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Cover Caption
A stunning image of M 31, the Andromeda Galaxy, captured by Subaru Telescope’s new ultra-widefield camera, Hyper Suprime-Cam (HSC). HSC’s field of view is nine times larger than the area ofthe full moon. It has a capability to capture almost all of the M 31, which is apparently the largest
one in the galaxies seen from Japan or Hawaii.

Postscript
Editor Publications Committee
HANAOKA, Yoichiro
UEDA, Akitoshi
OE, Masafumi
SÔMA, Mitsuru
NISHIKAWA, Jun
HAGIWARA, Yoshiaki
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
http://www.nao.ac.jp/
Printer AZDEP Corporation
Kimishima Bldg.
2-5-4 Naka-cho, Musashino-shi, Tokyo 180-0006, Japan
TEX: +81-422-50-0667
FAX: +81-422-50-0670

Annual Report of the
National Astronomical Observatory of Japan

Volume 16, Fiscal 2013

T A

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Preface

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O F

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O N T

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Masahiko HAYASHI
Director General
National Astronomical Observatory of JapanI Scientific Highlights April 2013 – March 2014001

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 Project Office
12. JASMINE Project Office
13. Extrasolar Planet Detection Project Office
14. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project
15. Solar-C Project Office
16. Astronomy Data Center
17. Advanced Technology Center
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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058
061
063
064
071
072
075
078
080
082
084
086
087
090
091
093
098
103
104
106
107
110

T

S

III Organization

111

IV Finance125

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

126

VI Research Collaboration

127

VII Graduate Course Education

129

VIII Public Access to Facilities

133

IX Overseas Travel

139

X Award Winners

139

XI Library, Publications140

XII Important Dates

141

XIII Publications, Presentations
1. Refereed Publications

143

2. Publications of the National Astronomical Observatory of Japan154

3. Report of the National Astronomical Observatory of Japan154

4. Conference Proceedings154

5. Publications in English

162

6. Conference Presentations

162

Annual Report of the
National Astronomical Observatory of Japan
Volume 16, Fiscal 2013

P R E F A 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 2013.
In fiscal year 2013, Japan started work to create
TMT. TMT is a 30 m diameter optical-infrared telescope
being constructed on Mauna Kea on Hawai`i Islandby 5 countries including Japan, the United States ofAmerica (University of California, California Instituteof Technology, the National Science Foundation), thePeople’s Republic of China, the Republic of India,
and Canada. Overall construction is scheduled to
begin in 2014. But Japan had the good fortune to haveits construction budget approved before the othernations. Japan bears responsibility for the most criticalcomponents, including the body of the telescopeand production of the nearly 600 segments for the
primary mirror. The Master Agreement establishing thefundamentals needed for the 5 nations to move forwardwith construction was completed and in July I signed iton behalf of the NAOJ. 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
is approaching when it will be a reality.
ALMA is continuing commissioning (the process ofconfirming and adjusting those complicated devices one
by one) while carrying out Cycle 1 observations. Also,
results from the Cycle 0 trial observations have started
to be released. ALMA has over 100 times more sensitive
than previous millimeter/submillimeter band radio
telescopes. I understood this mathematically, but when I
saw the actual data and realized what that really means,
I was amazed. The resolving power approaches 0.1 arcseconds, equivalent to the sharp images taken with the
Hubble Space Telescope or the Subaru Telescope using
adaptive optics.

Thanks to this overwhelming sensitivity andresolution, ALMA can zealously observe objects in the
distant Universe. Thinking back to when I was a graduate
student, CCD cameras were being mounted on the 3–4 mdiameter optical telescopes in the world and observing the
Universe out to a redshift of 3 (11.5 billion light-years.)
Seeing those observations, I thought it was a world thatJapan could never attain through any means. Even using
the Nobeyama 45-m Radio Telescope, detecting carbonmonoxide spectral lines from nearby galaxies required
an exposure time of about 1 hour per pointing. But todaywith the Subaru Telescope, we can see the redshift 7
Universe (12.9 billion light-years away) and ALMA
promises to detect even farther galaxies. I feel that wehave truly entered a new generation of astronomy.
ALMA is producing interesting results in the field ofplanetary system formation. One of the surprises we’ve
learned is that the dust which becomes the material forplanets is localized inside protoplanetary disks (gasdisks.) The biggest problem in modern planetary systemformation theory is how dust grains on the order of 1
micron in size amalgamate up to planetesimals on theorder of several kilometers in size. It is very difficultfor dust grains to collect and form planetesimals in thecase where the dust particles are scattered around thestar in the same formation as the gas disk. But if just the
dust grains are localized at areas within the gas disk, it
becomes especially easy for planetesimals to form. Thisis a very interesting result.
In addition, test observations with the ultra-wide-fieldprime focus camera (Hyper Suprime-cam) have finishedat the Subaru Telescope and the Strategic Observation
Program has been assigned 300 nights over the next 5
years. This camera’s survey speed (=limiting magnitude
x area of the field of view) is over 10 times greater thanprevious surveys. Thanks to this camera, the Subaru
Telescope’s observations will be the world’s forerunners
without question, until LSST (America’s Large Synoptic
Survey Telescope) becomes operational in the mid 2020’s.
Observations with this camera will elucidate the largescale distribution of dark matter in the Universe. It shouldbe able to constrain the characteristics of dark matter anddark energy in the quest to understand the evolution of
the large-scale structure of the Universe.
Noteworthy FY 2013 results, in addition to thosementioned above, are cited below. First, through yearsof observations by Mizusawa VLBI Observatory’s
VERA Project measuring the rotation of the galaxy withgreater accuracy than before, we learned that the galacticrotation velocity in the vicinity of the Sun is about 10 %faster than previous estimates. This shows that the Milky
Way’s mass (dark matter) is about 20 % larger than waspreviously thought. Also, using the Subaru Telescope’s
high contrast camera HiCIAO the extra-solar planet
survey project succeeded in the direct imaging of an
exoplanet with 4 times the mass of Jupiter (a Second
Jupiter.) It was determined that with TMT we should be
able to take a direct image of an Earthlike planet andanalyze its atmospheric composition.
In other matters deserving mention, I want to point out
the completion of the career path for technical staff. Thishas been an issue since before the NAOJ was established;
there have not been suitable high level positions intechnical fields, or people have not been appointed tothem. Now, technical staff can select the new career path,taking proper advantage of the freedom of the personnel
system which increased when we incorporated.
With the Subaru Telescope, NAOJ established its firstoverseas research facility. After that, ALMA proceeded
through cooperation with Europe and the Americas. In
the world of astronomy, this was the first instance of
this level of international collaboration. I think the factthat as one of the members of this kind of international
collaboration NAOJ participates as a principal partner
shows that, even from an international viewpoint,
Japanese astronomy has attained leading-edge status.
But I don’t believe that the internationalization ofJapanese university research institutions, NAOJ included,
has reached a sufficient level yet. An environment where
faculty who don’t speak Japanese can comfortably
conduct research has not been adequately prepared. Even
at NAOJ foreign research appointments are actively
proceeding, but I feel that to be seen by the world asa true international open astronomy research facility,internationalization is required in every aspect, including
the Administration Department. Similar problems also
arise with attempts to increase the number of womenfaculty members. I feel we must reexamine the entire
NAOJ, or even up to the level of the National Institutes of
Natural Sciences, to address these issues.

Masahiko HAYASHI
Director General of NAOJ

I Scientific Highlights(April 2013 – March 2014)
01 Magnetic Diffusion and Ion Nonlinear Dynamics in Magnetic Reconnection

Zenitani, S., et al.

003

02

Radiative Transfer Simulations of Neutron Star Mergers: Toward Multi-Messenger
Astronomy

Tanaka, M., et al.

004

03

Unusual Migration of the Prominence Activities in the Southern Hemisphere during
Cycle 23‒24

Shimojo, M.

005

Imanishi, M., Saito, Y.

006

Imanishi, M., Nakanishi, K.

007

06 Looking into the Sky of a Super-Earth

Narita, N., et al.

008

07 High Ecliptic Latitude Survey for Small Main-belt Asteroids

Terai, T., et al.

009

Terai, T., Itoh, Y.

010

Terai, T., et al.

011

Hashimoto, J., et al.

012

04 Subaru High-Spatial-Resolution Infrared Imaging of Gas-Rich Merging Galaxies
05 ALMA Observations of Luminous Infrared Galaxies Using Dense Gas Tracers

08 High-Precision Measurements of the Brightness Variation of Nereid
09 Time-series Photometry of Earth Flyby Asteroid 2012 DA14
10 NIR Polarimetric Imaging of Circumstellar Disks by Subaru/SEEDS
11

Construction of Gauge-invariant Variables of Linear Metric Perturbations on an Arbitrary
Background Spacetime

Nakamura, K.

013

12

On the Formation Timescale of Massive Cluster Ellipticals Based on Deep Near-infrared
Spectroscopy at z ~ 2Tanaka, M., et al.

014

Takeda, Y., et al.

015

Urakawa, S., et al.

016

Yagi, M., et al.

017

Sadakane, K., et al.

018

Fujii, M., Portegies Zwart, S.

019

18 Atmospheric Study of the Hot Uranus GJ3470b via Multi-band Simultaneous Photometry

Fukui, A., et al.

020

19 Star Formation Rate and Metallicity in Damped Lymanα System

Okoshi, K., et al.

021

20 Nature of Hα Selected Galaxies at z > 2. I. Main Sequence and Dusty Star-forming Galaxies

Tadaki, K.-i., et al.

022

Nature of Hα Selected Galaxies at z > 2. II. Clumpy Galaxies and Compact Star-forming
Galaxies

Tadaki, K.-i., et al.

023

22 High-Albedo C-Complex Asteroids In The Outer Main Belt: The Near Infrared Spectra

Kasuga, T., et al.

024

23 Development of High Damage Threshold and Ultra-low Loss Mirrors

Tatsumi, D., et al.

025

24 Detection of an Ultra-bright Submillimeter Galaxy behind the Small Magellanic Cloud

Takekoshi, T., et al.

026

Discovery of Hot Water Vapor Gas Disk around a Massive Protostar Candidate Orion KL
Source I

Hirota, T., et al.

027

26 Calibrating [OII] Star-formation Rates at z > 1 from Dual Hα-[O II] Imaging from HiZELS

Hayashi, M., et al.

028

Sato, B., et al.

029

Kashino, D., et al.

030

13 On the Sodium versus Iron Correlation in Late B-Type Stars
14 Visible Spectroscopic Observations of a Near-Earth Object, 2012 DA14
15 Starformation in Ram-pressure Stripped Gas Tail in the Virgo Cluster
16

Discovery of Disk Origin Narrow Metallic Absorption Lines Observed during the2009‒2011 Eclipse of ϵ Aurigae

17 The Core-Collapse Time of Star Clusters with Mass Functions

21

25

27 Planetary Companions to Three Intermediate-Mass GK Giants
28 Growth of Massive Galaxies in the Early Universe Revealed by Subaruʼs FMOS
29

Dense Optical and Near-Infrared Monitoring of CTA 102 during High State in 2012 with Oister;
Detection of Intra-Night “Orphan Polarized Flux Flare”

Itoh, R., et al.

031

30

Minute-scale Rapid Variability of the Optical Polarization in the Narrow-line Seyfert 1
Galaxy PMN J0948+0022

Itoh, R., et al.

032

31

Measurements of Coronal and Chromospheric Magnetic Fields Using Polarization
Observations by the Nobeyama RadioheliographIwai, K., Shibasaki, K.

033

001

32 600 Pixels MKID Superconductive Millimeter-wave Camera
33 The Mass-metallicity Relation at z ~ 1.4 Revealed with Subaru/FMOS
34 GRB 130427A: A Nearby Ordinary Monster

034

Yabe, K., et al.

035

Maselli, A., et al.

036

35

Numerical Treatment of Anisotropic Radiation Field Coupling with the Relativistic
Resistive Magnetofluids

Takahashi, H., Ohsuga, K.

037

36

Direct Imaging of a Compact Molecular Outflow from a Very Low Luminosity Object:
L1521F-IRS

Takahashi, S., et al.

038

Matsumoto, J.

039

Kasukabe, M., et al.

040

Kasukabe, M., et al.

041

37 Growth of Rayleigh-Taylor and Richtmyer-Meshkov Instabilities in Relativistic Jets
38 A Big-Bang Nucleosynthesis Limit on the Neutral Fermion Decays into Neutrinos
39

7Be Charge Exchange between 7Be3+ Ion and Exotic Long-lived Negatively Charged

Massive Particle in Big Bang Nucleosynthesis40

R-process Nucleosynthesis in the Central Engine of Gamma-Ray Bursts, i.e. Neutrino-Heated
Collapsar Jets

Nakamura, K., et al.

042

41

Supernova Neutrino Nucleosynthesis of Radioactive 92Nb and the Timescale for Solar
System Formation

Hayakawa, T., et al.

043

42

Asymmetric Neutrino Production in Magnetized Proto-Neutron Stars in Fully Relativistic
Mean-Field Theory and Application to Pulsar Kick and Rotational Spin Down

Maruyama, T., et al.

044

Suzuki, T., Kajino, T.

045

Sakai, N., et al.

046

Kuzuhara, M., et al.

047

Utsumi, Y., et al.

048

Hibi, Y., et al.

049

48 In-medium Effects on Neutrino Reactions inside the Neutron Star

Cheoun, M-.K., et al.

050

49 Neutron Stars in a Perturbative f(R) Gravity Model with Strong Magnetic Fields

Cheoun, M-.K., et al.

051

Kajino, T., et al.

052

Shibasaki, K., et al.

053

43 Astronomical Method to Determine the Neutrino Mass Hierarchy
44

Absolute Proper Motion of IRAS 00259+5625 with VERA: Indication of Superbubble
Expansion Motion

45 Direct Imaging of a Cold Jovian Planet Orbiting the Sun-like Star GJ 504
46 Reducing Systematic Error in Weak Lensing Cluster Surveys
47 Toward Realization of Submillimeter-wave Camera

50

Origin of Ultra High-Energy Neutrinos via Heavy-Meson Synchrotron Emission in Strong
Magnetic Fields

51 Long-term Global Solar Activity Observed by the Nobeyama Radioheliograph002

Sekimoto, Y., et al.

Magnetic Diffusion and Ion Nonlinear Dynamics
in Magnetic Reconnection			

ZENITANI, Seiji(NAOJ)			

				

SHINOHARA, Iku(JAXA/ISAS)

WADA, Tomohide(NAOJ)		

Collisionless magnetic reconnection is an important
process of energy release in space and astrophysicalplasmas. It is challenging to understand the physics ofcollisionless reconnection, because we have to deal withthe fully kinetic motion of all particle species. In thiswork, we study the ion kinetic motion in the reconnection
outflow region by means of 2D particle-in-cell (PIC)
simulations [1].
Collisionless reconnection exhibits a 3D structureof magnetic field lines, as they are dragged out-of-page(Fig. 1). This stems from the decoupling of the motionof electrons and ions. Such complex magnetic topology
makes it difficult to understand the particle dynamics.
Figure 2 shows an ion velocity distribution function(VDF), taken in the “Hall physics region” in Figure 1. As
can be seen, it is very different from an isotropic one ofgyrating ions.
We analyze this VDF in analogy with the nonlinear
particle dynamics in curved magnetic topology [2]. We
translate the VDF to a Poincaré map (the bottom-leftpanel in Fig. 2) in the curved field. The Poincaré map tells
us that the ions undergo chaotic motions instead of full
gyrations, and it brings deep insight to particle motions.
We extensively discuss the components of the VDF andthe relevant ion motions in Ref. [1]. For example, wefind that some ions are confined in a narrow path, the socalled “regular orbit.” This is evident in the small humpin the VDF and the closed circles in the Poincaré map, as
indicated by the arrows in Figure 2.
It is noteworthy that the ion ideal condition is violated→→
in the Hall-physics region, E + v→i × B ≠ 0, because
the ions no longer gyrate. Traditionally, the plasma
nonidealness has been considered as a signature of thereconnection diffusion-region. However, we argue that
this Hall-physics region is outside the diffusion region,
because the diffusion region should the place where the→system relaxes into the plasma frozen-in state of × (E→→+ v × B) = 0 [3]. The physics and the structure of thereconnection site should be reconsidered, taking these
updates into account.

NAGAI, Tsugunobu(Tokyo Institute of Technology)

UMEDA, Takayuki(Nagoya University)

Figure 1: The magnetic field lines in our 2D PIC simulation. The
rear panel (color contour) indicates the out-of-planecomponent, By (Reprinted from Ref. [1]).

Figure 2: (Main) Ion velocity distribution function in the Hallphysics region. (Bottom-left) Poincaré map for a
relevant parameter.

References[1] Zenitani, S., et al.: 2013, Phys. Plasmas, 20, 092120.
[2] Chen, P., Palmadesso, P. J.: 1986, J. Geophys. Res., 91, 1499.
[3] Zenitani, S., Umeda, T.: 2014, Phys. Plasmas, 21, 034503.

I Scientific Highlights

003

ΔRadiative Transfer Simulations of Neutron Star Mergers:
Toward Multi-Messenger Astronomy
TANAKA, Masaomi(NAOJ)		

		

WANAJO, Shinya

HOTOKEZAKA, Kenta(The Hebrew University of Jerusalem)

KYUTOKU, Koutaro(University of Wisconsin-Milwaukee)

KIUCHI, Kenta, SEKIGUCHI, Yuichiro, SHIBATA, Masaru(NAOJ)					Next-generation gravitational-wave telescopes, such
as Advanced LIGO, Advanced Virgo, and KAGRA,
are expected to directly detect gravitational waves
from neutron star (NS) mergers within about 200 Mpc.
However, the accuracy of positional localization withgravitational-wave telescopes is only about 10 – 100
deg2. Therefore, to fully understand the nature of thegravitational-wave sources, it is extremely important to
identify electromagnetic wave counterparts.
Optical/infrared emission powered by radioactive
decay of r-process nuclei synthesized in the NS merger
is one of the most promising counterparts. However,detailed theoretical prediction was difficult due to ourpoor understanding of photon transfer in the NS merger
ejecta. We succeeded in radiative transfer simulations of
NS merger including detailed r-process elements for the
first time (Figure 1, [1]) using Cray XC30 supercomputer(ATERUI) at Center for Computational Astrophysics(CfCA), NAOJ.
We show that the optical/infrared emission is fainterthan previously expected by a factor of 10. However,this emission is, in fact, detectable with 4 – 8 m classtelescopes (Figure 2). We also performed radiativetransfer simulations for the merger of black hole (BH)
and NS [2]. We showed that the observed brightness of
BH-NS mergers can be comparable to or even higher
than that of NS-NS mergers. In addition, we find that theemission from BH-NS mergers tends to be bluer thanthat from NS-NS mergers. Thanks to these properties, wemight be able to distinguish BH-NS merger events from
NS-NS merger events by multi-band observations.
Based on these results, we can determine the efficient
observing strategy to search for the electromagnetic
counterparts. Our simulations are one of the first steps
toward a new field of astronomy – “multi-messenger
astronomy” which combines observations of electromagnetic waves and gravitational waves.

(Kyoto University)

Figure 1: Snapshot of the radiative transfer simulation of NS
mergers.

Figure 2: Expected i-band light curves of NS-NS mergers at
200 Mpc. Red and blue lines show the models withdifferent equation of states.
References[1] Tanaka, M., Hotokezaka, K.: 2013, ApJ, 775, 113.
[2] Tanaka, M., et al.: 2014, ApJ, 780, 31.

004

I Scientific Highlights

Unusual Migration of the Prominence Activities
in the Southern Hemisphere during Cycle 23‒24
SHIMOJO, Masumi(NAOJ)The solar activity in Cycle 23‒24 shows differencesfrom the previous cycles that were observed with modern
instruments, e.g. long cycle duration and a small numberof sunspots. To appreciate the anomalies further, weinvestigated the prominence eruptions and disappearances
observed with the Nobeyama Radioheliograph during
over 20 years. Consequently, we found that theoccurrence of the prominence activities in the northernhemisphere is normal because the period of the number
variation is 11 years and the migration of the producing
region of the prominence activities traces the migrationof 11 years ago. On the other hand, the migration in thesouthern hemisphere significantly differs from that in
the northern hemisphere and the previous cycles. The
prominence activities occurred over -50 degrees latitudein spite of the late decay phase of Cycle 23, and the

1992

1995

1998

number of the prominence activities in the higher latitude
region (over -65 degrees) is very small even near thesolar maximum of Cycle 24. The results suggest that theanomalies of the global magnetic field distribution started
at the solar maximum of Cycle 23. Comparison of thebutterfly diagram of the prominence activities with themagnetic butterfly diagram indicates that the timing of
the rush to the pole" and the polar magnetic field closely
relates to the unusual migration. Considering that therush to the pole is made of the sunspots, the hemisphericasymmetry of the sunspots and the strength of the polar
magnetic fields are essential for understanding theanomalies of the prominence activities [1].
Reference[1] Shimojo, M.: 2013, PASJ, 65, S16.

Year
2001
2004

2007

2010

2013

90

Carrington Latitude

50

0

-50

-90
1850

1900

1950

2000
2050
Carrington Number

2100

2150

Figure 1: The butterfly diagram of the prominence activities and the photospheric magnetic field. The red dots indicate the dates and latitudesof the prominence activities and the grayscale shows the magnetic field distribution. The blue and green dashed lines indicate thesolar minimum and maximum.

I Scientific Highlights005

Subaru High-Spatial-Resolution Infrared Imaging
of Gas-Rich Merging Galaxies
				

IMANISHI, Masatoshi(NAOJ)			

According to the widely-accepted cold-dark-matterbased galaxy formation scenario, small gas-rich galaxies
collide and merge, and evolve into massive galaxies.
Recent observations of nearby galaxies have shownthat supermassive blackholes (SMBHs) with >106 solar
mass are ubiquitously present at the center of galaxies,
and that the masses of central SMBHs and galaxy stellar
components are correlated. When gas-rich galaxies collide
and merge, a large amount of gas is quickly transported to
the nuclear regions, and active starburst activity occurs.
At the same time, such gas can accrete onto the preexisting SMBHs, and such accreting SMBHs can become
luminous and be observed as active galactic nucleus(AGN) activity. Investigating these kinds of activity is
crucial to understand the galaxy formation process in theuniverse, but such activity is deeply obscured by gas anddust, so that observations at the wavelength of low dust
extinction are necessary.
We have developed a unique method to clearly distinguish between AGN and starburst activity, based onhigh-spatial-resolution, infrared K-band (2.2 μm) and L’band (3.8 μm) imaging observations, assisted with theadaptive optics system of the Subaru Telescope, because
the effects of dust extinction are small in these infrared
K- and L’-bands. Since a mass-accreting SMBH hasmuch higher radiative energy generation efficiency than
nuclear fusion reaction inside stars, an AGN can produce
a larger amount of hot (several 100 K) dust in the close
vicinity. Such hot dust produces strong infrared L’-band
emission, so that K‒L’ colors become distinctly different
between AGNs and starbursts, making the colors an
excellent indicator to distinguish between these kinds ofactivity.
We have observed 29 infrared-luminous gas-richmerging galaxies, and detected at least one active
SMBH in 28 sources, demonstrating that our infrared
method is very powerful to detect deeply buried AGNs
in merging galaxy nuclei. However, multiple AGNs havebeen found only in 4 sources (~15 %) (Figure 1). Since
multiple SMBHs are expected in merging galaxies, thesmall detectable fraction of multiple AGNs (=active
SMBHs) indicates that not all SMBHs are actively massaccreting and become luminous AGNs. AGN luminosity
is proportional to the mass accretion rate onto a SMBH.
The AGN luminosity, divided by SMBH mass, is widelyused to measure how active a SMBH is. We found that
the SMBH-mass normalized AGN luminosity is higher
in more massive SMBHs than less massive SMBHs inmerging galaxies [1].

006

I Scientific Highlights

SAITO, Yuriko(GUAS/NAOJ)

Since the gravitational force of a SMBH increases, in
proportion to the SMBH mass, more massive SMBH canattract a larger amount of surrounding material than lessmassive SMBH. However, our result means that activityof SMBH is higher for more massive SMBH, even after
the normalization by SMBH mass. Namely, the amountof accreting material onto SMBH increases more rapidly
than the increase of SMBH mass. Given the abovementioned relation between SMBH mass and galaxy
stellar mass, our result is interpreted that SMBHs are
more active in more massive galaxies. Recently, the socalled galaxy-downsizing phenomenon has widely been
discussed, where more massive galaxies are generally
redder in colors, and have finished major star-formationin an earlier cosmic age than less massive galaxies. Thisphenomenon apparently contradicts to the cold-darkmatter based galaxy formation scenario which postulates
that small galaxies are formed first. It is theoretically
proposed that if SMBHs are more active and AGN
radiation effects are stronger in more massive galaxies,
then this galaxy-downsizing phenomenon could be
reproduced. Our result may support this scenario.

Figure 1: Examples of infrared K- and L’-band images of merging
galaxies with detected multiple active SMBHs [1].

Reference[1] Imanishi, M., Saito, Y.: 2014, ApJ, 780, 106.

ALMA Observations of Luminous Infrared Galaxies
Using Dense Gas Tracers
IMANISHI, Masatoshi, NAKANISHI, Kouichiro(NAOJ)

Luminous infrared galaxies (LIRGs) emit strong
infrared radiation, and are usually formed by the collisionand merger of gas-rich galaxies. The strong infraredemission is originated in thermal radiation from dust
heated by dust-obscured starburst and/or AGN activity.
Compared to normal quiescently star-forming galaxies,
the fraction of dense gas is high in LIRGs. It is also
predicted that since starburst and AGN activity havedifferent effects to the surrounding dense gas, molecularemission line flux ratios can vary, depending on the
primary energy source. Molecular rotational J-transitionlines, seen in the (sub)millimeter wavelength range,usually do not suffer from significant dust extinction, sothat these lines can be used to understand the physicaland chemical properties deeply obscured by gas and dustat LIRGs’ nuclei. In ALMA Cycle 0, we observed six
LIRGs, using HCN, HCO+, and HNC J = 4‒3 lines, which
are good tracers of dense gas. Results of two LIRGs havebeen published [1,2].
In the starburst-dominated LIRG, NGC 1614, theobserved molecular lines are clearly spatially-resolved.
The emission peak is separated from the nucleus by ~0.6”(Figure 1). This is the location where strong starburst
activity is found. Our result supports the widely-argued
scenario that stars are formed inside dense molecular gas.
In NGC 1614, HCO+ J = 4‒3 emission is much stronger
than HCN J = 4‒3 emission (Figure 1).
In the starburst and AGN composite LIRG, IRAS
20551 ‒ 4250, the HCN-to-HCO + J = 4 ‒ 3 flux ratio ishigher than NGC 1614 (Figure 2). It has been known
that AGNs tend to show higher HCN-to-HCO+ J = 1‒0flux ratio than starburst-dominated galaxies. The same
trend is confirmed at the J = 4‒3 transition line. Since
the wavelength of J = 4 ‒ 3 transition is shorter thanJ = 1 ‒ 0 transition, we will be able to observe moredistant galaxies at J = 4 ‒ 3 with ALMA. Second, thevibrationally-excited HCN J = 4‒3 emission line (v2 = 1f)
is detected (Figure 3). This is the second detection of thisline in external galaxies. Infrared radiative pumping, byabsorbing 14 μm photons, is a plausible scenario for thisvibrational excitation. Since an AGN can emit stronger
infrared 14 μm photons, due to AGN-heated hot dust,
than starburst galaxies, HCN J-transition line emissionin AGNs could be enhanced due to this infrared radiative
pumping mechanism. Finally, in addition to the targetedlines, other lines, such as H2S 3(2,1)‒3(1,2) (369.1 GHz in
rest-frequency) and CH3CN v = 0 19(3)‒18(3) (349.4 GHz
in rest-frequency) emission lines, are clearly detected(Figure 2), demonstrating the high sensitivity of ALMA.

Figure 1: Spatial distribution of the red and blue componentsof HCN J = 4‒3 (Left) and HCO + J = 4‒3 (Right) inthe LIRG, NGC 1614. For HCN, the contours start at
0.4 Jy km s−1, and increases with 0.2 Jy km s−1. For HCO+,
the contours start at 0.5 Jy km s−1, and increase with
0.5 Jy km s−1.

Figure 2: ALMA spectrum of the LIRG, IRAS 20551‒4250.
The ordinate is flux (mJy beam−1), and the abscissa isobserved frequency (GHz).

Figure 3: Integrated intensity map of the vibrationally-excited
HCN J = 4‒3 (v 2 = 1f) emission line and expanded
spectrum around this line for IRAS 20551‒4250.
References[1] Imanishi, M., Nakanishi, K.: 2013, AJ, 146, 47.
[2] Imanishi, M., Nakanishi, K.: 2013, AJ, 146, 91.

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Looking into the Sky of a Super-Earth
NARITA, Norio1/2, FUKUI, Akihiko1, IKOMA, Masahiro3, HORI, Yasunori1, KUROSAKI, Kenji3
KAWASHIMA,Yui3, NAGAYAMA, Takahiro4, ONITSUKA, Masahiro2/1, SUKOM, Amnart2/1, NAKAJIMA, Yasushi5
NISHIYAMA, Shogo1, TAMURA, Motohide3/1, KURODA, Daisuke1, YANAGISAWA, Kenshi1
HIRANO, Teruyuki6, KAWAUCHI, Kiyoe6, KUZUHARA, Masayuki6, OHNUKI, Hiroshi6, SUENAGA, Takuya2/1
TAKAHASHI, Yasuhiro3/1, IZUMIURA, Hideyuki1, KAWAI, Nobuyuki6, YOSHIDA, Michitoshi7
1: NAOJ, 2: Graduate University for Advanced Studies, 3: University of Tokyo, 4: Nagoya University, 5: Hitotsubashi University, 6: Tokyo
Institute of Technology, 7: Hiroshima University

Super-Earths are emerging as a new type of exoplanetwith a mass and radius larger than the Earth's but lessthan those of ice giants in our Solar System, such as
Uranus or Neptune.
Current theories explain that a planet forms in a
protoplanetary disk. Hydrogen is a major component of a
protoplanetary disk, and water ice is abundant in an outerregion beyond a so-called “snow line.” Findings about
where super-Earths have formed and how they havemigrated to their current orbits point to the predictionthat hydrogen or water vapor is a major atmosphericcomponent of a super-Earth. Thus if one can determine
the major atmospheric component of a super-Earth,
one can then infer the planet’s birthplace and formation
history.
Planetary transits enable us to investigate changes
in the wavelength in the depth of dimming of the stellar
brightness (i.e., transit depth), which provide information
about the planet’s atmospheric composition. Thismethodology is referred to as transmission spectroscopy(see figure 1).
We focused on investigating the atmospheric featuresof one super-Earth, GJ 1214 b, which is one of the wellknown super-Earths discovered by the MEarth Project.
We used the two optical cameras Suprime-Cam and
FOCAS on the Subaru 8.2 m Telescope and the SIRIUS
camera on the IRSF 1.4 m telescope to see the feature of
GJ 1214 b’s atmosphere.
Our observations showed that GJ 1214 b’s atmospheredoes not display strong Rayleigh scattering ([1,2]: seefigure 2). This finding implies that the planet has a waterrich atmospher or a cloud-covered atmosphere.
Although there are only a small number of superEarths that astronomers can observe in the sky now, thissituation will dramatically change when the Transiting
Exoplanet Survey Satellite (TESS) begins its wholesky survey of small transiting exoplanets in our solar
neighborhood. When new targets become available, we
can study the atmospheres of many super-Earths. Suchobservations will allow us to learn even more about thenature of various super-Earths.
References[1] Narita, N., et al.: 2013a, PASJ, 65, 27.
[2] Narita, N., et al.: 2013b, ApJ, 773, 144.

008

I Scientific Highlights

Figure 1: An illustration of the relationship between thecomposition of the atmosphere and transmitted colorsof light. Top: If the sky has a clear, upward-extended,hydrogendominated atmosphere, Rayleigh scattering
disperses a large portion of the blue light from theatmosphere of the host while it scatters less of the red
light. Middle: If the sky has a less extended, waterrich atmosphere, the effect of the Rayleigh scattering ismuch weaker than in a hydrogen-dominated atmosphere.
In this case, transits in all colors have almost the sametransit depths. Bottom: If the sky has extensive clouds,
most of the light cannot be transmitted through theatmosphere, even though hydrogen dominates it. As aresult, transits in all colors have almost the same transit
depths. (Credit: NAOJ)

Figure 2: Observed transit depths and theoretical models for GJ
1214 b (based on [2]).

High Ecliptic Latitude Survey for Small Main-belt Asteroids			

TERAI, Tsuyoshi(NAOJ)			

Main-belt asteroids (MBAs) located in the asteroid
dense zone between Mars and Jupiter orbits continuously
collide with one another. Collisional evolution refers tochanges in the number-diameter distribution for asteroids,
hereinafter called size distribution, as collisions repeat
over time. Asteroids larger than ~100 m in diameter havea scaling law that the strength against impact disruption
increases with body size. The increasing degree of impact
strength is the primary factor that determines the size
distribution of MBAs [1]. Therefore, measurements of thesize distribution allow us to examine the asteroid strengthlaw The development of collisional evolution models ofMBAs is proceeding using the size distributions with avariety of size ranges obtained by a number of previous
survey observations.
However, MBA’s collisional evolution could havebeen different in the early solar system because newborn
Jupiter dynamically excited asteroid orbits (pumped
up eccentricities and inclinations) and sped up theircollision velocities much faster than at present [2]. We
know very little about the impact strength law under such
hypervelocity collisions. To address this question, we
focused our research on the size distribution of asteroids
with highly inclined orbits, because their collisional
velocities are significantly high and can provide
information about asteroid collisions with high velocity.
No previous observations have measured the size
distribution of high-inclination asteroids in the desirable
range of several hundred meters to several kilometerswhich is close to the boundary between the gravity-scaled
and strength-scaled regimes. We used Subaru/SuprimeCam to conduct an optical wide-field observation of small
main-belt asteroids with high inclinations. We surveyed
26.5 deg 2 of high ecliptic latitude fields around +25°
in two nights using our efficient method for detecting
moving object (figure 1).
As a result of our data analysis, 441 moving objects
were detected in good-condition data of 13.6 deg2 [3].
Orbital estimation indicates that about 380 of them are
MBA candidates Since the diameters of these asteroids
are too small to measure directly, we calculated theirsize from photometric brightness. Most of the detected
asteroids have diameters of 0.6‒6 km and inclinations
higher than 15°. We found that the slope of the size
distribution changes sharply around 1 km in diameter(figure 2). This is the same pattern that a previous study
confirmed in MBAs near the ecliptic plane dominatedby low-inclination asteroids. A careful comparison of
the size distribution in the range of 0.6‒5 km with thatof asteroids near the ecliptic plane revealed that high-

TAKAHASHI, Jun, ITOH, Yoichi(University of Hyogo)

inclination asteroids have a shallower size distribution.
We consider that hypervelocity collisions accelerate
the rate of increase in the impact strength according toasteroid size. It indicates that large bodies have a higher
disruptive strength and longer lifespan relative to tiny
bodies than the ecliptic asteroids during the dynamical
excitation phase in the early solar system.

Figure 1: (Left and center) Subaru/Suprime-Cam r'-band images
obtained at 20-min intervals. (Right) Processed image
from the original images. Only the moving asteroid
remains after the background objects were masked.

Figure 2: Cumulative size distribution of our MBA sample withthe detection limit of 0.56 km in diameter (dotted line).
The circles show the diameter range used for evaluationof the distribution slope and the crosses show theexcluded range. The blue and green solid lines show the
best-fit power laws in the ranges smaller/larger than 1 km,
respectively.

References[1] O'Brien, D. P., Greenberg, R.: 2003, Icarus, 164, 334.
[2] Bottke, W. F., et al.: 2005, Icarus, 175, 111.
[3] Terai, T., Takahashi, J., Itoh, Y.: 2013, AJ, 146, 111.

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009

High-Precision Measurements of the Brightness Variation of Nereid				

TERAI, Tsuyoshi(NAOJ)		

Neptune II Nereid, the second largest Neptuniansatellite, has a prograde orbit with a large semi-major axis
(0.05 Hill radius) as well as high eccentricity (0.75) andis categorized as an irregular satellite. Irregular satellites
are generally believed to have been captured fromheliocentric orbits by the host planets in the early solar
system. However, Goldreich et al. (1989) suggest that
Nereid originally formed close to Neptune in the circumplanetary disk, and was then transported outward due tothe perturbation by Neptune I Triton [1]. Each of previous
photometric observations for Nereid reported different
rotation period and brightness amplitude. Therefore, it is
proposed that Nereid's rotation is on chaotic variation [2]or has long-term variability produced by precession of thespin axis [3], both of which support the in-situ formation
model. In contrast, Grav et al. (2003) showed the rotation
period of 11.5 hr and exclude the possibility of chaotic
rotation [4]. The rotation state remains uncertain and theorigin has been yet poorly understood.
We measured the brightness variation of Nereid with
unprecedented precision using 3-night imaging dataaround Neptune obtained by Subaru/Suprime-Cam [5].
The resulting lightcurve (figure 1) shows the rotation
period of 11.5 ± 0.1 hr and peak-to-peak amplitude of
0.031 ± 0.001 mag. These values agree well with Grav
et al. (2003), indicating a constant rotation state. In
addition, the rapid spin rate rejects a chaotic rotation.
We also found the consistency of Nereid's rotation
period based on the size-rotation and color distributionsof trans-Neptunian objects (TNOs). It is likely that
Nereid originated as an immigrant body captured
from a heliocentric orbit. The source region could besame as TNOs, which is consistent with the outward
transportation model of TNOs [6].

010

I Scientific Highlights

ITOH, Yoichi(University of Hyogo)

Figure 1: Lightcurve of Nereid with a period of 5.75 hr. The
vertical axis shows the normalized magnitude corrected
for the difference of heliocentric/geocentric distancesand solar phase angle. The circles, triangles, and squares
represent data obtained on 2008 September 1, 2, and 29,
respectively. The dashed curve is the best-fit model witha peak-to-peak amplitude of 0.031 mag.

References[1] Goldreich, P., et al.: 1989, Science, 245, 500.
[2] Dobrovolskis, A. R.: 1995 Icarus, 118, 181.
[3] Schaefer, B. E., et al.: 2008, Icarus, 196, 225.
[4] Grav, T., Holman, M. J., Kavelaars, J. J.: 2003, ApJ, 591, L71.
[5] Terai, T., Itoh, Y.: 2013, PASJ, 65, 46.
[6] Gomes, R. S.: 2003, Icarus, 161, 404.

Time-series Photometry of Earth Flyby Asteroid 2012 DA14TERAI, Tsuyoshi, YOSHIDA, Fumi			

(NAOJ)		

URAKAWA, Seitaro(Japan Spaceguard Association)

TAKAHASHI, Jun(University of Hyogo)

OASA, Yumiko, OSHIMA, Goichi, ARATANI, Kenta, HOSHI, Hisaki
SATO, Taiki, USHIODA, Kazutoshi(Saitama University)

2012 DA14, a near-Earth object in diameter of several
ten meters, passed closely to the Earth at a distanceof about 27,700 km inside a geosynchronous orbit on
February 16, 2013 JST. Such a small asteroid is usually
too faint to be observed, The Earth flyby allowed us for
precise measurements of 2012 DA14 even with a small
telescope because the asteroid became brighter than 7th
magnitude in the optical. We focused on wide variationof the solar phase angle of 2012 DA14 around its closest
approach and performed a time-series photometricobservation to obtain the phase curve. It provides
useful indications of asteroid surface properties, suchas geometric albedo and regolith structure. This event
was an exciting opportunity to investigate the surface
properties of such a small asteroid.
Our observations have been carried out for 2 hours
around the closest approach of 2012 DA14 using the 0.55m telescope at Saitama University. Since the asteroid
moved on the sky with extremely high speed of ~50
arcmin min−1 in maximum, we mounted a CCD cameraon the prime focus to cover a wide field of view (32′ × 32′)
and took images sequentially with 0.5-sec exposures. The
instrument and technique allowed us to keep tracking theasteroid all over this observation. Fortunately, in contrast,
the phase angle was constant during the following night.
We performed an additional observation on the next night
to measure the rotational lightcurve.
Our periodogram analysis determined the rotational
period of 11.0 hr and peak-to-peak amplitude of 1.6
mag [1]. The best-fit synthetic model generated froma combination of a given phase curve and the obtained
rotational lightcurve shows that the slope of the phasecurve is significantly shallower than that of S-type
asteroids. 2012 DA14 has been classified as an L-type
asteroid [2,3] the typical geometric albedo of which
is low compared to S-type asteroids. This result isinconsistent with the known inverse correlation between
phase curve and geometric albedo, indicating that 2012
DA14 is likely to have a different surface property fromknown L-type asteroids. We suggest that 2012 DA 14
is coated with a coarse surface that lacks fine regolithparticles and/or a high albedo surface.

Figure 1: R-band images of 2012 DA14 at the closest approachwith 0.5-sec exposures. Time is shown in JST. The fieldof view covers 32′ × 32′.

Figure 2: Brightness variation of 2012 DA14 around the closest
approach. The horizontal axes show time (left) and solar
phase angle (right). The circles, solid lines, and dottedline are the data points, best-fit synthetic model, andmodel phase function, respectively.

References[1] Terai, T., et al.: 2013, A&A, 559, A106.
[2] de Leon, J., et al.: 2013, A&A, 555, L2.
[3] Urakawa, S., et al.: 2013, PASJ, 65, L9.

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011

NIR Polarimetric Imaging of Circumstellar Disks by Subaru/SEEDSHASHIMOTO, Jun1, WISNIEWSKI, John1, FOLLETTE, Katherine2, CLOSE, Laird2, MOMOSE, Munetake3
ANDREWS, Sean4, TAKAMI, Michihiro5, KARR, Jennifer5, KIM, Hyosun5, CHOU, Mei-Yin5, MAYAMA, Satoshi6
CURRIE, Thayne7, HODDAP, Klaus8, TAMURA, Motohide9, HAYASHI, Masahiko9, ISHII, Miki9, IYE, Masanori9
KANDORI, Ryo9, KUSAKABE, Nobuhiko9, KWON, Jangmi9, MORINO, Jun-ichi9, SUZUKI, Ryuji9, SUTO, Hirohi9
HENNING, Thomas10, BRANDER, Wolfgang10, FELDT, Markus10, WHITNEY, Barbara11, GRADY, Carol12
MCELWAIN, Michael12, KUDO, Tomoyuki9, EGNER, Sebastian9, GUYON, Olivier9, HAYANO, Yutaka9
HAYASHI, Saeko9, NISHIMURA, Tetsuo9, PYO, Tae-Soo9, TAKAMI, Hideki9, TAKATO, Naruhisa9
TERADA, Hiroshi9, TOMONO, Daigo9, USUDA, Tomonori9, KUZUHARA, Masayuki13, BRANDT, Timothy14
DONG, Ruobing14, JANSON, Markus14, KNAPP, Gillian14, TURNER, Edwin14, ITOH, Yoichi15, ABE, Lyu16
CARSON, Joseph17, GOTO, Miwa18, MATSUO, Taro19, MORO-MARTIN, Amaya20, MIYAMA, Syoken21
SERABYN, Eugene22, THALMANN, Christian23, WATANABE, Makoto24, YAMADA, Toru25
1: The University of Oklahoma, 2: The University of Arizona, 3: Ibaraki University, 4: Harvard-Smithsonian Center for Astrophysics, 5: Instituteof Astronomy and Astrophysics, 6: The Graduate University for Advanced Studies, 7: University of Toronto, 8: University of Hawaii, 9:
National Astronomical Observatory of Japan, 10: Max Planck Institute for Astronomy, 11: University of Wisconsin-Madison, 12: Goddard
Space Flight Center, 13: Tokyo Institute of Technology, 14: Princeton University, 15: Nishi-Harima Astronomical Observatory, 16: Universityof Nice, 17: College of Charleston, 18: Universitatssternwerte Munchen, 19: Kyoto University, 20: CAB-CSIC/INTA, 21: Hiroshima
University, 22: Jet Propulsion Laboratory, 23: University of Amsterdam, 24: Hokkaido University, 25: Tohoku University

SEEDS (Strategic Explorations of Exoplanets andDisks with Subaru survey) is the large survey project(2009-2014) utilizing near-infrared high-resolution
imaging in the Subaru Telescope. Here, we report new
results in 2013, especially in the survey of circumstellar
disks. The disk-survey in SEEDS aims to investigate
the relationship between planet formation and themorphology of the disk. We have published 15 papers
related to circumstellar disks by 2013, and reported SR
21 [1] and RY Tau [2] in 2013.
SR 21—This is a young stellar object (a massof 2.5 M ; an age of ~1 Myr) in Ophiuchus. Fig. 1(a)shows a clear inner cavity with a radius of 36 AU in
the central region of the disk around SR 21 has been
detected with sub-millimeter interferometry at 870 μm,
possibly suggesting gravitational interaction between
the disk and planet(s). These cavitated disks are referred
to as `transitional disk' and are unique samples forunderstanding planet formation. Fig. 1(b) presents
our near-infrared polarized intensity image at 1.6 μm.
Surprisingly, we cannot detect the cavity structure
clearly seen in the dust continuum image (fig. 1a). In
general, scattering light in the NIR wavelengths can tracesub- μm-size small dust grains, while dust continuum inthe sub-millimeter wavelengths can trace millimeter-sizelarge dust grains. Therefore, observing results in figs.
1 could indicate different spatial distibutions of small
and large dust grains. To understand spatial distibutionsof dust grains, we conducted modeling efforts using aMonte Carlo radiative transfer code. Consequently, wehypothesize polarized intensity at NIR is dominated by
an optically thin disk envelope or atmosphere component.
RY Tau—This object in Taurus is an active premainsequence star (a mass of 2 M; an age of 8 Myr). RY Tau
also has a cavitated disk with a radius of 15 AU. Fig. 2 isthe polarized intensity image at 1.6 μm of the disk around
RY Tau, showing a butterfly-like distribution. We haveconducted (a) modeling efforts using a radiative transfer

012

I Scientific Highlights(a) SR 21 Dust Continuum (b) Polarized Intensity(870 µm)(1.6 µm)

N

Cavity radiusE

1 arcsecond
125 AU

Figure 1: (a): The dust continuum image at 870 μm obtainedwith SMA. (b): The polarized intensity image obtained
at 1.6 μm. A software mask with a diameter of 0.″2 isused due to the bright central star. A white-dashed line
indicates a radius of a cavity seen in panel (a).

RY Tau Polarized Intensity Figure 2: The polarized intensity
image obtained at 1.6 μm.
(1.6 µm)
A software mask with adiameter of 0.″ 3 is used
due to the bright central
star, occulting the innercavity with a radius of 15
AU (~0.″1).
N
1 arcsecond
140 AUE

code to constrain the disk parameters by fitting SED;
and (b) monochromatic simulations of scattered light todetermine the dust and disk parameters by compareing thescattered light image. However, we cannot consistently
explain the observed polarized intensity, SED, and theviewing angle inferred by millimeter interferometry. We
sugget observed scattering light could be scattered in an
optically thin and geometrically thick layer above thedisk surface.
References[1] Follette, K., et al.: 2013, ApJ, 767, 10.
[2] Takami, M., et al.: 2013, ApJ, 772, 145.

Construction of Gauge-invariant Variables of Linear Metric Perturbations
on an Arbitrary Background Spacetime
NAKAMURA, Kouji(NAOJ)

Perturbation techiques are powerful in many areas ofphysics and the developments of perturbation theories
lead to physically fruitful results and interpretationsof natural phenomena. General relativity is one of thetheories in which the construction of exact solutions
is not so easy. It is also true that some exact solutions
well describe our universe, or gravitational field ofstars, but these exact solutions by themselves do notdescribe fluctuations around these exact solutions.
Therefore, general-relativistic linear perturbation theory
is a necessary technique to clarify the properties ofuctuations.
Besides linear perturbations, higher-order generalrelativistic perturbations also have very wide applications:cosmological perturbations; black hole perturbations; andperturbations of a spherical star. Thus, there are many
physical situations to which general-relativistic higherorder perturbation theory should be applied.
As is well known, general relativity is based on thegeneral covariance. Due to this general covariance, the“gauge degree of freedom”, which is the unphysicaldegree of freedom of perturbations, arises in generalrelativistic perturbations. To obtain physical results,
we have to fix this gauge degree of freedom or extract
some invariant quantities of perturbations. This situation
becomes more complicated in higher-order perturbations.
In some linear perturbation theories, there are so-calledgauge-invariant perturbation theories, in which one maytreat only variables that are independent of the gauge
degree of freedom. These gauge-invariant perturbation
theories are useful in many cases. Therefore, it isworthwhile to develop higher-order gauge-invariant
perturbation theory from a general point of view.
According to these motivations, we have been
discussed the general framework of higher-order generalrelativistic gauge-invariant perturbation theory andproposed a procedure to find gauge-invariant variables
for higher-order perturbations on an arbitrary backgroundspacetime whose metric is given by gab. This proposal isbased on the following single assumption:
Assumption: Suppose that we have the second-rank
tensor field hab whose gauge-transforamtion rule is given
by Y hab − X hab = £ ξ gab, where ξ a is the generator of thegauge-transformation. Then, there are a second-rank
tensor field Hab and a vector field X a such that the tensor
field hab is decomposed as hab = Hab +£ X gab, where thegauge-transformation rules for Hab and X a are given byaaa
Y Hab − X Hab = 0 and Y X − X X = ξ , respectively.
Confirming that the above assumption in the case ofcosmological perturbations is correct, we developed asecond-order gauge-invariant cosmological perturbation
theory. Through these developments, we find that ourgeneral framework of higher-order gauge-invariant
perturbation theory is well defined except for the above
asumption. Therefore, we proposed this assumption asa conjecture. If this conjecture is true, the higher-order
general-relativistic gauge-invariant perturbation theory
is completely formulated on an arbitrary backgroundspacetime and has very wide applications.
In Ref. [1], we proposed a scenario of a proof of
the above assumption based on the premise that thebackground spacetime admits Arnowitt-Deser-Misner
decomposition. We explicitly constructed the gaugeinvariant and gauge-variant parts of linear metricperturbations. Although some special modes are excludedin the proof in Ref. [1], we may say that the above
conjecture is almost correct for linear-order perturbations
on an arbitrary background spacetime.
Ref. [1] is the full version of our short letter [2].
This short letter is selected by the editors of Classicaland Quantum Gravity for inclusion in the “Highlightsof 2011-2012” collection on the basis of its novelty andscientfic impact. Furthermore, some ingredients which
was not discussed in Ref. [1] was written as an essay
for “the 2012 Essay Competition of the Gravity Reasrch
Foundation” as Ref. [3] and this essay received anhonorable mention.

References[1] Nakamura, K.: 2013, Prog. Theor. Exp. Phys., 2013, 043E02.
[2] Nakamura, K.: 2011, Class. Quantum Grav., 28, 122001.
[3] Nakamura, K.: 2012, Int. J. Mod. Phys. D, 21, 124004.

I Scientific Highlights013

On the Formation Timescale of Massive Cluster Ellipticals
Based on Deep Near-infrared Spectroscopy at z ~ 2		TANAKA, Masayuki(NAOJ)		

ZIRM, Andrew(Dark Cosmology Centre)		

TOFT, Sune

(Dark Cosmology Centre)		

DE BREUCK, Carlos(European Southern Observatory)		

KURK, Jaron(Max-Planck Institute for Extragalactic Physics)

The formation and evolution of massive galaxies is along-standing issue since the seminal work by [1]. Oneof the ways to address the issue is to observationallyconstrain the formation timescale of those galaxies.
We focus on one of the most prominent proto-cluster
PKS1138 at z = 2.16, where deep multi-wavelength data
are available.
We have obtained deep (~7 hours) near-infrared
spectra of some of the massive galaxies in the systemwith MOIRCS [2]. By combining the spectra and thebroadband photometry, we perform a detailed analysisof spectral distribution of galaxies to constrain redshifts
and physical properties of galaxies simultaneously. We
spectroscopically confirm, for the first time, that massivequiescent galaxies populate in high-density environment.
Fig. 1 shows the color-magnitude diagram of galaxies, inwhich the quiescent galaxies as shown by the red stars
occupy the reddest part of the red sequence. This likely
suggests that the red sequence in the process of forming.

Figure 1: Color-magnitude diagram of galaxies in the field of
PK1138. The filled stars are the member candidates
identified with the MOIRCS spectra, and the red andblue colors indicate quiescent and star forming nature ofgalaxies.

We then combine the spectra of these quiescentgalaxies as shown in Fig. 2. The spectrum is typical ofquiescent galaxies with a clear 4000 Å break. A hintof the CaII H+K absorption is observed. If real, this is014

I Scientific Highlights

MARCHESINI, Danilo(Tufts University)

KODAMA, Tadayuki, KOYAMA, Yusei(NAOJ)TANAKA, Ichi
(NAOJ)

the first detection of such a feature in high-z quiescentgalaxies in dense environments.

Figure 2: Stacked spectrum of the 4 quiescent galaxies. The
dashed spectrum is the noise spectrum and the smooth,solid spectrum is the best-fitting model spectrum shifted
downwards for clarity. The shaded area is strongly
affected by the atmospheric absorption.

Finally, we constrain the formation timescale of thesequiescent galaxies using (1) the location and dispersionof the red sequence, (2) full spectral analysis, and (3)two spectral features that are sensitive to different starformation timescales. The bottom-line of these analyses
is that the quiescent galaxies likely form at 3 <~ z <~ 4 witha timescale of z <
0.5
Gyr.
This
is
a
very
short
timescale~and it remains a puzzle how to form massive, compact
galaxies on such a short timescale.

References[1] Eggen, O. J., Lynden-Bell, D., Sandage, A. R.: 1962, ApJ, 136,
748.
[2] Tanaka, M., Toft, S., Marchesini, D., et al.: 2013, ApJ, 772, 113.

On the Sodium versus Iron Correlation in Late B-Type Stars
TAKEDA, Yoichi, KAWANOMOTO, Satoshi, OHISHI, Naoko(NAOJ)

producing abundance peculiarities in upper mainsequence stars. Generally, less attention seems to havebeen paid to Na in early-type chemically peculiar stars,
presumably because published observational data havebeen insufficient. Above all, diffusion calculations for
Na in the envelope of B-type stars with M >~ 2.5 Mseem
to have been rarely conducted so far. In this respect,
new contributions by theoreticians are desirably awaited
toward reasonably explaining the observational trend for
Na (along with O and Fe) confirmed in this investigation.
The more details of this study are described in [3].
crosses: FGK stars
open circles: A stars
filled circles:
late B stars (Teff < 11000 K)
0.5 filled
triangles:
late B stars (Teff > 11000 K)[Na/H]

It is naturally known that a close abundancecorrelation exists between Na and Fe in comparatively
old FGK stars (cf. [1]) as a result of Galactic chemical
evolution. However, the existence of similar relation
recently found for A-type stars ([2]) was quite
unexpected, since it is hard to understand this tendency
based on the present-day diffusion theory intending to
explain the diversified chemical peculiarity in late-B
through A type stars. In order to check whether this trend
in A-type stars persists into the regime of late B-typestars, we determined Na abundances for 30 selected
sharp-lined late B-type stars (10000 K < Teff < 14000 K)
by using the spectrum-fitting technique applied to the Na I
5890/5896 doublet lines, based on the high-dispersion
spectra obtained with the 188-cm reflector and HIDES
spectrograph at Okayama Astrophysical Observatory. The
results are depicted in Figure 1, from which the following
conclusions are drawn:— (1) In the regime of A-type stars (7000 K < Teff <10000 K), the mechanism causing chemical peculiarities(mainly Am anomalies in this case, characterized byoverabundance of Fe and underabundance of O) acts
nearly equally on both Na and Fe, so that a near-scaling
relation between [Na/H] and [Fe/H] ([Na/H] ~ 0.64 [Fe/H]) is realized despite that these two elements havesuffered appreciable abundance changes.
— (2) However, as T eff is increased (higher than
10000 K), this relation first becomes appreciably loosened
and ambiguous at the transition region (10000 K < Teff
< 11000 K), then the correlation eventually disappears
at 11000 K < T eff < 14000 K where [Na/H] stabilizes
almost at the primordial value, despite both O and Fe stillshow ve sin i-dependent anomalies. This suggests that thephysical process causing abundance peculiarities does
not work any more on Na at this higher-Teff regime oflate B-type stars, though it still operates on both Fe and O(typically exhibited by HgMn stars).
— (3) It is interesting to note that the “transition region”
stars at 10000 K < Teff < 11000 K are in the mass rangeof ~2.5‒3 M, which just corresponds to the region on
the HR diagram occupied by both HgMn stars and hot
Am stars nearly overlapped. We may state that these twogroups of non-magnetic chemically peculiar stars (Amstars and HgMn stars) could be roughly characterized by
the existence of Na‒Fe correlation (i.e., both elements
undergo abundance peculiarities in a similar manner) andthe absence of such connection (i.e., Fe suffers anomaly
while Na do not), respectively.
This consequence may serve as an important
observational constraint for understanding the mechanism

0

-0.5

-0.5

0
[Fe/H]

0.5

Figure 1: Abundance correlation between Na and Fe. Star
groups of different Teff are discriminated by symbols:
Crosses···FGK stars ([1]), open circles···sharp-lined
A-type stars ([2]), filled circles···late B-type stars with
Teff < 11000 K (this study), and filled triangles···lateB-type stars with Teff > 11000 K (this study).

References[1] Takeda, Y.: 2007, PASJ, 59, 335.
[2] Takeda, Y., et al.: 2012, PASJ, 64, 38.
[3] Takeda, Y., Kawanomoto, S., Ohishi, N.: 2014, PASJ, 66, 23.

I Scientific Highlights

015

Visible Spectroscopic Observations of a Near-Earth Object, 2012 DA14URAKAWA, Seitaro(Japan Spaceguard Association)
			

FUJII, Mitsugu

TAKAHASHI, Jun(University of Hyogo)

The observations of near-earth objects (NEO) aresuitable for the elucidation of taxonomy of sub-km-sizedasteroids because the brightness increases when a NEO
is close to the Earth. Most asteroids smaller than 100 m
are monolithic asteroids. The constructions are different
from the rubble-pile of sub-km-sized asteroids. To solve
the collisional processes and mineral compositions forsmall asteroids, it is important to investigate whether
the taxonomy has correlation between the construction
and the diameter by examining gradual but steadyobservational data accumulations. This study’s purpose isto obtain the taxonomy for 2012 DA14 at the time when
the object moves fast on the sky after its closest approachto the Earth. 2012 DA14 came close to the surface of the
Earth on February 15, 2013 at a distance of 27,700 km.
Its estimated diameter is around 45 m. The spectroscopic
observations for such a small asteroid require a largeaperture telescope, generally. However, the close distanceafter its closest approach to the Earth assists us in
conducting the spectroscopic observations using a smallaperture telescope if we have a skillful observational
technique corresponding to the fast sky motion.
We conducted the spectroscopic observation of 2012
DA14 at the Fujii Kurosaki Observatory (Longitude =133.6478° E, Latitude = 34.5100° N) with the Meade
0.4 m/f10 telescope on February 15, 2013. We used a
FBSPEC-III spectroscope of our own construction. The
FBSPEC-III is equipped with FLI ML6303E CCD with
3072 × 2048 pixels. The slit width and the provided
spectral resolution are 5″ and R ~ 500, respectively. Thisconfiguration permits the spectral range from 0.354
μm to 0.965 μm. Though we set an exposure time ofsix minutes, the fast sky motion of 2012 DA 14 madeit difficult to hold the image within the slit width forthe six-minute duration. Thus, we continued manual
reintroduction of 2012 DA 14 into the slit every eight
seconds for six minutes. By this procedure, we achieved
the effective exposure time of around nine seconds for
one frame. Since we obtained four frames, the total
effective exposure time is around 36 seconds.
The relative reflectance for 2012 DA14 is shown in
Figure 1. Though a typical error for relative reflectanceof 2012 DA 14 is around 0.02, the data with a lower
integration time have the errors of over 0.10 in awavelength region of shorter than 0.41 μm and longer
than 0.78 μm. The legend of “DA14 error” in Figure 1
indicates the error at the representative wavelength. The

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I Scientific Highlights

HANAYAMA, Hidekazu, TERAI, Tsuyoshi(Fujii Kurosaki Observatory)		

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

error at 0.85 μm is calculated by stacking the data from0.83 μm to 0.87 μm. The taxonomy is determined byfollowing the flow chart of Bus [1]. We conclude thattaxonomy of 2012 DA14 is an L-type because the relativereflectance at 0.75 μm and the overall slope satisfy therequirements for L-type [2]. The legend of “L-type”
in Figure 1 shows the range of relative reflectance for
L-type asteroids. The observational results are included
within the range of L-type. Our results are consistent withthe observational results by using 10.4 m Gran Telescopio
Canarias [3]. The consistency indicates that 2012 DA14
has not shown the apparent rotational color variation.

Figure 1: Relative reflectance for 2012 DA14.

References[1] Bus, S. J.: 1999, PhD thesis, Massachusetts Institute ofTechnology.
[2] Urakawa, S., et al.: 2013, PASJ, 65, L9.
[3] de León, J., et al.: 2013, A&A, 555, L2.

Starformation in Ram-pressure Stripped Gas Tail in the Virgo Cluster
YAGI, Masafumi, HATTORI, Takashi

GU, Liyi, NAKAZAWA, Kazuhiro, MAKISHIMA, Kazuo

		(NAOJ)					

		(Osaka University)

FUJITA, Yutaka(University of Tokyo)

AKAHORI, Takuya(University of Sydney)

We investigated starformation in the tail of
NGC4388, a galaxy in the Virgo cluster. The tail is oneof the most prominent ram-pressure stripping eventin nearby universe [1,2,3]. Its 30 kpc ionized tail was
first discovered by Suprime-Cam/Subaru imaging witha narrow-band filter of Hα at the redshift of the Virgocluster [1], and 110 kpc of HI tail was discovered by radio
observation [3] (Fig. 1). Recently, we investigated thetail with X-ray data [4]. In the study, we analysed publicarchived data of the region and found several Hα-excess
regions (HaRs), which would be associated with the tail[5].
We spectroscopically observed two HaRs at 66 kpc
from NGC4388 (Fig. 2) and another two at 35 kpc with
the FOCAS/Subaru. The redshifts of the four HaRs wereconsistent with the HI tail and [N II]/Hα vs [O III]/Hβ plot
indicated that they would be starforming regions.
With multiwavelength data from UV to MIR, we

YOSHIDA, Michitoshi(Hiroshima University)

estimated that their metallicity is comparable to solar
abundance, and the stellar age is several to ten Myr. The
total stellar mass of HaR-1 is estimated to be < 103 M,and those of other three are also as small as 104‒4.5 M.
The high metalicity and young age imply that they
formed after the gas was stripped from the NGC4388.
As HaR-1,2 are in front of the halo of M86, we cansee associated dark clouds. The extinction estimated fromBalmer decrement of the HaRs (E(B-V) ~ 0.6) is larger
than that estimated from imaging (E(B-V) ~ 0.05), whichsuggests that the starformation is ongoing in high density
regions. We also found that the positions of the stars andthe gas have an offset in HaR-2, which would be the same
phenomenon as “fireballs” found in the Coma cluster [6].
It means that ram-pressure is still effective at 66 kpc awayfrom the parent galaxy.

Figure 2: HaR-1,2 in multi-wavelengths.

References[1] Yoshida, M., et al.: 2002, ApJ, 567, 118.
[2] Yoshida, M., et al.: 2004, AJ, 127, 90.
[3] Oosterloo, T., van Gorkom, J.: 2005, A&A, 437, L19.
[4] Gu, L. et al.: 2013, ApJ, 777, L36.
[5] Yagi, M. et al.: 2013, ApJ, 778, 91.
[6] Yoshida, M., et al.: 2008, ApJ, 688, 918.
Figure 1: The tail of NGC4388. Background image is taken from
Sloan Digital Sky Survey. Blue contours show Hα tail [1]and magenta contours show HI tail [3]. The HaRs in thisstudy are shown as HaR-1,2,3, and 4.

I Scientific Highlights

017

Discovery of Disk Origin Narrow Metallic Absorption Lines
Observed during the 2009‒2011 Eclipse of ϵ Aurigae
SADAKANE, Kozo

(Osaka Kyoiku University)		
			

KAMBE, Eiji
(NAOJ)

HONDA, Satoshi(University of Hyogo)

The long period (27.1 yr) eclipsing binary є Aur (HD31964) consists of an F0 Ia supergiant star (primary) andan unseen secondary which is believed to be embedded
in a thick opaque disk. The central problem concerning
this system is that whether the primary star is a ordinary
massive supergiant (~15 M), as its spectrum implies, ora less massive star at the post-AGB stage of evolution.
We initiated spectroscopic observations of є Aur on 2008
October 1 using the HIDES spectrograph (Okayama
Astrophysical Observatory) and the GAOES spectrograph(Gunma Astronomical Observatory). The principal aimof the long-term monitoring observation is to clarify thenature of the primary by means of analyses of line profile
variations.
є Aur (HD 31964) has recently finished a two years

HASHIMOTO, Osamu(Gunma Astronomical Observatory)

SATO, Bun’ei(Tokyo Institute of Technology)

long eclipse starting in 2009 August and ending in 2011
August. From observations obtained during the eclipse,
we noticed temporal appearances of low excitation
absorption lines of neutral iron peak elements [1]. Several
0 eV lines of Fe I are detected near the end of the firsthalf of the eclipse. They had migrated toward shorter
wavelength and became much strong after the thirdcontact and then disappeared after the fourth contact(Figure 1). The radial velocity measured for these lines
follows that of the K I line at 7699 Å, implying that theselines originate in a rotating disk around the secondary
star which occults the primary star (Figure 2). A close
inspection of the data shows that the velocity of the Fe I
line is larger than that of the K I line. This means that
the Fe I line is formed at a inner part of the disk than theformation region of the K I line.
Similar behaviours are found for low excitation lines
of several iron peak elements such as Sc I, Ti I, V I, Cr I,
and Mn I. These lines are observed for only a short period
between the third contact (2011, March) and the fourthcontact (2011, August).
These observations demonstrates that the disk aroundthe secondary is axially non-symmetric and a clump ofrelatively cool gas is concentrated in a relatively small
localized region of the disk located at the egress side.

Figure 2: Variation of radial velocities of a Fe I line at 5110.435 Å(filled dots) and the K I resonance line at 7698.97 Å (opensquares). Symbols III and IV indicate epochs of the third
and the fourth contacts, respectively.
Figure 1: Time variation of an temporal absorption line. Verticaldashed line shows the rest wavelength. No trace of theline is visible outside of the eclipse phase.

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I Scientific Highlights

Reference[1] Sadakane, K., Kambe, E., Hashimoto, O., Honda, S., Sato, B.:
2013, PASJ, 65, L1.

The Core-Collapse Time of Star Clusters with Mass Functions
			

FUJII, Michiko

PORTEGIES ZWART, Simon(NAOJ)			

(Leiden Observatory)

Star clusters dynamically evolve due to two-bodyrelaxation. The relaxation process causes the shrink of thecluster core and the increase of the core density, which
are called as core collapse. In the dense core, binaries
form. They evolve to hard (tightly bound) binaries
via dynamical interactions with the surrounding stars.
During this process, the binaries give their energy to
the surrounding stars. Once the energy given from thebinaries exceed the potential energy of the cluster core,
the core bounces. The time until the core bounce is called
as core-collapse time [1].
Core-collapse time (tcc) is scaled by relaxation time
(trlx) and it is known that tcc = 15–20 trlx for systems withsingle-mass components. When the stars in a cluster
follow a mass function, the core-collapse time is much
shorter than that in the case of single components.
Using Monte-Carlo simulations, Gürkan et al. (2004)
showed that the core-collapse time with a mass function
follows tcc ∝ (mmax/m)−1.3, where mmax and m are themaximum and the mean mass of the cluster stars [2]. The
theoretical reason for this relation, however, has not been
understood.
We performed direct N-body simulations using
sixthorder Hermite scheme, with which we can treat
the interactions among binaries and their surroundingstars accurately and investigated the core collapse timeof star clusters with mass functions. We found that thecorecollapse time follows tcc ∝ (mmax/m)−1 (see Figure1). We also found that this relation is obtained from thefollowing equations. We assume that the core collapse
proceeds in the dynamical friction time-scale of the most
massive stars in the cluster. The dynamical friction time
is obtained as.

(1)

Since the relaxation time in the cluster core is written as,(2)

we obtain the core-collapse time scaled by the relaxation
time as.

found that this is because the core-collapse time must be
longer than the crossing time of the system. While thecrossing time is independent from N, the relaxation timeincreases with N. With a larger-N, therefore, the system
can reach a shorter core-collapse time (see Figure 1).
With the simulations, we also found that the core-collapse
time is estimated using the binding energy of the binary
formed in the cluster core [3].

Figure 1: The core-collapse time as a function of the maximum
mass of the cluster particles. Color symbols indicate
the results obtained from our simulations. Dashed line
shows the analytic result obtained from equation (3).
Dotted lines indicate the minimum core-collapse time(ten crossing time) for N = 2 k, 8 k, 32 k, and 128 k from
top to bottom.

References[1] Heggie, D., Hut, P.: 2003, The Gravitational Million-Body
Problem: A Multidisciplinary Approach to Star Cluster
Dynamics, by Douglas Heggie and Piet Hut, Cambridge
University Press.
[2] Gürkan, M. A., Freitag, M., Rasio, F. A.: 2004, ApJ, 604, 632.
[3] Fujii, M. S., Portegies Zwart, S.: 2014, MNRAS, 439, 1003.

(3)This relation is drawn as dashed line in Figure 1, andthe results obtained from our simulations agree with it.
In addition, the decrease of the core-collapse time stops
at some point, when we adopt a large mmax, and thisphenomenon depends on the number of particles (N). We

I Scientific Highlights

019

Atmospheric Study of the Hot Uranus GJ3470b
via Multi-band Simultaneous Photometry
FUKUI, Akihiko1, NARITA, Norio1, KUROSAKI, Kenji2, IKOMA, Masahiro2, YANAGISAWA, Kenshi1
KURODA, Daisuke1, SHIMIZU, Yasuhiro1,TAKAHASHI, Yasuhiro2/1, OHNUKI, Hiroshi3
ONITSUKA, Masahiro4, HIRANO, Teruyuki3, SUENAGA, Takuya4, KAWAUCHI, Kiyoe3/1
NAGAYAMA, Shogo1, OHTA, Kouji5, YOSHIDA, Michitoshi6, KAWAI, Nobuyuki3, IZUMIURA, Hideyuki1
1: NAOJ, 2: University of Tokyo, 3: Tokyo Institute of Technology, 4: Graduate University for Advanced Studies, 5: Kyoto University, 6:
Hiroshima University

GJ3470b is a low-mass (~14 M⊕) transiting planet
orbiting a nearby (~35 pc) M dwarf [1]. Although thisplanet is only 4 times the size of the Earth, because thehost star is also small, with about half the size of theSun, the system shows a relatively large transit depth.
In addition, the closeness to the system makes the hoststar bright, allowing us to investigate the nature of thesystem in detail. Especially, for such a system, we canprobe planetary atmospheric composition by measuringtransit depth (i.e., square of planet-to-star radius ratio) as
a function of wavelength. GJ3470b is the second lightest
planet among such atmospheric-researchable planets, andtherefore it is an important target to study the atmosphericnature of low-mass planets.
In this research, we conducted multi-band transit
observations of GJ3470b to study its atmosphere byusing the 188-cm and 50-cm telescopes both at Okayama
Astrophysical Observatory. We used the near-infrared
imaging and spectroscopic instrument ISLE with
J-band (~1.3 μm) filter which is mounted on the 188-cm
telescope, and an optical three-band simultaneous imager
mounted on the 50-cm telescope which enables to obtaing′ (~500 nm), Rc (~650 nm), and Ic (~800 nm) band images
simultaneously. At J band, thanks to the high performanceof the 188-cm telescope/ISLE and also thanks to the factthat the host star is especially bright in infrared becauseof its low temperature, we achieved a high-photometricprecision of ~1 mmag level (Figure 1).
Comparing the observed apparent planetary radii
across different passbands including the one at 4.5-μm
band obtained by Spitzer space telescope [2], we find thatthe planetary radius in J band is smaller than those inother wavelengths (Figure 2). This result can naturally be
explained by a hydrogen-dominated and hazy atmosphericmodel. On the other hand, if the planet was covered bythick clouds, light of any wavelengths would be equallyscattered by the clouds, and so the observed radii would
not depend on wavelength. Therefore, our results indicatethat this planet is probably not covered by thick clouds[3]. If true, future detailed observations of this planet willdetect many molecular features in its atmosphere without
being prevented by clouds.

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Figure 1: Transit light curves of GJ3470b obtained by the twotelescopes at Okayama Astrophysical Observatory.
The top (red) plot indicates the data from the 188-cm
telescope/ISLE, while the bottom three (orange, yellow,
and green) indicate those from the 50-cm telescope.

Figure 2: Planetary radius (shown in planet-to-star radius ratio) of
GJ3470b as a function of wavelength. The circles are thedata obtained in this research, while the triangle is thedata in 4.5-μm band obtained by Spitzer [2]. The blue
dotted line indicates a hydrogen-dominated and hazyatmospheric model, while the black dashed line indicatesa thick-cloud atmospheric model.
References[1] Bonls, X., et al.: 2012, A&A, 546, A27.
[2] Demory, B.-O., et al.: 2013, ApJ, 768, 154.
[3] Fukui, A., et al.: 2013, ApJ, 770, 95.

Star Formation Rate and Metallicity in Damped Lyman α System
OKOSHI, Katsuya

MINOWA, Yousuke, Kashikawa, Nobunari(Tokyo University of Science)				

The conversion process of gas into stars in ahierarchically evolving galactic halo can be a key role ingalaxy formation and evolution processes, and constrain
structure formation scenarios. In this view, it is quite
important to detect emissions from galaxies hosting
Damped Lyα systems (DLAs) [NHI ≥ 2 × 1020 cm−2] (DLA
galaxies), followed by the star formation rate (SFR)
measurements of the large amount of HI gas reservoirs.
The survey for DLA galaxies reveals the origin of
DLAs; at low-redshift (z < 1) , DLA galaxies consistof mixed morphological types of galaxies. However, at
high-z, it is not easy to identify the DLA galaxies in theemission because they are often faint and/or compact.
This requires selection strategies for identifying DLA
galaxies. For DLAs, a relation between the velocity
spread of the absorption line and the metallicity has been
confirmed similarly to the mass-metallicity relation.
This implies that the SFRs (or the stellar masses) of thehost galaxies correlate with the metallicities. Recently,
assuming the high-metallicity systems have the highSFRs, the survey for galaxies hosting high-metallicity
systems has recently led to several new detections (e.g.,[1]).
In Figure 1, we show the SFRs of DLA galaxies
at z > 2 as a function of the metallicities based on theliterature (red dots) and our results (blue dots) for DLA
galaxies toward two QSOs (Q0216+08, J0803+1313), anda gamma-ray burst (GRB050730) with the Keck/OSIRIS,
the Gemini/NIFS and the Subaru/MOIRCS (e.g., [2]). For
DLA galaxies currently identified, the high metallicity
systems have been successfully identified as bright
DLA galaxies at z > 2. Indeed, we have not obtained any
information about the DLA galaxies fainter than thosewith the SFR of ~1 M yr−1 except for an our detection(~0.97 M yr−1) [3]. To reveal the origin of DLAs, theluck of low-SFR samples requires deep surveys forgalaxies hosting low-metallicity systems. A semi-analytic
DLA model also predicts a positive correlation between
SFRs and metallicities at z = 2 (contours) [4].
Recent observation shows that Lyman Break Galaxies(LBGs) at z = 1 – 3 have median SFR of ~15 M  yr −1
based on the median age ~125 Myr [5]. This indicatesthat current samples of the bright DLA galaxies likely
arise from the LBG population. The faint end of Lyman
α Emitters (LAE) (SFR < 1 M yr−1) could also give riseto DLAs at z > 2 because the number densities and theincident rates agree well with those of DLAs [6]. The
consistency between the LBG/LAE populations and
DLA galaxies indicates that there is indeed some overlap
between them. The emission lines from DLAs provide(NAOJ)

the SFRs, the metallicities, and the number densities,
which can be compared with those of LBGs/LAEs. This
will remarkably improve our understanding of the originof DLAs and the missing link between the absorptionselected population and the emission-selected ones.

Figure 1: Star formation rates as a function of metallicities in
DLA galaxies at redshift z > 2. The SFR estimations areshown in red (e.g., [1]) and blue dots (our results and [2]).
The contour maps presents the SFRs of DLA galaxies at
z = 2 predicted by a model for DLA galaxy [4].

References[1] Fynbo, J. P. U., et al.: 2013, MNRAS, 436, 361.
[2] Minowa, Y., et al.: 2012, AJ, 144, 74.
[3] Kashikawa, N., et al.: 2014, ApJ, 780, 116.
[4] Okoshi, K., Nagashima, M., Gouda, N., Minowa, Y.: 2010, ApJ,
710, 1295.
[5] Hathi, N. P., et al.: 2013, ApJ, 765, 88.
[6] Rauch., et al.: 2008, ApJ, 681, 856.

I Scientific Highlights

021

Nature of Hα Selected Galaxies at z > 2.
I. Main Sequence and Dusty Star-forming Galaxies
TADAKI, Ken-ichi, KODAMA, Tadayuki, TANAKA, Ichi

				
			

(NAOJ)					KOYAMA, Yusei(NAOJ)		

I Scientific Highlights

SHIMAKAWA Rhythm(Graduate University for Advanced Studies / NAOJ)

The star formation rate (SFR) is one of the mostimportant parameters to characterize galaxy properties
and its redshift evolution as stars are newly formed
through cooling and collapse of molecular clouds ingalaxies. The sketch of the cosmic evolution of starformation activities is known as the “Madau plot” [1].
The cosmic SFR density increases by a factor of 10
from z = 0 to z ~ 1 and comes to its peak at z ~ 2, whichindicates that a large fraction of stars in galaxies at z = 0
were formed at z > 1. Therefore, star-forming galaxies atthe peak epoch are the key population for understanding
the formation and early evolution of galaxies.
We have been conducting a large and systematic Hαnarrow-band (NB) imaging campaign with MOIRCS on
Subaru Telescope called “MAHALO ‒ Subaru” project(MApping HAlpha and Lines of Oxygen with Subaru[2]). As part of this project, we observed a general field,
CANDEL-SXDF, where high-resolution optical and nearinfrared images by ACS/WFC3 on HST are publicly
available (Figure 1). At z = 2.2 and z = 2.5, a Hα emission
line is redshifted to be λc = 2.09 μm and λc = 2.315 μm,
respectively. To capture them, two narrow-band filters,
namely NB209 and NB2315 are used. NB2315 survey isespecially unique because z ~ 2.5 is the highest redshift
where we can observe H*** lines with ground-based
telescopes. 63 star-forming galaxies at z = 2.2 and 46 atz = 2.5 are identified on the basis of flux excesses in a
NB and rest-frame optical colors [3]. Moreover, we havemade a follow-up spectroscopy for 13 Hα emitters (HAEs)
at z = 2.2 and successfully detected the Hα emission linefrom 12 ones.
We found that about 42 % of the red, massive HAEs
with M* > 1010.8 M contain AGNs and most of the blue,
less massive ones are likely to be star-forming galaxies.
The AGNs may play an important role at the late stageof galaxy evolution. For the star-forming HAEs, thegasphase metallicities are estimated on the basis of [N II]/Hα ratios. We found that the metallicities of our sample
are significantly lower than those of local star-forming
galaxies at given stellar mass. This result is consistent
with previous studies [4]. Moreover, we investigated
the so-called “main sequence” of star-forming galaxies
at z > 2 based on our unique sample of HAEs [5]. The
dustiness of star formation is correlated with the offset
from the main sequence, suggesting that there are twokinds/modes of dusty star-forming galaxies: star-bursting022

HAYASHI, Masao(University of Tokyo)

galaxies and metal-rich normal star-forming galaxies.

Figure 1: The field coverages of our NB surveys with MOIRCS
are shown by green squares. Red squares and blue
polygons indicate the areas covered by CANDELS
WFC3 and ACS surveys, respectively.

References[1] Madau, P., et al.: 1996, MNRAS, 283, 1388.
[2] Kodama, T., et al.: 2013, in “The intriguing life of massive
galaxies”, proceedings of IAUS 295, ed., D. Thomas, in press.
[3] Tadaki, K., et al.: 2013, ApJ, 778, 114.
[4] Erb, D. K., et al.: 2006, ApJ, 644, 813.
[5] Daddi, E., et al.: 2007, ApJ, 670, 156.

Nature of Hα Selected Galaxies at z > 2.
II. Clumpy Galaxies and Compact Star-forming Galaxies
TADAKI, Ken-ichi, KODAMA, Tadayuki, TANAKA, Ichi

				
			

(NAOJ)					KOYAMA, Yusei(NAOJ)		

HAYASHI, Masao(University of Tokyo)

SHIMAKAWA Rhythm(Graduate University for Advanced Studies / NAOJ)

In the present Universe, there are a lot of galaxies
with a variety of morphologies (elliptical, disk, andlenticular, etc.). How did they evolve into the present-day
galaxies with different morphologies? Or, do we just look
galaxies in a different evolutionary phase? Snapshots ofgalaxy morphologies in the distant Universe would give
us hints to answer these questions. For understanding theevolution of galaxy morphologies, it would be especially
important to observe galaxies at z ~ 2 when the cosmic
star formation rate density peaks. High-resolution images
are needed to spatially resolve distant galaxies. Hubble
Space Telescope (HST) is the best instrument for suchstudies.
We have already constructed a clean sample of Hαemitter at z = 2.2 and z = 2.5 with MOIRCS on Subaru
Telescope in CANDELS-SXDF field, where highresolution optical and near-infrared images are publicly
available [1]. We present their morphological properties
such as clumps and compactness [2].
We found that about 42 % of star-forming galaxies
at z > 2 have clumps and their morphologies are
significantly different from those of the present-day
galaxies. The clumps near the galaxy center tend to be
red compared to outer clumps. They are likely to be a
protobulge component. We can not clearly tell whether
the origin of the red color is caused by dust extinction orold stellar population at the moment. But the presence of
mid-infrared emission in the galaxies with a red clumpsuggests dusty star formation is occurring in the redclumps because blue clumps should be less dusty. Fora few sample, we found clear evidence of high Hα/UVratio in the red clump, supporting dusty star formation in
the galaxy center (Figure 1). These results suggest that abulge component of galaxies is formed at z ~ 2.
We also study the stellar mass-size relation for oursample. While the most of Hα emitters at z ~ 2 follow the
local relation, suggesting that many galaxies have alreadyobtained disks as extended as the local ones, there are
two massive, compact star-forming galaxies, which arecalled “blue nugget” [3]. Massive quiescent galaxies atsimilar redshift are also known to be extremely compact(they are called “red nugget” [4]). Blue nuggets are likely
to be a direct progenitor of red nuggets. To reveal theevolutionary path from blue nuggets to red nuggets, weneed to construct a statistical sample of blue nuggets.

Figure 1: HST images of four Hα emitters at z > 2.

References[1] Tadaki, K., et al.: 2013, ApJ, 778, 114.
[2] Tadaki, K., et al.: 2014, ApJ, 780, 77.
[3] Barro, G., et al.: 2013, ApJ, 765, 104.
[4] van Dokkum, P. G., et al.: 2008, ApJ, 677, L5.

I Scientific Highlights

023

High-Albedo C-Complex Asteroids In The Outer Main Belt:
The Near Infrared Spectra		

KASUGA, Toshihiro

			(NAOJ)			

USUI, Fumihiko

OOTSUBO, Takafumi(ISAS/JAXA)		

HASEGAWA, Sunao(ISAS/JAXA)			

Outer main-belt asteroids are generally icy andprimitive (C-complex, primary) with low geometricalbedos (0.05). However, high-albedo C-complex
asteroids were identified by recent observations withAKARI (Usui et al. 2011). The findings offer scientificmotivation for the presence of unusual minerals in theobjects or, possibly, surface water ice. We carried out
near-infrared spectroscopic observations (1.1–2.5 μm)
using the Subaru-IRCS for the asteroids with highalbedos ( ≥ 0.1).
Kasuga et al. (2013) found no absorption featurescharacteristic of water ice (near 1.5 and 2.0 μm) in theobjects. Instead, the intimate mixtures models found Mgrich amorphous silicates. As for asteroid (1576) Fabiola,orthopyroxene (crystalline silicate) is also attainable(Figs. 1 & 2). Consequently, the moderate Mg-rich
amorphous or crystalline silicates are likely to cause thehigh-albedos [1].
The orthopyroxene is unlikely to be formed in the
C-complex asteroids (Kunihiro et al. 2004). Here, as
examples, we take the presence of the high temperaturecomponents (e.g. crystalline silicates (Mg-rich),chondrules, CAIs) in comets (e.g. Wooden et al. 2008).
Nakamura et al. (2008) focuses on the oxygen isotope
compositions in comet 81 P/Wild-2 which correspondto those of chondrules in carbonaceous chondrites,suggesting a link between comets and outer mainbelt objects. Following the sense, high temperaturecomponents may be common in outer main-belt asteroids.
These inclusions in meteorite surfaces are known toincrease albedo (Kamei & Nakamura 2002).

(Tohoku University)

KURODA, Daisuke(NAOJ)

Figure 1: Panel (a) shows reflection spectrum of (1576) Fabiola(black) and the model (red) using 0% water ice, 61%
amorphous carbon, and 39% amorphous pyroxene (with
80% Mg) by weight and grain size 6 μm ( χ 2 ~1.49).

Figure 2: Panel (b) is fitted by the model (green) 0% water ice,
54% amorphous carbon, and 46% orthopyroxene byweight and grain size 3 μm ( χ 2 ~1.28).

Reference[1] Kasuga, T., et al.: 2013, AJ, 146, 1.

024

I Scientific Highlights

Development of High Damage Threshold and Ultra-low Loss Mirrors
TATSUMI, Daisuke, UEDA, Akitoshi

				(NAOJ)				

Recent rapid progresses on high-power laser require‟high damage threshold” and ‟ultra-low loss” mirrors
for gravitational-wave detectors and various laser
experiments. There is no such mirror of which satisfy
both of requirements with the highest levels.
To realize it, coating qualities are being investigatedin collaboration with SIGMAKOKI CO., LTD. As aresult, we succeed to make the high-reflectivity mirrorof 99.99 % [1]. It has scattering loss of less than 10 ppm
as already described in the previous annual report. In
addition, it has a damage threshold of 446 J/cm2 for 10 ns
pulse lasers. The loss of less than 10 ppm is the highest
level in the world and the damage threshold is the bestvalue in Japan as far as we known.
At research hub for advanced nano characterizationin the University of Tokyo, we took photos of film crosssection by Scanning Electron Microscope (SEM) andTransmission Electron Microscope (TEM) and madeX-ray Photoelectron Spectroscopy to evaluate not only
elemental compositions but also binding energies of eachfilm contents. Figure 1 shows a cross-section of the film.
Uniform and dense films are formed. Furthermore, thefilm boundaries are also clear and flat.

YONEDA, Hitoki(ILS, UEC)

quantum beam experiment. In the KEK facility, an
inverse Compton scattering process between accelerated
electron and low-energy laser light make a hard X-ray
beam. To increase the X-ray luminosity, high power (lowenergy) pulse laser and its accumulation optical cavity
are needed. Development of the cavity is a collaborative
work with KEK.
As a part of the activity, our developed mirror wastested by Institute for Laser Technology to evaluate
its damage threshold. The measuring conditions are as
follows. The beam has a wavelength of 1064 nm, a pulse
width of 10 ns and its cross-section of 380 μm × 415 μm,
respectively. Incident angle to the mirror is 0 degree. The‟1-on-1” evaluation method was chosen. Total 23 shots
were flushed in the power density range of 220–470 J/
cm2. We obtained a damage threshold of 446 J/cm2. It
corresponds to 44.6 GW/cm2 for continuous-wave laser.
This measured value is the best among the database of
the Institute for Laser Technology. Because the past bestis 300 J/cm2 [2], we succeed to enhance the threshold bya factor of 1.5.
Our developed mirrors were delivered to the KAGRA
project for its pre-mode cleaner optical cavity as shownin Fig. 2. It is a milestone of KAGRA mirror evaluationgroup in NAOJ.

Figure 1: A film cross-section taken by a Transmission Electron
Microscope (TEM).

At the University of electro-communications, anellipsometer system with high-power CO2 laser irradiation
was set up to catch the premonitory phenomenon and toreveal the mechanism of break-down process of the film.
The above knowledgewere fed-back to the coatingprocess. The temperature control improvements andresidual gas reductions were performed step by step. As
a consequence of such steady progresses, we obtain thehigher-quality mirror than that of the start.
This high quality mirrors are also valuable for KEK

Figure 1: KAGRA mirror for a pre-mode cleaner cavity.

Finally, we express the great appreciation for
SIGMAKOKI’s staffs.
References[1] TATSUMI, D., UEDA, A., YONEDA, H., a talk at Japan
Physical Society, 2014 Spring, 27pTL-1.
[2] Database on high-power tolerance of optics,
http://www.ilt.or.jp/engindex.html

I Scientific Highlights

025Detection of an Ultra-bright Submillimeter Galaxy
behind the Small Magellanic Cloud
TAKEKOSHI, Tatsuya1/2, TAMURA, Yoichi3, MINAMIDANI, Tetsuhiro1/2/3, KOHNO, Kotaro3, OOGI, Taira1
SORAI, Kazuo1, HABE, Asao1, EZAWA, Hajime2, OSHIMA, Tai2, SCOTT, Kimberly S.4
AUSTERMANN, Jason E.5, KOMUGI, Shinya2, TOSAKI, Tomoka6, MIZUNO, Norikazu2, MULLER, Erik2
KAWAMURA, Akiko2, ONISHI, Toshikazu7, FUKUI, Yasuo8, MATSUO, Hiroshi2, ARETXAGA, Itziar9
HUGHES, David H.9, KAWABE, Ryohei2, WILSON, Grant W.10, YUN, Min S.10
1: Hokkaido University, 2: NAOJ, 3: University of Tokyo, 4: National Radio Astronomy Observatory, 5: University of Colorado, Boulder,
6: Joetsu University of Education, 7: Osaka Prefecture University, 8: Nagoya University, 9: Instituto Nacional de Astrofísica, Óptica yElectrónica, 10: University of Massachusetts, Amherst

Recent advances in millimeter (mm) and submillimeter(submm) continuum observations provide a chance toinvestigate the extreme star formation activity in the early
Universe via observations of submm-bright galaxies(SMGs). To reveal detail properties of the SMGs, strong
gravitational lensing magnification by foregroundgalaxies are helpful. We searched candidates of strongly
lensed-SMGs using the wide-field and high sensitivity
submm continuum data toward the Small Magellanic
Cloud (SMC) at 1.1 mm wavelength.
Continuum observations at 1.1 mm toward the SMC
were performed with the AzTEC camera [1] mounted
on the ASTE telescope [2]. We investigated an 1.21 deg2
field which has very weak contamination by the thermal
dust emission. The noise level is ~7 mJy beam−1, which is
sufficient to detect ultra-bright part of SMGs (S1.1 mm > 35mJy) over 5σ significance.
As a result of the investigation, we found a candidateof a ultra-bright SMG denominated as MM J01071-7302(hereafter MMJ0107). The 1.1 mm flux density of
MMJ0107 is 43.3 ±8.4 mJy, making it one of the brightest
SMGs found in AzTEC/ASTE 1.1 mm continuum
observations. We estimate the photometric redshifts andfar-infrared luminosity by the spectral energy distribution(SED) fittings of four galaxy templates. Figure 1 shows
the result of fitting. The fluxes of MMJ0107 from opticalto millimeter wavelength data are well-fitted by the
SED templates. This result reveals that MMJ0107 has
the redshift of 1.4–3.9 and the far-infrared luminosityof (0.3−2.2) × 10 14 μL  (μ is the magnification factor
by gravitational lensing), which corresponds to the starformation of 5600–39,000 μM  yr −1 , suggesting that
MMJ0107 is a highly magnified lensed SMG.
This study demonstrates that a high-redshift galaxy
can be reasonably separated from foreground objects
through multi-band photometry. Further investigation inexisting mm/submm data taken toward nearby galaxies
and Galactic star-forming regions allows us to findmore ultra-bright SMGs, and helps to reveal the detailproperties of the SMGs.
Our result was published in the Astrophysical Journal
Letters [3].

026

I Scientific Highlights

Figure 1: Result of SED fitting. Top: the reduced-χ 2 value ofeach template SED fittings with redshift. Bottom: thephotometric data points of MMJ0107 and template SEDs
that minimize the -χ 2.

References[1] Wilson, G. W., Austermann, J. E., Perera, T. A., et al.: 2008,
MNRAS, 386, 807.
[2] Ezawa, H., Kohno, K., Kawabe, R., et al.: 2008, Proc. SPIE,
7012, 701208.
[3] Takekoshi, T., Tamura, Y., Minamidani, T., et al.: 2013, ApJL,
774, L30.

Discovery of Hot Water Vapor Gas Disk
around a Massive Protostar Candidate Orion KL Source I		

HIROTA, Tomoya, HONMA, Mareki(NAOJ/GUAS)			

We have discovered a definite evidence of a hotmolecular gas disk around a massive protostar candidate
located in the nearest massive star-forming region
Orion KL by using VERA, the Japanese very long
baseline interferometer network operated by NAOJ, and
ALMA, a newly constructed millimeter/submillimeterinterferometer [1].
In the ALMA observations, we focused on thesubmillimeter water lines and detected two lines at
321 GHz (excitation energy of 1800 K) and 336 GHz(excitation energy of 2900 K) for the first time in Orion
KL. As a result, the 321 GHz line is found to be tracing
the jets similar to the SiO masers detected with VERA.
In contrast, the 336 GHz line, which is a vibratioanlly
excited line, is though to be emitted from a closer
vicinity to the central protostar Source I. According to thevelocity structure, the 336 GHz line can be explained bya rotating gas disk observed in the edge-on view (Figure1). Furthermore, we have found that (1) the temperatureof the disk is higher than 3000 K, (2) the central starshould have at least 7 Solar masses, and (3) the diameterof the disk is estimated as about 80 astronomical units
with the ring-like structure. This is the first time to reveal
physical and dynamical properties of the rotating disk
around Source I in Orion KL. The present study settles
the long-standing problem about a nature of Source I,
providing a definite evidence of a rotating gas disk. Our
results suggest that the massive protostar like Source
I could be formed via disk accretion as predicted for
low and intermediate mass stars (Figure 2). Future
higher resolution observations with ALMA will be able
to uncover more detailed properties and evolutionary
scenario of Orion KL Source I.

KURONO, Yasutaka(NAOJ/JAO)		

KIM, Mi Kyoung(KASI)

Gas moving awayfrom observer

50 astronomical unit
Gas moving toward
observerFigure 1: Distributions of the hot water vapor gas detected with
ALMA (color) and the SiO masers observed with VERA
(grey) associated with Source I. The colors indicate theradial velocity of the 336 GHz water line. The blue inthe lower left side means that the gas is moving awayfrom the observer, while the orange in the upper rightside does that it is moving toward. The SiO masers arethough to be tracing the root of the jet emanating fromthe disk surface.

Figure 2: An artistic view of a massive protostar candidate Source
I in Orion KL (see Figure 1).

Reference[1] Hirota, T., Kim, M. K., Kurono, Y., Honma, M.: 2014, ApJL,
782, L28.

I Scientific Highlights

027

Calibrating [OII] Star-formation Rates at z > 1
from Dual Hα-[OII] Imaging from HiZELSHAYASHI, Masao, KODAMA, Tadayuki

				
			

(NAOJ)				

BEST, N., Philip(Royal Observatory of Edinburgh)

Star formation rate (SFR) is one of the most important
properties to characterize the growth of a galaxy. The
luminosities of emission lines such as Hα (λ6563) and[O II] (λ3727) are widely used as an indicator to derive
the star formation activity of galaxies not only in thelocal Universe but also at high redshifts. However, theHα line, one of the best indicator well calibrated withthe data in the local Universe, is redshifted into near-IR
wavelengths for galaxies at z > 0.4, while the [O II] line
can be observed with an optical instrument until z ~ 1.7,
and thus many studies/surveys of star-forming galaxies
at z > 0.4 rely on [O II] luminosity. Moreover, while [O II]
luminosity is in general correlated with the star formation
activity, it also depends on the metal abundance and theionization state of nebular gas. The indirect relation withthe star formation activity complicates the estimationof SFR from [O II] luminosity. Thus, it is important tomake sure whether the ratio of [O II] to Hα luminosities
known in local star-forming galaxies is valid for high-z
galaxies as well by directly studying earlier epochs in the
Universe.
In this study, we investigate the mean relation
between Hα and [O II] luminosities for [O II] emitters at
z = 1.47 in the two fields, UDS and COSMOS, using a
stacking analysis which enables us to examine the Hαluminosity of galaxies at z = 1.47 even if the individual
galaxies are too faint to detect both Hα and [O II] emission
lines simultaneously. The main results we have foundare summarized below (see also our paper [1] for moredetails).
We find that on average there is positive correlation
between Hα and [O II] luminosities for not only brightgalaxies but also faint ones with [O II] luminosity down
to 10 41 erg s −1, i.e, SFR=1.4 M  yr−1. The trend thatgalaxies with higher [O II] luminosities have higher Hαluminosities is consistent with that of the local galaxies,
suggesting that [O II] luminosities can be used as anindicator of SFR even at the high redshift of z = 1.47.
However, we have to use the [O II ] luminosities
with caution to estimate SFRs at z = 1.47 based on therelation calibrated with local galaxies. This is because[O II]emitters at z = 1.47 show the observed Hα/[O II] line
ratios corresponding to AHα ~ 0.35 and are less subject
to dust attenuation than the local galaxies selected basedon [O II] luminosity (Figure 1). Therefore, [O II]-selected
emitters at z = 1.47 are likely to be biased toward less028

I Scientific Highlights

SOBRAL, David(Leiden University)

SMAIL, Ian(Durham University)

dusty populations.
On the other hand, we note a caveat to ourinterpretation of the results in terms of dust extinction
only, because the Hα/[O II] line ratio is also dependent on
the metallicity. Hence the discrepancy of the line ratio
between [O II] emitters at z = 1.47 and local galaxies at z
~ 0.1 may be explained in terms of metallicity difference.
Therefore, the possibility that the low Hα/[O II] ratio is
not only due to the lower dust extinction, but also thelower metallicities of [O II] emitters at z = 1.47 than local
galaxies, cannot be completely ruled out. To distinguishthe two factors of dust extinction and metallicity
completely, we require deep spectroscopy to obtain the
nebular emissions from the individual or stacked spectra.

Figure 1: The ratios of Hα to [O II ] for [O II ] emitters at z =1.47 are shown by red symbols as a function of [O II]
luminosity. The grey-scale map shows the distribution of
SDSS galaxies at z = 0.07–0.1, and the blue filled circles
represent median Hα/[O II] ratios for the local galaxies
in each [O II] luminosity bin. The dotted lines show theratio of Hα to [O II] in the case of each dust attenuationin Hα (AHα).

Reference[1] Hayashi, M., et al.: 2013, MNRAS, 430, 1042.

Planetary Companions to Three Intermediate-Mass GK Giants
SATO, Bun'ei, OMIYA, Masashi, HARAKAWA, Hiroki			(Tokyo Institute of Technology)				

IZUMIURA, Hideyuki, KAMBE, Eiji, TAKEDA, Yoichi

				

ITOH, Yoichi(NAOJ)					ANDO, Hiroyasu, KOKUBO, Eiichiro(University of Hyogo)			

(NAOJ)		

We have been carrying out a precise radial-velocity
survey for planets around 300 intermediate-mass(1.5–5 M) GK giants using the 188 cm telescope andthe HIDES spectrograph at Okayama AstrophysicalObservatory since 2001. The survey is one of the longcontinued planet search programs in the world, and wehave discovered 20 planets and 6 brown dwarfs so far,including those found by international collaborations.
Here we report new planets around three GK giants:
HD 2952 (K0III, 2.5 M), HD 120084 (G7III, 2.4 M),and ω Serpentis (G8III, 2.2 M) [1]. Our group has now
discovered about 40 % of the planets and brown dwarfs
currently known around intermediate-mass giants.
HD 120084 hosts an eccentric planet with minimum
mass of 4.5 MJUP in an orbit with semimajor axis of 4.3
AU and an eccentricity of 0.66 (Figure 1). The planet
has one of the largest eccentricities among those everdiscovered around intermediate-mass giants. Althoughseveral scenarios proposed for the origins of sucheccentric planets, including planet-planet scattering andsecular perturbations by an outer body, expect existenceof a distant companion, we can exclude the existence of abrown-dwarf companion within ~36 AU and a stellar one
within ~90 AU around HD 120084 considering the lackof long-term radial-velocity trend in the star.
HD 2952 and ω Serpentis host a relatively low-massplanet with minimum masses of 1.6 MJUP and 1.7 MJUP innearly circular orbits, respectively. The planets belong toa group of least-massive planets ever discovered aroundintermediate-mass giants. It is normally difficult to detect
planets less massive than 2 M JUP around such giants
because of the relatively larger stellar jitter (~10–20 m s−1)
compared to solar-type stars. However, our discoveries
demonstrate that it is still possible to detect such lessmassive planets, even around GK giants by high-cadence
observations (Figure 2).
We also found out that the radial-velocity variationsof stellar oscillations for G giants can be averaged out
down to a level of a few m s−1, at least on a timescale ofa week by high-cadence observations. This enables us todetect a short-period super-Earth around giant stars.
We plan to continue the survey further, and expand
it in anticipation of a coming era of space-based highprecision astrometry (GAIA) and high-precision
photometry (TESS, CHEOPS).

LIU, Yujuan(NAOC)YOSHIDA, Michitoshi(Hiroshima University)

IDA, Shigeru(Tokyo Institute of Technology)

Figure 1: Radial-velocity variations of HD 120084. HIDES-Slitdata are shown in filled red circles.

Figure 2: Radial-velocity variations of HD 2952. HIDES-Slit and
HIDES-Fiber data are shown in filled red circles andfilled blue triangles, respectively.

Reference[1] Sato, B., et al.: 2013, PASJ, 65, 85.

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029

Growth of Massive Galaxies in the Early Universe
Revealed by Subaruʼs FMOSKASHINO, Daichi(Nagoya University)

SILVERMAN, John

(Kavli IPMU/University of Tokyo)

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

FMOS-COSMOS survey team
We are catching a glimpse of the universe, over ninebillion years ago, when massive galaxies are creating newstars at remarkable rates, by using the Fiber Multi-Object
Spectrograph (FMOS) on the Subaru telescope [1].
FMOS can observe the emission line Hα redshifted
into near IR window from galaxies at z ~ 1–2. Hα is oneof the most well-calibrated indicators of star formationand has been widely used in studies of low-redshift
galaxies. Therefore the use of Hα enables us to comparewith other studies consistently over cosmic time. Overthe last few years, a tight correlation between stellar mass(M*) and star formation rate (SFR) has been reported bymany authors at different redshifts, namely called “starforming main sequence”. It has become one of mostintriguing subjects in galaxy evolution.
We observed 755 BzK-selected star forming galaxies
at 1.4 <~z<~ 1.7 in the COSMOS field using the H- and Jlong gratings (Fig. 1) through the “Intensive Program” (PI:J. Silverman) and the UH-time (PI: D. Sanders). In orderto estimate the intrinsic SFR, it is necessary to correct
Hα luminosities for dust extinction. One can estimate theextinction toward nebular emissions Eneb (B–V) from theBalmer decrement (Hα/Hβ). Since our data do not permit
an detection of Hβ for most individual galaxies, we coadded 89 spectra with both quality Hα detection and
the J-long coverage in three bins of reddening Estar (B–V) and measure the average ratio of Hα/Hβ. Comparing
the stellar and nebular extinction, we found averagerelation Eneb (B–V) ~ 1.2 Estar (B–V) for our sample, whichindicates that the two extinctions are more similar to eachother relative to the canonical relation. This possibly
implies a more uniform dust distribution as comparedwith the local galaxies.
Based on our result, we derived SFRs based on the
dust-corrected Hα luminosities for 271 galaxies withan Hα detection. Figure 2 shows a comparison of SFR
and M* illustrative of a main sequence that evolves with
redshift. With cosmic time, the sequence declines withlittle change of its slope. Our result at z ~ 1.6 also showsa tight correlation between these two quantities and lies in
between the sequences at z ~ 1 and ~ 2 with a consistentslope and normalization, which is ~20 times higher ascompared with the local galaxies.
This study establishes a main sequence based ona large sample in the high-redshift universe using thespectroscopic Hα emission lines. We refer the reader toour published paper [2] for more details.

030

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Figure 1: A part of a spectral image in the H-long band. The
horizontal axis refers to the wavelength direction whilethe vertical axis indicates individual spectra observed
through each fiber. Circles indicate the detection ofemission lines and the inset boxes show the intensity ofthe emission lines.

Figure 2: M* vs. SFR. The main sequences at different redshfts arealso shown by the dashed lines.

References[1] Subaru web release (2013/12/5).
[2] Kashino, D., et al.: 2013, ApJ, 777, L8.

Dense Optical and Near-Infrared Monitoring of CTA 102
during High State in 2012 with Oister;
Detection of Intra-Night “Orphan Polarized Flux Flare”
ITOH, Ryosuke1, FUKAZAWA, Yasushi1, TANAKA, T. Yasuyuki1, ABE, Yuhei2, AKITAYA, Hiroshi1
ARAI, Akira3, HAYASHI, Masahiko4, HORI, Takafumi5, ISOGAI, Mizuki6, IZUMIURA, Hideyuki4
KAWABATA, S. Koji1, KAWAI, Nobuyuki7, KURODA, Daisuke4, MIYANOSHITA, Ryo8,MORITANI, Yuki1
MOROKUMA, Tomoki9, NAGAYAMA, Takahiro10, NAKAMOTO, Jumpei2, NAKATA, Chikako5
OASA, Yumiko11, OHSHIMA, Tomohito5, OHSUGI, Takashi1, OKUMURA, Shin-ichiro12, SAITO, Yoshihiko7
SAITO, Yu13, SASADA, Mahito5, SEKIGUCHI, Kazuhiro4, TAKAGI, Yuhei3, TAKAHASHI, Jun3
TAKAHASHI, Yukihiro2, TAKAKI, Katsutoshi1, UEMURA, Makoto1, UENO, Issei1, URAKAWA, Seitaro12
WATANABE, Makoto2, YAMANAKA, Masayuki5, YONEKURA, Yoshinori13, YOSHIDA, Michitoshi1
1: Hiroshima University, 2: Hokkaido University, 3: University of Hyogo, 4: NAOJ, 5: Kyoto University, 6: Kyoto Sangyo University, 7:Tokyo Institute of Technology, 8: Kagoshima University, 9: The University of Tokyo, 10: Nagoya University, 11: Saitama University, 12: Japan
Spaceguard Association, 13: Ibaraki University

The relativistic jets are extremely powerful and fast
outflow of plasma which emerge from the vicinity to themassive black hole. The AGN jets are characterized byhigh kinetic powers and large-scale structure and radiatein all wavebands from the radio to the gamma-ray bands
via the synchrotron and the inverse Compton scattering
process. But the mechanism of collimation, production andacceleration are not understood.
CTA 102, classified as a flat spectrum radio quasar atz = 1.037, produced an exceptionally bright optical flarein 2012 September [1,2]. Following the Fermi Large Area
Telescope detection of enhanced γ-ray activity, we closely
monitored this source in the optical and near-infrared
bands for the 10 subsequent nights using 12 telescopes inJapan and South Africa [3].
On MJD 56197 (2012 September 27, ~4 days after
the peak of bright γ-ray flare), polarized flux showeda transient increase, while total flux and polarization
angle (PA) remained almost constant during the “orphan
polarized-flux flare.” We also detected an intra-night andprominent flare on MJD 56202. The total and polarized
fluxes showed quite similar temporal variations, but the
PA again remained constant during the flare. Interestingly,
the PAs during the two flares were significantly different
from the jet direction. The emergence of a new emission
component with a high polarization degree (PD) up to
40 % would be responsible for the observed two flares,
and such a high PD indicates the presence of a highlyordered magnetic field at the emission site. We argued thatthe well-ordered magnetic field and even the observed
directions of the PA, which is grossly perpendicular to thejet, are reasonably accounted for by transverse shock(s)propagating down the jet.

Figure 1: Multi-wavelength light curves of CTA 102 from
September 24 to October 3 in 2012. Top panel: NIR (Ksband) ux. Second panel: optical (RC-band) flux. Third
panel: polarized flux (PF) in the RC band. Fourth panel:polarization degree (PD) in the RC band. Bottom panel:polarization angle in the RC band.

References[1] Osterman Meyer, A., Miller, H. R., Marshall, K., et al.: 2009,
AJ, 138, 1902.
[2] Orienti, M., D'Ammando, F.: 2012, The Astronomer's Telegram,
4409, 1.
[3] Itoh, R., Fukazawa, Y., Tanaka, Y. T., et al.: 2013, ApJ, 768,
L24.

I Scientific Highlights

031

Minute-scale Rapid Variability of the Optical Polarizationin the Narrow-line Seyfert 1 Galaxy PMN J0948+0022
ITOH, Ryosuke1, TANAKA, T. Yasuyuki1, FUKAZAWA, Yasushi1, KAWABATA, S. Koji1
KAWAGUCHI, Kenji1, MORITANI, Yuki1, TAKAKI, Katsutoshi1, UENO, Issei1
UEMURA, Makoto1, AKITAYA, Hiroshi1, AKITAYA, Hiroshi1, YOSHIDA, Michitoshi1
OHSUGI, Takashi1, HANAYAMA, Hidekazu2, MIYAJI, Takeshi2, KAWAI, Nobuyuki3
1: Hiroshima University, 2: NAOJ, 3: Tokyo Institute of Technology

Fermi Gamma-ray Space Telescope has recently
detected MeV/GeV γ-ray emissions from five Radio-Loud
Narrow line Seyfert 1 galaxies (NLSy1s). It is widely
recognized that NLSy1 posses a relatively light central
black hole of ~106–107 M accreting at a very high rate
near the Eddington limit. Hence, NLSy1 is considered to
be a young AGN growing toward a super massive blackhole which is believed to have a mass of 108–109 M.
We report on optical photopolarimetric results of theradio-loud NLSy1 PMN J0948+0022 on 2012 December
to 2013 February triggered by flux enhancements in thenear infrared and γ-ray bands ([1,2]). We performed theoptical photometric observations of PMN J0948+0022
from 2012 December 20 to 2013 February 20, using the
HOWPol installed to the 1.5 m Kanata telescope and the
MITSuME installed to the 1.0 m Murikabushi telescope [3].
Figure 1 shows a long-term history of RC-band flux andspectral index. figure 2 shows an enlarged view of temporalvariation of the polarized flux (PF) and polarization angle(PA) on MJD 56281. The polarization degree (PD) reached
36 ± 3 % at the peak of the shortduration pulse, while thepolarization angle remained almost constant. The high PD
and minute-scale variability in PF provides clear evidenceof synchrotron radiation from a very compact emission
region with a highly ordered magnetic field. Such microvariability of polarization is also observed in several blazar
jets, but its complex relation between total flux and PD
are explained by a multi-zone model in several blazars.
The implied single emission region in PMN J0948+0022
might reflect a difference of jets between RL-NLSy1s andblazars.

Figure 1: Long-term histories of the optical flux and spectral
index taken by HOWPol and MITSuME. The upper
panel shows a light curve in the Rc band. The lower
panel shows a history of spectral index. The dashed lines
indicate the dates when high-density photopolarimetricobservations were performed.

Figure 2: Time profiles of the polarized flux and polarization angle
on MJD 56281. The solid line is the best-fit light curve.

References[1] Carrasco, L., Recillas, E., Miramon, J., et al.: 2012, The
Astronomer's Telegram, 4659, 1.
[2] D'Ammando, F., Orienti, M.: 2012, The Astronomer's Telegram,
4694, 1.
[3] Itoh, R., Tanaka. Y. T., Fukazawa, Y., et al.: 2013, ApJ, 775,
L26.

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Measurements of Coronal and Chromospheric Magnetic Fields
Using Polarization Observations by the Nobeyama Radioheliograph
IWAI, Kazumasa, SHIBASAKI, Kiyoto(NAOJ)The magnetic fields of the corona and thechromosphere are important to understand various
phenomena in the solar atmosphere. In magnetizedplasma, ordinary and extraordinary modes of the freefree emission have different optical depths. Hence, theradio circular polarization observation enables us toderive the longitudinal component of the magnetic field.
In this study, we have derived coronal and chromosphericmagnetic fields from circular polarization observations by
the Nobeyama Radioheliograph (NoRH) [1].
NoRH observes the full solar disk every 1 second at
17 GHz (intensity and circular polarization) and 34 GHz(intensity). We selected an active region located near
the center of the solar disk that has large longitudinalcomponent of the magnetic field. Then, a frequency
spectral index of the radio brightness temperature wasderived from the ratio of brightness temperatures at
34 GHz and 17 GHz. The brightness temperatures of thequiet Sun at 17 GHz and 34 GHz are assumed to be 10000
K and 9000 K, respectively [2]. The radio spectral index
of the quiet region is about 0.15 using this assumption.
The observed radio spectral index is between 0.2 and 0.6
around the active region.
The longitudinal component of the magnetic field isderivd as follows [3],(1)
where I is the brightness temperature, V is the brightness
temperature of the circularly polarized component, λ is
the wavelength in cm, and n is the power-law spectral
index of the brightness temperature. The derived
magnetic field is about 200 G at the center of the active
region, and 70 G at the edge of the active region. The
ratio between the observed radio magnetic field and thecorresponding photospheric magnetic field is about 0.4 to
0.6 at the center of the active region (Fig. 1).
The observed radio magnetic field contains bothof the coronal and chromospheric components [4]. We
assume that the solar atmosphere observed at microwave
range has two components; the optically thin corona
and the optically thick chromosphere. The radio circularpolarization images are compared with the ultraviolet
images observed by AIA and the photospheric magnetic
field observed by HMI, both onboard the SDO spacecraft.
Around the edge of the active region, the location of theobserved radio circular polarization corresponds to that of

the coronal magnetic field and its loop structures. On theother hand, the chromospheric component is dominant at
the center of the active region. Hence, it is suggested thatthe 17 GHz observation can derive both of the coronaland chromospheric magnetic fields. For the futurestudies, circular polarization observations at multiple
frequency bands are required to separate the coronal andchromospheric components more accurately.

Figure 1: Magnetic fields observed by HMI at 03:00 UT on April
13, 2012. Radio circular polarization at 17 GHz issuperimposed as contours: positive components in red,
0.5 %, 1.0 %; negative components in blue, 0.5 %, 1.0 %,1.5 %.

References[1] Iwai, K., Shibasaki, K.: 2013, PASJ, 65, S14.
[2] Selhorst, C. L., et al.: 2005, A&A, 433, 365.
[3] Bogod, V. M., Gelfreikh, G. B.: 1980, Sol. Phys., 67, 29.
[4] Grebinskij, A., et al.: 2000, A&AS, 144, 169.

I Scientific Highlights

033

600 Pixels MKID Superconductive Millimeter-wave Camera
SEKIMOTO, Y., NOGUCHI, T., KARATSU, K., MATSUO, H., DOMINJON, A.
OKADA, A. N., MITSUI, K., TSUZUKI, T.
(NAOJ)NITTA, T.

(Tsukuba University/NAOJ/JSPS)		

SEKINE, M., SEKIGUCHI, S., OKADA, T., SHU, S.
(University of Tokyo/NAOJ)			

NARUSE, M.

(Saitama University)

MKID (Microwave Kinetic Inductance Detector)
group at Advanced Technology Center is developing
superconductive camera in millimeter and submillimeter
wavelengthes for LiteBIRD which detects CMB B-mode
polarization and for Antarctica Dome Fuji telescope
which observes distant galaxies with a wide field of view,in collaboration with KEK, Riken, Tsukuba University,
Saitama University, and Okayama University. We
developed 220 GHz 600 pixels imaging array in 2013
fiscal year [1,2].

Figure 2: Si lens array and mixed epoxy anti-reflection layer (upperhalf). Slits reduce thermal stress of the Si and the AR [3].

Figure 1: MKID 220 GHz - 600 pixels camera [1]. The size isaround 6 cm.

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 byincoming photons. The resonant frequencies distributed
among 2–12 GHz are measured through a pair of coaxial
cables with frequency comb generated by a DAC. The
MKID is composed of a simple structure named CPW(co-planar waveguide), so a higher yield is expected.
To detect submillimeter-waves efficiently, thecamera combined a lens array with superconducting
planar antenna. Although silicon is an ideal material
for millimeter-wave lens in the aspects of low loss andlarge refractive index, it was not available for this lens,034

I Scientific Highlights

because it was technically difficult to fabricate such
Si lens array. ATC ME shop succeeded in fabricating
millimeter-wave Si lens array by a milling process witha high-speed spindle and small diameter end-mills.
We demonstrated symmetrical and low side-lobe beam
pattern of this camera with the Si lens array . Two kindsof cryogenic epoxies were mixed to match the refractive
index for Si and Alumina (Fig. 2) [3]. The AR thickness
was controlled by machining with the same fabrication
process as the Si lens array.
We also developed another AR of alumina using subwavelength structure (SWS). It is difficult to fabricate the
SWS on small lens array, however, it is possible for thelarge lenses of the re-imaging optics. Among a few meritsof SWS, this structure plays an important role as a low
pass filter or an IR block filter.
T. Noguchi et al. studied excess noise of MKID
generated by sub-gap states of superconducting [4]. A
readout circuit with a complex FFT board has been also
developed for 100 pixels MKID. The readout noise was
evaluated to be as low as that of a single-channel readout
system using an IQ mixer [5]. We are investigating awide field optics for MKID camera.
References[1] Nitta, T., et al.: 2013, JLTP, published online.
[2] Nitta, T.: 2014, PhD thesis, University of Tsukuba.
[3] Nitta, T., et al.: 2014, JLTP, published online.
[4] Noguchi, T., et al.: 2013, IEEE AS, 23, 1501404.
[5] Karatsu, K., et al.: 2013, JLTP, published online.

The Mass-metallicity Relation at z~1.4 Revealed with Subaru/FMOS
YABE, Kiyoto(NAOJ)			

TAMURA, Naoyuki(University of Tokyo, Kavli IPMU)

MORITANI, Yuki

OHTA, Kouji, IWAMURO, Fumihide(Kyoto University)			

YUMA, Suraphong(Tohoku University)

KIMURA, Masahiko, TAKATO, Naruhisa(University of Tokyo, ICRR)			

SUMIYOSHI, Masanao, MAIHARA, Toshinori(Hiroshima University)			

AKIYAMA, Masayuki(Kyoto University)			

(NAOJ)SILVERMAN, John
(University of Tokyo)

DALTON, Gavin, LEWIS, Ian, BONFIELD, David, LEE, Hanshin, CURTIS LAKE, Emma
MACAULAY, Edward, CLARKE, Fraser(Oxford University)

The gas-phase metallicity (hereafter metallicity) is oneof the important parameters in understanding the galaxy
formation and evolution. It is known that the metallicity
of galaxies correlates well with the stellar mass in thelocal Universe. This mass-metallicity relation still
remains unclear at higher redshift partly due to the small
sample size. We have carried out a NIR spectroscopic
survey of star-forming galaxies at z ~ 1.4 by using FMOS
(Fibre Multi Object Spectrograph) [1] on the Subaru
Telescope. We reported initial results [2] of this survey in
the NAOJ Annual Report 2012. Here, we report the massmetallicity relation at z ~ 1.4 constructed by using the
new results including the initial results [3].
We observed ~1200 target galaxies with K < 23.9
mag (AB), 1.2 ≤ zph ≤ 1.6, M* ≥ 109.5 M, F(Hα)expected≥ 5 × 10 −17 erg s−1 cm−2 in the SXDS (Subaru XMMNewton Deep Survey) field during the FMOS/GTO. The
basic data reduction was done with the FMOS standard
pipeline, and the spectral fitting including the effects of
OH-masks was carried out. For 343 objects, Hα emission
lines are detected with signal-to-noise (S/N) ratio larger
than 3. The metallicity is obtained from [N II] λ6584/Hαline ratio, after excluding possible candidates of active
galactic nuclei (AGNs). Due to the faintness of the [N II]
λ6584 lines, we apply the stacking analysis and construct
the mass-metallicity relation at z ~ 1.4.
We compare the mass-metallicity relation of oursample to the past results at different redshifts from z ~3 to z ~ 0 in literature. We found that the resultant massmetallicity relation at z ~ 1.4 is located between thoseat z ~ 0.8 and z ~ 2.2; the metallicity increases withdecreasing redshift from z ~ 3 to z ~ 0 at fixed stellar
mass. Thanks to the large size of the sample, we are able
to study the dependence of the mass-metallicity relation
on various galaxy physical properties. The average
metallicity from the stacked spectra is close to the local
fundamental metallicity relation (FMR) in the higher
metallicity part, but is > 0.1 dex higher in metallicity thanthe FMR in the lower metallicity part. We found thatgalaxies with larger E(B‒V), B‒R, and R‒H colours tend
to show higher metallicity by ~0.05 dex at fixed stellar
mass. We also found relatively clearer size dependence

that objects with smaller half light radius tend to show
higher metallicity by ~0.1 dex at fixed stellar mass,
especially in the low mass part. These dependences canbe partly explained by scenarios such as in-falling of
metal-poor gas, outflow of enriched gas, and different
star-formation efficiency.

Figure 1: The mass-metallicity relation at z ~ 1.4. Objects with[N II ] λ6584 S/N ratio of ≥ 3.0, 1.5 – 3.0 and < 1.5
are indicated by filled, open circles and upper limits,
respectively. Results from the stacking analysis areshown by filled stars with bootstrap error bars and linear
fit (thick line). The initial result is indicated by thin line.
The typical error for an individual object is presented on
the bottom-right corner.

References[1] Kimura, M., et al.: 2010, PASJ, 62, 1135.
[2] Yabe, K., et al.: 2012, PASJ, 64, 60.
[3] Yabe, K., et al.: 2014, MNRAS, 437, 3647.

I Scientific Highlights

035

GRB 130427A: A Nearby Ordinary Monster
MASELLI, Alessandro1, MELANDRI, Andrea1, NAVA, Lara1/2, MUNDELL, Carole G.3, KAWAI, Nobuyuki4/5
CAMPANA, Sergio1, COVINO, Stefano1, CUMMINGS, Jay R.6, CUSUMANO, Giancarlo1, EVANS, Philip A.7
GHIRLANDA, Giancarlo1, GHISELLINI, Gabriele1, GUIDORZI, Cristiano8, KOBAYASHI, Shiho3, KUIN, Paul M.9
LA PAROLA, Valentina1, MANGANO, Vanessa1/10, OATES, Samantha R.9, SAKAMOTO, Takanori11
SERINO, Motoko5, VIRGILI, Francisco3, ZHANG, Bin-Bin10, BARTHELMY, Scott D.12, BEARDMORE, Andrew P.7
BERNARDINI, Maria G.1, BERSIER, David3, BURROWS, David N.10, CALDERONE, Giorgio1/13
CAPALBI, Milvia1, CHIANG, James14, D'AVANZO, Paolo1, D'ELIA, Valerio1/15, DE PASQUALE, Massimiliano9
FUGAZZA, Dino1, GEHRELS, Neil12, GOMBOC, Andreja16/17, HARRISON, Richard M.3
HANAYAMA, Hidekazu18, JAPELJ, Jure16, KENNEA, Jamie A.10, KOPAC, Drejc16, KOUVELIOTOU, Chryssa12
KURODA, Daisuke18, LEVAN, Andrew J.19, MALESANI, Daniele20, MARSHALL, Francis E.12, NOUSEK, John A.10
O'BRIEN, Paul T.7, OSBORNE, Julian P.7, PAGANI, Claudio7, PAGE, Kim L.7, PAGE, Matthew9
PERRI, Matteo1/15, PRITCHARD, Tyler A.10, ROMANO, Patrizia1, SAITO, Yoshihiko4, SBARUFATTI, Boris1/10
SALVATERRA, Ruben1, STEELE, Iain3, TANVIR, Nial R.7, VIANELLO, Giacomo14, WIEGAND, Robert E.12
WIERSEMA, Klaas7, YATSU, Yoichi4, YOSHII, Taketoshi4, TAGLIAFERRI, Gianpiero1

1: Istituto Nazionale di Astrosica, 2: Astroparticle and Cosmology Laboratory, 3: Liverpool John Moores University, 4: Tokyo Institute ofTechnology, 5: RIKEN, 6: University of Maryland/NASA, 7: University of Leicester, 8: University of Ferrara, 9: University College London,
10: Pennsylvania State University, 11: Aoyama Gakuin University, 12: NASA, 13: Universita di Milano-Bicocca, 14: SLAC National Accelerator
Laboratory/Stanford University, 15: Agenzia Spaziale Italiana, 16: University of Ljubljana, 17: Centre of Excellence Space-si, 18: NAOJ, 19:
University of Warwick, 20: University of Copenhagen

The long-duration gamma-ray burst GRB 130427A,
detected on 27 April 2013, is the most powerful GRB(gamma-ray burst) at z < 0.9 with the luminosity of L ~ 3
× 1053 erg s−1 and the redshift of z = 0.34. We performed
multiwavelength observations with the Swift satellite
and ground-based facilities (Liverpool telescope, Faulkes
Telescope North, and MITSuME Telescopes) just after
the trigger event, and studied the X-ray, UV, and opticallight curves and spectral energy distributions, including
γ-ray and radio data [1].
GRB 130427A was also detected by the Fermi
Gamma-ray Burst Monitor (GBM) aboard the Fermi
Gamma-ray Space Telescope, and the high energy γ-ray
emission with the most energetic photon at 95 GeV wasdetected for 20 hours [2]. The Burst Alert Telescope(BAT) onboard the Swift satellite observed the highest
fluence for a GRB with a total fluence of 4.985 ± 0.002
× 10−4 erg cm−2 in the 15 – 150 keV band. In the X-ray
light curve, a break at 424 ± 8 s is detected between an
initially steep decay with index α0,x = 3.32 ± 0.17 anda flatter decay with index α1,x = 1.28 ± 0.01 (see Figure1). Then we found that a further break at 48 ± 22 ks isneeded to interpret a further steep decay with index α2,x =1.35 ± 0.02. In the optical and UV light curves, a break at
37 +4.7−4.0 ks is detected among a decay with index α1 = 0.96
± 0.01 and a further steep decay with index α2 = 1.36 +0.01−0.02 .
Assuming the break at 37 +4.7
−4.0 ks as a jet break, we canderive the opening angle of θj ~ 3° and the collimation
corrected energy of Eγ = 1051 erg.
It follows the spectral energy correlations between
the rest-frame peak energy Epeak(= 1028 ± 8 keV) andthe isotropic peak luminosity which are typically seenin the powerful GRBs at higher redshifts of z ~ 1–2 [3].
This suggests that these huge explosions are driven by
a common central engine from the early to the present

036

I Scientific Highlights

universe. Then, a broad-lined Type Ic supernova, SN
2013cq, associated with GRB 130427A was detected [4],which suggests the existence of supernovae associated withthe powerful and high-z GRBs.

Figure 1: Multiwavelength light curves of GRB 130427A [1]. γ-ray
data are from Fermi-LAT. X-ray data are from SwiftXRT and MAXI (Monitor of All-sky X-ray Image).
Optical data are from ground-based facilities, including
the Akeno Observatory (Tokyo Tech Akeno MITSuME
Telescope), Okayama Astrophysical Observatory(NAOJ), and Ishigakijima Astronomical Observatory(Mizusawa VLBI Observatory, NAOJ). Radio data arefrom VLA (Karl G. Jansky Very Large Array) [5]. Solidlines represent the light curves predicted by the vanEerten et al. synchrotron model [6].
References[1] Maselli, A., et al.: 2014, Science, 343, 48.
[2] Ackermann, M., et al.: 2014, Science, 343, 42.
[3] Nava, L., et al.: 2012, MNRAS, 421, 1256.
[4] Xu, D., et al.: 2013, ApJ, 776, 98.
[5] Laskar, T., et al.: 2013, ApJ, 776, 119.
[6] van Eerten, H., et al.: 2012, ApJ, 749, 44.

Numerical Treatment of Anisotropic Radiation Field
Coupling with the Relativistic Resistive Magnetofluids
TAKAHASHI, Hiroyuki, OHSUGA, Ken(NAOJ)

Radiation and/or magnetic fields, relativity, andresistivity play crucial roles in a number of highenergy astrophysical phenomena, such as blackhole accretion-disks, jets, disk winds, pulsar winds,
magnetar flares, core collapse supernovae, and gammaray bursts. For example, the magnetic field connecting
to the accretion disks around the black hole induces
the magnetohydrodynamic (MHD) turbulence by the
instability, i.e., the magnetorotational instability. The
magnetic field is tangled by the turbulent motion andamplified, leading to the angular momentum transport
outward. The gas loosing the angular momentum falls tothe black hole and this process liberates the gravitationalenergy. The twisted magnetic fields locally dissipate
due to the electric resistivity and the gas is heated up.
Some part of the gas internal energy is converted into theradiation energy through the emission process. So we canobserve the black hole binary system as very luminous
phenomena. Moreover, when a large amount of the gas
is supplied to this system, the radiation energy dominates
the magnetic and gas internal energies. Thus the radiation
field affects the dynamics of the accretion disks. Not only
the gas, but also the magnetic field, electric resistivity,
and the radiation field are all important ingredients tounderstand the high energy phenomena.
Takahashi [1] proposed a numerical scheme to take
into account the gas and radiation field in the frameworkof the special relativity. We advanced their work bytaking into account the magnetic field coincides with theelectric resistivity. Also in the previous work, an isotropic
radiation field in the comoving frame is assumed. This
assumption is valid only when the optical depth is muchlarger than unity, while the assumption is violated in
the optically thin regime. In this work, we relax thiscondition by taking into account the anisotropy of theradiation field [2].
We treat radiation field in the moment formalism,
which is obtained by integrating transfer equation inphoton's momentum space. Then we solve 0th and 1storder moment equations, which describe radiation energy(Er), and momentum (Fri ) conservation, respectively. In
the previous work, we determine the radiation stress Prijby assuming isotropic radiation field. In this paper, wegive an explicit form by assuming M-1 closure, which
admit anisotropy.
For the magnetic field and resistivity, we solved a fullset of Maxwell equations by assuming a simple Ohm's
law. The numerical schemes for solving these equations
are now developing, while they are now applied to some

Figure 1: Color shows Er at t = 47.3 μs, while white curves andarrows denote for magnetic field lines and radiation flux,
respectively.

high energy phenomena (e.g., [3]).
Figure 1 shows results obtained by applying ournumerical code to the relativistic Petschek type magnetic
reconnection. The initial condition is naively motivatedby the black hole accretion disks. The topology ofmagnetic fields changes at the origin and the gas isevacuated in ± X-direction. Due to the large optical depth
to the electron scattering, the radiation field is confinedin the outflow region with a small opening angle. We
compared results with and without radiation field andfound that the outflow speed is slower with radiation
than without it due to the radiation drag effect. Also thereconnection rate reduces due to this effect. Thus we canconclude that the radiation field would play an importantrole not only for a global structure of the accretion disks
but also in the small scale where the magnetic energy
dissipates and is converted to the thermal/kinetic energy.

References[1] Takahashi, H. R., et al.: 2013, ApJ, 764, 122.
[2] Takahashi, H. R., Ohsuga, K.: 2013, ApJ, 772, 127.
[3] Takahashi, H. R., et al.: 2011, ApJ, 739, L53.

I Scientific Highlights

037

Direct Imaging of a Compact Molecular Outflow
from a Very Low Luminosity Object: L1521F-IRS [1]		

TAKAHASHI, Satoko(NAOJ/JAO)			

OHASHI, Nagayoshi

Studying the earliest evolutionary phase of protostars
is an important topic for understanding the initialconditions of star formation. However, extremely young
proto-stars in a very early phase of the accretion process(≤ 104 yr) are less luminous when compared with welldeveloped protostars [2]. Unprecedented sensitivity
achieved with the Spitzer Space Telescope has revealeda large number of low-luminosity candidates, including
Very Low Luminosity Objects so called VeLLOs, which
has an internal luminosity of <0.1 L [3,4,5,6,7]. VeLLOs
are known as candidates of extremely young protostars,
proto-brown dwarfs, or young stellar objects, which are
in a low-state of accretion phase. The nature of VeLLOs
are not clear yet since the detailed high-angular resolution
observational studies are still limited in number.
We carried out the high-angular resolution interferometricobservations using the Submillimeter Array (SMA)
toward a well studied VeLLO, L1521F-IRS (d = 140 pc).
We have spatially resolved a compact and poorly
collimated molecular outflow in 12 CO(2–1) for the
first time (Figure 1). The outflow is aligned along theeast-west direction with a lobe size of ≈1000 AU. The
estimated outflow mass, maximum outflow velocity,and outflow force are (9.0–80) × 10−4 M , 7.2 km s−1,and (7.4–66) × 10 −7 M  km s −1 yr −1, respectively. The
estimated outflow parameters are similar to values
derived for other VeLLOs, and are located at the lower
end of values compared to previously studied outflows
associated with low- to high-mass star forming regions[8,9]. Low-velocity less collimated (1.5 km s −1/1200
AU) and higher-velocity compact (4.0 km s−1/920 AU)
outflow components are suggested from our observation.
The low-velocity component is not consistent with those
expected in the jet driven or wind driven outflow models,
but it could be related to the outflow driven from thefirst hydrostatic core (FHSC) since they are expected to
be of very low-velocity and less collimated as shown by
MHD simulations [10]. The high-velocity component
likely trace an undeveloped outflow from the protostar.
Detection of an infrared source and compact millimeter
continuum emission suggest the presence of the protostar,
while its low bolometric luminosity (0.034–0.07 L ),and small outflow, suggests that L1521F is in the earliest
protostellar stage (≤ 10 4 yr) and contains a substellar
mass object. The bolometric (or internal) luminosity of
L1521F-IRS suggests that the current mass accretion
rate is an order-of-magnitude lower than expected in thestandard mass accretion model (≈10−6 M yr−1; [11]),which may imply that L1521F-IRS is currently in a low

038

I Scientific Highlights(NAOJ)BOURKE, Tyler(Harvard-Smithsonian Center for Astrophysics)

activity phase.

Figure 1: An very compact molecular outflow imaged in CO(2–1)
using SMA (contours; This work [1]), superposed on theinfrared reflection nebula obtained in the 4.5 μm image
with Spitzer/IRAC [5].

References[1] Takahashi, T., et al.: 2013, ApJ, 774, 20.
[2] Stahler, S. W., et al.: 1980, ApJ, 242, 226.
[3] di Francesco, J., et al.: 2007, Protostars and Planets V,
University of Arizona Press, 17.
[4] Bourke, T. L., et al.: 2005, ApJ, 633, L129.
[5] Bourke, T. L., et al.: 2006, ApJ, 649, L37.
[6] Dunham, M. M., et al.: 2008, ApJS, 179, 249.
[7] Terebey, S., et al.: 2009, ApJ, 696, 1918.
[8] Dunham, M. M., et al.: 2011, ApJ, 742, 1.
[9] Wu, Y., et al.: 2004, A&A, 426, 503.
[10] Machida, M. N., et al.: 2008, ApJ, 676, 1088.
[11] Shu, F.: 1977, ApJ, 214, 488.

Growth of Rayleigh-Taylor and Richtmyer-Meshkov Instabilities
in Relativistic Jets
MATSUMOTO, Jin(NAOJ)

Relativistic jets are ubiquitous phenomena inastrophysical systems consisting of a compact object
surrounded by an accretion disk, such as active galactic
nuclei, microquasars, and potentially gamma-ray bursts.
The interaction of the jet with the surrounding medium
is a key process for the dynamics and stability of the jet.
Many studies have been done in order to investigate thepropagation dynamics of the relativistic jet assuming theaxisymmetric geometry. However, the non-axisymmetricevolution of the jet is still not understood well although
it might have a potential impact on the overall dynamics
and transverse structure of the jet.
In this research [1], the stability of the transverse
structure of the relativistic jet is investigated using
two-dimensional special relativistic hydrodynamic
simulations. An intriguing finding in our study isthat Rayleigh-Taylor and Richtmyer-Meshkov typeinstabilities can destroy cylindrical jet configuration as aresult of the naturally induced radial oscillating motion(Figure 1).
A radial inertia force naturally arises from a pressuremismatch between the jet and surrounding medium when
the jet propagates through the ambient medium. The
inertia force drives the radial oscillating motion of thejet, yielding the reconfinement region inside the jet [2].
When we consider the non-axisymmetric evolution of thejet, the radial oscillating motion of the jet can excite theRayleigh-Taylor instability at the jet interface.
The reconfinement region inside the jet is enclosedby the oblique shock. The convergence of the oblique
shock results in the excitation of an outward-propagating
shock wave at the center of the jet. When the shock wave
encounters the corrugated interface of the jet due to theRayleigh-Taylor instability, the Richtmyer-Meshkov
instability is secondarily excited between RayleighTaylor instability fingers.
During the radial oscillating motion of the jet, these
instabilities are amplified and repeatedly excited at thejet interface, and finally deform the transverse structureof the jet. This result suggests that the non-axisymmetricnature is essential for the stability of the relativistic jet tothe oscillation-induced instabilities.

Figure 1: Time evolution of the effective inertia γ2ρh in the jetexternal medium system. γ, ρ, and h are the Lorentz
factor, density, and specific enthalpy, respectively. At
the early evolutionary phase (top panels), the RayleighTaylor instability grows at the interface between the
jet and the surrounding medium. After an outwardpropagating shock wave excited at the center of the jetcollides with the contact discontinuity (jet interface), theRichtmyer-Meshkov instability is secondarily excited
between Rayleigh-Taylor instability fingers. Two of theRichtmyer-Meshkov instability fingers are marked byopen circles. Almost all fingerlike structures in panel (f)have their origin in the Richtmyer-Meshkov instability.

References[1] Matsumoto, J., Masada, Y.: 2013, ApJ, 772, L1.
[2] Matsumoto, J., Masada, Y., Shibata, K.: 2012, ApJ, 751, 140.

I Scientific Highlights

039

A Big-Bang Nucleosynthesis Limit on the Neutral Fermion Decays
into Neutrinos
KUSAKABE, Motohiko

BALANTEKIN, A. B.

(Korea Aerospace University/Soongsil University) (University of Wisconsin, Madison/NAOJ)			

KAJINO, Toshitaka(NAOJ/University of Tokyo)

The best direct limits on the neutrino magnetic
moment come from experiments with reactor
antineutrinos [1]. Astrophysical constraints are also
derived from studies on the cooling of red giant stars [2],and the helium synthesis in the Big Bang [3]. We consider
non-thermal photons produced in the decay of the heavy
sterile mass eigenstates in the early universe via theneutrino magnetic moment. We then derive constraints
imposed by the observed abundances of all the lightelements.
If neutrinos possess magnetic moments, a sterile state
would decay into another state by photon emission. The
radiative lifetime of such a sterile neutrino is given [4] as

PEHLIVAN, Y.

(NAOJ/Mimar Sinan Fine Arts University)

plane. Higher values of the magnetic moment correspondto shorter lifetimes of X [Eq. (1)]. Below the upper dotdashed line, the magnetic moment can be constrained
from the baryon-to-photon ratio considerations [9].
However, if the magnetic moment is too low, the decay
happens after the recombination epoch (lower dot-dashedline). This case is constrained from measurements ofγ-ray background and high energy neutrinos [5].

(1)
where, μeff is the effective magnetic moment that takeus from the heavy mass eigenstate i to the light mass
eigenstate j, and μB = e/2me is the Bohr magneton. Below,
we write the mass of the decaying state as mX.
If we ignore the mass of final mass eigenstate (m j
~ 10−2 eV), the energy of the produced photon is Eγ0 =2 + m 2 /2 , where p is the initial momentum of the√p¯ineutrino. Such photons can induce electromagnetic
cascade showers, and generate many less energetic
nonthermal photons. These nonthermal photons can thendisintegrate background light elements [5,6].
We naively assume that the relic abundance of X isthe thermal freeze-out abundance for weakly interacting
particles [7]. We adopt the method of [6] to calculate
the nonthermal nucleosynthesis. We calculate the massdependent effects of the radiative decay for the first time.
In this case, there are three parameters: 1) (n0X / n0γ ), thenumber ratio of the decaying sterile neutrino state X tothe background radiation before the decay of X, 2) τX,
the lifetime of the decaying eigenstate, or equivalently
the neutrino magnetic moment [Eq. (1)], and 3) Eγ0, theenergy of photon emitted at the radiative decay.
Steady state energy spectrum of the nonthermal
photons are dependent on m X. We calculated transfer
functions of nonthermal nuclei. A solution to the 7Li
abundance problem [8] is found in a parameter region
where the photodisintegration of 7Be is induced while
those of other light nuclei never occur since the energy ofnonthermal photons is below the energy thresholds.
Figure 1 shows the constraints in the (mX, |μeff|/μB)

040

I Scientific Highlights

Figure 1: Contours in the (m X, |μ eff| / μ B) plane for the adopted
constraints of the primordial abundances of D (red),
3He and 4He (black), and 7Li (blue). Regions with thenotation, over and low, indicate that they are excluded byoverproduction and underproduction, respectively. The
regions below solid lines for D, 3He, 4He, and dashedline for 7Li are excluded. The region bounded by two
dashed lines for D is also excluded. 7Li is overproducedin the region above solid 7Li lines. The region boundedby two dot-dashed line is excluded by the changeof baryon-to-photon [9]. The lower dot-dashed line
corresponds to the time of cosmological recombination.
This is reprinted from [10].

References[1] Beda, A. G., et al.: 2012, Adv. High Energy Phys., 2012,
350150.
[2] Raffelt, G. G., et al.: 1990, Phys. Rev. Lett., 64, 2856.
[3] Morgan, J. A.: 1981, Phys. Lett. B, 102, 247.
[4] Raffelt, G. G.: 1999, Phys. Rept., 320, 319.
[5] Ellis, J., et al.: 1992, Nucl. Phys. B, 373, 399.
[6] Kusakabe, M., et al.: 2006, Phys. Rev. D, 74, 023526.
[7] Ressell, M. T., Turner, M. S.: 1990, Comments Astrophys., 14,323.
[8] Aoki, W., et al.: 2009, ApJ, 698, 1803.
[9] Feng, J. L., et al.: 2003, Phys. Rev. D, 68, 063504.
[10] Kusakabe, M., et al.: 2013, Phys. Rev D, 87, 085045.

Be Charge Exchange between 7Be3+ Ion andExotic Long-lived Negatively Charged Massive Particle
in Big Bang Nucleosynthesis
7

KUSAKABE, Motohiko(Korea Aerospace University/Soongsil University)

CHEOUN, Myung-Ki(Soongsil University)

KIM, K. S.

(Korea Aerospace University)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

A serious problem in big bang nucleosynthesis (BBN)
is a discrepancy between primordial 7 Li abundance
predicted in standard BBN (SBBN) model and thoseinferred from observations of metal-poor stars [1,2]. In
SBBN, 7Li is produced mostly as 7Be, which transforms
into 7 Li by electron capture in a late epoch. A 7 Be
destruction can be caused by negatively charged massive
particles X − [3] with a large mass, mX  1 GeV, in BBN[4,5,6]. The X − particles become bound to positively
charged nuclides A, and form bound states A X . 7 Be
destruction proceeds via the recombination of 7Be with
X − followed by 7BeX + p → 8BX + γ through both atomic[4] and nuclear [5] excited states of 8BX. In previous
studies, only the radiative recombination of nuclides A
and X − [7] has been investigated. We, however, foundthat the nonradiative charge exchange reaction between
7Be3+ and X − contribute to the 7Be formation and theXsubsequent destruction.
The destruction of 7BeX occurs at the temperature
T 9 ≡ T/(10 9 K) ~ 0.4 [6]. The effective rate of 7 Be
recombination with X − through the 7Be3+ ion is givenby the product of the following three quantities: 1) the
number ratio of 7Be3+ to 7Be4+(=7Be), 2) the formation
rate of excited states 7Be*X via the reaction 7Be3+ + X − →7Be* + e−, and 3) the probability that produced 7Be* are
X
Xconverted to the ground state (GS), which is estimated by
the ratio of the transition rate to the GS 7BeX and the total
reaction rate of the 7Be*X.
The rate for 7Be to recombine with e− is much larger
than the Hubble expansion rate. The number ratio of
7 Be 3+ to 7 Be 4+ is then the equilibrium value via theefficient reaction 7Be4+ + e− 7Be3+ + γ.
We estimated the thermal reaction rate of the chargetransfer reaction 7Be3+ + X − → 7Be*X + e−. We assume
that the cross section roughly scales as the squared
Bohr radius of 7 Be 3+ . Excited states 7 Be *X produced
via the reaction experience bound-bound transitionsof the spontaneous and stimulated emissions and thephoto-absorption in the universe filled with the cosmic
background radiation (CBR). These are the GS formation
reactions.
The 7Be*X is destroyed via the following reactions: 1)
collisional ionization by e±, 7Be*X + e± → 7Be + X − + e±, 2)
the charge exchange reaction, 7Be*X + e− → 7Be3+ + X −,and 3) photoionization of 7Be*X by CBR. Reaction 1) is

KINO, Yasushi(Tohoku University)

important while 2) and 3) are not.
Figure 1 shows a result of BBN calculation [8]. The
effective recombination rates are derived as a functionof temperature, and used in this calculation. Dependingon the cross sections, abundance evolutions and thefinal abundances of 7Be and 7Be X is affected by therecombination of 7Be with X − through the 7Be3+ ion.

Figure 1: Abundances of normal nuclei (a) and X nuclei (b) as
a function of T 9. Xp and Y p are mass fractions of 1Hand 4He, respectively, while other lines correspond to
number abundances relative to that of 1H. Thick lines
correspond to the standard reaction rate for 7Be(e −,γ)7Be3+(X −, e−)7BeX, while thin solid, thick dot-dashedand dashed lines correspond to the cross sections of
7
Be3+(X −, e−)7Be*X multiplied by a factor of 0, 10 and
100, respectively. The dotted lines correspond to SBBN.
This is reprinted from [8].
References[1] Spite, F., Spite, M.: 1982, A&A, 115, 357.
[2] Aoki, W., et al.: 2009, ApJ, 698, 1803.
[3] Cahn, R. N., Glashow, S. L.: 1981, Science, 213, 607.
[4] Bird, C., et al.: 2008, Phys. Rev. D, 78, 083010.
[5] Kusakabe, M., et al.: 2007, Phys. Rev. D, 76, 121302.
[6] Kusakabe, M., et al.: 2008, ApJ, 680, 846.
[7] Dimopoulos, S., et al.: 1990, Phys. Rev. D, 41, 2388.
[8] Kusakabe, M., et al.: 2013, Phys. Rev. D, 88, 063514.

I Scientific Highlights

041

R-process Nucleosynthesis in the Central Engine of Gamma-Ray Bursts,
i.e. Neutrino-Heated Collapsar Jets

Rapid neutron-capture (r-process) nucleosynthesis
is responsible for about a half of the abundance of
nuclei heavier than iron. Even after many years ofstudy, the neutron-rich and probably high-entropy
astrophysical site for the r-process nucleosynthesis has
not yet been definitively identified. The collapsar model
for long-duration gamma ray bursts (GRBs) has been
proposed as a possible astrophysical site for the r-process
nucleosynthesis. In this model, the central core of a rotating
massive star collapses to a black hole. Angular momentum
in the progenitor star leads to the formation of an accretion
desk around the central black hole. Magnetic field
amplification and/or heating from the pair annihilation ofthermally generated neutrinos emanating from the accretion
disk can heat material in a polar funnel region. This leads toa relativistic outflow of matter along the polar axis.
In this study [1], we follow the hydrodynamic
evolution of material in the heated jet and the associatednucleosynthesis for a long duration time. For thispurpose, our hydrodynamic study involves several steps:(1) Fist, there is the initial collapse of the progenitor
massive star leading to the formation of the accretion disk
and black hole; (2) As the accretion disk heats up and themagnetic fields are amplified, a funnel region above thepole of the black hole is heated by neutrinos and magnetic
fields, and this heating leads to the launch of a relativistic
jet which is eventually dominated by the propagationof a hydrodynamic shock through the outer layers of
the progenitor; (3) The jet expands far enough from theaccretion disk to no longer be affected significantly byneutrino heating, then the ejected material is cooled into
the r-process temperature range 5 > T9 > 0.3. Here T9 is
the temperature in unit of 109 K.
We employ an initial progenitor model from the
35OC model of [2]. The step 1 is simulated based upona relativistic axisymmetric magneto-hydrodynamic
code [3], to describe the collapse of rotating magnetic
massive star. After the stable accretion disk surroundinga central black hole develops, MHD driven outflow
and neutrino-driven jet can launch from the funnel
region above the pole of the black hole (step2; [4]).
The late-time evolution of the associated jet (step 3) isthen followed using axisymmetric special relativistichydrodynamics. We utilized representative test particles
to follow the temperature, entropy, electron fraction
and density for material flowing within the jet fromejection from the accretion disk until several thousand042

I Scientific Highlights

SATO, Susumu, HARIKAE, Seiji(NAOJ/University of Tokyo)

kilometer above the black hole. The evolution of nuclear
abundances from nucleons to heavy nuclei for ejected
test particle trajectories is solved in a large nuclear
reaction network. Finally we find that an r-process-likeabundance distribution forms in material ejected in thecollapsar jet. In our model the ejected mass of r-processmaterial is high (~0.1 M). Nevertheless, this is a rare
event compared to, for example, normal supernovae andthe possible influence of such events on the abundance
distribution in metal-poor halo stars needs to be explored.
10.0

0.5

8.0

0.4

6.0

0.3

4.0

0.2

7

MATHEWS, Grant J.

(University of Notre Dame)		

KAJINO, Toshitaka(NAOJ/University of Tokyo)

y [10 cm]		

NAKAMURA, Ko(NAOJ/Waseda University)

2.0

0.1
2.0

7

4.0

2.0

x [10 cm]

7

4.0

2.0

x [10 cm]

7

4.0

x [10 cm]

Figure 1: Profile of electron fraction Ye for the jet at various stages
up to the end of the MHD + neutrino-heating simulation.
The low Ye material in the torus and the developing
central jet is clearly seen.

Relative number abundance

			

10

2

10

1

100
10-1
10

-2

10

-3

10

-4

10-5

60

80

100

120

140

160

180

200

220

Mass number

Figure 2: Final abundance pattern of the r-process compared withs.s. abundances (red dots). Solid, long-dashed, dottedand dot-dashed curves are the calculated abundances
for high-to-low entropy flows in the neutrino-heatedcollapsar jets.
References[1] Nakamura, K., et al.: 2013, Int. J. Modern Phys. E, 22, 30022.
[2] Woosley, S. E., Heger, A.: 2006, ApJ, 637, 914.
[3] Harikae, S., Takiwaki, T., Kotake, K.: 2009, ApJ, 704, 354.
[4] Harikae, S., Kotake, K., Takiwaki, T.: 2010, ApJ, 713, 304.

Supernova Neutrino Nucleosynthesis of Radioactive 92Nb
and the Timescale for Solar System Formation
NAKAMURA, Ko

CHIBA, Satoshi, IWAMOTO, Nobuyuki(Japan Atomic Eergy Agency)		

An unstable isotope 92Nb decays to the daughter
nucleus 92Zr by β decay with a half-life of 3.47 × 107
years. 92Nb does not exist in the present solar system.
However, [1] found evidence of its existence in earlysolar-system material in primitive meteorites. 92Nb has
the potential to be used as a nuclear chronometer tomeasure the time from the last nucleosynthesis event.
However, the astrophysical origin of 92Nb has remained
an unsolved problem. Figure 1 shows a partial nuclear
chart and typical nucleosynthesis reaction flows forisotopes with nuclear masses around A = 92. 92Nb can
only be synthesized by direct nuclear reactions such as
the (γ, n) reaction on 93Nb.
We have proposed that direct neutrino reactions incore collapse SNe (ν process) can naturally produce theobserved abundance of 92Nb [2]. One of the key inputs
for ν-process nucleosynthesis is a set of neutrino-induced
nuclear reaction cross sections. We calculate neutrinoinduced reaction rates using the quasiparticle random
phase approximation (QRPA) with neutron-proton pairing
as well as neutron-neutron, and proton-proton pairingcorrelations. We have calculated ν-process production
rates using the core-collapse SN model. We use a 15 solar
mass progenitor model with an explosion kinetic energyof 1051 erg. We take average energies of kT = 3.2, 4.0,
6.0 MeV for the electron neutrino, anti-electron neutrino,
and the other neutrinos (νμ and ντ), respectively. Figure 2
shows the calculated abundances.
We consider a scenario in which a significant
contribution to the observed 92Nb is produced by thesingle injection of material from a nearby SN before thesolar system formation or at early stages of solar systemformation (SSF). The material ejected from the last
SN will be diluted and then mixed with the collapsing
protosolar cloud. We conclude that the observed ratio canbe reproduced by mixing of 2 ×10−3 M of the SN ejecta
with the 1 M proto-solar material.

KAJINO, Toshitaka(NAOJ)		

(NAOJ/University of Tokyo)

CHEOUN, M. K.

MATHEWS, Grant J.

(Soongsil University)		

(University of Notre Dame)

Ru

Ru

96

98

Ru

99

EC decay after rp process or neutrino-p process
flow of γ process
Mo

Mo

92

94

Mo

95

96

Neutral current reaction
Nb

92

EC decay T1/2=34.7 Myr
Zr

90

89

Zr

91

93

Mo

Mo

97

flow of s process

Nb

Charged current
reaction
Zr

94

92

Y

Zr

β decay after r process

Figure 1: Partial nuclear chart around 92 Nb and the relevant
nucleosynthesis flows. Most isotopes are produced by
the s-process and/or beta-decay after the freeze out of
the r-process. Note that 92Nb can not be synthesized byeither process.
10 -7
10 -8

Mass fractions

HAYAKAWA, Takehito(Japan Atomic Eergy Agency)		

10 -9
10 -10
10 -11
10 -12
10 -1310 -14

2.0

2.5

3.0

3.5

Mass coordinate [Msun]

4.0

Figure 2: Calculated abundances as a function of interior mass fromthe supernova ν-process for a 15 solar mass progenitor
star with solar metallicity, and an explosion kinetic
energy of 10 51 erg. The solid-line (red) and dashedline (green) denote the abundances of 92Nb and 93Nb,
respectively. The dot-dashed (blue) line indicates the92
Zr abundance.
References[1] Hayakawa, T., et al.: 2013, ApJ, 779, L9.
[2] Harpper, C. L. Jr.: 1996, ApJ, 466, 437.

I Scientific Highlights

043

Asymmetric Neutrino Production in Magnetized Proto-Neutron Stars
in Fully Relativistic Mean-Field Theory
and Application to Pulsar Kick and Rotational Spin Down		

MARUYAMA, Tomoyuki(Nihon University)		

YASUTAKE, Nobutoshi

KAJINO, Toshitaka(NAOJ/University of Tokyo)		

CHEOUN, Myung-Ki, Ryu, Chung-Yeol(Chiba Institute of Technology)			

(Soongsil University)		

HIDAKA, Jun(NAOJ)

MATHEWS, Grant J.

(University of Notre Dame)

In our previous works [1,2], we calculated neutrino
scattering and absorption cross sections on hot and dense
magnetized neutron-star matter including hyperons under a strong magnetic field in a fully relativistic mean
field (RMF) theory [3]. The calculated results showedthat the magnetic contribution increases the neutrino
momentum emitted along the direction parallel to themagnetic field and decreases it along the opposite
direction. The enhancement and reduction are conjectured
to play a role of increasing the neutrinos emitted to the
Arctic area and decreasing them to the Antarctic area
when the magnetic field has a poloidal distribution. In thepresent work [4], as a next step, we consider the neutrino
production process though the direct URCA (DU) (e− + p→ n (Λ) + νe).
Here we assume that there is uniform magnetic field,
and that its strength is weaker than the strong interaction
order: √¯e B  μ B , where μ B is the baryon chemical
potential. We therefore treat the magnetic field in theperturbative way, and approximate the production crosssection as(1)
where σ0 is independent of B, and Δσ is proportional to B.
Fig. 1 shows Δσpr / σ 0pr as a function of the produced
neutrino angle θf, where the magnetic field is set to be B
= 1017 G, and the initial neutrino energy is taken to be thechemical potential.
We see that the magnetic-field gives rise to about 8% asymmetry in the production process at ρB = ρ0. As
the density increases, the magnetic contribution becomes
smaller, particularly in the system with Lambda.
The magnetic field increases emitted neutrinos in the
Arctic area and decreases those in the Antarctic area.
This magnetic contribution in the production process
turns out to be the same as that in the absorption process.
Therefore, the asymmetry by the magnetic field becomes
about twice by the addition of the production process, andenlarges the pulsar kick [2] and the spin deceleration [4].

044

I Scientific Highlights

Figure 1: Normalized magnetic part of the total production
probability per unit time cross section, Δσpr/σ 0pr, as afunction of final neutrino angle θf in the system without
hyperons (a) and with hyperons (b) for the entropy S/A= 1 under magnetic field of B = 1017 G. In each panel
dotted, solid, dash-dotted and dashed lines represent theresults at ρB = ρ0, 3ρ0 and 5ρ0, respectively.

References[1] Maruyama, T., et al.: 2011, Phys. Rev. D, 83, 081303(R).
[2] Maruyama, T., et al.: 2012, Phys. Rev. D, 86, 123003.
[3] Serot, B. D., Walecka, J. D.: 1997, Int. J. Mod. Phys. E, 6, 515.
[4] Maruyama, T., et al.: 2014, Phys. Rev. C, 89, 035801.

Astronomical Method to Determine the Neutrino Mass Hierarchy [1]			

SUZUKI, Toshio(Nihon University/NAOJ)

Neutrino-nucleus reaction processes play importantroles in the synthesis of rare elements such as 7Li, 11B,
138La and 180Ta in the explosive environments realized
in supernovae. We have constructed new shell-model
Hamiltonians by taking account of the proper tensor
components in the interactions so that they can explain
the new shell evolutions and new magic numbers in dripline nuclei. The new Hamiltonians, SFO [2] and GXPF1J[3] are found to be quite successful in describing thespin responses in nuclei such as Gamow-Teller transition
strengths in 12C, 14C, 56Fe and 56Ni.
As the neutrino-nucleus reactions are induced
dominantly by spin-dependent transitions, we can now
evaluate neutrino-nucleus reaction cross sections suchas on 12C and 56Fe accurately with the use of new shellmodel Hamiltonians [4,5]. Note that the experimental
neutrino-induced cross sections are available only forthese two nuclei. As the case for 12C was reported in the
Annual Report of NAOJ in 2012 [6], we show here thecase for 56Fe (ν, e−) 56Co induced by DAR neutrinos.
Calculated value obtained by using GXPF1J is σ = 259
×10 −42 cm 2 . Averaged value for several calculations
is σ th = (258 ± 57) × 10 −42 cm 2 [7], which is in good
agreement with the experimental value from KARMEN
Collaborations: σexp = (256 ±108 ±43) × 10−42 cm2 [8].
New neutrino-nucleus reaction cross sections
updated with the use of the new Hamiltonians areapplied to evaluate more precise theoretical estimatesof nucleosynthesis of 7Li, 11B and 55Mn including theneutrino processes in the supernova explosions [4,5].
The production yields of 7Li and 11B are found to beenhanced by 13~14 % for SFO-WBP compared to thosefor Woosley’s (HW92) [9], where WBP [10] is used forthe evaluation of neutrino-induced reactions on 4He.
Effects of ν-oscillations on the production yields of
7Li and 11B are investigated. Charged-current reactions
become also important in case of oscillations. A new
method to determine the neutrino mass hierarchy andthe mixing angle θ13 from the abundance ratio of 7Li/11B
is proposed. In the case of a normal hierarchy, the ratio
is shown to be enhanced by the oscillation effects forsin2 2θ13 ≥ 0.002 due to the existence of the high-density
resonance (see Fig. 1). The dependence of the ratio on
the interactions are rather modest as shown in Fig. 2.
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/11Bi on the oscillation parameters.
Note that the mass hierarchies can not be distinguishedonly with vacuum oscillations unless the CP phase is finite.

KAJINO, Toshitaka(NAOJ/University of Tokyo)

According to a recent work based on the deduction of
the ratio 7Li/11B from pre-solar grains of a meteorite [11],the inverse mass hierarchy is statistically more favored[12].

Figure 1: MSW effects in normal (left panel) and inverted (rightpanel) hierarchies. High-density resonance denotedas H-resonance occurs for νe (ν̄ e) in case of a normal(inverted) hierarchy, while low-density resonancedenoted as L-resonance occurs for νe in both hierarchies.

Figure 2: Comparison of the dependence of the abundance ratio
7Li/11B on the mixing angle θ
13 for both neutrino mass
hierarchies between SFO-WBP and HW92 cases. The
same set of neutrino temperatures, Tνe =3.2 MeV, Tν̄ e=5.0 MeV and Tνμ,τ = Tν̄μ,τ = 6 MeV, and total neutrinoenergy Eν = 3 × 1053 erg are taken for the both cases.
References[1] Suzuki, T., Kajino, T.: 2013, J. Phys. G, 40, 083101.
[2] Suzuki, T. et al.: 2003, Phys. Rev. C, 67, 044302.
[3] Honma, M., et al., 2005, J. Phys.: Conf. Ser., 20, 7.
[4] Suzuki, T. et al., 2006, Phys. Rev. C, 74, 034307.
[5] Suzuki, T. et al., 2009, Phys. Rev. C, 79, 061603.
[6] Suzuki, T. et al., 2012, Annual Report of NAOJ, 15, 56.
[7] Paar, N., et al., 2011, Phys. Rev. C, 84, 047305.
[8] Maschuw, R., et al., 1998, Prog. Part. Nucl. Phys., 40, 183.
[9] Woosley, S. E., et al., 1990, ApJ, 356, 272.
[10] Warburton, E. K., et al., 1992, Phys. Rev. C, 46, 923.
[11] Fujiya, W., et al., 2011, ApJ, 730, L7.
[12] Mathews, G. J., et al., 2012, Phys. Rev. D, 85, 105023.

I Scientific Highlights045

Absolute Proper Motion of IRAS 00259+5625 with VERA:
Indication of Superbubble Expansion Motion
		

SAKAI, Nobuyuki(Graduate University for Advanced Studies/NAOJ)

SATO, Mayumi(Max-Planck-Institut für Radioastronomie)

MOTOGI, Kazuhito(Yamaguchi University)

NAGAYAMA, Takumi, SHIBATA, Katsunori M., KANAGUCHI, Masahiro, HONMA, Mareki(NAOJ)

Since their first discovery by Heiles (1979) [1], shellor arc-like HI objects with sizes ranging from a few pc tomore than 1 kpc have been discovered in the Milky Way
Galaxy. The large H I objects (up to a few kiloparsecs
in scale) are called the superbubbles or supershells,
and they are believed to play a role in mass and energy
transportation from the disk to the halo. However, studies
about superbubbles were mainly conducted using 2D
positions on the sky and 1D line-of-sight velocities ofthe objects, meaning that there are uncertainties in terms
of precise physical parameters (e.g., size and expansion
velocity) of the objects. To understand 3D structure andkinematics of the superbubbles with VLBI astrometry,
we conducted VERA observations toward an H2O maser
emission of IRAS 00259+5625, an star-forming region
associated with the “NGC 281 superbubble” in the
Galaxy.
13 epoch VERA observations were conducted
between 2008 January and 2009 September to measure
trigonometric parallax and proper motions of the source.
The derived parallax, marginal, is 0.412 ± 0.123 mas,corresponding to a distance of 2.43 +1.03−0.56 kpc. Also, the(systematic) proper motions are (μαcos δ, μδ) = (−2.48 ±
0.32, −2.85 ± 0.65) mas yr−1 in the equatorial coordinates.
Combining the both results and the systemic velocity
obtained from a molecular emission provides an absolute
vertical motion (vb) of −17.9 ± 12.2 km s−1 with ~ 1.5σ
significance. The non-circular motion is shown in fig.
1 with previous VLBI results. Clearly, both NGC 281
and IRAS 00259+5625 show the vertical motions awayfrom the Galactic plane, indicating that the superbubble
expansion motions might be related to sequential
supernova explosions originated in the Galactic plane.
As for future expectations, more VERA observations
would give us an accurate understanding of thesuperbubble regions related to the Galaxy evolution in
the near future.

References[1] Heiles, C.: 1979, ApJ, 229, 533.
[2] Sakai, N., et al.: 2014, PASJ, 66, 3.

Figure 1: l vs. b map of NGC 281 superbubble is shown with white contours H I data and color 12CO (J=1–0) data. The positions of NGC 281(red), IRAS 00420+5530 (green), and IRAS 00259+5625 (yellow) are indicated. The map is velocity-integrated for the Perseusarm line-of-sight velocity range of VLSR = −60 to −25 km s−1. The observed non-circular motions of the three sources are plotted as
red (NGC 281), green (IRAS 00420+5530), and yellow arrows (IRAS 00259+5625). Note that we assumed a flat rotation model toderive the non-circular motions.

046

I Scientific Highlights

Direct Imaging of a Cold Jovian Planet Orbiting the Sun-like Star GJ 504
KUZUHARA, M.1, TAMURA, M.2/3, KUDO, T.4, JANSON, M.5/6, KANDORI, R.2, BRANDT, T. D.6/7
THALMANN, C.8, SPIEGEL, D.7, BILLER, B.9/10, CARSON, J.11, HORI, Y.2/12, SUZUKI, R.2, BURROWS, A.6
HENNING, T.10, TURNER, E. L.6, MCELWAIN, M. W.13, MORO-MARTÍN, A.14, SUENAGA, T.15
TAKAHASHI, Y. H.3, KWON, J.2/3, LUCAS, P.16, ABE, L.17, BRANDNER, W.10, EGNER, S.4, FELDT, M.10
FUJIWARA, H.4, GOTO, M.18, GRADY, C. A.13/19, GUYON, O.4, HASHIMOTO, J.20, HAYANO, Y.4/15, HAYASHI, M.2/15
HAYASHI, S. S.4/15, HODAPP, K. W.21, ISHII, M.2, IYE, M.2/15, KNAPP, G. R.6, MATSUO, T.22, MAYAMA, S.15
MIYAMA, S.23, MORINO, J.-I.2, NISHIKAWA, J.2/15, NISHIMURA, T.4, KOTANI, T.2, KUSAKABE, N.2
PYO, T.-S.4/15, SERABYN, E.24, SUTO, H.2, TAKAMI, M.25, TAKATO, N.4/15, TERADA, H.4, TOMONO, D.4
WATANABE, M.26, WISNIEWSKI, J. P.20, YAMADA, T.27, TAKAMI, H.2/15, USUDA, T.2/15
1: Tokyo Institute of Technology, 2: National Astronomical Observatory of Japan, 3: The University of Tokyo, 4: Subaru Telescope, 5: Queen's
University Belfast, 6: Princeton University, 7: Institute for Advanced Study, 8: ETH Zürich, University of Amsterdam, 9: University of
Edinburgh, 10: Max Planck Institute for Astronomy, 11: College of Charleston, 12: University of California, Santa Cruz, 13: Goddard Space
Flight Center, 14: CAB-CSIC/INTA, 15: The Graduate University for Advanced Studies, 16: University of Hertfordshire, 17: Université deNice-Sophia Antipolis, 18: Universitäts-Sternwarte München, 19: Eureka Scientific, 20: University of Oklahoma, 21: University of Hawaii,
22: Kyoto University, 23: Hiroshima University, 24: Jet Propulsion Laboratory, California Institute of Technology, 25: Academia Sinica, 26:
Hokkaido University, 27: Tohoku University

Among the techniques to observe extrasolar planets(exoplanets), direct imaging plays a crucial role in its
ability to probe for wide-orbit giant planets. Indeed, thistechnique is responsible for the majority of detections andcharacterizations of wide-orbit (r > ~10 AU) exoplanets.
The Strategic Exploration of Exoplanets and Disks
with Subaru (SEEDS) campaign has surveyed exoplanets
via the direct imaging technique since 2009. As part ofthis survey, a nearby G0-type star, GJ 504, was observed,
resulting in the discovery of a wide-orbit (r ~ 43.5 AU)
exoplanet (GJ 504b) orbiting the star [1] (see Fig. 1). The
GJ 504 system has an age of 160 +350
−60 Myr, inferred throughgyrochronology and chromospheric activity techniques(e.g., [2]). A comparison of GJ 504b’s age and measured
infrared luminosities with luminosity evolution models for
giant planets [3] yields an estimated mass of 4 +4.5
−1.0 Jupitermasses, placing GJ 504b among the lowest of exoplanets
ever directly imaged. Furthermore, since GJ 504b has
a relatively old age, the mass estimation is only weakly
influenced by uncertainties related to choices of initialconditions in the evolutionary models for giant planets [4].
Using the aforementioned luminosity-evolution models,an effective temperature of GJ 504b was estimated to be~510 K, making it significantly cooler than any previous
thermally imaged exoplanet. Compared with other directly
imaged exoplanets (e.g., HR 8799’s planets [5]), the J–Hcolor (~ −0.2) of GJ 504b is relatively blue, which may
suggest a less cloudy atmosphere.
According to core accretion theory, it is extremely
difficult to explain an in situ formation for a wide-orbit
giant planet like GJ 504b [6]. The true origin of GJ 504b
remains poorly constrained, as does its atmosphericproperties. However, its further characterization will help
scientists better understand the origins and properties of
GJ 504b, and thereby help uncover the more general origin
and evolution of wide-orbit exoplanets.

Figure 1: High-contrast images of the GJ 504 system. The J-(~1.2μm) and H-band (~1.6 μm) images were overlaid tocreate this false color-composite image, where blue andorange represent J and H band, respectively. In order tocompensate for the planet’s observed orbital motion, theJ-band image was rotated by 0.9°. The fluxes from thehost star were suppressed in the images, through dataprocessing. The planet GJ 504b is seen as a white spot at
a projected separation of ~43.5 AU from GJ 504 [1].

References[1] Kuzuhara, M., et al.: 2013, ApJ, 774, 11.
[2] Mamajek, E. E., Hillenbrand, L. A.: 2008, ApJ, 687, 1264.
[3] Baraffe, I., et al.: 2003, A&A, 402, 701.
[4] Spiegel, D. S., Burrows, A.: 2012, ApJ, 745, 174.
[5] Marois, C., et al.: 2008, Science, 322, 1348.
[6] Dodson-Robinson, S. E., et al.: 2009, ApJ, 707, 79.

I Scientific Highlights

047Reducing Systematic Error in Weak Lensing Cluster Surveys
		

UTSUMI, Yousuke

MIYAZAKI, Satoshi, HAMANA, Takashi(Hiroshima University)				

(NAOJ)GELLER, Margaret J., KURTZ, Michael J., FABRICANT, Daniel G.
(Smithsonian Astrophysical Observatory)			

DEll'ANTONIO, Ian P.
(Brown University)		

Weak lensing is a fundamental tool of modern
cosmology. A weak-lensing map provides a weighted“picture” of the projected surface mass density and thus aroute to identifying clusters of galaxies selected by mass.
Subtle issues limit the application of weak lensing maps
as sources of cluster catalogs. A serious astrophysicallimitation is the projection of large-scale structure along
the line-of-sight. An observational limitation is thepresence of systematic errors in the maps. In this study
we focus on a method of reducing these errors [1].
We use the B-mode signal to quantify this systematic
error and to test methods for reducing this error. We
show that two procedures are efficient in suppressing
systematic error in the B-mode: (1) refinement of themosaic CCD warping procedure to conform to absolute
celestial coordinates and (2) truncation of the smoothing
procedure on a scale of 10′. Application of theseprocedures reduces the systematic error to 20 % of its
original amplitude. We provide an analytic expression forthe distribution of the highest peaks in noise maps thatcan be used to estimate the fraction of false peaks in the
weak lensing κ-S/N maps as a function of the detection
threshold. Based on this analysis we select a threshold
S/N = 4.56 for identifying an uncontaminated set of weaklensing peaks in two test fields covering a total area of~3 deg2. Taken together these fields contain seven peaks
above the threshold. Among these, six are probablesystems of galaxies and one is a superposition. We
confirm the reliability of these peaks with dense redshift
surveys, x-ray and imaging observations. The systematic
error reduction procedures we apply are general and canbe applied to future large-area weak lensing surveys. Ourhigh peak analysis suggests that with a S/N threshold of
4.5, there should be only 2.7 spurious weak lensing peaks
even in an area of 1000 deg2 where we expect ~2000
peaks based on our Subaru fields.

Reference[1] Utsumi, Y., et al.: 2014, ApJ, 786, 93.

048

I Scientific Highlights

OGURI, Masamune(University of Tokyo)

Figure 1: One example of redshift distribution for Peak GTO
00. The filled histogram shows objects within a coneof 3′ radius centered on the weak lensing peak; theopen histogram shows objects within a 6′ cone. Bins inredshift are 0.002(1 + z) wide.

Figure 2: One example of close-up view for Peak GTO 00. The
image is 6′ × 6′. Contours show the weak lensing peak.
Small yellow circles identify galaxies in the redshift
peak centered at a mean z = 0.416.

Toward Realization of Submillimeter-wave Camera
HIBI, Y., MATSUO, H.
(NAOJ)WATANABE, D.
(Toho University)

In Advanced Technology Center of NAOJ, we aim
to develop submillimeter-wave imaging array with morethan 10,000 detector pixels. We have developed GaAsJFET cryogenic integrated circuits to readout large
number of submillimeter-wave SIS photon detectors.
Experimental demonstration of cryogenic readout
module as well as combination test of charge integrating
amplifiers with SIS photon detectors are reported.
The GaAs-JFET electronics can operate undercryogenic temperature with low power dissipation. In
2010 we have reported development of GaAs-JFET
cryogenic integrated circuits for charge integrating
amplifiers and multiplexers. In 2013 we have successfully
developed and demonstrated operation of 32-channel
cryogenic readout modules using the cryogenic circuits.
The size of the module is 40 mm × 30 mm × 2 mm with
input and output connectors. The module can multiplex
32-channel detector signals and output two voltage
signal. Room temperature electronics applied source andcontrol voltages to conduct evaluation of the 32-channel
cryogenic module [1,2]. Figure 1 shows the picture of themodule and an example of measured output signal.
The submillimeter-wave SIS photon detectors
are superconducting tunnel junction detectors whose
operation is based on photon assisted tunneling of quasiparticle current. SIS photon detectors made of niobium
junctions were cooled down to less than 1 K and DC
magnetic field was applied to suppress Josephson current.
We combined the SIS photon detectors and cryogenic
charge integrating amplifiers to readout detector current
signal. In this experiment there were no radiation input to
detectors but DC magnetic fields were applied to change
detector current. The detector currents were successfullymeasured by the change of the slope of output signal
as shown in figure 2, from which we estimated noise
equivalent power of 4 ×10−15 [W/Hz0.5] [1].
We have successfully developed multi-channel
read-out system for submillimeter-wave camera anddemostrated detector signal readout using charge
integrating amplifiers, and now ready to fabricate
submillimeter-wave imaging arrays for astronomical
observations.

SEKIGUCHI, S.

(University of Tokyo)

IKEDA, H.

(ISAS/JAXA)		

FUJIWARA, M.
(NICT)

Figure 1: a) The 32-channel cryogenic readout module. ‘Amp’
are 16-channel charge integrating circuits, ‘MUX’ are
32-channel multiplexers with sample-and-holds, ‘SR’are shift resistors and ‘VD’ are voltage distributors. b)
Output signals for 1 MΩ resistors in place of detectors
for bias voltages from +4 mV to −4 mV. Operation
temperature of the module was 4 K and their power
dissipation was 350 μW.

Figure 2: Output signal of charge integrating amplifiers fordifferent DC magnetic fields applied to detectors; 0, 55
and 59 Gauss for red, blue and green lines, respectively.

References[1] Hibi, Y., et al.: 2013, IEEE THz Sci. Tech., 3, 422.
[2] Watanabe, D.: 2014, Master thesis, Toho University.

I Scientific Highlights049

In-medium Effects on Neutrino Reactions inside the Neutron Star
Cheoun, M-.K.

(Soongsil University)

Tsushima, K.

I Scientific Highlights

Maruyama, T.

8(Nihon University)2

ρ=0.0ρ
ρ=0.5ρ00
ρ=1.0ρ
ρ=1.5ρ00
ρ=2.0ρ0ρ=2.5ρ07

1.5
σν [10-40 cm 2]

6

5

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(b)
ρ =0.0ρ0ρ =0.5ρ0ρ =1.0ρ0ρ =1.5ρ0ρ =2.0ρ0ρ =2.5ρ0

0.5

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0

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30 40 50
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Figure 1: Density dependence of total cross sections for νe + n→ e− + p (left) and νe + n → ν′e + n (right) reactions
in nuclear matter. Cross sections are decreased with
the increase of the density by ρ/ρo = 0 (black (solid))ρ/ρo = 0.5 (red (dashed)), 1.0 (blue (dotted)), 2.0 (yellow(short dotted)) and 2.5 (sky-blue (dot-dashed)) in bothreactions.
70.3

ρ=0.0ρ0ρ=0.5ρ0
ρ=1.0ρ0
Exp.

6

(b)

0.25

5

σν [10 -40 cm 2]

The nucleon form factors in free space are usually
thought to be modified when a nucleon is boundin a nucleus or immersed in a nuclear medium. We
investigated effects of the density-dependent axial andweak vector form factors on the electro-neutrino (νe) andantielectro-neutrino (ν̄e) reactions with incident energy Eν
≤ 80 MeV via neutral current (NC) and charged current(CC) for a nucleon in a nuclear medium or 12C. For thedensity-dependent form factors, we exploited the quarkmeson-coupling (QMC) model.
In CC reaction, about 5 % decrease of the νe reaction
cross section on the nucleon is shown to be occurred innormal density, ρ = ρo ~ 0.15 fm−3 (see Fig. 1 (left)), andalso about 5 % reduction of total νe cross section on 12C
is obtained by the modification of the weak form factors
for bound nucleons (Fig. 2 (left)). Density effects for bothcases are relatively small, but they are as large as theeffect by the Coulomb distortion of outgoing leptons inthe ν-reaction. However, density effects in the ν̄e reaction
reduced significantly about 30 % the cross sections forboth the nucleon and 12C cases [1].
For NC, about 12 % decrease of the total cross section
by the νe reaction on the nucleon is obtained at normal
density, ρ = ρo ~ 0.15 fm−3 (Fig. 1 (right)), as well as about
18 % reduction of the total νe cross section on 12C (Fig. 2(right)), by the modification of the weak form factors of
the bound nucleon.
However, similarly to the CC reaction, effects of thenucleon property change in the ν̄e reaction and reducesignificantly the cross sections about 30 % for the nucleon
in matter and 12C cases. In Refs. [1,2], we addressed thatsuch a large asymmetry in the ν̄e cross sections in bothreactions is originated from the different helicities of ν̄eand νe.
We have applied the QRPA formalism to 12 C(ν e ,−12e ) Ng.s.(1+) via CC and 12C(νe, ν′e)12C*(1+) via NC. The
reaction can be treated by the ΔJ = 1 transition from the0+ ground state of 12C to the 1+ ground state of 12N and
12B. Descriptions of the nuclear states are performedby the QRPA framework [3]. Recent neutrino facilities
present lots of fruitful data for the neutrino reaction in thequasi-elastic region. The study of the asymmetry between
the ν̄ and ν scattering by more data could be the valuable
alternative approach to understand the modification of thenucleon properties in a nuclear medium.

050

Saito, K.

(Tokyo University of Science)(Federal University of Rio Grande do Norte (UFRN))σν [10-40 cm 2]

Kajino, T.

(NAOJ/University of Tokyo)

Kim, K. S.

(Korea Aviation University)σν C [10 -41cm 2]

		

4

0.2

0.15

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ρ=0.0ρ0ρ=0.5ρ0
ρ=1.0ρ0

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0

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30

40

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50

60

70

80

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30 40 50
E [MeV]

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Figure 2: Density dependence in 12C(νe, e−)12Ng.s.(1+) (left) and12C(ν , ν′ )12C*(1+) (right) reactions. Uppermost (blacke e(solid)) curve (ρ = 0) in right panel is the same result as
the results by the 1+ transition as the Fig. 1 in Ref. [3],which neatly reproduced the energy-dependent crosssection data [4]. Cross sections are decreased similarly
to the nucleon case in Fig. 1.

References[1] Cheoun, M.-K., et al.: 2013, Phys. Lett. B, 723, 464.
[2] Cheoun, M.-K., et al.: 2013, Phys. Rev. C, 87, 065502.
[3] Cheoun, M.-K., et al.: 2010, Phys. Rev. C, 81, 028501.
[4] Athanassopoulos, C., et al.: 1997, Phys. Rev. C, 55, 2078.

Neutron Stars in a Perturbative f(R) Gravity Modelwith Strong Magnetic Fields [1]
CHEOUN, M.-K.

(Soongsil University)

RYU, C. Y.

(Hanyang University)		

DELIDUMAN, C.

(Mimar Sinan University)		

KAJINO, Toshitaka(NAOJ/University of Tokyo)

Neutron stars, as remnants of supernova explosions,are excellent probes of nuclear matter equation of state(EoS) in extreme environments. Neutron-star phenomena,such as the soft γ-ray repeaters and anomalous X-ray
pulsars are believed to provide evidence for magnetars. In
the interior of these magnetic neutron stars, the magnetic
field strength could be as high as 1018 G. Such strong
magnetic fields may affect properties of neutron stars via
the additional magnetic pressure and energy density andthe population of Landau levels. These additions in turnaffect the relative populations of various particles, andthe mass-radius relation.
Neutron stars are also one of the most naturallaboratories for gravity physics. Different gravity theories
would result in different modified Tolman–Oppenheimer–
Volkoff (TOV) equations and so one would expect
different predictions for mass-radius relation. Imprecisionin the terrestrial experiments on EoS is not an important
issue here, because these probe densities which are
an order of magnitude less than densities predicted inneutron star interior, whereas the curvature around aneutron star is almost 13 orders of magnitude larger thanthe largest curvature in the Solar System [2].
In this paper [1], we consider the combination ofstrong magnetic fields and modified gravity. To motivate
for this we note that in Kaluza-Klein gravity (the fivedimensional unification of gravity and electromagnetism)it may be natural to associate strong electromagnetic
fields with modified gravity. We investigate, therefore, theextent that strong interior magnetic fields of neutron stars
could be associated with modified gravity.
We adopt a perturbative approach to obtain modified
TOV equations in f(R) = R + αR2 gravity: we expand
metric functions and hydrodynamic functions P(r) andρ(r) perturbatively in α and then general relativistic
solution is taken as the zeroth order solution of the field
equations. This way 4th order differential equations
reduce to manageable 2nd order differential equations[3]. Then the effects of both the finite magnetic field andthe modified gravity are detailed for various values ofthe magnetic field and the perturbation parameter α alongwith a discussion of their physical implications.
Observation of a neutron star with a mass of m = 1.97
± 0.04 M [4] has placed a stringent constraint on many
neutron star EoS. There is an inconsistency between
this observation and the super-soft EoS [5] obtained by

GUNGOR, C., KELES, V.

(Istanbul Technical University)

MATHEWS, G. J.

(University of Notre Dame)interpreting heavy ion collision data FOPI/GSI [6]. We
find that the combination of a strong magnetic field and anegative perturbation due to modified gravity can easily
lead to maximum neutron star masses > 1.97 M evenfor a very soft nuclear EoS. We note that while magnetic
field stiffens the EoS, negative (positive) α values tend to
stiffen (soften) EoS (see Fig. 1). Hence, this may provide
an alternative means to satisfy the maximum neutron starmass constraint.

Figure 1: Mass-Radius relation corresponding to an EoS witha nph phase, i.e. including hyperons, with non-zeromagnetic field and various values of α.

References[1] Cheoun, M.-K., et al.: 2013, J. Cosmol. Astropart. Phys., 10, 021.
[2] Psaltis, D.: 2008, Living Rev. Relativ., 11, 9.
[3] Arapoglu, S., Deliduman, C., Eksi, K. Y.: 2011, J. Cosmol.
Astropart. Phys., 07, 020.
[4] Demorest, P. B., Pennucci, T., Ransom, S. M.: 2010, Nature,
467, 1081.
[5] Wen, D.-H., Li, B.-A., Chen, L.-W.: 2009, Phys. Rev. Lett., 103,
211102.
[6] Reisdorf, W., et al.: 2007, Nucl. Phys. A, 781, 459.

I Scientific Highlights

051

Origin of Ultra High-Energy Neutrinos
via Heavy-Meson Synchrotron Emission in Strong Magnetic Fields [1]
KAJINO, Toshitaka(NAOJ/University of Tokyo)
			

TOKUHISA, Akira

MATHEWS, Grant J.

(Nikon/University of Tokyo)

YOSHHIDA, Takashi(YITP, Kyoto University)		

We s t u d i e d t h e g e n e r a t i o n o f h e a v y - m e s o nsynchrotron emission due to the acceleration of ultrarelativistic protons (and possibly nuclei) in the presenceof strong magnetic fields (H >~ 10 15 G) in transient
astrophysical environments such as magnetar flares. We
then discovered that, in addition to the well known pion
synchrotron emission, heavy vector mesons like ρ, DS,
J/Ψ and ϒ could be generated with high intensity (~103
times the photon intensity) through strong couplings to
the ultra-relativistic nucleons in the strong magnetic field.
We propose in particular the synchrotron emission
and subsequent cooling and decay of the heavy ρ0 andϒ(1S) mesons by the burst of energetic neutrinos, via p→ p′ + ϒ(1S), ϒ(1S) → τ + + τ −, τ − → μ− + ν̄μ + ν τ and e−+ ν̄e + ν τ. We evaluate the spectra of escaping νe, νμ andν τ due to the decay of short lived τ-mesons.
We conclude the possible event rate in a terrestrial
PeV neutrino detector like ICECUBE [2]. We estimatethat neutrinos produced from the heavy vector-meson
synchrotron radiation from a strong magnetar SGR
burst will only be detectable with the current generationof detectors if the source is very nearby (< 30 pc).
Nevertheless, if ever detected, the existence of heavy
meson synchrotron emission might be identifiable by theunique signature of energetic tau neutrinos.

(University of Notre Dame/NAOJ)

FAMIANO, Michael A.

(Western Michigan University/NAOJ)

-10

-15

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14

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Figure 2: Upper (lower) graph is the calculated flux at the sourceof τ-neutrinos (μ-neutrinos) and their anti-particles as
the decay product of ϒ(1S)-mesons. The solid curveshows the spectrum for an injection energy of Eϒ(1S) =1020 eV with a magnetic field of H = 1.5 × 1011 G, andthe dashed curve is for Eϒ(1S) = 1018 eV with H = 1.5 ×
1013 G. In μ-neutrino spectrum the hard- and soft-energy
components arise from the decay of τ ±-leptons anddissipated μ ±-leptons, respectively.

Figure 1: Illustration of meson synchrotron emission frommagnetar flares that interact with ultra-relativistic
baryons. Heavy mesons like ϒ(1S) eventually decay toemit a burst of energetic neutrinos, via p → p′ + ϒ(1S),
ϒ(1S) → τ+ + τ−, τ− → μ− + ν̄μ + ντ and e− + ν̄e + ντ.

052

I Scientific Highlights

References[1] Kajino, T., et al.: 2014, ApJ, 782, 70.
[2] Aartsen, M. G., et al. (The IceCube Collaboration): 2013, Phys.
Rev. Lett., 111, 021103.

Long-term Global Solar Activity
Observed by the Nobeyama Radioheliograph
SHIBASAKI, Kiyoto(NAOJ)The Nobeyama Radioheliograph has been observing
the Sun since 1992 for more than 20 years. It can
synthesize full disk images of the Sun at 17 GHz. Dueto its long and steady operation and well calibrated
uniform data, long-term global solar activity of the Sun
can be studied. By using about 7,200 daily images, abutterfly diagram is synthesized and is studied [Figure 1].
The radio butterfly diagram has different features fromsunspot butterfly diagrams. Polar regions are bright at 17
GHz. The brightness of polar regions are well correlatedwith magnetic field strengths at polar regions. Both areanti-correlated with activities at low latitude, such asactive regions and solar flares. We can see both high andlow latitude activities in one radio butterfly diagram.
During the observation of 20 years, high and low latitude
brightness shows gradual decline. In the northernhemisphere, brightness at low and high latitudes arewell anti-correlated. On the other hand, the correlation
is rather weak in the southern hemisphere. We can findweakening of synchronization of activities between northand south hemispheres and also between high and low
latitude activities in the southern hemisphere.
Microwave enhancement associated with unipolarstrong magnetic field regions is an important message
to chromospheric heating mechanisms. As the emission
mechanism at 17 GHz from non-flaring regions is freefree, enhanced microwave brightness requires hotter
plasma around the upper chromosphere. In unipolar filed
regions, magnetic field has open structure and heatedatmosphere has to flow out along the field. Continuous
heating at or below the upper chromosphere proportional
to photospheric magnetic flux is necessary. To understandchromospheric heating in open field structures, detailed
studies of temperature structure above unipolar magnetic
field regions in coronal holes are needed.
Even though NoRH was designed and constructed forstudies of high energy phenomena on the Sun, it turned
out to be also a good instrument for studies of long-term
global solar activity. Observing frequency of 17 GHz
best fit to detect polar activity of the Sun which plays
important roles in global activity. Due to good design
and proper maintenance, operation of the instrument isquite stable. Even after more than 20 years of continuous
operation, observations are almost perfect. This enables
us to synthesize a radio butterfly diagram with which
long-term global solar activity can be studied. We are
currently facing a low solar activity period we havenever experienced with modern observing facilities inhands. This unusual activity is a good chance to deeply
understand solar activity itself and also its influence tosurrounding interplanetary space including the earth's
upper atmosphere. Especially, polar regions are known
as the sources of solar wind which fills the wholeinterplanetary space inside the heliosphere. We hope
NoRH can continue operation further and contribute tounderstand global solar activity [1].
Reference[1] Shibasaki, K.: 2013, PASJ, 65, S17.

Figure 1: Radio Butterfly Diagram.

I Scientific Highlights

053

II Status Reports of Research Activities
1. Subaru Telescope
The Subaru Telescope engages in open-use observations
using the Subaru Telescope (an 8.2 m large optical/infrared
telescope) at the top of Mauna Kea on the island of Hawai`i;
operation of an observational data archive system; observational
research; and research and development for telescope systems,
observational equipment, and data processing software.
A two-month downtime period was scheduled in Augustand September for FY 2013, during which time the telescope
underwent major maintenance, including recoating of the
primary mirror. As a new open-use instrument, the ultrawide-field camera Hyper Suprime-Cam (HSC) continued
test observations from the previous year, followed by thecommencement of open-use observations in March 2014.
Strategic programs include a wide-field imaging survey using
the HSC that began this year; the Strategic Explorations of
Exoplanets and Disks with Subaru (SEEDS) project using
the High-Contrast Instrument for the Subaru Next Generation
Adaptive Optics (HiCIAO), which was continued from FY
2009; and FastSound using the Fiber Multi-Object Spectrograph(FMOS), which began in FY 2011.
Open use for FY 2013 included a four-month period
beginning April 1, 2013, as part of S13A (from February 1,2013), a full six-month period of S13B starting on August 1, andthe initial two months of S14A, which began February 1, 2014.
This report contains statistics in relation to open use based on
only S13A and S13B terms.

1. Subaru Telescope Staff
As of the end of FY 2013, the Subaru Telescope Project
staff consisted of 19 dedicated faculty members including six
stationed at Mitaka, four engineers, and three administrative
staff members. Additional staff members include four researchexperts, three postdoctoral fellows, one research associate,and seven administration associates, all of whom stationed at
Mitaka. Moreover, 11 research/teaching staff members, 10 ofwhom are stationed at Mitaka, and two engineers at Mitaka areposted concurrently. The project also has 72 local staff members
dispatched from the Research Corporation of the University of
Hawaii (RCUH), including scientific assistants; engineers incharge of software and observational instruments; technicians
for facilities, machinery, vehicles, and laboratories; telescope/
instrument operators; secretaries; librarians; administrative staff;
researchers employed for Grant-in-Aid for Scientific Research;and graduate students. These staff members work together
in operating the telescope, observational instruments, andobservational facilities and in conducting open-use observations,
R&D, public outreach, and educational activities.

054

II Status Reports of Research Activities

2. Remarkable Observational Results
The following papers were published in FY 2013 on theimportant research results from observations using the Subaru
telescope:(1) In early Universe studies, a GRB which occurred only
1 billion years after the birth of the Universe was observed.
This high-accuracy spectroscopic observation captured for the
first time indications that the light emitted from the GRB wasabsorbed by hydrogen gas that was high in neutral atoms. Thisfinding serves as an evidence of our exploration of the early
Universe entering the epoch when the Universe was abundant inneutral hydrogen.
(2) In studies of the peak galactic evolution epoch, theproject used Subaru’s primary-focus wide-field near-infrared
spectrograph, known as FMOS, to examine the activity level ofstar formation in the Universe 10 billion light years distant andthe heavy elements and dust content in the ambient gas of themassive galaxies. The results indicate that the galaxies were in
their maturity. In addition, by using Suprime-Cam, 12 galaxies
at 9 billion light years which are releasing hot oxygen gas
into the inter-galactic regions that was wider than the galaxies
themselves were discovered. Such outflows would be driven by
giant black holes in the center or by explosive star-formation in
the midst of the galaxy formation process.
(3) In studies of black holes and accretion disks, an observation
using gravitational lensing succeeded in observing a quasar
at the distance of 10 billion light years from two different
angles, elucidating varying gas emissions three-dimensionally.
Moreover, a structural high-resolution infrared observationof colliding galaxies revealed that only 15 % of the objects
had plural numbers of supergiant black holes within them.
This finding is contrary to previous speculations. The galaxy
collisions were previously believed to be closely related to theblack hole activities; instead, the relationships had varieties.
(4) In protoplanetary disk observations, the strategic project
SEEDS using HiCIAO with a direct imaging method succeededin the world’s first detection of a planet that was the darkest andof the lowest temperature ever observed orbiting around a sunlike star. It also discovered a planetary system that involved aplanet in a retrograde motion together with other planets andaccompanying stars, which serves as suggestive evidence ofplanet configurations in retrograde motion.

3. Open Use
Open use is conducted with proposals called for every six
months. For the first and second halves of the year, the offeredperiods were from February 1 to July 31 (S13A) and from
August 1 to January 31 (S13B), respectively. Applications
were accepted at the NAOJ Mitaka campus. The Subaru Time
Allocation Committee, under the NAOJ Advisory Committee
for Optical and Infrared Astronomy, examines the proposals
and determines projects for adoption with reference to referee
evaluations from Japan and from overseas. The following
proposals were adopted: 52 proposals (85.5 nights) for S13A,
out of 143 submissions (368 nights), and 41 proposals (62.5nights) for S13B out of 146 submissions (362.6 nights). Shortterm projects were also conducted within the framework ofservice program observations. Of the aforementioned proposals
accepted for open use in S13A and S13B (excluding Universityof Hawaii time), 12 (10 in S13A and 2 in S13B) were conductedby non-Japanese PIs. The cumulative total of respondents,
including co-investigators, was 1,741 belonging to Japaneseorganizations and 532 belonging to overseas groups. The
cumulative total of researchers among accepted projects was 605
from Japan and 225 from overseas.
A cumulative total of 342 open-use observers, including
40 from overseas, participated in S13A and S13B. Calls forobservation proposals, examination of submissions, proceduresfor visiting the observatory, and domestic travel reimbursement
for Japanese researchers on their observational trips werehandled by the NAOJ Mitaka. The Subaru Telescope facility set
observation schedules and provided researchers with support inarranging accommodations, travel, and observation in Hawaii.
In open-use observations and UH time, 88.6 % of the telescope
time was operational, discounting weather-related factors andthe downtime scheduled for maintenance work including therecoating of the primary mirror. Instruments, network system,and telescope problems resulted in downtimes of roughly 3.9 %,0.8 %, and 6.7 %, respectively.
No remote observation from the Hilo Operations Support
Facility was conducted during S13A and S13B. Service
observations were performed for 13 nights. Observing time wasexchanged with the Gemini telescope and the Keck telescopein order to make effective use of the resources of the telescopegroup on Mauna Kea; two nights in S13A and 4.5 nights in
S13B were exchanged with Gemini, and four nights in S13A andsix nights in S13B with were exchanged with Keck.

4. Telescope Maintenance and Performance
Improvement
The main features of the telescope have remained at
the same performance levels as that in the previous year.
Technicians were dispatched from NAOJ Mizusawa, Mitaka,and Nobeyama this year to give support in executing the primary
mirror recoating. Before work began, however, some damage
was discovered on the back of the primary mirror element near
the edge, which was subsequently mended. The period of mirror

recoating served as a good opportunity for undertaking some ofthe difficult tasks while the telescope was in operation, such as
replacement of the Cassegrain automatic connector and partial
replacement of the pump for fluid static bearing. Other tasks
difficult to pursue with the primary mirror in position were also
completed, including maintenance work of the CO2 cleaning
facility, and repair and tuning of the Cassegrain atmosphericdispersion corrector optical system, which was affected bycoolant leakage occurred in FY 2011.
Further improvement was made on the telescope’s
performance and operational efficiency by upgrading thetelescope control devices that have been in use for at least
10 years. Local control devices submitted for upgrade or
refurbishment this year include a mount control system,
secondary mirror control system, tip–tilt motion control
system, field rotation control system, cable wind-up drive/
torque detection control system, AG/SH drive control system,
and focus-field rotation control system. In addition, the aging
windscreen’s unstable coupling was improved. Moreover, an
incident occurring in July was investigated in which the altitude
axis lost control. The cause was determined to be the aging
control circuit, which was subsequently resolved by replacing
the mount control system. Furthermore, a power outage insidethe dome related to the malfunctioning of a slip ring has been
examined to identify the cause.

5. Instrument Operation and Development
All eight open-use instruments have been operating stably
since last year. The HSC was introduced for open use and has
been operating since the S14A term. The following instruments
were provided for open use at the Subaru Telescope facility: aprime focus camera (Suprime-Cam), a faint object camera andspectrograph (FOCAS), a high-dispersion spectrograph (HDS),a near-infrared camera and spectrograph (IRCS), a cooled midinfrared camera and spectrograph (COMICS), a multi-object
infrared camera and spectrograph (MOIRCS), a Fiber MultiObject Spectrograph (FMOS), and laser guide star adaptive
optics (AO188/LGS).
The HSC was applied to test observations for seven nights
in June and five nights in October, 2013, as well as eight nights
in January and February 2014 for FY 2013. Despite the highincidence of inclement weather, conditions were sufficient for
performing the test observations roughly half of the time. The
issues identified through this testing included (1) scattering/straylight, (2) vacuum leak under extremely low humidity, and (3)partial movement defect in the CCD. The first issue was further
investigated, and the result was attributed to certain light patterns
due to the uneven filter permeability rather than scattering/stray light. The cause of the second issue was identified to be
the alumited groove on the O-ring. The third issue is still underinvestigation, and plans are underway to rectify the situation byadjusting the operational configurations. Basic performances
including image quality and system throughput were confirmed
to meet the requirements of the design. Therefore, the HSC
was put to open use and strategic observations in late March

II Status Reports of Research Activities055

2014. The following tasks must be performed in the future: (a)realizing an auto-focus mechanism, (b) developing a throughput
measurement system, (c) establishing operational stability of thefilter exchange device, (d) addressing the malfunctioning CCD,
and (e) establishing a data analysis support structure for openuse users. The following upgrades of the existing instruments
were performed: development of multi-object unit for the HDS,
replacement of the MOIRCS detectors and development of its
integral field units, preparation for the introduction of an integral
field unit for spectroscopy, and development of a polarizing
plate for the COMICS.
With respect to PI-type instruments, the HiCIAO highcontrast coronagraphic imager and the Kyoto3DII visible
integral field spectrograph were used in open-use observations.
The HiCIAO continued to play a central role in the SEEDS
strategic observational project, delivering successful results.
Moreover, new technology to reduce quasi-static speckle noise
was established for the Subaru Coronagraphic Extreme Adaptive
Optic (SCExAO), which is a high spatial resolution andcontrast coronagraph, and performance tests in adaptive optics
were conducted to achieve higher resolutions. Demonstrative
observations were also performed for two optical interferometer
modules known as VAMPIRES and FIRST that enabled
observation at an even higher spatial resolution. The RAVEN,a multi-object adaptive optics system under joint developmentwith Canadian research institutes, was transferred from Canada
to the Hilo Base Facility of the Subaru Telescope, and finetuning was executed in preparation for the test observation
scheduled in FY 2014. The RAVEN will be the demonstration
piece for the future Thirty-Meter Telescope (TMT) observational
instrument.
Also under development are a near-infrared spectrograph(infrared Doppler, IRD) yielding high wavelength stability and
CHARIS, an instrument for performing near-infrared integral
field spectroscopic observation at high spatial resolution in
combination with AO188 and the SCExAO. Reviews for
final designs and instrument acceptance were conducted forboth systems. These devices promise further developments in
exoplanet research. The IRD continues to be under considerationfor onsite operation, given its impact on the observatory.
A development is underway for an ultra-wide-field prime
focus spectrograph (PFS) for installation on the Subaru
telescope as the main instrument of the facility following the
HSC. The PFS uses 2,400 optical fiber positioners to divert
the light of celestial objects from the prime focus to four setsof spectrographs installed in the dome, enabling simultaneous
observation at wavelengths of 0.38 μm–1.26 μm. Progress wasmade in the design details in FY 2013, with some brought toproduction. The PFS is a complex international project witha large budget across several countries. Submitted for NAOJ
review from the perspective of project management, it transpired
because reconsideration was strongly recommended for realisticplanning up to the project completion, in accordance with thebudget status.
Following the HSC and PFS, another major project for
future undertaking is Ground-Layer Adaptive Optics (GLAO),

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which facilitates a correction of atmospheric turbulence in thewide field of view. This project involves the development of an
adaptive secondary mirror and a new wide-field near-infrared
camera and spectrograph. The Subaru Telescope aims to begin
operation GLAO as its main instrument in the 2020s to coincidewith the commencement of TMT observations. A review ofconcept design scheduled in FY 2013 was postponed; instead,possibilities for wider usage were explored with an eye oninternational collaborations.

6. Computer Systems/Software
The goal for FY 2013 was to achieve stable operation of
the fourth-generation computer system, which was installed in
February 2013. The system is running well with major error
reported thus far. In January 2014, illegal access was detected
to have been made to one of the Subaru Telescope’s computersfrom a Mitaka computer that had been under cyber-attack. No
sign of data leakage or falsification was detected, however. An
inappropriate management of access log-in details on the user’spart was a major factor leading to this incident. Therefore,
computer log-in details were changed at the Subaru Telescope
facility as an emergency countermeasure. Ways to monitor andrecord access from the Mitaka network are under discussion.
The data archive, which had been running on the basis of public
test operations since FY 2011, moved into a full-scale operation
under the new system. No major issues have been reported thus
far, and the new system is operating smoothly. An easy-to-use
interface was developed for this system to accommodate theactual level of utilization of the archive system. By installing
an inexpensive database engine, the operational cost wassignificantly reduced.
Along with the data archive management at Mitaka, theMitaka subsystem continues to provide support for the Subaru
telescope users, including remote observation monitoring. The
Web-based proposal application system, which was introducedin the S11B term, continues to operate with some improvements.
A system error occurred in March 2014 in the proposal
application for the S14B term due to insufficient testing after
the system update. Following the incident, the management
manual was reviewed to mandate sufficient testing after system
upgrades.
New computer systems were installed in FYs 2010 and2011 for enhanced efficiency in processing data from the HSC,
which generated a massive volume of data. For FY 2013, test
operations and modifications were undertaken for the processing
programs.
The license agreement for the dedicated network line
between Mitaka and the Subaru Telescope facility will expire in
March 2014. Therefore, an application was made to procure thededicated network line for use from April 2014.
Development commenced this year for a new computer
system to process Web-based applications for observational
visits, replacing the current system based on paper forms/FAX.
The new system is expected to be launched in the latter half of
FY 2014.

7. University/Graduate School Education
The number of research/teaching staff members posted
concurrently in Hawaii from the Graduate University for
Advanced Studies increased by two to a total of 11 members.
The number of graduate students of the Graduate University for
Advanced Studies who are supervised by the Subaru Telescope
teaching staff (including concurrent posts) increased to 16,
accounting for roughly half of all postgraduate students engaged
at the NAOJ. Full-time teaching staff at the Subaru Telescope
facility supervise nine graduate students.
Four graduate students were stationed at the Subaru
Telescope facility on a long-term basis in FY 2013, two ofwhom were from the Graduate University for Advanced Studies.
Educational activities for graduate students were also active at
Mitaka, in cooperation with the Division of Optical and Infrared
Astronomy. Eleven graduate students across Japan obtained
degrees for their research using Subaru telescope, marking
an increase by four from last year. Four students among thembelonged to the NAOJ optical/infrared group.
The Subaru Winter School was held for the first time at therecommendation of the Subaru Advisory Committee in February
2014. As a joint project with Korean KASI, it was held at the
KASI in Daejeon, South Korea, and a total of 25 Japanese andKorean postdoctoral researchers, as well as postgraduate andundergraduate students, participated. This school provided
workshops on data analysis and lectures on telescopes,
instruments, operation, science, and other topics. The Subaru
Observation Experience Program for undergraduate students
around the country and the Subaru Observation Workshop
for the Graduate University for Advanced Studies were also
conducted in November.
The Subaru Telescope facility also organizes Subaru
Seminars twice or three times per month (in English), in which
participants in open-use projects, visitors, and Subaru Telescope
staff report their latest research results. Other seminars areheld at Mitaka, in collaboration with NAOJ staff from different
sections or neighboring universities.

8. Public Information and Outreach Activities
A major social responsibility of the Subaru Telescope
facility is the response to or increase of the high levels ofinterest in astronomical research among the general public.
The Public Information and Outreach (PIO) Office has
been established in order to contribute to short- and longterm successes of projects and engages in three basic typesof activities. Particular care is taken in engaging with thelocal populace, as their understanding of the activities being
conducted at the Subaru Telescope facility is a key factor for
acceptance of these activities and next-generation projects by
the local community. The primary activity of the PIO Office isinformation sharing. The office has created a website in order toreach a wider audience with the scientific results produced by
the Subaru Telescope researchers and observatory activities aswell as press releases for public announcements and information

disclosure. This year, 21 research reports (10 in Japanese and 19
in English) and 84 articles (43 in Japanese and 41 in English) on
topics such as instrumental development, observatory activities,
and news items were published on the website. Information is
distributed to the media in Japan or locally in Hawaii directly orworldwide via the mailing service of the American Astronomical
Society, as appropriate. Apart from the website, the use of newcommunication tools is increasing regularly, including social
media such as Twitter and Facebook and video-streaming
on YouTube. Other continuing PIO activities include media
interviews (seven in Japanese and three in English), responses
to media inquiries (nine in Japanese and four in English), andresponse to various questions asked by officials from educational
institutions or science museums.
The second pillar of the Office’s activities is offering facility
tours to familiarize wide audience with the observatory’s
activities. For the Subaru Telescope (summit facility) tour
program offered since FY 2004, full-time specialist staff plays
a major role in promoting timely communications with visitors
and prospective visitors. The general visit program, which
can now be booked online, welcomed 521 people this year
excluding August and September, when general visitor reception
was suspended due to the deposition work of the primary
mirror. Special visits were arranged for 138 people, and the total
number was 1,269 visitors.
In addition to offering facility tours, the Operations Support
Facility provided lectures and occupational mentoring by staff
members and guidance by researchers to visiting students on
their research presentations. Facility tours were provided to 526
people in 50 groups this year.
The third pillar of the Office’s activities is educational
and promotional activities in the form of lectures and teaching
visits targeting the local community, as well as remote
lectures and courses conducted with participants in Japan via
teleconferencing. A total of 100 lectures and classes were given
at the Operations Support Facility, the Imiloa Astronomy Center,and other local venues, while eight guest lectures and 16 remote
lectures were given outside Hawaii Island such as in Japan.
Local school visits included 69 classes allocated to the Subaru
Telescope facility during a special one-week intensive coursewith the participation of the Mauna Kea Astronomical OutreachCommittee. This program enabled the promotion of astronomy
to more than 1,600 students.
Although the Subaru Telescope facility does not hold open
house events, it participated in two local events in Hilo together
with the Mauna Kea observatories to offer science workshops,
exhibitions, demonstrations and explanations. These events, inwhich the Mauna Kea observatories participate annually, offer
good opportunities for socializing with approximately 2,000
citizens, including families, school students, and teaching staff.

II Status Reports of Research Activities057

2. Okayama Astrophysical Observatory
The Okayama Astrophysical Observatory, (hereafter theobservatory) serves as the observing and research base of the
optical and infrared astronomy in Japan, and it promotes open
use primarily of the 188-cm telescope to universities throughout
the country. It also pursues joint R&D projects with universities,
contributing toward forming stronger foundations of astronomy
research at the universities. Concurrently, the observatory
pursues its own research activities, taking advantage of its
location and observational environment.
About 220 nights at the 188-cm telescope are exploited forobservations by researchers from across the country through theopen use every year. The observatory maintains and operates
the observing instruments and provides the observers withsupports 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 it engages
in a comprehensive survey of infrared-variable objects on
the Galactic plane. Another project is the upgrade of thefunctionalities of the 188-cm telescope in order to significantly
improve its planet searching capability through a Grant-in-Aid
for Scientific Research (Basic Research (A), FY 2011–2015) .
The personnel breakdown as of March 2014 was six
full-time staff members, including two associate professors,
one assistant professor, one chief research engineer, one
engineer, and one chief clerk; eleven contracted staff members,
including two research experts, two postdoctoral fellows, two
research supporters, three administrative supporters, and two
administrative maintenance staffs; and one temporary staff
member.

1. Open Use(1) Overview
The open use of the 188-cm telescope was suspended
between January and April to allow the major upgrade of thetelescope functionalities in 2013. The numbers of nights allottedto the open use in 2013 were 25 nights in the first semester (Mayto June this year) and 95.5 nights for the second semester (August
to December). Observing proposals were called for publicly.
The Okayama program subcommittee reviewed the submitted

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proposals and accepted one project observation program and 17
general observation proposals. Open-use observation generally
proceeded without incident. The successful upgrade of the 188cm telescope significantly reduced the occurrence of troubles
during observations. Discussions were held on the validity of
the anonymous application system, which was introduced in
2006, whereby the names of proposal applicants were concealed
from referees. The discussion was initiated at the programsubcommittee in June and was passed to the users’ meeting inAugust. These discussions were followed by judgment at the
program subcommittee in November, which considered theuser survey of October. The final plan was to abolish the system
and revert to the previous method, starting from the call forobserving proposals for the second semester of 2014.
(2) Observation/Research results
The majority of objects observed through the open use in2013 were stellar sources. Others included Solar System objects,
interstellar media, quasi-stellar objects, and AGN. The following
primary observation themes were noted: searching for exoplanets
via precise radial velocity measurement; elemental abundance
analysis of stars via high-dispersion spectroscopic observation;and the observation of exoplanet transits by precise near-infrareddifferential photometry, which increased precipitously in recent
years. Also increased were optical low-dispersion spectroscopic
observations of stars for classification and of sudden phenomena
for follow-ups. As in previous years, a number of observational
studies were conducted by individual groups of researchers
within the open-use framework, and their respective research
results were reported in meetings and conferences or were
published in peer-reviewed journals. Please see the proceedingsof the users’ meeting and relevant conferences and the reports
made at the annual meetings of the astronomical society ofJapan.
(3) Facility and Instrument Maintenance/Management
The high-dispersion Echelle spectrograph (HIDES) and its
fiber link system were connected to the 188-cm telescope in
April so that research data could be obtained smoothly. During
the maintenance period in June, the annual re-aluminizationof the primary mirror of the 188-cm telescope was passed.
Instead, the April work was continued, this time, to connect
the near-infrared imager/spectrograph (ISLE) and the Kyoto–
Okayama optical low-dispersion spectrograph (KOOLS) to thetelescope. Moreover, utmost efforts were made to maintain highobservation efficiency by conducting monthly cleaning of the
primary, secondary, and tertiary mirrors of the 188-cm telescope.
The dome was checked daily. Other maintenance work was also
performed, including a repair of the external panels of the dome
hemisphere and maintenance of the lifter floor controller inJune, replacement of the chiller for the aluminization chamber inAugust, repair of the upper/lower slit guiding rails in September
and March, servicing of the tro-reel in September, maintenanceof the controller of the aluminization chamber in October,maintenance of the dome controlling system in November, andreplacement of the power supply cables for the air-conditioners
and dome’s rotation brake in December. A failure of the powercollection points in the tro-reel occurred in October and acountermeasure based on the subsequent investigation of thecause was installed in the surrounding area during December–March. Lubrication of the telescope and dome, scheduled
for September maintenance every year, was missed this year.
The observatory, however, responded to the request for realuminization of the primary mirror of the 1.5-m Kanata
telescope at Hiroshima University in October. Work safety was
given priority in accomplishing the aforementioned maintenancework and observing instrument exchanges. One potentially
dangerous incident and four accidents occurred during FY 2013.
No one was injured on any of these occasions, and all five cases
were reported to the Industrial Health and Safety Committee.
(4) Conferences
The program subcommittee met on June 24 and November
14 to evaluate proposals for the open use of the second
semester of 2013 and the first semester of 2014, respectively,
and formulated an observation program for each semester. The
Okayama Users Meeting, also known as the 24th Optical andInfrared Users Meeting, was held at the Kurashiki City Art
Museum between August 1 and 3. The observatory reported its
present activities and overall conditions, particularly the statusof the 188-cm telescope following last year’s refurbishment.
Reports by others included research results from open-use
projects and user-led plans to develop new observational
instruments. Also discussed were the operations of other opticaland infrared observational facilities such as the Higashi–
Hiroshima Observatory and the networking of small- andmid-sized telescopes. On day three of the meeting, a report
was given on the progress of Kyoto University’s Okayama
3.8-m new technology optical and infrared telescope projectand proposals were presented on the initial research themes,
observing instrument plan, and operation systems before andafter completion. The proposals were followed by a stimulating
debate.

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. Its observing
capability 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 over the previous value and radial
velocity measurement precision of approximately 2 m/s, whichis comparable to the case of the Coudé light path. The test
observation of the link was conducted in 2010, and it has been
provided to the open use since 2011. The number of its use
increased steadily, and three academic journal papers and two
doctoral theses based on data taken using the fiber link were

published in FY 2013. Major work pursued in FY 2013 included
connecting the HIDES to the refurbished 188-cm telescope
system and website updates to enhance its user-friendliness.
Regarding the development of a nearly 100 K wavelength
resolution fiber link, some fine adjustments were made, andpreparations for test observations are in progress.
(2) ISLE (Near-Infrared Imager/Spectrograph)
The instrument ISLE is a near-infrared imager and lowor mid-dispersion spectrograph, and has been available for the
project observations and the academic degree support programs
since the second semester of 2011. It is the only open-use
instrument in East Asia that offers near-infrared spectroscopic
capability and is characterized as having 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, the ISLE has been in greater demandfor observations of exoplanet transits. Of the eight openuse observations actually conducted in 2013, four were
spectroscopic observations and the other four were exoplanet
transit observations, including one for the academic degree
support program.
(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, which had previously beena concern, was improved in FY 2009, relaxing the limitations
on imaging observations and on spectroscopic observationsof bright objects, in particular. Software improvements haveallowed for observations of non-sidereal motion objects andlong integration time is feasible for observations of Solar Systemobjects. The open-use applications for KOOLS have increased
due to a recent rise in demand for spectral classification andmonitoring observations.

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 3.8m telescope project as part of the future plan of the observatory.
Discussions were held on technological issues regarding thetelescope and dome through weekly TV conferences and inperson meetings held every three months. The supplemental
budget for FY 2013 allowed for the cost of constructing the main
telescope for the project, bringing the project into full action.
(2) The Optical & Near-Infrared Astronomy Inter-University
Cooperation ProgramThis program has entered its third year since its
commencement in 2011. The Okayama astrophysical observatory
has contributed the 188-cm, 91-cm, and 50-cm telescopes to

II Status Reports of Research Activities059

the program, and has taken a leading role along with the Officeof International Relations. The observatory provided a totalof 41 nights worth of observational data on three objects thisyear. It also took an active role in the information sharing,system developing, and actual observations for the cooperative
observation and education network, which the project aimed toestablish. The observatory was also actively involved in leading
the actual observations. Furthermore, it welcomed short-stayworkshop programs from other universities and gave handson instructions to the postgraduate students. One peer-reviewed
paper, in which data taken with the 50-cm telescope were also
used, on a GRB was published in the scientific journal Sciencein FY 2013, while GRBs have the highest priority among the
project’s scientific targets. Further, three additional papers were
published in relation to the project.
(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 2013, the automatic observation
scheduler performed observations on nearly every possible night;
34 GRBs were observed, with optical afterglows successfully
detected in four. Observation results were published as 17
GRB Coordinates Network (GCN) circulars. The monitoringof cataclysmic variables and Mira variables and observationsof exoplanet transits were concurrently performed in addition,
which resulted in publication of five peer-reviewed papers.
(4) Other
The observatory welcomed five third-year undergraduate
students from the University of Tokyo between August 5 and
7 and provided them with an opportunity to conduct highdispersion spectroscopic observation using the 188-cm telescopeduring the early half night on August 5.

4. Unique Research Projects(1) Detection of afterglow of distant GRBs and survey ofvariable 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 andcomprehensively 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. New
variable objects were successfully detected in a K-band image
obtained at the Galactic plane with the camera by subtracting
a corresponding Two Micron All Sky Survey (2MASS) image
from it, indicating the promising prospect of achieving the initial
objective. Fine optical adjustment was conducted in FY 2013 inorder to widen the area of good imaging quality within the fieldof view for higher survey efficiency.
(2) Automation of Exoplanetary System Searches
Through a Grant-in-Aid for Scientific Research (Basic
Research (A), “Automation of exoplanetary system searches,”

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representative: Hideyuki Izumiura, FY 2011–2015), a project isunderway to improve the functionalities of the 188-cm telescopeand its dome, to enhance the precision and stability of thetelescope, to facilitate automation of observation, and to further
expand the search for exoplanetary systems. Successful upgrade
was conducted last year on the drive and control systems as wellas the dome control system of the same telescope. This year,
integration work was undertaken on the observation system,
including the observing instruments, to achieve significantly
higher reliability and an improved observing efficiency byapproximately 20 % while maintaining the excellent easeavailable before the upgrade.
(3) East Asian Planet Search Network
The observatory also conducts studies focusing on the searchfor exoplanetary systems, involving researchers from South
Korea, China, Turkey, and Russia. The efforts continued in FY
2013 to secure telescope time for 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. Moreover, a
conference on exoplanet search based on precise radial velocity
measurement and asteroseismology was held on Ishigaki Islandon Sept. 4–6, 2013 with 16 participants from South Korea,
China, Germany, and Japan.

5. PR/Awareness Promotion Activities
An observatory representative delivered a lecture to nearly
60 people in Okayama City on July 7 as part of the Nation-Wide
Tanabata Participatory Lectures. Nearly 70 astronomy-related
questions were posed and answered at this year’s event. The
4D2U screening, co-hosted with the Okayama Astronomical
Museum, attracted 4,721 visitors. Seventeen observatory tours
were conducted for pupils from local elementary schools in
Asakuchi city and Yakage town. The observatory also responded
to eight lecture requests made by local boards of education andcommunity centers.

6. Contract Staff Transfers
The following transfers of contract staff members took
place in FY 2013: Hironori Tsutsui joined in April as a ResearchExpert member and subsequently left the position at the end of
February 2014 to be an Engineer at NAOJ beginning in March.
Akira Imada, a Postdoctoral Fellow, departed at the end of FY
2013 upon completion of his term.

3. Nobeyama Radio Observatory
1. 45-m Radio Telescope(1) Open Use
The 32nd open-use observation period began on December
16, 2013. The accepted proposals are listed below.
- General proposals for the first term: 20 including 2 fromoverseas (of 47 applications)- General proposals for the second term: 14 including 3 fromoverseas (of 30 applications)- Proposals for short programs: 12 including 2 from overseas (of26 applications)- Educational support (first and second terms): no proposal was
adopted (one application)
Two backup programs (of two applications) were accepted
for use in the case of inclement weather preventing ideal
observation. Of the two, one was taken as a backup program forgeneral application for the second term.
One open-use project with VERA was also conducted.
(2) Device Repair/Development
Maintenance work on and development of a newobservational system continued from the previous year.
- Following test runs, the computer update was implemented
during the summer to be able to conduct open-use
observations.
- The cable of a lightning arrester system installed in the antenna
exhibited partial dislocation. Therefore, it was removed
completely to eliminate the risk for safety reasons.
- Improvement was made to the dual-beam receiver TZ, andbeam 2 was released to open use in addition to beam 1 (themain beam). This receiver became widely used as a primary
receiver for the 100-GHz region.
- A 70-GHz receiver, T70, was released for open use.
- A new multi-beam receiver, the Four-beam Receiver System
on 45-m Telescope (FOREST), was installed and wascommissioned to do performance evaluations as well as test
observations.
- The Nobeyama Radio Observatory (NRO) supported the Z45
team in the installation of a 45-GHz receiver, Z45, funded
by a Grand-in-Aid for Scientific Research, particularly withhardware and software connections and test runs.
- The NRO added functions in the software related to the newreceivers.
- Remote observation from Mitaka was made available for openuse.
(3) Research Results
Two main projects, a star-formation project and a distantgalaxies project, pursued the 45-m telescope legacy project.
Their accomplishments are listed below.
(a) Legacy star-forming project: The Beam Array Receiver
System (BEARS) and TZ receivers were employed for mapping

observations of the nearby star-forming region Orion A and theAquila Rift in the W40 region. The filaments and shell-shaped
structures within the nebula in Orion A were observed in detailin 13CO. Furthermore, the data on Orion A is currently used fora high-resolution, large-scale map through combinationof 45-m
telescope and interferometer data in a joint research projectwith the Combined Array for Research in Millimeter-wave
Astronomy (CARMA). A scientific paper (Shimajiri et al. 2014)
was published using the data from the previous season, and afigure from the manuscript appeared on the cover of the journal
Astronomy and Astrophysics.
In the W40 observation, the molecular emission line data of
13CO elucidated the formation of the shell-shaped high-density
gases in the vicinity of the HII region, resulting in star formationin the high-density region.
(b) Submillimeter galaxies are important objects for the study ofgalactic formation at the beginning of the Universe. However,
because they are surrounded by large amount of dust, they
are extremely faint in the visible and infrared spectra, making
it extremely difficult to accurately determine their redshifts.
CO line observations of submillimeter galaxies are currently
underway using the SAM45 spectrometer and the dual-beamreceiver newly installed on the 45-m telescope, which hasenabled direct determination of the redshift of astronomical
objects. A blind redshift search was implemented this year
on four objects with unidentified redshifts including two
submillimeter galaxies discovered through an AsTEC camera
and two detected by the Herschel Space Observatory.

2. NMA-F (SPART project)
A group from Osaka Prefecture University is pursuing
the Solar Planetary Atmosphere Research Telescope (SPART)project to observe the Solar System’s planetary and atmosphericconditions by reusing the Nobeyama millimeter wave
interferometer 10-m radio telescope. This project is expected
to provide important and unique knowledge regarding theinfluences of core star activities on the internal and external
planetary environments and habitable zones in addition to
information about climatic conditions of our Solar System. The
azimuth actuator broke down at the end of last year, but it was
repaired this year by replacing a motor and adjusting the azimuth
gear. Motor vibration in the vertical direction was observed,
which was amended by replacing the motor adjustment. This
allowed for resuming the SPART operation, which had beensuspended since 2012. Additionally, a standing wave removal
filter was developed, and together with the improvement madeto the LO/IF system, the Osaka Prefecture University groupcommenced stationary observation in the 200-GHz region.
This has enabled dual-band observation in the 100-GHz and
200-GHz bands, which includes observation of isotopologues
and trace species at different levels of 12CO and 13CO with J

II Status Reports of Research Activities061

= 2−1, 1−0). As a result, a more accurate retrieval analysis ispossible, allowing for calculation of the mixing ratio and altitude
distributions of molecular probes, unlike that in the conventional
100-GHz band observation. The UNIX-based computers of
the old NMA were all replaced by Linux, controlled by Python
language, and brought entirely under remote operation.

3. Development of a Multicolor Millimeter/
Submillimeter Camera for Atacama Submillimeter
Telescope Experiment (ASTE)
Simultaneous imaging in multiple wavelengths in the
millimeter/submillimeter bands is vital tool for estimating theredshift of submillimeter galaxies and in studying the internal
structure of hot plasma in clusters of galaxies using the Sunyaev–
Zel’dovich effect. Moreover, it is crucial for constraining
physical quantities of the dust in star-forming regions andsetting a limit to the spectral index of the initial submillimeter
afterglow of GRBs. Thus, in order to succeed in large-scale
sky surveys with a continuum camera, the development of amulticolor millimeter/submillimeter camera with a Transition
Edge Sensor (TES) bolometer for observation at wavelengthsof 1.1 mm, 0.87 mm, and 0.46 mm is underway in collaboration
with the University of Tokyo, Hokkaido University, Universityof California Berkeley, and McGill University.
The Atacama Submillimeter Telescope Experiment (ASTE)
telescope was equipped with this bolometer camera receiverand succeeded in acquiring the “first light”image last year. This
year, test installation and observation were conducted from late
October 2013 to early January 2014 in order to examine in detailthe improved bolometer arrays and the optics. Countermeasures
were put in place against difficulties faced last year in thereceiver installation and cryocooler startability, which opened
a way to the smooth commencement of observation. It should
be noted, however, due to bad observing conditions underatmospheric instability during the period, tests were repeatedagain between early March and mid-April 2014. In contrast
to last year's session, where the prototype bolometer arrays
managed to image only bright planets, the celestial signals
were clearly identified from the massive star-forming region
NGC 6334 (NRO bulletin No. 132) within short 20 minutes
integration time. Other objects observed include submillimeter
galaxies and GRBs outside our Galaxy. The data are currently
under analysis.
The efforts in installation test runs, observation, and data
analyses has brought out the effective methods for enhancing
observational efficiency. Accordingly, the NRO engaged instudies and basic designs regarding further optimization of
the bolometer design, improvement of the software for tuning
the bolometer to its optimal operating configurations, andimprovement of readout system by doubling the number ofbolometer pixels per readout channel from 8 to 16, aiming toreach overall bolometer pixels of 1,000. Study is underway
for adding more colors based on the latest superconducting
technology, in preparation for a future upgrade to the final
version.

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4. Other(1) PR Activities at the Nobeyama Campus
Nobeyama has made the campus accessible to the public
at all times since the inauguration of the radio observatory in
1982. With the exception of a few days in late February of thisyear, when heavy snowfall forced the campus to close to the
public, the campus received a cumulative total of 58,543 visitors
throughout the year, including participants of special open house
events. Staff members conducted 18 guided tours, including
participants of Science Partnership Programs (SPPs) and Super
Science High School (SSH) students, while two requests for
lectures and 14 requests for on-site filming and interviews were
granted. In response to public request, the opening hours forviewing were extended by one hour, to18:00 during the summer
months (July 20–August 31).
The Campus Tour Week was launched during the summer
and was aimed at educational institutions (elementary, juniorhigh, and high schools). Staff members gave guided tours
for this program as well. Due to the insufficient length of theapplication period, only two groups took advantage of thisopportunity. However, visitors from the participating schools
said they thoroughly enjoyed their visits. For the workplace
visit initiative conducted between June and October, 10
students from 5 schools, primarily local junior high schools,
visited the observatory and had a chance to experience theobservatory’s routine work under staff guidance. For SPP/SSH
initiatives, seven schools visited the NRO and participated in
lectures, student presentations, and hands-on guidance of future
activities. Furthermore, The workshop of Radio Astronomical
Observation using the 45-m radio telescope was held again thisyear from September 17 to 21, with 12 undergraduate students
in attendance. While guidance to the students, from observations
to presentation of the results, requires significant effort, theevent offers an invaluable opportunity for undergraduates toexperience observations using a radio telescope.
In the area for permanent public access, an antenna
experience facility is available along with posters and panel
displays. A video continuously played in the visitor roomshows various facilities, introduces the history of the NRO,
and explains research results. For Internet-based PR activities,
the NRO runs a website with thorough explanation of theobservational equipment in operation onsite, and content
is increasing to include observational results as well as
introductory descriptions of radio astronomy.
(2) The Record 3 Million Visitors at Nobeyama Campus
Since the opening of the campus to the general public 32
years ago, the cumulative total of visitors to the campus reached
3 million on October 17. A ceremony was organized to celebrate
this achievement, with the 3 millionth visitor treated as anhonorable guest.
(3) Cooperation with Local Communities
The annual Nobeyama Special Open House was held
as usual, with contributions by Minamimaki village, theMinamimaki Chamber of Commerce, and its youth division.
Special sponsorship was made to the sora-girl event Tebura de
Hoshizora Kansho-kai, or drop-by star gazing event, hosted by
the Minamimaki Tourism Association. The NRO also joined theJapan Three Major Scenic Location for Star Gazing with the
Minamimaki Tourism Association: Night Sky Summit that took
place in Bisei-cho, Okayama prefecture.
(4) NRO Conference Workshops- July 24–25, 2013: The 31st NRO Users Meeting (representative:
Tomofumi Umemoto)- July 29–August 1, 2013: The 43rd Summer School for
Young Researchers on Astronomy and Astrophysics 2013
(representative Keisuke Nakagawa)- November 8, 2013: NRO Galactic Plane Survey Workshop(representative: Aya Higuchi)- December 6, 2013: CO Multiline Imaging of Nearby Galaxies(COMING) mini-workshop (representative: Kazuo Sorai)(5) Part-Time Research Staff Transfers○Researchers
Akihiko Hirota: assistant professor, NAOJ Chile Observatory
Tatsuhiro Sato: engineer, NAOJ Subaru Telescope

4. Nobeyama Solar Radio Observatory
1. Radioheliograph- and Radio Polarimeter-Based
Solar Observation and Solar Activity Status
After a long period of minimal solar activity, the 24thsolar activity cycle is approaching a peak period. According toobservational data, the first high point occurred at the beginningof 2012, followed by the second in early 2014. The first peak
was mainly due to activities in the northern hemisphere, whereas
the second peak was mainly attributed to activities in thesouthern hemisphere; the latter superseded the former. Similarity
in the activity pattern to that of the previous cycle was noted.
However, the active regions are small and short-lived comparedwith those in the previous cycles.
The radioheliograph, in continual use since 1992 with very
few failures, provides high-quality, constant data for open use.
One of the front-end receiver boxes installed behind the antenna
incurred a water leak, which resulted in damage to certain
parts. The situation has been rectified by parts replacement.
Data reception from all antennas is still good after 22 years,
and there is no sign of data deterioration. The radio polarimeterhas also produced well-calibrated data during the last 62 years,
since it started at Nagoya University’s Research Institute ofAtmospherics.
Influences from the decreased solar activities are recognizedin many different forms because there is heightened interest in
constant, well-calibrated radio observational data, which theNobeyama Solar Radio Observatory (NSRO) has provided overan extended period. Officials from the observatory are invited
more often to deliver lectures at conferences on space climate.

2. Continuing Radioheliograph Operation
Given such circumstances regarding solar activities,
researchers across the world have requested continuing operationof the Nobeyama radioheliograph. The chairpersons of the
Scientific Committee on Solar-Terrestrial Physics (SCOSTEP),

the International Astronomical Union, Division II (IAU, Div
II), and the European Solar Physics Division (ESPD) of theEuropean Physical Society have submitted written requests to thepresident of the National Institutes of Natural Sciences (NINS)
and the director general of NAOJ for continued radioheliographoperation in FY 2015 and thereafter. Domestically, the solar
community in Japan proposes the inter-university NextGeneration Heliospheric Environment Variation Observation
Network Plan to the Astronomy and Astrophysics Subcommitteeof Science Council of Japan, and the continuation of theradioheliograph operation at Nobeyama is included as a partof the plan. Discussions are underway for the realization of thecontinuous operation from 2015, consideration such frameworks
as funding by an international consortium, management by
Nagoya University’s Solar-Terrestrial Environment Laboratory,
and provision of equipment by NAOJ.

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 the information for their studies on solar phenomena,
space weather, and space climate. The data is also leveraged forthe 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 (CDAW13: September 30–October 4, 2013) heldto actively promote open use in Japan had 21 participants.
With lectures and exercises offered, four groups practiced data
analysis, and attendees subsequently reported the experience atvarious research conferences and to the astronomical society.
The Japan Solar Physics Community held a symposium titled
Solar Research at Activity Maximums: chromospheric plasma
analysis, space weather, and Solar-C at Kyoto University
from February 17 to 19, and the observatory presented its

II Status Reports of Research Activities063

undertakings as well as studies conducted during CSAW13.
Twenty papers were published in December in the special
edition SP1 of the Astronomical Society of Japan’s English
publication PASJ, volume 65, with a title “Twenty Years of
Nobeyama Radioheliograph.” Among the papers included wasan original paper presented at the International Symposium Solarphysics research by radio observation: radioheliograph over the
past 20 years and the future (Nagoya University: November
20–23, 2012).
Vi s i t i n g i n t e r n a t i o n a l r e s e a r c h e r s i n c l u d e d f o u r
representatives of the Korea Astronomy and Space Science
Institute (KASI), who stayed for three days to participate in ajoint research program. Others participating in open-use andjoint research during a few weeks include E. Kuprianova fromthe Pulkovo Astronomical Observatory in Russia, B. Ryabovfrom the Ventspils International Radio Astronomy Centre in
Latvia, A. Warmuth from the Leibniz Institute for Astrophysics
Potsdam in Germany, and V. Nakariakov from the UK.

4. Other
The NSRO participated in the summer student programof the Graduate University for Advanced Studies. It accepted
one undergraduate student for three weeks during summer andprovided him with research guidance on solar activity and space
climate using data available at the observatory. The Cutting
Edge Solar Research Experience Tour, which was organizedjointly by solar-related research institutions in Japan, offeredlectures and a guided tour of the observatory to 13 participants.
Regarding initiatives aimed for high schools, students from
Hakuyo High School in Kanagawa and Komagane TechnicalHigh School in Nagano participated in the SPP program, forwhich the observatory provided lectures and workshops. In
addition, Komagane Technical High School installed its own
radio telescope, for which the observatory rendered support. The
observation results from this telescope were presented to thejunior session of the Annual Spring Meeting of ASJ.
Further, K. Sujin, a research fellow, departed uponcompletion of his term.

5. Mizusawa VLBI Observatory
1. Project Overview
The main purpose of the Mizusawa VLBI Observatory,referred to in this section as “the Observatory,” is topromote observational astronomy using Very Long Baseline
Interferometry (VLBI). The Observatory mainly pursues
analyses of the Milkey Way based on the observational resultsof VLBI Exploration of Radio Astrometry (VERA), consistingof four 20-m radio telescopes of the National Astronomical
Observatory of Japan (NAOJ). It also co-operates several 32-m
radio telescopes installed at the Yamaguchi station in Yamaguchi
prefecture and Hitachi and Takahagi stations in Ibaraki
prefecture in collaboration with local universities in respective
regions. The Observatory performs the role of a key base for
VLBI research in Japan and East Asia, conducting joint research
as well as open-use observations with VERA in combination
with those radio telescopes, in collaboration with the Japanese
VLBI Network, and it extends activities to the East Asia VLBI
array in collaboration with Korea and China. Furthermore, theObservatory maintains and displays Japan Central Standard
Time at its Timekeeping Office.
In 2013, the Observatory began joint operation of ATERUI,
Center for Computational Astrophysics (CfCA) super computer
installed at the Mizusawa campus.
(1) VERAVERA is a project created mainly for elucidating the threedimensional structure of the Milky Way based on high-precision
astrometric observations of the maser sources within the galaxy.
It has been producing astrometric observation data regularly

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II Status Reports of Research Activities

since 2007, using an unprecedented method of dual-beam phasereferencing that utilizes four 20-m radio telescopes locatedrespectively at the Mizusawa, Iriki, Ogasawara, and Ishigakijima
stations. In FY 2013, the Observatory performed the operationand maintenance of the observation array as scheduled andpursued scientific research based on the observational data.
The current main correlator for VERA, an FX correlator set
up at the Mitaka station, is coming to the end of its lifetime andis showing some difficulties in operation even with maintenanceand parts replacement. Therefore, a process is underway for
replacement with a software-based correlator hereafter referred
to as software correlator.
(2) Optical Fiber-connected VLBIIn the Optical Fiber-Connected VLBI observational system,
signals received by radio telescopes at multiple stations areconnected via a high-speed fiber optics network, allowing for areal-time broadband observational system. This system connects
a 32-m radio telescope at the Geospatial Information Authorityof Japan (GSI) in Tsukuba, an 11-m radio telescope at Gifu
University, a 32-m radio telescope at the Yamaguchi Stationof the NAOJ, and an 11-m radio telescope at the Tomakomai
Space Observatory of Hokkaido University via an opticalcommunications network. Signals are transmitted to the NAOJ
Mitaka campus via the Security Innovation Network (SINET)
of a 10-GbE line at 2.4 Gbps. The NAOJ Mitaka campus isequipped with a real-time correlator and disk recording devices;
therefore, it has the capacity for correlation both in real timeand post-processing, as dictated by necessity such as the needfor immediate information distribution. The Mitaka campus

receives live broadband observational data from universitybased stations, records the information on magnetic devices, andforwards it to the East Asia correlation center in South Korea.
(3) Japanese VLBI network Observation
A network is developing between twelve VLBI observation
stations in Japan that includes four NAOJ VERA stations, the11-m radio telescope at Hokkaido University Tomakomai, the34-m radio telescope at the National Institute of Information andCommunications Technology (NICT) Kashima, the 32-m radio
telescope at GSI Tsukuba, the 64-m radio telescope at the Usuda
Deep Space Center of Japan Aerospace Exploration Agency(JAXA), the 45-m radio telescope at NAOJ Nobeyama, the 11-mradio telescope at Gifu University, the 32-m radio telescope at
NAOJ Yamaguchi, and the two 32-m radio telescopes of the
NAOJ Ibaraki Observatory respectively in Hitachi and Takahagi.
The objectives are to conduct high-precision mapping at a highdynamic range in the regions of 6.7 GHz, 8 GHz, and 22 GHz
and to observe methanol masers in the 6.7-GHz band and watermasers in the 22-GHz band.
(4) Japan–Korea, East Asia VLBI Observation
The Japan–Korea VLBI observation utilizes the Japan–
Korea VLBI array (KaVA), which combines VERA and the
Korean VLBI Network (KVN) with three 21-m radio telescopesof the Korea Astronomy and Space Science Institute, to pursue
high-sensitivity, high-precision VLBI observations. A pilot caseof its open use commenced in FY 2013.
The East Asia VLBI Network includes VERA, KVN, andthe Japanese VLBI Network as well as the Chinese VLBI
Network (CVN) with its four observation stations in China. ThisVLBI observational network is the world’s largest, involving
more than 20 stations and a baseline of 6,000 km.
(5) Gravitational Observation and Geodetic VLBI Research
The Mizusawa station conducts VLBI/GPS-based
positioning as well as gravitational observations using a
superconducting gravimeter. The Ishigakijima station conducts
continued observation also using a superconducting gravimeter.
The geodetic VLBI observations employ a method forrecording at 1 Gbps in the 22-GHz region. This method wasdeveloped uniquely for geodetic observation and was applied
for practical use, achieving stable maximal positional precision
on a regular basis. Geodetic observations were implemented
several times for open-use observation between VERA andKVN to connect their networks, and KVN’s coordinates were
subsequently provided. Mizusawa and Ishigakijima stations
regularly participate in the international observations conductedby an international project for the VLBI observations (JADE,IVS-T2) in order to connect the coordinates for the VERA
network to the global coordinate system.
(6) Ishigakijima Astronomical Observatory
This observatory has a 105-cm optical infrared telescope
known as Murikabushi, which is equipped with the MITSuME
three-color simultaneous imaging camera system. Taking

advantage of the locational conditions at latitude 24° N andlongitude 124° E, it engages in gamma-ray burst (GRB)
afterglow observations as well as observational studies ofsupernova explosions and sudden phenomena that occur incomets and planetoids. The Observatory plays an important rolein the Optical and Infrared Synergetic Telescopes for Education
and Research (OISTER), an observational network establishedin 2011.
The Observatory also provides the general public with
opportunities for astronomical observations on weekends andnational holidays. It also makes educational contributions byoffering extracurricular activities for high school students and a
joint course given at the University of the Ryukyus.

2. Project Progress(1) VERA
1) Overall Research
VERA has been active for a little more than a decade. It
continued astrometric observations in FY 2013 at a pace ofapproximately 40 celestial objects per year. A cumulative totalof more than 170 object observations was completed by the endof FY 2013. Ten papers were published in FY2 2013, including
nine papers featured in the Astronomical Herald special edition
on VERA, published by the Astronomical Society of Japan.
These papers discussed the VERA project and galactic
astronomy and included a wide range of activities and researchcovering the areas of fixed stars, new-star forming regions,active galactic nuclei (AGN), and open-use research between the
Atacama Large Millimeter/submillimeter Array (ALMA) and
KaVA. Some topics are relevant to the research described below.
Another special edition of PASJ, the Astronomical Societyof Japan’s English publication, is under preparation and will
focus on VERA. The society is planning to include astrometricobservations, detailed observations of maser objects, and resultsfrom AGN observations using VERA. Also noteworthy for 2013is the capturing of a massive protoplanetary disk structure in
the Orion region by combining the data of ALMA and VERA,
which has enabled the research to enter a new stage.
For the VERA astrometric observations, Imai et al. (2013)
measured the annual parallax of the celestial object IRAS 182860959. Known as “the water fountain,” this object is movingfrom the last stage of stellar evolution, which is a red giant
Asymptotic Giant Branch (AGB) star to a planetary nebula at areported distance of approximately 3.61 kpc (11,700 light-years).
This study not only determined the mass of celestial objects
based on accurate distance data but also presented a clear imageof a water maser bipolar outflow being ejected like a fountain,
thus rendering itself as a valuable model case for studying
the rare water fountain phenomenon. VERA actively engages
in AGB star investigation. Takeuti et al. (2013) also pursued
theoretical research of AGB stars based on such investigations.
In the area of star-formation, Kim et al. (2013) conducted an
observation of water masers in the massive star-forming region
W75N. They were the first to indicate an on-going evolutionary

II Status Reports of Research Activities

065

process in which the celestial object’s typical shell-shaped
outflow transformed into a bipolar form. Furthermore, they used
dual-beam simultaneous observation to monitor radio flares of
the X-ray binary star Cygnus X-3 (CygX-3) including a blackhole and neutron stars (Kim et al. 2013). The study indicatedthe possibility of structural changes during radio flares within
CygX-3 and obtained evidence of concurrent jet projection with
X-ray spectral status change through simultaneous observation.
An open-use study conducted with the Japanese VLBI
Network (JVN), released an observational report of methanol
masers in the 6.7-GHz band within a massive star-forming
region. Sawada-Satoh et al. (2013) successfully identified that
activities of methanol masers in S269 are driven by outflows
from young stars,
whereas Sugiyama et al. (2013) succeeded in capturing animage of the gas surrounding a radio source in Cepheus A thatrevolved concentrically and fell into the center. Both studies
are significant because they succeeded in measuring threedimensional motions of methanol masers in which the propermotion is difficult to measure. These outcomes are substantial
additions to the knowledge of mass radiation and accretion in
massive-star formation.
Additionally, a study has begun with a new perspective of
combining VERA and the emerging observational outcomesof the ALMA cycle 0 in FY 2013. In their study concerning
the massive-star-forming region Orion KL, Hirota et al. (2014)
combined the submillimeter water molecular emission line dataobtained during ALMA cycle 0 with the SiO maser data obtained
through VERA and succeeded in high-definition imaging ofa circumstellar gas disk near the massive protostar known as“radio source I” and an emerging jet. This achievement has
been published on the NAOJ website. Hagiwara et al. (2013)
succeeded in detecting the world’s first submillimeter watermasers at the AGN Circinus during ALMA cycle 0, adding to a
growing anticipation for advancement in VLBI-based researchof external galaxies.
Moreover, the Gamma-Ray Emitting Notable AGN
Monitoring by Japanese VLBI (GENJI) project, created tomonitor AGN at a high frequency, leveraging calibrated celestial
data as part of VERA project observations, began regular
operation in FY 2010; its first report was given by Nagai et al.
(2013). Many studies have reported observations of AGN athigh spatial resolution using VERA, including multi-wavelength
observations of PKS 1510-089, a study conducted jointly withan Italian group (Orienti et al. 2013); an observation combinedwith an X-ray of the gamma ray undetermined celestial object
2FGL J1502.1+5548 (Takahashi et al. 2013); an observation of
objects with high-speed absorption lines by outflows known as
Broad Absorption Line (BAL) quasars (Doi et al. 2013); andan observation of the supermassiveblack hole at the center ofthe Milky Way, Sgr A* (Akiyama et al. 2013). With discussions
for prospective studies of AGN underway, members of the
Observatoryare making good contributions to the international
VLBI observations in the millimeter/submillimeter region (Lu etal. 2013).
The aforementioned VLBI observational studies have066

II Status Reports of Research Activities

been extended to KaVA. The first KaVA open-use observationcommenced in FY 2013. Developmental phases of the East
Asia VLBI Network (EAVN) has been discussed at various
conferences for installment of the antenna in Shanghai.
2) Geophysical/Geodetic Research
Because VERA is in a transitional period toward a newrecording system and correlators, a geodetic VLBI observation/
analysis system is undergoing preparation for adaptation to
VERA’s new recording/correlation system. The new system has
been tested for verification. The observatory developed a systemfor obtaining geodetic data from the software correlator outputs,
and the results successfully verified that the new system attained
the same level of accuracy as the existing VERA geodetic
solutions. Furthermore, the geodetic solution demonstrated
improvement through an application of ionospheric delay
obtained from the global total electron content (TEC) modelto the 22-GHz band geodetic VLBI, which was hitherto being
observed at a single frequency in the 22-GHz band.
The coordinates of each VERA station are provided in adaily coordinate catalog containing the Earth’s crust shift dataobtained from continuous observations of VLBI and Global
Positioning System (GPS). The coordinates of the Mizusawa
station have not as yet been stabilized under the ongoing postfluctuation following the Tohoku Pacific Coast Earthquake(Great East Japan Earthquake). The coordinates of VERA
are calculated by fixing its coordinates and displacement rates
between 2005 and 2008 to the global coordinate solution
provided by the Geospatial Information Authority of Japan andby obtaining the relative positions and displacement values.
The marginal error in VERA astrometric observations iscaused by radio wave propagation delay owing to annual surface
displacement and moisture in the atmosphere. The annual
fluctuation is not considered in the VERA positioning catalog
because although there is a degree of annual millimeter-level
fluctuation in the coordinates obtained through continuous GPS
observations conducted at the VERA station, such fluctuations
are not recognized in the VERA solutions; in addition, theircauses are not verified. An improvement must be made in
the future in the perpendicular accuracy of the solutions bydeploying the data on solutions of propagation delay in theatmospheric moisture produced through the GPS analysis as
well as the Meteorological Agency’s objective data, as well
as external data by ray tracing. To improve the accuracy ofgeodetic solutions, some issues must be addressed such as
an improvement in observational methods by increasing therecording bandwidth of VERA’s new system and adopting a newinternational VLBI observational system.
The displacement velocity field of the Japanese Archipelago
was significantly altered over a broad range by the Tohoku
Pacific Coast Earthquake that occurred on March 11, 2011. The
coordinates of the Mizusawa station had exhibited a gradualsouthwesterly movement of just more than 10 mm per annum
before the earthquake; however, the movement was altereddramatically to east–southeast after the earthquake, continuingeven three years later. Similar findings are confirmed from theEarth crust strain observations conducted at the Esashi Earth
Tides Station. Such observational data are being accumulated
because they are invaluable for understanding the strainreleasing process in the Earth’s crust or upper mantle during alarge-scale earthquake.
3) Operation History
Observations at the four VERA stations are performed
remotely from the array operation center at Mizusawa, with
4,115 hours of observations performed over 504 sessions
in FY 2013. These included VERA open-use observations,
VERA project observations for measuring annual parallax
to calculate the distances to astronomical objects, fringe
detection test observations for maser objects, and candidates forcontinuum sources constituting positional references, geodetic
observations, Japanese VLBI Network observations, and openuse observations with KaVA as well as test observations. The
number and length of these VLBI observations are as follows:- VERA open-use observation (including open use with KVN):
516 hours over 69 sessions- VERA project, test observations: 2,358 hours over 336 sessions- VERA geodetic observations: 664 hours over 27 sessions- Japanese VLBI Network observations: 189 hours over 22
sessions- KaVA project (excluding open use): 388 hours over 50
sessions.
The VLBI observational data was correlated at the Mitaka
VLBI correlation center; the correlation data for the open use
observations and Japanese VLBI Network observations weresent to the principal investigators; and those for the Project
observations and geodetic observations were sent to the analysts
in charge.
4) MaintenanceRegular observations continued in FY 2013 using the VERA
and other telescopes or instruments. The Observatory undertook
necessary maintenance and repairs to ensure stable operations.
The VERA Maintenance Group undertook systematic
performance checks, repairs, and maintenance of broadband
magnetic tape recording devices and also arranged formaintenance by the manufacturer once a year. Everyday upkeep
such as antenna greasing, painting, and repairs was performedby each station. The antennas at stations on remote islands
require frequent repainting and mechanical maintenance, forwhich necessary arrangements were made for timely execution.
It has been more than 10 years since the VERA antennas
were installed, and the wear to their directional rails in theazimuth (AZ) has resulted in lower AZ platforms. This effectis particularly recognizable at the Ishigakijima station, where amajor height adjustment of the AZ platform was executed during
the antenna maintenance work. Similarly, the drive systems havedeteriorated to cause instability to observational operations. As
preventive measures, deteriorated expendable parts in the drive
system such as power modules and condensers were replaced.
Given the finite maintenance budget, the annual maintenancewas divided into two phase. The first phase excluded electricalsystem maintenance as much as possible and included only
mechanical annual maintenance procedures; replacement ofoil sealant for gear boxes; replacement of jack motors fordual-beams, which have failed on occasion; and AZ platform
height adjustment at the Ishigakijima station. The second phaseincluded expendable parts replacements within the drive system,
together with a limited range of electrical system maintenancework. Regarding the dual-beam jack motor failure, 2B motor
cables were also replaced.
Regular maintenance work was undertaken for receiver
performance. In addition, a high-spec, low-noise amplifier
replaced the old amplifier on the Left Hand Circularly Polarized(LHCP) side to be utilized for the regular VERA operation
because high-performance, low-noise amplifiers had been
installed at the Mizusawa and Iriki stations when they introduced
dual-polarization observation in the 43-GHz band. This has
successfully lowered the receiver-end noise temperature byapproximately 30 K at these stations.
A pin-point repainting was executed at the Ogasawara
station, whereas an overall repainting was conducted at the Iriki
station. The Ishigakijima station underwent waterproofing of thefoundation; replacement of the feedome membrane, which wasdeveloped by the observatory; and an overhaul of the hydrogenmaser atomic clock.
5) Technological Development
The agenda for major technological development includes
the development of a software-based correlator to replace theaging FX correlator and a disk-based recording/playback device
to replace the magnetic tape recording device for which the
manufacturer warranty has expired.
In the development of the software correlator, performance
evaluation is close to completion, albeit only in the FX
correlator compatible mode. This will constitute the basis
for a regular operation in addition to the current tapecorrelator processing. The SiO maser multi-line observations,enabled by the software correlator’s wide bandwidth andspectroscopicfunction, confirmed some possibilities for new
scientific endeavor. Considerations on details commenced in
FY 2013, and preparations for a plan to install the software
correlator at Mizusawa are underway including the necessary
arrangements for purchases and installation of power systems
and air conditioning in the room. Once the software correlator
is in operation, it will be possible to process more than 1 Gbps
of broadband data recordings and to significantly increase thenumber of spectral points, bringing considerable advantages to
VERA’s astrometric observations.
In parallel to the replacement of the software correlators,
aged tape recording devices are scheduled to be replaced byhard-disk-based devices. This will enable 2–4 Gbps recording,well exceeding the current 1 Gbps; performance tests and test
operations will be conducted to verify this speed.
Disk recording/playback device development has focusedon two observational modes: an OCTAVIA- and OCTADISKbased 2 Gbps, 2 channel broadband recording system and a 1
Gbps recording system serving as a replacement for DIR2000.

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This equipment has already been introduced at the various
stations in parallel with existing systems. This year, test runs
were performed in tandem with observations to standardize andstabilize the operation of the existing systems. As a result, somevaluable outcomes for stable operation were obtained, including
the discovery that certain hard drive disks (HDDs) caused
system failures when run under the OCTADISK-based system.
In addition, an 8-Gbps ultra-broadband system structure
has been rolled out at the four VERA stations, and research anddevelopment (R&D) is aimed at improving VLBI performancein an attempt to increase the bandwidth for future deployment.
Imaging performance and sensitivity improvement were
evaluated to demonstrate the value of the ultra-broadband
observations. Development of the Korea–Japan Joint VLBICorrelator (KJJVC) is also underway. The development of adisk buffer system, for which Japan was primarily responsible,
was completed. Test observations with KVN were performed,
and the correlation of data from KVN was handled using the
FX correlator, thereby making contributions toward regular
execution of the correlation.
(2) Optical Fiber-connected VLBIIn FY 2013, the optical fiber-connected VLBI was deployedmainly in scientific operations used as a sub-array of theJapanese VLBI Network. Real-time observations, together withbroadband observations, played an important part in improving
the sensitivity of the Japanese VLBI Network and constructing
an interferometer array that connected a diversity of stations.
In particular, disk recording and correlation were conducted at
Mitaka in a VERA-compatible mode during the observation,using the same digital filters as those of VERA. Support wasgiven to each station for operating broadband recording devices,in assistance with the Japanese VLBI Network.
A JGN line from Otemachi to Mizusawa was installed intandem with movement of the supercomputer to Mizusawa.
At the Mitaka campus, researchers verified a 4-Gbps realtime recording of the data from Mizusawa in FY 2013 afterconnecting the JGN and SINET lines at Otemachi.
(3) Japanese VLBI Network Observation
Defects were found in the Takahagi 32-m telescope’s
elevation axis motor and the bearing for the coupling, which are
now under repair.
At the Ibaraki station, a single-dish observation of methanol
maser sources is ongoing daily, using a 6-–9 GHz band receiver.
In FY 2013, the Yamaguchi and Ibaraki stations participatedin the East Asia VLBI Network observations that employedbroadband recording systems. These stations also participatedin the test observation of the global VLBI network, using theInternet protocol (IP)-VLBI system.
A short baseline VLBI observation is undertaken nearly
daily with participations by the NAOJ Mizusawa 10-m telescopeand other telescopes at the Ibaraki, Kashima, and Gifu stations
with the objective of capturing the flares accompanying the gas
accretion at the center of the galaxy, which has been of greatinterest in recent years. Exchanges between universities and068

II Status Reports of Research Activities

research institutes have been actively pursued. Postgraduate
students at Nagoya University and the University of Tsukuba
joined research teams at Ibaraki University and the Universityof Tsukuba. Two researchers have exchanged their positions
between Ibaraki and Yamaguchi Universities, and they engage
in the Japanese VLBI Network research activities at theirrespective institutions. In FY 2013, one postgraduate student
from Ibaraki University was stationed at the Mizusawa VLBI
Observatory (Mitaka) to study the data analysis of the Japanese
VLBI Network and subsequently published a master’s thesis.
In addition, several postgraduate students from Yamaguchi
and Ibaraki Universities published their master’s theses on
the Japanese VLBI Network and research based at the Ibaraki
station.
The Japanese VLBI Network observation projects
continued in FY 2013, and four peer-reviewed papers were
published. Funds transferred to the concerned universities
allowed officials at these universities to perform telescope
maintenance and to hire postdoctoral fellows at their discretion.
An operation meeting is held biweekly, in which stations
report their situations and discuss operational conditions andpolicies. Observations adopted through the proposal system are
conducted approximately 150 hours per year. An operationalcore group was formed for a regular holding of observations.
Osaka Prefecture University also participated in the receiverdevelopment that started in 2007. Ibaraki University joined in
2008, and a framework was established for Ibaraki University
to take charge of observational operations in tandem with thetransfer of two 32-m radio telescopes belonging to the KDDI
Ibaraki Satellite Communications Center to the NAOJ. In
2009, a 6.7-GHz receiver was installed, followed by successful
methanol maser observation. Since FY 2010, VLBI observationsin the frequency bands of 6.7–9 GHz and 22 GHz using two
32-m telescopes have been made possible at the Ibaraki station.
The Ibaraki station suspended operations temporarily following
the 2011 Great East Japan Earthquake. However, it resumed
a test operation after the initial reconstruction efforts at the
beginning of FY 2012, followed by a full recovery after thesecond reconstruction work executed at the end of FY 2012.
JAXA held a workshop on the use of antennas in scientificobservation, and the Japanese VLBI Network reported thatthe same Usuda 64-m radio telescope was in great demand forcontinued use. The methanol maser VLBI survey observation
since 2008 was joined by the Shanghai station and was
successful in capturing images of maser sources in 35regions.
Expectations are high for the future elucidation of the maser
sources’ internal proper motions of the gas that surrounds young,massive objects. A radio exploration of blazar objects thatradiate high-energy gamma rays was conducted using the opticalfiber-connected VLBI broadband recording system. At the Asia–
Pacific Radio Science Conference (AP–RASC 2013), the Young
Scientist Awards were given for observation of methanol masers
through the Japanese VLBI Network (Koichiro Sugiyama,
Yamaguchi University) and the VLBI observation of gamma
ray objects (Kotaro Niinuma, Yamaguchi University) In orderto achieve high spacial resolution, which cannot be attained

within the Japanese VLBI Network, the Yamaguchi and Ibaraki
stations participated in the East Asia VLBI Network three times;
the Korean and Chinese VLBI networks also took part. Those
stations commenced operation of observations utilizing thebroadband disk recording devices installed at their sites. The
hydrogen maser atomic clock of the 11-m telescope at Gifu
University was serviced to correct defects.
(4) Japan/Korea, East Asia VLBI Observation
As the KaVA performance tests progressed, three science
working groups (WGs) for AGN, star formation, and late-typestars proactively pursued test observations and gained fruitfulresults. Concurrently, the first open-use proposals were called forby the end of FY 2013. Test observations have produced resultsin AGN as well as study results of methanol maser objects in
the 6.7-GHz band. The Korea Astronomy and Space Science
Institute accommodates the KJJVC for correlating these data,
which are available for open use. Director meetings between
Japan and Korea were held as necessary to discuss issues in thisregard.
(5) Ishigakijima Astronomical Observatory
The three-color simultaneous imaging camera MITSuME
was developed through joint research between the Tokyo
Institute of Technology and Okayama Astrophysical Observatory(OAO). The camera was moved to the Ishigakijima Observatory
this year, and the Observatoryis now responsible for its
maintenance. This camera system is in full use today, producing
immediate results in observing afterglow of GRBs and sudden
phenomena of supernova, planetoids, and comets to international
acclaim.
A course conducted in cooperation with the University of
the Ryukyus has entered its fifth year. It is particularly popular
for the classroom lectures at the university and the observational
workshops at Ishigakijima, attracting twice as many applicantsas available spots. In FY 2014, the Observatory will collaborate
in broadcasting university lectures to be viewed in Ishigakijima.
In February, an exchange agreement was made with the Nayoro
City Observatory, which house a 1.6-m telescope belonging
to Hokkaido University. The “Chura-boshi (beautiful star)
Research Team” workshop for local high school students, joinedby students from Fukushima prefecture achieved discoveries of
new planetoids and radio stars.
In July, the city of Ishigaki’s Starry Sky Educational Room,
set up at the observatory site, commenced screening of NAOJ’s
four-dimensional digital universe known as 4D2U. A rapid
increase of interest in celestial observations has been notedamong residents of Ishigakijima
Island, and coinciding with the opening of a new airport, theObservatory attracted 13,000 visitors this year, marking a 30 %increase over that in the previous year.
Collaboration with the Nayoro City Observatory is also
underway, where a 1.6-m telescope belonging to Hokkaido
University is installed. Officials have organized civic lectureson astronomy and other events jointly with “Gurukun-Juku,”a group of local people who follow a course at Japan’s Open

University. In response to the request, collaboration with
officials of local Chambers of Commerce and tourism in Ishigaki
city and Taketomi town is developing to leverage the night sky
in community revitalization.

3. Open Use/Joint Research(1) Open Use
The Observatory began to arrange a semiannual call foropen use in FY 2013. Nine proposals were made for a total of
458 hours of observation for the FY 2014 first half-period openuse 22- GHz, 43- GHz, and 6.7-GHz band observations. One
proposal for 88 hours was made from abroad. These proposals
were considered by a VLBI program subcommittee based on
judgments of referees selected from researchers in relevant fields
in Japan. Subsequently, they selected four proposals for a totalof 120 hours.
Observations commenced in January 2014.
Open use of the KaVA was also called for at the sametime for the first half-period of FY 2014, and 13 proposals
were received for a total of 477 hours. These proposals wereconsidered by referees from both VERA and the KVN and were
forwarded to the VERA/KVN joint time allocation committee
for assessment. Seven proposals were selected for a total of
240 hours, and the first observation started in February 2014.
Observational data produced through an open use of the KVN
will be correlated using the KJJVC installed at the Korea
Astronomy and Space Science Institute.
(2) Japanese VLBI Network
In tandem with observation via the Japanese VLBI Network,a joint research agreement was entered by Hokkaido University,
the University of Tsukuba, Gifu University, Yamaguchi
University, Kagoshima University, Ibaraki University, Osaka
Prefecture University, GSI, and NICT. This joint research isin progress. The Institute of Space and Astronautical Science(ISAS) at JAXA is also in a close collaborative relationship.
(3) Joint Research between Japan and Korea
Researchers in Japan and Korea engaged in science WGs for
AGN, star formation and late-type stars using KaVA. A generalscience WG was held twice in Korea for this purpose, in which
the KaVA project observation plan was developed. Furthermore,
KJJVC performance tests and evaluation of functions compatible
with various observational modes were jointly conducted for aregular operation of 1 Gbps and 16-station correlation.
(4) Joint Research
The joint research agreement with GSI provides for geodetic
VLBI observations (JADE observations) within Japan. A research
agreement with the Helmholtz Centre Potsdam GFZ German
Research Centre for Geosciences (GFZ–Potsdam) in Germany
is the basis of the GPS and Galileo satellite observations. The
data obtained through the GPS observations have been madepublic as International GPS Service (IGS) observational points.
The Esashi Earth Tides Station distributes strain meter data

II Status Reports of Research Activities069

and other information from the driftway in real time to relevant
research organizations as part of a research agreement with
the Earthquake Research Institute of the University of Tokyo.
Facilities are applied to open use in a broad sense of the term.

4. Public Relations (PR) and Awareness Promotion
Activities(1) Open house events
April 14: The fourth Open Observatory event (a special open
house event at the Ibaraki University Center for Astronomy andthe Ibaraki station of the Mizusawa VLBI Observatory, NAOJ)
was held with approximately 1,000 visitors.
July 7: NAOJ Mizusawa VLBI Observatory Kagoshima
station at Kinkowan Koen, Kagoshima City, held Tanabata
Matsuri in collaboration with the city of Kagoshima andKagoshima University, which featured a 6-m radio telescope.
Approximately 300 people attended.
August 10: The VERA Iriki station was opened to the public
as part of the Yaeyama Kogen Star Festival 2013 with more than
1,500 visitors in attendance.
August 3–18: The 2013 South Island Star Festival was held
simultaneously with a special open house of the VERA Ishigaki
station and the Ishigakijima Astronomical Observatory; thedimmed-light stargazing event received approximately 8,500
visitors. An astronomical observation party at the Ishigakijima
Astronomical Observatory was attended by 851 visitors, and a
special public opening of the VERA station had 246 visitors.
August 24: The Iwate Galaxy Festival 2013, a special open
house of the Mizusawa station, was held with nearly 3,000
visitors.
November 7–9: A special open house of the VERA
Ogasawara station, Star Island 2013, was held in conjunction
with JAXA Space Education Center for the first time andattracted 433 visitors during the three-day event.
February 16, 2014: The Ishigakijima Astronomical
Observatory entered into an exchange agreement with the
Nayoro City Observatory in Hokkaido.
(2) High School Student Hands-on Events
June 29–30: The Seventh Z Star Research Team event wasorganized to use the VERA Mizusawa station radio telescope,for which a preliminary session was held with five prospective
participants.
August 3–5: The Seventh Z Star Research Team event washeld for high school students in Iwate prefecture, including thosefrom the disaster-stricken areas. Five students participated anddiscovered new celestial objects successfully.
August 7–9: The VERA Ishigakijima station and the
Ishigakijima Astronomical Observatory held the Churaboshi Research Team workshop for high school students from
Okinawa and Fukushima prefectures with 21 attendees. One
group engaged in radio observation and discovered two newmaser objects for the first time in three years. Moreover, anothergroup undertook visible light observation using the Murikabushi
telescope and discovered five planetoids.

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The University of the Ryukyus and NAOJ began offering
this joint course in 2009; 2014 marks the program’s fifth
year. Classroom lectures at the university took place between
August 12 and 15, and observational workshops were held in
Ishigakijima from August 26 to 29 with a total of 32 participants.
A hands-on radio observation program was conducted at the
VERA observation station using a 20-m radio telescope. The
Murikabushi was also deployed to observe a nebula, andparticipants learned about image processing.
(3) Other
The Observatory contributed to extracurricular activities andworkplace visits offered to elementary and junior high school
students in Oshu City. It also provided hands-on workshops
for high school students from Iwate prefecture, Tokyo, andFukushima.
The Ishigakijima VERA station and Ishigakijima
Astronomical Observatory contributed to the education ofelementary, junior high, and high school students, as well as
tertiary education for elderly groups and women’s societies.
In addition to the commemorative lecture delivered by NAOJ
Director General Hayashiat the South Island Star Festival, alecture on astronomy was given by guest lecturer Yuko Kakazu
on March 30 near the Subaru Telescope at NAOJ. Other lecturesby request included a night sky workshop offered to tours fromthe Japanese Open University, the NHK Academy of Distance
Learning, and Sundai Gakuen Senior High School.
Observatory officials participated as panelists at the Starry
Sky Summit and gave a preliminary lecture on astronomy
organized at Bisei Astronomical Observatory. In addition, theObservatory offered internships to local high school students
and gave guided tours. Other public relations (PR)/awarenesspromotion activities included presentations and consultationsorganized for hotel and travel agencies, and members of tourism
associations in Ishigaki city and Taketomi town adopted “Stars
in the sky are brilliant resources for local tourism” as a thematic
slogan.

5. Timekeeping Office Operations
The Timekeeping Office operates four cesium atomic
clocks together with a hydrogen maser atomic clock at theMizusawa VERA station. The four cesium atomic clocks andthe timekeeping operation system were moved downstairs in
the main building last year into the underground atomic clock
room and the atomic clock management room, respectively.
No breakdown or other problems occurred as a result of the
move, and the facilities have been operating stably, contributing
to determine Coordinated Universal Time through continuous
management and operation of the time system. The beam tube
in the cesium clock Cs6 was replaced because it approaching
its warranty expiration. Moreover, changes were made to
the procedures for submitting comparative time data to theInternational Bureau of Weights and Measures (BIPM), whichkeeps the international atomic time (TAI). The NTP protocol
provides Japan Central Standard Time on a network. This

service has been in great demand; more than 900,000 daily visits
have been recorded this year.

6. Educational Activities
Regarding postgraduate education, the Observatory assisted
three graduate students each from the University of Tokyo and
the Graduate University for Advanced Studies. Two students,

one each from these universities, were conferred PhDs. One
master’s student from Tokai University was accepted as avisiting graduate student. Undergraduate students from the
University of Tokyo, Meisei University, and the Universityof the Ryukyus were accepted as summer students of the
Graduate University for Advanced Studies and received researchguidance. In addition, staff members at the station visited these
universities to deliver lectures.

6. Solar Observatory
The Solar Observatory primarily engages in the operationof solar observational facilities on the west side of the 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 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 the Mitaka campus, had continued theobservation of active region photospheric vector magnetic
fields and H-alpha 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 the solar surface, this instrument is designed
to perform full-disk polarimetric observation to obtain highaccuracy vector magnetic field information in order to shed lightupon the origins of the solar activity cycle. This polarimeter isequipped with a 15-cm infrared lens and performs slit scanningobservations using infrared spectral lines (photosphere: iron,1.56 μm line; chromosphere: helium, 1.08 μm line), which arehighly sensitive to the magnetic field. This allows for constantacquisition of unprecedented infrared polarization data of
the photosphere and chromosphere of the entire solar disk.
However, the infrared camera was damaged by lightning inAugust this year, and subsequent observation was suspended.
Although the repair required a considerable amount of time, thecamera’s condition currently has been sufficiently restored forresuming observation. An emergency replacement camera has
been installed to complement the system so that observation cancontinue in the event of camera failure.

(2) Regular Observation of Sunspots/Faculae/H-alpha Flares
Sunspot observations have been performed continually since1929. This observation is currently conducted via automatic
detection of sunspots on digital images captured with a 10-cm
refractor and a 2 k × 2 k pixel charge coupled device (CCD)
camera mounted on the new (full-disk) sunspot telescope.
Observations were conducted for 267 days in 2013, fromJanuary to December.
Although full-disk solar image data are a widely needed
resource in the astrophysics/geophysics community, someof these synoptic instruments are getting out of date. Efforts
are underway to update the photospheric and chromosphericimaging instruments and to further flesh out data. For instance,
the SFT has started advanced observations in the H-alpha line
to acquire full-disk, high-resolution images. It enables to obtain
Doppler velocity information based on imaging at multiple
wavelengths around H-alpha with high temporal resolution
allowing for more completely capturing active phenomena anda broad dynamic range by a combination of multiple exposure
times. This advancement has enabled us to observe many
phenomena in recent heightened solar activities such as flaresand prominence eruptions. The observatory also uses the SFT
to conduct regular imaging observation at the G-band (430nm) and continuum wavelengths. The regular observational
data described above, including real-time images, are available
on the website of the observatory. Using a Grant-in-Aid for
Scientific Research, a spectrograph system with a coelostat isunder development to perform long-term, full-disk observation,
including more quantitative velocity and magnetic fieldobservations. A laboratory for this project was set up this year.
The observatory maintains other existing equipment to allow
for everyday observation, as well as experimental use.

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
and those from nearly 100 years of various types of solar
observations. The various phenomena occurring in the solar–
terrestrial environment must be studied in terms of both sudden,
short-term events (space weather) and of gradual changes

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071

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 are of 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.
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
The Norikura Solar Observatory ceased operation in 2009,and its facilities were transferred to the NINS. However, theNorikura Green-line Imaging System (NOGIS) coronagraph,
which allows for advanced observations such as coronalvelocity field measurements, can be put to better use if it
is allowed to continue observations at a suitable location
overseas. Therefore, it is in the process of being transferred to
the Yunnan Astronomical Observatory in China. This year, theentire coronagraph, including the refurbished telescope tube,
was transferred to the Lijian (Gaomeigu) Observaotry, andtemporary installation has been completed. Closely following
this, a joint test observation between Japan and China took place
locally and produced good results. Staff on the Chinese side
are currently continuing test observations. Other international
cooperation includes support for the Japan–Peru collaborative
solar observations, with which the Solar Observatory has been
involved since 2004.
A research plus business conference, dubbed as the annual
users meeting, has been held every year jointly with otherorganizations. Beginning this year, however, the meeting is
combined with the solar research symposium for the entire solar
community, where topics in relation to open use and future plans
are also discussed. This year, the conference was held at Kyoto
University between February 17 and 19.
Because the observatory deals with fundamental solar data,
images in the solar observatory database are often used in school
textbooks. The observatory actively responded to approximately
20 applications for image use in FY 2013.
Regarding personnel transfers, Chief Engineer, Toshihiko
Kobiki, who was engaged part-time in work for the Chile
Observatory, has been transferred to the Chile Observatory fulltime due to increased workload there. Moreover, research expert
KentaroYaji replaced a staff member who departed last year, andIsao Suzuki departed upon completion of his term.

7. NAOJ Chile Observatory
The ALMA project involves a plan for operating a gigantic
radio telescope for receiving millimeter and submillimeter waves
by deploying 66 high-precision parabolic antennas in the 5,000-m
altitude Atacama highlands in northern Chile. This international
collaborative project includes East Asia, Europe, and North
America, and NAOJ plays the central role in the East Asian part.
ALMA is projected to have an observational resolution of nearly
ten times higher than that of the Subaru telescope or the Hubble
Space Telescope. Early scientific observations with ALMA
began in FY 2011 with some of the telescopes, and full operationcommenced in FY 2012. This report describes progress made in
the construction in Japan and for the entire project and includes
the progress of the scientific observations and other activities
such as public information and outreach initiatives. The ASTE
telescope is a single-dish 10-m submillimeter telescope installedin the Atacama highlands. It is operated to make headway
into submillimeter observations in the southern hemisphere inpreparation of the approaching ALMA era. The ASTE telescope
had been operated by the Nobeyama Radio Observatory until
FY 2011. In FY 2012, the operation was transferred to theChile Observatory to have an organic liaison with the ALMA
telescope. This report also describes progress regarding the
ASTE telescope.

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1. ALMA Project Progress(1) Overall progress
Construction of the ALMA telescope is in its final stage.
The 66th antenna was delivered to the Joint ALMA Observatory
in September 2013. A full-scale scientific observation began its
Cycle 1 in January 2013. The call for observation proposals for
Cycle 2, due to begin in June 2014, was closed on December 5,
2013, and the submitted proposals were given to the referees forconsideration.
The commissioning observations to be run concurrently withthe scientific observations have shown good progress. These
include an interferometer test via long baseline, test observations
using Band-4, Band-8, and Band-10 receivers developed inJapan, polarimetric observation tests, and solar observation tests.
In tandem with the inauguration ceremony held in Chilein March 2013, a special lecture event was organized in Japanat Hitotsubashi Hall, Tokyo, on May 15, 2013, to celebrate theinauguration. This event was attended by approximately 200
guests including members of the Japanese Diet, researchers,
and corporate representatives, who were all deeply involved in
the ALMA project. The memorial lecture delivered by Tetsuo
Hasegawa, Director of NAOJ Chile Observatory, was broadcast

via the Internet.
(2) Progress in development in JapanThe 16 antennas developed in Japan, including four 12-m
and twelve 7-m antennas, were delivered to the Joint ALMA
Observatory by the end of FY 2012. These antennas have been
installed at the AOS at an altitude of 5,000 m and were deployedin testing and scientific observations.
Fabrication of the Band-4, Band-8, and Band-10 receivers
was completed in FY 2013, and the receivers were shipped to
Chile. The Band-8 and Band-10 receivers successfully obtained
their first interferometer images in September 2013 and February
2014, respectively. These receivers are currently deployed in
test observations. Cycle 2, due to commence in June 2014, isscheduled to employ the Band-4 and Band-8 receivers for openuse observations.

2. ALMA Open-Use and Scientific Observation
The second round of open-use observations of the ALMA
telescope commenced in January 2013 for Cycle 1. The details
of Cycle 1 include interferometric observations using at least
thirty-two 12-m parabolic antennas with a maximum baselineof 1 km, Atacama Compact Array (ACA) observations, andfour frequency bands (Band-3, -6, -7, and -9), in addition to a
maximum of 150 fields of view for mosaic observation. The
ACA observations are interferometric observations using at leastnine 7-m parabolic antennas and single-dish observations using
at least two 12-m antennas. Several impediments followed thestart of the open-use observations such as inclement weather,technical troubles in the local infrastructure including power
outages, and a labor strike by the local staff; thus, the numberof observations conducted was very low until September 2013.
These adverse conditions considerably delayed the completionof Cycle 1, which ended in May 2014 rather than the scheduled
date of October 2013. Cycle 1 reached a completion rate of only
60 % at the time of its termination. Therefore, it was decided thatapproved but uncompleted observation programs were carriedover to Cycle 2.
An open call for the third round of open-use observations
was issued for Cycle 2. The details of Cycle 2 as advertised
include interferometric observations using at least thirtyfour 12-m parabolic antennas with a maximum baseline of
1.5 km, ACA observations, six frequency bands (Band-3, -4,-6, -7, -8, and -9), and a maximum of 150 fields of view formosaic, and polarimetric observation. Before the public call
was closed at 00:00 JST on December 5, 2013, 1,381 proposals
were submitted, 273 of which were from East Asia. Scientificevaluation of the observation proposals took place between
March 10 and 14, 2014, in London, Ontario. Proposals werereviewed by 78 science assessors, 17 of whom were from East
Asia. Of the 1,381 proposals, 353 were designated as “highest
priority.” Of these 353 proposals, 83 (23.5 %) were from East
Asia, and the proportion of observation time allocated for East
Asian projects was 22.3 %. Cycle 2 is scheduled to commence inJune 2014.

ALMA open use has produced a number of scientificachievements. Those focusing mainly on East Asian projects
are described below. Nami Sakai of the University of Tokyoand others conducted an observation of a young protostar in the
Taurus constellation L1527 and made the world’s first discovery
of a centrifugal barrier creating a ring-shaped shocked region
formed in the protoplanetary disk. Misato Fukagawa of Osaka
University and her team observed a young star known as HD
142527 in the constellation Lupus, and they identified the dust
continuum, potential planetary components, and formation of anasymmetrical ring of protoplanetary disks around the star. Thisconvincing evidence of planet-formation occurring far from its
primary star was captured successfully for the first time ever.
Lai Shih-Ping of the National Tsing Hua University in Taiwan
and her team discovered the youngest protoplanetary disk everobserved. Takeshi Sakai and others of the University of ElectroCommunications observed an infrared dark cloud in the Aquila
to discover a high-temperature molecular cloud, known as a Hot
Core, that was 10 times larger in size than those conventionallyreported. Masami Ouchi of the University of Tokyo and others
conducted an observation of the early cosmic giant blob Himikoby using ALMA and the Hubble Space Telescope. With the latter,they discovered three giant blue galaxies. With ALMA, they
confirmed that no radio wave was detected in fine solid particles(dust) or atomic carbons. Their observation led to the suggestionthat Himiko is highly likely in a very early phase of galaxy
formation because it is composed mainly of primitive hydrogenand helium gases. Takuma Izumi and others of the University ofTokyo observed dense gas surrounding the active, giant nucleus
of NGC 1097 and reported that the high volume of HCN aroundthe AGN is due to the high temperature of the environment
under the influence of a black hole. Bunyo Hatsukade of Kyoto
University and his team successfully detected 15 new, extremely
dark galaxies, revealing that nearly 80 % of hitherto unidentified
millimeter waves from the Universe originated in dust particles
in faint galaxies.

3. Educational Activities and Internship
The Chile Observatory held a graduate school guidance
session on June 15, 2013. Four undergraduate students attended
the session, engaging in lectures given by teachers andsocializing with current graduate students.

4. Public Outreach Activities
In May 2013, the Chile Observatory hosted a week-long
ALMA booth at the Japanese Geoscience Union Meeting. Civic
lectures and a Science Cafe were organized on 17 occasions in
FY 2013 to communicate ALMA’s current activities to numerous
visitors through conversation and to popularize ALMA and its
results.
The project website published 47 news articles and sevenpress releases. A mailing-list-based newsletter also continues ona monthly basis with approximately 2,500 subscribers. Updated,detailed information is available on Twitter (@ALMA_Japan),

II Status Reports of Research Activities

073

with nearly 16,300 followers as of the end of FY 2013.
Approximately 60 newspaper/journal articles were posted,reporting scientific discoveries from the Early Scienceobservations. ALMA was featured in television programs 14
times. In addition to news reports on ALMA’s observational
achievements, composite programs such as “Tanken Bakumon”
on Nippon Housou Kyoukai (NHK) and “Yume no Tobira+”(“Gates to Dream”) on Tokyo Broadcasting System (TBS)featured ALMA as the main topic, introducing the project
in depth and showing people involved in its operation. Suchprograms effectively conveyed ALMA’s virtues to a massaudience.
As part of the construction film project continuing since FY
2003, the observatory produced two films that were screened in
FY 2013: film footage of the inauguration ceremony in Chile anda promotional film recorded in 2011 that shows the development
processes of the ALMA antennas. The development of thereceivers at the Advanced Technology Center (ATC) was also
filmed together with developer interviews.
The series “Bienvenido a ALMA,” in which ALMA staff
members discuss their work, continues to be featured in the
NAOJ newsletter, which is also published on the ALMA
website.
ACA, which was developed by Japan, was awarded a2013 Good Design Gold Award, endorsed by the Ministry of
Economy, Trade and Industry of Japan. Replicas of a band-10
receiver and a superconductor-insulator-superconductor (SIS)
receiver, together with description panels, were displayed at
the Good Design Exhibition 2014 held from October 30 toNovember 4 at Tokyo Midtown in Tokyo. As a Good DesignAward candidate institute, we delivered a speech at thedesigners’ presentations held at the event venue.

5. International Collaboration (committees, etc.)
Various committees are frequently organized forinternational collaboration in the ALMA project. The ALMA
board has met twice, and the ALMA Scientific Advisory
Committee was summoned three times in FY 2013. In addition,
teleconferences been conducted for both groups on a nearmonthly basis. Moreover, the ALMA Annual External Review
met over the course of one week in October 2013, and the
ALMA East Asian Scientific Advisory Committee has also
conducted teleconferences nearly each month. To maintainclose communication in implementing the international project,meetings and teleconferences are held more frequently for
individual areas of concern.

6. Workshops and Town Meetings• July 8-9, 2013 NAOJ Mitaka
East Asian (EA) ALMA Development Workshop• September 24, 2013 Ehime University
ALMA Cycle 2 Town Meeting• September 24, 2013 JAXA/ISAS
ALMA Cycle 2 Town Meeting074

II Status Reports of Research Activities• September 26, 2013 Kagoshima University
ALMA Cycle 2 Town Meeting• October 3, 2013 University of Tokyo Institute for Cosmic
Ray Research/Institute for the Physics andMathematics of the Universe (IPMU)
ALMA Cycle 2 Town Meeting• October 2, 2013 Nagoya University
ALMA Cycle 2 Town Meeting• October 3, 2013 Kyoto University
ALMA Cycle 2 Town Meeting• October 7, 2013 Hiroshima University
ALMA Cycle 2 Town Meeting• October 9, 2013 Tohoku University
ALMA Cycle 2 Town Meeting• October 9-10, 2013 NAOJ Subaru Telescope
ALMA Cycle 2 Town Meeting• October 17, 2013 Osaka Prefecture University
ALMA Cycle 2 Town Meeting• October 28, 2013 KASI, South Korea
ALMA Cycle 2 Town Meeting• October 30, 2013 Hokkaido University
ALMA Cycle 2 Town Meeting• November 18, 2013 NAOJ Mitaka
ALMA Cycle 2 Town Meeting (first session)• November 22, 2013 NAOJ Mitaka
ALMA Cycle 2 Town Meeting (second session)

7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research including
Industry-University Collaboration Expenses
Kiuchi, Hitoshi; Ministry of Internal Affairs andCommunications (SCOPE): R&D of chromatic dispersion
compensation using round-trip phase measurement

8. Research Staff Changes(1) Hired
Rie Miura: project assistant researcher
James Chibueze: project assistant researcher
Cinthya Herrera: project assistant researcher
Yiping Ao: project assistant researcher(2) Departed or transferred
Hiroshi Nagai: postdoctoral fellow, transferred to the Chile
Observatory to assume the position of project assistant professor
Eiji Akiyama: postdoctoral fellow, transferred to the Chile
Observatory to assume the position of a project assistantprofessor

9. Main Visitors
May 1-3, 2013
Mr. Akito Arima, a former Minister of Education of Japan,
visited the ALMA Operations Support Facility, Array Operations
Site, and JAO (Joint ALMA Office) Santiago Central Office.

10. Progress of ASTE telescope
The ASTE telescope is designed to promote full-fledged
submillimeter astronomical research in the southern hemisphereand to develop/verify observational equipment and support
methods. With the ALMA construction entering its final stages
and early science observations successfully beginning, the ASTE
telescope will be engaged mainly to provide observational
evidence for strengthening ALMA observation proposals.
Development will be pursued for extension of ALMA’s future
performance.
A public call was made in FY 2013 for open-use observation
proposals for spectroscopic observations in the 345-GHz bandwith the goal of making the astronomical community moreaccessible. To render support for researchers contributing tothe observational performance enhancement for the ASTE
telescope, the Guaranteed Time Observation (GTO) scheme
was established, which allowed these researchers to offer

suggestions. When the application call was closed on June 10,2013, 47 proposals for open-use observations and GTO slots had
been made including 39 for open use and eight for GTO. These
proposals were considered by officials at the Chile Observatory,
and 21 proposals were subsequently adopted including 13
for open use and eight for GTO. Two proposals intended for
GTO had to be canceled due to facility breakdown. Open-use
observation was conducted from the ASTE Mitaka operation
room between August 19 and October 7, 2013.
A group of researchers from the University of Tokyo andthe University of Electro-Communications conducted a test
observation using the 0.9/1.5-THz receivers for one month in
October 2013. Finally, a group led by the Nobeyama Radio
Observatory, the University of Tokyo, and Hokkaido University
conducted a test observation of the 270/350-GHz band TES
bolometer camera from November 2013 through April 2014 inpreparation for its release for open-use observations due to begin
in 2015.

8. Center for Computational Astrophysics
1. Overview
The Center for Computational Astrophysics (CfCA)
carried out the management of a group of open-use simulation
computers centered around a general-purpose supercomputer
and the special purpose computer for gravitational N-bodyproblems; implementation of new open-use computer systems;
research and development for computational astrophysics
applications; and promotional activities for astronomical
numerical simulation and their results. The supercomputer was
updated this year. The new supercomputer that is installed at
the Mizusawa VLBI Observatory, Cray XC30 (as known as
ATERUI), is endowed with the world’s highest computational
capacity for supercomputers for astronomy at 500 Tflops.
The center also continued operation of other computerssuch as GRAPE-7 and GRAPE-DR, which are dedicated forgravitational N-body problems, in addition to servers including
small-scale computational PC clusters. Efforts in visualizing
astronomical data also continue.

2. Open Use(1) Computer Systems
This year marked the first usage of the upgradedastronomical simulation system, which includes the mainsupercomputers of the open-use computers for this project.
Circumstances necessitated this system to be installed at
the Mizusawa VLBI Observatory. Thus, the Cray XC30
with theoretical peak performance of more than 500 Tflops
was introduced with partial support by the Mizusawa VLBI
Observatory. This system realized a performance improvementof approximately 20-fold over the systems operated for thesame purpose until last year. With the dedicated work of all
involved, difficult tasks of system upgrade and installation at
the Mizusawa VLBI Observatory were successfully completed,and the new equipment has performed with no major issues,enabling its users to make academically significant progress.
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 by researchersin Japan and overseas. In particular, the GRAPE system, also
known as the Mitaka Underground Vineyard (MUV) system),is promoted for its effective open use. The center undertook
development, improvement, and maintenance for both hardware
and software for the system this year. One of the major events ofthis year was the test operation of GRAPE-9. This system has aperformance improvement of roughly 10-fold over 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 2012 on studies that involved the
project’s open-use computers. It was revealed that 82 such
papers were published.
Drupal, a content management system introduced for data

II Status Reports of Research Activities

075exchange with users of open-use computers, is presently used
for providing information and transmitting various application
forms as necessary. The periodical “CfCA News” is anadditional channel of information dissemination. The center
leverages this newsletter to inform people of all useful andnecessary information regarding the computer system. A subsidy
system for publishing and advertising is continuing this year for
research papers in which the results were obtained by using thecenter’s computers. Although no case was adopted in FY 2012
for payout in FY 2013, three papers were accepted in FY 2013
for payout in the same year at approximately 250,000 JPY.
□ Statistics on Cray XC30
Operating hours- Annual operating hours: 8506.8- Annual core operating ratio: 84.83 %Users- Category S: 3 adopted in the first term, 0 in the second term;
total 3- Category A: 11 adopted at the beginning of the year, 2 in thesecond term; total 13- Category B: 60 adopted at the beginning of the year, 4 in thesecond term; total 64- Category D: 10 adopted at the beginning of the year, 2 in thesecond term; total 12- Category Trial: 32, year total- Category I: 1, year total□ Statistics on the GRAPE system
Users- Category A: 4 adopted at the beginning of the year, 1 in thesecond term; total 5- Category B: 5 adopted at the beginning of the year, 0 in thesecond term; total 5- Category Trial: 2, year total□ Statistics on the PC cluster
Operating hours- Annual operating hours: 7117.0- Annual job operating ratio: 75.7 %- Total users: 34, year total(2) Tutorials and Users Meeting
The center organized various lectures and workshops
to provide the users of the open-use computer system witheducational and promotional opportunities, as well as to train
young researchers. The details are shown below. In addition, ausers meeting was held to serve as a forum for direct informationexchange. Many participated in the meeting, and discussions
were fruitful.
□ Cray XC30 system workshop: April 16, 2013, 43 attendees□ Cray XC30 workshop for intermediate users: June 27, 2013,27 attendees□ Cray XC30 optimization seminar: October 31, 2013, 7
attendees

076

II Status Reports of Research Activities□ N-body simulation Winter School: January 15–17, 2014, 18
attendees□ Users meeting: January 28–29, 2014, 47 attendees

3. PR Activities
In tandem with the commencement of open use of the Cray
XC30 ATERUI, press conferences were held at the Mizusawa
VLBI Observatory (May 27, 2013, Iwate prefecture) and the
National Institute of Informatics (May 29, 2013, Tokyo). The
events were broadcasted on two local television stations andwere featured in the “Space News” program on TV Tokyo.
Many other media outlets also reported the news, including“Asahi” and “Yomiuri” newspapers, other local newspapers,
and the astronomy journal “Hoshi Navi.” The CfCA took
part in the special open house event of the Mizusawa VLBI
Observatory, Iwate Galaxy Festival 2013, held on August 24
this year. About 600 visitors attended a guided tour of the
ATERUI and experienced a close-up observation of the facility.
Lectures were also organized at the Oshu Space and Astronomy
Museum, also known as Yugakukan, to coincide with the event.
In addition, Assistant Professor Takashi Ito, spoke on numericalsimulations for astronomy, and Assistant Professor Tomoya
Takiwaki, spoke on research of supernova explosions simulatedusing the ATERUI. These occasions in this event were featured
on local television and in newspapers, constituting considerable
coverage with vibrant local enthusiasm. The ATERUI was also
introduced to people visiting the Nobeyama campus for its open
house event on the same day by using live broadcasting via
Mizusawa’s supercomputer operation room.
At the Mitaka open house event held in October 2013, theCfCA made the computer room accessible to the public andprovided an informative project on simulation astronomy withcommentaries about the GRAPE and the PC cluster. A live
broadcast was also arranged by connecting the supercomputer
operation room of the Mizusawa VLBI Observatory to the
Mitaka campus to introduce the ATERUI to those visiting
Mitaka. The CfCA has begun to accept group tours of their
computer room in the Mitaka campus, in which visitors are
given explanations of the GRAPE and the PC cluster in the mainroom. In preparation for press release articles, support has been
given on the results gained from open-use projects. The CfCA
published a web release about a research using the PC cluster
in November 2013. Titled “Crowding Out of Giants by Dwarfs:
an Origin for the Lack of Companion Planets in Hot Jupiter
Systems,” the study was conducted by Masahiro Ogihara,
postdoctoral fellow from Nagoya University. Moreover, aTwitter account was created for the CfCA (@CfCA_NAOJ)
as part of the PR activities, and news on research results,
lecture informations, media appearances, and other topics are
disseminated through this channel.

4. 4D2U ProjectThe 4D2U project continued content development this year.
A movie on simulation titled “Electromagnetic Radiation from

Neutron Star Mergers” was released on the website in March
2014. For the four-dimensional digital universe viewer, “Mitaka,”
a new feature was developed to display comets in response tohigh user demand, although the viewer itself did not undergo aversion update. The Starry Sky Educational Room was launchedat the Ishigakijima Astronomical Observatory in July 2013, forwhich the 4D2U project provided all compatible 4D2U contents.
The 4D2U demonstration using the dispatch system wasconducted at the VERA Ogasawara station for its open house
event. Local residents who visited the station on this occasion
enjoyed a special program to experience the latest astronomy
findings through stereoscopic vision. The 4D2U contents werealso provided to the Science Hills Komatsu (Komatsu city,
Ishikawa prefecture), where a stereoscopic dome projection
system was recently installed. This installation is the fourthof its kind in Japan. The management of regular and group
screenings of the 4D2U Dome Theater has moved to the Public
Relations Center this year, and the 4D2U project has begun
a discussion on a new dome projection system. In particular,a stereoscopic system using active shutter was discussed as apossible practical application because its projection is brighter
than that of the stereoscopic spectroscopy currently used in
the Dome Theater. This measure to upgrade the system of theDome Theater in the latter half of this year was discussed with
the Public Relations Center. Moreover, a Twitter account was
created for the 4D2U (@4d2u) as part of the PR activities. The
information disseminated through this channel includes regular
screening enrollments, events featuring 4D2U contents, andmedia appearances.

5. External Activities(1) Joint Institute for Computational Fundamental Science
The Joint Institute for Computational Fundamental Science(JICFuS) is an inter-organizational institute establishedin February 2009 as a collaboration base between threeorganizations such as the Center for Computational Sciences(CCS) of the University of Tsukuba, the High Energy
Accelerator Research Organization, known as KEK, and the
NAOJ to provide active support for computational scientificresearch. The CfCA forms the core of NAOJ’s contribution
to the JICFuS. In particular, the institute engages primarily
in computer-aided theoretical research into the fundamental
physics in the elementary particle physics, nuclear physics, andastrophysics. The scientific goal of the institute is to promote
fundamental research based on computational science byencouraging 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 theircommunity to provide considerate and rigorous support to thepresent and future researchers. Another important mission of
the institute is to provide researchers around Japan with advice
regarding efficient supercomputer use and the high-performancecomputing development of novel algorithms to meet researchgoals from the perspective of computer specialists.

In FY 2013, Hiroyuki Takahashi and Tomoya Takiwaki
were engaged as project assistant professors to implement
research plans. Takahashi newly developed a plasma
simulation code to solve basic equations of relativistic radiation
magnetohydrodynamics (MHD) based on the first principle.
By performing the global simulations of black hole accretion
disks, he revealed that the black holes are able to rapidly growup via mass accretion. This is closely related the unresolved
issue in astrophysics: how the stellar mass black holes grow to
the supermassive black holes. Takiwaki carried on the threedimensional simulations of core-collapse supernovae using
the supercomputer “K.” His research is key for various studies
within the framework of the JICFuS because supernovae areclosely related to elementary particle and nuclear physics.
Although the mechanism of supernova explosions is a longstanding enigma that has been debated problem for more than 60
years, the research of the supernovae is considerably progressedby numerical simulations with most realistic setting using
supercomputer K.
Representing the CfCA, Professor Kohji Tomisaka andAssistant Professor Ken Ohsuga of the NAOJ participate inbimonthly JICFuS steering committee meetings to engage
in deliberations on spurring computational science-based
developments in astrophysics research through discussions
with other committee members who specialize in nuclear andelementary particle physics.
(2) HPCI Consortium
As a participant in the government-led High-Performance
Computing Infrastructure (HPCI) project since its planningstage in FY 2010, the center has engaged in the promotion of
the HPC research field in Japan, centering on the use of thenational K supercomputer. Although the center is involved with
the JICFuS-led HPCI Strategic Program Field 5 as mentionedin (1), the 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 devoidof voting rights as well as the obligation to pay membershipfees. Continuing from last year, a number of conferences and
WGs have been held in which participants discuss a nextgeneration national supercomputing framework to follow the K.
At present, discussions are underway about a plan to replace a
set of multiple large-scale systems serving as the second layer in
addition to adoption of a top-level national system like K within
five or six years. The approval of the Ministry of Education,
Culture, Sports, Science, and Technology (MEXT) was givenby the end of the year to allocate a budget for the developmentof a next-generation system. Post-K generation equipment isscheduled to commence operation after FY 2019. In principle,
therefore, it is possible for the NAOJ to play a central role in the
post-K generation HPC through participation in this discourse.

II Status Reports of Research Activities077

6. Contract Staff Transfers
The following staff members were hired on a contract basis in
FY 2013.
Research experts : Jin Matsumoto, Shigeru Wakita, and Yayoi
Narazaki
Research associates: Yuya Ariyoshi, Taira Oogi, and Hinako
Fukushi

The following contract staff members departed in FY 2013.
Research experts: Jin Matsumoto, Shigeru Wakita, and Yayoi
Narazaki
Postdoctoral fellow: Akihiro Suzuki
Research associates: Yuya Ariyoshi and Taira Oogi

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). The NAOJ has been
implemented this satellite project under a joint research
agreement with the ISAS/JAXA. A major theme of the scientificgoals of the Hinode satellite is to shed light on the coronalheating mechanism through a more multifaceted understandingof magnetohydrodynamic MHD phenomena occurring in thesolar atmosphere.
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 fromthe ISAS/JAXA. The SOT was developed mainly by the NAOJ,
and the focal plane package (FPP) was developed by the US
National Aeronautics and Space Administration (NASA) and
Lockheed Martin.
With regard to the XRT, NASA and the Smithsonian
Astrophysical Observatory (SAO) are responsible for the
optics system and frame, and Japan (ISAS/JAXA, NAOJ) is
responsible for the focal plane camera. The EIS is the resultof an even broader international cooperation. The structureand electrical system were developed by the UK Science andTechnology Facilities Council (STFC) and University College
London; the optics system was developed by NASA and theNaval Research Laboratory (NRL); and the University of Osloin Norway assisted with the terrestrial testing equipment and
the Quick Look system. The NAOJ actively participated in
the development of EIS/satellite interface, satellite integration
testing, and launch experiments. After a successful launch, the
NAOJ has continued its active involvement by acting as themain institution for collecting and analyzing data acquired by
the satellite.
The Hinode Science Working Group (SWG), composedof representatives from the international team, offers support
in scientific operation and data analysis. Together with two
members from the European Space Agency (ESA), the WG has

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II Status Reports of Research Activities

a total of 15 members, including three from the Hinode Science
Center (HSC) such as Sakurai, chairman from November/project
scientist; Suematsu, SOT; 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) andSekii (SOT).
FY 2013 marks the seventh year since the satellite’s launch.
Extremely good evaluations were received from the evaluationcommittees of a senior review class held at respective space
agencies during FY 2012–2013. These accolades made it
possible for the satellite to continue operation for the next
few years at the current operational level. The operation of
the Focused Mode will commence in FY 2014. A test run was
conducted 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 as andan effective aperture of 50 cm without atmospheric seeing. The
focal plane package consists of three types of optics systems
and imaging functions for maintaining the desired performancelevel. Operational modifications have enabled the maintenanceof a sound field of view even in the narrow band filter imager
system, in which image degradation was detected initially in partof the field of view.
The XRT has the capacity of capturing the solar coronalplasma via soft X-rays. The telescope has inherited the grazing
incidence optics system and has improved in spatial resolution.
Its wavelength characteristics have been improved to allow
for observation of the solar coronal plasma over a broader
temperature range. Resolution is close to 1 as. Calibration is
now possible for temporal variations in spectral characteristics
due to surface contamination on the detector, and the telescopeis available for analysis via its spectral characteristics. The
EIS obtains temperatures, densities, and velocities of thechromosphere, transition region, and coronal plasma thoroughthe 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 observation from the chromosphere and the transition region,
located between the photosphere and the corona, to the corona.
A mission data processor (MDP) was installed to manage
observations and to acquire data via the three telescopes. The
coordinated observation using the three telescopes is 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 is primarily downlinked
at the Kagoshima station (USC) and at Norway’s Svalsat
station through collaboration with the ESA, allowing for dataacquisition for every orbit. Scientific operation was again
performed in FY 2013 via S-band data reception. The S-band
reception frequency was increased with help from the ESA and
NASA, allowing for continuation of regular, stable scientificoperation.
Obtained data is collected at the 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 243 days in FY 2013, 70 days of which were for contracted
work. Moreover, the contribution rates to the scientific operationof the HSC were 27.8 % (domestic) and 16.8 % (overall).
Instantaneous publication of all data acquired by Hinode began
on May 27, 2007, with stable continuation, implemented by the
HSC.
Calls for Hinode Operation Plans (HOP), which encourages
proposals for open-use observation together with other satellites
and terrestrial observational equipment, promotes joint
observations among solar researchers worldwide. As of March
2014, 254 applications have been received. In particular, core
HOP proposals made by members of the scientific instrument
team became refined over multiple implementations, andsystematic observations have yielded extensive results that canbe amplified to studies on solar activity cycles.

2. Hinode Satellite Data Analysis
The NAOJ HSC aims to construct an analytical environmentand database for scientific analysis of data from the Hinodesatellite 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 the scientific outputs gained from the Hinodesatellite by providing a suitable environment for analyzing thesatellite data, facilitating access to Hinode observational databy distributing the analyzed data, and constructing a data searchsystem.
As part of its educational and public outreach (E/PO)

activities, the HSC also uses the latest observational data toraise 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 2013, HSC staff members and students published 18
peer-reviewed papers related to Hinode, bringing the total to
227 papers by the end of March 2014. Cumulatively, 725 peerreviewed papers have been published on Hinode-related topics.
Publications of papers in this category continue at a pace ofnearly 100 papers per year 7 1/2 years after the satellite’s launch.

3. Deliberations on the Solar-C Project
In April 2013, the sub-project Solar-C Planning Office,headed by Hara, was promoted to the Solar-C Project Office(A-project, also headed by Hara). Details of its activities aredescribed in the office’s own report.

4. Other Activities
In FY 2013, four postdoctoral fellows were engaged as
members of the HSC including one project assistant professor,
one project assistant researcher, one postdoctoral fellow, and
one Japan Society for the Promotion of Science (JSPS) fellow.
Hinode Science Meetings for Japanese and international solar
researchers are held on a regular basis to promote heliophysicalresearch using the Hinode scientific satellite. The seventhmeeting took place between November 12 and 15, 2013, in thecity of Takayama, Gifu prefecture. The Hida Observatory of
Kyoto University’s School of Science was a co-organizer.
In addition to the aforementioned activities, HSC researchand educational staff members have presented scientificobservation results at numerous symposia of solar-related
subjects either by invitation or by active participation. The
HSC has also invited international researchers to engage incollaborative research. The following researchers have visitedthe center from overseas on a long-term stay of at least one
month:
Name
Eric Priest
Bruce Lites
Robert Cameron

Organization (Country)
University of St. Andrews (UK)High Altitude Observatory (USA)Max Planck Institute for Solar System
Research (Germany)

Table 1. Long-term Visitors.

II Status Reports of Research Activities079

10. Gravitational Wave Project Office
1. Research(1) Development of KAGRA
1) Introduction
The activity of the gravitational wave project office isfocused on the realization of the KAGRA project. KAGRA isa gravitational wave detector based on a laser interferometerwith arms 3 km in length. It is currently under construction in
the Kamioka mine (Gifu prefecture). At the end of FY 2013 theexcavation of the tunnels and caverns that will host the detector,
an important milestone for the project, had been completed (seeFig. 1). In parallel, most of the vacuum envelope and cryostats
have been built and their installation will be one of the main
activities in FY 2014. The completion of iKAGRA and a shortobservation run will be the main milestones in FY 2015.
At NAOJ the activity was focused on the design, prototyping
and tests of the components for the vibration isolation system,
the auxiliary optics system and the mirror characterization. The
GW project office is also involved in the project management
through the system engineering office and the executive office.
In addition the team has been contributing in the field of safety,
public relations and project publications control.
2) Vibration isolation
The vibration isolation is a very important system forthe success of KAGRA. It should provide the seismic noise
attenuation in the detection band and should reduce the mirror
speed at low frequencies. It consists of several components
including the pre-isolator, the mechanical filters based on thegeometric anti-spring filter, and the so called “payload”, which
includes the mirror and all the components required for its
suspension and control.
During FY 2013 the prototype of the “payload” wasassembled and it was tested in the 20 m lab. The test of one of
the KAGRA vibration isolation chains was started at TAMA.
A frame around one of the TAMA vacuum chambers was built
and tested for this purpose. The prototype of the pre-isolator

Figure 1: Picture of one of the KAGRA tunnels. The KAGRA tunnels
excavation was completed in FY 2013.

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II Status Reports of Research Activities

was also moved to TAMA and its installation will start soon.
In parallel the prototype of one of the mechanical filters, theso-called bottom filter, was successfully built thanks to a very
effective collaboration with ATC.
3) Auxiliary optics system
The Auxiliary Optics Subsystem (AOS) consists of several
kinds of optics including the baffles and beam dumps for straylight mitigation, the beam reducing telescopes, the high quality
viewports and the optical local sensors (optical lever) for
measuring the interferometer mirrors positions.
The optical simulations to estimate the stray-light noisewith the designed optical baffle system in the arm cavities havebeen completed and the performance was estimated to fulfill
the KAGRAʼs requirement. One of the large baffles (400 mm
diameter) should be installed in a cryostat (20 K); the structure
to support such a baffle was studied. The 250 baffles for the arm-ducts, which will be installed along with 3-km arm ducts in2014, were all delivered to the Kamioka site as planned.
The beam reducing telescope will sense the tilts of thesapphire mirrors for the 3-km arms and it is indispensablefor the long-term stability of the interferometer operation. Its
conceptual design effort is ongoing.
4) Mirror development
Development of coatings for KAGRA optics is progressing.
The scattering loss of the last coatings were as small as 8 ppm.
This value is only a factor of two from the best levels in theworld. Power tolerance of the coating reached to 446 J/cm2. To
our knowledge, this value is the best ever for laser wavelength of1064 nm. The mirrors for the pre-mode-cleaner were delivered
to the KAGRA project and will be tested soon.
(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. The multi-messenger means collaborative observation
with infra-red light, neutrino, gamma-ray and X-ray detectors.
The group aims to survey KAGRA detector noises and to reduce
the false alarm rate of the detector.
2) Theoretical research on General Relativity
General-relativistic higher-order perturbation theories
have very wide applications in cosmology, black hole, andgravitational waves. In spite of these many applications, the“gauge issue” in general-relativistic perturbations is a delicate
problem. Therefore, it has been discussed in the framework ofgeneral-relativistic higher-order gauge-invariant perturbation
theory from a general point of view. In 2013, a full paper waspublished showing that the general framework developed by Dr.
Kouji Nakamura is applicable to perturbations on an arbitrary
background space-time.
(3) R&D
1) R&D for upgrades of KAGRATAMA is one of the core laboratories where R&D withexcellent interferometric sensors and controls can be conducted.
Among other features, the long optical cavities of 10 m and
300 m long are especially valuable. To make maximum useof it, a filter cavity experiment was planned. The key item ofthis experiment is high-quality (ultra-low loss) mirrors. In
the last couple of years, such mirrors have been developed incollaboration with Sigma Koki in Japan as described in theprevious section, and further studies are in progress now. If
is filter cavity with squeezed vacuum light is introduced to
KAGRA, event rates of not only double neutron stars binary
coalescences but also double black-holes binaries will increaseby factor of 10. In parallel, a proposal to develop crystalline
coatings for low loss mirrors was submitted to JSPS andapproved.
2) DECIGO/DPF
Following the change of JAXA’s concept for the small
scientific satellite series, we revised our plan for DECIGO/
DPF. The mission’s main goals were changed slightly so that themain objective of DPF will be to test several key technologies
like drag-free flight, stabilized laser source in space, andinterferometric displacement sensor in space as a precursor to
DECIGO, rather than a gravimeter for the geophysical purposes.
With these changes, we have submitted our proposal of DPF to
JAXA.
At NAOJ we are developing the interferometric sensor.
In FY 2013 a test bench to simulate free-falling test masses insome degrees of freedom by means of a torsion pendulum wasrealized. According to our evaluations, the main force noise on
the interferometer test masses will be caused by residual gases.
By finite element analysis, we designed a housing box aroundthe test mass to mitigate this noise

2. Education
The gravitational wave project office contributed to theteaching of general relativity and gravitational waves at
SOKENDAI. We also contributed to the teaching of “Fluid
mechanics and the group motion model” at Hosei University.
The office supported the SOKENDAI Asian winter schoolon Astrophysics with a lecture on Gravitational Waves research
and a visit of the TAMA facility. Many students visited the
TAMA facility: during FY 2013 we received 173 university
students and 181 high school students.
One graduate student from SOKENDAI and one
undergraduate student from Ochanomizu University did theirresearch projects in our office. We are encouraging NAOJ tostart an internship program to attract more students from abroadin general and from other Asian countries in particular.

3. Publications, presentations and workshops
organization
The office members were authors of 12 publications on
international journals and of 13 presentations to international
conferences. 59 presentations were also given to conferences inJapan.
During FY 2013 we started the organization of the 6th
Korea-Japan workshop that will take place at NAOJ on Junethe 20th and 21st, 2014. We also contributed to the organizationof the Gravitational Wave Advanced Detector Workshop that is
took place in Takayama in May 2014.

4. Outreach
The gravitational wave project office contributed to a special
issue of the NAOJ news devoted to gravitational wave researchthat was published on March 2013. The office contributed to
the NAOJ open days on October by opening the TAMA facility
to the public. Visits of the TAMA facility were also given
to officials from MEXT, from the Space Telescope Science
Institute and from the Italian Embassy. Finally a press release
was issued jointly with ICRR and KEK when the KAGRA
tunnel excavation was completed.

5. Relationships with industry
We have been supporting the development of techniques forultra-high quality optics by collaborating with a few Japanesecompanies. In particular work was done in collaboration with
Sigma Koki. The company is aiming at improving the polishingof substrates and the quality of coatings. The NAOJ mirror
group evaluate coatings qualities, and the results are fed back to
the process.

6. Personnel
At the beginning of FY 2013 the project had a total of 12
personnel including one affiliated associate professor, fiveassistant professors (two of which were on secondment to
ICRR), three engineers, two administrators (shared with the
Jasmine project) and one postdoc plus 2 students. During theyear, one professor and two postdocs joined the team. One of the
postdocs left for a permanent position at the end of February andanother arrived at the end of his contract at the end of March.
One of the two assistant professors on loan to ICRR ended his
term and returned to NAOJ to take the lead of the vibration
isolation tests.

II Status Reports of Research Activities081

11. TMT Project Office
The TMT Project Office of Japan is pursuing theconstruction of a giant telescope with an aperture of 30 m ina collaborative project formed by researchers from countries
including Japan, USA, Canada, China, and India. Preparation
for construction, a key phase in the project, due to commence in
FY 2014 is underway, and mass production of segment mirrors
for the primary mirror was initiated in FY 2013. The Project
Office was further reinforced with the recruitment of additional
staff members. At the end of FY 2013, full-time staff at the
TMT Project Office included four professors, three associate
professors, one chief research engineer, one specially appointed
senior specialist, two research experts, one research associate,
one project research expert, and two administration associates
joined by three associate professors and three assistantprofessors by concurrent appointments.

1. TMT Project Developments in Japan and Overseas
NAOJ TMT Project Office staff members participated in
TMT board meetings, science advisory committees, and external
reviews, held quarterly since 2007 in Pasadena, California,
and contributed to discussions for formulating an international
collaboration. To assist in the evaluation of this large-scaleacademic research project, the Project Office collaborated
with the Science Council of Japan to prepare the project’s
milestone scheme, which was subsequently developed into aplan at the MEXT Council for Science and Technology. NAOJ’s
participation in the TMT project was approved in FY 2012 as
one of the new projects for advancing the large-scale academic
research frontier. In addition to the inclusion in the national
budget for FY 2013, this allowed for budgeting of the materials
for the primary mirror and a TMT-related facility installationin the supplementary budget for FY 2012, respectively giving
impetus to the processes of preliminary telescope structure
design and mirror material polishing. Japan is the first country

Figure 1: Signing of the Thirty-Meter Telescope (TMT) major
agreement in July 2013. In attendance were officials from the National
Astronomical Observatory of Japan (NAOJ) and international chief
scientists representing five countries and six institutions.

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II Status Reports of Research Activities

to officially commence TMT construction and is thus in theposition to lead the international collaboration project.
In July 2013, a board meeting was held in Hawaii in which
officials from the six participating institutions finalized the
TMT master agreement with its signing by their respective
representative scientific authorities. Additional agreementsthat need to be finalized prior to the inauguration of the TMTInternational Observatory were drafted by the Hogan Lovells
international law firm, and deliberations were conducted. The
preparation of all of the agreements was completed by March of2014 following successful negotiations to make the agreements
consistent with the Japanese budgetary frameworks and toclarify entitlements and obligations therein. Officials from Japan,
China, the California Institute of Technology, and the Universityof California are expected to sign the agreements, and thosefrom India and Canada are expected to sign the agreements
at a later date. When all necessary signatures are in place, theTMT International Observatory will be inaugurated. As soon as
official permission for the construction is issued, the observatory
will announce the beginning of the construction work.

2. Research Conferences and Lectures
An international workshop to discuss scientific research by
TMT was held in Tokyo in October. Also, a large group fromJapan participated in the TMT Science Forum held in Hawaii
in July. In Japan, a special TMT session was conducted at theAnnual Spring Meeting of the ASJ held in March. Through a
TMT Project Office subcommittee, the Project Office continues
to engage in its effort to incorporate opinions from the science
community. The dissemination of information about TMT has
been improved in particular by renewing the TMT Project Officewebsite, which publishes updates on the project progress aswell as Japan’s role in the project. TMT newsletter vols. 37, 38,
and 39 were published. The Project Office has also publishedpamphlets in both Japanese and English and has worked toraise public awareness of the project through events such as
lectures delivered at various places around the country andby displaying informative panels at various events including
the NINS Symposium and Inter-University Research InstituteSymposium. The Project Office has continued to be committed
in raising donations for the TMT project. A plaque listing thenames of donors for the first term (up to March 2013), including
six corporations and 1,583 individuals, is currently displayed at
the Subaru Telescope Hilo base facility. The office has screened
TMT promotion films and delivered lectures at various science
centers and planetariums throughout the country with the helpof Club TMT, a community launched two years ago. The Project
Office has also provided approximately 50 lectures and visiting
workshops for the public.

3. Promotion of Tasks Assigned to Japan:
the Construction of the Main Telescope andPrimary Mirror as well as the Development ofObservational Instruments
In the overall scheme of constructing the TMT, Japanis provisionally assigned the tasks of constructing the main
structure of the telescope and primary mirror and fabrication ofparts of observational instruments.
For the primary mirror, Japan is expected to provide all of
the mirror blanks for the segment mirrors. The production of
the first 60 mirror blanks was completed in FY 2013. The taskof polishing the segment mirrors is also partially delegatedto Japan, and the first batch of 12 mirrors has undergone theprocess of aspherical surface grinding. The development andverification of the technology for mass production was initiatedin preparation for aspherical surface polishing that will be
conducted in the future.
The main TMT telescope must weigh significantly lessthan if it were to be built as a straightforward scale up in sizeof a conventional large-scale telescope and at the same timeachieve higher tracking accuracy. The Project Office undertook
the work of preliminary design including the optimization of
the preliminary structure design for the main telescope andplanning of its onsite assembly procedures, a base-isolation
system to withstand a giant once in a millennium earthquake,and mechanical interfaces for observational devices. The
resulting preliminary design passed the international assessment
conducted in November, allowing the project to commence thedetailed design phase in FY 2014.
Japan will perform the task of fabricating a near-infrared
imaging camera and spectrograph known as IRIS, which is oneof the three components of the first observational instruments
to be installed prior to the commencement of TMT observation.
Prototypes fabricated in FY 2013 include optical components
and its supporting structure, a low temperature drive system,
and a vibration-proof system. These components are necessary
for attaining relative astrometry within a wavefront error of 30
nm and 30 μas. Discussions are underway for Japan to performthe fabrication of a camera system and other mechanisms
such as the WFOS/MOBIE (Multi-Object Broadband Imaging
Echellette), and conceptual designs were created in preparationof their construction.

Figure 2: Preliminary design developed for the telescope’s main
structure.

Figure 3: 60 mass-produced mirror blanks.

II Status Reports of Research Activities083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 (theMiky Way) and to perform infrared (Kw-band: 1.5–2.5 μm)
measurements of annual parallaxes, proper motions, andpositions of stars at a high precision of 1/100,000 as (10 μas)
in order to determine with high reliability the distances andtransverse velocities of the stars within approximately 10 kpc
from the Earth in the surveyed direction. Nearly 1 million stars
can be measured with high precisions in the Galactic bulge
with a relative error of annual parallax within 10 %, which isnecessary for accurate determination of the distance. By using
observational data to construct a phase space distributionof gravitational matters, astrometric surveys of the bulge
forming the core of the Galaxy promise to be major scientificbreakthroughs in our understanding of the structure of galactic
bulges and the causes of their formation, the history of starformation within bulges, and the co-evolution of bulges andsupermassive black holes, which is closely related to these
phenomena.
Prior to commencement of the JASMINE mid-sized
scientific satellite project, two projects of small size and ultrasmall size are implemented to progressively build up thescientific results and to accumulate the necessary technicalknowledge and expertise. The Nano-JASMINE micro-satellite
project, with a primary mirror aperture of 5-cm class, iscurrently underway to test part of the technologies used for
the JASMINE and to produce scientific results based on theastrometric information of bright objects in the neighboring
space. Despite its small aperture, the satellite is capable of alevel of observational precision comparable to the Hipparcos
satellite, and the combination of the observational data from
Nano-JASMINE and the Hipparcos Catalogue is expected
to produce more precise data on proper motions and annual
parallaxes. The satellite is scheduled for launch in the second
half of 2015. An additional plan is underway to launch a smallscale JASMINE satellite (Small-JASMINE), with a primary
mirror aperture of 30-cm class, in around FY 2019. This satellite
will engage in observations of only a limited area around thebulge and certain specific astronomical objects. This smallsized version has a goal of obtaining advanced scientific results
at an early stage. A mid-sized JASMINE satellite, with a main
aperture of approximately 80 cm, is designed for surveying
the entire bulge and is targeted for launch in the 2020s.
Internationally, Japan shares responsibilities with the ESA byengaging in infrared observation of the bulge, which is a method
suitable for observations in the direction of the Galactic center,
whereas the ESA performs visible-light observation of the entire
sky at a precision of 10 μas with the Gaia Project.

084

II Status Reports of Research Activities(2) Major Progress in FY 2012
1) Organization of the office
The JASMINE Project Office is composed of four fulltime staff members, seven staff members with concurrent posts,
two postdoctoral fellows, one research associate, one technicalassociate, and three graduate students. Significant contributions
were made by members of the following organizations: the
NAOJ TAMA Project Office; Kyoto University’s Graduate
School of Science; the Systems Engineering (SE) Office,Aerospace R&D Directorate (ARD), and ISAS at JAXA; theUniversity of Tokyo’s School of Engineering; Tokyo Universityof Marine Science and Technology; and the University ofTsukuba.
2) Progress of the Nano-JASMINE Project
The project will engage in an actual space mission using an
ultra-small satellite to accomplish the following objectives: tomake Japan’s first foray into space astrometry, to accumulatetechnical experience in onboard data acquisition and the likenecessary for the upcoming JASMINE project, and to achievescientific results on , for an example, the dynamical structure in
the neighborhood of the Solar System.
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; at present, launching is scheduled for the second halfof 2015. Moreover, the construction of the rocket has been
completed, and work on interface adjustment between the rocket
and the satellite is in progress. Assembly of the flight modelthat will be actually launched into space was completed in FY
2010, and additional testing was conducted using the extra timeyielded by the launch delay to further ensure project success.
Maintenance of the satellite has also been performed. The
project continued with the preparation of ground communication
stations in relation to the satellite operation. The second
operation training program, simulating the actual operation,
was held for one month, during which operational issues wereidentified and addressed.
Steady progress was also made in the development ofalgorithms and software required to determine astrometric
information from raw observational data at the required level ofprecision. International cooperation with the data analysis teamfor the Gaia Project was conducted smoothly. The Gaia Project
involves observational and analytical methods similar to thoseof the Nano-JASMINE. A Japanese WG led by Ryoichi Nishi of
Niigata University continued to engage actively in investigating
the scientific results expected by the Nano-JASMINE.
3) Overview of planning and developing Small-JASMINE
The objective of the Small-JASMINE project is to use athree-mirror optical system telescope with a primary mirror
aperture of 30 cm to perform infrared astrometric observations(Hw band: 1.1–1.7 μm). An additional goal is to measure annual
parallaxes at precisions of 10–20 μas and proper motions, ortransverse angular velocities across the celestial sphere, atprecisions of 10–50 μas/year in the direction of an area of few
square degrees from the Galactic center within the bulge andthe direction of a number of specific astronomical objects ofinterest in order to create a catalogue of the positions and their
movements of stars on the celestial sphere within these regions.
The project is unique in that unlike the Gaia Project, observation
will be performed in the near-infrared band, in which the effectof absorption by dust is weak, and the same astronomical object
can be observed frequently. This project will help to achieve
revolutionary breakthroughs in astronomy and basic physics,
including the structure and history of the formation of the
Galactic bulge; the co-evolution of the Galactic bulge and themassive black hole in the Galactic center; the orbital elementsof X-ray binary stars; the physics of fixed stars, star formations,and planetary systems; and gravitational lensing. Such data willallow for the compilation of a more meaningful catalog whencombined with data from ground-based observations of the lineof-sight velocities and chemical compositions of stars in thebulge. 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 andmanufacturer’s propositions that started in 2009 continued
to consider the design of the satellite system to ascertain thetarget precision in astrometric measurements 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 of Tsukuba and including
volunteers from diverse fields in Japan, continued to makescientific considerations and other activities such as conceptual
planning and design and technical testing. International project
collaboration continued in FY 2013. As planning progressed, themission proposal was fully prepared and submitted in February
2014, and the ISAS public call began accepting enrollments on
December 28, 2013.
International partnerships to gain further understanding of
the Galactic bulge have been formed with multiple overseas
groups engaging in ground-based high-dispersion spectroscopic
observations to determine the line-of-sight velocities andchemical compositions for bulge stars. In particular, Steven
Majewski of the University of Virginia, the principal
investigator (PI) of the US Apache Point Observatory (APO)
Galactic Evolution Experiment (APOGEE) Project, offered ajoint proposal for the APOGEE-2 project as an extension of theoriginal APOGEE project to engage in bulge observations in thesouthern hemisphere because the project is suitable for bulge

observations. The telescope employed will be equipped witha high-dispersion spectroscope, an identical model to that of
APOGEE. The joint proposal was subsequently submitted. An
official memorandum of understanding was 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.

II Status Reports of Research Activities085

13. Extrasolar Planet Detection Project Office
The Extrasolar Planet Detection Project Office cooperates
with researchers interested in exoplanet science at universities
around the country under the NAOJ’s initiative to promote
the development of technologies in general for observing
exoplanets and their formation processes as well as to organize
exoplanet related observations. It engages in the developmentof observational equipment, the promotion of research, mission
planning, and R&D of common core technologies. The
project also spearheads some exoplanet-related international
collaborations. Specifically, the R&D focuses on the following
core areas:(1) Development, maintenance, and operation of HiCIAO andimplementation of SEEDS.
(2) Development of the next novel observation instrument, theIRD, for the Subaru telescope and observation planning todetect terrestrial exoplanets.
(3) Technical planning of the TMT/Second Earth Imager for
TMT (SEIT) instruments and the missions of WFIRST–
AFTA Coronograph (WACO) and the Japanese Terrestrial
Planet Finder (JPTF) for direct observations of terrestrial
planets as well as promotion of relevant international
collaborations.
(4) Research in the interstellar medium and the formationof stars and planets via wide-field imaging polarization
observations using the Infrared Survey Facility (IRSF)
telescope in South Africa.

project using Subaru, commenced in October 2009 withcooperation from more than 100 researchers across Japan andworldwide. Observations are continuing smoothly.
(2) Infrared Doppler Instrument (IRD)
Development is underway for a high-precision highdispersion infrared spectrometer equipped with a radial
velocity precision of approximately 1 m/s. It aims to realize
an IRD instrument for detecting habitable terrestrial planets
around the M-type and other low-mass stars. The budget forthe project is based on a JSPS Specially Promoted Research
project led by Motohide Tamura and funded by Grants-in-Aid
for Scientific Research for FYs 2010–2014. The optical system
was fabricated, fiber selection was conducted for guiding lightfrom astronomical objects and comb light, and experimentsfor optical frequency comb generation were pursued. Planningfor investigations of planets around the M-type stars also
progressed.

The office was served by five full-time staff members,
three staff members with concurrent positions, and six full-time
postdoctoral fellows in FY 2013. It published 26 peer-reviewed
papers and 11 non-refereed papers and issued 39 reports
including speeches at international conferences, all in English.
In the Japanese language, it published one peer-reviewed
paper, three standard papers, and 57 reports including academic
conference presentations.

1. Development of the Next Observational
Instruments Intended for Exoplanet Research
for the Subaru Telescope and Implementationof Observational Research(1) High Contrast Instrument for the Subaru Next Generation
Adaptive Optics (HiCIAO)
Development of the HiCIAO modular high-contrast
observational instrument has been completed. This instrument isdesigned for direct observation of exoplanets and circumstellar
disks, where the exoplanets are formed, using an 8.2-m
telescope, for which the system is equipped with a coronagraphand simultaneous differential imaging technologies such aspolarizations and multiple wavelengths and angles. Design andfabrication began in FY 2004. Performance test observations
were completed in FY 2009, and SEEDS, the first strategic

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Figure 1: High-Contrast Instrument for the Subaru Next Generation
Adaptive Optics (HiCIAO) image capturing an exoplanet orbiting aroundthe solar-type star GJ 504, visible as the white spot at the top right. The
mass of this planet is estimated to be 3–5 times that of Jupiter, and due
to its older age it has one of the lowest uncertainties of mass estimatesamong planets ever observed directly. The central star with suppressedbrightness and its positional indicator, represented by a cross, are shownat the bottom left.

2. Technical Planning of a Space Mission and
Next-Generation Observational Instruments
for Extremely Large Terrestrial Telescopes forthe Direct Observation of Terrestrial Planets,
including International Collaboration(1) WFIRST-AFTA Coronagraph (WACO) and Japanese
Terrestrial Planet Finder (JTPF)
The scientific goal of the WACO and JTPF missions is
to observe low-mass planets such as terrestrial planets andsuper earths via direct imaging in the search for signs of life.
The WACO WG was established as the main body to conduct
basic experiments of WACO. Jet Propulsion Laboratory (JPL)
test beds were employed to implement performance tests withcollaborators.
(2) Second Earth Imager for TMT (SEIT)
Technical and scientific planning of the new SEIT
observational instrument continued to realize the detectionof terrestrial planets using the 30-m next-generation TMT. A
proof-of-concept optical system was constructed for the SEIT
observational method, and demonstrations were performed.

3. Research/Educational/Outreach Activities
Research was conducted into exoplanets, the disks in which
they form, and related fields including rogue planets, browndwarfs, star/planet formation, and normal stars. A total of 26
peer-reviewed scientific papers were published. In particular,
eight papers addressed the SEEDS project. Two noteworthy
results were made. In the first, first-ever clear direct imaging ofsolar planet GJ 504b using the HiCIAO led to a discovery andsuccessful capture of a second Jupiter (Fig. 1) with multi-color
imaging. In the second, detailed structures of SR21, RY Tau, andSz91 were elucidated through high-resolution observation of a
protoplanetary disk, again using the HiCIAO. Other activities
include a planet and brown dwarf search in the Pleiades by
SEEDS, research on the planetary atmosphere using infraredtransit observation, and brown dwarfs and/or star-forming
research by the UK Infrared Deep Sky Survey/VISTA Variablesin the Via Lactea (UKIDSS/VVV) project. SEEDS continued tofollow its procedures smoothly this year. Theoretical researchand research via Doppler methods were also conducted.
Twelve graduate students were offered research guidanceand engaged in exoplanet research and related R&D. Numerous
lectures, publications for the general public, and press releases
were delivered on exoplanets, disks, and general astronomy.

14. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project
1. Lunar explorer Kaguya (SELENE): Publicationof Data and Lunar Research(1) Publication of Kaguya data
Data from the RISE Project on the topography and the freeair gravity anomaly, as well as processed data for Bouguer
gravity anomalies and crustal thickness, have been available tothe public on the NAOJ website since July 2010, where gravity
field and topographic data are occasionally updated. Data can beaccessed at the following sites:
Japanese: http://www.miz.nao.ac.jp/rise-pub/English: http://www.miz.nao.ac.jp/rise-pub/en(2) Study of the Internal Structure of the Moon
The internal structure and composition of the Moon havesignificant impacts on understanding the lunar origin andevolution. Hitherto, attempts have been made to estimate
the internal structure by using the data from Apollo seismic
network, as well as gravity fields, tidal Love number, androtational variation data. NASA’s Gravity Recovery and Interior
Laboratory (GRAIL) data have further improved the accuracyof the tidal Love number k2. In view of this, geodetic data suchas mass, the moment of inertia, and tidal Love numbers h2 andk2 were used together with the P- and S-wave travel times ofmoonquakes to recalculate the internal structure of the Moon.
With the assumption of a five-layer model including the crust,

upper, middle and lower mantles, and core, the Markov chain
Monte Carlo (MCMC) methods yielded a larger core radiusof the Moon than the constraints obtained through Kaguya’smagnetic field observation. This discrepancy is now underconsideration for possible explanations, including the existenceof a low-velocity zone near the core-mantle boundary.

2. Future Lunar/Planetary Exploration Projects(1) High-precision VLBI Observation of Lunar Gravity field:
Planning and Component Technology Development
The GRAIL lunar explorer has significantly improved thelunar gravity field model; therefore, we were required to revise
our scientific goal regarding the improvement of a lunar gravity
field model by SELENE-2 VLBI. Before doing this, our current
research results were summarized and published as a paper
focusing on the following four points: (a) designing a radiosource to be installed on the lunar lander and consideration
for saving of electric power, (b) estimating the accuracy of
VLBI observation, (c) estimating the accuracy of lunar gravity
field recovery, and (d) designing a thermal-proof antenna tosurvive the temperature environment on the lunar surface forelectrical property analysis. In addition, the following items
were considered from the perspective of future lunar/planetary
explorations and component technology development:

II Status Reports of Research Activities

087i) Antenna thermal tolerance
Since last year, investigation continued in developing anantenna to survive the lunar surface temperature ranging from−200 °C to +120 °C. Macor (dielectric material) considered
for the base substrate material has been confirmed to meetthe performance requirements under the above temperature
conditions after thermal vacuum tests.
ii) Discussion for providing two beams for the S and X bands inthe 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 in the SELENE-2 mission. In order toachieve more precise dual-beam S/X band VLBI observations,
the RISE Project Office and the Mizusawa VLBI Observatory
continued planning of the joint project using a Grant-in-Aid for
Scientific Research, Category A (‘Research on Lunar/Planetary
Inner Structures via Satellite VLBI Observation: Size, State, andOrigin of Metal Cores’).
The Vivaldi antenna was selected as a model for adoption.
An antenna element was designed using electromagnetic
analysis software, and its shape was optimized. A computer
simulation confirmed that the antenna is able to perform at therequired performance level. A prototype single-element device
was fabricated and subjected to a performance test, followed byfabrication of a multi-element version, which was integrated toform a phased-array antenna. Tests confirmed that the antennaachieved almost all of the target performances.
(2) Development Experiment for Lunar Laser Ranging (LLR)
and Studies of the Internal Structure of the Moon
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 the lack of reflectors in the southern hemisphereand the time difference between the two ends of reflector arrays
generated by libration, the level of precision has hitherto been
insufficient for determining small variations in the process ofenergy dissipation in the lunar interior. As part of SELENE-2, a
proposal has been made to set up a new single reflector mirror
in the southern hemisphere away from the reflectors alreadyin place, allowing for high-precision measurement of lunar
rotational variation.
Investigations in FY 2013 focused on the following points:i) Retroreflector mirrors
Material selection and mirror-forming methods were
investigated for the fabrication of an LLR retroreflector
to be mounted on the lander. Monocrystalline silicon was
selected as the best mirror material for thermal-structural andoptical analyses after tests under the simulated lunar surface
environment. A thermal vacuum test under the lunar surface
environment further verified the suitability of this material.

088

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Three-plane bonding and single-piece manufacturing wereconsidered as methods of forming the mirror. In three-planebonding, the critical issues are minimal distortion during thebonding process and lasting stability after bonding. However, itturned out that optical contact bonding, which was considered
as preferred candidate, requires a curing temperature of morethan 800 °C to improve the bonding strength, which remains
as a challenge for the future work. For a single-piece mirror,
preparatory technological development was pursued inconjunction with a tri-party agreement with the Chiba Instituteof Technology and Tokyo University of Science, aiming toutilize Ion Beam Figuring (IBF).
ii) Terrestrial ranging station tests
To realize LLR observation, experimental lunar laser
ranging was conducted jointly with NICT, using the upgraded
NICT Koganei satellite laser ranging (SLR) system for lunar
observation. The experiments included not only actual lunar
ranging, but also experimental ranging to retroreflectors aboard
Earth-orbiting satellites.
iii) LLR data analysis simulation
A group formed mainly of first-year graduate studentsof the Graduate University for Advanced Studies started thedevelopment of software for the analysis of the LLR data
through lunar tidal deformation and rotational variation to
improve the precision level of estimating the internal structureof the Moon. The three stages of the development consist of
the construction of an observational model, generation of anephemeris, and estimation of initial values and parameters. For
the first stage, a model with residual error between −10 and+10 cm has been developed, which is comparable to the latest
planetary and lunar ephemeris DE430.
(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 observation of lunar
rotational variations to constrain the internal structure of theMoon. Because measurement can be conducted independently of
lunar orbital motion, this small telescope is capable of detecting
miniscule variations in the rotation of the Moon, allowing for
determination of whether the lunar core is molten.
In FY 2013, the RISE Project Office and Iwate University
jointly conducted in-laboratory overall testing of the terrestrial
observational model known as the Breadboard Model (BBM), an
improved version of the model telescope, by using an artificial
light source with the goal of conducting actual star observations.
The testing involved imaging of a mock star created under an
artificial light source, using mercury pool developed during FY2012 which is less susceptible to vibration, and determining therelationship between variations of star-image center, groundvibration, and inclination of the telescope tube.

(4) Development of the Laser Altimeter (LIDAR) of Hayabusa 2
and Studies of Shape and Gravity Fields of Asteroid
The RISE Project Office participated in the development of
LIDAR together with the Chiba Institute of Technology and the
University of Aizu. LIDAR, a laser altimeter used to estimate
asteroid shape and gravity fields, is scheduled to be on board
the Hayabusa 2 asteroid explorer slated for launch at the endof 2014. Investigation is underway for science promotion anda hardware testing plan for scientific maturation. The project isplanned to make scientific contributions in gravity (object mass)
determination and photometry.
The investigations in FY 2013 focused on the following
points:i) ranging tests using a flight model, hardware tests using groundsupport equipment, and accuracy estimation of asteroid surface
albedo calculated through the intensity ratio of transmitting andreceiving laser.
ii) detail planning of a laser link experiment in which the laser
is transmitted from the ground SLR station toward Hayabusa 2
spacecraft.
iii) development of a quick-look software and verification at the
integration tests.
iv) theoretical calculation of size and density of circum-asteroid
dust for hardware development.
v) extension of SLR data analysis software (c5++) developed bya team led by Hitotsubashi University to interplanetary use fororbit and gravity field estimation of the asteroid.
vi) discussions at the Shape Model Team Meeting on methods
for shape estimation of the asteroid using LIDAR and the
Optical Navigation Camera (ONC).
vii) scientific discussions at the Integrated Science WG on how
to combine the data obtained by other scientific instruments withthose by LIDAR.
(5) Development of a Ganymede Laser Altimeter (GALA) for
the Jupiter Icy Moon Explorer (JUICE) mission and studies of
the internal structures of Jovian moons
As the GALA was officially selected by the ESA as one of
the JUICE mission payloads following a proposal submission
in FY 2012, the RISE Project Office officially commenced
activities as a main GALA-Japan team member. Japan will
undertake the development of receiving telescope as a part ofthe laser altimeter system. Dr. Matsumoto of the RISE Project
Office also leads the gravity/rotational variation subgroup within
the Japanese part of the science team. The following points wereconsidered in FY 2013:ii) deliberation on the specifications of thermal–structural
analysis to be outsourced to a manufacturer.

3. Educational Activities/PR
One student enrolled at the Graduate University for
Advanced Studies for the RISE Project Office, and the officeprovided the student with seminars. Five RISE membersdelivered lectures on a part-time basis to graduate students at
the University of Aizu and two RISE members served as parttime lecturers at Iwate University for half year each. The officeaccepted a first-year graduate student of the Graduate University
for Advanced Studies for lab rotation.
The RISE Project Office continues to engage in raisingpublic awareness regarding the Kaguya project. The office’s
website, http://www.miz.nao.ac.jp/rise/en, was revamped toallow for regular posting of updated information.

4. Joint Research/International Collaborations
Joint research into the basic development of a lunar lander/
explorer (LLR and ILOM) is conducted by the Faculty ofEngineering at Iwate University, with monthly meetings held
alternately at Iwate University and the NAOJ Mizusawa.
This collaboration is in accordance with ‘the Memorandumon Basic Issues Concerning Research and Developmentof Scientific Instruments for Lunar Landing Exploration’,
which was exchanged between members of the RISE Project
Office and the Faculty of Engineering at Iwate University.
The memorandum was renewed in 2010. The two groups willcontinue collaborating in the R&D of scientific instruments forlunar landing exploration.
The RISE Project Office continues to collaborate with agroup from Shanghai Astronomical Observatory in China,
which has been a collaborator in the observation of the Kaguya
spacecraft. The parties further engage in data analysis and joint
research into future projects on the basis of ‘the Memorandumof Understanding for Cooperative VLBI Observations between
Shanghai Astronomical Observatory and National Astronomical
Observatory of Japan’, which was renewed in 2009.
With a group of Kazan Federal University, Russia, which
is well reputed in theoretical investigation into the internal
structure of the Moon, joint research continues to establish
a new theory of lunar rotation, along ‘the Memorandum ofUnderstanding for Cooperative Research between Kazan Federal
University and National Astronomical Observatory of Japan on
VLBI and Astrometrical Observations’, which was renewed in2010. Possible collaborations between the two countries were
explored for future lunar exploration projects.

i) detailed laser link calculation (performance model) to serve as
the basis for the hardware design.

II Status Reports of Research Activities089

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) sounding rocket
experiment.

1. Solar-C Project
The Solar-C is a planned project and may become Japan’s
fourth solar observation satellite, after Hinotori, Yohkoh, andHinode. The plan is to realize the launch in the early years of
2020s. The project is intended to investigate the solar magnetic
plasma activities that influence space weather and space
climate around the Earth. The investigations will involve thechromospheric magnetic-field and high-resolution imaging/
spectroscopic observations that have not been achieved. The
themes include three major problems in solar research: solar
flares, chromospheric/coronal heating, and solar magnetic cycle
activity. An additional theme is magnetic plasma processes suchas magnetic reconnection and MHD waves. The tasks include
revealing the fundamental small-scale magnetic structuresderived directly or indirectly from the Hinode observationsand visualizing the magnetic structures in terms of activities
and interactions. The Solar-C will conduct high-resolution(0.1–0.3 arcsecs) observations of images, polarization, andspectroscopy over the area from the photosphere to corona byusing onboard instruments. The observational instruments for
the Solar-C consist of SUVIT with 1.4-m aperture for observing
the photosphere and chromosphere, EUVST for spectroscopic
observation from the chromosphere to corona, and XIT for
capturing images of the transition region and corona. Since its
establishment, the Solar-C project WG has involved Japanese
researchers in addition to many non-Japanese specialists.
Provisionally, Japan will be responsible for the launch vehicle,
satellite, and one of major science instruments, whereas the US
and European 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 managed by Prof. Watanabe,
NAOJ, set up within the Steering Committee for Space Scienceat the ISAS/JAXA; NAOJ researchers play key roles in the
project activities. The Solar-C Planning Office was set up at the
NAOJ in FY 2008 as a sub-project to the HSC, dedicated to the
Solar-C project. It was promoted to the Solar-C Project Office in
FY 2013 as an A-project independent from the HSC, continuing
the preparatory work for realization of the satellite project withfive full-time staff members and 11 members with concurrent
positions/postdoctoral fellows.

2. CLASP Project
The CLASP project is an observational sounding rocket
experiment aiming to detect solar magnetic fields in the090

II Status Reports of Research Activities

chromosphere 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 US, and other countries. The payload consistsof a far-ultraviolet (FUV) telescope and a spectro-plarimeterthat are prepared in Japan to conduct a polarization observation,with components contributed by the US (CCD cameras) andFrance (concave grating). The system then will be mounted
on an American sounding rocket for the launch in the US. The
Japanese PI is Kano, assistant professor at the NAOJ, wholeads postdoctoral fellows and assistant professors to pursue
designing, equipment development, and testing.

3. Major Activities in FY 2013
Although the progress was made in the feasibility studies
and component developments of the large optical telescopeand satellite system, much of the time was used for making
amendments to the mission proposal. The office organized aSolar-C Science Meeting in Takayama on November 11, 2013,
one day before the Seventh Hinode Science Meeting (Hinode-7),
with 143 participants including 91 international participants.
Deliberations on the large telescope and satellite system yielded
the following developments:(1) A budget for wavefront error was proposed during
the discussion on equipping the primary mirror, which will
be directly exposed to the solar light, with heat pipes forthermal exhaust in order to achieve the diffraction limit of
the large telescope. (2) Reflective systems were consideredas the base of the collimator at the rear end of the telescope,and its design was discussed for fabrication. (3) Tolerance of
the instrument positions against the telescope and ideas fortolerance distribution of the built-in optical elements were
derived from the optical design of spectro-polarimeter withphysical processes of diffraction and polarization. (4) Progress
was made in the development of the mechanisms indispensablefor the polarization observation. (5) The degradation of Hinode’s
throughput was further understood, the investigation into which
would help to understand the throughput degradation of the
Solar-C telescope. (6) The conformity of the strength of the
optical bench for the telescope was verified. (7) Investigations
on component technologies for realizing the pointing stability
superior to that of the Hinode led to clarification of thespecifications of new components. (8) Progress was made inplanning the methods for testing at the system level. (9) Issues
were identified through studies on mission data processing after
receipt from the observational system. Preparation was also inprogress for testing of the near infrared detector intended for the
spectro-polarimeter.
The CLASP project entered the development stage fullyin the latter half of FY 2012, and it anticipates a prospective
development budget for the flight equipment during FY 2013,

aiming for the launch at the summer of FY 2015. In FY 2013, thedeveloped elements were measured at the synchrotron radiation
facility of the Institute for Molecular Science, and flight models
were delivered for examinations including review of design andfabrication and testing of the assembly. The CLASP project hasreceived a significant contribution from the ATC in terms ofthe design, fabrication of necessary components, and testing ofsome of the flight models.

4. Other
The CLASP project has offered an invaluable opportunity

for graduate students and postdoctoral fellows to engage inand experience the development of observational instruments.
These young researchers can use this opportunity as avaluable steppingstone for the future development in space
instrumentation, including the Solar-C.
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.

16. Astronomy Data Center
1. Overview
The role of the Astronomy Data Center (hereafter ADC) is
not only to maintain a research infrastructure via the smooth
operation of a group of fundamental systems, but also to engage
in research and development towards future expansions of openuse computer system and research infrastructure. Its activity
consists of DB/DA Project, Network Project, Japanese Virtual
Observatory (JVO) Project, Hyper Suprime-Cam Data Analysis
Software Development Project, and works related to the openuse computer system.

2. Accomplishments(1) DB/DA Project
The DB/DA Project engages in database- and database
analysis-related research and development, as well as thehandling (collection / management / sharing) of astronomical
data. The DB/DA project has made various types of astronomical
data public, such as astronomical catalogues, the SAO/NASA
Astrophysics Data System (ADS), and all-sky image data (DSS,
DSS2), for use by astronomers and educators in Japan andoverseas (http://dbc.nao.ac.jp/).
The Subaru–Mitaka–Okayama–Kiso Archive (SMOKA)
database (http://smoka.nao.ac.jp/), the key player of the project,provides access to various archival data from the Subaru
telescope, the 188-cm telescope of the OAO, the 105-cm
Schmidt telescope at the University of Tokyo Kiso Observatory,
the MITSuME telescope operated by the Tokyo Institute ofTechnology (two 50-cm telescopes) and the Kanata telescope(150 cm) at the Higashi–Hiroshima Observatory of Hiroshima
University. It has yielded numerous research breakthroughs.
Nearly 8.77 million frames and 46 TB of observational data
(excluding environmental and meteorological data) are available
for viewing in the SMOKA as of May 2014. In FY 2013, 23
papers using SMOKA data were published in peer-reviewed
journals, amounting to 158 published papers as of May 2014.
System improvement continued on the SMOKA in FY 2013

for developing an advanced search function and enhanced
operational efficiency. The Kiso Observatory made its wide-fieldcamera (KWFC) accessible to the public, and the DB/DA project
developed a system for publicizing all-sky monitoring images(Okayama and Hiroshima).
(2) Network Project
The ADC operates network systems that connect its
headquarters at the Mitaka Campus with branches distributed
around Japan and with a wide-area network connecting with
regional ones. We report the following noteworthy operational
results for FY 2013:
1) High-speed connection for inter-observatory network:
For the purpose of R&D of next-generation communication
technology in relation to the NICT’s JGN-X project, theMizusawa station installed a 10-Gbps telecommunication circuit,which was connected to the JGN-X network in April 2013. The
network speed of more than 10 Gbps was achieved between the
Mizusawa and Tokyo bases, and the network is utilized for the
CfCA, the VERA project, and the post-2011 earthquake recovery
efforts, among others.
2) R&D system designed for the CfCA supercomputer system:
The CfCA supercomputer system stretches over theMizusawa and Mitaka campuses. The ADC in collaboration
with the CfCA developed a highly cost-efficient high-speed
router (40 Gbps) and storage cache (accelerator) for efficient
communication between the bases. This system, known as
Renjaku, won the Fujitsu Award at the Open Router Competition
during the Interop 2013 Conference.
3) Special classes for students from elementary and junior highschools in the earthquake-affected areas:
The ADC held three special classes primarily geared towardelementary and junior high schools in the earthquake-affected
region, in which the classrooms were connected with the Subaru
Telescope facility via a real-time link. These events were hosted

II Status Reports of Research Activities091

jointly with supporting enterprises in Japan and abroad, as wellas with Mozilla Japan.
(3) Japanese Virtual Observatory (JVO) Project
The JVO project engaged in the development and operationof a portal site (http://jvo.nao.ac.jp/portal), providing worldwide
access to astronomical data, in order to promote data-intensive
astronomical research.
The following activities were pursued in FY 2013:
The interface design was revamped to improve usabilityof the JVO portal site; the JVO continued the disseminationof ALMA data; the WebQL, a program to display images andspectrum data from the ALMA telescope on web browsers, wasequipped with almost all of the features planned at the beginningof its development and provides service in the public domain;
the development of a desktop viewer, Vissage, also continues
and is led by members from the Chile observatory (ALMA
Japan); the JVO project members delivered presentations of the
ALMA data distribution system on various occasions, including
an annual meeting of the Astronomical Society of Japan, anInternational Virtual Observatory Alliance conference, and an
Astronomical Data Analysis Software and Systems (ADASS)
conference; the JVO project held VO workshops with eightparticipants; and the JVO underwent source code refactoring.
Moreover, the JVO project members conducted scientificresearch using the JVO; the results were published as a refereed
paper in the Astrophysical Journal, which was also published on
the NAOJ website.
(4) Analysis Software Development Project for Hyper SuprimeCam
The analysis software development project for the HSC
began in January 2009, which engages the following tasks forenhancing the accuracy and efficiency of analysis of the datafrom the HSC: planning and implementation of parallelized
and distributed processes, methods of correcting instrumental
distortion, methods of calibrating object position and brightness
in individual 104 CCDs.
Test observations using the HSC were fully implemented
in FY 2013, during which time the software developed in2011 for post-observational on-site analysis at the Subaru
Telescope’s Operations Support Facility was put to repeatedactual operations. A problem brought forward from the previous
year, such that the analysis process took roughly 5 min before
completing all of the data from 104 CCDs, was addressed;
various modifications reduced the time to 2.5 min. Furthermore,visualization was achieved almost instantaneously via a web
browser, contributing to the construction of support tools for
operating observations. Regarding the image processing, aseries of tasks are now available ― reduction of each CCD,
mosaicking CCD images, and catalogue generation. Further
work will involve the enhancement of precision levels for certain
processes and introduction of new measurement algorithms.
Other directions will be further explored.

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The database for managing the post-analysis data has also
been equipped with functions initially conceived, which brings
the database construction agenda using the test observation datafrom the beginning of the project to close to its completion.
The integration work with the analysis software was also
implemented, and nearly all data processing procedures were
installed. The database will further evolve with the goalof realizing a more efficient search engine and improved
operations.
(5) Works Related to the Open-Use Computer System
It is one of primary responsibilities of the ADC, as an interuniversity research institute, to operate the open-use computer
system. The new rental computer system, the NAOJ Data
Analysis–Archival–Publication System commenced its operation
on March 1, 2013, and consists of a Multi-Wavelength Data
Analysis subsystem; a Large-Scale Data Archival–Publication
subsystem including MASTARS, SMOKA, HSC, and ALMA
archives; a VO subsystem; a Solar Data Archival–Analysis–
Publication subsystem; and the Mizusawa Data Analysis
subsystem. The system is in good condition with no major
problems. System improvement will continue in performance,
usability, security, and management.
As of FY 2013, the Multi-Wavelength Data Analysis andSolar Data Archival–Analysis–Publication subsystems had 175
and 171 users, respectively. 145 refereed papers were produced
using the open-use system in peer-reviewed journals in FY 2013.
The following workshops were held as part of the open-use
activities, including joint events:
1. C (programming language) workshop: July 24–26, 2013: 12
participants
2. The Graduate University for Advanced Studies Summer
School: workshop on radio observational data analysis (ADC
provided the analysis environment)
August 12–September 9, 2013: four participants
3. IDL workshop: FITS analysis: September 17–18, 2013: 10
participants
4. Early Winter School on N-body simulation: January 15–17,
2014: 18 participants
5. VO workshop, Autumn 2014: January 27–28, 2014: eightparticipants(total participants: 54)

3. OtherAs part of PR activities, 61 issues of “Information fromADC” (Nos. 325–385) were published in FY 2013. These issues
were published on the website and were distributed via e-mail.

17. Advanced Technology Center
1. Overview of the Organization and Activities
The ATC engages in the development of astronomical
observation instruments, focusing on prioritized areas fordeveloping instruments intended for supporting NAOJ projects
and on advanced technology to contribute to future projects.
The prioritized area development in FY 2013 included thedevelopment of the ALMA receivers, HSC, the Kamioka
Gravitational Wave Detector (KAGRA) telescope, and an
observational instrument of the InfraRed Imaging Spectrometer(IRIS) for TMT. Regarding the advanced technology development,
the ATC pursued the preliminary development of a radio
receiver in view of future post-ALMA projects and preliminary
development for astronomical observations from space.
The Advisory Committee for Advanced Technology,
including external committee members, discusses the ATCʼsinvolvement in NAOJ projects and human resource plans. The
main agenda in FY 2013 was the center's involvement in the
TMT projects. Issues concerning daily operation of the center
are addressed on the basis of deliberations by the Advanced
Technology Steering Committee. Various items were discussed
at the meeting, including a request for a subsidy for strategic
development expenses, a request for engineer reinforcement,
the liaison with the TMT project, and progress reports regardingATCʼs internal projects.
Fabrication of the ALMA receiver was completed in FY
2013, bringing the terms for many contract staff members toan end. The ATC needs to pursue the receiverʼs maintenance incollaboration with the Chile Astronomical Observatory in the
future. The ATC is also in discussion regarding methods formaintaining and enhancing its performance as a domestic center
for radio receiver development.
The HSC has been already entered an observation phase,and current issues include stabilizing the instrument operationand establishing a support structure for data analysis.
For the development of the TMT observational equipment,
development of the optical system for the IRIS has madeprogress, and the ATC is engaged in information sharing with
the TMT Project Office on development of the Wide-Field
Optical Spectrometer (WFOS)/Multi-Object Broadband Imaging
Echellette (MOBIE). Plans are underway on facility design andspecifications of the Advanced Technology Experiment Building(TMT wing) to be constructed through these exchanges.
Regarding the KAGRA project, the main task was thedevelopment of baffles for an auxiliary optics system tosupport suppression of stray light. In FY 2013, the ATC began
development of a plan to create and mass-produce a prototype ofa multi-strata anti-spring filter for fitting the mirror and isolating
vibration.
The joint development research and facility open-use
continue status-quo, although difficulties in securing experimentspace have persisted. Aging of the facilities at the Development
Building (south) became apparent in FY 2013, and somefacilities that had been in use for more than 10 years at theDevelopment Building (north) developed functional problems. A
discussion is underway to renew the facilities at the completionof the TMT Building.

2. Workshops and Development Support Facilities(1) Mechanical Engineering Shop
The Mechanical Engineering (ME) Shop engages in acomprehensive manufacturing process to fabricate experimental
and observational instruments, from design to fabrication andshape measurements. Three teams including design, fabrication,and measuring/ultra-precision fabrication teams cooperate toadvance projects leveraging their expertise.
The design team has handled the structural design of
KAGRA’s auxiliary optics system and the mechanical structure
design of TMT/IRIS imaging parts since the previous year.
For KAGRA’s auxiliary optics system, the following was
performed:- Design of the main mirror mount for i-KAGRA- Design of a narrow-angle scattering baffle bench- Thermal analysis of a wide-angle scattering baffle- Design of an optical lever pylon- Consultation for the fabrication of a prototype bottom filter
For mechanical design of TMT/IRIS imaging parts, thefollowing were pursued:- Design and testing of various mechanical testing instruments
such as motors and bearings- Creation and testing of a prototype cold-stop mechanism- Creation and testing of a prototype kinematic lens cell
- Design of a filter-replacement mechanism
In addition, the ATC gave support to the launch of the HSC
and dealt with some defects. In order to ensure compatibility
with the IRIS imaging parts design, to be fully developed in
FY 2014, the facilities were reinforced with an installation ofsoftware for nonlinear/irregular analyses.
The fabrication team accomplished fabrication of the massproduction parts for the ALMA receiver on time. Further,an additional order for spare parts (units for seven) was also
accomplished on schedule. In tandem with the commencementof an element testing experiment for the IRIS, the teamundertook fabrication of prototype parts for the low-temperaturedrive system.
For the KAGRA project, the team fulfilled the request fora prototype of a vibration isolation system bottom filter andundertook fabrication of main parts in an installable condition.
The team also fabricated a special spring composed of maraging
steel for the vibration isolation system and succeeded in creatinga prototype in an installable condition.
The team also succeeded in high-precision fabrication of
onboard parts for the CLASP rocket including three types ofsuper Invar kinematic mounts in five units and delivered themof flight model parts. A continued attempt is made to create

II Status Reports of Research Activities093

improved prototypes of a mechanical deformable mirror, which
has been under development since last year by ISAS/JAXA.
The ultra-precision fabrication team engaged in a joint
development research project with external institutions andresponded to fabrication requests. The joint development research
was involved the development of an ultra-precision milling
process using a monocrystalline diamond tool, in collaboration
with the Mechanical Engineering Center of the KEK. Details
have been discussed for achieving enhanced efficiency in mirror
surface machining of an X-band accelerator tube disc.
A project continuing from last year with the Institute for
Molecular Science and Nagoya University involves the grindingof MgF2 aspherical lenses using a monocrystalline diamond bit.
It is pursuing an investigation into machining conditions forpractical applications.
For the prototype production of the Microwave Kinetic
Inductance Detector (MKID) lens array, which the ATC pursues
internally, a cutting process of the 721 elements array and antireflective (AR) film coating and was successfully achieved,
advancing the project closer to testing. The fabrication of acorrugated horn array began, which works excellently in multiband communication. The goal is to complete this project at theearliest opportunity.
The ME Shop handled with 107 requests for manufacturing
or repairs in FY 2012, 16 of which were brought forward into
FY 2013. Including these cases, 123 requests were received; 116
were completed while seven cases were forwarded to FY 2014.
Eight cases were outsourced.
The following requests were received in FY 2013 (numbersin brackets are cases forwarded into FY 2014):
Brought forward from FY 2012
ATC
Subaru Telescope
HSC
TMT
Exoplanet Exploration Project
Solar Observatory
HinodeSolar-C/CLASP
ALMA
RISE
VLBI
KAGRA
Gravitational Wave Project OfficePublic Relations Center
External organizations
Institute of Astronomy, Tokyo
ISAS/JAXA
Total

16 (2)
13 (2)
31
10
14 (1)
1
2
32 (1)
11
2
2
3
4
1
8 (1)
7
1

107 (7)(2) Optical Shop
A. Regular operation and maintenance- Measurement equipment maintenance including daily
inspection

094

II Status Reports of Research Activities- Measurement-related consultations (71)
- Repairs/updating of facilities (updating the digital camera for
MM-40 microscope and replacing the laser and laser powersource of Zygo GPI™ interferometer)- Calibration of Legex 910 (January 20–24, 2014)- Recording backups of the measurement data stored in themeasurement equipment
B. Measurement instruments open use (including use in joint
research) April 2013–March 2014
- Measurement equipment use: 412
Within ATC: 145
ALMA: 9NAOJ and Institute of Astronomy of the University ofTokyo: 184
Outside NAOJ: 74- Large three-dimensional measurement device Legex 910 use: 51
The Legex 910 was utilized regularly throughout the year for a
total of 91 days.
For ALMA and HSC: 37 (by operators of each group)
Optics Shop use by request: 14(3) Optical Infrared Detector GroupThe optical infrared detector group mainly provides support
for visible light detectors. The work related to HSCʼs CCD is
gradually nearing its end, although worldwide inquiries remain
regarding the usage instructions or properties of fully depleted
CCD, which the group handled. The group also undertook
replacement/upgrading of observational instruments. This year,
it helped to upgrade the 3DII CCDs, one of the instruments
transferred for the Subaru. The activities are conducted mainly
by students of the Institute of Astronomy, University of Tokyo.
The ATCʼs work involved a range of activities, from designingof a dewar to performance tests of CCDs, and provided support
for handling the devices.
(4) Thin Film Deposition Unit
The ATC collaborated with the Institute for Cosmic Ray
Research of the University of Tokyo in the development
research of high-precision optical elements using thin-film
coating technology, a project carried over from last year. This
year, preliminary experiments were conducted on the functional
properties of the mirror and thin film that changed during
low-temperature cooling, in preparation for the mirror forgravitational wave interferometer. In a collaboration with the
Kavli IPMU, the agenda was to develop a wide-band AR coating
for the Subaru PFS; thus, the preliminary experiments were run,and equipment modification and adjustment was conducted.
(5) Space Chamber Shop
The Space Chamber workshop provides support for open
use of the vacuum chamber, clean room, and other facilities
belonging to the ATC. Some of the major results for open
use are as follows: The ATC vacuum chamber was used in
tests for the CLASP sounding rocket experiment performedby the Ultraviolet Synchrotron Radiation Facility (UVSOR)

synchrotron radiation facility, and the vacuum chamber was also
used for various vacuum experiments performed as part of thenext solar observation satellite SOLAR-C project. In addition,
low-temperature motor tests for the filter exchange mechanismof the Wide-field Imaging Surveyor for High-Redshift (WISH)
satellite were performed. Otherwise, small vacuum chambers
were nearly in constant use for outgas measurement andother tests, whereas an environmental chamber was used intemperature cycling tests for parts of observational equipment.
(6) Facility Service Unit
Because the ATC has a limited number of lab rooms,
projects are accepted according to availability. Lab capacity
continued to be below the demand level in FY 2013, and the unit
is managed with users’ understanding. The shortage was easedslightly by swapping lab rooms for different projects during theterm time.
The ATC’s experiment facilities, including the clean room,
were used in FY 2013 by the following projects or organizations:ATC, ALMA, KAGRA gravitational wave, TMT, Division ofRadio Astronomy, HSC, JASMINE, Division of Optical andInfrared Astronomy, Extrasolar planet exploration, Subaru
Telescope, Hinode Science, and Solar-C/CLASP. The clean
room 101 in the Development Building (north) is dedicated tothe development of satellites and is used for the development
projects of the small-sized JASMINE (JASMINE Project
Office), satellite Hodoyoshi 3 (Nakasuga Lab, University ofTokyo), and CLASP (CLASP/Hinode Science).
A roof of the Development Building (south) incurred awater leak due to the decay of waterproofing materials on
the roof. Because water leaks have occurred every year, theATC is considering a complete refurbishment. Moreover,the Development Building (south) underwent a lighting
refurbishment in which light sources have been replaced with
LEDs in all labs and other rooms. The work started last year
came and was completed except for that in one laboratory, where
the LED brightness was deemed insufficient; the refurbishment
work is continuing in FY 2014. The air conditioning systemin the Development Building (north) has been in use for 10
years and has started to cause some facility breakdowns. In
particular, the temperature control units failed, disabling theroom temperature controls. Therefore, the units were all updated
to newer models.
A clean booth was installed last year in a lab allocated to the
KAGRA gravitational wave telescope, and its filter unit began
to cause noise and vibration to the extent that it interfered withwork conducted in adjacent labs. The lab resumed operation
after the noise and vibration were reduced to a tolerable level
through the installation of soundproofing, repositioning ofequipment, and isolation of the vibration.
Annual inspections of cranes 0.5 ton or more are mandatedby law and are duly performed. Due to tight schedules for lab
usage, the annual inspections were conducted in two phases thisyear. Since load testing is mandatory for cranes of more than 3
tons, the 4.8-ton crane at the Development Building (north) is
scheduled to undergo testing in 2014.

Rust-induced decay found in the leg of a cold evaporator(CE) through annual inspection was handled by application of a
new layer of paint. Gas storage tanks with a capacity of 1,000 L
or more are regulated by the High Pressure Gas Safety Act,
which provides that a 20th-year pressure test is mandatory. The
tank onsite is working normally 19 years after its fabrication;
however, plans are under consideration for purchasing a new CE
and installing a liquid nitrogen gas production facility in viewof the Advanced Technology Building for the TMT, scheduled
for operation in FY 2015. Major management duties are diverse
and include mandatory day-to-day inspection and operational
management of the buildings, electrical equipment, and CE
equipment, as well as the management of clean rooms, fresh-air
treatment units for the clean rooms, private power generators,
operation of the Electrical Shop, management of chemical
substances, and disposal of used chemicals. Some contributions
were made to the architectural planning of the Advanced
Technology Building for the TMT from the viewpoint of facility
management.
Mr. Hiroshi Mikoshiba, who was responsible for facility
maintenance and management, was transferred to Nobeya Radio
Observatory in April 2013. His two-year contributions weremuch appreciated.

3. Project Support
Calls for open-use projects were held twice in FY 2013,
resulting in the ATC equipment being used for five joint R&D
projects and 27 other projects. Details of these uses are describedin the section on Facility Open Use, including the names ofproject leaders and research themes. Results of these projects areposted on the ATC website.

4. Development in Prioritized Areas(1) Development of SIS Device for ALMA
Fabrication of devices for the ALMA-specification band4 and band-8 receivers continued from last year. By December
2013, devices were provided for 73 units of receivers tobe shipped. Currently, further devices needed for receiver
maintenance are in production.
The manufacturing equipment for the new SIS element
introduced in FY 2012 underwent performance testing, anddevice prototypes were created, verifying the capacity to
produce devices in good condition. A plan is currently underdiscussion to use the equipment for developing an SIS element
for band-10 receivers and to create a prototype in terms ofpreferable conditions for manufacturing good devices.
(2) ALMA Band-4
At the production rate of 3.75 units per month, exceeding thetarget rate of three, the testing and production of 73 units wascompleted in November, and the receivers were delivered onschedule by the end of December 2013. A future task is to forma maintenance team in cooperation with the Chile Astronomical
Observatory to handle failures and breakdowns.

II Status Reports of Research Activities095

(3) ALMA Band-8
73 units of band-8 cartridge receivers (385–500 GHz)
were delivered to JAO by November 2013. Subsequently,
the ATC handled the assembly of seven spare cartridge units
and the repairs of returned units. Drawings and instructions
were collated for maintenance purposes. Preparations were
undertaken to lease the leak-rate measurement equipment to be
used for the cartridge cooling system and vacuum base plate, in
support of the mass-fabrication of band-1 receivers pursued by
the Academia Sinica Institute of Astronomy and Astrophysics(ASIAA) in Taiwan.
(4) ALMA Band-10
At the astonishing production rate of four units per month,
the testing and production of 73 units was completed by theend of December, and they were delivered on schedule by theend of March 2014. Future agendas include the formation of amaintenance team in cooperation with the Chile Astronomical
Observatory and the pursuit of receiver upgrades as well as
development of next-generation receivers.
(5) Hyper Supreme-Cam (HSC)In FY 2013, the HSC was applied to test observations forseven nights in June, five nights in October, and eight nights
in January and February 2014. Despite the high incidence ofinclement weather, conditions were sufficient to perform thetest observations roughly half of the time. The defects identified
through this observation included (a) scattering/stray light, (b)vacuum leak under extremely low humidity, and (c) partial
movement defect in CCDs. The (a) test was further investigated
and the results indicated certain light patterns due to unevenfilter permeability rather than scattering/stray light. The causeof the (b) test result was identified to be the alumited grooveon the O-ring. The (c) test is still under monitoring, and an
investigation is underway to rectify the situation by adjusting
the operational configurations. Basic performances including
image quality and system throughput were confirmed to meetthe requirements to the design. Therefore, the HSC was put toopen use and strategic observations in late March 2014. The
following tasks must be pursued in the future: (a) realizing an
auto-focus mechanism, (b) developing a detection efficiency
measurement system, (c) establishing operational stabilityof a filter replacement device, (d) addressing the CCDs withmovement defects, and (e) establishing a data analysis support
structure for open-use users.
(6) IRIS, the TMT Onboard Observational Instrument
Development is underway for an imaging system for the
IRIS, the first observational instrument for the next-generation
extremely large TMT, which began in FY 2011. Currently
at the preliminary designing stage, the IRIS system is onschedule to be submitted to external reviews in December 2014.
Work continues from last year, with ME Shop staff members
performing a leading role in prototype demonstrations ofcomponent technologies and designing the actual system basedon the prototypes, as listed below:

096

II Status Reports of Research Activities- Performance tests of a prototype Cold Stop Stage for a lowtemperature drive system- Implementation and analysis of the vibration tests using
prototype lens cells- Fabrication of prototype off-axis aspherical mirrors- Design of an actual filter-replacement mechanism- Design of an actual lens cell assembly machine- Packaging design of the actual IRIS
(7) KAGRA gravitational Wave Telescope
The development of KAGRA’s auxiliary optics and vibration
isolation systems are pursued in collaboration with the TAMA
Project Office. The development relevant to the auxiliary optics
system included the system design of KAGRA’s interferometer
against stray light and the relation baffles required. Five typesof baffles were developed, the largest of which was 800 mm
in diameter. Four types have particularly high sensitivity inconverting gravitational wave signals into light signals andwill be installed in KAGRA’s vital 3-km arms. The plan is toinstall, in the order of closer to farther from the primary mirrorof the interferometer, a wide-angle scattering baffle, a cryo-ductshield, and a narrow-angle scattering baffle. Furthermore, baffle
arrays are to be installed in the arms at appropriate intervals.
These baffles are designed to collectively keep stray lightinduced noise under 1/100 of the total noise level. The ATC ME
Shop helps with the development of the structural design andassembly methods because in countering the noise induced bystray light, careful attention must be paid not only to the baffle’s
noise absorption and scattering but also to its mechanicalstructure. The optics design is pursued primarily on the basis of
ray tracing simulations performed with the assistance of external
optics systems corporations. The vibration isolation system is a
device to be mounted on the mirrors in the KAGRA to isolatethem from vibrations and is composed of multi-strata anti-spring
filters. The ATC planned to manufacture one of the filters, anda prototype was made in FY 2013. First, the ATC’s Machine
Shop fabricated some parts of the anti-spring filter. The mostchallenging part of this task was to develop a geometric antispring (GAS) filter that combined maraging steel board springs,
a key structure for isolating vibration. However, the ATC
succeeded in establishing the process from material procurement
through fabrication to performance tuning. GAS filters were
hitherto available only from very few overseas organizations
with the capacity of material procurement and manufacturing.
The establishment of the technology and process in Japan
will serve as a foundation for future development of vibration
isolation technology in the country.
Priority was also given to the development of the main
KAGRA unit, and advanced technology development was
pursued toward improving the performance of next-generation
detectors for the KAGRA.
The ATC developed a torsion-bar antenna (TOBA), aiming
to achieve an observation of gravitational waves at lower
frequencies than those observed by the KAGRA and other large
laser interferometer gravitational wave telescopes. At present, theworld’s highest known sensitivity has been attained in the 0.1-Hz

band. R&D continues for further improvement of the sensitivity.
Also in progress is the development of a main interferometer
unit and a signal acquisition system for the Decihertz
Interferometer Gravitational wave Observatory (DECIGO)
Pathfinder (DPF), a prelude satellite for the DECIGO spacegravitational wave antenna project. Efforts were focused
primarily on the design and fabrication of the interferometer
module (BBM) for the gravitational wave sensor unit. It wasdetermined recently that residual gas surrounding the test mass
would produce noises similar to Brownian motion far more thanpreviously speculated. Therefore, an encasement was designed
to house the test mass in order to reduce such noises. The noise
generation mechanism is relevant not only to gravitational wave
observational satellites but also to terrestrial gravitational wave
telescopes such as the KAGRA. The revised noise reduction
method will contribute to the future enhancement of sensitivity
in the KAGRA and other telescopes.

5. Advanced Technology Development(1) Radio Cameras
Development of a millimeter/submillimeter microwave
kinetic inductance detector (MKID) camera is in progress. The
camera is intended for the LiteBIRD, with observation of the
B-mode polarization in the cosmic microwave background (CMB)
radiation, and for the Antarctic terahertz telescopes. A millimeter
microwave 700 pixel MKID camera was developed with an
integrated silicone lens array. Further design was developed by Mr.
Tomu Nitta and others in 2013 to increase the lens array density toachieve 2,000 pixels. An AR coating for a silicone lens array wasdeveloped, a mix of two types of epoxy resins was applied, andthe thickness was optimized by post-application machining thesame group in 2014. Also pursued were the development of a lowtemperature wide-angle optics system (1.0°) to connect the highresolution camera and the telescope and prototyping of the 0.1 K
cooling system. These advancements were reported in a PhD
thesis by Mr. Tomu Nitta, University of Tsukuba, and an masterʼsdissertation by Mr. Shigeyuki Sekiguchi, University of Tokyo.
A high-speed dual-element Fast Fourier Transform (FFT)
circuit for MKID readout was developed and tested against asingle-element readout circuit by Dr. Kenichi Karatsu and others
in 2014, the results of which verified the formerʼs sufficiently low
noise level.
The development of the superconductive imaging
submillimeter-wave camera (SISCAM), using an SIS ray
detector and a gallium arsenide field-effect transistor (GaAsJFET) ultra-low-temperature integrated circuit (IC), proceeded
to the construction of a system to automatically control the
32-channel readout circuit module, which was performed to attainan extraction of parameters for optimal motion conditions bychannels. Y. Hibi and others reported the testing of the integration
with the detector and 32-channel module movements in 2013.
(2) Space Optics
Activities to observe astronomical bodies from the outerspace are pursued by using rockets and artificial satellites

to facilitate the realization of future space projects. In FY
2013, foundational development was furthered toward theimplementation of the CLASP rocket test project and thesatellite projects of the WISH and Solar-C. As part of the
WISH project, which involves observations in the near-infraredband, drive tests were performed for a low-temperature motor
for the filter exchange mechanism under a low-temperature
vacuum environment. Because the CLASP project seeks toperform magnetic field observation of the Solar chromosphereand transition region via hydrogen Lyman alpha spectrum,
observational instruments were developed and a calibration test
apparatus was conducted in preparation for flight tests in FY
2015. In the second half of FY 2013, a temporary assembly of
the flight model also began.
Also in FY 2013, the testing of prototypes and prospective
flight models of optical elements was conducted usingsynchrotron radiation. For this testing, the ATC transferreda measurement system developed onsite to the Institute for
Molecular Science. In addition, resources at the ATC were
mobilized to conduct various tests to verify the capacity anddurability, in a mechanical environment, of the slit unit andthe component products developed for the slit-jaw optics
system in the CLASP polarization spectrometer; the rotational
uniformity of the rotating wave plate drive mechanism, which iscurrently under development for use in flight; and contamination
evaluation monitoring observation, among other things.
In relation to the Solar-C project, optical performance tests
were conducted on the optical integral field unit (IFU) using fiber
optic bundles and an image slicer model utilizing the reflective
field. Both were developed during the foundational developmentof the polarizing spectrometer. Progress was also made in the
preparations for low-temperature performance tests of the nearinfrared sensor in order to develop a near-infrared camera.
(3) Development of Near-infrared and Visible CMOS Image Sensors
Image sensors for astronomical observations must maintaina low noise for detecting very subtle light, whereas readout ICs
for consumer use presuppose high-speed readout, which makes
it difficult to achieve a low noise level. Herein lies the necessity
to develop an IC optimized for astronomical observations.
This year, the ATC participated in the Silicon on Insulator(SOI) Pixel Sensor Project pursued by the KEK, and produced aprototype of a visible complementary metal-oxide semiconductor(CMOS) image sensor based on the low-noise readout IC
previously fabricated as a test piece. The SOI technology has
enabled achievement of high sensitivity in the near-infraredband, which was hitherto unattainable by conventional CMOS
image sensors. Si semiconductor detectors do not detect nearinfrared. For the near-infrared image sensor to compensate forthis limitation, the indium gallium arsenide (InGaAs) image
sensor marketed by Hamamatsu Photonics was evaluated. In
addition, the ATC undertook the assembly of quantum efficiency
measurement equipment and pixel sensitivity distribution
measurement equipment to be deployed in the testing of thesenear-infrared image sensors.

II Status Reports of Research Activities097

18. Public Relations Center
1. Overview

3. Public Relations Office

The Public Relations Center engages in the publication,
promulgation, and promotion of scientific achievements
made not only by the NAOJ but and by others in the field ofastronomy in general to raise public awareness,; to respondto reports of discovery of new astronomical objects,; and toprovide ephemeris and other astronomical information more
directly relevant to people’s everyday activities, such as sunrise
and sunset times. The Center center is formed of six offices andone unit: including the Public Relations Office, the Outreachand Education Office, the Ephemeris Computation Office, theMuseum Planning Office, the Library Unit, the Publications
Office, and the General Affairs Office. The activities of each
office will be reported hereafter.

The Public Relations Office actively promoted scientificdevelopments yielded through various projects conducted by the
NAOJ, including the Chile Observatory, the Subaru Telescope,
the HSC, the Extrasolar Planet Detection Project, and theNobeyama Radio Observatory. It also promoted the results of joint
research projects conducted with universities and other researchorganizations through press conferences and web releases. In
cooperation with the Outreach and Education Office, the Public
Relations Office also ran awareness campaigns on meteor showers
and other astronomical phenomena of interest to the public.
Social networking services such as Twitter and Facebook
have proven to be valuable new tools in sharing information.

2. Personnel
The Public Relations Center was served in FY 2013 byDirector Toshio Fukushima and the following staff members:
two professors, one associate professor, two assistant professors(one holding a concurrent post), four research engineers, one
senior engineer, one engineer, one chief of the library, four
research experts (one holding a concurrent post), 20 Public
Relations and Outreach staff members, two research associates,
and two administration associates. The following members
joined the center:
Yuriko Watanabe, Public Relations and Outreach staff(Outreach and Education Office), April 1, 2013; Tamami
Yamaguchi, Public Relations and Outreach staff (Outreachand Education Office), and Lundock Ramsey, research
associate (Public Relations Office), June 1, 2013; Kumiko S.
Usuda, research expert (Museum Planning Office), July 1,
2013; Naotsugu Mikami, Public Relations and Outreach staff(Public Relations Office), August 1, 2013; Yasuhisa Shioya,
Public Relations and Outreach staff (Public Relations Office),
September 1, 2013; and Osamu Okoshi, Public Relations andOutreach staff (Outreach and Education Office), January 10,
2014. Outgoing staff members included Takuya Okawa, Public
Relations and Outreach staff, on May 31, 2013; Akira Hirai,
Public Relations and Outreach staff, and Tamami Yamaguchi,
Public Relations and Outreach staff, on December 31, 2013.

Month
April 2013
May 2013
June 2013
July 2013

Access counts
412,619450,406
427,197519,303(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.
NAOJ e-mail newsletters Nos. 103–128 were issued,
containing headlines of 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 thestatus of various NAOJ projects such as open house events andregular observation sessions at the Mitaka Campus and position
openings. More than 35,000 followers were counted at the endof March 2014.
(2) Publicizing developments
Information releases were actively presented, totaling 26
articles (Tables 2, 3).
As part of the Astronomy Lecture for Science Journalists,
the 19th lecture theme was “Comets: fascinating facts,” and the20th was “Mapping the Universe.” The lectures were streamed
over the Internet for journalists only. The lectures were also
recorded to be viewed by journalists who missed the event andalso by those journalists who attended and wish to review thematerial. The system is proving to be successful given the factthat more real-time viewers over the Internet were counted than
the number of participants onsite at the 19th lecture.

Month
Access counts
August 2013
1,335,182
September 2013
612,646
October 2013
818,752
November 2013
1,560,285
Total: 8,505,648

Month
December 2013
January 2014
February 2014
March 2014

Access counts
917,320
634,935
364,096452,907

Table 1: Monthly website access statistics on Public Relations Office website, NAOJ Public Relations Center (April 2013–March 2014).

098

II Status Reports of Research Activities

April 23, 2013

Ubiquitous infrared polarization in the star/planet-forming region and life homochirality

May 7, 2013

Completion of the installation of 16 Japan-made parabolic antennas for the ALMA telescope, at the Array Operations Site

May 31, 2013

'Population poll' of the galaxies behind dusts

June 4, 2013

Japan commences mainstream construction work on TMTJune 7, 2013

The ALMA discovers a comet crib

June 12, 2013
August 9, 2013
August 23, 2013

Sunny super-Earth? First successful observation of the atmosphere of a low-mass exoplanet GJ 3470 b
Success in a velocity measurement of the supernova shock wave traveling through interstellar molecular cloud

September 4, 2013
October 4, 2013
October 10, 2013
October 23, 2013
November 5, 2013
November 11, 2013
November 15, 2013
November 18, 2013
November 22, 2013
December 6, 2013
December 6, 2013
January 17, 2014
January 28, 2014
March 4, 2014

The sky of the super-Earth in blue light
The ALMA telescope discovers giant hot cocoons surrounding a baby star
Urbanite massive black hole: 'observational' results from VO
Comet ISON viewed via the Subaru telescope
Population poll of asteroids on inclined orbital plane[Breaking News] Comet ISON and comet Lovejoy reveal nuclei, captured by the Subaru telescope
Seven NAOJ Mitaka properties registered as tangible cultural heritage[Breaking News] Ultra wide-field prime focus camera, High Suprime-Cam captured long tail of the comet ISON
[Breaking News] Subaru telescope investigates the comet ISON after luminous increase
Marching to the Beat: Subaru's FMOS reveals the well-orchestrated growth of massive galaxies in the early Universe[Breaking News] The Subaru telescope reveals the detailed structure of Comet Lovejoy's tail
ALMA discovers a formation site of a giant planetary system
Subaru telescope scrutinizes active supermassive black holes revealed in merging galaxies
Origins of massive objects: Hot steam gas disks discovered around massive stars

Star nursery gently wrapped in dust particles

Table 2: Web releases.

May 27 and 29, 2013
July 31, 2013
August 5, 2013
February 20, 2014

Go! The world's fastest astronomical supercomputer
Consummation of the brand-new ultra wide-field camera-the first light image
Subaru telescope's imaging discovery of a second Jupiter shows the power and significance of the SEEDS project
Subaru telescope detects rare form of nitrogen in comet ISON
Table 3: Press Conferences.

(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: In tandemwith the full commencement of the large-scale project of TMT
construction, the center helped to revamp the website of the
TMT. In response to the JASMINE Project Office’s request
to boost PR activities for small-sized JASMINE project, thecenter rendered support in creating new pamphlets as well asplanning and conducting lectures for science journalists. Help
was also given to the project’s own lectures for the generalpublic, from preparation to organization. In particular, creating
an application form for online pre-registration and developing
lists of applicants have become standard practices for the Public
Relations Office.

4. Outreach and Education Office(1) Handling general inquiries
Inquiries were made by the media, governmental offices,and the general public. The Outreach and Education Office
responded to 7,094 telephone inquiries (Table 4) and 127 letters,
79 of which were official documents. The office also received
326 inquiries via the Internet (Table 5).

(2) Educational and Outreach Activities
The astronomical phenomena campaigns, which werebidirectional information-sharing initiatives, began in FY 2004.
Two events were organized this year: “Perseid Meteors 2013” inAugust 2013 (with 1,312 reports), and “Let’s Go Out and Find
the Comet ISON” in November (with 1,963 reports).
The “Fureai (Friendly) Astronomy” project, in its fourthyear, provided events to 47 schools, covering all that applied,with 4,865 pupils in attendance. Many feedback responses fromthe pupils expressed their interest in seeing stars or aspiration
for becoming astronomers, suggesting that the event was a good
opportunity to familiarize the children with astronomy and to
inspire them by meeting and learning from astronomers. Fortytwo lecturers participated.
The Summer Vacation Junior Astronomy Workshop wasorganized jointly with the “You are Galileo!” project on July
25 for elementary, junior high, and high school students.
Enrollment was necessary, and 40 places were offered. Nearly
80 people participated, including accompanying adults, andenjoyed handcrafting telescopes with instructions on how to
use them. Concurrently, lectures were delivered on the themeof the “You are Galileo!” project and astronomical phenomenain the summer sky. An additional observational event “Summer

II Status Reports of Research Activities

099

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

Solar info Lunar info Ephemeris info
248
104
58
207
206
54
257
140
41
233
129
71

Time
22
8
14
11

Solar System Universe
178
78
299
102
658
106
165
66

Astronomy
117
149
112
101

Other
790
1021
766
583

Total
1595
2046
2094
1359

Table 4: Telephone inquiries made to the Public Relations Office of the NAOJ Public Relations Center (April 2013–March 2014).

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

Solar info Lunar info Ephemeris info
11
4
1
4
5
1
3
3
2
2
7
2
20
19
6

Time
2
2
1
0
5

Solar System Universe
13
7
13
21
29
14
4
18
59
60

Astronomy
21
29
34
18
102

Other
20
14
7
14
55

Total
79
89
93
65
326

Table 5: Internet inquiries made to the Public Relations Office of the NAOJ Public Relations Center (April 2013–March 2014).

Vacation Junior Star-Gazing Party” was offered free to the public
on July 25 and 26. Weather conditions were disappointing,however, leading to participation by 191 people including 64 on
the first day and 127 on the second.
The Public Relations Center participated as the secretariat
for the Mitaka Open House Day, a special public event held at
Mitaka and organized by the steering committee. This two-day
event was held on October 18 and 19 with the theme “Explorationof the roots of galaxies and planets through ALMA Telescope.”
It was co-hosted by the Institute of Astronomy, School of
Science, the University of Tokyo, and the Department of
Astronomical Science at the School of Physical Sciences of the
Graduate University of Advanced Studies. Despite the inclement
weather on both days, the event was successful, attracting a
total of 4,176 visitors. The success was owing to the effective
consideration of each project’s program, achieving the same
number of visitors as that in the previous year. The event catered
to a wide range of age groups and offered viewing of facilities
not open normally to the public, interactive panel displays, minilectures, and popular quizzes and games.
The fourth International Science Film Festival was coheld 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 59 science
museums, planetariums, and film theaters in Japan, with morethan 1 million people participating. The central events were heldin the forms of a kick-off event (National Museum of Emerging
Science and Innovation), a science film cafe and workshop(Science Museum), a science film cafe and Riken Day (Science
Museum), and Dome Festa (Hitachi Big Theater).
The annual event “Star Week: Getting to Know the Starry
Sky” was presented during the first week of August, with theparticipation of 83 astronomy-related facilities providing 133
collaborative events.
The “Astronomy for Beginners” co-hosted every year with
the Tamarokuto Science Center was held on December 1 andconsisted of a lecture on comets, sunspot observation in the oldequatorial telescope dome, and a regular guided tour around thefacilities, with a total of 40 visitors enjoying their experience.

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The NAOJ Research Conference, “The Second Conference
on Universal Design for Astronomy Education” was organized
and co-hosted by the Japanese Society for Education and
Popularization of Astronomy on September 28 and 29 at the
Mitaka headquarters. Participation from a diverse culture wasachieved, from people engaging in promulgation of astronomy
education to those with disabilities and their supporters, for a
total of 124 individuals. Among the participants, eight werevisually impaired, 14 were hearing impaired, and one required
the use of a wheelchair. To ensure that information was madeavailable to participants with disabilities, Information andCommunication Media Support was provided in the formsof resources in Braille, sign language interpreters, and a PCenabled note-taking system in which the essence of remarks is
inputted via PC and projected onto a screen.
The Ninth Workshop for Popularizing Cutting-Edge
Astronomy was held at the Kavli IPMU from November 17 to
19, with the main theme of cosmology. A total of 75 researchersand people engaging in education or promotion of astronomy
took part.
The “You are Galileo!” event was organized jointly with
the Office of International Relations and was held on March 2,
2014, at the Royal University of Phnom Penh, Cambodia. Withroughly 100 educators and university students in attendance,
the event included lectures, handcraft workshops to maketelescopes, and celestial observation. For the event, 22 sets oftelescope assemblies with tripods and one 10-cm equatorialreflecting telescope were donated for local use.
Makali’i image analysis software, developed for the purposeof applying FITS data obtained through the Subaru telescopeand other research observations to astronomical educationand outreach initiatives, is distributed by the Public Relations
Center in Japan and overseas via the Internet. The poster “Onein every home: Diagram of Our Universe 2013,” available in
A1 and A2 sizes in Japanese with English on the reverse side,
was transcribed to web pages in Japanese and English following
its publication last year. A new poster “The Solar System,”available in A1 and A2 sizes in Japanese only, was also createdin collaboration with the PCOST.

(3) Community activities
In FY 2013, 37,187 visitors were welcomed at the “Mitaka
Picture Book House in the Astronomical Observatory Forest,”
which opened on July 7, 2009, based on the Agreement on
Mutual Cooperation concluded between the NAOJ and the cityof Mitaka on February 4, 2009. Along with joint projects suchas the “Ohisama Ippai (plenty suns)” exhibition held from July
2011 through June 2012 and the “Uchuu de Ikiteru (living inspace)” exhibition held from July 2012 through June 2013, theOutreach and Education Office engaged in events at the Mitaka
Picture Book House in the Astronomical Observatory Forest,
including modern and traditional Tanabata celebrations andmoon-viewing parties, in cooperation with staff members fromthe municipal office of Mitaka City and local volunteers.
The event “Astronomy Pub” has been held at Mitaka
Network University and hosted by the non-profit organization(NPO) Mitaka Network University Promotion Organization
since FY 2009. It provides for 20 participants at a time and isheld in the evening on the third Saturday of every month except
August. The Public Relations Office also assisted in presenting
Star Sommelier Mitaka, an astronomical guide training course
hosted by Mitaka Network University that provides telescope
operation workshops and other related events.

5. Ephemeris Computation Office
The Ephemeris Computation Office estimates calendarrelated phenomena such as the apparent positions of theSun, Moon, and stars on the basis of international standards
and publishes the “Calendar and Ephemeris” as part of thecompilation of almanacs, which is one of the NAOJ’s raisonsd’être.
(1) The office published the 2014 edition of the Calendar andEphemeris, the 2014 version of the calendrical section of the
Rika Nenpyo, and the 2015 edition of the Reki Yoko (posted
in the official gazette on February 3, 2014). The web-based
Calendar and Ephemeris adopted the IAU WG Cartographic
Coordinates and Rotational Elements (CCRE) Report 2009 forplanetary axis of rotation to display a visual radius (excluding
light penetration) on the solar-centric coordinates and a polar
visual radius on the planet-centric coordinates.
(2) The website (http://eco.mtk.nao.ac.jp/koyomi/) published
EphemerisWiki-Tonight’s Sky powered by Google Maps,and various tools were updated to Google Maps v3. New
arrangements were made to the Today’s Sky, in tandem withannual events and campaigns, to display positions of various
objects such as Comets Lemmon, ISON, Lovejoy and Encke;
Nova Delphinus 2013/Nova Centauri 2013; and radiant points ofthe 2013 Perseid meteor shower/2013 Geminids meteor shower.
As a result, the total access in FY 2013 reached 32 million hits.
(3) The Japan Association for Calendars and Culture Promotion
hosted its third General Meeting and a Calendar Presentation
Ceremony. The office also took part in the selection committee

for the Best 36 Words of the Season, hosted by the Japan
Weather Association, and published the results.
(4) The office hosted regular exhibitions in collaboration withthe library, selecting from the NAOJ’s invaluable collection ofancient archive in the Chinese/Japanese languages. The themesof the 48th and 49th exhibitions were “Tides” and “The Moon
and Ephemeris,” respectively. These exhibits can also be viewed
at the Rare Book section 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 two parttime, handled reports of new astronomical objects and othercommunications submitted to the NAOJ. This year, 20 reports
were made including new object discoveries, verification
requests, and others. Of these, seven were about new stars or
supernovae, eight were on comets or comet-like objects, twowere on fireballs, one was about planets, and two were on
luminous objects.
Amid the many false alarms attributed to known supernovae,
comets, ghost images of bright stars, and the like, a discovery
of a supernova reported in July was relayed via the NAOJ
to the IAU Central Bureau for Astronomical Telegrams. The
reporter was subsequently recognized as the sole discoverer ofSupernova 2013dy.

6. Museum Project Office
In FY 2013, the open house initiative team was reorganizedfrom the Outreach and Education Office into the old Archive
Office and was renamed as the Museum Project Office. Due tothe nature of the work involved, some parts of the activities wereconducted jointly with the Outreach and Education Office.
(1) Open House events
As in previous years, regular semimonthly screenings were
held at the 4D2U Dome Theater on an advance booking basis
for the second and fourth Saturdays of the month. A total of 22
sessions were held with 1,893 audience members. Moreover,69 group screenings were held with 2,143 participants, and 59
tours were organized, attracting 635 visitors. The grand total forthese events at the 4D2U Theater was 150 sessions with 4,671
viewers.
Annual observations featuring the 50-cm telescope for public
use were organized concurrently with the 4D2U Dome Theater
open house events, regardless of weather conditions. Advancebooking (300 places for each session) was introduced in FY
2012 for these events. A total of 22 sessions were held with 4,740
participants. The Mitaka open house events held throughout
FY 2013 had 18,552 visitors. Including workplace visits, 147
group tours were conducted with 5,828 visitors in FY 2013, and284 media interviews were granted. Guided tours of the Mitaka
campus began in June 2011 as part of the Archive Office/OpenHouse initiative. Each tour is conducted on an advance booking
basis with a group of 20 participants. Tours are organized in two
courses: the Registered Tangible Cultural Heritage course on the

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first Tuesday and second Sunday of the month and the Important
Cultural Heritage and Geodesy-related Sites course on the third
Tuesday and fourth Sunday. The office welcomed 469 people forthe tours, and participants expressed their enjoyment.
(2) Planning Museum and Managing Archive
The Museum Project Office engaged in collecting andorganizing historically important observational and measurement
data and equipment for preservation. Improvements on thepreservation and display methods were discussed, and thefounding principles and organization of the NAOJ Museum(tentative name) were formulated. The Mizusawa and Nobeyama
joined discussions for the preparation of the museum concept.
Three meetings were held at respective campuses this year,
and various requests and present circumstances of these bases
were heard. The City of Mitaka made seven applications forregistering the architectural properties at the NAOJ Mitaka
for tangible cultural heritage and received responses fromthe committee on November 15. The Mitaka is now home to
10 cases of registered tangible cultural heritage items. A plan
to engage volunteer guides on the NAOJ premises is underconsideration in order to respond to an increasing demand forgroup tours and guided tours. The office gave support to the
NAOJ Guide Volunteer Training Course organized by the NPO
Mitaka Network University Promotion Organization, which
was completed by nine people. Preparations are underway tocommence guided tours conducted by these trained volunteers
next year. The Astronomical Society of Japan Spring Meeting2013 offered a program of lectures titled “The History of
Astronomy: Collection of Historical Resources and Survey.”
During the two-day event, 25 lectures were scheduled with morethan 60 participants each day, revealing the popularity of thisarea of interest among researchers.
Function restoration work was performed on the Solar Tower
Telescope as part of the fourth-year execution of the annual
NINS president’s discretionary budget. The coelostat mirror
and primary mirror were depositioned, followed by a successful
solar light introduction. Seismic isolators were installed for the
display cases exhibiting lenses and glass objects. In addition,
dehumidifiers with capacities appropriate for the exhibition
rooms were installed to improve in-room conditions for theexhibits. For visitor reception improvements, a visit guide
was prepared in Braille, and on-site explanation displays werereviewed for the Braille parts. An introduction movie was also
created.
Preparations are underway for requesting an equipment
upgrade for the 4D2U Dome Theater from the budget in FY
2014 in addition to a budgetary request for the Museum Project.,

7. Library Activities
Along with its regular work in collecting and organizing
academic journals and literature on or related to astronomy
for internal and external students and researchers, the library
digitized rare documents in FY 2013 and made the data
accessible to the public. The library also organized and released

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an archive catalogue covering the period between roughly thelate 19th century and the early 20th century. It also engaged
in inspecting its collections and compiling an inventory andresource data. The library publishes a volume of literarycollections and types of journals held at the Mitaka Library andother NAOJ observatories, together with the current status of
NAOJ’s ongoing publications, in the publications of the NAOJ.

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, Nos. 237–248 (April 2013–March 2014)- Annual Report of NAOJ Vol. 25, Fiscal 2012 (Japanese)- Annual Report of NAOJ Vol. 15, Fiscal 2012 (English)
The office also continued its efforts in improving the NAOJ
News content. In particular, strategic PR promotion of various
projects, which were fully activated in FY 2012, was realized inincreased printing volumes, with six projects as main features tofurther promote these projects including ALMA in May issue,
TMT in June, CfCA in August, HSC in November, and Subaru
in December, as well as KAGRA in the February 2014 issue.
The office will continue its efforts in close collaboration withother offices to produce integrative, supporting articles so that
the NAOJ News content will be shared and used creatively byeach project to promote them in PR. The Publications Office isalso pursuing the planning stage of an idea to develop NAOJ’s
comprehensive PR/educational materials and its base platformby re-editing materials and articles published by the office,including NAOJ Pamphlets, Annual Reports, and other content
of NAOJ News. Other publications included the 2014 ALMA
Telescope calendar, which featured images captured by thetelescope; this edition was the ninth since its first production in2005. The office also helped to create the poster for the Mitaka
Special Open House Event again this year, and support wasalso given to the publication of Rika Nenpyo, a chronologicalscientific table. As part of the initiative to digitize publication
content, the office developed a new e-book platform thatallows for seamless content viewing by smartphones andPCs. Digitizing back publications and reorganizing them into
electronic content are tasks for the future. The Publications
Office will pursue dual-channel data dissemination of prints andInternet-based media.

19. Division of Optical and Infrared Astronomy
1. Overview
The Division of Optical and Infrared Astronomy oversees the
Okayama Astrophysical Observatory and the Subaru Telescope(Project C); the TMT Project Office and the Gravitational Waves
Project Office (Project B); and the JASMINE Project Officeand Extrasolar Planet Detection Project Office (Project A). The
primary purpose of the division is facilitating and invigorating
projects and individual research through personnel exchanges toplace researchers in environments more suitable for their individual
projects. While pursuing seminal observational and developmental
research, the division furthers these goals to launch new projects
as necessary. The division also actively engages in graduate
education efforts to foster next-generation talents. These activities
are based on the concept that the Division of Optical and Infrared
Astronomy is a center for personnel exchange between the Subaru
Telescope facility engaging in open use, and universities andresearch institutes in Japan, focusing on developmental research
into new instruments and observational research. This concept
was developed when the Subaru telescope was constructed.
Almost all NAOJ members in optical- and infrared-related
fields have positions at the division and engage in either thedivision or Projects A, B, or C. They may also have concurrent
positions in at times 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 2013 consisted of two professors, one associate professor,
three assistant professors, and five JSPS research fellows.
The division coordinates educational, research, andadministrative activities for all research divisions and projects
except for the TAMA and JASMINE projects. The TMT
project has come to an expansive stage in which the telescope
fabrication has been started. Personnel transfer often occurs
within the Optical and Infrared Astronomy Division in tandemwith this progress. The division plays an increasingly importantrole in coordinating between the Subaru Telescope and TMT
projects. The division as a whole maintains and operates
facilities as auxiliaries to research such as mailing lists and web
servers, for various optical- and infrared-related projects suchas the Subaru Telescope, TMT, Extrasolar Planet Detection,
TAMA, and JASMINE.
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 activities of projects that
support open use.

2. Observational Research(1) Observational Research Using Various Types of Telescopes
Observational research utilizing the Subaru telescopefocuses on a wide variety of fields such as cosmology, galaxy
formation and evolution, the formation of stars and planets, thestructure and evolution of the Milky Way, stellar spectroscopy,

objects within the Solar System, structures around late-typestars, and the search for exoplanets. In addition to observationsof the Comets ISON and Lovejoy, research was conductedon star formation in the Virgo Cluster and the ionization ofgas ejected from galaxies. The search for extrasolar planets
continued using direct imaging methods.
Research in other areas is also in progress, including
astronomical phenomena based on old ephemeris and otherdocuments and statistical research using astronomical archive
data and the astronomical database, with a focus on AGN, or
automatic identification and mechanical classification of galaxies
treated as the important data.
As part of research using astronomical archive data,
quantitative comparison research on photometric zero-points
between the publicly available Subaru Deep Field/Subaru XMM
Deep Field (SDF/SXDF) catalogs and the SDSS catalog was
also performed. Another research undertaken was on the hostgalaxy 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 low-ionization
nuclear emission regions (LINERs) was conducted alongwith Korean researchers. The site survey in western Tibet for
constructing a telescope also 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, implemented hardware andsoftware improvements for direct imaging and observation of
protoplanetary discs, and participated in the development of thenext-generation Extreme AO and a new coronagraph. In relation
to the data archive, the division joins the file-system-based
technology WG convened by the Society of Scientific Systems
to explore the possibilities for overcoming difficulties arisingfrom storage expansion, thus enhancing storage usage.

4. Operational Support for the Subaru Telescope
The Division of Optical and Infrared Astronomy offers
support for the open use of the Subaru telescope. This includes
organizing open calls for open-use programs, program
selection, administration, and management of open-use-related
travel expenses, and promoting PR activities for the Subaru
telescope. The division also gives support to the managementof data analysis systems in collaboration with the Astronomy
Data Center. Moreover, the division also supports the Subaru
Spring/Autumn Schools co-hosted with the Subaru Telescope
facility and the Astronomy Data Center, and Subaru telescopeobservation classes.

II Status Reports of Research Activities

1035. Research Environment Maintenanceinstruments and TMT succeeding the Subaru telescope.

The division manages the printers and rented multifunction
photocopiers in the Subaru Building, teleconferencing systems
on the second and third floors, sub-networks, and data backup
servers for the Subaru Office as part of its efforts to maintainthe research environment. In connection with the discontinued
support for Windows XP, the office gave assistance in the OS
upgrade to Windows 7. The teleconferencing system was also
due for an upgrade because the service for the previous model
was terminated. Currently, the Internet server is also undergoingan upgrade. Further, the division took a leading role in the
response to an unauthorized access incident that occurred in
January 2014.

7. PR, Outreach, and Discovery of New Astronomical
Objects

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

The division cooperates with the Public Relations Centerin supporting PR/outreach activities such as publication of andpress conferences on the Subaru telescope research results anddiscoveries of new astronomical objects. An active participant ina special public event held at Mitaka (Mitaka Open House Day),
the Division of Optical and Infrared Astronomy provided minilectures and exhibits and planned projects appealing to elementaryand junior high school students such as magnet puzzles.

8. Educational Activities
The Division of Optical and Infrared Astronomy provides
postgraduate education to 26 graduate students from the
Graduate University of Advanced Studies, the University ofTokyo, the Tokyo University of Agriculture and Technology,
Nihon University, and other organizations.
Division staff members gave active contributions toseminars and self-directed studies. The division participated in
the “Fureai Astronomy” project, providing pupils at elementaryand junior high schools with opportunities to be familiarized andappreciate astronomy, dispatching lecturers to various schools
around the country.

20. Division of Radio Astronomy
The Division of Radio Astronomy oversees the Nobeyama
Radio Observatory, Mizusawa VLBI Observatory, RISE Lunar
Exploration Project, and Atacama Large Millimeter Array(ALMA) in Japan; scientists and engineers of these projects
are attached to the Division of Radio Astronomy. The division
coordinates radio astronomy research between these radio
astronomical projects. The respective project report shows details
on the lastest status and research results of each project. Keywordsof scientific research in the Division of Radio Astronomy are Big
Bang, early Universe, galaxy formation, black holes, galactic
dynamics, star formation, planetary system formation, planetsand satellites, the Moon, the material evolution in the universe,
and the origin of life as the ultimate theme and so on. Radio
astronomy unravels mysteries and phenomena of the universe by
studying pictures taken at radio wavelengths invisible to humaneyes. Details of each research result are reported in sectionsof these projects and the Scientific Highlights. The Radio
Astronomy Frequency Subcommittee is established within thedivision, engaging in discussions on protection against artificial
interference generated by electrical equipment, which causes
major obstacles in radio astronomical observations.

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1. Radio Astronomy Frequency Subcommittee
The mission of the Radio Astronomy Frequency
Subcommittee is to protect the environment for radio
astronomy observations. Karl Jansky of the US in 1932 first
discovered radio waves emitted by astronomical objects, albeit
accidentally. Since then, dramatic advances have been madein radio observation methods, showing us new perspectives of
the Universe that differ from those obtained through opticalobservations. Just as optical pollution from artificial lightsources is an obstacle in optical observation, artificial radio
interference generated by electronic devices which surround us
is a major obstacle in radio observations.
Breathtaking advancement has been achieved in wirelesscommunication technologies in recent years, and wirelesscommercial products such as mobile phones and wireless LANs
are ubiquitous. Television broadcasting services have also
shifted into digital, providing various nice features. The areas ofradio applications will further expand in the future owing to its
efficiency: the wide and flexible applicability of this useful andfinite resource. Therefore, further efforts will be necessary for
maintaining the sky for better radio astronomy observations.

(1) Role and Organizationation
The purpose of the Radio Astronomy Frequency
Subcommittee is to ensure that radio astronomical observations
are free from artificial interference and to raise public awarenessof the importance of the protection activities. Radio astronomical
observation does not emit radio waves; thus, it does notinterfere with other wireless communications. A proactive
approach is needed to widely raise awareness of the efforts
to protect the environment for radio observations. Regularexplanatory sessions are provided at the Ministry of Internal
Affairs and Communications (MIC) and regional Bureaus of
Telecommunications to solicit appreciation of the importance ofprotecting the field.
The mediation between the community of radio astronomy
and commercial wireless operators is led by the MIC within
Japan and internationally by the ITU Radiocommunication
Sector (ITU-R) of the United Nations. As part of theactivities for FY 2013, the subcommittee took an active role
in representing the Japanese community of radio astronomy
researchers on various occasions in these mediation efforts.
The subcommittee is composed of members from the NAOJ
and representatives of universities and research institutes inJapan.
(2) Current Challenges
In order to handle issues of interference, the Radio
Astronomy Frequency Subcommittee remains responsive to
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 that users are licensed
because it operates in low-level, though its bandwidths is wide.
- 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 as the wireless business varies widely dependingon the frequency band used. Fortunately, radio astronomy
observations have been given priority in a number of frequency
bands under the ITU Radio Regulations (RR). However,negotiations will be necessary between the radio applicationand the radio astronomy if the same priority level is to beshared within certain band. Radio astronomy observation
involves detection of extremely faint radio waves from distantastronomical object. Terrestrial radio waves, even extremely
faint and unwanted waves, can have a substantial adverse effecton radio astronomy observations.
Sources of interference that need to be addressed continue
to increase and include the following devises and systems: the23 GHz CATV wireless connecting system in emergency, whereammonia observations are affected; 21 GHz next-generation

satellite broadcasting, where water maser observations areaffected; 1600 MHz emergency satellite mobile phones, where
the observation of pulsars and the like are affected; and anumber of new UWB wireless applications used by logistics
and manufacturing industries, where geodetic observations areaffected; and high-speed power line communications (PLC),
where decameter-band observations are affected.
(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 the 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 inopinion-forming through its regular attendance at the Asia/
Pacific Region (APG) meetings in preparation for WRC-15, asa delegate representing Japan. In FY 2013, the subcommittee
pursued the protection of radio astronomy frequency bands
through the participations in the ITU-R WP7D meetings heldin Geneva in June and September and the APG meeting held inAustralia in June 2014, in addition to other relevant meetingsand conferences.
(4) Activities in Japan
Two major domestic activities were pursued by the Radio
Astronomy Frequency Subcommittee: participation in various
committees hosted by the MIC and with MIC’s authorization
direct negotiations with wireless operators who generate radio
interference. Negotiations with the interference sources represent
a major part of the subcommittee’s activities in Japan.
The committee hosted by the MIC organizes domestic
tactics in preparation for international conferences, preparing
Japan’s positions on various wireless issues. Other MICrelated meetings provide opportunities for discussing the radio
application technologies concerning the MIC’s wireless policy,
and for negotiating with wireless operators on interference issues
under MIC authorization. Negotiations directly affecting theprotection of radio astronomy observations have been conductedconcurrently up to the interference problems in regard to societal
and technological trends.
Several examples of the interference problems discussed in
the section (2) above are given below.
One example is the advent of UWB wireless applications,used in positioning and tracking material flow in manufacturing
and logistics industries. The applications in the UWB frequency
band induces interference in VLBI geodetic observations todetect movement of plates in plate tectonics. Although thisII Status Reports of Research Activities

105

band is not under RR protection, it is vital from the perspectiveof predicting earthquakes and is the subject of special
consideration by the MIC. For 24-GHz automotive radars, newregulations have been prepared to make an automatic turnoff function a mandatory standard feature so that the device
is disabled upon reaching areas at certain proximity to radio
observatories. A wider scale of the distribution is predicted
for 76-GHz and 79-GHz band automotive radars, which are
currently under development status. 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
and other molecules in insterstellar matter. This 45-m telescope
located in Japan carries its significance in relation to the ALMA
international project, 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 orderto reach a mutually acceptable 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
under 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 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.
A new radio wave application is being planned for 21 GHz
next-generation satellite broadcasting with a picture resolution
16-fold higher than that of the current HDTV. This band is nearthe 22 GHz radio astronomy band, which is important for water
vapor observation. Because the radio signals from the satellite
approach the ground from outer space, their detrimental effects areeasily anticipated. PLC utilizing home power lines affects radio
astronomy observations in low-frequency bands below 30 MHz. A
petition against unduly hasty introduction of PLC was submitted
to the MIC jointly with the ASJ and the Society of Geomagnetismand Earth, Planetary and Space Sciences. A press conference wasorganized to raise broad public awareness of the relevant facts.
Moreover, the subcommittee engaged in making applications
to the MIC, requesting frequency protection of NAOJ telescopes
in addition to those owned by the Japanese community of radio
astronomy on their behalf.

21. Division of Solar and Plasma Astrophysics
The Division of Solar and Plasma Astrophysics is made ofstaff members from the Solar Observatory, the Hinode Science
Center, and the Nobeyama Solar Radio Observatory, and thedivivion conducts research on the Sun in close liaison with theirrespective projects. This year, all members in the division areagain on a concurrent-posting basis.
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 helioseismic explorationsof the internal structure of the Sun, as well as the explorationsof Sun-like stars and cosmic jets, taking MHD as a common
methodology. The solar group at NAOJ started observations
from space in the very early stage of Japanʼs space program. The
division has been involved in the development of the Hinodesatellite, which is currently in orbit, and plays a major role inits scientific operation. Research is also underway in the field ofground-based observation for developing new instruments for
the Solar Flare Telescope and other telescopes. In addition, thedivision engages in sustained long-term observations of solar
phenomena such as sunspots, flares, and corona and works withrelated overseas organizations to exchange data and releasepublications.

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1. Integrated Solar Physics Research
The time is ripe for solar physics to integrate theoretical andobservational studies from space and the ground. The Hinodesatellite has been operated stably this year as well. Thanks to thehigh acclaim earned through reviews by space agencies aroundthe world (FY 2012/13) for Hinode’s scientific results, all ofthese organizations are committed to continuing operation of
the Hinode in FY 2014 until FY 2015/16. The Division of Solarand Plasma Astrophysics hosted the seventh Hinode Science
Meeting, held in Takayama city between November 12 and 15,
2013.

2. Educational Activities
Tutorials were provided to students under supervision ofteachers who belonged to the Division of Solar and Plasma
Astrophysics in FY 2013, including four students from the
University of Tokyo, one of whom left prematurely, andtwo from the Graduate University for Advanced Studies. In
addition, one graduate student was tutored at the division. The
division also supported research activities such as attendanceof international research conferences and observations in Japanand abroad, irrespective of the projects of division members andstudents. Moreover, the division also cooperated with Kyoto

University and Nagoya University with support from various
NAOJ projects to plan and conduct tours for undergraduate
students to visit solar-related research organizations and to
experience the latest research in the field.

3. International Cooperation
The Hinode mission is an international endeavor involving
NASA in the US, the UK STFC, the European ESA, and theNorwegian Space Centre (NSC) in Norway. Meetings of the
Hinode Science Working Group (HSWG) are regularly held
to discuss a framework for international cooperation and open
use in the satellite’s scientific operation in order to produce
scientific results. The Division of Solar and Plasma Astrophysics
continued its efforts in making all data obtained by the Hinode
immediately available to the public. The Science Schedule
Coordinators (SSCs: Sekii and Watanabe, NAOJ) hold monthly
teleconferences in order to solicit observational projects such

as Hinode Operation Plans (HOPs) from solar researchers
around the world to facilitate maximum observational results
through projects using the scientific equipment on Hinodeand joint observational projects in combination with othersolar observation satellites/terrestrial equipment. With theestablishment of the Solar-C Project Office as Category-A
project this year (headed by Hara), the Solar-C mission proposal
was prepared in anticipation for an international collaboration
and was drafted with the help of ISAS/JAXA-WG (chief:
Watanabe). Preparation is underway for submission of proposal
to respond to an annoucement of opportunity for the next
strategic medium-sized satellite, which is expected to take placesome time next year.
One member, Suematsu is taking part in the SWG meetingof the US Advanced Technology Solar Telescope (ATST).
Several plans are under consideration for future terrestrial
observation projects that would involve collaborations withvarious institutions in Japan and with East Asian countries

22. Division of Theoretical Astronomy
1. Overview
The Division of Theoretical Astronomy aimed at achieving
exceptional international research results both in quality andquantity toward the accomplishment of the following four goals
set by the NAOJ, and it engaged in research activities for FY
2013 accordingly:- Advance the world’s cutting-edge theoretical research.
- Pursue theoretical astronomy research, particularly in areas thatinvolve the NAOJ supercomputer or large-scale observational
equipment to give insight into new observational instruments.
- Encourage collaborations between researchers in Japan andstrengthen the country’s theoretical astronomy research.
- Invigorate postgraduate education.
The division handles a wide variety of themes in theoreticalresearch, addressing a diversity of hierarchical structure of the
Universe in terms of formation/evolution process, dynamics,
and physical state of matter, covering a span from the early
Universe to galaxies, stars, planetary formation, compact object
activity, and astrophysical plasma phenomena. The Divisionof Theoretical Astronomy aims to facilitate Japan’s highcompetitiveness on the international plane through continuous
production of world’s 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
as visiting professors, visiting project research fellows, andlong-term research fellows, who actively engage in various
research projects. In particular, the division has fostered researchdevelopments to create an influential research center for young
researchers and is actively engaged in personnel exchanges with
universities and research institutes. The division’s full-time,associate, assistant, 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, theUniversity of Tokyo, and the Graduate School of Ochanomizu
University; joint research with observational astronomy using
observational satellites of various frequency bands such as the
Subaru, ALMA, and Nobeyama radio telescopes; and interdisciplinary research with physics of elementary particle/
atomic nuclei. In addition, the division actively organizes
numerous cross-disciplinary international conferences, domestic
meetings, and seminars for the fields of theoretical astronomy,observational astronomy, and experimental physics, and it leads
research activities in various fields of astronomical science.

2. Current Staff and Transfers
In FY 2013, the dedicated staff of the Division of Theoretical
Astronomy included two professors, two associate professors,and four assistant professors in addition to one professor andone assistant professor who concurrently hold primary positions
at the Center for Computation Astrophysics. In addition toresearch and educational staff, the division was served by threeproject assistant professors, including two NAOJ postdoctoral
fellows and one JSPS fellow, in addition to one administration
associate who gave support to research and the educational staff
mentioned above. Takeshi Inoue and Michiko Fujii assumed thepositions of assistant professor and project assistant professor in
March 2014 and September 2013, respectively.

II Status Reports of Research Activities

1073. Research Results
The research papers published in the publication category IV
with the Division member(s) as primary author(s) or presenter(s)are listed below. Categories with fewer than 10 publications
have been omitted.
Peer-reviewed papers in English: 56
Papers in English (conference proceedings, non-reviewed
papers): 34
Reports in English (speeches at international conferences): 72
Some of the research results are included in the researchhighlights listed at the beginning of this report. The following
highlights include research in which the division members tookleading roles:- Ion nonlinear dynamics in collisionless magnetic reconnection(Seiji Zenitani et al.)
- Toward multi-messenger astronomy: radiative transfer
simulation of binary star neutron star merger (Masaomi Tanaka
et al.)- New constraints on primordial magnetic fields from the CMB(Dai Yamazaki et al.)- Cosmological constraint against the fourth-generation neutrino
from Big Bang nucleosynthesis (Toshitaka Kajino et al.)- Ionic excitation process in the early Universe and solution for
the Big Bang lithium problem (Toshitaka Kajino et al.)
- R-process nucleosynthesis near GRB center object (collapserjet) (Ko Nakamura, Toshitaka Kajino, G. J. Mathews et al.)- Supernova neutrino formation of radioactive isotope 92Nb anddetermination of time passage in the formation of the Solar
System (Toshitaka Kajino, Ko Nakamura, G. H. Mathews etal.)- Relative equilibria theory applied to asymmetrical neutrino
generation, pulsar kick, and spin deceleration in themagnetized proto-neutron stars (Toshitaka Kajino, Jun Hidaka,
G. J. Mathews et al.)- Many-body quantum effects and neutrino response within
neutron stars (Toshitaka Kajino et al.)- f(R) theory of gravitation and the structure of ultra-magnetizedneutron stars (Toshitaka Kajino et al.)
- A new theoretical method to determine the unknown neutrino
mass-hierarchy (Toshitaka Kajino et al.)- Heavy neutron synchrotron radiation in the ultra-magnetic field
and the origin of ultra-high-energy cosmic neutrinos (Toshitaka
Kajino et al.)The following research results are published on the
Division’s website (http://th.nao.ac.jp/) among researchhighlights:- Solution to the lithium problem in Big-Bang nucleosynthesis
in hybrid axion dark matter model (Toshitaka Kajino et al.)- Static compression of porous dust aggregates (Akimasa
Kataoka et al.)108

II Status Reports of Research Activities- Early galactic chemical evolution and r-process nucleosynthesis
in black-hole forming supernovae (Toshitaka Kajino et al.)- Growth of Rayleigh–Taylor and Richtmyer–Meshkov
instabilities in relativistic jets (Jin Matsumoto et al.)- Optical/Infrared Emission from Neutron Star Merger (Masaomi
Tanaka et al.)- Ion nonlinear dynamics in magnetic reconnection (Seiji
Zenitani et al.)- The seeds of planets are fluffy (Akimasa Kataoka et al.)- Stringent constraint on the 4th flavor-generation of neutrino
from Big-Bang nucleosynthesis (Toshitaka Kajino et al.)- New constraints on primordial magnetic fields from the CMB(Dai Yamazaki et al.)- Theoretical explanation of the origin of Niobium 92 as
supernova explosion neutrino: evaluation of the period 1–30
million years from supernova explosion to the birth of the
Solar System (Toshitaka Kajino et al.)
- A new theoretical method to determine the unknown neutrino
mass-hierarchy (selected as a highlight topical review of 2013
in Journal of Physics G) (Toshitaka Kajino et al.)- The moment of core collapse in star clusters with a massfunction (Michiko Fujii et al.)- Structure of magnetized molecular filaments (Kohji Tomisaka
et al.)- Some remarks on the diffusion regions in magnetic
reconnection (Seiji Zenitani et al.)
- CMB with the background primordial magnetic field (DaiYamazaki et al.)

4. Educational Activities
To supplement Section III on activities of research andeducational staff members as part-time lecturers at universities
and graduate schools, the lecture subjects are listed below:
Toshitaka Kajino: Fundamentals of theoretical astronomy at
the Graduate University for Advanced Studies; science of time,
space, and matter, and fundamentals of physics at Gakushuin
University; modern physics at Japan Women’s University;
astrophysics at Jissen Women’s University; nuclear physics at
Meiji University.
Tetsuhiro Kudoh: Space and Earth science at the University
of Electro-Communications.
Eiichiro Kokubo: Introduction to planetary science at theTokyo Institute of Technology; special lecture in celestialmechanics V at the Graduate School of the University of Tokyo.
Fumitaka Nakamura: Special lecture in physical sciences at
Osaka Prefecture University; special lecture in space sciences 1
at Hokkaido University.
Takashi Hamana: Geology at the Tokyo University ofAgriculture and Technology.
Yasunori Hori: Introduction to astronomy at Kanagawa
University.
Grant J. Mathews: Special lecture titled “Cosmology andAstrophysics” at the Graduate School of the University ofTokyo.

Tetsuhiro Kudoh led a group of undergraduate students invisiting actual research sites during the Summer Student eventof the Graduate University of Advanced Studies. Moreover,various contributions were made to education at the high-schoollevel. Toshitaka Kajino delivered a Super Science High School
lecture titled “Discovering the Birth of Matter” at Kashiwazaki
Senior High School in Niigata, and Eiichiro Kokubo delivereda Super Science High School lecture titled “Cosmo-science: theEarth in the Universe” at Hibiya High School in Tokyo.

5. PR and Outreach Activities
The Division of Theoretical Astronomy actively engaged inpublic promotions and outreach activities by offering lectures
to the general public. The following lectures were delivered
this year: Ken Ohsuga: “Computational exploration to black
holes” held at Asahi Culture Center, Yokohama; Toshitaka
Kajino: “The birth of the Universe and origin of Life,” deliveredat the First civic lecture Manabi no Mori hosted by Aomori
University and Aomori Akenohoshi Junior College; “The birthof the Universe: tempospaciality and symmetry violation” and“Element traveling through Space: Neutrinos and Origin ofLife” at the Professor Lecture hosted by Inagi City Board of
Education; Eiichiro Kokubo: “The Origin of the Solar System:from Star Dust to Planet” at a science seminar of The PhysicalSociety of Japan; “From Star Dust to the Planet Earth” as part of
the ASJ open lecture “Uchu wa date janai!?”; “From Star Dust
to the Planet Earth and the Moon” for the Japan Association for
Calendars and Culture Promotion; “Junior lecture: the Earth in
the Universe” and “the Oort Cloud, the home of Comet ISON”
at Asahi Culture Center Shinjuku; “Home of comets: the Oort
Cloud” and “The Beauty in the Moon” at Ikebukuro Community
College; “Experiment to create the Earth using Supercomputer”
at the Koriyama City Fureai Science Center SPACEPARK
and “From Star Dust to the Planet Earth” at an open lecture
for pioneering the future of Iwate held in Morioka; Masaomi
Tanaka: “Computational exploration of supernova explosions”
at Asahi Culture Center, Yokohama, and “The destiny ofBetelgeuse: will there be a supernova explosion?” for Civic
Astronomy, Sumida; Takashi Hamana: “Dark matter and darkenergy in Space” at Asahi Culture Center, Yokohama; Michiko
Fujii: “Galaxies revealed through the latest astronomy” at Asahi
Culture Center, Yokohama; and Dai Yamazaki: “Polarizationof CMB and Next-Generation Cosmology” at Asahi Culture
Center, Yokohama.

6. International Collaborations
Toshitaka Kajino performed duties of the following posts:
editorial board member for the UK Institute of Physics “Journalof Physics”; review panel member of the European Science
Foundation Euro GENESIS Project; international examiner for
the Science, Technology and Innovation Council of Canada;international associate for the European Centre for Theoretical
Studies in Nuclear Physics and Related Areas (ECT*) and the
Swiss National Science Foundation (SNSF). Eiichiro Kokubo

served as a member of the Organizing Committee of the IAU’s
Extrasolar Planets Commission.
Research staff of the Division of Theoretical Astronomy
played leading roles in organizing The 12th International
Symposium on the Origin of Matter and Evolution of Galaxies at
Tsukuba International Congress Center and the Sokendai Asian
Winter School 2013: Science Eyes and Minds towards Cosmic
Horizon, co-hosted by faculties of Astronomical Sciences andSpace Sciences. These staff members made contributions ofdisseminating research progress made in Japan to the world andencouraged international exchanges.
An agreement was made between the NAOJ and ECT*,
both signing the Memorandum of Understanding mediatedthrough the Division of Theoretical Astronomy. This agreement
encompasses the scientific advancement in bordering areas
between astronomy and astro/nuclear/particle/condensed-matterphysics by promoting an exchange of scientists and postgraduate
students for international conferences, joint research projects,
and university education programs in mutual collaboration. An
international workshop is planned at the ECT* (Trento, Italy)
in September 2014, titled “Nuclear Physics and Astrophysics
of Neutron-Star Mergers and Supernovae and the Origin of
R-Process Elements.”

7. Awards
Akimasa Kataoka was awarded the best presentation award
by the Japanese Society for Planetary Sciences.

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 inastronomy and an international astronomical research institution
by providing an excellent research environment. It engages invarious joint research projects with visiting researchers fromoverseas, with the help of Grants-in-Aid for Scientific Research,government subsidies for operating expenses, and the NAOJ
budget for guest visitors. The main international visitors to theDivision are listed below:
Akif B. Balantekin, (University of Wisconsin–Madison, US)
Ramon Brasser, (Academia Sinica, Taiwan)
Grant J. Mathews, (University of Notre Dame, US)
Myung-Ki Cheoun, (Soongsil University, South Korea)
Yamac Deliduman, (Mimar Sinan Fine Arts University, Turkey)
Poshak Gandhi, (Durham University, UK)
Motohiko Kusakabe, (Korea Aerospace University, South
Korea)
Roland Diehl, (Max Planck Institute, Germany)
Chung-Yoel Ryu, (Hanyang University, South Korea)
MacKenzie Warren, (University of Notre Dame, US)

II Status Reports of Research Activities10923. Office of International Relations
The Office of International Relations strives in promoting
autonomous research activities by planning and implementing
strategies for the NAOJ’s international research effortscharacteristic to the institution as a whole. It also andsupports efforts to strengthen the foundation for expanded
internationalization. The office’s main activities include
supporting international collaborative projects; liaising withoverseas astronomical research organizations; gathering andproviding information on international activities; offering
support for hosting international conferences, workshops, andseminars; providing support for visiting international researchersand students; and assisting Japanese research organizations forinternational partnerships.

1. International Collaborative Project Support
The office gathers and provides information necessary forpursuing well-organized international research collaborations
on its own initiative, and it serves as a liaison point forinternational activities, engages in international agreements orprovides 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) between June 28 and 29, 2013 at theSmithsonian Submillimeter Telescope, Hilo Island, Hawaii. The
four institutions forming the EACOA include the NAOC, theNAOJ, KASI, and the ASIAA in Taiwan. The office also issued
a public call for the EACOA postdoctoral fellowship program in
2014. In addition, it co-hosted the EACOA East Asia Workshop
on Joint Research via Mid/Small-aperture Telescopes held June
21–25, 2013, at NAOC in Kunming, China.
In tandem with the agreement signed between the NAOJ
and IAU to establish the IAU Office for Public Outreach,the Office undertook an international call for the positionsof Public Outreach Coordinators. The Office of International
Relations also cooperated with EACOA member organizations
in supporting the activities of the IAU Office for Astronomy

110

II Status Reports of Research Activities

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 supported by
the 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 researchersand 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 in ensuring a pleasant experience. The office also
provides general information useful for everyday activities.

5. Assistance in International Partnerships
Involving Japanese Research Organizations
The Office of International Relations assists universities andother educational and research organizations in Japan to engage
in international partnerships. It also liaises with the International
Strategy Headquarters and the International Cooperation Officeat the NINS to coordinate international collaborations. The
office oversaw the Optical and Infrared Synergetic Telescopesfor Education and Research (OISTER) project conducted by
the OAO, the Ishigakijima Astronomical Observatory, and nine
Japanese universities.
The collaboration with the Office of International Relations
at the NINS yielded a workshop for international joint research
associates in which the office was involved from the planningstages to the preparation of a manual for hosting international
researchers and in giving English-language master seminars tovarious NINS organizations. The office also cooperated with the
Administrative Bureau of the NINS to dispatch two NINS officeadministrators to the Subaru Telescope facility for overseas
training.

III Organization
1. Organization

Project(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)

TAMA 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
CenterAstronomy Data Center
Advanced Technology Center
Public Relations Center
Division
Division of Optical and Infrared Astronomy
Division of Radio Astronomy
Division of Solar and Plasma Astrophysics
Division of Theoretical Astronomy
Research Enhancement Strategy Office
Research Evaluation Support Office
Office of International Relations
Human Resources Planning Office
Safety and Health Management Office
Administration Department
III Organization

111

2. Number of Staffs(2014/3/31)
Permanent Employee
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
Employee on Annual Salary System
Fixed-term Employee
Full-time Contract Employee
Part-time Contract Employee

1
156
27
0
38
9
61
0
21
36
53
3
35
88
163

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

112

III Organization

Hayashi, Masahiko
Watanabe, Junichi
Kobayashi, Hideyuki
Takami, Hideki
Sakurai, Takashi

4. Research Departments
Chief Engineer
Postdoctoral Fellow

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
Postdoctoral Fellow
Postdoctoral Fellow
Administration Department
Manager
General Affairs Section
Chief
Staff
Accounting Section
Chief
Hyper Suprime-Cam
Director
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Chief Engineer

Arimoto, Nobuo
Arimoto, Nobuo
Iye, Masanori
Usuda, Tomonori
Ohashi, Nagayoshi
Mizumoto, Yoshihiko
Aoki, Wakou
Ichikawa, Shinich
Iwata, Ikuru
Kashikawa, Nobunari
Kodama, Tadayuki
Takato, Naruhisa
Takeda, Yoichi
Terada, Hiroshi
Noumaru, Junichi
Hayashi, Saeko
Yutani, Masami
Imanishi, Masatoshi
Komiyama, Yutaka
Shirasaki, Yuji
Tomono, Daigo
Hayano, Yutaka
Minowa, Yosuke
Yagi, Masafumi
Pyo, Tae-soo
Tazawa, Seiichi
Omata, Koji
Kurakami, Tomio
Namikawa, Kazuhito
Negishi, Satoru
Suda, Takuma
Yabe, Kiyoto
Kobayashi, Hideki
Kobayashi, Hideki
Sugawara, Satoshi
Furuhata, Tomoyuki
Miyazaki, Satoshi
Takata, Tadafumi
Komiyama, Yutaka
Nakaya, Hidehiko
Furusawa, Hisanori
Tanaka, Masayuki
Uraguchi, Fumihiro

Kamata, Yukiko
Okura, Yuki

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
Kanbe, Eiji
Assistant Professor
Engineer
Tsutsui, Hironori
Postdoctoral Fellow
Imada, Akira
Postdoctoral Fellow
Fukui, Akihiko
Administration Office
Administration Section
Chief
Seto, Nobuyoshi
Nobeyama Radio Observatory
Director
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
Engineer
Postdoctoral Fellow
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Administration Office
Deputy Manager
General Affairs Section
Chief
Accounting Section
Chief
Staff

Kuno, Nario
Kuno, Nario
Nakamura, Fumitaka
Kanzawa, Tomio
Ishizuki, Sumio
Umemoto, Tomofumi
Oshima, Tai
Takano, Shuro
Iwashita, Hiroyuki
Mikoshiba, Hiroshi
Ishikawa, Shinichi
Miyazawa, KazuhikoHanda, Kazuyuki
Miyazawa, Chieko
Wada, Takuya
Morokuma, Kana
Takekoshi, Tatsuya
Minamidani, Tetsuhiro

Otsuka, Tomoyoshi
Otsuka, Tomoyoshi
Sasaki, Hiroaki
Kobayashi, Kazuhito

Nobeyama Solar Radio Observatory
Director
Hanaoka, Yoichiro
Professor
Shibasaki, Kiyoto
Chief Research Engineer Kawashima, Susumu
Assistant Professor
Shimojo, Masumi
Chief Engineer
Shinohara, Noriyuki

III Organization

113

Postdoctoral Fellow

Iwai, Kazamasa

Mizusawa VLBI Observatory
Director
Kawaguchi, Noriyuki
Professor
Kawaguchi, Noriyuki
Professor
Kobayashi, Hideyuki
Associate Professor
Agata, Hidehiko
Associate Professor
Shibata, Katsunori
Associate Professor
Hanada, Hideo
Associate Professor
Honma, Mareki
Chief Research Engineer Satou, Katsuhisa
Assistant Professor
Kameya, Osamu
Assistant Professor
Kouno, Yusuke
Assistant Professor
Jike, Takaaki
Assistant Professor
Sunada, Kazuyoshi
Assistant Professor
Tamura, Yoshiaki
Assistant Professor
Hagiwara, Yoshiaki
Assistant Professor
Hirota, Tomoya
Research Engineer
Asari, Kazuyoshi
Research Engineer
Ishikawa, Toshiaki
Research Engineer
Oshima, Norio
Research Engineer
Suzuki, Syunsaku
Research Engineer
Fukushima, Hideo
EngineerUeno, Yuji
Engineer
Shizugami, Makoto
Postdoctoral Fellow
Sawada, Satoko
Postdoctoral Fellow
Matsumoto , Naoko
Postdoctoral Fellow
Yamauchi, Aya
Specially Appointed
Nagayama, Takumi
Research Staff
Specially Appointed
Kim, Jeoung Sook
Research Staff
Administration Office
Deputy Manager
Hommyo, Susumu
General Affairs Section
Chief
Hommyo, Susumu
Accounting Section
Chief
Koseki, Tatsuya
Staff
Kato, Masahiro
Ishigakijima Astronomical Observatory
Associate Professor
Agata, Hidehiko
Research Engineer
Oshima, Norio
Research Engineer
Fukushima, Hideo
Postdoctoral Fellow
Hanayama, Hidekazu
Time Keeping Office
Head
Kawaguchi, Noriyuki
Chief Research Engineer Satou, Katsuhisa
Research Engineer
Asari, Kazuyoshi
Solar Observatory
Director
Professor
Professor
Associate Professor
Associate Professor
Chief Engineer

114

III Organization

Hanaoka, Yoichiro
Sakurai, Takashi
Shibasaki, Kiyoto
Suematsu, Yoshinori
Hanaoka, Yoichiro
Shinoda, Kazuya

Postdoctoral Fellow
NAOJ Chile Observatory
Director
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor
Specially Appointed
Associate Professor
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Research Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Specially Appointed
Research Staff

Otsuji, Kenichi

Hasegawa, Tetsuo
Iguchi, Satoru
Ogasawara, Ryusuke
Kameno, Seiji
Tatematsu, Kenichi
Hasegawa, Tetsuo
Asayama, Shinichiro
Iono, Daisuke
Oishi, Masatoshi
Okuda, Takeshi
Kiuchi, Hitoshi
Kuno, Nario
Kosugi, Joji
Saito, Masao
Mizuno, Norikazu
Komugi, Shinya
Shinnaga, Hiroko
Kawashima, Susumu
Watanabe, Manabu
Umemoto, Tomofumi
Ezawa, Hajime
Oshima, Tai
Kamazaki, Takeshi
Sawada, Tsuyoshi
Shimojo, Masumi
Sugimoto, Masahiro
Takahashi, Satoko
Nakanishi, Koichiro
Hiramatsu, Masaaki
Hirota, AkihikoMatsuda, Yuichi
Espada Fernandez,
DanielAkiyama, Eiji
Saigou, Kazuya
Nagai, Hiroshi
Hatsukade, Bunyo
Muller, Erik
Ashitagawa, Kyoko
Nakazato, Takeshi
Kato, Yoshihiro
Kobiki, ToshihikoNakamura, Kyoko
Kurono, Yasutaka

Specially Appointed
Research Staff
Postdoctoral Fellow
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Administration Department
Manager
Chief
Senior Staff

Chibueze, James Okwe
Kawamura, Akiko
Miura, Rie
Ao, Yiping
Herrera Contreras,
Cinthya Natalia
Chiba, Kurazou

Yamaguchi, Takahiro
Tsukano, Satomi
Yamamoto, ShinichiCenter for Computational Astrophysics
Director
Kokubo, Eiichiro
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kouji
Assistant Professor
Ito, Takashi
Assistant Professor
Ohsuga, Ken
Assistant Professor
Inoue, Tsuyoshi
Assistant Professor
Kudoh, Takahiro
Assistant Professor
Tanaka, Masaomi
Specially Appointed
Takahashi, Hiroyuki
Assistant Professor
Specially Appointed
Takiwaki, Tomoya
Assistant Professor
Postdoctoral Fellow
Ishitsu, Naoki
Hinode Science Center
Director
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Specially Appointed
Research Staff
Postdoctoral Fellow
Specially Appointed
Research Staff

Watanabe, Tetsuya
Sakurai, Takashi
Shibasaki, Kiyoto
Suematsu, Yoshinori
Sekii, TakashiHara, Hirohisa
Katsukawa, Yukio
Kano, Ryohei
Kubo, Masahito
Shimojo, Masumi
Ishikawa, Ryohko
Bando, Takamasa
Nishizuka, Naoto
Kato, Yoshiaki
Antolin, Patrick

B Projects

TAMA Project OfficeDirector
Specially Appointed
Professor

Ando, Masaki
Flaminio, Raffaele

Affiliated AssociateAndo, Masaki
Professor
Assistant Professor
Akutsu, Tomotada
Assistant Professor
Ueda, Akitoshi
Assistant Professor
Takahashi, Riyutaro
Assistant Professor
Tatsumi, Daisuke
Research Engineer
Ishizaki, Hideharu
Research Engineer
Torii, Yasuo
Chief Engineer
Tanaka, Nobuyuki
Postdoctoral Fellow
Nakamura, Kouji
Specially Appointed
Pena Arellano, Fabian
Research Staff
ErasmoSecondment (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
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Postdoctoral Fellow
Postdoctoral Fellow
Specially Appointed
Senior Specialist

Iye, Masanori
Iye, Masanori
Usuda, Tomonori
Takami, Hideki
Yamashita, Takuya
Aoki, Wakou
Kashikawa, Nobunari
Terada, Hiroshi
Kodama, Tadayuki
Takato, Naruhisa
Miyashita, Takaaki
Imanishi, Masatoshi
Suzuki, Ryuji
Yagi, Masafumi
Hashimoto, Tetsuya
Wanajo, Shinya
Kozu, Akihito

A Projects

JASMINE Project OfficeDirector
Professor
Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Chief Research Engineer
Research Engineer
Postdoctoral Fellow
Specially Appointed
Research Staff

Gouda, Naoteru
Gouda, Naoteru
Kobayashi, Yukiyasu
Takato, Naruhisa
Hanada, Hideo
Araki, Hiroshi
Tsujimoto, Takuji
Noda, Hirotomo
Yano, Taihei
Tsuruta, Seiitsu
Asari, Kazuyoshi
Niwa, Yoshito
Yamaguchi, Masaki

Extrasolar Planet Detection Project OfficeDirector
Tamura, Motohide
Professor
Kokubo, Eiichiro
Affiliated Professor
Tamura, Motohide

III Organization

115

Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Research Staff
Postdoctoral Fellow
Postdoctoral Fellow
RISE ProjectActing Director
Professor
Professor
Professor
Associate Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Chief Engineer
Postdoctoral Fellow
Postdoctoral Fellow
SOLAR-C Project OfficeDirector
Professor
Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Chief Engineer
Chief Engineer
Specially Appointed
Research Staff

Izumiura, Hideyuki
Suto, Hiroshi
Nakajima, Tadashi
Nishikawa, Jun
Morino, Jun-ichi
Narita, Norio
Kandori, Ryo
Kotani, Takayuki
Nishiyama, Shogo

Hanada, Hideo
Gouda, Naoteru
Kokubo, Eiichiro
Kobayashi, Yukiyasu
Hanada, Hideo
Matsumoto, Koji
Tsuruta, Seiitsu
Araki, Hiroshi
Kouno, Yusuke
Tsujimoto, Takuji
Noda, Hirotomo
Yano, Taihei
Asari, Kazuyoshi
Ishikawa, Toshiaki
Tazawa, Seiichi
Oshigami, Shoko
Yamada, RyuheiHara, Hirohisa
Sakurai, Takashi
Watanabe, Tetsuya
Suematsu, YoshinoriHara, Hirohisa
Katsukawa, Yukio
Kano, Ryohei
Kubo, Masahito
Ishikawa, Ryohko
Bando, Takamasa
Kobiki, Toshihiko
Shinoda, Kazuya
Narukage, Noriyuki

Centers
Astronomy Data Center
Director
Professor
Professor
Associate Professor

116

III Organization

Oishi, Masatoshi
Mizumoto, Yoshihiko
Kokubo, Eiichiro
Ichikawa, Shinich

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
Postdoctoral Fellow
Postdoctoral Fellow
Specially Appointed
Research Staff
JVO Project
Head
Associate Professor
Assistant Professor
Advanced Technology Center
Director
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
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research 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

Oishi, Masatoshi
Kosugi, Joji
Shibata, Katsunori
Takata, Tadafumi
Noumaru, Junichi
Ito, Takashi
Oe, Masafumi
Kano, Ryohei
Shimojo, Masumi
Shirasaki, Yuji
Takano, Shuro
Furusawa, Hisanori
Inoue, Goki
Fukui, Asami
Eguchi, Satoshi
Komiya, Yutaka
Yoshida, Tessei

Mizumoto, Yoshihiko
Oishi, Masatoshi
Shirasaki, Yuji

Noguchi, Takashi
Noguchi, Takashi
Iwata, Ikuru
Uzawa, Yoshinori
Sekimoto, YutaroHara, Hirohisa
Matsuo, Hiroshi
Miyazaki, Satoshi
Okada, Norio
Akutsu, Tomotada
Kano, Ryohei
Kojima, Takafumi
Suzuki, Ryuji
Nakaya, Hidehiko
Iizuka, Yoshizo
Sato, Naohisa
Noguchi, Motokazu
Fukushima, Mitsuhiro
Fujii, Yasunori
Mikoshiba, Hiroshi
Ikenoue, Bungo
Ito, Tetsuya
Inata, Motoko
Iwashita, Hikaru
Uraguchi, Fumihiro
Obuchi, Yoshiyuki
Kaneko, Keiko
Kamata, Yukiko
Kubo, Koichi
Takahashi, Toshikazu
Tamura, Tomonori
Fukuda, Takeo

Chief Engineer
Chief Engineer
EngineerEngineer
Postdoctoral Fellow
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Public Relations Center
Director
Professor
Professor
Associate Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Engineer
Postdoctoral Fellow
Chief
Public Relations Office
Head
Assistant Professor
Engineer
Outreach Office
HeadMuseum Project Office
Head
Associate Professor
Research Engineer
Senior Engineer
Ephemeris Computation Office
Head
Senior Engineer
Science Culture Promotion Unit
Head
Library
Chief
Publications Office
HeadVice-Head
Administration OfficeHeadMiyazawa, Chieko
Waseda, Koichi
Tsuzuki, Toshihiro
Mitsui, Kenji
Karatsu, Kenichi
Narukage, Noriyuki
Dominjon, Agnes
Micheline

Fukushima, Toshio
Fukushima, Toshio
Watanabe, Junichi
Agata, Hidehiko
Ikuta, ChisatoSoma, Mitsuru
Oshima, Norio
Katayama, Masato
Sasaki, Goro
Fukushima, Hideo
Matsuda, Kou
Nagayama, Shiyogo
Kasuga, Toshihiro
Hori, Mayumi
Ikuta, ChisatoSoma, Mitsuru
Nagayama, Shiyogo
Agata, Hidehiko
Oshima, Norio
Agata, Hidehiko
Sasaki, Goro
Matsuda, Kou
Katayama, Masato
Matsuda, Kou
Agata, HidehikoHori, Mayumi
Fukushima, Toshio
Fukushima, Hideo
Matsuda, Kou

Divisions
Division of Optical and Infrared Astronomy
Director
Mizumoto, Yoshihiko
Professor
Arimoto, Nobuo
Professor
Iye, Masanori

Professor
Usuda, Tomonori
Professor
Ohashi, Nagayoshi
Professor
Gouda, Naoteru
Professor
Kobayashi, Yukiyasu
Professor
Sekiguchi, Kazuhiro
Professor
Takami, Hideki
Professor
Mizumoto, Yoshihiko
Professor
Yamashita, Takuya
Associate Professor
Aoki, Wakou
Associate Professor
Izumiura, Hideyuki
Associate Professor
Iwata, Ikuru
Associate Professor
Ukita, Nobuharu
Associate Professor
Kashikawa, Nobunari
Associate Professor
Kodama, Tadayuki
Associate Professor
Sasaki, Toshiyuki
Associate Professor
Takato, Naruhisa
Associate Professor
Takeda, Yoichi
Associate Professor
Terada, Hiroshi
Associate Professor
Noumaru, Junichi
Associate Professor
Hayashi, Saeko
Chief Research Engineer Koyano, Hisashi
Chief Research Engineer Miyashita, Takaaki
Chief Research Engineer Yutani, Masami
Assistant Professor
Akutsu, Tomotada
Assistant Professor
Imanishi, Masatoshi
Assistant Professor
Ueda, Akitoshi
Assistant Professor
Komiyama, Yutaka
Assistant Professor
Suto, Hiroshi
Assistant Professor
Soma, Mitsuru
Assistant Professor
Takahashi, Riyutaro
Assistant Professor
Tatsumi, Daisuke
Assistant Professor
Tsujimoto, Takuji
Assistant Professor
Tomono, Daigo
Assistant Professor
Nakajima, Tadashi
Assistant Professor
Nishikawa, Jun
Assistant Professor
Hayano, Yutaka
Assistant Professor
Pyo, Tae-soo
Assistant Professor
Minowa, Yosuke
Assistant Professor
Morino, Jun-ichi
Assistant Professor
Yagi, Masafumi
Assistant Professor
Yanagisawa, Kenshi
Assistant Professor
Yano, Taihei
Specially Appointed
Matsuoka, Yoshiki
Assistant Professor
Research Engineer
Ishizaki, Hideharu
Research Engineer
Torii, Yasuo
Research Engineer
Tazawa, Seiichi
Chief Engineer
Omata, Koji
Chief Engineer
Kurakami, Tomio
Chief Engineer
Tanaka, Nobuyuki
Chief Engineer
Namikawa, Kazuhito
Chief Engineer
Negishi, Satoru
Engineer
Tsutsui, Hironori
Secondment (to The University of Tokyo)
Assistant Professor
Oishi, Naoko

III Organization

117

Division of Radio Astronomy
Director
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer

118

III Organization

Iguchi, Satoru
Iguchi, Satoru
Ogasawara, Ryusuke
Kameno, Seiji
Kawaguchi, Noriyuki
Kawabe, Ryohei
Kobayashi, Hideyuki
Tatematsu, Kenichi
Hasegawa, Tetsuo
Asayama, Shinichiro
Iono, Daisuke
Okuda, Takeshi
Kiuchi, Hitoshi
Kuno, Nario
Kosugi, Joji
Saito, Masao
Shibata, Katsunori
Hanada, Hideo
Honma, Mareki
Matsumoto, Koji
Mizuno, Norikazu
Kawashima, Susumu
Kanzawa, Tomio
Satou, Katsuhisa
Tsuruta, Seiitsu
Watanabe, Manabu
Araki, Hiroshi
Ishizuki, Sumio
Umemoto, Tomofumi
Ezawa, Hajime
Espada Fernandez,
DanielOshima, Tai
Kamazaki, Takeshi
Kameya, Osamu
Kouno, Yusuke
Sawada, Tsuyoshi
Jike, Takaaki
Sugimoto, Masahiro
Sunada, Kazuyoshi
Takano, Shuro
Takahashi, Satoko
Tamura, Yoshiaki
Nakanishi, KoichiroNoda, Hirotomo
Hagiwara, Yoshiaki
Hiramatsu, Masaaki
Hirota, Akihiko
Hirota, Tomoya
Matsuda, Yuichi
Miyoshi, Makoto
Asari, Kazuyoshi
Ashitagawa, Kyoko
Ishikawa, Toshiaki
Iwashita, Hiroyuki

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

Suzuki, Syunsaku
Nakazato, Takeshi
Ishikawa, Shinichi
Miyazawa, KazuhikoKato, Yoshihiro
Kobiki, ToshihikoNakamura, Kyoko
Handa, Kazuyuki
Miyazawa, Chieko
Ueno, Yuji
Shizugami, Makoto
Wada, Takuya

Division of Solar and Plasma Astrophysics
Director
Watanabe, Tetsuya
Professor
Sakurai, Takashi
Professor
Shibasaki, Kiyoto
Professor
Watanabe, Tetsuya
Associate Professor
Suematsu, Yoshinori
Associate Professor
Sekii, Takashi
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Hara, Hirohisa
Assistant Professor
Katsukawa, Yukio
Assistant Professor
Kano, Ryohei
Assistant Professor
Kubo, Masahito
Assistant Professor
Shimojo, Masumi
Research Engineer
Bando, Takamasa
Chief Engineer
Shinoda, Kazuya
Chief Engineer
Shinohara, Noriyuki
Division of Theoretical Astronomy
Director
Tomisaka, Kouji
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kouji
Professor
Yoshida, Haruo
Associate Professor
Kajino, Toshitaka
Associate Professor
Nakamura, Fumitaka
Assistant Professor
Ohsuga, Ken
Assistant Professor
Kudoh, Takahiro
Assistant Professor
Inoue, Tsuyoshi
Assistant Professor
Tanaka, Masaomi
Assistant Professor
Hamana, Takashi
Specially Appointed
Zenitani, Seiji
Assistant Professor
Specially Appointed
Fujii, Michiko
Assistant Professor
Specially Appointed
Fujimoto, Keizo
Assistant Professor
Postdoctoral Fellow
Yamazaki, Dai

5. Research Support Departments
Research Enhancement Strategy OfficeDirector
Kobayashi, Hideyuki
Specially Appointed
Ota, Masahiko
Senior Specialist
Specially Appointed
Suematsu, Sayaka
Senior Specialist
Specially Appointed
Yamamiya, Osamu
Senior Specialist
Research Evaluation Support OfficeDirector
Watanabe, Junichi
Office of International Relations
Director
Sekiguchi, Kazuhiro
Professor
Sekiguchi, Kazuhiro
Administration Office
Deputy Manager
Seto, Yoji
International Academic Affairs Section
Chief
Kikkawa, Hiroko
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
Administration Department
General Manager
Sato, Tadashi
General Affairs Division
Manager
Goto, Tsutomu
Deputy Manager
Seto, Yoji
Information Technology Specialist
Specialist
Yoshikawa, Ikuko
Personnel Accounting Specialist
Specialist
Kikuchi, Jinichi
General Affairs Section
Chief
Yoshikawa, Ikuko
Staff
Sugimoto, Naomi
Staff
Takada, Miyuki
Staff
Yamafuji, Yasuto
Vehicle Driver
Amemiya, Hidemi
Personnel Section
Chief
Yamanochi, Mika
Staff
Furukawa, Shinichiro
Payroll Section
Chief
Kikuchi, Jinichi
Staff
Iida, Naoto
Employee Section
Chief
Yamaura, Mari
Staff
Kawashima, Ryota

Research Support Section
Chief
Staff
Staff
Child Care Leave
Staff
Staff
Financial Affairs Division
Manager
Senior Specialist
Audit Specialist
Specialist
General Affairs Section
Chief
Staff
Budget Section
Chief
Staff
Asset Management Section
Chief
Senior Staff
Purchase Validation Center
Senior Staff
Accounting Division
Manager
Contract Specialist
Specialist
Accounting Section
Chief
Staff
Procurement Section
Chief
Senior Staff
Staff
Staff
Facilities Division
Manager
General Affairs Section
Chief
Staff
Planning Section
Chief
Maintenance Section
Chief
Staff

Sato, Yoko
Matsukura, Koji
Yoshimura, Tetsuya
Ouchi, Kaori
Goto, Michiru
Yamaguchi, Yutaka
Miura, Norio
Miura, Susumu
Miura, Susumu
Mizokawa, Yuko
Fujiwara, Kenichi
Hiramatsu, Naoya
Miura, Norio
Sato, Kanako
Sato, Kanako
Hyuga, Tadayuki
Onishi, Tomoyuki
Kamezawa, Takayuki
Chiba, Satoko
Onishi, Tomoyuki
Chiba, Yoko
Okubo, Kazuhiko
Sakamoto, Misato
Ono, Kazuo
Yamada, Tomohiro
Nakagawa, Yukie
Murakami, KazuhiroSato, Takashi
Shibata, Jumpei

III Organization

1196. Personnel change
Research and Academic Staff
Date
Name
ChangeEspada Fernandez,
2013/4/1
Hired
Daniel2013/5/1

Takahashi, Satoko

Hired

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

2013/8/1

Pyo, Tae-Soo

Hired

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

2014/1/1

Nakazato, Takeshi

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

2014/3/1

Inoue, Tsuyoshi

HiredDivision of Theoretical Astronomy,
Assistant Professor

2014/3/15

Hirota, Akihiko

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

2013/5/14

Komugi, Shinya

Resigned

NAOJ Chile Observatory, Associate
Professor

Previous Affiliated Institute, Position

Division of Radio Astronomy(NAOJ Chile Observatory),
Assistant Professor
Division of Optical andInfrared Astronomy (Okayama
Astrophysical Observatory),
Research Engineer

2013/6/30

Sakamoto, Akihiro

Resigned

2014/3/31

Kuno, Nario

Resigned

University of Tsukuba

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

2014/3/31

Uzawa, Yoshinori

Resigned

National Institute of Information andCommunications Technology

Advanced Technology Center,
Associate Professor

2014/3/31

Kawaguchi,
NoriyukiContract
Expired2013/4/1

Asayama, Shinichiro Promoted

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

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

2013/6/1

Iwata, Ikuru

Promoted

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

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

2013/6/1

Usuda, Tomonori

Promoted

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

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

2014/1/1

Tazawa, Seiichi

Reassigned

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

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

Engineering Staff
Date

120

New Affiliated Institute, Position
Division of Radio Astronomy (NAOJ Chile
Observatory), Assistant Professor

Name

Change2014/3/1

Tsutsui, Hironori

Hired2014/3/31

Ishikawa, Shinichi

RetiredIII Organization

Division of Radio Astronomy(Mizusawa VLBI Observatory),
Professor

New Affiliated Institute, Position

Previous Affiliated Institute, Position

Division of Optical and Infrared Astronomy(Okayama Astrophysical Observatory),
Engineer
Division of Radio Astronomy(Nobeyama Radio Observatory),
Senior Engineer

Administrative Staff
Date
Name

Change2013/4/1

Ono, Kazuo

Hired

2013/4/1

Honmyo, Susumu

Hired

Mizusawa VLBI Observatory
Administration Office, Chief

National Institute of technology,
Ichinoseki College

2013/4/1

Yoshikawa, Ikuko

Hired

Administration Department General Affairs
Division General Affairs Section, Chief

Hitotsubashi University

2013/4/1

Kikuchi, Jinichi

Hired

Administration Department General Affairs
Division, Specialist

The University of Tokyo

2013/4/1

Sato, Takashi

Hired

Administration Department Facilities
Division Maintenance Section, Chief

The University of Tokyo

2013/4/1

Seto, Nobuyoshi

HiredOkayama Astrophysical Observatory
Administration Section, Chief

Okayama University

2013/4/1

Takada, Miyuki

HiredAdministration Department General Affairs
Division General Affairs Section, Staff

2013/8/1

Kobayashi, Kazuhito Hired

Nobeyama Radio Observatory Accounting
Section, Staff

2013/8/1

Sakamoto, Misato

Hired

Administration Department Accounting
Division Procurement Section, Staff

2013/9/1

Matsukura, Koji

HiredAdministration Department General Affairs
Division Research Support Section, Staff

2013/7/31

Takahashi, Masaru

Resigned

Shinshu University

New Affiliated Institute, Position
Administration Department Facilities
Division, Manager

Previous Affiliated Institute, Position
Tokyo University of the Arts

Shinshu University

Nobeyama Radio Observatory
Accounting Section, Staff
Administration Department
Financial Affairs Division, Staff

2013/12/31 Ushio, Maiko

Resigned

2014/3/31

Sato, Tadashi

Resigned

The Graduate University for Advanced
Studies

Administration Department,
General Manager

2014/3/31

Goto, Tsutomu

Resigned

The University of Electro-Communications

Administration Department
General Affairs Division, Manager

2014/3/31

Yamaguchi, Yutaka

Resigned

Shizuoka University

Administration Department
Financial Affairs Division,
Manager

2014/3/31

Kamezawa, Takayuki Resigned

Tokyo Gakugei Univerisity

Administration Department
Accounting Division Accounting
Section, Chief

2014/3/31

Shibata, Jumpei

Resigned

National Institution For Youth Education

Administration Department
Facilities Division Maintenance
Section, Staff

2013/4/1

Seto, Yoji

Promoted

Office of International Relations
Administration Office, Chief

National Institutes of Nature
Sciences

2013/4/1

Otsuka, Tomoyoshi

Promoted

Nobeyama Radio Observatory
Administration Office, Chief

Nobeyama Radio Observatory
General Affairs Section, Chief

2013/4/1

Sato, Kanako

Promoted

Administration Department Financial
Administration Department
Affairs Division Asset Management Section, General Affairs Division Employee
Senior Staff
Section, Staff

Employee on Annual Salary System
Date
Name
ChangeNew Affiliated Institute, Position
Hinode Science Center, Specially Appointed
Assistant Professor

2013/4/1

Ishikawa, Ryoko

Hired2013/4/1

Tanaka, Masayuki

HiredSubaru Telescope, Specially Appointed
Assistant Professor

2013/4/1

Shinnaga, Hiroko

Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

Previous Affiliated Institute, Position

III Organization

121

122

2013/4/1

Nagai, Hiroshi

Hired

NAOJ Chile Observatory, Specially
Appointed Assisitant Professor

2013/4/1

Akiyama, Eiji

Hired

NAOJ Chile Observatory, Specially
Appointed Assisitant Professor

2013/4/1

Nagayama, Takumi

Hired

Mizusawa VLBI Observatory, Specially
Appointed Postdoctoral Fellow

2013/4/1

Takekoshi, Tatsuya

HiredNobeyama Radio Observatory, Specially
Appointed Postdoctoral Fellow

2013/4/1

Miura, Rie

Hired

NAOJ Chile Observatory, Specially
Appointed Postdoctoral Fellow

2013/4/1

Yoshida, Tessei

Hired

Astronomy Data Center, Specially Appointed
Postdoctoral Fellow

2013/4/1

Yamaguchi, Masaki

Hired

JASMINE Project Office, Specially
Appointed Postdoctoral Fellow

2013/4/1

Nishizuka, Naoto

Hired

Hinode Science Center, Specially Appointed
Postdoctoral Fellow

2013/4/1

Kurono, Yasutaka

Hired

NAOJ Chile Observatory, Specially
Appointed Postdoctoral Fellow

2013/4/16

Chibueze, James
Okwe

Hired

NAOJ Chile Observatory, Specially
Appointed Postdoctoral Fellow

2013/5/1

Herrera Contreras,
Cinthya Natalia

Hired

NAOJ Chile Observatory, Specially
Appointed Postdoctoral Fellow

2013/5/1

Pena Arellano,
Fabian Erasmo

Hired

Gravitational Wave Project Office, Specially
Appointed Postdoctoral Fellow

2013/5/15

Komugi, Shinya

Hired

NAOJ Chile Observatory, Specially
Appointed Associate Professor

2013/5/16

Suematsu, Sayaka

Hired2013/6/1

Ao, Yiping

Hired2013/7/1

Hatsukade, Bunyo

Hired

NAOJ Chile Observatory, Specially
Appointed Assisitant Professor

2013/7/1

Minamidani,
Tetsuhiro

HiredNobeyama Radio Observatory, Specially
Appointed Postdoctoral Fellow

2013/9/1

Flaminio, Raffaele

HiredGravitational Wave Project Office, Specially
Appointed Professor

2013/9/1

Fujii, Michiko

Hired

Division of Theoretical Astronomy,
Specially Appointed Assistant Professor

2013/9/1

Dominjon, Agnes
Micheline

Hired

Advanced Technology Center, Specially
Appointed Postdoctoral Fellow

2013/9/1

Antolin, Patrick

Hired

Hinode Science Center, Specially Appointed
Postdoctoral Fellow

2013/9/30

Matsuoka, Yoshiki

HiredDivision of Optical and Infrared Astronomy,
Specially Appointed Assistant Professor

2013/9/30

Narukage, Noriyuki

HiredAdvanced Technology Center, Specially
Appointed Postdoctoral Fellow

2013/9/30

Friedrich, Daniel
Dieter

Hired

Gravitational Wave Project Office, Specially
Appointed Postdoctoral Fellow

2013/10/15

Kandori, Ryo

Hired

Extrasolar Planet Detection Project Office,Specially Appointed Postdoctoral Fellow

2013/12/1

Kim, Jeoung Sook

Hired

Mizusawa VLBI Observatory, Specially
Appointed Postdoctoral Fellow

2013/5/24

Reed, Sarah Jane

Resigned

III Organization

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

Specially Appointed Senior Specialist
NAOJ Chile Observatory, Specially
Appointed Postdoctoral Fellow

Public Relations Center, Specially
Appointed Senior Specialist2013/12/31 Yamamiya, Osamu

Resigned

Human Resources Planning Office, Specially Specially Appointed SeniorAppointed Senior Specialist
Specialist

2013/12/31 Suematsu, Sayaka

Resigned

Human Resources Planning Office, Specially Specially Appointed SeniorAppointed Senior Specialist
Specialist

2014/2/28

Friedrich, Daniel
DieterResigned

2014/3/31

Chibueze, James
Okwe

Resigned

2014/3/31

Nishizuka, Naoto

Contract
Expired2014/3/31

Chiba, Kurazo

Contract
ExpiredEngineering Promotion Office, Specially
Appointed Senior Specialist

Research Administrator Staff
Date
Name

Change2014/1/1

Yamamiya, Osamu

Hired

Previous Affiliated Institute, Position
New Affiliated Institute, Position
Human Resources Planning Office, Specially Specially Appointed SeniorAppointed Senior Specialist
Specialist

2014/1/1

Suematsu, Sayaka

Hired

Human Resources Planning Office, Specially Specially Appointed SeniorAppointed Senior Specialist
Specialist

2014/2/1

Ota, Masahiko

Hired

Safety and Health Management Office,Specially Appointed Senior Specialist

Gravitational Wave Project Office,Specially Appointed Postdoctoral
Fellow
NAOJ Chile Observatory, Specially
Appointed Assisitant Professor

NAOJ Chile Observatory, Specially
Appointed Postdoctoral Fellow
Hinode Science Center, Specially
Appointed Postdoctoral Fellow
NAOJ Chile Observatory, Specially
Appointed Senior Specialist

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.
Foreign Visiting Researcher
NameYan, Jianguo
Cameron, Robert Harold
Mathews, Grant James
Lites, Bruce William
Priest, Eric Ronald

Period2013/4/11 ~ 2014/3/20
2013/7/16 ~ 2013/9/13
2013/6/12 ~ 2013/12/20
2013/9/18 ~ 2013/11/15
2013/10/17 ~ 2013/11/15

Affiliated InstituteWuhan University
Max Planck Institute
University of Notre Dame
National Center for Atmospheric Research
University of St Andrews

7. Advisory Committee for Research and Management
Members
From universities and related institutes
Umemura, Masayuki University of Tsukuba
Ohta, Kouji
Kyoto University
Onishi, Toshikazu
Osaka Prefecture University
Okumura, Sachiko
Japan Women's University
Kajita, Takaaki
The University of Tokyo○ Kusano, Kanya
Nagoya University
Nakagawa, Takao
Japan Aerospace Exploration Agency
Nagahara, Hiroko
The University of Tokyo
Matsumoto, Ryoji
Chiba University
Yamada, Toru
Tohoku University

From NAOJ
Arimoto, Nobuo
Iye, Masanori
Kawaguchi, Noriyuki
Gouda, Naoteru
Kobayashi, Hideyuki
Sakurai, Takashi
Takami, Hideki
Tomisaka, Kohji
Hasegawa, Tetsuo
Fukushima, Toshio● Watanabe, Junichi

Subaru Telescope
TMT Project OfficeMizusawa VLBI Observatory
JASMINE Project OfficeMizusawa VLBI Observatory
Solar Observatory
TMT Project Office
Division of Theoretical Astronomy
NAOJ Chile Observatory
Public Relations Center
Public Relations Center● Chairperson ○ Vise-Chairperson
Period: April 1, 2012 - March 31, 2014
III Organization

123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
Professor Emeritus (Tokyo Astronomical Observatory)
Takase, Bunshiro
Akabane, Kenji
Moriyama, Fumio
Kozai, Yoshihide
Staff Emeritus (International Latitude Observatory of Mizusawa)
Hosoyama, Kennosuke

124

III Organization

IV Finance
Revenue and Expenses (FY2013)
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
Rexenue-Expenses

Budget13,247,252
593,582
83,30439,924528,224
0
14,492,286
Budget13,287,176
3,332,346
9,954,830
593,582
83,304528,224
14,492,286
Budget0

Final Account13,366,515
426,800
138,218
52,434
425,541
4,704
14,414,212
Final Account12,618,742
3,172,304
9,446,438
426,800
138,218
321,482
13,505,242
Final Account908,970

Budget − Final Account−119,263
166,782−54,914−12,510
102,683−4,70478,074
Budget − Final Account668,434
160,042508,392
166,782−54,914206,742
987,044
Budget − Final Account−908,970

IV Finance125

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2013
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)Scientific Research (C)Specially Promoted Research
Young Scientists (B)
JSPS Fellows
Research Activity Start-up
Total

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

Total

8

164,800

49,440214,240

2
8
4
0
0
0
9
1
32

53,70049,8006,100
0
0
0
10,7101,100
286,210

16,11014,940
1,830
0
0
0
0
330
82,65069,81064,7407,930
0
0
010,7101,430
368,860

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding
15,750
4,725
1,600
480
12,8003,840
30,1509,045

Total
20,4752,080
16,64039,195

2. Multi-year Fund for FY 2013
Research Categories

Number of Selected Projects

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

15
2
12
29

3. Partial Multi-year Fund for FY2013

126

Research Categories

Number of
Selected Projects

Scientific Research (B)Young Scientists (A)
Total

4
3
7

Budget (Series of Single-year Grants)(Unit: ¥1,000)
Direct Funding Indirect Funding
Total
17,9005,370
23,2707,800
2,340
10,14025,7007,710
33,410V KAKENHI (Grants-in-Aid for Scientific Research)

Budget (Multi-year Fund)(Unit: ¥1,000)
Direct Funding Indirect Funding Total
10,1003,030 13,130
8,100
2,430 10,530
18,2005,460 23,660

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
45-m telescope (General Proposal)
45-m telescope (Education Program)
45-m telescope (Short Program)
45-m telescope (Back-up Program)
Nobeyama Solar Radio Observatory
Mizusawa VLBIOpen Use at
VERA
Project/Center Observatory
Nobeyama Radio
Observatory

Astronomy Data Center

Number of
Total
Accepted Number of
Proposal Researcher

Note

1
17
0
93
*1
34
0
12
2
33

24 (0)
2 Institutes
99 (0)
10 Institutes
00342 (40) 60 Institutes, 12 Countries*1*1
212 (36) 38 Institutes, 11 Countries0
79 (10) 25 Institutes, 6 Countries
17
5 Institutes
118 (69) 30 Institutes, 9 Countries

4

33 (16)

16 Institutes, 6 Countries

175

175 (5 atforeigninstitutes)

36 Institutes, 4 Countries,
Total amount of requested
data 20.4 TB

Center for Computational Astrophysics
173
173 47 Institutes, 6 Countries
Hinode Science Center130
130 (43) 52 Institutes, 14 Countries
Facility Use27
123 (2)51 Institutes
Advanced
Technology Center
Joint Research and Development
537
12 Institutes
ALMA
*2
*2
*2
NAOJ Chile
ASTE
13
72
14 Institutes
Observatory
Mopra
37
247 27 Institutes, 7 Countries
Joint Development Research
8
8 Institutes
Joint Research2
2 Institutes
Research Assembly15
9 Institutes
The number of foreign researchers shown in brackets ( ) is included in the total.
Notes shows the number of institutes and foreign countries represented by the proposal PIs. The country count does not include Japan.
*1 The observation data is open to the public on the web. No application is needed to use the data.
*2 Cycle 1 is supposed to end in May 2014. There is no data to show here.

VI Research Collaboration

1272. Commissioned Research Fellows
Visiting Scholars
Period: April 1, 2013 - March 31, 2014
No.
Name
1 Onishi, Toshikazu
2 Sakamoto, Seiichi
3 Namiki, Noriyuki

Position at NAOJ
Visiting Professor
Visiting Professor
Visiting Professor

4 Hayashi, Yoshi-yuki

Visiting Professor

5
6
7
8
9
10
11

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

Fujisawa, Kenta
Momose, Munetake
Imai, Hiroshi
Iwata, Takahiro
Oka, Tomoharu
Hirata, Naru
Yonekura, Yoshinori

12 Nomura, Hideko

Visiting Associate Professor

13 Kurayama, Tomoharu

Visiting Research Fellow

14 Nishimura, Shunji

Visiting Research Fellow

Affiliated Institute
Host Project/Center/Division
Osaka Prefecture University
NAOJ Chile Observatory
Japan Aerospace Exploration Agency NAOJ Chile Observatory
Chiba Institute of Technology
RISE Project
Astronomy Data Center/Center
Kobe University
for Computational Astrophysics
Yamaguchi University
Mizusawa VLBI Observatory
Ibaraki University
NAOJ Chile Observatory
Kagoshima University
Mizusawa VLBI Observatory
Japan Aerospace Exploration Agency RISE Project
Keio University
NAOJ Chile Observatory
University of Aizu
RISE Project
Ibaraki University
Mizusawa VLBI Observatory
Division of TheoreticalTokyo Institute of Technology
Astronomy
Teikyo University of Science
Mizusawa VLBI Observatory
Division of Theoretical
RIKEN
Astronomy

JSPS (Japan Society for the Promotion of Science) Postdoctoral Research Fellows
Name
Koyama, Yusei
Hori, Yasunori
Ishikawa, Shinnosuke
Kwon, Jungmi
Tadaki, Kenichi
Niino, Yuu
Hada, Kazuhiro
Matsuoka, Yoshiki

Host Researcher
Arimoto, Nobuo
Kokubo, Eiichiro
Suematsu, Yoshinori
Watanabe, JunichiIye, Masanori
Kashikawa, Nobunari
Honma, Mareki
Kashikawa, Nobunari

JSPS (Japan Society for the Promotion of Science) Foreign Research Fellows
Name
GLESENER, Lindsay Erin

128

VI Research Collaboration

Program
PeriodHost Researcher
Postdoctoral Fellowship for North American and European
2013/12/1~2014/1/31 Hara, Hirohisa
Researchers

VII Graduate Course Education
1. Department of Astronomical Science, School of Physical Sciences,
the Graduate University for Advanced Studies
The Graduate University for Advanced Studies wasestablished as an independent graduate university without
undergraduate courses via partnerships with inter-university
research institutes for the sake of advancing graduate education.
There used to be four schools – Cultural and Social
Studies, Mathematical and Physical Sciences, Life Science,and Advanced Sciences before the reorganization of the Schoolof Mathematical and Physical Sciences into the schools ofPhysical Sciences, High Energy Accelerator Science, andMultidisciplinary Sciences in April 2004. Now the total ofsix schools are offering doctoral education and research
opportunities.
NAOJ has been accepting three-year doctoral course
students since FY 1992 and five-year students since FY 2006
for the Department of Astronomical Science at the School ofPhysical Sciences. (The School of Mathematical and PhysicalSciences was reorganized into the School of Physical Sciencesin April 2004.)(1) Objective of the Department of Astronomical Science
The Department of Astronomical Science aims to train
students, through observational, theoretical or instrument
development research in astronomy or in related 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 2013, the Department of Astronomical Science accepted
four students in the Basic Course and three 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 November
13 to 15, 2013, as well as the 2013 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 Education

129

(5) Number of Affiliated Staff (2014/3/31)
Chair of the Department of Astronomical Science
Optical and Near Infrared Astronomy Course
Professors
Associate Professors
Lecturer
Assistant Professors
Radio Astronomy Course
Professors
Associate Professors
Assistant Professors
General Astronomy and Astrophysics Course
Professors
Associate Professors
Assistant Professors
Total

1
9
12
1
9
6
10
18
8
11
14
99

(6) Graduate Students (30 students)
1st year (5 students)
Name
Principal Supervisor
Supervisor
Okutomi, Koki
Tomisaka, Koji
Watanabe, Junichi
Onoue, Masafusa Kashikawa, Nobunari Miyazaki, Satoshi
Nagasawa, Ryosuke Hanada, Hideo
Matsumoto, Koji
Baba, Haruka
Aoki, Wako
Usuda, Tomonori
Usuda, Tomonori
Ryu, Tsuguru
Hayashi, Saeko
2nd year (7 students)
Principal Supervisor
Supervisor
Name
Yang, Yi
Hayashi, Saeko
Usuda, Tomonori
Kashikawa, Nobunari Kodama, Tadayuki
Ishikawa, Shogo
Onishi, Kyoko
Iguchi, Satoru
Kuno, Nario
Onitsuka, Masahiro Usuda, Tomonori
Takato, Naruhisa
Sakurai, Junya
Miyazaki, Satoshi Kobayashi, Yukiyasu
Shimakawa, Rizumu Kodama, Tadayuki Arimoto, Nobuo
Suzuki, Taiki
Oishi, Masatoshi
Saito, Masao
3rd year (6 students)
Principal Supervisor
Supervisor
Name
Kodama, Tadayuki
Aoki, Sumire
Arimoto, Nobuo
Saito, Yuriko
Imanishi, Masatoshi Kashikawa, Nobunari
Hashizume, Katsuya Osuga, Ken
Tomisaka, Koji
Saito, Masao
Matsuzawa, Ayumu Iguchi, Satoru
Oh, Daehyeon
Aoki, Wako
Takami, Hideki
Suematsu, Yoshinori Hara, Hirohisa
Giono, Gabriel

130

VII Graduate Course Education

Name
Kataoka, Akimasa
Shino, Nagisa
Min, Cheul HongToshikawa, Jun

4th year (4 students)
Principal Supervisor
Supervisor
Tomisaka, Koji
Nakamura, Fumitaka
Honma, Mareki
Shibata, Katsunori
Honma, Mareki
Shibata, Katsunori
Kashikawa, Nobunari Kodama, Tadayuki

5th year (8 students)
Principal Supervisor
Supervisor
Name
Ishizaki, Yoshifumi Kashikawa, Nobunari Iye, Masanori
Imase, Keisuke
Kodama, Tadayuki Kashikawa, Nobunari
Suenaga, Takuya
Usuda, Tomonori
Aoki, Wako
Sakai, Nobuyuki
Honma, Mareki
Shibata, Katsunori
Sako, Nobuharu
Watanabe, Tetsuya Sekii, Takashi
Sukom, Amnart
Hayashi, Saeko
Izumiura, Hideyuki
Kaithakkal, Anjali John Suematsu, Yoshinori Sekii, Takashi
Pan, Hsi-An
Kuno, Nario
Iono, Daisuke
Research Student (1 student)
Name
Supervisor
Tsuchiya, Tomoe
Watanabe, Junichi2. Education and Research Collaboration with Graduate Schools
Name
Okada, Takashi
Kasuga, Megumi
Kato, Yuta
Sakai, Daisuke
Tezuka, Kenjiro
Baba, Fuko
Hirai, Yutaka
Lee, Minju
Aso, Yusuke
Iwaki, Daichi
Ohashi, Satoshi
Saito, Toshiki
Shibagaki, Shota
Shibata, Takashi
Sekiguchi, Sigeyuki
Tagawa, Hiromichi
Miyagawa, Kenta
Aoki, Kunichika
Koyamatsu, Shin
Sekine, Masakazu
Hara, TakujiHara, Chihomi
Fujii, Kosuke
Akiyama, Kazunori
Kiyokane, Kazuhiro
Fujii, Akihiko
Ueda, Junko
Koyama, Shoko
Takahashi, Yasuhiro
Hayashi, Takayuki
Higuchi,Yuichi
Rusu Cristian Eduard
Kasai, Miho
Kubo, Daiki
Watanabe, Dota

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

Supervisor
Sekimoto, YutaroHara, Hirohisa
Mizuno, Norikazu
Kobayashi, Hideyuki
Gouda, Naoteru
Hara, Hirohisa
Kajino, Toshitaka
Kawabe, Ryohei
Ohashi, Nagayoshi
Iye, Masanori
Mizuno, Norikazu
Kawabe, Ryohei
Kajino, Toshitaka
Kokubo, Eiichiro
Sekimoto, Yutaro
Gouda, Naoteru
Hara, Hirohisa
Hara, Hirohisa
Ohashi, Nagayoshi
Sekimoto, Yutaro
Gouda, Naoteru
Kawabe, Ryohei
Mizuno, Norikazu
Kobayashi, Hideyuki
Mizuno, Norikazu
Kokubo, Eiichiro
Kawabe, Ryohei
Kobayashi, Hideyuki
Tamura, Motohide
Kobayashi, Hideyuki
Iye, Masanori
Iye, Masanori
Matsuo, Hiroshi
Matsuo, Hiroshi
Matsuo, Hiroshi

3. Commissioned Graduate Students
Doctoral Course
Ui, Takahiro
Oya, Masahito
Mizuno, Izumi
Nomura, Mariko
Horie, Masaaki
Sekiguchi, Takanori
Ono, Yoshito

Affiliated Institute
Hiroshima University
Nihon University
Kagoshima University
Ochanomizu University
Nihon University
The University of Tokyo
Tohoku University

Period2013/4/1~2014/3/31
2013/4/1~2014/3/31
2013/4/1~2014/3/31
2013/4/1~2013/12/31
2013/4/1~2014/3/31
2013/12/1~2014/3/31
2014/1/6~2014/3/31

Supervisor
Yamashita, Takuya
Watanabe, Junichi
Kuno, Nario
Tomisaka, Kouji
Watanabe, Junichi
Flaminio, Raffaele
Iwata, Ikuru

Master's Course
Chida, Hikaru
Fukase, Masao
Hokama, Kazuki

Affiliated InstituteTokai University
Nihon University
University of the Ryukyus

Period2013/4/1~2014/3/31
2013/4/1~2014/3/31
2013/4/1~2014/3/31

Supervisor
Honma, Mareki
Watanabe, Junichi
Honma, Mareki

VII Graduate Course Education

1314. Degrees Achieved with NAOJ Facilities
Name

132

DegreePan, Hsi-An

Doctor of Philosophy, SOKENDAI

Sakai, Nobuyuki

Doctor of Philosophy, SOKENDAI

Suenaga, Takuya

Doctor of Philosophy, SOKENDAIIshizaki, Yoshifumi

Master of Science, SOKENDAI

Hashizume, Katsuya

Master of Science, SOKENDAIVII Graduate Course Education

ThesisEnvironmental Dependence of Star Formation in Nearby Barred Spiral
Galaxies
Spiral Structure and Non-Circular Motions of the Milky Way Galaxy
Revealed by VLBI Astrometry
Brown Dwarfs and Planetary Mass Objects in Star Forming Regions:
Toward the Low Mass End of Initial Mass Function
Search for quasars at redshift 7 using Subaru telescope
Global structure of super-critical accretion flows and outflows inradiation hydrodynamic simulations

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: 18,552
Open facilities: 65-cm Telescope Dome (Observatory
History Museum), 20-cm Telescope Dome, Solar Tower
Telescope, Exhibit Room, Housing of Repsold Transit
Instrument (Transit Instrument Museum), Astronomical
Instruments Museum, Gautier Meridian Circle, Old Library[Regular Star Gazing Party]
Dates: Friday before second Saturday; fourth Saturday
Visitors: 4,740 (22 events)
Open facility: 50-cm public telescope[Special Open-House Event] Mitaka Open House Day
Dates: October 18 (Fri), 2013, 14:00–19:00
October 19 (Sat), 2013, 10:00–19:00
Topic: The Origin of Galaxies and Planets Explored by
ALMA
Visitors: 4,176[Open year-round]
Dates: April to March (except for New Year season), 9:00–
17:00 daily
Visitors: 14,593
Open facilities: Kimura Hisashi Memorial Museum, VERA
20 m antenna, 10 m VLBI antenna[Special Open Day] Held as part of Iwate Galaxy Festival 2013
(Hours: 10:00–21:00)
An open house event was held on campus with cooperationfrom the Oshu Space and Astronomy Museum (Yugakukan),which opened in the city of Oshu in April 2008.
Date: August 24 (Sat), 2013, 10:00–16:00
Visitors: 3,016 (total for Galaxy Festival, of which 942
participated in Open House)

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 theInstitute of Astronomy (“Exploring the Mysteries of Black Holesfrom the South American Atacama Desert” Kotaro Kohno,
Professor, the University of Tokyo) and by NAOJ (“Solving
the Mysteries of Galaxy Evolution with ALMA” Iono Daisuke,
Associate Professor, NAOJ; “Approaching the Site of Star
Formation with ALMA” Nagayoshi Ohashi, Professor, NAOJ.)
Neither day had favorable weather, but the plans of eachproject were realized. Attendance was comparable to theprevious year. In addition to the opening of facilities normallyclosed to the public, interactive displays and mini-lectures, there
were also games and quizzes popular with children to engage awide 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.

As last year, the event was co-hosted with Ihatov Space
Action Center and the city of Oshu. The event opened witha performance by a marching band from a local elementary
school, and featured workshop corners run by local university
and high school students, along with other forms of community
involvement.
Attractions included discussions of the research results
obtained from the VERA and RISE projects, a tour of the 20m
parabolic antenna, a commemorative photo booth, plastic bottle
rockets, a quiz game, and guided tours of the Kimura Hisashi
Memorial Museum.
To the delight of visitors, the Memorial Museum's
exhibitions included a special exhibition of hand-written lettersand similar memorabilia of the museum’s First Director Kimura
Hisashi, for the 70th anniversary of his death in 2013.
The main attraction this time was the super-computer“Aterui”.This tour was so popular that all vacancies were filled,with many interested visitors unable to participate due to thestrong demand.
A live internet connection was also established toNobeyama, where an event was held in conjunction with a
special open house. A lecture was delivered by Saeko Hayashi
and Seiichi Tazawa of Hilo campus, who connected live from
Hawaii to talk about the research results obtained with the
Subaru Telescope. Evening events for the Iwate Galaxy Festival
2013 included a lecture given by Associate Professor Makoto
Yoshikawa of JAXA on “Asteroid Mission: New Challenges for
Hayabusa 2”. Attractions in the Astronomy Museum included
experiments titled “Science’s Mystery”, demonstrations by ascientist and a workshop by internship students. The festival was
brought to its successful conclusion with a stargazing session.

VIII Public Access to Facilities

133

Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for New Year season)
Visitors: 1,689[Special Open House]
Date: August 11 (Sat), 2013 10:00–21:00
Visitors: Approximately 1,500
The special open house event was repeated this year in
conjunction with Yaeyama Kogen Star Festival 2013 hosted
by the executive committee primarily formed by membersof Satsuma-Sendai city hall and Kagoshima University. The
antenna had been repaired and re-coated for the first time ina decade, with work finishing the day before the special open
house. Many visitors were welcomed by the brand new purewhite antenna. Regular annual antenna tours, demonstrationsof observational equipment, mini-lecture events, and stargazing
sessions were held in the VERA 20m radio telescope and 1m
optical/infrared telescope facilities, proving to be a hit withvisitors all day long. A lecture was given by Kokubo of CfCA
about the Moon. Also popular were the physics experiments
attended by a total of 200 students, offering a chance toexperience the joy of scientific experimentation.
Ogasawara: VERA Ogasawara Station[Open year-round]
Dates: April to March (except for New Year season)
Visitors: 6,371[Special Open House]
Date: November 11 (Sat), 2013, 10:00–17:00
Visitors: 188
A special open house event was again held this year under
the name “Star Island 2013.” Once again a free shuttle bus
was available and the event proved popular with community
members, with similar attendance to previous years. Attractions
included discussions of the research results obtained by the
VERA and RISE projects, hands-on sessions in operating the
20m radio telescope, mystery experiment corners and quiz
games, as well as a four-dimensional digital planetarium showfeaturing 4D2U technology that was a central attraction toaudience members. NAOJ also cooperated in a stargazing
session on November 7th hosted by the local astronomy club,held in favorable weather conditions, with many students
attending as part of school trips. The event was an unprecedented
success, attended by approximately 200 visitors. Lectures werealso given by Oshigami of the RISE Projects and Utsumaki
of JAXA Space Center at the Ogasawara Visitor Center on
November 8th.
Ishigakijima: VERA Ishigakijima Station[Open year-round]
Dates: April to March (except for New Year season); premises
are open to the public 24 hours/day, and observation rooms
are also open during the hours of 10:00–16:30.
Visitors: 15,213

134

VIII Public Access to Facilities[Special Open House]
Date: August 11 (Sat), 2013, 10:00–17:00
Visitors: 246
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.
Ishigakijima: Ishigakijima Astronomical Observatory[Open year-round]
Dates: April to MarchOpen Hours: Wednesdays through Sundays (except for New
Year season), 10:00–17:00
Stargazing sessions: Evenings on Saturdays, Sundays,
Holidays, and Star Festival weekdays (19:00–22:00), three
30-minute sessions per evening (four in August)
Visitors: 12,915
Open facilities: Murikabushi 105-cm optical/infrared
telescope, interior of observation dome (including exhibitsof astronomical images)[2012 South Island Star Festival]
Dates: August 3 (Sat) to August 18 (Sun), 2013
Visitors: 10,546
This year, the VERA station of Ishigakijima was finallycompleted, just in time for the 12th anniversary of the Star
Festival of the Southern Island.
There were approximately 8,500 visitors attending thedimmed-light stargazing event under a stunning night sky ofunprecedented clarity.
Ishigakijima Astronomical observatory has been able tofulfill its main objective as a pivotal research facility, while
making important steps towards a successful interchange withthe local community and drawing in a large number of visitors
interested in its activity. Such attention is expected to continue
growing during next year’s season. This interaction is important
for the institution, and we expect this bond to continue tostrengthen and prove beneficial for all.

3. Nobeyama Campus

4. Okayama Campus[Regular Open]
Open Time: 8:30–17:00 (every day except around New YearDays (Dec. 29 to Jan. 3), especially, open until 18:00 during
the summer (Jul. 20 to Aug. 31))
Visitors: 55,808
Open facilities: 45-m Radio Telescope, Nobeyama Millimeter
Array, Nobeyama Radioheliograph, etc. (just viewing)[Open House Day]
Date: August 24 (Sat), 2013, 9:30–16:00
Visitors: 2,735

Okayama Astrophysical Observatory[Open year-round]
Dates: 9:00–16:30 daily
Visitors: 12,935
Open facilities: Window view of 188-cm reflecting telescope[Special Open House]
Date: August 31 (Sat), 2013, 9:30–16:30
Visitors: 515

The Nobeyama branch was crowded with 2,735 visitorson the 2013 Open House Day. The theme of the Day was“Link up with the Cosmos, the Sun, and the Life”. We had
two lectures on the theme, which attract large audiences every
year. One was “Variations of the Solar Activity found out
by Radio Observations —Current Solar Status seen in Long
Term Observations” by Prof. Shibasaki, Kiyoto (NAOJ). The
other was “Biotic Species in the Universe —Searching for
Origins of Life” by Dr. Ohishi, Masatoshi (NAOJ). We hadsome established events such as demonstrations of 45 -m Radio
Telescope observations, touch the main reflector panel, radio
detector handicrafts, short lectures, a stamp rally, and so on. In
addition, new exhibitions by NRO alumni and other project staff
members took place. Nobeyama was very lively on that day.

The special open house event for FY 2013 was co-hosted
with the Okayama Astronomical Museum on August 31 (Sat).
The nearly one-hour special lecture given by NAOJ director
general Masahiko Hayashi on “How the Universe got to berecognized” in the dome of the 188-cm reflecting telescope was ahuge success, with nearly 100 audience members in attendance.
The lecture was broadcast over the Internet with assistance fromthe Public Relations Center. In addition, three short lectures
were given by professor Tetsuya Nagata of Kyoto University on“3.8m telescope unlock the mystery of black holes” gatheringa total attendance of 100. The always-popular tours of the main
mirror of the 188-cm reflecting telescope were conducted in
the morning and afternoon with maximum capacities of 120
participants. Planetarium showings, astronomy-related crafts,
and constellation/astronomy bingo were held at the Okayama
Astronomical Museum. Because it was raining, there weresome events which were canceled. But, we think many visitors
enjoyed themselves.
The special open house event was co-hosted with the
Asakuchi City Board of Education, with support from theYakage Town Board of Education. In particular, the Observatory
would like to thank the members of the Asakuchi City Boardof Education for their considerable assistance in arranging
complimentary shuttle bus service between the Observatory and
Kamogata Station on the JR San’yo Main Line.
[Special Stargazing Party]
Date: October 12 (Sat), 2013, 17:00–21:45
Visitors: 108
122 applications for 360 applicants were received. The firstquarter moon and the M15 globular cluster were viewed.
Special stargazing parties co-hosted with the Okayama
Astronomical Museum were held twice over the course of theyear, in spring and fall. Maximum participation for each special
session was 100. As applications exceeded capacity for bothsessions in previous years, participants were selected by lottery,with 120 winners being selected to allow for cancellations.
Main events included tours of the Okayama Astronomical
Museum, planetarium shows, astronomical observation using the
188-cm reflecting telescope, and descriptions of the night sky.

VIII Public Access to Facilities

1355. Subaru Telescope[Summit Facility]
Dates open for public tour: 95 (these dates are listed in the
public tour program page at the Subaru Telescope’s web site,
the tour was suspended in August and September due to themirror coating and other telescope work)
Public tour visitors: 521
Special tour visitors: 138 visits, 776 visitors
As some special tours were conducted during public tour
programs, the total number of actual visitors was 1,269.
[Base Facility]
Special tour visitors: 50 visits, 526 visitors[Outreach activities]
1. Gave a lecture at the Subaru Telescope’s base facility in
Hilo
2013
April 25: Two astronomers gave Japanese lectures at theSubaru Telescope’s base facility in Hilo for the conference
participants of “ASIAGRAPH 2013” held at University of
Hawai’i at Hilo.

December 13: Subaru Telescope staff gave a Japanese
lecture at the Subaru Telescope’s base facility in Hilo forstudents of Masuda Senior High School from Shimane.
2014
January 6: Subaru Telescope staff gave a Japanese lecture at
the Subaru Telescope’s base facility in Hilo for students of
Wakimachi High School from Tokushima.
January 9: Subaru Telescope staff gave a Japanese lecture at
the Subaru Telescope’s base facility in Hilo for students ofSeisho High School from Nara.
January 28: Subaru Telescope staff gave a Japanese lecture
at the Subaru Telescope’s base facility in Hilo for students ofSanbonmatsu High School from Kagawa.
February 24: Subaru Telescope staff gave a Japanese lecture
at the Subaru Telescope’s base facility in Hilo for students ofTokyo Institute of Technology.

July 29: Subaru Telescope staff gave a Japanese lecture
at the Subaru Telescope’s base facility in Hilo for theMusashidai Senior High School students from Fukuoka.

February 26: Subaru Telescope staff gave a Japanese lecture
at the Subaru Telescope’s base facility in Hilo for highschool students from Okinawa.

August 5: Subaru Telescope staff gave a Japanese lecture
at the Subaru Telescope’s base facility in Hilo for Miyako
Town delegates from Fukuoka.

March 4: Subaru Telescope staff gave a Japanese lecture at
the Subaru Telescope’s base facility in Hilo for students ofIiyama Kita High School from Nagano.

September 12: Subaru Telescope staff gave a Japanese
lecture at the Subaru Telescope’s base facility in Hilo forstudents of Tokai University.

March 17: Subaru Telescope staff gave a Japanese lecture at
the Subaru Telescope’s base facility in Hilo for students of
Ena High School from Gifu.

October 1: Subaru Telescope staff gave a Japanese lecture at
the Subaru Telescope’s base facility in Hilo for students ofNamiki Secondary School from Ibaraki.
October 26: Subaru Telescope staff gave a Japanese/English
mixed lecture at the Subaru Telescope’s base facility in
Hilo for students of the Hawaii Japanese School (Rainbow
Gakuen) from Honolulu.

2. Remote presentation
2013
April 28: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to the National Museum of Emerging
Science and Innovation in Tokyo.

November 12: Subaru Telescope staff gave a Japanese
lecture at the Subaru Telescope’s base facility in Hilo forstudents of Kunori Gakuen High School from Yamagata.

May 10: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to the Science Museum in Tokyo.
[Kagakugijutsukan]

November 18–21: Staff of Subaru Telescope and NAOJ
conducted two observation programs together - one for
SOKENDAI graduate students course work and the other forundergraduate students chosen from universities in Japan for
their experience.

June 17: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Koyodai Elementary School in
Miyagi. (as part of supporting the recovery effort fromMarch 11, 2011 disaster)December 2&4: Subaru Telescope staff gave Japanese136

lectures at the Subaru Telescope’s base facility in Hilo forstudents of Senri High School from Osaka.

VIII Public Access to Facilities

July 19: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Tokyo Future University in Tokyo.
July 19: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to the Science Museum in Tokyo.
[Kagakugijutsukan]
July 22: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Wakayama Shin-ai Junior and SeniorHigh School.
August 9: Subaru Telescope staff gave a Japanese presentation
via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Galaxcity (Adachi Children Future
Creation Hall) in Tokyo.
September 26: Subaru Telescope staff gave presentation via
remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Sendai Shirayuri Gakuen.
October 28: Subaru Telescope staff gave two Japanesepresentations via remote conferencing system from theSubaru Telescope’s base facility in Hilo to Masuda SeniorHigh School in Shimane.
November 1: Subaru Telescope staff gave a Japanesepresentation via remote conferencing system from theSubaru Telescope’s base facility in Hilo to Nayoro City
Observatory.
November 19: Subaru Telescope staff gave Japanesepresentations via remote conferencing system from theSubaru Telescope on Mauna Kea to Kavli IPMU for Ichita
Yamamoto, Minister of State for Special Missions.
December 5: Subaru Telescope staff gave a Japanesepresentation via remote conferencing system from the Subaru
Telescope’s base facility in Hilo to Okinawa Shogaku Juniorand Senior High School in Okinawa.
December 6: Subaru Telescope staff gave a Japanesepresentation via remote conferencing system from theSubaru Telescope’s base facility in Hilo to Arakawa 3rd
Intermediate School in Tokyo.
2014
January 15: Subaru Telescope staff gave a Japanesepresentation via remote conferencing system from theSubaru Telescope’s base facility in Hilo to Aizu Wakamatsu
3rd Junior High School in Fukushima. (as part of supporting
the recovery effort from March 11, 2011 disaster)

3. Lectures, demonstrations, workshops etc. in the vicinity
2013
April 22: Subaru Telescope staff gave astronomy
demonstration in English at an Earth Day event in Waimea.
May 5: A total of 25 Subaru Telescope staff members
provided a big booth of information and demonstrations
about the Subaru Telescope and new discoveries from it at
the AstroDay event in Hilo and interacted with hundreds offamilies in the local community.
July 2: Subaru Telescope staff gave a lecture in English at asummer school program at Kamehameha School.
July 26: Subaru Telescope staff provided astronomy
workshop and assisted stargazing during the PacificAstronomy and Engineering Summit (including high school
students from the Island of Hawaii, Canada, Japan, China,
and India.)
August 4: Subaru Telescope staff gave Japanese a presentation
at Kilauea Military Camp for Japanese intermediate school
students from the Tsunami/Nuclear power plant disaster
afflicted area.
August 10: Subaru Telescope staff gave a presentation
in English for local high school students about meteors(shooting stars) and recent topics of Solar System research,
at Mauna Kea State Park.
October 18: Two astronomers of Subaru Telescope gave
presentation in English at Maunakea Sky lecture series at‘Imiloa Astronomy Center.
2014
February 27: Subaru Telescope staff made demonstrations
and provided information in English at the Job Expo in Hilotargeting to the high school students.
March 6–14: For the Journey through the Universe program,21 staff members of the Subaru Telescope went to 69 classes
in local public schools (from Preschool to 12th grade) anddelivered presentations, hands-on experiences, and otherdemonstrations in English.
March 7: 5 staff members of the Subaru Telescope madepresentations in English at the Master Educator Workshop.
March 9: Subaru Telescope staff had a booth of information
and astronomy demonstrations at an open house event at‘Imiloa Astronomy Center.

VIII Public Access to Facilities

1374. Lectures in Japan
2013
March 14: Subaru Telescope staff gave a lecture andtelescope workshop at Mitaka 1st Elementary School inTokyo.
March 19: Subaru Telescope staff gave a presentation at the
Rotary Club of Tokyo Azabu meeting in Tokyo.
March 22: Subaru Telescope staff gave a presentation at theMuseum of Emerging Science in Tokyo.
March 24: Subaru Telescope staff gave a lecture at the
University of the Ryukyus in Okinawa.
March 27: Subaru Telescope staff gave a lecture at the
Okinawa Institute of Science and Technology Graduate
University.(OIST)March 29: Subaru Telescope staff gave a lecture at Naha
Makishi Ekimae Hoshizora Kominkan in Okinawa.
March 30: Subaru Telescope staff gave a lecture at Ishigaki
City Library in Okinawa.
5. Others
2013
June 26: Director Arimoto of the Subaru Telescope wasinterviewed in a radio broadcast program in Honolulu.

138

VIII Public Access to Facilities

IX Overseas Travel
Research and Academic Staff Overseas Travel
country/area

category

Business Trip

Korea
24
China
27
Hong Kong
0
Taiwan49
Malaysia
0Singapore0
Thailand2
Philippines
0Indonesia
0
Other areas in Asia
3
UK
9
Italy
11
Germany
21
France10
Russia3
Other areas in Europe
18
USA
44
Canada2
Hawaii77
Guam, Saipan
0Australia
9
Other areas in Oceania
0
Mexico0Brazil3
Other areas in South and Central America *44
Middle East2
Africa2others0
Total
360* Most travelers to South and Central America went to Chile.

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

24
27
0
49
0
0
2
0
0
3
9
11
21
10
3
18
44
2
77
0
9
0
0
3
44
2
2
0
360

X Award Winners
Award Recipients
Ishiguro, Masato; Hasegawa, Tetsuo;
Iguchi, Satoru
Hara, Hirohisa
Iye, Masanori
Morita Array, Atacama Large Millimeter/
submillimeter Array
Mizusawa VLBI Observatory
Fukuda, Takeo; Nishino, Tetsuo

Award

Date

The Commendation for Science and Technology by the Minister of
Education, Culture, Sports, Science and Technology
Prizes for Science and Technology (Research Category) 20132013/4/16

National Institutes of Natural Sciences Young Researcher Award 2013
Japan Academy Prize 2013, The Japan Academy

2013/6/16
2013/6/17

Good Design Gold Award 2013, Japan Institute of Design Promotion

2013/11/7

NAOJ Director General Prize (Research and Education Category) 2013
NAOJ Director General Prize (Engineering Category) 20132014/3/6
2014/3/6

IX Overseas Travel, X Award Winners

139

XI Library, Publications
1. Library
Number of books in each library (2014/3/31)
Japanese Books
Mitaka16,540
Okayama217
Nobeyama
1,224
Mizusawa
4,942
Hawaii
1,481
Total
24,404Foreign Books
45,1233,290
6,256
18,067
4,050
76,786

Total
61,6633507
7,480
23,0095,531
101,190

Number of journal titles in each library (2014/3/31)
Japanese Journals
Foreign Journals
Mitaka613
767
Okayama4
18
Nobeyama
16
82
Mizusawa
659
828
Hawaii
18
22
Total
1,310
1,717

Total
1,380
22
98
1,487
40
3,027

2. Publication
Here we list continuing publications produced by NAOJ in FY 2013.
The data is based on publications delivered to the libraries.
Mitaka01) Report of the National Astronomical Observatory of Japan, Vol. 15, no. 1–4, 2 issues
02) Annual Report of the National Astronomical Observatory of Japan (in Japanese), no. 25, 2012, 1 issue03) Annual Report of the National Astronomical Observatory of Japan (in English), vol. 15, Fiscal Year 2012, 1 issue04) National Astronomical Observatory Reprint, No. 2464-2547, 88 issues05) Calendar and Ephemeris, 2014, 1 issue06) NAOJ News, No. 237–248, 12 issues07) Guide of National Astronomical Observatory of Japan (Japanese), 1 issue08) Guide of National Astronomical Observatory of Japan (English), 1 issue09) Chronological Scientific Tables, 2014, 1 issue
Okayama10) Okayama Users Meeting Fiscal Year 2013 (24th Optical/Infrared Users Meeting), 1 issue

140

XI Library, Publications

XII Important Dates
April 1, 2013 – March 31, 20142013
April 14

Fourth Open Observatory event held at the Ibaraki University Center for Astronomy and the NAOJ Mizusawa
VLBI Observatory Ibaraki Station, with approximately 1,000 visitors in attendance.

April 22

Subaru Telescope staff gave astronomy demonstrations in English at an Earth Day event in Waimea.

April 26

All 16 of the ALMA antennas developed by Japan were installed at the Array Operations Site by the Joint ALMA
Observatory. These are named the "Morita Array" after the late Professor Morita for his contributions.

May 5

A total of 25 Subaru Telescope staff members provided a big booth of information and demonstrations about
the Subaru Telescope and new discoveries from it at the AstroDay event in Hilo and interacted with hundreds offamilies in the local community.

May 15The ALMA Inauguration Commemorative lecture was held at Hitotsubashi Hall with 203 participants.

June 9A NAOJ/Subaru Telescope lecture meeting “Pursing the Biggest Explosions in the Universe” held in Hitotsubashi
Hall with over 300 visitors in attendance.

June 17

Subaru Telescope staff gave a Japanese presentation via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Koyodai Elementary School in Miyagi (as part of supporting the recovery effort from March
11, 2011 disaster.)June 29–
June 30Pre-event workshop held for 5 high school students scheduled to attend the Seventh Z-star Research Team event
using the radio telescope at the VERA Mizusawa station to search for masers, to improve the understanding of theparticipants.

July 7The Star Festival using 6m antenna was held at the NAOJ Mizusawa VLBI Observatory Kagoshima station in
Kagoshima city Kinko Bay Park, co-hosted with Kagoshima city and Kagoshima University, with approximately
300 participants in attendance.

July 25

On Hawai`i Island, the scientific authorities of each participating country signed a Master Agreement for theconstruction of TMT (Thirty Meter Telescope.) From Japan, NAOJ Director Masahiko Hayashi signed theagreement.

July 25–
July 26“Summer Break Junior Astronomical Classes + You are Galileo” and “Summer Break Junior Astronomical
Observation Sessions” held in Mitaka.

July 29–
August 2

Facility Guide Week for Educational Organization was carried out.

August 1–
September 29

Fourth International Festival of Scientific Visualization—Connecting with Others Through Science—held withover 1 million visitors attending during the festival period.

August 3–
August 5

Seventh Z-star Research Team event held for high school students from Iwate Prefecture including tsunami-struck
areas, with 5 participants attending. Team succeeded in detecting an astronomical object.

August 3–
August 18

The Southern Island of Star Festival 2013 held together with a special open house event at the VERA Ishigakijima
Station and Ishigakijima Astronomical Observatory with approximately 8,500 visitors to a dimmed-light stargazing
event; an astronomical observation party at the Ishigakijima Astronomical Observatory, attended by 851 visitors;
and a special public opening of the VERA Station attended by 246 visitors.

August 7–
August 9

Chura-boshi Research Team workshop for high school students in Okinawa Prefecture and Fukushima Prefecture
held at VERA Ishigakijima Astronomical Observatory, with 21 participants in attendance. One team using radiowaves discovered 2 masers for the first time in 3 years. A second team using visible light observations with the
Murikabushi telescope discovered 5 asteroids.

August 10

Special open house of VERA Iriki station held jointly with the Yaeyama Kogen Star Festival 2013, with over 1,500
visitors in attendance.

XII Important Dates

141

August 24

Iwate Galaxy Festival 2013, a special event for the Mizusawa region, held with approximately 3,000 visitors inattendance.

August 24

Open House day of Nobeyama Observatory. There were 2,735 visitors for this event.

August 31

Special open house event held at Okayama Astrophysical Observatory, with 515 visitors in attendance.

September 17– Observation training of Radio Astronomy at Nobeyama Radio Observatory for Undergraduate Students was
September 21 performed; there were 12 participants.
October 8

19th Astronomy Lecture for Science Reporters held, with 41 participants from 30 organizations in attendance and50 viewers through internet broadcast.

October 12

Fall 2013 Special Stargazing Party held at Okayama Astrophysical Observatory, with 108 visitors in attendance (outof 360 applicants).

October 17

The number of visitors to the NAOJ Nobeyama Campus reached 3 million.

October 18–
October 19

Mitaka Open House Day held, with 4,176 visitors in attendance.

November 7–
November 9Star Island 2013 open house event of VERA Ogasawara Station held jointly with JAXA Space Education Center for
the first time, with 433 visitors in 3 days.

November 18–
November 21

Staff of the Subaru Telescope and NAOJ conducted two observation programs together - one for SOKENDAI
graduate student course work and the other for undergraduate students chosen from universities in Japan for theirexperience.

November 19

Subaru Telescope staff gave Japanese presentations via remote conferencing system from the Subaru Telescope on
Mauna Kea to Kavli IPMU for Ichita Yamamoto, Minister of State for Special Missions.

November 20

A ceremony for FY 2013 continuous service recognition held. Six NAOJ staff members were recognized: Toshitaka
Kajino, Hiroshi Matsuo, Naohisa Sato, Susumu Miura, Kazuhiro Murakami and Yoshihiro Kato.

December 5

The ALMA Morita Array was awarded the Gold Award of Good Design Award 2013. The Special Award Ceremony
was held at a hotel in Tokyo with the attendance of Professor Hasegawa, Director of the Chile Observatory.

2014

142

January 15

Subaru Telescope staff gave a Japanese presentation via remote conferencing system from the Subaru Telescope’s
base facility in Hilo to Aizu Wakamatsu 3rd Junior High School in Fukushima (as part of supporting the recovery
effort from March 11, 2011 disaster.)February 16

Ishigakijima Astronomical Observatory concluded exchange agreement with Nayoro municipal astronomical
observatory, Hokkaido.

March 6–
March 14

For the Journey through the Universe program, 21 staff members of the Subaru Telescope went to 69 classes in thelocal public schools (from Preschool to 12-th grade) and delivered presentations, hands-on experiences, and otherdemonstrations in English.

March 7

5 staff members of the Subaru Telescope made presentations in English at the Master Educator Workshop.

March 28

A ceremony for FY 2013 continuous service recognition for retiring staff members held. Two staff members wererecognized: Shinichi Ishikawa and Noriyuki Kawaguchi.

XII Important Dates

XIII Publications, Presentations
1. Refereed Publications
Abramov-Maximov, V. E., Efremov, V. I., Parfinenko, L. D., Solov'ev,
A. A., Shibasaki, K.: 2013, Long-period oscillations of sunspots
according to simultaneous ground-based and space observations,Geomag. Aeron., 53, 909-912.
Abramov-maximov, V. E., Efremov, V. I., Parfinenko, L. D., Solov'ev, A.
A., Shibasaki, K.: 2013, Long-Term Oscillations of Sunspots from
Simultaneous Observations with the Nobeyama Radioheliograph andSolar Dynamics Observatory, PASJ, 65, S12.
Abu-Zayyad, T., et al. including Oshima, A.: 2013, Correlationsof the Arrival Directions of Ultra-High Energy Cosmic Rays
with Extragalactic Objects as Observed by the Telescope Array
Experiment, ApJ, 777, 88.
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440, 012041.
Hara, C., Kawabe, R., Shimajiri, Y., Ueda, J., Kurono, Y., Tsukagoshi,T., Nakamura, F., Saito, M., Wilner, D.: 2013, Discovery of the
Rotating Molecular Outflow and Disk in the Class-0/Protostar[BHB2007]#11 in Pipe, ASP Conf. Ser., 476, Eds. R. Kawabe, N.
Kuno, S. Yamamoto, 373-374.
Hatsukade, B., Takeuchi, T. T., Pollo, A., Kohno, K., Aretxaga, I.,
Autermann, J. E., Ezawa, H., Hughes, D. H., Ikarashi, S., Iono,
D., Kawabe, R., Nakanishi, K., Oshima, T., Perera, T., Scott, K.
S., Tamura, Y., Williams, C. C., Wilson, G. W., Yun, M. S.: 2013,
Clustering Properties of 1.1 mm-Selected Submillimetre Galaxies
Unconverted by AzTEC Deep Surveys, ASP Conf. Ser., 476, Eds. R.
Kawabe, N. Kuno, S. Yamamoto, 269-270.
Heiderman, A., Evans, N. J., Gebhardt, K., Blanc, G. A., Davis, T.,
Papovich, C. J., van den Bosch, R., Iono, D., Yun, M., VIXENSTeam: 2013, Star Formation Rate and Gas Relations in the Arp 299

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Merger from the VIXENS Survey, AAS Meeting #223, 117.03.
Hempel, M., et al. including Tamura, M.: 2014, VISTA Variables in the
Vía Láctea (VVV): Halfway Status and Results, The Messenger, 155,
24-29.
Hibi, Y., Sun, J, Qin, H., Matsuo, H., Kang, L., Chen, J., Wu, P., 2013,
Developments of the Cryogenic Integrated Circuits with GaN/AlGaN
HEMTs and the New High Sensitivity Terahertz Detectors, 10th
International Workshop on Low Temperatures Electronics, Eds. C.
Ferrari, et al., 25-29.
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.
Hirota, T., Suzuki, T., Ohishi, M., Sakai, T., Sakai, N., Yamamoto, S.:
2013, Observational Studies of Chemically Young Dark Cloud Cores,
ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 325-326.
Hirota, T., Tsuboi, M., Fujisawa, K., Honma, M., Kawaguchi, N.,
Kim, M. K., Kobayashi, H., Kurono, Y., Imai, H., Omodaka, T.,
Shibata, K. M., Shimoikura, T., Yonekura, Y.: 2013, High-Resolution
Observations of Centimeter/(Sub)Millimeter H2O Masers in Orion
KL with VERA and ALMA, ASP Conf. Ser., 476, Eds. R. Kawabe, N.
Kuno, S. Yamamoto, 327-328.
Honma, M.: 2013, Maser Astrometry with VERA and the Galaxy's
Structure, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S.
Yamamoto, 81-84.
Ikarashi, S., Kohno, K., Aretxaga, I., Arumugam, V., Caputi, K., Dunlop,
J., Hatsukade, B., Hughes, D., Iono, D., Ivison, R., Kawabe, R.,
Motohara, K., Nakanishi, K., Ohta, K., Suzuki, K., Tamura, Y.,
Umehata, H., Wilson, G., Yabe, K., Yun, M.: 2013, AzTEC/ASTE
Deep and Wide Submillimeter Galaxy Survey in the Subaru/XMMNewton Deep Field: Identification of VLA, Spitzer and HerschelCounterparts to 1100-μm-Selected Galaxies and Redshifts, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 265-268.
Iono, D., Ueda, J., Yun, M. S., Crocker, A., Espada, D., Hatsukade,B., Kaneko, H., Kawabe, R., Harayanan, D., Tamura, Y.: 2013,
Charting the Evolution of Merger Remnants Through Molecular Gas
Observations, ASP Conf. Ser., 477, Eds. W.-H. Sun, C. K. Xu, N. Z.
Scoville, D. B. Sanders, 297-298.
Ishimoto, D., Nomura, H., Heinzeller, D., Walsh, C., Millar, T. J., Saigo,
K.: 2013, The Influences of Disk Winds on Chemical Evolution of
Plotoplanetary Disks, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno,
S. Yamamoto, 393.
Ishitsuka, J., et al. including Morita, S., Otsuji, K., Narukage, N.: 2014,
Within the International Collaboration CHAIN: a Summary of Events
Observed with Flare Monitoring Telescope (FMT) in Peru, Sun andGeosphere, 9, 85-96.
Ito, T., Yoshida, F., Fukushima, H., Sato, H., Takahashi, S., Nakamura, T.,
Dermawan, B., Miyasaka, S., Sato, Y., Ip, W.-H., Chen, W.-P.: 2013,
Lightcurve of (4507) 1990FV, Minor Planet Bulletin, 40, 206-207.
Ito, T., Yoshida, F.: 2014, Development of an Asian-wide observation
network for the solar system small bodies: a JSPS Asia-Africa
Science Platform during 2009-2011, New Results in Observations
and Space Exploration of Asteroids, Macau University of Science andTechnology, Eds. W.-H. Ip, 41689.
Izumi, T., Kohno, K., Martín, S., Sheth, K., Matsushita, S., Espada, D.,
NGC 1097 collaborators: 2013, X-ray Irradiated Dense Molecular

156

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Medium in the Active Nucleus of NGC 1097, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 309.
Jeong, S., Imai, N., Miyatake, H., Kajino, T.: 2014, Origin of matter andevolution of galaxies, AIP Conf. Proc. 1594, Eds. S. Jeong, N. Imai, H.
Miyatake, T. Kajino, 1-4.
Jeschke, E., Inagaki, T., Kackley, R.: 2013, Introducing the Ginga FITS
Viewer and Toolkit, ASP Conf. Ser., 475, Eds. D. N. Friedel, 319-322.
Jeschke, E.: 2013, Ginga: an open-source astronomical image viewer
and toolkit, Proceedings of the 12th Python in Science Conference,Eds. S. van der Walt, J. Millman, K. Huff,
Jike, T., Tamura, Y., Shizugami, M., VERA Group: 2013, VERA
Geodetic Activities, IVS 2012 Anuual Report, Eds. D. Baver, D.
Behrend, K. Armstrong, 116-119.
Jovanovic, N., Cvetojevic, N., Guyon, O., Martinache, F., Lawrence, J.:
2013, Detecting exoplanets with extreme adaptive optics and a single
mode fibre fed spectrograph, Proc. of European CLEO, CH-P.15.
Jovanovic, N., Gross, S., Arriola, A., Charles, N., Tuthill,P., Norris, B.,
Stewart, P., Lawrence, J., Withford, M.: 2013, Imporved perfromance
characteristics for the integrated photonics pupil remapping
interferometer Dragonfly, Proc. of European CLEO, CF/IE-P.42.
Jovanovic, N., Guyon, O., Martinache, F., Clergeon, C., Singh, G.,
Vievard, S., Kudo, T., Garrel, V., Norris, B., Tuthill, P., Stewart, P.,
Huby, E., Perrin, G., Lacour, S.: 2013, SCExAO as a precursor toan ELT exoplanet direct imaging instrument, Proc. Third AO4ELT
Conf., Eds. S. Esposito, L. Fini, 94.
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 ProtoNeutron Star, AIP Conf. Proc. 1594, Eds. S. Jeong, N. Imai, H.
Miyatake, T. Kajino, 319-325.
Kajino, T.: 2013, Nuclear weak interactions, supernova nucleosynthesis
and neutrino oscillation, J. Phys.: Conf. Ser., 445, 012024.
Kajino, T., Nakamura, K., Sato, K., Shaku, K., Yoshida, T., Hayakawa,T., Chiba, S., Yamazaki, D., Cheoun, M.-K., Mathews, G. J.: 2013,
Supernova Nucleosynthesis, Neutrino Mass and Oscillation, andNuclear Weak Interactions, Nuclear Structure Problems, Proceedingsof the French-Japanese Symposium, Eds. H. Otsu, et al., 161-166.
Kambe, E., Sadakane, K., Hashimoto, O., Honda, S., Sato, B.: 2014, Lineprofile Variations of the Primary of the Epsilon Aurigae Eclipsing
Binary System, ASP Conf. Ser., 479, Eds. H. Shibahashi, 203-207.
Kameno, S., Nakai, N., Honma, M.: 2013, ALMA Extended Array, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 402-403.
Kameno, S., Nakai, N., Honma, M.: 2013, ALMA Extended Array, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 409-410.
Kameno, S., Yamaki, H., Mizuno, I., Beppu, H., Imai, H., Kuno, N.,
Akashi, T.: 2013, Optimization by Smoothed Bandpass Calibration inRadio Spectroscopy, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno,
S. Yamamoto, 407-408.
Kaneko, H., Kuno, N., Iono, D., Tamura, Y., Tosaki, T., Nakanishi, K.,
Sawada, T.: 2013, Molecular Gas Properties and Star Formation inInteracting Galaxies, ASP Conf. Ser., 477, Eds. W.-H. Sun, C. K. Xu,
N. Z. Scoville, D. B. Sanders, 83-86.
Kaneko, H., Kuno, N., Iono, D., Tamura, Y., Tosaki, T., Nakanishi, K.,
Sawada, T.: 2013, Molecular Gas Properties and Star Formation inInteracting Galaxies, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno,
S. Yamamoto, 273-274.

Katsukawa, Y., Ichimoto, K., Suematsu, Y., Hara, H., Kano, R.,
Shimizu, T., Matsuzaki, K.: 2013, Design progress of the Solar UVVis-IR Telescope (SUVIT) aboard SOLAR-C, Proc. SPIE 8862, Solar
Physics and Space Weather Instrumentation V, Eds. S. Fineschi, J.
Fennelly, 88620S.
Kawabe, R., Kohno, K., Yamamoto, S., Tamura, Y., Totani, T., Kitayama,T., Komatsu, E., Onishi, T., Oshima, T., Honma, M., Matsuhara, H.,
Nakanishi, K., Iono, D., Kuno, N., Momose, M., New Telescope
Working Group: 2013, A Large Millimeter and Submillimeter Telescope
Project: ALMA-SPICA Synergy Telescope ("ASTE-II"), ASP Conf. Ser.,
476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 425-431.
Kawasaki, W., Eguchi, S., Shirasaki, Y., Komiya, Y., Kosugi, G.,
Ohishi, M., Mizumoto, Y.: 2013, Vissage: An ALMA-VO Desktop
Application, ASP Conf. Ser., 475, Eds. D. N. Friedel, 303-306.
Kino, M., Takahara, F., Hada, K., Doi, A.: 2013, Energy densities ofmagnetic field and relativistic electrons at the innermost region of the
M87 jet, EPJ Web of Conf., 61, Eds. J. L. Gomez, 01009.
Kiuchi, H.: 2013, Photonic microwave/millimeter-wave generationand transmission techniques for ALMA, 2nd International VLBI
technology workshop, 25.
Kiyokane, K., Saito, M., Saigo, K., Kurono, Y., Momose, M., Tsukagoshi,T., NRO45m SF-Legacy Team: 2013, Mapping Observation toward
Protostellar Core L1527, ASP Conf. Ser., 476, Eds. R. Kawabe, N.
Kuno, S. Yamamoto, 375.
Klaassen, P., Juhasz, A., Mathews, G., Mottram, J., De GregorioMonsalvo, I., van Dishoeck, E., Takahashi, S., Akiyama, E.,
Chapillon, E., Espada, D., Hales, A., Hogerheijde, M., Rawlings, M.,
Schmalzl, M., Testi, L., 2013, ALMA detection of a disk wind fromHD 163296, Protostars and Planets VI, #1K040.
Kobayashi, K., Sakai, Y., Sasaki, M., Kakimoto, S., Takano, S.: 2013,
A Study on the Excitation Mechanism of Methyl Formate in Orion
KL by using Transitions in the Vibrational Excited States, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 377-378.
Koda, J., Yagi, M., Boissier, S., Gil de Paz, A., Imanishi, M., Meyer, J.
D., Madore, B. F., Thilker, D. A.: 2013, The Initial Mass Function in
the Outskirts of M83, ASP Conf. Ser., 477, Eds. W.-H. Sun, C. K. Xu,
N. Z. Scoville, D. B. Sanders, 3.
Kodama, T., Hayashi, M., Koyama, Y., Tadaki, K., Tanaka, I.,
Shimakawa, R.: 2013, Mahalo-Subaru: Mapping Star Formation at
the Peak Epoch of Massive Galaxy Formation, Proc. IAU Symp. 295,
Eds. D. Thomas, A. Pasquali, I. Ferreras, 74-77.
Kodama, T., Tanaka, I., Hayashi, M., Koyama, Y., Tadaki, K.,
Shimakawa, R., Kohno, K., Tamura, Y.: 2013, From Mahalo-Subaru
to Gracias-ALMA: Resolving Galaxy Formation at Its Peak Epoch,
ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 37.
Kojima, H., et al. including Oshima, A.: 2013, A Proposal of a Multi
Directional Neutron Telescope for Observations of Galactic Cosmic
Rays, The 33rd International Cosmic Ray Conference (ICRC2013),
ID:0663.
Kojima, H., et al. including Oshima, A.: 2013, Swinson Flow and the
Tilt Angle of the Neutral Current Sheet, The 33rd International
Cosmic Ray Conference (ICRC2013), ID:0656.
Kojima, H., et al. including Oshima, A.: 2013, Rigidity Dependence of
Forbush Decreases, The 33rd International Cosmic Ray Conference(ICRC2013), ID:0654.
Kojima, T., Fujii, Y., Asayama, S., Uzawa, Y., 2013, Local Oscillator

noise suppression by a balanced SIS mixer in 0.9 THz band,
IRMMW-THz2013, DOI: 10.1109/IRMMW-THz.2013.6665822
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.:2014, Astrophysical S-factor for destructive reactions of lithium-7 in
big bang 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.: 2014,
Study for Big-Bang Nucleosynthesis oncerning Lithum Isotopes, Proc.
12th Asia Pacific Physics Conf. (APPC12), JPS Conf. Proc. 1, 013055.
Komiya, Y., Yamada, S., Suda, T., Fujimoto, M. Y.: 2013, The stellar
initial mass function in the early universe revealed from old stellar
populations in our neighbourhood, Proc. IAU Symp. 295, Eds. D.
Thomas, A. Pasquali, I. Ferreras, 322-322.
Komugi, S., Miura, R., Onodera, S., Kuno, N., Tosaki, T., NRO MAGiC
Team: 2013, Fundamental Planes of the interstellar Medium, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 57-60.
Kudoh, T., Yokoyama, T., Matsumoto, R.: 2014, Magnetohydrodynamic
Numerical Simulation of Parker Instability in Interstellar Gas
with Cosmic Ray Pressure, Proc. 12th Asia Pacific Physics Conf.
(APPC12), JPS Conf. Proc. 1, 15105.
Kuno, N.: 2013, Giant Molecular Clouds M33 and M83, ASP Conf. Ser.,
476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 41-48.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB
130427B: MITSuME Ishigakijima upper limits, GRB Coordinates
Network, Circular Service, 14499, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB
130427A: MITSuME Ishigakijima Optical Observation after 2 days,
GRB Coordinates Network, Circular Service, 14513, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB
130427A: MITSuME Ishigakijima Optical Observation after 5 days,
GRB Coordinates Network, Circular Service, 14534, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB
130725A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 15033, 1.
Kuroda, D., Hanayama, H., Yanagisawa, K., Shimizu, Y., Toda, H.,
Miyaji, T., Watanabe, J., Nagayama, S., Yoshida, M., Ohta, K., Kawai,N.: 2013, GRB 130427A: MITSuME Okayama and Ishigakijima
Optical Observation after 1 day, GRB Coordinates Network, CircularService, 14498, 1.
Kuroda, D., Hanayama, H., Yanagisawa, K., Shimizu, Y., Toda, H.,
Miyaji, T., Watanabe, J., Nagayama, S., Yoshida, M., Ohta, K., Kawai,N.: 2013, Swift trigger 575905/ GRB 131026A: Mitsume okayama
and ishigakijima optical upper limits, GRB Coordinates Network,
Circular Service, 15389, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130806A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 15077, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130722A: MITSuMEXIII Publications, Presentations

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Okayama Optical upper limits, GRB Coordinates Network, CircularService, 15021, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130612A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 14889, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130604A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 14760, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130603A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 14734, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130511A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 14625, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130508A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 14611, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130505A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 14568, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130504A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 14562, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130427B: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 14477, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130427A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 14465, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140302A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 15911, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140215A: MITSuMEOkayama Optical Observation, GRB Coordinates Network, CircularService, 15848, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140211A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 15817, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140129A: MITSuMEOkayama Optical upper limits, GRB Coordinates Network, CircularService, 15771, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama, S.,
Yoshida, M., Ohta, K., Kawai, N.: 2014, GRB 140114A: MITSuME

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Okayama Optical upper limits, GRB Coordinates Network, CircularService, 15741, 1.
Kusakabe, M., Kim, K. S., Cheoun, M.-K., Kajino, T., Kino, Y., Mathews,
G. J.: 2014, 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.
Kwon, J., Tamura, M.: 2013, Near-Infrared Circular Polarimetry inStar Forming Regions: Implication for Astrobiology, International
Astrobiology Workshop 2013, 1023.
Lee, M., Hiwaki, H., Kameno, S.: 2013, Jet Kinematics and Absorbing
Matter in the Quasar 1413+135, ASP Conf. Ser., 476, Eds. R. Kawabe,
N. Kuno, S. Yamamoto, 291-292.
Liu, S.-Y., Takano, S., Line Survey Team: 2013, Nobeyama 45M
Telescope Legacy Project: Line Survey of IRDC G28.64+0.06, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 367-368.
Lozi, J., Belikov, R., Schneider, G., Guyon, O., Pluzhnik, E., Thomas, S.,
Martinache, F.: 2013, Experimental study of a low-order wavefront
sensor for a high-contrast coronagraphic imager at 1.2 lambda/D,
Proc. Third AO4ELT Conf., Eds. S. Esposito, L. Fini, 66.
Maruyama, T., Hidaka, J., Kajino, T., Yasutake, N., Kuroda, T., Cheoun,
M.-K., Ryu, C.-Y., Mathews, G. J.: 2014, Asymmetric Neutrino
Emission Process in Rapid Spin-Deceleration of Magnetized ProtoNeutron Stars, Proc. 12th Asia Pacific Physics Conf. (APPC12), JPS
Conf. Proc. 1, 013042.
Mathews, G. J., Kajino, T., Yamazaki, D., Kusakabe, M., Cheoun, M.K.: 2014, Origin of matter and space-time in the big bang, AIP Conf.
Proc. 1594, Eds. S. Jeong, N. Imai, H. Miyatake, T. Kajino, 5-11.
Mathews, G. J., Meixner, M., Olson, J. P., Suh, I.-S., Kajino, T.,
Maruyama, T., Hidaka, J., Ryu, C.-Y., Cheoun, M.-K., Lan, N. Q.:
2013, Updates of the nuclear equation of state for core-collapse
supernovae and neutron stars: effects of 3-body forces, QCD, andmagnetic fields, J. Phys.: Conf. Ser., 445, 012023.
Matsui, K., Sorai, K., Baba, J., Watanabe, Y., Kuno, N.: 2013, High Gas
Fraction of Barred Spiral Galaxies at z ~ 0.1–0.2, ASP Conf. Ser.,
476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 277-278.
Matsumoto, E., Tominaga, N., Tanaka, M., Hsiao, E., Contreras, C.,
Gonzalez, C., Morrell, C., Phillips, M.: 2013, Supernova 2013ba,
Central Bureau Electronic Telegrams, 3465, 1.
Matsumoto, J., Masada, Y.: 2013, Rayleigh-Taylor and RichtmyerMeshkov Instabilities in Relativistic Hydrodynamic Jets, EPJ Web ofConf., 61, Eds. J. L. Gomez, 20136102005.
Matsunaga, N., Fukue, N., Kobayashi, N., Ikeda, Y., Yamamoto, R., Kyu, S.,
Hamano, S., Yasui, C., Tsujimoto, T., Aoki, W., Nishiyama, S., Nagata,T., Genovali, K., Inno, L., Bono, G.: 2014, Near-infrared spectroscopyof Cepheids in the Galactic nuclear disk, Proc. IAU Symp. 298, Eds. S.
Feltzing, G. Zhao, N. A. Walton, P. A. Whitelock, 429-429.
Michimura, Y., Matsumoto, N., Ohmae, N., Kokuyama, W., Aso, Y.,
Ando, M., Tsubono, K.: 2014, Testing Lorentz Invariance with a
Double-Pass Optical Ring Cavity, Proceedings of the Sixth Meetingon CPT and Lorentz Symmetry, Eds. V. A. Kostelecký, 216-219.
Miyamoto, Y., Nakai, N., Kuno, N.: 2013, Disruption of Giant Molecular
Associations by Shear Motion in the Spiral Galaxy M51, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 281-282.
Miyamoto, Y., Nakai, N., Kuno, N.: 2014, The Influence of Shear
Motion on Evolution of Giant Molecular Associations, ASP Conf.
Ser., 480, Eds. M. S. Seigar, P. Treuthardt, 259-262.

Momose, M., Morita, A., Okamoto, Y., Fukagawa, M., Honda, M., Muto, T.,
Takeuchi, T., Hashimoto, J., Tamura, M., SEEDS/HiCIAO/AO188
Teams: 2013, Near-Infrared Imaging Observations of Circumstellar
Disk around HD 169142 with Subaru/HiCIAO, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 389.
Momose, M., Morita, A., Okamoto, Y., Fukagawa, M., Honda, M., Muto,T., Takeuchi, T., Hashimoto, J., Tamura, M., SEEDS/HiCIAO/AO188
Teams: 2013, Near-Infrared Imaging Observations of Circumstellar
Disk around HD 169142 with Subaru/HiCIAO, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 141Moriya, T., Blinnikov, S. I., Tominaga, N., Yoshida, N., Tanaka,
M., Maeda, K., Nomoto, K.: 2014, Light Curve Modeling ofSuperluminous Supernovae, Proc. IAU Symp. 296, Eds. A. Ray, R. A.
McCray, 86-89.
Morokuma, T., Tominaga, N., Tanaka, M., Saito, Y., Akitaya, H.,
Moritani, Y., Itoh, R., Ui, T., Maehara, H., Mameta, K.: 2014,
Supernova 2014Q = PSN J08185022+5706029, Central Bureau
Electronic Telegrams, 3806, 1.
Motogi, K., Fujisawa, K., Sugiyama, K., Niinuma, K., Sorai, K.,
Honma, M., Hirota, T., Yonekura, Y., Hachisuka, K., Walsh, A. J.:
2013, New Detection of an Extremely Blue-shift Dominated Jet in
G353.273+0.641: A Possible Disk-Jet System on 100 AU Scale, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 381-382.
Muraoka, K., Matsui, K., Akashi, T., Kuno, N., Iwashita, H., Miyazawa,C., Koyano, M., Baji, H., Maekawa, J., Nakajima, T., Onodera,
S., Sakai, T., Kimura, K., Maezawa, H., Onishi, T., Ogawa, H.:
2013, Test Observations of a New 100 GHz Wave-Band FOur-beam
REceiver System on the Nobeyama 45-m Telescope (FOREST), ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 417-418.
Nagai, H., Orienti, M., Kino, M., Doi, A., Giovannini, G., Asada, K.,
D'Ammando, F., Haga, T., Giroletti M., Hada, K.: 2013, Probing theRadio Counterpart of Gamma-ray Flaring Region in 3C 84, EPJ Web
of Conf., 61, Eds. J. L. Gomez, 04008.
Nagasawa, R., Otsubo, T., Hanada, H.: 2014, Development of software
for high-precision LLR data analysis, Proc. 18th International
Workshop on Laser Ranging - Pursuing Ultimate Accuracy &Creating New Synergies -, Local Organising Committee and Program
Committee of 18th International Workshop on Laser Ranging, 13P014_1-4.
Nakahara, H., Iwai, K., Nakanishi, H.: 2013, A high-speed FFT basedon a six-step algorithm: Applied to a radio telescope for a solar
radio burst, The International Conference on Field-Programmable
Technology (FPT 2013), 430-433.
Nakajima, K., Yamada, Y., Takahashi Y. O., Ishiwatari, M., Ohfuchi, W.,
Hayashi, Y.-Y.: 2013, The variety of spontaneously generated tropicalprecipitation patterns found in APE results, Journal of MeteorologicalSociety of Japan, 91A, 91-141.
Nakajima, K., Yamada, Y., Takahashi Y. O., Ishiwatari, M., Ohfuchi, W.,
Hayashi, Y.-Y.: 2013, The variety of forced atmospheric structure in
response to tropical SST anomaly found in APE results, Journal of
Meteorological Society of Japan, 91A, 143-193.
Nakajima, T., Takano, S., Kohno, K., line survey team: 2013, Nobeyama
45m Telescope Legacy Project: Line Survey of Galaxies, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 299-300.
Nakamura, F., Ogawa, H., Kameno, S., Kimura, K., Mizuno, I.,
Tokuda, K., Kozu, M., Tanaka, T., Iono, D., Takano, S., Dobashi,K., Matsumoto, T., Kuno, N., Kawabe, R., Onishi, T., Momose, M.,
Shinnaga, H., Yamamoto, S., Maezawa, H., Hirota, T.: 2013, The
CCS 45 GHz Zeeman Project: Magnetic Field Measurements Towards
Prestellar Cores, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S.
Yamamoto, 239-242.
Nakamura, K.: 2013, 3+1 gauge-invariant variables for perturbations on
Schwarzschild background spacetime, JGRG 23, Eds. H. Asada, etal., 14.
Namiki, N., et al. including Yoshida, F.: 2014, Scientific Use of LIDAR
Data of Hayabusa-2 Mission, New Results in Observations andSpace Exploration of Asteroids, Macau University of Science andTechnology, Eds. W.-H. Ip, 74-96.
Narita, N.: 2013, Toward Detections and Characterization of Habitable
Transiting Exoplanets, International Astrobiology Workshop 2013,
1065.
Narukage, N., Ishikawa, R., Aoki, K., Miyagawa, K., Kobiki, T., Kano,
R., Bando, T., Tsuneta, S.: 2013, Development of the Cold Mirror
Coating (Reflective Narrow Band Filter) across 300 mm Diameter for
Lyman-Alpha Line (121.6 nm), UVSOR Activity Report 2012, 46.
Narukage, N., Ishikawa, S., Kobiki, T., Kano, R., Bando, T., Tsuneta,
S.: 2013, Development of the Multi-Layer Coating for the HighEfficiency Reflective Polarizer in Lyman-Alpha Line (121.6 nm),UVSOR Activity Report 2012, 47.
Niino, Y.: 2013, The Mass-SFR-Metallicity Relation of Star Forming
Galaxies and Its Evolution: Implications for GRB/SN Host Galaxies,
EAS Publications Ser. 61, Eds. A. J. Castro-Tirado, J. Gorosabel, I. H.
Park, 427-429.
Nishimura, Y., Sakai, N., Watanabe, Y., Sakai, T., Hirota, T., Yamamoto,S.: 2013, Observations of Deuterated Species toward Low-Mass
Prestellar and Protostellar Cores, ASP Conf. Ser., 476, Eds. R.
Kawabe, N. Kuno, S. Yamamoto, 343-344.
Noda, H., Mizuno, T., Kunimori, H., Takeuchi, H., Namiki, N.:
2014, Alignment measurement with optical transponder system of
Hayabusa-2 LIDAR, Proc. 18th International Workshop on Laser
Ranging - Pursuing Ultimate Accuracy & Creating New Synergies-, Local Organising Committee and Program Committee of 18th
International Workshop on Laser Ranging, 13-Po06_1-6.
Nomura, H., Walsh, C., Millar, T. J., Aikawa, Y.: 2013, Diagnosing Gas
Dispersal Processes in Protoplanetary Disks, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 209-212.
Oe, M.: 2013, The effectiveness and impact of JGN-X network in thefield of astronomy, APAN/APII Workshop 2013, APII03.
Ohishi, M., Hirota, T., Kaifu, N., Suzuki, T., Motoki, Y., Ozeki, H.:
2013, Absorption Features of CH3NH2 Towards SgrB2 (M), LPI
Contributions, 1766, 1766, 1009.
Ohishi, M.: 2013, Annual Report for 2012 of IUCAF, Radio Science
Bulletin, 344, 11-12.
Ohishi, M.: 2013, Search for Large Molecules and Spectral Line
Surveys, NARIT Conf. Ser. 1, Proceedings of the 11th Asian-PacificRegional IAU Meeting (APRIM2011), Eds. S. Komonjinda, Y. Y.
Kovalev, D. Ruffolo, 274-280.
Omiya, M., Sato, B., Harakawa, H., Kuzuhara, M., Hirano, T., Narita,N., IRD Team: 2013, Search for Habitable Planets Around LowMass Stars Using the InfraRed Doppler Instrument, International
Astrobiology Workshop 2013, 1037.
Onishi, K., Iguchi, S., Okuda, T.: 2013, Derivation of the Mass of

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Super-Massive Black Hole, ASP Conf. Ser., 476, Eds. R. Kawabe, N.
Kuno, S. Yamamoto, 275-276.
Onodera, S., Kuno, N., Tosaki, T., Muraoka, K., Miura, R., Kohno,K., Nakanishi, K., Sawada, T., Komugi, S., Kaneko, H., Hirota, A.,
Kawabe, R.: 2013, NRO M33 All-Disk Survey of Giant Molecular
Clouds (NRO MAGiC): Properties of Giant Molecular Clouds in M33,
ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 303-304.
Oogi, T., Habe, A.: 2013, Dry minor mergers and the size evolution ofhigh-z compact massive early-type galaxies, Proc. IAU Symp. 295,
Eds. D. Thomas, A. Pasquali, I. Ferreras, 183.
Oshima, A., et al.: 2013, An anisotropy of galactic cosmic rays observedwith GRAPES-3, The 33rd International Cosmic Ray Conference(ICRC2015), ID:0821.
Peters-Limbach, M. A., Groff, T. D., Kasdin, N. J., Driscoll, D., Galvin,
M., Foster, A., Carr, M. A., LeClerc, D., Fagan, R., McElwain, M.
W., Knapp, G., Brandt, T., Janson, M., Guyon, O., Jovanovic, N.,
Martinache, F., Hayashi, M., Takato, N.: 2013, The optical designof CHARIS: an exoplanet IFS for the Subaru telescope, Proc. SPIE
8864, Techniques and Instrumentation for Detection of Exoplanets
VI, Eds. S. Shaklan, 88641N.
Saito, T., Iono, D., Yun, M., Ueda, J., Espada, D., Hagiwara, Y., Imanishi,M., Motohara, K., Nakanishi, K., Sugai, H., Tateuchi, K., Kawabe, R.:
2013, ALMA Observations of the IR-Bright Merger VV114, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 287-290.
Sakai, T., Sakai, N., Furuya, K., Aikawa, Y., Hirota, T., Yamamoto,S.: 2013, Chemical Compositions of Massive Clumps in Early
Evolutionary Stages of High-Mass Star Formation, ASP Conf. Ser.,
476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 371-372.
Sakao, T., Narukage, N., Shimojo, M., Watanabe, K., Suematsu, Y.,
Imada, S., Ishikawa, S.: 2013, The soft X-ray photon-counting
spectroscopic imager for the Sun, Proc. SPIE 8862, Solar Physics
and Space Weather Instrumentation V, Eds. S. Fineschi, J. Fennelly,
88620T.
Sakurai, T., Gao, Y., Kuzanyan, K.: 2013, Magnetic Helicity as a Probeof Magnetic Flux-Tube Dynamics in the Solar Interior, Proc. IAU
Symp. 294, Eds. A. G. Kosovichev, E. de Gouveia Dal Pino, Y. Yan,
301-306.
Sawada, T., Hasegawa, T., Koda, J., Handa, T., Sugimoto, M.: 2013,
Structured Molecular Gas Reveals Galactic Spiral Arms, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 279-280.
Sawada-Satoh, S., Akiyama, K., Kino, M., Nagai, H., Niinuma, K.:
2013, VERA monitoring of a blazar OJ 287, EPJ Web of Conf., 61,
Eds. J. L. Gomez, 08007.
Sekido, T. S., Oka, T., Tsuboi, Y., Asaki, Y., Yonekura, Y., Kaneko,
H., Miyamoto, Y., Seta, M., Nakai, N., Kameya, O., Miyoshi, M.,
Takaba, H., Wakamatsu, K., Fukuzaki, Y., Morimitsu, T., Omodaka,
M. T., Handa, T.: 2013, NICT VLBI Observations of Sgr A* at 8 GHz
and 2 GHz, The Astronomer's Telegram, 5024.
Shibagaki, S., Kajino, T., Chiba, S., Lorusso, G., Nishimura, S.,
Mathews, G. J.: 2014, Realistic fission models, new beta-decay halflives and the r-process in neutron star mergers, AIP Conf. Proc. 1594,
Eds. S. Jeong, N. Imai, H. Miyatake, T. Kajino, 394-398.
Shimajiri, Y., Sakai, T., Kitamura, Y., Tsukagoshi, T., Saito, M.,
Nakamura, F., Momose, R., Kawabe, R.: 2013, Spectral-Line
Survey at Millimeter and Submillimeter Wavelengths toward an
Outflow-shocked Region, OMC2-FIR 4, ASP Conf. Ser., 476, Eds. R.

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Kawabe, N. Kuno, S. Yamamoto, 341-342
Shimoikura, T., Dobashi, K., Onishi, T., Ogawa, H., Kimura, K.,
Nishimura, A., Nakamura, F., Saito, H.: 2013, Cluster Formationin the Sh247/ Sh252/ BFS52 Regions, ASP Conf. Ser., 476, Eds. R.
Kawabe, N. Kuno, S. Yamamoto, 365-366
Shimojo, M.: 2013, Unusual migration of the prominence activities inrecent solar cycles, Proc. IAU Symp. 300, Eds. B. Schmieder, J.-M.
Malherbe, S.T. Wu, 161-167.
Shirasaki, Y., Kawasaki, W., Eguchi, S., Komiya, Y., Kosugi, G.,
Ohishi, M., Mizumoto, Y.: 2013, Web and Desktop Applications for
ALMA Science Verification Data, ASP Conf. Ser., 475, Eds. D. N.
Friedel, 403-405.
Singh, G., Martinache, F., Baudoz, P., Guyon, O., Clergeon, C., Matsuo,
T.: 2013, Lyot-based ultra-fine pointing control system for phasemask coronagraphs, Proc. Third AO4ELT Conf., Eds. S. Esposito, L.
Fini, id. #7.
Sodor, A., et al. including Kambe, E.: 2014, Extensive spectroscopic andphotometric study of HD 25558, a long orbital-period binary with
two SPB components, Proc. IAU Symp. 301, Eds, J. A. Guzik, W. J.
Chaplin, G. Handler, A. Pigulski, 491-492.
Sôma, M.: 2013, Transit of Venus - Halley's Recommendation and This
Year's Phenomenon, Proc. Third Symp. on "Historical Records andModern Science", Eds. M. Sôma, K. Tanikawa, 28-32.
Sugimoto N., Takagi M., Matsuda, Y., Takahashi, Y. O., Ishiwatari, M.,
Hayashi, Y.-Y.: 2013, Baroclinic modes in the atmosphere on Venus
simulated by AFES, Theor. Appl. Mech. Japan, 61, 11-21.
Sugiyama, K., Fujisawa, K., Hachisuka, K., Yonekura, Y., Motogi, K.,
Honma, M., Hirota, T., Sawada-Satoh, S., Niinuma, K., Murata, Y.,
Doi, A., Ogawa, H., Shen, Z.-Q.: 2013, The VLBI Imaging Survey of
the 6.7 GHz Methanol Masers using the JVN/EAVN, ASP Conf. Ser.,
476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 347-348.
Suzuki, K., Kohno, K., Tanaka, I., Kodama, T., Hatsukade, B., Tamura,Y., Nakanishi, K., Iono, D., Kajisawa, M., Ikarashi, S., Umehata,
H., Ivison, R. J., Wilson, G. W., Yun, M. S., Hughes, D. H., Aretxaga,
I., Zeballos, M.: 2013, Sub-mm Singledish and InterferometricObservations of the Proto-Cluster around 4C 23.56 at z = 2.5, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 263.
Suzuki, T., Honma, M., Balantekin, A. B., Kajino, T., Chiba, S.: 2014,
New neutrino-nucleus reaction cross sections at solar, reactor andsupernova neutrino energies, EPJ Web of Conf. 66: INPC 2013 –International Nuclear Physics Conference, Eds. S. Lunardi, P. G.
Bizzeti, S. Kabana, C. Bucci, M. Chiari, A. Dainese, P. Di Nezza, R.
Menegazzo, A. Nannini, C. Signorini, J. J. Valiente-Dobon, 07025.
Suzuki, T., Ohishi, M., Hirota, T.: 2013, Distribution of CCS and HC3N
in L1147: A Less Evolved Molecular Cloud, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 329-330.
Takahashi, S., Saigo, K., Ho, P. T. P., Tomida, K.: 2013, Spatially Resolving
an Extremely Young Intermediate-mass Protostar in Orion, ASP Conf.
Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 397-398.
Takakuwa, S., Saito, M., Lim, J., Saigo, K., Hanawa, T., Matsumoto, T.:2013, Keplerian Circumbinary Disk and Accretion Streams aroundthe Protostellar Binary System L1551 NE, ASP Conf. Ser., 476, Eds.
R. Kawabe, N. Kuno, S. Yamamoto, 135.
Takano, S., et al. including Hirota, T., Ohashi, N., Ohishi, M., Umemoto,T.: 2013, Nobeyama 45 m Telescope Legacy Project: Line Survey, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 193-196.

Takehiro, S., Sasaki, Y., Hayashi, Y.-Y., Yamada, M.: 2013, Differential
rotation and angular momentum transport caused by thermal convection
in a rotating spherical shell./Differential rotation and angularmomentum transport caused by thermal convection in a rotating
spherical shell, ASP Conf. Ser., 479, Eds. H. Shibahashi, 285-294.
Tamura, M.: 2014, SEEDS: Strategic Explorations of Exoplanets andDisks with Subaru, Proc. IAU Symp. 299, Eds. B. Matthews, J.
Graham, 12-16.
Tamura, Y., Tatamitani, Y., Takahashi, S., Horigome, O., Maekawa,J., Kohno, K., Sakai, T., Taniguchi, A.: 2013, A New "Off-point-less"
Method for Mm/submm Spectroscopy with a Frequency-Modulation
Local Oscillator, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S.
Yamamoto, 401-402
Tanaka, M., Akitaya, H., Ui, T., Ebisuda, N., Mameta, K., Fukuda,S., Morokuma, T., Tominaga, N.: 2014, Supernova 2014S, Central
Bureau Electronic Telegrams, 3814, 1.
Tanaka, M., Fukuda, S., Morokuma, T., Tominaga, N.: 2014, Supernova
2014T, Central Bureau Electronic Telegrams, 3815, 1.
Tanaka, M., Phillips, M., Hsiao, E., Holmbo, S., Contreras, C., Akitaya,
H., Moritani, Y., Fukuda, S., Mameta, K., Takahashi, K., Morokuma,
T., Tominaga, N.: 2014, Supernova 2014U IN NGC 3859, Central
Bureau Electronic Telegrams, 3816, 1.
Tanaka, M., Tominaga, N., Kikuchi. Y., Ukita, N., Mori, K., Matsumoto,E., Morokuma, T., Iwata, I.: 2013, Supernova 2013fk IN UGC 1442
= PSN J01573355-0205572, Central Bureau Electronic Telegrams,
3567, 1.
Tanaka, T., Awazu, Y., Nakamura, F., Sugitani, K., Shimajiri, Y.,
Kawabe, R., Onishi, T., Yoshida, H.: 2013, The Dynamical state ofFilamentary infrared Dark cloud, Serpens South, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 363-364.
Thomas, S., Pluzhnik, E., Lozi, J., Belikov, R., Witteborn, F., Greene, T.,
Schneider, G., Guyon, O.: 2013, Improving the broadband contrast at
small inner working angles using image sharpening techniques, Proc.
Third AO4ELT Conf., Eds. S. Esposito, L. Fini, id. #79.
Tokuda, K., Kozu, M., Kimura, K., Muraoka, K., Maezawa, H., Onishi,T., Ogawa, H., Nakamura, F., Kuno, N., Takano, S., Iono, D.,
Kawabe, R., Kameno, S.: 2013, A New 45 GHz Band Receiver with
Dual Polarization for NRO 45-m Telescope, ASP Conf. Ser., 476,
Eds. R. Kawabe, N. Kuno, S. Yamamoto, 403-406.
Tokudome, T., Sakai, N., Sakai, T., Takano, S., Yamamoto, S., NRO
Line survey Project Members: 2013, Nobeyama 45m Telescope
Legacy Project: Line Survey of L1527, ASP Conf. Ser., 476, Eds. R.
Kawabe, N. Kuno, S. Yamamoto, 55-356.
Tominaga, N., Kikuchi. Y., Ukita, N., Mori, K., Tanaka, M., Matsumoto,E., Morokuma, T., Iwata, I.: 2013, Supernova 2013fi = PSN
J03043856+4213494, Central Bureau Electronic Telegrams, 3563, 2.
Tosaki, T., Miura, R. E., Kohno, K., Kuno, N., Onodera, S., MAGiC
team: 2013, Molecular Gas and Star Formation in Giant H II
Regions of M33, ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S.
Yamamoto, 305-306.
Tsai, A.-L., Urata, Y., Takahashi, S., Chuang, C.-J.: 2013, Constrain the
SED Type of Unidentified Fermi Objects, J. Astron. Space Sci., 30,
123-125.
Tsuboi, M., et al. including Kameya, O., Miyoshi, M.: 2013, Report of
the Daily Monitor of Sgr A* at 22 GHz, The Astronomer's Telegram,
5184.

Tsuboi, M., et al. including Kameya, O., Miyoshi, M.: 2013, Possiblebrightening at 22 GHz of Sgr A*, The Astronomer's Telegram, 5013.
Tsujimoto, T.: 2013, Galactic Chemical Evolution in the Context of the
Recently Revealed SNe Ia Delay Time Distribution, Proc. IAU Symp.
281, Eds. R. Di Stefano, M. Orio, M. Moe, 251-252.
Tsukagoshi, T., Momose, M., Hashimoto, J., Kudo, T., Andrews,
S., Ohashi, N., Kitamura, Y., Saito, M., Wilner, D., Tamura, M.,
Kawabe, R.: 2013, Submillimeter and Near Infrared Studies for the
Evolved Transition Disk around Sz 91, ASP Conf. Ser., 476, Eds. R.
Kawabe, N. Kuno, S. Yamamoto, 391.
Ueda, J., Iono, D., Petitpas, Yun, M. S., Ho, P. T. P., Kawabe, R., Mao,
R.-Q., Martin, S., Matsushita, S., Peck, A. B., Tamura, Y., Wang, J.,
Wang, Z., Wilson, C. D., Zhang, Q.: 2013, Unveiling the Physical
Properties and Kinematics of Molecular Gas in the Antenna Galaxies
with the SMA, ASP Conf. Ser., 477, Eds. W.-H. Sun, C. K. Xu, N. Z.
Scoville, D. B. Sanders, 311-312.
Ueda, J., Iono, D., Yun, M., Wilner, D., Narayanan, D., Hatsukade, B.,
Tamura, Y., Kaneko, H., Crocker, A., Espada, D., Kawabe, R.: 2013,
Reformation of Cold Molecular Disks in Merger Remnants, ASP
Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 61.
Ueno, S., et al. including Morita, S.: 2014, International Collaboration
and Academic Exchange of the CHAIN Projrct in this Three Years(Period), Sun and Geosphere, 9, 97-103.
Uzawa, Y.: 2013, Superconducting Microwave/Terahertz Wave
Device Technology -First-Light from the Band-10 SIS Receiverat the Atacama Large Millimeter/submillimeter Array (ALMA),
Superconductivity Web21, 45-48.
Watanabe, J., Kasuga, T., Terai, T., Miyazaki, S., Ohta, K., Murooka,
F., Ohnishi, T., Yamasaki, T., Mito, H., Aoki, T., Soyano, T.,
Tarusawa, K., Matsunaga, N., Sako, S., Kobayashi, N., Doi, M.,
Enomoto, T.: 2013, Faint Meteor Observation by Large-Format
CMOS Sensor with 1.05-m Kiso Schmidt, Meteoroids 2013, Eds. T. J.
Jopek, F. Rietmeijer, J. Watanabe, I. P. Williams, 119-121.
Williamson, D. L., et al. including Hayashi, Y.-Y.: 2013, The Aqua
Planet Experiment (APE): Response to changed SST fields, Journalof Meteorological Society of Japan, 91A, 57-89.
Yamaguchi, T., Takano, S., Sakai, N., Watanabe, Y., Yamamoto, S.,
NRO Line Survey Team Members: 2013, Shock Chemistry in LowMass Star-Forming Regions, ASP Conf. Ser., 476, Eds. R. Kawabe, N.
Kuno, S. Yamamoto, 321-322.
Yamashita, T., Komugi, S., Matsuhara, H., Armus, L., Inami, H.,
Stierwalt, S., Kohno, K., Iono, D., Arimatsu, K.: 2013, 12CO (J=1–0)
Survey with NRO 45 m of GOALS Luminous Infrared Galaxies: Star
Formation Efficiency against Galactic Merger and AGN Activity,
ASP Conf. Ser., 476, Eds. R. Kawabe, N. Kuno, S. Yamamoto, 297.
Yonekura, Y., Saito, Y., Saito, T., Mori, T., Soon, K. L., Momose, M.,
Yokosawa, M., Ogawa, H., Fujisawa, K., Sugiyama, K., Motogi,K., Takaba, H., Sorai, K., Nakai, N., Kameno, S., Kobayashi, H.,
Kawaguchi, N., Hachisuka, K.: 2013, Development of 32-m Radio
Telescopes for Monitoring Observations of Methanol Masers, H2O
Masers, and Radio Continuum, ASP Conf. Ser., 476, Eds. R. Kawabe,
N. Kuno, S. Yamamoto, 415-416.
Yoshida, F.: 2014, Current knowledge of Jupiter Trojans - toward
the Solar Power Sail mission -, New Results in Observations andSpace Exploration of Asteroids, Macau University of Science andTechnology, Eds. W.-H. Ip, 43-59.

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5. Publications in English
Flaminio, R.: 2014, Thermal Noise in Laser Interferometer Gravitational
Wave Detectors' in: 'Advanced Interferometers and the Search for
Gravitational Waves', pp 225-249, Ed. Massimo Bassan, Astrophysics
and Space Science Library 404, Springer Internatioal Publishing,
Switzerland.
Kawabe, R., Kuno, N., Yamamoto, S.: 2013, New Trends in Radio
Astronomy in the ALMA Era: The 30th Anniversary of Nobeyama
Radio Observatory, Astronomical Soc. of the Pacific, San Francisco,Calif.

6. Conference Presentations
Agata, H.: 2013, Introduction to Astronomy and Astronomical Educaton
on NAOJ, Discover the COSMOS consortium and Global Hands-On
Universe conference, (Volos, Greece, Aug. 2-4, 2013).
Agata, H.: 2013, Education and Outreach at the National Astronomical
Observatory of Japan, Communicating Astronomy with the Public
2013 (CAP 2013), (Warsaw, Poland, Oct. 14-18, 2013).
Agata, H.: 2014, Introduction to Astronomy and Astronomical Educatonon National Astronomical Observatory of Japan, You are Galileo!
Workshop in Cambodia, (Pnonpen, Cambodia, Feb. 3, 2014).
Aimi, Y., Fukagawa, M., Yasuda, T., Yamashita, T., Kawabata, K.,
Uemura, M., Arai, A., Sasada, M., Ohsugi, T., Yoshida, M., Shibai, H.:
2013, Simultaneous Visible and Near-Infrared Variability of ClassicalT Tauri Stars, IAU Symp. 299: Exploring the formation and evolutionof planetary systems, (Victoria, Canada, Jun. 2-7, 2013).
Akiyama, E., Espada, D., Kiytamura, Y., Chapillion, E., Takahashi,S., Vlahkis, C.: 2013, The Radial and Vertical Gas Disk Structure in
HD163296: 1st ALMA Science Verification Results, Transformational
Science with ALMA: From Dust to Rocks to Planets Formation and
Evolution of Planetary Systems, (Kona, HI, USA, Apr. 8-13, 2013).
Akiyama, E., Kusakabe, N., Tamura, M., Kudo, T., Hashimoto, J.,
Momose, M., Tsukagoshi, T., Kitamura, Y.: 2013, High-Contrast
Near-Infrared Polarization Imaging and Structural Analysis in
Millimeter/Sub-Millimeter wavelengths in MWC480, Protostars andPlanets IV, (Heidelberg, Germany, Jul. 15-20, 2013).
Akiyama, E., Walsh, C., Nomura, H., Aikawa, Y., Okuzumi, S., Miller, T.,
Momose, M.: 2013, Unveiling the MRI through Ionization Fractionof Protoplanetary Disks Using Ionization Tracers, East-Asian ALMA
Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Akutsu, T., DECIGO Working group: 2013, DECIGO and DECIGO
Pathfinder, 10th Amaldi Conference on Gravitational Wavs, (Warsaw,
Poland, Jul. 7-13, 2013).
Akutsu, T., Saito, Y., Takahashi, R., Sakakibara, Y., Izumi, K., Niwa, Y.:
2013, Stray-Light Control in KAGRA, 10th Amaldi Conference on
Gravitational Wavs, (Warsaw, Poland, Jul. 7-13, 2013).
Ando, M.: 2013, Observation of Gravitational Waves, Multi-Messengers
from Core-Collapse Supernovae, (Fukuoka, Japan, Dec. 2-6, 2013).
Ando, M.: 2013, Gravitational-Wave Telescopes, 6th OECD Meeting of
the Astroparticle Physics International Forum, (Toyama, Japan, Oct.
29, 2013).
Ando, M.: 2013, KAGRA, Large-scale Cryogenic Gravitational-Wave

162

XIII Publications, Presentations

Telescope, Workshop on Scientific Project Management, (Tokyo,
Japan, Oct. 16, 2013).
Ando, M.: 2013, KAGRA and Gravitational-Wave Experiments, 12th
Asia Pacific Physics Conf. (APPC12), (Chiba, Japan, Jul. 17, 2013).
Ando, M.: 2013, Recent News from KAGRA, PAC34, The 34th Program
Advisory Committee Meeting, (Hanford, WA, USA, Jun. 4, 2013).
Antolin, P.: 2013, Forward modelling of MHD kink oscillations in thesolar corona, The 7th Hinode Science Meeting, (Takayama, Gifu,
Japan, Nov. 12-15, 2013).
Ao, Y.: 2013, CO line SEDs in local (U)LIRGs with the APEX, East-Asian
ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Aoki, W.: 2013, Subaru/HDS, 10th Potsdam Thinkshop 2013 High
Resolution Optical Spectroscopy, (Potsdam, Brandenburg, Germany,
May 28-30, 2013).
Araki, H., Kashima, S., Noda, H., Kunimori, H., Mashiko, H., Otsubo,T., Utsunomiya, S., Matsumoto, Y.: 2013, Development of the Retroreflector on the Moon for the Future Lunar Laser Ranging, AOGS
10th Annual Meeting, (Brisbane, Australia, Jun. 24-28, 2013).
Araki, H., Kashima, S., Noda, H., Kunimori, Mashiko, H., Otsubo, T.,
Utsunomiya, M., Matsumoto, Y.: 2013, Development of the Retroreflector on the Moon for the Future Lunar Laser Ranging, 18th
International Workshop on Laser Ranging - Pursuing Ultimate Accuracy& Creating New Synergies -, (Fujiyosida, Japan, Nov. 11-15, 2013).
Araya, A., Tamura, Y., Tsubokawa, T.: 2013, Development of a Compact
Absolute Gravimeter with a Bulit-in Accelerometer and Silent-Drop
Mechanism, IAG Symposium on Terrestrial Gravimetry: Static andMobile Measurements (TG-SMM2013), (Saint Petersburg, Russia,
Sep. 17-20, 2013).
Ariyoshi, Y., Hanada, T., Kawamoto, S.: 2013, Influence of Small
Satellites' Post-mission Disposal with Enlarging Effective Crosssectional Area, The 29th International Symposium on SpaceTechnology and Science, (Nagoya, Japan, Jun. 2-9, 2013).
Asayama, S., Knee, L., Lopez, B., Whyborn, N., JAO SIG, JAO ADE:
2013, ALMA AIV Processing of Array Elements, 2013 Asia-PacificRadio Science Conference, (Taipei, Taiwan, Sep. 3-7, 2013).
Aso, Y.: 2013, The formation of a Keplerian disk around a late-stage
protostar, East-Asian ALMA Science Workshop 2013, (Taipei,
Taiwan, Sep. 2-4, 2013).
Barkin Y., Hanada, H., Matsumoto, K., Sasaki, S., Leal, J. M. F.,
Barkin, M.: 2013, The theory of the moon rotation and determinationof fourth mode its free physical libration, Japan Geoscience Union
Meeting 2013, (Chiba, Japan, May 19-24, 2013).
Barkin Y., Perov, S., Sidorenkov, N., Hanada, H.: 2013, New ﬁndings
in Earth's sciences, Japan Geoscience Union Meeting 2013, (Chiba,
Japan, May 19-24, 2013).
Barkin, Y., Hanada, H., Ferrandiz, J., Matsumato, K., Sasaki, S.,
Barkin, M.: 2013, The theory of the moon rotation and determinationof fourth mode its free physical libration, Japan Geoscience Union
Meeting 2013, (Chiba, Japan, May 19-24, 2013).
Barkin, Y., Hanada, H., Sasaki, S., Barkin, M.: 2013, Method ofanalysis of existance of the zones of lower seismic velocities ofplanets and satellites, Japan Geoscience Union Meeting 2013, (Chiba,
Japan, May 19-24, 2013).
Baty, H., Pétri, J., Zenitani, S.: 2013, Explosive tearing mode reconnection
in relativistic plasmas: application to the Crab flares, Shocks,
Reconnection, and Particle Acceleration in Plasma-fluids, (Lyon,

France, Jun. 20-21, 2013).
Baty, H., Pétri, J., Zenitani, S.: 2013, Explosive tearing mode reconnection
in relativistic plasmas: application to the Crab flares, From Black
Holes to Cosmic Rays: when plasmas go wild, (Ecole de Physiquedes Houches, France, Oct. 14-18, 2013).
Casadio, C., Gomez, J. L., Giroletti, M., Giovannini, G., Hada, K.,
Fromm, C., Perucho, M., Marti, J.-M.: 2013, A sensitive study ofthe peculiar jet structure HST-1 in M87, The Innermost Regions ofRelativistic Jets and Their Magnetic Fields, (Granada, Spain, Jun. 1014, 2013).
Chibueze, J. O.: 2013, 2013 Hot Core Detection in NGC 6334I(N) SM2
Object with Sub-millimeter Array (SMA), East-Asian ALMA Science
Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Chida, H.: 2014, Long-term monitoring of 3C 84 with VERA at 22 GHzfrom 2011 to 2013, VERA-KVN science workshop, (Kagoshima,
Japan, Jan. 20-21, 2014).
Chou, M.-Y., Takami, M., Manset, N., Beck, T., McGregor, P., White, M.,
Karr, J. L., Liu, H. B., Chen, W.-P., Panwar, N., Pyo, T.-S., GalvanMadrid, R., Shang, H.: 2013, Monitoring Long-term Variability of
Optical Spectra and Extended Jets for Active T Tauri Stars, Protostars
and Planets IV, (Heidelberg, Germany, Jul. 15-20, 2013).
Debes, J. H., et al. including Tamura, M.: 2014, STIS High Contrast
Imaging of HD 15745 on Solar System Scales: Inspecting the Fan,AAS Meeting #223, (Washington DC, USA, Jan. 5-9, 2014).
Doi, A., Hada, K., Nagai, H., Kino, M., Honma, M., Akiyama, K.,
Oyama, T., Kono, Y.: 2013, ALMA Continuum Spectrum of the M87
Nucleus. Quasi-simultaneous continuum observations at bands-3, 6, 7,
and 9, The Innermost Regions of Relativistic Jets and Their Magnetic
Fields, (Granada, Spain, Jun. 10-14, 2013).
Eguchi, S., Kawasaki, W., Shirasaki, Y., Komiya, Y., Kosugi, G.,
Ohishi, M., Mizumoto, Y., Kobayashi, T.: 2013, Demonstration of a
Data Distribution System for ALMA Data Cubes, Astronomical Data
Analysis Software and Systems (ADASS) Conference, (Waikoloa
Beach Marriott, HI, USA, Sep. 29-Oct. 3, 2013).
Espada, D.: 2013, High resolution Molecular Gas Studies in Nearby
Galaxies, East-Asian ALMA Science Workshop 2013, (Taipei,
Taiwan, Sep. 2-4, 2013).
Flaminio, R.: 2013, Status of KAGRA, ELITES meeting, (Tokyo, Japan,
Dec. 4-5, 2013).
Flaminio, R.: 2014, Status of KAGRA, LIGO-Virgo meeting, (Nice,
France, Mar. 17-21, 2014).
Fujii, K., Minamidani, T., Kawamura, A., Mizuno, N., Muller, E.,
Onishi, T., Fukui, Y.: 2013, Molecular gas studies on N48 & N49,
MegaSAGE Meeting 2013, (Heidelberg, Germany, Sep. 23-27, 2013).
Fujii, M.: 2014, The mass function of star clusters formed in turbulent
molecular clouds, The Impact of Galactic Structure on Star
Formation, (Sapporo, Japan, Feb. 16-21, 2014).
Fujimoto, K., Sydora, R. D.: 2013, Anomalous transport induced byplasmoid formations in collisionless magnetic reconnection, 12th
International Workshop on the Interrelationship between Plasma
Experiments in the Laboratory and in Space (IPELS2013), (Nagano,
Japan, Jul. 1-5, 2013).
Fujimoto, K.: 2013, PIC simulation of magnetic reconnection withadaptive mesh refinement, 11th International School/Symposium forSpace Simulations (ISSS11), (Zhongli, Taiwan, Jul. 21-28, 2013).
Fukagawa, M., Tsukagoshi, T., Momose, M., Saigo, K., Ohashi, N.,

Kitamura, T., Muto, T., Nomura, H., Kobayashi, H., Takeuchi, T.,
Akiyama, E., Aso, Y., Honda, M., Fujiwara, H., Takashi, S., Shibai,
H., Inutsuka, S.: 2013, ALMA Observations of the AsymmetricallyGapped Disk around HD 142527, Transformational Science with
ALMA: From Dust to Rocks to Planets Formation and Evolution ofPlanetary Systems, (Kona, HI, USA, Apr. 8-13, 2013).
Fukagawa, M., Hashimoto, J., Grady, C. A., Momose, M., Wisniewski,
J. P., Okamoto, Y., Muto, T., Kusakabe, N., Bonnefoy, M., Kotani,T., Maruta, Y., Tamura, M., SEEDS/HiCIAO/AO188 Collaboration:
2013, Near-Infrared Polarimetric Imaging of Disks around Young
Intermediate-mass Stars in SEEDS, Protostars and Planets VI,(Heidelberg, Germany, Jul. 15-20, 2013).
Fukui, A., Narita, N., Ikoma, M., Hori, Y., Kurosaki, K., Kawashima,Y.: 2013, Atmospheric Study of Transiting Planets through Opticaland Infrared Observations, The 5th Subaru International Conference,
Exoplanets and Disks: Their Formation and Diversity II, (Kona, HI,
USA, Dec. 8-12, 2013).
Furusawa, H.: 2013, Status and Issues of HSC Data Analysis, HSC
collaboratin meeting, (Tokyo, Japan, Aug. 30-Sep. 1, 2013).
Furusho, R., Ootsubo, T., Honda, M., Watanabe, J., Fuse, T., Ishiguro,
M.: 2013, SPICA Spectroscopy of Cometary Refractory and Icy Dust
Grains, SPICA Science Conference 2013 (From exoplanet to distantgalaxies: SPICA's new window on the cool universe), (Tokyo, Japan,
Jun. 18-21, 2013).
Furusho, R., Shinoda, T., Terai, T., Watanabe, J.: 2013, Imaging
Polarimetry of recent 13 Comets/Nuclei, AOGS 10th Annual
Meeting, (Brisbane, Australia, Jun. 24-28, 2013).
Geers, V., Scholz, A., Muzic, K., Dawson, P., Jayawardhana, R., Tamura,M.: 2013, SONYC: Sub-stellar Objects in Nearby Young Clusters,
Protostars and Planets VI, (Heidelberg, Germany, Jul. 15-20, 2013).
Gonzalez, A., Uzawa, Y.: 2013, Investigation on ALMA Band 4 CrossPolarization Performance, International Symposium on Space Tetahertz
Technology 2013, (Groningen, Netherlands, Apr. 8–10, 2013).
Gonzalez, A., Uzawa, Y.: 2013, Analysis of ALMA band 4 Crosspolarization Frequency Behavior, 2013 Asia-Pacific Radio Science
Conference, (Taipei, Taiwan, Sep. 3-7, 2013).
Goto, M.: 2013, Analytical solution of the Hanle effect in view of
CLASP and future polarimetric solar studies, The 7th Hinode Science
Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Goto, M.: 2013, Intuitive understanding of the Hanle effect, 7thInternational Workshop on Solar Polarization, (Kunming, China, Sep.
9-14, 2013).
Gouda, N.: 2013, Infrared Space Astrometry mission for the Galactic
Bulge, WISH Science Workshop: Exploring the Darkness, (Tokyo,
Japan, Dec. 2-3, 2013).
Grady, C., SEEDS team: 2013, Transitional Disks Associated with
Intermediate-Mass Stars:Results of the SEEDS Intermediate-Mass
Star, The 5th Subaru International Conference, Exoplanets and Disks:
Their Formation and Diversity II, (Kona, HI, USA, Dec. 8-12, 2013).
Guyon, O., Mateen, M., Liang, M., Hart, M., Oliker, M., Codona, J.:
2013, Putting the non-linear Curvature Wavefront Sensor on the 6.5m
MMT telescope, Adaptive Optics for ELTs 3, (Florence, Italy, May
30, 2013).
Guyon, O.: 2013, Optical tricks to image and study habitable exoplanets,
SETI institute lecture, (Mountain View, California, USA, Aug. 6, 2013).
Guyon, O.: 2013, High Contrast Imaging: New Techniques and Scientific

XIII Publications, Presentations

163

Perspectives for ELTs, Adaptive Optics for ELTs 3, (Florence, Italy,
May 30, 2013).
Guyon, O.: 2014, Coronagraphy - From State of the Art to the Near
Future, Search for Life Beyond the Solar System, (Tucson, AZ, USA,
Mar. 16-21, 2014).
Guyon, O.: 2014, LOWFSC & PSF for Exoplanets, LOWFSC & PSF for
Exoplanets, (Pasadena, CA, USA, Feb. 26-27, 2014).
Guyon, O.: 2014, On-sky wavefront correction with a 2048 actuator MEMS,
SPIE Photonics West, (San Francisco, CA, USA, Feb. 7-12, 2014).
Guyon, O.: 2014, Imaging exoplanets, SPIE Photonics West, (SanFrancisco, CA, USA, Feb. 7-12, 2014).
Hada, K.: 2013, Multi-frequency multi-epoch VLBI observations of
the M87 jet, IAU Symp. 304: Multiwavelength AGN Surveys andStudies, (Yerevan, Armenia, Oct. 7-12, 2013).
Hada, K.: 2013, Probing the inner jet of M87; from the jet base to HST1, The Innermost Regions of Relativistic Jets and Their Magnetic
Fields, (Granada, Spain, Jun. 10-14, 2013).
Hada, K.: 2013, Probing the relativistic jet of M87 with ALMA, Science
with ALMA Band-2 Workshop in Europe, (Bologna, Italy, May 2728, 2013).
Haga, T., Doi, A., Murata, Y., Sudou, H., Kameno, S., Hada, K., Nagai, H.:
2013, The core shift measurements for two-sided jets affected by FreeFree absorption using VLBA, The Innermost Regions of Relativistic
Jets and Their Magnetic Fields, (Granada, Spain, Jun. 10-14, 2013).
Hagino, M., Sakurai, T.: 2013, Butterfly Diagram of Magnetic Helicity
in Active Regions, Helicity Thinkshop on Solar Physics, (Beijing,
China, Aug. 27-31, 2013).
Hagiwara, Y., Suzuki, S., Oyama, T.: 2013, Upgrade of the VERA
telescopes for Dual-polarization Receiving (Poster), 5th KaVA Joint
Science WG Meeting, (Jeju, Korea, Jun. 17-19, 2013).
Hagiwara, Y.: 2014, EAVN test observations: current status, VERAKVN science workshop, (Kagoshima, Japan, Jan. 20-21, 2014).
Hagiwara, Y.: 2014, Extragalactic Submillimeter H2O masers, Workshop
on Insterstellar Medium and Masers, (Kagoshima, Japan, Mar. 27-28,
2014).
Hanada, H., Kikuchi, F., Noda, H., Matsumoto, K., Kunimori, H., Araki,
H., Kashima, S., Tsuruta, S., Asari, K., Sasaki, S.: 2013, Geodetic
Observations for Study of Interior of the Moon in SELENE-2 andFuture Missions, The 1st Beijing International Forum on Lunar andDeep-space Exploration 2013, (Beijng, China, Sep. 3-6, 2013).
Hanada, H., Kikuchi, F., Noda, H., Matsumoto, K., Kunimori, H.,
Araki, H., Kashima, S., Tsuruta, S., Asari, K., Sasaki, S.: 2013,
Geodetic Observations for Study of Interior of the Moon and theplanets in SELENE-2 and Future Missions, The 4th Moscow Solar
System Symposium (4M-S3), (Moscow, Russia, Oct. 14-18, 2013).
Hanada, H., Tsuruta, S., Araki, H., Asari, K., Kashima, S., Tazawa,S., Noda, H., Matsumoto, K., Sasaki, S., Funazaki, K., Satoh, A.,
Taniguchi, H., Kato, H., Kikuchi, M., Itou, Y., Chiba, K., Inaba, K.,
Yokokawa, R., Utsunomiya, S., Ping, J., Petrova, N., Gusev, A.,
Gouda, N., Yano, T., Yamada, Y., Niwa, Y., Kunimori, H., Iwata,T., Heki, K.: 2013, Some technological problems in developmentof a small telescope for gravimetry, IAG Symposium on Terrestrial
Gravimetry: Static and Mobile Measurements (TG-SMM2013), (SaintPetersburg, Russia, Sep. 17-20, 2013).
Hanada, H., Tsuruta, S., Araki, H., Asari, K., Kashima, S., Tazawa,S., Noda, H., Matsumoto, K., Sasaki, S., Funazaki, K., Satoh, A.,

164

XIII Publications, Presentations

Taniguchi, H., Kato, H., Kikuchi, M., Itoh, Y., Chiba, K., Inaba, K.,
Yokokawa, R., Utsunomiya, S., Gouda, N., Yano, T., Yamada,Y.,
Niwa, Y., Kunimori, H., Ping, J., Iwata, T., Heki, K.: 2013, Sometechnological problems in development of a small Telescope forselenodesy and geodesy, Japan Geoscience Union Meeting 2013,(Chiba, Japan, May 19-24, 2013).
Hanaoka, Y., Sakurai, T.: 2013, Infrared Stokes Polarimeter at NAOJ/
Mitaka, IAU Symp. 300: Nature of Prominences and their role inSpace Weather, (Paris, France, Jun. 10-14, 2013).
Hanayama, H.: 2013, Dust Structure of 213P/Van Ness and Cometary
Condensations, Mini-Workshop on Solar System Primitive Objects,(Seoul, Korea, Jun. 13-14, 2013).
Hanayama, H.: 2013, Report of EAYAM, 9th East Asian Meeting on
Astronomy, (Taipei, Taiwan, Oct. 14-18, 2013).
Hara, H.: 2013, Spectroscopy at the Site of Magnetic Reconnection in
the X-class Solar Flare on 2013 May 15, The 7th Hinode Science
Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda, H.,
Haruyama, J.: 2013, Frequency-dependence of the tidal dissipation on
the Moon: Effect of the low-viscosity zone at the lowermost mantle,
Japan Geoscience Union Meeting 2013, (Chiba, Japan, May 19-24,
2013).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda, H.,
Haruyama, J.: 2013, Frequency-dependence of the tidal dissipation on
the Moon: Effect of the low-viscosity zone at the, 18th International
Workshop on Laser Ranging - Pursuing Ultimate Accuracy &Creating New Synergies -, (Fujiyosida, Japan, Nov. 11-15, 2013).
Hashimoto, J., SEEDS/AO188/HiCIAO team: 2013, High resolution/high contrast near infrared imaging survey of protoplanetary disks
and exoplanets with Subaru/HiCIAO, Exoplanets and brown dwarfs:
Mind the gap, (Hertfordshire, UK, Sep. 2-5, 2013).
Hashimoto, J., SEEDS/AO188/HiCIAO team: 2013, High resolution/high contrast near infrared imaging survey of protoplanetary disks
and exoplanets with Subaru/HiCIAO, University of Tokyo Forum,(Sao Paulo, Brazil, Nov. 7, 2013).
Hashimoto, J., SEEDS/AO188/HiCIAO team: 2013, NIR observationsof protoplanetary disks, The 5th Subaru International Conference,
Exoplanets and Disks: Their Formation and Diversity II, (Kona, HI,
USA, Dec. 8-12, 2013).
Hatsukade, B.: 2013, ALMA Observations of High-z Star-forming
Galaxies, East-Asian ALMA Science Workshop 2013, (Taipei,
Taiwan, Sep. 2-4, 2013).
Hayano, Y.: 2013, Overview of Subaru GLAO, Subaru Ground Laser
AO Science Workshop, (Sapporo, Japan, Jun. 13-14, 2013).
Herrera, C.: 2013, Early stages of cluster formation in the Antennae
merger, East-Asian ALMA Science Workshop 2013, (Taipei, Taiwan,
Sep. 2-4, 2013).
Hesse, M., Aunai, N., Zenitani, S., Kuznetsova, M. M., Birn, J.: 2013,
The mysteries of the diffusion region in asymmetric systems, AGU
Fall Meeting 2013, (San Francisco, CA, USA, Dec. 9-13, 2013).
Hesse, M., Aunai, N., Zenitani, S., Kuznetsova, M., Birn, J.: 2013,
Magnetic reconnection in asymmetric systems: x-line orientationand guide field acceleration, European Geosciences Union General
Assembly 2013, (Vienna, Austria, Apr. 7-12, 2013).
Hibi, Y., Sun, J, Qin, H., Matsuo, H., Kang, L., Chen, J., Wu, P.: 2013,
Developments of the Cryogenic Integrated Circuits with GaN/AlGaNHEMTs and the New High Sensitivity Terahertz Detectors, 10th
International Workshop on Low Temperatures Electronics, (Paris,
France, Oct. 14-17, 2013).
Hirai, Y., Hidaka, J., Saitoh, T. R., Fujii, M., Shibagaki, S., Mathews,
G. J., Kajino, T.: 2014, Chemo-Dynamical Evolution of Dwarf
Spheroidal Galaxies, 11th Russbach School on Nuclear Astrophysics,(Russbach, Austria, Mar. 9-15, 2014).
Hirai, Y., Kajino, T., Hidaka, J., Shibagaki, S., Mathews, G. J.: 2013,
Chemo-Dynamical Evolution of Colliding Dwarf Spheroidal Galaxies,
12th International Symposium on Origin of Matter and Evolution of
Galaxies (OMEG12), (Tsukuba, Japan, Nov. 18-22, 2013).
Hirota, T.: 2013, ALMA Cycle 0 Observation of Orion Radio Source
I, Orion Nebula Cluster as a Paradigm of Star Formation workshop,(Baltimore, MD, USA, Oct. 13-16, 2013).
Hirota, T.: 2013, ALMA Observations of the Millimeter/Submillimeter
H2O Masers in Orion KL, Asia-Pacific regional URSI conference(AP-RASC), (Taipei, Taiwan, Sep. 3-7, 2013).
Hirota, T.: 2013, Observational Studies of H2O Maser Burst In OrionKL With VERA And ALMA, A Neapolitan of Masers: Variability,
Magnetism and VLBI, (Sydney, Australia, May 20-22, 2013).
Hirota, T.: 2013, Report from SFR sub-WG, VERA-KVN science
workshop, (Jeju, Korea, Jun. 20-21, 2013).
Hirota, T.: 2014, Recent results of millimeter/submillimeter observationsof H2O and CH3OH masers, Workshop on Insterstellar Medium andMasers, (Kagoshima, Japan, Mar. 27-28, 2014).
Hirota, T.: 2014, Status report of SFRs sub-WG, VERA-KVN science
workshop, (Kagoshima, Japan, Jan. 20-21, 2014).
Honma, M.: 2013, Galactic structure revealed by maser astrometry with
VERA, Asia-Pacific regional URSI conference (AP-RASC), (Taipei,
Taiwan, Sep. 3-7, 2013).
Honma, M.: 2013, Event-horizon-scale observations of super-massive
black holes with mm/sub-mm VLBI, Relativistic Jets in AGNs 2013,(Tokyo, Japan, Nov. 22, 2013).
Hori, Y., Ida, S., Lin, D. N. C.: 2013, Characterizing Low-Mass Planets
Orbiting Cool Stars with Water and Hydrogen, The 5th Subaru
International Conference, Exoplanets and Disks: Their Formation andDiversity II, (Kona, HI, USA, Dec. 8-12, 2013).
Hori, Y., Ida, S., Lin, D. N. C.: 2013, Water Content and Hydrogen-Rich
Atmospheres of ExoEarths Orbiting Cool Stars, The 1st COSPAR
Symposium: Planetary Systems of our Sun and other Stars, and the
Future of Space Astronomy, (Bangkok, Thailand, Nov. 11-15, 2013).
Hori, Y., Ida, S., Lin, D. N. C.: 2014, Water content and hydrogen-richatmospheres of sub-/super-Earths orbiting cool stars, Exoclimes III:The Diversity of Planetary Atmospheres, (Davos, Switzerland, Feb.
2-9, 2014).
Igarashi, A., Mori, M., Nitta, S.: 2013, A New Concept of TransonicGalactic Outflows in a Cold Dark Matter Halo with a Central SuperMassive Black Hole, 12th Asia Pacific Physics Conf. (APPC12),(Chiba, Japan, Jul. 14-19, 2013).
Iguchi, S.: 2013, ALMA Status: Construction and Early Science
Operation, 2013 Asia-Pacific Radio Science Conference, (Taipei,
Taiwan, Sep. 3-7, 2013).
Iguchi, S.: 2013, Overview and status of ALMA development program
including progress (instrumental and science) at other executives, EA
ALMA Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Imanishi, M.: 2013, Infrared and (sub)mm energy diagnostic of nearby

ULIRGs, A Panchromatic View of Galaxy Evolution 30 Years after
IRAS, (Paphos, Cyprus, Jun. 10-14, 2013).
Imanishi, M.: 2013, ALMA Cycle 0 observations of nearby luminous
infrared galaxies using high density molecular gas tracers, East-Asian
ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Iono, D.: 2013, ALMA First Science Results, 2013 Asia-Pacific Radio
Science Conference, (Taipei, Taiwan, Sep. 3-7, 2013).
Iono, D.: 2013, Overview and status of ALMA development program
including progress (instrumental and science) at other executives, EA
ALMA Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Iono, D.: 2013, Introduction and anticipated specs for band 11, EA
ALMA Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Ishiguro, M., Müller, T., Durech, J., Choi, Y. J., Sekiguchi, T., Takahashi,J., Hanayama, H., Kuroda, D., Hasegawa, S.: 2013, Progress
Report: Hayabusa 2 Observation Sub-Group, Hayabusa 2 Joint
Science Team Meeting, (Tokyo, Japan, Sep. 19-20, 2013).
Ishikawa, R.: 2013, New diagnostic tool for magnetic fields in low-β
plasma: CLASP, The 7th Hinode Science Meeting, (Takayama, Gifu,
Japan, Nov. 12-15, 2013).
Ishikawa, R.: 2013, Precision VUV spectro-polarimetry for solar
chromospheric magnetic field measurements, 7th International
Workshop on Solar Polarization, (Kunming, China, Sep. 9-14, 2013).
Ishikawa, S., Krucker, S., Christe, S., Ramsey, B., Glesener, L., Saito,
S., Takashi, T., Watanabe, S., Tajima, T., Tanaka, T.: 2013, Highsensitivity hard X-ray imaging and spectroscopy with the Focusing
Optics X-ray Solar Imager (FOXSI) sounding rocket, Japan
Geophysical Union 2013, (Chiba, Japan, May 19-24, 2013).
Ishikawa, S.-N.: 2013, High-sensitivity hard X-ray solar observation
with the FOXSI rocket, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Ishiyama, K., Kumamoto, A., Ono, T., Yamaguchi, Y., Haruyama, J.,
Ohtake, M., Katoh, Y., Terada, N., Oshigami, S.: 2014, Estimation of
the bulk permittivity and porosity of the lunar uppermost mare basalt
based on the SELENE observation data, 45th Lunar and Planetary
Science Conference, (Woodlands, TX, USA, Mar. 17-21, 2014).
Ito, T., Higuchi, A.: 2013, Dynamical evolution of the Oort cloud newcomets, AOGS 10th Annual Meeting, (Brisbane, Australia, Jun. 2428, 2013).
Ito, T., Higuchi, A.: 2013, Dynamical behavior of the Oort Cloud newcomets in planetary region, 2013 NCTS Taiwan-Japan Symposium on
Celestial Mechanics and N-Body Dynamics, (Hsinchu, Taiwan, Dec.
6-7, 2013).
Ito, T.: 2013, Activity and budget plan of the NAOJ group in 2013, The
4th Maidanak Users Meeting, (Tarusa, Russia, Jul. 1-4, 2013).
Iwai, K., Shibasaki, K.: 2013, Measurements of Coronal and
Chromospheric Magnetic Fields using Polarization Observations by
the Nobeyama Radioheliograph, The 7th Hinode Science Meeting,(Takayama, Gifu, Japan, Nov. 12-15, 2013).
Iwai, K., Shibasaki, K.: 2013, Measurements of Coronal and
Chromospheric Magnetic Fields using Polarization Observations
by the Nobeyama Radioheliograph, International CAWSES-II
Symposium, (Nagoya, Japan, Nov. 18-22, 2013).
Iwata, T., Haruyama, J., Ohtake, M., Otake, H.: 2013, Results ofIntegrated Sciences Using the Data of SELENE/Kaguya Mission,
AOGS 10th Annual Meeting, (Brisbane, Australia, Jun. 24-28, 2013).
Iwata, T., Matsumoto, K., Ishihara, Y., Harada, Y., Kikuchi, F., Sasaki,

XIII Publications, Presentations

165

S.: 2013, Measurements of Martian rotational variations by space
geodetic techniques, Japan Geoscience Union Meeting 2013, (Chiba,
Japan, May 19-24, 2013).
Iwata, T.: 2014, A Study on the sample return mission for lunar
highlands, maria, and vertical holes, SELENE Symposium 2014 International Symposium of Lunar Science and Exploration using
data from Multi-Instruments -, (Tokyo, Japan, Mar. 4-5, 2014).
Izumiura, H.: 2013, OAO 188cm Reflector Refurbished: current status
and future issues, The 8th Workshop on Astronomy with Precise
Radial Velocity Measurements, (Ishigaki, Japan, Sep. 4-6, 2013).
Kaithakkal, A. J., Tsuneta, S., Suematsu, Y., Kubo, M., Shiota, D.,
Shimojo, M.: 2013, Association of Polar Faculae with the Polar
Magnetic Patches as Revealed with Hinode Observations, Japan
Geophysical Union 2013, (Chiba, Japan, May 19-24, 2013).
Kaithakkal, A. J.: 2013, The Association of Polar Faculae with Polar
Magnetic Patches Examined with Hinode/SOT-SP Observations, The 7th
Hinode Science Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Kajino, T., Yamazaki, D. G., Ichiki, K., Mathews, G. J., Aoki, W.,
Fujiya, W., Cheoun, M. K., Suzuki, T., Otsuka, T., Balantekin, B.,
Deliduman, Y., Hayakawa, T., Chiba, S., Hidaka, J., Shibagaki,S., Hirai, Y.: 2013, Cosmological and Supernova Neutrinos andNucleosynthesis, 27th Texas Symposium on Relativistic Astrophysics,(Dallas, TX, USA, Dec. 8-13, 2013).
Kajino, T.: 2013, Cosmological and Supernova Neutrinos, International
Workshop on Neutrino Physics and Astrophysics, (South Dakota,
USA, Jul. 15-26, 2013).
Kajino, T.: 2013, Supernova Neutrinos and Explosive Nucleosynthesis,
7th European Physical Society Summer School on Nuclear
Astrophysics, (Catania, Italy, Sep. 15-27, 2013).
Kajino, T.: 2013, Big-Bang Nucleosynthesis and Neutrinos – I,
Supernova Nucleosynthesis and Neutrinos - II, IBS Workshop on
Rare Isotopes and Nuclear Astrophysics with Related Topics, (Pohang,
Korea, Sep. 25-27, 2013).
Kajino, T.: 2013, Big-Bang Cosmology and Neutrinos, SOKENDAI
Asian Winter School 2013, (Tokyo, Japan, Nov. 11-15, 2013).
Kajino, T.: 2013, Supernova Constraints on Neutrino Oscillationand Equation of States of Proto-Neutron Stars, 12th International
Symposium on Origin of Matter and Evolution of Galaxies(OMEG12), (Tsukuba, Japan, Nov. 18-22, 2013).
Kajino, T.: 2014, Element Genesis in Cosmology and Astrophysics, USJapan Joint Workshop on Nuclear Science Frontier explored by UltraHigh Power Lasers, Laser Institute, (Osaka, Japan, Feb. 3, 2014).
Kajino, T.: 2014, Element Genesis in the Big-Bang and Supernovae,
Workshop on Neutrinos and Nuclear Astrophysics, (Tokyo, Japan,
Feb. 21, 2014).
Kamata, Y., Nakaya, H., Kawanomoto, S., Miyazaki, S.: 2013, Resultsof Acceptance Tests of Hyper Suprime-Cam CCDs, ScientificDitector Workshop 2013, (Florence, Italy, Oct. 7-11, 2013).
Kamazaki, T.: 2013, First CSV Results with the ACA Correlator, 2013 AsiaPacific Radio Science Conference, (Taipei, Taiwan, Sep. 3-7, 2013).
Kambe, E.: 2013, Status Report on HIDES/OAO-1.88m, The 8thWorkshop on Astronomy with Precise Radial Velocity Measurements,(Ishigaki, Japan, Sep. 4-6, 2013).
Kameno, S.: 2013, ALMA extended array, EA ALMA Development
Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Kameno, S.: 2013, ALMA extended array, ALMA Workshop on Long

166

XIII Publications, Presentations

Baseline and Phase Correction, (Tokyo, Japan, Dec. 25-26, 2013).
Kano, R.: 2013, Relation between magnetic fields and horizontal
velocity in an active region, The 7th Hinode Science Meeting,(Takayama, Gifu, Japan, Nov. 12-15, 2013).
Kano, R.: 2014, Sounding Rocket Experiment: CLASP (Chromosphric
Lyman-Alpha Spectro-Polarimeter), ISSI Team Meeting (ID: 283),(Bern, Switerland, Jan. 27-31, 2014).
Karatsu, K., Nitta, T., Sekine, M., Sekiguchi, S., Sekimoto, Y.,
Noguchi, T., Uzawa, Y., Matsuo, H., Kiuchi, A., Naruse, M.: 2013,
Measurement of MKID Performance with High-speed and Wide-band
Readout System, 15th International Workshop on Low Temperature
Detectors, (Pasadena, USA, Jun. 24-28, 2013).
Karatsu, K., Nitta, T., Sekine, M., Sekiguchi, S., Sekimoto, Y., Noguchi,T., Uzawa, Y., Matsuo, H., Kiuchi, H., Miyachi, A., Naruse, M.:
2013, Development of MKID Camera for Future Ground-based
CMB Observations, International Conference on Cosmic Microwave
Background, (Okinawa, Japan, Jun. 10-14, 2013).
Kashikawa, N.: 2013, A LyA Emitter with an Extremely Large Restframe Equivalent Width of 900A at z=6.5, Galaxy Evolution overFive Decades, (Cambridge, UK, Sep. 3-6, 2013).
Kashikawa, N.: 2013, When I wish upon WISH, WISH Science
Workshop: Exploring the Darkness, (Tokyo, Japan, Dec. 2-3, 2013).
Kashikawa, N.: 2014, High-z quasar sciences, Quasor Science with
HSC: Toward the First Results, (Taipei, Taiwan, Jan. 14-16, 2014).
Kashima, S., Hanada, H., Araki, H., Noda, H., Kunimori, H.: 2013,
Optical Response Simulation of Corner Cube Reﬂectors for SELENE2
Mission, Japan Geoscience Union Meeting 2013, (Chiba, Japan, May
19-24, 2013).
Kashima, S., Hanada, H., Araki, H., Tsuruta, S.: 2013, Developementof the telescope for ILOM (In-site Lunar Orientation Measurement)using the DOE (Diffractive Optical Elemen, Japan Geoscience Union
Meeting 2013, (Chiba, Japan, May 19-24, 2013).
Kashiwagi, K., Suzuki, S., Tanaka, Y., Kotani, T., Nishikawa, J., Suto,
H., Tamura, M., Kurokawa, T.: 2013, 400-nm-Spanning Astro-Comb
Directly Generated from Synthesized Pump Pulse with Repetition
Rate of 12.5 GHz, Conference on Lasers and Electro Optics 2013
(CLEO 2013), (San Jose, USA, Jun 6-14, 2013).
Kasuga, M.: 2013, Calibration on EIS Instrumental Width from
Observations and Its Application, The 7th Hinode Science Meeting,(Takayama, Gifu, Japan, Nov. 12-15, 2013).
Kasuga, T., Iijima, T., Watanabe, J.: , Is a 2004 Leonid meteor spectrum
captured in a 182 cm telescope?, Meteoroids 2013, An International
Conference on Minor Bodies in the Solar System, (Poznan, Poland,
May 26-30, 2013).
Kataoka, A., Tanaka, H., Okuzumi, S., Wada, K.: 2013, Static compressionof fluffy dust aggregates in protoplanetary disks, Ice and Planet
Formation Workshop, (Lund, Sweden, May 15-17, 2013).
Kataoka, A.: 2013, Fluffy dust forms icy planetesimals by static
compression, The 5th Subaru International Conference, Exoplanets
and Disks: Their Formation and Diversity II, (Kona, HI, USA, Dec.
8-12, 2013).
Kato, Y., Mouri, N., Hibino, Y., Otsuji, K., Sakae, T., Hagino, M., Oi, A.,
Ueno, S., Ichimoto, K.: 2013, Simultaneous multi-line observation ofEllerman bombs using the DST in Hida observatory, The 7th Hinode
Science Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Kato, Y.: 2013, Chromospheric and Coronal Wave Generation in theNetwork Magnetic Elements Through the Magnetic Pumping, The 7th
Hinode Science Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Kato, Y.: 2013, Detecting chromospheric magneto-acoustic body wave
near the MBPs by using Mg II h&k lines, The 7th Hinode Science
Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Katsukawa, Y., Ichimoto, K., Suematsu, Y., Hara, H., Kano, R., Shimizu,T., Matsuzaki, K.: 2013, Design progress of the Solar UV-Vis-IR
Telescope (SUVIT) aboard SOLAR-C, SPIE Optics+Photonics, (San
Diego, CA, USA, Aug. 25-29, 2013).
Katsukawa, Y.: 2013, Imaging and spectroscopic studies of rapid eventsin the solar chromosphere, 12th International Workshop on theInterrelationship between Plasma Experiments in the Laboratory andin Space (IPELS2013), (Nagano, Japan, Jul. 1-5, 2013).
Katsukawa, Y.: 2013, Physics of the Sun, 10th Japanese-German
Frontiers of Science Symposium, (Kyoto, Japan, Nov. 1-3, 2013).
Katsukawa, Y.: 2013, Implication of the magnetic power spectra derived
with the Hinode SP, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Katsukawa, Y.: 2013, Study of 3D Fine-Scale Structure and Dynamics
of Solar Polar Faculae, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Katsukawa, Y.: 2013, Implication of the magnetic power spectra derived
with the Hinode, The 7th Hinode Science Meeting, (Takayama, Gifu,
Japan, Nov. 12-15, 2013).
Kawaguchi, N., Kim, J. S., Shibata, K. M., Lee, S. S., Honma, M.,
Cho, S. H., Byun, D. Y., Oh, S. J., Roh, D. G., Kobayashi, H.: 2013,
A Joint VLBI Array of VERA and KVN, Asia-Pacific regional URSI
conference (AP-RASC), (Taipei, Taiwan, Sep. 3-7, 2013).
Kawaguchi, N.: 2013, A road to the VERA 86-GHz observation, VERAKVN science workshop, (Jeju, Korea, Jun. 20-21, 2013).
Kawaguchi, N.: 2013, VERA Contribution to the EAVN, The 6th East
Asia VLBI Workshop 2013, (Jeju, Korea, Jun. 17-19, 2013).
Kero, J., Szasz, C., Nakamura, T., Terasawa, T., Nishimura, K., Tsutsumi,
M., Fujiwara, Y., Ueda, M., Watanabe, J., Abe, S., Abo, M., Tanaka,Y., Yamamoto M.: 2013, The MU radar meteor head echo database,Meteoroids 2013, An International Conference on Minor Bodies in
the Solar System, (Poznan, Poland, May 26-30, 2013).
Kim, J.- S., Kim, S.-W., Kurayama, T., Honma, M., Sasao, T., Surcis,
G., Canto, J., Torrelles, J. M., Kim, S. J.: 2013, New Insights on the
Outflow Evolution in the Massive Star-forming Region W75N, The
6th East Asia VLBI Workshop 2013, (Jeju, Korea, Jun. 17-19, 2013).
Kim, J.-S., Kim, S.-W., Lee, S. S., Han, M. H., Kang, S. C., Shin, J. M.,
Byun, D. Y.: 2013, KVN Polarization Observation of 2013 Small
flares in Black Hole Microquasar Cygnus X-3 during MOGABA
Project, The 13th Italian-Korean Symposium on Relativistic
Astrophysics, (Ewha Womans University, Korea, Jul. 15-19, 2013).
Kim, M. K.: 2013, 44 GHz methanol imaging observation with KVN, The
6th East Asia VLBI Workshop 2013, (Jeju, Korea, Jun. 17-19, 2013).
Kim, M. K.: 2013, Masers In Orion-KL, A Neapolitan of Masers: Variability,
Magnetism and VLBI, (Sydney, Australia, May 20-22, 2013).
Kim, S.-W., Kim, J.-S., Kurayama, T., Honma, M., Sasao, T.: 2013, Jetejection Event during a Soft-to-Hard X-ray transition in Microquasar
Cygnus X-3, The 6th East Asia VLBI Workshop 2013, (Jeju, Korea,
Jun. 17-19, 2013).
Kime, A., Matsuyama, S., Fukui, R., Sakao, T., Suematsu, Y., Yamauchi,
K.: 2013, Development of an X-ray slope profiler for Wolter mirror- Performance evaluation using wave-optical simulator -, The
MEADOW 2013 workshop (Metrology, Astronomy, Diagnostics andOptics Workshop), (Trieste, Italy, Oct. 28-30, 2013).
Kino, M., Takahara, F., Hada, K., Doi, A.: 2013, Energy densities ofmagnetic field and relativistic electrons at the innermost region of
the M87 jet, The Innermost Regions of Relativistic Jets and Their
Magnetic Fields, (Granada, Spain, Jun. 10-14, 2013).
Kitai, R., Watanabe, H., Otsuji, K.: 2013, Morphological study ofpenumbral formation, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Kiuchi, H.: 2013, Photonic LO signal generation and distribution
techniques for VLBI, and an artificial calibration source for ALMA
high-site, EA ALMA Development Workshop 2013, (Tokyo, Japan,
Jul. 7-8, 2013).
Kiuchi, H.: 2013, Photonic microwave/millimeter-wave generationand transmission techniques for ALMA, 2nd International VLBI
technology workshop, (Jeju, Korea, Oct. 10-12, 2013).
Kiuchi, H.: 2013, Characteristics and possible problems of ALMA line
length corrector, and the possibilities of other mechanisms, ALMA
Workshop on Long Baseline and Phase Correction, (Tokyo, Japan,
Dec. 25-26, 2013).
Kiyokane, K.: 2013, Two-dimensional angular momentum distribution
toward protostellar cores, East-Asian ALMA Science Workshop
2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Kobayashi, H., Cho, S. H., Kawaguchi, N., Fujisawa, K., Zhen, Z.
G., Honma, M., Shibata, K. M., Kim, J. S., Rho, D. G., Lee, S.
S., Hachisuka, K., Asada, K., Inoue, M.: 2013, East Asian VLBI
Network -Status and Future-, Asia-Pacific regional URSI conference(AP-RASC), (Taipei, Taiwan, Sep. 3-7, 2013).
Kobayashi, H.: 2013, Status and Future of EAVN, The 6th East Asia
VLBI Workshop 2013, (Jeju, Korea, Jun. 17-19, 2013).
Kodama, T., Koyama, Y., Tadaki, K., Hayashi, M., Tanaka, I.,
Shimakawa, R.: 2013, The progenitors of cluster early-type galaxies
under rapid construction at z~2, Tracing Cosmic Evolution with
Clusters of Galaxies, (SESTO, Italy, Jul. 4, 2013).
Kodama, T., Koyama, Y., Tadaki, K., Hayashi, M., Tanaka, I.,
Shimakawa, R.: 2013, The progenitors of cluster early-type galaxies
under rapid construction at z~2, Galaxy Evolution over Five Decades,(Cambridge, UK, Sep. 3-6, 2013).
Kojima, H., et al. including Oshima, A.: 2013, A Proposal of a Multi
Directional Neutron Telescope for Observations of Galactic Cosmic
Rays, The 33rd International Cosmic Ray Conference (ICRC2013),(Rio de Janeiro, Brazil, Jul. 2-9, 2013).
Kojima, H., et al. including Oshima, A.: 2013, Swinson Flow and the Tilt
Angle of the Neutral Current Sheet, The 33rd International Cosmic Ray
Conference (ICRC2013), (Rio de Janeiro, Brazil, Jul. 2-9, 2013).
Kojima, H., et al. including Oshima, A.: 2013, Rigidity Dependence of
Forbush Decreases, The 33rd International Cosmic Ray Conference(ICRC2013), (Rio de Janeiro, Brazil, Jul. 2-9, 2013).
Kojima, T., Fujii, Y., Uzawa, Y., Asayama, S.: 2013, Local Oscillator
noise suppression by a balanced SIS mixer in 0.9 THz band,
IRMMW-THz2013, (Mainz, Germany, Sep. 1-6, 2013).
Kojima, T., Uzawa, Y.: 2013, Multibeam Heterodyne Receiver For
ALMA, EA ALMA Development Workshop 2013, (Tokyo, Japan,
Jul. 7-8, 2013).
Kojima, T.: 2013, Multi-beam receiver for ALMA, EA ALMAXIII Publications, Presentations

167

Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Kokubo, E.: 2013, The Basic Dynamical Model of Terrestrial Planet
Formation, The 1st COSPAR Symposium: Planetary Systems of ourSun and other Stars, and the Future of Space Astronomy, (Bangkok,
Thailand, Nov. 11-15, 2013).
Kokubo, E.: 2013, Formation of Terrestrial Planets from Protoplanets:
Effects of System Size and Position, The 5th Subaru International
Conference, Exoplanets and Disks: Their Formation and Diversity II,(Kona, HI, USA, Dec. 8-12, 2013).
Komiya, Y., Shirasaki, Y., Ohishi, M., Mizumoto, Y.: 2013, Black holemass dependence of the scale length of cross-correlation between
AGNs and galaxies, European Week of Astronomy and Space
Science, (Turku, Finland, Jul. 8-13, 2013).
Komiya, Y., Suda, T., Fujimoto, M. Y.: 2013, Current signatures andsearch for Pop. III stars in the Local Universe, European Week of
Astronomy and Space Science, (Turku, Finland, Jul. 8-13, 2013).
Komugi, S.: 2013, ALMA Array Performance and Calibration, 2013 AsiaPacific Radio Science Conference, (Taipei, Taiwan, Sep. 3-7, 2013).
Kotani, T., et al. including Narita, N., Tamura, M., Nishikawa, J.,
Hayano, Y., Oya, S., Kokubo, E., Izumiura, H.: 2013, Exoplanet
science with the SPICA Coronagraph Instrument, SPICA Science
Conference 2013 (From exoplanet to distant galaxies: SPICA's new
window on the cool universe), (Tokyo, Japan, Jun. 18-21, 2013).
Kotani, T., et al. including Tamura, M.: 2013, Detection andcharacterization of extra-solar planets by infrared radial velocity
and high-contrast imaging instruments, 9th East Asian Meeting on
Astronomy, (Taipei, Taiwan, Oct. 14-18, 2013).
Kotani, T., IRD team: 2013, IRD: InfraRed Doppler Instrumentfor Subaru Telescope, The 5th Subaru International Conference,
Exoplanets and Disks: Their Formation and Diversity II, (Kona, HI,
USA, Dec. 8-12, 2013).
Kotani, T., Tamura, M., Matsuo, T., Murakami, N., Kawahara, H.,
IRD team, SEIT team: 2013, Detection and characterization of extrasolar planets by infrared radial velocity and high-contrast imaging
instruments, 9th East Asian Meeting on Astronomy, (Taipei, Taiwan,
Oct. 14-18, 2013).
Koyama, Y.: 2013, SPICA distant cluster survey: unveiling thedust-obscured star formation activity triggered by young cluster
environments, SPICA Science Conference 2013 (From exoplanet to
distant galaxies: SPICA's new window on the cool universe), (Tokyo,
Japan, Jun. 18-21, 2013).
Koyama, Y.: 2013, From MAHALO-Subaru to ALOHA-TMT: unveilinginternal physics of distant galaxies across environment, TMT Scienceand Instrumentation Workshop (Astronomy in the TMT Era), (Tokyo,
Japan, Oct. 16-17, 2013).
Koyama, Y.: 2013, Environmental Effects on Galaxy Dynamics and Star
Formation in the Distant Universe, Subaru GLAO Science Workshop
2013, (Sapporo, Japan, Jun. 14, 2013).
Koyama, Y.: 2014, A systematic study of AGNs in clusters and AGN
environment with HSC, Quasor Science with HSC: Toward the First
Results, (Taipei, Taiwan, Jan. 14-16, 2014).
Kubo, M., et al. including Kano, R., Bando, T., Narukage, N., Ishikawa,
R., Katsukawa, Y., Ishikawa, S., Suematsu, Y., Hara, H., Goto,M.: 2013, A Sounding Rocket Experiment for the Chromospheric
Lyman-Alpha Spectro-Polarimeter (CLASP), 7th Solar Polarization
Workshop (SPW#7), (Kunming, China, Sep. 9-13, 2013).

168

XIII Publications, Presentations

Kudo, T., et al. including Tamura, M.: 2013, SEEDS: Direct Imagingof Exoplanets and Their Forming Disks with the Subaru Telescope,
Transformational Science with ALMA: From Dust to Rocks toPlanets Formation and Evolution of Planetary Systems, (Kona, HI,
USA, Apr. 8-13, 2013).
Kudoh, T.: 2013, Magnetohydrodynamics of interstellar gas, SOKENDAI
Asian Winter School 2013, (Tokyo, Japan, Nov. 11-15, 2013).
Kumamoto, A., Ishiyama, K., Ono, T., Kobayashi, T., Oshigami, S.,
Haruyama, J.: Determination of the effective dielectric constant of
the lunar surface based on the radar echo intensity observed by the
Kaguya, 45th Lunar and Planetary Science Conference, (Woodlands,
TX, USA, Mar. 17-21, 2014).
Kurosaki, K., Ikoma, M., Hori, Y.: 2013, Threshold Mass and Radii
for Survival of Photo-Evaporating Low-Density Low-Mass Planets
Orbiting G-Type and M-Type Stars, Kepler Science Conferences II,(Moffett Field, USA, Nov. 4-8, 2013).
Kurosaki, K., Ikoma, M., Hori, Y.: 2013, Theoretical mass-radiusrelationships of water-rich low-mass exoplanets: effects of thermal
evolution and mass loss, Protostars & Planets VI, (Heidelberg,
Germany, Jul. 15-20, 2013).
Kuzuhara, M., et al. including Tamura, M.: 2013, Studies of Exoplanetary
Systems with Subaru Telescope, 9th East Asian Meeting on
Astronomy, (Taipei, Taiwan, Oct. 14-18, 2013).
Kuzuhara, M., et al. including Tamura, M.: 2013, A Report of the SEEDS
Exoplanets and Disks Direct Imaging Survey, The 1st COSPAR
Symposium: Planetary Systems of our Sun and other Stars, and the
Future of Space Astronomy, (Bangkok, Thailand, Nov. 11-15, 2013).
Kuzuhara, M., SEEDS team: 2013, SEEDS Direct Imaging Survey for
Exoplanets, The 5th Subaru International Conference, Exoplanets andDisks: Their Formation and Diversity II, (Kona, HI, USA, Dec. 8-12,2013).
Kwon, J., Tamura, M.: 2013, Infrared Polarimetric Studies of Star andPlanet Forming Regions, AGU Fall Meeting 2013, (San Francisco,
CA, USA, Dec. 9-13, 2013).
Kwon, J., Tamura, M.: 2013, Infrared Polarimetric Studies toward Star
and Planet Forming Regions, 9th East Asian Meeting on Astronomy,(Taipei, Taiwan, Oct. 14-18, 2013).
Kwon, J., Tamura, M.: 2013, Near-Infrared Circular Polarimetry of NGC
6334-V: The Origin of Circular Polarization, The 6th meeting on
Cosmic Dust, (Kobe, Japan, Aug. 5-9, 2013).
Kwon, J., Tamura, M.: 2013, A Near-Infrared Linear and Circular
Polarization Survey of Star Forming Regions, Protostars & Planets
VI, (Heidelberg, Germany, Jul. 15-20, 2013).
Kwon, J., Tamura, M.: 2013, Infrared Polarimetric Studies of Star andPlanet Forming Regions, AGU Fall Meeting 2013, (San Francisco,
CA, USA, Dec. 9-13, 2013).
Lee, M.: 2013, The Gas Dynamics Of Centaurus A From Near The
Circumnuclear Disk (~100 pc) To The Center Of The Galaxy, East-Asian
ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Lin, Z.-Y., Ip, W.-H., Lin, C.-H., Yoshida, F.: 2013, Broadband
Photometry of asteroid 1998 QE2 (285263) during its closest
approach of May-June 2013, 9th East Asian Meeting on Astronomy,(Taipei, Taiwan, Oct. 14-18, 2013).
Mathews, G. J.: 2013, Exploring the world of parallel universes and extra
dimensions, Workshop on Nuclear and Particle Physics, (Fukuoka,
Japan, Sep. 6, 2013).

Mathews, G. J.: 2013, Primordial Nucleosynthesis: A Cosmological Pointof View - Part I – Background, Seventh European Summer School on
Experimental Nuclear Atrophysics, (Santa Tecla, Italy, Sep. 15-27, 2013).
Mathews, G. J.: 2013, Primordial Nucleosynthesis: A Cosmological Pointof View - Part II – Frontier, Seventh European Summer School on
Experimental Nuclear Atrophysics, (Santa Tecla, Italy, Sep. 15-27, 2013).
Mathews, G. J.: 2013, Key Issues regarding the physics of neutrinos
and nucleosynthesis in core-collapse neutrinos - Part I- Supernova
Explosion Mechanism, IBS Workshop on Rare Isotopes and Nuclear
Astrophysics with Related Topics, (Pohang, Korea, Sep. 25-27, 2013).
Mathews, G. J.: 2013, Key Issues regarding the physics of neutrinos
and nucleosynthesis in core-collapse neutrinos - Part II- Supernova
Nucleosynthesis, IBS Workshop on Rare Isotopes and Nuclear
Astrophysics with Related Topics, (Pohang, Korea, Sep. 25-27, 2013).
Mathews, G. J.: 2013, The case for Dark Flow: “Observational evidence
for and against cosmic flow, quantum entanglement and parallel
universes”, Astronomy Colloquium, (Tokyo, Japan, Oct. 8, 2013).
Mathews, G. J.: 2013, The case for Dark Flow: “Observational evidence forand against cosmic flow, quantum entanglement and parallel universes”,
Astrophysics Seminar, (Notre Dame, IN, USA, Oct. 15, 2013).
Mathews, G. J.: 2013, Key Issues regarding the physics of neutrinos
and nucleosynthesis in core-collapse neutrinos, American PhysicalSociety Meeting, Division of Nuclear Physics, (Newport News, VA,
USA, Oct. 27, 2013).
Mathews, G. J.: 2013, “A density functional equation of state forsupernova collapse: Effects of 3-body forces, hadrons and thetransition” to quark gluon plasma, International Workshop on Nuclear
equation of state with strangeness, (Saitama, Japan, Nov. 14, 2013).
Mathews, G. J.: 2013, The case for Dark Flow: Observational evidence
for and against cosmic flow, quantum entanglement and parallel
universes, SOKENDAI Asian Winter School 2013, (Tokyo, Japan,
Nov. 11-15, 2013).
Mathews, G. J.: 2013, Observational evidence for and against cosmic
flow, quantum entanglement and parallel universes, 12th International
Symposium on Origin of Matter and Evolution of Galaxies(OMEG12), (Tsukuba, Japan, Nov. 18-22, 2013).
Mathews, G. J.: 2013, Key Issues regarding the physics of neutrinos andnucleosynthesis in core-collapse neutrinos, 27th Texas Symposium
on Relativistic Astrophysics, (Dallas, TX, USA, Dec. 8-13, 2013).
Matsuda, Y.: 2013, ALMA Blind [C II]158 μm Line Emitter Survey, EastAsian ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Matsuda, Y.: 2013, Ly-alpha morphology-density relation at high-z,
9th Marseille Cosmology Conference, Physical Processes of Galaxy
Formation: Consensus and Challenges, (Aix-en-Provence, France,
Jul. 22-26, 2013).
Matsumoto, J., Masada, Y.: 2013, Rayleigh-Taylor and RichtmyerMeshkov Instabilities in RelativisticHydrodynamic Jets, The
Innermost Regions of Relativistic Jets and Their Magnetic Fields,(Granada, Spain, Jun. 10-14, 2013).
Matsumoto, J., Masada, Y.: 2013, Rayleigh-Taylor and RichtmyerMeshkov Instabilities in Relativistic Hydrodynamic Jets, YIPQS
long-term workshop, supernovae and gamma-ray burst 2013, (Kyoto,
Japan, Oct. 14-Nov.15, 2013).
Matsumoto, K., Yamada, R., Kikuchi, F., Goossens, S., Kamata, S.,
Iwata, T., Hanada, H., Ishihara, Y., Sasaki, S.: 2013, A simulation
study for constraining the lunar internal structure by geodetic andseismic data, Japan Geoscience Union Meeting 2013, (Chiba, Japan,
May 19-24, 2013).
Matsumoto, K., Yamada, R., Kikuchi, F., Iwata, T., Hanada,
H., Ishihara, Y., Kamata, S., Sasaki, S.: 2013, Radius of lunar
core estimated by GRAIL results, AGU Fall Meeting 2013, (SanFrancisco, CA, USA, Dec. 9-13, 2013).
Matsumoto, K.: 2013, A simulation study for constraining the lunar internal
structure by geodetic and seismic data, International Symposium on
Planetary Sciences (IAPS2013), (Shanghai, China, Jul. 1-4, 2013).
Matsumoto, K.: 2014, Deep interior structure of the Moon inferred fromthe Apollo seismic data and the latest selenodetic, SELENE Symposium2014 - International Symposium of Lunar Science and Exploration using
data from Multi-Instruments -, (Tokyo, Japan, Mar. 4-5, 2014).
Matsumoto, N., KVN+VERA star formation science sub-WG members:
2013, VLBI Imaging of a 44 GHz CH3OH Maser with KVN+VERA,
Asia-Pacific regional URSI conference (AP-RASC), (Taipei, Taiwan,
Sep. 3-7, 2013).
Matsumoto, N.: 2013, Fringe check observations of SiO maser sources
toward the galactic center, The 6th East Asia VLBI Workshop 2013,(Jeju, Korea, Jun. 17-19, 2013).
Matsumoto, N.: 2013, VLBI Imaging Of 44 GHz Methanol Maser
Sources With KVN+VERA Array, A Neapolitan of Masers: Variability,
Magnetism and VLBI, (Sydney, Australia, May 20-22, 2013).
Matsumoto, N.: 2013, VLBI imaging of 44 GHz methanol maser sources
with KVN+VERA array, The 6th East Asia VLBI Workshop 2013,(Jeju, Korea, Jun. 17-19, 2013).
Matsumoto, N.: 2014, KaVA and JVN/VERA observations of 44/6.7
GHz methanol masers toward G18.34+1.78 SW, VERA-KVN science
workshop, (Kagoshima, Japan, Jan. 20-21, 2014).
Matsumoto, N.: 2014, KaVA observations of 44 GHz methanol masers
toward IRAS18151-1208 MM2, Workshop on Insterstellar Medium
and Masers, (Kagoshima, Japan, Mar. 27-28, 2014).
Matsuo, H.: 2013, Application of Photon Counting Detectors for Terahertz
Measurements, International Workshop on Optical Terahertz Scienceand Technology 2013, (Kyoto, Japan, Apr. 1-5, 2013).
Matsuo, H.: 2013, Fast and high-dynamic range imaging withsuperconducting tunnel junction detectors, 15th International Workshop
on Low Temperature Detectors, (Pasadena, USA, Jun. 24-28, 2013).
Matsuo, H.: 2013, Beyond ALMA or ALMA in Space, EA ALMA
Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Matsuo, H.: 2013, Photon Counting Technology for Terahertz Astronomy,
2013 Asia-Pacific Radio Science Conference, (Taipei, Taiwan, Sep.
3-7, 2013).
Matsuo, H.: 2013, Photon Counting Technology for Terahertz Astronomy,
10th International Workshop on Low Temperatures Electronics, (Paris,
France, Oct. 14-17, 2013).
Matsuo, H.: 2014, Photon Counting Terahertz Interferometry (PCTI),
1st FISICA Workshop Science Goals of a Sub-arcsecond Far-infrared
Space Observatory, (Rome, Italy, Feb. 17-18, 2014).
Min, C.: 2013, Orbit Determination for Symbiotic Star, R Aquarii, with
VERA SiO masers Astrometry, The 6th East Asia VLBI Workshop
2013, (Jeju, Korea, Jun. 17-19, 2013).
Min, C.: 2013, VERA Observations of SiO masers toward Symbiotic
star R Aquarii, Workshop on symbiotic stars, binary, post-AGB andrelated objects, (Wierzba, Poland, Aug. 18-23, 2013).
Miura E. R., Kohno, K., Tosaki, T., Espada, D., Hwang, N., Kuno, N.,

XIII Publications, Presentations

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Okumura S., Hirota, A., Muraoka, K., Onodera, S., Minamidani, T.,
Komugi, S., Nakanishi, K., Sawada, T., Kaneko, H., Kawabe, R.:
2013, Giant Molecular Evolutions in the nearby spiral galaxy M33,
East-Asian ALMA Science Workshop 2013, (Taipei, Taiwan, Sep.
2-4, 2013).
Miyachi, A., Kojima, T., Fujii, Y., Takeda, M., Uzawa, Y., Kroug, M.,
Noguchi, T.: 2013, Precision polishing of device backside for ALMABand 10 SIS mixer, AMDE2013, (Gunma, Japan, Dec. 19, 2013).
Miyamoto, H., et al. including Iwata, T.: 2013, Science and landing-site
candidates of the MELOS 1 EDL demonstrator, Japan Geoscience
Union Meeting 2013, (Chiba, Japan, May 19-24, 2013).
Momose, M., Tsukagoshi, T., Fukagawa, M., Saigo, K., Ohashi, N.,
Kitamura, Y., Akiyama, E., Aso, Y., Takeuchi, T., Kobayashi, H.,
Muto, T., Nomura, H., Honda, M., Fujiwara, H., Shibai, H., Inutsuka,
S.: 2013, ALMA Observations of the Asymmetrically Gapped Disk
around HD 142527, 2013 Asia-Pacific Radio Science Conference,(Taipei, Taiwan, Sep. 3-7, 2013).
Momose, M.: 2013, Planet Formation and Exoplanets, EA ALMA
Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Morita, S., Sakurai, T., Hanaoka, Y., Suzuki, I., NAOJ Solar Database
Team: 2013, Database of Over 90 Years Observations of the Sunat the National Astronomical Observatory of Japan, International
CAWSES-II Symposium, (Nagoya, Japan, Nov. 18-22, 2013).
Motogi, K., Sugiyama, K., Sorai, K., Walsh, A. J., Niinuma, K.,
Honma, M., Hirota, T., Yonekura, Y., Hachisuka, K., Fujisawa, K.:
2013, Time-resolved Studies of the High Mass Protostellar Object
G353.273+0.641, Asia-Pacific regional URSI conference (AP-RASC),(Taipei, Taiwan, Sep. 3-7, 2013).
Motogi, K., Sugiyama, K., Walsh, A. J., Niinuma, K., Sorai, K., Honma,
M., Hirota, T., Yonekura, Y., Fujisawa, K.: 2013, Detection of thebullet-like SiO jet and dense CH 3CN envelope around the highmass protostellar object G353.273+0.641, Protostars and Planets IV,(Heidelberg, Germany, Jul. 15-20, 2013).
Mouri, N., Kato, Y., Hibino, Y., Otsuji, K., Sakae, T., Oi, A., Ichimoto,K., Hagino, M., Kitai, R.: 2013, Development of the Mobile
Spectrograph for Educational Observation, The 7th Hinode Science
Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Nagai, H., Orienti, M., Kino, M., Doi, A., Giovannini, G., Asada, K.,
D'Ammando, F., Haga, T., Giroletti M., Hada, K.: 2013, Probing
the Radio Counterpart of Gamma-ray Flaring Region in 3C 84, The
Innermost Regions of Relativistic Jets and Their Magnetic Fields,(Granada, Spain, Jun. 10-14, 2013).
Nagai, H.: 2013, Commissioning Status of ALMA Polarization
Observation, 2013 Asia-Pacific Radio Science Conference, (Taipei,
Taiwan, Sep. 3-7, 2013).
Nagai, H.: 2013, Millimeter and Submillimeter Observation of Blazars
with ALMA, East-Asian ALMA Science Workshop 2013, (Taipei,
Taiwan, Sep. 2-4, 2013).
Nagasawa, R., Otsubo, T., Hanada, H.: 2013, Development of software
for high-precision LLR data analysis, 18th International Workshop
on Laser Ranging - Pursuing Ultimate Accuracy & Creating New
Synergies -, (Fujiyosida, Japan, Nov. 11-15, 2013).
Nagayama, T.: 2013, Measurement Of The Galactic Constants With
VERA, A Neapolitan of Masers: Variability, Magnetism and VLBI,(Sydney, Australia, May 20-22, 2013).
Nakahara, H., Iwai, K., Nakanishi, H.: 2013, A high-speed FFT based

170

XIII Publications, Presentations

on a six-step algorithm: Applied to a radio telescope for a solar
radio burst, The International Conference on Field-Programmable
Technology (FPT 2013), (Kyoto, Japan, Dec. 9-22, 2013).
Nakamura, K.: 2013, 3+1 gauge-invariant variables for perturbations
on Schwarzschild background spacetime, The 23rd workshop on
General Relativity and Gravitation in Japan, (Hirosaki, Japan, Nov.
5-8, 2013).
Namiki, N., Kobayashi, M., Kimura, J., Hussmann, H., Lingenauber,
K., Oberst, J., GALA-Japan Team: 2013, Development of JUICE/
Ganymede Laser Altimeter (GALA), Japan Geoscience Union
Meeting 2013, (Chiba, Japan, May 19-24, 2013).
Namiki, N., Mizuno, T., Hirata, N., Noda, H., Senshu , H., Yamada,R., Ikeda, H., Matsumoto, K., Oshigami, S., Miyamoto, H., Abe,S., Sasaki, S., Araki, H., Tazawa, S., Shizugami, M., Ishihara, Y.,
Kobayashi, M., Wada, K., Demura, H., Kimura, J., Yoshida, F., Hirata,
N.: 2013, Scientific Use of LIDAR data of Hayabusa-2 Mission, AOGS
10th Annual Meeting, (Brisbane, Australia, Jun. 24-28, 2013).
Namiki, N.: 2013, Lunar Internal Structure Estimated From Local
Admittance between Gravity and Topography, The 1st BeijingInternational Forum on Lunar and Deep-space Exploration 2013,(Beijng, China, Sep. 3-6, 2013).
Narita, N., Fukui, A., Ikoma, M., Hori, Y., Kurosaki, K., Kawashima,Y.: 2014, Multi-Color Simultaneous Transit Photometry of Planets
around Cool Host Stars, Exoclimes III: The Diversity of Planetary
Atmospheres, (Davos, Switzerland, Feb. 2-9, 2014).
Narita, N.: 2013, Transiting Exoplanet Search and Characterization with
Subaru's New Infrared Doppler Instrument (IRD), The 5th Subaru
International Conference, Exoplanets and Disks: Their Formation andDiversity II, (Kona, HI, USA, Dec. 8-12, 2013).
Narita, N.: 2013, Role of Japanese Telescopes, TESS Science Team
Meeting, (Boston, USA, May 19, 2013).
Narita, N.: 2013, Exoplanetary Science with Multi-Object Spectrographswith GLAO, Subaru GLAO Science Workshop 2013, (Sapporo,
Japan, Jun. 14, 2013).
Narita, N.: 2013, Science Cases for Transiting Planetary Systems withSPICA, SPICA Science Conference 2013 (From exoplanet to distantgalaxies: SPICA's new window on the cool universe), (Tokyo, Japan,
Jun. 18-21, 2013).
Narita, N.: 2013, Exploring New Worlds with TMT, TMT Science
Forum, (Kona, HI, USA, Jul. 22-23, 2013).
Narita, N.: 2013, Toward Detections and Characterization of Habitable
Transiting Exoplanets, International Astrobiology Workshop 2013,(Sagamihara, Japan, Nov. 28-30, 2013).
Narita, N.: 2014, Japanese New Instruments for Studying Transiting
Exoplanets, Exoclimes III: The Diversity of Planetary Atmospheres,(Davos, Switzerland, Feb. 11, 2014).
Narukage, N.: 2013, UV spectropolarimeter design for precise
polarization measurement with 0.1 % accuracy, The 7th Hinode
Science Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Narukage, N.: 2013, Solar Jets as Sources of Outflows, Heating andWaves ~Wave Generation by Magnetic Reconnection~, 2013 Meetingof the Americas, American Geophysical Union, (Cancun, Mexico,
May 20-23, 2013).
Narukage, N.: 2013, Fractal Structure (Turbulence) and SOC of aCurrent Sheet in a Solar Flare via Dynamic Magnetic Reconnection,
ISSI meeting (Self-Organized Criticality and Turbulence), (Bern,Swizerland, Sep. 16-20, 2013).
Niino, Y.: 2013, The Redshift Evolution of the Relation between Stellar
Mass, SFR, and Gas Metallicity, SCCS6 2013 Conference, Feeding,Feedback, and Fireworks: Celebrating Our Cosmic Landscape,(Hamilton Island, Australia, Jun. 24-28, 2013).
Niinuma, K., Fujinaga, Y., Kimura, A., Akutagawa, K., Fujisawa, K.,
Sugiyama, K., Motogi, K., Oyama, T., Mizuno, S., Takemura, S.,
Kono, Y.: 2013, VLBI Observation of Fermi/LAT Un-associatedGamma-ray Sources, Asia-Pacific regional URSI conference (APRASC), (Taipei, Taiwan, Sep. 3-7, 2013).
Nishikawa, J., Oya, M., Horie, M., Sato, K., Fukase, M., Murakami,N., Kotani, T., Tamura, M., Tanaka, Y., Kurokawa, T., Kumagai, S.:
2013, A coronagraph system with unbalanced nulling interferometer:
upgrade of 2013, The 5th Subaru International Conference,
Exoplanets and Disks: Their Formation and Diversity II, (Kona, HI,
USA, Dec. 8-12, 2013).
Nishimura, S.: 2013, Decay Spectrposcopy, The 1st RIBF-RISP
Workshop, (Seoul, Korea, Nov. 6-7, 2013).
Nishimura, S.: 2013, Neutron rich nuclei lifetimes for r-process, Seventh
European Summer School on Experimental Nuclear Atrophysics,(Santa Tecla, Italy, Sep. 15-27, 2013).
Nishimura, S.: 2013, Decay spectroscopy of exotic nuclei at RIBF,
Symposium Nuclear Structure Physics with Advanced GammaDetector Arrays (NSP13), (Padva, Italy, Jun. 10-12, 2013).
Nishimura, S.: 2014, Decay spectroscopy of r-process nuclei, 11th
Russbach School on Nuclear Astrophysics, (Russbach, Austria, Mar.
9-15, 2014).
Nishimura, S.: 2014, Decay spectroscopy o very neutron-rich nuclei at
RIBF, 25th International Nuclear Physics Conference (INPC2013),(Firenze, Italy, Jun. 2-7, 2013).
Nishiyama, S., Hatano, H., Nagata, T., Tamura, T.: 2013, Large Scale
Magnetic Field Configuration in the Galactic Center, The Galactic
Center Black Hole Laboratory, (Granada, Spain, Nov. 19-22, 2013).
Nishiyama, S., Yasui, K., Nagata, T., Yoshikawa, T., Tamura, M.,
Uchiyama, H.: 2013, The Origion of the Galactic Center Diffuse
X-ray emission investigated by near-infrared imaging and polarimetricobservations, The Galactic Center: Feeding and Feedback in a Normal
Galactic Nucleus, (Santa Fe, USA, Sep. 30-Oct. 4, 2013).
Nishiyama, S., Yasui, K., Nagata, T., Yoshikawa, T., Tamura, M.,
Uchiyama, H.: 2014, The Origion of the Galactic Center Diffuse
X-ray emission investigated by near-infrared observations, Suzaku
MAXI 2014 Expanding the Frontiers of the X-ray Universe, (Ehime,
Japan, Feb. 19-22, 2014).
Nishiyama, S.: 2013, Probing Space-time Structure near Massive
Black Hole with Orbiting Stars, TMT Science and Instrumentation
Workshop (Astronomy in the TMT Era), (Tokyo, Japan, Oct. 16-17,
2013).
Nishiyama, S.: 2013, Observations of the Galactic Center with Subaru/
GLAO, Subaru Ground Layer AO Science Workshop, (Sapporo,
Japan, Jun. 13-14, 2013).
Nishizuka, N., Hara, H., Brooks, D., Nishida, K.: 2013, Hinode
Spectroscopic Observation of Magnetic Reconnection in a Solar Flare,
Japan Geophysical Union 2013, (Chiba, Japan, May 19-24, 2013).
Nishizuka, N., Karlicky, M., Janvier, M., Barta, M.: 2013, Plasmoid
Ejections observed in Radio emissions and Particle Acceleration in
Solar Flares, CESRA Workshop 2013, (Prague, Czech Republic, Jun.

24-29, 2013).
Nishizuka, N., Nishida, K., Shibata, K.: 2013, Fractal Reconnection andStochastic Particle Acceleration induced by Prominence Eruption,
IAU Symp. 300: Nature of Prominences and their role in Space
Weather, (Paris, France, Jun. 10-14, 2013).
Nishizuka, N.: 2013, Nonlinear Fragmentation of Flare Current Sheets,
The 7th Hinode Science Meeting, (Takayama, Gifu, Japan, Nov. 1215, 2013).
Nishizuka. N.: 2013, Plasmoids, Fractal Reconnection and Particle
Acceleration in Solar Flares and Laboratory Experiments, 12th
International Workshop on the Interrelationship between Plasma
Experiments in the Laboratory and in Space (IPELS2013), (Nagano,
Japan, Jul. 1-5, 2013).
Nitta, T., Sekiguchi, S., Sekimoto, Y., Mitsui, K., Okada, N., Karatsu, K.,
Naruse, M., Sekine, M., Matsuo, H., Noguchi, T., Seta, M., Nakai, N.:
2013, Anti-Reflection (AR) Coating for Cryogenic Silicon and Alumina
Lenses at Millimeter-Wave Bands, 15th International Workshop on
Low Temperature Detectors, (Pasadena, USA, Jun. 24-28, 2013).
Nitta, T., Sekimoto, Y., Karatsu, K., Naruse, M., Sekine, M., Sekiguchi,S., Matsuo, H., Noguchi, T., Mitsui, K., Okada, N., Seta, M., Nakai,
N.: 2013, Close-Packed Silicon-Lens Antennas for Millimeter-Wave
MKID Camera, 15th International Workshop on Low Temperature
Detectors, (Pasadena, USA, Jun. 24-28, 2013).
Noda, H., Boggs, D. H., Williams, J. G.: 2013, LLR simulation study for
future observations, Japan Geoscience Union Meeting 2013, (Chiba,
Japan, May 19-24, 2013).
Noda, H., Mizuno, T., Kunimori, H., Takeuchi, H., Namiki, N.:
2013, Alignment measurement with optical transponder system of
Hayabusa-2 LIDAR, 18th International Workshop on Laser Ranging Pursuing Ultimate Accuracy & Creating New Synergies -, (Fujiyosida,
Japan, Nov. 11-15, 2013).
Nomura, H., Walsh, C., Millar, T. J., Aikawa, Y.: 2013, Diagnosing Gas
Dispersal Processes in Protoplanetary Disks, Protostars & Planets VI,(Heidelberg, Germany, Jul. 15-20, 2013).
Nomura, M., Ohsuga, K., Wada, K., Takahashi, H.: 2013, Radiationhydrodynamic simulation of line-driven disk wind, EAST-ASIA AGN
Workshop 2013, (Hokkaido, Japan, Aug. 20-23, 2013).
Oh, S. J., Roh, D. G., Yeom, J. H., Oh, C. S., Jung, J. S., Jung, D. K.,
Yoon, Y. J., Miyazaki, A., Oyama, T., Kawaguchi, N., Kobayashi,
H., Shibata, K. M.: 2013, Status of East Asian VLBI Correlator,
Asia-Pacific regional URSI conference (AP-RASC), (Taipei, Taiwan,
Sep. 3-7, 2013).
Ohishi, M.: 2013, Data Intensive Astronomy, 9th EAMA, (Taoyuan,
Taiwan, Oct. 14-18, 2013).
Ohishi, M.: 2013, Discovery of Absorption Features of CH3NH2 towards
SgrB2(M), The 1st COSPAR Symposium: Planetary Systems of ourSun and other Stars, and the Future of Space Astronomy, (Bangkok,
Thailand, Nov. 11-15, 2013).
Ohishi, M.: 2013, Discovery of Absorption Features of CH3NH2 towards
SgrB2(M), International Astrobiology Workshop 2013, (Sagamihara,
Japan, Nov. 28-30, 2013).
Ohishi, M.: 2014, VOEvent and its Applications, 2nd Annula
Symposium: New Developments in Astrophysics Through MultiMessenger Observations of Gravitational Wave Sources , (Tokyo,
Japan, Jan. 13-15, 2014).
Ohsuga, K.: 2013, Radiation-MHD simulations of accretion flows

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and outflows around black holes, Black holes, jets and outflows,(Kathmandu, Nepal, Oct. 14-18, 2013).
Ohsuga, K.: 2013, Global simulations of super-Eddington accretion
flows and outflows, Radiative Processes Near Black Holes, (Princeton,
USA, May 1-3, 2013).
Oka, T.: 2013, Probing the Galactic Center with ALMA after 2020, EA
ALMA Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Onishi, K., Iguchi, S., Sheth, K., Kohno, K.: 2013, Supermassive blackhole mass estimation for the nearby galaxy NGC 1097 with ALMA
Cycle 0 data, East-Asian ALMA Science Workshop 2013, (Taipei,
Taiwan, Sep. 2-4, 2013).
Oogi, T., Habe, A., Ishiyama, T.: 2013, Dry mergers and size evolutionof early-type galaxies, 2013 COSMOS Team Meeting, (Kyoto, Japan,
May 20-24, 2013).
Oshigami, S., Watanabe, S., Yamaguchi, Y., Yamaji, A., Kobayashi,T., Kumamoto, A., Ishiyama, K., Ono, T.: 2014, Mare volcanism:
Reinterpretation based on Kaguya Lunar Radar Sounder data, 45th
Lunar and Planetary Science Conference, (Woodlands, TX, USA,
Mar. 17-21, 2014).
Oshigami, S., Yamaguchi, Y., Mitsuishi, M., Momose, A., Yajima,
T. Murakami, T., Morozumi, H.: 2013, Mineralogical mapping of
Nevada using airborne hyperspectral data: Applying the Composite
MSAM, International Symposium on Remote Sensing 2013, (Chiba,
Japan, May 15-17, 2013).
Oshima, A., et al.: 2013, Rigidity Dependence of Forbush Decreases,
International CAWSES-II Symposium, (Nagoya, Japan, Nov. 18-22,
2013).
Oshima, A., et al.: 2013, An anisotropy of galactic cosmic rays observedwith GRAPES-3, The 33rd International Cosmic Ray Conference(ICRC2013), (Rio de Janeiro, Brazil, Jul. 2-9, 2013).
Oshino, S., Hori, Y.: 2013, N-body Simulations for Planetary Accretionin the Presence of Hot Jupiter, The 5th Subaru International
Conference, Exoplanets and Disks: Their Formation and Diversity II,(Kona, HI, USA, Dec. 8-12, 2013).
Otsuji, K., Sakurai, T., Kuzanyan, K.: 2013, Statistical Analysis of
Current Helicity Using Hinode/SOT SP Data, The 7th Hinode Science
Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Otsuji, K.: 2013, Emergence and Reconnection of Magnetic Fields in
the Solar Photosphere and Chromosphere, Asia Oceania Geosciences
Society, (Brisbane, Austraria, Jun. 24-28, 2013).
Oya, M., Nishikawa, J., Horie, M., Sato, K., Fukase, M., Murakami, N.,
Kotani, T., Tamura, M., Tanaka, Y., Kurokawa, T., Kumagai, S.: 2013,
Adaptive optics operation with a focal plane wavefront sensing in acoronagraph, The 5th Subaru International Conference, Exoplanets
and Disks: Their Formation and Diversity II, (Kona, HI, USA, Dec.
8-12, 2013).
Ozaki, S., Miyazaki, S., Yamashita, T., Tanaka, Y., Hattori, T.,
Okada, N., Mitsui, K., Fukushima, M., Obuchi, Y.: 2013,
Developmant of an optical integral field unit with an image slicer,
TMT Science and Instrumentation Workshop (Astronomy in the TMTEra), (Tokyo, Japan, Oct. 16-17, 2013).
Saigo, K.: 2013, ALMA Observation of a Prototypical Protostellar Binary
System L1551 NE - Keplerian Cirsumbinary Disk and Accretion
Streams, East-Asian ALMA Science Workshop 2013, (Taipei, Taiwan,
Sep. 2-4, 2013).
Saito, M.: 2013, Recent Progress of Observations of Protoplanetary

172

XIII Publications, Presentations

Disks at mm - submm, The 5th Subaru International Conference,
Exoplanets and Disks: Their Formation and Diversity II, (Kona, HI,
USA, Dec. 8-12, 2013).
Saito, T.: 2013, ALMA observations of various gas phases in the IRbright merger VV114, East-Asian ALMA Science Workshop 2013,(Taipei, Taiwan, Sep. 2-4, 2013).
Sakai, N.: 2013, Absolute Proper Motion Of IRAS 00259+5625, A
Neapolitan of Masers: Variability, Magnetism and VLBI, (Sydney,
Australia, May 20-22, 2013).
Sakai, N.: 2013, Absolute Proper Motion of IRAS 00259+5625 with
VERA, The 6th East Asia VLBI Workshop 2013, (Jeju, Korea, Jun.
17-19, 2013).
Sakai, N.: 2014, Astrometry of massive star-forming region IRAS 074272400 with VERA, VERA-KVN science workshop, (Kagoshima,
Japan, Jan. 20-21, 2014).
Sako, N., Shimojo, M., Watanabe, T., Sekii, T.: 2013, An energetics
study of the X-ray jets, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Sako, N.: 2013, An energetics study of X-ray jets, The 7th Hinode
Science Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Sakurai, T.: 2013, Recent Climate of Solar Physics, The Second AsiaPacific Solar Physics Meeting, (Hangzhou, China, Oct. 24-26, 2013).
Sasaki, S., Kikuchi, F., Matsumoto, K., Noda, H., Araki, H., Hanada,
H., Yamada, R., Kunimori, H., Iwata, T.: 2013, Investigation oflunar interior volatile from the state of the core and the lower mantle:
SELENE-2 VLBI-LLR proposals, Japan Geoscience Union Meeting
2013, (Chiba, Japan, May 19-24, 2013).
Sasaki. T., Yao, Y., Ohshima, N., Mikami, Y., Yoshida, M., Okada,N., Koyano, H., Sekiguchi, K., Liu, L.: 2013, A China-Japan
Collaborative Site Survey in west Tibet - Sky clearness at Gar/Ali,
Tibet -, 9th East Asian Meeting on Astronomy, (Taipei, Taiwan, Oct.
14-18, 2013).
Sato, K., Nishikawa, J., Oya, M., Horie, M., Tanaka, Y., Kumagai, S.,
Kurokawa, T., Murakami, N.: 2013, Speckle noise reduction by
focal plane wave-front sensing in high contrast imaging optics, 18th
Microoptics Conference (MOC'13), (Tokyo, Japan, Oct. 27-30, 2013).
Sato, M., Watanabe, J., Ohkawa, T.: Observation of October Draconids
2011 in Maidanak Observatory and Study of its Peak time,
Meteoroids 2013, An International Conference on Minor Bodies in
the Solar System, (Poznan, Poland, May 26-30, 2013).
Sato, M., Watanabe, J.: Forecast of Enhanced Activity of Eta-Aquariids
in 2013, Meteoroids 2013, An International Conference on Minor
Bodies in the Solar System, (Poznan, Poland, May 26-30, 2013).
Sato, S., Misawa, H., Tsuchiya, F., Obara, T., Iwai, K., Masuda, S.,
Miyoshi, Y.: 2013, Fine spectral structures of a solar radio typeII burst observed with AMATERAS, International CAWSES-II
Symposium, (Nagoya, Japan, Nov. 18-22, 2013).
Sawada, T., Hasegawa, T., Koda, J., Handa, T., Sugimoto, M.: 2013,
Structural Variation of Molecular Gas across the Galactic Spiral Arms,
Phases of the ISM, (Heidelberg, Germany, Jun. 29-Aug. 1, 2013).
Sawada, T., JAO CSV team: 2013, Commissioning New Capabilities
of ALMA, 2013 Asia-Pacific Radio Science Conference, (Taipei,
Taiwan, Sep. 3-7, 2013).
Sawada-Satoh, S., Akiyama, K., Kino, M., Nagai, H., Niinuma, K.:
2013, VERA monitoring of a blazar OJ 287, The Innermost Regions
of Relativistic Jets and Their Magnetic Fields, (Granada, Spain, Jun.

10-14, 2013).
Sawada-Satoh, S.: 2013, Apparent inward motion of the parsec-scale jet
and gamma-ray flares in OJ287 during 2011-2012, Relativistic Jets in
AGNs 2013, (Tokyo, Japan, Nov. 22, 2013).
Sawada-Satoh, S.: 2014, Apparent inward motion of the parsec-scale
jet and gamma-ray flares in OJ287 during 2011-2012, VERA-KVN
science workshop, (Kagoshima, Japan, Jan. 20-21, 2014).
Schneider, G., et al. including Guyon, O., Tamura, M.: 2014, Technology
Demonstration Milestone #1 for the EXoplanetary Circumstellar
Environments and Disk Explorer (EXCEDE) II. Science Drivers and
Implications, AAS Meeting #223, (Washington DC, USA, Jan. 5-9,2014).
Sekiguchi, K., et al. including Agata, H., Yoshida, F., Komiyama,
H.: 2013, "You Are Galileo!", Communicating Astronomy with the
Public 2013 (CAP 2013), (Warsaw, Poland, Oct. 14-18, 2013).
Sekii, T.: 2013, Helioseismic studies of the solar cycle, Mysteries of the
Solar Magnetic Field, (Warwick, UK, Sep. 4, 2013).
Sekii, T.: 2014, Recent developments in helioseismology, Image
Processing Workshop, (Mitaka, Tokyo, Japan, Jan. 7-8, 2014).
Sekimoto, Y.: 2013, Development of Millimeter-wave MKID camera
for LiteBIRD and Antarctica Dome Fuji Telescope, ASIAA seminar,(Taipei, Taiwan, May 15, 2013).
Sekimoto, Y.: 2013, Submillimeter-wave 10 kilo-pixel camera for futureradio astronomy, 2013 Asia-Pacific Radio Science Conference,(Taipei, Taiwan, Sep. 3-7, 2013).
Sekine, M., Sekimoto, Y., Noguchi, T., Miyachi A., Karatsu K., Nitta,
T., Sekiguchi, S., Naruse, M.: 2013, Yeild improvement of Nb/Al bilayer MKID camera, Asian Conference on Applied Superconductivity
and Cryogenics, (Cappadocia, Turkey, Oct. 23-25, 2013).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G. J.: 2013, Realistic
fission model and the r-process in neutron star mergers, Seventh
European Summer School on Experimental Nuclear Atrophysics,(Santa Tecla, Italy, Sep. 15-27, 2013).
Shibagaki, S., Kajino, T., Chiba, S., Mathews, G. J.: 2013, Realistic
fission model and the r-process in neutron star mergers, JUSTIPENJUSEIPEN Workshop, (Wako, Japan, Dec. 9-12, 2013).
Shibagaki, S., Kajino, T., Chiba, S., Nishimura, S., Giuseppe, L.,
Nakamura, K., Mathews, G. J., Famiano, M.: 2013, Realistic fission
model, new beta-decay half lives and the r-process in neutron starmergers, 12th International Symposium on Origin of Matter and
Evolution of Galaxies (OMEG12), (Tsukuba, Japan, Nov. 18-22, 2013).
Shibasaki, K.: 2013, Long-term Global Solar Activities Studied by the
Nobeyama Radioheliograph, Space Climate 5, (Oulu, Finland, Jun.
15-19, 2013).
Shibasaki, K.: 2013, Polar Magnetic Field and Microwave Brightening,
CESRA Workshop 2013, (Prague, Czech Republic, Jun. 24-29, 2013).
Shimojo, M.: 2013, The next functions for ALMA solar observations, EA
ALMA Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Shimojo, M.: 2013, Unusual migration of the prominence activities inrecent solar cycles, IAU Symp. 300: Nature of Prominences and theirrole in Space Weather, (Paris, France, Jun. 10-14, 2013).
Shinn, J.-H., Pyo, T.-S., Lee, J.-J., Lee, H.-G., Kim, H.-J., Koo, B.-C.,
Sung, H., Chun, M. Y., Lyo, A.-R., Moon, D.-S., Kyeong, J., Park, B.G., Hur, H., Lee, Y.-H.: 2013, Jets and Outflows from Young Stellar
Objects in the Carina Nebula Observed in [Fe II] 1.64 μm, Protostars
and Planets IV, (Heidelberg, Germany, Jul. 15-20, 2013).

Shinnaga, H.: 2013, Zeeman Observations with ALMA, EA ALMA
Development Workshop 2013, (Tokyo, Japan, Jul. 7-8, 2013).
Shinnaga, H.: 2013, Zeeman Observations with ALMA, East-Asian
ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Shino, N.: 2013, About A Relationship Of 44 GHz And 6.7 GHz CH3OH
Masers In The Massive Star Formation Regions, A Neapolitan of Masers:
Variability, Magnetism and VLBI, (Sydney, Australia, May 20-22, 2013).
Shino, N.: 2013, Proposal of the observation of 44 GHz methanol maser
using KVN+VERA, The 6th East Asia VLBI Workshop 2013, (Jeju,
Korea, Jun. 17-19, 2013).
Shinohara, I., Kojima, H., Nagai, T., Zenitani, S., Fujimoto, M.:
2013, Geotail Observation of Plasma Wave Activity at aroundthe Reconnection X lines, 12th International Workshop on theInterrelationship between Plasma Experiments in the Laboratory andin Space (IPELS2013), (Nagano, Japan, Jul. 1-5, 2013).
Shiota, D., Shimojo, M., Kaithakkal, A. J., Tsuneta, S.: 2013, Magnetic
evolution at over 70 degrees latitude during the polarity reversal, The 7th
Hinode Science Meeting, (Takayama, Gifu, Japan, Nov. 12-15, 2013).
Sôma, M.: 2014, Mistakes in the Xuanming Calendar（ 宣 明 暦 ），The
Eighth International Conference on Oriental Astronomy (ICOA-8),(University of Science and Technology of China & Anhui Museum,
China, Mar. 26-28, 2014).
Stark, C. C., et al. including Tamura, M.: 2014, HD 181327 Debris Disk
Asymmetries: Signs of a Planet or Geometric Projection Effects?,
AAS Meeting #223, (Washington DC, USA, Jan. 5-9, 2014).
Suematsu, Y.: 2013, Science Objectives and Instrument Designs of the
SOLAR-C Mission, 1st SOLARNET - 3rd EAST/ATST meeting,(Oslo, Canada, Aug. 5-8, 2013).
Suematsu, Y.: 2013, Solar Flare Kernel Observations with Integral Field
Spectroscopy in H-alpha Lineand SDO, AGU Fall Meeting 2013, (SanFrancisco, CA, USA, Dec. 9-13, 2013).
Suematsu, Y.: 2013, MgII280nm Observation - Technical Prospect, The
4th Solar-C Science Meeting, (Takayama, Gifu, Japan, Nov. 11, 2013).
Sugimoto, M.: 2013, ALMA System Performance Verification, 2013 AsiaPacific Radio Science Conference, (Taipei, Taiwan, Sep. 3-7, 2013).
Sugiyama, K., et al. including Sawada-Satoh, S., Matsumoto, N.,
Honma, M., Hirota, T.: 2013, The VLBI Monitor Project for the 6.7
GHz Methanol Masers Using the Jvn/eavn, Protostars and Planets IV,(Heidelberg, Germany, Jul. 15-20, 2013).
Sugiyama, K., Fujisawa, K., Hachisuka, K., Yonekura, Y., Motogi,
K., Sawada-Satoh, S., Matsumoto, N., Furukawa, N., Saitoh, Y.,
Hirano, D., Honma, M., Hirota, T., Niinuma, K., Murata, Y., Doi, A.,
Shen, Z.-Q., Ogawa, H.: 2013, JVN/EAVN Monitor Project for the 6.7
GHz Methanol Masers, Asia-Pacific regional URSI conference (APRASC), (Taipei, Taiwan, Sep. 3-7, 2013).
Suzuki, A.: 2013, Relativistic radiation-hydrodynamical calculations ofsupernova shock breakout, YIPQS long-term workshop, supernovae
and gamma-ray burst 2013, (Kyoto, Japan, Oct. 14-Nov.15, 2013).
Suzuki, A.: 2013, Hydrodynamical models for a successful/failed jetfrom a massive star and implications to low-luminosity GRBs,
YIPQS long-term workshop, supernovae and gamma-ray burst 2013,(Kyoto, Japan, Oct. 14-Nov.15, 2013).
Suzuki, A.: 2014, Hydrodynamical models for a successful/failed jetfrom a massive star and implications to low-luminosity GRBs,
Suzaku MAXI 2014 Expanding the Frontiers of the X-ray Universe,(Ehime, Japan, Feb. 19-22, 2014).

XIII Publications, Presentations

173

Suzuki, S., Kashiwagi, K., Tanaka, Y., Okuyama, Y., Kotani, K.,
Nishikawa, J., Suto, H., Tamura, M., Kurokawa, T.: 2013,12.5 GHz Near-IR Frequency Comb Generation Using Optical Pulse
Synthesizer for Extra-Solar Planet Finder Subaru, Nonlinear Optics
2013 (NLO 2013), (Kohala Coast, USA, Jul. 21-26, 2013).
Takahashi, R., Akutsu, T., Saito, Y., Sakamoto, N.: 2013, Optimizationof Diamond-Like Carbon (DLC) Films as Anti-Reflection Coatings,
AVS 60th International Symposium & Exhibition, (Longbeach, CA,
USA, Oct. 27-Nov. 1, 2013).
Takahashi, R.: 2013, Vibration Isolation System for KAGRA, 4th KoreaJapan Workshop on KAGRA, (Osaka, Japan, Jun. 10-11, 2013).
Takahashi, R.: 2013, Current Status of KAGRA, Beijing Gravitational
Waves Workshop, (Beijing, Chaina, Jul. 1-2, 2013).
Takami, M., SEEDS team: 2013, Vertical structures of protoplanetarydisks inferred from near-IR imaging polarimetry, The 5th Subaru
International Conference, Exoplanets and Disks: Their Formation andDiversity II, (Kona, HI, USA, Dec. 8-12, 2013).
Takiwaki, T.: 2014, Linkage between hydrodynamical instability and SN
explosion in 3D simulations, SN2NS workshop, (Paris, France, Feb. 5,2014).
Takiwaki, T.: 2014, Magnetohydrodynamic (MHD) Mechanism ofCore-Collapse Supernovae, SOKENDAI Asian Winter School 2013,(Tokyo, Japan, Nov. 11-15, 2013).
Takiwaki, T.: 2014, Linkage between hydrodynamical instability and SN
explosion observed in 3D simulations, Nuclear Astrophyics Group
Seminar, (Basel, Swithland, 2014).
Tamada, Y., Murata, T., Hattori, M., Oya, S., Hayano, Y., Kamei,
Y., Hasebe, M.: 2013, Optical Property Analyses of Plant Cell for
Adaptive Optics Microscopy, 2013 International Symposium on
Optomechatronic Technologies, (Jeju, Korea, Oct. 28-30, 2013).
Tamura, M., Kwon, J.: 2013, Near-Infrared Circular Polarization
Images of NGC 6334-V, AOGS 10th Annual Meeting, (Brisbane,
Australia, Jun. 24-28, 2013).
Tamura, M.: 2013, Exoplanets and Disks Studies with SEEDS andSteps toward TMT, "TMT Science and Instrumentation Workshop(Astronomy in the TMT Era)", (Tokyo, Japan, Oct. 16-17, 2013).
Tamura, Y., Kohno, K., Oshima, T., Inoue, S., Hirota, A., Sato, T.,
Takekoshi, T., Minamidani, T., Izumi, T., Maekawa, J., Kawabe,R., Taniguchi, A., Takahashi, S., Tatamitani, Y., Horigome, O.,
Sakai, T., Kuno, N.: 2014, (Toward) search for early afterglow
of GRBs based on new sub/mm instrumentation, The 2nd Annual
Symposium on New Developments in Astrophysics Through MultiMessenger Observations of Gravitational Wave Sources, (Tokyo,
Japan, Jan 13-15, 2014).
Tanaka, M.: 2013, Photometric redshifts with Bayesian priors on
physical properties of galaxies, Photometric redshifts for large-scale
surveys, (ASIAA, Taiwan, Sep. 4-6, 2013).
Tanaka, M.: 2013, Formation and evolution of massive early-typegalaxies, TMT Science and Instrumentation Workshop (Astronomy in
the TMT Era), (Tokyo, Japan, Oct. 16-17, 2013).
Tanaka, M.: 2013, Synergy between WISH and optical surveys from theground, WISH Science Workshop: Exploring the Darkness, (Tokyo,
Japan, Dec. 2-3, 2013).
Tanaka, M.: 2013, Optical Emission from Neutron Star Merger,
Gravitational Waves - Revolution in Astronomy and Astrophysics,(Kyoto, Japan, Jun. 2-7, 2013).

174

XIII Publications, Presentations

Tanaka, M.: 2013, Optical Transient Survey with Medium-Size
Telescopes, EACOA Medium-Size Telescope Science Workshop,(Kunming, China, Jun. 21-25, 2013).
Tanaka, M.: 2013, Time Domain Science with TMT, TMT Science
Forum, (Kona, HI, USA, Jul. 22-23, 2013).
Tanaka, M.: 2013, Radioactively Powered Emission from Neutron Star
Merger, YIPQS long-term workshop, supernovae and gamma-ray
burst 2013, (Kyoto, Japan, Oct. 14-Nov.15, 2013).
Tanaka, M.: 2013, Optical Observations of Extragalactic Supernovae,
Multi-Messengers from Core-Collapse Supernovae, (Fukuoka, Japan,
Dec. 2-6, 2013).
Tanaka, M.: 2014, Updates on photo-z's, Quasor Science with HSC:
Toward the First Results, (Taipei, Taiwan, Jan. 14-16, 2014).
Tanaka, Y., Watanabe, H., Kawate, T., Ichimoto, K., Shibasaki, K.,
Otsuji, K., Miyagosi, T.: 2013, Longitudinal structure of the polar
field reversal and decadal trend of the sunspot’s gyroresonanceemissions in 17 GHz, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Tanikawa, K., Sôma, M.: 2014, Delta T Variantions from AD 1133 to AD
1267, The Eighth International Conference on Oriental Astronomy(ICOA-8), (University of Science and Technology of China & Anhui
Museum, China, Mar. 26-28, 2014).
Tatematsu, K.: 2013, Status of ALMA Science Operation, East-Asian
ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Terai, T., Takahashi, J., Itoh, Y.: 2013, High Ecliptic Latitude Survey
for Small Main-Belt Asteroids, 45th Meeting of the Division forPlanetary Science, (Denver, USA, Oct. 6-11, 2013).
Terai, T., Yoshida, F., Urakawa, S., Abe, S., Sekiguchi, T.: 2013, Nearinfrared Spectroscopy of Ices on Trans-Neptunian Objects, TMT
Science and Instrumentation Workshop (Astronomy in the TMT Era),(Tokyo, Japan, Oct. 16-17, 2013).
Toriumi, S., Ilonidis, S., Sekii, T., Yokoyama, T.: 2013, Detection of theemerging magnetic flux beneath the visible surface of the Sun, Japan
Geophysical Union 2013, (Chiba, Japan, May 19-24, 2013).
Tsujimoto, T.: 2013, Joint stripping of SN Ia and AGB ejecta frominteracting dwarf galaxies, SCCS6 2013 Conference, Feeding,Feedback, and Fireworks: Celebrating Our Cosmic Landscape,(Hamilton Island, Australia, Jun. 24-28, 2013).
Tsujimoto, T.: 2013, Chemical evidence for joint stripping of SN Ia and
AGB ejecta from interacting dwarf galaxies, 9th Marseille Cosmology
Conference, Physical Processes of Galaxy Formation: Consensus andChallenges, (Aix-en-Provence, France, Jul. 22-26, 2013).
Uchiyama, M., Miyata, T., Sako, S., Kamizuka, T., Asano, K., Okada,K., Nakamura, T., Yamashita, T., Fujiyoshi, T., Yoshii, Y.: 2013,
Observation of Massive Star Forming Regions at 30 Microns,
Protostars and Planets IV, (Heidelberg, Germany, Jul. 15-20, 2013).
Ueno, S., et al. including Morita, S., Otsuji, K.: 2013, Report of
Cooperative Observations between Hida Observatory & Hinode
Satellite (HOP0012, 0075, 0128), The 7th Hinode Science Meeting,(Takayama, Gifu, Japan, Nov. 12-15, 2013).
Umemoto, T.: 2013, NRO Legacy Project: CO Galactic Plane Survey, EastAsian ALMA Science Workshop 2013, (Taipei, Taiwan, Sep. 2-4, 2013).
Urakawa, S., Terai, T., Sekiguchi, T., Abe, S., Yoshida, F.: 2013, HighSpatial Resolution Imaging for Small Solar System Bodies and Dwarf
Planets, TMT Science and Instrumentation Workshop (Astronomy in
the TMT Era), (Tokyo, Japan, Oct. 16-17, 2013).

Usui, F., Hasegawa, S., Muller, T. G., Yoshida, F., Terai, T., Kasuga,
T.: 2013, Mid-infrared asteroid survey: from AKARI to SPICA,
SPICA Science Conference 2013 (From exoplanet to distant galaxies:
SPICA's new window on the cool universe), (Tokyo, Japan, Jun. 1821, 2013).
Uzawa, Y., Fujii, Y., Gonzalez, A., Kaneko, K., Kroug, M., Kojima, T.,
Kuroiwa, K., Miyachi, A., Saito, S., Makise, K., Wang, Z., Asayama,
S.: 2013, Development and testing of terahertz SIS receivers by using
NbTiN for the ALMA project, IUMRS-ICAM2013, (Qingdao, China,
Sep. 22-28, 2013).
Uzawa, Y., Fujii, Y., Gonzalez, A., Kaneko, K., Kroug, M., Kojima, T.,
Kuroiwa, K., Miyachi, A., Saito, S., Makise, K., Wang, Z., Asayama,
S.: 2013, Development and testing of terahertz SIS receivers for the
ALMA project, 3rd IWFASD, (Shanghai, China, May 31, 2013).
Uzawa, Y., Fujii, Y., Gonzalez, A., Kaneko, K., Kroug, M., Kojima, T.,
Kuroiwa, K., Miyachi, A., Saito, S., Makise, K., Wang, Z., Asayama,
S.: 2013, Development and testing of the 0.78-0.95 THz SIS receivers
for the ALMA project, 2013 Asia-Pacific Radio Science Conference,(Taipei, Taiwan, Sep. 3-7, 2013).
Uzawa, Y., on behalf of Band 10 team: 2013, Band 11 Receiver
Development, EA ALMA Development Workshop 2013, (Tokyo,
Japan, Jul. 7-8, 2013).
Wada, T.: 2013, Axisymmetric Pulsar Magnetosphere with Particle
Method III: Dipole and Quadrupole magnetic field case, 4th Fermi
Asian Network (FAN) Workshop, (HongKong, China, Jul. 8-12, 2013).
Walawender, J., Guyon, O., Butterfield, M., Mery, R., Dalgleish, H.,
Morris, M.: 2013, Project Panoptes, Astronomical Data Analysis
Software & Systems, (Waikoloa, HI, USA, Sep. 29-Oct. 3, 2013).
Watanabe, J., Kasuga, T., Terai, T., Miyazaki, S., Ohta, K., Murooka, F.,
Ohnishi, T., Yamasaki, T., Mito, H., Aoki, T., Soyano, T., Tarusawa,
K., Matsunaga, N., Sako, S., Kobayashi, N., Doi, M., Enomoto, T.:2013, Faint Meteor Observation by Large-Format CMOS Sensor with
1.05-m Kiso Schmidt Telescope, Meteoroids 2013, An International
Conference on Minor Bodies in the Solar System, (Poznan, Poland,
May 26-30, 2013).
Watanabe, J., Sato, M.: Correction Effect to the Radiant Dispersion
in case of Low Velocity Meteor Showers, Meteoroids 2013, AnInternational Conference on Minor Bodies in the Solar System,(Poznan, Poland, May 26-30, 2013).
Watanabe, J., Tabe, I.: Jovian Impact Flashes and their Monitoring
Campaign, AOGS 10th Annual Meeting, (Brisbane, Australia, Jun.
24-28, 2013).
Watanabe, J., Tabe, I.: , Jovian Impact Flashes and their Implication to
Small Solar System Bodies, International Symposium on Planetary
Sciences (IAPS2013), (Shanghai, China, Jul. 1-4, 2013).
Watanabe, J.: Jovian Impact Flashes and their Implication to Meteoroids
in Outer Region of Solar System, Meteoroids 2013, An International
Conference on Minor Bodies in the Solar System, (Poznan, Poland,
May 26-30, 2013).
Watanabe, T.: 2013, Hot Reconnection Outflows Associated to an
X-class Flare, The 7th Hinode Science Meeting, (Takayama, Gifu,
Japan, Nov. 12-15, 2013).
Watanabe, T.: 2013, Solar-C Mission Proposal - Mission Goals, The 4thSolar-C Science Meeting, (Takayama, Gifu, Japan, Nov. 11, 2013).
Yabe, K., Ohta, K., Iwamuro, F., Yuma, S., Akiyama, M., Tamura, N.,

Dalton, G., Silverman, J.: 2013, The mass-metallicity relation ofstar-forming galaxies at z~1.4 revealed with Subaru/FMOS, Galaxy
Evolution over Five Decades, (Cambridge, UK, Sep. 3-6, 2013).
Yabe, K.: 2013, NIR Spectroscopy of star-forming galaxies at z~1.4 with
Subaru/FMOS, 2013 COSMOS Team Meeting, (Kyoto, Japan, May
20-24, 2013).
Yabe, K.: 2013, WISH sensitivity and survey plan, WISH Science
Workshop: Exploring the Darkness, (Tokyo, Japan, Dec. 2-3, 2013).
Yagi, M., Obara, T., Kagitani, M., Yoneda, M., Kumamoto, A., Misawa,
H., Tsuchiya, F., Iwai, K., Terada, N., Ono, T., Ohya, H.: 2013,
Database of optical and radio wave observation network of the
Tohoku University, International CAWSES-II Symposium, (Nagoya,Japan, Nov. 18-22, 2013).
Yaji, K.: 2013, Communicating Solar Observations among Amateurs,
Educators, Professionals and the Public, Communicating Astronomy
with the Public 2013 (CAP 2013), (Warsaw, Poland, Oct. 14-18, 2013).
Yaji, K.: 2013, Hinode Education and Outreach Activities in Recent
Years and in Future, The 7th Hinode Science Meeting, (Takayama,Gifu, Japan, Nov. 12-15, 2013).
Yamada, R., Matsumoto, K., Kikuchi, F., Sasaki, S.: 2013, ScientificEvaluations of the VLBI Observation on Future Lunar Explorations,
AOGS 10th Annual Meeting, (Brisbane, Australia, Jun. 24-28, 2013).
Yamada, R., Noda, H., Araki, H.: 2014, Distributions of Seismic
Moments of Deep Moonquakes and Estimation of Lunar Mantle
Structure, 45th Lunar and Planetary Science Conference, (Woodlands,
TX, USA, Mar. 17-21, 2014).
Yamada, R.: 2014, Improvement in determination accuracy of lunar interior
structure from analysis of new lunar gravity data, SELENE Symposium2014 - International Symposium of Lunar Science and Exploration using
data from Multi-Instruments -, (Tokyo, Japan, Mar. 4-5, 2014).
Yamada, Y., Gouda, N., Yoshioka, S., Hozumi, S., Nishi, R.: 2013, Kyoto
University contribution, GENIUS Kick off Meeting, (Barcelona,
Spain, Dec. 4-5, 2013).
Yamada, Y., Gouda, N., Yoshioka, S., Hozumi, S.: 2013, NanoJASMINE:
Status, news, open issues, AGIS 19, (St. Petersburg, Russia, Jun. 6-7,
2013).
Yamaguchi, M., et al. including Morita, S., Otsuji, K., Narukage, N.: 2013,
Statistical Study of Filament Eruptions and Moreton Waves Observed by
the Flare Monitoring Telescope at Hida Observatory, Kyoto University,
The 7th Hinode Science Meeting, (Takayama, Gifu, Japan, Nov. 1215, 2013).
Yamaguchi, M.: 2013, Inverse Compton emission model with theradiation from shocked Be disk in the gamma-ray binary PSR B125963, The 33rd International Cosmic Ray Conference (ICRC2013), (Riode Janeiro, Brazil, Jul. 2-9, 2013).
Yamazaki, D., Ichiki, K., Takahashi, K.: 2013, Constraint on the multilognormal magnetic field, SKA Science Workshop in East Asia 2013,(Nagoya, Japan, Jun. 5-7, 2013).
Yamazaki, D., Ichiki, K., Takahashi, K.: 2013, Constraint on the multilognormal magnetic field from the CMB, International Conference on
Cosmic Microwave Background, (Okinawa, Japan, Jun. 10-14, 2013).
Yamazaki, D., Ichiki, K., Takahashi, K.: 2013, Multi-lognormal
magnetic field limits from the cosmic microwave background, 19thInternational Symposium on Particles, Strings and Cosmology,(Taipei, Taiwan, Nov. 20-26, 2013).

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Yanagisawa, K.: 2013, Okayama Astrophysical Observatory Wide
Field Camera, EACOA Medium-Size Telescope Science Workshop,(Kunming, China, Jun. 21-25, 2013).
Yanagsawa, K., Yoshida, M., Ohta, K., Kawai, N.: 2014, Current Status
of Okayama Astrophysical Observatory Wide Field Camera, 2ndAnnula Symposium: New Developments in Astrophysics ThroughMulti-Messenger Observations of Gravitational Wave Sources ,(Tokyo, Japan, Jan. 13-15, 2014).
Yonekura, Y., Saito, Y., Mori, T., Soon, K. L., Momose, M., Yokosawa,
M., Ogawa, H., Fujisawa, K., Takaba, H., Sorai, K., Nakai, N.,
Kameno, S., Kobayashi, H., Kawaguchi, N.: 2013, Development ofa New VLBI Station: Takahagi and Hitachi 32-m Radio Telescopes in
Ibaraki Station, Asia-Pacific regional URSI conference (AP-RASC),(Taipei, Taiwan, Sep. 3-7, 2013).
Yoshida, F., Lin, E., Ip, W.-H., Chen, Y.-T.: 2013, Multi-photometricobservation of sub-km Main Belt Asteroids, 9th East Asian Meetingon Astronomy, (Taipei, Taiwan, Oct. 14-18, 2013).
Yoshida, F., Souami, D., Yagi, M.: 2013, Lightcurve Observation of Subkm Main Belt Asteroids by Subaru Telescope, AOGS 10th Annual
Meeting, (Brisbane, Australia, Jun. 24-28, 2013).
Yoshida, F., Terai, T., Ito, T., Urakawa, S., Furusyo, R.: 2013, Water inour solar system from past to future and new taxonomy of asteroids,
WISH Science Workshop: Exploring the Darkness, (Tokyo, Japan,
Dec. 2-3, 2013).
Yoshida, F.: 2013, Photometric observations of asteroids at Maidanak in
2011-2012, The 4th Maidanak Users Meeting, (Tarusa, Russia, Jul.
1-4, 2013).
Zenitani, S., Miyoshi, T.: 2013, Magnetohydrodynamic structure of aplasmoid in fast reconnection in low-beta plasmas, 11th International
School/Symposium for Space Simulations (ISSS11), (Zhongli,
Taiwan, Jul. 21-28, 2013).
Zenitani, S., Shinohara, I., Nagai, T., Wada, T.: 2013, Ion nonlinear
dynamics in magnetic reconnection, 12th International Workshop on
the Interrelationship between Plasma Experiments in the Laboratory
and in Space (IPELS2013), (Nagano, Japan, Jul. 1-5, 2013).
Zenitani, S., Shinohara, I., Nagai, T., Wada, T.: 2013, Kinetic aspects of
the ion current layer in an outflow exhaust in magnetic reconnection,
Reconnexion Physics Forum, (NASA Goddard Space Flight Center,
Online talk, Oct. 29, 2013).
Zenitani, S., Shinohara, I., Nagai, T., Wada, T.: 2013, Magnetic diffusion
and ion nonlinear dynamics in magnetic reconnection, AGU Fall
Meeting 2013, (San Francisco, CA, USA, Dec. 9-13, 2013).
Zenitani, S., Shinohara, I., Nagai, T.: 2013, Geotail observation of thedissipation region in magnetotail reconnection, 12th International
Workshop on the Interrelationship between Plasma Experiments in the
Laboratory and in Space (IPELS2013), (Nagano, Japan, Jul. 1-5, 2013).
Zenitani, S., Shinohara, I., Nagai, T.: 2013, Kinetic aspects of the ion
current layer in an outflow exhaust in magnetic reconnection, 12th Asia
Pacific Physics Conf. (APPC12), (Chiba, Japan, Jul. 14-19, 2013).
Zenitani, S.: 2013, Magnetic diffusion and ion nonlinear dynamics inmagnetic reconnection, ISAS Workshop: Magnetospheric Plasmas
2013, (Tokyo, Japan, Nov. 11-13, 2013).
Zenitani, S.: 2013, Magnetic diffusion and ion nonlinear dynamics inmagnetic reconnection, 11th International School/Symposium forSpace Simulations (ISSS11), (Zhongli, Taiwan, Jul. 21-28, 2013).
Zenitani, S.: 2014, The structure of the diffusion region in collisionless

176

XIII Publications, Presentations

reconnection: Theory, simulation, and observation, Parker Reconnection
Workshop 2014, (Sao Jose dos Campos, Brazil, Mar. 18-21, 2014).

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