Cover Caption
ALMA image of the protoplanetary disk around HL Tauri.
The new ALMA observations reveal substructures within the disk that have never been seen before.
Credit: ALMA (ESO/NAOJ/NRAO)

Postscript
Editor Publications Committee
HANAOKA, Yoichiro
UEDA, Akitoshi
OE, Masafumi
SÔMA, Mitsuru
NISHIKAWA, Jun
HIROTA, Tomoya
YOSHIDA, Haruo
Publisher National Institutes of Natural Sciences
National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan
TEL: +81-422-34-3600
FAX: +81-422-34-3960
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Annual Report of the
National Astronomical Observatory of Japan

Volume 17, Fiscal 2014

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 2014 – March 2015

001

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

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074
077
080
081
084
086
089
092
094
096
099
101
102
104
105
106
111
116
118
121
122
125

T

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III Organization

126

IV Finance147

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

148

VI Research Collaboration

149

VII Graduate Course Education

151

VIII Public Access to Facilities

156

IX Overseas Travel

162

X Award Winners

163

XI Library, Publications164

XII Important Dates

165

XIII Publications, Presentations
1. Refereed Publications

167

2. Publications of the National Astronomical Observatory of Japan179

3. Report of the National Astronomical Observatory of Japan179

4. Conference Proceedings

179

5. Publications in English

187

6. Conference Presentations

187

Annual Report of the
National Astronomical Observatory of Japan
Volume 17, Fiscal 2014

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 for fiscal year
2014.
In February 2015, NAOJ conducted an External Review
in order to evaluate our achievements over the last five years
from an international standpoint. The first sentence of theevaluation report states, “The most significant development of
the last five years must be the growing and highly successful
Japanese participation in major international astronomical
projects.” This refers primarily to ALMA and TMT. With
the Subaru Telescope, Japanese optical-infrared astronomy
attained world leading status. But at the same time, that wasalso the limit of what Japan could accomplish as a single
country in the field of large telescope construction. Now,
NAOJ is making important contributions to major large-scaleinternational projects, such as ALMA and TMT.
Thanks to our experiences with the Subaru Telescope,
resistance in the Japanese astronomical community to building
telescopes overseas disappeared. It was naturally assumed thatfor ALMA the radio antennas would be established overseas
and that the construction and operation would be carried out as
an international project. This was a new challenge for NAOJ.
Fortunately as part of the reorganization and incorporationof NAOJ in 2004, the personnel system was reconsidered
and the project system was established, allowing flexible

reorganization to facilitate large international projects. It also
became possible for individuals with valuable specializedskills to participate in large international projects as contracted
staff. Furthermore, because NAOJ represents Japan in thesekinds of large international projects, our obligations as aninter-university research institute are clear: to make large
contributions to the advancement of research throughout allof Japan in the field of astronomy. I think the high evaluation
we received from the international community in last fiscal
year’s External Review is a result of these changes in NAOJ’s
structure and philosophy.
In 2014, NAOJ’s Philosophy was codified. Our Vision
is “to be innovators striving to solve the mysteries of the
Universe.” Our Mission has 3 pillars: to develop and constructlarge-scale cutting-edge astronomical research facilities andpromote their open access aiming to expand our intellectual
horizons; to contribute to the development of astronomy asa world leading research institute by making the best use ofa wide variety of large-scale facilities; and to bring benefits
to society through astronomy public outreach. Our Products/
Deliverables are: to explore the unknown Universe andprovide new insight into astronomy; to make our researchoutcomes widely known to society and pass on our dreams tofuture generations; and to mentor next-generation researchers
for their role on the world-stage.

With respect to the extremely large optical-infrared
telescope TMT under construction in Hawai`i, the Master
Agreement, which provides the foundation to proceedwith construction within an international framework,
was completed and President Katsuhiko Sato signed it on
behalf of the National Institutes of Natural Sciences in April
2014. Having received this approval, the TMT International
Observatory was incorporated as a nonprofit corporation in
the following month (May) and a groundbreaking ceremony
was held in October. TMT is a 30 m diameter optical-infrared
telescope being constructed on Maunakea on Hawai`i Island by
5 countries including Japan, the United States of America (theUniversity of California, the California Institute of Technology,
and the National Science Foundation), the People’s Republicof China, the Republic of India, and Canada. Japan bears
responsibility for the most critical components, including
the body of the telescope and production of the nearly 600
segments for the primary mirror. The search for signs of life in
the Universe is one of the stated major targets for TMT. This
statement sounds like a dream, but I am confident the day isapproaching when it will be a reality.
ALMA is continuing commissioning (the process ofconfirming and adjusting the numerous devices one by one)while carrying out Cycle 2 observations. From September toNovember in 2014, long-baseline test observations spanning
ranges of up to 15 km were conducted with surprisingly goodresults. Multiple concentric ring structures can be seen in the
picture of the protoplanetary disk around the young star HL
Tauri taken with a high angular resolution of 0.03 arcseconds.
It is thought that these structures might indicate locations
where planets are forming. Until now, there have been pictures
drawn showing how sites of planet formation were expected
to look, but an actual image is more powerful than I had everimagined. This long-baseline capability will be offered foropen use in Cycle 3, which begins in 2015. Using this, we can
expect many planetary systems forming around young stars to
be found rapidly in the coming years.
At the Subaru Telescope, the Strategic Science Programusing the ultra-wide-field prime focus camera (Hyper
Suprime-Cam) has started. This camera’s survey speed (=limiting magnitude x area of the field of view) is over 10times greater than previous surveys. What’s more, thanks tothis camera the Subaru Telescope’s observations will be theworld’s forerunners without question, until LSST (America’s
Large Synoptic Survey Telescope) becomes operational in the
mid-2020s. Observations with this camera will investigate thenature of dark matter and dark energy which determine theevolution of the large scale structure of the Universe.
Right now the Subaru Telescope is in its prime,
continuously producing outstanding scientific results. In fiscal
year 2014 for example, among the stars born in the early
Universe, a star with peculiar chemical abundance ratios
was discovered relatively close to the Solar System within
our Milky Way Galaxy. This star is thought to have been
formed from the gas left over after the first stars born after
the Big Bang, with masses hundreds of times that of the Sun,
exploded in supernovae. The first stars formed in the Universe
were said to have had masses nearly 1000 times that of theSun. But there had been no clear evidence to support that until
now. These observational results provide the first proof.
The Subaru Telescope also observed a location wherelithium had been produced in the gas expanding from a nova
(an explosive nuclear fusion phenomenon which occurs

when hydrogen accumulates on the surface of a white dwarf).
Lithium, the next lightest element after hydrogen and helium,
was produced in only trace amounts during the Big Bang(about one-billionth the number of hydrogen atoms). Thislithium was absorbed into normal stars and destroyed in theircores. But in fact, the amount of lithium has increased as
the Universe has evolved. Where this lithium was produced
had been a mystery. This discovery directly verified thecircumstances of lithium synthesis.
In addition to the 3 large projects listed above, VERA of theMizusawa VLBI Observatory and the Korean KVN together
formed KaVA to start joint VLBI observations. The large-scale
cryogenic gravitational wave telescope KAGRA, supported incooperation with the University of Tokyo Institute for Cosmic
Ray Research and the High Energy Accelerator Research
Organization, has made important progress, including starting
construction of the laser interferometer.
Last fiscal year, in response to the aging of the 4D2U Dome
Theater, the control computer network and projectors were
upgraded. At the same time, the “3D glasses” were changed toan active shutter system. As a result, across the entire dome theimage has become brighter and more vivid. Simulations of thelarge scale structure of the Universe or Saturn’s rings can fool
you into thinking that you are drifting in space. In addition,
the seating capacity was doubled and it has become possible
to enter without having to first remove your shoes. With these
improvements, the number of days the Dome Theater is open
to the public has been increased in FY 2015. So we expect
more guests than ever to be able to enjoy it.
Finally, in 2014 the East Asian Observatory was founded.
This was established with the goal of making a permanent
basis for large international projects in East Asia in responseto the increasing size and internationalization of telescope
plans which I described above. The founding members are
the National Astronomical Observatory of Japan; the Instituteof Astronomy and Astrophysics of ACADEMIA SINICA in
Taiwan; the Korea Astronomy and Space Science Institute;and the National Astronomical Observatories of the Chinese
Academy of Sciences. There are still a number of unknowns
about how the East Asian Observatory will develop after this.
If we take as an example the European Southern Observatory,
which is currently leading the world in ground-based telescope
projects, we feel it is important to approach the activities of
the East Asian Observatory calmly and deliberately.

Masahiko HAYASHI
Director General of NAOJ

I Scientific Highlights(April 2014 – March 2015)
Solar Rotation Inferred from Radial Velocities of the Sun-as-a-Star during the 2012 May
21 Eclipse
02 The Opposition Effect of the Asteroid 4 Vesta

Takeda, Y., et al.

003

Hasegawa, S., et al.

004

03 Lightcurve Survey of V-Type Asteroids in the Inner Asteroid Belt

Hasegawa, S., et al.

005

Kwon, J., et al.

006

Tsuji, T., Nakajima, T.

007

Coronal Mass Ejections Observed at the Total Solar Eclipse on 13 November 2012

Hanaoka, Y., et al.

008

Mare Volcanism: Reinterpretation Based on Kaguya Lunar Radar Sounder Data

Oshigami, S., et al.

009

Statistical Analysis of the Horizontal Divergent Flow in Emerging Solar Active Regions

Toriumi, S., et al.

010

Imanishi, M., Nakanishi, K.

011

Takakuwa, S., et al.

012

Shibuya, T., et al.

013

Zenitani, S.

014

Structure and Mass of Filamentary Isothermal Cloud Threaded by Lateral Magnetic Field

Tomisaka, K.

015

Two γ-Ray Bursts from Dusty Regions with Little Molecular Gas

Hatsukade, B.

016

Fine Strand-Like Structure in the Solar Corona from Magnetohydrodynamic Transverse
Oscillations

Antolin, P., et al.

017

16 Formation of Carbon Grains in Red-Supergiant Winds of Very Massive Population III Stars

Nozawa, T., et al.

018

Origins of Large Amounts of Dust Grains and Unusual Extinction Curves in HighRedshift Dusty Quasars

Nozawa, T., et al.

019

Fujimoto, K.

020

01

Near-Infrared Circular Polarization Survey in Star-Forming Regions: Correlations and04
Trends

05
06
07
08
09
10
11
12
13
14
15

17

Near-Infrared Spectroscopy of M Dwarfs. I. CO Molecule as an Abundance Indicator ofCarbonEnergy Diagnostics of Nearby Luminous Infrared Galaxies Using ALMA
Growth Process of a Protostellar Binary Revealed with ALMA
Gas Kinematics of Lyman α Emitters at z ~ 2.2
High-Speed Fluid Dynamics in Magnetic Reconnection in a Low-β Plasma

18 Waves and Electron Heating in the Reconnection Separatrix Regions
19 Explosive Lithium Production in the Classical Nova V339 Del

Tajitsu, A., et al.

021

Discovery of Dramatic Optical Variability in a Possible Radio-Loud Narrow-Line Seyfert
20
1 Galaxy

Tanaka, M., et al.

022

21

Universal Profiles of the Intracluster Medium from Suzaku X-Ray and Subaru Weak
Lensing Obesrvations

Okabe, N., et al.

023

22

Spectrum of Gamma-Ray Burst’s Afterglow Indicates the Beginning of the Reionization
ProcessNiino, Y., Totani, T.

024

Michikoshi, S., Kokubo, E.

025

23 Pitch Angle of Galactic Spiral Arms
24

Identification of the Progenitors of Rich Clusters and Member Galaxies in Rapid
Formation at z > 2

Shimakawa, R., et al.

026

25

An Early Phase of Environmental Effects on Galaxy Properties Unveiled by Near-Infrared
Spectroscopy of Protocluster Galaxies at z > 2

Shimakawa, R., et al.

027

26

Visible-Wavelength Spectroscopy of Subkilometer-Sized Near-Earth Asteroids with a Low
Delta-v

Kuroda, D., et al.

028

Hirota, T., et al.

029

27 Mapping Observations of the Continuum Emission in Orion KL with ALMA
28 VERA and ALMA Observations of the Maser Burst in Orion KL
29 Evidence fot a Gas-Rich Major Merger in a Proto-cluster at z = 2.5
30

Near-Infrared Brightness of the Galilean Satellites Eclipsed in Jovian Shadow: A New
Technique to Investigate Jovian Upper Atmosphere

31 Discovery of Extended Ionized Clouds in a Cluster of Galaxies at z ~ 0.4
32 Rapid Change of the Plasma Tail of C/2013 R1(Lovejoy)
Studying Near-Infrared Extragalactic Background with the Cosmic Infrared Background
33
ExpeRiment-2 (CIBER-2)

Hirota, T., et al.

030

Tadaki, K., et al.

031

Tsumura, K., et al.

032

Yagi, M., et al.

033

Yagi, M., et al.

034

Shirahata, M., et al.

035

001

34

A Study on the Methyl Formate in Its Ground and Torsional Excited State Toward Orion
KL Using ALMA Sceience Verification Data

35 Discovery of a Disk Gap Candidate at 20 AU in TW Hya

036

Akiyama, E., et al.

037

36

Revised Big-Bang Nucleosynthesis with Exotic Dark Matter Particle: Detailed Quantum
Mechanical Calculation

Kusakabe, M., et al.

038

37

Asymmetric Neutrino Emission from Magnetized Proto-Neutron Stars: Effects ofAbsorption Cross-Sections in Iso-Entropical Conditions

Maruyama, T., et al.

039

38

Cosmological Solutions to the Big-Bang Lithium Problem: Big-Bang Nucleosynthesis
with Photon Cooling, X-Particle Decay and a Primordial Magnetic Field

Yamazaki, D. G., et al.

040

39 Supernova Nucleosynthesis of 26Al and Nuclear Structure of 26Si

Komatsubara, T., et al.

041

Accelerated Evolution of the Lyα Luminosity Function at z >~ 7 Revealed by the Subaru
40
Ultra-Deep Survey

Konno, A., et al.

042

41 Opacity of Fluffy Dust Aggregates

Kataoka, A., et al.

043

Okumura, S.-i., et al.

044

Otsuji, K., et al.

045

Sekimoto, Y., et al.

046

Survey Observations of Geosynchronous Orbit Objects and Short-Term Variability
42
Observations Using the Time-Delay Integration Method

43

Statistical Analysis of Current Helicity and Twist in Solar Active Regions over the Phasesof the Solar Cycle Using the Spectro-Polarimeter Data of Hinode44 Developments of Wide Field Millimeter/Submillimeter Instruments
45 The Gas Inflow and Outflow Rate in Star-Forming Galaxies at z ~ 1.4

Yabe, K., et al.

047

Enhancement of CO(3–2)/CO(1–0) Ratios and Star Formation Efficiencies in Supergiant46
H II Regions

Miura, R. E., et al.

048

47 Witness of Gas Infall and Outflow in the Young Starburst Dwarf Galaxy NGC 5253

Miura, R. E., et al.

049

Unresolved Mixed Polarity Magnetic Fields at Flux Cancellation Site in Solar Photosphere48
at 0". 3 Spatial Resolution

Kubo, M., et al.

050

The First Very Long Baseline Interferometry Image of a 44 GHz Methanol Maser with the
KVN and VERA Array (KaVA)

Matsumoto, N., et al.

051

50 Torus-Fitting Method in Two-Dimensional Galactic Potentials

Yano, T., et al.

052

Discovery of Star Formation in the Extreme Outer Galaxy Possibly Induced by a High51
Velocity Cloud Impact

Izumi, N., et al.

053

Koyama, Y., et al.

054

Aoki, W., et al.

055

Yamada, K., et al.

056

Kaithakkal, A. J., et al.

057

Ota, K., et al.

058

Niinuma, K., et al.

059

Kano, R., et al.

060

Ishikawa, R., et al.

061

Warren, MacKenzie L., et al.

062

Mathews, G. J., et al.

063

62 The In-Medium Effects on the Neutrino Reaction in Dense Matter

Cheoun, M.-K., et al.

064

63 Induced Amino Acid Chirality from Strong Magnetic Fields in Interstellar Environments

Famiano, M. A., et al.

065

Pehlivan, Y., et al.

066

Kajino, T., et al.

067

Narukage, N., et al.

068

Narukage, N.

069

49

52 Discovery of a Rich Galaxy Cluster Candidate at z = 1.52
53 A Chemical Signature of First-Generation Very-Massive Stars
54

The Moment Approach for Resolving the Orbital Elements of Astrometric Binaries:
Possible Application to Cygnus X-1

55

Photospheric Flow Field Related to the Evolution of the Sun’s Polar Magnetic Patches
Observed by Hinode SOT

56

ALMA Observation of 158 μm [C II] Line and Dust Continuum of a z = 7 Normally StarForming Galaxy in the Epoch of Reionization

57 KVN and VERA Array (KaVA) Observations of Bright AGN Jets
58 Photospheric Properties of Warm EUV Loops and Hot X-Ray Loops
59

Toward the Inversion of the Scattering Polarization and the Hanle Effect in the Hydrogen
Lyα Line

60 Sterile Neutrino Oscillations in Core-Collapse Supernova Simulations
61

Supernova Relic Neutrinos and the Supernova Rate Problem: Analysis of Uncertainties
and the Role of Failed Supernovae

64 Neutrino Magnetic Moment, CP Violation and Flavor Oscillations in Matter
65 Neutrino Oscillation and Nucleosynthesis in Core-Collapse Supernova Explosion
66 Vacuum Ultraviolet Spectro-Polarimeter Design for Precise Polarization Measurements
67 Evidence of Electron Acceleration around the Reconnection X-point in a Solar Flare
002

Hirota, T., et al.

Solar Rotation Inferred from Radial Velocities of the Sun-as-a-Starduring the 2012 May 21 Eclipse
TAKEDA, Yoichi

				OHSHIMA, Osamu(NAOJ)(Mizushima Technical High School)

KAMBE, Eiji, TODA, Hiroyuki, KOYANO, Hisashi, NARITA, Norio, SEKII, Takashi(NAOJ)

SATO, Bun’ei		(Tokyo Institute of Technology)

NAKAMURA, Yasuhisa(Fukushima University)

With an aim to examine how much information ofsolar rotation can be obtained purely spectroscopicallyby observing the Sun-as-a-star during the 2012 May 21
eclipse (Fig. 1) at Okayama Astrophysical Observatory,
we studied the variation of radial velocities (Vr ), whichwere derived by using the iodine-cell technique basedon a set of 184 high-dispersion spectra consecutively
obtained over the time span of ~ 4 hours.
NEd68. 4910( 0%)

Nmoon movement
directionNW

sun movement
direction

E

W

E

d

68. 3889
( 0%)

W

S

S

N

N

68.d4729
(30%)

E

W

N

68.d4549(62%)

W

Figure 2: Behavior of σ(A, B) (standard deviation in fitting thesimulated Vr (t) with the observed Vr (t)).

S

S

E

d

68. 4049
(33%)

N

W

E

N

d

d

68. 4368
(93%)

W

E

68. 4208
(66%)

W

O-C

E

S

0

1500
S

The resulting V r (t) was confirmed to show thecharacteristic variation (Rossiter–McLaughlin effect)caused by time-varying visibility of the solar disk.
By comparing the observed V r (t) curve with thetheoretical ones, which were simulated with the latitude(ψ) dependent solar rotation law ω sidereal (ψ) = A +B sin 2 ψ (deg day −1 ), we found that the relation B −5.5A + 77 gives the best fit as seen from the minimum
trough of σ (A, B) (O−C standard deviation in the A–B
plane; cf. Fig. 2), though separate determinations of A
and B were not possible. This relationship is consistent
with the real values known for the Sun (A  14.5, B −2.8), as can be confirmed in Fig. 3 where the theoreticalcurve corresponding to (A = 14.5, B = −2.75) case iscompared with the observation. This consequence may
provide a prospect of getting useful information on stellar

500

open circle: observed Vrsolid line: modeled Vr(A = 14.5, B = -2.75)-1(m s )

Figure 1: Solar eclipse on 2012 May 21 at Okayama AstrophysicalObservatory.

1000

0

cal

S

Vr

S

-500

-1000
-1500

68.35

68.4
68.45
JD (2456000+)

68.5

Figure 3: Comparison of the theoretical Vr (t) coresponding to (A =14.5, B = −2.75) with the observed Vr (t).

rotation of eclipsing binaries from radial-velocity studies
during eclipse, if many spectra of sufficiently high timeresolution are available. See [1] for more details of thisstudy.
Reference[1] Takeda, Y., et al.: 2015, PASJ, 67, 10.

I Scientific Highlights

003

The Opposition Effect of the Asteroid 4 Vesta
HASEGAWA, Sunao1, MIYASAKA, Seidai2, TOKIMASA, Noritaka3, SOGAME, Akito4, IBRAHIMOV, Mansur A.5
YOSHIDA, Fumi6, OZAKI, Shinobu6, ABE, Masanao1, ISHIGURO, Masateru7, KURODA, Daisuke6
1: ISAS/JAXA, 2: Tokyo Metropolitan Government, 3: Sayo Town Office, 4: Tokai University, 5: Russian Academy of Sciences, 6: NAOJ, 7:
Seoul National University

We present the results of photometric observations
carried out for the asteroid 4 Vesta in the B, Rc, and z’bands at a minimum phase angle of 0.1 degrees withfour small telescopes: the 0.064 m refracting telescope at
ISAS, JAXA in Sagamihara, the 0.36 m Ritchey–Chrétien
telescope at the Miyasaka Observatory, the 0.076 m
refracting telescopeat the Nishiharima Astronomical
Observatory, and the 0.6 m Zeiss reflecting telescope at
the Maidanak Astronomical Observatory.
The magnitudes reduced to unit distance and phaseangle were MB (1, 1, 0) = 3.83, MRc = 2.67, and Mzʹ (1, 1,0) = 3.03 mag. The absolute magnitude obtained fromthe IAU H–G function [1] is ~0.1 mag darker than themagnitude at a phase angle of 0 degrees determined fromthe Shevchenko function [2] and Hapke models with thecoherent backscattering effect term [3] (see Fig. 1, 2). Our
photometric measurement allowed us to derive geometricalbedos of 0.35 in the B band, 0.41 in the Rc band, and0.31 in the z’ bands through the Hapke model with thecoherent backscattering effect term [4]. The porosityof the optically active regolith on the asteroid 4 Vesta
was estimated from the Hapke model to be ρ = 0.4–0.7
yielding the bluk density of 0.9–2.0 × 103 kg m−3 [4].
It is evident that the opposition effect for the asteroid
4 Vesta makes a contribution to not only the shadowhiding effect, but also the coherent backscattering effectthat appears from about 1 degrees. The amplitude of thecoherent backscatter opposition effect for Vesta increases
with a brightening of reflectance. By comparison withother solar system bodies, we suggest that multiplescattering on an optically active scale may contributeto the amplitude of the coherent backscatter opposition
effect (BC 0) [4].

Figure 1: Fitted phase curves for asteroid Vesta using the IAU
H–G phase function [1] and the Shevchenko function [2].

Figure 2: Fitted phase curves for asteroid Vesta obtained with the
Hapke model [3].

References[1] Bowell, E.. et al.: 1989, Asteroid II, 524.
[2] Shevchenko, V. G.: 1996, Lunar Planet. Sci., 27, 1193.
[3] Hapke, B.: 2002, Icarus, 157, 523.
[4] Hasegawa, S., et al.: 2014, PASJ, 66, 89.

004

I Scientific Highlights

Lightcurve Survey of V-Type Asteroids in the Inner Asteroid Belt
HASEGAWA, Sunao1, MIYASAKA, Seidai2, MITO, Hiroyuki3, SARUGAKU, Yuki3, OZAWA, Tomohiko4
KURODA, Daisuke5, NISHIHARA, Setsuko1/3, HARADA, Akari1/3, YOSHIDA, Michitoshi6
YANAGISAWA, Kenshi5, SHIMIZU, Yasuhiro5, NAGAYAMA, Shogo5, TODA, Hiroyuki5, OKITA, Kichi5
KAWAI, Nobuyuki7, MORI, Machiko8, SEKIGUCHI, Tomohiko9, ISHIGURO, Masateru10
ABE, Takumi1, ABE, Masanao1
1: ISAS/JAXA, 2: Tokyo Metropolitan Government, 3: The University of Tokyo, 4: Misato Observatory, 5: NAOJ, 6: Hiroshima University, 7:Tokyo Institute of Technology, 8: Japan Women’s University, 9: Hokkaido University of Education, 10: Seoul National University

To constrain the rotational rate distribution ofasteroids sourced from asteroid 4 Vesta, the lightcurves of
13 V-type asteroids: 1933 Tinchen, 2011 Veteraniya, 2508
Alupka, 3657 Ermolova, 3900 Knezevic, 4005 Dyagilev,
4383 Suruga, 4434 Nikulin, 4796 Lewis, 6331 1992 FZ1,
8645 1998TN, 10285 Renemichelsen, and 10320 Reiland
were observed using the 1.05 m Schmidt telescope andthe 0.30 m Dall–Kirkham telescope (K.3T) at the Kiso
Observatory (MPC code 381), the 0.36 m Ritchey–
Chrétien telescopethe at the Miyasaka Observatory (MPC
code 366), the 0.50 m Classical–Cassegrain telescope(MITSuME) at the Okayama Astrophysical Observatory(MPC code 371), the 1.05 m Cassegrain telescope at
the Misato Observatory (no MPC code), and the 2.24 m
telescope (UH88) in Hawaii (MPC code 568). Using
past lightcurve data archive for V-type asteroids and ourobservations with the exception of 4434 Nikulin and10285 Renemichelsen, we determined the rotational ratesof V-type asteroids (e.g., Fig. 1, 2) [1].
The distribution of rotational rates of 59 V-type
asteroids which includes our 11 new and 48 previous
results in the inner main belt, including 29 members of
the Vesta family, which are regarded as being ejecta fromthe asteroid 4 Vesta, is not consistent with the best-fit
Maxwellian distribution. This inconsistency may be dueto the effect of thermal radiation Yarkovsky–O’Keefe–
Radzievskii–Paddack (YORP) torques, which implies
that the collision event that formed vestoids is sub-billion
to several billion years in age [1]. This is consistent withnumerical simulations of the Vesta family [2] and cratercounting of asteroid 4 Vesta by the Dawn mission [3].

References[1] Hasegawa, S., et al.: 2014, PASJ, 66, 54.
[2] Marzari, F., Farinella, P., Davis, D.: 1999, Icarus, 142, 63.
[3] Marchi, S., et al.: 2003, Science, 336, 690.

Figure 1: Composite rotational lightcurve of the asteroid 1933
Tinchen.

Figure 2: Composite rotational lightcurve of the asteroid 2011
Veteraniya.

I Scientific Highlights

005

Near-Infrared Circular Polarization Survey
in Star-Forming Regions: Correlations and Trends
KWON, J., TAMURA, M.

HOUGH, J. H.

(University of Tokyo/NAOJ)(University of Hertfordshire)

NAKAJIMA, Y.

LUCAS, P. W.

(Hitotsubashi University)(University of Hertfordshire)

We have conducted a systematic near-infraredcircular polarization (CP) survey in star-forming regions,covering high-mass, intermediate-mass, and low-mass
young stellar objects [1]. All the observations were madeusing the SIRPOL imaging polarimeter on the Infrared
Survey Facility 1.4 m telescope at the South African
Astronomical Observatory. We present the polarization
properties of 10 sub-regions in 6 star-forming regions(Figure 1). The polarization patterns, extents, andmaximum degrees of linear and circular polarizations areused to determine the prevalence and origin of CP in the

KUSAKABE, N.

NAGATA, T.

(NAOJ)(Kyoto University)

NAGAYAMA T.

KANDORI, R.

(Kagoshima University)		

(NAOJ)

star-forming regions. Our results show that the CP patternis quadrupolar in general, the CP regions are extensive,
up to 0.65 pc, the CP degrees are high, up to 20 %, andthe CP degrees decrease systematically from high- to
low-mass young stellar objects. The results are consistent
with dichroic extinction mechanisms generating the highdegrees of CP in star-forming regions.
Reference[1] Imanishi, M., Saito, Y.: 2014, ApJ, 780, 106.

Figure 1: Stokes I and V images observed from the IRSF 1.4-m telescope. (a) OMC-1 (b) NGC 6334-V (c) NGC 6334-IV (d) OMC-2 (e)OMC-3 (f) Cha IRN (g) L1551. (Credit: KWON, Jungmi)

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Near-Infrared Spectroscopy of M Dwarfs.
I. CO Molecule as an Abundance Indicator of Carbon
			

TSUJI, Takashi(The University of Tokyo)

M dwarfs are the largest stellar group in thesolar neighborhood. Because of their small masses,
the lifetimes of M dwarfs are longer than the ageof the Universe, and M dwarfs are composed of thesamples of all the populations including very old ones.
Unfortunately, our understanding of this large and richstellar group is rather poor compared to other stellar
groups. This is largely due to the difficulty of observing
M dwarfs because of their faintness. Recent progress,
however, overcame the observational barriers to someextent, especially in the field of stellar interferometry,infrared spectroscopy, astrometry and photometry fromspace.
Based on the near-infrared spectra of 42 M dwarfs,
carbon abundances are determined from the ro-vibrationallines of the CO(2–0) band. We apply Teff values based on
the angular diameters if available or use the Teff values ina log Teff − M3.4 relation (M3.4 is the absolute magnitudeat 3.4 μm based on the WISE W1 flux and the Hipparcos
parallax) to estimate Teff values of objects for whichangular diameters are unknown.
On the observed spectrum of the M dwarf, thecontinuum is depressed by the numerous weak lines of
H2O and only the depressed continuum or the pseudocontinuum can be seen. On the theoretical spectrum of
M dwarf, the true continuum can be evaluated easily but
the pseudo-continuum can also be evaluated accurately
thanks to the recent H 2 O line database. Then the
spectroscopic analysis of the M dwarf can be done byreferring to the pseudo-continuum both on the observed
and theoretical spectra. Since the basic principle of thespectroscopic analysis should be the same whether thetrue- or pseudo-continuum is referred to, the difficulty
related to the continuum in cool stars can in principle beovercome. Then the numerous CO lines can be excellent
abundance indicators of carbon, since almost all the
carbon atoms are in stable CO molecules which suffer
little effect of the uncertainties in photospheric structure,and carbon abundances in late-type stars can best be
determined in M dwarfs rather than in solar type stars.
The resulting C/Fe ratios for most M dwarfs arenearly constant at about the solar value based on thehigh classical carbon abundance rather than the recently
revised lower value. This result implies that the solar
carbon abundance is atypical for its metallicity among thestellar objects in the solar neighborhood if the downward
revised carbon abundance is correct.

NAKAJIMA, Tadashi(NAOJ)

Figure 1: log T eff − M 3.4 relation. T eff values are based oninterferometry (blue) or infrared flux method (red).

Figure 2: Carbon abundances log AC vs. Metallicities obtained byother infrared spectroscopy. The upper(/lower) locus is
C/M ratio for the high(/low) solar value ().

Reference[1] Tsuji, T., Nakajima, T.: 2014, PASJ, 66, 98.

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Coronal Mass Ejections Observed at the Total Solar Eclipse
on 13 November 2012
		HANAOKA, Yoichiro		(NAOJ)		

NAKAZAWA, Jun(Yamanashi Cement Company)

SAKAI, Yoshiaki(Chiba Prefectural Kazusa High School)

OHGOE, Osamu(Solar Eclipse Information Center)

SHIOTA, Kazuo(Solar Eclipse Information Center)

White light observations of the total solar eclipse
on 13 November 2012 were made at two sites, where
the totality occurred 35 minutes apart. Structure of thecorona from the solar limb to a couple of solar radii wasobserved with a wide dynamic range and a high signal-tonoise ratio [1].
At the east limb, a flare, which was accompanied by acoronal mass ejection (CME), occurred between the two
observations of the eclipse, and a CME was observed at
the second totality (Figure 1a and the left square in the
Figure 1b). The eclipse observation shows both of the
CME and related dimming between 1–2 R. This factsuggests that the CME material had been located in thisheight range.
On the other hand, a balloon-like structure at thewest limb (Figure 1b, the right square) observed at theeclipse developed to a CME later on, and was observed
by SOHO/LASCO (Figure 1d). The balloon-like structure
located between 1–2 R is considered to be the source of
the CME.
Both the CMEs show that the source region of CMEs
was located in this height range, where the material andthe magnetic field of CMEs were located before theeruption. This height range includes the gap between theextreme ultraviolet observations of the lower corona andthe spaceborne white-light observations of the higher
corona, but the eclipse observation shows that this height
range is essentially important to study the CME initiation.
The eclipse observation is basically just a snapshot ofCMEs, but it indicates that future continuous observationsof CMEs within this height range are promising.

Reference[1] Hanaoka, Y., Nakazawa, J., Ohgoe, O., Sakai, Y., Shiota, K.:
2014, Solar Phys., 289, 2587.

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I Scientific Highlights

Figure 1: (a) Image of the white-light corona at 21:14 UT of the
13 November 2012 eclipse. Many raw images werestacked to increase the signal-to-noise ratio, and finestructures of the corona were enhanced. (b) Relative
difference of the eclipse corona between 20:39 UT and
21:14 UT. Squares show the CME-related structures.
(c) Aligned composite of the CME at the east limb on a
SDO/AIA 211 Å image (negative) at the flare maximum(20:53:59) (< 1 R), the eclipse corona difference image(21:14−20:39; 1–2.1 R), and a SOHO/LASCO relative
difference image between 22:11:03 and 20:39:45 (>2.1 R). (d) Aligned picture of the CME at the west limb
consisting of an image of the eclipse corona showing
the pre-CME loop structure (< 2.1 R), and a SOHO/LASCO relative difference image between 20:39:45 (13November) and 06:23:25 (14 November) (> 2.1 R). The
solar north is to the top in all the panels.

Mare Volcanism:
Reinterpretation Based on Kaguya Lunar Radar Sounder Data
OSHIGAMI, Shoko

WATANABE, Shiho, YAMAGUCHI, Yasushi(NAOJ)				

KOBAYASHI, Takao(Nagoya University)		

YAMAJI, Atsushi(Kyoto University)

KUMAMOTO, Atsushi, ISHIYAMA, Ken, ONO, Takayuki(Korean Institute of Geoscience and Mineral Resources)			

The volumes of single geological units withdifferent ages and compositions are essential for
revealing characteristics of mare volcanisms and forconstraining the thermal history of the Moon. Recently,
the thicknesses of mare basalt units were indirectly
estimated from Clementine multispectral data [1]. The
results were derived for only limited areas and showed awide variation, implying large uncertainty. At present, thegeological structures under the lunar maria are directly
investigated using sounder observations. The Lunar RadarSounder (LRS) onboard Kaguya detected widespreadhorizontal reflectors under some nearside maria [2].
The LRS detects echoes from subsurface horizons withabrupt changes in dielectric constants [3] at the apparent
depths smaller than about 1 km [4]. Oshigami et al. [5]concluded that the reflectors correspond to the interfaces
between basalt units with different FeO contents.
Therefore the LRS data allow us to discuss the volume ofeach basalt unit.
We correlated subsurface reflectors with the surface
geologic units, the ages of which have been estimated byseveral researchers [e.g., 6], to evaluate the thicknesses
and volumes of the units. The estimated thicknesses andvolumes of the geologic units were the order of 101 to 102
m (Figure 1) and 103 to 104 km3 (Figure 2), respectively,
and showed positive correlations with unit ages within thesame mare basin [7]. Previous studies indicated that the
typical thicknesses of single basalt flows were about 10 m
or less in most of the studied sites [8]. These estimations
suggest that the geologic units are made up of dozens of(Tohoku University)

lava flows. The long-term average eruption rates were
estimated to be the order of 10−5 to 10−2 km3/yr (Figure 3)[7].

Figure 2: Estimated volumes of mare basalt units.

Figure 3: Estimated average eruption rate of mare basalt.

Figure 1: Estimated thicknesses of mare basalt units.

References[1] Weider, S. Z., et al.: 2010, Icarus, 209, 323-336.
[2] Ono, T., et al.: 2009, Science, 323, 909-912.
[3] Ono, T., Oya, H.: 2000, Earth Planets Space, 52, 629-637.
[4] Oshigami, S., et al.: 2009, Geophys. Res. Lett., 36, L18202.
[5] Oshigami, S., et al.: 2012, Icarus, 218, 506-512.
[6] Hiesinger, H., et al.: 2000, J. Geophys. Res., 105(E12), 2923929275.
[7] Oshigami, S., et al.: 2014, J. Geophys. Res. Planets, 119(5),1037-1045.
[8] Brett, R.: 1975, Geochim. Cosmochim. Acta, 39, 1135-1141.

I Scientific Highlights009

Statistical Analysis of the Horizontal Divergent Flowin Emerging Solar Active Regions
TORIUMI, Shin(NAOJ)		

HAYASHI, Keiji

YOKOYAMA, Takaaki(Stanford University)		

It is widely accepted that the formation of active
regions of the Sun is caused by emerging magnetic
fields from the convection zone [1]. In the previous
MHD simulation studies (e.g., [2]), we pointed out thatthe emerging magnetic fields push up the local (nonmagnetized) plasma above their heads. It is therefore
expected that the horizontal divergent flow (HDF) appears
before the magnetic flux itself emerges at the visible
surface of the Sun. In fact, the HDF was observationallydetected in a flux emergence event we selected [3]. In
this work [4], we analyzed the HDFs in many more flux
emergence events and investigated the physical state of
the subsurface magnetic fields, which we cannot directly
observe.
We analyzed flux emergence events that wereobserved by the Helioseismic and Magnetic Imager(HMI) on board the Solar Dynamics Observatory (SDO).
We searched for the events that appeared in the eastern
hemisphere with a heliocentric angle θ ≤ 60° during theperiod between 2010 May and 2011 June (14 months)
and picked up 23 events. Figure 1(a) is a sample of theevents, showing the line-of-sight magnetic field.
Out of the 23 events, 6 clear HDFs were detectedby the method previously developed in [3], while 7
additional events that were detected by visual inspection
were added to this statistic analysis. The distribution of
the events is shown in Figure 1(b). From this map, one
may find that the flux emergence events are distributedin the mid-latitude bands of both hemisphere and thatthe clear HDFs are concentrated in the area with aheliocentric angle θ > 30°. As a result of the statisticalanalysis, we found that the duration of the HDF is on
average 61 minutes and the maximum HDF speed is on
average 3.1 km s−1. We also estimated the rising speed of
the subsurface magnetic fields to be 0.6–1.4 km s−1. These
values are consistent with the previous one-event analysis[3] as well as the numerical simulation results [2].

(The University of Tokyo)(a)Heliographic distribution
1.0(b)
Clear HDF
HDF by eye
No HDF

0.5
y/RSun

		

0.0

-0.5

-1.0
-1.0

-0.5

0.0
x/RSun0.5

1.0

Figure 1: (a) Example of flux emergence data showing lineof-sight magnetic field strength. The black and whiteplus signs are the flux-weighted centers of positive
and negative polarities, respectively, measured in therectangular box. 1 pixel corresponds to 0.5 arcsec. (b)Heliographic distribution of the flux emergence events.
Figures reproduced from [4].

References[1] Parker, E. N.: 1955, ApJ, 121, 491.
[2] Toriumi, S., Yokoyama, T.: 2013, A&A, 553, A55.
[3] Toriumi, S., et al.: 2012, ApJ, 751, 154.
[4] Toriumi, S., et al.: 2014, ApJ, 794, 19.

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Energy Diagnostics of Nearby Luminous Infrared Galaxies Using ALMAIMANISHI, Masatoshi, NAKANISHI, Kouichiro(NAOJ)

Luminous infrared galaxies (LIRGs) are formed bygas-rich galaxy mergers. Their large infrared luminosities
are powered by starburst and/or supermassive-blackholedriven, active galactic nucleus (AGN) activity in dustobscured regions. To investigate the nature of these dustobscured energy sources of LIRGs, observations at the
wavelengths of low dust extinction are crucial. An AGN
has two important different properties, when compared
to starburst activity. First, an AGN has much higher
emission surface brightness, and so produces a larger
amount of hot (several 100 K) dust, than a starburst.
Second, the X-ray to UV luminosity ratio is higher in an
AGN than a starburst. Due to these different properties,
AGN and starburst can have different physical/chemical
effects to the surrounding molecular gas, and so can
produce different molecular line flux ratios. Since
rotational transition lines of molecules are found at thealmost dust-extinction-free (sub)millimeter wavelength,
emission line flux ratios of multiple molecules could be a
powerful tool to scrutinize dust-obscured energy sourcesof LIRGs. Since molecular gas in LIRGs is usually athigh density, observations of molecules with high dipole
moments, such as HCN, HCO+, and HNC, are useful toinvestigate the physical properties of LIRGs. We haveconducted HCN, HCO+, HNC J = 4–3 observations, at thesubmillimeter 350 GHz range, of six LIRGs whose energy
sources were diagnosed based on previously obtained
infrared spectra [1]. Our primary aim is to confirm thedichotomy of molecular line flux ratios as a functionof primary energy source (i.e., AGN or starburst), andto investigate if this method is effective to scrutinize
unknown dust-obscured energy sources of distant LIRGs.
Figure 1 shows an example of ALMA data. Figure 2
plots the observed molecular line flux ratios. Among fivesources marked with filled stars, four (except IR22491)
were diagnosed to be buried-AGN important, and tend
to show higher HCN/HCO + J = 4 – 3 flux ratios thanstarburst-dominated regions in the LIRG, NGC 1614
(marked with filled circles). This HCN flux enhancementin AGNs could be qualitatively explained by widely
proposed scenarios of (1) HCN abundance enhancement,
relative to HCO +, in an AGN, (2) HCN J = 4 – 3 flux
enhancement by infrared radiative pumping, in addition
to collisional excitation, and (3) more HCN J = 4 – 3
excitation (higher critical density than HCO+ J = 4–3) in an
AGN than a starburst. The energy source of the remaining
one LIRG (IR22491) is still uncertain. In this LIRG,
further investigations are required, because its molecularline flux ratio could be largely affected by galaxy-wide
turbulence, as inferred from its large molecular line width[1]. Future ALMA observations of other LIRGs withknown energy sources at other rotational transition lines
are needed to confirm the effectiveness of molecular line
flux ratios as the method of energy diagnostics of LIRGs
and to understand the physical origin of the observed
molecular line flux ratios.

Figure 1: Integrated intensity maps (Top) and spectra (Bottom)of the LIRG, IRAS 08572+3915. (Left): HCN J = 4–3,
(Right): HCO+ J = 4–3. In the integrated intensity maps,
the filled elliptical circles at the lower-left parts represent
ALMA beam sizes. In the spectra, the ordinate is flux
(mJy beam−1) and the abscissa is optical velocity (km s−1).

Figure 2: Molecular line flux ratios of LIRGs obtained in our
ALMA Cycle 0 data. The abscissa is HCN/HNC J=4–3
flux ratio, and the ordinate is HCN/HCO+ J=4–3 flux
ratio.
Reference[1] Imanishi, M., Nakanishi, K.: 2014, AJ, 148, 9.

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Growth Process of a Protostellar Binary Revealed with ALMA
TAKAKUWA, Shigehisa(ASIAA) 		

		

LIM, Jeremy

SAITO, Masao(NAOJ)(University of Hong-Kong)

HANAWA, Tomoyuki(Chiba University)		

We report results of our ALMA Cycle 0 observationof a protostellar binary L1551 NE, which show thatthe protostellar binary is growing through the massaccumulation from the surrounding circumbinary material[1].
More than half of stars with masses similar to the
Sun are known to be binaries [2,3]. Studies of formationand growth processes of binaries are thus essential
for comprehensive understanding of star formation.
Protostellar binaries are surrounded by disks of molecular
gas and dusts, “circumbinary disks” (hereafter CBDs),
and are considered to grow through accumulation of thematerials from the CBDs. Resolutions and sensitivities
of previous observations are, however, not high enoughto investigate the structures and gas motion in the CBDs,
and to discuss the feeding process of the materials to thecentral protostellar binaries. The spatial resolution andsensitivity of our ALMA Cycle 0 observation of L1551
NE are ~1.6 times and ~6 times higher than those attainedin our previous SMA observations [4,5], respectively, andthus we are able to investigate internal structures and gas
motions in the circumbinary disk of L1551 NE in detail.
Figure 1 (left) shows the observed L1551 NE imageof the dust-continuum emission at a 0.9-mm wavelength.
There are compact components associated with theindividual binary stars (cross marks), “circumstellar
disksˮ. The circumstellar disks are surrounded by a larger(r ~300 AU) CBD, which exhibits U-shaped feature to thesouth of the protostellar binary, emission protrusions to
the northwest which curls to the northeast, and emission
minima between these features and the protostellar binary.
Gas motions in the CBD as revealed in the C18O (J = 3–2)
line show faster rotations than the local Keplerian rotationand expanding motions in these continuum features, andslower rotations and infalling motions in the regions of
the continuum emission minima.
To interpret physics of these observed structuresand gas motions in the CBD around L1551 NE, we
conducted numerical simulations of the CBD using
the supercomputer ATERUI in National Astronomical
Observatory of Japan (NAOJ) (Figure 1 right) [6]. The
theoretical image shows two spiral arms stemming fromthe individual binary stars, which constitute the CBD. In
those spiral arms the gas rotates with the velocity fasterthan the local Keplerian rotation velocity, and exhibits
expanding motion. On the other hand, in the inter-arm
regions the gas rotates slower, and exhibits infalling

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SAIGO, Kazuya(Osaka Pref. University)

MATSUMOTO, Tomoaki(Hosei University)

HO, Paul, T. P.
(ASIAA)

motion toward the central protostellar binary. This isbecause of the exchange of the angular momenta inside
the CBD, caused by the non-axisymmetric gravitational
torques from the central binary. These simulation results
reproduce the observed structures and gas motions in
the CBD around L1551 NE quantitatively; that is, our
ALMA observation unveiled the growth process of the
protostellar binary by removing the angular momenta of
the surrounding material and capturing those materials.
Our ALMA Cycle 2 proposal to observe L1551 NE
at a ~0 ″. 1 angular resolution has been approved, andthe observation will be made in the summer 2015. We
anticipate that the observation will reveal the spiral arm
features and gas motions in the CBD unambiguously, andthat we will be able to discuss physical mechanism to set
final masses and mass ratios of binary stars.

Figure 1: (Left) ALMA image of L1551 NE in the 0.9-mm dustcontinuum emission. Crosses denote the positions of the
protostellar binary, and a filled ellipse at the bottom-rightcorner the synthesized beam (0 ″. 72×0 ″. 36; P.A.=9.1º).
(Right) Theoretically-predicted 0.9-mm dust-continuum
image of L1551 NE obtained from our numericalsimulation using the NAOJ supercomputer ATERUI.

References[1] Takakuwa, S., et al.: 2014, ApJ, 796, 1.
[2] Raghavan, D., et al.: 2010, ApJS, 190, 1.
[3] Reipurth, B., et al.: 2014, Protostars and Planets VI, 267.
[4] Takakuwa, S., et al.: 2012, ApJ, 754, 52.
[5] Takakuwa, S., et al.: 2013, ApJ, 776, 51.
[6] Matsumoto, T.: 2007, PASJ, 59, 905.

Gas Kinematics of Lyman α Emitters at z ~ 2.2
SHIBUYA, Takatoshi(ICRR)		

ONO, Yoshiaki

OUCHI, Masami(ICRR/University of Tokyo)

NAKAJIMA, Kimihiko*(California Institute of Technology)		

RAUCH, Michael

HASHIMOTO, Takuya(Lyon Observatory)

GAUTHIER, Jean-Rean(ICRR/University of Tokyo) (Observatories of the Carnegie Institution of Washington) (California Institute of Technology)		

SHIMASAKU, Kazuhiro, GOTO, Ryosuke

MORI, Masao, UMEMURA, Masayuki(University of Tokyo)					Lyα Emitters (LAEs) are an important populationof high-z star-forming galaxies in the context of galaxy
formation. Additionally, LAEs are used to measure
the neutral hydrogen fraction at the reionizing epoch,
because Lyα photons are absorbed by intergalactic
medium. However, Lyα emitting mechanism is not fully
understood due to the highly-complex radiative transfer
of Lyα in the interstellar medium.

Figure 1: Rest-frame Lyα EW as a function of Δv Lyα and Δv IS. Red
symbols represent our z ~ 2.2 LAEs [2].

Lyα emissivity may not only depend on the spatial
ISM distribution, but on the gas kinematics as well. The
gas kinematics of LAEs has been evaluated from theLyα velocity offset (Δv Lyα) with respect to the systemic
redshift (z sys) traced by nebular emission lines (e.g, [O III]).
Hashimoto et al. (2013) find an anti-correlation between
Lyα equivalent width (EW) and Δv Lyα [1]. However,Δv Lyα is thought to increase with both resonant scatteringin H I gas clouds as well as galactic outflow velocity. The
gas kinematics can be investigated more directly from thevelocity offset between interstellar (IS) absorption linesof the rest-frame UV continuum and z sys (IS velocity
offset; Δv IS).
We present a statistical study of Δv Lyα and Δv IS for
LAEs at z  2. We make a sample of 22 LAEs based on
our deep Keck/LRIS observations, in conjunction with
spectroscopic data from the Subaru/FMOS program
and the literature [2,3]. We confirm the anti-correlation
between Lyα EW and Δv Lyα (Fig. 1). Our LRIS data

(University of Tsukuba)

successfully identify blue-shifted multiple IS absorption
lines in the UV continua of four LAEs on an individual
basis (Fig. 2). The average Δv IS is −200 ~ −300 km s−1,
indicating LAE’s gas outflow with a velocity comparable
to typical LBGs. The results of our study suggest that
LAEs have a small N HI compared to LBGs.

Figure 2: Normalized UV spectra of the four continuum detected
LAEs [2].

References[1] Hashimoto, T., et al.: 2013, ApJ, 765, 70.
[2] Shibuya, T., et al.: 2014, ApJ, 788, 74.
[3] Nakajima, K., et al.: 2012, ApJ, 745, 12.

* NAOJ at the time of publication.

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High-Speed Fluid Dynamics in Magnetic Reconnection in a Low-β Plasma
ZENITANI, Seiji(NAOJ)In the solar corona, in the planetary magnetosphere,
and in other astrophysical settings, magnetic reconnection
often occurs in a low-β plasma, in which the magnetic
pressure is higher than the plasma pressure. Surprisingly,
much less is known about low-β reconnection, partially
due to numerical difficulties and partially due to lack ofattention. Recently, new features of low-β reconnection
were reported in magnetohydrodynamic (MHD)
simulations with shock-capturing codes. Zenitani etal. [1,2] discovered new normal shocks and a repeatedshock-reflection near a magnetic island (plasmoid) at thereconnection jet front.
In this work, we extend our previous researches on
the plasmoid structure in low-β reconnection. Using ahigh-accuracy HLLD code [3], shocks, discontinuities,
and their intersections are resolved and clarified in
unprecedented detail. Figure 1 is a snapshot of thereconnection-plasmoid system in run 1 in Ref. [4]. The
color indicates vertical MHD velocities. There are two
triangle-trains, as indicated by the white circles. They
correspond to shock-reflections in a supersonic jet, theso-called “shock diamonds.” The right ones are overexpanded shock-diamonds in front of the plasmoid.
The left ones are under-expanded shock-diamonds,
hidden inside the reconnection jet. In addition, contact
discontinuities and a slow expansion fan from shockcrossing points are found. All these structures are
summarized in the 2015 edition of the “plasmoid
diagram” (Figure 2).
From the physics viewpoint, these structures areoutcome of high-speed fluid effects or compressible fluid
effects. High-speed fluid dynamics plays an importantrole in a low-β plasma, because an Alfvénic reconnection
jet easily becomes transonic or supersonic. Underlying
mechanisms are similar to those in aerospace engineeringand in astrophysical jet physics. Since the mechanisms
are common, similar shocks and shock-dissipation willtake place in plasmoid-dominated turbulent reconnection.
We have a prospect that the high-speed effects will be
important in various astrophysical MHD systems, inwhich Alfvén speed becomes supersonic.
The simulation code for Ref. [4] is publicly available
at arXiv:1503.01920. Fortran 90 files are archived in agzipped tar file in the “Other formats” link.

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Figure 1: A snapshot of run 1 in Ref. [4]. Vertical MHD velocities
are shown in color: the upward (downward) velocity ingreen (red). The black curves show the magnetic fieldlines.

Figure 2: Schematic diagram of the plasmoid structure. Based on
Fig. 7 in Ref. [2], it further contains recent updates inRef. [4].

References[1] Zenitani, S., et al.: 2010, ApJ, 716, L214.
[2] Zenitani, S., Miyoshi, T.: 2011, Phys. Plasmas, 18, 022105.
[3] Miyoshi, T., Kusano, K.: 2005, J. Comput. Phys., 208, 315.
[4] Zenitani, S.: 2015, Phys. Plasmas, 22, 032114.

Structure and Mass of Filamentary Isothermal CloudThreaded by Lateral Magnetic Field
TOMISAKA, Kohji(NAOJ)

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 with aself-consistent field method [4]. Figure 1 shows typicalsolutions of cross-cut of these filaments. Top and bottom
panels show solutions with low and high center-tosurface density ratios, respectively.
We obtained an empirical relation between the
maximum supported mass against the self-gravity, λ max,
and magnetic flux, Φcl, as,
λ max  0.24 Φcl /G 1/2 + 1.66 c2s /G ,where Φcl, G, and cs represent, respectively, one-half ofthe magnetic flux per unit length of the filament, Newton's
gravitational constant, and the isothermal sound speedof the filament gas. For Φcl > 3 pc μG (cs /190 m s−1)2,
the magnetic force (the Lorentz force) plays more
important role than the thermal pressure in determining
the equilibria. It is known that axisymmetric isothermal
clouds have a maximum mass which is supported
against the self-gravity by the magnetic field as M max
 Φ2D /2πG1/2, where Φ2D represents the magnetic flux
threading the cloud. The importance of this article isthat structure and the maximum mass of the filaments,
which are building blocks of molecular clouds, are firstly
determined theoretically.
References[1] Men’shchikov, A., et al.: 2010, A&A, 518, L103.
[2] Sugitani, K., et al.: 2011, ApJ, 734, 63.
[3] Strittmatter, P., A.: 1966, MNRAS, 132, 359.
[4] Tomisaka, K.: 2014, ApJ, 785, 24.

Figure 1: Structure of the isothermal filament laterally threaded
by magnetic field. Long dashed lines running vertically
represent the magnetic field lines. Closed solid lines are
iso-density contours. Contour lines are placed for 1, 2,
3, 5, 10, 20, 30, 50, 100, and 200 times the density at thesurface. Non-dimensional initial radius of the filament
is taken as R0 = 2 and the plasma beta of the ambient
gas outside the filament is taken as β0 = 1. We plotted
two typical solutions with different center-to-surface
density ratios, 10 (upper) and 300 (lower). Vertical andhorizontal axes mean nondimensional distances from thecenter of the filament.

I Scientific Highlights

015

Two γ-Ray Bursts from Dusty Regions with Little Molecular Gas
HATSUKADE, Bunyo(NAOJ)

Long-duration gamma-ray bursts (GRBs) are thought
to be associated with the explosions of massive stars.
Because GRBs are bright enough to be observable inthe cosmological distances, they are expected to be a
new tool to scrutinize the obscure details of the distant
Universe. Although multi-wavelength observations of
GRB host galaxies have been conducted, the environment
where GRBs occur is still unclear due to the lack ofspatially-resolved observations of molecular gas anddust. Previous searches for CO in GRB host galaxies did
not detect any emission [1,2,3,4]. Molecules have been
detected as absorption in the spectra of GRB afterglows[5], but absorption lines probe the interstellar medium
only along the line of sight, so it is not clear whether themolecular gas represents the general properties of theregions where the GRBs occur.
We conducted observations of the CO emission line
and 1.2-mm continuum towards two GRB hosts (GRB
020819B at z = 0.41 and GRB 051022 at z = 0.81) using
the Atacama Large Millimeter/submillimeter Array(ALMA). The CO emission line is clearly detected at thenuclear region of the GRB 020819B host and the GRB
051022 host (Figure 1). This is the first case for detecting
spatially resolved molecular gas emission in GRB hosts[6]. The 1.2-mm continuum emission is also detected inboth GRB hosts. The spatially resolved continuum mapof the GRB 020819B host shows that the emission issignificantly detected only at the GRB site.
We found that the spatial distributions of molecular
gas and dust are clearly different in the GRB 020819B
host. The ratio of molecular gas mass to dust mass at the
GRB site is significantly lower than that of the nuclear
region, indicating that the GRB occurred under particular
circumstances within the host. The molecular gas-to-dust
ratio at the GRB site is also lower than those of the Milky
Way and nearby star-forming galaxies [7], suggestingthat the star-forming environment where GRBs occur
is different from those in local galaxies. The possible
reasons for the deficit of molecular gas in the GRB site
are that much of the dense gas has been dissipated by astrong interstellar UV radiation field, which is expected inregions with intense star formation. The lack of molecular
gas in optical spectra of GRB afterglows has beenreported [8] and a possible explanation is the dissociationof molecules by ambient UV radiation with 10–100 times
the Galactic mean value from the star-forming regions[8,9].

016

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Figure 1: Velocity-integrated CO maps (left), 1.2-mm continuum
maps (middle) obtained with ALMA, and opticalR-band images (right) of the GRB 020819B host (top)and the GRB 051022 host (bottom). The magenta crossrepresents the position of radio afterglow. ALMA beam
is shown at the bottom left. Original figure from [6].

References[1] Kohno, K., et al.: 2005, PASJ, 57, 147.
[2] Endo, A., et al.: 2007, ApJ, 659, 1431.
[3] Hatsukade, B., et al.: 2007, PASJ, 59, 67.
[4] Hatsukade, B., et al.: 2011, ApJ, 738, 33.
[5] Prochaska, J. X., et al.: 2009, ApJ, 691, L27.
[6] Hatsukade, B., et al.: 2014, Nature, 510, 247.
[7] Draine, B. T., et al.: 2007, ApJ, 663, 866.
[8] Tumlinson, J., et al.: 2007, ApJ, 668, 667.
[9] Whalen, D., et al.: 2008, ApJ, 682, 1114.

Fine Strand-Like Structure in the Solar Corona from
Magnetohydrodynamic Transverse Oscillations
ANTOLIN, Patrick(NAOJ)			

YOKOYAMA, Takaaki(University of Tokyo)			

The organisation of fine-scale structure in the coronalhigh-Reynolds environment is a major unknown in solar
physics. One of the leading theories for explaining theheating of the solar corona consists on the ubiquitous
existence of small-scale locations where efficient energy
release through magnetic reconnection takes place,a scenario leading to the concept of nanoflares [1].
According to that theory, coronal loops, closed magnetic
flux tubes permeating the solar corona, are expected tohave a braided field substructure, which would favour
the occurrence of magnetic reconnection and therefore
nanoflares. Due to the strongly anisotropic thermal
conduction in the corona, nanoflares are expected to
produce strand-like structure. The existence of strands
as substructure of larger coronal structure such as loops
has therefore been considered as strong evidence for aleading role of reconnection in the heating of the corona[2].
Transverse MHD waves are now known to beubiquitous in the solar atmosphere [3-6]. Such waves arecharacterised by periods of a few minutes, amplitudes ofa few km/s and show generally strong damping, which isusually explained through resonant absorption, a processof energy conversion from the transverse motion to
local Alfvén waves at the boundary of the flux tube [79]. In this Letter [10] we have suggested an alternative
mechanism for generation of strand-like structure in EUV
lines by establishing a link with the ubiquitous small
amplitude transverse MHD oscillations observed in thecorona. Through three-dimensional MHD simulations
combined with proper forward modelling we have shownthat small amplitude transverse MHD waves can leadin a few periods time to strand-like structure in loops
in EUV intensity images. Low amplitude transverse
MHD oscillations matching those presently observed in
the corona lead to Kelvin-Helmholtz instabilities (KHI)
that deform the cross-sectional area of loops [11-13].
Azimuthal flows at the boundary of the flux tube areenhanced by resonant absorption, thereby facilitating theonset of the instability. A coupling takes place in which
the KHI extracts the energy from the resonance anddumps it into heat through the generation of vortices andcurrent sheets. Strands result as a complex combinationof the vortices and the line-of-sight angle, and can beobserved for spatial resolutions of a tenth of loop radius.
Transverse MHD waves may therefore play an importantrole in the heating and morphology of the solar corona.

VAN DOORSSELAERE, Tom(KU Leuven)

Figure 1: Left: Snapshot of the emission line flux of Fe IX
171.073 Å for several cross-sections along half acoronal loop subject to a transverse MHD wave. Right:
KHI vortices produced by the wave appear as strandlike structure in intensity. The lower half of the loop
shows the full numerical resolution, while the upper
half corresponds to a spatial resolution of 10 % the loop
radius R.

References[1] Parker, E. N.: 1988, ApJ, 330, 474.
[2] Klimchuk, J. A.: 2006, Sol. Phys., 234, 41.
[3] Okamoto, T. J., et al.: 2007, Science, 318, 1577.
[4] Tomczyk, S., et al.: 2007, Science, 317, 1192.
[5] Lin, Y.: 2011, Space Sci. Rev., 158, 237.
[6] McIntosh, S. W., et al.: 2011, Nature, 475, 477.
[7] Ionson, J. A.: 1978, ApJ, 226, 650.
[8] Sakurai, T., et al.: 1991, Sol. Phys., 133, 227.
[9] Goossens, M., et al.: 2002, A&A, 394, L39.
[10] Antolin, P., et al.: 2014, ApJ, 787, L22.
[11] Heyvaerts, J., Priest, E. R.: 1983, A&A, 117, 220.
[12] Ofman, L., et al.: 1994, Geophys. Res. Lett., 21, 2259.
[13] Terradas, J., et al.: 2008, ApJ, 687, L115.

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017

Formation of Carbon Grains in Red-Supergiant Windsof Very Massive Population III StarsNOZAWA, Takaya(NAOJ)

			

YOON, Sung-Chul(Seoul National University)

NOMOTO, Ken’ichi(Kavli IPMU)		

MAEDA, Keiichi(Kyoto University)

KOZASA, Takashi(Hokkaido University)

LANGER, Norbert(Argelander-Institut für Astronomie der Universität Bonn)

The origin of cosmic dust in the early universe has
been hotly debated since the discoveries of huge amountsof dust grains in high-redshift (z ≥ 5) quasars.Although
the characteristic mass of the early generation of stars
remains to be clarified, recent calculations of stellar
evolution found that non-rotating Population III stars withthe zero-age main sequence mass of MZAMS > 250 M
undergo convective dredge-up of a large amount ofcarbon and oxygen from the helium-burning core to thehydrogen-rich envelope during the red-supergiant (RSG)
phase [1]. This may lead to enrichment of the surrounding
medium with CNO elements via RSG winds, which canserve as formation sites of dust in the early universe.
We investigate the formation of carbon dust in astellar wind during the RSG phase of a very massive
Population III star with M ZAMS = 500 M  [2].The
calculations are performed by applying the formulation of
non-steady-state dust formation [3]. The formula enables
us to evaluate the size distribution of newly formed grains
and their condensation efficiency defined as the fractionof free carbon atoms that are locked up in grains.
The results of the calculations show that, in a carbonrich wind with a constant velocity, carbon grains canform with a lognormal-like size distribution, and that
all of the carbon available for dust formation finallycondense into dust for wide ranges of the mass-loss rate
( ≥ 8 × 10−5 M yr−1) and wind velocity (1–100 km s−1)(see Figs. 1 and 2). These results indicate that, at most,
1.7 M of carbon grains can form in total during the RSG
phase of 500 M Population III stars. We note that these
newly formed grains could not be destroyed by the blast
wave arising from a supernova explosion because sucha very massive star would finally collapse into a black
hole. Thus, the derived high dust yield could place very
massive primordial stars as important sources of dust at
the very early epoch of the universe if the initial massfunction of Population III stars was top-heavy.
We also propose a new formation scenario of carbonrich ultra-metal-poor stars; such primitive low-massstars were born in the gas clouds that were enriched withcarbon grains and CNO elements from Population III
RSGs.

Figure 1: Final average radius (a ave, ∞) and final condensation
efficiency (fcon, ∞) of carbon grains formed in mass-loss
winds of a 500 M Popularion III RSG as a function ofmass-loss rate Ṁ for a fixed wind velocity of vw = 20 km s−1.

Figure 2: Same as Figure 1, but as a function of wind velocity vw
for a fixed mass-loss rate of Ṁ = 3 × 10−3 M yr−1.

References[1] Yoon, S.-C., Dierks, A., Langer, N.: 2012, A&A, 542, A113.
[2] Nozawa, T., et al.: 2014, ApJ, 787, L17.
[3] Nozawa, T., Kozasa, T.: 2013, ApJ, 776, 24.

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Origins of Large Amounts of Dust Grains and Unusual Extinction Curves
in High-Redshift Dusty Quasars
NOZAWA, Takaya

ASANO, Ryosuke S., TAKEUCHI, Tsutomu T.

(NAOJ)				

(Nagoya University)				

There are many pieces of evidence that the extinction
curves of quasars beyond z = 4 are different from those of
low-z quasars and that a huge amount of dust is present
in their host galaxies. These indicate that the earlyinterstellar medium (ISM) was rapidly enriched with dust
grains whose properties were different than the nearby
ones. The previous dust evolution models argued that,in addition to dust grains ejected from supernovae andasymptotic giant branch stars, grain growth via accretionof gaseous metals in the ISM is required to account forthe observed dust mass. However, these models assumed
a representative grain size or a specific grain size
distribution throughout the galaxy evolution, and thus
could not make any prediction on extinction curves.
Recently, we constructed an evolution model of size
distribution of interstellar dust by taking into accountthe fundamental physical processes of formation anddestruction of dust [1]. This model enables us to predict
the extinction curves in galaxies as a function of time[2]. Based on this state-of-the-art dust evolution model,
we investigate how the massive amounts of dust and theunusual extinction curves in high-z dusty quasars can be
reproduced in a self-consistent manner.
First, we demonstrate that the Milky-Way extinction
curve is reproduced by introducing a moderate fraction( 0.2) of dense molecular-cloud phases in the ISM
for a graphite-silicate dust model. Then, we show thatthe peculier extinction curves in high-z quasars can be
explained by taking a much higher molecular-cloud
fraction (≥ 0.5) (Fig. 1), which leads to more efficientgrain growth and coagulation. The large dust content
in high-z quasar hosts is also found to be a naturalconsequence of the enhanced dust growth (Fig. 2). We
also find that the major composition of carbonaceous
dust in high-z dusty quasars is amorphous carbon rather
than graphite. These results indicate the differences in theproperties of carbonaceous dust and in the condition of
the ISM between low-z and high-z galaxies.

References[1] Asano, R. S., et al.: 2013, MNRAS, 432, 637.
[2] Asano, R. S., et al.: 2014, MNRAS, 440, 134.
[3] Nozawa, T., et al.: 2015, MNRAS, 447, L16.
[4] Maiolino, R., et al.: 2004, Nature, 431, 533.

HIRASHITA, Hiroyuki(ASIAA)

Figure 1: Calculated UV extinction curves at t = 1 Gyr. The
dotted, thick solid, and dashed lines show the results forthe mass fraction of the molecular-cloud phase of 0.5,
0.7, and 0.9, respectively. The hatched region draws
the range of the extinction curve for the high-z quasar
J1048+4637 at z = 6.2 [4]. For comparison, the SMC
extinction curve is denoted by the thin solid line. The
figure is taken from [3].

Figure 2: Time evolutions of dust-to-gas mass ratios (solid) andmetallicity (dashed) obtained from the dust evolution
model in a high-z quasar. The case with grain growth(red solid) can reach the observed high dust-to-gas mass
ratio ( 0.01), while the case without grain growth (bluesolid) cannot. The figure is taken from [3].

I Scientific Highlights

019

Waves and Electron Heating in the Reconnection Separatrix Regions
FUJIMOTO, Keizo(NAOJ)

Magnetic reconnection is a natural energy converter,
releasing explosively the magnetic field energy into
plasma kinetic energy. It is a typical multi-scale
phenomenon where the magnetic dissipation takes place
predominantly in a microscopic region formed aroundthe x-line, while the topological change of the fieldlines causes large-scale plasma convection. Magnetic
reconnection is universal process in space plasma
leading to explosive phenomena such as geomagnetic
substorms and solar flares. The purpose of this researchis to understand the fundamental processes of magnetic
reconnection and to establish the universal model
applicable to real phenomena under complicated initial/
boundary conditions. In particular, this paper focuseson the roles of microscopic waves in the reconnection
processes.
Recent satellite observations in the geomagnetotail
have shown that the wave activities are significantly
enhanced in a broad range of frequency around theseparatrices of anti-parallel magnetic reconnection where
the guide-field is negligibly small [1]. The waves wererecognized as lower hybrid waves, Langmuir waves,electrostatic solitary waves (ESWs), and whistler waves.
In most cases, they were associated with cold electron
beams and density cavity. However, because of thelimited space-time resolutions of the observations, it has
been difficult to identify the generation mechanisms of
the waves and their roles in magnetic reconnection.
We have developed a new electromagnetic particlein-cell model with adaptive mesh refinement (AMRPIC model) in order to achieve efficient multi-scale
kinetic simulations [2]. Recently we further applied an
open boundary condition to the AMR-PIC model, whichenabled us to pursue longer-time evolution of magnetic
reconnection. Using the 2D AMR-PIC code, we have
performed a large-scale simulation of anti-parallel
magnetic reconnection with more realistic parameters of
the geomagnetotail (e.g., the mass ratio mi /me = 400 andthe background density nb /n0 = 0.04) than most previous
simulations.
As a result, the simulation has successfully
reproduced the waves consistent with those observed
frequently in the separatrix regions of magnetic
reconnection in the geomagnetotail (see upper panelof Fig. 1). The key process generating the waves isintense parallel acceleration of the electrons due to anelectrostatic potential jump formed in a localized regionof the inflow side of the separatrices. The intense electron
beams trigger the electron two-stream instability andthe beam-driven whistler instability. The Buneman020

I Scientific Highlights

instability is also excited due to moderate electron beams
arising upstream the potential jump. The electron twostream instability generates the Langmuir waves, while
the Buneman instability gives lower hybrid waves.
Both modes evolve the ESWs in the nonlinear phases.
The Langmuir waves trap the electrons in the parallel
direction and forms a flat-top distribution with highenergy cutoff (lower left panel of Fig. 1), which is wellconsistent with the observations. On the other hand, thewhistler waves scatter the electrons in the perpendicular
direction, producing isotropic distribution with nonthermal high-energy tail [3] (lower right panel of Fig. 1).

Figure 1: Wave activities seen in the parallel electric field aroundthe reconnection region (upper panel) and the electron
distribution functions (lower panels) in each wave active
region.

References[1] Viberg, H., et al.: 2013, Geophys. Res. Lett., 40, 1032.
[2] Fujimoto, K.: 2011, J. Comput. Phys., 230, 8508.
[3] Fujimoto, K.: 2014, Geophys. Res. Lett., 41, 2721.

Explosive Lithium Production in the Classical Nova V339 Del						

TAJITSU, Akito, AOKI, Wako
(NAOJ)		

NAITO, Hiroyuki(Nagoya University/Nayoro Observatory)

Lithium (Li) is a key element in the study of thechemical evolution of the universe because it likely has
been produced by Big Bang nucleosynthesis,interactions
between energetic cosmic rays and interstellar matter,
evolved low-mass stars, novae, and supernova
explosions. The observed Li evolutionary curve has aplateau for young Galactic ages (< 2.5 Gyr) followed by asteep rise. This indicates that a relatively low-mass stellar
component is a major source of Li in the recent universe[1]. Some low-mass evolved stars have indeed beenfound to have Li-enriched surfaces. However, such Li
could be easily depleted by convection in stellar surface
and envelope, because Li should be destroyed inside stars
where temperature is higher than 2.5 million K. Nova
eruptions, which have evolved from low-mass binaries,
are also assumed to be candidates for Li suppliers. No
direct evidence, however, for the supply of Li fromevolved stellar objects to the Galactic medium has yet
been found. The origin of Li and its production process
have long been an unsettled question in cosmology andastrophysics.
We have provided the first direct evidence to solve
this question by spectroscopic observations of a classicalnova [2]. The post-outburst spectra of V339 Del (=Nova
Delphini 2013) were obtained using the high dispersion
spectrograph (HDS) of the 8.2-m Subaru Telescopeat four epochs (+38, +47, +48, and +52 days after the
maximum). These spectra contain a series of broad
emission lines originating from neutral hydrogen andother permitted transitions of neutral or singly ionizedspecies (e.g., Fe II , He I , Ca II ). Most of these broad
emission lines are accompanied by sharp and blueshifted multiple absorption lines at their blue edges (v rad~ −1000 km s−1). Among these absorption line systems,
we have noticed two remarkable pairs of absorption
features in the UV range near 312 nm. These correspondto the absorption components originating from theresonance doublet lines of a singly ionized radioactive
isotope of beryllium, 7Be. Figure 1 displays the blueshifted absorption line systems of Hη, Ca II K, and the
7Be II doublet in the spectrum obtained at +47 day. Afterruling out the possibilities of alternative identifications,
we concluded that these absorption features at 312 nm arecaused by 7Be.
Our spectroscopic detection of 7Be in a classicalnova immediately connects to the production of 7Li. The
production of 7Be via the nuclear reaction 3He ( α , γ ) 7Be

SADAKANE, Kozo

(Osaka Kyoiku University)

ARAI, Akira(Kyoto Sangyo University/University of Hyogo)

in novae has been studied theoretically [3]. Furthermore,
the 7Be absorption lines are found in highly blue-shifted
flows. This means that it will soon decay to 7Li in coolerinterstellar or circumstellar matter on a time scale givenby the half-life of 7Be (53.22 days). The 7Be abundancein the absorbing gas system estimated from the strengthsof their absorption lines is perhaps 3–10 times as muchas models predict. Since V339 Del appears to be one ofthe ordinary classical novae, the 7Be production found in
this object might be occurring in many classical novae. In
near future, more observations of other nova explosions
will provide much clearer model of Li evolution.

Figure 1: The blue-shifted absorption line systems in +47 days.
All lines have two components of velocities at −1268
and −1103 kms−1. Thanks to the high resolution of thespectrum (~ 0.0052 nm), we can clearly distinguish themfrom the doublet of 9Be II at 313.0422 and 313.1067 nm(green lines).

References[1] Prantzos, N.: 2012, A&A, 542, A67.
[2] Cameron, A. G. W., Fowler, W. A.: 1971, ApJ, 164, 111.
[3] Tajitsu, A., et al.: 2015, Nature, 518, 381.

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021

Discovery of Dramatic Optical Variability
in a Possible Radio-Loud Narrow-Line Seyfert 1 Galaxy
TANAKA, Masaomi(NAOJ)		

MOROKUMA, Tomoki(University of Tokyo)		

TOMINAGA, Nozomu

				(Konan University)

ITOH, Ryosuke, AKITAYA, Hiroshi(Hiroshima University)and KISS collaboration

is likely a NLS1 at z = 0.840 (Figure 2), however withunusually strong narrow emission lines. The estimatedblack hole mass of ~107 M implies bolometric nuclear
luminosity close to the Eddington limit.
Interestingly, SDSS J1100+4421 is also found to be
an extremely radio-loud object, with a radio loudness
parameter of R  4 × 102 – 3 × 103, which implies thepresence of relativistic jets. In addtion, the 1.4 GHz
radio image of the source shows an extended structurewith a linear size of about 100 kpc (Figure 1). If SDSS
J1100+4421 is a genuine NLS1, this radio structure
would then be the largest ever discovered in this type ofactive galaxies. Our discovery demonstrates that highcadence surveys are potentially useful to search for sucha rare class of AGNs and to study the jet production/duty
cycle in the growing BHs.

Figure 1: Upper: Discovery image of SDSS J1100+4421 takenon 2014 Feb 23 UT (middle), compared with the SDSS
image (left) and the FIRST 1.4 GHz radio image (right).
Lower: Light curves of SDSS J1100+4421 around thediscovery epoch.

It is widely accepted that active galactic nuclei (AGNs)
are powered by supermassive black holes (BHs) accretingat high rates. Among AGNs, narrow-line Seyfert 1
galaxies (NLS1s) are of a particular interest, since AGNsof this peculiar type are believed to have relatively small
BH masses (106–108 M) and very high accretion rates.
By these properties, it had been inferred that NLS1s are aradio-quiet class of AGNs, and that young BHs in NLS1s
that undergo rapid growth via high-rate accretion do not
produce relativistic jets.
We discovered dramatic variability in SDSS
J1100+4421 (Figure 1) by the high-cadence opticaltransient survey Kiso Supernova Survey (KISS, [1,2]).
The source brightened in the optical by at least a factorof three within about half a day (Figure 1). Spectroscopic
observations with Subaru/FOCAS suggest that this object

022

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Figure 2: Optical spectra of SDSS J1100+4421 taken with Subaru/
FOCAS.

References[1] Morokuma, T., et al.: 2014, PASJ, 66, 114.
[2] Tanaka, M., et al.: 2014, ApJ, 793, L26.

Universal Profiles of the Intracluster Medium
from Suzaku X-Ray and Subaru Weak Lensing Obesrvations
OKABE, Nobuhiro1/2, UMETSU, Keiichi3, TAMURA, Takayuki4, FUJITA, Yutaka5, TAKIZAWA, Motokazu6
ZHANG, Yu-Ying7, MATSUSHITA, Kyoko8, HAMANA, Takashi9, FUKAZAWA, Yasushi1
FUTAMASE, Toshifumi10, KAWAHARADA Madoka4, MIYAZAKI, Satoshi9, MOCHIZUKI, Yukiko8
NAKAZAWA, Kazuhiro11, OHASHI, Takaya12, OTA, Naomi13, SASAKI, Toru8, SATO, Kosuke8, TAM, Sutieng14
1: Hiroshima University, 2: Kavli IPMU, University of Tokyo, 3: ASIAA, 4: JAXA, 5: Osaka University, 6: Yamagata University, 7: Universität
Bonn, 8: Tokyo University of Science, 9: NAOJ, 10: Tohoku University, 11: University of Tokyo, 12: Tokyo Metropolitan University, 13: Nara
Women’s University, 14: National Taiwan University

We conduct a joint X-ray and weak-lensing study offour relaxed galaxy clusters (Hydra A, A478, A1689 andA1835) observed by both {\it Suzaku} and Subaru out tovirial radii, with an aim to understand recently-discovered
unexpected feature of the intracluster medium (ICM) in
cluster outskirts. We show that the average hydrostaticto-lensing total mass ratio for the four clusters decreases
from ~70 % to ~40 % as the overdensity contrast
decreases from 500 to the virial value. The averagegas mass fraction from lensing total mass estimates
increases with cluster radius and agrees with the cosmic
mean baryon fraction within the virial radius, whereas
the X-ray-based gas fraction considerably exceeds thecosmic values due to underestimation of the hydrostatic
mass. We also develop a novel advanced method for
determining normalized cluster radial profiles for
multiple X-ray observables by simultaneously taking into
account both their radial dependence and multivariatescaling relations with weak-lensing masses. Although thefour clusters span a range of halo mass, concentration,
X-ray luminosity and redshift, we find that the gas
entropy, pressure, temperature and density profiles are
all remarkably self-similar when scaled with the weaklensing M200 mass and r 200 radius. As shown in Figure 1[1], the entropy monotonically increases out to ~0.5 r 200~r 1000 following the accretion shock heating model K(r)∝ r 1.1 [2], and flattens at >~ 0.5 r 200. The universalityof the scaled entropy profiles indicates that thethermalization mechanism over the entire cluster region(> 0.1 r 200 ) is controlled by gravitation in a common
way for all clusters, although the heating efficiency inthe outskirts needs to be modified from the standard r 1.1
law. The bivariate scaling functions of the gas density
and temperature reveal that the flattening of the outskirts
entropy profile is caused by the steepening of thetemperature, rather than the flattening of the gas density.
Thus, gas clumpiness [4], leading to an overestimate of
the observed gas density, cannot be responsible for all of
the flatness of the outskirts entropy.

Figure 1: Normalized entropy profile as a function of the radiusscaled by r 200 . Red diamonds, blue triangle, green
squares and magenta circles denote the normalized
entropy for A478, Hydra A, A1689, and A1835,
respectively. The normalization is K*(M200, z)=K0 E(z)−4/3
a2(M200 E(z)/1014 h −1
70 M) , where K0 = 359.61 [keV cm ]and a = 0.63. The black solid curve represents the bestfit universal entropy profile. The entropy profile atr <~ 0.5 r 200 follows r 1.1 as predicted by the standard
model [2] and becomes flat at r >~ 0.5 r 200. The blackdashed curve shows the best-fit profile for the othermodel [3].

References[1] Okabe, N., et al.: 2014, PASJ, 66, 99.
[2] Tozzi, P., Norman, C.: 2001, ApJ, 546, 63.
[3] Lapi, A., et al.: 2010, A&A, 516 A34.
[4] Nagai, D., Lau, E. T.: 2011, ApJ, 731, L10.

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023

Spectrum of Gamma-Ray Burstʼs Afterglow
Indicates the Beginning of the Reionization Process
				

NIINO, Yuu(NAOJ)The intergalactic gas became neutral by the cosmic
recombination. On the other hand, the intergalactic gas
is ionized in the present Universe. To account for thisdifference between the past and present, there must havebeen a transition era of re-ionization after the dark age of
the Universe, which was filled with neutral gas. However,scientists do not yet know when this transition occurredor understand how the process took place. One strong
possibility is that the ultraviolet (UV) radiation fromthe first-generation galaxies in the one-billion-year-old
Universe ionized the hydrogen gas in the intergalactic
space. Therefore, it is very important to identify when the
re-ionization occurred relative to the formation of the first
generation of light-emitting objects.
Previous studies of the re-ionization have focused on
galaxies or quasars. Observations of galaxies are indirectin that a number-count decreases when neutral hydrogengas obscures their light. Observations of quasars directly
measure the absorption features in their spectra causedby neutral hydrogen. However quasars occur in themost developed regions of galaxy evolution, and theirown radiation ionizes the surrounding material. These
factors make it difficult to estimate the neutral gas inthis environment. In contrast, GRBs allow the direct
measurement of neutral hydrogen and also overcome thedrawbacks of the quasar approach.Although studies basedon GRBs are highly desirable, the rare occurrence of
GRBs bright enough to enable detailed analysis has beena challenge. The only previously available data about reionization was the current team’s 2006 report of data fromobservations of GRB 050904 from the Subaru Telescope.
This past data proved that the ionization rate was alreadyhigh in that era, without any sign of intergalactic neutralhydrogen [1].
A research team composed of scientists fromthe University of Tokyo, the National Astronomical
Observatory of Japan, the Tokyo Institute of Technology
and others observed the afterglow of GRB 130606A on
June 6, 2013 and studied its spectrum in great detail [2].
Its afterglow was bright enough in the visible wavelength
to allow for analysis, despite its great distance at aredshift of 5.913. Its distance situates the object at a timeclose to the presumed re-ionization era. The data from
Subaru Telescope clearly show that intergalactic, neutralhydrogen gas accounts for the observed absorption
feature (Figure 1). Further analysis led the team toconclude that more than 10 % of the hydrogen gas was
neutral relative to the total amount of hydrogen. This024

I Scientific Highlights

TOTANI, Tomonori(University of Tokyo)

means that the Universe still had a high proportion ofneutral hydrogen gas when it was one billion years old.
This is the first time that a research team has made aquantitative measurement of such a high proportion ofneutral gas during this era.
This finding marks a significant beginning forscientists to understand the era that preceded reionization. Next generation telescopes, whether inspace or ground-based, such as the future Thirty-MeterTelescope (TMT), will definitely show how the first
generation galaxies formed in the primordial Universeand more clearly define the process of transition from an
opaque, neutral-hydrogen-filled Universe to a transparent,
re-ionized one.

Figure 1: Visible wavelength spectrum of the afterglow of GRB
130606A at redshift of z = 5.913, when the Universe
was a mere one billion years old. Due to its redshift, theLyman-alpha line (originally 1215 Å) is at 8400 Å. The
analysis of a distinctive feature (i.e., the wing feature)
between 8000–8400 Å contributed to the estimate of theratio of neutral hydrogen relative to the entire amount ofhydrogen.

References[1] Totani, T., et al.: 2006, PASJ, 58, 485.
[2] Totani, T., et al.: 2014, PASJ, 66, 63.

Pitch Angle of Galactic Spiral Arms
MICHIKOSHI, Shugo, KOKUBO, Eiichiro(NAOJ)In a differentially rotating disk, a leading density
pattern rotates to a trailing one due to the shear. If
Toomre’s Q value is larger than unity but not too much,the amplitude of the pattern can be enhanced during therotation. This mechanism is called swing amplification[1]. If a perturber such as the corotating overdense region
exists, trailing patterns form. In N-body simulations,since a disk consists of a finite number of stars, small
density noise always exists. Thus, even if there is not a
perturber, the small leading wave always exists, and thetrailing wave can grow spontaneously due to the swing
amplification mechanism. The spirals generated by theswing amplification are not stationary but transient andrecurrent, which appear and disappear continuously. Thistransient and recurrent picture is supported by N-bodysimulations for multi-arm spirals [2].
One of the key parameters that characterize spiralarms in disk galaxies is a pitch angle that measures theinclination of a spiral arm to the direction of galacticrotation. The pitch angle differs from galaxy to galaxy,
which suggests that the rotation law of galactic disks
determines it [3]. In order to investigate the relation
between the pitch angle of spiral arms and the shear
rate of galactic differential rotation, using local N-bodysimulations and linear analyses, we study the pitch angleof the spiral arms with various parameter sets [4].
We performed local N-body simulations of purestellar disks based on the epicycle approximation. We
do not consider an entire disk but a small rotating patchby employing a local shearing box. This treatment
reduces the number of necessary particles in a simulation
significantly, and enables us to perform high resolution
simulations. The typical density snapshot and the
autocorrelation function are shown in Figure 1. The x-axis
is directed radially outward, the y-axis is parallel to thedirection of rotation. Spiral or wake structures are formed
due to gravitational instability and they are trailing.
We quantitatively evaluated the pitch angle using the
autocorrelation function with various parameters. The
result is summarized in Figure 2. We found the clear
trend that the pitch angle θ decreases with the shear rate Γ.
Using the formulation of the collisionless Boltzmann
equation, we performed linear analyses of the swing
amplification and found that the pitch angle of the mostamplified wave for Q >~ 1.5 is given as

results suggest that the spiral arms in this simulation
are formed by the swing amplification from the leading
wavelet in the density fluctuation.

Figure 1: Surface density snapshot (left) and the autocorrelation
function for the shear rate Γ = 1.0.

Figure 2: The pitch angle of the spiral arms in N-body simulations
as a function of Γ. The solid curve denotes the pitch
angle formula given by Equation (1).

References[1] Julian, W. H., Toomre, A.: 1966, ApJ, 146, 810.
[2] Fujii, M. S., et al.: 2011, ApJ, 730, 109.
[3] Seigar, M. S., et al.: 2006, ApJ, 645, 1012.
[4] Michikoshi, S., Kokubo, E.: 2014, ApJ, 787, 174.

(1)
As shown in Figure 2, the pitch angle formula agrees
well with the results of the numerical simulations. TheseI Scientific Highlights

025

Identification of the Progenitors of Rich Clusters and Member Galaxies
in Rapid Formation at z > 2
SHIMAKAWA, Rhythm, KODAMA, Tadayuki

		

TANAKA, Ichi

(NAOJ/SOKENDAI)				

(NAOJ)		

TADAKI, Ken-ichi(Max-Planck-Institut)

HAYASHI, Masao, KOYAMA, Yusei(NAOJ)

Galaxy clusters are the largest self-gravitational
system in the Universe, in which member galaxies
have some unique characteristics in their morphology,
dynamics and such as. However, nobody has not reached
yet on revealing their physical origins observatinally.
Such an environmental dependence of galaxy
formation seen in between galaxy clusters and generalfields is a key issue to understand an entire pictureof galaxy formation process. In order to resolve thisproblem, protoclusters above the redshift of two are
the ideal laboratories since cluster galaxies are still invigorous forming processes in those regions.
With this background, we conducted the near-infrared
spectroscopic observation to Hα-selected galaxies
associated with two rich protoclusters (PKS1138–262 atz = 2.2 and USS1558–003 at z = 2.5) in March–April 2013.
These protoclusters are found by our distant-protocluster
survey named ‘MAHALO-Subaru’ [1]. The observation
motivates on confirming dynamical masses and velocity
structures of the protoclusters [2], and also on studying
physical properties of star-forming galaxies in them. This
will provide us with crucial insights on searching foran early phase of environmental dependence of galaxy
formation.
As a result, total integration time of more than 2 hrs
for each target gave us with line spectra located at 1.3–2.5
μm in 27 & 36 objects in PKS1138–262 and USS1558–
003, respectively. Those data were derived from low
resolution grism (HK500) attached with MOIRCS,
near-infrared multi-object spectrograph on the Subaru
telescope. We observed 80 % out of the targets during 5nights, and then finally confirmed 70 % spectroscopicallyamong them (Fig. 1).
Founded on the datasets, we explore the dynamicalmasses of the protoclusters by using velocity dispersionof the members located at those cluster cores. The results
show that both of two protoclusters have about 1014 M.
Interestingly, this exactly follows the typical mass growth
history of today’s most massive class of galaxy clusters(~1015 M) predicted by cosmological simulations [3,4].
So far, we have some non-confirmed members andneed to investigate more details of velocity structuresof these quite rich protoclusters. Future MOSFIRE(on the Keck I telescope) observation will satisfy suchrequirements.

026

I Scientific Highlights

Figure 1: Composite color image of the protocluster PKS1138–
262, based on the data taken by Hubble Space Telescope(F814W & F475W). Yellows are spectroscopicallyconfirmed members including the past works. Whites do
not still have spectroscopic data, and yet are Hα-selectedgalaxies by our past narrow-band imaging.

Figure 2: Redshift versus cluster dynamical masses. The yellow
stars show our results and the others are derived fromthe past works. The red and the pink lines are the typicalmass growth history of massive cluster haloes with
1–2×1015 M predicted by theoretical simulations [3,4].

References[1] Kodama, T., et al.: 2013, IAUS, 295, 74.
[2] Shimakawa, R., et al.: 2014, MNRAS, 441, L1.
[3] Shimizu, I., et al.: 2012, MNRAS, 427, 2866.
[4] Chiang, Y.-K., et al.: 2013, ApJ, 779, 127.

An Early Phase of Environmental Effects on Galaxy Properties
Unveiled by Near-Infrared Spectroscopy of Protocluster Galaxies at z>2
SHIMAKAWA, Rhythm, KODAMA, Tadayuki

TADAKI, Ken-ichi

				(NAOJ/SOKENDAI)			(Max-Planck-Institut)

HAYASHI, Masao, KOYAMA, Yusei, TANAKA, Ichi
(NAOJ)

Metals in the Universe are produced in the interiorsof stars as they evolve and then released into surrounding
gas through supernova explosions or stellar winds known
as ‘chemical evolution’. This means that the metallicity of
the gases provides us with crucial insights on formation
mechanisms of the galaxies. This work tries to diagnose
the presence of environmental dependence of galaxy
formation by investigating the gaseous metallicity of the
protocluster galaxies at the redshift around two.
The metallicity of the gases in the protocluster
galaxies can be derived from line ratios of multiple
spectral lines emitted from them. Based on the line
spectra taken by MOIRCS on the Subaru telescope, weestimated their gaseous metallicities [1] and comparedthem with those in the general field [3]. As a result,
we find the excess of their gaseous metallicities in the
protocluster regions by 0.10–0.15 dex relative to those ofgalaxies in the general fields (Figure 1). The metallicity
excess in the protoclusters suggests biased star-formation
histories in the dense regions. This may be caused byseveral effects as below,• Recycling chemically enriched gas• Stripping metal poor HI gas in outer region• Advanced stage of downsizing galaxy evolution• Top-heavy initial mass function• Sampling bias
Among these possibilities, we suggest that the above
two scenario may be the most effective factors thatcause different gaseous metallicities of the protocluster
galaxies, because gas inflow/outflow processes strongly
control the chemical enrichment along with the stellar
nucleosynthesis. If so, we can also explain the larger
offset of the gaseous metallicities of the protoclusters
from those in the fields at higher redshifts (Figure 1)
since the redshift around two is considered to be the peak
epoch of inflow and outflow activities. The result suggeststhat galaxy formation has already been influenced byenvironmental conditions in the era that star-formation
activities are the most active across the universe. This
would be an early phase of strong environmental effects
seen in the present galaxy clusters.
However, we cannot fully rule out the otherpossibilities so far, and therefore we need to continue
exploring the detailed physical properties of individual
forming galaxies in the protoclusters to find clear
evidence that proves such a hypothesis.

Figure 1: The offset of the averaged gaseous metallicities
12+log(O/H) of protocluster at z ~ 2 (red; [1,4,7]) &cluster at z ~ 0 (black; [5,6]) galaxies from those ingeneral fields in the literature plotted against stellar
mass.

References[1] Shimakawa, R., et al.: 2015, MNRAS, 448, 666.
[2] Shimakawa, R., et al.: 2014, MNRAS, 441, L1.
[3] Erb, D. K., et al.: 2006, ApJ, 644, 813.
[4] Kulas, K. R., et al.: 2013, ApJ, 774, 130.
[5] Ellison, S. L., et al.: 2009, MNRAS, 396, 1257.
[6] Hughes, T. M., et al.: 2013, A&A, 550, A115.
[7] Valentino, F., et al.: 2015, ApJ, 801, 132.

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027

Visible-Wavelength Spectroscopyof Subkilometer-Sized Near-Earth Asteroids with a Low Delta-v
KURODA, Daisuke1, ISHIGURO, Masateru2, TAKATO, Naruhisa1, HASEGAWA, Sunao3, ABE, Masanao3
TSUDA, Yuichi3, SUGITA, Seiji4, USUI, Fumihiko4, HATTORI, Takashi1, IWATA, Ikuru1
IMANISHI, Masatoshi1, TERADA, Hiroshi1, CHOI, Young-Jun5, WATANABE, Sei-ichiro6, YOSHIKAWA, Makoto3
1: NAOJ, 2: Seoul National University, 3: ISAS/JAXA, 4: The University of Tokyo, 5: Korea Astronomy and Space Science Institute, 6:
Nagoya University

The research on near-Earth asteroids (hereafterNEAs) has entered a new phase thanks to sample-return
space explorations together with state-of-the-art large
ground-based telescopes. NEAs with a low delta-v, which
is defined in terms of the criterion for accessibility, are
known as potential candidates for exploration including
flybys, rendezvous, sample return, and human missions.
However, only a small percent of known NEAs have been
observed in the effort to acquire physical characteristics,
because most such asteroids have short windows ofobservable opportunity.
In our work [1], to investigate the spectroscopic
properties of the unclassified asteroids, we performed
visible spectroscopic observations during two years
from 2011 at the Subaru (FOCAS: [2]), GEMINI-North(GMOS: [3]), GEMINI-South (GMOS) and Okayama
188 cm (KOOLS: [4]). Ten NEAs among these asteroids
share features of both the sub-kilometer-size with 18.8
≤ H < 21.7 and the low delta-v of less than 7 km/sec.
All observations were in the long-slit mode with thewide slit (2–6″ wide slit), and the low resolution grating(or grsim). The reflectance spectrum of an asteroid was
obtained from the raw asteroid spectrum by dividing itby the spectrum of a standard solar analog star. The final
spectrum of each asteroid was summed up and re-binned
to match a resolution based on the instrument settings.
Figures 1 shows the asteroid spectra from FOCAS. All
spectra provide wavelength coverage from roughly 0.5 to
0.9 μm.
A total of 13 asteroids were classified by comparing a
best fit between our data and the visible parts of the mean
Bus-DeMeo spectra [5]. We find that eleven asteroids
are classified as S-complex1) and one asteroid as V-type.
Most S-complex asteroids (eight out of eleven, ~70 %)have spectra similar to subgroups of Q or Sq-type,suggesting that these objects are less matured against
space weathering.
In [1], we show their spectra and discuss dominanceof S-complex asteroids based on the previous research.
It is clear that S-complex asteroids make up the majorityof low delta-v asteroids. We further found that thefractions of S/C-complexes 2) are less dependent ondelta-v. Although we examined the fractions based on
1) S-type or the associated types of Q, O, A, Sr, Sq-type2) C-type or the associated types of B, F, G type028

I Scientific Highlights

the absolute magnitude H to study the observational bias,
we concluded that the dominance of S-complex asteroids
is not sampling bias based on either delta-v or absolutemagnitude H criteria.

Figure 1: Visible spectra of six NEAs obtained with FOCAS at theSubaru telescope. All spectra are normalized to 0.55 μm.
Their error bars are evaluated in terms of Poisson errors
including the gain and readout noise and the uncertainty
depending on the airmass mismatch.

References[1] Kuroda, D., et al.: 2015, PASJ, 66, 1.
[2] Kashikawa, N., et al.: 2002, PASJ, 54, 819.
[3] Hook, I. M., et al.: 2004, PASP, 116, 425.
[4] Yoshida, M., et al.: 2005, J. Korean Astron. Soc., 38, 117.
[5] DeMeo, F. E., et al.: 2009, Icarus, 202, 160D.

Mapping Observations of the Continuum Emissionin Orion KL with ALMA		HIROTA, Tomoya, HONMA, Mareki(NAOJ/SOKENDAI)			

We have carried out high-resolution observationsof millimeter and submillimeter continuum emission
from the Orion KL region, the nearest site of massive
star-formation, using ALMA cycle 0 data [1]. Total
11 compact continuum sources are identified in both
ALMA band 6 (245 GHz) and band 7 (339 GHz)
images, including the Hot Core, Compact Ridge, SMA1,
IRc4, IRc7, and Source I (Figure 1). A spectral energy
distribution (SED) of each source can be determined toconstrain physical properties such as size, mass, hydrogen
number density, and column density assuming the dust
graybody emission.
Among 11 identified compact continuum sources,
Source I, which is a massive protostar candidate, is thebrightest with an unresolved structure even in the longer
uv length than 200 kλ. It is thought that the continuum
emission from Source I is associated with a circumstellar
disk around a massive protostar object. We investigate
its SED from centimeter to submillimeter wavelengths
employing previously published result (Figure 2). The
SED of Source I can be approximately fitted with asingle power-law index of 1.97 suggesting an optically

KURONO, Yasutaka(NAOJ/JAO)			

KIM, Mi-Kyoung(KASI)

thick black body emission. To explain this SED, weemploy the H− free-free emission as an opacity source,which is an interaction between neutral hydrogen atoms/
molecules and electrons. The temperature, density, andmass of the circumstellar disk associated with Source
I are constrained by the SED of H− free-free emission.
Nevertheless, the fitting result shows a significant
deviation from the observed flux densities. We next
calculate the SED by including the thermal dust graybody
SED to explain excess emission at higher frequency.
Future higher resolution and high frequency observations
with ALMA will be crucial to constrain the emission
mechanism and physical properties of the circumstellar
disk associated with Source I.

Figure 2: Spectral energy distribution of Source I, the mostbrightest continuum source in Orion KL. Flux densities
are taken from previous literatures [2], except for our
245 GHz and 339 GHz data.A solid line indicates thebest-fit single power-law model, F ν = pν q, with theindex of 1.97. A dashed line indicates the combinationof power-law and graybody SEDs, with the power-law
index of 1.60.

Figure 1: Continuum map of Orion KL observed with ALMAat band 7. The contours start at the −5σ level with aninterval of 10σ (5, 15, 25, ...). Crosses indicate thepositions of the point sources identified by our mapping.

References[1] Hirota, T., Kim, M. K., Kurono, Y., Honma, M.: 2015, ApJ,
801, 82.
[2] Plambeck, R. L., et al.: 2013, ApJ, 765, 40.

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029

VERA and ALMA Observations of the Maser Burst in Orion KL		HIROTA, Tomoya, HONMA, Mareki(NAOJ/SOKENDAI)			

FUJISAWA, Kenta(Yamaguchi University)		

KIM, Mi-Kyoung(KASI)We have been carrying out monitoring observations of
the 22 GHz H2O maser burst (supermaser) in the nearest
massive star-forming region Orion KL using VERA since2011 March [1,2]. In the present study, we have continued
our monitoring of the supermaser until the end of 2013,
and revealed the detailed properties of its time variation.
As a result, we detect several flux maxima during ourmonitoring period in 2011–2013, and the maximum flux
density is recorded in June 2012 with the flux densityof 135000 Jy (Figure 1). This flux maximum is smaller
by a factor of 10 compared with the previous bursts in
1979–1985 and 1998–1999. In addition, the time variationin each flux maximum show a symmetric flux increase/decrease with timescales of 2–7 months. The supermaser
is found to consist of two spatial/velocity components
with proper motions almost parallel to the northeastsouthwest bipolar outflow in Orion KL (Figure 2).
With the newly obtained ALMA data, we investigate
the physical properties of environment of the supermaser.
We find that the supermaser is located in the Compact
Ridge, which is an interacting region with the bipolar
outflow and the ambient cloud. We identify thesupermaser close to the methylformate (HCOOCH 3)
line and continuum emission peaks. The velocity
structure of the HCOOCH 3 line shows an evidenceof shocked molecular gas. On the other hand, we can
not detect submillimeter H 2 O lines in the Compact
Ridge, suggesting that the submillimeter H2O lines arethermalized.
Our results support a scenario that the supermaser
is excited in the shocked molecular gas in the Compact
Ridge, and it could be explained by a beaming effectduring the amplification process rather than changes inphysical conditions.

KURONO, Yasutaka

TSUBOI, Masato

IMAI, Hiroshi

YONEKURA, Yoshinori(NAOJ/JAO)		

(Kagoshima University)(ISAS/JAXA)(Ibaraki University)

Figure 1: Flux density variation of the 22 GHz supermaser
observed with VERA. Filled and open symbols represent
the total and correlated flux densities, respectively, forthe 7.5 km s−1 component.

Figure 2: Channel maps of the 22 GHz supermaser observed with
VERA. Each arrow indicates the proper motion vector.
Contour levels are 2000, 4000, 6000, 8000, 10000, and
12000 Jy beam−1. Gray arrows represent the absoluteproper motions while black arrows indicate the propermotion with respect to the powering source of thebipolar outflow, Source I.

References[1] Hirota, T., et al.: 2011, ApJ, 739, L59.
[2] Hirota, T., et al.: 2014, PASJ, 66, 106.

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Evidence for a Gas-Rich Major Merger in a Proto-Cluster at z = 2.5
TADAKI, Ken-ichi, KODAMA, Tadayuki

		(NAOJ)		

				
		

TAMURA, Yoichi

SHIMAKAWA Rhythm(SOKENDAI/NAOJ)

KOHNO Kotaro(University of Tokyo)		

HAYASHI, Masao, KOYAMA, Yusei(University of Tokyo)		

TANAKA, Ichi

(Subaru Telescope)

HATSUKADE, Bunyo(NAOJ)

Properties of galaxies seen in the local universe
strongly depend on their surrounding environments, as
is well known from the morphology–density relation.
Early-type galaxies are frequently observed in highdensity regions such as clusters and late-type galaxies arecommon in low-density regions. Such spatial segregation
could be related to formation processes and subsequent
quenching mechanisms of star formation, which probably
take place at high redshift. Given high number densitiesof star-forming galaxies in proto-clusters at z > 2, we
naturally expect a high frequency of major-merger events.
We have conducted CO J = 1 – 0 emission line
observations with the Jansky Very Large Array (JVLA)[1]. The target field is a proto-cluster at =2.53, USS1558003, including 20 Hα emitters (HAEs). We have detected
the CO emission line from three galaxies (ID 191, ID 193,
and ID 213) of our sample. Using MIPS 24 μm and JVLA33 GHz images, we derive a total infrared (IR) luminosityof L IR = 5.1 × 1012 L  for ID 193. Assuming that the bulkof the IR luminosity is powered by star formation, we
find ID 193 to have a high SFR of 886 M  yr–1.
The separation between ID 191 and ID 193 is about
4 arcsec corresponding to 32 kpc in the physical scale
and the velocity offset is 300 km s–1, suggesting that they
are probably in the initial stage of a merger. Moreover,the derived SFR of 886 M  yr–1 in ID 193 is higher by afactor of about seven with respect to the M*-SFR relationof normal HAEs (main~sequence) and is similar to thatof SMGs, where extremely high star formation is thought
to be driven by major mergers. In Figure 1, we also plot
ID 193 on the L IR-L'CO diagram to compare this withother populations taken from the literature. ID 193 has ahigher IR luminosity compared to normal star-forming
galaxies at a fixed CO luminosity and are situated close
to the regime of low-redshift ULIRGs.
Given a violent star-formation activity (SFR = 886
M  yr–1), high L IR/L'CO ratio (high SFE) and red opticalcolor, we interpret ID 193 as a star-bursting galaxy driven
by a gas-rich merger with ID 191 or another galaxy.

(NAOJ)SUZUKI, Kenta(University of Tokyo)

Figure 1: IR vs. CO J = 1 – 0 luminosities of ID 193 (red square)along with SMGs at z> 1 (green stars: [2,3,4]), ULIRGs
at z < 1 (green crosses: [5]), and optical/near-IR selected
star-forming galaxies at z> 1 (black circles: [6]). Dashedblack and red lines show the best-fitting relations fornormal star-forming galaxies and luminous mergers [7].

References[1] Tadaki, K., et al.: 2014, ApJL, 788, L23.
[2] Harris, A. I., et al.: 2010, ApJ, 723, 1139.
[3] Ivison, R. J., et al.: 2011, MNRAS, 412, 1913.
[4] Ivison, R. J., et al.: 2013, ApJ, 772, 137.
[5] Solomon, P. M., et al.: 1997, ApJ, 478, 144.
[6] Aravena, M., et al.: 2012, MNRAS, 426, 258.
[7] Genzel, R., et al.: 2010, MNRAS, 407, 2091.

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031

Near-Infrared Brightness of the Galilean Satellites
Eclipsed in Jovian Shadow:
A New Technique to Investigate Jovian Upper Atmosphere
TSUMURA, Kohji1, ARIMATSU, Ko2, EGAMI, Eiichi3, HAYANO, Yutaka2, HONDA, Chikatoshi4
KIMURA, Jun5, KURAMOTO, Kiyoshi6, MATSUURA, Shuji7, MINOWA, Yosuke2, NAKAJIMA, Kensuke8
NAKAMOTO, Taishi5, SHIRAHATA, Mai2, SURACE, Jason9, TAKAHASHI, Yasuto6, WADA, Takehiko10
1: Tohoku University, 2: NAOJ, 3: Arizona University, 4: University of Aizu, 5: Tokyo Institute of Technology, 6: Hokkaido University, 7:
Kwansei Gakuin University, 8: Kyushu University, 9: California Institute of Technology, 10: Japan Aerospace Exploration Agency

Using the Subaru Telescope and Hubble Space
Telescope, we have found that Ganymede and Callisto
remain slightly bright at near-infrared (~1.5 μm) evenwhen in the Jovian shadow and not directly illuminatedby the Sun (Fig. 1) [1]. Their eclipsed brightness was~10−6 of their uneclipsed brightness, which is low enoughthat this phenomenon has been undiscovered until now.
In addition, Europa in eclipse was not detected except
a rare case explained later. Likewise, Ganymede was
not detected at 3.6 μm by the Spitzer Space Telescope,suggesting a significant wavelength dependence (Fig. 2).
We considered several possibilities to understand why
the satellites remain ever-so-slightly bright even when
they are in eclipse. A possibility of illumination from
Jupiter by lightning, aurora, and nightside airglow wasinvestigated. However, it is difficult for these illuminators
to explain the fact that the brightness of Europa was muchdarker than the others because Europa was located closer
to Jupiter. Next possibility of atmospheric emission fromthe satellites was also rejected, because the non-detectionof Ganymede in eclipse at 3.6 μm is difficult to explain
by its atmosphere expected to have OH molecules (Fig. 2)[2]. Only once we detected Europa in eclipse, and it was
explained by sunlight reflected from Io out of eclipse
located near Europa on that day, but we also confirmedthat such reflection from other satellites out of eclipse
cannot explain the brightness of Ganymede and Callisto
in eclipse we detected.
The most plausible explanation is indirect forward
scattering of sunlight by hazes in the upper Jovian
atmosphere. Based on this theory, the fact that Europa
was darker than the others can be explained because theeffect of the scattered sunlight should be less at a satellite
closer to Jupiter. In addition, the similarity between
spectra of Jupiter and Ganymede in eclipse (Fig. 2) canbe also explained because Ganymede was illuminated by
the sunlight through Jovian upper atmosphere. If it is thecase, this new method of studying the upper atmosphereof Jupiter via transmitted sunlight provides a basis for the
study of the exoplanet atmosphere, whose atmosphereis investigated via transmitted starlight during transit
observations.

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Figure 1: Images of Ganymede (left) and Callisto (right) obtained
while they are eclipsed by Jupiter.

Figure 2: Spectral energy distribution of Ganymede in eclipse.
Spectra of Jupiter [3] and the Earths atmosphere [4] arealso shown, scaled to the Ganymede brightness.

References[1] Tsumura, K., et al.: 2014, ApJ, 789, 122.
[2] Marconi M. L.: 2007, Icarus, 190, 155.
[3] Rayner, J. T., et al.: 2009, ApJS, 185, 289.
[4] Stair A. T. Jr., et al.: 1985, J. Geophys. Res., 90, 9763.

Discovery of Extended Ionized Clouds in a Cluster of Galaxies at z~0.4
YAGI, Masafumi

		

			

GU, Liyi

NAKATA, Fumiaki, HATTORI, Takashi(NAOJ)		(SRON)				(NAOJ)

KOYAMA, Yusei, KODAMA, Tadayuki(NAOJ/SOKENDAI)			

Extended ionized clouds (EIGs) in intergalactic space
has been reported by several studies of nearby clusterof galaxies [1-8] The clouds are thought to be made by
ram-pressure stripping and/or galaxy interactions. Parent
galaxies of EIGs tend to show post-starburst signature,especially in lower mass galaxies [8]. The stripping of thegas is therefore thought to be an important mechanismof the evolution of galaxies in clusters. There is also
a study that the number of post-starburst galaxies in acluster increases with redshift and typical luminosity ofthe post-starburst galaxies is larger at z = 0.4 than ourneighborhood [9]. One can thus expect that there are
more EIGs at z = 0.4. Nevertheless, no systematic survey
has been tried so far.
There are two z ~ 0.4 cluster of galaxies obtained with
the Subaru prime focus camera (Suprime-Cam), whichhave narrow-band data of redshifted Hα at the cluster’s
redshift; Abell 851 (A851) and CL0024+17 (CL0024)[10-12]. We re-analyzed the data with an improved
method for extended objects and searched for EIGs. In
A851, we found 9 EIGs, while none in CL0024.
We then identified possible parent galaxy of the
9 EIGs in A851. Five have redshift information inliterature and/or unpublished data. We used Faint Objects
Camera and Spectrograph (FOCAS) of the Subaru
Telescope to obtain the rest 4, to confirm that all of the
9 parent galaxies are the member of A851. Moreover, in
30 × 25 arcmin of field of view of Suprime-Cam, the 9EIGs exist within 2.3 arcmin (750 kpc) from the center ofthe cluster. These results suggests that the EIGs exist in
A851 and they are ionized hydrogen clouds.
Six of the nine parents show an emission out of stellar
distribution (Fig. 1 top), which implies a ram-pressure
stripping. We also used Hubble Space Telescope (HST)
images to see the morphology. Four of the nine show
asymmetry in the distribution of stars (Fig. 1 bottom),which implies a recent galaxy interaction. The spectrum
and color of the parents shows that the parents are either
starforming galaxy or post-starburst one.
Regarding kinematics, we found that 6 or 7 EIG
parents belong to a subcluster of A851 which is now
infalling onto the main cluster. Compared with CL0024,
which has no EIGs, the infalling subcluster showsa higher fraction of EIG parents with a statisticalsignificance. Our result resembles an example in a nearcluster [3] that gas stripping is caused by the infall ofsubcluster.

YOSHIDA, Michitoshi(Hiroshima University)

Figure 1: Examples of EIG in A851. Top-left and top-center are
50 arcsec (270 kpc) square, and the others are 25 arcsec(140 kpc) square. North is top, and east to the left. (Left)
broad-band (z)-subtracted narrow-band (NB921) image
from Subaru Suprime-Cam archived data. White shows
strong emission in NB, and it corresponds to Hα at theA851 redshift. The red contour is 3σ isophote of NB-z,
and the green contour shows 90 % flux isophote of theparent galaxy. The enclosed black ring around objects
are artifacts caused by different seeing size of NB andz. (Center) Three color composite of NB921, z, and R.
Hα is red in this color assignment. (Right) ACS/HST
F816W image from the HST archive. The bottom galaxy(C2) shows asymmetric stellar distribution.

References[1] Gavazzi, G., et al.: 2001, ApJ, 563, L23.
[2] Yoshida, M., et al.: 2002, ApJ, 567, 118.
[3] Cortese, L., et al.: 2006, A&A, 453, 847.
[4] Yagi, M., et al.: 2007, ApJ, 660, 1209.
[5] Sun, M., et al.: 2007, ApJ, 671, 190.
[6] Yoshida, M., et al.: 2008, ApJ, 688, 918.
[7] Kenney, J. D. P., et al.: 2008, ApJ, 687, L69.
[8] Yagi, M., et al.: 2010, AJ, 140, 1814.
[9] Poggianti, B. M., et al.: 2004, ApJ, 601, 197.
[10] Kodama, T., et al.: 2004, MNRAS, 354, 1103.
[11] Koyama, Y., et al.: 2011, ApJ, 734, 66.
[12] Koyama, Y., et al.: 2013, MNRAS, 434, 423.
[13] Yagi, M., et al.: 2015, AJ, 149, 36.

I Scientific Highlights

033

Rapid Change of the Plasma Tail of C/2013 R1 (Lovejoy)						

YAGI, Masafumi(NAOJ)

KODA, Jin

(Stony Brook University)

KOYAMA, Yusei, KODAMA, Tadayuki

I Scientific Highlights

YOSHIDA, Michitoshi(NAOJ/SOKENDAI)			

In Dec. 2013, we had a time in morning twilight inan open use program of extragalactic objects with the
Subaru Prime Focus Camera. As a bright comet (C/2013
R1 (Lovejoy)) was seen, we took its image in I-band andV-band for educational and public outreach purposes. We
then found that the shape of the plasma tail changed in a
few minutes [1].
The comet was at 0.55 au from the earth, and suncomet-earth angle was 83°. 2 at the observation time. We
observed the plasma tail nearly edge-on, which is an
ideal condition for the study on the time variation of thestructure of the tail. The physical scale of the tail was
about 400 km/arcsec considering the slight inclination.
We quantitatively evaluated two changes of the shape,
which were first visually identified; a motion of two
knots in the tail and the change of the width of the tail.
The knots was detected and measured in unsharp-masked
images after masking of elongated background stars(Figure 1). In plasma tails of comets, we observe CO+
and H2O+ in I-band, while mainly CO+ in V-band. Thus
the difference of shapes in I- and V-bands may be due tothe difference of distribution of these ions. We howeverconsider that the same knots were observed in I and
V-bands, because the motion of the two knots in the Iand V-bands lie on the same relation as shown in Figure 2.
The speed of them are 20, 25 km/s along the tail, and 3.8,
2.2 km/s across the tail. The speed of knots along the tailwould correspond to the speed of the flow of the plasma
tail. The change of the width is then measured in I-band,considering the flow speed, and it was 8 km/s at each sidein 8 minutes (from the start of the first exposure to theend of the last exposure).
In Table 1, the speed of structures in plasma tails
along the tails in literature are summarized. The speed
obtained in this study, ~22 km/s, are less than half of theprevious studies. As we observed the knots near to the
nucleus (~300,000 km), the value may reflect the initial
speed of the tail before the acceleration by the solar wind.
However, three times larger speed was obtained in studyof 1P/Halley at a comparable distance from the nucleus.
We need to accumulate the data in order to identify whatis the key parameter to the speed; size of the structure,solar activity, ecliptic latitude, solar distance of the comet,
etc. Efficient observation strategy is required including a
use of large telescopes.

034

FURUSHO, Reiko(Tsuru University/NAOJ)(Hiroshima University)

Figure 1: Cutouts of unsharped masked images of the comet tail.
The nucleus to the top, the plasma tail is along y-axis,
and the two arrows show the knots. Six exposures wereshown in order of time from the left to the right. Black
horizontal line indicates 300,000 km distance from thenucleus. The knots moved downstream.

Figure 2: Motion of the two knots. Open and filled circle
correspond to each knot. The left panel shows motion
across the tail, the right along the tail. Left three data
points are in I-band, and right three are in V-band.

speed

Distancefrom nucleus

various [2]

44 ±10.9 km/s

< 107 km

1P/Halley [3]65.8 km/s

4 – 9×105 km

C/1996 B2 [4]99.2 km/s~5×106 km

C/1995 O1 [5]500 km/s~7×107 km

50 –100 km/s
20 –25 km/s

~106 kmcomet

C/2001 Q4,
C/2002 T7 [6]C/2013 R1 (this work)~3×105 km

Table 1: Speed of structures in comet tails.

References[1] Yagi, M., et al.: 2015, AJ, 149, 36.
[2] Niedner, M. B. Jr.: 1981, ApJS, 46, 141.
[3] Saito, T., et al.: 1987, A&A, 187, 209.
[4] Kinoshita, D., et al.: 1996, PASJ, 48, L83.
[5] Brandt, J. C., et al.: 2002, Earth, Moon, and Planets, 90, 15.
[6] Buffington, A., et al.: 2008, ApJ, 677, 798.

Studying Near-Infrared Extragalactic Backgroundwith the Cosmic Infrared Background ExpeRiment-2 (CIBER-2)
SHIRAHATA, Mai

MATSUURA, Shuji, ARAI, Toshiaki, WADA, Takehiko(NAOJ)					SANO, Kei

(University of Tokyo)(ISAS/JAXA)				

ONISHI, Yosuke(Tokyo Institute of Technology)		

TSUMURA, Khoji(Tohoku University)

MATSUMOTO, Toshio(ASIAA)

BOCK, James, ZEMCOV, Michael, KORNGUT, Phillip(Caltech/JPL)

LANZ, Alicia, HRISTOV, Viktor, BATTLE, John, MASON, Peter, MORFORD, Tracy(Caltech)

COORAY, Asantha

LEE, Dae-Hee				(University of California)		 (KASI)

We present the current status of the Cosmic Infrared
Background ExpeRiment-2 (CIBER-2) project, whose
goal is to make a rocket-borne measurement of theCosmic Infrared Background (CIB), under collaborate
with U.S.A., South Korea, and Taiwan.
The extragalactic background is the integrated lightof all extragalactic sources of emission back to the early
Universe. At near-infrared wavelengths, measurementof the CIB is a promising way to detect the diffuse lightfrom the first collapsed structures at redshift z ~ 10, which
are impossible to detect as individual sources. However,recently, the intra-halo light (IHL) model [1] is advocatedas the main contribution to the CIB, and our new resultof the CIB fluctuation [2] is also supporting this model.
In this model, CIB is contributed by accumulated lightfrom stars in the dark halo regions of low-redshift (z<2)
galaxies, those were tidally stripped by the interactionof satellite dwarf galaxies. Thus, in order to understandthe origin of the CIB, both the spatial fluctuation
observations with multiple wavelength bands and theabsolute spectroscopic observations for the CIB are
highly required.
After the successful initial CIBER experiment [3],we are now developing a new instrument CIBER-2 [4],which is a sounding-rocket borne payload comprisinga 28.5-cm aluminum telescope and three broad-band,wide-field imaging cameras (Fig. 1). The three widefield (2.3 × 2.3 degrees) imaging cameras use the 2K ×2K
HgCdTe Hawaii-2RG arrays, and cover the near-infrared
wavelength range of 0.5–0.9 μm, 0.9–1.4 μm and 1.4–2.0
μm, respectively. Combining a large area telescope withthe high sensitivity detectors, CIBER-2 will be able tomeasure the spatial fluctuations in the CIB after removing
foreground point-sources at a > 24 AB-mag limit.
Additionally, we will use a linear variable filter installed
just above the detectors so that a measurement of theabsolute spectrum of the CIB is also possible.
In the year of 2014, the conceptual design of the
instruments and the development of new technology havebeen completed. The lens fabrications, the manufactureof the lens barrel, and telescope assembly will be done in
the year of 2015, and the performance evaluation test at
the LN2 temperature is also scheduled. CIBER-2 plans atleast two flights in the same configuration described here.
The first flight is planned for 2016 with the second flight
to follow six months or one year later.

Figure 1: Model of the CIBER-2 instrument. A 28.5 cm Cassegrain
telescope directs light into the imaging optics, where
beam splitters divide the light into three imaging optics(Arm-S, Arm-M, Arm-L). Each optical path travels to
one of three focal plane assemblies, where a broadband
filter subdivided the light into two wavelength bands
which are both recorded by a single detector array fora total of 6 bands. A small segment of each detector
array is also covered by a linear-variable filter. The
imaging optics is mounted to an optical bench thatconnects the Cassegrain telescope assembly to a liquid
nitrogen cryostat. Radiative shielding is provided by aradiatively-cooled door and cryogenically-cooled popup baffle that extends during observations.

References[1] Cooray, A., et al.: 2012, Nature, 490, 514[2] Zemcov, M., et al.: 2014, Science, 346, 6210.
[3] Zemcov, M., et al.: 2013, ApJS, 207, 31.
[4] Lanz, A., et al.: 2014, Proceedings of the SPIE, 9143, 91433N.

I Scientific Highlights

035

A Study on the Methyl Formate
in Its Ground and Torsional Excited States
Toward Orion KL Using ALMA Sceience Verication Data		HIROTA, Tomoya(SOKENDAI/NAOJ)		

KOBAYASHI, Kaori, SAKAI, Yusuke(University of Toyama)

Methyl formate (HCOOCH 3) was first identified
toward Sgr B2 [1] and more than 1000 transitions wereidentified in the star-forming regions including Orion
Kleinmann-Low (KL) since then. Methyl formate has
an internal rotor which is equivalent to the torsional
vibration. This mode is a low-lying state. The rotationaltransition in the first torsional excited state of thismolecule was firtst identified toward Orion KL in 2007[2]. In 2012, even transitions in the second torsional
excited state were observed by using the Nobeyama 45 m
Radio Telescope [3].
In this study, we analyzed the ALMA science
verification data of Orion KL (band 6) that contains manytransitions in the ground and torsional excited states. It
was confirmed in the previous study [3] that there is adifference between the vibrational temperature and therotational temperature. The higher spatial resolution ofthis new ALMA data will help us to clarify the difference.
Figure 1 shows the integrated intensity maps of methyl
formate. These maps shows the similarity of populationin each vibrational state. We have analyzed two velocity
components toward the Compact Ridge and one velocity
component toward the Hot Core. It was confirned that thevibrational temperature and the rotational temperature ofeach component agreed within their uncertainties [4].

Figure 1: Integrated intensity maps of methyl formate in the
ground, the first torsional excited, the second torsional
excited states. The green circles shown represent theCompact Ridge and Hot Core.

References[1] Brown, R. D., et al.: 1975, ApJ, 197, L29.
[2] Kobayashi, K., et al.: 2007, ApJ, 657, L17.
[3] Takano, S., et al.: 2012, PASJ, 64, 89.
[4] Sakai, Y., Kobayashi, K., Hirota, T.: 2015, ApJ, 803, 97.

036

I Scientific Highlights

Discovery of a Disk Gap Candidate at 20 AU in TW Hya
AKIYAMA, Eiji1, MUTO, Takayuki2, KUSAKABE, Nobuhiko1, KATAOKA, Akimasa3, HASHIMOTO, Jun1
TSUKAGOSHI, Takashi4, KWON, Jangmi5, KUDO, Tomoyuki1, KANDORI, Ryo1, GRADY, Carol A.6
TAKAMI, Michihiro7, JANSON, Markus8, KUZUHARA, Masayuki9, HENNING, Thomas10
SITKO, Michael L.11/12, CARSON, Joseph10/13, MAYAMA, Satoshi14, CURRIE, Thayne1
THALMANN, Christian15, WISNIEWSKI, John P.16, MOMOSE, Munetake4, OHASHI, Nagayoshi1, ABE, Lyu17
BRANDNER, Wolfgang10, BRANDT, Timothy D.18, EGNER, Sebastian1, FELDT, Markus10, GOTO, Miwa19
GUYON, Olivier1, HAYANO, Yutaka1, HAYASHI, Masahiko1, HAYASHI, Saeko1, HODAPP, Klaus W.20
ISHII, Miki1, IYE, Masanori1, KNAPP, Gillian R.18, MATSUO, Taro21, MCELWAINE, Michael W.22
MIYAMA, Shoken23, MORINO, Jun-Ichi1, MORO-MARTIN, Amaya24/25, NISHIMURA, Tetsuro1
PYO, Tae-Soo1, SERABYN, Eugene26, SUENAGA, Takuya14, SUTO, Hiroshi1, SUZUKI, Ryuji1
TAKAHASHI, Yasuhiro1/5, TAKATO, Naruhisa1, TERADA, Hiroshi1, TOMONO, Daigo1, TURNER, Edwin L.5/18
WATANABE, Makoto27, YAMADA, Toru28, TAKAMI, Hideki1, USUDA, Tomonori1, TAMURA, Motohide1/5
1: NAOJ, 2: Kogakuin University, 3: University of Heidelberg, 4: Ibaraki University, 5: The University of Tokyo, 6: Eureka Scientific, 7:
Academia Sinica, 8: Stockholm University, 9: Tokyo Institute of Technology, 10: Max Planck Institute for Astronomy, 11: Space Science
Institute, 12: University of Cincinnati, 13: College of Charleston, 14: The Graduate University for Advanced Studies, 15: ETH Zurich, 16:
The University of Oklahoma, 17: Universite de Nice Sophia-Antipolis, 18: Princeton University, 19: Universitäts-Sternwarte München, 20:
University of Hawaii, 21: Kyoto University, 22: Goddard Space Flight Center, 23: Hiroshima University, 24: Space Telescope Science Institute,
25: Johns Hopkins University, 26: Jet Propulsion Laboratory, 27: Hokkaido University, 28: Tohoku University

Explorations and studies of protoplanetary disks
reveal important physical processes that are fundamental
to the formation and evolution of planetary systems.
As part of the Strategic Explorations of Exoplanets
and Disks with Subaru (SEEDS) project for exploring thecircumstellar disk structure, TW Hya, an analog of theearly solar nebula, was selected because it is particularly
accommodating to investigations of its geometricalstructure with high spatial resolution and sensitivity due
to its close distance of 54 pc.
As results of the observations, the scattered light fromthe disk was detected from 0.2 to 1.5 asec (11–81 AU)
from the central star and the polarized image shows aring-like depression, probably a gap at ~20 AU from thecentral star as shown in Fig. 1 [1], similar to the 80 AU
gap previously reported from the Hubble Space Telescope(HST) images [2]. Several gap formation mechanisms,
such as disk–planet interaction, photoevapolation,
grain growth, or dust filtration, has been proposed. Our
observation suggests the possibilities of planet formationand grain growth because the observed radial profile canwell be explained by the gap formation model by a planet[3] and the observed depression can also be reproduced
by a change in dust scale height due to grain growth.
In addition to the HST result, our observation revealed
the multiple ring-like gap structure in TW Hya, implyingthat multiple planets are forming as a planetary system.
In near future, ALMA and next-generation astronomical
telescope, TMT, will provide convincing information
about the origin of gaps and shed new light on planet
formation.

Figure 1: H-band polarized intensity image of TW Hya. The dark
filled circle at the center indicates a software mask withr = 0.2 asec.

References[1] Akiyama, E., et al.: 2015, ApJ, 802, L17.
[2] Debes, J. H., et al.: 2013, ApJ, 771, 45.
[3] Jang-Condell, H., Turner, N. J.: 2012, ApJ, 749, 153.

I Scientific Highlights

037

Revised Big-Bang Nucleosynthesis with Exotic Dark Matter Particle:
Detailed Quantum Mechanical Calculation
KUSAKABE, Motohiko(Korea Aerospace University/Soongsil University)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

KIM, K. S.

(Korea Aerospace University)

KINO, Yasushi(Tohoku University)		

We extensively reanalyze effects of an exotic longlived negatively charged massive particle [1], i.e., X −, on
big bang nucleosynthesis (BBN). The BBN model with
the X − particle was suggested to explain the discrepancy
between 6,7Li abundances predicted in standard BBN
model and those inferred from spectroscopic observationsof metal-poor stars (e.g., [2]). In this model, 7Be is
destroyed via the recombination with X − followed byradiative proton capture, i.e., 7Be(X −,γ) 7Be X (p,γ) 8B X
[3,4].
First, we study the effects of uncertainties in nuclear
charge distributions for X-nuclei in BBN. We showthat different charge distributions can result in resonant
nuclear reaction rates that differ by significant factors
through changes in resonance energy heights.
Second, we calculate precise rates for the radiative
recombinations of 7Be, 7Li, 9Be, and 4He with X −. We
calculate nonresonant rates taking account of respective
partial waves of scattering states and respective boundstates. It is found that the finite sizes of nuclear charge
distributions cause deviations in bound and continuum
wave functions from those derived assuming that nuclei
are point charges. We find that for a heavy mass, m X>~ 100 GeV, the transition, d-wave → 2P, is the mostimportant recombination reaction for 7Li and 7,9Be withan X − particle. This fact is completely different from thecase of hydrogen-like electronic ions. As for 7Be and 7Li,
bound states of the nuclear first excited states (7Be* and7Li*) with X − can operate as effective resonances. The
resonant reaction rates are then also calculated.
Figure 1 shows rates for the nuclear recombination
with X − as a function of temperature T 9 = T/(10 9 K)
for mX = 1000 GeV. Curves correspond to the sums of
nonresonant and resonant reaction rates. The new rates for
7Be, 7Li, and 9Be are larger than the previous rates, whilethat for 4He is smaller than the previous rate. Importantly,
the 7Be rate in the present study is more than 6 times
larger than the existing rate. This improvement leads to asignificantly better constraint on the X − properties. The
present rates for 7Li and 9Be are also significantly larger
than the previous rates. The present 4He rate is, on theother hand, not significantly different for temperatures T9<~ 0.1 where the recombination effectively proceeds.
Third, we suggest a new reaction for 9Be production:
the radiative recombination of 7Li and X − followedby the deuteron capture. This reaction can enhance the038

I Scientific Highlights

CHEOUN, Myung-Ki(Soongsil University)

MATHEWS, Grant. J.

(University of Notre Dame)primordial 9Be abundance which may be detectable infuture observations of metal-poor stars.
We derive binding energies and mass excessesof X-nuclei, and rates and Q-values for β-decays andnuclear reactions involving the X − particle. We calculate
BBN and find that amounts of 7Be destruction depend
significantly on the charge distribution of the 7Be nucleus.
Finally, the most realistic constraints on the initialabundance and the lifetime of the X − are deduced.
Parameter regions for the solution to the 7Li problem arederived, and primordial 9Be abundances in the parameterregions are also predicted.

Figure 1: Total rates for nuclear recombination with X − in thecase of mX = 1000 GeV as a function of temperature.
Solid lines show the recombination rates derived in thisstudy, while dashed lines show the rates adopted in theprevious studies (e.g., [3,4]). This is reprinted from [5].

References[1] Cahn, R. N., Glashow, S. L.: 1981, Science, 213, 607.
[2] Aoki, W., et al.: 2009, ApJ, 698, 1803.
[3] Bird, C., et al.: 2008, Phys. Rev. D, 78, 083010.
[4] Kusakabe, M., et al: 2008, ApJ, 680, 846.
[5] Kusakabe, M., et al.: 2014, ApJS, 214, 5.

Asymmetric Neutrino Emission from Magnetized Proto-Neutron Stars:
Effects of Absorption Cross-Sections in Iso-Entropical Conditions [1]		

MARUYAMA, Tomoyuki(Nihon University)		

YASUTAKE, Nobutoshi(Chiba Institute of Technology)		

KAJINO, Toshitaka(NAOJ/University of Tokyo)

CHEOUN, Myung-Ki, RYU, Chung-Yeol(Soongsil University)		

In our previous works [2], we calculated neutrino
scattering and absorption cross sections on hot and dense
magnetized proto-neutron-star (PNS) matter including
hyperons under a strong magnetic field in a relativistic
mean field (RMF) theory. The calculation results showedthat the magnetic contribution increases the neutrino
momentum emitted along the direction parallel tothe magnetic field and decrease it along the opposite
direction.
These works have been done in the isothermal model,
which is not realistic because the temperature decreaseas the radial position becomes farther from the center of
the PNS. In addition, the mean-field used in the previous
works cannot allow neutron stars mass of 2 M.
To get more realistic results, we introduce the newparameter-sets of RMF and calculate the neutrino crosssections in the isoentropic conditions. Fig. 1 shows total

HIDAKA, Jun(Meisei University)

MATHEWS, Grant. J.

(University of Notre Dame)energies per baryon, temperature profiles, and number
fractions for constituent particles in an isoentropic systemwith entropy per baryon S/A = 1.
In Fig. 2, we show the magnetic part of the absorption
cross-section as a function of the initial neutrino angle inthe matter with S/A =1 and B = 1018 G.
At ρ B = ρ 0 , the magnetic field suppresses theabsorption cross-sections in a direction parallel to themagnetic field by about 8.3 % for an entropy per baryon
of S/A = 1. The suppression of σA for S/A = 1 at ρB = ρ0
turns out to be much larger than in an isothermal modelwith T = 20 MeV, because the temperature at this density
in the isoentropic model is only about T = 7 MeV. At
lower temperature the magnetic contribution becomeslarger. However, at higher densities and temperatures the
suppression is comparable in the two models.

Figure 2: Ratio of the magnetic part of the absorption crosssection ΔσA to the cross-section without a magneticfield σA0. The thick and thin lines indicate the results formatter with and without Λs, respectively. The strengthof the magnetic field is B = 1018 G, and neutrino incident
energies are taken to be equal to the neutrino chemical
potentials.

Figure 1: Density dependence of the total energy per baryon ET /A(a), Temperature T (b) and proton fractions xp of neutronstar matter at a lepton fraction YL = 0.4 and for entropy
per baryon S/A = 1. Solid and dashed lines represent
results with and without Λ particles, In the lower panel (c)a dot-dashed line indicates the xΛ fraction.

References[1] Maruyama, T., et al.: 2014, Phys. Rev. D, 90, 067302.
[2] Maruyama, T., et al.: 2012, Phys.Rev. D, 86, 123003.

I Scientific Highlights

039

Cosmological Solutions to the Big-Bang Lithium Problem:
Big-Bang Nucleosynthesis with Photon Cooling,
X-Particle Decay and a Primordial Magnetic Field		

YAMAZAKI, Dai G.
(NAOJ) 		

			

KUSAKABE, Motohiko(Korea Aerospace University/Soongsil University)

MATHEWS, Grant. J.

(University of Notre Dame)

The 7 Li abundance calculated in BBN with thebaryon-to-photon ratio fixed from fits to the CMB power
spectrum is inconsistent with the observed lithium
abundances on the surface of metal-poor halo stars.
Previous cosmological solutions proposed to resolve
this 7Li problem include photon cooling (possibly via
the Bose-Einstein condensation of a scalar particle)or the decay of a long-lived X-particle (possibly thenext-to-lightest supersymmetric particle). In this paper
we reanalyze these solutions, both separately and inconcert. We also introduce the possibility of a primordial
magnetic field (PMF) into these models. We constrain
the X-particles and the PMF parameters by the observed
light element abundances using a likelihood analysis toshow that the inclusion of all three possibilities leads toan optimum solution to the lithium problem. We deduceallowed ranges for the X-particle parameters and energy
density in the PMF that can solve 7Li problem.
We have calculated BBN taking into account threepossible cosmological extensions of the standard BBN.
These include photon cooling, the radiative decay of
X particles, and the possible existence of a PMF. In
particular, we consider the possible combination of all
three paradigms simultaneously in a new hybrid model.
We then utilized a maximum likelihood analysis todeduce constraints on the parameters characterizing the
X particles (τ X [s], ζ X [GeV]) and the energy density of the
PMF (ρB = B2/8π) from the observed abundances of lightelements up to Li.
From Fig. 1, as a result, we obtained ranges for the
X-particle parameters given by
4.06 < log (τ X [s]) < 6.10 (95 % C.L.),−9.70 < log (ζ X [GeV]) < −6.23 (95 % C.L.),
also find that the hybrid model with a PMF gives thebetter likelihood than that without a PMF, and the best fit
and 2σ upper bound on the energy density of the PMF are
B = 1.89 nG at a = 1.0 (the best fit),
B < 3.05 nG at a = 1.0 (95 % C.L.),
We discussed the degeneracy between the parametersof the X particle and the PMF. Since the parametersof X particle are mainly constrained by the D and 7Li
abundances, while the energy density of the PMF isconstrained by the 4He abundance, we found there are no
significant degeneracies between parameters of the PMF
and the X particle.

040

I Scientific Highlights

KAJINO, Toshitaka(NAOJ/University of Tokyo)

CHEOUN, Myung-Ki(Soongsil University)

Figure 1: Constraint on the X particle parameters and the PMF
strength and energy density.

Reference[1] Yamazaki, D. G., et al.: 2014, Phys. Rev. D, 90, 023001.

Supernova Nucleosynthesis of 26Al and Nuclear Structure of 26Si [1]
KOMATSUBARA, T.

(Institute for Basic Science)

KUBONO, S.

(RIKEN)			

OZAWA, A., ITO, Y., ISHIBASHI, Y.

(INFN, Catania)

			(JAEA)MORIGUCHI, T.

(University of Tsukuba)		

HAYAKAWA, S.

HAYAKAWA, T., SHIZUMA, T.

(NCCCRI)			

BINH, Dam Nguyen(Vietnamese Academy for Science and Technology)

SETOODEHNIA, K.

(University of Notre Dame)

The level scheme above the proton threshold in 26Si
is crucial for evaluating the 25Al( p, γ)26Si stellar reaction,
which is important for understanding the astrophysicalorigin of the long-lived cosmic radioactivity 26Al (T1/2 =7.17×105 y) in the Galaxy. The β-delayed γ-ray from the
26Al was measured by satellite γ-ray telescope. Therefore,
the 26 Al is considered to be created in supernovae,
classical novae, and massive stars. Because the half-lifeof this isotope is much shorter than the age of the Galaxy,it has been continuously created reached equilibrium
value.
The isotope 26Al is produced the nucleosynthesis
flow of 25Al (e+ ν)25Mg ( p, γ)26Al. There is a bypass flow
25Al ( p, γ)26Si (e+ ν)26mAl (e+ ν)26Mg, that does not emit
the characteristic γ-ray. Therefore, the 25Al ( p, γ) 26Si
reaction is a key reaction to evaluate the production of the
26Al. The reaction rate of the (p, γ) reaction is dominatedby narrow-resonant reactions with 0+, 1+, and 3+ states.
Those are sensitive to their excitation energies above theproton threshold in 26Si.
The excited states in 26Si have been studied using
an in-beam γ-ray spectroscopy technique with the24Mg (3He, nγ)26Si reaction. γ-rays emitted from excitedstates in 26Si have been measured using large volume
HPGe detectors. As the result of the experiments the level
scheme of 26Si is shown in Figure 1. The 0+ and 1+ states
were well observed above the proton threshold. The spinparity of one of the most important states at 5890.0keV has been assigned as 0+ by γ – γ angular correlation
measurements in this work.
According to the newly determined excitationenergies the astrophysical nuclear reaction rate is
calculated as a function of temperature T 9 as shownin Figure 2. The contribution of the 0 + resonance ismodestly increased; however, the role of the 3+ level isstill dominant as discussion [2]. In order to elucidate theabundance of galactic 26Al more extensive effort might
be essential to observe the crucial 3+ state just above theproton threshold.
References[1] Komatsubara, T., et al.: 2014, Euro. Phys. Jour. A, 50, 136.
[2] Parikh, A., José, J.: 2013, Phys. Rev. C, 88, 048801.

YAMAGUCHI, H., KAHL, D.
(CNS)

CHEN, A. A., CHEN, J.
(McMaster University)

KAJINO, T.

(NAOJ/University of Tokyo)

Figure 1: Level scheme of 26Si. The 0+ level at 5890 keV above theproton threshold has been observed with present work.

Figure 2: Astrophysical reaction rate NA<σv> for the 25Al(p,γ)26Si
reaction. Resonance reactions through 0+, 1+, and 3+ are
shown as well as the direct component DC. Contribution
by the 3+ is dominant at high temperature.

I Scientific Highlights

041

Accelerated Evolution of the Lyα Luminosity Function at z >~7
Revealed by the Subaru Ultra-Deep Survey
KONNO, Akira, OUCHI, Masami, ONO, Yoshiaki, SHIMASAKU, Kazuhiro, SHIBUYA, Takatoshi(University of Tokyo)

				

FURUSAWA, Hisanori(NAOJ)			

NAKAJIMA, Kimihiko(Observatoire de Geneve)

NAITO, Yoshiaki, MOMOSE, Rieko, YUMA, Suraphong				(University of Tokyo)				

Cosmic reionization is an event where protons andelectrons being combined at z ~ 1100 were reionized.
Lyα photons emitted from Lyα emitters (LAEs) at theepoch of reionization (z >~ 6) would be attenuated by
the neutral hydrogen (HI) in the intergalactic medium(IGM) around the LAEs. Therefore, evolution of the Lyαluminosity function (LF) is used as a probe of cosmic
reionization. In previous studies, whether or not the Lyα
LF evolves from z = 6.6 is debated [1,2]. Observations
for z ~ 7.3 LAEs with Subaru telescope have also been
conducted [3]. However, they cannot clearly conclude
whether the Lyα LF evolves from z = 6.6 to ~ 7.3 due tothe relatively shallow imaging that just reaches the bright
Lyα luminosity limit of L(Lyα) ~ 1.0 × 1043 erg s−1.
To solve the debate, one needs to detect a number of z
= 7.3 LAEs down to the Lyα luminosity limit comparable
to those of z = 6.6 LAE samples, and to derive the Lyα
LF at z = 7.3 with a good accuracy. We have developed
a new custom narrowband filter, NB101, to detect faintLAEs at z = 7.3. Since our NB101 has a significantly
narrower/sharper FWHM than filters used in the previous
Subaru z ~ 7.3 surveys, NB101 is more sensitive to anemission line than these filters. Using Subaru/SuprimeCam with our NB101, we have observed SXDS andCOSMOS fields (~ 0.5 deg2) with a total integration timeof 106 hr, which is one of the longest ever performed at
Subaru telescope. We have reached a limiting luminosityof L (Lyα) = 2.4 × 10 42 erg s −1 , which is about fourtimes deeper than those achieved by the previous Subaru
studies for z ~ 7.3 LAEs and comparable to the luminosity
limits of previous Subaru z = 3 – 6 LAE surveys. Our
observations allow us to derive the Lyα LF at z = 7.3 withan unprecedented accuracy.
We identify in total of seven LAEs at z = 7.3 (Fig. 1)
and conclude that the Lyα LF decreases from z = 6.6
to 7.3 at the >90 % confidence level [4]. Moreover, bycalculating the Lyα luminosity densities, we find a rapid
decrease of the Lyα LF at z ~ 7 for the first time (Fig. 2).
Because no such accelerated evolution of the ultraviolet(UV) LF or the cosmic star formation rate (SFR) is foundat z ~ 7, this accelerated Lyα LF evolution is explained byphysical mechanisms different from a pure SFR decrease[4]. By the comparison of simple theoretical models, weestimate the HI fraction, xHI, of IGM at z = 7.3. However,042

I Scientific Highlights

IYE, Masanori(NAOJ)

because there is a possible tension between our x HI
estimate and the measurements of Thomson scattering
optical depth of cosmic microwave background, theaccelerated Lyα LF evolution cannot be explained by asimple scenario of rapid increase of xHI [4]. These results
may support new physical pictures suggested by recent
theoretical studies, such as the existence of HI clouds
within cosmic ionized bubbles [5]. We refer the reader toour published paper [4] for more details.

Figure 1: Color composite images of z = 7.3 LAEs found in the
NB101 ultra-deep imaging survey [6].

Figure 2: Evolution of Lyα (red) and UV (blue) luminosity
densities [4]. The evolution of Lyα luminosity density
is accelerated at z >~ 7, while the UV luminosity density
rapidly decreases at z >~ 8.
References[1] Hibon, P., et al.: 2010, A&A, 515, A97.
[2] Clement, B., et al.: 2012, A&A, 538, A66.
[3] Shibuya, T., et al.: 2012, ApJ, 752, 114.
[4] Konno, A., et al.: 2014, ApJ, 797, 16.
[5] Bolton, J. S., et al.: 2013, MNRAS, 429, 1695.
[6] Subaru web release (2014/11/18).

Opacity of Fluffy Dust Aggregates						

KATAOKA, Akimasa(SOKENDAI/NAOJ)		

TANAKA, Hidekazu(Hokkaido University)		

Planetesimals are believed to form by coagulation ofdust grains in protoplanetary disks [1]. How micron-sized
dust grains grow to kilometer-sized planetesimals has
been an unsolved problem toward the complete planet
formation theory; the intermediate-sized bodies havebeen believed to be poorly sticky, easily disrupted bycollisions, or to quickly fall onto the central star.
On the other hand, observations on protoplanetarydisks have put a constraints on planet formation theory.
The sub-mm emission of the disk carries informationof dust grains in protoplanetary disks because theemission is believed to be optically thin and thus it
directly reflects the opacity of dust grains. In addition
to SMA or CARMA, the launch of ALMA enables us toinvestigate even the spatial distribution of dust grains
in protoplanetary disks. The proposed planetesimalformation theory should be tested by observations.
The recent study has shown that dust grains coagulate
in protoplanetary disks to form fluffy aggregates.
Theoretical studies have shown that the internal density of
dust aggregates is expected to be as small as 10−4 g cm−3[2]. Disk observations, on the other hand, are interpreted
as the emission from compact grains. The emission may
come from fluffy aggregates. Therefore, the previous
observations should be reinterpreted with highly porous
aggregates instead of compact grains. As a first step, in
this paper, we investigate the optical properties of suchhighly porous aggregates.
Figure 1 shows the main result of the paper [3]. If thedust aggregates have a radius a and the filling factor f,
the absorption opacity κ abs does not change if the productaf has a constant value. Figure 1 shows the case of af =1 mm (see the paper [3] for physical understanding).
This result suggests that the sub-mm emission of
protoplanetary disks might not be from millimeter-sizedcompact grains but from fluffy dust aggregates thathave 10 meter in size and 10−4 in filling factor. We also
proposed a way to distinguish between compact grains
and porous dust aggregates with spatial distribution ofspectral index of the sub-mm emission of protoplanetarydisks. It requires a high spatial resolution and a highsensitivity, which is achievable with ALMA. In near
future, therefore, ALMA observations is expected
to reveal whether there are fluffy dust aggregates inprotoplanetary disks.

OKUZUMI, Satoshi(Tokyo Institute of Technology)

NOMURA, Hideko(Tokyo Institute of Technology)

Figure 1: This figure represents κ abs [cm2 g−1] in the case of af =1 mm. Each line shows the cases of the filling factor of f
= 1, 10−1, 10−2, 10−3, 10−4.

References[1] Hayashi, C.: 1981, Prog. Theoret. Phys. Suppl., 70, 35.
[2] Kataoka, A., Tanaka, H., Okuzumi, S., Wada, K.: 2013, A&A,
557, L4.
[3] Kataoka, A., Okuzumi, S., Tanaka, H., Nomura, H.: 2014, A&A,
568, A42.

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043

Survey Observations of Geosynchronous Orbit Objects and Short-Term
Variability Observations Using the Time-Delay Integration Method
OKUMURA, Shin-ichiro(Japan Spaceguard Association/NAOJ)		
(Japan Space Forum)		

NISHIYAMA, Kota, TAKAHASHI, Noritsugu(Japan Spaceguard Association)		

The “Time-Delay Integration (TDI)” method is anelectronic scan technique which captures the image ofa moving object across the field of view. In this casean exposure is made by shifting electrical charge while
a mechanical shutter is open. To make the electronicscan, the CCD parallel registers (the CCD columns) are
precisely oriented in the direction of the moving object
and the clocking rate of parallel charge transfer must be
synchronized to the motion of the object. In its simplest
use in astronomy, the parallel transfer rate is tuned tosidereal rate, so that the charge is moving across the
CCD at the same rate as the sky moving across the fieldof view, when the telescope tracking is turned off. This
technique was used to perform the Sloan Digital Sky
Survey [1] and many other digital sky surveys.
In contrast to this method, the TDI technique can beapplied backwards in case of detecting geosynchronous
Earth orbit objects [2,3]. In this manner, the CCD chip isaligned such that its parallel registers are oriented in the
East-West direction but turned 180°. The telescope tracks
at sidereal rate and the charge on the CCD is shifted inreverse, also at the sidereal rate. The two sidereal rates
cancelled each other and the effect of Earth rotation isremoved.
To synchronize the parallel charge transfer rate to
the motion of the object, charge transfer timing can be
set by editing a clock pattern description file. For an
object drifting northward or southward, its drift motion
can be canceled by adjusting the mount position angleof the CCD, e.g., by using the mechanical Cassegrain
instrument rotator [3].
We also propose a new application method of getting
short-term light curves with TDI mode. When thestationary object is observed in TDI mode, it is imaged asa streak. The light curve is easy to extract from the streak,because the streak is sure to be horizontal. We applied
this technique to observe short-term light curves of spacedebris, with the telescope drive at the “track rate” (objecttracking) mode [3].
Figure 1 shows an example of the extraction of thelight curve of a geosynchronous object. Light curves of
the reference stars can also be extracted from the image
and used to correct the short-term variation in atmosphericconditions. The time resolution can be adjusted suitably
according to the brightness and the variable period of theobject. This method of detecting a short-term variability

044

I Scientific Highlights(JAXA)			

NAKAYA, Hidehiko(NAOJ)YOSHIKAWA, Makoto(JAXA/ISAS)

can be applied for a variety of objects such as stars, solar
system bodies, geosynchronous orbit objects, and low
Earth orbit objects. It can also be used for the light-curve
observations of transient objects which might show shortterm variability and of which the precise time informationis needed.

Magnitude

TANAKA, Wataru

YANAGISAWA, Toshifumi

Time (sec, start time: 2456051.150093 JD)
Figure 1: Example of the extraction of the light curve of ageosynchronous object. Upper: close-up of a TDI image
obtained with a 30-s exposure, lower: light curve of
the object, extracted from the upper image. Samplinginterval is 0.14 sec.

References[1] Gunn, J. E., et al.: 1998, AJ, 116, 3040.
[2] Gehrels, T.: 1991, Space Sci. Rev., 58, 347.
[3] Okumura, S., et al.: 2014, PASJ, 66, 115.

Statistical Analysis of Current Helicity andTwist in Solar Active Regions over the Phases of the Solar Cycle
Using the Spectro-Polarimeter Data of HinodeOTSUJI, Kenichi, SAKURAI, Takashi

				(NAOJ)				

Magnetic flux tubes in the solar convection layer
emerge to the surface and form sunspots and emerging
flux regions. The active regions including sunspots
have magnetic fields exceeding 3000 G and produce
many active phenomena. The magnetic field in an active
region can be twisted by the solar dynamo process
when it is generated, or by the interaction with theconvection motion during its ascent from the bottom of
the convection zone. To measure the twist of the field,
the current helicity was introduced. The current helicity
is derived from vector magnetic field components atthe solar surface, i.e. photosphere. The line-of-sight (z)component of current helicity HC z is,

KUZANYAN, Kirill(IZMIRAN)

more detailed and long period variations of the current
helicity on active regions, a larger statistical analysis
using SOT/SP data up to the current date (~2015) is now
ongoing.

(1)
where ··· represents the spatial averaging, x and y aresolar east-west and north-south directions, respectively.
From the definition, the right/left-handed helical field lines
are characterized by positive/negative current helicity.
The preceding studies found a tendency that the negative/
positive helicity is dominant in the northern/southernhemisphere. The data used for these studies are, however,obtained from the ground-based observations, whichsuffered from the atmospheric seeing effect and so on.
We have carried out a statistical study on thecurrent helicity of solar active regions observed with
the Spectro-Polarimeter (SP) of Hinode Solar Optical
Telescope (SOT). We used SOT-SP data of 558 vector
magnetograms of a total of 80 active regions obtained
from 2006 to 2012. This period covers from the end of
the solar cycle-23 to the middle of cycle-24. To avoid the
projection effect, we excluded the data obtained near thesolar limb. We divided the area of an active region intoweak (< 300 G) and strong (300 ~ 1000 G) field ranges tocompare the contributions from different field strengths.
Figure 1 shows the time-latitude diagram of current
helicity calculated for individial active regions. The colorand size of the circles indicate the sign and magnitude ofcurrent helicity.
The result of weak field area shows the same
distribution of current helicity as the preceding studies.
On the other hand, the strong field area shows the
opposite dependency, i.e. positive current helicity inthe northern hemisphere and negative in the south. This
opposite natures may come from the difference of theorigins of strong and weak magnetic fields. To investigate

Figure 1: The temporal-latitude diagram of current helicity forevery active regions observed by SOT/SP from 2006 to
2012. The upper/lower image represents the result of
the area with weak (< 300 G)/strong (300 ~ 1000 G) field
range, respectively.

Reference[1] Otsuji, K., Sakurai, T., Kuzanyan, K.: 2015, PASJ, 67, 6.

I Scientific Highlights045

Developments of Wide Field Millimeter/Submillimeter Instruments
SEKIMOTO, Y., NOGUCHI, T., KARATSU, K., NITTA, T.*, MATSUO, H., DOMINJON, A.
OKADA, N., MITSUI, K., TSUZUKI, T.
(NAOJ)SEKINE, M., SEKIGUCHI, S., OKADA, T., SHU, S.

			(University of Tokyo/NAOJ)			

MKID (Microwave Kinetic Inductance Detector)
group of Advanced Technology Center is developing
superconductive camera in millimeter and submillimeter
wavelengthes for Antarctica terahertz telescope whichobserves distant galaxies with a wide field of view andfor LiteBIRD which detects CMB B-mode polarizationin collaboration with University of Tsukuba, Saitama
University, KEK, and Riken. We reported four
papers with a theme of wide field of view millimter/submillimeter instruments in 2014 fiscal year.
1. Wide Field 0.1 K Cryosytem [1]
MKID camera which is a new technology (P.
Day et al. 2003) is a Cooper pair breaking detector.
Superconducting resonators in MKID sense surface
impedance variations owing to quasi-particles generate
by incoming photons. It is necessary to cool MKID to1/7of the superconducting critical temperature (Tc). We havedeveloped a compact 0.1 K cryosystem (Fig. 1) with adilution refrigerator by Taiyo Nissan Co. As a result, an
MKID detector of Tc = 700 mK can be operated in thiscryostat, which can detect photons of higher frequencies
than 50 GHz. The key to the wide field of view is a large
diameter silicon lens and its anti-reflection coating.
Moreover, nested reflective baffles reduce stray lights.

NARUSE, M.

(Saitama University)

four reflective mirrors and one cooling refractive. The
free-forming surface is used for the mirrors to expand
the FoV. The cooling lens is an alumina lens of 60 cm inthe diameter. Wide FoV survey at terahertz is realized by
combining 20000 pixels MKID camera.
3. 700 pixels Si Lens Array [3]To detect submillimeter-waves efficiently, the camera
combined a lens array with superconducting planarantenna. A 700 pixels silicon lens array was machinedwith a high-speed spindle (Figure 2). Moreover, a mixed
epoxy anti-reflection coating [5] was applied with thesame way. The thickness of the ARC is controlled with
1 % accuracy. With these technologies, superconducting
cameras with high efficiency became possible.

Figure 2: 700 pixels Si lens array and 220 GHz MKID camera.

Figure 1: Compact 0.1 K cryosystem [1] and wide FoV (1.0
degree) terahertz optics [2].

2. Wide Field Terahertz Optics [2]A wide field of view (FoV) optics with a main
observation frequency 0.85 THz of Antarctica 10 m
terahertz telescope has been designed (Figure 1). It relays
from a F #6 Nasmyth focus to a F #1 detector focus with
* JSPS PD fellow, from 1-Apr-2015, Univ. of Tsukuba

046

I Scientific Highlights

4. CMB B-mode Polarization [4]Observations of B-mode polarization of cosmic
microwave background radiation (CMB) sense theinflation theory (K. Sato 1981). This paper reports
MKID developments in collaboration with NAOJ, KEK,
Riken. It demonstrates noise of the detector, the beammeasurement, and the readout circuit. The polarization
sensitivity is higher than that of BICEP2.
At ATC, we are developing broad band devices with
MKIDs as well as wide FoV instruments.
References[1] Sekiguchi, S., et al.: 2015, IEEE TST, 5, 49.
[2] Tsuzuki, T., et al.: 2015, JATIS, 1, 025002.
[3] Mitsui, K., et al.: 2015, JATIS, 1, 025001.
[4] Karatsu, K., et al.: 2015, IEICE 98-C, 207.
[5] Nitta, T., et. al.: 2014, JLTP, 176, 677.

The Gas Inflow and Outflow Rate in Star-Forming Galaxies at z ~ 1.4
YABE, Kiyoto*(University of Tokyo/Kavli IPMU)

OHTA, Kouji

AKIYAMA, Masayuki(Kyoto University)

TAMURA, Naoyuki(University of Tokyo/Kavli IPMU)(Tohoku University)

YUMA, Suraphong(University of Tokyo/ICRR)		

The gas flow into and out of galaxies have asignificant impact on the formation and evolution ofgalaxies. The outflow of enriched gas causes the decreaseof the gas metallicity (hereafter metallicity) of galaxies
and results in a presence of the stellar mass-metallicity
relation of galaxies. Feedback from outflows plays animportant role for the star-formation activity and thestructure formation of a galaxy. On the other hand,
the inflow of gas into galaxies is relatively difficult toobserve. In this work, we try to constrain the gas inflow
and outflow rate of star-forming galaxies at z ~ 1.4 byemploying a simple analytic model for the chemical
evolution of galaxies. The sample is constructed basedon a large near-infrared (NIR) spectroscopic sample
observed with Subaru/FMOS [1].
The sample used in this work is originated fromthe K-band selected galaxy sample in the Subaru
XMM-Newton Deep Survey and UKIDSS Ultra Deep
Survey field (SXDS/UDS). We selected galaxies withK ≤ 23.9 mag, phot-z of 1.2 ≤ z ph ≤ 1.6, the stellar
mass of M* ≥ 109.5 M, and the expected Hα flux of
F (Hα) ≥ 5×10 −17 erg s −1 cm −2 . During the FMOS/
GTOs, engineering runs, and open-use observations,~1200 objects were observed by using FMOS with low
resolution mode with the typical on-source exposure timeof 3 – 4 hours. In total, significant Hα emission lines withsignal-to noise ratio (S/N) ≥ 3 are detected from 343
objects [2,3].
The metallicity is derived from the [N II] λ6584/Hα
emission line ratio. We use the calibration of N2 method[4]. The resulting metallicity ranges widely from ~0.3 to~1.4 Z. The gas mass is estimated from the observed Hαluminosity by assuming the Kennicutt-Schmidt (K-S) law[5], where the SFR surface density (ΣSFR) is calculated
from the intrinsic Hα luminosity corrected for the dust
extinction and r 50 derived from the image in B-band as
the galaxy size. The gas mass fraction (μ) is defined as μ
= Mgas / (M* + Mgas), where Mgas and M* are gas mass andstellar mass, respectively. The resulting gas mass fraction
is widely distributed from ~0.2 to ~0.8 with the medianvalue of 0.47.
We employ the least-χ 2 fittings for the observed gas
mass fraction, stellar mass, and metallicity with a simple
analytic model of chemical evolution of galaxies:

IWAMURO, Fumihide(Kyoto University)

DALTON, Gavin, LEWIS, Ian(Oxford University)where y Z is a true yield, and fi and fo are infall and outflow
rate which are normalized by the SFR, respectively, and(2)where M 0gas is the initial primordial gas mass. The joint
χ 2 fitting shows the best-fit inflow rate is ~1.8 and theoutflow rate is ~0.6 in unit of star-formation rate (SFR).
By applying the same analysis to the previous
studies at z ~ 0 and z ~ 2.2, it is shown that the bothinflow rate and outflow rate decrease with decreasing
redshift, which implies the higher activity of gas flow
process at higher redshift. The decreasing trend of the
inflow rate from z ~ 2.2 to z ~ 0 agrees with that seen in
the previous observational and theoretical works withdifferent methods, though the absolute value is generally
larger than the previous works. The outflow rate and its
evolution from z ~ 2.2 to z ~ 0 obtained in this work agree
well with the independent estimations in the previous
observational works.

Figure 1: The best-fit inflow rate (left) and outflow rate (right) inunit of M yr−1 as a function of redshift. The results arecompared to the previous results at various redshifts intheoretical and observational works.

References[1] Yabe, K., et al.: 2015, ApJ, 798, 45.
[2] Yabe, K., et al.: 2012, PASJ, 64, 60.
[3] Yabe, K., et al.: 2014, MNRAS, 437, 3647.
[4] Pettini, M., Pagel, B. E. J.: 2004, MNRAS, 348, L59.
[5] Kennicutt, R. C.: 1998, ApJ, 498, 541.

(1)
* belonged to NAOJ when the paper was published.

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047

Enhancement of CO(3–2)/CO(1–0) Ratios and Star Formation
Efficiencies in Supergiant HII Regions
MIURA, Rie E.1/2, KOHNO, Kotaro3/4, TOSAKI ,Tomoka5, ESPADA, Daniel1/6/7, HIROTA, Akihiko1
KOMUGI, Shinya1, OKUMURA, Sachiko K.8, KUNO, Nario1/7, MURAOKA, Kazuyuki9
ONODERA, Sachiko10, NAKANISHI, Kouichiro1/6/7, SAWADA, Tsuyoshi1/6, KANEKO, Hiroyuki1/7/11
MINAMIDANI, Tetsuhiro1, FUJII, Kosuke1/2, KAWABE, Ryohei1/6
1: NAOJ, 2: University of Tokyo, 3: Institute of Astronomy, 4: Research centre for Early Universe, 5: Joetsu University of Education, 6: Joint
ALMA Observatory, 7: Graduate University for Advanced Studies, 8: Japan Woman’s University 9: Osaka Prefecture University, 10: Meisei
University, 11: University of Tsukuba

Based on wide-field and high-sensitivity (1σ =16 – 32 mK in Tmb for a velocity resolution of 2.5 km s−1)
CO(J = 3 – 2) observations with a spatial resolution of
100 pc using the ASTE 10 m telescope [1], we present
evidence that super giant HII regions (GHRs) and otherdisk regions of the nearby spiral galaxy, M33, occupy
distinct locations in the correlation between moleculargas, ΣH2, and the star formation rate surface density, ΣSFR[2]. Star formation efficiencies (SFEs), defined as ΣSFR/
ΣH2, in GHRs are found to be ~1 dex higher than in otherdisk regions (Fig. 1). The CO(3– 2)/CO(1– 0) integrated
intensity ratio, R3–2/1–0, is also higher than the averageover the disk (Fig. 2). Such high SFEs and R3–2/1–0 canreach the values found in starburst galaxies, whichsuggests that GHRs may be the elements building up alarger-scale starburst region. Three possible contributions
to high SFEs in GHRs are investigated: (1) the I CON(H2) conversion factor, (2) the dense gas fraction traced
by R3–2/1–0, and (3) the initial mass function (IMF). We
conclude that these starburst-like properties in GHRs canbe interpreted by a combination of both a top-heavy IMF
and a high dense gas fraction, but not by changes in the
ICO-N(H2) conversion factor. We suggest a scenario thatthe parental molecular gas would tend to get denser in theaccumulated gas around the first generation stars, while
rapidly consumed by SF, eroded, and dissipated due tomore massive stars in GHRs. This results in high SFE
and densities.

References[1] Miura, R. E., Kohno, K., et al.: 2012, ApJ, 761, 37.
[2] Miura, R. E., et al.: 2014, ApJ, 788, 167.
[3] Daddi, E., et al.: 2010, ApJ, 714, L118.

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Figure 1: SFR vs. molecular gas surface densities for GHRs (redfilled stars, NGC 604 and NGC 595) and for non-GHRs(blue filled contour) in M33, compared with that of othergalaxies from [3] (and references therein).

Figure 2: Plot of the R 3-2/1-0 vs. SFE H 2 (CO J=3–2) (left) andSFEH2 (CO J=1–0) (right). Data for GHRs are shown as red
points, while that for non-GHRs as blue contours. The
data points in several annuli of starburst galaxy M83 areshown as green filled (unfilled) triangles, representing
the centre (disk).

Witness of Gas Infall and Outflow
in the Young Starburst Dwarf Galaxy NGC 5253
MIURA, Rie E.1, ESPADA, Daniel1/2/3, SUGAI, Hajime4, NAKANISHI, Kouichiro1/2/3, HIROTA, Akihiko1/2
1: NAOJ, 2: Joint ALMA Observatory, 3: Sokendai University, 4: Kavli Institute for the Physics and Mathematics of the Universe

The nearest (d = 3.8 Mpc) young nuclear starburst,
NGC 5253, is arguably the best laboratory forunderstanding the star-formation process at the very earlystage of a starburst. NGC 5253 is a compact blue dwarf
galaxy, hosting several young clusters with ages ranging
between <2.5 – 50 Myr and experiencing a few bursts
in a short period. In the center of the galaxy, there is a
deeply embedded radio compact (1–2 pc size) HII region
excited by 4700 O stars. It is powered by two massive(~3 × 106 M) and young (~3.5 Myr) super stellar clusters(SSCs) separated by 0″. 3 (correponding to ~6 pc).
We present 12 CO(2 – 1) observations towards thedwarf galaxy NGC 5253 using the Submillimeter Array(Fig. 1; [1]). The data shows that a large amount ofmolecular gas is located in the central ~200 pc starburst
region, physically associated with two young superstellar clusters (SSCs). The molecular gas traced by
12CO(2–1) is elongated along the minor axis (dust lane)of the galaxy and its kinematics suggest that there is an
inflow of molecular gas to the direction of the central
SSCs, as is also observed in HI gas at a larger scale. Dueto their correlation in spatial and velocity domains, thecentral SSCs were likely formed from molecular gas in
the nucleus. We compare the 12CO(2–1) with available
H2 1–0 S(1) data, and show that while the relatively coldgas traced by 12CO(2–1) is distributed along the dustlane, the warm gas traced by H2 1–0 S(1) is associatedwith the central HII region and other star-forming regions.
Interestingly, a cavity in the H2 1 – 0 S(1) emission isfound to be spatially correlated with a Hα shell. This Hαshell may trace a bipolar outflow from the central SSCs
and the H2 1–0 S(1) gas the shocked gas by the outflow
encountering the surrounding quiescent gas. We calculate
molecular gas inflow rate of ~2 M yr−1, star formation
rate of 0.3–0.5 M yr−1, and an ionized gas outflow being
emitted from the SSCs with a rate of (5–25)×10−3 M yr−1.

Figure 1: Top) The three-color composite image of HST/ACS
F300W (blue), F658N (Hα; green), and F814W (red)images. The field of view of the SMA observations isshown as a circle. Bottom) The SMA CO(2–1) map
of NGC 5253 in color scale and black contour. The
blue contours correspond to the 230 GHz continuum
emission. The yellow star corresponds to the two
massive and young SSCs. The black crosses are thetwo identified giant molecular clouds in this study.
The synthesized beam size of the SMA observations isshown at the right bottom corner.

Reference[1] Miura, R. E., et al.: 2015, PASJ, 67, 1.

I Scientific Highlights049

Unresolved Mixed Polarity Magnetic Fields at Flux Cancellation Site
in Solar Photosphere at 0 ″. 3 Spatial Resolution
			

KUBO, Masahito(NAOJ)			

LOW, Boon Chye, LITES, Bruce W.

Mutual disappearance of opposite-polarity
magnetic elements from the solar surface following
their apparent “collisions” are often observed in lineof-sight magnetograms. This phenomenon is called“magnetic flux cancellation”. The study of magnetic flux
cancellation is important for understanding the nature of
the flux removal process from the solar surface layers.
Five flux cancellation events at granular scales were
investigated with the vector magnetic field measurements
at high spatial resoluiton by Hinode spectropolarimeter,
and the horizontal magnetic fields between the canceling
opposite-polarity magnetic elements were detected inonly one event that takes place in a small emerging flux
region [1]. This finding is interesting since almost all
theoretical scenarios proposed to explain photosphericflux cancellation expect an increase in the horizontal
magnetic field between the canceling opposite-polarity
magnetic elements.
We investigate circular polarization (Stokes V )profiles at the polarity inversion line (PIL) formed bycanceling opposite-polarity magnetic elements (Figure 1)[2]. This cancellation event was located just outside
an active region NOAA 10944 on 2007 March 2 andits temporal evolution was investigated in Ref [1]. The
Hinode spectropolarimeter provides the Stokes profiles
with a 0 ″. 15 slit width and a 0 ″. 16 pixel sampling along
the slit. A highly asymmetric, strongly redshifted Stokes
V profile in the Fe I 630.25 nm line is observed at the PIL(Figure 2b). The observed anomalous Stokes V profile isreproduced successfully by a simple summation of thenearly symmetric Stokes V profiles observed at pixels
immediately adjacent to the PIL, as shown by the diamondsymbols in Figure 2b. Similar results are obtainedat the neighboring pixel along the PIL (Figure 2d)or obtained for Fe I 630.15 nm line. This result suggeststhat the anomalous Stokes V profiles observed at the PIL
are not indications of a flux removal process, but are
the result of a mixture of unresolved, opposite-polarity
magnetic fields at an estimated resolution element of
about 0 ″. 3. The hitherto undetected flux removal process
accounting for the larger-scale disappearance of magnetic
elements during the observing period is likely to also fall
below resolution.

050

I Scientific Highlights(High Altitude Observatory)

Figure 1: Total circular polarization map for the whole flux
cancellation region (panel a), and for the cancelingmagnetic bipole (panel b). The solid box of panel a
is identical to the field of view of panel b. The green
symbols in panel b represent pixels at the polarity
inversion line. The blue and red symbols represent
pixels next to the polarity inversion line, and they havenegative and positive magnetic polarity, respectively.

Figure 2: The red and blue solid lines in panel a and the green line
in panel b represent the observed Stokes V profiles of the
Fe I 630.25 nm line at pixels represented by red, blue,
green cross symbols in panel b of Figure 1, respectively.
The diamond symbols in panel b show the profile
synthesized from the observed red and blue profiles inpanel a. Panels c and d are same as their upper panels,
but for the pixels represented by the triangle symbols inpanel b of Figure 1. The vertical dotted line represents
the averaged position of the line centers over the map.

References[1] Kubo, M., et al.: 2010, ApJ, 712, 1321.
[2] Kubo, M., et al.: 2014, ApJ, 793, L9.

The First Very Long Baseline Interferometry Imageof a 44 GHz Methanol Maser with the KVN and VERA Array (KaVA)		

MATSUMOTO, Naoko(NAOJ)		

HIROTA, Tomoya(SOKENDAI/NAOJ)		

KIM, Kee-Tae, KIM, Mikyoung				 (KASI)

We obtained a first VLBI image of a 44 GHz class I
methanol maser with KaVA (KVN and VERA Array),which is a newly combined array of KVN (Korean
VLBI Network) and VERA (VLBI Exploration of Radio
Astrometry) (Figure 1) [1].
The imaged 44 GHz methanol maser is associatedwith a millimeter core MM2 in a massive star-forming
region IRAS 18151–1208. The distance of this source isestimated to be 3 kpc [2]. This 44 GHz methanol maser
source was newly detected in the course of KVN singledish survey as one of the brightest source with a total flux
density of about 500 Jy [3].
The absolute positions of the maser component
with v LSR = 29.4 km s −1 is derived to be α J 2000.0 =18h17m49.s95, δ J 2000.0 = −12°08′06.5″ with the error of~ 20″ from a fringe-rate mapping in our VLBI data [1].
This result suggest that the maser components detected in
our observation are associated with a region around the
younger millimeter core MM2 than MM1 [5] which is
pre-UC HII region [4].
The compact maser components were detected withthe synthesized beam size of 2.7 milliarcseconds ×
1.5 milliarcseconds (mas) [1]. Minimum size in the maser
components is ~ 5 mas × 2 mas, corresponding to thelinear size of ~ 15 AU × 6 AU at the distance of 3 kpc.
Brightness temperature of the maser components ranges~ 3.5 × 108 – 1.0 × 1010 K. These values are higher than alower limit of 108 K estimated with the previous highest
spacial resolution image with ~ 50 mas observed with
Very Large Array (VLA).
This VLBI observation for 44 GHz methanol maser
would be expected to be powerful tool to obtain accurate
positions and proper motions to identify maser pumping
sources.

SUGIYAMA, Koichiro(Ibaraki University)

KaVA SFR group members

Figure 1: An intensity map of a 44 GHz methanol-maser
component of v LSR = 29.8 km s−1 associated with IRAS
18151–1208 MM2. Synthesized beam is shown in thebottom-left corner.

References[1] Matsumoto, N., et al.: 2014, ApJ, 789, L1.
[2] Sridharan, T. K., et al.: 2005, ApJ, 634, L57.
[3] Kim, K. T. in prep.
[4] Marseille, M., et al.: 2008, A&A, 488, 579[5] Sakai, T., Sakai, N., Hirota, T., Yamamoto, S.: 2010, ApJ, 714,
1658.

I Scientific Highlights

051

Torus-Fitting Method in Two-Dimensional Galactic Potentials
YANO, Taihei(NAOJ)		

UEDA, Haruhiko(Akita University)

A new method called a torus-fitting method (hereafter
TF method), by which a generating function is derived
numerically for models of the Galactic potential in whichalmost all orbits are regular is proposed. We found that
the TF method can be applied to major orbit families (boxand loop orbits) in some two-dimensional potentials.
Furthermore, the TF method is still applicable to resonant
orbit families. Hence, the TF method is useful for
analysing real Galactic systems in which a lot of resonant
orbit families might exist [1].
The surface of section (x, px) with y = 0 in thelogarithmic potential with q = 0.9 and Rc = 0.14 is shownin Fig. 1. The solid curves represent the target tori derived
by the direct calculation of the orbits of five test particles.
The plus symbols show the reconstructed target tori byuse of the TF method. We find that the reconstructed tori
correspond very well to the tori derived directly from theorbits. It proves that the TF method works very well for
major orbits. Furthermore, the square symbols represent
the target tori derived by the TF method in which thegenerating functions are estimated by the interpolation
technique. The interpolation also works very well for
major orbits.
We aply this mehod also for minor orbits. The brief
procedure for the minor orbit is as follows. Illustrationof the resonant torus and the additional curve is shown atleft in Fig. 2. The resonant torus can be reconstructed by
the two pseudotori. One of the pseudo-tori consists of theadditional curve (except for the additional curve inside
the resonant tours) and the upper part of the resonant
torus as shown at upper right. Another one consists of theadditional curve (except the additional curve inside theresonant tours) and the lower part of the resonant torus asshown at lower right. We can reconstruct the minor orbit
using these two pseudo-tori.
The surface of section (x, px) with y = 0 in thelogarithmic potential with q = 0.6 and Rc = 0.14 is shownin Fig. 3. The solid lines represent the target tori derived
by the numerical calculation of the orbits of test particles.
The plus symbols show the reconstructed target tori
containing resonant tori reconstructed using the above
procedure. This shows that the TF method works very
well also for minor orbits.

HARA, Takuji(University of Tokyo)

GOUDA, Naoteru(NAOJ)

Figure 1: The surface of section (x, px) with y = 0 in thelogarithmic potential. Solid lines represent the target
tori derived by the numerical calculations. The plus
symbols show the reconstructed target tori. The squaresymbols represent the target tori using the interpolation
technique.

Figure 2: Method to aply for the minor orbit.

Figure 3: Application of the torus fitting method to the minor
orbit.
Reference[1] Ueda, H., Hara, T., Gouda, N., Yano, T.: 2014, MNRAS, 444,
2218.

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Discovery of Star Formation in the Extreme Outer Galaxy
Possibly Induced by a High-Velocity Cloud Impact [1]
IZUMI, Natsuko, KOBAYASHI, Naoto, YASUI, Chikako, HAMANO, Satoshi(University of Tokyo)

			

TOKUNAGA, Alan T.

(University of Hawaii)			

The extreme outer galaxy (EOG), which we define
as the region with a Galactocentric radius (RG) of morethan 18 kpc [2], has a very different environment fromthe solar neighborhood with a much lower gas density(< 1/10) [3], lower metallicity (~1/10) [4], and little orno perturbation from the spiral arms. Such a region not
only defines the size and shape of our Galaxy, but it also
serves as an excellent laboratory for studying the starforming process in low-density and low-metallicity
environments. Because such environments may have
similar characteristics that existed in the early phaseof Galaxy formation [2], we might be able to directly
observe the galaxy formation processes in unprecedented
detail at a much closer distance than distant galaxies.
Digel Clouds, which are composed of eightmolecular clouds (Cloud1-8), were discovered by thevery first survey of molecular clouds in EOG [5]. We
observed Cloud1, which has the largest dynamical mass
among all of the Digel Clouds and perhaps the largest
Galactocentric radius (RG = 22 kpc; kinematic distance)
among all known clouds in the Galaxy, at CO lines with
NRO 45 m telescope as well as NIR wavelengths (J, H,
KS bands) with Subaru 8.2 m telescope, and discoveredstar forming regions (Figure 1).
Using the cluster member, we estimated thephotometric distance of the clusters to be RG ≥ 19 kpc,
which is consistent with the kinematic distance. We also
derived the age of the clusters to be less than 1 Myr, using
the disk fraction of the clusters, which is the percentage
of cluster members with a optically thick circumstellar
dust disk [6,7]. The clusters have lower star formation
efficiency (~1 %) than in the solar neighborhood, whichmight suggest some environmental dependence.
Because of the low-density, triggered formation as
opposed to spontaneous formation may play a crucialrole in the EOG [8,9]. On the sky, Cloud 1 is located very
close to the HI peak of high-velocity cloud (HVC). [10,11]
suggested the interaction between the HVC and theGalactic disk, and there are some HI intermediate velocity
structures between the HVC and the Galactic disk, whichindicates an interaction between them. We suggest thepossibility that the HVC impacting on the Galactic disk
has triggered star formation in Cloud 1. Such process
may have occurred frequently in the early phase of theformation of the Galaxy.

SAITO, Masao(NAOJ/SOKENDAI)

Figure 1: Left) HI map around Cloud 1 (from DRAO data: v LSR= −104.5 ~ −99.6 km s−1). The white contours show the
integrated 12CO(1–0) map of Cloud 1 (from our NRO
45 m telescope data: v LSR = −104.1 ~ −99.1 km s−1), andcontour levels are at 2σ, 3σ, 5σ, 7σ (1σ = 0.5 K km s−1).
The white and red boxes show the mapping size of
the NRO 45 m observation and the field of view of the
Subaru (4′ × 7′; MOIRCS), respectively. The large andsmall white filled circles at the lower right corner show
the resolution of the DRAO (~58″) and NRO 45 m
telescope (~17″), respectively. Right) JHK pseudo color
images of the Cloud 1 clusters from our Subaru data.
The white contours show the same as the 12CO map asin the left panel. The yellow dotted circles show thedefined cluster regions (radius of Cloud 1a circle: 14″,
Cloud 1b: 28″).

References[1] Izumi, N., et al.: 2014, ApJ, 795, 66.
[2] Kobayashi, N., et al.: 2008, ApJ, 683, 178.
[3] Wolfire, M. G., et al.: 2003, ApJ, 587, 278.
[4] Smartt, S. J., Rolleston, W. R. J.: 1997, ApJ, 481, L47.
[5] Digel, S., et al.: 1994, ApJ, 422, 92.
[6] Yasui, C., et al.: 2009, ApJ, 705, 54.
[7] Yasui, C., et al.: 2010, ApJ, 723, L113.
[8] Elmegreen, B. G.: 2011, EAS Publications Series, 51, 45.
[9] Elmegreen, B. G.: 2012, in IAU Symp. 284, The Spectral
Energy Distribution of Galaxies, 317.
[10] Lockman, F. J.: 2003, ApJ, 591, L33.
[11] Morras, R., Bajaja, E., Arnal, E. M.: 1998, A&A, 334, 659.

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Discovery of a Rich Galaxy Cluster Candidate at z = 1.52
KOYAMA, Yusei(NAOJ/JAXA)			

KODAMA, Tadayuki(NAOJ)			

HAYASHI, Masao, TANAKA, Ichi

054

I Scientific Highlights(MPE/NAOJ)SHIMAKAWA, Rhythm				(NAOJ)					Galaxy environment has strong impacts ongalaxy properties. It is well established that highdensity environments such as clusters of galaxies are
dominated by red passive galaxies, whilst low-density
field environments are dominated by blue star-forming
galaxies [1]. Distant galaxy clusters are progenitors of
local massive clusters, and therefore, they are important
targets for studying how the cluster galaxies grow within
high-density environments through cosmic time.
Searching distant clusters generally requires a squaredegree scale huge area survey as they are rare objects. An
alternative, effective way to find galaxy over densities
is to investigate the field around high-z radio galaxies.
High-z radio galaxies are believed to be progenitors ofpresent-day central cluster galaxies (cD galaxies), anda number of studies have successfully reported “protoclusters” around high-z radio galaxies (e.g. [2]).
We have completed an imaging survey of a field of
the radio galaxy 4C 65.22 (z = 1.52) with Suprime-Camand MOIRCS on the Subaru Telescope. In addition to the
Br′z′JHKs broad-band photometry, we also used a narrowband filter NB1657 on MOIRCS (λ c = 1.657 μm) which
can capture the Hα emission lines at the radio galaxy’s
redshift [3].
Our data revealed the large-scale distribution ofgalaxies around the radio galaxy as shown in Fig. 1. In
this plot, the black and red symbols represent z ~ 1.5galaxies selected with photometric redshift technique,demonstrating a factor of > 10× over-density around theradio galaxy. In particular, the red symbols in the plot
denote those having red z′ – J colors; they are expected
to be quiescent galaxies. It is interesting to point out thatthe trend that such red (quiescent) galaxies are strongly
clustered at the peak of galaxy distribution is qualitatively
consistent with the situation in the local universe.
For those having significant excess in the NB1657
photometry, we carefully inspected their broad-bandcolors to identify the Hα emitters at z~ 1.52 (shown withthe blue squares in Fig. 1). Clearly, the Hα emitters are
distributed in the outskirts of the cluster core (avoiding
the highest-density region), which is consistent with
our similar Hα study in a z ~ 0.8 cluster [4]. Therefore
we suggest that the newly discovered structure at z ~ 1.5
reported here is likely a rich galaxy cluster at z ≈ 1.52.
Interestingly, our recent star-forming galaxy survey
in another cluster at a similar redshift [5] reported a highfraction of star-forming galaxies within cluster core

TADAKI, Ken-ichi(GUAS)

environments. Therefore our new data suggest that there
is a diversity in the properties of z ~ 1.5 clusters, and we
speculate that the redshift of z ~ 1.5 is a key epoch forunderstanding the cluster galaxy evolution.
By comparing the Hα emitters near the central cluster
and in the outer fields, we also reported that there is nostrong environmental dependence of the star formation
rate (SFR) versus stellar mass (M) relation at z ~ 1.5,
which is consistent with our recent study [6]. Our study
thus demonstrates that the fraction of star-forming
galaxies does change with environment (at z~1.5), but aslong as we focus on star-forming galaxies, their properties
are not strongly correlated with environment.

Figure 1: A 2-D map of galaxies around the 4C 65.22 radio galaxy(shown with yellow star). The photo-z selected galaxies
with 1.3 < zphot < 1.7 are shown with black circles (andtheir density shown with contours), among which red
symbols show the location of red (passive) galaxies
selected with z′ – J colors. The blue squares show Hαemitters at z = 1.52. Two large circles show 250 and
500 kpc from the density peak.

References[1] Dressler, A.: 1980, ApJ, 236, 351.
[2] Venemans, B. P., et al.: 2007, A&A, 461, 823.
[3] Koyama, Y., et al.: 2014, ApJ, 789, 18.
[4] Koyama, Y., et al.: 2010, MNRAS, 403, 1611.
[5] Hayashi, M., et al.: 2010, MNRAS, 402, 1980.
[6] Koyama, Y., et al.: 2013, MNRAS, 434, 423.

A Chemical Signature of First-Generation Very-Massive Stars
AOKI, W.1, TOMINAGA, N.2, BEERS, T. C.3, HONDA, S.4, LEE, Y. S.5
1: NAOJ, 2: Konan University, 3: University of Notre Dame, 4: University of Hyogo, 5: New Mexico State University

First-generation stars are objects formed in the early
Universe from gas clouds containing only hydrogen andhelium. They are the probable precursors of the formationof the Universe’s structure and chemical enrichment.
Recent numerical simulations suggest that a fraction ofvery-massive stars with masses exceeding one hundred
times that of the Sun could have formed in the early
Universe, even though the large majority of first stars
formed with masses of ten to a hundred times that of
the Sun [1]. Their strong UV radiation and energetic
explosions are likely to have had a significant impact on
the evolution of stellar systems.
Supernova explosions ejected elements formed by the
first massive stars and dispersed them into the gas thatformed the next generations of stars. Stars with masses
slightly less than the Sun’s have very long lifetimes
enough to survive until now. The Milky Way contains suchlow-mass stars with low overall metal content, including
the elements produced by the first massive stars. The
distinctive chemical abundance patterns of these stars canbe used to estimate the masses of the first stars.
High-resolution spectroscopy for low-mass stars withlow metallicity determines their chemical abundances
and identifies stars that recorded the abundance patterns
associated with the first stars that had several tens of solar
masses and produced large amounts of carbon and otherlight elements [2]. However, no previous research of lowmass metal-poor Milky-Way stars has found the signatureof supernova explosions of very-massive stars with morethan 100 solar masses, which synthesize large amounts ofiron but little carbon.
Searches for such stars require larger surveys of very
metal-poor stars, which was realized by the Sloan Digital
Sky Survey (SDSS). We selected candidates for very
metal-poor stars from the SDSS spectra, and used theHigh Dispersion Spectrograph mounted on the Subaru
Telescope to conduct a high-resolution spectroscopic
follow-up of a large sample of low-mass metal-poorstars. We discovered a star, SDSS J001820.5-093939.2(SDSS J0018-0939), that exhibits a very peculiar set ofchemical abundance ratios [3]. Whereas the star contains
an amount of iron 300 times lower than the Sun’s, it issignificantly deficient in lighter elements such as carbon
and magnesium.
Nucleosynthesis models for supernova explosionsof massive stars, which successfully reproduce theabundance ratios found in most of the early-generationstars previously known, do not readily explain thechemical abundance ratios observed in the newly

discovered star (Figure 1). Rather, explosion models ofvery-massive stars can explain both the relatively highabundance ratio of iron as well as the low abundancesof lighter elements. This means that this star most likely
preserves the elemental abundance ratios produced by afirst-generation very-massive star.
Further modeling of chemical yields of firstgeneration very-massive stars is strongly desired. If moredetailed study of this star confirms the existence of verymassive stars, this new discovery will provide strong
support for the predictions of the mass distribution of firststars.

Figure 1: Elemental abundances measured for SDSS J0018-0939(circles) and a comparison star (triangles) comparedwith supernova nucleosythesis models. (upper) The
abundance pattern of the comparison star is explained bya core-collapse supernova model, whereas that of SDSS
J0018-0939 is not reproduced by possible variationsof the models. Cobalt and Scandium, as well as heavy
neutron-capture elements, are also deficient. (lower)
Some basic features of the abundance pattern of SDSS
J0018-0939 are explained by supernova nucleosynthesis
models for very massive stars.
References[1] Hirano, S., et al.: 2014, ApJ, 781, 60.
[2] Frebel, A., et al.: 2005, Nature, 434, 871.
[3] Aoki, W., et al.: 2014, Science, 345, 912.

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055

The Moment Approach for Resolving the Orbital Elementsof Astrometric Binaries: Possible Application to Cygnus X-1
		YAMADA, Kei, ASADA, Hideki(Hirosaki University)			

YAMAGUCHI, Masaki

Resolving the orbital elements of astrometric binaries
has been the important issue for measuring the masses ofstars. The masses of main sequence stars are important toclarify the stellar population and evolution. The massesof compact objects, i.e., white dwarfs, neutron stars, andblack holes, are important to clear the nature of theseobjects.
“A moment approach” is one of methods for resolving
the orbital elements, which is developed by Iwama etal [1]. The future astrometric observations such as Gaia
and Small-JASMINE enable us to measure the stellar
positions at a precision of the 10-microarcsecond level.
This means that we may be able to measure the orbital
elements of close binaries such as high mass X-ray
binaries with the period of a few days, i.e., Cygnus X-1,
whose period is about 6 days. Here, we should note thatthe observational data are numerous, for example, about
100 data points for Gaia and about 105 data points for
Small-JASMINE. If these data points are isochronous,
they are expected to show a spacial bias due to thedifference of the velocity of the star on the celestial
sphere. Therefore the spacial moments due to the bias
allow us to measure the orbital elements of astrometricbinaries. This moment approach would be useful for
obtaining recovered values as trial values of the steepest
descent method for reaching the best-fitting parametervalues.
The previous study [1] have room for improvement.
Temporal information is not incorporated in the previous
approach, where only the spacial bias is considered andthe time of each data is neglected. The stellar position
is determined by the orbital phase which is directly
related to the time, so that the information of the timeis important to constrain the orbital parameter. To
incorporate temporal information, of N observed points
we average the coordinate of na observed points which
are neighboring positions. Using averaged data points,
which show better accuracies, we apply the moment
approach to calculate the orbital elements.
Figure 1 shows the apparent orbits for the meanvalues of the recovered parameters using the approach inthe paper [1] and the present one. Here, σ represents theobservational error for each position measurement in unitof the semi-major axis of the trial binary. In Figure 1, weset (σ, N, na) = (5, 10000, 100). We see that the present
approach significantly improves the previous one for theorbit shape.
Let us consider a possible application to Cyg

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GOUDA, Naoteru(SOKENDAI/NAOJ)

X-1, whose angular radius is ~0.03 mas. The required
precision of the Small-JASMINE is 0.01 mas, so that
we expect that the orbit of Cyg X-1 will be detected by
Small-JASMINE. The calculational results show thatthe semi-major axis is expected to be recovered with anaccuracy comparable to the true value from astrometricobservations alone. Therefore, it is more convenient tostart with the values that are recovered from the present
moment approach and next to use the steepest descentmethod for finally reaching the best-fitting parametervalues. This manuscript is a review of the paper [2].

Figure 1: The apparent orbits for the mean values of the recovered
parameters. The solid curve is the apparent ellipse forthe true parabeters, and the dotted and dashed curves
denote orbits for the mean value of the recovered
parameters from the approach in [1] and the present one,respectively.

References[1] Iwama, H., Asada, H., Yamada, K.: 2013, PASJ, 65, 2.
[2] Yamada, K., Yamaguchi, M. S., Asada, H., Gouda, N.: 2014,
PASJ, 66, 5.

Photospheric Flow Field
Related to the Evolution of the Sun’s Polar Magnetic Patches
Observed by Hinode SOT
KAITHAKKAL, A. J., SUEMATSU, Y., KUBO, M.

		(SOKENDAI/NAOJ)			

The distribution and evolution of the Sun’s polar
magnetic field is of vital importance to understand theorigin of the solar magnetism, its periodic variation andthe heliospheric magnetic flux. Recent high resolution
observations from the Hinode satellite have revealed
that the polar region is dominated by unipolar magnetic
patches which possess magnetic fields with field strengths
exceeding 1 kG. The basic properties, mechanism of
formation and reversal of the polar magnetic fields are
topics which are yet to be resolved.
To investigate the role of photospheric flow fields
in the formation and evolution of the polar magnetic
patches, we conducted spectro-polarimetric observations
with Hinode SOT-SP in the north and south polar caps
on 2013 Nov 11, 2013 Nov 13, 2013 Dec 08, 2013 Dec
11, 2014 Jan 17, 2014 Jan 23 and 2014 Mar 08. The
SP recorded full Stokes spectra of the two Fe I lines
at 630.15 nm and 630.25 nm with the fast map mode
whose slit-scanning step is 0.32″ and integration time ineach step is 3.2s. Image sequences were obtained witha cadence of 16 minutes and the FOV was 80″×164″.
Photospheric vector magnetic fields were derived byMilne-Eddington inversion for those pixels with Stokes
Q, U or V peaks larger than 5 sigma. The variation of theflows with height was examined by the bisector analysisof the Fe I 630.15 nm line profile at four line depths.
We found many unipolar appearances and disappearances in the data. Converging horizontal flows areobserved outside the magnetic patches during the entire
lives of the patches. The converging flow is best observed
at a height close to the solar photosphere. We also
observed a weak converging flow around the retraced
patch location 16 minutes before the patch appearance.
The result implies that polar magnetic patches are formedby the accumulation of flux fragments by the horizontal
converging flows. In addition to direct cancellation
between opposite polarity patches, we observed unipolar
disappearance of polar patches. We speculate that thesepatches diffuse away into smaller fragments with flux
below the detection limit of the instrument and eventually
undergo cancellation with opposite polarity fragments.

SHIOTA, D.

(Nagoya University)		

IIDA, Y., TSUNETA, S.
(ISAS/JAXA)

Figure 1: The average Doppler velocity profiles along N-S
direction indicating converging flows at line bisector
positions in the order of line intensity from top to bottom
panel at time of patch appearance. The plots on the left
panel represent horizontal velocity field outside thepatch and that on the right represent the velocity fieldwithin the patch.

Reference[1] Kaithakkal, A. J., Suematsu, Y., Kubo, M., Iida, Y., Shiota, D.,
Tsuneta, S.: 2015, ApJ, 799, 139.

I Scientific Highlights

057

ALMA Observation of 158 μm [CII] Line and Dust Continuum of a z = 7
Normally Star-Forming Galaxy in the Epoch of Reionization
OTA, Kazuaki1, WALTER, Fabian2, OHTA, Kouji3, HATSUKADE, Bunyo4, CARILLI, Chris L.5
DA CUNHA, Elisabete6, GONZÁLEZ-LÓPEZ, Jorge2, DECARLI, Roberto2, HODGE, Jacqueline A.5
NAGAI, Hiroshi4, EGAMI, Eiichi7, JIANG, Linhua8, IYE, Masanori4, KASHIKAWA, Nobunari4
RIECHERS Dominik A.9, BERTOLDI, Frank10, COX, Pierre11, NERI, Roberto12, WEISS, Axel13
1: University of Cambridge, 2: Max-Planck Institute for Astronomy, 3: Kyoto University, 4: NAOJ, 5: National Radio Astronomy Observatory,
6: Swinburne University of Technology, 7: University of Arizona, 8: Peking University, 9: Cornell University, 10: University of Bonn, 11:
ALMA, 12: Institut de Radio Astronomie Millimétrique, 13: Max-Planck Institute for Radio Astronomy

High-z star-forming galaxies in the epoch ofreionization (EoR) have been usually detected via their
Lyα lines or UV continua. However, as UV light traces
only ionized gas/stars, we have seen merely a portion ofstar formation in galaxies. Another aspect yet unexploredis dust-obscured star formation, and rest frame farinfrared (FIR) lines and continuum can probe it as theyreflect fuel for star formation and light from stars once
absorbed and re-emitted by dust, respectively. FIR lightsfrom EoR galaxies are redshifted to (sub)millimeter andobservable from the ground by Atacama Large Millimeter/
submillimeter Array (ALMA). Among many FIR lines,
158 μm [CII] is the strongest line of an interstellar medium
and suited for probing faint distant galaxies.
We conducted ALMA observations of the [CII] line
and FIR continuum of a normally star-forming galaxy in
EoR, a z= 6.96 Lyα emitter (LAE) IOK-1 [1]. We found it
undetected in both [CII] and continuum to σline = 240 μJy
beam−1 (40 km s−1 channel) and σcont = 21 μJy beam−1.
Comparison of UV–FIR spectral energy distribution(SED) of IOK-1, including our ALMA limit, to those of
several types of galaxies suggests that IOK-1 is similar to
local dwarf/irregular galaxies in SED shape rather thanhighly dusty/obscured galaxies (Figure 1). Moreover, our3σ FIR continuum limit implies intrinsic dust mass Mdust< 6.4 × 10 7 M, FIR luminosity L FIR < 3.7 × 10 10 L(42.5–122.5 μm), total IR luminosity LIR < 5.7 × 1010 L(8–1000 μm) and dust-obscured star formation rate(SFR) < 10 M yr−1, if we assume that IOK-1 has a dust
temperature and emissivity index typical of local dwarf
galaxies. This SFR is 2.4 times lower than one estimatedfrom the UV continuum, suggesting that < 29 % of thestar formation is obscured by dust. Meanwhile, 3σ [CII]
flux limit converts to luminosity L[CII] < 3.4 × 107 L .
Locations of IOK-1 and previously observed LAEs on
the L[CII] vs. SFR and L[CII]/LFIR vs. LFIR diagrams imply
that LAEs in EoR have significantly lower gas and dust
enrichment than AGN-powered systems and starbursts
at similar/lower redshifts as well as local star-forming
galaxies (Figure 2).

Reference[1] Ota, K., et al.: 2014, ApJ, 792, 34.

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Figure 1: SED of IOK-1 (Data points. Triangles are 3σ upper
limits). Our ALMA 3σ upper limit on 1.26 mm
continuum is the red triangle while those from previous
studies the open triangles. For comparison, various
local galaxy SEDs including (not including) cosmic
microwave background effects on FIR continua areshown by color coded dotted (solid) lines.

Figure 2: L [CII] versus SFR for different types of objects compiled
by us [1]. The arrows indicate upper limits. The dottedline is the correlation for local late-type galaxies. The
solid line with shaded region is the correlation for local
star-forming galaxies with 2σ scatter. The dashed line isthe correlation for L FIR > 1012 L sources.

KVN and VERA Array (KaVA) Observations of Bright AGN Jets		

NIINUMA, K.

LEE, S. S., KINO, M., SOHN, B.W.

(Yamaguchi University)		

(Korea Astronomy and Space Science Institute)

On Behalf of KaVA AGN Sub Working Group/KaVA Science Working Group(http://kava.kasi.re.kr/kava main.php)

KaVA is a VLBI array that combines the Korean
VLBI Network (KVN) and the VLBI Exploration ofRadio Astrometry (VERA), and its baseline lengths range
from 305 to 2270 km. The observing frequencies of 23
GHz and 43 GHz are available. Table 1 summarizes the
specifications of each array. As shown in Table 1, eacharray compensates for the weakness of the other, they arecomplementary, which makes KaVA a very promising
VLBI facility.
Table 1: Brief array specications of each VLBI facility.
Array
KVN
Baseline [km](Shortest/Longest)
Fringe spacing [mas](K-/Q-band)

305 ／ 476
5.6 ／ 3.0

VERA

KaVA

1019 ／ 2270 305 ／ 2270
1.2 ／ 0.6

1.2 ／ 0.6

To evaluate the imaging capability of KaVA for
extended sources, we carried out test observations for
4C 39.25 (relatively compact structure), 3C 273 (extended
bright knotty jet structure), and M 87 (extended smoothjet structure) at both K-/Q-band with bandwidth of 32
MHz on 2013 April 13 and 14. Only 128 Mbps recording
mode (bandwidth of only 32 MHz) allows us to conduct
test observations in commissioning phase.
Based on the test observations, we clarified KaVA canachieve the substantially high dynamic range exceeding
1000 for the sources having the extended structures witheven the bandwidth of only 32 MHz and the on-source
time of an hour, if we perform the observation as covering
the spatial frequency uniformly within an hour angle
spread of a total observation time of 6–8 h [1]. As shownin Figure 1, an extended jet structure in KaVA images arewell reproduced compared with the one in VERA image.
The dynamic range derived from KaVA observations is
at least three times higher than only VERA observations.
This imaging capability of KaVA has a great advantage
for the AGN jet science.

Reference[1] Niinuma, K., Lee, S. S., Kino, M., et al.: 2014, PASJ, 66, 103.

Figure 1: VLBI images of M87 observed by VERA (top) and
KaVA (bottom) at 23 GHz, respectively. In each panel,peak intensities and image noise levels are indicated in
the bottom-right corner and synthesized beams are also
shown in the bottom-left corner in each image. In the
top-right corner, the date and linear scale at the distanceof each source are shown. Contours of each image begin
at five times of image rms, and increase in 2n/2 steps.

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059

Photospheric Properties of Warm EUV Loops and Hot X-Ray Loops
			

KANO, Ryouhei(NAOJ)

UEDA, Kohei(University of Tokyo)		

We investigated the photospheric properties (vector
magnetic fields and horizontal velocity) in a welldeveloped active region, NOAA AR 10978, by using
the Hinode Solar Optical Telescope (SOT), especiallyfor discussing what makes coronal loops so different in
temperature from “warm loops” (1–2 MK) observed in
EUV wavelengths to “hot loops” (> 3 MK) in X-rays [1].
We found that outside sunspots the magnetic filling factor
f in network varies with location, and anti-correlatedwith the horizontal random velocity vSD (Figure 1). For
explaining this anti-correlation, it is not necessary to
use the hypothesis that the dense magnetic flux tubes
suppresses their mobility on the photosphere [2]. If we
accept that the observed magnetic features consist ofunresolved magnetic flux tubes, this anti-correlation canbe explained by the ensemble average of the flux-tube
motion driven by small-scale random flows. This simple
model suggests the equation ofvSD =vo d D−1 f −1/2
for f < ( d /λ )2, (1)=vo λ D−1 		
for f > ( d / λ )2, (2)where d and D are the diameter of flux tube and theresolution of this analysis, respectively, and vo and λare the small-scale flow velocity and its spatial scale,respectively. The observed data are consistent with d ~77 km, vo ~ 2.6 km s−1 and λ ~ 120 km as shown by thedashed line in Figure 1a.
We also found that outside sunspots there is no
significant difference between warm and hot loops either
in the magnetic properties except the inclination or in thehorizontal random velocity at their footpoints, which are
identified with the Hinode X-ray Telescope (XRT) andthe Transition Region and Coronal Explorer (TRACE).
The energy flux injected into the coronal loops by theobserved photospheric motion of the magnetic fields isestimated to be 2 ×106 erg s−1 cm−2, which is the same forboth warm and hot loops (Figure 2). This suggests that
coronal situation (e.g. loop length) plays more importantrole for making a variety of temperature in active-region
coronal loops than the photospheric parameters.

TSUNETA, Saku
(ISAS/JAXA)

Figure 1: (a) Scattered plot between magnetic filling factor andhorizontal random velocity. A gray scale and contours
show the number density of the data points outside
sunspots. (b) Histograms of the horizontal random
velocity outside sunspots. Different lines indicate
different filling factors: 0.20–0.25 (black), 0.30–0.35(blue), 0.40–0.45 (green), 0.50–0.55 (orange) and 0.60–
0.65 (red). The peaks indicated by dot-dashed lines arealso shown by crosses in panel-(a).

Figure 2: Histograms of photospheric properties at the footpoints
located outside sunspots: (a) intrinsic field strength, (b)inclination and (c) filling factor of magnetic fields, and(d) standard deviation of horizontal velocity. Grey andblack lines correspond the footpoints of warm and hotloops, respectively.

References[1] Kano, R., Ueda, K., Tsuneta, S.: 2014, ApJ, 782, L32.
[2] Katsukawa, Y., Tsuneta, S.: 2005, ApJ, 621, 498.

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Toward the Inversion of the Scattering Polarization and the Hanle Effectin the Hydrogen Lyα LineISHIKAWA, Ryohko1, ASENSIO RAMOS, Andrés2, BELLUZZI, Luca3, MANSO SAINZ, Rafael2ŠTĚPÁN, Jiří4, TRUJILLO BUENO, Javier2, GOTO, Motoshi5, TSUNETA, Saku6
1: NAOJ, 2: Instituto de Astrosica de Canarias, 3: Istituto Ricerche Solari Locarno/Kiepenheuer-Institut für Sonnenphysik, 4: AstronomicalInstitute of the Academy of Sciences, 5: National Institute for Fusion Science, 6: ISAS/JAXA

The chromosphere and the transition region of the
Sun are the interface region between the cool photosphereof 104 K, where the ratio of gas to magnetic pressure β > 1,
and the 106 K corona, where β < 1. In this region, it isbelieved that energy dissipation and energy transportation
to the upper layers are taking place via the magnetic
fields. Thus, magnetic field measurements in the upper
chromosphere and above (i.e., low β region), are essential
for understanding the thermal structure and dynamical
activities of the solar atmosphere. However, the familiar
Zeeman effect has the limited applicability since themagnetic field there is expected to be rather weak and thespectral lines originating from these atmospheric layers
are broad. The Hanle effect, that magnetic field induces
the modification of the linear polarization caused by theanisotropic radiation field (i.e., scattering polarization), is
expected to be a suitable diagnostic tool. Indeed, recent
developments in the theory and modeling of polarizationin spectral lines have suggested that information on themagnetic field in low β region could be encoded in some
UV lines via the Hanle effect [1], and motivated thedevelopment of the CLASP sounding rocket experiment,
which aims to measure the linear polarization profiles at
the hydrogen Lyα line (λ = 121.6 nm) for the first time
[2,3,4].
In our work [5], we clarify the information thatthe Hanle effect can provide by applying a Stokes
inversion technique by means of a database search inview of the CLASP experiment. The database contains
all theoretical Lyα Q/I and U/I profiles for all possible
values of the field strength, inclination, and azimuth,
assuming a one-dimensional semi-empirical model ofthe quiet-sun atmosphere. We focus on understanding
the sensitivity of the inversion results to the noise as wellas the ambiguities inherent to the Hanle effect. We findthat it is difficult to uniquely determine the magnetic
parameters only from the CLASP observables (i.e.,
linear polarization profiles) (Fig. 1), and simultaneous
measurements to constrain one of magnetic parameters
are critically important. Our conclusion is that spectropolarimetry with CLASP can be a suitable diagnostic toolfor investigating the magnetism of the transition region,
especially when complemented with the information on
the azimuthal direction of the magnetic field that can bederived from other instruments.

Figure 1: χ 2 map in the parameter space of field strength,
inclination, and azimuth (magnetic parameters which
are statistically accepted at one σ level as a result of
inversion of a given simulated observable are shownwith black) [5]. Noise expected for the CLASP
experiment [3] is assumed.

References[1] Trujillo Bueno, J., et al.: 2011, ApJ, 738, L11.
[2] Kubo, M., et al.: 2014, ASP Conf. Ser., 489, 307.
[3] Ishikawa, R., et al.: 2014, Solar Physics, 289, 4727.
[4] Narukage, N., et al.: 2015, Applied Opt., 54, 2080.
[5] Ishikawa, R., et al.: 2014, ApJ, 787, 159.

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061

Sterile Neutrino Oscillations in Core-Collapse Supernova Simulations
WARREN, MacKenzie L., MEIXNER, Matt, MATHEWS, Grant J.
(University of Notre Dame)			HIDAKA, Jun(Meisei University)		

Despite recent developments in computational
methods and better understanding of the relevant microphysics and hydrodynamics [1], the detailed explosion
mechanism for core-collapse supernovae is still not
known. Nevertheless, whatever the explosion mechanism
is, it is clear the neutrinos play a very important role even
if new neutrino physics may ultimately required to drive
the explosion.
In our paper [2] we have explored a new way by
which even non-exploding spherical supernova models
can be made to explode. In this case the explosion occurs
via the introduction of new neutrino physics during
the explosion. Specifically, we consider the possible
resonant mixing [3,4] between a sterile neutrino and anelectron neutrino (or anti-neutrino). A sterile neutrino isa postulated right-handed neutrino that does not interact
with normal matter except by vacuum oscillations [2].
We have made core-collapse supernova simulations[2] that allow oscillations between electron neutrinos (ortheir anti particles) with right-handed sterile neutrinos.
We have considered a range of mixing angles and sterile
neutrino masses including those consistent with sterile
neutrinos as a dark matter candidate. We then examined
whether such oscillations can impact the core bounceand shock reheating in supernovae. We identified the
optimum ranges of mixing angles and masses that
dramatically enhance the supernova explosion by
efficiently transporting electron anti-neutrinos from thecore to behind the shock where they provide additional
heating. We show that an interesting oscillation in theneutrino luminosity develops due to a cycle of depletionof the neutrino density by conversion to sterile neutrinos
that shuts off the conversion, followed by a replenishedneutrino density as neutrinos transport through the core.
We found that, for a broad range of sterile neutrino
masses and mixing angles, an efficient transport of antineutrino flux can occur by the resonant conversion ofelectron anti-neutrinos into sterile neutrinos in the corefollowed by the reverse process behind the shock. This is
illustrated in Figure 1 from put paper which shows thata substantial enhancement in the explosion energy canoccur by this efficient transfer of energy out of the coreby the conversion of electron anti-neutrinos to sterile
neutrinos. In particular, sterile neutrino masses consistent
with a dark matter candidate can lead to an explosion.
Thus, we can solve both the supernova explosion
problem and dark matter problem with a single solution.

062

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KAJINO, Toshitaka(NAOJ/University of Tokyo)

We have also shown [2] that this process could leadto a unique neutrino luminosity evolution that may be
detectable with a future detector like Hyper-Kamiokande.

Figure 1: Contours from [2] showing the enhancement in the
supernova kinetic energy, relative to an explosion
without a sterile neutrino present. The dashed line
encloses the region of a factor of 1.5× enhancement
to the kinetic energy and the solid line encloses theregion of a factor of 10× enhancement. The regionof the parameter space that characterizes dark mattercandidates is below the intersection of the two shadedlines of the figure.

References[1] Janka, H.-T.: 2012, Ann. Rev. Nucl. Part. Sci., 62, 407.
[2] Warren, M. L., et al.: 2014, Phys. Rev. D, 90, 103007.
[3] Hidaka, J., Fuller, G.: 2006, Phys. Rev. D, 74, 125015.
[4] J. Hidaka, J., Fuller, G.: 2007, Phys. Rev. D, 76, 083516.

Supernova Relic Neutrinos and the Supernova Rate Problem:
Analysis of Uncertainties and the Role of Failed Supernovae
MATHEWS, Grant J.

(University of Notre Dame)HIDAKA, Jun(Meisei University)

We have investigated [1] the possibility of detecting
the various contributions to the supernova relic neutrino
background in a 106 ton next-generation water Čerenkov
detector such as the proposed Hyper-Kamiokande.
Massive stars (M ≥ 8 M) culminate their evolution ascore collapse supernovae (CC-SNe). Such supernovae are
unique sources for all three flavors of energetic neutrinos.
Neutrinos emerge from deep within the interior ofcore collapse supernovae. As such, supernova neutrinos
have the potential to provide information regarding thephysical processes that take place inside the star. The
emitted neutrinos can almost freely stream from the timeof the early galaxy formation epoch until the present time
without absorption in the intergalactic material. Hence,the detection of this diffuse background of accumulated
neutrinos can be used to study the supernova history
from the beginning of galaxy formation [1,2] and also
provide information on neutrino properties such as flavor
oscillations and/or the neutrino temperatures produced insupernova explosions.
We analyzed prospects for measuring the average
neutrino temperatures and also the prospect of solving
the disparity between the supernova rate inferred fromthe cosmic star formation rate and that directly observed[2]. Figure 1 shows an example of the predicted neutrino
spectrum in the case that a large population of faintblack-hole forming supernovae are needed to explain
the supernova rate problem [1]. Figure 2 illustrates
how one might determine the average electron antineutrino temperature from the detected positron event
rate. This figure shows the ratio of the event rate at theobserved spectrum peak to the rate at 25 MeV. There isa very strong correlation between this ratio and neutrino
temperature that characterizes the different representative
supernova models identified. Even in different neutrino
oscillation cases the relationship between characteristic
neutrino temperature from the supernova models and thisratio is quite robust.

KAJINO, Toshitaka(NAOJ/University of Tokyo)		

SUZUKI, Jyutaro(NAOJ)

Figure 1: Example of the predicted e+ energy spectra from relicneutrinos as a function of e+ energy where Eν = Ee+ +1.3 MeV. In this case failed fSNe account for a factor of
two difference between supernova rate deduced from themassive SFR and the observed supernova rate. Different
bands correspond to different neutrino oscillation
scenarios. Grey areas denote the backgrounds fromterrestrial reactors and atmospheric neutrinos.

Figure 2: Sensitivity or the average neutrino temperature ratioof events at the observed positron peak to events witha positron energy of 25 MeV, corresponding to the 7
fiducial SN collapse models studied in [1].

References[1] Mathews, G. J., et al.: 2014, ApJ, 790, 115.
[2] Horiuchi, S., et al.: 2011, ApJ, 738, 154.

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063

The In-Medium Effects on the Neutrino Reaction in Dense Matter
		CHEOUN, M.-K.

(Soongsil University)

SO, W. Y.

(Kangwon University)

KIM, K. S.

(Korea Aviation University)

KAJINO, Toshitaka(NAOJ/University of Tokyo)		

Nowadays neutrino scattering becomes one of usefultools for understanding neutrino physics as well as
neutrino astrophysics. But most of the scattering data
were extracted by the neutrino scattering off target nuclei.
Moreover incident neutrino energy ranges from a few
MeV to tens of GeV. As well known in other projectiles,
we need to understand target nuclear structure probed by
the weak interaction. Then it would be very helpful toknow from which energy region we have to include thestructure effect and how to include it in the analysis ofneutrino scattering.
Moreover, strong recent evidence for the modificationof nucleon properties in a nuclear medium has beenreported using the electromagnetic (EM) nucleon form
factors measured in polarized (e→, e′ p→) and (e→, e′ n→)scattering on some light nuclei [1]. Since the weak form
factors also may be affected by the modification of the
EM form factors, Since the weak-vector currents and EM
currents form iso-vector and vector currents, one might
naturally expect that the modification of weak-vector
form factors occurs in a similar manner to that of the EMform factors. Refs. [2] explored nuclear structure effects
in those data directly using robust nuclear structure andreaction theories in the relativistic framework.
In this work, we report one of the answers regarding
the question. In Fig. 1, we show our theoretical total
cross sections of neutrino and anti-neutrino scattering
off hydrogen and 12 C target and compared to the
MiniBooNE and NOMAD neutrino data, whose energy
ranges are up to about 100 and 102 GeV, respectively[3]. These results were carried out by the elementary
process, i.e. neutrino scattering off a free nucleon, by
taking into account the in-medium effect for 12C using
the density-dependent form factors estimated by thequark meson coupling (QMC) model [4]. Effects of the
in-medium (difference between red and black curves)
turn out to be small compared to the experimental error
bars. In particular, neutrino scattering above 1 GeV
can be properly described by the elementary process,irrespective of neutrino types and their current types. But,
below 1 GeV region, it is found that one needs to include
nuclear structure as well as Fermi motion of nucleons forthe neutrino scattering.

064

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KIM, Hungchong(Kookmin University)

MARUYAMA, Tomoyuki(Nihon University)

Figure 1: (Color online) Results of ν + n → μ− + p (upper) and ν̄ +p → μ+ + n (lower) for a nucleon in H and 12C. Results
for a free neutron (proton) and neutron (proton) in a
carbon target are denoted as solid (black) and dotted (red)curves, respectively. Data are MiniBooNE and NOMAD
in Refs. [5] and [6], respectively.

References[1] Brooks, W. K., Strauch, S., Tsushima, K.: 2011, J. Phys. Conf.
Ser., 299, 012011.
[2] Martinez, M. C., et al.: 2004, Phys. Rev. C, 69, 034604.
[3] Cheoun, M.-K., et al.: 2015, J. Phys. G, 42, 045102.
[4] Cheoun, M.-.K., et al.: 2013, Phys. Rev. C, 87, 065502.
[5] Aguilar-Arevalo, A. A., et al.: 2010, Phys. Rev. D, 81, 092005 .
[6] Lyubushkin, V., et al.: 2009, Eur. Phys. J. C, 63, 355.

Induced Amino Acid Chirality from Strong Magnetic Fields
in Interstellar Environments
FAMIANO, Michael A.

(Western Michigan University)		
			

BOYD, Richard N., KAJINO, Toshitaka(NAOJ/University of Tokyo)		

KOEHLER, Katrina(Los Alamos National Laboratory)

Recent work [1,2] has suggested that the chiralityof the amino acids could be established in the magnetic
field of a nascent neutron star from a core-collapse
supernova via processing by the neutrinos that would beemitted. This model, the Supernova Neutrino Amino Acid
Processing Model, or SNAAP model, not only appears to
produce a small chiral imbalance, but al-ways produces
the same sign of the chirality. This is also consistent withevidence that the origin of amino acid chirality may be
non-terrestrial in nature [3,4,5].
We have studied the capability of the SNAAP model
for selective destruction of one molecular chirality. Thisextends previous work [2] to include the dynamical
effects that would be produced on the amino acids thatwere included in meteoroids that were large enoughto escape destruction by the supernova photons as
they passed by a nascent neutron star. This model has
many similarities to nuclear magnetic resonance, eventhough it is essentially classical. The study does showthat the amino acids contained in a large meteoroid
could undergo orientation from the magnetic field of
the neutron star, subsequent chiral sub-state selection
from the combination of that field and the rotation of themeteoroids, and finally chiral selection by the neutrinos
emitted as the neutron star produced by a core-collapse
supernova cools over its characteristic few second
cooling time.
A Monte Carlo code was written to simulate strong
neutrino interactions with amino acids in the vicinity ofneutron stars [6]. This model assumes that the neutrinos
emitted from the nascent neutron star would interact withthe amino acids, which had been oriented by the neutronstars magnetic field. These molecules would have to becontained in large meteoroids that happened to be passing
by the star as it became a supernova, so that they could
survive the high temperature environment existing near
the star. The crucial interaction that destroys 14N is 14N +νe → 14C + e+. It was also assumed that some imbalancein the total angular momentum of the molecules would
be achieved, perhaps by the Buckingham effect [7,8],
so that the conversion of 14N to 14C would, because ofa spin selection effect on the strength of the interaction,
selectively destroy one orientation compared to the other.
These amino acids would have to be contained in large
meteoroids that happened to be passing by the star as it
became a supernova, so that they could survive the high

ONAKA, Takashi(University of Tokyo)

HULBERT, Sarah(The Ohio State University)

temperature environment existing near the star.
For this study, the bulk polarization of 14 N was
calculated for various meteoroid impact parameters(distance of closest approach), speeds, rotational speeds,
and neutron star magnetic field. A subset of results
are shown in Figure 1 for various impact parameters.
Coupling the nitrogen spin to the molecular spin can
result in a bulk molecular polarization coupling to theoverall chirality.

Figure 1: Polarization angle distributions for three models whichvary by distance of closest approach.

References[1] Boyd, R. N., et al.: 2010, Astrobiology, 10, 561.
[2] Boyd, R. N., et al.: 2011, Int. J. Mol. Sci., 12, 3432.
[3] Kvenvolden, K., et al.: 1970, Nature, 228, 923.
[4] Cronin, J. R., et al.: 1997, Science, 275, 951.
[5] Glavin, D. P., et al.: 2010, Met. Plan. Sci, 45, 1948.
[6] Famiano, M. A., et al.: 2014, Symmetry, 6, 909.
[7] Buckingham, A. D.: 2004, Chem. Phys. Lett., 398, 1.
[8] Buckingham, A. D., Fischer, P.: 2006, Chem. Phys., 324, 111.
[9] Boyd, R. N.: 2012, Stardust, Supernovae and the Molecules ofLife, Springer (New York).

I Scientific Highlights

065

Neutrino Magnetic Moment,
CP Violation and Flavor Oscillations in Matter [1]
PEHLIVAN, Y.

(Mimar Sinan University/NAOJ)

BALANTEKIN, A.B.

(University of Wisconsin)

In both the Early Universe, and the intense astrophysicalneutrino sources such as the core collapse supernovae,
neutrinos are believed to undergo nonlinear forms offlavor evolution which result from the many-body effects
due to neutrino-neutrino scattering. These oscillations
are very different from the vacuum oscillations of theneutrinos or the MSW effect in the sun, and are generally
termed collective neutrino oscillations. Although thecollective neutrino oscillations are highly nonlinear, they
were shown to possess several dynamical symmetries
under a two-flavor mixing scenario [2].
In this paper, we show that these symmetries also
emerge in the realistic three-flavor mixing case and thatthey are present even when the CP-symmetry is broken
in the neutrino sector. One practical consequence of theexistence of such symmetries is that they give rise toconserved quantities which reduce the complexity of thenonlinear evolution and allow one to make some model
independent statements [2]. For example, although theneutrino energy spectrum itself changes nonlinearlywith time, the conserved quantities give rise to invariant
spectra which are functionals of the former and constantin time (Fig. 1).
We also examine the interplay between the possible
CP violation features of neutrinos, their anomalous
magnetic moments, and the collective flavor oscillations
with a particular focus on the inherent many-body natureand the symmetries of the latter. We show that, as longas neutrino magnetic moment can be ignored (e.g., if
the magnetic field is not very strong) the CP-violating
effects factor out of the evolution operator and evolve
independently of the nonlinear flavor transformations. In
particular, this tells us that, even if CP violation exist in
the neutrino sector, collective oscillations can not amplify
its effects the way they amplify some other features, suchas the mass hierarchy.
However, even the tiny anomalous magnetic momentsof neutrinos may play a part in some astrophysical andcosmological scenarios [3]. We show that, in this case
the CP violating effects cannot be strictly factorized
any more. However, one can carry out a mathematical
trick and still factor out the CP violating effects fromcollective oscillations by defining an effective magnetic
moment. This effective magnetic moment includes theCP-violating Dirac phase in its definition and is different
for neutrinos and antineutrinos, reflecting the fact that
CP violation and magnetic moment are intertwined in an
inseparable way during the flavor evolution. However,066

I Scientific Highlights

KAJINO, Toshitaka(NAOJ/University of Tokyo)

since the neutrino magnetic moment is small enoughto be conveniently studied in a first order perturbation
approach, this allows us to treat the unfactorized CP
violation effects perturbatively in the first order as well.
The formulation we use in this paper is based on thesymmetries of the Hamiltonian describing the collective
neutrino flavor evolution and therefore is valid under very
general conditions. In particular, it is valid even in thepresence of many-body quantum entanglements which
are generally ignored by mean field type approximations.

Figure 1: Upper panel: Energy spectra of the neutrinos froma proto-neutron star. Lower Panel: Corresponding
invariant spectra.

References[1] Pehlivan, Y., Balantekin, A. B., Kajino, T.: 2014, Phys. Rev. D,
90, 065011.
[2] Pehlivan, Y., et al.: 2011, Phys. Rev. D, 84, 065008.
[3] Kusakabe, M., et al.: 2013, Phys. Rev. D, 87, 085045.

Neutrino Oscillation and Nucleosynthesis
in Core-Collapse Supernova Explosion [1]
KAJINO, Toshitaka(NAOJ/University of Tokyo)

MATHEWS, Grant. J.

(University of Notre Dame)

Neutrino interactions are the key component of themechanism for supernova explosions. Foremost is therole of neutrinos in the explosion itself. Much effort is
now invested in understanding the transport of neutrinos
from the core and the role of neutrino heated convectionin the outer envelopes. They also play an important rolein the associated nucleosynthesis, and current topics are
regarding the synthesis of the ν-process isotopes 180Ta,
138La and light isotopes 7Li and 11B and impact on theneutrino-flavor oscillations [1].
Most important neutrino-flavor mixing is due toMikheyev-Smirnov-Wolfenstein (MSW) matter effect [2].
The adiabatic condition can be written as

HAYAKAWA, Takehito(Japan Atomic Energy Agency)(3)

where U ei are elements of the Cabbibo-KobayashiMasukawa matrix in neutrino sector. We can predict thedifference of the neutrino signals which depend on mass
hierarchy and EoS of proto-neutron stars in mega-ton Gd
loaded Water-Chrenkov detector at Hyper-Kamiokande
[5].

(1)
The flavor oscillations occur for a matter density ρres of(2)
where ρres is in units of g cm−3, Δm2 ~ 10−3 eV is thedifference in the square of the neutrino mass eigenstates,and θ is the relevant mixing angle. This implies that theresonant flavor mixing occurs among active neutrinos at
the matter density ~103 g cm−3 located just below the O/Clayer at Mr ≈ (3.4–4)M as shown in Fig. 1.
The dependence on θ13 enters here for the 13-mixing
resonance. The associated increase in the electron
neutrino temperature increases the rates of chargedcurrent ν-process reactions. Although the heavy ν-processelements are produced in the inner layers and unaffectedby the MSW resonance, the light isotopes 7Li and 11B are
sensitive to the 13 mixing. Moreover, the ratio depends
on the still unknown neutrino mass hierarchy [1].
Since the recent reactor and accelerator experiments
give sin2 2θ13 ~ 0.1, the neutrino mass hierarchy can be
determined from the strong, robust dependence of theabundance ratio 7Li/11B on the oscillation parameters [1].
According to a recent work based on the deduction of theratio 7Li/11B from so-called pre-solar supernova grains ofa meteorite [3], we can conclude that the inverted mass
hierarchy is statistically more favored [4].
We also discussed the flavor mixing effects on
the observed signals of supernova neutrinos on Earth[5]. Independent of the neutrino mass hierarchy in theefficient flavor mixing, the observed neutrino fluxes
might become

Figure 1: Produced Li, Be, and B isotopes as a function of interiormass of core-collapse supernova. Note the large spikein 11B and 7Li production in the O/C and He/C shells.

References[1] Kajino, T., Mathews, G. J., Hayakawa, T.: 2014, J. Phys. G, 41,044007.
[2] Wolfenstein, L.: 1978, Phys. Rev. D, 20, 2634; Mikheyev, S. P.
Smirnov, A. Yu.: 1985, Sov. J. Nucl. Phys., 42, 813.
[3] Fujiya, W., Hoppe, P., Ott, U.: 2011, ApJ, 730, L7.
[4] Mathews, G. J., et al.: 2012, Phys. Rev. D, 85, 105023.
[5] Mathews, G. J., et al.: 2014, ApJ, 790, 115.

I Scientific Highlights

067

Vacuum Ultraviolet Spectro-Polarimeter
Design for Precise Polarization Measurements
NARUKAGE, Noriyuki					(NAOJ)

Precise polarization measurements in the vacuum
ultraviolet (VUV) region provide a new means for
inferring weak magnetic fields in the upper atmosphereof the Sun and stars [1]. We propose a VUV spectropolarimeter design ideally suited for this purpose (seeFigure 1) [2]. This design is proposed and adopted for
the NASA-JAXA Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP), which will record the linear
polarization (Stokes Q and U) of the hydrogen Lyman-αline (121.567 nm) profile. The expected degree ofpolarization is on the order of 0.1 % [1].
Our spectro-polarimeter has two optically symmetricchannels to simultaneously measure orthogonal linear
polarization states with a single concave diffraction
grating that serves both as the spectral dispersion element
and beam splitter (see Figure 1). This design has a

CLASP teamminimal number of reflective components with a high
VUV throughput. Consequently, these design features
allow us to minimize the polarization errors causedby possible time variation of the VUV flux during thepolarization modulation and by statistical photon noise[3].
The CLASP has been assembled as shown in Figure 2
and shipped to United States in April 2015. The CLASP
is planned to be launched at the White Sands Missile
Range in New Mexico in September 2015.

References[1] Trujillo Bueno, J., et al.: 2011, ApJ, 738, L11.
[2] Narukage, N., et al.: 2015, Applied Opt., 54, 2080.
[3] Ishikawa, R., et al.: 2014, Sol. Phys., 289, 4727.

Figure 1: The VUV spectro-polarimeter design for CLASP. The complete optical layout of CLASP, consisting of the telescope, spectropolarimeter, and slitjaw optics, is shown. A light trap is located between the slit and the grating to absorb the zeroth-order beamdiffracted by the grating.

Figure 2: The assembled CLASP instrument. When the CLASP is launched, the instrument is covered with the rocket skin (semitransparent
shell in this picture). The optical path is indicated with blue lines.

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I Scientific Highlights

Evidence of Electron Acceleration
around the Reconnection X-point in a Solar FlareNARUKAGE, Noriyuki(NAOJ)

Particle acceleration is one of the most significant
features that are ubiquitous among space and cosmic
plasmas. It is most prominent during flares in the caseof the Sun, with which huge amount of electromagnetic
radiation and high-energy particles are expelled
into the interplanetary space through acceleration ofplasma particles in the corona. Though it has been wellunderstood that energies of flares are supplied by themechanism called magnetic reconnection based on theobservations in X-rays and EUV with space telescopes,
where and how in the flaring magnetic field plasmas areaccelerated has remained unknown due to the low plasma
density in the flaring corona.
We report the first observational identification of
the energetic non-thermal electrons around the pointof the ongoing magnetic reconnection (X-point) [1].
The location of the X-point is identified by soft X-ray
imagery (Figure 1 (b)–(d)). There is microwave emission
from non-thermal electrons (negative alpha index) mostclearly seen around the X-point (Figure 1 (k)–(m)).
This indicates that there are energetic electrons present
around the X-point during the course of the magnetic
reconnection. Meanwhile, the soft X-ray observationsof the flare were in good agreement, in a morphologicalsense, with the canonical reconnection picture (Figure 1(a)) from which we expect, in addition to the inflow, bidirectional outflow of plasma particles and magnetic
fields away from the X-point towards the bright soft
X-ray loop and in the opposite direction. Assuming thepresence of the expected reconnection outflow, it would
be reasonable to conclude that the energetic non-thermal
electrons are supplied from, namely, accelerated at, theregion around the X-point rather than assuming that they
travel from a region lower in altitude than the X-point
against the counter-streaming downward outflow, or thatthey come from a region higher in altitude beyond the
X-point against the counter-streaming upward outflow
from the X-point.

Reference[1] Narukage, N., Shimojo, M., Sakao, T.: 2014, ApJ, 787, 125.

Figure 1: Soft X-ray and microwave observations of the 6 August 1999
flare. (a) Schematic illustration of the reconnection picture
for the flare. (b)–(d) Soft X-ray images taken with the AlMg
filter of Yohkoh/SXT. The location of the reconnection
X-point is indicated by a black circle in each panel. (e)–(g) Electron temperature distribution derived with the filter
ratio method from pairs of soft X-ray images obtained with
the AlMg and Be119 filters of Yohkoh/SXT. (h)–(j) 17 GHz
microwave brightness temperature maps from Nobeyama
Radioheliograph (NoRH). (k)–(m) Spatial distribution of
power-law index of microwave flux density spectra (alphaindex) derived from NoRH 17 GHz and 34 GHz data.

I Scientific Highlights

069

II Status Reports of Research Activities
1. Subaru Telescope
1. Subaru Telescope Staff
As of the end of FY 2014, the Subaru Telescope Project
staff consisted of 19 dedicated faculty members including six
stationed at Mitaka, six engineers, and three administrative
staff members. Additional staff members include five researchexperts, one postdoctoral fellow, and seven administration
associates, all of whom are stationed at Mitaka. Moreover, 11
research/teaching staff members, 10 of whom are stationed at
Mitaka, and two engineers at Mitaka are posted concurrently.
The project also has 83 local staff members dispatched fromthe 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 the FY 2014, Subaru Telescope produced many outstanding
scientific outcomes which were published in major international
journals. Below are some examples:(1) Deep high-z imaging observation with Suprime-Cam, theoptical wide-field camera, discovered seven Ly-alpha emittersat z ~ 7. The very low number density of such high-z galaxies(only 1/5 of that at z < 6.6) strongly suggests that the neutral
gas fraction (H I) in the Universe increases rather abruptly fromz = 6.6 towards z ~ 7, which thus prevents Ly-alpha photons fromescaping and reaching us. This result has a strong impact on the
study of re-ionization in the early Universe.
(2) High resolution optical spectroscopy with HDS of a very
metal poor star in the Milky Way Galaxy revealed an abnormalabundance pattern of chemical elements, characterized by low
abundances of Carbon, Magnesium and Cobalt. This pattern
can only be reproduced by a model of the supernova explosionof a super massive star (1000 times more massive than theSun). Such a high mass for the first generation of stars had
been theoretically favored and proposed, but this was the firstobservational evidence to support this scenario.
(3) High resolution optical spectroscopy with HDS of a nova,
which was discovered in Aug 2013, revealed that a large amountof Lithium has been synthesized in this nova. Lithium is thought

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to be synthesized in many ways and at various places such as the
Big-Bang, the inter-stellar medium, or in stars like novae andsupernovae. Thus Lithium provides us key information about
the origin and evolution of matter in the Universe. This was thefirst direct detection of a site where Lithium was synthesizedand ejected. This confirmed that nova explosions are indeed the
major supplier of the Lithium seen in the present-day Universe.
(4) High spatial resolution imaging of one of Jupiter’s Galilean
satellites with NIR camera IRCS assisted by adaptive optics
unveiled the fact that the satellite is illuminated, though only
at low level (1/100 of the normal brightness), even when it’s
eclipsed by Jupiter. This indicates that sun light refracted by thematter in the atmosphere above Jupiter’s surface illuminates theGalilean satellite in Jupiter’s shadow.

3. Open Use
The Subaru call for open use proposals is issued every six
months. The periods are from February 1 to July 31 (S14A) andfrom August 1 to January 31 (S14B). The Mitaka office of the
Subaru Telescope at the National Astronomical Observatoryof Japan (NAOJ) campus accepts the submitted proposals.
The Subaru Time Allocation Committee, established under the
NAOJ advisory committee for optical and infrared astronomy,
selects the proposals to accept, based on the evaluations andcomments of the referees. In S14A, 70 programs (104 nights)
were accepted out of 163 submitted proposals, requesting 403.6
nights in total. In S14B, 58 proposals (103 nights) were acceptedout of 133 submitted proposals, requesting 366.7 nights in total.
In S14A and S14B respectively, there were 11 and 3 accepted
open use proposals by foreign principal investigators, excluding
University of Hawai`i observing time. The number of applicants
involved in the submitted proposals was 1806 for Japanese
researchers (Japanese astronomers at any institute and nonJapanese astronomers belonging to Japanese institutes) and 642
for foreign researchers. The number of researchers in accepted
proposals was 891 for Japanese astronomers and 260 for foreign
astronomers.
In S14A and S14B, the number of open use visiting
observers was 422, of which 60 were foreign astronomers.
34 astronomers observed remotely from Mitaka. The Mitaka
office of the Subaru Telescope takes care of proposal handlingand evaluation, travel procedures and travel support for theobservers. The Hawai`i office makes the observing scheduleand supports the accommodations and transportation for visiting
observers in Hawai`i. In S14A and S14B, 94.8 % of the open use
time (including University of Hawai`i time) was used for actual
astronomical observations, after excluding the weather factor
and downtime due to primary mirror coating. About 3.4 %, 0.2 %,and 1.6 % of observing time was lost due to instrument trouble,
communication trouble, and telescope trouble, respectively.
In S14A and S14B, remote observations from Hilo were notconducted. However, remote observations from Mitaka, whereobservers in Mitaka could participate in observations remotely,in addition to on-site observers at the summit, were conductedwith limited function as a trial, for 8 programs with 30 nights.
Service observations were made for 7 nights. To makethe best use of the limited resources at observatories on top of
Maunakea, Subaru Telescope has been exchanging telescope
time with Keck and Gemini. The number of time exchangenights between Subaru Telescope and W. M. Keck Observatory
was 5 in S14A and 3 in S14B. That between Subaru Telescopeand Gemini was 6 in S14A and 5 in S14B.

4. Telescope Maintenance and Performance
Improvement
The general performance of the Subaru Telescope continues
to be maintained the same as in the previous year. This year,
both the optical tertiary mirror and infra-red tertiary mirrors
were recoated. During the recoating work, the mechanical driveof the tertiary mirrors was re-adjusted to improve reliability.
Day crews took over the installation and removal work of both
Hyper Suprime-Cam (HSC) and its filter exchange unit (FEU).
As troubleshooting, the mirror cover open/close sensors, main
shutter open/close sensors, and shutters of the Shack-Hartmann
sensor were replaced. The rubber springs of the dome bogie
have been replaced. Some new functions were added to the Top
Unit Exchanger (TUE) for secure operation. The dome barcode
system has also been upgraded. We also strived to conduct
preventive maintenance.
In addition, while promoting improvements in theperformance and operational efficiency of the Subaru Telescope,renovation proceeded for the telescope control units whichhave been in place for more than 10 years since installation.
The following local control units were renovated or modified inthis year: cover control unit (CVCU), field rotator control unit
for primary focus (FRCU (PF)), atomic dispersion corrector
control unit (ADCU), dome rotation servo control processor
unit (DRPU), dome control unit (DCU), tertiary mirror control
unit (TMCU), balancer control unit (BLCU), telescope control
workstations (TWS), and primary mirror actuator CPU cards.
This year, maintenance of the main shutters, dome bogies,
and the top screens was also carried out in addition to theannual mechanical maintenance. Of special note this year is thedevelopment of a script that checks whether certain telescopeconditions should be expected or not. This script is run every
morning and can find some minor problems, which indicate apotentially critical situation.

5. Instrument Operation and New Development
The nine open-use facility instruments of Subaru Telescope
have been operated stably in FY 2014. 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 beginning of open-use observations in FY 2013,
the software and hardware of HSC have been continuously
improved. As a result, the operation of the filter exchangesystem, shutter, and auto-guider system have been stabilized
significantly. Discussions on how to handover the operationand maintenance of HSC from the development team to theobservatory are underway.
There are several upgrade projects for the other facility
instruments: a MOS unit for HDS, an upgrade of the MOIRCS
detectors, and implementation of polarimetric functions to
IRCS and COMICS. For the HDS MOS unit, the supporting
structure was transported to Hawai`i and study of its mechanicalinterface to the telescope has been started. The fabrication of
optical components such as fibers is still ongoing in Japan. For
the MOIRCS detectors, we have succeeded in operating thearrays and started characterization and parameter optimization.
The IRCS polarization function has been tested on sky and, after
characterizing the polarimetric performance and examining thecalibration strategy, it was decided to open the polarimetry mode
starting from S15B.
In parallel to those upgrade projects, discussions on how
we maintain or stop operations of the facility instruments
are underway. To establish the plan for Subaru Telescopes’s
instrumentation, we summarized information such ascompetitiveness, demand, publications, and work load formaintenance/troubleshooting of the facility instruments.
Based on the results, an instrument plan was proposed to thecommunity in the User’s Meeting. Discussions and planning of
Subaru Telescope’s instrumentation including decommission offacility instruments are still ongoing.
In FY 2014, two carry-in (PI-type) instruments HiCIAO(high-contrast coronagraph imager) and Kyoto-3DII (optical
integral field spectrograph) have continued to be operated.
The commissioning of a coronagraphic extreme adaptive
optics (SCExAO) instrument has been performed. The testsof some operation modes of SCExAO including low-orderwavefront correction, quasi-static speckle nulling, and theaperture masking interferometer (VAMPIRE) which enables
high-spatial resolution imaging in visible bands, have been
completed in FY 2014. These operation modes have been usedin open use observations since the S14B semester and are taking
an important role in the direct imaging observation of extrasolar planets. SCExAO has been commissioning a high-orderwavefront correction mode, which realizes extreme adaptive
optics correction. There are plans to open this mode to open use
observes on a trial basis starting from S15A.
A Multi-Object Adaptive Optics (MOAO) sciencedemonstrator (RAVEN), which has been developed incollaboration with Canadian institutes, successfully saw first

II Status Reports of Research Activities

071

light at the Subaru Telescope in May 2014 and demonstrated theperformance of the MOAO system. As a science demonstrator
for a future TMT MOAO system, RAVEN will conduct
additional test observations for evaluating its performance andperform science observation in S15A.
There are new PI-type instruments, IRD (InfraRed Doppler
instrument) and CHARIS (Coronagraphic High Angular
Resolution Imaging Spectrograph), which are currently
being developed. The IRD project has been reviewed by theobservatory since FY 2013 and officially approved in FY 2014.
These two instruments are planned to be transported to the
Subaru Telescope in FY 2015 and to conduct commissioning
observations in FY 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 multi-field
imager and spectrograph). We are reviewing the acceptance of
SWIMS and MIMIZUKU by considering the impacts to theexisting observatory resources.
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 Suprime-Cam(HSC). The PFS has about 2400 optical fibers distributed overthe 1.3 degree field of view of the prime focus which feed thelight of the astronomical objects to four identical spectrographs
which will be placed in the telescope dome. The spectrographmodules cover wavelengths ranging from 0.38 μm to 1.26 μm
simultaneously. Since the PFS is being developed throughinternational collaborations between several countries with alarge budget scale, the project has been reviewed by the NAOJ
headquarter in terms of the management of the project before
approving the PFS as an official project of the Subaru Telescope.
In FY 2014, the Subaru Telescope officially approved the PFS
project by considering the astronomical importance of the
project and the future instrument plan of the Subaru Telescope.
We are conducting a conceptual study of Subaru Telescope’s
next large facility instrument following HSC and PFS, which
will be one of the flagship instruments at the Subaru Telescopein the era of TMT. We have studied the concept of a widefield near-infrared imager and multi-object spectrographassisted by ground-layer adaptive optics (GLAO), which
uniformly improves image quality over a wide field of viewby correcting only for the turbulence at the ground layer ofthe Earth’s atmosphere by using an adaptive secondary mirror.
In FY 2014, the design of the wide-field near-infrared multiobject spectrograph has been discussed in collaboration with
an Australian institute. We are planning to have a conceptual
design review which summarizes the studies of GLAO and nearinfrared instruments discussed so far.

6. Computers and Network
One of our goals for this year was the same as a goal fromthe previous year - to stably operate the fourth generation system

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of computers and network called STN4. Reliable operation wasachieved without serious troubles or attacks/intrusions such as
illegal access.
Archiving observation data on the current system has beenongoing since the pervious year. The archive is operational
without serious problems. We have been developing a userinterface that is suitable to download large amounts of data in abatch process per requests by users who wish to download datataken by Hyper Suprime-Cam (HSC) with the Strategic Science
Program (SSP).
The data archive system in Mitaka is also operating stably.
We officially rolled out remote observations from Mitaka
using the Remote Observation Monitor System for a limited
amount of time. In this fiscal year, 25 observation programs
utilized the remote observation monitor system for 28 nights.
More programs will use the remote system in the future. The
proposal Management System (ProMS) also worked very well.
Computers for HSC data analysis were procured in
Fiscal Years 2010 and 2011. This year, storage, an interactive
processing server, and a database server were added to thesystem. The current system requires the storage to send andreceive large amounts of data to/from the clients. But the current
storage is not fast enough to handle that amount of data andmakes overall performance subpar. Therefore, we decided totest a fast data I/O software replacing NFS. The test system
including hardware and filesystem software was delivered by theend of this fiscal year. Setting up the test system is planned forearly in the coming fiscal year.
The dedicated network link between Hawai`i and Mitaka
has been procured with a single year contract since April 2014.
Bidding was conducted to select the provider to supply the
network link in this fiscal year. The link speed will become 2
Gbps, double the past speed, considering the increase in traffic
due to HSC observations. A provider was selected successfully
and we prepared our own network system so that it can connect tothe network service that the provider will start from April 2015.
We have rolled out the online visitor form replacing paper/
fax starting from the S14B semester. We are also developing
another visitor form for Remote Observation Monitor users at
Mitaka.

7. Education (Under-Graduate and Graduate
Courses)
The number of Subaru staff members in Hilo who wereconcurrently appointed by SOKENDAI (graduate school) wasten. The number of SOKENDAI students who had primarysupervisors affiliated with Subaru Telescope (including those
concurrently belonging to Subaru Telescope) was 18 whichconstituted more than a half of the entire 32 SOKENDAI
students hosted in NAOJ. Of which nine had supervisors who
primarily belonged to Subaru Telescope.
In FY 2014, Subaru Telescope hosted four graduate students
for long stays, of which two 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 throughout Japan who
obtained master’s degrees and PhD’s based on Subaru Telescope
data were 11 and 4, respectively. Of which 3 and 1 belonged tothe division of Optical and IR Astronomy, respectively.
We also regularly hosted a series of educational programs
at Subaru Telescope. In September 2014, we hosted a Subaru
autumn school in which 6 graduate and 6 under-graduate
students from all over Japan participated and learned the
reduction and analysis of Subaru Telescope data and heard a
series of lectures. In November, under the recommendationof the Subaru advisory committee, we co-hosted the 1st
China-Subaru workshop in Shanghai in which many students
and postdocs participated. Moreover, in October, we hosted
two Subaru Telescope observation training courses, one forundergraduate students from all over Japan, and the other for
new SOKENDAI students at NAOJ. In the Subaru Telescope
Hilo office, we had regular Subaru seminars in English 2–3
times a month, where open-use observers, visitors, and Subaru
Telescope staff members presented their newest research. Alsoin the Subaru Telescope Mitaka office, we had numerous official
and informal seminars, many of which were jointly organizedwith 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 of 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 2014, there
were 21 web-postings (10 in Japanese, 11 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 45 (24 inJapanese, 21 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 30 (28 in Japanese, 4 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
up-close for guests from Japan and from around the world.
Except for December when the tour program was suspended toallow safe work for the tertiary mirrors’ recoating, a total of 559
people visited through this program. There are 111 additionalgroups who visited through special tour programs and resulted
in the total head count of 1,252 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 base building are most of the time
accompanied by other activities described in the next majortask area, namely: special lectures, hands-on sessions, orpresentations by the student group. A total of 41 groups, with
451 people, visited the base facility this year.
Task3: Public outreach which includes lectures in the local
community, special presentation in the schools, and remotepresentation for Japanese schools or museums. PIO provided/
coordinated 56 lectures at the base facility or in its vicinity
such as at the ‘Imiloa Astronomy Center. There were 12
lectures outside of the island, and 14 remote lectures for off-site
locations. The local lectures included 26 classroom presentations
during the Journey Through The Universe program, and reached
out to 736 students in the local schools.
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. 600 selected students between
grades 4 and 12 (upper elementary school to high school) withfamilies and teachers from all over the island gathered for thisevent. PIO provided 4 hands-on workshops and an exhibit booth.

II Status Reports of Research Activities073

2. Okayama Astrophysical Observatory
The Okayama Astrophysical Observatory, (hereafter theObservatory) serves as the observing and research base of
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.
About 230 nights at the 188-cm telescope are exploited forobservations by researchers from across the country throughopen use every year. The Observatory maintains and operates
the observing instruments and provides the observers withsupport for observations, travel expenses, accommodations,
every day needs, etc. It also engages in improving the open-use
observing instruments, developing new open-use instruments,and supporting brought-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) and use it in acomprehensive survey of infrared-variable objects in the Galactic
plane. Another project is the upgrade of the functionalitiesof the 188-cm telescope in order to improve significantly 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 positively.
The personnel breakdown as of March 2015 was six fulltime staff members, including two associate professors, one
assistant professor, one chief research engineer, one engineer,and one chief clerk; twelve contracted staff members,
including three research experts, one postdoctoral fellow, threeresearch supporters, three administrative supporters, and two
administrative maintenance staffs; and one temporary staff
member.

1. Open Use(1) Overview
The numbers of nights allotted to the open use in 2014 were
122.5 nights for the first semester (2014A, January to June) and
110.5 nights for the second semester (2014B, July to December).
Observing proposals were called for publicly each semester.
The Okayama program subcommittee reviewed the submitted
proposals and accepted 1 project observation program, 1074

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academic degree support program, and 12 general observation
proposals in 2014A, and did 1, 1, and 12 in 2014B. A proposal
from Turkey, one from the Republic of Korea, and one from
Hawai`i were accepted in 2014B and the Observatory supported
their observations with human resources. The anonymous
application system was abolished after 2014A as planned andreverted to the previous system starting from 2014B. Open-use
observation generally proceeded without incident.
(2) Observation/Research Results
The majority of objects observed through the open use in2014 were stellar sources including pre-main sequence stars.
Others included Solar System objects, AGNs, and quasistellar objects. The following primary observation themes
were noted: searching for exoplanets via precise radial velocity
measurement; exploration of the physical properties andactivities of binary stars via high-dispersion spectroscopy; andthe observation of exoplanet transits by precise near-infrareddifferential photometry, which increased precipitously in recent
years. Optical low-dispersion spectroscopic observations ofstars for classification and of sudden phenomena for followups remained significant since last year. 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’s drive and controller were renewed
and the connections between the telescope and the observing
instruments were established by the end of FY 2013. A report
was published on the details of the refurbishment in FY 2014
(Kuroda et al. 2015, Report of the National Astronomical
Observatory of Japan, Vol.17, 19–39). The telescope control
software was elaborately improved to enhance its user-friendlinessand safety while observing as well as its maintainability.
During the maintenance period in June, the annual realuminization of the primary mirror of the 188-cm telescope
and the subsequent optical axis alignment of the smaller mirrors
against the primary were completed. The 1.5-m primary mirrorof the KANATA telescope at Hiroshima University and theprimary mirror of the ISAS 1.3-m telescope were also accepted
for re-aluminization in the period this year. Participants in thealuminization work from these organizations were given NAOJmandated safety and hygiene training as necessary. Lubricationof the telescope and dome was conducted in July. Utmost
efforts were made to maintain high observing efficiency byconducting monthly cleaning of the primary, secondary, andtertiary mirrors of the 188-cm telescope after October. Also
intensive maintenance was applied to the hydraulic system of
the aluminization vacuum chamber, to prevent oil leakage which
had been an issue to be solved for years, including refurbishmentof the oil cylinders and renewal of the oil pipes from September

to March.
The dome was checked daily. Other maintenance work wasalso performed, including repairing the worn-down guiding
rails for the upper and lower slit doors in August, repairing theexternal panels of the dome hemisphere to prevent rain leakage
in June and August, repainting the dome periphery in July,
replacing deteriorated metal mesh at the bottom of the dome
wind channel in August and November, installing an internalroof east of the north pier of the telescope inside the dome toprevent rain leakage from falling onto the observing instruments
in September, repairing the painting of the cat walk floor in
March, renewing deteriorated power lines and contactors (atany time), and replacing old lighting equipment on the firstfloor with LED lights in August. Asphalt pavement around thetelescope dome was renewed as well.
Much attention was paid to the operation and maintenanceof the facility and equipment. It is to be noted that soundproofing work was done for the second time to a visitor’s roomon the second floor of the main building, resulting in four
proofed rooms. Work safety was given priority in accomplishing
the aforementioned maintenance work and observing instrument
exchanges. As a result, no accidents or incidents whatsoever
occurred during FY 2014.
(4) Conferences
The program subcommittee for the 188-cm telescope met
on May 16 and November 14 to evaluate proposals for open
use in 2014B and 2015A (first semester of 2015), respectively,
and formulated an observation program for each semester. The
Okayama Users Meeting, also known as the 25th Optical andInfrared Users Meeting, was held at Mitaka Campus of NAOJ
on August 11 and 12.
Various reports were made: current status of the
Observatory, execution summary of the program subcommittee,
preparation status of remote observing facilities of the 188cm telescope, two user-led plans to develop new observational
instruments for the 188-cm telescope, etc. Reports by others
included research results from open-use projects. Also discussed
were the operations of other optical and infrared observational
facilities such as the Higashi–Hiroshima Observatory and the
networking of small- and mid-sized telescopes. On the second
day of the meeting, a report was given on the progress of Kyoto
University’s Okayama 3.8-m New Technology Optical andInfrared Telescope project and proposals were presented for the
initial research themes, observing instrument plan, and operation
systems before and after completion. The proposals were
followed by a stimulating debate.
In addition, the seventeenth liaison conference oncooperation for astronomical observations at Okayama
Astrophysical Observatory of the National Astronomical
Observatory of Japan led by the Okayama prefectural office washeld in Okayama-city in October 2014, aiming at preserving
the environment for astronomical observations. In the meeting,continuation of the cooperative framework was confirmed
among the participants.

2. Developing 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. Major work
pursued in FY 2014 included replacing the controller computer;
improving the autoguider to cope with dimmer stars throughstray light mitigation and software version-ups; and preparing
for the adoption of KOOLS-IFU (see “(3) KOOLS” below)
into the Cassegrain unit of the HIDES fiber link (see below).
Accepted proposals to HIDES as a whole were 6 and 6 in 2014A
and 2014B, including 1 and 1 project observations, respectively.
The observing capability of HIDES is currently being
improved by introducing fiber links. The high-efficiency fiber
link with approximately 50-K wavelength resolution now offers
an improvement in throughput of nearly one magnitude overthe previous value and radial velocity measurement precisionof approximately 2 m/s, which is comparable to the case of the
Coudé light path. The link test observations were conducted in
2010, and it has been provided for open use since 2011. Two
academic journal papers were published from the use of the fiber
link in FY 2014. Seven open-use programs including those fromthree new PIs and one ToO observation were performed with it
in 2014. It’s usage increased steadily. Besides, a high resolution
fiber link with a spectral resolution of nearly 100,000 was also
developed. It was evaluated by providing it for trial use with the
project observation program since 2015A. It will be provided foropen use in CY 2016.
(2) ISLE (Near-Infrared Imager/Spectrograph)
The instrument ISLE is a near-infrared imager and lowor mid-dispersion spectrograph, and has been available forthe project observations and the academic degree support
programs since the second semester of 2011 (2011B). It is
the only open-use instrument in East Asia that offers nearinfrared spectroscopic capability and is characterized ashaving the world’s best low-noise readout capability (less than
10 electrons). Having achieved a high precision for relative
photometry of one milli-magnitude level, ISLE is in greater
demand for observations of exoplanet transits. The numbers of
open-use programs using ISLE conducted in semesters 2014A
and 2014B were 5 and 3, respectively, which included 1 and 1
academic degree support programs, respectively. Four of themwere spectroscopy and the other four were imaging photometryof exoplanet transits.
(3) KOOLS (Kyoto-Okayama Optical Low-dispersion Spectrograph)
This instrument was made available for open use as a PI-type
instrument in FY 2008 and has since been in stable operation.
The CCD output linearity is good enough. Non-sidereal motion
objects can be tracked for long integration times. The open-use
applications for KOOLS have increased due to a recent rise indemand for spectral classification and monitoring observations.
There are 4 and 6 accepted proposals for 2014A and 2014B,
respectively. An integral field unit (IFU) using a fiber-bundle
was developed by a team at Kyoto University, as one of the

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075

candidate first generation instruments for Kyoto University’s
Okayama 3.8 m New Technology Optical and Infrared Telescope
project. Its input part was installed into the Cassegrain unit of
the HIDES fiber link and its output part into KOOLS under the
support from the Observatory. Its commissioning was performedon two nights provided from the Observatory time. IFU will
be delivered as a PI-type open-use instrument starting fromsemester 2015B. However, KOOLS itself has begun to havevarious small troubles and is in need of intensive maintenancefor long-term usage.
(4) Others
A remote observing environment was prepared to enable
observers to perform their open-use observations with the 188cm telescope from remote sites over the internet in FY 2014.
After testing it many times inside the Observatory, it was
confirmed that smooth observations are feasible from outside
the Observatory with the help of some open-use observers at
remote sites. It will be further polished preparing to open theenvironment for open-use.
Meanwhile, a carry-in instrument newly developed for the
188-cm telescope, “MuSCAT,” was accepted for performanceverification (MuSCAT is an acronym for Multicolor
Simultaneous Camera for studying Atmospheres of Transiting
exoplanets). The Observatory allowed four observing nightsfrom the Observatory time for the commissioning.

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 Nagoya
University and Nano Optonics Energy Inc., regarding the 3.8-m
telescope project as part of the future plan for the Observatory.
Discussions were held on technological issues regarding thetelescope and dome through weekly TV conferences and inperson meetings held every three months. The main telescope
was constructed and tuned in a temporary hanger placed in the
Observatory in FY 2014.
(2) The Optical & Near-Infrared Astronomy Inter-University
Cooperation Program
The Program has entered its fourth 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 35 nights worth of observational
data on seven objects this year. Four of the objects were gammaray bursts, which are the main target of the Program. Afterglows
were detected at multiple sites in the network for three of them.
Another source was observed simultaneously by the Program
and the inter-university VLBI cooperation program as a first076

II Status Reports of Research Activities

trial. Two peer-reviewed papers were published utilizing
OISTER. Another 61 peer-reviewed papers that have something
to do with the Program were published, in 9 of which OISTER
played a vital role. A joint special session “Inter-university
cooperation across radio, optical, and infrared” between the
Program and the inter-university VLBI cooperation program washeld at the annual autumn meeting of the Astronomical Societyof Japan in 2014. The fifth workshop of the Program was held,
this time open for the first time to general researchers who did
not belong to the network. Priority was given to publicizing the
research results from the Program on the web page of OISTER
this FY.
(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 2014, the automatic observation
scheduler performed observations on nearly every possible night;
27 GRBs were observed, with optical afterglows successfully
detected in three. Observation results were published as 16
GRB Coordinates Network (GCN) circulars. Besides, six peerreviewed papers were produced from monitoring of Miravariables and comets and observations of supernovae, AGNs,
and exoplanet transits that were conducted when the telescope
was free.
(4) Other
The Observatory welcomed five third-year undergraduate
students and the supervisor from the University of Tokyo
between August 14 and 15 and provided them with anopportunity to conduct high-dispersion spectroscopic
observation using the 188-cm telescope during the early half ofthe night on August 14. A summary of this activity over the past
several years was presented by the supervisor on a poster at theusers’ meeting held on August 11 and 12.

4. Unique Research Projects(1) Detection of the Afterglow of Distant GRBs and Survey of
Variable Stars in the Galactic Plane Using the Ultra-Wide-Field
Infrared Camera
A project is underway to identify infrared counterparts forobjects such as distant GRBs and gravitational wave sources andto comprehensively survey infrared variable stars in the Galactic
plane by converting the 91-cm telescope into an infrared
camera with an ultra-wide field of view of 1 square degree.
Almost uniform imaging quality was achieved across a square
field of view of 0.48 degree by 0.48 degree (for 1-k detector)
after a fine adjustment of the telescope optics in FY2014. An
automatic focusing mechanism was installed and semi-automatic
observations became available. A pilot monitoring program wasinitiated in the Ks-band toward a selected area in the Galactic
Plane to assess the feasibility of variable star surveys.
(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 functionality 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. A function
was developed to automatically correct for the drift of the best
focus position by inferring the drift based on the temperature
distribution across the telescope tube through thermos-sensors
attached to the telescope truss tube in FY 2014 (see Kamiya
et al. 2014, V220a at the Annual assembly of the autumn ASJ
meeting 2014). Another new functionality was investigated tofurther improve the telescope pointing by measuring the small
movement of the primary mirror in the cell and correcting thepointing error due to the movement, which would help advancethe automation of the telescope operation and observation.
(3) East Asian Planet Search Network
The Observatory also conducts studies focusing on the
search for exoplanetary systems, involving researchers fromThe Republic of Korea, the People’s Republic of China, theRepublic of Turkey, and Russia. The efforts continued in FY
2014 to secure telescope time on the Korean 1.8-m telescope,
Chinese 2.16-m telescope, Turkish 1.5-m telescope, and theObservatory’s own 1.88-m telescope for continued searches for
exoplanetary systems around G-type giant stars. One exoplanetcandidate was discovered from the collaboration with Chinesecolleagues, and four binary systems consisting of a G-type

giant and a low-mass companion were identified through thecollaboration with Turkish and Russian colleagues in this fiscal
year. Both results were published in peer-reviewed journals.

5. PR/Awareness Promotion Activities
An Observatory representative delivered a lecture tonearly 20 people in Okayama City on Monday, July 7 as partof the Nation-Wide Tanabata Participatory Lectures. Nearly
50 astronomy-related questions from the public were posed
irregularly to the Observatory and were answered appropriately
this year. The 4D2U screening, co-hosted with the Okayama
Astronomical Museum, attracted 3,854 visitors.
Twenty-two Observatory tours were conducted, including
those for pupils from local elementary schools in Asakuchi city
and Yakage town. The Observatory also responded to six lecture
requests made by local boards of education and community
centers.

6. Contract Staff Transfers
The following transfers of contract staff members took place
in FY 2014: Kouki Kamiya joined as a Research Supporter in
October and Hiroyuki Maehara did so as a Research Expert inNovember. Research Supporter Yasuhiro Shimizu left at the
expiration of his term at the end of March. Postdoctoral Fellow
Akihiko Fukui left the position at the end of March when his
term expired.

3. Nobeyama Radio Observatory
1. 45-m Radio Telescope(1) Open Use Observations
The 33rd open use observations started on December 15,
2014 as scheduled (observers for the backup program stayed in
the observatory starting from December 1, 2014).
The statistics of the proposals are as follows,“General Proposal 1st period”: 16 accepted including 5 fromabroad (34 submitted),“General Proposal 2nd period”: 13 accepted including 4 fromabroad (21 submitted),“Short Program”: 9 accepted (15 submitted),“Education Program” (1st and 2nd periods): 0 accepted (0submitted).
“Backup Program”, which is carried out when weather is not
acceptable for the main observations: 1 accepted (1 submitted).
In addition, the 45-m telescope joined the VERA open use
observations: 3 proposals.

The multi-beam receiver BEARS and the AC45 spectrometer
were decommissioned.
(2) Improvements and Developments
Maintenance of the 45-m telescope, the receiver systems, thecryogenics, etc. were performed.
• The antenna foundation made of concrete was leveled becauseof its unacceptable amount of tilt. The design was completed
for the subreflector servo system replacement to be installed
next year.
• End to end holographic measurement tests were done aiming
to improve the surface accuracy of the 45-m telescope.
• Test measurements for the improvement of the performance ofthe beam transmission system were carried out.
• The new multi-beam receiver FOREST was installed and used
for the legacy project observations (observatory internal use)after basic performance evaluation and test observations.
• New AD converters were installed in the 4 intermediate
frequency lines among the 16 lines and were used in open-use
observations. They exhibit smaller frequent-spurious-signals

II Status Reports of Research Activities077

and show better linearity performance.
• NRO supported user instrument including the Z45 receiver at
45 GHz band, digital spectrometer ROACH, and a 90/150 GHz
continuum camera.
• The help desk for open-use observers became operational, andits manual was released.
(3) Scientific Results
We are carrying out the (a) Star Formation Legacy Project,(b) Galactic plane Survey, and (c) Nearby Galaxy Project aslegacy projects with the 45-m telescope. The star formation
project and the Galactic plane survey project obtained scientific
data and their results are described below.
(a) Star Formation Legacy ProjectIn the Star Formation Legacy Project, we conducted largescale mapping observations toward nearby star-forming regions:
the Orion A molecular cloud and W40 H II region in 13CO andC18O. For the Orion A cloud, we combined the 45-m 13CO datawith the CARMA interferometer data to obtain a 13CO largescale map whose angular resolution is about 5 arcsecond. Fromthe combined map, we identified many filaments in the cloud.
For the W40 region, we found shell-like dense molecular gas
clumps around the H II region. The comparison between theinfrared data and the 45-m data suggest that the gas clumps areinteracting with the expanding shell created by the H II region.
(b) Galactic Plane Survey Project
We are conducting a simultaneous survey of the 12CO, 13CO,
and C18O J = 1–0 emission lines in the Galactic Plane using
the new multi-beam receiver FOREST installed on the 45-m
telescope. We plan to make maps of the inner Galaxy (10d < l <50d, b = ±1d) and the outer Galaxy (198d < l < 236d, b = ±1d)including the spiral arms and bar structure. In 2014, we covered
areas with 24 and 7 square degree for a total of 31 square degree.
We have revealed a wide range of molecular clouds and theirfine structures, e.g. filaments that have not been seen in previous
surveys.

2. SPARTTo better understand the influence of the activities of hoststars on the middle and lower atmospheres of terrestrial planets,
including solar system planets and exoplanets, we have been
performing monitoring observations for millimeter-waveband
spectral lines of carbon monoxide (12CO J = 1–0: 230.538 GHz,J = 2–1: 115.2712018 GHz, 13CO J = 2–1: 230.3986765 GHz)in the middle atmospheres of Mars and Venus with a 10-m
telescope, the Solar Planetary Atmosphere Research Telescope(SPART), since it was launched in 2011. The SPART employs
highly sensitive 100- and 200-GHz double-band superconducting
SIS heterodyne detectors and a 1-GHz-band digital fast-Fouriertransform spectrometer with a frequency resolution of 61 kHz.
Heterodyne spectroscopy with high frequency resolution is a
powerful tool for observing the weak and narrow spectral lines
of minor constituents in the middle atmospheres of planets.

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II Status Reports of Research Activities

This season we repaired the elevation-motor of the telescope.
An example of the results we found from the SPART monitoringis that the disk-averaged mixing ratio of carbon monoxide derived
at an altitude of approximately 80 km in Venus has slightly
changed since 2012. This phenomenon may be linked to solar
activities in the current 24th solar cycle. Middle atmospheres ofterrestrial planets like Mars and Venus lacking magnetospheres
may be directly affected by energetic events of the host stars.
Over the coming six years solar activities will be lowered
toward the solar minimum phase. Therefore, it is important
to continue the monitoring research with the SPART for
understanding of how atmospheric conditions of terrestrial
planets balance physically and chemically under activities ofhost stars.

3. Development of a Multicolor Millimeter/
Submillimeter Camera for the Atacama
Submillimeter Telescope Experiment (ASTE)
Extensive large-scale sky surveys in the millimeter/
submillimeter bands with a multicolor continuum camera are
indispensable for various types of research including estimating
the redshift of submillimeter galaxies, using the SunyaevZel'dovich effect to study the internal structure of hot plasma
in clusters of galaxies, and constraining the physical propertiesof the dust in star-forming regions and the spectral index of theinitial submillimeter afterglow of gamma ray bursts (GRBs).
Thus, we, in collaboration with the University of Tokyo,
Hokkaido University, the University of California Berkeley,
and McGill University, are developing a multicolor millimeter/
submillimeter camera based on a very sensitive Transition Edge
Sensor (TES) bolometer for observations at wavelengths of 1.1
mm, 0.87 mm, and 0.46 mm.
We deployed our bolometer camera on the ASTE Telescopeduring March and April of 2014. At that time, thanks to theexcellent observing conditions, we managed to explore the starforming regions in our Galaxy, submillimeter galaxies, and
GRBs outside our Galaxy. Thus, this year, we’ve been focusedon analyzing the observational data obtained in that run, andimproving the performance and efficiency of the observing
system based on these results. We’ve worked out the solution
to the problems in the yield of the bolometer array and thereadout device, and the time consuming algorithm for tuning
the operating parameters of the bolometers. Solving these
problems will increase the observing sensitivity and efficiency,
respectively. Furthermore, we’ve worked on an issue inherent tobolometers with TES sensors; namely that they lose sensitivity
if the weather improves after they have been tuned. We came up
with a solution to overcome this issue by employing a movable
blackbody radiation source. This will drastically widen the range
of weather conditions for which observations are possible.
In order to increase the number of observing bands in the
future, increasing the number of pixels read out is inevitable.
Therefore, the multiplexing technologies to double the numberof bolometer pixels read out per readout device from 8 to 16
were carefully considered. As a result, we showed that increasingthe multiplexing factor to 12 pixels per a readout device ispossible with minor changes to the current readout system.
Finally, we’ve started the development of the add-on fore optics
which will open a new window to conduct polarization sensitive
observations with our bolometer camera.

4. Misc.
(1) PR Activities at the Nobeyama Campus
The Nobeyama Campus has been accessible to the public
since the inauguration of the observatory in 1982. The numberof visitors this summer decreased compared with previous years
due to bad weather. The campus received a cumulative total of
51,535 visitors throughout the year, including participants of thespecial open house events in August. This is the smallest number
except the opening year 1982. Staff members conducted 30
guided tours, including tours for Science Partnership Programs(SPPs) participants, Super Science High School (SSH) students,
and the Campus Tour Week. Additionally, five requests for
lectures and 22 requests for on-site filming and interviews were
granted. These kinds of requests increased owing to improved
relations with Local Communities.
The Campus Tour Week was scheduled during summer andwas aimed at educational institutions (elementary, junior high,and high schools). Staff members gave guided tours for thisprogram as well. Six groups took advantage of this opportunity.
Most visitors from the participating schools said they thoroughly
enjoyed their visits. For the workplace visit initiative conducted
between July and October, 18 students from 7 schools, primarily
local junior high schools, visited the observatory and had achance to experience the observatory’s routine work understaff guidance. For SPP/SSH initiatives, six schools visited the
NRO and participated in lectures, student presentations, andhands-on guidance of future activities. Furthermore, the Radio
Astronomical Observations workshop using the 45-m radio
telescope was held again this year from June 2 to 6, with 12
undergraduate students in attendance. Because senior students
can take part in the workshop in June, the grade compositionof the participants is different from the normal year. Although
instruction to the students, from observations to presentationof the results, requires significant staffs’ effort, the event offers
an invaluable opportunity for undergraduates to experienceobservations using a radio telescope.
In the area for permanent public access, an antenna model
is available along with posters and panel displays. A video
continuously played in the visitor room shows various facilities,
introduces the history of the NRO, and explains research resultswith the 45-m telescope. For Internet-based PR activities, the
NRO runs a website which is expanding to include observational
results as well as introductory descriptions of radio astronomy.
In particular, these posters, panel displays, and web pages
were modified to reflect the close of Nobeyama Solar Radio
Observatory at the end of the fiscal year.
(2) Cooperation with Local Communities
The annual Nobeyama Special Open House Day was heldwith contributions by Nagano Prefecture as well as Minamimaki
Village, and the Minamimaki Chamber of Commerce alongwith its youth division. Jimoto Kansha Day (Thanks Day for
the Locals) was held as the Special Open House for locals(Minamimaki and Kawakami villages) with Nobeyama Station of
Education and Research, Center of Alpine Field Science, in the
Faculty of Agriculture of Shinshu University and Yatsugatakeforest in the Agriculture and Forestry research center of Tsukuba
University. Special sponsorship was provided to the Sora-girl
event “Tebura de Hoshizora Kansho-kai” (“Drop-by Star Gazing
Event”) hosted by the Minamimaki Tourism Association. The
NRO also joined the Japan Three Major Scenic Location for Star
Gazing with the Minamimaki Tourism Association: Night Sky
Summit that took place in Ishigaki City, Okinawa Prefecture.
Also, two lectures were held 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).
(3) Referbishment Plan for the Nobeyama Millimeter Array
Building
The building for the Nobeyama Millimeter Array will berenovated to install an exhibition area focusing on the National
Institutes of Natural Science (NINS) as well as the NAOJ, inorder to establish a PR center for not only astronomy, but also
for all of the natural sciences. The preliminary survey and thedesign of the building were complete before the construction
work scheduled in the next year.
(4) NRO Conference Workshops• July 15, 2014
NRO Galactic Plane Survey Mini-Workshop (representative:
Tomofumi Umemoto)• July 23-24, 2014
32nd NRO Users Meeting (representative: Shuro Takano)• July 28-31, 2014
44th Summer School on Astronomy and Astrophysics for
Young Researchers 2014 (representative: Akira Oka)
(5) Education
NRO accepted two postgraduate students. The one visiting
student from Kagoshima University got a Ph.D. on polarization
capability of a new receiver this year. The other visiting student
from Toho University got her Master degree on chemical
reaction of carbon chain molecules.
(6) Part-time Research Staff Transfers• Specially Appointed Research
Tatsuya Takekoshi: Specially Appointed Research, NAOJ
Chile Observatory• Researcher
Kana Morokuma: Specially Appointed Research, NAOJ Chile
Observatory• Researcher Supporter
Hiroyuki Nishitani: Engineer, NAOJ Nobeyama Radio
Observatory

II Status Reports of Research Activities079

4. Nobeyama Solar Radio Observatory
1. Closure of the Nobeyama Solar Radio
Observatory Project and Future Operationof the Nobeyama Radioheliograph and theNobeyama Radiopolarimeters
The termination of the operation of the Nobeyama
Radioheliograph (NoRH), which has been the main observational
instrument of the Nobeyama Solar Radio Observatory (NRSO),
was scheduled to occur in FY 2014. Along with this, the closureof NSRO was also scheduled at the end of the FY 2014. On theother hand, some users had thought to continue the operation of
the Radioheliograph. They proposed that the Solar Terrestrial
Environment Laboratory (STEL) of Nagoya University borrows
the instrument from NAOJ and operates it through cooperation
with an international consortium (ICCON) formed by someinstitutes, both foreign and domestic, who are willing to help
the operation financially. NAOJ approved this proposal, and an
agreement between NAOJ and Nagoya University was madeto continue the operation of NoRH for three (six at maximum)
years, with technical support by the Nobeyama Radio
Obseravtory (NRO).
The continuation of the operation of the Nobeyama
Radiopolarimeters (NoRP) was also requested by some users.
NAOJ decided to transfer it to NRO from NSRO to continue theoperation.
Data from these instruments will be released by the
Astronomical Data Center of NAOJ and STEL of Nagoya
University from now on, and the environment for the data
analysis has been prepared. Researchers in the world can freely
access the data as always.
Because it was decided to continue to operate instruments,
maintenance work has been done intensively in this fiscal year
to operate the instruments steadily after next fiscal year. It was
decided to move the personnel of NSRO who are working at
the Nobeyama campus to NRO, where they will deal with theremaining work for the solar radio instruments as a part oftheir duties. Various duties of NSRO were mainly taken overby NRO, and the NSRO project was dissolved at the end of FY
2014 as scheduled.

2. Radioheliograph- and Radio PolarimeterBased Solar Observations
At the beginning of FY 2014, operation of NoRH and NoRP
were assumed to be terminated in the middle of the fiscal year
to wind up the NSRO project. However, because it was decided
to continue the operation of both of the instruments from FY
2015 on, the termination of the operation was cancelled and thesolar observations until the end of the fiscal year were continued
almost stably, though there was some instrument trouble.

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3. Open Use, Joint Research, and Consortium
Activities
All observational data are made available to the public, andresearchers working in relevant fields in Japan and abroad have
utilized this information for their studies on solar phenomena,
space weather, and space climate. The data are also leveraged
for the purposes of education and PR. A consortium of university
users, represented by Satoshi Masuda, promotes open use inJapan (http://solar.nro.nao.ac.jp/HeliCon_wiki/). A data analysis
workshop (CDAW14: September 29–October 3, 2014) held toactively promote open use in Japan had 18 participants. Lecturesand exercises were offered; four groups practiced data analysis,
and attendees subsequently reported the experience at various
research conferences and to the astronomical society. The Japan
Solar Physics Community held a symposium entitled “Solar
Activity at the 24th Solar Maximum and Future Prospect for
Solar Physics” at Nagoya University from February 16 to 18,
and the Observatory presented its undertakings as well as studies
conducted during CDAW14.
Drs. H. Ezawa and H. Matsuo of NAOJ carried out anexperiment to use NoRH as an intensity interferometer, and they
confirmed that NoRH element antennas can work as an intensity
interferometer.
Regarding visiting international researchers, Drs. B. Hnat,
D. O'Connell, and D. Kolotkov from the University of Warwick(UK) studied oscillatory phenomena using the data from NoRH.
Drs. J. Huang and Y. Zhang from the National Astronomical
Observatories of China studied solar flares and their precursors.
From the USA, Dr. S. White made synoptic charts of the circularpolarization to investigate the global chromospheric magnetic
field, and Dr, S. Yashiro (NASA) prepared tools for remote
operation by members of ICCON.

4. Other
An issue of the Astronomical Herald, entitled “The Special
Issue for the Nobeyama Radioheliograph”, including six articles
related to NoRH, was published by the Astronomical Societyof Japan. Graduate students of SOKENDAI, Tokai University,and Ibaraki University, and undergraduate students of Shinshu
University and Meisei University studied solar physics with thedata from NSRO. The Cutting Edge Solar Research Experience
Tour, which was organized jointly by solar-related research
institutions in Japan, offered lectures and a guided tour of theobservatory to 11 participants. Regarding initiatives aimed forhigh schools, Komagane Technical High School in Nagano
installed its own radio telescope, for which the observatory
rendered support, and its students participated in the SPP
program, and the observation results from this telescope were
presented to the junior session of the Annual Spring Meeting of
ASJ.
At the end of the fiscal year, K. Shibasaki (Professor)

retired. K. Iwai (Postdoctoral Fellow) departed upon completionof his term. From the next fiscal year, M. Shimojo (AssistantProfessor) will belong to the Chili Observatory, and N.

Shinohara (Senior Engineer), M. Takemura and H. Shinkai(Administrative Supporters) will belong to NRO.

5. Mizusawa VLBI Observatory
At NAOJ Mizusawa VLBI Observatory, we operate VLBI
(Very Long Baseline Interferometry) facilities such as VERA(VLBI Exploration of Radio Astrometry) and KaVA (KVN
and VERA Array), and provide these unique facilities to theuser community in Japan and East Asia to support the research
activities at universities and research institutes. At the sametime, we conduct astronomical research using these VLBI
arrays on the Galactic structure, star-forming regions, latetype stars, AGNs and so on. In addition to the operation of
VERA, which is a dedicated array for VLBI astrometry, we
support the maintenance and operation of the Yamaguchi 32-m
Radio Telescope and two 32-m radio telescopes at Ibaraki incollaboration with local universities. Furthermore, we promoteinternational collaboration, particularly in the East Asian
region through the joint operation of KaVA and the East AsianCorrelation Center at KASI (Korea Astronomy and Space
Science Institute) as well as through preparatory operation of
the East Asian VLBI Network which is a joint array between the
People’s Republic of China, Japan, and the Republic of Korea.
Also we keep Japan Central Standard Time as an
obligation of NAOJ, and maintain Esashi Earth Tides Station
for geophysics researches, and Ishigaki-jima Astronomical
Observatory mainly for public outreach.

1. VERA(1) Observations and Common Use Observations
The four stations of VERA were operated by remotecontrol from AOC Array Operation Center) at NAOJ Mizusawa
Campus. In FY 2014, we conducted a total of 399 (3,733 hours)
observations with VERA, such as common use observations,project observations, 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.
VERA common-use call-for-proposals with the 43, 22, and
6.7 GHz bands for semesters 2014B (July to December) and2015A (January to June) were released in June and November,respectively. A total of 15 proposals, which requested a total
time of 632.5 hours, were submitted.
Referees elected from scientists in related fields and by the
VLBI program committee evaluated the proposals and a total of
9 proposals (270.5 hours) were accepted in 2014B and 2015A.

(2) Science Result
Last year, we continued the project observations of
VERA and produced science outputs on high-accuracy maser
astrometry. In particular, we have published the third VERASpecial Issue in PASJ (Publications of the Astronomical Societyof Japan) succeeding the previous ones in FY 2008 and FY
2011. In this special issue, seven papers were published in FY
2014, and more papers are to come in another volume. The
published outputs in FY 2014 include astrometric measurementsof Galactic star-forming regions IRAS 20056+3350, IRAS
20143+3634, IRAS 22555+6213, NGC 2264, NGC 6334,
and late-type stars RW Lep, T Lep and so on. Also, we havebeen continuously trying to improve the astrometric accuracyof VERA. We are now getting hints of parallaxes for 10-kpc
sources. We will continue this activity and will hopefully be able
to regularly obtain parallaxes for 10-kpc sources.
We also conducted simulation work to evaluate the accuracyof Galactic parameters that would be obtained by VLBI
astrometry of 300 to 500 maser sources. It turned out that those
Galactic rotation parameters would be determined to the level ofa few percent and parameters of perturbations (such as spirals)
would be determined to the 10 percent level, provided parallaxes
could be measured for a few hundred sources. In addition tothis work, we published a review paper summarizing the mostup to date science outputs and technology development of highaccuracy VLBI astrometry.
Beyond VLBI astrometry, VERA produced interesting
results on Orion-KL source I through joint observations with
ALMA, and also on gamma-ray active AGN monitoring as apart of GENJI (Gamma-ray Emitting Notable AGN monitoringwith Japanese VLBI) program.

2. JVN (Japanese VLBI Network)
JVN is operated as a joint research project of NAOJ andseven universities. JVN consists of VERA and radio telescopes
operated by universities and research institutes, ISAS, JAXA,NICT, and GSI, distributed throughout Japan. VLBI observations
by JVN were done for 400 hours at 3 bands of 6.7, 8, and 22
GHz in FY 2014. Single Dish Observations related to JVN werealso done from 2,000 to 4,000 hours at each telescope.
The main subjects of research are active galactic nuclei andmasers-star formation.
Scientific results obtained with JVN were published as four
papers, while eight more papers reported JVN related scientific

II Status Reports of Research Activities081

studies. FUJISAWA Kenta et al. (2014) reported the first result of
a 6.7 GHz methanol maser survey by JVN, where the Shanghai
25-m Telescope took part in the observation. This is the first
result of EAVN (East-Asian VLBI Network) Observatory.
Masers can be used as tracers for gases around high-mass youngstellar object. SUGIYAMA Kouichiro et al. (2014) reported
the first detection of rotation and infalling motions around ahigh-mass YSO, Cepheus A-HW2. The Astronomical Societyof Japan held a special session of “University Collaboration in
Astronomy” in “The 2014 Autumn Meeting”, in which morethan 30 invited contribution review talks were presented.
Education is also one of the aims of university collaboration
in VLBI. More than 20 students conducted under-graduate study
using JVN. Similarly, more than 10 master-course students
completed their master’s theses using JVN, and two Ph.D.
students finished their theses using JVN directly or indirectly.
Research meetings related to JVN were held six times in FY
2014, and many university students made presentations and talks
in these meetings.

3. Japan-Korea VLBI
(1) Observations and Common Use Observations
A total of 80 (757 hours) VLBI observations, common use
observations, and test observations were conducted by KaVA(KVN and VERA Array) with the 43 and 22 GHz bands. The
data of the seven VLBI stations were correlated at the KoreaJapan Correlation Center at KASI Daejeon campus in Korea.
KaVA common-use call-for-proposals for semesters
in 2014B and 2015A were made in June and November,respectively. In total, 14 proposals requesting a total time of
498 hours were submitted. Through the evaluations by referees
elected from scientists in related fields and subsequent decision
made by the VERA and KVN combined Time Allocation
Committee, a total of nine proposals (330 hours) were acceptedin 2014B and 2015A.
(2) Results of Research
Last year, we published two refereed papers reporting on
the initial results of KaVA observations. One of the reports
was on the first VLBI images of 44 GHz methanol masers inmassive-star-forming regions, and the other showed the AGN jet
imaging capability of KaVA. These papers are the first papers
ever made based on KaVA data, and both demonstrate the highimaging capability of the seven station array. Furthermore,another paper is under preparation to report multi-transition
SiO maser observations of late-type stars. These activities are
made through KaVA science working groups consisting ofresearchers not only at NAOJ and KASI, but also at universities
and research institutes in Japan and Korea. These KaVA science
working groups have been discussing and preparing the KaVA
large programs, in which relatively large amounts of KaVA
observation time will be invested, so that the science outputs anduniqueness of KaVA will be further extended.

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4. EAVNEAVN has been developed under the agreement of our
Consortium. An observation team for conducting EAVN test
experiments, which consists of representatives from Japan,
China, and Korea, was organized in FY 2013. Since then, theteam has been leading VLBI experiments linking existing radio
telescopes in East Asia through close international collaboration.
In FY 2014, VLBI experiments aiming to detect interferometricfringes from the telescopes in East Asia have been conducted
several times. The telescopes which participated in theexperiments were: VERA and 32-m telescopes located at
Yamaguchi and Ibaraki Universities, the Tsukuba 32-m
Telescope, Shanghai 25-m and 65-m Telescopes, Kunming 40-m
Telescope, Urumqi 25-m Telescope, and three telescopes of
the Korean VLBI Network. The experiments were conducted
at 8 and 22 GHz, and VLBI data were processed by using the“Korea-Japan Correlation Center” located at Daejong in Korea.
VLBI fringes were detected from most of these telescopes anddetailed data analysis is ongoing.
These activities are being reported in EAVN workshops
which are held almost every year, where future plans forexperiments are discussed as well. The latest EAVN workshop
was held in the Republic of Korea. And this year, the workshop
will take place in July at Sapporo.

5. Geodesy and Geophysics
The regular geodetic sessions of VERA are allocated two or
three times every month to maintain baseline accuracy. Amongthese geodetic sessions, VERA internal geodetic observations
are performed once or twice every month at K-band, andMizusawa and Ishigaki-jima participate in IVS sessions at S/
X-band on a once per month basis. Thanks to the high sensitivity
at K-band, the maximum number of scans at K-band is 800 per
station per day. In FY 2014, we participated in six T2 sessions
and four JADE sessions.
VERA internal geodetic observations were carried out 17
times. The final estimation of the geodetic parameters is derived
by using the software developed by the VERA team.
After “The Great East Japan Earthquake” (Mw =9.0), VERA
Mizusawa was displaced by coseismal crustal movement andpostseismic creeping. For FY 2014, the creeping continued,
though the speed declined. According to the newest analysis, thecoseismal steps are X = −2,013 mm, Y= −1,380 mm, and Z =−1,072 mm, and the displacement by creeping during 2014 is X
= −91 mm, Y = −61 mm, and Z = −31 mm.
Continuous GPS observations at VERA stations are carriedout in order to detect short term coordinate changes and to
estimate atmospheric propagation delay. The results of GPS
positioning also show large postseismic creeps even though
4 years have passed since the occurrence of “The Great East
Japan Earthquake.” The crustal deformation observed by thestrainmaters at “Esashi Earth Tides Station” is consistent withthe postseismic displacements observed by VLBI and GPS.
Continuous gravity observations with superconducting

gravimeters are carried out at Mizusawa and Kamioka. Similar
observation is carried out at Ishigaki-jima as a joint project withother university groups. The features of the annual change areobserved and studied by several techniques including VLBI,
GPS, and gravimeters.

6. System Development
We replaced the magnetic tape recorders with new harddisk recorders and also replaced the FX correlator working
at a 1 Gbps data rate with software correlation. We confirmed
sufficient performance in scientific processing and continuous
operation after small revisions to the software. We allocatedthe software correlator systems to Mizusawa, and contributed
modifications to the KJCC (Korea-Japan Correlation Center)system with scientific evaluations of the observations by
KaVA. We started intense consideration of future plans for theobservatory. A possible plan to join the SKA (Square Kilometer
Array) project and the development of high frequency VLBI
are being discussed. We performed several basic development
projects including ultra-wideband A/D convertors and a highaccuracy antenna surface for the primary reflector for mm/submm VLBI observations.

7. Timekeeping Office Operations
The Timekeeping Office operates four cesium atomic
clocks together with a hydrogen maser atomic clock at
Mizusawa VERA 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; more than
900,000 daily visits have been recorded last year.
The master clock has been changed from Cs8 to Cs6,
which showed better stability characteristics than Cs8 lastyear. The layout of the Timekeeping Operation Room has beenreorganized because VERA AOC has been moved from Mitaka
to Mizusawa.

8. Ishigaki-Jima Astronomical Observatory
Thirteen years have passed since the completion of VERA
Ishigakijima and the start of the “Star Festival of South Island”
in Ishigakijima. As the main event of the star festival, 8,000
people participated in the “Light-down Starry Sky Party”, eventhough it was cloudy.
In unison with “Star Festival of South Island”, the first“Meteorite Exhibition” ever held in Okinawa Prefecture washeld in cooperation with Nayoro Municipal Observatory, and754 people enjoyed the exhibition.
The Annual Planetarium Screenings were held from August
7 to 10, and 734 people participated.
The Second Japan Starlight Sky Summit was held in
Ishigakijima on October 19 in cooperation with the Bisei

Astronomical Observatory and the Nobeyama Radio Observatory.
Professor HASEGAWA Tetsuo who is the director of NAOJ
Chile Observatory gave a memorial lecture in which 350 people
participated. At the same time, we performed the planetarium
program “Wish upon a star of the Southern Island”, which was
jointly hosted by Ishigaki-jima Observatory and Ishigaki-City.
1,364 people came and enjoyed this program from October 17 to
23.
These activities of NAOJ Ishigakijima Astronomical
Observatory greatly contribute to not only observational studies,but also to regional development such as school education,
lifelong learning, tourism, and so on, through cooperation withlocal communities.

9. Public Relations (PR) and AwarenessPromotion Activities(1) Open House Events
On April 13, 2014: the Fifth Open Observatory Event held at
the Ibaraki University Center for Astronomy, and NAOJ
Mizusawa VLBI Observatory, Ibaraki Station, withapproximately 700 visitors.
On July 6: The Star Festival at the site of the 6 m antenna at Kinko
Bay Park in Kagoshima-city co-hosted with Kagoshima-Cityand Kagoshima University, with approximately 350 visitors.
On August 10: the Special Open House of VERA Iriki Station
was supposed to be jointly held with “The Yaeyama Kogen
Star Festival 2014”, but was called off due to a strong
typhoon.
On August 16: A mission briefing session by WAKATA Koichi,
an astronaut of JAXA (Japan Aerospace Exploration
Agency) who stayed on the ISS (International Space Station)
as the commander, held as an event related to “Iwate Galaxy
Festival 2014”, with approximately 1,000 visitors.
On August 30: “Iwate Galaxy Festival 2014”, open house of the
NAOJ Mizusawa Campus, held with 847 visitors.
On October 19: In cooperation with Bisei Astronomical
Observatory and Nobeyama Radio Observatory, “The second
Japan Starlit Sky Summit” was held in Ishigaki-city, and 350
came to the main meeting places such as a memorial lecture
by HASEGAWA Tetsuo (ALMA), 1,364 entered screeningsof the planetarium “Wish upon a star of the Southern Island”
which were held at the same time (October 17 to 23) inIshigaki-jima Astronomical Observatory and Ishigaki-city.
On February 15, 2015: “The 14th Star Island” open house eventof VERA Ogasawara Station was held, with 213 visitors.
(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 17,021b) VERA Iriki Observatory 2,000c) VERA Ogasawara Observatory 7,535d) VERA Ishigaki-jima Observatory 2,754

II Status Reports of Research Activities

083e) Ishigaki-jima Astronomical Observatory 12,790(3) Review of the Contents of Our Website
Websites related to the Mizusawa VLBI Observatory and thenumber of visitors are:Contents list
Mizusawa VLBI
Observatory
VERA Mizusawa
Observatory
KIMURA Memorial
MuseumVERA Ishigaki-jimaObservatory

Sessions Internet users Page Views
23,894

15,24775,769

9,163

6,307

30,829

1,657

1,313

5,319

80,92051,662

185,037

10. Education(1) Undergraduate and Graduate Education
The Observatory accepted three graduate students fromthe University of Tokyo and two from SOKENDAI (Graduate
University for Advanced Studies). A student from the Universityof Tokyo was conferred a Ph.D. and awarded the Universityof Tokyo President’s Prize. Two master’s students, one from
Tokai University and another from Kagoshima University, were
accepted as visiting graduate students and completed master’stheses. Undergraduate students from Tohoku University,

Okayama University, Yamaguchi University, and Kyushu
University were accepted as summer students of SOKENDAI.
The University of the Ryukyus and NAOJ began offering thisjoint course in FY 2009. Classroom lectures at the university
took place on August 11, 13, 14, and 15, and observational
workshops were held in Ishigaki-jima from August 25 to 28,
with a total of 31 participants. A hands-on radio observation
program was conducted at the VERA Ishigaki-jima Station
and Ishigaki-jima Astronomical Observatory. In addition, staff
members at the station visited these universities to deliverlectures.
(2) High School Student Hands-On Events“The 8th Z-Star Research Team Workshop” was held to use
the VERA Mizusawa antenna; five high school students from
Iwate prefecture were accepted. A preliminary session was held
June 28 and 29, and observations were done August 2 to 4. As
a result, students successfully discovered a new maser source.
During August 18 to 20, VERA Ishigaki-jima Station and
Ishigaki-jima Astronomical Observatory held “The Churaboshi
Research Team Workshop” for thirteen high school students
from Okinawa, Fukushima, and Fukuoka prefectures. It wasorganized with support from JSPS. One of the groups detected
a new maser source using the VERA Ishigaki-jima antenna. The
Observatory supported the SSH (Super Science High School)
research activities for a high school in Akita Prefecture using theMizusawa 20-m antenna.

6. Solar Observatory
The Solar Observatory primarily engages in the operationof solar observational facilities on the west side of Mitaka
Campus. It conducts both observational and theoretical studiesof the structure of the outer solar atmosphere, including thephotosphere, chromosphere, corona, and solar wind, andactive phenomena such as sunspots, faculae, prominences, andflares. This observatory performs regular observations using
instruments such as the Solar Flare Telescope (SFT) and also
conducts expeditions to observe total solar eclipses. It is also
engaged in the development of new observational instruments
and the planning of future ground-based solar observations.
Regular observations of sunspots and flares have been carriedout for extended periods, and the resulting data are provided toresearchers.

1. Observational Facilities in Mitaka(1) Magnetic Field Observation
The SFT, which has been the main instrument of theobservatory at Mitaka Campus, has continued observations ofactive region photospheric vector magnetic fields and H-alpha084

II Status Reports of Research Activities

flares since its completion of 1992. The main instrument on
the SFT since 2010 is an infrared Stokes polarimeter. Whereas
previous magnetic field observations covered part of thesolar surface, this instrument is designed to perform full-disk
polarimetric observation to obtain high accuracy vector magnetic
field information in order to shed light upon the origins of the solar
activity cycle. This polarimeter is equipped with a 15-cm infraredlens and performs slit scanning observations 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 constant acquisition of unprecedented infrared
polarization data for the photosphere and chromosphere of
the entire solar disk. It had taken about two hours to cover thefull Sun with a slit scan for each wavelength range, but a new
system which enables us to observe two wavelength ranges
simultaneously using two cameras has just been installed. Now
the new system is under testing, and after its completion, thedata acquisition will be conducted more efficiently.
In this fiscal year, concentrated maintenance work for the
SFT was done, and some deteriorated parts of the telescope were
replaced.

(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
with a 10-cm refractor and a 2 k × 2 k pixel charge coupleddevice (CCD) camera mounted on the new (full-disk) sunspot
telescope. Observations were conducted for 261 days in 2014,
from January to December. A huge sunspot, which is the largest
one in the last 24 years, appeared in this year. The Hinodeproject and the Solar Observatory jointly released some related
images to the public on November 19.
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
are underway to update the photospheric and chromosphericimaging instruments and to further flesh out the data. For
instance, the SFT has started advanced observations in the
H-alpha line to acquire full-disk, high-resolution images. It
can obtain Doppler velocity information based on imaging
at multiple wavelengths around H-alpha with high temporal
resolution, allowing it to more completely capture active
phenomena, and a broad dynamic range through a combinationof multiple exposure times. This advancement has enabled us
to observe many phenomena in recent heightened solar activity,
such as flares and prominence eruptions. The observatory alsouses the SFT to conduct regular imaging observations in the
G-band (430 nm) and continuum wavelengths. The regularobservational data described above, including real-time images,
are available on the website of the observatory. Using a Grantin-Aid for Scientific Research, a spectrograph system witha coelostat is under development to perform long-term, fulldisk observations, including more quantitative velocity andmagnetic field observations. An improvement to the coelostat
was conducted this year. The observatory maintains otherexisting equipment to allow for everyday observation, as well as
experimental use.

Data publicized via the website were previously stored on aserver owned by the observatory. The information has since beentransferred 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 the data 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.
The solar optical observations carried out at Hiraiso Solar
Observatory of the National Institute of Information andCommunications Technology are considered to be terminated.
To examine the possibility of utilizing the instruments in the
future at other institutes, discussions and on-site inspections
have been conducted.
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 toopen use and future plans are also discussed. The conference washeld at Nagoya University between February 16 and 18, 2015.
Because the observatory deals with fundamental solardata, there are often requests to use images from the Solar
Observatory database in school textbooks, to contribute to articles
in newspapers or magazines, and to help public events held bymuseums. The observatory actively responded to these requests.
Regarding personnel transfers, research expert Naomasa
Kitagawa replaced a staff member who departed last year. Dr
K. Kuzanyan of IZMIR, Russia, started his ten month stay as a
JSPS fellow in September 2014.

2. Opening of Data Archives to Public
The Solar Observatory has made nearly 16.2 TB of data
available to the public online, including data from the current
observations of white light, H-alpha, and magnetic fields aswell as those from nearly 100 years of various types of solar
observations. The various phenomena occurring in the solarterrestrial environment must be studied in terms of both sudden,
short-term events (space weather) and in terms of 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-alphaimages recorded on film, photographic plates, and hand-drawn
sketches, all of which have an importance of their own. The
observatory will make these also available to the public because
they are digitized and organized. As some of the world’s oldest
records of solar activities, these materials are expected to add
particular insight into future research.

II Status Reports of Research Activities085

7. NAOJ Chile Observatory
The ALMA Project is a global partnership of East Asia (ledby Japan), Europe, and North America (led by the United States)
to construct and operate a gigantic millimeter/submillimeterradio telescope deploying 66 high-precision parabolic antennas
in the 5000 m altitude Atacama highlands in northern Chile.
ALMA is projected to achieve a spatial resolution nearly tentimes higher than that of the Subaru Telescope or the Hubble
Space Telescope. Early scientific observations with ALMA
began in FY 2011 with a partial number of antennas and fulloperation commenced in FY 2012. This report describes the
progress of the project, which includes results of the open-use
scientific observations and public outreach activities. The ASTE
telescope is a single-dish 10-m submillimeter telescope locatedin the Atacama highlands. It has been operated to make headway
into submillimeter observations toward the ALMA Era. The
report also describes the progress regarding the ASTE telescope.

1. ALMA Project Progress
Along with the scientific observations, commissioning
observations of ALMA have been underway. These include
long-baseline observation tests, polarimetric observation tests,
and solar observation tests.
In particular, intensive long-baseline observation tests
were made from September through November 2014 withan extended antenna configuration of up to 15 km for theverification of equipment performance, new observation
methods, and efficient calibration methods. As a result of thesetest observations, astronomers successfully made the firstdetailed image of a protoplanetary disk around the young star
HL Tau at an extraordinary high resolution of 0.035 arcsec(equivalent to 40000/20 vision). The high sensitivity andresolution of ALMA made it possible to reveal several gaps
which are seemingly produced by the gravitational influence ofplanets forming in the disk. This is a remarkable result which
could reshape our understanding of planetary formation theory.
Another outstanding result with ALMA was an unprecedentedly
sharp image of an asteroid Juno and a lensed galaxy SPD.81,
which demonstrated the high potential of ALMA. The data forthese results have already been made available on the ALMA
Archive, and many papers based on them have been written
by astronomers. Following the success of these long-baseline
test observations, the maximum baseline will be extended up
to 10 km in the ALMA Cycle 3 Call for Proposals for scientificobservations that will be scheduled from October 2015.

2. ALMA Open-Use and Scientific Observations
The third round of open-use observations of ALMA
commenced in June 2014 with Cycle 2. The details of Cycle
2 include interferometric observations using thirty-four 12-m
parabolic antennas, Atacama Compact Array (ACA) observations(interferometric observation with nine 7-m antennas and single-

086

II Status Reports of Research Activities

dish observations with two 12-m antennas), six frequency bands(Bands 4 and 8 are added to Bands 3, 6, 7, and 9), a maximum
baseline of 1.5 km (for Bands 3 to 7) or 1 km (for Bands 8 and 9),
and a maximum of 150 fields of view for mosaic observations
and polarimetric observations.
An open call for the fourth round of open-use observations
was issued for Cycle 3. The details of Cycle 3 as advertised
include interferometric observations using thirty-six 12-m
antennas, ACA observations (interferometric observation withten 7-m antennas and single-dish observations with two 12-m
antennas), seven frequency bands (Band 10 is newly added toBands 3, 4, 6, 7, 8, and 9), a maximum baseline of 10 km (forBands 3 to 6), 5 km (for Band 7), or 2 km (for Bands 8 to 10)
and a maximum of 150 fields of view for mosaic observations
and polarimetric observations. The deadline of the public calls
for proposals for Cycle 3 is set at 00:00 JST on April 24, 2015.
Cycle 3 is scheduled to commence in October 2015.
Open use of ALMA has produced a number of scientificachievements. This section describes some of these focusing
mainly on East Asian projects. A research group led by Bunyo
Hatsukade at NAOJ observed galaxies hosting gamma ray bursts(GRBs), the brightest explosive phenomenon in the Universe,using ALMA and successfully detected radio emissions frommolecular gas for the first time. Also, this observation revealed
the spatial distribution of molecular gas and dust, showingthat gamma ray bursts occurred in a remarkably dust-richenvironment. A research team led by Kazuki Tokuda at Osaka
Prefecture University conducted ALMA observations of thegas cloud MC27 in the constellation Taurus and found twostarless high-density gas cores and an arc-shaped high-density
gas region, which is assumed to be formed by the dynamic
gravitational interaction of multiple gas cores that are very close
to the initial stage of star formation. A research group led by
Junko Ueda at NAOJ observed 37 galaxies that are in their final
stages of merger using ALMA and several other radio telescopes.
The group found that, among the 30 colliding galaxies fromwhich molecular radio emission have been detected, 24 galaxies
have rotating molecular gas disks and half of them haveextended gas disks that are larger than the stellar bulges at thegalactic centers. This is the first observational evidence showingthat mergers of two or more galaxies will lead to the formationof a new galaxy with a gas disk structure at a high rate. A
research team led by Shigehisa Takakuwa at the Academia
Sinica, Institute of Astronomy and Astrophysics, (ASIAA),
Taiwan, observed the baby binary stars L1551NE and founda gas disk surrounding both stars (known as a circumbinarydisk) with spiral arms of molecular gas extending from thedisk toward the binary stars. This is the first image that shows
the twin stars shaking the surrounding circumbinary disk andinducing the gas motion falling onto the twin stars. A researchteam led by Shuro Takano at NAOJ observed the central part ofthe spiral galaxy M77 and discovered that organic molecules areconcentrated in a region surrounding a supermassive black hole

at its center. This result shows that the black hole is surrounded
by a large amount of dust and gas which is shielded from X-rays
and UV photons. These findings will be a key to understanding
the mysterious environment around supermassive black holes.
A research group led by Aya Higuchi at Ibaraki University
conducted observations of the massive-star forming region
IRAS 16547-4247 and revealed the presence of multiple, at least
two, gas outflows from a protostar at the center. Also the radio
observation results of molecular line emissions of methanol
revealed in vivid detail an hourglass structure created by gas
outflows spreading outward.

This work was exhibited in an exhibition titled “THE FABMIND: Hints of the Future in a Shifting World” from October
2014 through February 2015 at the 21_21 DESIGN SIGHT in
Roppongi, Tokyo, which provided a good opportunity for many
people who are familiar with design and art to know more about
ALMA and its scientific achievements.

5. International Collaboration (committees, etc.)

The NAOJ Chile Observatory held a graduate school
guidance session on June 14, 2014. Eight undergraduate students
attended the session, engaging in lectures given by teachers andtalks with current graduate students.

The ALMA project has various committees, which holdmeetings frequently for international collaboration. The ALMA
Board has met twice, and the ALMA Scientific Advisory
Committee (ASAC) was summoned three times in FY 2014.
In addition to these, teleconferences have been held on a nearmonthly basis by these committees and the East-Asia ALMA
Science Advisory Committee (EASAC). Each working groupholds meetings and teleconferences more frequently to maintainclose communication in implementing the international project.

4. Public Outreach Activities

6. Workshops and Town Meetings

In April 2014, the NAOJ Chile Observatory hosted a weeklong ALMA booth at the Japanese Geoscience Union Meetingin Yokohama. The NAOJ Chile Observatory organized public
lecturers and Science Cafe events on 19 occasions in FY 2014 toprovide updated information and increase interest in ALMA andits scientific achievements through conversations with a large
number of visitors.
The NAOJ ALMA project website published 44 news
articles and seven press releases. A mailing-list-based newsletterhas been issued on a monthly basis with approximately 2,500
subscribers. Updated, detailed information is available on
Twitter (@ALMA_Japan), with nearly 22,000 followers as ofthe end of FY 2014.
Approximately 50 newspaper/journal articles wereposted, reporting scientific discoveries from the Early Scienceobservations and test observations. ALMA was featured in threetelevision programs. In addition to news reports on ALMA’s
observational achievements, there was a program showing
people involved in the ALMA project in depth such as “Fathers
Working in the World 6”, which effectively increased interests in
ALMA and appealed to a mass audience.
As part of the construction film project continuing since
FY 2013, the NAOJ Chile Observatory produced a new film
showing the development of the receivers at the Advanced
Technology Center (ATC) in FY 2014, and filmed interviews
with developers of the ACA correlators.
The NAOJ newsletter featured ALMA in the February 2015
issue with an article summarizing the ALMA project and its
scientific achievements, including interviews with ALMA staff
members stationed in Chile. The series “Bienvenido a ALMA”
in which ALMA staff members introduce their work, continues
to be featured in the NAOJ newsletter, which is also made public
on the ALMA website.
ALMA MUSIC BOX was created by translating the ALMA
radio data into music with the support of designers and artists.

• June 17 to 18, 2014 NAOJ Mitaka
ASTE/ALMA Development Workshop• July 14 to 17, 2014 Jeju, Korea
EA ALMA Science Workshop• October 27 to 29, 2014 NAOJ Mitaka
ALMA/ASTE/Mopra Users Meeting• December 8 to 11, 2014 Tokyo International Forum
International Workshop “Revolution in Astronomy with ALMA
- the 3rd year -”• December 13 to 14, 2014 NAOJ Mitaka
ALMA Postdoc Symposium• March 5, 2015 Ehime University
ALMA Cycle 3 Town Meeting• March 25, 2015 Kogakuin University
ALMA Cycle 3 Town Meeting• March 26, 2015 Japan Aerospace Exploration Agency (JAXA)
Institute of Space and Astronautical Science
ALMA Cycle 3 Town Meeting• April 2, 2015 Kagoshima University
ALMA Cycle 3 Town Meeting• April 8, 2015 NAOJ Mitaka
ALMA Cycle 3 Town Meeting

3. Educational Activities and Internship

7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research including
Industry – University Collaboration Expenses
None

8. Research Staff Changes(1) Hired• Patricio Sanhueza: project research staff(2) Departed or transferred

II Status Reports of Research Activities087

• Hiroshi Nagai: project assistant professor, transferred to the
NAOJ Chile Observatory to assume the position of a project
associate professor.
• Shinya Komugi: project associate professor, departed to
Kogakuin Univeristy to assume the position of an associate
professor.
• Hiroko Shinnaga: project associate professor, departed to
Kagoshima University to assume the position of an associate
professor.
• Chibueze, James: project assistant professor, departed to
University Nigeria to assume the position of a lecturer.

9. Main Visitors• August 5, 2014
Dr. Kyosuke Nagata, President of University of Tsukuba,
visited the Santiago Central Office of the Joint ALMA Office(JAO) and had a meeting with the ALMA Director Pierre Cox.
• November 6, 2014
Dr. Hiroyuki Takeda, Vice Dean of the School of Science at the
University of Tokyo, and others visited the ALMA Operations
Support Facility (OSF) and the Array Operations Site (AOS).
• November 26, 2014
Dr. Kaoru Yamanouchi, Vice Dean of the School of Scienceat the University of Tokyo, and others visited the ALMA
Operations Support Facility (OSF) and the Array Operations
Site (AOS).

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 andobservation methods for submillimeter astronomy. With ALMA
entering its operation phase, ASTE will be engaged mainly
to provide observational evidence for strengthening ALMA
observation proposals and to pursue developments for theenhancement of ALMA’s future performance.
Two public calls were made in FY 2014 for open-use
observation proposals for spectroscopic observations in the 345
GHz band: the first call (2014a) was from June to September
and the second call (2014b) from October to December. To
render support for researchers contributing to the observational
performance enhancement of ASTE, the Guaranteed Time
Observation (GTO) scheme has been offered since FY 2013,
which allows them exclusively to make proposals for GTO slots.
A total of 59 proposals for open-use observations and GTO
slots had been made including 28 for open use and five for GTO
during the first call, and 25 for open use and one for GTO during
the second call. These proposals were reviewed by the programsubcommittee at the NAOJ Chile Observatory and 38 proposals
were subsequently adopted including 20 for open use and fivefor GTO during the first call, and 12 for open use and one
for GTO during the second call. Open-use observations wereconducted from the ASTE Mitaka operation room between June
16 and December 19, 2014.

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In June 2014, the ASTE/ALMA Development Workshop
was held at NAOJ Mitaka Campus to discuss future instruments
to improve the observational capability of ASTE and future
development for ALMA performance enhancements. In response
to a call for proposals for future ASTE instruments made in
November 2014, three development proposals were submitted,
and subsequently adopted as candidate future instrument
development programs for ASTE by the reviewers selected fromthe Japanese ASAC members.

8. Center for Computational Astrophysics
1. Overview
The Center for Computational Astrophysics (CfCA) has been
operating a system of open-use computers for simulations centeredaround a general-purpose supercomputer and the special-purpose
computers for gravitational many-body problems; carryingout research and development of computational astrophysics;
and performing astronomical research with simulations. The
main supercomputer of the present system, ATERUI (Cray
XC30), was reinforced this year. Now ATERUI has a theoreticalpeak performance of 1 Pflops, making it the world’s fastest
supercomputer for astronomy. The center also continued
operation of other computers such as GRAPE-7, GRAPE-DR,
and GRAPE-9 which are dedicated to gravitational many-bodyproblems, in addition to general-purpose servers. Efforts invisualizing astronomical data also continue.

2. Open use(1) Computer Systems
This year marked the second year of the upgradedastronomical simulation system, which includes the mainsupercomputers of the open-use computers for this project.
The CPUs of the main super computer, Cray XC30, which isinstalled and operating at Mizusawa VLBI Observatory, haveall been updated, 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 from Cray Japan Inc., the center has
built the following equipment to aid the open-use operations:a series of dedicated computers for gravitational N-bodyproblems, known as GRAPEs; PC clusters for small to mediumscale 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 conducted byresearchers in Japan and overseas. In particular, the GRAPE
system is promoted for its effective open use. The center
undertook development, improvement, and maintenance for boththe hardware and software of the system this year. One of the
major events of this year was the test operation of GRAPE-9.
This system has a performance improvement of roughly 10-foldover the current GRAPE-7.
Computational resources are allocated to the XC30,
GRAPEs, and minor computational PC clusters in accordancewith a formal evaluation process. Their usage and application/
results for this year are listed below. The CfCA conducteda survey this year on the number of peer-reviewed papers
published in English in FY 2013 on studies that involved the
project’s open-use computers. It was revealed that 79 papers
were published in total in that fiscal year.
Drupal, a content management system introduced for dataexchange with users of open-use computers, is presently used

for providing information and transmitting various application
forms as necessary. The periodical CfCA News is an additional
channel of information dissemination. The center leverages
this newsletter to inform people of all useful and necessary
information regarding the computer system. A subsidy systemfor publishing and advertising is continuing this year for
research papers in which the results were obtained by using thecenter’s computers.
One paper was accepted in FY 2013 for payout in FY 2014,
while four papers were accepted in FY 2014 for payout in thesame year at approximately 400,000 JPY.
□ Statistics on the Cray XC30
Operating hours- Annual operating hours: 8088.6- Annual core operating ratio: 88.37 %Users- Category S: 1 adopted in the first term, 0 in the second term;
total 1- Category A: 14 adopted at the beginning of the year, 1 in thesecond term; total 15- Category B: 56 adopted at the beginning of the year, 9 in thesecond term; total 65- Category MD: 13 adopted at the beginning of the year, 3 in thesecond term; total 16- Category Trial: 44, annual total- Category I: 0, annual total□ Statistics on the GRAPE system
Users- Category A: 4 adopted at the beginning of the year, 0 in thesecond term; total 4- Category B: 6 adopted at the beginning of the year, 3 in thesecond term; total 9- Category Trial: 1, annual total□ Statistics on PC cluster
Operating hours- Annual operating hours: 8690.0- Annual job operating ratio: 71.7 %Total number of users: 39, annual 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, ausers’ meeting was held to serve as a forum for direct informationexchange. Many participated in the meeting, and discussions
were fruitful.
□ Cray XC30 workshop for beginning users: August 20, 2014, 6
attendees

II Status Reports of Research Activities089□ Cray XC30 workshop for intermediate users: January 19,
2015, 14 attendeesof simulations and the videos for press releases were publishedthrough this channel.

□ IDL visualization workshop: August 21, 2014, 11 attendees

4. 4D2U Project□ AVS visualization workshop: August 22, 2014, 11 attendees

In FY 2014, the 4D2U project added a new member forcontent development. A movie based on simulations titled“Formation and Evolution of Dark Matter Halos (II. Formationof the Large-Scale Structure of the Universe)” was released on
the 4D2U website in March 2015. This content was distributedwith 360 degree panoramic video for the first time. Viewing thisformat with a head mounted display (HMD) provides a realistic
experience. The updated versions of the four-dimensional
digital universe viewer, “Mitaka,” were released in December
2014 (ver.1.2.2), February 2015 (ver.1.2.2a, ver1.2.2b and beta
version for Oculus Rift) and March 2015 (ver.1.2.3). Theseversions of Mitaka included new functions, such as displaying
the 3D surface of the Moon and plotting the positions of objects
observed by the VERA project. In particular, the beta version forOculus Rift and version 1.2.3 which can project with the Dome
Master format expanded the usage of Mitaka. The imaging speedof Mitaka was made faster and faster every update.
The 4D2U project supported and provided contents for
exhibitions held in museums and galleries. For example,“mission[SPACExART]―beyond cosmologies” (Museum ofContemporary Art Tokyo, June 7 to August 31, 2014), “Mysteryof the Moon” (Konica Minolta Plaza, July 15 to August 10,2014) and “Depictions of Space” (Tokyo Dome City Space
Museum TeNQ, February 28 to June 28, 2015). In addition,
4D2U demonstrations using the dispatch system were conducted
at events held by the Hiroshima Astrophysical Science Center(July 20, and August 22 – 24, 2014). Local visitors enjoyedspecial programs to experience the latest astronomy findings
through 3D vision. Moreover, 4D2U contents were provided
for TV programs, planetarium programs, lecture presentations,books and so on.
In cooperation with the Public Relations Center, the 4D2U
project installed a new projection system for the 4D2U Dome
Theater. On March 17, 2015 the renewal of the 4D2U Dome
Theater was announced on the NAOJ website. The newest
movie content “Formation and Evolution of Dark Matter Halos(II. Formation of the Large-Scale Structure of the Universe)”
was produced and released for this renewal. Mitaka ver.1.2.2
was developed and installed on the new dome system.
A Twitter account @4d2u has been operated to provide
information about 4D2U. In addition, a Youtube channel for
4D2U was created as part of the PR activities, and movie
contents of 4D2U can be watched on this channel.

□ N-body simulation Winter School: January 26–28, 2015, 16
attendees□ Users meeting: January 20-21, 2015, 56 attendees

3. PR Activities
CfCA took part in the special open house of Mizusawa
Campus, Iwate Galaxy Festival 2014, held on August 30, 2014.
About 600 visitors attended the ATERUI guided tours andexperienced a close-up view of the facility. These occasions
were featured on local television programs and in newspapers.
At the Mitaka Open House held in October 2014, CfCA madethe 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 theopen house, CfCA has accepted five groups of high school
students and companies for tours of the computer room in
Mitaka Campus.
In FY 2014, three press releases were issued from CfCA;“The K computer simulation indicates that the neutrinoheating mechanism causes supernova explosions” (April
18, 2014, Tomoya Takiwaki, Assistant Professor at CfCA),“Supercomputer for Astronomy “ATERUI” Upgraded to Double
its Speed” (November 13, 2014), and “The K computer figuresout the mechanism of electron acceleration” (February 27, 2015,
Tsunehiko Kato, Research Expert at CfCA). In addition, thepress release from the NAOJ Chile Observatory, “Astronomers
Identify Gas Spirals as a Nursery of Twin Stars through ALMA
Observation” (December 4, 2014), included the results ofcalculations by ATERUI (Professor Tomoaki Matsumoto, Hosei
University).
Moreover, the results obtained by ATERUI were presented
with short articles on the CfCA website. “The Astronomical
Herald” published by the Astronomical Society of Japan featured
CfCA in Vol.108 No.2 and No.3 in 2015. The introduction of
CfCA by Prof. Eiichiro Kokubo and six articles about simulation
studies by the CfCA computers appeared in these volumes.
CfCA assisted GOTO Inc. in making the planetarium program“Space Analyzer”. This program features supercomputers used
for astronomical research, and presents results obtained by
ATERUI, GRAPE and K computer. This program was screenedat the Kobe Science Museum from September 2014 to March2015.
A Twitter account @CfCA_NAOJ has been operated toprovide information about CfCA. In addition, the Youtube CfCA
channel was created as part of the PR activities, and the movies

090

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5. External Activities(1) Joint Institute for Computational Fundamental Science
The Joint Institute for Computational Fundamental Science(JICFuS) is an inter-organizational institute established in
February 2009 as the basis for collaboration 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 JICFuS. In particular,
the institute engages primarily in computer-aided theoreticalresearch into the fundamental physics in elementary particle
physics, nuclear physics, and astrophysics. The scientific goalof the institute is to promote fundamental research based oncomputational science by encouraging interdisciplinary research
between elementary particle physics, and astrophysics. In
addition to its ability as a single organization, a major feature of
the institute is the cooperation of its three member organizations
and their communities to provide considerate and rigorous
support to present and future researchers. Another importantmission of the institute is to provide researchers around Japan
with advice regarding efficient supercomputer use and thehigh-performance computing development of novel algorithms
to meet research goals from the perspective of computer
specialists. In addition to ‘HPCI Strategic Program Field 5 “theorigin of matter and the Universe” ’, JICFuS has been adopted
for ‘Research and Development, Application Development ofscientific/social issues that require particular attention by the useof POST K-computer’ in FY 2014.
In order to implement research plans, Hiroyuki Takahashi
and Tomoya Takiwaki (until July) were engaged as project
assistant professors, and Tomomhisa Kawashima (from May)was engaged as a project researcher in FY 2014. Takahashi and
Kawashima developed a new plasma simulation code to solve
basic equations of relativistic radiation magnetohydrodynamics(MHD) based on first principles. By performing global
simulations of black hole accretion disks, they revealed that theblack holes are able to grow up rapidly via mass accretion. Thisis closely related to an unresolved issue in astrophysics: howstellar mass black holes grow into supermassive black holes.
Takiwaki carried out three-dimensional simulations of corecollapse supernovae using the supercomputer “K.” His researchis key for various studies within the framework of JICFuS,
because supernovae are closely related to elementary particle
and nuclear physics. Although the mechanism of supernova
explosions is a long-standing enigma that has been debated formore than 60 years, the research into supernovae has progressedconsiderably through numerical simulations with the most
realistic parameters using the K computer.
Representing CfCA, Professor Kohji Tomisaka and AssistantProfessors Ken Ohsuga and Tsuyoshi Inoue of NAOJ participate
in bimonthly JICFuS steering committee meetings to engage
in deliberations on how to spur computational science-based
developments in astrophysics research through discussions
with other committee members who specialize in nuclear andelementary particle physics.

computer. Although the center is involved with the JICFuS-led
HPCI Strategic Program Field 5 as mentioned in (1), its activity
in the HPCI consortium is fundamentally independent. The
HPCI consortium is an incorporated association established in
April 2012, and the center is currently an associate member able
to express views, obtain information, and observe overall trends
in the planning: however, it is devoid of voting rights as wellas the obligation to pay membership fees. Continuing from lastyear, a number of conferences and WGs have been held in which
participants discuss a next-generation national supercomputing
framework to follow the K computer.
This year the budget allocation was officially approved forthe development of a next-generation system, called “post-K”,
by the Ministry of Education, Culture, Sports, Science,
and Technology (MEXT). The institutes and groups for its
development have been established. Now detailed discussions
as to how we develop and use the post-K system have begun inrelated communities.
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 HPC
through participation in this discourse.

6. Contract Staff Transfers
The following staff members were employed on a contract
basis in this FY:(Research experts) Hirotaka Nakayama, Tsunehiko Kato
(Postdoctoral fellows) Shun Furusawa, Tomohisa Kawashima(Research associates) Yukihiko Hasegawa, Yuji Matsumoto
The following contract staff members departed in this FY:(Research expert) Tomoya Takiwaki (assistant professor)(Postdoctoral fellow) Naoki Ishitsu(Research associates) n/a(2) HPCI Consortium
As a participant in the government-led High-Performance
Computing Infrastructure (HPCI) project since its planning stage
in FY 2010, the center has engaged in the promotion of the HPC
research field in Japan, centering on the use of the national K

II Status Reports of Research Activities091

9. Hinode Science Center
The scientific satellite Hinode is an artificial satellite thatwas 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 has implemented
this satellite project under a joint research agreement with ISAS/
JAXA. A major theme of the scientific goals of the Hinodemission is to elucidate the coronal heating mechanism througha more multifaceted understanding of magnetohydrodynamic(MHD) phenomena occurring in the solar atmosphere. The
satellite actually made many 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 tocorona. The onboard telescopes were developed as part of awide-ranging international collaboration with assistance from
ISAS/JAXA. The 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 regards to 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 result of an even broader
international cooperation. The structure and electrical systemwere developed by the UK Science and Technology Facilities
Council (STFC) and University College London; the optics
system was developed by NASA and the Naval ResearchLaboratory (NRL); and the University of Oslo in Norway
assisted with the terrestrial testing equipment and the Quick
Look system. NAOJ actively participated in the development of
the EIS/satellite interface, satellite integration testing, and launch
experiments. After a successful launch, NAOJ has continued
its active involvement by acting as the main institution forcollecting 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, including three from the Hinode Science
Center (HSC): Sakurai (Chairman/project scientist), Suematsu(SOT), and Watanabe (EIS). Science Schedule Coordinators
have been 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 2014 marks the eighth year since the satellite’s launch.
Extremely good evaluations were received from the seniorreview class evaluation committees held at the respective
space agencies during FY 2012–2013. These accolades madeit possible for the satellite to continue operation for the next
few years at its current operational level. The operation of092

II Status Reports of Research Activities

the Focused Mode was conducted in the June and January –February periods of FY 2014 after a test run in January 2014.

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
arcsecond 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 performance level. Operational modifications haveenabled the maintenance of a sound field of view even in the
narrow band filter imager system, in which image degradation
was detected initially in part of the field of view.
The XRT has the capacity of imaging the solar coronalplasma via soft X-rays. The telescope has inherited thegrazing 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 abroader temperature range. Resolution is close to 1 arcsecond.
Calibration is now possible for temporal variations in spectral
characteristics due to surface contamination on the detector,
and the telescope is available for analysis via its spectral
characteristics.
The EIS obtains temperatures, densities, and velocities
for the chromosphere, transition region, and coronal plasma
thorough 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 observations from the chromosphere and the transition
region, located between the photosphere and the corona, to thecorona itself.
A mission data processor (MDP) was installed to manage
observations and to acquire data via the three telescopes.
Coordinated observations using the three telescopes are vital toachieve the scientific goals of the Hinode satellite, in which the
MDP plays a crucial oversight role. 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 are primarily downlinked at
the Kagoshima station (USC) and at Norway’s Svalsat station
through collaboration with ESA, allowing for data acquisition
during every orbit. Scientific operation was again performed
in FY 2014 via S-band data reception. The S-band reception
frequency was increased with help from ESA and NASA,
allowing for continuation 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 211 days in FY 2014, 68 days of which were for contracted
work. Moreover, the contribution rates to the scientificoperation of HSC were 24.9 % (domestic) and 15.7 % (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 observation together with othersatellites and terrestrial observational equipment, promotejoint observations among solar researchers worldwide. As of
March 2015, a total of 284 applications have been accepted.
In particular, core HOP proposals made by members of thescientific instrument team have became refined over multiple
implementations, and systematic observations have yielded
extensive results that can be expanded to studies on solar activity
cycles.

2. Hinode Satellite Data Analysisof Science (JSPS) fellow. The project assistant professor(Ishikawa, R.) was hired as an NAOJ assistant professor in June.
Hinode Science Meetings for Japanese and international solar
researchers are held on a regular basis to promote heliophysicalresearch using the Hinode scientific satellite. The eighth meeting
was combined with the “2014 Living With a Star (LWS) science
meeting,” and took place between November 2 and 6, 2014, inthe city of Portland, Oregon (USA). The NASA Marshall Space
Flight Center (MSFC) was a co-organizer.
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
Uitenbork, Han
Kuhn, Jeffrey

Organization (Country)
National Solar Observatory (USA)
University of Hawaii (USA)

Table 1. Long-Term Visitors.

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 purpose is to promote rigorous collaborative research
between researchers in Japan and abroad by maximizing thescientific outputs gained from the Hinode satellite by providing asuitable environment for analyzing the satellite data, facilitating
access to Hinode observational data by distributing the analyzed
data, and constructing a data 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 2014, HSC staff members and students published
14 peer-reviewed papers related to Hinode, bringing the total
to 241 papers by the end of March 2015. Cumulatively, a totalof 810 peer-reviewed papers have been published on Hinoderelated topics. Publication of papers in this category continues at
a pace of nearly 100 papers per year, even 8 1/2 years after thesatellite’s launch. Intensified collaborative research with newly
launched missions and advanced ground-based facilities near
the solar activity maximum will further enhance the number of
research papers for solar activity.

3. Other Activities
In FY 2014, three postdoctoral fellows were engaged as
members of HSC, including one project assistant professor, one
postdoctoral fellow, and one Japan Society for the Promotion

II Status Reports of Research Activities09310. Gravitational Wave Project Office
The activities of the Gravitational Wave Project Office(GWPO) are focused on the realization of the Large-scale
Cryogenic Gravitational-wave Telescope in the Kamioka mine
(KAGRA). KAGRA is a gravitational wave detector basedon a laser Michelson interferometer with arms 3 km in lengththat is currently under construction. The project is realizedin collaboration with ICRR and KEK in the framework of a
MoU about the development of gravitational wave astronomy.
According to the plan, the project construction should becompleted in 2017 and the first observation run should takeplace shortly afterwards. KAGRA should join the international
network of gravitational wave detectors in the USA and inEurope and contribute to the opening of gravitational wave
astronomy. In parallel the GWPO is preparing for KAGRA data
analysis and is conducting R&D for future upgrades to KAGRA
and for the development of DECIGO.

1. Development of KAGRA
In order to further clarify the role of NAOJ within KAGRA,a MoU with ICRR has been established in FY 2014. According
to the MoU the GWPO is responsible for the development of
the vibration isolation system (VIS), the auxiliary optics system(AOS), part of the mirror characterization equipment (MIR)
and the overall interferometer optical design. In FY 2014 JSPS
approved a Specially Promoted Research for the developmentof KAGRA. Part of the funding was allocated to NAOJ for
the development of VIS and AOS. In addition, the GWPO iscontributing to the project management, particularly for theactivities of the executive office, the system engineering office,the committee for publication control, the publication relationcommittee and the safety committee. The main achievement

at the site in FY 2014 has been the installation of the vacuum
system and the beginning of the installation of the interferometer.
In order to support on-site activity more efficiently, the GWPO
made preparations for a branch at Kamioka which just opened
on April 1st 2015.
(1) Vibration Isolation
The vibration isolation system (VIS) is composed of thesuspensions required to isolate all the interferometer components
from ground vibrations. Fifteen VIS’s are required for KAGRA.
Four different types of suspensions have been developed at
NAOJ for this purpose. During FY 2014 the VIS design has been
finalized and construction has been completed for most of thecomponents of initial KAGRA. Some of the development work
has been done in collaboration with the Advanced Technology
Center (ATC) of NAOJ. In particular, the bottom filters weredeveloped in close collaboration with ATC. We also acquired
the first ensemble of four inverted pendulums in collaboration
with Nikhef. The first prototype of one complete suspension
was assembled to be tested at TAMA. In parallel we started
installation of the vibration isolation systems for the input modecleaner at the Kamioka site.
(2) Auxiliary Optics System
The auxiliary optics subsystem consists of several kinds of
optics including optical baffles, beam dumps, beam reducing
telescopes, high quality viewports and the optical local
sensors (optical levers) for the mirrors of the interferometer.
The installation of 250 pieces of the arm-duct optical baffles,
which are designed to reduce noise due to stray light, hasbeen completed in both 3 km long arms of KAGRA. Opticalsimulations to estimate the stray-light noise with the designed

Figure 1: KAGRA construction progress: while the arm ducts are installed at Kamioka, the first full prototype of the vibration isolation system is tested in
one of the TAMA vacuum chamber at Mitaka.

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optical baffle system in the arm cavities were finished in the lastyear, and the performance was estimated to fulfill KAGRA’s
requirement. One of the large baffles (400 mm diameter) should
be installed in a cryostat (20 K), and the structure to support
such a baffle is being discussed. The beam reducing telescope
will sense the tilts of the main cryogenic mirrors in the 3-km
arms, making it indispensable for the long-term stability of theinterferometer operation. Its conceptual design was finished andsome of the required optics were delivered.
(3) Mirrors Development
Sapphire mirrors are the most important optics for KAGRA.
Therefore, tests to determine their quality are necessary. NAOJGWPO already made a scatter-meter for the mirrors. It canmeasure the total amount of scattering with a level of 1 ppm.
In FY 2014, an optical absorption measurement system wasintroduced in the TAMA experimental room. It has the potential
to measure absorption less than 1.5 ppm/cm for the sapphire
substrates. Now it is being fine-tuned to improve its stability.

2. Data analysis and theory(1) Data Analysis Preparation
Based on the approved Grant-in-Aid for Scientific Researchon Innovative Areas “New Developments in Astrophysics
through Multi-Messenger Observations of Gravitational Wave
Sources,” preparations for multi-messenger analysis are in
progress. To reduce the false alarm rate of the KAGRA detector,
a physical environmental monitoring system is necessary. Now
the system has been installed in the X-end room at the Kamiokasite. The recorded data were analyzed by the KAGRA detector
characterization sub-group. The noise veto information will beshared by GW search systems.
(2) Theoretical Research on General Relativity
General-relativistic higher-order perturbation theories
have very wide applications for cosmology, black holes, andgravitational waves. Therefore, a framework for generalrelativistic higher-order gauge-invariant perturbation theory
has been discussed from a general point of view. In 2014
it was shown that the general framework developed by Dr.
Kouji Nakamura is applicable to any-order perturbations on
an arbitrary background space-time. In addition Dr. Nakamura
together with Dr. Masaki Ando also proposed a precise
derivation of the resultant response of a rotating torsion barantenna when acted upon by gravitational waves.

3. R&D(1) R&D for Upgrades of KAGRA
In parallel with the development of KAGRA, the GWPO
continues to carry out an R&D program to prepare future
detector upgrades. We seek external funds to support thisprogram. In FY 2014 we completed a cryogenic infrastructure to
test optical components for KAGRA at cryogenic temperature.
In parallel we started a collaboration with the Institutefor Molecular Science to study the quantum behavior ofmacroscopic objects. For this purpose, a large vacuum chamber
was funded by NINS via an intra-institute funding program.
Finally we started R&D to study the capabilities of mirrors
based on crystalline coatings. The goal is to reduce the thermal
noise in precision measurements based on optical cavities such
as GW detectors. This project was funded by JSPS. In FY 2014
we also submitted to JSPS a larger scale project hoping torealize frequency dependent squeezed states of light using the
TAMA infrastructure.
(2) DECIGO/DPF
In FY 2014 the DECIGO Pathfinder (DPF) proposal,
submitted to JAXA for the next scientific mission, wasrejected. One of the main reasons was the lack of available
manpower since the gravitational-wave community in Japanis concentrating on the construction of KAGRA. However thescientific significance of DECIGO has been recognized by
JAXA. So we revised the roadmap to DECIGO.
As a “pathfinder,” we will do R&D on the ground anduse airplanes to make a free-fall environment to test each unit
developed for DECIGO. The revised R&D plan was submitted
to JSPS and was approved.
In NAOJ, an interferometric sensor is being developed. In
this fiscal year, we made a test bench with balancing masses(“yajirobee”) for simulating the test masses to achieve free-fallin some degrees of freedom on the ground. The controllability ofthe masses are shown experimentally.

4. Education
During FY 2014 one master’s student from SOKENDAI and
one undergraduate student each from Ochanomizu University
and from Tokyo University of Science did their research projects
in the GWPO. All of them obtained their degrees. In addition,
one PhD student from ICRR is continuing his research at NAOJ
to do his thesis on the KAGRA vibration isolation system. The
GWPO also hosted one PhD student from Niigata University
under the NAOJ research visitor program; an undergraduate
student from the USA under the International REU programin Gravitational-Wave physics funded by NSF; and two
undergraduate students under the SOKENDAI summer student
program. Within the SOKENDAI program we also hosted amaster’s student from the University of Pisa who then applied
and was accepted as a PhD student at the U-Tokyo. The GWPO
also contributed to teaching with regular classes given at the
Department of Astronomy of U-Tokyo and at Hosei University.
Punctual classes were given also at Ochanomizu University,
the SOKENDAI summer school and at the department ofEngineering of U-Tokyo.

5. Publications, presentations and workshops
organization
The office members were authors of 34 publications ininternational journals and of 11 presentations to international

II Status Reports of Research Activities095conferences. 30 presentations were also given to conferences inJapan.
During FY 2014 we organized the 6th Korea-Japanworkshop that took place at NAOJ on June 20th and 21st, 2014.
We also contributed to the organization of the Gravitational
Wave Advanced Detector Workshop in Takayama in May 2014.

6. Outreach
KAGRA had a tunnel completion ceremony in July.
Following this event, a TV program by NHK featured KAGRA
and the office contributed to it. We also had an interview byMainichi-shinbun about KAGRA yielding a newspaper article
in January. The office contributed to the NAOJ open days in
October by showing the TAMA facility and the ATC’s clean
room for assembling KAGRA components to the public. Visits
to the TAMA facility were also given to several groups of highschool students, college students, and people from privatecompanies.

7. Relationships with industry
We continue the collaboration with a Japanese company
aimed at improving the quality of low loss mirrors. In particular,
we fabricated an ultra-low loss rigid cavity using the opticalcontact method. The specification for the reflectance of themirrors is 99.999 % and the target loss factor is less than 5 ppm.
The cavity is now under inspection.

8. Personnel
At the beginning of FY 2014 the project included a total of
14 personnel, including one specially appointed professor, two
associate professors (one of which is affiliated with U-Tokyo),five assistant professors (of which one is assigned to ICRR),
three engineers, two administrative staffs (shared with the
Jasmine project) and one postdoc. During the year one postdoc,
one specially appointed researcher, one specially appointed
specialist and one research associate joined the team, so that at
the end of the year the GWPO had 18 staff members. In addition
one PhD student, one master’s student and two undergraduate
students did their research project in the GWPO. We also hosted
a research director from CNRS (France) who visited our officefor one-and-a-half months.

11. TMT-J Project Office
The TMT Project is a construction project to build anextremely large telescope with 30 meter aperture through thecollaboration of five partner countries comprised of Japan,
the United States of America, Canada, the People’s Republicof China and the Republic of India. The TMT-J (TMT Japan)
Project Office heads the project for NAOJ. In Fiscal Year2014, an agreement was executed establishing the key projectprinciples and work share assignment for TMT construction.
TMT International Observatory was founded for the purposeof construction and operation of TMT and the commencementof the construction of TMT was declared. For its part in theconstruction, Japan is fabricating the primary mirror segments,
designing the telescope structure, and designing/studying
science instruments.
At the end of Fiscal Year 2014, 3 Professors, 3 Associate
Professors, 1 Chief Research Engineer, 2 Specially Appointed
Senior Specialists, 1 Research Administrator Staff, 2 ResearchExperts, 1 Research Supporter, 1 Public Outreach Official,
1 Specially Appointed Research Staff Member, 1 Specially
Appointed Project Research Staff Member, and 2 Administrative
Supporters were in full-time positions for the Project Office. In
addition, 1 Professor, 4 Associate Professors, and 5 AssistantProfessors from the Advanced Technology Center, Subaru
Telescope and NAOJ Chile Observatory have concurrent
positions in the TMT-J Project Office and take part in activities

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that include the development of TMT science instruments at theAdvanced Technology Center.

1. Commencement of Construction by the TMT
Project
The TMT-J Project Office of NAOJ has participated inquarterly TMT Board meetings held since 2007 as well as in the
Science Advisory Committee and external review committee
meetings to give shape to the international collaboration. By
April 2014, this effort led to the execution of agreements by the
final authorities of each participating organization that set the
key principles and schedules for construction; work share andthe basis for observing time allocation; and the establishmentof the TMT International Observatory which would assume therole of constructing and operating TMT. In May of the same
year, TMT International Observatory (TIO) was incorporated
in the USA. At this point, the National Institute of Natural
Sciences (NINS), National Astronomical Observatories ofChinese Academy of Sciences, University of California andCalifornia Institute of Technology became official members of
the project by executing the project agreements. The Departmentof Science and Technology of India and National ResearchCouncil of Canada followed by becoming official members withthe approval of the project budget in December of the same yearfor India and April 2015 for Canada. Along with the 6 members,
the Association of Universities for Research in Astronomy
joined the project as an Associate Member representing the USA
in anticipation of later becoming a full-fledged member. Japan
also has a role in leading the international collaboration witha TMT Board Member representing Japan appointed as Vice
Chairperson of the TMT International Observatory Board ofGovernors.
In July of 2014, commencement of construction was
declared with the approval of a sublease from the Universityof Hawai`i to TMT International Observatory for the TMT
construction site on the summit of Maunakea and the completionof all paperwork and procedures to use the land for construction.
In October, a groundbreaking ceremony was held in Hawai`i andonsite construction commenced.
In Japan, the construction of TMT was approved as one of
the new projects for the Promotion of Large Scientific Research
Projects in Fiscal Year 2013 and fabrication of the primary
mirror segments and preliminary design of the telescope
structure was performed. In Fiscal Year 2014, in addition todomestic progress related to the fabrication of the primary
mirror, detailed designs of the telescope structure, and thedevelopment of science instruments (explained below), Japan

also initiated payments to TMT International Observatory tocover Japan’s share of operating expenses that include onsite
construction costs.

2. Japan’s Progress on Its Work Share – theTelescope Structure and Fabrication of thePrimary Mirror Segments
Japan is officially charged by the executed agreementswith responsibility for the design/manufacture of the telescope
structure, the primary mirror segments and sections of thescience instruments.
(1) Fabrication of the Primary Mirror Segments
The plan for the primary mirror calls for Japan to fabricate
all of the segment mirror blanks and to spherically grind theblanks as part of its work share. In 2014, 39 blanks were
fabricated, 18 of which were spherically grounded. Because
Japan is also in charge of polishing 30 % of the mirror segments,
we developed and demonstrated technology with the capacity
to mass produce aspherically polished segments. We also
performed aspherical grinding on 15 segment blanks.
(2) Design of the Telescope Structure and Its Control System
The plan for the telescope structure is to have the detailed
design of the telescope completed in 2 years starting from
Fiscal Year 2014, based on the preliminary design from Fiscal
Year 2013. The control system of the telescope structure
passed its preliminary design review in April 2014, followedby the primary mirror segment exchange mechanism (Segment
Handling System) in November, enabling both to continue on to
the detailed design phase. In addition, fabrication and evaluationof prototypes are underway for large structures that are difficult
to fabricate and require fabrication with extreme precision. In
February 2015, the first design review was held for the main
telescope structure.

Figure 1: Conceptual image of TMT once constructed.

(3) Science Instruments
Japan is responsible for fabricating a portion of the first-light
instruments as part of the international collaboration.
Japan is in charge of fabricating the imaging component
for the Infrared Imaging Spectrometer (IRIS). In fiscal year
2014, optical design of the imaging system that will enable theaddition of a highly demanded high-contrast optics system andwide-field capability in the imaging system was proposed to the
TMT Science Advisory Committee and approved.
For the Wide Field Optical Spectrometer (WFOS), Japan
continued its conceptual study from Fiscal Year 2013 inanticipation that it will be placed in charge of the camera system.
The availability of high quality large diameter glasses for thecamera system was confirmed through investigations.

3. Evaluation of Scientific Research with TMT
and Public Relations Activities
Figure 2: Execution of the TMT agreement by the President of NINS.

Continued effort is made to reflect the opinions of the

II Status Reports of Research Activities097

community through actions such as the TMT-J Science Advisory
Committee (TMT-J SAC). A tool for evaluating scienceobservation performance in the preparation of proposals forscientific research to be undertaken with TMT was proposed by
TMT-J SAC and is being developed by the TMT-J Project Office.
It has been made internationally available and has been usedby many researchers. 14 special feature articles on TMT witha brief overview of the project, current status of construction,and science feasibility studies were published in three special
issues of the Astronomical Herald of the Astronomical Societyof Japan.
While the Science Advisory Committee of the TMTInternational Observatory performed a central role in studying
the scientific research feasible with TMT, Japan played a majorrole in the TMT International Science Development Teams(ISDTs) established in 2013 with researchers from Japan
participating as conveners in five of the eight science categories.
The TMT Project, particularly the status of Japan’s work
share, is introduced on the TMT-J Project Office home page.
Preparations were made to update the English web page tomake information about the progress made on the project byJapan available overseas. TMT Newsletters volumes 40 to 43
were delivered. Public outreach was undertaken by performing

Figure 3: Detailed design of the telescope structure in development.

Figure 4: Aspherical grinding of a primary mirror segment.

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lectures all over Japan and through exhibits made available
through organizations such as the NINS Symposium and InterUniversity Research Institute Symposium. Continued efforts toraise donations for the TMT Project resulted in donations fromone corporation and 732 individuals in 2014 (between January
and December).
With the support of “Club TMT” formed in 2012 to support
the project, TMT was introduced in screenings and lectures atscience museums and planetarium all around Japan. About 50
lectures and classes on demand were held for the public.
Public relations/outreach and contributions to workforce
development and education were performed by Workforce
Pipeline, Education, Public Outreach and Communications(WEPOC), an international study team. In October 2014,
WEPOC opened an assembly in Tokyo where outreach activities
performed within Japan and at the Subaru Telescope in Hawai`i,
as well as Hawai`i instruction courses for high school students
that included visits to the Subaru Telescope were introduced.
Activities of the assembly also included visits to science
museums.

12. 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 and to
perform infrared (Kw-band: 1.5–2.5 μ) measurements of annual
parallaxes, proper motions, and celestial coordinates of the stars
at a high accuracy of 1/100,000 arcsecond (10 μas) in orderto 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 forannual parallaxes less than 10 %. This is necessary for accurate
distance determination. By using observational data to constructa phase space distribution of gravitational matter, astrometricsurveys of the bulge of the Milky Way promise to make major
scientific breakthroughs in our understanding of the structureof galactic bulges and the causes of their formation; the historyof star formation within bulges; and the co-evolution of bulges
and supermassive black holes, which is closely related to theaforementioned 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 2021. 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 2030s. 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 2014
1) Organization of the office
The JASMINE Project Office is composed of four fulltime staff members, six staff members with concurrent posts,
two postdoctoral fellows, one research associate, one technicalassociate, and four graduate students. Significant contributions
were made by members of the following organizations: the
NAOJ Gravitational Wave Project Office; 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 School of Engineering; Tokyo
University of Marine Science and Technology; the University ofTsukuba; 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 accumulatetechnical experience in onboard data acquisition and the likenecessary for the upcoming JASMINE project, achieve scientificresults in the study of dynamical structures in the vicinity of the
Solar System, and the analysis of star formation based on stellar
motions in star formation regions.
The satellite is 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 postponed due to delays inconstruction work at the Alcantara Space Center launch site in
Brazil. On the other hand, the construction of the rocket has
been completed, and work on interface adjustment between therocket and the satellite is in progress. Assembly of the flightmodel that will actually be launched into space was completed
in FY 2010. The extra time yielded by the launch delay has beenused for additional testing to further ensure project success.
Maintenance of the satellite has also been performed. The project
has continued to prepare terrestrial communication stations
related to satellite operation. Steady progress was also madein 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. The Gaia Project involves observational and analyticalmethods similar to those of Nano-JASMINE. A Japanese WG
led by Ryoichi Nishi of Niigata University continued to engage
actively in investigating the scientific results obtained in the
future by Nano-JASMINE.
3) Overview of Planning and Developing 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

II Status Reports of Research Activities099

(Hw band: 1.1–1.7 μm). A goal is to measure annual parallaxes
at a precision of 10–20 μas and proper motions, or transverse
angular velocities across the celestial sphere, at 10–50 μas/year in
the direction of an area of a few degrees from the Galactic center
within the bulge and in the directions of a number of specificastronomical objects of interest in order to create a catalogueof the positions and movements of stars within these regions.
The project is unique in that unlike the Gaia Project, the sameastronomical object can be observed frequently and observation
will be performed in the near-infrared band, in which the effectof absorption by dust is weak. This project will help to achieve
revolutionary breakthroughs in astronomy and basic physics,
including the formation history of the superrmassive black holeat the Galactic center; the gravitational field in the Galactic
nuclear bulge and the activity around the Galactic center; theorbital elements of X-ray binary stars and the identification of acompact object in a X-ray binary; the physics of fixed stars; starformation; planetary systems; and gravitational lensing. Suchdata will allow for the compilation of a more meaningful catalog
when combined with data from terrestrial observations of theline-of-sight velocities and chemical compositions of stars in thebulge. Conceptual planning and design of the Small-JASMINE
satellite system and detailed planning of the subsystems beganin November 2008 with cooperation from nearly 10 engineersfrom JAXA’s SE Office, 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 for the ISAS
call for small-sized scientific satellite mission proposals. The
name and submission requirements were altered in FY 2013;
it is now known as Epsilon onboard Space Science Missions.
The SWG, led by Masayuki Umemura of the University ofTsukuba and including volunteers from diverse fields in Japan,
continued to make scientific considerations. Other activities
such as conceptual planning, design, technical testing andinternational project collaboration have been continued. As
planning progressed, the full mission proposal was preparedand submitted in February 2014. Although Small-JASMINE
was not selected as a final candidate, it should be remarked thatthe evaluation committee gave Small-JASMINE high scores.
Furthermore the evaluation committee suggested a specificneeded improvement. To date, we have already promised that
Small-JASMINE can make this improvement. We have been
making a revised mission proposal in preparation for the next
ISAS call for proposals.
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)

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Galactic Evolution Experiment (APOGEE) Project, offered ajoint proposal for the APOGEE-2 project as an extension of
the original APOGEE project to engage in bulge observationsin the southern hemisphere because the project is suitable forbulge observations. The telescope employed will be equippedwith a high-dispersion spectroscope, an identical model to thatof APOGEE. The joint proposal has been submitted. An official
memorandum of understanding has been exchanged among
the APOGEE-2 team and members of the fourth Sloan Digital
Sky Survey (SDSS-IV) Collaboration and Small-JASMINE tostrengthen international partnerships and to achieve scientificgoals related to the Galactic bulge.

13. Extra-Solar Planet Detection Project Office (Exoplanet Project Office, EPO)
The Extra-Solar Planet Detection Project Office (EPO) will
manufacture/maintain large-scale instrumentation and develop
new technologies and observational methods for exoplanet
research. The goal is to make contributions as a center of
excellence in this field and promote observations of exoplanetsand studies of their formation. The EPO promotes not only
instrumentation, but also cutting-edge observational researchusing these state-of-the-art instruments in collaboration withdomestic and international researchers. The science themes are
not limited to exoplanets and their formation. They also include
brown dwarfs and star/planet formation. The main themes in thelast 5 years are:(1) The development/upgrade/maintenance/operation of the highcontrast imager HiCIAO and the promotion of the SEEDS
survey project.
(2) The development of the new IR Doppler instrument IRD andplanning its observations.
(3) The development of the high contrast instruments SEIT (for
TMT) and WACO (for WFIRST, formerly SPICA/SCI and
JTPF activities.)(4) The instrument development and maintenance for smaller
telescopes (Okayama/MuSCAT multi-channel optical camera,
IRSF/SIRIUS 3-band infrared camera and IRSF/SIRPOL
3-band infrared polarimeter).
In FY 2015, the project consisted of 5 main staff members,
3 joint appointment staff members, and 5 postdocs. There were
36 refereed papers in English, 4 non-refereed papers in English,
14 presentations in English, 1 refereed paper in Japanese, 2
non-refereed papers in Japanese, 5 books in Japanese, and 49
presentations in Japanese.

1. Development of the Subaru next Generation
Exoplanet Instruments and Exoplanet
Observational Researches

dwarfs. The budget is based on JSPS Grant-in-Aid forSpecially Promoted Research (PI: Motohide Tamura). The final
manufacturing of the main componets, fiber experiments, laser
frenqucy comb, and total asemble are being conducted. Science
discussions on habitable planets around M dwarfs are also
proceeding.

2. Exoplanet Instrument Developments for
Future Space and Ground-Based Telescopes
and International Collaborations(1) WACO (WFIRST-AFTA Coronagraph) and JTPF (Japanese
Terrestrial Planet Finder)
These missions aim to directly image and characterize Earthlike planets and super-Earths for signatures of life. As a memberof the WACO working group, coronagraph performance tests
at the JPL testbed are conducted with collaborators with otherJapanese collaborators.
(2) SEIT (Second Earth Imager for TMT)The aim of the SEIT instrument is direct imaging andcharacterization with the 30 m telescope TMT. Both technicaland science discussions are being conducted, including opticaldemonstration tests.

3. Science Research, Education, and Outreach
The SEEDS project was successfully completed in January
2015 without any major troubles. In this year, a planet (< 15Jupiter masses) is confirmed at r ~ 47 au around Herbig Aestar HD100546. The planet is not point-like but extended,probably suggesting the presence of circum-planetary structures.
Spiral structures are also detected in the protoplanetary disk.

(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 with the 8.2 m Subaru
Telescope, which can utilize various differential imaging
techniques to distinguish polarization, multi-band observations,and angles. The project started in 2004 and its performanceverification was completed in 2009. The main survey of first
Subaru Strategic Program SEEDS (Strategic Explorations of
Exoplanets and Disks with Subaru) with more than 100 people
continued from October 2009 until January 2015, without any
serious troubles.
(2) IRD (Infrared Doppler Instrument)
IRD is a high precision (~1 m/s) radial velocity spectrometerworking at near-infrared wavelengths. It’s aim is to detect
habitable Earth-like planets around M dwarfs and brown

Figure 1: A gallery of protoplanetary and debris disks detected by the
SEEDS project in near-infrared wavelengths.

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101

A statistical survey of ~250 SEEDS stars was made and thefrequency of stars having objects at 10–100 au around them with
masses between 5–70 Jupiter-masses is about 2 %. W. M. KeckObservatory and the Subaru Telescope were used in cooperation
for a survey of 120 M stars to search for giant planets.
The SEEDS also directly imaged many protoplanetary disks.
It detected scattered light for the first time, which revealed
asymmetric structures of the disk around a young star IRS48(a.k.a. WLY 2–48). A review paper was published on the direct
imaging of protoplanetary disks around Herbig Ae stars. Aninternational collaboration using Hubble Space Telescopeobservations detected about 10 debris disks.
Ten graduate students are supervised for exoplanets andrelated topics. Many public talks, publications, and press
releases are made on exoplanets, disks, and other astronomical
fields.

14. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project Office
1. Component Technology Development for
Future Lunar/Planetary Exploration Projects(1) Radio Source for VLBI Observation of Lunar/Planetary
Gravity Field:
In 2014, a new lunar gravity field model was publicizedbased on the recent observations by the GRAIL lunar explorer.
The tidal Love number derived from the new gravity model
has improved more than expected, and its accuracy exceeds
our scientific goal for SELENE-2 VLBI. Therefore, we wererequired to revise thoroughly our development plan.
i) Analysis of Electric Property and Thermal Tolerance of Macor
Antenna
Because financial support from the SELENE-2 mission
was terminated when the mission was halted by JAXA, wecancelled fabrication of the Breadboard Model (BBM) for theantenna board. Instead, in the context of future lunar/planetary
explorations and component technology development, weinvestigated the electrical properties of the Macor material thatcomprises the base substrate of the antenna. We measured thedielectric constant of the base substrate material in relation tochanging ambient temperature in a vacuum chamber simulating
the environment on the surface of the Moon (−200 °C to +120
°C). The test results have been accepted by a peer-reviewed
international journal.
ii) Studies of the Internal Structure of the Moon
Investigation for the elastic and viscous structure of the
deep interior of the Moon continued in FY 2014 by combining
the selenodetic and seismic data. The expected accuracy of
the internal structure based on the accuracy of selenodetic
observations was studied quantitatively and submitted to aninternational journal.
iii) Discussion for Providing Two Beams for the S and X Bandsin the 20-m VERA AntennaSame-beam S-band VLBI observation had been considered
for the primary method of differential VLBI observation
between the orbiter and the lander. The Vivaldi antenna was

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selected as the model to be adopted. An antenna element was
designed using electromagnetic analysis software, and its shape
was optimized. A computer simulation confirmed that theantenna is able to perform at the required performance level.
(2) Development Experiment for Lunar Laser Ranging (LLR)
The distance between the Moon and the Earth can be
accurately measured by transmitting a laser from a telescopeon Earth to laser retroreflectors that were placed on the lunar
surface by the US Apollo missions and Soviet lunar exploration
missions and observing the reflected photons, thereby allowing
for investigation of lunar rotational variations. Due to thelack of reflectors in the southern hemisphere and the timedifference between the two ends of reflector arrays generated bylibration, the level of precision has hitherto been insufficient for
determining small variations in the process of energy dissipationin the lunar interior.
Aiming to fabricate an LLR retroreflector to be mounted
on the lander, material selection and mirror-forming methods
were investigated. Preparatory technological development was
pursued in conjunction with a tri-party agreement with the
Chiba Institute of Technology and Tokyo University of Science,
aiming to utilize Ion Beam Figuring (IBF). Monocrystalline
silicon and glass ceramics to be used as the mirror material
were tested and their stability was verified in a simulated lunar
surface environment in a thermal vacuum chamber. Instead ofClearceram-EX, monocrystalline silicon was selected as the best
mirror material for thermal-structural and optical analyses.
(3) Development of In Situ Lunar Orientation Measurement(ILOM) Telescope
Research is underway to install an ILOM, which is like asmall Photographic Zenith Tube (PZT) telescope, on the lunar
surface and to perform high-precision observations of lunar
rotational variations to constrain the internal structure of theMoon. Because measurement can be conducted independent
from lunar orbital motion, this small telescope is capable ofdetecting miniscule variations in the rotation of the Moon,
allowing us to determine whether or not the lunar core is molten.
The mercury pool developed in FY 2013, which is less

susceptible to vibration, was installed in the Breadboard Model(BBM) of the telescope. The imaging performance of the BBM
was examined by using an artificial light source; we determined
the relationship between variations of the star-image center,ground vibrations, and the inclination of the telescope tube.
Also, the frame of the telescope for ground observation was
fabricated.
(4) Development of the Laser Altimeter (LIDAR) of Hayabusa 2i) ranging tests using a flight model, hardware tests using groundsupport equipment, and accuracy estimation for asteroid surface
albedo calculated through the intensity ratio of the transmitted
and received lasers.
ii) development of a quick-look software and verification during
the integration tests.

FY 2014. In accordance with this memorandum, joint research
into the basic development of a lunar lander/explorer (LLR andILOM) is conducted by the Faculty of Engineering at Iwate
University, with monthly meetings held alternately at Iwate
University and NAOJ Mizusawa Campus.
Joint research continues with a group from Kazan Federal
University, Russia, which is well respected in theoreticalinvestigation into the internal structure of the Moon, to establish
a new theory of lunar rotation, in line with ‘the Memorandumof Understanding for Cooperative Research between Kazan
Federal University and National Astronomical Observatory ofJapan on VLBI and Astrometrical Observations,’ which was
renewed in 2010. A two-day workshop on the internal structureof the Moon was held at Mitaka and Mizusawa Campuses using
a Grant-in-Aid for Bilateral Research from the Japan Society for
the Promotion of Science. Seventeen Russian scientists attended
at this workshop and visited the RISE office in Mizusawa.

iii) theoretical calculation of the size and density of circumasteroid dust for hardware development.
(5) Development of a Ganymede Laser Altimeter (GALA) for
the Jupiter Icy Moon Explorer (JUICE) Mission
GALA was officially selected by ESA as one of the JUICE
mission payloads following a proposal submission in FY 2012,
and the RISE Project Office officially commenced activities
as a main GALA-Japan team member. Japan will undertakethe development of a receiving telescope as a part of the laser
altimeter system.
i) detailed laser link calculations (performance model) to serveas the basis for the hardware design.
ii) deliberation on the specifications for the thermal–structural
analysis to be outsourced to a manufacturer.
iii) The RISE Project Office leads the gravity/rotational variation
subgroup within the Japanese part of the science team.

3. Educational Activities/PR
Six RISE members delivered lectures on a part-timebasis to graduate students at the University of Aizu for twosemesters; and two RISE members served as part-time lecturers
at Iwate University for a half year each. The office accepted
two undergraduate students from Iwate University through aninternship program, and one undergraduate student from Kobe
University in the summer student program of the Graduate
University for Advanced Studies (SOKENDAI).

4. Joint Research/International Collaborations‘The Memorandum on Basic Issues Concerning Researchand Development of Scientific Instruments for Lunar Landing
Exploration’ was renewed between members of the RISE Project
Office and the Faculty of Engineering at Iwate University in

II Status Reports of Research Activities10315. Solar-C Project Office
The SOLAR-C Project Office engaged in planning the next
solar observation satellite project, SOLAR-C, and implemented
the preparation of the flight components for the Chromospheric
Lyman-Alpha SpectroPolarimeter (CLASP) to be flown on asounding rocket experiment. In Fiscal Year (FY) 2014 the JAXASOLAR-C working group (WG) led by Prof. Watanabe submitted
the SOLAR-C proposal for the JAXA Strategic Middle-Class
Satellite Mission. The CLASP team has executed the assembly
and testing of the CLASP flight model in the ATC cleanroom forthe flight operation scheduled in the summer of 2015.

1. SOLAR-C Project
SOLAR-C is a planned project which may become Japan’s
fourth solar observation satellite, after Hinotori, Yohkoh, andHinode. The plan is to realize the launch in the early years of the2020s. The project is intended to investigate the solar magnetic
plasma activities that influence space weather and space climate
around the Earth. The investigations will be the first to involvethe chromospheric magnetic-field and achieve high-resolution
imaging/spectroscopic observations from space. The themes
include major problems in solar research: the heating of thechromospherice/corona, the origin of solar explosive events,and variation in the solar spectral irradiance. The tasks include
resolving the fundamental small-scale magnetic structuresderived directly or indirectly from the Hinode observations andvisualizing the activities and interactions of magnetic structures.
SOLAR-C will conduct high-resolution (0.1 – 0.3 arcsecs)
observations of radiance, polarization, and spectroscopy over
the outer atmosphere from the photosphere to the corona byusing onboard instruments. The instruments for SOLAR-C consistof SUVIT with a 1.4 m aperture for observing the photosphereand chromosphere; EUVST for spectroscopic observation fromthe chromosphere to the corona; and HCI for capturing imagesof the transition region and corona. 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 USA and European space
agencies and institutions will deal with other major instruments
through a large-scale international collaboration.
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,dedicated to the SOLAR-C project. It was promoted to become
the SOLAR-C Project Office in FY 2013 as an A-project
independent from the Hinode Science Center. It continues the
preparatory work for the satellite project with four full-time
staff members and 11 members with concurrent positions/
postdoctoral fellows.

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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
observation of the hydrogen Lyman-alpha spectrum. Planningand basic development of the project started in FY 2009. The
project involves an international research team with participationfrom Japan, the USA, and other countries. The CLASP project
entered the development stage fully in the latter half of FY
2012, and received a prospective development budget for theflight equipment during FY 2013. The payload consists of a
far-ultraviolet (FUV) telescope and a spectro-polarimeter to
conduct polarization observations which were prepared in Japan,
with components contributed by the USA (CCD cameras andcontrol computers) and France (a spherical concave grating).
The system then will be mounted on an American sounding
rocket for launch in the USA in summer 2015. The Japanese
PI is R. Kano, an assistant professor at the NAOJ, who leads
postdoctoral fellows and assistant professors to pursue design,
instrument development, and testing.

3. Major Activity in FY 2014
The major activity on SOLAR-C in FY 2014 was tomake and submit the SOLAR-C mission proposal for the
JAXA Strategic Middle-class Satellite Mission. The JAXASOLAR-C WG helped the European scientists with making
another SOLAR-C proposal for the ESA M4 opportunity, which
was submitted in Jan 2015 to get development funds for theEuropean contribution. The WG submitted the mission proposal
to JAXA in Feb 2015. Both examination outcomes will come inthe early part of FY 2015.
The instrument assembly, testing, and calibrations were
performed on CLASP for the flight operations in summer 2015.
For the installation of components supplied by the USA partnergroup, the USA scientists and engineers joined the assembly
and test activities in Japan. The CLASP project has received
significant contributions from the ATC in design, fabrication ofnecessary components, and testing of some of the flight models.

4. Others
Although the SOLAR-C Project Office is reimbursed by the
NAOJ for its general operation and emergencies, a large part ofthe expenses for supporting the project preparation is funded byother sources including the Grant-in-Aid for Scientific Research,
JAXA’s strategic R&D fund for basic development andexperiment of onboard instruments, and research grants from theprivate sector.
T. Kobiki is going to leave the SOLAR-C project at the endof FY 2014 and T. Bando is going to move to another project in
May 2015.

16. Astronomy Data Center
1. Introduction
The Astronomy Data Center (ADC) is a central core ofcomputing and archiving for astronomical data and supports
scientists around the world through the provision of our wide
variety of data center services. In addition, ADC is driving
forward research and development programs for future
generations of services. Our activity is organized into the DB/
DA Project, Network Project, JVO Project, Project for HSC
Data Analysis/Archiving Software Development, and the Openuse computer system and service.

2. ADC Report(1) DB/DA Project
The DB/DA-project conducts research and development on
astronomical databases and data analysis. It also opens various
astronomical data to researchers and educators (http://dbc.nao.
ac.jp/).
SMOKA (http://smoka.nao.ac.jp/) is the core of the DB/
DA-project and presents 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). The total amount of opened data ismore than 10 million frames (54 TB) as of May 2015. SMOKA
contributes to many astronomical products. The total number ofrefereed papers using SMOKA data is 173.
(2) Network Project
The network project designs and operates NAOJ information
network infrastructure for the Mitaka Headquarters and thebranch offices. The noteworthy topics of this fiscal year are as
follows.
1) Upgrading International circuit between Tokyo and Hawai`i:
NAOJ operates a high bandwidth network between Hawai`i andTokyo for transmitting the huge amount of science data from
Subaru Telescope. In this year, we upgraded from ATM based
155 Mbps circuit to Ethernet based 1 Gbps circuit. Also westarted a NAOJ data center service in Honolulu and the NAOJ
network has been connected to the Honolulu Internet exchange(HIX) and the DRF Internet service provider in the UnitedStates.
2) Mizusawa 10 Gbps R&D Project: We are continuing R&D forhigh traffic data transfer architecture for science data exchangeon Mizusawa 10 Gbps circuit committed to the NICT JGN-X
project. In this year, we made a partnership with Intel and are
now implementing “Renjyaku+” which is based on the Intel
Data Plane Development Kit. It’s able to exchange digital datawith an actual transmitting rate over 100 Gbps.

implemented basic functions such as, “Quick Search,” “BasicVO Search,” “Parallel VO Search.” We also implemented
functions to display the search progress, to view the search
results, and to access data stored on JVOSpace. We added a newfeature to the JVO/ALMA data archive which enables users tosearch data based on the observed frequencies. The JVO/ALMA
data archive system was demonstrated at the ASJ meeting
held at Yamagata University. A cross identification system wasdeveloped to identify the same objects among big catalogs,
which enables cross identification from 20 billion records in
10 minutes. VO school was held in January 2015, and threeparticipants learned how to use the JVO portal and several VO
tools. The all-sky image data taken by AKARI/FIS have been
incorporated into the JVO database system, and they are now
accessible with the VO interface.
(4) Project for HSC Data Analysis/Archiving Software Development
This project started in January 2009. The main purpose
is to develop the data analysis pipeline and data archiving
software for Hyper Suprime-Cam (HSC). Our main efforts areconcentrated on the implementation of the software to achieveeffective data analysis/archiving by parallel and distributed
processing; precise photometric and astrometric calibrations;and correction of various effects originating from the camera
system.
The Strategic Survey Program (SSP) using HSC began in
March 2014 and we started to have stable large data output(about 300–400 GB per night). We ran the data analysis pipeline
software on the data, produced databases storing the results,
and released them to the SSP team collaborators twice during
the fiscal year (in September 2014 and February 2015). The
amount of released data is about 50 TB, the number of image
files is 200 thousand, the number of objects listed in the released
catalog is about 80 million and the database size is about
2 TB. We’ve developed various software for getting images
or catalog data using the database through web browsers, andthey are now operating stably. We are planning to improvethe usability and to also add many functions for effective data
search/retrieval to accelerate scientific activities based on thereleased data. The computers/hardware for the data release arein stable operation and software with minimum functions is in
the operational phase. Improvements to the functions and new
development for the data analysis pipeline software are still
essential for achieving the planned accuracies for the calibration/measurement of celestial objects in the images. The on-site data
analysis system developed since 2011 is now in the operational
phase, and performed well in SSP and open-use observation
with observer support tools, such as an observation log viewer,
which allows browsing of the data analysis results through a
web browser. This is a large contribution towards the smooth
operation of the Subaru Telescope.

(3) JVO Project
We continued development of JVO portal version 2. We

II Status Reports of Research Activities

105

(5) Open-Use Computer System and Service
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 “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 FY 2014, the total number of users and data requests were
384 users and 31 TB, respectively.
During the course of inter-university research, we also heldor supported some workshops on using software and systems.
The dates and numbers of participants in FY 2014 were as
follows.

1. SOKENDAI summer school, July 31–September 8, 2014, 3
users (Supported)
2. Subaru autumn school 2014, September 24–26, 2014, 12 users
3. ALMA CASA tutorial, October 29, 2014, 32 users (Support)
4. IDL School for FITS analysis, December 9–10, 2014, 12 users
5. N-body simulation winter school, January 26–28, 2015, 13 users
6. VO School, February 26–27, 2015, 3 users
7. SQL school, March 3–4, 2015, 7 users
In FY 2014, the schools were held a total of 7 times for 82
users.

3. Others
As part of outreach and promotion activities, 90 issues of“ADC News” were published from No.386 to No.436 in FY
2014. The news was distributed by e-mail to users and appearedon the ADC webpages.

17. 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
for both current on-going astronomy programs and for future
programs.

Figure 1: New Organization Chart of ATC from October 2014.

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The development of ALMA receivers has been one of
the “prioritized area developments,” and their fabrication andshipment were concluded in FY 2013. In FY 2014, some of
the receivers with degraded performance were sent back to
ATC for maintenance. In the ATC management committee,
discussions were held about reorganizing ATC for ALMA
receiver maintenance and other development activities. The new
ATC organization shown in Figure 1 started in October 2014.
ALMA receiver development teams were divided into threegroups, which are “ALMA receiver maintenance”, “advanced
receiver development,” and “telescope receiver development.”
The “telescope receiver development” group works on receiverdevelopments within the common use programs.
The “prioritized area developments” includes instrument
development for IRIS, to be used with the Thirty Meter
Telescope (TMT), and for the gravitational wave telescope
KAGRA. The design and production of equipment have been
supported by the mechanical engineering shop (ME shop).
Another “prioritized area program,” Hyper Suprime-Cam (HSC),
started observations in March 2014.
The “advanced technology developments” includes
development for radio imaging arrays, the solar-observing
rocket-borne instrument CLASP, and others. CLASP isscheduled to be launched in summer 2015.
The oversight committee of ATC with non-NAOJ members

discussed ATC activities on current projects and R&D for
future programs. In FY 2014, ATC activities for ALMA receiverdevelopment were reviewed and will feedback to ongoingprograms such as TMT. R&D programs will be reviewed in FY
2015 accordingly.

2. Workshops and Development Support Facilities(1) Mechanical Engineering Shop (ME shop)
The aim of the ME shop is to work on design, machining,and evaluation of astronomy instruments, in other word to
support astronomy “MONOZUKURI” (fabrication). Threeteams for the corresponding functions (design, machining, andevaluation) work efficiently using their advanced skills.
The design team worked hard on structural designs of
KAGRA’s auxiliary optics subsystem (AOS) and TMT/IRIS’s
focal plane assembly.
For KAGRA, the following items have been performed:• Design of mirror mount for BRT (Beam Reducing Telescope)• Vibration analysis of the BRT structure• Design, assembly, and evaluation of mirror suspension XYθ
traverse mechanism• Assembly of six ‘bottom filters’• Mechanical design and vibration analysis of Type-Bp mirror
suspension• Vibration analysis and improvement of Type-A mirror
suspension
For TMT/IRIS, the following items have been performed:• Design of atmospheric dispersion corrector (ADC), cold stop,
filter exchange mechanism and detector mount• Test fabrication and evaluation of ADC• Test fabrication of the filter exchange mechanism• Vibration test of a kinematic lens cell
• Design and fabrication of a medium-sized cryogenic vacuum
chamber.
For other programs, there were the following items:• Support of HSC on-sight evaluation• Design of a universal support mechanism for ALMA receivers• Design of a 4-element horn array and a detector mount.
The machining team worked on KAGRA and TMT/IRIS
instrumentation as well as numerous requests from NAOJ and
non-NAOJ users. For KAGRA it machined 11 sets of bottom
filter parts on schedule; this followed the proto-type machining
in the previous year. One of the materials for the bottom filter‘maraging steel’ with high stiffness was successfully machined
within the required accuracy. In FY 2014, an additional request
was received to machine the ‘recoil masses’ from the material
Ti-6Al-4V. After test fabrication of 2 sets of recoil masses, 8
sets were successfully fabricated. For TMT/IRIS, mechanicalparts and interfaces for ADC were fabricated after component
evaluation feedback, which all serves to help realize cryogenic
operation of the instrument. Other machining includes kinematic

mounts made of invar for CLASP; a waveguide for the ionengine of ISAS; and waveguide and horn components for radio
imaging array development.
In the field of super-precision machining, work has been
done in collaboration with other institutes and upon users’
requests for precision machining. In one of the collaborative
programs, we performed super-precision milling using singlecrystal diamond tools in collaboration with the High Energy
Accelerator Research Organization (KEK). The program aimed
to achieve efficient machining of a mirror surface for the
X-band acceleration disk; test fabrication and evaluation were
performed. Another collaborative program was conducted with
the Institute for Molecular Science and Nagoya University.
This one, which continued from FY 2013, involved machining
MgF2 aspherical lens using a single-crystal diamond tool
and was successfully concluded. For submillimeter-wave
camera development, wide-band corrugated feed-horns havebeen fabricated by a milling process, which resulted in good
performance, and machining started for a 4-element corrugatedfeed-horn array.
The ME shop accepted 132 machining or repair requests
in FY 2014. With 7 programs carried over from FY 2013, 133
out of 139 programs have been concluded and 6 programs arecarried over to FY 2015. There were 7 programs requested fromoutside NAOJ. The following table shows the requests in FY
2014. (Numbers in the parenthesis show the programs carriedover to FY 2015.)
Carried over from FY 2013
ATC
HSC
TMT/IRIS
KAGRA
SOLAR-C/CLASP
Solar Observatory
Subaru Telescope
ALMA
ASTE
RISE
ADC
Exo-Planet
JASMINE
FOREST7
23 (3)
1
10
17 (2)
36
6
1
7
1
2
2
13 (1)
4
1

Other Divisions

2

Outside NAOJU Tokyo
JAXA/ISAS
Total

4
2

139 (6)(2) Optical Shop
A. Management and maintenance• Measuring instrument maintenance (such as daily inspections)• Technical consulting for users: 67• Repair and upgrade

II Status Reports of Research Activities

107Interferometer ZYGO-GPI alignment camera exchange
Solid Spece-3700 repair
Replacement of HEPA filters in the optical shop
B. Open use of measurement instruments (April 2014 - March 2015)• The number of annual users: 391
ATC internal: 159
NAOJ and the Institute of Astronomy, University of Tokyo: 196
Other organizations: 36• Use of LEGEX910 (large-scale 3-D measurement machine): 37
ALMA and HSC: 13
Measurement requests to the optical shop: 24
Number of operating days: 50(3) Optical and Infrared Detector GroupThe group supports domestic and foreign instrument groups
who use fully-depleted back illuminated CCDs (FDCCD). Since
last year, at the request of a domestic group we have upgraded
and tested a cryogenic dewar and a cooler for Kyoto3DII
camera, a PI instrument of Subaru Telescope. This new camera
will operate on the telescope in FY 2015. Furthermore, forforeign instrument groups using FDCCDs, we responded totheir requests by e-mail, upgraded the manual on the website,
and also conversed with them at conferences. We also attempted
to set up an evaluation system for the detectors of the Solar-C
project, which will be evaluated in FY 2015.
(4) Thin Film Processing Unit
For the SuMIRe (Subaru Measurement of Images andRedshifts) project, we fabricated wideband anti-reflection
coating on the micro-lenses of input optical fibers. The 3500
lenses were coated successfully by high performance multilayer.
The lenses are being evaluated at Subaru Telescope.
(5) Space Chamber Shop
The shop supports common use programs that use vacuum
chambers and equipment in clean rooms. Major common use
programs include usage of the vacuum chamber at the Institutefor Molecular Science to evaluate the CLASP instrument using
the UVSOR synchrotron facility, as well as usage of the spacechamber in the ATC clean room for various thermal analyses
under vacuum. The next generation solar observing satellite
program, SOLAR-C, used the space chamber for a variety ofexperiments. Another program, the Wide-field Imaging Surveyor
for High-redshift (WISH), used the facility to evaluate cryogenic
motors for the filter exchange mechanism. Subaru Telescopeused the facility to evaluate optical filters for instruments.
Another small vacuum chamber is often used for out-gas
measurements, and a thermostatic oven was used for thermal
cycle tests of various components.
(6) Facility Management Unit
This unit manages ATC facilities including the buildings,
electric facilities, daily maintenance of the Cold Evaporator (CE),
maintenance of building equipment, oversight of construction,and management of hazardous material and laboratory equipment.

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Concerning the building facilities and equipment, wechanged the lighting apparatus from old fluorescent lamps
to new LED balls in 5 laboratories and a machine shop.
Illumination was largely improved in each laboratory, and in themachine shop it became bright enough for precision machining
anywhere in the room. The coolant water circulation facility
underwent annual maintenance and the rust was removed fromthe duct line. However, an accidental break down of the pumpoccurred and users had to rely on public tap water for a period.
All the crane facilities had annual maintenance, and a 4.8-ton
crane had an additional check of its load bearing ability. Afteran inspection by the Labor Standards Inspection Office, it was
revealed that four sets of fume hoods did not meet the required
ventilation performance for toxic fumes. In addition, one of the
fume hoods needed to neutralize fumes from hydrogen fluoridebased solvent, and a so-called Scrubber is to be installed. Mostof the organic solvents, oils, and fats are now stored in a separate
hazardous material storehouse. In addition, the unit cooperated
with a new building under construction for the TMT program
which will be completed in FY 2015.
Concerning the laboratory usage including clean rooms, themain users are ATC members, KAGRA, TMT, the Division ofRadio Astronomy, HSC, JASMINE, the Division of Optical andInfrared Astronomy, the Exo-planet team, Subaru Telescope, andthe SOLAR-C/CLASP team. KAGRA used a clean room in thesouth building and CLASP used one in the north building. The
CLASP team finished instrument evaluation before March 2015,
and was prepared to launch from the United States of America insummer 2015.

3. Open Use Programs
In FY 2014, ATC announced and accepted open use programs
twice a year. ATC facilities were used for 7 “collaborative
development programs” and 30 “facilities use programs.”
Information about these programs is presented in “Common use
of ATC facilities” with names of the leaders and research titles.
Reports from the open use programs are also presented on the
ATC homepage.

4. Prioritized Area Developments(1) ALMA Band 4, 8, 10
In the ALMA project, mass-production of the Band-4, -8,
and -10 receiver cartridges (the development of which Japanis responsible for) and their shipment to Chile were completed
within FY 2013. In FY 2014, problems occurring at the Chilesite were responded to, and in September, while some of thework still remained, the PAS (Provisionary Acceptance on-Site)tests were completed.
The teams “ALMA receiver maintenance”, “advanced
receiver development” and “telescope receiver development”
have been created by reorganizing the previous receiverdevelopment teams for Bands 4, 8, and 10. The purpose ofthis was to formalize the framework for receiver cartridge
maintenance, to be able to broadly apply the technology

cultivated through the development of ALMA to othertelescope receivers, and to propel forward the development ofadvanced receivers for the future. Under the strong leadershipof the director of ATC, work efficiency has been improvedby coordination between teams for appropriate placement of
personnel, and by sharing instruments and equipments.
Regarding the ALMA project, the “ALMA receiver
maintenance” and “advanced receiver development” teams
will continue to be placed in the category of “prioritized area
developments.” With respect to the maintenance of ALMA
receivers, we will steadfastly carry out the maintenance ofreceiver cartridges for Bands 4, 8, and 10. In addition, withregard to “advanced receiver development,” we will pushforward with receiver development that supports the futureof ALMA, such as wide bandwidth, multi-pixel, and higher
frequency receivers. Also, “telescope receiver development”
will be placed in the “advanced technology developments” andwe will push forward with the development of receivers to beinstalled in telescopes such as the Nobeyama 45-m Telescopeand ASTE.
(2) Hyper Suprime-Cam (HSC)
HSC has been used for the regular science operations since
March 24, 2014. This includes both Subaru Strategic Programand normal open-use observation. During FY 2014, the numberof nights allocated to HSC program was April: 11 nights, June:
18 nights, September: 16 nights, November: 19 nights, January:
12 nights, March: 19 nights; for a total of 95 nights (including
engineering nights). We lost four nights in June due to camera
hardware trouble. Several incidents occurred simultaneously
including shutter failure due to the battery of the real time clock
running out and hardware trouble in the HSC control computers.
Because the prime focus is hard to reach, it took more nights tosolve all of these problems. In the early part of FY 2014, we had
minor troubles with the mechanics of the shutters and the filter
exchangers which affected the operation. We had a great deal of
supports from ATC engineering staff near the end of 2014, andall of the problematic mechanics were fixed. As a result, most of
the troubles never occurred during the last two observing runs in
Jan.–March.
Through the engineering runs we confirmed the expected
image quality as well as the throughput of the camera. Using theengineering runs, we improved coordination between HSC andthe telescope control software to make things run parallel. This
enables efficient observation; 90 % of the usable time is now
dedicated to science exposures.
We have a couple of left over items for FY 2015 including
the investigation and replacement of problematic CCDs, thedevelopment of the throughput monitoring system, and a new
single lamp flat field system.
(3) IRIS Instrument for TMT
We have been continuing development of the IRIS instrument
for the Thirty Meter Telescope (TMT) since 2011.
In the preliminary design phase, which started in March
2013, we proposed an optical design which solves all major

problems including (1) optimum field configuration between
the imager and spectrographs, (2) optical distortion of an
atmospheric dispersion corrector (ADC) in the spectrographs,and (3) application of high contrast optics. The new optics
design also achieves 4 times larger field of view than theprevious conceptual design with all the requirements satisfied
without significant increase in the cost. The design has been
approved by the TMT Board. The optical design continued
evolving to an all reflective design which is now regarded as abaseline.
We also made good progress in fabricating prototype
coatings and filters with higher throughput than ever to realize“high throughput, low wavefront error optics.”(4) Gravitational Wave Telescope KAGRA
We developed KAGRA’s auxiliary optics subsystem (AOS)
and vibration isolation subsystem (VIS) with the Gravitational
Wave Project Office.
For AOS, some of the mechanical design aspects for thelarge optical baffles are ongoing. There are five kinds of suchbaffles, and their maximum diameter is around 800 mm. Amongthem, four kinds of baffles are located inside the two 3-km armsof KAGRA, where gravitational wave signals will be converted
to optical signals with high sensitivity. In an interferometricgravitational wave detector, noise contributions due to straylights are generally determined by the product of the seismic
fluctuations of the baffles, their surfaces’ blackness, and thecoupling factor of stray light to the main beam mode of theinterferometer. So the baffles should be designed considering
not only the blackness of scattering from the baffle surface but
also their mechanical stiffness. For the mechanical design of thebaffles, the ME shop is supporting finite element analysis of thestructures and helping some discussions on how to assemble andinstall the system.
In addition, we have designed a beam reducing telescope,
which also belongs to KAGRA-AOS. The telescope systems will
be located at the end of each 3-km arm of KAGRA to monitor
the tilt and shift of the beam line, and to provide feedback
signals to the control system. It consists of an optical part,
vibration isolation part, and signal processing part. In FY2014
we designed the optical part.
KAGRA-VIS is a suspension system to isolate the mirrors
required for the KAGRA interferometer from seismic fluctuation.
The system consists of multi-stage isolation filters; the ME shop
has manufactured some parts for the seven pieces of the bottom
filters, and has also performed assembly work, tests, and packing
for delivery. The ME shop has also manufactured two units ofrecoil masses, which will be suspended to reduce the fluctuationsof the mirrors. The recoil masses are made of a special metal, Ti6Al-4V, because of its nice magnetism and conductivity. Though
it was the first time for the ME shop to work with the material, it
successfully machined them. The traversers which support mostof the suspended parts in vacuum and move around smoothly
to place the mirrors as planned, have been designed, assembled,
and tested.

II Status Reports of Research Activities

1095. Advanced Technology Developments(1) Telescope Receiver Developments
Based on the ALMA receiver developments, the “telescope
receiver development” team started its activities, including
development of the Nobeyama FOREST receiver and the345/450 GHz band receiver of the ASTE telescope. We havealso pushed forward the basic study of a cryostat for enabling
simultaneous use of multiple receiver cartridges. ATC can
increase the technology standards of the community by giving
feedback using the technologies and knowledge accumulated
through development of specific projects, and benefit thetechnology developments of other projects, universities, andresearch institutions. It is also important to make the best use of
the achievements of the projects.
(2) Radio Imaging Array Development
In collaboration with the University of Tsukuba, Saitama
University, KEK, and RIKEN, the MKID (Microwave Kinetic
Inductance Detector) group of the Advanced Technology Centeris developing superconductive cameras in millimeter andsubmillimeter wavelengths for the Antarctica terahertz telescope,
which observes distant galaxies with a wide field of view, andfor LiteBIRD, which detects CMB B-mode polarization.
We had progress in the following areas for development ofwide-field-of-view millimeter and submillimeter instruments in
FY 2014.
1) Wide field and compact 0.1 K cryogenic system
2) Wide field of view (1 degree) terahertz optics
3) Anti-reflection coated 700 pixels Si lens-array4) CMB B-mode polarization MKID camera
Tom Nitta, a JSPS Research Fellow for Young Scientists,
moved to the University of Tsukuba as an assistant professor
starting from April 1, 2015.
(3) Terahertz Intensity Interferometry
Intensity measurements of astronomical sources can be used
to realize a type of intensity interferometer known as a HanburyBrown and Twiss interferometer. These are based on thequantum optical behavior of thermal photons. To advance thistechnology in terahertz frequencies, we have started a study on
the measurement of intensity correlations and delay times, andtheir applications to aperture synthesis imaging. In collaboration
with Nobeyama Solar Radio Observatory, Nobeyama
Radioheliograph was used to measure intensity correlation ofsolar 17 GHz radiation and successfully measured delay timewith a precision less than 10 psec with an integration time of 50
msec. Development of superconducting tunnel junction detectors
started to measure terahertz photon pulses, and a concept studyof photon counting terahertz interferometry was performed. The
development activity was supported by a grant from Matsuo
Academic Foundation.
(4) Space Optics
Activities to observe astronomical objects from spaceby using sounding rockets and science satellites have been110

II Status Reports of Research Activities

pursued to realize future space science missions. In FY
2014, fundamental development was executed for the ongoing sounding rocket mission CLASP and for future satellite
missions WISH and SOLAR-C. In FY 2013 the CLASP project,which is a mission to observe solar magnetic fields in thechromosphere and transition region via the hydrogen Lyman
alpha line at 121.6 nm, entered the phase of preparing the flight
instrument. In FY 2014, it moved to the stage of assembling
and testing the flight instrument in the ATC clean room. The
CLASP spectro-polarimetric capability was finally calibrated
by the end of FY 2014 with a UV calibration light source thatwas developed in ATC. The CLASP payload is to be launchedin summer 2015 from a launch site in the USA. For a planned
future solar observing satellite mission SOLAR-C, the first
prototype component developments have been carried out for
the waveplate to modulate the polarization state and for animage slicer optical unit to realize the 2D spectro-polarimetry,in addition to performance evaluation of a near-infrared imaging
device. A collaborative study on the contamination control
for optical surfaces that are exposed to solar UV illumination
has been performed with the JAXA research and development
branch.
(5) Near-IR Imaging Sensor Developments
A commercial InGaAs near-infrared image sensor, which is a
product of a domestic manufacturer, was evaluated at cryogenic
temperatures to improve the readout performance. However,the noise and dark current was still high for astronomical
observation. We have designed a low noise CMOS readout
integrated circuit to improve the readout performance of the
InGaAs image sensors.
General purpose data acquisition systems, MESSIA, havebeen used at several astronomical observatories over the last
decade. We have developed a new version by using a circuitboard originally developed for Hyper Suprime-Cam. As a final
evaluation, we have installed the new system onto an instrumentof the KANATA telescope operated by Hiroshima University,and started test observations.

18. Public Relations Center
1. Overview

Official); and Yuriko Watanabe (Public Outreach Official).

The Public Relations Center engages in the publication,
promulgation, and promotion of scientific achievements madenot only by NAOJ but also by others in the field of astronomy
in general to raise public awareness; responds to reports of
discoveries of new astronomical objects; and provides theephemeris and other astronomical information directly related
to people’s everyday activities, such as sunrise and sunset
times. The Center is comprised of seven offices and one 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.
The activities of each office are reported hereafter.

3. Public Relations Office

2. Personnel
In FY 2014, the Public Relations Center was composed of
Director Toshio Fukushima and the following staff members: 2
Professors, 1 Associate Professor, 3 Assistant Professor (2 holdconcurrent posts), 4 Research Engineers, 1 Senior Engineer,
1 Engineer, 1 Chief of the Library, 2 Specially Appointed
Senior Specialist, 4 Research Experts (1 holding a concurrentpost), 23 Public Outreach Official, 1 Research Supporter, and 2
Administrative Supporter.
Cheung Sze-Leung (Specially Appointed Senior Specialist,
IAU Office for Astronomy Outreach); Tatsuya Uzumaki (Public
Outreach Official, Outreach and Education Office); Hiroshi
Futami (Public Outreach Official, Museum Project Office); andTakaaki Takeda (Public Outreach Official, Museum Project
Office) joined the Center on April 1, 2014. Yukiko Shibata (Public
Outreach Official, Outreach and Education Office) joined on
August 1. Shiomi Nemoto, (Public Outreach Official, Museum
Project Office) and Satomi Hatano (Public Outreach Official,
Outreach and Education Office) joined on March 1, 2015.
The following members relocated: Tatsuya Uzumaki (Public
Outreach Official, September 30); Chisato Ikuta (AssistantProfessor, November 30); Mayumi Hori (Chief of the Library,
March 31, 2015). The following members retired: Norio
Ohshima (Research Engineer); Hideo Fukushima (ResearchEngineer); Shoichi Itoh (Public Outreach Official); Yukie Baba
(Public Outreach Official), Hitoshi Masuzawa (Public OutreachMonthApril 2014
May 2014
June 2014
July 2014

Access counts
576,378
451,804
408,358
634,310The Public Relations Office actively promoted scientificdevelopments produced by various NAOJ Projects including
the NAOJ Chile Observatory and the Subaru Telescope. It
also promoted the results of joint research projects conductedwith universities and other research organizations throughpress conferences and web releases. In cooperation with theOutreach and Education Office, the Public Relations Officealso conducted awareness campaigns for the lunar eclipse,
meteor showers and other astronomical phenomena of interest
to the public. An internet broadcast of the October 8 total lunar
eclipse garnered approximately 30,000 viewers.
(1) Multimedia-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 to the website.
In response to trends in society’s use of the internet,
the Japanese webpage was updated in August to betteraccommodate smart phones.
NAOJ e-mail newslet ters No. 129 –142 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.
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 2015, the number of followers
exceeds 47,000.
(2) Publicizing Developments
There were 16 research result announcements (compared to
26 in FY 2013 and 17 in FY 2012.) Information releases wereactively presented, totaling 26 articles (Tables 2, 3).
In the perennially popular Astronomy Lectures for Science
Journalists program, the title of the 21st lecture was “The Startof Construction for TMT,” held before the September 30, 2014
groundbreaking ceremony for the Thirty Meter TelescopeMonth
Access counts
August 2014
1,180,446
September 2014
696,725
October 2014
2,179,203
November 2014
581,852
Total: 8,996,425

Month
December 2014
January 2015
February 2015
March 2015

Access counts
532,836
641,761
470,296642,456

Table 1: Monthly website access statistics for the Public Relations Office website, NAOJ Public Relations Center (April 2014–March 2015).

II Status Reports of Research Activities

111

May 21, 2014
July 7, 2014

Revealing the Complex Outflow Structure of Binary UY Aurigae
Still hot inside the Moon: Tidal heating in the deepest part of the lunar mantle

July 29, 2014

Next-Generation Thirty Meter Telescope Begins Construction in Hawaii

August 18, 2014

Mysterious Space Tornado Formation Process Clarified (Japanese Only)

September 17, 2014 Creating Pancakes using Galaxy Collisions-Violent Origins of Disk Galaxies Probed by Radio Telescopes
November 7, 2014 Revolutionary ALMA Image Reveals Planetary Genesis
November 13, 2014 Supercomputer for Astronomy “ATERUI” Upgraded to Double its Speed
November 19, 2014 Huge Sunspots and their Magnetic Structure observed by “Hinode”
December 4, 2014

Astronomers Identify Gas Spirals as a Nursery of Twin Stars through ALMA Observations

February 26, 2015

ALMA Revealed Surprisingly Mild Environment around a Supermassive Black Hole
(Japanese, English release by NAOJ Chile Observatory)

March 31, 2015

ALMA Disentangles Complex Birth of Giant Stars
Table 2: Web releases.

June 3, 2014
June 19, 2014
July 3, 2014
August 8, 2014
February 2, 2015

Giant Explosion Buried in Dust: ALMA Probes Environment around Gamma Ray Bursts
Jupiter’s Moons Remain Slightly Illuminated, Even in Eclipse
Dynamical Star-Forming Gas Interaction Witnessed by ALMA
A Chemical Signature of First-Generation Very-Massive StarsClassical Nova Explosions are Major Lithium Factories in the Universe
Table 3: Press Conferences.

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

Solar info Lunar info Ephemeris info
204
116
45
200
284
46
230
324
78
214
130
71

Time
6
8
3
15

Solar System Universe
168
65
150
68
294
85
186
74

Astronomy
107
118
125
106

Other
774
995
669
468

Total
1485
1869
1808
1264

Table 4: Telephone inquiries made to the Outreach and Education Office of the NAOJ Public Relations Center (April 2014–March 2015).

(TMT). A total of 37 participants listened ardently to theproject progress report and lectures about the key science. The
materials used in the lectures where distributed to participants
beforehand. We also concentrated on a way to deliver thelectures via the internet for reporters who can’t attend.
(3) Activities as NAOJ’s Public Relations Center
The following activities were pursued in addition to theCenter’s regular task of aiding research result releases.
The Public Relations Office produced 6 videos in both
English and Japanese to introduce the research activities at
NAOJ to a broad public audience. The titles included “Analyzing
the Universe at multiple wavelengths,” “Telescope: Going backthrough the Universe’s History,” and “Research and Education
at NAOJ.” As of the end of March 2015, these videos have beenviewed a total of approximately 10,000 times.
The Office also helped Projects with their own lectures
for the general public. In November it assisted with a lecture
introducing the successes of the Subaru Telescope, whichcelebrated its 15th Anniversary, and the expectations for TMT.
This was co-sponsored by Sendai Astronomical Observatory.
This was the first time one of these lectures was attempted
outside of Tokyo. In December, the Office assisted withlectures presenting the latest results from ALMA.
The Off ice also and cooperated with documentation

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and offered exhibit materials and image contents for thelarge events “Space Expo 2014” (presented by NHK andothers) and “Hikari- The Wonder of Light” (presented by the
National Museum of Science and Nature and others). Training
in photography was offered twice, in June and October, toimprove the skills of outreach personnel in each project. In
July, Social Networking Service (SNS) training was offered to
all NAOJ personnel to elucidate communication using SNS.

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 6,426 telephone inquiries (Table 4) and141 letters, 69 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, 2 were conducted: “Summer Nights: Let’s Count
Shooing Stars, 2014” in August (346 responses) and “Let’s
Observe the Total Lunar Eclipse” in October (1,293 responses).
The “Fureai (Friendly) Astronomy” project, in its 5th

year, provided events to 51 schools, covering all that applied,with 4,812 pupils in attendance. Many of the responses fromthe pupils expressed interest in seeing stars or aspiration forbecoming astronomers, suggesting that the event was a good
opportunity to familiarize the children with astronomy andto inspire them by meeting and learning from astronomers. A
total of 42 lecturers participated.
On August 4 (Monday) and 5 (Tuesday) during summer
vacation “Summer Vacation Junior Star-Gazing Party + You
are Galileo!” events were held for elementary, junior high,and high school students (application required, maximum
capacity 50 participants). Including guardians, the numberof participants to hear lectures about handcrafting and using
telescopes exceeded 100 on both days. There were a total of 217
participants (112 on August 4 and 105 on August 5).
The Public Relations Center participated as the secretariat
for the Mitaka Open House Day, a special public event held at
Mitaka Campus and organized by the steering committee. This
two-day event was held on October 18 and 19 with the theme“TMT Challenging the Frontiers of Space.” It was co-hosted by
the Institute of Astronomy, School of Science, the Universityof Tokyo, and the Department of Astronomical Science at the
School of Physical Sciences of the Graduate University of
Advanced Studies. Both days were graced with clear skies.
Events thrived with 4,768 visitors, the most ever, in attendance.
Each Project offered a selection of activities based on their own
expertise which were suitable for a wide range of age groups.
Activities included the viewing of facilities not normally open
to the public, interactive panel displays, mini-lectures, andpopular quizzes and games.
The 5th International Science Film Festival was co-hosted
between August 1 and September 29, with more than 100
participating affiliates. Screenings of science films and otherevents such as a stamp-collection rally were held at 36 science
museums, planetariums, and film theaters in Japan, withmore than 1 million people participating. The Kickoff Event(Hiratsuka City Museum) Dome Festa (Hiroshima Children’sMuseum) and Closing Event (Koriyama City Fureai Science
Center) were held as the core events.
The “NAOJ Tours” cohosted each year with Tamarokuto
Science Center were held on Monday, January 5 and Sunday,
March 8. These days consisted of a sunspot observation eventat the 20-cm Telescope Dome, self-guided tours along the tour
course, star chart production, explanations of the theory behindnavigation, and a stargazing party at the 50-cm Telescope for
Public Outreach. Each day had a total of 40 participants, for a
total of 80.
“The 10th Workshop for Popularizing Cutting-Edge
Ast ronomy @ A LM A in Chile” was held at the Chile
Observatory focusing on ALMA. A total of 25 researchers andpeople engaging in education or astronomy promotion took part.
The Office conducted the following events in Mongolia, aspart of the “You are Galileo!” project from June 30 to July 6,
2014, in cooperation with the Office of International Relations
with support from the Foundation for Promotion of Astronomy.
On July 1, a lecture and handmade telescope workshop washeld at an elementary school in Byan Ulgi Mongolia with 40
participants. Additionally, a stargazing event was held in a
nomad camp with approximately 50 participants. The “1st East
Asian Astronomical Education and Outreach Workshop” washeld July 3-5, at the National University of Mongolia in thecity of Ulaanbaatar. A total of 35 participants from 5 countries(Nepal, Hong Kong, Portugal, Japan and Mongolia) attended.
The data reduction software Makali`i, developed toenable FITS data obtained from Subaru Telescope scienceobservations and other sources to be used in astronomy
education and outreach, was distributed via the internet todomestic and international users. The Outreach and Education
Off ice cooperated with the Japan Foundation of Public
Communication on Science and Technology to produce the“Hikari-zu” (Light Diagram) poster (A1, A2 sizes, both
Japanese only).
(3) Community Activities
The “Mitaka Picture Book House in the Astronomical
Observatory Forest” welcomed 38,911 visitors in FY 2014.
The Outreach and Education Office participated in planning
the “Stars and Constellations” (July 2013 – June 2014) and“Picture Books and Space” (July 2014 – June 2015) exhibits.
In addition, it cooperated with staff members from the Mitaka
City municipal offices and local volunteers for modern andtraditional Tanabata celebrations and Moon-Viewing parties.
Furthermore, it cooperated on the “Mitaka Picture Book
House in the Astronomical Observatory Forest, Picture Book
Original Drawings Hallway Exhibit Contest.” The best pieces,“Kimi Ni Mieru Yoni” (“So You Can See” text and pictures by
Hiromu Aono) and “Hoshi Miru Ojisan” (“The Man Watching
the Stars” text and pictures by Nao Mori), were publishedwith Bun-Shin Publishing as the “Picture Book House in the
Astronomical Observatory Forest Compilation Series,” createdin NAOJ’s hometown.
The Outreach and Education Office conducted the 6th“Mitaka Solar System Walk” in cooperation with the non-profit
organization (NPO) Mitaka Network University Promotion
Organization. Held from September 20 to October 26, stamps
were placed at 154 shops and 63 facilities, including NAOJ
Mitaka Campus and the Mitaka City Municipal Office, for a
total of 217 locations around Mitaka. Approximately 15,000
guide-maps/stamp-sheets were distributed, of which 2,665
people turned theirs in for a prize. The total number of stamps
was 275,315; the average number of stamps collected was 103
per person. The number of participants who collected all of thestamps was 63. It was a good chance to tour the Solar System
while promoting commerce and industry and providing families
with a way to enjoy 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 20 participants at a time and is held in the evening on the
3rd Saturday of every month except August. The Outreach and
Education Office also assisted in presenting Star Sommelier
Mitaka, an astronomical guide training course hosted by

II Status Reports of Research Activities

113

Mitaka Network University that provided telescope operation
workshops and other related events.

5. Ephemeris Computation Office
The Ephemeris Computation Office estimates calendricalphenomena such as the apparent positions of the Sun, Moon,and planets on the basis of international standards and publishes
the “Calendar and Ephemeris” as part of the compilation ofalmanacs, which is one of NAOJ’s raisons d’être.
(1) The office published the 2015 edition of the Calendar andEphemeris, the 2015 version of the calendrical section of the
Rika Nenpyo, and the 2016 edition of the Reki Yoko (posted in
the official gazette on February 2, 2015). In the 2016 Reki Yoko,
DE430 is adopted as the standard ephemeris instead of DE405.
The internet edition of the Calendar and Ephemeris was also
updated to match what was published in the Reki Yoko.
(2) As for the website (http://eco.mtk.nao.ac.jp/koyomi/index.
html.en), the contents of the Ephemeris Wiki were expanded
and all of the contents were made mobile friendly. The Officecooperated with promotional campaigns again this year.
The position of Comet Lovejoy and the radiant points of the
Perseids and Geminids meteor showers were published in
the Astronomical Information section of the website. Neither
the total lunar eclipse nor the New Year’s sunrise had good
weather, but the page view still exceeded 28 million.
(3) The Japan Association for Calendars and Culture Promotion
hosted its 4th General Meeting, the Calendar Presentation
Ceremony, and two Symposia on the Traditional Calendar 2033
A.D. Problem.
(4) The Office hosted regular exhibitions in collaboration with
the Library, selecting from NAOJ’s invaluable collection ofhistorical archives written in Chinese/Japanese. The themes of
the 50th and 51st exhibitions were “Weather Documentationfrom Towns” and “Star Charts” 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 two full-time and twopart-time, handled reports of new astronomical objects andother communications submitted to NAOJ. Lately, about 20
reports per year have been submitted. But this year there wasa total of 32 reports including confirmation requests for newcelestial object candidates and other reports. The contents
were: 12 novae/supernovae, 10 comets (including cometary
objects), 8 luminous objects, 1 fixed star, and 1 astronomical
phenomena question. Particularly in recent years, there has
been an increase in cases where the ghost images of brightstars produced when using a filter to eliminate light pollution
have been mistaken for comets. In amongst the many examples
reporting an already known comet or a planet as a new

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object, the report of a supernova in September bares mention.
Simultaneous to the discoverer reporting it to NAOJ, it wasalso reported to Kyushu University’s Hitoshi Yamaoka. Hitoshi
Yamaoka sent a notice to the International Astronomical Union
Central Bureau for Astronomical Telegrams. This event was
acknowledged as Supernova 2014cy.

6. Museum Project Office
In FY 2013, the section responsible for managing publicaccess to the facilities was reorganized and the name changed
from the Archive Office to the Museum Project Office. Some ofthese activities are managed in cooperation with the Outreachand Education Office.
(1) Facility Opening Events
Except for the 4 month stoppage from December 2014 toMarch 2015 to replace worn out equipment, regular showings
were held at the 4D2U Dome Theater twice a month (the day
before the 2nd Saturday and the 4th Saturday) as in previous
years. Advance reservations were required. The 15 events
this year attracted 1,359 participants. An additional 54 group
screenings were held with 1,543 participants, and 69 tours wereorganized with 622 participants.
Regular stargazing parties held with the 50-cm Telescopefor Public Outreach were scheduled the same days as 4D2U
theater screenings. These were held regardless of cloudy or
rainy weather. Advance booking (300 people for each session)
was introduced in FY 2012 for these events. A total of 23
sessions were held with 5,161 participants.
A total of 19,754 people visited the Mitaka Campus Visitors'
Area in FY 2014. We conducted 197 tours for 5,992 guests,
including 60 workplace visits by schools. There were also 357
media interviews granted. So that diverse guests can enjoy theopen facilities, we developed English, Chinese, Korean, andSpanish versions of the “NAOJ Mitaka Campus Guidebook.”
We also produced an “NAOJ Mitaka Campus Workbook” withquestions elementary students can find the answers to while
touring the facilities.
Guided tours of Mitaka Campus began in June 2011 aspart of the Archive Office/Open House initiative. Each tour
is conducted on an advance booking basis for a group of 20
participants. Tours are organized into two courses: the “South
Course” focusing on Registered Tangible Cultural Heritage
offered on the 1st Tuesday and 2nd Sunday of the month andthe “North Course” focusing on Important Cultural Heritage
and Geodesy-related sites held on the 3rd Tuesday and 4th
Sunday. The Office accommodated 422 people during thetours. In addition, we created the “Mitaka Campus Guided
Tour Handbook” and distributed it to the participants.
(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 themethods and environment for displaying them. The Office alsoestablished the basic concept for the NAOJ Museum (tentativename) including both facility opening efforts and archive works.
On April 25, 2014, seven historically important buildings in
NOAJ Mitaka Campus became Registered Important Cultural
Properties: the Repsold Transit Instrument Housing, Housingof Gautier Meridian Circle, First Meridian Mark Building ofGautier Meridian Circle, Second Meridian Mark Buildingof Gautier Meridian Circle, Old Library and its Warehouse,
Gatehouse, and the Front Gate. This brings the total number ofRegistered Important Cultural Properties to 10.
Guide Volu nteers were registered f rom among thegraduates of the “NAOJ Guide Volunteer Training Course”
sponsored by NPO Mitaka Network University Promotion
Organization (refereed to below as Mitaka Network University)
in FY 2013. Mitaka Network University held the 2nd “NAOJ
Guide Volunteer Training Course.” Four people enrolled,
graduated, and were registered as NAOJ Guide Volunteers.

7. Library Unit
In addition to the normal work of collecting and sorting
scientific journals and books focusing on astronomy andoffering them to students and researchers inside and outside of
NAOJ, the Library continued to digitalize important documents
and open the data to the public. Also the library collection waschecked and the catalog of contents was maintained.

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. 249– No.260 (April 2014–March 2015)- Annual Report of NAOJ Vol. 26, Fiscal 2012 (Japanese)- Annual Report of NAOJ Vol. 16, Fiscal 2013 (English)- Annual Report of NOAJ Vol. 15 Supplement Fiscal 2012(English)I n FY 2014, i n addit ion to nor mal operat ions, thePublications Office tried to strengthen its ability to reachinternational readers. First of all, it produced the “Annual
Report of NAOJ Vol. 15 Supplement Fiscal 2012” completingthe translation of the Japanese Version. Likewise, English
Volume 16 was also a complete translation. NAOJ News
also started producing feature articles and series related tointernationalization. (The September edition’s theme wasinternational education and outreach. The 1st installment ofthe ‘NAOJ Foreign Staff Interviews’ series appeared in the
December edition.) The Office investigated the possibility of
producing an international edition of the Rika Nenpyo. In daily
work, to support the outreach activities of various Projects

through NAOJ News, special editions focusing on feature series
were systematically produced. Extra copies were printed andgiven to the relevant Project’s outreach personnel. The special
edition themes were: “Museum” (April), “Library” (June),“TMT” (August), “Vapor Deposition Techniques” (January),and “ALMA” (February). From now, we plan to develop andshare NAOJ News articles so that they can be used as a sourceof content for each Project’s outreach activities. To this end,
we promote close cooperation to produce comprehensive,
fundamental articles. To facilitate this flow, we are reediting
various levels of articles issued by the Publications Office
to construct integrated NAOJ public relations, outreach, andeducation contents (and a basic platform for these). At the sametime, we are in the process of producing a digital book basedon the last 12 years of articles from the “Annual Report of
NAOJ Research Highlights” as a prototype for promoting thedigitalization and integration of published contents. In addition
to periodicals, the Office produced the 2015 calendar “Historical
Observational Instruments of NAOJ.” This is the 10th calendar
produced since 2005. The office also helped to create the poster
for the Mitaka Special Open House Event again this year, andsupport was also given to the publication of the “Rika Nenpyo,
Chronological Scientific Tables.”

9. International Astronomical Union Office for
Astronomy OutreachIn 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 by the Public Relations Center Outreach and
Education Office. Cheung Sze-Leung started work as theOutreach Coordinator in April. Since then the OAO has been
located in a new office within the Public Relations Center: theIAU Office for Astronomy Outreach. IAU OAO is responsible
for IAU’s international outreach activities, in cooperation with
the Outreach and Education Office and others. In FY 2014 itprimarily conducted the work for the International Year of
Light 2015 “Cosmic Light” and the NameExoWorlds Contest.
“The Globe at Night – Sky Brightness Monitoring Network
Users Workshop” was held January 7-9, 2015 at NAOJ Mitaka
Campus. There were a total of 30 attendees from Hong Kong,
the Republic of Korea, Taiwan, Nepal, Mongolia, the Republicof the Philippines, and Japan.

II Status Reports of Research Activities11519. Division of Optical and Infrared Astronomy
1. Overview

2. Observational Research

The Division of Optical and Infrared Astronomy oversees
the Okayama Astrophysical Observatory, the Subaru Telescope(C Project), the TMT-Japan Project Office, the Gravitational
Waves Project Office (B Projects), the JASMINE Project Office,and Extrasolar Planet Detection Project Office (A Projects). The
primary purpose of the division is facilitating and invigorating
projects and individual research through personnel exchanges
to place researchers in environments more suitable for theirindividual projects. While pursuing seminal observational anddevelopmental research, the division launches new projects
as necessary to further these goals. The division also actively
engages in graduate education efforts to foster next-generation
talent. These activities are based on the concept that the Divisionof Optical and Infrared Astronomy is a center for personnel
exchange between the Subaru Telescope facility engaging inopen use, and universities and research institutes in Japan,
focusing on developmental research into new instruments andobservational research. This concept was developed when the
Subaru Telescope was constructed.
Almost all NAOJ members in optical- and infrared-related
fields have positions in the division and engage in either thedivision or A, B, or C Projects. At times, they may also haveaffiliated positions in many other projects. The division and thevarious projects carry equal weight in organizational terms. The
primary staff of the Division of Optical and Infrared Astronomy
in FY 2014 consisted of one professor, one associate professor,
three assistant professors, one specially-appointed assistantprofessor and two JSPS research fellows.
The division coordinates educational, research, andadministrative activities for all research divisions and projects
except for the Gravitational Wave, JASMINE, and TMTJapan (TMT-J) projects. The TMT-J project has come to an
expansive stage in which the telescope fabrication has been
started. In tandem with this progress, personnel transfer occurs
often within the Optical and Infrared Astronomy Division. The
division plays an increasingly important role in coordinating
between the Subaru Telescope and TMT-J projects. The
division as a whole maintains and operates facilities to support
research; e.g., a mailing list server for the Mitaka offices of
the Subaru Telescope, TMT-J, Extrasolar Planet Detection,
and Gravitational Wave Project Offices; and a web server for
members of the Mitaka offices of the Subaru Telescope, TMT-J,and Extrasolar Planet Detection Project Offices, as well as
graduate students in the division.
The remainder of this report will focus on the research
projects conducted by full-time members of the Division of
Optical and Infrared Astronomy and the activities of projects
that support open use.

(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; thestructure and evolution of the Milky Way; stellar spectroscopy;
objects within the Solar System; structures around late-typestars; and the search for exoplanets. A rapid change in the shapeof the plasma tail of Comet Lovejoy (C/2013 R1) was analyzed.
Observations of extended ionized objects in nearby galaxies andclusters of galaxies were performed, and the data is now being
analyzed. The search for extrasolar planets continued using
direct imaging methods.
Research in other areas is also in progress, including
astronomical phenomena based on old ephemerides and otherdocuments, and statistical research into automatic identificationof AGN using public astronomical archive data and astronomical
databases.
As part of the research using astronomical archive data,
statistical research into stripped gas from galaxies in clusters
was performed. Other research undertaken was on the hostgalaxies of AGN using SDSS imaging/spectroscopy data.
(2) International Cooperative Observational Research
The division also engages in international collaborative
studies with overseas researchers. Research on star formationin the outer parts of nearby galaxies, and on low surface
brightness dwarf galaxies were conducted with a US researcher.
The site survey in western Tibet for constructing a telescopealso continues in cooperation with the National Astronomical
Observatory of China (NAOC).

3. Subaru Telescope-Related Observational
Instrument Development
The division searched for planetary candidates using the
HiCIAO infrared coronagraph, and implemented hardware andsoftware improvements for direct imaging and observation of
protoplanetary discs. The division analyzed the relation between
the real seeing conditions and the environment in the Subaru
Telescope’s enclosure using a computational fluid dynamics’
model provided by other institutions.
In relation to the data archive, the division joins the filesystem-based technology WG convened by the Society of
Scientific Systems to explore the possibilities for overcoming
difficulties arising from storage expansion. For this purpose,guidelines for assessment and analysis of storage systemcapability were investigated and reported.

4. Operational Support for the Subaru Telescope
The Division of Optical and Infrared Astronomy offers

116

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support for the open use of the Subaru Telescope. This includes
organizing open calls for open-use programs, program selection,
administration, and management of open-use-related travel
expenses, and promoting PR activities for the Subaru Telescope.
The division also gives support to the management of data
analysis systems in collaboration with the Astronomy Data
Center. Moreover, the division also supports the Subaru Autumn
Schools co-hosted with the Subaru Telescope and the Astronomy
Data Center, and Subaru Telescope observation classes.

5. Research Environment Maintenance

Graduate University of Advanced Studies, the University ofTokyo, the Tokyo University of Agriculture and Technology,
Tokyo Institute of Technology, Nihon University, and International
Christian University.
Division staff members made active contributions toseminars and self-directed studies. The division participated in
the “Fureai (Friendly) Astronomy” project, dispatching lecturers
to various elementary and junior high schools around thecountry to provide pupils with opportunities to become familiar
with and appreciate astronomy.

The division manages the printers and rented multifunction
photocopiers in the Mitaka Subaru Building, teleconferencing
systems on the second and third floors, sub-networks, and data
backup servers for the Subaru Telescope Mitaka office as partof its efforts to maintain the research environment. The divisionassisted in replacing a UPS battery, updating shared storage for
the Subaru Telescope Mitaka office, and setting up computers
for newcomers. The teleconferencing system and the web server
were replaced. The contents of the division homepage wererenewed. An office migration was performed to meet a requestfrom the TMT-J office.

6. Planning of the Next-generation Large-Scale
Project
The Division of Optical and Infrared Astronomy is engaged
in planning large post-Subaru projects in optical and infrared
astronomy such as TMT and the JASMINE series. A framework
for collaboration between ISAS and NAOJ also needs to beestablished.
A study group on next-generation large disk and computing
systems was launched with KEK, which will handle voluminous
data in five to ten years in the future. Discussions revolve aroundarchival hardware and software 10 years in the future to serve as
an astronomical database for the next-generation observational
instruments and TMT succeeding the Subaru Telescope.

7. PR, Outreach, and Discovery of New
Astronomical Objects
The division cooperates with the Public Relations Centerin supporting PR/outreach activities, such as publications andpress conferences on Subaru Telescope research results anddiscoveries of new astronomical objects. An active participant
in a special public event held at Mitaka (Mitaka Open HouseDay), the Division of Optical and Infrared Astronomy provided
mini-lectures and exhibits and planned projects appealing toelementary and junior high school students such as magnet
puzzles.

8. Educational Activities
The Division of Optical and Infrared Astronomy provides
postgraduate education to 19 graduate students from the

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11720. Division of Radio Astronomy
The Division of Radio Astronomy oversees Nobeyama
Radio Observatory, Mizusawa VLBI Observatory, RISE Lunar
Exploration Project, and NAOJ Chile Observatory operating
the Atacama Large Millimeter/submillimeter Array (ALMA)
and 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 among themselves. The research themes of the Divisionof Radio Astronomy are represented by keywords such as Big
Bang, early Universe, galaxy formation, black holes, galactic
dynamics, star formation, planetary system formation, planetsand satellites, the Moon, the evolution of interstellar matter, andthe origin of life in the context of the evolution of the Universe.
Radio astronomy unravels mysteries and phenomena in the
Universe through radio waves, which are invisible to humaneyes. The detailed research results are reported in each project’s
section and in the research highlights. The Radio Astronomy
Frequency Subcommittee has been established within thedivision, engaging in discussions on protection against artificial
interference generated by electrical/electronic devices, whichcause major obstacles in radio astronomical observations.

1. Radio Astronomy Frequency Subcommittee
The mission of the Radio Astronomy Frequency
Subcommittee is to protect the environment for radio astronomy
observations. In 1932, Karl Jansky of the USA 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 optical pollution from artificial light sources is an
obstacle in optical observation, artificial radio interference
generated by the electrical/electronic devices which surroundus is a major obstacle in radio observations. Breathtaking
advancement has been achieved in wireless communication
technologies in recent years, and wireless commercial products
such as mobile phones, wireless LANs, and automotive radars
are widely used. The areas of radio applications will further
expand in the future owing to its ubiquitous nature but becauseof that unique capability, compatibility among various radio
services, including both active and passive ones, will become aserious issue. Frequency is a finite resource and its sharing is anunavoidable issue. Therefore, further efforts will be necessary
for maintaining the sky free from artificial interference for betterradio astronomy observations.
(1) Role and Organization
The purpose of the Radio Astronomy Frequency Subcommittee
is to ensure that radio astronomical observations are free from
artificial interference and to raise public awareness of the118

II Status Reports of Research Activities

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 2014, the subcommittee
took an active role in formulating the opinion of the Japaneseradio astronomical community (on behalf of the Japanese radio
astronomers) in these coordination efforts.
The subcommittee is composed of members from NAOJ andrepresentatives of universities and research institutes in Japan.
(2) Current Challenges
A sharing study between active radio services and radio
astronomy is crucial for compatibility under the condition of limited
availability of frequency resources. Some rules and regulations
have been established to address the issue of interference
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-wide-band(UWB) technology does not necessitate an operator license
because it is operated at low-levels and wide bandwidths.
Additionally, there has been a rapid increase in demand forhigher frequencies. For example, 76 and 79 GHz automotive
radar are being introduced, aiming to reduce car accidents
resulting in injury or death. And, transportation of high speed
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 effect of interference arising from such radio applications(e.g. wireless business) varies widely depending on the frequency
band used. The radio astronomy observations have been given
priority in a number of frequency bands within the range of
13.36 MHz and 275 GHz under the ITU Radio Regulations(RR). However, negotiations will be necessary between someradio services and radio astronomy if the same priority level isto be shared within a certain band or under adjacent/proximity

conditions. In terrestrial radio applications, unwanted out-ofband signals (spurious signals), even extremely faint ones, canhave a chance of substantial adverse effects on radio astronomy
observations.
Sources of interference that need to be addressed continue
to increase and include the following devices and systems:
the 23 GHz CATV wireless transmission system used inemergencies, where ammonia observations are affected;
21 GHz next-generation satellite broadcasting, where watermaser observations are affected; 1600 MHz mobile satellite
phones used in emergencies, where the observation of pulsars
and the like are affected; and a number of new UWB wirelessapplications used by logistics and manufacturing industries,
where geodetic observations are affected; and high-speed powerline communications (PLC), where decameter-band observations
are affected. 79 GHz automotive radars around Nobeyama
Observatory will cause deterioration in its observation results,
or rather tend to make its observations impossible in the near
future. Radio astronomy observations in the 60 GHz bandare not common because of the high rate of absorption in theatmosphere. Albeit in fact, the 60 GHz system must be watchedclosely in its second harmonics in terms of adverse effects on
CO observations in the 115 GHz band.
(3) International Activities
The ITU’ Radio Regulations (RR), which allocatesradio frequencies to wireless applications, are revised once
every three to four years in the World Radiocommunication
Conference (WRC). The most recent meeting was WRC-12,
held in February 2012. The RR include frequency bands inwhich radio astronomy observation is prioritized. Preparatory
conferences need to be held in Geneva annually in preparation
for the upcoming WRC-15 to discuss necessary matters forthe revision of the RR. 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 in various
international conferences, representing the Japanese communityof radio astronomy researchers. It has also contributed toopinion-forming through its regular attendance at the Asia/
Pacific Region (APG) meetings in preparation for WRC-15, asa delegate representing Japan. In FY 2014, the subcommittee
pursued the protection of radio astronomy frequency bands
through participation in the ITU-R WP7D meetings held in
Geneva in May and October and the ITU-R WP1A meeting heldin Geneva in June. The subcommittee also has participated in
the APG meetings held in Australia in June 2014 and in Thaiin February 2015, in addition to other relevant meetings andconferences.
(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 wireless operators
who generate radio interference, and promotion to raise publicawareness 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
have been conducted concurrently to dealing with the interference
problems in relation to societal and technological trends.
Several examples of the interference problems discussed in
section (2) above are given below. One example is the adventof UWB wireless applications, used in positioning and tracking
material flow in manufacturing and logistics industries. The
applications in the UWB frequency band induce interference in
VLBI geodetic observations to detect movement of the plates inplate tectonics. Although this band is not under RR protection,
it is vital from the perspective of predicting earthquakes and is
the subject of special consideration by the MIC. For 24 GHz
automotive radars, new regulations have been prepared to makean automatic turn-off function a mandatory standard feature sothat the device is disabled upon reaching certain areas aroundradio observatories. A wider scale of distribution is predicted
for 76 GHz and 79 GHz band automotive radars, which justemerged in the market. Of particular concern are the possible
effects of interference from these radars on the 45-m Radio
Telescope at the Nobeyama Radio Observatory, which engages
in observations of spectral-lines of deuterated compounds andother molecules in interstellar matter. The observations withthe 45-m Radio Telescope located in Japan will continue tocarry significance in relation to the international project ALMA,
which is based in Chile and involves 66 high-performance radio
telescopes at an altitude of 5,000 m. Since automotive radars
are highly relevant to human life safety, negotiations have been
conducted with careful analysis in order to reach a mutuallyacceptable agreement.
The 23 GHz band is deployed for emergency wirelesscommunications at times of natural disasters that lead to abreakdown of CATV networks. Ammonia molecular lines (RRprotected band) overlap with the 23 GHz band due to redshifts
from the expansion of the Universe. An additional point forconsideration is that the 1.6 GHz band may be of important
use at times of natural disasters for satellite-based mobile
communications rather than terrestrial wireless communications.
The MIC performed as a mediator in discussions regarding
interference issues caused by satellite phones using geostationary
and non-geostationary (orbiting) satellites, and an agreement
on usage conditions was concluded between the parties: service
providers which create the interference and the Radio Astronomy
Frequency Subcommittee representing the radio astronomical
observatories, bearing in mind the importance of the emergency
use of satellite phones at times of natural disasters.

II Status Reports of Research Activities

119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 stageof the satellite. The filter is currently under development in
NHK Science & Technology Research Laboratories based ona series of discussions at NAOJ Mitaka Campus. PLC utilizing
home power lines affects radio astronomy observations in lowfrequency bands below 30 MHz. A petition against unduly hasty
introduction of PLC was submitted to the MIC jointly with ASJ
and the Society of Geomagnetism and Earth, Planetary andSpace Sciences. A press conference was organized to raise broad
public awareness of the relevant facts. Radio observations in the
60 GHz band are not common because of the high atmosphericabsorption rate in that frequency range. Albeit in fact, the 60
GHz system must be watched closely in terms of the trends of its
proliferation in the market, since interference from it may affect
CO observations in the 115 GHz band, which is within the bandof the second harmonics of the 60 GHz radio system.
Moreover, the subcommittee engages in making applications
to the MIC, requesting frequency protection of NAOJ telescopes,
in addition to those owned by the Japanese community 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.

120

II Status Reports of Research Activities21. 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, the Solar-C Project Office, and the Nobeyama
Solar Radio Observatory, and conducts research on the Sun inclose liaison with these respective projects. The operation of
the Nobeyama Radioheliograph was transferred to the SolarTerrestrial Environment Laboratory of Nagoya University, andthe Nobeyama Solar Radio Observatory was closed at the end of
fiscal year 2014 (March 2015). Shin Toriumi has been appointed
as an NAOJ fellow and joined the division in April. The
graduate students supervised by the staff of the above-mentioned
projects also belong to the division. All the permanent staff ofthese projects are affiliated with the division.
The division conducts both theoretical and observational
research into the inner structure of the Sun and outer solar
atmosphere including the photosphere, chromosphere, corona,solar wind, and various phenomena in the magnetized plasma
such as flares, sunspots, solar faculae, and prominences. The
division’s theoretical research includes helioseismology studiesof the internal structure of the Sun, and applications of plasma
physics and magnetohydrodynamics to various phenomena on
the Sun as well as on Sun-like stars. The solar group at NAOJ
started observations from space in the very early stages ofJapan’s space program. The division has participated in thedevelopment of the Hinode satellite, which is currently in orbit,
and is playing a major role in its scientific operation. Research isalso being carried out using the Radioheliograph at Nobeyama
and the Solar Flare Telescope and other telescopes in the Mitaka
campus. In addition, the division has been conducting long-termmonitoring observations of solar activity, and the obtained data
are open to the community.

Ph.D. in September.
The division, in cooperation with Kyoto University andNagoya University, supported the annual research-experience
tour for undergraduate students; about ten students visited
solar-related research organizations and experienced the latest
research in the field.

3. International Cooperation
Y. Katsukawa succeeded Y. Suematsu as 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 are also under consideration for future
ground-based telescopes that would involve collaborations with
East Asian countries and Peru.

1. Research in Solar Physics
NAOJ fellow Toriumi published three papers in refereed
journals as lead author. They are (1) on the formation and flare
activity of delta-type sunspots derived from a combination ofdata analysis and numerical simulation, (2) on the detection ofhorizontal flows on the surface of the Sun prior to the emergenceof magnetic flux from below, and (3) a review article on theflux emergence phenomenon presented at the 7-th Hinode
Symposium. He also has been promoting collaborative researchwith international partners.
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 organizer was M. Shimojo.

2. Educational Activities
The teaching staff of the division supervised three graduate
students from the University of Tokyo and two from the
Graduate University for Advanced Studies (SOKENDAI).
Among them Anjali John Kaithakkal of SOKENDAI obtained a

II Status Reports of Research Activities12122. Division of Theoretical Astronomy
1. Overview
The Division of Theoretical Astronomy (DTA) aimed atachieving internationally outstanding research accomplishments
both in quality and quantity for the following four goals whichwere set by the NAOJ Board, and engaged in research activities
for FY 2014 accordingly:- Advance world class cutting-edge theoretical research.
- Pursue theoretical astronomy research, particularly in areasthat utilize NAOJ supercomputers or large-scale observational
instruments to give further insight into their newest
developments.
- 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 hierarchicalstructure of the Universe in terms of formation and evolution
processes; dynamics; and the physical state of matter. This
research spans astronomy and astrophysics from the early
Universe to galaxies, stars, planetary formation, activities
of compact objects, and plasma phenomena. 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 an influential 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
observational facilities of 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. It also leads research activities in various
related fields of astronomical science. The division started a newseries of DTA symposia and organized two meetings in 2014122

II Status Reports of Research Activities

entitled “Formation and evolution of planets in star forming
regions and in the environment of star clusters” and “Activity
and magnetic properties of compact astronomical objects.”

2. Current Members and Transfers
In FY 2014, the dedicated faculty of the Division ofTheoretical Astronomy included two professors, two associate
professors, and four assistant professors. Another adjunctprofessor and one adjunct assistant professor concurrently holdprimary positions at the Center for Computation Astrophysics. In
addition to these research and educational members, the division
was served by five project assistant professors, including two
NAOJ postdoctoral fellows and one JSPS fellow; one EACOA
fellow; and one administration associate who gave full support
to all activities of the division. Among them Takaya Nozawa andYasuhiro Hasegawa were appointed project assistant professor
and EACOA fellow in April and September 2014, respectively.
Takahiro Kudoh, an assistant professor, was promoted toassociate professor and moved to Nagasaki University.

3. Research Results
The publication category IV research papers 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: 64- Papers in English (conference proceedings, non-reviewed
Papers, etc.): 38- Reports in English (talks at international conferences): 70- Reports in Japanese (talks at national meetings, etc.): 84
Some of the research results are presented as the researchhighlights listed at the beginning of this report. The following
highlights include research in which the division members tookleading roles:- Discovery of Dramatic Optical Variability in a Possible RadioLoud Narrow-Line Seyfert 1 Galaxy (Masaomi Tanaka, et al.)- High-speed Fluid Dynamics in Magnetic Reconnection in a
Low-β Plasma (Seiji Zenitani)- Formation of Carbon Grains in Red-supergiant Winds of Very
Massive Population III Stars (Takaya Nozawa, et al.)- Origins of Large Amounts of Dust Grains and Unusual
Extinction Curves in High-redshift Dusty Quasars (Takaya
Nozawa, et al.)- Opacity of fluffy dust aggregates (Akimasa Kataoka, et al.)- The initial mass function of star clusters (Michiko Fujii)- Polarization Structure of Magnetically Supported Molecular
Filaments (Kohji Tomisaka)- Neutrino Oscillation and Nucleosynthesis in Core-Collapse

Supernova Explosion (Toshitaka Kajino, et al.)- Cosmological solutions to the Big-Bang Lithium problem: Bigbang nucleosynthesis with photon cooling X-particle decay
and a primordial magnetic field (Toshitaka Kajino, et al.)- Supernova Nucleosynthesis of 26Al and Nuclear Structure of
26Si (Toshitaka Kajino, et al.)- The in-medium effects on the neutrino reaction in dense matter(Toshitaka Kajino, et al.)- Induced Amino Acid Chirality From Strong Magnetic Fields inInterstellar Environments (Toshitaka Kajino, et al.)- Asymmetric Neutrino Emission from Magnetized ProtoNeutron Stars: Effects of Absorption Cross-Sections in Isoentropical Conditions (Toshitaka Kajino, et al.)
- Revised Big-Bang Nucleosynthesis with Exotic Dark Matter
Particles: Detailed Quantum Mechanical Calculation (Toshitaka
Kajino, et al.)- Supernova Relic Neutrinos and the Supernova Rate Problem:
Analysis of Uncertainties and the role of Failed Supernovae(Toshitaka Kajino, et al.)- Neutrino Magnetic Moment, CP Violation and Flavor
Oscillations in Matter (Toshitaka Kajino, et al.)- Sterile neutrino oscillations in core-collapse supernova
simulations (Toshitaka Kajino, et al.)Toshitaka Kajino: Special lectures on cosmology and nuclear
astrophysics at the Graduate School of Hokkaido University;
fundamentals of theoretical astronomy at the Graduate
University for Advanced Studies; science of time, space,and matter, and fundamentals of physics 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, andspecial astronomy investigation II at the Graduate School of
the University of Tokyo.
Takahiro Kudoh: Space and Earth science at the University ofElectro-Communications.
Eiichiro Kokubo: Planetary science at the University ofTokyo; special lectures on planetary formation theory at
the Graduate School of Kyoto University; introduction ofplanetary formation at Ryukyu University.
Fumitaka Nakamura: Astronomy investigation at the Graduate
University for Advanced Studies.
Takashi Hamana: Geology at the Tokyo University ofAgriculture and Technology.
Haruo Yoshida: Gravitational mechanics at the Graduate
University for Advanced Studies.

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

Toshitaka Kajino delivered a Super Lecture entitled “Birthof the Universe, Life and Intelligence and the Future” in SSHKorea Joint Symposium held at Kashiwazaki Senior HighSchool in Niigata. Kohji Tomisaka and Takahiro Kudoh led agroup of undergraduate students in visiting actual research sites
during the Summer Student event of the Graduate University of
Advanced Studies.

- Stochastic electron acceleration during spontaneous turbulent
reconnection in a strong shock wave (Tsunehiko Kato, et al.)- Shocking structure in a supersonic reconnection jet (Seiji
Zenitani)- The initial mass function of star clusters (Michiko Fujii)- The world's most extensive simulation of the Milky Way
galaxy (Michiko Fujii)- Revealing Large Amounts of Dust and Unusual Extinction
Curves in the Early Universe (Takaya Nozawa, et al.)- Discovery of a Blue Star at the Location of Supernova 2011dh(Takaya Nozawa, et al.)- Formation of Carbon Grains in Very Massive Primordial Stars(Takaya Nozawa, et al.)- Two- and Three-dimensional Neutrino-hydrodynamics
simulations of Core-collapse Supernovae (Tomoya Takiwaki,
et al.)- Opacity of fluffy dust aggregates (Akimasa Kataoka, et al.)- Cosmological solutions to the Lithium problem: Big-bang
nucleosynthesis with photon cooling, X-particle decay and aprimordial magnetic field (Toshitaka Kajino, et al.)
- A New Production Mechanism for Ultra-High-Eneregy Cosmic
Ray (UHECR) Neutrinos (Toshitaka Kajino, et al.)

4. Educational Activities
The lecture subjects are listed below to supplement Section
III on activities for research and educational adjunct lecturership at the universities and graduate schools:

5. 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:
Michiko Fujii: “Spiral galaxies made by gravitational force” at
Science Live Show Universe.
Takashi Hamana: “Dark matter and dark energy in Space” atAsahi Culture Center Yokohama.
Toshitaka Kajino: “Origin of the elements in the cosmos; Thebirth of the Universe and its mysterious connection withlife” at the meeting of 1953 class union of the University ofTokyo.
Eiichiro Kokubo: “New travelogue to the Solar System” at
Ikebukuro Community College, “The Earth in the Universe”
at Mitaka City College, “Hometown of planets” and “Newworld – exo-planets discovered” at Asahi Culture Center
Kyoto and Shinjyuku, “Origin of the Solar System” atGunma Prefecture Observatory, “Origin of the Earth andMoon” at Sakae China-Japan Center.
Ken Ohsuga: “Computational approach to black holes” at Asahi
Culture Center, Yokohama.

II Status Reports of Research Activities

123

Masaomi Tanaka: “Supernova explosions and the origin ofelements” at Asahi Culture Center Shinjyuku.

6. International Collaborations
Toshitaka Kajino performed duties of the following posts:
editorial board member for the UK Institute of Physics “Journalof Physics G”; review panel member of the European Science
Foundation Euro GENESIS Project; 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*); andinternational referee for the Swiss National Science Foundation(SNSF). Eiichiro Kokubo served as a member of the Organizing
Committee of the IAU’s Extrasolar Planets Commission.
The Division of Theoretical Astronomy played leading roles
in organizing the following international conferences:- The First NAOJ-ECT* International Workshop on “Nuclear
Physics and Astrophysics of Neutron-Star Mergers andSupernovae and the Origin of R-Process Elements,” Trento
in Italy, Sept. 8 - 12 in 2014. This international workshop
was held based upon the agreement made between the NAOJ
and ECT*, both signing the Memorandum of Understanding
mediated through the Division of Theoretical Astronomy.
This agreement encompasses the scientific advancement inborder areas between astronomy and astro-, nuclear-, particle-,and condensed-matter physics by promoting an exchangeof scientists and postgraduate students for international
conferences, joint research projects, and university education
programs in mutual collaboration.
- NAOJ-RIKEN Joint HPCI Workshop on “Physics of NeutronStars and Supernova Explosions,” RIKEN Wako in Japan, Dec.
16 - 20 in 2014.
- NAOJ-Beihang University Joint International Workshop on
Cosmology and Nuclear Astrophysics, Beijing in China, Jan.
20 - 23 in 2015.

7. Awards
Takeshi Inoue received a 2014 Research Encouragement
Award of the Astronomical Society of Japan. Akimasa Kataoka
was awarded the President’s Prize and Nagakura Research
Encouragement Prize of The Graduate University of Advanced
Studies. Seiji Zenitani was elected an Excellent Reviewerof 2014 for the Journal of Earth, Planets and Science (EPS)of the Society of Geomagnetism and Earth Planetary andSpace Sciences. A journal paper written by Toshio Suzuki and
Toshitaka Kajino 2013, J. Phys. G40, 083101 was selected as ahighlight of 2013.

8. Main Visitors from Overseas
The Division of Theoretical Astronomy strives to fulfill its
roles as a center of excellence in Japan for theoretical studies
in astronomy and astrophysics, and also as an international

124

II Status Reports of Research Activities

research institution by providing an excellent research
environment. It engages in various joint research projects withvisiting researchers from overseas, with the help of Grants-inAid for Scientific Research, government subsidies for operating
expenses, the NAOJ budget for guest visitors, and others. The
main international visitors of FY 2014 to the division are listed
below:
Akif B. Balantekin, (University of Wisconsin–Madison, US)
Myung-Ki Cheoun, (Soongsil University, South Korea)
Cemsinan Deliduman, (Mimar Sinan Fine Arts University,
Turkey)Yamac Deliduman, (Mimar Sinan Fine Arts University, Turkey)
Kyungsik Kim, (Korea Aerospace University, Republic ofKorea)
Motohiko Kusakabe, (Korea Aerospace University, Republic ofKorea)Man Hoi Lee, (University of Hong Kong, China)
Grant J. Mathews, (University of Notre Dame, USA)
Steven Rieder, (University of Groningen, Netherland)
Chung-Yoel Ryu, (Hanyang University, South Korea)
Edwin L. Turner, (Princeton University, USA)
Toshiya Ueta, (University of Denver, USA)
Ghil-Seok Yang, (Hangyang University, Republic of Korea)

23. Office of International Relations
The Office of International Relations strives in promoting
autonomous research activities by planning and implementing
strategies for NAOJ’s international research efforts characteristic
to the institution as a whole. It also supports efforts to strengthen
the foundation for expanded internationalization.
The office’s main activities include supporting international
collaborative projects; liaising with overseas astronomical
research organizations; gathering and providing information oninternational activities; offering support for hosting international
conferences, workshops, and seminars; providing support for
visiting international researchers and students; and assisting
Japanese universities and research organizations for international
partnerships.

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. The office gathers and accumulates
necessary and practical information for arranging agreements
and contracts with overseas universities or research institutions,
including precautions and problem solving, by means ofconducting consultations or investigations on individual casesand provides such information as required. The Office ofInternational Relations also offers advice and consultations,and responds to inquiries on a case-by-case basis. Other
matters handled by the office include signing agreements andmemoranda for international collaborations and addressing
export security control issues in relation to overseas joint
research projects.

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 August 17, 2014 at Daejeon, Korea.
The four institutions forming EACOA are NAOC (China),
KASI (Korea), ASIAA (Taiwan), and NAOJ (Japan). The officealso issued a public call for the EACOA postdoctoral fellowship
program for 2015. In addition, it presented NAOJ’s projects
and research results by displaying an exhibit at the IAU AsiaPacific Regional Meeting held on August 18 – 22 at Deajeon,
Korea. Furthermore, the office supported the activities of the
IAU Office for Public Outreach. The Office of International
Relations also cooperated with EACOA member organizations
in supporting the activities of the IAU Office for Astronomy
Development (OAD) in the East Asia region.

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 toinquiries regarding administrative issues. The office also offers
advice to organizations or individuals for contact as appropriate,
coordinating between organizations and gathering relevant
information.

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.
This involved consultation on visa applications and otherprocedures as well as general issues in relation to their stays inJapan to help ensure a pleasant experience. The office started
to run a new support service called “Support Desk” providing
general information useful for everyday activities. Japanese
language lessons for newly arrived non-Japanese speaking staff
members and students were also conducted.

5. Assistance in International Partnerships
Involving Japanese Research Organizations
The Office of International Relations helps 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. The collaboration with the Office of International
Relations at NINS yielded a workshop for international joint
research associates in which the office was involved from theplanning stages to the preparation of a manual for hosting
international researchers and in giving English-language masterseminars to various NINS organizations.

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125

III Organization
1. Organization

Projects(C Projects)

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

Nobeyama Solar Radio Observatory
Mizusawa VLBI Observatory
Solar Observatory
NAOJ Chile Observatory
Center for Computational Astrophysics

Director General

Hinode Science Center
Vice-Director General (on General Affairs)(B Projects)

Gravitational Wave Project OfficeVice-Director General (on Finance)
Director of Engineering
Director of Research Coordination

TMT Project Office(A Projects)

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

126

III Organization

2. Number of Staff Members(2015/3/31)
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
158
29
0
36
11
62
0
20
37
55
8
63
79
148

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

Hayashi, Masahiko
Watanabe, Junichi
Kobayashi, Hideyuki
Takami, Hideki
Gouda, Naoteru

III Organization

1274. Research Departments
Projects
C Projects

Subaru Telescope
Director
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Engineer
Specially Appointed
Research Staff
Postdoctoral Fellow
Research Expert
Research Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administration Department
ManagerManager
General Affairs Section
Chief

128

III Organization

Arimoto, Nobuo
Arimoto, Nobuo
Iye, Masanori
Mizumoto, Yoshihiko
Ohashi, Nagayoshi
Usuda, Tomonori
Aoki, Wakou
Hayashi, Saeko
Ichikawa, Shin-ichi
Iwata, Ikuru
Kashikawa, Nobunari
Kodama, Tadayuki
Nomaru, Junichi
Takato, Naruhisa
Takeda, Yoichi
Terada, Hiroshi
Yutani, Masami
Hayano, Yutaka
Imanishi, Masatoshi
Komiyama, Yutaka
Minowa, Yosuke
Okita, Hirofumi
Pyo, Tae-soo
Shirasaki, Yuji
Yagi, Masafumi
Tazawa, Seiichi
Kurakami, Tomio
Namikawa, Kazuhito
Negishi, Satoru
Omata, Koji
Tamura, Tomonori
Sato, Tatsuhiro
Tadaki Kenichi
Yabe, Kiyoto
Yamanoi, Hitomi
Schramm, Malte
Kuwata, Hitomi
Mochinaga, Chizuru
Noguchi, Masumi
Takamoto, Masami
Yamada, Narumi
Yoshida, Chie
Kobayashi, Hideki
Seto, Yoji
Kobayashi, Hideki

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

Seto, Yoji
Sugawara, Satoshi
Furuhata, Tomoyuki
Alpiche, Dex
Aoki, Kentaro
Aso, Yusuke
Balbarino, Michael
Berghuis, Jennie
Bergstrom, Andrew(Will)
Birchall, DanielCastro, Timothy
Clergeon, Christophe
Cook, David
Currie, Thayne
Doi, Yoshiyuki
Doughty, Danielle
Elms, BrianEndo, Banri
Fabricius, Maximilian
Ferre, Mateu Anna
Ferreira, James
Finet, Francois
Formanek, Keiko
Frayser, Suzanne
Fujiwara, Hideaki
Fujiyoshi, Takuya
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
Kudo, Tomoyuki
Kyono, Eiji
Lemmen, Michael
Leonard, Alex
Letawsky, Michael
Lozi, Julien
Micheva, Genoveva

RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
Hyper Suprime-Cam
Director
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Chief Engineer
Chief Engineer
Postdoctoral Fellow
Research Expert
Research Expert
Research Expert
Research Expert
Administrative Supporter

Morris, Marita
Murai, Rieko
Nabeshima, Yoshitake
Nakano, Wakako
Nakata, Fumiaki
Niimi, Yuka
Nishimura, Tetsuro
Ono, Yoshito
Otsuka, Masaaki
Otsuki, Noriko
Oya, Makoto
Park, Hong Soo
Pathak, Prashant
Ramos, LucioRoth, Noriko
Saito, Yuriko
Shimakawa, Rythm
Shubert, Kiaina
Singh, Garima
Spencer, Robin
Sur, Ryoko
Tait, Philip
Tajitsu, Akito
Takiura, Koki
Tamae, Richard
Tanaka, Makoto
Tanaka, Yoko
Terai, Tsuyoshi
Thunell, Johnathan
Tomono, Daigo
Toyofuku, Ralph
Tsang, Emiko
Wages, Keith
Walawender, Joshua
Weber, Mark
Williams, Joshua
Winegar, Tom
Wung, Matthew
Yamazaki, Kohei
Yeh, Sherry (Chia-Chen)
Miyazaki, Satoshi
Takata, Tadafumi
Furusawa, Hisanori
Komiyama, Yutaka
Nakaya, Hidehiko
Tanaka, Masayuki
Kamata, Yukiko
Uraguchi, Fumihiro
Okura, Yuki
Kawanomoto, Satoshi
Koike, Michitaro
Mineo, Sogo
Yamada, Yoshihiko
Uekiyo, Hatsue

Okayama Astrophysical Observatory
Director
Izumiura, Hideyuki
Associate Professor
Izumiura, Hideyuki
Associate Professor
Ukita, Nobuharu
Chief Research Engineer Koyano, Hisashi
Assistant Professor
Yanagisawa, Kenshi
Specially Appointed
Kambe, Eiji
Assistant Professor
Engineer
Tsutsui, Hironori
Postdoctoral Fellow
Fukui, Akihiko
Research Expert
Kuroda, Daisuke
Research Expert
Maehara, Hiroyuki
Research Supporter
Kamiya, Koki
Research Supporter
Shimizu, Yasuhiro
Research Supporter
Toda, Hiroyuki
Administration Office
Administration Section
Chief
Setou, Nobuyoshi
Administrative Supporter Katayama, Kumiko
Administrative Supporter Shibukawa, Hiroko
Administrative Supporter Yamashita, Ayako
Administrative
Koyama, Shoji
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
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Senior Engineer
Chief Engineer
Chief Engineer
EngineerEngineer
Postdoctoral Fellow
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Technical Expert
Research Supporter

Watanabe, Noriaki

Saito, Masao
Nakamura, Fumitaka
Saito, Masao
Iwashita, Hiroyuki
Kanzawa, Tomio
Ishizuki, Sumio
Oshima, Tai
Takano, ShuroUmemoto, Tomofumi
Minamidani, Tetsuhiro
Mikoshiba, Hiroshi
Miyazawa, KazuhikoHanda, Kazuyuki
Miyazawa, Chieko
Nishitani, Hiroyuki
Wada, Takuya
Morokuma, Kana
Nishimura, Atsushi
Takekoshi, Tatsuya
Kinugasa, Kenzo
Maekawa, JunOya, Masaaki
Takahashi, Shigeru
Tatamitani, Yoshio
Nishioka, Makiko
Arai, Hitoshi

III Organization

129

Administrative Supporter Hatakeyama, Eiko
Administrative Supporter Ide, Hidemi
Consultant
Naito, AkihikoConsultant
Saito, Yasufumi
Research Assistant Staff Mizuno, Izumi
Administration Office
Deputy Manager
Otsuka, Tomoyoshi
General Affairs Section
Chief
Otsuka, Tomoyoshi
Administrative Supporter Kikuchi, Kikue
Administrative Supporter Yoda, Chizuko
Administrative
Fuji, Shigeru
Maintenance Staff

Sato, Katsuhisa
Hagiwara, Yoshiaki
Hirota, Tomoya
Jike, Takaaki
Kameya, Osamu
Kono, Yusuke
Sunada, Kazuyoshi
Tamura, Yoshiaki
Asari, Kazuyoshi
Fukushima, Hideo
Ishikawa, Toshiaki
Oshima, Norio
Suzuki, Shunsaku
Shizugami, Makoto
Ueno, Yuji
Matsumoto, Naoko
Sawada, Satoko

Administrative
Maintenance Staff

Ide, Hiroko

Administrative
Maintenance Staff

Kadoshima, Junko

Administrative
Maintenance Staff

Kikuchi, Michiko

Administrative
Maintenance Staff

Kikuchi, Tsuyoshi

Specially Appointed
Research Staff

Nagayama, Takumi

Administrative
Maintenance Staff

Koike, Ikuko

Specially Appointed
Research Staff

Tazaki, Fumie

Administrative
Maintenance Staff

Kurane, Tsugeru

Specially Appointed
Research Staff

Wu, Yuanwei

Administrative
Maintenance Staff

Saito, Arayo

Administrative
Maintenance Staff

Tsuchiya, Junko

Administrative
Maintenance Staff
Accounting Section
Chief
Chief
Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter

Yoshizawa, Usaji
Sasaki, Hiroaki
Shimizu, Hidetoshi
Kobayashi, Kazuhito
Kodaira, Toshiko
Takasawa, Mitsue
Tokui, Chisato

Nobeyama Solar Radio Observatory
Director
Hanaoka, Yoichiro
Professor
Shibasaki, Kiyoto
Chief Research Engineer Kawashima, Susumu
Assistant Professor
Shimojo, Masumi
Senior Engineer
Shinohara, Noriyuki
Postdoctoral Fellow
Iwai, Kazumasa
Administrative Supporter Shinkai, Hisako
Administrative Supporter Takemura, Miwako
Mizusawa VLBI Observatory
Acting Director
Professor
Professor
Associate Professor
Associate Professor
Associate Professor

130

Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
EngineerEngineer
Postdoctoral Fellow
Postdoctoral Fellow
Specially Appointed
Research Staff

III Organization

Takami, Hideki
Honma, Mareki
Kobayashi, Hideyuki
Agata, HidehikoHanada, Hideo
Shibata, Katsunori

Kim, Jeoung Sook

Specially Appointed
Miura, Mitsuo
Senior Specialist
Research Expert
Hanayama, Hidekazu
Research Expert
Kanaguchi, Masahiro
Research Expert
Oyama, Tomoaki
Technical Expert
Funayama, Hiroshi
Technical Expert
Kuji, Seisuke
Technical Expert
Miyaji, Takeshi
Administrative Expert
Oikawa, Shinichi
Research Supporter
Asakura, Yu
Research Supporter
Isono, Yoko
Research Supporter
Matsukawa, Yuki
Research Supporter
Yamashita, Kazuyoshi
Research Supporter
Yamauchi, Aya
Administrative Supporter Komori, Akiyo
Administrative Supporter Yoshihara, Keiko
Administration Office
Deputy Manager
Hommyo, Susumu
General Affairs Section
Chief
Hommyo, Susumu
Staff
Iida, Naoto
Administrative Supporter Kikuchi, Sachiko
Administrative Supporter Oizumi, Yuka
Administrative Supporter Sasaki, Mie
Accounting Section
Chief
Koseki, Tatsuya
Administrative Supporter Sasaki, Mie
Administrative Supporter Takahashi, Yumi
Ishigakijima Astronomical Observatory
Head
Miyaji, Takeshi
Associate Professor
Agata, Hidehiko

Research Engineer
Research Engineer
Research Expert
Technical Expert
Time Keeping Office
Head
Research Engineer
Solar Observatory
Director
Professor
Professor
Associate Professor
Associate Professor
Chief Engineer
Postdoctoral Fellow
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
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor

Fukushima, Hideo
Oshima, Norio
Hanayama, Hidekazu
Miyaji, Takeshi
Sato, Katsuhisa
Asari, Kazuyoshi

Hanaoka, Yoichiro
Sakurai, Takashi
Shibasaki, Kiyoto
Hanaoka, Yoichiro
Suematsu, Yoshinori
Shinoda, Kazuya
Otsuji, Kenichi
Kitagawa, Naomasa
Morita, Satoshi
Yaji, Kentaro
Nishino, Hideko
Sugimoto, Junko

Hasegawa, Tetsuo
Hasegawa, Tetsuo
Iguchi, Satoru
Kameno, Seiji
Ogasawara, Ryusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Asayama, Shinichiro
Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Mizuno, Norikazu
Ohishi, Masatoshi
Okuda, Takeshi

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

Oshima, Tai
Sawada, Tsuyoshi
Shimojo, Masumi
Sugimoto, Masahiro
Takahashi, Satoko
Umemoto, Tomofumi
Akiyama, Eiji

Specially Appointed
Assistant Professor

Chibueze, James Okwe

Specially Appointed
Assistant Professor

Erik, Muller

Specially Appointed
Assistant Professor

Hatsukade, Bunyo

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

Saigo, Kazuya
Ashitagawa, Kyoko
Nakazato, Takeshi
Kobiki, ToshihikoNakamura, Kyoko
Kato, Yoshihiro
Ao, Yiping

Specially Appointed
Research Staff

Herrera Contreras,
Cinthya Natalia

Specially Appointed
Research Staff

Kurono, YasutakaSpecially Appointed
Research Staff

Miura, Rie

Specially Appointed
Research Staff

Sanhueza Nunez,
Patricio Andres

Specially Appointed
Research Staff

Ueda, Junko

Specially Appointed
Senior Specialist

Fukui, Hideharu

Specially Appointed
Senior Specialist

Kawasaki, Wataru

Kawamura, Akiko

Specially Appointed
Senior Specialist

Kobayashi, Tsuyoshi

Specially Appointed
Associate Professor

Komugi, Shinya

Specially Appointed
Senior Specialist

Kuniyoshi, Masaya

Specially Appointed
Associate Professor

Nagai, Hiroshi

Specially Appointed
Senior Specialist

Matsui, Takayuki

Shinnaga, Hiroko

Specially Appointed
Senior Specialist

Morita, Eisuke

Specially Appointed
Senior Specialist

Saito, Motoi

Specially Appointed
Senior Specialist

Shimoda, Takanobu

Specially Appointed
Senior Specialist

So, Ryoken

Specially Appointed
Senior Specialist

Sugimoto, Kanako

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

Kawashima, Susumu
Kikuchi, Kenichi
Watanabe, Manabu
Espada Fernandez,
DanielEzawa, Hajime
Hiramatsu, Masaaki
Hirota, Akihiko
Kamazaki, Takeshi
Matsuda, Yuichi
Nakanishi, Kouichiro

Specially Appointed
Senior Specialist
Research Expert

Yamada, Masumi
Fujimoto, Yasuhiro

III Organization

131

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

Inoe, Norio
Ishimaru, Fumiaki
Kawakami, Shinnosuke
Nakamura, Koji
Noma, Naoko
Nukatani, Sorahiko
Sakuma, Naoko
Shibuya, Masaru
Tomimuro, Hisashi
Yasui, Takashi
Kamada, Masako
Kusuno, Kozue
Uchida, Ayako
Yamazaki, Toshitaka
Kono, Izumi
Matsunaga, Choko
Saito, Naoko
Sakurai, Junko
Uchida, Rena
Onishi, Kyoko
Gabriela Krapivka
FloresJoaquin Collao
Lorena Toro
Maria Angelica Ramos
Nicolas Silva
Oscar Mendez
Veronica Gareca
Yamaguchi, Takahiro
Tsukano, Satomi
Yamaguchi, Takahiro
Hiramatsu, Naoya

Center for Computational Astrophysics
Director
Kokubo, Eiichiro
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kohji
Assistant Professor
Inoe, Tsuyoshi
Assistant Professor
Ito, Takashi
Assistant Professor
Kudo, Takahiro
Assistant Professor
Ohsuga, Ken
Assistant Professor
Tanaka, Masaomi
Specially Appointed
Takahashi, Hiroyuki
Assistant Professor

Hinode Science Center
Director
Professor
Professor
Specially Appointed
Professor
Specially Appointed
Professor
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Specially Appointed
Research Staff
Technical Expert
Research Supporter

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

Watanabe, Tetsuya
Sakurai, Takashi
Shibasaki, Kiyoto
Kuhn, Jeffrey Richard
Uitenbroek, Han
Hara, Hirohisa
Sekii, Takashi
Suematsu, Yoshinori
Ishikawa, Ryoko
Kano, Ryohei
Katsukawa, Yukio
Kubo, Masahito
Shimojo, Masumi
Bando, Takamasa
Antolin, Patrick
Inoe, Naoko
Nakada, Yuichiro

B Projects

Gravitational Wave Project OfficeDirector
Flaminio, RaffaeleSpecially Appointed
Flaminio, Raffaele
Professor
Associate Professor
Aso, Yoichi
Affiliated AssociateAndo, Masaki
Professor
Specially Appointed
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Chief Engineer
Specially Appointed
Research Staff

Barsuglia, Matteo
Akutsu, Tomotada
Takahashi, Ryutaro
Tatsumi, Daisuke
Ueda, Akitoshi
Ishizaki, Hideharu
Torii, Yasuo
Tanaka, Nobuyuki

Specially Appointed
Assistant Professor

Takiwaki, Tomoya

Specially Appointed
Research Staff

Furusawa, ShunSpecially Appointed
Research Staff

Pena Arellano, Fabian
ErasmoKawashima, Tomohisa

Specially Appointed
Research Staff

Zeidler, Simon

Ishitsu, Naoki
Kato, TsunehikoNakayama, HirotakaSpecially Appointed
Senior Specialist
Research Supporter

Specially Appointed
Research Staff
Postdoctoral Fellow
Research Expert
Research Expert

132

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

III Organization

Barton, Mark Andrew

Hirata, Naoatsu
Nakamura, Koji

Administrative Supporter Kondo, Mihoko
Administrative Supporter Yoshizumi, Mizuho
Secondment (to The University of Tokyo)
Assistant Professor
Oishi, Naoko
TMT Project OfficeDirector
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Postdoctoral Fellow
Postdoctoral Fellow
Specially Appointed
Research Staff

Usuda, Tomonori
Iye, Masanori
Takami, Hideki
Usuda, Tomonori
Yamashita, Takuya
Aoki, Wakou
Kashikawa, Nobunari
Kodama, Tadayuki
Kosugi, George
Miyazaki, Satoshi
Takato, Naruhisa
Terada, Hiroshi
Packham, Christopher
CharlesMiyashita, Takaaki
Hayano, Yutaka
Imanishi, Masatoshi
Sugimoto, Masahiro
Suzuki, Ryuji
Yagi, Masafumi
Hashimoto, Tetsuya
Wanajo, Shinya
Harakawa, Hiroki

Specially Appointed
Senior Specialist

Chapman, Junko

Specially Appointed
Senior Specialist

Kozu, Akihito

Specially Appointed
Senior Specialist
Research Expert
Research Expert
Research Supporter
Research Supporter
Public Outreach Official
Administrative Supporter
Administrative Supporter

Sugiyama, Motokuni
Ishii, Miki
Ozaki, Shinobu
Inatani, Junji
Rusu, Cristian Eduard
Tajima, Toshiyuki
Haranaka, Miyuki
Yamaguchi, Chiyu

A Projects

JASMINE Project OfficeDirector
Professor
Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Chief Research Engineer

Gouda, Naoteru
Gouda, Naoteru
Kobayashi, Yukiyasu
Hanada, Hideo
Takato, Naruhisa
Araki, Hiroshi
Noda, Hirotomo
Tsujimoto, Takuji
Yano, Taihei
Tsuruta, Seiitsu

Research Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Research Supporter
Technical Supporter

Asari, Kazuyoshi
Shirahata, Mai
Yamaguchi, Masaki
Utsunomiya, Shin
Kashima, Shingo

Extrasolar Planet Detection Project OfficeDirector
Tamura, Motohide
Professor
Kokubo, Eiichiro
Affiliated Professor
Tamura, Motohide
Specially Appointed
Ojha, Devendra Kumar
Professor
Associate Professor
Izumiura, Hideyuki
Assistant Professor
Kotani, Takayuki
Assistant Professor
Morino, Junichi
Assistant Professor
Nakajima, Tadashi
Assistant Professor
Nishikawa, Jun
Assistant Professor
Suto, Hiroshi
Specially Appointed
Narita, Norio
Assistant Professor
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Research Expert
Research Supporter
Research Assistant Staff
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
Postdoctoral Fellow
Specially Appointed
Research Staff

Kandori, Ryo
Omiya, Masashi
Kusakabe, Nobuhiko
Kurokawa, Takashi
Oya, Masato

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

Research Expert
Kikuchi, Fuyuhiko
Administrative Supporter Sato, Sayaka
SOLAR-C Project OfficeDirector
Professor
Professor

Hara, Hirohisa
Sakurai, Takashi
Watanabe, Tetsuya

III Organization

133

Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Senior Engineer
Chief Engineer
Specially Appointed
Research Staff
Technical Expert
Administrative Supporter

Hara, Hirohisa
Suematsu, Yoshinori
Ishikawa, Ryoko
Kano, Ryohei
Katsukawa, Yukio
Kubo, Masahito
Bando, Takamasa
Kobiki, Toshihiko
Shinoda, Kazuya
Narukage, Noriyuki
Inoe, Naoko
Fujiyoshi, Marie

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

134

Ohishi, Masatoshi
Kokubo, Eiichiro
Mizumoto, Yoshihiko
Ichikawa, Shin-ichi
Kosugi, George
Nomaru, Junichi
Ohishi, Masatoshi
Shibata, Katsunori
Takata, Tadafumi
Furusawa, Hisanori
Ito, Takashi
Kano, Ryohei
Oe, Masafumi
Shimojo, Masumi
Shirasaki, Yuji
Takano, ShuroInoe, Goki
Fukui, Asami
Higuchi, Yuichi

Specially Appointed
Research Staff

Kawaguchi, Toshihiro

Specially Appointed
Research Staff

Yoshida, Tessei

Specially Appointed
Research Staff
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Supporter
Research Supporter
Administrative Supporter
Administrative Supporter
Research Assistant Staff

Zapart, Christopher
AndrewAbe, Miki
Asano, Eiji
Furusawa, Junko
Isogai, Mizuki
Nakajima, Kimihiko
Nakane, Makiko
Tanaka, Nobuhiro
Fujikawa, Makiko
Noda, Sachiyo
Aida, Kanako
Ishii, Yuko
Suzuki, Taiki

III OrganizationJVO Project
Head
Associate Professor
Assistant Professor

Mizumoto, Yoshihiko
Ohishi, Masatoshi
Shirasaki, Yuji

Advanced Technology Center
Director
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor

Noguchi, Takashi
Noguchi, Takashi
Takami, HidekiHara, Hirohisa
Iwata, Ikuru
Matsuo, Hiroshi
Miyazaki, Satoshi
Sekimoto, Yutaro
Okada, Norio
Akutsu, Tomotada
Kano, Ryohei
Kojima, Takafumi
Nakaya, HidehikoSuzuki, Ryuji
Gonzalez Garcia,
AlvaroResearch Engineer
Research Engineer
Research Engineer
Research Engineer
Research 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
Chief Engineer
Chief Engineer
Postdoctoral Fellow
EngineerEngineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert
Research Expert

Fujii, Yasunori
Fukushima, Mitsuhiro
Iizuka, Yoshizo
Noguchi, Motokazu
Sato, Naohisa
Kubo, Koichi
Takahashi, Toshikazu
Fukuda, Takeo
Ikenoue, Bungo
Inata, Motoko
Ito, Tetsuya
Iwashita, Hikaru
Kamata, Yukiko
Kaneko, Keiko
Miyazawa, Chieko
Obuchi, Yoshiyuki
Tamura, Tomonori
Uraguchi, Fumihiro
Waseda, Koichi
Karatsu, Kenichi
Mitsui, Kenji
Tsuzuki, Toshihiro
Dominjon, Agnes
Micheline
Narukage, Noriyuki
Furutani, Akio
Iwakuni, Mikio
Kamada, Chiyoshi
Karatsu, Miki
Konuma, Mika
Matthias, Kroug
Saito, Sakae
Soga, TomioResearch Expert
Research Expert
Technical Supporter
Technical Supporter
Technical Expert
Technical Expert
Administrative Supporter
Administrative Supporter
Administrative Supporter
Public Relations Center
Director
Professor
Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Chief Senior Engineer
Engineer
Chief
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Research Expert
Research Expert
Research Expert
Research Expert
Research 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
Public Outreach Official

Takahashi, Yasuo
Uemizu, Kazunori
Hayashi, Ritsuko
Kano, Mitchell Senei
Kumagai, Kazuyoshi
Nishino, Tetsuo
Kuroda, Kyoko
Murakami, Hiromi
Yoshida, Taeko

Fukushima, Toshio
Fukushima, Toshio
Watanabe, Junichi
Agata, Hidehiko
Hiramatsu, Masaaki
Ikuta, ChisatoSoma, Mitsuru
Fukushima, Hideo
Katayama, Masato
Oshima, Norio
Sasaki, Goro
Matsuda, Kou
Nagayama, Syogo
Hori, Mayumi
Cheung, Sze-Leung
Lundock, Ramsey Guy
Komiyama, Hiroko
Ono, Tomoko
Takata, Hiroyuki
Usuda-Sato, Kumiko
Kume, KaoriBaba, Yukie
Endoh, Isao
Fujita, Tokiko
Futami, Hiroshi
Hatano, Satomi
Ishikawa, Naomi
Ishizaki, Masaharu
Itoh, Shoichi
Iwashiro, Kuninori
Koike, Akio
Kubo, Maki
Masuzawa, Hitoshi
Mikami, Naotsugu
Naito, Seiichiro
Natsugari, Satomi
Nemoto, Shiomi
Oguri, Junko
Ohgoe, Osamu
Shibata, Yukiko
Shioya, Yasuhisa
Takeda, Takaaki
Udzumaki, Tatsuya

Public Outreach Official
Administrative Supporter
Administrative Supporter
Public Relations Office
Head (2014 Dec.1-)
Head (-2014 Nov.30)
Engineer
Specially Appointed
Senior Specialist
Research Expert
Research Expert
Research Supporter
Public Outreach Official
Public Outreach Official
Public Outreach Official
Outreach and Education Office
HeadPublic 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
Museum Deliberation Office
Head
Associate Professor
Research Engineer
Chief Senior Engineer
Research Expert
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Public Outreach Official
Ephemeris Computation Office
Head
Chief Senior Engineer
Public Outreach Official
Library
Chief
Public Outreach Official
Public Outreach Official
Publications Office
HeadVice-Head
Research Expert
Public Outreach Official
Public Outreach Official

Watanabe, Yuriko
Aoki, Makiko
Noguchi, Sayumi
Hiramatsu, Masaaki
Ikuta, Chisato
Nagayama, Syogo
Lundock, Ramsey Guy
Komiyama, Hiroko
Ono, Tomoko
Kume, Kaori
Mikami, Naotsugu
Natsugari, Satomi
Shioya, Yasuhisa
Agata, Hidehiko
Fujita, Tokiko
Hatano, Satomi
Ishikawa, Naomi
Ishizaki, Masaharu
Itoh, Shoichi
Masuzawa, Hitoshi
Naito, Seiichiro
Ohgoe, Osamu
Shibata, Yukiko
Udzumaki, Tatsuya
Oshima, Norio
Agata, Hidehiko
Sasaki, Goro
Matsuda, Kou
Usuda-Sato, KumikoBaba, Yukie
Endoh, Isao
Fujita, Tokiko
Futami, Hiroshi
Koike, Akio
Nemoto, Shiomi
Takeda, Takaaki
Watanabe, Yuriko
Katayama, Masato
Matsuda, Kou
Endoh, Isao
Hori, Mayumi
Kubo, Maki
Oguri, Junko
Fukushima, Toshio
Fukushima, Hideo
Takata, Hiroyuki
Iwashiro, Kuninori
Kubo, Maki

III Organization

135

Office for Astronomy Outreach of the IAU
HeadAgata, HidehikoSpecially Appointed
Cheung, Sze-Leung
Senior Specialist
Public Outreach Official Shibata, Yukiko
General Affairs Office
Head
Matsuda, Kou
Administrative Supporter Aoki, Makiko
Administrative Supporter Noguchi, Sayumi

Divisions
Division of Optical and Infrared Astronomy
Director
Mizumoto, Yoshihiko
Professor
Arimoto, Nobuo
Professor
Gouda, Naoteru
Professor
Iye, Masanori
Professor
Kobayashi, Yukiyasu
Professor
Mizumoto, Yoshihiko
Professor
Ohashi, Nagayoshi
Professor
Sekiguchi, Kazuhiro
Professor
Usuda, Tomonori
Professor
Yamashita, Takuya
Associate Professor
Aoki, Wakou
Associate Professor
Aso, Yoichi
Associate Professor
Hayashi, Saeko
Associate Professor
Iwata, Ikuru
Associate Professor
Izumiura, Hideyuki
Associate Professor
Kashikawa, Nobunari
Associate Professor
Kodama, Tadayuki
Associate Professor
Nomaru, Junichi
Associate Professor
Sasaki, Toshiyuki
Associate Professor
Takato, Naruhisa
Associate Professor
Takeda, Yoichi
Associate Professor
Terada, Hiroshi
Associate Professor
Ukita, Nobuharu
Chief Research Engineer Koyano, Hisashi
Chief Research Engineer Miyashita, Takaaki
Chief Research Engineer Yutani, Masami
Assistant Professor
Akutsu, Tomotada
Assistant Professor
Hayano, Yutaka
Assistant Professor
Imanishi, Masatoshi
Assistant Professor
Komiyama, Yutaka
Assistant Professor
Kotani, Takayuki
Assistant Professor
Minowa, Yosuke
Assistant Professor
Morino, Junichi
Assistant Professor
Nakajima, Tadashi
Assistant Professor
Nishikawa, Jun
Assistant Professor
Okita, Hirofumi
Assistant Professor
Pyo, Tae-soo
Assistant Professor
Soma, Mitsuru
Assistant Professor
Suto, Hiroshi
Assistant Professor
Takahashi, Ryutaro
Assistant Professor
Tatsumi, Daisuke
Assistant Professor
Tomono, Daigo

136

III Organization

Assistant Professor
Tsujimoto, Takuji
Assistant Professor
Ueda, Akitoshi
Assistant Professor
Yagi, Masafumi
Assistant Professor
Yanagisawa, Kenshi
Assistant Professor
Yano, Taihei
Specially Appointed
Matsuoka, Yoshiki
Assistant Professor
Research Engineer
Ishizaki, Hideharu
Research Engineer
Tazawa, Seiichi
Research Engineer
Torii, Yasuo
Chief Engineer
Kurakami, Tomio
Chief Engineer
Namikawa, Kazuhito
Chief Engineer
Negishi, Satoru
Chief Engineer
Omata, Koji
Chief Engineer
Tamura, Tomonori
Chief Engineer
Tanaka, Nobuyuki
Engineer
Sato, Tatsuhiro
Engineer
Tsutsui, Hironori
Administrative Supporter Kimura, Hiroko
Research Assistant Staff Toshikawa, Jun
Secondment (to The University of Tokyo)
Assistant Professor
Ohishi, Naoko
Division of Radio Astronomy
Director
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor

Iguchi, Satoru
Hasegawa, Tetsuo
Honma, Mareki
Iguchi, Satoru
Kameno, Seiji
Kawabe, Ryohei
Kobayashi, Hideyuki
Namiki, Noriyuki
Ogasawara, Ryusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Asayama, Shinichiro
Hanada, Hideo
Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Matsumoto, Koji
Mizuno, Norikazu
Okuda, Takeshi
Saito, Masao
Shibata, Katsunori
Iwashita, Hiroyuki
Kanzawa, Tomio
Kawashima, Susumu
Kikuchi, Kenichi
Sato, Katsuhisa
Tsuruta, Seiitsu
Watanabe, Manabu
Araki, Hiroshi
Espada Fernandez,
DanielEzawa, Hajime

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
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
Chief Engineer
EngineerEngineerEngineerEngineer
Research Expert
Research Supporter

Hagiwara, Yoshiaki
Hiramatsu, Masaaki
Hirota, Akihiko
Hirota, Tomoya
Ishizuki, Sumio
Jike, Takaaki
Kamazaki, Takeshi
Kameya, Osamu
Kono, Yusuke
Matsuda, Yuichi
Miyoshi, Makoto
Nakanishi, KouichiroNoda, Hirotomo
Oshima, Tai
Sawada, Tsuyoshi
Sugimoto, Masahiro
Sunada, Kazuyoshi
Takahashi, Satoko
Takano, Shuro
Tamura, Yoshiaki
Umemoto, Tomofumi
Asari, Kazuyoshi
Ashitagawa, Kyoko
Ishikawa, Toshiaki
Mikoshiba, Hiroshi
Nakazato, Takeshi
Suzuki, Shunsaku
Kobiki, Toshihiko
Miyazawa, KazuhikoNakamura, Kyoko
Handa, Kazuyuki
Kato, Yoshihiro
Miyazawa, Chieko
Nishitani, Hiroyuki
Shizugami, Makoto
Ueno, Yuji
Wada, Takuya
Tatsuzawa, Kaichi
Okayasu, Rikako

Research Engineer
Senior Engineer
Chief Engineer

Bando, Takamasa
Shinohara, Noriyuki
Shinoda, Kazuya

Division of Theoretical Astronomy
Director
Tomisaka, Kohji
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kohji
Professor
Yoshida, Haruo
Specially Appointed
Turner, Edwin Lewis
Professor
Associate Professor
Kajino, Toshitaka
Associate Professor
Nakamura, Fumitaka
Assistant Professor
Hamana, Takashi
Assistant Professor
Inoe, Tsuyoshi
Assistant Professor
Kudo, Takahiro
Assistant Professor
Tanaka, Masaomi
Specially Appointed
Fujii, Michiko
Assistant Professor
Specially Appointed
Assistant Professor

Fujimoto, Keizo

Specially Appointed
Assistant Professor

Nozawa, TakayaSpecially Appointed
Assistant Professor

Sotani, HajimeSpecially Appointed
Assistant Professor
Administrative Supporter
Administrative Supporter
Research Assistant Staff

Zenitani, Seiji
Izumi, Shioko
Kano, Kaori
Kataoka, Akimasa

Division of Solar and Plasma Astrophysics
Director
Sakurai, Takashi
Professor
Sakurai, Takashi
Professor
Shibasaki, Kiyoto
Professor
Watanabe, Tetsuya
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Hara, Hirohisa
Associate Professor
Sekii, Takashi
Associate Professor
Suematsu, Yoshinori
Assistant Professor
Ishikawa, Ryoko
Assistant Professor
Kano, Ryohei
Assistant Professor
Katsukawa, Yukio
Assistant Professor
Kubo, Masahito
Assistant Professor
Shimojo, Masumi
Specially Appointed
Toriumi, Shin
Assistant Professor

III Organization

137

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

Suematsu, Sayaka

Specially Appointed
Yamamiya, Osamu
Senior Specialist
Research Evaluation Support OfficeDirector
Watanabe, Junichi
Specially Appointed
Hori, Kuniko
Senior Specialist
Office of International Relations
Director
Sekiguchi, Kazuhiro
Professor
Sekiguchi, Kazuhiro
Research Expert
Komiyama, Hiroko
Research Expert
Yoshida, Fumi
Administration Office
Deputy Manager/Senior
Onishi, Tomoyuki
Specialist
International Academic Affairs Section
Chief
Kikkawa, Hiroko
Administrative Supporter Ito, Yoshihisa
Administrative Supporter Momma, Yoko
Human Resources Planning OfficeDirector
Yamamiya, Osamu
Specially Appointed
Suematsu, Sayaka
Senior Specialist
Safety and Health Management OfficeDirector
Takami, Hideki
Specially Appointed
Ota, Masahiko
Senior Specialist
Technical Expert
Kashiwagi, Yuji
Engineering Promotion OfficeDirector
Specially Appointed
Senior Specialist

138

III Organization

Takami, Hideki
Chiba, Kurazo

Administration Department
General Manager
Sasaki, Tsuyoshi
General Affairs Division
Manager
Harada, Eiichiro
Deputy Manager
Onishi, Tomoyuki
Information Technology Specialist
Specialist
Yoshikawa, Ikuko
Personnel Accounting Specialist
Specialist
Kikuchi, Jinichi
General Affairs Section
Chief
Yoshikawa, Ikuko
Staff
Takada, Miyuki
Staff
Yamafuji, Yasuto
Staff
Yoshimura, Tetsuya
Vehicle Driver
Amemiya, Hidemi
Administrative Expert
Murakami, Sachiko
Administrative Expert
Noguchi, Koki
Administrative Supporter Kobayashi, Kayo
Administrative Supporter Odate, Noriko
Administrative Supporter Seki, Kumi
Personnel Section
Chief
Yamanochi, Mika
Staff
Isozaki, Yuka
Staff
Takai, Tetsuya
Payroll Section
Chief
Kikuchi, Jinichi
Staff
Furukawa, Shinichiro
Specially Appointed
Yamamoto, Chieko
Senior Specialist
Administrative Supporter Aiba, Narukazu
Employee Section
Chief
Yamaura, Mari
Staff
Kawashima, Ryota
Research Support Section
Chief
Sato, Yoko
Staff
Matsukura, Koji
Staff
Okubo, Kazuhiko
Administrative Supporter Aka, Shizuno
Administrative Supporter Okuda, Yutaka
Administrative Supporter Takeuchi, Kaori
Administrative Supporter Torii, Makiko
Child Care Leave
Staff
Goto, Michiru
Staff
Ouchi, KaoriFinancial Affairs Division
ManagerNemoto, Nobuyuki
Senior Specialist
Miura, Norio
External Funding Specialist
Specialist
Miura, Susumu
Audit Specialist
Specialist
Yamamoto, Shinichi
Administrative Supporter Amano, Hiroshi
Administrative Supporter Kawano, Chie

Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
General Affairs Section
Chief
Staff
Administrative Supporter
Administrative Supporter
Budget Section
Chief
Staff
Staff
Administrative Supporter
Asset Management Section
Chief
Senior Staff
Purchase Validation Center
Senior Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Accounting Division
Manager
Contract Specialist
Specialist
Accounting Section
Chief
Senior Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Procurement Section
Chief
Staff
Staff
Staff
Administrative Expert
Administrative Supporter
Administrative Supporter
Administrative Supporter
Facilities Division
Manager
Administrative Expert
General Affairs Section
Chief
Staff
Administrative Supporter
Planning Section
Chief
Administrative Supporter

Sato, Chieko
Shioyama, Erika
Urushibata, Kozue
Yasuda, Masako

Maintenance Section
Chief
Staff

Sato, Takashi
Hayashigura, Koji

Miura, Susumu
Mizokawa, Yuko
Kono, Midori
Okada, Kazuko
Fujiwara, Kenichi
Katou, Masahiro
Yokota, Banri
Matsubara, Michiko
Miura, Norio
Sato, Kanako
Sato, Kanako
Nakagomi, Kimitoshi
Nishimura, Misako
Taniai, Tomoko
Tanigaki, Yukio
Hyuga, Tadayuki
Chiba, Yoko
Sukigara, Yuji
Chiba, Satoko
Kobayashi, Rina
Nagasawa, Fumi
Okada, Junko
Chiba, Yoko
Kayamori, Shinji
Sakamoto, Misato
Sugimoto, Naomi
Sato, Masako
Murai, Chikako
Takano, Ayako
Uchida, Shimako
Ono, Kazuo
Asada, Tsuneaki
Yamada, Tomohiro
Nakagawa, Yukie
Hasegawa, Chisato
Murakami, Kazuhiro
Tsukamoto, Izumi

III Organization

1396. Personnel change

140

Research and Academic Staff
Date
Name

Change2014/4/1

Namiki, Noriyuki

Hired2014/4/1

Aso, Yoichi

HiredDivision of Optical and Infrared Astronomy(Gravitational Wave Project Office),
Associate Professor

2014/4/1

Kikuchi, Kenichi

HiredDivision of Radio Astronomy (NAOJ Chile
Observatory), Chief Research Engineer

2014/4/1

Okita, Hirofumi

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

2014/6/1

Ishikawa, Ryoko

Hired

Division of Solar and Plasma Astrophysics(Hinode Science Center, Specially(Hinode Science Center), Assistant Professor Appointed Assistant Professor)

2014/8/1

Sakamoto, Seiichi

HiredDivision of Radio Astronomy (NAOJ Chile
Observatory), Professor

2014/8/1

Kotani, Takayuki

HiredDivision of Optical and Infrared Astronomy(Extrasolar Planet Detection Project Office),
Assistant Professor

2014/11/30

Ikuta, Chisato

Resigned(Japan Aerospace Exploration Agency)

2014/12/31 Tomono, Daigo

Resigned

2015/3/31

Kudoh, Takahiro

Resigned(Nagasaki University)

Division of Theoretical Astronomy,
Assistant Professor

2015/3/31

Hagiwara, Yoshiaki

Resigned(Toyo University)

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

2015/3/31

Takano, Shuro

Resigned(Nihon University)

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

2015/3/31

Fukushima, Hideo

Resigned

Public Relations Center, ResearchEngineer

2015/3/31

Iye, Masanori

RetiredDivision of Optical and Infrared
Astronomy (TMT Project Office),
Professor

2015/3/31

Shibasaki, Kiyoto

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

2015/3/31

Sasaki, Toshiyuki

RetiredDivision of Optical and Infrared
Astronomy, Associate Professor

2015/3/31

Yutani, Masami

Retired2015/3/31

Koyano, Hisashi

Retired2015/3/31

Oshima, NorioContract
ExpiredIII Organization

New Affiliated Institute, Position
Division of Radio Astronomy (RISE
Project), Professor

Previous Affiliated Institute, Position(Chiba Institute of Technology)(The University of Tokyo)(Japan Aerospace Exploration
Agency)Public Relations Center, AssistantProfessor
Division of Optical and Infrared
Astronomy (Subaru Telescope),
Assistant Professor

Division of Optical and Infrared
Astronomy (Subaru Telescope),
Chief Research Engineer
Division of Optical and Infrared
Astronomy (Okayama AstrophysicalObservatory), Chief ResearchEngineer
Public Relations Center, ResearchEngineer2014/10/1

Iwashita, Hiroyuki

Promoted

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

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

2015/3/1

Honma, Mareki

Promoted

Division of Radio Astronomy (Mizusawa
VLBI Observatory), Professor

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

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Engineering Staff
Date

Name

2014/4/1

Sato, Tatsuhiro

Hired

Division of Optical and Infrared Astronomy(Subaru Telescope), Engineer

2015/3/1

Nishitani, Hiroyuki

HiredDivision of Radio Astronomy (Nobeyama
Radio Observatory), Engineer

2014/8/1

Shinohara, Noriyuki

Promoted

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

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

2014/8/1

Kubo, Koichi

Promoted

Advanced Technology Center, SeniorEngineer

Advanced Technology Center ,Chief Engineer

2014/8/1

Kobiki, Toshihiko

Promoted

Division of Radio Astronomy (NAOJ Chile
Observatory), Senior Engineer

Division of Radio Astronomy(NAOJ Chile Observatory), Chief
Engineer

2014/8/1

Takahashi, Toshikazu Promoted

Advanced Technology Center, SeniorEngineer

Advanced Technology Center ,Chief Engineer

2014/8/1

Nakamura, Kyoko

Promoted

Division of Radio Astronomy (NAOJ Chile
Observatory), Senior Engineer

Division of Radio Astronomy(NAOJ Chile Observatory), Chief
Engineer

2014/9/1

Matsuda, Kou

Promoted

Public Relations Center, Chief SeniorEngineer

Public Relations Center, SeniorEngineer

Administrative Staff
Date

Name

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

2014/4/1

Sasaki, Tsuyoshi

HiredAdministration Department, General
Manager(Iwate University)

2014/4/1

Harada, Eiichiro

Hired

Administration Department General Affairs
Division, Manager(National Institutes for the
Humanities)

2014/4/1

Nemoto, Nobuyuki

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

2014/4/1

Sukigara, Yuji

HiredAdministration Department Accounting
Division Accounting Section, Chief(Tokyo Gakugei Univerisity)

2014/4/1

Hayashigura, Koji

HiredAdministration Department Facilities
Division Maintenance Section, Staff(The University of Tokyo)

2014/8/1

Shimizu, Hidetoshi

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

2014/8/1

Isozaki, Yuka

Hired

Administration Department General Affairs
Division Personnel Section, Staff

2014/8/1

Kayamori, Shinji

HiredAdministration Department Accounting
Division Procurement Section, Staff

2015/2/1

Yokota, Banri

Hired

Administration Department Financial
Affairs Division Budget Section, Staff

2015/3/1

Takai, Tetsuya

HiredAdministration Department General Affairs
Division Personnel Section, Staff

III Organization141

2014/7/31

Sasaki, Hiroaki

Resigned(Shinshu University)

Nobeyama Radio Observatory
Administration Office Accounting
Section, Chief

2014/7/31

Kobayashi, Hideki

Resigned(Kochi University)

Subaru Telescope Administration
Department, Administrative
Manager
Administration Department
Financial Affairs Division Budget
Section, Staff

2014/12/15 Kato, Masahiro

Resigned

2015/3/31

Kikuchi, Jinichi

Resigned(The University of Tokyo)

Administration Department
General Affairs Division, Specialist

2015/3/31

Miura, Susumu

Resigned(Tokyo Gakugei Univerisity)

Administration Department
Financial Affairs Division General
Affairs Section, Chief

2015/3/31

Hori, Mayumi

Resigned(The University of Tokyo)

Public Relations Center, Library
Section, Chief

2015/3/31

Okubo, Kazuhiko

Resigned(The Graduate University for Advanced
Studies)

Administration Department
General Affairs Division Research
Support Section, Staff

2015/3/31
2015/3/31

Hyuga, Tadayuki
Ono, Kazuo

RetiredRetired2014/8/1

Seto, Yoji

Promoted

Subaru Telescope Administration
Department, Administrative Manager

Office of International Relations
Administration Office, Chief

2014/8/1

Onishi, Tomoyuki

Promoted

Administration Department General Affairs
Division, Deputy Manager

Administration Department
Accounting Division, Specialist

2014/8/1

Chiba, Yoko

Promoted

Administration Department Accounting
Division Procurement Section, Chief

Administration Department
Accounting Division Procurement
Section, Senior Staff

2014/8/1

Yamamoto, Shinichi

Promoted

Administration Department Financial Affairs
Division, Specialist

NAOJ Chile Observatory
Administration Department
Financial Section, Senior Staff

2014/10/1

Chiba, Satoko

Promoted

Administration Department Accounting
Division Accounting Section, Senior Staff

Administration Department
Accounting Division Accounting
Section, Staff

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

Employee on Annual Salary System

142

Date

Name

2014/4/1

Kawamura, Akiko

Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2014/4/1

Chibueze, James
Okwe

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2014/4/1

Gonzalez Garcia,
AlvaroHired

Advanced Technology Center, Specially
Appointed Assistant Professor

2014/4/1

Toriumi, Shin

Hired

Division of of Solar and Plasma Astrophysics,
Specially Appointed Assistant Professor

2014/4/1

Nozawa, Takaya

HiredDivision of Theoretical Astronomy, Specially
Appointed Assistant Professor

2014/4/1

Tadaki, Kenichi

Hired

Subaru Telescope, Specially Appointed
Research Staff

2014/4/1

Higuchi, Yuichi

Hired

Astronomy Data Center, Specially Appointed
Research Staff

2014/4/1

Zapart, Christopher
Andrew

Hired

Astronomy Data Center, Specially Appointed
Research Staff

III Organization(NAOJ Chile Observatory, Specially
Appointed Research Staff)

2014/4/1

Harakawa, Hiroki

Hired

TMT Project Office, Specially Appointed
Research Staff

2014/4/1

Nishimura, Atsushi

Hired

Nobeyama Radio Observatory, Specially
Appointed Research Staff

2014/4/1

Furusawa, Shun

Hired

Center for Computational Astrophysics,
Specially Appointed Research Staff

2014/4/1

Shirahata, Mai

HiredJASMINE Project Office, Specially
Appointed Research Staff

2014/4/1

Cheung, Sze Leung

Hired

Public Relations Center, Specially Appointed
Senior Specialist

2014/4/1

Shimoda, Takanobu

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/4/1

Kobayashi, Tsuyoshi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/4/1

Morita, Eisuke

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/4/1

Sugimoto, Kanako

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/4/1

Kawasaki, Wataru

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/4/1

Matsui, Takayuki

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/4/1

Yamada, Masumi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/5/1

Sugiyama, Motokuni

Hired

TMT Project Office, Specially Appointed
Senior Specialist

2014/5/1

Kawashima,
Tomohisa

Hired

Center for Computational Astrophysics,
Specially Appointed Research Staff

2014/5/1

Kawaguchi,
Toshihiro

Hired

Astronomy Data Center, Specially Appointed
Research Staff

2014/5/19

Wu, Yuanwei

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2014/6/1

Zeidler, Simon

Hired

Gravitational Wave Project Office, Specially
Appointed Research Staff

2014/7/1

Sotani, Hajime

HiredDivision of Theoretical Astronomy, Specially
Appointed Assistant Professor

2014/7/15

Omiya, Masashi

Hired

Extrasolar Planet Detection Project Office,Specially Appointed Research Staff

2014/9/1

Sanhueza Nunez,
Patricio Andres

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2014/9/1

Barton, Mark
Andrew

Hired

Gravitational Wave Project Office, Specially
Appointed Research Staff

2014/10/1

Minamidani,
Tetsuhiro

HiredNobeyama Radio Observatory, Specially
Appointed Assistant Professor

2014/10/1

Yamada, Ryuhei

Hired

RISE Project, Specially Appointed Research
Staff

2014/10/1

Tazaki, Fumie

Hired

Mizusawa VLBI Observatory, Specially
Appointed Research Staff

2014/10/1

Kuniyoshi, Masaya

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/10/1

Zang, Liangjian

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/11/1

Ueda, Junko

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2014/11/1

Hirata, Naoatsu

Hired

Gravitational Wave Project Office, Specially
Appointed Senior Specialist(Nobeyama Radio Observatory,Specially Appointed Research Staff)

III Organization143

2014/11/1

Nagai, Hiroshi

Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor(NAOJ Chile Observatory, Specially
Appointed Assistant Professor)

2015/1/1

Yamamoto, Chieko

HiredAdministration Department General Affairs
Division, Specially Appointed Senior Specialist

2015/2/1

Saito, Motoi

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/5/31

Ishikawa, Ryoko

Resigned(Division of Solar and Plasma Astrophysics
Hinode Science Center, Specially(Hinode Science Center), Assistant Professor) Appointed Assistant Professor

2014/7/31

Takiwaki, Tomoya

Resigned

Center for Computational
Astrophysics, Specially Appointed
Assistant Professor

2014/8/31

Komugi, Shinya

Resigned

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2014/9/30

Tadaki, Kenichi

Resigned

Subaru Telescope, Specially
Appointed Research Staff

2014/9/30

Minamidani,
Tetsuhiro

Resigned(Nobeyama Radio Observatory, Specially
Appointed Assistant Professor)

Nobeyama Radio Observatory,Specially Appointed Research Staff

2014/10/31 Nagai, Hiroshi

Resigned(NAOJ Chile Observatory, Specially
Appointed Associate Professor)

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2014/11/30

Shinnaga, Hiroko

Resigned(Kagoshima University)

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2015/1/31

Chibueze, James
Okwe

Resigned

2015/3/31

Miura, Rie

Resigned(NAOJ Chile Observatory, Specially
Appointed Assistant Professor)

NAOJ Chile Observatory, Specially
Appointed Research Staff

2015/3/31

Herrera Contreras,
Cinthya Natalia

Resigned(NAOJ Chile Observatory, Specially
Appointed Assistant Professor)

NAOJ Chile Observatory, Specially
Appointed Research Staff

2015/3/31

Kawaguchi,
Toshihiro

Resigned

Astronomy Data Center, Specially
Appointed Research Staff

2015/3/31

Kandori, Ryo

Contract
ExpiredExtrasolar Planet Detection Project
Office, Specially Appointed
Research Staff

2015/3/31

Nagayama, Takumi

Contract
Expired(Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist)

Mizusawa VLBI Observatory,Specially Appointed Research Staff

2015/3/31

Yamaguchi,
Takahiro

Contract
Expired(Office of International Relations, Specially
Appointed Senior Specialist)

NAOJ Chile Observatory
Administration Department,
Specially Appointed Senior Specialist

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

Research Administrator Staff
Date

144

Name

2014/4/1

Chapman, Junko

Hired

Research Enhancement Strategy Office,
TMT Project Office, Specially Appointed
Senior Specialist

2014/4/1

Hori, Kuniko

HiredResearch Enhancement Strategy Office,Research Evaluation Support Office,Specially Appointed Senior Specialist

2014/4/1

Lundock, Ramsey
Guy

Hired

Research Enhancement Strategy Office,Public Relations Center, Specially Appointed
Senior Specialist

2014/4/1

Chiba, Kurazo

Hired

Research Enhancement Strategy Office,Engineering Promotion Office, Specially
Appointed Senior Specialist

III Organization

2014/4/1

Fukui, Hideharu

HiredResearch Enhancement Strategy Office,
NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2014/10/1

Miura, Mitsuo

HiredResearch Enhancement Strategy Office,Mizusawa VLBI Observatory, Specially
Appointed Senior Specialist

2014/9/30

Suematsu, Sayaka

Foreign Visiting Researcher
Name
Kuhn, Jeffrey Richard
Ojha, Devendra Kumar
Turner, Edwin Lewis
Uitenbroek, Han
Barsuglia, Matteo
Packham, Christopher Charles

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

Resigned

Period2014/5/27 ~ 2014/6/20
2014/9/11 ~ 2014/9/20
2014/6/9 ~ 2014/7/8
2014/9/4 ~ 2014/10/31
2015/2/5 ~ 2015/3/5
2014/4/7 ~ 2014/5/16
2014/5/19 ~ 2014/6/30
2014/6/4 ~ 2014/8/13

Affiliated Institute
University of Hawaii (U.S.A)
Tata Institute of Fundamental Research (India)
Princeton University (U.S.A)
National Solar Observatory (U.S.A)
Centre National de la Recherche Scientifique (France)
The University of Texas at San Antonio, UTSA (U.S.A)

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

7. Advisory Committee for Research and Management
Members
From universities and related institutes
Kajita, Takaaki
The University of Tokyo○ Kusano, Kanya
Nagoya University
Momose, Munetake
Ibaraki University
National Institute for Fusion
Murakami, Izumi
Science
Japan Aerospace Exploration
Nakagawa, Takao
AgencyOhta, Kouji
Kyoto University
Okumura, Sachiko
Japan Women's University
Sugita, Seiji
The University of Tokyo
Umemura, Masayuki University of Tsukuba
Yamada, Toru
Tohoku University

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

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

III Organization

1458. Professors Emeriti and Staffs Emeriti
Professor Emeritus (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
Professor Emeritus (Tokyo Astronomical Observatory)
Akabane, Kenji
Moriyama, Fumio
Kozai, Yoshihide146

III Organization

IV Finance
Revenue and Expenses (FY2014)
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

Budget13,273,727
2,382,752
88,99941,378653,223
1,574
16,441,653
Budget13,316,679
3,535,534
9,781,145
2,401,752
69,999653,223
16,441,653
Budget0

Final Account
13,897,144
2,241,797
81,356
61,071
258,288
4,209
16,543,865
Final Account13,600,573
3,433,737
10,166,836
2,268,797
54,356
250,458
16,174,184
Final Account369,681(Unit: ¥1,000)
Budget − Final Account−623,417
140,955
7,643−19,693394,935−2,635−102,212
Budget − Final Account−283,894
101,797−385,691
132,955
15,643402,765
267,469
Budget − Final Account−369,681

IV Finance147

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2014
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)JSPS Fellows
Research Activity start-up
Publication of Scientific Research Results
Total

Budget (thousand yen)
Direct Funding Indirect Funding

Total

8

97,50029,250126,750

3
10
1
8
2
1
33

60,60076,800
2,100
9,100
1,600
1,000
248,700

18,18023,040
630
2,730
480
0
74,31078,78099,8402,730
11,8302,080
1,000
323,010

Budget (thousand yen)
Direct Funding Indirect Funding
16,705
5,012
2,000
600
15,878
4,763
34,583
10,375

Total
21,7172,600
20,641
44,958

2. Multi-year Fund for FY 2014
Research Categories

Number of Selected Projects

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

14
2
18
34

3. Partial Multi-year Fund for FY2014

148

Research Categories

Number of
Selected Projects

Scientific Research (B)Young Scientists (A)
Total

4
2
6

Budget (Series of Single-year Grants)(thousand yen)
Direct Funding Indirect Funding
Total
8,900
2,670
11,5708,600
2,580
11,18017,5005,250
22,750V KAKENHI (Grants-in-Aid for Scientific Research)

Budget (Multi-year Fund)(thousand yen)
Direct Funding Indirect Funding
2,600
780
5,000
1,500
7,600
2,280

Total
3,380
6,500
9,880

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)

Subaru Telescope
Solar Observatory

Open Use at
Project/Center

45-m telescope (General Proposal)
45-m telescope (Education Program)
Nobeyama Radio
Observatory
45-m telescope (Short Program)
45-m telescope (Back-up Program)
Nobeyama Solar Radio Observatory
Mizusawa VLBIVERAObservatory

Number of
Total
Accepted Number of
Proposal Researcher
2
24
1
128

43 (0)
155 (4)30 (0)
422 (60)

2 Institutes
12 Institutes, 2 Countries
3 Institutes
77 Institutes, 14 Countries

*
29
0
9
1
34

*
188 (64)070 (15)9 (2)150 (107)*
46 Institutes, 11 Countries
18 Institutes, 5Countries
3 Institutes
40 Institutes, 15 Countries18

114 (46)

19 Institutes, 7 Countries

384 (54
at foreign
institutes)
198
125 (42)
139
52
1,846
(1,511)209 (44)161 (36)

83 Institutes, 15 Countries,
Total amount of requested
data 31 TB
47 Institutes, 9 Countries
46 Institutes, 14 Countries
58 Institutes
15 Institutes

Astronomy Data Center

384

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

198
125
30
7

ALMA

196

ASTE
Mopra

32
20
9
2
17
0

NAOJ Chile
Observatory

Note

227 Institutes, 34 Countries
21 Institutes, 10 Countries
22 Institutes, 12 Countries
8 Institutes
2 Institutes
12 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 observation data is open to the public on the web. No application is needed to use the data.

VI Research Collaboration

1492. Commissioned Research Fellows
Visiting Scholars (Domestic)
Period: April 1, 2014 - March 31, 2015 *April 1, 2014 - July 31, 2014
Name
Onishi, Toshikazu
Sakamoto, Seiichi*
Fujisawa, Kenta
Momose, Munetake
Imai, Hiroshi
Iwata, Takahiro
Oka, Tomoharu

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

Affiliated Institute
Osaka Prefecture University
Japan Aerospace Exploration Agency
Yamaguchi University
Ibaraki University
Kagoshima University
Japan Aerospace Exploration Agency
Keio University

Kotake, Kei

Visiting Associate Professor

Fukuoka University

Takahashi, Keitaro
Hagino, Kouichi
Hirata, Naru

Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor

Kumamoto University
Tohoku University
The University of Aizu

Masuda, Satoshi

Visiting Associate Professor

Nagoya University

Yonekura, Yoshinori
Asaki, Yoshiharu

Visiting Associate Professor
Visiting Research Fellow

Ibaraki University
Japan Aerospace Exploration Agency

Oshima, Akitoshi

Visiting Research Fellow

Chubu University

Kurayama, Tomoharu
Naruse, Masato

Visiting Research Fellow
Visiting Research Fellow

Teikyo University of Science
Saitama University

Host Project/Center/Division
NAOJ Chile Observatory
NAOJ Chile Observatory
Mizusawa VLBI Observatory
NAOJ Chile Observatory
Mizusawa VLBI Observatory
RISE Project
NAOJ Chile Observatory
Center for Computational
Astrophysics
Division of Radio Astronomy
Division of Theoretical Astronomy
RISE Project
Nobeyama Solar Radio
Observatory
Mizusawa VLBI Observatory
NAOJ Chile Observatory
Center for Computational
Astrophysics
Mizusawa VLBI Observatory
Advanced Technology Center

JSPS (Japan Society for the Promotion of Science) Postdoctoral Research Fellows
Name
Ishikawa, Shinnosuke
Niino, Yuu
Hada, Kazuhiro
Ueda, Junko
Sakai, Nobuyuki
Nitta, Tomu
Nomura, Mariko
Hayashi, Masao

Research Subject
Study of solar flare particle acceleration with high-sensitivity and high-resolution
X-ray imaging spectroscopic observations
Probing Cosmic Star Formation at High Redshifts via Afterglows and Host
Galaxies Gamma-Ray Bursts
Probing a relativistic jet in a supermassive black hole with high-resolution radio
monitoring observations
Unveiling the evolution of merging galaxies from the formation of cold moleculargas disks
Outer Rotation Curve of the Galaxy with VERA
Development of a superconducting 1000 pixels camera for the antarctic
submillimeter telescopeThree Dimensional Radiation Hydrodynamic Calculations of Outflows fromAccretion Disks and Studies of Absorption Lines in Active Galactic Nuclei
Formation and evolution of elliptical galaxies revealed by internal structures ofgrowing progenitors in galaxy clusters

Host Researcher
Suematsu, Yoshinori
Kashikawa, Nobunari
Homma, Mareki
Iono, Daisuke
Honma, Mareki
Sekimoto, Yutaro
Osuga, Ken
Kodama, Tadayuki

JSPS (Japan Society for the Promotion of Science) Foreign Research Fellows
Name
None

150

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 as an independent graduate university
without undergraduate courses via partnerships with interuniversity 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 field, in anenvironment with the most advanced observational instruments
and supercomputers, as researchers who work at forefront ofworld-class research; experts who carry out the 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 five-year doctoral course)
Three (per year in 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 who also
have the needed theoretical and creative aptitude 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 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 FY2012, 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 2014, the Department of Astronomical Science accepted
four students in the Basic Course and four students in the
Advanced Research Course. The Department also offered thee-learning class “Introduction to Observational Astronomy II” asa school-wide common basic subject, as well as the “Exercise in
Scientific English” class, in order to provide a good foundation
for students at the graduate school.
In order to better prepare students for the international stage,
the Department hosted the Asia Winter School during February
10 to 13, 2015, as well as the 2014 Summer Student programat Mitaka, Mizusawa, Nobeyama and Hawaii 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 Education151

(5) Number of Affiliated Staff (2015/3/31)
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
10
13
1
10
6
8
18
8
11
15
101

(6) Graduate Students (30 students)
1st year (3 students)
Name
Principal Supervisor
Supervisor
Sasahira, Rinko
Osuga, Ken
Tanaka, Masaomi
Kodama, Tadayuki
Michiyama, Tomonari Iono, Daisuke
Yamamoto, Moegi

Kodama, Tadayuki

2nd year (5 students)
Name

Principal Supervisor

Okutomi, Koki

Aso, Yoichi

Flaminio, Raffael

Onoue, Masafusa

Kashikawa, Nobunari

Miyazaki, Satoshi

Nagasawa, Ryosuke

Hanada, Hideo

Matsumoto, Koji

Baba, Haruka

Aoki, Wako

Usuda, Tomonori

Development of infrared instruments and observational research
for the search of earth-like planets

Ryu, Tsuguru

Hayashi, Saeko

Usuda, Tomonori

Study of exoplanets and brown dwarfs from optical and infraredobservations

3rd year (9 students)
Name
Yang, Yi

Supervisor

ThesisResearch for sensitivity improvement of gravitational wave
detectors
Studies on High-z quasars by wide-field imaging observation
Development of software for precise LLR data analysis andstudy of Lunar rotation

Principal Supervisor
Supervisor
Usuda, Tomonori
Hayashi, Saeko
Kashikawa,
Kodama, Tadayuki
Nobunari

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

Onishi, Kyoko

Iguchi, Satoru

Kuno, Nario

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

Onitsuka, Masahiro

Usuda, Tomonori

Takato, Naruhisa

Kobayashi, Hiroshi

Osuga, Ken

Sakurai, Junya

Miyazaki, Satoshi

Tomisaka, Koji
Kobayashi,
Yukiyasu

Shimakawa, Rizumu

Kodama, Tadayuki

Arimoto, Nobuo

Suzuki, Taiki

Oishi, Masatoshi

Saito, Masao

Ishikawa, Shogo

152

Iwata, Ikuru

Thesis
The co-evolution of galaxies and black holes
Observing Starburst Galaxies Using ALMA
The peak epoch of galaxy formation explored by SWIMS-18
surveyVII Graduate Course Education

The observational study of the atmospheres of the exoplanetsand the brown dwarfs
Radiation Hydrodynamic Study of Gas Flow Around Black-Holes
Study of large scale structures in the universe through wide
field imaging
Physical properties and environmental dependence of galaxies
at their peak epoch of formation
Research on Organic Molecules in the Universe

Suzuki, Tomoko

Kodama, Tadayuki

Iono, Daisuke

Galaxy anatomy at the peak epoch of galaxy formation

4th year (5 students)
Name
Aoki, Sumire

Principal Supervisor
Arimoto, Nobuo

Supervisor
Kodama, Tadayuki

Saito, Yuriko

Imanishi, Masatoshi Hayashi, Saeko

ThesisOrigin of Morphology of Elliptical Galaxies
Investigating the supermassive black hole to spheroidal stellar
mass ratio at z~3

Matsuzawa, Ayumu

Iguchi, Satoru

Saito, Masao

Oh, Daehyeon

Aoki, Wako

Takami, Hideki

Giono, Gabriel

Suematsu, Yoshinori Hara, Hirohisa

5th year (8 students)
Name

Principal Supervisor

Imase, Keisuke

Kodama, Tadayuki

Kaithakkal, Anjali
John

Research of absorbing plasma around SMBH of M87 by cm
and mm wavelength
A study of extrasolar planets and their formation sites based on
infrared observations
Study of Optical Tests in Ly-α for CLASP Instrumentation

Supervisor
Kashikawa,Nobunari

ThesisNear-Infrared Spectroscopic Observation of Broad Line
Regions in Nearby Active Galactic Nuclei"

Suematsu,
Yoshinori

Watanabe, Tetsuya

Study of Solar Spectro-polarimetry and Magnetic Reversal of
the Sun's Poles

Kataoka, Akimasa

Tomisaka, Koji

Nakamura,
Fumitaka

Theoretical modeling of the structure evolution of dust
aggregates in the early stage of planet formation

Sako, Nobuharu

Watanabe, Tetsuya

Sekii, Takashi

Obsservational Investigation of Short-Lived Activity Creation
Processes in the Solar Atmosphere

Shino, Nagisa

Honma, Mareki

Shibata, Katsunori

Toshikawa, Jun
Min, Cheul Hong

Kashikawa, Nobunari Kodama, Tadayuki
Honma, Mareki
Shibata, Katsunori
Izumiura,
Hayashi, Saeko
HideyukiSukom, Amnart

Research Student (1 student)
Name
Supervisor

Yang, Yongzhang

Hanada, Hideo

Testing the formation scenario of massive stars by CH3OH
maser
Observational study on high-z clusters
Research for a symbiotic star using VERA
Study of star and planetary formation process and theexoplanets based on infrared observations

ThesisResearch of the interior of the moon and the planet based on an application ofrotation theory

VII Graduate Course Education

1532. Education and Research Collaboration with Graduate Schools
Name
Isoe, Mari
Ito, Yuta

Affiliated InstituteSupervisor
The University of Tokyo Kokubo, Eiichiro
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

SHU, Shibo
Okada, Takashi

The University of Tokyo Sekimoto, Yutaro
The University of Tokyo Sekimoto, Yutaro

Kasuga, Megumi

The University of Tokyo Hara, Hirohisa

Kato, Yuta

The University of Tokyo Mizuno, Norikazu

Sakai, Daisuke

The University of Tokyo Kobayashi, Hideyuki

Tezuka, Kenjiro

The University of Tokyo Gouda, Naoteru

Baba, Fuko

The University of Tokyo Hara, Hirohisa

Hirai, Yutaka

The University of Tokyo Kajino, Toshitaka

Lee, Minju

The University of Tokyo Kawabe, Ryohei

Aso, Yusuke

The University of Tokyo Ohashi, Nagayoshi

Ohashi, Satoshi

The University of Tokyo Mizuno, Norikazu

Saito, Toshiki
Shibagaki, Shota
Shibata, Takashi

The University of Tokyo Kawabe, Ryohei
The University of Tokyo Kajino, Toshitaka
The University of Tokyo Kokubo, Eiichiro

Sekiguchi, Sigeyuki The University of Tokyo Sekimoto, Yutaro

Millimeter VLBI studies on astronomical observation with
the KVN and VERA Array and the VERAThe Study of Star Formation and Interstellar Medium in the
Galactic Plane
Development of MKID camera
The development of submm-camera for observing CMB
An observational study on coronal heating throughinvestigation of photospheric properties at the footpoints ofcoronal loops
Herschel Protocluster Survey
Study for revealing dynamics in the Galactic Center region
with VLBI
Resolving degeneracy with regard to gravitational
microlensing by astrometry
A case study of energy transfer in the chromosphere with
IRIS and Hinode
Chemodynamical evolution of dwarf galaxies
Environmental effects on galaxy evolution from the JVLA
continuum observation towards a protocluster 4C23.56
Formation and growth of protoplanetary disks
Chemical evolution of the star-forming cores in the giant
molecular clouds
Starburst and SMBH Formation in Merging Galaxies
r-process nucleosynthesis
Study of Planet Formation
Development of MKID camera for wide field millimeterwave observations
The study of merge process of primal galaxy black holes
with the dynamical friction by gas
Formation and Evolution of Protoplanetary Disks
Development of Bi-layer MKID camera
Construction of a galactic dynamical model withastrometric data

Tagawa, Hiromichi

The University of Tokyo Gouda, Naoteru

Koyamatsu, Shin
Sekine, Masakazu

The University of Tokyo Ohashi, Nagayoshi
The University of Tokyo Sekimoto, YutaroHara, Takuji

The University of Tokyo Gouda, Naoteru

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

The effects of stellar feedbacks on the molecular cloudformation in the Large Magellanic Cloud

Akiyama, Kazunori

The University of Tokyo Kobayashi, Hideyuki

Millimeter VLBI studies on the innermost region of AGNs
with the KVN and VERA Array and the Event Horizon
Telescope

Kiyokane, Kazuhiro The University of Tokyo Mizuno, Norikazu

154

Thesis
Theoretical Study of Planet Formation
Galactic structure and evolution
Studies on sub-arcsecond transition-region structures at thefootpoints of coronal loops in the active-region plage

Fujii, Akihiko

The University of Tokyo Kokubo, Eiichiro

Kasai, Miho

Toho University

Matsuo, Hiroshi

Kubo, Daiki

Toho University

Matsuo, Hiroshi

Takano, Akihiro

Kobe University

Ohashi, Nagayoshi

VII Graduate Course Education

Research of kinematic structure of low-mass star formation
process with Radio telescope
Theoretical study on the formation and the evolution of
spatial structure in dense planetary rings
Establishment of stable operation of SIS photon detectors
Experimental studies on readout electronics for SIS photon
detectors
Radio Observations of Star Forming Regions

3. Commissioned Graduate Students
Doctoral Course

Affiliated Institute

Period2014/4/1 ~2015/3/31

Supervisor

Ono, Yoshito

Tohoku University

Oya, Masahito

Nihon University

2014/4/1 ~2015/3/31

Watanabe, Junichi

Sekiguchi, Takanori

The University of Tokyo

2014/4/1 ~2015/3/31

Development of Vibration Isolation System
Flaminio, Raffaele for Large-Scale Cryogenic Gravitational Wave
Telescope KAGRA

Mizuno, Izumi

Kagoshima University

2014/4/1 ~2015/3/31

Saito, Masao

Master's Course

Affiliated Institute

Period2014/4/1 ~2015/3/31

Iwata, Ikuru

ThesisVerifications of Multi-Object AO system using
RAVEN

Supervisor
Iono, Daisuke

Development of Interferometer for direct
observations of exoplantets

Polarization calibration method for single-dishradio observations.
ThesisObserving Distant Galaxies Using the NRO 45m
and ALMA

Kurahashi, Takuya

Meisei University

Okuyama, Yasushi

Tokyo Universityof Agriculture andTechnology

2014/4/1 ~2015/3/31

Watanabe, Junichi

Development of precise spectrograph and studies
of exoplanets

Kajita, Satoshi

Tokai University

2014/4/1 ~2015/3/31

Watanabe, Tetsuya

Study of non-thermal particles in the precursory
phenomena of solar flares

Kawauchi, Kiyoe

Tokyo Institute ofTechnology

2014/4/1 ~2015/3/31

Aoki, Wako

The high resolution transmission spectroscopy of
the Earth atmosphere using the lunar eclipse dataSato, Kazuma

Tokyo Universityof Agriculture andTechnology

2014/4/1 ~2015/3/31

Watanabe, JunichiHigh Contrast Optics for direct observations of
exoplanets

Taniguchi, Kotomi

Toho University

2014/4/1 ~2015/3/31

Saito, Masao

13

Nakahara, Satomi

Kagoshima University

2014/4/1 ~2015/3/31

Honma, Mareki

VLBI multi-epochs observations of the lowluminosity AGN M84

Aoki, Misa

International Christian
University

2014/10/1 ~2015/3/31

Aoki, Wako

Origins of r-process studied by chemical
abundances of metal-poor stars with Subaru/HDS

Sunaga, Naoki

Shizuoka University

2014/10/1 ~2015/3/31

Kajino, Toshitaka

High Energy Astrophysics Phenomena and theOrigin of Elements

C isotopic fractionation of HC5N in TMC-1

4. Degrees Achieved with NAOJ Facilities
Name
Sako, Nobuharu
Anjali John Kaithakkal
Kataoka, Akimasa
Toshikawa, Jun

DegreeDoctor of Philosophy, SOKENDAI
Doctor of Philosophy, SOKENDAI
Doctor of Philosophy, SOKENDAI
Doctor of Philosophy, SOKENDAI

Imase, Keisuke

Master of Science, SOKENDAI

ThesisStatistical Study of X-ray Jets using Hinode/XRT
A Study on the Photospheric Polar Magnetic Patches of the Sun
Planetesimal Formation via Fluffy Dust Aggregates
Growth History of Galaxy Clusters Traced by Protoclusters at z ~ 3– 6
Near-Infrared Spectroscopic Observation of Broad Line Regions in
Nearby Active Galactic Nuclei

VII Graduate Course Education

155

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 season (December
28–January 4)
Visitors: 19,754
Open facilities: Observatory History Museum (65-cm
Telescope Dome), 20-cm Telescope Dome, Solar
Tower Telescope, Exhibition Room, Repsold Transit
Instrument Housing, Astronomical Instruments
Museum, Gautier Meridian Circle, Old Library[Open year-round]
Dates: April to March (except for New Year season), 9:00–
17:00 daily
Visitors: 17,021
Open facilities: Kimura Hisashi Memorial Museum, VERA
20-m antenna, 10-m VLBI antenna
The open house event is held at the campus with thecooperation of the Oshu Space and Astronomy Museum (OSAM:
Yugakukan) located in the campus.
Date: August 16 (Sat.), 2014, 17:00–20:00 (Pre-event)August 30 (Sat.), 2014, 10:00–16:00 (Exhibition)
Visitors: Approximately 1,000 (Pre-event) , 847(Exhibition)[Regular Star Gazing Party]
Dates: Friday before second Saturday; fourth Saturday
Visitors: 5,161 (23 events)
Open facility: 50-cm Telescope for Public Outreach[Special Open-House Event] Mitaka Open House Day
Dates: October 24 (Fri), 2014, 14:00–19:00
October 25 (Sat), 2014, 10:00–19:00
Topic: TMT Challenging the Frontiers of Space
Visitors: 4,768
This event is jointly sponsored by NAOJ, the Universityof Tokyo School of Science Institute of Astronomy, and the
SOKENDAI Department of Astronomical Science. 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 University of Tokyo Institute of Astronomy (“Seeing the
Universe in Infrared – The Advancing TAO Telescope Project”
Kentaro Motohara, Associate Professor at the University ofTokyo [in Japanese]) and NAOJ (“The Search for Planets andLife Outside the Solar System” Edwin L. Turner – Professor at
Princeton University [in English with simultaneous Japanesetranslation]; “At Last! Construction Starts for the Thirty
Meter Telescope” Masanori Iye, Professor at SOKENDAI [inJapanese]).
Both days benefited from clear weather, helping attendance
reach a record high. In addition to the opening of facilities
normally closed to the public, interactive displays and minilectures, there were also games and quizzes popular withchildren to engage a wide range of ages.
* Custom group tours (Dantai Kengaku), 4D2U Theater
showings, and Guided Tours were also offered. Refer to the
Public Relations Center report for details.

156

VIII Public Access to Facilities[Special Open Day] Held as part of Iwate Galaxy Festival 2014
(Hours: 10:00–21:00)
As a pre-event for the Iwate Galaxy Festival, a mission
de-briefing session by JAXA astronaut Koichi Wakata washeld during Part 1 of the Special Open House Day. Here hespoke about his activities in the six months he spent on theInternational Space Station as its first Japanese commander.
Part 2 featured “the Special Lecture on Space” panel
with Koichi Wakata, Mareki Honma (Associate Professor in
Mizusawa VLBI Observatory), and Koji Matsumoto (Associate
Professor in the RISE Project).
Like last year, the Open Day was co-hosted with Ihatov
Space Action Center/the Oshu Space and Astronomy Museum(OSAM: Yugakukan) and the city of Oshu. The Open Day
included strong involvement by the local community, such asa performance by a marching band from a local elementary
school at the opening, workshop corners run by local university
students, and others.
NAOJ offered tours of the 20-m parabolic antenna, acommemorative photo booth, plastic bottle rockets, a quiz game,guided tours of the Kimura Hisashi Memorial Museum, andexhibits explaining the research highlights of VERA, RISE andCfCA projects.
In the Kimura Hisashi Memorial Museum, special guided
tours named "Kimura Hisashi Memorial Museum guided tour"and "the guided tour of the stars tonight” held by the Young
Astronauts Club - Japan Mizusawa Z- Chapter were wellreceived.
Open Day events also included a special lecture by Shogo
Tachibana, Associate Professor of Hokkaido University, entitled“Hayabusa-2 —a dream in the Age of Discovery of the Solar
System—”. This talk was given to a full house, with a goodatmosphere.
OSAM (Yugakukan) offered such attractions as “Science’s
Mystery” experiments, scientific performances by a scientist,and a workshop by internship students. Due to bad weather, alecture about the stars was held instead of the stargazing party,

to close the festival with great success.
Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for New Year season)
Visitors: Approximately 2,000[Special Open Day]
Date: August 10 (Sun.), 2014, 10:00–21:00
This year’s special open house event was canceled due to atyphoon.
Ogasawara: VERA Ogasawara Station[Open year-round]
Dates: April to March (except for New Year season)
Visitors: 7,535[Special Open Day]
Date: February 15 (Sun.), 2015, 10:00–17:00
Visitors: 213
A special open house event was held again this year under
the name “Star Island 14”. Like last year, the free shuttle buses
were appreciated by the visitors. The number of visitors wasmore than 200. NAOJ offered such attractions as exhibits about
the research results of VERA, RISE and Okayama AstrophysicalObservatory projects, mystery experiment corners and quiz
games, as well as a 4D2U digital planetarium show, which
was very popular among visitors. On February 14, NAOJ also
cooperated in a stargazing session hosted by the local astronomy
club. It was held in favorable weather conditions, and the event
was an unprecedented success. Space lectures were also given
by Sawada from the Mizusawa VLBI Observatory and Yamada
from the RISE Project at the Ogasawara Visitor Center on thenight of February 15.
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: 2,754[Special Open day]Dates: August 3 (Sun.), 2014, 10:00–17:00
Visitors: 264

national holiday, it is opened and closed on the nextday) 10:00–17:00
Stargazing sessions: Evenings on Saturdays, Sundays,
Holidays, and Star Festival weekdays (19:00–22:00),
two 30-minute sessions per evening (four in August)
4D2U screening: from 15:00 to 15:30 every day that theobservatory is open
Visitors: 12,790 (877 during the Star Festival of the Southern
Island)Open facilities: Murikabushi 105-cm optical/infrared
telescope, Hoshizora Manabi no Heya (featuring
the 4D2U “four dimensional digital universe”),
interior of observation dome (including exhibits ofastronomical images)
The “Hoshizora Manabi no Heya”, constructed adjacentto the observatory in 2013 by the city of Ishigaki, was very
popular, welcoming 3,488 guests.
[Star Festival of the Southern Island 2014]
Dates: August 2 (Sat.) to August 10 (Sun.), 2014
Visitors: 10,950
This year is the 13th anniversary of both the completionof VERA Ishigaki-jima Station and the Star Festival of theSouthern Island. Approximately 8,000 visitors attended thedimmed-light stargazing event even though it was cloudy.
In addition, the first meteorite exhibition in Okinawa
prefecture was held in cooperation with the Nayoro Municipal
Astronomical Observatory. The number of visitors was 754. And
734 people visited the annual planetarium show (from August 7
to 10).
The activities at Ishigaki-jima Astronomical Observatory
boosts regional promotion like school education, lifelong
learning and sightseeing. The cooperation agreement between
NAOJ and the Tourism Association of the city of Ishigaki has
been finalized concluded. And it is widely recognized that starry
sky can be used as a tourism resource. Considering this situation,
we will continue to strengthen our ties with other associations.

Held in conjunction with the Star Festival of the Southern
Island.
As in previous years, attractions included antenna tours,
Purikura (photo booth stickers), merchandise, commemorative
lectures, and exhibits.
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 a

VIII Public Access to Facilities

157

3. Nobeyama Campus

4. Okayama Campus[Regular Open]
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: 48,837
Open facilities: 45-m Radio Telescope, Nobeyama Millimeter
Array, Nobeyama Radioheliograph, etc. (justviewing)Okayama Astrophysical Observatory[Open year-round]
Dates: 9:00–16:30 daily
Visitors: 10,867
Open facilities: Window view of 188-cm reflecting telescope[Open House Day]
Date: August 23 (Sat), 2014, 9:30–16:00
Visitors: 2,698
The Nobeyama branch was crowded with 2,698 visitors on
the 2014 Open House Day. The theme of the Day was “Radio
Astronomy, from Nobeyama to the World!” Like every year, we
had two lectures on the theme, which attracted large audiences.
One was “From Nobeyama to the World: 45 years of Solar
Radio Astronomy” by Dr. Hiroshi Nakajima (NAOJ). The otherwas “The Radio Universe: Results From Nobeyama and ALMAin South America” by Prof. Ken’ichi Tatematsu (NAOJ). We
had some established events such as touch the main reflector
panel of 45-m Radio Telescope, radio detector handicrafts, shortlectures, and a stamp rally. In addition, the antenna handicrafts
and original calendar events by NRO alumni, other project staff
members, and volunteers took place. Also the participation of
the Nagano Pref. PR character, ARUKUMA, made Nobeyama
more festive on that day.
[Jimoto Kansha Day (Thanks Day for the locals)]Date: November 8 (Sat), 2014, 13:30–19:00
Visitors: 65
The local people have said that they have difficulty
participating in the the Open House Day, which occurs
during the farming season and they do not have a clear
understanding of what we (not only NRO but also Tsukuba
and Shinshu Universities) study in Nobeyama. In responsethese comments, we established this event in cooperation
with Tsukuba University, Agricultural and Forestry ResearchCenter, Yatsugatake Forest and Shinshu University, Faculty ofAgriculture, Education and Research Center of Alpine Field
Science. We had an introduction lecture from each institute anda guided tour of the NRO. In addition, we tried a star gazing
party, which was not held due to bad weather. We got a sense ofachievement from the event, hearing a comment “This is the firsttime I’ve known what they study here.”

158

VIII Public Access to Facilities[Special Open House]
Date: August 30 (Sat), 2014, 9:30–16:30
Visitors: 632
The special open house event for FY 2014 was co-hosted
with the Okayama Astronomical Museum on August 30 (Sat).
We had two special lecture at 188cm reflecting telescopein the dome. The first lecture, by NAOJ vice-director general
Junichi Watanabe, was “Why deviate?
Predicting comets. - Comet ISON as an example -”.
The second lecture, by Professor Tetsuya Nagata of Kyoto
University, was “Kyoto University 3.8-m telescope, the start ofconstruction”. The two lectures attracted nearly 140 audience
members. The lectures were broadcast over the Internet withassistance from the Public Relations Center. The always-popular
tours of the main mirror of the 188-cm reflecting telescopewere conducted in the morning and afternoon with maximum
capacities of 120 participants. The exhibition of the 50-cm
reflecting telescope was conducted in two Tokyo Institute ofTechnology students. Planetarium showings, solar observations
by 15-cm telescope, astronomy-related crafts, constellation/
astronomy bingo, and an astronomy quiz rally were held at
the Okayama Astronomical Museum. We think many visitors
enjoyed themselves. The special open house event was cohosted with the Asakuchi City Board of Education, with support
from the Yakage Town Board of Education. In particular, theObservatory would like to thank the members of the Asakuchi
City Board of Education for their considerable assistancein arranging complimentary shuttle bus service between the
Observatory and Kamogata Station on the JR San’yo Main Line.
[Special Stargazing Party]
Date: April 4 (Sat), 2014, 18:00–22:15
Visitors: 92
159 applications for 519 applicants were received.
Date: November 1 (Sat), 2014, 17:00–21:15
Visitors: 78
121 applications for 328 applicants were received.
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. Due to rain, both of thespecial stargazing parties conducted facility tours instead.

5. Subaru Telescope[Summit Facility]
Dates open for public tour: 99 (these dates are listed in the
public tour program page at the Subaru Telescope’s
web site, the tour was suspended in December due tothe telescope work)
Public tour visitors: 559
Special tour visitors: 111visits, 717 visitors
As some special tours were conducted during public tour
programs, the total number of actual visitors was 1,252.
[Base Facility]
Special tour visitors: 41 visits, 451 visitors[Public information]
Primary means of public information is posting at theofficial website http://subarutelescope.org• Science results from the Subaru Telescope – 10 Japaneseand 11 English articles• Depicting special activities or making announcement
on CfA, recruitment – 24 Japanese and 21 English
articlesSupplemented by the social media via official accounts suchas Twitters, Facebook page, and YouTube – 197 Japaneseand 138 English posting• 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 (forJapanese), SubaruTelescopeNAOJe (for English)
1. Gave a lecture at the Subaru Telescope’s base facility in Hilo2014
May 29: Subaru Telescope staff gave a lecture at the Subaru
Telescope’s base facility in Hilo for the “Senior University
Net”.
June 10: Subaru Telescope staff gave a lecture at the Subaru
Telescope’s base facility in Hilo for the “Higashi Hiroshima
Chamber of Commerce” and “Japanese Chamber ofCommerce and Industry in Hawaii”.
June 26: Subaru Telescope staff gave a lecture at the Subaru
Telescope’s base facility in Hilo for the NASA Explorer
Team (teachers from Key Penninsula Middle School).
July 21: Subaru Telescope staff gave a lecture at the Subaru
Telescope’s base facility in Hilo for the Ritsumeikan HighSchool students from Kyoto and Waiakea High School
students in Hilo.

July 25: Subaru Telescope staff gave a lecture at the Subaru
Telescope’s base facility in Hilo for the Sumoto High School
students from Hyogo.
August 12: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the junior highschool students from Nago City of Okinawa.
August 22: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Kawagoe
High School students from Saitama.
September 12: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Tokyo City
University students.
September 16: Subaru Telescope staff gave a lecture at
the Subaru Telescope’s base facility in Hilo for the Toho
University students.
September 23: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Sapporo
Nihon University Senior High School students from
Hokkaido.
September 26: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the University of
Ryukyus students.
October 8: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Masuda
High School students from Shimane.
October 13: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Meijo
University High School students from Aichi.
October 17: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Namiki HighSchool students from Ibaraki.
November 10: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Kunori
Gakuen High School students from Yamagata.
November 13: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Group from
Germany (MPIA, “Sterne und Weltraum”).
December 2 & 3: Subaru Telescope staff gave a lecture at
the Subaru Telescope’s base facility in Hilo for the SenriHigh School students from Osaka.
2015
January 5: Subaru Telescope staff gave a lecture at the

VIII Public Access to Facilities

159

Subaru Telescope’s base facility in Hilo for the Wakimachi
High School students from Tokushima.

conferencing system from the Subaru Telescope’s base facility
in Hilo to the Saji Astro Park in Saji City of Tottori.

January 8: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Seisho HighSchool students from Nara.

July 28: Subaru Telescope staff gave a presentation via remote
conferencing system from the Subaru Telescope’s base facility
in Hilo to Wakayama Shin-ai High School in Wakayama.

January 27: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Sanbonmatsu
High School students from Kagawa.

August 1: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s basefacility in Hilo to the Galaxity in Adachi Ward of Tokyo.

March 6: Subaru Telescope staff gave a lecture at the Subaru
Telescope’s base facility in Hilo for the Iiyama-Kita HighSchool students from Nagano.

September 5: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s basefacility in Hilo to the Galaxity in Adachi Ward of Tokyo.

March 8: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the RitsumeikanHigh School students from Kyoto and Waiakea High School
students in Hilo.

September 6: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s
base facility in Hilo to the Science Museum in Tokyo for its“Universe” live show.

March 10: Subaru Telescope staff gave a lecture at theSubaru Telescope’s base facility in Hilo for the Ritsumeikan
Uji High School students from Kyoto.

December 5: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s basefacility in Hilo to Arakawa 3rd Junior High School in Tokyo.

2. Remote presentation

3. Lectures, demonstrations, workshops etc. in the vicinity

2014

2014

May 22 & 23: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s basefacility in Hilo to the Nagoya City Museum in Aichi.

July 21-25: Subaru Telescope staff provided astronomy
workshop during the Pacific Astronomy and Engineering
Summit (including high school students from Japan, U.S.A,
Canada, China, and India).

June 17: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s basefacility in Hilo to Izumo High School in Shimane.
June 27: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s
base facility in Hilo to the DNA Expedition Service Lab/
Seodaemun Museum of Natural History in Korea.

September 13-14: Subaru Telescope staff gave a lecture andpanel discussion at the HawaiiCon in Waikoloa.
November 15: Subaru Telescope staff made a presentation at
the Office of Mauna Kea Management talk for volunteers at
Hale Pohaku.
2015

July 3: Subaru Telescope staff gave a presentation via remote
conferencing system from the Subaru Telescope’s base facility
in Hilo to the Masuda City for its Science Town event in
Shimane.
July 11: Subaru Telescope staff gave a presentation via remote
conferencing system from the Subaru Telescope’s base facility
in Hilo to Tokyo Mirai University in Tokyo.
July 22 & 29: Subaru Telescope staff gave a presentation via
remote conferencing system from the Subaru Telescope’s basefacility in Hilo to University of Ryukyus in Okinawa.
July 25: Subaru Telescope staff gave a presentation via remote

160

VIII Public Access to Facilities

January 24: Subaru Telescope staff provided astronomy four
workshop during the Onizuka Science Day at the Universityof Hawaii at Hilo.
February 7: Subaru Telescope staff gave a lecture for the
Universe Tonight at Visitor Information Station, Maunakea.
March 1-5: For the Journey through the Universe program,
Subaru Telescope staff went to 26 classes in local publicschools and delivered presentations, hands-on experiences,and other demonstrations.

4. Lectures in Japan2014
April 2: Subaru Telescope staff gave a lecture at the.Nanbu
Iryo Center in Okinawa.
April 4: Subaru Telescope staff gave a lecture at the.Nago
City Museum in Okinawa.
May 19: Subaru Telescope staff gave a lecture at the.Ishima
Junior High School in Tokushima.
June 7: Subaru Telescope staff gave a lecture at the.Asahi
Culture Center in Yokohama.

2015
January 27: Subaru Telescope staff made presentation about
the Subaru Telescope at the Onizuka Science Day eventat the University of Hawaii at Hilo and interacted withhundreds of families in the local community.
March 1: Subaru Telescope staff provided an exhibition
with many hands-on activities about the Subaru Telescopeat‘Imiloa Astronomy Center’s open house and interactedwith hundreds of families in the local community.

6. Media coverage
Japanese 28, English 8

June 26: Subaru Telescope staff gave a lecture at the.Tohodai
Elementary School in Osaka.
July 16: Subaru Telescope staff gave a lecture at the
University of Ryukyus in Okinawa.
September 19: Subaru Telescope staff gave a lecture at the.
Mitaka 5th Elementary School in Tokyo.
November 15: Subaru Telescope staff gave a Special public
lecture at Sendai Astronomical Observatory in Miyagi.
2015
February 12: Subaru Telescope staff gave a lecture at the.
Seibudai Niiza Junior High School in Saitama.
March 14: Subaru Telescope staff gave a lecture at the.
Across in Fukuoka.
March 15: Subaru Telescope staff gave a lecture at the.
Kokura High School in Fukuoka.
March 16: Subaru Telescope staff gave a lecture at theKokura Junior High School Attached to Fukuoka Universityof Education in Fukuoka.

5. Others
2014
April 26: Subaru Telescope staff participated in Merrie
Monarch Festival Parade with observatory group of Mauna
Kea and interacted with local community.
May 3: Subaru Telescope staff provided a big booth withmany hands-on activities about the Subaru Telescope at the
AstroDay event in Hilo and interacted with hundreds offamilies in the local community.

VIII Public Access to Facilities161

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

category

Business Trip

Korea
50
China
16
Hong Kong
0
Taiwan14
Malaysia
0Singapore0
Thailand1
Philippines
0Indonesia
0
Other areas in Asia
6
UK
4
Italy
15
Germany
23
France15
Russia18
Other areas in Europe
39
USA
100
Canada27
Hawaii76
Guam, Saipan
0Australia
2
Other areas in Oceania
0
Mexico1
Brazil0
Other areas in South and Central America *40
Middle East
5
Africa4others0
Total
456* Most travelers to South and Central America went to Chile.

162

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
0
0
0
0
0

50
16
0
14
0
0
1
0
0
6
4
15
23
15
18
39
100
27
76
0
2
0
1
0
40
5
4
0
456

X Award Winners
Award Recipients
Sakurai, Takashi

Affiliated Division
Division of Solar and Plasma
Astrophysics

Job Title
Professor

Sekiguchi, Kazuhiro

Division of Optical andInfrared Astronomy, Office of Professor
International Relations

Watanabe, Junichi

Public Relations Center

Agata, Hidehiko

Award

Date
1 May,
2014

Japan Geoscience Union Fellow
Diploma of Honor, Mongolian
Academy of Sciences

29 May,2014

Vice-Director
General, Professor

Diploma of Honor, Mongolian
Academy of Sciences

29 May,2014

Public Relations Center

Associate Professor

Diploma of Honor, Mongolian
Academy of Sciences

29 May,2014

Honma, Mareki

Mizusawa VLBI Observatory

Associate Professor

National Institutes of Natural Sciences 15 June,
Young Researcher Award, 2014
2014

Hada, Kazuhiro

Mizusawa VLBI Observatory

JSPS Postdoctoral
Fellow

Inoue Research Award for Young
Scientists, 2014

4 February,
2015

NAOJ Director General Prize(Research and Education Category)

17 March,
2015

NAOJ Chile Observatory
Advanced Technology
CenterHonma, Mareki

Mizusawa VLBI Observatory

Professor

The PASJ Excellent Paper Award,
2014

19 March,
2015

Inoe, Tsuyoshi

Division of Theoretical
Astronomy

Assistant Professor

The ASJ Young Astronomer Award,
2014

19 March,
2015

X Award Winners

163

XI Library, Publications
1. Library
Number of books in each library (2015/3/31)
Japanese Books
Mitaka16,849Okayama
220
Nobeyama
1,222
Mizusawa
4,942
Hawaii
1,512
Total
24,745

Foreign Books
45,3683,318
6,260
18,067
4,170
77,183

Total
62,2173,538
7,482
23,0095,682
101,928

Number of journal titles in each library (2015/3/31)
Japanese Journals
Foreign Journals
Mitaka622
774
Okayama4
18
Nobeyama
16
82
Mizusawa
659
828
Hawaii
18
18
Total
1,319
1,720

Total
1,396
22
98
1,487
36
3,039

2. Publication
Here we list continuing publications produced by NAOJ in FY 2014.
The data is based on publications delivered to the libraries.
Mitaka01) Report of the National Astronomical Observatory of Japan, Vol. 16, 2 issues
02) Annual Report of the National Astronomical Observatory of Japan (in Japanese), no. 25, 2013, 1 issue03) Annual Report of the National Astronomical Observatory of Japan (in English), vol. 15, Fiscal Year 2013, 1 issue04) Annual Report of the National Astronomical Observatory of Japan (in English), vol. 15, Supplement, Fiscal 2012, 1 issue05) National Astronomical Observatory Reprint, No. 2548–2650, 103 issues06) Calendar and Ephemeris, 2015, 1 issue07) NAOJ News, No. 249–260, 12 issues
08) Guide to the National Astronomical Observatory of Japan (Japanese), 1 issue09) Guide to the National Astronomical Observatory of Japan (English), 1 issue
10) Chronological Scientific Tables, 2015, 1 issue164

XI Library, Publications

XII Important Dates
April 1, 2014 – March 31, 2015
2014
4 April

Spring 2014 Special Stargazing Party held at Okayama Astrophysical Observatory, with 92 visitors in attendance (outof 519 applicants).

13 AprilFifth Open Observatory event held at the Ibaraki University Center for Astronomy and the NAOJ Mizusawa VLBI
Observatory Ibaraki Station, with approximately 700 visitors in attendance.

26 AprilSubaru Telescope staff participated in Merrie Monarch Festival Parade with observatory group of Mauna Kea andinteracted with the local community.

3 May

Subaru Telescope staff provided a big 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.

2 June ~6 JuneRadio Astronomy Observation training held at Nobeyama Radio Observatory for Undergraduate Students with 12
participants

28 June ~29 JunePre-event workshop held for 5 high school students scheduled to attend the Eighth Z-star Research Team event
using the radio telescope at the VERA Mizusawa station to search for masers, to improve the understanding of theparticipants.

6 JulyThe Star Festival held using the 6-m antenna at the NAOJ Mizusawa VLBI Observatory Kagoshima station in
Kagoshima city Kinko Bay Park, co-hosted with Kagoshima city and Kagoshima University, with approximately
350 visitors in attendance.

21 July ~25 July

Subaru Telescope staff provided astronomy workshop during the Pacific Astronomy and Engineering Summit(including high school students from Japan, U.S.A, Canada, China, and India).

28 July ~1 August

Facility Guide Week for Educational Organization was carried out at Nobeyama Campus.

1 August ~28 September

Fifth International Festival of Scientific Visualization—Connecting with Others Through Science—held with over1 million visitors attending during the festival period.

2 August ~4 August

Eighth Z-star Research Team event held for high school students from Iwate Prefecture, including tsunami-struck
areas, with 5 participants attending. The team succeeded in detecting a water-maser signal from an astronomical
object.

2 August ~10 August

The Southern Island of Star Festival 2014 held together with a special open house event at the VERA Ishigaki-jima
Station and Ishigaki-jima Astronomical Observatory with approximately 10,950 visitors to the whole Star Festival.
Events included an astronomical observation party at the Ishigaki-jima Astronomical Observatory, attended by 877
visitors; and a special public opening of the VERA Station attended by 264 visitors.

4 August ~5 August“Summer Break Junior Astronomical Classes + You are Galileo” held in Mitaka.

10 August

The special open house of VERA Iriki station was scheduled to be held jointly with the Yaeyama Kogen Star
Festival 2014, but was canceled due to a typhoon.

16 AugustA mission debriefing session by JAXA astronaut Koichi Wakata was held as a pre-event of Iwate Galaxy Festival
2014, a special open house day of Mizusawa campus. There were approximately 1,000 visitors in attendance.

18 August ~20 August

Chura-boshi Research Team workshop for high school students in Okinawa Prefecture, Fukushima Prefecture
and Fukuoka Prefecture held at VERA Ishigaki-jima Station and Ishigaki-jima Astronomical Observatory, with
21 participants in attendance. One team using radio-waves discovered 1 masers. A second team using visible lightobservations with the Murikabushi telescope discovered 2 asteroids.

23 August
30 August
30 August
30 September

19 OctoberOpen House day of Nobeyama Campus. There were 2,698 visitors for this event.
Iwate Galaxy Festival 2014, a special open house day of Mizusawa campus, held with 847 visitors in attendance.
Special open house event held at Okayama Astrophysical Observatory, with 632 visitors in attendance.
The 21th Astronomy Lecture for Science Reporters “The Start of Construction for TMT” held, with 37 participantsin attendance. The event was also broadcast over the internet for reporters who could not attend.
The second “Third-term Election of the Japanese Stars, Starry Sky Summit” was held in Ishigaki-shi throughcooperation between the Beautiful Star Astronomical Observatory of Biseicho, Ihara-shi, Okayama and Nobeyama
Radio Observatory. 350 guests entered the main event area, were the program included a memorial event (in honorof Tetsuo Hasegawa, ALMA). 1,364 guests attended the planetarium show “Wish upon the Starry Island” which
was shown simultaneously (October 17–23) at Ishigaki-jima Astronomical Observatory and Ishigaki-shi.

XII Important Dates

165

24 October ~25 October

Mitaka Open House Day held, with 4,768 visitors in attendance.

1 November

Fall 2014 Special Stargazing Party held at Okayama Astrophysical Observatory, with 78 visitors in attendance (outof 338 applicants).

8 November“Jimoto Kansha Day (Thanks Day for the locals)” was held with Tsukuba and Shinshu Universities at NobeyamaCampus. There were 65 local participants.

15 November

The NAOJ/Subaru Telescope lecture meeting 2014 “Subaru Telescope: Looking to Space” held in Sendai
Astronomical Observatory Kato Kosaka Hall with 147 visitors in attendance.

25 November

A ceremony for FY 2014 continuous service recognition held. 11 NAOJ staff members were recognized: Kazuhiro
Sekiguchi, Junichi Nomaru, Naruhisa Takato, Hidehiko Agata, Yutaro Sekimoto, Hirohisa Hara, Kazuyoshi
Sunada, Takuji Tsujimoto, Makoto Miyoshi, Ryutaro Takahashi, Koji Omata.

7 December

A NAOJ lecutre meeting “Cool Univserse: Tracing Our Roots with ALMA” held in Tokyo International Exchange
Center, Plaza Heisei, International Conference Hall with 196 visitors in attendence

8 December ~11 December

291 astronomers (182 astronomers from 21 overseas countries ) gathered and discussed the latest research results by
ALMA at The “Revolution in Astronomy with ALMA 3rd Year”, which was held at the Tokyo International Forum
hosted by NAOJ.

2015

166

27 January

Subaru Telescope staff made presentation about the Subaru Telescope at the Onizuka Science Day event at the
University of Hawaii at Hilo and interacted with hundreds of families in the local community.

15 FebruaryStar Island 14 open house event of VERA Ogasawara Station held, with 213 visitors in attendance (more than the
average year).

1 March ~5 MarchFor the Journey through the Universe program, Subaru Telescope staff went to 26 classes in local public schools
and delivered presentations, hands-on experiences, and other demonstrations.

30 March

A ceremony for FY 2014 continuous service recognition for retiring staff members held. 9 staff members wererecognized: Masanori Iye, Norio Oshima, Kazuo Ono, Hisashi Koyano, Toshiyuki Sasaki, Kiyoto Shibasaki,
Tadayuki Hyuga, Hideo Fukushima, Masami Yutani.

XII Important Dates

XIII Publications, Presentations
1. Refereed Publications
Aartsen, M. G., et al. including Flaminio, R., Fujimoto, M. K.: 2014,
Multimessenger search for sources of gravitational waves and highenergy neutrinos: Initial results for LIGO-Virgo and IceCube, Phys.
Rev. D, 90, 102002.
Aasi, J., et al. including Flaminio, R., Fujimoto, M. K.: 2014,
Gravitational Waves from Known Pulsars: Results from the Initial
Detector Era, ApJ, 785, 119.
Aasi, J., et al. including Flaminio, R., Fujimoto, M. K.: 2014, Applicationof a Hough search for continuous gravitational waves on data fromthe fifth LIGO science run, Classical Quantum Gravity, 31, 085014.
Aasi, J., et al. including Flaminio, R., Fujimoto, M. K.: 2014,
Constraints on Cosmic Strings from the LIGO-Virgo GravitationalWave Detectors, Phys. Rev. Lett., 112, 131101.
Aasi, J., et al. including Flaminio, R., Fujimoto, M. K.: 2015, Searchingfor stochastic gravitational waves using data from the two colocated
LIGO Hanford detectors, Phys. Rev. D, 91, 022003.
Aasi, J., et al. including Flaminio, R., Fujimoto, M. K.: 2014, The
NINJA-2 project: detecting and characterizing gravitational
waveforms modelled using numerical binary black hole simulations,Classical Quantum Gravity, 31, 115004.
Aasi, J., et al. including Flaminio, R., Fujimoto, M. K.: 2014, Methods
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Gonzalez, A., Fujii, Y., Kaneko, K., Kroug, M., Kojima, T., Kuroiwa,
K., Miyachi, A., Makise, K., Wang, Z., Asayama, S., Uzawa, Y.:
2014, ALMA band 10 (787-950 GHz): summary of the productionof 73 receivers and first light results, Proc. SPIE 9153, Eds. W. S.
Holland, J. Zmuidzinas, 91530N.
Groff, T., Kasdin, N. J., Limbach, M. A., Galvin, M., Carr, M. A., Knapp,G., Brandt, T., Loomis, C., Jarosik, N., Mede, K., McElwain, M. W.,
Janson, M., Guyon, O., Jovanovic, N., Takato, N., Martinache, F.,
Hayashi, M.: 2014, Construction and status of the CHARIS highcontrast imaging spectrograph, Proc. SPIE 9147, Eds. S. K. Ramsay, I.
S. McLean, H. Takami, 91471W.
Gusev, A., Ping, J., Hanada, H., Kikuchi, F., Kosov, A., Li, J., Titov, O.:

180

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2014, Radio Navigation Beacons on the Moon, Lunar Geodetic VLBI
System, Physical Libration of the Moon for Chang'E-3/4, Luna-Glob,
Luna-Resource and SELENE-2 Projects, IVS 2014 General Meeting
Proc. "VGOS: The New VLBI Network", Eds. D. Behrend, K. D.
Baver, K. L. Armstrong, 485-489.
Guyon, O., Hayano, Y., Tamura, M., Kudo, T., Oya, S., Minowa, Y.,
Lai, O., Jovanovic, N., Takato, N., Kasdin, J., Groff, T., Hayashi, M.,
Arimoto, N., Takami, H., Bradley, C., Sugai, H., Perrin, G., Tuthill,P., Mazin, B.: 2014, Adaptive optics at the Subaru telescope: current
capabilities and development, Proc. SPIE 9148, Eds. E. Marchetti, L.
M. Close, J.-P. Veran, 91481R.
Hada, K., Giroletti, M., Giovannini, G., Casadio, C., Beilicke, M.,
Cesarini, A., Cheung, C. C. T., Doi, A., Gomez, J. L., Kino M.,
Nagai, H.: 2014, Continuing EVN monitoring of HST-1 in the jetof M87, Proc. 12th European VLBI Network Symposium and Users
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Hagino, M., Ichimoto, K., Kimura, G., Nakatani, Y., Kawate, T., Shinoda,
K., Suematsu, Y., Hara, H., Shimizu, T.: 2014, Development of auniversal tunable filter for future solar observations, Proc. SPIE 9151,
Eds. R. Navarro; C. R. Cunningham; A. A. Barto, 91515V.
Hamano, S., Kobayashi, N., Kondo, S., Tsujimoto, T., Okoshi, K.,
Shigeyama, T.: 2014, Type-Ia SNR at z = 3.5 seen in the three lines ofsight toward the gravitationally lensed QSO B1422+231, AIP Conf.
Proc. 1594, Eds. S. Jeong, N. Imai, H. Miyatake, T. Kajino, 117-122.
Hanada, H., et al. including Tsuruta, S., Araki, H., Asari, K.,
Kashima, S., Tazawa, S., Noda, H., Matsumoto, K., Gouda, N.,
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in development of a small telescope for gravimetry, IAG Symp. on
Terrestrial Gravimetry: Static and Mobile Measurements Proc., Ed. A.
K. Krytova, 198-203.
Handa, T., et al. including Agata, H.: 2015, Mitaka “Taiyokei” (solar
system) walk; a collaborative science outreach program by institues,
local government, and shopping stores, XXVIIIth IAU General
Assembly, Highlights of Astronomy 16, Ed. T. Montmerle, 650.
Handa, T., Hata, K., Hara, T., Horaguchi, T., Hiramatsu, M., Arai, T.,
Sato, Y., Ohnishi, K.: 2015, A Global view of the Eclipse over the
Earth (GEE) in 2009 and 2012, XXVIIIth IAU General Assembly,
Highlights of Astronomy 16, Ed. T. Montmerle, 651.
Hara, T., Naoteru, G., Yano, T., Yamada, Y.: 2014, Evaluation ofcentroiding algorithm error for Nano-JASMINE, Proc. SPIE 9143, Eds.
J. M. Oschmann, M. Clampin, G. G. Fazio, H. A. MacEwen, 914354.
Hayano, Y., Akiyama, M., Hattori, T., Iwata, I., Kodama, T., Lai, O.,
Minowa, Y., Ono, Y. H., Oya, S., Takiura, K., Tanaka, I., Tanaka,
Y., Arimito, N.: 2014, ULTIMATE-SUBARU: project status, Proc.
SPIE 9148, Eds. E. Marchetti, L. M. Close, J.-P. Veran, 91482S.
Helminiak, K. G., Kuzuhara, M., Kudo, T., Tamura, M., Usuda,T., Hashimoto, J., Matsuo, T., McElwain, M. W., Momose, M.,
Tsukagoshi, T.: 2015, SEEDS — Direct Imaging Survey for
Exoplanets and Disks, 18th Cambridge Workshop on Cool Stars,
Stellar Systems, and the Sun, Eds. G. van Belle, H. C. Harris, 749-758.
Hibi, Y., Jiandong, S., Hua, Q., Matsuo, H., Lin, K., Jian, C., Peiheng, W.:
2014, Cryogenic GaN/AlGaN HEMT ICs and fabrication probabilityof monolithic sensor of super- and semiconductor devices, 11th Int.
Workshop on Low Temperature Electronics (WOLTE), 25-28.
Hirai, Y., Kajino, T., Hidaka, J., Shibagaki, S., Mathews, G. J.: 2014,
Chemo-dynamical evolution of colliding dwarf spheroidal galaxies, AIPConf. Proc. 1594, Eds. S. Jeong, N. Imai, H. Miyatake, T. Kajino, 58-63.
Hiramatsu, M.: 2015, Communicating ALMA with the Public in Japan,
XXVIIIth IAU General Assembly, Highlights of Astronomy 16, Ed. T.
Montmerle, 639.
Honma, M.: 2014, Maser Astrometry with VLBI and Galactic Structure,
Proc. 12th European VLBI Network Symposium and Users Meeting,Eds. A. Tarch, M. Giroletti, L. Feretti, 55.
Ichikawa, K., Imanishi, M., Ueda, Y., Nakagawa, T., Shirahata, M.,
Kaneda, H., Oyabu, S.: 2014, Unveiling Energy Contribution ofBuried AGN in Infrared Galaxie, Proc. of “Suzaku-MAXI 2014:
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Petre, K. Mitsuda, 323.
Iguchi, S., Iono, D.: 2014, What are scientifically valuable developments
for ALMA enhancement?, Proc. SPIE 9145, Eds. L. M. Stepp, R.
Gilmozzi, H. J. Hall, 914520.
Iizuka, R., et al. including Umemoto, T., Hirota, T., Hanayama, H.:
2014, Simultaneous Multi-Wavelength Observations of Large Flarestars, Proc. of “Suzaku-MAXI 2014: Expanding the Frontiers of the
X-ray Universe”, Eds. M. Ishida, R. Petre, K. Mitsuda, 154.
Inoue, T.: 2014, Three-Dimensional Simulation of Molecular Cloud
Formation, Astrophysics and Space Science Proc., 36, 165.
Ishikawa, R., Bando, T., Hara, H., Ishikawa, S., Kano, R., Kubo, M.,
Katsukawa, Y., Kobiki, T., Narukage, N., Suematsu, Y., Tsuneta,
S., Aoki, K., Miyagawa, K., Ichimoto, K., Kobayashi, K., Auchere,
F., CLASP team: 2014, Precision VUV Spectro-Polarimetry for Solar
Chromospheric Magnetic Field Measurements, ASP Conf. Ser. 489,
Solar Polarization 7, Eds. K. N. Nagendra, J. O. Stenflo, Zhongquan
Qu, M. Sampoorna, 319-321.
Itoh, R., Kawaguchi, K., Moritani, Y., Hashimoto, O., Kinugasa, K.,
Morihana, K., Takahashi, J., Itoh, Y., Imai, M., Watanabe, M., Nogami,D., Kawai, N.: 2014, MAXI J1932+091/Swift J193310.4+091141:
Optical Counterpart with Emission Lines, The Astronomer’s
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Jike, T., Tamura, Y., Shizugami, M.: 2014, VERA 2013 Geodetic
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Jovanovic, N., et al. including Guyon, O., Clergeon, C., Singh, G.,
Kudo, T., Minowa, Y., Hayano, Y., Lai, O., Kotani, T.: 2014,
Development and recent results from the Subaru coronagraphic
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I. S. McLean, H. Takami, 91471Q.
Jovanovic, N., Guyon, O., Martinache, F., Schwab, C., Cvetojevic, N.:
2014, How to inject light efficiently into single-mode fibers, Proc.
SPIE 9147, Eds. S. K. Ramsay, I. S. McLean, H. Takami, 91477P.
Kajino, T., Aoki, W., Balantekin, A. B., Cheoun, M.-K., Hayakawa,T., Hidaka, J., Hirai, Y., Kusakabe, M., Mathews, G. J., Nakamura,K., Pehlivan, Y., Shibagaki, S., Suzuki, T.: 2014, Cosmological andsupernova neutrinos, AIP Conf. Proc. 1604, Eds. B. Szczerbinska, R.
Allahverdi, K. Babu, B. Balantekin, B. Dutta, T. Kamon, J. Kumar, P.
Sandick, 193-200.
Kajino, T., Aoki, W., Cheoun, M.-K., Hayakawa, T., Hidaka, J., Hirai,
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Supernova neutrinos and explosive nucleosynthesis, AIP Conf. Proc.
1595, Eds. C. Spitaleri, L. Lamia, R. G. Pizzone, 84-97.
Kajino, T., Aoki, W., Cheoun, M.-K., Hayakawa, T., Hidaka, J.,

Hirai, Y., Mathews, G. J., Nakamura, K., Shibagaki, S., Suzuki, T.:2014, Supernova constraints on neutrino oscillation and EoS for
proto-neutron star, AIP Conf. Proc. 1594, Eds. S. Jeong, N. Imai, H.
Miyatake, T. Kajino, 319-325.
Kamata, Y., Nakaya, H., Kawanomoto, S., Miyazaki, S.: 2014, A
few phenomena on the fully depleted CCDs at the engineeringobservation of Hyper Suprime-Cam, Proc. SPIE 9154, Eds. A. D.
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Kamegai, K., Takanashi, N., Hiramatsu, M., Naito, S.: 2015,
Communicating Astronomy in a Metropolis and Disaster Area Activities of the Tenpla Project, XXVIIIth IAU General Assembly,
Highlights of Astronomy 16, Ed. T. Montmerle, 634.
Kameno, S., Miccolis, M., Sugimoto, M., Nakos, T.: 2014, Efficientspurious signal detection and mitigation in single-dish radio
spectroscopy, Proc. SPIE 9153, Eds. W. S. Holland, J. Zmuidzinas,
91532L.
Kameno, S., Mizuno, I., Nakamura, F., Kuroo, M., Kano, A.,
Kawaguchi, N., Shibata, K. M., Kuno, N., Takano, S., Kuji, S.:
2014, The software-based polarization spectrometer PolariS, Proc.
SPIE 9153, Eds. W. S. Holland, J. Zmuidzinas, 91532D.
Kawasaki, W., Eguchi, S., Shirasaki, Y., Komiya, Y., Kosugi, G.,
Ohishi, M., Mizumoto, Y.: 2014, Vissage: Recent Development
Status, ASP Conf. Ser. 485, Astronomical Data Analysis Software andSystems XXIII, Eds. N. Manset, P. Forshay, 285-288.
Kim, J. S., Kim, S. W.: 2014, Transition in the Outflow Evoution of theMassive Star-forming Region W75N, Proc. 12th European VLBI
Network Symposium and Users Meeting, Eds. A. Tarch, M. Giroletti,
L. Feretti, 42.
Kitagawa, Y., Ozaki, S., Motohara, K., Konishi, M., Takahashi, H.,
Tateuchi, K., Todo, S., Kato, N., Yoshikawa, T.: 2014, Concept andoptical design of the near-infrared integral field unit for SWIMS,
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Kiuchi, H.: 2014, A wide-bandwidth chromatic dispersion measurement
method, Proc. MWP 2014, TuED-5, IEICE, IEEE MTT-S, 383-385.
Kiuchi, H., Yamada, M., Sugimoto, M., Saito, M.: 2014, A Holography
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Antenna and the Measured Surface Deformation, Proc. SPIE 9145,
Eds. L. M. Stepp, R. Gilmozzi, H. J. Hall, 91454J.
Kobayashi, Y., Niwa, Y., Yano, T., Gouda, N., Hara, T., Yamada, Y.:
2014, Measurement of pixel response functions of a fully depleted
CCD, Proc. SPIE 9154, Eds. A. D. Holland, J. Beletic, 91541W.
Kodama, T., Hayashi, M., Koyama, Y., Tadaki, K., Tanaka, I.,
Shimakawa, R., Suzuki, T., Yamamoto, M.: 2015, Mapping andresolving galaxy formation at its peak epoch with Mahalo-Subaru andGracias-ALMA, Proc. IAU Symp. 309, B. L. Ziegler, F. Combes, H.
Dannerbauer, M. Verdugo.,
Koike, M., Furusawa, H., Takata, T., Price, P., Okura, Y., Yamada, Y.,
Yamanoi, H., Yasuda, N., Bickerton, S., Katayama, N., Mineo, S.,
Lupton, R., Bosch, J., Loomis, C.: 2014, Web-based data providing
system for Hyper Suprime-Cam, Proc. SPIE 9149, Eds. A. B. Peck, C.
R. Benn, R. L. Seaman, 914920.
Koike, M., Furusawa, H., Takata, T., Price, P., Okura, Y., Yamada, Y.,
Yamanoi, H., Yasuda, N., Bickerton, S., Katayama, N., Mineo, S.,
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Analysis Software and Systems XXIII, Eds. N. Manset, P. Forshay,
297-300.
Komatsubara, T., Kwon, Y. K., Moon, J. Y., Kim, Y.-K., Moon, C.-B.,
Ozawa, A., Sasa, K., Onishi, T., Yuasa, T., Okada, S., Kajino, T.:
Astrophysical S-factor for destructive reactions of lithium-7 in bigbang nucleosynthesis, AIP Conf. Proc. 1594, Eds. S. Jeong, N. Imai, H.
Miyatake, T. Kajino, 18-22.
Komatsubara, T., Yuasa, T., Onishi, T., Saito, Y., Okada, S., Sasa, K.,
Ozawa, A., Hayakawa, T., Shizuma, T., Kajino, T., Kubono, S.:
Study for Big-Bang Nucleosynthesis oncerning Lithum Isotopes,
Conf. Proc. of the 12th Asia Pacific Physics Conf., 013055.
Kotani, T., et al. including Tamura, M., Suto, H., Nishikawa, J., Aoki,
W., Usuda, T., Kurokawa, T., Morino, J.-I., Narita, N., Kokubo,
E., Hayano, Y., Izumiura, H., Kambe, E., Kudo, T., Kusakabe,N., Fukui, A., Guyon, O., Harakawa, H., Hayashi, M., Kuzuhara,
M., Takami, H., Takato, N., Terada, H.: 2014, Infrared Doppler
instrument (IRD) for the Subaru telescope to search for Earthlike planets around nearby M-dwarfs, Proc. SPIE 9147, Eds. S. K.
Ramsay, I. S. McLean, H. Takami, 914714.
Krumholz, M. R., Bate, M. R., Arce, H. G., Dale, J. E., Gutermuth, R.,
Klein, R. I., Li, Z.-Y., Nakamura, F., Zhang, Q.: 2014, Star Cluster
Formation and Feedback, Protostars and Planets VI, 243-266.
Kubo, M., et al. including Kano, R., Bando, T., Narukage, N., Ishikawa,
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Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
140419A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 16132, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
140629A: MITSuME Ishigakijima Optical Observation, GRB
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Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
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140705A: MITSuME Ishigakijima upper limits, GRB Coordinates
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Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
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140824A: MITSuME Ishigakijima upper limits, GRB Coordinates
Network, Circular Service, 16734, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
140907A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 16794, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
141031B: MITSuME Ishigakijima Upper limits, GRB Coordinates
Network, Circular Service, 17012, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
141109A: MITSuME Ishigakijima Upper limits, GRB Coordinates
Network, Circular Service, 17049, 1.

182

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Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
141121A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 17091, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
141121A: MITSuME Ishigakijima Optical Observation after 3 days,
GRB Coordinates Network, Circular Service, 17098, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB
141121A: MITSuME Ishigakijima Optical Observation after 7days,
GRB Coordinates Network, Circular Service, 17114, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140408A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16086, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140419A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 16131, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140423A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 16160, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140502A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16209, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140521A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16314, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140614B: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16405, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140706A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16524, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140916A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16823, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 141015A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
16917, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 141212A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
17172, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 141220A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
17204, 1.

Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 141225A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
17244, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB140907A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 16793, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150120B: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
17331, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150203A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
17395, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2015, GRB 150302A: MITSuMEOkayama upper limits, GRB Coordinates Network, Circular Service,
17537, 1.
Kusakabe, M., Kim, K. S., Cheoun, M.-K., Kajino, T., Kino, Y.,
Mathews, G. J.: New effects of a long-lived negatively charged
massive particle on big bang nucleosynthesis, AIP Conf. Proc. 1594,
Eds. S. Jeong, N. Imai, H. Miyatake, T. Kajino, 29-34.
Lai, O., Véran, J. P., Herriot, G., White, J., Ball, J., Trujillo, C.: 2014,
Altair performance and upgrades, Proc. SPIE 9148, Eds. E. Marchetti,
L. M. Close, J.-P. Veran, 914838.
Lanz, A., Arai, T., Battle, J., Bock, J., Cooray, A., Hristov, V., Korngut,
P., Lee, D., Mason, P., Matsumoto, T., Matsuura, S., Morford, T.,
Onishi, Y., Shirahata, M., Tsumura, K., Wada, T., Zemcov, M.:
2014, Studying extragalactic background fluctuations with the Cosmic
Infrared Background ExpeRiment 2 (CIBER-2), Proc. SPIE 9143, Eds.
J. M. Oschmann, M. Clampin, G. G. Fazio, H. A. MacEwen, 91433N.
Lardiere, O., Andersen, D., Blain, C., Bradley, C., Gamroth, D., Jackson,
K., Lach, P., Nash, R., Venn, K., Veran, J.-P.; Correia, C., Oya, S.,
Hayano, Y., Terada, H., Ono, Y. H., Akiyama, M.: 2014, Multiobject adaptive optics on-sky results with Raven, Proc. SPIE 9148,
Eds. E. Marchetti, L. M. Close, J.-P. Veran, 91481G.
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, Jansky VLA
S-band view of Hα emitters (HAEs) associated with a protocluster
4C23.56 at z = 2.5, Proc. IAU Symp. 309, B. L. Ziegler, F. Combes, H.
Dannerbauer, M. Verdugo, 287-288.
Lozi, J., Belikov, R., Thomas, S. J.; Pluzhnik, E., Bendek, E., Guyon, O.,
Schneider, G.: 2014, Experimental study of a low-order wavefront
sensor for high-contrast coronagraphic imagers: results in air and in
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Maruyama. T., Hidaka, J., Kajino, T., Yasutake, N., Kuroda, T., Cheoun,
M.-K., Ryu, C.-Y., Mathews, G. J.: Asymmetric Neutrino Emission
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Miura, N., Oh-ishi, A., Aoki, S., Mogaki, H., Kuwamura, S., Baba, N.,
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Moore, A. M., et al. including Suzuki, R., Ikenoue, B., Obuchi, Y.,
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186

XIII Publications, Presentations

K., Matsunaga, N., Sako, S., Kobayashi, N., Doi, M., Enomoto,T.: 2014, Faint meteor observation by large-format CMOS sensor
with 1.05-m Kiso schmidt telescope, The Meteoroids 2013, Eds.
T. J. Jopek, F. J. M. Rietmeijer, J. Watanabe, I. P. Williams, A. M.
University Press, 325-328.
Watanabe, T.: 2014 , The Solar-C Mission, Proc. SPIE 9143, Eds. J. M.
Oschmann, M. Clampin, G. G. Fazio, H. A. MacEwen, 91431O.
Woillez, J., Perrin, G., Lai, O., Reynaud, F., Baril, M., Dong, Y., Fedou,P., Kotani, T., Vergnole, S., Wizinowich, P.: 2014, Ohana, Improving
the Performances of Current Optical Interferometers’ Future Designs,
Eds. L. Arnold, H. Le Coroller, J. Surdej, 175-179.
Yaji, K., Tonooka, H., Shimojo, M., Tokimasa, N., Suzuki, D.,
Nakamichi, A., Shimoikura, I.: 2015, Hinode, the Sun, andPublic Outreach, XXVIIIth IAU General Assembly, Highlights ofAstronomy 16, Ed. T. Montmerle, 649.
Yamada, S., Suda, T., Komiya, Y., Aoki, W., Fujimoto, M. Y.: 2014,
Analysis of enrichment histories for elements and two modes of starformation during the early evolution of Milky Way, AIP Conf. Proc.
1594, Eds. S. Jeong, N. Imai, H. Miyatake, T. Kajino, 93-98.
Yamada, Y., et al. including Takata, T., Furusawa, H., Koike, M.,
Yamanoi, H., Mineo, S.: 2014, Development of a Database System
for Data Obtained by Hyper Suprime-Cam on the Subaru Telescope,
ASP Conf. Ser. 485, Astronomical Data Analysis Software andSystems XXIII, Eds. N. Manset, P. Forshay, 243-246.
Yamada, Y., et al. including Takata, T., Furusawa, H., Koike, M.,
Yamanoi, H., Mineo, S.: 2014, Development of database system fordata obtained by Hyper Suprime-Cam on Subaru Telescope, Proc.
SPIE 9149, Eds. A. B. Peck, C. R. Benn, R. L. Seaman, 91492I.
Yamamoto, R., Fukue, K., Matsunaga, N., Yasui, C., Hamano, S.,
Kobayashi, N., Tsujimoto, T., Kondo, S., Ikeda, Y.: 2014, SUBARU/
IRCS near-infrared spectroscopy of the young cluster GLIMPSE9 in
the inner galaxy, AIP Conf. Proc. 1594, Eds. S. Jeong, N. Imai, H.
Miyatake, T. Kajino, 64-69.
Yanagisawa, K., Shimizu, Y., Okita, K., Kuroda, D., Koyano, H.,
Tsutsui, H., Toda, H., Izumiura, H., Yoshida, M., Ohta, K., Kawai,N., Yamamuro, T.: 2014, Okayama astrophysical observatory wide
field camera, Proc. SPIE 9147, Eds. S. K. Ramsay, I. S. McLean, H.
Takami, 91476D.
Yonetoku, D., et al. including Okita, H., Yanagisawa, K.: 2014,
High-z gamma-ray bursts for unraveling the dark ages mission HiZGUNDAM, Proc. SPIE 9144, Eds. T. Takahashi, J.-W. A. den Herder,
M. Bautz, 91442S.
Yoshida T., Ebisawa K., Tsujimoto M., Ohsuga K., Nakagawa Y.,
Nomura M.: 2014, Spectral calculation through outflows aroundcompact objects and its hydrodynamic simulation, 40th COSPAR
Scientific Assembly, 3727.
Yoshii, T., Saito, Y., Yatsu, Y., Tachibana, Y., Kawai, N., Hanayama, H.,
Mitsume Telescope Team, Maxi Team: 2014, Optical observations ofa black hole binary MAXI J1910-057 with the MITSuMe Telescope,Proc. of “Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray
Universe”, Eds. M. Ishida, R. Petre, K. Mitsuda, 260.

5. Publications in English
Flaminio, R.: 2014, Thermal noise in laser interferometer gravitational
wave detectorsʼ in ‘Advanced Interferometers and the Search for
Gravitational Waves’, Springer International Publishing, Cham.
Fukushima, T.: 2014, “Elliptic functions and elliptic integrals forcelestial mechanics and dynamical astronomy” in Frontiers in
Relativistic Celstial Mechanics Vol.2: Applications and Expreiments(S.M. Kopeikin ed.), 187-226, de Gruyter, Berlin.
Mutschke, H., Posch, Th., Zeidler, S.: 2015, Contribution to the book
“Laboratory Astrochemistry”; Eds: Schlemmer, S., Giesen, T.,
Mutschke, H., Jaeger, C., Wiley-VCH, Weinheim.
Hesse, M., Aunai, N., Kuznetsova, M., Zenitani, S., Birn, J.: 2015, AGU
Geophysical Monograph 207: Chapter 15: Magnetic Reconnection
in Different Environments: Similarities and Differences (259–267),
Wiley, Weinheim.

6. Conference Presentations
Abe, S., Kero, J., Nakamura, T., Fujiwara, Y., Watanabe, J.: 2014,
Orbital evolution of Geminids and Quadrantids by middle and upper
atmosphere radar observations, Asteroids, Comets, Meteors 2014
(ACM 2014), (Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Abe, S., Kero, J., Nakamura, T., Fujiwara, Y., Watanabe, J.: 2014,
Statistical Distribution of the Solar System Dusts by Meteor Head
Echo Observations with the Large-aperture Radar, AOGS 11th Annual
Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Agata, H., Sekiguchi, K., Renchin T.: 2014, “You Are Galileo!”, 1st East
Asian Astronomical Education and Outreach Workshop, (Uranbatol,
Mongolia, July. 3-5, 2014).
Agata, H.: 2014, Astronomy as a part of culture, APRIM 2014: 12th AsiaPacific IAU Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Agata, H.: 2014, Education & Outreach Concept and Strategy at National
Astronomical Observatory of Japan (NAOJ), Astronomy Communication
Seminar, ePOD/ESO, (ESO, Munich, Germany, Aug. 25, 2014).
Agata, H.: 2014, Education and Outreach Connept of NAOJ, Opening
Ceremony of Majmaah University Astronomical Observatory,(Majmaah, Saudi Arabia, Dec. 16-18, 2014).
Akiyama, M., Oya, S., Ono, Y. H., Takami, H., Ozaki, S., Hayano, Y.,
Iwata, I., Hane, K., Wu, T., Yamamuro, T., Ikeda, Y.: 2014, TMTAGE: wide field of regard multi-object adaptive optics for TMT,
Adaptive Optics Systems IV, (Monreal, Canada, Jun. 22-27, 2014).
Akutsu, T., on behalf of KAGRA Collaboration: 2014, Large-scale
cryogenic gravitational-wave telescope in Japan: KAGRA, 10th Int.
LISA Symp., (Gainesville, Florida, USA, May 18-23, 2014).
Akutsu, T., et al.: 2014, Mitigation of Stray-Light Noise in KAGRA,
Gravitational Wave Advanced Detector Workshop 2014, (Takayama,
Japan, May 25-30, 2014).
Ando, M.: 2014, DECIGO and DECIGO Pathfinder, 10th Int. LISA
Symp., (Gainesville, Florida, USA, May 18-23, 2014).
Ando, M.: 2014, DECIGO: Space Gravitational-wave Antenna,
RESCEU APCosPA Summer School on Cosmology and Particle
Astrophysics, (Matsumoto, Japan, Aug. 3, 2014).

Antolin, P.: 2015, 1-D & 1.5-D MHD simulations of thermal instability,
ISSI Workshop - Bern, (Bern, Switzerland, Feb. 23-27, 2015).
Antolin, P.: 2014, Implications for coronal heating and magnetic fields
from coronal rain observations and modelling, 4th Int. Workshop on
small-scale solar magnetic fields, (Bairisch-Kölldorf, Austria, Apr.
23-25, 2014).
Antolin, P., Kleint, L., Pereira, T., Katsukawa, Y., De Pontieu, B.: 2014,
Coronal rain observed with IRIS, 40th COSPAR Scientific Assembly,(Moscow, Russia, Aug. 2-10, 2014).
Antolin, P., Vissers, G., Pereira, T., Rouppe van der Voort, L.,
Katsukawa, Y., De Pontieu, B., Scullion, E.: 2014, The MultiThermal and Multi-Strand Nature of Coronal Rain, 2014 Living Witha Star (LWS) Science Meeting, (Portland, OR, USA, Nov. 2-6, 2014).
Antolin, P., Vissers, G., Rouppe van der Voort, L., Pereira, T., Scullion,
E.: 2015, The multi-thermal and multi-stranded nature of coronalrain, ISSI Workshop - Bern, (Bern, Switzerland, Feb. 23-27, 2015).
Antolin, P., Yokoyama, T., Van Doorsselaere, T.: 2014, Fine strand-likestructure in the corona from MHD transverse oscillations, 4th Int.
Workshop on small-scale solar magnetic fields, (Bairisch-Kölldorf,
Austria, Apr. 23-25, 2014).
Antolin, P., Yokoyama, T., Van Doorsselaere, T.: 2014, Fine strandlike structure in the corona from MHD transverse oscillations, 40th
COSPAR Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Antolin, P., Yokoyama, T., Van Doorsselaere, T., Uitenbroek, H.,
Okamoto, T. J., De Pontieu, B.: 2014, Strand-like Structure andCharacteristic Spectral Signatures of Transversely Oscillating Flux
Tubes in the Solar Corona, 2014 Living With a Star (LWS) Science
Meeting, (Portland, OR, USA, Nov. 2-6, 2014).
Ao, Y., Matsuda, Y., Beelen, A., Henkel, C., Omont, A., Tatematsu, K.,
Zheng, Z., Cen, R., Weiss, A., Menten, K. M., Norris, R., De Breuck,
C., Lehnert, M., Mao, M., Francis, P., Lagache, G., Kovacs, A.:
2014, What powers Lyman alpha Blobs?, East Asia ALMA Science
Workshop, (Jeju, Korea, Jul. 14-17, 2014).
Aoki, W.: 2014, High-resolutions spectroscopy of extremely metalpoor stars found with SDSS and LAMOST, China-Subaru workshop,(Shanghai, China, Nov. 29-Dec. 1, 2014).
Araki, H., Kashima, S., Noda, H., Kunimori, H., Chiba, K., Otsubo,T., Utsunomiya, M., Matsumoto, Y.: 2014, Development of the retroreflector on the moon for the future Lunar Laser Ranging, JapaneseRussian Lunar-Planetary Workshop (JRLPW2014), (Mitaka, Tokyo,
Japan, Oct. 21/Mizusawa, Iwate, Japan, Oct. 24, 2014).
Araki, H., Kashima, S., Noda, H., Kunimori, H., Chiba, K., Otsubo,T., Utsunomiya, S., Matsumoto, Y.: 2014, Development of the retroreflector on the moon for the future Lunar Laser Ranging, 40th
COSPAR Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Barkin Y., Hanada, H., Barkin, M.: 2014, The drift and steps of thecenter of mass of the Moon with respect to the crust and interpretationof unexplained secular changes of the lunar orbit, The Fifth Moscow
Solar System Symp., (Moscow, Russia, Oct. 13-18, 2014).
Barkin, Y., Hanada, H.: 2014, About drift, oscillations and steps of thecenter of mass of the Moon, Japan Geoscience Union Meeting 2014,(Yokohama, Japan, Apr. 27-May 2, 2014).
Barkin, Y., Hanada, H., Matsumoto, K., Barkin, M.: 2014, The free andforced librations of the Moon with liquid shell and solid core, Japan
Geoscience Union Meeting 2014, (Yokohama, Japan, Apr. 27-May 2,2014).

XIII Publications, Presentations

187

Baty, H., Pétri, J., Zenitani, S.: 2014, Explosive reconnection of the
double tearing mode in relativistic plasmas: application to the Crabnebula, 41st EPS Conf. on Plasma Physics, (Berlin, Germany, Jun.
23-27, 2014).
Bigelow, B. C., Radovan, M. V., Bernstein, R. A., Onaka, P. M., Yamada,
H., Isani, S., Miyazaki, S., Ozaki, S.: 2014, Conceptual design of the
MOBILE imaging spectrograph for TMT, SPIE Astronomical Telescopes+ Instrumentation 2014, (Montreal, Canada, June 22-27, 2014).
Bowler, B. P., Liu, M. C., Shkolnik, E., Tamura, M.: 2015, The Outer
Architecture of M Dwarf Planetary Systems, AAS Meeting #225,(Seattle, WA, USA, Jan. 4-8, 2015).
Burns, R. A., Handa, T., Nagayama, T., Omodaka, T., Nakagawa, A.,
Nakanishi, H.: 2014, Trigonometric Distance to IRAS 20056+3350:
Massive Star Forming Region in the Solar Circle, APRIM 2014: 12th
Asia-Pacific IAU Regional Meeting, (Daejeon, South Korea, Aug.
18-22, 2014).
Chong, C.-C., Nakamura, F.: 2015, Evaluation of Single Dish Zeeman
Observation using ALMA Band-1 Reciever, The 3rd Workshop on
Large Aperture Sub/mm Telescope in the ALMA Era, (Mitaka, Tokyo,
Japan, Mar. 10-11, 2015).
Cheung, S. L.: 2014, International Year of Light, Public naming of
exoplanets, and the IAU Office for Astronomy Outreach, Annual
Meeting of the Astronomical Society of the Republic of China(Taiwan), (Nantou, Taiwan, May 23-25, 2014).
Cheung, S. L.: 2014, International Year of Light, Public naming of
exoplanets, Int. Planetarium Society Annual Meeting, (Beijing,
China, Jun. 23-27, 2014).
Cheung, S. L.: 2014, Light Pollution and the Night Sky Brightness
Measurment, 1st East Asian Astronomical Education and OutreachWorkshop, (Uranbatol, Mongolia, July. 3-5, 2014).
Cheung, S. L.: 2014, International Year of Light, Public naming of
exoplanets, and the IAU Office for Astronomy Outreach, 1st East
Asian Astronomical Education and Outreach Workshop, (Uranbatol,
Mongolia, July. 3-5, 2014).
Cheung, S. L.: 2014, International Year of Light, Public naming of
exoplanets, Asia Pacific IAU Regional Meeting 2014, (Daejeon,South Korea, Aug. 18-22, 2014).
Cheung, S. L.: 2014, International Year of Light, Public naming of
exoplanets, Middle East African Regional IAU Meeting 2014, (Beirut,
Leabon, Sep. 1-6, 2014).
Cheung, S. L.: 2014, Cosmic Light, Astronomy Education Alliance
Meeting 2014, (Lisbon, Portugal, Sep. 8-12, 2014).
Cheung, S. L.: 2014, International Year of Light, Public naming of
exoplanets, Annual Meeting of the Chinese Astronomical Society,(Xian, China, Oct. 27-29, 2014).
Cheung, S. L.: 2015, Light Pollution and the IAU Cosmic Light
Activities, Opening Ceremony of the Int. Year of Light 2015, (Paris,
France, Jan. 19-20, 2015).
Cheung, S. L.: 2015, Astronomy Outreach as Profession, East Asia
Young Astronomers Meeting 2015, (Taipei, Taiwan, Feb. 9-12, 2015).
Chibueze, J. O., Sakanoue, H., Nagayama, T., Omodaka, T., Handa, T.,
Kamezaki, T., Burns, R. A., Kobayashi, H., Nakanishi, H., Honma,
M., Ueno, Y.: 2014, Trigonometric Parallax of IRAS 22555+6213
with VERA: 3-Dimensional View of Sources Along the Same Lineof Sight, APRIM 2014: 12th Asia-Pacific IAU Regional Meeting,(Daejeon, South Korea, Aug. 18-22, 2014).

188

XIII Publications, Presentations

Chida, H.: 2014, Probing Very Early Stage of Radio Source Evolution in
NGC 1275 with VERA, 12th EVN Symposium 2014, (Cagliari, Italy,
Oct. 7-10, 2014).
Chida, H.: 2014, Probing very Early Stage of Radio Source Evolution
in NGC 1275 with VERA, Eating VLBI (East Asia To Italy: Nearly
Global VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Chida, H.: 2014, Long Term Monitoring 3C 84 with VERA at 22 GHzfrom 2011 to 2013, The 7th KaVA Joint Science WG Meeting,(Yamaguchi, Japan, Jul. 7-9, 2014).
Currie, T. M., Burrows, A. S., Girard, J., Cloutier, R., Fukagawa, M.,
Sorahana, S., Kuchner, M. J., Kenyon, S., Madhusudhan, N., Itoh, Y.,
Jayawardhana, R., Matsumura, S., Pyo, T.-S.: 2015, New, Near-to-Mid
Infrared High-Contrast Imaging of the Young Extrasolar Planets, HR
8799 bcde, AAS Meeting #225, (Seattle, WA, USA, Jan. 4-8, 2015).
Ezawa, H., Matsuo, H., Shibasaki, K., Iwai, K., Shimojo, M.,
Shinohara, N., Honma, M., Murata, Y.: 2015, Towards the Intensity
Interferometry at Terahertz Wavelengths, The 26th Int. Symp. on Space
Terahertz Technology, (Cambridge, MA, USA, Mar. 16-18, 2015).
Ferré-Mateu, A.: 2014, Hunting Relic galaxies in the Nearby Universe,
Getting a grip into galactic girths, (IPMU, Tokyo, Japan, Feb. 2-6, 2015).
Ferré-Mateu, A.: 2014, Traveling across cosmic time with MOIRCS,
2014 Subaru Autumn School, (NAOJ, Tokyo, Japan, Sep. 24-26, 2014).
Fissel, L. M., et al. including Nakamura, F.: 2015, Detailed Magnetic
Field Morphology of the Vela C Molecular Cloud from the
BLASTPol 2012 flight, AAS Meeting #225, (Seattle, WA, USA, Jan.
4-8, 2015).
Flaminio, R.: 2014, Status and Prospect of Gravitational Waves detectors,
The 24th workshop on General Relativity and Gravitation in Japan,(IPMU, Tokyo University, Kashiwa, Japan, Nov. 10-14, 2014).
Flaminio, R.: 2014, Status of KAGRA, 6th Einstein Telescope Symp.,(Lyon, France, Nov. 19, 2014).
Fujii, Y., Kojima, T., Kroug, M., Ogawa, H., Uzawa, Y.: An Integrated
Low-Noise Balanced SIS Mixer for 780-950GHz, 15th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia, (Mie,Japan, Dec. 15-17, 2014).
Fujimoto, K.: 2014, Wave Activities and Electron Acceleration near
the Separatrices of Magnetic Reconnection, US-Japan Workshop on
Magnetic Reconnection (MR 2014), (Tokyo, Japan, May 20-24, 2014).
Fujimoto, K.: 2014, Kinetic Modeling of Collisionless Magnetic
Reconnection in Three Dimension, 9th Annual Int. Conf. on
Numerical Modeling of Space Plasma Flows (ASTRONUM2014),(Long Beach, CA, USA, Jun. 23-27, 2014).
Fujimoto, K.: 2014, Waves and electron acceleration in the separatrix
regions of magnetic reconnection, 40th COSPAR Scientific Assembly,(Moscow, Russia, Aug. 2-10, 2014).
Furusawa, S., Nagakura, H., Sumiyoshi, K., Yamada, S.: 2014, The
influence of inelastic neutrino interactions with light clusters on corecollapse supernova simulations, State of the Art in Nuclear Cluster
Physics, (Yokohama, Japan, May 26-30, 2014).
Furusawa, S., Nagakura, H., Sumiyoshi, K., Yamada, S.: 2014, Inelastic
neutrino interactions with light nuclei in core-collapse supernova
simulations, Int. Symp. on Neutrino Nuclear Responses for Neutrino
Studies in Nuclei, (Osaka, Japan, Nov. 5-6, 2014).
Furusawa, S.: 2014, Equations of state at sub-nuclear densities andweak interactions in Supernovae, HPCI Int. Workshop on Study of
Neutron Stars and Core-Collapse Supernovae, (Wako, Japan, Dec.

16-20, 2014).
Furusawa, S.: 2015, Equation of State in Core-Collapse Supernova
Simulations, Multi-messengers from core-collapse supernovae 2015
(MMCOCOS2015) , (Arlington, VA, USA, Mar. 2-6, 2015).
Furusho, R., Shinoda, T., Terai, T., Watanabe, J.: 2014, Imaging
Polarimetric Survey on Cometary Dust Coma Activities, AOGS 11th
Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Furusho, R., Terai, T., Shinoda, T., Watanabe, J.: 2014, C/2012
S1 (ISON), C/2013 R1 (Lovejoy), and updates of the imaging
polarimetric survey, Asteroids, Comets, Meteors 2014 (ACM 2014),(Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Furusho, R., Terai, T., Watanabe, J.: 2014, Imaging Polarimetry of
C/2012 S1 (ISON) and C/2013 R1 (Lovely), AOGS 11th Annual
Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Galitzki, N., et al. including Nakamura, F.: 2015, Submillimeter Dust
Polarimetry with the BLAST-TNG Telescope, AAS Meeting #225,(Seattle, WA, USA, Jan. 4-8, 2015).
Getling, A., Ishikawa, R., Buchnev, A.: 2014, Formation of sunspot
groups: Do we see manifestations of the rising-tube mechanism?, 40th
COSPAR Scientific Assembly, (Moscow, Russia, Aug. 2-10, 2014).
Gilhool, S., Tamura, M., Usuda, T., Blake, C.: 2015, Stellar Radial
Velocities with Subaru/IRCS and an Ammonia Absorption Cell, AAS
Meeting #225, (Seattle, WA, USA, Jan. 4-8, 2015).
Gonzalez, A.: 2014, Study of optics for ALMA receivers, Chile-Japan
Academic Forum in U.Tokyo “Astrophysics and Astronomical
Instrumentation”, (Tokyo, Japan, Oct. 8-9, 2014).
Gonzalez, A., Fujii, Y., Kaneko, K., Kroug, M., Kojima, T., Kuroiwa,
K., Miyachi, A., Makise, M., Wang, Z., Asayama, S., Uzawa, Y.:
2014, ALMA band 10 (787-950 GHz): summary of the production of
73 receivers and first light results, SPIE Astronomical Telescopes +Instrumentation 2014, (Montreal, Canada, Jun. 22-27, 2014).
Gonzalez, A., Soma, T., Shiino, T., Kaneko, K., Uzawa, Y., Yamamoto,S.: 2014, Beam Measurement Characterization and Optics Tolerance
Analysis of a 900 GHz HEB receiver for the ASTE telescope, 39th
International Conference on Infrared, Millimeter, and Terahertz
Waves (IRMMWTHz14), (Tucson, USA, Sep. 14-19, 2014).
Gonzalez, A.: 2014, Contribution of NAOJ to ALMA band 1 optics
35-52 GHz, 15th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Mie, Japan, Dec. 15-17, 2014).
Gonzalez, A.: 2015, The need of compact profiled corrugated horns at
longer mm-waves (ALMA band 1) and at around 1 THz (band 10),The 26th Int. Symp. on Space Terahertz Technology, (Cambridge,
MA, USA, Mar. 16-18, 2015).
Gosic, M., Bellot-Rubio, L. R., Orozco-Suarez, D., Katsukawa, Y.:
2014, Flux emergence in the solar internetwork and its contribution to
the network, 40th COSPAR Scientific Assembly , (Moscow, Russia,
Aug. 2-10, 2014).
Gouda, N.: 2014, JASMINE/Nano-JASMINE/overview, CU9/GENIUS
plenary meeting, (Vienna, Austria, Jul. 7-9, 2014).
Gusev, A., Ping, J., Petrova, N., Hanada, H.: 2014, Fine effects ofspin-orbit dynamics of the Moon, Lunar radio beacons and Lunar
Navigation Almanac for ChangE-3/4, Luna-Glob-Resource,
SELENE-2 missions, The Fifth Moscow Solar System Symp.,(Moscow, Russia, Oct. 13-18, 2014).
Guyon, O.: 2014, Searching for Habitable Worlds and Life in the Universe
with Optics, 50yr anniversary of the college of optical sciences special

lecture, (University of Arizona, AZ, USA, Oct. 23, 2014).
Guyon, O.: 2014, Optical Tricks to find and study Exoplanets, OpticalSociety of America Student Leadership Chapter, (Tucson, AZ, USA,
Oct. 19, 2014).
Guyon, O.: 2014, Exoplanets, HawaiiCon 2014, (Kohala Coast, HI,
USA, Sep. 12-14, 2014).
Guyon, O.: 2014, Low-order Wave-front Sensing and Control, andPoint-spread-function Calibration, for Direct Imaging of Exoplanets,
Exo-PAG, (Boston, MA, USA, Jun. 6, 2014).
Guyon, O.: 2014, Imaging exoplanets with MKIDs on Subaru Telescope,
Institute for Astronomy University of Hawaii Tech Talk, (Hilo, HI,
USA, Apr. 17, 2014).
Hada, K.: 2014, Continuing EVN monitoring of HST-1 in the jet of
M87, 12th EVN Symposium 2014, (Cagliari, Italy, Oct. 7-10, 2014).
Hada, K.: 2014, M87, Eating VLBI (East Asia To Italy: Nearly Global
VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Hagiwara, Y., An, T., Jung, T. H., Roh, D. G., Zhang, M., Hao, L., Fujisawa,
K., Yonekura, Y., Baan, W., Kim, J. S., Kobayashi, H.: 2014, Current
Status of the EAVN Experiments, APRIM 2014: 12th Asia-Pacific IAU
Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Hagiwara, Y.: 2014, Status of VLBI in Japan and East Asia, Eating VLBI
(East Asia To Italy: Nearly Global VLBI) 2014, (Bologna, Italy, Oct.
13-14, 2014).
Hagiwara, Y.: 2014, Planning Italy-Japan observations, Eating VLBI (EastAsia To Italy: Nearly Global VLBI) 2014, (Bologna, Italy, Oct. 1314, 2014).
Hagiwara, Y.: 2014, Recent Status of the EAVN Experiments, The 7th
KaVA Joint Science WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Hagiwara, Y.: 2015, Recent status of EAVN experiments, The 8th KaVA
Joint Science WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Hagiwara, Y.: 2015, Future project EAVN/SKA, UST-GUAS Radio
astronomy winter school 2015, (Jeju, Korea, Feb. 10-13, 2015).
Hanada, H., Kikuchi, F., Noda, H., Matsumoto, K., Kono, Y., Tsuruta,
S., Asari, K., Araki, H., Kashima, S., Funazaki, K., Kunimori, H.,
Sasaki, S.: 2014, Present status of VLBI, ILOM and LLR for future
lunar missions, Chang’E Lunar Dynamics Workshop (CLDW2014),(Beijing, China, Jun. 2-7, 2014).
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., Petrova, N., Gusev, A.: 2014, Developmentof a telescope for observation of the lunar rotation and experimentson the ground, The Fifth Moscow Solar System Symp., (Moscow,
Russia, Oct. 13-18, 2014).
Hanada, H., Tsuruta, S., Asari, K., Chiba, K., Inaba, K., Funazaki, K.,
Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Araki, H., Noda,
H., Kashima, S.: 2014, Observations of lunar rotation on the Moon:
possibility and problems, Japan Geoscience Union Meeting 2014,(Yokohama, Japan, Apr. 27-May 2, 2014).
Hanada, H.: 2014, ILOM project: status and perspective, JapaneseRussian Lunar-Planetary Workshop (JRLPW2014), (Mitaka, Tokyo,
Japan, Oct. 21/Mizusawa, Iwate, Japan, Oct. 24, 2014).
Hanaoka, Y., Sakurai, T., IRMag Group: 2014, Solar Full-Disk
Polarization Measurement with the Fe I 15648 Line, IAU Symp. 305,
(Punta Leona, Costa Rica, Nov. 30-Dec. 5 2014).
Hanayama, H.: 2015, Observations of Solar System Objects with
Murikabushi 105cm Telescope, East Asia Young Astronomers

XIII Publications, Presentations

189

Meeting 2015, (Taipei, Taiwan, Feb. 9-12, 2015).
Handa, T., Soejima, T., Nakano, M., Omodaka, T., Nagayama, T.,
Chibeze, J. O., Baba, T., Kamezaki, T.: 2014, Star Formation and
the Molecular Gas Property in W4 West (AFGL333) Region, APRIM
2014: 12th Asia-Pacific IAU Regional Meeting, (Daejeon, South
Korea, Aug. 18-22, 2014).
Hara, H.: 2014, SOLAR-C Science Goals and Requirements, 2014
Living With a Star (LWS) Science Meeting, (Portland, OR, USA,
Nov. 2-6, 2014).
Hara, H.: 2014, Spectroscopy of Reconnection Inflow and Outflow in
Solar Flares, 40th COSPAR Scientific Assembly , (Moscow, Russia,
Aug. 2-10, 2014).
Hara, H.: 2014, The SOLAR-C Mission, 40th COSPAR Scientific
Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Hara, T., Naoteru, G., Yano, T., Yamada, Y.: 2014, Evaluation of centroiding
algorithm error for Nano-JASMINE, SPIE Astronomical Telescopes +Instrumentation 2014, (Montreal, Canada, June 22-27, 2014).
Haruyama, J., et al. including Iwata, T.: 2014, Unprecedented Zipangu
Underworld of the Moon Exploration (UZUME), AOGS 11th Annual
Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Hatsukade, B.: 2014, Two Gamma-ray Vursts from Dusty Regions with
Little Molecular Gas, Revolution in Astronomy with ALMA - The
3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Hayano, Y., Hayashi, S.: 2014, Subaru Telescope: Its instruments andlarge optics, Int. Symp. on Advances in Abrasive Technology, (Kona,
USA, Sep. 13, 2014).
Hayano, Y., Tamada, Y., Hattori, M., Oya, S., Kamei, Y., Murata, T.,
Hasebe, M.: 2014, Adaptive optics and its application to bioimaging,
JSAP-OSA Joint Symposia, (Sapporo, Japan, Sep. 17-20, 2014).
Hayashi, M., Kodama, T., Koyama, Y., Tadaki, K., Tanaka, I.,
Shimakawa, R., Matsuda, Y., Sobral, D., Best, P. N., Smail, I.: 2014,
Mapping the large-scale structure around a z = 1.46 galaxy cluster in
3-D, Multiwavelength-surveys: Galaxy formation and evolution fromthe early universe to today, (Dubrovnik, Criatua, May 12-16, 2014).
Helminiak, K. G., Konacki, M., Ratajczak, M., Jordán, A., Espinoza, N.,
Brahm, R., Kambe, E., Ukita, N.: 2014, Multiples among detachedeclipsing binaries from the ASAS catalog, Living Together: Planets,
Host Stars and Binaries, (Litomysl, Czech Rep., Sep. 8-12, 2014).
Herrera, C.: 2014, Star Formation and Turvulence in the Antennae
Overlap Region, Revolution in Astronomy with ALMA - The 3rdYear -, (Tokyo, Japan, Dec. 8-11, 2014).
Hesse, M., Aunai, N., Kuznetsova, M., Zenitani, S.: 2014, Electron
scale physics in magnetic reconnection, European Geosciences Union
General Assembly 2014, (Vienna, Austria, Apr. 27-May 2, 2014).
Hesse, M., Aunai, N., Zenitani, S., Kuznetsova, M., Birn, J.: 2014,
Symmetric and asymmetric reconnection: brothers separated at birth?,
US-Japan Workshop on Magnetic Reconnection (MR 2014), (Tokyo,
Japan, May 20-24, 2014).
Hesse, M., Aunai, N., Zenitani, S.: 2014, The transition from symmetricto asymmetric collisionless magnetic reconnection, 40th COSPAR
Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Hibi, Y., Jiandong, S., Hua, Q., Matsuo, H., Lin, K., Jian, C., Peiheng, W.:
2014, Cryogenic GaN/AlGaN HEMT ICs and fabrication probabilityof monolithic sensor of super- and semiconductor devices, 11th Int.
Workshop on Low Temperature Electronics (WOLTE), (Grenoble,
France, Jul. 7-9, 2014).

190

XIII Publications, Presentations

Hidaka, J., Kajino, T., Mathews, G. J., Suuki, J.: Supernova relicneutrino, HPCI Int. Workshop on Study of Neutron Stars and CoreCollapse Supernovae, (Wako, Japan, Dec. 16-20, 2014).
Hirai, Y., Ishimaru, Y., Saitoh, T. R., Fujii, M. S., Kajino, T.: 2014,
Enrichment of r-process elements in dwarf spheroidal galaxies withchemical and dynamical evolution model, Fourth Joint Meeting of the
Nuclear Physics Divisions of the American Physical Society and the
Physical Society of Japan, (Waikoloa, HI, USA, Oct. 7-11, 2014).
Hirata, N., Matsumoto, K., Kimura, J., Kitazato, K.: 2014, Constraining
the distribution of regolith deposits from the gravitational potential
field on small asteroids, Asteroids, Comets, Meteors 2014 (ACM2014), (Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Hirota, T., Kim, M. K., Honma, M.: 2015, ALMA observations of a hotmolecular disk around Orion KL Source I, Icy Grain Chemistry for
Formation of Complex Organic Molecules: From Molecular Clouds
to Protoplanetary Disks, Comets and Meteorites, (Tokyo, Japan, Mar.
5-7, 2015).
Hirota, T.: 2014, Observational study of star-forming regions with
VERA and beyond, Eating VLBI (East Asia To Italy: Nearly Global
VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Hirota. T.: 2014, Detection of a Hot Molecular Disk around a Massive
Protostar Candidate Orion KL Source I, Revolution in Astronomy
with ALMA - The 3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Hirota, T.: 2014, Status of SFRs sub-WG, The 7th KaVA Joint Science
WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Hirota, T.: 2015, Status of SFRs sub-WG, The 8th KaVA Joint Science
WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Hirota, T.: 2015, KaVA SFR large proposal, The 8th KaVA Joint Science
WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Hirota, T.: 2015, Star-formation and interstellar matter, UST-GUAS
Radio astronomy winter school 2015, (Jeju, Korea, Feb. 10-13, 2015).
Honma, M.: 2014, Maser Astrometry with VLBI and Galactic Structure,
12th EVN Symposium 2014, (Cagliari, Italy, Oct. 7-10, 2014).
Honma, M.: 2014, VERA Science Results, APRIM 2014: 12th Asia-Pacific
IAU Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Honma, M.: 2014, Super resolution imaging, Eating VLBI (East Asia To
Italy: Nearly Global VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Honma, M.: 2014, Summary and Conclusions, Eating VLBI (East Asia To
Italy: Nearly Global VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Honma, M.: 2014, Report from Astrometry WG, The 7th KaVA Joint
Science WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Honma, M.: 2015, VERA and the Galaxy, UST-GUAS Radio astronomy
winter school 2015, (Jeju, Korea, Feb. 10-13, 2015).
Hussmann, H., et al. including Araki, H., Namiki, N., Noda, H.:
2014, Investigation of the Galilean Moons with the Ganymede
Laser Altimeter (GALA), Japan Geoscience Union Meeting 2014,(Yokohama, Japan, Apr. 27-May 2, 2014).
Ikeya, M., Sakai, T., Kojima, T., Noguchi, T.: 2014, Reduction of
Leakage Current of Nb SIS Junctions by Adding an Extra Al Layer,
15th Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Mie, Japan, Dec. 15-17, 2014).
Imanishi, M.: 2015, High-spatial-resolution infrared imaging search forburied dusl AGNs in merging galaxies, Unveiling the AGN/Galaxy
Evolution Connection, (Puerto Varas, Chile, Mar. 9-13, 2015).
Inoue, T., Fukui, Y.: 2014, Formation of Massive Filamentary Cloud
Cores behind Shock Wave, Star Formation Across Space and Time,(Noordwijk, Netherlands, Nov. 11-14, 2014).
Inoue, T., Fukui, Y.: 2014, Formation of Massive Molecular Cloud Coresby Cloud Collision, East Asia Numerical Astrophysics Meeting,(Suwon, Korea, Sep. 15-19, 2014).
Inoue, T.: 2015, Dynamical Evolution of the Magnetzied Interstellar
Medium, Nagoya Workshop on the Interstellar Hydrogen, (Nagoya,Japan, Mar. 26-28, 2015).
Iono, D.: 2014, ALMA Science Highlights, General Assembly and
Scientific Symposium (URSI GASS), 2014 XXXIth URSI, (Beijing,
China, Aug. 16-23, 2014).
Iono, D.: 2014, ALMA/ASTE Future Development, 15th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia, (Mie,Japan, Dec. 15-17, 2014).
Iwai, K., Miyoshi, Y., Masuda, S., Tsuchiya, F., Morioka, A., Misawa, H.:
2014, Spectral Structures and Their Generation Mechanisms for Solar
Radio Type-I Bursts, 11th Annual General Meeting of Asia Oceania
Geosciences Society, (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Iwai, K., Shibasaki, K., Nozawa, S., Takahashi, T., Sawada, S.,
Kitagawa, J., Miyazaki, S., Kashiwagi, H.: 2014, Coronal Vector
Magnetic Field and the Plasma Beta Determined from the Nobeyama
Radioheliograph and Multiple Satellites Observations, 11th Annual
General Meeting of Asia Oceania Geosciences Society, (Sapporo,
Japan, Jul. 28-Aug. 1, 2014).
Iwata, I.: 2014, Constraints on LyC escape fraction from direct
observations of z ~ 3 galaxies, Lyman Continuum Leakage andCosmic Reionization, (Stockholm, Sweden, Aug. 13-15, 2014).
Iwata, T., Haruyama, J., Ohtake, M., Morota, T., Hasebe, N., Ishihara, Y.,
Hashizume, K., Katayama, Y., Kato, S., Kato, Y., Kono, I., Kusano,H., Nagaoka, H., Otsuki, M., Shirao, M., Tsumaki, T., Ueta, A.,
Watanabe, K.: 2014, A Study on the Sample Return Mission for Lunar
Highlands, Maria, and Vertical Holes, AOGS 11th Annual Meeting(AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Iwata, T., Kawakatsu, Y., Murakami, G., Ezoe, Y., Kameda, S., Keika, K.,
Arai, T., Matsuura, S., Imamura, T., Ogohara, K.: 2015, Solar System
Sciences using DESTINY, Symposium on Planetary Science 2015,(Sendai, Japan, Feb. 16-18, 2015).
Iwata, T., Kawakatsu, Y., Murakami, G., Ezoe, Y., Kameda, S., Keika,
K., Arai, T., Matsuura, S., Imamura, T., Ogohara, K.: 2015, Studies
on solar system explorations using DESTINY: the Demonstration andExperiments of Space Technology for INterplanetary VoYage, The
46th Lunar and Planetary Science Conf., (The Woodlands, TX, USA,
Mar. 16–20, 2015).
Iwata, T., Kawakatsu, Y.: 2014, A study for candidate scientificinstruments for DESTINY: Demonstration and Experiment of SpaceTechnology for Interplanetary Voyage, Japan Geoscience Union
Meeting 2014, (Yokohama, Japan, Apr. 27-May 2, 2014).
Iwata, T., Kitazato, K., Abe, M., Arai, T., Nakauchi, Y., Nakamura,T., Hiroi, T., Matsuoka, M., Matsuura, S., Ozaki, M., Watanabe,S.: 2014, Performances of Flight Model of NIRS3: the Near
Infrared Spectrometer on Hayabusa-2, AOGS 11th Annual Meeting(AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Iwata, T., Kitazato, K., Abe, M., Arai, T., Nakauchi, Y. Nakamura,T., Osawa, T., Hiroi, T., Matsuoka, M., Matsuura, S., Ozaki, M.,
Watanabe, S.: 2014, Performances of Flight Model of NIRS3: theNear Infrared Spectrometer on Hayabusa-2, European Planetary
Science Congress 2014, (Cascais, Portugal, Sep. 7–12, 2014).

Iwata, T., Matsumoto, K., Ishihara, Y., Kikuchi, F.: 2014, Measurementsof Martian rotational variations using Mars Entry-Descent-Landing
and Surface Exploration Technologies Demonstrator, Japanese-Russian
Lunar-Planetary Workshop (JRLPW2014), (Mitaka, Tokyo, Japan, Oct.
21/Mizusawa, Iwate, Japan, Oct. 24, 2014).
Izumiura, H.: 2014, AKARI Observations of Evolved Satrs, The
Universe in the light of AKARI Synergy with future Large Space
Telescopes, (Oxford, UK, Jul. 9-11, 2014).
Izumiura, H.: 2014, EAPSNET: an East-Asian Planet Search NETwork,
APRIM 2014: 12th Asia-Pacific IAU Regional Meeting, (Daejeon,South Korea, Aug. 18-22, 2014).
Kajino, T.: Big-Bang and Supernova Neutrinos and Nucleosynthesis, 5th
Carpathian Summer School in Physics, (Sinaia, Romania, Jun. 13-26,
2014).
Kajino, T.: Supernova as a Laboratory for Element Genesis and Neutrino
Physics, 18th Int. Workshop on Astro-Nuclear Physics, (Seoul, Korea,
Aug. 18-20, 2014).
Kajino, T.: Roles of Nuclear Charge-Current responses in Supernova
Nucleosynthesis and Neutrinos, Int. Symp. on Neutrino Nuclear Responses
for Neutrino Studies in Nuclei, (Osaka, Japan, Nov. 5-6, 2014).
Kajino, T.: R-process in Neutron Star Mergers and Supernovae, 13th Int.
Symp. on Nuclei in the Cosmos, (Debrecen, Hungary, Sep. 7-11, 2014).
Kajino, T.: Critical roles of fission in the r-process nucleosynthesis inbinary neutron-star mergers and Galactic evolution, 22nd ASRC Int.
Workshop on Nuclear Fission and Exotic Nuclei, (Tokai, Japan, Dec.
3-5, 2014).
Kajino, T.: R-process in Neutron Star Mergers and Supernovae, Nuclear
Physics and Astrophysics of Neutron-Star Mergers and Supernovae,
and the Origin of R-Process Elements, (Trento, Italy, Sep. 8-12, 2014).
Kajino, T.: Big-Bang and Supernova Neutrinos and Nucleosynthesis,
NUBA Int. Conf. Nuclear Physics and Astrophysics, (Antalya,
Turkey, Sep. 15-21, 2014).
Kajino, T.: Element Genesis in the Universe, Int. Workshop on Nuclear
Astrophysics, (Beijing, China, Jan. 21-23, 2015).
Kameno, S., Miccolis, M., Sugimoto, M., Nakos, T.: 2014, Efficientspurious signal detection and mitigation in single-dish radio
spectroscopy, SPIE Astronomical Telescopes + Instrumentation 2014,(Montreal, Canada, June 22-27, 2014).
Kameno, S., Mizuno, I., Nakamura, F., Kuroo, M., Kano, A., Kawaguchi,N., Shibata, K. M., Kuno, N., Takano, S., Kuji, S.: 2014, The softwarebased polarization spectrometer PolariS, SPIE Astronomical Telescopes+ Instrumentation 2014, (Montreal, Canada, June 22-27, 2014).
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.: 2014, 22 GHz Monitoringof Sgr A* during the G2 Peri-Center Passing with Japanese VLBI
Network, APRIM 2014: 12th Asia-Pacific IAU Regional Meeting,(Daejeon, South Korea, Aug. 18-22, 2014).
Kameya, O.: 2014, Activity of the Mizusawa 10m Radio Telescope, The 7th
KaVA Joint Science WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Kameya, O.: 2015, Activity of the Mizusawa 10m radio telescope andpulsar observations using VERA, The 8th KaVA Joint Science WG
Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Kano, R., CLASP team: 2014, Exploration of Magnetic Fields in
Solar Chromosphere by High-Precision Lyman-Alpha Polarimetry,
Astronomical Polarimetry 2014, (Grenoble, France, May 26-30, 2014).

XIII Publications, Presentations

191

Kano, R., Ishikawa, R., Narukage, N., Bando, T., Katsukawa, Y.,
Kubo, M., Ishikawa, S., Kobayashi, K., Trujillo Bueno, J., Auchère,F., CLASP team: 2014, Chromospheric Lyman-alpha spectropolarimeter (CLASP), 40th COSPAR Scientific Assembly , (Moscow,
Russia, Aug. 2-10, 2014).
Karatsu, K., Kojima, T., Sekimoto, Y., Nitta, T., Sekine, M., Sekiguchi,
S., Okada, T., Shu, S., Noguchi, T., Uzawa, Y., Matsuo, H., Kiuchi,
H., Naruse, M.: 2014, Development of Superconducting Low Pass
Filter for Ultra Low Noise Measurement System of Microwave
Kinetic Inductance Detector, The 25th Int. Symp. on Space Terahertz
Technology, (Moscow, Russia, Apr. 27-30, 2014).
Kashikawa, N.: 2014, High-z science summary, Evolution of SMBHs
with HSC: First results from initial dataset, (Academia Sinica,
Taiwan, Dec. 18-20, 2014).
Kashikawa, N.: 2014, TMT science cases, 3rd Annual Symp. of theInnovative Area on Multi-messenger Study of Gravitational Wave
Sources, (Hiroshima, Japan, Dec. 19-21, 2014).
Kasuga, M.: 2014, Different Photospheric Magnetic Properties atFootpoints between Hot and Warm Coronal Loops in Active Regions,2014 Living With a Star (LWS) Science Meeting, (Portland, OR,
USA, Nov. 2-6, 2014).
Kasuga, T., Usui, F., Ootsubo, T., Hasegawa, S., Kuroda, D., Shirahata,
M., Okamura, N.: 2014, High-albedo C-complex outer-belt asteroids:
The near-infrared spectra, Asteroids, Comets, Meteors 2014 (ACM2014), (Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Kataoka, A.: 2014, Planetesimal formation via fluffy dust aggregates,
The influence of material and temperature on the dust coagulation in
protoplanetary disks, (Sapporo, Japan, Aug. 5-7, 2014).
Kataoka, A.: 2015, Observational properties of fluffy dust aggregates,
Transition Disks and Planet Formation, (Lorentz Center, Leiden,
Nederland, Mar. 2-6, 2015).
Katsukawa, Y.: 2014, Properties of small-scale jets in the solar
chromosphere revealed through spectroscopic observations, 11th
Annual General Meeting of Asia Oceania Geosciences Society,(Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Katsukawa, Y.: 2014, Progress in our understanding of the solar surface
magnetism provided by HINODE, 11th Annual General Meeting of Asia
Oceania Geosciences Society, (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Katsukawa, Y., Otsuji, K., Tarbell, T.: 2014, Study of High-Speed Flows
Associated with Chromospheric Transients Around a Sunspot, 2014
Living With a Star (LWS) Science Meeting, (Portland, OR, USA,
Nov. 2-6, 2014).
Kawabe, R.: 2014, Extremely Dense Core: Evidence for a First
Hydrostatic Core, Revolution in Astronomy with ALMA - The 3rdYear -, (Tokyo, Japan, Dec. 8-11, 2014).
Kawaguchi, T.: 2015, Towards Radio Surveys of Massive Black Holes,
The 3rd Workshop on Large Aperture Sub/mm Telescope in the
ALMA Era, (Mitaka, Tokyo, Japan, Mar. 10-11, 2015).
Kawaguchi, T., Saito, Y., Miki, Y., Mori, M.: 2014, Relics of Galaxy
Merging: Optical Emission from a Star Cluster Trailing a Wandering
Massive Black Hole in the M31 Halo, Evolution of SMBHs with
HSC: First results from initial dataset, (Academia Sinica, Taiwan,
Dec. 18-20, 2014).
Kawaguchi, T., Saito, Y., Miki, Y., Mori, M.: 2015, Relics of Galaxy
Merging: Observational Predictions for a Wandering Massive Black
Hole and Accompanying Star Cluster in the M31 Halo, Black Holes

192

XIII Publications, Presentationsin Dense Star Clusters, (Aspen, USA, Jan. 17-22, 2015).
Kawashima, T., Ogawa, T., Ono, T., Oda, H., Matsumoto, R.: 2014,
Global Three-Dimensional MHD Simulations of Disk Dynamo,
4th East-Asian School and Workshop on Laboratory, Space,
Astrophysical Plasmas, (Harbin, China, Jul. 28-Aug. 1, 2014).
Kawashima, T., Ogawa, T., Ono, T., Oda, H., Matsumoto, R.: 2014,
X-Ray Flares Induced by the Magnetic Reconnection in Black Hole
Accretion Flows, US-Japan Workshop on Macnetic Reconnection,(Tokyo, Japan, May 20-23, 2014).
Kero, J., Nakamura, T., Szasz, C., Kastinen, D., Watanabe, J.,
Yamamoto, M., Fujiwara, Y., Abo, M., Tanaka, Y., Abe, S.: 2014,
Shigaraki middle and upper atmosphere radar meteor-head-echo
database, Asteroids, Comets, Meteors 2014 (ACM 2014), (Helsinki,
Finland, Jun. 30-Jul. 4, 2014).
Kikuchi, F.: 2014, Some effective methods and instruments for VLBI
observation of lunar and planetary explorer, Japanese-Russian LunarPlanetary Workshop (JRLPW2014), (Mitaka, Tokyo, Japan, Oct. 21/
Mizusawa, Iwate, Japan, Oct. 24, 2014).
Kikuchi, F., Matsumoto, K.: 2014, Optimal configuration of dualspacecraft radio occultation observation for future lunar ionosphere
exploration, European Geosciences Union General Assembly 2014,(Vienna, Austria, Apr. 27-May 2, 2014).
Kikuchi, K.: 2014, ALMA Future Development, 15th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia, (Mie,Japan, Dec. 15-17, 2014).
Kim, J. H.: 2015, The Effect of Large-Scale Structure on the Formationof Disk Galaxies : Specific Angular Momentum Point of View, AAS
Meeting #225, (Seattle, WA, USA, Jan. 4-8, 2015).
Kim, J. S.: 2014, Transition in the Outflow Evoution of the Massive
Star-forming Region W75N, 12th EVN Symposium 2014, (Cagliari,
Italy, Oct. 7-10, 2014).
Kim, J. S.: 2014, Preliminary Report of Monitoring Cyg X-3 to Catch
Flares, The 7th KaVA Joint Science WG Meeting, (Yamaguchi,
Japan, Jul. 7-9, 2014).
Kim, J. S.: 2015, Transition of Outflow Morphology in the Massive Starforming Region W75N, The 8th KaVA Joint Science WG Meeting,(Gyeongju, Korea, Jan. 13-15, 2015).
Kim, K. T., Hirota, T., KVN+VERA Star Formation Working Group:
2014, Observational Studies of Star-forming Regions with KVN
and KVN+VERA, APRIM 2014: 12th Asia-Pacific IAU Regional
Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Kitagawa, Y., Ozaki, S., Motohara, K., Konishi, M., Takahashi, H.,
Tateuchi, K., Todo, S., Kato, N., Yoshikawa, T.: 2014, Concept andoptical design of the near-infrared integral field unit for SWIMS,Advances in Optical and Mechanical Technologies for Telescopes
and Instrumentation, (Monreal, Canada, Jun. 23-27, 2014).
Kitazato, K., Iwata, T., Abe, M., Ohtake, M., Matsuura, S., Arai, T.,
Nakauchi, Y., Tsumura, K., Hirata, N., Senshu, H., Watanab, S.: 2015,
In-Flight Performance of the Hayabusa-2 Near-Infrared Spectrometer(NIRS3), The 46th Lunar and Planetary Science Conf., (The
Woodlands, TX, USA, Mar. 16–20, 2015).
Kobayashi, H., Hagiwara, Y., Cho, S. H., Kim, J. S., Hong, X., Shen,
Z. Q., EAVN Team: 2014, Status and Feature of East Asian VLBI
Network, APRIM 2014: 12th Asia-Pacific IAU Regional Meeting,(Daejeon, South Korea, Aug. 18-22, 2014).
Kobayashi, Y., Niwa, Y., Yano, T., Gouda, N., Hara, T., Yamada, Y.:2014, Measurement of pixel response functions of a fully depleted
CCD, SPIE Astronomical Telescopes + Instrumentation 2014,(Montreal, Canada, June 22-27, 2014).
Kodama, T.: 2014, The ancestors of cluster early-type galaxies seen in
proto-clusters around HzRGs, International Conference on Powerful
AGN, (Port Douglas, Australia, Jun. 20, 2015).
Kodama, T.: 2014, Mapping and resolving galaxy formation at its
peak epoch with Mahalo-Subaru and Gracias-ALMA, Int. Conf. on
Galaxies in 3D across the Universe, (Vienna, Austria, Jul. 10, 2014).
Kodama, T.: 2015, Proto-clusters at high-z: structures and stellar
populations, Int. Conf. on Back at the Edge of the Universe, (Sintra,
Portugal, Mar. 19, 2015).
Kojima T., Fujii, Y., Soma, T., Yamamoto, S., Uzawa, Y.: 2015,
Development of a Terahertz HEB Mixer-Amplifier with SiGe HBTs,
The 26th Int. Symp. on Space Terahertz Technology, (Cambridge,
MA, USA, Mar. 16-18, 2015).
Kojima T., Kroug, M., Gonzalez, A., Asayama, S., Uzawa, Y.: 2015,
Design of Superconducting On-chip Frequency Multiplexers fora Low-noise Multiband Receiver, The 26th Int. Symp. on Space
Terahertz Technology, (Cambridge, MA, USA, Mar. 16-18, 2015).
Kojima, T., Fujii, Y., Soma, T., Yamamoto, S., Uzawa, Y.:
2014, Development of a Terahertz Receiver Incorporating a
Superconducting Mixer Integrated with a SiGe Low-Noise Amplifier,15th Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Mie, Japan, Dec. 15-17, 2014).
Kojima, T., Gonzalez, A., Uzawa, Y.: 2014, Design and Loss
Measurement of Substrate Integrated Waveguides at Terahertz
Frequencies, The 25th Int. Symp. on Space Terahertz Technology,(Moscow, Russia, Apr. 27-30, 2014).
Kokubo, E.: 2014, Formation of Close-in Super-Earths by Giant Impacts,
Exoplanetary Science, (Quy Nhon, Vietnam Apr. 20-26, 2014).
Kokubo, E.: 2014, Formation of Terrestrial Planets from Protoplanets:
Effects of System Size and Position, Complex Planetary Systems,(Namur, Belgium, Jul. 7-11, 2014).
Kokubo, E.: 2014, Exploring Planet Fromation by N-Body Simulations,
Stellar N-Body Dynamics, (Sexten, Italy, Sep. .8-12, 2014).
Kokubo, E.: 2014, Formation of Close-in Super-Earths by Giant
Impacts, German-Japanese Meeting Exo-Planets and their Formation,(Heidelberg, Germany, Nov. 4-7, 2014).
Kolotkov, D., Nakariakov, V., Nisticò, G., Shibasaki, K., Kupriyanova,
E.: 2014, Spatial Structure of Multimode Oscillations in a Solar Flareon 14 May 2013 in EUV and Radio Bands, 40th COSPAR Scientific
Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Kotake, K.: 2014, Multimessenger observables from core-collapse
supernovae: some strategies, Brainstorming meeting, (Basel,
Switzerland, Sep. 23-Oct. 3, 2014).
Kotake, K.: 2014, Multimessenger observables from multi-D corecollapse supernova simulations, Nuclear Physics and Astrophysics of
Neutron-Star Mergers and Supernovae, and the Origin of R-Process
Elements, (Trento, Italy, Sep. 8-12, 2014).
Kotake, K.: 2014, Multi-D Core-Collapse Supernova Explosions andthe Multi-Messenger Signatures, 40th COSPAR Scientific Assembly ,(Moscow, Russia, Aug. 2-10, 2014).
Kotake, K.: 2015, International Workshop on Neutrino Physics andAstrophysics, Mimar Sinan Fine Arts University, (Istanbul, Turkey,
Mar. 16-20, 2015).

Kozak, P., Watanabe, J., Sato, M.: 2014, Anomalous meteors fromthe observations with super-isocon TV systems, Asteroids, Comets,
Meteors 2014 (ACM 2014), (Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Kozuki, Y., Ishida, H., Hasegawa, Y., Kuroiwa, K., Kimura, K.,
Muraoka, K., Maezawa, H., Ohnishi, T., Ogawa, H., Asayama, S.,
Minamidani, T., Kojima. T., Fujii, Y., Noguchi, T., Nakajima, T.,
Kato, C., Fujii, Y., Yamamoto, H.: 2015, Development for a wideband
100 GHz SIS mixer, The 26th Int. Symp. on Space Terahertz
Technology, (Cambridge, MA, USA, Mar. 16-18, 2015).
Kozuki, Y., Ishida, H., Hasegawa, Y., Kuroiwa, K., Kimura, K., Muraoka,
K., Maezawa, H., Ohnishi, T., Ogawa, H., Asayama, S., Minamidani,T., Kojima. T., Fujii, Y., Noguchi, T., Nakajima, T., Kato, C.,
Kuwahara, T., Fujii, Y., Yamamoto, H.: 2014, 100 GHz SIS mixer withwide IF bandwidth, 15th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Mie, Japan, Dec. 15-17, 2014).
Kubo, M., et al. including Kano, R., Ishikawa, R., Bando, T., Narukage,N., Katuskawa, Y., Isahikawa, S., Suematsu, Y., Hara, H., Giono, G.:2014, A Sounding Rocket Experiment for the Chromospheric LymanAlpha Spectro-Polarimeter (CLASP), IAU Symp. 305, (Punta Leona,
Costa Rica, Nov. 30-Dec. 5 2014).
Kubo, M., et al. including Kano, R., Bando, T., Narukage, N.,
Ishikawa, R., Katsukawa, Y., Ishikawa, S., Suematsu, Y., Hara,H.: 2014, Exploration of Magnetic Fields in Solar Chromosphere by
a Sounding Rocket Experiment for the Chromospheric Lyman-Alpha
Spectro-Polarimeter (CLASP), 11th Annual General Meeting of Asia
Oceania Geosciences Society, (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Kubo, M., Low, B. C., Lites, B. W.: 2014, Unresolved mixed polarity
magnetic fields at flux cancellation site in solar photosphere at 0 ″.3
spatial resolution, IAU Symp. 305, (Punta Leona, Costa Rica, Nov.
30-Dec. 5 2014).
Kubo, Y., Watari, S., Ishii, M., Ishibasashi, H., Iwai, K.: 2014, Developmentof New Solar Radio Telescope in NICT, 40th COSPAR Scientific
Assembly, (Moscow, Russia, Aug. 2-10, 2014).
Kudoh, T., Yokoyama, T., Kudoh, Y., Matsumoto, R.: 2014, Numerical
Simulation of Cosmic-ray Parker Instability, US-Japan Workshop on
Magnetic Reconnection (MR 2014), (Tokyo, Japan, May 20-24, 2014).
Kudoh, T., Yokoyama, T., Kudoh, Y., Matsumoto, R.: 2014, Nonlinear
Evolution of Cosmic Ray Parker Instability, Plasma 2014, (Niigata,Japan, Nov. 18-21, 2014).
Kumamoto, A., Ishiyama, K., Kobayashi, T., Oshigami, S., Haruyama, J.:
2014, Determination of the Dielectric Constant of the Lunar Surface
Based on the Radar Echo Intensity Observed by the Kaguya, AOGS 11th
Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Kumamoto, A., Ishiyama, K., Oshigami, S., Haruyama, J., Goto, Y.: 2015,
High Permittivity Regions in Oceanus Procelluram and Mare Imbrium
Found by · SELENE (Kaguya), The 46th Lunar and Planetary Science
Conf., (The Woodlands, TX, USA, Mar. 16–20, 2015).
Kupriyanova, E., Shibasaki, K., Melnikov, V.: 2014, Spatially Resolved
Minute Periodicities in Flaring Microwave Emission, 40th COSPAR
Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Kuznetsov, A., Reznikova, V., Van Doorsselaere, T., Antolin, P.:
2014, Simulations of gyrosynchrotron microwave emission froman oscillating magnetic loop, 40th COSPAR Scientific Assembly ,(Moscow, Russia, Aug. 2-10, 2014).
Liu, W., Antolin, P.: 2015, Prominences & coronal rain - Similarities anddifferences, ISSI Workshop - Bern, (Bern, Switzerland, Feb. 23-27, 2015).

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Liu, W., De Pontieu, B., Okamoto, J., Vial, J.-C., Title, A., Antolin, P.,
Berger, T., Uitenbroek, H.: 2014, First High-resolution Spectroscopic
Observations by IRIS of a Fast Prominence Eruption Associated witha CME on 2014-May-09, 2014 Living With a Star (LWS) Science
Meeting, (Portland, OR, USA, Nov. 2-6, 2014).
Liu, W., Berger, T., Antolin, P., Schrijver, K.: 2014, IRIS Observations ofCoronal Rain and Prominences: Return Flows of the ChromosphereCorona Mass Cycle, American Astronomical Meeting 2014, (Boston,
USA, Jun. 1-5, 2014).
Lundock, R.: 2014, Ramsey Lundock on Writing for Sci Fi, HawaiiCon
2014, (Kohala Coast, HI, USA, Sep. 12-14, 2014).
Lundock, R., Plait, P., Ferdowsi, B., Hamond, G. B.: 2014, Putting theScience in Sci Fi, HawaiiCon 2014, (Kohala Coast, HI, USA, Sep.
12-14, 2014).
Matsuda Y.: 2014, The ALMA Patchy Deep Survey: A blind search for[C II] emitters at z ~ 4.5, Revolution in Astronomy with ALMA - The
3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Matsuda, Y.: 2014, The ALMA Patchy Deep Survey: A blind search for[C II] emitters at z ~ 4.5, Transformational Science in the ALMA Era:
Multi-Wavelength Studies of Galaxy Evolution, (Charlottesville, VA,
USA, Aug. 4-7, 2014).
Matsumoto, K.: 2014, Geodetic observations and insights into theinterior, GALA General Meeting, (Tokyo, Japan, May 7-8, 2014).
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, The 46th Lunar and Planetary Science Conf., (The
Woodlands, TX, USA, Mar. 16–20, 2015).
Matsumoto, K., Yamada, R., Kikuchi, F., Kamata, S., Ishihara, Y.,
Iwata, T., Hanada, H., Sasaki, S.: 2014, Lunar internal structure
modeling using Apollo seismic travel time data and the latest
selenodetic data from GRAIL and LLR, AGU Fall Meeting 2014, (SanFrancisco, CA, USA, Dec. 15-19, 2014).
Matsumoto, K., Yamada, R., Kikuchi, F., Kamata, S., Iwata, T.,
Ishihara, Y., Hanada, H., Sasaki, S.: 2014, Deep Interior Structureof the Moon Inferred from Apollo Seismic Data and the Latest
Selenodetic Data, AOGS 11th Annual Meeting (AOGS2014),(Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Matsumoto, K., Yamada, R., Kikuchi, F., Kashima, S., Ishihara, Y.,
Iwata, T., Hanada, H., Sasaki, S.: 2014, Lunar internal structure
modeling using Apollo seismic travel time data and the latest
selenodetic data, The Fifth Moscow Solar System Symp., (Moscow,
Russia, Oct. 13-18, 2014).
Matsumoto, K., Yamada, R., Kikuchi, F., Kashima, S., Ishihara, Y.,
Iwata, T., Hanada, H., Sasaki, S.: 2014, Lunar internal structure
inferred from Apollo seismic travel time data and the latest
selenodetic data, Japanese-Russian Lunar-Planetary Workshop(JRLPW2014), (Mitaka, Tokyo, Japan, Oct. 21/Mizusawa, Iwate,
Japan, Oct. 24, 2014).
Matsumoto, N.: 2014, ALMA proposals from the SFR science sub-WG,
The 7th KaVA Joint Science WG Meeting, (Yamaguchi, Japan, Jul.
7-9, 2014).
Matsumoto, N.: 2015, Imaging test of 44 GHz methanol maser with
KaVA, The 8th KaVA Joint Science WG Meeting, (Gyeongju, Korea,
Jan. 13-15, 2015).
Matsuo, H.: 2014, Photon Statistics for Space Terahertz Astronomy, The

194

XIII Publications, Presentations

25th Int. Symp. on Space Terahertz Technology, (Moscow, Russia,
Apr. 27-30, 2014).
Matsuo, H.: 2014, Photon Counting Terahertz Interferometry, A
Community Workshop to Plan the Future of Far-Infrared Space
Astrophysics, (NASA/GSFC, MD, USA, May 12-13, 2014).
Matsuo, H.: 2014, Photon counting technologies for future terahertz
astronomy, SPIE Astronomical Telescopes + Instrumentation 2014,(Montreal, Canada, June 22-27, 2014).
Matsuo, H.: 2014, Photon statistics as a tool for radio astronomy, General
Assembly and Scientific Symposium (URSI GASS), 2014 XXXIthURSI, (Beijing, China, Aug. 16-23, 2014).
Matsuo, H.: 2014, Proposal of Space Terahertz Interferometry, 15th
Workshop on Submillimeter-Wave Receiver Technologies in Eastern
Asia, (Mie, Japan, Dec. 15-17, 2014).
Matsuo, H.: 2015, Combination of Double Fourier and Intensity
Interferometers, The 2nd EU-FP7 FISICA Workshop, (Maynooth,Ireland, Jan. 28-29, 2015).
Matsuo, H.: 2015, Aperture Synthesis Imaging with Fourier and Intensity
Interferometers, Fourier Transform Spectroscopy (FTS) OSA topicalmeeting, (Lake Arrowhead, CA, USA, Mar. 1-4, 2015).
Matthias, K., Ikeya, M., Kojima, T., Noguchi, T.: 2014, High Current
Density SIS Junctions Based on Nb/Al,AlN/Nb Tri-layers, 15th
Workshop on Submillimeter-Wave Receiver Technologies in Eastern
Asia, (Mie, Japan, Dec. 15-17, 2014).
Matthias, K., Ikeya, M., Kojima, T., Noguchi, T.: 2015, High Current
Density SIS Junctions Based on Nb/Al,AlN/Nb Tri-layers, The 26th
Int. Symp. on Space Terahertz Technology, (Cambridge, MA, USA,
Mar. 16-18, 2015).
Micheva, G., Iwata, I., Inoue, A. K.: 2014, New analysis of LyC leakingz ~ 3 galaxies in the SSA22 field, Lyman Continuum Leakage andCosmic Reionization, (Stockholm, Sweden, Aug. 13-15, 2014).
Min, C.: 2015, A long-period observations of SiO masers toward a
symbiotic star R Aquarii, The 8th KaVA Joint Science WG Meeting,(Gyeongju, Korea, Jan. 13-15, 2015).
Mitsui, K., Nitta, T., Okada, N., Sekimoto, Y., Karatsu, K., Sekiguchi,
S., Sekine, M., Noguchi, T.: 2014, Fabrication of 721-pixel siliconlens array of a microwave kinetic inductance detector camera, SPIE
Astronomical Telescopes + Instrumentation 2014, (Montreal, Canada,
June 22-27, 2014).
Miyazaki, S.: 2014, Hyper Suprime-Cam (Invited Plenary Talk), SPIE
Astronomical Telescopes + Instrumentation 2014, (Montreal, Canada,
June 22-27, 2014).
Motogi, K., Sugiyama K., Walsh, A. J., Hirota T., Honma, M., Niinuma,
K. Yonekura, Y., Fujisawa, K.: 2014, The Face-on Accretion System
in High Mass Star-Formation; Dusty Infalling Streams down to 15
Astronomical Unit, Revolution in Astronomy with ALMA - The 3rdYear -, (Tokyo, Japan, Dec. 8-11, 2014).
Nagai, H., Kino, M., Koyama, S., Liuzzo E.: 2014, Discovery of mm/
submm Emission from Large Scale Jets in Quasars, East Asia ALMA
Science Workshop, (Jeju, Korea, Jul. 14-17, 2014).
Nagai, H., et al. including Nakanishi, K.: 2014, ALMA Polarimetry:
Current Status and Prospects for Cycle 3, Astronomical Polarimetry
2014, (Grenoble, France, May 26-30, 2014).
Nagai, H., et al. including Nakanishi, K.: 2014, ALMA Polarization
Science Verification: 3C286, Revolution in Astronomy with ALMA The 3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).

Nagai, T., Shinohara, I., Zenitani, S.: 2014, Kinetic Aspects of Magnetic
Reconnection in the Magnetotail with the Spacecraft Geotail, USJapan Workshop on Magnetic Reconnection (MR 2014), (Tokyo,
Japan, May 20-24, 2014).
Nagayama, T., Omodaka, T., Handa, T., Kobayashi, H., Burns, R. A.: 2014,
Radio Astrometric Observations and the Galactic Constant as Basis of
the Galactic Kinematics Study, APRIM 2014: 12th Asia-Pacific IAU
Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Naka, C., Ogawa, S., Shinnaka, Y., Fujiwara, H., Furusho, R., Kawakita,
H., Kobayashi, H., Watanabe, J., Yagi, M., Yoshida, M.: Lowdispersion spectroscopic observations of comets C/2012 S1 (ISON)
and C/2013 R1 (Lovejoy) by the Subaru Telescope, Asteroids, Comets,
Meteors 2014 (ACM 2014), (Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Nakahara, S.: 2014, Multi-epoch, quasi-simultaneous 22/43GHz
observations of the M84 nucleus with VERA, 12th EVN Symposium
2014, (Cagliari, Italy, Oct. 7-10, 2014).
Nakahara, S.: 2014, Multi-epoch, quasi-simultaneous 22/43GHz
observations of the M84 nucleus with VERA, Eating VLBI (East Asia To
Italy: Nearly Global VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Nakamura, F.: 2014, Revealing the Initial Conditions of Cluster Formation:
The Case of Serpens South, The Early Life of Stellar Clusters: Formation
and Dynamics, (Copenhargen, Denmark, Nov. 3-7, 2014).
Nakamura, F.: 2014, Cluster Formation Triggered by Cloud-Cloud
Collision: The Case of Serpens South, Star Formation Across Spaceand Time, (Noordwijk, Netherlands, Nov. 11-14, 2014).
Nakamura, F.: 2014, Synergy of JCMT and NRO:The Case of Star
Formation Project, JCMT Science Workshop, (NAOJ, Tokyo, Japan,
Sep. 1-2, 2014).
Nakamura, F.: 2014, Cluster Formation Triggered by Filament Collisions,
Revolution in Astronomy with ALMA - The 3rd Year -, (Tokyo, Japan,
Dec. 8-11, 2014).
Nakamura, F.: 2014, Protostellar Jets and Stellar Feedback, Gravityʼs
Loyal Opposition: The Physics of Star Formation Feedback, (Santa
Barbara, CA, USA, May 23, 2014).
Nakamura, F.: 2015, Magnetic Field in Star-Forming Regions, The 3rdWorkshop on Large Aperture Sub/mm Telescope in the ALMA Era,
(Mitaka, Tokyo, Japan, Mar. 10-11, 2015).
Nakamura, K.: 2014, Recursive structure in the definitions of gaugeinvariant variables for any order perturbations, The 24th workshop
on General Relativity and Gravitation in Japan, (IPMU, Tokyo
University, Kashiwa, Japan, Nov. 10-14, 2014).
Nakamura, T., Yamamoto, M., Tanaka, Y., Kero, J., Szasz, C., Watanabe,J., Abe, S., Kastinen, D.: 2014, Precise Orbit Determination of
Meteors by HPLA Radar and the MU Radar Meteor Head Echo
Database, 40th COSPAR Scientific Assembly , (Moscow, Russia,
Aug. 2-10, 2014).
Nakanishi, K., Nagai, H., Fomalont, E., Corder, S., Moellenbrock,G., Tang, Y.-W.: 2014, ALMA Polarization: Commissioning andVerification Status, Astronomical Polarimetry 2014, (Grenoble,
France, May 26-30, 2014).
Nakanishi, K., Nagai, H., Fomalont, E., Cortes, P., Remijan, A.,
Vlahakis, C., Corder, S., Moellenbrock, G., Tang, Y.-W., Hills, R., the
ALMA science team: 2014, ALMA Polarization: Current Status andExtension of Capability, Revolution in Astronomy with ALMA - The
3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Nakanishi, K., Sorai, K., Nakai, N., Kuno, N., Matsubayashi, K., Sugai,

H., Takano, S., Kohno, K., Nakajima, T.: 2015, Millimeter Hydrogen
Recombination Line in the Center of NGC 253, Dissecting Galaxies
Near and Far: High Resolution Views of Star Formation and the ISM,
(Santiago, Chile, Mar. 23-27, 2015).
Nakanishi, K., Sorai, K., Nakai, N., Kuno, N., Matsubayashi, K., Sugai, H.,
Takano, S., Kohno, K., Nakajima, T.: 2014, Ionized gas observation
toward a nearby starburst galaxy NGC 253, Revolution in Astronomy
with ALMA - The 3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Namiki, N.: 2014, GALA-Japan Status, GALA General Meeting, (Tokyo,
Japan, May 7-8, 2014).
Namiki, N., Kimura, J., Kobayashi, M., Hussmann, H., Lingenauber,
K., Team Gala-japan: 2014, Development of JUICE/Ganymede
Laser Altimeter (GALA), Japan Geoscience Union Meeting 2014,(Yokohama, Japan, Apr. 27-May 2, 2014).
Namiki, N., Kobayashi, M., Kimura, J., Hussmann, H., Lingenauber, K.,
Gala Japan: 2014, Development of JUICE/Ganymede Laser Altimeterin Japan, AOGS 11th Annual Meeting (AOGS2014), (Sapporo, Japan,
Jul. 28-Aug. 1, 2014).
Namiki, N., et al. including Yamada, R., Noda, H., Shizugami, M.,
Hirata, N., Matsumoto, K., Oshigami, S., Yoshida, F., Araki, H.,
Tazawa, S.: 2015, Performance of Hayabusa-2 LIDAR in Acceptanceand Verification Tests, The 46th Lunar and Planetary Science Conf.,(The Woodlands, TX, USA, Mar. 16-20, 2015).
Namiki, N., et al. including Yamada, R., Noda, H., Shizugami, M.,
Hirata, N., Matsumoto, K., Oshigami, S., Yoshida, F., Araki, H.,
Tazawa, S.: 2014, Development and tests of Hayabusa-2 LIDAR,AOGS 11th Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28Aug. 1, 2014).
Narita, N.: 2014, Exoplanet ISDT Activity Report: Exploring OtherWorlds with TMT, TMT Science Forum 2014, (Tucson, AZ, USA,
Jul. 17-19, 2014).
Narukage, N., Kano, R., Bando, T., Ishikawa, R., Kubo, M., Katsukawa,Y., Ishikawa, S., Suematsu, Y., Hara, H., Tsuneta, S., Auchere,F.: 2014, UV spectropolarimeter design for precise polarization
measurement and its application to the CLASP for explorationof magnetic fields in solar atmosphere, 40th COSPAR Scientific
Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Naruse, M., Tanoue, H., Arai, K., Sekimoto, Y., Noguchi, T., Taino,T., Myoren, H.: 2014, Superconducting On-chip Spectrometers at
Sub-millimeter Wavelength, The 25th Int. Symp. on Space Terahertz
Technology, (Moscow, Russia, Apr. 27-30, 2014).
Niino, Y., Nagamine, K., Zhang, B.: 2014, Metallicity Measurements of
GRB Explosion Sites: Lessons from HII regions in M31, Swift: 10
years of discovery, (Rome, Italy. Dec. 2-5. 2014).
Noda, H., Kunimori H., Araki, H.: 2014, Lunar Laser Ranging Trial at
Koganei SLR Station, 40th COSPAR Scientific Assembly , (Moscow,
Russia, Aug. 2-10, 2014).
Noda, H., Kunimori, H., Araki, H., Kashima, S., Otsubo, T., Katayama,
M., Hanada, H., Utsunomiya, S., Fuse, T., Chiba, K., Funazaki, K.,
Matsumoto, Y.: 2014, LLR Development Status in Japan, AOGS 11th
Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Noda, H., Mizuno, T., Namiki, N., Senshu, H., Yamada, R., Hirata,N., LIDAR-Science Team.: 2015, Scientific Measurements of
Hayabusa-2 Laser Altimeter (LIDAR), The 46th Lunar and Planetary
Science Conf., (The Woodlands, TX, USA, Mar. 16–20, 2015).
Nozawa, T.: 2014, Dust Production in a Variety of Types of Supernovae,

XIII Publications, Presentations

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Cosmic Dust VII, (Osaka, Japan, Aug. 4-8, 2014).
Ogawa, S., Shinnaka, Y., Boice, D., Fujiwara, H., Furusho, R., Kawakita,
H., Kobayashi, H., Watanabe, J., Yagi, M., Yoshida, M.: 2014, The
Spatial Distributions of Daughter Species in Comet C/2013 R1 (Lovejoy),
AAS, DPS meeting 46, (Tucson, AZ, USA, Nov. 9-14, 2014).
Ohishi, M.: 2014, ITU-R Recommendations and Reports, RA series,
IUCAF School on Spectrum Management, (Santiago, Chile, Apr.
7-11, 2014).
Ohishi, M.: 2014, IUCAF Activity Report between 2011 and 2014,
General Assembly and Scientific Symposium (URSI GASS), 2014
XXXIth URSI, (Beijing, China, Aug. 16-23, 2014).
Ohishi, M.: 2014, Chemical Evolution of N-bearing Organic Molecules
Leading to Glycine, APRIM 2014: 12th Asia-Pacific IAU Regional
Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Ohishi, M.: 2014, Chemical Evolution of N-bearing Organic Molecules
Leading to Glycine, Workshop on Interstellar Matter 2014, (Sapporo,
Japan, Oct. 16, 2014).
Ohishi, M.: 2015, Discovery of Objects Richest in CH3NH2, Candidates
for Future Glycine Surveys, Grain Chemistry Workshop, (Tokyo,
Japan, Mar. 5, 2015).
Ohishi, N., Miyoki, S., Uchiyama, T., Miyakawa, O., Ohashi, M.: 2014,
Safety management of an underground-based gravitational wave
telescope: KAGRA, SPIE Astronomical Telescopes + Instrumentation
2014, (Montreal, Canada, June 22-27, 2014).
Ohsuga, K.: 2014, Global Radiation-MHD Simulations of SuperEddington Accretion Flows and Outflows, Hyper Accretoion, (IPMU,
Chiba, Japan, Apr. 7-11, 2014).
Ohsuga, K.: 2014, Super-Eddington Accretion Flows and Outflows; amodel for ULXs, ULXs-Implications for our View of the Universe,(Lorentz Center, Leiden, Netherlands, Mar. 31 - Apr. 4, 2014).
Ohtake, M., Iwata, T., Haruyama, J.: 2014, Mineralogy within theSouth Pole-Aitken Basin on the Moon, AOGS 11th Annual Meeting(AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Okamoto, J., Antolin, P., De Pontieu, B., Uitenbroek, H., Van
Doorsselaere, T., Yokoyama, T.: 2014, Observational Evidence ofResonant Absorption in Oscillating Prominence, AGU Fall Meeting
2014, (San Francisco, CA, USA, Dec. 15-19, 2014).
Okutomi, K., Akutsu, T., Ando, M., Nikaido, M., Tanaka, N., Torii,
Y., Sato, S., Izumi, K., Chen, D., DPF Working Group: 2014,
Development of Inertial Sensor for DECIGO Pathfinder, 10th Int.
LISA Symp., (Gainesville, Florida, USA, May 18-23, 2014).
Ootsubo, T., Usui, F., Takita, S., Watanabe, J., Honda, M., YanamandraFisher, Padma A., Kawakita, H., Furusho, R., Kasuga, T., Fuse,
T.: 2014, Mid-infrared Observation of Comet C/2012 S1 (ISON)
with Subaru+COMCIS, AOGS 11th Annual Meeting (AOGS2014),(Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Ootsubo, T., Usui, F., Takita, S., Watanabe, J., Yanamandra-Fisher,P., Honda, M., Kawakita, H., Furusho, R.: 2014, Mid-infraredobservations of sungrazing comet C/2012 S1 (ISON) with the Subaru
Telescope, Asteroids, Comets, Meteors 2014 (ACM 2014), (Helsinki,
Finland, Jun. 30-Jul. 4, 2014).
Oshigami, S., Senshu, H., Wada, K., Kobayashi, M., Namiki, N.,
Mizuno, T.: 2014, Detection of levitation dust around the asteroid
by Hayabusa-2 LIDAR, AOGS 11th Annual Meeting (AOGS2014),(Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Oshigami, S., Senshu, H., Yamada, R., Namiki, N., Mizuno, T.,

196

XIII Publications, Presentations

Hayabusa-2 LIDAR science team: 2015, Detectability of levitation
dust around the asteroid by Hayabusa-2 LIDAR, The 46th Lunar andPlanetary Science Conf., (The Woodlands, TX, USA, Mar. 16–20, 2015).
Oka, T., Geballe, T. R., Goto, M., Usuda, T.: 2014, Temperature, Density,
Ionization Rate, and Morphology of Diffuse Gas Near the Galactic
Center Probed by H 3+, 69th Int. Symp. on Molecular Spectroscopy,(University of Illinois, Urbana-Champaign, Jun. 16-20, 2014).
Otsuji, K., Shibasaki, K., Tanaka, Y., Miyagoshi, T.: 2014,
Statistical analysis of the gyroresonance sources using Nobeyama
Radioheliograph and sunspot sketches, Japan Geoscience Union
Meeting 2014, (Yokohama, Japan, Apr. 27-May 2, 2014).
Oya, S.: 2014, Ground-layer turbulence evaluation project at Subaru
Telescope, Adapting to the Atmosphere Conf. 2014, (Durham, UK,
Sep. 15-18, 2014).
Oyama, T.: 2014, A progress report on the development and performanceof OCTAVE-DAS for VERA, JVN and Japanese e-VLBI (OCTAVE),
12th EVN Symposium 2014, (Cagliari, Italy, Oct. 7-10, 2014).
Oyama, T.: 2014, The development and performance of OCTAVE-DAS
and Correlator System, Eating VLBI (East Asia To Italy: Nearly
Global VLBI) 2014, (Bologna, Italy, Oct. 13-14, 2014).
Oyama, T.: 2015, Report on the results of test broadband observations of
VERA, The 8th KaVA Joint Science WG Meeting, (Gyeongju, Korea,
Jan. 13-15, 2015).
Ozaki, S., Tanaka, Y., Hattori, T., Mitsui, K., Fukushima, M., Okada,N., Obuchi, Y., Tsuzuki, T., Miyazaki, S., Yamashitam, T.: 2015,
FOCAS IFU: Current status, Subaru Users Meeting, (Mitaka, Tokyo,
Japan, Jan. 13-15, 2015).
Ozaki, S., Tanaka, Y., Hattori, T., Mitsui, K., Fukushima, M., Okada,N., Obuchi, Y., Tsuzuki, T., Miyazaki, S., Yamashitam, T.: 2014,
Development of a slicer integral field unit for the existing optical
spectrograph FOCAS: progress, Advances in Optical and MechanicalTechnologies for Telescopes and Instrumentation, (Monreal, Canada,Jun. 23-27, 2014).
Pyo, T.-S., Hayashi, M., Beck, T. L., Chris, C. J., Takami, M.: 2014,
Complicated Structure of Interacting Young Binary System: Outflows
and Gas-Streams, Thirty Meter Telescope Science Forum, (Tucson,
AZ, USA, Jul. 16-19, 2014).
Pyo, T.-S., Hayashi, M., Beck, T. L., Chris, C. J., Takami, M.: 2014,
Unveiling Comples Outflow Structure of UY AUR, APRIM 2014:
12th Asia-Pacific IAU Regional Meeting, (Daejeon, South Korea,
Aug. 18-22, 2014).
Rapson, V., Kastner, J., Andrews, S. M., Hines, D. C., Macintosh, B.,
Millar-Blanchaer, M., Tamura, M.: 2015, Near-infrared Scattered
Light Imaging of the Protoplanetary Disk Around V4046 Sgr with theGemini Planet Imager, AAS Meeting #225, (Seattle, WA, USA, Jan.
4-8, 2015).
Reznikova, V., Antolin, P., Van Doorsselaere, T.: 2014, Forward modelingof gyrosynchrotron emission perturbations by sausage mode, 40th
COSPAR Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
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., Tateuchi, K., Lee, M., Yamashita, T., Michiyama,T., Kawabe, R.: 2014, Diffuse and Dense Gas in Nearby Luminous
Infrared Galaxies, Revolution in Astronomy with ALMA - The 3rdYear -, (Tokyo, Japan, Dec. 8-11, 2014).
Saito, T., Iono, D., Yun, M. S., Ueda, J., Nakanishi, K., Sugai, H.,

Espada, D., Imanishi, M., Motohara, K., Hagiwara, Y., Tateuchi, K.,
Lee, M., Kawabe, R.: 2014, Investigating AGN/starburst activities
through ALMA multi-line observations in the mid-stage merger
VV114, IAU Symp. 309, (Wien Univ., Austria, Jul. 7-11, 2014).
Saito, T., Iono, D., Yun, M. S., Ueda, J., Nakanishi, K., Sugai, H., Espada,D., Imanishi, M., Motohara, K., Hagiwara, Y., Tateuchi, K., Lee,
M., Kawabe, R.: 2014, Investigating AGN/starburst activities through
ALMA multi-line observations in the mid-stage merger VV114, East
Asia ALMA Science Workshop, (Jeju, Korea, Jul. 14-17, 2014).
Saito, Y., Yatsu, Y., Yoshii, T., Usui, R., Kurita, S., Ito, K., Tachibana,Y., Yano, Y., Tanigawa, T., Kawai, N., Kuroda, D., Yanagisawa, K.,
Hanayama, H.: 2014, Optical follow-up observation of the transient
objects with the Akeno telescope, Suzaku-MAXI 2014: Expanding the
Frontiers of the X-ray Universe, (Ehime, Japan, Feb. 19-22, 2014).
Sakai, N.: 2014, Direct comparison between VERA, VLBA and EVN
astrometry results and an analytic gas dynamics model, 12th EVN
Symposium 2014, (Cagliari, Italy, Oct. 7-10, 2014).
Sakai, N.: 2015, Activity and future of the galactic astrometry sub-WG,
The 8th KaVA Joint Science WG Meeting, (Gyeongju, Korea, Jan.
13-15, 2015).
Sako, N.: 2014, A Study of Acceleration Mechanisms of X-ray Jets, 2014
Living With a Star (LWS) Science Meeting, (Portland, OR, USA,
Nov. 2-6, 2014).
Santos, F. P., et al. including Nakamura, F.: 2015, Comparing polarizedsubmm emission and near-infrared extinction polarization in the Vela
C giant molecular cloud, AAS Meeting #225, (Seattle, WA, USA,
Jan. 4-8, 2015).
Sawada, T., Hasegawa, T., Koda, J.: 2015, ALMA Reveals Internal
Structure of Molecular Clouds in the LMC at Various Evolutionary
Stages, Dissecting Galaxies Near & Far, (Santiago, Chile, Mar. 2327, 2015).
Sawada, T., Hasegawa, T., Koda, J.: 2014, ALMA Reveals Internal
Structure of Molecular Clouds in the LMC at Various Evolutionary
Stages, Revolution in Astronomy with ALMA - The 3rd Year -,(Tokyo, Japan, Dec. 8-11, 2014).
Sawada-Satoh, S., Akiyama, K., Niinuma, K., Nagai, H., Kino, M.,
DʼAmmando, F., Koyama, S., Hada, K., Orienti, M., Honma, M.,
Shibata, K. M., Ueno, Y.: 2014, Apparent Inward Motion of theParsec-scale Jet in the BL Lac Object OJ 287 Simultaneously with theGamma-ray Flares during 2011-2012, APRIM 2014: 12th Asia-Pacific
IAU Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Sawada-Satoh, S.: 2014, VERA Frequent Monitoring of the Parsecscale Jet in the BL Lac Object OJ 287 Simultaneous with the Gammaray Flares during 2011-2012, 12th EVN Symposium 2014, (Cagliari,
Italy, Oct. 7-10, 2014).
Sawada-Satoh, S.: 2014, Current Status of VERA, 2014 Radio
Telescope Users Meeting, (Muju, Korea, Jul. 22-25, 2014).
Sawada-Satoh, S.: 2014, VERA/GENJI Monitoring of OJ 287 in 20102013, Eating VLBI (East Asia To Italy: Nearly Global VLBI) 2014,(Bologna, Italy, Oct. 13-14, 2014).
Sawada-Satoh, S.: 2015, HCN & HCO+ absorptions on NGC 1052, The 8th
KaVA Joint Science WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Sekiguchi, K.: 2014, NAOJ-NDU collaboration on the 60 cm telescope,
MEARIM III, (Beirut, Lebanon, Sep. 1-16, 2014).
Sekiguchi, S., Nitta, T., Karatsu, K., Sekimoto, Y., Okada, N.,
Tsuzuki, T., Sekine, M., Okada, T., Shu, S., Naruse, M., Dominjon,

A., Noguchi, T., Kashima, S., Matsuo, H.: 2014, Development of
a Compact Cold Optics for Millimeter and Submillimeter Wave
Observations, The 25th Int. Symp. on Space Terahertz Technology,(Moscow, Russia, Apr. 27-30, 2014).
Sekii, T.: 2014, Rotation of KIC 11145123, HELAS VI/SOHO-28,(Goettingen, Germany, Sep. 1-5, 2014).
Sekii, T.: 2014, Helioseismic Studies of Solar Dynamics, 2014 Living Witha Star (LWS) Science Meeting, (Portland, OR, USA, Nov. 2-6, 2014).
Sekimoto, Y., Karatsu, K., Nitta, T., Sekine, M., Sekiguchi, S., Okada,T., Shu, S., Noguchi, T., Dominjon, A., Naruse, M.: 2015, Design of
MKID focal plane array for LiteBIRD, The 26th Int. Symp. on Space
Terahertz Technology, (Cambridge, MA, USA, Mar. 16-18, 2015).
Sekimoto, Y., Nitta, T., Karatsu, K., Sekine, M., Sekiguchi, S., Okada,T., Shu, S., Noguchi, T., Naruse, M., Mitsui, K., Okada, N., Tsuzuki,T., Dominjon, A., Matsuo, H.: 2014, Developments of wide fieldsubmillimeter optics and lens antenna-coupled MKID cameras, SPIE
Astronomical Telescopes + Instrumentation 2014, (Montreal, Canada,
June 22-27, 2014).
Sekimoto, Y., Nitta, T., Karatsu, K., Sekine, M., Sekiguchi, S., Okada, T.,
Shu, S., Noguchi, T., Naruse, M., Mitsui, K., Okada, N., Tsuzuki, T.,
Dominjon, A., Matsuo, H.: 2014, Developments of wide field-of-view
MKID cameras for millimeter and submillimeter astronomy, The 8th
European Conf. on Antennas and Propagation (EuCAP 2014), (Hague,
The Netherlands, Apr. 6-11, 2014).
Senshu, H., Oshigami, S., Yamada, R., Kobayashi, M., Namiki, N.,
Mizuno, T., and Hayabusa-2 LIDAR science team: 2015, Dust countmode of LIDAR onboard Hayabusa-2, The 46th Lunar and Planetary
Science Conf., (The Woodlands, TX, USA, Mar. 16–20, 2015).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G.: 2014, Rolesof fission, Neutron Star Mergers and Supernovae in R-Process
Nucleosynthesis, Fourth Joint Meeting of the Nuclear Physics
Divisions of the American Physical Society and the Physical Societyof Japan, (Waikoloa, HI, USA, Oct. 7-11, 2014).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G.: 2014, R-process
nucleosynthesis in neutron star merger with new fission model,
13th International Symposium on Nuclei in the Cosmos, (Debrecen,
Hungary, Sep. 7-11, 2014).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G.: 2014, R-process
nucleosynthesis in neutron star merger with new fission model,
NIC2014 School, (Debrecen, Hungary, Jun. 30-Jul. 4, 2014).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G.: 2014, R-Process in
Neutron Star Merger with a New Fission Model, 2nd Int. Conf. on
Advances in Radioactive Isotope Science, (Tokyo, Japan, Jun. 1-6,
2014).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G.: 2014, Roles of Fission,
Neutron Star Mergers and Supernovae in R-Process Nucleosynthesis,
5th Carpathian Summer School in Physics, (Sinaia, Romania, Jun. 1326, 2014).
Shibagaki, S., Kajino, T., Mathews, G. J., Chiba, S.: 2014, R-process
in neutron-star mergers with a new fission model, 2nd Int. Conf. on
Advances in Radioactive Isotope Science, (Tokyo, Japan, Jun. 1-6, 2014).
Shibagaki, S., Kajino, T., Mathews, G. J., Chiba, S.: 2014, Impactof nuclear fission on r-process nucleosynthesis and origin of solar
r-process elements, 5th Carpathian Summer School in Physics,(Sinaia, Romania, Jun. 13-26, 2014).
Shibasaki, K.: 2014, Why microwave emission is a good proxy of solar

XIII Publications, Presentations

197

activity?, 11th Annual General Meeting of Asia Oceania Geosciences
Society, (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Shibasaki, K.: 2014, Magnetic field in high-beta plasma: spontaneous
formation of magnetic flux tubes, 14th European Solar Physics
Meeting, (Dublin, Ireland, Sep. 8-12, 2014).
Shimojo, M.: 2014, New Window of Sol. Phys.ics: Solar observations
with ALMA, 2014 Living With a Star (LWS) Science Meeting,(Portland, OR, USA, Nov. 2-6, 2014).
Shimojo, M., Hales, A., Sawada, S., Hills, R., Remijan, A., Corder,
S., Yagoubov, P., Sugimoto, M., Asayama, S., Brajsa, R., Bastian,T., Solar development study team of NA & EU-ARC: 2014, New
window of solar physics: Solar observations with ALMA, 2014
Living With a Star (LWS) Science Meeting, (Portland, OR, USA,
Nov. 2-6, 2014).
Shino, N.: 2014, Methanol maser observation massive star formation
region IRAS 18089-1732 and IRAS20198+3716, The 7th KaVA Joint
Science WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Shino, N.: 2015, Methanol maser observation of massive star formation
region IRAS 18089-1732 & IRAS 20198+3716, The 8th KaVA Joint
Science WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Shinohara, I., Kojima, H., Nagai, T., Zenitani, S., Fujimoto, M.: 2014,
Geotail observation of low frequency wave activity in a 3D structureof magnetotail reconnection site, AGU Fall Meeting 2014, (SanFrancisco, CA, USA, Dec. 15-19, 2014).
Shirahata, M., Nakagawa, T., Oyabu, S., Usuda, T.: 2014, NearInfrared spectroscopy of CO ro-vibrational absorption toward heavily
obscured AGNs, The Universe in the light of AKARI Synergy with
future Large Space Telescopes, (Oxford, UK, Jul. 9-11, 2014).
Shirasaki, Y.: 2014, AGN-Galaxy clustering and its dependence on themass of the Supermassive Black Hole, Clustering Measurements ofActive Galactic Nuclei, (Garching, Germany, Jul. 14-18, 2014).
Sôma, M.: 2014, Observations of the Annular Eclipse on 2012 May 21
by General Public in Japan, APRIM 2014: 12th Asia-Pacific IAU
Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Sôma, M.: 2014, Reliability of Eclipse Records in Japanese Ancientand Medieval Period, Intensive Workshop on Ancient and Medieval
Eclipse Data: Compilation of Eclipse Data and Examination of their
Reliability, (Tokyo, Japan, Nov. 27-28, 2014).
Sotani, H., Iida, K., Oyamatsu, K., Ohnishi, A.: 2014, Finding of a
new nuclear matter parameter characterizing low-mass neutronstars, Fourth Joint Meeting of the Nuclear Physics Divisions of
the American Physical Society and the Physical Society of Japan,(Waikoloa, HI, USA, Oct. 7-11, 2014).
Sotani, H.: 2014, Possible constraint on nuclear saturation parameters
via neutron star observations, NEB 16 - Recent Developments in
Gravity, (Mykonos, Greece, Sep. 17-20, 2014).
Sotani, H.: 2014, Constraints on the nuclear saturation parameters via
neutron star observations, Quarks and Compact Stars, (Beijing,
China, Oct. 20-22, 2014).
Suematsu, Y., Kaithakkal, A. J.: 2014, Fine-Scale Structure of Solar
Polar Faculae and their relation to Magnetic Patches, AGU Fall
Meeting 2014, (San Francisco, CA, USA, Dec. 15-19, 2014).
Suematsu, Y., Kaithakkal, A. J.: 2014, Fine-scale Structure andDynamics of Solar Polar Faculae and Magnetic Patches, 11th Annual
General Meeting of Asia Oceania Geosciences Society, (Sapporo,
Japan, Jul. 28-Aug. 1, 2014).

198

XIII Publications, Presentations

Suematsu, Y., Koyama, M., Sukegawa,T., Enokida, Y., Saito, K., Okura,Y.,
Nakayasu, T., Ozaki, S., Tsuneta, S.: 2014, Development of Compact
Integral Field Unit for Spaceborne Solar Spectro-polarimeter, Int. Conf.
on Space Optics 2014, (Tenerife, Spain, Oct. 7-10, 2014).
Suematsu, Y., Ueno, S.: 2014, Dynamics of Solar Flare Kernels Observedwith 3D Spectroscopy in H-alpha Line and SDO, 2014 Living With aStar (LWS) Science Meeting, (Portland, OR, USA, Nov. 2-6, 2014).
Suematsu, Y., Sukegawa, T., Okura, Y., Nakayasu, T., Enokida, Y.,
Koyama, M., Saito, K., Ozaki, S., Tsuneta, S.: 2014, Developmentof micro image slicer of integral field unit for spaceborne solar
spectrograph, Advances in Optical and Mechanical Technologies forTelescopes and Instrumentation, (Monreal, Canada, Jun. 23-27, 2014).
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.: 2014, The VLBI
Monitor Project for the 6.7 GHz Methanol Masers Using the JVN/
EAVN, APRIM 2014: 12th Asia-Pacific IAU Regional Meeting,(Daejeon, South Korea, Aug. 18-22, 2014).
Sunada, K.: 2015, VERA Maser surveys, The 8th KaVA Joint Science
WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Takahashi, H. R., Ohsuga, K.: 2014, Numerical Study of Super Critical
Accretion Disks, Plasma Conf. 2014, (Niigata, Japan, Nov. 18-21, 2014).
Takahashi, H. R., Ohsuga, K.: 2014, Numerical Study of Jets andOutflows from Super Critical Accretion Disks, ULXs-Implications
for our View of the Universe, (Lorentz Center, Leiden, Netherlands,
Mar. 31 - Apr. 4, 2014).
Takahashi, H. R., Ohsuga, K.: 2014, Explicit-Implicit Scheme forSpecial Relativistic Magnetohydrodynamics, Hyper-Accretion 2014,
Kashiwa, Japan, Apr. 7-11, 2014).
Takahashi, R.: 2014, Vibration Isolation System for KAGRA, 6th KoreaJapan Workshop on KAGRA, (Mitaka, Japan, Jun. 20-21, 2014).
Takahashi, S., ALMA science team: 2014, The ALMA High-Frequency
Campaign, Revolution in Astronomy with ALMA - The 3rd Year -,(Tokyo, Japan, Dec. 8-11, 2014).
Takano. S.: 2014, Distribution of Molecules in the Circumnuclear Disk
and Surrounding Starburst Ring in the Seyfert Galaxy NGC 1068
Observed with ALMA, Revolution in Astronomy with ALMA - The
3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Tamura, M., SEEDS team: 2015, SEEDS, Subaru Users Meeting,(Mitaka, Tokyo, Japan, Jan. 13-15, 2015).
Tamura, M., et al.: 2014, Direct Imaging of Giant Exoplanets, 40th
COSPAR Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Tamura, M.: 2014, Exoplanet and Disk Imaging with Subaru, WFIRST
Workshop, (Pasadena, USA, Nov. 17, 2014).
Tamura, M.: 2014, Direct imaging explorations of exoplanets/disks andfuture Earth-like planet studies with Subaru, China-Subaru workshop,(Shanghai, China, Nov. 29-Dec. 1, 2014).
Tamura, M.: 2015, SEEDS, Origins 2014, (Nara, Japan, Jul. 6-11, 2014).
Tamura, Y.: 2014, GPS Measurement at VERA Sites, The 7th KaVA
Joint Science WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Tanaka, M.: 2014, Subaru Hyper Suprime-Cam Survey, Future Directions
in Galaxy Cluster Surveys, (Paris, France, Jun. 23-27, 2014).
Tanaka, M.: 2014, Direct Measurements of the Formation Timescalesof Massive Cluster Ellipticals based on Deep Near-IR Spectroscopy,
Multiwavelength-surveys: Galaxy formation and evolution from theearly universe to today, (Dubrovnik, Criatua, May 12-16, 2014).

Tanaka, M.: 2014, Supernova Science with Subaru/Hyper SuprimeCam, Chile-Japan Academic Forum in U.Tokyo “Astrophysics andAstronomical Instrumentation”, (Tokyo, Japan, Oct. 8-9, 2014).
Tanaka, M.: 2014, Electromagnetic Emission from Neutron Star
Mergers, Nuclear Physics and Astrophysics of Neutron-Star Mergers
and Supernovae, and the Origin of R-Process Elements, (Trento, Italy,
Sep. 8-12, 2014).
Tanaka, M.: 2014, Transient Science with Hyper Suprime-Cam, Synergyof HSC and Hiroshima CORE-U projects for Galaxy Cluster andAstronomical Transients, (Hiroshima, Japan, Aug. 27, 2014).
Tanaka, M.: 2014, Time-Domain Science, Thirty Meter Telescope
Science Forum, (Tucson, AZ, USA, Jul. 16-19, 2014).
Tanaka, M.: 2015, Time-Domain Science with Subaru/HSC andGravitational Wave Objects, The 3rd Workshop on Large Aperture
Sub/mm Telescope in the ALMA Era, (Mitaka, Tokyo, Japan, Mar.
10-11, 2015).
Tanikawa, K., Sôma, M.: 2014, Historical Astronomy in National
Astronomical Obervatory of Japan: Long-term variations of the delayof the Earth rotation, APRIM 2014: 12th Asia-Pacific IAU Regional
Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Tanikawa, K., Sôma, M.: 2014, Historical Astronomy and Eclipses,
Intensive Workshop on Ancient and Medieval Eclipse Data:
Compilation of Eclipse Data and Examination of their Reliability,(Tokyo, Japan, Nov. 27-28, 2014).
Tatsumi, D., Ueda, A., Yoneda, H., Sato, K.: 2014, Low-loss and highdamage-threshold mirror development for gravitational-wave detectors,
SPIE Laser Damage 2014, (Bolder, CO, USA, Sep. 14–17, 2014).
Tazaki, F.: 2015, Super-resolved image of M87 with Sparse Modeling,
The 8th KaVA Joint Science WG Meeting, (Gyeongju, Korea, Jan.
13-15, 2015).
Stanke, T., et al. including Nakamura, F.: 2015, Apex Large CO
Heterodyne Survey, The Soul of High-Mass Star Formation Conf.,(Puerto Varas, Chile, Mar. 15–20, 2015).
Toriumi, S., Iida, Y., Kusano, K., Bamba, Y., Imada, S.: 2014, How Are
Strong Flares Produced in the Sun? Flux Emergence and Formationof NOAA AR 11158, European Geosciences Union General Assembly
2014, (Vienna, Austria, Apr. 27-May 2, 2014).
Toriumi, S., Iida, Y., Kusano, K., Bamba, Y., Imada, S.: 2014, Magnetic
Reconnection in the Formation of a Flare-productive Solar Active
Region, US-Japan Workshop on Magnetic Reconnection (MR 2014),(Tokyo, Japan, May 20-24, 2014).
Toriumi, S., Iida, Y., Kusano, K., Bamba, Y., Imada, S.: 2014, Flux
emergence and formation of a flare-productive active region, 40th
COSPAR Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Toriumi, S.: 2014, Magnetic Reconnection in Emerging Active Regions,2014 Living With a Star (LWS) Science Meeting, (Portland, OR,
USA, Nov. 2-6, 2014).
Toriumi, S., Katsukawa, Y., Antolin, P.: 2014, Observation of Magnetic
Reconnection and Recurrent Cool Jets in Emerging Active Region
NOAA 11974, 2014 Living With a Star (LWS) Science Meeting,(Portland, OR, USA, Nov. 2-6, 2014).
Toriumi, S.: 2014, Magnetic Fields in Emerging Active Regions, 4th Int.
workshop on small scale solar magnetic fields, (Bairisch Kölldorf,
Austria, Apr. 23-25, 2014).
Toriumi, S.: 2014, Emerging Magnetic Fields in Active Regions of the Sun,

9th Annual Int. Conf. on Numerical Modeling of Space Plasma Flows(ASTRONUM2014), (Long Beach, CA, USA, Jun. 23-27, 2014).
Toriumi, S.: 2014, Magnetic Reconnection in Emerging Active Regions,2014 LWS/Hinode/IRIS Workshop, (Portland, OR, USA, Nov. 2-6,
2014).
Tsujimoto, T.: 2014, Observational test on the origin of r-process fromlocal dwarf spheroidal galaxies, The r-process: status and challenges,(Seattle, USA, Jul. 28-Aug. 1, 2014).
Tsuzuki, T., Nitta, T., Imada, H., Seta, M., Nakai, N., Sekiguchi, S.,
Sekimoto, Y.: 2014, Design of wide-field Nasmyth optical system
for a submillimeter camera, SPIE Astronomical Telescopes +Instrumentation 2014, (Montreal, Canada, June 22-27, 2014).
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. J., Kawabe, R., Pan, H.: 2014, Investigating the evolutionof merger remnants from the formation of gas disks, IAU Symp. 309,
(Wien Univ., Austria, Jul. 7-11, 2014).
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. J., Kawabe, R., Pan, H.: 2014, Investigating the evolutionof merging galaxies via cold molecular gas, Revolution in Astronomy
with ALMA - The 3rd Year -, (Tokyo, Japan, Dec. 8-11, 2014).
Ueda, J.: 2014, Cold Molecular Gas in Merger Remnants, East Asia
ALMA Science Workshop, (Jeju, Korea, Jul. 14-17, 2014).
Ueda, J.: 2014, A Kiloparsec Scale Molecular Gas Disk in Latestage Mergers, Transformational Science in the ALMA Era: MultiWavelength Studies of Galaxy Evolution, (Charlottesville, VA, USA,
Aug. 4-7, 2014).
Uemoto, K., Ohtake, M., Yokota, Y., Yamamoto, S., Nakamura,R., Haruyama, J., Matsunaga, T., Ishihara, Y., Iwata, T.: 2015,
Distribution of Impact Melt Generated by the South Pole-Aitken
Impact, The 46th Lunar and Planetary Science Conf., (The
Woodlands, TX, USA, Mar. 16–20, 2015).
Usuda, T., et al. including Inatani, J., Iye, M.: 2014, Preliminary
design study of the TMT Telescope structure system: overview, SPIE
Astronomical Telescopes + Instrumentation 2014, (Montreal, Canada,
June 22-27, 2014).
Usuda-Sato, K., Tomita, A.: 2014, Astronomy for Development
Approaches in Asia, APRIM 2014: 12th Asia-Pacific IAU Regional
Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Uzawa, Y., Fujii, Y., Gonzalez, A., Kaneko, K., Kroug, M., Kojima,T., Miyachi, A., Makise, K., Terai, H., Wang, Z., Asayama, S.: 2014,
Performance of mass-produced terahertz SIS receiver for the ALMA
telescope, Applied Superconductivity Conf. 2014, (Charlotte, NC,
USA, Aug. 10-15, 2014).
Uzawa, Y., Fujii, Y., Kroug, M., Makise, K., Kojima, T., Miyachi, A.,
Gonzalez, A., Kaneko, K., Saito, S., Terai, H., Wang, Z., Asayama,
S.: 2014, Performance of Terahertz Superconducting Receivers for
the ALMA Telescope, The 9th Int. Symp. on Intrinsic Josephson
Effect and THz Plasma Oscillations in High-Tc Superconductors,(Kyoto, Japan, Nov. 30-Dec. 3, 2014).
Uzawa, Y., Makise, K., Kojima, T., Kroug, M., Saito, S., Fujii, Y.,
Gonzalez, A., Kaneko, K., Terai, H., Wang, Z.: 2014, Characterizationof NbTiN films for superconducting terahertz circuitry, 15th
Workshop on Submillimeter-Wave Receiver Technologies in Eastern

XIII Publications, Presentations

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Asia, (Mie, Japan, Dec. 15-17, 2014).
Wakita, S., Nakamura, T., Ikeda, T., Yurimoto, H.: 2014, Thermal
modeling for the parent bodies of asteroid Itokawa, 11th Annual
General Meeting of Asia Oceania Geosciences Society, (Sapporo,
Japan, Jul. 28-Aug. 1, 2014).
Wakita, S., Nakamura, T., Ikeda, T., Yurimoto, H.: 2014, Thermal historyof the parent bodies of asteroid Itokawa, Asteroids, Comets, Meteors
2014 (ACM 2014), (Helsinki, Finland, Jun. 30-Jul. 4, 2014).
Watanabe, J., Enomoto, T., Terai, T., Kasuga, T., Miyazaki, S., Oota, K.,
Muraoka, F., Onishi, T., Yamasaki, T., Mito, H., Aoki, T., Soyano,T., Tarusawa, K., Matsunaga, N., Sako, S., Kobayashi, N., Doi,
M.: 2014, Faint-meteor survey with a large-format CMOS sensor,
Asteroids, Comets, Meteors 2014 (ACM 2014), (Helsinki, Finland,
Jun. 30-Jul. 4, 2014).
Watanabe, J., Sugawara, K., Furusho, R., Kawakita, H., Shinoda, T.,
Ootsubo, T., Ishiguro, M., Sarugaku, Y., Tsukada, K., Abe, S., Terai,T., Yagi, M., Kasuga, T., Akisawa, H., Fuse, T., Ueno, S.: 2014,
What Happened to C/2012 S1(ISON), AOGS 11th Annual Meeting(AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Watanabe, T.: 2014, The Solar-C Program; Next Japanese-led Sun
Observing Mission, 11th Annual General Meeting of Asia Oceania
Geosciences Society, (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Watanabe, T., Hara, H., Imada, S., Watanabe, K.: 2014, Velocity
structure of solar flare plasmas, 40th COSPAR Scientific Assembly ,(Moscow, Russia, Aug. 2-10, 2014).
Watanabe, T., Hara, H., Watanabe, K., Imada, S.: 2014, Plasma
Eruptions Seen in EIS during a C8.3 Flare on 2014 April 4, 2014
Living With a Star (LWS) Science Meeting, (Portland, OR, USA,
Nov. 2-6, 2014).
Watanabe, T., Solar-C WG, Office for Solar-C: 2014, Brief Report on
SOLAR-C Status, 2014 Living With a Star (LWS) Science Meeting,(Portland, OR, USA, Nov. 2-6, 2014).
Wei, L., Antolin, P., Sun, X., Berger, T., Okamoto, T.: 2015, Hybrid
Prominence-Coronal Rain Complex in a Supra-arcade Fan Geometry,
ISSI Workshop - Bern, (Bern, Switzerland, Feb. 23-27, 2015).
Wu, B., Loo, Van, Nakamura, F., Tan, J. C.: 2014, Role of GMC Collisions
in Dense Filament, Clumps, and Star Formation, Filamentary Structure in
Molecular Clouds, (NRAO Charlottesville, VA, USA, Oct. 10-11, 2014).
Wu, Y.: 2014, Maser Astrometry with BeSSeL, Status and Progress, The 7th
KaVA Joint Science WG Meeting, (Yamaguchi, Japan, Jul. 7-9, 2014).
Wu, Y.: 2015, AGB candidates from WISE and AKARI, The 8th KaVA
Joint Science WG Meeting, (Gyeongju, Korea, Jan. 13-15, 2015).
Yagi, M.: 2015, Ghosts in Suprime-Cam, Subaru Users Meeting, (Mitaka,
Tokyo, Japan, Jan. 13-15, 2015).
Yaji, K.: 2014, Communicating Solar Astronomy, NAOJ Workshop at
ESO Garching, (Munich, Germany, Aug. 25-26, 2014).
Yaji, K.: 2015, Solar Eclipse in Japan : Past & Future, Discussion ofn
Thai-Japanse Astronomy, Star-Gazing & Cultual Exchange 2-15,(Chang Mai, Thailand, Jan. 13, 2015).
Yamada, R., Araki, H., Noda, H., Matsumoto, K.: 2014, Constraints
on source parameters on deep moonquakes and lunar inteior structure,
AGU Fall Meeting 2014, (San Francisco, CA, USA, Dec. 15-19, 2014).
Yamada, R., Ishihara, Y., Kobyashi, N., Murakami, H., Shiraishi, H.,
Hayakawa, M., Tanaka, S.: 2014, Exploration of lunar seismic activity
and lunar interior structure by one penetrator station, AOGS 11th
Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).

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XIII Publications, Presentations

Yamada, R., Senshu, H., Sinsuke, A., Yoshida, F., Hirata, N., Ishihara, Y.,
Hirata, N., Noda, H., Namiki, N.: 2014, Estimation of geometericalbedo of the 1999JU3 using the laser altimeter (LIDAR) data in
Hayabusa-2 mission, AOGS 11th Annual Meeting (AOGS2014),(Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Yamada, R., Shiraishi, H., Kobayashi, N., Murakami, H., Tanaka, S.,
Takeuchi, N., Ishihara, Y., Hayakawa, M., Garicia, R., Lognonne, P.:
2014, Exploration of lunar interior structure using the penetrator network,
Japanese-Russian Lunar-Planetary Workshop (JRLPW2014), (Mitaka,
Tokyo, Japan, Oct. 21/Mizusawa, Iwate, Japan, Oct. 24, 2014).
Yamaguchi, M. S., Yano, Y., Gouda, N.: 2014, Exoplanet exploration
for brown dwarfs with infrared astrometry, 40th COSPAR Scientific
Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Yamamoto, K., Haruyama, J., Kobayashi, S., Ohtake, M., Iwata, T.,
Ishihara, Y.: 2015, Multiple Plateaux Development Prior to Lunar
Dichotomy Formation, The 46th Lunar and Planetary Science Conf.,(The Woodlands, TX, USA, Mar. 16–20, 2015).
Yamamoto, S., Soma, T., Nishimura, Y., Watanabe, Y., Sakai, N., Shiino,T., Oguchi, O., Sakai, T., Maezawa, H., Kojima, T., Gonzalez,
A., Uzawa, Y.: 2014, THz Observations from the Ground, ALMA
Development Workshop 2014, (Mitaka, Tokyo, Jun. 17-18, 2014).
Yanagisawa, K., Shimizu, Y., Okita, K., Kuroda, D., Koyano, H.,
Tsutsui, H., Toda, H., Izumiura, H., Yoshida, M., Ohta, K., Kawai,N., Yamamuro, T.: 2014, Okayama astrophysical observatory wide
field camera, SPIE Astronomical Telescopes + Instrumentation 2014,(Montreal, Canada, June 22-27, 2014).
Yang, Y., Ping, J., Hanada, H.: 2014, Variation of the plume line and its
application to earthquake research, Japanese-Russian Lunar-Planetary
Workshop (JRLPW2014), (Mitaka, Tokyo, Japan, Oct. 21/Mizusawa,Iwate, Japan, Oct. 24, 2014).
Yonekura, Y., Saito, Y., Sugiyama, K., Miyamoto, Y., Soon, K. L.,
Momose, M., Ogawa, H., Fujisawa, K., Takaba, H., Sorai, K., Nakai,N., Omodaka, T., Oyama, T., Kono, Y., Kobayashi, H., Kawaguchi,
N.: 2014, Development of Takahagi and Hitachi 32-m Radio
Telescopes for JVN/EAVN, APRIM 2014: 12th Asia-Pacific IAU
Regional Meeting, (Daejeon, South Korea, Aug. 18-22, 2014).
Yonetoku, D., et al. including Okita, H., Yanagisawa, K.: 2014,
High-z gamma-ray bursts for unraveling the dark ages mission HiZGUNDAM, SPIE Astronomical Telescopes + Instrumentation 2014,(Montreal, Canada, June 22-27, 2014).
Yoshida T., Ebisawa K., Tsujimoto M., Ohsuga K., Nakagawa Y.,
Nomura M.: 2014, Spectral calculation through outflows aroundcompact objects and its hydrodynamic simulation, 40th COSPAR
Scientific Assembly , (Moscow, Russia, Aug. 2-10, 2014).
Yoshida, F., Kaifu, N., Working group of “Stars of Asia”: 2014, Starsof Asia, APRIM 2014: 12th Asia-Pacific IAU Regional Meeting,(Daejeon, South Korea, Aug. 18-22, 2014).
Yoshida, F., Lin, H.-W., Chen, Y.-T., Souami, D., Bouquillon, S., Ip, W.H., Chang, C. K., Nakamura, T., Dermawan, B., Yagi, M., Souchay,
J.: 2014, Colors and spin period distributions of sub-km main belt
asteroids, 46th Annual Meeting Division for Planetary Sciences,(Arizona, USA, Nov. 9-14, 2014).
Yoshida, F., Souami, D., Bouquillon, S., Nakamura, T., Dermawan,
B., Yagi, M., Souchay, J.: 2014, Lightcurves of hundred sub-km
main belt asteroids, Asteroids, Comets, Meteors 2014 (ACM 2014),(Helsinki, Finland, Jun. 30-Jul. 4, 2014).

katsukawa, Y.: 2014, Reconnection in the solar magnetic fields beyond
HINODE, 40th COSPAR Scientific Assembly, (Moscow, Russia,
Aug. 2-10, 2014).
Zenitani, S., GEOTAIL project: 2014, Coordination/Collaboration
between Geotail and MMS, THEMIS, Cluster, GEM mini workshop
2014, (San Francisco, USA, Dec. 14, 2014).
Zenitani, S., Hesse, M., Kuznetsova, M., Klimas, A., Umeda, T.: 2014, The
structure of the diffusion region in magnetic reconnection, AOGS 11th
Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Zenitani, S., Shinohara, I., Nagai, T., Wada, T.: 2014, The secrets of theion diffusion region in collisionless magnetic reconnection, European
Geosciences Union General Assembly 2014, (Vienna, Austria, Apr.
27-May 2, 2014).
Zenitani, S., Shinohara, I., Nagai, T., Wada, T.: 2014, Magnetic
diffusion and ion nonlinear dynamics in magnetic reconnection, USJapan Workshop on Magnetic Reconnection (MR 2014), (Tokyo,
Japan, May 20-24, 2014).
Zenitani, S., Shinohara, I., Nagai, T., Wada, T.: 2014, Kinetic Aspects of
the Ion Current Layer in a Reconnection Outflow Exhaust, AOGS 11th
Annual Meeting (AOGS2014), (Sapporo, Japan, Jul. 28-Aug. 1, 2014).
Zenitani, S.: 2014, A new picture of the central engine of kinetic magnetic
reconnection, 6th East-Asian Numerical Astrophysics Meeting(EANAM6), (Kyung Hee U., Suwon, Korea, Sep. 15-19, 2014).
Zenitani, S.: 2014, Magnetic reconnection as a showcase of compressible
fluid dynamics, 6th East-Asian Numerical Astrophysics Meeting(EANAM6), (Kyung Hee U., Suwon, Korea, Sep. 15-19, 2014).
Zenitani, S.: 2014, Some thoughts on asymmetric reconnection, GEM
mini workshop 2014, (San Francisco, USA, Dec. 14, 2014).
Zenitani, S.: 2014, Low-beta MHD reconnection as a showcase ofcompressible fluid dynamics, AGU Fall Meeting 2014, (San Francisco,
CA, USA, Dec. 15-19, 2014).

XIII Publications, Presentations

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