectroscope, identical to that of APOGEE. The
joint proposal has been submitted. An official memorandum of
understanding has been exchanged among the APOGEE-2 team,members of the fourth Sloan Digital Sky Survey (SDSS-IV)
Collaboration, and Small-JASMINE to strengthen international
partnerships and to achieve scientific goals related to the
Galactic Bulge.
As planning has progressed so far, the full mission proposal
was prepared and submitted in January 2016 to the ISAS callfor small-sized scientific satellite mission proposals and the
Small-JASMINE mission is going through the ISAS selection
process. Small-JASMINE has successfully passed the review

held by the space science committee at ISAS in May 2017 andhad an international review at ISAS in December 2017. Theinternational review committee has given us action items for the
next development phase and much useful advice. We have been
making preparations for the next review at ISAS to upgrade thedevelopment phase.

II Status Reports of Research Activities08311. Extra-Solar Planet Detection Project Office (Exoplanet Project Office, EPO)
The Extra-Solar Planet Detection Project Office cooperates
with researchers interested in extra-solar planets at various
universities, centered around NAOJ to promote the developmentof overall technologies and organize related observations withthe goal of observing exoplanets and their formation sites.
We conduct observational instrument development, researchpromotion, mission planning, and R&D to develop common
basic technologies. We also promote international partnerships
related to exoplanets, which are the focus of this project office.
Specifically, research and development have continued centeredaround the following 4 themes:(1) The development/maintenance/operation of high-contrast
observational instruments using the Subaru Telescope
to directly observe exoplanets: HiCIAO, SCExAO, and
CHARIS; and the promotion of the SEEDS survey and postSEEDS projects.
(2) The development of the new IR Doppler instrument IRD andplanning its observations.
(3) The development of the high-contrast instrument TMT/SEIT,and promoting technological review and related international
collaborations for the WFIRST/CGI, and HabEx missions.
(4) Research into star and planet formation and the interstellar
medium through wide field-of-view polarimetric imaging
with the IRSF telescope located in South Africa.
The project office evolved in to a new institute, the“Astrobiology Center” of NINS in December, 2017. There are
37 refereed papers in English and 89 presentations in this year.

1. Development of the Subaru Next Generation
Exoplanet Instruments and Exoplanet
Observational Research(3) SCExAO (Subaru Coronagraphic Extreme Adaptive Optics)
and CHARIS IFUEXPO has been involved in the development of these nextgeneration high-contrast instrumentations being carried out at
Hawai`i and Princeton, respectively (Fig. 2).

2. Exoplanet Instrument Development for
Future Space and Ground-based Telescopes
and International Collaborations(1) WFIRST Coronagraph and HabEx (Habitable Planet Explorer)
These missions aim to directly image and characterize theEarth-like planets and super-Earths for signatures of life. Asa member of the WACO working group (currently WFIRSTWG), a coronagraph performance test at the JPL testbed is being
conducted with collaborators.
(2) SEIT (Second Earth Imager for TMT)The aim of this project is the direct imaging andcharacterization with the SEIT instrument on the Thirty Meter
Telescope (TMT). Both technical and science discussions are
made, including optical demonstration tests.

3. Science Research, Education, and Outreach
The SEEDS project successfully finished in January 2015
without any major troubles. SEEDS has published about 60
papers so far. Post-SEEDS activitiers using the next generation
direct imaging are also promoted.

(1) HiCIAO (High Contrast Instrument for the Subaru Next
Generation Adaptive Optics)
HiCIAO is a coronagraph camera for direct imaging
of exoplanets and circumstellar disks for the 8.2-m Subaru
Telescope, which can simultaneously utilize various imaging
modes to differentiate by polarizations, multi-bands, andangle. The first Subaru Strategic Program SEEDS (Strategic
Explorations of Exoplanets and Disks with Subaru) with morethan 100 participants continued from October 2009 to January
2015 without any serious troubles.
(2) IRD (Infrared Doppler Instrument)
IRD is a high precision (~1 m/s) radial velocity spectrometerworking at near-infrared wavelengths, whose aim is to detect
habitable Earth-like planets around M dwarfs and brown dwarfs(Fig. 1). Science discussions on habitable planets around M
dwarfs are also proceeding.
Figure 1: First light image of IRD obtained on the Subaru Telescope.
Both stellar spectra and laser frequency comb spectra are imaged on thedetector through optical fbers.

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II Status Reports of Research Activities

About ten graduate students are supervised for exoplanetsand related topics. Many public talks, publications, and press
releases are made on exoplanets, disks, and other astronomical
fields.

Figure 2: Point source image at 1.93 micron from an extreme adaptive
optics system SCExAO and infrared integral field spectrometer. The four
point-like structures are artificial point sources made by a deformablemirror for accurate astrometry. From Brandt et al. 2017.

II Status Reports of Research Activities08512. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project Office
1. Project Overview
In FY 2017, operation preparation of the Laser Altimeter(LIDAR) of Hayabusa2 for arrival at the target asteroid was
carried out. At the same time, a test of the thermal strap of the
Ganymede Laser Altimeter (GALA) for the Jupiter Icy Moon
Explorer (JUICE) mission was conducted. Also, the RISE
Project Office proposed a new plan for a future asteroid mission
as a planetary science project within the National Astronomical
Observatory of Japan.
The RISE Project Office (1) arranged and determined thecontents of the initial check-out test and nominal observation,(2) confirmed the analytical procedures of the landing site
selection, (3) prepared for data publishing by revising the typesof open data and drawing up ancillary documents, (4) conductedcrossover simulations for precise determination of the Hayabusa2
spacecraft’s position, and studied the spatial distribution andtemporal variation of the expected laser footprints and crossover
points, and (5) investigated the performance of LIDAR albedo
mapping by using a LIDAR engineering model, and examined
the reflectivity of the meteorite by changing phase angle asa cross-calibration between LIDAR and three other optical
instruments on board.
For GALA, a thermal strap of the detector was tested
under various thermal conditions and its elastic properties were
measured. Furthermore, the detector sensor was tested in onebar atmosphere with different temperatures aiming to advancethe thermal design. A RISE Project Office member presented at
an international science meeting in June 2017 about a radiation
test and its influence on the receiver detector. This work has
been already accepted by a peer-review journal.
For the Martian Moons explorer (MMX), in order toconstrain the moment of inertia and internal density variations of
Phobos, the Office members carefully examined and confirmed
mission requirements and prerequisites of in-situ observations,such as how low an orbit of the spacecraft could be for density
measurements, and how significant images taken near theasteroid are for determining shape models and rotational state.
For a future plan of the RISE Project Office, a RISE review
was carried out at Mizusawa Campus from April 24 to 25. The
review panels carefully examined input packages in advance,then returned a list of possible problems. Following replies
from the RISE Project Office, the Planetary Science Advisory
Committee and the RISE Project Office discussed intensively to
put together a new proposal for asteroid exploration.

2. Educational Activities/Internship
Seven RISE members delivered lectures in turns at theundergraduate school of the University of Aizu for half a year.
Also, one RISE member served as a part-time lecturer at the
University of Tokyo for half a semester for an undergraduate
class and half a semester for a graduate class. The Office086

II Status Reports of Research Activities

accepted one undergraduate student from University alliance of
Tohoku. Furthermore, one student of SOKENDAI was acceptedfor each of the “laboratory rotation class” and “Experimental
radio astronomy class.”

3. Outreach/PRIn FY 2017, the Office members volunteered for Kirari
Oshu Astronomy School of Oshu City for four times as well as
3 times for Fureai Astronomy classes. RISE members attended
both Mizusawa and Ishigakijima Campus open house days. They
not only interacted with the guests, but also provided special
lectures.

4. Joint Research/International Collaborations
From Russia, Ms. Ekaterina Kronrod visited the Office forone month for joint research on thermo-mineralogical modelingof the lunar mantle. In July, the summer school was held for
Chinese, Korean, and Japanese students who are studying
planetary sciences. An Office member attended this summer
school together with 3 graduate students from Japan to promotescience interaction among the three countries.

5. Career Development
A new research expert joined the Office in August. And one
research expert left the RISE Project Office in March because
he was hired as an assistant professor of Institut de Physique duGlobe de Paris.

13. Solar-C Project Office
The SOLAR-C Project Office has engaged in planning thenext solar observation satellite project SOLAR-C, promoting thesounding rocket experiments FOXSI-3 (Focusing Optics X-ray
Imaging Spectrometer) and CLASP (the Chromospheric LAyer
Spectro Polarimeter), and also preparing for participation in thelarge balloon-borne experiment Sunrise-3.

1. SOLAR-C Project
SOLAR-C is a planned project and may become Japan’s
fourth solar observation satellite, after Hinotori, Yohkoh, andHinode. The plan is to realize the launch in the 2020’s. The
project is intended to investigate the solar magnetic plasma
activities that influence space weather and space climate aroundthe Earth. The investigations involve the high-resolution imaging/ spectroscopic observations of the outer solar atmosphere witha seamless temperature coverage that has not been achieved todate. The themes include major problems in solar research: theheating mechanism of the chromosphere/corona, the origin ofsolar explosive events, and the mechanism of the solar magnetic
activity cycle. Since its establishment, the SOLAR-C project
WG has involved many non-Japanese specialists in addition to
Japanese researchers. Provisionally, Japan will be responsible
for the launch vehicle and satellite; and the science instruments
will be developed through the international collaborations with
the U.S. and European space agencies and institutions.

2. Small-sized Projects(1) CLASP Project
The CLASP project is an observational sounding rocket
experiment aiming to detect solar magnetic fields in thechromosphere and transition region through polarization
observation in the ultraviolet wavelengths. Planning and basic
development started in FY 2009. The project involves aninternational research team with participation from Japan, theU.S., and other countries. The spectropolarimeter was preparedin Japan with components provided by the U.S. and France, andan American sounding rocket is used for the flight. The CLASP
project entered the development stage fully in the latter half of
FY 2012 and carried out the first flight experiment in September
2015. The second flight experiment is scheduled for 2019
and will change the observed spectral line from H I Lyα to thechromospheric Mg II line at 280 nm.
(2) Sunrise-3 Project
The Sunrise-3 project is the third balloon-borne experimentin the German Sunrise program. The preparation of the plan
started in FY 2015 for the flight experiment scheduled in 2021.
Under the international collaboration, the Japanese team will
jointly develop a high-resolution spectropolarimeter that isequivalent to the science instrument for a future space mission.
The project will tackle the development demonstration of astate-of-the–art remote-sensing instrument and the challenges tofront-line science studies ahead of the satellite observations.
(3) FOXSI-3 Project
The FOXSI-3 project is the approved third observationalsounding rocket experiment in the US FOXSI program withfocusing hard X-ray telescopes and is planned to be conducted
in 2018. One of the hard X-ray detectors is to be replaced by thehigh-speed CMOS camera that was developed by the Japanese
team for soft X-ray coronal imaging spectroscopy. The soft
X-ray energy spectrum is to be obtained at each CMOS imaging
pixel by photon counting.

3. Major Activity in FY 2017
The SOLAR-C proposal, which was submitted to JAXA in
February 2015, was not selected in the mission definition review
as the candidate for the 1st JAXA Strategic Large-class Satellite
Mission. The SOLAR-C WG has been working to refine themission concept and rebuild the international collaboration
framework aiming at re-submitting the proposal to the next
opportunity for a JAXA Strategic Large-class Satellite Mission.
At the same time, the SOLAR-C WG has been studying thepossibility of realizing a part of the SOLAR-C science inearlier stages by using the opportunity provided by the JAXA
Competitively-chosen Middle-class Satellite Mission. In termsof international collaboration, the science objectives team for the
next generation solar physics mission (NGSPM-SOT), which
was formed at the request of the space agencies JAXA, NASA,and ESA in 2016, has completed its task, i.e., to prioritize thepotential JAXA-led solar physics missions for launch in the
mid-2020’s, and delivered the final report to the three agencies
in July 2017. By taking the provisional schedule of JAXA’s
space missions in the forthcoming 10 years into account, andafter extensive discussions in the solar physics community inJapan, the SOLAR-C WG decided to position the UV-EUV
Spectroscopic Telescope (EUVST), which was regarded as themost important instrument in the 2020’s by the NGSPM-SOT, as
the top priority project, and submitted the mission proposal for
SOLAR-C_EUVST to JAXA’s Competitively-chosen Middleclass Satellite Mission in January 2018.
Since publishing the first science results from the flight
experiment in September 2015, the CLASP project has been
preparing for the second flight experiment, which is scheduled
for 2019. The Japanese CLASP team fabricated new flightcomponents, which are needed to observe a different spectral
window from the first flight, and started the assembly of thetelescope and the spectrograph. The proposal for the gondola
for Sunrise-3 has also been approved by NASA in this fiscal
year, and Sunrise-3 is scheduled to be flown in FY 2021. We
made the optical, mechanical, and thermal designs of theSunrise Chromospheric Infrared spectroPolarimeter (SCIP), anddeveloped mechanisms for the polarization modulator and image

II Status Reports of Research Activities087

scanner. The interfaces with various European components wereclarified. About half of total budget for CLASP-2 and Sunrise-3
was funded by JAXA through the Small-size Solar Observing
Program. The development of a high-speed CMOS camera for
FOXSI-3 was completed successfully and the combination testwith the X-ray mirror provided by the US team was performed.
The FOXSI-3 project is now in the final prepartations for flightin summer of 2018.

4. Others
Although the SOLAR-C Project Office is reimbursed by
NAOJ for its general operation and emergencies, a large part ofthe expenses for supporting the project preparation is funded byother sources including a Grant-in-Aid for Scientific Research,
JAXA’s strategic R&D fund for basic development andexperiments for onboard instruments, and research grants fromthe private sector.

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14. Astronomy Data Center
1. Introduction

4. JVO Project

The Astronomy Data Center (ADC), a central core ofcomputing and archiving for astronomical data, supports
scientists worldwide by providing a variety of data center
services. In addition, ADC is driving forward research anddevelopment programs for future generations of service. Our
activities consist of the DB/DA Project, Network Project, JVO
Project, HSC Data Analysis/Archiving Software Development
Project, and open-use computer system and service.

ALMA WebQL v3 (renamed to FITS WebQL), whichbecame a Web based quick-look service for generic FITS data,
was released. This service will also be used to display the
Nobeyama data. A desktop version of FITS WebQL was also
released. This can be used to display a user's own FITS files in a
web browser. New VO service search interfaces, JVOIndex andJVOExplorer, were released. JVOIndex is a GUI to enable a user
to search a VO service based on the index extracted from the VO
resource metadata. JVOExplorer is a GUI to find a VO service
by tracing the hierarchical structure of the resource identifier.
Preparation for releasing the Nobeyama Legacy data sets of
FUGIN, COMING, and the Star Formation project was carriedout. Those data will be released in June 2018. Collaboration
between JVO and C-SODA of JAXA/ISAS is going on. Total
access count for the JVO services was 5.85 million and the
download size was 1.24 TB in the 2017 fiscal year.

2. DB/DA Project
The DB/DA-project conducts research and development
on astronomical Data Bases and Data Analysis. It also opens
various astronomical data to researchers and educators (http://
dbc.nao.ac.jp/). SMOKA (http://smoka.nao.ac.jp/) is thecore of the DB/DA-project and opens archival data of the
Subaru Telescope, OAO 188-cm Telescope, Kiso 105-cm
Schmidt Telescope (the University of Tokyo), MITSuME 50cm telescopes (Tokyo Institute of Technology), and 150-cm
KANATA Telescope (Hiroshima University). The total amountof opened data is about 20 million frames (154 TB) as of May
2018. SMOKA contributes to many astronomical products. The
total number of refereed papers using SMOKA data is 220 as of
May 2018.

3. Network Project
The Network Project designs and operates NAOJ
information network infrastructure for the Mitaka Headquarters
and branch offices. Noteworthy topics of this fiscal year are as
follows.
(1) NAOJ and the WIDE project are jointly operating theTranspac, the US-JAPAN Academic research and education
network. The Transpac has had 100 Gbps bandwidth of circuits
between Tokyo and Seattle since 2016. In 2017, SINET, JGN,
and the University of Hawai`i submitted applications to use
this circuit. Also, a new high-bandwidth optical circuit has beendeveloped between the University of Hawai`i at Hilo and Subaru
Telescope.
(2) A computer security incident was caused by inappropriate
information management and unsuitable service configuration.
NAOJ CSIRT (Computer Security Incident Response Team)was responsible for responding to and reviewing this incident
and reported that the probability of information leakage wasextremely low. We will consider effective measures to preventa recurrence of the problem; the computer system and operation
standards will be updated.

5. HSC Data Analysis/Archiving Software
Development
This project started in January 2009, to primarily develop
the data analysis pipeline and data archiving software forHyper Suprime-Cam (HSC). Our main efforts focus on theimplementation of the software for effective data analysis/archiving by parallel and distributed processing, for the sake of
precise photometric and astrometric calibrations, by correcting
various effects originated from the camera system. HSC
operation has been stable, generating a large volume (300–400
GB/night) of data.
In the Subaru Strategic Program (SSP) with HSC, started
in March 2014, we performed data analysis of the SSP dataand produced databases storing the processed results. We madethe 6th internal data release to the SSP team collaborators in
September 2017, which covers over 225 sq. degree areas in all
bands, full depth. The total size of image products reached 280
TB, and the catalog database stores about 350 million objects.
We have continued developing various user interface software
for getting images or catalog products using the database throughweb browsers. The first HSC public data release (PDR) service
launched in February 2017 hosts more than 600 registered users
from institutes across 35 countries. Based on the data releases,
40 scientific and technical papers have been published in the
PASJ HSC special issue (2018.1), and more outcomes from the
HSC data will be anticipated. The hardware and software for thedata releases are in a stable operation, even after renewal of thecomputer platform in March 2018. We have been working on
improvements to the pipeline functions to achieve the planned
accuracies for calibrations/measurements of objects. The onsite data analysis system being developed since 2011 has played
an important role for supporting SSP and general observations
including queue-mode observations. The next-generation multi-

II Status Reports of Research Activities089

object spectrograph PFS at Subaru Telescope will start its
commissioning with early-delivered hardware components thisyear. We have been involved in discussions of data formats, anddevelopment of science data archives which are tied to the HSC
products.

6. Open-use Computer System and Service
The rental open-use computer system, “National
Astronomical Observatory of Japan: Data analysis, archive, andservice system”, was replaced and the new system 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”, “Large data archive and service subsystem(MASTARS; SMOKA; HSC science archive; ALMA dataarchive; VERA data archive; NRO data archive and sharedservers; Okayama data archive; and Solar archive)”, “JVO
subsystem”, “Data analysis subsystem in Mizusawa Campus”,“Development subsystem”, and “Open-use terminals andprinters in Mitaka Campus.”
The total storage, memory, and number of CPU coresin the new system are about 17 PB, 22 TB, and 2,200 cores,
respectively. The total storage volume is about 3 times that ofthe previous system (The total memory and the number of CPU
cores are about 1.7 times and 1.1 times those of the previous
system, respectively).
In the course of the Inter-University Research we held andsupported some workshops on using software and systems, too.
The dates and numbers of participants in JFY 2017 were as
follows.
1. 1st Python + Jupyter notebook data analysis school, Jul 13–
14, 2017, 12 users
2. HSC imaging analysis school, Jul 20–21, 2017, 12 users
3. SOKENDAI summer student program (Support), Aug 1–31,
2017, 10 users
4. 2nd Python + Jupyter notebook data analysis school, Aug
24–25, 2017, 12 users
5. Subaru Autumn school 2017 (Co-host), Sep 19–22, 2017, 14
users
6. IDL School for FITS data analysis, Oct 26–27, 2017, 5 users
7. IRAF/PyRAF installation school, Dec 19, 2017, 3 users
8. N-body simulation school, Jan 24–26, 2018, 13 users
9. Solar data analysis workshop, Mar 26–28, 2018, 9 users.
The total number of participants in the schools in JFY 2017
was 90 users.

7. Others
As part of outreach and promotions activities, 129 issues of“ADC News” were published from No. 580 to No. 708 in JFY
2017. The news was distributed by E-mail to users and appearedon the ADC web pages. The number of “ADC News” in JFY
2017 is about 1.5 times the last year because of the replacementof the computer system.

090

II Status Reports of Research Activities15. Advanced Technology Center (ATC)
1. Organization and Summary of Activities in ATC
At the Advanced Technology Center (ATC), we are working
on the development of astronomical observation equipment thatis requested by and to be used in the projects driven forward
by the National Astronomical Observatory of Japan as "priority
area development" and development research contributing
to the future astronomical projects as “advanced technology
development.”
Furthermore, in FY 2017 we have finished setting up a new
R&D framework called “Basic Technology Development,”
which does not belong to either category of “priority area
development” or “Advanced Technology Development.” Those
research and development themes shall be realized or dissolved
within two years starting from 2016. At the same time, theAdvisory Committee for ATC discusses the approach to researchand development issues to be tackled at ATC, in particular, inorder to make clear the direction of selecting the themes for“advanced technology development,” as well as how to approach
them, and to review the activities being done in ATC.
As one of the “high priority areas for development,”
development of ALMA receivers (Bands 4, 8, 10) has been donewith the highest priority. The shipping of all cartridge receivers
was completed in FY 2013 (by March 2014). Since then, while
keeping the central importance of the maintenance of the ALMA
receivers, we have been carrying out ALMA future development
and studies for upgrades to the receivers of the Nobeyama 45-m
Radio Telescope and ASTE telescope.
As another “high priority area for development,”
development of the observational instruments Infrared Imaging
Spectrograph (IRIS) and Wide-Field Optical Spectrometer(WFOS) for the Thirty Meter Telescope (TMT) were promoted.
In addition, as key parts of the gravitational wave telescope
KAGRA under construction in Kamioka Gifu, the anti-vibration
system and auxiliary optical system were successfully developed
mainly in ATC.
For “advanced technology development,” the main themesof research and development are comprised of the developmentof space-borne solar observation telescopes: CLASP-2 andSUNRISE-3; the development of radio astronomical receivers
and the support of such development outside NAOJ; and theupgrade and maintenance of the ultra-broad field of viewprimary focus camera, Hyper-Suprime-Cam, operating at theSubaru Telescope.
In the “basic technology development,” we will focus
on "development of radio cameras" and "infrared detector
development" as the themes of technology development aiming
for the development of basic technologies, both for future
detectors and observation instruments.

2. Workshops and Development Support
Facilities(1) Mechanical Engineering Shop (ME shop)
The Mechanical Engineering (ME) shop engages in acomprehensive manufacturing process to fabricate experimental
and observational instruments, from design to fabrication andverification. Three teams including design, fabrication, andmeasurement teams cooperate to advance projects by leveraging
their expertise.
The design team has mainly been working on mechanicaldesigns for TMT/IRIS and KAGRA. In addition, the team has
started to work for TMT/WFOS, CLASP-2, and SUNRISE-3.
Major contributions to the projects are as follows.
[TMT/IRIS project]-Design work
Cryostat for mirror surface measurement
Opt-Mech design of pupil viewing optics-Testing
Glass to metal bonding tests-Meetings and Reviews
Preliminary design review[TMT/WFOS project]-Design work
Conceptual design of mask exchange mechanism(mechanisms, facilities, cost, etc.)-Meetings and Reviews
WFOS Trade Study Down-Select Review.
[KAGRA project]-Design work
Suspension system for Narrow Angle Baffle-Assembly and verification
Vibration isolation table for Beam Reducing Telescope
Optics mounts for Beam Reducing Telescope
Suspension system for Wide Angle Baffle
Bottom filters for mirror suspensions.
[CLASP-2 project]-Design work
Design verification of magnifier and mirror holders
Slit holder and pinhole array holder-Assembly and verification
Process control of fabrication and black plating of structural
parts
Bonding of flight mirrors and holders[SUNRISE-3 project]-Design work
Detailed design of opt-mechanical parts for spectropolarimeter
Thermal structural analysis and shock response analysis
Integrated opt-mechanical analysis
Design verification of overall structure
The fabrication team has been working on the auxiliary
optical system of KAGRA, and has fabricated five-axis lens

II Status Reports of Research Activities091

positioners for the Beam Reducing Telescopes. In addition, blade
springs that are made from beryllium copper and Maraging
steel for the vibration isolation system and various parts of theauxiliary optical system were delivered.
For TMT/IRIS, mechanical parts for test equipment weremachined in order to be able to supply them upon request fromthe design team.
For airborne instrumentation, we completed fabrication of
the flight models of mirror holders for the M4 and M5 mirrors
equipped on CLASP-2. Flight parts and a test jig for the
SUNRISE-3 and FOXSI-3 projects were delivered.
In collaborative development programs, we have been
fabricating the base plate and height adjusting plate final
models for the Tomo-e Gozen project under development by
the University of Tokyo, Institute of Astronomy. In addition, we
responded to requests to fabricate the improved receiver holder,parts for cooling tests of anti-reflection coatings, and othercomponents for a radio wave camera (MKID)
The ultra-precision section of the fabrication team has
responded to fabrication requests as follows.
-Trial of the profiled horn for ALMA Band 10 including microfabrication of grooves on the narrow area.
-Development of a new type anti-reflection coating using glass
beads for the Si lens array of the radio wave camera MKID.
-Fabrication of the slicing mirror jig for an image slicer.
-Trial of a high resolution grating.
Furthermore, it was found that a malfunction (out-of-step)in the ultra-precision processing machine occurs when repeatinghigh load processes. As a result of verification processing, it was
revealed that depending on the combination of material, tool,and processing condition, there is a region causing malfunction
without machine error due to overload by repetition for multiple
iteration processing.
The measurement team has responded to not justmeasurement requests but also supported fabrication in order toassure the high specifications.
Table 1 shows the number of fabrication and measurement
requests in FY 2017.
(2) Thin Film Processing Unit
Fundamental experiments were continued to design and todevelop the concrete coating processes, taking into account theapplications and expected performance.
Multilayer design software using the multilayer/WKBJ
approximation for inhomogeneous layers is being built.
An interface program for the fabrication system is underdevelopment.
(3) Space Chamber Shop and Space Optics
Acquisition and accumulation of fundamental technologies
for space observations using platforms such as balloons,sounding rockets, and satellites are progressing with involvementin the research and development of ongoing project activities.
In FY 2017, in collaboration with the SOLAR-C Project Officeand the ME shop, we have assisted the development activities

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II Status Reports of Research Activities

Table 1: The requests in FY 2017.
From FY 2016
ATC
TMT/IRIS
KAGRA
ASTE
SOLAR-C,CLASP-2,SUNRISE-3,FOXSI-3
Astrobiology Center
Division of Optical and Infrared Astronomy
Division of Radio Astronomy
Public Relations Center
Solar Science Observatory
Subaru Observatory
External Organizations
IoA, Univ. of Tokyo
Univ. of Tsukuba
JAXA/ISAS
Total
To FY 2018

5
6
3
20
1
13
3
1
1
2
2
5
4
9
1
75
4

of solar observation projects (CLASP-2, SUNRISE-3) thatare situated as Advanced Technology Developments in ATC.
Concerning the CLASP-2 sounding-rocket experiment inwhich observations of the solar chromospheric magnetic fields
are planned at ultraviolet wavelengths, we have supported thedevelopment of flight components for the second flight. Amongthese activities, the facilities of the Space Chamber Shop were
frequently used for the vacuum bakeout of the flight parts andoutgassing measurements before assembly. The developmentof the light source for polarization calibration was completed,including the confirmation of the brightness of the ultraviolet
lamp and the spectral profile of emission lines to be used. In
the SUNRISE-3 project aiming at observing high-resolution
chromospheric magnetic fields from a balloon altitude, afacility of the Space Chamber Shop was used for the outgassing
measurement of test blackened metals after the surface finish
that is to be applied to holders and mounts of optical elements.
(4) Optical Shop
Activity of optical shop in 20171) Management
We are providing some optical measurement systems andtechnical consulting about the measurement system for open-use
users as usual and doing daily inspections in order to keep themeasurement systems in good condition.
2) Repairing and upgrading measurement systems• Replacement of the light source for the FT/IR spectrometer (FT/IR 410)• Replacement of the light source for the autocollimator (Nikon
model 6D)
• Cleaning of the optical system of the UV-VIS-NIR
Spectrophotometer (Solid Spec3700).
• Installation of the small diameter fiberscopes (OLYMPUS
IF2D5-6-E)

3) Open use• The number of annual user: 268
NAOJ: 208 (including 87 from ATC)
External organizations: 60 (including 12 from Institute of
Astronomy, University of Tokyo)• Use of LEGEX910 (large-scale 3-D measurement machine): 9
Number of operating days: 16• Technical consulting for users: 48

Hinode Science team, and SOLAR-C/CLASP-2. Projects
that require high cleanliness in equipment development use
cleanrooms. In the 110 cleanroom of the No.1 building and the
101 large cleanroom of the No.2 building, equipment related
to KAGRA was developed. In addition, the main body of the
CLASP telescope successfully launched in the United States in2015 will return and new equipment will be developed at the
101 large cleanroom of the No.2 building as a new CLASP-2.

(5) Optical and Infrared Detector GroupWe have conducted twice the joint purchasing program of
MESSIA6, a general purpose focal plane array controller for
astronomical instruments, as part of shared use of the Advanced
Technology Center so far. As continuing user support for
MESSIA6, we assisted the development of a CCD camera for
Nishi-Harima Astronomical Observatory and the University of
Hyogo. In this year, we advised on the design of a cryogenic
dewar to install e2v CCD’s.

3. Prioritized Area Developments(6) Facility Management Unit
The Facility Management Unit conducts the managementof ATC facilities including the buildings, and electric facilities;
daily maintenance of the Cold Evaporator (CE); maintenance ofbuilding equipment; oversight of construction; and managementof hazardous material and laboratory equipment.
Regarding the four draft chambers used for cleaning work
etc. in the clean room, we have re-renovated one unit that did
not meet the regulation values. As the circulation cooling water
facility and the water pipeline become polluted due to aging,inspection and cleaning work including the outdoor cooling
tower was carried out to prevent deterioration of water quality.
As a countermeasure against the decrease in positive air pressure
inside the cleanrooms and resulting degradation in the cleanness,
the filter units in the outdoor air-compressor have been replaced.
Also, we investigated the possibility of storing and keeping
combustible gas cylinders in an outdoor chamber in accordancewith the High Pressure Gas Safety Law.
With regard to the newly built No. 3 building (TMT
building), construction of circulating cooling water facilities
has been finished, which enables the use of refrigerators in eachlaboratory. Cold evaporator (CE) piping connections have been
done to distribute nitrogen gas to each laboratory.
There are many projects that use laboratory equipment,
including ATC members, KAGRA, TMT, the Division of Radio
Astronomy/Chile Observatory, HSC, JASMINE, the Divisionof Optical and Infrared Astronomy, Extrasolar Planet Detection
Project Office (now the Astrobiology Center), Subaru Telescope,(1) ALMA receiver maintenance of Band 4, 8, 10
For the ALMA project, the mass-production and shipment toChile of the Band 4, 8, and 10 receiver cartridges, which wereassigned to Japan, were completed in FY 2013. In Chile, mostof the receivers have been installed and operated in the ALMA
antennas, and many scientific results have been published. At
the Advanced Technology Center (ATC), the ALMA receiver
maintenance team has the responsibility of reparing the defective
receiver cartridges. In FY 2017, one Band 4 and two Band 10
receiver cartridges were repaired and delivered to Chile.
Table 2 shows the total number of defective receiver
cartridges broken down into "initial failure" and "aging failure."
And also shown are the number of receiver cartridges repaired
in FY 2017, and the number of receiver cartridges remaining to
be repaired. The remaining repaired Band 4 receiver cartridge isplanned to be stored as a spare receiver cartridge to be install onan antenna. Its shipping was delayed because of the approachingend of the fiscal year. The remaining defective Band 10 receiver
cartridges, which are possibly due to degradation of electricaldevices, are still inside of the antennas and have not returned toJapan yet. The unloading of defective receiver cartridges must
follow the system operation cycle at the ALMA site because
the receiver cartridges are loaded into cryostats installed on theantennas. A defective receiver cartridge is unloaded when thecryostat is uninstalled from an antenna for maintenance of thecryostat. And then, the defective receiver cartridge will return toJapan after unloading, to be investigated in detail to determine
the cause of the failure and then repaired. We have continued
good collaboration with local engineers in Chile for monitor the
status of receiver cartridges, such as periodic health checks, andcarry out maintenance operations by taking measures.
The repairing of defective receiver cartridges caused byinitial failure is almost finished. Although defects caused byaging failure are infrequent at present because of good quality
control during mass-production, this is not enough to predict andjudge the defect frequency caused by aging failure at the current

Table 2: Total number of defective receivers.
Receiver

Total

Breakdown
Initial failure

Aging failure

Repaired in FY 2017

Remained
1

Band 48

4

41Band 8

17

14

3

0

0

Band 10

21

6

15

2

3

II Status Reports of Research Activities093

moment. It is very important to keep the long-term maintenancesystem in ATC to continue to be able to respond promptly.
(2) TMTWe, the IRIS-Japan team at ATC, have been continuing
development of the first generation Thirty Meter Telescope(TMT) instrument IRIS since 2011.
The Preliminary Design Phase is continuing in FY 2017.
We defined and released the design requirement documentof the IRIS imager, for which NAOJ/ATC has been taking
responsibility, and interface control documents between the
IRIS imager and other IRIS subsystem. Also we finishedthe preliminary software and electronics design of the IRIS
imager. The cost of the IRIS imager in the final design phaseand fabrication phase has been estimated and documented. All
these designs and documents were reviewed and accepted at
the review (Preliminary Design Review 2) in September, 2017.
After the PDR-2, we started the final design phase from October
2017.
In parallel, we have conducted the prototype experiment
on bonding strength between optical substrates and metal pads.
Also we measured the high-precision aspheric mirror.
We have been working on a conceptual study of a WFOS
camera system, which is another first generation instrumentof TMT. There are three competitive concepts for the WFOS
camera system, one of which is being developed in NAOJ, i.e.
a high resolution multi-object spectrometer based on an ‘image
slicer’ where object images are sliced into three to achive anarrower effective slit width. We have been also working on theconceptual study of the camera system of the spectrograph. This
continues in FY 2017. In particular, we proposed the conceptual
solution of the system for changing the mask plates, whichis the main part of the system. We also carried out the opticaldesign as well as the tolerance analysis of the image slicer
module in ATC.
(3) KAGRA
We have developed KAGRA's auxiliary optics subsystem(AOS) and vibration isolation subsystem (VIS) with theGravitational-wave project office (GWPO).
About AOS, we have continued the design of the wideangle baffle (WAB)'s suspension and started the cooling test. We
have also done the design of the narrow-angle baffle (NAB)'s
suspension, the assembly and the installation of one of thetransmission monitors (TMS), and the assembly of two TMS's
vibration isolation stages.
The WAB will be located close to KAGRA's main mirror toabsorb stray light from the mirror in wide angle, and thus needs
to be cooled down along with the mirror. The cooling test of the
WAB has started in March 2018 as scheduled, after finishingthe installation into the actual KAGRA cryostat. A TMS will belocated at the end of each 3-km arm optical cavity of KAGRA
to monitor the tilt and shift of the beam line, and make feedback
signals to the control system. We assembled, tested, and shipped
one of the TMS’s, and it has been installed at KAGRA in March2018 as scheduled. In addition, two TMS vibration isolation

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II Status Reports of Research Activities

stages have been assembled at the large clean room in ATC.
KAGRA-VIS is a subsystem to suspend mirrors required
for the KAGRA interferometer to isolate them from seismic
disturbance. The system consists of multi-stage isolation
mechanical filters. Most of the parts of the isolation system havebeen brushed up, assembled, and tested by the ME shop. So the
ME shop is essential for KAGRA. In this fiscal year, we mostly
completed the major VIS works assigned to ATC; we assembled,
tested, and shipped the remaining two mechanical filters,"bottom filters," cooperating with GWPO. After some discussion
about the schedule, the remaining six "standard filters" werebrought to Kamioka, and then GWPO took care of them. In
addition, the remaining one traverser was assembled, tested, andshipped as well.
As shared uses of the ATC facilities, the three-dimensional
measurement system (FARO) was used several times to evaluate
the installation accuracy in the KAGRA tunnel, and the location
accuracy of the ears for the main mirrors at University of
Toyama.

4. Advanced Technology Developments(1) CLASP-2/SUNRISE/SOLAR-C
ATC has assisted the design and assembly of the instrumentsin the development activities of the solar observation projects(CLASP-2, SUNRISE-3) of the SOLAR-C Project Office.
In CLASP-2 aiming at the measurement of chromosphericmagnetic fields in the ultraviolet wavelengths, the design ofthe new optical system and the design confirmation of newly
introduced structures have been carried out for the flight
instrument. In the SUNRISE-3 project aiming at observing
high-resolution chromospheric magnetic fields from a balloon
altitude, ATC has carried out the detailed optical design ofthe spectropolarimeter operating in near-infrared wavelength
ranges and the design of holder and mount structures supporting
the major optical elements in the instrument. The structural
strength under environmental conditions has been confirmed
through a modeling activity of a finite element model of theentire instrument. The degree of thermal deformation of thestructure under the operating temperature range and the degreeof deterioration of optical performance due to the thermal
deformation have also been evaluated in the in-house activity.
(2) Telescope Receiver Developments
1) Telescope Receiver Developments
Based on the technical skills acquired through the ALMA
receiver developments, the “telescope receiver development”
team has provided support and development for telescope
receiver of other projects and institutes. We have responsibility
for the trouble-shooting of the ASTE new receiver that wedeveloped in 2016. Also, technical support for the DESHIMA
receiver (TU Delft) elements such as the support structure
and chopper was done. We maintain good collaboration withother radio telescopes being developed by universities (Nagoya
University, Osaka Prefecture University, Kwansei Gakuin

University). Fabrication of two ALMA Band 8 mixers was done
for the APEX telescope through a manufacturing cooperation
contract with the Max-Planck-Institut für Radioastronomie.
ATC can increase the technology standards of thecommunity by giving feedback using the technologies andknowledge accumulated through development of specificprojects, and promote the technology development of otherprojects, universities, and research institutions. It is also
important to make the best use of the achievements of the
projects.
2) Development of advanced future receivers
In the field of future developments in heterodyne receivers,
we focus on two main activities. Firstly, we are involved ininternational collaboration for the development of the ALMA
receivers in frequency bands not implemented in the array
yet: Band 1 and Band 2. Secondly, we have started receiverdevelopment to support future upgrade plans for ALMA in
three main directions: ultra wideband, terahertz, and multibeam
receivers.
1.ALMA Band 1, 2+ and 2+3 receivers
ATC supported, in close collaboration with Chile
Observatory, the ALMA Band 1 receiver project led by ASIAA
in Taiwan through several technical studies. We also supported
the different initiatives led by North America (Band 2+, 67-95
GHz) and Europe (Band 2+3, 67-116 GHz) to develop a Band 2
receiver for ALMA, with waveguide components and receiver
optics designs and measurements. Both studies successfully
passed their Preliminary Design Review meetings in FY 2017.
With respect to component design, we successfully designed
dielectric lenses, corrugated horns, and OMT’s with wideband
performance and low loss.
2. Ultra-Wideband receiver
In terms of RF bandwidth, we are developing SIS mixers
with the goal of covering the full ALMA Band 7+8 (275-500
GHz). Based on the development of DSB mixers in last fiscal
year, we have demonstrated a 2SB mixer which satisfies ALMA
requirements in the full 275-500 GHz band. We have worked on
the experiment of a sideband separating receiver based on digitaltechnologies in collaboration with University of Chile.
With respect to IF bandwidth, we have analyzed a SISmixer-preamplifier module in detail, which extends IF
bandwidth to 3-18 GHz, and designed a 2nd prototype to allow
wider bandwidth.
3. Terahertz receiver
In FY 2017, we designed, fabricated, and measured
the performance of 1.25-1.57 THz receiver optics based on
corrugated horns. Measurement results are compliant withthe stringent requirements of ALMA, and represent the best
performance ever measured at these high frequencies.
With respect to superconducting mixers, we demonstrated
lower noise and wider bandwidth ALMA Band-10 (787950 GHz) SIS mixers by employing high current density SIS

junctions.
4. Multibeam receiver
We have established the concept for planar integrationof multibeam SIS receivers, which allows us to realize avery compact multibeam frontend with dual polarization anda sideband separation scheme. We have demonstrated thefeasibility with a concept-proof model at 2 mm wavelength,
showing a cross-polarization level lower than -20 dB together
with the noise temperature. We are proceeding toward a fourbeam demonstrating model.
(3) SIS junction development
During the past year our junction technology based on Nb/
AlNx/Nb tri-layers has been further refined and high quality
junctions with current densities jc = 10 – 60 kA/cm2 are now
fabricated on a regular basis. The excellent degree of reliability
in the fabrication process is made possible by having access tohigh-level equipment in the ATC clean room, maintained by ourgroup, for thin film deposition, lithography, and dry etching,among others.
SIS mixers based on our high-jc junction technology arebeing used in various types of low noise receivers, either as partof an upgrade or demonstrating advanced receiver capabilities:
several ALMA Band 8 type cartridges have been delivered to
the APEX telescope (operated by partners from Max-PlanckInstitute Bonn, Germany), we demonstrated ultra wide IF andRF bandwidths and state-of-the-art sensitivity performance inthe 790-950 GHz band.
In parallel with the development of high-Jc junctions, wehave made encouraging progresses in fabricating SIS mixers
on free-standing membranes. This technique is essential to
implement the new concept of planar integration of multibeam
receivers. We have established a dedicated fabrication processbase on SOI (silicon on insulator) wafers. From this process,prototype planar integrated circuit chips have been successfully
fabricated, which were used for RF performance demonstration.
Compared with the SIS mixer chips that we have fabricated, thisplanar circuit is considerably larger in circuit format and more
complicated in fabrication. This brought about new challenges
to our cleanroom and new motivation of future development.
We also setup a new piece of equipment, a plasma-enhanced
chemical vapor deposition (PE-CVD) system (PD-200STLT,
Samco Co.) to improve the junction quality by enhancing thestep-coverage of the insulating layer. The insulator fabricatedwith PE-CVD is also considered to be less lossy at RF, which isessential for superconducting detectors.
(4) HSC
During the fiscal year of 2017, HSC has been intensively
used for 130 nights. Half of the observing times were allocatedto the Subaru Strategic Program (HSC-SSP) and the otherhalf were for general observer programs including UH time,and Gemini/Keck exchange time. Over the year, we had two
mechanical problems in the Filter Exchange Units (FEU’s) andeach time we had to ask Uraguchi-san, who designed the FEU’s,

II Status Reports of Research Activities095

to do the trouble shooting. Minimum impacts on the actual
observations were recorded. However, because HSC has been
operated for more than four years since its first light, we started
to encounter troubles occasionally which had not been expected
originally. Therefore, new maintenance schemes should beworked out in collaboration with the Subaru Telescope staff. In
the meantime, as for the concerned CCD trouble, we observed
no new problems and we keep following the progress. At thedetector lab, we successfully worked out a new clock pattern
to reduce the readout time of a CCD and cut 5 seconds byaccepting a gain loss of 2/3. We applied the clock pattern on theactual HSC camera and will make a test observing run to see if
we have other side effects.

5. Basic Technology Development(1) MKID camera /CMB Instruments
We are developing a wide field of view, broadband, and highsensitivity millimeter / submillimeter wave instrument.
In collaboration with the University of Tsukuba and Saitama
University, we have developed a superconducting MKID camera
for a future Antarctica terahertz telescope. As a pathfinder, the
MKID camera was installed on the Nobeyama 45-m Radio
Telescope.
In collaboration with KEK, ISAS, Kavli IPMU, and Riken,
we are developing LiteBIRD and GroundBIRD which observe
B-mode polarizations of the cosmic microwave backgroundradiation (CMB). The LiteBIRD has been selected as one of thehigher priority projects of the master plan 2017 of the Science
Council of Japan.
In this year, the following research results were obtained.
1) Design of the sub-wavelength structure for the broad-band
antireflection coating of the Si lens of the LiteBIRD LowFrequency Telescope.
2) Larger focal plane detector of lens-coupled MKID (37 pixels→ 109 pixels)
3) Antireflection coating with glass beads on Si lens array4) Optical measurements of the MKID camera for the Nobeyama
45-m Radio Telescope (109 pixels)
5) Optimization of the readout system of the MKID camera(2) Near-IR Imaging Sensor Developments
There were two requirements to fabricate near-infrared
image sensors by a domestic manufacturer, which were low
noise, and small pixel large format. So far, we have almost
achieved them separately. From this year, we will employ anewer CMOS manufacturing process to achieve both low noiseand small pixel large format in the same chip, expecting a
potential to output near-infrared data complementary to optical
CCD sensors. We have designed a small format trial chip with
the newer CMOS process in this year.
(3) Multicolor Millimeter/Submillimeter Continuum Camera
To efficiently estimate the redshift of submillimeter
galaxies, study the internal structure of hot plasma in clustersof galaxies using the Sunyaev-Zel’dovich effect, and constrain

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II Status Reports of Research Activities

physical properties of the dust in star-forming regions and thespectral index of the initial submillimeter afterglow of gamma
ray bursts (GRB’s), we, in collaboration with the Universityof Tokyo, Hokkaido University, the University of California
Berkeley, and McGill University, are developing a multicolor
millimeter/ submillimeter camera. We presented two papers on
a novel method, tested during the FY 2016 commissioning run,to calibrate the input power and detector nonlinearity. For the
coming upgrade, to make the most effective use of the focal
plane, we made a design of the multichroic detector utilizing theon-chip frequency selective filters, based on the electromagnetic
simulation, which will enable the simultaneous triple band
observations.
Furthermore, we are developing an add-on polarimeter,
Apol, and a moderate resolution spectrometer, DESHIMA, in
collaboration with the Chinese University of Hong Kong and
TUDelft, respectively. By taking full advantage of our lessons
learned with our multicolor camera, we performed the end
to end test of DESHIMA on the ASTE telescope. As a result,
we succeeded not only in detecting the first light from anastronomical object as scheduled but also in achieving a bonus
goal of detecting molecular line emission from an external
galaxy.
(4) Development of Terahertz Intensity Interferometry
Terahertz Intensity Interferometry is being developed.
Achievements of this year include realization of an extremely
low leakage SIS junction with 1 pA in collaboration with
the National Institute of Advanced Industrial Science andTechnology (AIST), which can be used for fast terahertz photon
counting. Twin-slot antenna coupled SIS photon detectors
were designed for 500 GHz and fabricated. Simulation studies
on aperture synthesis imaging with intensity interferometry
were formalized and quantitative comparison was madeagainst standard amplitude interferometry. This development is
supported by the JAXA grant for basic R&D for future spacescience missions and the grant-in-aid for challenging exploratory
research programs from JSPS.

6. Open Use Programs, Joint Research andDevelopment
We accepted open use programs of ATC facilities twice ayear including 15 collaboration programs and 30 facility use
programs. Applicant names and program titles are listed in thesection “Open Use Programs etc.” Results of the programs canbe found on the ATC homepage.

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 reportsof discoveries of new astronomical objects; and provides
the ephemeris and other astronomical information directly
related to people’s everyday activities, such as sunrise andsunset times. In FY 2017, the Center has been comprised of 6
offices and 1 unit: the Public Relations Office, the Outreachand Education Office, the Ephemeris Computation Office,the Library Unit, the Publications Office, the IAU Office for
Astronomy Outreach (OAO), and the General Affairs Office.

2. Personnel
In FY 2017, the Public Relations Center was composed of
Director Toshio Fukushima and the following staff members:
2 professors, 2 associate professors, 1 assistant professor (oneholds concurrent posts), 1 research engineer, 1 chief senior
engineer, 1 chief engineer, 1 chief, 6 specially appointed seniorspecialists, 2 research experts, 19 public outreach officials, 1
research supporter, and 2 administrative supporters.
On April 1, 2017, public outreach official Takashi Horiuchi
arrived in the Outreach and Education Office and transferred
to Ishigakijima Astronomical Observatory, Mizusawa VLBI
Observatory on December 1, 2017.
On March 1, 2018, public outreach official Hironori Itoarrived in the Public Relations Office and public outreach
official Ayako Fujimura arrived in the Publications Office.

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 Outreach and
Education Office, the Public Relations Office also conducted
observation campaigns to promote astronomical phenomena ofMonth
April 2017
May 2017
June 2017
July 2017

Access counts
360,945429,503
390,178
417,534

interest to the public, like the meteor showers. To improve theskills of outreach personnel, the officials attended workshops
such as copyright seminars.
(1) Online-Based Information Sharing
The Public Relations Office runs the NAOJ website (http://
www.nao.ac.jp/en/), disseminating information via the internet.
Table 1 shows the access counts for the website.
Along with the completion of open-use at Okayama
Astrophysical Observatory, a special website “Okayama
Astrophysical Observatory: An Overview of the Past, Present,
and Future (Japanese version)” was opened in collaboration
with Okayama Astrophysical Observatory to preserve its
results for future generations.
The office opened Twitter accounts and Facebook accounts
in Japanese and English sequentially from 2010. We havebeen actively disseminating information on social networking
services. Our office disseminates information on the statusof various NAOJ projects such as public visits, regularstargazing parties at Mitaka Campus, and position openings,
both in English and Japanese. As of the end of March 2018,
the number of Japanese version twitter followers exceeds
160,000. Information dissemination via the English version of
Twitter, the interactive NAOJ quizzes on Twitter, as well as
the release of visual images on Instagram have been conducted
continuously this year.
NAOJ e-mail newslet ters No.172–188 were issued,
introducing research results and NAOJ hosted events.
We continued to produce videos explaining research
results, videos explaining astronomical phenomena, and videos
introducing outreach activities. Including English versions,
22 original videos were produced. The videos are uploaded
mainly on YouTube. As of the end of March 2018, these videos
have accumulated a total of 1,383,083 minutes of play time and385,982 views. Continued from last year, our office performed
live stream broadcasting five times of heavenly bodies withthe 50-cm Telescope for Public Outreach. There were about
7,590 viewers in total. We were also invited to do an official
live broadcast for niconico and there were more than 30,000
viewers. In addition, we conducted live internet broadcasts oflectures on the Special Open House Day for Nobeyama Radio
Observatory and Mitaka Open House Day.

Month
Access counts
August 2017806,200
September 2017
490,786
October 2017
630,664
November 2017
418,373
Total: 7,780,629

Month
December 2017
January 2018
February 2018
March 2018

Access counts
1,094,577
1,674,509
653,580
413,780

Table 1: Monthly website access statistics for the Public Relations Office website, NAOJ Public Relations Center (April 2017–March 2018).

II Status Reports of Research Activities

097

Project PR movie “Public Relations Center”

English Version

Project PR movie “Okayama Astrophysical Observatory”

English Version

Project PR movie “Subaru Telescope”

English Version

Project PR movie “NAOJ Chile Observatory”

English Version

Mitaka Campus Public Visits Reach 200,000 Guests!*

Japanese Version

Project PR movie “Solar Science Observatory”
Eclipse - Crossroads in the Sky
National Astronomical Observatory of Japan: Striving to Solve the Mysteries of the Universe
Time-lapse photography of Phoenicid meteor shower (marked)
Project PR movie “Gravitational Wave Project Office”
Project PR movie “Subaru Telescope” 2nd version
Total Lunar Eclipse on January 31
Exploring the Universe with “Subaru”*
Operation Guide for the HSC Viewer*
Message from New Director General of NAOJ, Dr. Saku Tsuneta“Mitaka” Now Delivers More Realistic Universe in More Languages*

Japanese/English Versions
Japanese/English Versions
Japanese caption Version
Japanese/English Versions
Japanese/English Versions
Japanese Version
Japanese/English Versions
Japanese/English Versions
Japanese/English Versions
Japanese/English Versions

Table 2: Summary of Produced Videos.

April 12, 2017
April 28, 2017
May 18, 2017
June 13, 2017
June 14, 2017
August 2, 2017
August 25, 2017
September 28, 2017 (EN)
September 5, 2017 (JP)September 11, 2017 (EN)
August 8, 2017 (JP)September 29, 2017
October 5, 2017
October 31, 2017
November 6, 2017
November 10, 2017
November 17, 2017
November 21, 2017 (EN)
August 3, 2017 (JP)January 12, 2018
January 25, 2018
February 6, 2018
February 14, 2018
February 20, 2018
February 22, 2018
March 13, 2018 (EN)March 5, 2018 (JP)Collisions generate gas in debris disksFirst Global Simulation Yields New Insights into Ring System
First Direct Exploration of Magnetic Fields in the Upper Solar Atmosphere - Ultraviolet spectropolarimetry
opens a new window for solar physics research ALMA Hears Birth Cry of a Massive Baby Star
Nobeyama 45-m Radio Telescope Developed by the National Astronomical Observatory of Japan and
Mitsubishi Electric Recognized as “IEEE Milestone”
Running Out of Gas: Gas Loss Puts Brakes on Stellar Baby Boom
Phoenicid Meteor Shower from Dead Comet Arises again after 58 Years*
First Detection of an Intermediate-Mass Black Hole Candidate in the Milky Way
Photosynthesis under the light conditions different from the Earth: New prediction of a detection wavelengthfor searching phototrophs on exoplanets
Supersonic gas streams left over from the Big Bang drive massive black hole formation
Surface Helium Detonation Spells End for White Dwarf
Minor Merger Kicks Supermassive Black Hole into High Gear
Forest of Molecular Signals in Star Forming Galaxy
Winds blowing off a dying star
Solar Minimum Surprisingly Constant - More than Half a Century of Observation yields New Discovery
Uncovering the Origins of Galaxies' Halos
Black Hole Spin Cranks-up Radio Volume
FUGIN Project: Large-scale Exploration of the Invisible Milky Way - Making the Most Detailed Radio Mapof the Milky Way
HINODE Captures Record Breaking Solar Magnetic Field
Rotating Dusty Gaseous Donut around an Active Supermassive Black HoleNo relation between a supermassive black hole and its host galaxy!? - The co-evolution mystery deepened bya new ALMA observation
Rare first moment of stellar explosion captured by amateur astronomer
Double or Nothing: Astronomers Rethink Quasar Environment
Table 3: Web Releases.

October 17, 2017
February 27, 2018

Astronomers Follow Gravitational Waves to Treasure
Early science results from the Hyper Suprime-Cam Survey
Table 4: Press Conferences.

098

II Status Reports of Research Activities

(2) Research Result PR
There were 25 research result announcements (compared
to 20 in FY 2016 and 27 in FY 2015). For press releases aimed
towards overseas audiences, the Office has continued to use
the delivery services of the American Astronomical Society,
AlphaGalileo, and EurekAlert! from AAAS. We released all
the research releases in both English and Japanese. We madevideos introducing the content indicated with a * mark.
In the perennially popular Astronomy Lectures for Science
Journalists program, the 24th lecture entitled “Approaching the
Mysteries of the Solar Corona from Magnetic Field Observation- Present and Prospects for Solar Research - ” was held on July25, 2017. Nineteen people (8 companies) participated in thelecture.
(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. The
Public Relations Office organized lectures with research
projects. On February 4, 2018, the NAOJ lecture meeting/23rd
ALMA public lecture “ALMA Explores the Cold Universe Revealing the Mysteries of Planets' Birth - ” was held with 265
guests in attendance.
We ordered an outside filmmaker to make a 2nd episode of“NAOJ Topics,” a video introducing NAOJ’s research activities
for the public (Japanese and English versions).
For the purpose of promoting the use of the contents on
the website and improving the work efficiency, we updated the“Terms of Use of the Website of NAOJ.”
We opened the special site “NAOJ VR.” Visitors canexperience a virtual tour of Mitaka Campus.
To publicize NAOJ abroad, we hosted/co-hosted booths
at overseas meetings where the press and museum personnel
gather (World Conference of Science Journalists in San
Francisco October 2017, Science Centre World Summit 2017 in
Tokyo November 2017, and AAAS meeting in Austin February2018).
Upon request from the Graduate University for Advanced
Studies (SOKENDAI), we translated the website of the
Department of Astronomical Science, School of PhysicalSciences, SOKENDAI, into English.
(4) New Astronomical Objects
Four staff members, including one full-time and three parttime, handled reports of new astronomical objects and othercommunications submitted to NAOJ. In this fiscal year, there
was a total of 18 reports including confirmation requests for
new celestial object candidates and other reports. The contents
were: 4 novae/supernovae, 5 variable stars/transient objects, 4comets, 4 luminous objects, 1 other. Among the many examplesof reporting a known asteroid or ghosts as a new object, thereport of an object in March 2018, was communicated via
NAOJ to the IAU Central Bureau for Astronomical Telegrams
and was recognized as an independent discovery of Nova Canis
Majoris 2018.

(5) Citizen Astronomy
From FY 2016, the Public Relations Office has promoted“Citizen Astronomy,” in which the public plays a part inastronomical research activities using observational data
released by NAOJ. Citizen astronomy is one example of“Citizen Science” projects in which researchers / research
institutes and the public collaborate on scientific activities. In
FY 2017, we considered a concrete citizen astronomy programusing the first dataset published in February 2017 from theHyper Suprime-Cam Subaru Strategic Plan (HSC-SSP) done by
the Subaru Telescope and Hyper Suprime-Cam. We developed
the user-friendly website to display the HSC images and opened
it to the public. We developed a program to determine theshapes of colliding galaxies by using the website. In order toverify the functions and browsing capabilities of this program,a workshop was held on January 8, 2018 for educational
officials and astronomy enthusiasts with 26 participants. Under
the initiative of the Public Relations Center, this program isbeing promoted through cooperation with the Subaru Telescopeand Astronomy Data Center.

4. Outreach and Education Office(1) Public Visits
A total of 21,310 people participated in Mitaka Campus
Public Visits (former name was Visitors’ Area) in FY 2017. In
addition, the group tours in 2017 consisted of 111 general tours(4,171 guests), and 30 workplace visits by schools (361 guests),and 5 others such as inspections (108 guests), for a total of 153
tours accommodating 4,640 guests. Therefore, 25,950 guests
visited Mitaka Campus in total. Note that for the integrated
studies, lectures by researchers, question-and-answer sessions,and visits to research facilities also took place. The officedeveloped an audio guide for most of the Visitors’ Area,
including making the scripts for the audio guide and recording
them in Japanese and English.
Regular stargazing parties were held twice a month (theday before the 2nd Saturday and the 4th Saturday) with the 50cm Telescope for Public Outreach. These were held regardlessof cloudy or rainy weather. Advance booking (300 people foreach session; a lottery system from April to September andadvanced reservations until filled system from October toMarch) was introduced in FY 2012 for these events. A totalof 23 sessions were held with 4,772 participants this year. In
addition to this, the telescope was used by 15 groups (794people) for group tours, inspections, etc.; so a total of 5,566
people observed with the 50-cm Telescope for Public Outreach.
The Outreach and Education Office held the regular public
screenings at the 4D2U Dome Theater four times per month (1st,
2nd, 3rd Saturday, the day before the 2nd Saturday). Advanced
reservations were required for these. A total of 45 screenings
were held this year, with 5,097 guests participating. For fiveof the regular public screenings, the office held “Astronomers’
Talks” where researchers talked about the latest researchand these were popular. Group screenings were performedon Wednesdays and Fridays for 69 groups (2,007 people). In

II Status Reports of Research Activities099

addition, 93 group tours (1,384 people) were organized and a
total of 8,488 guests watched the 4D2U stereoscopic movies.
Guided tours corresponding to cultural property events(November 3 and March 21, advanced reservations needed) andthe NAOJ Solar Tower Telescope Special Open Days (November
4, November 5, March 24, and March 25, no reservations
needed) were held with 1,058 attendees.
(2) Telephone Inquiries
The office received inquiries from the media, government
offices, and the general public. The Outreach and Education
Office responded to 5,320 telephone inquiries (Table 5) and 111
letters, 48 of which were official documents.
(3) Educational and Outreach Activities
The “FUREAI (Friendly) Astronomy” project, now in its
8th year, provided lectures to 85 schools which is the highest
number of schools ever. In this fiscal year, a total of 57 lecturers
provided events for 7,801 students. In eight years, 47,149
students in total have attended the lectures in 481 schools from
Hokkaido in the north to Okinawa in the south.
“Summer Nights: Let’s Count Shooting Stars 2017 (August2017)”, “Let’s Gaze at the Geminid Meteor Shower 2017
(December 2017)”, and “Let’s Observe the Total Lunar Eclipse
2018 (January 2018)” were held and we received 1,411 reports,
2,569 reports, and 2,042 reports, respectively.
For three days from July 31 (Mon) to August 2 (Wed),“Astronomy Classes for Kids in Summer” events were held forelementary and junior high school students around the Mitaka
area. Each day had different themes (assembly of telescopes,
three-dimensional star handcrafts, and radio telescopeobservation) with 138 participants in total. Participants
experienced things unique to the observatory, such as beingtaught by astronomers and using the teaching material
produced in collaboration with projects.
The Public Relations Center participated as the secretariat
for the “Mitaka Open House Day”, a special public event heldat Mitaka Campus and organized by the steering committee.
This two-day event was held on October 13 (Friday) andOctober 14 (Saturday) with the theme “The Universe, Hot andCold.” It was co-hosted by the Astrobiology Center, National
Institutes of Natural Sciences; the Institute of Astronomy, theSchool of Science, the University of Tokyo; and the Departmentof Astronomical Science at the School of Physical Sciencesof the Graduate University of Advanced Studies. The event
flourished: 303 guests attended on pre-open day, and 2,966
guests attended on open day, so 3,269 guests attended in total.

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

Solar
Lunar
Ephemeris Ephemeris
134
101
127
90
163
137
157
258

Activities included the viewing of facilities not normally open
to the public, interactive panel displays, mini lectures, quizzes
and games that are popular among children, and a virtual
reality experience. Each Project offered a selection of activities
based on their own expertise which were suitable for a wide
range of age groups.
(4) Community Activities
The “Mitaka Picture Book House in the Astronomical
Observatory Forest” welcomed 38,457 visitors in FY 2017.
The Outreach and Education Office supervised the exhibition“Elements of Things - How We are Made - (July 2017 - June2018).” We also cooperated with an opening ceremony, modern
and traditional Tanabata events, moon viewing event, and otherevents. In addition, through the “Mitaka Picture Book Housein the Astronomical Observatory Forest, Picture Book Original
Drawings Hallway Exhibit Contest” which started from FY
2013, the Outreach and Education Office cooperated in theselection of 6 winning books.
The Outreach and Education Office conducted the 9th“Mitaka Solar System Walk” from September 22 (Fri) to
Sunday, October 22 (Sun) in cooperation with Mitaka City andthe non-profit organization (NPO) Mitaka Network University.
Stamps were placed at 246 shops and facilities around Mitaka
City. Adding 18 limited event stamps, 264 stamps were placed
and this is a record number. Approximately 20,000 guide-maps/
stamp sheets were distributed, of which 3,256 people turned
theirs in for a prize. The number of participants who collected
all the stamps was 380. It was a good chance to tour the Solar
System while promoting commerce, industry, sightseeing andproviding people a way to enjoy Mitaka and rediscover thecity’s charm.
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 and also assisted by providing
teachers and workshops.
The “Information Space of Astronomy and Science” forwhich Mitaka City, Mitaka Network University, and Mitaka
City Planning Board co-operate celebrated the third year
since its opening and 7 exhibitions were held in FY 2017. The
Public Relations Center had proposed 2 of these exhibitions
and helped with 3 lectures. Also, the office offered outreachand monthly astronomical information images through largescale information displays and “Cosmic Reading Bookstore
Corner,” a display of sample books available to read whichchanges themes (once every 2 months), and cooperated on the

Ephemeris

Time

35
49
44
38

7
5
8
5

Solar System Universe
158
176
198
126

120
108
103
110

Astronomy

Other

Total

97
103
89
97

577
677
581
642

1229
1335
1323
1433

Table 5: Telephone inquiries made to the Outreach and Education Office of the NAOJ Public Relations Center (April 2017–March 2018).

100

II Status Reports of Research Activities

“M Marche Project” conducted on the 4th Sunday of every
month. We welcomed 11,062 guests in the 2017 fiscal year
and celebrated 40,000 visitors since the opening. It has been
acknowledged as a location in town where science can be easily
accessed.
(5) Merchandizing BusinessContinued from the last fiscal year, the Office cooperated
with merchants who organized the NAOJ original goods andaided in making them. Especially this year, there was a neweffort that made use of NAOJ’s intellectual property suchas packaged products of teaching materials developed for
Astronomy Classes for Kids in Summer. In addition to vending
machines dispensing capsule toys which are already in place,the office invited the merchants to place a “Jumbo Carddass
Machine,” so that they can sell photo cards. The off ice
contributed to placing the sales location at the Mitaka OpenHouse Day and Special Open House Day for Nobeyama Radio
Observatory. A total of 1,424 items of these goods were sold in
the fiscal year. In order to share information on merchandizing
know-how, we invited the public relations specialists of eachproject to a meeting and exchanged opinions about NAOJ
original goods, which are spreading to all projects.
(6) International Activities
NAOJ and Leiden Universit y (the Netherlands) coorganized “Astronomy Museums, Visitor Centres & Public
Obse r vat or ie s Work shop” at L eide n Un ive r sit y f rom
September 27 to September 29, 2017. This workshop is about
the activities of astronomical museums, visitor centers, etc.,
and was conducted at NAOJ Mitaka Campus for the first timein September 2015. We plan to hold it every two years andthis is the second time that it had been held. About 30 people
participated and there were 25 lectures, workshops, etc.
In cooperation with IAU/OAD (South Africa), Leiden
University and others, we are proposing and discussing about
making the international guidelines on astronomy education
with the IAU executive department and commission C1.
From March 24 to March 28, 2018, NAOJ and Fukuoka
City co-hosted CAP2018 (Communicating Astronomy with
the Public 2018) at the Fukuoka City Science Museum with
446 participants from 53 countries. The CAP2018 main theme
was “Communicating Astronomy in Today’s World: Purpose& Methods.” This edition was the largest CAP Conference
ever. The conference hosted 5 plenary sessions with 24 plenary
talks, 141 parallel sessions, including a planetarium session; 24
workshop sessions with 20 unique workshops, 111 posters, anda special session dedicated to the 100 Year Anniversary of the
IAU.

5. Ephemeris Computation Office
The Ephemeris Computation Office (ECO) estimates
calendrical phenomena such as the apparent positions of theSun, Moon, and planets on the basis of international standards
and publishes the “Calendar and Ephemeris” as part of thecompilation of almanacs, which is one of NAOJ’s raisons d’être.
(1) ECO published the 2018 edition of the Calendar andEphemeris, the 2018 version of the calendrical section of the
Rika Nenpyo (Chronological Scientific Tables), and the 2019
edition of the Reki Yoko (posted in the official gazette on
February 1, 2018). The Calendar and Ephemeris webpage was
updated to match what was published in the Reki Yoko.
(2) As for the website (http://eco.mtk.nao.ac.jp/koyomi/index.
html.en), ECO continuously updated the contents of theEphemeris Wiki and worked on checking the accessibility
sequentially. ECO cooperated with the astronomical phenomena
awareness campaigns again this year. The radiant points of the
Perseid and Geminid meteor showers were published in the
Astronomical Information section of the website. There wereabout 25 million page views for this fiscal year.

Figure 1: Pageview Statistics of ECO Website.

(3) The Japan Association for Calendars and Culture Promotion
hosted Calendar Culture Mini Forum, its 7th General Meeting,and the Calendar Presentation Ceremony.
(4) ECO hosted regular exhibitions in collaboration with
the Library, selecting from NAOJ’s invaluable collectionof historical archives for Japanese and Chinese books. The
theme of the 56th permanent exhibition was “Achievements of
Sekisui Nagakubo.” This exhibit can also be viewed at the Rare
Materials Exhibition of the Library’s website, in Japanese only
(http://library.nao.ac.jp/kichou/open/index.html).

6. Library Unit
The Library Unit collects and sorts scientific journals andbooks in order to make them available for the research and

II Status Reports of Research Activities

101

study of NAOJ researchers and students. In recent years, withthe continuing digitalization of scientific materials, the portionof the materials in electronic format has increased.
For non-NAOJ personnel who wish to use the Mitaka
Librar y materials, the Librar y is open to the public on
weekdays. In FY 2017, 232 non-NAOJ personnel came to use
the Library. Also for researchers and students belonging toother organizations, we loan books or provide photocopies via
the institute’s library. In FY 2017, photocopies or loans were
provided in a total of 93 cases.
Important documents, especially those originating from theEdo Era Tenmonkata (Shogunate Astronomer), are preserved
while taking into account the environment of a specialized
library. Images of some of the important documents areavailable to the public on the Library Unit homepage.
On June 1, 2017, the Unit updated the library information
system. This improved the convenience of the Online Public
Access Catalog (OPAC).
During the Mitaka Open House Day festivities in October,
we opened part of the Mitaka Library to the public as in thepast. We extended the subject themes again as we did in Fiscal
Year 2016. In addition to materials for general and young
readers, we actually allowed visitors to take a look at many
specialized books related to astronomy.
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.

7. 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 29 Fiscal 2016 (Japanese)• Annual Report of the National Astronomical Observatory ofJAPAN Volume 19 Fiscal 2016 (English)• Report of the National Astronomical Observatory of JAPAN
Volume 19 (Japanese)• Publication of the National Astronomical Observatory ofJAPAN Volume 14• NAOJ Pamphlet (Japanese)• NAOJ Pamphlet (English)• NAOJ News, No. 285 – No. 293 (April 2017 – March 2018)• NAOJ Calendar (The 13th in the series)• Radio Astronomy Public Relations Comic “ALMAr’s
Adventure” (#7)
• NAOJ Publicity Poster Series (#7 and #8)
Continuing from the previous year, the Publications
Office strove to strengthen its international publication ability
and digital publication ability. Regarding the production of
an international edition of the Rika Nenpyo (Chronological
Scientific Tables), we finished proofreading and we are in the102

II Status Reports of Research Activities

final editing process. In digitalization efforts, we expanded the
Publications Office’s digital publication website for e-books
and prepared for publication of contents by categorizingthem into “public relations,” “science writing,” “academic,”and “general.” In normal business, the Office produced anddistributed the Annual Report of the NAOJ, Publication of
NAOJ, and the NAOJ pamphlets. In particular, the Officepromoted multilingualization of the pamphlet, produced a
Spanish version in addition to Japanese and English, prepareddata for Chinese and Korean versions, and prepared to publish
five language versions in total.
In the systematic production of special editions withthe goal of developing project outreach support in NAOJ
News, extra copies of each of the special editions (“People
Advancing the TMT Project Vol. 02 Special Edition” April;“People Advancing the TMT Project Vol. 03 Special Edition”
November; “CfCA Special Edition” October; and “Okayama
Astrophysical Observatory Special Edition” March 2018) wereprinted and these aided the outreach efforts of each project.
From now on, to develop and share NAOJ News articles as aresource to be used as outreach content for each project, weplan to promote the production of overall, basic articles throughclose cooperation with researchers and promote internationalmagazine compiling. Other than periodicals, the 2018 calendar“Okayama Astrophysical Observatory” (the 13th since 2005)
was created. The Office provided native check services to the
Public Relations Office; CfCA; the Graduate University for
Advanced Studies; the NAOJ Directorate, and CAP2018 forEnglish language publications, contributing to the expansion
and en hancement of NAOJ’s inter national infor mation
dissemination. In addition, like in other years editing support
was also given to the publication of the “Rika Nenpyo 2018
(Chronological Scientific Tables, Astronomy section).”

8. International Astronomical Union Office for
Astronomy Outreach (IAU/OAO)
Inter national Astronomical Union (IAU) Off ice for
Astronomy Outreach (OAO) is tasked to communicate withand manage National Outreach Contacts (NOC’s, windows foroutreach in each country) as a priority issue. The Office also
started to discuss new selection methods and guidelines for
NOC’s in order to smoothly and continuously develop the NOC
activities in each country.
In FY 2017, the editing and publishing of the CAP journal
returned from the European Southern Observatory (ESO) to
NAOJ for the first time in four years. Journal #23 was issued
in February 2017 and 2,700 copies of the printed edition were
distributed, mainly overseas. The online edition can be freely
browsed at the IAU web page.
For international information provision, the office posted a
total of 460 postings from OAO on IAU social media during FY
2017. The Facebook community grew by 23 % and the Twittercommunity by 22 %. Meanwhile, the IAU Astronomy Outreach
Newsletter (e-mail news) was delivered 24 times and 300 items
of information were provided to 4,600 subscribers all over theworld. The newsletter has been translated and redistributed
into four different languages by collaborators in the respective
countries. The Office is also responsible for making the website
contents (Themes) of the IAU website for the Public.
We are promoting the Astronomy Translation Network(translation work by volunteer network) as an NAOJ proposal
project for OAO activities. There are 144 registered volunteers
and five working groups (Indonesian, Portuguese, Chinese,
Spanish, and French) have started work for each language.
For the international conference CAP2018 in Fukuoka, theOAO Coordinator participated in the operation as one of the
Co-Chairs of the Science Organizing Committee, and the OAO
Sub-Coordinator was in charge of public relations and making
the proceedings as the Vice-Chair of the Local Organizing
Committee. For the details of the conference, please refer to thesection of the Outreach and Education Office, which hosted theconference.
In addition, OAO participated in the “Strategic Plan
2020–2030,” IAU’s plan for the next ten years, during FY 2017.
In cooperation with the IAU 100 Secretariat established at the
IAU secretariat and Leiden University, OAO is preparing theIAU 100 project as one of the implementing organizations of
the IAU 100 anniversary project in 2019.
In cooperation with the Outreach and Education Office,
NARIT (Thailand), and IAU/OAD, we held the “You are
Galileo!” workshop at the University of Mandalay (Myanmar)on November 29–30, 2017.

II Status Reports of Research Activities10317. Division of Optical and Infrared Astronomy

104

1. Overview

2. Observational Research

The primary objectives of divisions in NAOJ are facilitating
and invigorating projects and individual research throughpersonnel exchanges to place researchers in environments moresuitable for their individual projects. While pursuing challenging
exploratory research on observation and development, theDivision furthers these goals by launching new projects asnecessary. The Division also actively engages in graduate
education efforts to foster next-generation talent. These activities
are based on the concept that the Division of Optical andInfrared Astronomy is a center for personnel exchange between
Subaru Telescope, which engages in open use, and universities
and research institutes in Japan, which focus on developmental
research into new instruments and observational research. This
fundamental principle has been developed since the Subaru
Telescope was constructed.
The Division of Optical and Infrared Astronomy oversees
OAO (Okayama Astrophysical Observatory) and Subaru
Telescope (C Projects); the TMT-Japan (TMT-J) Project
Office and the Gravitational Wave Project Office (B Projects);
and the JASMINE Project Office and the Extrasolar Planet
Detection Project Office (A Projects). The Extrasolar Planet
Detection Project Office migrated to the Astrobiology Centerof the National Institutes of Natural Sciences on December
31, 2017. This transition extends its vision to explore "life in
the Universe" and uncover its mysteries. Most of its members
concurrently held positions of the Division. The Division and
the Projects carry equal weight in organizational terms. Almost
all NAOJ members in optical- and infrared-related fields havepositions in the Division with either the Division or one of the A,
B, or C Projects as the primary appointment. At times, they may
also have concurrent positions in other projects. The primarystaff of the Division of Optical and Infrared Astronomy in FY
2017 consisted of one professor, five assistant professors, four
research affiliates, and three JSPS postdoctoral fellows.
The Division coordinates educational, research, andadministrative activities for Subaru Telescope Mitaka Office andthe Extrasolar Planet Detection Project Office. Since personnel
transfer often occurs within the Division of Optical and Infrared
Astronomy, the Division plays an increasingly important role incoordinating between Subaru Telescope and the TMT-J Project
Office. The Division as a whole maintains and operates facilities
which are auxiliary to research, such as mailing lists and web
servers for Division of Optical and Infrared Astronomy-related
projects such as Subaru Telescope, TMT-J, the Extrasolar Planet
Detection Project Office, Gravitational Wave Project Office, andJASMINE Project Office. The remainder of this report will focus
on the research projects conducted by the primary staff of theDivision of Optical and Infrared Astronomy and the activities ofprojects that support open use.

(1) Observational Research Using Various Types of Telescopes

II Status Reports of Research Activities

Observational research utilizing the Subaru Telescopefocuses on a wide variety of fields such as cosmology; galaxy
formation and evolution; the formation of stars and planets; thestructure and evolution of the Milky Way; stellar spectroscopy;
Solar System bodies; and the search for exo-planets.
Optical and Infrared Synergetic Telescopes for Education
and Research (OISTER) is a NAOJ-lead initiative to form a
network of small aperture size, 0.5 meter to 2.0 meter, telescopes
owned by universities around Japan and overseas to promote
Time Domain Astronomy research and graduate level astronomy
education. FY 2017 marked the achievement of one of the mostimportant objectives, successful observations of a gravitational
wave source (GW170817). A result of Time Domain Astronomy
research by OISTER was presented in a “You are Galileo!”workshop.
With great help from both Subaru Infrared Camera andSpectrograph (IRCS) and the second-generation adaptive optics(AO188) high angular resolution observations for star-forming
galaxies at z~2.5 were realized in order to investigate theirinternal structures. By combining adaptive optics (AO188) andnarrow-band filters, spatially resolved maps of star-forming
regions within galaxies were obtained. Observation of extended
ionized gas in a cluster of galaxies with the Subaru Telescope
was also conducted.
Utilizing the Sloan Digital Sky Survey (SDSS) catalogue,
four scientific reports were published. Two of them focused on
low-ionization broad absorption line quasars. The third shows
evidence for higher black hole spin in radio-loud quasars. This
result was made into an NAOJ press release with the help of
NAOJ’s Public Relations Office. The fourth report focused on
the quenching of super massive black hole (SMBH) growth.
This shows the first observational evidence that the number
fraction of radio-loud quasars increases with the mass of the
SMBH’s above a critical BH mass of 2 × 109 M.
The dust torus cooling timescale once the active galactic
nucleus (AGN) is quenched was estimated. The dust torus
emission completely disappears within 100 years for most of the
AGN luminosity range.
Combining data from the Gemini optical and NuSTAR
X-ray observatories, a study on the relevance of the nuclear
geometrical structure of the AGN to the extension of ionizedgas on host galaxy scales was conducted. Based on ALMA
submillimeter/millimeter and Chandra X-ray data, observational
study on an active galactic nucleus (AGN) was conducted,
particularly focusing on the effects of its X-ray radiation on thesurrounding interstellar media.
A study on protoplanetary disks by using both Subaru and
ALMA observations is on-going. An observational proposal to
ALMA was approved. Now the obtained ALMA data are being

analyzed.
(2) International Cooperative Observational Research
The Division also engages in international collaborative
studies with overseas researchers.
Site survey for a future large infrared telescope in thewestern Tibet area was continued in cooperation with the
National Astronomical Observatories and Chinese Academy of
Sciences (NAOC). Based on past meteorological data in China,
clear-sky probabilities in the area were evaluated. This result
was presented in the NAOJ Symposium on Engineering in
Astronomy 2017.
A study on extended ultraviolet regions around galaxies
continues with researchers in the USA.
(3) Research Using Archives
The image data of all Kiso Ultraviolet-Excess Galaxies
were released on the website of Kiso Observatory, Universityof Tokyo. A paper on this work was published. Digitization of
Kiso Schmidt plates continued. As of the end of FY 2017, wehave scanned 2393 plates out of about 7000 plates, together
with some special project plates. These data are archived in the
Astronomical Data Archive Center (ADAC), NAOJ, and will be
opened for public access.
Research on the verification of astronomical phenomena
described in the New Testament is being done jointly with the
National Institutes for the Humanities. Studies of astronomical
phenomena based on other old ephemerides and documents arecontinuing.
A study on the relics of past interaction in the outskirts ofnearby galaxies was conducted.

3. Observational Instrument Development
Studies of coronagraph masks for the Subaru Telescope and
WFIRST were conducted.
The Infrared Doppler Instrument (IRD) at Subaru Telescope
was developed and engineering runs were conducted with a laser
frequency comb system as a spectrograph drift calibrator.
One of the topics of interest is the search for the undiscovered“axion,” a dark matter candidate. An axion will interact witha magnetic field and create a photon. To investigate thisphenomenon both laser interferometric techniques and longsuperconducting magnets are powerful tools. A joint NAOJ and
KEK group has started to discuss this experiment.
The analysis of ghosts in Hyper Suprime-Cam continued.
For the Hosei Twin Astronomical Telescopes (HOTATE), we
supported observations, improvement, and the construction of
the data archive.

4. Operational Support for Subaru Telescope
The Division of Optical and Infrared Astronomy offers
support for the open use of the Subaru Telescope. This includes

organizing open calls for open-use programs, program selection,
administration, management of open-use-related travel expenses,
and promoting PR activities for Subaru Telescope. The Divisionalso provides support for various research conferences held at
Mitaka Campus.

5. Research Environment Maintenance
A web server has been maintained for research activity PR.
In this year both the web server and the mailing-list server were
replaced with new hardware. And also the web contents wererestructured to improve robustness.
The Division manages the printers and rented multi-function
photocopiers; sub-networks; and data backup servers for Subaru
Telescope Mitaka Office as part of its efforts to maintain the
research environment, and also gives assistance for setting-up
computers for new administrative supporters.

6. PR, Outreach, and Discoveries of New
Astronomical Objects
The Division cooperates with the Public Relations Center insupporting matters related to discoveries of new astronomical
objects and PR/outreach activities such as web releases andpress conferences related to Subaru Telescope research results.
The Division actively participates in a special public event
held at Mitaka Campus (Mitaka Open House Day).
To introduce the activities of the Division of Optical andInfrared Astronomy, we contributed to the Symposium of theInter-University Research Institute Corporations in 2017.

7. Contributions to International Committees
and Events
As a cooperative program between EACOA (East AsianCore Observatory Association) and SEAAN (South-East Asian
Astronomy Network), the “You are Galileo!” workshop washeld at Mandalay University, Myanmar on November 29 & 30,
2017.
NAOJ, with Hyogo University, conducts a joint programwith the National Astronomical Observatory of Vietnam, Nha
Trang to strengthen our research and education capabilities.

8. Hosting Scientific Conferences and Meetings
Department members contributed as SOC and LOC cochairs to the East Asian Young Astronomers Meeting (EAYAM)
2017 in Ishigaki Island.
The 8th OISTER workshop was held at NAOJ Mitaka
Campus on December 14 & 15, 2018.

9. Visitors
The OISTER program conducted short-term visiting
observation training courses for 14 graduate students. In March
2018, researchers from Hyogo University and NAOJ visited Nha

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Trang and one researcher from Vietnam came to Japan for theobservation programs. Prof. Xue-bing Wu in the Kavli Institutefor Astronomy and Astrophysics at Peking University visited
NAOJ. Prof. Jin Koda of Stony Brook University also visited.

10. Educational Activities
The Division of Optical and Infrared Astronomy provides
postgraduate education to 20 graduate students from the
Graduate University of Advanced Studies, the University ofTokyo, Tokyo University of Agriculture, and Japan Women’s
University.
Division staff members made active contributions toseminars and self-directed studies. Since April 2015 we haveheld a 30-minute seminar in the afternoon every day throughout
the year. In December, we held the annual workshop of theDivision of Optical and Infrared Astronomy so that staff
members and graduate students can understand the current
studies and interests of each other.

106

II Status Reports of Research Activities18. Division of Radio Astronomy
The Division of Radio Astronomy oversees Nobeyama
Radio Observatory, Mizusawa VLBI Observatory, the RISE
Lunar Exploration Project, and NAOJ Chile Observatory
operating the Atacama Large Millimeter/submillimeter Array(ALMA) and Atacama Submillimeter Telescope Experiment(ASTE). The scientists and engineers of these projects areattached to the Division of Radio Astronomy to conduct radio
astronomy research under mutual cooperation among theseradio astronomy projects. The research themes of the Divisionof Radio Astronomy are represented by keywords such as Big
Bang, early Universe, galaxy formation, black holes, galactic
dynamics, star formation, planetary system formation, planetsand satellites, the Moon, the evolution of interstellar matter, andthe origin of life in the context of the evolution of the Universe.
Radio astronomy unravels mysteries and phenomena in the
Universe through radio waves, which are invisible to humaneyes. The detailed research results are reported in each project’s
section and in the research highlights. The Radio Astronomy
Frequency Subcommittee has been established within thedivision, engaging in discussions on protection against artificial
interference generated by electrical equipment, which causes
major obstacles in radio astronomical observations.

1. Radio Astronomy Frequency Subcommittee
The mission of the Radio Astronomy Frequency
Subcommittee is to protect the environment for radio astronomy
observations. In 1932, Karl Jansky of the U.S.A. first discovered
radio waves emitted by astronomical objects, albeit accidentally.
Since then, dramatic advances have been made in radio
observation methods, showing us new perspectives of the
Universe invisible at the optical spectrum. Four Novel Prizes
have been awarded to achievements made in the field of radio
astronomy so far.
Just as light pollution from artificial light sources is an
obstacle in optical observation, artificial radio interference
generated by the electronic devices surrounding us is a major
obstacle in radio observations. As breathtaking advancement
has been achieved in wireless communication technologies
in recent years, wireless commercial products such as mobile
phones, wireless LAN’s, and automotive radars are widelyused. The areas of radio applications will continue to expandin the future owing to their ubiquitous nature. But becauseof its unique capabilities, compatibility among various radio
services, including both active and passive ones, will become aserious issue. Frequency is a finite resource and its sharing is anunavoidable issue. Therefore, further efforts will be necessary
for maintaining the sky free from artificial interference for betterradio astronomy observations.
(1) Role and Organization
The purpose of the Radio Astronomy Frequency Subcommittee is to ensure that radio astronomical observations arefree from artificial interference and to raise public awarenessof the importance of protection activities. Radio astronomical
observation does not emit radio waves; thus, it does notinterfere with other wireless communications. A proactive
approach is needed to widely raise awareness of the efforts
to protect the environment for radio observations. Regularexplanatory sessions are provided at the Ministry of Internal
Affairs and Communications (MIC) and regional Bureaus of
Telecommunications to solicit appreciation of the importance ofprotecting the field.
The coordination between the community of radio astronomy
and commercial wireless operators is led by the MIC in Japanand internationally by the International Telecommunication
Union (ITU) Radiocommunication Sector (ITU-R) of the United
Nations. As part of the activities for FY 2017 the Subcommittee
took an active role in formulating the opinion of the Japaneseradio astronomical community (on behalf of the Japanese radio
astronomers) in these coordination efforts.
The Subcommittee is composed of members from NAOJ
and representatives of universities and research institutes inJapan.
(2) Current Challenges
A sharing study between active radio services and radio
astronomy is crucial for compatibility under the conditionof limited availability of frequency resources. Some rules
and regulations have been established to address the issue ofinterference cooperatively. The Radio Astronomy Frequency
Subcommittee remains responsible for taking measures for
new developments in wireless services including the following
challenges.
• Significant increase in wireless activities in response to natural
disasters:
After the Great East Japan Earthquake in 2011, risk of radio
interference has been increased by new wireless communication
services prepared for natural disasters.
• Development of new radio applications:
There has been a rapid increase in demand for higher
frequencies. 76 GHz automobile radars become common.
Wide band radars up to 81 GHz may become more popular as
they may reduce car accidents resulting in injury or death. It is
anticipated that industrial structures will dramatically changewith the advent of the fifth generation mobile phone technology
allowing high-speed, multiple concurrent connections, and ultralow latency, which will be installed into various mobile phones.
Some satellite operators launched new plans for improving
broad-band communication to ships and planes globally.
• Reassigning of vacant frequency bands resulting fromenhanced efficiency in radio use:
The digitization of television broadcasting has created vacant
frequency bands, which have been reassigned for mobile phones
and other applications.

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107

The effect of interference arising from such radio
applications (e.g. wireless business) varies widely depending on
the frequency band used. Radio astronomy observations havebeen given priority in a number of frequency bands within therange between 13.36 MHz and 275 GHz under the ITU Radio
Regulations (RR). However, negotiations will be necessary
between some radio services and radio astronomy if the samepriority level is to be shared within a certain band or underadjacent/proximity conditions. Even faint signals of negligible
significance to general radio services, can have a chance of
substantial adverse effects on radio astronomy observations.
Sources of interference that need to be addressed continue
to increase and include the following devices and systems:
the 23 GHz CATV wireless transmission system used inemergencies, where ammonia observations are affected; 21
GHz next-generation satellite broadcasting, where water maser
observations are affected; 1.6 GHz mobile satellite phones for
emergencies, where the observation of pulsars and the likeare affected; the fifth generation mobile phones, where siliconmonoxide (SiO) maser observations are affected by the 43.5
GHz band (one of the candidate frequency bands); and Ka-band
broad-band communication from airliners to satellites, wherewater maser observations are affected. 79 GHz automotive
radars around Nobeyama Radio Observatory have considerable
impact on the observing conditions. Although radio astronomy
observations in the 60 GHz band are not common because of thehigh rate of absorption in the atmosphere, the 60 GHz system
must be watched closely because its second harmonic can haveadverse effects on CO observations in the 115 GHz band.
(3) International Activities
The ITU Radio Regulations (RR), which allocate radio
frequencies to wireless applications, are revised once every three
to four years in the World Radiocommunication Conference(WRC). The RR includes frequency bands in which radio
astronomy observation is prioritized. Among these meetings,
the Radio Astronomy Frequency Subcommittee is regularly
involved in the WP7D (radio astronomy) and WP1A (frequency
management) meetings. The Subcommittee also takes part invarious international conferences, representing the Japanesecommunity of radio astronomy researchers.
In FY 2017, the Subcommittee participated in the ITU-R
WP7D meetings held in April and October in Geneva. In
these meetings, the following items were discussed as major
agenda items related to radio astronomy: modernization of
Global Maritime Distress Safety Systems (GMDSS) utilizing
1.6 GHz satellite communication; upgrades of the maritime
radio communication system utilizing the 160 MHz maritime
mobile-satellites, establishment of a correspondence group forcompatibility studies to ensure compatibility between vehicle
radars and radio astronomy, identification of frequency bandcandidates for the new International Mobile Telecommunications(IMT2020), and so on. The WRC-19, which is scheduled for
2019, aims to identify frequency bands for IMT2020 from 11
candidate frequency bands ranging from 24 GHz to 86 GHz andto allocate active services to frequencies above 275 GHz.

108

II Status Reports of Research Activities(4) Activities in JapanThe three major domestic activities of the Radio Astronomy
Frequency Subcommittee include: participation in various
committees and working groups hosted by the MIC, direct
negotiations with wireless operators regulated by the MIC, andinformative activities to raise public awareness about radio
interference to radio astronomical observations. Negotiations
with wireless operators to reduce interference sources represent
a major part of the Subcommittee’s activities in Japan.
The committees and working groups hosted by the MIC are
to formulate Japan’s strategies on various wireless issues forinternational conferences. Other MIC-related meetings provide
opportunities for discussing the radio application technologies
related to MIC’s wireless policy, and for negotiating on
interference issues with wireless operators authorized by MIC.
Negotiations directly affecting the protection of radio astronomy
observations have been conducted concurrently to dealing with
the interference problems related to societal and technologicaltrends.
Several examples of the interference problems discussed in
section (2) above are given below.
In November 2015, WRC-15 resolved to allocate 77.5–78
GHz to the radiolocation service, allowing automotive vehicles
to utilize the whole 76–81 GHz band for their radar, which may
invite large scale commercial use of high-resolution automobile
radars in the 76 GHz and 79 GHz bands. Of particular concern
are the possible effects of interference from these radars on
the 45-m radio telescope at Nobeyama Radio Observatory,
which engages in observations of spectral-lines of deuterated
compounds and other molecules in interstellar matter. The
observations with the Nobeyama 45-m Radio Telescope
located in Japan will continue to carry significance in relation
to the international project ALMA, which deploys 66 highperformance radio telescopes at an altitude of 5,000 m in Chile.
Since automotive radars are highly relevant to human life safety,
negotiations have been conducted with careful analysis in orderto reach a mutually acceptable agreement.
A new radio wave application is being planned for 21 GHz
next-generation satellite broadcasting with a picture resolution
16-fold higher than that of the current HDTV. This band is nearthe 22 GHz radio astronomy band, which is important for watermaser observation. The radio signals from the satellite comefrom outer space. Their detrimental effects need to be alleviatedwith a filter at the output stage of the satellite. The NHK Science& Technology Research Laboratories developed a bandpass
filter to suppress spurious signals to an acceptable level. The
measurement results of radio emissions from the satellite
launched in December 2017 verified that the filter has a proper
protective effect against radio interference.
Radio observations in the 60 GHz band are not common
because of the high atmospheric absorption rate in thatfrequency range. Albeit in fact, the 60 GHz system must be
watched closely in terms of its proliferation in the market, sinceinterference from it may affect CO observations in the 115 GHz
band, which is within the band of the second harmonics of the
60 GHz radio system.

In response to the update plan of the satellite systems
announced by Iridium LLC (U.S.A.), the committee started
discussions aiming to reduce radio interference risks caused byunwanted emissions from the 1.6 GHz signal to the astronomy
band (OH maser observations). Discussions are being held on
what interference risks are involved and what measures should
be taken to alleviate radio interference.
The World Radiocommunication Conference (WRC) will
determine the frequency band for the next-generation mobile
phones in 2019. The MIC organized a joint working groupwith some radio services and organizations including the Radio
Astronomy Frequency Subcommittee. The Subcommittee played
an active role in preparing a joint study report regarding the 11
candidate frequency bands given in the WRC-19 Agenda Items.
Additionally, radio astronomy observations could be
adversely affected by some of the new wireless technologies:
wireless power transmission (WPT) for electric vehicle
energy charging (non-beam), next generation railway radio
communication systems between bullet trains and trackside, andso on. The Subcommittee continues to monitor their progressand shares the information with related radio astronomers.
Moreover, the Subcommittee has been engaged in making
applications to the MIC to request frequency protection for
the NAOJ telescopes as well as other telescopes owned by theJapanese community of radio astronomers on their behalf.
Collecting actual interference cases at various observatories
is also important. To raise public awareness about “Interference
to Radio Astronomy,” these collected cases are effectively
used in presentations by our community members. We are also
preparing tutorial materials for the general public. As opticalastronomers are actively working to protect their observation
environment against artificial light, we, radio astronomers, aremaking the same efforts for the sake of continuing observations
in radio astronomy in coming ages.

II Status Reports of Research Activities10919. Division of Solar and Plasma Astrophysics
The Division of Solar and Plasma Astrophysics is mainly
made of staff members from the Solar Science Observatory andthe Solar-C Project Office. It conducts research on the Sun inclose coordination with these projects. An NAOJ fellow andgraduate students supervised by the staff of the above-mentioned
projects also belong to the Division.
The Division conducts both theoretical and observational
research into the inner structure of the Sun and outer solar
atmosphere including the photosphere, chromosphere, corona,and solar wind; and various phenomena in the magnetizedplasma such as flares, sunspots, solar faculae, and prominences.
The Division’s theoretical research includes helioseismology
studies of the internal structure of the Sun, and applicationsof plasma physics and magnetohydrodynamics to various
phenomena on the Sun as well as on Sun-like stars. The solargroup at NAOJ started observations from space in the very earlystages of Japan’s space program. The Division has participatedin the development of the Hinode satellite, which is currently
in orbit, and is playing a major role in its scientific operation.
Research is also being carried out using the Solar Flare
Telescope and other telescopes in Mitaka Campus. In groundbased observations, the Division conducted research to introduce
and utilize new technologies in the Solar Flare Telescope andhas been conducting long-term monitoring observations of solar
activity, and the obtained data are open to the community.

1. Research in Solar Physics
NAOJ fellow S. Toriumi published one paper in a refereed
journal as lead author. This work is about the numerical MHD
modeling of flare-productive active regions, and he revealed theevolution processes by which subsurface magnetic fields create
magnetically energetic active regions above the surface. He also
published three refereed papers as a co-author, including forexample, theoretical investigations of the relationship between
flare durations and magnetic structures, and research related
to 18th Century Japanese sunspot sketches. Toriumi has beenpromoting collaborative research with international partners; heinvited Dr. V. Pipin of the Institute of Solar-Terrestrial Physics,
Russian Academy of Sciences, and conducted collaborative
research on solar-stellar dynamos and starspots.
The Division has a seminar (on Friday afternoon, roughly
twice a month) whose speakers are from both inside and outsideof the Division. The organizer for this year was S. Toriumi.

2. Educational Activities
The teaching staff of the Division supervised three graduate
students from SOKENDAI (the Graduate University for
Advanced Studies) and one from the University of Tokyo.
Among them, Y. Hatta passed the examination for the Master’s
thesis. The Division, in cooperation with Kyoto University andNagoya University, supported the annual “Leading-edge Solar

110

II Status Reports of Research Activities

Research-Experience Tour” in March for undergraduate students;
nine students visited solar-related research organizations andexperienced the latest research in the field.

3. International Cooperation
Y. Katsukawa has been a member of the Science Working
Group of the Daniel K. Inouye Solar Telescope, a 4-m telescope
under construction at Haleakala, Hawai`i. In Europe, another4-m solar telescope is now in the planning stage. NAOJ sent a
Letter of Intent and is watching the progress. Several plans arealso under consideration for future ground-based telescopesthat would involve collaborations with East Asian countries andPeru.

20. Division of Theoretical Astronomy
1. Overview

2. Current Members and Transfers

The Division of Theoretical Astronomy (DTA) aimed atachieving internationally outstanding research results bothin quality and quantity toward the accomplishment of thefollowing four goals that were set by the NAOJ Board, and isengaged in research activities for FY 2017 accordingly:- Advance the world class cutting-edge theoretical research.
- Pursue theoretical astronomy research, particularly inareas that utilize the NAOJ supercomputer or large-scaleobservational instruments to give further insight into their
new development.
- Encourage collaborations among researchers in Japan andstrengthen the domestic theoretical astronomy research.
- Invigorate postgraduate education.
The division handles a wide variety of themes in theoreticalastronomy research, addressing a diversity of hierarchicalstructure of the Universe in terms of formation and evolution
processes, dynamics, and physical state of matter, coveringa span from the early Universe to galaxies, stars, planetaryfor mat ion, act iv it ies of compact object s, a nd pla sma
phenomena in astronomy and astrophysics; joint researchwith observational astronomy using observational facilities
of various frequency bands such as the Subaru, ALMA, andNobeyama radio telescopes; and interdisciplinary research withphysics of elementary particles and atomic nuclei.
The Division of Theoretical Astronomy aims to facilitate
Japan’s high competitiveness on the international plane throughcontinuous production of world leading research results andoffers a superb research environment as a base for theoreticalresearch accessible to researchers in Japan and overseas. It
has accepted a wide range of both Japanese and international
researchers as visiting professors, visiting project research
fellows, and long-term research fellows who actively engage
in various research projects in the division. In particular,
the division has fostered research developments to create an
influential research center for young researchers and is actively
engaged in personnel exchanges with many universities andresearch institutes. In addition, the division actively organizes
numerous cross-disciplinar y inter national conferences,domestic meetings, and seminars for the fields of theoreticalastronomy and astrophysics, observational astronomy, andexperimental physics, and it leads research activities in various
related fields of astronomical science. The division’s fulltime professors, associates, assistants, and project assistantprofessors, together with NAOJ postdoctoral fellows and JSPS
fellows, conduct a variety of unique research projects involving
postgraduate students from the Graduate University of
Advanced Studies, the University of Tokyo, and the Graduate
School of Japan Women’s University.

In FY 2017, the dedicated faculties of the Divisionof Theoretical Astronomy included two professors, two
associate professors, and four assistant professors in addition
to one adjunct professor and one adjunct assistant professor
who concurrently held primary positions at the Center for
Computation Astrophysics. In addition to these research andeducational members, the division was served by four project
assistant professors, including one research associate, two JSPS
fellow, one EACOA fellow, and in addition one administration
associate who gave full support to all activities of the division.
Among them Akimasa Kataoka, an assistant professor, joined
our division from December in 2017, Ken Ohsuga, an assistantprofessor, moved to Tsukuba University as a professor, andMasaomi Tanaka, an assistant professor, moved to Tohoku
University as an associate professor at the end of March in2018.

3. Research Results
The research papers and presentations in the international
conferences carried out by the division member(s) as author(s)or presenter(s) are listed below. Categories with fewer than 5
publications have been omitted.
- Peer-reviewed journal papers in English: 117- Journal papers in English (proceedings of the meetings): 10- Reports in English (talks at international conferences): 50(invited talks: 21)- Reports in Japanese (talks at national meetings, etc.): 34
Some of the research results are presented as the researchhighlights listed at the beginning of this report. The following
highlights include research in which the division members tookleading roles:- General Relativistic Radiation M H D Simulations ofSupercritical Accretion onto a Magnetized Neutron Star:
Modeling of Ultraluminous X-Ray Pulsars (Takahashi, H. &Ohsuga, K.)- Superluminous transients at AGN centers from interaction
between black hole disk winds and broad-line region clouds(Moriya, T., Tanaka, M., Ohsuga, K. et al.)- Big Bang Nucleosynthesis and Modern Cosmology (Kajino, T.
et al.)- Big-Bang Lithium Problem, and Effects of Long-Lived
Negatively Charged Massive Par ticles on Pr imordial
Nucleosynthesis (Kajino, T. et al.)- The new hybrid BBN model with the photon cooling, X
particle, and the primordial magnetic field (Kajino, T. et al.)- Production of Left-handed Amino Acids in Space in the
Supernova Neutrino Amino Acid Processing (SNAAP) Model

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(Kajino, T. et al.)
- Sele c t ion of A m i no Acid Homo ch i r a l it y i n St el la r
Environments (Kajino, T. et al.)- Short-baseline electron antineutrino disappearance study byusing neutrino sources from 13C + 9Be reaction (Kajino, T. et al.)Partnership for Advanced Computing in Europe (PRACE);
international associate for the European Centre for Theoretical
Studies in Nuclear Physics and Related Areas (ECT*); andinternational referee for the Swiss National Science Foundation(SNSF).

The following research results are released on the division’s
website (http://th.nao.ac.jp/) as research highlights:

The Division of Theoretical Astronomy played leadingroles in organizing the following international conferences:- Rare first moment of stellar explosion captured by amateur
astronomer (Tanaka, M., Moriya, T. et al.)- Discovery of a supernova beyond the standard explosion
paradigm (Moriya, T. et al.)- Astronomers Follow Gravitational Waves to Treasure (Tanaka,
M. et al.)- Surface Helium Detonation Spells End for White Dwarf(Tanaka, M. et al.)- The effect of collective neutrino oscillations on vp process
nucleosynthesis (Sasaki, H., Kajino, T. et al.)- Efficiency of Metal Mixing in Dwarf Galaxies (Hirai, Y.,
Kajino, T. et al.)
- ALMA polarization observation of the protoplanetary disk
around HL Tau (Kataoka, A. et al.)- First Global Simulation Yields New Insights into Ring System(Kokubo, E. et al.)

- 14th International Symposium on “Origin of Matter and
Evolution of Galaxies,” Institute of Basic Science in Daejeon,
Korea, June 26–29 in 2017. (Participants; 110)
- International Symposium on “Cosmic Dust X,” NAOJ Mitaka,
August 14–18 in 2017. (Participants; 55)- International Symposium on “Stellar Evolution, Supernova andNucleosynthesis Across Cosmic Time,” University of Tokyo,
Kavli Institute, September 19–29 in 2017. (Participants; 56)- East-Asian AGN Workshop 2017, University of Tokyo,
Kagoshima University, December 4–6 in 2017. (Participants;
107)- Inter national Workshop on “Impact of Exotic Nuclear
Structure on Explosive Nucleosynthesis,” Beihang University,
China, November 22–24 in 2017. (Participants; 59)- International Workshop on “WFIRST-Subaru Synergistic
Observations,” NAOJ Mitaka, December 18–20 in 2017.
(Participants; 88)- International Symposium “GWASNe2018,” NAOJ Mitaka,
January 29–31 in 2018. (Participants; 44)- The 8th DTA Symposium on “Challenge to super-Earths
and their atmospheres,” NAOJ Mitaka, March 6–8 in 2018.
(Participants; 41)

4. Domestic Collaborations
The Division of Theoretical Astronomy played leadingroles in organizing the following domestic conferences:- Symposium on “Stellar formation and the role of magnetic
field in Galactic structure formation,” Kagoshima University,
December 20–22 in 2017. (Participants; 45)- 7th TDA Symposium on “Neut ron Stars: Theor y andObservation,” NAOJ Mitaka, November 22–24 in 2017.
(Participants; 67)-30th RIRONKON Symposium on “Beyond the Horizon of
Stellar Astrophysics,” University of Tokyo Hongo, December
25–27 in 2017. (Participants; 182)
Toshitaka Kajino performed duties as a chairman of Japan
Forum of Nuclear Astrophysics for planning and managing
international and domestic conferences related to cosmonuclear physics and promoting research collaboration in related
fields such as astronomy, astrophysics and nuclear physics inJapan.

5. International Collaborations
Eiichiro Kokubo served on the organizing committeeof Commission A4 (Celestial Mechanics and Dynamical
Astronomy) of IAU.
Toshitaka Kajino perfor med duties of the following
posts: international referee for the Science, Technology andInnovation Council of Canada; international referee for112

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6. Educational Activities
The lecture subjects are listed below to supplement Section
III on activities of research and educational adjunct lecturership at the high schools, universities, and graduate schools:- Eiichiro Kokubo: Earth and Planetary Science I at the
University of Tokyo; SSH lecture on The Earth in the
Universe at Hibiya high school.
- Haruo Yoshida: UEC passport program seminar entitled
Integrable and non-integrable problems in classical mechanics
for the first year students of the University of ElectroCommunications.
- Tomoya Takiwaki: Special lectures III on Numerical Physics,
at the Graduate Course of Chiba University.
- Toshitaka Kajino: Lectures on fundamentals of theoreticalastronomy at the Graduate University for Advanced Studies;science of time, space, and matter, and fundamentals ofphysics at Gakushuin University; astrophysics and modern
physics at Japan Women’s University; astrophysics at Jissen
Women’s University; nuclear physics at Meiji University;
astronomy investigation I & II, reading papers in turn I & II,
and special astronomy investigation II at the Graduate Schoolof the University of Tokyo.

7. Outreach Activities
The Division of Theoretical Astronomy actively engaged inpublic promotions and outreach activities by offering lectures
to the general public. The following lectures were delivered
this year:- Eiichiro Kok ubo: “Sat ur n f rom Cassini: A Beautif ulRing World” at Aasahi Culture Center at Yokohama andNakanoshima, “New Solar System 2017” at Ikebukuro
Community College, “From Stardust to the Earth” at SpaceExpo.
- Takiwaki Tomoya: “Supernova Explosion simulated bySupercomputer, A Telescope for Theory” (Mitaka Network
Un ive r sit y), “ Sup e rc omput e r reve als t he Ex plosion
Mechanism of Supernovae” (Asahi Culture Center Shonan).
- Takashi Moriya: “Origin of the elements” (Asahi Culture
Center Yokohama).
- Toshitaka Kajino: “Nobel Prize on Modern Cosmology:
Beginning of the Universe and the Discovery of Cosmic
Microwave Background Radiation” (Asahi Culture Center
Yokohama).

GAO, Weijia (Beijing Normal University, P. R. China)
HASAGAWA Yasuhiro (NASA Jet Propulsion Laboratory)
LAMBRECHTS, Michiel (Lund University, Sweden)
LIM, Wanggi (University of Florida, USA)
MATTHEW, Kenworthy (Leiden University, Netherland)
MATHEWS, Grant J. (University of Notre Dame, USA)
MAZZALI, Paolo (Liberpool John Moores University)
NORMAN, Colin Arthur (Johns Hopkins University)
PEHLIVAN, Yamac (Mimar Sinan University of Fine Art,
Turkey)PENZLIN, Anna (Heidelberg University, Germany)
PIAN, Elena (Italian National Institute of Astrophysics/
Institute of Space Astrophysics and Cosmic Physics, Italy)
RICHMOND, Michael (Rochester Institute of Technology)
TAN, Jonathan (University of Florida)
VOROBIEV, Eduard (Technical University of Vienna)

8. Awards
Masaomo Tanaka received the NCU-DELTA Young
Astronomer Lectureship Award (October 18 in 2017) in Taiwan.
Toshitaka Kajino received the honors of One Thousand Talents
Plan Foreign Expert (April 15 in 2017) and State Special
Recruited Expert (1 January 2018) in the People’s Republic ofChina.

9. Main Visitors from Overseas
The Division of Theoretical Astronomy strives to fulfill its
roles as a center of excellence in Japan for theoretical studies
in astronomy and astrophysics and also as an international
research instit ution by providing an excellent research
environment. It engages in various joint research projects withvisiting researchers from overseas, with the help of Grants-inAid for Scientific Research, government subsidies for operating
expenses, the NAOJ budget for guest visitors, and others. The
main international visitors of FY 2017 to the division are listed
below:BALANTEKIN, Akif B. (University of Wisconsin–Madison,USA)
BAUER, Franz (Pontificia Universidad Catolica de Chile,
Chili)
CAI, Maxwell (Leiden University, Netherland)
CASELLI, Paola (Max-Planck-Institute, Germany)
CHAU, Ching Chong (Academia Scinica, Taiwan)
CHEOUN, Myung-Ki (Soongsil University, South Korea)
DELIDUMAN, Cemsinan (Mimar Sinan University of Fine
Art, Turkey)
FAMIANO, Michael A. (Western Michigan University, USA)

II Status Reports of Research Activities113

21. Office of International Relations
The Office of International Relations strives to promote andfacilitate further internationalization at NAOJ by maintaining
an environment where multi-cultural researchers and students
can engage cooperatively in research and educational activities.
Specifically, the Office’s main activities include supportinginternational collaborative projects; managing Security Export
Control; offering support for hosting international conferences,
workshops, and seminars; hosting booths at international events,
and providing support for visiting international researchersand students. In FY 2017 the Office continued to work closelywith the Executive Advisor to the Director General in charge ofinternational research coordination.

1. International Collaborative Project Support
The Office of International Relations handled administrative
coordination in approval processes to sign agreements andmemoranda for international collaborations, conducting
preliminary reviews for legal documentation, and managing
export security control for export of goods or transfer oftechnology. In FY 2017, nineteen international agreements, newand renewed, were signed including ones under the name of
NINS. In the area of security export control, activities included
review and processing of 150 cases (293 items). Out of them,an individual export license as well as a re-export license under
EAR was required in one case, which we processed accordingly
and obtained the licenses. A security export control briefing
was held three times at Mitaka (June: 39 attendants, July: 48
attendants, and March: 6 attendants (in English)) and once in
Hawai`i (July: 6 attendants) for improving the knowledge andawareness of NAOJ staff. In addition to these briefings, anexplanation hosted by NINS was held in January 2018. The total
number of attendants reached 150.

2. Liaison Work for Overseas Astronomical
Research Organizations
The Office of International Relations joined the EAO(East Asian Observatory) financial committee meeting held inparallel with the JCMT mid-term review on July 24–29, 2017 in
Hawai`i. The office participated in the exchange of opinions forfinancially healthy management of EAO/JCMT. Also, the officesupported the East Asian Young Astronomers Meeting (EAYAM)
held at Ishigaki Island on November 13–17, 2017.
The Office also assisted the Executive Advisor to the
Director General in charge of international research coordination
upon coordinating with the other 3 institutions forming the East
Asian Core Observatories Association (EACOA) including
NAOC (China), KASI (Republic of Korea), and ASIAA (Taiwan)
for selection of the 2018 EACOA/EAO postdoctoral fellowship
program recipients.
We hosted an NAOJ booth at the ASIA-Pacific Regional
IAU Meeting held at Taipei during July 3–7, 2017 and AAS (The114

II Status Reports of Research Activities

American Astronomical Society) meeting at Washington D.C.
during January 7–14, 2018 to promote research results and to
explain the current status of each project. Though it was our firsttime attending AAS, the reaction from the participants was muchgreater than we expected. We would like to keep attending AAS
for the time being.
Furthermore, the Office supported the activities of the Officefor Astronomical Outreach of the IAU (IAU OAO) and the IAU
Office for Astronomy Development (OAD, located in South
Africa). We supported CAP2018 held at Fukuoka during March
23–29, 2018 as an LOC member.
Same as last year, the Public Relations Office was
responsible for overseas activities in relation to the generalpublic, while the Office of International Relations was in chargeof activities related to overseas researchers.

3. Support for Hosting International
Researchers and Students
T h e O ff i c e e n h a n c e d i t s f r a m e w o r k f o r o ff e r i n gorganizational support for research, education, and living
arrangements for foreign researchers and exchange students.
The Support Desk offers support services to ease difficulties
for foreigners living in Japan. It supports, on-site if required,covering various matters such as administrative procedures atmunicipal and other governmental offices, finding and moving
into an apartment, and other various procedures and applications
for starting up a new life, consultation on shopping, children’s
education, health and others, and gathering/providing useful
information relating to everyday life. The Support Desk has
been highly appreciated by users. To provide better services,
Support Desk has been changed to be 2 staff × 3 days each shift.
Thus, on Thursday when both of the SD staff members are at
the office, we hold regular meetings between the SD staff andthe other office members. As a result, the smooth transfer of ongoing issues, as well as information sharing, became possible.
The Office continued the Japanese language lessons, helping
foreign members of NAOJ acquire beginner level capability,and for FY 2017, a combination of E-learning features andclassroom lessons were provided, as was in the previous year.
The Office continued its activities to support non-Japanese
speaking staff, by translating various forms for applications andnotices, including e-mail text and explanations of procedures(112 documents).

4. Assistance in International Partnerships
Involving Japanese Research Organizations
The Office oversaw the Optical and Infrared Synergetic
Telescopes for Education and Research (OISTER) project
conducted by Okayama Astrophysical Observatory, Ishigakijima
Astronomical Observatory, and nine Japanese universities.
Although the budget for the OISTER project was transferredto the Research Promotion Division from FY 2017 onward, theOffice continued to provide administrative support.
Also the Office provided support for the Asian Core
Observatories Initiative led by the Executive Advisor to the
Director General in charge of international research coordination
under NINS’s research enhancement program with the Research
University Network of Japan.

II Status Reports of Research Activities

115III Organization
1. Organization
Projects(C Projects)

Subaru Telescope
Okayama Astrophysical Observatory
Nobeyama Radio Observatory
Advisory Committee for Research and Management

Mizusawa VLBI Observatory
Solar Science Observatory
NAOJ Chile Observatory
Center for Computational Astrophysics(B Projects)

Director General

Gravitational Wave Project OfficeVice-Director General (on General Affairs)
Vice-Director General (on Finance)
Director of Engineering
Director of Research Coordination
Executive Advisors to the Director General

TMT-J Project Office(A Projects)

JASMINE Project Office
Extrasolar Planet Detection Project Office(~2017.12)

RISE Project
SOLAR-C Project Office
Centers
Astronomy Data Center
Advanced Technology Center
Public Relations Center
Divisions
Division of Optical and Infrared Astronomy
Division of Radio Astronomy
Division of Solar and Plasma Astrophysics
Division of Theoretical Astronomy
Research Enhancement Strategy Office
Research Evaluation Support Office
Office of International Relations
Human Resources Planning Office
Safety and Health Management Office
Engineering Promotion Office
Administration Department

116

III Organization

2. Number of Staff Members
Director General
Research and Academic Staff
Professor
Executive Engineer
Associate Professor
Chief Research Engineer
Assistant Professor
Research Associate
Research Engineer
Engineering Staff
Administrative Staff
Research Administrator Staff
Employees on Annual Salary System
Full-time Contract Employees
Part-time Contract Employees
Part-time Contract Employees Transferring to the
Mandatory Retirement System(2018/3/31)
1
151
25
0
40
11
60
0
15
37
59
11
149
44
124
3

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

Watanabe, Jun-ichi
Kobayashi, Hideyuki
Takami, Hideki
Gouda, Naoteru

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

Ogasawara, Ryusuke
Sekiguchi, Kazuhiro

Hayashi, Masahiko

III Organization

117

4. Research Departments
Projects
C Projects

Subaru Telescope
Director
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor

Yoshida, Michitoshi
Ohashi, Nagayoshi
Yoshida, Michitoshi
Iwata, Ikuru
Noumaru, Junichi
Takato, Naruhisa
Takeda, Yoichi
Tanaka, Masayuki
Iwashita, Hiroyuki
Imanishi, Masatoshi
Komiyama, Yutaka
Koyama, Yusei
Minowa, Yosuke
Okita, Hirofumi
Ono, Yoshito
Onodera, Masato
Pyo, Tae-Soo
Hayashi, Masao

Specially Appointed
Assistant Professor

Izumi, Takuma

Research Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Engineer
Specially Appointed
Research Staff

Bando, Takamasa
Namikawa, Kazuhito
Omata, Koji
Tamura, Tomonori
Sato, Tatsuhiro
Niino, Yuu

Specially Appointed
Senior Specialist

Ikeda, Hiroyuki

Specially Appointed
Senior Specialist

Koike, Michitaro

Specially Appointed
Senior Specialist

Mineo, Sogo

Specially Appointed
Senior Specialist

Nakajima, Masayo

Specially Appointed
Senior Specialist

Oishi, Yukie

Specially Appointed
Senior Specialist

Okura, Yuki

Specially Appointed
Senior Specialist

Taniguchi, Akimitsu

Specially Appointed
Senior Specialist

Yamada, Yoshihiko

Specially Appointed
Senior Specialist

Yamanoi, Hitomi

Research Expert
Kawanomoto, Satoshi
Administrative Supporter Kuwata, Hitomi

118

III Organization

Administrative Supporter Noguchi, Masumi
Administrative Supporter Shibata, Junko
Administrative Supporter Suehiro, Yoko
Administrative Supporter Takamoto, Masami
Administrative Supporter Yoshida, Chie
Administration Department
ManagerSeto, Yoji
General Affairs Section
Chief
Chiba, Satoko
Accounting Section
Chief
Sugawara, Satoshi
RCUH
RCUH
Alpiche, Dex
RCUH
Aoki, Kentaro
RCUH
Balbarino, Michael
RCUH
Boggess, Christopher
RCUH
Castro, Timothy
RCUH
Clergeon, Christophe
RCUH
Conol, JonahRCUH
Doi, Yoshiyuki
RCUH
Elms, Brian
RCUH
Endo, Mari
RCUH
Ferreira, James
RCUH
Formanek, Keiko
RCUH
Fujiwara, Hideaki
RCUH
Fujiyoshi, Takuya
RCUH
Gaskin, Roberta
RCUH
Gorman, William
RCUH
Guyon, Olivier
RCUH
Hasegawa, Kumiko
RCUH
Hattori, Takashi
RCUH
Inagaki, Takeshi
RCUH
Jeschke, Eric
RCUH
Kackley, Russell
RCUH
Kakazu, Yuko
RCUH
Kerns, Michael
RCUH
Kim, Ji Hoon
RCUH
Koshida, Shintaro
RCUH
Kudo, Tomoyuki
RCUH
Kyono, Eiji
RCUH
Lee, Chien-Hsiu
RCUH
Lemmen, Michael
RCUH
Letawsky, Michael
RCUH
Lozi, Julien
RCUH
Medeiros, Carolyn
RCUH
Mieda, Etsuko
RCUH
Morris, Marita
RCUH
Murai, Rieko
RCUH
Nabeshima, Yoshitake
RCUH
Nakata, Fumiaki
RCUH
Niimi, Yuka
RCUH
Nishimura, Tetsuo
RCUH
Otsuki, Noriko

RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH

Ramos, LucioRoth, Noriko
Rousselle, Julien
Rusu, Cristian
Sahoo, Ananya
Schubert, Kiaina
Spencer, Robin
Suh, Hyewon
Sur, Ryoko
Suzuki, Yuko
Tait, Philip
Tajitsu, Akito
Takagi, Yuhei
Takiura, Koki
Tamae, Richard
Tanaka, Makoto
Tanaka, Yoko
Terai, Tsuyoshi
Tomono, Daigo
Toyofuku, Ralph
Tsang, EmikoWahl, Matthew
Weber, Mark
Williams, Joshua
Winegar, Tom
Wung, Matthew
Yoshida, Hiroshige
Yoshiyama, Naomi

Okayama Astrophysical Observatory
Director
Izumiura, Hideyuki
Associate Professor
Izumiura, Hideyuki
Associate Professor
Ukita, Nobuharu
Specially Appointed
Kambe, Eiji
Associate Professor
Assistant Professor
Engineer
Specially Appointed
Research Staff

Yanagisawa, Kenshi
Tsutsui, Hironori
Matsubayashi, KazuyaSpecially Appointed
Senior Specialist

Fukui, Akihiko

Research Expert
Kuroda, Daisuke
Research Supporter
Toda, Hiroyuki
Administration Office
Administration Section
Chief
Tanabe, Keizo
Administrative Supporter Katayama, Kumiko
Administrative Supporter Shibukawa, Hiroko
Administrative Supporter Yamashita, Ayako
Administrative
Koyama, Shoji
Maintenance Staff
Administrative
Watanabe, Noriaki
Maintenance Staff
Nobeyama Radio Observatory
Director

Tatematsu, Kenichi

Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor

Tatematsu, Kenichi
Kanzawa, Tomio
Ishizuki, Sumio
Minamidani, Tetsuhiro
Umemoto, Tomofumi
Torii, Kazufumi

Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
EngineerEngineer
Specially Appointed
Research Staff

Mikoshiba, Hiroshi
Handa, Kazuyuki
Kurakami, Tomio
Miyazawa, Chieko
Miyazawa, Kazuhiko
Shinohara, Noriyuki
Nishitani, Hiroyuki
Wada, Takuya
Kaneko, Hiroyuki

Specially Appointed
Research Staff

Kim, Gwanjeong

Specially Appointed
Research Staff

Miyamoto, Yusuke

Specially Appointed
Senior Specialist

Hamada, KanameSpecially Appointed
Senior Specialist

Kinugasa, Kenzo

Specially Appointed
Senior Specialist

Oya, Masaaki

Research Expert
Maekawa, Jun
Research Expert
Takahashi, Shigeru
Technical Expert
Hayashi, Mitsuru
Technical Expert
Ide, Hidemi
Technical Expert
Inoue, Norio
Research Supporter
Matsuo, Mitsuhiro
Administrative Supporter Hatakeyama, Eiko
Administration Office
Deputy Manager
Otsuka, Tomoyoshi
General Affairs Section
Chief
Otsuka, Tomoyoshi
Administrative Supporter Kikuchi, Kikue
Administrative Supporter Shinkai, Hisako
Administrative Supporter Yoda, Chizuko
Administrative
Fuji, Shigeru
Maintenance Staff
Administrative
Maintenance Staff

Hinata, Shigeto

Administrative
Maintenance Staff

Ide, Hiroko

Administrative
Maintenance Staff

Kadoshima, Junko

Administrative
Maintenance Staff

Kikuchi, Michiko

Administrative
Maintenance Staff

Kikuchi, Tsuyoshi

Administrative
Maintenance Staff

Koike, Ikuko

III Organization

119Administrative
Maintenance Staff

Tsuchiya, Junko

Administrative
Maintenance Staff

Yokomori, Yasuyuki

Accounting Section
Chief
Miyabara, Yasuhide
Senior Staff
Takahashi, Masaru
Administrative Supporter Kodaira, Toshiko
Administrative Supporter Takasawa, Mitsue
Administrative Supporter Takemura, Miwako
Administrative Supporter Tokui, Chisato
Mizusawa VLBI Observatory
Director
Professor
Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Chief Engineer
Engineer
Specially Appointed
Research Staff

120

Honma, Mareki
Honma, Mareki
Kobayashi, Hideyuki
Shibata, Katsunori
Sato, Katsuhisa
Hada, Kazuhiro
Hirota, Tomoya
Jike, Takaaki
Kameya, Osamu
Kono, Yusuke
Sunada, Kazuyoshi
Tamura, Yoshiaki
Ishikawa, Toshiaki
Suzuki, Syunsaku
Ueno, Yuji
Hirano, Ken
Akahori, Takuya

Technical Expert
Sato, Gen
Technical Expert
Sato, Kaori
Technical Expert
Shimada, Kanae
Technical Expert
Takahashi, Ken
Technical Expert
Yamashita, Kazuyoshi
Technical Expert
Yoshida, Toshihiro
Administrative Expert
Endo, Kana
Research Supporter
Kudo, Yohei
Research Supporter
Matsueda, Chika
Technical Supporter
Konishi, Satoru
Administrative Supporter Komori, Akiyo
Administrative Supporter Uekiyo, Hatsue
Administration Office
Deputy Manager
Hommyo, Susumu
General Affairs Section
Chief
Hommyo, Susumu
Staff
Iida, Naoto
Administrative Supporter Murakami, Mie
Administrative Supporter Oizumi, Yuka
Administrative Supporter Sasaki, Mie
Accounting Section
Chief
Ito, Hiromasa
Administrative Supporter Kikuchi, Sachiko
Administrative Supporter Takahashi, Yumi
Ishigakijima Astronomical Observatory
Director
Honma, Mareki
Time Keeping OfficeDirector
Sato, Katsuhisa
Solar Science Observatory
Director
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Senior Engineer
Specially Appointed
Research Staff

Watanabe, Tetsuya
Watanabe, Tetsuya
Hanaoka, Yoichiro
Katsukawa, Yukio
Suematsu, Yoshinori
Sekii, Takashi
Shinoda, Kazuya
Joshi, Anand Diwakar

Specially Appointed
Research Staff

Hanayama, Hidekazu

Specially Appointed
Research Staff

Horiuchi, Takashi

Specially Appointed
Research Staff

Sakai, Nobuyuki

Specially Appointed
Research Staff

Sugiyama, Koichiro

Specially Appointed
Research Staff

Tazaki, Fumie

Specially Appointed
Research Staff

Lee, Kyoung Sun

Specially Appointed
Senior Specialist

Adachi, Yuki

Specially Appointed
Senior Specialist

Morita, Satoshi

Specially Appointed
Senior Specialist

Kim, Mi Kyoung

Specially Appointed
Senior Specialist

Miura, Mitsuo

Specially Appointed
Senior Specialist

Nagayama, Takumi

Research Expert
Hagino, Masaoki
Research Expert
Yaji, Kentaro
Technical Expert
Inoue, Naoko
Research Supporter
Ishii, Shuichi
Administrative Supporter Kano, Kaori
Administrative Supporter Sugimoto, Junko

Specially Appointed
Senior Specialist

Oyama, Tomoaki

Specially Appointed
Senior Specialist

Ozawa, TomohikoTechnical Expert
Technical Expert
Technical Expert

Asakura, Yu
Hachisuka, Kazuya
Matsukawa, Yuki

III Organization

NAOJ Chile Observatory
Director
Professor
Professor
Professor
Professor

Sakamoto, Seiichi
Iguchi, Satoru
Kameno, Seiji
Mizuno, Norikazu
Ogasawara, Ryusuke

Specially Appointed
Research Staff

Ao, Yiping

Specially Appointed
Research Staff

Guzman Fernandez,
Andres Ernesto

Specially Appointed
Research Staff

Hashimoto, TakuyaSpecially Appointed
Research Staff

Izumi, Natsuko

Specially Appointed
Research Staff

Kroug, Matthias Nils

Specially Appointed
Research Staff

Lu, Xing

Specially Appointed
Research Staff

Nishimura, Yuri

Kawamura, Akiko

Specially Appointed
Associate Professor

Nagai, Hiroshi

Specially Appointed
Research Staff

Salinas Poblete, VachailNicolasSpecially Appointed
Associate Professor

Nakanishi, Koichiro

Specially Appointed
Research Staff

Sanhueza Nunez,
Patricio Andres

Specially Appointed
Associate Professor

Tafoya Martinez, DanielSpecially Appointed
Research Staff

Silva Bustamante,Andrea Ludovina

Kikuchi, Kenichi
Nakamura, Kouji
Watanabe, Manabu
Ezawa, Hajime
Hiramatsu, Masaaki
Hirota, Akihiko
Ishii, Shun
Kamazaki, Takeshi
Matsuda, Yuichi
Sawada, Tsuyoshi
Shimojo, Masumi
Takahashi, Satoko
Akiyama, Eiji

Specially Appointed
Research Staff

Takahashi, Sanemichi

Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor

Specially Appointed
Research Staff

Tanaka, Kei

Specially Appointed
Research Staff

Tokuda, Kazuki

Specially Appointed
Research Staff

Walker, Daniel Lewis

Specially Appointed
Research Staff

Wang, Tao

Specially Appointed
Research Staff

Wu, Yu-Ting

Specially Appointed
Research Staff

Zahorecz, Sarolta

Egusa, Fumi

Specially Appointed
Senior Specialist

Fujimoto, Yasuhiro

Specially Appointed
Assistant Professor

Hull, Charles Lindsay
Hopkins

Specially Appointed
Senior Specialist

Fukui, Hideharu

Specially Appointed
Assistant Professor

Miura, Rie

Specially Appointed
Senior Specialist

Furutani, Akio

Specially Appointed
Assistant Professor

Okamoto, Joten

Specially Appointed
Senior Specialist

Horie, Yosaku

Specially Appointed
Assistant Professor

Saigou, KazuyaSpecially Appointed
Senior Specialist

Ikeda, Emi

Specially Appointed
Assistant Professor

Ueda, Junko

Specially Appointed
Senior Specialist

Kawakami, Kazuyuki

Specially Appointed
Assistant Professor

Ashitagawa, Kyoko
Nakazato, Takeshi
Yamada, Masumi
Kato, Yoshihiro
Kobiki, ToshihikoNakamura, Kyoko
Ito, Tetsuya
Shizugami, Makoto

Specially Appointed
Senior Specialist

Kawasaki, Wataru

Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Engineer

Specially Appointed
Senior Specialist

Kobayashi, Tsuyoshi

Specially Appointed
Senior Specialist

Konuma, Mika

Specially Appointed
Senior Specialist

Matsui, Takayuki

Specially Appointed
Senior Specialist

Miel, Renaud Jean
Christophe

Professor
Specially Appointed
Professor

Sakamoto, Seiichi
Hasegawa, Tetsuo

Associate Professor
Associate Professor
Associate Professor

Asaki, Yoshiharu
Asayama, Shinichiro
Gonzalez Garcia,
AlvaroAssociate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor

Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Okuda, Takeshi
Espada Fernandez,
DanielSpecially Appointed
Associate Professor

III Organization

121

Specially Appointed
Senior Specialist

Miyachi, Akihira

Specially Appointed
Research Staff

Asahina, Yuta

Specially Appointed
Senior Specialist

Morita, Eisuke

Specially Appointed
Research Staff

Ohtani, YukariSpecially Appointed
Senior Specialist

Nakamoto, Takashi

Specially Appointed
Senior Specialist

Oshino, Shoichi

Specially Appointed
Senior Specialist

Nakanishi, Takashi

Specially Appointed
Senior Specialist

Niizeki, Yasuaki

Specially Appointed
Senior Specialist

Nishikawa, Tomoko

Specially Appointed
Senior Specialist

Nukatani, Sorahiko

Research Expert
Kato, Tsunehiko
Research Expert
Nakayama, Hirotaka
Research Expert
Wakita, Shigeru
Research Supporter
Fukushi, Hinako
Research Supporter
Hasegawa, Satoki
Research Supporter
Oshigami, Shoko
Research Supporter
Taki, Tetsuo
Administrative Supporter Kimura, Yuko

Specially Appointed
Senior Specialist

Okumura, Yuji

Specially Appointed
Senior Specialist

Otawara, Kazushige

Specially Appointed
Senior Specialist

Shimoda, Takanobu

Specially Appointed
Senior Specialist

So, Ryoken

Specially Appointed
Senior Specialist

Uemizu, Kazunori

Specially Appointed
Senior Specialist

Yoshino, Akira

Research Expert
Sakuma, Naoko
Technical Expert
Tanaka, Rie
Administrative Expert
Kamada, Masako
Research Supporter
Ban, Makiko
Research Supporter
Yamazaki, Toshitaka
Technical Supporter
Hayashi, Ritsuko
Administrative Supporter Kono, Izumi
Administrative Supporter Otawara, Hikaru
Administrative Supporter Saito, Naoko
Chile Employee
Chile Employee
Aguilera, Javier
Chile Employee
Ichiyama, Kotoyo
Chile Employee
Jara, Ricardo
Chile Employee
Krapivka, Gabriela
Chile Employee
Toro, Lorena
Chile Employee
Zenteno, Javier
Administration Department
Manager
Okumura, Yuji
General Affairs Section
Chief
Tsukano, Satomi
Accounting Section
Chief
Okumura, Yuji
Center for Computational Astrophysics
Director
Kokubo, Eiichiro
Professor
Kokubo, Eiichiro
Assistant Professor
Osuga, Ken
Specially Appointed
Takahashi, Hiroyuki
Assistant Professor

122

III Organization

B Projects

Gravitational Wave Project OfficeDirector
Flaminio, RaffaeleSpecially Appointed
Flaminio, Raffaele
Professor
Associate Professor
Affiliated Associate
Professor

Aso, YoichiAndo, Masaki

Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor

Akutsu, Tomotada
Leonardi, Matteo
Ohishi, Naoko
Takahashi, Ryutaro
Shoda, Ayaka

Research Engineer
Chief Engineer
Specially Appointed
Research Staff

Ishizaki, Hideharu
Tanaka, Nobuyuki
Barton, Mark Andrew

Specially Appointed
Research Staff

Capocasa, Eleonora

Specially Appointed
Research Staff

Pena Arellano, Fabian
ErasmoSpecially Appointed
Research Staff

Zeidler, Simon

Specially Appointed
Senior Specialist

Hirata, Naoatsu

Specially Appointed
Senior Specialist

Tapia, San Martin Enzo
NicolasAdministrative Expert
Ohyama, Megumi
Research Supporter
Harada, Mikiko
Administrative Supporter Sakamoto, Eri
Administrative Supporter Yoshizumi, Mizuho
TMT-J Project OfficeDirector
Professor
Professor
Professor
Associate Professor
Associate Professor

Usuda, Tomonori
Saito, Masao
Usuda, Tomonori
Yamashita, Takuya
Aoki, Wako
Hayashi, Saeko

Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor

Kashikawa, Nobunari
Sugimoto, Masahiro
Terada, Hiroshi
Oya, Shin

Assistant Professor*
Assistant Professor
Assistant Professor*
Specially Appointed
Assistant Professor*

Nakajima, Tadashi
Nishikawa, Jun
Suto, Hiroshi
Hashimoto, Jun

Chief Research Engineer Miyashita, Takaaki
Assistant Professor
Yasui, Chikako
Specially Appointed
Hattori, Masayuki
Assistant Professor

Specially Appointed
Assistant Professor*

Hori, Yasunori

Specially Appointed
Research Staff*

Komatsu, Yu

Specially Appointed
Research Staff

Harakawa, Hiroki

Specially Appointed
Research Staff

Konishi, Mihoko

Specially Appointed
Research Staff

Kubo, MarikoSpecially Appointed
Research Staff*

Kuzuhara, Masayuki

Specially Appointed
Research Staff

Ozaki, Shinobu

Specially Appointed
Research Staff

Omiya, Masashi

Specially Appointed
Research Staff

Schramm, Malte

Specially Appointed
Research Staff*

Suzuki, Taiki

Specially Appointed
Senior Specialist

Chapman, Junko

Specially Appointed
Senior Specialist*

Kusakabe, NobuhikoSpecially Appointed
Senior Specialist

Endo, Tatsuki

Research Supporter
Kurokawa, Takashi*concurrently appointed in NINS

Specially Appointed
Senior Specialist

Kozu, Akihito

Specially Appointed
Senior Specialist

Kusumoto, Hiroshi

Specially Appointed
Senior Specialist

Shindo, Miwa

Specially Appointed
Senior Specialist

Sugiyama, Motokuni

Research Expert
Ishii, Miki
Special Senior Specialist Inatani, Junji
Research Supporter
Tajima, Toshiyuki
Administrative Supporter Haranaka, Miyuki
Administrative Supporter Tabata, Miwa
Administrative Supporter Tatsugi, Tomoko
Administrative Supporter Yamaguchi, Chiyu
RCUH
Iye, Masanori

RISE Project
Director
Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Specially Appointed
Research Staff

Namiki, Noriyuki
Namiki, Noriyuki
Hanada, Hideo
Matsumoto, Koji
Tsuruta, Seiitsu
Araki, Hiroshi
Noda, Hirotomo
Asari, Kazuyoshi
Tazawa, Seiichi
Higuchi, Arika

Specially Appointed
Research Staff

Kawamura, Taichi

Specially Appointed
Research Staff

Yamamoto, Keiko

Administrative Supporter Sato, Sayaka

A Projects

JASMINE Project OfficeDirector
Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Research Staff

Gouda, Naoteru
Gouda, Naoteru
Tsujimoto, Takuji
Ueda, Akitoshi
Yano, Taihei
Baba, Junichi

Research Supporter
Research Supporter
Technical Supporter
Research AssistantMase, Ichiro
Utsunomiya, Shin
Kashima, Shingo
Kumamoto, Jun

Extrasolar Planet Detection Project Office (~2017.12)
Director
Tamura, Motohide
Assistant Professor*
Kotani, Takayuki

SOLAR-C Project OfficeDirector
Professor
Associate Professor*
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Research Staff

Ichimoto, Kiyoshi
Ichimoto, Kiyoshi
Goto, MotoshiHara, Hirohisa
Kano, Ryouhei
Ishikawa, Ryoko
Kubo, Masahito
Narukage, Noriyuki
Song, Donguk

Research Supporter
Tsuchiya, Chie
Administrative Supporter Fujiyoshi, Marie*concurrently appointed in NINSIII Organization

123Centers
Astronomy Data Center
Director
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Specially Appointed
Research Staff

Takata, Tadafumi
Ichikawa, Shinichi
Ohishi, Masatoshi
Takata, Tadafumi
Furusawa, Hisanori
Ito, Takashi
Oe, Masafumi
Shirasaki, Yuji
Inoue, Goki
Honma, Hidetomo

Kubo, Koichi
Takahashi, Toshikazu
Uraguchi, Fumihiro
Fukuda, Takeo
Ikenoue, Bungo
Inata, Motoko
Iwashita, Hikaru
Kaneko, Keiko
Mitsui, Kenji
Waseda, Koichi
Ezaki, Shohei
Sakai, Ryo
Tsuzuki, Toshihiro
Hayashi, Kohei

Specially Appointed
Research Staff

Sorahana, Satoko

Specially Appointed
Research Staff

Nagai, Makoto

Specially Appointed
Senior Specialist

Kamegai, Kazuhisa

Specially Appointed
Research Staff

Uchiyama, Mizuho

Specially Appointed
Senior Specialist

Makiuchi, Shinichiro

Specially Appointed
Senior Specialist

Saito, Sakae

Specially Appointed
Senior Specialist

Ozawa, Takeaki

Specially Appointed
Senior Specialist

Tanaka, Nobuhiro

Specially Appointed
Senior Specialist

Yamanaka, Satoshi

Technical Expert
Aiba, Kazukiyo
Technical Expert
Katsumoto, tatsuo
Administrative Supporter Kuroda, Kyoko
Administrative Supporter Murakami, Hiromi
Administrative Supporter Yoshida, Taeko
Research AssistantKozuki, Yuto

Specially Appointed
Senior Specialist

Zapart, Christopher
Andrew

Research Expert
Furusawa, Junko
Research Expert
Isogai, Mizuki
Research Supporter
Fujikawa, Makiko
Research Supporter
Noda, Sachiyo
Research Supporter
Utsumi, Motomu
Administrative Supporter Ishii, Yuko
JVO Project
Director
Ohishi, Masatoshi
Advanced Technology Center
Director
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Senior Engineer

124

Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
EngineerEngineerEngineer
Specially Appointed
Research Staff

III Organization

Noguchi, Takashi
Noguchi, Takashi
Takami, Hideki
Hayano, Yutaka
Matsuo, Hiroshi
Miyazaki, Satoshi
Shan, Wenlei
Fujii, Yasunori
Okada, Norio
Kojima, Takafumi
Nakaya, Hidehiko
Oshima, Tai
Suzuki, Ryuji
Fukushima, Mitsuhiro
Obuchi, Yoshiyuki
Sato, Naohisa
Kamata, Yukiko

Public Relations Center
Director
Professor
Professor
Associate Professor
Associate Professor
Research Engineer
Chief Senior Engineer
Chief Engineer
Chief of Library Section
Specially Appointed
Senior Specialist

Fukushima, Toshio
Fukushima, Toshio
Watanabe, Jun-ichi
Agata, Hidehiko
Yamaoka, Hitoshi
Katayama, Masato
Matsuda, Ko
Nagayama, Shogo
Todoriki, Tatsuya
Cheung, Sze Leung

Specially Appointed
Senior Specialist

Ishikawa, Naomi

Specially Appointed
Senior Specialist

Lundock, Ramsey Guy

Specially Appointed
Senior Specialist

Pires Canas, Lina Isabel

Specially Appointed
Senior Specialist

Tsuzuki, Hiroko

Specially Appointed
Senior Specialist

Usuda-Sato, Kumiko

Research Expert
Research Expert
Research Supporter
Public Outreach Official
Public Outreach Official
Public Outreach Official

Ono, Tomoko
Takata, Hiroyuki
Kume, KaoriEndo, Isao
Fujimura, Ayako
Fujita, Tokiko

Public Outreach Official Hamura, Taiga
Public Outreach Official Hatano, Satomi
Public Outreach Official Ishizaki, Masaharu
Public Outreach Official Ito, Hironori
Public Outreach Official Koike, Akio
Public Outreach Official Kubo, Maki
Public Outreach Official Mikami, Naotsugu
Public Outreach Official Naito, Seiichiro
Public Outreach Official Natsugari, Satomi
Public Outreach Official Nemoto, Shiomi
Public Outreach Official Ogoe, Osamu
Public Outreach Official Oguri, Junko
Public Outreach Official Shibata, Yukiko
Public Outreach Official Shioya, Yasuhisa
Public Outreach Official Takabatake, Noriko
Public Outreach Official Takeda, Takaaki
Administrative Supporter Aoki, Makiko
Administrative Supporter Noguchi, Sayumi
Public Relations OfficeDirector
Yamaoka, Hitoshi
Outreach and Education OfficeDirector
Agata, Hidehiko
Ephemeris Computation OfficeDirector
Katayama, Masato
Library
ChiefTodoriki, Tatsuya
Publications OfficeDirector
Fukushima, Toshio
The Office for Astronomy Outreach of the IAU
Director
Agata, Hidehiko
Administration OfficeDirector
Matsuda, Ko

Divisions
Division of Optical and Infrared Astronomy
Division Chair
Kashikawa, Nobunari
Professor
Gouda, Naoteru
Professor
Ohashi, Nagayoshi
Professor
Saito, Masao
Professor
Sekiguchi, Kazuhiro
Professor
Usuda, Tomonori
Professor
Yamashita, Takuya
Professor
Yoshida, Michitoshi
Specially Appointed
Tamura, Motohide
Professor*
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor

Aoki, Wako
Aso, Yoichi
Hayashi, Saeko
Iwata, Ikuru
Izumiura, Hideyuki
Kashikawa, Nobunari
Noumaru, Junichi
Sugimoto, Masahiro

Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor*
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor*
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor*
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor*

Takato, Naruhisa
Takeda, Yoichi
Tanaka, Masayuki
Terada, Hiroshi
Ukita, Nobuharu
Iwashita, Hiroyuki
Miyashita, Takaaki
Akutsu, Tomotada
Imanishi, Masatoshi
Komiyama, Yutaka
Kotani, Takayuki
Koyama, Yusei
Leonardi, Matteo
Minowa, Yosuke
Morino, Jun-ichi
Nakajima, Tadashi
Nishikawa, Jun
Ohishi, Naoko
Okita, Hirofumi
Ono, Yoshito
Onodera, Masato
Pyo, Tae-soo
Sôma, Mitsuru
Suto, Hiroshi
Takahashi, Ryutaro
Tatsumi, Daisuke
Tsujimoto, Takuji
Ueda, Akitoshi
Yagi, Masafumi
Yanagisawa, Kenshi
Yano, Taihei
Yasui, Chikako
Hashimoto, Jun

Specially Appointed
Assistant Professor*

Hori, Yasunori

Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
EngineerEngineer
Specially Appointed
Research Staff*

Bando, Takamasa
Ishizaki, Hideharu
Namikawa, Kazuhito
Omata, Koji
Tamura, Tomonori
Tanaka, Nobuyuki
Sato, Tatsuhiro
Tsutsui, Hironori
Komatsu, Yu

Specially Appointed
Research Staff*

Konishi, Mihoko

Specially Appointed
Research Staff*

Kuzuhara, Masayuki

Specially Appointed
Research Staff*

Omiya, Masashi

Specially Appointed
Research Staff*

Suzuki, Taiki

Specially Appointed
Senior Specialist*

Kusakabe, Nobuhiko

III Organization

125Administrative Supporter Kimura, Hiroko
Research AssistantOnoue, Masafusa*concurrently appointed in NINSDivision of Radio Astronomy
Division Chair
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor

126

III Organization

Iguchi, Satoru
Honma, Mareki
Iguchi, Satoru
Kameno, Seiji
Kawabe, Ryohei
Kobayashi, Hideyuki
Mizuno, Norikazu
Namiki, Noriyuki
Ogasawara, Ryusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Asaki, Yoshiharu
Asayama, Shinichiro
Gonzalez Garcia,
AlvaroHanada, Hideo
Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Matsumoto, Koji
Okuda, Takeshi
Shibata, Katsunori
Kanzawa, Tomio
Kawashima, Susumu
Kikuchi, Kenichi
Nakamura, Kouji
Sato, Katsuhisa
Tsuruta, Seiitsu
Watanabe, Manabu
Araki, Hiroshi
Ezawa, Hajime
Hada, Kazuhiro
Hiramatsu, Masaaki
Hirota, Akihiko
Hirota, Tomoya
Ishii, Shun
Ishizuki, Sumio
Jike, Takaaki
Kamazaki, Takeshi
Kameya, Osamu
Kono, Yusuke
Matsuda, Yuichi
Minamidani, Tetsuhiro
Miyoshi, Makoto
Noda, Hirotomo
Sawada, Tsuyoshi
Shimojo, Masumi
Sunada, Kazuyoshi
Takahashi, Satoko
Tamura, Yoshiaki
Umemoto, Tomofumi

Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
EngineerEngineerEngineerEngineer
Specially Appointed
Senior Specialist

Asari, Kazuyoshi
Ashitagawa, Kyoko
Ishikawa, Toshiaki
Mikoshiba, Hiroshi
Nakazato, Takeshi
Suzuki, Syunsaku
Tazawa, Seiichi
Yamada, Masumi
Handa, Kazuyuki
Kato, Yoshihiro
Kobiki, Toshihiko
Kurakami, Tomio
Miyazawa, Chieko
Miyazawa, KazuhikoNakamura, Kyoko
Shinohara, Noriyuki
Ito, Tetsuya
Ueno, Yuji
Hirano, Ken
Nishitani, Hiroyuki
Shizugami, Makoto
Wada, Takuya
Takebayashi, Yasuo

Research Supporter
Research Assistant

Tsuneyama, Junko
Taniguchi, Kotomi

Division of Solar and Plasma Astrophysics
Division Chair
Hanaoka, Yoichiro
Professor
Watanabe, Tetsuya
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Hara, Hirohisa
Associate Professor
Kano, Ryouhei
Associate Professor
Katsukawa, Yukio
Associate Professor
Sekii, Takashi
Associate Professor
Suematsu, Yoshinori
Assistant Professor
Ishikawa, Ryoko
Assistant Professor
Kubo, Masahito
Assistant Professor
Narukage, Noriyuki
Specially Appointed
Toriumi, Shin
Assistant Professor
Senior Engineer

Shinoda, Kazuya

Division of Theoretical Astronomy
Division Chair
Tomisaka, Kohji
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kohji
Professor
Yoshida, Haruo
Associate Professor
Kajino, Toshitaka
Associate Professor
Nakamura, Fumitaka
Assistant Professor
Hamana, Takashi
Assistant Professor
Kataoka, Akimasa
Assistant Professor
Ohsuga, Ken
Assistant Professor
Takiwaki, Tomoya
Assistant Professor
Tanaka, Masaomi

Specially Appointed
Assistant Professor

Moriya, Takashi

Specially Appointed
Assistant Professor

Nozawa, TakayaSpecially Appointed
Assistant Professor

Ogihara, Masahiro

Specially Appointed
Assistant Professor

Shirasaki, MasatoSpecially Appointed
Assistant Professor

Sotani, HajimeSpecially Appointed
Research Staff

Kawashima, Tomohisa

Specially Appointed
Research Staff

Kusune, Takayoshi

Specially Appointed
Research Staff

Wu, Benjamin

Administrative Supporter Izumi, Shioko

III Organization

1275. Research Support Departments
Research Enhancement Strategy OfficeDirector
Kobayashi, Hideyuki
Specially Appointed
Asaga, Akitaka
Senior Specialist

Okamoto, Koichi
Kashiwagi, Yuji
Tsuchiya, Tatsumi

Specially Appointed
Senior Specialist

Chapman, Junko

Specially Appointed
Senior Specialist

Fukui, Hideharu

Specially Appointed
Senior Specialist

Hasuo, Ryuichi

Specially Appointed
Senior Specialist

Hori, KunikoSpecially Appointed
Senior Specialist

Lundock, Ramsey Guy

Specially Appointed
Senior Specialist

Miura, Mitsuo

Specially Appointed
Senior Specialist

Noda, Noboru

Specially Appointed
Senior Specialist

Okamoto, Koichi

Specialist (Personnel
Accounting)Ishii, KatsuhikoSpecially Appointed
Senior Specialist

Suzui, Mitsukazu

Specially Appointed
Senior Specialist

Noguchi, Koki

Specially Appointed
Senior Specialist

Yamamiya, Osamu

Specially Appointed
Senior Specialist

Takahashi, Hidehiro

Research Evaluation Support OfficeDirector
Watanabe, Jun-ichi
Specially Appointed
Hori, Kuniko
Senior Specialist

Specially Appointed
Senior Specialist

Yamamoto, Chieko

Office of International Relations
Director
Specially Appointed
Senior Specialist

Hasuo, Ryuichi
Haruki, Mutsumi

Specially Appointed
Senior Specialist

Hasuo, Ryuichi

Specially Appointed
Senior Specialist

Komiyama, Hiroko

Specially Appointed
Senior Specialist

Matsumoto, Mizuho

Support Desk
Research Supporter
Research Supporter

Shirato, Reiko
Yamanaka, Wakana

Human Resources Planning OfficeDirector
Yamamiya, Osamu
Specially Appointed
Noda, Noboru
Senior Specialist
Specially Appointed
Senior Specialist

Yamamiya, Osamu

Safety and Health Management OfficeDirector
Okamoto, Koichi

128

Specially Appointed
Senior Specialist
Technical Expert
Technical Expert

III Organization

Engineering Promotion OfficeDirector
Takami, Hideki
Chief Research Engineer Kawashima, Susumu
Specially Appointed
Suzui, Mitsukazu
Senior Specialist
Administration Department
General Manager
General Affairs Division
Manager
Deputy Manager
Specialist (Information
Technology)

General Affairs Section
Chief
Staff
Staff
Staff
Vehicle Driver
Administrative Expert
Administrative Expert
Administrative Supporter
Administrative Supporter
Personnel Section
Chief
Staff
Staff
Staff
Payroll Section
Chief
Staff
Staff
Administrative Supporter
Administrative Supporter
Employee Affairs Section
Chief
Staff
Staff
Administrative Expert

Sasagawa, Hikaru
Harada, Eiichiro
Furuhata, Tomoyuki
Chiba, Yoko

Chiba, Yoko
Matsukura, Koji
Mochimaru, Shiori
Morita, Akitsugu
Amemiya, Hidemi
Murakami, Sachiko
Noguchi, Utako
Kobayashi, KayoSeki, Kumi
Yamanouchi, Mika
Isozaki, Yuka
Iwasaki, Yumi
Sakamoto, Misato
Ishii, Katsuhiko
Furukawa, Shinichiro
Inoue, Miyuki
Aiba, Narukazu
Momma, Yoko
Yamaura, Mari
Ouchi, Kaori
Saito, Masahiro
Noguchi, Megumi

Research Promotion Division
Manager
Ishibashi, Kazuya
Senior Specialist
Onishi, Tomoyuki
Administrative Supporter Ito, Yoshihisa
Research Support Section
Chief
Goto, Michiru
Staff
Nakagawa, Yukie
Administrative Expert
Tanaka, Midori
Administrative Expert
Yoshizawa, Mariko
Administrative Supporter Komoda, Chizuru
Administrative Supporter Suzuki, Yoshiko
Administrative Supporter Torii, Makiko
Administrative Supporter Urushibata, Kozue
Graduate School Section
Chief
Fujimori, Mihiro
Administrative Expert
Inoue, Mizuho
International Academic Affairs Section
Staff
Takada, Miyuki
MEXT Trainee
Staff
Yamafuji, Yasuto
Financial Affairs Division
Manager
Honda, Daisuke
Deputy Manager
Ikeda, Hiroshi
Specialist (Audit)
Ishikawa, Junya
Staff
Hiramatsu, Naoya
General Affairs Section
Chief
Yamamoto, Shinichi
Administrative Supporter Sasaki, Sayuri
Budget Section
Chief
Akaike, Makoto
Staff
Masuda, Akio
Administrative Supporter Ishida, Mikiko
Asset Management Section
Chief
Kikkawa, Hiroko
Staff
Takahashi, Sachiko
Purchase Validation Center
Chief
Kikkawa, Hiroko
Administrative Supporter Nakagomi, Kimitoshi
Administrative Supporter Shibui, Junko
Administrative Supporter Tsukamoto, Satoko
Accounting Division
Manager
Tanaka, Masaru
Specialist (Contract)
Miura, Susumu
Accounting Section
Chief
Sato, Yoko
Staff
Okubo, Kazuhiko
Administrative Supporter Kobayashi, Rina
Administrative Supporter Shinomiya, Miho
Administrative Supporter Suzuki, Yukiko
Procurement Section
Chief
Yamazaki, Go
Staff
Kayamori, Shinji
Staff
Sugimoto, Naomi

Staff
Consultant
Administrative Expert
Administrative Supporter
Facilities Division
Manager
General Affairs Section
Chief
Staff
Administrative Supporter
Planning Section
Chief
Administrative Supporter
Maintenance Section
Chief

Takai, Tetsuya
Hyuga, Tadayuki
Sato, Masako
Ochiai, Nana
Takahashi, Kazuhisa
Kawashima, Ryota
Tamura, Makoto
Hasegawa, Chisato
Murakami, Kazuhiro
Nagata, Yomogi
Narisawa, Hiroyuki

III Organization

129

6. Personnel change
Director General

130

Date

Name

Change2018/3/31

Hayashi, Masahiko

Contract
ExpiredNew Affiliated Institute, Position(Division of Optical and Infrared
Astronomy, Professor)

Previous Affiliated Institute,
Position
Director General

Research and Academic Staff
Date
Name

Change2017/4/1

Yoshida, Michitoshi

Hired(Hiroshima University Hiroshima
Division of Optical and Infrared Astronomy
Astrophysical Science Center,(Subaru Telescope), Professor
Professor)

2017/10/1

Leonardi, Matteo

Hired

Division of Optical and Infrared Astronomy (Max Planck Institute for Gravitational(Gravitational Wave Project Office),
Physics (Albert Einstein Institute),
Assistant Professor
Postdoctoral Researcher)2017/11/1

Ono, Yoshito

Hired

Division of Optical and Infrared Astronomy (Laboratory of Astrophysics of(Subaru Telescope), Assistant Professor
Marseille, Post-doctoral Fellow)

2017/12/1

Kataoka, Akimasa

Hired

Division of Theoretical Astronomy,
Assistant Professor

2018/3/1

Tanaka, Masayuki

HiredDivision of Optical and Infrared Astronomy (Subaru Telescope, Specially(Subaru Telescope), Associate Professor
Appointed Assistant Professor)

2017/4/30

Kodama, Tadayuki

Resigned(Tohoku University Graduate School of
Science, Professor)

Division of Optical and Infrared
Astronomy (Subaru Telescope),
Associate Professor
Advanced Technology Center,
Associate Professor

New Affiliated Institute, Position

Previous Affiliated Institute, Position(Division of Theoretical Astronomy,
Specially Appointed AssistantProfessor)

2017/9/30

Sekimoto, Yutaro

Resigned(Japan Aerospace Exploration Agency
Institute of Space and Astronautical
Science Department of Space Astronomy
and Astrophysics, Professor)

2018/3/31

Takami, Hideki

Resigned(Advanced Technology Center, Specially
Appointed Professor (Distinguished
Professor))

Advanced Technology Center,
Professor

2018/3/31

Tanaka, Masaomi

Resigned(Tohoku University Graduate School of
Science, Associate Professor)

Division of Theoretical Astronomy,
Assistant Professor

2018/3/31

Ohsuga, Ken

Resigned(University of Tsukuba Center for
Computational Sciences, Professor)

Division of Theoretical Astronomy(Center for Computational
Astrophysics), Assistant Professor

2018/3/31

Noguchi, Takashi

RetiredAdvanced Technology Center,
Professor

2018/3/31

Watanabe, Tetsuya

RetiredDivision of Solar and Plasma
Astrophysics (Solar Science
Observatory), Professor

2018/3/31

Ukita, Nobuharu

RetiredDivision of Optical and Infrared
Astronomy (Okayama AstrophysicalObservatory), Associate Professor

2018/3/31

Hanada, Hideo

RetiredDivision of Radio Astronomy (RISE
Project), Associate Professor

2018/3/31

Miyashita, Takaaki

RetiredDivision of Optical and Infrared
Astronomy (TMT-J Project Office),
Chief Research Engineer

2018/3/31

Kawashima, Susumu

RetiredDivision of Radio Astronomy(Engineering Promotion Office), Chief
Research Engineer

III Organization

Division of Radio Astronomy(Mizusawa VLBI Observatory), Chief
Research Engineer

2018/3/31

Sato, Katsuhisa

Retired2017/12/1

Katsukawa, Yukio

Promoted

Division of Solar and Plasma Astrophysics(Solar Science Observatory), Associate
Professor

Division of Solar and Plasma
Astrophysics (SOLAR-C Project
Office), Assistant Professor

2017/12/1

Gonzalez Garcia,
AlvaroPromoted

Division of Radio Astronomy (NAOJ
Chile Observatory), Associate Professor

Division of Radio Astronomy (NAOJ
Chile Observatory), AssistantProfessor

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Engineering Staff
Date

Name

2017/4/1

Sakai, Ryo

HiredAdvanced Technology Center, Engineer

2018/3/1

Kurakami, Tomio

Promoted

Division of Radio Astronomy (Nobeyama
Radio Observatory), Senior Engineer

Division of Radio Astronomy(Nobeyama Radio Observaory), Chief
Engineer

2018/3/1

Uraguchi, Fumihiro

Promoted

Advanced Technology Center, SeniorEngineer

Advanced Technology Center, Chief
Engineer

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Administrative Staff
Date

Name

2017/4/1

Ishibashi, Kazuya

HiredAdministration Department Research
Promotion Division, Manager(University of Toyama)

2017/4/1

Honda, Daisuke

HiredAdministration Department Financial
Affairs Division, Manager(Ministry of Education, Culture,
Sports, Science and TechnologyJapan)

2017/4/1

Takahashi, Kazuhisa

Hired

Administration Department Facilities
Division, Manager(Tokyo University of Foreign Studies)

2017/4/1

Ishii, Katsuhiko

HiredAdministration Department General
Affairs Division Payroll Section, Chief(Tokyo Gakugei University)

2017/4/1

Fujimori, Mihiro

Hired

Administration Department Research
Promotion Division Graduate Student
Affairs Section, Chief(The University of Tokyo)

2017/4/1

Miura, Susumu

Hired

Administration Department Research
Promotion Division External Funding
Specialist(Tokyo Gakugei University)

2017/4/1

Iwasaki, Yumi

Hired

Administration Department General
Affairs Division Personnel Section, Staff

2017/4/1

Okubo, Kazuhiko

HiredAdministration Department Accounting
Division Accounting Section, Staff

2017/4/1

Tamura, Makoto

Hired

Administration Department Facilities
Division General Affairs Section, Staff

2017/8/1

Takahashi, Masaru

HiredNobeyama Radio Observatory
Administration Office Accounting
Section, Senior Staff(Shinshu University)

2017/7/31

Iijima Kunio

Resigned(Shinshu University)

Nobeyama Radio Observatory
Administration Office Accounting
Section, Senior Staff

2018/3/31

Amemiya, Hidemi

Retired(Administration Department General
Affairs Division, Consultant)Administration Department General
Affairs Division General Affairs
Section, Vehicle Driver(The Graduate University for
Advanced Studies)

III Organization131

2018/3/31

Hommyo, Susumu

Retired(Mizusawa VLBI Observatory
Administration Office, Consultant)Mizusawa VLBI Observatory
Administration Office, Deputy Manager
and Chief of General Affairs Section

2017/8/1

Sugawara, Satoshi

Promoted

Subaru Telescope Administration
Department Accounting Section, Chief

Subaru Telescope Administration
Department Accounting Section,
Senior Staff

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Employee on Annual Salary System
Date

132

Name

2017/4/1

Izumi, Takuma

Hired

Subaru Telescope, Specially Appointed
Assistant Professor

2017/4/1

Kataoka, Akimasa

Hired

Division of Theoretical Astronomy,
Specially Appointed Assistant Professor

2017/4/1

Sugiyama, Koichiro

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2017/4/1

Tazaki, Fumie

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2017/4/1

Saito, Toshiki

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/4/1

Nishimura, Yuri

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/4/1

Wang, Tao

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/4/1

Baba, Jun'ichi

Hired

JASMINE Project Office, Specially
Appointed Research Staff

2017/4/1

Nagai, Makoto

Hired

Advanced Technology Center, Specially
Appointed Research Staff

2017/4/1

Kinugasa, Kenzo

Hired

Nobeyama Radio Observatory, Specially
Appointed Senior Specialist

2017/4/1

Hamada, Kaname

Hired

Nobeyama Radio Observatory, Specially
Appointed Senior Specialist

2017/4/1

Morita, Satoshi

HiredSolar Science Observatory, Specially
Appointed Senior Specialist

2017/4/1

Yamada, Yoshihiko

HiredSubaru Telescope, Specially Appointed
Senior Specialist

2017/4/1

Koike, Michitaro

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2017/4/1

Mineo, Sogo

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2017/4/1

Oshino, Shoichi

HiredCenter for Computational Astrophysics,
Specially Appointed Senior Specialist

2017/4/1

Miyachi, Akihira

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2017/4/1

Otawara, Kazushige

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist(NAOJ Chile Observatory, Specially
Appointed Senior Specialist)

2017/4/1

Furutani, Akio

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist(NAOJ Chile Observatory, Specially
Appointed Senior Specialist)

2017/4/1

Tanaka, Nobuhiro

HiredAstronomy Data Center, Specially
Appointed Senior Specialist

2017/4/1

Yamanaka, Satoshi

HiredAstronomy Data Center, Specially
Appointed Senior Specialist

2017/4/1

Usuda, Kumiko

HiredPublic Relations Center, Specially
Appointed Senior Specialist

III Organization(Mizusawa VLBI Observatory,Specially Appointed Research Staff)

2017/4/1

Saito, Sakae

Hired

Advanced Technology Center, Specially
Appointed Senior Specialist

2017/4/10

Sasada, Mahito

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2017/5/1

Adachi, Yuki

Hired

Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2017/5/1

Nishikawa, Tomoko

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2017/6/5

Kusune, Takayoshi

HiredDivision of Theoretical Astronomy,
Specially Appointed Research Staff

2017/7/1

Hanayama,
Hidekazu

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2017/8/1

Higuchi, Arika

Hired

RISE Project, Specially Appointed
Research Staff

2017/8/1

Okura, Yuki

HiredSubaru Telescope, Specially Appointed
Senior Specialist

2017/9/1

Hull, Charles
Lindsay Hopkins

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2017/9/1

Shirasaki, Masato

Hired

Division of Theoretical Astronomy,
Specially Appointed Assistant Professor

2017/9/1

Walker, Daniel Lewis Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/9/1

Nakajima, Masayo

HiredSubaru Telescope, Specially Appointed
Senior Specialist

2017/10/1

Akahori, Takuya

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2017/10/1

Wu, Yu-Ting

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/10/1

Hayashi, Kohei

HiredAdvanced Technology Center, Specially
Appointed Research Staff

2017/10/1

Kim, Mi Kyoung

Hired

Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2017/10/1

Yamanoi, Hitomi

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2017/10/1

Kobayashi, Tsuyoshi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2017/10/1

Matsumoto, Mizuho

Hired

Office of International Relations, Specially
Appointed Senior Specialist

2017/11/1

Tafoya Martinez,
DanielHired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2017/11/1

Kim, Gwanjeong

HiredNobeyama Radio Observatory, Specially
Appointed Research Staff

2017/11/1

Wu, Benjamin

Hired

Division of Theoretical Astronomy,
Specially Appointed Research Staff

2017/12/1

Hattori, Masayuki

Hired

TMT-J Project Office, Specially Appointed
Assistant Professor

2017/12/1

Horiuchi Takashi

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2017/12/1

Nakanishi, Takashi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2017/12/1

Endo, Tatsuki

Hired

TMT-J Project Office, Specially Appointed
Senior Specialist

2018/1/1

Tanaka, Kei

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2018/1/15

Capocasa, Eleonora

Hired

Gravitational Wave Project Office,Specially Appointed Research Staff

III Organization

133

134

2018/2/1

Ueda, Junko

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2018/2/1

Salinas Poblete,
Vachail Nicolas

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2018/2/1

Silva Bustamante,Andrea Ludovina

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2018/2/13

Guzman Fernandez,
Andres Ernesto

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2018/3/1

Ozawa, Tomohiko

Hired

Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2018/3/1

Shindo, Miwa

Hired

TMT-J Project Office, Specially Appointed
Senior Specialist

2018/3/1

Haruki, Mutsumi

Hired

Office of International Relations, Specially
Appointed Senior Specialist

2018/3/1

Takahashi, Hidehiro

Hired

Administration Department General Affairs
Division, Specially Appointed Senior
Specialist

2017/6/9

Neelamkodan,
NaslimResigned

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/6/15

Hayashi, Yusuke

Resigned

Subaru Telescope, Specially
Appointed Senior Specialist

2017/6/22

Muller, Erik Michael

Resigned

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2017/8/31

Dominjon, Agnes
Micheline

Resigned

Advanced Technology Center,
Specially Appointed Research Staff

2017/9/30

Hasebe, Takashi

Resigned

Advanced Technology Center,
Specially Appointed Research Staff

2017/10/31 Takagi, Yuhei

Resigned

Subaru Telescope, Specially Appointed
Research Staff

2017/11/30

Resigned

Kataoka, Akimasa(Division of Theoretical Astronomy,
Assistant Professor)

Division of Theoretical Astronomy,
Specially Appointed AssistantProfessor
Mizusawa VLBI Observatory,Specially Appointed Research Staff

2017/12/31 Sasada, Mahito

Resigned

2018/2/28

Tanaka, Masayuki

Resigned

2018/3/20

Sugimoto, Kanako

Resigned

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2018/3/31

Kawamura, Taichi

Resigned

RISE Project, Specially Appointed
Research Staff

2018/3/31

Hayashi, Kohei

Resigned

Advanced Technology Center,
Specially Appointed Research Staff

2018/3/31

Yamanaka, Satoshi

Resigned

Astronomy Data Center, Specially
Appointed Senior Specialist

2017/5/18

Wu, Yuanwei

Contract
ExpiredMizusawa VLBI Observatory,Specially Appointed Research Staff

2017/9/30

Saito,Toshiki

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Research Staff

2017/9/30

Kuniyoshi, Masaya

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Senior Specialist

2018/1/31

Saito, Motoi

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Senior Specialist

III Organization(Division of Optical and Infrared
Astronomy (Subaru Telescope), Associate
Professor)

Subaru Telescope, Specially Appointed
Assistant Professor

Kambe, Eiji

Contract
Expired2018/3/31

Kawamura, Akiko

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Associate Professor

2018/3/31

Akiyama, Eiji

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Assistant Professor

2018/3/31

Miyamoto, Yusuke

Contract
Expired2018/3/31

Matsubayashi,
KazuyaContract
ExpiredOkayama Astrophysical Observatory,Specially Appointed Research Staff

2018/3/31

Asahina, Yuta

Contract
ExpiredCenter for Computational
Astrophysics, Specially Appointed
Research Staff

2018/3/31

Konuma, Mika

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Senior Specialist

2018/3/31

Nukatani, Sorahiko

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Senior Specialist

2018/3/31

Kozu, Akihito

Contract
ExpiredTMT-J Project Office, Specially
Appointed Senior Specialist

2018/3/31

Komiyama, Hiroko

Contract
Expired

Office of International Relations,
Specially Appointed Senior Specialist

2017/9/1

2018/1/1

2018/1/1(Subaru Telescope, Specially Appointed
Associate Professor)

Okayama Astrophysical Observatory,Specially Appointed Associate
Professor

2018/3/31(NAOJ Chile Observatory, Specially
Appointed Assistant Professor)

Gravitational Wave Project Office,Specially Appointed Professor*Seconded based on the Agreement of
Cross Appointment with Centre Nationalde la Recherche Scientifique (CNRS)

Nobeyama Radio Observatory,Specially Appointed Research Staff

Gravitational Wave Project Office,Specially Appointed Professor

Flaminio, Raffaele

Changed(Seconded)

Omiya, Masashi

Astrobiology Center Astrobiology
Reassigned Equipment Development Office, Specially
Appointed Research Staff

National Astronomical Observatoryof Japan Extrasolar Planet Detection
Project Office, Specially Appointed
Research Staff

Konishi, Mihoko

Astrobiology Center Astrobiology
Reassigned Equipment Development Office, Specially
Appointed Research Staff

National Astronomical Observatoryof Japan Extrasolar Planet Detection
Project Office, Specially Appointed
Research Staff

Research Administrator Staff
Date

Name

ChangeNew Affiliated Institute, Position

2017/4/1

Okamoto, Koichi

Hired

Research Enhancement Strategy Office(Safety and Health Management Office),
Specially Appointed Senior Specialist

2017/10/1

Suzui, Mitsukazu

HiredResearch Enhancement Strategy Office(Engineering Promotion Office), Specially
Appointed Senior Specialist

2017/11/1

Asaga, Akitaka

HiredResearch Enhancement Strategy Office,Specially Appointed Senior Specialist

2018/1/1

Noda, Noboru

Hired

Research Enhancement Strategy Office(Human Resources Planning Office),
Specially Appointed Senior Specialist

Yamamiya, Osamu

Contract
Expired2018/3/31

Previous Affiliated Institute,
Position

Research Enhancement Strategy
Office (Human Resources Planning
Office), Specially Appointed Senior
Specialist

III Organization

135

136

Foreign Visiting Researcher
Name
Richmond, Michael William

2017/4/1

Norman, Colin Arthur

2017/4/2~

2017/5/1

Deliduman, Cemsinan
Deliduman, Yamac

2017/4/2
2017/4/2~~

2017/7/30
2017/7/30

Pipin, Valerii

2017/4/4~

2017/6/29

Tan, Jonathan
Brun, Allan Sacha Rodolphe
Overzier, Roderik Adriaan
Andreani, Paola Michela

2017/4/15
2017/9/14
2017/11/1
2018/1/14~~~~

2017/5/15
2017/12/15
2017/11/30
2018/2/24

III Organization

Period~ 2017/5/30

Affiliated InstituteRochester Institute of Technology (U.S.A.)
Johns Hopkins University, Physics and Astronomy & Space
Telescope Science Institute (U.S.A.)
Mimar Sinan Fine Arts University (Turkey)
Mimar Sinan Fine Arts University (Turkey)
Institute of Solar-Terrestrial Physics, Siberian Branch Russian
Academy of Sciences (Russia)
University of Florida (U.S.A.)
CEA-Saclay (France)
National Observatory, Rio de Janeiro (Brazil)
European Southern Observatory (Germany)7. Advisory Committee for Research and Management
Members
From universities and related institutes
Chiba, Seiji
Graduate School of Science andFaculty of Science, Tohoku
University
Doi, Mamoru

School of Science, The Universityof TokyoFujisawa, Kenta

The Research Institute for Time
Studies at Yamaguchi University

Ichimoto, Kiyoshi

Hida Observatories, Graduate
School of Science, Kyoto
University

Kajita, Takaaki

Institute for Cosmic Ray Research,
The University of Tokyo

Matsushita, Kyoko

Faculty of Science Division1, Tokyo
University of Science

Mitsuda, Kazuhisa

Institute of Space and Astronautical
Science

Murakami, Izumi

National Institute for Fusion
Science○ Momose, Munetake

College of Science, Ibaraki
University

Sugita, Seiji

From NAOJ
Gouda, Naoteru
Hasegawa, Tetsuo
Honma, Mareki
Kobayashi, Hideyuki
Kokubo, Eiichiro
Sakamoto, Seiichi
Takami, Hideki
Tomisaka, Kohji
Usuda, Tomonori● Watanabe, Jun-ichi
Yoshida, Michitoshi

JASMINE Project Office
NAOJ Chile Observatory
Mizusawa VLBI Observatory
Mizusawa VLBI Observatory
Center for Computational
Astrophysics
NAOJ Chile Observatory
Advanced Technology Center
Division of Theoretical Astronomy
TMT-J Project OfficePublic Relations Center
Subaru Telescope● Chairperson ○ Vise-Chairperson
Period: April 1, 2016 – March 31, 2018

School of Science, The Universityof Tokyo

III Organization

1378. Professors Emeriti
Professors Emeriti (NAOJ)
Kakuta, Chuichi
Hiei, Eijiro
Yamashita, Yasumasa
Nishimura, Shiro
Hirayama, Tadashi
Miyamoto, Masanori
Nariai, Kyouji
Okamoto, Isao
Nakano, Takenori
Kodaira, Keiichi
Yokoyama, Koichi
Oe, Masatsugu
Kinoshita, Hiroshi
Nishimura, Tetsuo
Kaifu, Norio
Ishiguro, Masato
Inoue, Makoto
Kawano, Nobuyuki
Andou, Hiroyasu
Karoji, Hiroshi
Chikada, Yoshihiro
Noguchi, Kunio
Fujimoto, Masakatsu
Manabe, Seiji
Miyama, Shoken
Kawaguchi, Noriyuki
Iye, Masanori
Shibasaki, Kiyoto
Sakurai, Takashi
Arimoto, Nobuo
Kobayashi, Yukiyasu
Mizumoto, Yoshihiko138

III Organization

IV Finance
Revenue and Expenses (FY2017)
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

Budget10,175,004
415,990
1,308,800
49,691
333,3620
12,282,847
Budget10,224,695
3,531,387
6,693,308
415,990
1,308,800
333,362
12,282,847
Budget0

Final Account10,685,620
415,972
1,308,800
61,860560,4480
13,032,700
Final Account9,964,054
3,553,345
6,410,709
415,972
1,308,800
367,710
12,056,536
Final Account976,164(Unit: ¥1,000)
Budget − Final Account−510,616
18
0−12,169−227,086
0−749,853
Budget − Final Account
260,641−21,958
282,59918
0−34,348
226,311
Budget − Final Account−976,164

IV Finance139

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2017
Research Categories

Number of Selected Projects

Scientific Research on Innovative Areas(Research in a proposed research area)
Scientific Research (S)Scientific Research (A)Scientific Research (B)Young Scientists (A)Research Activity Start-up
JSPS Research Fellows
JSPS International Research Fellows
Publication of Scientific Research Results
Total

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

Total

8

85,20025,560110,760

1
10
9
3
3
9
1
1
45

15,20083,20028,80020,100
2,800
9,900
800
500
246,500

4,560
24,960
8,640
6,030
840
2,970
0
0
73,56019,760108,160
37,44026,1303,640
12,870800
500
320,060

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding
23,500
7,050
4,600
1,380
19,0005,700
47,10014,130Total
30,5505,980
24,70061,2302. Multi-year Fund for FY 2017
Research Categories

Number of Selected Projects

Scientific Research (C)Challenging Exploratory Research
Young Scientists (B)
Total

24
6
21
51

3. Partial Multi-year Fund for FY 2017140

Research Categories

Number of
Selected Projects

Young Scientists (A)
Total

1
1

Budget (Series of Single-year Grants)(Unit: ¥1,000)
Direct Funding Indirect Funding
Total
100
30
130
100
30
130

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

Budget (Multi-year Fund)(Unit: ¥1,000)
Direct Funding Indirect Funding Total
0
0
0
0
0
0

VI Research Collaboration
1. Open Use
TypeProject/Center

Okayama
AstrophysicalObservatory

Category

Number of
Total
Accepted Number of
Proposals Researchers

188-cm Reflector Telescope (Project Program)
188-cm Reflector Telescope (Normal Program)
188-cm Reflector Telescope (Student Program)
188-cm Reflector Telescope(Miscellaneous Program)
188-cm Reflector Telescope (ToO Program)

Subaru Telescope
Solar Observatory

Nobeyama Radio
Observatory
Open Use at
Project/Center
Mizusawa VLBI
Observatory

Ground-based Solar Observatory
Solar Observing satellite “Hinode”
45-m telescope (Regular Program)
45-m telescope (Short Program)
45-m telescope (Large Program)
45-m telescope (Back-up Program)
45-m telescope (GuaranteedTimeObservations)45-m telescope (Director’s Discretionary Time)
VERA

Astronomy Data Center
Center for Computational Astrophysics
Facility Use
Advanced
Technology Center
Joint Research and Development
NAOJ Chile
Observatory

ALMA (Cycle 4)

*

Notes

2
26
0

33(0)
202(25)

2 Institutes
12 Institutes, 6 Countries

1

6(0)

1 Institute

1
79

10(0)
271(61)

2 Institutes
53 Institutes, 8 Countries*
77(31)
204(88)43(1)158(143)
12(1)
11(0)

*
31Institutes, 11 Countries
48 Institutes, 13 Countries
16 Institutes, 1 Country
70 Institutes, 16 Countries
1 Institute, 1 Country
5 Institutes

77
26
9
1
1
2
0
23

135(70) 28 Institutes, 14 Countries369
369 (24 at foreign 20 Institutes, 13 Countries
institutes)
270
270 59 Institutes, 10 Countries31
140(3)
57 Institutes, 1 Country
15
87(3)34 Institutes, 1 Country
4,857
475
397 Institutes, 42 Countries(4,257)20
149(23) 24 Institutes, 5 Countries
10
9 Institutes
17
6 Institutes
0

ASTE
Joint Development Research
Research Assembly
NAOJ Symposium
The number of foreign researchers shown in brackets ( ) is included in the total.
Notes show the number of institutes and foreign countries represented by the proposal PI’s. The country count does not include Japan.
The period of ALMA (Cycle 4) is September, 2017 from October, 2016.
* The observation data is open to the public on the web. No application is needed to use the data.

VI Research Collaboration

1412. Commissioned Research Fellows
Visiting Scholars (Domestic)
Period: April 1, 2017 – March 31, 2018
Name
Kuno, Nario
Otsubo, Toshimichi
Niinuma, Koutaro
Sagawa, Hideo
Sekine, Yasuhito
Shima, Tatsushi
Yanagisawa,
Toshifumi
Nakagawa, Akiharu

Position at NAOJ
Visiting Professor
Visiting Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor

Affiliated Institute
University of Tsukuba
Hitotsubashi University
Yamaguchi University
Kyoto Sangyo University
The University of Tokyo
Osaka University

Visiting Associate Professor

Japan Aerospace Exploration Agency

Visiting Research Fellow

Kagoshima University

Host Project/Center/Division
Nobeyama Radio Observatory
RISE Project
Mizusawa VLBI Observatory
NAOJ Chile Observatory
RISE Project
Division of Theoretical Astronomy
Center for Computational
Astrophisics
Mizusawa VLBI Observatory

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

Name

Acceptance
PeriodHost Researcher

Arimatsu, Kou

Exploring the outer solar system by stellar occultations
observed with wide-field high-speed cameras

2015.4.1~2018.3.31

Watanabe, Jun-ichi

Shirasaki, Masato

Probing Cosmic Dark Matter and Dark Energy with HigherOrder Statistics of Weak Gravitational Lensing

2015.4.1~2017.8.31

Hamana, Takashi

Shinnaka, Yoshiharu

Physicochemistry of the early solar nebula: Thermal history ofcometary dust and isotopic fractionation of cometary volatile

2015.4.1~2018.3.31

Watanabe, Jun-ichi

Yamauchi, Aya

Research in the structure of a distant region of our galaxy
using a new distance measurement method with VERA

2015.4.1~2018.3.31

Honma, Mareki

Ichikawa, Kohei

Revealing the coevolution of black holes and galaxies throughthe newly discovered population of AGN

2016.4.1~2018.3.31

Imanishi, Masatoshi

Shibagaki, Shota

Revealing origin of r-process elements with astrophysicalsimulations

2017.4.1~2018.3.31

Kajino, Toshitaka

Suzuki, Tomoko

Galaxy anatomy before the peak epoch of galaxy formation:
investigation of internal physical processes and theirenvironmental dependence

2017.4.1~2018.3.31

Kashikawa, Nobunari

Tadaki, Kenichi

Revealing evolutionary pathways from disk- to ellipticalgalaxies with ALMA2017.4.1~2020.3.31

Iono, Daisuke

Kawamuro, Taiki

Constraints on Supermassive Black Hole Growth Rates with
Observations at Submm/mm Wavelengths, and Investigationof the Growth History

2017.4.1~2020.3.31

Imanishi, Masatoshi

JSPS (Japan Society for the Promotion of Science) Foreign Research Fellows
Name
Cataldi, Gianni
Wu, Benjamin
Pattle, Katherine Miranda
Lopez Rodriguez, Enrique142

VI Research Collaboration

Period2016/11/21 ~ 2018/11/20
2016/9/27 ~ 2017/9/26
2017/8/21 ~ 2017/10/20
2018/3/19 ~ 2018/4/18

Host Researcher
Ohashi, Nagayoshi
Nakamura, Fumitaka
Hasegawa, Tetsuo
Kashikawa, Nobunari

VII Graduate Course 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 the 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 students since FY 2006
for the Department of Astronomical Science at the School ofPhysical Sciences. (The School of Mathematical and PhysicalSciences was reorganized into the School of Physical Sciencesin April 2004.)(1) Objective of the Department of Astronomical Science
The Department of Astronomical Science aims to train
students, through observational, theoretical, or instrument
development research in astronomy or in related fields, in anenvironment with the most advanced observational instruments
and supercomputers, as 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 annually:
Two (for the five-year doctoral course)
Three (for the three-year doctoral course)
Degree: Doctor of Philosophy(2) Admission Policy
The Department of Astronomical Sciences seeks students
with a strong interest in astronomy and the Universe; apassion for unraveling scientific questions through theoretical,
observational, and instrument development research; andstudents who have not only basic academic skills, but also
theoretical and creative aptitude required for advanced research.

(3) Department Details (Course Offerings)
Optical and Near Infrared Astronomy[Educational and Research Guidance Field]
Ground-based astronomy / Optical and infrared telescope
system / Planets / Sun, stars and interstellar matter /Galaxies and cosmology
Radio Astronomy[Educational and Research Guidance Field]
Ground-based astronomy / Radio telescope system / Sun,stars and interstellar matter / Galaxies
General Astronomy and Astrophysics[Educational and Research Guidance Field]
High-precision astronomical measurement / Astronomy
from space / Data analysis and numerical simulation /Earth, Planets, and the Sun / Galaxies and cosmology(4) Course-by-Course Education Program to Cultivate
Researchers in Physical Sciences with Broad Perspectives
The School of Physical Sciences began its “Course-byCourse Education Program to Develop Student Research
Capability and Aptitude” in FY 2009 as a part of MEXT’s
Program for “Enhancing Systematic Education in Graduate
Schools.” Currently the School is carrying out its succeeding
program, “Course-by-Course Education Program to Cultivate
Researchers in Physical Sciences with Broad Perspectives”
since FY 2012, offering four specific courses to the students:
the Basic Course, the Advanced Research Course, the Project
Research Course, and the Development Research Course. In
FY 2017, from the Department of Astronomical Science four
students were accepted in the Basic Course and two students in
the Advanced Research Course. The Department also offered thee-learning class “Introduction to Observational Astronomy II” asa school-wide common basic subject, as well as the “Exercise in
Scientific English” class, in order to provide a good foundation
for students at the graduate school.
The 2017 Summer Student programs were held at
Mitaka, Mizusawa, Kamioka, and Chili Campuses to allow
undergraduate students a chance to experience research at
the Department of Astronomical Science. In addition to theexisting Research Assistant system, the Department also
provided Associate Researcher positions for the students of the
Department of Astronomical Science.

VII Graduate Course Education

143

(5) Number of Affiliated Staff (2018/3/31)
Chair of the Department of Astronomical Science
Optical and Near Infrared Astronomy Course
Professors
Associate Professors
Lecturer
Assistant Professors
Radio Astronomy Course
Professors
Associate Professors
Assistant Professors
General Astronomy and Astrophysics Course
Professors
Associate Professors
Assistant Professors
Total

1
9
14
1
16
8
11
18
5
14
14
111

(6) Graduate Students (33 students)

144

1st year (5 students)
Name
Liang, Yongming

Principal Supervisor
Supervisor
Kashikawa, Nobunari Tanaka, Masayuki

Ito, Kei

Kashikawa, Nobunari Matsuda, Yuichi

Tsukui, Takashi

Iguchi, Satoru

Nagai, Hiroshi

Study on the Radio galaxy formation with Supermassive Black
Hole

Tsuda, Shuichiro

Honma, Mareki

Shibata, Katsunori

Measuring the Physical Properties near the Super-Massive
Black Holes with the Event Horizon Telescope

Namiki, Shigeru

Kashikawa, Nobunari Iwata, Ikuru

2nd year (5 students)
Name

Principal Supervisor

Ishikawa, Hiroyuki

Usuda, Tomonori

Hayashi, Saeko

Tanioka, Satoshi

Aso, Yoichi

Flaminio, Raffaele

Direct measurement of the coating thermal noise using
cryogenic optical cavities

Hatta, Yoshiki

Sekii, Takashi

Watanabe, Tetsuya
Katsukawa, Yukio

Asteroseismic measurements of internal rotation of stars via
solving inverse problems

Hosokawa, Kou

Kotani, Takayuki

Takami, Hideki
Usuda, Tomonori

Development of a new high-resolution spectrograph with aspatial resolution and study of an exoplanet characterization

Watanabe, Noriharu

Usuda, Tomonori

Takami, Hideki
Aoki, Wako

Observational Studies of Orbital Evolution of Various
Exoplanets System

3rd year (9 students)
Name

Principal Supervisor

Cui, Yuzhu

Honma, Mareki

Nagai, Hiroshi

Sahoo, Ananya

Minowa, Yosuke

Takato, Naruhisa

Zhao, Yuhang

Akutsu, Tomotada

Flaminio, Raffaele

Fukagawa, Nao

Aoki, Wako

Iono, Daisuke

VII Graduate Course Education

Supervisor

Supervisor

Title of Research Project
Mapping the most massive large-scale structures through HI
The study of protoclusters based on wide-imaging observationsof Subaru Telescope

The evolution of galaxies in the cluster at z~1.5 and theenvironmental effect there

Title of Research Project
The search and inspection of extrasolar habitable planets with aview to the discovery of the extraterrestrial life in the future

Title of Research Project
Observational study of jets in active galactic nuclei with theEast Asian VLBI Network
Advanced wavefront control in adaptive optics for exoplanet
imaging
Frequency dependent squeezing for gravitational wave detector
Star formation and gas flows of the distant galaxies as revealed
by chemical evolution

Ando, Misaki

Iono, Daisuke

Kambara, Nagaaki
Kikuta, Satoshi

Sekii, Takashi
Imanishi, Masatoshi

Saito, Masao
Espada, Daniel
Watanabe, Tetsuya
Matsuda, Yuichi

Matsuno, Tadafumi

Aoki, Wako

Komiyama, Yutaka

Yoshida, Masaki

Suematsu, Yoshinori Hara, Hirohisa

4th year (3 students)
Name

Principal Supervisor

Kim, Jungha

Honma, Mareki

Supervisor

Shibata, Katsunori

Observing Colliding Galaxies Using ALMA
Local helioseismology
AGN feedback to low-mass galaxy formation at high redshift
Pioneering stellar research to clarify the formation history of
the Galactic halo
Study of Solar Chromospheric Dynamic Phenomena bySpectro-polarimetric Observations

Title of Research Project
Understanding the circumstellar structure of high-mass youngstellar objects based on KaVA observations
Observing Starburst Galaxies Using ALMA
Search for distant clusters of galaxies with Subaru HSC andevolution of galaxy populations

Michiyama, Tomonari Iono, Daisuke

Nakanishi, Koichiro

Yamamoto, Moegi

Iwata, Ikuru

Koyama, Yusei

5th year (11 students)
Name

Principal Supervisor

Okutomi, Koki

Aso, Yoichi

Onoue, Masafusa

Kashikawa, Nobunari Miyazaki, Satoshi

Exploration of Low-luminosity Quasars and the Growth ofSuper Massive Black Holes in the Reionization EpochBaba, Haruka

Aoki, Wako

Usuda, Tomonori

Development of infrared instrument and observational study forthe survey of Earth-like planets

Ryu, Tsuguru

Hayashi, Saeko

Usuda, Tomonori

High-Contrast Imaging for Intermediate-Mass Giants with
Long-Term Radial Velocity Trends

Yang, Yi

Hayashi, Saeko

Usuda, Tomonori

Direct Imaging of Planets and Protoplanetary Disks in Binary
Systems

Sakurai, Junya

Miyazaki, Satoshi

Komiyama, Yutaka

Study of large scale structures in the universe through wide
field imaging

Supervisor

Flaminio, Raffaele

Title of Research Project
Development of low-frequency vibration isolation system fortest masses in gravitational-wave telescope KAGRA

Uchiyama, Hisakazu Kashikawa, Nobunari Matsuda, Yuichi

The study of the large scale structure based on wide-fieldimaging observation of Subaru Telescope

Taniguchi, Kotomi

Saito, Masao

Ohishi, Masatoshi

Chemical evolution and mechanisms of carbon-chain moleculesin star-forming regions

Kobayashi, Hiroshi

Ohsuga, Ken

Tomisaka, Kohji

Pathak, Prashant

Takami, Hideki

Minowa, Yosuke

Sukom, Amnart

Tomisaka, Kohji

Hayashi, Saeko

Radiation Hydrodynamics Simulations of Clumpy Outflows
from Black-Hole Accretion Disks
Chromaticity effects on high resolution imaging
Study of star and planetary formation process and theexoplanets based on infrared observations

VII Graduate Course Education1452. Education and Research Collaboration with Graduate Schools

146

Name
Guo, Kangrou
Lee, Sujin
Ishiduka, Noriyoshi
Kashiwada, Yuuki
Kuroki, Shunshi

Affiliated Institute
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo

Supervisor
Kokubo, Eiichiro
Kobayashi, Hideyuki
Hara, Hirohisa
Gouda, Naoteru
Flaminio, Raffaele

Sato, Kazuki

The University of Tokyo Sakamoto, Seiichi

Tanimoto, Yuta
Chin, Kah Wuy
Terasawa, Shoko
Luo, Yudong
Inooka, Kota
Choi, Insa
Shimizu, Takayuki
Tatsuuma, Misako
Mori, Kanji
Yamaguchi,
Masayuki

The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo
The University of Tokyo

Sasaki, Hirokazu

The University of Tokyo Kajino, Toshitaka

Study the origin of heavy elements through the collective
neutrino oscillations in core-collapse supernovae

Fujii, Yoshinori

The University of Tokyo Flaminio, Raffaele

Development of the vibration isolation system for the
KAmioka Gravitational-wave Antenna

Fujita, Ayato

The University of Tokyo Gouda, Naoteru

Analysis of the solar motion and the Galaxy’s rotationconsidering orbital resonance

Kuramochi, Kazuki

The University of Tokyo Kobayashi, Hideyuki

Observational demonstration of RIAF with sub-mm VLBI
using Sparse Modeling

Lee, Minju

The University of Tokyo Kawabe, Ryohei

Environmental effect on galaxy evolution using atomic andmolecular lines

Kato, Yuta

The University of Tokyo Sakamoto, Seiichi

Star forming activity in the z=2–3 proto-clusters with Infrared
Space telescope

Sakai, Daisuke

The University of Tokyo Kobayashi, Hideyuki

Shibata, Takashi

The University of Tokyo Kokubo, Eiichiro

Hirai, Yutaka

The University of Tokyo Kajino, Toshitaka

Marchio, Manuel

The University of Tokyo Flaminio, Raffaele

Yamashita, Takuya
Kawabe, Ryohei
Ohashi, Nagayoshi
Kajino, Toshitaka
Yamashita, Takuya
Ohashi, Nagayoshi
Sekimoto, Yutaro
Kokubo, Eiichiro
Kajino, Toshitaka

The University of Tokyo Kawabe, Ryohei

VII Graduate Course Education

Title of Research Project
Formation and evolution of planetary systems
Study of highly precise astronomy by using VLBI
Study of Fine Structures in Superhot Components of Solar Flare
Analysis of the dynamical structure of the Galaxy
Development of vibration isolation system for the KAGRA
Observational Study of Star/Planetary System Formation with
Radio Telescopes
Observational studies of exoplanets
Developments of Ultra-Wideband Spectrometers using KIDs
A study on star formation using radio interferometers
Big Bang Nucleosynthesis and Big Bang Model
Observational studies of rapidly variable objects
A study on the protostar L1489 IRS using radio interferometers
Design of Wide Field CMB Polarization Instruments
Planetary formation
Nucleosynthesis in X-ray bursts
Super Resolution Imaging of Protoplanetary disk Using
Sparse Modeling

Dynamical study of molecular clouds in the Galactic centerwith radio observations
Spin of planets
Chemo-dynamical evolution of galaxies deduced fromr-process elements
Development, characterization and improvement of themirrors for the KAGRA gravitational wave detector

3. Commissioned Graduate Students
Doctoral Course

Affiliated Institute

PeriodSupervisor

Title of Research Project

Kozuki, Yuto

Osaka Prefecture
University

2017/4/1~
2018/3/31

Noguchi, Takashi

Research and development of a superconducting
wideband receiver at millimeter and submillimeter
wavelengths

Silva, Andrea

Tufts University

2017/4/1~
2017/12/31

Iono, Daisuke

ALMA Observations of Starburst Galaxies

Kumamoto, Jun

Tohoku University

2017/4/1~
2018/3/31

Gouda, Naoteru

Theoretical Prediction for the Milky Way
Evolution Using Galactic Dynamics

Master’s Course

Affiliated InstituteJapan Women's
University

Period2017/4/1~
2017/9/30

Supervisor
Nakamura,
Fumitaka

Title of Research Project
Observational Study of Orion Molecular Cloudwith a dense gas tracer

Kooriba, Motohiro

Tokyo Universityof Agriculture andTechnology

2017/4/1~
2018/3/31

Watanabe, Junichi

Generation of wavelength-variable broadband
comb and its application to precision spectroscopy

Suzuki, Shunta

Osaka Prefecture
University

2017/4/1~
2018/3/31

Kawabe, Ryohei

Multicolor TES Bolometer Camera for the ASTE
TelescopeMorozumi,
Tatsuhiko

The University of Tokyo

2017/4/1~
2017/9/30

Aso, Yoichi

Development of Beam Reducing Telescope

Sakata, Misaki

The University ofElectro-Communications

2017/10/1~
2018/3/31

Matsuo, Hiroshi

Development of THz photon counting technologies
with superconducting tunnel junction detectors

Tomura, Akihiro

The University ofElectro-Communications

2017/10/1~
2018/3/31

Development of treaquency-dependent squeezing
Flaminio, Raffaele for quantum noise reduction in the gravitational
wave defector

Miyachi, Yusuke

Yamaguchi University

2017/10/1~
2018/3/31

Honma, Mareki

Comparing study between high precision
astrometry results with VERA and a simulation
result based on the density wave theory

Mochizuki, Chisato

Japan Women's
University

2017/10/1~
2018/3/31

Kashikawa,Nobunari

The Properties of Ultra Diffuse Galaxies exploredby Subaru Telescope

Yatabe, Kazuki

The University ofElectro-Communications

2017/10/1~
2018/3/31

Hayano, Yutaka

Experiment and evaluation for TMT/IRIS
prototype.

Oyamada, Shuri

4. Degrees Achieved with NAOJ Facilities
Name

DegreeTitle of Research ProjectFirst On-sky Closed-loop Atmospheric Dispersion Compensation:
Demonstration of Sub-milliarcsecond Residual Dispersion AcrossH-bandPathak, Prashant

Doctor of Philosophy, SOKENDAI

Yang, Yi

Doctor of Philosophy, SOKENDAI

Onoue, Masafusa

Doctor of Philosophy, SOKENDAI

Kobayashi, Hiroshi

Doctor of Philosophy, SOKENDAI

Three-Dimensional Radiation-Hydrodynamic Simulation of Clumpy
Outflow and Its Application to Supercritical Accretors around Black
Holes

Taniguchi, Kotomi

Doctor of Philosophy, SOKENDAIFormation Mechanisms of Cyanopolyynes and Chemical Evolution in
the High-Mass Star-Forming Regions

Near-Infrared High-Resolution Polarimetry Observations towards
Protoplanetary Disks in Binary/Multiple Systems
Exploration of the Cosmic Dawn with High-Redshift Quasars

VII Graduate Course Education

147

VIII Public Access to Facilities
1. Mitaka Campus

2. Mizusawa Campus[Open year-round]
Dates: April to March, 10:00–17:00
Every day except for New Year’s season (December
28–January 4)
Visitors: 21,310
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[Open year-round]
Dates: April to March (except for the New Year’s season),
9:00–17:00 daily
Visitors: 19,389
Open Facilities: Kimura Hisashi Memorial Museum, VERA
20-m antenna, 10-m VLBI antenna[Regular Star Gazing Party]
Dates: Friday before second Saturday; fourth Saturday
Visitors: 4,772 (23 events)
Open Facility: 50-cm Telescope for Public Outreach[4D2U Theater Showings]
Dates: Friday before second Saturday; first, second, andthird Saturdays
Visitors: 5,097 (45 events)
Open Facility: 4D2U Dome Theater[Special Open-House Event] Mitaka Open House Day
Dates: October 13 (Fri), 2017, 14:00–19:00
October 14 (Sat), 2017, 10:00–19:00
Topic: The Universe, Hot and Cold
Visitors: 3,269
This event is jointly sponsored by NAOJ, the Universityof Tokyo Graduate School of Science Institute of Astronomy,
the SOKENDAI Department of Astronomical Science, and the
NINS Astrobiology Center. It has been held for 2 days each year,
starting from 2010.
The perennially popular lectures related to this year’s
theme were hosted by the Institute of Astronomy, University ofTokyo (“The WARM Universe Observed from Atacama, Chile”
Takashi Miyata, Professor) and NAOJ (“ALMA Gazing at theCold Universe” Tetsuo Hasegawa, NAOJ Specially Appointed
Professor; and “Hot Solar Corona as Seen from Space” Ryohei
Kano, NAOJ Associate Professor).
* Guided tours corresponding to group tours (Dantai Kengaku)
and cultural property tours were also held. In addition, the“Information Space of Astronomy and Science” was openedin 2015 near the south entrance of Mitaka Station to distributeinformation.

148

VIII Public Access to Facilities

The open house event is held at the campus with thecooperation of the Oshu Space and Astronomy Museum (OSAM:
Yugakukan) located in the campus.
[Special Open Day] Held as part of Iwate Galaxy Festival 2017
(Hours: 10:00-20:30)
Date: August 19 (Sat.), 2017, 10:00–20:30
Visitors: Approximately 1,165 (Until 16:30)
Same as last year, the Open Day was co-hosted with
Ihatov Space Action Center / the Oshu Space and Astronomy
Museum (OSAM: Yugakukan) and the city of Oshu. The event
was opened with a performance by a marching band from a
local elementary school. NAOJ offered such attractions as
exhibits about the research results of VERA, RISE, and CfCA;
tours of the 20-m parabolic antenna; a commemorative photobooth; plastic bottle rocket launching; quiz game; tours of thesupercomputer “ATERUI;” and a special guided tour of theArray Operations Center (AOC) and the VLBI correlator.
Special lectures about black holes were given by Motohide
Tamura, Professor of University of Tokyo, Mareki Honma,
Director of the Mizusawa VLBI Observatory, and Noriyuki
Namiki, Professor of the RISE Project, and were enormously
well received.
OSAM (Yugakukan) offered various experiments in thescience stalls, workshops, etc., which were carried out by
student interns. The Open Day was a great success to strengthenties with the local people.
Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for the New Year’s season)
Visitors: 1,602[Special Open Day]
Date: August 12 (Sat.), 2017, 12:00–21:00
Visitors: 3,800
This special open event was held in conjunction with
“Yaeyama Highland Star Festival 2017” hosted by the executive
committee primarily formed by members of Satsuma-Sendai
city hall and Kagoshima University.
At the NAOJ VERA 20-m radio telescope and theKagoshima University 1-m optical/infrared telescope facilities,guided tours of the telescopes and observation building
were held. NAOJ offered such attractions as parent-childscience experiments, plastic bottle rocket launching, 4D2U
(4-Dimentional Digital Universe) screening, and a stargazing
party at night. This time samples of space foods were offered by
JAXA, and were well received.
The special lecture of the year was given by Osamu
Kameya, Assistant Professor, from Mizusawa VLBI
Observatory. All visitors had fun and were satisfied with
scientific programs offered in this festival.
Ogasawara: VERA Ogasawara Station[Open year-round]
Dates: April to March (except for the New Year’s season)
Visitors: 8,340[Special Open Day]
Date: January 20 (Sat.), 2018, 10:00–16:00
Visitors: 167
A special open house event was held this year again under
the name “Star Island 17.” Same as last year, the free shuttle
buses were appreciated by the visitors. The number of visitors
was 167. (Because the number of residents in the island is about
2,000, approximately 10 % of the islanders visited this event.)
NAOJ offered such attractions as exhibits about the research
results of VERA and RISE, driving experience of the 20-m
parabolic antenna, quiz games, a commemorative photo booth,and short lectures.
On the night before the special open house, a Space Lecture
was given by Saeko Hayashi, Associate Professor, at the
Ogasawara Visitor Center, and was attended by 30 people.
A stargazing party was held by the local Ogasawara
astronomy club on the day following the special open house, and
NAOJ members also joined.
Ishigakijima: VERA Ishigakijima Station[Open year-round]
Dates: April to March (except for the New Year’s season);premises are open to the public 24 hours/day, andthe observation rooms are open during the hours of
10:00–16:30
Visitors: 2,577

Ishigakijima: Ishigakijima Astronomical Observatory[Open year-round]
Dates: April to MarchOpen Hours: Wednesdays through Sundays (Except for
the New Year’s season; when Monday is a national
holiday, it is opened and closed on the following
Tuesday/Wednesday), 10:00–17:00
Stargazing Sessions: Evenings on Saturdays, Sundays,
Holidays, (20:00–22:00), two 30-minute sessions per
evening
4D2U Screenings: from 15:00 to 15:30 every day when the
Observatory is open
Visitors: 14,192 (1,043 during the Southern Island Star
Festival)
Open Facilities: Murikabushi 105-cm optical/infrared
telescope, Hoshizora Manabi no Heya (Starry Sky
Study Room) (featuring the 4D2U “four dimensional
digital universe"), interior of observation dome
(including exhibits of astronomical images)
The “Hoshizora Manabi no Heya” (Starry Sky Study Room),
constructed adjacent to the observatory in 2013 by the city ofIshigaki, was very popular, welcoming 4,478 guests.
[Southern Island Star Festival 2017]
Dates: August 12 (Sat.) to August 20 (Sun.), 2017
Visitors: 11,337
This year is the 16th anniversary of both the completionof VERA Ishigakijima Station and the Southern Island Star
Festival. Approximately 9,000 visitors attended the dimmedlight stargazing event blessed with finer weather than everbefore. The annual planetarium screening was attended by 581.
The activities at Ishigakijima Astronomical Observatory
boost regional programs like school education, lifelong learning,and sightseeing. The cooperation agreement between NAOJ
and the Tourism Association of the city of Ishigaki has been
finalized. And it is widely recognized that the starry sky can beused as a tourism resource. Considering this situation, we willcontinue to strengthen our ties with other associations.

[Special Open day]
Date: August 13 (Sun.), 2017, 10:00-17:00
Visitors: 273
The Special Open Day was held as a part of the Southern
Island Star Festival.
Same as previous years, attractions like antenna tours, acommemorative photo booth, merchandise, commemorative
lectures, and exhibits were offered.

VIII Public Access to Facilities

1493. Nobeyama Campus[Regular Open]
Open Time: 8:30–17:00 (every day except around New
Year’s Day (Dec. 29 to Jan. 3), open until 18:00
during the summer (Jul. 20 to Aug. 31))
Visitors: 42,760Open Facilities: 45-m Radio Telescope, Nobeyama Millimeter
Array, Nobeyama Radioheliograph, etc. (just viewing)
and NINS Nobeyama Exhibition Room[Open House Day]
Date: August 26 (Sat.), 2017, 9:30–16:00
Visitors: 2,093
The theme of the 2017 Open House Day was “Nagano
Prefecture is the Astro-Prefecture ~Starry sky in Shinshu is apromenade to the Universe.” We had two lectures on the theme,
which attract large audiences every year. One was “Nagano
Prefecture, which can be felt to be close to the Universe” by
Prof. Ohnishi, Kouji (National Institute of Technology, Nagano
Collage). The other was “The radio luminous Milky Way – theGalactic plane survey by the Nobeyama 45-m Radio Telescope”
by Dr. Umemoto, Tomofumi (NAOJ).
Even though it rained in the early morning, the weather was
getting better at the opening time, and we were blessed withgood weather as a whole. However, we had 2,093 visitors, which
was less than in a normal year because the weather forecast was
not so good. We had some established hands-on events suchas touch the main reflector panel of the 45-m Radio Telescope,
antenna handicrafts, radio detector handicrafts, and antennaorigami. At the NINS Exhibition Room, the presentation of the
4D theater and exhibitions of other institutes were carried out.
In addition, the ALMA team presented the ALMA VR systemand some short lectures. Moreover, we had a welcome greetingby the NRO character, Dr. Nobeyama and “Nagano Prefectureis the Astro-Prefecture” stamp-rally event. The Open House
day was filled with events because we were supported by many
people from the local people and Shinshu University, Faculty ofAgriculture as well as NAOJ and other institutes of NINS.
[Jimoto Kansha Day (Thanks Day for the locals)]Date: December 9 (Sat.), 2017, 13:00–18:30
Visitors: 55
The local people have difficulty participating in the OpenHouse Day during the farming season. They have said thatthey do not know much about what we, not only NRO but also
Tsukuba and Shinshu Universities, study in Nobeyama.
In order to respond to these comments, we establishedthis event in cooperation with Shinshu University, Faculty ofAgriculture, Education and Research Center of Alpine Field
Science and Tsukuba University, Agricultural and Forestry
Research Center, Yatsugatake Forest. This year, the Jimoto
Kansha Day was hosted by NRO at the NINS Nobeyama
Exhibition Room, which opened to the public in April 2017.

150

VIII Public Access to Facilities

We had many events such as a tour of NRO facilities, thelectures from each institute, 4D theater, and star gazing party.
The lectures were “On the biological research of the Japanese
dormouse” from Tsukuba University, “Will you take notice of
the available nitrogen for sustainable agriculture?” from Shinshu
University, and “The Milky Way observed by the Nobeyama
45-m Radio Telescope” from NRO. There was another event thesame day in Minamimaki Villiage, so the number of participants
was somewhat less than when NRO had hosted it before in
2014. The festival had a friendly atmosphere with the parents
and children braving the cold to stay until the star gazing party.

4. Okayama Campus

5. Subaru Telescope

Okayama Astrophysical Observatory[Open year-round]
Dates: 9:00–16:30 daily
Visitors: 5,980 (Period: April 1–October 4)Open Facilities: Window view of Okayama 188-cm
Reflector Telescope[Summit Facility Tour]
Dates open for public tour: 41 (these dates are listed in the
public tour program page at the Subaru Telescope’s
web site. Among the 41 days, 10 tour days werecancelled due to the windscreen incident. No tours
scheduled during the winter months of October toMarch)
Public Tour Visitors: 307
Special Tour Visitors: 67 groups, 370 visitors[Special Stargazing Party]
Date: August 11 (Fri.), 2017, 18:30–22:25
Visitors: 81
198 applications for 548 applicants were received. M13 andSaturn were viewed.

[Base Facility Tour]Special Tour Visitors: 23 groups, 252 visitors[Public information]○ Primary means of public information is posting at the official
website https://subarutelescope.org• Science results from the Subaru Telescope – 6 Japaneseand 6 English article• Depicting special activities or making announcements
on Calls for Proposals, recruitment, etc. – 24 Japaneseand 19 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 at the Subaru Telescope’s base facility in Hilo: 18
cases, reached 579 people
2. Remote presentations, mainly to Japan: 10 cases, reached 546
people3. Lectures, demonstrations, workshops, etc. in the vicinity: 66
cases, reached 1,578 people
4. Lectures in Japan: 31 cases, reached 1,978 people
5. Others - Exhibits etc.: 13 cases, reached approximately 6,065
people
6. Media coverage: 22 Japanese media. 10 English media.

VIII Public Access to Facilities151

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

category

Business Trip

South Korea
46
China
19
Thailand10
Taiwan33
Hong Kong
2
Singapore
2
Indonesia
0Philippines
0
Other areas in Asia
16
Hawai`i
65
U.S.A.
116
Australia
11
Italy
15
U.K.
10
France17
Canada7
Guam, Saipan
1Germany
39
Other areas in Europe and Oceania
37
Mexico5
Brazil0Africa6
Other areas in South and Central America *
39
Total
496
* Most travelers to South and Central America went to Chile.

152

IX Overseas Travel

Training

Total

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

46
19
10
33
2
2
0
0
16
65
116
11
15
10
17
7
1
39
37
5
0
6
39
496

X Award Winners
Award Recipients
Kajino, Toshitaka

Affiliated Division
Division of Theoretical
Astronomy

Associate Professor

Award
One Thousand Talents Plan: Foreign
ExpertsDate
2017/4/15

Professor/Professor/
Assistant Professor

FY2017 The Commendation for Scienceand Technology by the Minister of
Education, Culture, Sports, Scienceand Technology, Prizes for Science andTechnology ( Research Category)

2017/4/19

NAOJ

Professor Emeritus

The Order of the Sacred Treasure, Goldand Silver Star

2017/5/9

Solar Science
Observatory

Assistant Professor

The 6th NINS Young Researcher's Prize

2017/6/11--

IEEE Milestone

2017/6/14

Honma, Mareki
Kobayashi, Hideyuki
Hirota, Tomoya

Mizusawa VLBI
Observatory

Kodaira, Keiichi
Katsukawa, Yukio
Nobeyama 45-m Radio
Telescope
ALMA

Job Title--

Categoría Especial, Premio ICARE 20172017/9/11

NAOJ (ALMA,
Nobeyama 45-m Radio
Telescope, VERA, and
GRAPE)--IEICE Milestone

2017/9/15

Akiyama, Eiji

NAOJ Chile
Observatory

Specially Appointed
Assistant Professor“Best Researcher 2016” from the Japanese
2017/9/28
Society for Planetary Sciences

Gonzalez Garcia,
AlvaroNAOJ Chile
Observatory

Assistant Professor

IEEE RADIO 2017 Young Scientist
Award

2017/9/28

Kashikawa, Nobunari

TMT-J Project Office

Associate Professor

Award for excellent reviewers, FY2017
KAKENHI2017/9/29

Tanaka, Masaomi

Division of Theoretical
Astronomy

Assistant Professor

NCU-DELTA Young Astronomer
Lectureship Award

2017/10/18

Toriumi, Shin

Division of Solar andPlasma Astrophysics

Specially Appointed
Assistant Professor

2017 APSPM Young Scientist Best
Presentation Award

2017/11/10

Nakayama, Hirotaka/Baba, Junichi 4D2U
Project

Center for Computational Research Expert/
Astrophysics/JASMINE Specially Appointed
Project Office/ Research Staff/ -the Grand Prix for the VR Category of the
Lumiere Japan Awards 20172017/11/15

Kajino, Toshitaka

Division of Theoretical
Astronomy

State Specially Recruited Expert

2018/1/1

Nakayama, Hirotaka/Baba, Junichi 4D2U
Project
Kosugi, George
Nakazato, Takeshi
Sugimoto, Kanako

Nagai, Hiroshi
Nakanishi, Koichiro
Kameno, Seiji
Charles L. H. Hull

Associate Professor

Center for Computational Research Expert/
Astrophysics/JASMINE Specially Appointed
Project Office/ Research Staff/ Associate Professor/
NAOJ Chile
Research Engineer/
Observatory
Specially Appointed
Senior Specialist

NAOJ Chile
Observatory

Specially Appointed
Associate Professor/
Specially Appointed
Associate Professor/
Professor/Specially
Appointed AssistantProfessor“Best VR Science Experience” at the 20182018/2/12
Lumiere Awards

2017 NAOJ Director General Prize

2018/3/2

2017 NAOJ Director General Prize

2018/3/2

X Award Winners

153

154

Saigou, Kazuya
Ohashi, Nagayoshi
Akiyama, Eiji
Fujiwara, Hideaki

Chile Observatory/
Subaru Telescope/
Chile Observatory/
Subaru Telescope

Specially
Appointed AssistantProfessor/Professor/
Specially Appointed
Assistant Professor/
RCUH

2017 PASJ Excellent Paper Award

2018/3/15

Kano, Ryohei

SOLAR-C Project
OfficeAssociate Professor

The 4th ISAS Award (FY 2017)2018/3/22

X Award Winners

XI Library, Publications
1. Library
Number of books in each library (2018/3/31)
Japanese Books
Mitaka17,574
Okayama62
Nobeyama
1,225
Mizusawa
4,979
Hawai`i
1,660
Total
25,500Foreign Books
45,9291,006
6,294
18,1004,623
75,952

Total
63,503
1,068
7,519
23,0796,283
101,452

Number of journal titles in each library (2018/3/31)
Japanese Journals
Foreign Journals
Mitaka360
1,677
Okayama08Nobeyama
16
82
Mizusawa
659
828
Hawai`i
15
15
Total
1,050
2,610

Total
2,037
8
98
1,487
30
3,660

2. Publication
Here we list continuing publications produced by NAOJ in FY2017.
(Mitaka)01) Report of the National Astronomical Observatory of Japan, Vol. 19: 1 issue02) Annual Report of the National Astronomical Observatory of Japan (in Japanese), No. 29, Fiscal Year 2016: 1 issue03) Annual Report of the National Astronomical Observatory of Japan (in English), Vol. 19 Fiscal Year 2016: 1 issue04) National Astronomical Observatory Reprint, No. 2886–3026; 141 issues05) Calendar and Ephemeris, 2018; 1 issue06) NAOJ News, No. 285–293; 12 issues07) Guide to the National Astronomical Observatory of Japan pamphlet (Japanese); 1 issue08) Guide to the National Astronomical Observatory of Japan pamphlet (English); 1 issue09) Rikanenpyo (Chronological Scientific Tables), 2018; 1 issue10) Publication of the National Astronomical Observatory of Japan Vol. 14

XI Library, Publications

155

XII Important Dates
April 1, 2017 – March 31, 20182017
April 16

Eighth Open Observatory event held at the Ibaraki University Center for Astronomy and the NAOJ Mizusawa
VLBI Observatory Ibaraki Station, with 500 visitors in attendance.

April 20

The ALMA Observatory issued the ALMA Cycle 5 call for proposals for scientific observations which start from
October 2017 and received by the deadline a total of 1661 observation proposals from astronomers around the world.

April 25

As part of a continuing education program for staff, Subaru Telescope held “Subaru Makali’i Seminar” to learn
Hawaiian culture, language, and history with lectures from experts in the field. Three seminars were held in 2017 on
April 25, May 24, and December 6 and the Subaru staff learned Polynesian navigation and Hawaiian perspectives.

April 27~
July 2

An exhibit “ALMA Explores the Dark Universe” held at the Information Space of Astronomy and Science.

April 29
May 6
June 5~9
June 11
June 14

The presentation ceremony of the IEEE milestone plaque for the Nobeyama 45-m Radio Telescope, the following
commemorative party, and lectures were held at Josui-Kaikan in Tokyo. There were about 110 participants invitedfor the ceremonies.

June 16

The unveiling ceremony of the IEEE milestone plaque and pedestal for the Nobeyama 45-m Radio Telescope was held
in Nobeyama Radio Observatory. We had about 20 invited participants including the mayor of Minamimaki Village.

June 25

Prof. Takaaki Kajita, Director of the Institute for Cosmic Ray Research, the University of Tokyo visited the ALMA
Array Operations Site.

July 6

Seiichi Sakamoto, the director of NAOJ Chile Observatory gave a lecture as a Tanabata event at the Japanese Schoolin Santiago.

July 7

Subaru Telescope held the annual Tanabata Star Festival together with the Japanese Chamber of Commerce andIndustry of Hawai`i to deepen cultural exchanges and promote astronomy.

July 7~
September 17

An exhibit “The Universe Seen over Nobeyama” held at the Information Space of Astronomy and Science.

July 16

The Star Festival held using the 6-m antenna at the NAOJ Mizusawa VLBI Observatory Kagoshima station in
Kagoshima City Kinko Bay Park, co-hosted with Kagoshima City and Kagoshima University, with approximately
350 visitors in attendance.

July 24~28
July 25
July 29
July 31~
August 1

156

The opening ceremony of NINS Nobeyama Exhibition Room and the press conference with the President of NINS
were held in Nobeyama Campus. There were about 30 participants including some journalists and writers.
Subaru Telescope staff interacted with the public during the AstroDay event in a shopping mall in Hilo.
Observation training of Radio Astronomy at Nobeyama Radio Observatory for Undergraduate Students was
performed; there were 12 participants.
A lecture “ALMA Deepens the Mysteries of the Universe” held at the Information Space of Astronomy and Science.

Facility Guide Week for Educational Organizations was carried out at Nobeyama Radio Observatory.
“The 24th NAOJ Lecture for the Science Media” held at Hitotsubashi Hall with 19 reporters (8 companies) inattendance.
Mr. Yoshinobu Hiraishi, the Ambassador of Japan to Chile visited the ALMA Array Operations Site.
“Astronomy Classes for Kids in Summer 2017” held in Mitaka Campus.

August 4~6

Eleventh Z-star Research Team event held for high school students in the six Tohoku prefectures, with 12 participants
attending. The 12 participants were divided into two groups of A and B for observations using the VERA 20-m radio
telescope and data analysis. The A squad detected 1 heavenly body (G037.419+01.513) for the first time in 23 years,
and unfortunately the B squad was not able to detect meaningful water maser radio waves, but detected 1 heavenly
body (RT-Her) for the first time in several years.

August 6

A lecture “Observing the Invisible Universe with Radio Waves” held at the Information Space of Astronomy and Science.

August 9~11

Chura-boshi Research Team workshop for high school students held at VERA Ishigakijima Station and Ishigakijima
Astronomical Observatory, with 7 participants from Ishigakijima, and 3 participant from main island of Okinawa
in attendance. The students were divided into two groups to perform observations, a radio wave observation group
and an optical wavelenght group using the Murikabushi Telescope. The radio wave observation group was not able
to detect a new maser object. The optical wavelength group using the Murikabushi Telescope was also unable todetect anything.

XII Important Dates

August 9~
September 8

As a part of the summer student program held by NAOJ and the Department of Astronomical Science of the
Graduate University for Advanced Studies (SOKENDAI), two undergraduate students from Tokyo Institute ofTechnology and Kyoto University stayed at Chile Observatory and conducted research with ALMA data.

August 11

Summer 2017 Special Stargazing Party held at Okayama Astrophysical Observatory, with 81 visitors in attendance(out of 548 applicants).

August 12~20

Southern Island Star Festival 2017 held together with a special open house event at the VERA Ishigakijima Station
and Ishigakijima Astronomical Observatory among other facilities with approximately 11,337 visitors to the wholeStar Festival. Events included an astronomical observation party at Ishigakijima Astronomical Observatory,
attended by 1,043 visitors; and a special public opening of the VERA Station attended by 273 visitors. In addition,
a commemorative lecture by Vice-Director General Junichi Watanabe had approximately 100 participants.

August 12

Special open house of VERA Iriki station held jointly with the Yaeyama Highland Star Festival 2017, withapproximately 3,800 visitors in attendance.

August 19
August 25~26
August 26

Iwate Galaxy Festival 2017, a special open house day of Mizusawa Campus, held with approximately 4,000 visitors
in attendance.
NAOJ Chile Observatory held a traditional Tanabata event in San Pedro de Atacama.
Open House day of Nobeyama Radio Observatory. There were 2,093 visitors for this event.

August 28~31

The observation training class in Ishigakijima “Learning about Space through astronomical observation”(common education subject) based on the cooperation agreement between the University of the Ryukyus and the
National Astronomical Observatory was carried out at the VERA Ishigakijima observation station, Ishigakijima
Astronomical Observatory, and there were 33 participants.

August 29~
September 3

Graduate students from the Department of Astronomical Science, SOKENDAI (Graduate University for
Advanced Studies) and astronomy major students from the University of Hawai`i at Hilo worked together to do anobservation program at the Subaru Telescope.

September 22~ An exhibit “Mitaka Solar System Walk - Let’s walk in the Mini Mini Solar System” held at the Information Space
November 5of Astronomy and Science.
September 28

Their Imperial Highnesses Prince and Princess Akishino visited Chile. Seiichi Sakamoto, the director of the NAOJ
Chile Observatory explained the activities of NAOJ in Chile.

October 10~13

Aiming to capture the first-ever photograph of “a shadow of the black hole” through VLBI observations combining
worldwide millimeter and sub-millimeter telescopes, the EHT (Event Horizon Telescope) and international
collaboration with 13 participating country held its first imaging workshop after nearly 10 years of work.

October 13~14“Mitaka Open House Day” held with 3,269 visitors in attendance.

October 21~22

The 29th national convention of “Hoshizora-no-machi, Aozora-no-machi (Streets of starry sky and blue sky)”
was held in Minamimaki Village by the Ministry of the Environment with the host of Minamimaki Village, andcooperation from Nobeyama Radio Observatory. Also, Takamadonomiya Princess Hisako visited Nobeyama Radio
Observatory and the NINS Nobeyama Exhibition Room.

October 26~28

The Public Relations Center co-hosted a joint booth (with three Japanese universities) at the World Conference of
Science Journalists (WCSJ) in San Francisco.

October 27

Four buildings formally registered as Tangible Cultural Properties with the Council for Cultural Affairs 1) Mainbuilding of the former Latitude Observatory (now the Oshu Space & Astronomy Museum) 2) the main building of theprovisional Latitude Observatory (now the Kimura Hisashi Memorial Museum) 3) the visual zenith telescope housingof the provisional Latitude Observatory 4) the target stand and cover for the visual zenith telescope.

November 1

NAOJ Decadal Planning Workshop was held in NAOJ Mitaka Campus. The subtitle of this workshop was “Imagine
all of you are the Director General today.” Many staff members discussed the future direction of our organizational
structure and research activities.

“The 15th Mizusawa VLBI observatory users meeting” was held, and 11 of the 55 participants were students.
November 3~4 The participants ranged from youths to seniors. It was a substantial meeting with lively discussion about
Japanese, East Asian, and world wide VLBI.
November
15~17

The Public Relations Center hosted a booth at the Science Centre World Summit 2017 (SCWS2017) at the National
Museum of Emerging Science and Innovation (Miraikan).

November 21

A ceremony for FY 2017 continuous service recognition was held. 6 NAOJ staff members were recognized: Seiichi
Sakamoto, Tomonori Usuda, Kenshi Yanagisawa, Fumihiro Uraguchi, Go Yamazaki.

December 9“Jimoto kansha Day (Thanks Day for the locals)” was held at NINS Nobeyama Exhibition Room hosted by
Nobeyama Radio Observatory. It was carried out by 3 Nobeyama Institutes (Tsukuba and Shinshu Universities andNobeyama Radio Observatory). There were 55 participants.

XII Important Dates

157

December
21~22“The 37th Symposium on Astronomy Technology” held to promote astronomy related technology. It seems to be
popular as a chance to meet and talk with people from other organizations, projects, and research institutes whom
you normally don't have chance to speak with informally.

December
26~27

The NAOJ Chile Observatory, together with the Nobeyama Radio Observatory hosted the ALMA/45-m/ASTE
Users Meeting in NAOJ Mitaka.

2018
January 6~10
January 7
January 12~13
January 19~20
January 27

A total of 12 undergraduate students from Japan and University of Hawai`i at Hilo participated in the observation
experience program at the Subaru Telescope. This was the first time for students in Hilo to join Subaru’s
observation experience program.
Minister Masaji Matsuyama of the Cabinet Office visited the Subaru Telescope’s facilities in Hilo and Maunakea.
Mr. Toshiei Mizuochi, State Minister for Ministry of Education, Culture, Sports, Science and Technology visited
ALMA.
Star Island 17 open house event of VERA Ogasawara Station held, with 167 visitors in attendance.
Staff of the Subaru Telescope held a science workshop and hosted an interactive booth at the annual Onizuka
Science Day at the University of Hawai`i at Hilo.

February 3

The Second “Nagano is a Astro-Prefecture” meeting was held in the campus of the National Institute ofTechnology, Nagano College by the executive committee consisting of Nobeyama Radio Observatory, National
Institute of Technology, Nagano College, Shiojiri Star Party, and so on.There were about 80 participants.

February 4

The 23rd ALMA public lecture titled “ALMA Telescope Exploring the Cold Universe-To Solve the Mysteries ofPlanetary Formation with State-of-the Art Technology” was held by NAOJ at the Tokyo International Exchange
Center. The event attracted 265 participants.

February
16~18

The Public Relations Center hosted a joint booth with JSPS and two Japanese universities at the American
Association for the Advancement of Science (AAAS) annual meeting in Austin.

February 20

NAOJ Engineering Decadal Planning Workshop was held in NAOJ Mitaka Campus. The subtitle of this workshop
was “Engineering at NAOJ: Review of the Past Decade, Strategy for the Next Decade.” Many staff members
discussed about the direction of future development at NAOJ.

March 2President Mariko Hasegawa of the Graduate University for Advanced Studies (SOKENDAI) visited the Subaru
Telescope’s facilities in Hilo and Maunakea.

March 5~9

Staff of the Subaru Telescope visited classes in the public schools in Hilo and vicinity during the Journey throughthe Universe program.

March 24~28

IAU, NAOJ, and Fukuoka City co-hosted “Communicating Astronomy with the Public Conference (CAP2018)”
held at Fukuoka City Science Museum with 446 participants from 53 countries in attendance.

March 31

A ceremony for FY 2017 continuous service recognition for retiring staff members was held. 8 staff members wererecognized: Takashi Noguchi, Tetsuya Watanabe, Hideo Hanada, Nobuharu Ukita, Susumu Kawashima, Katsuhisa
Sato, Susumu Hommyo.

NAOJ staff participated in the FUREAI (Friendly) Astronomy program by visiting schools and talking about their
Throughout thework and the Subaru Telescope. This outreach program started eight years ago and was spearheaded by Dr. Nobuo
year
Arimoto, the former Director of the Subaru Telescope.
Together with other Maunakea Observatories, Subaru Telescope started a special tour program “Kamaʻāina
Throughout theObservatory Experience (KOE)” dedicated to Hawai`i residents. In 2017, Subaru conducted 10 KOE tours for a
year
total of 120 visitors. KOE is separate from Subaru’s public tour program that started in 2004.

158

XII Important Dates

XIII Publications, Presentations
1. Refereed Publications
Abbott, B. P., et al. including Flaminio, R., Vetro, F., Aoki, K., Aoki,
W., Finet, F., Fujiyoshi, T., Furusawa, H., Kim, J. H., Koshida, S.,
Kuroda, D., Lee, C.-H., Matsubayashi, K., Nagai, H., Nakata, F.,
Okita, H., Tajitsu, A., Tanaka, I., Tanaka, M., Terai, T., Yoshida,M., Kawamuro, T., Castellon, J. L. N.: 2017, Multi-messenger
Observations of a Binary Neutron Star Merger, ApJL, 848, L12.
Abbott, B. P., et al. including Flaminio, R.: 2017, Effects of waveformmodel systematics on the interpretation of GW150914, ClassicalQuantum Gravity, 34, 104002.
Abbott, B. P., et al. including Flaminio, R.: 2017, Search for gravitational
waves from Scorpius X-1 in the first Advanced LIGO observing run
with a hidden Markov model, Phys. Rev. D, 95, 122003.
Abbott, B. P., et al. including Flaminio, R.: 2017, Search forintermediate mass black hole binaries in the first observing run ofAdvanced LIGO, Phys. Rev. D, 96, 022001.
Abbott, B. P., et al. including Flaminio, R.: 2017, All-sky search forperiodic gravitational waves in the O1 LIGO data, Phys. Rev. D, 96,062002.
Abbott, B. P., et al. including Flaminio, R.: 2017, First low-frequency
Einstein@Home all-sky search for continuous gravitational waves inAdvanced LIGO data, Phys. Rev. D, 96, 122004.
Abbott, B. P., et al. including Flaminio, R.: 2017, First narrow-bandsearch for continuous gravitational waves from known pulsars inadvanced detector data, Phys. Rev. D, 96, 122006.
Abbott, B. P., et al. including Flaminio, R.: 2017, GW170104:
Observation of a 50-Solar-Mass Binary Black Hole Coalescence at
Redshift 0.2, Phys. Rev. Lett., 118, 221101.
Abbott, B. P., et al. including Flaminio, R.: 2017, GW170814: A ThreeDetector Observation of Gravitational Waves from a Binary Black
Hole Coalescence, Phys. Rev. Lett., 119, 141101.
Abbott, B. P., et al. including Flaminio, R.: 2017, GW170817:
Observation of Gravitational Waves from a Binary Neutron Star
Inspiral, Phys. Rev. Lett., 119, 161101.
Abbott, B. P., et al. including Flaminio, R.: 2017, Search for continuous
gravitational waves from neutron stars in globular cluster NGC 6544,
Phys. Rev. D, 292, 082005.
Abbott, B. P., et al. including Flaminio, R.: 2017, A gravitational-wave
standard siren measurement of the Hubble constant, Nature, 551,
85–88.
Abbott, B. P., et al. including Flaminio, R.: 2017, First Search for
Gravitational Waves from Known Pulsars with Advanced LIGO, ApJ,
839, 12.
Abbott, B. P., et al. including Flaminio, R.: 2017, Search for
Gravitational Waves Associated with Gamma-Ray Bursts during theFirst Advanced LIGO Observing Run and Implications for the Origin
of GRB 150906B, ApJ, 841, 89.
Abbott, B. P., et al. including Flaminio, R.: 2017, Upper Limits on
Gravitational Waves from Scorpius X-1 from a Model-based Crosscorrelation Search in Advanced LIGO Data, ApJ, 847, 47.
Abbott, B. P., et al. including Flaminio, R.: 2017, Gravitational Waves

and Gamma-Rays from a Binary Neutron Star Merger: GW170817
and GRB 170817A, ApJL, 848, L13.
Abbott, B. P., et al. including Flaminio, R.: 2017, Estimating theContribution of Dynamical Ejecta in the Kilonova Associated with
GW170817, ApJL, 850, L39.
Abbott, B. P., et al. including Flaminio, R.: 2017, On the Progenitor of
Binary Neutron Star Merger GW170817, ApJL, 850, L40.
Abbott, B. P., et al. including Flaminio, R.: 2017, Search for Post-merger
Gravitational Waves from the Remnant of the Binary Neutron Star
Merger GW170817, ApJL, 851, L16.
Abbott, B. P., et al. including Flaminio, R.: 2017, GW170608:
Observation of a 19 Solar-mass Binary Black Hole Coalescence,
ApJL, 851, L35.
Abbott, B. P., et al. including Flaminio, R.: 2018, All-sky search forlong-duration gravitational wave transients in the first Advanced
LIGO observing run, Classical Quantum Gravity, 35, 65009.
Abbott, B. P., et al. including Flaminio, R.: 2018, Effects of data quality
vetoes on a search for compact binary coalescences in Advanced
LIGO's first observing run, Classical Quantum Gravity, 35, 65010.
Abbott, B. P., et al. including Flaminio, R.: 2018, First Search for
Nontensorial Gravitational Waves from Known Pulsars, Phys. Rev.
Lett., 120, 031104.
Abbott, B. P., et al. including Flaminio, R.: 2018, GW170817:
Implications for the Stochastic Gravitational-Wave Background from
Compact Binary Coalescences, Phys. Rev. Lett., 120, 091101.
Abdellaoui, G., et al. including Kajino, T., Mizumoto, Y., Watanabe, J.,
JEM EUSO Collaboration: 2017, Meteor studies in the framework of
the JEM-EUSO program, Planet. Space Sci., 143, 245–255.
Abdellaoui, G., et al. including Kajino, T., Mizumoto, Y., Watanabe, J.,
JEM EUSO Collaboration: 2017, Cosmic ray oriented performancestudies for the JEM-EUSO first level trigger, Nucl. Instrum. Methods
Phys. Res., Sect. A, 866, 150–163.
Acernese, F., et al. including Flarninio, R.: 2017, Status of the Advanced
Virgo gravitational wave detector, Int. J. Mod. Phys. A, 32, 1744003.
Acero, F., et al. including Inoue, T.: 2017, Prospects for Cherenkov
Telescope Array Observations of the Young Supernova Remnant RX
J1713.7-3946, ApJ, 840, 74.
Aharonian, F., et al. including Kawamuro, T.: 2018, Hitomi observationof radio galaxy NGC 1275: The first X-ray microcalorimeter
spectroscopy of Fe-K alpha line emission from an active galactic
nucleus, PASJ, 70, 13.
Aharonian, F., et al. including Moriya, T. J.: 2018, Search for thermal
X-ray features from the Crab nebula with the Hitomi soft X-ray
spectrometer, PASJ, 70, 14.
Aihara, H., et al. including Furusawa, H., Hayashi, Y., Ikeda, H.,
Kamata, Y., Kawanomoto, S., Koike, M., Komiyama, Y., Mineo,
S., Miyazaki, S., Obuchi, Y., Oishi, Y., Takata, T., Tanaka, M.,
Tanaka, Y., Uraguchi, F., Yamada, Y., Yamanoi, H., Arimoto, N.,
Finet, F., Furusawa, J., Hattori, T., Hayashi, M., Imanishi, M.,
Iwata, I., Kashikawa, N., Koshida, S., Lee, C. H., Matsuoka, Y.,
Nakata, F., Onodera, M., Onoue, M., Pyo, T. S., Tait, P. J., Terai,T., Usuda, T., Yeh, S.: 2018, First data release of the Hyper Suprime-

XIII Publications, Presentations

159

Cam Subaru Strategic Program, PASJ, 70, S8.
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S., Kashima, S., Funazaki, K., Satoh, A., Taniguchi, H., Kato,
H., Kikuchi, M., Sasaki, H., Hasegawa, T., Yano, T., Gouda, N.,
Kobayashi, Y., Yamada, Y., Iwata, T., Gusev, A.: 2017, Developmentof a Small Telescope like PZT and Effects of Vibrations of Mercury
Surface and Ground Noise, Gyroscopy and Navigation, 8, 304–319.
Hattori, M., Tamada, Y., Oya, S., Hayano, Y., Kamei, Y.: 2017, Basicexperiments of laser beam correction by adaptive optics microscope
for the accurate manipulation of biological tissues, Proc. SPIE,
10251, Eds. T. Yatagai, Y. Aizu, O. Matoba, Y. Awatsuji, 102511J2.
Jike, T.: 2017, VERA Geodetic VLBI System, 2nd General Meeting of
the Asia-Oceania VLBI Group for Geodesy and Astrometry, Ed. L.
McCallum, http://auscope.phys.utas.edu.au/aov/about/2ndaovgm.
html
Jovanovic, N., Guyon, O., Kotani, T., Kawahara, H., Hosokawa, K.,
Lozi, J., Males, J., Ireland, M., Tamura, M., Mawet, D., Schwab, C.,
Norris, B., Leon-Saval, S., Betters, C., Tuthill, P.: 2017, Developing

180

XIII Publications, Presentations

post-coronagraphic, high-resolution spectroscopy for terrestrial planet
characterization on ELTs, Proc. AO4ELT5, 076.
Jovanovic, N., et al. including Guyon, O., Lozi, J., Tamura, M.,
Kotani, T., Kawahara, H., Pathak, P.: 2017, Pioneering highcontrast science instruments for planet characterization on giant
segmented mirror telescopes, Proc. AO4ELT5, 075.
Kim, D. W., Trippe, S., Lee, S. S., Park, J. H., Kim, J. Y., Algaba, J. C.,
Hodgson, J. A., Kino, M., Zhao, G. Y., Wajima, K., Kang, S., Oh, J.,
Lee, T., Byun, D. Y., Kim, S. W., Kim, J. S.: 2017, The MillimeterRadio Emission of Bl Lacertae During Two gamma-Ray Outbursts, J.
Korean Astron. Soc., 50, 167–178.
Kojima, T., Kroug, M., Uemizu, K., Niizeki, Y., Takahashi, H., Uzawa,
Y.: 2017, Performance of a Wide IF SIS-Mixer-Amplifier Module for
ALMA Band 8 (385–500 GHz), Proc. Twenty-Eighth Inter. Symp. on
Space Terahertz Technology, NRAO Library.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2017, GRB 170921A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,21905, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2017, GRB 170903A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
21801, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2017, GRB 170317A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 20899, 1.
Le Duigou, J.-M., et al. including Lozi, J.: 2017, First results of
the PERSEE experiment, Proc. SPIE, 10565, Eds. B. Cugny, E.
Armandillo, N. Karafolas, 105650W.
Le Duigou, J.-M., et al. including Lozi, J.: 2017, Final results of
the PERSEE experiment, Proc. SPIE, 10564, Eds. B. Cugny, E.
Armandillo, N. Karafolas, 105640E.
Lee, C.-H.: 2017, A Closer Look at CVSO30b: Transiting Exoplanetor Circumstellar Dust Clump?, Research Notes of the American
Astronomical Society, 1, 41.
Lee, C.-H.: 2017, Identifying Rings in IFU Surveys, Research Notes of
the American Astronomical Society, 1, 12.
Lee, C.-H.: 2017, Microlensing and Its Degeneracy Breakers: Parallax,
Finite Source, High-Resolution Imaging, and Astrometry, Universe, 3,53.
Lozi, J., Guyon, O., Jovanovic, N., Goebel, S., Pathak, P., Norris, B.,
Martinache, F., N Diaye, M., Mazin, B., Walter, A.: 2017, SCExAO:
lessons learned for a future TMT instrument, Proc. AO4ELT5, , 080.
Maehara, H.: 2017, High-dispersion spectroscopy of the probablemicrolensing event TCP J05074264+2447555, The Astronomer’s
Telegram, 10919.
Matsuo, H., Ezawa, H., Kiuchi, H., Honma, M., Murata, Y,, Ukibe,M., Fujii, G., Shiki, S., Sakata, M.: 2018, Developments of Terahertz
Intensity Interferometry using SIS Photon Counting Detectors, 11th
Superconducting SFQ VLSI Workshop, Ed. M. Hidaka, 18–22.
Matsuo, H., Ezawa, H., Kiuchi, H., Honma, M., Murata, Y.: 2018,
Proposal of Photon Counting Terahertz Interferometry, JAXA Special
Publication JAXA-SP-17-009E, Eds. T. Ootsubo, I. Yamamura, K.
Murata, T. Onaka, 261–264.
Miura, R. E., Espada, D., Nakanishi, K., Hirota, A., Sugai, H.: 2017,

Super-star-cluster forming clouds in the young starburst galaxy NGC
5253, Memorie della Societa Astronomica Italiana, 88, 834.
Nakamura, K., Fujimoto, M.-K.: 2017, Double Balanced Homodyne
Detection, Proc. of the 27th workshop on General Relativity andGravitation in Japan, http://home.hiroshima-u.ac.jp/~jgrg27/files/
Kouji_Nakamura.pdf
N’Diaye, M., Martinache, F., Jovanovic, N., Lozi, J., Guyon, O., Norris,
B., Ceau, A., Mary, D.: 2017, Mitigate the impact of ELT architecture
on AO performance: learn from today s telescopes to characterize andprevent the island effect, Proc. AO4ELT5, 132.
Nishimura, A., Yamagishi, M., Matsuo, M., Fujita, S., Taniguchi, K.,
Takekoshi, T., Minamidani, T., Tokuda, K.: 2017, Nobeyama 45-M
CO Survey For Cygnus-X: Possible Evidences For Formation of
DR21 And W75N By Cloud-Cloud Collision, Galaxy Evolution
Across Time, 24, 806080.
Nozawa, T.: 2017, Overall Dust Inputs from Core-Collapse Supernovae
in the Galaxy, Memorie della Societa Astronomica Italiana, 88, 447–
450.
Onodera, M.: 2017, Metallicity and Ionization Condition of Ism in StarForming Galaxies at High Redshift, Galaxy Evolution Across Time,24, 808187.
Pathak, P., Guyon, O., Jovanovic, N., Lozi, J., Martinache, F., Minowa,
Y., Kudo, T., Kotani, T., Takami, H.: 2017, Closed-loop atmosphericdispersion compensation: on-sky demonstration of sub-milliarcsecond
residual dispersion across H-band, Proc. AO4ELT5, 110.
Soma, M., et al.: 2017, NOVA CANIS MAJORIS 2018 = TCP
J07134590-2112330, CBET 4499, Ed. D. W. E. Green.
Sotani, H.: 2017, Prospect for observational discriminant of thegravitational theories, Proc. of the MG14 Meeting on General
Relativity, Eds. M. Bianchi, R. T. Jantzen, R. Ruffini, 1567–1570.
Sotani, H.: 2017, Identifications of quasi-periodic oscillations observedin soft-gamma repeaters with crustal torsional oscillations, Proc. of
the MG14 Meeting on General Relativity, Eds. M. Bianchi, R. T.
Jantzen, R. Ruffini, 4121–4124.
Sotani, H., Tatsumi, T.: 2017, Hybrid Stars as a Third Family of
Compact Objects, JPS Conf. Proc. 20, Eds. T. Tatsumi, T. Maruyama,
T. Muto, 011031.
Sotani, H.: 2017, Protoneutron Star Properties via Gravitational Wave
Asteroseismology, JPS Conf. Proc. 20, Eds. T. Tatsumi, T. Maruyama,
T. Muto, 011047.
Suematsu, Y., Saito, K., Koyama, M., Enokida, Y., Okura, Y., Nakayasu,
T., Sukegawa, T.: 2017, Development of micro-mirror slicer integral
field unit for space-borne solar spectrographs, CEAS Space Journal, 9,421-431.
Suematsu, Y., Koyama, M., Sukegawa, T., Enokida, Y., Saito, K.,
Okura, Y., Nakayasu, T., Ozaki, S., Tsuneta, S.: 2017, Developmentof compact integral field unit for spaceborne solar spectropolarimeter, Proc. SPIE, 10563, Eds. Z. Sodnik, B. Cugny, N.
Karafolas, 105634M.
Suzuki, R., Harakawa, H., Schoeck, M., Ellerbroek, B.: 2017,
Instrument requirements for precision relative astrometry using TMT/
IRIS, Proc. AO4ELT5, 071.
Tamada, Y., Hayano, Y., Murata, T., Oya, S., Honma, Y., Kanazawa,M., Miura, N., Hasebe, M., Kamei, Y., Hattori, M.: 2017, Adaptive
optical imaging through complex living plant cells, Proc. SPIE,
10251, Eds. T. Yatagai, Y. Aizu, O. Matoba, Y. Awatsuji, 102510K3.

Tomisaka, K.: 2017, Magnetohydrostatic structures of magneticallysupported filaments and their stability, Memorie della Societa
Astronomica Italiana, 88, 571.
Usuda-Sato, K., Iizuka, R., Yamaoka, H., Handa, T.: 2018, The
Japanese Experience of the NameExoWorlds Competition:
Translating Official Information into Japanese to Enable Domestic
Groups to Participate in a Global Event, Communicating Astronomy
with the Public Journal, Ed. S.-l. Cheung, 13–19.
Wang, H., Yurchyshyn, V., Liu, C., Ahn, K., Toriumi, S., Cao, W.: 2018,
Strong Transverse Photosphere Magnetic Fields and Twist in Light
Bridge Dividing Delta Sunspot of Active Region 12673, Research
Notes of the American Astronomical Society, 2, 8.
Wang, K., Zahorecz, S., Cunningham, M. R., Toth, L. V., Liu, T., Lu, X.,
Wang, Y., Cosentino, G., Sung, R.-S., Sokolov, V., Wang, S., Wang,
Y., Zhang, Z., Li, D., Kim, K.-T., Tatematsu, K., Testi, L., Wu, Y.,
Yang, J., SAMPLING collaboration: 2018, First Data Release of the
ESO-ARO Public Survey SAMPLING – SMT “All-sky” Mappingof Planck Interstellar Nebulae in the Galaxy, Research Notes of theAmerican Astronomical Society, 2, 2.
Yamada, Y., Shirasaki, Y., Nishi, R.: 2018, Nano-JASMINE and smallJASMINE data analysis, Proc. IAU Symp. 330, Eds. A. RecioBlanco, P. de Laverny, A. G. A. Brown, T. Prusti, 104–105.
Yamanaka, M., et al. including Hanayama, H., Maehara, H., Sekiguchi,K., Nagayama, T., Team OISTER: 2017, OISTER Follow-up
Observations of the bright Type IIP supernova SN 2017eaw, AAS
Meeting #231, 446.08.
Yamaoka, H., Nakamura, Y.: 2017, NOVA IN OPHIUCHUS = PNV
J17184490-2454220 = PNV J17184504-2454221, Central Bureau
Electoronic Telegrams 4453, Ed. D. W. E. Green, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida, M.,
Ohta, K., Kawai, N.: 2017, GRB 170317A: MITSuME Okayama Ksband upper-limit, D Coordinates Network, Circular Service, 20892, 1.
Yano, T., JASMINE-WG: 2017, Infrared astrometric satellite, SmallJASMINE Clarification of the formation process of the super massive
black hole and Analysis of the gravitational potential, The scienceof Gaia and future challenges, Ed. D. Hobbs, http://www.astro.lu.se/
gaia2017/slides.html
Yano, T., JASMINE-WG: 2018, Clarification of the formation processof the super massive black hole by Infrared astrometric satellite,
Small-JASMINE, Proc. IAU Symp. 330, Eds. A. Recio-Blanco, P. de
Laverny, A. G. A. Brown, T. Prusti, 360–361.
Yokoyama, T., Fukai, R., Tsujimoto, T.: 2018, Meteoritical Perspectiveon the Origin of r-Process Nuclides in the Solar System, 49th Lunarand Planetary Science Conference, 1159.

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182

5. Publications in English

6. Conference Presentations

Shimizu, T., et al. including Sakurai, T., Suematsu, Y., Watanabe, T.,
Hara, H., Lee, K.-S., Kubo, M., Katsukawa, Y., Ichimoto, K.,
Ishikawa, R., Shimojo, M., Yaji, K., Inoue, N.: 2018, First Ten
Years of Hinode Solar On-Orbit Observatory, Astrophysics and Space
Science Library, Volume 449, Eds. T. Shimizu, S. Imada, M. Kubo,
Springer Nature Singapore, Singapore.
Jike, T., Tamura, Y.: 2017, VERA 2015 and 2016 Geodetic Activities,
International VLBI Service for Geodesy and Astrometry 2015+2016
Biennial Report, NASA, Greenbelt, MD.
Konishi, M., Tamura, M.: 2017, Collected Papers of the Subaru SEEDS
Project 2006-2016, Astorbiology Center, Tokyo.
Tamura, M.: 2018, Handbook of Exoplanets “HiCIAO and IRD: Two
Exoplanet Instruments for the Subaru 8.2 m Telescope”, Springer,
Switzerland.
Yamaoka, H.: 2017, Handbook of Supernovae “Discovery, Confirmation,
and Designation of Supernovae”, Springer, Switzerland.

Agata, H.: 2017, The Outreach & Education Concept and Strategy of
NAOJ, Astronomy Museums, Visitor Centers & Public Observatories
Workshop, (Leiden, Netherland, Sep. 27–29, 2017).
Agata, H., Canas, L.: 2017, CAP Conferences Series - Communicating
Astronomy in Today’s World:Purpose & Methods -, Global Hands-On
Universe Conference 2017, (Bowling Green, KY, USA, Aug. 14–19,
2017).
Agata, H., Sekiguchi, K., Naito, S., Cheung, S.: 2017, “You are Galileo !”,You are Galileo Workshop, (Mandalay, Myanmar, Nov. 29–30, 2017).
Agata, H., Takanashi, N., Ando, K.: 2018, Introduction of JapaneseSociety for Education and Popularization of Astronomy,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24–28, 2018).
Agata, H., Takata, H., Tsuzuki, Y., Kashima, S.: 2018, One telescopefor one family - “You are Galileo!” project of NAOJ Episode II -,Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24–28, 2018).
Agata, H., Canas, L., Karino, S., Russo, P., Govender, K.: 2017,
Astronomy Education Curriculum - Initial steps towards the IAU
international recommendations and guidelines -, Global Hands-On
Universe Conference 2017, (Bowling Green, KY, USA, Aug. 14-19,2017).
Aoki, W., Ishii, M.: 2018, Experiences related to the TMT site problem
in Japan, Communicating Astronomy with the Public 2018, (Fukuoka,
Japan, Mar. 24-28, 2018).
Aoki, W., Li, H. N., Matsuno, T., Kumar, Y. B., Shi, J., Suda, T.,Zhao, G.: 2017, Lithium-rich very metal-poor stars discovered withLAMOST and Subaru, The 14th Int. Symp. on Origin of Matter and
Evolution of Galaxies (OMEG2017), (Daejeon, Korea, Jun. 27-30,
2017).
Aoki, W.: 2017, r-process obseevations, 9th European Summer Schoolon Experimental Nuclear Astrophysics, (Santa Tecla, Italy, Sep. 1724, 2017).
Aoki, W.: 2017, CEMP-no stars, A Celebration of CEMP and a Gala of
GALAH, (Melborne, Australia, Nov. 13-17, 2017).
Aoki, W.: 2017, CEMP stars in the Milky Way and dwarf galaxies,
Stellar Evolution, Supernova Nucleosynthesis Across Cosmic Time,(Chiba, Japan, Sep. 18-29, 2017).
Arai, M., Agata, H., Yamazaki, N., Akiyama, R.: 2018, Introduction of
Astro-Tourism in Japan “Sora Tourism” -As a strategy to promotescience culture -, Communicating Astronomy with the Public 2018,(Fukuoka, Japan, Mar. 24-28, 2018).
Araki, H., et al. including Namiki, N., Noda, H., Oshigami, S.: 2017,
Performance Model Simulation of Ganymede Laser Altimeter(GALA) for the JUICE Mission, Joint Conference : 31st ISTS, 26th
ISSFD, and 8th NSAT, (Ehime, Japan, Jun. 3-9, 2017).
Aso, Y.: 2018, Status of the ground based interferometric gravitational
wave detectors, Gravitational-Wave Astronomy of core-collapse
SuperNovae (GWASNe) Workshop, (Mitaka, Japan, Jan. 29, 2018).
Canas, L., Agata, H., Karino, S., Yamaoka, H.: 2017, Efforts on bringing
together the Asia-Pacific astronomy communication community, 2017
Asia-Pacific Regional IAU Meeting, (Taipei, Taiwan, Jul. 3–7, 2017).
Canas, L., Agata, H., Cheung, S. L., Shibata, Y.: 2018, IAU and the
Public: IAU Office for Astronomy Outreach (OAO) Communications,

XIII Publications, Presentations

Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Canas, L., Agata, H., Yamaoka, H., Karino, S.: 2018, Communicating
Astronomy with the Public 2018: efforts on bringing together theinternational astronomy communication community, Communicating
Astronomy with the Public 2018, (Fukuoka, Japan, Mar. 24-28,
2018).
Cheung, S. L., Walker, C.: 2018, Dark Skies for all, Communicating
Astronomy with the Public 2018, (Fukuoka, Japan, Mar. 24-28,
2018).
Cheung, S. L., Agata, H., Canas, L., Shibata, Y.: 2018, Connections
with IAU OAO and Commission C1, Astronmoy Education Meeting,(Kagoshima, Japan, Mar. 30, 2018).
Cheung, S. L., Agata, H., Canas, L., Shibata, Y., IAU NOCs:
2018, Updates from the IAU Office for Astronomy Outreach,Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Cheung, S. L.: 2017, Astronomy Communication and Informal
Education, ITCA Colloquium 2017, (Bangkok, Thailand, Aug. 7-11,2017).
Cheung, S. L., Agata, H., Canas, L., Shibata, Y.: 2017, OAO and
UNAWE collaboration, UNAWE (Universe Awareness) Japan
Workshop, (Shizuoka, Japan, Apr 5-6, 2017).
Cheung, S. L., Agata, H., Canas, L., Shibata, Y.: 2017, IAU Officefor Astronomy Outreach's role on supporting the Astronomy for
Development, Fourth Middle-East and Africa Regional IAU Meeting,(Addis ababa, Ethiopia, May 22-25, 2017).
Cheung, S. L., Agata, H., Canas, L., Shibata, Y.: 2017, IAU for the
Public, 2017 Asia-Pacific Regional IAU Meeting, (Taipei, Taiwan,
Jul. 3-7, 2017).
Cheung, S. L., Agata, H., Canas, L., Shibata, Y.: 2017, OAO Roles in
the Global Arena, South East Asia Astronoy Network Meeting 2017,(Mandalay, Myanmar, Nov. 29-30, 2017).
Currie, T., Guyon, O., Kasdin, N. J., Brandt, T., Groff, T., Jovanovic,
N., Lozi, J., Chilcote, J. K., Uyama, T., Ascensio-Torres, R.,
Tamura, M., Norris, B.: 2018, Early Direct Imaging and Spectral
Characterization of Extrasolar Planets with the SCExAO/CHARIS,AAS Meeting #231, (Washington, D. C., USA, Jan, 8-12, 2018).
Drilleau, M., Blanchette-Guertin, J. F., Kawamura, T., Lognonné,P., Wieczorek, M.: 2017, Seismic velocity and crustal thickness
inversions: Moon and Mars, EGU General Asembly 2017, (Vienna,
Austria, Apr. 23-28, 2017).
Egusa, F., Usui, F., Murata, K., Yamashita, T., Yamamura, I., Onaka, T.:2017, Revised calibration for near- and mid-infrared images fromAKARI/IRC pointed observations in Phases 1 and 2, The Cosmic
Wheel and the Legacy of the AKARI Archive: from galaxies andstars to planets and life, (Tokyo, Japan, Oct. 17-20, 2017).
Egusa, F.: 2017, Gas and stellar spiral arms and their offsets in the
grand-design spiral galaxy M51, 2017 Asia-Pacific Regional IAU
Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Enya, K., et al. including Namiki, N., Noda, H., Araki, H., Oshigami, S.,
Matsumoto, K.: 2017, JUICE/GALA-J (1) : The Ganymede Laser
Altimeter (GALA) for the JUICE mission - Introduction and current
status, JpGU-AGU Joint Meeting 2017, (Chiba, Japan, May 20-25,
2017).
Espada, D., Matsushita, S., Miura, R. E., Israel, F. P., Neumayer, N.,

Martin, S., Henkel, C., Izumi, T., Iono, D., Aalto, S., Ott, J., Peck, A.
B., Quillen, A. C., Kohno, K.: 2017, Disentangling the properties of
the circumnuclear disk of Centaurus A with ALMA, East-Asia AGN
Workshop 2017, (Kagoshima, Japan, Dec. 4-6, Japan).
Espada, D., Matsushita, S., Miura, R. E., Israel, F. P., Neumayer, N.,
Martin, S., Henkel, C., Izumi, T., Iono, D., Aalto, S., Ott, J., Peck, A.
B., Quillen, A. C., Kohno, K.: 2017, Disentangling the properties of
the circumnuclear disk of Centaurus A with ALMA, The role of gas
in galaxy dynamics, (Valetta, Malta, Oct. 2-6, 2017).
Ezaki, S., Shan, W., Asayama, S., Noguchi, T., Iguchi, S.: 2017,
Development of Multi-Beam Superconducting Heterodyne Receiverfor Radio Telescopes, The 19th East Asia Sub-millimeter-wave
Receiver Technology Workshop, (Taipei, Taiwan, Nov. 28-30, 2017).
Ezaki, S., Shan, W., Kroug, M., Kojima, T., Gonzalez, A., Asayama, S.,
Noguchi, T.: 2017, Fabrication and Characterization of (100) Silicon
Membranes for a Multi-beam Superconducting Heterodyne Receiver,17th International Workshop on Low Temperature Detectors,(Kurume, Fukuoka, Japan, Jul. 17-21, 2017).
Ezawa, H., Matsuo, H., Ukibe, M., Fujii, G., Shiki, S.: 2017, Progress
towards Photon Counting Detectors for Terahertz Astronomy, 17th
International Workshop on Low Temperature Detectors, (Kurume,
Fukuoka, Japan, Jul. 17-21, 2017).
Ezawa, H., Matsuo, H., Ukibe, M., Fujii, G., Shiki, S.: 2018, SIS
Photon Detectors for Terahertz Astronomy, 29th IEEE International
Symposium on Space Terahertz Technology, (Pasadena, CA, USA,
Mar. 26-28, 2018).
Flaminio, R.: 2017, Latest results on crystalline coatings
characterization, Gravitational Wave Advanced Detector Workshop(GWADW), (Hamilton Island, Australia, May 7-12, 2017).
Flaminio, R.: 2017, Status of Advanced Virgo & Frequency Dependent
Squeezing, The Ninth Australasian Conference on General Relativity
and Gravitation, (Perth, Australia, Dec. 27-30, 2017).
Flaminio, R.: 2018, Optical performance of ‘large-area’ crystalline
coatings, Virgo collaboration meeting, (Cascina, Italy, Jan. 22-25,
2018).
Fouchard, M., Higuchi, A., Ito, T.: 2017, Flux of 'new' long-period
comets: confrontation of numerical simulations with observations,Asteroids, Comets, Meteors 2017, (Montevideo, Urugai, April 10-14,
2017).
Fujita, T., Agata, H., Arimoto, N.: 2018, Deliver astronomers to a lotof classrooms! - The “Fureai (Friendly) Astronomy” project, NAOJ –,Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Fujita, Y., Nagai, H.: 2017, Jets and a cold chaotic disk in the central
pc of the Perseus cluster, AAS HEAD meeting #16, (Sun Valley, ID,
USA, Aug. 20-24, 2017).
Fukuda, Y., Aoyama, Y., Doi, K., Hayakawa, H., Okuno, J., Nishijima, J.,
Kazama, T., Yamamoto, K., Higashi, T., Shibuya, K.: 2017, Geodetic
studies of GIA and ice sheet changes by JARE, Joint Scientific
Assembly of IAG-IASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Fukui, A.: 2017, Multiband Photometry of K2 Transiting Planets with
MuSCAT and MuSCAT2, Kepler & K2 Science Conference IV,(Moffett Field, CA, USA, Jun. 19-23, 2017).
Fukui, A.: 2017, Scientific Results Obtained with OAO188cm/
MuSCAT, 10th Workshop on Astronomy with Precise Radial Velocity
Measurements, (Nara, Japan, Oct. 29-Nov. 2, 2017).

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Fukui, A.: 2017, Transit Photometry of Earth-sized Planets with
MuSCAT, 10th RESCEU/Planet2 Symposium: Planet Formation
around Snowline, (Tokyo, Japan, Nov. 28-30, 2017).
Fukui, A.: 2018, Challenge in Atmospheric Observations of M-dwarf
Planets in Optical Wavelengths, DTA Symposium VIII: Challenge to
Super-Earths and Their Atmospheres, (Mitaka, Tokyo, Japan, Mar.
6-8, 2017).
Fukushima, K., Kobayashi, K., Hirota, T.: 2017, Methanol maser
survey at 3 mm band with the Nobeyama 45 m radio telescope,
NRO45m/ASTE Single Dish Science Workshop 2017, (Nobeyama,
Nagano, Japan, Aug. 28-29, 2017).
Gonzalez, A., Kaneko, K., Asayama, S., Srikanth, S., Effland, J., Saini,K.: 2017, ALMA band 2+ (67-95 GHz) receiver optics, 2017 IEEE
Radio and Antenna Days of the Indian Ocean (RADIO), (Cape Town,
South Africa, Sep. 25-28, 2017).
Gonzalez, A., Kaneko, K., Asayama, S.: 2017, Receiver optics for
ALMA band 11 (1.25-1.57 THz), 42nd International Conference on
Infrared, Millimeter, and Terahertz Waves (IRMMW-THz), (Cancun,
Mexico, Aug. 27-Sep. 1, 2017).
Gouda, N., JASMINE-WG: 2017, Outline of Infrared Space Astrometry
missions: JASMINE, IAU Symp. 330: Astrometry and Astrophysics
in the Gaia Sky, (Nice, France, Apr. 24-28, 2017).
Gouda, N.: 2017, JASMINE series, The science of Gaia and futurechallenges, (Lund, Sweden, Aug. 30-Sep. 1, 2017).
Groff, T., Chilcote, J., Brandt, T., Kasdin, N. J., Galvin, M., Loomis, C.,
Rizzo, M., Knapp, G., Guyon, O., Jovanovic, N., Lozi, J., Currie,T., Takato, N., Hayashi, M.: 2017, First light of the CHARIS highcontrast integral-field spectrograph, SPIE Optics + Photonics, (San
Diego, CA, USA, Aug. 6-10, 2017).
Gusev, A., Hanada, H., Kosov, A., Ping, J., Vasilyev, M.: 2017, Moon's
physical librations, tides and the interior: results and perspects,
SELENE Symposium, (Tokyo, Japan, Sep. 13-14, 2017).
Guyon, O., Lozi, J., Jovanovic, N., Males, J.: 2017, SCExAO: A
prototyping platform for ELTs Extreme-AO, AO4ELT5, (Tenerife,
Spain, Jun. 25-30, 2017).
Hachisuka, K.: 2018, High velocity water maser features in W3 (H2O),High Mass Star Formation Workshop 2018, (Yamaguchi, Japan, Mar.
22-23, 2018).
Hada, K.: 2017, East Asian VLBI Network (EAVN) observations of
nearby supermassive black holes in SgrA and M87, 2017 Asia-PacificRegional IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Hada, K.: 2017, EATING VLBI observations in 2016/2017, Eating
VLBI Workshop 2017, (Jeju, Korea, Oct. 30-Nov. 1, 2017).
Hada, K.: 2017, EAVN Campaign Observations of Sgr A/M87, 2017
KaVA/EAVN Joint Science Working Group Meeting, (Daejeon,
Korea, Nov. 22-23, 2017).
Hada, K.: 2018, Recent EAVN activities and future prospects withThailand, NARIT Key Science Workshop: Masers & Molecular Lines
in Radio Astronomy, (Chiang Mai, Thailand, Jan. 15, 2018).
Hada, K.: 2018, Introduction to Radio Astronomy & Facilities, NARITSOKENDAI Winter School 2018; Astropysical Masers & Molecular
Lines in Radio Astronomy, (Chiang Mai, Thailand, Jan. 16-19, 2018).
Hamano, K., Tanaka, R., Yoshida, S., Miyachi, A., Nishikawa, K.,
Kawasaki, S.: 2017, Design of concurrent dual-band rectifier withharmonic signal control, 2017 IEEE MTT-S International Microwave
Symposium, (Honololu, HI, USA, Jun. 4-9, 2017).

184

XIII Publications, Presentations

Hanada, H., Tsuruta, S., Asari, K., Araki, H., Funazaki, K., Satoh,A., Taniguchi, H., Kikuchi, M.: 2017, A method for attitude control
of telescopes making use of an inverted pendulum, Internationals c i e n t i f i c c o n f e r e n c e F U N D A M E N TA L A N D A P P L I E DPROBLEMS OF MECHANICS (FAPM-2017), (Moscow, Russia
Oct. 24-27, 2017).
Hanada, H., Tsuruta, S., Asari, K., Araki, H., Noda, H., Kashima, S.,
Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Sasaki,
H., Hasegawa, T., Yano, T., Gouda, N., Kobayashi, Y., Yamada,Y., Iwata, T.: 2017, Summary of results of experiments with theground experiment model of the telescope for ILOM (In-situ Lunar
Orientation Measurements) and future prospects, Japan Geoscience
Union Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Hanaoka, Y.: 2017, Chirality of Solar Prominences Revealed by
Polarization Observations, GAISH seminar of the Moscow State
University, (Moscow, Russia, Jun. 27, 2017).
Hanaoka, Y., Sakurai, T.: 2017, Chirality of the Magnetic Field in
Solar Filaments, Helicity Thinkshop 3, (Tokyo, Japan, Nov. 19-24,
2017).
Hanaoka, Y., Sakurai, T., IRMag Group: 2017, Statistical Study of theMagnetic Field in Solar Filaments, The 4th Asia-Pacific Solar Physics
Meeting (APSPM2017), (Kyoto, Japan, Nov. 7–10, 2017).
Hanayama, H.: 2017, Ishigakijima Astronomical Observatory and
Murikabushi 105cm Telescope, East Asia Young Astronomers
Meeting 2017, (Ishigaki, Japan, Nov. 13-17, 2017).
Hara, H.: 2017, High-speed flows and turbulent structures in eruptive
flares, Joint Hinode-11/IRIS-8 Science Meeting, (Seattle, WS, USA,
May. 30-Jun. 2, 2017).
Harada, Y., Matsumoto, K.: 2017, A Comparative Study on Tidal
Dissipation of the Solid Earth and Moon with Internal Structures
Including Low-Viscosity Layers, SELENE Symposium, (Tokyo,
Japan, Sep. 13-14, 2017).
Harada, Y., Matsumoto, K.: 2017, Tidal Dissipation of the Solid Earthwith an Internal Structure Including a Low-Viscosity Layer, JpGUAGU Joint Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Haratani, K., Yamaguchi, T., Nakajima, T., Kojima, T., Asayama, S.,
Suzuki, K., Hasegawa, Y., Watanabe, I., Uzawa, Y., Ogawa, H.,
Mizuno, A.: 2017, Development of a waveguide-type multiplexer
in 200 GHz band for simultaneous observation of atmosphericmolecular lines, The 19th East Asia Sub-millimeter-wave ReceiverTechnology Workshop, (Taipei, Taiwan, Nov. 28-30, 2017).
Hashimoto, J.: 2017, Next Step of SEEDS, Future Exploration of Star
and Planet Formation with Subaru, (Taipei, Taiwan, Dec. 7-9, 2017.
Hashimoto, J.: 2017, Aperture Masking Observations with SCExAO/CHARIS, CHARIS International Workshop, (Tokyo, Japan, Dec. 1516, 2017).
Hashimoto. T.: 2017, Kinematics in a z=7.15 Lyman Alpha Emitter
Revealed by the [OIII] 88 micron and [CII] 158 micron Lines
Detected with ALMA, East-Asia ALMA Science Workshop 2017,(Daejon, Korea, Nov. 27-29, 2017).
Hashimoto. T.: 2017, ALMA fellow program report, ALMA/45m/ASTE
Users Meeting 2017, (Mitaka, Tokyo, Japan, Dec. 26-27, 2017).
Hashimoto. T.: 2018, Kinematics in a z=7.15 Lyman Alpha Emitter
Revealed by the [OIII] 88 micron and [CII] 158 micron Lines
Detected with ALMA, Tokyo Spring Cosmic Lyman-Alpha Workshop(Sakura CLAW), (Tokyo, Japan, Mar. 26-30, 2018).

Hayano, Y., Chun, M., Packham, C., Honda, M.: 2017, Development of
extreme narrow band filter for LGS daytime use, AO4ELT5, (Tenerife,
Spain, Jun. 25-30, 2017).
Hayano, Y., Minowa, Y., Koyama, Y., Yoshida, M., Iwata, I., Hattori,
T., Clergeon, C., Tanaka, I., Takato, N., Oya, S., Takami, H.,
Akiyama, M., Kodama, T., Watanabe, T., Motohara, K., Rigaut, F.,D’orgeville, C., Arimoto, N.: 2017, Subaru Wide-Field Strategy
towards 2020, Center for AO, fall retreat, (Lake Arrowhead, CA,
USA, Oct. 19-22, 2017).
Hayashi, M.: 2017, Studies of NB emission line galaxies at z<1.5, HSC
collaboration meeting, (Sendai, Japan, May 15-17, 2017).
Hayashi, M.: 2017, Evolutionary phases of gas-rich galaxies in a galaxy
cluster at z=1.46, Early Stages of Galaxy Cluster Formation (GCF)
2017: Mergers, Proto-clusters, and Star Formation in Overdense
Environment, (Garching, Germany, Jul. 17-21, 2017).
Hayashi, M.: 2017, Evolutionary phases of gas-rich galaxies in a galaxy
cluster at z=1.46, Challenges in Galaxy Evolution: from black holes
to the cosmic web, (Florence, Italy, Aug. 28-Sep. 1, 2017).
Hayashi, M.: 2017, Molecular gas properties of galaxies in a high-z
X-ray cluster at z=1.46, Sharp Views of Galaxy Formation and
Evolution Japan-German (JSPS-DAAD) Workshop, (Sendai, Japan,
Nov. 1-3, 2017).
Heenatigala, T., Yamani, A., Canas, L., Shibata, Y.: 2018, Elevator
Pitches and Debunking Pseudoscience for Asia and Beyond,Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Higuchi, A., Kokubo, E.: 2018, Inner Solar System Objects with
Hyperbolic Orbits: Interstellar Origin or Oort Cloud Comets?, PERCInternational Symposium on Dust and Parent Bodies, (Chiba, Japan,
Feb. 26-28, 2018).
Higuchi, A., Ida, S.: 2017, Temporary Capture of Asteroids by an
Eccentric Planet, AOGS (Asia-Oceania Geosciences Society),(Suntec, Singapore, Aug. 6-11, 2017).
Higuchi, A., Kokubo, E.: 2018, Inner Solar System Objects with
Hyperbolic Orbits: Interstellar Origin or Oort Cloud Comets?, The
Transneptunian Solar System, (Coimbra, Portugal, Mar. 25-29, 2018).
Higuchi, A., Ida, S., Tanigawa, T.: 2017, Duration of temporary captureof asteroids around an eccentric planet, European Planetary Science
Congress (EPSC) 2017, (Riga, Latvia, Sep. 17-22, 2017).
Hiramatsu, M.: 2018, Public Acceptance of ALMA in Japan,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Hirata, N., Matsumoto, K., Michikami, T., Kimura, J., Kitazato, K.:
2017, Constraints on global distribution of regolith deposits on theasteroid 162173 Ryugu, JpGU-AGU Joint Meeting 2017, (Chiba,
Japan, May 20-25, 2017).
Hirota, T.: 2018, Observational experience program for high school
students at the VERA Ishigaki-jima station, Communicating
Astronomy with the Public 2018, (Fukuoka, Japan, Mar. 24-28,
2018).
Hirota, T., Kim, K. T.: 2017, Understanding high-mass star formation
through KaVA observations of water and methanol masers, 2017
Asia-Pacific Regional IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Hirota, T.: 2017, Recent progress in high-mass star-formation studies
with ALMA, East-Asia ALMA Science Workshop 2017, (Daejon,
Korea, Nov. 27-29, 2017).

Hirota, T.: 2017, Observations of submillimeter H2O and SiO lines inOrion KL region, Evolution of Molecules in Space, (Sapporo, Japan,
Jun. 27-29, 2017).
Hirota, T.: 2017, ALMA observations of submillimeter H2O and SiOlines in Orion Source I, IAU Symp. 336: Astrophysical Masers:
Unlocking the Mysteries of the Universe, (Cagliari, Italy, Sep. 4-8,2017).
Hirota, T.: 2017, Italy-Japan collaboration of high-mass star-formation
studies, Eating VLBI Workshop 2017, (Jeju, Korea, Oct. 30-Nov. 1,2017).
Hirota, T.: 2017, "Understanding high-mass star formation through
KaVA observations of water and methanol masers (2) - Second year",2017 KaVA/EAVN Joint Science Working Group Meeting, (Daejeon,
Korea, Nov. 22-23, 2017).
Hirota, T.: 2018, Future KaVA+TNRT (or extended EAVN) for Starformation Studies, NARIT Key Science Workshop: Masers &Molecular Lines in Radio Astronomy, (Chiang Mai, Thailand, Jan.
15, 2018).
Hirota, T.: 2018, ISM & Star Formation II - Chemistry, NARITSOKENDAI Winter School 2018; Astropysical Masers & Molecular
Lines in Radio Astronomy, (Chiang Mai, Thailand, Jan. 16-19, 2018).
Hirota, T.: 2018, Molecular line view in the heart of Orion Nebula,
NARIT-SOKENDAI Winter School 2018; Astropysical Masers &Molecular Lines in Radio Astronomy, (Chiang Mai, Thailand, Jan.
16-19, 2018).
Hirota, T.: 2018, High Resolution Observations of Orion Source I, High
Mass Star Formation Workshop 2018, (Yamaguchi, Japan, Mar. 2223, 2018).
Honda, R., Imanishi, Y., Tamura, Y.: 2017, Gravimetric Connection with
CG type Relative Gravimeter in Kamioka, JpGU-AGU Joint Meeting
2017, (Chiba, Japan, May 20-25, 2017).
Honma, M.: 2017, Maser Astrometry and Galactic structure studies
with VLBI, IAU Symp. 336: Astrophysical Masers: Unlocking the
Mysteries of the Universe, (Cagliari, Italy, Sep. 4-8, 2017).
Honma, M.: 2018, Maser Astrometry with VLBI and Galaxy Structure,
NARIT-SOKENDAI Winter School 2018; Astropysical Masers &Molecular Lines in Radio Astronomy, (Chiang Mai, Thailand, Jan.
16-19, 2018).
Hori, Y., Ogihara, M.: 2017, Atmospheric Growth of the TRAPPIST-1
Planets, Habitable Worlds 2017: A System Science Workshop,(Laramie, WY, USA, Nov. 13- 17, 2017).
Hori, Y., Ogihara, M.: 2017, Atmospheric Growth of a (Non-)Migrating
Planets: Application to the TRAPPIST-1 Planets, Astrobiology 2017,(Coyhaique, Chile, Nov. 26-Dec. 1, 2017).
Hwang, Y.-J., et al. including Gonzalez, A.: 2017, Performance of thefirst three preproduction 35–50 GHz receiver front-ends for atacama
large millimeter / submillimeter array, 47th European Microwave
Conference (EuMC), (Nuremberg, Germany, Oct. 10-12, 2017).
Ichikawa, K.: 2017, Is there a maximum mass for supermassive black
holes?, East Asia Young Astronomers Meeting 2017, (Ishigaki, Japan,
Nov. 13-17, 2017).
Ichikawa, K.: 2017, What TMT/MICHI tells us on AGN and Black
Holes, TMT forum 2017; Beyond First Light, (Mysuru, Indisa, Nov.
7-9, 2017).
Ichikawa, K.: 2017, The complete IR view of the Swift/BAT 70 month
AGN catalog, Elusive AGN in the next era, (Fairfax, VA, USA, Jun.

XIII Publications, Presentations185

12-15, 2017).
Ichikawa, K.: 2017, Complete Infrared view of the 70 month Swift/BAT
AGN catalog, Quasars at all cosmic epochs, (Padova, Italy, Apr. 2-7,2017).
Ichikawa, K.: 2017, Discovery of a dying AGN in Arp 187, Unveilingthe Physics Behind Extreme AGN Variability, (University of Virgin
Island, USA, Jul. 11-14, 2017).
Imanishi, M.: 2017, ALMA molecular line observations as a tool toscrutinize elusive deeply buried AGNs in luminous infrared galaxies,
Elusive AGN in the next era, (Fairfax, VA, USA, Jun. 12-15, 2017).
Imanishi, M.: 2017, ALMA molecular line observations of luminous
infrared galaxies as a tool to scrutinize elusive deeply buried AGNs,
Behind the Curtain of Dust II, (Sexten, Itary, Jul. 3-7, 2017).
Imanishi, Y., Nawa, K., Tamura, Y., Ikeda, H., Honda, R., Okada, T.,Okubo, M.: 2017, Combined use of a superconducting gravimeter and
Scintrex gravimeters for hydrological correction of measurements A superhybrid gravimetry, JpGU-AGU Joint Meeting 2017, (Chiba,
Japan, May 20-25, 2017).
Imanishi, Y., Nawa, K., Tamura, Y., Ikeda, H., Honda, R., Okada, T.,Okubo, M.: 2017, Combined use of a superconducting gravimeter and
Scintrex gravimeters for hydrological correction of precise gravity
measurements - A superhybrid gravimetry, Joint Scientific Assemblyof IAG-IASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Inoue, N.: 2018, Challenge to communicate the basics of scientific resultsfrom the solar observing satellite Hinode, Communicating Astronomy
with the Public 2018, (Fukuoka, Japan, Mar. 24–28, 2018).
Iono, D.: 2017, Extragalactic Science Using mm/submm Arrays,
XXXIInd International Union of Radio Science General Assembly &Scientific Symposium, (Montreal, Canada, Aug. 19-26, 2017).
Irimajiri, Y., Gonzalez, A., Ochiai, S., Kawakami, A., Uzawa, Y.: 2018,
Beam pattern measurements of a quasi-optical HEB mixer at 2 THz,
29th IEEE International Symposium on Space Terahertz Technology,(Pasadena, CA, USA, Mar. 26-28, 2018).
Ishiguro, M., Müller, G. T., Ďurech, J., Perna, D., Barucci, A. M.,
Kuroda, D.: 2017, Physical Characterization of (162173) Ryugu,
The JAXA HAYABUSA 2 Mission Target, From Lijiang to theOort cloud: international workshop on Solar System small bodies
exploration, (Lijiang, China, Jun. 25-27, 2017).
Ishiharu, T., Wada, T., Miyachi, A., Watanabe, K., Kaneda, H., Suzuki, T.:2017, Fabrication of silicon-supported germanium blocked impurity
band detectors for infrared astronomy, 11th International ”Hiroshima”
Symposium on the Development and Application of Semiconductor
Tracking Detectors (HSTD11) in conjunction with 2nd Workshop on
SOI Pixel Detectors (SOIPIX2017), (Okinawa, Japan, Dec. 10-15,
2017).
Ishii, M., Aoki, W.: 2018, Public relations, education and outreach on
TMT project in Japan, Communicating Astronomy with the Public
2018, (Fukuoka, Japan, Mar. 24-28, 2018).
Ishikawa, N., Agata, H., Ishizaki, M., Fujita, T., Endoh, I.: 2017,
Outreach & Education Concept and Strategy of NAOJ, 2017 AsiaPacific Regional IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Ishikawa, R., Katsukawa, Y., Antolin, P., Toriumi, S.: 2017, Temporaland Spatial Scales of Coronal Rain, Joint Hinode-11/IRIS-8 Science
Meeting, (Seattle, WS, USA, May. 30-Jun. 2, 2017).
Ishikawa, R., et al. including Okamoto, T. J., Kano, R., Song, D.,
Kubo, M., Narukage, N., Yoshida, M., Tsuzuki, T., Hara, H.,

186

XIII Publications, Presentations

Shinoda, K., Suematsu, Y., Goto, M.: 2017, CLASP2: HighPrecision Spectro-Polarimetry in Mg II h & k, Joint Hinode-11/IRIS8 Science Meeting, (Seattle, WS, USA, May. 30-Jun. 2, 2017).
Ishikawa, R.: 2017, UV spectro-polarimetry with CLASP 1 & 2
sounding rocket experiments, High-resolution Solar Physics: Past,
Present, Future NSO Workshop #30, (Sacramento Peak, NM, USA,
Aug. 7-11, 2017).
Ishizaki, M., Agata, H., NAOJ Campaign Team: 2018, Astronomical
Phenomena Observation Campaigns for general public conducted by
NAOJ, Communicating Astronomy with the Public 2018, (Fukuoka,
Japan, Mar. 24-28, 2018).
Izumi, T.: 2017, MM/submm energy diagnostic in the ALMA era,
Elusive AGN in the next era, (Fairfax, VA, USA, Jun. 12-15, 2017).
Izumi, T.: 2017, Do Circumnuclear Dense Gas Disks Drive the Growthof SMBHs?, Behind the Curtain of Dust II, (Sexten, Itary, Jul. 3-7,2017).
Izumi, T.: 2017, Feeding, feedback, and evolution of active galactic
nuclei revealed by ALMA, ALMA-J Seminar, (Tokyo, Japan, Jul. 12,2017).
Izumi, T.: 2017, Ultra-high resolution study of AGN dusty/molecular tori
and the surrounding environments, ALMA Long-Baseline Workshop,(Kyoto, Japan, Oct. 3-5, 2017).
Izumi, T.: 2017, ALMA observations of cold ISM toward AGN-hostgalaxies near and far, ISAS Seminar, (Tokyo, Japan, Oct. 26, 2017).
Izumi, T.: 2017, On the disappearance of a cold molecular torus aroundthe low-luminosity active galactic nucleus of NGC 1097, East-Asia
ALMA Science Workshop 2017, (Daejon, Korea, Nov. 27-29, 2017).
Izumi, T.: 2017, SHELLQs-ALMA: submm properties of galaxies
hosting less-luminous quasars at z > 6, Distant Galaxies from the Far
South, (Bariloche, Argentina, Dec. 11-15, 2017).
Izumi, T.: 2017, SHELLQs-ALMA: submm properties of galaxies
hosting less-luminous quasars at z > 6, East-Asia AGN Workshop
2017, (Kagoshima, Japan, Dec. 4-6, Japan).
Joshi, A. D.: 2018, Pre-Eruption Oscillations in a Quiescent Filament,
Dynamic Sun II: Solar Magnetism from Interior to the Corona, (Siem
Reap, Angkor Wat, Cambodia, Feb. 12-16, 2018).
Joshi, A. D: 2018, Statistical Study of Eruptive and Disappearing
Filaments, IAU Symp. 340: Long-term datasets for the understandingof solar and stellar magnetic cycles, (Jaipur, India, Feb. 19-24, 2018).
Jovanovic, N., Guyon, O., Kotani, T., Kawahara, H., Hosokawa, K.,
Lozi, J., Males, J., Ireland, M., Tamura, M., Mawet, D., Schwab, C.,
Norris, B., Leon-Saval, S., Betters, C., Tuthill, P.: 2017, Developing
post-coronagraphic, high-resolution spectroscopy for terrestrial planet
characterization on ELTs, AO4ELT5, (Tenerife, Spain, Jun. 25-30,
2017).
Jovanovic, N., et al. including Guyon, O., Lozi, J., Tamura, M., Kotani,T., Kawahara, H., Pathak, P.: 2017, Pioneering high contrast
science instruments for planet characterization on giant segmented
mirror telescopes, AO4ELT5, (Tenerife, Spain, Jun. 25-30, 2017).
Kajino, T.: 2017, Neutrino collective oscillation on physics of neutronstar mergers and supernovae, International Conference on Neutrino
and Nuclear Physics, (Catania, Italy, Oct. 15-21, 2017).
Kajino, T.: 2017, Galactic Chemodynamical Evolution and the Origin of
R-process Elements, Hirshegg Workshop on Neutron Star Mergers:
From Gravitational Waves to Nucleosynthesis, (Hirschegg, Austria,
Jan. 25-21, 2017).

Kajino, T.: 2017, Origin of r- and np-processes in supernovae andneutron star mergers, 16th International Symposium on Capture
Gamma-Ray Spectroscopy and Related Topics, (Sghanghai, China,
Sep. 18-22, 2017).
Kajino, T.: 2017, Solving the mystery of r-process and np-process:Merger vs. supernova, International Conference on Nuclear Physics
in Astrophysics, (Catania, Italy, Jun. 18-22, 2017).
Kajino, T.: 2017, Solving the mystery of r-process and np-process,The 14th Int. Symp. on Origin of Matter and Evolution of Galaxies(OMEG2017), (Daejeon, Korea, Jun. 27-30, 2017).
Kajino, T.: 2017, Impact of Neutron Star Merger vs. Supernova
Nucleosynthesis and Neutrino Physics, International Workshop on
Theories of Astronomical Big Bangs, (Wako, Japan, Nov. 6-10,2017).
Kajino, T.: 2017, Neutron Star Merger and Supernova Nucleosynthesis:
Impact on Neutrino Physics, International Symposium on
Perspectives of the Physics of Nuclear Structure, (Tokyo, Japan, Nov.
1-4, 2017).
Kamegai, K., Goto, A., Science Live Show UNIVERSE Members: 2018,
Communicating Astronomy in the Science Live Show UNIVERSE,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Kamegai, K., Inoue, H.: 2018, Measurement of Night Sky Brightness
with a Mobile Phone App, Communicating Astronomy with the
Public 2018, (Fukuoka, Japan, Mar. 24-28, 2018).
Kamegai, K., Yaji, K., Sugawara, R., Chimons: 2018, Science LiveShow UNIVERSE at CAP2018, Communicating Astronomy with the
Public 2018, (Fukuoka, Japan, Mar. 24-28, 2018).
Kano, R., Ishikawa, R., Winebarger, A., Auchere, F., Trujillo Bueno, J.,
Narukage, N., Kobayashi, K., Bando, T., Katsukawa, Y., Kubo,
M., Ishikawa, S., Giono, G., Hara, H., Suematsu, Y., Tsuneta, S.,
Champey, P., Belluzzi, L., Štěpán, J., De Pomtieu, B., McKenzie,D., Rachmeler, L., Okamoto, T. J., the CLASP/CLASP2 teams:
2017, Ultraviolet spectropolarimetric observations to probe the solar
chromosphere and transition region, 1st Asia-Pacific Conference on
Plasma Physics (AAPPS-DPP), (Chengdu, China, Sep. 18-22, 2017).
Karino, S., Agata, H., Canas, L.: 2018, Toward an establishment of a
GLOBAL CURRICULUM of ASTRONOMY as a comprehensive
science, Communicating Astronomy with the Public 2018, (Fukuoka,
Japan, Mar. 24-28, 2018).
Kasdin, N. J., Groff, T., Brandt, T., Currie, T., Rizzo, M., Chilcote, J.
K., Guyon, O., Jovanovic, N., Lozi, J., Norris, B., Tamura, M.:
2018, The CHARIS Integral Field Spectrograph with SCExAO: Data
Reduction and Performance, AAS Meeting #231, (Washington, D. C.,
USA, Jan, 8-12, 2018).
Kataoka, A.: 2017, millimeter-wave polarization of protoplanetarydisks: alignment or scattering?, Submm/mm/cm QUESO Workshop
2017 (QUESO2017), (Garching, Germany, Oct. 25-27, 2017).
Kataoka, A.: 2017, millimeter-wave polarization as a tool ofinvestigating the planet formation, JpGU-AGU Joint Meeting 2017,(Chiba, Japan, May 20-25, 2017).
Kataoka, A.: 2017, millimeter-wave polarization as a tool of investigating
the planet formation, East-Asia ALMA Science Workshop 2017,(Daejon, Korea, Nov. 27-29, 2017).
Kataoka, A.: 2017, Measuring the grain size in protoplanetary disks
by ALMA polarization observations, The origin of galaxies, stars,

and planets in the era of ALMA - A Symposium to honor Professor
Anneila Sargent, (Pasadena, CA, USA, Nov. 29-Dec. 1, 2017).
Kataoka, A.: 2018, Millimeter-wave polarization of protoplanetarydisks: alignment or scattering?, Magnetic Fields or Turbulence:
Which is the critical factor for the formation of stars and planetarydisks?, (Hsinchu, Taiwan, Feb. 6-9, 2018).
Kato, T., Agata, H., Usuda-Sato, K., Canas, L., Naito, S.: 2018, From
Earth to the Edge of the Universe: Mitaka software as a tool for
education and communication, Communicating Astronomy with the
Public 2018, (Fukuoka, Japan, Mar. 24-28, 2018).
Katsukawa, Y.: 2017, Power of Space-Based Spectropolarimetry for
Diagnostics of Magnetic Fields on the Solar Surface and Above, 7thSolar Orbiter Workshop, (Granada, Spain, Apr. 3-7, 2017).
Katsukawa, Y.: 2017, Temporal and height evolution of spectrum line
profiles in penumbral microjets, Joint Hinode-11/IRIS-8 Science
Meeting, (Seattle, WS, USA, May. 30-Jun. 2, 2017).
Kawabe, R.: 2018, New 50-m class Single Dish Telescope: Large
Submillimeter Telescope (LST), 2017 Asia-Pacific Regional IAU
Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Kawakami, A., Horikawa, J., Shimakage, H., Hyodo, M., Saito, S.,
Tanaka, S., Uzawa, Y.: 2017, Hot electron bolometer mixer for
operation in the mid-infrared region, 13th European Conference on
Applied Superconductivity (EUCAS2017), (Geneva, Italy, Sep. 1721, 2017).
Kawakami, A., Horikawa, J., Shimakage, H., Hyodo, M., Saito, S.,
Tanaka, S., Uzawa, Y.: 2017, Design and fabrication of mid-infrared
superconducting hot-electronbolometers, 17th International Workshop
on Low Temperature Detectors, (Kurume, Fukuoka, Japan, Jul. 1721, 2017).
Kawakami, A., Irimajiri, Y., Yamashita, T., Ochiai, S., Uzawa, Y.: 2017,
Investigation of Hot Electron Bolometer Mixer using Magnetic Thin
Film, The 19th East Asia Sub-millimeter-wave Receiver Technology
Workshop, (Taipei, Taiwan, Nov. 28-30, 2017).
Kawakami, A., Irimajiri, Y., Yamashita, T., Ochiai, S., Uzawa, Y.: 2018,
Extension of IF band of THz hot electron bolometer mixer using
magnetic thin film, 29th IEEE International Symposium on Space
Terahertz Technology, (Pasadena, CA, USA, Mar. 26-28, 2018).
Kawamura, T., Lognonné, P.: 2017, Source Time Function and Source
Parameters of Lunar Quakes and Impacts, Joint Scientific Assemblyof IAG-IASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Kawamuro, T.: 2017, Suzaku Observations of Moderately Obscured(Compton-thin) Active Galactic Nuclei Selected by Swift/BAT Hard
X-ray Survey, Elusive AGN in the next era, (Fairfax, VA, USA, Jun.
12-15, 2017).
Kawamuro, T.: 2017, AGN nuclear structure studied by X-ray spectral
analysis, and the relevance to the surrouding ionized gas, East Asia
Young Astronomers Meeting 2017, (Ishigaki, Japan, Nov. 13-17,2017).
Kawamuro, T.: 2017, AGN nuclear structure studied by X-ray spectral
analysis, and the relevance to the surrouding ionized gas, East-Asia
AGN Workshop 2017, (Kagoshima, Japan, Dec. 4-6, Japan).
Kawashima, T.: 2018, Black hole shadow images with partially-SSA
thick accretion flows: possible evidence of a highly spinning blackhole, Dawn of a new era for black hole jets in active galaxies, (Sendai,
Japan, Jan. 25-27, 2018).
Kawate, T., Ishii, T., Nakatani, Y., Ichimoto, K., Asai, A., Morita, S.,

XIII Publications, Presentations

187

Masuda, S.: 2017, Temporal Evolution and Spatial Distributionof White-light Flare Kernels in a Solar Flare, AAS Solar Physics
Division Meeting, (Portland, OR, USA, Aug. 21-25, 2017).
Kim, J., Ishiguro, M., Bach, Y. P., Kuroda, D., Naito, H., Kim, Y., Kwon,
Y. G., Imai, M., Kuramoto, Watanabe, M.: 2017, The polarimetricstudy of (331471) 1984QY1: an asteroid in comet-like orbit, 2017
FALL 97th KAS MEETING, (Yeosu, Korea, Oct. 12-13, 2017).
Kim, J.: 2017, Dynamics of jets/outflows from high-mass young stellar
objects revealed by combination of ALMA and KaVA observations,
East-Asia ALMA Science Workshop 2017, (Daejon, Korea, Nov. 2729, 2017).
Kim, J.: 2017, Dynamics of jet/outflow driven by high-mass youngstellar object revealed by KaVA 22 GHz water maser observations,
IAU Symp. 336: Astrophysical Masers: Unlocking the Mysteries of
the Universe, (Cagliari, Italy, Sep. 4-8, 2017).
Kim, J.: 2017, Dynamics of Jet/Outflow Driven by High-Mass Young
Stellar Object Revealed by KaVA 22 GHz Water Maser Observations,2017 KaVA/EAVN Joint Science Working Group Meeting, (Daejeon,
Korea, Nov. 22-23, 2017).
Kim, J.: 2018, PhD Project Presentation, NARIT-SOKENDAI WinterSchool 2018; Astropysical Masers & Molecular Lines in Radio
Astronomy, (Chiang Mai, Thailand, Jan. 16-19, 2018).
Kim, J.: 2018, Dynamics of jets/outflows driven by high mass youngstellar objects revealed by KaVA and ALMA observations, High
Mass Star Formation Workshop 2018, (Yamaguchi, Japan, Mar. 2223, 2018).
Kimura, J., Kamata, S., Matsumoto, K., Oshigami, S., Namiki, N.,
Kuramoto, K., Sasaki, S., Enya, K., Kobayashi, M., Kobayashi,S., Araki, H., Noda, H., Ishibashi, K., Saito, Y., Hussmann, H.,
Lingenauber, K.: 2017, JUICE/GALA-J (2): Science targets of the
GAnymede Laser Altimeter (GALA) for the JUICE mission, JpGUAGU Joint Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Kishikawa, R., Seita, H., Miyachi, A., Furuse, Y., Nakaoka, T.,
Yoshida, S., Nishikawa, K., Horibe, M., Kawasaki, S.: 2017, Hybrid
semiconductor integrated recitifer for wireless power transmission
into spacecraft, WPTC 2017 - Wireless Power Transfer Conference,(Taipei, Taiwan, May 10-12, 2017).
Kiuchi, H.: 2017, Photonic techniques for a Long Baseline RadioInterferometer, ALMA Long Baseline Workshop, (Kyoto, Japan, Oct.
3-5, 2017).
Kohzuma, S., Yamaoka, H., Karino, S., Ohtsuki, K.: 2018, Science pub
within local culture - An interactive communication event in Japan,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Kojima, T., Kroug, M., Gonzalez, A., Uemizu, K., Kaneko, K.,
Miyachi, A., Kozuki, Y., Shan, W., Asayama, S.: 2018, Developmentof a waveguide SIS mixer in the 275–500 GHz band and dual band
evaluation system, 29th IEEE International Symposium on Space
Terahertz Technology, (Pasadena, CA, USA, Mar. 26–28, 2018).
Kojima, T., Uzawa, Y., Shan, W.: 2018, Observation of positive gain
by a combination of quas iparticle SIS up and down frequency
converters, 29th IEEE International Symposium on Space Terahertz
Technology, (Pasadena, CA, USA, Mar. 26-28, 2018).
Kokubo, E.: 2017, Orbital Architecture of Planetary Systems Formed by
Giant Impacts, Accretion and Early Differentiation of the Earth andTerrestrial Planets, (Nice, France, May 29-Jun. 3, 2017).

188

XIII Publications, Presentations

Kokubo, E.: 2017, Orbital Architecture of Planetary Systems Formed by
Giant Impacts, Exoplanets and Planet Formation, (Shanghai, China,
Dec. 11-15, 2017).
Komatsu, Y.: 2017, Effective light absorption in photosynthesis aroundthe M star environment using excited states calculations, Astrobiology
2017, (Coyhaique, Chile, Nov. 26-Dec. 1, 2017).
Komiyama, Y.: 2017, Binary Fraction from Hyper Suprime-Cam Deep
Imaging Survey for the Local Group Dwarf Galaxies, ESO Workshop
The Impact of Binaries on Stellar Evolution, (Garching, Germany,
Jul. 3-7, 2017).
Komiyama, Y.: 2017, HSC Wide and Deep Imaging Survey for the
Milky Way Satellite Galaxies, IAU Symp. 334: Rediscovering our
Galaxy, (Potsdam, Germany, Jul. 10-14, 2017).
Koyama, Y.: 2017, Panoramic and Microscopic Views of Cluster Galaxy
Formation Near and Far, Sharp Views of Galaxy Formation and
Evolution Japan-German (JSPS-DAAD) Workshop, (Sendai, Japan,
Nov. 1-3, 2017).
Koyama, Y.: 2017, The Nature and Environment of (Dusty) StarForming Galaxies Near and Far Revealed by AKARI, The Cosmic
Wheel and the Legacy of the AKARI Archive: from galaxies andstars to planets and life, (Tokyo, Japan, Oct. 17-20, 2017).
Koyama, Y.: 2017, The nature of Hα selected galaxies along the hugecosmic web across cosmic time with Subaru, Early Stages of Galaxy
Cluster Formation (GCF) 2017: Mergers, Proto-clusters, and Star
Formation in Overdense Environment, (Garching, Germany, Jul. 1721, 2017).
Kronrod, E. V., Matsumoto, K., Kuskov, O. L., Kronrod, V. A., Yamada,R., Kamata, S.: 2018, Adjustment of Geophysical and Geochemical
Models of the Moon, 49th Lunar and Planetary Science Conference,(The Woodlands, TX, USA, Mar. 19-23, 2018).
Kronrod, E., Matsumoto, K., Yamada, R., Kuskov, O., Kronrod, V.:
2017, Internal Structure of the Moon Inferred from Apollo Seismic
Data, Selenodetic Grail and LLR Data and Thermodynamic
Constraints, JpGU-AGU Joint Meeting 2017, (Chiba, Japan, May 2025, 2017).
Kroug, M., Ezaki, E., Uemizu, K., Kojima, T.: 2017, A 275 – 500
GHz Heterodyne Receiver with High-jc SIS Junctions: Concept
and Measurements, XXXIInd International Union of Radio Science
General Assembly & Scientific Symposium, (Montreal, Canada, Aug.
19-26, 2017).
Kroug, M., Kojima, T., Fujii, Y., Ohtawara, K., Miyachi, A., Uzawa,
Y.: 2018, Noise Performance of ALMA Band10 Receivers Employing
High-Jc SIS Mixers, 29th IEEE International Symposium on Space
Terahertz Technology, (Pasadena, CA, USA, Mar. 26-28, 2018).
Kroug, M., Kojima, T., Noguchi, T.: 2017, Niobium Based SIS
Junctions with Ultra-High Current Density and Low Leakage, The
19th East Asia Sub-millimeter-wave Receiver Technology Workshop,(Taipei, Taiwan, Nov. 28-30, 2017).
Kubo, M., Katsukawa, Y., Kano, R., Ishikawa, R., Narukage, N.,
Bando, T., Suematsu, Y., Giono, G., Tsuneta, S., Ishikawa S.,
Winebarger, A., Kobayashi, K., Trujillo Bueno, J., Auchère, F.: 2017,
Discovery of Short-timescale Oscillations in the Transition Region
by CLASP, Joint Hinode-11/IRIS-8 Science Meeting, (Seattle, WS,
USA, May. 30-Jun. 2, 2017).
Kubo, M., Katsukawa, Y., Kano, R., Ishikawa, R., Narukage, N.,
Bando, T., Suematsu, Y., Giono, G., Tsuneta, S., Ishikawa S.,

Winebarger, A., Kobayashi, K., Trujillo Bueno, J., Auchère, F.: 2017,
Short-timescale Oscillations in the Transition Region by CLASP at
High “Temporal” Resolution, High-resolution Solar Physics: Past,
Present, Future NSO Workshop #30, (Sacramento Peak, NM, USA,
Aug. 7-11, 2017).
Kubo, M.: 2017, 3D Magnetic Field Configuration of Magnetic Flux
Cancellations by IBIS-Hinode-IRIS Campaign Observation, Joint
Hinode-11/IRIS-8 Science Meeting, (Seattle, WS, USA, May. 30-Jun.
2, 2017).
Kuramoto, K., et al. including Matsumoto, K., MMX study team: 2017,
Martian Moons eXploration (MMX): connecting small bodies with
habitable planets, JpGU-AGU Joint Meeting 2017, (Chiba, Japan,
May 20-25, 2017).
Kusakabe, N.: 2018, New challenges for publi outreach by Astrobiology
center of japan, Communicating Astronomy with the Public 2018,(Fukuoka, Japan, Mar. 24-28, 2018).
Kwon, Y. G., Ishiguro, M., Kuroda, D., Kawabata, K. S., Nakaoka,
T., Kawabata, M., Uemura, M., Shinnaka, Y., Akitaya, H.: 2017,
Spectropolarimetric Signals of Comet 2P/Encke During Its 2017
Apparition, 2017 FALL 97th KAS MEETING, (Yeosu, Korea, Oct.
12-13, 2017).
Lee, C.-H.: 2017, Time-domain studies of M31, East Asia Young
Astronomers Meeting 2017, (Ishigaki, Japan, Nov. 13-17, 2017).
Lee, C.-H.: 2017, A closer look at the CVSO30 exoplanet system, Know
Thy Star, Know Thy Planet, (Pasadena, CA, USA, Oct. 9-12, 2017).
Lee, C.-H.: 2017, Follow-up planetary microlensing events with SubaruAO, Sagan Summer Workshop, (Pasadena, CA, USA, Aug. 7-11,2017).
Lee, C.-H.: 2017, Time-domain studies of M31, Large Surveys of Great
Andromeda Galaxy, (Leiden, Netherlands, Jul. 1-14, 2017).
Lee, C.-H.: 2017, Time-domain studies of M31, 2017 Asia-PacificRegional IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Lee, C.-H.: 2017, Properties of eclipsing binary from all-sky surveys,
Kepler & K2 Science Conference IV, (Moffett Field, CA, USA, Jun.
19-23, 2017).
Lee, K.-S.: 2017, IRIS observation for the flares occurred at the AR
12297 during 2015 March 9-15, Daiwa-Adrian Workshop, (Holmbury
St Mary, UK, Jul. 19-21, 2017).
Lee, K.-S., Hara, H., Imada, S, Watanabe, K.: 2017, Spectroscopic andstereoscopic observation of a loop-top source of an M1.3 limb solar
flare, Joint Hinode-11/IRIS-8 Science Meeting, (Seattle, WS, USA,
May. 30-Jun. 2, 2017).
Lee, K.-S., Hara, H., Imada, S, Watanabe, K., Anand, A. D.: 2017,
Spectroscopic and stereoscopic observation of a loop-top source ofan M1.3 limb solar flare, ISEST Workshop, (Jeju, Korea, Sep. 18-22,2017).
Lee, K.-S., Hara, H., Watanabe, K., Anand, A. D., Imada, S.: 2017,
Spectroscopic observation of a loop-top source of an M1.3 limb solar
flare, The 4th Asia-Pacific Solar Physics Meeting (APSPM2017),(Kyoto, Japan, Nov. 7–10, 2017).
Lee, K.-S., Imada, S., Watanabe, K., Bamba, Y., Brooks, D. H.: 2017,
Multi-Wavelength Spectroscopic Observations of a White Light Flare
Produced Directly by Non-thermal Electrons, AAS Solar Physics
Division Meeting, (Portland, OR, USA, Aug. 21-25, 2017).
Leonardi, M.: 2018, Status of Kagra and TAMA300 squeezing
experiment, Gravitational-waves Science & technology, (Padova,

Italy, Mar. 1, 2018).
Lozi, J., Guyon, O., Jovanovic, N., Goebel, S., Pathak, P., Norris, B.,
Martinache, F., N’Diaye, M., Mazin, B., Walter, A.: 2017, SCExAO:
lessons learned for a future TMT instrument, AO4ELT5, (Tenerife,
Spain, Jun. 25-30, 2017).
Maehara, H.: 2017, Starspot activity and superflares on solar-type stars,
Kepler & K2 Science Conference IV, (Moffett Field, CA, USA, Jun.
19-23, 2017).
Maehara, H.: 2017, Starspot activity and superflares on solar-type stars,
JpGU-AGU Joint Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Maehara, H.: 2017, Starspot activity and superflares on solar-type stars,
The 4th Asia-Pacific Solar Physics Meeting (APSPM2017), (Kyoto,
Japan, Nov. 7–10, 2017).
Matsuda, Y.: 2017, The environment of submillimetre galaxies, SMG20- Twenty years of Submillimetre Galaxies: Star-forming galaxies athigh redshifts, (Durham, UK, Jul. 31-Aug. 2, 2017).
Matsuda, Y.: 2018, ALMA observations of Lyman alpha blobs at z=3.1,
Tokyo Spring Cosmic Lyman-Alpha Workshop (Sakura CLAW),(Tokyo, Japan, Mar. 26-30, 2018).
Matsumoto, K., Hirata, N.: 2018, Phobos shape and rotation modeling,
The first international meeting for MMX remote sensing consortium,(Tokyo, Japan, Mar. 9-10, 2018).
Matsuo, H., Ezawa, H., Kawamura, Y., Kubo, D., Okada, N.,
Shimomukai, R.: 2017, Compact 0.8 K Helium-4 Sorption Cooler,
17th International Workshop on Low Temperature Detectors,(Kurume, Fukuoka, Japan, Jul. 17-21, 2017).
Matsuo, H., Ezawa, H., Kiuchi, H., Honma, M., Murata, Y., Ukibe,M., Fujii, G., Shiki, S., Sakata, M.: 2018, Developments of Terahertz
Intensity Interferometry using SIS Photon Counting Detectors, 11th
Superconducting SFQ VLSI Workshop, (Tsukuba, Japan, Feb. 7-8,
2018).
Matsuo, H., Ezawa, H., Kiuchi, H., Honma, M., Murata, Y.: 2017,
Proposal of Photon Counting Terahertz Interferometry, The Cosmic
Wheel and the Legacy of the AKARI Archive: from galaxies andstars to planets and life, (Tokyo, Japan, Oct. 17-20, 2017).
Matsuo, H., Ezawa, H., Kiuchi, H., Honma, M., Murata, Y.:
2018, Prospects of Terahretz Intensity Interferometry, 29th IEEE
International Symposium on Space Terahertz Technology, (Pasadena,
CA, USA, Mar. 26-28, 2018).
Matsuo, H.: 2017, THz Interferometry from Dome A, Annual General
Meeting of AFoPS 2017, (Shanghai, China, Sep. 7-8, 2017).
Matsu’ura, R. S., Karakama, I., Umino, N., Tamura, Y., Iio, Y.,
Kasahara, M.: 2017, The current status of archives of the old analog
seismograms in Japan, and some examples of their preliminary
contribution to seismology, Joint Scientific Assembly of IAGIASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Miura, R. E., Espada, D., Matsushita, S., Martin, S.: 2017, A GMC
catalog for the Circumnuclear Disk of Centaurus A, East-Asia AGN
Workshop 2017, (Kagoshima, Japan, Dec. 4-6, Japan).
Miura, R. E., Espada, D., Nakanishi, K., Hirota, A., Sugai, H.: 2017,
Super Star Cluster Forming Cloud in the Young and Nearby Starburst
Galaxy NGC5253, Francesco’s Legacy - Star Formation in Space andTime, (Firenze, Italy, Jun. 5-9, 2017).
Miura, S., Ikeda, H., Kim, T.-H., Tamura, Y.: 2017, Comparison ofSuperconducting and Spring Gravimeters at the Mizusawa VLBI
Observatory of the National Astronomical Observatory of Japan,

XIII Publications, Presentations

189

EGU General Asembly 2017, (Vienna, Austria, Apr. 23-28, 2017).
Miura, S., Kim, T.-H., Ikeda, H., Tamura, Y.: 2017, Comparison ofSuperconducting and Spring Gravimeters at the Mizusawa VLBI
Observatory of the National Astronomical Observatory of Japan,
JpGU-AGU Joint Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Miura, S., Kim, T.-H., Ikeda, H., Tamura, Y.: 2017, Comparison ofsuperconducting and spring gravimeters at the Mizusawa VLBI
observatory of the National Astronomical Observatory of Japan, Joint
Scientific Assembly of IAG-IASPEI, (Kobe, Japan, Jul. 30-Aug. 4,2017).
Mizuno, A., Haratani, K., Iwata, H., Nakajima, T., Nagahama, T.,
Asayama, S., Kojima, T., Suzuki, K.: 2017, Development of amillimeter-wave spectrometer system equipped with a new frequency
multiplexer for multi-line observation, The Eighth Symposium on
Polar Science, (Tokyo, Japan, Dec. 4-8, 2017).
Momose, M.: 2017, Characteristics of dust particles in protoplanetarydisks: New insights obtained by ALMA, ALMA Long Baseline
Workshop, (Kyoto, Japan, Oct. 3-5, 2017).
Momose, M.: 2017, The studies of nearby star forming regions andprotoplanetary disks with ALMA, Future Exploration of Star andPlanet Formation with Subaru, (Taipei, Taiwan, Dec. 7-9, 2017).
Momose, M.: 2017, Observations of dust continuum emission at 1.3mm
from the protoplanetary disk around DG Tau, JpGU-AGU Joint
Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Moriya, T. J.: 2017, Predicted but unobserved supernovae, SouthAmerican Supernovae 2017, (La Serena, Chile, Apr. 24-26, 2017).
Moriya, T. J.: 2017, Connecting supernovae with their progenitors:
progress and open questions, Evolution and Explosion of Massive
Stars, (Dublin, Ireland, May 25-26, 2017).
Moriya, T. J.: 2017, Theories of superluminous supernovae, Fifty-One
Erg 2017, (Corvallis, OR, USA, Jun. 5-8, 2017).
Moriya, T. J.: 2017, The interaction of ejecta with the CSM/ISM, Eta
Carinae, LBVs, and Supernova Impostors, (Pittsburgh, PA, USA, Jun.
19-23, 2017).
Moriya, T. J.: 2017, How can magnetars mimic 56 Ni decay?,
Superluminous supernovae in the next decade, (Garching, Germany,
May 2-26, 2017).
Moriya, T. J.: 2017, Interaction in Type IIP Sne, Evolution and
Explosion of Massive Stars, (Dublin, Ireland, May 25-26, 2017).
Moriya, T. J.: 2017, Finding supernovae at the reionization era with
Subaru and WFIRST, WFIRST-Subaru synergitic observation
workshop, (Tokyo, Japan, Dec. 18-20, 2017).
Murdoch, N., Kenda, B., Kawamura, T., Spiga, A., Lognonné, P.,
Mimoun, D., Banerdt, W. B.: 2017, Simulating the seismic pressure
noise on Mars, European Planetary Science Congress (EPSC) 2017,(Riga, Latvia, Sep. 17-22, 2017).
Nagai, H.: 2017, ALMA Polarimetric Observations Of Centaurus A,
Submm/mm/cm QUESO Workshop 2017 (QUESO2017), (Garching,
Germany, Oct. 25-27, 2017).
Nagai, H.: 2017, Accretion Flow Properties of NGC 1275: A View
Through Faraday Screen, Polarised Emission from Astrophysical Jets,(Ierapetra, Greece, Jun. 12-16, 2017).
Nagai, T., Agata, H., Itoh, S.: 2018, Astronomical communication
activities through business, Communicating Astronomy with the
Public 2018, (Fukuoka, Japan, Mar. 24-28, 2018).
Naito, S., Takanashi, N., Sensui, T., Tsuchiya, T., Uriu, K., RTC

190

XIII Publications, Presentations

administration team: 2018, The TENPLA Project : Communicating
Astronomy in the urban life – The activity of Roppongi Tenmon
Club, Communicating Astronomy with the Public 2018, (Fukuoka,
Japan, Mar. 24-28, 2018).
Nakamura, K., Fujimoto, M.-K.: 2017, Double Balanced Homodyne
Detection, 18th KAGRA face to face meeting, (Tokyo, Japan, Dec.
5-6, 2017).
Nakamura, K., Fujimoto, M.-K.: 2017, Double Balanced Homodyne
Detection, 27th workshop on General Relativity and Gravitation in
Japan, (Hiroshima, Japan, Nov. 27-Dec. 1, 2017).
Nakamura, K., Fujimoto, M.-K.: 2018, Double Balanced Homodyne
Detection, YKIS2018a Symposium: General Relativity - The Next
Generation -, (Kyoto, Japan, Feb. 19-23, 2018).
Nakamura, K., Fujimoto, M.-K.: 2018, Double Balanced Homodyne
Detection, The First Annual Area Symposium of Innovateve Area:
Gravitational Wave Physics and Astronomy: Genesis, (Chiba, Japan,
Mar. 5-7, 2018).
Narukage, N., Ishikawa, S.: 2017, Soft X-ray Photon Counting
Capability of a Back-Illuminated High-Speed CMOS Sensor, 8thInternational Conference on New Developments in Photodetection,(Tours, France, Jul. 3-7, 2017).
Narukage, N.: 2017, X-ray imaging-spectrometers for the next solar
satellite mission, RHESSI 16th Workshop / MinXSS 1st Workshop,(Boulder, CO, USA, Jun. 19-24, 2017).
Narukage, N.: 2017, Photon counting type imaging spectrometer forsolar soft x-rays, SPIE Optical Engineering + Applications, (San
Diego, CA, USA, Aug. 6-10, 2017).
N’Diaye, M., Martinache, F., Jovanovic, N., Lozi, J., Guyon, O., Norris,
B., Ceau, A., Mary, D.: 2017, Mitigate the impact of ELT architecture
on AO performance: learn from today s telescopes to characterize
and prevent the island effect, AO4ELT5, (Tenerife, Spain, Jun. 25-30,
2017).
Nozawa, T.: 2017, Dust Formation Theory in Astronomical
Environments, Fifty-One Erg 2017, (Corvallis, OR, USA, Jun. 5-8,2017).
Ogawa, K., Kawamura, T., Ishihara, Y., Tsuji, T., Kobayashi, T.,
Yamada, R., Araya, A., Tanaka, S., Takeuchi, N.: 2017, Conceptual
Study of Small Active Seismic Exploration Package on Moons andSmall Bodies, Joint Scientific Assembly of IAG-IASPEI, (Kobe,
Japan, Jul. 30-Aug. 4, 2017).
Ogihara, M.: 2017, Formation of close-in super-Earths in disks evloving
via disk winds, Accretion and Early Differentiation of the Earth andTerrestrial Planets, (Nice, France, May 29-Jun. 3, 2017).
Ogihara, M.: 2017, Formation of close-in super-Earths in disks evolving
via disk winds and implications for the origin of outer planets,
Exocllipse 2017, (Boise, ID, USA, Aug. 20-24, 2017).
Ogihara, M.: 2018, Formation of close-in super-Earths in a disk
evolving via disk winds, DTA Symposium VIII: Challenge to SuperEarths and Their Atmospheres, (Mitaka, Tokyo, Japan, Mar. 6-8,
2017).
Ogihara, M.: 2017, Effects of magntically driven disk winds on type I
migration, JpGU-AGU Joint Meeting 2017, (Chiba, Japan, May 2025, 2017).
Ohgoe, O.: 2018, Popularization of solar eclipse observation by“Nissyoku Jyouhou Center (the solar eclipse information center ofJapan)”, Communicating Astronomy with the Public 2018, (Fukuoka,

Japan, Mar. 24-28, 2018).
Ohya, K., Miyachi, A., Tachikawa, S., Sakurai, A., Nagasaka, Y.: 2017,
Evaluation of IR emitter with periodic array for spacecraft radiator,
68th International Astronautical Congress 2017, (Adelaide, Australia,
Sep. 25-29, 2017).
Oi, Y., Yokoyama, T., Toriumi, S.: 2017, MHD Simulations of Formationand Eruption of a Magnetic Flux Rope in a Quadrupolar Active
Region with a Delta-Sunspot, Flux Emergence Workshop 2017,(Budapest, Hungary, Jun. 12-16, 2017).
Oka, T.: 2017, Galactic Center Studies with ALMA Long Baselines,
ALMA Long Baseline Workshop, (Kyoto, Japan, Oct. 3-5, 2017).
Oka, T.: 2017, Signature of Past Star Forming Activity in the Central
Molecular Zone of Our Galaxy, SFDE17: from Local Clouds toDistant Galaxies, (Quy Nhon, Vietnam, Aug. 7-11, 2017).
Okamoto, J., Sakurai, T.: 2017, The Strongest Magnetic Field in
Sunspots, Joint Hinode-11/IRIS-8 Science Meeting, (Seattle, WS,
USA, May. 30-Jun. 2, 2017).
Okamoto, J., Sakurai, T.: 2017, The Strongest Magnetic Field in
Sunspots, AGU Fall Meeting 2017, (New Orleans, LA, USA, Dec.
11-15, 2017).
Okamoto, J.: 2017, Solar MHD phenomena observed by Hinode,
1st Asia-Pacific Conference on Plasma Physics (AAPPS-DPP),(Chengdu, China, Sep. 18-22, 2017).
Onoue, M.: 2018, Studies of Quasar Contribution to Reionizationand Early Growth of SMBHs with Subaru Wide-field Surveys,
Cosmological Signals from Cosmic Dawn to the Present, (Aspen,
CO, USA, Feb. 5-9, 2018).
Orienti, M., Brunetti, G., Mack, K.-H., Nagai, H., Paladino, R., Prieto,M. A.: 2017, ALMA Polarization Observations Of The Particle
Accelerators In The Peculiar Hot Spot 3C 445 South, Submm/mm/cm
QUESO Workshop 2017 (QUESO2017), (Garching, Germany, Oct.
25-27, 2017).
Otsubo, T., Matsuo, K., Aoyama, Y., Yamamoto, K., Hobiger, T., Kubooka, T., Sekido, M., Hugentobler, U., Koenig, R.: 2017, Effective
expansion of satellite laser ranging network for improving geodetic
products and satellite orbits, Joint Scientific Assembly of IAGIASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Oyama, T.: 2017, First simultaneous mapping of four 7 mm SiO maserlines using the new broad band VLBI System (OCTAVE-system),
IAU Symp. 336: Astrophysical Masers: Unlocking the Mysteries of
the Universe, (Cagliari, Italy, Sep. 4-8, 2017).
Pathak, P., Guyon, O., Jovanovic, N., Lozi, J., Martinache, F.,
Minowa, Y., Kudo, T., Kotani, T., Takami, H.: 2017, Closed-loop
atmospheric dispersion compensation: on-sky demonstration of
sub-milliarcsecond residual dispersion across H-band, AO4ELT5,(Tenerife, Spain, Jun. 25-30, 2017).
Pigulski, A., et al including Kambe, E., Ukita, N.: 2017, tau Ori and tau
Lib: Two new massive heartbeat binaries, The Third BRITE Science
Conference, (Quebec, Canada, Aug. 7-10, 2017).
Quintero Noda, C., Katsukawa, Y., Kubo, M., Shimizu, T., Oba,
T., Anan, T., Ichimoto, K., Hara, H., Suematsu, Y.: 2017,
Chromospheric polarimetry through multi-line observations of the
770 nm and 850 nm spectral regions, 15th Euroepan Solar Physics
Meeting, (Budapest, Hungary, Sep. 4-8, 2017).
Quintero Noda, C., Katsukawa, Y., Kubo, M., Shimizu, T., the Sunrise/
SCIP Team: 2017, Chromospheric polarimetry through multi-line

observations of the 770 and 850 nm spectral regions, The 4th AsiaPacific Solar Physics Meeting (APSPM2017), (Kyoto, Japan, Nov.
7–10, 2017).
Rusu, C. E.: 2017, Subaru Telescope Adaptive Optics Observationsof Gravitationally Lensed Quasars, East Asia Young Astronomers
Meeting 2017, (Ishigaki, Japan, Nov. 13-17, 2017).
Sagawa, H., Takagi, M., Maezawa, H., Saigo, K.: 2017, Venus upper
atmospheric dynamics inferred from the Doppler-shift observationsof submm CO line: Comparison with GCM experiments, European
Planetary Science Congress (EPSC) 2017, (Riga, Latvia, Sep. 17-22,2017).
Sai, J., Ohashi, N., Saigo, K., Matsumoto, T., Takakuwa, S., Saito, M.,
Aso, Y., Aikawa, Y., Kurose, I., Yen, H.-W., Tomisaka, K., Tomida, K.,
Machida M.: 2017, ALMA Cycle 2 Observations of Class I Protostar
L1489 IRS: Misaligned Disk Structure, East-Asia ALMA Science
Workshop 2017, (Daejon, Korea, Nov. 27-29, 2017).
Saito, T., Iono, D., Takakuwa, S., Tsukamoto, Y., Kanagawa, K., Saigo,
K., Kawabe R.: 2018, Assessing the Future Capability of ALMA at
50 km Baselines, ALMA Long Baseline Workshop, (Kyoto, Japan,
Oct. 3-5, 2017).
Saito, T.: 2017, Revealing Physical, Chemical, and Morphological
Structures of Nearby Luminous Infrared Galaxies, Behind the Curtainof Dust II, (Sexten, Itary, Jul. 3-7, 2017).
Sakai, D.: 2017, VLBI astrometry of a water maser source in the Sgr
B2 complex with VERA, IAU Symp. 336: Astrophysical Masers:
Unlocking the Mysteries of the Universe, (Cagliari, Italy, Sep. 4-8,2017).
Sakai, N.: 2017, Eight new astrometry results of 6.7 GHz CH3OH and 22
GHz H2O masers in the Perseus arm, IAU Symp. 336: Astrophysical
Masers: Unlocking the Mysteries of the Universe, (Cagliari, Italy,
Sep. 4-8, 2017).
Sakai, N.: 2017, Progress and Timeline for KaVA Astrometry Mode
Open, 2017 KaVA/EAVN Joint Science Working Group Meeting,(Daejeon, Korea, Nov. 22-23, 2017).
Schulze, A.: 2017, New constraints on the black hole spin in radio-loudquasars, Quasars at all cosmic epochs, (Padova, Italy, Apr. 2-7, 2017).
Schulze, A.: 2017, The active black hole mass function at z~4 fromCOSMOS and SDSS, COSMOS Team Meeting 2017., (Kyoto, Japan,
Jul. 4-7, 2017).
Schulze, A.: 2017, New constraints on the black hole spin in radio-loudquasars, East Asia Young Astronomers Meeting 2017, (Ishigaki,
Japan, Nov. 13-17, 2017).
Schulze, A.: 2017, The nature of luminous LoBAL quasars revealed bynear-IR spectroscopy, East-Asia AGN Workshop 2017, (Kagoshima,
Japan, Dec. 4-6, Japan).
Sekiguchi, K., OISTER Team: 2017, Time Domain Studies by OISTER
Collaboration, IAU Symp. 339: Southern Horizons in Time-Domain
Astronomy, (Stellenbosch, South Africa, Nov. 13-17, 2017).
Sekii, T.: 2018, Solar space missions: Japanese plans, Future Directions
in Heliophysics, (Abu Dhabi, UAE, Jan. 16-19, 2018).
Sekii, T.: 2018, Stellar rotation inferred by asteroseismology,
Asteroseismology and its impact on other branches of astronomy,(Tokyo, Japan, Mar. 19-20, 2018).
Shan, W.: 2017, Accurate Measurement of Gain Saturation ofSuperconductor-Insulator-Superconductor, 17th International
Workshop on Low Temperature Detectors, (Kurume, Fukuoka, Japan,

XIII Publications, Presentations

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Jul. 17-21, 2017).
Shan, W., Ezaki, S., Asayama, S., Noguchi, T., Iguchi, S.: 2018,
Planar-integration of Arrayed SIS Receiver Frontends, 29th IEEE
International Symposium on Space Terahertz Technology, (Pasadena,
CA, USA, Mar. 26-28, 2018).
Shibata, Y., Heenatigala, T., Usuda-Sato, K.: 2017, Collaboration in
the Astronomy Translation Network, UNAWE (Universe Awareness)
Japan Workshop, (Shizuoka, Japan, Apr 5-6, 2017).
Shibata, Y., Usuda-Sato, K., Canas, L.: 2017, Astronomy Translation
Network - A Global Need for EPO, 2017 Asia-Pacific Regional IAU
Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Shibata, Y., Usuda-Sato, K., Simard, G., Heenatigala, T., Canas L.,
Cheung, S. L., Agata, H.: 2018, Astronomy Translation Network:
the Challenges of Translating Astronomy Resources Globally,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Shimojo, M., et al. including Hirota, A., Sawada, T., Asayama,S., Sugimoto, M.: 2017, New window of solar physics: Solarobservations with ALMA, Joint Hinode-11/IRIS-8 Science Meeting,(Seattle, WS, USA, May. 30-Jun. 2, 2017).
Shimojo, M., Hudson, H. S., White, S. M., Bastian, T. S., Iwai, K.:
2017, The First ALMA Observation of a Solar Plasmoid Ejection
from an X-ray Bright Point, URSI 2017 General Assembly & Science
Symposiums: HJ24: Solar, Planetary, and Heliospheric Radio
Emissions, (Montreal, Canada, Aug. 28-26, 2017).
Shimojo, M., Hudson, H. S., White, S. M., Bastian, T. S., Iwai, K.: 2017,
The First ALMA Observation of a Solar Plasmoid Ejection from an
X-ray Bright Point, AGU Fall Meeting 2017, (New Orleans, LA,
USA, Dec. 11-15, 2017).
Shimojo, M., Iwai, K., Asai, A., Nozawa, S., Minamidani, T., Saito, M.:
2017, Variation of the Solar Microwave Spectrum in the Last Half
Century, The 4th Asia-Pacific Solar Physics Meeting (APSPM2017),(Kyoto, Japan, Nov. 7–10, 2017).
Shinozaki, B., Ezaki, S., Odou, T., Makise, K., Asano T.: 2017,
Superconducting Fluctuations above Tc and pair breaking parametersof two dimensional Niobium Nitride Films, 28th International
Conference on Low Temperature Physics, (Gothenburg, Sweden,
Aug. 9-16, 2017).
Shirasaki, Y.: 2017, Clustering of galaxies around AGN in the HSC
Wide survey, East-Asia AGN Workshop 2017, (Kagoshima, Japan,
Dec. 4-6, Japan).
Sôma, M.: 2018, Date of Christ's Crucifixion, Indian Institute of
Astrophysics Extramural Talk, (Bengaluru, India, Mar. 5, 2018).
Sôma, M.: 2018, Earth rotation determined from occultation records,
Importance of Records of Ancient Eclipses for History of Astronomy,(Bengaluru, India, Mar. 3, 2018).
Song, D., Chae, J., Kwak, H., Kano, R., Yurchyshyn, V., Moon, Y.,
Lim, E., Lee, J.: 2017, Three-minute Sunspot Oscillations Driven by
Magnetic Reconnection in a Light Bridge, The 4th Asia-Pacific Solar
Physics Meeting (APSPM2017), (Kyoto, Japan, Nov. 7–10, 2017).
Sotani, H.: 2017, Gravitational wave asteroseismology with protoneutronstars, 29th International Texas Symposium on Relativistic
Astrophysics, (Cape Town, South Africa, Dec. 3-8, 2017).
Sotani, H.: 2017, Pulse profiles from a pulsar in scalar-tensor gravity,
29th International Texas Symposium on Relativistic Astrophysics,(Cape Town, South Africa, Dec. 3-8, 2017).

192

XIII Publications, Presentations

Sotani, H.: 2017, Imprint of nuclear bubble structure in torsional
oscillations, 29th International Texas Symposium on Relativistic
Astrophysics, (Cape Town, South Africa, Dec. 3-8, 2017).
Squires, G., Brewer, J., Dawson, S., Okada, S., Garnier, W., Hiramatsu,
M., Russo, P., Yamaoka, H., Yurkewic, K.: 2018, Practical tools for“Making the Case” for Workforce, Education, Public Outreach &Communication, Communicating Astronomy with the Public 2018,(Fukuoka, Japan, Mar. 24-28, 2018).
Suematsu, Y.: 2017, High Resolution Observations of Solar Spicules:
Model Constraints, High-resolution Solar Physics: Past, Present,
Future NSO Workshop #30, (Sacramento Peak, NM, USA, Aug. 7-11,2017).
Suematsu, Y.: 2017, Observational Constraints on the Formation Models
of Chromospheric Spicules, Joint Hinode-11/IRIS-8 Science Meeting,(Seattle, WS, USA, May. 30-Jun. 2, 2017).
Suematsu, Y.: 2017, High Resolution Observations of Spicules in UpperPhotospheric Lines, The 4th Asia-Pacific Solar Physics Meeting(APSPM2017), (Kyoto, Japan, Nov. 7–10, 2017).
Sugiyama, K., Yonekura, Y., Saito, Y., Nagase, K., Yasui, Y., Satoh,
H., Miyamoto, Y., Aoki, K., Yamaguchi, T., Momose, M., Motogi,
K., Fujisawa, K., Honma, M., Uchiyama, M., Matsumoto, N.,
Hachisuka, K., Inayoshi, K., Tanaka, K., Hosokawa, T.: 2017, Longterm and highly frequent monitor of the 6.7 GHz methanol masers
to research periodic flux variations using Hitachi 32-m, 2017 AsiaPacific Regional IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Sugiyama, K.: 2017, Long-term and highly frequent monitor of 6.7
GHz methanol masers to statistically research periodic flux variations
around high-mass protostars using Hitachi 32-m, IAU Symp. 336:
Astrophysical Masers: Unlocking the Mysteries of the Universe,(Cagliari, Italy, Sep. 4-8, 2017).
Sugiyama, K.: 2017, KaVA PET Activities and New Observation Modesin 2018A, 2017 KaVA/EAVN Joint Science Working Group Meeting,(Daejeon, Korea, Nov. 22-23, 2017).
Sugiyama, K.: 2018, Collaboration with the 40-m TNRT through flux
variability of masers, NARIT Key Science Workshop: Masers &Molecular Lines in Radio Astronomy, (Chiang Mai, Thailand, Jan.
15, 2018).
Sugiyama, K.: 2018, Flux Variability of Masers, NARIT-SOKENDAI
Winter School 2018; Astropysical Masers & Molecular Lines inRadio Astronomy, (Chiang Mai, Thailand, Jan. 16-19, 2018).
Sugiyama, K.: 2018, Periodic Flux Variability in High-mass Star
Forming Regions, High Mass Star Formation Workshop 2018,(Yamaguchi, Japan, Mar. 22-23, 2018).
Sunada, K.: 2017, VERA single-dish observations, IAU Symp. 336:
Astrophysical Masers: Unlocking the Mysteries of the Universe,(Cagliari, Italy, Sep. 4-8, 2017).
Suzuki, R., Harakawa, H., Schoeck, M., Ellerbroek, B.: 2017,
Instrument requirements for precision relative astrometry using TMT/
IRIS, AO4ELT5, (Tenerife, Spain, Jun. 25-30, 2017).
Suzuki, T., Kodama, T., Tadaki, K.-i., Hayashi, M., Koyama, Y.,
Shimakawa, R., Tanaka, I., Minowa, Y., Yamamoto, M., Sobral,D., Smail, I., Best, P. N.: 2017, Star-forming activity and interstellar
medium conditions of the [OIII]-selected galaxies before the peak
epoch, Galaxy Evolution Across Time, (Paris, France, Jun. 12-16,
2017).
Suzuki, T., Ohishi, M., Saito, M., Hirota, T., Liton, M., Wakelam,

V.: 2017, Formation process to glycine with suprathermal hydrogenatoms, Astrobiology 2017, (Coyhaique, Chile, Nov. 26-Dec. 1, 2017).
Suzuki, T.: 2017, Star-forming activity and interstellar medium conitionsof [OIII]-selected galaxies at z~3.2, Challenges in Galaxy Evolution:from black holes to the cosmic web, (Florence, Italy, Aug. 28-Sep. 1,
2017).
Tadaki, K.: 2017, ALMA view of high-redshift galaxies, East-Asia
ALMA Science Workshop 2017, (Daejon, Korea, Nov. 27-29, 2017).
Tadaki, K.: 2017, Bulge formation in the most massive galaxies at
z=2, The Physics of Quenching Massive Galaxies at High Redshift ,(Leiden, Netherlands, Nov. 6-10, 2017).
Tadaki, K.: 2017, Rotating starburst cores in the most massive galaxies
at z=2, Galaxy Evolution Across Time, (Paris, France, Jun. 12-16,
2017).
Takagi, K., Tsunekawa, S., Kobayashi, K., Hirota, T., Matsushima,F.: 2018, Microwave Zeman Effect of Methanol, The 2nd Asian
Workshop on Molecular Spectroscopy, (Taoyuan, Taiwan, Mar. 9-10,2018).
Takagi, Y.: 2017, Revealing the Evolution Timescale of Protoplanetary
Disks with High-resolution Spectroscopy, Future Exploration of Star
and Planet Formation with Subaru, (Taipei, Taiwan, Dec. 7-9, 2017.
Takahashi, H. R.: 2017, Radiation Magnetohydrodynamic Simulationsof Accretion Flows and Outflows, AAPPS-DPP, (Cheng Du, China,
Sep. 18-23, 2017).
Takahashi, R.: 2017, Installation status of vibration isolation system,
The 3rd International Meeting on KAGRA, (Taipei, Taiwan, May 2122, 2017).
Takeda, Y.: 2018, Spectroscopic analysis of red giants in the Kepler
field: stellar parameters and chemical abundances, Asteroseismology
and its impact on other branches of astronomy, (Tokyo, Japan, Mar.
19-20, 2018).
Takiwaki, T.: 2017, Three dimensional simulation of core-collapse
supernovae: effect of stellar rotation, Fifty-One Erg 2017, (Corvallis,
OR, USA, Jun. 5-8, 2017).
Takiwaki, T.: 2017, Rotation aided neutrino driven explosion, Workshop
on The Progenitor-Supernova-Remnant Connection, (Ringberg,
Germany, Jul. 24-29, 2017).
Takiwaki, T.: 2017, Three dimensional simulations of rapidly rotatingcore-collapse supernovae, IAU Symp. 339: Southern Horizons in
Time-Domain Astronomy, (Stellenbosch, South Africa, Nov. 13-17,2017).
Takiwaki, T.: 2017, Oblate Supernova Explosions Aided by Rotation,
Deciphering the Violent Universe, (Playa del Carmen, Mexico, Dec.
11-15, 2017).
Takiwaki, T.: 2018, C01 Progress Report, The First Annual Area
Symposium of Innovateve Area: Gravitational Wave Physics andAstronomy: Genesis, (Chiba, Japan, Mar. 5-7, 2018).
Tamura, M., Murakami, N., Yamada, T.: 2018, Japanese Participation to
WFIRST, The Stanford Meeting, (Pasadena, CA, USA, Mar. 2018).
Tamura, M.: 2017, Habitable Planet Seraches around Red Dwarfs:
Ground and Space, JpGU-AGU Joint Meeting 2017, (Chiba, Japan,
May 20-25, 2017).
Tamura, M.: 2017, Direct Imaging of Giant Exoplanets and Disks, 10th
RESCEU/Planet2 Symposium: Planet Formation around Snowline,(Tokyo, Japan, Nov. 28-30, 2017).
Tamura, M.: 2017, Subaru SCExAO/CHARIS/IRD: Synergy on

exoplanet sciences, WFIRST-Subaru synergitic observation
workshop, (Tokyo, Japan, Dec. 18-20, 2017).
Tamura, Y., Imanishi, Y., Ikeda, H., Nawa, K., Sugihara, M., Miyakawa,A.: 2017, Twelve Years of Gravity Observation at Kamioka witha Superconducting Gravimeter, JpGU-AGU Joint Meeting 2017,(Chiba, Japan, May 20-25, 2017).
Tamura, Y., Jike, T., Manabe, S.: 2017, Geodetic Observations in
Mizusawa VLBI Observatory, Joint Scientific Assembly of IAGIASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Tanaka, I.: 2017, Subaru Studies of the Ha Emitters in the 4C+23.56
protocluster at z=2.49, Sharp Views of Galaxy Formation and
Evolution Japan-German (JSPS-DAAD) Workshop, (Sendai, Japan,
Nov. 1-3, 2017).
Tanaka, M.: 2017, Hyper Suprime-Cam Subaru Strategic Program,
LSST School and Workshop: Getting ready to do science with LSST,(Lyon, France, Jun. 14, 2017).
Tanaka, M.: 2017, Overview of HSC Photo-z's, Photometric Redshifts
for Large Surveys 2017, (Sendai, Japan, May 18, 2017).
Tanaka, M.: 2017, Kilonova Emission from Compact Binary
Mergers: Opacities of Lanthanide-rich and Lanthanide-free Ejecta,
Electromagnetic Signatures of r-process Nucleosynthesis in NeutronStar Binary Mergers, (Seattle, WA, USA, Jul. 24-Aug. 18, 2017).
Tanaka, M.: 2017, Optical/NIR Follow-up Observations of NeutronStar Mergers, The Physics of Extreme-Gravity Stars, (Stockholm,
Sweden, Jun. 5-30, 2017).
Tanaka, M.: 2017, Kilonova/Macronova Emission from Neutron Star
Mergers, Deciphering the Violent Universe, (Playa del Carmen,
Mexico, Dec. 11-15, 2017).
Tanaka, M.: 2017, Optical/NIR Spectroscopy of GW Sources, TMT
Science Forum 2017, (Mysore, India, Nov. 7-9, 2017).
Tanaka, M.: 2017, Gravitational Wave Sources: NS mergers, kilonovae,
and the origin of r-process elements, Stellar Evolution, Supernova
Nucleosynthesis Across Cosmic Time, (Chiba, Japan, Sep. 18-29,
2017).
Tanaka, M.: 2017, Opacites and light curves of kilonovae,
Electromagnetic Signatures of r-process Nucleosynthesis in NeutronStar Binary Mergers, (Seattle, WA, USA, Jul. 24-Aug. 18, 2017).
Tanaka, M.: 2017, Overview: Kilonova, Electromagnetic Signatures ofr-process Nucleosynthesis in Neutron Star Binary Mergers, (Seattle,
WA, USA, Jul. 24-Aug. 18, 2017).
Tanaka, M.: 2017, Kilonova/Macronova Emission from Dynamical andWind Ejecta of Compact Binary Mergers, The Physics of ExtremeGravity Stars, (Stockholm, Sweden, Jun. 5-30, 2017).
Tanaka, M.: 2018, Time domain astronomy and gravitational wave
sources, CREST International Symposium on Big Data Application,(Tokyo, Japan, Jan. 16-17, 2018).
Tanaka, Y.: 2018, Constraint on the magnetic fields of exoplanets byradio observations and future expectations, ALMA workshop forsolar system planetary observation, (Mitaka, Japan, Mar. 7-8, 2018).
Tanikawa, K.: 2018, The Astronomical Aspect of the Locality of a
Civilization, Indian Institute of Astrophysics Extramural Talk,(Bengaluru, India, Mar. 2, 2018).
Tanikawa, K.: 2018, Short-term variations of Delta T and climatechanges, Importance of Records of Ancient Eclipses for History of
Astronomy, (Bengaluru, India, Mar. 3, 2018).
Tazaki, F., Hada, K., Honma, M., Akiyama, K., Ikeda, S., Kuramochi,

XIII Publications, Presentations

193

K.: 2017, Super-resolution Imaging of Jet Base and Core of M87 at
10-100 Rs Scale with Sparse Modeling, 2017 Asia-Pacific Regional
IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Terai, T., Yoshida, F.: 2017, Jupiter Trojan Survey with Subaru/Hyper
Suprime-Cam, Asteroids, Comets, Meteors 2017, (Montevideo,
Urugai, April 10-14, 2017).
Toriumi, S., Katsukawa, Y., Cheung, M. C. M.: 2017, Various Local
Heating Events in the Earliest Phase of Flux Emergence, Joint
Hinode-11/IRIS-8 Science Meeting, (Seattle, WS, USA, May. 30-Jun.
2, 2017).
Toriumi, S., Katsukawa, Y., Cheung, M. C. M.: 2017, Various Local
Heating Events in the Earliest Phase of Flux Emergence, Flux
Emergence Workshop 2017, (Budapest, Hungary, Jun. 12-16, 2017).
Toriumi, S., Sakurai, T.: 2017, Largest Sunspots in History: Magnetic
Flux Content, Emergence Rate, and Generation Mechanism, Joint
Hinode-11/IRIS-8 Science Meeting, (Seattle, WS, USA, May. 30-Jun.
2, 2017).
Toriumi, S., Schrijver, C. J., Harra, L. K., Hudson, H., Nagashima, K.:
2017, Magnetic Properties of Solar Active Regions that Govern Large
Solar Flares and Eruptions, Joint Hinode-11/IRIS-8 Science Meeting,(Seattle, WS, USA, May. 30-Jun. 2, 2017).
Toriumi, S., Schrijver, C. J., Harra, L. K., Hudson, H., Nagashima, K.:
2017, Magnetic Properties of Solar Active Regions that Govern Large
Solar Flares and Eruptions, 48th SPD Meeting, (Portland, OR, USA,
Aug. 21-25, 2017).
Toriumi, S., Takasao, S.: 2017, Numerical Modeling of Flare-productive
Active Regions of the Sun, AGU Fall Meeting 2017, (New Orleans,
LA, USA, Dec. 11-15, 2017).
Toriumi, S.: 2017, Observation and Modeling of Flare-productive Active
Regions, Flux Emergence Workshop 2017, (Budapest, Hungary, Jun.
12-16, 2017).
Toriumi, S.: 2017, Physical Processes of Flux Emergence and Active
Region Formation, The 4th Asia-Pacific Solar Physics Meeting(APSPM2017), (Kyoto, Japan, Nov. 7–10, 2017).
Toriumi, S.: 2017, Observation and Modeling of Flare-productive Active
Regions of the Sun, Helicity Thinkshop 3, (Tokyo, Japan, Nov. 19-24,
2017).
Tsujimoto, T.: 2017, r-process enrichment traced by Pu and Ba near
the sun and in the Draco, Observational Signatures of r-process
nucleosynthesis in neutron star mergers, (Seattle, WS, USA, Jul. 31Aug. 4, 2017).
Tsujimoto, T.: 2017, Galactic Archaeology with Planetary Nebula study,
Planetary Nebula Research with Subaru Telescope in the Era ofInternational Partnership, (Hong Kong, China, Dec. 11-13, 2017).
Uemura, R., Masuda, S., Kano, R.: 2017, Statistical Study of Activeregion Microflares Observed with Hinode/XRT, The 4th Asia-Pacific
Solar Physics Meeting (APSPM2017), (Kyoto, Japan, Nov. 7–10,
2017).
Usuda, T.: 2017, Thirty Meter Telescope (TMT) Project Status, 2017
Asia-Pacific Regional IAU Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Usuda, T.: 2017, Japan's Contributions for TMT (Thirty Meter
Telescope), The 22d "Science in Japan" Forum US-Japan Astronomy:
Partnerships & Opportunities, (Cosmos Club, Washington, D.C.,
USA, Jun. 9, 2017).
Usuda-Sato, K.: 2017, Presentations at preschools and kindergartens in
Hawai`i, UNAWE (Universe Awareness) Japan Workshop, (Shizuoka,

194

XIII Publications, Presentations

Japan, Apr 5-6, 2017).
Usuda-Sato, K.: 2017, Inclusivity and NAOJ Mitaka Visitors' Area,
Astronomy Museums, Visitor Centers & Public Observatories
Workshop, (Leiden, Netherland, Sep. 27-29, 2017).
Usuda-Sato, K., Agata, H., Fujiwara, H., Horiuchi, T., Koike, M.,
Miyazaki, S., Naito, S., Tanaka, M., Yaji, K., Yamaoka, H.:
2018, Exploring the Universe with the real observational data of the
Subaru Telescope, Communicating Astronomy with the Public 2018,(Fukuoka, Japan, Mar. 24-28, 2018).
Usuda-Sato, K., Canas, L., Shibata, Y., Mineshige, S.: 2017,
Astronomy for Inclusion: A Chance for Regional and International
Cooperation, 2017 Asia-Pacific Regional IAU Meeting, (Taipei,
Taiwan, Jul. 3-7, 2017).
Usuda-Sato, K., Mineshige, S., Canas, L.: 2018, Astronomy for
Inclusion: building network and sharing hands-on resoureces,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Usuda-Sato, K., Nakayama, H., Fujiwara, H., Futami, H., Iwashiro,
K., Usuda, T.: 2017, Developing Tactile Models of NAOJ-Related
Telescopes with a 3D Printer, 2017 Asia-Pacific Regional IAU
Meeting, (Taipei, Taiwan, Jul. 3-7, 2017).
Usuda-Sato, K., Mineshige, S., Canas, L.: 2018, Astronomy for
Inclusion: building network and sharing hands-on resources,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Uzawa, Y., Kojima, T., Shan, W., Gonzalez, A., Kroug, M.: 2017,
Investigation of SIS up-converters for use in multi-pixel receivers,
17th International Workshop on Low Temperature Detectors,(Kurume, Fukuoka, Japan, Jul. 17-21, 2017).
Uzawa, Y., Kojima, T.: 2017, Development of Superconducting
THz Receivers for Radio Astronomy, MTSA2017&TeraNano 8,(Okayama, Japan, Nov. 19-23, 2017).
Wada, T., et al. including Miyachi, A., Nakaya, H.: 2017, Developmentof a far-infrared image sensor with Si-supported Ge BIB detector and
FD-SOI cryo-CMOS ROIC hybritized by nano-particle deposition
Au-bump, 11th International “Hiroshima” Symposium on theDevelopment and Application of Semiconductor Tracking Detectors(HSTD11) in conjunction with 2nd Workshop on SOI Pixel Detectors(SOIPIX2017), (Okinawa, Japan, Dec. 10-15, 2017).
Wakita, S., Nozawa, T., Hasegawa, Y.: 2017, Size constraints onpresolar silicate grains from atomic diffusion processes in thermally
evolving planetesimals, The 10th meeting on Cosmic Dust, (Mitaka,
Japan, Aug. 14-18, 2017).
Wong, K. C.: 2017, Cosmology from Gravitational Lens Time Delays,2017 Asia-Pacific Regional IAU Meeting, (Taipei, Taiwan, Jul. 3-7,2017).
Wong, K. C.: 2017, Cosmology from Gravitational Lens Time Delays,
Shedding Light on the Dark Universe, (Lanzhou, China, Aug. 30-Sep.
1, 2017).
Wong, K. C.: 2017, Cosmology from Gravitational Lens Time Delays,
Stellar Populations and the Distance Scale, (Beijing, China, Sep. 1115, 2017).
Wong, K. C.: 2017, Cosmology from Gravitational Lens Time Delays,
East Asia Young Astronomers Meeting 2017, (Ishigaki, Japan, Nov.
13-17, 2017).
Wong, K. C.: 2017, Strong Gravitational Lensing Observations with

ALMA, East-Asia ALMA Science Workshop 2017, (Daejon, Korea,
Nov. 27-29, 2017).
Wong, K. C.: 2018, Strong Lensing Science from the Hyper SuprimeCam SSP, AAS Meeting #231, (Washington, D. C., USA, Jan, 8-12,2018).
Wong, K. C.: 2018, Environments of Strong Lens Galaxies in the HSC
SSP, Astronomical Society of Japan, Spring 2018 Meeting, (Chiba,
Japan, Mar. 14-17, 2018).
Yagi, M.: 2017, Ram pressure stripped ionized gas found from narrowband imaging with the Subaru Telescope, EWASS 2017: European
Week of Astronomy and Space Science, (Prague, Czech, Jun. 26-30,
2017).
Yagi, M.: 2017, Several intergalactic ionized gas in clusters of galaxies,
Galaxy Evolution in Groups and Clusters at “low” redshift: theory
and observations, (Tegernsee, Germany, Dec. 11-15, 2017).
Yamada, Y., Shirasaki, Y., Nishi, R.: 2017, Nano-JASMINE andsmall-JASMINE data analysis, IAU Symp. 330: Astrometry andAstrophysics in the Gaia Sky, (Nice, France, Apr. 24-28, 2017).
Yamamoto, K., Fukuda, Y., Motoyama, H.: 2017, Ice-sheet mass balancein the Shirase Glacier Basin Revealed by stake observations, SMB
model, and GRACE satellite gravity data, AGU Fall Meeting 2017,(New Orleans, LA, USA, Dec. 11-15, 2017).
Yamamoto, K., Matsumoto, K., Otsubo, T., Namiki, N., Hayabusa2
Astrodynamics Team: 2017, Simulation study for crossover orbit
analysis of Hayabusa2 (2), JpGU-AGU Joint Meeting 2017, (Chiba,
Japan, May 20-25, 2017).
Yamamoto, K., Matsumoto, K., Otsubo, T., Namiki, N., Hayabusa3
Astrodynamics Team: 2017, Simulation of Hayabusa2 crossover orbit
analysis using laser altimeter data, Joint Scientific Assembly of IAGIASPEI, (Kobe, Japan, Jul. 30-Aug. 4, 2017).
Yamamoto, K., Wada, T., Mita, M., Miyachi, A.: 2017, Developmentof optical devices with Subwavelength Structure, 11th International”Hiroshima” Symposium on the Development and Application of
Semiconductor Tracking Detectors (HSTD11) in conjunction with
2nd Workshop on SOI Pixel Detectors (SOIPIX2017), (Okinawa,
Japan, Dec. 10-15, 2017).
Yamaoka, H.: 2017, The experience of A Science Pub with High-energy
scientists, Making the Case 2017, (Pasadena, CA, USA, Apr. 11-13,
2017).
Yamaoka, H.: 2017, Introduction of the session: how to reach the public
and NAOJ/Japan efforts, 2017 Asia-Pacific Regional IAU Meeting,(Taipei, Taiwan, Jul. 3-7, 2017).
Yamaoka, H.: 2018, Nationwide lecture activity during Tanabata period,
Communicating Astronomy with the Public 2018, (Fukuoka, Japan,
Mar. 24-28, 2018).
Yano, T., JASMINE-WG: 2017, Clarification of the formation process ofthe super massive black hole by Infrared astrometric satellite, SmallJASMINE, IAU Symp. 330: Astrometry and Astrophysics in the Gaia
Sky, (Nice, France, Apr. 24-28, 2017).
Yano, T., JASMINE-WG: 2017, Infrared astrometric satellite, SmallJASMINE Clarification of the formation process of the super massive
black hole and Analysis of the gravitational potential, The science ofGaia and future challenges, (Lund, Sweden, Aug. 30-Sep. 1, 2017).
Yokoyama, T., Fukai, R., Tsujimoto, T.: 2018, Meteoritical Perspectiveon the Origin of r-Process Nuclides in the Solar System, 49th Lunarand Planetary Science Conference, (The Woodlands, TX, USA, Mar.

19-23, 2018).
Yokoyama, T., Kazama, T., Fukuda, Y., Miura, S., Kim, T.-H., Tamura,Y.: 2017, Physical modeling of hydrological gravity changes observedby the iGrav-003 superconducting gravimeter in Southeast Alaska,
JpGU-AGU Joint Meeting 2017, (Chiba, Japan, May 20-25, 2017).
Yokoyama, T., Oi, Y., Toriumi, S.: 2017, MHD simulations of formationand eruption of a magnetic flux rope in an active region with a deltasunspot, 48th SPD Meeting, (Portland, OR, USA, Aug. 21-25, 2017).
Yoshida, S., Hamano, K., Miyachi, A., Nishikawa, K., Kawasaki, S.:
2017, Evaluation of a C-band rectifier using Si substrate for HySIC
application, WPTC 2017 - Wireless Power Transfer Conference,(Taipei, Taiwan, May 10-12, 2017).
Yoshida, F., Terai, T.: 2017, Size Frequency Distributions of JupiterTrojans, Hildas and Main Belt Asteroids, Lunar and Deep-space
Exploration, (Beijing, China, Sep. 19-22, 2017).
Yoshida, M., Suematsu, Y., Hara, H., Ishikawa, R.: 2017, Study in
the Cusp Region of 7 March 2015 Solar Flare with IRIS and SDO
Observations, Joint Hinode-11/IRIS-8 Science Meeting, (Seattle, WS,
USA, May. 30-Jun. 2, 2017).
Yoshida, M., Suematsu, Y., Ishikawa, R., Kano, R., Narukage,N., Bando, T., Winebarger, A., Kobayashi, K., Trujillo Bueno, J.,
Auchere, F.: 2017, Wave Propagation on Spicules Observed by
Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), The 4th
Asia-Pacific Solar Physics Meeting (APSPM2017), (Kyoto, Japan,
Nov. 7–10, 2017).
Yoshida, M.: 2017, Current Status of Subaru Telescope and It's FuturePlan, WFIRST-Subaru synergitic observation workshop, (Tokyo,
Japan, Dec. 18-20, 2017).
Yoshida, M.: 2017, Current Status of Subaru Telescope and Comments
to PFS Collaboration, PFS collaboration meeting, (Kashiwa, Japan,
Nov. 28-30, 2017).
Yoshida, M.: 2017, Subaru-EAO international partnership, Annual
Meeting of Korean Astronomical Society, (Yeosu, Korea, Oct. 12-14,
2017).
Yoshida, M.: 2017, Status Report of Subaru Telescope, Keck Science
Meeting, (Santa Cruz, CA, USA, Sep. 13-14, 2017).
Yoshida, M.: 2017, Summary of the research of the A02 sub-project,
Final Symposium of the Innovative Area on Multi-messenger Studyof Gravitational Wave Sources , (Kyoto, Japan, Aug. 24-26, 2017).
Yoshida, M.: 2017, Subaru Telescope: Current Status and Future, JSPS
Japan-United States Science Collaboration Symposium, (Washigton,
D. C., USA, June 9, 2017).
Yoshida, M.: 2017, Current Status and Future Plans of Subaru Telescope,
The 48th annual meeting of the Canadian Astronomical Society,(Edmonton, Canada, May 29-Jun. 1, 2017).
Yoshida, M.: 2018, Annual Report of Subaru Telescope 2017, Subaru
Users Meeting 2017, (Mitaka, Japan, Jan. 17-19, 2018).
Zeidler, S., Akutsu, T., Torii, Y., Aso, Y., Flaminio, R.: 2017,
Scatterometer at NAOJ: applying material investigation for KAGRA,
Gravitational Wave Advanced Detector Workshop (GWADW),(Hamilton Island, Australia, May 7-12, 2017).

XIII Publications, Presentations

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