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Cover Caption
Dark matter distribution (contour lines) determined by weak lensing analysis in a part (14 arc
minute by 9.5 arc minute) of an image taken with Subaru Telescope’s Hyper Suprime-Cam.
Credit: NAOJ/HSC Project

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
2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan
TEL: +81-422-34-3600
FAX: +81-422-34-3960
http://www.nao.ac.jp/
Kyodo Telecom System Information Co., Ltd.
4-34-17 Nakahara, Mitaka-shi, Tokyo 181-0005, Japan
TEX: +81-422-46-2525
FAX: +81-422-46-2528

Annual Report of the
National Astronomical Observatory of Japan

Volume 18, Fiscal 2015

T A

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Preface

E

O F

C

O N T

E

N

Masahiko HAYASHI
Director General
National Astronomical Observatory of JapanI Scientific Highlights April 2015 – March 2016

001

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

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060
064
067
071
073
076

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081
084
087
089
091
092
094
096
101
108
110
113
114
117

T

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III Organization

119

IV Finance143

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

144

VI Research Collaboration

145

VII Graduate Course Education

147

VIII Public Access to Facilities

152

IX Overseas Travel

158

X Award Winners

159

XI Library, Publications160

XII Important Dates

161

XIII Publications, Presentations
1. Refereed Publications

163

2. Publications of the National Astronomical Observatory of Japan176

3. Report of the National Astronomical Observatory of Japan176

4. Conference Proceedings

177

5. Publications in English

184

6. Conference Presentations

184

Annual Report of the
National Astronomical Observatory of Japan
Volume 18, Fiscal 2015

P R E FA C E

Masahiko HAYASHI
Director General of NAOJ

It is my pleasure to present the Annual Report of the
National Astronomical Observatory of Japan.

(KEK). Attempts in Japan to directly detect gravitational
waves began in the 1970’s with the creation of a resonant-In 2015, the new 4D2U system, with an updated control

mass detector by Dr. Hiromasa Hirakawa at the University ofcomputer network and projectors, was opened to the public.

Tokyo. Laser interferometer type detectors started at NAOJ

The overall brightness increased and the colors become morefrom the 1980’s; and in the 1990’s TAMA300 with 300 m

vivid. During simulations of the large-scale structure of thearm-lengths was completed and succeeded in continuous

Universe or of Saturn’s Ring you actually accept the illusion

operation. At NAOJ, making the best use of experiences likethat you are really floating in space. So that as many people

these, the Advanced Technology Center has been developing

as possible can experience this feeling, which words cannot

key components for KAGRA such as the end mirror vibration

adequately convey, the seating of the Dome Theater has been

isolation systems, utilizing 14 m high multistage pendulums,

doubled and the number of days offering public screenings

and the main interferometer, which creates laser light

has also been increased.

interference patters with orthogonal 3 km arms. With KAGRAIn February of 2016, it was announced that LIGO had

added to the LIGO and VIRGO gravitational wave detector

directly detected gravitational waves. Currently in Japan, thenetwork, the locations of gravitational wave sources will be

Large-scale Cryogenic Gravitational Wave Telescope KAGRA

able to be determined with a precision of a couple of degrees.

is being constructed in Kamioka, led by the University of

We are looking forward to that day.

Tokyo Institute for Cosmic Ray Research (ICRR) together

ALMA continues to show its true capabilities through longwith the National Astronomical Observatory of Japan (NAOJ)

baseline observations which became possible with ALMA

and the High Energy Accelerator Research Organization

Cycle 3 observations starting from October 2015. Multiple-

ring structures, like the protoplanetary disk of HL Tauri

Hawai`i, the Maunakea Conservation District Use Permit wasobserved year before last, have been found surrounding otherinvalidated by the Hawai`i Supreme Court in December ofyoung stars. From variations in the submillimeter spectrum

2015. This was extremely disappointing, especially since theemitted by dust at different locations within the disk, theconstruction of TMT near the summit of Maunakea is now

spatial distribution of the dust sizes continues to be clarified. It

supported by about 70 % of the people in the State of Hawai`i.

has reached a point where we can do research into the essence

The reason given for invalidating the permit was that thereof planetary system formation by observing where in the disk

was a problem in the procedure used by the State of Hawai`idust particles are growing and planetesimals are forming, etc.

to grant the Conservation District Use Permit. The actual

It is worth noting that thanks to ALMA’s extremely highconstruction of TMT near the top of Maunakea has not been

sensitivity, it is now possible to detect the far-infrared fine-condemned. At NAOJ, together with the TMT International

structure lines of carbon and oxygen from galaxies in the

Observatory, we have reapplied for a Conservation District

distant Universe. These emission lines are good indicators of

Use Permit for the summit area of Maunakea while working

star formation activity. But because they are in the far infrared,

even harder than before to obtain the understanding of thethey can’t be observed from the ground, so previously they

local people.

had only been observed by using flying instruments. But when

From the experience with the Subaru Telescope, thethe redshift exceeds 3 (i.e. the distance exceeds 12 billion

resistance in the Japanese astronomy community to building

light-years) the observed wavelengths of these emission lines

telescopes overseas disappeared. For ALMA it was a naturalshift to submillimeter waves, making them visible to ALMA.

assumption that the telescopes would be arrayed overseas; theThis is an excellent observational method to understandconstruction and operation also proceeded as an international

the details of star formation in the early Universe and the

project. For NAOJ, that was a new challenge. Fortunately,

history of element production. Recently, the redshifted 88 μm

with the incorporation of NAOJ in 2004 the personnel system

wavelength emission line of ionized oxygen has been detected

for academic faculty was reconsidered and the project systemcoming from a galaxy more than 13.1 billion light-years away

was established, changing the organizational structure to give

discovered by the Subaru Telescope.

it the flexibility needed for large international projects. It also

At the Subaru Telescope, the strategic program using the

became possible to have people with exceptional, specialized

ultra-wide-field prime-focus camera (Hyper Suprime-Cam) is

skills participate in large international projects as contract

proceeding smoothly. This camera’s survey speed (= limiting

employees. Moreover by representing Japan in this kind ofmagnitude x field of view area) is more than 10 times thatlarge international project, NAOJ’s duty as an inter-universityof previous surveys. Equipped with this camera, the Subaru

research institute became better defined; this role has

Telescope will without a doubt be on the world’s leading edge

become making great contributions to strengthening researchof observations until the U.S.A.’s Large Synoptic Survey

throughout all of Japan in the field of astronomy. Based on

Telescope starts operation in the mid-2020’s. Observations

considerations like these, from here forward we would likeby this camera will elucidate the distribution of dark matterto continue efforts towards realizing large-scale international

across wide regions (and a wide range of distances) in thecollaboration projects.

Universe. Hopefully we will be able to pursue the evolutionof the large-scale structure of the Universe and get closer tounderstanding the true nature of dark matter and dark energy.
In addition there is KaVA (KVN and VERA Array), thejoint research observation project utilizing both the Japaneseand the South Korean VLBI networks which started in Fiscal
Year 2014. Combining the strengths of VERA, which obtains
high resolution, and KVN, which can detect spatially extended
elements with high sensitivity, it ascertained that jets from
active galactic nuclei (black holes) are accelerated to nearly
the speed of light at their bases.
Regarding TMT, the next-generation extremely large
optical-infrared telescope scheduled to be constructed in

Masahiko HAYASHI
Director General of NAOJ

I Scientific Highlights(April 2015 – March 2016)01 Rapidly Rising Transients from Subaru/HSC Transient Survey

Tanaka, M., et al.

003

Fujimoto, K., Takamoto, M.

004

Hatsukade, B., et al.

005

Hatsukade, B., et al.

006

Takeda, Y., et al.

007

Hada, K., et al.

008

Notsu, Y., et al.

009

Koyama, Y., et al.

010

Enrichment of r-process Elements in Dwarf Spheroidal Galaxies in Chemo-dynamical
Evolution Model

Hirai, Y., et al.

011

10 Physical Conditions of Supernova Ejecta as Viewed from the Sizes of Presolar Al2O3 Grains

Nozawa, T., et al.

012

11

The Sloan Digital Sky Survey Reverberation Mapping Project: Post-Starburst Signatures in
Quasar Host Galaxies at z < 1

Matsuoka, Y., et al.

013

12

The Ages, Metallicities, and Element Abundance Ratios of Massive Quenched Galaxies atz  1.6

Onodera, M., et al.

014

Tomisaka, K., et al.

015

Kwon, J., et al.

016

15 Early Cosmic Merger of Multiple Black Holes

Tagawa, H., et al.

017

16 Planetary System Formation in Protoplanetary Disk around HL Tauri

Akiyama, E., et al.

018

Mathews, G. J., et al.

019

Mathews, G. J., et al.

020

Mathews, G. J., et al.

021

Lorusso, G., et al.

022

Nakamura, K., et al.

023

Hirota, T., et al.

024

23 Astrometry of Galactic Star-Forming Region IRAS 20126+4104 with VERA

Nagayama, T., et al.

025

Monitoring Observations of the Jupiter-Family Comet 17P/Holmes during its 201424
Perihelion Passage

Kwon, Y. G., et al.

026

Maruyama, T., et al.

027

Oh, D., et al.

028

Michikoshi, S., Kokubo, E.

029

Toriumi, S., et al.

030

Zenitani, S.

031

Hayashi, M., et al.

032

Shirasaki, M.

033

02 Large-Scale Energy Conversion Mechanism of Collisionless Magnetic Reconnection
03

High-resolution ALMA Observations of SDP.81. II. Molecular Clump Properties of a Lensed
Submillimeter Galaxy at z = 3.042

04 Optical–Infrared Properties of Faint 1.3 mm Sources Detected with ALMA
05 Carbon, Oxygen, and Sodium Abundances of Red Giant Stars
06

High-sensitivity 3 mm VLBI Observations of M87: Imaging the Jet Base Near theSupermassive Black Hole07 High Dispersion Spectroscopy of Solar-type Superflare Stars
08 Predicting Dust Extinction Properties of Galaxies from Hα/UV Ratio
09

13 Polarization Structure of Magnetically Supported Molecular Filaments
14 Wide-field Infrared Polarimetry of the Ophiuchi Cloud Core

17 Constraints on the Birth of the Universe and Origin of Cosmic Dark Flow
18

Possible Evidence for Planck-scale Resonant Particle Production during Inflation from the
CMB Power Spectrum

19 Constraints on Pre-inflation Fluctuations in a Nearly Flat Open ΛCDM Cosmology
20 Universality of the Supernova r-Process and Radioactive Nuclei
21 R-process Nucleosynthesis in the MHD+neutrino-heated Collapsar Jet
22 The 658 GHz Vibrationally Excited H2O Maser in Orion Source I

25

Pion Production from Proton Synchrotron Radiation under Strong Magnetic Fields in
Relativistic Quantum Approach

26 Near-infrared Imaging Polarimetry of LkCa 15: A Possible Warped Inner Disk
27 Pitch Angle of Self-Gravity Wakes in Dense Planetary Ring
28 Explosions and Jet Ejections in a Developing Sunspot Light Bridge
29 Initializing Relativistic Velocity Distribution Functions in Plasma Simulations
30 Physical Conditions of the Interstellar Medium in Star-forming Galaxies at z ~ 1.5
31 All-sky Simulations of Gravitational Lensing

001

32

A Numerical Scheme for Special Relativistic Radiation Magnetohydrodynamics Based on
Solving Time-dependent Radiative Transfer Equation

Ohsuga, K., Takahashi, H.

034

33

Discovery of About 1000 Ultra Diffuse Galaxies in the Coma Cluster: Opening the Low
Surface Brightness Universe with Archival DataKoda, J., et al.

035

Konishi, M., et al.

036

Tonegawa, M., et al.

037

Matsumoto, K., et al.

038

Takahashi, H. R., Ohsuga, K.

039

Momose, M., et al.

040

Shibagaki, S., et al.

041

Onishi, K., et al.

042

Higuchi, A., Kokubo, E.

043

Sekimoto, Y., et al.

044

Yabe, K., et al.

045

Maeda, K., et al.

046

Hori, Y., et al.

047

Okamoto, S., et al.

048

Kuroda, T., et al.

049

34 Discovery of an Inner Disk Component around HD 141569 A
35 FastSound: The Subaru FMOS Galaxy Redshift Survey
36Internal Structure of the Moon Inferred from Apollo Seismic Data and Latest Selenodetic
Data

37

Radiation Drag Effects in Black Hole Outflows from Super-critical Accretion Disks via
Special Relativistic Radiation Magnetohydrodynamics Simulations

38

Near-infrared Imaging Observations of Circumstellar Disk around HD 169142 with Subaru/
HiCIAO

39 Nuclear Fission and Solution of r-Process Underproduction Problem
40 Black Hole Mass Measurement in Nearby Galaxy Using Molecular Gas Dynamics
41 Effect of Stellar Encounters on Comet Cloud Formation
42 Developments of Millimeter-wave MKID Camera
43

The Mass-metallicity Relation and the Fundamental Metallicity Relation at z ~ 1.4 Revealedwith the Subaru FMOS Galaxy Redshift Survey (FastSound)

44 A Strong Interaction between The Ejecta of SN IIb 2013df and The CSM
45 Deep Impact on Close-in Super-Earths: Atmospheric Escape and Material Mixing
46 M81 Galactic Archaeology with Subaru/Hyper Suprime-Cam
47

A New Multi-Energy Neutrino Radiation-Hydrodynamics Code in Full General Relativity
and Its Application to Gravitational Collapse of Massive Stars

48

Multi-wavelength Observations of the Black Widow Pulsar 2FGL J2339.6–0532 withOISTER and Suzaku

Yatsu, Y., et al.

050

49

Outer Rotation Curve of the Galaxy with VERA III: Astrometry of IRAS 07427+2400 and
Test of the Density-wave Theory

Sakai, N., et al.

051

50 Optical and Near-Infrared Polarimetry for a Highly Dormant Comet 209P/LINEAR

Kuroda, D., et al.

052

51 Mapping Dark Matter by HSC via Weak Lensing

Miyazaki, S., et al.

053

52 The Host Galaxy of a Fast Radio Burst FRB150418

Keane, E. F., et al.

054

Johnson, M. D., et al.

055

53 Mangetic Field Structure Near the Event Horizon of Sgr A*

002

Rapidly Rising Transients from Subaru/HSC Transient Survey
TANAKA, Masaomi(NAOJ)		

TOMINAGA, Nozomu

MOROKUMA, Tomoki, YASUDA, Naoki(Konan University) 			

FURUSAWA, Hisanori, MORIYA, Takashi		(University of Tokyo)

BAKLANOV, Petr V., BLINNIKOV, Sergei I.

(NAOJ)						(ITEP, Russia)

and HSC Transient Collaboration

-1

-21.0

|Δm/Δt| (mag day )1

10

06aj t<1d(2520A)

-20.0

0.1

PS1 rapid transients

Absolute magnitude

-19.0
-18.0

PS1-13arp(1990A)-17.0

11fe (2600A)

10aq(2130A)

-16.0

11ht
(2590A)

-15.0
-14.0
-13.0
-12.0
-11.0

08ax (2600A)

14gp (2920A)
14or (2620A)
14ha (3080A)
14jr (3450A)
14ef (3060A)
0.1

07Y (2590A)

1

-1

10

Rising timescale (day mag )Figure 2: Summary of absolute magnitudes and rising timescale oftransients.

Figure 1: Images of rapidly rising transients (g- and r- band twocolor composite images, 8″ × 8″ size). Three objects outof the five samples are shown. From top to bottom, eachpanel shows the discovery images, references images
and difference images.

The transient sky has been intensively explored byvarious surveys in the last decade. One of the importantdiscovery spaces for transient surveys is phenomena
with a short timescale less than ~ 1 day. There are, infact, several theoretical expectations for short-timescaletransients, such as supernova (SN) shock breakout (~ 1hr) and the subsequent cooling emission (a few days). In
addition to these, there might also be unknown kind oftransients with a short duration since our knowledge on
the short-timescale transients is still limited.
To explore the short-timescale transient sky, we have
performed a high-cadence transient survey with the
Subaru telescope and Hyper Suprime-Cam (HSC). We
discovered five transients at z = 0.384 – 0.821 (Figure 1)
showing the rising rate faster than 1 mag per 1 day inthe restframe near-ultraviolet wavelengths. The absolutemagnitudes of the five objects range from −16 to −19
mag in the restframe near-ultraviolet wavelengths, andthey all show blue colors, g − r < −0.2 mag. The risingrate and brightness of our samples are the most similar
to those of the very early phase (< a few days after the
explosion) of core-collapse SNe, such as SN 2010aq andPS1-13arp detected by GALEX at the very early phases(Figure 2). A conservative estimates suggest that theevent rate of rapidly rising transients is higher than ~ 9 %of core-collapse SN rates.
We find that the light curves of the three faint objects
agree with the cooling envelope emission from the
explosion of red supergiants. The other two luminous
objects are, however, brighter and faster than the coolingenvelope emission. We interpret these two objects to be
the shock breakout from dense wind with the mass loss
rate of ~ 10−3 M yr−1, as also proposed for PS1-13arp.
This mass loss rate is higher than that typically observed
for red supergiants. The event rate of these luminous
objects is higher than ~ 1 % of core-collapse supernova
rate, and thus, our study implies that more than ~ 1 % of
massive stars can experience an intensive mass loss at a
few years before the explosion.

Reference[1] Tanaka, M., et al.: 2016, ApJ, 819, 5.

I Scientific Highlights003

Large-Scale Energy Conversion Mechanismof Collisionless Magnetic Reconnection				

FUJIMOTO, Keizo(NAOJ)		

Magnetic reconnection is a natural energy converter
which allows explosive energy release of the magnetic
field energy into plasma kinetic energy. The reconnection
processes inherently involve multi-scale process. The
reconnecting of the field lines takes place predominantly
in a small region called the diffusion region formed
around the x-line, while the fast plasma jets resulting
from reconnection extend to a distance far beyond theion kinetic scales from the x-line. The large-scale energy
conversion associated with reconnection is expected
to have a significant impact on a variety of global
scale phenomena in space such as geo-magnetosphericsubstorms and solar flares. However, the multi-scale
nature of reconnection makes it difficult to model thelarge-scale behaviour and, therefore, to evaluate theactual impact on such the global systems.
Large-scale dynamics of magnetic reconnection has
been investigated in the magnetohydrodynamics (MHD)
framework. A fast reconnection can be achieved throughplasma acceleration at a pair of slow mode shocks
extending from the x-line [1]. Although the so-called
Petschek model was based on an approximated solutionof the MHD equations, the model has been widelybelieved to exist in real space because the self-consistent
MHD simulations successfully reproduced the model.
Satellite observations in the Earth’s magnetotail havealso shown the evidences of slow shock-like structuresin association with magnetic reconnection. On the other
hand, a number of particle-in-cell (PIC) simulations haverevealed that both the ions and electrons are accelerated
through the Speiser-type motions in the vicinity of the
x-line. The distinct scales of the Speiser orbit of the ionsand electrons result in an ion-electron decoupling motion
generating the Hall current system . The associated Hall
magnetic field has been often observed in the Earth’s
magnetosphere and laboratory experiments.
The question arising here is how the kinetic process
around the x-line connects to an MHD-scale dynamics
of reconnection far downstream of the x-line. In order
to investigate the large-scale evolution of collisionlessreconnection, we have developed a new electromagnetic
PIC model with adaptive mesh refinement (AMRPIC model) [2], which facilitates large-scale kinetic
simulations of multi-scale processes. The system size inthe current simulation is L x × L z = 655 λ i × 328 λ i with
λ i the ion inertia length. The highest resolution is 32,768
× 16,384 and the maximum number of particles is ~1010 for each species. The simulation employs an open
boundary condition both in the x and z directions.

004

I Scientific Highlights

TAKAMOTO, Makoto(University of Tokyo)

(a)

(b)

Figure 1: 2D snapshots at t = 140 of (a) the out-of-plane current
density J y and (b) the ion flow speed |V ix | with themagnetic field lines in solid curves. The green arrows in(b) represent the ion flow vectors.

Figures 1a and 1b show the out-of-plane current
density and the ion outflow speed, respectively, after along-time evolution of collisionless reconnection. The
width (in z) of the exhaust reaches ≈ 30 λ i that is muchlarger than the ion gyro-radius in the lobe region. One
can see that the current sheet is elongated significantlyin the downstream direction far beyond the ion kinetic
scales, in contrast with the Petschek model. The
elongated current sheet reminds us of a slow reconnectionin the MHD framework. However, we found that the
diffusion region is localized around the x-line, so thatthe reconnection process is more similar to the Petschek
model in this sense.
One of the important characteristics of the Petschek
model is energy conversion at slow mode shocks.
We consider the Rankine-Hugoniot (RH) conditions
based on the ideal MHD equations across the exhaustboundary far downstream of the x-line. It is found that
the RH conditions are almost satisfied at the exhaustboundary, even though the distribution functions of theions and electrons are far from the Maxwellian. Thisis because the RH conditions provide only a series ofconservation laws along the plasma flow. In other words,
these conditions do not always guarantee the existenceof shocks in the kinetic systems. In fact, we found thatthe energy conversion hardly occurs at the boundaries,
implying that they are not slow mode shocks. Instead,the ions are accelerated mostly in the current sheet due tothe Speiser motions even in the region far downstream of
the x-line. Therefore, the current simulation suggests thatcollisionless reconnection differs from classical MHD
reconnection models even in large scale beyond theion kinetic scales and kinetic treatments is necessary todescribe reconnection in collisionless plasmas [3].
References[1] Petschek, H. E.: 1964, NASA Spec. Publ., SP-50, 425.
[2] Fujimoto, K.: 2011, J. Comput. Phys., 230, 8508.
[3] Fujimoto, K., Takamoto, M.: 2016, Phys. Plasmas, 23, 012903.

High-resolution ALMA Observations of SDP.81. II.
Molecular Clump Properties of a Lensed Submillimeter Galaxy
at z = 3.042
				

HATSUKADE, Bunyo(NAOJ)		

TAMURA, Yoichi(University of Tokyo)

IONO, Daisuke, MATSUDA, Yuichi, HAYASHI, Masao

				(NAOJ)				

Deep and wide-field submillimeter surveys haveuncovered dust-obscured star-forming galaxies at highredshift (referred to as submillimeter galaxies; SMGs).
SMGs have intense star-forming activity with starformation rates (SFRs) of a few 100 – 1000 M  yr −1,
which could be triggered by gas-rich galaxy mergers.
SMGs and local ultra-luminous infrared galaxies are
known to be on the same relation on the molecular gas
mass–far infrared (FIR) luminosity plane (MH2−L FIR)or molecular gas surface density–SFR surface density
plane (Σ H2–Σ SFR), so-called ‘burst sequence’ high abovethat of ‘normal’ star-forming galaxies at local and z ~1–3 universe. In order to investigate the star-forming
properties of SMGs, spatially resolved observations ofmolecular gas are essential. However, only a handful ofstudies exists due to the limited spatial resolution andsensitivity of existing instruments.
We studied spatially-resolved properties of molecular
gas and dust in a gravitationally-lensed SMG H-ATLAS
J090311.6 +003906 (SDP.81) at z = 3.042 revealed by the
Atacama Large Millimeter/submillimeter Array (ALMA)[1]. We identified 14 molecular clumps in the CO(5–4)
line data. The surface density of molecular gas and starformation rate of the clumps are more than three orders ofmagnitude higher than those found in local spiral galaxies(Figure 1). The clumps are placed in the ‘burst’ sequencein the Σ H2–Σ SFR plane, suggesting that z ~ 3 molecular
clumps follow the star-formation law derived for local
starburst galaxies. With our gravitational lens model[2], the positions in the source plane are derived for themolecular clumps, dust clumps, and stellar components
identified in the Hubble Space Telescope image. The
molecular and dust clumps are confined within a ~2 kpc
region, while the spatial extent of the stellar components
is as large as ~6 kpc and offset toward the west. The
molecular clumps have a systematic velocity gradient in
the north-south direction, which may indicate a rotating
gas disk. One possible scenario is that the components ofmolecular gas, dust, and stars are distributed in a severalkpc scale rotating disk, and the stellar emission is heavily
obscured by dust in the central star-forming region.
Alternatively, SDP.81 can be explained by a merging
system, where dusty starbursts occur in the region where
the two galaxies collide, surrounded by tidal features
traced in the stellar components.

OGURI, Masamune(University of Tokyo)

Figure 1: Molecular gas surface density–SFR surface density plot[1]. The molecular clumps of SDP.81 are plotted as red
circles. The vertical and horizontal dotted line represents
the 2σ detection limit on the surface density of molecular
gas and SFR, respectively, for a clump with a source size
comparable to the beamsize. For comparison we also
plot data points taken from literature: Milky Way clouds,
giant H II regions in M33, local disk galaxies, local
starbursts, z ~ 1–2 star-forming galaxies, SMGs, and a
spatially-resolved lensed SMG SMM J21352. The solid,
dashed, and dot-dashed lines represent the gas depletiontime scale of 10 Myr, 100 Myr, and 1 Gyr, respectively.
If the filling factor is less than unity, the data points of
SDP.81 shift to the upper-right direction.

References[1] Hatsukade, B., Tamura, Y., Iono, D., et al.: 2015, PASJ, 67, 93.
[2] Tamura, Y., Oguri, M., Iono, D., et al.: 2015, PASJ, 67, 72.

I Scientific Highlights

005

Optical–Infrared Properties of Faint 1.3 mm Sources Detected with ALMA			

HATSUKADE, Bunyo(NAOJ)		

SEKO, Akifumi(Kyoto University)		

OHTA, Kouji(Kyoto University)

MAKIYA, Ryu(Kavli IPMU)		

Since the fraction of dust-obscured star formation
to the total star formation increases with redshift,observations at infrared (IR) to millimeter/submillimeter(mm/submm) wavelengths are essential to understandthe cosmic star formation history and the galaxy
evolution. Deep and wide-field surveys uncovered a
new population of mm/submm–bright galaxies at highredshifts (SMGs). SMGs are highly obscured by dust,
and the resulting thermal dust emission dominates thebolometric luminosity. The energy source of mm/submm
emission is primarily from intense star formation activity,with star-formation rates (SFRs) of 102–103 M yr−1. The
heavy dust obscuration in SMGs makes it difficult tounderstand their optical/near-infrared (NIR) properties.
In addition, the coarse angular resolution of single dishtelescopes (> 15″) prevents from identifying optical/
NIR counterparts. The advent of ALMA has changed thissituation thanks to its high sensitivity and high angularresolution.
We studied optical-IR properties of faint 1.3~mm
sources (S1.3 mm = 0.2–1.0 mJy) detected with ALMA in
the Subaru/XMM-Newton Deep Survey (SXDS) field[1]. We conducted ALMA band 6 observations toward
20 star-forming galaxies at z ~ 1.4 [2,3]. The targets
were extracted from a stellar mass limit (> 10 9.5 M )
sample whose redshifts and Hα SFR were obtained by
NIR spectroscopy. We detected 8 sources at SN ≥ 4.0,
of which three sources are the original targets of ALMA
observations and five sources are serendipitously-detectedsources. We searched for optical/IR counterparts of the
8 ALMA-detected sources in a K-band source catalog.
Four ALMA sources have K-band counterpart candidates
within a 0.4″ radius. Comparison between ALMAdetected and undetected K-band sources in the sameobserving fields shows that ALMA-detected sources tend
to be brighter, more massive, and more actively formingstars. While many of the ALMA-identified SMGs inprevious studies lie above the sequence of star-forming
galaxies (main sequence) in stellar mass–SFR plane,
our ALMA sources are located in the sequence (Figure1), suggesting that the ALMA-detected faint sources
are more like ‘normal’ star-forming galaxies rather than‘classical’ SMGs.
We found a region where multiple ALMA sources andK-band sources reside in a narrow photometric redshift
range (z ~ 1.3–1.6) within a radius of 5″ (42 kpc if we
assume z = 1.45). This is possibly a pre-merging system006

I Scientific Highlights

YABE, Kiyoto(Kavli IPMU)AKIYAMA, Masayuki(Tohoku University)

Figure 1: Comparison of stellar mass and SFR for the ALMA
sources identified with the original targets (circles), the
ALMA serendipitous source (square), ALMA-identified
SMGs in previous studies (crosses), and the K-bandsources (dots).

Figure 2: Multi-wavelength images around the multiple ALMA
sources (ALMA 1.3 mm, B, Ks, 3.6 μm, and 24 μm). The
dashed circle shows a region within a radius of 5″.

and we may be witnessing the early phase of formation ofa massive elliptical galaxy (Figure 2).

References[1] Hatsukade, B., Ohta, K., Yabe, K., et al.: 2015, ApJ, 810, 91.
[2] Hatsukade, B., et al.: 2013, ApJ, 769, L27.
[3] Seko, A., Ohta, K., Yabe, K., et al.: 2016, ApJ, 819, 82.

Carbon, Oxygen, and Sodium Abundances of Red Giant StarsOMIYA, Masashi, HARAKAWA, Hiroki

Consequently, the abundance characteristics of C
(mildly deficient), O (barely changed or only slightly
deficient), and Na (mildly enriched) observed in red
giants are reasonably explained by the recent theoreticalsimulations. This consistency indicates that a substantial
or intrinsic modification of the theory (such as aninclusion of special non-canonical deep mixing) is notnecessary.
See [2] for more details of this study.
0.6

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<[C/Fe]>, δ[C/Fe](a)<[O/Fe]>, δ[O/Fe]“Are the surface C, O, ad Na abundances of red giants(suffering from evolution-induced dredge-up of nuclearprocessed materials) consistent with the prediction fromthe canonical theory of envelope mixing?” In order toanswer this question while adequately taking into accountthe chemical evolution effect (i.e., initial abundance at thetime of star formation should be taken as the reference todetect the purely evolution-induced abundance change),
we compared the abundances of C, O, and Na for 239
evolved red giants with those of 160 unevolved dwarfs at
the same metallicity, where the abundancees were derived
by non-LTE analysis of C I 5052/5380, O I 7771–5, andNa I 6160 lines based on the spectra obtained with 188 cm
reflector+HIDES spectrograph at Okayama AstrophysicalObservatory.
The resulting [X/Fe] vs. [Fe/H] diagrams (X = C,O, and Na) plotted for giants and dwarfs are shown in
Figure 1, where the mean [X/Fe] at each metallicity
group (0.1 dex bin within −0.4 ≤ [Fe/H] ≤ +0.2) alongwith the distribution of [X/Fe]giants – [X/Fe]dwarfs
are also presented. We can state from this figure thatthe abundance changes (compared to the initial values
when stars were formed) in the red-giant phase causedby evolution-induced envelope mixing area moderatedecrease of C by ~ 0.2 dex, only a slight decrease of O by <~ 0.1 dex, and a marginal increase of Na by ~ 0.1–0.2 dex.
By comparing these results with the theoreticalpreductions from recent stellar evolution calculations
published by [1], we can draw the following consequences:― Regarding oxygen, our observational result (only aslight deficiency by < ~ 0.1 dex) satisfactorily matches
the theoretical expectation that the surface O abundances
are hardly altered (the predicted decrease is < ~ 0.05 dex
at most). This means that the current theory for the
mixing in the envelope of evolved stars is quite sufficientto account for the observed oxygen abundances of red
giants, without any necessity to invoke a non-canonicaldeep mixing causing a significant dredge-up of ON-cycle
product.
― Similarly, the observed mild enrichment of Na anddeficiency of C are reasonably consistent with theoreticalsimulations (e.g., for typical case of 2.5 M  star ofsolar-metallicity around T eff ~ 4800–5000 K), which
predict an underabundance of C by ~ 0.2–0.3 dex andan overabundance of Na by ~ 0.2–0.3 dex. Though theobserved extents of anomaly (~ 0.2 dex deficiency for C
and ~ 0.1–0.2 dex enrichment for Na) appear somewhat
smaller than the theoretical predictions, we may state thattheory and observation are reasonably consistent witheach other.

(NAOJ)<[Na/Fe]>, δ[Na/Fe]

SATO, Bun’ei(Tokyo Institute of Technology)			

[C/Fe]5052/5380(NAOJ)[O/Fe]7773

TAKEDA, Yoichi[Na/Fe]6160

		

-0.2
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Figure 1: Left: comparison of [X/Fe] vs. [Fe/H] relations (X = C
or O or Na) for 239 red giants (filled symbols) with thoseof 160 FGK dwarfs (open symbols). Right: mean [X/Fe] at each metallicity group where error bars denotethe standard deviations, while bar graphs represent themean abundance differences between giants and dwarfs
defined as [X/Fe]giants – [X/Fe]dwarfs.

References[1] Lagarde, N., et al.: 2012, A&A, 543, A108.
[2] Takeda, Y., et al.: 2015, PASJ, 67, 24.

I Scientific Highlights

007

High-sensitivity 3 mm VLBI Observations of M87:
Imaging the Jet Base Near the Supermassive Black HoleHADA, Kazuhiro1, KINO, Motoki2, DOI, Akihiro1, NAGAI, Hiroshi1, HONMA, Mareki1
AKIYAMA, Kazunori1, TAZAKI, Fumie1, LICO, Rocco4, GIROLETTI, Marcello4
GIOVANNINI, Gabriele4, ORIENTI, Monica4, HAGIWARA, Yoshiaki5
1: NAOJ, 2: KASI, 3: ISAS/JAXA, 4: INAF-IRA, 5: Toyo University

Understanding the formation, collimation andpropagation of relativistic jets in active galactic nuclei(AGN) is a longstanding concern in high-energy
astrophysics. Recent theoretical progress based on
general relativistic magneto-hydrodynamical simulations
has begun to reveal the detailed physics of jet formation
regions within 10–100 Schwarzschild radii (Rs) from thecentral black hole. It is therefore important to present
detailed observations that can directly image the relevant
scales.
The radio galaxy M87 at the center of the Virgocluster shows one of the nearest (16.7 Mpc) AGN jets.
Due to the proximity and the large mass of the central
black hole, the jet formation region has been imaged
on a scale of 100 Rs with cm-VLBI. More recently, an
extremely compact structure below 6 Rs has been resolved
with the global mm-VLBI array project at 1.3 mm (Event
Horizon Telescope; EHT). However, the EHT is stilltechnically challenging to synthesize interferometricimages due to the severe atmospheric disturbance and thelimited number of available stations. Consequently, there
still remains a large gap in our current understandingof this jet between the cm-VLBI and the EHT. In thiscontext, an important bridge to connect this gap isobservational study at a wavelength of 3 mm.
In 2014 February we conducted high-sensitivity 3 mm
VLBA observations of M87 in concert with the GreenBank Telescope (GBT) [1]. The results are shown in
Figure 1. Thanks to the large collecting area of the GBT,
we obtained images of the M87 jet at a unprecedented
quality, where the image dynamic range improved bya factor of greater than 10 from previous VLBA-only
images. We found a complicated evolution of the jet
forming between 10 and 100 Rs from the black hole.
Moreover, we detected significant polarized emission
from the jet base near the black hole, where a highlypolarized (up to 20 %) feature was seen, suggesting thepresence of a well-ordered magnetic field at this scale.
This may be in agreement with the magnetically-driven
jet scenario. A further increase in the array sensitivity isnecessary. The upcoming incorporation of the phasedALMA to the existing mm/submm VLBI network
will allow us to image the jet launching structure andassociated magnetic-field structure in much more detail.

008

I Scientific Highlights

Figure 1: VLBA+GBT 3 mm images of the M87 jet [1]. The top
panel shows the observed total intensity image, while
the bottom panel (colored) indicates the observed
polarization emission (the contours describe the total
intensity). At the bottom-right corner of each panel the
beam size is shown by the filled ellipse.

Reference[1] Hada, K., et al.: 2016, ApJ, 817, 131.

High Dispersion Spectroscopy of Solar-type Superflare Stars		

HONDA, Satoshi

MAEHARA, Hiroyuki(University of Hyogo)		

SHIBAYAMA, Takuya(Nagoya University)			

NOTSU, Shota(NAOJ)		

(Kyoto University)

NOGAMI, Daisaku, SHIBATA, Kazunari

Flares are energetic explosions on the surface of thestars, and are thought to occur by intense releases ofmagnetic energy stored around starspots. Superflares areflares 10~106 times more energetic (~1033–38 erg) thanthe largest solar flares (~1032 erg). Recently, we analyzed
the data of the Kepler spacecraft, and discovered 1547
superflares on 279 solar-type (G-type main sequence)stars [1,2]. This discovery was very important since itenabled us to conduct statistical analysis of superflares forthe first time, but more detailed observations were needed
to investigate detailed properties of superflare stars.
Based on the initial discovery, we carried out highdispersion spectroscopic observations on 50 solar-type
superflare stars with Subaru/HDS [3,4].
1. More than half of the observed 50 stars show noevidence of binarity. We confirmed the characteristicsof the target stars (e.g., temperature, surface gravity) as
similar to those of the Sun.
2. On the basis of the Kepler data, superflare stars show
somewhat regular, periodic changes in their brightnesses(Figure 1). The typical periods range from one day to a
few tens of days. Such variations are explained by therotation of the star with its large starspots [5]. If this istrue, the timescales of the brightness variations should
correspond to the stars’ rotation speeds. Spectroscopic
observations allow us to estimate the rotation velocity
from the broadening of absorption lines, and we confirm
that a velocity derived from spectroscopic data matches
the brightness variation timescale as the star rotates. In
addition, the measured rotation velocity of some target
superflare stars is as slow as that of the Sun.
3. Based on solar observations, it is known that, theintensity of the Ca II line is a good indicator of starspot
coverage. We investigated this line, and found that there
is a correlation between the amplitude of the brightness
variation of the Kepler data and the intensity of Ca II
8542Å line (Figure 2). We then confirmed that superflarestars have large starspots compared with sunspots.
These results confirm that stars similar to the Sun canhave superflares if they have large starspots. In the future,in addition to the continuing spectroscopic observations
with Subaru Telescope, we will conduct observations
with the Kyoto University’s Okayama 3.8m telescope,
which is now under construction. This will allow them toinvestigate more detailed properties and changes in longterm activity of superflare stars.

(Kyoto University)

Figure 1: The brightness variation of solar-type superflarestars (from Kepler data). In addition to the sudden
brightenings caused by flares, quasi-periodic brightness
variations with periods of about 15 days are seen. Right:
An artificial image of a superflare star seen with visible
light. This figure shows a large superflare (shown inwhite) occurring in the large starspot area.

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r0(8542)NOTSU, Yuta

(Kyoto University)v sin i >10 [km s ]5< v sin i ≤10v sin i ≤5
Sun

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Figure 2: The quantity r0(8542) (the residual core flux normalized
by the continuum level at the line cores of the Ca II
8542Å) as a function of the amplitude of stellar
brightness variation estimated from Kepler data.

References[1] Maehara, H., et al.: 2012, Nature, 485, 478.
[2] Shibayama, T., et al.: 2013, ApJS, 209, 5.
[3] Notsu, Y., et al.: 2015, PASJ, 67, 32.
[4] Notsu, Y., et al.: 2015, PASJ, 67, 33.
[5] Notsu, Y., et al.: 2013, ApJ, 771, 127.

I Scientific Highlights009

Predicting Dust Extinction Properties of Galaxies from Hα/UV Ratio
KOYAMA, Yusei1, KODAMA. Tadayuki1, HAYASHI, Masao1, SHIMAKAWA, Rhythm2, YAMAMURA, Issei3
EGUSA, Fumi1, OI, Nagisa3, TANAKA, Ichi1, TADAKI, Ken-ichi4, TAKITA, Satoshi3, MAKIUTI, Sin’itiro3
1: NAOJ, 2: GUAS, 3: JAXA, 4: MPEStar formation rate (SFR) is one of the mostfundamental parameters which characterize the natureof galaxies. The Hα line (6563Å) is widely used as agood indicator of SFRs and is well calibrated in the local
universe. With recent advents of sensitive near-infraredfacilities, it is becoming easier to observe Hα line ofhigh-z galaxies. However, to reliably measure SFRs, it
is important to derive their extinction levels. Ideally, wewant to use Hα/Hβ (4861Å) ratio (i.e. Balmer decrement)
to measure the dust extinction, but it is usually impossible
to detect faint Hβ line from individual high-z galaxies.
In this work, we use SDSS (DR7) spectroscopic
catalog, in combination with GALEX FUV all-sky survey
data, to establish empirical calibration to predict Hαextinction (AHα) from the observed Hα/UV luminosity
ratio [1]. As shown in Fig. 1, we find that there is apositive correlation between LHα/L UV ratio and A Hα,but at the same time there is a large scatter around thecorrelation. We find that this scatter is related to various
galaxy properties–––e.g. stellar mass. We find that more
massive galaxies tend to have higher AHα at a fixed LHα/
LUV ratio (the color coding of Fig. 1 indicates averagestellar mass of galaxies measured at each pixel). By
quantifying this trend, we demonstrate that we are able
to predict dust extinction levels of individual galaxies bycombining Hα, UV, and stellar mass information.
Furthermore, by combining the AKARI FIR allsky survey data, we compare the AHα and LIR/LUV ratio(Fig. 2). LIR/LUV represents the dust extinction for stellar
continuum light, whilst AHα indicates extinction toward
nebular lines. As demonstrated in Fig. 2, we show that
more massive galaxies tend to show higher extinctionlevels toward nebular regions at fixed L IR/L UV ratio.
The difference between the extinction toward nebularand stellar continuum lights is often interpreted as aconsequence of different star/dust geometry within thegalaxies. Our results therefore suggest that internal dust
geometry of galaxies could depend on stellar mass ofgalaxies, and this can be (at least a part of) the physicalexplanations of the trend that we reported in Fig. 1.

Reference[1] Koyama, Y., et al.: 2015, MNRAS, 453, 879.

010

I Scientific Highlights

Figure 1: Hα dust extinction derived from Hα/Hβ as a functionof Hα/UV ratio. The color coding indicates the averagestellar mass of galaxies in each pixel. More massive
galaxies tend to be more heavily obscured by dust atfixed Hα/UV.

Figure 2: Hα extinction as a function of IR/UV ratio. The colorof the data points indicate their stellar mass. AHα shows
extinction for nebular emission lines, whilst IR/UV ratio
reflects extinction for stellar continuum light. Moremassive galaxies tend to have higher extinction for
nebular lines.

Enrichment of r-process Elements in Dwarf Spheroidal Galaxies
in Chemo-dynamical Evolution Model
HIRAI, Yutaka(University of Tokyo/NAOJ)

FUJII, Michiko S.

(University of Tokyo)

ISHIMARU, Yuhri(International Christian University)

HIDAKA, Jun(Meisei University/NAOJ)

The rapid neutron capture process (r-process) is oneof the main processes to synthesize elements heavier thaniron. Recent astronomical high-dispersion observations
have shown that there are large star-to-star scattersin extremely metal-poor stars of the Milky Way halo.
Nevertheless, astrophysical sites of r-process have notyet been identified. Nucleosynthesis calculations suggestthat binary neutron star mergers are the promisingastrophysical site of r-process. In contrast, previous
galactic chemical evolution studies pointed out that it isdifficult to reproduce the observed r-process abundancein extremely metal-poor stars by neutron star mergers
due to their long merger time and low occurrence rate[1]. However, most previous studies did not consider thegalaxy formation process. Extremely metal-poor stars
would have formed before the Milky Way halo gains large
mass. It is thus required to calculate chemical evolution
with models of the Milky Way progenitor haloes.
In this study, we performed a series of hydrodynamical simulations of galaxies assuming that neutronstar mergers are the major astrophysical site of r-process[2]. The simulations were performed using N-body/hydrodynamic code, ASURA [3]. In ASURA, we
calculate gas cooling, thermal feedback from supernovae,chemical evolution as well as N-body/hydrodynamic
calculations. We assume neutron star mergers with amerger time of 100 Myr occur with 0.5 % of the rate ofsupernovae. We adopt the isolated dwarf galaxy modelwith its halo mass of 7 ×108 M in order to perform highresolution simulations.
Figure 1 shows [Eu/Fe] as a function of [Fe/H]
predicted by this simulation. According to Figure 1,
the dispersion of [Eu/Fe] appears at [Fe/H] ~ −3. Thisfeature is consistent with observations of extremely
metal-poor stars. This means that it is possible to explain
the observed r-process abundance in extremely metalpoor stars by neutron star mergers with merger times of~100 Myr. We find that the metallicity is constant over~300 Myr from the onset of star formation due to low
star formation rate suppressed by supernova feedback in
dwarf galaxies. We confirm that merger times shorter than
500 Myr do not significantly affect the distribution of
r-process elements. We moreover find that metal mixing
in star-forming region avoids producing extremely
r-process rich stars, which are inconsistent with theobservation, due to the low rate of neutron star mergers.

SAITOH, Takayuki R.

(Tokyo Institute of Technology)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

The r-process elements observed in the Milky-Way halo
might originate in accreted dwarf galaxies. This study
supports that neutron star mergers are the promising siteof r-process elements on the point of chemo-dynamical
evolution of galaxies.

Figure 1: [Eu/Fe] as a function of [Fe/H] [2]. Color contour is thenumber of stars produced in this model. Yellow curve anddash-dotted curve are the median, first, and third quartilesof model prediction, respectively. Circles and squares
are the observed values of stars in the Galactic halo
and the Local Group dwarf galaxies, respectively. The
observational data are taken from SAGA database [4].

References[1] Argast, D., Samland, M., Thielemann, F.-K., Qian, Y.-Z.: 2004,
A&A, 416, 997.
[2] Hirai, Y., Ishimaru, Y., Saitoh, T. R., Fujii, M. S., Hidaka, J.,
Kajino, T.: 2015, ApJ, 814, 41.
[3] Saitoh, T. R., Daisaka, H., Kokubo, E., et al.: 2008, PASJ, 60,
667.
[4] Suda, T., Katsuta, Y., Yamada, S., et al.: 2008, PASJ, 60, 1159.

I Scientific Highlights

011

Physical Conditions of Supernova Ejecta as Viewed from the Sizes
of Presolar Al2O3 Grains
NOZAWA, Takaya, WAKITA, Shigeru

		(NAOJ)				

Presolar grains are tiny solid particles identified
in meteorites thanks to their anomalous isotopic
composition, and are invaluable fossils that allow us todirectly observe the detailed chemical compositions andsizes of stellar dust. Among the presolar grains that areconsidered to have originated in core-collapse supernovae(SNe), Al2O 3 grains are of great importance because
Al2O3 is known to be one of the major components of
SN condensates [1,2]. In particular, the measured sizes ofpresolar Al2O3 grains are 0.5–1.5 μm in diameter [3,4],
which are much larger than those (< 0.05 μm) predictedfrom theoretical calculations of dust formation in SNe[e.g., 5].
With the aim of clarifying the formation condition ofsuch large Al2O3 grains, we investigate the condensationof Al2O3 grains for wide ranges of density and coolingrate of the gas [6]. The calculations are performed
by applying the formulation of non-steady-state dust
formation [7]. The formula enables us to estimate the size
distribution of newly formed grains and the condensation
efficiency defined as the fraction of Al atoms that arelocked up in Al2O3 grains.
We first show that the average radius a ave,∞ andcondensation efficiency fcon,∞ of newly formed Al2O3
grains are nicely described by a non-dimensional quantity
Λ on, defined as the ratio of the timescale on which thesupersaturation ratio increases to the collision timescaleof Al atoms at dust formation. Figure 1 shows that theformation of Al2O3 grains can be realized at Λ on ≥ 1,
and fcon,∞ = 1 at Λ on ≥ 20. Since Λ on is approximately
proportional to the product of gas density and coolingtimescale, the average radius is larger for a higher gas
density and/or a slower gas cooling.
Then we find that, in order to produce Al2O3 grains
with radii larger than 0.25 μm as measured in meteorites,Λ on should be higher than 3 × 10 4. Such a high Λ on
could be achieved by adopting more than one order ofmagnitude higher gas density than that presented by the
one-dimensional SN model. This indicates that presolar
Al2O3 grains might be formed in dense gas clumps within
the SN ejecta. Our analysis strongly suggests that themeasured sizes of presolar grains can be a powerful toolfor constraining the physical conditions and structure of
the SN ejecta.

012

I Scientific Highlights

HASEGAWA, Yasuhiro(NASA JPL)		

KOZASA, Takashi(Hokkaido University)

Figure 1: Average radius (a ave,∞) and condensation efficiency( fcon,∞) of newly formed Al2O3 grains as a function ofΛ on, which is defined as the ratio of the supersaturation
timescale (τsat) to the collision timescale of Al atoms(τcoll) at dust formation. The results for four different
cooling rates (T(t) ∝ t −3(γ−1)where γ = 1.1, 1.3, 1.5, and1.7) are shown in different colors but they are plotted
as almost the same curve. The hached region draws the
expected range of Λ on for the formation of Al2O3 grainsin the Al-rich region, referring to the one-dimensionalmodel of a Type II-P SN [8]. The solid vertical line
indicates the minimum value of Λ on necessary for
explaining the radii larger than 0.25 μm as measured forpresolar Al2O3 grains.

References[1] Douvion, T., Lagage, P. O., Pantin, E.: 2002, A&A, 369, 589.
[2] Rho, J., et al.: 2008, ApJ, 673, 271.
[3] Choi, B.-G., Huss, G. R., Wasserburg, G. J.: 1998, Science, 282,
1284.
[4] Nittler, L. R., Alexander, C. M. O’D., Wang, J., Gao, X.: 1998,
Nature, 393, 222.
[5] Nozawa, T., et al.: 2003, ApJ, 598, 785.
[6] Nozawa, T., Wakita, S., Hasegawa, Y., Kozasa, T.: 2015, ApJ,
811, L39.
[7] Nozawa, T., Kozasa, T.: 2013, ApJ, 776, 24.
[8] Kozasa, T., et al.: 2009, ASP Conf. Ser., 414, Cosmic Dust:
Near and Far, ed. Th. Henning, E. Gr¨un, & J. Steinacker (SanFrancisco, CA: ASP), 43.

The Sloan Digital Sky Survey Reverberation Mapping Project:
Post-Starburst Signatures in Quasar Host Galaxies at z < 1
MATSUOKA, Yoshiki1, STRAUSS, Michael A.2, SHEN, Yue3/4, BRANDT, William N.5, GREENE, Jenny E.2
HO, Luis C.3, SCHNEIDER, Donald P.5, SUN, Mouyuan5/6, TRUMP, Jonathan R.5
1: NAOJ, 2: Princeton University, 3: Peking University, 4: Carnegie Observatories, 5: The Pennsylvania State University, 6: Xiamen University

Quasar host galaxies are key for understanding therelation between galaxies and the supermassive black
holes (SMBHs) at their centers. We present a study of
191 broad-line quasars and their host galaxies at z < 1,using high signal-to-noise ratio (SNR) spectra producedby the Sloan Digital Sky Survey Reverberation Mapping
project [1]. Clear detection of stellar absorption lines
allows a reliable decomposition of the observed spectra
into nuclear and host components, using spectral modelsof quasar and stellar radiations as well as emission lines
from the interstellar medium. We estimate age, mass
M*, and velocity dispersion σ* of the host stars, the starformation rate (SFR), quasar luminosity, and SMBH massM•, for each object. The quasars are preferentially hosted
by massive galaxies with M* ~ 1011 M characterized
by stellar ages around a billion years, which coincides
with the transition phase of normal galaxies from the blue
cloud to the red sequence (Figure 1). The host galaxies
have relatively low SFRs and fall below the main
sequence of star-forming galaxies at similar redshifts.
These facts suggest that the hosts have experienced an
episode of major star formation sometime in the pastbillion years, which was subsequently quenched or
suppressed. The derived M• – σ* and M• – M* relations
agree with our past measurements and are consistent
with no evolution from the local Universe. The present
analysis demonstrates that reliable measurements ofstellar properties of quasar host galaxies are possible withhigh-SNR fiber spectra, which will be acquired in large
numbers with future powerful instruments such as the
Subaru Prime Focus Spectrograph.

Figure 1: Rest-frame (u – r) colors and stellar masses of the quasar
host galaxies in this work (red dots) and in [2] (bluedots). The typical error for the present sample is shownby the error bar at the bottom right corner. The small
gray dots and contours, drawn at logarithmically stepped
levels of number density, represent non-AGN galaxies
at 0.5 < z < 1.0 taken from the COSMOS/UltraVISTA
K-band selected catalog. The dots are given small
random offsets to improve visibility. The dashed lines
mark the SSP colors with t* = 0.03, 0.1, 0.3, 1, 3, and10 Gyr, as labelled. The quasar hosts are preferentiallyhosted by massive galaxies distributed from the massive
tip of the blue cloud to the red sequence. Their meanstellar age (t* ~ 1 Gyr) corresponds to the gap of thebimodal distribution of inactive galaxies, where blue
star-forming galaxies may be rapidly transitioning to thered sequence.

References[1] Matsuoka, Y., Strauss, M. A., Shen, Y., et al.: 2015, ApJ, 811,
91.
[2] Matsuoka, Y., Strauss, M. A., Price, T. N., III, DiDonato, M. S.:
2014, ApJ, 780, 162.

I Scientific Highlights

013

The Ages, Metallicities, and Element Abundance Ratios of Massive
Quenched Galaxies at z  1.6
ONODERA, Masato, CAROLLO, C. Marcella, TACCHELLA, Sandro(ETH Zurich)		

RENZINI, Alvio, MANCINI, Chiara(INAF–Osservatorio Astronomico di Padova)

ARIMOTO, Nobuo(NAOJ/Graduate University for Advanced Studies)		YAMADA, Yoshihiko(NAOJ)			

GOBAT, Raphaël

(Korea Institute for Advanced Study)

We studied the ages, metallicities ([Z/H]), andα-element abundance ratios ([α/Fe]) of stellar populationsin quenched and passively evolving galaxies byusing MOIRCS on Subaru Telescope [1]. The sample
galaxies were selected in the COSMOS field and theirspectroscopic redshifts range in 1.25 < z < 2.09 with amean of 1.6. Since these galaxies are extremely faint,
it is difficult to study stellar population properties
spectroscopically for individual objects. Therefore, we
carried out our analysis by stacking 24 spectra to obtainan adequate S/N ratio, resulting in a stacked spectrumwith an equivalent integration time of 200 hours.
We measured a set of Lick indices [2, 3] and comparedthem with the prediction from stellar population synthesis
models [4] to obtain the stellar population parameters ofz  1.6 passively evolving galaxies. The resulting stellar
population parameters are log10 age/Gyr = 0.04 +0.10−0.08 , [Z/H]+0.12= 0.24 +0.20,
and[α/Fe]=
0.31.
In
particular,
this is the
−0.12
−0.14
first time that stellar [α/Fe] is measured at z > 1.
Comparing the stellar population parameters above
with low redshift counterparts of our sample at 0 < z < 1,
all of them show excellent agreement with passive
evolution of the stellar populations, and we found theformation redshift of them as zf  2.3. This supportsa scenario that these passively evolving galaxies haveformed by z  2.3 and evolved passively since then. The[α/Fe] ratio indicates a short formation timescale, at most
1 Gyr.
We then investigated star-forming precursors of thepassively evolving galaxies we studied. Since the age ofthe sample is well constrained to be  1 Gyr, progenitors
must be star-forming galaxies at z  2.3. Indeed, starforming galaxies at z  2.3 with similar stellar masses
show star formation rates of a few hundred solar masses
per year, which agrees well with that expected from thestellar population parameters we derived above. If thesestar-forming galaxies form stars at this rate, they willgrow in mass with which no corresponding counterpart
exists in the local Universe. Therefore, they must soon bequenched due to some physical mechanisms and follow
passive evolution to present.

014

I Scientific Highlights

CAPPELLARI, Michele(INAF–Osservatorio Astronomico di Padova)

DADDI, Emanuele(CEA Saclay)

STRAZZULLO, Veronica(Ludwig-Maximilians University)

References[1] Onodera, M., et al.: 2015, ApJ, 808, 161O.
[2] Worthey, G., Ottaviani, D. L.: 1997, ApJS, 111, 377.
[3] Trager, S. C., et al.: 1998, ApJS, 116, 1.
[4] Thomas, D., et al.: 2011, MNRAS, 412, 2183.
[5] Jrgensen, I., Chiboucas, K.: 2013, AJ, 145, 77.
[6] Spolaor, M., et al.: 2010, MNRAS, 408, 272.

Polarization Structure of Magnetically Supported Molecular Filaments
TOMISAKA, Kohji(NAOJ)

equilibrium filaments observed from the line of sightspecified with two angles θ and φ (see Fig. 2 left). We
showed the models with (θ, φ)=(80°, 90°) in Figure 2.
The middle panel corresponds to a low-density filamentof Fig. 1 (left). Low polarization degree comes fromthe configuration in which the line of sight is nearlyparallel to the large-scale B-field. On the other hand, ahigh-density filament with ρc /ρs = 300 (right) shows apolarization pattern as if B-field were perpendicular to thefilament. This may explain the fact that the perpendicularconfiguration is so commonly observed.

Observations of thermal dust emissions with Herschelsatellite have revealed that molecular clouds consist of
many filaments [1]. That is, the molecular filaments are
the building blocks of interstellar clouds. On the other
hand, near IR interstellar polarization indicates thefilaments are extending in the perpendicular direction to
the interstellar magnetic field [2].
Equilibrium solutions of isothermal clouds, in which
the gravity is balanced with the Lorentz force, thermalpressure and the external pressure, are obtained witha self-consistent field method [3]. Figure 1 shows two
typical such solutions, where the left one has a low
density-contrast between the center and the surface ρc /ρs= 10 while the right one has a higher contrast ρc /ρs = 300.
Here, we studied polarization structures of the thermal
dust emissions expected for the magnetized filaments [4].
The polarization of the thermal dust emissions comesfrom dusts which are aligned to the interstellar magnetic
field. Expected polarization pattern is calculated for theReferences[1] Men’shchikov, A., Andre, Ph., Didelon, P., et al.: 2010, A&A,
518, L103.
[2] Sugitani, K., Nakamura, F., Watanabe, M., et al.: 2011, ApJ,
734, 63.
[3] Tomisaka, K.: 2014, ApJ, 785, 24.
[4] Tomisaka, K.: 2015, ApJ, 807, 47.

Figure 1: Isothermal filaments threaded by lateral magnetic fields, which were obtained under the assumption of mechanical equilibrium using
a self-consistent field method [3]. These two models have the identical magnetic flux, isothermal sound speed and external pressure
but different central density (left: ρc = 10 ρs; right: ρc = 300 ρs).
Pol(max)= 0.5%
Sigma max=21.5 min=19.5

φ-2•104

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4

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n

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2•104

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Pol(max)=15.4%
Sigma max=22.5 min=17.5= 10.00

4•104

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4•10 4

R2b1N641/rhoc300/th=80/phi=090

6•104

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= 10.00

20.5

R2b1N641/rhoc10/th=80/phi=090

6•10 4

4
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5
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2•104

4•104

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Figure 2: Left: relation between the filament and the observing line-of-sight. Expected polarization patterns of the low-density filament(middle), and the high-density filament (right). The polarization degree and its direction (electromagnetic wave B-vector) are shownby false-color and short bars, respectively.

I Scientific Highlights

015

Wide-field Infrared Polarimetry of the Ophiuchi Cloud Core
KWON, J.

TAMURA, M.

(University of Tokyo/JSPS) (University of Tokyo/NAOJ)NISHIYAMA, S.

(Miyagi University of Education)

KUSAKABE, N.
(NAOJ)		

We have conducted wide and deep near-infrared
imaging polarimetry of the ρ Ophiuchi cloud complex [1].
Aperture polarimetry in the JHK s band was conducted
for 2136 sources in all three bands, of which 322
sources have significant polarizations in all the JHK s
bands and have been used for a discussion of the coremagnetic fields in the ρ Ophiuchi cloud complex. Thereis a positive correlation between degrees of polarizationand H – K s color up to H – K s ≈ 3.5. The magnetic
field structures in the core region are revealed up toat least AV ≈ 47 mag and are unambiguously definedin each sub-region (core) of Oph-A, Oph-B, Oph-C,
Oph-E, Oph-F, and Oph-AC. Their directions, degrees
of polarization, and polarization efficiencies differ but

Figure 1: Comparison between infrared and optical polarimetry [1].

016

I Scientific Highlights

HOUGH, J. H.

(University of Hertfordshire)

NAGATA, T.

(Kyoto University)		

NAKAJIMA, Y.

(Hitotsubashi University)

KANDORI, R.
(NAOJ)

their changes are gradual. Therefore, the magnetic fields
seem to be connected from core to core, rather than as asimple overlap of the different cloud core components.
Comparing our results with the large-scale field structures
obtained from previous optical polarimetric studies [2],we suggest that the magnetic field structures in the core
were distorted by the cluster formation in this region,
which may have been induced by shock compression
due to wind/radiation from the Scorpius–Centaurus
association.
References[1] Kwon, J., et al.: 2015, ApJS, 220, 17.
[2] Vrba, J., et al.: 1976, AJ, 81, 958.

Early Cosmic Merger of Multiple Black HolesTAGAWA, Hiromichi

UMEMURA, Masayuki

				

GOUDA, Naoteru(University of Tsukuba)

YANO, Taihei(NAOJ)At redshifts higher than six quasars are found thatpossess SMBHs with the mass higher than 109 M [1].
The formation history of these SMBHs is among themost significant unsolved issues in astrophysics. For
SMBHs to grow from such first star remnants throughmass accretion at z > 6, a super-Eddington accretion rate
is requisite. However, the continuous accretion is unlikely
to be sustained due to feedbacks, and thus the average
mass accretion rates should be lower than the Eddington
rate [2]. Another possible pathway of SMBH formation is
the merger of BHs. If the merger of multiple black holes
precedes the growth via gas accretion, the merged BH
can be a seed of a supermassive black hole.
Recent radiation hydrodynamic simulations on theformation of first stars show that several or more stars
form in a primordial gas cloud with the density of around107 cm−3 and the extension of 1000 AU, where the gas
fraction is 99 % [3]. In this circumstance, BH remnantsof first stars are most likely subject to the dynamical
friction by abundant gas. The gas dynamical friction
has been considered as a mechanism that prompts the
BH merger. Hitherto, the merger processes by the gas
dynamical friction have been investigated in the case of
two massive BHs (e.g. Escala 2004, Escala 2005). In ourstudy, we explore the merger of multiple BHs, supposing
a first-generation object of ~ 105–106 M or a gas-richprimordial galaxy of ~ 108–109 M.
The simulations incorporate such general relativistic
effects as the pericentre shift and gravitational wave
emission.
As a result, we find that multiple BHs are able tomerge into one BH within 100 Myr in a wide range ofparameters. In the case of MBH = 30 M, if multiple BHs
are embedded in the gas density with ngas = 5×106 to
108 cm−3, then all the BHs can merge together over six
orders of BH density as ρ BH = 72 – 7.2 × 10 7 M pc−3.
The merger mechanism is revealed to be categorized into
three types: gas drag-driven merger (type A), three bodydriven merger (type C), and interplay-driven merger (typeB). We find the relation between the merger mechanism
and the ratio of the gas mass within the initial BH orbit(M gas) to the total BH mass (∑ M BH). Type A merger
55occurs if Mgas >~ 10 ∑ MBH, type B if Mgas <~ 10 ∑ MBH,
and type C if Mgas  105 ∑ MBH. Supposing the gas and
BH density based on the recent numerical simulations on
first stars, all the BH remnants from first stars are likely tomerge into one BH through the type B or C mechanism.

(University of Tokyo/NAOJ)YAMAI, Yuki

(Mitsubishi Space Software co., Ltd.)The present results imply that the BH merger may
contribute significantly to the formation of supermassive
BHs at high redshift epochs [4].
1010t N=10(type A)
t N=10(type B)
t N=10(type C)
t N=3
t N=2

MBH=30 Msun
rtyp=0.1 pc

9

10

8

10

t [yr](University of Tokyo)

107
6

10

5

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104
103

4

10

5

10

6

10

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10

8

9

10 10
n gas [cm-3]

10

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Figure 1: Merger time in ten-BH systems (tN=10) as a functionof gas number density ngas. Red, pink, and blue open
symbols represent the results of the type A, B, and C
mergers, respectively. Green- and brown-filled symbols
are the results of two-BH (t N=2) and three-BH (t N=3)
systems, respectively.

References[1] Fan, X.: 2001, AJ, 122, 2833.
[2] Milosavljevic, M., Couch, S. M., Bromm, V.: 2009, ApJ, 696,
146.
[3] Susa, H., Hasegawa, K., Tominaga, N.: 2014, ApJ, 792, 32.
[4] Tagawa, H., et al.: 2015, MNRAS, 451, 2174.

I Scientific Highlights

017

Planetary System Formation in Protoplanetary Disk around HL Tauri
AKIYAMA, Eiji1, HASEGAWA, Yasuhiro1/2/3, HAYASHI, Masahiko1/4, and IGUCHI, Satoru1/4
1: NAOJ, 2: NASA JPL, 3: Caltech, 4: The Graduate University for Advanced Studies

Since the outstanding pictures of HL Tau protoplanetary disk are unveiled, it has been demanded toinvestigate how much we can constrain the disk structure
and physical properties. We re-processed the ALMA
long-baseline science verification data taken toward HL
Tauri [1] and improved the image quality by modifying
data flagging and contriving ways to make deconvolution
as shown in Figure 1. Assuming the observed gaps are
opened up by currently forming, unseen bodies, weestimate the mass of such hypothetical bodies at thefirst 4 gaps from the central star based on following two
approaches; the Hill radius analysis and a more elaborated
approach developed from the angular momentum transfer
analysis in gas disks. For the former, the measured gap
widths are used for estimating the mass of the bodies,while for the latter, the measured gap depths are utilized[2]. As a result, their masses are comparable to or lessthan the mass of Jovian planets. By evaluating Toomre’s
gravitational instability (GI) condition and cooling effect,
we find that the GI might be a possible mechanism andcan occur in the region beyond r ~ 52 AU, where both ofthe conditions are simultaneously met as shown by theshaded area in Figure 2.
Since the disk might be gravitationally unstable onlyin the outer region of the disk, inward planetary migration
would be needed to construct the current architecture of
the observed disk. We estimate the gap-opening mass
(Mgap) to show what type of migration can take place inthe HL Tau system, and can be expressed as(1)

As a result of comparing planet masses with Mgap,
planets are sufficiently massive to open up a gap intheir gas disk via disk-planet interactions, and hence
the planets will undergo type II migration. Combining
GIs with inward migration, we conjecture that all of
the observed gaps may be a consequence of bodies thatmight have originally formed at the outer part of the disk,
and have subsequently migrated to the current locations.
While ALMA’s unprecedented high spatial resolution
observations can revolutionize our picture of planet
formation, more dedicated observational and theoreticalstudies are needed to fully understand the HL Tauri
images.

018

I Scientific Highlights

Figure 1: Comparison of the 0.87 mm continuum dust emissionof HL Tau between our re-processed image (a) and thearchive data (b).

Figure 2: Panel (a) represents the surface density distributionof Kwon et al. (2011) model (solid curve) [3] and theminimum surface density of gas (Σgmin) that is required
to trigger GIs (dashed curve). Panel (b) shows the radial
temperature distribution given by power low function(solid curve) and the minimum disk temperature (Tmin)that satisfies the cooling condition of the GI (dashedcurve). The shaded area in both panels represents theregion where the GI can be invoked.

References[1] ALMA Partnership, Brogan, C. L., Perez, L. M., et al.: 2015,
ApJ, 808, L3.
[2] Kanagawa, K. D., Muto, T., Tanaka, H., et al.: 2015, ApJ, 806,
L15.
[3] Kwon, W., Looney, L. W., Mundy, L. G.: 2011, ApJ, 741, 3.

Constraints on the Birth of the Universe and Origin of Cosmic Dark Flow
MATHEWS, Grant J.

GANGOPADHYAY, Mayukh R., GARNAVICH, P., ROSE, B.

(University of Notre Dame/NAOJ)			
			

ICHIKI, Kiyotomo(Nagoya University)		

This paper [1] reviewed several constraints on newphysics in the early universe including resonant particle
creation [2] and Supersymmetry motivated inflation in the
M-theory landscape leading to a cosmic dark flow. Suchdark flow is the result of quantum entanglement with aneighboring universe that persists during inflation [1].
This residual curvature would appear as a bulk motion of
the universe with respect the the CMB frame corrected
for motion with respect to the cosmic dipole moment.
We summarized [1] recent constraints on the dark
(or bulk) flow velocity based upon a new analysis of
the deviations from Hubble flow in the SNIa redshiftdistance relation. We made two analyses: one identifying
the three dimensional Cartesian velocity components; theother analyzing the cosine dependence on the sky of thedeviation from Hubble flow. Fits were for z < 0.05 andz > 0.05 using both the Union2.1 [3] and SDSS-II [4,5]supernova surveys. We also studied [1] simulated data inwhich a bulk flow was imposed to determine whether thedifficulty in detecting a bulk flow at high redshift is due
to uncertainty in the redshift-distance relation, confusion
with peculiar velocities, or the absence of a bulk flow.
We found [1] a bulk flow velocity of 270 ± 30 km s−1 inthe direction (l, b) = (295 ± 30, 10 ± 5)° in the Cartesiananalysis, while the cosine analysis gave 325 ± 50 km s−1
in the direction (l, b) = (276 ± 15, 37 ± 3)°, consistent
with previous analyses. In the redshift bin z > 0.05,
however, we found [1] only marginal evidence for a bulk
flow velocity. We also found that the SDSS-II supernova
data set has insufficient sky coverage to provide ameaningful result.
Galaxies in which a SN Ia has occurred provide,
perhaps, the best alternative ([1] and refs therein) because
their distances are better determined. However there arefewer data available. There has been a wide variety inthe attempts to find a bulk flow in SN Ia data sets. Our
study [1] differed from that of the previous analyses inseveral key aspects. We made an independent analysis
based upon two different approaches and two separate
data sets. We utilized a MCMC fit to the three Cartesiancomponents of bulk flow velocity rather than the velocity
magnitude in galactic coordinates. This approach had
better stability near the Galactic pole. We then also
analyzed the same data by searching for a deviation from
Hubble flow with a cos θ angular dependance on the sky.
These studies established the robustness of these twocomplementary techniques for identifying the magnitude(University of Notre Dame)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

and direction of the bulk flow and confirmed previous
detections of a bulk flow out to at least z = 0.05.
Having established the viability of the methods
adopted, we then applied them for the first time to thelarge sample of (~ 1000) galactic redshifts and SN Ia
distances from the SDSS-II survey [4,5]. However, wefound that the analysis of the SDSS-II data was severely
limited by the paucity of data in the direction of thecosmic dipole moment. We establish [1] that there isa detectable bulk flow at low redshifts, but at best amarginal detection for high redshifts.
From simulated data sets, we deduced [1] that thecurrent uncertainty at high redshifts arises mostly fromthe current error in the distance modulus. We estimated [1]that with a sample like the Union2.1 data set, a detection
would require both significant sky coverage of SNIa out
to z = 0.3 and a distance modulus error reduction from 0.2
to ≤0.02 mag. However, a greatly expanded data set of 3
× 104 events might detect a bulk flow even with a typicaldistance modulus error of 0.2 mag as may be achievablewith the next generation of large surveys like LSST.

References[1] Mathews, G. J., et al.: 2015, Int. J. Mod. Phys. A, 30, 1545022.
[2] Mathews, G. J., et al.: 2015, Phys. Rev. D, 92, 123519.
[3] Suzuki, N., et al.: 2012, ApJ, 746, 85.
[4] Sako, M., et al.: 2007, AJ, 135, 348.
[5] Frieman, J. A., et al.: 2008, AJ, 135, 338.
[6] Planck Collaboration, Planck XVI: 2014, A&A, 566, A54.

I Scientific Highlights

019

Possible Evidence for Planck-scale Resonant Particle Production
during Inflation from the CMB Power Spectrum
MATHEWS, Grant J.

(University of Notre Dame/NAOJ)GANGOPADHYAY, Mayukh(University of Notre Dame)		

The Planck Satellite has provided the highest
resolution yet available in the determination of the power
spectrum of the cosmic microwave background (CMB)[1]. Analysis of this power spectrum provides powerfulconstraints on the physics of the very early universe [1].
The primordial power spectrum is believed toderive from quantum fluctuations generated during
the inflationary epoch. In this paper [2] we analyzed apeculiar feature visible in the observed power spectrum
near multipoles ℓ = 10–30. This is an interesting region
in the CMB power spectrum because it corresponds
to angular scales that are not yet in causal contact, sothat the observed power spectrum is close to the true
primordial power spectrum.
An illustration of the Planck observed power
spectrum in this region is shown in Figure 1. Although
the error bars are large, there is a noticeable systematicdeviation in the range ℓ = 10–30 below the best fit based
upon the standard ΛCDM cosmology with a powerlaw primordial power spectrum. This same features isvisible in the CMB power spectrum from the Wilkinson
Microwave Anisotropy Probe (WMAP) [3], and hence,
are likely a true feature in the CMB power spectrum.
The line drawn on Figure 1 shows a fit to the the ℓ= 10–30 dip in the Planck CMB power spectrum based
upon a model for the creation of N nearly degeneratetrans-Planckian massive fermions during inflation. The
best fit to the CMB power spectrum implies an optimum
feature at k* = 0.0011 ± 0.0004 h Mpc−1 (wave number
at the resonant frequency) and an amplitude of A ≈ 1.7± 1.5. For monomial inflation potentials consistent with
the Planck tensor-to-scalar ratio, this feature corresponds
to the resonant creation of nearly degenerate particles
with m ~ 8–11 mpl / λ3/2 and a Yukawa coupling constant λbetween the fermion species and the inflaton field of λ ≈(1.0 ± 0.5)N −2/5 for N degenerate fermion species.
If the present analysis is correct, this may be one of
the first hints at observational evidence of new particle
physics at the Planck scale. Indeed, one expects a plethoraof particles at the Planck scale, particularly in the context
of string theory. Perhaps, the presently observed CMB
power spectrum contains the first suggestion that a subset
of such particles may have coupled to the inflaton fieldleaving a relic signature of their existence in the CMB
primordial power spectrum.

020

I Scientific Highlights

ICHIKI, Kiyotomo(Nagoya University)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

Figure 1: (Color online) CMB power spectrum in the range of ℓ
= 3–50 Points with error bars are from the Planck Data
Release [1]. The dashed line shows the best standard
ΛCDM fit to the Planck CMB power spectrum based
upon a power-law primordial power spectrum. The solidline shows the best fit for a model with resonant particle
creation during inflation.

References[1] Planck Collaboration, Planck XX: 2016, A&A, 594, A20.
[2] Mathews, G. J., et al.: 2015, Phys. Rev. D, 92, 123519.
[3] Hinshaw, G., et al. (WMAP Collaboration): 2013. ApJS, 208,19.

Constraints on Pre-inflation Fluctuations
in a Nearly Flat Open ΛCDM Cosmology
					

MATHEWS, Grant J.

(University of Notre Dame/NAOJ)

LAN, Nguyen Q.

(Hanoi National University of Education)

There is now a general consensus that we live in anearly flat universe. The best fit of the combined CMB +HiL + BAO fit by the Planck collaboration [1] obtained
a closure content of the universe to be Ω0 = 1.005+0.0062−0.0065
implying a curvature content of Ωk ≡ 1 − Ω0 = −0.0005+0.0065−0.0062 . This is indeed very close to exact flatness.
Nevertheless, in this paper [2] we considered thepossibility that the present universe is slightly open, i.e.
Ω0 ≥ 0.994 at the 95 % confidence level. In this case any
fluctuations that existed before inflation might now be
visible on the horizon. In our paper [2], we determined
what constraints can be placed on inhomogeneities in the
pre-inflation universe based upon current cosmologicalobservations. Such pre-inflation isocurvature fluctuations
would appear as a distortion in the cosmic microwave
background dipole moment and can be characterized as acosmic dark flow velocity vDF.
We developed a simple analytical model in which
the pre-inflation universe contained a plane-wave
sinusoidal inhomogeneity as an isocurvature fluctuation.
. The wavelength of thefluctuation can then be parameterized by: λi = lHi−1, The
pre-inflation universe is then characterized by: 1) the
scale l of the fluctuation in the inflaton field; 2) the initial
closure parameter of the universe Ωi; and 3) the fractionof the energy density of the universe in the inflaton field f
as the universe enters the inflationary epoch.
Figure 1 from [2] summarizes values for Ω i and lthat satisfy the constraint f < 1 based upon the upper
limit vDF = 254 km s−1 from the Planck analysis of the
KSZ effect, and the constraint that the quadrupole andhigher moments not exceed the value from the observed
CMB power spectrum. The upper region shows that only
values of l near unity can satisfy this constraint while
the the upper limit to the initial closure parameter is Ωi <
0.4 (Ωk,i > 0.6) as f → 1. Indeed, from these constraints
alone we find that the pre inflation fluctuation in the
power spectrum must reside at least ~80 times the current
Hubble scale. Such fluctuations are also constrainedby the near flatness of the current universe. Indeed, alltogether we find that the wavelength of the pre-inflation
fluctuation must be of order the Hubble scale as inflation
begins. Also, if there is a pre-inflation component tothe current cosmic dipole moment, then the initial preinflation closure parameter could have been as large as Ωi< 0.4 (Ωk,i > 0.6).

SUH, InSaeng(University of Notre Dame)

KAJINO, Toshitaka(NAOJ/University of Tokyo)
1

l
0.8
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0.2
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Figure 1: Constraints on the pre-inflation parameters as a functionof the fraction f of the initial pre-inflation energy density
in the inflaton field for a present dark flow velocity of
254 km s−1 from the upper limit to the Planck analysis[3]. Lower shaded region shows allowed values for the
initial closure parameter Ω i. Upper shaded region shows
the allowed values of the wavelength parameter l.

References[1] Planck Collaboration, Planck XVI: 2014, A&A, 566, A54.
[2] Mathews, G. J., et al.: 2015, Phys. Rev. D, 92, 123514.
[3] Planck Collaboration, Planck XIII: 2014, A&A, 561, A97.

I Scientific Highlights

021

Universality of the Supernova r-Process and Radioactive Nuclei [1]
LORUSSO, Giuseppe(NPL/RIKEN)			

NISHIMURA, Shunji

SHIBAGAKI, Shota, KAJINO, Toshitaka(RIKEN)			

(NAOJ/University of Tokyo)

for international EURICA collaboration
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124
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121
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118
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115
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106
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103
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44
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104

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46

40

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2.65

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2.75

2.8

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102

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Mass to charge ratio A/Q

Figure 1: Particle Identification Plot. Nuclei on the right side of
the red line were studied for the first time [1].

10

Solar system abundance

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Solar system abundance

The discovery of how chemical elements are made instars is one of the humanity’s greatest achievement but
several important questions are still unanswered. Oneof them surely concerns the rapid neutron capture (r)process, a key to the creation of the elements from Iron
to Uranium (Z=26–92). The astrophysical site and exact
mechanism of the r process have not yet been identified
with certainty, a problem requiring astrophysics,
astronomy, particle and nuclear physics to work together.
We have produced and studied exotic nuclei withneutron number N ≈ 82 that have filled or nearly filled
neutron shells configuration. These nuclei lie in thepathway of r process nucleosynthesis predicted for someof the most promising r process sites such as neutrinodriven wind in core-collapse supernovae. The enhanced
stability of these nuclei is reflected in the large abundanceof Xe and Te in the solar system. The experiment
aimed at half-life measurements, was carried out at theRadioactive Ion Beam Factory (RIBF, RIKEN) where
exotic nuclei were produced by fission of a Uranium
beam induced by collision with a Be target. Fission
fragments were unambiguously identified (see Fig. 1) andtheir following decay studied with the WAS3ABi silicon
stopper and the EURICA germanium array.
The study evidences the persistence of shell structure
and robust half-life systematics that underpin our current
understanding of exotic neutron-rich nuclei. The newmeasurements also have a direct impact in r processmodels that achieve \emph{hot} conditions, i.e., strong(n, γ)⇔(γ, n) equilibrium (see Fig. 2). In this case wefind that the new data alleviate the long standing model
underproduction of isotopes just below and above themass A ≈ 130 peak, and greatly improve the descriptionof rare-earth elements. The latter is a prerequisite forunderstanding why the abundance of such elements
matches coherently solar system and metal-poor stars (rprocess universality), and what is the full elemental rangeof such universal feature.

1

10-1

10-2

80

100

120

140

160

180

200

220

240

Mass number A
Figure 2: Comparison between the r process solar systemabundance pattern and the abundances calculated (a)without and (b) with our new half-lives [1].

Reference[1] Lorusso, G., et al.: 2015, Phys. Rev. Lett., 114, 192501.

022

I Scientific Highlights

R-process Nucleosynthesis in the MHD+neutrino-heated Collapsar Jet
KAJINO, Toshitaka, SATO, Susumu, HARIKAE, Seiji

MATEHWS, Grant J.

(NAOJ/University of Tokyo)		

Nucleosynthesis by a process of rapid neutroncapture (the r-process) accounts for about a half of theabundance of nuclei heavier than iron. Two possible
astrophysical sites of r-process production, supernovae
and neutronstar mergers, have been discussed by many
researchers. In the case of supernovae, neutrino-driven
wind from a central proto-neutronstar was XXX. Recent
state-of-the-art numerical simulations, however, do
not produce high-entropy and neutron-rich conditions
necessary for r-process. For neutronstar merger models,the low rate and the long time delay of binary mergers
are incompatible with the history of Galactic chemical
evolution deduced from observations of r-processelements in metal-poor stars.
In this article [1], we consider long-duration gammaray bursts (LGRBs) as another astrophysical site for the
r-process. The collapsar model [2] is a favored model forthe formation of observed LGRBs. In the collapsar model,
the central core of a rotating massive star collapses to a
black hole and forms an accretion disk around the black
hole. Harikae et al. [3] simulated LGRB evolution basedon the collapsar scenario and found that a relativistic jet
along the polar axis can be launched, mainly powered byheating from the pair annihilation of thermally generated
neutrinos emanating from this accretion disk. In orderto follow the evolution of mass elements in the jet, wehave employed 20,000 tracer particles moving withthe material. We have followed the time evolution oftemperature, density, and electron fraction (Ye) for the
tracer particles and calculated nucleosynthesis by meansof a large nuclear network involving about 5,000 nuclei.
Of the 20,000 tracer particles, 1289 of them were
determined to be participating in the jet. About a half ofthem have high electron fraction (Ye > 0.4) and r-process
is unlikely. On the other hand, some particles show very
neutron-rich composition (Ye ~ 0.1). They also present
a wide variety of entropy per baryon in unit of the
Boltzmann constant (S/kB) from ~ 10 to more than 1,000.
Figure 1 shows the final isotopic abundance
distribution for all 1289 particles emitted in the jet.
Here, we can see that this collapsar simulation produceselements up to the mass number A = 195 r-process peak.
We found that particles with very high entropy perbaryon (S/kB ~ 1,000) can produce heavy elements up to
the third r-process abundance peak and even beyond to
the actinides. On the other hand, particles with relatively
low entropy per baryon (S/kB ~ 100) only produce lightelements up to the 2nd r-process peak as is evident in
Figure 1. The elemental abundances with 140 < A < 180
is referred to the universality region and approximately(University of Notre Dame)

reproduced by our calculations.
Our results, however, includes some problems suchas the r-process peaks appearing at slightly higher mass
numbers. Further investigation is necessary to evaluate
the role of LGRBs in r-process nucleosynthesis.

10 2

Relative abundance

NAKAMURA, Ko(Waseda University)			

10 1
10 0

10 -1
10 -2
10 -3
10 -4
10 -5

60

80

100

120

140

160

Mass number A

180

200

220

Figure 1: Calculated r-process abundance pattern (solid line)
in long-duration gamma-ray bursts, compared withsolar-system r-process abundances (red). Yields arenormalized to 153Eu. Dotted, dashed and dot-dashed lines
display respectively the abundance yields for the typicalflows of high (S/kB = 1000), intermediate (100) and low(25) initial entropy/baryons.

References[1] Nakamura, K., et al.: 2015, A&A, 582, A34.
[2] Woosley, S. E.: 1993, ApJ, 405, 273.
[3] Harikae, S., Takiwaki, T., Kotake, K.: 2009, ApJ, 704, 354.

I Scientific Highlights

023

The 658 GHz Vibrationally Excited H2O Maser in Orion Source I
HIROTA, Tomoya, HONMA, Mareki

KIM, Mi-Kyoung(NAOJ/SOKENDAI)			

We carried out an observational study of the 658 GHz
vibrationally excited H2O maser line (ν2 = 1, 11, 0–10, 1,
E l = 2329 K) toward a massive protostar candidate
Source I in the Orion KL region using the Atacama Large
Millimeter/Submillimeter Array (ALMA) in cycle 0 [1].
The observation was carrid out at ALMA band 9 withthe longest baseline length of 385 m, which achieved thespatial resolution of 0.28″×0.25″.
The 658 GHz H 2 O line is found to be emitted
from a compact structure with the size of ~100 AU(Figure 1). The source structure is elongated along
the northeast-southwest direction parallel to the lowvelocity (18 km s−1) molecular outflow (Figure 1). The
most remarkable feature is a velocity gradient along thenorthwest-southeast direction, which is perpendicular tothe outflow axis and the source elongation suggesting arotating structure. A spectral profile shows an asymmetricstructure with the brighter red-shifted component as seen
in other H2O lines [2] and SiO masers [3] (Figure 2). The
observed flux density and the compact structure suggest
a high brightness temperature of >2×10 4 K, which isconsistent with a strong maser emission.
These basic properties suggest that the 658 GHz H2Oline is most likely emitted from the base of the northeastsouthwest low-velocity (18 km s −1) molecular outflow
ejected from a rotating disk around Source I. Our results
demonstrate that the vibrationally excited H2O line at
658 GHz could be a unique tracer of hot molecular gas
close to the central protostar as proposed for anothersubmillimeter H2O line at 321 GHz [2] and the 43 GHz
SiO masers [3].

(KASI)

Vlsr [km s -1]

1.0

14
0.5
12
Dec offset [arcsec]

			

0.0

10

8
-0.5
6
-1.0

1.0

0.5

0.0

-0.5

RA offset [arcsec]

Figure 1: Moment 0 (contour) and 1 (color) maps of the 658 GHz
H 2 O line emission. The contour levels are 10 %,30 %, 50 %, 70 %, and 90 % of the peak intensity of3923 Jy beam−1 km s−1. A black cross corresponds tothe position of Source I determined by the continuum
emission. A synthesized beam size is shown at thebottom-left corner. Position offset is measured withrespect to the continuum peak.

1200

1000

References[1] Hirota, T., Kim, M. K., Honma, M.: 2016, ApJ, 817, 168.
[2] Hirota, T., et al.: 2014, ApJ, 782, L28.
[3] Kim, M. K., et al.: 2008, PASJ, 60, 991.

Flux [Jy]

800

600

400

200

0

-200
-20

-10

0

10

V lsr [km s -1 ]Figure 2: Spectrum of the 658 GHz H2O line.

024

I Scientific Highlights

2030

Astrometry of Galactic Star-Forming Region IRAS 20126+4104
with VERANAGAYAMA, Takumi, KOBAYASHI, Hideyuki, CHIBUEZE, James
SATO, Katsuhisa, UENO, Yuji, SHIZUGAMI, Makoto(NAOJ)OMODAKA, Toshihiro, HANDA, Toshihiro, BURNS, A. Ross
(Kagoshima University)

Offset (mas)

1
R.A.

Decl.

0

-1

2010

Year

2011 2010

Year

2011

Figure 1: Paralllax of IRAS 20126+4104.

6

20126
Galactic latitude (degree)

We report astrometric observation results of IRAS
20126+4104 with the VLBI Exploration of Radio
Astrometry (VERA). The parallax was obtained to be
0.750 ±0.092 mas, corresponding to a distance of 1.33 +0.19−0.15
kpc. We found IRAS 20126+4104 has a large peculiar
motion of approximately 16 ±4 km s−1 which is originatedwith the expanding motions of the Cygnus superbubble.
These results are published in Nagayama et al. (2015) [1].
IRAS 20126+4104 is associated with the Cygnus
superbubble which is expected to be located near theSun, and is extended over large angular size. Since thenumerous sources at different distances from 0.4 to
4 kpc located along the line of sight direction of thissuperbubble [2], the measurement of the distance andproper motion by VLBI astrometry is important forstudying the structures of this superbubble.
We made VERA observations of 22.235080 GHz H2O
masers in IRAS 20126+4104 during 2010–2011. IRAS
20126+4104 and a position reference source J2007+4029
were observed with VERA dual-beam system. The
position of IRAS20126+4104 was measured using thephase-referencing method.
Figure 1 shows the measured parallax motion. We
can find a sinusoidal motion a period of 1 year caused
by a parallax. The parallax of IRAS 20126+4104 wasmeasured to be 0.750 ± 0.092 mas, corresponding a
distance of 1.33 +0.19−0.15 kpc. This is consistent with theparallax measured with VLBA [3].
The peculiar motion of IRAS 20126+4104 is
estimated to be (Δvl, Δvb, Δvr) = (−3 ± 4, 15 ± 4, −11 ± 4)
km s−1 from the observed proper motion of (μα cos δ, μδ)= (−4.15 ± 0.51, −4.07 ± 0.51) mas yr−1 and LSR velocity
of vLSR = −3.5 ± 4 km s−1. This peculiar motion of IRAS
20126+4104 appears to be associated with the expansionof Cygnus superbubble. The interpolated position of
IRAS 20126+4104 ~3.6 Myr ago, which is the expansion
time-scale of the Cygnus superbubble, is consistent withthe center of OB type-stars’s expanding motion observedwith Hipparcos [4].

420
2 mas yr-1

82

80
78
76
Galactic logitude (degree)74

Figure 2: The peculiar motion of IRAS 20126+4104 (red cone).
The bule arrows show the peculiar motions of OB
type stars measured by Hipparcos [4]. The backgroundcontour shows the ROSAT 1/4 kev map of the Cygnus
supserbubble [2].

References[1] Nagayama, T., et al.: 2015, PASJ, 67, 66.
[2] Uyanker, B., et al.: 2001, A&A, 371, 675.
[3] Moscadelli, L., et al.: 2011, A&A, 526, A66.
[4] Comeron, F., Torra, J., Gomez, A. E.: 1998, A&A, 330, 975.

I Scientific Highlights

025

Monitoring Observations of the Jupiter-Family Comet 17P/Holmes
during its 2014 Perihelion Passage
KWON, Yuna G.1, ISHIGURO, Masateru1, HANAYAMA, Hidekazu2, KURODA, Daisuke2, HONDA, Satoshi3
TAKAHASHI, Jun3, KIM, Yoonyoung1, LEE, Myung Gyoon1, CHOI, Young-Jun4, KIM, Myung-Jin4
VAUBAILLON, Jeremie J.5, MIYAJI, Takeshi2, YANAGISAWA, Kenshi2, YOSHIDA, Michitoshi6, OHTA, Kouji7
KAWAI, Nobuyuki8, FUKUSHIMA, Hideo2, WATANABE, Jun-Ichi2
1: Seoul National University, 2: NAOJ, 3: University of Hyogo, 4: Korea Astronomy and Space Science Institute, 5: Observatoire de Paris, 6:
Hiroshima University, 7: Kyoto University, 8: Tokyo Institute of Technology

Figure 1: Comet 17P/Holmes immediately after its 2014 perihelion
passage.

2.06
101
Fraction of Active Area

17P/Holmes is known as an object that underwent
a historic outburst in October, 2007. Subsequent
observation revealed that the refractory surface layer (socalled dust mantle) was blown off by the outburst and thenucleus remained active around its aphelion passage in2010, showing lingering dust tail even beyond 5 AU [1].
In this study, we performed a monitoring observation of
17P/Holmes during its 2014 perihelion passage that is thefirst time after the outburst, using the 105 cm Murikabushi
telescope at the Ishigakijima Astronomical observatory,
the 50 cm telescope at the Okayama AstrophysicalObservatory (OAO), the 188 cm telescope at OAO, the2 m Nayuta telescope at the Nishi-Harima Astronomical
Observatory (University of Hyogo), the 1.8 m telescopeat the Bohyunsan Optical Astronomy Observatory (Korea
Astronomy and Space Science Institute), and the 50 cm
telescope at the Siding Spring Observatory (operated byiTelescope). We investigated the dust production and thefractional active area using these data [2].
Figure 1 shows selected RC-band images just after its
2014 perihelion passage. The active dust emission seen
after the outburst could not be confirmed, although thecircumnuclear coma and the feeble tail were confirmed.
Figure 2 shows the active area fraction estimated fromthe observation as a function of the heliocentric distance(upper horizontal axis) or the true anomaly (lower
horizontal axis). Although the fraction was 20 – 40 % justafter the 2007 outburst, it was significantly decreased
to 0.1 – 0.3 % during its 2014 perihelion passage. We
presumed from these results that the fresh nucleus would
be covered with the newly formed dust mantle to beinactive in only several years. The dust layer of ~10 cm
would be piled up to the nucleus from the estimation of
the ejected dust amount. This suggests that icy volatilematerials in the comet can be maintained with the dust
piled up only ~10 cm.

Outbound5.2

r h [AU]

Inbound

I Scientific Highlights

Outbound

5.2

Paper I
Inbound 2013
Outbound 2014
Outbound 20152007 Outburst

100

10-1

2015 Minor eruption

10-2
10-3
0

Pre-outburst data

90

180

270
θf [deg]

0

90

180

Figure 2: Time evolution of the active area fraction over thecometary surface.

References[1] Ishiguro, M., et al.: 2013, ApJ, 778, 19.
[2] Kwon, Y., et al.: 2016, ApJ, 818, 67.

026

2.06

Pion Production from Proton Synchrotron Radiation
under Strong Magnetic Fields in Relativistic Quantum Approach [1]			

MARUYAMA, Tomoyuki(Nihon University)		

KAJINO, Toshitaka(NAOJ/University of Tokyo)

CHEOUN, Myung-Ki, KWON, Yongshin, RYU, Chung-Yeol

MATHEWS, Grant J.

(Soongsil University)			

where Fμν ≡ ∂μ Aν − ∂ν Aμ, mN is the proton mass, and κp
is the proton AMM. By solving Eq. (1), we then obtain
the energy eigenvalues as

where n is the Landau level number, s = ± 1 is the spinindex, and pz is z-component of the proton momentum.
In Fig. 1 we show the initial and final spin-dependenceof the proton differential pionic decay widths with (a)and without (b) the AMM with a proton kinetic energyof 1 GeV, emitted pion energy of 300 MeV and a strengthof the magnetic field to be 5 × 1018 G. These widths areaveraged over the initial Landau levels 0 ≤ nmax − ni ≤ 9.
When κ p = 0, the contributions from the spin-flip
transition, si = −sf, are about 100 times larger than thoseof the spin non-flip, si = sf. The spin-flip contributions
become much larger than those from the spin non-flip
reaction.
When the AMM is included, only the contribution
from si = −sf = 1 is about 10,000 times larger than those of
the other channels. When si = −sf = 1, the effects of the AMM
and spin-flip are synchronized, and they increase very

(University of Notre Dame)largely, while the two effects cancel when si = −sf = 1.
Thus, we have found that the proton AMM largely
contributes to the pion production. We can clarify thiseffect by solving the Dirac equation in a strong magnetic
field in a fully relativistic and quantum mechanical way.
Furthermore, we found that the AMM effect becomeslarger as the magnetic field decreases when the initialenergy is fixed while the AMM effects diminish as the
proton energy increases when the magnetic field is fixed.
When B ~ 1015 G, the proton is expected to be ep ~ 1 TeV,
and the maximum Landau level number becomes about
1011, but one expects the AMM effect to remain becauseof the above results.
As for future studies, we must consider a method totreat huge numbers of the Landau levels for the magnetic
field of B ~ 10 15 G. We should have to derive a new
formulation including effects of the AMM from the exact
formulation given in this paper.
101
102 d 2 Γ/ d eπ d Ωπ

It is widely accepted that soft gamma repeaters (SGRs)
and anomalous X-ray pulsars (AXPs) correspond tomagnetars [2]. In the magnetars a proton is expected to beaccelerated in a strong magnetic field and to emit photons
through the synchrotron radiation. The meson-nucleon
couplings are about 100 times larger than the photonnucleon coupling, and the meson production process is
expected to exceed photon synchrotron emission in thehigh energy regime.
However, the synchrotron radiation has beenstudied only in the semi-classical framework [3] andit has not treated discretized Landau levels and theanomalous magnetic moment (AMM) of protons. In
this work [1], then, we study the pion production fromproton synchrotron radiation in the relativistic quantum
approach.
We assume a uniform magnetic field along thez-direction, B = (0, 0, B), and take the electro-magnetic
vector potential Aμ to be A = (0, 0, xB, 0) at the positionr ≡ (x, y, z). The relativistic proton wave function ψ~ isobtained from the following Dirac equation:

102 d 2 Γ/ d eπ d Ωπ

			

100

(a)

10−1

κp ≠ 0−1 → −1−2+1 → −1−1 → +1

10−3+1 → +1

10

10−4
10−5
10−1
(b)
10−2
10−3
10−4
10−5
−1.0
−0.5

κp = 00.0

cos θπ0.5

1.0Figure 1: The differential pionic decay widths of protons with(a) and without (b) the AMM included. The widths
are averaged over initial Landau numbers, 0 < nmax −ni < 9. The solid, dot-dashed, dashed, and dotted lines
represents the results when si = −sf = −1, si = −sf = 1, si =sf = 1, and si = sf = −1, respectively, where si( f ) indicatesthe initial (final) spin of the proton.
References[1] Maruyama, T., et al.: 2015, Phys. Rev. D, 91, 123007.
[2] Mereghetti, S.: 2008, Annu. Rev. Astron. Astrophys., 15, 225.
[3] Tokushita, A., Kajino, T.: 1999, ApJ. 525, L117.

I Scientific Highlights

027

Near-infrared imaging Polarimetry of LkCa 15:
A possible Warped Inner Disk [1]OH, Daehyeon1/2, HASHIMOTO, Jun3/2, TAKATO, Naruhisa1, TAMURA, Motohide3/4/2, and SEEDS team
1: SOKENDAI, 2: NAOJ, 3: Astrobiology Center, 4: The University of Tokyo

References[1] Oh, D., et al.: 2016, PASJ, 68, L3.
[2] Thalmann, C., et al.: 2015, ApJ, 808, L41.
[3] Sallum, S., et al.: 2015, Nature, 527, 342.
[4] Kraus, A. L., Ireland, M. J.: 2012, ApJ, 745, 5.
[5] Hashimoto, J., et al.: 2011, ApJ, 729, L17.
[6] Mouillet, D., et al.: 1997, MNRAS, 292, 896.
[7] de JuanOvelar, M., et al.: 2013, A&A, 560, A111.

028

I Scientific Highlights

42 AU
0.3 arcsec

NE

1 arcsec

140 AU

Figure 1: Elliptical fitting results of the inner disk (purple),the gap (yellow), and the outer disk (red). White star
indicates the location of LkCa 15. Green and orange
stars indicate where the planet candidates LkCa 15 b andc were detected in 2014, respectively [3]. Empty green
and orange circles indicate the locations of two infrared
sources seen in 2009-2010 [4], which are assumed as
LkCa 15 b and c, respectively.

Normalised Flux × Constant

The protoplanetary disks around young stars are
considred as the main birthplace of giant gas planets.
Numerous pectral energy distribution (SED) analyses on
disk-host stars have suggested the presence of cavities
in several disks, such as gaps and central holes. These
structures are believed as a sign of transition fromoptically thick dust disk to optically thin debris disk, andthese disks in the intermediate phase have been called
transitional disks (with central hole) and pre-transitional
disks (with gap). Currently, the most convincible
mechanism to form cavities in the disks is gravitational
interaction with planets in the disks. However, there is noclear observational evidence to explain the formation ofthese disk structures.
LkCa 15 is a solar-like T-Tauri star located in the
Taurus-Auriga region ~140 pc away from us. Previous
studies using SED and optical wavelengths imaging
revealed that the disk of LkCa 15 is a pre-transitional disk
with large gap and optically thick inner disk [1,2]. The
pre-transitional disk of LkCa 15 could have a evidence of
disk-planet interaction, and we conducted high-contrast
and high-resolution near-infrared polarimetric differential
imaging observation with HiCIAO and AO188 on LkCa
15 disk, as a part of SEEDS (Strategic Explorations of
Exoplanets and Disks with Subaru).
From the resultant image, the wide gap structure(width <~ 27 au) and the inner disk were resolved andclear enough to be quantitatively analysed (Fig. 1,2).
It shows that the inner disk has misaligned position
angle of 13° ± 4° with respect to that of the outer disk.
This suggests that the inner disk is possibly warped.
Warped disks were observed from several objects (e.g.,
AB Aurigae [5] and β Pictoris [6]), however, this is thefirst clear observational evidence of warped disk aroundyoung T-Tauri star. From the comprehensive discussion
including previous studies on disk-planet interactions[7,8] and LkCa 15 optical imaging [2], the large gap andthe warped inner disk of LkCa 15 both are indicative ofa multiple planetary system with a mass of <~ 1 MJup in
LkCa 15 system.

r -2.5 r 2.0

104

Major NE

3

Major SWr -2.5

Minor NW

r -2.2

Minor SEr -1.8

10

102

10

1

r -3.6r 1.2 r -3.1

NW
100

-1

10

NE
SE

SW

Radius (arcsec)

0.5

1

Figure 2: Radial surface brightness profiles with 1σ error bars at
major and minor axes.

Pitch Angle of Self-Gravity Wakes in Dense Planetary Ring
MICHIKOSHI, Shugo

KOKUBO, Eiichiro(University of Tsukuba)			

In Saturn’s ring, gravitational forces between
particles tend to form gravitationally bound clumps,
while differential rotation tears them apart. Due to thesecompeting processes, spatial structures called self-gravity
wakes appear (Salo 1992). The self-gravity wakes are
non-axisymmetric structures on sub-kilometer scales. The
A and B rings exhibit a remarkable asymmetric brightness
variation (Camichel 1958). Salo et al. (2004) found that
this asymmetric brightness variation was explained by
self-gravity wakes. Thus, the existence of self-gravity
wakes was indirectly supported by the observations.
The physical mechanism of the self-gravity wakes has
not been understood completely. It was suggested thatthe swing amplification mechanism may be applicable(Toomre 1981, Salo 1995). The pitch angle of the spiralarms formed by the swing amplification was obtained(Michikoshi and Kokubo 2014). From this estimation, thepitch angle of the self-gravity wakes should be about 10°,which does not depend on the Saturnicentric distance.
However, the observational studies indicate that the pitch
angle increases with the Saturnicentric distance (Hedman
et al. 2007). Therefore, to understood this discrepancy,
we investigated the pitch angle of the self-gravity wakesby N-body simulations (Michikoshi et al. 2015).
We performed the local shearing box simulations.
The inelastic collisions among particles were considered.
The self-gravity was calculated by GRAPE-DR in NAOJ.
The typical self-gravity wakes are shown in Figure 1. The
self-gravity wakes are trailing structures. We calculated
the pitch angle from the autocorrelation function.
We confirmed that the pitch angle increases with theSaturnicentric distance (Figure 2).
To understand this trend, we considered the simple
model of the self-gravity wakes. Comparing the timescalesof self-gravity and the shear, we obtained the estimate of
the pitch angle
tan θ ∝ a3/2,(1)
where a is the Saturnicentric distance. This estimateagrees well with the numerical simulations. Our results
suggest that the pitch angle is determined by the strengthof the self-gravity relative to the shear.

(NAOJ)

Figure 1: Surface density normalized by the averaged surface
density. The clear self-gravity wakes are observed.
ρp = 0.45 g cm−3100
80

θ [deg.]

			

60
40
20
0

0.8

0.9

1

1.1

1.2

1.3

1.4

a [105 km]

Figure 2: The pitch angle against the Saturnicentric distance. The
red open and blue filled squares denote the pitch angle in
the high and low density regions, respectively.

References[1] Salo, H.: 1992, Nature, 359, 619.
[2] Camichel, H.: 1958, A&A, 21, 231.
[3] Salo, H., Karjalainen, R., French, R. G.: 2004, Icarus, 170, 70.
[4] Toomre, A.: 1981, Structure and Evolution of Normal Galaxies(Cambridge: Cambridge Univ. Press).
[5] Michikoshi, S., Kokubo, E.: 2014, ApJ, 787, 174.
[6] Hedman, M. M., et al.: 2007, AJ, 133, 2624.
[7] Michikoshi, S., et al.: , ApJ, 812, 151.

I Scientific Highlights

029

Explosions and Jet Ejections in a Developing Sunspot Light Bridge
TORIUMI, Shin, KATSUKAWA, Yukio, CHEUNG, Mark C. M.
(NAOJ, LMSAL)

Light bridges (LBs), the elongated structures
dividing sunspot umbra, are known to produce repeatedexplosions and jet ejections, and thus have been a targetof observational studies [1]. One importance of the LBs
is that they separate the existing spots and eventuallylead to their collapse [2]. Although the LBs are known
to appear also in developing active regions (ARs), there
were few such observational studies.
In this study, aiming at the cause of activity in thedeveloping sunspot LBs, we analyzed observation data of
NOAA AR 11974 (Fig. 1: top).
From the photospheric vector magnetogram taken
by Hinode/SOT, it was revealed that the elongated LB
harbors weak, horizontal magnetic fields inside andis sandwiched between strong, vertical fields of thesurrounding pores (pre-mature sunspots). Observational
data of the IRIS satellite, which simultaneously targeted
the same region, show that smaller-scale explosions
and jet ejections occur repeatedly in the chromosphereabove the LB. Especially, the UV spectra indicate that therepeated explosions are caused by magnetic reconnection,
the plasma process that releases magnetic energy. Fromthese results, we obtained a physical picture that the
explosions and jets in the LBs are caused by repeatedreconnection between the horizontal fields of LBs andvertical fields of ambient pores.
However, there remained outstanding questions suchas why LBs appear in the developing ARs, what the 3D
magnetic and velocity structures of the LBs are, and whyreconnection occurs repeatedly above the LBs. In order toanswer to those questions, we then carried out a radiative
magnetohydrodynamic (MHD) simulation including
convection that reproduces the spot formation [4], andanalyzed the simulation result (Fig. 1: bottom).
We found that, in the subsurface layer, when thevertical fields of two pores approach each other to createa single sunspot, they trap a plasma that contains weak,horizontal magnetic fields. Since there exists a thermal
convection inside the trapped plasma, the horizontal
fields are transported upward repeatedly with a certain
time scale and create a LB in the surface layer. Therefore,
we can conclude that the observed explosions and jets inthe chromosphere above the LB are caused by repeatedreconnection between the magnetic flux transported fromthe interior and the flux of surrounding pores [5].
The above results indicate that the repetitive
reconnection observed in the Sun may be driven bymagneto-convective evolution in the interior. Similar
explosions and jets are reported in sunspot umbrae andpenumbrae, which suggests that these features may be a030

I Scientific Highlights

common phenomena of convection in strong backgroundfields.

㻴㼕㼚㼛㼐㼑㻌㼛㼎㼟㼑㼞㼢㼍㼠㼕㼛㼚㻼㼛㼞㼑㼟㻸㼕㼓㼔㼠㻌㼎㼞㼕㼐㼓㼑
20,000 km㻺㼡㼙㼑㼞㼕㼏㼍㼘㻌㼟㼕㼙㼡㼘㼍㼠㼕㼛㼚㻼㼛㼞㼑㼟

10,000 km㻸㼕㼓㼔㼠㻌㼎㼞㼕㼐㼓㼑

Figure 1: (Top) Hinode observation of NOAA AR 11974.
(Bottom) MHD simulation of sunspot formation.
References[1] Shimizu, T., et al.: 2009, ApJ, 696, L66.
[2] Katsukawa, Y., et al.: 2007, PASJ, 59, S577.
[3] Toriumi, S., et al.: 2015, ApJ, 811, 137.
[4] Cheung, M.C.M, et al.: 2010, ApJ, 720, 233.
[5] Toriumi, S., et al.: 2015, ApJ, 811, 138.

Initializing Relativistic Velocity Distribution Functions
in Plasma Simulations
ZENITANI, Seiji(NAOJ)

Particle-in-cell (PIC) simulations and Monte-Carlosimulations are important research tools in modern
astrophysics. In these numerical simulations, particle
velocities are usually initialized by random variables
with certain algorithms. For example, the Box–Muller
algorithm [1] is popularly used to generate a Maxwell–Boltzmann distribution. It is summarized in Table 1 anddescribed in many textbooks. One can also incorporate
the bulk velocity, by considering an offset to the particle
velocities.
Since relativistic plasma processes have been
growing in importance in high-energy astrophysics,
there is a strong demand for algorithms to deal withrelativistic velocity distribution functions of plasmas.
However, algorithms to generate relativistic velocity
distributions are not well established. Here, “relativistic
velocity distributions” contain both relativistically-hot
distributions and/or relativistically-moving distributions.
Our recent article [2] summarize the state-of-art
algorithms to deal with both of them. Going back to theoriginal article by Russian mathematician Sobol [3], we
review standard algorithms [4] to generate a relativistic
Maxwellian (Jüttner–Synge distribution) at a rest frame.
We further propose two rejection methods to deal withthe spatial part of the Lorentz transformation of arbitrary
distribution functions, which has never been discussed inprevious literature. These results are summarized in Table
2. We note that our algorithms are drastically simpler thansimilar attempts in recent years.
We hope that these algorithms are useful in relativistic
kinetic simulations in high-energy astrophysics.

Table 1: Box–Muller algorithm.

Table 2: Sobol algorithm with the flipping method.

References[1] Box, G. E. P., Muller, M. E.: 1958, Annals of Mathematical
Statistics, 29, 610.
[2] Zenitani, S.: 2015, Phys. Plasmas, 22, 042114.
[3] Sobol, I. M.: 1976, in Monte Carlo Methods in Computational
Mathematics and Mathematical Physics, p.24 [in Russian].
[4] Pozdnyakov, L. A., Sobol, I. M., Sunyaev, R. A.: 1983,
Astrophys. Space Phys. Rev., 2, 189 (Translation).

I Scientific Highlights

031

Physical Conditions of the Interstellar Medium
in Star-forming Galaxies at z ~ 1.5
HAYASHI, Masao1, KASHIKAWA, Nobunari1, LY, Chun2, SHIMASAKU, Kazuhiro3, MOTOHARA, Kentaro3
GOTO, Ryosuke3, NAITO, Yoshiaki3, MALKAN, A. Matthew4, NAGAO, Tohru5
1: NAOJ, 2: NASA, 3: University of Tokyo, 4: UCLA, 5: Ehime University

We perform Subaru/FMOS near-infrared spectroscopyof 118 star-forming galaxies at z ~ 1.5 in the Subaru Deep

Figure 1: The line ratio of [O III]/[O II], which is sensitive toionization parameter, as a function of R 23 ([O II ]λ3727+[O III]λλ4959,5007)/Hβ) (upper) and stellar mass
(lower). The black circles show the ratio of the individual
galaxies, while red pentagon and blue diamonds show
the average ratios derived from the stacked spectra.
Different populations up to z ~ 3 are also shown; Lyαemitters (LAEs) at z = 2–3 (open squares: [2,3,4,5]),
Lyman break galaxies (LBGs) at z = 2–3 (open triangles:[6,7,8,9,10,11]), star-forming galaxies at z = 1–2 (openstars: [4,12,13]), star-forming galaxies at z < 1 (asterisks:[14,15,16,17,18]), and green pea galaxies (GPs) (opencircles:[19]). The contours show the distribution of starforming galaxies (blue), composite objects (green), andAGNs (red) in the local Universe, respectively.

032

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Field which are selected as [O II] λ3727 emitters from
Subaru/Suprime-Cam narrow-band imaging. Hα emission
line is detected in 115 galaxies, [O III] λ5007 emission
line in 45 galaxies, and Hβ, [N II ] λ6584, and [S II ]λλ6716,6731 in 13, 16, and 6 galaxies, respectively. Since
we already detect [O II] emission line by narrow-band
imaging, the 6 strong nebular emission lines are available
in the individual and composite rest-frame optical spectra
to investigate physical conditions of the interstellar
medium in star-forming galaxies at z ~ 1.5.
Figure 1 shows that typical star-forming galaxies atz ~ 1.5 have strong [O III] emission lines and that the[O III]/[O II] ratios are larger than normal star-forming
galaxies in the local Universe. These results suggest thatstar-forming galaxies at z ~ 1.5 have a higher ionization
parameter than the local galaxies. There is a dependenceof the [O III]/[O II] ratios on stellar mass in the sense thatless massive galaxies have larger [O III]/[O II] ratios.
Since we also reveal that the electron density is consistent
with local galaxies, we argue that the high ionization ofgalaxies at high redshifts is due to a harder radiation field
by a young stellar population and/or an increase in thenumber of ionizing photons from each massive star.
In this study, we also find a tight correlation between
Hα and [O II] and that the line ratios of Hα/[O II] areconsistent with those of local galaxies. Thus, [O II] isuseful to estimate star formation rate of galaxies evenat z ~ 1.5. See [1] for more details of the results anddiscussions.
References[1] Hayashi, M., et al.: 2015, PASJ, 67, 80.
[2] Fosbury, R. A. E., et al.: 2003, ApJ, 596, 797.
[3] Erb, D. K., et al.: 2010, ApJ, 719, 1168.
[4] Christensen, L., et al.: 2012, MNRAS, 427, 1953.
[5] Nakajima, K., et al.: 2013, ApJ, 769, 3.
[6] Pettini, M., et al.: 2001, ApJ, 554, 981.
[7] Maiolino, R., et al.: 2008, A&A, 488, 463.
[8] Mannucci, F., et al.: 2009, MNRAS, 398, 1915.
[9] Richard, J., et al.: 2011, MNRAS, 413, 643.
[10] Wuyts, E., et al.: 2012, ApJ, 755, 73.
[11] Belli, S., et al.: 2013, ApJ, 772, 141.
[12] Queyrel, J., et al.: 2009, A&A, 506, 681.
[13] Rigby, J. R., et al.: 2011, ApJ, 732, 59.
[14] Savaglio, S., et al.: 2005, ApJ, 635, 260.
[15] Maier, C., et al.: 2005, ApJ, 634, 849.
[16] Henry, A., et al.: 2013, ApJ, 776, L27.
[17] Ly, C., et al.: 2014, ApJ, 780, 122.
[18] Ly, C., et al.: 2015, ApJ, 805, 45.
[19] Cardamone, C., et al.: 2009, MNRAS, 399, 1191.

All-sky Simulations of Gravitational Lensing
SHIRASAKI, Masato(NAOJ)

Gravitational lensing is one of the most promisingtools to probe matter density distribution in the Universe.
The foreground gravitational field causes small image
distortion of distant galaxies. The small distortion
contains, collectively, rich cosmological information
about the matter distribution. We can reconstruct theforeground mass distribution from observed image of
distant galaxies with statistical analysis. Ongoing andupcoming imaging surveys such as Hyper Suprime-Cam(HSC) survey in the near future, will provide the largest
dark matter map we have never seen before. Therefore,
it is important and timely to investigate the cosmologicalinformation content of the reconstructed mass map.
In order to realize the realistic situation in galaxy
imaging surveys, we perform gravitational lensing
simulations on curved full sky as shown in Figure 1. We
then utilize these simulations to create two hundredsof mock weak lensing catalogs with the proposed sky
coverage in ongoing HSC survey. These mock catalogs
enable us to study the statistical property of reconstructedmass map from gravitational lensing observables.

analytic models and large numerical simulations. Weaklensing selection of clusters does not rely on conventional
assumptions such as the relation between luminosityand mass and/or hydrostatic equilibrium, allowing us toconstruct clean cluster sample. We first develop a halomodel to predict the abundance and the clustering of
weak lensing selected clusters. Observational effects suchas galaxy shape noise are included in our model.
We show that our theoretical model agrees well withthe ensemble average of statistics and their covariances
calculated directly from the mock catalogues. Witha typical selection threshold, ignoring shape noisecorrection causes overestimation of the clustering of
weak lensing selected clusters with a level of about 10 %,and shape noise correction boosts the cluster abundance
by a factor of a few.
Furthermore, we extend our theoretical framework tomodel the statistical properties of clusters in variants ofcosmological models as well as in the standard ΛCDM
model in Ref [2]. We use a large set of realistic mockweak lensing catalogs as well as analytic models to makea forecast for constraining two competing cosmologicalmodels, the wCDM model and modified gravity model,
with our lensing statistics. We show that weak lensing
selected clusters are excellent probes of cosmology whencombined with cosmic shear power spectrum even in
the presence of galaxy shape noise and masked regions.
With the information from weak lensing selected clusters,
the precision of cosmological parameter estimates canbe improved by a factor of ~1.6 and ~8 for the wCDM
model and modified gravity model, respectively. The
HSC survey with sky coverage of 1250 degrees squared
can constrain the equation of state of dark energy w0 witha level of Δw0 ~ 0.1. It can also constrain the additional
scalar degree of freedom in the f(R) gravity model witha level of | fR0| ~ 5 × 10−6, when constraints from cosmic
microwave background measurements are incorporated.

References[1] Shirasaki, M., Hamana, T., Yoshida, N.: 2015, MNRAS, 453,
3043-3067.
[2] Shirasaki, M., Hamana, T., Yoshida, N.: 2016, PASJ, 68, 414.
Figure 1: One of our simulated gravitational lensing maps. The
red regions represent high surface mass density regions,while the blue regions correspond to under-dens regionsin the Universe.

In Ref [1], we explore a variety of statistics of clusters
selected with cosmic shear measurement by utilizing both

I Scientific Highlights

033

A Numerical Scheme for Special Relativistic Radiation Magnetohydrodynamics
Based on Solving Time-dependent Radiative Transfer Equation
OHSUGA, Ken(Graduate University for Advanced Studies/NAOJ)		

Radiation transport (including the interaction between
the matter and the radiation) and magnetic fields play
important roles in a number of astrophysical phenomena.
Although some of approximate methods (Flux-limited
diffusion approximation [1], M1-closure method [2],and the Eddington approximation) are employed in orderto numerically solve the radiation fields, the accurate
radiation fields are not always obtained by such methods.
Recently, a new algorithm were proposed for theradiation magnetohydrodynamics (RMHD), in which thetime-dependent radiation transfer equation is solved andthe radiation energy density, flux, and stress tensor are
calculated by angular quadrature of the specific intensity[3]. However, their numerical code is accurate to O(v/c),and total energy as well as momentum of the radiation
magnetofluids is not necessarily conserved. We develop
a numerical scheme for solving the equations of fully
special relativistic RMHD, in which the conservationof total mass, momentum, and energy of the radiation
magnetofluids is guaranteed.
We propose a new method for RMHD, in which
we solve the fully special relativistic RMHD equations[4]. By solving the time-dependent radiation transfer
equation, the energy density, the flux, stress tensor forthe radiation, are computed by angular integrating of thespecific intensity. Ad hoc closure relation as used in FLD
approximation, M-1 closure method, and the Eddington
approximation is not required. The advection terms are
explicitly solved, and the source terms, which describe
the gas-radiation interaction, are implicitly integrated.
In Figure 1, we show the results of the relativistic shocktube problem, the gas density (ρ), the gas pressure (pg),the four velocity (u z), the radiation energy density (Erad),z ), zz-component of the Eddington
the radiation flux (F radzz ). The red lines indicate our results, and thetensor (D~ radresults by the Eddington approximation and M1-closure
method are plotted by blue and orange lines. The dottedlines in the panels of Erad, F zrad, and D~ zz
rad represent thereference solutions. We find that our results nicely agreewith the reference solutions. Our code shows reasonable
results in some numerical tests for propagating radiation
and radiation hydrodynamics.

034

I Scientific Highlights

TAKAHASHI, Hiroyuki R.
(NAOJ)

Figure 1: One-dimensional plots of the density, gas pressure,four velocity, radiation energy density, radiation flux,
and zz-component of the Eddington tensor for the nonrelativistic strong shock.

References[1] Levermore, C. D., Pomraning, G. C.: 1981, ApJ, 248, 321.
[2] Gonzalez, M., Audit, E., Huynh, P.: 2007, A&A, 464, 429.
[3] Jiang, Y.-F., Stone, J. M., Davis, S. W.: 2014, ApJS, 213, 7.
[4] Ohsuga, K., Takahashi, H. R.: 2016, ApJ, 818, 162.

Discovery of About 1000 Ultra Diffuse Galaxies in the Coma Cluster:Opening the Low Surface Brightness Universe with Archival Data
KODA, Jin

YAGI, Masafumi, YAMANOI, Hitomi, KOMIYAMA, Yutaka(NAOJ/Joint ALMA Observatory/Stony Brook University)			

Forty-seven low surface brightness (LSB) galaxies
were recently discovered in the direction of the Comacluster [1]. If they really reside in the cluster, thesegalaxies, namely ultra-diffuse galaxies (UDGs), have
only ~1/1000 of the Milky Way (MW)’s stellar mass(~107–8 M), but being as large as the MW in size withthe effective radius of re ~> 1.5 kpc. Such diffuse andpuffy stellar structures are subject to tidal disruption
in the cluster's gravitational potential [1,2]. If they are
long-lived, these stellar systems must be protected by alarge amount of dark matter halo, suggesting them to bepotential “dark galaxies”. Therefore, UDGs in clusters
provide an important clue to studies of galaxy formationand evolution, galactic dark matter, and galaxy clusters.
We analyzed archival data from the Subaru Prime
Focus Camera (Suprime-Cam) and discovered 854 UDGs
in the Coma cluster, ~ 20 times more than previously
reported [3]. Many of them (332) are Milky Way-sizedwith very large effective radii of re >1.5 kpc. About 2/3of the Coma cluster field (4.1 degree2) was observed bySuprime-Cam in the past, having deep R band images
with partial B, i, and Hα band coverage.
This significant leap in sample size enhanced ourknowledge of this important galaxy population. Our
discovery suggests about 1,000 UDGs in the Coma cluster
after accounting for the whole cluster size comparedto the smaller Subaru field. The Subaru UDGs show
a distribution concentrated clearly around the cluster
center, strongly suggesting that the great majority are(likely longtime) cluster members. They are a passively
evolving population, lying along the red sequence inthe color-magnitude diagram with no signature of Hαemission. Star formation was, therefore, quenched in thepast. They have exponential light profiles, effective radiire ~ 800 pc – 5 kpc, effective surface brightnesses μ e(R) =25–28 mag arcsec−2, and stellar masses ~ 1 × 107 M – 5
× 108 M. There is also a population of nucleated UDGs.
Some MW-sized UDGs appear closer to the cluster center
than previously reported; their survival in the strong tidal
field, despite their large sizes and longevities, indicatesa large dark matter fraction protecting the diffuse stellar
component. The indicated baryon fraction < 1 % is lessthan the cosmic average, and thus the gas must have been
removed (from the possibly massive dark halo). The UDG
population is elevated in the Coma cluster compared to
the field, indicating that the gas removal mechanism isrelated primarily to the cluster environment.
Beyond the importance of UDGs, this study clearly(NAOJ)

demonstrated the treasury value of archival data, andunveiled the new discovery space of the low surface
brightness universe using the Subaru telescope and its
large format cameras.

Figure 1: Subaru BRi color image of the ~6′ × 6′ region (~ 170 ×
170 kpc2 region at d = 97.7 Mpc) out of the 4.1 degree2
Subaru coverage. The van Dokkum’s Dragonfly UDGs
and Subaru UDGs are marked respectively with yellow
and green circles with a diameter of 20″ (~ 9.5 kpc).

References[1] van Dokkum, P. G., Abraham, R., Merritt, A., et al.: 2015, ApJ,
798, L45.
[2] Penny, S. J., Conselice, C. J., de Rijcke, S., Held, E. V.: 2009,
MNRAS, 393, 1054.
[3] Koda, J., Yagi, M., Yamanoi, H., Komiyama, Y.: 2015, ApJ,
807, L2.

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035

Discovery of an Inner Disk Component around HD 141569 A
KONISHI, Mihoko1*, GRADY, Carol A.2/3, SCHNEIDER, Glenn4, SHIBAI, Hiroshi5, MCELWAIN, Michael W.3
NESVOLD, Erika R.6, KUCHNER, Marc J.3, CARSON, Joseph7, DEBES, John. H.8, GASPAR, Andras4
HENNING, Thomas K.9, HINES, Dean C.8, HINZ, Philip M.4, JANG-CONDELL, Hannah10
MORO-MARTÍN, Amaya8, PERRIN, Marshall8, RODIGAS, Timothy J.6, SERABYN, Eugene11
SILVERSTONE, Murray D.2, STARK, Christopher C.8, TAMURA, Motohide12/1/13, WEINBERGER, Alycia J.6
WISNIEWSKI, John. P.14
1: NAOJ, 2: Eureka Scientific, 3: Goddard Space Flight Center, 4: The University of Arizona, 5: Osaka University, 6: Carnegie Institutionof Washington, 7: College of Charleston, 8: Space Telescope Science Institute, 9: Max Planck Institute for Astronomy, 10: University of
Wyoming, 11: Jet Propulsion Laboratory, 12: Astorobiology Center, 13: University of Tokyo, 14: University of Oklahoma

Planets are considered to form in protoplanetarydisks during star formation process. Protoplanetarydisks and planets interact with each other. Thus, detailunderstanding of disk structures is important in order
to elucidate star and planet evolution. Disks have been
imaged recently, and it has become clear that they havecomplex structures.
This work [1] is focused on a disk around HD 141569 A(spectral type: B9.5, age: 5 Myr). This is a young debris
disk, containing various complex structures that havebeen imaged in the optical and near-infrared (e.g., [2,3,4]).
The disk has a double-ring structure (inner and outer ring)with spiral structures, and a cavity inside the inner ring(< 175 AU). In addition, emission from dust and CO gas
has been detected inside the inner ring using mid-infrared(e.g., [5]) and CO emission lines (e.g., [6]). We obtaineddisk images in the optical, using Space Telescope Imaging
Spectrograph (STIS) aboard on Hubble Space Telescope(HST) as a part of general observer program (GO 13786).
The scattered light from an inner disk component within
the known inner ring was firstly detected, after adopting
suitable analysis in that the scattered light from the disk
and star light were divided. The inner disk component
extends from 0″.4 (46 AU) to 1″. 0 (120 AU) in deprojected
stellocentric distance, with no gaps or a cavity. A spiral
was detected at 130 AU. A pericenter offset of 6 AU may
exist towards the north. An unseen planet would trigger
such spiral and gap structures between the inner disk
component and the inner ring. However, our data indicatethat there is no point source heavier than 9 MJ in thegap. On the other hand, the mass of the planet that could
create such gap is < 1 MJ, as estimated by the dynamical
model [7]. Thus, we cannot reject the possibility that an
unseen planet creates the gap.

* Affiliation was Osaka University when the paper was published.

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Figure 1: HD 141569 A disk image (see [1]). Nomenclature isannotated on the lower panel that is the same image as
the upper panel. Star mark indicates the HD 141569 A
position. Component C is the inner disk component that
we discovered.

References[1] Konishi, M., et al.: 2016, ApJ, 818, L23.
[2] Weinberger, A. J., et al.: 1999, ApJ, 525, L53.
[3] Mouillet, D., et al.: 2001, A&A, 372, L61.
[4] Clampin, M., et al.: 2003, AJ, 126, 385[5] Fisher, R. S., et al.: 2000, ApJ, 532, L141.
[6] Goto, M., et al.: 2006, ApJ, 652, 758.
[7] Nesvold, E. R., Kuchner, M. J.: 2015, ApJ, 798, 83.

FastSound: The Subaru FMOS Galaxy Redshift Survey
TONEGAWA, Motonari1, TOTANI, Tomonori1, OKADA, Hiroyuki1, AKIYAMA, Masayuki2, DALTON, Gavin3
GLAZEBROOK, Karl4, IWAMURO, Fumihide5, MAIHARA, Toshinori5, OHTA, Koji5, SHIMIZU, Ikkoh1
TAKATO, Naruhisa6, TAMURA, Naoyuki7, YABE, Kiyoto6, BUNKER, Andrew J.3/7, COUPON, Jean8FERREIRA, Pedro G.3, FRENK, Carlos S.9, GOTO, Tomotsugu10, HIKAGE, Chiaki11, ISHIKAWA, Takashi5
MATSUBARA, Takahiko11, MORE, Surhud7, OKUMURA, Teppei7, PERCIVAL, Will J.12
SPITLER, Lee R.13/14, SZAPUDI, Istvan15
1: University of Tokyo, 2: Tohoku University, 3: University of Oxford,4: Swinburne University of Technology, 5: Kyoto University, 6: NAOJ,
7: Kavli IPMU, 8: University of Geneva, 9: University of Durham, 10: National Tsing Hua University, 11: Nagoya University, 12: Portsmouth
University, 13: Australian Astronomical Observatory, 14: Macquarie University, 15: University of Hawaii

Table 1: Number of emission lines and estimated contamination
rate for several S/N thresholds.
S/N ≥ 5.0
S/N ≥ 4.5
S/N ≥ 4.0
S/N ≥ 3.5

Line Number
3,080
3,769
4,797
6,805

Contamination
2.3 %
4.5 %
9.2 %
22.2 %

RSD was detected with 4σ confidence level from aclustering analysis with this data [2], giving the linear
growth rate of the large-scale structure (fσ8 = 0.482 +0.116−0.116 atz = 1.4), which is consistent with the prediction of ΛCDM
model. Fundamental metallicity relation of FastSoundgalaxies was also examined using detected Hα and [N II]
lines [5].
Redshift catalog has been created from these data [4]and become public (http://www.kusastro.kyoto-u.ac.jp/
Fastsound/index.html) and accessible to anyone.
CFHTLS W2

36.5

36.0 35.5 35.0
RA (J2000) [deg ]

34.5

34.0

−5.0

−4.5

37.0

DEC (J2000) [deg ]−4.0 −3.5 −3.0 −2.5

−5.5

−2.0

DEC (J2000) [deg ]
−5.0
−4.5
−4.0

CFHTLS W1

136.0 135.5 135.0 134.5 134.0 133.5 133.0
RA (J2000) [deg ]CFHTLS W4−0.5

DEC (J2000) [deg ]
0.0
0.5
1.0

DEC (J2000) [deg ]52.5 53.0 53.5 54.0

54.5

1.5

55.0

CFHTLS W3

52.0
51.5

Recent precision cosmological observations
have revealed that our Universe is in the phase ofan accelerated expansion currently. However, thisunexpected acceleration is still a mystery, with possible
two descriptions: an exotic form of energy with negative
pressure (dark energy) and breakdown of generalrelativity on cosmological scales (modified gravity).
FastSound project is a redshift survey with FMOS on
Subaru telescope, probing a distant Universe beyond
redshift one for the first time. The primary goal is todetect an anisotropy in the 3-D distribution of galaxies
brought by redshift space distortion (RSD), measure
the growth rate of the large-scale structure fσ 8 , andtest gravity theories by comparing fσ8 with theoreticalpredictions.
The observation was carried out over 35 nights from
April 2012 to July 2014, taking spectra of ~47,000
galaxies over 20 deg 2. Target selection was based on
optical 5 bands (u*g'r'i'z') of CFHTLS Wide 1–4. The
image data was processed using the standard reduction
pipeline of FMOS [1], followed by automated emission
line detection by a dedicated software algorithm [3],resulting in ~4,000 emission line detections. Table 1
shows the number of emission lines and estimatedcontamination rate for several S/N thresholds, andFigure 1 is the galaxy distribution on the celestial sphere.

217

216

215
214
RA (J2000) [deg ]

213

212

335.5

335.0 334.5 334.0
RA (J2000) [deg ]

333.5

333.0

Figure 1: The 2-D distribution of FastSound galaxies. Blue
dots are galaxies whose emission lines are detected innormal spectrum, while red dots are those for which
the line detection algorithm find signals in inverted (−1multiplied) spectrum. The latter gives an estimation offalse detection rate.

References[1] Iwamuro, F., et al.: 2012, PASJ, 64, 59.
[2] Okumura, T., et al.: 2016, PASJ, 68, 38.
[3] Tonegawa, M., et al.: 2015, PASJ, 67, 31.
[4] Tonegawa, M., et al.: 2015, PASJ, 67, 81.
[5] Yabe, K., et al.: 2015, PASJ, 67, 102.

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037

Internal Structure of the Moon Inferredfrom Apollo Seismic Data and Latest Selenodetic Data
MATSUMOTO, Koji, YAMADA, Ryuhei, KIKUCHI, Fuyuhiko, HANADA, Hideo(NAOJ)

ISHIHARA, Yoshiaki, IWATA, Takahiro

038

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final stage of magma ocean solidification, sank down to
the deep interior due to gravitational instability.

0
200

(b)

(c)

(d)
0
200
800

400
600
800
1000
1200
1400

400

1000

600
800

1200

1000

1400

3400 3600

Depth [km](a)Megaregolith
Crust

The knowledge of the internal structure of the Moon
is a key to understand the origin and the evolution of
our nearest celestial body. The Apollo seismic data havebeen successfully used to infer its internal structure.
However, the network consisted of only a few near-side
observation points, and the deepest source is locatedat roughly 1200 km depth (~540 km radius). Thus, themodels of the lunar interior deeper than 1200 km are
different by authors (e.g., [1,2]), leaving the structurenear the center uncertain. On the other hand, information
on density and viscoelastic profiles can be obtained bymeasuring moments of inertia and tidal response of theMoon through observation of lunar rotation and gravity
variations. Recently, Gravity Recovery and Interior
Laboratory (GRAIL) mission has accurately observedslight tidal change in gravity, and estimates of quality
factor have also been updated [3]. It is also shown by
numerical calculations that frequency dependence of thequality factor can be explained by existence of ultra lowviscosity zone at the base of the lower mantle [4]. This
study explores eight-layer lunar internal structure models
with such a deep-seated low-viscosity zone which areconsistent with both the data sets of the latest selenodetic
data and Apollo seismic data [5].
Fig. 1 shows vertical profiles inferred by Markov chain
Monte Carlo algorithm. Estimated value of mean crustal
thickness is 44 ± 10 km, that of fluid outer core radius is
335 +60−115 km, that of solid inner core with assumed densityof 8000 kg/m 3 is < 260 km, those of P- and S-wave
velocities in the low-velocity zone above the core-mantle
boundary are VP = 7.1 ± 1.0 km/s and VS = 2.9 ± 0.5 km/s,
and that of the viscosity of the same zone is about 3 ×
1016 Pa s, respectively. The top of the low-velocity andlow-viscosity zone is located at about 570 km from thecenter and this zone is considered to extend into the deep
moonquake region. Although previous study suggeststhat the thickness and density of the low-velocity zone
are 150 km and 3400 kg/m3 [1], respectively, those values
inferred by this study are > 170 km and 3450 – 3650 kg/m3,
respectively. This density at the the pressure near the
core-mantle boundary of about 4.5 GPa is consistent withthat of titanium-rich basalt measured by high-pressureand high-temperature experiments [6]. Such a Ti-richcomposition deep in the mantle supports a lunar evolution
model involving lunar mantle overturn in which the Tirich material, that was formed in the upper mantle at the

SASAKI, Sho(ISAS/JAXA)			

Upper mantle
Middle mantle
Lower mantle
Low velocity zone
Fluid outer core
Solid inner core

(Hokkaido University)			

Depth [km]

KAMATA, Shunichi

1200
1400

1600

1600
12345678

1 2 3 4 5 6 7 8 9Layer #Vp [km/s]

0

1

2

3

4

Vs [km/s]

54000 6000 8000

Density [kg/m3]

Figure 1: Vertical profiles of (a) modeled layer, (b) P wave
velocity, (c) S wave velocity, and (d) density. A darker
black color indicates a higher probability of occurrence.
Green broken lines indicate the 2-sigma uncertainty of
our results. Models by [1] and [2] are indicated as red
and blue dotted lines, respectively.

References[1] Weber, R. C., et al.: 2011, Science, 331, 309-312.
[2] Garcia, R. F., et al.: 2011, Phys. Earth Planet. Inter., 188, 96113.
[3] Williams, J. G., Boggs, D. H.: 2015, J. Geophys. Res., 120, 689724.
[4] Harada, Y., et al.: 2014, Nat. Geosci., 7, 569-572.
[5] Matsumoto, K., et al.: 2015, Geophys. Res. Lett., 42, 73517358.
[6] Sakamaki, T., et al.: 2010, Earth Planet. Sci. Lett., 299, 293297.

Radiation Drag Effects in Black Hole Outflows
from Super-critical Accretion Disks
via Special Relativistic Radiation Magnetohydrodynamics Simulations
TAKAHASHI, Hiroyuki R., OHSUGA, Ken(NAOJ)

A black hole accretion disk system is one of the mostenergetic phenomena in the universe. A mass accretion
onto the black holes results in efficient gravitationalenergy release. According to the mass accretion rate,
three accretion modes, i.e., standard disk model,
radiatively inefficient accretion flow model, and slim disk
model have been proposed. Whereas these three models
are established by one-dimensional approach, multidimensional effects are also very important because jets
and outflows are observed in black hole accretion disk
system. Also the relativistic effects should be taken into
account since the jet velocity is close to the light speed.
For the case of high accretion rate (slim disk), a radiation
is an important ingredient for understanding disk andjet structures. The radiation pressure dominates the gaspressure, so that the most of energy is transported in
the form of radiation. Such a large amount of radiationenergy would form the radiatively driven jets or outflows.
Thus, the relativistic radiation magnetohydrodynamic(RRMHD) simulations are required to study theradiatively-driven high-velocity outflows. In thispaper, we performed RRMHD simulation to study themechanisms of outflow acceleration and determine theoutflow speed [1].
Figure 1 shows overall structure of the accretion
disks. At this time (t = 10 s), the accretion rate onto
the black hole is M·  1000 M Edd . Here M· Edd is the
Eddington accretion rate M· Edd ≡ 4π GMBH/cκes = 1.4 ×
10 18 (M BH/10 M ) g s −1, where G is the gravitational
constant, c is the light speed, MBH = 10 M is the blackhole mass, and κes is the opacity for electron scattering.
Thus the super-critical accretion is stably realized.
Besides the accretion flow, a fast relativistic outflow isobserved just above the accretion disks (arrows in theright panel). The direction of velocity vector almost
coincides with the radiation flux vector (arrows in the left
panel), indicating that the relativistic flow is accelerated
by the radiation force. The gas is accelerated at the small
altitudes, and its velocity finally saturates at the outerregion (z >~ 100 rS, where rS is the Schwarzschild radius).
The terminal outflow velocity is about 0.3 – 0.4 c, which
nicely agrees with the jets speed (0.26 c) observed in
SS433. Considering the outflow acceleration, a balance
between two forces determines the terminal velocity. First
one is the radiation flux force, which pushes the gas awayfrom the accretion disks. Then the gas is accelerated
upward. The accelerated gas is subjected to the radiation

drag force, which prevents the outflow from further
acceleration. By comparing these two forces, the outflow
velocity is estimated at 0.3–0.4 c. We observed that these· ·4results are justified in the range of 102 <~ M / MEdd <~ 10 .

t=10s
12.0

14.0

16.0

200

200

150

150

100

100

50

50

0

0

-50
-50
-100 -80 -60 -40 -20 0-9.0 -7.0 -5.0 -3.0 -1.0

20 40 60 80 100

Figure 1: Overall structure of the super critical accretion disks.
Left and right colors show the radiation energy density
and gas density. The arrows show the radiation flux
(left) and the velocity (right). Solid and dashed curves
denotes where the total and effective optical depths
become unity.

Reference[1] Takahashi, H. R., Ohsuga, K.: 2015, PASJ, 67, 60.

I Scientific Highlights

039

Near-infrared Imaging Observations of Circumstellar Disk
around HD 169142 with Subaru/HiCIAO
MOMOSE, Munetake1, MORITA, Ayaka1, FUKAGAWA, Misato2, MUTO, Takayuki3, TAKEUCHI, Taku4, HASHIMOTO, Jun2/5
HONDA, Mitsuhiko6, KUDO, Tomoyuki2, OKAMOTO, Yoshiko K.1, KANAGAWA, Kazuhiro D.7, TANAKA, Hidekazu8
GRADY, Carol A.9/10/11, SITKO, Michael L.12/13, AKIYAMA, Eiji2, CURRIE, Thayne2, FOLLETTE, Katherine B.14
MAYAMA, Satoshi15, KUSAKABE, Nobuhiko2/5, ABE, Lyu16, BRANDNER, Wolfgang17, BRANDT, Timothy D.18
CARSON, Joseph C.19, EGNER, Sebastian2, FELDT, Markus17, GOTO, Miwa20, GUYON, Olivier2, HAYAHO, Yutaka2
HAYASHI, Masahiko2, HAYASHI, Saeko S.2, HENNING, Thomas17, HODAPP, Klaus W.21, ISHII, Miki2, IYE, Masanori2
JANSON, Markus24, KANDORI, Ryo2, KNAPP, Gillian R.23, KUZUHARA, Masayuki4, KWON, Jungmi24, MATSUO, Taro25
McELWAIN, Michael W.9, MIYAMA, Shoken26, MORINO, Jun-Ichi2, MORO-MARTIN, Amaya23/27, NISHIMURA, Tetsuo2
PYO, Tae-Soo2, SERABYN, Eugene28, SUENAGA, Takuya2/15, SUTO, Hiroshi2, SUZUKI, Ryuji2, TAKAHASHI, Yasuhiro H.2/24
TAKAMI, Michihiro29, TAKATO, Naruhisa2, TERADA, Hiroshi2, THALMANN, Christian30, TOMONO, Daigo2
TURNER, Edwin L.23/24, WATANABE, Makoto31, WISNIEWSKI, John32, YAMADA, Toru33, TAKAMI, Hideki2
USUDA, Tomonori2, TAMURA, Motohide2/5/24
1: Ibaraki University, 2: NAOJ, 3: Kogakuin University, 4: Tokyo Tech., 4: ABC, 6: Kurume University, 7: Szczecin University, 8: Tohoku Univsersity, 9:Goddard Space Flight Center, 10: Eureka Scientific, 11: Goddard Center for Astrobiology, 12: Space Science Institute, 13: University of Cincinnati, 14:
University of Arizona, 15: Sokendai, 16: Universitè de Nice-Sophia Antipolis, 17: Max Planck Institute for Astronomy, 18: Institute for Advanced Study,
Princeton, 19: College of Charleston, 20: Universitäts-Sternwarte München, 21: University of Hawaii, 22: Stockholm University, 23: Princeton University,
24: University of Tokyo, 25: Osaka University, 26: Hiroshima University, 27: CAB-CSIC/INTA, 28: Jet Propulsion Laboratory, 29: Institute of Astronomy
and Astrophysics, Academia Sinica, 30: University of Amsterdam, 31: Hokkaido University, 32: University of Oklahoma, 33: ISAS/JAXA(arcsec)

1.2
0.8

0

0.4
0.0

-1
+1

log(PI in [mJy arcsec-2])

+1

0-1

(arcsec)

Figure 1: PI image with HiCIAO. Green circle and whitecross indicate the masked region and stellar position,
respectively.

040

I Scientific Highlights

0.2

Radius [arcsec]
0.4
0.6 0.8 1.0

10-2[mJy arcsec ]1.6

with a transition zone, exhibiting an apparent gap in r =40–70 au.
The observed radial profile of the PI is reproduced bya minimally flaring disk with an irregular surface density
distribution or with an irregular temperature distribution
or with the combination of both. The depletion factorof surface density in the inner power-law region (r <50 au) is derived to be ≥ 0.16 from a simple model
calculation. The obtained PI image also shows small scale
asymmetries in the outer power-law region. Possible
origins for these asymmetries include corrugation of thescattering surface in the outer region, and shadowing
effect by a puffed up structure in the inner power-law
region.

Mean Suface Brightness

HD 169142 is a Herbig Ae star (A8 Ve) located at
a distance of 145 pc from the Sun [1]. Interferometricobservations at millimeter and submillimeter wavelengths
revealed a circumstellar disk around HD 169142, withthe radius of 1.4″ (≈ 200 au) and with its inclination
angle of 13° [2,3]. Near-infrared imaging with the HST
coronagraph also detected scattered light with similar
size [1]. The amount of excess emission at mid-infrared
wavelengths is small, suggesting that the outer disk is
truncated at ~ 0.15″ (~ 20 au) from the star [4,5]. We
carried out polarization differential imaging (PDI) of thedisk scattered light in H-band with Subaru/HiCIAO.
Figure 1 shows the obtained polarized intensity (PI)image. The emission scattered by dust particles at thedisk surface in 0.2″ ≤ r ≤ 1.2″, or 29 ≤ r ≤ 174 au, issuccessfully detected. The azimuthally-averaged radial
profile of the PI, shown in Figure 2, manifests a double
power-law distribution, in which the PIs in r = 29–52 au
and r = 81.2–145 au respectively show r −3-dependence.
These two power-law regions are connected smoothly

1

30

50
70
100
Radius [AU]Figure 2: Azimuthally-averaged radial profile of PI surface
brightness.
References[1] Grady, C. A., et al.: 2007, ApJ, 665, 1391.
[2] Raman, A., et al.: 2006, ApJ, 131, 2290.
[3] Panic, O., et al.: 2008, A&A, 491, 219.
[4] Meuus, G., et al.: 2010, A&A, 518, L124.
[5] Honda, M., et al.: 2012, ApJ, 752, 143.
[6] Momose, M., et al.: 2015, PASJ, 67, 83.

Nuclear Fission and Solution of r-Process Underproduction Problem
						

SHIBAGAKI, Shota, KAJINO, Toshitaka

MATHEWS, Grant J.

(University of Tokyo/NAOJ)		

CHIBA, Satoshi(Tokyo Institute of Technology)(University of Notre Dame/NAOJ)NISHIMURA, Shunji(RIKEN Nishina Center/NAOJ)

LORUSSO, Giuseppe(National Physical Laboratory/RIKEN Nishina Center/University of Surrey)

the elements produced in the NDW and NSM model
supplement the underproduced elements of the MHDJ
model, and the resulting total elemental abundance
pattern is very close to the solar-system r-process
abundances.
-2

10

Weak (NDW)
Main (MHDJ)
Fission Recycling (NSM)
Sum

-3

10
Abundance Yi

The origin of heavy elements like gold and uranium,
called r-process elements, is one of the important mysteryin astrophysics. There are several candidates for r-processsources such as the neutrino-driven wind (NDW) of corecollapse supernovae (CCSNe), magnetohydrodynamic
jets (MHDJs) from CCSNe and binary neutron-starmergers (NSMs), but the major r-process source has notbeen identified yet.
Although the formation process of the characteristic
r-process abundance peaks around mass numbers 130
and 195 is understood well, the elemental abundances
just above and below those peaks are frequently
underproduced by more than an order of magnitude in
the literature. This underproduction has been interpreted
as the result of the strong shell closure. It is known thatthe resulting elemental abundances matches well to thesolar-system r-process abundances if the shell effects
is quenched enough. However, there is no experimental
evidence of the shell quenching, and some alternative
solutions of the underproduction problem are desirable.
We proposed a scenario that contribution of NSMs
solves the underproduction problem. In such neutronrich environments, like NSMs, that neutron-rich fissile
nuclei are synthesized, the resulting r-process elemental
abundances are sensitive to the applied fission model.
We performed numerical simulations of r-process
nucleosynthesis for dynamical ejecta from the NSM
model [1,2,3] with a realistic fission model. We used
an extended version of the nuclear reaction network
described in [4], where some nuclear reactions basedon the KTUY nuclear mass model and a new fission
fragment distributions model [5] are newly adopted.
The red line in Figure 1 [6] shows the result of
the nucleosynthesis simulation for the NSM model incomparison with the solar-system r-process abundances[7] represented in the black dots. The flat abundance
pattern between A = 100 and 160, which has not beenfound in the literature, is due to the new fission model
adopted, which predicts that a wide mass range of fission
products is formed. The results of the nucleosynthesis
simulations for the NDW model and the MHDJ modeltaken from [8,9] are also plotted in Figure 1. Those
three models shows the completely different elemental
abundance patterns. The total abundance curve fromall models is shown as the black line. We found that

10-4
10-5
10-6
-7

10

80

100

120

140

160

180

200

Mass Number A
Figure 1: Solar-system isotopic r-process abundance pattern.
Observation (black dots) vs. theoretical calculation
which consists of the r-process in magnetohydrodynamic
jet supernova model (blue), neutrino-driven wind model(green), binary neutron-star merger model (red) and totalsum (black).

References[1] Terasawa, M., et al.: 2001, ApJ, 562, 470.
[2] Chiba, S., et al.: 2008, AIP Conf. Proc., 1016, 162.
[3] Korobkin, O., et al.: 2012, MNRAS, 426, 1940.
[4] Piran, T., et al.: 2013, MNRAS, 430, 2121.
[5] Rosswog, S., et al.; 2013, MNRAS, 430, 2585.
[6] Shibagaki, S., et al.: 2016, ApJ, 816, 79.
[7] Goriely, S.: 1999, A&A, 342, 881.
[8] Wanajo, S.: 2013, ApJ, 770, L22.
[9] Nishimura, N., et al.: 2012, Phys. Rev. C, 85, 048801.

I Scientific Highlights

041

Black Hole Mass Measurement in Nearby Galaxy
Using Molecular Gas Dynamics(SOKENDAI/NAOJ)		

Abstract— A new method is carried out to measure
SuperMassive Black Hole (SMBH) mass in the centerof nearby galaxy NGC 1097, by using dense moleculargas dynamics traced with HCN(J=1–0). The dynamics isobserved with Atacama Large Millimeter/submillimeter
Array (ALMA). This work demonstrates the capabilityof radio interferometers to measure SMBH mass, whichhelps to better understand the evolution of black holes
and hence their host galaxies. The original paper ispublished by Astrophysical Journal in June 2015 [1].
Here we quote the published paper and our related works.
Introduction— Observations and studies particularlyin the last two decades have shown that every stellar
spheroids harbor SuperMassive Black Holes (SMBHs;
larger than 106 M where M is the mass of the sun)in their centers [2]. Meanwhile, developed observing
facilities allowed us to measure the SMBH mass in someof the nearby galaxies by using different dynamical
methods. The measured SMBH mass (M BH ) areempirically known to be tightly correlated to host galaxy
bulge properties such as central velocity dispersionof stars (known as MBH − σ relation, [2,3,4,5]). These
correlations, together with recent numerical simulations,suggest that galaxy and black hole evolves by influencing
each other. SMBH mass is thus considered to be the key
parameter to better understand the growth of galaxy and
SMBH. SMBH mass measuring method using moleculargas dynamics, observed with radio interferometers,
enables one to measure more SMBH mass in thisAtacama Large Millimeter/submillimeter Array (ALMA)
era. Reference [1] and [6] started this method with newly
developed radio interferometers. With a larger sample
realized with this new method, correlations such as MBH− σ relation are expected to be better constrained, andeventually makes the co-evolutionary process of galaxy
and black hole to be better understood.
Data— NGC 1097 is a nearby Type-1 Seyfert galaxy
at a distance of 14.5 Mpc [7] (~70 pc arcsecond−1). The
nucleus is located at RA (J2000.0) = 02 h 46 m 18 s .96,
DEC (J2000.0) = −30°16′28″.9 [8]. The SMBH massin NGC 1097 is estimated to be (1.2 ± 0.2) × 108 M byusing the empirical MBH − σ relation from [3] with anobserved σ = 196 ± 5 km s−1 [9].
SMBH mass measurement— We measure the SMBH
mass in NGC 1097 by using molecular gas dynamics
observed with ALMA. The method is described inreference [1], while we give a short summary here.
A Position-Velocity Diagram (PVD) is cut along the042

I Scientific Highlights

SHETH, Kartik(National Aeronautics and Space Administration)

KOHNO, Kotaro(The University of Tokyo)

galaxy major axis (P.A = 130°) from the observed datato compare with the model velocity field, calculated by
MGE_circular_velocity method [10] and Kinematic
Molecular Simulation (KinMS) [6]. The model considersa mass-to-light ratio (M/L) and SMBH mass as freeparameters. We run a grid simulation to obtain MBH =+0.03
81.40 +0.27−0.32 × 10 M , M/L = 5.14 −0.04 with a reduced chisquare χ2red = 1.09 realized by the best fit (see Figure).

300

model parameters:
MB H = 1.4
M/L = 5.14
:model:observed

200
Velocity (km/s)

ONISHI, Kyoko, IGUCHI, Satoru

100
0

-100
-200
-300

2=113
2 =1.09
red
-10

-5

0
5
offset (arcsec)

10

Figure 1: Comparison of the observed PVD and the model (greyscale filled contours and yellow points) and the model(black contours and purple lines). Model parameters are
set to be MBH = 1.40 × 108 M, M/L = 5.14. The reduced
chi-square is χ 2red = 1.09 with the degree of freedom of104.

References[1]Onishi, K., et al.: 2015, ApJ, 806, 39.
[2]Kormendy, J., Ho, L. C.: 2013, Ann. Rev. Astron. Astrophys., 51,511.
[3] McConnell, N. J., Ma, C.-P.: 2013, ApJ, 764, 184.
[4] Ferrarese, L., Merritt, D.: 2000, ApJ, 539, L9.
[5] Gltekin, K., et al.: 2009, ApJ, 698, 198.
[6] Davis, T. A., et al.: 2013, Nature, 494, 328.
[7] Tully, R. B.: 1988, Nearby Galaxies Catalog (Cambridge:
Cambridge University Press).
[8] Hummel, E., et al.: 1987, A&AS, 70, 517.
[9] Lewis, K. T., Eracleous, M.: 2006, ApJ, 642, 711.
[10] Cappellari, M., et al.: 2002, ApJ, 578, 787.

Effect of Stellar Encounters on Comet Cloud Formation			

HIGUCHI, Arika(Tokyo Institute of Technology)		

The Oort Cloud is a spherical comet reservoir
surrounding the Solar system [1]. Observations andstatistical studies estimate that it consists of more than
1012 comets and is on the order of 104–105 AU in size(e.g., [2]). Now it is generally accepted that the comets
are residual planetesimals from planet formation and are
originally inside the planetary region. In the standard
scenario of the Oort cloud formation, passing stars
randomize and eject planetesimals from the Solar system
by giving velocity kicks. The perturbations from passingstars, due to their random-walk nature, may play animportant role in the production of the nearly isotropic
inclination distribution of planetesimals Many authors
have examined this effect, however, their main interest
is in the production of long-period comets from thespherical Oort cloud (e.g., [3]).
In the present paper we investigate the effect of stellar
encounters on the evolution of a planetesimal disk, fromthe point of view of Oort Cloud formation. We calculate
the evolution of a planetesimal disk into a spherical
Oort cloud due to the perturbation from passing stars
for 10 Gyr. We use the classical impulse approximation
to calculate the perturbation from the passing stars. The
stellar encounters are assumed to occur with random
directions and follow the distribution dns/db ∝ b, wheren s and b are a number of stellar encounters and theposition vectors to the star from the Sun, respectively.
The time interval to the next stellar encounter is given
according to a Poisson distribution [3].
The number of planetesimals decreases while the
distributions of the orbital elements approach the isotropic
distribution. We fit the decay curve empirically using
the standard exponential decay curve and the stretchedexponential decay defined by the Kohlrausch formula [6].
Let Pbound denotes the survival rate of planetesimals in the
Solar system. The empirical fit for Pbound for the standard
exponential decay is

KOKUBO, Eiichiro(NAOJ)

times to the Oort cloud. We show that if the initialplanetesimal disk has the semimajor axes distribution
dn/da ∝ a−2, which is produced by planetary scattering[7]. the e-folding time for planetesimals in the Oort
cloud is ~10 Gyr at any heliocentric distance r (Fig. 1).
This uniform e-folding time over the Oort cloud meansthat the supply of comets from the inner Oort cloud tothe outer Oort cloud is sufficiently effective to keep thecomet distribution as dn/dr ∝ r−2. We also show thatthe final distribution of the semimajor axes in the Oort
cloud is approximately proportional to a−2 for any initial
distribution [8].

Figure 1: Standard e-folding time against r.

References[1] Oort, J. H.: 1950, Bull. Astron. Inst. Netherlands, 11, 91.
[2] Dones, L., et al.: 2004, In Comet II.
[3] Heisler, J., Tremaine, S., Alcock, C.: 1987, ICARUS, 70, 269.
[4] Dobrovolskis, A. R., Alvarellos, J. L., Lissauer, J. J.: 2007
ICARUS, 188, 481.
[5] Higuchi, A., Kokubo, E., Mukai, T.: 2006, AJ, 131, 1119.
[6] Higuchi, A., Kokubo, E.: 2015, AJ, 150, 17.

where a0 is the initial semimajor axes of the planetesimals, m * and v * are the stellar mass and velocity,respectively, and fenc is the encounter frequency per 1
Myr within 1 pc from the Sun.
We also show the radial variations of the e-folding

I Scientific Highlights043

Developments of Millimeter-wave MKID Camera
SEKIMOTO, Y., DOMINJON, A., KARATSU, K., NOGUCHI, T., MATSUO, H., SHAN, W. L., KIUCHI, H.
(NAOJ)SEKINE, M., SEKIGUCHI, S., SHU, S.

NITTA, T., YAMADA, Y., HISAMATSU, S.

(University of Tokyo/NAOJ)			

MKID (Microwave Kinetic Inductance Detector)
group of Advanced Technology Center is developing
superconductive camera in millimeter and terahertz
wavelengths for Antarctica terahertz telescope/Nobeyama
45m telescope which observes distant galaxies with wide
field-of-view and for LiteBIRD which detects CMB
B-mode polarization in collaboration with University ofTsukuba, Saitama University, ISAS/JAXA, KEK, andRiken. Five papers related to millimeter/submillimeter
MKID instruments were published in 2015 fiscal year.
1. Nb/Cu bilayer MKIDMKID is a Cooper pair breaking detector, in which
superconducting resonators sense variations of the surface
impedance caused by quasi-particles, which are generated
by higher frequency photons than the gap frequency. A
gap frequency is proportional to the critical temperature(Tc) of a superconductor film. For aluminum, Tc = 1.1 K
corresponds to the gap frequency of 90 GHz. If the gap
frequency (or Tc) can be adjusted, it makes easier to use
MKID for millimeter and submillimeter observations.
Dominjon et al. [1] have developed Nb/Cu bilayer
MKID. The T c of the bilayer can be settled by the
thickness of Nb and Cu. Fig. 1 shows the evoluation of Tc
as a function of the Nb layer thickness.

Figure 1: (Left) Evoluation of the critical temperature Tc of the
Nb/Cu bilayer respect to the Nb layer thickness [1].
(Right) A resonance of MKID taken by a frequency
sweeping FFT readout system [2].

2. Frequency sweeping readout
MKID is capable of frequency multiplexing with highQ superconducting resonators. To utilize this advantage,
we are developing multi-channel FFT readout system. A
frequency sweeping readout with synchronizing the FFTinterval has been proposed and demonstrated [2]. This
enables us to read multi-channel MKIDs with a large
dynamic range (Fig. 1).

044

I Scientific Highlights(University of Tsukuba)		

NARUSE, M.

(Saitama University)

3. Dual polarization MKID camera
A combination of Si lens array and double slot
antenna connected to MKID has been developed (eg.
Nitta et al., 2014). This paper demonstrates singlelayer dual polarization capability of the lens and double
slot antenna with MKID (Fig. 2), which improves thesensitivity of millimeter observations [3].

Figure 2: (Left) A picture of the dual polarization antenna coupled
to an MKID. (Right) Corrugated-horn coupled OMTMKID focal plane of LiteBIRD.

4. LiteBIRD focal plane design
Observations of B-mode polarization of cosmic
microwave background radiation (CMB) sense theinflation theory (K. Sato, 1981), which explains the hot
big-bang. This paper shows a focal plane design withcorrugated horn coupled OMT-MKID of LiteBIRD (Fig.
2), which observes CMB B-mode polarization from thegravitational wave.
5. Radiation tolerance of MKID
Radiation tolerance of Al-MKID has been
investigated. NEP of MKD has been measured at thelevel of 2 × 10−18 W/√H̄z before and after the total doseof 10 k rad, which corresponds 5 years absorption at theLagrange point [5].

References[1] Dominjon, A., et al.: 2016, IEEE Trans. Appl. Supercond., 26,
online available.
[2] Kiuchi, H., et al.: 2016, IEEE Trans. Terahertz Sci. Technol., 5,456.
[3] Naruse, M., et al.: 2015, Int. J. Infrared Millimeter THz, 37,
128.
[4] Sekimoto, Y., et al.: 2015, ESA antenna workshop.
[5] Karatsu, K., et al.: 2016, JLTP online available.

The Mass-metallicity Relationand the Fundamental Metallicity Relation at z ~ 1.4
Revealed with the Subaru FMOS Galaxy Redshift Survey (FastSound)
YABE, Kiyoto(Kavli IPMU)		OHTA, Kouji(Kyoto University)

ELLIS, Richard(Caltech)

AKIYAMA, Masayuki
GLAZEBROOK, Karl

(Swinburne University of Technology)

IMANISHI, Masatoshi, TAKATO, Naruhisa

		

BUNKER, Andrew, DALTON, Gavin(Tohoku University)			

(Subaru Telescope)			

(Oxford University)

GOTO, Tomotsugu(National Tsing Hua University)

IWAMURO, Fumihide(Kyoto University)		

TAMURA, Naoyuki(Kavli IPMU)OKADA, Hiroyuki, SHIMIZU, Ikkoh, TONEGAWA, Motonari & TOTANI, Tomonori(University of Tokyo)

The gas-phase metallicity (hereafter, metallicity) is
one of the key parameters required for understanding
galaxy formation and evolution. Although enormous
efforts on studying the correlation between the stellar
mass and metallicity (hereafter mass-metallicity relation)and the dependence of star-formation rate (SFR) on
the mass-metallicity relation (hereafter fundamental
metallicity relation) have been made, those at $z>1$
still remain unclear because the sample size is still
limited. FastSound is a galaxy redshift survey of galaxies
at z = 1.2–1.5 with Fiber Multi-Object Spectrograph(FMOS) on the Subaru Telescope. Although the main
goal of the project is the detection of the redshift spacedistortion (RSD) to test the general theory of relativity
by measuring the growth rate of large-scale structure andto constrain modified gravity models for the origin of
the accelerated expansion of the universe [1], the large
sample of galaxies is very useful for the study of galaxies
at this redshift.
Here, we present the results from the near-infrared
sample of FastSound consisting of ~4,000 galaxies atz ~ 1.4 with significant Hα detection [2]. We measure
the metallicity from the [N II]λ6583/Hα emission line
ratio of the composite spectra in various stellar massand SFR bins. The resulting mass-metallicity relation is
generally in agreement with previous results obtained ina similar redshift range to that of our sample. Although
no clear dependence of the mass-metallicity relation with
SFR is found, our result at z ~ 1.4 roughly agrees withthe fundamental metallicity relation at z ~ 0.1 with fiber
aperture corrected SFR [3,4].
We detect significant [S II ]λλ6716,6731 emission
lines from the composite spectra. The electron density
estimated from the [S II]λλ6716,6731 line ratio ranges
from 10 – 500 cm−3, which generally agrees with that oflocal galaxies. The distribution of our sample on [N II]
λ6583/Hα vs. [S II]λλ6716,6731/Hα is different from thatfound locally. From the obtained N2S2 index, we estimate
the nitrogen-to-oxygen abundance ratio (N/O), and findthat the N/O in galaxies at z ~ 1.4 is significantly higher

than the local values at a fixed metallicity and stellar
mass (Figure 1). The metallicity at z ~ 1.4 recalculatedwith this N/O enhancement taken into account decreases
by 0.1 – 0.2 dex and the resulting metallicity is lower
than the local fundamental metallicity relation.

Figure 1: The N/O against the metallicity (top panel) and thestellar mass (bottom panel). The color of symbols of oursample represents SFR. Solid, dashed, dotted and dashedcurves show the location of local galaxies at z < 0.3. The
vertical and horizontal dashed line indicate the solar
abundance and the solar abundance ratio, respectively.

References[1] Tonegawa, M., et al.: 2015, PASJ, 67, 81.
[2] Yabe, K., et al.: 2015, PASJ, 67, 102.
[3] Andrews, B. H., Martini, P.: 2013, ApJ, 765, 140.
[4] Zahid, H. J., et al.: 2014, ApJ, 792, 75.

I Scientific Highlights

045

A Strong Interaction between The Ejecta of SN IIb 2013df and The CSM
MAEDA, Keiichi1/2, HATTORI, Takashi3, MILISAVLJEVIC, Dan4, FOLATELLI, Gaston2/5, DROUT, Maria R.4
KUNCARAYAKTI, Hanin6, MARGUTTI, Raffaella4, KAMBLE, Atish4, SODERBERG, Alicia4
TANAKA, Masaomi3, KAWABATA, Miho7, KAWABATA, Koji7, YAMANAKA, Masayuki1/8, Nomoto, Ken’ichi2
KIM, Ji Hoon3, SIMON, Joshua D.9, PHILLIPS, Mark M.9, PARRENT, Jerod4, NAKAOKA, Tatsuya7
MORIYA, Takashi10, SUZUKI, Akihiro1, TAKAKI, Katsutoshi7, ISHIGAKI, Miho2, SAKON, Itsuki2
TAJITSU, Akihito3, IYE, Masanori3
1: Kyoto University, 2: The University of Tokyo, 3: NAOJ, 4: Harvard-Smithsonian Center for Astrophysics, 5: Instituto de Astrofísica de La
Plata, 6: Universidad de Chile, 7: Hiroshima University, 8: Konan University, 9: Carnegie Observatories, 10: University of Bonn

Type IIp supernovae are believed to be an explosionof a red supergiant, while type Ib/c supernovae (SNe Ib/c) are an outcome of an explosion of a star which has
lost most of the hydrogen envelope before the explosion.
They should represent different evolutionary paths, andthus a unified understanding of these phenomena is key
to clarifying the unresolved nature of massive stellar
evolution in the final centuries. SNe IIb retain a small
but non-negligible amount of the hydrogen envelope atthe time of the explosion, about the Solar mass or less,and thus they represent a link between SNe IIp and Ib/
c. Their progenitors have diverse properties from a blue
supergiant to a red supergiant, which are difficult tounderstand in the standard stellar evolution theory [1,2].
We have performed follow-up observations of SN IIb
2013df [3]. Especially surprising was a spectral feature
at ~600 days after the explosion, obtained through the
Subaru/FOCAS. At ~200 days, SN 2013df showed aspectrum similar to other SNe, characterized by forbiddenlines of heavy elements. However, at ~600 days the
spectrum showed a dramatic change, showing a strong
Hα emission (Fig. 1). This transition is interpreted asfollows: early on the SN was powered by radioactive
decays of 56Co, while later on the interaction between the

expanding SN ejecta and circumstellar materials (CSM)
became a dominant energy source. Such a transition has
never been seen previously except for SN IIb 1993J.
This observational finding indicates that at least a
fraction of SNe IIb have a large amount of CSM, namely
they experience a huge mass loss in the last ~1000 years.
On the other hand, for other SNe IIb the ejecta-CSM
interaction have never been observed (Fig. 1) [4]. We
have discovered that there is a relation between the massloss rate and the radius of the progenitor (Fig. 2). A more
extended progenitor is associated with a larger mass loss
rate just before the explosion. It seems that SNe IIb froma more extended progenitor are the explosions during astrong binary interaction phase, while those from a lessextended progenitor have a delay between the binaryinteraction and the explosion. A confirmation of the idea
will require further studies, but in any case our discovery
places a new and strong constraint on the unresolved
nature of the final evolution of massive stars.

Figure 2: A relation between the progenitor radius and the CSM
density (i.e., the mass loss rate) [3].

Figure 1: Late time spectra of SN 2013df as compared to those of
SNe IIb 1993J and 2011dh at similar epochs [3].

046

I Scientific Highlights

References[1] Van Dyk, S. D., et al.: 2014, AJ, 147, 37.
[2] Folatelli, G., et al.: 2015, ApJ, 811, 147.
[3] Maeda, K., et al.: 2015, ApJ, 807, 35.
[4] Maeda, K., et al.: 2014, ApJ, 785, 95.

Deep Impact on Close-in Super-Earths:
Atmospheric Escape and Material Mixing					HORI, Yasunori(NAOJ/Astrobiology Center)

LIU, Shangfei(Rice University/LANL)

LIN, Douglas N. C.

ASPHAUG, Eric

(University of California, Santa Cruz)

A violent collision between two objects is thought
to occur repeatedly at the advanced stage of planet
formation. In the Solar System, a giant impact is believed
to be closely-related to a moon-forming event and theorigin of highly-tilting Uranus. Recently, the Kepler
telescope has revealed that close-in super-Earths, namely
1–10 Earth-mass planets orbiting within 0.1 AU, arecommon and abundant in the Milky Way. They are likely
to have experienced giant impacts as well while migrating
inward their host stars via disk-planet interactions. A
mass-radius relation for transiting super-Earths suggeststhat some of them are rocky planets with no atmosphere,
whereas super-Earths with thick atmospheres of <10 wt % exist. Such a diversity of their bulk compositions
should reflect formation processes, one of which could bea giant impact.
We performed three-dimensional hydrodynamic
simulations of a giant impact between a super-Earthand an Earth-sized planet using Cray XC30 at NAOJ
and examined an impact-driven atmospheric loss and athermal state and material mixing inside a target planet
after the impact [1]. Figure 1 shows that snapshots of two
giant impact simulations: (top) a low-velocity head-on
collision (vesc) on 4.3 M⊕ and (bottom) a high-velocity
one (3vesc) on 10 M⊕. We assumed that each target has
a rocky/iron core surrounded by a H/He atmosphere of
7.5 wt % and the projectile is a naked rocky/iron core.
In a high-velocity case, the atmosphere heated by apropagating shock wave expands beyond the Hill radiusof a target, and then escapes from it rapidly. A hot andwell-mixed interior triggers vigorous convection. On
the other hand, a low-velocity collision allows a target
to retain a large fraction of its original atmosphereand produce a non-uniform distribution of chemicalcompositions inside itself, which leads to an inefficientheat transport (e.g. double-diffusive convection).
Collisional histories of super-Earths can strongly affectthermal evolution as post-formation processes. Also,
giant impact would be one of key factors that cause thediversity of bulk compositions as seen in the mass-radiusrelation of transiting super-Earths.

(Arizona State University)

(a)

(e)

(d)

109 cm(b)

ρ ( g cm-3 )

(c)

101

10-3

1010 cm

(a)

(e)

10-7

(d)

109 cm(b)

ρ ( g cm-3 )

(c)

101

10-3

1010 cm

10-7

Figure 1: Snapshots of two giant impact simulations on a closein super-Earth orbiting at 0.1 AU around 1 M⊕. (Top) a
low-velocity collision : the density distribution acrossslices in the planets’ orbital plane (a) before the impact,(b) immediately after, (c) at 1.56 hours, and (d) at 18
hours after the impact. (Bottom) a high-velocity collision: panels (a)–(d) are snapshots taken at the start of the
impact, at 15 minutes, at 1.5 hr and at 21.5 hr after the
impact, respectively. The dashed circle overplotted on
the planet indicates its Hill sphere. The parent star is in
the direction of the white arrow.

Reference[1] Liu, S. -F., Hori, Y., Lin, D. N. C., Asphaug, E.: 2015, ApJ, 812,
164.

I Scientific Highlights047

M81 Galactic Archaeology with Subaru/Hyper Suprime-Cam
OKAMOTO, Sakurako

ARIMOTO, Nobuo, YAMADA, Yoshihiko(Shanghai Astronocmial Observatory)			

FERGUSON, Annette M. N., BERNARD, Edouard J.

		(University of Edinburgh)			

The currently favored cosmological models are
based on the idea of hierarchical structure formation:
the structures in the universe such as galaxies develop
from small “overdensities” to become large-scale objects[1]. The Milky Way and M81 grew over time via theagglomeration of numerous smaller building blocks,
some of which may have survived later mergers to
become present-day dwarf satellite galaxies [2]. Over thelast decade, a number of new satellite galaxies, stellar
streams, and over-densities around the Milky Way andthe M31 have been discovered in the large photometricsurveys [3]. However, the outskirts of two large spirals
are the only places that have been surveyed to sufficiently
faint depths to enable detailed tests of hierarchical galaxy
assembly process across wide scales.

Figure 1: Dereddened CMD of stellar objects. The dashed boxes
delineate the selection criteria for different stellar
populations and are used to construct the maps of young
and old stellar contents presented in Fig. 2.

We are conducting a state-of-the-art wide-field
mapping survey of the M81 Group with Hyper SuprimeCam (HSC) on Subaru. Figure 1 shows the resulting
color-magnitude diagram (CMD) of roughly 550,000 dereddend point sources found in the 4 deg2 area aroundM81 [4]. Theoretical isochrones are overlaid to aid

048

I Scientific Highlights(NAOJ)IRWIN, Mike J.

(University of Cambridge)

UTSUMI, Yousuke(Hiroshima University)in understanding the range of stellar populations. The
left panel of Figure 2 shows the spatial distribution ofstars in young MS and MS+cHeB boxes of Figure 1.
Overall distribution of young stars agrees extremely
well with those of the HI blobs. Bright stars are mainly
located in the inner disk of M81, while most of youngstars in the outlying associations are fainter than i0 ~ 24
and have similar luminosity distributions each other,suggesting that star formation in these tidal features wassynchronized and may have stopped about 30 Myr ago.
The right panel of Figure 2 shows the spatial distributionof RGB stars. A tidal stream between M81 and M82
can clearly be seen, and the outer regions of M82
and NGC 3077 exhibit an S-shaped morphology. The
NGC 3077 halo is extended far beyond the R25 (r = 2.7′).
Numerical modeling suggests the encounters between
NGC 3077, M81, and M82 took place ~200–300 Myr ago,
which may not leave enough time to restore equilibriumin the NGC 3077 halo. The dwarf galaxies such as IKN
and BK5N cannot be seen in the maps of young stars, but
appear as overdensities of old populations, implying they
have not formed as a result of the recent interaction.

Figure 2: Left: The spatial distribution of MS and cHeB stars
that are color coded according to the luminosity withtransparency. Right: The spatial distribution of RGB
stars. The color of each point represents the (g– i)0 colorof star with transparency. The solid lines are R25 radii ofgalaxies.
References[1] White, S., Frenk, C.: 1991, ApJ, 379, 52.
[2] Mihos, J., et al.: 2005, ApJ, 631, L41.
[3] Willman, B., et al.: 2005, ApJ, 626, 85.
[4] Okamoto, S., et al.: 2015, ApJ, 809, L1.

A New Multi-Energy Neutrino Radiation-Hydrodynamics Codein Full General Relativity and Its Application
to Gravitational Collapse of Massive Stars		

KURODA, Takami
TAKIWAKI, Tomoya, KOTAKE, Kei				(NAOJ)(University of Basel)

Gravitational collapse of massive stars initiate
supernovae that are one of the most bright objects in theuniverse. The mechanism of core-collapse supernovae is
not clarified yet though the steady progress of supernova
simulations. We explain two reasons. (i) Supernovae
are not reproduced in a simple numerical setup. (ii) The
ultimate simulations that employ all required physicalingredient, have not been performed although wesometimes observe explosions in the simulations under arelatively realistic situations.
An huge energy of 1053 ergs is released when an ironcore of a massive star collapses and become a neutronstar. A portion of the energy is used to push a shock wavethat are generated at that time and propagates from thecenter to the outer region. The shock experience strong
cooling via the process of photo-dissociation of iron, thatis inverse process of the nuclear fusion. An importantlesson of one dimensional (1D) spherically symmetricsimulations is that the shock stalls at 150 km due to thecooling process [1].
Recently two dimensional (2D) or three dimensional(3D) simulations are performed thanks to thedevelopment of super-computers [2]. In this setup, we
can employ effect of convection: some matters go upward
while the others go downward. We observe shock revivals
in the setup since the convection promotes neutrino
heating process. While the neutrino takes the thermalenergy away in the vicinity of the neutron stars, thatgives thermal energy to the matter in outer region. The
convection efficiently conveys the thermal energy givenby the neutrino heating to the vicinity of the shock where
the energy is required to revive the shock. The convection
relaxes the condition of the neutrino luminosity required
to the shock revival by 30–50 %.
The next problem arises. How reliable are such multidimensional simulations? Unfortunately the results ofthe simulation strongly depends on their input physics.
Different groups show different results even if they use
same progenitor models. To solve the problem, we should
construct ultimate models which employ all physicalknowledge we have. For the purpose, we developed a
new code that solve multi-group neutrino transport underfully general relativistic framework [3].
In Fig. 1, we compare our new methods with theprevious work. We evaluate the methods with 4 axises.
Left top is dimensionality of hydrodynamics andright top is schemes employed to solve the radiation-hydrodynamics. Right bottom is sophistication levelof micro-physics i.e. the number of neutrino reactions
considered in the simulation. Left bottom is treatment of
the gravity. Our new code (red) [3] takes high score in the
diagram compared to the previous works [1,2]. We canobtain most reliable results with the new code.

Figure 1: C o m p a r i s o n o f t h e m et h o d u s e d i n s u p e rn o v asimulations.

References[1] Sumiyoshi, K., Yamada, S., Suzuki, H., et al.: 2005, ApJ, 629,
922.
[2] Takiwaki, T., Kotake, K., Suwa, Y.: 2012, ApJ, 749, 98.
[3] Kuroda, T., Takiwaki, T., Kotake, K.: 2016, ApJS, 222, 20.

I Scientific Highlights

049

Multi-wavelength Observations of the Black Widow Pulsar
2FGL J2339.6–0532 with OISTER and Suzaku
KATAOKA, J., TAKAHASHI, Y.

I Scientific Highlights(Tokyo Institute of Technology)

SEKIGUCHI, K.

on behalf of OISTER team

(NAOJ)

that the pulsar wind from the central MSP is already inthe particle-dominant stage at 1011 cm from the pulsar.
This may critically constrain the acceleration mechanismof the pulsar wind.
300(a) Phase folded light-curves(b) Spectral energy distributions at increasing phase

R-bandV-bandB-bandH-bandKs-band250

Energy Flux [µJy]A millisecond pulsar (MSP) is believed to evolve froma dead pulsar in a binary system via mass accretion froma companion star that has spun up the pulsar for billionsof years. Indeed, most MSPs are discovered in binary
systems; however, isolated MSPs also exist. The missing
link between the isolated MSPs and binary MSPs is black
widow pulsars in which a sufficiently spun up pulsar is
evaporating its companion with its powerful pulsar wind.
In this study we focus on the newly found black widow
pulsar 2 FGL J2339.6$-$0532 discovered by the Fermi
gamma-ray observatory to clarify the intermediate stage
between the accretion-driven phase and the rotationpowered phase utilizing optical and X-ray telescopes.
In optical we utilized the Optical and Infrared
Synergetic Telescopes for Education and Research:
OISTER for covering wide wave band from KS to B-band
and the entire orbital motion. The target was observed
from 22 Sep to Oct 7 2011 with 14 telescopes. The
resultant light curves folded with the orbital period of 4.63
hr are shown in Fig. 1—Left. Fig. 1—Right shows the
SED at various orbital phases, indicating that the surface
temperature varies from 3200 K to 8000 K coincident
with the orbital motion. Assuming a simple geometry,
we constrained the range of the inclination angle ofthe binary system to 50° < i < 59°, which enables us todiscuss the interaction between the pulsar wind and thecompanion in detail.
In X-rays the target was observed with the Suzaku
X-ray observatory for 96 ks. The obtained X-ray spectrum
was well fitted with a two component model function
consists of a black body with a temperature of TBB 0.15 ±0.06 keV and a power law function with a photon index ofΓ = 1.14 +0.14−0.15 . Fig. 2 shows X-ray light curves as functionsof orbital phase for 3 energy bands. In low energy band
below 1 keV, the intensity of the target seems uniform.
Taking into account the size of black body emitter of R ~0.28 km, the soft and steady component can be originatedin the surface of pulsar. While in the Hard X-rays, theintensity shows periodic variation synchronized with theoptical light curves, indicating that the hard X-rays arefrom the shocked pulsar wind covering the companion
surface rather than the pulsar itself. Assuming a thinemitting region covering the companion, we constrained
the magnetization parameter to σ < 0.1. This result means

050(Tokyo Institute of Technology)

YOSHII, T., ARIMOTO, M., SAITO, Y.

200

phase = 0.4~0.5
phase = 0.3~0.4
phase = 0.2~0.3
phase = 0.1~0.2
phase = 0.0~0.1

150
100
50
0

0

0.2

0.4

0.6

0.8

1

1.2

1.4

1.6

1.8

1

2

Orbital Phase

3

4

5

6

7

8 9 10Frequency [1014 Hz]

Figure 1: Left—Multi-color light curves from K S to B-band.
Right—SEDs for various orbital phases.
Folded period: 16683.6585600000 s

Counts [s−1]

NAKAMORI, T.

(Yamagata University)

PIKE, S.

(Brown University)(a) 0.4−1.0 keV

0.015
0.01
5×10−30Counts [s−1]SHIBATA, S.

(Yamagata University)

TACHIBANA, Y., KAWAI, N.

(Waseda University)		

(b) 2.0−4.0 keV

0.015
0.01
5×10−30Counts [s−1]

YATSU, Y.

(Tokyo Institute of Technology)(c) 4.0−8.0 keV

0.015
0.01
5×10−300

0.5

1Orbital Phase

Start Time 15741 14:28:32:096

1.5

2Stop Time 15743 19:28:01:748

Figure 2: X-ray light curves at various energy band.

Reference[1] Yatsu, Y., Kataoka, J., Takahashi, Y., et al.: 2015, ApJ, 802, 84.

Outer Rotation Curve of the Galaxy with VERA III:
Astrometry of IRAS 07427+2400 and Test of the Density-wave Theory
SAKAI, Nobuyuki1, NAKANISHI, Hiroyuki2, MATSUO, Mitsuhiro2, KOIDE, Nagito2, TEZUKA, Daisuke2
KURAYAMA, Tomoharu3, SHIBATA, Katsunori M.1, UENO, Yuji1, HONMA, Mareki1
1: NAOJ, 2: Kagoshima University, 3: Teikyo University of Science

Spiral arm is the most prominent structure in disk
galaxies. However, the origin and evolution are still
unknown. Since the 1960s theoretical and observational
studies about the spiral arm have been conducted and “thedensity-wave theory” and “the dynamical spiral theory”
were proposed. In the deinsity-wave theory, the spiralarm regarded as quasi steady structure (static externalpotential) is incorporated into a basic equation of stellar
disk or gas disk, and one can explore the dynamical
evolution of the disk. On the other hand, the dynamicalspiral theory has been proposed based on a N-bodysimulation in which the spiral arm is destroyed andregenerated within several rotational periods.
A big issue on the spiral arm research is that
there have been no observational data which can becompared with the theories. Since the 2000s astrometry
observations (obtaining 6D kinematic information) by
VLBI technology have been conducted on the Milky Way
scale (~20 kpc). Especially for the Perseus arm as solar
neighborhood arm, the Galactic shock predicted fromthe deinsity-wave theory has been observed in the arm.
(e.g. Sakai et al. 2012 [1]). We aimed to do astrometry
observation toward the infrared source IRAS 07427+2400
associated with the Perseus arm and to verify analytic
solution based on the density-wave theory (Piñol-Ferrer
et al. 2012 [2]) by combining previous VLBI results.
We conducted VLBI astrometry observations with
VERA and measured a trigonometric parallax of 0.185± 0.027 mas for IRAS 07427+2400. Combined withprevious VLBI results (total 27 sources), we comparedthose with the dynamical model. As a result, we
succeeded to make a spiral potential model which canreproduce observed non-circular motions (= observables− circular motion model 1)(Fig. 1). In Fig. 1 gas orbit
model (••) is also represented and we can see an offset
between crowded gas orbits and the bottom of the spiralpotential model.
Given that a dominant component in a galactic
disk is star, fig. 1 suggests an offset between star andgas distributions. In external disk galaxies, it has beenreported that galactic (spiral) morphology varies atdifferent observing wavelengths (Griv et al. 2015 [3]).
Recent N-body/hydrodynamic simulation has showed the“offset” described above (Baba et al. 2015 [4]).

In Autumun of 2016 stellar astrometry results will be
provided by the Gaia satellite. It is expected to understandspiral arm physics in detail by directly confirming the“offset”.

Figure 1: Sakai et al. (2015) [5]. Astrometry results for the Perseusarm (27 sources) and comparison with the dynamical
model of the gas disk (Piñol-Ferrer et al. 2012). Blue
denotes the bottom of the spiral potential model, which
deviates from crowded gas regions.

References[1] Sakai, N., et al.: 2012, PASJ, 64, 108.
[2] Piñol-Ferrer, N., Lindblad, P. O., Fathi, K.: 2012, MNRAS, 421,
1089.
[3] Griv, E., et al.: 2015, MNRAS, 453, 1981.
[4] Baba, J., Morokuma-Matsui, K., Egusa, F.: 2015, PASJ, 67, L4.
[5] Sakai, N., et al.: 2015, PASJ, 67, 69.

1

For a circular motion model, a flat rotation curve was assumed with Θ(R) =240 km s−1.}

I Scientific Highlights

051

Optical and Near-Infrared Polarimetry
for a Highly Dormant Comet 209P/LINEAR
KURODA, Daisuke1, ISHIGURO, Masateru2, WATANABE, Makoto3, AKITAYA, Hiroshi4, TAKAHASHI, Jun5
HASEGAWA, Sunao6, UI, Takahiro4, KANDA, Yuka4, TAKAKI, Katsutoshi4, Itoh, Ryosuke4, MORITANI, Yuki4/7
IMAI, Masataka3, GODA, Shuhei3, TAKAGI, Yuhei5, MORIHANA, Kumiko5, HONDA, Satoshi5, ARAI, Akira5/8
HANAYAMA, Hidekazu1, NAGAYAMA, Takahiro9, NOGAMI, Daisaku10, SARUGAKU, Yuki7, MURATA, Katsuhiro11
MOROKUMA, Tomoki7, SAITO, Yoshihiko12, OASA, Yumiko13, SEKIGUCHI, Kazuhiro1, WATANABE, Jun-ichi1
1: NAOJ, 2: Seoul National University, 3: Hokkaido University, 4: Hiroshima University, 5: University of Hyogo, 6: JAXA, 7: The University of Tokyo,
8: Kyoto Sangyo University, 9: Kagoshima University, 10: Kyoto University, 11: Nagoya University, 12: Tokyo Institute of Technology, 13: Saitama
University

The linear polarization of light scattered by airlesssolar system objects (i.e. comets and asteroids) is a
useful tool for investigating the physical properties of
their surfaces. The phase-polarization curves display acommon behaviour, having a negative polarization branch
at 0 < α ≤ 20°, positive branch at α ≥ 20° and maximum
polarization around α = 90°–100°, where α denotes thesolar phase angle (i.e. Sun-object-observer’s angle). The
phase-polarization curves of asteroids, usually observedin the main-belt at a low phase angle (α < 30°), provide
information about composition (i.e. taxonomic type),
optical properties, porosity of the surface regolith layers,
and so on (see [1,2,3]). In contrast, comets, which areusually enclosed in a dust coma plus gas contamination,
have been observed with polarimeters at a wide rangeof phase angles, providing the composition, size andstructure (fluffy or compact) of dust grains in comae [4,5].
Although several near-Earth asteroids and active
comets were observed at large phase angles, little is
known about the polarimetric properties of bare comet
nuclei at large phase angles. Whenever comets areobserved at large phase angles (i.e. α > 90°), their nuclei
are supposed to shrouded in thick cometary comae,
because comets are located within 1 AU in the geometry
where they are heated up, creating outflow of dust
particles and sublimating ice.
In this work [6], we attempted to obtain unique dataof the linear polarization degree, P, for a bare cometary
nucleus as well as dust particles of the highly dormant
Jupiter-Family Comet, 209P/LINEAR (hereafter 209P).
Optical and near-infrared polarimetric observations of209P were conducted for five nights in 2014 April-May
using two telescopes: the Hiroshima Optical and NearInfraRed camera (HONIR) on the 1.5-m Kanata telescopeat the Higashi-Hiroshima Astronomical Observatory,
Hiroshima, and the visible Multi-Spectral Imager (MSI)
on the 1.6-m Pirka telescope at Hokkaido University’s
Nayoro Observatory in Hokkaido, Japan.
Our results suggested that no significant difference
was found in Rc- and J-band. Because of its low activity,
we were able to determine the linear polarization degreesof the coma dust particles and nucleus independently,+1.0
that is Pn = 30.3 +1.3
−0.9 % at α = 92.2° and Pn = 31.0 −0.7 % at
+0.4
α = 99.5° for the nucleus, and Pc = 28.8 −0.4 % at α = 92.2°

052

I Scientific Highlights

and 29.6 +0.3
−0.3 % at α = 99.5° for the coma. By fitting with
the Lumme and Muinonen function [7,8], we deduced
the maximum polarization Pmax = 30.8 % (nucleus) and29.6 % (coma), respectively.
High Pmax value of the dust coma is consistent with apolarization classification scheme described by [9]. We
employed an empirical function for relating Pmax of thenucleus to the albedo [10] , and found that we obtained
a good estimate of the albedo when we assumed theeffective size of the regolith particles of ≈1–100 μm.

Figure 1: Phase angle dependence of polarization for 209P
nucleus (filled circles) and coma (open circles) takenwith MSI. Regarding data taken with HONIR (indicatedby crosses), we adopted blended signals of nucleus andcoma with relatively large aperture (3 × FWHM) due toinadequate tracking of the telescope. For comparison,
we show polarization degrees of other comets in the
R-band region (about 650 ± 50 nm), which are mostly
attributed to light scattered by dust particles in comae.
Two fit lines with the Lumme and Muinonen function[7,8], high Pmax (solid line and open diamonds) and low
Pmax (dashed line and open triangles) comprise the PDS
archive [11].
References[1] Dollfus, A., et al.: 1989, Asteroids II, 594.
[2] Shkuratov, Yu., et al.: 2002, Icarus, 159, 396.
[3] Gil-Hutton, R., et al.: 2014, A&A, 569, A122.
[4] Zubko, E., et al.: 2011, J. Quant. Spectrosc. Radiat. Transfer,
112, 1848.
[5] Kolokolova, L., et al.: 2007, A&A, 463, 1189.
[6] Kuroda, D., et al.: 2015, ApJ, 814, 156.
[7] Goidet-Devel, B., et al.: 1995, Planet. Space Sci., 43, 779.
[8] Penttilä, A., et al.: 2005, A&A, 432, 1081.
[9] Levasseur-Regourd, A. C., et al.: 1996, A&A, 313, 327.
[10] Dollfus, A.: 1998, Icarus, 136, 69.
[11] Kiselev, N., et al.: 2006, NASA PDS.

Mapping Dark Matter by HSC via Weak Lensing
MIYAZAKI, Satoshi1/2, OGURI Masamune3, HAMANA, Takashi1, TANAKA, Masayuki1, MILLER, Lance4
UTSUMI, Yousuke5, KOMIYAMA, Yutaka1, FURUSAWA, Hisanori1, SAKURAI, Junya2/1
KAWANOMOTO, Satoshi1, NAKATA, Fumiaki1, URAGUCHI, Fumihiro1, KOIKE, Michitaro1
TOMONO, Daigo1, LUPTON, Robert6, GUNN, James6, KAROJI, Hiroshi7, AIHARA, Hiroaki3
MURAYAMA, Hitoshi3, TAKADA, Masahiro3
1: NAOJ, 2: SOKENDAI, 3: University of Tokyo, 4: Oxford University, 5: Hiroshima University, 6: Princeton University, 7: NINS

Since the first discovery in 2001, ‛Cosmic Shear:
weak lensing by Large Scale Structure (LSS)’ has becomea standard tool to examine the LSS and its evolution.
Because sparse sampling of background galaxies issufficient (5 to 10 galaxies/arcmin 2), observation ofrelatively large and bright galaxies are only required.
Thus, it is regarded as one of the most promising tool toprobe the growth rate. However, because the observation
does not directly map LSS, the discrimination of thesignal from noise is not so straightforward.
Clusters of galaxies, on the other hand, is a classicalprobe of the growth rate but the key is how to sample
clusters and measure the mass. Weak lensing could be
potentially powerful again here but observation ally
more demanding. In order to locate the dark matter
concentration directly via lensing, sufficiently higher
resolution mass map is crucial which requires highnumber density of faint background galaxies. SuprimeCam has been one of the ideal facility instruments
because it features unique combination of the large
aperture and the sharp imaging which enables precise
measurement of faint galaxies. Hyper Suprime-Cam(HSC) is developed to make the survey speed even fasterand to realize a very wide survey (> 1000 deg2).
HSC saw the first light in January 2013 andengineering observations followed. After the initialround of adjustments we obtained the scientific images
on two contiguous HSC fields. The figure on the rightshows the dark matter map reconstructed from the shapesof 220,000 galaxies over the field using weak lensing
technique. The density reflects the strength of lensing
signal. The locations of significant peaks on the map(signal-to-noise ratio > 4.5) are marked by circles where
we expect the existence of dark matter concentrations.
We could also expect that galaxies are attracted by
the dark matter gravity and these concentration would
be recognized as clusters of galaxies. This expectation
is indeed verified by the cross-correlation of the peakson the mass map and clusters identified by multi-color
images where color sequences of member galaxies aresearched using CAMIRA algorithm. We confirmed that
all the significant peaks accompany clusters of galaxies.
This suggests the reliability of the mass map.
We are able to estimate the redshift to the dark matter
concentration using the colors of associated galaxies. On
the histogram inserted at the lower-right corner of the

figure, we show the redshift distribution of the clusters.
Two spikes are clearly visible which should stem from
LSS accidentally located along the line of sight. This
clearly suggests that we would have to observe much
much wide field so that the local structures are averaged
to obtain useful cosmological information.
This is exactly what we are working on right now.
We started a wide field observation campaigns inMarch, 2014 as one of the Subaru Strategic Program
in collaboration with more than 200 CoIs. We plan tocover 1400 deg2 and it would take about five years tocomplete. Our primary objective of the survey is totest the currently standard ΛCDM with unprecedented
precision. In particular, we are interested in whether
modification of the Einstein's gravity theory is necessary
because weak lensing technique, among other techniquessuch as SNIa and BAO, uniquely probes the effect ofgravity. We will certainly measure the cosmic shear asother lensing survey projects do. In addition, using thesame data, we will be able to detect more dark matter
concentrations which, we expect, enables us to make aunique contribution to observational cosmology.

Figure 1: Weak lensing mass map (contour). Peak positions aredesignated by circle where dark matter halos are located.
Histogram shows the redshift distribution of the halos
estimated by the color of associated galaxies to thesehalos.
References[1] http://www.subarutelescope.org/Projects/HSC/j_index.html[2] Miyazaki, S., Oguri, M., Hamana, T., et al.: 2015, ApJ, 807, 22.

I Scientific Highlights

053

The Host Galaxy of a Fast Radio Burst FRB150418
KEANE, E. F.1/2/3, JOHNSTON, S.4, BHANDARI, S.2/3, BARR, E.2, BHAT, N. D. R.3/5, BURGAY, M.6
CALEB, M.2/3/7, FLYNN, C.2/3, JAMESON, A.2/3, KRAMER, M.8/9, PETROFF, E.2/3/4, POSSENTI, A.6
VAN STRATEN, W.2, BAILES, M.2/3, BURKE-SPOLAOR, S.10, EATOUGH, R. P.8, STAPPERS, B. W.9
TOTANI, T.11, HONMA, M.12/13, FURUSAWA, H.12, HATTORI, T.14, MOROKUMA, T.11, NIINO, Y.12
SUGAI, H. 11, TERAI, T.14, TOMINAGA, N.11/15, YAMASAKI, S.11, YASUDA, N.11, ALLEN, R.2, COOKE, J.2/3
JENCSON, J.16, KASLIWAL, M. M.16, KAPLAN, D. L.17, TINGAY, S. J.3/5, WILLIAMS, A.5, WAYTH, R.3/5
CHANDRA, P.18, PERRODIN, D.6, BEREZINA, M.8, MICKALIGER, M.9, BASSA, C.19
1: SKA Organisation, 2: Swinburne University of Technology, 3: CAASTRO, 4: CSIRO, 5: Curtin University, 6: INAF, 7: Australian National
University, 8: MPIfR, 9: University of Manchester, 10: NRAO, 11: University of Tokyo, 12: NAOJ, 13: SOKENDAI, 14: Subaru Telescope,
15. Konan University, 16: California Institute of Technology, 17: University of Wisconsin-Milwaukee, 18: Tata Institute of Fundamental
Research, 19: ASTRON

Fast Radio Burst (FRB) is a short radio burst lasting
only 1 msec observed at GHz band. The nature of FRB
is still mystery and various models are proposed ranging
from a radio interference from the Earth to a burst of anastronomical object at a cosmological distance. FRBs
show a large dispersion along the frequency, and its
plausible interpretation is that the radio burst originatesfrom a cosmological explosive event, and it is observed
after long-distance travel through the inter-galactic
plasma. However, there has been no detection of the hostgalaxy of any FRB or its redshift measurement.
FRB150418, detected on 18 April 2015, was first
discovered with the Parkes telescope multi-beamreceivers, and follow-up observations with ATCA
detected a compact, variable radio source in one of theParkes beams. The source has rapidly faded within 1
week after the burst, and showed larger flux variation
in lower frequency, indicating that the source has adifferent nature from radio AGN and is most likely
a radio afterglow of the FRB. The optical follow-up
with the Subaru telescope detected an elliptical galaxy
at the position of the radio afterglow, and the redshiftmeasurement with Subaru revealed that the host hasa redshift of 0.492. This is the first detection of the
FRB host galaxy and its redshift. The host galaxy is anelliptical galaxy with little sign of star formation, which
provides a strong constraint on the possible origin of
the FRB. Meanwhile, the redshift is consistent with the
expectation from the standard cosmology with missing
baryons in the form of inter-galactic plasma, confirmingthat a large fraction of missing-baryon is in the intergalactic medium.

Figure 1: Upper-images: An optical image of the Parkes multibeam fields (circles), with the zoom-up images on theright showing the FRB-host elliptical galaxy discovered
with Subaru. Bottom-panel: The spectrum of theelliptical galaxy taken with Subaru, which matches wellwith the template of an elliptical galaxy at a redshift of
0.492.

Reference[1] Keane, E., et al.: 2016, Nature, 539, 453.

054

I Scientific Highlights

Mangetic Field Structure Near the Event Horizon of Sgr A*
JOHNSON, M. D.1, FISH, V. L.2, DOELEMAN, S. S.1/2, MARRONE, D. P.3, PLAMBECK, R. L.4
WARDLE, J. F. C.5, AKIYAMA, K.2/6/7, ASADA, K.8, BEAUDOIN, C.2, BLACKBURN, L.1, BLUNDELL, R.1
BOWER, G. C.8, BRINKERINK, C.9, BRODERICK, A. E.10/11, CAPPALLO, R.2, CHAEL, A. A.1, CREW, G. B.2
DEXTER, J.12, DEXTER, M.4, FREUND, R.3, FRIBERG, P.13, GOLD, R.14, GURWELL, M. A.1, HO, P. T. P.8
HONMA, M.6/15, INOUE, M.8, KOSOWSKY, M.1/2/5, KRICHBAUM, T. P.16, LAMB, J.17, LOEB, A.1, LU, R.2/16
MACMAHON, D.4, MCKINNEY, J. C.14, MORAN, J. M.1, NARAYAN, R.1, PRIMIANI, R. A.1, PSALTIS, D.3
ROGERS, A. E. E.2, ROSENFELD, K.1, SOOHOO, J.2, TILANUS, R. P. J.9/18, TITUS, M.2
VERTATSCHITSCH, L.1, WEINTROUB, J.1, WRIGHT, M.4, YOUNG, K. H.1, ZENSUS, J. A.16, ZIURYS, L. M.3
1: Harvard-Smithsonian CfA, 2: MIT Haystack Observatory, 3: Steward Observatory, 4: UC Berkeley, 5: Brandeis U., 6: NAOJ, 7: U. Tokyo,
8: ASIAA, 9: Radboud U., 10: Perimeter Institute, 11. U. Waterloo, 12: MPE, 13: JCMT, 14: Maryland U., 15: SOKENDAI, 16: MPIfR, 17:
OVRO, 18: Leiden Observatory

It is widely believed that the magnetic field plays animportant role in the Active Galactic Nuclei through theaccretion process as well as jet formation. However, todate there has been no direct confirmation of existenceof magnetic field around the event horizon scale ofsuper-massive black holes. In order to study the detailed
physical properties of the vicinity of super-massive black
holes, we have observed Sgr A*, the super-massive blackhole at the Galactic center, with a 1-mm VLBI array in
the US. The array consists of four telescopes at threestations, namely, CARMA in California, SMT in Arizona
and SMA/JCMT in Hawaii, and has the maximum
baseline of ~4000 km.
We have detected for the first time the linear
polarization from the emission at a scale of ~6 blackhole radii (Figure 1). The data indicate that the magnetic
field structure is partially ordered as seen in Figure 2.
The figure shows the relation of the polarization
fraction against the visibility amplitude, and images A–
D corresponds to models with various magnetic fieldstructures. Model B matches well with the observations,and Model D, which is based on the GRMHD simulation,is also consistent with the observations. The firstdetection of magnetic field around the black hole certifies
that the forthcoming observations of super-massive black

Figure 1: Fractional polarization and polarization angle of Sgr
A* along the baselines. The direction of lines shows thepolarization angle and the color shows the fractionalpolarization.

holes with EHT (Event Horizon Telescope) will enable us
to better understand the physical properties in the vicinityof the super-massive black holes.

Figure 2: Relation with the polarization fraction and the visibility
amplitude (top). Images A–D show models with various
structure of magnetif field. Model B well matcheswith the observations, and model D, which is basedon the GRMHD simulation is also consistent with theobservations.
Reference[1] Johnson., M. et al.: 2016, Science, 350, 1242.

I Scientific Highlights

055

II Status Reports of Research Activities
1. Subaru Telescope
1. Subaru Telescope Staff
As of the end of FY 2015, the Subaru Telescope Project staff
consisted of 18 dedicated faculty members (five of whom arestationed at Mitaka), five engineers, and three administrative
staff members. Additional staff members include two speciallyappointed research staff, three specially appointed seniorspecialists, five research experts, and six administration
associates, all of whom are stationed at Mitaka. Moreover, 13
research/teaching staff members, 12 of whom are stationed at
Mitaka and one of whom is stationed at Pasadena; and three
engineers, two of whom are stationed at Mitaka and one ofwhom is stationed at Nobeyama are posted concurrently. The
project also has 79 local staff members dispatched from the
Research Corporation of the University of Hawaii (RCUH),
including scientific assistants; engineers in charge of softwareand 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 thetelescope, observational instruments, and observational facilities;
and in conducting open-use observations, R&D, public outreach,and educational activities.

2. Science Highlights
In FY 2015, Subaru Telescope produced many outstanding
scientific outcomes which were published in major international
journals. Below are some examples:(1) Deep NIR spectroscopy of 24 quiescent galaxies at aroundz = 1.6 (9.5 billion years ago) with MOIRCS provides us witha precise composite spectrum. By comparing it with a spectral
synthesis model, it is found that the average stellar age in thesegalaxies is very old (1.5 billion years) and the duration of starformation is very short (<1 billion years). We are thus likely to
be witnessing the progenitors of present-day elliptical galaxies.
(2) Super wide-field imaging of nearby spiral galaxy M81 and its
two interacting companion galaxies with Hyper Suprime-Cam(HSC) has revealed that the young main-sequence stars in thesegalaxies nicely follow the neutral hydrogen gas distribution
which bridges the multiple interacting galaxies. This suggeststhat the gas is tidally stripped due to interactions and the newstars are formed in the gas during the course of the hierarchicalassembly and mergers of galaxies.
(3) High contrast camera HiCIAO, combined with the adaptive
optics system which corrects for atmospheric disturbance in056

II Status Reports of Research Activities

astronomical images, has been conducting high resolution
imaging of circum-stellar disks around young stars. A circular
gap at only 20 AU away from the central star is newly
discovered. Together with another known outer gap alreadyfound by HST, this disk turns out to have a double ring gap
structure. This suggests that multiple (two) planets are being
formed simultaneously, and it gives us a new insight into theformation of planets in the proto-planetary disks.
(4) High Dispersion Spectrograph (HDS) targeted 50 solartype stars with a “super-flare” event, a gigantic explosion at thesurface of the star. The spectra have confirmed that (1) thosestars are single systems, (2) spin velocities derived from theline widths match the periods of their light curves, and that (3)a shallow absorption line profile is seen as evidence of a strong
magnetic field. These results all suggest that the appearance ofa giant black spot on the stellar surface leads to the launch of asuper-flare.

3. Open Use
The Subaru open use call for proposals is issued every six
months. The periods are from February 1 to July 31 (S15A) andfrom August 1 to January 31 (S15B). The Mitaka office of the
Subaru Telescope at the National Astronomical Observatoryof Japan (NAOJ) campus accepts submitted proposals. The
Subaru Time Allocation Committee, established under the
NAOJ advisory committee for optical and infrared astronomy,
selects accepted proposals, based on the evaluation andcomments of referees. In S15A, 64 programs (102 nights) were
accepted out of 162 submitted proposals, requesting 427 nights
in total. In S15B, 57 proposals (97 nights) were accepted outof 161 submitted proposals, requesting 372.5 nights in total.
Short duration service observations were also conducted. In
S15A and S15B, 5 and 2 accepted open-use proposals were byforeign principal investigators, excluding University of Hawai`iobserving time. The number of applicants in submitted proposals
was 2083 for Japanese researchers (Japanese astronomers
at any institute and non-Japanese astronomers belonging toJapanese institutes) and 748 for foreign researchers. The numberof researchers in accepted proposals was 899 for Japanese
astronomers and 274 for foreign astronomers.
In S15A and S15B, the number of open-use visiting
observers was 343, of which 58 were foreign astronomers.
69 astronomers observed remotely from Mitaka. The Mitaka
office of the Subaru Telescope takes care of proposal handlingand evaluation, and travel procedures for observers and theirtravel support. The Hilo office makes the observing scheduleand supports the accommodation and transportation of visiting
observers in Hawai`i. In S15A and S15B, 95.7 % 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 1.5 %, 0.3 %,and 2.5 % of observing time was lost due to instrument trouble,
communication trouble, and telescope trouble, respectively.
In S15A and S15B, remote observations from Hilo were notconducted. However, remote observations from Mitaka, whereobservers in Mitaka can participate in observations remotely,in addition to on-site observers at the summit, were conducted
for 24 programs with 47 nights. Service observations weremade for 12 nights. To make the best use of limited resources
at observatories on top of Maunakea, Subaru Telescope has
been exchanging telescope time with W. M. Keck Observatory
and Gemini Observatory. The number of time exchange nights
between Subaru Telescope and Keck was 3 in S15A and 6 in
S15B. That between Subaru Telescope and Gemini was 5 in
S15A and 3 in S15B.

4. Telescope Maintenance and Performance
Improvement
During scheduled maintenance work on the telescope andthe enclosure on February 22, the optical-side mirror hatch got
stuck. The mirror hatch was restored to its normal position as
of February 27, then the open-use observations were resumed
on February 29. The mirror hatch is not operational at the timeof writing this text. Because normal performance of the mirror
hatch is required for the primary mirror recoating work in thenext year, we are considering making some repair plans.
Other general functions and capabilities of the Subaru
Telescope are continuing to be maintained the same as theprevious year.
This year, both the dome angle and the top screen position
barcodes and these controllers were renovated. A laser distancemeter was installed on the top unit exchanger (TUE) to improve
the accuracy and reliability. Some acceleration measurementson the telescope were carried out for better understanding thetelescope tracking performance. In addition, while promoting
improvements in performance and operational efficiency of the
Subaru Telescope, renovation was conducted on the telescope
control units, which were installed more than 10 years ago. The
local control units that were renovated or modified in this year
were: the dome control unit (DCU), the dome rotation processor
unit (DRPU), and the telescope control workstations (TWS).
The major causes of the telescope failures is considered tobe aging, human error, and adverse weather. This year included
a small amount glycol leakage, wind screen malfunction,
dropping of the dome lateral guide roller (LGR), breakdownof the lower mirror cover, malfunction of the upper mirror
cover, trouble in the Cassegrain-optical secondary mirror unit,
top screen malfunction, failure of the 80-ton crane control,
uninterruptible power supply (UPS) glitch, and the mirror hatch
incident. Bad weather caused a malfunction of the dome shutter
and the elevation axis angle sensors, forcing observations to becanceled. A small earthquake occurred, although there was no
significant damage observed. Some dips and cracks on the dome

rail were found. These dips and cracks should be repaired in thenear future.
Additionally, the same as the previous year, we used thetelescope status log for the preventive maintenance of thetelescope and the enclosure.

5. Instrumentation
The nine open-use facility instruments of Subaru Telescope
have been operated stably in FY 2015. Those instruments are
Hyper Suprime-Cam (HSC), Subaru Prime Focus Camera(Suprime-Cam), Faint Object Camera And Spectrograph(FOCAS), High Dispersion Spectrograph (HDS), Infrared
Camera and Spectrograph (IRCS), Cooled Mid-infrared Camera
and Spectrograph (COMICS), Multi-Object Infrared Camera
and Spectrograph (MOIRCS), Fiber Multi-Object Spectrograph(FMOS), and 188-elements Adaptive Optics and Laser GuideStar system (AO188/LGS).
Since the last fiscal year, there have been discussions on
how we maintain or stop operations of the facility instruments.
Following the instrument plan proposed in last January, it was
decided to terminate the operation of FMOS by the end of April,2016 in order to accept a next generation facility instrument
PFS.
The operation of HSC has been stable, similar to the last
fiscal year. To further stabilize the operation, the replacementof the instrument control computer (OBCP) with new hardware
and an improvement of the filter exchange unit (FEU) have been
performed while consulting closely with the HSC development
team. In addition, the implementation of a new dome-flat
lamp system with improved uniformity is ongoing to better
calibrate HSC data. However, because of the increased numberof observing runs of HSC, there are concerns over the limited
amount of time for instrument maintenance works and the strong
restrictions on the observing schedule due to the limited numberof filters available in an observing run. We are trying to improve
the instrument exchange procedures to resolve those concerns.
There are several upgrade projects for the other facility
instruments. The installation of new detectors (HAWAII2RGs) in MOIRCS has been done successfully and it achieved
engineering first light in December, 2015. In preparation for the
first open-use observation in 2016 after the upgrade, we havebeen working on the characterization of the instrument with
the new detectors and further improvement of the operation.
The other ongoing upgrade projects are the fiber MOS unit for
HDS; the polarimetric function in thermal infrared for IRCS
and in mid-infrared for COMICS; the integral field unit (IFU)
for FOCAS and MOIRCS; and the Transponder-Based Aircraft
Detector (TBAD) for the LGS system.
In FY 2015, three carry-in (PI-type) instruments HiCIAO(high-contrast coronagraph imager), Kyoto-3DII (optical integral
field spectrograph), and SCExAO (Subaru Coronagraphic
Extreme Adaptive Optics) have been offered through the Subaru
open-use program. SCExAO has been commissioning a highorder wave-front correction mode, which realizes extreme
adaptive optics correction. This mode has been offered throughII Status Reports of Research Activities057

the Subaru open-use program on a trial basis since S15A.
A Multi-Object Adaptive Optics (MOAO) sciencedemonstrator (RAVEN), which has been developed incollaboration with Canadian institutes, has conducted
additional test observations and science observations in S15A
and demonstrated the performance of the MOAO system.
RAVEN finished its operation at the Subaru Telescope and wastransported back to Canada to be used as a test bed.
There are new PI-type instruments, IRD (InfraRed Doppler
instrument) and CHARIS (Coronagraphic High Angular
Resolution Imaging Spectrograph), which are currently being
developed toward the first light observations expected in July
2016. Other than these approved new instruments, there are new
PI-type instrument carry-in proposals from the University ofTokyo; SWIMS (Simultaneous-color Wide-field Infrared Multiobject Spectrograph) and MIMIZUKU (mid-infrared multifield Imager and spectrograph). Considering the impacts to theexisting observatory resources, the acceptance review process
for these two instruments is currently suspended until the
installation of the other new PI type instruments at the summit
has been completed.
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 Hyper SuprimeCam (HSC). The PFS has about 2400 optical fibers distributed
over the 1.3 degree field of view of the prime focus. The fibers
feed the light from astronomical objects to four identical
spectrographs which will be placed in the telescope dome. The
spectrograph modules cover the wavelength range from 0.38 μm
to 1.26 μm simultaneously. The subcomponents of PFS are being
developed at each partner institute, aiming for engineering firstlight in 2018. Subaru Telescope is responsible for modifying
the telescope and enclosure to accept PFS and the design
work progressed. A Chinese consortium has officially joined
PFS collaboration and NAOJ will handle their funds for PFS
development.
We are conducting a conceptual study of the next large
facility instrument following HSC and PFS, which will be oneof the flagship instruments at the Subaru telescope in the era of
TMT. We have studied the concept of a wide-field near-infrared
imager and multi-object spectrograph assisted by a ground-layer
adaptive optics (GLAO) system, which uniformly improves
image quality over a wide field of view by correcting only forthe turbulence at the ground layer of the Earth’s atmosphere byusing an adaptive secondary mirror. In FY 2015, the concepts
for the GLAO, wide-field near-infrared instruments, and theirscience cases were summarized in the study report and reviewed
by the external reviewers.

058

illegal access.
Observation data archiving has been ongoing from theprevious year. The archive is operational without serious
problems. We provide a user interface that is suitable todownloading large amounts of data in a batch process per
requests by users who wish to download data taken by Hyper
Suprime-Cam (HSC) during its Strategic Science Program (SSP).
The data archive system in Mitaka is also operating reliably.
We officially rolled out remote observations from Mitaka
using the remote observation monitor system for a limited
amount of time. During observation semesters from February
2015 through January 2016, 24 observation programs utilized
the remote observation monitor system for 47 nights. This wasa significant increase in the nights where the remote observation
monitor system was used since last year, when 25 observation
programs used 28 nights. In expectation of the increase in thenumber of nights when the remote observation monitor system
is used, we hired research fellows to provide support to theusers of the remote observation monitor system. The Proposal
Management System (ProMS) also worked very well.
Computers for HSC data analysis (HSC On-site Data
Analysis System) were procured in fiscal years 2010 and 2011.
We added storage, an interactive processing server, and a
database server to the system in 2015.
The current system requires fast transfer of large volumesof data between the storage and processing servers. Datatransfer speed of the current system is not fast enough tomeet our requirements. We must wait for over 30 minutes
before data reduction starts; in cases of observations with veryfrequent exposures this causes delays in deciding whether or
not to continue observation. Therefore, we experimented withreplacing NFS with a fast data I/O software; the result was
several times faster data I/O. We decided to continue the test
in a test environment with more computers to simulate theproduction system. The additional hardware was delivered by
the end of this fiscal year. Configuration and performance testsof the test system are planned in 2016.
The dedicated network link between Hawai`i and Mitaka
has been procured with a single year contract since April 2014.
Bidding was held to select the network link provider for 2016.
The link speed will become 1 Gbps, based on the data rate form
HSC and the actual data amount used during 2015. A provider
was selected successfully and we prepared our own network
system so that it can connect to the network service that theprovider will offer starting from April 2016.
The online visitor forms for those who visit Subaru
Telescope in Hilo for observation and for those who visit NAOJ
in Mitaka for remote observation monitoring are operating.

6. Computers and Network

7. Education (Under-graduate and Graduate
Courses)

One of our goals of this year was the same as a goal of theprevious year - to stably operate the fourth generation systemof computers and network called STN4. Stable operation wasachieved without serious troubles or attacks/intrusions such as

The number of Subaru Telescope staff members in Hilo whowere concurrently appointed by SOKENDAI (graduate school)
was ten. The number of SOKENDAI students who had primarysupervisors affiliated with Subaru Telescope (including those

II Status Reports of Research Activities

concurrently belonging to Subaru Telescope) was 16, whichconstituted half of the total 32 Sokendai students hosted in
NAOJ. Of which eight had supervisors who belonged primarily
to Subaru Telescope.
In FY 2015, Subaru Telescope hosted 7 graduate students
for long stays, of which 2 were SOKENDAI students. On topof that, intensive education activities were seen also in Mitaka
in cooperation with the Division of Optical and IR Astronomy.
The numbers of graduate course students in all of Japan who
obtained master’s degrees and PhD’s based on Subaru Telescope
data were 17 and 6, respectively, of which one each belonged to
the Division of Optical and IR Astronomy.
We also regularly hosted a series of educational programs
at Subaru Telescope. In September 2015, we hosted a Subaru
Autumn School in which 13 under-graduate students from allover Japan participated and learned the reduction and analysis of
Subaru Telescope data and heard a series of lectures. Moreover,in October, we hosted two Subaru Telescope observation
training courses, one for 8 undergraduate students from all overJapan, and the other for 7 new SOKENDAI students at NAOJ.
In the Hilo Office, we had regular Subaru Telescope seminars in
English 2-3 times a month, where open-use observers, visitors,
and Subaru Telescope staff members presented their own new
research. Also in the Subaru Telescope Mitaka office, we hadmany 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 Public Information and Outreach (PIO) office istasked with addressing the accountability for what the Subaru
Telescope does and is keenly aware of the importance of citizens
understanding our work, for both the short-term and long-term
success of the project. The increased importance of positiveawareness in the local community has profound meaning for the
next generation telescope project on Maunakea. Therefore PIO
pays more attention to the interaction with the local community,
in its three major areas of tasks.
Task 1: Disseminating information about the results fromthe Subaru Telescope and the work at the Subaru Telescope. The
primary tools are the postings on our own website; providingpress releases to the Japanese, local, and international media;
and holding press conferences. During fiscal year 2015, there
were 31 web-postings (14 in Japanese, 17 in English) about
the discoveries from the Subaru Telescope. Articles about the
instrument development, the work and the activities at theSubaru Telescope, and other announcement totaled 52 (25 inJapanese, 27 in English). Some postings are also distributed
through the media as well as posting services such as theAmerican Astronomical Society’s mailing exploder. Many
articles appeared in the Japanese newspapers, and some in thelocal newspapers; with more prevailing in the on-line postings.
In addition, newer tools such as Twitter, Facebook, andYouTube are becoming more useful in spreading awareness in atimely manner. The PIO office is making extra effort in providing
striking visuals for such social media postings. Filming requests
from outside totaled more than 22 (13 in Japanese, 9 in English),in addition to the numerous inquiries/questions from the media,
educational institutions, and museums.
Task 2: Provide escorted tours for the public and specialgroups to see the facility. The public tour program that started in
2004 continues to provide opportunities to see the telescope upclose for guests from Japan and from around the world. Except
for summer months when the tour program was suspended dueto the access issues on Maunakea, a total of 421 people visited
through this program. There were 131 additional groups who
visited through special tour programs and resulted in a totalhead count of 923 people who visited the summit facility. The
tours are all escorted by the assigned staff, in either Japanese or
English language.
Facility tours of the Hilo Base Facility are most of thetime accompanied by other activities described in the next
major task area, namely: special lectures, hands-on sessions, orpresentations by the student group. A total of 67 groups, with
393 people, visited the base facility this year.
Task3: Public outreach includes lectures in the local
community, special presentations in the schools, and remotepresentations for Japanese schools or museums. PIO provided/
coordinated 93 lectures at the Hilo Base Facility or in its
vicinity such as at the ‘Imiloa Astronomy Center. There were 10
lectures outside of the island, and 15 remote lectures for off-site
locations. The local lectures included 55 classroom presentations
during the Journey through the Universe program.
In place of an open house, the staff of the Subaru Telescope
participated in the annual AstroDay event at the local shopping
mall. Observatories on Maunakea, ‘Imiloa Astronomy Center,
Maunakea Visitor Information Station, and other astronomyrelated groups participated in this event. More than 2000 people
visited this family-friendly event.
Another special local event where many astronomy
observatories participate is the annual Onizuka Science Day
at the University of Hawai`i at Hilo. Six-hundred selectedstudents between grades 4 and 12 (upper elementary school tohigh school) with families and teachers from all over the islandgathered for this event. PIO provided 4 hands-on workshops andan exhibit booth.
There was a very significant event in August 2015 which
was the International Astronomical Union’s General Assemblyin Honolulu. PIO provided a booth and dispatched staff toanswer questions, in addition to providing special tours of thetelescope.

II Status Reports of Research Activities059

2. Okayama Astrophysical Observatory
Okayama Astrophysical Observatory, (hereafter theObservatory) serves as the observing and research base of
the optical and infrared astronomy in Japan, and it promotes
open use, primarily of the 188-cm telescope, to universities
throughout the country. It also pursues joint R&D projects with
universities, contributing toward forming stronger foundations
for astronomy research at the universities. Concurrently,
the Observatory pursues its own research activities, taking
advantage of its location and observational environment.
Every year, about 240 nights at the 188-cm telescopeare exploited for observations by researchers from across thecountry through the open use. The Observatory maintains andoperates the observing instruments and provides the observers
with support for observations, travel expenses, accommodations,
everyday needs, etc. It also engages in improving the open-use
observing instruments, developing new open-use instruments,and supporting carry-in instruments from other institutions.
Several joint projects with universities have been conducted,
including Kyoto University’s Okayama 3.8-m New Technology
Optical and Infrared Telescope Project and the Tokyo Institute ofTechnology’s Gamma-Ray Burst Optical Afterglow Follow-up
Project. Meanwhile, the 188-cm telescope, the 50-cm telescope,and the 91-cm telescope of the Observatory are involved in“The Optical & Near-Infrared Astronomy Inter-University
Cooperation Program” supported by MEXT, which commenced
in 2011.
The Observatory’s unique research activities include a
project designed to convert the 91-cm telescope into an ultrawide-field near-infrared camera (OAO-WFC). It also engages
in a comprehensive survey of infrared-variable objects in
the Galactic plane. Another project is the upgrade of thefunctionalities of the 188-cm telescope in order to significantly
improve its planet searching capability through a Grant-in-Aid
for Scientific Research (Basic Research (A), FY 2011–2015).
Collaborations with foreign researchers are also continued
actively.
The personnel breakdown as of March 2016 was five fulltime staff members, including two associate professors, one
assistant professor, one engineer, and one chief clerk; ten
contracted staff members, including three research experts, one
postdoctoral fellow, one research supporter, three administrative
supporters, and two administrative maintenance staff members;
and one temporary staff member.

1. Open Use(1) Overview
The numbers of nights allotted to open use in 2015 were
115 for the first semester (2015A, January to June) and 124 forthe second semester (2015B, July to December). Observing
proposals were called for publicly each semester. The Okayama
program subcommittee reviewed the submitted proposals andaccepted 1 project observation program, 1 academic degree060

II Status Reports of Research Activities

support program, 13 general observation proposals, and 1
miscellaneous observation proposal (introduced in 2015A) in
2015A, and accepted 1, 1, 13, and 0 in 2015B. One proposal
from Hawai`i was accepted in 2015A, and one from Turkey andone from Hawai`i were accepted in 2015B. The Observatory
supported their observations with human resources. Open-use
observation generally proceeded without incident.
(2) Observation/Research Results
The majority of objects observed through the open use
in 2015 were stellar sources and exoplanets. Others included
supernovae, galaxies outside the Milky Way, AGNs, and quasistellar objects. The following primary observation themes
were noted: exoplanet search and binary-mass determination
via precise radial velocity measurements; exploration of thephysical properties and activities of single and binary stars via
high-dispersion spectroscopy; and the observation of exoplanet
transits by precise near-infrared differential photometry.
Optical low-dispersion spectroscopic observations of stars
for classification remained significant. As in previous years, anumber of observational studies were conducted by individual
groups of researchers within the open-use framework, andtheir respective research results were reported in meetings andconferences or were 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 pointing accuracy and to automate the highdispersion spectroscopic observations with the fiber-feeding
system in this FY 2015. The remote observing environment has
been refined further since FY 2014 and has been made available
for open use since 2015B. During the maintenance period inJune, the annual re-aluminization of the primary mirror of the
188-cm telescope and the subsequent optical axis alignment of
the smaller mirrors against the primary were completed. Efforts
were made to simplify the re-aluminization process. The 1.5m primary of the KANATA Telescope at Hiroshima University
was also accepted for re-aluminization in the maintenanceperiod this year. Participants in the aluminization work from thatorganization were given NAOJ-mandated safety and hygiene
training as necessary. Lubrication of the telescope and dome was
performed in July. Utmost efforts were made to maintain highobserving efficiency by conducting monthly cleanings of the
primary, secondary, and tertiary mirrors of the 188-cm telescope
after October.
The dome was checked daily. Other maintenance work wasalso performed, including the repair of the iron part of the hatch
opening on the second floor and repainting of the scaffold of
the vacuum aluminizing chamber in May; repair of the worndown guide rails for the lower slit door in October; and repairof the external panels of the dome hemisphere to prevent rainleakage in November. Much attention was paid to the operationand maintenance of the facility and equipment. The wire ropeof the dome slit door driver was inspected and investigations
continued in order to determine the causes of the unusually
rapid deterioration of the wire rope and possible measures
to prevent the deterioration. Work safety was given priority
in accomplishing the aforementioned maintenance work andobserving instrument exchanges. The Administration Office andReception Room on the first floor of the Main Building wererenovated and the Director’s Room was moved from the second
floor to in-between these two rooms. The asphalt pavement of
the parking spaces west of the main building and the access roadfrom the city road to the parking lot were renewed as well.
(4) Conferences
The program subcommittee for the 188-cm telescope met
on June 16 and November 17 to evaluate proposals for the open
use of 2015B and 2016A (first semester of 2016), respectively,
and formulated an observation program for each semester.
The Okayama Users Meeting, also known as the 26th Opticaland Infrared Users Meeting, was held in the Large Seminar
Room of NAOJ Mitaka Campus on August 17 and 18. Various
reports were made: current status of the Observatory, execution
summary of the program subcommittee, full operation of theremote observing environment, automation of observing,
etc. Reports on three new user-led instruments for the 188cm telescope were also made. Discussions were held on the
future operation of Target-of-Opportunity (ToO) observations
and operation of open-use observing instruments. A special
session was arranged on the era of the Kyoto 3.8-m telescopeand detailed discussions were held among Okayama users,
Kyoto University staff, and NAOJ staff (see the printed versionof the Proceedings of the FY 2015 Users Meeting for details).
Further reports were made on the research results from openuse projects, progress of the Kyoto University 3.8-m telescope
project including observing instruments, and operations of otheroptical and infrared observational facilities such as the Higashi–
Hiroshima Observatory.

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, provided for open use. Development of
the fiber-link system (HIDES-F) since FY 2006 has continued
to improve its observing capabilities. Open use of the highefficiency (HE) fiber link with approximately 50-K wavelength
resolution has continued since 2011A. The HE link offers an
improvement in throughput of nearly one magnitude over theprevious value 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 nearly 120K wavelength resolution started to be offered as a PI-type openuse instrument in 2016A. The HR link provides a 4 times better
sensitivity at maximum than the case of the Coudé light path.

This year the total numbers of accepted proposals to HIDES
were 7 and 9 in 2015A and 2015B, including 1 and 1 project
observations, respectively.
(2) ISLE (Near-Infrared Imager/Spectrograph)
The open-use instrument ISLE is a near-infrared imager andlow- or mid-dispersion spectrograph, and has been available
for project observations and the academic degree support
programs since 2011B. It is the only open-use instrument inEast Asia that offers near-infrared spectroscopic capability andis characterized as having the world’s best low-noise readout
capability (less than 10 electrons). Relative photometry at
the one milli-magnitude level is regularly achievable with its
imaging mode for bright sources. A YJH-band filter brought inby a user was installed in FY 2015, which extended the shorter
wavelength limit for spectroscopy from J-band edge (~1.16 μm)
to Y-band edge (~0.96 μm). By using the YJH-band filter andthe existing HK-band filter, it became possible to obtain a wellconnected spectrum from Y-band to K-band. The numbers of
open-use programs using ISLE conducted in semesters 2015A
and 2015B were 6 and 3, respectively; which included 1 and 1
academic degree support programs, respectively; and 1 and 0
miscellaneous category programs, respectively. Five of themwere spectroscopy and the other four were imaging photometry.
(3) KOOLS (Kyoto-Okayama Optical Low-dispersion Spectrograph)
This instrument provides imaging and spectroscopic
capability in the optical. It has been available for open use as a
PI-type instrument since 2008A. High observing efficiency has
been achieved by improving CCD output linearity and autoguider functionality and by introducing CCD charge shufflingand VPH grisms. Non-sidereal motion objects can be tracked
for long integration times. The integral field unit using a fiberbundle developed by a team at Kyoto University was madeavailable to observers as a PI-type open-use instrument startingfrom semester 2015B. When it is used, its input part is installed
into the Cassegrain unit of the HIDES fiber link and so is its
output part is installed into KOOLS. Accepted proposals were 4
and 2 for 2015A and 2015B, respectively.
(4) Others
MuSCAT (MUlti-color Simultaneous Camera for studying
Atmospheres of Transiting exoplanets) was accepted as a carryin observing instrument for open use on the 188-cm telescope.
Its use in the open-use time began in 2015B. It can achieve
0.05 % accuracy in relative photometry for a star of 10th
magnitude at V-band when it performs a series of one-minuteexposures.

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 the

II Status Reports of Research Activities

061

Nano-Optonics Institute (Astro-Aerospace, Inc.), regarding
the 3.8-m telescope project as part of the future plan of the
Observatory. Discussions were held on technological issues
regarding the telescope and observing instruments throughweekly TV conferences and in-person meetings held every threemonths. The project proceeded significantly with the telescope
construction having been included in the supplementary budget
of FY 2013 and the dome construction in the main budget of FY
2015.
(2) The Optical & Near-Infrared Astronomy Inter-University
Cooperation Program
The Program has entered its fifth year since its
commencement in 2011. The Observatory has contributed the
188-cm, 91-cm, and 50-cm telescopes to the Program, andhas taken a leading role along with the Office of International
Relations. Through the cooperative observational andeducational network, OISTER, established by the Program, theObservatory provided a total of 49 nights worth of observational
data on five objects this year. Two of the objects were targets ofcollaborative observations with the X-ray astronomical satellite“Suzaku” or of simultaneous VLBI observations with VERA. As
for the immediate follow-ups of gamma-ray bursts, which are
the main targets of the program, there were 19 alerts that wereobservable from the Observatory, observations were performed
six times and afterglows were detected in two of them. Threepeer-reviewed papers were published utilizing OISTER. Another20 peer-reviewed papers that have something to do with theProgram were published. The sixth workshop on the Program
was held.
(3) Gamma Ray Burst (GRB) Optical Follow-up Project
Optical follow-up observations of GRBs are in progress incooperation with the Tokyo Institute of Technology’s Kawai
Laboratory. During FY 2015, the automatic observation
scheduler performed observations on nearly every possible night;
15 GRBs were observed, with optical afterglows successfully
detected in two. Observation results were published as 12 GRB
Coordinates Network (GCN) circulars. In addition, followup observations of candidate gravitational wave sources andmonitoring of eclipsing binaries and comets were concurrently
performed, which resulted in publication of two peer-reviewed
papers. The telescope operation was suspended for a month due
to a malfunction in the dome rotation mechanism. A worn-out
roller in the machinery was replaced and measures were taken
against abrasion.
(4) Other
The Observatory welcomed five third-year undergraduate
students and their supervisor from the University of Tokyo
between August 12 and 14 and provided them with anopportunity to conduct high-dispersion spectroscopic
observations using the 188-cm telescope during the early halfnight on August 12.
Development of a near-infrared observing system dedicatedto bright star photometry (IR-TMT) continued in collaboration

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II Status Reports of Research Activities

with researchers at Tohoku University. The system consists ofa wide-field infrared camera with 30-mm aperture developedby researchers at Tohoku University being mounted on theequatorial mounting of a 30-cm class telescope housed in a 4-m
dome at the Observatory. It aims to produce a high precision
photometric catalog of bright stars in the near-infrared. The
control system of the equatorial mounting was developed by
the Observatory and the near-infrared camera by the Tohoku
University researchers. The camera was placed on the mounting
in December and various adjustments were carried out for test
observations of astronomical objects.

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 of currently 0.25
square degrees, observations were conducted to identify infrared
counterparts for objects such as GRBs and gravitational wave
sources. Along with them, a comprehensive survey of infraredvariable stars in the Galactic plane was carried out. In FY 2015a region of 6 square-degrees in the constellation Scutum wasobserved at the Ks-band about 70 times, and a region of 16
square-degrees in the constellation Cygnus was observed about
12 times. Many variable star candidates were identified.
(2) Automation of Exoplanetary System Searches
Through a Grant-in-Aid for Scientific Research (Basic
Research (A), “Automation of exoplanetary system searches,”
representative: Hideyuki Izumiura, FY 2011–2015), a projectis underway to improve the functionalities of the 188-cm
telescope and its dome, to enhance the precision and stabilityof the telescope, to facilitate automation of observation, and tofurther expand the search for exoplanetary systems. The 188cm telescope and its dome were refurbished in FY 2012 forthis purpose. A new control system including the observing
instruments was achieved in FY 2013. An automatic focus
correction system was developed in FY 2014. Functionality
was developed to improve the overall pointing accuracy bysensing small movements of the 188-cm reflector primary mirror
in its cell. Also, development advanced for a system capableof performing automatic observations based on observing
instruction.
(3) East Asian Planet Search Network
The Observatory also conducts studies focusing on the
search for exoplanetary systems, involving researchers fromSouth Korea, China, Turkey, and Russia. Efforts continued
in FY 2015 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. It
should be noted that a system consisting of a G-type giant withpossibly two mutually-retrograde planets was discovered fromthe collaboration with Chinese colleagues and was published ina peer-reviewed journal.

5. PR/Awareness Promotion Activities
An Observatory representative delivered a lecture tonearly 20 people in Okayama City on Tuesday, July 7 as partof the Nation-Wide Tanabata Participatory Lectures. About
40 astronomy-related questions from the public were posed
irregularly to the Observatory and were answered appropriately.
The 4D2U screenings, co-hosted with the Okayama
Astronomical Museum, attracted 4,740 visitors. Nineteen
Observatory tours were conducted, including those for pupils
from local elementary schools in Asakuchi City and Yakage
Town. The Observatory also responded to three lecture requests
made by local boards of education and community centers. It
should be noted that the Observatory received special publicity
during the NameExoWorlds campaign led by the IAU from2014 to 2015. Of the first 20 stars with planets for naming, six
had planets discovered by the 188-cm telescope and the highdispersion echelle spectrograph HIDES(-F) with fiber-link at
the Observatory. The names of the stars and their planets were
determined by public votes from all over the world and thenames were announced by the IAU on December 15, 2015.

6. Contract Staff Transfers
The following transfers of contract staff members took place
in FY 2015: Akihiko Fukui joined as a Project Research Fellow
in April and Kouki Kamiya resigned as a Research Support Staff
Member at the end of September.

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063

3. Nobeyama Radio Observatory
1. Nobeyama 45-m Radio Telescope(1) Open Use Observations
The 34th open use observations period started on December
1, 2015. In addition a new four pixel receiver FOREST withlimited capabilities has been offered since Jan 6, 2016 asscheduled. The “Education Program” was not offered.
The statistics of the proposals are as follows, “General
Proposals 1st period”: 13 accepted including 2 from abroad (25submitted), “General Proposals 2nd period”: 8 accepted withnone from abroad (21 submitted), “Short Programs”: 5 accepted(9 submitted), “Backup Programs,” which are carried out when
weather is not acceptable for the main observations: 2 accepted(3 submitted). One proposal for “General Proposals 2nd period”
was accepted as a “Backup Program” as recommended by theTime Allocation Committee. In addition, 2 proposals for the
45-m telescope’s participation in VERA open use observations
were conducted. The S80 and S100 receivers and the AOS were
decommissioned.
(2) Improvements and Developments
Maintenance of the 45-m telescope, the receiver systems, thecryogenics, etc. was performed.
- The replacement of the subreflector servo system wascompleted. A plan was developed for the millimeter wave
calibration drive system repairs to be conducted next year.
- Surface measurements with the holography system andsurface adjustment were performed. Consequently the surface
accuracy of the 45-m telescope was improved.
- Gold foil was put on the 2nd and 3rd mirrors to reduce the lossof the beam transmission system and decreasing the antennanoise temperature by about 10 K at 3 mm.
- Some parts of the new multi-pixel receiver FOREST were
replaced and the gain stability and linearity were improved.
- New AD converters were installed in all the intermediate
frequency lines and were used in open use observations.
- NRO supported user instruments including the Z45 receiverin the 45 GHz band, the digital spectrometer ROACH, and a
90/150 GHz continuum camera.
(3) Scientific Results
We are carrying out the (a) Star Formation Project, (b)Galactic Plane Survey, and (c) Nearby Galaxy Project as legacy
projects with the 45-m telescope. The star formation project and
the Galactic plane survey project obtained scientific data andtheir results are described below. Research results from openuse observations are given separately in the Scientific Highlights
section of this document.
(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

064

II Status Reports of Research Activities(1–0), C18O (1–0), and N2H+ (1–0). Many cores and clumps
have been identified from structure analysis of these data. We
succeeded in finding a protostellar molecular outflow in theOrion Molecular Cloud data by using existing data taken by
BEARS.
(b) Galactic Plane Survey Project (FUGIN: FOREST Ultra-wide
Galactic plane survey In Nobeyama)
We are conducting the highest resolution simultaneous
survey to date of the 12CO (1–0), 13CO (1–0), and C18O (1–0)
emission lines in the Galactic Plane using FOREST aboard the
45-m telescope. We plan to make maps of the inner Galaxy andthe outer Galaxy including the spiral arms and bar structure. In
2015, we covered areas with 46 and 28 square degrees for a totalof 74 square degrees. In the last two years, 115 square degrees
have been mapped. As a result, we have revealed a wide rangeof molecular clouds and their fine structures and also found a
new cloud-cloud collision system and an interacting region witha supernova.
(c) Nearby Galaxy Project (COMING: CO Multi-line Imaging
of Nearby Galaxies)
We started COMING (CO Multi-line Imaging of Nearby
Galaxies) in April 2015 to map more than 200 nearby galaxies
in 12CO, 13CO, and C18O J = 1–0 emission lines using FOREST.
As of now, mapping observations of more than 40 galaxies arecomplete. Among our samples, the precise 13CO/12CO line ratio
has been obtained for a barred galaxy NGC 2903. Excitation
analysis revealed that star formation efficiency is determinedby molecular gas density. In addition, through comparison witharchived data of CO (J = 3–2), it became clear that gas content
depends on the surface gas density in dwarf galaxy NGC 2976.

2. Radio Polarimeters
Nobeyama Radio Observatory took over operation of theRadio Polarimeters at the beginning of the H27 (2015) fiscal
year. On a monthly basis, the data are examined by solar
research groups in Kyoto University, in Ibaraki University,
NICT, and NAOJ Solar Observatory and are archived as publicdata in the NAOJ Astronomy Data Center so that researchers allover the world can access them.

3. Research Support(1) SPART (10-m telescope) (Osaka prefecture Univ.)
To better understand the influence of the activities of hoststars on the atmospheric environments of habitable planets,
we have been carrying out monitoring observations in the 100
and 200 GHz bands with a 10-m telescope, the Solar Planetary
Atmosphere Research Telescope (SPART). In conjunction
with the refurbishment of the Interferometer Building (IB), all
the NMA systems were removed and the new control room

for SPART was installed. Hereafter, the SPART system andits observations will be exposed to visitors. For corrective
maintenance in 2015, carbon dust in the Az/El motors wasremoved and the 4K-GM/JT compressor leakage was repaired.
Observations started in March 2015, and we successfully
demonstrated that CO mixing ratios in Venus’s middle
atmosphere were gradually decreasing. Comparative studies
with the Radio Polarimeter data in Nobeyama are now ongoing. In the coming year, atmospheric conditions on Venus andMars are predicted to vary as the solar activity moves toward its
minimum. Monitoring observations enable us to study chemical
networks, dynamics, and the effects of high energy particles. We
initiated a joint study with the Japanese Venus Climate Orbiter
AKATSUKI.
(2) Nobeyama Radioheliograph (Nagoya Univ.)
In FY 2015, an international consortium (ICCON) assumed
operation of the Nobeyama Radioheliograph (NoRH, see
http://hinode.stelab.nagoya-u.ac.jp/ICCON/). The remote
operating system via internet has functioned very well. About
30 researchers from six countries (China, Japan, Korea, Russia,
the UK, and the USA) participated in operation, including thesystem health check and data verification. Observational data
are automatically transferred to NAOJ and Nagoya Univ. andare stored/maintained there. NoRH data are used by researchers
all over the world to study short-time scale phenomena, such as
solar flares, and to study long-term activity as well. Recently,
a methodology to determine the magnetic field intensity in thesolar corona has been established. Then a press release wasissued in February 2016 and an article was inserted in a science
newspaper. On March 9 in 2016, a partial solar eclipse was
successfully observed and the microwave images during theeclipse are released on the homepage of the Institute for SpaceEarth Environmental Research (ISEE), Nagoya Univ.

4. Public Outreach(1) PR activities at Nobeyama Campus
The Nobeyama Campus received a cumulative total of
52,614 visitors throughout the year, including participantsin special open house events. Staff members conducted 42
guided tours, including ones for Super Science High School(SSH) students and the Campus Tour Week, while 3 requests
for lectures and 22 requests for on-site filming and interviews
were granted. These requests, especially those by some local
broadcast stations in Nagano prefecture, increased due toefforts to strengthen cooperation with local communities. The
Campus Tour Week for educational institutions was scheduledduring the summer. Though only 1 group took advantage ofthis opportunity, students in the group enjoyed the visit. For
the workplace visit, 7 students from 4 schools, primarily local
junior-high schools, visited the observatory. Also, we conducteda career educational program for local high-school students andexperience training for local teachers. For SSH initiatives, twoschools visited NRO and participated in lectures.
In the area for permanent public access, an antenna

experience facility and some introduction movies are available
along with posters and panel displays. In this year, we renovated
all the panel displays and a brochure for children in order for
visitors to become more familiar with NRO. The website of
NRO presents introductory descriptions of radio astronomy andsome events as well as observational results.
(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 the forests of the
University of Tsukuba. Special sponsorship was made to thesora-girl event “Tebura de Hoshizora Kansho-kai (Dropby Star Gazing Event),” hosted by the Minamimaki Tourism
Association. NRO has also participated in the “Three Major
Scenic Locations for Star Gazing in Japan • Night Sky Summit”
conducted with the sponsorship of the Minamimaki Tourism
Association since the planning stage. Also, a training course andexaminations were carried out through a special partnership with
Shinshu-Saku Hoshizora Annai-nin, which was managed by
Saku Koiki Rengo (the Union of local governments in the Saku
area).
The “Artist in Residence” Program was carried out at NRO,
organized by Siga-Kogen Romance Art Museum. Participating
artists were inspired to make some artworks, which were
exhibited in the special exhibition “Viewing the Universe”,
held in the Museum from July to October. Also, one of the oldreceivers from the 45-m radio telescope was displayed in the
exhibition.
(3) Improvement Plan for the Nobeyama Millimeter Array Building
The building of the Nobeyama Millimeter Array will be
improved to install an exhibition area highlighting NINS as
well as NAOJ, in order to establish a PR center not only for
astronomy but also for the natural science. The improvement
work on the building and installation of the 4D2U theater werecarried out in this year.
(4) NRO Conference Workshops- Nov 2, 2015
NRO Galactic Plane Survey Workshop 2015 (representative:
Atsushi Nishimura)- July 28-30, 2015
NRO-ALMA Science/Development Worksho p 2015
(representatives: Masao Saito (NRO), Daisuke Iono (Chile
Observatory)- Oct 20-22, 2015
ALMA/45m/ASTE/Mopra Users Meeting 2015
(representative: Daisuke Iono (Chile Observatory), Masao
Saito (NRO))

II Status Reports of Research Activities065

5. Education
NRO accepted two postgraduate students. One is a firstyear Ph.D. student in SOKENDAI studying chemical reactionsof carbon chain molecules. The other one is a visiting student
from Kagoshima University whose research is a molecular cloud
survey in the outer Galaxy and development of a new digitalspectrometer using ROACH technology.
SOKENDAI held the workshop on Radio Astronomical
Observation using the Nobeyama 45-m Radio Telescope from
June 1 to 5, with 12 undergraduate students in attendance. The
majority of the participants were 4th year students, just about todecide their course after graduation. While guiding the students,from observations to presentation of the results, requires
significant effort, the event offers an invaluable opportunity
for undergraduates to experience observations using a radio
telescope and to think of their future career.

6. Misc. Activities(1) Hiring
Hiroyuki Kaneko: Specially appointed research staff
Yusuke Miyamoto: Specially appointed research staff(2)Transfer
Jun Nishimura: Specially appointed research staff (to Nagoya
University)

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4. Mizusawa VLBI Observatory
NAOJ Mizusawa VLBI Observatory operates VLBI (VeryLong Baseline Interferometry) facilities such as VERA (VLBI
Exploration of Radio Astrometry) and KaVA (KVN and VERA
Array), and provides these unique facilities to the internationaluser community to support the research activities at universities
and research institutes. In the meantime, astronomical researchusing these VLBI arrays is conducted mainly on the Galactic
structure, celestial masers, AGNs and so on. Using the uniquedual-beam system which is capable of phase referencing byobserving two sources simultaneously, VERA conducts highaccuracy astrometry of maser sources and determines thedetailed structure of the Milky Way. In addition to the operationof VERA, maintenance and operation support were provided
to the Yamaguchi 32-m Radio Telescope and two Ibaraki 32-m
radio telescopes in collaboration with the local universities.
International collaboration has been promoted particularly in the
East Asia region through the joint operation of KaVA and theEast Asian VLBI Network, the latter of which is a joint VLBI
array between the People’s Republic of China, Japan, and theRepublic 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 geophysical research,and Ishigakijima Astronomical Observatory is jointly operated
with the local city for public outreach and astronomical 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 2015, a total of 427 (3670 hours) VLBI
observations were conducted with VERA, such as commonuse observations, VERA project observations, fringe detection
observations 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 the Mitaka
VLBI Correlation center in NAOJ Mitaka Campus until 2014;
in 2015 these processing functions were moved to the Mizusawa
correlation center. The correlated data were sent to eachresearcher for the case of common-use and JVN observations
and to persons in charge of data analysess in the case of project
data and geodesy data. Iriki station was damaged by a typhoonat the end of August. Due to this damage, Iriki station was
unavailable for VERA observations for about two months.
VERA common-use calls-for-proposals with the 43, 22, and
6.7 GHz bands for semesters 2015B and 2016A were released in
May and November, respectively. A total of 11 proposals, which
requested a total time of 462 hours, were submitted, including 3
proposals for 130 hours from overseas. Based on the evaluations
by referees elected from scientists in related fields, the VLBI
program committee decided to accept a total of 7 proposals (227hours) in 2015B and 2016A.
(2) Science Research
In FY 2015, the second part of the PASJ VERA special issue
has been published as a continuation from the one in FY 2014.
The FY 2015 part included 6 papers, and in total there have been
13 papers in the VERA special issues in 2014—2015. This has
been the third PASJ VERA special issue after the ones in FY
2008 and FY 2011.
As the results of the project observations of VERA,
the parallaxes and proper motions have been reported forfive galactic star-forming regions, namely, G48.99−0.30,
G49.19−0.34, IRAS 20126+4104, IRAS 21379+5106, andIRAS 07427−2400. The last source is located in the Perseus
spiral-arm, and together with the previously published sources
associated with the arm, non-circular motion associated with
the Perseus spiral-arm was successfully detected, showing
systematic inward motion toward the Galactic center and lagging
behind the Galactic rotation. It has been shown that the motions
can be described well by a density-wave-type spiral model. Thisis the first result on the Galactic non-circular motion based on
VERA astrometry, and thus it is one of the milestones of the
Galactic structure study with VERA. Simulation studies havebeen performed to evaluate the expected accuracy with which
future VLBI astrometry will be able to constrain the Galactic
parameters. It is demonstrated that astrometric measurementsfor ~300 sources will provide accuracies of a few % for the
Galactic fundamental parameters and accuracies of about 10 %for the parameters associated with the non-circular motion andasymmetric structure, such as spiral arms and/or bar.
Astrometric results are also published for a late-type star U
Lyn, and the data are used to calibrate the Period-Luminosity
relation of Mira-type variables based on U Lyn and 8 othersources for which accurate distances have been measured so far.
Other than the Galactic astrometry, astrometric observationsof the core position of TeV blazar Mrk 501 have been used
to constrain the Lorentz factor of the jet, demonstratingthat accurate VLBI astrometry has a wide range of possible
applications other than Galactic structure studies.

2. JVN (Japanese VLBI Network)
The Japanese VLBI Network (JVN) is operated as a joint
research project of NAOJ and seven universities. JVN consistsof VERA and radio telescopes operated by universities andresearch institutes such as ISAS/JAXA, NICT, and GSI. VLBI
observations by JVN were done for 250 hours at 3 bands of 6.7,
8, and 22 GHz in FY 2015. Single Dish Observations related
to JVN were also done about 2000 hours at each telescope.
The major research topics are AGNs, masers, and star forming
regions.
The main subjects of research are active galactic nuclei
and masers in star-forming regions. Scientific results obtained

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with JVN were published as four papers, while ten more papers
reported JVN related scientific studies. Fujinaga et al. (2016)
reported the results of a gamma-ray-emitting-AGN survey
through high-sensitivity VLBI observations. Sugiyama et al.
(2016) reported the first results of internal motion in a 6.7 GHz
methanol maser source obtained by EAVN (East-Asian VLBI
Network) including JVN. Yonekura et al. (2016) reported on thetelescope and observing system of Ibaraki station. Nine papers
including the above four will be published as a special issue of
PASJ in FY 2016.
Education is also one of the main aims of university
collaboration in VLBI. Twenty-nine students conducted undergraduate studies using JVN and related research activities.
Sixteen master-course students completed their master’s theses
using JVN, and two Ph.D. students finished their theses using
JVN. Many university students made presentations and talks inresearch meetings related to JVN.

3. Japan-Korea Joint VLBI (KaVA)

068

three large programs are ongoing, each of which is led by oneof the three KaVA science working groups (AGN, star-forming
regions, and late-type stars). Not only researchers in NAOJ/KASI but also many external researchers (universities in Japan/
Korea, Australia, Italy, etc.) are joining these projects. Scientificoutcomes based on these programs will be expected to emerge
from the next year.

4. EAVN
Aiming at expanding the capability of international VLBI
over East Asia, the development of the East-Asian VLBI
Network (EAVN) is currently underway as a collaboration
between Japan, South Korea, and China. Technical assessmentof the array and test observations are promoted by the JapanKorea-China joint task force (the so-called Tiger Team), andin FY 2015 a report summarizing the successful detections offringes over the last few years was published in the proceedingsof an international conference (Wajima et al. 2015). Following
this success, in FY 2015 further test observations wereconducted to evaluate the imaging performance of the EAVN
array at 8, 22, and 43 GHz. Detailed reports of these data willappear next year.
Meanwhile, recently there is a growing discussion toward
the future construction of a new VLBI facility in Thailand(Thailand VLBI Network; TVN). In these circumstances,in FY 2015 a KaVA science workshop was held in Thailand
in collaboration with local astronomers, and discussed thepossibility and potential impact of the future extension of TVN
by joining the EAVN.
In FY 2015 the annual EAVN workshop was held at
Hokkaido University, and the next meeting in FY 2016 will takeplace in China.

(1) Observations and Common-Use Observations
In 2015, a total of 121 (1023 hours) VLBI observations,common-use observations and test observations, were conductedby KaVA (KVN and VERA Array) with the 43 and 22 GHz
bands. The data of the seven VLBI stations were correlated
at the Korea-Japan Joint Correlation Center at KASI Daejeon
Campus in South Korea.
KaVA common-use call-for-proposals for semesters
2015B and 2016A were made in May and November of 2015,
respectively. In total, 20 proposals requesting a total time of736 hours were submitted. Through the evaluations by referees
elected from scientists in related fields and subsequent decisions
made by the VERA and KVN combined Time Allocation
Committee, a total of 15 proposals (507 hours) were accepted in
2015B and 2016A.

5. Geodesy and Geophysics(2) Results of Research
Following the successful opening of KaVA common-use
observations and the first publications of KaVA papers in FY
2014, the science productivity of KaVA is growing satisfactorily
with the stable array operation throughout FY 2015. As for
AGN science, the detailed motions of relativistic jets are now
regularly monitored for a number of sources; three refereed
papers were published on several bright blazars including 3C345
during FY 2015. Moreover, our KaVA monitoring of the M87 jet
made the first discovery of a superluminal motion near the black
hole. The talk on this result was selected for a press release at
the ASJ meeting in March 2016 and was picked up by many
media outlets, returning scientific results from KaVA to thebroad general public. Another refereed paper reporting a detailed
imaging of SiO masers around the late-type star WX Psc wasalso accepted.
The KaVA Large Program has finally started from late FY
2015, which aims at performing ambitious, high-scientificimpact studies with KaVA by spending a large amount (typicallymore than 100 hours per year) of the machine time. Currently

The regular geodetic sessions of VERA are allocated two or
three times per month to maintain baseline accuracy of the array.
VERA internal geodetic observations are performed once or
twice per month using K-band, and the VERA Mizusawa station
participates in IVS sessions using S- and X-bands on a once-permonth basis. In order to improve stability among the geodetic
results, experimental geodetic VLBI observations which use
newly developed high speed samplers and recorders were started
and geodetic results were obtained from 8-Gbps recording data.
In FY 2015, 11 IVS sessions and 17 sessions of VERA
internal geodetic observations were conducted. The final
estimation of geodetic parameters is derived by using thesoftware developed by the VERA team.
After “The 2011 off the Pacific coast of Tohoku Earthquake”(Mw=9.0), VERA Mizusawa was displaced by co-seismic crustal
movement, and post-seismic creeping continued to be detected
in FY 2015. According to the newest analysis, the co-seismic
steps are X = −2.066 m, Y = −1.420 m, and Z = −1.064 m; andthe displacement by creeping during FY 2015 is X = −0.101 m,
Y = −0.056 m, and Z = −0.015 m.

II Status Reports of Research Activities

Continuous GPS observations at VERA stations are carriedout in order to detect short term coordinate variations andto estimate atmospheric propagation delays. The results of
GPS positioning also show a post-seismic motion to the Eastsouth-east of Mizusawa even though 5 years have passed
since the occurrence of the 2011 off the Pacific coast of
Tohoku Earthquake. Continuous gravity observations withsuperconducting gravimeters are carried out at Mizusawa andKamioka. Similar observation is carried out at Ishigakijima
as a joint project with other institutes and university groups.
The features of the annual change are observed and studied
by several techniques including VLBI, GPS, and gravimeters.
The strain and tilt observation data obtained at 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.

6. System Development

performed in collaboration with Japanese universities. There
were six published refereed papers for which the observations at
IAO played an important role, including the study of the comet
17P/Holmes.
The number of participants in the “Southern Island Star
Festival,” which has been held for 14 times, has also been
increasing, and 9000 people attended the light-down stargazing
party. Since FY 2015 is the 70th anniversary of the end of WorldWar II, the movie “Vega shining over the battlefield,” producedby the Yamanashi Prefectural Science Center, was screenedin the astronomy lecture room, and a Japanese Tanka contest
on “Stars and Peace” was held by inviting famous Tanka poet
Machi Tawara to be a selector. Eventually about 11,000 people
participated in the festival.
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. The
asteroid (372024) that was discovered by the high school
students who participated in the workshop in 2008 was named“Ayapani” by public subscription.
On the other hand, interaction and personnel exchange withJapanese public astronomical observatories were promoted. The
star summit was held in Minamimaki, Nagano, where Nobeyama
Radio Observatory is located. The special rice-fish called "Space
Medaka" were donated from by Saji Observatory in Saji, Tottori,
and they are being bred in Ishigaki City, Nagura elementary andjunior-high school.

In 2015, the magnetic tape recorders were replaced withnew hard disk drive recorders, and the Mitaka FX correlator
was also replaced with a newly developed software correlator.
The software correlator is located at Mizusawa Campus and is
now in regular operation. The modifications to the KJCC (Korea
Japan Correlation Center) system were done based on the feedback from scientific evaluation of the KaVA observations.
Discussions on future development have been done in particular
toward high frequency VLBI and SKA as future extensionsof VLBI activities. Basic design and development were done
including a low power consumption optical transmitter, ultrawideband A/D convertors, high accuracy surface reflectors, andballoon-borne radio interferometry.

In order to promote public outreach, special open house
events were done as follows, and regular campus visits are alsooffered throughout all the seasons as summarized below.

7. Timekeeping Office Operations(1) Open House Events

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) server at
the Timekeeping Office provides “Japan Central Standard Time”
on a network. This service has been in great demand with morethan 1,500,000 daily visits recorded last year.

April 19, 2015
The Sixth Open Observatory Event held at the Ibaraki
University Center for Astronomy, and NAOJ Mizusawa VLBI
Observatory, Ibaraki station, with approximately 230 visitors.

8. Ishigakijima Astronomical Observatory
FY 2015 is the 10th year since Ishigakijima Astronomical
Observatory (IAO) was opened in FY 2006. Since “Room for
Learning the Starlit Sky” was established as an annex to theobservatory by Ishigaki City in FY 2013 to screen 4D2U (FourDimensional Digital Universe), the number of visitors per year
has increased to more than 14,000 people in FY 2015.
In terms of the research at IAO, observations of transient
objects such as gamma-ray bursts and Solar System objects were

9. Public Relations (PR) and Awareness

July 4
The 23rd Tanabata Star Festival at the site of the 6-m
antenna at Kinko Bay Park in Kagoshima City co-hosted with
Kagoshima City and Kagoshima University, with approximately
100 visitors.
August 8
The special open house of VERA Iriki station held jointlywith “The Yaeyama Highland Star Festival 2015,” withapproximately 4000 visitors in attendance.
August 15–23
The “Southern Island Star Festival 2015” held together witha special open house event at the VERA Ishigakijima station
and Ishigakijima Astronomical Observatory with 10,930 visitors

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to the whole “Star Festival.” Events included an astronomical
observation party at Ishigakijima Astronomical Observatory,
attended by 877 visitors; and a special public opening of the
VERA station attended by 238 visitors.
August 22“Iwate Galaxy Festival 2015”, open house of NAOJ
Mizusawa Campus, held with 660 visitors in attendance.
February 14, 2016
“Star Island 15,” open house event of VERA Ogasawara
Station held with 222 visitors in attendance.
(2) Regular Public Visiting
Throughout the year, the following stations are open to
public on a regular basis.
The numbers of visitors to each facility is as follows,a) VERA Mizusawa Observatory 17,415
The open house event is held at the campus with thecooperation of the Oshu Space and Astronomy Museum(OSAM: Yugakukan) located in the campus.
b) VERA Iriki Station 1551
c) VERA Ogasawara Station 8540d) VERA Ishigakijima Station 2713e) Ishigakijima Astronomical Observatory 13,906
Stargazing sessions: Evenings on Saturdays, Sundays.
The “Room for Learning the Starlit Sky” (featuring the
4D2U “Four-Dimensional Digital Universe”), constructedadjacent to the observatory in FY 2013 by Ishigaki City, wasvery popular, welcoming 3925 guests.
(3) Access Statistics of the Website Contents
Websites related to Mizusawa VLBI Observatory and thenumber of visitors are:Contents List
Mizusawa VLBI
Observatory
VERA
Kimura Hisashi
Memorial Museum
Ishigakijima
Astronomical
Observatory

Sessions Internet Users Page Views
24,201

17,33772,608

11,678

6,778

39,952

5,726

5,057

8,646

80,76950,319161,242

10. Education(1) University and Post-Graduate Education
Regarding postgraduate education, the Mizusawa
VLBI Observatory assisted two graduate students from the
University of Tokyo and two from SOKENDAI for their PhD/
master’s research. One of the students from the Universityof Tokyo completed his master's thesis. One master's student
from Tokai University was accepted as a visiting graduate

070

II Status Reports of Research Activitiesstudent. Undergraduate students from Tohoku University
and Tokai University were accepted as summer students of
SOKENDAI. The Observatory staff organized “The Radio
Astronomy Winter School 2016” in collaboration with NARIT(National Astronomical Research Institute in Thailand) andUST (University of Science and Technology, South Korea).
The school was held February 15-19, 2016 at Chiang Mai in
Thailand. About 30 students from Asian countries attended the
School. The University of the Ryukyu and NAOJ have offereda joint course on astronomy from FY 2009. Classroom lecturesat the university took place August 24-27, and observational
workshops were held in Ishigakijima from September 1 to 4,
with a total of 25 participants. In addition, staff members ofMizusawa VLBI Observatory give lectures at the University ofTokyo and Tohoku University as visiting professors.
(2) Research Experience for High School Students“The 9th Z Star Research Team Event” was held August 1-3
to use the VERA Mizusawa antenna for observation. Eleven highschool students from Iwate Prefecture attended. During August
12-14, the VERA Ishigakijima station and The Ishigakijima
Astronomical Observatory held “The Chura-boshi Research
Team Workshop” for 18 high school students from Ishigakijima.
It was organized under support from JSPS. One of the groups
detected a new maser source using the VERA Ishigakijima
station, and presented the results in the open-house of VERA
Ishigakijima station. Mizusawa VLBI Observatory supported theSSH (Super-Science High-school) research activities for Yokote
Seiryo High School in Akita Prefecture to use the Mizusawa
20-m antenna. The observational results were presented in “The
Junior Session” in the annual meeting of “The Astronomical
Society of Japan”.

5. Solar Observatory
The Solar Observatory primarily engages in the operationof solar observational facilities on the west side of Mitaka
Campus and in the development of new observational
instruments. It conducts both observational and theoreticalstudies of the structure of the outer solar atmosphere, including
the photosphere, chromosphere, corona, and solar wind; andactive phenomena such as sunspots, faculae, prominences,and flares. This observatory performs regular observations
using instruments such as the Solar Flare Telescope (SFT) andalso conducts expeditions to observe total solar eclipses. It
is also engaged in the planning of future ground-based solar
observations. Regular observations of sunspots and flares havebeen carried out for extended periods, and the resulting data areprovided to researchers.

1. Observational Facilities in Mitaka(1) Magnetic Field Observation
The SFT, which has been the main instrument of the
Observatory at Mitaka Campus, has continued observations ofactive region photospheric vector magnetic fields and H-alphaflares since its full completion in 1992. The main instrumenton the SFT since 2010 is an infrared Stokes polarimeter.
Whereas previous magnetic field observations covered part ofthe solar surface, this instrument is designed to perform fulldisk polarimetric observation to obtain high accuracy vector
magnetic field information in order to shed light upon the originsof the solar activity cycle. This polarimeter is equipped witha 15-cm infrared-transmitting lens and performs slit scanningobservations using infrared spectral lines (photosphere: iron,1.56 μm line; chromosphere: helium, 1.08 μm line), which
are sensitive to the magnetic field. This allows for constantacquisition of unprecedented infrared polarization data for thephotosphere and chromosphere of the entire solar disk. It had
taken about two hours to cover the full Sun with a slit scan foreach wavelength range, but a new system enables us to observe
two wavelength ranges simultaneously using two cameras
installed in 2014. The data acquisition is now conducted more
efficiently. To further improve the data quality, the installation ofan advanced infrared camera with a large format and low readout noise is being conducted, using a grant from the Project for
Solar-Terrestrial Environment Prediction (PSTEP), Grants-inAid for Scientific Research on Innovative Areas.
(2) Regular Observation of Sunspots/Faculae/H-alpha Flares
Sunspot observations have been performed continuously
since 1929. These observations are currently conducted via
automatic detection of sunspots in digital images captured witha 10-cm refractor and a 2 k × 2 k pixel charge coupled device(CCD) camera mounted on the new (full-disk) sunspot telescope.
Observations were conducted for 241 days in FY 2015, from
April to March.
Although full-disk solar image data are a widely needed

resource in the astrophysics/geophysics community, some ofthese synoptic instruments are becoming out of date. Efforts areunderway to update the photospheric and chromospheric imaging
instruments and to further flesh out the data. For instance, theSFT has started advanced observations in the H-alpha line toacquire full-disk, high-resolution images. It can obtain Doppler
velocity information based on imaging at multiple wavelengths
around H-alpha. High temporal resolution allows it to more
completely capture active phenomena, and a combination ofmultiple exposure times allows for a broad dynamic range.
Further improvement in dynamic range and read-out noise wasaccomplished using sCMOS cameras installed in this year.
This advancement has enabled us to observe many phenomena,such as flares and prominence eruptions, even during the recent
downturn in solar activity. The Observatory also uses the SFT
to conduct regular imaging observations in the G-band (430 nm)
and continuum wavelengths. In addition, CaII K (393 nm) filter
observation has started this year.
The regular observational data described above, including
real-time images, are available on the website of the
Observatory. Using a Grant-in-Aid for Scientific Research, aspectrograph system with a coelostat is under development
to perform long-term, full-disk observations, including morequantitative velocity and magnetic field observations. An
improvement to the spectrograph room was conducted this year.
The Observatory maintains other existing equipment to allow
for everyday observation, as well as experimental use.

2. Opening of Data Archives to the Public
The Solar Observatory has made nearly 16.2 TB ofdata available to the public online, including data from thecurrent observations of white light, H-alpha, and magnetic
fields as well as those from nearly 100 years of various typesof solar observations. The various phenomena occurring inthe solar-terrestrial environment must be studied in terms ofboth sudden, short-term events (space weather) and in termsof gradual changes occurring over years or decades (space
climate). The Observatory will continue providing fundamental
data for these studies. The Observatory possesses nearly 100
years of accumulated records, including continuum images,
Ca II K-line images, and H-alpha images recorded on film,
photographic plates, and hand-drawn sketches, all of whichhave an importance of their own. The Observatory will makethese available to the public as well when they are digitizedand organized. As some of the world’s oldest records of solar
activities, these materials are expected to add particular insight
into future research. Higher bit digitization of old Ca II K line
images improving the data quality was conducted this year asa part of research activity for the PSTEP, Grants-in-Aid for
Scientific Research on Innovative Areas.
Data publicized via the website were previously stored
on a server owned by the Observatory. The information has

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071

since been transferred to the Astronomy Data Center, where
all relevant data servers have been managed in an integrated
fashion. The same data are stored at multiple locations in thedata center, serving as a backup in case of disaster.

3. Other Activities/Personnel Transfers
International cooperation includes support for the Japan–
Peru collaborative solar observations, with which the Solar
Observatory has been involved since 2004. In addition to thecollaboration in solar spectrograph installation and operationin Peru, relocation of the 10-cm coronagraph which had beenused in Norikura Solar Observatory is envisioned. For thispurpose, the coronagraph was reassembled and used to run
test observations at Norikura Corona Observatory, this year.
The Solar Observatory also supports the operation of another10-cm coronagraph with a NOGIS filter system in a Chinese
observatory (3200 m elevation) in Yunnan province. This
coronagraph was relocated from Norikura in 2013 to observe
two dimensional intensity and velocity fields of the solar coronain the coronal green line of Fe XIV (530.3 nm).
The solar optical observations at Hiraiso Solar Observatoryof the National Institute of Information and Communications
Technology are considered to be terminated. To examine thepossibility of utilizing the instruments in the future at otherinstitutes, their removed H-alpha Lyot filter and telescope/coelostat for solar magnetic field measurements were placed instorage at Mitaka this year.
A research plus business conference, dubbed as the annual
users meeting, has been held every year jointly with otherorganizations. The meeting is combined with the solar research
symposium for the entire solar community, where topics related
to open use and future plans are also discussed. The conference
was held at NAOJ between February 15 and 17, 2016.
Observation of the total solar eclipse of March 9, 2016 inIndonesia was conducted by Drs. Hanaoka and Morita. The
observation was not so successful because of a cloudy sky, butsome data of prominence and corona through the clouds wereobtained.
Because the Observatory deals with fundamental solardata, there are often requests to use images from the Solar
Observatory database in school textbooks, to contribute toarticles in newspapers or magazines, and to help public events
held by museums. The Observatory actively responded to theserequests.
Regarding personnel transfers, Dr. Masaoki Hagino replaceda previous research expert, Dr. Naomasa Kitagawa. Dr. Anand
Joshi will take a position as specially appointed research staff
at the start of the new fiscal year, after the departure of Dr.
Ken’ichi Otsuji. Prof. Takashi Sakurai was honorably discharged
in the end of FY 2015, March 2016.

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6. NAOJ Chile Observatory
The ALMA Project is a global partnership of East Asia (ledby Japan), Europe, and North America (led by the United States)in cooperation with other nations to construct and 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 achieve a
spatial resolution nearly ten times higher than that of the Subaru
Telescope or the Hubble Space Telescope. Early scientificobservations with ALMA began in FY 2011 with a limited
number of antennas and full operation commenced in FY 2012.
This report describes the progress of the ALMA project, which
includes the results of the open-use scientific observations andpublic outreach activities. The ASTE telescope is a single-dish10-m submillimeter telescope located in the Atacama highlands.
It has been operated to make headway into submillimeter
observations toward the ALMA Era. This report also describes
the progress of the ASTE telescope.

1. ALMA Project Progress
Along with scientific observations, ALMA commissioning
observations have been underway, including polarization tests
and solar observation tests.
NAOJ staff members played leading roles in the polarization
tests and solar observation tests. As demonstrated by Koichiro
Nakanishi and Hiroshi Nagai for polarization, and Masumi
Shimojo for solar observation tests, East Asian researchers havebeen taking the initiative in the international teams. Also Band
10 receivers, the highest observing frequency band, became
available for scientific operations starting from the fourth roundof open-use observations of ALMA (Cycle 3) which started in
FY 2015. The sub-components developed by Japan, such as theantennas, correlators, and receivers (Bands 4, 8, and 10), areworking properly for the operations.

2. ALMA Open-Use and Scientific Observations
The fourth round of open-use observations of ALMA
commenced in October 2015 as Cycle 3. The Cycle 3 main
capabilities include: interferometric observations using thirtysix 12-m parabolic antennas; Atacama Compact Array (ACA)
observations (interferometric observation with ten 7-m antennas
and single-dish observations with two 12-m antennas); sevenfrequency bands (Bands 3, 4, 6, 7, 8, 9, and newly-added Band10 ); maximum baselines greatly extended from 1.5 km to 10
km (for Bands 3 to 6), 5 km (for Band 7) and 2 km (for Band 8
to 10); and polarization for continuum observations. In responseto the Cycle 3 call for proposals, 1578 observation proposals
were submitted from all over the world. This figure exceeded
the world’s highest number of proposals ever recorded, which
was submitted to the Hubble Space Telescope. Such a highsubmission rate to ALMA shows high expectations for “theglobal telescope ALMA” with the potential to contribute to awide-range of fields such as galaxy formation, star and planet
formation, the Solar System, astrobiology, and interstellar
chemistry.
An open call for the fifth round of open-use observations
was issued as Cycle 4. The anticipated capabilities of Cycle
4 include: interferometric observations using forty 12-m
antennas; ACA observations (interferometric observation withten 7-m antennas and single-dish observations with three 12-m
antennas); seven frequency bands (Bands 3, 4, 6, 7, 8, 9, and10), maximum baselines of 12.6 km (for Bands 3 to 6), 6.8
km (for Band 7), and 3.7 km (for Bands 8 to 10). Cycle 4 also
provides new opportunities for large programs that require longobservations exceeding 50 hours; millimeter-wavelength VLBI
observations; ACA stand-alone mode; solar observations; andpolarization for spectral line and continuum observations. The
public call for Cycle 4 proposals is set to close at 00:00 JST on
April 22, 2016. Cycle 4 is scheduled to start in October 2016.
Open use of ALMA has already produced a number ofscientific achievements. This section describes some of them,focusing mainly on East Asian projects. A research group led
by Yoichi Tamura at the University of Tokyo found several dust
clouds with a size of 500 light-years distributed inside SDP.81
through detailed analyses of the image of the gravitationallylensed galaxy SDP.81 captured by high-resolution observations
with ALMA and comparison of this image to its gravitationallens model. The results of their study also indicate the existenceof a supermassive black hole over 300 million times more
massive than the Sun at the center of the foreground galaxy.
A research group led by Kyoko Onishi at SOKENDAI (The
Graduate University for Advanced Studies) observed the barredspiral galaxy NGC 1097 with ALMA and through a detailed
study on the kinematics of molecular gas at the center of thegalaxy found that this galaxy harbors a supermassive black hole
140 million times more massive than the Sun. This research
result is based on the ALMA observation data obtained withina two-hour observation, which demonstrates the outstanding
capability of ALMA in the mass measurement of supermassive
black holes. A research team led by Hideki Umehata
successfully captured a cluster of nine starburst galaxies in acluster of young galaxies 11.5 billion light years away from the
Earth (at the center of a “proto-Great Wall” known as the largest
structure in the Universe). This result supports the idea that the
proto-Great Wall is the matrix that supports the formation ofgalaxies. This could lead to unveiling the formation process of
starburst galaxies and their subsequent evolutionary process. A
research team led by Yusuke Aso at the University of Tokyo andNagayoshi Ohashi at NAOJ observed a proto-star called TMC1A and revealed the movements of the inner rotating gas disk
around the proto-star and the outer gas envelope with the highest
accuracy ever achieved. The high-sensitivity observations
with ALMA made it possible to directly observe the boundary
between the disk surrounding the proto-star and the outerinfalling gas envelope. These results are very important in

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finding out when the proto-planetary disk appears in the processof star formation and how it evolves.

3. Educational Activities and InternshipTwo undergraduate students joined research activities on
an internship at the NAOJ Chile Observatory office in Mitaka:
one came from the University of Science and Technology of
Hanoi in Vietnam from June through September 2015; and theother from the FTP University in Vietnam from January throughMarch 2016.

4. Public Outreach Activities
Approximately 35 newspaper/journal articles were publishedin Japan, reporting the achievements of scientific observations
and test observations with ALMA, while there were 14
Japanese television/radio programs that featured ALMA. In
these programs, they showed the results of ALMA observations
in various fields of astronomy; in particular, a news program
called “News 7” on NHK G channel covered ALMA focusing
on the field of astrobiology. In online media, “IFLScience!” (ascientific website with a great number of subscribers) posted
an article on ALMA observation results delivered by Japanese
researchers, which was shared and liked on Facebook by 17,000
users. As seen in this example, the scientific results by Japanese
researchers have been increasingly propagated worldwide.
The NAOJ ALMA website posted 43 news articles and eightpress releases. A mailing-list-based newsletter has been issued ona monthly basis with approximately 2,500 subscribers. Updated,detailed information is available on Twitter (@ALMA_Japan),with nearly 27,500 followers as of the end of FY 2015.
In May 2015, NAOJ Chile Observatory hosted a week-long
ALMA booth at the Japanese Geoscience Union Meeting heldin Makuhari Messe. NAOJ Chile Observatory organized public
lectures and science cafe events on 26 occasions in FY 2015 toprovide updated information and increase interest in ALMA andits scientific achievements through conversation with a large
number of visitors. Especially, the 21st ALMA public lecture
titled “Star and Planet Formation Explored by ALMA” held
in Osaka Science Museum on December 12, 2015 attracted a
big audience exceeding 200, which was a great opportunity toprovide the latest scientific results to the public.
As part of the construction film project continuing since FY
2003, NAOJ Chile Observatory produced a new film that shows
the development of the receivers at the Advanced Technology
Center (ATC), focusing on the development and production ofreceiver cartridges in FY 2014. In addition to this, interviews
with developers of the ACA correlators were also filmed.
The NAOJ newsletter featured ALMA in the September
2015 issue with an article summarizing the ALMA project andits scientific achievements so far, including interviews with
ALMA staff members at the ALMA Regional Center to widely
cover the staff members supporting the open use and promoting
their scientific activities, including their enthusiasm and passion
for the work.

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From mid-March 2015, ALMA started to welcome public
visits to the ALMA Operations Support Facility (OSF) at analtitude of 2900 meters. Every Saturday and Sunday, ALMA
admits up to 40 people/day (advance registration is required).
Visitors to the OSF can have a guided tour including the control
room, and watch videos on ALMA. Each time, registration
reaches full capacity soon after the start of registration. Public
visits to ALMA are now becoming good opportunities toprovide many people live experience of the workplace of ALMA
researchers.

5. International Collaboration (committees,etc.)
Two agreements concerning the operations and developmentof ALMA were concluded between the National Institutesof Natural Sciences (NINS) and Academia Sinica in Taiwan(AS) on July 21, 2015, and between the National Astronomical
Observatory of Japan (NAOJ) and Academia Sinica Institute of
Astronomy and Astrophysics in Taiwan (ASIAA) on July 27,
2015 respectively. On December 15, 2015, representatives of the
National Institutes of Natural Sciences (NINS), the European
Southern Observatory (ESO) and the U.S. National Science
Foundation (NSF) gathered in Tokyo and signed a trilateralagreement concerning the operations of ALMA.
Since ALMA is an international collaboration project,meetings are held frequently by various committees. In FY
2015, the ALMA Board met face-to-face once, 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. In
addition, face-to-face meetings and teleconferences have been
held on a quarterly basis among the East-Asia ALMA Science
Advisory Committee (EASAC). Each working group holds
meetings and teleconferences more frequently to maintain close
communication in implementing their tasks in the international
project.

6. Workshops and Town Meetings• July 28 to 30, 2015 NAOJ Nobeyama Radio Observatory(NRO)
NRO-ALMA Science/Development Workshop 2015
• October 20 to 22, 2015 NAOJ Mitaka
ALMA/45-m/ASTE/Mopra Users Meeting• December 8 to 11, 2015 I-site Nanba
International Workshop “EA ALMA Science Workshop”• March 9, 2016 Ehime University
ALMA Cycle 4 Town Meeting• March 22 to 23, 2016 Kagoshima University
ALMA Cycle 4 Town Meeting• March 25, 2016 Kyoto University
ALMA Cycle 4 Town Meeting• April 4, 2016 NAOJ Mitaka
ALMA Cycle 4 Town Meeting7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research including
Industry –University Collaboration Expenses• Daisuke Iono: Inamori Grant Program by the Inamori
Foundation• Satoru Iguchi: Grant for Japan-related Research Projects by the
Sumitomo Foundation

8. Research Staff Changes(1) Hired• Kana Matsui: specially appointed research staff• Fumi Egusa: specially appointed research staff• Tatsuya Takekoshi: specially appointed research staff(2) Departed or transferred• Rie Miura: specially appointed research staff, hired as a
specially appointed assistant professor at NAOJ Chile
Observatory• Junko Ueda: specially appointed research staff, transferred to
the Harvard-Smithsonian Center for Astrophysics as a postdoctoral fellow• Yasutaka Kurono: specially appointed research staff

9. Main Visitors• April 23, 2015
Mr. Naoto Nikai Ambassador of Japan to Chile, visited the
ALMA Operations Support Facility (OSF) and the Array
Operations Site (AOS)• May 6, 2015
A group of researchers from universities in Taiwan visited the
OSF and AOS• May 8, 2015
Mr. Kosaburo Nishime, State Minister for Internal Affairs andCommunications (MIC) and his party; Dr. Fumihiko Tomita,
Vice President of the National Institute of Information andCommunications Technology (NICT), Dr. Shinro Mashiko,Vice President of NICT, and Mr. Pedro Huichalaf, Vice
Minister (Undersecretary) of Telecommunications, visited the
OSF and AOS• October 16 to 18, 2015
Dr. Akihiro Kubota, Professor at Tama Art University visited
the OSF and AOS

Other than 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 ESO. Therefore, having ASTE
operated by Japan will be a big advantage in strengthening
ALMA proposals and in implementing our strategies for further
extending the capabilities of observing equipment. Looking to
the future, ASTE is also important since it provides opportunities
for nurturing young researchers who will play key roles in theequipment development for the next generation. In the near
future, ASTE will be incorporated into the open-use program
to have organic collaboration with the Nobeyama 45-m Radio
Telescope.
Three public calls were made in FY 2015 for open-use
observation proposals: the first call (2015a) for spectroscopic
observations in 345 and 460 GHz bands was from June to
September, the second call (2015b) and an additional call forspectroscopic observations only in the 345 GHz band (2015c)
from October to December. To render support for researchers
contributing to enhancing the observational performance of
ASTE, the Guaranteed Time Observation (GTO) scheme has
been offered since FY 2013. This allows them exclusively tomake proposals for the GTO slots. A total of 53 proposals foropen-use observations and GTO slots had been made including
25 for open use and one for GTO in the first call; 12 for open
use in the second call; and 15 for open use in the additional call.
These proposals were reviewed by the NAOJ Chile Observatory
program subcommittee and 41 proposals were subsequently
adopted, including 22 for open use and one for GTO in thefirst call; 11 for open use in the second call; and seven in the
additional call. Open-use observations were carried out fromthe ASTE Mitaka operation room, other universities or research
institutes between June 8 and December 18, 2015.

10. Progress of ASTE Telescope
The ASTE telescope has been operated to promote fullfledged submillimeter astronomical research in the southernhemisphere and to develop/verify observational equipment
and methods. With the ALMA telescope entering its operation
phase in FY 2012, ASTE will be engaged mainly to provide
observational evidence for strengthening ALMA observation
proposals and to pursue development for enhancing ALMA’s
future performance.

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7. Center for Computational Astrophysics
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 the special-purpose computers for gravitational manybody problems; carrying out research and development ofcomputational astrophysics; and performing astronomical
research with simulations. The main supercomputer of thepresent system, ATERUI (Cray XC30), has a theoretical peak
performance of 1 Pflops, which makes it the world's fastest
supercomputer for astronomy. The Center also continued
operation of other computers such as GRAPE-DR and GRAPE-9
that are dedicated for gravitational many-body problems, inaddition to general-purpose servers. Efforts in visualizing
astronomical data also continue.

2. Open Use(1) Computer Systems
This year marked the third year of the upgraded astronomical
simulation system, which includes the open-use supercomputer
Cray XC30. The main supercomputer installed and underoperation at Mizusawa VLBI Observatory had all of its CPUs
upgraded last year, and its theoretical peak performance is now
as high as 1 Pflops. 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 GRAPEs; PC cluster
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, to encourage
effective open use of the GRAPE system, the Center undertook
development, improvement, and maintenance of both hardware
and software for the system this year. Major events of this year
were the end of GRAPE-7 operations and the official operationof GRAPE-9. This system offers a roughly 10-fold performance
improvement over GRAPE-7.
Computational resources are allocated from the XC30,
GRAPEs, and smaller computational PC cluster in accordancewith a formal review process. The statistics of applications andapprovals for this year are listed below. Our Center conducteda survey this year on the number of peer-reviewed papers
published in English in FY 2014 on studies that involved the
project's open-use computers. It turned out that 75 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,for providing users with information and transmitting various

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application forms as necessary. The regular CfCA News is anadditional channel of information dissemination. The Center
leverages this newsletter to inform people of all useful andnecessary information regarding the computer system. A subsidy
system for publishing and advertising is continuing this year for
research papers whose major results were obtained by using theCenter's computers. No paper was accepted in FY 2014 forpayout in FY 2015, while four papers were accepted in FY 2015
for payout in the same year at approximately 500,000 JPY.
□ Statistics on the Cray XC30
Operating hours- Annual operating hours: 8561.0- Annual core operating ratio: 87.13 %Users- Category S: 1 adopted in the first term, 0 in the second term;
total 1- Category A: 13 adopted at the beginning of the year, 2 in thesecond term; total 15- Category B: 70 adopted at the beginning of the year, 15 in thesecond term; total 85- Category MD: 15 adopted at the beginning of the year, 3 in thesecond term; total 18- Category Trial: 45, year total- Category I: 0, year total□ Statistics on the GRAPE system
Users- Category A: 3 adopted at the beginning of the year, 0 in thesecond term; total 3- Category B: 6 adopted at the beginning of the year, 0 in thesecond term; total 6- Category Trial: 0, year total□ Statistics on PC cluster
Operating hours- Annual operating hours: 7764.7- Annual job operating ratio: 73.3 %Total users: 37, year total(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. Note that in FY 2015, the CfCA Users
Meeting was held at Mizusawa VLBI Observatory, Iwate.
□ Cray XC30 workshop for intermediate users: January 15,
2016, 4 attendees□ N-body simulation Winter School: January 20-22, 2016, 16
attendees□ Users meeting: January 28-29, 2016, 63 attendees

3. PR Activities
CfCA took part in the special open house of Mizusawa
Campus, Iwate Galaxy Festival 2015, held on August 22,
2015. About 150 visitors attended the ATERUI guided tours
and experienced a close-up look at the facility. Dr. Tomoaki
Ishiyama, Associate Professor at Chiba University and oneof the users of ATERUI, was invited to this event as a special
lecturer and talked about the latest results of his researchobtained through ATERUI's simulations. At the Mitaka open
house held on October 24, 2015, CfCA made the computer room
accessible to the public and introduced simulation astronomy
with GRAPE and the PC cluster. A live broadcast was also
arranged by connecting the supercomputer operation room in
Mizusawa Campus to Mitaka Campus to introduce ATERUI
to those visiting Mitaka. In addition to the open house, CfCA
has accepted two groups of high school students to tour thecomputer room in Mitaka Campus. Moreover, CfCA ran a boothat the 19th NINS Symposium "From the Universe to Brains"Big Bang" of the Natural Science Researches" held at Nagoya
University on September 20, 2015 and introduced research
results from simulation astronomy calculated by the CfCA
system.
In FY 2015, two press releases were issued from CfCA:“The World’s Largest Scale Dark Matter Simulation fromthe Beginning of the Universe to the Present Performed bySupercomputers” (May 1, 2015, Tomoaki Ishiyama, Associate
Professor at Chiba University) and “Origin of Saturn’s F Ringand Its Shepherd Satellites Revealed” (August 18, 2015, Ryuki
Hyodo, Graduate Student at Kobe University). In addition, thepress release from the NAOJ Hinode Science Center, “Hinode,
IRIS, and ATERUI Cooperate on 70 year old Solar Mystery,
Magnetically driven resonance helps heat the Sun's atmosphere!”(August 24th, 2015), included a result of calculations by
ATERUI (Dr. Patrick Antolin, NAOJ). A Twitter account @CfCA_NAOJ and YouTube channel have been operated toprovide information about CfCA.

4. 4D2U ProjectIn FY 2015, the 4D2U project continued to develop andprovide movie contents and software. A movie about simulations
titled “Formation and Evolution of Dark Matter Halos (II.
Formation of the Large-Scale Structure of the Universe) ver.2”
was released on the 4D2U website in May 2015. Distributionof the dome master format data was also started. Other movies,“Giant Impact of protoplanets”, “Dynamics of Saturn's Ring
(II. Propeller Structure)”, and “Formation of plametesimals”
have been developed. Updated versions of the four-dimensional
digital universe viewer, “Mitaka,” were released in June 2015(ver.1.2.4), July 2015 (ver.1.2.5), November 2015 (ver.1.3.0)

and March 2016 (ver.1.3.1). These versions of Mitaka included
the new functions, e.g. displaying probes like New Horizonsand Hayabusa2, multilingual displays, and depiction of solar
and lunar eclipses. On February 9, 2016, the 4D2U Project put
out a press release about the multilingualization of Mitaka. The
imaging speed of Mitaka was made faster and faster with every
update.
On April 2, 2015, the 4D2U Project and Public Relations
Center (PRC) held a press tour of the renewed 4D2U Dome
Theater. A total of 26 of media affiliates from 22 companies
attended and various news outlets picked up the renewed
theater as news. In cooperation with PRC, we enhanced English
contents, such as the English websites of 4D2U and Mitaka,
the English manual of Mitaka, English instructions for 4D2U
movies, and terms of use. We started to accept applications forusage of 4D2U contents in English in October 2015. The 4D2U
Project supported and provided content for exhibitions held inmuseums and galleries, including “Moon + Sun Exhibition”(Konica Minolta Plaza, Apr. 22 - May 8, 2015), “The Feeling of
the Four-Dimensional Universe” (Ehime University Museum,May 20 - Jul. 27, 2015) and “Forms of the state-of-the-art
Network” (Chiba Museum of Science and Industry, Oct. 17 Dec. 6, 2015). The dome master data of the latest movie contents“Formation and Evolution of Dark Matter Halos (II. Formationof the Large-Scale Structure of the Universe) ver.2”, “Giant
Impact of Protoplanets,” and “Dynamics of Saturn's Ring (II.
Propeller Structure)” were provided for a planetarium program“Cyber Universe Ver.2” screened at Katsushika City Museum(Oct. 6 - Dec. 27, 2015). In addition, Mitaka and some movie
contents were used in the 5 minute TV program “Planet Kanko(Site seeing) Taxi” (total 5 stories, produced by Office Raft)broadcast on NHK. Moreover, 4D2U contents were provided
for TV programs, planetarium programs, lecture presentations,books, and so on. In FY 2015, the 4D2U Project gave Mitaka(Standard version and Head Mounted Display version)
demonstrations at the open houses of Mizusawa and Mitaka
campuses and the 19th NINS Symposium “From the Universe
to Brains “Big Bang” of the Natural Science Researches.” Many
visitors enjoyed Mitaka outside of the 4D2U Dome Theater.
A Twitter account @4d2u and YouTube Channel have been
operated to provide information about 4D2U.

5. External Activities(1) Joint Institute for Computational Fundamental Science
The Joint Institute for Computational Fundamental Science(JICFuS) is an inter-organizational institute establishedin February 2009 as a collaboration base between threeorganizations: 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. The CfCA
forms the core of NAOJ’s contribution to the JICFuS. In
particular, the institute engages primarily in computer-aided
theoretical research into fundamental physics in elementary
particle physics, nuclear physics, and astrophysics. The scientific

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goal 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 abilities as a single organization, a major
feature of the institute is the cooperation of its three member
organizations and their communities to provide considerate
and rigorous support to present and future researchers. Anotherimportant mission of the institute is to provide researchers
around Japan with advice regarding efficient supercomputeruse and the development of novel high-performance computing
algorithms to meet research goals from the perspective ofcomputer specialists. In addition in FY 2014, JICFuS was
adopted as one of the “Research and Development, Application
Development of scientific/social issues that require particularattention by the use of a Post-K computer.” The program started
this year.
In order to implement research plans, Hiroyuki Takahashi
was engaged as a project assistant professor, and Tomohisa
Kawashima was engaged as a project researcher. Takahashi
developed a new plasma simulation code to solve basic equationsof general relativistic radiation magnetohydrodynamics (MHD).
By performing global simulations of black hole accretion disks,
he revealed that jet power and gas temperature increase via
the extraction of the rotational energy of the black hole. He
also developed a radiation-MHD code by which the radiationtransport is more exactly solved. Kawashima developed aradiation transfer code in curved space-time. In addition, he
performed numerical simulations of gas accretion onto neutronstars polar regions, since some of the candidates thought to be
black holes have been identified as neutron stars instead. As aresult, he revealed that the observed large luminosities can be
reproduced even in the neutron star accretion flows.
Representing the CfCA, Professor Kohji Tomisaka andAssistant Professors Ken Ohsuga and Tsuyoshi Inoue of NAOJ
participate in bimonthly JICFuS steering committee meetings toengage in deliberations on spurring computational science-based
developments in astrophysics research through discussions
with other committee members who specialize in nuclear andelementary particle physics.
(2) HPCI Consortium
As a participant in the government-led High-Performance
Computing Infrastructure (HPCI) project since its planningstage in FY 2010, the Center has engaged in the promotion of
the HPC research field in Japan, centering on the use of thenational “K” supercomputer. Note that although the Centeris involved with the JICFuS-led HPCI Strategic Program
Field 5 as well as Priority Issue 9 to be tackled using a Post-K
computer as mentioned in (1), the activities in the HPCI
consortium are basically independent from them. The HPCI
consortium is an incorporated association established in April
2012, and the Center is currently an associate member thatis able to express views, obtain information, and observe
overall trends in the planning, although we lack voting rights
as well as the obligation to pay membership fees. Continuingfrom last year, a number of conferences and WGs have been

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held where participants discussed a next-generation national
supercomputing framework to follow the “K.” As of this year,
the post-K project has officially started with some budget
from the Ministry of Education, Culture, Sports, Science, andTechnology (MEXT). The concrete details of its operation
are being disused actively. Now the detailed discussions as to
how we fully exploit the resources of the post-K system havebegun in relevant communities and organizations. The Post-K
generation equipment is scheduled to commence operation
after FY 2019. In principle, therefore, it is possible for NAOJ
to play a central role in the post-K generation HPCI throughparticipation in this discourse.

6. Contract Staff Transfers
The following staff members were hired on a contract basis in
this FY:(Research experts) n/a(Postdoctoral fellows) Yuta Asahina(Research associates) n/a
The following contract staff members departed in this FY:(Research experts) Yayoi Narazaki(Postdoctoral fellows) Shun Furusawa, Tomohisa Kawashima(Research associates) Yukihiko Hasegawa, Yuji Matsumoto

8. Hinode Science Center
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). NAOJ implemented this satellite
project under a joint research agreement with ISAS/JAXA. A
major theme of the scientific goals of the Hinode mission is toshed light on the coronal heating mechanism through a more
multifaceted understanding of magnetohydrodynamic (MHD)
phenomena occurring in the solar atmosphere. The satellite has
actually made a lot of discoveries related to these subjects.
Hinode is equipped with three telescopes including thesolar optical telescope (SOT), the X-ray telescope (XRT), andthe extreme ultraviolet (EUV) imaging spectrometer (EIS). It
engages in simultaneous observations of the detailed magnetic
fields and velocity fields on the surface of the photosphere andthe brightness and velocity fields from the chromosphere to thecorona. The onboard telescopes were developed as part of awide-ranging international collaboration with assistance from
ISAS/JAXA. SOT was developed mainly by NAOJ, and the
focal plane package (FPP) was developed by the US National
Aeronautics and Space Administration (NASA) and Lockheed
Martin.
With regard to the XRT, NASA and the Smithsonian
Astrophysical Observatory (SAO) are responsible for the
optics system and frame, and Japan (ISAS/JAXA, NAOJ)
is responsible for the focal plane camera. EIS is the resultof an even broader international cooperation. The structureand electrical system were developed by the UK Science andTechnology Facilities Council (STFC) and University College
London; the optics system was developed by NASA and theNaval Research Laboratory (NRL); and the University of Osloin Norway assisted with the terrestrial testing equipment and
the Quick Look system. NAOJ actively participated in thedevelopment of the EIS/satellite interface, satellite integration
testing, and launch experiments. After a successful launch,
NAOJ has continued its active involvement by acting as themain institution for collecting and analyzing data acquired by
the satellite.
The Hinode Science Working Group (SWG), composedof representatives from the international team, offers support
in scientific operation and data analysis. Together with two
members from the European Space Agency (ESA), the WG has
a total of 15 members three from the Hinode Science Center(HSC) including Sakurai, Chairman/project scientist; Suematsu,
SOT; and Watanabe, EIS. Science Schedule Coordinators havebeen organized to leverage the open-use observation system.
Many of the Japanese coordinators are NAOJ staff members,
including Watanabe (Chairman/EIS) and Sekii (SOT).
FY 2015 marks the ninth year since the satellite's launch.
The 2015 NASA Senior Review results for Hinode were ranked
in the top 3 among 15 missions under the control of NASA’s
Heliophysics Division, which assured adequate NASA funding
for the near future. ESA will continue to support Hinode withthe current level of funding at least until the end of FY 2017.
The funding from STFC was also renewed for Hinode until
March 2019. The request for the Hinode mission extension will
also be submitted to ISAS/JAXA in FY 2016.

1. The Hinode Satellite: Onboard Telescopes
and Scientific Operation
The SOT is a telescope used for obtaining photosphericmagnetic field vectors via polarimetric observations ofabsorption lines. It has the capacity for continuous observation
at the diffraction limit with a spatial resolution of 0.2–0.3 arcsec
and an effective aperture of 50 cm without atmospheric seeing.
The focal plane package consists of three types of optics systems
and imaging functions for maintaining the desired performancelevel. Operational modifications have enabled longterm
maintenance of a sound field of view even in the narrow band
filter imager system, in which image degradation was initiallydetected in part of the field of view. The power supply for thefiltergraph (FG) camera failed on February 25, 2016. The FG
system has been powered off, and stopped operation sincethen. Currently the cause of the trouble and the possibility forrecovery are under investigation.
The XRT has the capacity of capturing the solar coronalplasma via soft X-rays. The telescope has inherited the grazing
incidence optics system and has improved in spatial resolution.
Its wavelength characteristics have been improved to allow
for observation of the solar coronal plasma over a broader
temperature range. Resolution is close to 1 arcsec. Calibration is
now possible for temporal variations in spectral characteristics
due to surface contamination on the detector, and the telescopeis available for analysis via its spectral characteristics.
The EIS obtains temperatures, densities, and velocitiesof the chromosphere, transition region, and coronal plasma
thorough the spectroscopic observation of EUV emission lines.
The instrument allows for spectroscopy and imaging at multiple
wavelengths via the operation of slits and slots. Its purpose is
to investigate the manner in which energy is conveyed from its
generation in the photosphere until its dissipation in the corona
by observing from the chromosphere (located between thephotosphere and the corona) through the transition region to thecorona.
A mission data processor (MDP) was installed to manage
observations and to acquire data via the three telescopes.
Coordinated observations using the three telescopes, in which
the MDP plays a crucial oversight role, are vital to achieve thescientific goals of the Hinode satellite. Particularly for the XRT,
functions such as the exposure time adjustment, the regionof interest (ROI) selection, and the flare detection logic arehandled by the MDP, which requires close coordination with thetelescopes.
Data from the Hinode satellite is primarily downlinked at
the Kagoshima station (USC) and at Norway’s Svalsat station

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through collaboration with ESA, allowing for data acquisition
for every orbit. Scientific operation was again performed in FY
2015 via S-band data reception. The S-band reception frequency
was increased with help from ESA and NASA, allowing forcontinuation of regular, stable scientific operation.
Obtained data is collected at ISAS/JAXA, converted into the
FITS format, and provided to researchers around the world in
the form of Level-0 data, which is close to raw data. HSC staff
members and students took part in satellite operation for a totalof 200 days in FY 2015, 119 days of which were for contracted
work. Moreover, the contribution rates to the scientific operationof the HSC were 27.3 % (domestic) and 17.2 % (overall).
Instantaneous publication of all data acquired by Hinode began
on May 27, 2007, with stable continuation, implemented by
HSC.
Calls for Hinode Operation Plans (HOP), which encourage
proposals for open-use observations together with othersatellites and terrestrial observational equipment, promotejoint observations among solar researchers worldwide. As of
March 2016, a total of 302 applications have been accepted.
In particular, core HOP proposals made by members of thescientific instrument team became refined over multiple
implementations, and systematic observations have yielded
extensive results that can help develop studies on solar activity
cycles.

2. Hinode Satellite Data Analysis
NAOJ HSC aims to construct an analytical environment anddatabase for scientific analysis of data from the Hinode satellite
in a central organization, allowing it to function as a research
center. The goals are to maximize the scientific outputs gained
from the Hinode satellite by offering researchers in Japan andother countries a data analysis environment; and to promoterigorous collaborative research between researchers in Japanand abroad by facilitating access to Hinode observational data
thorugh distribution of the analyzed data and construction of adata search system.
As part of its educational and public outreach (E/PO)
activities, HSC also uses the latest observational data to raise
public awareness of the relationship between solar researchand everyday life so that the importance of solar research isappreciated. The Center has offered press releases, web releases,
and media appearances; responded to interview requests fromtelevision programs and journals; and provided materials for
publicizing scientific results.
In FY 2015, HSC staff members and students published 9
peer-reviewed papers related to Hinode (among the total of 20
papers), bringing the total to 250 papers by the end of March2016. Cumulatively, a total of 887 peer-reviewed papers havebeen published on Hinode-related topics. Publications of papers
in this category continue at a pace of nearly 100 papers per year
9 1/2 years after the satellite’s launch. Intensified collaborative
research with newly launched missions and advanced groundbased facilities near the solar activity maximum will further
enhance the number of research papers for solar activity.

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3. Other Activities
In FY 2015, two postdoctoral fellows were engaged as
members of HSC, and both of them were project assistantprofessors. One fellow was hired as a ministry office college
lecturer in September. The contract term of the other fellow
expired at the end of March 2016, but he had an offer to becomea researcher at the University of St. Andrews in the United
Kingdom.
The Hinode Science meetings for Japanese and international
researchers have been held regularly to advance reserarch infields related to solar physics thorugh use of the Hinode satellite.
The ninth Hinode Science meeting took place during September
14 – 18, 2015, in Queen’s University, Belfast (Northern Ireland,
UK).
In addition to the aforementioned activities, HSC researchand educational staff members have presented scientificobservation results at numerous symposia on solar-related
subjects either by invitation or by active participation. HSC has
also invited international researchers to engage in collaborative
research. The following researchers have visited the Center fromoverseas on a long-term stay of at least one month:
Name

Organization (Country)

Cheung, Mark C. M.

Lockeed Martin Solar andAstrophysical Laboratory (USA)Gizon, Lorent

Max-Planck Institut fürSonnensystem (Germany)

Table 1. Long-term Visitors.

9. Gravitational Wave Project Office2015 has been marked by the first detection of a gravitational
wave from the coalescence and merger of binary black
holes made by LIGO in the United States. This observation,
announced by the LIGO and Virgo collaborations last February,
demonstrates that gravitational wave observatories able todetect the coalescence of binary black holes within 1 Gpc cancontribute to the start of gravitational wave astronomy. In themeantime, the Gravitational Wave Project Office (GWPO) of
NAOJ has pursued the construction of KAGRA in Kamioka.
In particular, the office contributed to the installation of initial
KAGRA and its operation. To facilitate this activity, a branch of
the office was opened at Kamioka. In parallel, the preparationof the components for baseline KAGRA (bKAGRA) continued
with the goal of starting its operation in 2018.

1. Development of KAGRA
KAGRA is an interferometric gravitational wave detector
being constructed at an underground site in Kamioka, Gifuprefecture. In addition to the quiet underground environment,
the use of cryogenic mirrors to reduce the thermal noise makes
KAGRA a unique instrument among other large gravitational
wave detectors. At the end of FY 2015, KAGRA successfully
conducted the first test operation of the 3 km interferometer at

Figure 1: Happy faces after the installation of the PR3 suspension system
into a vacuum chamber.

room temperature with a simplified interferometer configuration
called iKAGRA. The test run provided us with opportunities totest some of the key facility issues, such as the alignment of the
3 km beam ducts, and to gain important insights into the upgradeof the interferometer to the final configuration.
NAOJ is contributing to several aspects of KAGRA. The
largest responsibilities are development and installation ofultra-high performance vibration isolation systems for theinterferometer mirrors. Other technical contributions include
the auxiliary optics, mirror characterization facility, and thedesign of the optical configuration and the control strategy forthe main interferometer. NAOJ is also contributing to the project
management through the activities of the executive office, thesystem engineering office, the committee for publication control,
the publication relation committee, the safety committee, andthe KAGRA Scientific Congress (KSC) board.
(1) Vibration Isolation
The vibration isolation system (VIS) is composed of thesuspensions required to isolate all the interferometer components
from ground vibrations. Four different types of suspensions
having different complexities to meet the varied isolation
requirements of different components have been developed at
NAOJ for this purpose. In FY 2015, one of the large suspensions
was installed into a KAGRA vacuum chamber to support a
mirror called PR3. The suspension worked successfully during
the iKAGRA test operation. Based on the experience gained
from the installation and operation of the PR3 suspension,
we are preparing other large suspensions for the upgradedinterferometer (bKAGRA). In addition to this, a total of fivesmall suspensions were prepared and used for the mode cleaner
mirrors and the end test masses of iKAGRA.
(2) Auxiliary Optics
The auxiliary optics subsystem consists of several kindsof optical components including optical baffles, beam dumps,
beam reducing telescopes (BRT), high quality viewports,
cameras to monitor the beam spots on the mirrors, and theoptical local sensors (optical levers) for the mirrors. Many viewports were installed in FY 2015 and used in iKAGRA. Seven
optical levers were installed and reliably provided the alignment
information of the mirrors during the operation of iKAGRA.
Ten digital video cameras were also installed to provide realtime, on-demand, pictures of the interferometer beams at various
locations.
Tests of materials for high quality optical baffles and highpower beam dumps continued using scatterometers developedby our group. Some of the additional large baffles necessary
for bKAGRA were designed and delivered. Optical parts of thebeam reducing telescopes (BRTs) for bKAGRA were purchased
and the design work of the vibration isolation stage for them has
progressed.

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081

(3) Mirror Characterization
The optical absorption measurement system delivered lastyear was adjusted and is fully operational now. Validation of
the calibration and simulations to separate the absorptions on
the surface and the absorptions in the bulk of a sample were
performed. We measured a small sample of a candidate sapphire
crystal for KAGRA mirrors and found a very low absorption
value. Preparation for the measurement of large size samples isongoing.
(4) iKAGRA Interferometer Operation
The KAGRA main interferometer commissioning team,including GWPO members, successfully aligned and locked theiKAGRA interferometer in a relatively short time (3 weeks). The
calibration of the interferometer was also performed by GWPO
members. GWPO members took shifts at the Kamioka site tooperate the interferometer during the test run.

2. R&D(1) R&D for Upgrades of KAGRA
While building bKAGRA, the GWPO pursues research anddevelopment to investigate and prepare for future upgrades to
KAGRA. In this context, the TAMA infrastructure is being used
to develop frequency dependent squeezing, one of the mostpromising solutions to improve the sensitivity of detectors like
KAGRA that are limited by quantum noise. To this purpose,a 300-m long high-finesse cavity is being built. Thanks to thisexperiment we established collaborations and received students
from abroad. The absorption measurement bench developed
to characterize the KAGRA mirror is also used to study theperformances of crystalline coatings, a possible solution to
reduce coating thermal noise. Thermal noise investigations arealso the objective of another experiment now starting at ATC
and aiming at the direct measurement of mirror thermal noiseat cryogenic temperature. Finally, crackling noise is being
investigated in collaboration with ICRR.
(2) DECIGOThe DECIGO group continued discussion on the designof DECIGO satellites as well as its precursor, Pre-DECIGO.
After the first detection of gravitational waves, we started toreconsider the sensitivity of Pre-DECIGO and its achievable
angular resolution for the signals based on its orbit from theviewpoint of science.

3. Education
In FY 2015 the office includes three PhD students and one
master’s student. In addition, we received an undergraduate
student from Toyama University under the SOKENDAI summer
students program. We also received a visit by a master’s
student from Beijing Normal University for 1.5 months and a
PhD student from CNRS/APC (France) for a duration of threemonths.

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4. Outreach
KAGRA held an inauguration ceremony for the completionof the 1st phase facility in November. GWPO members
contributed to the organization and the operation of thisceremony. Some GWPO members were featured in broadcast
programs on NHK international TV and NHK radio. The
NAOJ annual lecture was organized as part of the lecture seriescelebrating 100 years of general relativity. A GWPO member
gave a talk at the event. GWPO members also gave public
lectures at the NINS president’s press conference, Tamarokuto
Science Center, and the National Science Museum. The
office contributed to the NAOJ open house days in Octoberby showing the TAMA facility and the ATC clean room forassembling KAGRA components to the public. TAMA300
continued to serve as one of the featured facilities for visitors
to Mitaka Campus by accepting many of them throughout theyear. GWPO Kamioka branch members took care of some of thevisitors to the KAGRA site.

5. International Collaboration and Visitors
GWPO is a member of the KAGRA collaboration, ascientific collaboration which includes also members fromabroad. Apart from KAGRA, GWPO has collaborations with
CNRS/APC (France), Beijing Normal University (BNU, China),
the University of Hamburg (Germany), and CNRS/LMA (France)in the context of R&D for future upgrades to KAGRA. In thisframework we received visits by Dr. Barsuglia from CNRS andby Prof. Zhu from BNU. We also had several exchanges with
the Virgo collaboration, with which one of the office members isaffiliated. We received a visit by Dr. Vocca from the Universityof Perugia (Italy) who then joined the KAGRA collaboration.
As usual we received several visitors at TAMA including Dr.
Nguyen Quynh Lan from Hanoi (Vietnam), Dr. Gilles Hammondfrom the University of Glasgow (Scotland), the Japan Societyof Mechanical Engineering, and a group of students from an
educational project in Romania.

6. Publications, Presentations and Workshops
Organization
The members of the office have authored 17 peer reviewed
publications, including the paper reporting the “Observationof a binary black hole merger” which received a lot of interest
both in the scientific community and in the public. Moreover 9
presentations were given by the office members at international
conferences. On the occasion of the 100th anniversary of theestablishment of general relativity, we participated in organizing
a series of public lectures across Japan.

7. Acquisition of External Funds
GWPO did not receive external funds apart from thoserelated to 8 grants allocated by JSPS.

8. Staff
There were no transfers of non-regular staff members. One
administrative supporter and one research engineer retired andwere replaced this year. One JSPS postdoc joined the Project inApril 2015 to work on KAGRA. Overall in FY 2015 the Project
included 2 faculty members, 8 research staff, 4 engineers, 3administrative staff, and 4 graduate students.

II Status Reports of Research Activities08310. TMT-J Project Office
The TMT Project is a project to build an extremely large
30-meter telescope under the collaboration of five partnercountries including Japan, the United States of America, Canada,
China, and India. Heading the project for NAOJ is the TMT-J
Project Office. In 2014, an agreement was executed between
the participating organizations, TMT International Observatory
was founded to assume the construction and operation of theobservatory, and construction commenced. Japan is responsible
for the fabrication of the telescope primary mirror, the design
and fabrication of the telescope structure as well performing its
onsite installation and adjustment, and the design and productionof science instruments.
Although the commencement of full-fledged construction
was planned for Fiscal Year 2015, construction was halted due
to a protest movement against construction. Additionally, theSupreme Court of Hawai`i ruled in favor of a claim that cited aproblem in the approval process of the land use permit for theMaunakea Conservation District and remanded it in December
2015. Although this has caused delays to construction onsite,mass production of the telescope primary mirror, detailed designof the telescope structure, and the design and development ofscience instruments have proceeded according to plan in Japanfor Fiscal Year 2015.
The TMT-J Project Office currently has 2 Professors, 4
Associate Professors, 1 Chief Research Engineer, 1 Specially
Appointed Associate Professor, 3 Specially Appointed Senior
Specialists, 1 URA employee, 2 Research Experts, 2 Research
Supporters, 2 Specially Appointed Research Staff Members,
2 Administrative Supporters, and 1 RCUH employee in fulltime positions. In addition, 1 Professor, 5 Associate Professors,
2 Assistant Professors, and 1 Research Engineer from theAdvanced Technology Center, Subaru Telescope, and the NAOJ
Chili Observatory (ALMA) 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), National Astronomical
Observatories of Chinese Academy of Sciences, Universityof California, California Institute of Technology, Departmentof Science and Technology of India, and National ResearchCouncil of Canada. The Association of Universities for Researchin Astronomy (AURA, USA) participating as an Associate
Member is taking steps for the USA to eventually participate as
an official participant. TMT International Observatory, operated
according to deliberations and decisions made in quarterly084

II Status Reports of Research Activities

Board meetings of the TMT Board of Governors, is overseeing
the construction work performed in each country as well as
developing the onsite infrastructure. The board meetings wereattended by 3 representatives from Japan, one of whom served
as the Vice Chairperson of the Board.
Although full-fledged construction at the summit of
Maunakea was slated to begin in April 2015, construction
was forced to halt due to building momentum in the protest
movement at Maunakea. Efforts were made to resumeconstruction with the aid of the University of Hawai`i, but in
December the Supreme Court of Hawai`i ruled the land use
permission approval process for the Maunakea Conservation
District, the site of planned construction, to be flawed,
consequently invalidating the Conservation District Use Permit.
The permit was initially approved by the State of Hawai`i in
April 2013, but a claim was filed regarding the permit review
process. Although the ruling did not find fault in the content
of the permit itself, because a redo of the review process isnecessary, a new review process will be commenced by the Stateof Hawai`i sometime after February 2016, the month in which
the ruling was officially remanded.
In Japan, the construction of TMT was approved as oneof the new projects for the Promotion of Large Scientific
Research Projects in Fiscal Year 2013. Fabrication of the
primary mirror and design of the telescope structure have been
performed since then. In Fiscal Year 2015, along with making
progress in the fabrication of the primary mirror, detailed
design of the telescope structure, and development of science
instruments (explained below), payments were initiated as partof Japan’s contribution to cover operating expenses for the TMTInternational Observatory and contribute to the progress of thisinternational-scale construction.

2. Japan’s Progress on Its Work Share – theTelescope Structure and Fabrication of thePrimary Mirror
For the construction of TMT, Japan is responsible for thedesign/fabrication of the telescope structure and a portion of
the fabrication of the primary mirror and science instruments as
according to the executed agreements. Progress made in Fiscal
Year 2015 is described below.
(1) Fabrication of the mirror segments of the primary mirror
The TMT primary mirror is comprised of 492 mirrors
segments. Including replacements, a total of 574 mirror segments
must be fabricated. The processes required in the fabrication of
mirror segments are: fabrication of the mirror blanks, spherical
grinding of the front and back surfaces, polishing of the backsurface, aspherical surface grinding/polishing, machining andmounting them onto a support assembly. These processes arefollowed by the final finish and coating process before a mirror
segment is installed on the telescope. Of these processes, theplan calls for Japan to fabricate the mirror blanks and to performspherical grinding on all 574 segment mirrors. In Fiscal Year
2015, 65 mirror blanks were fabricated and spherical grinding
was performed on 63. The plan is also for Japan to perform
aspherical grinding/polishing and mounting to a support
assembly for approximately 30% of the mirror segments. In
Fiscal Year 2015, aspherical grinding was completed for 33
mirrors, and a mass production line for aspherical polishing had
begun, producing 6 polished mirrors.
(2) Design of the telescope structure and its control system
Japan is responsible for the design and production of thetelescope structure which functions as a mount for the science
instruments and optics systems, including the primary mirror,
and points them in the direction of a target astronomical object.
Work on the detailed design of the telescope structure wasinitiated in Fiscal Year 2014 using the baseline design received
in Fiscal Year 2013. The first international design review washeld in February 2015 and was followed by international reviewsof the control system and detailed design held respectively in
July 2015 and February 2016, all of which were passed.
(3) Science instruments
Japan is responsible for fabricating a portion of the first-light
instruments as part of the international collaboration.
In regards to the Infrared Imaging Spectrometer (IRIS),
Japan is responsible for fabricating its imaging component.
Work in Fiscal Year 2015 included preliminary design andperformance assessment of the optics in the imager andpreliminary design for the mechanics of the support systemof the optics. Also, in coordination with the team of IRIS
international collaborators, Japan made contributions toward
preparation of a requirements document for the overall
instrument and evaluation of the system. Vibration analysis of
the overall IRIS system in particular was spearheaded by Japan’s
development team.
For the Wide Field Optical Spectrometer (WFOS),
conceptual study is underway with Japan expected to be
responsible for the camera system. In Fiscal Year 2015,
corrections were made to the assumed effects of theheterogeneous properties of the fluorite lens on the imaging
performance as well as corrections to the optics design of thecamera system associated with the change in the layout of
WFOS.

Figure 1: Conceptual image of a constructed TMT.

Figure 2: Segment Handling System (SHS) (provided by Mitsubishi
Electric).

3. Evaluation of Scientific Research by TMT
and Public Relations Activities
Japan held a key role in the TMT scientific researchevaluation spearheaded by the Science Advisory Committee of
TMT International Observatory through continued participationin the International Science Development Teams (ISDTs)
established in 2013. In Fiscal Year 2015, a report (Thirty
Meter Telescope Detailed Science Case: 2015) was compiled
and published. The TMT Science Forum held once a year
since 2013 was held in Washington DC in June 2015 where

Figure 3: Aspherical grinding of a mirror segment of the primary mirror(provided by Canon).

the possibilities of key scientific observation programs weredebated. Preparations were made for the 2016 TMT Science
Forum expected to be held in Kyoto in May.
In Japan, continued effort is being made to reflect the

II Status Reports of Research Activities085

opinions of the community through organizations such as
the TMT-J Science Advisory Committee (JSAC). Publicchances to support TMT related science meetings were offered
for the purpose of promoting plan proposals for scientificobservation research and new science instruments utilizing
TMT. Additionally, the strategic fundamental research fund
for the purpose of elementary technology development for thedevelopment and design of next generation science instruments
continued to be made available. As a result, funding support wasawarded to 5 development plans, including those requested byuniversities.
The TMT Project, particularly Japan’s role in the project
and the status of the project itself are introduced in the TMT-J
Project Office website. Additionally, TMT Newsletters No.44
through 46 were delivered. Efforts were made in publicawareness through lectures held in various areas throughout
Japan and exhibits at the National Institutes of Natural Sciences
Symposium and Inter-University Research Institute Symposium.
Approximately 50 lectures and requested classes were held forthe public.
Contributions were also made by making an on-demand
lecturer available for the science/technology education and PR
event “Journey through the Universe” (March 2016) held in
Hawai`i where TMT is to be constructed.
Donations to the TMT project raised continually; one
corporation and approximately 1000 individuals provided
donations in 2015 (from January to December).

086

II Status Reports of Research Activities11. 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 accuracy of 1/100,000 arcsecond (10μas) in order to determine with high reliability the distances
and transverse velocities of stars within approximately 10 kpc
of the Earth in the surveyed direction. Nearly 1 million stars
can be measured with 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 scientificsatellite project, an ultra-small size project and a small size
project were implemented to progressively build up scientificresults and to accumulate the necessary technical knowledge andexpertise. 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 the astrometric information
for bright objects in nearby space. Despite its small aperture,
the satellite is capable of observational precision comparable
to the Hipparcos satellite. The combination of observational
data from Nano-JASMINE and the Hipparcos Catalogue is
expected to produce more precise data on proper motion andannual parallax. 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 2022. This satellite will engage
in observations of a limited area around the nuclear bulge andcertain specific astronomical objects. This small-sized version
has the goal of obtaining advanced scientific results at an earlystage. The mid-sized JASMINE satellite, with a main apertureof approximately 80 cm, is designed for surveying the entire
bulge and is targeted 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 observationof the bulge, which is a method suitable for observations in the
direction of the Galactic Center.

(2) Major Progress in FY 2015
1) Organization of the Office
The JASMINE Project Office is composed of five fulltime staff members, six staff members with concurrent posts,
two postdoctoral fellows, one research associate, one technicalassociate, and five graduate students. Significant contributions
were made by members of the following organizations:
Kyoto University’s Graduate School of Science; the Systems
Engineering (SE) Office, Aerospace R&D Directorate(ARD), and ISAS at JAXA; the University of Tokyo’s Schoolof Engineering; Tokyo University of Marine Science andTechnology; 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. On the other hand, we now
have the possibility that the Europena Space Agency (ESA) 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. A Japanese WG led by Ryoichi Nishi of Niigata
University continued to actively engage in investigating thescientific results to be obtained in the future by Nano-JASMINE.
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, atless than or equal to 50 μas/year in the direction of an area of

II Status Reports of Research Activities087

a few degrees from the Galactic Center within the 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 uniquein 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 theformation history of the superrmassive black hole at the Galactic
Center; the gravitational field in the Galactic Nuclear Bulge andthe activity around the Galactic Center; the orbital elements of
X-ray binary stars and the identification of the compact object
in an X-ray binary; the physics of fixed stars; star formation;planetary systems; and gravitational lensing. Such data willallow for the compilation of a more meaningful catalog whencombined with data from terrestrial observations of the lineof-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, ARD, and ISAS with a focus on thesatellite’s vital elements such as thermal structure, attitudecontrol, and orbit.
Against this background, in-house discussions andmanufacturers’ propositions, which started in 2009, continued toconsider the design of the satellite system to ascertain the target
precision in astrometric measurement as a general objective in
preparation for submitting a mission proposal to the ISAS callfor small-sized scientific satellite mission proposals. The SWG,
led by Masayuki Umemura of the University of Tsukuba andincluding volunteers from diverse fields in Japan, continued
to make scientific considerations. Other activities such asconceptual planning, design, technical testing 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 teamand 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 call for088

II Status Reports of Research Activities

small-sized scientific satellite mission proposals.

12. Extra-Solar Planet Detection Project Office (Exoplanet Project Office, EPO)
The Extra-Solar Planet Detection Project Office cooperates
with researchers interested in extra-solar planet 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.

assemble were conducted. It was then shipped to Hawai`i.
Science discussions on habitable planets around M dwarfs arealso proceeding.
(3) SCExAO (Subaru Coronagraphic Extreme Adaptive Optics)
and CHARIS IFU
EPO has been involved in the development of these nextgeneration high-contrast instrumentations being carried out at
Hawai`i and Princeton, respectively.

2. Exoplanet instrument development for
future space and ground-based telescopes andinternational 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 WFIRST

There were 38 refereed papers in English, 2 non-refereed
papers in English, 36 presentations in English, 1 refereed paperin Japanese, 8 non-refereed papers in Japanese, 2 books inJapanese, and 57 presentations in Japanese.

1. Development of the Subaru Next Generation
Exoplanet Instruments and Exoplanet
Observational Research(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. In this year, HiCIAO wasused mainly in combination with SCExAO.
(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 browndwarfs. The budget is based on JSPS Grant-in-Aid for Specially
Promoted Research FY 2010-2014 (PI: Motohide Tamura).
Fiber experiments, laser frequency comb completion, and total

Figure 1: Multiple gaps in the TW Hya disk observed in near-IR.

Figure 2: IRD spectrometer. Top cover removed.

II Status Reports of Research Activities

089

WG), a coronagraph performance test at 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. A review paper was published. Other
major results are: direct imaging discovery of a gap at 20 au in
the protoplanetary disk around TW Hya (multiple gaps); direct
imaging discovery of a unique disk around SU Aur; revealing
gapped disks around DoAr 28 and HD 169142; and discovery ofa tilted inner disk around LkCa 15.
International collaborations using HiCIAO brought thediscovery of interesting features originating from gravitational
instabilities arising from mass accretion in the disks around FU
Ori stars.
Ten graduate students are supervised for exoplanets andrelated topics. Many public talks, publication, and press releases
are made on exoplanets, disks, and other astronomical fields.

090

II Status Reports of Research Activities13. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project Office
1. Project Overview

3. Outreach/PRIn FY 2015, calibration data for the Laser Altimeter (LIDAR)
of Hayabusa2 was collected and its laser-link experiment was
carried out. Also, a conceptual design of the Ganymede Laser
Altimeter (GALA) for the Jupiter Icy Moons Explorer (JUICE)
mission was made. The Hayabusa2 asteroid explorer was
launched on December 3, 2014; initial test operations finishedin January; and Hayabusa-2 is underway to C-type asteroid,
Ryugu. Before rendezvous with Ryugu will start in the summerof 2018, the RISE Project Office collected calibration datanecessary for two major scientific goals of the laser altimeter,that is, albedo observation and dust detection. An engineeringmodel of the laser altimeter was used for this calibration. The
collected data and their evaluation were published in January in
an international journal for future use with observation results.
From October to December in FY 2015, taking advantage ofHayabusa2’s Earth swing-by, RISE Project Office members
attempted a laser-link experiment with Hayabusa2. Laser
pulses transmitted from Mt. Stromlo station in Canberra weresuccessfully received by Hayabusa2’s laser altimeter, andestablished a one-way link over 6.6 million km between aground station on the Earth and the spacecraft in interplanetary
space. This is the third successful experiment conducted beyond
the lunar orbit. For GALA, the RISE Project Office members
developed a tool to simulate the quality of laser signals startingfrom the laser oscillator, reflecting on the surface of the icy
satellite, and finally being received by the electric circuits of
the receiver system. An increase of noise in the laser signal istaken into account in the simulation. Thus this tool allows us toconstrain the instrument requirements quantitatively. At the sametime, the members studied variations of slope and roughness
at the surface of the icy satellites using the highest resolution
images in order to narrow the most ambiguous options of thesimulation.

In FY 2015, the Office members volunteered for Ihatove
Science School of Oshu City 11 times as well as Fureai
Astronomy classes 4 times.

4. Joint Research/International Collaborations
One member of the RISE Project Office served as a section
president of Asia Oceania Geosciences Society. From Russia,
a researcher of Vernadsky Institute of Geochemistry andAnalytical Chemistry visited the Office for two months for joint
research on thermo-mineralogical modeling of the lunar interior.
The RISE Project Office invited five researchers from Russia,
the U.S.A., Germany, South Korea, and China to promoteinternational partnerships.

5. Career Development
One research expert left the RISE Project Office in Marchas his term ended. To fill this vacancy, the Office opened anannouncement of a job opportunity for specially appointed
research staff. On the other hand, another specially appointed
research staff member left the Office in March and is now
employed as a lecturer at Kougakuin University.

2. Educational Activities/Internship
Seven RISE members delivered 18 lectures on a parttime basis to graduate students at the University of Aizu; andtwo RISE members served as part-time lecturers at Iwate
University for half a year each. Also at Kyoto University andKyushu University, two members served as part-time lecturers.
The Office accepted two third-year undergraduate students of
Iwate University for a week, and one fourth-year undergraduate
student from Kazan University in Russia for a 2 month-longinternship. As summer students of the Graduate University for
Advanced Studies, two third-year undergraduate students of the
University of Aizu and the University of Tokyo were accepted
for three weeks. In January, a third-year undergraduate studentof Taiwan Central University visited the Office for 3 weeks andstudied crater statistics of the Moon under the supervision of the
Office members.

II Status Reports of Research Activities091

14. Solar-C Project Office
The SOLAR-C Project Office has engaged in planning thenext solar observation satellite project, SOLAR-C, and has
executed the launch operation of a sounding-rocket experiment,
the Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP).
In addition, since the middle of Fiscal Year 2015, the Project has
started preparatory activity for proposing a re-flight program ofa German solar balloon 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 mid-2020’s.
The project is intended to investigate the solar magnetic plasma
activities that influence the space weather and space climate
around the Earth. The investigations involve the measurementof magnetic fields in the chromosphere and high-resolution
imaging/spectroscopic observations that have not beenpreviously achieved. The themes include major problems in solar
research: the heating of the chromosphere/corona, the originof solar explosive events, and the variation of solar spectral
irradiance. 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, satellite, and one of the major science
instruments, whereas the US and European space agencies andinstitutions will deal with the other major instruments throughinternational collaborations.
The main body in this project is the Next Solar Observation
Satellite Project Working Group led by Prof. Watanabe, NAOJ,
set up within the Advisory Committee for Space Science at
ISAS/JAXA; NAOJ researchers play key roles in the project
activities. The SOLAR-C Planning Office was set up at NAOJ
in FY 2008 as a sub-project in the Hinode Science Center(HSC), dedicated to the SOLAR-C project. It was promoted
to the SOLAR-C Project Office in FY 2013 as an A-project
independent from HSC, continuing the preparatory work forthe realization of the satellite project with five full-time staff
members and eleven members with concurrent positions/
postdoctoral fellows.

2. CLASP Project
The CLASP project is an observational sounding rocket
experiment aiming to detect solar magnetic fields in thechromosphere and transition region through polarization
observations of the hydrogen Lyman-alpha (H Lyα) spectrum.
Planning and basic development of the project started in FY
2009. The project involves an international research team withparticipation from Japan, the USA, and other countries. The
CLASP project entered the development stage fully in the latter
half of FY 2012 and carried out its first flight experiment in mid2015. The payload consists of a far-ultraviolet (FUV) telescope

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and a spectro-polarimeter that were prepared in Japan to conduct
polarization observations, with components contributed by
the USA (CCD cameras and control computers) and France (aspherical concave grating). In the CLASP program, an Americansounding rocket is used for the flight operation at the US White
Sands launch site.

3. Major Activity in FY 2015
The SOLAR-C proposal, which was submitted to JAXA in
February 2015, was not selected in the mission definition review
as the candidate of the 1st JAXA Strategic Middle-class Satellite
Mission. The SOLAR-C plan involves large international
contributions, but in January of the same year, a proposal aiming
to win approval for these international collaborations was not
adopted by the European Space Agency (ESA). One of the major
reasons cited in the JAXA review is that the large international
collaborations assumed in the proposal have not yet been
established. So the SOLAR-C WG is conducting the refinementof science objectives and the optimization of the mission sizefor the next opportunity. In FY 2015, the Project also studied
the feasibility and cost estimate for a large telescope of reduced
aperture and the thermal structure of the spectropolarimeter, andcarried out test production of polarimetric optical components
for performance verification.
The CLASP sounding-rocket experiment was carried out on
September 3, 2015 at the US White Sands launch site. The flight
was successful, returning the world’s first polarimetric spectraof the H Lyα lines with a high precision of 0.1%. While doing
the data analysis, the international CLASP team has started the
preparations for the 2nd flight.
After receiving notification that the JAXA review committee
for the Strategic Middle-class Satellite Mission had not adopted
the SOLAR-C proposal, the Project received an invitation froma German solar research group to participate in the German
balloon re-flight project, Sunrise-3, scheduled for around2020. A spectropolarimeter with a performance similar to the
SOLAR-C payload is to be developed. The Project aims todemonstrate the development of the state-of-the–art remotesensing instrument needed for SOLAR-C and overcome thechallenges of conducting leading-edge science observatinos
from an experiment balloon.

4. Others
Although the SOLAR-C Project Office is reimbursed by
NAOJ for its general operation and emergencies, a large partof the expenses for supporting the project preparation is fundedby other sources, including the Grant-in-Aid for Scientific
Research, JAXA’s strategic R&D fund for basic development
and experiment of onboard instruments, and research grants
from the private sector.
Prof. K. Ichimoto of Kyoto University became aconcurrently appointed professor in the Project in April 2015. T.
Bando moved to Subaru Telescope after April 2015. R. Kano got
promoted to associated professor in October. Prof. T. Sakurai
retired at the end of FY 2015. K. Watanabe, who started as aproject research fellow in April 2015, left NAOJ in October
2015 to become a faculty member of a university.

II Status Reports of Research Activities093

15. Astronomy Data Center
1. Introduction
The Astronomy Data Center (ADC) is a central core ofcomputing and archiving for astronomical data. It 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 are organized into the DB/DA Project, Network
Project, JVO Project, HSC Data Analysis/Archiving Software
Development Project, and open-use computer system service.

2. ADC Report(1) DB/DA Project
The DB/DA-project conducts research and development on
astronomical Data Bases and Data Analysis. Various astronomy
data are made available to the public, such as astronomical
catalogs, the Astrophysical Data System (ADS), and all-sky
imaging data (DSS, DSS2). It also makes various astronomical
data available to researchers and educators (http://dbc.nao.
ac.jp/).
SMOKA (http://smoka.nao.ac.jp/) is the core of the DB/
DA-project. It provides archival data of the Subaru Telescope,
OAO 188-cm Telescope, Kiso 105-cm Schmidt Telescope (theUniversity of Tokyo), MITSuME 50-cm telescopes (Tokyo
Institute of Technology), and KANATA 150-cm Telescope(Hiroshima University). Stable operation continued throughcooperation with each observatory, producing many scientificresults. The total amount of open data (excluding environmental
and atmospheric data) is more than 12 million frames (71 TB)
as of May 2016. There were 16 papers published in major peer
reviewed journals which were produced using SMOKA data.
The cumulative number of refereed papers using SMOKA data
is 192. Continuing from the previous year, in 2015 system
improvements were implemented to develop and streamline
advanced retrieval functions (e.g. moving celestial object
retrieval). In addition, in September 2015, data from HONIR on
the Kanata Telescope at Higashi-Hiroshima Observatory was
opened to the public; and starting from January 2016, position
correction data for the Tokyo Institute of Technology MITSuME
Telescopes was offered.
(2) HSC Data Analysis/Archiving Software Development ProjectThis project started in January 2009. The main purpose
is to develop the data analysis pipeline and data archiving
software for the Subaru Telescope’s wide-field-of-view primefocus camera, Hyper Suprime Cam (HSC), using 104 CCD’s.
Most of our efforts are concentrated on the implementation of
the software for: effective data analysis/archiving by paralleland distributed processing; precise photometric and astrometriccalibrations; and correction of various effects originating fromthe camera system.
From March 2014, the Strategic Survey Program (SSP)094

II Status Reports of Research Activities

using HSC started and we began to have consistent large data
output (about 300–400 GB per night). We preformed data
analysis of the SSP data, produced a database storing the results,
and made the third and fourth data releases to the SSP teamcollaborators during this fiscal year (in September 2015 andJanuary 2016). In the latest data release in January 2016, theimage data involve 1.5 million files with a total size reaching
about 200 TB. The catalog database stores about 280 million
objects in a 10 TB database volume. We have developed various
user interface software for retrieving image or catalog data using
the database through web browsers; many of these functions
have been offered to collaborators. The computers/hardware forthe data release are in stable operation and the software is in theoperational phase with minimum functions. Major problems in
the pipeline software have been significantly reduced, althoughfurther improvements to functions in the pipeline software arestill necessary to achieve the planned accuracies for calibrations/
measurements of celestial objects in the images. The on-site data
analysis system developed from 2011 is now in the operational
phase, and performed well in the SSP and open-use observations.
It features observer support tools, such as the observation log
viewer, which allows browsing of the data analysis results
through a web browser. Although there are still little problems,
this system has made large contributions to the smooth operationof the Subaru Telescope.
(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) 100 Gbps Network service development and operation:
We acquired and operated circuit links faster than 100 Gbps
between Otemachi—Mitaka, Otemachi—Higashi-Shinagawa
and Mizusawa–Sendai. Transmission equipment has been
constructed and operated for each link. Between Mizusawa andSendai 40 Gbps of the 160 Gbps cables, and 100 Gbps cables
between Mitaka—Otemachi and Otemachi—Higashi-Shinagawa
were laid and have started operation. The Mizusawa–Sendai
circuit has been connected to SINET5 and JGN. The Mitaka—
Otemachi circuit increased the Data Center’s base connection
speed. The Otemachi—Higashi-Shinagawa circuit has beenconnected to the 100 Gbps circuit to the United States ofAmerica.
2)100 Gbps capability network beta service: Wide area 100 Gbps
circuits such as the 100 Gbps circuit to the USA, WIDE, and
SINET were maintained. To make the best use of these circuits,
equipment has been increased in part of the host network,
making capability on the NAOJ network service equivalent to
100 Gbps.
3) ADC Relocation: For more effective network operation, racks

to consolidate the circuits and transmission devices locatedin the Otemachi data center were relocated next to the racks
operated by the WIDE project’s data center.

through a web browser. Although there are still little problems,
this system has made large contributions to the smooth operationof the Subaru Telescope.

(4) JVO Project
The trial version of JVO portal 2, with a greatly reviseduser interface to improve its usability, was released. JVOSky,where data can be retrieved from a map of the sky, was updated
from a GoogleSky base to a new sky-map GUI using AladinLite developed by CDS. This update enabled it to display
the data taken at high latitude without distortion. All of theobservation data of Suprime-Cam taken before April 6, 2014
was reprocessed using the most recent reduction pipeline. The
data was released on the JVO portal. JVO ALMA archive was
updated to implement a new feature that enables users to searchdata based on object names defined in the Simbad database.
ALMA WebQL for quick-look images of ALMA data was
updated. Utilizing ultra-high-speed SSDs with a PCI-Express
interface enabled users to start a quick look of an ALMA data
cube within a few second, even for 10 GB of data. The design of
the GUI was greatly modified and improved, as a result accessto the ALMA archive was significantly increased.

(6) Open-use Computer System and Services
The new rental open-use computer system, “National
Astronomical Observatory of Japan: Data analysis, archiveand service system,” has been in operation since March, 2013.
The system plays a leading role as part of the Inter-University
Research Institute.
The system consists of the “Multi-Wavelength data analysis
subsystem”, “Large data archive and service subsystem(MASTARS, SMOKA, HSC science, ALMA, VERA, NRO,
Okayama, and Catalog archive service)”, “JVO subsystem”,“Solar data archive, analysis and service subsystem”, “Dataanalysis subsystem in Mizusawa campus”, and “Development
subsystem”.
The total storage, memory, and number of CPU cores within
the system are about 6 PB, 13 TB, and 2000 cores, respectively.
In JFY 2015, the total number of users was 372 (including 53
users of overseas institutes).
In the course of inter-university research we held andsupported some workshops on using the software and systems,
and offered a computer environment for data reduction practice.
The dates and numbers of participants in JFY 2015 were as
follows.

(5) HSC Data Analysis/Archiving Software Development ProjectThis project started in January 2009. The main purpose
is to develop the data analysis pipeline and data archiving
software for the Subaru Telescope’s wide-field-of-view primefocus camera, Hyper Suprime Cam (HSC), using 104 CCD’s.
Most of our efforts are concentrated on the implementation of
the software for: effective data analysis/archiving by paralleland distributed processing; precise photometric and astrometriccalibrations; and correction of various effects originating fromthe camera system.
From March 2014, the Strategic Survey Program (SSP)
using HSC started and we began to have consistent large data
output (about 300–400 GB per night). We preformed data
analysis of the SSP data, produced a database storing the results,
and made the third and fourth data releases to the SSP teamcollaborators during this fiscal year (in September 2015 andJanuary 2016). In the latest data release in January 2016, theimage data involve 1.5 million files with a total size reaching
about 200 TB. The catalog database stores about 280 million
objects in a 10 TB database volume. We have developed various
user interface software for retrieving image or catalog data using
the database through web browsers; many of these functions
have been offered to collaborators. The computers/hardware forthe data release are in stable operation and the software is in theoperational phase with minimum functions. Major problems in
the pipeline software have been significantly reduced, althoughfurther improvements to functions in the pipeline software arestill necessary to achieve the planned accuracies for calibrations/
measurements of celestial objects in the images. The on-site data
analysis system developed from 2011 is now in the operational
phase, and performed well in the SSP and open-use observations.
It features observer support tools, such as the observation log
viewer, which allows browsing of the data analysis results

1. SOKENDAI Summer School (Reduction Environment
Support), Aug. 3–Sep. 4 2015, 7 users
2. IDL School for FITS Data Analysis (Sponsor), Sep. 15–16
2015, 9 users
3. Subaru Autumn School 2015 (Co-sponsor), Sep. 28–Oct. 1
2015, 13 users
4. Subaru Experiential Observation and Research (Reduction
Environment Support), Nov. 11, 2015–Mar. 31 2016, 8 users
5. C Language School (Sponsor), Nov. 17–19 2015, 10 users
6. N-body Simulation School (Co-sponsor), Jan. 20–22 2016, 16
users
7. SOKENDAI Asian Solar Physics Winter School (Co-sponsor),
Jan. 26–28 2016, 30 users
8. IRAF/PyRAF School (Sponsor), Feb. 16–17 2016, 10 users
9. ALMA Data Science Experience (Reduction Environments
Support), Mar. 7–11 2016, 3 users
The total number of participants of the schools in JFY 2015
was 106 users.

3. Others
As part of outreach and promotion activities, 45 issues of“ADC News” were published from No. 437 to No. 482 in JFY
2015. The newsletters were distributed by E-mail to users andappeared on the ADC web pages.

II Status Reports of Research Activities095

16. Advanced Technology Center (ATC)
1. Organization and Summary of Activities in ATC
The Advanced Technology Center has been working on
developments for astronomy instruments in general. Our
programs are divided into “prioritized area developments” and“advanced technology developments” to meet requirements
both for current on-going astronomy programs and for future
programs.
Development, fabrication, and shipment of the ALMA
receivers for band-4, 8, and 10, which had proceeded as“prioritized area developments,” were concluded in FY 2013. In
the middle of FY 2014, the ALMA receiver development group
was reformed and divided into three groups: the ALMA receiver
maintenance group, the ALMA advanced receiver developmentgroup, and the telescope receiver development group. In FY
2015, the ALMA receiver maintenance group was responsible
for repairing the problems in shipped receivers; the ALMA
advanced receiver development group conducted basic researchon the extension of RF and IF frequencies as well as the multibeam receiver; and the telescope receiver development group
was responsible for upgrading the performance of the 45-m
FOREST receiver and ASTE receivers. In the middle of FY
2015, the ASTE radio camera development group was moved
to ATC from Nobeyama Radio Observatory to strongly support
its activity for the commissioning observations at the ASTE
telescope to be held in early FY 2016.
For prioritized area development, in FY 2015 we pushedforward the development of Thirty Meter Telescope (TMT)
observation equipment such as IRIS, WFOS/MOBIE, and thedevelopment of control and vibration isolation equipment andmirror holders for the gravity wave telescope, KAGRA. The
design and production of those devices have been supported by
the mechanical engineering shop (ME Shop). The optical system
of IRIS has been largely modified utilizing all reflective mirrors,
followed by the re-design and re-analysis of opto-mechanicalsystem and optical performance. In parallel, experiments using
prototype system are proceeding. Since Hyper Suprime-Cam(HSC) has started observing runs from March, 2014, HSC was
moved to “advanced technology development” from “prioritizedarea development” and the HSC development group was
responsible for improvements and repairing the problems of
HSC.
The “advanced technology developments” includes
developments for radio imaging arrays, the solar-observing
rocket-borne instrument CLASP, and others. Concerning
CLASP, the development of the device was completed in 2014
and it was sent to the White Sands launching site in early 2015.
Then it was successfully launched in September, 2015 andsuccessful observation of the solar chromosphere has beenachieved.
The oversight committee of ATC, including non-NAOJ
members, has been discussing about ATC activities on current
projects and R&D for future programs, based on requests

096

II Status Reports of Research Activities

from the Director General. In FY 2015, ATC activities for thedevelopment of TMT and KAGRA were reviewed and will
feedback to ongoing programs. R&D programs for the radio
camera and infrared detectors were also reviewed in FY 2015
accordingly.

Figure 1: New Organization Chart of ATC (FY 2015).

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 andshape measurements. Three teams including design, fabrication,and measuring/ultra-precision fabrication teams, cooperate toadvance projects by leveraging their expertise.
The design team has been taking charge of mechanicaldesigns for KAGRA auxiliary optics and TMT/IRIS imager andworking on several challenges such as[Mechanical design of KAGRA]- Design of the vibration isolation table for the Beam Reducing
Telescope- Design of the five-axis lens positioner for the Beam Reducing
Telescope- Design of the winch mechanism for the main mirrors in thePower Recycler and Beam Splitter- Assembly of Bottom Filters for the vibration isolation system
for the KAGRA auxiliary optics subsystem[Design of TMT/IRIS]- Design and thermal structural analysis of an optical element
holder in cryogenic conditions- Seismic response analysis of overall IRIS structure- Cryogenic endurance test of mechanical components (ballbearing and ball screw) for the Imager

Table 1: The requests in FY 2015.

- Cryogenic endurance test of a drive mechanism on the filter
exchanger for the Imager for TMT/IRIS.
The fabrication team has been working on the vibration
isolation system of KAGRA since last year, and delivered
internal parts for 11 sets of Bottom Filters. And the cylinders,made of Ti-6Al-4V, to be used as Recoil Masses for payloadsof the suspension systems were also delivered. Fabrication of
the five axis-lens positioner for the Beam Reducing Telescope
has started recently. For TMT/IRIS, mechanical parts for the
cryogenic endurance test were machined and supplied uponrequest from the design team. In addition, the team finishedtest parts made of super invar for thermal testing of the SmallJASMINE structure. And, as for the holders of the pupil
mirror array and the slit mirror array for the integral field unit
on the Subaru Telescope, final production has started basedon experience gained from prototyping. Manufacturing of a
37-pixel corrugated horn array was initiated in collaboration
with the ultra-precision fabrication team.
The ultra-precision fabrication and measurement teamhas responded to fabrication requests and also has enhanced
collaborative research with external institutes. The teamestablished an ultra-precision milling process for the wideband
corrugated horn array, the development of which has been led
by ATC, and the horn array with 4 pixels was successfully
finished. Manufacturing has started for the 37-pixel horn
array that is regarded as the next subject. Also, in regards tothe corrugated horn for the ALMA Band 10 receiver, the datarequired for machining was obtained and manufacturing isabout to start. Regarding the collaborative research with the
Mechanical Engineering Center of KEK, ultra-precision millingusing single-crystal diamond cutting tools has been discussed.
Technical cooperation in trial machining and evaluation was
conducted to investigate the specific machinery that is capableof an efficient mirror finishing for the X-band acceleration disk.
The collaborative research with the Institute for Molecular
Science and Nagoya University has continued in considerationof achievements up until present.
The ME Shop accepted 90 machining or repair requests
in FY 2015. With 4 programs carried over from FY 2014, 89
out of 94 programs have been concluded and 5 programs arecarried over to FY 2016. There were 9 programs requested fromexternal organizations. The following table shows the requests
in FY 2015.
(2) Optical Shop
1) Management and maintenance• Maintenance of measuring instruments (such as daily
inspections)• Technical consulting for users (47)
• Repair and upgrade- Exchange of PC for NH-3SP (Mitaka Kohki Co. Ltd.)- Installation of Keyence VR-3000.
And others

From FY2014 FY2015
ATC

1

TMT/IRIS

22

To FY2016
1

4

KAGRA

2

9

ALMA

5

ASTE

2

CLASP, CLASP2, SOLAR-C

6

HSC

1

JASMINE

3

Exoplanet Project Office17

Public Relations Center1

Solar Observatory

9

Nobeyama Radio Observatory

1

Subaru Telescope

1

2

1

External organizations
IoA, Univ. of Tokyo

5

JAXA/ISAS

1

2

Ibaraki University

1

Other

1
Total

4

90

1
5

2) Open use of measurement instruments (April 2015 - March2016)• Number of user: 286
NAOJ: 211(including 107 from ATC)
External organizations: 75• Use of LEGEX910 (large-scale 3-D measurement machine): 6
Number of operating days: 10(3) Thin Film Processing Unit
We evaluated the wideband anti-reflection coating on the
microlenses in front of the optical fiber input for the SuMIRe(Subaru Measurement of Images and Redshifts) project, which
was fabricated in the last fiscal year. We confirmed the required
quality and performance for this purpose, but also determinedthat we have reached the limits of current techniques. For
further improvement of anti-reflection coatings, fundamental
experiments are carried out to design and develop the concrete
processes for coating, which takes into account the applicationand expected performance of inhomogeneous multilayers.
(4) Optical and Infrared Detector GroupWe have executed a joint purchasing program for MESSIA6,
a focal plane array controller for astronomical instruments,
as one of the open-use devices of the Advanced Technology
Center. MESSIA6 was build based on the electronics developedfor Hyper Suprime-Cam in cooperation with the University ofTokyo, and the High Energy Accelerator Research Organization(KEK). It is optimized for general purpose to control
astronomical instruments which use focal plane arrays. In thisyear, a total of 14 sets were purchased for 2 divisions of NAOJ
and 4 other organizations. We are providing the documentation,
and will support the users for installing MESSIA6 onto theirinstruments.

II Status Reports of Research Activities097

(5) Space Optics
Activities to observe astronomical objects from space bysounding rockets and science satellites have been pursued
to realize future space science missions. In FY 2015, basic
development was conducted for flight operation of a sounding
rocket mission CLASP, which aimed to observe magnetic fields
at the height of the solar chromosphere and the transition region,and for a future satellite mission SOLAR-C. The development
activity for a future satellite mission WISH has terminatedwithin ATC.
Immediately after the completion of the CLASP instrument,
it was transported to the U.S. at the beginning of the fiscal year.
The flight experiment was executed on September 3, 2015 at asounding-rocket launch site in the U.S. It has become the firstsuccessful flight for observing high-precision polarimetry of the
H Lyα from the Sun. The design and fundamental experiments
for the next flight started in the latter half of the fiscal year.
For a planned future solar observing satellite mission
SOLAR-C, the development and testing of prototype
components have been carried out for the waveplate andnarrow-bandpass filters meeting space-qualified specifications,in addition to the performance evaluation of a near-infrared
imaging device for the high-speed spectro-polarimetry.
(6) Facility Management Unit
The Facility Management Unit conducts the managementof ATC facilities including the buildings, electric facilities;
daily maintenance of the Cold Evaporator (CE); maintenance ofbuilding equipment; oversight of construction; and managementof hazardous material and laboratory equipment.
Concerning the buildings facilities and equipment,
we replaced four draft chambers. We attached a scrubber
decontamination device to the draft chamber using hydrogen
fluoride-based solvent for washing in order to remove thetoxic substances included in the exhaust, so that the amount in
the exhaust gas is less than the regulation value. Because thedischarge ventilation performance was lower than the regulation
value, we changed the motor of the blower and increased theventilation performance to more than the regulation values.
In the other 3 draft chambers, we changed the motors of theblowers to increase the ventilation performance to more than
the regulation value as well. Many problems occurred in the air
conditioner. Three rooms in the radio development laboratory
were broken at the same time and restoration required twomonths. Because deterioration of the water pipes increases
the degree of coolant pollution, we increased checks of thecirculation coolant facilities to prevent pollution of the water. We
cooperated with an advanced technology experiment building(TMT) construction plan completed in March 2015.
The main users of the laboratories were 11 projects including
ATC members, KAGRA, TMT, Radio Department/Chile
Observatory, HSC, JASMINE, Optical and Infrared Department,
Exo-planet team, Subaru Telescope, Hinode Science team,and SOLAR-C/CLASP. Programs that used clean rooms were
KAGRA in the south building and CLASP in the north building.
After completion in March, CLASP was launched in the United

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II Status Reports of Research Activities

States in September 2015 and successfully observed the Sun.

3. Open Use Programs
In FY 2015, ATC called for and accepted open use programs
twice a year. ATC facilities were used for 8 “collaborative
development programs” and 30 “facilities use programs”.
Information about these programs is presented in “Common
use of ATC facilities” with the names and research titles of the
program leaders. Reports from the open use programs are alsopresented on the ATC homepage.

4. Prioritized Area Developments(1) ALMA Band 4, 8, 10
For the ALMA project, the mass-production and shipment
to Chile of the Band 4, 8 and 10 receiver cartridges, which wereassigned to Japan, were completed in FY 2013. In Chile, most of
the receivers have been installed and are operating 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 to correct receiverdefects, and repaired one Band 8 receiver and six Band10
receivers during FY 2015.
Table 2: Total number of failed receivers.
Receiver

Total

Breakdown
Initial failure

Aging failure

Band 4

6

3

3

Band 817

14

3Band 1015

6

9Table 2 shows the total number of failed receivers broken
down into “initial failure” and “aging failure.” The initial failuresof Band 4 receivers included improper design at the initialdevelopment phase, and the number of failures has decreased
after the design was revised. Similarly, most of the initial failuresof Band 8 receivers were due to the improper design, and thenumber of failures has decreased after the design was revised.
In contrast, the initial failures of Band 10 receivers pertained tothe turn-on sequence for several amplifiers. This problem washandled by replacing the amplifiers. The aging failure of Band
10 receivers is from degradation of electrical devices; we havealready identified the lots with high degradation possibilities.
It is expected that the defects will decrease by replacing thedevices from such lots with those from lots with low degradation
possibilities.
Although the number of failing Band 4 and Band 8 receivers
seems to be decreasing in FY 2015, this is not enough to judge
the defect frequency owing to aging failure, because it has notbeen long since they started operation in ALMA. It is very
important to keep the long-term maintenance system in ATC.
(2) Development of advanced receivers
Development of ultra-wideband, terahertz, and multibeam

heterodyne receivers has been started as future ALMA
upgrades. Dr. Wenlei Shan was appointed Associate Professor
in the Advanced Technology Center in November 2015, andconsequently, the structure of the receiver development team has
been reorganized.
1) Ultra wideband receiver
We have proceeded with the development of a band 7+8
receiver covering the frequency range 275-500 GHz. We havesuccessfully fabricated SIS junctions with high current density,
ranging from 10 to 50 kA/ cm2, and high quality, which is one of
the key technologies for future receiver development. Based on
this new junction technology, we have also demonstrated lownoise and wider RF band mixer performance than typical band-8
mass-produced SIS mixers. As a parallel project, we have started
research and development of a multiband low-noise receiver
aiming at improved sensitivity and simultaneous observation ofmulti-line spectra.
2) Terahertz receivers
We have pushed forward with the establishment of areconfigurable beam pattern measurement system and withthe development of superconducting mixers and corrugatedfeed horns for the 1.2-1.6 THz band. We have demonstrated
heterodyne response using a waveguide HEB mixer incollaboration with the University of Tokyo. We have also
demonstrated competitive performance of the corrugated hornantenna with respect to ALMA specifications by using theestablished beam pattern measurement system.
3) Multibeam receiver
We have started the conceptual design of a novel multibeam
receiver based on planar circuits. Additionally, together with
the Korea Astronomy and Space Science Institute (KASI), we
have started collaborative research and development aiming at
the installation of a wideband multibeam receiver on the ASTE
telescope. This later project is led by KASI.
(3) SIS junction development
In order to fabricate a millimeter- and sub-millimeter-wave
low-noise receiver having either an octave signal bandwidthor a signal frequency higher than 1 THz, we conducted
research and development for high quality Nb/Al type SIS
junctions with extremely high current densities (15 – 30 kA/cm2), which are expected to be essential key devices for thosereceivers. According to the study of I-V characteristics as wellas the detailed analysis of the distribution profiles of Al andNb observed by the STEM (scanning transmission electron
microscope) for the conventional Nb/Al/AlOx/Nb type SIS
junction, we found that the AlOx is considerably damaged by
the upper Nb, and that an increase of the subgap leakage current
might result from such damage. A Nb/Al/AlOx/Al/Nb type SIS
junction with an ultra-thin (~ 5 nm) Al film inserted between the
AlOx film and the upper Nb film was designed to prevent directcontact between the Nb and AlOx film to minimize the damage
to the AlOx film. We tried to make the Nb/Al/AlOx/Al/Nb type

SIS junction and found that a very high-quality (RSG/RN>20)
SIS junction with an extremely high current density (~45 kA/cm2) can be obtained in this way. Although, up to now, it has
been considered quite difficult to produce a high-quality SIS
junctions with such an extremely high current density, we haverecently succeeded in producing a SIS junction, which has not
only a high quality but also an extremely high current density,
for the first time in the world. This achievement gives us a brightoutlook, particularly for the development of receivers covering
the frequency band (275-500 GHz) of ALMA band 7 and 8.
(4) TMTWe have been continuing development of the first generation
Thirty Meter Telescope (TMT) instrument IRIS since 2011.
Light Preliminary Design Phase extension, LPDP-E (Jan. –Dec. 2015) and Light Preliminary Design Phase 2016 extension,
LPDP-2016E (Jan. – Dec. 2016) continued in FY 2015. We
proceed with the optical design of the IRIS imager which NAOJ
has a responsibility to develop, focusing on the opto-mechanicaldesign. We have improved the optical design with all reflective
surfaces, which meet the requirements for wave-front error
across the entire field of view of 34 arcsec square by optimizing
the symmetry of optical parameters. Further, we proposeda solution for packaging the imager optics into the sciencecryostat and started designing the opto-mechanical components
to support all optics.
We introduced the progress and status of opto-mechanicaldesign of the IRIS imager and integration plan at the mechanicaland integration mini review on August 13, 2015 in Pasadena
California. Also we presented the latest optical design in theface-to-face meeting on November 5 and 6, 2015. IRIS teammembers have approved the solution for the optical design of
the IRIS imager.
In parallel, the IRIS-J team has been continuing vibration
analysis for IRIS combined with the adaptive optics system for
TMT, NFIRAOS. In prototype experiments and trial fabrications
looking ahead to the coming final design phase and fabrication
phase, major issues are the durability of the bearings under the
cryogenic conditions, the cooling characteristics of the opticalsubstrate, and trail production of the high-reflectivity coating.
We have been working on a conceptual study for a camera
system of WFOS, which is another first generation instrumentof TMT. We have investigated the degradation of image quality
caused by the inhomogeneity of lens made of fluorite crystal.
Also we made a modification and upgrade to the optical designfor the camera system due to a change in the layout of WFOS.
(5) Gravitational wave telescope KAGRA
We developed KAGRA’s auxiliary optics subsystem (AOS)
and vibration isolation subsystem (VIS) with the Gravitational
Wave Project Office.
About AOS, we have continued the design and manufactureof some parts of the transmission monitor system (TMS). The
telescope system will be located at the end of each 3-km arm
optical cavity of KAGRA to monitor the tilt and shift of thebeam line, and make feedback signals to the control system. The

II Status Reports of Research Activities099

beam reducing telescope (BRT), which is a part of the TMS,
need to be aligned in ultra high vacuum after laser light will befinally resonant in the 3-km optical cavities; for example, 5-axes
lens holders have been designed for the BRTs. In addition, theBRTs need to be isolated from vibrations as done for the othermirrors of the KAGRA interferometer, and the design of thevibration isolation stages for BRTs are ongoing.
KAGRA-VIS is a system to suspend mirrors required for the
KAGRA interferometer to isolate them from seismic fluctuation.
The system consists of multi-stage isolation mechanical filters;
ME shop has finished manufacturing all the parts for the bottom
filters, and also done assembly works, tests before the shipping.
The ME shop has also manufactured all the pieces of recoil
masses (made of 64-Ti), which will be suspended to reduce
fluctuations of the mirrors. In addition, design, manufacture,and the tests of some jigs to hang the mirrors (the hanging
frame) and winch system for the mirrors and recoil masses havebeen done. Then, ME shop have involved in the final design,
manufacture, and the tests of most of the suspension chain bywhich the PR3 mirror (among the main mirrors, only this mirror
in initial-phase KAGRA will be also used for the next stage) has
been suspended and the hanging jig. As a result, iKAGRA wasable to start the test run in the end of March of 2016.

5. Advanced Technology Developments(1) Telescope Receiver Developments
Based on the technical skills acquired through thedevelopment of ALMA receivers, the “telescope receiverdevelopment” team has responsibility for the development of the
Nobeyama FOREST receiver and the fabrication and tests of acryostat for enabling simultaneous use of multiple receivers in
the ASTE telescope. And also, we maintain good collaboration
with other radio telescopes pursued by universities, such as
NANTEN2 pursued by Nagoya University and the receiver for
the Greenland Telescope (GLT) pursued by Osaka Prefecture
University.
ATC can increase the technology standards of the community
by giving feedback using the technologies and knowledge
accumulated through development of specific projects, and canprovide technology developments to other projects, universities
and research institutions. It is also important to make the bestuse of the achievement of the projects.
(2) MKID Camera
The MKID (Microwave Kinetic Inductance Detector)
group of the Advanced Technology Center is developing a
superconducting camera in millimeter and submillimeter
wavelengths for the Antarctica terahertz telescope, whichobserves distant galaxies with a wide field of view, and for the
LiteBIRD satellite, which detects CMB B-mode polarization,in collaboration with the University of Tsukuba, Saitama
University, KEK, ISAS, Kavli IPMU, and RIKEN. The
following papers were published in FY 2015.
1) Study of superconducting Bi-layer MKID (A. Dominjon et al.

100

II Status Reports of Research Activities

2016 IEEE AS)
2) Broadband (Octave band) corrugated horn array (S. Sekiguchi
et al. 2015 LTD)
3) Design of MKID focal plane array for LiteBIRD (Y. Sekimoto
et al. 2015)4) Radiation tolerance of MKID (K. Karatsu et al. 2016 JLTP)(3) Hyper Suprime-Cam (HSC)
HSC has been used for regular science operations since
March 24, 2014. This includes both the Subaru Strategic
Program and the normal open-use observations. During FY
2015, 111 nights were allocated to HSC programs (among these
53 nights were for Subaru Strategic Programs). Minor problems
occurred in the mechanism of shutter and filter exchange andsome of the main CCDs, however, there were no nights where
instrument problems completely prevented observations,fortunately. These problems were handled and settled throughthe comprehensive support from the ATC engineering staff. Onsite maintenance service of the filter exchanger was conducted.
Fabrication, integration, testing and adjustment of a spare forthe shutter was completed in Mitaka. This spare is scheduled to
be shipped to Hawai`i early in FY 2016. For the CCD failures,it has to be coped with changes in the operating conditions, byverifying the testing unit of CCD in a Mitaka laboratory. On
the other hand, it turned out that the uniformity of the existing
flat lamp modules on the telescope was not sufficiently goodconsidering the target accuracy of HSC photometry. So a newflat lamp produced by a single light source has been installed on
the ceiling of the camera. Some adjustments related to this flat
lamp still remain and underway. In the next fiscal year, FY 2016,
we plan to install new
calibration unit for HSC camera using monochrometer.
(4) Near-IR Imaging Sensor Developments
In areas of electronics and detector developments, we havemade a trial chip of a low noise Indium Gallium Arsenide(InGaAs) image sensor based on a commercial product, forwhich the cost is expected to be lower than existing nearinfrared sensors, in cooperate with KEK, Hiroshima University,and Kagoshima University. We also investigated making a larger
format sensor and new readout electronics to use the InGaAs
image sensor in a near-infrared wide field camera.

17. Public Relations Center
1. Overview

3. Public Relations Office

The Public Relations Center engages in the publication,
promulgation, and promotion of scientific achievements madenot only by NAOJ but also by others in the field of astronomy
in general to raise public awareness; responds to 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. Starting from FY 2014 with the addition of the
IAU Office for Astronomy Outreach (OAO), the Center has
been comprised of 7 offices and 1 unit: the Public Relations
Office, the Outreach and Education Office, the Ephemeris
Computation Office, the Museum Project Office, the Library
Unit, the Publications Office, the IAU Office for Astronomy
Outreach (OAO), and the General Affairs Office.

Through press conferences and web releases, the Public
Relations Office actively developed public outreach activities
focused around the results of each Project, first and foremost
ALM A and Subar u Telescope, including open use andcollaborative results with other universities and research
institutes. In addition, in cooperation with the Outreach and
Education Office, the Public Relations Office also conducted
observation campaigns to promote astronomical phenomena ofinterest to the public, like the solar eclipse and meteor showers.

2. Personnel
In FY 2015, the Public Relations Center was composed of
Director Toshio Fukushima and the following staff members:
2 professors, 1 associate professor, 2 assistant professors (bothhold concurrent posts), 2 research engineers, 1 senior engineer,1 engineer, 1 Chief of the Library, 2 specially appointed
senior specialist, 4 research experts (1 holding a concurrentpost), 20 public outreach officials, 1 research supporter, and 2
administrative supporters.
On April 1, 2015 Chief of the Library Tatsuya Todoriki
arrived and public outreach official Takao Ibaraki and public
outreach official Taiga Hamura arrived in the Outreach and
Education Office. On April 6, 2015, specially appointed seniorspecialist Pires Canas Lina Isabel arrived in the IAU Officefor Astronomy Outreach; on June 1, research supporter Chie
Tsuchiya arrived; on September 1, Naomi Ishikawa waspromoted to specially appointed senior specialist; on October
1, public outreach official Noriko Takabatake arrived in the
Outreach and Education Office; and on December 8, public
outreach official Diaz Rosas Elian Abril arrived in the IAU
Office of Astronomy Outreach.
On March 31, research engineer Goro Sasaki and public
outreach official Diaz Rosas Elian Abril finished their terms.
In addition research supporter Chie Tsuchiya transferred to the
Hinode Science Center.

Month
April 2015
May 2015
June 2015
July 2015

Access counts
1,187,930
542,548
513,154595,883(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.
NAOJ e -mail newslet ters No.143-158 were issued ,containing headlines for major news events with hyperlinks
to pages with further details. The Astronomy Information
Telephone Service, which provides voice news updated on asemimonthly basis, issued 24 messages in total. This service
was discontinued at the end of this fiscal year.
Through the Twitter social networking service, employedsince October 2010, the Office disseminates information on
the status of various NAOJ projects such as open house events,
regular stargazing parties at Mitaka Campus and position
openings. As of the end of March 2016, the number of followers
exceeds 60,000. Starting from this fiscal year,we utilized theEnglish versions of Twitter and Facebook to strengthen our
English language information distribution.
(2) Press Releases and Media Relations
There were 25 research result announcements (compared
to 16 in FY 2014 and 26 in FY 2013). For press releases aimed
towards overseas audiences, we have increased the use of theAmerican Astronomical Society and AlphaGalileo which havebeen employed up to now, and from FY 2015 have started touse EurekAlert! which is operated by the American Association
for the Advancement of Science.
In the perennially popular Astronomy Lectures for Science
Journalists program, the 22nd lecture entitled “What does
the Rikanenpyo (Chronological Scientific Tables) Tell Us
Now” was held on November 24, 2015. Thirty-nine peopleMonthAccess counts
August 2015
1,026,205
September 2015
544,748
October 2015
623,754
November 2015
466,582
Total: 7,943,067

Month
December 2015
January 2016
February 2016
March 2016

Access counts
850,441535,655
523,145533,022

Table 1: Monthly website access statistics for the Public Relations Office website, NAOJ Public Relations Center (April 2015–March 2016).

II Status Reports of Research Activities

101

April 7, 2015

Unprecedented views of lensed galaxy and asteroid Juno taken with ALMA

May 12, 2015

Great Progress towards the Origin of R-process

June 1, 2015

Astronomers Discover a Young Solar System Around a Nearby Star

June 9, 2015

ALMA uses ‘Natural Telescope’ to Image Monstrous Galaxy near the Edge of the Universe

June 18, 2015

ALMA Precisely Measures Black Hole Mass

June 23, 2015
June 26, 2015
August 5, 2015

Astronomers Discover More than 800 Dark Galaxies in the Famous Coma Cluster
Unexpectedly Little Black-hole Monsters Rapidly Suck up Surrounding Matter
The Ghostly Remnants of Galaxy Interactions Uncovered in a Nearby Galaxy Group

August 24, 2015

Hinode, IRIS, and ATERUI Cooperate on 70 year old Solar Mystery: Magnetically driven resonance helps heat
the Sun’s atmosphere!

August 27, 2015

Discovering Dust-Obscured Active Galaxies as They Grow

September 10, 2015
September 25, 2015
September 30, 2015
October 15, 2015
December 4, 2015
December 5, 2015
December 7, 2015
December 18, 2015
January 15, 2016
February 4, 2016
February 25, 2016
February 25, 2016
March 3, 2016
March 10, 2016
March 10, 2016

Oxygen is not Definitive Evidence of Life on Habitable Extrasolar Planets“Fossils” of galaxies reveal the formation and evolution of massive galaxies
Mechanism of explosions and plasma jets associated with sunspot formation revealed
ALMA telescope unveils rapid formation of new stars in distant galaxies
Event Horizon Telescope Reveals Magnetic Fields at Milky Way’s Central Black Hole
ALMA Spots Monstrous Baby Galaxies Cradled in Dark Matter
Radio Shadow Reveals Tenuous Cosmic Gas Cloud
Final Results of NameExoWorlds Public Vote Released
Signs of Second Largest Black Hole in the Milky Way - Possible Missing Link in Black Hole Evolution
A Violent Wind Blown from the Heart of a Galaxy Tells the Tale of a Merger
Subaru-HiCIAO Spots Young Stars Surreptitiously Gluttonizing Their Birth Clouds
New Fast Radio Burst Discovery Finds ‘Missing Matter’ in the Universe
ALMA Spots Baby Star’s Growing Blanket
Deciphering Compact Galaxies in the Young Universe
Mysterious Infrared Light from Space Resolved Perfectly
Table 2: Web releases.

July 2, 2015
November 6, 2015

Dark Matter Map Begins to Reveal the Universe’s Early History
KAGRA’s Initial Operation To Begin Soon
Table 3: Press Conferences.

Video Visualization of TMT When Complete
The First Dark Matter Map Drawn by Hyper Suprime-Cam on the Subaru Telescope
Undertaking Galactic Archeology in M81 using the Very Wide Field of View Prime Focus Camera
Geminid meteor shower
ALMA 12-Meter Antenna Paper Model
What is a Meteor Shower? (Long version/Short version)*
Mitaka Open House Day Report*
Fureai (Friendly) Astronomy PR
The Opening of the Information Space of Science and Astronomy

Japanese, English Versions
Japanese, English Versions
Japanese, English Versions of Each

Table 4: Table 4: Summary of Produced Videos (* in preparation for release)participated in lectures and panel discussions about the history
and articles of the Rikanenpyo, which started 90 years ago.
(3) Supporting NAOJ-wide Public Outreach Activities
The following activities were pursued in addition to theCenter’s regular task of aiding research result releases.
We continued to produce videos explaining research
results, videos explaining astronomical phenomena, andvideos introducing outreach and education activities. Including
English versions, 14 were produced (including those in102

II Status Reports of Research Activities

preparation for public release). These videos introduce a wide
range of general activities, not just NAOJ research. As of theend of March 2016, these videos have accumulated a total of
15,000 views.
The Office also helped Projects with their own lectures forthe general public. The NAOJ lecture meeting “The Challenge
which Exceeded Space-Time: General Relativity’s 100th
Anniversary and Gravitational Wave Astronomy,“ was held
on September 18, 2015 and the ALMA public lecture/Osaka
Science Museum Special Night “Exploring the Mysteries

of Star and Galaxy Formation with ALMA” was held on
November 4, 2015.
In addition, we provided media support for a facility tour
and press conference on November 6, 2015, corresponding
to the completion of the initial experiment facility for thelarge-scale gravitational wave telescope KAGRA; and forthe opening ceremony for the Astrobiology Center National
Institutes of Natural Sciences, held on November 20.
As cooperation for the renewal of NAOJ Project webpages,
we provided support to the Gravitational Wave Project Officeand the Hinode Science Center.
Last fiscal year, “Multiwavelength Universe” a special site
providing explanations of astronomical observations for thegeneral public was opened. This year we opened an English
language version.

4. Outreach and Education Office(1) Handling General Inquiries
The Office received inquiries from the media, government
offices, and the general public. The Outreach and Education
Office responded to 6,606 telephone inquiries (Table 5) and
156 letters, 66 of which were official documents. The Office
stopped accepting inquiries via the internet in April 2014.
(2) Educational and Outreach Activities
The astronomical phenomena awareness campaigns
started as bidirectional information sharing initiatives in FY
2004. This year, 3 were conducted: “Let’s Observe the Total
Lunar Eclipse 2015” April 2015 (434 responses); “SummerNights: Let’s Count Shooting Stars 2015” August 2015 (2,875
responses); “Let’s Watch the Geminid Meteor Shower 2015”
December 2015 (1,550 responses).
The “Fureai (Friendly) Astronomy” project, now in its 6thyear, provided events to 60 schools out of the 71 which applied,reaching 5,743 students. A total of 42 lecturers participated.
On July 23 (Thursday) and July 24 (Friday) during summer
vacation “Summer Vacation Junior Star-Gazing Party” eventswere held for elementary, junior high, and high school students(application required, maximum capacity 50 participants eachday). Lectures about the assembly and use of planetarium
projection machines and telescopes, and star gazing parties
were held. A total of 103 people participated.
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 23 (Friday) and24 (Saturday) with the theme “The Challenges Awaiting
Astrobiology.” It was co-hosted by the Astrobiology Center,

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

Solar info Lunar info Ephemeris info
210
118
50
179
189
78
201
133
84
250
130
79

National Institutes of Natural Sciences; the Institute of
Astronomy, the School of Science, the University of Tokyo;
and the Department of Astronomical Science at the Schoolof Physical Sciences of the Graduate University of Advanced
Studies. The 23rd was cloudy, but the 24th was clear. The
event flourished: over the 2 days, a record high of 5,036 guests
attended. Each Project offered a selection of activities basedon their own expertise which were suitable for a wide rangeof age groups. Activities included the viewing of facilities notnormally open to the public, interactive panel displays, minilectures, and popular quizzes and games.
The 6th International Science Film Festival was co-hosted
between August 1 (Saturday) and September 30 (Wednesday),in cooperation with 69 collaborating organizations andgroups, with the main theme of the “International Year of
Light (IYL2015)” declared by the United Nations. Screenings
of science films and other events such as a stamp-collection
rally were held at 49 science museums, planetariums, andfilm theaters in Japan, with more than 1 million people
participating. The Kickoff Event (Nakano Zero Planetarium)
and Dome Festa (Koriyama City Fureai Science Center) were
held as the core events.
The “NAOJ Tours” cohosted each year with Tamarokuto
Science Center were held on Sunday March 20. They were
popular with a total of 80 guests, 40 in the morning and 40
in the afternoon, participating in tours of the 4D2U Dome
Theater, a sunspot observation event at the 20-cm Telescope
Dome, and self-guided tours along the tour course. In addition,group tours (self-guided) held on Saturday July 18, Sunday July
19, and Saturday August 22 were well received with 70 guests
attending each, for a total of 210.
From November 15 (Sunday) to 17, “The 11th Workshop forPopularizing Cutting-Edge
Astronomy” was held with the theme “Astrobiology” at
NAOJ Mitaka Campus and Japan Agency for Marine-Earth
Science and Technology Yokosuka Headquarters. A total of 67
researchers and people connected to education and outreachparticipated.
The “You are Galileo!” program received support from theNonprofit Public Organization: Foundation for Promotion of
Astronomy, and was held this year in Indonesia, in cooperation
with the Office of International Relations and OAO. A “You are
Galileo!” workshop was conducted on March 11 and a public
lecture was conducted on March 12 at Mulawarman University
in Samarinda City. The workshop was attended by 25 people,
and the lecture by 140 people.
The data reduction software Makali`i, developed toenable FITS data obtained from Subaru Telescope scienceobservations and other sources to be used in astronomy
Time
21
18
5
11

Solar System Universe
201
81
232
109
361
99
170
150

Astronomy
102
177
125
150

Other
827
896
665
505

Total
1610
1878
1673
1445

Table 5: Telephone inquiries made to the Outreach and Education Office of the NAOJ Public Relations Center (April 2015–March 2016).

II Status Reports of Research Activities

103education and outreach, was distributed via the internet todomestic and international users. Starting from March 2016,
the distribution method was changed so that the software canbe downloaded freely without registering.
We participated in the International Year of Light 2015
“Cosmic Light” events: a special website “Matters of Cosmic
Light” was opened to the public and updated; Cosmic Light
astronomical object photo panels were produced and displayed;in cooperation with Konicaminolta Plaza, the “Hubble Space
Telescope Astrophotography Exhibit” was held; etc.
(3) Community Activities
The “Mitaka Picture Book House in the Astronomical
Observatory Forest” welcomed 42,401 visitors in FY 2015.
The Outreach and Education Office is conducting events at
Mitaka Picture Book House in the Astronomical Observatory
Forest including the “Dou Ugoku? Ochiru Korogaru (How do
You Move? Fall and Roll)” exhibit, modern and traditional
Tanabata events, moon viewing, etc. in cooperation with the
Mitaka City Municipal Office and local volunteers. In addition,
through the “Mitaka Picture Book House in the Astronomical
Observatory Forest, Picture Book Original Drawings Hallway
Exhibit Contest” which started from FY 2013, the Outreachand Education Office cooperated in the selection of 3 winningbooks. The grand prize winner “Noboreboshisama (Rising Star,
made by Tomoaki Kunii)” is scheduled to be published as partof the “Picture Book House in the Astronomical Observatory
Forest Compilation Series” in FY 2016.
The Outreach and Education Office conducted the 7th“Mitaka Solar System Walk” in cooperation with Mitaka
City and the non-profit organization (NPO) Mitaka Network
University Promotion Organization. Held from September 20(Saturday) to October 25 (Sunday). Stamps were placed at 170
shops and 67 facilities, including NAOJ Mitaka Campus andthe Mitaka City Municipal Office, for a total of 237 locations
around Mitaka. Approximately 18,000 guide-maps/stampsheets were distributed, of which 3,296 people turned theirs
in for a prize. The total number of stamps was 413,425; theaverage number of stamps collected was 125.4 per person. The
number of participants who collected all of the stamps was 339.
It was a good chance to tour the Solar System while promoting
commerce and industry and providing families with a way toenjoy Mitaka and rediscover the city’s charm.
The event “Astronomy Pub” has been held at Mitaka
Network University and hosted by the NPO Mitaka Network
University Promotion Organization since FY 2009. It provides
for 25 participants at a time and is held in the evening on the
3rd Saturday of every month except August. The Outreachand Education 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 in providing
presentations, telescope operation workshops, and other related
events.
With the aim of creating a meeting point suitable for“Mitaka, a Town with an Observatory,” the “Information

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Space of Science and Astronomy” opened along Mitaka’s Chuo
Dori, near the South Exit of JR Mitaka Station, on September
26, 2015. Established jointly by 4 partners: NAOJ, Mitaka
City, Mitaka Network University, and Mitaka City Planning
Board, it depends of the coordinated efforts of 11 groups,
including those aiming to invigorate the area in front of Mitaka
Station and the groups related to science and astronomy.
NAOJ offered photograph panels for the planned exhibitions;
held collaborative lecture meetings; offered outreach andmonthly astronomical information images through large-scale
information displays; and cooperated on the M Marche Project
conducted the 4th Sunday of every month. In addition, we arealso conducting the “Cosmic Reading Bookstore Corner,” adisplay of sample books available to read which changes themes
once every 2 months. In the half-a-year from September 26 toMarch 31, the “Information Space of Science and Astronomy”
welcomed 9,981 guests and was acknowledged as a location in
town where science can be easily accessed.

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 2016 edition of the Calendar andEphemeris, the 2016 version of the calendrical section of the
Rikanenpyo (Chronological Scientific Tables), and the 2017
edition of the Reki Yoko (posted in the official gazette on
February 1, 2016). The Calendar and Ephemeris webpage was
updated to match what was published in the Reki Yoko. In
addition the 22nd lecture entitled “What does the Rikanenpyo
Tell Us Now” was held in cooperation with the Public Relations
Office.
(2) As for the website (http://eco.mtk.nao.ac.jp/koyomi/
index.html.en), ECO continuously updated the contents ofthe Ephemeris Wiki. ECO cooperated with the astronomical
phenomena awareness campaigns again this year. The radiantpoints of the Perseid and Geminid meteor showers were
published in the Astronomical Information section of thewebsite. There were about 25 million page views for this fiscal
year.
(3) The Japan Association for Calendars and Culture Promotion
hosted its 5th General Meeting, the Calendar Presentation
Ceremony, and a symposium on the Traditional Calendar 2033
A.D. Problem.
(4) ECO hosted regular exhibitions in collaboration with
the Library, selecting from NAOJ’s invaluable collection ofhistorical archives written in Chinese/Japanese. The themesof the 52nd and 53rd exhibitions were “Official Documentsfrom the Meiji Era to the beginning of the Showa Era” and“Achievements of Harumi Shibukawa - II” respectively. These
exhibits 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).
(5) 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 16 reports including confirmation requests for
new celestial object candidates and other reports. The contents
were: 9 novae/supernovae, 3 comets, 3 luminous objects,
and 1 asteroid. Among the many examples of reporting avariable star or asteroid as a new object, 2 novae reported in
October, were communicated via NAOJ to the IAU Central
Bureau for Astronomical Telegrams and were recognized as anindependent discovery of Nova Ophiuchi 2015 No. 2 (V2949
Oph) and the discovery of Nova Sagittarii 2015 No. 4 (V5850
Sgr). Again in November, a supernova was reported. The
discoverer himself reported it to NAOJ and the IAU Central
Bureau simultaneously. It was recognized as the discovery ofSupernova 2015as.

6. Museum Project Office
For the 3 Fiscal Years from 2013 to 2015, part of the duties
for managing public access to the facilities was separated fromthe Outreach and Education Office and handled as the “Museum
Project Office.” But at the end of fiscal year 2015, the mission of
the Museum Project Office ended. So starting from FY 2016, it
was reintegrated back into the Outreach and Education Office.
(1) Facility Opening Events
With regards to the opening of the 4D2U Dome Theater in
FY 2015, at the end of the previous fiscal year, renovations were
performed to repair equipment and increase seating. In April,
it was reopened to the public. Starting from this fiscal year,
regular showings were held at the 4D2U Dome Theater 3 times
per month (the day before the 2nd Saturday, the 3rd Saturday,
and the 4th Saturday). Advance reservations were required. In
this 1 year period, a total of 35 events were held, in which 4,446
guests participated. An additional 70 group screenings were
held with 1,983 participants, and 119 tours were organized with
1,670 participants. In total, 224 screenings were held and a totalof 8,099 guests enjoyed 4D2U’s stereoscopic images.
Regular stargazing parties held with the 50-cm Telescopefor Public Outreach were held twice a month (the day before the
2nd Saturday and the 4th Saturday). These were held regardlessof cloudy or rainy weather. Advance booking (300 people foreach session) was introduced in FY 2012 for these events. A
total of 23 sessions were held with 4,717 participants.
A total of 19,729 people visited the Mitaka Campus Visitors'
Area in FY 2015. In addition the group tours in 2015, consistedof 129 general tours (4,797 guests), and 37 workplace visits byschools (536 guests), for a total of 166 tours accommodating
5,333 guests. Note that in the workplace visits, lectures by
researchers and question-and-answer sessions also took place.

The name of the Mitaka Campus Tour was changed to“Tangible Cultural Heritage Tour.” Advanced reservations are
required, 20 person capacity. This year a total of 204 people
participated. The “Tangible Cultural Heritage Tours” ceased
operation at the end of March 2016.
(2) Museum Planning and Archive Management
To prevent historically important observations, measuring
devices, and documents from being scattered and lost, theOffice is conducting investigations to continue improving thecollection, sorting, and preservation of articles and improve themethods and environment for displaying them. In cooperation
with Mizusawa Campus and Nobeyama Campus, the Officealso established the basic concept for the NAOJ Museum(tentative name) including both facility opening efforts andarchive works.
The Office sponsored the International Symposium on
the NAOJ Museum for 3 days, September 27-29, 2015, at
Mitaka Headquarters. This symposium summarized theresearch results of the “Forming an International Space forLearning Based on Research in the Natural Sciences” Project(Discretionary Budget of the Head of National Institutes of
Natural Science, provided from FY 2010 to FY 2015). It wasalso planned with the goals of domestic and international
publicity and exchanging opinions about the “NAOJ Museum
Concept Plan” focusing on the newly created limited time office“Museum Project Office” within the Public Relations Center.
The symposium received support from the Nonprofit Public
Organization: Foundation for Promotion of Astronomy. Ninetyfour guests from 9 countries (China, South Korea, Thailand,
Indonesia, Germany, Netherlands, Portugal, U.S.A., and Japan)
attended the event in person while 7 people in 6 locations inJapan and overseas (Mizusawa, Nobeyama, Okayama, Subaru
Telescope Summit Facility and Hilo Base Facility, Indonesia,
and U.S.A.) participated via the TV conference system. The
results of the 3 days of discussion are summarized in “TheMitaka Declaration.” In addition, there were indications thatthe consensus among all participants regarding the NAOJ
Museum Plan was that it should aim to be open by 2020.
Proposed at the initiative of the participants, “The Mitaka
Declaration”is addressed to NAOJ and JAXA, urging themto change their copyright r ules regarding astronomical
images, videos, etc. to be more generous, in line with otherorganizations such as NASA and ESO/ESA.

7. Library Unit
The Library Unit collects and sorts scientific journals andbooks in order to make them available for the research andstudy of NAOJ researchers and students. In recent years, withthe continuing digitalization of scientific materials, the portionof the materials in electronic format has increased.
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 2015, 323 non-NAOJ personnel came to use
the Library. Also for researchers and students belonging to

II Status Reports of Research Activities

105

other organizations, we loan books or provide photocopies via
the institute’s library. In FY 2015, photocopies or loans were
provided in a total of 86 cases.
Important documents, especially those originating from theEdo Era Tenmonkata (Shogunate Astronomer), are preserved
while taking into account the environment of a specialist
library. Images of some of the important documents areavailable to the public on the Library Unit homepage.
During the Mitaka Open House Day festivities in October,part of the Mitaka Library is opened to the public so thatpeople can freely examine the documents, focusing primarily
on documents which appeal to the general public and younger
age groups.
The number of books and journals owned by Mitaka
Library and each observatory and the condition of continuing
NAOJ publications are published in Section XI Library,
Publications.

8. Publications Office
The Publications Office continued its activities in planning,
editing, and printing NAOJ’s original materials for PR andpromotions. The following periodicals were also published thisyear:
• NAOJ Pamphlet (Japanese)• NAOJ Pamphlet (English)• NAOJ News, No. 261–No. 272 (April 2015–March 2016)• Annual Report of the National Astronomical Observatory ofJAPAN Volume 27 Fiscal 2014 (Japanese)• Annual Report of the National Astronomical Observatory ofJAPAN Volume 17 Fiscal 2014 (English)• R a d io Ast ronomy P ubl ic Relat ion s com ic “A l ma r’s
Adventure” (#5)
• NAOJ Publicity Poster Series (#2, #3)
Continuing from the previous year, in FY 2015 thePublications Office strove to strengthen its international
publication ability and digital publication ability. In particular,
as the first step in the production of an international edition of
the Rikanenpyo (Chronological Scientific Tables), an English
translation of the entire volume was created. Accompanying
this, a publishing partner was selected and a production
schedule was set, putting us on a concrete business plan.
In digitalization and the conversion of contents produced/
published (to be published) to digital format, the Publications
Office developed “NAOJ-Universal Multi-Publication System(NAO-JUMPS)” a system capable of automatically collecting
material about any arbitrarily chosen subject. The digital
data for the past 12 years of the ANNUAL REPORT OF
THE NATIONAL ASTRONOMICAL OBSERVATORY OF
JAPAN Research Highlights articles (approximately 1300
pages), and fixed layout NAOJ News articles (approximately
1300 pages) were input and test operations were conducted.
In addition, looking ahead we developed a general-purpose
electronic book distribution platform capable of distributing
to the general market via the internet, “NAOJ-Delivering106

II Status Reports of Research Activities

next-generation e-books (NAOJ-Deneb),” which will work inconcert with JUMPS in the future; and we started productionof the first book for NAOJ-Deneb. In normal business, theOffice produced and distributed the NAOJ pamphlets and the
ANNUAL REPORT OF THE NATIONAL ASTRONOMICALOBSERVATORY OF JAPAN. In the systematic production of
special editions with the goal of developing project outreachsupport in NAOJ News, extra copies of each of the special
editions (“ALMA Special Edition” September; “Okayama
Astrophysical Observatory/Search for Exoplanets Special
Edition” October; “CLASP Solar Observations Special Edition”
January; and “Solar Observatory Special Edition” March) 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. Other than periodicals, the 2016 calendar“Collection of ALMA Observational Images” (the 11th since2005) was created. In addition, like in other years the Officealso helped to create the poster for the Mitaka Special OpenHouse Event again this year, and support was also given to the
publication of the “Rikanenpyo, Chronological of Scientific
Tables).”9. International Astronomical Union Office for
Astronomy Outreach (IAU/OAO)In FY 2012 the International Astronomical Union (IAU)
and NAOJ exchanged a memorandum of understanding toestablish the IAU Office for Astronomy Outreach (OAO)
at NAOJ Mitaka Campus. In FY 2014 the IAU OAO wasestablished in the Public Relations Center. In FY 2015 theOffice primarily conducted International Year of Light 2015
“Cosmic Light” activities and the Name ExoWorlds Contest.
As advocated by the European Physical Society (EPS),
on December 20, 2013 the United Nations declared theInternational Year of Light (IYL2015). IAU also decided
to participate in the theme of Cosmic Light in March 2014.
Overall, IYL2015 was conducted in 94 countries with over
100 organizations participating. Under the overall broad
theme of “Light and Light-based Technologies” for theInternational Year of Light, IAU developed the stance of“Protecting the Darkness of the Night Sky.” IAU solicited
proposals from the entire world and selected the following 5
cornerstone projects: 1. Gallieoscope – 16,000 constructible
telescopes were distributed. 2. Light Beyond the Bulb - Over
30 countries participated, holding astrophotography exhibits inapproximately 675 locations. 3. EDU kit (Teaching Materials
Related to Cosmic Light) – These materials were used at morethan 140 events in more than 40 countries. 4. DARK SKY
METER App. – This free to use 2015 edition application
was downloaded 3,442 times, and 7,290 reports were filed. 5.
Quality Lighting Teaching Kit – 100 sets of this light pollution
study kit were shipped.
In addition OAO, in cooperation with the Japanese Society
for Education and Popularization of Astronomy, sponsored theJapanese closing ceremony of the International Year of Lighton January 11, 2016 at Tokyo University of Science. There werea total of 95 participants, including the 15 oral presentations,
16 poster presentations, and 17 activity report power point
presentations. In addition, in cooperation with the Outreachand Education Office and the Office of International Relations,on March 8, on the occasion of the March 9 Indonesia solar
eclipse, the Office conducted a solar eclipse viewing workshop
at SMK Negeri 2 (Technical Collage) Ternate City, Indonesia,
for a total of 500 on-island school teachers and students.
As part of the Name ExoWorlds Contest, 644 groups (166groups in Japan) registered in the worldwide call for group
registration (deadline June 1, 2015). The 20 planetary systems
to be named this time were chosen by a vote of the registeredorganizations. The planetary system names proposed by theregistered groups were accepted until June 15 of the same year;
247 naming proposals were submitted from 45 countries. The
proposals were received and a web election where everyone
could vote was held from August 11 to October 31; 573,242
votes were cast from 182 countries. (A total of 5,411 votes were
cast from Japan, 0.94 % of the total.) The results of this naming
were published on December 15. Excluding tau Bootis (where
the highest scoring name didn’t meet the naming guidelines),
19 planetary systems (14 stars and 31 planets) had names
decided.
I n a d d it io n , OAO c o n d u c t e d t h e d e velo p m e nt ofcooperative relations with National Outreach Contacts (NOC)(outreach facilitators in each country); construction of a
network between skill-holders, including amateur astronomers
and astronomy clubs, for the advancement of astronomy
education; establishment and maintenance of a database ofworld astronomy clubs, observatories, and research institutions;production of information distribution media, such as the
IAU Newsletter, pamphlets, videos, etc.; the management of
IAU’s social media; and cooperation for NAOJ’s international
relations and education and outreach activities.

II Status Reports of Research Activities10718. Division of Optical and Infrared Astronomy
1. Overview
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 to launch new projects as necessary.
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 and Infrared 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 wasconstructed.
The Division of Optical and Infrared Astronomy oversees
OAO (Okayama Astrophysical Observatory) and Subaru
Telescope (C Projects); the TMT-Japan (TMT-J) Project Officeand the Gravitational Wave Project Office (B Projects); and the
JASMINE Project Office and the Extrasolar Planet Detection
Project Office (A Projects). The Division and the Projects carryequal weight in organizational terms. Almost all NAOJ members
in optical- and infrared-related fields have positions in the
Division and engage in either the Division or one of the A, B, or
C Projects. At times, they may also have concurrent positions inother projects. The primary staff of the Division of Optical andInfrared Astronomy in FY 2015 consisted of two professors, four
assistant professors (including one specially appointed assistantprofessor), and three JSPS research fellows.
The Division coordinates educational, research, andadministrative activities for Subaru Telescope Mitaka Officeand Extrasolar Planet Detection Project Office. Since personnel
transfer often occurs within the Division of Optical and Infrared
Astronomy, the Division plays an increasingly important rolein coordinating between Subaru Telescope and 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, 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.

2. Observational Research(1) Observational Research Using Various Types of Telescopes
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; the108

II Status Reports of Research Activities

structure and evolution of the Milky Way; stellar spectroscopy;
solar system bodies; and the search for exo-planets. A surveyof high-z quasars was conducted in the survey data of Hyper
Suprime-Cam (HSC) on the Subaru Telescope. Ionized hydrogenclouds around a nearby star-burst merger were observed, andthe investigation into the merging history and gas ejection was
published. The search for extrasolar planets continued using
direct imaging methods. In cooperation with researchers inuniversities using the Optical and Infrared Synergetic Telescopesfor Education and Research (OISTER) network, observational
studies were conducted on transient objects and moving objects,
which include Gamma-ray bursts, supernovae, X-ray novae,
novae, dwarf novae, and Near-Earth Objects.
(2) International Cooperative Observational Research
The Division also engages in international collaborative
studies with overseas researchers. A study on a companion dwarf
galaxy was conducted with researchers in the USA, France, andSpain. The galaxy was found by chance in data acquired forstudying star formation in the outer regions of nearby galaxies.
The site survey in western Tibet continues in cooperation with
the National Astronomical Observatories, Chinese Academyof Sciences (NAOC). Discussions for the site assessment andconstruction of a telescope were held with researchers of NAOC,
the Purple Mountain Observatory and Hiroshima University.
Installation work of the NDU (Notre Dame University-Louaize
in Lebanon) 60-cm telescope, which was previously used atGeisei Observatory, Kochi Prefecture and refurbished by NAOJ
were supported.
(3) Research Using Archives
The celestial map on the ceiling of the stone chamber of theKitora Tumulus was analyzed in detail. Studies of astronomical
phenomena based on old ephemerides and other documents
continued. A statistical study on Ultra Diffuse Galaxies in
the Coma Cluster was conducted using archive data from theSubaru Telescope. The study of the host galaxies of active
galactic nucleus (AGN) using SDSS imaging/spectroscopy data
continued. The catalog of Kiso Ultraviolet-excess Galaxies(KUG) was updated using recent image surveys such as SDSS.
The results were opened to the public. Digitization of Kiso
Schmidt plates was also started.

3. Observational Instrument Development
The effect of the environment inside the dome on seeing sizeat the Subaru Telescope has been studied through collaboration
with Chofu Aerospace Center of JAXA (Japan Aerospace
Exploration Agency), Tokyo Denki University, and RIKEN. A
fluid calculation and a water-flow experiment were performed,
and the procedure to compare the results with the data from theSubaru Telescope environment sensors in the dome has been
investigated. Analysis of the ghost images of bright stars in theSubaru prime focus camera was conducted and a presentation
was made about correction methods. Commissioning of thetelescope at Hosei University and their observations using it
were supported.

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 supported the Subaru Autumn School co-hosted with
Subaru Telescope and Astronomy Data Center; and Subaru
Telescope observation classes.

every day throughout the year. In December, we held the annual
workshop of the Division of Optical and Infrared Astronomy
so that staff members and graduate students can understandthe current studies and interests of each other. The Divisionparticipated in the “Fureai Astronomy” project, dispatchinglecturers to various schools around the country, providing pupils
at elementary and junior high schools with opportunities to learn
about and appreciate astronomy.

5. Research Environment Maintenance
The Division manages the printers and rented multi-function
photocopiers in the Subaru Building; teleconferencing systems
on the second and third floors; sub-networks; and data backup
servers for Subaru Telescope Mitaka Office as part of its efforts
to maintain the research environment. The Division maintains
the web servers and their contents, and also gives assistance forsetting-up computers for new administrative supporters.

6. Planning of Next-generation Large-Scale
Projects
The Division is engaged in planning post-Subaru large
projects in optical and infrared astronomy, such as TMT and the
JASMINE series. A framework for collaboration between ISAS/JAXA (Institute of Space Astronautical Science) and NAOJ also
needs to be established. The preparation for the assessment of
new infrared detectors has started.

7. PR, Outreach, and Discovery of New
Astronomical Objects
The Division cooperates with the Public Relations Center insupporting matters related to the discovery of new astronomical
objects and PR/outreach activities such as publications and press
conferences related to Subaru Telescope research results. The
Division actively participates in a special public event held at
Mitaka Campus (Mitaka Open House Day).

8. Educational Activities
The Division of Optical and Infrared Astronomy provides
postgraduate education to 23 graduate students from the
Graduate University of Advanced Studies, the University ofTokyo, Hiroshima University, Tokyo University of Agriculture
and Technology, Nihon University, International Christian
University, and Hosei University. Division staff members madeactive contributions to seminars and self-directed studies. Since
April 2015 we have held a 30-minute seminar in the afternoon

II Status Reports of Research Activities10919. 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, which promotes
radio astronomy research to harmonize these radio astronomy
projects. The research themes of the Division of Radio
Astronomy are represented by keywords such as Big Bang, early
Universe, galaxy formation, black holes, galactic dynamics, starformation, planetary system formation, planets and satellites, theMoon, the evolution of interstellar matter, and the origin of lifein the context of the evolution of the Universe. Radio astronomy
unravels mysteries and phenomena in the Universe through radio
waves, which are invisible to human eyes. The detailed research
results are reported in each project’s section and in the researchhighlights. The Radio Astronomy Frequency Subcommittee has
been established within the division, engaging in discussions onprotection against artificial interference generated by electricalequipment, which causes major obstacles in radio astronomical
observations.

are free from artificial interference and to raise public awarenessof the importance of the 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 within Japan and internationally by the International
Telecommunication Union (ITU) Radiocommunication Sector(ITU-R) of the United Nations. As part of the activities for FY
2015 the Subcommittee took an active role in formulating theopinion of the Japanese radio astronomical community (onbehalf 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.

1. Radio Astronomy Frequency Subcommittee(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. New operations involving wireless communications
have increased following the Great East Japan Earthquake in2011, resulting in an increase in radio interference.
- Development of new radio applications. The ultra-wideband (UWB) technology does not require an operator license
because it is operated at low-levels and wide bandwidths. On
the other hand, there has been a rapid increase in demand forhigher frequencies. For example, 76 and 79 GHz automotive
radars are being introduced, aiming to reduce car accidents
resulting in injury or death. And, transportation of highspeed and high volume data, such as HDTV quality video,
is becoming possible through 60 GHz radio transmission
systems.
- Reassigning of vacant frequency bands resulting fromenhanced efficiency in radio use. The digitization of television
broadcasting has created vacant frequency bands, which havebeen reassigned for mobile phones and other applications.

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. The fact is that four
Novel Prizes have been awarded to achievements made in thefield of radio astronomy.
Just as light pollution from artificial light sources is an
obstacle in optical observation, artificial radio interference
generated by the electronic devices which surround us is amajor obstacle in radio observations. Breathtaking advancement
has been achieved in wireless communication technologies inrecent years, and wireless commercial products such as mobile
phones, wireless LANs, and automotive radars are widelyused. The areas of radio applications will further expand in
the future owing to its ubiquitous nature. But because of its
unique capabilities, compatibility among various radio services,
including both active and passive ones, will become a serious
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

110

II Status Reports of Research Activities

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. Unwanted out-of-band signals(spurious signals), even extremely faint ones, can have a chanceof 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; 1600 MHz mobile satellite phones
used in emergencies, where the observation of pulsars and thelike are affected; a number of new UWB wireless applications
used by logistics and manufacturing industries, where
geodetic observations are affected; and high-speed power line
communications (PLC), where decameter-band observations areaffected. 79 GHz automotive radars around Nobeyama Radio
Observatory will cause deterioration in its observation results,
or rather tend to make its observations impossible in the near
future. Although radio astronomy observations in the 60 GHz
band are not common because of the high rate of absorption in
the atmosphere, the 60 GHz system must be watched closely
because its second harmonic can have adverse 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 2015, the Subcommittee participated in the ITU-R
WP7D meetings held in May, the WP1A meeting in June, andWRC-15 meeting in November in Geneva.WRC-15 resolved
to provide a wider regulatory option for realizing global flighttracking of commercial airplanes and allocated additionalfrequency bands to the Maritime-mobile satellite service and theEarth exploration-satellite (active) service.
One major point of contention in WRC-15 was additionalfrequency band allocation to international mobile telephones(IMT). Finally, an agreement was reached for possible allocationof some frequency bands in 30–50 GHz to IMT at WRC-19 tobe held in 2019. Also, WRC-15 agreed to add the allocation ofactive services at frequencies above 275 GHz to the WRC-19
agenda.

(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 for the MIC’s authorization with wirelessoperators who generate radio interference, and promotion
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
held to organize domestic tactics in preparation for international
conferences, defining Japan’s positions on various wirelessissues. Other MIC-related meetings provide opportunities fordiscussing the radio application technologies related to MIC’s
wireless policy, and for negotiating with wireless operators on
interference issues under MIC authorization. Negotiations directly
affecting the protection of radio astronomy observations havebeen conducted concurrently to dealing with the interference
problems related to societal and technological trends.
Several examples of the interference problems discussed in
section (2) above are given below.
For 24 GHz automotive radars, new regulations have been
prepared to make an automatic turn-off function a mandatory
standard feature so that the device is disabled upon reachingcertain areas around radio observatories.
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 automobile radars. Of
particular concern are the possible effects of interference fromthese 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 is based in Chile andinvolves 66 high-performance radio telescopes at an altitude of
5,000 m. Since automotive radars are highly relevant to humanlife safety, negotiations have been conducted with carefulanalysis in order to 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 isnear the 22 GHz radio astronomy band, which is important forwater maser observation. The radio signals from the satellite
approach the ground from outer space. Their detrimental effects
need to be alleviated with a filter at the output stage of thesatellite. In FY 2015, the NHK Science & Technology ResearchLaboratories developed a prototype bandpass filter to suppress
spurious signals to an acceptable level. NHK plans to verify
its performance further on a future satellite set to launch in
December, 2017.
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

II Status Reports of Research Activities

111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.
To further improve disaster measures, the MIC will evaluate
the approval of a U.S. mobile satellite phone service using 1.6
GHz signals (Earth to space) in FY 2016. Its out-of-band signal,
however, may affect the adjacent RAS band observing OH
masers. In FY 2015, the Subcommittee started evaluation of new
operating conditions proposed by Global Star Inc. (U.S.).
The Cabinet Office of the Japanese government is planningto launch three (#2–#4) Quasi-Zenith Satellites in FY 2017
to improve the accuracy of the radiolocation service. Since
there was a risk that the message communications signal in the
2.2 GHz band could affect the VLBI observations, sharing andcompatibility studies were performed by the Subcommittee
and Cabinet Office. They found mutually agreeable operating
conditions and signed a compatibility study confirmation
document.
Additionally, radio astronomy observations could be
adversely affected by some of the new wireless technologies:
high speed image data transmissions from drones to ground
receivers, wireless power transmission (WPT) for electricvehicle energy charging (non-beam), WPT from spacebased solar power satellites to Earth (beam), and so on. The
Subcommittee continues to monitor their progress and shares
this information with related radio astronomers.
M o r e o v e r, t h e S u b c o m m i t t e e e n g a g e s i n m a k i n gapplications to the MIC, requesting frequency protection for
NAOJ telescopes, in addition to those owned by the Japanesecommunity of radio astronomers on their behalf.
The collection of actual interference cases at every
observatory 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 material for the general public.
As optical astronomers are engaging in protection of theirobservation environment against artificial light, we, radio
astronomers, are making the same efforts for the sake ofcontinuing observations in radio astronomy in coming ages.

112

II Status Reports of Research Activities20. Division of Solar and Plasma Astrophysics
The Division of Solar and Plasma Astrophysics is mainly
made of staff members from the Solar Observatory, the Hinode
Science Center, and the Solar-C Project Office. It conducts
research on the Sun in close coordination with these projects.
An NAOJ fellow and graduate students supervised by the staffof the above-mentioned projects also belong to the Division.
All of the permanent staff of these projects is affiliated with theDivision.
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.

Research-Experience Tour” in March for undergraduate students;
about ten students visited solar-related research organizations
and experienced 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. Several plans arealso under consideration for future ground-based telescopesthat would involve collaborations with East Asian countries andPeru.

1. Research in Solar Physics
NAOJ fellow S. Toriumi published two papers in refereed
journals as lead author. Both of them are on the energy release
phenomena occurring suddenly and periodically at lightbridges in sunspots. In these papers he (1) revealed the energy
release mechanism based on observational data taken with
Hinode and IRIS, and (2) elucidated the cause of the periodicity
based on numerical simulations. He also has been promoting
collaborative research with international partners; he invited
Dr. M. Cheung of the Lockheed Martin Solar and AstrophysicalLaboratory as a guest associate professor, and organized two
scientific meetings including Dr. M. Cheung as a guest.
The Division has a seminar (on Friday afternoon, roughly
twice a month) whose speakers are from both inside and outsideof the Division. This year's organizers were K. Watanabe and S.
Toriumi.

2. Educational Activities
The teaching staff of the Division supervised three graduate
students from the Graduate University for Advanced Studies(SOKENDAI). Among them, Gabriel Giono obtained a Ph.D. in
March. The Division, in cooperation with Kyoto University andNagoya University, supported the annual “Leading-edge Solar

II Status Reports of Research Activities113

21. Division of Theoretical Astronomy
1. Overview

2. Current Members and Transfers

The Division of Theoretical Astronomy (DTA) engaged inresearch activities in FY 2015 aimed at achieving internationally
outstanding research results in both quality and quantity, basedon the following four goals that were set by the NAOJ Board:

In FY 2015, the dedicated faculty of the Division ofTheoretical Astronomy included two professors, two associate
professors, and four assistant professors. In addition, one adjunctprofessor and one adjunct assistant professor concurrently holdprimary positions at the Center for Computation Astrophysics.
In addition to these research and educational members, theDivision was served by five project assistant professors, one
project research associate, one JSPS fellow, three EACOA
fellows, and one administration associate who gave full support
to all activities of the Division. Among these members, Michiko
Fujii, a specially appointed Associate Professor, transferred
to an associate professor position at the University of Tokyo;
and Tomoya Takiwaki, an assistant professor, joined us fromFebruary in 2016.

- Advance world class cutting-edge theoretical research.
- Pursue theoretical astronomy research, particularly in areas thatutilize the NAOJ supercomputer or large-scale observational
instruments to give further insight into the development of new
observational instruments.
- Encourage collaborations among researchers in Japan andstrengthen domestic theoretical astronomy research.
- Invigorate postgraduate education.
The Division handles a wide variety of themes in theoreticalastronomy research, addressing a diversity of hierarchicalstructures of the Universe in terms of formation and evolution
processes, dynamics, and the physical state of matter. This
research covers a span from the early Universe to galaxies,
stars, planetary formation, activities of compact objects, andplasma phenomena in astronomy and astrophysics. The Divisionof Theoretical Astronomy aims to facilitate Japan’s highcompetitiveness on the international plane through continuous
production of world leading research results and offers asuperb research environment as a base for theoretical researchaccessible to researchers in Japan and overseas. It has accepted
a wide range of both Japanese and international researchers asvisiting professors, visiting project research fellows, and longterm research fellows who actively engage in various research
projects in the Division. In particular, the Division has fosteredresearch developments to create a powerful research centerfor young researchers and is actively engaged in personnel
exchanges with many universities and research institutes. The
Division’s full-time professors, associates, assistants, and project
assistant professors, 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, the Graduate Schoolof Ochanomizu University and the Graduate School of Shizuoka
University; joint research with observational astronomy using
satellite campuses observing various frequency bands such as
the Subaru Telescope, ALMA, and Nobeyama radio telescopes;
and interdisciplinary research with the physics of elementary
particles and atomic nuclei. In addition, the Division actively
organizes numerous cross-disciplinary international conferences,domestic meetings, and seminars for the fields of theoreticalastronomy and astrophysics, observational astronomy, andexperimental physics. The Division also leads research activities
in various fields related to astronomical science.

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II Status Reports of Research Activities

3. Research Results
The number of research papers in listed Section IV,
Publications, published by the Division member(s) as author(s)or presenter(s) are listed below. Categories with fewer than 10
publications have been omitted.
- Peer-reviewed papers in English: 89- Papers in English (conference proceedings, non-reviewed
papers, etc.): 14- Reports in English (talks at international conferences): 65- Reports in Japanese (talks at national meetings, etc.): 45
Some of the research results are presented in the researchhighlights listed at the beginning of this report. The following
highlights include research in which the Division members tookleading roles:- Polarization Structure of Filamentary Clouds (Kohji Tomisaka)- Rapidly Rising Transients from Subaru/HSC Transient Survey(Masaomi Tanaka, et al.)
- A New Multi-energy Neutrino Radiation-Hydrodynamics
Code in Full General Relativity and Its Application to theGravitational Collapse of Massive Stars (Tomoya Takiwaki, etal.)- Enrichment of r-process Elements in Dwarf Spheroidal
Galaxies in Chemo-dynamical Evolution Model (Yutaka Hirai,
et al.)- Physical Conditions of Supernova Ejecta as Viewed from theSizes of Presolar Al2O3 Grains (Takaya Nozawa)- Pitch Angle of Self-Gravity Wakes in Dense Planetary Ring
(Shugo Michikoshi, et al.)
- Initializing relativistic velocity distribution functions in plasma
simulations (Seiji Zenitani, et al.)- All-sky simulations of gravitational lensing (Masato Shirasaki,
et al.)

- A Numerical Scheme for Special Relativistic Radiation
Magnetohydrodynamics Based on Solving Time-dependent
Radiative Transfer Equation (Ken Ohsuga, et al.)- Radiation Drag Effects in Black Hole Outflows from Supercritical Accretion Disks via Special Relativistic Radiation
Magnetohydrodynamics Simulations (Hiroyuki Takahashi, etal.)- Nuclear Fission and Solution of r-Process Underproduction
Problem (Shota Shibagaki, et al.)- Effect of Stellar Encounters on Comet Cloud Formation (Arika
Higuchi, et al.)
- R-process Nucleosynthesis in the MHD+neutrino-heated
Collapsar Jet (Toshitaka Kajino, et al.)- Constraints on the birth of the universe and origin of cosmic
dark flow (Toshitaka Kajino, et al.)- Pion Production from Proton Synchrotron Radiation under
Strong Magnetic Fields in Relativistic Quantum Approach(Toshitaka Kajino, et al.)- Possible Evidence for Planck-scale Resonant Particle
Production during Inflation from the CMB Power Spectrum(Toshitaka Kajino, et al.)- Constraints on Pre-inflation Fluctuations in a Nearly Flat Open_CDM Cosmology (Toshitaka Kajino, et al.)- Universality of the Supernova r-Process and Radioactive
Nuclei (Toshitaka Kajino, et al.)The following research results were released on the
Division’s website (http://th.nao.ac.jp/index_en.html) as researchhighlights:- Conversion of Hadronic Matter to Quark Matter in NeutronStars (Shun Furusawa, et al.)- New Model on the Origin of the Heavy Elements: Solving theUnderproduction Problem of the r-Process (Shota Shibagaki,
Toshitaka Kajino, et al.)- Galactic Spiral Arms by Swing Amplification (Shugo
Michikoshi, Eiichiro Kokubo, et al.)
- Large-scale structure of magnetic reconnection by means ofkinetic simulations (Keizo Fujimoto, et al.)- Origin of r-process elements in galactic chemodynamical
evolution (Yutaka Hirai, Michiko Fujii, Toshitaka Kajino, etal.)- Pitch Angle of Self-Gravity Wakes in Saturn’s rings (Shugo
Michikoshi, Eiichiro Kokubo, et al.)- Probing the Stellar Explosions with Presolar Grains (Takaya
Nozawa, et al.)- All sky simulations of gravitational lensing (Masato Shirasaki,
Takashi Hamana, et al.)- Polarization Structure of Magnetically Supported Molecular
Filaments (Kohji Tomisaka)- Great Progress towards the Origin of R-process (Shota
Shibagaki, Toshitaka Kajino, et al.)- Loading relativistic velocity distributions in particle
simulations (Seiji Zenitani, et al.)- The initial mass function of star clusters (Michiko Fujii, et al.)- Quantum theoretic approach to in-medium effects on theneutrino scattering (Toshitaka Kajino, et al.)

4. Domestic Collaborations
The Division of Theoretical Astronomy played leading roles
in organizing the following domestic conferences:- National Meeting on Galactic Evolution 2015, Sakata-Hirata
Hall at Nagoya University, June 3 – 5 in 2015.
- UKAKUREN (Japan Forum of Nuclear Astrophysics) Meeting,
NAOJ Mitaka Campus, February 22 – 24 in 2016.
- Winter School on Nuclear Matter in Neutron Stars investigatedby Experiments and Astronomical Observations (Grant-In-Aid
for Scientific Research on Innovative Areas), NAOJ Mitaka
Campus, February 24 – 26 in 2016.
- National Meeting on Frontier of Cosmic Plasma; beyond
Heliosphere, Solar-Terrestrial Environment Laboratory at
Nagoya University, March 2 – 4 in 2016.
- TDA Symposium on Time-domain Astronomy, NAOJ Mitaka
Campus, March 4 – 5 in 2016.
- National Meeting on Frontier and Perspective of the Researchof Magnetic Reconnection, NAOJ Mitaka Campus, March 28– 29 in 2016.

5. International Collaborations
Toshitaka Kajino performed duties in the following posts:
review panel member of the Institute of Physics (Journal of
Physics G.); international referee for the Science, Technology
and Innovation Council of Canada; international associate for
the European Centre for Theoretical Studies in Nuclear Physics
and Related Areas (ECT*); and international referee for the
Swiss National Science Foundation (SNSF).
The Division of Theoretical Astronomy played leading roles
in organizing the following international conferences:- 3rd DTA Symposium on The Origins of Planetary Systems:
from the Current View to New Horizons, NAOJ Mitaka
Campus, June 1 – 4 in 2015.
- International Symposium on Physics and Astronomy of
Neutron Stars and Supernovae, NAOJ Mitaka Campus, June
22 – 23 in 2015.
- Star Formation Workshop 2015, NAOJ Mitaka Campus, June
29 – July 1 in 2015.
- The 8th meeting on Cosmic Dust, Chiba Institute ofTechnology Sky Tree Campus, August 17 – 21 in 2015.
- Symposium on Hierarchy and Holism in Natural Science,
NAOJ Mitaka Campus, February 5 – 6 in 2016.

6. Educational Activities
The basic information for the adjunct lecture-ship activities
of research and education staff at universities and graduate
schools is listed in Section III. The lecture subjects are listed
below to supplement that information.
Eiichiro Kokubo: “Planetary Science” at the University

II Status Reports of Research Activities

115

of Tokyo; “Origin and Structure of Planetary Systems” at the
University of the Ryukyus.
Toshitaka Kajino: “Lectures on Fundamentals of Theoretical
Astronomy” 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
School of the University of Tokyo.
Takashi Hamana: “Geology” at the Tokyo University ofAgriculture and Technology.
Keizo Fujimoto: “Computational Science and Genesis of
Nature” at the Graduate University for Advanced Studies.
Eiichiro Kokubo delivered SSH lectures entitled “Simulation
Astronomy” and “Cosmo-science” at Hibiya High School andKanazawa Izumigaoka High School, respectively.

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 thisyear:
Eiichiro Kokubo; “Origin of the Solar System – Kyoto
model” at Chushiro Hayashi Memorial Lecture; “What is
Pluto?” at Ikebukuro Community College; “Hometown ofPlanets” Hiroshima University and Chiba University; and “Earthin the Universe” at Asahi Culture Center Fukuoka.
Toshitaka Kajino; “Frontiers in Cosmo-nuclear astrophysics”
at Osaka City University, and “Introduction to Element Genesis:
The birth of the Universe and origin of matter, elements in thecosmos” at Asahi Culture Center Yokohama.
Seiiji Zenitani; “The Importance is Invisible: looking at
the explosive phenomena in Earth’s backyard” at the National
University Corporation Tsukuba University of Technology.

8. Awards
Masaomi Tanaka received a 2015 Research Encouragement
Award of the Astronomical Society of Japan.

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 inastronomy and astrophysics and also as an international research
institution by providing an excellent research environment.
It engages in various joint research projects with visiting
researchers from overseas, with the help of Grants-in-Aid
for Scientific Research, government subsidies for operating
expenses, and the NAOJ budget for visiting research fellows
and others. The main international visitors to the Division in FY

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II Status Reports of Research Activities

2015 are listed below:
Myung-Ki Cheoun (Soongsil University, South Korea)
Tjarda Boekholt (Laiden Observatory, Netherland)
Grant J. Mathews (University of Notre Dame, U.S.A.)
Motohiko Kusakabe (University of Notre Dame, U.S.A.)
Zhi-Yun Li (University of Virginia, U.S.A.)
Wing-Kit Lee (Academia Sinica, Taiwan)
Anaelle J. Maury (Saclay Nuclear Research Centre, France)
John J. Tobin (Laiden Observatory, Netherland)
Akif B. Balantekin (University of Wisconsin–Madison, U.S.A.)
Michael A. Famiano (Western Michigan University, U.S.A.)
Ghil-Seok Yang (Soongsil University, South Korea)
Eun-ja Ha (Soongsil University, South Korea)
Kyun-jin Kwak (Ulsan National Institute of Science &Technology, South Korea)
Yichen Zhang (University of Chile, Chile)
James M. Lattimer (State University of New York, U.S.A.)
Friedrich Thielemann (University of Basel, Switzerland)
Yamac Deliduman (Mimar Sinan Fine Arts University, Turkey)

22. Office of International Relations
The Office of International Relations, along with performing
information-gathering/–provision and other activities related tointernational research and educational cooperation, strives topromote and facilitate further internationalization at NAOJ by
providing the various services and environments required for
multi-cultural researchers and students to engage in researchand educational activities in cooperation with each other.
Specifically, the office’s main activities include supportinginternational collaborative projects; liaising with overseas
astronomical research organizations; gathering and providing
information on international activities; offering support for
hosting international conferences, workshops, and seminars;
providing support for visiting international researchers andstudents; and assisting Japanese universities and researchorganizations in international partnerships. In FY 2015 theOffice’s working scheme changed and the Office started working
closely with the Executive Advisor to the Director General in
charge of international research coordination.

1. International Collaborative Project Support
The Office gathers and provides information necessary
for pursuing international research collaborations on its own
initiative. It also serves as a liaison point for international
activities; engages in international agreements or provides
support for doing so; and accumulates procedural andadministrative knowledge, through consultations orinvestigations on individual cases, to enter into and implement
collaboration with overseas universities or research institutions.
Other matters handled by the Office include administrative
coordination in approval processes to sign agreements andmemoranda for international collaborations, support for signingceremonies, and export security control for the export ofgoods or transfer of technology. In FY 2015, ten international
agreements, new and renewed, were signed including ones
under the name of NINS. In the area of security export control,
the activities included review and processing of 37 cases andsecurity export control briefings for improving the knowledge
and awareness of NAOJ staff held seven times at Mitaka,
Mizusawa, Nobeyama, and Okayama with more than 100
attendees.

2. Liaison Work for Overseas Astronomical
Research Organizations
The Office of International Relations organized the annual
directorate meeting of the East Asian Core Observatories
Association (EACOA) on October 11, 2015 at Incheon, South
Korea. The signing ceremony for the renewed Memorandumof Understanding (MOU) of EACOA was held at the meeting.
This MOU extends the term of EACOA activities, including the
EACOA postdoctoral fellowship program, for another 5 years.
The four institutions forming EACOA include NAOC (China),

NAOJ (Japan), KASI (South Korea), and ASIAA (Taiwan). The
Office also coordinated with the other 3 institutes for selectionof 2016 EACOA postdoctoral fellowship program. The officealso cooperated with NAOC for the East Asia Ground-based
Telescope Construction Sites Survey. In addition, it presented
NAOJ's projects and research results by displaying an exhibit atthe 29th IAU General Assembly held August 3 - 15 at Honolulu,
Hawai`i in the USA. Furthermore, the office supported theactivities of the IAU Office for Astronomy Outreach. The Officeof International Relations also cooperated with EACOA member
organizations in supporting the activities of the IAU Office for
Astronomy Development (OAD).

3. Support for Hosting International Research
Conferences, Workshops, and Seminars
The Office of International Relations offers support forthe planning and implementation of international research
conferences, workshops, and seminars hosted or supportedby NAOJ. The work involves consultation and responses
to inquiries regarding administrative issues. The office alsooffers advice about organizations or individuals to contact as
appropriate, coordinates between organizations, and gathering
relevant information. In FY 2015 the office supported
international research conferences and other conferencesby preparing the documentation required for Japanese visa
applications for 50 foreign participants in total.

4. 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 forforeigners living in Japan. It offers support, on-site if required,covering various matters such as administrative procedures atmunicipal and other governmental offices; finding and moving
into an apartment; various other procedures and applications
for starting up a new life; consultation on shopping, children’s
education, health and other subjects; and gathering/providing
useful information relating to everyday life. The Support Desk
has been highly appreciated by users. Besides daily life matters,
the office expanded its activities as an intermediary between
administrative staff and non-Japanese speaking researchers bytranslating/interpreting in-house procedures, applications andnotices. The office continued the Japanese language lessons,
helping foreign members of NAOJ to acquire beginner level
capability, for FY 2015 with E-learning features added to theclassroom lessens. Including renewals, support was given to 37
visa applications: 8 for staff and family members, 13 for invitedresearchers, and 16 of visitor/long stay researchers.

II Status Reports of Research Activities

1175. Assistance in International Partnerships
Involving Japanese Research Organizations
The Office of International Relations assists universities andother educational and research organizations in Japan to engage
in international partnerships. It also liaises with the International
Strategy Headquarters and the International Cooperation Officeat NINS to coordinate international collaborations. The Officeoversaw the Optical and Infrared Synergetic Telescopes for
Education and Research (OISTER) project conducted by OAO,
Ishigakijima Astronomical Observatory, and nine Japanese
universities.

118

II Status Reports of Research Activities

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 Observatory
NAOJ Chile Observatory
Center for Computational Astrophysics
Hinode Science Center

Director General(B Projects)

Vice-Director General (on General Affairs)

Gravitational Wave Project Office
TMT-J Project OfficeVice-Director General (on Finance)
Director of Engineering
Director of Research Coordination(A Projects)

JASMINE Project Office
Extrasolar Planet Detection Project Office
RISE Project
SOLAR-C Project Office

Executive Advisor to the Director General

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
Administration Department

III Organization

1192. Number of Staff Members(2016/3/31)
Regular Employees
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
Fixed-term Employees
Full-time Contract Employees
Part-time Contract Employees

1
153
27
0
41
10
57
0
18
36
55
9
99
59
134

3. Executives
Director General
Vice-Director General
on General Affairs
on FinanceDirector of Engineering
Director of Research Coordination
Executive Advisor to the Director General120

III Organization

Hayashi, Masahiko
Watanabe, Junichi
Kobayashi, Hideyuki
Takami, Hideki
Gouda, Naoteru
Ogasawara, Ryusuke
Sekiguchi, Kazuhiro

4. Research Departments
Projects

Specially Appointed
Senior Specialist

Hayashi, Yusuke

C Projects

Specially Appointed
Senior Specialist

Ikeda, Hiroyuki

Specially Appointed
Senior Specialist

Momose, Rieko~2015.10.31

Specially Appointed
Senior Specialist

Oishi, Yukie

Specially Appointed
Senior Specialist

Sakamoto, Ken~2015.12.31

Subaru Telescope
Director
Professor
Professor
Professor
Professor
Specially Appointed
Professor

Arimoto, Nobuo
Arimoto, Nobuo
Mizumoto, Yoshihiko
Ohashi, Nagayoshi
Usuda, Tomonori
Renzini, Alvio

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

Aoki, Wako
Hayano, Yutaka
Hayashi, Saeko
Ichikawa, Shinichi
Iwata, Ikuru
Kashikawa, Nobunari
Kodama, Tadayuki
Miyazaki, Satoshi
Noumaru, Junichi
Takata, Tadafumi
Takato, Naruhisa
Takeda, Yoichi
Terada, Hiroshi
Iwashita, Hiroyuki
Furusawa, Hisanori
Imanishi, Masatoshi
Komiyama, Yutaka
Koyama, Yusei
Minowa, Yosuke
Nakaya, Hidehiko
Okita, Hirofumi
Onodera, Masato
Pyo, Tae-soo
Shirasaki, Yuji
Yagi, Masafumi
Tanaka, Masayuki

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

Bando, Takamasa
Tazawa, Seiichi
Kamata, Yukiko
Kurakami, Tomio
Namikawa, Kazuhito
Negishi, Satoru
Omata, Koji
Tamura, Tomonori
Uraguchi, Fumihiro
Sato, Tatsuhiro
Ichikawa, Kohei

Specially Appointed
Research Staff

Toshikawa, Jun

Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administration Department
Manager
General Affairs Section
Chief
Staff
Accounting Section
Chief
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH

Kawanomoto, Satoshi
Koike, Michitaro
Mineo, Sogo
Yamada, Yoshihiko
Yamanoi, Hitomi
Kuwata, Hitomi
Mochinaga, Chizuru
Noguchi, Masumi
Takamoto, Masami
Yamada, Narumi
Yoshida, Chie
Seto, Yoji
Seto, Yoji
Sugawara, Satoshi
Furuhata, Tomoyuki
Alpiche, Dex
Aoki, Kentaro
Aso, Yusuke
Balbarino, Michael
Berghuis, Jennie
Bergstrom, Andrew(Will)
Birchall, Daniel
Bulger, Joanna
Castro, Timothy
Clergeon, Christophe
Cook, David
Currie, Thayne
Doi, Yoshiyuki
Doughty, Danielle
Elms, BrianEndo, Mari
Fabricius, Maximilian
Ferre Mateu, Anna
Ferreira, James
Finet, Francois
Formanek, Keiko
Fujiwara, Hideaki
Fujiyoshi, Takuya

III Organization

121

122

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

Gaskin, Roberta
Gorman, William
Guthier, Debbie
Guyon, Olivier
Hasegawa, Andrew
Hasegawa, Kumiko
Hattori, Takashi
Helminiak, Krzysztof
Hopkins, James
Inagaki, Takeshi
Iwasaki, Alan
Jeschke, Eric
Jovanovic, Nemanja
Kackley, Russell
Kakazu, Yuko
Kim, Ji Hoon
Koshida, Shintaro
Koyamatsu, Shin~2015.06.03

RCUH
RCUH
RCUH
RCUH
RCUH

Kudo, Tomoyuki
Kyono, Eiji
Lee, Chien-Hsiu
Lemmen, Michael
Leonard, Alex
~2015.08.07

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

Letawsky, Michael
Lozi, Julien
Micheva, Genoveva
Morris, Marita
Murai, Rieko
Nabeshima, Yoshitake
Nakano, Wakako
Nakata, Fumiaki
Niimi, Yuka
Nishimura, Tetsuo
Otsuki, Noriko
Pathak, Prashant
Ramos, LucioRoth, Noriko
Saito, Yuriko~2016.03.08

RCUH
RCUH

Shubert, Kiaina
Singh, Garima~2015.11.04

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

Spencer, Robin
Sur, Ryoko
Tait, Philip
Tajitsu, Akito
Takiura, Koki
Tamae, Richard
Tanaka, Makoto
Tanaka, Yoko
Terai, Tsuyoshi
Thunell, Johnathan
Tomono, Daigo
Toyofuku, Ralph

III Organization

RCUH
RCUH

Tsang, Emiko
Wages, Keith~2015.11.27

RCUH

Walawender, Joshua~2016.02.05

RCUH
RCUH
RCUH
RCUH
RCUH
RCUH

Weber, Mark
Williams, Joshua
Winegar, Tom
Wung, Matthew
Yeh, Sherry (Chia-Chen)
Yoshiyama, Naomi

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

Tsutsui, Hironori
Fukui, Akihiko

Research Expert
Research Expert
Research Supporter

Kuroda, Daisuke
Maehara, Hiroyuki
Kamiya, Koki
~2015.09.30

Research Supporter
Administration Office
Administration Section
Chief
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Nobeyama Radio Observatory
Director
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
EngineerEngineerToda, Hiroyuki

Setou, Nobuyoshi
Katayama, Kumiko
Shibukawa, Hiroko
Yamashita, Ayako
Koyama, Shoji
Watanabe, Noriaki

Saito, Masao
Nakamura, Fumitaka
Saito, Masao
Kanzawa, Tomio
Kawashima, Susumu
Ishizuki, Sumio
Minamidani, Tetsuhiro
Umemoto, Tomofumi
Mikoshiba, Hiroshi
Handa, Kazuyuki
Miyazawa, Chieko
Miyazawa, Kazuhiko
Shinohara, Noriyuki
Kurakami, Tomio
Nishitani, Hiroyuki
Wada, Takuya

Specially Appointed
Research Staff

Kaneko, Hiroyuki

Specially Appointed
Research Staff

Miyamoto, Yusuke

Specially Appointed
Research Staff

Nishimura, Atsushi

Research Expert
Kinugasa, Kenzo
Research Expert
Maekawa, Jun
Research Expert
Oya, Masaaki
Research Expert
Takahashi, Shigeru
Research Expert
Tatamitani, Yoshio
Technical Expert
Nishioka, Makiko
Research Supporter
Arai, Hitoshi
Administrative Supporter Hatakeyama, Eiko
Administrative Supporter Ide, Hidemi
Consultant
Saito, Yasufumi
Research AssistantMatsuo, Mitsuhiro
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

Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Chief Engineer
EngineerEngineer
Specially Appointed
Research Staff

Honma, Mareki
Kobayashi, Hideyuki
Agata, HidehikoHanada, Hideo
Shibata, Katsunori
Sato, Katsuhisa
Hada, Kazuhiro
Hirota, Tomoya
Jike, Takaaki
Kameya, Osamu
Kono, Yusuke
Sunada, Kazuyoshi
Tamura, Yoshiaki
Asari, Kazuyoshi
Ishikawa, Toshiaki
Suzuki, Syunsaku
Ueno, Yuji
Hirano, Ken
Shizugami, Makoto
Kim, Jeoung Sook

Specially Appointed
Research Staff

Matsumoto, Naoko

Specially Appointed
Research Staff

Motogi, Kazuhito

Ide, Hiroko

Specially Appointed
Research Staff

Sakai, Nobuyuki

Administrative
Maintenance Staff

Kadoshima, Junko

Specially Appointed
Research Staff

Tazaki, Fumie

Administrative
Maintenance Staff

Kikuchi, MichikoSpecially Appointed
Research Staff

Wu, Yuanwei

Administrative
Maintenance Staff

Kikuchi, Tsuyoshi

Specially Appointed
Senior Specialist

Kanaguchi, Masahiro

Administrative
Maintenance Staff

Koike, Ikuko

Specially Appointed
Senior Specialist

Miura, Mitsuo

Administrative
Maintenance Staff

Kurane, Tsugeru

Specially Appointed
Senior Specialist

Nagayama, Takumi

Administrative
Maintenance Staff

Saito, Arayo

Specially Appointed
Senior Specialist

Oyama, Tomoaki

Administrative
Maintenance Staff
Administrative
Maintenance Staff

Tsuchiya, Junko

Administrative
Maintenance Staff

Yoshizawa, Usaji

Research Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Research Supporter

Hanayama, Hidekazu
Asakura, Yu
Sato, Kaori
Funayama, Hiroshi
Matsukawa, Yuki
Miyaji, Takeshi
Nishizawa, Akihisa
Yoshida, Toshihiro
Akiyama, Kazunori~2015.08.31

Accounting Section
Chief
Senior Staff
Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Mizusawa VLBI Observatory
Director

Shimizu, Hidetoshi
Iijima, Kunio
Kobayashi, Kazuhito~2015.07.31
Kodaira, Toshiko
Takasawa, Mitsue
Takemura, Miwako
Tokui, Chisato

Honma, Mareki

Research Supporter
Isono,Yoko
Research Supporter
Matsueda, Chika
Administrative Supporter Komori, Akiyo
Administrative Supporter Uekiyo,Hatsue
Administration Office
Deputy Manager
Hommyo, Susumu
General Affairs Section

III Organization

123ChiefStaff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Accounting Section
Chief
Chief

Hommyo, Susumu
Iida, Naoto
Kikuchi, Sachiko
Oizumi, Yuka
Sasaki, Mie

Specially Appointed
Associate Professor

Kawamura, Akiko

Specially Appointed
Associate Professor

Koda, Jin

Specially Appointed
Associate Professor

Nagai, Hiroshi

Ito, Hiromasa
Koseki, Tatsuya~2015.06.30

Specially Appointed
Associate Professor

Nakanishi, Koichiro

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

Kikuchi, Kenichi
Watanabe, Manabu
Ezawa, Hajime
Hiramatsu, Masaaki
Hirota, Akihiko
Kamazaki, Takeshi
Matsuda, Yuichi
Sawada, Tsuyoshi
Shimojo, Masumi
Takahashi, Satoko
Umemoto, Tomofumi
Akiyama, Eiji

Hanaoka, Yoichiro
Sakurai, Takashi
Hanaoka, Yoichiro
Suematsu, Yoshinori
Shinoda, Kazuya
Otsuji, Kenichi~2015.09.30

Specially Appointed
Assistant Professor

Hatsukade, Bunyo

Specially Appointed
Assistant Professor

Herrera Contreras,
Cinthya Natalia~2015.08.31

Specially Appointed
Assistant Professor

Miura, Rie

Hagino, Masaoki
Morita, Satoshi
Yaji, Kentaro
Nishino, Hideko
Sugimoto, Junko

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

Ashitagawa, Kyoko
Nakazato, Takeshi
Kobiki, ToshihikoNakamura, Kyoko
Ito, Tetsuya
Kato, Yoshihiro
Ao, Yiping

Specially Appointed
Research Staff

Egusa, Fumi

Specially Appointed
Research Staff

Kurono, YasutakaSpecially Appointed
Research Staff

Morokuma, Kana

Specially Appointed
Research Staff

Sanhueza Nunez,
Patricio Andres

Specially Appointed
Research Staff

Takekoshi, Tatsuya

Administrative Supporter Sasaki, Mie
Administrative Supporter Takahashi, Yumi
Ishigaki-jima Astronomical Observatory
Director
Miyaji, Takeshi
Associate Professor
Agata, Hidehiko
Research Expert
Hanayama, Hidekazu
Technical Expert
Miyaji, Takeshi
Time Keeping Office
HeadSato, Katsuhisa
Research Engineer
Asari, Kazuyoshi
Solar Observatory
Director
Professor
Associate Professor
Associate Professor
Senior Engineer
Specially Appointed
Research Staff
Research Expert
Research Expert
Research Expert
Administrative Supporter
Administrative Supporter
NAOJ Chile Observatory
Director
Professor
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor

124

Hasegawa, Tetsuo
Hasegawa, Tetsuo
Iguchi, Satoru
Kameno, Seiji
Ogasawara, Ryusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Asaki, Yoshiharu
Asayama, Shinichiro
Espada,Fernandez Daniel

Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor

Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Mizuno, Norikazu
Oishi, Masatoshi
Okuda, Takeshi
Erik, Muller

Specially Appointed
Research Staff

Ueda, Junko~2015.09.30

Specially Appointed
Senior Specialist

Fukui, Hideharu

Specially Appointed
Senior Specialist

Furutani, Akio

Specially Appointed
Senior Specialist

Horie, Yosaku

Specially Appointed
Associate Professor

Fukagawa, MisatoSpecially Appointed
Senior Specialist

Ikeda, Emi

III Organization

Specially Appointed
Senior Specialist

Kawakami, Kazuyuki

Specially Appointed
Senior Specialist

Kawasaki, Wataru

Specially Appointed
Senior Specialist

Kobayashi, Tsuyoshi

Specially Appointed
Senior Specialist

Konuma, Mika

Specially Appointed
Senior Specialist

Kuniyoshi, Masaya

Specially Appointed
Senior Specialist

Matsui, Takayuki

Specially Appointed
Senior Specialist

Miel, Renaud

Specially Appointed
Senior Specialist

Morita, Eisuke

Specially Appointed
Senior Specialist

Nakamoto, Takashi

Specially Appointed
Senior Specialist

Nakamura, Koji

Specially Appointed
Senior Specialist

Nukatani, SorahikoSpecially Appointed
Senior Specialist

Administration Department
Manager
General Affairs Section
Chief
Accounting Section
Chief
Staff

Okumura, Yuji
Tsukano, Satomi
Okumura, Yuji
Hiramatsu, Naoya

Center for Computational Astrophysics
Director
Kokubo, Eiichiro
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kohji
Assistant Professor
Inoue, Tsuyoshi
Assistant Professor
Ito, Takashi
Assistant Professor
Ohsuga, Ken
Assistant Professor
Takiwaki, Tomoya
Assistant Professor
Tanaka, Masaomi
Specially Appointed
Takahashi, Hiroyuki
Assistant Professor
Ishikawa, Toshiaki
Shizugami, Makoto
Asahina, Yuta

Otawara, Kazushige

Research Engineer
Engineer
Specially Appointed
Research Staff

Saito, Motoi

Specially Appointed
Research Staff

Furusawa, ShunSpecially Appointed
Senior Specialist

Shimoda, Takanobu

Specially Appointed
Research Staff

Kawashima, Tomohisa

Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist

So, Ryoken

Research Expert
Research Expert
Research Expert

Specially Appointed
Senior Specialist

Sugimoto, Kanako

Kato, TsunehikoNakayama, Hirotaka
Narazaki, Yayoi~2015.09.30

Specially Appointed
Senior Specialist

Yamada, Masumi

Specially Appointed
Senior Specialist

Yoshino, Akira

Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert

Fujimoto, Yasuhiro
Inoue, Norio
Sakuma, Naoko
Shibuya, Masaru
Tomimuro, Hisashi
Yasui, Takashi~2015.08.31

Research Expert
Research Expert
Research Supporter
Research Supporter
Research Supporter
Administrative Supporter

Oshino, Shoichi
Wakita, Shigeru
Fukushi, Hinako
Hasegawa, YukihikoMatsumoto, Yuji
Kimura, Yuko

Administrative Expert
Research Supporter
Research Supporter
Research Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Consultant
AUI Staff

Kamada, Masako
Saito, Tomoki
Uchida, Ayako
Yamazaki, Toshitaka
Kohno, Izumi
Matsunaga, Choko
Otawara, Hikaru
Saito, Naoko
Hyuga, Tadayuki
Krapivka Flores,
Gabriela

AUI Staff
AUI Staff

Collao, Joaquin
Toro, Lorena

Hinode Science Center
Director
Professor
Specially Appointed
Professor

Watanabe, Tetsuya
Sakurai, Takashi
Gizon, Laurent Claude~2015.08.31

Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Research Staff

Hara, Hirohisa
Sekii, Takashi
Suematsu, Yoshinori
Ishikawa, Ryoko
Kano, Ryouhei
Katsukawa, Yukio
Kubo, Masahito
Shimojo, Masumi
Antolin, Patrick

Technical Expert
Research Supporter
Research Supporter

Inoue, Naoko
Ishii, Shuichi
Tsuchiya, Chie

III Organization125

B Projects

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

Aso, YoichiAndo, Masaki

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

Akutsu, Tomotada
Oishi, Naoko
Takahashi, Ryutaro
Tatsumi, Daisuke
Ishizaki, Hideharu
Torii, Yasuo
Tanaka, Nobuyuki
Barton, Mark Andrew

Specially Appointed
Research Staff

Pena Arellano,
Fabian Erasmo

Specially Appointed
Research Staff

Zeidler, Simon

Specially Appointed
Senior Specialist

Hirata, Naoatsu

Research Supporter
Harada, Mikiko
Administrative Supporter Kondo, Mihoko~2016.02.29
Administrative Supporter Yoshizumi, Mizuho
TMT-J Project OfficeDirector
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor

126

Usuda, Tomonori
Takami, Hideki
Usuda, Tomonori
Yamashita, Takuya
Aoki, Wako
Hayano, Yutaka
Kashikawa, Nobunari
Kodama, Tadayuki
Kosugi, George
Miyazaki, Satoshi
Sugimoto, Masahiro
Takato, Naruhisa
Terada, Hiroshi
Oya, Shin

Specially Appointed
Associate Professor

Packham,Christopher Charles~2015.08.11

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

Miyashita, Takaaki
Imanishi, Masatoshi
Suzuki, Ryuji
Tazawa, Seiichi
Harakawa, Hiroki

Specially Appointed
Research Staff

Hashimoto, Tetsuya

III Organization

Specially Appointed
Senior Specialist

Chapman, Junko

Specially Appointed
Senior Specialist

Kozu, Akihito

Specially Appointed
Senior Specialist

Sugiyama, Motokuni

Research Expert
Research Expert
Research Supporter
Research Supporter
Administrative Supporter
Administrative Supporter
RCUH

Ishii, Miki
Ozaki, Shinobu
Inatani, Junji
Tajima, Toshiyuki
Haranaka, Miyuki
Yamaguchi, Chiyu
Iye, Masanori

A Projects

JASMINE Project OfficeDirector
Professor
Professor
Specially Appointed
Professor

Gouda, Naoteru
Gouda, Naoteru
Kobayashi, Yukiyasu
Hensler,
Georhard Max Franz~2015.11.25

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

Hanada, Hideo
Takato, Naruhisa
Tsuruta, Seiitsu
Araki, Hiroshi
Noda, Hirotomo
Tsujimoto, Takuji
Ueda, Akitoshi
Yano, Taihei
Asari, Kazuyoshi
Shirahata, Mai~2015.12.31

Specially Appointed
Research Staff

Yamaguchi, Masaki

Research Supporter
Technical Supporter

Utsunomiya, Shin
Kashima, Shingo

Extrasolar Planet Detection Project OfficeDirector
Tamura, Motohide
Professor
Kokubo, Eiichiro
Affiliated Professor
Tamura, Motohide
Associate Professor
Izumiura, Hideyuki
Assistant Professor
Kotani, Takayuki
Assistant Professor
Morino, Jun-ichi
Assistant Professor
Nakajima, Tadashi
Assistant Professor
Nishikawa, Jun
Assistant Professor
Suto, Hiroshi
Specially Appointed
Hashimoto, Jun
Assistant Professor
Specially Appointed
Assistant Professor

Hori, Yasunori

Specially Appointed
Assistant Professor

Narita, Norio

Specially Appointed
Research Staff

Omiya, Masashi

Specially Appointed
Senior Specialist

Kusakabe, Nobuhiko

Research Supporter
Kandori, Ryo
Research Supporter
Kurokawa, Takashi
Administrative Supporter Miyamae, Miwako
RISE Project
Director
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Research Expert
Administrative Supporter
SOLAR-C Project OfficeDirector
Professor
Professor
Affiliated Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Senior Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff

Namiki, Noriyuki
Gouda, Naoteru
Kobayashi, Yukiyasu
Kokubo, Eiichiro
Namiki, Noriyuki
Hanada, Hideo
Matsumoto, Koji
Tsuruta, Seiitsu
Araki, Hiroshi
Kono, Yusuke
Noda, Hirotomo
Tsujimoto, Takuji
Yano, Taihei
Asari, Kazuyoshi
Tazawa, Seiichi
Oshigami, Shoko
Yamada, Ryuhei
Kikuchi, FuyuhikoSato, Sayaka

Hara, Hirohisa
Sakurai, Takashi
Watanabe, Tetsuya
Ichimoto, Kiyoshi
Goto, MotoshiHara, Hirohisa
Kano, Ryouhei
Sekii, Takashi
Suematsu, Yoshinori
Ishikawa, Ryoko
Katsukawa, Yukio
Kubo, Masahito
Shinoda, Kazuya
Narukage, Noriyuki
Watanabe, Kyoko~2015.09.30

Technical Expert
Inoue, Naoko
Administrative Supporter Fujiyoshi, Marie

Centers
Astronomy Data Center
Director
Professor

Oishi, Masatoshi
Kokubo, Eiichiro

Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Engineer

Mizumoto, Yoshihiko
Ichikawa, Shinichi
Kosugi, George
Noumaru, Junichi
Oishi, Masatoshi
Shibata, Katsunori
Takata, Tadafumi
Furusawa, Hisanori
Ito, Takashi
Oe, Masafumi
Shimojo, Masumi
Shirasaki, Yuji
Inoue, Goki
Fukui, Asami~2015.11.15

Specially Appointed
Research Staff

Higuchi, Yuichi

Specially Appointed
Research Staff

Yoshida, Tetsuo

Specially Appointed
Research Staff

Zapart,Christopher Andrew

Research Expert
Research Expert
Research Expert
Research Expert
Research Supporter
Research Supporter
Research Supporter
Administrative Supporter
Research Assistant
JVO Project
Head
Associate Professor
Assistant Professor
Advanced Technology Center
Director
Professor
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
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor

Asano, Eiji
Furusawa, Junko
Isogai, Mizuki
Tanaka, Nobuhiro
Fujikawa, Makiko
Noda, Sachiyo
Taguchi, Shoya
Ishii, Yuko
Suzuki, Taiki
Mizumoto, Yoshihiko
Oishi, Masatoshi
Shirasaki, Yuji

Noguchi, Takashi
Noguchi, Takashi
Takami, HidekiHara, Hirohisa
Hayano, Yutaka
Iwata, Ikuru
Kano, Ryouhei
Matsuo, Hiroshi
Miyazaki, Satoshi
Sekimoto, Yutaro
Shan, Wenlei
Fujii, Yasunori
Kikuchi, Kenichi
Okada, Norio
Akutsu, Tomotada
Kojima, Takafumi
Nakaya, Hidehiko
Oshima, Tai
Suzuki, Ryuji

III Organization

127

128

Specially Appointed
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Engineer
Specially Appointed
Research Staff

Gonzalez Garcia,
AlvaroFukushima, Mitsuhiro
Iizuka, Yoshizo
Noguchi, Motokazu
Obuchi, Yoshiyuki
Sato, Naohisa
Kubo, Koichi
Miyazawa, Chieko
Takahashi, Toshikazu
Fukuda, Takeo
Ikenoue, Bungo
Inata, Motoko
Iwashita, Hikaru
Kamata, Yukiko
Kaneko, Keiko
Mitsui, Kenji
Tamura, Tomonori
Uraguchi, Fumihiro
Waseda, Koichi
Tsuzuki, Toshihiro
Dominjon, Agnes
Micheline

Specially Appointed
Research Staff

Karatsu, Kenichi~2015.07.31

Specially Appointed
Research Staff

Narukage, Noriyuki

Specially Appointed
Senior Specialist

Ezaki, Shohei

Specially Appointed
Senior Specialist

Karatsu, Miki

Specially Appointed
Senior Specialist

Niizeki, Yasuaki

Specially Appointed
Senior Specialist

Uemizu, Kazunori

Research Expert
Research Expert
Research Expert
Technical Expert
Technical Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter

Matthias, Kroug
Ozaki, Shinobu
Saitou, Sakae
Nishino, Tetsuo
Hayashi, Ritsuko
Kuroda, Kyoko
Murakami, Hiromi
Yoshida, Taeko

Public Relations Center
Director
Professor
Professor
Associate Professor
Specially Appointed
Associate Professor

Fukushima, Toshio
Fukushima, Toshio
Watanabe, Junichi
Agata, HidehikoKinoshita, Daisuke~2016.02.15

Specially Appointed
Associate Professor

Kozak, Pavlo~2015.07.10

Assistant Professor
Assistant Professor
Research Engineer

Hiramatsu, Masaaki
Soma, Mitsuru
Katayama, Masato

III Organization

Research Engineer
Chief Senior Engineer
Chief Engineer
Library Chief
Specially Appointed
Senior Specialist

Sasaki, Goro
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

Research Expert
Research Expert
Research Expert
Research Expert
Reaearch Supporter
Reaearch Supporter
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Administrative Supporter
Administrative Supporter
Public Relations Office
Head
Chief Engineer
Research Expert
Research Expert
Research Supporter
Public Outreach Official
Public Outreach Official
Public Outreach Official
Outreach and Education Office
HeadSpecially Appointed
Senior Specialist
Public Outreach Official

Komiyama, Hiroko
Ono, Tomoko
Takata, Hiroyuki
Usuda-Sato, Kumiko
Kume, Kaori
Tsuchiya, Chie
Diaz, Rosas Elian Abril
Endo, Isao
Fujita, Tokiko
Futami, Hiroshi
Hamura, Taiga
Hatano, Satomi
Ibaraki, Takao
Ishizaki, Masaharu
Iwashiro, Kuninori
Koike, Akio
Kubo, Maki
Mikami, Naotsugu
Naito, Seiichiro
Natsugari, Satomi
Nemoto, Shiomi
Oguri, Junko
Ohgoe, Osamu
Shibata, Yukiko
Shioya, Yasuhisa
Takabatake, Noriko
Takeda, Takaaki
Aoki, Makiko
Noguchi, Sayumi
Hiramatsu, Masaaki
Nagayama, Shogo
Komiyama, Hiroko
Ono, Tomoko
Kume, Kaori
Mikami, Naotsugu
Natsugari, Satomi
Shioya, Yasuhisa

Agata, Hidehiko
Ishikawa, Naomi
Endo, Isao

Public Outreach Official Fujita, Tokiko
Public Outreach Official Hamura, Taiga
Public Outreach Official Hatano, Satomi
Public Outreach Official Ibaraki, Takao
Public Outreach Official Ishizaki, Masaharu
Public Outreach Official Naito, Seiichiro
Public Outreach Official Ohgoe, Osamu
Public Outreach Official Takabatake, Noriko
Museum Deliberation Office
Head
Agata, Hidehiko
Research Engineer
Sasaki, Goro
Senior Engineer
Matsuda, Ko
Research Expert
Usuda-Sato, Kumiko
Public Outreach Official Endo, Isao
Public Outreach Official Fujita, Tokiko
Public Outreach Official Futami, Hiroshi
Public Outreach Official Koike, Akio
Public Outreach Official Nemoto, Shiomi
Public Outreach Official Takeda, Takaaki
Ephemeris Computation Office
HeadKatayama, Masato
Senior Engineer
Matsuda, Ko
Public Outreach Official Endo, Isao
Library
ChiefTodoriki, Tatsuya
Public Outreach Official Kubo, Maki
Public Outreach Official Oguri, Junko
Publications Office
Head
Fukushima, Toshio
Research Expert
Takata, Hiroyuki
Public Outreach Official Iwashiro, Kuninori
Public Outreach Official Kubo, Maki
The Office for Astronomy Outreach of the IAU
HeadAgata, HidehikoSpecially Appointed
Cheung, Sze Leung
Senior Specialist
Specially Appointed
Senior Specialist
Research Expert
Public Outreach Official
Public Outreach Official
General Affairs Office
HeadAdministrative Supporter
Administrative Supporter

Pires Canas, Lina Isabel
Usuda-Sato, KumikoDiaz, Rosas Elian Abril
Shibata, Yukiko
Matsuda, Ko
Aoki, Makiko
Noguchi, Sayumi

Divisions
Division of Optical and Infrared Astronomy
Division Chair
Mizumoto, Yoshihiko
Professor
Arimoto, Nobuo
Professor
Gouda, Naoteru
Professor
Kobayashi, Yukiyasu
Professor
Mizumoto, Yoshihiko
Professor
Ohashi, Nagayoshi

Professor
Professor
Professor
Associate Professor
Associate Professor
Associate 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
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

Sekiguchi, Kazuhiro
Usuda, Tomonori
Yamashita, Takuya
Aoki, Wako
Aso, Yoichi
Hayashi, Saeko
Iwata, Ikuru
Izumiura, Hideyuki
Kashikawa, Nobunari
Kodama, Tadayuki
Noumaru, Junichi
Sugimoto, Masahiro
Takato, Naruhisa
Takeda, Yoichi
Terada, Hiroshi
Ukita, Nobuharu
Iwashita, Hiroyuki
Miyashita, Takaaki
Akutsu, Tomotada
Imanishi, Masatoshi
Komiyama, Yutaka
Koyama, Yusei
Minowa, Yosuke
Morino, Jun-ichi
Nakajima, Tadashi
Nishikawa, Jun
Oishi, Naoko
Okita, Hirofumi
Onodera, Masato
Pyo, Tae-soo
Soma, Mitsuru
Takahashi, Ryutaro
Tatsumi, Daisuke
Tsujimoto, Takuji
Ueda, Akitoshi
Yagi, Masafumi
Yanagisawa, Kenshi
Yano, Taihei
Matsuoka, Yoshiki

Research Engineer
Research Engineer
Research Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
EngineerEngineer
Administrative Supporter
Research AssistantResearch AssistantResearch AssistantBando, Takamasa
Ishizaki, Hideharu
Torii, Yasuo
Namikawa, Kazuhito
Negishi, Satoru
Omata, Koji
Tamura, Tomonori
Tanaka, Nobuyuki
Sato, Tatsuhiro
Tsutsui, Hironori
Kimura, Hiroko
Onoue, Masafusa
Shimakawa, Rizumu
Ui, Takahiro~2015.12.31

JSPS Postdoctoral Fellow Hayashi, Masao

III Organization

129

JSPS Postdoctoral Fellow Niino, Yu
JSPS Postdoctoral Fellow Uchiyama, Mizuho
Division 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
Associate Professor
Associate Professor
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
Research Engineer

130

III Organization

Iguchi, Satoru
Hasegawa, Tetsuo
Honma, Mareki
Iguchi, Satoru
Kameno, Seiji
Kawabe, Ryohei
Kobayashi, Hideyuki
Namiki, Noriyuki
Ogasawara, Ryusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Asaki, Yoshiharu
Asayama, Shinichiro
Espada,Fernandez Daniel
Hanada, Hideo
Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Matsumoto, Koji
Mizuno, Norikazu
Okuda, Takeshi
Saito, Masao
Shibata, Katsunori
Kanzawa, Tomio
Kawashima, Susumu
Kikuchi, Kenichi
Sato, Katsuhisa
Tsuruta, Seiitsu
Watanabe, Manabu
Araki, Hiroshi
Ezawa, Hajime
Hada, Kazuhiro
Hiramatsu, Masaaki
Hirota, Akihiko
Hirota, Tomoya
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
Asari, Kazuyoshi

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

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

Research Expert
Research Supporter

Tatsuzawa, Kaichi
Tsuneyama, Junko

Division of Solar and Plasma Astrophysics
Division Chair
Sakurai, Takashi
Professor
Sakurai, Takashi
Professor
Watanabe, Tetsuya
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Hara, Hirohisa
Associate Professor
Kano, Ryouhei
Associate Professor
Sekii, Takashi
Associate Professor
Suematsu, Yoshinori
Assistant Professor
Ishikawa, Ryoko
Assistant Professor
Katsukawa, Yukio
Assistant Professor
Kubo, Masahito
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
Specially Appointed
Balantekin, Akif Baha
Professor~2015.11.23
Specially Appointed
Professor

Cheoun, Myung-Ki~2016.02.24

Specially Appointed
Professor

Deliduman, Yamac~2015.11.23

Specially Appointed
Professor

Mathews, Grant James~2015.11.09

Associate Professor
Associate Professor

Kajino, Toshitaka
Nakamura, Fumitaka

Specially Appointed
Associate Professor

Famiano,Michael Andrew~2015.11.23

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

Hamana, Takashi
Inoue, Tsuyoshi
Ohsuga, Ken
Takiwaki, Tomoya
Tanaka, Masaomi
Fujii, Michiko~2015.12.31

Specially Appointed
Assistant Professor

Fujimoto, Keizo

Specially Appointed
Assistant Professor

Nozawa, TakayaSpecially Appointed
Assistant Professor

Sotani, HajimeSpecially Appointed
Assistant Professor

Zenitani, Seiji

Specially Appointed
Research Staff

Michikoshi, Shugo

Administrative Supporter Izumi, Shioko
Administrative Supporter Kano, Kaori

III Organization

1315. Research Support Departments
Research Enhancement Strategy OfficeDirector
Kobayashi, Hideyuki
Specially Appointed
Chapman, Junko
Senior Specialist
Specially Appointed
Senior Specialist

Chiba, Kurazo

Specially Appointed
Senior Specialist

Fukui, Hideharu

Specially Appointed
Senior Specialist

Hori, KunikoSpecially Appointed
Senior Specialist

Lundock, Ramsey Guy

Specially Appointed
Senior Specialist

Miura, Mitsuo

Specially Appointed
Senior Specialist

Ota, MasahikoSpecially Appointed
Senior Specialist

Yamamiya, Osamu

Research Evaluation Support OfficeDirector
Watanabe, Junichi
Specially Appointed
Hori, Kuniko
Senior Specialist
Office of International Relations
Director
Specially Appointed
Senior Specialist
Research Expert
Research Expert
Administration Office
Deputy Manager/Senior
Specialist

Yamaguchi, Takahiro
Yamaguchi, Takahiro
Komiyama, Hiroko
Yoshida, Fumi
Onishi, Tomoyuki

International Academic Affairs Section
Staff
Takada, Miyuki
Administrative Supporter Ito, Yoshihisa
Administrative Supporter Momma, Yoko
Human Resources Planning OfficeDirector
Yamamiya, Osamu
Safety and Health Management OfficeDirector
Takami, Hideki
Specially Appointed
Ota, Masahiko
Senior Specialist
Technical Expert
Engineering Promotion OfficeDirector
Specially Appointed
Senior Specialist
Administration Department
General Manager

132

III Organization

Kashiwagi, Yuji

Takami, Hideki
Chiba, Kurazo

Sasaki, Tsuyoshi

General Affairs Division
Manager
Harada, Eiichiro
Deputy Manager
Onishi, Tomoyuki
Administrative Supporter Torii, Makiko
Information Technology Specialist
Specialist
Yoshikawa, Ikuko
Graduate School Specialist
Specialist
Kikkawa, Hiroko
Administrative Supporter Okuda, Yutaka
Personnel Accounting Specialist
Specialist
Watanabe, Yukika
General Affairs Section
Chief
Yoshikawa, Ikuko
Senior Staff
Goto, Michiru
Staff
Mochimaru, Shiori
Staff
Yoshimura, TetsuyaSpecially Appointed
Noguchi, Koki
Senior Specialist
Vehicle Driver
Administrative Expert
Administrative Supporter
Administrative Supporter
Administrative Supporter
Personnel Section
Chief
Staff
Staff
Payroll Section
Chief
Staff
Specially Appointed
Senior Specialist
Administrative Supporter
Employee Affairs Section
Chief
Staff
Staff
Research Support Section
Chief
Administrative Expert
Administrative Supporter
Financial Affairs Division
Manager
Senior Specialist
Audit Specialist
Specialist
External Funding Section
Specialist
Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter

Amemiya, Hidemi
Murakami, Sachiko
Kobayashi, Kayo
Noguchi, Utako
Seki, Kumi
Yamanochi, Mika
Isozaki, Yuka
Sakamoto, Misato
Watanabe, Yukika
Furukawa, Shinichiro
Yamamoto, Chieko
Aiba, Narukazu
Yamaura, Mari
Ouchi, Kaori
Saito, MasahiroSato, Yoko
Haruki, Mutsumi
Takeuchi, Kaori
Nemoto, Nobuyuki
Miura, Norio
Ishikawa, Junya
Chiba, Satoko
Yamafuji, Yasuto
Komoda, Chizuru
Sato, Chieko
Urushibata, Kozue
Yasuda, Masako

General Affairs Section
Chief
Yamamoto, Shinichi
Administrative Supporter Okada, Kazuko
Budget Section
Chief
Akaike, Makoto
Staff
Yokota, Banri
Administrative Supporter Matsubara, Michiko
Asset Management Section
Chief
Sato, Kanako
Administrative Supporter Komoda, Chizuru
Purchase Validation Center
Chief
Sato, Kanako
Administrative Supporter Hosoi, Chiho
Administrative Supporter Nakagomi, Kimitoshi
Administrative Supporter Taniai, Tomoko
Administrative Supporter Tanigaki, Yukio
Accounting Division
Manager
Tanaka, Masaru
Contract Specialist
Specialist
Chiba, Yoko
Accounting Section
Chief
Sukigara, Yuji
Staff
Miyata, Yusuke
Administrative Supporter Kobayashi, Rina
Administrative Supporter Nagasawa, Fumi
Procurement Section
Chief
Chiba, Yoko
Staff
Kayamori, Shinji
Staff
Sugimoto, Naomi
Staff
Takai, Tetsuya
Consultant
Hyuga, Tadayuki
Administrative Expert
Sato, Masako
Childcare Leave
Administrative Supporter Takano, Ayako
Facilities Division
Manager
Watanabe, Matsuo
Administrative Expert
Asada, Tsuneaki
General Affairs Section
Senior Staff
Kawashima, Ryota
Staff
Nakagawa, Yukie
Administrative Supporter Hasegawa, Chisato
Planning Section
Chief
Murakami, Kazuhiro
Administrative Supporter Tsukamoto, Izumi
Maintenance Section
Chief
Sato, Takashi
Staff
Hayashigura, Koji

III Organization

1336. Personnel change
Research and Academic Staff
Date
Name

Change2015/4/1

Koyama, Yusei

Hired2015/5/15

Asaki, Yoshiharu

2015/11/1

New Affiliated Institute, Position
Division of Optical and Infrared Astronomy(Subaru Telescope), Assistant Professor

Previous Affiliated Institute, Position

Hired

Division of Radio Astronomy (NAOJ Chile
Observatory), Associate Professor(Japan Aerospace Exploration
Agency)Shan, Wenlei

Hired

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

2015/12/1

Minamidani,
Tetsuhiro

Hired

Division of Radio Astronomy (Nobeyama
Radio Observatory), Assistant Professor

2016/2/1

Hada, Kazuhiro

Hired

Division of Radio Astronomy (Mizusawa
VLBI Observatory), Assistant Professor

2016/2/1

Takiwaki, Tomoya

HiredDivision of Theoretical Astronomy, AssistantProfessor

2016/3/1

Onodera, Masato

Hired

Division of Optical and Infrared Astronomy(Subaru Telescope), Assistant Professor

2015/6/30

Nakanishi,
Kouichiro

Resigned(NAOJ Chile Observatory, Specially
Appointed Associate Professor)

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

2016/3/31

Hasegawa, Tetsuo

Resigned(NAOJ Chile Observatory, Specially
Appointed Professor)

Division of Radio Astronomy(NAOJ Chile Observatory),
Professor

2016/3/31

Iizuka, Yoshizo

Resigned

Advanced Technology Center,Research Engineer

2016/3/31

Sakurai, Takashi

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

2016/3/31

Torii, Yasuo

RetiredDivision of Optical and Infrared
Astronomy (Gravitational Wave
Project Office), Research Engineer

2016/3/31

Sasaki, Goro

RetiredPublic Relations Center, ResearchEngineer

2015/4/1

Sugimoto, Masahiro

Promoted

Division of Optical and Infrared Astronomy(TMT-J Project Office), Associate Professor

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

2015/8/1

Hayano, Yutaka

Promoted

Division of Optical and Infrared Astronomy(TMT-J Project Office), Associate Professor

Division of Optical and Infrared
Astronomy (Subaru Telescope),
Assistant Professor

2015/8/1

Espada Fernandez,
DanielPromoted

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

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

2015/11/1

Kano, Ryohei

Promoted

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

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

2016/1/1

Fujii, Yasunori

Promoted

Advanced Technology Center,
Chief Research Engineer

Advanced Technology Center,Research Engineer

Reassigned Astrobiology Center, Assistant Professor

NAOJ Division of Optical andInfrared Astronomy (Extrasolar
Planet Detection Project Office),
Assistant Professor

2015/4/1

134

Suto, Hiroshi

III Organization(Nobeyama Radio Observatory,Specially Appointed AssistantProfessor)

2015/4/1

Kotani, Takayuki

Reassigned Astrobiology Center, Assistant Professor

NAOJ Division of Optical andInfrared Astronomy (Extrasolar
Planet Detection Project Office),
Assistant Professor

2016/1/1

Obuchi, Yoshiyuki

Reassigned

Advanced Technology Center,Research Engineer

Advanced Technology Center,
Chief Engineer

Engineering Staff
ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Date

Name

2016/3/1

Hirano, Ken

Hired

2015/11/15

Fukui, Asami

Resigned

2015/4/1

Shinoda, Kazuya

Promoted

Division of Solar and Plasma Astrophysics(Solar Observatory), Senior Engineer

Division of Solar and Plasma
Astrophysics (Solar Observatory),
Chief Engineer

2015/4/1

Handa, Kazuyuki

Promoted

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

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

2015/4/1

Miyazawa, Chieko

Promoted

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

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

2015/7/1

Ueno, Yuji

Promoted

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

Division of Radio Astronomy(Mizusawa VLBI Observatory),
Engineer

2015/8/1

Mitsui, Kenji

Promoted

2015/8/1

Nagayama, Syogo

Promoted

Advanced Technology Center,
Chief Engineer
Public Relations Center, Chief Engineer

Advanced Technology Center,
Engineer
Public Relations Center, Engineer

ChangeNew Affiliated Institute, Position

Division of Radio Astronomy (Mizusawa
VLBI Observatory), Engineer
Astronomy Data Center, Engineer

Administrative Staff
Previous Affiliated Institute,
Position(National Museum of Nature andScience,Tokyo)

Date

Name

2015/4/1

Watanabe, Matsuo

Hired

Administration Department Facilities
Division, Manager

2015/4/1

Watanabe, Yukika

Hired

Administration Department General Affairs
Division Payroll Section, Chief(Tokyo Gakugei Univerisity)

2015/4/1

Todoriki, Tatsuya

HiredPublic Relations Center Administration
Office Library Section, Chief(The University of Tokyo)

2015/4/1

Miyata, Yusuke

Hired

Administration Department Accounting
Division Accounting Section, Staff(The Graduate University for
Advanced Studies)

2015/4/1

Mochimaru, Shiori

Hired

Administration Department General Affairs
Division General Affairs Section, Staff

2015/4/1

Saito, Masahiro

Hired

Administration Department General Affairs
Division Employee Affairs Section, Staff

2015/7/1

Akaike, Makoto

Hired

Administration Department Financial
Affairs Division Budget Section, Chief(The University of Tokyo)

2015/7/1

Ito, Hiromasa

Hired

Mizusawa VLBI Observatory
Administration Office Accounting Section,
Chief(Iwate University)

2015/8/1

Iijima, Kunio

Hired

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

III Organization135

2015/6/30

Koseki, Tatsuya

Resigned(Ministry of Economy, Trade and Industry)

Mizusawa VLBI Observatory
Administration Office Accounting
Section, Chief

2015/6/30

Fujiwara, Kenichi

Resigned(The University of Tokyo)

Administration Department
Financial Affairs Division Budget
Section, Chief

2015/7/31

Kobayashi, Kazuhito Resigned(Shinshu University)

Nobeyama Radio Observatory
Administration Office Accounting
Section, Staff

2016/3/31

Sasaki, Tsuyoshi

Resigned(Nagoya University)

General Manager

2016/3/31

Miura, Norio

Resigned(The University of Tokyo)

Administration Department
Financial Affairs Division, External
Funding Senior Specialist

2016/3/31

Yoshikawa, Ikuko

Resigned(Hitotsubashi University)

Administration Department General
Affairs Division General Affairs
Section, Chief

2016/3/31

Sukigara, Yuji

Resigned(Tokyo Gakugei Univerisity)

Administration Department
Accounting Division Accounting
Section, Chief

2016/3/31

Sato, Takashi

Resigned(The University of Tokyo)

Administration Department
Facilities Division Maintenance
Section, Chief

2016/3/31

Setou, Nobuyoshi

Resigned(Okayama University)

Okayama AstrophysicalObservatory Administration Office
Administration Section, Chief

2015/4/1

Kawashima, Ryota

Promoted

Administration Department Facilities
Division General Affairs Section, Senior
Staff

Administration Department General
Affairs Division Employee Affairs
Section, Staff

2015/7/1

Goto, Michiru

Promoted

Administration Department General Affairs
Division General Affairs Section, Senior
Staff

Administration Department
General Affairs Division General
Affairs Section, Staff

2015/10/1

Sato, Kanako

Promoted

Administration Department Financial
Administration Department
Affairs Division Asset Management Section, Financial Affairs Division Asset
ChiefManagement Section, Senior Staff

2015/10/1

Chiba, Satoko

Promoted

Administration Department Financial Affairs
Division, External Funding Specialist

2015/4/1

Yamada, Tomohiro

Okazaki Administration Center, Financial
Reassigned Affairs Department Financial Affairs
Division, Specialist

2015/7/1

Mizokawa, Yuko

Reassigned

Administrative Bureau Financial Affairs
Division Financial Affairs Section, Staff

NAOJ Administration Department
Financial Affairs Division General
Affairs Section, Staff

2015/7/1

Tanaka, Masaru

Reassigned

NAOJ Administration Department
Accounting Division, Manager

Administrative Bureau General
Affairs Divison, Deputy Manager

2016/1/1

Ishikawa, Junya

Reassigned

NAOJ Administration Department Financial
Affairs Division, Audit Specialist

Administrative Bureau Laison and
Planning Division, Specialist

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Administration Department
Financial Affairs Division, External
Funding Senior Staff
NAOJ Administration Department
Facilities Division General Affairs
Section, Chief

Employee on Annual Salary System

136

Date

Name

2015/4/1

Muller, Erik Michael

Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2015/4/1

Fukagawa, Misato

Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

III Organization

2015/4/1

Miura, Rie

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor(NAOJ Chile Observatory,Specially Appointed Research
Staff)

2015/4/1

Herrera Contreras,
Cinthya Natalia

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor(NAOJ Chile Observatory,Specially Appointed Research
Staff)

2015/4/1

Hashimoto, Tetsuya

Hired

TMT-J Project Office, Specially Appointed
Research Staff

2015/4/1

Toshikawa, Jun

Hired

Subaru Telescope, Specially Appointed
Research Staff

2015/4/1

Ichikawa, Kohei

Hired

Subaru Telescope, Specially Appointed
Research Staff

2015/4/1

Egusa, Fumi

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2015/4/1

Morokuma, Kana

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2015/4/1

Matsumoto, Naoko

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2015/4/1

Sakai, Nobuyuki

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2015/4/1

Motogi, Kazuhito

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2015/4/1

Oshigami, Shoko

Hired

RISE Project, Specially Appointed Research
Staff

2015/4/1

Kaneko, Hiroyuki

Hired

Nobeyama Radio Observatory, Specially
Appointed Research Staff

2015/4/1

Miyamoto, Yusuke

Hired

Nobeyama Radio Observatory, Specially
Appointed Research Staff

2015/4/1

Otsuji, Kenichi

HiredSolar Observatory, Specially Appointed
Research Staff

2015/4/1

Watanabe, Kyoko

Hired

SOLAR-C Project Office, Specially
Appointed Research Staff

2015/4/1

Fukui, Akihiko

HiredOkayama Astrophysical Observatory,Specially Appointed Research Staff

2015/4/1

Asahina, Yuta

Hired

Center for Computational Astrophysics,
Specially Appointed Research Staff

2015/4/1

Michikoshi, Shugo

Hired

Division of Theoretical Astronomy,
Specially Appointed Research Staff

2015/4/1

Karatsu, Kenichi

HiredAdvanced Technology Center, Specially
Appointed Research Staff

2015/4/1

Momose, Rieko

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2015/4/1

Okumura, Yuji

Hired

NAOJ Chile Observatory Administration
Department, Specially Appointed Senior
Specialist

2015/4/1

Furutani, Akio

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2015/4/1

Konuma, Mika

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2015/4/1

Nukatani, Sorahiko

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2015/4/1

Nakamura, Koji

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2015/4/1

Otawara, Kazushige

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

III Organization

137

138

2015/4/1

Kanaguchi,
Masahiro

Hired

Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2015/4/1

Oyama, Tomoaki

Hired

Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2015/4/1

Nagayama, Takumi

Hired

Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2015/4/1

Niizeki, Yasuaki

HiredAdvanced Technology Center, Specially
Appointed Senior Specialist

2015/4/1

Ezaki, Shohei

HiredAdvanced Technology Center, Specially
Appointed Senior Specialist

2015/4/1

Karatsu, Miki

Hired

Advanced Technology Center, Specially
Appointed Senior Specialist

2015/4/1

Uemizu, Kazunori

Hired

Advanced Technology Center, Specially
Appointed Senior Specialist

2015/4/6

Pires Canas, Lina
IsabelHired

Public Relations Center, Specially Appointed
Senior Specialist

2015/6/1

Packham,Christopher Charles

Hired

TMT-J Project Office, Specially Appointed
Associate Professor

2015/6/1

Miel, Renaud Jean
Christophe

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2015/7/1

Nakanishi, Kouichiro Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2015/7/1

Sakamoto, Ken

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2015/7/1

Noguchi, Koki

Hired

Administration Department General Affairs
Division, Specially Appointed Senior
Specialist

2015/8/1

Gizon, Laurent
Claude

Hired

Hinode Science Center, Specially Appointed
Professor

2015/8/1

Kawakami,
Kazuyuki

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2015/9/1

Takebayashi, Yasuo

Hired

Division of Radio Astronomy, Specially
Appointed Senior Specialist

2015/9/1

Ishikawa, Naomi

Hired

Public Relations Center, Specially Appointed
Senior Specialist

2015/10/1

Oya, Shin

Hired

TMT-J Project Office, Specially Appointed
Associate Professor

2015/10/9

Mathews, Grant
James

Hired

Division of Theoretical Astronomy, Specially
Appointed Professor

2015/10/22

Balantekin, Akif
Baha

Hired

Division of Theoretical Astronomy, Specially
Appointed Professor

2015/10/22 Deliduman, Yamac

Hired

Division of Theoretical Astronomy, Specially
Appointed Professor

2015/10/23

Famiano, Michael
Andrew

Hired

Division of Theoretical Astronomy, Specially
Appointed Associate Professor

2015/12/1

Horie, Yosaku

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/1/1

Ikeda, Emi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/1/1

Nakamoto, Takashi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/1/1

Yoshino, Akira

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

III Organization(Mizusawa VLBI Observatory,Specially Appointed Research
Staff)(Division of Radio Astronomy(NAOJ Chile Observatory),
Assistant Professor)

2016/1/15

Ikeda, Hiroyuki

HiredSubaru Telescope, Specially Appointed
Senior Specialist

2016/1/28

Renzini, Alvio

Hired

Subaru Telescope, Specially Appointed
Professor

2016/2/1

Hayashi, Yusuke

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2016/3/1

Oishi, Yukie

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2015/7/31

Karatsu, Kenichi

Resigned

Advanced Technology Center,
Specially Appointed Research Staff

2015/8/31

Herrera Contreras,
Cinthya Natalia

Resigned

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2015/9/30

Ueda, Junko

Resigned

NAOJ Chile Observatory, Specially
Appointed Research Staff

2015/9/30

Otsuji, Kenichi

Resigned

Solar Observatory, Specially
Appointed Research Staff

2015/9/30

Watanabe, Kyoko

Resigned

SOLAR-C Project Office, Specially
Appointed Research Staff

Resigned

Subaru Telescope, Specially
Appointed Senior Specialist

2015/10/31 Momose, Rieko(Division of Radio Astronomy (Nobeyama
Radio Observatory), Assistant Professor)

Nobeyama Radio Observatory,Specially Appointed AssistantProfessor

Minamidani,
Tetsuhiro

Resigned

2015/12/31 Fujii, Michiko

Resigned

Division of Theoretical Astronomy,
Specially Appointed AssistantProfessor

2015/12/31 Shirahata, Mai

Resigned

JASMINE Project Office, Specially
Appointed Research Staff

2015/12/31 Sakamoto, Ken

Resigned

Subaru Telescope, Specially
Appointed Senior Specialist

2016/3/31

Fukagawa, Misato

Resigned

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2016/3/31

Gonzalez Garcia,
AlvaroResigned

2016/3/31

Ichikawa, Kohei

Resigned

Subaru Telescope, Specially
Appointed Research Staff

2016/3/31

Oshigami, Shoko

Resigned

RISE Project, Specially Appointed
Research Staff

2016/3/31

Antolin, Patrick

Resigned

Hinode Science Center, Specially
Appointed Research Staff

2016/3/31

Furusawa, Shun

Resigned

Center for Computational
Astrophysics, Specially Appointed
Research Staff

2016/3/31

Nishimura, Atsushi

Resigned

Nobeyama Radio Observatory,Specially Appointed Research Staff

2016/3/31

Yamada, Masumi

Resigned

2015/8/11

Packham,Christopher Charles

Contract
ExpiredTMT-J Project Office, Specially
Appointed Associate Professor

2015/8/31

Gizon, Laurent
ClaudeContract
ExpiredHinode Science Center, Specially
Appointed Professor

2015/11/9

Mathews, Grant
James

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed Professor

2015/11/30(Division of Radio Astronomy (NAOJ Chile
Observatory), Assistant Professor)(Division of Radio Astronomy (NAOJ Chile
Observatory), Research Engineer)

Advanced Technology Center,
Specially Appinted AssistantProfessor

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

III Organization139

2015/11/23

Balantekin, Akif
Baha

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed Professor

2015/11/23

Deliduman, Yamac

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed Professor

2015/11/23

Famiano, Michael
Andrew

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed Associate
Professor

2016/3/31

Renzini, Alvio

Contract
ExpiredSubaru Telescope, Specially
Appointed Professor

2016/3/31

Fujimoto, Keizo

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed AssistantProfessor

2016/3/31

Hashimoto, Tetsuya

Contract
ExpiredTMT-J Project Office, Specially
Appointed Research Staff

2016/3/31

Yamaguchi, Masaki

Contract
ExpiredJASMINE Project Office, Specially
Appointed Research Staff

2016/3/31

Kawashima,
Tomohisa

Contract
ExpiredCenter for Computational
Astrophysics, Specially Appointed
Research Staff

2016/3/31

Michikoshi, Shugo

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed Research Staff

2016/3/31

Yoshida, Tessei

Contract
ExpiredAstronomy Data Center, Specially
Appointed Research Staff

2016/3/31

Kurono, Yasutaka

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Research Staff

2015/4/1

Narita, Norio

Reassigned

Astrobiology Center Specially Appointed
Assistant Professor

NAOJ Extrasolar Planet Detection
Project Office, Specially Appointed
Assistant Professor

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Research Administrator Staff
Date

Name

2015/4/1

Yamaguchi,
Takahiro

Hired

Chiba, Kurazo

Contract
Expired2016/3/31

Foreign Visiting Researcher
Name
Hensler, Gerhard Max Franz
Cheoun, Myung-Ki
Kinoshita, Daisuke
Kozak, Pavlo
Koda, Jin

Research Enhancement Strategy Office,
Office of International Relations, Specially
Appointed Senior Specialist

Period2015/4/10~ 2015/5/20
2015/10/7~ 2015/11/25
2015/12/26 ~ 2016/2/24
2015/7/2~ 2015/9/5
2016/1/21~ 2016/2/15
2015/5/12~ 2015/7/10
2015/7/21~ 2015/9/19
2016/1/1~ 2016/3/31(NAOJ Chile Observatory
Administration Department,
Specially Appointed Senior
Specialist)
Research Enhancement Strategy
Office, Engineering Promotion
Office, Specially Appointed Senior
Specialist

Affiliated Institute
University of Vienna (Austria)
Soongsil University (South Korea)
Institute of Astronomy, National Central University (Taiwan)
Astronomical Observatory of Kyiv,
Taras Shevchenko National University (Ukraine)
The State University of New York at Stony Brook (U.S.A)

In the Research and Academic Staff personel list, we only listed reassignments from Engineering Staff.
In the Research and Academic Staff and Administrative Staff personel lists, we only listed reassignments from/to other NINS
organizations.

140

III Organization

7. Advisory Committee for Research and Management
Members
From universities and related institutes
Umemura, Masayuki Faculty of Pure and Applied Sciences,
University of Tsukuba
Ohta, Kouji

Graduate School of Science,
Kyoto University

Okumura, Sachiko

Graduate School of Science,
Japan Women’s University

Kajita, Takaaki

Institute for Cosmic Ray Research,
The University of Tokyo○ Kusano, Kanya

Institute for Space-EarthEnvironmental Research,
Nagoya University

Sugita, Seiji

Graduate School of Science,
The University of Tokyo

Nakagawa, Takao

Institute of Space and Astronautical
Science

Murakami, Izumi
Momose, Munetake

National Institute for Fusion Science
College of Science,
Ibaraki University

Yamada, Toru

Institute of Space and Astronautical
Science

From NAOJ
Arimoto, Nobuo
Usuda, Tomonori
Gouda, Naoteru
Kobayashi, Hideyuki
Sakurai, Takashi
Takami, Hideki
Tomisaka, Kohji
Noguchi, Takashi
Hasegawa, Tetsuo● Watanabe, Junichi

Subaru Telescope
TMT-J Project Office
JASMINE Project OfficeMizusawa VLBI Observatory
Solar Observatory
Advanced Technology Center
Division of Theoretical Astronomy
Advanced Technology Center
NAOJ Chile Observatory
Public Relations Center● Chairperson ○ Vise-Chairperson
Period: April 1, 2014 – March 31, 2016

III Organization

1418. Professors Emeriti and Staffs Emeriti
Professors Emeriti (NAOJ)
Kakuta, Chuichi
Hiei, Eijiro
Yamashita, Yasumasa
Nishimura, Shiro
Kozai, Yoshihide
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
Professors Emeriti (Tokyo Astronomical Observatory)
Akabane, Kenji
Moriyama, Fumio
Kozai, Yoshihide

142

III Organization

IV Finance
Revenue and Expenses (FY2015)
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

Budget12,323,709
2,445,830
49,90042,286
728,722
268,528
15,858,975
Budget12,634,523
3,528,180
9,106,343
2,445,830
49,900728,722
15,858,975
Budget0

Final Account
12,809,347
2,151,220
49,900244,370
239,092
264,995
15,758,924
Final Account13,318,712
3,499,935
9,818,777
2,151,220
49,900230,173
15,750,005
Final Account
8,919(Unit: ¥1,000)
Budget − Final Account−485,638
294,6100−202,084
489,630
3,533
100,051
Budget − Final Account−684,189
28,245−712,434
294,6100498,549
108,970
Budget − Final Account−8,919IV Finance143

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2015
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)JSPS Fellows
Research Activity Start-up
Grant-in-Aid for Publication of Scientific Research
Results
Total

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

Total

10

89,60026,880116,480

2
13
4
1
9
2

53,300114,100
19,700
7,100
10,4001,700

15,99034,230
5,910
2,130
2,820
510

69,290148,330
25,6109,230
13,220
2,210

1

1,000

0

1,000

42

296,900

88,470385,370

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding
20,700
6,210
7,400
2,220
14,5004,350
42,60012,780Total
26,9109,620
18,85055,3802. Multi-year Fund for FY 2015
Research Categories

Number of Selected Projects

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

19
4
17
40

3. Partial Multi-year Fund for FY2015

144

Research Categories

Number of
Selected Projects

Scientific Research (B)Young Scientists (A)
Total

3
2
5

Budget (Series of Single-year Grants)(Unit: ¥1,000)
Direct Funding Indirect Funding
Total
2,500
750
3,250
1,500
450
1,950
4,000
1,200
5,200

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

Budget (Multi-year Fund)(Unit: ¥1,000)
Direct Funding Indirect Funding Total
500
150
650
0
0
0
500
150
650

VI Research Collaboration
1. Open Use
TypeProject/Center

Okayama
AstrophysicalObservatory

Category
188cm Reflector Telescope (Project Program)
188cm Reflector Telescope (Normal Program)
188cm Reflector Telescope (Student Program)
188cm Reflector Telescope(Miscellaneous Program)

Subaru Telescope
Solar Observatory
Nobeyama Radio
Observatory
Mizusawa VLBIOpen Use at
Observatory
Project/Center

Number of
Total
Accepted Number of
Proposal Researcher

45-m Telescope (General Proposal)
45-m Telescope (Short Program)
45-m Telescope (Back-up Program)
VERA

2
26
2

36 (0)
146 (5)18 (0)

2 Institutes
16 Institutes, 3 Countries
3 Institutes

1

5 (0)

1Institutes

121

343 (58) 64 Institutes, 15 Countries

*

21
5
3

*
*
204 (79) 64 Institutes, 14 Countries
32 (3)
15 Institutes, 1Countries
85 (62) 41Institutes, 13 Countries

22

116 (62) 28 Institutes, 10 Countries

Astronomy Data Center

372

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

210
116
30
8

NAOJ Chile
Observatory

Note

ALMA (Cycle2)

353

ASTE
Mopra

41
19
12
1
20
0

372 (53
at foreign 80 Institutes, 16 Countries
institutes)
210 46 Institutes, 8 Countries
116 (33) 40 Institutes, 11Countries
124
53 Institutes
43
18 Institutes
3,523
324 Institutes, 35 Countries(3,049)251 (38) 40 Institutes, 8 Countries
144 (35) 24 Institutes, 7 Countries
9 Institutes
1 Institutes
16 Institutes

Joint Development Research
Joint 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 PIs. The country count does not include Japan.
The period of ALMA (Cycle2) is September, 2015 from June, 2014.
* The observation data is open to the public on the web. No application is needed to use the data.

VI Research Collaboration

1452. Commissioned Research Fellows
Visiting Scholars (Domestic)
Period: April 1, 2015 – March 31, 2016
Name

Position at NAOJ

Uzawa,Yoshinori

Visiting Professor

Onishi, Toshikazu
Oka, Tomoharu
Tanihata,Isao
Nagao,Toru

Visiting Professor
Visiting Professor
Visiting Professor
Visiting Professor

Affiliated Institute
NICT,Terahertz Technology ResearchCenterOsaka Prefecture University
Keio University
Osaka University
Ehime University

Hayashi,Shousuke

Visiting Professor

Kobe University

Momose, Munetake
Kotake, Kei
Kobayashi, Kaori
Komugi, Shinya
Sagawa,Hideo
Sorai,Kazuo
Takahashi, Keitaro
Niinuma, Koutaro

Visiting Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor

Ibaraki University
Fukuoka University
Toyama University
Kogakuin University
Kyoto Sangyo University
Hokkaido University
Kumamoto University
Yamaguchi University

Oshima, Akitoshi *Visiting Associate Professor

Chubu University

Asaki, Yoshiharu
Kurayama, Tomoharu

Visiting Research Fellow
Visiting Research Fellow

Japan Aerospace Exploration Agency
Teikyo University of Science

Host Project/Center/Division
NAOJ Chile Observatory
NAOJ Chile Observatory
NAOJ Chile Observatory
Division of Theoretical Astronomy
TMT-J Project Office
Center for Computational
Astrophysics
NAOJ Chile Observatory
Division of Theoretical Astronomy
NAOJ Chile Observatory
NAOJ Chile Observatory
NAOJ Chile Observatory
Nobeyama Radio Observatory
Division of Radio Astronomy
Mizusawa VLBI Observatory
Center for Computational
Astrophysics
NAOJ Chile Observatory
Mizusawa VLBI Observatory* Vititing Research Fellow until July, 12, 2015.

JSPS (Japan Society for the Promotion of Science) Postdoctoral Research Fellows
Name
Hada, Kazuhiro

Host Researcher
Research Subject
Probing a relativistic jet in a supermassive black hole with high-resolution radio
Honma, Mareki
monitoring observations

Niinou, Yuu

Probing Cosmic Star Formation at High Redshifts via Afterglows and Host Galaxies
Kashikawa, Nobunari
Gamma-Ray Bursts

Hayashi, Masao

Formation and evolution of elliptical galaxies revealed by internal structures ofKodama, Tadayuki
growing progenitors in galaxy clusters

Arimatsu, Kou

Exploring the outer solar system by stellar occultations observed with wideWatanabe, Junichi
field high-speed cameras

Uchiyama, Mizuho

Studying stellar evolution of forming massive young stellar objects with the midYamashita, Takuya
infrared variability observations

Shouda, Ayaka

Development of the multi-messenger observation system for a gravitational-wave
Flaminio, Raffaele
detector

Shirasaki, Masato

Probing Cosmic Dark Matter and Dark Energy with Higher-Order Statistics of Weak
Hamana, Takashi
Gravitational Lensing

Shinnaka, Yoshiharu

Physicochemistry of the early solar nebula: Thermal history of cometary dust and
Watanabe, Junichiisotopic fractionation of cometary volatile

Yamauchi, Aya

Research in the structure of a distant region of our galaxy using a new distance
Honma, Mareki
measurement method with VERAJSPS (Japan Society for the Promotion of Science) Foreign Research Fellows
Name
None

146

VI Research Collaboration

Program

PeriodHost Researcher

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 sake 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 admitted:
Two (per year in the five-year doctoral course)
Three (per year in 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 / Earthand planets / Sun, stars and interstellar matter / 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
2015, the Department of Astronomical Science accepted five
students in the Basic Course and two students in the Advanced
Research Course. The Department also offered the e-learningclass “Introduction to Observational Astronomy II” as aschool-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.
In order to better prepare students for the international
stage, the Department hosted the Asia Winter School during
January 26 to 28, 2016, as well as the 2015 Summer Student
program at Mitaka, Mizusawa and Okayama campuses toallow undergraduate students a chance to experience researchat the Department of Astronomical Science. In addition to
the existing Research Assistant system, the Department also
provided Associate Researcher positions for the students of the
Department of Astronomical Science.

VII Graduate Course Education

147

(5) Number of Affiliated Staff (2016/3/31)
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
13
1
14
8
9
16
7
13
14
105

(6) Graduate Students (32 students)
1st year (5 students)
Name

Principal SupervisorAndo, Misaki

Iono, Daisuke

Kambara, Nagaaki

Sekii, Takashi

Supervisor
Saito, Masao
Espada, Daniel
Watanabe, Tetsuya

Kikuta, Satoshi

Imanishi, Masatoshi

Kodama, Tadayuki

Matsuno, Tadafumi

Aoki, Wako

Arimoto, Nobuo

Yoshida, Masaki

Suematsu, Yoshinori Hara, Hirohisa

2nd year (2 students)
Name

Principal Supervisor

Michiyama, Tomonari Iono, Daisuke
Kodama, Tadayuki

3rd year (7 students)
Name
Okutomi, Koki
Onoue, Masafusa

Principal Supervisor
Supervisor
Aso, Yoichi
Flaminio, Raffael
Kashikawa, Nobunari Miyazaki, Satoshi

Nagasawa, Ryosuke

Hanada, Hideo

Matsumoto, Koji

Baba, Haruka

Aoki, Wako

Usuda, Tomonori

Ryu, Tsuguru

Hayashi, Saeko
Kashikawa,Nobunari

Usuda, Tomonori

Saito, Masao

Oishi, Masatoshi

Taniguchi, Kotomi

148

VII Graduate Course Education

Observing Colliding Galaxies Using ALMA
Local helioseismology
Observational study of the formation and evolution of galaxies
and supermassive blackholes
Observational study of metal-poor stars to reveal the history of
the near-field UniverseOn the Structure and Heating Mechanism of Solar
Chromosphere and Corona

Supervisor
Research Theme
Kodama, Tadayuki
Observing Starburst Galaxies Using ALMA
Nakanishi, Koichiro
Iwata, Ikuru
Searching for distant clusters with Subaru/HSC

Yamamoto, Moegi

Uchiyama, Hisakazu

Research Theme

Matsuda, Yuichi

Research Theme
Development of laser interferometer module torwards DECIGOStudies on High-z quasars by wide-field imaging observation
Development of software for precise LLR data analysis andstudy of Lunar rotation
Development of infrared instruments and observational research
for the search of earth-like planets
Direct-imaging for intermediate mass giants with RV trends
The study of large-scale structures based on wide-imaging
observations of Subaru telescope
Establishment of new chemistry for carbon-chain molecules instar-forming regions

4th year (10 students)
Name
Yang, Yi

Principal Supervisor
Hayashi, Saeko
Kashikawa,Nobunari

Supervisor
Usuda, Tomonori

Onishi, Kyoko

Iguchi, Satoru

Iono, Daisuke

Observational study towards black-hole mass: resolving thecoevolution process of black hole and galaxy

Onitsuka, Masahiro

Usuda, Tomonori

Takato, Naruhisa

The observational study of the atmospheres of the exoplanetsand the brown dwarfs

Sakurai, Junya

Miyazaki, Satoshi

Kobayashi,
Yukiyasu

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

Shimakawa, Rizumu

Kodama, Tadayuki

Arimoto, Nobuo

Physical conditions of star-forming galaxies at the epoch ofgalaxy assembly and their environmental dependence

Suzuki, Taiki

Oishi, Masatoshi

Saito, Masao

Research on Organic Molecules in the Universe

Pathak, Prashant

Takami, Hideki

Minowa, Yosuke

Development of Adaptive Optics system and Coronagraph for
Subaru Telescope, and observational study of extrasolar planets

Kobayashi, Hiroshi

Osuga, Ken

Tomisaka, Kohji

Radiation Hydrodynamics Simulations of Clumpy Outflows
from Black-hole Accretion disks

Suzuki, Tomoko

Kodama, Tadayuki

Iono, DaisukeStar formation activities at the epoch just before the peak epochof galaxy formation probed by [O III] emitters

5th year (8 students)
Name

Principal Supervisor

Ishikawa, Shogo

Aoki, Sumire
Saito, Yuriko
Matsuzawa, Ayumu
Oh, Daehyeon
Min, Cheul Hong
Giono, Gabriel
Shino, Nagisa
Sukom, Amnart

Kodama, Tadayuki

Research Theme
Observation and Research on Circumbinary Planets
Measurement of dark halo mass by clustering analysis of starforming galaxies

Supervisor
Research Theme
Kodama, Tadayuki
The origin of the morphology of elliptical galaxy
Arimoto, Nobuo
Takada, Tadafumi
Kashikawa, Nobunari Investigating the supermassive black hole to spheroidal stellar
Imanishi, Masatoshi
mass ratio at z~3
Hayashi, Saeko
Research of pointing performance verification method of ALMA
Iguchi, Satoru
Saito, Masao
at sab mm wavelength and absorbing plasma around SMBH
Observational Research on formation of exoplanets and brown
Aoki, Wako
Takami, Hideki
dwarfsHonma, Mareki
Shibata, Katsunori Research for a symbiotic star using VERA
Study of Optical Tests in Ly-α for CLASP Instrumentation
Suematsu, Yoshinori Hara, Hirohisa
Honma, Mareki
Shibata, Katsunori Testing the formation scenario of massive stars by CH3OH maser
Study of star and planetary formation process and theTomisaka, Kohji
Hayashi, Saeko
exoplanets based on infrared observations

Research Student (4 student)
Name
Supervisor

Yang, Yongzhang
Cheng, Chen
De Leon, Jerome
PitogoChida, Hikaru

Research Theme
Research of the interior of the moon and the planet based on an application ofHanada, Hideo
rotation theory
Nakamura, Fumitaka Observational Research of Nearby Star-Forming Regions

Usuda, Tomonori

Near-Infrared Observations of Protoplanetary Disks and Exo-Planets

Honma, Mareki

Probing very Early Stage of Radio Source Evolution in 3C 84 with VERAVII Graduate Course Education149

2. Education and Research Collaboration with Graduate Schools
Name
Kurose, Ippei

Affiliated InstituteSupervisor
The University of Tokyo Ohashi, Nagayoshi

Sakai, Iori

The University of Tokyo Kobayashi, Yukiyasu

Sasaki, Hirokazu

The University of Tokyo Kajino, Toshitaka

Tatsuuma, Misako

The University of Tokyo Kokubo, Eiichiro

Fujii, Yoshinori

The University of Tokyo Flaminio, Raffaele

Fujita, Ayato

The University of Tokyo Gouda, Naoteru

Isoe, MariThe University of Tokyo Kokubo, Eiichiro

Ito, Yuta

The University of Tokyo Gouda, Naoteru

Kimura, Yasuhisa

The University of Tokyo Hara, Hirohisa

Kuramochi, Kazuki

The University of Tokyo Kobayashi, Hideyuki

Kuwahara, Sho

The University of Tokyo Mizuno, Norikazu

Kato, Yuta

The University of Tokyo Mizuno, NorikazuStar forming activity in the z=2–3 proto-clusters with Infrared
Space telescope

Sakai, Daisuke

The University of Tokyo Kobayashi, Hideyuki

Dynamical study of the Galactic center region with VLBI
observations

Hirai, Yutaka

The University of Tokyo Kajino, Toshitaka

Lee, Minju

The University of Tokyo Kawabe, Ryohei

Marchio, Manuel

The University of Tokyo Flaminio, RaffaeleShu, Shibo
Aso, Yusuke

The University of Tokyo Sekimoto, Yutaro
The University of Tokyo Ohashi, Nagayoshi

Ohashi, Satoshi

The University of Tokyo Mizuno, Norikazu

Saito, Toshiki

The University of Tokyo Kawabe, RyoheiStar Formation and SMBH Activities in Merging Galaxies
from High –density Molecular Gas Tracers

Shibagaki, Shota

The University of Tokyo Kajino, Toshitaka

Revealing the origin of r-process elements with astrophysicalsimulations

Shibata, Takashi

The University of Tokyo Kokubo, Eiichiro

Theoretical Study of Formation and Evolution of Planetary
Systems

Sekiguchi, Sigeyuki The University of Tokyo Sekimoto, Yutaro

150

ThesisObservational Study of Star Forming Regions
Development of equipment and data analysis related to
JASMINE
Neutrino oscillation in super novas
Theoretical Study of Formation and Evolution of Planetary
Systems
Development of the vibration isolation system for the
KAmioka GRavitational-wave Antenna
Dynamical Structure and its Evolution of the Milky Way
Theoretical Study of Formation and Evolution of Planetary
Systems
The dynamical structure of the Galaxy
Study of Sub-arcsec Transition-Region Structures at theFootpoints of Active-Region Loops
A test of in-beam phase referencing with VERA
Triggered star formation of the young massive clusters by thecloud-cloud collisions

Origin of the r-process elements in galactic chemodynamical
evolution model
Environmental effects on galaxy evolution in protoclusters
Development, characterization and improvement of themirrors for the KAGRA gravitational wave detector
Development of MKID camera
Environmental effects on star and disk formation
Chemical evolution of the star-forming cores in the giant
molecular clouds

Development of broadband polarization MKID camera for
Cosmic Microwave Background B-mode observations
Early cosmic merger of multiple black holes
Formation and Evolution of Protoplanetary Disks
Development of superconducting device for wideband
observation of CMB B-mode polarization

Tagawa, Hiromichi
Koyamatsu, ShinThe University of Tokyo Gouda, Naoteru
The University of Tokyo Ohashi, Nagayoshi

Sekine, Masakazu

The University of Tokyo Sekimoto, YutaroHara, Takuji

The University of Tokyo Gouda, Naoteru

Construction of the galaxy model with phase space
distribution

Hara, Chihomi

The University of Tokyo Kawabe, Ryohei

Structures and Kinematics of Dense gas and Molecular
Outflow in YSOs.

Fujii, Kosuke

The University of Tokyo Mizuno, Norikazu

Observational Study of the triggered star formation in the
Large Magellanic Cloud

Kiyokane, Kazuhiro The University of Tokyo Mizuno, Norikazu

Observational Study of Star Formation process with radio
observations

VII Graduate Course Education

3. Commissioned Graduate Students
Doctoral Course
Silva, Andrea

Affiliated Institute
PeriodDepartment of Physics and 2015/4/1~
Astronomy, Tufts University 2016/3/31

Supervisor

ThesisIono, Daisuke

ALMA Observations of Starburst Galaxies

Matsuo, Mitsuhiro

Kagoshima University

2015/4/1~
2016/3/31

Saito, Masao

Observations of molecular clouds in the outergalaxy with a wideband digital spectrometer

Ui, Takahiro

Hiroshima University

2015/4/1~
2016/3/31

Yamashita, Takuya

Observational study of the young planet
2MASSJ0525+0125

Oya, Masahito

Nihon University

2015/4/1~
2016/3/31

Watanabe, Junichi

Development of precise adaptive optics for direct
observation of extrasolar planets

Sekiguchi, Takanori

The University of Tokyo

2015/4/1~
2015/9/30

Flaminio, Raffaele

Development of Vibration Isolation System for
KAGRA

Master’s Course

Affiliated Institute

PeriodSupervisor

ThesisMori, Takahiro

Tokyo Universityof Agriculture andTechnology

2015/4/1~
2016/3/31

Watanabe, Junichi

Wideband Laser frequency comb for IR Doppler
observation

Aoki, Misa

International Christian
University

2015/4/1~
2015/9/30

Aoki, Wako

Study of Galactic chemical evolution based onabundance analysis of metal-poor stars

Kozuki, Yuto

Osaka Prefecture
University

2015/4/1~
2016/3/31

Noguchi, Takashi

100 GHz SIS Mixer with wide RF and IF
bandwidth

Sunaga, Naoki

Shizuoka University

2015/4/1~
2015/9/30

Kajino, Toshitaka

Primordial nucleosynthesis in the early universe

Tsuchiya, Chie

The Open University ofJapan

2015/4/1~
2016/3/31

Watanabe, Junichi

Effect of Earth’s motion to expansion of radiantpoints in meteor showers

Fukagawa, Nao

International Christian
University

2015/10/1~
2016/3/31

Kodama, Tadayuki

Inflow and Outflow of Gas in Galaxies and Its
Mass Dependence

4. Degrees Achieved with NAOJ Facilities
Name

DegreeThesisDirect Imaging Analysis of the Circumstellar Disks and Planetarymass Companions on Wide Orbit Around a Disk-host StarOh, Daehyeon

Doctor of Philosophy, SOKENDAI

Giono, Gabriel

Doctor of Philosophy, SOKENDAI

Novel Instrumentation to Reach the 0.1 % Polarization Accuracy for
the Chromospheric Lyman-Alpha Spectro-Polarimeter

Nagasawa, Ryosuke

Master of Science, SOKENDAI

Development of software for precise LLR data analysis and study of
Lunar rotation

VII Graduate Course Education

151

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: 19,729
Open Facilities: 65-cm Telescope Dome (Observatory
History Museum), 20-cm Telescope Dome, Solar
Tower Telescope, Exhibit Room, Repsold Transit
Instrument Building (Transit Instrument Museum),
Astronomical Instruments Museum, Gautier Meridian
Circle, Old Library[Open year-round]
Dates: April to March (except for the New Year’s season),
9:00–17:00 daily
Visitors: 17,415
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: 4,717 (23 events)
Open Facility: 50-cm Telescope for Public Outreach[4D2U Theater Showings]
Dates: Friday before second Saturday; third and fourth
Saturdays
Visitors: 4,446 (35 events)
Open facility: 4D2U Theater[Special Open-House Event] Mitaka Open House Day
Dates: October 23 (Fri), 2015, 14:00–19:00
October 24 (Sat), 2015, 10:00–19:00
Topic: The Challenges Awaiting Astrobiology
Visitors: 5,036
This event is jointly sponsored by NAOJ, the Universityof Tokyo School of Science Institute of Astronomy, the
SOKENDAI Department of Astronomical Science, and the
newly established 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 of Tokyo (“The Long
Road: 13.8 Billion Years from the Start of the Universe to
Us” Masuo Tanaka, Associate Professor, University of Tokyo)
and NAOJ (“Astrobiology, Opening ‘New Worlds’ in the
Universe” Motohide Tamura, Professor, University of Tokyo,
NAOJ, Astrobiology Center; and “Astrobiology, Approaching
the Origins of Life” Akihiko Yamagishi, Professor, Tokyo
Univsersity of Pharmacy and Life Science).
* Guided tours corresponding to group tours (Dantai Kengaku)
were also held. In addition the “Information Space of Scienceand Astronomy” was opened in 2015 near the south entrance of
Mitaka Station to distribute information.

The campus is opened to the public in cooperation with
the Oshu Space & Astronomy Museum (OSAM: Yugakukan)
located in the campus.
[Special Open Day] Held as part of Iwate Galaxy Festival 2015
(Festival Hours: 10:00-21:00)
Date: August 22 (Sat.), 2015, 10:00–16:30
Visitors: Approximately 660
Same as last year, the Open Day was co-hosted with Ihatov
Space Action Center / the Oshu Space & Astronomy Museum(OSAM: Yugakukan) and the city of Oshu.
Although a performance by a marching band from a local
elementary school and tours of the 20-m parabolic antenna werecanceled due to rain, NAOJ offered a chance to experience
operating the 20-m parabolic antenna; a commemorative photobooth; plastic bottle rocket launching; a quiz game; tours of thesupercomputer “Aterui”; a science cafe; and exhibitions of theresearch highlights of the VERA, RISE, and CfCA projects.
As a new event for this year, a special guided tour of theKimura Hisashi Memorial Museum, the Array Operations
Center (AOC), and the VLBI correlator was carried out, and waswell received.
A special lecture was given by Tomoaki Ishiyama, Associate
Professor at Chiba University, entitled “Approaching the darkside of the Universe with the power of a supercomputer —dark matter structure formation—”. He covered studies on
the formation and evolution of the structure of the Universe
using supercomputers. His talk was easy to understand for theaudience.
OSAM (Yugakukan) offered various experiments in thescience stalls, workshops, etc., which were carried out by thestudents on internships. The Special Open Day was a great
success, strengthening ties with the local people.
Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for the New Year’s season)
Visitors: Approximately 1,551[Special Open Day]
Date: August 8 (Sun.), 2015, 12:00–20:00
Since a typhoon hit the VERA Iriki station and the public

152

VIII Public Access to Facilities

open event was canceled last year, in 2015 the event was held forthe first time in two years. This special open event was held inconjunction with “Yaeyama Highland Star Festival 2015” 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 telescopes and observation building were held
dozens of times. An astronomical 3D movie was presented by
the 4D2U project team for the first time at Iriki station. As the
special lecture for the year, Dr. Yoshiaki Tamura from Mizusawa
VLBI Observatory gave a talk about “the Great Eastern Japan
Earthquake” from the perspective of a geophysicist. At night,a public stellar observation was held under the starlit sky. All
visitors had fun and were satisfied the with many scientificprograms offered in this festival.
Ogasawara: VERA Ogasawara Station[Open year-round]
Dates: April to March (except for the New Year’s season)
Visitors: 8,540[Special Open Day]
Date: February 14 (Sun.), 2016, 10:00–16:30
Visitors: 222
A special open house event was held this year again under
the name “Star Island 15.” Same as last year, the free shuttle
buses were appreciated by the visitors. The number of visitors
was 222, which was more than last year. Because the number ofthe residents on the island is about 2,000, more than 10 % of theislanders visited this event.
NAOJ offered such attractions as exhibits about the research
results of VERA, RISE, and TMT; science experiments; quiz
games; and short lectures.
On February 13, a stargazing party was held by the
local Ogasawara astronomy club, and NAOJ members also
participated. Thanks to good weather, the number of visitors
reached about 50.
In addition, Space Lectures were also given by Nobuyuki
Sakai of the Mizusawa VLBI Observatory and Hiroki Harakawa
of TMT-Japan at the Ogasawara Visitor Center on the night ofFebruary 14.
Ishigaki-jima: VERA Ishigaki-jima Station[Open year-round]
Dates: April to March (except for the New Year’s season);premises are open to the public 24 hours/day, andthe observation rooms are open during the hours of
10:00–16:30
Visitors: 2,713

The Special Open Day was held as a part of the Southern
Island Star Festival.
Same as previous years, attractions like antenna tours, photobooth stickers, merchandise, commemorative lectures, andexhibits were offered.
Ishigaki-jima: Ishigaki-jima Astronomical Observatory[Open year-round]
Dates: April to MarchOpen Hours: Wednesdays through Sundays (Except for
the New Year’s season; when Monday/Tuesday is anational holiday, it is opened and closed on the nextday.), 10:00–17:00
Stargazing sessions: Evenings on Saturdays, Sundays,
Holidays, and Star Festival week days (19:00–22:00),
two 30-minute sessions per evening (four in August)
4D2U screenings: from 15:00 to 15:30 every day when the
Observatory is open
Visitors: 13,906 (1,032 during the Southern Island Star
Festival)
Open facilities: Murikabushi 105-cm optical/infrared
telescope, Hoshizora Manabi no Heya (Room of
Learning the Starlit Sky) (featuring the 4D2U “FourDimensional Digital Universe”), interior of theobservation dome (including exhibits of astronomical
images)The “Hoshizora Manabi no Heya” (Room of Learning theStarlit Sky), constructed adjacent to the Observatory in 2013 by
the city of Ishigaki, was very popular, welcoming 3,925 guests.
[Southern Island Star Festival 2015]
Dates: August 15 (Sat.) to August 23 (Sun.), 2015
Visitors: 10,930
This year is the 14th anniversary of both the completionof VERA Ishigaki-jima Station and the Southern Island Star
Festival. Approximately 9,000 visitors attended the light-down
stargazing event blessed with better weather than ever before.
In addition, because this was the 70th anniversary of theend of World War II, a film named “Vega shining over thebattlefield” produced by the Yamanashi Prefectural Science
Museum was screened every day during the period, and these
became memorial screenings. The annual planetarium screening
was attended by 435.
The activities at Ishigaki-jima Astronomical Observatory
help regional development through 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 be used as a tourism resource. Considering this situation, we
will continue to strengthen our ties with other associations.

[Special Open day]
Date: August 16 (Sun.), 2015, 10:00-17:00
Visitors: 238

VIII Public Access to Facilities

1533. Nobeyama Campus

4. Okayama Campus[Open year-round]Open Time: 8:30–17:00 (every day except the New Year’s
season (Dec. 29 to Jan. 3), open until 18:00 during
the summer (Jul. 20 to Aug. 31))
Visitors: 50,185
Open facilities: Nobeyama 45-m Radio Telescope, Nobeyama
Millimeter Array, Nobeyama Radioheliograph, etc.
(viewing only)

Okayama Astrophysical Observatory[Open year-round]
Dates: 9:00–16:30 daily
Visitors: 11,126
Open Facilities: Window view of Okayama 188-cm
Reflector Telescope[Open House Day]
Date: August 22 (Sat.), 2015, 9:30–16:00
Visitors: 2,429
The Nobeyama branch was crowded with 2,429 visitors on
the 2015 Open House Day. The theme of the Open House Day
was “Searching for the Origin of Life in the Universe.” We had
two lectures on the theme, which attract large audiences every
year. One was “The Search for Life in the Universe” by theformer Director, Prof. Miyama, Shoken . The other was “Biotic
Species in the Universe 2 –Life is linked with the Universe”
by Dr. Ohishi, Masatoshi (NAOJ). We had some establishedhands-on events such as touch the main reflector panel of the
Nobeyama 45-m Radio Telescope, the antenna handicrafts, solar
radio wave detector handicrafts, and the antenna origami. In
addition, some short lectures and the Q&A corner were carriedout. These events were held by 119 staff members, including
NRO alumni, other project staff members, and volunteers.
Also with NRO character, Dr.Nobeyama and Nagano Pref. PR
character, ARUKUMA. NRO was more festive on that day.
[Jimoto Kansha Day (Thanks Day for the locals)]Date: October 10 (Sat.), 2015, 13:30–19:00
Visitors: 76
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 established this event incooperation with Tsukuba University, Agricultural and Forestry
Research Center, Yatsugatake Forest and Shinshu University,
Faculty of Agriculture, Education and Research Center of Alpine
Field Science. As an event, we had the forest and trees rally forwalking around 4 points in Tsukuba University Meguminomori(the Mercy Forest), which had its opening ceremony on thesame day. It was very popular among the visitors. We also had
an introduction from each institute about its research activities.

154

VIII Public Access to Facilities[Special Open House]
Date: August 29 (Sat.), 2015, 9:30–16:30
Visitors: 366
We had two Exoplanet Naming commemorative lectures at
the 188-cm reflector telescope in the dome.
The first lecture, by Associate Professor Bun-ei Sato ofTokyo Institute of Technology, was “Exoplanets found on
Okayama.” The second lecture, by Professor Norio Narita of
the AstroBiology Center/NINS, was “Exploring exoplanetswith the new observation instrument MuSCAT on the 188-cm
telescope.” The both 90 minute lectures attracted nearly 110
audience members. The special open house event was co-hosted
with Asakuchi City and the Asakuchi City Board of Education,with support from the Yakage Town Board of Education. In
particular, the Observatory would like to thank the members of
Asakuchi City and the Asakuchi City Board of Education for
their considerable assistance in arranging complimentary shuttle
bus service between the Observatory and temporary parking at
Kamogata Station on the JR San’yo Main Line.
[Special Stargazing Party]
Date: April 11 (Sat.), 2015, 18:30–22:45
Visitors: 112
186 applications for 544 applicants were received. Castor ofGemini and Jupiter were viewed.
Date: November 3 (Tue., Culture Day), 2015, 17:00–21:15
Visitors: 103
76 applications for 192 applicants were received. Vega of
Lyra and globular cluster M15 were viewed.
Special stargazing parties co-hosted with the Okayama
Astronomical Museum were held twice over the course of theyear, in spring and fall. Maximum participation for each special
session was 100. As applications exceeded capacity for bothsessions, participants were selected by lottery, with 120 winners
being selected to allow for cancellations.

5. Subaru Telescope[Summit Facility Tour]
Dates open for public tour: 77 (these dates are listed in the
public tour program page at the Subaru Telescope’s
web site; the tour was cancelled during the summer
due to the road closure, 16 days were affected;
no tours scheduled during the winter months ofDecember to March)
Public tour visitors: 421 (due to the road closure, etc., morethan 100 people were not able to visit)
Special tour visitors: 131 visits, 538 visitors
As some special tours were conducted during public tour
programs, the total number of actual visitors was 923.
*Special note: During the summer from late June to midAugust, the tours were cancelled due to the closure of theMaunakea access road and Visitor Information Station. The
period corresponds to summer vacation in Japan, the U.S.A.,
and many other places, so it had a large impact on the tour
program.
[Base Facility Tour]Special tour visitors: 67 visits, 393 visitors[Public information]
Primary means of public information announcement isposting it on the official website http://subarutelescope.org• Science results from the Subaru Telescope – 14
Japanese and 17 English articles• Depictions of special activities, or announcements
about Calls for Proposals and recruitment – 14 Japaneseand 24 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 (for English, started February 2015)• YouTube channels – SubaruTelescopeNAOJ (for Japanese),
SubaruTelescopeNAOJe (for English)[Outreach]
1. Lectures at Subaru Telescope’s Hilo Base Facility
2015
July 13: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility to the Upward Bound Summer
Workshop for local high school students.
July 24: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility to the PAES (Pacific Astronomy& Engineering Summer Summit) for high school students from
5 countries.

August 5: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the junior high School
students from Nago City in Okinawa.
August 18: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Fukushima Kenjin Kai
members.
August 19: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Kanto Gakuin HighSchool students from Kanagawa.
August 19: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the junior high school
students from Fukushima.
August 20: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Waseda Koto Gakuin
High School students from Tokyo.
August 24: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Kawagoe High School
students from Saitama.
August 26: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Hibiya High School
students from Tokyo.
September 23: Subaru Telescope staff gave a lecture at
Subaru Telescope’s Hilo Base Facility for the Japanese Group(astronomy supporters from Japan).
September 28: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the University of the Ryukyus
students.
October 15: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Namiki Secondary School
students from Ibaraki.
November 18: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Osaka Kokusai Science
Club members.
November 20: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the selected high school
students from Okinawa.
December 7: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Ryugasaki Daiichi HighSchool students from Ibaraki.
December 8: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Senri High School
students from Osaka.

VIII Public Access to Facilities

155

2016
January 8: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Seisho High School
students from Nara.
January 26: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Sanbonmatsu High School
students from Kagawa.
March 2: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Nagaoka High School
students from Niigata.
March 15: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Ritsumeikan Uji HighSchool students from Kyoto.
March 17: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Masuda High School
students from Shimane.
March 23: Subaru Telescope staff gave a lecture at Subaru
Telescope’s Hilo Base Facility for the Kanagawa University
High School students.

conferencing system from Subaru Telescope’s Hilo Base Facility
to Science Museum in Tokyo.
November 9: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to Masuda High School in Shimane.
November 16: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to Masuda High School in Shimane.
November 27: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to the Galaxity in Adachi Ward of Tokyo.
December 2: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to Matsubara Junior High School in Shiga.
December 11: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to Arakawa 3rd Junior High School in Tokyo.
December 18: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to Inagawa Town in Hyogo.

2. Remote Presentation

2016

2015

February 12: Subaru Telescope staff gave a presentation via
remote conferencing system from Subaru Telescope’s Hilo Base
Facility to Wakayama Shin-Ai High School.

April 25: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to Science Museum in Tokyo.
June 6: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to Science Museum in Tokyo.

March 5: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to Science Museum in Tokyo.

3. Lectures, Demonstrations, Workshops, etc. in the Vicinity
June 8: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to Izumo High School in Shimane.
July 2: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to Masuda City in Shimane for its Science Town event.
July 14: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to the University of the Ryukyus in Okinawa.
July 17: Subaru Telescope staff gave a presentation via remote
conferencing system from Subaru Telescope’s Hilo Base Facility
to Tokyo Mirai University in Tokyo.
October 31: Subaru Telescope staff gave a presentation via remote

156

VIII Public Access to Facilities

2015
April 17: Subaru Telescope staff gave a lecture and panel
discussion for the Journey master educators workshop, career
panel discussion at the ʻImiloa Astronomy Center in Hilo.
May 3: Subaru Telescope staff gave a lecture at the Honpa
Hongwanji Betsuin in Hilo.
July 13: Subaru Telescope staff gave a lecture at the Lyman
Museum in Hilo.
July 21: Subaru Telescope staff gave a lecture for the PAES (PacificAstronomy & Engineering Summer Summit) program at the
University of Hawai`i at Hilo.

August 18: Subaru Telescope staff gave a lecture for the highschool students from China at the University of Hawai`i at Hilo.

November 4: Subaru Telescope staff gave two lectures for
Ritsumeikan High School students in Kyoto.

August 21: Subaru Telescope staff gave a lecture for the highschool students from Sumoto City, Hyogo and the local highschool students at the Kilauea Military Camp.

November 6: Subaru Telescope staff gave a lecture at Niwakubo
Junior High School in Osaka (as part of the Fureai “Friendly”
Astronomy Program).

Sepember 10–13: Subaru Telescope staff gave three lectures at
HawaiiCon.

5. Others

October 16: Subaru Telescope staff gave a lecture at the ʻImiloa
Astronomy Center in Hilo.
November 17: Subaru Telescope staff gave a lecture for the Chiba
Meitoku High School students at the University of Hawai`i at
Hilo.
2016
January 2: Subaru Telescope staff gave a lecture at the Visitor
Information Station, Maunakea.
January 10: Subaru Telescope staff gave a lecture for the Seisa
Junior High School students from Kanagawa at the Kilauea
Military Camp.
January 30: Subaru Telescope staff provided four astronomy
workshops during Onizuka Science Day at the University of
Hawai`i at Hilo.
March 7–11: For the Journey through the Universe program,
Subaru Telescope staff went to 55 classes in local public schools
and delivered presentations, hands-on experiences, and otherdemonstrations.

4. Lectures in Japan
2015

2015
May 2: Subaru Telescope staff provided a booth with many
hands-on activities about the Subaru Telescope at the AstroDay
event in Hilo and interacted with hundreds of families in the local
community.
August 2: Subaru Telescope staff provided a booth at the Aloha
Art Festival in 'Imiloa Astronomy Center, Hilo.
August 3–14: Subaru Telescope staff provided a booth and gave
demonstrations at the IAU General Assembly in Honolulu.
2016
January 27: Subaru Telescope staff provided a booth and gave
demonstrations at a special event at 'Imiloa Astronomy Center in
Hilo.
January 30: Subaru Telescope staff made presentations about
the Subaru Telescope at the Onizuka Science Day event at the
University of Hawai`i at Hilo and interacted with hundreds offamilies in the local community.
February 18: Subaru Telescope staff provided a booth at the
Career Expo and gave demonstrations for local Junior HighSchool and High School students in Hilo.

April 5: Subaru Telescope staff gave a lecture at Science Museumin Tokyo.

February 21: Subaru Telescope staff provided an exhibition withmany hands-on activities about the Subaru Telescope at the ‘Imiloa
Astronomy Center’s open house and interacted with a wide rangeof age groups in the local community.

October 5 & 7: Subaru Telescope staff gave a lecture at the Nanbu
Medical Center and Nanbu Child Medical Center in Okinawa.

March 26: Subaru Telescope staff provided an exhibition withother observatories and interacted with the local community.

October 6: Subaru Telescope staff gave a lecture for Okinawa
Shogaku High School and Junior High School students in
Okinawa.

6. Media Coverage
Japanese 14, English 8

October 8: Subaru Telescope staff gave a lecture at the Ishigaki
City Hall in Okinawa.
November 2: Subaru Telescope staff gave a lecture at theInternational Science Fair at Ritsumeikan High School in Kyoto.

VIII Public Access to Facilities157

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

category

Business Trip

South Korea
47
China
19
Thailand
9
Taiwan22
Hong Kong
1
Singapore4
Indonesia
1
Philippines
0
Other areas in Asia
6
Hawai`i
83
U.S.A.
89
Australia
9
Italy
11
U.K.
22
France25
Canada4
Guam, Saipan0Germany
17
Other areas in Europe and Oceania
56
Mexico0Brazil0Africa3
Other areas in South and Central America *
35
Total
463
* Most travelers to South and Central America went to Chile.

158

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

47
19
9
22
1
4
1
0
6
83
89
9
11
22
25
4
0
17
56
0
0
3
35
463

X Award Winners
Award Recipients
Miyazaki, Satoshi;
Komiyama, Yutaka;
Kawanomoto, Satoshi

Affiliated Division
Advanced Technology
Center/Subaru Telescope/
Subaru Telescope

Job Title

Award

Date

Associate
Professor/AssistantProfessor/ResearchExpert

The Commendation for Scienceand Technology by the Minister of
Education, Culture, Sports, Scienceand Technology Prizes for Science andTechnology (Research Category) 2015

2015/4/15

D&AD Digital Design Wood Pencil

2015/5/21

Royal Astronomical Society 2015
Group Achievement Award ingeophysics

2015/7/2

The Second ISAS Award

2016/2/6

PARTY/National
Astronomical
Observatory of Japan
Hinode Extreme
Ultraviolet Imaging
Spectrometer (EIS) team

Hinode Science Center

Suematsu, Yoshinori

Hinode Science Center

Associate Professor

Chiba,Kurazo;
Kawashima, Susumu:
Kikuchi, Kenichi

NAOJ Chile Observatory

Specially Appointed
Senior Specialist/
2015 NAOJ Director General Prize
Chief ResearchEngineer/Chief
Research Engineer

2016/3/4

Tatsuzawa, Kaichi;
Okayasu, Rikako;
Saito,Yasufumi

Division of Radio
Astronomy/Division ofRadio Astronomy/Advanced
Technology Center

Research Expert/
Research
Supporter/ResearchExpert2015 Director General Prize

2016/3/4

Miyazaki, Satoshi

Advanced Technology
Center

Associate Professor

20th Chushiro Hayashi Prize

2016/3/15

Tanaka, Masaomi

Division of Theoretical
Astronomy

Assistant Professor

27th Japan Astronomical Society
Research Award

2016/3/16

Iye, Masanori

TMT-J Project Office

RCUH/Professor
emeritus

The International Society for OpticalEngineering, SPIE Senior Fellow—

X Award Winners

159

XI Library, Publications
1. Library
Number of books in each library (2016/3/31)
Japanese Books
Mitaka17,277
Okayama
220
Nobeyama
1,225
Mizusawa
4,957
Hawaii
1,568
Total
25,247

Foreign Books
45,487
3,344
6,279
18,074
4,259
77,443

Total
62,764
3,564
7,504
23,031
5,827
102,690

Number of journal titles in each library (2016/3/31)
Japanese Journals
Foreign Journals
Mitaka637
773
Okayama4
18
Nobeyama
16
82
Mizusawa
659
828
Hawaii
18
18
Total
1,334
1,719

Total
1,410
22
98
1,487
36
3,053

2. Publication
Here we list continuing publications produced by NAOJ in FY 2015.
The data is based on publications delivered to the libraries.
Mitaka01) Report of the National Astronomical Observatory of Japan, Vol. 17: 1 issue02) Annual Report of the National Astronomical Observatory of Japan (in Japanese), no. 27, Fiscal Year 2014: 1 issue03) Annual Report of the National Astronomical Observatory of Japan (in English), vol. 17, Fiscal Year 2014: 1 issue04) National Astronomical Observatory Reprint, No. 2651–2748; 98 issues05) Calendar and Ephemeris, 2016; 1 issue06) NAOJ News, No. 261–272; 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), 2016; 1 issue10) National Astronomical Observatory of Japan 2015 External Review Report; 1 issue160

XI Library, Publications

XII Important Dates
April 1, 2015 – March 31, 20162015
April 2

Accompanying the reopening of the 4D2U Dome Theater, a private showing was held for the press, with 26 guests
in attendance.

April 11

Spring 2015 Special Stargazing Party held at Okayama Astrophysical Observatory, with 112 visitors in attendance(out of 544 applicants).

April 19

Sixth Open Observatory event held at the Ibaraki University Center for Astronomy and the NAOJ Mizusawa VLBI
Observatory Ibaraki Station, with approximately 230 visitors in attendance.

April 23

The Joint ALMA Observatory issued the ALMA Cycle 4 call for proposals for early scientific observations whichstarts from October 2015 and received by the deadline a total of 1,582 observation proposals from astronomers
around the world, which exceeded the number of proposals for Cycle 2 that counted 1,382. A total of 3,608
astronomers are engaged in the submitted proposals for Cycle 3 as either principal investigators or co-investigators.

May 2

Subaru Telescope staff provided a booth with many hands-on activities about the Subaru Telescope at the AstroDay
event in Hilo and interacted with hundreds of families in the local community.

May 7~8

Mr. Kosaburo Nishime, State Minister for Internal Affairs and Communications and his party visited the
Operations Support Facility (OSF) and Array Operations Site (AOS) of ALMA for a study tour.

May 25~28“Artists in Residence in NAOJ Nobeyama” was held in Nobeyama Radio Observatory by Siga-Kogen Roman
Museum (Yamanouchi-machi, Nagano). There were 5 participants who were artists related with Nagano Prefecture.

June 1~5
June 23~24
July 4
July 7
July 21Observation training of Radio Astronomy at Nobeyama Radio Observatory for Undergraduate Students was
performed; there were 12 participants.
“Summer Break Junior Astronomical Classes + You are Galileo!” held in the Mitaka area.
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
100 visitors in attendance.
NAOJ Chile Observatory staff members gave a lecture as a Tanabata event at the Japanese School in Santiago.
Subaru Telescope staff gave a lecture for the PAES (Pacific Astronomy & Engineering Summer Summit) program atthe University of Hawaii at Hilo.

July 21~24,
July 27

Facility Guide Week for Educational Organization was carried out at Nobeyama Radio Observatory.

July 27

The National Astronomical Observatory of Japan (NAOJ) and the Academia Sinica Institute of Astronomy andAstrophysics (ASIAA) in Taiwan signed an agreement concerning ALMA, following the conclusion of a prioragreement concerning the operations and development of ALMA which was entered into as of July 21 between the
National Institutes of Natural Sciences of Japan (NINS) and Academia Sinica (AS) in Taiwan. These agreements
will further strengthen cooperation between Japan and Taiwan for the operations of ALMA.

August 1~3

Ninth Z-star Research Team event held for high school students in the six Tohoku prefectures, with 11 participants
attending. The participants were divided into two groups and searched new water vapor masers using VERA
Mizusawa 20m radio telescope. One team found 3 maser candidates from variable stars and the other team found 3
maser candidates from star forming regions.

August 1~3

The VLBI experiment was successfully carried out connecting ALMA's antennas and six VLBA's antennas of the
National Radio Astronomy Observatory.

August 1
Sixth International Festival of Scientific Visualization — International Year of Light 2015 — held with over 1~September 30 million visitors attending during the festival period.
August 8

Special Open House of VERA Iriki station held jointly with the Yaeyama Highland Star Festival 2015, withapproximately 4,000 visitors in attendance.

August 12~14

Chura-boshi Research Team workshop for the local Yaeyama high school in Ishigaki-jima held at VERA Ishigakijima Station and Ishigaki-jima Astronomical Observatory, with 18 participants in attendance. One team using
radio-waves discovered 1 maser. A second team using visible light observations with the Murikabushi telescope
discovered 3 asteroids.

XII Important Dates

161

August15~23

The Southern Island of Star Festival 2015 held together with a special open house event at the VERA Ishigaki-jima
Station and Ishigaki-jima Astronomical Observatory with approximately 10,930 visitors to the whole Star Festival.
Events included an astronomical observation party at the Ishigaki-jima Astronomical Observatory, attended by 257
visitors; and a special public opening of the VERA Station attended by 238 visitors.

August 22
August 22
August 29

Iwate Galaxy Festival 2015, a special open house day of Mizusawa Campus, held with 660 visitors in attendance.
Open House day of Nobeyama Radio Observatory. There were 2,429 visitors for this event.
Special Open House event held at Okayama Astrophysical Observatory, with 366 visitors in attendance.

September 26~October 25“Information Space of Science and Astronomy” (Mitaka Station, South Exit, Chuo Street) opened. Special exhibit“Commemorating the International Year of Light, Cosmic Light” opened with 5,482 guests in attendance.
* Established as a joint establishment with the Mitaka City Planning Board in cooperation with Mitaka City and
Mitaka Network University, this space distributes information about astronomy and the Universe. In the half-a-year
before the end of the fiscal year, it welcomed 9,981 guests.

September 27 “International Symposium on the NAOJ Museum” held with 96 guests attending from 9 countries; 7 guests~September 29 participated via internet relay from Japan and other countries.
October 10“Jimoto Kansha Day (Thanks Day for the Locals)” was held at Tsukuba Univ. Forest. It was carried out by 3
Nobeyama Institutes (Tsukuba and Shinshu Universities and Nobeyama Radio Observatory). There were 76
participants.

October 14

The Joint ALMA Office (JAO) welcomed 30 students of the Japanese School in Santiago including those at thethird grade or higher and gave a tour for their out-of-school activity.

October 18

The third “three selections of Japanese starry sky summit” was held in Minamimaki-mura by the executive
committee consisting of Minamimaki tourist association, Minamimaki-mura, and Nobeyama Radio Observatory.
This summit also cooperated with Ishigaki and Bisei astronomical observatory.

October 23~October 24

Mitaka Open House Day held, with 5,036 visitors in attendance.

November 3

Fall 2015 Special Stargazing Party held at Okayama Astrophysical Observatory, with 103 visitors in attendance (outof 192 applicants).

November 24

22th Astronomy Lecture for Science Reporters “In what does Rikanenpyo tell us now?” held, with 39 participantsin attendance.

November 25

A ceremony for FY 2015 continuous service recognition held. 5 staff members were recognized: Takashi Ito,
Tomoyuki Onishi, Ikuko Yoshikawa, Hiroko Kikkawa, Yukiko Kamata.

As part of the reconstruction support for the children in the areas affected by the Great East Japan Earthquake, theDecember 3~4 NAOJ Chile Observatory provided distance learning connecting ALMA Operations Support Facility (OSF) with ajunior high school in Fukushima Prefecture and an elementary school in Miyagi Prefecture.
December 12

ALMA public lecture/Osaka Science Museum Special Night “Exploring with ALMA” held, with 200 guests in
attendance.

December 13

NAOJ lecture meeting “The challenge which exceeded space-time: General Relativity’s 100th Anniversary andGravitational Wave Astronomy” held at Hitotsubashi Hall, Hitotsubashi University with 400 guests in attendance.

December15

The National Institutes of Natural Sciences of Japan (NINS), the European Southern Observatory (ESO), and the
National Science Foundation (NSF) signed an agreement concerning the operations of ALMA in Tokyo.

2016
January 7~February 21

162

Photo exhibit “Observatory Landscapes” opened at “Information Space of Science and Astronomy” with 1,404 guests
in attendance.

January 28

The NAOJ Chile Observatory gave talks at a summer camp for students from the first to fourth grades of the Japanese
School in Santiago.

January 30

Subaru Telescope staff made presentation about the Subaru Telescope at the Onizuka Science Day event at the
University of Hawai'i at Hilo and interacted with hundreds of families in the local community.

February 14

Star Island 15 open house event of VERA Ogasawara Station held, with 222 visitors in attendance (more than the
average year).

March 7~11

For the Journey through the Universe program, Subaru Telescope staff went to 55 classes in local public schools anddelivered presentations, hands-on experiences, and other demonstrations.

March 30

A ceremony for FY 2015 continuous service recognition for retiring staff members held. 4 staff members wererecognized: Takashi Sakurai, Goro Sasaki, Yasuo Torii, Yoshizo Iizuka.

XII Important Dates

XIII Publications, Presentations
1. Refereed Publications
Aasi, J., et al. including Fujimoto, M.-K., Hayama, K., Kawamura,S., Mori, T., Nishida, E., Nishizawa, A.: 2015, Characterization of
the LIGO detectors during their sixth science run, Classical Quantum
Gravity, 32, 115012.
Abbott, B. P., et al. including Flaminio, R., LIGO ScientificCollaboration, Virgo Collaboration: 2016, Astrophysical Implicationsof the Binary Black Hole Merger GW150914, ApJ, 818, L22.
Abbott, B. P., et al. including Flaminio, R., LIGO ScientificCollaboration, Virgo Collaboration: 2016, Observation ofGravitational Waves from a Binary Black Hole Merger, Phys. Rev.
Lett., 116, 061102.
Abbott, B. P., et al. including Flaminio, R., LIGO ScientificCollaboration, Virgo Collaboration: 2016, GW150914: Implications
for the Stochastic Gravitational-Wave Background from Binary Black
Holes, Phys. Rev. Lett., 116, 131102.
Abbott, B. P., et al. including Flaminio, R., LIGO ScientificCollaboration, Virgo Collaboration: 2016, GW150914: The Advanced
LIGO Detectors in the Era of First Discoveries, Phys. Rev. Lett., 116,
131103.
Akiyama, E., et al. including Kusakabe, N., Kataoka, A., Hashimoto,J., Kwon, J., Kudo, T., Kandori, R., Currie, T., Ohashi, N., Egner,
S., Guyon, O., Hayano, Y., Hayashi, M., Hayashi, S., Ishi, M., Iye,
M., Miyama, S., Morino, J.-I., Nishimura, T., Pyo, T.-S., Suenaga,T., Suto, H., Suzuki, R., Takahashi, Y. H., Takato, N., Terada, H.,
Tomono, D., Takami, H., Usuda, T., Tamura, M.: 2015, Discovery
of a Disk Gap Candidate at 20 AU in TW Hydrae, ApJ, 802, L17.
Akiyama, E., Hasegawa, Y., Hayashi, M., Iguchi, S.: 2016, Planetary
System Formation in the Protoplanetary Disk around HL Tauri, ApJ,
818, 158.
Akiyama, K., et al. including Hada, K., Nagai, H., Honma, M.: 2015,
230 GHz VLBI Observations of M87: Event-horizon-scale Structureduring an Enhanced Very-high-energy γ-Ray State in 2012, ApJ, 807,
150.
Akiyama, M., et al. including Furusawa, H., Takata, T., Takato, N.,
Sekiguchi, K.: 2015, The Subaru-XMM-Newton Deep Survey(SXDS). VIII. Multi-wavelength identification, optical/NIR
spectroscopic properties, and photometric redshifts of X-ray sources,
PASJ, 67, 82.
ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi,
K., Espada, D., Kameno, S., Nagai, H., Sawada, T., Takahashi,S., Tatematsu, K., Kurono, Y., Iguchi, S., Hasegawa, T., Saito, M.,
Inatani, J., Mizuno, N., Asayama, S., Kosugi, G., Morita, K.-I.,
Chiba, K., Kawashima, S., Ohashi, N., Ogasawara, R., Sakamoto,S., Noguchi, T., Chikada, Y., Hiramatsu, M., Iono, D., Shimojo,
M., Komugi, S., Muller, E., Herrera, C., Miura, R. E., Ueda, J.,
Chibueze, J., Kiuchi, H., Ukita, N., Sugimoto, M., Kawabe, R.,
Hayashi, M., Kaifu, N., Ishiguro, M.: 2015, The 2014 ALMA Long
Baseline Campaign: An Overview, ApJ, 808, L1.
ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi,
K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Akiyama,E., Kawamura, A., Nguyen Luong, Q., Sanhueza, P., Kurono, Y.:
2015, The 2014 ALMA Long Baseline Campaign: First Results fromHigh Angular Resolution Observations toward the HL Tau Region,
ApJ, 808, L3.
ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi,
K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Ao, Y.,
Hatsukade, B., Matsuda, Y., Iono, D., Kurono, Y.: 2015, The 2014
ALMA Long Baseline Campaign: Observations of the Strongly
Lensed Submillimeter Galaxy HATLAS J090311.6+003906 at z =3.042, ApJ, 808, L4.
ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi,
K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Kurono,Y., Tatematsu, K.: 2015, The 2014 ALMA Long Baseline Campaign:
Observations of Asteroid 3 Juno at 60 Kilometer Resolution, ApJ,
808, L2.
Alonso-Herrero, A., et al. including Imanishi, M.: 2016, A mid-infrared
spectroscopic atlas of local active galactic nuclei on sub-arcsecond
resolution using GTC/CanariCam, MNRAS, 455, 563-583.
Ando, R., Kohno, K., Tamura, Y., Izumi, T., Umehata, H., Nagai, H.:
2016, New detections of Galactic molecular absorption systems
toward ALMA calibrator sources, PASJ, 68, 6.
Antolin, P., Okamoto, T. J., De Pontieu, B., Uitenbroek, H., Van
Doorsselaere, T., Yokoyama, T.: 2015, Resonant Absorptionof Transverse Oscillations and Associated Heating in a Solar
Prominence. II. Numerical Aspects, ApJ, 809, 72.
Antolin, P., Vissers, G., Pereira, T. M. D., van der Voort, L. R., Scullion,
E.: 2015, The Multithermal and Multi-stranded Nature of CoronalRain, ApJ, 806, 81.
Ao, Y., Matsuda, Y., Beelen, A., Henkel, C., Cen, R., De Breuck, C.,
Francis, P. J., Kovács, A., Lagache, G., Lehnert, M., Mao, M. Y.,
Menten, K. M., Norris, R. P., Omont, A., Tatemastu, K., Weiß, A.,
Zheng, Z.: 2015, What powers Lyα blobs?, A&A, 581, A132.
Aoki, W.: 2015, Molecular Line Formation in the Extremely Metal-poor
Star BD+44 493, ApJ, 811, 64.
Arai, T., Matsuura, S., Bock, J., Cooray, A., Kim, M.-G., Lanz, A., Lee,
D.-H., Smidt, J., Matsumoto, T., Nakagawa, T., Onishi, Y., Korngut,P., Shirahata, M., Tsumura, K., Xemcov, M.: 2015, Measurements of
the Mean Diffuse Galactic Light Spectrum in the 0.95 μm to 1.65 μm
Band from CIBER, ApJ, 806, 69.
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M. W., Leviton, D. B., Miller, K. H., Quijada, M. A., Guyon, O.,
Jovanovic, N., Takato, N., Hayashi, M.: 2015, The CHARIS IFS
for high contrast imaging at Subaru, Proc. SPIE 9605, Ed. S. Shaklan,
96051C.
Gusev, A., Hanada, H., Petrova, N., Ping, J.: 2015, Physical librations
and free nutations of the three-layer Moon for ChangE-3/4, LunaGlob-Resource, SELENE-2 missions, SPACEKAZAN- IAPS-2015,
153-155.
Gusev, A., Hanada, H., Petrova, N.: 2015, Physical librations and theinternal structure of a multilayer resonant moons in the Solar System,
SPACEKAZAN- IAPS-2015, 73-85.
Hagiwara, Y., Horiuchi, S., Doi, A., Miyoshi, M.: 2015, Extragalactic
Sub-millimeter H2O Maser - Detection of a 321 GHz Water Maser inCircinus Galaxy, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 131-132.
Hanada, H., Tsuruta, S., Asari, K., Araki, H., Noda, H., Kashima, S.,
Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Sasaki,
H., Shinke, S., Petrova, N., Gusev, A.: 2015, Ground experimentsof a small telescope like PZT for observations on the Moon,
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Hanaoka, Y., Sakurai, T., IRMag Group: 2015, Solar Full-Disk
Polarization Measurement with the Fe I 15648 Angstrom Line,
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Hatsukade, B., Ohta, K., Endo, A., Nakanishi, K., Tamura, Y.,
Hashimoto, T., Kohno, K.: 2015, Gamma-ray Bursts from Dusty
Regions with Little Molecular Gas, ASP Conf. Ser., 499, Eds. D.
Iono, K. Tatematsu, A. Wootten, L. Testi, 47-50.
Hayatsu, N., Yoshida, N., Matsuda, Y., Shimizu, I.: 2015, Detectability
and Statistical Properties of the [C II ] Emitter in CosmologicalHydrodynamic Simulations, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 79-80.
Hełminiak, K. G., Konacki, M., Ratajczak, M., Jordán, A., Espinoza, N.,
Brahm, R., Kambe, E., Ukita, N.: 2015, Multiples Among Detached
Eclipsing Binaries from the ASAS Catalog, ASP Conf. Ser., 496, Eds.
S. M. Rucinski, T. Guillermo, Z. Miloslav, 76-81.
Hidaka, J., Mathews, G. J., Kajino, T., Suzuki, J.: 2015, Equationof State of Proto-Neutron Star and Failed Supernova Neutrino,
JPS Conf. Proc. 6 (Int. Conf. on Advances in Radioactive Isotope
Science), Eds. T. Otsuka, H. Enyo, et al., 30137.
Hirai, Y., Ishimaru, Y., Saitoh, T. R., Fujii, M. S., Hidaka, J., Kajino,
T.: 2016, Astrophysical site(s) of r-process elements in galactic
chemodynamical evolution model, EPJ Web of Conf., 109, Eds. W.-P.
Liu, Z.-H. Li, Y.-B. Wang, B. Guo, Y.-P. Shen, 02001.
Hirota, T., Kim, M. K., Kurono, Y., Honma, M.: 2015, Detection ofa Hot Molecular Disk Around a Massive Protostar Candidate Orion
KL Source I, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 225-228.
Ide, H., Kinugasa, K., Nishioka, M., Mikoshiba, H., Miyazawa, K.,
Shinohara, N., Saito, M., Naito, S., Suzuki, Y., Ohnishi, K.: 2016,
Artist in Residence in Nobeyama Radio Observatory, Proc. of the“Astronomy museums and related activities”, Eds. K. Usuda-Sato, S.
Nemoto, H. Agata, 146-153.
Jenniskens, P., Borovicka, J., Watanabe, J., Consolmagno, G., Jopek,
T., Vaubaillon, J., Abe, S., Janches, D., Ryabova, G., Ishiguro, M.,
Zhu, J.: 2015, Division III: Commission 22: Meteors, Meteorites andInterplanetary Dust, Transactions IAU, Vol. 10, Issue T28, 120-123.
Jike, T., Tamura, Y., Shizugami, M.: 2015, VERA 2014 Geodetic
Activities, IVS 2014 Annual Report, Eds. K. D. Baver, D. Behrend, K.
L. Armstrong, 87-89.
Jung, T., Dodson, R., Han, S. T., Rioja, M. J., Byun, D. Y., Honma, M.,
Stevens, J., de Vicente, P., Sohn, B. W.: 2015, Measureing the Core
Shift Effect in AGN Jets with the Extended Korean VLBI Network, J.
Korean Astron. Soc., 48, 277-284.
Kameya, O., Funayama, H.: 2016, Kimura Hisashi Memorial Museumin NAOJ Mizusawa Campus, Proc. of the “Astronomy museums andrelated activities”, Eds. K. Usuda-Sato, S. Nemoto, H. Agata, 154157.
Kameya, O., Funayama, H.: 2016, Collaboration of Kimura Hisashi
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Kameya, O., Tsuboi, M., Asaki, Y., Yonekura, Y., Miyamoto, Y., Kaneko,
H., Seta, M., Nakai, N., Miyoshi, M., Takaba, H., Wakamatsu, K.,
Fukuzaki, Y., Morimitsu, T., Sekido, M.: 2015, 22 GHz Monitoring of
SGR A* During the G2 Peri-center Passing with the Japanese VLBI
Network, Publ. Korean Astron. Soc., 30, 649-650.
Kataoka, A., Muto, T., Momose, M., Tsukagoshi, T., Fukagawa, M.,
Shibai, H., Hanawa, T., Murakawa, K.: 2015, Expected Polarization

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Kato, Y., Matsuda, Y., Smail, I., Swinbank, M., Alexander, D., Geach, J.,
Lehmer, B., Tamura, Y., Umehata, H., Kohno, K., Kubo, M., Yamada,T., Hayashino, T., Erb, D., Steidel, C.: 2015, Protocluster Survey at z
= 2.23: from Herschel to ALMA, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 25-26.
Kinugasa, K., Nishioka, M., Mikoshiba, H., Miyazawa, K.,
Shinohara, N., Ide, H., Saito, M.: 2016, The Record 3 Million
Visitors and the NINS PR Center in the NAOJ Nobeyama Campus,
Proc. of the “Astronomy museums and related activities”, Eds. K.
Usuda-Sato, S. Nemoto, H. Agata, 65-70.
Kitazato, K., Iwata, T., Abe, M., Ohtake, M., Tsumura, K., Ishikawa, T.,
Takato, N., Nakauchi, Y., Arai, T., Senshu, H., Hirata, N., Takagi, Y.,
Hayabusa2 NIRS3 Team: 2016, Near-Infrared Spectroscopy of the
Earth and Moon During the Hayabusa2 Earth Swing-By, 47th Lunarand Planetary Sci. Conf., 2158.
Kojima, H., Antia, H. M., Dugad, S. R., Gupta, S. K., Hayashi, Y.,
Jagadeesan, P., Jain, A., Kawakami, S., Mohanty, P. K., Nonaka, T.,
Oshima, A., Rao, B. S., Shibata, S., The GRAPES-3 Collaboration:
2015, Rigidity dependence of the intensity variations of galactic
cosmic rays, 34th Int. Cosmic Ray Conf., 163.
Kojima, H., Antia, H.M., Dugad, S. R., Gupta, S.K., Hayashi, Y.,
Jagadeesan, P., Jain, A., Kawakami, S., Mohanty, P. K., Nonaka, T.,
Oshima, A., Rao, B. S., Shibata, S., The GRAPES-3 Collaboration:
2015, An estimation of the diffusion coefficient of galactic cosmic raysin the heliosphere near the Earth, 34th Int. Cosmic Ray Conf., 160.
Komatsubara, T., Yuasa, T., Onishi, T., Saito, Y., Okada, S., Sasa, K.,
Ozawa, A., Hayakawa, T., Shizuma, T., Kajino, T., Kubono, S.: 2015,
Study for Big Bang Nucleosynthesis Concerning Lithium Isotopes,
JPS Conf. Proc. 6 (Int. Conf. on Advances in Radioactive Isotope
Science), Eds. T. Otsuka, H. Enyo, et al., 13055.
Kuncarayakti, H., Aldering, G., Anderson, J. P., Arimoto, N., Doi,
M., Galbany, L., Hamuy, M., Hashiba, Y., Kruehler, T., Maeda, K.,
Morokuma, T., Usuda, T.: 2015, Constraining Supernova Progenitors:
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Kurahashi, T., Iono, D., Hatsukade, B., Matsuda, Y., Ueda, J., Saito,T., Kato, Y., Michiyama, T., High-z Legacy Team: 2015, Nobeyama
Molecular Gas Observations of Distant Bright Galaxies, ASP Conf.
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Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB
150818A: MITSuME Ishigakijima upper limits, GRB Coordinates
Network, Circular Service, 18174, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB
150910A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 18276, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB
150910A: MITSuME Ishigakijima Optical Observation after 1 day,
GRB Coordinates Network, Circular Service, 18288, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB

150910A: MITSuME Ishigakijima Optical Observation after 2 days,
GRB Coordinates Network, Circular Service, 18301, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB
150912A: MITSuME Ishigakijima upper limits, GRB Coordinates
Network, Circular Service, 18304, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB
151029A: MITSuME Ishigakijima upper limits, GRB Coordinates
Network, Circular Service, 18534, 1 .
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB
151029A: MITSuME Ishigakijima upper limits, GRB Coordinates
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Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB
160131A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 18968, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB
160131A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 18968, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150423A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
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Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150527A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
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Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150910A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 18267, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150911A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
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Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 151006A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
18402, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 151021A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
18431, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 151022A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
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Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 151031A, GRB
Coordinates Network, Circular Service, 18547, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
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18761, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB 160104A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
18825, 1.
Kuzuhara, M., Tamura, M., Hełminiak, K. G., Mede, K., Brandt,
T., Janson, M., Kandori, R., Kudo, T., Kusakabe, N., Hashimoto,J.: 2015, The SEEDS High-Contrast Imaging Survey: Exoplanet
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Lee, M., Suzuki, K., Kohno, K., Tamura, Y., Iono, D., Hatsukade, B.,
Nakanishi, K., Tanaka, I., Kodama, T., Tadaki, K., Ikarashi, S., Ueda,
J., Umehata, H., Saito, T., Kawabe, R.: 2015, Dusty, Intensively Star
Forming Hα Emitters (HAEs) in Protocluster 4C23.56, ASP Conf. Ser.,499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 27-28.
Lee, M., Suzuki, K., Kohno, K., Tamura, Y., Iono, D., Hatsukade, B.,
Nakanishi, K., Tanaka, I., Kodama, T., Tadaki, K., Ikarashi, S.,
Ueda, J., Umehata, H., Saito, T., Kawabe, R.: 2015, Deep JVLA and
ALMA observations of dusty star forming galaxies in protocluster
4C23.56 at z = 2.5, IAU General Assembly, Meeting #29, 2254344.
Lee, S. S., Oh, C. S., Roh, D. G., Oh, S. J., Kim, J., Yeom, J. H., Kim,
H. R., Jung, D. G., Byun, D. Y., Jung, T., Kawaguchi, N., Shibata,K. M., Wajima, K.: 2015, A New Hardware Correlator in Korea:
Performance Evaluation Using KVN Observations, J. Korean Astron.
Soc., 48, 125-137.
Lin, S.-J., Shimajiri, Y., Hara, C., Lai, S.-P., Nakamura, F., Sugitani,K., Kawabe, R., Kitamura, Y., Yoshida, A., Tatei, H., Akashi, T.,
Tsukagoshi, T.: 2015, Influence of Interstellar FUV Radiation on the
Abundance Ratio of 13CO to C18O in L 1551, IAU General Assembly,
Meeting #29, 2256988.
Liu, H. B., Takami, M., Kudo, T., Hashimoto, J., Dong, R., Vorobyov, E.
I., Pyo, T.-S., Fukagawa, M., Tamura, M., Henning, T., Dunham, M.
M., Karr, J. L., Kusakabe, N., Tsuribe, T.: 2016, Circumstellar disksof the most vigorously accreting young stars, Sci. Adv., 2, e1500875.
Liuzzo, E., Nagai, H., Giovannini, G., Mignano, A.: 2015, The Jet of the
BL Lac Object PKS 0521-365 in the mm-Band: ALMA Observations,
ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L.
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Maehara, H., Ayani, K., Itoh, R., Takata, K., Kawabata, K. S.: 2015,
Spectroscopic identification of ASASSN-15qi as an FU Ori-likeobject, The Astronomer’s Telegram, 8147.
Maehara, H., Fujii, M., Arai, A.: 2015, Spectroscopic identification of
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The Astronomer’s Telegram, 8127.
Maehara, H.: 2016, Pre-discovery observations of MASTER OT
J004514.13+420007.2, The Astronomer’s Telegram, 8606.
Maruyama, T., Cheoun, M.-K., Kajino, T., Mathews, G. J.: 2015,
Pion Production from Proton Synchrotron Radiation under Strong
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Maruyama, T., Hidaka, J., Kajino, T., Yasutake, N., Kuroda, T., Cheoun,
M.-K., Ryu, C.-Y., Mathews, G. J.: 2015, Asymmetric Neutrino
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Kuroda, T., Cheoun, M.-K., Ryu, C.-Y., Mathews, G. J.: 2015,
Nuclear Equation of State and Asymmetric Neutrino Emission fromProto-Neutron Stars, JPS Conf. Proc. 6 (Int. Conf. on Advances inRadioactive Isotope Science), Eds. T. Otsuka, H. Enyo, et al., 30061.
Matsuda, Y., APDS Team: 2015, The ALMA Patchy Deep Survey: A
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Iono, K. Tatematsu, A. Wootten, L. Testi, 77-78.
Matsumoto, K., Yamada, R., Kikuchi, F., Kamata, S., Ishihara, Y.,
Iwata, T., Hanada, H., Sasaki, S.: 2015, Internal Structure of theMoon Inferred from Apollo Seismic Data and Selenodetic Data fromGRAIL and LLR, SPACEKAZAN- IAPS-2015, 86-88.
Mendillo, C. B., Brown, J., Martel, J., Howe, G. A., Hewasawam, K.,
Finn, S. C., Cook, T. A., Chakrabarti, S., Douglas, E. S., Mawet,D., Guyon, O., Singh, G., Lozi, J., Cahoy, K. L., Marinan, A. D.:
2015, The low-order wavefront sensor for the PICTURE-C mission,
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Meyer, J. D., Mason, B., Impellizzeri, V., Kameno, S., Fomalont, E.,
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Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 361-362.
Michiyama, T., Iono, D., Ueda, J., Saito, T.: 2015, CO(3–2)/CO(1–0)
Ratio of Molecular Gas Outflow in NGC 3256, ASP Conf. Ser., 499,
Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 139-140.
Momose, M., Muto, T., Hanawa, T., Fukagawa, M., Tsukagoshi, T.,
Saigo, K., Kataoka, A., Nomura, H., Takeuchi, T., Akiyama, E.,
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Kobayashi, H., Honda, M., Aso, Y., Takahashi, S. Z.: 2015, Gas andDust Structures of the Protoplanetary Disk around HD 142527, ASP
Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi,
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Morokuma-Matsui, K., Baba, J., Sorai, K., Kuno, N.: 2015, CO
Emissions from Optically Selected Galaxies at z ~ 0.1–0.2: Tight
Anti-Correlation Between Molecular Gas Fraction and 4000
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Tatematsu, A. Wootten, L. Testi, 157-158.
Muller, E., Kempen, T., Mizuno, N., Kawamura, A., Minamidani, T.:2015, Candidate Filament Collision in the SMC; Energy Distribution
within the SFR N66/NGC346, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 251-252.
Nagai, H., Nakanishi, K., Paladino, R., Moellenbrock, G., Fomalont, E.,
Amigano, A., Vahakis, C., Remijan, A., ALMA Polarization Team:
2015, ALMA Polarization Science Verification: 3C 286, ASP Conf.
Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 357-358.
Nakajima, T., Takano, S., Kohno, K., Harada, N., Herbest, E., Tamura, Y.,
Izumi, T., Taniguchi, A., Tosaki, T.: 2015, High-Resolution Imaging
in 3-mm and 0.8-mm Bands and Abundances of Shock/Dust Related
Molecular Toward the Seyfert Galaxy NGC 1068 Observed with
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L. Testi, 109-110.
Nakamura, F., et al. including Kawabe, R., Nishitani, H., Kameno, S.,
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by Filament Collisions in Serpens South, ASP Conf. Ser., 499, Eds. D.
Iono, K. Tatematsu, A. Wootten, L. Testi, 239-240.
Nakanishi, K., Nagai, H., Fomalont, E., Cortes, P., Remijan, A.,
Vlahakis, C., Corder, S., Moellenbrock, G., Tang, Y.-W., Hills, R.,

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Nakanishi, K., Sorai, K., Nakai, N., Kuno, N., Matsubayashi, K.,
Sugai, H., Takano, S., Kohno, K., Nakajima, T.: 2015, Ionizes Gas
Observation Toward a Nearby Starburst Galaxy NGC 253, ASP Conf.
Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 117-120.
Nakano, S., Itagaki, K., Kazarovets, E., Samus, N., Shappee, B. J.,
Maehara, H., Kojima, T., Hirosawa, K., Noguchi, T., Fujii, M.: 2015,
V1831 Aql = N Aql 2015 = PNV J19215012+1509248, IAU Circ.
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Nakano, S., Itagaki, K., Shappee, B. J., Maehara, H., Kojima, T.,
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Narita, N., Onitsuka, M., Fukui, A., PEaCH Team.: 2015, Long-termtransit observations for a hot Jupiter around a T-Tauri star, IAU
General Assembly, Meeting #29, 2254942.
Narukage, N., Kubo, M., Ishikawa, R., Katsukawa, Y., Ishikawa,
S., Kobiki, T., Giono, G., Kano R., Bando, T., Tsuneta, S.: 2015,
Evaluation of the VUV Coating Performed on the Flight Mirrors of
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Nemoto, S., Usuda-Sato, K., Matsuda, K., Sasaki, G., Nakagiri, M.,
Agata, H., Funayama, H., Kameya, O., Kinugasa, K., Toda, H.,
Yanagisawa, K., Baba, Y.: 2016, Historical Intems Database of
the NAOJ Museum, Proc. of the “Astronomy museums and related
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Nishimura, A., Umemoto, T., Minamidani, T., Kuno, N., Tosaki, T.,
Fujita, S., Matsuo, M., Tsuda, Y., Ohashi, S.: 2015, Nobeyama 45m
CO Galactic Plane Survey: Filament Properties and Star Formation in
M17, IAU General Assembly, Meeting #29, 2247474.
Nishimura, Y., Shimonishi, T., Watanabe, Y., Sakai, N., Aikawa, Y.,
Kawamura, A., Yamamoto, S.: 2015, Spectral Line Survey Toward
Quiescent Giant Molecular Clouds in the Large Magellanic Cloud,
ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L.
Testi, 165-166.
Nishioka, M., Kinugasa, K., Mikoshiba, H., Miyazawa, K., Shinohara,N., Ide, H., Saito, M.: 2016, Making Brochure and Original Goodsin the NAOJ Nobeyama Campus, Proc. of the “Astronomy museums
and related activities”, Eds. K. Usuda-Sato, S. Nemoto, H. Agata,140-145.
Nishiyama, K., Kabashima, F., Kojima, T., Nakano S., Fujikawa, S.,
Soma, M., Masi, G., O'Connor, S., Waagen, E.O., Kiyota, S., Yusa,
T., Ayani, K., Fujii, M.: 2015, V2949 OPHIUCHI = NOVA OPH
2015 No. 2 = TCP J17344775-2409042, Central Bureau Electronic
Telegrams, Ed. D.W.E. Green, 4150.
Oh, H., Pyo, T.-S., Yuk, I.-S., Park, B.-G.: 2015, Long-Slit Spectroscopyof Parsec-Scale Jets from DG Tauri, J. Korean Astron. Soc., 48, 113-123.
Ohashi, S., Tatematsu, K., Choi, M., Kang, M., Umemoto, T., Lee, J.-E.,
Hirota, T., Yamamoto, S., Mizuno, N.: 2015, The Chemical Variationin the Orion A Cloud Cores, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 191-192.
Oka, T., Mizuno, R., Miura, K., Takekawa, S., Tanaka, K.: 2015,
Spectral Line Survey and Mapping Observations toward the HVCC
CO–0.40–0.22, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 175-176.

Onishi, K., Iguchi, S., Sheth, K., Kohno, K.: 2015, Measurement of theBlack-Hole Mass in NGC 1097 using ALMA, ASP Conf. Ser., 499,
Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 161-162.
Onishi, T., Nishimura, A., Tokuda, K., Harada, R., Dobashi, K.,
Shimoikura, T., Kitamura, Y., Ogawa, H.: 2015, Large-Scale
Molecular Gas Survey in 12CO, 13CO and C18O (J=2–1) with the
Osaka 1.85 m mm-submm Telescope, IAU General Assembly,
Meeting #29, 2252707.
Onishi, T., Tokuda, K., Saigo, K., Kawamura, A., Fukui, Y., Matsumoto,T., Inutsuka, S.-i., Machida, M., Tomida, K., Tachihara, K.: 2015,
ALMA Observations of a High-density Core in Taurus: Dynamical
Gas Interaction at the Possible Site of a Multiple Star Formation, ASP
Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi,
211-214.
Pyo, T.-S., Hayashi, M., Beck, T., Davis, C. J., Takami, M.: 2015,
Unveiling Complex Outflow Structure of UY Aur, Publ. Korean
Astron. Soc., 30, 109-112.
Ratajczak, M., Hełminiak, K. G., Konacki, M.: 2015, Studies of Long
Period Eclipsing Binaries, ASP Conf. Ser., 496, Eds. S. M. Rucinski, T.
Guillermo, Z. Miloslav, 311.
Saito, M., de Gregorio, I., Team SOLA: 2015, The Soul of Lupus with
ALMA (SOLA) Project Overview, ASP Conf. Ser., 499, Eds. D. Iono,
K. Tatematsu, A. Wootten, L. Testi, 215-216.
Saito, T., Iono, D., Ueda, J., Nakanishi, K., Imanishi, M., Hagiwara,
Y., Yun, M. S., Kaneko, H., Komugi, S., Espada, D., Sugai, H.,
Motohara, K., Lee, M., Kawabe, R., Yamashita, T.: 2015, Molecular
Gas Excitation and Chemistry in Nearby LIRGs with ALMA, IAU
General Assembly, Meeting #29, 2254284.
Saito, T., Iono, D., Ueda, J., Yun, M. S., Nakanishi, K., Imanishi, M.,
Hagiwara, Y., Kaneko, H., Komugi, S., Espada, D., Motohara, K.,
Sugai, H., Yamashita, T., Tateuchi, K., Lee, M., Michiyama, T.,
Kawabe, R.: 2015, Diffuse and Dense Gas in Nearby Luminous
Merging Galaxies, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 133-135.
Sakao, T., Matsuyama, S., Kime, A., Goto, T., Nishihara, A., Nakamori,H., Yamauchi, K., Kohmura, Y., Miyake, A., Hashizume, H.,
Maezawa, T., Suematsu, Y., Narukage, N.: 2015, Development ofprecision Wolter mirrors for future solar x-ray observations, Proc.
SPIE 9603, Eds. S. L. O’Dell, G. Pareschi, 96030U.
Sanhueza, P., Jackson, J. M., Zhang, Q., Foster, J., Guzmán, A.: 2015, A
Massive, Prestellar Clump Hosting no High-Mass Cores, ASP Conf.
Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 245-246.
Sano, H., Fukui, Y., Yoshiike, S., Fukuda, T., Tachihara, K., Inutsuka, S.,
Kawamura, A., Fujii, K., Mizuno, N., Inoue, T., Onishi, T., Acero,F., Vink, J.: 2015, Revealing the Large-Scale Structures of Interstellar
Gas Associated with the Magellanic SNR N132D, ASP Conf. Ser.,499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 257-260.
Sawada, T., Hasegawa, T., Koda, J.: 2015, ALMA Reveals Internal
Structure of Molecular Clouds in the LMC, ASP Conf. Ser., 499, Eds.
D. Iono, K. Tatematsu, A. Wootten, L. Testi, 253-254.
Sawada-Satoh, S., Akiyama, K., Niinuma, K., Nagai, H., Kino, M.,
D’Ammando, F., Koyama, S., Hada, K., Orienti, M., Honma, M.,
Shibata, K. M.: 2015, Apparent Inward Motion of the Parsec-Scale
Jet in the BL Lac Object OJ287 during the 2011-2012 γ-ray Flares,
Publ. Korean Astron. Soc., 30, 429-432.
Sekiguchi, K., Yoshida, F.: 2015, NAOJ’s activities on Astronomy for

Development : Aiding Astronomy Education in Developing Nations.
in Highlights of Astronomy, XXVIIIth General Assembly - Highlights
of Astronomy 16, Eds. T. Montmerle, 553.
Sekimoto, Y., Dominjon, A., Noguchi, T., Okada, N., Mitsui, K., Obuchi,
Y., Sekine, M., Sekiguchi, S., Shu, S., Nitta, T., Naruse, M.: 2015,
Design of MKID focal plane array for LiteBIRD, Proceedings of ESA
antenna conference, Eds. E. Saenz, K. Klooster, B. Shortt, L. Duvet.
Seko, A., Ohta, K., Hatsukade, B., Yabe, K.: 2015, Properties of
Molecular Gas in Star-Forming Galaxies at z ~ 1.4 with ALMA, ASP
Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 43-46.
Shibagaki, S., Kajino, T., Mathews, G. J., Chiba, S.: 2015, Impact of
the nuclear fission on r-process nucleosynthesis and the origin ofsolar r-process elements, AIP Conf. Proc. 1645 (Carpathian Summer
School of Physics 2014), Eds. C. Spitaleri, et al., 402-405.
Shibagaki, S., Kajino, T., Mathews, G. J., Chiba, S.: 2015, R-Process
in Neutron Star Merger with a New Fission Model, JPS Conf. Proc.
6 (Int. Conf. on Advances in Radioactive Isotope Science), Eds. T.
Otsuka, H. Enyo, et al., 20030.
Shimakawa, R., Kodama, T., Hayashi, M., Tadaki, K., Suzuki, T. L.,
Koyama, Y., Tanaka, I., Yamamoto, M.: 2015, Toward unveilinginternal properties of HII regions and their connections at the cosmic
noon era, IAU General Assembly, Meeting #29, 2235631.
Shimizu, E., Ali, S., Sakaue, H. A., Kato, D., Murakami, I., Hara, H.,
Watanabe, T., Nakamura, N.: 2015, Intensity ratio in EUV spectraof highly charged Fe ions: Experimental evaluation of astrophysicalplasma model, J. Phys.: Conf. Ser., 635, 052061.
Shinnaga, H., Humphreys, E., Indebetouw, R., Villard, E., Kern, J.,
Davis, L., Miura, R. E., Nakazato, T., Sugimoto, K., Kosugi, G.,
Akiyama, E., Muders, D., Wyrowski, F., Williams, S., Lightfoot,J., Kent, B., Momjian, E., Hunter, T., ALMA Pipeline Team: 2015,
ALMA Pipeline: Current Status, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 355-356.
Shinohara, I., Fujimoto, M., Nagai, T., Zenitani, S., Kojima H.: 2016,
Low-frequency Waves in the Tail Reconnection Region, AGU
Geophysical Monograph 216, Eds. A. Keiling, D.-H. Lee, V.
Nakariakov, 181-191,
Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto, Y.: 2015, Propertiesof galaxies around the most massive SMBHs, IAU General Assembly,
Meeting #29, 2252576.
Sirbu, D., Thomas, S. J., Belikov, R., Lozi, J., Bendek, E., Pluzhnik,
E., Lynch, D. H., Hix, T., Zell, P., Schneider, G., Guyon, O.:
2015, EXCEDE technology development IV: demonstration ofpolychromatic contrast in vacuum at 1.2 λ/D, Proc. SPIE 9605, Ed. S.
Shaklan, 96050J.
Sliwa, K., Wilson, C. D., Iono, D., Peck, A. B., Matsushita, S.: 2015,
Around the Ring We Go: The Cold, Dense Ring of Molecular Gas
in NGC 1614, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 141-142.
Soam, A., Kwon, J., Maheswar, G., Tamura, M., Lee, C. W.: 2015,
Optical and NIR Polarimetry of a Core L328 with Proto-Brown
Dwarf, Revolution in Astronomy with ALMA: The Third Year. Proc.
a Conf., Eds. D. Iono, K.-I. Tatematsu, A. Wootten, L. Testi, 293.
Soma, M., Tanikawa K.: 2015, Reliability of Eclipse Records in Japanese
Ancient Periods, Intensive Workshop on Ancient and Medieval
Eclipse Data: Compilation of Eclipse Data and Examination of their
Reliability, Eds. M. Soma, K. Tanikawa, 49-52.

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Soma, M., Tanikawa, K.: 2015, Determination of ΔT and Lunar Tidal
Acceleration from Ancient Eclipses and Occultations, New Insights
From Recent Studies in Historical Astronomy: Following in theFootsteps of F. Richard Stephenson, Eds. W. Orchiston, D. Green, R.
Strom, 11-23.
Soma, M.: 2015, Observations of the Annular Eclipse on 2012 May
21 by the General Public in Japan, APRIM 2014: Proc. 12th AsianPacific Regional IAU Meeting, Eds. Y. C. Minh H. Kim, 753-755.
Soma, M.: 2015, Observations of the Annular Eclipse on 2012 may 21
BY the General Public in Japan, Publ. Korean Astron. Soc., 30, 753.
Stoehr, F., Grothkopf, U., Meakins, S., Bishop, M., Uchida, A., Testi,
L., Iono, D., Tatematsu, K., Wootten, A.: 2015, ALMA Cycle 0
Publication Statistics, The Messenger, 162, 30-35.
Sugai, H., et al. including Takato, N., Ueda, A.: 2015, Prime Focus
Spectrograph for the Subaru telescope: massively multiplexed opticaland near-infrared fiber spectrograph, J. Astron. Telescopes Systems, 1,035001.
Sugiyama, K., Fujisawa, K., Hachisuka, K., Yonekura, Y., Motogi, K.,
Sawada-Satoh, S., Matsumoto, N., Saito, Y., Hirano, D., Hayashi, K.,
Shen, Z. Q., Honma, M., Hirota, T., Murata, Y., Doi, A., Niinuma, K.,
Dodson, R., Rioja, M., Ellingsen, S., Chen, X., Kim, K. T., Ogawa, H.:
2015, The VLBI Monitoring Project for 6.7 GHz Methanol Masers
Using the JVN/EAVN, Publ. Korean Astron. Soc., 30, 645-647.
Sugiyama, K., Yonekura, Y., Motogi, K., Saito, Y., Fujisawa, K., Ishii, S.,
Momose, M., Honma, M., Tazaki, F., Tanaka, K. E. I., Hosokawa,T., Uchiyama, M., Inayoshi, K.: 2015, Flux Monitoring of 6.7 GHz
Methanol Maser to Systematically Research Periodic Variations
Using the Hitachi 32-m, Publ. Korean Astron. Soc., 30, 129-131.
Suzuki, T., Honma, M., Otsuka, T., Kajino, T.: 2015, Electron-Capture
Rates for Exotic Nuclei at Stellar Environments, JPS Conf. Proc.
6 (Int. Conf. on Advances in Radioactive Isotope Science), Eds. T.
Otsuka, H. Enyo, et al., 30029.
Suzuki, T., Kajino, T., Honma, M., Toki, H., Otsuka, T.: 2015, Rolesof Nuclear Weak Processes in Stars, Exotic Nuclei (IASEN-2013)- Proc. of the First Int. African Symp. on Exotic Nuclei, Eds. Y. E.
Penionzhkevich, et al., 129-139.
Suzuki, T., Yoshida, T., Wanajo, S., Kajino, T., Otsuka, T.: 2015, BetaDecay Rates for Exotic Nuclei and R-Process Nucleosynthesis,
JPS Conf. Proc. 6 (Int. Conf. on Advances in Radioactive Isotope
Science), Eds. T. Otsuka, H. Enyo, et al., 30063.
Takakuwa, S., Saito, M., Saigo, K., Matsumoto, T., Lim, J., Hanawa,
T., Ho, P. T. P.: 2015, Spiral Arms and Mass Accretion in the
Circumbinary Disk around the Protostellar Binary System L1551
NE Revealed with ALMA, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 287-288.
Takeda, T., Kato, T., Narazaki, Y., Nakayama, H., Fukushi, H.,
Agata, H., Kokubo, E.: 2016, Four-Dimensional Digital Universe
Project, Proc. of the “Astronomy museums and related activities”,
Eds. K. Usuda-Sato, S. Nemoto, H. Agata, 131-135.
Takekawa, S., Oka, T., Tanaka, K., Matsumura, S., Miura, K., Sakai, D.:2015, Millimeter-wave Spectral Line Surveys Toward the Galactic
Circumnuclear Disk and Sgr A*, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 173-174.
Takekawa, S., Oka, T., Tanaka, K.: 2015, Deep Mapping Observationsof the Galactic Circumnuclear Disk with Two Single-dish Telescopes,
ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L.

182

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Testi, 171-172.
Tamura, M.: 2016, SEEDS - Strategic explorations of exoplanets anddisks with the Subaru Telescope -, Proc. Japan Academy, Ser. B:
Physical and Biological Sciences, 92, 45-55.
Taniguchi, A., Kohno, K., Tamura, Y., Izumi, T., Takano, S., Nakajima, T.,
Tosaki, T.: 2015, Spatial Distribution of CO Isotopologue Abundance
Ratios in the Center of NGC 1068, ASP Conf. Ser., 499, Eds. D. Iono,
K. Tatematsu, A. Wootten, L. Testi, 107-108.
Tanikawa K., Soma, M.: 2015, Historical Astronomy and Eclipses,
Intensive Workshop on Ancient and Medieval Eclipse Data:
Compilation of Eclipse Data and Examination of their Reliability,
Eds. M. Soma, K. Tanikawa, 1-15.
Tatematsu, K., Hirota, T., Ohashi, S., Choi, M., Lee, J. E., Yamamoto,S., Umemoto, T., Kandori, R., Kang, M., Mizuno, N.: 2015, Thermal
Starless Ammonia Core Surrounded by CCS in the Orion A Cloud,
ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L.
Testi, 189-190.
Terazono, J., Sakamoto, S., Yoshikawa, M., Wakabayashi, N., Watanabe,J.: 2016, Japanese Lunar and Planetary Exploration Outreach — 17
Years’ History of “The Moon Station” —, Proc. of the “Astronomy
museums and related activities”, Eds. K. Usuda-Sato, S. Nemoto, H.
Agata, 161-167.
Tokuda, K., Osaki, S., Maezawa, H., Onishi, T., Saigo, K., Kawamura,A., Fukui, Y., Tachihara, K.: 2015, Extensive Surveys of Dense Coresin Taurus in High Density Molecular Tracers, ASP Conf. Ser., 499,
Eds. D. Iono, K. Tatematsu, A. Wootten, L. Testi, 193-194.
Ueda, J., Iono, D., Yun, M. S., Crocker, A. F., Narayanan, D., Komugi, S.,
Espada, D., Hatsukade, B., Kaneko, H., Matsuda, Y., Tamura, Y.,
Wilner, D., Kawabe, R., Pan, H.-A.: 2015, Investigating Nuclear andExtended Molecular Gas in the Final Stages of Mergers, IAU General
Assembly, Meeting #29, 2256394.
Umehata, H., Kohno, K., Tamura, Y., Iono, D., Nakanishi, K., Hatsukade,B., Ikarashi, S., Izumi, T., Matsuda, Y., Ivison, R., Yun, M., Wilson,
G., Hughes, D.: 2015, Dusty Starbursts within a z = 3 Large Scale
Structure, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 29-30.
Urata, Y., Huang, K., Takahashi, S.: 2015, Gamma-Ray Burst Afterglowswith ALMA, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 339-340.
Usuda-Sato, K., Museum Project Office Members: 2016, Introductionof the NAOJ Museum Plan, Proc. of the “Astronomy museums andrelated activities”, Eds. K. Usuda-Sato, S. Nemoto, H. Agata, 19-26.
Usuda-Sato, K., Tomita, A.: 2015, Astronomy for Development;
Approaches in Asia, APRIM 2014: Proc. 12th Asian-Pacific Regional
IAU Meeting, Eds. Y. C. Minh H. Kim, 731-733.
Uzawa, Y., Makise, K., Kojima, T., Saito, S., Kroug, M., Fujii, Y.,
Gonzalez, A., Kaneko, K., Terai, H., Wang, Z.: 2015, Characterizationof NbTiN Films for Superconducting Terahertz Circuitry, 15th
Int. Superconductive Electronics Conf. 2015 (ISEC2015), Eds.
N. Yoshikawa, Y. Hatsukade, A. Saito, T. Taino, Y. Yamanashi, T.
Yamashita, MF-P11.
Wedemeyer, S., Bastian, T., Braja, R., Barta, M., Shimojo, M., Hales,
A., Yagoubov, P., Hudson, H.: 2015, Solar ALMA Observations - A
New View of Our Host Star, ASP Conf. Ser., 499, Eds. D. Iono, K.
Tatematsu, A. Wootten, L. Testi, 345-346.
Wedemeyer, S., Bastian, T., Braja, R., Barta, M., Shimojo, M.: 2015,

Solar Simulations for the Atacama Large Millimeter Observatory
Network, ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A.
Wootten, L. Testi, 341-342.
Yamada, M., Yoo, J., Zenitani, S.: 2016, Energy conversion andinventory of a prototypical magnetic reconnection layer, Astrophysics
and Space Science Library, 427, Eds. W. Gonzalez, E. Parker, 143179.
Yamada, R., Shiraishi, H., Nebut, T., Lognonne P., Asari, K., Tanaka, S.:
2015, Seismic observation using the broadband seismometers targeted
for moonquake, 5th Int. Symp. on Technology for Sustainability(ISTS2015), K-20.
Yamaguchi, Y., Kohno, K., Tamura, Y., Matsuda, Y.: 2015, Constraints
on the CO Luminosity Function at z ~ 1 Using ALMA Archival Data,
ASP Conf. Ser., 499, Eds. D. Iono, K. Tatematsu, A. Wootten, L.
Testi, 61-62.
Yamaoka, H., Maehara, H., Kaneko, S., Noguchi, T., Kiyota, S.,
Yusa, T.: 2015, Probable New Dwarf Nova in Orion = TCP
J05002724+1334199, Central Bureau Electronic Telegrams, Ed.
D.W.E. Green, 4207.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida, M.,
Ohta, K., Kawai, N.: 2015, GRB 150910A: MITSuME Okayama
Ks-band Observation, GRB Coordinates Network, Circular Service,
18278, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida,M., Ohta, K., Kawai, N.: 2015, GRB150911A MITSuME Okayama
Ks-band upper-limit, GRB Coordinates Network, Circular Service,
18282, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida, M.,
Ohta, K., Kawai, N.: 2015, GRB 151006A: MITSuME Okayama
Ks-band upper-limit, GRB Coordinates Network, Circular Service,
18408, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida, M.,
Ohta, K., Kawai, N.: 2015, GRB 151021A: MITSuME Okayama
Ks-band upper-limit, GRB Coordinates Network, Circular Service,
18435, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida, M.,
Ohta, K., Kawai, N.: 2015, GRB 151022A: MITSuME Okayama
Ks-band upper-limit, GRB Coordinates Network, Circular Service,
18440, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Izumiura, H., Yoshida, M.,
Ohta, K., Kawai, N.: 2016, GRB 160104A: MITSuME Okayama
Ks-band upper-limit, GRB Coordinates Network, Circular Service,
18819, 1.
Yeh, S. C. C., Tsai, C.-W., Geballe, T. R., Herrera, C. N.: 2015,
Mid-infrared [NeII] Imaging of Young Massive Star Clusters Near
Galactic Nuclei, IAU General Assembly, Meeting #29, A. Nota, C.
Charbonnel, 2246331.
Yilmaz, M., Selam, S. O., Izumiura, H., Bikmaev, I., Sato, B., Keskin,V., Kambe, E.: 2015, RTT150 Planet Search Program at TUG:
Results from Seven Years of Observation, ASP Conf. Ser., 496, Eds. S.
M. Rucinski, T. Guillermo, Z. Miloslav, 378-379.
Yoshii, T., Kawai, N., Hanayama, H., Saito, Y., Yatsu, Y.: 2015, X-ray
and optical observations of a compact black hole binary MAXI
J1910-057: implication for the companion and evidence for the jetturn-on, IAU General Assembly, Meeting #29, 2257355.
Yoshikoshi, T., Clay, R. W., Matsubara, Y., Miyo, K., Mori, M., Naito,

T. Nishijima, K. Ohishi, M. Okuda, T., Oshima, A., Rowell, G. P.,
Saito, T., Sako, T., Tajima, H., Terasawa, T., Yamamoto, T.: 2015, A
3-Meter Atmospheric Cherenkov Telescope as a Test Bench for VeryHigh Energy Gamma-Ray Astrophysics Projects, 34th Int. Cosmic
Ray Conf., 1300.

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184

5. Publications in English

6. Conference Presentations

Canas, L., et al.: 2016, Inspired by Light: Reflections from theInternational Year of Light 2015, SPIE, EPS, ICTP, USA.
Edited by Usuda-Sato, K., Nemoto, S., Agata, H.: 2016, Astronomy
Museums and Related Activities: Proceedings of the International
Symposium on the NAOJ Museum, NAOJ, Tokyo.
Iono, D., Tatematsu, K., Wootten, A., Testi, L.: 2015, Proceedings ofthe International Conference “Revolution in Astronomy with ALMA:The Third Year”, ASP, San Francisco.
Soma, M., Tanikawa, K.: 2015, Proceedings of Intensive Workshop on
Ancient and Medieval Eclipse Data: Compilation of Eclipse Data andExamination of their Reliability, NAOJ, Tokyo.

Agata, H., Furusho, R.: 2015, Makalii and Subaru Telescope Images,
Global Hands-On Universe Conference 2015, (Honolulu, HI, USA,
Aug. 4-5, 2015).
Akiyama, E., et al. including Kusakabe. N., Tamura, M.: 2015,
Multiple gap structure of TW Hydrae, Protoplanetary Disk Dynamics
and Planet Formation, (Kanagawa, Japan, Sep. 29-Oct. 2, 2015).
Akiyama, E., Kusakabe. N., Muto, T., Kataoka, A., Tamura, M., SEEDS/HiCIAO/AO188 Team: 2015, Discovery of a disk gap candidate at 20
AU in TW Hydrae, Disc Dynamics & Planet Formation, (Lancashire,
UK, Jun. 29-Jul. 3, 2015).
Akiyama, E.: 2015, ALMA Capabilities and Science Review of HL Tau,
3rd DTA Symposium: The Origins of Planetary Systems: From theCurrent View to New Horizons, (Tokyo, Japan, Jun. 1-4, 2015).
Akiyama, E.: 2015, Planet Formation in the Protoplanetary Disk around
HL Tauri, East Asian ALMA Science Workshop 2015, (Osaka, Japan,
Dec. 8-11, 2015).
Akiyama, E.: , ALMA Single Dish Pipeline and ALMA Quality
Assurance (AQUA) System, NRO-ALMA Science/Development
Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Akiyama, K.: 2015, 230 GHz (1.3 mm) VLBI observations of M87
with the Event Horizon Telescope, 8th East Asia VLBI Workshop,(Sapporo, Japan, Jul. 8-10, 2015).
Akutsu, T., for the KAGRA collaboration: 2016, Status of KAGRA,
LSC-Virgo March 2016 meeting, (Pasadena, CA, USA, Mar. 14-18,
2016).
Ando, M.: 2015, The Physical Condition of the Gas in the Luminous
Galaxy NGC 1614, East Asian ALMA Science Workshop 2015,(Osaka, Japan, Dec. 8-11, 2015).
Anthes Rich, E., Wisniewski, J. P., Hashimoto, J., Brandt, T., Kuzuhara,
M., Tamura, M.: 2015, Discovery of Low Mass Binary with Super
Jupiter Companion, American Astronomical Society, ESS meeting#3, (Hawaii, USA, Nov. 29-Dec. 4, 2015).
Ao, Y.: 2015, Submm observations towards LABs, East Asian ALMA
Science Workshop 2015, (Osaka, Japan, Dec. 8-11, 2015).
Aoki, W.: 2015, Very Low Mass Stars with Extremely Low Metallicity
in the Milky Way's Halo, IAU Symp. 317: The General Assembly of
Galaxy Halos Structure, Origin and Evolution, (Honolulu, HI, USA,
Aug. 3-7, 2015).
Aoki, W.: 2015, Metal-poor stars in the Galactic halo and dwarf galaxies,
First stars, galaxies, and black holes: Now and Then, (Groningen,
Netherland, June 15-19, 2015).
Aoki, W.: 2015, Observational constraints on r-process, Quarks toUniverse in Computational Science, (Nara, Japan, Nov. 4-8, 2015).
Asai, A., Isobe, H., Ueno, S., Shinbori, A., Kitai, R., Shiota, D., Morita,
S.: 2016, Solar Ultraviolet Radiation estimated from Solar Images,
Int. Symp. PSTEP-1: Toward the Solar-Terrestrial Environment
Prediction as Science and Social Infrastructure, (Nagoya, Japan, Jan.
13-14, 2016).
Asayama, A., Saini, K., Yagoubov, P., Whyborn, N., Siringo, G.:2015, ALMA Front End and Its Performances, 36th ESA AntennaWorkshop, (Noordwijk, the Netherlands, Oct. 6-9, 2015).
Baba, Y., Ishikawa, T.: 2015, Nearly 120 Years of Science History inDanger: The Collections in the National Astronomical Observatory ofJapan, Mizusawa, Int. Symp. on the NAOJ Museum, (Tokyo, Japan,

XIII Publications, Presentations

Sep. 27-29, 2015).
Barkin Y., Hanada, H., Barkin, M.: 2015, Precession, nutation, polemotion and variations of LOD of the Earth and the Moon, Japan
Geoscience Union Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Barnes, P., Muller, E., Nguyen-Luong, Q., Nguyen, H.: 2015, The
Three-mm Ultimate Mopra Milky Way Survey (ThrUMMS): A New
View of the Molecular Milky Way, IAU XXIX General Assembly,(Honolulu, HI, USA. Aug. 3-14, 2015).
Bastian, T. S., Barta, M., Brajsa, R., Chen, B., De Pontieu, B.,
Fleishman, G., Gary, D., Hales, A., Hills, R., Hudson, H., Iwai, K.,
Shimojo, M., White, S., Wedemeyer, S., Yan, Y.: 2015, The Atacama
Large Millimeter/Submillimeter Array: a New Asset for Solar andHeliospheric Physics, IAU XXIX General Assembly, (Honolulu, HI,
USA. Aug. 3-14, 2015).
Belikov, R., Bendek, E., Thomas, S., Males, J., Lozi, J.: 2015, How
to directly image a habitable planet around Alpha Centauri with a~30–45 cm space telescope, SPIE Optics + Photonics, (San Diego,
CA, USA, Aug. 9-13, 2015).
Bellot Rubio, L., Gosic, M., del Toro Iniesta, J. C., Katsukawa, Y.: 2015,
The origin and fate of internetwork magnetic elements, 9th Hinode
Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Bendek, E. A., Belikov, R., Lozi, J., Thomas, S., Males, J., Weston, S.,
McElwain, M.: 2015, Space telescope design to directly image thehabitable Zone of Alpha Centauri, SPIE Optics + Photonics, (San
Diego, CA, USA, Aug. 9-13, 2015).
Canas, L., Cheung, S. L.: 2015, International Astronomical Union (IAU)
Directory for World Astronomy Network, Int. Symp. on the NAOJ
Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Canas, L., Cheung, S. L.: 2015, International Astronomical Union(IAU) Directory for World Astronomy Network, IAU XXIX General
Assembly, (Honolulu, HI, USA, Jul. 30-Aug. 15, 2015).
Canas, L., Ortiz-Gil, A.: 2015, Astronomy for Inclusion, UNAWE
workshop 2015, (Leiden, Netherlands, Oc. 5-10, 2015).
Capocasa, E., Barsuglia, M., Degallaix, J., Pinard, L., Straniero, N.,
Schnabel, R., Somiya, K., Aso, Y., Tatsumi, D., Flaminio, R.:
2015, Losses estimation in a 300-m filter cavity and quantum noise
reduction in KAGRA, 4th ELiTES general meeting, (Tokyo, Japan,
Dec. 2-3, 2015).
Cheung, S. L.: 2015, IAU Office for Astronomy Outreach, IAU XXIX
General Assembly, (Honolulu, HI, USA. Aug. 3-14, 2015).
Cheung, S. L.: 2015, Science Center, Planetariums, Public Observatories
and OAO, Int. Symp. on the NAOJ Museum, (Tokyo, Japan, Sep. 2729, 2015).
Cheung, S. L.: 2015, IAU Outreach Initatives and Projects, dotAstronomy
7, (Sydney, Australia, Nov. 3-6, 2015).
Cheung, S. L.: 2015, OAO-SEAAN partnership and the Total Solar
Eclipse 2016, South East Asian Astronomer Network Meeting 2015,(Krabi, Thailand, Nov. 30-Dec. 1, 2015).
Cheung, S. L.: 2015, Planetarium and OAO, Int. Symp. on the NAOJ
Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Cheung, S. L., Pun, J. C. S., So, C. W., Shibata, Y., Walker, C., Agata,H.: 2015, Globe at Night - Sky Brightness Monitoring Network, IAU
XXIX General Assembly, (Honolulu, HI, USA. Aug. 3-14, 2015).
Chiba, M., Tanaka, M., Komiyama, Y.: 2015, Subaru Hyper Suprime
Cam Survey of the Andromeda Halo, IAU XXIX General Assembly,(Honolulu, HI, USA. Aug. 3-14, 2015).

Dominjon, A., Noguchi, T., Sekine, M., Karatsu, K., Sekimoto, Y.,
Okada, T., Shibo, S., Sekiguchi, S., Nitta, T.: 2015, Microwave
Kinetic Inductance Detectors with Superconductor Bilayer, The 16th
Workshop on Submm Wave Receiver Technologies in Eastern Asia,(Nanjing, China, Nov. 22-25, 2015).
Egusa, F.: 2015, CO(1-0) Mapping Survey of ~100 Nearby Spiral
Galaxies with ALMA, ALMA Workshop for Large Proposals on
Nearby Galaxies, (Tokyo, Japan, Aug. 25-26, 2015).
Egusa, F.: 2015, CO survey of ~100 nearby spiral galaxies with ALMA,
ALMA/45m/ASTE/Mopra Users Meeting 2015, (Tokyo, Japan, Oct.
20-22, 2015).
Egusa, F.: 2015, Large Proposal Plans for Nearby Galaxies, East Asian
ALMA Science Workshop 2015, (Osaka, Japan, Dec. 8-11, 2015).
Egusa, F.: 2015, Review of recent observations of nearby galaxies with
NRO45m and ALMA, NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Espada, D.: 2015, Galaxies and AGN studies with ALMA, East Asian
ALMA Science Workshop 2015, (Osaka, Japan, Dec. 8-11, 2015).
Ferré-Mateu, A., Mezcua, M., Trujillo, I., Balcells, M., van den Bosch,R.: 2015, Witnessing a different (co-)evolution for relic massive
galaxies and their Übermassive black holes, EWASS 2015, (LaLaguna, Spain, Jun. 22-26, 2015).
Flaminio, R.: 2015, The case of a cryogenic interferometer: KAGRA,The Next Detectors for Gravitational Wave Astronomy, (Beijing,
China, Apr. 6-May 8, 2015).
Flaminio, R.: 2015, The cryogenic challenge: status of the KAGRA
project, The 11th Edoardo Amaldi Conference on Gravitational
Waves, (Gwangju, Korea, June 21-26, 2015).
Flaminio, R.: 2015, Frequency dependent squeezing experiment at
TAMA, KAGRA F2F Meeting, (Toyama, Japan, Aug. 25-28, 2015).
Fujii, M.: 2015, Formation of intermediate-mass black holes in starclusters, Max’s 4 questions in X-ray astronomy to be addressed with
ASTRO-H, (Tokyo, Japan, Jul. 31, 2015).
Fujii, M.: 2015, The Origin of the Mass Function of Star Clusters, XXIXIAU General Assembly FM18: Scale-free processes in the universe,(Honolulu, HI, USA, Aug. 12-14, 2015).
Fujii, M.: 2015, The formation and dynamical evolution of young starclusters, MODEST-15S, (Kobe, Japan, Dec. 7-11, 2015).
Fujii, M.: 2015, The origin of the variety of star clusters, Star Formation
Workshop 2015, (Mitaka, Japan, June 29-Jul. 1, 2015).
Fujii, M., Portegies Zwart, S.: 2015, Formation of young massive
clusters from turbulent molecular clouds, IAU Symp. 316: Formation,
evolution, and survival of massive star clusters, (Honolulu, HI, USA,
Aug. 11-14, 2015).
Fujii, Y., Sekiguchi, T., Takahashi, R., Aso, Y., Barton, M., Peña
Arellano, F. E., Shoda, A., Akutsu, T., Ishizaki, H., Tatsumi, D.,
Hirata, N., Hayama, K., Okutomi, K., Miyamoto, T., Ishizuka, H.,
Flaminio, R.: 2015, Status of KAGRA vibration isolation system,
The 11th Edoardo Amaldi Conference on Gravitational Waves,(Gwangju, Korea, June 21-26, 2015).
Fujita, C., Ozeki, H., Kobayashi, K.: 2015, The Microwave Spectroscopyof Aminoacetonitrile in the Vibrational Excited State, Int. Symp. on
Molecular Spectroscopy, 70th meeting, (Urbana-Champagne, IL,
USA, Jun. 22-26, 2015).
Fujiwara, H.: 2015, Observational Research with Subaru Telescope,
SEAYAC 2015, (Krabi, Thailand, Dec. 3-4, 2015).

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185

Fujiwara, H.: 2015, Infrared Observation of Warm Debris Disks,
Exoplanets in Lund 2015, (Lund, Sweden, May 6-8, 2015).
Fukagawa, M., Grady, C. A., Wisniewski, J. P., Ohta, Y., Momose, M.,
Matura, Y., Kotani, T., Okamoto, Y., Hashimoto, J., Muto, T., Sitko,
M., Follette, K., Bonnefoy, M., Kusakabe, N., Tamura, M., SEEDS/HiCIAO/IRCS/AO188 Collaboration: 2015, Non-axisymmetricstructure in million-year-old discs around intermediate-mass stars,
Disc Dynamics & Planet Formation, (Lancashire, UK, Jun. 29-Jul. 3,2015).
Fukagawa, M.: 2015, A review of recent observations of protoplanetarydisks, Protoplanetary Disk Dynamics and Planet Formation,(Kanagawa, Japan, Sep. 29–Oct. 2, 2015).
Fukagawa, M.: 2015, Recent advances in understanding planet
formation, NRO-ALMA Science/Development Workshop 2015,(Nagano, Japan, Jul. 28-30, 2015).
Fukui, A.: 2015, Characterization of microlensing planetary systems by
AO imaging, From super-earths to brown dwarfs: who's who?, (Paris,
France, Jun. 29-Jul. 3, 2015).
Fukui, A.: 2016, Toward the Metallicity Measurements of Microlensing
Planetary Host Stars, 20th Microlensing Workshop, (Paris, France,
Jan. 13-15, 2016).
Furusawa, H.: 2015, Software and database: A review of S15A
workarounds, Understanding Evolution of Quasars: Collaboration
between Theoretical Models and Initial HSC Survey, (Kagoshima,
Japan, Dec. 1-3, 2015).
Furusawa, H.: 2015, Status of SSP data release production, HSC
Collaboration Meeting, (Princeton, NJ, USA, Jul. 27-19, 2015).
Furusawa, H.: 2016, Status of Data Release Preparation, HSC
Collaboration Meeting, (Taipei, Taiwan, Jan. 13-15, 2016).
Furusawa, H.: 2015, Equations of state at sub-nuclear densities
and weak interactions in Supernovae, Physics and Astronomy
of Neutron Stars and Supernovae, (Tokyo, Japan, Jun. 21-22, 2015).
Furusawa, S.: 2015, Equation of State of Supernova Matter with
Ensembles of Nuclei, International Numazu Workshop on Challengesof Modeling Supernovae with Nuclear Data, (Shizuoka, Japan, Sep.
1-4, 2015).
Furusawa, S.: 2015, Equation of state including full nuclear ensemble insupernova simulations, Quarks to Universe in Computational Science,(Nara, Japan, Nov. 4-8, 2015).
Geballe, T. R., Oka, T., Lambrides, E., Yeh, S. C. C., Schlegelmilch, B.,
Goto, M., Westrick, C. W.: 2015, New Background Infrared Sources
For Studying the Galactic Center's Interstellar Gas, Int. Symp. on
Molecular Spectroscopy, 70th meeting, (Urbana-Champagne, IL,
USA, Jun. 22-26, 2015).
Giono, G., Ishikawa, R., Narukage, N., Kano, R., Katsukawa, Y.,
Kubo, M., Ishikawa, S., Bando, T., Hara, H., Suematsu, Y.,
Winebarger, A., Kobayashi, K., Auchère, F., Trujillo Bueno, J.: 2015,
CLASP: reaching below the 0.1 % polarization sensitivity, 9th Hinode
Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Gonzalez, A.: 2015, Optical design considerations for a large dishantenna in ALMA, NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Gonzalez, A.: 2015, Design of optics for ALMA receivers at NAOJ, 36th
ESA Antenna Workshop, (Noordwijk, the Netherlands, Oct. 6-9, 2015).
Gonzalez, A., Tapia, V., Finger, R., Asayama, S., Huang, T.: 2015,
Alternative Optics Design for the ALMA Band 1 Receiver (35-186

XIII Publications, Presentations

52 GHz), 9th European conference on Antennas and Propagation,(Lisbon, Portugal, Apr. 12-17, 2015).
Gouda, N.: 2015, Infrared Space Astrometry missions: JASMINE,
Division A meeting at the XXIX General Assembly of IAU,
(Honolulu, USA, Aug. 7-10, 2015).
Grady, C. A., et al. including Tamura, M.: 2015, Decoding Debris System
Substructures: Imprints of Planets/Planetesimals and Signatures ofExtrinsic Influences on Material in Ring-Like Disks, AAS Meeting#227, (Kissimmee, FL, USA, Jan. 4-8, 2016).
Gusev, A., Hanada, H., Petrova, N., Ping, J.: 2015, Physical librations
and free nutations of the three-layer Moon for ChangE-3/4, LunaGlob-Resource, SELENE-2 missions, 2nd IAPS Scientific Assembly,(Kazan, Russia, Jun. 1-4, 2015).
Gusev, A., Hanada, H., Petrova, N.: 2015, Physical librations and theinternal structure of a multilayer resonant moons in the Solar System,
2nd IAPS Scientific Assembly, (Kazan, Russia, Jun. 1-4, 2015).
Guyon, O., Jovanovic, N., Lozi, J.: 2015, Direct imaging and spectroscopic
characterization of habitable planets with ELTs, Extreme Solar
Systems III, (Waikoloa, HI, USA, Nov. 29-Dec. 4, 2015).
Hada, K.: 2015, Deep imaging and monitoring of the collimation andacceleration region of the M87 jet, 8th East Asia VLBI Workshop,(Sapporo, Japan, Jul. 8-10, 2015).
Hada, K.: 2016, (Lecture) AGN, NARIT-UST-GUAS Radio Astronomy
Winter School 2016, (Chiang Mai, Thailand, Feb.15-19, 2016).
Hada, L.: 2016, M87 monitor project with KaVA: current status, The
10th NARIT-KaVA Joint Science WG meeting, (Krabi, Thailand,
Feb. 22-24, 2016).
Hagino, M., Ichimoto, K., Ueno, S., Kimura, G., Otsuji, K., Kitai, R.,
Zhong, L., Xu, Z., Shinoda, K., Hara, H., Suematsu, Y., Shimizu,
T.: 2015, Development of the Universal Tunable Filter and Highresolution Imaging Observation with the Fuxian Solar Observatory,
Coimbra Solar Physics Meeting: Ground-based Solar Observations in
the Space Instrumentation Era, (Coimbra, Portugal, Oct. 5-9, 2015).
Hamana, T.: 2015, Cosmological constraints from Subaru weak lensing
cluster counts, Theoretical and Observational Progress on Large-scale
Structure of the Universe, (Garching, Germany, Jul. 20-24, 2015).
Hanada, H., Tsuruta, S., Asari, K., Araki, H., Noda, H., Kashima, S.,
Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Sasaki,
H., Shinke, S., Petrova, N., Gusev, A.: 2015, Ground experiments ofa small telescope like PZT for observations on the Moon, 2nd IAPS
Scientific Assembly, (Kazan, Russia, Jun. 1-4, 2015).
Hanada, H., Tsuruta, S., Asari, K., Araki, H., Noda, H., Kashima,S., Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M.,
Yokokawa, R., Shinke, S.: 2015, Summary of the development of asmall telescope for lunar rotation and the experiments on the ground,
Japan Geoscience Union Meeting 2015, (Chiba, Japan, May 24-28,
2015).
Hanada, H.: 2015, International Cooperation in NAOJ Mizusawa :Result of Kaguya, and possibility in the future, Japan Geoscience
Union Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Hanaoka, Y., the Solar Observatory of NAOJ: 2015, Past and Presentof the Synoptic Observations of the Sun at the National Astronomical
Observatory of Japan, Coimbra Solar Physics Meeting: Groundbased Solar Observations in the Space Instrumentation Era, (Coimbra,
Portugal, Oct. 5-9, 2015).
Hara, H., Glesener, L.: 2015, Coronal Velocity Fields near an ImpulsiveHard X-ray Source Located above Soft X-ray Flare Loops, 9thHinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Hara, H.: 2015, Unresolved Plasma Motions in Coronal Loops, Coronal
Loop Workshop VII, (Cambridge, UK, Jul. 21-23, 2015).
Hara, H.: 2015, The SOLAR-C Mission, 3rd Asia-Pacific Solar Physics
Meeting (APSPM 2015), (Soule, South Korea, Nov. 3-6, 2015).
Hara, H.: 2016, Reconnection-associated Dynamic Structures from EUV
Observations in Solar Flares, 2016 US-Japan Workshop on Magnetic
Reconnection (MR2016), (Napa, CA, USA, Mar. 7-11, 2016).
Hara, H.: 2016, The SOLAR-C Mission, ISEE Workshop 2015, (Nagoya,Japan, Mar. 22-25, 2016).
Harada, R., Onishi, T., Hughes, A., Meixner, M., Sewilo, M., Indebetouw,
R., Nayak, O., Tokuda, K., Morioka, Y., Fukui, Y., Kawamura, A.,
Wong, T., Bernard, J.-P.: 2015, Investigating formation of isolated
intermediate/massive YSOs in the LMC, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda, H.,
Haruyama, J.: 2015, Strong tidal heating inside an ultralow-viscosity
zone over the lunar core-mantle boundary, Japan Geoscience Union
Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Harakawa, H., Sato, B., Omiya, M., Fischer, D. A., Hori, Y., Ida, S.,HIDES-F team: 2015, Search for Exoplanets around Metal-Rich
FGK Stars, Exoplanets and Disks: Their Formation and Diversity III,
(Ishigaki, Japan, Feb. 21-24, 2016).
Harra, L. K., Baker, D. Sterling, A., Edwards, S., Hara, H., Howe, R.
van Driel-Gesztelyi, L.: 2015, Exploring polar regions and coronahole boundaries through coronal spectroscopy, 9th Hinode Science
Meeting, (Belfast, UK, Sep. 14-17, 2015).
Hasegawa, T.: 2015, SgrB2(N): A bipolar outflow and rotating hot core
revealed by ALMA, East Asian ALMA Science Workshop 2015,(Osaka, Japan, Dec. 8-11, 2015).
Hatsukade, B., Ohta, K., Endo, A., Nakanishi, K., Tamura, Y.,
Hashimoto, T., Kohno, K.: 2015, Gamma-ray bursts from dusty
regions with little molecular gas, Gas, Dust, and Star-Formation in
Galaxies from the Local to Far Universe, (Plantanias-Chania, Crete,
Greece, Apr. 25-29, 2015).
Hatsukade, B.: 2015, High-resolution ALMA observations of SDP.81.
II. Molecular clump properties of a lensed submillimeter galaxy at
z = 3.042, ALMA/45 m/ASTE/Mopra Users Meeting 2015, (Tokyo,
Japan, Oct. 20-22, 2015).
Hatsukade, B.: 2015, High-resolution ALMA observations of SDP.81:
Molecular clump properties of a lensed submillimeter galaxy at z =3.042, East Asian ALMA Science Workshop 2015, (Osaka, Japan,
Dec. 8-11, 2015).
Hatsukade, B.: 2015, Gamma-ray bursts from dusty regions with little
molecular gas, IAU XXIX General Assembly, (Honolulu, HI, USA,
Aug. 3-14, 2015).
Hatsukade, B.: , Recent studies of distant galaxies with NRO 45 m
and ALMA, NRO-ALMA Science/Development Workshop 2015,(Nagano, Japan, Jul. 28-30, 2015).
Hayano, Y.: 2016, Adaptive optics in astronomy and the future
perspective, Symposium on Super adaptive optics with wave
field correction: Toward perfect imaging of the universe and liveorganisms, (Mitaka, Japan, Mar. 23, 2016).
Hayano, Y., Chun, M., Honda, M.: 2015, Development and on-sky
experiment of narrow band filter for daytime AO observation using

laser guide star in mid-infrared wavelength, AO4ELT4, (Lake
Arrowhead, CA, USA, Oct. 26-30, 2015).
Hayashi, M.: 2015, NAOJ Projects and E/PO Activities, Int. Symp. on
the NAOJ Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Herrera, C. N., Boulanger, F., Falgarone, E. G., des Forets, G. P.,
Garcia-Burillo, S., Iono, D., Guillard, P.: 2015, The ALMA viewof the Antennae galaxy collision, IAU XXIX General Assembly,(Honolulu, HI, USA, Aug. 3-14, 2015).
Herrera, C. N., Boulanger, F.: 2015, Stellar feedback from a massive
Super Star Cluster in the Antennae merger, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Hirai, Y., Ishimaru, Y., Saitoh, T. R., Fujii, M. S., Hidaka, J., Kajino, T.:2015, Astrophysical site(s) of r-process elements in galactic chemodynamical evolution model, The 13th International Symposium on
Origin of Matter and Evolution of Galaxies (OMEG2015), (Beijing,
China, Jun. 24-27, 2015).
Hirai, Y., Ishimaru, Y., Saitoh, T. R., Fujii, M. S., Hidaka, J., Kajino,
T.: 2015, Chemo-dynamical evolution model: Enrichmentof r-process elements in the Local Group dwarf galaxies,
IAU Symp. 317: The General Assembly of Galaxy Halos
Structure, Origin and Evolution, (Honolulu, HI, USA, Aug. 3-7, 2015).
Hiramatsu, M.: 2015, ALMA Public Outreach, ALMA/45m/ASTE/
Mopra Users Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Hirano, T., Sato, B., Masuda, K., Benomar, O., Takeda, Y., Omiya, M.,
Harakawa, H.: 2015, Search for Close-in Planets around Evoloved
Stars with Phase-curve variations and Radial Velocity Measurements,
IAU XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14,2015).
Hirota, A.: 2015, Giant Molecular Clouds and Star Formation in Nearby
Galaxy M83, East Asian ALMA Science Workshop 2015, (Osaka,
Japan, Dec. 8-11, 2015).
Hirota, T., Matsumoto, N., Hada, K., Sawada-Satoh, S.: 2016, AIPS
tutorial, NARIT-UST-GUAS Radio Astronomy Winter School 2016,(Chiang Mai, Thailand, Feb.15-19, 2016).
Hirota, T.: 2015, Observational study of (sub)millimeter maser lines instar-forming regions, High Mass Star Formation Workshop, (Tokyo,
Japan, Jul. 22, 2015).
Hirota, T.: 2015, CASA Users Committee Report, ALMA/45m/ASTE/
Mopra Users Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Hirota, T.: 2016, Hot water disk around Orion Source I, Workshop on
Astrochemistry in Star and Planet Formation, (Wako, Japan, Feb. 16,2016).
Hirota, T.: 2016, Status report of SFRs sub-WG, The 10th NARIT-KaVA
Joint Science WG meeting, (Krabi, Thailand, Feb. 22-24, 2016).
Hirota, T.: 2016, Proposal of new science cases for SFRs studies with
KaVA, The 10th NARIT-KaVA Joint Science WG meeting, (Krabi,
Thailand, Feb. 22-24, 2016).
Honma, M.: 2015, Current status of EHT and related activities in Japan,
8th East Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Honma, M.: 2016, (Lecture) VERA, NARIT-UST-GUAS Radio Astronomy
Winter School 2016, (Chiang Mai, Thailand, Feb.15-19, 2016).
Honma, M.: 2016, EAVN and SKA, Australia-Japan School on Low
Frequency Astrometry in the SKA Era, (Kagoshima, Japan, Mar. 2831, 2016).
Hori, Y.: 2015, Can ExoEarths be Habitable?: Origin and Evolutionof Planetary Atmospheres, Astrobiology: A Japanese-German

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Colloquium, (Kiel, Germany, Dec. 8-10, 2015).
Hori, Y.: 2015, Recent Developments in Planetary Interiors under High
Pressure, International Workshop on Warm Dense Matter 2015,(Kurashiki, Okayama, Japan, Aug. 8-13, 2015).
Hori, Y.: 2015, The Interior Structure of Jupiter Towards Future
Missions of the Jovian System, 48th ISAS Lunar and PlanetarySymp., (Sagamihara, Kanagawa, Japan, Jul. 29-31, 2015).
Hori, Y.: 2015, Peer into a Nutshell: The Interior of Jupiter, Science
Workshop for the Giant Planet System, (Ookayama, Tokyo, Japan,
Apr. 14, 2015) .
Hori, Y.: 2016, The Atmospheres and Water on Our Terrestrial Planets
and Other Planets, Symposium on Hierarchy and Holism in Natural
Sciences, (Mitaka, Tokyo, Japan, Feb. 5-6, 2016).
Hori, Y., Liu, S-F., Lin, D. N. C., Asphaug, E.: 2015, A Collisional
Origin for the Coexistence of Volatile-poor Super-Earths and MiniNeptunes in the Proximity of Their Host Stars, Extreme Solar
Systems III, (Waikoloa, HI, USA, Nov. 29-Dec. 4, 2015).
Hori, Y., Liu, S-F., Lin, D. N. C., Asphaug, E.: 2015, A Collisional
Origin for the Coexistence of Volatile-poor Super-Earths and MiniNeptunes in the Proximity of Stars, Exoplanetary Atmospheres andHabitability: Thermodynamics, Disequilibrium, and Evolution Focus
Group, (Nice, France, Oct. 12-16, 2015).
Hori, Y., Liu, S-F., Lin, D. N. C., Asphaug, E.: 2016, Deep Impact on a
Super-Earth in the Vicinity of a Central Star, Exoplanets and Disks:
Their Formation and Diversity III, (Ishigaki, Japan, Feb. 21-24, 2016).
Ichikawa, K.: 2015, Outflow/inflow study of buried AGN through 4.7 μm
CO absorption line, TMT Thermal infrared science & instrument
workshop, (Tokyo, Japan, Jun. 12, 2015).
Ichikawa, K.: 2015, On the torus structure and the detection of polarized
broad emission lines in AGN, East Asia AGN workshop 2015,(Changchun, China, Jul. 14-16, 2015).
Ichikawa, K.: 2015, Determining the dust torus covering factor using
clumpy torus models in IR, Prospects, challenges and evolution of
AGN modeling in the Astro-H Era, (Tokyo, Japan, Oct. 21-22, 2015).
Ide, H., Kinugasa, K., Suzuki, Y., Nishioka, M., Mikoshiba, H.,
Miyazawa, K., Shinohara, N., Saito, M., Ohnishi, K.: 2015, Artist
in Residence at the Nobeyama Radio Observatory, NAOJ, Int. Symp.
on the NAOJ Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Iguchi, S.: 2015, ALMA project report, ALMA/45m/ASTE/Mopra Users
Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Iguchi, S.: 2015, Compact Array vs Large Single Dish Telescope which is more cost-effective -, NRO-ALMA Science/Development
Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Ikeya, M., Kojima, T., Sakai, T., Noguchi, T.: 2015, Reduction of
Leakage Current of Nb SIS Junctions by Adding an Extra Al Layer,
15th Int. Superconductive Electronics Conf. 2015 (ISEC2015),(Nagoya, Japan, Jul. 6-9, 2015).
Ikeya, M., Kojima, T., Sakai, T., Noguchi, T.: 2015, Evaluation
and Analysis of Nb/Al/AlOx/Al/Nb Junctions, 16th Workshop
on Submillimeter-Wave Receiver Technologies in Eastern Asia ,(Nanjing, China, Nov. 22-25, 2015).
Imanishi, M.: 2015, ALMA observations of molecular gas in the close
vicinity of AGNs, Torus 2015 The unification scheme after 30 years,(Winchester, UK, Sep. 14-17, 2015).
Imanishi, M.: 2015, Optically-elusive buried dual AGN population in
infrared-luminous gas/dust-rich galaxy mergers and implication for

188

XIII Publications, Presentations

feedback to galaxies, Demographics and environment of AGN frommulti-wavelength surveys, (Chania, Greece, Sep. 21-24, 2015).
Inoue, A., Shimizu, I., Okamoto, T., Yoshida, N., Matsuo, H., Tamura, Y.:
2015, Prediction of emission line fluxes of gravitationally lensed very
high-z galaxies, IAU XXIX General Assembly, (Honolulu, HI, USA,
Aug. 3-14, 2015).
Inoue, T.: 2015, MHD Simulations of Massive Star Formation Triggeredby Cloud Collision, Star Formation Workshop 2015, (Mitaka, Japan,
June 29-Jul. 1, 2015).
Inoue, T.: 2015, Magnetohydrodynamic Simulation of Supernova ShockWave in Realistic Interstellar Medium, The 1st Conference on Laser
Energetics, (Yokohama, Japan, Apr. 22-24, 2015).
Iono, D.: 2015, Mopra report, ALMA/45 m/ASTE/Mopra Users Meeting
2015, (Tokyo, Japan, Oct. 20-22, 2015).
Iono, D.: 2015, ALMA Workshops and Large Proposals, ALMA/45m/
ASTE/Mopra Users Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Iono, D.: 2015, ALMA Future Development, ALMA/45m/ASTE/Mopra
Users Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Iono, D.: 2015, ALMA Future Development, NRO-ALMA Science/
Development Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Ishigaki, M. N., Tsujimoto, T., Shigeyama, T., Aoki, W.: 2015,
Chemical evolution of r-process elements in Draco dwarf spheroidal
galaxies, “IAU Symp. 317: The General Assembly of Galaxy Halos
Structure, Origin and Evolution”, (Honolulu, HI, USA, Aug. 3-7,2015).
Ishiguro, M., Kuroda, D., Kim, Y., Kwon, Y., Hanayama, H., Miyaji, T.,
Honda, S., Takahashi, J., Watanabe, J.-I.: 2015, Multiple Outburstsof a Short-Periodic Comet 15P/Finlay, Korean Astronomical Society
2015 Spring Meeting, (Seoul National University, South Korea, Apr.
15-17, 2015).
Ishikawa, R., et al. including Kano, R., Bando, T., Narukage, N.,
Katsukawa, Y., Kubo, M., Giono, G., Hara, H., Suematsu, Y.:
2015, CLASP: a UV spectropolarimeter on a sounding rocket for
probing the chromosphere-corona transition region, IAU XXIX
General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Ishikawa, R., et al. including Kano, R., Bando, T., Narukage, N.,
Katsukawa, Y., Kubo, M., Giono, G., Hara, H., Suematsu, Y.:
2015, Initial Results of Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP), 3rd Asia-Pacific Solar Physics Meeting(APSPM 2015), (Soule, South Korea, Nov. 3-6, 2015).
Iye, M.: 2015, Subaru Telescope, Adaptive Optics, and Thirty Meter
Telescope, The 1st International Conference on Advanced Imaging,(Tokyo, Japan, Jun. 17-19, 2015).
Iye, M.: 2015, The Thirty Meter Telescope Project, Camera and Photo
Imaging Show 2016, (Yokohama, Japan, Feb. 28, 2016).
Izumiura, H.: 2015, The Future of the Okayama AstrophysicalObservatory, The 9th Workshop on Astronomy with Precise Radial
Velocity, (Lijiang, YN, China, Oct. 27-29, 2015).
Jike, T.: 2015, Current status and future view of VERA Geodesy, 1stAsia-Oceania-VLBI Meeting, (Tasmania Univ. Hobart, Austraria,
Nov. 19, 2015).
Jike, T.: 2016, VERA K-band Geodetic VLBI Experiment Using Newly
Developed High Speed Sampler and Recorder, 9th IVS General
Meeting, (Johanesburg, South Africa, Mar. 15, 2016).
Kajino, T.: 2015, Explosive nucleosynthesis: A Probe of Cosmic andSupernova Neutrinos, The 13th International Symposium on Origin

of Matter and Evolution of Galaxies (OMEG2015), (Beijing, China,
Jun. 24-27, 2015).
Kajino, T.: 2015, Supernova Neutrinos and Nucleosynthesis, The 5thInternational Symposium on Neutrinos and Dark Matter, (Jyuaskyla,
Finland, Jun. 1-5, 2015).
Kajino, T.: 2015, Quest for Nuclear Physics and the Origin of R-Process,The 3rd International Conference on Nuclear Structure andDynamics, (Portoroz, Slovenia, Jun. 15-19, 2015).
Kajino, T.: 2015, Galactic Evolution of the R-Process Elements andthe Universality, International Numazu Workshop on Challenges ofModeling Supernovae with Nuclear Data, (Shizuoka, Japan, Sep. 1-4,
2015).
Kajino, T.: 2015, Solving Coalescence Time Scale Problem of GRB
R-Process in Galactic Chemo-Dynamics, Gamma-Ray Burst
Workshop, (Wako, Saitama, Japan, Aug. 31-Sep. 2, 2015).
Kajino, T.: 2015, Neutrino Physics in Astrophysics, and the Originof R-Process, The 8th European Summer School on Experimental
Nuclear Astrophysics, (St. Tecla, Catania, Italy, Sep. 13-20, 2015).
Kajino, T.: 2015, Origin of R-Process Elements in Galactic Evolution
and Relic Supernova Neutrinos, Korean Physical Society 2015 Fall
Meeting, (Gyeonju, Korea, Oct. 21-23, 2015).
Kajino, T.: 2015, Galactic Evolution of Supernova and Merger
R-Process, Quarks to Universe in Computational Science, (Nara,
Japan, Nov. 4-8, 2015).
Kajino, T.: 2016, Neutrino Astrophysics in Supernovae, KIAS/KNRC
School on Neutrino Physics, (KIAS, Seoul, Korea, Feb. 15-17, 2016).
Kambe, E.: 2015, Recent status and updates of HIDES/OAO, The 9thWorkshop on Astronomy with Precise Radial Velocity, (Lijiang, YN,
China, Oct. 27-29, 2015).
Kameya, O., Funayama, H.: 2015, Collaboration of Kimura Hisashi
Memorial Museum and Oshu Space and Astronomy Museum in
NAOJ Mizusawa Campus, Int. Symp. on the NAOJ Museum, (Tokyo,
Japan, Sep. 27-29, 2015).
Kameya, O., Funayama, H.: 2015, Kimura Memorial Museum in
NAOJ Mizusawa Campus, Int. Symp. on the NAOJ Museum, (Tokyo,
Japan, Sep. 27-29, 2015).
Kameya, O.: 2015, Current Status of the Mizusawa 10m Radio telescope,
8th East Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Kaneko, H.: 2015, Large Massive Molecular Gas Cloud at the Collision
Front of the Interacting Galaxies in Early Stage, Gas, Dust, and StarFormation in Galaxies from the Local to Far Universe, (PlantaniasChania, Crete, Greece, Apr. 25-29, 2015).
Kaneko, H.: 2015, COMING-TAO Collaboration “COMING-PLUS”,
TAO/SWIMS Sceince Workshop 2015, (Mitaka, Japan, Sep. 17-18,
2015).
Kaneko, H.: 2015, Molecular Collision Front in Interacting Galaxies,
East Asian ALMA Science Workshop 2015, (Osaka, Japan, Dec. 8-11,2015).
Kaneko, H.: 2016, Effects of Galaxy Interactions on Molecular Gas
Properties, From Stellar Evolution to Galaxy Formation, (Nobeyama,
Japan, Mar. 7-9, 2016).
Kang, M., Choi, M., Stutz, A. M., Tatematsu, K.: 2015, [HDCO]/[H2CO]
ratios toward extremely cold protostars in Orion, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Kano, R., et al. including Narukage, N., Ishikawa, R., Bando, T.,
Katsukawa, Y., Kubo, M., Giono, G., Hara, H., Suematsu, Y.: 2015,

Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), 9thHinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Kashiwagi, K., Kurokawa, T.: 2015, Photonic Arbitrary Waveform
Generation Using Optical Pulse Synthesizer and Its Applications,
PIERS 2015, (Prague, Czech Republic, Jul. 6-9, 2015).
Kato, C., Nakajima, T., Akiyama, N., Ito, M., Urushihara, K., Koga,
M., Yamamoto, H., Mizuno, A., Kojima, T., Fujii, Y., Asayama,S., Noguchi, T., Kozuki, Y., Hasegawa, Y., Ogawa, H.: 2015,
Development of superconducting device for millimeter-wave
atmospheric radiometer, Founding Symposium for the Institute forSpace-Earth Environmental Research, (Nagoya, Japan, Nov. 4-5,2015).
Kato, C., Nakajima, T., Akiyama, N., Ito, M., Urushihara, K., Koga, M.,
Yamamoto, H., Mizuno, A., Kojima, T., Fujii, Y., Asayama, S.,
Noguchi, T., Kozuki, Y., Hasegawa, Y., Ogawa, H.: 2015, Progressof the development of series junction SIS device in 100 and 200 GHz
band, NRO-ALMA Science/Development Workshop 2015, (Nagano,
Japan, Jul. 28-30, 2015).
Katsukawa, Y., Kimura, Y., Okamoto, T. J., Tarbell, T.: 2015, HINODEIRIS observation of penumbral microjets in the chromosphere andtheir transition region counterpart, 9th Hinode Science Meeting,(Belfast, UK, Sep. 14-17, 2015).
Katsukawa, Y., Kimura, Y., Okamoto, T. J., Tarbell, T.: 2015, IRIS
Observation of Penumbral Microjets in the Chromosphere and their
Transition Region Counterpart, IRIS-4 Workshop, (Boulder, CO,
USA, May. 18-22, 2015).
Kawabe, R.: 2015, LST, NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Kawamura, A., Onishi, T., Harada, R., Morioka, Y., Tokuda, K.,
Meixner, M., Indebetouw, R., Sewilo, M., Nayak, O., Saigo, K.,
Fukui, Y.: 2015, Giant molecular clouds in the Large Magellanic
Cloud seen in sub-parsec scales by ALMA, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Kawamura, A.: 2015, Development of our study with 45m and ALMA:
Molecules in the active galaxy NGC 1068, ALMA/45m/ASTE/Mopra
Users Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Kawamura, A.: 2015, Tracing an evolution of giant molecular clouds inthe LMC, East Asian ALMA Science Workshop 2015, (Osaka, Japan,
Dec. 8-11, 2015).
Kawashima, T., Matsumoto, Y., Matsumoto, R.: 2015, Time evolution of
the Sgr A* accretion flow interacting with the G2 cloud, QUCS 2015,(Nara, Japan, Nov. 4-8, 2015).
Kawashima, T., Matsumoto, Y., Matsumoto, R.: 2015, On the time
evolution of the Sgr A* accretion flow interacting with the G2 cloud,8th East Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Kawashima, T., Matsumoto, Y., Matsumoto, R.: 2015, Time evolutionof the Sgr A* accretion flow interacting with a gas cloud, Black Hole
Accretion and AGN Feedback, (Shanghai, China, Jun. 1-5, 2015).
Kawashima, T., Ohsuga, K., Takahashi, H., Mineshige, S., Yoshida,T., Matsumoto, R.: 2015, Photon Spectra of Super-critical Black
Hole Accretion Flows, Prospects, challenges and evolution of AGN
modeling in the Astro-H Era, (Tokyo, Japan, Oct. 21-22, 2015).
Kim, J. S.: 2016, Recent Water Maser distribution for Massive Star
Formation Region in Cepheus A, The 10th NARIT-KaVA Joint
Science WG meeting, (Krabi, Thailand, Feb. 22-24, 2016).
Kimura, Y., Hara, H.: 2015, Properties of the sub-arcsecond structure

XIII Publications, Presentations

189

observed in Transition region under Coronal loop, Japan Geoscience
Union Meeting 2015, (Chiba, Japan, May. 24-28, 2015).
Kinugasa, K., Nishioka, M., Mikoshiba, H., Miyazawa, K., Shinohara,N., Ide, H., Saito, M.: 2015, The Record of 3 Million Visitors andthe NINS PR Center in the NAOJ Nobeyama Campus, Int. Symp. on
the NAOJ Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Kitazato, K., Iwata, T., Abe, M., Ohtake, M., Tsumura, K., Ishikawa, T.,
Takato, N., Nakauchi, Y., Arai, T., Senshu, H., Hirata, N., Takagi, Y.,
Hayabusa2 NIRS3 Team: 2016, Near-Infrared Spectroscopy of the
Earth and Moon During the Hayabusa2 Earth Swing-By, 47th Lunarand Planetary Sci. Conf., (The Woodlands, TX, USA, Mar. 21-25,
2016).
Kiuchi, H.: 2015, MKID readout: Frequency sweeping scheme readout
system, B-mode from space, (Chiba, Japan, Dec. 10-16, 2015).
Kobayashi, H.: 2015, EAVN status and future, 8th East Asia VLBI
Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Kobayashi, K., Tsunekawa, S.: 2015, Development of a Room
Temperature Chirped Pulse Fourier Transform Microwave
Spectrometer, Symposium on Advanced Molecular Spectroscopy,(Tokyo, Japan, Jul. 18-19, 2015).
Koda, J.: 2015, ALMA is not sensitive enough, ALMA Workshop forLarge Proposals on Nearby Galaxies, (Tokyo, Japan, Aug. 25-26,
2015).
Koda, J.: 2015, Subaru Deep Imaging of Diffuse (Parts of) Galaxies,
Caltech Infrared Processing and Analysis Center Science Talk,(Pasadena, CA, USA, Oct. 21, 2015).
Koda, J.: 2015, Evolution of the ISM in the Milky Way and Nearby
Galaxies, Caltech Colloqouim, (Pasadena, CA, USA, Nov. 18, 2015).
Koda, J.: 2015, Linking galactic and extragalactic gas and dust surveys,
IAU XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14,2015).
Koda, J.: 2015, Evolution of the interstellar medium in the Milky Way
and nearby galaxies, NRAO Socoro Colloquium, (Socoro, NM, USA,
Sep. 18, 2015).
Kodama, T., Hayashi, M., Tadaki, K., Shimakawa, R., Suzuki, T.,
Yamamoto, M., Tanaka, I.: 2015, Proto-clusters and the earlyenvironmental effects, Galaxy clusters and galaxy formaiton, (Yonsei
Univ., Korea, Oct. 19-23, 2015).
Kodama, T., Hayashi, M., Tadaki, K., Shimakawa, R., Suzuki, T.,
Yamamoto, M., Tanaka, I.: 2015, Early environmental effects inproto-clusters at the cosmic high noon, RSAA Colloquia, (ANU,
Australia, Oct. 12, 2015).
Kodama, T., Hayashi, M., Tadaki, K., Shimakawa, R., Suzuki, T.,
Yamamoto, M., Tanaka, I.: 2015, Early environmental effects inproto-clusters at the cosmic high noon, AAO Colloquium, (AAO,
Australia, Oct. 15, 2015).
Kodama, T., Hayashi, M., Tadaki, K., Shimakawa, R., Suzuki, T.,
Yamamoto, M., Tanaka, I.: 2015, Galaxy ecology: How does
environmewnt matter?, Department colloquium, (Yonsei Univ.,
Korea, Oct. 23, 2015).
Kodama, T., Hayashi, M., Tadaki, K., Shimakawa, R., Suzuki, T.,
Yamamoto, M., Tanaka, I.: 2015, Proto-clusters as the site of earlyenvironmental effects on galaxy formation explored by Mahalo andup-coming surveys on Subaru, ALMA, and TAO, In the footsteps ofgalaxies: Tracing the evolution of environmental effects, (Soverato,
Italy, Sep. 7-11, 2015).

190

XIII Publications, Presentations

Kodama, T., Hayashi, M., Tadaki, K., Shimakawa, R., Suzuki, T.,
Yamamoto, M., Tanaka, I.: 2016, From galaxy evolution to cluster
formation, From stellar-evolution to galaxy formation, (Yatsugatake,Japan, Mar. 7-9, 2016).
Kodama, T., Mahalo-Subaru Team, Gracias-ALMA Team, HSC-HSC
Team: 2015, Physical states of galaxies across various environments,
PFS-SSP galaxy survey workshop, (Kashiwa, Japan, Nov. 13, 2015).
Kodama, T., Mahalo-Subaru Team, SWIMS-18 Team: 2015, Nature ofstar forming galaxies at the peak epoch of galaxy formation, SuabruKeck synergy workshop, (Sendai, Miyagi, Japan, Sep. 1-2, 2015).
Kodama, T., Motohara, K., Mahalo-Subaru Team, SWIMS-18 Team:
2015, Super multi-colour, wide-field, NIR imaging survey with
Subaru and TAO, Galaxies of Many Colours, (Marstrand, Sweden,
Jun. 1-5, 2015).
Kodama, T., ULTIMATE-Subaru Team: 2015, ULTIMATE-K imaging
survey, ULTIMATE Science workshop, (AAO, Australia, Oct. 16, 2015).
Kohno, K., et al. including Kodama, T., Hatsukade, B., Yobe, K.,
Hayashi, M., Iono, D., Matsuda, Y., Nakanishi, K., Kawabe, R.:
2015, SXDF-UDS-CANDELS-ALMA 1.5 arcmin2 deep survey, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Kokubo, E.: 2015, Formation of Close-in Terrestrial Planets by Giant
Impacts: The Basic Scaling Laws, Extreme Solar Systems III,
(Waikoloa, HI, USA, Nov. 29-Dec. 4, 2015).
Kokubo, E.: 2016, Orbital Structure of Planetary Systems Formed by
Giant Impacts, Exoplanets and Disks: Their Formation and Diversity
III, (Ishigaki, Japan, Feb. 21-24, 2016).
Komiyama, Y.: 2016, Outskirts of Local Group Dwarf Galaxies
Revealed by Subaru Hyper Suprime-Cam, IAU Symp. 321: Fornationand evolution of galaxy outskirts, (Toledo, Spain, Mar. 14-18, 2016).
Kono, S., Yokoyama, T., Toriumi, S., Katsukawa, Y.: 2015, Onedimensional numerical simulations and observations of MHD wave
propagation in the solar chromospheric regions with strong magnetic
fields, IRIS-4 Workshop, (Boulder, CO, USA, May. 18-22, 2015).
Koshida, S.: 2015, Reverberation Measurements of the Inner Radius of
the Dust Torus in 17 Seyfert Galaxies, Torus 2015 The unification
scheme after 30 years, (Winchester, UK, Sep. 14-17, 2015).
Koyama,Y.: 2015, Galaxy anatomy with Subaru: our new challenge
beyond MAHALO-Subaru, MPE Infrared Group Retreat, (Bavaria,
Germany , Dec. 9-12, 2015).
Koyama,Y.: 2015, A systematic study of the geometry of stars and dust
within distant star- forming galaxies with PFS, PFS-SSP galaxy
survey workshop, (Kashiwa, Japan, Nov. 13, 2015).
Koyama,Y.: 2016, ULTIMATE-Subaru current status, Subaru Users
Meeting FY2015, (Atami, Japan, Jan. 19-21, 2016).
Kroug, M.: 2015, SIS Mixers for Ultra-Wide RF Bandwidth Operation,
16th Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia , (Nanjing, China, Nov. 22-25, 2015).
Kumamoto, A., Yamaguchi, Y., Yamaji, A., Kobayashi, T., Oshigami, S.,
Ishiyama, K., Nakamura, N., Goto, Y.: 2015, Studies based on global
subsurface radar sounding of the Moon by SELENE (Kaguya) Lunar
Radar Sounder (LRS): A summary, AGU Fall meeting 2015, (SanFrancisco, CA, USA, Dec. 14-18, 2015).
Kuzuhara, M., Tamura, M., Hełminiak, K. G., Mede, K., Brandt,
T., Janson, M., Kandori, R., Kudo, T., Kusakabe, N., Hashimoto,J.: 2015, The SEEDS High-Contrast Imaging Survey: Exoplanet
and Brown Dwarf Survey for Nearby Young Stars Dated with

Gyrochronology and Activity Age Indicators, Extreme Solar Systems
III, (Waikoloa, HI, USA, Nov. 29-Dec. 4, 2015).
Kwon, Y., Ishiguro, M., Hanayama, H., Kuroda, D., Honda, S.,
Takahashi, J., Sarugaku, Y., Kim, Y., Vaubaillon, J. J., Miyaji, T.,
Yanagisawa, K., Yoshida, M., Ohta, K., Kawai, N., Fukushima, H.,
Watanabe, J.-I.: 2015, A Monitoring Observation of Comet 17P/
Holmes during 2014 Apparition, Korean Astronomical Society 2015
Spring Meeting, (Seoul National University, South Korea, Apr. 1517, 2015).
Lee, M., Suzuki, K., Kohno, K., Tamura, Y., Iono, D., Hatsukade, B.,
Nakanishi, K., Tanaka, I., Kodama, T., Tadaki, K., Ikarashi, S.,
Ueda, J., Umehata, H., Saito, T., Kawabe, R.: 2015, Deep JVLA and
ALMA observations of dusty star forming galaxies in protocluster
4C23.56 at z = 2.5, IAU XXIX General Assembly, (Honolulu, HI,
USA, Aug. 3-14, 2015).
Lin, S.-J., Shimajiri, Y., Hara, C., Lai, S.-P., Nakamura, F., Sugitani,K., Kawabe, R., Kitamura, Y., Yoshida, A., Tatei, H., Akashi, T.,
Tsukagushi, T.: 2015, Influence of Interstellar FUV Radiation on the
Abundance Ratio of 13CO to C18O in L 1551, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Louvet, F., Nguyen-Luong, Q.: , The origin of massive clusters: fromhyper-massive clouds to mini-bursts of star formation, IAU XXIX
General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Lozi, J., Guyon, O., Jovanovic, N., Singh, G., Doughty, D., Pathak, P.,
Goebel, S., Kudo, T.: 2015, SCExAO: the most complete instrument
to characterize exoplanets and stellar environments, Extreme Solar
Systems III, (Waikoloa, HI, USA, Nov. 29-Dec. 4, 2015).
Lundock, R.: 2015, Mad Science Crash Course, HawaiiCon, (Kohala
Coast, HI, USA, Sept. 10-13, 2015).
Maehara, H.: 2015, Superflares on G-type stars discovered with Kepler
mission, VarSITI SCOSTEP conference “Superflares and the Sun in
the cycle formation epoch”, (Tel Aviv, Israel, Apr. 28-May 1, 2015).
Maehara, H.: 2015, Statistical properties of superflares on solar-typestars, The first K2 Science Conference, (Santa Barbara, USA, Nov.
2-5, 2015).
Maehara, H.: 2016, Superflares and starspot activity on solar-type stars,
Superflare Workshop 2016 “Superflares on Solar-type Stars and Solar
Flares, and Their Impacts on Exoplanets and the Earth”, (Kyoto,
Japan, Mar. 1-4, 2015).
Maehara, H., Shibayama, T., Notsu, Y., Notsu, S., Honda, S., Nogami, D.,
Shibata, K.: 2015, Statistical properties of superflares on solar-typestars based on the Kepler 1-min cadence data, IAU Symp. 320: Solarand Stelar Flares and Thire Effects on Planets, (Honolulu, HI, USA,
Aug. 3-14, 2015).
Makise, K., Terai, H., Uzawa, Y.: 2015, NbN/AlN/NbN/TiN tunnel
junctions on Si (100) substrate for superconducting devices, 12th
European Conference on Applied Superconductivity (EUCAS2015),(Lyon, France, Sep. 6-10, 2015).
Makise, K., Terai, H., Uzawa, Y.: 2015, Growth of (100)-oriented
NbN thin films on Silicon substrate using TiN buffer layer, 15th
Int. Superconductive Electronics Conf. 2015 (ISEC2015), (Nagoya,Japan, Jul. 6-9, 2015).
Marchio, M., Cella, G.: 2015, Bayesian approach to the locking problem
for high finesse suspended optical cavities, GWADW2015, (Alaska,
USA, May. 17-22, 2015).
Marchio, M., Tatsumi, D., Flaminio, R.: 2015, Mirror absorption bench

setup and commissioning, KAGRA F2F Meeting, (Toyama, Japan,
Aug. 25-28, 2015).
Matsuda, Y.: 2015, ALMA 860um continuum observations of 100kpcscale Ly-alpha Blobs at z =3.1, East Asian ALMA Science Workshop
2015, (Osaka, Japan, Dec. 8-11, 2015).
Matsuda, Y.: 2015, Lyman-alpha blobs, MIAPP 2015 Workshop,(Garching, Germany, Jul. 27-Aug. 21, 2015).
Matsumoto, K., Ikeda, H.: 2016, Inhomogeneous Two-Layer Internal
Structure and Moments of Inertia of Phobos, 47th Lunar andPlanetary Sci. Conf., (The Woodlands, TX, USA, Mar. 21-25, 2016).
Matsumoto, K., Yamada, R., Kikuchi, F., Kamata, S., Ishihara, Y.,
Iwata, T., Hanada, H., Sasaki, S.: 2015, Internal Structure of theMoon Inferred from Apollo Seismic Data and Selenodetic Data fromGRAIL and LLR, 2nd IAPS Scientific Assembly, (Kazan, Russia,
Jun. 1-4, 2015).
Matsumoto, K., Yamada, R., Kikuchi, F., Kamata, S., Ishihara, Y.,
Iwata, T., Hanada, H., Sasaki, S.: 2015, On low-velocity zone at thebottom of the lunar mantle, Japan Geoscience Union Meeting 2015,(Chiba, Japan, May 24-28, 2015).
Matsumoto, N.: 2015, Fringe check observations of SiO maser sources
toward the Galactic center and antennanodding mode with KaVA, 8thEast Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Matsumoto, N.: 2015, VLBI imaging of 44 GHz methanol maser with
KaVA, High Mass Star Formation Workshop, (Tokyo, Japan, Jul. 22,2015).
Matsumoto, N.: 2016, (Lecture) Star forming region: VLBI observation,
NARIT-UST-GUAS Radio Astronomy Winter School 2016, (Chiang
Mai, Thailand, Feb.15-19, 2016).
Matsumoto, N.: 2016, KaVA PET activity, The 10th NARIT-KaVA Joint
Science WG meeting, (Krabi, Thailand, Feb. 22-24, 2016).
Matsumoto, N.: 2016, KaVA SFR science sub-WG: JVN follow-up
observations for G10.32-0.26 and G18.34-1.78, The 10th NARITKaVA Joint Science WG meeting, (Krabi, Thailand, Feb. 22-24, 2016).
Matsumoto, Y., Kokubo, E.: 2015, Formation of Close-in Super-Earths
by Giant Impacts: Effects of Initial Eccentricities and Inclinations ofProtoplanets, Extreme Solar Systems III, (Waikoloa, HI, USA, Nov.
29-Dec. 4, 2015).
Matsumoto, Y., Kokubo, E.: 2015, The eccentricities and inclinationsof planets formed through in situ accretion of protoplanets, 3rd DTA
Symposium: The Origins of Planetary Systems: From the Current
View to New Horizons, (Tokyo, Japan, Jun. 1-4, 2015).
Matsumoto, Y., Kokubo, E.: 2016, In Situ Accretion of Close-in
Super-Earths: Effects of Initial Eccentricities and Inclination ofProtoplanets, Exoplanets and Disks: Their Formation and Diversity
III, (Ishigaki, Japan, Feb. 21-24, 2016).
Matsuo, H.: 2015, Terahertz Interferometry with Milli-Arcsecond
Angular Resolution, Bringing Far Infrared Interferometry Into Vision,(London, UK, Dec. 15-17, 2015).
Matsuo, H., Ezawa, H., Kojima, T., Kawamura, Y., Sakurai, D.: 2015,
Readout electronics for THz photon counter, The 16th Workshop
on Submm Wave Receiver Technologies in Eastern Asia, (Nanjing,
China, Nov. 22-25, 2015).
Matsuoka, Y.: 2015, Search for z > 6 quasars, Understanding Evolutionof Quasars: Collaboration between Theoretical Models and Initial
HSC Survey, (Kagoshima, Japan, Dec. 1-3, 2015).
Matsuoka, Y.: 2015, AGN observations in the coming PFS-SSP survey,

XIII Publications, Presentations

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PFS-SSP galaxy survey workshop, (Kashiwa, Japan, Nov. 13, 2015).
Matsuoka, Y.: 2015, Search for distant (z > 6) quasars with SWIMS +Subaru/HSC, TAO/SWIMS Sceince Workshop 2015, (Mitaka, Japan,
Sep. 17-18, 2015).
Matsuoka, Y.: 2015, AGN observations with Subaru/PFS, Subaru Prime
Focus Spectrograph science workshop, (Mitaka, Japan, Jul. 9, 2015).
Matsuoka, Y.: 2015, HSC high-z quasar survey project, Subaru/HSC SSP
survey collaboration meeting, (Princeton, USA, Jul. 27-29, 2015).
Matsuoka, Y.: 2016, Subaru high-z exploration of low-luminosity quasars,
Subaru Users Meeting FY2015, (Atami, Japan, Jan. 19-21, 2016).
Matsuzawa, A.: , Optical Seeing Properties on the Pointing Verification
for ALMA Antenna, NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Mendillo, C. B., Brown, J., Martel, J., Howe, G. A., Hewasawam, K.,
Finn, S. C., Cook, T. A., Chakrabarti, S., Douglas, E. S., Mawet,D., Guyon, O., Singh, G., Lozi, J., Cahoy, K. L., Marinan, A. D.:
2015, The low-order wavefront sensor for the PICTURE-C mission,
SPIE Optics + Photonics, (San Diego, CA, USA, Aug. 9-13, 2015).
Michiyama, T.: 2015, Star Forming Molecular Gas in Merging Galaxies~ASTE observation~, East Asian ALMA Science Workshop 2015,(Osaka, Japan, Dec. 8-11, 2015).
Minamidani, T.: 2015, NRO Future Development, NRO-ALMA Science/
Development Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Miura, R.: 2015, High Velocity Compact Clouds in Nearby Young
Starburst Galaxy NGC 5253, East Asian ALMA Science Workshop
2015, (Osaka, Japan, Dec. 8-11, 2015).
Miyamoto, Y., Nakai, N., Seta, M., Salak, D., Nagai, M., Ishii, S.,
Yamauchi, A.: 2015, Hot gas in the center of the Seyfert galaxy NGC
3079, IAU XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14,2015).
Miyoshi, M.: 2015, Caravan-submm and a mm/sub-mm VLBI network
in East Asia, NRO-ALMA Science/Development Workshop 2015,(Nagano, Japan, Jul. 28-30, 2015).
Momose, M.: 2015, Long Baseline Observations with ALMA~Impact
by the image of HL Tau~, ALMA/45m/ASTE/Mopra Users Meeting
2015, (Tokyo, Japan, Oct. 20-22, 2015).
Momose, M. 2015, Udenkon report, ALMA/45m/ASTE/Mopra Users
Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Momose, M.: 2015, Follow-up studies related to the high-resolution
imaging of HL Tau, East Asian ALMA Science Workshop 2015,(Osaka, Japan, Dec. 8-11, 2015).
Momose, M.: 2016, Observations of Protoplanetary disks with ALMA,
Exoplanets and Disks: Their Formation and Diversity III, (Ishigaki,
Japan, Feb. 21-24, 2016).
Morokuma, K.: 2015, Search for molecular gas in XUV disk of M83,
ALMA/45m/ASTE/Mopra Users Meeting 2015, (Tokyo, Japan, Oct.
20-22, 2015).
Morokuma, K.: 2015, Tight anti-correlation between Dn4000 andmolecular gas mass fraction of galaxies, NRO-ALMA Science/
Development Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Morokuma-Matsui, K., Baba, J., Sorai, K., Kuno, N.: 2015, Tight anticorrelation between molecular gas fraction and 4000 Å break strength,
Gas, Dust, and Star-Formation in Galaxies from the Local to Far
Universe, (Plantanias-Chania, Crete, Greece, Apr. 25-29, 2015).
Morokuma-Matsui, K., Koda, J., Takekoshi, T., Saito, M., Nakanishi,
H., Boissier, S., Madore, B. F., Boselli, A., Gil de Paz, A., Thilker,

192

XIII Publications, Presentations

D., Yagi, M., Sorai, K., Kuno, N.: 2016, Search for molecular gas
in XUV disk of M83, IAU Symp. 321: Fornation and evolution ofgalaxy outskirts, (Toledo, Spain, Mar. 14-18, 2016).
Morokuma-Matsui, K.: 2015, Redshift evolution of gas fraction ofgalaxies in 0<z<2, East Asian ALMA Science Workshop 2015,(Osaka, Japan, Dec. 8-11, 2015).
Motogi, K.: 2015, Multi-scale view of the face-on accretion system
around G353.273+0.641, High Mass Star Formation Workshop,(Tokyo, Japan, Jul. 22, 2015).
Motte, F., Bontemps, S., Nguyen-Luong, Q.: 2015, HOBYS and
W43, two more steps towards a Galaxy-wide understanding of starformation, IAU XXIX General Assembly, (Honolulu, HI, USA, Aug.
3-14, 2015).
Muller, E.: 2015, Complete survey of the Galactic fourth quadrant in 4
lines, ALMA/45m/ASTE/Mopra Users Meeting 2015, (Tokyo, Japan,
Oct. 20-22, 2015).
Muraki, Y., et al. including Watanabe, K.: 2015, Simultaneous
Observation of Solar Neutrons from the ISS and High Mountain
Observatories in association with a flare on July 8, 34th International
Cosmic Ray Conference, (The Hague, Jul. 30-Aug. 6, 2015).
Nagai, H.: 2015, Long-term Radio and Gamma-ray Properties of 3C84, 5th Workshop on Compact Steep Spectrum and GHz-Peaked
Spectrum Radio Sources, (Rimini, Italy, May 27-29, 2015).
Nagai, H.: 2015, Millimeter Spectrum of Blazars and Its Connection
with High Energy Emission, East Asian ALMA Science Workshop
2015, (Osaka, Japan, Dec. 8-11, 2015).
Nagai, H.: 2015, ALMA Polarization Commissioning and Implication for
Future Projects (II), NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Nagasawa, R., Otsubo, T., Sekido, M., Hanada, H.: 2015, Softwaredevelopment for precise LLR data analysis and initial results ofparameter estimation for lunar motion, Japan Geoscience Union
Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Nakajima, T., Kato, C., Ito, M., Akiyama, N., Fujii, Y., Yamamoto,H., Mizuno, A., Kojima, T., Fujii, Y., Noguchi, T., Asayama,S., Kozuki, Y., Ogawa, H., Sakai, T.: 2015, Development of theSeries Junction Superconducting Device in 100 and 200 GHz Band,
ALMA/45 m/ASTE/Mopra Users Meeting 2015, (Tokyo, Japan, Oct.
20-22, 2015).
Nakamura, F.: 2015, ALMA Observations toward the nearest clusterforming region, East Asian ALMA Science Workshop 2015, (Osaka,
Japan, Dec. 8-11, 2015).
Nakamura, F.: 2015, Cluster Formation Triggered by Filament
Collisions in Serpens South, IAU Symp. 315, (Honolulu, HI, USA,
Aug. 3-14, 2015).
Nakamura, F.: 2015, Stellar Feedback in Clustered Star Formation,
6th Zermatt ISM meeting Conditions and Impact of Star Formation:
From Lab to Space, (Zermatt, Switherland, Sep. 7-11, 2015).
Nakamura, F.: 2016, ALMA View of Nearest Cluster-forming Region,
Rho Ophiuchus Cloud, Astronomy at Taj, (India, Feb. 15-19).
Nakamura, F., Kameno, S., Dobashi, K., Shimoikura, T., Taniguchi, K.:
2015, CCS Zeeman Observations toward TMC-1, Star Formation
2015: From Clouds to Cores, (Mitaka, Japan, June 25-27, 2015).
Nakanishi, K., Nagai, H.: 2015, ALMA Polarization Commissioning
and Implication for Future Projects (I) & (II), NRO-ALMA Science/
Development Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).

Nakanishi, K., Sorai, K., Nakai, N., Kuno, N., Matsubayashi, K., Sugai,
H., Takano, S., Kohno, K., Nakajima, T.: 2015, Millimeter/Submillimeter Hydrogen Recombination Line in the Center of NGC 253,
East Asian ALMA Science Workshop 2015, (Osaka, Japan, Dec. 8-11,2015).
Nakanishi, K.: 2015, ALMA Archive, ALMA/45 m/ASTE/Mopra Users
Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Nakanishi, K.: 2015, ALMA Polarization Commissioning and Implication
for Future Projects (I), NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Namiki, N., Enya, K., Kobayashi, M., Kimura, J., Araki, H., Noda, H.,
Kashima, S., Utsunomiya, S., Ishibashi K., Oshigami, S., Kobayashi,S., Fujii, M., Hussmann, H., Lingenauber, Oberst, K.: 2015,
Development of JUICE/Ganymede Laser Altimeter (GALA), Japan
Geoscience Union Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Narita, N.: 2015, Future Missions of Transit Surveys and Characterizations,
3rd DTA Symposium: The Origins of Planetary Systems: From theCurrent View to New Horizons, (Tokyo, Japan, Jun. 1-4, 2015).
Narita, N.: 2015, Exoplanet ISDT Activity Report: TMT’s Prospects for
Exoplanets, TMT Science Forum 2015, (Washington D.C., USA, Jun.
23-25, 2015).
Narita, N.: 2015, Possible Contribution of the Subaru telescope to TESS
follow-up, Suabru-Keck synergy workshop, (Sendai, Miyagi, Japan,
Sep. 1-2, 2015).
Narita, N.: 2015, Introduction of Japanese Facilities for K2 Follow-up
Observations and Latest Results, The first K2 Science Conference,(Santa Barbara, USA, Nov. 2-5, 2015).
Narita, N.: 2016, Possible Subaru-TESS Synergy Campaign, Subaru
Users Meeting FY2015, (Atami, Japan, Jan. 19-21, 2016).
Narita, N.: 2016, Toward detections of habitable terrestrial planets
around the Solar neighborhood, Symposium on Hierarchy and Holism
in Natural Sciences, (Mitaka, Tokyo, Japan, Feb. 5-6, 2016).
Narita, N., Enomoto, T., Masaoka, S., Kusakabe, N.: 2016, Titania
may produce abiotic oxygen atmospheres on habitable exoplanets,
Extreme Solar Systems III, (Waikoloa, HI, USA, Nov. 29-Dec. 4, 2015).
Narukage, N., Shimojo, M., Sakao, T.: 2015, Evidence of Electron
Acceleration around the Reconnection X-point in a Solar Flare, 9thHinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Nemoto, S., Usuda-Sato, K., Matsuda, K., Sasaki, G., Nakagiri, M.,
Agata, H., Funayama, H., Kameya, O., Kinugasa, K., Toda, H.,
Yanagisawa, K., Baba, Y.: 2015, Historical Items Database of the
NAOJ Museum, Int. Symp. on the NAOJ Museum, (Tokyo, Japan,
Sep. 27-29, 2015).
Nguyen-Luong, Q., Motte, F., Nguyen, H., Schneider, N., Louvet, F.: ,COnnecting LOcal to GLObal star formation via MIni-starburst, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Nguyen-Luong, Q.: 2015, Searching for the densest massive dense
cores, East Asian ALMA Science Workshop 2015, (Osaka, Japan,
Dec. 8-11, 2015).
Nguyen-Luong, Q.: 2015, Connecting local to global star formation via
ministarburst, NRO-ALMA Science/Development Workshop 2015,(Nagano, Japan, Jul. 28-30, 2015).
Nishikawa, J., Oya, M., Murakami, N., Tamura, M., Kurokawa,T., Tanaka, K.: 2015, Imperfect Pre-coronagraph for contrast
enhancement with speckle area nulling control, In the spirit ofBernard Lyot, (Montréal, USA, Jun. 22-26, 2015).

Nishikawa, J., Oya, M., Murakami, N., Tamura, M., Kurokawa, T.,
Tanaka, K.: 2015, Imperfect Pre-coronagraph for additional contrast,
Pathways 2015: Pathways Towards Habitable Planets, (Bern,
Schweizerische, Jul. 13-17, 2015).
Nishikawa, J., Oya, M., Murakami, N., Tamura, M., Kurokawa, T.:2015, Contrast enhancement with pre-coronagraph and dark-hole, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Nishimura, A., Umemoto, T., Minamidani, T., Kuno, N., Tosaki, T.,
Fujita, S., Matsuo, M., Tsuda, Y., Ohashi, S.: 2015, Nobeyama 45 m
CO Galactic Plane Survey: Filament properties and star formation in
M17, IAU XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14,2015).
Nishioka, M., Kinugasa, K., Mikoshiba, H., Miyazawa, K., Shinohara,N., Ide, H., Saito, M.: 2015, Making Brochure and Original Goodsin the NAOJ Nobeyama Campus, Int. Symp. on the NAOJ Museum,(Tokyo, Japan, Sep. 27-29, 2015).
Noda, H., Mizuno, T., Kunimori, H., Takeuchi, H., Senshu, H., Ogawa,N., Saiki, T., Yamaguchi, T., Pollard, A., Moore, C., Namiki, N.,
Tsuda, Y.: 2016, Establishment of laser link between ground stationand Hayabusa2 LIDAR, 47th Lunar and Planetary Sci. Conf., (The
Woodlands, TX, USA, Mar. 21-25, 2016).
Notsu, Y., Honda, S., Maehara, H., Notsu, S., Shibayama, T., Nogami,D., Shibata, K.: 2015, High dispersion spectroscopy of solar-type
superflare stars with Subaru/HDS, IAU Symp. 320: Solar and Stelar
Flares and Thire Effects on Planets, (Honolulu, HI, USA, Aug. 3-14,2015).
Nozawa, T.: 2015, Dust Production Factories in the Early Unvierse,
Frascati Workshop 2015: Multifrequency Behavior of High Energy
Cosmic Sources, (Palermo, Italy, May 25-31, 2015).
Nozawa, T.: 2015, On the Reddening Law Observed for Type Ia
Supernovae, Cosmic Dust VIII, (Tokyo, Japan, Aug. 17-21, 2015).
Ohashi, N.: 2016, ALMA Observations of Formation and Evolutionof Disks around Protostars, Astrochemistry with ALMA cycle 4,(Bordeaux, France, Jan. 12-13, 2016).
Ohashi, N.: 2016, Compact SO emission around protostars: Possible
rings due to accretion shocks?, From clouds to protoplanetary disks:
the astrochemical link, (Belrin, German, Oct. 5-8, 2015).
Ohsuga, K.: 2015, Radiation magnetohydrodynamics simulations ofaccretion flows and outflows around black holes, "Quarks to Universein Computational Science", (Nara, Japan, Nov. 4-8, 2015).
Ohsuga, K.: 2015, Radiation-magnetohydrodynamics simulations ofblack hole accretion flows and outflows, Prospects, challenges andevolution of AGN modeling in the Astro-H Era, (Tokyo, Japan, Oct.
21-22, 2015).
Ohsuga, K.: 2015, Theory of black hole accretion flows and outflows,
Max’s 4 questions in X-ray astronomy to be addressed with
ASTRO-H, (Tokyo, Japan, Jul. 31, 2015).
Ohsuga, K.: 2015, Radiation-MHD simulations of black-hole accretion
flows and outflows, Black Hole Accretion and AGN Feedback,(Shanghai, China, Jun. 1-5, 2015).
Oka, T.: , The Galactic Center - Recent Progress and Future Perspectives -,NRO-ALMA Science/Development Workshop 2015, (Nagano, Japan,
Jul. 28-30, 2015).
Okuda, T.: 2015, Long term plan for ASTE, ALMA/45m/ASTE/Mopra
Users Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Onishi, K.: 2015, Black-Hole Mass Estimation using Molecular Gas

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Dynamics, East Asian ALMA Science Workshop 2015, (Osaka,
Japan, Dec. 8-11, 2015).
Onishi, T.: 2015, High-mass star formation in the LMC as seen by
ALMA, East Asian ALMA Science Workshop 2015, (Osaka, Japan,
Dec. 8-11, 2015).
Onishi, T.: 2015, Star Formation in the Large Magellanic Cloud: Tracing
an Evolution of Giant Molecular Clouds, NRO-ALMA Science/
Development Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Onodera, M., Carollo, C. M., Lilly, S., Tacchella, S., Renzini,
A., Arimoto, N., Capak, P., Scoville, N., Daddi, E., Tatehora, S.,
Zamorani, G.: 2016, ISM excitation and metallicity of star-forming
galaxies at z ~ 3.3 from near-IR spectroscopy, From stellar-evolution
to galaxy formation, (Yatsugatake, Japan, Mar. 7-9, 2016).
Oshigami, S., Watanabe, S., Yamaguchi, Y., Yamaji, A., Kobayashi,T., Kumamoto, A., Ishiyama, K., Ono, T.: 2015, Mare volcanism:
Reinterpretation based on Kaguya Lunar Radar Sounder data, JSEDI
Symposium 2015, (Tokyo, Japan, Sep. 24-26, 2015).
Oshima, A.: 2015, An estimation of the diffusion coefficient of galactic
cosmic rays in the heliosphere near the Earth, 34th International
Cosmic Ray Conference, (The Hague, Jul. 30-Aug. 6, 2015).
Oshino, S., Matsumoto, Y., Kokubo, E.: 2015, Terrestrial Planet
Formation around Low-Mass Stars: Effect of the Mass of Central
Stars, American Astronomical Society, ESS meeting #3, (Hawaii,
USA, Nov. 29-Dec. 4, 2015).
Oshino, S., Matsumoto, Y., Kokubo, E.: 2016, Terrestrial Planet
Formation around Low-Mass Stars: Effect of the Mass of Central
Stars, Exoplanets and Disks: Their Formation and Diversity III,
(Ishigaki, Japan, Feb. 21-24, 2016).
Otsuji, K., Sakurai, T., Kuzanyan, K., Hagino, M.: 2015, Current
Helicity and Twist of Solar Magnetic Fields from Hinode/SOT SP
and Ground Based Telescopes Data, 9th Hinode Science Meeting,(Belfast, UK, Sep. 14-17, 2015).
Oya, M., Nishikawa, J., Murakami, N., Tamura, M., Kurokawa, T.,
Tanaka, K.: 2015, A new dark-hole control of speckle area nulling(SAN) method, Pathways 2015: Pathways Towards Habitable Planets,(Bern, Schweizerische, Jul. 13-17, 2015).
Oyama, T.: 2015, A progress report on the development and performanceof OCTAVE-DAS and Correlator System, 8th East Asia VLBI
Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Oyama, T.: 2016, Results of test broad band vlbi observations with
VERA+Yonsei21m using OCTAD and OCTADISK2, The 10th
NARIT-KaVA Joint Science WG meeting, (Krabi, Thailand, Feb. 2224, 2016).
Sagawa, H.: 2015, New frontier of the Solar system observations with
ALMA, ALMA/45m/ASTE/Mopra Users Meeting 2015, (Tokyo,
Japan, Oct. 20-22, 2015).
Saito, M.: 2015, Status and Plans for Nobeyama 45m, NRO-ALMA
Science/Development Workshop 2015, (Nagano, Japan, Jul. 28-30,
2015).
Saito, M.: 2015, Performance of Atacama Compact Array Antennas for
ALMA, 36th ESA Antenna Workshop, (Noordwijk, the Netherlands,
Oct. 6-9, 2015).
Saito, M.: 2015, Future (Sub)Millimeter Development in Japan, U.S.
Radio/Millimeter/Submillimeter Science Futures in the 2020s,(Chicago, USA, Dec.15-17, 2015).
Saito, T., Iono, D., Ueda, J., Nakanishi, K., Imanishi, M., Hagiwara,

194

XIII Publications, Presentations

Y., Yun, M. S., Kaneko, H., Komugi, S., Espada, D., Sugai, H.,
Motohara, K., Lee, M., Kawabe, R., Yamashita, T.: 2015, Molecular
Gas Excitation and Chemistry in Nearby LIRGs with ALMA, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Sakai, N.: 2015, Test of the density-wave theory based on VLBI
astrometry results, 8th East Asia VLBI Workshop, (Sapporo, Japan,
Jul. 8-10, 2015).
Sakai, N.: 2016, Progress report from KaVA Galactic Astrometry subWG, The 10th NARIT-KaVA Joint Science WG meeting, (Krabi,
Thailand, Feb. 22-24, 2016).
Sakai, N.: 2016, Test of the density-wave theory using VLBI astrometry
results, The 10th NARIT-KaVA Joint Science WG meeting, (Krabi,
Thailand, Feb. 22-24, 2016).
Sakai, N.: 2016, Galactic astrometry science, Australia-Japan School on
Low Frequency Astrometry in the SKA Era, (Kagoshima, Japan, Mar.
28-31, 2016).
Sanhueza, P.: 2015, A Massive, Prestellar Clump hosting no High-Mass
Prestellar Cores, East Asian ALMA Science Workshop 2015, (Osaka,
Japan, Dec. 8-11, 2015).
Sasai, Y., et al. including Watanabe, K.: 2015, Upgrade of a dataacquisition system for SciBar Cosmic Ray Telescope (SciCRT) at Mt.
Sierra Negra, Mexico, 34th International Cosmic Ray Conference,(The Hague, Jul. 30-Aug. 6, 2015).
Sasaki, H.: 2016, Collective neutrino flavor oscillations and application
to supernova nucleosynthesis, 13th Russbach School on Nuclear
Astrophysics, (Russbach, Austria, Mar. 6-12, 2016).
Sekimoto, Y.: 2015, Broadband and wide-field focal plane with MKID,
The 16th Workshop on Submm Wave Receiver Technologies in
Eastern Asia, (Nanjing, China, Nov. 22-25, 2015).
Sekimoto, Y.: 2015, MKID focal plan array for LiteBIRD, B-mode fromspace, (Chiba, Japan, Dec. 10-16, 2015).
Seko, A., Ohta, K., Hatsukade, B., Yabe, K.: 2015, Properties ofInterstellar Medium in Star-Forming Galaxies at z~1.4 revealed with
ALMA, IAU XXIX General Assembly, (Honolulu, HI, USA, Aug.
3-14, 2015).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G. J.: 2015, Relative
Contributions of the r-Process in Supernova and Neutron Star Merger,
The 13th International Symposium on Origin of Matter and Evolutionof Galaxies (OMEG2015), (Beijing, China, Jun. 24-27, 2015).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G. J.: 2015, The role offission in the r-process in dynamical ejecta from neutron star mergers,
Workshop on Microphysics In Computational Relativistic Astrophysics(MICRA2015), (Stockholm, Sweden, Aug. 17-21, 2015).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G. J.: 2015, Rolesof fission in the r-process, The 5th International Workshop on
Compound-Nuclear Reactions and Related Topics (CNR*15), (Tokyo,
Japan, Oct. 19-23, 2015).
Shibata, Y., Cheung, S. L., Pun, J., So, C., Walker, C., Agata, H.:
2015, Early Performance and Results from the Globe at Night - Sky
Brightness Monitoring Network, IAU XXIX General Assembly,(Honolulu, HI, USA, Aug. 3-14, 2015).
Shimojo, M., ALMA Solar Development Team: 2015, Solar Observations
with ALMA, 3rd Asia-Pacific Solar Physics Meeting (APSPM 2015),(Soule, South Korea, Nov. 3-6, 2015).
Shimojo, M., ALMA Solar Development Team: 2015, Solar Observations
with ALMA, Hinode 9, (Belfast, UK, Sep. 14-17, 2015).

Shimojo, M., ALMA Solar Development Team: 2016, Performance ofSolar mm-wave Observations with ALMA, ALMA-IRIS-DKIST
Workshop 'The Sun's Chromosphere in the Era of ALMA, IRIS, and
DKIST', (Boulder, CO, USA, Mar. 15-18, 2015).
Shimojo, M., Bastian, T., White, S., Iwai, K., Wedemeyer, S., Hudson,
H., Brajsa, R., Barta, M., Hales, A., Hirota, A. Remijan, A., Solar
Development Team of EA/NA/EU-ARC: 2015, Solar Observations
with ALMA, 9th Hinode Science Meeting, (Belfast, UK, Sep. 14-17,2015).
Shimojo, M., Iwai, K., Asai, A., Nozawa, S., Minamidani, T., Saito,
M.: 2015, Variation of Solar Microwave Spectrum in the Last Half
Century, 3rd Asia-Pacific Solar Physics Meeting (APSPM 2015),(Soule, South Korea, Nov. 3-6, 2015).
Shimojo, M., Iwai, K., Asai, A., Nozawa, S., Minamidani, T., Saito,
M.: 2015, Variation of Solar Microwave Spectrum in the Last Half
Century, 9th Hinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Shino, N.: 2015, Investigating methanol maser observation of massive
star forming region IRAS18144-1732 and IRAS20198+3716, 8thEast Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Shino, N.: 2016, Investigating methanol maser observation of massive
star forming region IRAS18144-1723, The 10th NARIT-KaVA Joint
Science WG meeting, (Krabi, Thailand, Feb. 22-24, 2016).
Shirahata, M., Matsuura, S., Tsumura, K., Arai, T., Sano, K., Ohnishi Y.,
Matsumoto, T., Bock, J., Zemcov, M., Korngut, P., Lanz, A., Hristov,V., Battle, J., Wada, T., Cooray, A., Smidt, J.: 2015, Developmentof the telescope and imagers for the Cosmic Infrared Background
ExpeRiment 2, The Near-IR Background II: From reionization to thepresent epoch, (Munich, Germany, Jun. 1-3, 2015).
Shirasaki, M.: 2015, Search for Gamma-ray from Luminous Red
Galaxies, ICM Physics and Modeling, (Garching, Germany, June 1517, 2015).
Shirasaki, M.: 2015, Probing cosmology with weak lensing selectedclusters, Theoretical and Observational Progress on Large-scale
Structure of the Universe, (Garching, Germany, Jul. 20-24, 2015).
Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto, Y.: 2015, Propertiesof galaxies around the most massive SMBHs, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Shirasaki, Y., Zapart, C., Ohishi, M., Mizumoto, Y., Kawasaki, W.,
Kobayashi., T., Kosugi, G., Kawaguchi, T., Eguchi, S., Ishihara, Y.,
Yamada, H., Hiyama, T., Nakamoto, H.: 2015, Current status of JVO
portal, ADASS XXV, (Sydney, Australia, Oct. 25-29, 2015).
Shoda, A.: 2015, Torsion-bar Antenna Experiment, GWADW2015,(Alaska, USA, May. 17-22, 2015).
Shimojo, M.: 2015, Solar observations with ALMA, NRO-ALMA Science/
Development Workshop 2015, (Nagano, Japan, Jul. 28-30, 2015).
Sirbu, D., Thomas, S. J., Belikov, R., Lozi, J., Bendek, E., Pluzhnik,
E., Lynch, D. H., Hix, T., Zell, P., Schneider, G., Guyon, O.: 2015,
EXCEDE technology development IV: demonstration of polychromatic
contrast in vacuum at 1.2 λ/D, SPIE Optics + Photonics, (San Diego,
CA, USA, Aug. 9-13, 2015).
Soma, M.: 2015, When and where were the observations made for thecelestial map in the Kitora Tumulus?, International Symposium on
Historical Astronomy, (Seoul, Korea, Sept. 23-24, 2015).
Sotani, H.: 2015, Mass formula for low-mass neutron stars and its
application, 5th International Symposium on Nuclear Symmetry

Energy (NuSYM15), (Krakow, Poland, Jun. 29-Jul. 2, 2015).
Sotani, H.: 2015, Nuclear equation of state and crustal torsional
oscillations, Compact Stars and Black Holes, (Tuebingen, Germany,
Jul. 7-9, 2015).
Sotani, H.: 2015, Prospect for Observational Discriminant of theGravitational Theories, Fourteenth Marcel Grossmann Meeting(MG14), (Rome, Italy, Jul. 12-18, 2015).
Sotani, H.: 2015, Identifications of Quasi-Periodic Oscillations Observedin Soft-Gamma Repeaters with Crustal Torsional Oscillations,
Fourteenth Marcel Grossmann Meeting (MG14), (Rome, Italy, Jul.
12-18, 2015).
Srikanth, S., Gonzalez, A.: 2015, ALMA band 2 optics: preliminary
results, 1st URSI Atlantic Radio Science Conference, (Gran Canaria,
Spain, May 18-25, 2015).
Suematsu, Y.: 2015, Fine-scale Structure and Motion of Penumbral
Filaments Revealed with Hinode G-band and Ca II H Filtergrams, 9thHinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Suematsu, Y.: 2015, The SOLAR-C Mission, AGU Fall meeting 2015,(San Francisco, CA, USA, Dec. 14-18, 2015).
Suematsu, Y., Solar-C Working Group: 2015, The SOLAR-C
Mission: Science Objectives and Current Status, Coimbra Solar
Physics Meeting: Ground-based Solar Observations in the Space
Instrumentation Era, (Coimbra, Portugal, Oct. 5-9, 2015).
Sugimoto, K.: 2015, CASA update, ALMA/45 m/ASTE/Mopra Users
Meeting 2015, (Tokyo, Japan, Oct. 20-22, 2015).
Tagawa, H., Umemura, M., Gouda, N.: 2015, Accretion versus merger
in the early growth of massive black holes, “Quarks to Universein Computational Science”, (Nara, Japan, Nov. 4-8, 2015).
Tagawa, H., Umemura, M., Gouda, N.: 2015, Early cosmic merger ofmultiple black holes, First stars, galaxies, and black holes: Now andThen, (Groningen, Netherland, June 15-19, 2015).
Takahashi, H. R.: 2016, 3D-reconection of supercritical accretion disks
in relativistic radiation magnetohydrodynamics, 2016 US-Japan
Workshop on Magnetic Reconnection (MR2016), (Napa, CA, USA,
Mar. 7-11, 2016).
Takahashi, H. R., Ohsuga, K., Kawashima T., Sekiguchi, Y.: 2015,
Relativistic Radiation Magnetohydrodynamic Simulations ofBlack Hole Accretion Disks and Outflows, “Quarks to Universein Computational Science”, (Nara, Japan, Nov. 4-8, 2015).
Takahashi, H. R., Ohsuga, K., Kawashima T., Sekiguchi, Y.: 2015,
Numerical Study of Super Critical Accretion Disks, Black Hole
Accretion and AGN Feedback, (Shanghai, China, Jun. 1-5, 2015).
Takakuwa, S., Yen, H.-W., Ohashi, N., Chou, T.-L., Aso, Y., Saigo, K.,
Saito, M., Machida, M. N., Tomida, K., Aikawa, Y., Tomisaka, K.,
Koyamatsu, S., Takahashi, S. Z.: 2015, SMA and ALMA Studies ofProtoplanetary-Disk Formation around Low-mass Protostars, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Takata, T.: 2016, Status of database/Data release plan, HSC Collaboration
Meeting, (Taipei, Taiwan, Jan. 13-15, 2016).
Takato, N.: 2015, PFS activities at Subaru in 2015, 7th PFS collaboration
meeting, (Marseille, France, Dec. 14-18, 2015).
Takeda, T., Kokubo, E., Agata, H., Kato, T., Nakayama, H., Narasaki,Y., Fukushi, H.: 2015, Four Dimensional Digital Universe Project,Int. Symp. on the NAOJ Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Takeda, Y.: 2016, Activities and related properties of solar-type stars,

XIII Publications, Presentations

195

Superflare Workshop 2016 “Superflares on Solar-type Stars and Solar
Flares, and Their Impacts on Exoplanets and the Earth”, (Kyoto,
Japan, Mar. 1-4, 2015).
Takeda, Y.: 2016, Fundamental parameters of red giants in collaboration
with asteroseismology and high-dispersion spectroscopy, Workshop
on “Galactic archaeology - Asteroseismology”, (Mitaka, Tokyo,
Japan, Mar. 22, 2016).
Takekoshi, T.: 2015, Physical Properties of the 1.1 mm selected Giant
Molecular Clouds in the Small Magellanic Cloud, IAU XXIX
General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Takiwaki, T.: 2015, Study of Core-Collapse Supernova Explosions,
Comprehensive Studies of Neutron Stars, (Saitama, Japan, Nov. 24,2015).
Takiwaki, T.: 2015, Asymmetric ejecta in three dimensional simulations ofcore-collapse supernovae, Symposium on Supernovae and Supernova
Remnants (SNSNR2015), (Sagamihara, Japan, Nov. 9, 2015).
Takiwaki, T.: 2015, A new class of rotational explosion in core-collapse
supernovae, QUCS 2015, (Nara, Japan, Nov. 4-8, 2015).
Takiwaki, T.: 2015, Dependence of nuclear equation of state onsupernova explosion, International Numazu Workshop on Challengesof Modeling Supernovae with Nuclear Data, (Shizuoka, Japan, Sep.
1-4, 2015).
Takiwaki, T.: 2015, How supernova simulations are affected by input
physics, Workshop on Microphysics In Computational Relativistic
Astrophysics (MICRA2015), (Stockholm, Sweden, Aug. 17-21, 2015).
Takiwaki, T.: 2015, How equation of state affects explosions of corecollapse supernovae, Physics and Astronomy of Neutron Stars andSupernovae, (Tokyo, Japan, Jun. 21-22, 2015).
Takiwaki, T.: 2016, Gravitational wave signals from three dimensional
simulations of Core-Collapse Supernovae, 4th Annual Symposium of
the Innovative Area on Multi-messenger Study of Gravitational Wave
Sources, (Chiba, Japan, Feb. 18- 20, 2016).
Tamura, M.: 2015, Subaru Direct Imaging Survey of Wide-Orbit
Exoplanets and Solar-System-Scale Disks, IAU XXIX General
Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Tamura, M.: 2015, Development of Astrobiology with Exoplanet
Explorations, Japan Geoscience Union Meeting 2015, (Chiba, Japan,
May 24-28, 2015).
Tamura, M.: 2015, NINS Astrobiology Center: Development of
Astrobiology with Exoplanet Explorations, NAI/EC and Iternational
Partner In-person Meeting, (Chicago, USA, Jun. 19-20, 2015).
Tamura, M.: 2015, Subaru Observations of Exoplanets and Toward
TMT: A Role of the New Astrobiology Center at NINS, Astrobiology
Workshop, (Kiel, Germany, Dec. 9, 2015).
Tamura, M.: 2016, Workshop summary, Post-SEEDS Workshop,(Mitaka, Japan, Feb. 21, 2016).
Tamura, M.: 2016, Exoplanet exploration with IRSF/SIRIUS and future,
IRSF Workshop 2016, (Cape Town, South Africa, Mar. 3, 2016).
Tamura, M., SEEDS team: 2016, Five Years of SEEDS: Strategic
Exploration of Exoplanets and Disks with Subaru, Subaru Users
Meeting FY2015, (Atami, Japan, Jan. 19-21, 2016).
Tamura, M., SEEDS team: 2016, Five Years of the Subaru SEEDS
Direct Imaging Survey and Next Steps, Exoplanets and Disks: Their
Formation and Diversity III, (Ishigaki, Japan, Feb. 21-24, 2016).
Tamura, Y., Imai, H.: 2015, ITRF Coordinates of the NRO 45 m
Telescope, ALMA/45 m/ASTE/Mopra Users Meeting 2015, (Tokyo,

196

XIII Publications, Presentations

Japan, Oct. 20-22, 2015).
Tamura, Y.: 2016, Measuring the Atmospheric Effects with External
Data, Australia-Japan School on Low Frequency Astrometry in the
SKA Era, (Kagoshima, Japan, Mar. 28-31, 2016).
Tanaka, M.: 2015, Electromagnetic Emission from Compact Binary
Mergers, The 25th Workshop on General Relativity and Gravitationin Japan, (Kyoto, Japan, Dec. 7-11, 2015).
Tanaka, M.: 2015, Radiative Transfer Simulations in Compact Star
Mergers, Quarks to Universe in Computational Science, (Nara, Japan,
Nov. 4-8, 2015).
Tanaka, M.: 2015, Supernovae: Toward Multiwavelength Studies,
Paving the Way to Simultaneous Multi-Wavelength Astronomy,(Leiden, Netherlands, July 13-17, 2015).
Tanaka, M.: 2015, Radioactively-powered emission from compact
binary mergers, Gravitational Wave Physics and Astronomy
Workshop (GWPAW) 2015, (Osaka, Japan, June 17-20, 2015).
Tanaka, M.: 2015, Optical/infrared emission from neutron star mergers,
South American Supernovae (SAS) 2015, (Santiago, Chile, Apr. 2830, 2015).
Tanaka, M., Chiba, M., Komiyama, Y.: 2015, Discovery of new dwarf
galaxies around NGC4631 with Subaru/Hyper Suprime-Cam, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Tanaka, M.: 2015, HSC Website / Reports from the Photo-z, Low-z,
Archeology Working Groups, HSC Collaboration Meeting,(Princeton, NJ, USA, Jul. 27-19, 2015).
Tanaka, M.: 2015, Photometric Redshifts, 新学術領域「なぜ宇宙は加速するのか ? - 徹底的究明と将来への挑戦 -」発足シンポジウム ,(Tokyo, Japan, Sep. 20-21, 2015).
Tanaka, M.: 2015, Some thoughts on the PFS-SSP galaxy survey, PFSSSP galaxy survey workshop, (Kashiwa, Japan, Nov. 13, 2015).
Tanaka, M.: 2015, Strategic Surveys with Hyper Suprime-Cam andPrime-Focus Spectrograph, Workshop for ALMA Large Proposalof gAlactic Cold gAs (ALPACA) Survey, (NAOJ, Japan, Dec. 1-2,
2015).
Tanaka, M.: 2016, Photometry / Reports from the Photo-z and Low-z
Working Groups / HSC website, HSC Collaboration Meeting, (Taipei,
Taiwan, Jan. 13-15, 2016).
Tanaka, M.: 2016, The Missing Satellite Problem Outside of the Local
Group, IAU Symp. 321: Fornation and evolution of galaxy outskirts,(Toledo, Spain, Mar. 14-18, 2016).
Tanaka, Y., Yamada, Y., Kurokawa, T.: 2015, Distance measurement
using second harmonic signal component of two-photon absorption
photocurrent from Si-APD, CLEO 2015, (San Jose, CA, USA, May
10-15, 2015).
Tanikawa, K., Soma, M.: 2015, On the eclipse of 延烏郎 and 細烏女
in Samguk-Yusa, International Symposium on Historical Astronomy,(Seoul, Korea, Sept. 23-24, 2015).
Tatematsu, K.: 2015, Statistics from cycle 2, and APRC results for cycle
3, ALMA/45 m/ASTE/Mopra Users Meeting 2015, (Tokyo, Japan,
Oct. 20-22, 2015).
Tatematsu, K.: 2015, New capabilities and observing mode for cycle 4,
ALMA/45m/ASTE/Mopra Users Meeting 2015, (Tokyo, Japan, Oct.
20-22, 2015).
Tazaki, F.: 2015, M87 Image at 43 GHz with “Sparse Modeling”, 8thEast Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Terazono, J., Sakamoto, S., Yoshikawa, M., Wakabayashi, N., Watanabe,

J.: 2015, Japanese Lunar and Planetary Exploration Outreach 17 years’ history of “The Moon Station”, Int. Symp. on the NAOJ
Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Tokuda, K., Onishi, T., Saigo, K., Kawamura, A., Fukui, Y., Matsumoto,T., Inutsuka, S., Machida, M. N., Tomida, K., Tachihara, K.: 2015,
ALMA Observations of a High-density Core in Taurus: Dynamical
Gas Interaction at the Possible Site of a Multiple Star Formation, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Toriumi, S., Iida, Y., Kusano, K., Bamba, Y., Imada, S.: 2015,
Observation and Modeling of a Quadrupolar Flare-productive Active
Region, Flux Emergence Workshop 2015, (Boulder, CO, USA, Jun.
15-19, 2015).
Toriumi, S., Katsukawa, Y., Cheung, M. C. M.: 2015, Hinode, SDO and
IRIS observation and MHD modeling of light bridge structures, 9thHinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Toriumi, S., Katsukawa, Y, Cheung, M. C. M.: 2015, Light Bridge
Structures Formed in Emerging Active Regions, Flux Emergence
Workshop 2015, (Boulder, CO, USA, Jun. 15-19, 2015).
Toriumi, S., Katsukawa, Y, Cheung, M. C. M.: 2015, Hinode, SDO
and IRIS observation and MHD modeling of light bridge structures,
Hinode 9, (Belfast, UK, Sep. 14-17, 2015).
Toriumi, S.: 2015, Light Bridge Structure in a Developing Sunspot
Region, 5th International workshop on small scale solar magnetic
fields, (Bairisch Kölldorf, Austria, Apr. 21-24, 2015).
Toriumi, S.: 2015, Solar Active Regions: From Birth to Eruption, Japan
Geoscience Union Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Toriumi, S.: 2015, Emerging flux and active region evolution, Hinode 9(Solar-C meeting), (Belfast, UK, Sep. 18, 2015).
Tsujimoto, T.: 2015, Chemical footsteps of r-nuclides in satellite
galaxies of Local Group, In the footsteps of galaxies: Tracing theevolution of environmental effects, (Soverato, Italy, Sep. 7-11, 2015).
Ueda, J., Iono, D., Yun, M. S., Crocker, A. F., Narayanan, D., Komugi,
S., Espada, D., Hatsukade, B., Kaneko, H., Matsuda, Y., Tamura,Y., Wilner, D., Kawabe, R., Pan, H.-A.: 2015, Investigating nuclear
and extended molecular gas disks in the final stages of mergers, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Ueda, J., Iono, D., Yun, M. S., Crocker, A. F., Narayanan, D., Komugi,
S., Espada, D., Hatsukade, B., Kaneko, H., Matsuda, Y., Tamura,Y., Wilner, D., Kawabe, R., Pan, H.-A.: 2015, Investigating nuclear
and extended molecular gas disks in the final stages of mergers, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Umemoto. T.: 2015, NRO Galactic Plane Survey (FUGIN) Legacy
Project, ALMA/45m/ASTE/Mopra Users Meeting 2015, (Tokyo,
Japan, Oct. 20-22, 2015).
Umemoto. T.: 2015, Nobeyama 45 m CO Galactic Plane Survey:
Progress of 2014, NRO-ALMA Science/Development Workshop
2015, (Nagano, Japan, Jul. 28-30, 2015).
Usuda-Sato, K.: 2015, Introduction of the NAOJ Museum Plan, Int.
Symp. on the NAOJ Museum, (Tokyo, Japan, Sep. 27-29, 2015).
Usuda-Sato, K., Iizuka, R., Yamaoka, H., Agata, H., NameExoWorlds
Working Group Members: 2015, Inspiring People to Participate in the
NameExoWorlds Contest, IAU XXIX General Assembly, (Honolulu,
HI, USA, Aug. 3-14, 2015).
Uyama, T., Tamura, M., Hashimoto, J., Kuzuhara, M.: 2015, Search
for Exoplanets around Young Stellar Objects by Direct Imaging,
American Astronomical Society, ESS meeting #3, (Hawaii, USA,

Nov. 29-Dec. 4, 2015).
Uzawa, Y., Makise, K., Kojima, T., Saito, S., Kroug, M., Fujii,Y., Gonzalez, A., Kaneko, K., Terai, H., Wang, Z.: 2015,
Characterization of NbTiN Films for Superconducting Terahertz
Circuitry, 15th Int. Superconductive Electronics Conf. 2015
(ISEC2015), (Nagoya, Japan, Jul. 6-9, 2015).
Uzawa, Y., NAOJ receiver group, NICT remote sensing group: 2016,
Terahertz radio astronomy applications and activities at NICT, SpainJapan Joint workshop on Millimetre-wave and Terahertz, (Madrid,
Spain, Mar. 17-18, 2016).
Wakita, S., Matsumoto, Y., Oshino, S., Hasegawa, Y.: 2016,
Planetesimal Collisions as a Heating Event for Chondrule Formation,
47th Lunar and Planetary Sci. Conf., (The Woodlands, TX, USA,
Mar. 21-25, 2016).
Watanabe, J.-i., Nakagiri, M.: 2015, Candidates of World Heritage Sites
of Astronomy in Japan, IAU XXIX General Assembly, (Honolulu,
HI, USA, Aug. 3-14, 2015).
Watanabe, J.-i., Sasaki, G., Nakagiri, M., Ohshima, N.: 2015,
Discovery of Japan's Oldest Photographic Plates of a Starfield, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Watanabe, K., Masuda, S.: 2015, A Statistical Approach to a Better
Understanding of the Conditions that Produce White-Light
Enhancements in Solar Flares, 9th Hinode Science Meeting, (Belfast,
UK, Sep. 14-17, 2015).
Watanabe, K., Masuda, S., Kitagawa, J.: 2015, Characteristics thatenhance white-light emission in solar flares, AOGS 12th Annual
Meeting, (Singapore, Aug. 2-7, 2015).
Watanabe, K., Uchida, K., Kobayashi, K., Matsushima, F., Moriwaki,
Y.: 2015, Laser Spectroscopic Study of CaH in the B 2S+ and D
2S+ States, Int. Symp. on Molecular Spectroscopy, 70th meeting,(Urbana-Champagne, IL, USA, Jun. 22-26, 2015).
Watanabe, K., Masuda, S., Kitagawa, J.: 2015, Characteristics thatenhance white-light emission in solar flares, Japan Geoscience Union
Meeting 2015, (Chiba, Japan, May 24-28, 2015).
Watanabe, T., Solar-C WG, Office for Solar-C: 2015, The Solar-C
Mission, 9th Hinode Science Meeting, (Belfast, UK, Sep. 14-17, 2015).
Wootten, A., Corder, S. A., Iono, D., Testi, L.: 2015, ALMA: Millimeter/
submillimeter Astronomy at high sensitivity and resolution, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Wu, Y. W.: 2015, Trigonometric parallax of HMSFR G035.20-1.74, 8thEast Asia VLBI Workshop, (Sapporo, Japan, Jul. 8-10, 2015).
Wu, Y. W.: 2016, Current Calibration strategies for VLBI astrometry,
Australia-Japan School on Low Frequency Astrometry in the SKA
Era, (Kagoshima, Japan, Mar. 28-31, 2016).
Yaji, K.: 2015, Coodinated Solar Observation with High Schools let's observe the sun with Hinode, IAU XXIX General Assembly,(Honolulu, HI, USA, Aug. 3-14, 2015).
Yaji, K.: 2015, Communicating Solar Astronomy to the Public, IAU
XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Yaji, K.: 2015, Solar Observation Data Education in Classroom,
GHOU2015, (Honolulu, HI, USA, Aug. 4-5, 2015).
Yamada, R., Shiraishi, H., Nebut, T., Lognonne P., Asari, K., Tanaka,
S.: 2015, Seismic observation using the broadband seismometers
targeted for moonquake, 30th ISTS, (Kobe, Japan, Jul. 4-10, 2015).
Yamada, Y., Gouda, N., Yoshioka, S.: 2015, JASMINE data analysis,
Division A meeting at the XXIX General Assembly of IAU,

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(Honolulu, USA, Aug. 7-10, 2015).
Yamashita, T., Komugi, S., Matsuhara, H., Armus, L., Inami, H., Ueda,
J., Iono, D., Kohno, K., Stierwalt, S., Arimatsu, K., Evans, A.: 2015,
The Nobeyama 45 m 12CO(J=1–0) Survey of local Luminous Infrared
Galaxies, IAU XXIX General Assembly, (Honolulu, HI, USA, Aug.
3-14, 2015).
Yanagisawa, K., Yoshida, M., Ohta, K., Kawai, N., Izumiura, H.: 2015,
Wide Field NIR Imager at Okayama Astrophysical Observatoty,
Gravitational Wave Physics and Astronomy Workshop (GWPAW)
2015, (Osaka, Japan, June 17-20, 2015).
Yanagisawa, K.: 2016, Current Status of OAO-WFC, 4th Annual
Symposium of the Innovative Area on Multi-messenger Study ofGravitational Wave Sources, (Chiba, Japan, Feb. 18-20, 2016).
Yeh, S. C. C., Seaquist, E. R., Matzner, C. D., Pellegrini, E. W.: 2015,
Molecular and Ionized Hydrogen in 30 Doradus, Feedback in the
Magellanic Clouds, STSci Workshop, (Baltimore, MD, USA, Oct.
5-7, 2015).
Yeh, S. C. C., Tsai, C.-W., Geballe, T. R., Herrera, C. N.: , Mid-infrared[Ne II] Imaging of Young Massive Star Clusters Near Galactic Nuclei,
IAU XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Yoshida, H.: 2016, A trip searching for integrability criteria over 120
years, 3-rd Conference on Finite Dimensional Integrable Systems inGeometry and Mathematical Physics 2015, (Bedlewo, Poland, Jul.
12-17, 2015).
Yun, M. S., Gim, H., Morrison, G., Hales, C. A., Momjian, E., Owen, F.,
Kellermann, K., Aretxaga, I., Giavalisco, M., Hughes, D., Lowenthal,J., Miller, N., Kawabe, R., Kohno, K.: 2015, Tracing Evolution ofStarbursts and AGNs using Ultra-deep Radio and mm/smm Surveys,
IAU XXIX General Assembly, (Honolulu, HI, USA, Aug. 3-14, 2015).
Zenitani, S.: 2015, Numerical Modeling of Relativistic Reconnection:
Kinetic, Two-fluid, and MHD Simulations, Relativistic Jets: Creation,
Dynamics, and Internal Physics, (Krakow, Poland, Apr. 20-24, 2015).
Zenitani, S.: 2015, Particle acceleration in relativistic magnetic
reconnection, AOGS 12th Annual Meeting, (Singapore, Aug. 2-7, 2015).
Zenitani, S.: 2015, High-speed fluid dynamics in magnetic reconnection
in a low-beta plasma, AGU Chapman Conference, (Fairbanks, AK,
USA, Sep. 27-Oct. 2, 2015).
Zenitani, S.: 2015, High-speed fluid dynamics in magnetic reconnection
in a low-beta plasma, ISAS Workshop: Magnetospheric Plasmas
2015, (Tokyo, Japan, Dec. 1-3, 2015).
Zenitani, S.: 2015, Loading Relativistic Maxwell Distributions in
Particle Simulations, AGU Fall meeting 2015, (San Francisco, CA,
USA, Dec. 14-18, 2015).
Zenitani, S.: 2016, Particle dynamics in the electron current layer incollisionless magnetic reconnection, 2016 US-Japan Workshop on
Magnetic Reconnection (MR2016), (Napa, CA, USA, Mar. 7-11, 2016).
Zenitani, S.: 2016, High-speed fluid dynamics in magnetic reconnection
in a low-beta plasma, 2016 US-Japan Workshop on Magnetic
Reconnection (MR2016), (Napa, CA, USA, Mar. 7-11, 2016).
Zenitani, S.: 2016, Particle dynamics and nongyrotropic distributionfunctions in collisionless magnetic reconnection, International
GEMSIS and ASINACTR-G2602 Workshop, (Nagoya, Japan, Mar.
22-25, 2016).
Zenitani, S., Miyoshi, T.: 2015, High-speed fluid dynamics in magnetic
reconnection in a low-beta plasma, AOGS 12th Annual Meeting,(Singapore, Aug. 2-7, 2015).

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