Cover Caption
A large molecular cloud, Lynds 1641 in Orion, imaged by the Prime Focus Camera (Suprime-Cam) of the Subaru telescope. Many jets,
accompanied by Herbig-Haro objects, which are produced by newborn stars, were newly discovered (Reipurth et al. Astronomical Journal 140,
699, 2010).

Postscript
EditorPublisher

Printer

Publications Committee
HANAOKA, Yoichiro
UEDA, Akitoshi
OE, Masafumi
SÔMA, Mitsuru
NISHIKAWA, Jun
MIYOSHI, Makoto
YOSHIDA, Haruo
National Institutes of Natural Sciences

National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan
TEL: +81-422-34-3600
FAX: +81-422-34-3960
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FAX: +81-3-3331-2541

Annual Report of the
National Astronomical Observatory of Japan

Fiscal 2010

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Shoken MIYAMA
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National Astronomical Observatory of Japan

Preface

I Scientific Highlights April 2010 – March 2011

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II Publications, Presentations
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Refereed Publications

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Publications of the National Astronomical Observatory of Japan

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Report of the National Astronomical Observatory of Japan079

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Conference Proceedings

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Publications in English

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Annual Report of the
National Astronomical Observatory of Japan
Fiscal 2010

P R E F A C E

Shoken MIYAMA
Director General of NAOJ

We are pleased to present the Annual Report of the
National Astronomical Observatory of Japan (NAOJ) for
fiscal 2010.
On March 11, 2011, Japan was hit by the biggest
earthquake ever recorded. The earthquake and subsequenttsunami destroyed a number of houses and buildings andclaimed large number of lives (the number of people
deceased and missing has exceeded 20,000.) It is hard
to imagine the heartache and difficulty that the bereaved
families are going through. I would like to express mydeepest sympathies to the victims and their families.
Some of the NAOJ facilities were also damaged by
the earthquake including VERA antenna of the Mizusawa
VLBI Observatory in Oshu, two VLBI antennas in
Takahagi and Hitachi, and 45-m antenna in Nobeyama.
Damaged antennas will be restored with allocateddisaster restoration budget. Two NAOJ campuses in
Mizusawa and Mitaka had no serious damages, but insome rooms, books and files on the shelf fell down on
the floor. In addition to these direct damages, electricity
to the Mizusawa campus was cut for several days andemployees during the business trip were prevented fromreturning home due to paralyzed transportation network
over a few days. In the Mitaka campus too, many
employees were unable to get home on the day of theearthquake and they were forced to stay at their office or
Cosmos-Kaikan (accommodation for researchers visiting

the Mitaka Campus.) Although the earthquake caused
widespread damage in northeastern Japan, there wereno casualties among NAOJ employees, their families or
postgraduate students studying at NAOJ.
Tokyo Electric Power Company executed planned
power outage in the Kanto Region including Tokyo
for several weeks after the earthquake to make up
for the shortage of its generating capacity due to the
shutdown of the reactors at the Fukushima Daiichi
nuclear plant. To respond to the nationwide efforts tosave energy, we set up a task force to control power
consumption at the NAOJ facilities and decided to use
electricity at the Mitaka campus in the following orderof priority: (1) Development of the ALMA receivers
and HyperSuprimeCam for Subaru Telescope, which are
under development in global partnership; (2) Operationof open-use instruments; (3) Advancement of researches;and (4) Maintaining appropriate work environment (e.g.
using air conditioner). For further reduction, we requested
degraded operation of super computers that consume vast
amounts of electricity.
Having experienced a big earthquake, we becameaware of various problems of our safety procedures suchas evacuation from the building, safety confirmationof employees, and prompt setup of an emergency
headquarters. As for myself, I was in central Tokyo on
business at the time of the earthquake and could not getback to Mitaka for paralyzed traffic. We learned from

this experience that nothing is predictable in a chaotic
situation just after the disaster. To be more prepared for
emergency, we are developing new safety measures asfollows: (1) Ensuring emergency communication contact
and making plans for prompt setup of an emergency
headquarters with various cases in mind; (2) Preparing
emergency communication means such as satellite
telephone system between Mitaka and other branches(we learned that ordinary communication tools become
unavailable just after the earthquake.); (3) Building
stockpiles of blankets and emergency food for persons
unable to return home and preparing public-address
system that can be used even during power outage; (4)Establishing a backup system of valuable data for risk
diversification by making use of NAOJ facilities locatedin various places in Japan; and (5) as a future challenge,
discussing the provision of in-house power generation
system in case of a blackout.
After the nuclear accident at the Fukushima Daiichi
nuclear plant, Japan was terrified by radioactive materials
leaking from the plant. Although the NAOJ Mitaka
campus is located far from the nuclear plant (over 200 kmaway) and the radiation level does not seem so high, someof the foreign researchers left Japan for fear of radioactive
contamination. Moreover, many of the international
conferences scheduled for 2011 were cancelled, and we
had to make various arrangements for it.
In the affected Tohoku region (northeastern Japan),many postgraduate students were temporarily prevented
from studying at their universities. NAOJ provided somerooms at the Mitaka campus to support them. We willcontinuously make every effort to provide assistance forthe disaster victims.
The other sad news was the passing of three professors
emeritus at NAOJ: Masaki Morimoto in November 2010;
Shinzo Enome in March 2011; and Yasujiro Wako in
April 2011. I was really shocked by the news of theirsudden passing. They were all distinguished astronomers
and I learned a lot from them. I would like to extend
my profound gratitude to them and offer my deepest
condolences to their families.
I would not go into the details of the activities of eachproject and division here, which will be described indetail under the section of Scientific Highlights, but I’dlike to touch on the progress of ALMA that announced its
first call for proposals for Early Science Operation at theend of March 2011. Open-use observation with sixteen
12-m antennas is scheduled to start from October 2011.
Although the performance of ALMA in the Early Science
Operation phase falls far short of that in the full-scale
operation phase with fifty-four 12-m antennas and twelve
7-m antennas, ALMA already boasts the world’s highest
performance at millimeter/submillimeter wavelengths.
With the angular resolution 10 times better than Subaru or
Hubble Space Telescope, ALMA is about to explore new
astronomy. I hope ALMA will achieve unprecedented
results and contribute to the growth of young researchers
who will work all over the world.
Another event I should mention here is the 50th
anniversary of the Okayama Astrophysical Observatory(OAO). We are very pleased that the observatory has
achieved many scientific results over the past 50 years
in cooperation among a lot of people, including thoseworking in the observatory, former employees, andneighboring local municipal offices. It would be no
exaggeration to say that the scientific achievements,
technologies, and know-how of open-use operations
obtained at the OAO led to the success of Subaru
Telescope in Hawaii. The OAO is expected to play acentral role in the inter-university project that will startfrom 2012, as well as in a joint development of the 3.8-m
telescope with Kyoto University and Nagoya University.
With the upcoming completion of the 3.8-m telescope,
we are making a future plan for the OAO with a newform of installation in mind toward the realization of theThirty Meter Telescope (TMT), which is a big challenge
in the field of optical and infrared astronomy. We willcontinuously make our best effort toward high goals,
while discussing the future role of the OAO.

Shoken MIYAMA
Director General of NAOJ

I Scientific Highlights(April 2010 – March 2011)

01 Chromospheres in Metal-Poor Stars Revealed from the He I 10830 Å Line
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06
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10

The AGN–nuclear-starburst connections in a high-luminosity AGN
population
Active supermassive blackholes deeply buried in luminous infrared
galaxies, unveiled with AKARI infrared satellite
The Central Mass Distribution of the Lensing Cluster SDSS J1004+4112
Direct Measurement of Dark Halo Ellipticity with Weak Lensing
Formation of collapsing cores in subcritical magnetic clouds : threedimensional MHD simulations with ambipolar diffusion
The Primordial Origin Model of Magnetic Fields in Spiral Galaxies
Improvements in lunar gravity field modeling and orbit determination fromSELENE multi-satellite tracking data types
Parent Galaxies of Extended Emission Line Regions in the Coma Cluster
A New Hypothesis of Moscoviense Basin Formation: Double Impact
Formation

Near-infrared Imaging Circular Polarimetr y of the Orion Nebula
11 using IRSF telescope with SIRPOL and Implications for the Origin of
Homochirality
12 Origin of Molecular Outflow Determined from Thermal Dust Polarization
13 Second-order gauge-invariant cosmological perturbation theory
14 The origin and evolution of the halo PN BoBn1
A large number of z > 6 galaxies around a QSO at z = 6.43: Evidence for a
15
protocluster?
16 Subaru Lightcurve Observations of Sub-km-sized Main-belt Asteroids
Elliptically Weighted HOLICs for Weak-lensing Shear Measurement. I.
17
Definitions and Isotropic Point-spread Function Correction
18 Forty seven new T dwarfs from the UKIDSS Large Area Survey
Mass-Dependent Clustering History of K-selected Galaxies at z < 4 in
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SXDS/UDS Field
20 Development of On-site Data Analysis System for Suprime-Cam
21 RMHD Simulations of Low-Mass Star Formation Processes
Transition from a Toroidal to a Poloidal Magnetic Field in the Galactic
22
Center23 An achromatic eight-octant phase-mask coronagraph using photonic crystal
Environ ment of super massive black holes obser ved with Vir t ual
24
Observatory
25 MOIRCS Narrow-Band Survey for Distant Clusters of Galaxies
Production of High Temperature Plasmas During the Early Phases of a C9.7
26
Flare
A Deep Survey of z = 7 Lyα Emitters and Reionization with the Red27
sensitive CCDs on the Subaru Telescope Suprime-Cam
Temporal Relation between the Disappearance of Penumbral Fine-Scale
28
Structure and Evershed Flow
29 Discovery of an Excess of Hα Emitters around 4C+23.56 at z = 2.49
30 Extremely metal poor stars and Chemical Evolution in the Early Universe

TAKEDA, Y.,
TAKADA-HIDAI, M.

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IMANISHI, M. et al.

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IMANISHI, M. et al.

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OGURI, M.
OGURI, M., et al.

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KUDOH, T., BASU, S.

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SOFUE, Y., et al.

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GOOSSENS, S., et al.

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YAGI, M., et al.

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ISHIHARA, Y., et al.

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FUKUE, T., et al.

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TOMISAKA, K.
NAKAMURA, K.
OTSUKA, M., et al.

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UTSUMI, Y., et al.

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DERMAWAN, B., et al.

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OKURA, Y., FUTAMASE, T.

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ISHII, M., et al.

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FURUSAWA, J., et al.

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FURUSAWA, H., et al.
TOMIDA, K., et al.

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NISHIYAMA, S., et al.

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MURAKAMI, N., et al.

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SHIRASAKI, Y., et al.

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KOYAMA, Y., et al.

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WATANABE, T., et al.

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OTA, K., et al.

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KUBO, M., et al.

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TANAKA, I., et al.
KOMIYA, Y., et al.

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Cosmic Star Formation Activity at z = 2.2 Probed by Hα Emission LineTADAKI, K.-i., et al.
Galaxies
Neutrino-heated gamma-ray bursts
KOTAKE, K., et al.
Small-JASMINE: Current Status
YANO, T., et al.
Observation of a Binary Black Hole just before its Merger
IGUCHI, S., et al.
Photospheric Magnetic Activities triggering X-ray Microflares around a
KANO, R., et al.
Well-developed Sunspot
Evolution of a Nuclear Gas Disk and Gas Supply to the Galactic Center
NAMEKATA, D.
Subar u Telescope Detects Clues for Understanding the Origin of
HASHIMOTO, T., et al.
Mysterious Dark Gamma-Ray Bursts
Near-infrared spectroscopy of massive star-forming galaxies at z  2
ONODERA, M., et al.
Distance Measurement of Star-Forming Region IRAS 05137+3919 in Far
HONMA, M., et al.
Outer Galaxy
Connection of Super Massive Black Hole and galaxy in Active galaxy
OI, N., et al.
Neutrino oscillation and expected event rate of supernova neutrinos in
KAWAGOE, S., et al.
adiabatic explosion model
Origin of rare isotope Ta-180 in supernova-neutrino nucleosynthesis
HAYAKAWA, T., et al.
A New Type of Small-Scale Downflow Patches in Sunspot Penumbrae
KATSUKAWA, Y., JURČÁK, J.
Latest model calculation of big bang nucleosynthesis catalyzed by a longKUSAKABE, M., et al.
lived massive particle
Discriminating Planetary Migration Mechanisms by the SEEDS Project
NARITA, N., et al.
Nano-JASMINE Ready to Launch!
KOBAYASHI, Y., et al.
Performance evaluation of Nano-JASMINE telescope flight model
NIWA, Y., et al.
Inclined Orbits Prevail in Exoplanetary Systems
NARITA, N., et al.
Short Lifetime of Protoplanetary Disks in Low-metallicity Environments
YASUI, C., et al.
Direct Imaging of Fine Structures in Giant Planet Forming Regions of the
HASHIMOTO, J., et al.
Protoplanetary Disk around AB Aurigae
Imaging of a Transitional Disk Gap in Reflected Light: Indications of Planet
THALMANN, C., et al.
Formation Around the Young Solar Analog LkCa 15
Outflow in a Luminous Quasar AKARI J1757+5907
AOKI, K., et al.
Magnetic Energy Dissipation in the Outer Crust of Neutron Stars
TAKAHASHI R. H.
Constraints on the neutrino mass and the primordial magnetic field
YAMAZAKI, Dai G., et al.
A Novel Jet Model: Magnetically Collimated, Radiation-Pressure Driven
TAKEUCHI, S., et al.
Jet
Formation of Terrestrial Planets from Protoplanets under a Realistic
KOKUBO, E., GENDA, H.
Accretion Condition
N-body Simulation of Planetesimal Formation Through Gravitational
MICHIKOSHI, S., et al.
Instability of a Dust Layer in Laminar Gas Disk
Light Element Synthesis in Core-collapse Supernovae
NAKAMURA, K., et al.
Quantum Statistical Corrections to Astrophysical Photodisintegration Rates
MATHEWS, Grant J., et al.
Origin of Chirality of the Amino Acids
BOYD, Richard N., et al.
Recurrent Planet Formation and Intermittent Protostellar Outflows
MACHIDA, M., et al.
Dust and Chemical Abundances of the Sagittarius Dwarf Galaxy Planetary
OTSUKA, M., et al.
Nebula Hen2-436
Polarization Interferometric nulling coronagraph for high-contrast imaging
MURAKAMI, N., et al.
Speckle level suppression using an unbalanced nulling interferometer in a
YOKOCHI, K., et al.
high-contrast imaging system
Outburst of Comet 217P/LINEARSARUGAKU, Y., et al.

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Chromospheres in Metal-Poor Stars Revealed from the He I 10830 Å Line
(Tokai University)that two types of chromospheres exist:——(1) The rotation-dependent chromospheric activity(seen in less-aged population I stars still rotating
appreciably), for which organized magnetic fields
generated by the dynamo mechanism is responsible.
——(2) The “basal” chromosphere of the minimum
level (ubiquitously existing but detectable only in old
population II stars of very slow rotation), sustainedby nonmagnetic/ non-rotation mechanism (such as thedissipation of acoustic waves).
See [1] for more details of this study.
2.5

2

1.5

-4

-3

-2
-1
[Fe/H]

0

Figure 1: Logarithmic equivalent width (log EW) measured for the
He I 10830 line, plotted against the metallicity ([Fe/H]).
The results for 24 dwarfs (log g > 3) and 9 giants (log g< 3) are discriminated by filled (blue) and open (green)
symbols, respectively. The Sun is indicated by the large(red) filled circle.

BD +44 493

10826

He I 10830.2

The atmospheric temperature of a star like the Sun
gradually decreases with height, from T ~ 6000 K in
the photosphere down to T ~ 4000 – 5000 K at thetemperature minimum. However, as we go further
upward, the temperature begins to rise again, reaching
up to T ~ 104 K at a thin layer called “chromosphere”.
While such a temperature rise (chromospheric heating)must be caused by the transformation of some type of
extra energy into thermal energy, it is generally believedthat the dissipation of the magnetic energy in themagnetically active region may be responsible for this.
One evidence supporting this view is the fact that thechromospheric activity tends to be lower for older stars(Skumanich law), which may be reasonably interpreted
as the tendency of slower rotation for more aged stars(having suffered deceleration for a longer time), alongwith the above-mentioned scenario that magnetic fields
created by rotation-induced dynamo are the cause of thechromospheric heating.
However, this activity–age–rotation relation has been
confirmed only for comparatively young population I diskstars (with ages on the order of ~ 108–9 years), and little is
known about the existence of chromospheres in very old
metal-poor halo stars (age of ~ 1010 years). Since rotation
is likely to have almost come to rest in such old stars
because of having suffered the long-lasting deceleration
mechanism (magnetic braking), we may expect thatchromospheres do not exist in these stars.
In order to confirm this expectation, we investigatedwhether the high-excitation He I line at 10830 Å(chromospheric indicator because its visibility means
the existence of a high-temperature layer of T ~ 104 K)
is observed in 33 disk/halo stars of various metallicities(from [Fe/H] ~ +0.3 down to [Fe/H] ~ −3.7) based on thehigh-dispersion spectra (R ~ 20000) obtained on 2009
July by using IRCS+AO188 of the Subaru telescope.
We then found, rather unexpectedly, that this He I
10830 Å line is seen in absorption in almost all stars,
the strength of which is nearly constant irrespective of
the metallicity at [Fe/H] < −0.5 (cf. Figure 1). Actually,
even BD+44 493 (the most metal-poor star among oursample, which must be very old with an extremely low
metallicity of [Fe/H] = −3.7 ) clearly shows an absorption
feature of this line (Figure 2). This is an evidence thatchromospheric activity at a basal level persists even forvery old stars, despite that their rotations are considered
to be slowed down and incapable of sustaining a dynamo,
suggesting that some kind of chromospheric heating
mechanism independent of rotation/magnetism (e.g.,
acoustic heating) may take place. Accordingly, we suspect

TAKADA-HIDAI, Masahide

Si I 10827.1(NAOJ)			

log EWthis study (mÅ)

TAKEDA, Yoichi

Normalized intensity

			

0.02

10830
10834
Wavelength (Å)

Figure 2: The spectrum of BD+44 493 ([Fe/H] = −3.7) in theneighbourhood of the He I 10830 line (red symbols). The
blue solid line represents the Gaussian-fit function used
for evaluation of the equivalent width.
Reference[1] Takeda, Y., Takada-Hidai, M.: 2011, PASJ, 63, S547.

I Scientific Highlights

003

The AGN–nuclear-starburst connections
in a high-luminosity AGN population		

IMANISHI, Masatoshi

		

KAWAKATU, Nozomu(University of Tsukuba)			

Recent observations have shown that supermassive
blackholes (SMBHs) are ubiquitously present at thecenter of galaxy spheroids (bulges and elliptical galaxies)
and that the masses of SMBHs and galaxy spheroidal
stars are correlated, suggesting that SMBHs and galaxies
interact and coevolve each other.
Active Galactic Nuclei (AGNs) are the objects whichconvert gravitational energy generated through active
mass accretion onto a SMBH, to radiative energy, and areshining very brightly. SMBHs in AGNs are in a growingup phase, so that it is important to investigate theproperties of star-formation (starburst) in AGNs, in orderto understand the interplay and co-evolution of SMBHs
and stars in the universe.
To observationally tackle this issue, it is indispensable
to use an indicator with which to disentangle AGN
and starburst activity clearly. Polycyclic Aromatic
Hydrocarbons (PAH) emission features, seen in infrared
3–20 μm spectra, are detected in star-forming regions,but not in AGNs, because of the PAH destruction bystrong Xrays from AGNs. Thus, PAH emission is a goodprobe of starburst activity. Furthermore, effects of dust
extinction at infrared 3–20 μm are so small, compared
to UV and optical wavelength ranges, that starburst
luminosity is reasonably quantifiable from the observed
PAH emission.
Previous observations have indicated that in a low- tomoderate-luminosity AGN population, AGN and nuclear
starburst luminosities positively correlate, namely, massaccretion onto a SMBH is higher in an AGN accompaniedwith more luminous nuclear starburst activity. However, it
is observationally unclear whether the same relation holds
in a high-luminosity AGN population. Theoretically, twocontradictory scenarios were proposed.
(1) The mass accretion rate onto a central SMBH iscontrolled by starburst-induced viscosity, so that AGN
luminosity should increase with increasing nuclear
starburst luminosity. In this case, a similar luminosity
correlation between AGN and nuclear starburst is
expected in a high-luminosity AGN population.
(2) When nuclear starburst activity is intense, a large
amount of gas is consumed for a starburst, and thus
the remaining amount of gas accreted onto a SMBH
decreases. In this scenario, starburst activity should be
relatively weaker in a high-luminosity AGN population,compared to low- to moderate-luminosity AGNs. It was
desirable to observationally distinguish between these004

I Scientific Highlights

ICHIKAWA, Kohei, TAKEUCHI, Tomoe(NAOJ) 					(Kyoto University)

OI, Nagisa, IMASE, Keisuke(GUAS/NAOJ)

two scenarios.
We have performed infrared 3–4 μm (L-band) slit
spectroscopy of 30 PG QSOs, the representative highluminosity AGN population in the local universe, using
the IRCS infrared spectrograph attached to the Subaru
8.2 m telescope. Based on the observed luminosity of the
3.3 μm PAH emission feature, we quantitatively estimatedthe nuclear starburst luminosity in these objects andconfirmed that the AGN – nuclear-starburst luminosity
correlation holds in a wide luminosity AGN range (Figure1)[1], supporting the scenario (1).

Figure 1: The abscissa and ordinate are indicators of AGN andnuclear starburst luminosities, respectively. Stars are theresults for PG QSOs (= high-luminosity AGNs) obtainedin this work. Filled stars are objects with detectable 3.3
μm PAH emission in individual spectra. Open star isthe plot for the composite spectrum of PAH-undetectedsources in individual spectra. Open circles are the plots
for Seyfert galaxies (= low- to moderate-luminosity
AGNs) previously studied. The nuclear starburst to
AGN luminosity ratios are similar in AGNs with a wide
luminosity range.

Reference[1] Imanishi, M., et al.: 2011, PASJ, 63, S447.

Active supermassive blackholes deeply buried in luminous infrared
galaxies, unveiled with AKARI infrared satellite
		

IMANISHI, Masatoshi			

NAKAGAWA, Takao, SHIRAHATA, Mai(NAOJ) 					OHYAMA, Yoichi(ASIAA/TAIWAN)		

Luminous infrared galaxies (LIRGs) emit the bulkof their large luminosities (>1011 L ) in the infrared,
and thus must possess luminous energy sources hidden
behind dust. Most LIRGs are gas-rich mergers, and thedust obscured energy sources can be merger-induced
starburst activity (energy generation by nuclear fusion
reaction inside stars) or AGN activity (the release ofgravitational energy generated by a mass-accretingsupermassive blackhole, and conversion to radiative
energy) or the combination of the two. Since LIRGs are
the dominant galaxy population in the distant universeat z >1, in terms of the cosmic infrared radiation density,
understanding the hidden energy sources of the LIRG
population is important to uncover the history of galaxy
formation and supermassive blackhole growth in theearly universe. Distant LIRGs are generally too faint toinvestigate in detail with existing observing facilities,
so that comprehensive understanding of nearby LIRGs
continues to play an important role.
For this purpose, infrared spectroscopy at λ > 2.5 µm
is effective, because effects of dust extinction are small.
Furthermore, Polycyclic Aromatic Hydrocarbons (PAH)emission features, found in this infrared wavelength
range, can be used to distinguish between a starburst andan AGN, because the features are seen only in a starburst,
but not in an AGN (due to PAH destruction by AGN’sstrong X-ray radiation). Finally, the optical depths of dust
absorption features in this infrared wavelength range canbe used to discriminate a starburst, where stellar energy
sources and dust are spatially well-mixed, or a buried
AGN, where the energy source (= a compact massaccreting supermassive blackhole) is more centrallyconcentrated than dust.
In nearby ultraluminous infrared galaxies with LIR> 1012 L, since the compact nuclear regions (< several
100 pc) dominate the total luminosities, narrow slit
spectroscopy using infrared spectrographs attachedto ground-based large telescopes and Spitzer infrared
satellite has been widely applied to understand thephysical nature. However, for LIRGs with LIR < 1012 L,spatially-extended emission is important, so thatspectroscopy with large apertures is indispensable toquantitatively estimate the relative energetic importanceof starbursts and buried AGNs.
We have performed infrared 2.5–5 µm slitless
spectroscopy of >100 nearby LIRGs, using the IRC
infrared instrument onboard the AKARI infrared satellite,(ISAS/JAXA)ONAKA, Takashi(University of Tokyo)

and separated starburst-dominated LIRGs and buried
AGN important sources, based on infrared spectral
shapes (Figure 1). We found the trend that the energetic
importance of buried AGNs increases with increasinggalaxy infrared luminosity (Figure 2)[1,2].

Figure 1: (Left): Infrared 2.5–5 μm spectrum of a starburstdominated luminous infrared galaxy. PAH emission andhydrogen recombination lines (Brβ, Brα, Pfβ) are strong,
and the continuum slope is flat. (Right): Spectrum of aburied AGN dominated galaxy. PAH emission is very
weak, and strong dust absorption features are detected.
The continuum is red, and steeply rising with increasing
wavelength.

Figure 2: The abscissa and ordinate mean galaxy infrared
luminosity and the detection rate of a luminous buried
AGN, respectively. Buried AGNs become importantwith increasing galaxy infrared luminosity.

References[1] Imanishi, M., et al.: 2008, PASJ, 60, S489.
[2] Imanishi, M., et al.: 2010, ApJ, 721, 1233.

I Scientific Highlights

005

The Central Mass Distribution of the Lensing Cluster SDSS J1004+4112
OGURI, Masamunee(NAOJ)

The cluster SDSS J1004+4112 represents a rareexample of a quasar lensed by a massive foregroundcluster of galaxies, which was discovered in 2003 fromthe Sloan Digital Sky Survey data[1]. It consists of fiveimages of a quasar at z = 1.734 produced by a cluster at z
= 0.68. In addition, several background galaxies at z = 2–3
are also found to form multiple images (see Fig. 1).
Here we analyzed image configurations of many
multiple images and time delays between quasar images
to explore the central mass distribution of the cluster indetails[2]. For this purpose, we developed a new lensing
software called glafic, which implements the fast lensequation solver and several optimization methods toderive best-fit mass models.
Fig. 1 shows the best-fit mass model. The model
successfully reproduces all the image configurations aswell as time delays between quasar images. In the model
the center of the dark matter distribution agrees well withthe position of the central galaxy, in marked contrast
to some of previous modeling of this system in which
the offset between the dark matter center and central
galaxy has been reported. Fig. 2 indicates that the radial
mass distribution also shows an excellent agreementwith the mass distribution inferred from Chandra X-ray
observation[3].
The result suggests that the cluster is highly relaxedsystem which have formed in the early universe. In
contrast, the standard structure formation model predicts
that high-redshift clusters, as explored above, tend to beunrelaxed. The existence of such relaxed cluster alreadyat z = 0.68 therefore should be confronted with numericalsimulations.
Note that the lensing software glafic presented aboveis publicly available at
http://www.slac.stanford.edu/~oguri/glafic/

Figure 1: To p : H u b b l e S p a c e Te l e s c o p e i m a g e o f S D S S
J1004+4112, with quasar images indicated by A-E.
Bottom: Critical curves for z = 1.734 (thick) and z = 3.33
(thin) obtained for the best-fit mass model.

References[1] Inada, N., et al.: 2003, Nature, 426, 810.
[2] Oguri, M.: 2010, PASJ, 62, 1017.
[3] Ota, N., et al.: 2006, ApJ, 647, 215.

Figure 2: The radial mass distribution inferred from lensing
analysis is compared with Chandra X-ray result.

006

I Scientific Highlights

Direct Measurement of Dark Halo Ellipticity with Weak Lensing
OGURI, Masamune(NAOJ)		

TAKADA, Masahiro(University of Tokyo)		

Clusters of galaxies are the system that galaxies
are gravitationally bound thanks to the large amount ofdark matter inside the clusters. Their density structureis determined mainly by the property of unknown dark
matter particles as well as global history of the evolutionof density fluctuations. Therefore, clusters of galaxies
serve as an ideal laboratory to test the current standard
structure formation scenario. The density structure has
been well predicted by the so-called N-body simulation,
which indicates that the dark matter distribution inclusters (dark halo) is highly flattened and deviates
significantly from the simple spherical symmetric mass
distribution[1]. Its observational test is very important,as the predicted shape reflects the cold and collisionlessassumptions on dark matter particles, but the difficultylies in the unseen nature of dark matter.
We conducted detailed analysis of Subaru Suprimecam images[2] of 25 X-ray selected massive clusters
to measure the ellipticity of projected dark matter
distribution using weak lensing technique[3]. In particular
we developed a method to analyze the two-dimensional
shear map directly, without a priori assumption on thecenter of the dark matter distribution, which leads toreliable and robust measurements of the ellipticity (Fig. 1).
A challenge lies in the weakness of the lensing signals
which limits the detailed study. Here we adopt highquality
wide-field Subaru images, and combine results for 25
clusters, to detect the deviation from spherical symmetryat 7σ level (Fig. 2). The measured mean ellipticity of 〈e =0.46 ± 0.04 is in excellent agreement with 0.42 predictedby N-body simulations, which represents the first directconfirmation of the flattened dark matter distribution, an
important theoretical prediction of the current standard
model. Our result also demonstrates the feasibility of
exploring the nature of dark matter via flattening in thedark matter distribution.

OKABE, Nobuhiro(ASIAA)

SMITH, Graham P.

(University of Birmingham)

Figure 1: Subaru Suprime-cam image of Abell 2390, along withdark matter distribution inferred from weak lensing.
Weak lensing distortions, which are obtained byaveraging shapes of background galaxies, are shown by
white bars. Dark matter densities measured by the weaklensing signal are indicated by purple hue.

〈

References[1] Jing, Y. P., Suto, Y.: 2002, ApJ, 574, 538.
[2] Okabe, N., Takada, M., Umetsu, K., Futamase, T., Smith, G. P.:
2009, PASJ, 62, 811.
[3] Oguri, M., Takada, M., Okabe, N., Smith, G. P.: 2010, MNRAS,
405, 2215.

Figure 2: The likelihood distribution of average dark halo
ellipticities among the cluster sample analyzed. The
vertical solid line indicates the expected mean ellipticity
from N-body simulation predictions.

I Scientific Highlights

007Formation of collapsing cores in subcritical magnetic clouds:
three-dimensional MHD simulations with ambipolar diffusion
				

KUDOH, Takahiro(NAOJ)		

BASU, Shantanu(University of Western Ontario)

We have performed fully three-dimensional magnetohydrodynamic simulations of collapsing core formationin molecular clouds with subcritical mass-to-flux ratio,
including ambipolar diffusion[1]. Some of our major
findings are as follows.
• Core formation in subcritical clouds is generally
slow. The core develops gradually over an ambipolar
diffusion time. When the initial mass-to-flux ratio is 0.5
times a critical value, the formation time is about 3×107
years for an initial midplane number density 104 cm−3.
• The core formation time is shortened by strong velocity
fluctuations. When the average strength of the velocity
fluctuation is 3 times the sound speed, the formation
time is about 5×106 years for the same cloud describedabove.
• The core formation time scales as tcore ∝ 1/√¯ρpeak, whereρpeak is the value of the density peak during the firstcompression in the time evolution of the maximum
density.
• In the case of a highly subcritical cloud, the coreformation time does not strongly depend on the initial
mass-to-flux ratio even when there is strong velocity
fluctuation.
• Once a core forms, the density, velocity, and magnetic
field structure of the core do not strongly depend on theinitial strength of the velocity fluctuation. The infall
velocities are subsonic and the magnetic field lines
show weak hourglass shapes.
Figure 1 shows a close-up view of a core that is
obtained in this simulation. The iso-surface contour
shows the logarithmic density and the lines represent
the magnetic field. The core is located in a filamentary
structure that was induced by the initial velocity
fluctuation. The magnetic field lines show an hourglass
shaped structure because of the infall motion into thecenter of the core.
Figure 2 shows the core formation time as a functionof ρpeak, where ρpeak is defined as the value of the density
peak during the first compression in the time evolutionof the maximum density on z = 0. It shows that the coreformation time is shorter when the density peak ρpeak isgreater, and indicates that it is nearly proportional to1/√¯ρpeak. The density dependence is similar to that derived
in quasistatically contracting magnetically supported
cores, assuming a force balance of the magnetic force andgravity in the core.

008

I Scientific Highlights

Figure 1: Isosurface of the logarithmic density, and the magnetic
field lines near a core. The spatial scale is ~ 0.5pc.

Figure 2: Core formation time as a function of the density peakduring the rst compression in its time evolution (t0 
2.5 × 105 year, ρ0  4 × 1020 g cm−3). The filled and open
squares represent the results for the initial k−4 and k0
spectra, respectively. The dashed line shows that thecore formation time is nearly proportional to 1/√¯ρpeak.
The dotted line represents the free fall time of gas withdensity ρpeak for comparison.

Reference[1] Kudoh, T., Basu, S.: 2011, ApJ, 728, 123.

The Primordial Origin Model of Magnetic Fields in Spiral Galaxies
SOFUE, Yoshiaki(Meisei University / University of Tokyo)

MACHIDA, Mami

(Kyushu University)			

KUDOH, Takahiro(NAOJ)

We propose a primordial-origin model for composite
configurations of global magnetic fields in spiral galaxies(Figure 1)[1].

Figure 1: Schematic illustration of magnetic fields in spiralgalaxies, including our Galaxy.

Figure 2: Origin of S, R and V fields from a tilted lopsided
magnetic field in a rotating gaseous disk.

We show that a uniform tilted magnetic field wound
up into a rotating disk galaxy can evolve into composite
magnetic configurations comprising bisymmetric spiral(S=BSS), axisymmetric spiral (A=ASS), plane-reversed
spiral (PR), and/or ring (R) fields in the disk, and vertical(V) fields in the center (Figure 2). By MHD simulations
we show that these composite galactic fields are indeed
created from a weak primordial uniform field, and thatthe different configurations can co-exist in the same
galaxy (Figure 3). We show that spiral fields trigger
the growth of two-armed gaseous arms. The centrally
accumulated vertical fields are twisted and produce jets
toward the halo. We find that the more vertical was theinitial uniform field, the stronger is the formed magnetic
field in the galactic disk.
Reference[1] Sofue, Y., Machida, M., Kudoh, T.: 2010, PASJ, 62, 1191.

Figure 3: MHD simulation of the primordial origin model ofmagnetic field in a disk galaxy. The snap shot is taken at~ 140 My. Curves show the magnetic lines of force. Blueand green surface show the iso-surface of the density.
The initial magnetic field is uniform and its inclination
to the rotation axis is 45º. The tilted field lines arewound up to create S configuration near the disk plane
and V configuration in the central region.

I Scientific Highlights009

Improvements in lunar gravity field modeling and orbit determinationfrom SELENE multi-satellite tracking data types
GOOSSENS, Sander, MATSUMOTO, Koji, KIKUCHI, Fuyuhiko, SATO, KaoriHANADA, Hideo, ISHIHARA, Yoshiaki, NODA, Hirotomo, ARAKI, Hiroshi(NAOJ)

LIU, Qinghui, CHEN, Ming, HARADA, Yuji, KAWANO, Nobuyuki(SHAO)NAMIKI, Noriyuki(Chiba Inst. Tech.)

IWATA, Takahiro

LEMOINE, Frank, ROWLANDS, David(JAXA/ISAS)			

The launch of SELENE, which acquired the first
direct tracking data over the farside of the Moon by theuse of 4-way Doppler data between a relay satellite andthe main satellite, has resulted in a dramatic improvementof the knowledge of the global lunar gravity field[1,2].
In addition to the 4-way Doppler data, same-beamdifferential VLBI data between the two sub-satellites
and two stations on Earth were also collected using the
VERA network, and foreign stations in two international
campaigns. The strength of differential VLBI data derives
from the differencing out of common measurement errors,
resulting in a precise measurement. Together with the
SELENE 2-way and 4-way tracking data and historical
tracking data, the VLBI data were processed into a newlunar gravity field model called SGM100i[3] (Fig. 1). The
use of VLBI data allow longer arc lengths for the subsatellites, increasing the sensitivity with respect to thelower degrees of the gravity field model. The resulting
model shows a drastically improved performance in orbit
determination, especially for edge-on geometries (where
the satellite orbits over the deep farside). Correlations
with topography also show an increase over the farside.

(NASA GSFC)

laser altimeter (at points where the ground tracks ofdifferent orbits intersect, the same topography shouldbe measured), a comprehensive assessment of orbit
precision was undertaken, and it was shown that the orbit
precision of all satellites was improved when comparedto the standard case using only 2-way data. The biggest
improvements are for the main satellite during edgeon periods. Altimetry crossovers further help to obtainsmooth orbit errors (computed from overlaps) at a levelof 18 m throughout the mission[4] (Fig. 2).

Figure 2: Orbit overlap results for the SELENE main orbiter using
various tracking data types. The label “XO” stands foraltimeter crossovers.

References[1] Namiki, N., et al.: 2009, Science, 323, 900.
[2] Matsumoto, K., et al.: 2010, J. Geophys. Res., 115, E06007.
[3] Goossens, S., et al.: 2011, J. Geod., 85, 205.
[4] Goossens, S., et al.: 2011, J. Geod., in press.
Figure 1: Free-air gravity anomalies at the lunar surface for the
SGM100i model. The nearside is on the right.

SELENE was unique in the sense that it consisted ofthree satellites orbiting the Moon simultaneously, with avariety of terrestrial based tracking systems between all
the satellites: 2-way tracking for each separate satellite,
4-way between one sub-satellite and the main satellite,
and differential VLBI between the two sub-satellites.
Using all these tracking data types, and data from the010

I Scientific Highlights

Parent Galaxies of Extended Emission Line Regions in the Coma Cluster
YAGI, Masafumi, KOMIYAMA, Yutaka, KASHIKAWA, Nobunari, FURUSAWA, Hisanori(NAOJ)YOSHIDA, Michitoshi(University of Hiroshima)		

CARTER, DavidOKAMURA, Sadanori(University of Tokyo)(Liverpool John Moores University)

GRAHAM, Alister W.

MILLER, Neal A.

(Swinburne University of Technology) (University of Maryland)

MOBASHER, Bahram(University of California, Riverside)

JOGEE, Shardha(University of Texas at Austin)

We constructed a special filter for Subaru/SuprimeCam so that we can catch the Hα emission at the redshiftof the Coma cluster, and conducted a survey of the Comacluster. We discovered extended ionized hydrogen clouds
out of galaxies, and reported[1,2]. In this year, we listedsuch clouds up, and investigate the statistical features of
their parent galaxies[3]. Most of the parents are found to
be starforming or post-starburst galaxies. Their velocity
relative to the cluster is typically greater than 1000 km/s.
We also compared the samples with galaxies with an UV
asymmetry[4], which is a signature of a gas-stripping
event, and found that the UV asymmetric galaxies are
ALL included in the parent galaxies of the Hα clouds.
These results suggest that the parent galaxies once lived
out of the cluster and trapped by the gravity of the cluster.
When they fell into the cluster, the gas was stripped by
the interaction with the cluster hot gas and/or tidal forceof the cluster. In this picture, we can imagine that if aparent galaxy is less massive with less gas they will soon
lose all the gas to stop the starformation, while massive
ones will hold gas to continue starformation. Such a
correlation between the mass and the starformation is also
confirmed. Previous studies show such extended ionized
clouds in other clusters[5,6,7,8,9,10], but they are two ina cluster at most. In this study, we first reported many (14)parent galaxies in one cluster, and investigated the parents
and their spatial and velocity distribution statistically.

References[1] Yagi, M., et al.: 2007, AJ, 660, 1209.
[2] Yoshida, M., et al.: 2008, ApJ, 688, 918.
[3] Yagi, M., et al.: 2010, AJ, 140, 1814.
[4] Smith, R. J., et al.: 2010, MNRAS, 408, 1417.
[5] Gavazzi, G., et al.: 2001, ApJL, 563, L23.
[6] Yoshida, M., et al.: 2002, ApJ, 567, 118.
[7] Cortese, L., et al.: 2007, MNRAS, 376, 157.
[8] Sun, M., Donahue, M., Voit, M.: 2007, ApJ, 671, 170.
[9] Kenney, J. D. P., et al.: 2008, ApJL, 687, L69.
[10] Sun, M., et al.: 2010, ApJ, 708, 964.
Figure 1: An example of the extended ionized clouds in the Comacluster. B-band, R-band, and Coma Halpha clouds areshown as blue, green and red, respectively. The extended
ionized clouds are seen as red. The bar at bottom rightshows 10 kpc scale.

I Scientific Highlights

011

A New Hypothesis of Moscoviense Basin Formation:
Double Impact Formation
ISHIHARA, Yoshiaki(NAOJ) 			

MOROTA, Tomokatsu(ISAS/JAXA)			

NAKAMURA, Ryosuke(AIST)GOOSSENS, Sander, SASAKI, Sho(NAOJ)

Selenodetic observations of the SELENE (Kaguya)
mission provided us with globally accurate lunar gravity
model[1] and high resolution lunar shape model[2].
Using those models, lunar crustal thickness model was
also improved[3]. Recently, many studies, focused oninterior structures of lunar impact basins, are conducted.
The Moscoviense basin is a mare-filled multi-ringbasin located north-western lunar farside, and has thehighest Bouguer gravity anomaly[1] and the thinnest cruston the Moon[3]. Because of ring offset and innermost
partial ring (Figure 1), the Moscoviense basin formation
was thought as an oblique impact. Comparing with theFreundlich-Sharonov basin (normal impact origin), theMoscoviense basin has a larger mantle plug than that of

the Freundlich-Sharonov basin (Figure 1). Pre-impact
depth of the Moho and outermost-ring size of both basins
were almost the same (Figure 1), so the difference inmantle plug is probably due to the size of excavation.
However, the excavation depth of an oblique impact isshallower than that of a normal impact. The large mantle
plug of the Moscoviense basin is therefore hard to explain
by a single oblique impact. We propose a new hypothesis
for the Moscoviense basin formation, which is called“double-impact formation”[4]. This new hypothesis can
explain offset of ring structures as difference of impact
locations of first and second impact, and large mantle
plug as a result of two-times of dynamic uplift process by
first and second impact. The probability of occurence of
double impact basin is about 50% for the Moscoviensebasin case (Figure 2). This probability is not so small as
to reject a double impact origin of the Moscoviense basin.

Figure 2: Cumulative frequency of the closest distance of impact
locations for 50 random impact on the Moon. The
arrow indicates the distance between the centers of theinnermostand ourmost-ring features of the Moscoviensebasin (80 km).

Figure 1: Topography (top), Moho structure (middle), and profiles(bottom) of the Moscoviense basin (left) and theFreundlich-Sharonov basin (right).

012

I Scientific Highlights

References[1] Matsumoto, K., et al.: 2010, JGR, 115, E06007.
[2] Araki, H., et al.: 2009, Science, 323, 897.
[3] Ishihara, Y., et al.: 2009, Geophys. Res. Lett., 36, L19202.
[4] Ishihara, Y., et al.: 2011, Geophys. Res. Lett., 38, L03201.

Near-infrared Imaging Circular Polarimetry of the Orion Nebulausing IRSF telescope with SIRPOL and Implications
for the Origin of Homochirality
FUKUE, Tsubasa(NAOJ)TAMURA, Motohide

KANDORI, Ryo, KUSAKABE, Nobuhiko(NAOJ / Graduate University for Advanced Studies)			

HOUGH, James H.

(University of Hertfordshire)

BAILEY, Jeremy(University of New South Wales)

LUCAS, Philip W.

(NAOJ)

WHITTET, Douglas C. B.

(Rensselaer Polytechnic Institute)

NAKAJIMA, Yasushi, HASHIMOTO, Jun(University of Hertfordshire) 			

The origin of biomolecular homochirality is alongstanding mystery. The terrestrial living material
consists almost exclusively of one enantiomer, L-aminoacids. Amino acids in several meteorites have been foundto have enantiomeric excesses of the same handedness
as that seen in biological amino acids. Such detectionof enantiomeric excesses in meteorites is consistent
with the hypothesis that terrestrial life was seeded by
the delivery of organics from outer space during theheavy bombardment phase of early Earth. Enantiomeric
excesses can be produced by circularly polarized lightthrough asymmetric photochemistry.
We report a wide-field and deep near-infrared (Ksband: 2.14 μm) circular polarization image in the Orion
nebula, where massive stars and many low-mass stars are
forming[1]. We use SIRPOL on the IRSF 1.4 m telescopein South Africa for the polarimetry.
Our results reveal that a high circular polarization
region is spatially extended around the massive starforming region, the BN/KL nebula (Fig. 1). Significant
circular polarization extends over a region about 400
times the size of the solar system. However, other regions
show no significant circular polarization. Most of thelow-mass young stars do not show detectable extended
structure in either linear or circular polarization, in
contrast to the BN/KL nebula.
Our results and the feature of the Orion nebula implies
as follows: If our solar system formed in a massive
starforming region and was irradiated by net circularly
polarized radiation, then enantiomeric excesses could
have been induced, through asymmetric photochemistry,in the parent bodies of the meteorites and subsequently
delivered to Earth. These could then have played a role inthe development of biological homochirality on Earth.

(NAOJ)

Figure 1: This image shows the degree of circular polarization of
the Orion star-forming region. Yellow color expresses
left-handed circular polarization, where the electric
vector of light is rotated anticlockwise. Red color
expresses righthanded circular polarization. The blackbar denoted by (A) expresses about 400 times the sizeof the solar system, and the bar by (B) shows about 100
times the size of the Solar System.

Reference[1] Fukue, T., Tamura, M., Kandori, R., Kusakabe, N., Hough,J. H., Bailey, J., Whittet, D. C. B., Lucas, P. W., Nakajima,Y., Hashimoto, J.: 2010, Origins of Life and Evolution of
Biospheres, 40, 335.

I Scientific Highlights

013

Origin of Molecular Outflow Determined from Thermal Dust Polarization
TOMISAKA, Kohji(NAOJ)As the origin of molecular outflows ejected fromprotostars, there are two major explanations: magnetic
drive and entrainment. In the former, gas is magneticallydriven and forms an outflow, In the latter, an optical jet
which is ejected in the vicinity of a protostar entrains
outer molecular gas and forms the outflow.
In order to conclude the problem, it is essential toobserve the geometry of the magnetic field. We study
the expected polarization for the thermal radiation fromthe magnetically aligned dust grains in the outflow[1].
Dust grains are aligned with their major axis being
perpendicular to the magnetic field. Emission fromsuch dust grains is polarized with the B-vector being
perpendicular to the major axis. Figure 1 represents anoutflow reproduced in the axisymmetric MHD simulationof the gravitational collapse of the molecular core[2]. Thisshows that a disk forms in the perpendicular direction to
the magnetic field, which extends horizontally, and thatan outflow is ejected in perpendicular direction to thedisk.
Observing along the line-of-sight (los) specified withthe angle from the z-axis θ, the Stokes’ parameters q
and u, which represent the polarization, are calculatedwith two angles, γ (the angle between the magnetic field
and the celestial plane) and ψ (the position angle of the
projected magnetic field) as
where we perform the integration
along the los.
Figure 2 indicates the expected polarization observation. This indicates (1) the pole-on (θ = 0º: top) viewhas an axisymmetric pattern. The molecular outflow isobserved as a ring with a relatively high polarization
degree whose B-vector is toward the azimuth direction.
(2) Observing edge-on (θ = 90º: bottom), the pattern ismirror-symmetric and the disk has a higher polarization
degree than the outflow. (3) Between these two (θ = 60º:
middle), the pattern is 180º rotation-symmetry and both
the disk and the outflow have lower polarization degree.
These are characteristic for the configuration that themagnetic field has both poloidal and toroidal components.
The fact that the outflow has a toroidal magnetic
field is a direct evidence of magnetic drive. When one ofthe patterns shown above is found, this indicates there
exists the toroidal magnetic field and thus the outflow ismagnetically driven.

Figure 2: Expected distribution of the total intensity of the dust
thermal emissions (black contour), polarization degree(white contour and color), and the directions of observed
B-vector (black bar). (top) pole-on, (middle) θ = 60°,
and (bottom) edge-on.
Figure 1: Simulation of molecular outflows. Solid and dashedlines represent, respectively, the isodensity contours andthe poloidal magnetic field lines. Spatial extent is aslarge as 3000 AU × 6000 AU.

014

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References[1] Tomisaka, K.: 2002, ApJ, 575, 306.
[2] Tomisaka, K.: 2011, PASJ, 63, 147.

Second-order gauge-invariant cosmological perturbation theory
NAKAMURA, Kouji(NAOJ)

Due to the precise measurement of the Cosmic Microwave Background (CMB) by WMAP, the “precisioncosmology” has begun. The farthest region which
we can observe by electromagnetic waves is the “lastscattering surface” which corresponds to the epochof the recombination of the hydrogen atom. This lastscattering surface is observed as the CMB of 2.7 K by
us. CMB is isotropic at the zeroth-order approximation,and its fluctuations (the first-order approximation) have
the Gaussian property. Further, just now, Planck is trying
to observe non- Gaussian nature (the second-orderapproximation).
Theory of cosmology should also be developed
more precisely. Following to the above observations, itis necessary to construct the theory order by order. The
second-order approximation is established by the generalrelativistic second-order cosmological perturbation theory.
Although the some issues of this theory was alreadycompleted in 2003[1], we have made great progress by
the recent works.
In general relativity, gravity is represented by curved
spacetimes and their metric. In its perturbation
theories, we introduce two spacetime manifolds. One is
the “physical spacetime” ( ,). We want to clarify
the properties of this manifold through perturbations.
Another is the “background spacetime” (,) whichhave nothing to do with
but we introduce this as areference of perturbations. We also write the relation
betweenandby the perturbative expansion as(1)
Althoughandare distinct, through Eq. (1), we
implicitly introduce the correspondence of points onthese two manifold. This correspondence is called“gauge”. However, this correspondence is not unique
but there is the degree of freedom in the choice of thiscorrespondence due to the general covariance in thetheory. This is called the “gauge degree of freedom”. Thisgauge degree of freedom arises from the relation between
andand have nothing to do with the properties
ofitself. Therefore, this gauge degree of freedom isunphysical. In general-relativistic perturbation theory,
we have to exclude this gauge degree of freedom to
obtain physical results. One of ways to do so is “gaugeinvariant perturbation theories”. In these theories, weonly treat “gauge-invariant perturbative variables” which
are independent of the gauge degree of freedom. In linear
theories, gauge-invariant formulations have been wellstudied, however, in higher-order perturbation theories, it
was non-trivial.

In Ref. [1], we assumed that the linear metric perturbation hab is decomposed as
(2)
where
and X a are gauge-invariant and gaugedependent parts of h ab , respectively. Based on thisassumption, we showed that the second-order metricperturbation lab, the perturbation Q1 of first order, and theperturbation Q2 of the second order for an arbitrary tensor
field Q are decomposed as
(3)
(4)
(5)
Here,
, , andare gauge-invariant part of lab, (1)Q,and (2)Q, respectively. We also showed that perturbationsof the spacetime curvatures[2] and perturbations formatter fields[3] are also decomposed as Eqs. (4) and (5).
Therefore, these formulae are universal.
In the above formulation, we assumed the decomposition (2) only. Then, we confirmed this assumption
in the case of homogeneous isotropic backgrounduniverse, derived the second-order field equations, andconfirmed the consistency of these field equations[4,5.6].
Thus, we constructed the second-order gauge-invariant
cosmological perturbation theory, successfully, and it
is published as an invited review paper[7]. Finally, we
can expect the further development of this second-ordergauge-invariant perturbation thoery and comparison withobservations.

References[1] Nakamura, K.: 2003, Prog. Theor. Phys., 110, 723.
[2] Nakamura, K.: 2005, Prog. Theor. Phys., 113, 481.
[3] Nakamura, K.: 2009, Phys. Rev. D, 80, 124021.
[4] Nakamura, K.: 2006, Phys. Rev. D, 74, 101301(R).
[5] Nakamura, K.: 2007, Prog. Theor. Phys., 117, 17.
[6] Nakamura, K.: 2009, Prog. Theor. Phys., 121, 1321.
[7] Nakamura, K.: 2010, Advances in Astronomy, 2010, 576273.

I Scientific Highlights

015

The origin and evolution of the halo PN BoBn1OTSUKA, Masaaki

TAJITSU, Akito, IZUMIURA, Hideyuki(Space Telescope Science Insititute)		

Galactic halo planetary nebulae (PNe) are interesting
objects as they provide direct insight into the final
evolution of old, low-mass halo stars, and they are able toconvey important information for the study of lowmass
star evolution and the early chemical conditions of the
Galaxy. About 14 objects have been identifend as halo
members from their location and kinematics since the
PN K 648 was discovered in the globular cluster M 15.
However, in extremely metal-poor and C- and N-rich ([C,N/O]> 0, [Ar/H]< −2) halo PNe, there are unresolved
issues on chemical abundances and evolution time scales.
BoBn 1 (PN G108.4-76.1) is one of the C- and N-richand extremely metal-poor halo PNe ([C, N/O]> 1, [Ar/H]=−2.22 ± 0.09, [Fe/H]= −2.39 ± 0.14; this work).
We have performed a comprehensive chemical
abundance analysis of the extremely metal-poor halo PN
BoBn 1 based on IUE archive data, Subaru/HDS spectra,
VLT/UVES archive data, and Spitzer/IRS spectra[1]. We
have detected over 600 lines in total and calculated ionicand elemental abundances of 13 elements using detected
optical recombination lines and collisionally excited
lines. In the optical high-dispersion spectra, we detected
emission lines of fluorine and s-process elements such as
rubidium, krypton, xenon, and barium. The amounts of [F/H], [Kr/H], and [Xe/H] suggest that BoBn 1 is the mostF-rich among F-detected PNe and is a heavy s-processelement rich PN. The enhancement of C, N, and heavys-process element is comparable to carbon and s-processenhanced metal-poor (CEMP-s) stars with [Fe/H] > −2.5[2]. This suggests that BoBn1 shares a similar origin an
evolutionary history with CEMP-s stars.
We built photo-ionization model using non-LTE theoretical stellar atmosphere models to check consistency
between elemental abundances derived by empiricalmethods and from the model and to investigate theproperties of the central star, ionized nebula, and dust
in a self-consistent way to fit the IR wavelength region.
We compared the observed elemental abundances withtheoretical nucleosynthesis model predictions for single
stars and binaries with Z = 10−4. The observed elemental
abundances except for N could be explained either by a
1.5 M single star model or a binary model composed of
0.75 M + 1.5 M stars. Using theoretical evolutionary
tracks for post-AGB stars, we found that the progenitor of
the central star was perhaps a 1–1.5 M star and evolved
into a system of a white dwarf with a core mass of~0.62 M and an ~0.09 M ionized nebula. We estimatedthe dust mass of 5.8 × 10 −6 M  in the nebula, which
composes of amorphous carbon and PAHs. The presenceof carbon dust indicates that BoBn 1 has experienced the016

I Scientific Highlights(NAOJ)		

HYUNG, Siek

(Chungbuk National University)

third dredge up (TDU) during the thermal pulse AGB
phase.
The progenitor might have been initially quite N-rich.
The He-flash-driven deep mixing might be responsible
for the over-abundance of N. From careful considerationof observational results and a comparison between BoBn
1 and K 648 in M 15, we propose that the progenitor
was a binary and had experienced coalescence during
its evolution to become a C- and N-rich PN. The similar
evolutionary scenario would be also applicable to K 648[3].

Figure 1: [Xe or Ba/Ar]-[C/Ar] diagram. The [Xe/Ar] value of
BoBn 1 is upper limit. The diagram indicates that the C
and s-process elements are certainly synthesized in thesame layer and brought up to the stellar surface by the
TDU.

References[1] Otsuka, M., et al.: 2010, ApJ, 723, 658.
[2] Aoki, W., et al.: 2007, ApJ, 655, 492.
[3] Alves, D. R., et al.: 2000, AJ, 120, 2044.

A large number of z > 6 galaxies around a QSO at z = 6.43:
Evidence for a protocluster?
UTSUMI, Yousuke(The Graduate University for Advanced Studies / NAOJ)

GOTO, Tomotsugu(Institute for Astronomy, University of Hawaii / Subaru Telescope)

KASHIKAWA, Nobunari, MIYAZAKI, Satoshi, KOMIYAMA, Yutaka(The Graduate University for Advanced Studies / NAOJ)				FURUSAWA, Hisanori(NAOJ) 		

QSOs have been thought to be important for tracing
highly biased regions in the early universe, from which
the present-day massive galaxies and galaxy clusters
formed. While overdensities of star-forming galaxies
have been found around QSOs at 2 < z < 5[1,2,3], thecase for excess galaxy clustering around QSOs at z > 6 isless clear. Previous studies with HST have reported thedetection of small excesses of faint dropout galaxies insome QSO fields, but these surveys probed a relatively
small region surrounding the QSOs[4]. To overcome thisproblem, we have observed the most distant QSO at z =6.4 using the large field of view of the Suprime-Cam (34´
× 27´. Newly-installed red-sensitive fully depleted CCDs
allowed us to select Lyman break galaxies (LBG) at z ~ 6.4
more efficiently. We found seven LBGs in the QSO field,
whereas only one exists in a comparison field[5]. The
significance of this apparent excess is difficult to quantify
without spectroscopic confirmation and additional control
fields. The Poisson probability to find seven objects when
one expects four is ~10%, while the probability to findseven objects in one field and only one in the other is lessthan 0.4%, suggesting that the QSO field is significantly
overdense relative to the control field. These conclusions
are supported by a comparison with a cosmological SPH
simulation which includes the higher order clusteringof galaxies. We find some evidence that the LBGs are
distributed in a ring-like shape centered on the QSO witha radius of ~3 M pc. There are no candidate LBGs within
2 Mpc from the QSO, i.e., galaxies are clustered aroundthe QSO but appear to avoid the very center. These
results suggest that the QSO is embedded in an overdense
region when defined on a sufficiently large scale (i.e.
larger than an HST/ACS pointing). This suggests that
the QSO was indeed born in a massive halo. The central
deficit of galaxies may indicate that (1) the strong UVradiation from the QSO suppressed galaxy formation inits vicinity, or (2) that star-formation closest to the QSO
occurs mostly in an obscured mode that is missed by our
UV selection.

Roderik, Overzier(Max-Planck Institut f¨ur Astrophysik)

Figure 1: The probability distribution of how many galaxies
would be found within the field of view of Suprime-Cam
using our selection criteria. The solid histogram is basedon the simulation of galaxy formation at z = 7 while thedashed histogram is the poisson distribution assuming
the average value is (7 + 1)/2 = 4. The solid and thedashed arrows indicate the number of galaxies in the
QSO field and the SDF comparison field, respectively.

References[1] Djorgovski, S. G., et al.: 2003, ApJ, 596, 67.
[2] Miley, G. K. et al.: 2004, Nature, 427, 47.
[3] Kashikawa, N., et al.: 2007, ApJ, 663, 765.
[4] Kim, S., et al.: 2009, ApJ, 695, 809.
[5] Shimasaku, K., et al.: 2005, PASJ, 57, 447.
[6] Utsumi, Y., et al.: 2010, ApJ, 721, 1680.

I Scientific Highlights

017

Subaru Lightcurve Observations of Sub-km-sized Main-belt Asteroids
DERMAWAN, Budi

(Bandung Institute of Technology)

NAKAMURA, Tsuko(Teikyo-Heisei University)

Investigations of the spin period and shape distributions for a certain asteroid group using their lightcurve
observations are essential to understand collisional
evolution of that group. We therefore conducted
lightcurve observations of such asteroids with the Subaru
telescope + Suprime-Cam, which can detect many asteroids in a single field of view at the same time. And
from them we selected main belt asteroid (MBAs) anddetermined their spin periods and shapes. Although
about 4000 asteroids are currently listed in the spin
period catalogue, it includes a very small number of subkm-sized MBAs which are considered to be outcomesfrom the collisional evolution in the main asteroid belt.
Meanwhile, most asteroids detected by our Subaru
observation are in the size range between 0.1–1 km indiameter. Hence we would say that our observation is thefirst dedicated lightcurve observation of sub-km-sizedasteroids.
The observation was done in October 2001. We
surveyed a sky field of 34´× 27´ near opposition and theecliptic, covering a time-span of 8.3 hours for a single
night. As a result we detected 127 asteroids down to alimiting magnitude of R ≈ 24.6 mag. Among them, we
picked up 68 asteroids showing reliable spin periods.
Out of 68 asteroids, it turned out that the spin periodsof 33 asteroids are faster than 2.2 h, which are often
called fast-rotator MBAs (FRAs). The fraction of fastrotating asteroids is found to be about 48%. This is thefirst observational confirmation on the existence of FRAs
among sub-km MBAs; those detected small MBAs fill up
the region that used to be almost void of asteroids in thespin period vs size distribution (see Fig. 1)[1].
We calculated the shapes of 68 asteroids based on
their lightcurve amplitudes and then found a tendency
that FRAs are more spherical than non FRAs. Thistendency was confirmed by rigorous statistical tests[2].
Our conclusion is that most of the fast-rotators show astrong trend that they are more spherical in shape thanany other groups. Considering several timescales of theorbital and rotational evolution for small asteroids in themain asteroid belt, we showed that the above mentioned
trend is not due to coincidence but primordial. Therefore,
referring to shape distributions of impact fragments
produced in laboratory experiments, our discovered
sphericity preference of small fast-rotating asteroids
probably requires some spin deceleration mechanisms,
which selectively worked on all elongated objects during
their impact formation and/or subsequent evolution.

018

I Scientific Highlights

YOSHIDA, Fumi
(NAOJ)

Figure 1: Distribution of size vs. spin period for know asteroids(open circles and open squares) and very small asteroids
discovered (filled triangles) in this survey observation.
Asteroids being above the horizontal line of 2.2 h are
FRAs.

Figure 2: Diameter vs. lightcurve amplitude for 68 sub-kmsized
MBAs.

References[1] Dermawan, B., Nakamura, T., Yoshida, F.: 2011, PASJ, 63,
S555.
[2] Nakamura, T., Dermawan, B., Yoshida, F.: 2011, PASJ, 63,
S577.

Elliptically Weighted HOLICs for Weak-lensing Shear Measurement. I.
Definitions and Isotropic Point-spread Function Correction
			

OKURA, Yuki

(NAOJ)			

Restriction of cosmological parameters is mostimportant study of Cosmology. These cosmologicalparameters can express behavior of the universe fromearly universe to future, and because these parameters
contain the dark energy and the dark matter, thisrestriction is a one of chances to investigate them. Oneof methods of the restriction is to measure the power
spectrum of mass of large scale structure which depends
on cosmological parameters, and because gravitational
lensing are made by mass distribution, cosmologicalparamters can be restricted by measuring cosmic shear
which is made by mass distoributioin of large scale
structure.
Shear is a component of distortion by gravitational
lensing and is analyzed by weak lensing analysis method.
One of the most widely used analysis is KSB method[1]which measures quadrupole moments, defines ellipticity
by the moments and estimates shear from the ellipticity.
KSB method can obtain shear easily, but precision is nothigh by rough correction and approximation. Because
cosmic shear is especially weak, it is widely recognisedthat KSB method doesn’t have enough precision.
Therefore many new analysis methods and corrections
have been developed.
Our studies HOLICs[2] also developed new analysis
methods. HOLICs method series can obtain more precise
results by using higher order moments. KSB method has
a systematic error which is due to approximate a ellipticalweight function by a circular weight function. E-HOLICs
method can avoid the error by using the elliptical weight.
This systematic error can be estimated in simple case. If
image is simple elliptical Gaussian which has ellipticity
δ true, estimated ellipticity by KSB method δ estimate is
obtained as

FUTAMASE, Toshifumi(Tohoku University)

Figure 1: Plots of results of tests of STEP 2. The left side shows
results of the KSB method and the right side shows
results of the E-HOLICs method, with the selection
rh > 3.3 (pixels), S/N > 20, and |δ intrinsic| < 1.0. The
horizontal axis represents the value of inputted shear(answer), and the vertical axis represents the value of thedifference between estimated shear and inputted shear.
The subscripts 1 and 2 are components of directions.

KSB method. We can see the dependencies on ellipticityof these methods.
We developed E-HOLICs method which can correct
the systematic error which depends on ellipticity which
KSB method has. However , there are other manysystematic error, for example these depend on S/N. We
still must correct much systematic error for analysing
cosmic.

References[1] Kaiser, N., Squires, G., Broadhurst, T.: 1995, ApJ, 449, 460.
[2] Okura, Y., Futamase, T.: 2011, ApJ, 730, 9.
[3] Massey, R., et al.: 2007, MNRAS, 376, 13.

Therefore KSB method estimate ellipticity with overestimation. However, E-HOLICs method can obtain δtrue
without systematic error in this situation.
For verification, we tested E-HOLICs method with
“Shear TEsting Programme 2” simulation data[3], andobtain the results that KSB method has a systematic error
which depended on ellipticity and E-HOLICs method
doesn’t have the systematic error. Figure 1 shows theresult, the horizontal axis means input shear and thevertical axis means difference between estimated shear
and input shear, and left hand is plots of the result of KSB
method and right hand is plots of the result of E-HOLICs

I Scientific Highlights

019

Forty seven new T dwarfs from the UKIDSS Large Area Survey(NAOJ)				

BURNINGHAM, Ben, PINFIELD, David(University of Hertfordshire)

Observations in the 1980–90s have established thatthe conventional spectral sequence from O to M stars isfollowed by even cooler dwarf stars—Some L dwarfs andall T dwarfs (Teff <~ 1300 K) correspond to “brown dwarf”
whose mass is below 0.075 solar masses. Previous large
area surveys (e.g., 2MASS, SDSS) have discovered about
600 L dwarfs and 100 T dwarfs so far. On the other hand,a deeper large area survey is necessary to detect more andcooler (i.e., intrinsically fainter) brown dwarfs, which will
extend our understanding of star and planet formation,
both through detailed study of individual systems andthrough statistical population studies. Ongoing UKIDSS
Large Area Survey (LAS) meets the requirement. The
UKIDSS/LAS will cover 4000 sq. degrees using the
UKIRT Wide Field Camera (WFCAM), with 4 mag
deeper detection limit than 2MASS. From the resultant
data, the coolest T dwarfs and, further more, a new classof dwarfs cooler than T (Y dwarfs) are expected to befound.
The Cool Dwarf Science Working group, an international collaboration including UK and Japanese
astronomers, has developed the selection method using
UKIDSS Y JHK colors and the combination of SDSSz-J, i-z to select L/T and Y dwarf candidates. Followup
spectroscopy using large telescopes such as Subaru
and Gemini is adopted to determine their spectral types
finally. As a result, (1) we have discovered 80 T dwarfs
from 980 sq. degrees of sky, which means that the
number of known T dwarfs have been almost doubled(as of 2010)[1]; (2) the coolest star ever known has
been discovered by the UKIDSS[2] (Figure 1); (3) wehave identified spectrally peculiar objects, which may
represent hitherto unrecognised tracers of composition
and/or gravity[1] (Figure 2). We have used our sample toestimate space densities for T6-T9 dwarfs. Our analysis
suggests that the substellar mass function is declining
at lower masses, which is at odds with results for young
clusters.
After the completion of UUKIDSS/LAS, we expect
to discover Y dwarfs together with hundreds of T dwarfs,
which will shed light on the formation processes ofsubstellar objects, the Initial Mass Function (IMF) andthe formation history.

KUZUHARA, Masayuki(University of Tokyo)

and the UKIDSS Cool Dwarf Science Working Group

Figure 1: History of the coolest brown dwarf discovered: T dwarfs
discovered by UKIDSS ( ) and previous surveys ( ) areplotted against their discovery year.

□

ISHII, Miki, TAMURA, Motohide				Figure 2: Example of a peculiar spectral type (ULAS J1034).
CH4-J index implies an earlier type than that suggestedby the H20-J index.

References[1] Burningham, B., et al.: 2010, MNRAS, 406, 1885.
[2] Lucas, P. W., et al.: 2010, MNRAS, 408, 56.

020

I Scientific Highlights

Mass-Dependent Clustering History of K-selected Galaxies at z < 4in SXDS/UDS Field
FURUSAWA, Junko, SEKIGUCHI, Kazuhiro, TAKATA Tadafumi, FURUSAWA, Hisanori(NAOJ)SHIMASAKU, Kazuhiro(University of Tokyo)		

SIMPSON, Chris(Liverpool John Moores University)		

It has been a big challenge to study galaxy formationand evolution in an observational manner at the epochs
above the redshift 2, by means of star formation rate,
stellar masses, and spatial clustering of galaxies.
However, those studies suffered from observational
limits and have been performed only for paritcular galaxy
populations which are selected based on galaxy colors.
The discussions for each population were done separately
and relation among them have been uncertain. Our study
aimed at discussing the galaxy formation and evolution
across the populations by using the whole galaxy
populations which is selected by photometric redshift(photo-z).
The stellar mass of galaxies is a key parameter todescribe galaxy formation and evolution, since it isrelevant to the star formation history of galaxies. In
various surveys on different patches of the sky havebeen undertaken for this scientific driver, reaching aninteresting common view in which star formation rates
of high-mass galaxies seem to get mild and stable earlier
than those of lowmass galaxies. However, there still
remain significant differences in the amplitudes and theepoch of the active star formation among the surveys invarious mass ranges of galaxies, needing a more wideand deep observation to give a stringent clue to thosequestions.
We investigated mass-dependent galaxy evolution
based on a large sample of (~50,000) K-band selectedgalaxies in a multi-wavelength catalog of the Subaru/
XMM-Newton Deep Survey (SXDS) and the UKIRTInfrared Deep Sky Survey/Ultra Deep Survey (UDS).
This unique dataset in a contiguous deep (KAB ≤ 23.5)
and wide field covering a 10 times larger area than thosein other surveys with equivelent depths, allows us todiscuss reliable stellar mass functions and clustering ofgalaxies up to z = 4 based on a photo-z technique. In
addition, we obtained spectroscopic redshifts, especiallyfor galaxies at z > 2 with Subaru/MOIRCS, confirmingthat the accuracy of our photo-z is sufficiently good to
discuss the galaxy evolution.
Detailed discussions of the relation between stellar
masses and evolution of clustering of galaxies is a uniqueand primary result of this study. The findings include thefollowings: (1) An increase of the stellar mass density
in the universe is more rapid at z > 2 and gets relatively
smaller at the below z ~ 2. (2) Evolution of the galaxy
clustering depends on the stellar masses of galaxies,

AKIYAMA, Masayuki(Tohoku University)in which higher-mass galaxies tend to show stronger
clustering. This trend seem to apply up to z = 4 (Figure 1).
(3) Comparison between star-forming galaxy population(sBzK) and quiescent pupulation (pBzK) shows no clear
correlation in redshift and clustering strength of the two
pupulations. Post star-formation pupulations tend to havestronger clustering.

Figure 1: The redshift evolution of correlation lengths of various
types of objects. Filled symbols show our result. Dottedlines show the correlation lengths of dark haloes withfour different typical masses. Hollow symbols showcorrelation lengths of the different populations of objects(Double black circles: present-day clusters of galaxies[1]. Double light green squares: present-day luminous
early-type galaxies and Brown diamonds: EROs[2].
Purple triangles: DRGs, Blue circles: sBzKs with various
K magnitude range and Cyan crosses: LBGs[3]).

References[1] Bahcall, N. A., et al.: 2003, ApJ, 599, 814.
[2] Overzier, R.A., et al.: 2003, A&A, 405, 53.
[3] Hayashi, M., et al.: 2007, ApJ, 660, 72.

I Scientific Highlights

021

Development of On-site Data Analysis System for Suprime-Cam
FURUSAWA, Hisanori, OKURA, Yuki

		

(NAOJ)			

MINEO, Sogo

TAKATA, Tadafumi, NAKATA, Fumiaki(University of Tokyo)			

(NAOJ)TANAKA, Manobu, KATAYAMA, Nobuhiko, ITOH, Ryosuke

				

MIYAZAKI, Satoshi, KOMIYAMA, Yutaka

				
				

(NAOJ)		

UCHIDA, Tomohisa(KEK)		We develop on-site quick data analysis system for theprime-focus camera Suprime-Cam at Subaru Telescope[1]. This system is designed to assist observation withSuprime-Cam and to improve productivity of scientificoutcomes[2], by considering the following subjects:(1) Automated evaluation of data quality: In order
to assist observations, we target automation of data
evaluation during the night. In typical observations
with Suprime-Cam, data check is a burdensome task for
observers, and it was difficult to conduct sufficient data
evaluation. We consider assisting the qualitative data
evaluation at the observing site is a key to improve theproductivity of the observation. The new on-site data
analysis system performs automated data check for every
data frame, deriving qualitative information of data
quality, including seeing, median ellipticity of stellar
sources, sky-background level, and read noise level
estimated from the overscan regions. Variation of thosevalues againt time are shown on a web browser withina couple of minutes after the data acquisition. Coarse
astrometric calibration and determination of photometriczeropoint for reference fields are also performed. The
obserevers can grasp the achievement of their observation
at some point and plan the next exposures.
(2) Management of data evaluation results in database:
We also aim at efficient recording and making use of thederived data evaluation results. This system employs
database (DB) to register all the derived information
and analysis history in the data check processes. Dataframes are tagged based on thresholding values for
quality information of seeing, sky-background level,
and the number of detected sources. The observers caneasily choose data frames which satisfy requirements
by clicking a web browser only several times. Mosaicstacking analysis to check depths of data or creation offlat frames can also be applied to those particular rangeof frames upon request. The evaluation results in DB hasan advantage of making it easier to pick up necessary
data frame only in the final analysis after the observation,
which may be more useful in a large and long-term survey
programs. As a future prospect, the DB information could
contribute to construct useful data archive by adding
extra-information of the observing situation such as022

I Scientific Highlights

YASUDA, Naoki(KEK)					(University of Tokyo)

UTSUMI, Yousuke(Graduate University for Advanced Studies / NAOJ)

AIHARA, Hiroaki(University of Tokyo)

weather conditions, status of the instrument etc.
This system uses paralellized processing on multiple
PC nodes, in order to facilitate data evaluation exposure
to exposure. Analysis applications are made of in-house
C/C+/Python codes, open sources, and a commercialbased
middleware on a 64-bit Linux OS. This system has been
operated since March 2010 in Suprime-Cam observations(Figure 1). In prospective large imaging surveys with thenext-generation instrument HSC, experience in this study
will play an important role for making efficient executionof the survey and constructing a useful data archive[3].

Figure 1: A snapshot of the on-site data analysis system, whichshows a summary window for the automated data check,
web-basis result monitor, and a result of flux calibration.

References[1] Miyazaki, S., et al.: 2002, PASJ, 54, 833.
[2] Furusawa, H., et al.: 2011, PASJ, 63, S585.
[3] Furusawa, H., et al.: 2010, Proc. SPIE, 7740, 83.

RMHD Simulations of Low-Mass Star Formation Processes
TOMIDA, Kengo, TOMISAKA, Kohji(The Graduate University for Advanced Studies / NAOJ)

MACHIDA, Masahiro N., SAIGO, Kazuya

				(NAOJ)				

A first core is a transient object formed in the earlyphase of star formation. It mainly consists of molecularhydrogen and is in quasi-hydrostatic equiribrium bygas pressure and rotation. This object evolves under theaccretion from the envelope, and it begins dynamicalcollapse due to H 2 dissociation when the central
temperature exceeds about 2000 K (the second collapse).
The lifetime of a first core is short, about several thousandyrs, but it plays a critical role in star formation processes
because it is related to important phenomena such as
circumstellar disk formation, binary fragmentation,
bipolar molecular outflow, and so on. First cores havenot been observed yet since it was theoretically predicted
by Larson (1969), but recently several candidates arereported. Now, it is expected that we can observe firstcores directly by ALMA.
We performed radiation magnetohydrodynamic
simulations of star formation in a rotating magnetizedcloud core using our newly developed code[1]. We foundthat the mass, size and lifetime of the first core are 1.5–
2 times larger compared to previous simulations without
radiation transfer, due to shock and radiation heating. On
the other hand, the structure and velocity of the outflow
driven by magnetic fields do not differ significantly.
Incorporating radiation transfer is crucial to discuss thestability and observational properties of first cores.
Formation of ~1 M stars is well studied so far, but,
it is well known that there are rather larger number ofsmaller molecular cloud cores and stars. Some of first

MATSUMOTO, Tomoaki(Hosei University)

core candidates recently reported are also suggested
to be less massive, ~0.1 M. Motivated by these facts,
we investigated the evolution of the first core in a very
lowmass molecular cloud core whose mass is 0.1 Musing RHD simulations[2]. We found that the first corein the very low-mass molecular cloud core evolves
slowly under the influence of radiation cooling, and lives
significantly longer compared to fiducial 1 M cases, atleast more than 14,000 yrs. This evolution is qualitatively
different from that of typical 1 M models. This result
suggests that first cores may be more common thanprevious predictions. We calculated the observational
properties of this model, and showed that it is faint but
observable with ALMA and Herschel. We also presented
a strategy to observe such a first core and distinguish itfrom other evolutionary phases.

Figure 2: Cross-sections of first cores in 1 M(top) and 0.1 M(bottom) molecular cloud cores (left: density, right:
temperature). In the low-mass model, almost all the gas
in the cloud core quickly accretes onto the first core andthe envelope becomes very thin. The low-mass model issignificantly colder than 1 M model because of weakaccretion and efficient radiative cooling.

References[1] Tomida, K., et al.: 2010, ApJ, 714, L58.
[2] Tomida, K., et al.: 2010, ApJ, 725, L239.
Figure 1: A bipolar outflow is launched from the first core. Whitelines are magnetic field lines.

I Scientific Highlights

023

Transition from a Toroidal to a Poloidal Magnetic Fieldin the Galactic Center
NISHIYAMA, Shogo, NAGATA, Tetsuya, YISHIKAWA, Tatsuhito(Kyoto University)

TAMURA, Motohide, SUENAGA, Takuya

			

MATSUNAGA, Noriyuki, KATO, Daisuke		(University of Tokyo) 		

The detailed nature and origin of the very strong
magnetic field (MF) in the central few-hundred pc of
the Galaxy has been a subject of controversy for nearlya quarter of century, and is important in understanding
many phenomena in this region. Previous observations
have been mainly based on sub-millimeter polarimetricobservations of dense molecular clouds, or radio
observations of non-thermal radio filaments. The former
show that the MFs in dense molecular clouds runs almost
parallel to the Galactic plane, indicating a toroidal
MF[1]. By contrast, the radio filaments are aligned
nearly perpendicular to the Galactic plane, and are highlypolarized along the filaments’ long axes, suggesting alarge-scale, pervasive poloidal MF in the intercloud
medium[2].
We report observations of the Galactic center (GC)region with a wide-field near-infrared polarimeter
SIRPOL on IRSF. Near-infrared polarimetry enables
us to probe the direction of the MFs not only in thedense molecular clouds, but in the intercloud regions
toward the GC. Fig. 1 shows the MF direction (E-vectorsof polarization in the K S band) in the GC. The MF
direction has strong dependence on the Galactic latitude.
The histogram of the MF direction at | b | ≤ 0 °. 4 has aclear peak of ~90° (the direction parallel to the plane),suggesting a toroidal MF configuration in this region.
At higher Galactic latitude (| b | > 0 °. 4), the mean MF
direction appears to swing to the direction nearly
perpendicular to the Galactic plane. These results suggest
a transition of the large-scale MF configuration fromtoroidal to poloidal in the GC region, at | b | ~ 0°. 4[3,4].
Previously, the MF configuration of the GC has been
viewd as poloidal in the diffuse, interstellar (intercloud)medium, and approximately parallel to the Galactic
plane only in the dense molecular clouds. The new data
presented here shows a toroidal MF prevails at | b | < 0.°4,
even outside dense molecular clouds, which radio andsub-mm surveys show are mostly confined to within ~0.°2of the Galactic plane. Toward higher Galactic latitudes(| b | > 0°. 4), the field changes from toroidal to poloidal
configuration.

024

I Scientific Highlights

HATANO, Hirofumi, NAGAYAMA, Takahiro(NAOJ)						(Nagoya University)

HOUGH, James, H.

(University of Hertfordshire)

SUGITANI, Koji

(Nagoya City University)

Figure 1: NIR mosaic image of the Galactic center (GC) region
covering 2 °. 0 × 2 °. 0 in the Galactic coordinate, takenwith the IRSF telescope and NIR camera SIRPOL.
The three NIR bands are J (blue, 1.25 μm), H (green,
1.63 μm), and KS (red, 2.14 μm). The central-parsec starcluster of the GC is the bright yellow blob in the centerof the image. Observed E-vectors of polarization are alsoplotted with cyan bars whose length indicates the degreeof polarization. The vectors are averaged in a circle of
2 .′ 4 radius with a 3 .′ 0 grid, and plotted with thick bars
(detected with more than 3σ) and thin bars (detectedwith 2–3σ).

References[1] Novak, G., et al.: 2003, ApJ, 583, L83.
[2] Yusef-Zadeh, F., et al.: 2004, ApJS, 155, 421.
[3] Nishiyama, S., et al.: 2009, ApJ, 690, 1648.
[4] Nishiyama, S., et al.: 2010, ApJ, 722, L23.

An achromatic eight-octant phase-mask coronagraphusing photonic crystal
MURAKAMI, Naoshi		(Hokkaido University)		

TAMURA, Motohide

			(NAOJ)			

NISHIKAWA, Jun(NAOJ)

BABA, Naoshi(Hokkaido University)

For direct detection of faint exoplanets, high-contrast
imagers would be indispensable for strongly suppressing
central bright stars. In particular, extremely high contrastof 10−10 will be needed for detecting Earth-like planets.
An eight-octant phase-mask (EOPM) coronagraph is
one of promising concepts because of its high-contrast
performance, small inner working angle, and simple
optical configuration[1]. The EOPM divides a stellar
image into eight-octant sectors and provides π-phasedifference between adjacent sectors. Then a destructive
interference occurs inside pupil area on a reimaged pupil
plane, and the stellar light is totally diffracted outside
the pupil area. The diffracted stellar light is blocked
by a diaphragm called Lyot stop. On the other hand, aplanetary image, formed at an off-axis position on the
EOPM, will not be totally blocked by the Lyot stopand can be detected at a final focal plane. For detecting
extremely faint planetary signal and carrying out
spectroscopic characterizations, achromatic high-contrast
imagers will be required.
We manufactured a coronagraphic mask basedon photonic-crystal technology for realizing a fully
achromatic EOPM[2]. The photonic crystal holds
periodic nanostructure of refractive indices, and exhibits
anisotropic properties of effective dielectric constants.
The manufactured photonic-crystal mask consists of aneight-octant half-wave plates with fast axes of ± 45°.
As shown in figure 1, extremely small central defect,an order of submicron, was realized by the photoniccrystal technology. The photonic-crystal mask operates
as an fully-achromatic EOPM when the mask is placed
between two crossed polarizers with axes of 0° and 90°.
We carried out laboratory demonstration of the
EOPM coronagraph using two laser light sources withdifferent wavelengths as a simulated star (DPSS laser
with λ = 532 nm, and He-Ne laser with λ = 633 nm).
Figure 2 shows the experimental results. The light fromthe simulated star was strongly suppressed, and peak-topeak contrasts of 7 × 10−6 and 3 × 10−6 were obtained forthe DPSS and the He-Ne lasers, respectively. In a halo
region, contrasts of about 10−6 and 10−7 were obtained
for the both lasers at 3 and 13 λ/D, respectively. We
expect improved coronagraphic performance with a useof extreme adaptive optics systems, because we assume
that the residual speckle noise mainly comes from phaseaberrations of the optical components.

YOKOCHI Kaito(Tokyo University / NAOJ)

ABE, Lyu(Université de Nice-Sophia Antipolis)

Figure 1: A picture and a scanning electron microscope image of aphotonic-crystal coronagraphic mask. (manufactured by
the Photonic Lattice, Inc.)

Figure 2: Experimental results of laboratory demonstration: (left)
acquired coronagraphic images and (right) radial profilesof noncoronagraphic and coronagraphic images.

References[1] Murakami, N., et al.: 2008, PASP, 120, 1112.
[2] Murakami, N., et al.: 2010, ApJ, 714, 772.

I Scientific Highlights

025

Environment of supermassive black holes observedwith Virtual Observatory
SHIRASAKI, Yuji, OHISHI, Masatoshi, MIZUMOTO, Yoshihiko, TAKATA, Tadafumi(NAOJ)			TANAKA, Masahiro(University of Tsukuba)		

It is believed from observational evidences that mostgalaxies have a supermassive black hole at their centers.
A lot of theoretical models for the formation of thesupermassive black holes have been proposed. According
to the one of the most promising models, at first, a lot of
massive stars are formed as a result of a galaxy merger,
then intermediate-mass black holes are formed by thecollisions of these massive stars. Then the intermediatemass black holes move to the center of the galaxy, merge
with the other intermediate-mass black holes, and thenproduce a supermassive black hole. Thus it is expectedthat supermassive black holes are mostly produced atenvironment of high galaxy density. The supermassive
black hole accretes the surrounding matter and emit
strong radiation, which can be observed as an active
galactic nucleus (AGN). It is observationally found thatthe number density of AGN peaks at around redshift two,
which corresponds to the universe of ten billions years
ago, and is thought that the supermassive black holes
were produced mostly at this epoch. Thus it is expectedthat the AGNs produced in this epoch are found in theenvironment of high galaxy density. Studies of AGN
environment have been conducted by many authors byusing data obtained from large surveys such as the SDSS,
however, the redshift of observable galaxies is limited
to 0.6. To extend the study toward higher redshift use ofa large telescope is inevitable, however, it is difficult toobtain enough observation time for measuring the AGN
environment with good enough statistics.
We decided to use archive data of the Suprime-Cam
attached on the Subaru telescope to conduct the study of
AGN environment at higher redshift. Japanese Virtual
Observatory (JVO) 1 provides reduced Suprime- Cam dataand enables correlation search among dataset provided
at any VO of the world. We retrieved cutout images of
the Suprime-Cam around AGNs, measured number ofgalaxies as a function projected distance from the AGNs,
and derived cross correlation function between AGNs andgalaxies[1]. We also used UKIDSS catalog, which is dataobtained by the UKIRT infrared telescope. In this study,
about two thousands of AGNs at redshift from 0.3 to
3.0 were analyzed (Figure 1). As a result, we found thatthe high redshift AGNs reside at environment of higher
galaxy density, where it is expected that galaxy merger
happened more frequently (Figure 2).
1026

http://jvo.nao.ac.jp

I Scientific Highlights

YASUDA, Naoki(IPMU)

Figure 1: Sky distribution of AGNs analyzed in this work inequatorial coordinate.

Figure 2: Projected cross correlation function between AGNs andgalaxies.

Reference[1] Shirasaki, Y., et al.: 2011, PASJ, 63, S469.

MOIRCS Narrow-Band Survey for Distant Clusters of Galaxies
KOYAMA, Yusei(University of Tokyo)		

HAYASHI, Masao(NAOJ)		

KODAMA, Tadayuki(NAOJ)			

OKAMURA, Sadanori(University of Tokyo)		

It is well established that properties of galaxies, suchas colors and morphologies, are strongly correlated withenvironment where they reside. For example, highdensity regions such as clusters of galaxies are filledwith ellipticals or lenticulars(S0s), with little on-goingstar-formation activity[1]. However, it is still unclear
when and how this strong environmental dependence
is established. To understand what happens on galaxies
during the hierarchical assembly in the past Universe,
studying distant clusters of galaxies is critically importantsince they are in the younger stages of the present-day
clusters.
Targeting the large-scale structure around a distantgalaxy cluster, RXJ1716+6708 at z = 0.81 (hereafter
RXJ1716), identified in our previous study[2], we
performed a wide-field Hα emitter survey for this fieldusing a narrow-band filter (NB119; λc = 1.19 μm) installedon MOIRCS/Subaru, which perfectly matches to the Hαline at z = 0.81. The Hα line (λrest = 6563 Å) is one of
the best indicators of star formation activity in galaxies.
However, it shifts to near-infrared regime at z > 0.4, sothat it has been quite difficult to conduct an intensive Hαbased study for the distant Universe. We note that thisstudy is the first wide-field Hα line survey for distant(z > 0.5) clusters, and revealed the Hα-based star forming
activity along the filamentary large-scale structures forthe first time.
Our survey shows that the Hα emitters are distributed
clearly along the large-scale structure (Fig. 1). On theother hand, we also find that the Hα emitters avoid thevery central cluster region. This suggests that the star
forming activity in the cluster core has already been
completely quenched at z ~ 0.8, while in the cluster
surrounding region, a large fraction of galaxies are still
actively forming stars. This result is also consistent withthat obtained through our wide-field 15 μm imaging
campaign[3] with AKARI (see red circles in Fig. 1).
We measured star formation rates (SFR) independently from the Hα and mid-infrared (rest-frame 8 μm)
luminosities, and find that the extinction at Hα is ~1 mag
for moderately star forming galaxies, which is consistent
with local spirals. However, in the extremely dusty cases,
this value exceeds ~3 mag. These very dusty galaxies
show red colors, and some of them are on the red
sequence whose colors are consistent with those expected
for “non-star-forming” galaxies. More impor-tantly,
we find that such very dusty galaxies (probably in the

SHIMASAKU, Kazuhiro(University of Tokyo)

TANAKA, Ichi
(NAOJ)TOKOKU, Chihiro(Tohoku University)

Figure 1: Spatial distribution of the cluster member galaxies
around the RXJ1716 cluster at z = 0.81. The dashedline rectangles show our 8 FoVs of MOIRCS. Black
dots represent all the phot-z selected galaxies within ourobserved field. Blue squares, green pentagons, and filled
red circles indicate the Hα emitters, the red Hα emitters,
and the mid-infrared sources detected in our AKARI
15 μm imaging. Contours are drawn based on surface
number density of cluster member galaxies.

transitional phase under some environmental effects) aremost commonly seen in the cluster surrounding groups
or filaments, strongly supporting the importance ofthe cluster surrounding environment as a key place forshaping the environmentally-driven galaxy evolution.
Thus, taking a great advantage of the widefield capabilityof Subaru Telescope, we revealed the evidence that the
dust-obscured activities of galaxies (dusty starbursts and/or AGNs) are indeed taking place in the cluster in-fallregions, suggesting a strong link between these hidden
activity and environmental effects.

References[1] Dressler, A.: 1980, ApJ, 236, 351.
[2] Koyama, Y., et al.: 2007, MNRAS, 382, 1719.
[3] Koyama, Y., et al.: 2008, MNRAS, 391, 1758.

I Scientific Highlights

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Production of High Temperature Plasmas
During the Early Phases of a C9.7 FlareWATANABE, Tetsuya, HARA, Hirohisa

			(NAOJ)			

The early phases of a C9.7 flare on 2007 June 6 wereobserved by the EIS instrument on board the Hinodemission with an EIS study that enabled a high-cadence
raster observation over an area of 240 arcsec × 240 arcsec,
by rastering of the 1 arcsec slit utilizing scan jumps of
10 arcsecs in the heliocentric E-W direction. The timecadence of rastering was about 160 seconds[1].
Sections of raster images obtained between 17:20:09
and 17:20:29 (UT) show a few bright patches of emission
from Fe XXIII/Fe XXXIV lines at the footpoints of flaring
loops and these footpoints show dominating blue-shiftedcomponents of −(300–400) km s−1 while Fe XV/XIV lines
are nearly stationary, Fe XII lines and/or lowertemperaturelines show slightly red-shifted features, and Fe VIII, Si VII
to He II lines show ~ + 50 km s−1 redshifted components.
The density of the 1.5–2 MK plasma at these footpoints
is estimated to to be 3 × 1010 cm−3 by Fe XIII/XIV line pairsaround the maximum of the flare.
High-temperature loops connecting the footpoints
appear in the Fe XXIII/XXIV images taken over 17:22:49–
17:23:08 (UT) which is near the flare peak. Line profilesof these high-temperature lines at this flare peak timeshow only slowly-moving components. The concurrent
cooler Fe XVII line at 254.8 Å is relatively weak, indicating
the predominance of high-temperature plasma (> 107 K)
in these loops.
The rapid appearance of flaring loops in theflareline raster images can be explained by high-speed
chromospheric evaporation of ~400 km s−1. However, thisplasma might not be in ionization equilibrium, because
the relaxation time scale to reach ionization equilibrium isestimated to require more than 300 seconds, if the density
is assumed to be that in preflare; (3–4) × 109 cm−3 whichis the situation expected in the scenario of explosive
evaporation[2].

STERLING, A. C.
(MSFC/NASA)

Harra, L. K.

(MSSL/UCL)

Figure 1: Monochromatic raster images of EIS emission lines of
Fe XXIII λ263.76 (bottom panels). The EIS raster images
are constructed by using 10 arcsec jumps in the E-W
direction. The top-left panel shows a twice-expanded
image of white-square area in the Fe XXIII image (middle
panel) obtained over 17:19:10–17:21:41 (UT), in which
prominent flaring loop footpoints are denoted as A, B, C,
and D. The X-Ray Telescope (XRT) observed the flarewith Ti-poly filter at the times of 17:20:24 and 17:22:44(UT).

Figure 2: Temperature dependence of plasma motions in the initial
phases of the flare at Footpoint A of Figure 1: Negative(positive) velocities represent blue (red) line shifts in theordinate, and they are plotted against their line formation
temperatures. Line-center positions of high-speed
components are connected by dashed line.

References[1] Watanabe, T., Hara, H., Sterling, A. C., Harra, L. K.: 2010, ApJ,
719, 213.
[2] Fisher, G. H. Canfield, C. C., McClymont, A. N.: 1985, ApJ,
289, 434.

028

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A Deep Survey of z = 7 Lyα Emitters and Reionization
with the Red-sensitive CCDs on the Subaru Telescope Suprime-Cam
OTA, Kazuaki

IYE, Masanori, KASHIKAWA, Nobunari(Kyoto University)			

(NAOJ)				

TOTANI, Tomonori

KOBAYASHI, Masakazu A. R.

(Kyoto University)			

			(NAOJ)			

HARAYAMA, Atsushi, KODAKA, Natsuki(Saitama University)			

SHIMASAKU, Kazuhiro, OUCHI, Masami(University of Tokyo)

NAGASHIMA, Masahiro(Nagasaki University)

MOROKUMA, Tomoki(University of Tokyo)

FURUSAWA, Hisanori, TAJITSU, Akito, HATTORI, Takashi(NAOJ)

We conducted a deep narrowband NB973 (FWHM =200 Å centered at 9755 Å) survey of z = 7 Lyα emitters(LAEs) in the Subaru/XMM-Newton Deep Survey
Field, using the fully depleted CCDs newly installedon the Subaru Telescope Suprime-Cam, which is twice
more sensitive to z = 7 Lyα at ~1 µm than the previous
CCDs[1] (Figure 1). Reaching the depth 0.5 magnitude
deeper than our previous survey in the Subaru Deep
Field that led to the discovery of a z = 6.96 LAE[2,3], we
detected three probable z = 7 LAE candidates (Figure 2).

Figure 1: Suprime-Cam filter transmission, skylines, atmospherictransmission and quantum efficiencies of old CCDs
and new fully depleted CCDs (thin-solid, thin-dotted,
shortdashed, long-dashed and thick-solid curves,
respectively). New CCDs are twice more sensitive to z =7 Lyα at ~9730 Å.

Figure 2: The multi-waveband images of the three candidate z = 7
LAEs. They are detected only in NB973.

Even if all the candidates are real, the LAE number
density n Lyα and Lyα luminosity density ρ Lyα at z = 7

are ~7.7–54% and ~5.5–39% of those at z = 5.7 to the
Lyα line luminosity limit of L(Lyα) ~ 9.2 × 1042 erg s−1(Figure 3). This could be due to evolution of the LAE
population at these epochs as a recent galaxy evolution
model predicts that the LAE modestly evolves from z = 5.7
to 7[4]. However, even after correcting for this effect ofgalaxy evolution, nLyα and ρLyα still show deficits from z =5.7. This might reflect the attenuation of Lyα emission by
neutral hydrogen remaining at the epoch of reionizationand suggests that reionization of the universe might not
be complete yet at z = 7, supporting the possible higher
neutral fraction at the earlier epochs at z > 6 suggestedby the previous surveys of z = 5.7–7 LAEs, z ~ 6 quasars
and z > 6 γ-ray bursts.

Figure 3: Number density nLyα, Lyα luminosity density ρLyα andstar formation rate density SFRDLyα of LAEs at z = 3.1,
3.7, 4.5, 5.7, 6.6, 7 to Lyα luminosity limit 9.2×1042 erg
s−1 (See [1] for details). Horizontal errors are the redshift
range of each survey. The vertical errors include bothcosmic variance and Poisson errors. The plus symbols
with solid lines show the expected densities, when theuniverse is fully reionized, calculated by using a LAE
evolution model[4].
References[1] Ota, K., et al.: 2010, ApJ, 722, 803.
[2] Iye, M. N., et al.: 2006, Nature, 443, 186.
[3] Ota, K., et al.: 2008, ApJ, 677, 12.
[4] Kobayashi, M. A. R., et al.: 2010, ApJ, 708, 1119.

I Scientific Highlights029

Temporal Relation between the Disappearance of Penumbral
Fine-Scale Structure and Evershed Flow		

KUBO, Masahito(NAOJ)		

ICHIMOTO, Kiyoshi(Kyoto University)

LITES, Bruce W.

(High Altitude Observatory)

SHINE, Richard A.

(Lockheed Martin Solar and Astrophysics Laboratory)

Sunspot penumbrae consist of many fine-scale radial
filaments. Their fine-scale structures reflect complex
magnetic field structures in penumbrae: azimuthal
fluctuations of the penumbral magnetic field inclinationand field strength are well observed at the scale of theintensity fluctuations. A systematic outward flow called
Evershed flow is closely related to the formation of
penumbral fine-scale magnetic field structures. Evershed
flows are radial outward flows propagating along thepenumbral horizontal magnetic fields, and their origin isrising hot gas well observed in the inner penumbra.
We investigate the temporal relation between theEvershed flow, dot-like bright features (penumbral grain),the complex magnetic field structure, and dark coresalong bright filaments in a sunspot penumbra. We use
the dark core in order to trace the center of the brightfilament (Figure 1). It is believed that a pile-up of hot
plasma along the center of the bright penumbral filament
pushes up the τ = 1 surface into the upper layer, where thetemperature is lower. As a result, a dark lane (dark core)
is observed along the top of the cusp of the τ = 1 surface.
This study confirms that the appearance anddisappearance of the Evershed flow and penumbra grains
occur at nearly the same time and are associated withchanges of the inclination angle of the magnetic fieldfrom vertical to more horizontal (Figure 2)[1]. Thissuggests that both convection (penumbral grains) andhorizontal fields in the penumbra are necessary for (orcaused by) the formation of the Evershed flow. The close
correlation between the Evershed flow, convection, andmore horizontal fields supports recent models wherein
the Evershed flows are convective flows in the inclined
magnetic field lines in the penumbra.
The dark core of the bright filament also appears
coincidental with the Evershed flow. However, we findthat the dark-cored bright filament survives at least for 10–20 minutes after the disappearance of the Evershed flow.
If the Evershed flow only caused a pile-up of hot plasmaalong the bright filament, the dark core should disappear
within a cooling timescale after the end of the Evershed
flow. However, the dark core is continuously observed
without the Evershed flow for a period much longer thana cooling timescale in the photosphere. This suggests that
local heating along the bright filament of the penumbra
is important for maintaining its brightness, in addition toheat transfer by the Evershed flow.

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Figure 1: left: G-band intensity image obtained with the Solar
Optical Telescope aboard Hinode. The intensity isnormalized to the mean intensity of the quiet area
outside the sunspot. The axes represent the positions
with respect to the disk center. right: Time series ofG-band images in the white box of the left panel. The
dots with intervals of 1˝ are linearly aligned on a darkcore in the bright penumbral filament. Note that the darkcore disappears at 14:18 UT.

Figure 2: Space vs. time plots along the dotted lines in Figure 1for (a) G-band intensity, (b) Doppler velocity, and (c)magnetic field inclination. The contours represent the
Doppler velocity of −0.4 km s−1. The positive (negative)
Doppler velocities indicate a redshift (blueshift) inunits of km s−1. The magnetic field with the line-of-sightdirection is represented by the inclination angle of 0
degree.

Reference[1] Kubo, M., et al.: 2011, ApJ, 731, 84.

Discovery of an Excess of Hα Emitters around 4C+23.56 at z = 2.49
TANAKA, Ichi, KODAMA, Tadayuki

		

BREUCK, Carlos De, VENEMANS, Bram, VERNET, Joël(NAOJ)					KURK, Jaron D.

(Max-Planck-Institut für extraterrestrische Physik)

ICHIKAWA, Takashi(Tohoku University)

			

(UCL)

TANIGUCHI, Yoshiaki(Ehime University)

MATSUDA, Yuichi(University of Durham)

SEYMOUR, Nick

(European Southern Observatory)

PACKHAM, Chris(University of Florida)

STERN, Daniel(Jet Propulsion Laboratory)

1 Aim and Method
Most of massive galaxies in clusters generally show
no structure with homogeneously red color. It has beenshown from the studies of stellar populations that they areformed through the intense star-formation that happened
at z > 2, then evolved passively until today. Therefore, we
may be able to observe the site of major star-formation on
the progenitors of such massive cluster galaxies directly
if we go and find protoclusters lying at the redshifts of 2
to 4.
However, the number of known protoclusters are still
small. Especially, the number of those lying at 2 < z < 2.7
where we can observe their Hα emission from the groundis only a few. Availability of Hα emission is importantbecause it is the best tracer of the star-formation
activity. Hα emission is one of the most familiar lines
for astronomy and so it is well-calibrated through alarge number of histric studies. It is much less affectedby dust extinction compared to the UV continuum or
Lyα emission which we use to explore the very distantuniverse.
In order to find the formation site of cluster galaxies
in the act, we embarked a survey of massive star-forming
galaxies in the putative protocluster lying around theradio galaxy 4C+23.56 at z = 2.5, one of the most distantobject which we can observe the redshifted Hα from theground. We choose the field because 4C+23.56 was oncesuggested to have a possible protocluster[2,3]. To enabledetecting the redshifted Hα emission at z = 2.48, weemployed a custom-made narrowband filter and installed
it into MOIRCS instrument on Subaru Telescope.
The observation was carried out making use of theobservatory time. The field had a deep Spitzer MIPS midinfrated data in the archive. We used the MIPS 24 µm
photometry data for supplementary purpose, because itis the independent probe of the star-formation and works
even under extreme dust extinction.
2 Results
We have found 11 candidate Hα emission-line
galaxies (hereafter HAEs) to a flux limit of ~7.5 × 10−17
erg s−1 cm−2[1]. This is about 5 times more than expectedfrom the field counts. The distribution of HAEs on the

KAJISAWA, Masaru(Tohoku University / Ehime University)

ZIRM, Andrew(University of Copenhagen)

STOCKTON, Alan

(University of Hawaii)

sky is tightly confined to a 1.2-Mpc-radius area at z = 2.49.
Contrary to the usual assumption, 4C+23.56 is situatedat the western edge of the emitter distribution and not
at the center. Analysis of the MIPS 24 μm imaging also
shows that there is about 2.5 times more faint sources. All
but two of the 11 HAEs are also found in the MIPS data.
The inferred star-formation activity in the proto-clusterfrom those dataset is very high, with the median SFR a
few 100 M yr−1. What is more, most of those extreme
star-forming galaxies are quite massive ( > 1011 M). It isquite rare that we observe such intense star-formation ona number of massive galaxies in cluster core region at z <1.5. This suggests that we may be witnessing the very end
stage of massive cluster galaxy formation. The area willserve the ideal targets for science with ALMA.

Figure 1: The Hα emitters discovered around 4C+23.56 (green
objects with red open boxes). A part of the MOIRCS
FOV is shown. Reproduced from our press release at
http://subarutelescope.org (Feb 1, 2011).
References[1] Tanaka, I., et al.: 2011, PASJ, 63S, 415.
[2] Knopp, P., Chambers, C.: 1997, ApJS, 109, 367.
[3] Kajisawa, M., et al.: 2006, MNRAS, 371, 577.

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Extremely metal poor stars and Chemical Evolution
in the Early Universe
		

KOMIYA, Yutaka

SUDA, Takuma, HABE, Asao, FUJIMOTO, Masayuki(NAOJ)				

Extremely metal-poor (EMP, [Fe/H] < −2.5 in thispaper) stars are stars formed in the early universe in termsof chemical evolution. They are formed at high redshift
but are still shining with the glow of nuclear burning in
the Local Group. Hundreds of the EMP stars has been
identified in the Milky Way halo and element abundancesof these stars are revealed by follow-up spectroscopic
observations. They provide a means of probing theearliest phases of the evolution of the Milky Way andsupernovae in the early universe. Among them, two hyper
metal-poor (HMP) stars with [Fe/H] < −5 are the mostmetal deficient objects observed yet.
In our previous study[1], we give constraint on theinitial mass function (IMF) of the EMP stars and argue
that typical mass of EMP stars is ~10M. Changeover of
the IMF affects the chemical evolution of the Milky Way.
We investigate early phases of the chemical evolutionof the Galaxy and formation history of EMP stars using
hierarchical chemical evolution models. We build amerger tree of the Galaxy according to the extended
Press-Schechter theory. We follow the chemical
evolution along the tree, and compare the model results
to the metallicity distribution function (MDF) and theabundance ratio distribution of EMP stars. We also study
the feedback effect from the very massive population III
stars.
The MDF predicted by the hierarchical model with thehigh mass IMF consistent with observations[2]. Secondand later generations of stars in each dwarf primordial
galaxies distribute at [Fe/H] > −4 and stars with [Fe/H]< −4 are the first stars in mini-halos. Observational
scarcity of HMP stars indicate that the IMF of first stars
are shifted to higher mass than EMP stars. Abundance
ratio distributions predicted by the high mass IMF is also
consistent with observations[3].
We further study the effects of the surface pollution
through the accretion of interstellar matter (ISM) onto
stars along the chemical and dynamical evolution of
the Galaxy. Because of shallower potential of smaller
minihalos, the accretion of ISM in the mini-halos inwhich these stars were born is dominant. It can accountfor the surface iron abundances as observed for the HMP
stars if the cooling and concentration of gas in their birthminihalos is taken into account.

032

I Scientific Highlights(Hokkaido University)

Figure 1: Dashed and solid lines shows predicted MDF before
and after surface pollution, respectively. Dark and lightshaded histograms denote distributions of Pop. III dwarf
and giant, respectively. (This figure is reprinted from[2])Figure 2: Abundance distributions of metal poor stars. Red: Model
results. black: Observations. (This figure is reprinted from
[3])

References[1] Komiya, Y., et al.: 2007, ApJ, 658, 367.
[2] Komiya, Y., et al.: 2010, ApJ, 717, 542.
[3] Komiya, Y.: 2011, ApJ, 736, 73.

Cosmic Star Formation Activity at z = 2.2
Probed by Hα Emission Line Galaxies				

TADAKI, Ken-ichi

KODAMA, Tadayuki, HAYASHI, Masao(University of Tokyo)				

KOYAMA, Yusei(University of Tokyo)		

(NAOJ)TANAKA, Ichi
(NAOJ)

Since recent observations in optical and near-infrared
wavelength indicate that the volume-averaged starformation rate (SFR) increases from z = 0 to z ~ 1 andplateaus at z ~ 2, it is likely that a large fraction of stars ingalaxies at present-day formed at z > 1. The AGN activity
and the redshift distribution of submm galaxies (SMG)
also peak at this epoch. Therefore the redshift range of z
= 2–3 is the epoch when galaxies have the most intensive
evolution. It is absolutely imperative to build a statisticalsample of star forming galaxies at z = 2–3 in order tounderstand the cosmic star formation history and theearly evolution of galaxies.
Taking the advantage that Hα line at z = 2.19 is freefrom any strong OH sky emission line, we have made acustom-made narrow-band filter, namely, NB209 filter.
This narrow-band filter captures Hα emission from thegalaxies at z = 2.19 ± 0.02. The imaging survey has been
carried out with MOIRCS on the Subaru telescope with
the NB209 filter in GOODS-N field. The survey reached a
3σ limiting magnitude of 23.6 (NB209) which corresponds
to a 3σ limiting line flux of 2.5 × 10 −17 erg s −1 cm −2over a 56 arcmnin2 contiguous area. Also, we used the
MORICS Deep Survey (MODS) photometric catalog[1],which contains optical (UBV i´z´, near-infrared (JHKs),
mid-infrared and X-ray data. Using these dataset, wehave identified 12 Hα emitters at z = 2.2 on the basis ofnarrow-band excesses and photometric redshifts. Oneof them is likely to be a AGN because a Xray emission
is detected from this object. For the seven new emittersout of 12, including the AGN candidate, we obtained
near-infrared spectra with MOIRCS on multiobject
spectroscopy (MOS) mode. Because an emission line,
whose flux is above 3σ, is detected from all of them, it
is confirmed that our criteria is effective and robust in
selecting genuine Hα emitters at z = 2.2.
The Hα line, a hydrogen’s Balmer series line emitted
from ionized gas (i.e., HII region) around hot youngstars, is one of the best SFR indicators. It has many
great advantages; being less affected by dust extinction,
providing a survey with high sensitivity, and having been
well calibrated in the local Universe. We have estimatedstar formation rates (SFR) and stellar masses (Mstar) for
individual galaxies from Hα flux and Ks-band magnitude.
The average SFR and Mstar is 27.8 M    yr−1 and 4.0 × 1010
M, respectively.
The evolution of galaxies depends strongly on theenvironment. Because field galaxies are antithetical to

TOKOKU, Chihiro(Tohoku University)

cluster galaxies in terms of environment, we can directly
examine the environmental dependence of star formation
activity by comparing the properties of emitters among
different environments. In addition to the present generalfield survey, we have estimated SFRs and stellar masses
for a large sample of star forming galaxies both in clusters
and in the other general field at various redshifts. Figure
1 indicates that the evolution of star formation activities
both in the fields and in the clusters. We find that the starformation activity is reduced rapidly from z = 2.5 to z =0.8 in the cluster environment, while it is only moderatelychanged in the field environment. This result suggeststhat the timescale of galaxy formation is different among
different environments, and the star forming activities inhigh density regions eventually overtake those in lower
density regions as a consequence of “galaxy formationbias” at high redshifts.

Figure 1: The evolution of star formation activities of the line
emitting galaxies. Filled circles and open circles indicate
Hα emitters and [OII] emitters, respectively.

Reference[1] Kajisawa, M., et al.: 2011, PASJ, 63S, 379.

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033

Neutrino-heated gamma-ray bursts
KOTAKE, Kei, HARIKAE, Seiji, TAKIWAKI, Tomoya(NAOJ)

Gamma-ray bursts (GRBs) have long attracted
the attention of astrophysicists since their accidental
discovery in 1970s. Regarding the long-duration GRBs,
there have been accumulating observations identifying a
massive stellar collapse as their origin. For their central
engines, the so-called collapsar has received quite someinterest for more than decade.
In the collapsar scenario, the central cores withsignificant angular momentum collapse into a black hole.
Neutrinos emitted from the accretion disk heat matterin the polar funnel region to launch the GRB outflows.
Paczynski (1990) pioneerlingly proposed that the energy
deposition proceeds predominantly via neutrino andantineutrino annihilation into electron and positron (e.g.,ν+ ν̄ → e − + e +, hereafter “neutrino pair annihilation”).
There have been only a few studies pursuing thepossibility of generating jets by the energy deposition
via neutrino pair annihilation. This is mainly because
the neutrino emission from the accretion disk generally
becomes highly aspherical, thus demanding us to solve a
multidimensional neutrino transfer problem.
We have presented a numerical code and scheme forcalculating the deposition of energy and momentum via
neutrino pair annihilation in a Kerr spacetime, in which
we solve the general relativistic radiative equation along
the null geodesics[1]. The charged-current β-processes
are taken into account, which are dominant in the vicinityof the accretion tori. With these improvements, the newly
developed code would provide a more realistic estimationof the annihilation rates than before.
As for the hydrodynamic data (such as density,
electron fraction, and entropy), we take the ones at 9.1
s after the onset of gravitational collapse for model J0.8
(Figure 1, left panel), which show a clear accretiondisk and BH system with the polar funnel regions along
the spin axis of the disk. The position of the innerboundary of the computational domain is set to be 4 M,which mimics the event horizon of the BH. We set theKerr parameter a* = 0.999 to mimick the extreme Kerr
geometry.
To trigger the neutrino-heating explosion, theneutrino-heating timescale should be smaller than theadvection timescale, which is characterised by thefreefall timescale in the polar funnel regions (e.g., [2]).
This condition is akin to the condition of the successful
neutrino-driven explosion in the case of core-collapse
supernovae.
The right panel of Figure 1 depicts the ratio ofthe dynamical τ dyn to the heating timescales τ heat foran extreme Kerr geometry, showing that the ratio

034

I Scientific Highlights

becomes greater than unity in the polar funnel regions.
This indicates the possible formation of the neutrinodriven outflows there, if coupled to the collapsar’shydrodynamics. Our obtained results here suggest theneutrino pair annihilation has a potential importanceequal to the conventional magnetohydrodynamic
mechanism for igniting the GRB fireballs.

Figure 1: Left panel shows hydrodynamic configuration employedin the ray-tracing calculation. This is the snapshot at
9.1 s after the onset of gravitational collapse for model
J0.8 when the accretion disk is in a stationary state(see [3] for more detail). The logarithmic density (ing cm−3, left-half) and temperature (in K, right-half) are
shown. The white solid line denotes the area where thedensity is equal to 1011 g cm−3, representing the surfaceof the accretion disk. The central black circle (≈ 4 M)
represents the inner boundary of our computations Rightpanel is τdyn/τheat (:the dynamical timescale τdyn versus
the heating timescale τheat) in an extreme Kerr geometry(left).

References[1] Harikae, S., Kotake, K., Takiwaki, T., Sekiguchi, Y.-i.: 2010,
ApJ, 720, 614.
[2] Kotake, K., Sato, K., Takahashi, K.: 2006, Reports of Progress
in Physics, 69, 971.
[3] Harikae, S., Kotake, K., Takiwaki, T.: 2010, ApJ, 713, 304.

Small-JASMINE: Current Status
YANO, Taihei, GOUDA, Naoteru, KOBAYASHI, Yukiyasu, TSUJIMOTO, Takuji
HASTUTORI, Yoichi, TAMURA, Tomonori(NAOJ)YAMADA, Yoshiyuki(Kyoto University)		

				

FUJIWARA, Ken, KOYANAGI, Jun

YASUDA, Susumu, UTSUNOMIYA, Shin

(ISAS/JAXA)				

NIWA, Yoshito(University of Tokyo)

We have been investigating the validity of satellite
system of Small-JASMINE. There is no fatal problem
in the system at this present stage. We have changed theobservational wave-length from K-band to H-band in2010 in order to remove the refrigerator because it is too
expensive. Accordingly we now investigate mainly thefollowing points for the system.
◦ Cooling system using Peltier device◦ Attitude of the satellite◦ Baffle of the telescope
In addition to the above issues, we have picked up
the following three important issues in order to achieve
the aim of Small-JASMINE project[1]. (A) SmallJASMINE is required to measure the positions of stars
with high accuracy from the huge amount of data during
the observational period. (B) The high stabilization of thethermal environment in the telescope is required. (C) The
attitude-pointing stability of these satellites with subpixel
accuracy is also required. Here we concentrate on thesethree issues.
1 Measuring the positions of stars with high accuracy
Determination of positions of star images on a
detector with high precision is very important. We willshow the laboratory experiment that we can determine
the positions of star images on the detector with highprecision.
In order to accomplish such a precision, we take thefollowing two procedures. (1) We determine the positionsof star images on the detector with the precision of about
0.01 pixel for one measurement, using an algorithm forestimating them from photon weighted means of the star
images. (2) We determine the positions of star images
with the precision of about 0.0001–0.00001 pixel, whichcorresponds to that of 10 micro-arcsec, using a large
amount of data over 100000 measurements. We havealready shown the validity of the procedure (1). For theprocedure (2), we have shown the expected accuracy of
positions of stars using 100000 data by now.

(JAXA)JASMINE-WG

In order to accomplish a measurement of positionsof stars with high accuracy, we must make a modelof the distortion of the image on the focal plane withthe accuracy of less than 0.1nm. We have investigatednumerically that the above requirement is achieved if thethermal variation is within about 1 K /0.75h. We haveinvestigated the validity of the following algorithm inorder to determine the positions of stars.
◦ Distortions of the image of the first and second order are
solved from the observational data of adjacent images.
◦ The displacement of higher order (higher than thirdorder) is small enough to neglect.
We examine the thermal structure analysis and obtain
the distortion of images on the focal plane. Then we
calculate the displacement of each order.
We have ascertained that more than third orderdisplacement is less than the required value of 0.1 nm.
Then, our algorithm will work well.
3 The attitude-pointing stability of the satellite
We need high precision attitude-pointing stability
with sub-pixel accuracy. Then, we develop a Tip-tilt
mirror (TTM) servo system in order to achieve a pointing
stability with an accuracy of 190 mas/7 sec. We use star
images for correction of pointing error. Now we prepare
for experiment of TTM servo system.

Reference[1] Yano, T., et al.: 2011, EAS Publications Series, 45, 449-452.

2 The high stabilization of the thermal environment
Image on a detector is distorted if the telescope
expands or shrinks by the variation of the thermal
environment.

I Scientific Highlights

035

Observation of a Binary Black Hole just before its Merger
			

IGUCHI, Satoru(NAOJ)OKUDA, Takeshi

SUDOU, Hiroshi(Nagoya University)		

In the galaxy formation process, galaxy clusters are
believed to evolve into a giant elliptical galaxy throughnumerous galaxy mergers. Recent observational results
show possible evidence that BBHs exist in the center ofgiant galaxies and may merge to form a supermassive
black hole in the process of their evolution. Clarifying
the BBH formation mechanism is essential for the studyof galaxy mergers in galaxy formation, as well as for theunderstanding of the role of black hole mergers in theevolution of supermassive black holes and the detectionof gravitational waves at the phase of BBH orbital decay.
We first detected a periodic flux variation on acycle of 93 ± 1 days (Fig. 1) from the 3-mm monitoring
observations of a giant elliptical galaxy 3C 66B[1],with which an orbital motion with a period of 1.05 ±0.03 years had been observed[2]. The detected signal
period is shorter than the orbital period; however it
can be explained by the Doppler-shifted modulation
associated with the orbital motion of a BBH. Assumingthat the BBH has a circular orbit and that the jet axis isparallel to the binary angular momentum (Fig. 2), ourobservational results demonstrate the presence of a very
close BBH that has a binary orbit with an orbital periodof 1.05 ± 0.03 years, an orbital radius of (3.9 ± 1.0)× 10−3−3pc, an orbital separation of (6.1+1.0
pc, the larger−0.9)× 10+0.5
9black hole mass of (1.2−0.2) × 10 M, and the smaller black+4.7
hole mass of (7.0−6.4) × 108 M. Since it is supposed thata black hole emits strong gravitational waves in the final
stage of merger, the decay time of a BBH estimated from2
the gravitational radiation is (5.1 +60.5−2.5 ) × 10 years. The
black hole merger is one of the most spectacular natural
phenomena in the universe and our observational results
show that the black hole collisions may have important
implications for the formation of a supermassive blackhole in the evolution process.

(Gifu University)

Figure 1: (a) Peak flux monitoring data of the core of 3C 66B
at millimeter wavelength, observed with NMA (filledsquares; 93.716 GHz) and PdBI (filled circles; 86.2
GHz). (b) Lomb- Scargle periodogram of the flux
monitoring data above. The data shows the periodicityof 93 ± 1 days with a 98 % probability.
aLine of sightJet direction
Jet direction

Jet direction
Orbital angularmomentum direction

Orbital angularmomentum directioniv : jet outflow
velocityv : jet outflow
velocity

References[1] Iguchi, S., Okuda, T., Sudou, H.: 2010, ApJ, 724, 166.
[2] Sudou, H., Iguchi, S., Murata, Y., Taniguchi, Y.: 2003, Science,
300, 1263.

R

R
vbl

Center of gravity
vbl m : smaller B H

M : larger BH

m : smaller BH

Center of gravity

M : larger BH

Figure 2: Two schematic geometries of a BBH. We assume thatthe BBH in 3C 66B has a circular orbit, that the jet islinked to the accretion disk around one of the two black
holes, and that the jet axis is parallel to the total angularmomentum of the binary. The observed jet is formed byeither (a) the smaller massive black hole (with a mass ofm) or by (b) the larger massive black hole (with a massof M).

036

I Scientific Highlights

Photospheric Magnetic Activities triggering X-ray Microflaresaround a Well-developed Sunspot
		KANO, Ryouhei(NAOJ)		

SHIMIZU, Toshifumi(JAXA/ISAS)			

Microflares, which are small energetic events in thesolar corona, are an example of dynamical phenomena
suitable for understanding energy release processes inthe solar corona. We identified 55 microflares arounda well-developed sunspot surrounded by a moat withhigh-cadence X-ray images from the Hinode X-Ray
Telescope (Figure 1), and searched for their photosphericcounterparts in line-of-sight magnetograms taken with
the Hinode Solar Optical Telescope. We found opposite
magnetic polarities encountering each other aroundthe footpoints of 28 microflares, while we could not
find such encounters around the footpoints of the other27 microflares. Emerging magnetic fluxes in the moat
were the dominant origin for causing the encountersof opposite polarities (21 of 28 events; Figure 2 left).
Unipolar moving magnetic features with the negative
polarity same as the sunspot definitely caused theencounters of opposite polarities for 5 microflares (Figure
2 right). The decrease of magnetic flux, i.e., magnetic
flux cancellation, was confirmed at the encounteringsite in typical examples of microflares. Microflares
were not isotropically distributed around the spot; themicroflares with emerging magnetic fluxes were observedin the direction where magnetic islands with the samepolarity as the spot were located at the outer boundaryof the moat, while the microflares with negative moving
magnetic features were observed in the direction where
magnetic islands with the polarity opposite to the spot
were located at the outer boundary of the moat. We also
found that emerging magnetic fluxes in the moat had aunique orientation in which the same polarity as the spot
is closer to the spot than the other. These observational
results lead to two magnetic configurations including
magnetic reconnection for triggering energy release atleast in a half of microflares around the spot, and suggestthat the global magnetic structures around the spot
strongly affect what kinds of polarity encounters areformed in the sunspot moat[1].

TARBELL, Theodore D.
(LMSAL)

Figure 1: X-ray image taken with the Hinode/XRT. Somemicroflares used in the paper are shown by arrows.

Reference[1] Kano, R., Shimizu, T., Tarbell, T. D.: 2010, ApJ, 720, 1136.
Figure 2: Microflares triggered by a emergning magnetic flux (left)
and a moving magnetic feature (right). They are shownby arrows on the magnetograms. Brightening in Ca II H
line were also observed.

I Scientific Highlights

037

Evolution of a Nuclear Gas Disk and Gas Supply to the Galactic Center
NAMEKATA, Daisuke(Univeristy of Tsukuba)

Gas supply to galactic centers is important for
activities in galactic centers and growth of super-massive
black holes (SMBHs). To elucidate relation between
gas supply processes to galactic centers and activities
in galactic centers is also important for understanding
the evolution of galaxies. We have studied the relation
between gas supply from the Galactic disk to the central
60 pc region in our Galaxy and stellar and gas distribution
in this region. A part of our study[1] was published by
support of NAOJ. Here, we report the results of [1].
In the central 60 pc, there are three young massive starclusters (Central cluster, Arches cluster, and Quintuplet
cluster). Each of the clusters contains a hundred of
massive stars and masses of the clusters is estimated tobe ~104 M, if we assume the Salpeter-type IMF[2]. The
Central cluster exists within the central 1 pc and the otherclusters exist at the projection distance of 30 pc from the
Galactic center. How these clusters are formed remains
unclear. At the radius of 2–5 pc, there is also a massive
molecular gas ring called the circumnuclear disk (CND).
Its mass is estimated to be ≤ 106 M[3]. How the CND
is formed and how the CND is related with the Centralcluster are uncertain. The clusters have similar ages,
indicating that the clusters are formed simultaneously by
the same process. In [1], we consider the possibility that
the CND and the star clusters are formed simultaneously
by the evolution of a self-gravitationally unstable gas disk
(hereafter, the nuclear gas disk) whose radius is muchlarger than the radius of the CND. We assume that gas issupplied from the Galactic disk to the nuclear gas disk
continuously.
In order to investigate this possibility, we performedhigh resolution two-dimensional hydrodynamic
simulations of the nuclear gas disk taking into accountselfgravity and radiative cooling. All the simulations arecarried out on Cray XT4 af CfCA of NAOJ.
The evolution of the nuclear gas disk is as follows.
The outer part of the nuclear gas disk frist becomes
self-gravitationally unstable by the gas supply from the
Galactic disk. By self-gravitational instability, small
gas clumps with the mass of ≈ 10 3 M  are formed in
the outer part of the nuclear gas disk. These gas clumps
coalescences into more massive gas clumps. Thesemassive gas clumps gravitationally interacts with eachother and exchange their angular momentum. By this,angular momentum transfer is induced in the nuclear gas
disk and gas is supplied to smaller radii. The typical massof massive gas clumps are 104–105 M. We found thatthese massive gas clumps can reach the Galactic center
without being destroyed by strong tidal force produced

038

I Scientific Highlights

by the SMBH and the nuclear star cluster. Figure 1 shows
the migration of a massive gas clump to the Galactic
center.
Recently, low angular momentum cloud capture by
the SMBH is proposed as the formation mechanismof the Central cluster[4]. They showed that in order toreproduce the observations, the mass of the gas clump
must be comparable to 104–105 M. These masses are
consistent with the mass of the gas clumps that migrate
to the Galactic center in our simulations. Thus, theselfgravitational instability of the nuclear gas disk may
explain the origin of gas clump assumed in[4].

Figure 1: Migration of a massive gas clump to the Galactic center.

References[1] Namekata, D., Habe,A.: 2011, ApJ, 731, 57.
[2] Figer, D., et al.: 1999, ApJ, 525, 750.
[3] Montero-Castaño, M., Herrnstein, R. M., Ho, P. T.: 2009, ApJ,
695, 1477.
[4] Bonnell, I., Rice, W.: 2008, Science, 321, 1060.

Subaru Telescope Detects Clues for Understanding the Origin of
Mysterious Dark Gamma-Ray Bursts
				

HASHIMOTO, Tetsuya(NAOJ)		

YABE, Kiyoto(Kyoto University)

OHTA, Kouji

Aoki, Kentaro, TANAKA, Ichi

KAWAI, Nobuyuki

Subaru GRB Team

(Kyoto University)		
(Tokyo Institute of Technology)

Gamma-ray bursts (GRBs) are one of the mostprofound mysteries in current astronomy. A lowmetallicity single-star explosion scenario is generally
being accepted as a explanation of the origin of GRBs
in theory[1] and observation[2]. However adding to thecomplexity of understanding GRBs are “dark GRBs”,
which have extremely faint afterglows and/or cannot be
detected in the optical band, are particularly elusive andhave rarely been investigated, even though they may
make up close to half of all GRBs.
The opportunity to know more about dark GRBs
came on March 25, 2008 when a dark GRB without its
optical afterglow. Only 9 hours after the burst, we used
the Subaru Telescope, mounted with its Multi-Object
Infrared Camera and Spectrograph (MOIRCS), to obtain
nearinfrared images of the field around the GRB andunveil its mysterious nature, the only detection of a
GRB host galaxy and its afterglow in the near-infrared(Figure 1). The rapid observational system of the Subaru
Telescope, its strong light-gathering power, and nearinfrared observations with its wide-field instrument
facilitated this successful discovery. Theoretical models
predict much brighter GRB afterglows than the relatively
faint afterglow that our images detected in the nearinfrared wavelength. We propose that our findings
demonstrate that a large amount of dust around the GRB
strongly suppressed the brightness of the afterglow in the
optical and near-infrared wavelengths. A high-metallicity
environment typically produces a very dusty environment
like this. Did it do so in this case?
To explore this question, we followed-up our
research about a year after our initial observation. We
used the Subaru Prime Focus Camera (Suprime-Cam)to obtain optical images of the GRB’s field that could
be used to investigate the properties of the host galaxy.
We successfully detected the host galaxy, this time inthe optical band. This allowed us to examine various
properties of the host galaxy by comparing the observedbrightness of the GRB host in various wavelengths withmodel spectra of the galaxy. We found that this hostgalaxy has a stellar mass comparable to that of the Milky
Way and is one of the most massive GRB host galaxies.
More massive galaxies generally tend to show higher
metallicity[3]. We calculated the expected metallicity of
the host galaxy by relating its stellar mass to metallicity
and found that its expected metallicity is by far thehighest among metallicities previously confirmed for(NAOJ)

GRB host galaxies[4].
How, then, could we explain our findings? A
lowmetallicity single-star explosion scenario does notalign with the current our findings that the host galaxyof this dark GRB has high metallicity. Our findings
open the possibility that dark GRBs may originate froma type of explosion process other than that of the morewellinvestigated GRBs. A binary-star merger scenario[5] has been proposed in the past as another possible
explanation for the origin of GRBs. Since this scenario
can account for the occurrence of GRBs in highmetallicity environment, we point out the possibility
that this dark GRB originated in a binary-star system.
Our results demonstrate that research on dark GRBs is
an important key to revealing the origin of the whole
population of GRBs.
We may even throw light on the hypothesis[6] that a
GRB within the Milky Way may be responsible for themass extinction that occurred on Earth about 435 million
years ago during the Ordovician Period. Until now, this
explanation was deemed unlikely because of the highmetallicity environment of the Milky Way[7].

Figure 1: Afterglow of the dark GRB and its host galaxy takenwith the Subaru Telescope’s MOIRCS. Image (a) was
taken 9 hours after the burst. Image (b) was taken 34
hours after the burst. Image (c) shows the afterglow afterimage (b) is subtracted from image (a). A green circle
in (a) shows the uncertainty of the position of the X-ray
afterglow.

References[1] Woosley, S. E., Bloom, J. S.: 2006, ARA&A, 44, 507.
[2] Modjaz, M., et al.: 2008, AJ, 135, 1136.
[3] Erb, D. K., et al.: 2006, ApJ, 644, 813.
[4] Hashimoto, T., et al.: 2010, ApJ, 719, 378.
[5] Nomoto, K. I., et al.: 1995, Phys. Rep., 256, 173.
[6] Melott, A. L., et al.: 2004, IJAsB, 3, 55.
[7] Stanek, K. Z., et al.: 2006, AcA, 56, 333.

I Scientific Highlights

039

_2
Near-infrared spectroscopy of massive star-forming galaxies at z ~(ETH Zürich)		

KONG, Xu

(USTC, China)

ARIMOTO, Nobuo

CIMATTI, Andrea(Università di Bologna)

I Scientific Highlights(CEA-Saclay)		

BROADHURST, TomRENZINI, Alvio(INAF-Padova)

ALEXANDER, Dave M.

(University of Basque Country)

We have obtained near-infrared (near-IR) spectra ofa sample of BzK-selected, massive star-forming galaxies(sBzKs; [1]) at 1.5 < z < 2.3 that were obtained with
OHS/CISCO at the Subaru telescope and with SINFONIat the VLT[2]. Among the 28 sBzKs observed, Hαemission was detected in 14 objects, and for 11 of them
the [N II] λ6583 flux was also measured. Multiwavelength
photometry[3] was also used to derive stellar masses andextinction parameters, whereas Hα and [N II] emissions
have allowed us to estimate star-formation rates (SFR),
metallicities, ionization mechanisms, and dynamicalmasses.
In order to enforce agreement between SFRs fromHα with those derived from rest-frame UV and midinfrared, additional obscuration for the emission lines (thatoriginate in H II regions) was required compared to theextinction derived from the slope of the UV continuum.
We have also investigated the stellar mass-metallicity
relation (Figure 1), as well as the relation between stellar
mass and specific SFR (SSFR), and compared them to theresults in other studies. At a given stellar mass, the sBzKs
appear to have been already enriched to metallicities
close to those of local star-forming galaxies of similar
mass. At the similar redshift range, the sBzKs presented
here tend to have higher metallicities compared to thoseof UV-selected galaxies, indicating that near-infrared
selected galaxies tend to be a chemically more evolved
population.
The sBzKs show SSFRs that are systematically higher,
by up to ~ 2 orders of magnitude, compared to those of
local galaxies of the same mass. The relation between
SSFR and stellar mass of Hα detected sample is consistent
with that for so-called main-sequence star-forming
galaxies at z  2 derived through multiwavelength SED
modeling[4] and radio stacking analysis[5] with a coupleof outliers reaching very high SSFRs similar to those ofsubmillimeter selected galaxies which are thought to bein violent star-forming phases driven by stochastic events
like major merger.
The empirical correlations between stellar mass andmetallicity, and stellar mass and SSFR are then comparedwith those of evolutionary population synthesis models[6]constructed either with the simple closed-box assumption,or within an infall scenario. Within the assumptions thatare built-in such models, it appears that a short timescale
for the star-formation (100 Myr) and large initial gas
mass appear to be required if one wants to reproduce both
relations simultaneously.

040

DADDI, Emanuele(NAOJ/GUAS)		

(Durham University)

9.4
9.2
12 + log(O/H)

ONODERA, Masato

9.0
8.8
8.6
8.4
8.2
8.0
9.0

9.5

10.0

10.5
11.0
log(M /M )

11.5

12.0

Figure 1: Mass-metallicity relation for sBzK galaxies in this study(filled square) compared with UV-selected z  2 galaxies(green dot-dashed line; [7]), z  0.7 galaxies (cyancircles; [8]), and local galaxies from SDSS (orange solidline; [9]).

References[1] Daddi, E., et al.: 2004, ApJ, 617, 746.
[2] Onodera, M., et al.: 2010, ApJ, 715, 385.
[3] Kong, X., et al.: 2006, ApJ, 638, 72.
[4] Daddi, E., et al.: 2007, ApJ, 670, 156.
[5] Pannella, M., et al.: 2009, ApJ, 698, L116.
[6] Fioc, M., Rocca-Volmerange, B.: 1997, A&A, 326, 950.
[7] Erb, D. K., et al.: 2006, ApJ, 644, 813.
[8] Savaglio, S., et al.: 2005, ApJ, 635, 260.
[9] Tremonti, C. A., et al.: 2004, ApJ, 613, 898.

Distance Measurement of Star-Forming Region IRAS 05137+3919
in Far Outer Galaxy
HONMA, Mareki, HIROTA Tomoya, KAN-YA, Yukitoshi, KAWAGUCHI, Noriyuki
KOBAYASHI, Hideyuki, KURAYAMA, Tomoharu, SATO, Katsuhisa(NAOJ)Star forming regions in far outer Galaxy are interesting targets because they can be used to trace extent
of the Galaxy disk and also because they provide alaboratory to study how star formation occurs in an
extreme environment with less metallicity and without
presence of spiral arm. So far several star-forming
regions are expected to exist in the far outer Galaxy
with a Galacto-centric distance larger than 15 kpc[1],and extensive studies have been conducted for someof these potential star-forming regions in the far outer
Galaxy[2]. However, their distance estimates were basedon kinematic distances and/or assumed luminosities ofyoung stars. Therefore, it is still highly uncertain whether
these star-forming regions are indeed located in sucha distant area, and hence astrometric confirmations aredefinitely required.
As an astrometric observation of such a star-forming
region in the far outer Galaxy, we have monitored an H2O
maser source associated with star forming region IRAS
05137+3919, which is located toward the anti-center
direction (l = 168°) with its kinematic distance of 12 kpc.
Although H 2O maser spots in IRAS 05137+3919 are
relatively variable in flux, we have determined a parallaxof � = 0.086 ± 0.027 mas (see Figure 1), corresponding
to a source distance of D = 11.6 +5.3
−2.8 kpc[3]. The parallax
detection is only 3-σ level and thus the uncertainty
is fairly large. Nevertheless, from this result we canstrongly constrain on the minimum distance of IRAS
05137+3919, which is 8.3 kpc at 90% confidence level.
This can be seen from the bottom panel of figure 1, wherea parallax significantly larger than 0.1 mas is inconsistent
with observations. The parallax obtained in this study isbasically consistent with the previous distance estimateof 12 kpc based on kinematic distance. Assuming the
Galaxy center’s distance of R0 = 8.5 kpc, the minimum
distance of 8.3 kpc is converted to a minimum Galactocentric distance of 16.7 kpc (again at 90% confidence
level). Therefore, the present study provides the first
astrometric confirmation that there indeed exists a starforming region in the far outer Galaxy.
The minimum distance obtained in this study isbeyond the distance of spiral arm that is measured basedon astrometry (such as Outer arm, corresponding to~13 kpc toward the direction of IRAS 05137+3919).
This result indicates that star formation process there is
triggered by other mechanism rather than spiral shocks,
imposing an interesting question on how stars form in theouter region of the Galaxy.

Figure 1: Maser spot motions in IRAS 05137+3919 along theEast-West direction. Top panel shows the observed
motions of 6 spots (sum of parallax and proper motion),and bottom panel is the parallax components after
removing the proper motions. Curves show the best-fit
results.

References[1] Diegel, S., et al.: 1994, ApJ, 422, 92.
[2] Kobayashi, N., et al.: 2008, ApJ, 683, 178.
[3] Honma, M., et al.: 2011, PASJ, 63, 17.

I Scientific Highlights

041

Connection of SuperMassive Black Hole and galaxy in Active galaxy
OI, Nagisa, IMANISHI, Masatoshi, IMASE, Keisuke(The Graduate University for Advanced Studies/NAOJ)

Active Galactic Nuclei (AGNs) emit the bulk of
their large luminosity (> 1010 L). An engine of AGN is
believed the release of gravitational energy generated bya mass-accreting onto SuperMassive Black Hole (SMBH)
and conversion to radiative energy. Recent observations
have revealed that formation of galaxies and SMBHs are
related to each other. Since a tight correlation between
masses of bulges (stellar masses) and SMBHs has beenfound, understanding the mechanism of connection
between AGN and host galaxy is important to uncover
the histories of SMBH and galaxy formations. However
since size of host galaxy is more than 1000 times
larger than that of AGN, it is difficult to connect them
directly. It is more likely that kinematics and/or energy isinteract with each material locally, then the relationshipbetween AGN and galaxy might be made, so that
understanding of relationship of them at a galaxy center
continues to play an important role. Some theories of thephysical mechanism at a galaxy center predict different
relationships between AGN and nuclear starburst
activities. To distinguish these theories, it is necessary to
study AGNs over a wide AGN luminosity range including
lowluminosity AGNs.
Infrared (IR) spectroscopy at λ = 2–4 μm is effective toinvestigate the nuclear starbursts, because effects of dust
extinction are small. Furthermore, Polycyclic Aromatic
Hydrocarbons (PAH) emission feature, found in this IR
wavelength range, can be used to distinguish between anemission of starbursts and AGN, because the feature areseen only in a starburst, but not in an AGN (due to PAH
destruction by AGN’s strong X-ray radiation). Moreover,
the CO absorption features in this IR wavelength range
can be used to estimate contributions an emission ofstellar and AGN. These features enable us to discriminate
an emission of starbursts and of AGN spectroscopicallyin an unresolved central region with spatially existingobserving facilities.
Narrow slit spectroscopy using IR spectrographs
attached to ground-based telescopes has applied
to prevent an emission of galaxy central from an
contamination by stars in an extended galaxy, and toinvestigate activities of nuclear starbursts. We have
performed IR 2–4 μm spectroscopy of 22 low-luminosity
nearby AGNs using the SpeX IR instrument attachedto the IRTF telescope, and estimated nuclear starburst
activities quantitatively (Fig. 1). We combined oursample with previous highluminosity AGNs[1], and thencompared the activities of nuclear starbursts with thoseof AGN. As a result, we found the positive correlation
between them over a wide AGN luminosity range (Fig. 2).

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I Scientific Highlights

The result strongly supports the theory that nuclear
starbursts remove much more angular momentum frommaterials and encourage an AGN activity, that is “nuclear
starbursts control the activity of AGN”[2].

Figure 1: (left): Near infrared spectrum of a starburst dominatedactive galaxy. PAH emission (top) and CO absorption(bottom) features are strong. (right): Spectrum of an
AGN dominated galaxy. Both of PAH emission and COabsorption features are very weak.

Figure 2: Nuclear starburst activities (ordinate) versus AGN
activities (abscissa). The more active the nuclear
starbursts activities are, the more active the AGN
activities are.

References[1] Imanishi, M., Wada, K.: 2004, ApJ, 617, 214.
[2] Oi, N., et al.: 2010, PASJ, 62, 1509.

Neutrino oscillation and expected event rate of supernova neutrinos
in adiabatic explosion model
KAWAGOE, Shio, YOSHIDA, Takashi

		

			

KAJINO, Toshitaka(University of Tokyo)		

SUMIYOSHI, Kohsuke

the number of high-energy neutrinos
the number of low-energy neutrinos(1)

where x refers to SK or SNO. The time-dependent
ratio shows clearer signal of the shock propagation thatexhibits remarkable decrease by at most factor ~2 for νˉe ininverted hierarchy, whereas it exhibits smaller change by~10% for νe in normal hierarchy (Figure 1). Both ratios
RSK and RSNO increase with sin2 2θ13 . For a given θ13, the(Tokyo University of Science)

YAMADA, Shoichi(Numazu College of Tschnology)

There are a lot of problems concerning to themechanism of core-collapsed supernova explosions andsupernova neutrinos[1]. Since 99% of the gravitationalenergy of the collapsed core is released as neutrinos. Mostof neutrino oscillation parameters have been determinedby the various neutrino experiments. However, it is still
very difficult to determine three neutrino oscillation
parameters of the mass difference between 1–3 mass
eigenstates ∆m 213, the mixing angle θ 13 , and the CP
violation phase δ[2]. It is one of the most importantresearch topics of particle physics to determine theseparameter values, and it is expected that the neutrinos
are important keys to solve how supernova explosions
succeed.
We calculate the supernova in adiabatic explosion
model using an implicit Lagrangian code for generalrelativistic spherical hydrodynamics[3,4]. The numericaltables of Shen’s equation of state (EOS) and Timmes’s
EOS are adopted for the high and low density mattersin this code, respectively. We solve the time evolutionof the neutrino wave function along the density profile
of our result, and we obtains survival probabilitiesof the neutrinos. The neutrinos change their flavorsat resonance of neutrino oscillations, and the shockpropagation influences the resonance. In the case of thenormal hierarchy (the inverted hierarchy), the survival
probabilities of ν e ( νˉ e ) are influenced by the shock
wave[5]. Using these survival probabilities, we obtain
the energy spectra of the neutrinos passed through the
exploding supernova. We calculate expected event ratesof the supernova neutrinos with Super-Kamiokande (SK)and SNO [4].
The expected event rates depend on θ 13, and theinfluence of the shock wave appears when sin 2 2θ 13
is larger than 10−3. The neutrino signals for the shockpropagation is decreased compared with the case without
shock. We define time-dependent ratio of the events ofhigh-energy to low-energy neutrinos,Rx =SUZUKI, Hideyuki(NAOJ/University of Tokyo)(Waseda University)

ratios with shock are smaller than the ratios without theshock. Therefore, observing time-dependent ratio of theneutrino events thus would provide a piece of very useful
information to constrain θ13 and the mass hierarchy, andeventually help understanding the propagation how theshock propagates inside the star.
RSNO

RSK

normal hierarchy

2.6
2.5

5

2.4

4

2.3

3

2.2

2

2.1
2.6

1
6

sin22 13=10-3

2.5

4

2.3

3

2.2

2

4

2.3

3

2.2

2

2.1
2.6

1
6

2

-5

sin 2 13=10

4

2.3

3

2.2

2

0

2

4

6

sin22 13=10-5

5

2.4

2.1

sin22 13=10-4

5

2.4

2.5

sin22 13=10-3

1
6

sin22 13=10-4

2.5

sin22 13=10-2

5

2.4

2.1
2.6

inverted hierarchy

6

sin22 13=10-2

8

10

1

0

2

4

6

8

10

Time [s]Time [s]Figure 1: Left panels are RSNO in the normal hierarchy, and rightpanels are RSK in the inverted hierarchy for sin2 2θ13 =10−2, 10−3, 10−4 and 10−5 from top to bottom. Solid anddashed lines are the calculated results with and without
shock wave, respectively.

References[1] Woosley, S. E., et al.: 1986, ApJ, 24, 205.
[2] Apollonio, M., et al.: 2003, PRD, 68, 093003.
[3] Yamada, S.: 1997, ApJ, 475, 720.
[4] Kawagoe S., et al.: 2010, PRD, 81, 123014.
[5] Kawagoe S., et al.: 2009, JCAP, 9, 033.

I Scientific Highlights043

Origin of rare isotope Ta-180 in supernova-neutrino nucleosynthesis
HAYAKAWA, Takehito, CHIBA, Satoshi

				(JAEA)			

MOHR, Peter

		

MATHEWS, Grant J.

(Diakoniekrankenhaus Schw¨abisch Hall) (University of Notre Dame)

The astrophysical origin of an isotope, 180Tam, hasremained an unsolved problem. This isotope has two
unique features. First this is the rarest isotope in the solar
system. Second the ground state decays by β decay witha half-life of 8.15 hr, whereas an excited state is a longlived isomer with a half-life of ≥ 1015 yr. This nucleus
is bypassed by the major nucleosynthesis mechanismsof the s and r processes. Thus exotic processes havebeen proposed but they have only underproduced theabundance of the rarest isotope 180Ta[1,2]. The mostpopular scenario in recent times is the production in theν process via the 181Ta(ν, ν′n)180Ta and 180Hf(νe, e)180Ta
neutrino reactions in core-collapse supernovae[3,4].
However, they overproduce the 180Ta solar abundance.
They noted that the observed 180mTa abundance can not
be inferred from their calculations until the branching
between the long-lived isomer and the ground state is
known.

1297
1087

10 +

5-

419.516+415.44

4-

317.8

5+

310.05

3210-

233.9
171.0
130.48107.6

4+184.34

3+

110.5

2+
1+

39.5
0

T1/2=8.15 h

11 -505.0310 -279.93

9-

77.1

9+

374.038+

177.76

Meta-stable Isomer

180

Ta

Isomer Structure

Figure 1: Schematic view of nucleosynthesis of 180Ta.

In the ν process, low-spin excited states in 180Ta are
predominantly populated from 180Hf by Gamow-Tellertransitions and subsequently decay preferentially to the1+ ground state. However, in a high temperature photon
bath of supernovae, the meta-stable isomer is excitedfrom the ground state by (γ, γ’) reactions through highly
excited states. Moreover, the transition rate between the
ground state and the isomer is affected by the changing
temperature. Therefore, the final isomeric branching ratio

I Scientific Highlights

should be evaluated by a time-dependent calculation.
We have proposed a model that the excited statesof 180Ta as consisting of two sets of nuclear states: 1)
the ground state structure, which consists of the groundstate plus the excited states with strong transitions to theground state; and 2) the analogous isomeric structure(see Fig. 1). For T9 = 0.1–1.0 all excited states lower thana few hundred keV are populated. After the freezeout
each excited state decays to either the ground state or
the isomer. In the transitional region, strongly connectedstates are only partly thermalized and two structures arelinked between the weak γ transitions. We calculate thetime-dependent calculation based on the two structure
model taking into account previously measured linking
transitions.
We finally obtain the isomer residual ratio of 0.39 at
the freeze-out. It should be noted that this ratio is almost
independent of the astrophysical parameters such as
the supernova neutrino energy spectrum, the explosion
energy, the temperature time constant, and the peaktemperature in the ν process layers. With this ratio we
can reproduce the solar abundance of 180Ta by neutrino
nucleosynthesis and an electron neutrino temperature ofkT ≈ 4 MeV[5,6].

595.26Ground State

Ground State Structure044

KAJINO, Toshitaka(NAOJ/University of Tokyo)

References[1] Beer, H., Ward, R. A.: 1981, Nature, 291, 308.
[2] Yokoi, K., Takahashi, K.: 1983, Nature, 305, 198.
[3] Woosley, S. E., et al.: 1990, ApJ, 356, 272.
[4] Byelikov, A., et al.: 2007, Phys. Rev. Lett., 98, 082501.
[5] Hayakawa, T., et al.: 2010, Phys. Rev. C, 81, 052801(R).
[6] Hayakawa, T., et al.: 2010, Phys. Rev. C, 82, 058801.

A New Type of Small-Scale Downflow Patches in Sunspot Penumbrae
				

KATSUKAWA, Yukio(NAOJ)

It has been known that high-speed outward flows,
called Evershed flows, take place along magnetic fieldlines in a sunspot penumbra. High resolution and highprecision spectro-polarimetric observations with Hinodehave provided lots of knowledge on relationship between
filamental magnetic structures and the Evershed flows inpenumbrae, which helps to understand how the highspeed
flows are driven by strong interaction between inclined
fields and convection. In contrast, Hinode has revealed
that there are small-scale flows in and around a sunspot
that cannot be explained by the Evershed flows and has
not been realized before.
The penumbral flow studied in this paper is oneof the flow structures newly discovered with Hinode.
Observations with the Spectro-Polarimeter (SP) aboard
the Solar Optical Telescope (SOT) clearly show existenceof patchy downflow structures in a penumbra which are
different from the Evershed flows[1]. Sunspot magnetic
fields consist of vertical and horizontal magnetic
components with respect to the solar surface, and they
form interlaced magnetic field configuration. The patchy
structures associated with the downflow have a size of
300–400 km, and are located within the vertical magnetic
component. While the flow structures associated with
the Evershed flow typically have duration of tens ofminutes to one hour, the newly discovered downflows are
relatively transient phenomena and have duration of only
a few minutes. The small size and short duration probably
made it difficult to find the downflow patches in previous
observations. Analysis of polarized spectrum line profiles
reveals that the velocity of the downflow is about 1 km/s
in the lower photospheric layer, and is almost zero in theupper photosphere.
The penumbral downflows have importance becausesome of the downflows are temporally and spatiallycoincident with the chromospheric brightenings above
the penumbra. It is expected that magnetic reconnection
between the vertical and horizontal magnetic fields
generates bi-directional jets; the downward flow isobserved in the photosphere, and the upward flow isobserved in the chromosphere as a transient brightening.
In this case, the finding of the downflows strongly
supports that magnetic reconnection takes place inthe photosphere. On the other hand, no counterpart is
detected in the chromosphere for some of the downflows.
One reason is that the observation does not have enoughtemporal resolution to detect temporal coincidence of thetransient downflows and the brightenings. Some of thedownflows are observed to appear after disappearance of
the Evershed flows, which suggests that cooled materialsJURČÁK, Jan(Academy of Sciences of the Czech Republic)

drain down along magnetic fields after interruptionof heat transport by the Evershed flow. The process ispossibly related with the disappearance of the filamental
magnetic fields[2]. It is required to acquire a simultaneous
observation of the photosphere and the chromospherewith high temporal resolution to get a better grasp on thecause of the downflows.

Figure 1: Sunspot penumbra observed with the Hinode SpectroPolarimeter (SP). Here are shown maps of contin- uum
intensities (left top), intensities of circular polarization(right top), red shifts of the circular polarization (leftbottom), and chromospheric brightenings seen in Ca II H
ltergrams (right bottom). The red contours indicate down
ow patches, and the arrows indicate the chromosphericbrightenings coin- cident with the down ows.

References[1] Katsukawa, Y., Jurčák, J.: 2010, A&A, 524, A20.
[2] Jurčák, J., Katsukawa, Y.: 2010, A&A, 524, A21.

I Scientific Highlights045Latest model calculation of big bang nucleosynthesis catalyzed
by a long-lived massive particle
						

KUSAKABE, Motohiko(University of Tokyo)		

YOSHIDA, Takashi(University of Tokyo)		

In standard big bang nucleosynthesis (BBN) withthe baryon-to-photon ratio inferred from WMAP, 7Li
is produced mostly as 7Be (Fig. 1a, dashed lines). Subsequently, 7Be is transformed into 7Li by electron capture.
A problem of standard BBN is a discrepancy between
the predicted and observed abundances of (6 and) 7Li[1].
One of solutions is catalysis reactions by negatively
charged massive particles X −s[2]. We solve numericallythe nonequilibrium nuclear and chemical reaction
network for this X −-catalyzed BBN[2] with improved
reaction rates derived from rigorous quantum many-body
calculations[3]. We adopt all of their rates, and choose
their 7BeX (p, γ)8BX rate for an infinite X − mass case.
Figure 1 shows a result of BBN calculation[4]. The
X − particles recombine with 7Be at T9 ~ 0.5. The 7BeX
(Fig. 1b) is then destroyed by the 7BeX (p, γ)8BX reaction,
primarily through the atomic excited state of 8B X[5],and secondarily through the atomic ground state 8B*(1+,0.770 MeV)X composed of the 8B*(1+, 0.770 MeV) nuclear
excited state and an X −[6]. At T9 ~ 0.1, the X −particles
bind to 4He. Then, the reaction 4HeX (d, X −)6Li operates,and 6Li and 6LiX (after the recombination) are produced.
Neutral X-nuclei, i.e., pX, dX, and tX, mainly react with
4
He nuclei to lose their X −s leaving 4HeX. The abundancesare, therefore, kept low. Their nuclear reactions are thus
not important.
The 8BeX (p, γ)9BX reaction through the 9B*Xa atomic
excited state is weak because its resonance energy is large[3]. The resonant 8BeX (n, X −)9BeX reaction through thestate 9Be*(1/2+, 1.684 MeV)X is not likely to operate since
the state is estimated to be not a resonance but a boundstate located below the 8BeX + n threshold[3].
We assume that the present cold dark matter (DM)was partly produced by the decay of X ± particles, i.e.,
Y DM ≥ Y X. Using the WMAP-CMB constraint on thecold DM density and the X − abundance needed for asolution to the Li problems, a limit on the mass mDM isderived. Comparing this mass to the suggested allowed
region, e.g., 40 GeV < mDM < 200 GeV from the CDMS
experiment, implies that only an X − particle which decays
via the weak interaction can have existed with sufficientabundance to reduce the 7Li produced in BBN (see Fig. 6of [2] for this case).
In this revised model there is no signature in theabundances of nuclei heavier than Be. We predict thatthe primordial 9Be abundance in the allowed parameterregion is negligible, 9 Be/H < O(10 −25), and far less046

I Scientific Highlights

KAJINO, Toshitaka(NAOJ/University of Tokyo)

MATHEWS, Grant J.

(University of Notre Dame)than the most stringent upper limit of 9Be/H < 10−14[7].
9BeX is destroyed through the process 9BeX (p, 6Li)4HeX[2]. Another isobar, i.e., 9BX can be produced without
experiencing the decays. The decay of the X −, however,induces reactions 9BX → p + 8Be + (decay products) since
the 9B is unstable to the proton decay. The 9Be production
through 9BX is, thus, not possible

Figure 1: Abundances of normal (a) and X-nuclides (b) as afunction of temperature T9 ≡ T/(109 K). The parameters
are the abundance ratio of X to baryon YX ≡ nX /nb = 0.05
and the lifetime τX = ∞. This is reprinted from[1].
References[1] Aoki, W., et al.: 2009, ApJ, 698, 1803.
[2] Kusakabe, M., et al.: 2008, ApJ, 680, 846.
[3] Kamimura, M., et al.: 2009, Prog. Theor. Phys., 121, 1059.
[4] Kusakabe, M., et al.: 2010, Phys. Rev. D, 81, 083521.
[5] Bird, C., et al.: 2008, Phys. Rev. D, 78, 083010.
[6] Kusakabe, M., et al.: 2007, Phys. Rev. D, 76, 121302.
[7] Ito, H., et al.: 2009, ApJ, 698, L37.

Discriminating Planetary Migration Mechanisms by the SEEDS Project
NARITA, Norio1, KUDO, Tomoyuki1, BERGFORS, Carolina2, NAGASAWA, Makiko3
THALMANN, Christian2, SATO, Bun’ei3, SUZUKI, Ryuji1, KANDORI, Ryo1, JANSON, Markus4
GOTO, Miwa2, BRANDNER, Wolfgang2, IDA, Shigeru3, ABE, Lyu5, CARSON, Joseph2/6
EGNER, Sebastian, E.1, FELDT, Markus2, GOLOTA, Taras1, GUYON, Olivier1/7, HASHIMOTO, Jun1
HAYANO, Yutaka1, HAYASHI, Masahiko1, HAYASHI, Saeko1, HENNING, Thomas2, HODAPP, Klaus, W.8
ISHII, Miki1, KNAPP, Gillian, R.9, KUSAKABE, Nobuhiko1, KUZUHARA, Masayuki1/10, MATSUO, Taro11
McELWAIN, Michael, W.9, MIYAMA, Shoken1, MORINO Jun-Ichi1, MORO-MARTIN, Amaya2
NISHIMURA, Tetsuro1, TAE-SOO, Pyo1, SERABYN, Eugene11, SUENAGA, Takuya1/12, SUTO, Hiroshi1
TAKAHASHI, Yasuhiro, H.1/12, TAKAMI, Michihiro13, TAKATO, Naruhisa1, TERADA, Hiroshi1
TOMONO, Daigo1, TURNER, Edwin, L.9/10, WATANABE, Makoto14, YAMADA, Toru15
TAKAMI, Hideki1, USUDA, Tomonori1, TAMURA, Motohide1
1: NAOJ, 2: Max Planck Institute for Astronomy, 3: Tokyo Institute of Technology, 4: University of Toronto, 5: Universite de Nice SophiaAntipolis, 6: College of Charleston, 7: University of Arizona, 8: University of Hawaii, 9: Princeton University, 10: University of Tokyo, 11: Jet
Propulsion Laboratory, California Institute of Technology, 12: Graduate University for Advanced Studies, 13: Academia Sinica, 14: Hokkaido
University, 15: Tohoku University

Planetary orbits reflect their migration history. It
is now known that there are many exoplanets witheccentric and/or highly tilted orbits. Those exoplanets are
considered to migrated through planet-planet scatteringor the Kozai migration. It is difficult, however, todiscriminate these two migration mechanisms, since theboth mechanisms predict eccentric and/or highly tilted
orbits. To discriminate the two migration mechanisms, it
it necessary to search for counterparts of their migration(e.g., giant planets for planet-planet scattering or a distantcompanion for the Kozai migration). We thus started
high-contrast direct imaging observations for eccentricor tilted planetary systems in the SEEDS (Strategic
Explorations of Exoplanets and Disks with Subaru)
project.
We first observed a retrograde planetary system
HAT-P-7, for which the Subaru telescope found theretrograde orbit of HAT-P-7b in 2009[1], with the
HiCIAO (High Contrast Instrument for the Subaru Next
Generation Adaptive Optics) onboard the Subaru. We
found that there are two companion candidates around the
HAT-P-7 system (see Figure 1)[2]. Although it is not yet
known whether those candidates are physically associatedwith HAT-P-7 or not, if associated, those companions
are M stars and separated by at least 1000 AU. We thencalculated whether those companion candidates can cause
the Kozai migration for the inner retrograde planet. We
found that it is impossible for the companion candidates
to cause the Kozai migration in the presence of an outerplanet around the retrograde planet (reported by [3]). As
a result, we conclude that it is the most plausible that theretrograde planet HAT-P-7b has migrated through planetplanet scattering. The SEEDS project will conduct thiskind of observations for dozens of planetary systems todiscriminate planetary migration mechanisms.

Figure 1: An image of HAT-P-7 taken with the Subaru HiCIAO.
Two companion candidates are detected around
HAT-P-7. The field of view is 12″ × 12″. North is up andeast is to the left.

References[1] Narita, N., et al.: 2009, PASJ, 61, L35-L40.
[2] Narita, N., et al.: 2010, PASJ, 62, 779-786.
[3] Winn, J. N., et al.: 2009, ApJ, 703, L99-L103.

I Scientific Highlights

047

Nano-JASMINE Ready to Launch!
KOBAYASHI, Yukiyasu. GOUDA, Naoteru, YANO, Taihei(NAOJ / Graduate Univeristy for Advanced Studies)				

HATSUTORI, Yoichi(NAOJ)			

YAMADA, Yoshiyuki(Kyoto University)

NIWA, Yoshito, MUROOKA, Junpei, SAKO, Nobutada, NAKASUKA, Shin’ichi(University of Tokyo)

Nano-JASMINE is almost complete except for the
final arrangements (Figure 1). The satellite is due forlaunch in the current fiscal year (2011)[1]. The bus part ofNano- JASMINE satellite was developed at the Nakasuka
laboratory, University of Tokyo, which has considerable
experience in developing very small satellite systems.
The mission part of the satellite was developed jointly
by the National Astronomical Observatory and Kyoto
University. The developed satellite will be launched fromthe Alcantara Space Launcher onboard the Cyclone-4
rocket, which has been developed by Uclaina[2].

Figure 1: The Nano-JASMINE flight model in the ATC large clean
room after experiments of optical alignments.

Nano-JASMINE is the first in a series of astrometry
satellites promoted by the JASMINE project office.
Although the satellite’s telescope has a diameter of only
5 cm, it will survey the entire sky in the zw-band (0.6–1.0 μm) during its 2-year operational life. It is expectedthat the satellite will measure more than 60,000 stars ofmagnitude less than 7 with an accuracy of less than 3mas[3]. The European Space Agency (ESA) HIPPARCOS
performed similar observations approximately 20
years ago; our mission can benefit from the large time
gap between the HIPPARCOS observations and ourobservations, which will help us to measure accurately
the proper motion of a large number of stars. Because thevarious techniques employed to achieve precise stellar
positioning used in this mission will also be used insubsequent JASMINE missions, it is a great opportunity
for the JASMINE team to verify and evaluate thesetechniques using real satellite data.

048

I Scientific Highlights

After the launch, we will use the Mizusawa 10 m
antenna and the new 3 m antenna installed atop the 7thbuilding of the engineering department at the Universityof Tokyo. We are now in the process of installing datatransfer instruments at both these antenna stations, andare developing data transfer software. In the preliminary
stages of satellite operation, the necessary satellite severcontrol will be performed from the Kiruna tracking
station, located in the northern part of Sweden. The
Kiruna tracking station, which is located inside the Arctic
Circle, ensures a longer visibility time. Therefore, it issuitable for this mission because our satellite will belaunched to a sun-synchronized orbit.
Analysis of the data acquired by Nano-JASMINE iscomplicated because the amount of data is enormous andall data must be solved integrated. GAIA, promoted by
the ESA, has the same observation approach. It is known
that GAIA’s analysis tool can be used for analyzing
Nano-JASMINE data[4]. The GAIA team has welcomed
the use of their tool for analyzing Nano-JASMINE data,
because they are interested in validating their tool withreal satellite data. We have reached a memorandum ofcooperation with the ESA for analyzing Nano- JASMINE
data.
References[1] Kobayashi, Y., et al.: 2010, SPIE, 7731, 77313Z.
[2] Niwa, Y., et al.: 2010, SPIE, 7731, 773141.
[3] Hatsutori, Y. et al.: 2011, EAS Publ. Series, 45, 397.
[4] Yamada, Y. et al.: 2011, EAS Publ. Series, 45, 135.

Performance evaluation of Nano-JASMINE telescope flight model				NIWA, Yoshito(NAOJ)		

HATSUTORI, Yoichi(IBM Japan, Ltd.)KOBAYASHI, Yukiyasu, GOUDA, Naoteru, YANO, Taihei

				(NAOJ)					Nano-JASMINE is a very small, 35-kg mass, satellite
for space astrometry[1,2], which will be launched by
Cyclone-4 rocket from Brazil in 2011. The satellite
is developed by National Astronomical Observatoryof Japan, Kyoto University and University of Tokyo.
Nano-JASMINE mounts a 5-cm effective diametertelescope and a time-delay integration (TDI) controlled
fully depleted charge coupled device (FDCCD) image
sensor which is sensitive to wavelength of zw-band(600 < λ < 1000 nm). Nano-JASMINE will perform
firsttime demonstrations and experimentations for Japan
astrometry mission in space. These trials are targetingfor Japan Astrometry Satellite Mission for Infrared
Exploration (JASMINE)[3]. By Nano-JASMINE mission,
we are also going to measure positions of ten or twenty
thousands of stars of zw < 7.5 mag for all-sky with anaccuracy of about 3 milli-arcsecond.
Astrometry is a field of observational astrophysics
that measures positions and proper motions of stars
on the celestial sphere, and determines the distances
to stars from the earth using trigonometric parallaxes
due to earth orbit around the sun. Space telescopes for
astrometry have much more advantage than groundbased telescopes; because of the effect of atmosphericmotions, observed star images are blurry in the case ofground-based observations. Therefore, HIPPARCOS waslaunched by ESA in 1989, and observed about hundredsof thousands of star positions around the all-sky with
one milli-arcsecond angular accuracy. In 2011, almost
22 years have passed since the end of the HIPPARCOS
mission. Then, the errors in proper motions haveaccumulated over the years; the individual motions ofstars and their uncertainties are large enough to degrade
the HIPPARCOS data during these two decades of blank.
Therefore, the Nano- JASMINE mission is beneficial.
Currently, satellite functional tests, which include
electrical integration tests, vibration tests, thermal
vacuum tests, and radiation tests, have almost finished,
and long duration operational tests are in the process in
preparation for the launch in August 2011. In this paper,
we report a result of performance evaluation of mission
system: a measurement of wave front error for thetelescope.
If there are mirror surface errors for the telescope,such errors cause optical aberrations. Accordingly, shapesof point spread functions (PSF) are distorted, and thecentroids of stellar images will be changed from true
positions. Total budget for root mean square (RMS)

YAMADA, Yoshiyuki(Kyoto university)

wave front error is λ/14 at λ = 800 nm. The wave front
error was measured for each mirror surface by use ofa Zygo interferometer. The results are shown in Fig. 1.
The total RMS wave front errors are both λ/17 at λ =800 nm for upper and lower optical system. We also
directly measured total wave front error for the fabricatedtelescope, which was placed in vacuum chamber andcool downed to 223 K, which is equal to the operating
temperature on the orbit. As a result, the total RMS wave
front errors are λ/19 and λ/21 for upper and lower opticalsystem, respectively. This result indicates that the error
level fulfills the requirement so that the telescope is given
assurance for diffraction-limited performance on theorbit.

Figure 1: Top left: the flight model of Nano-JASMINE. Top right:
the flight model of the telescope mirrors; M1 and M2 are
hyperboloid mirrors as a primary mirror and a secondary
mirror, respectively. M3 ~ M4 are flat mirrors. Bottom:
wave front error of each mirror surface.

References[1] Kobayashi, Y., et al.: 2006, SPIE, 6265, 626544 1-10.
[2] Hatsutori, Y., et al.: 2009, Proc. of the 27th ISTS, 2009-m-10.
[3] Gouda, N.: 2011, EAS Publications Series, 45, 393-396.

I Scientific Highlights049

Inclined Orbits Prevail in Exoplanetary Systems
						

NARITA, NorioHIRANO, Teruyuki(NAOJ)

SATO, Bun’ei(MIT/University of Tokyo)

AOKI, Wako, TAMURA, Motohide(Tokyo Institute of Technology)			

Since the discovery of the first exoplanet in 1995,
scientists have identified more than 500 exoplanets,
planets outside of our solar system, nearly all of which
are giant planets. Most of these giant exoplanets closely
orbit their host stars, unlike our solar system’s giant
planets, like Jupiter, that orbit the Sun from a distance.
Accepted theories propose that these giant planets
originally formed from abundant planet-forming materials
far from their host stars and then migrated to their current
close locations. Different migration processes have beensuggested to explain close-in giant exoplanets.
Disk-planet interaction models of migration focus
on interactions between the planet and its protoplanetarydisk, the disk from which it originally formed. Sometimes
these interactions between the protoplanetary disk andthe forming planet result in forces that make the planet
fall toward the central star. This model predicts that the
spin axis of the star and the orbital axis of the planet
will be in alignment with each other. Planet-planet
interaction models of migration have focused on mutual
scatterings among giant planets. Migration can occur
from planet scattering, when multiple planets scatter
during the creation of two or more giant planets within
the protoplanetary disk. While some of the planets scatterfrom the system, the innermost one may establish a final
orbit very close to the central star. Another planet-planet
interaction scenario, Kozai migration, postulates that thelong-term gravitational interaction between an inner giant
planet and another celestial object such as a companion
star or an outer giant planet over time may alter theplanet’s orbit, moving an inner planet closer to the central
star. Few-body interactions, including planetplanet
scattering and Kozai migration, could produce an inclined
orbit between the planet and the stellar axis.
Overall, the inclination of the orbital axes of closein planets relative to the host stars’ spin axes emerges asa very important observational basis for supporting or
refuting migration models upon which theories of orbital
evolution center. We have conducted observations with
the Subaru Telescope to investigate these inclinations
for several systems so far. We measured the RossiterMcLaughlin (hereafter, RM) effect of the systems andfound evidence that some of their orbital axes incline
relative to the spin axes of their host stars.
The RM effect refers to apparent irregularities in
the radial velocity or speed of a celestial object in theobserver’s line of sight during planetary transits. Unlike
the spectral lines that are generally symmetrical in050

I Scientific Highlights(NAOJ)

measures of radial velocity, those with the RM effectdeviate into an asymmetrical pattern. Such apparent
variation in radial velocity during a transit reveals thesky-projected angle between the stellar spin axis andplanetary orbital axis. Subaru Telescope has participatedin previous discoveries of the RM effect, which we haveinvestigated for over ten exoplanetary systems thus far.
Among the observed planetary systems, we newly foundthat TrES-4b has a well-aligned orbit[1], whereas XO4b[2] and HAT-P-11b[3] have highly inclined orbits (seeFigure 1). The latest observational results about the RM
effect, including those obtained independently of thefindings reported here, suggest that about one-third of theobserved systems have highly inclined planetary orbits.
The few-body scenario of migration, whether caused byplanet-planet scattering or Kozai migration, rather thanthe planetdisk scenario could account for their migration
to the present locations.

Figure 1: Illustration of the HAT-P-11 System Based on Observations from Subaru Telescope.

References[1] Narita, N., et al.: 2010, PASJ, 62, 653-660.
[2] Narita, N., et al.: 2010, PASJ, 62, L61-L65.
[3] Hirano, T., et al.: 2011, PASJ, 63, S531-S536.

Short Lifetime of Protoplanetary Disks in Low-metallicity Environments			

YASUI, Chikako, SAITO Masao

KOBAYASHI, Naoto(NAOJ)			

(University of Tokyo)

TOKUNAGA, Alan T.

TOKOKU, Chihiro(University of Hawaii)		

In order to understand protoplanetary disk evolution
and planet formation in a wider range of environments
than previously studied, we explored the lifetime ofprotoplanetary disks in the outermost Galaxy (Rg >~ 15kpc), which are known to have a very different metallicity
from the solar neighborhood, [M/H] ~ −1 dex.
We obtained the deep near-infrared (NIR) images ofsix young clusters that are located in the outer Galaxy
with known metallicity of [O/H]  −0.7 dex using Subaru
8.2 m telescope[1]. We derived disk fraction for eachcluster (Figure 1) and estimated disk lifetime in theenvironments (Figure 2). As a result, we found that disk
fraction of the low-metallicity clusters declines rapidlyin < 1 Myr, which is much faster than the ~ 5–7 Myr
observed for the solar-metallicity clusters, suggestingthat disk lifetime shortens with decreasing metallicity
possibly with an ~10Z dependence[2].
Since the shorter disk lifetime reduces the time
available for planet formation, this could be one of the
major reasons for the well-known “planet-metallicity
correlation”, which states that the probability of a star
hosting a planet increases steeply with stellar metallicity.
The reason for the rapid disk dispersal could be theincrease of the mass accretion rate, and/or the effective(Tohoku University)

far-ultraviolet and/or X-ray photoevaporation due to thelow extinction; however, another unknown mechanism
for the outer Galaxy environment could be contributing
significantly. Although more quantitative observational
and theoretical assessments are necessary, our resultspresent the first direct observational evidence that cancontribute to explaining the planet-metallicity correlation.

JHK Disk Fraction (%)

				[O/H] = 0
[O/H] = −0.7

Age (Myr)
Figure 2: Disk fraction as a function of cluster age. JHK disk
fractions of the young clusters with low metallicity
are shown by red filled circles, while those of young
clusters with solar metallicity are shown by black filled
circles. The black line shows the disk fraction evolution
under solar metallicity, while the red arrow shows the
proposed JHK disk fraction evolution in low-metallicity
environments.

References[1] Yasui, C., et al.: 2009, ApJ, 705, 54.
[2] Yasui, C., et al.: 2010, ApJ, 723, L113.

Figure 1: The way of deriving disk fraction for an example
cluster, the Cloud 2-N cluster. Disk fraction is definedas the frequency of NIR excess stars (located in orange
highlighted region) within a young cluster.

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051

Direct Imaging of Fine Structures in Giant Planet Forming Regionsof the Protoplanetary Disk around AB Aurigae*
HASHIMOTO, Jun1, TAMURA, Motohide1, FUKUE, Tsubasa1, KOKUBO, Eiichiro1, KANDORI, Ryo1
KUSAKABE, Nobuhiko1, MATSUO, Taro1, MIYAMA, Syoken1, MORINO, Jun-ichi1, SUTO, Hiroshi1
KUDO, Tomoyuki1, GOLOTA, Taras1, GUYON, Olivier1, HAYANO, Yutaka1, HAYASHI, Masahiko1
HAYASHI, Saeko1, ISHII, Miki1, NISHIMURA, Tetsuo1, PYO, Tae-Soo1, TAKATO, Naruhisa1
EGNER, Sebastian1, TERADA, Hiroshi1, TOMONO, Daigo1, TAKAMI, Hideki1, USUDA, Tomonori1
MUTO, Takayuki2, FUKAGAWA, Misato3, INUTSUKA, Shu-ichiro4, HONDA, Mitsuhiko5, GOTO, Miwa6
HENNING, Thomas6, CARSON, Joseph6, BRANDER, Wolfgang6, FELDT, Markus6, THALMANN, Christian6
KNAPP, Gillian7, MCELWAIN, Michael7, TURNER, Edwin7, MORO-MARTIN, Amaya7
MOMOSE, Munetake8, OKAMOTO, Yoshiko8, OHASHI, Nagayoshi9, TAKAMI, Michihiro9, GRADY, Carol10
HODDAP, Klaus11, WISNIEWSKI, John12, JANSON, Markus13, ABE, Lyu14, MAYAMA, Satoshi15
SUZUKI, Ryuji16, WATANABE, Makoto17, YAMADA, Toru18
1: NAOJ, 2: Tokyo Institute of Technology, 3: Osaka University, 4: Nagoyo University, 5: Kanagawa University, 6: Max Planck Institutefor Astronomy, 7: Princeton University, 8: Ibaraki University, 9: Institute of Astronomy and Astrophysics, 10: Goddard Space Flight Center,
11: University of Hawaii, 12: University of Washington, 13: University of Toronto, 14: University of Nice, 15: The Graduate University for
Advanced Studies, 16: TMT Observatory Corporation, 17: Hokkaido University, 18: Tohoku University

1-0.5

Outer ring

B

E
P3

P1
F
P2
G

Inner ring

C

0.5
-0.5
-1
R.A. offset (arcsecond)(mJy/arcsec 2)

0

-0.5

-100

10

0

A

-50

0.5

-50 -100 -150

AU
0

N
E

0

50

D

50
Ring gap

150 100

Dec. offset (arcsecond)0
0.5-50 -100 -150 100-0.5

I Scientific Highlights

0

0

052

50

0.5

* Based on data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan.

AU
100

1

Circumstellar disks are usually formed around youngstars and are intricately tied to the origin of planets (e.g.,[1]). Giant planets have been considered to form via gas
accretion onto rocky cores in such disks (e.g., [2]), which
can successfully explain “normal” giant planets likeours. However, recent direct detections of companionswith masses of a few up to a few tens of MJ at distances> 20 AU, beyond what had been thought to be the planet
forming zone (e.g., [3]), pose a challenge for the standard
core-accretion scenario where planets are formed in-situ.
Thus, information on the detailed structures of the inner (r< 50 AU) regions of protoplanetary disks is crucial.
We report high-resolution 1.6 μm polarized intensity(PI) images of the circumstellar disk around the Herbig
Ae star AB Aur at a radial distance of 22 AU (0 ″. 15) up
to 554 AU (3 ″. 85)[4], which have been obtained by thehigh-contrast instrument HiCIAO with the dual-beampolarimetry. We revealed complicated and asymmetricalstructures in the inner part (< 140 AU) of the disk, while
confirming the previously reported outer (r > 200 AU)
spiral structure. We have imaged a double ring structure
at ~40 and ~100 AU and a ring-like gap between the two(Fig. 1). We found a significant discrepancy of inclination
angles between two rings, which may indicate that thedisk of AB Aur is warped. Furthermore, we found sevendips (the typical size is ~45 AU or less) within two rings,
as well as three prominent PI peaks at ~40 AU. The
observed structures, including a bumpy double ring, aring-like gap, and a warped disk in the innermost regions,provide essential information for understanding theformation mechanism of recently deteced wide-orbit (r> 20 AU) planets.

-1
100

Figure 1: PI image with a coronagraphic occulting mask of 0.″3
diameter (left) and the features (right). Central position(0, 0) is the stellar position. The outer and inner rings
are denoted by the dashed ellipsoids. The solid ellipsoid
indicates the wide ring gap. The dashed circles (A to G)
represent small dips in the two rings. The filled diamond,circle, and square represent the geometric center of theinner ring, ring gap, and outer ring, respectively. The
field of view in both images is 2.″0 by 2.″0. The solid
circle in the left-bottom inset represents the spatial
resolution of 0.″06.

Reference[1] Shu, F. H., Adams, F. C., Lizano, S.: 1987, ARA&A, 25, 23.
[2] Pollack, J. B., el al.: 1996, Icarus, 124, 62.
[3] Marois, C., et al.: 2008, Science, 322, 1348.
[4] Hashimoto, J., et al.: 2011, ApJ, 729, L17.

Imaging of a Transitional Disk Gap in Reflected Light:
Indications of Planet Formation Around the Young Solar Analog LkCa 15*
THALMANN, Christian1, GOTO, Miwa1, HENNING, Thomas1, CARSON, Joseph1, BRANDER, Wolfgang1
FELDT, Markus1, GRADY, Carol2, WISNIEWSKI, John3, JANSON, Markus4, FUKAGAWA, Misato5
SHIBAI, Hiroshi5, HONDA, Mitsuhiko6, MULDERS, Gijs7, MIN, Michiel8, KNAPP, Gillian9
MCELWAIN, Michael9, TURNER, Edwin9, MORO-MARTIN, Amaya9, HODDAP, Klaus10, ABE, Lyu11
SERABYN, Eugene12, TAKAMI, Michihiro13, KUDO, Tomoyuki14, GOLOTA, Taras14, GUYON, Olivier14
HAYANO, Yutaka14, HAYASHI, Masahiko14, HAYASHI, Saeko14, ISHII, Miki14, NISHIMURA, Tetsuo14
PYO, Tae-Soo14, TAKATO, Naruhisa14, EGNER, Sebastian14, TERADA, Hiroshi14, TOMONO, Daigo14
TAKAMI, Hideki14, USUDA, Tomonori14, FUKUE, Tsubasa14, HASHIMOTO, Jun14, KANDORI, Ryo14
KUSAKABE, Nobuhiko14, KUZUHARA, Masayuki14, MATSUO, Taro14, MIYAMA, Syoken14
MORINO, Jun-ichi14, SUTO, Hiroshi14, TAMURA, Motohide14, SUZUKI, Ryuji15
WATANABE, Makoto16, YAMADA, Toru17
1: Max Planck Institute for Astronomy, 2: Goddard Space Flight Center, 3: University of Washington, 4: University of Toronto, 5: Osaka
University, 6: Kanagawa University, 7: University of Amsterdam, 8: University of Utrecht, 9: Princeton University, 10: University of Hawaii,
11: University of Nice, 12: Jet Propulsion Laboratory, 13: Institute of Astronomy and Astrophysics, 14: NAOJ, 15: TMT Observatory
Corporation, 16: Hokkaido University, 17: Tohoku University

The circumstellar disks of gas and dust around newly
formed stars are believed to be the birthplaces of giant
planets. In some protoplanetary disks, evidence of gaps
or inner cavities has been revealed through analysis of
the infrared spectral energy distribution (SED; e.g., [1])or interferometry at infrared (e.g., [2]) or millimeter
wavelengths (e.g., [3]). These objects have been termed“transitional” disks, since they are thought to represent atransitional state of partial disk dissipation between the
protoplanetary disk stage and the debris disk stage.
We present H- and Ks-band imaging data resolving
the gap in the transitional disk around LkCa 15, revealing
the surrounding nebulosity[4]. We detect sharp ellipticalcontours delimiting the nebulosity on the inside as wellas the outside, consistent with the shape, size, ellipticity,and orientation of starlight reflected from the far-side
disk wall, whereas the near-side wall is shielded fromview by the disk’s optically thick bulk. We note thatforward scattering of starlight on the near-side disk
surface could provide an alternate interpretation of
the nebulosity. In either case, this discovery provides
confirmation of the disk geometry that has been proposed
to explain the spectral energy distributions (SED) of
such systems, comprising an optically thick disk withan inner truncation radius of 46 AU enclosing a largely
evacuated gap. Our data show an offset of the nebulosity
contours along the major axis, likely corresponding to aphysical pericenter offset of the disk gap. This reinforces
the leading theory that dynamical clearing by at least
one orbiting body is the cause of the gap. Based on
evolutionary models, our high-contrast imagery imposes
an upper limit of 21 MJup on companions at separations

outside of 0.″1 and of 13 MJup outside of 0.″2. Thus, wefind that a planetary system around LkCa 15 is the most
likely explanation for the disk architecture.

Figure 1: Ellipse fits to the inner and outer boundaries of thescattered light nebulosity seen in the HiCIAO H-band
LOCI image after median filtering on the spatial scale of
5 pixels 1 FWHM and derotation by −29.3° (based on
the position angle of 150.7 in [5]). The inner (orange)and outer (red) ellipses are offset from the star along the
major axis by 51 mas and 57 mas and rotated by −4° and−3°, respectively. Their centers are marked by orange
and red plus signs, respectively, while the star’s position
is indicated by a white plus sign.

References[1] Calvet, N., et al.: 2002, ApJ, 568, 1008.
[2] Ratzka, T., et al.: 2007, A&A, 471, 173.
[3] Brown, J. M., et al.: 2009, ApJ, 704, 496.
[4] Thalmann, C., et al.: 2010, ApJ, 718, L87.
[5] Pietu, V., et al.: 2007, A&A, 476, 163.

* Based on data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan.

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053

Outflow in a Luminous Quasar AKARI J1757+5907
			

AOKI, Kentaro(NAOJ)OYABU, Shinki(Nagoya University)

ARAV, Nahum, EDMONDS, Doug

				

(Virginia Tech)			

DUNN, Jay P.

(Augusta State University)

KORISTA, Kirk T.

(Western Michigan University)

MATSUHARA, Hideo, TOBA, Yoshiki(Institute of Space and Astronautical Science)

Over the past decade it has been regarded that themass of the black hole and the mass of the galactic bulge
has the tight correlation. The black hole mass is ~0.1% of
the bulge mass[1]. The outflow phenomena of gas is oneof processes which may connect the growth of galactic
bulge and black hole. Active black holes is capable toblow out gas in the host galaxies and may suppress
the star formation activities (e.g., [2]). In fact outflow
phenomena are ubiquitous among the galaxies which
possess active black holes. The blueshifted absorption
lines are the sign of the outflow. However, it has been
still unclear the details of outflow phenomena aroundthe black hole. The basic knowledge of the outflow
are vague: How much amount of gas has been blown
out? How long does the outflow last? Does the outflow
significantly affect the star formation in the host galaxy?
We selected a luminous quasar, AKARI J1757+5907
as the target. This quasar was discovered during thefollow-up observations of AKARI mid-infrared All-Sky
Survey[3,4]. The follow-up low-resolution spectroscopy
revealed that AKARI J1757+5907 is a z = 0.615 quasar
that shows blueshifted absorption lines. Its apparent
magnitude is 15th and very suitable for high resolution
spectroscopy of absorption lines. More than three hours
integration was done with HDS attached to the Subaru 8.2
m telescope. The resolving power was R ~ 36000.
Our high resolution spectroscopy revealed that theabsorption consists of 9 distinct troughs (Figure 1).
We can measure accurate column densities of He I*,
Fe II and Mg II for the troughs at ~ −1000 km s −1. We
use photoionization models to constrain the ionization
parameter, total hydrogen column density, and thenumber density of the outflowing gas. These constraints
yield lower limits for the distance, and mass flow rate
for the outflow of 3.7 kpc, and 70 M yr−1, respectively.
This distance contrasts with the previous understandingof the outflow which occurs at the close to the black hole.
The our derived mass flow rate and the velocity is similar
to those recently discovered in massive post-starburst
galaxies[5].
This research has been published in “Outflow inOverlooked Luminous Quasar: Subaru Observations of
AKARI J1757+5907” PASJ, 63, S457 (2011).

054

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Figure 1: Outflow troughs in AKARI J1757+5907. Ordinate is anormalized flux density, and abscissa is velocity fromthe systemic redshift (z = 0.61525). Blended parts aredenoted as dotted spectra. The dashed vertical line
indicates the position of the blue component of [O III]emission line of this quasar. The velocity of that [O III]
corresponds to the trough at ~ −1000 km s−1.

References[1] Häring, N., Rix, H.-W.: 2004, ApJ, 604, L89.
[2] Di Matteo, T., Springel, V., Hernquist, L.: 2005, Nature, 433,
604.
[3] Ishihara, D., et al.: 2010, A&A, 514, A1.
[4] Murakami, H., et al.: 2007, PASJ, 59, 369.
[5] Tremonti, C. A., Moustakas, J., Diamond-Stanic, A. M.: 2007,
ApJ, 663, L77.

Magnetic Energy Dissipation in the Outer Crust of Neutron Stars
TAKAHASHI R. Hiroyuki(NAOJ)

Pushed by the accumulating observations of radio
pulsars and accreting neutron stars (NSs), extensive
studies have been performed to understand the evolutionof magnetic fields in neutron stars. The radio pulsars are
generally categorized into two classes: young (< 107 yr)
pulsars with the magnetic field strength B  1010~13 G, andthe old millisecond radio pulsars, which have magnetic
field strength as low as 10 8~9 G. While most radio
pulsars are isolated objects, the millisecond pulsars are
predominantly in binaries, suggesting that the magnetic
fields decay with time, perhaps by an accretion of matterfrom the binary companion.
For the isolated radio pulsars, it remains as an open
question whether the NS magnetic fields do or do notdecay with time. Recently, the discovery of magnetars,
which would be a isolated NS with stronger magnetic
fields (B ~ 1015 G) has provided evidences for magnetic
energy dissipation in neutron star[1], whose timescale is~10 Myr[2]. At present, these ideas and new observations
seem to favor the existence of the magnetic field decay inthe isolated NSs.
Goldreich & Reisenegger[3] proposed a pioneeringmodel of the magnetic field decay inside NSs, in which
the large scale magnetic field is affected by the Hallturbulence. The magnetic energy is transported to thesmaller scale due to the Hall cascade, leading to thedissipation via the Ohmic dissipation. The existence ofHall turbulence and the cascading process are numericallyconfirmed by electron Magnetohydrodynamic (EMHD)
simulations[4]. However, the dissipation process, whichshould govern the magnetic field decay in NSs, cannot betreated consistently due to the MHD approximations.
In this paper, we perform Particle-In-Cell (PIC)
simulations aiming to understand the decaying process inNSs[5]. Since the Maxwell equations and the equationsof motion of plasma particles are consistently solved in
PIC simulations, we can study the dissipation process
without introducing phenomenological parameter (i.e.,
the electric resistivity).
Figure 1 shows numerical results of PIC simulations.
Color shows the magnetic energy of turbulent fields andwhite curves denote for the magnetic field lines at theinitial (left) and final (right) states. The initial magnetic
field is consist of the uniform field that models the global
field penetrating the NS and of the turbulent field thatwould be originated from the Hall cascade. The energy
of initially imposed turbulent field is transported to thesmaller scale through whistler waves. Since whistler
waves propagate almost parallel to the global magnetic
field lines, the cascading process becomes anisotropic.

When the turbulent energy is cascaded down to theelectron inertial scale, the magnetic energy is dissipated
and the electrons are heated. The electrons with lower
energy are heated in parallel to the magnetic field
due to the Landau damping, while the electrons withhigher energy is heated perpendicular to the magnetic
field lines due to the cyclotron resonance. These two
dissipation mechanisms make the electron distributionfunction anisotropic. Such the anisotropy of electron
temperature is observed in magnetars, suggesting that theplasmas near the surface of NSs is heated by dissipation
processes described above. Since the time scale of these
dissipation processes is much shorter than the observed
decay timescale, we speculate that the decay time scale isdetermined by the cascading time.

Figure 1: Numerical results of PIC simulations. Color and curves
show the turbulent magnetic field energy and magnetic
field lines at the initial (left) and final (right) states.

References[1] Pons, J. A., Miralles, J. A., Geppert, U.: 2009, A&A, 496, 207.
[2] Thompson, C., Duncan, R. C.: 1996, ApJ, 473, 322.
[3] Goldreich, P., Reisenegger, A.: 1992, ApJ, 395, 250.
[4] Cho, J., Lazarian, A.: 2004, ApJ, 615, L41.
[5] Takahashi, H. R., Kotake K., Yasutake N.: 2011, ApJ, 728, 151.

I Scientific Highlights

055Constraints on the neutrino mass and the primordial magnetic field
				
			

YAMAZAKI, Dai G.
(NAOJ)		

KAJINO, Toshitaka(NAOJ/University of Tokyo)

Recently cosmological observations and groundexperiments constrain the neutrino-mass of order < 0.1–
1 eV. If the velocities of such finite-mass neutrinos withthe finite-mass are enough large, the time evolution ofdensity fluctuations in the neutrinos free-streaming scale
will be impeded. Therefore it is very important to limit
the neutrino mass. At the same time, magnetic fields havebeen observed in clusters of galaxies with a strength of
0.1–1.0 μG. One possible explanation for such magnetic
fields in galactic clusters is the existence of a primordial
magnetic field (PMF) of order 1 nG whose field lines
collapsed as the cluster formed. The PMF could haveinfluenced a variety of phenomena in the early universe
such as the cosmic microwave background (CMB)[1],and the formation of the large scale structure (LSS)[2].
In this regard, the alternative normalization parameter
σ8 is of particular interest as a measure of large-scale
structure effects. It is defined as the root-mean-squareof the matter density fluctuations in a comoving sphereof radius 8h −1 Mpc. It is determined by a weighted
integral of the matter power spectrum. Observations
which determine σ 8 provide information about thephysical processes affecting the evolution of densityfield fluctuations and the formation of structure on
cosmological scales.
In this article, We consider the effect of a PMF on σ8
and compare theoretically deduced values for σ8 with theobserved range. In this way we show that the degeneracy
between the effects of a PMF and that of a finite neutrinomass on the matter density fluctuations can be effectively
broken by combining the analysis with the CMB data at
higher multipoles. We thus obtain not only insight into theunderlying physical processes of density field fluctuationsin the presence of a PMF, but also place new constraints
on the amplitude and spectral index of the PMF and thesum of neutrino mass[3].
Figure 1 shows the constraints on the PMF parameterBλ and the sum of neutrino masses Σmν for various fixedvalues of nB and ranges of σ8 as the caption. The expectedparameters of the PMF from the combined analysis of the
CMB and observed magnetic fields in galactic clusters
is Bλ < 2.0 nG(1σ) and < 3.0 nG(2σ), while the expectedvalue of σ8 based upon observations is 0.75 < σ8 <0.85.
For this range of σ8, the sum of the neutrino masses isconstrained to be ∑ Nν mν < 0.11 eV without the PMF. On
the other hand, considering the PMF, from Fig. 1, the sumof the neutrino masses is constrained to be ∑ Nν mν < 0.24
eV on nB = −1.5 and < 0.6 eV on nB = −2.5 for Nν = 3.

056

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ICHIKI, Kiyotom(Nagoya University)

MATHEWS, Grant J.

(University of Notre Dame)

This is a larger upper limit than that deduced previously
because the effect of the PMF cancels the effect ofneutrinos on the density fluctuations.
We confirm that the upper limit on the neutrino massfrom σ8 in the presence of a PMF is heavier than withouta PMF even if we consider the matter contributions. We
also have shown that the prior limited range on the sumof neutrino masses and PMF parameters is within the
expected range for σ8 from observations of the LSS. In
principle, by applying our method to future observations
it will be possible to obtain not only the upper but also
the lower limits to the neutrino mass from cosmology inthe presence of a PMF.

Figure 1: Excluded and allowed regions of ranges for σ8 in theparameter plane of PMF amplitude B λ vs. mass ofneutrinos ∑ Nν = 3 mν. nB is the power-law spectral index
of the PMF. All painted Regions indicate ranges of σ8
as 0.75 < σ8 < 0.85 and gray, sky blue and blue ragions
show Bλ > 3.0 nG, 2.0 nG < Bλ < 3.0 nG and Bλ < 2.0 nG,
respectively.

References[1] Yamazaki, D. G., et al.: 2010, Phys. Rev. D, 81, 023008.
[2] Yamazaki, D. G., et al.: 2008, Phys. Rev. D, 78, 123001.
[3] Yamazaki, D. G., et al.: 2010, Phys. Rev. D, 81, 103519.

A Novel Jet Model: Magnetically Collimated,
Radiation-Pressure Driven Jet
TAKEUCHI, Shun
(Kyoto University)

OHSUGA, Ken(Graduate University for Advanced Studies / NAOJ)

Relativistic jets from compact objects are ubiquitous
phenomena in the Universe, but their driving mechanism
has been an enigmatic issue over many decades. There
are two models proposed: magnetohydrodynamic (MHD)jets which are driven by the magnetic process[1] andradiation-hydrodynamic (RHD) jets which are poweredby the strong radiation-pressure force[2].
In the MHD jets, the magnetic effects work toaccelerate and collimate the jets. However, we should
remark that most of the previous MHD disk-jet
simulations assumed that the underlying accretion flows
are radiatively inefficient accretion flow (RIAF)[3,4]. The
MHD jets launched from the RIAF can not account for
the highly relativistic jets of the Galactic microquasars,
since their high luminosities implies that the central black
holes are surrounded by the luminous accretion disks.
The luminous (super-Eddington) accretion flows drive
the RHD jets. However, the opening angle of the RHD
jets is thought to be relatively wide, since the there is noeffective collimation mechanism.
Here, we propose a new type of jets, radiationmag
netohydrodynamic (RMHD) jets, based on our global
RMHD simulation of luminous accretion flow onto a
black hole shining above the Eddington luminosity[5].
In Figure 1, the accretion flow (the gas mass density,
brown) and the RMHD jet in which velocities exceed
the escape velocity (the velocity, white, blue) are plotted.
The high-speed jet (~0.6c–0.7c) is represented by blue.
White lines indicate the magnetic field lines. The zzcomponent of the radiation-pressure tensor (color), P0zz ,overlaid with the radiation-pressure force vectors (arrows)
on the meridional plane is projected on the left wall
surface, while the magnetic pressure from the azimuthalcomponent of the magnetic field (color), Bφ2 /8�, overlaid
with the Lorentz force vectors (arrows) on the meridional
plane is projected on the right wall surface.
We find that the RMHD jet can be accelerated up to
the relativistic speed by the radiation-pressure force andis collimated by the Lorentz force of a magnetic tower,
inflated magnetic structure made by toroidal magnetic
field lines accumulated around the black hole, thoughradiation energy greatly dominates over magnetic energy.
This magnetic tower is collimated by a geometricallythick accretion flow supported by radiation-pressure
force. This type of jet may explain relativistic jets from
Galactic microquasars, appearing at high luminosities.

MINESHIGE, Shin
(Kyoto University)

Figure 1: Bird’s-eye view of the luminous accretion flow andthe associated RMHD jet. The RMHD jet (blue) is
accelerated by the strong radiation-pressure force fromthe super- Eddington disk (brown) and is collimated by
the Lorentz force of a magnetic tower (white lines).

References[1] Lovelace, R. V. E.: 1976, Nature, 262, 649.
[2] Bisnovatyi-Kogan, G. S., Blinnikov, S. I.: 1977, A&A, 59, 111.
[3] Ichimaru, S.: 1977, ApJ, 214, 840.
[4] Narayan, R., Yi, I.: 1994, ApJ, 428, L13.
[5] Ohsuga, K., Mineshige, S., Mori, M., Kato, Y.: 2009, PASJ, 61,
L7.

I Scientific Highlights057

Formation of Terrestrial Planets from Protoplanets
under a Realistic Accretion Condition				

KOKUBO, Eiichiro(NAOJ)		

It is generally accepted that the final stage ofterrestrial planet formation is the giant impact stage
where protoplanets or planetary embryos formed byoligarchic growth collide with one another to form planets[1,2]. This stage has been mainly studied by N-bodysimulations. So far all N-body simulations have assumed
perfect accretion in which all collisions lead to accretion.
However, this assumption would be inappropriate forgrazing impacts that may result in escape of an impactor
or hit-and-run. By performing Smoothed-Particle
Hydrodynamic (SPH) collision simulations, [3] estimatedthat more than half of all collisions between like-sized
protoplanets do not simply result in accumulation of alarger protoplanet, and this inefficiency lengthens thetimescale of planet formation by a factor of 2 or more,
relative to the perfect accretion case. The accretion
inefficiency can also change planetary spin. [4] foundthat under the assumption of perfect accretion, thetypical spin angular velocity of planets is as large as thecritical spin angular velocity for rotational instability.
However, in reality, the grazing collisions that have highangular momentum are likely to result in a hit-and-run,
while nearly head-on collisions that have small angularmomentum lead to accretion. In other words, small
angular momentum collisions are selective in accretion.
Thus, the accretion inefficiency may lead to slower
planetary spin, compared with the perfect accretion case.
We clarify the statistical properties of terrestrial
planets formed by giant impacts among protoplanets
under a realistic accretion condition[5]. We derive an
accretion condition for protoplanet collisions in terms ofcollision parameters, masses of colliding protoplanets
and impact velocity and angle, by performing collisionexperiments with an SPH method. We implement therealistic accretion condition in N-body simulations
and probe its effect to further generalize the model ofterrestrial planet formation. We derive the statistical
dynamical properties of terrestrial planets from resultsof a number of N-body simulations and compare theresults with those in [6] and [4] where perfect accretion isadopted.
For the standard protoplanet system, the statisticalproperties of the planets obtained are the following.
About half of collisions in the realistic accretion model do
not lead to accretion. However, this accretion inefficiency
barely lengthens the growth timescale of planets. The
numbers of planets and Earth-sized planets are n  3–4
and nM  2, respectively. The growth timescale is about
6–7 × 107 years. The masses of the largest and second-058

I Scientific Highlights

GENDA, Hidenori(University of Tokyo)

largest planets are M1  1.2 M⊕ and M2  0.7 M⊕. The
largest planets tend to form around a1  0.8 AU, while
a2 is widely scattered in the initial protoplanet region.
Their eccentricities and inclinations are  0.1. These
results are independent of the accretion model. The RMS
spin angular velocity for the realistic accretion model
is about 30% smaller than that for the perfect accretion
model that is as large as the critical spin angular velocity
for rotational instability (Fig. 1). The spin angularvelocity and obliquity of planets obey Gaussian andisotropic distributions, respectively, independently of theaccretion model.

Figure 1: Average spin angular velocity of all planets formed in
the 50 runs of the realistic (circle) and perfect (square)
accretion models is plotted against their mass M withmass bin of 0.1 M⊕. The error bars indicate 1-σ and thedotted line shows ωcr. [5]References[1] Wetherill, G. W.: 1985, Science, 228, 877.
[2] Kokubo, E., Ida, S.: 1998, Icarus, 131, 171.
[3] Agnor, C., Asphaug, E.: 2004, ApJ, 613, L157.
[4] Kokubo, E., Ida, S.: 2007, ApJ, 671, 2082.
[5] Kokubo, E., Genda, H.: 2010, ApJ, 714, L21.
[6] Kokubo, E., Kominami, J., Ida, S.: 2006, ApJ, 642, 1131.

N-body Simulation of Planetesimal Formation
Through Gravitational Instability of a Dust Layer in Laminar Gas Disk
MICHIKOSHI, Shugo, KOKUBO, Eiichiro				(NAOJ)				

In the standard scenario of planet formation,planetesimals are the precursors of planets. Their
formation process is one of the unsolved problems of
the planet formation theory. Beginning with micronsized dust grains, they grow to centimeter size in a
protoplanetary disk via collisional agglomeration. The
least understood growth phase is growth from centimetersize to kilometer size.
One of the possible models for planetesimal formationis the gravitational instability model. A very thin anddense layer of settled dust aggregates in the mid-plane ofthe protoplanetary disk may be gravitationally unstable.
Then the gravitational collapse of the dust layer occurs,
and kilometer-sized planetesimals are formed directly.
This scenario has the advantage of a very rapid formation
timescale, which is on the order of the Keplerian time.
The linear analyses of the gravitational instability of
dust layers have been performed extensively[1]. However,the nonlinear stage of the gravitational instability has notbeen studied well. We have investigated the planetesimalformation by gravitational instability by local N-bodysimulations[2,3]. In this study, we have considered theeffect of gas drag force[4].
According to the linear analysis of gravitational
instability without gas drag force, the stability of the disk
is characterized by Toomre’s Q value. When Q < 1, thedisk is unstable. On the other hand, the linear analysis
with gas drag force shows that the dust layer is always
secularly unstable although Toomre’s Q value is larger
than unity.
In the initial stage, the growth time of the gravitational
instability is longer than the timescales of the dust
sedimentation and the decrease of the velocity dispersion.
Thus, the velocity dispersion decreases and the disk
shrinks vertically. As the velocity dispersion becomes
sufficiently small, the gravitational instability finallybecomes dominant.
We found that the the formation process is divided
into three stages qualitatively: the formation of wakelike
density structures, the creation of planetesimal seeds, andtheir collisional growth.
The top-right panel of Figure 1 shows the first stageof the planetesimal formation. The non-axisymmetricdensity structures appear. These structures are wellknown in the dense planetary rings, which are caused by
the gravitational instability.
As shown in the left-bottom panel of Figure 1, in thedense part of wakes, the wakes break into many fragment
due to self-gravity. These are the planetesimal seeds.

INUTSUKA Shu-Ichiro(Nagoya University)

After the formation of planetesimal seeds, the rapid
collisional growth begins. Several large planetesimals areformed and absorb almost all small particles.

Figure 1: The snapshots of the N-body simulation of the planetesimal formation at t = 0.0 TK (top-left), t = 0.4 TK (topright), t = 0.8 TK (bottom-left), t = 1.2 TK (bottom-right),
where TK is Keplerian period.

References[1] Sekiya, M.: 1983, Prog. Theor. Phys., 69, 1116.
[2] Michikoshi, S., et al.: 2007, ApJ, 657, 521.
[3] Michikoshi, S., Kokubo, E., Inutsuka, S.-i.: 2009, ApJ, 703,
1363.
[4] Michikoshi, S., Kokubo, E., Inutsuka, S.-i.: 2010, ApJ, 719,
1021.

I Scientific Highlights059

Light Element Synthesis in Core-collapse Supernovae			

NAKAMURA, Ko

YOSHIDA, Takashi, SHIGEYAMA, Toshikazu(NAOJ)				

(University of Tokyo)

KAJINO, Toshitaka(NAOJ / Graduate University for Advanced Studies)

Most of elements lighter than iron are synthesized via
thermonuclear burning reactions in stars. Light-elementisotopes such as Li, Be, and B (LiBeB) are, however,not produced in stellar burning phase because of theabsence of stable nuclei with mass number of 8 and thefragility of 7Li against hot proton. They are known tobe produced from some cosmological and astrophysicalprocesses: 7Li from big bang nucleosynthesis; 7Li and 11B
from asymptotic giant branch (AGB) stars and novae;
and all stable isotopes of LiBeB from Galactic cosmicray(CR) nucleosynthesis. Another possible candidate is
the neutrino-induced nucleosynthesis in core-collapse
supernovae, where a fraction of neutrinos emitted forma proto-neutron star would interact with stellar materials
and produce 11B in inner C-rich shells and 7Li in He-richenvelopes (Figure 1).
The supernova neutrino process is necessary to
account for the high 11 B-to- 10 B ratio observed inmeteoritres. We investigated the neutrino process in
Type Ic supernovae (SNe Ic), which should be terminal
explosion of massive stars without H and He envelopes,
to evaluate accurately the contribution of the neutrino
process to Galactic Li(Be)B. Previous studies werelimited in Type II explosions and this is the first report on
the neutrino process in SNe Ic.
We consider a very energetic explosion of a 15 M
C/O star with the explosion energy E ex = 3 × 10 52 erg
corresponding to SN 1998bw. The explosion is simulatedwith 1-dimensional special-relativistic hydrodynamic
code and nucleosynthesis is calculated as a postprocess.
We assume a supernova neutrino model that neutrino
luminosity decreases exponentially with a time scale of
3 s and that the neutrino temperature of each species does
not change with time.
Our results[1] show that light elements are produced
via the neutrino process both in the innermost region
and in the outer envelope. In the innermost region, 4He
coming from α-rich freezeout is excited by neutrinos thendecays to 3H and 3He, followed by α-capture reactions to
produce 7Li and 7Be. In the outer layers, neutral current
reactions of neutrinos produce 11B (and 11C). SNe Ic can
produce LiBeB also by spallation reactions[2]. Resulting
yield of 11 B from our SN 1998bw model with total
neutrino energy of 3 × 1053 erg is about 1.6 × 10−6 M,which is comparable to the value estimated from typicalSNe II model[3].
However, the frequency of highly energetic SNe Ic isquite low and borons in meteorites should be dominated060

I Scientific Highlights

by those that originated from SNe II and Galactic
CRs. Contribution from SNe Ic might be outstanding
in metaldeficient stars because an SN Ic progenitor issurrounded by its wind material and the light elements
produced in the explosion are likely to be inherited
directly by next generations of stars, which would showhigh BeB abundances as a Be-rich halo star HD106038[4].

Figure 1: Nuclear reaction chain associated with LiBeB. left:
Reactions in H and He burning. right: Neutrino-induced
reactions producing 7Li and 11B.

References[1] Nakamura, K., et al.: 2010, ApJ, 718, L137.
[2] Nakamura, K., Shigeyama, T.: 2004, ApJ, 610, 888.
[3] Rauscher, T., et al.: 2002, ApJ, 576, 323.
[4] Smiljanic, R., et al.: 2008, MNRAS, 385, L93.

Quantum Statistical Corrections to
Astrophysical Photodisintegration Rates
			

MATHEWS, Grant J.

(University of Notre Dame)

BALANTEKIN, A. B.

(University of Wisconsin)		

PEHLIVAN, Yamac(Mimar Sinan Fine Arts University)

KAJINO, Toshitaka

KUSAKABE, Motohiko(NAOJ/University of Tokyo)

Tabulated rates for astrophysical photodisintegration
reactions make use of Boltzmann statistics for thephotons involved as well as the interacting nuclei. In
this work[1] we have derived analytic corrections for
the Planck-spectrum quantum statistics of the photon
energy distribution. These corrections can be deduced
directly from the detailed-balance condition without
the assumption of equilibrium as long as the photons
are represented by a Planck spectrum. Moreover wehave shown that these corrections affect not only thephotodisintegration rates but also modify the conditionsof nuclear statistical equilibrium as represented in the
Saha equation. We deduced new analytic corrections tothe classical Maxwell- Boltzmann statistics which caneasily be added to the reverse reaction rates of existing
reaction network tabulations.
The key expressions in this work are the determinationof revised thermonuclear reaction rates as,(University of Tokyo)

e.g. near the neutron or proton drip lines. To the extent
that such nuclei are beta-decay waiting points, forexample, the altered statistics will affect the timescale forthe build up of abundances. Another possible applicationof the corrections deduced here is for the ionization
equilibrium of atomic or molecular species with a low
ionization potential in stellar atmospheres.
We have examined possible effects of these corrections on the r-process, the rp-process, explosive siliconburning, the γ-process, and big bang nucleosynthesis. We
find that, in most cases one is quite justified in neglecting
these corrections. The correction is largest for reactions
near the drip line for an r-process with very high neutron
density, or an rp-process at high-temperature[1] .
136

Cd(n,γ)

137

Cd

10

(1)
1

R

where T 9 is the temperature in units of 10 9 K, N A is
Avagadro’s number, [N A σv(T 9 )*] is the tabulated
thermonuclear reaction rate[2] in units of cm3 mol−1 s−1,
Q is in units of MeV, and μ̂ is the reduced mass in atomic
mass units. There is also a revised Saha equation of NSE

0.1

0.01

(2)
The quantity R in the Egs. (1) and (2) is the newcorrection for the difference between Maxwell Boltzmann
and Planckian statistics for the photons. We have shown[1] that this correction factor can be written

0

1

2

3

4

5

T9

6

7

8

9

10

Figure 1: Correction factor R for the reverse rate of the 136Cd(n, γ)
137
Cd reaction relevant to the r-process abundance peaknear A = 130 for a high neutron-density environment.
This was generated from Eq. (3) using the REACLIB
compilation[2]. For typical r-process temperatures, T9 ~1–2, the correction is ~6%.

(3)
The advantage of writing the expression this way is that it
can be quickly deduced from existing reaction rate tables
such as REACLIB[2].
The deviation of photodisintegration and NSE due toquantum statistics may impact the evolution of explosive
nucleosynthesis environments for which one canencounter nuclei with small photodissociation thresholds,

References[1] Mathews, G., et al.: 2011, ApJ, 727, 10.
[2] Cyburt, et al.: 2010, ApJ, 89, 240; (REACLIB): http://groups.
nscl.msu.edu/jina/reaclib/db/

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061

Origin of Chirality of the Amino Acids
BOYD, Richard N.

(Lawrence Livermore National Lab., University of California)
			

KAJINO, Toshitaka(NAOJ/University of Tokyo)

Half a century ago it was demonstrated by Miller[1] and Urey that at least some of the 20 amino acids onwhich we depend for life could be produced in a spark
discharge in a chemical environment that may haveexisted early in the Earth’s history. Thus the model ofsuch an environment in a lightning storm became theaccepted means for producing amino acids on Earth.
However, the amino acids have been found to have a lefthanded chirality, whereas the Miller-Urey mechanism
produces equal numbers of left- and right-handed
molecules. Furthermore, amino acids have been foundin meteorites[2], and those that have a preferred chirality
had more lefthanded molecules than right-handed
molecules (at a level of 10%). Several mechanisms havebeen suggested as being the means by which the aminoacid chirality is established. One widely accepted one
involves circularly polarized light impinging on themolecules that are produced on Earth, although circularly
polarized x-rays in the interstellar medium have also beensuggested as a driver of chirality.
However, during the past several years, we havedeveloped a model[3,4] for establishing amino acidchirality in the interstellar medium by selective molecular
destruction of one chirality by neutrinos from asupernova. In this model, the strong magnetic field fromthe protoneutron star would orient the 14N nuclei thatare common to the amino acids to produce a significant
fraction of those nuclei with their spins aligned with theneutrino spin. Neutrino helicity is a conserved quantum
number, which is aways −1 for neutrinos and +1 forantineutrinos, namely the symmetry of left- or righthandedness is maximally broken in nature.
Angular momentum conservation requires thatthe ν + 14N → 14C + e+ reaction (ν denotes an electron
antineutrino) requires transfer of one unit of angularmomentum from the neutrino wave function when thespins are aligned, whereas the reaction could proceedwith no angular momentum transfer when the spins are
not aligned. This inhibits the reaction by roughly anorder of magnitude for the aligned case, skewing themagnetic substate distribution in favor of one 14N spin
configuration and, therefore, one molecular chirality[5].
The intense magnetic field also modifies the antineutrino
cross sections, thereby creating an antineutrino flux that is
asymmetric by 3%[6]. This combination of effects would
create a small chirality preference; we estimate it to be a
maximum of 1 × 10−6.
While the Galactic supernovae are not capable062

I Scientific Highlights

Onaka, Takashi(University of Tokyo)of processing all the molecules in the galaxy, several
mechanisms exist for amplifying this chirality preference,and for spreading it throughout the Galaxy. It is also
believed[3,4] that once a chirality preference wasestablished on Earth, more amplification would drive that
preference to homochirality.

Figure 1: Schematic diagram of the magnetic fields, B, surrounding a nascent neutron star and the spins of the 14N
nuclei, SN, and of the neutrinos, Sν, emitted from thecollapse of the supernova that created the neutron star.

References[1] Miller, S. L.: 1953, Science, 117, 528.
[2] Cronin, J. R., Pizzarello, S.: 1997, Science, 275, 951.
[3] Boyd, R. N., Kajino, T., Onaka, T.: 2010, Astrobiology, 10, 561.
[4] Boyd, R. N., Kajino, T., Onaka, T.: 2011, Int. J. Mol. Sci., 12,3432.
[5] Buckingham, A. D.: 2004, Chem. Phys. Lett., 398, 1.
[6] Maruyama, T., et al.: 2011, Phys. Rev. D, 83, 081303(R).

Recurrent Planet Formation and Intermittent Protostellar Outflows
MACHIDA, Masahiro(Kyushu University)

Since 1995, over 550 exo-planets have been discovered.
It is considered that a large fraction of exo-planets are thegas giant planet. Recently, some planets were observed
by SUBARU telescope with direct image. They orbit at>10 AU far from the central star. However, the classicalplanet formation theory cannot explain the formation ofsuch planets. To understand the formation of such planets,
we need to consider the formation of the circumstellar
disk, in which planet forms. In this study, we investigated
the formation of the circumstellar disk from the prestellar
cloud stage. As the initial state, we adopted the spherical
cloud. Then, we added the rotation and magnetic fieldcomparable to the observation to this cloud.
As a result of calculation, we found that dissipationof the magnetic field is closely related to the formation of
the gas giant planet[1]. Our previous studies showed thatthe first core that is formed before the protostar formation
is directly transformed into the circumstellar disk after the
protostar formation[2,3]. At the moment of the birth ofthe protostar, the circumstellar disk is more massive thanthe protostar and is gravitationally unstable. However,when the initial cloud is very weakly (or no) magnetized,a spiral structure develops in the circumstellar disk, andit effectively transfers the angular momentum outward.
Then, the gas in the circumstellar disk falls onto thecentral star and the surface density gradually decreases.
Therefore, the circumstellar disk becomes stable against
gravity and suppresses fragmentation or the gas giant
planet formation.
On the other hand, when the magnetic field dissipatesin the circumstellar disk, fragmentation occurs and thegas giant planet appears. The circumstellar disk has alower surface density in the outer disk region where
the ionization degree is relatively high and magnetic
field is well coupled with neutral gas. Thus, the angularmomentum in such region effectively transfers by themagnetic braking, and the gas can flow into the innerdisk region. In addition, the magnetic field drives the
protostellar outflow as shown in Figure 1. The magnetic
field is decoupled from the neutral gas in the innerdisk region, because higher surface density lowers theionization degree. In such a region, the magnetic fielddissipates by the Ohmic dissipation. As a result, theangular momentum transfer due to the magnetic field
is not effective. Thus, the gas accumulates and the disk
surface density continues to increase because the gas
flows from the outer region. Finally, the disk becomes
highly unstable against the gravity and fragmentation
occurs to form the gas giant planet. However, afterfragmentation, the protoplanet falls onto the protostar

because the massive disk gravitationally interacts with
protoplanet. After the falling, fragmentation occurs andprotoplanet appears again. The planet formation and its
falling onto the protostar last until the infalling gas isdepleted. It is considered that the planet appeared justbefore the infalling envelope is depleted evolves into
the gas giant planet orbiting the region far from thecentral star. In addition, protoplanet’s motion disturbs
the protostellar outflow. The protostellar outflow
synchronizes with the orbital motion of the protoplanet.
We may confirm the existence of the protoplanet and its
orbital motion from the intermittent outflow.

Figure 1: Gas giant planet formation due to the gravitational
instability in the protoplanetary disk. Color and lines
represent the gas density and magnetic field line,
respectively. The yellow structure above the disk
indicates the protostellar outflow.

References[1] Machida, M. N., Inutsuka, S., Matsumoto, T.: 2011a, ApJ, 729,
42.
[2] Machida, M. N., Matsumoto, T.: 2011b, MNRAS, 413, 2767.
[3] Machida, M. N., Inutsuka, S., Matsumoto, T.: 2010, ApJ, 724,
1006.

I Scientific Highlights063

Dust and Chemical Abundances of the Sagittarius Dwarf Galaxy
Planetary Nebula Hen2-436
OTSUKA, Masaaki, MEIXNER, Margaret				

HYUNG, Siek

(STScI)			

TAJITSU, Akito, IZUMIURA, Hideyuki(Chungbuk National University)				

(NAOJ)We have estimated elemental abundances and dust
mass of the planetary nebula (PN) Hen2-436 in the
Sagittarius (Sgr) spheroidal dwarf galaxy using ESO/VLTFORS2, Magellan/MMIRS, and Spitzer/IRS spectra.
We have detected candidates of fluorine [F II]λ4790,
krypton [Kr III]λ6826, and phosphorus [P II]λ7875 lines
and successfully estimated the abundances of theseelements for the first time. These elements are known
to be synthesized by neutron capture process in the Herich intershell during the thermally pulsing AGB phase.
We present a relation between C, F, P, and Kr abundancesamong PNe and C-rich stars. The detections of F and Kr
in Hen2-436 support the idea that F and Kr together with
C are synthesized in the same layer and brought to thesurface by the third dredge-up (Fig. 1).

and the age is ~3000 yr after the AGB phase. The observed
elemental abundances of Hen2-436 can be explainedby a theoretical nucleosynthesis model with a star of
initial mass 2.25 M, Z = 0.008 and LMC compositions.
We have estimated the dust mass to be 2.9 × 10 −4 M (amorphous carbon only, Fig. 2a) or 4.0 × 10 −4 M (amorphous carbon and PAH, Fig. 2b). Based on theassumption that most of the observed dust is formed
during the last two thermal pulses and the dust-to-gas
mass ratio is 5.58 × 10 −3, the dust mass-loss rate andthe total mass-loss rate are < 3.1 × 10.8 M  yr −1 and< 5.5 × 10.6 M  yr −1, respectively. Our estimated dust
mass-loss rate is comparable to a Sgr dwarf galaxy AGB
star with similar metallicity and luminosity[1].

Figure 1: (a): The [F/Ar]–[C/Ar] diagram. The typical error isindicated by the cross (the same for the other diagrams).
BoBn1 is a Sgr PN. (b): The [P/Ar]–[C/Ar] diagram. (c):The [Kr/Ar]–[C/Ar] diagram.

Figure 2: The predicted SED from Cloudy modelings (blue lines).
The observed data are indicated by the black lines
or circles. In the inner small boxes we plot the radio
data and the predicted SED. (a) The predicted SED by
Cloudy considering amorphous carbon only. (b) The
predicted SED considering amorphous carbon and PAH
grains.

To investigate the status of the central star of the PN,
nebula condition, and dust properties, we construct atheoretical spectral energy distribution (SED) model tomatch the observed SED with Cloudy. By comparing
the derived luminosity and temperature of the central starwith theoretical evolutionary tracks, we conclude that theinitial mass of the progenitor is likely to be ~1.5–2.0 M
064

RIEBEL, David(Johns Hopkins University)

I Scientific Highlights

Reference[1] Otsuka, M., et al.: 2011, ApJ, 729, 39.

Polarization Interferometric nulling coronagraphfor high-contrast imaging
		

MURAKAMI, Naoshi(Hokkaido University)

NISHIKAWA, Jun, TAMURA, Motohide

				
		

(NAOJ)		

TAKEDA, Mitsuo(The University of Electro-Communications)

We propose a novel nulling interferometer based onpolarization interferometry, which we call a polarizationinterferometric nulling coronagraph (PINC), for direct
detection of extrasolar planets[1]. The PINC is a fullysymmetric modified Michelson interferometer using
polarizing beam splitters (PBS), in which achromatic
half-wave plates (HWP) such as Fresnel rhombs are
installed. Two crossed polarizers (± 45°) are also installedin front of and behind the interferometer. The HWPs
provide an achromatic π-phase difference between twolight beams from subapertures (SA1, SA2) extracted froma telescope pupil, and eliminate an on-axis star light(Fig. 1, top).
From Jones calculus, the achievable contrast of the
PINC has been estimated to be about 10−10 at 5 λ/D over a

YOKOCHI, Kaito(Tokyo University of Agriculture and Technology/NAOJ)KUROKAWA, Takashi(Tokyo University of Agriculture and Technology)

BABA, Naoshi(Hokkaido University)

wavelength range from 1.6 to 2.2 μm. We also carried out
laboratory experiments on the PINC using two laser lightsources (wavelengths of λ = 532 and 671 nm). Figure1(bottom) shows a picture of the laboratory simulator of
the PINC. As the HWPs, we used commercially-available
Fresnel rhombs made of BK7. Figure 2a,b shows resultsof the laboratory experiments. As a result, we obtained
a halo suppression level of about 10−6 at 5 λ/D for both
wavelengths.
The experimentally acquired contrast curves(Fig. 2a,b) were well fitted to those of the computer simulations assuming a phase aberration of 3 nm rms andan optical-path difference (OPD) error of 3.7 nm (Fig.
2a’,b’). Thus it is expected that higher contrasts will be
realized by introducing a high-performance OPD control
and an extreme adaptive optics system.

Figure 2: Experimental results of laboratory demonstrations: (left)
acquired coronagraphic images and (right) radial profilesof coronagraphic images obtained by (a,b) experimentsand (a’,b’) numerical simulations.

Reference[1] Murakami, N., et al.: 2010, Appl. Opt., 49, D106.

Figure 1: (Top) A principle and (bottom) a laboratory simulator of
the PINC.

I Scientific Highlights

065

Speckle level suppression using an unbalanced nulling interferometerin a high-contrast imaging system
YOKOCHI, Kaito

MURAKAMI, Naoshi(Tokyo University of Agriculture and Technology / NAOJ)(NAOJ)		

TAKEDA, Mitsuo(The University of Electro-Communications)

High-contrast imaging systems with a stellar halo
suppression level of 10−10 are required for direct detectionof Earth-like extra-solar planets. Here λ/10000 rms
wavefront quality is required for the optics to suppress
the speckle level, and a coronagraph will be used toreduce the diffracted light of a parent star.
We investigated a novel high-contrast imaging systemwith an unbalanced nulling interferometer (UNI) followedby phase and amplitude correction (PAC) adaptive
optics (AO), which not only can reduce starlight but also
can suppress the speckle level by a virtual wavefront
correction beyond the limit of the AO performance[1].
The present system consists of four stages, i.e., afirst AO, the UNI, the PAC AO, and a final coronagraph(Fig. 1). In the experiments the UNI adopted a modified
lateral shearing Mach-Zehnder interferometer which
we call PINC (Polarization Interferometric Nulling
Colonagraph[2]. We did not use the first AO here. We
confirmed that the aberrations of the input wavefront
were sufficiently magnified by the UNI, cf., λ/100 rms
to λ/16 rms, thanks to the amplitude difference between
the two wavefronts which were split and combined in the
UNI.
Next at the PAC AO system, the magnified aberrations
were effectively corrected in amplitude and phase withtwo deformable mirrors (Boston Micromachines Corp.)
to the initial aberration level of λ/100 rms (Fig. 2). Herethe electric field distribution was suppressed to λ/550 rms
virtually by the product with the reduced mean amplitudeafter the UNI, although the observed aberration level
was identical to the initial wavefront (AO performance).
According to the pupil plane field, the suppression levelof the speckle pattern at the focus of the final coronagraph(3D Sagnac nulling interferometer) was 7.0 × 10−4, which
was 0.073 times reduction from the initial (AO-limited)
DeformablemirrorCorrected
wavefronts
Arm1

Aberration-magnified
Re-corrected
wavefronts
wavefronts
DM2

ND
Incoming
wavefronts
Telescope

WFS
Arm2First adaptive optics
(AO)

UNI

DM1
WFS
PAC (Second AO) Nulling interferometeror coronagraph

Figure 1: Schematic of coronagraph optics with UNI (unbalanced
nulling interferometer).

066

I Scientific Highlights

ABE, Lyu

TAVROV, Alexander(University of Nice)(Space Research Institute)

KUROKAWA, Takashi(Tokyo University of Agriculture and Technology)

level of 9.5 × 10−3.
Thus we demonstrated that the wavefront correction
after the aberration magnification by the UNI can reduce
the wavefront aberrations and the speckle level beyond
the limit of the AO performance, and the UNIPAC would
be an effective wavefront correction method in highcontrast imaging systems.

0.6
0.4
Imaginary part [a.u.]

NISHIKAWA, Jun, TAMURA, Motohide			(Hokkaido University)

UNI

0.2
0

PAC
Arm1

Arm2

-0.2
-0.4
-0.6

0

0.2

0.4
0.6
0.8
Real part [a.u.]1

1.2

Figure 2: Electric field changes with the UNI (unbalanced nullinginterferometer) and PAC (phase amplitude correction)
processes.

References[1] Yokochi, K., et al.: 2011, Opt. Express, 19, 4957.
[2] Murakami, N., et al.: 2010, Appl. Opt., 49, D106.

Outburst of Comet 217P/LINEAR				SARUGAKU, Yuki
(ISAS/JAXA)		

UENO, Munetaka, USUI, Fumihiko				

ISHIGURO, Masateru(Seoul National University)(ISAS/JAXA)				

Comet 217P/LINEAR is a short-period comet detectedby the Lincoln Near-Earth Asteroid Research programas the name indicates. The discovery was on 2001 July
11, and was confirmed as a Jupiter family comet having
a period of 7.8 years. Because the most recent perihelion
passage was expected on 2009 September, we monitored
this comet with the Kiso 105 cm Schmidt Telescope.
The images revealed a day-by-day variation of the 217P/
LINEAR shape, indicating an outburst occurred. Since
our observation started before the outburst event, we
examined the morphological evolution of the expanding
dust cloud produced by the outburst[1]. It was found thatthe dust cloud expanded at a velocity of 120–140 m s−
1
and that the comet became brighter by 1.7–2.3 mag.
Using the observational result, we estimated that theonset time was 2009 October 13.4, and that the total mass
released by the outburst was in the range of 106–109 kg.
No fragments or split nuclei brighter than 18.5 mag(1.1 km in radius) were confirmed in our observations.
Compared with other outbursts[2], we concluded that it
was a relatively small event for an outburst.

WATANABE, Junichi(NAOJ)

Reference[1] Sarugaku, Y., et al.: 2010, ApJ, 724, L118-L121.
[2] Watanabe, J.-I., et al.: 2009, PASJ, 61, 679-685.

Figure 1: Rc band images of 217P/LINEAR observed on 2009 October 11–15, and 17. Sky brightness is subtracted. The upper right boxes
show close up images near nuclei with contour lines of 10−4.5, 10−4.0, 10−3.5, 10−3.0, and 10−2.5 W m−2 sr−1 μm−1 from the outer side.
The arrows in the October 13 image indicate the Sun direction (Sun), the angular momentum vector (L), and comet movement (v) on
the projected plane, respectively. The appearances of 217P/LINEAR on October 11 and 12 were similar, but clearly changed day by
day after October 13. It was found that the dust cloud expanded and was blown away by the radiation pressure.

I Scientific Highlights

067

II Publications, Presentations
1. Refereed Publications
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010,
Search for Gravitational-wave Inspiral Signals Associated with
Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First
Science Run, ApJ, 715, 1453-1461.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Allsky search for gravitational-wave bursts in the first joint LIGOGEO-Virgo run, Phys. Rev. D, 81, 102001.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010,
Search for gravitational waves from compact binary coalescencein LIGO and Virgo data from S5 and VSR1, Phys. Rev. D, 82,
102001.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010,
TOPICAL REVIEW: Predictions for the rates of compact
binary coalescences observable by ground-based gravitationalwave detectors, Class. Quantum Grav., 27, 173001.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010,
First Search for Gravitational Waves from the Youngest Known
Neutron Star, ApJ, 722, 1504-1513.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010,
Calibration of the LIGO gravitational wave detectors in thefifth science run, Nucl. Instrum. Methods. Phys. Res. A, 624,
223-240.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2011,
Search for gravitational waves associated with the August 2006
timing glitch of the Vela pulsar, Phys. Rev. D, 83, 042001.
Abbott, B. P., et al. including Hayama, K., Kawamura, S.: 2010,
Searches for Gravitational Waves from Known Pulsars with
Science Run 5 LIGO Data, ApJ, 713, 671-685.
Abbott, B. P., et al. including Hayama, K., Kawamura, S.: 2010,
Search For Gravitational-wave Bursts Associated with Gammaray Bursts using Data from LIGO Science Run 5 and Virgo
Science Run 1, ApJ, 715, 1438-1452.
Agatsuma, K., Arai, K., Fujimoto, M.-K., Kawamura, S., Kuroda,K., Miyakawa, O., Miyoki, S., Ohashi, M., Suzuki, T., Takahashi,R., Tatsumi, D., Telada, S., Uchiyama, T., Yamamoto, K.,
CLIO collaborators: 2010, Thermal-noise-limited undergroundinterferometer CLIO, Class. Quantum Grav., 27, 084022.
Amanullah, R., et al. including Furusawa, H., Kashikawa, N., The
Supernova Cosmology Project: 2010, Spectra and Hubble Space
Telescope Light Curves of Six Type Ia Supernovae at 0.511 < z< 1.12 and the Union2 Compilation, ApJ, 716, 712-738.
Ando, H., Tsuboi, Y., Kambe, E., Sato, B.: 2010, Oscillations in
the G-type Giants, PASJ, 62, 1117-1126.
Ando, K., Nagayama, T., Omodaka, T., Handa, T., Imai, H.,
Nakagawa, A., Nakanishi, H., Honma, M., Kobayashi, H.,
Miyaji, T.: 2011, Astrometry of Galactic Star-Forming Region
ON2N with VERA: Estimation of the Galactic Constants, PASJ,63, 45-51.
Ando, M., et al. including Kawamura, S., Agatsuma, K., Ejiri,Y., Fujimoto, M., Fukushima, M., Hayama, K., Ishizaki, H.,

068

II Publications, Presentations

Izumi, K., Kotake, K., Nakamura, K., Nishida, E., Obuchi,Y., Ohishi, N., Okada, N., Suzuki, R., Takahashi, R., Torii,
Y., Ueda, A., Yamazaki, T.: 2010, DECIGO and DECIGO
pathfinder, Class. Quantum Grav., 27, 084010.
Aoki, K.: 2010, Broad Balmer-Line Absorption in SDSS
J172341.10+555340.5, PASJ, 62, 1333.
Aoki, K., Oyabu, S., Dunn, J. P., Arav, N., Edmonds, D., Korista
K. T., Matsuhara, H., Toba, Y.: 2011, Outflow in Overlooked
Luminous Quasar: Subaru Observations of AKARI J1757+5907,
PASJ, 63, S457.
Aoki, W., Beers, T. C., Honda, S., Carollo, D.: 2010, Extreme
Enhancements of r-process Elements in the Cool Metal-poor
Main-sequence Star SDSS J2357-0052, ApJ, 723, L201-L206.
Arai, A., et al. including Yamashita, T., Okita, K., Yanagisawa,
K.: 2010, Optical and Near-Infrared Photometry of Nova V2362
Cyg: Rebrightening Event and Dust Formation, PASJ, 62,1103-1108.
Arimatsu, K., Izumiura, H., Ueta, T., Yamamura, I., Onaka, T.:2011, Detection of the Detached Dust Shell of U Antliae at Midinfrared Wavelengths with AKARI/IRC, ApJ, 729, L19.
Arimoto, M., et al. including Shirasaki, Y.: 2010, Spectral-Lag
Relations in GRB Pulses Detected with HETE-2, PASJ, 62, 487.
Asaki, Y., Deguchi, S., Imai, H., Hachisuka, K., Miyoshi, M.,
Honma, M.: 2010, Distance and Proper Motion Measurementof the Red Supergiant, S Persei, with VLBI H 2 O Maser
Astrometry, ApJ, 721, 267-277.
Baba, J., Saitoh, T. R., Wada, K.: 2010, On the Interpretation of
the l-v Features in the Milky Way Galaxy, PASJ, 62, 1413-1422.
Barro, G, Perez-Gonalez, P. G., Ashby, M. L. N, Kajisawa, M.,
Miyazaki, S., Villar, V., Yamada, T.: 2011, UV-to-FIR Analysis
of Spitzer/IRAC Sources in the Extended Groth Strip. I. Multiwavelength Photometry and Spectral Energy Distributions,
ApJS, 193, 13.
Bayliss, M. B., Gladders, M. D., Oguri, M., Hennawi, J. F., Sharon,
K., Koester, B. P., Dahle, H.: 2011, The Redshift Distribution of
Giant Arcs in the Sloan Giant Arcs Survey, ApJ, 727, L26.
Bayliss, M. B., Hennawi, J. F., Gladders, M. D., Koester, B. P.,
Sharon, K., Dahle, H., Oguri, M.: 2011, Gemini/GMOS
Spectroscopy of 26 Strong-lensing-selected Galaxy Cluster
Cores, ApJS, 193, 8.
Bedding, T. R., et al. including Kambe, E., Izumiura, H.: 2010,
Multi-Site Campaign to Measure Solar-Like Oscillations inProcyon. II. Mode Frequencies, ApJ, 713, 935-949.
Bekki, K., Tsujimoto, T.: 2010, Origin of the Unusually Low
Nitrogen Abundances in Young populations of the Large
Magellanic Cloud, ApJ, 721, 1515-1522.
Berger, T. E., Slater, G., Hurlburt, N., Shine, R., Tarbell, T., Title,
A., Lites, B. W., Okamoto, T. J., Ichimoto, K., Katsukawa,Y., Magara, T., Suematsu, Y., Shimizu, T.: 2010, Quiescent
Prominence Dynamics Observed with the Hinode Solar Optical
Telescope. I. Turbulent Upflow Plumes, ApJ, 716, 1288-1307.
Bernat, D., et al. including Martinache, F.: 2010, A CloseCompanion Search Around L Dwarfs Using Aperture Masking
Interferometry and Palomar Laser Guide Star Adaptive Optics,
ApJ, 715, 724-735.
Boyd, R. N., Kajino, T., Onaka, T.: 2010, Supernovae and the
Chirality of the Amino Acids, Astrobiology, 10, 561-568.
Burningham, B., Leggett, S. K., Lucas, P. W., Pinfield, D. J., Smart,
R. L., Day-Jones, A. C., Jones, H. R. A., Murray, D., Nickson,E., Tamura, M., Zhang, Z., Lodieu, N., Tinney, C. G., Zapatero
Osorio, M. R.: 2010, The discovery of a very cool binary
system, MNRAS, 404, 1952-1961.
Burningham, B., et al. including Tamura, M., Ishii, M., Kuzuhara,
M.: 2010, 47 new T dwarfs from the UKIDSS Large Area Survey,
MNRAS, 406, 1885-1906.
Bussey, D. B., McGovern, J. A., Spudis, P. D., Neish, C. D.,
Noda, H., Ishihara, Y., Sorensen, S.-A.: 2010, Illumination
conditions of the south pole of the Moon derived using Kaguya
topography, Icarus, 208, 558-564.
Caselli, P., Keto, E., Pagani, L., Aikawa, Y.: 2010, Water vapor
toward starless cores: The Herschel view, A&A, 521, 29-33.
Cheoun, M. K., Ha, E., Kajino, T.: 2011, Neutrino reactions on
Ar40 for solar and core-collapsing supernova neutrinos, Phys.
Rev. C, 83, 28801.
Cheoun, M. K., Ha, E., Kim, K. S., Kajino, T.: 2010, Neutrino
reactions via neutral and charged current by quasi-particle
random phase approximation (QRPA), J. Phys. G, 37, 55101.
Cheoun, M. K., Ha, E., Lee, S. Y., Kim, K. S., So, W. Y., Kajino, T.:2010, Neutrino reactions on 12C by the quasiparticle randomphase approximation, Phys. Rev. C, 81, 28501.
Cheoun, M. K., Hayakawa, T., Kajino, T., Chiba, S.: 2010,
Neutrino reactions on La138 and Ta180 via charged and neutral
currents by the quasiparticle random phase approximation,
Phys. Rev. C, 82, 35504.
Currie, T., et al. including Pyo, T.-S.: 2011, A Combined
Subaru/VLT/MMT 1–5 μm Study of Planets Orbiting HR
8799: Implications for Atmospheric Properties, Masses, andFormation, ApJ, 729, 128-147.
Dawson, J. R., McClure-Griffiths, N. M., Kawamura, A., Mizuno,N., Onishi, T., Mizuno, A., Fukui, Y.: 2011, Supershells as
Molecular Cloud Factories: Parsec Resolution Observations of
H I and 12CO(J = 1–0) in GSH 287+04-17 and GSH 277+00+36,
ApJ, 728, 127.
Deguchi, S., Koike, K., Kuno, N., Matsunaga, N., Nakashima, J.,
Takahashi, S.: 2011, SiO Maser Spectra of V407 Cyg after the2010 March Nova Outburst, PASJ, 63, 309-315.
Deguchi, S., Nakashima, J., Zhang, Y., Chong, S. S. N., Koike,
K., Kwok, S.: 2010, SiO and H2O Maser Observations of Red
Supergiants in Star Clusters Embedded in the Galactic Disk,
PASJ, 62, 391-407.
Deguchi, S., Shimoikura, T., Koike, K.: 2010, SiO Maser Survey
off the Galactic Plane: A Signature of Streaming Motion, PASJ,62, 525-546.
Derwaman. B., Nakamura, T., Yoshida, F.: 2011, Subaru lightcurve
observations of sub-km-sized main-belt asteroids, PASJ, 63,
S555.
Ebizuka, N., Ichiyama, K., Yamada, T., Tokoku, C., Onodera, M.,
Hanesaka, M., Kodate, K., Katsuno Uchimoto, Y., Maruyama,

M., Shimasaku, K., Tanaka, I., Yoshikawa, T., Kashikawa,N., Iye, M., Ichikawa, T.: 2011, Cryogenic Volume-Phase
Holographic Grisms for MOIRCS, PASJ, 63, S605-S612.
Escapa, A., Fukushima, T.: 2011, Free Translational Oscillationsof Icy Bodies with a Subsurface Ocean using a Variational
Approach, AJ, 141, 77-101.
Espada, D., Peck, A. B., Matsushita, S., Sakamoto, K., Henkel,
C., Iono, D., Israel, F. P., Muller, S., Petitpas, G., Pihlstrom,Y., Taylor, G. B., Trung, D. V.: 2010, Disentangling the
Circumnuclear Environs of Centaurus A: II. On the Nature of
the Broad Absorption Line, ApJ, 720, 666-678.
Finoguenov, A., et al. including Sekiguchi, K.: 2010, X-ray groups
and clusters of galaxies in the Subaru-XMM Deep Field,
MNRAS, 403, 2063-2076.
Fish, V. L., et al. including Honma, M., Oyama, T.: 2011, 1.3 mm
Wavelength VLBI of Sagittarius A*: Detection of Time-variable
Emission on Event Horizon Scales, ApJ, 727, L36.
Fok, H. S., Shum, C. K., Yi, Y., Araki, H., Ping, J., Williams, J. G.,
Fotopoulos, G., Noda, H., Goossens, S., Huang, Q., Ishihara,Y., Matsumoto, K., Oberst, J., Sasaki, S.: 2011, Accuracy
assessment of lunar topography models, Earth, Planets andSpace, 63, 15-23.
Fomalont, E., Johnston, K., Fey, A., Boboltz, D., Oyama, T.,
Honma, M.: 2011, The Position/Structure Stability of FourICRF2 Sources, AJ, 141, 91.
Fontani, F., Cesaroni, R., Furuya, R. S.: 2010, Class I and Class II
methanol masers in high-mass star-forming regions, A&A, 517,
A56.
Fujii, M., Iwasawa, M., Funato, Y., Makino, J.: 2010, The Origin
of S-stars and a Young Stellar Disk: Distribution of Debris Starsof a Sinking Star Cluster, ApJ, 716, L80-L84.
Fujiwara, H., Onaka, T., Ishihara, D., Yamashita, T., Fukagawa, M.,
Nakagawa, T., Kataza, H., Ootsubo, T., Murakami, H.: 2010,
Enstatite-rich Warm Debris Dust Around HD165014, ApJ, 714,
L152-L156.
Fukagawa, M., Tamura, M., Itoh, Y., Oasa, Y., Kudo, T., Hayashi,
S. S., Kato, E., Ootsubo, T., Itoh, Y., Shibai, H., Hayashi, M.:
2010, Subaru Near-Infrared Imaging of Herbig Ae Stars, PASJ,62, 347-370.
Fukue, T., Tamura, M., Kandori, R., Kusakabe, N., Hough, J.
H., Bailey, J., Whittet, D. C. B., Lucas, P. W., Nakajima, Y.,
Hashimoto, J.: 2010, Extended High Circular Polarization in
the Orion Massive Star Forming Region: Implications for theOrigin of Homochirality in the Solar System, Origins of Lifeand Evolution of Biospheres, 40, 335.
Fukui, A., et al. including Narita, N., Tamura, M.: 2011, Measurementsof Transit Timing Variations for WASP-5b, PASP, 63, 287-300.
Fukushima, T.: 2010, Fast Computation of Incomplete Elliptic
Integral of First Kind by Half Argument Transformation, Numer.
Math., 116, 687-719.
Fukushima, T.: 2010, Precise Computation of Acceleration due to
Uniform Ring or Disk, Celest. Mech. Dyn. Astron., 108, 339-356.
Furusawa, H., Okura, Y., Mineo, S., Takata, T., Nakata, F.,
Tanaka, M., Katayama, N., Itoh, R., Yasuda, N., Miyazaki, S.,
Komiyama, Y., Utsumi, Y., Uchida, T., Aihara, T.: 2011, First
On-Site Data Analysis System for Subaru/Suprime-Cam, PASJ,

II Publications, Presentations069

63, S585-S603.
Furusawa, J., Sekiguchi, K., Takata, T., Furusawa, H., Shimasaku,
K., Simpson, C., Akiyama, M.: 2011, The Mass-dependent
Clustering History of K-selected Galaxies at z < 4 in the SXDS/UDS Field, ApJ, 727, 111-123.
Furuya, R. S., Cesaroni, R., Shinnaga, H.: 2011, Infall, outflow, androtation in the G19.61-0.23 hot molecular core, A&A, 525, A72.
Gallagher, A. J., Ryan, S. G., García Pérez, A. E., Aoki, W.: 2010,
The barium isotopic mixture for the metal-poor subgiant star
HD 140283, A&A, 523, A24.
Geers, V., Scholz, A., Jayawardhana, R., Lee, E., Lafrenière, D.,
Tamura, M.: 2011, Substellar Objects in Nearby Young
Clusters (SONYC). II. The Brown Dwarf Population of ρ
Ophiuchi, ApJ, 726, 23.
Gobat, R., Daddi, E., Onodera, M., Finoguenov, A., Renzini, A.,
Arimoto, N., Bouwens, R., Brusa, M., Chary, R.R., Cimatti, A.,
Dickinson, M., Kong, X., Mignoli, M.: 2010, A mature clusterwith X-ray emission at z = 2.07, A&A, 526, A133.
Goossens, S., Matsumoto, K., Liu, Q., Kikuchi, F., Sato, K.,
Hanada, H., Ishihara, Y., Noda, H., Kawano, N., Namiki, N.,
Iwata, T., Lemoine, F. G., Rowlands, D. D., Harada, Y., Chen, M.:
2011, Lunar gravity field determination using SELENE samebeam differential VLBI tracking data, J. Geod., 85(4), 205-228.
Goossens, S.: 2010, Applying spectral leakage corrections to gravity
field determination from satellite tracking data, Geophys. J. Int.,
181, 1459-1472.
Goswami, A., Aoki, W.: 2010, HD209621: abundances of neutroncapture elements, MNRAS, 404, 253-264.
Goto, M., et al. including Terada, H., Usuda, T.: 2010, Fundamental
Vibrational Transition of CO During the Outburst of EX Lupi in
2008, ApJ, 728, 5.
Goto, T., et al. including Kodama, T., Hwang, N.: 2010, Environmental
dependence of 8 μm luminosity functions of galaxies at z ~ 0.8.
Comparison between RXJ1716.4+6708 and the AKARI NEPdeep field, A&A, 514, A7-11.
Goto, T., et al. including Hwang, N.: 2010, Evolution of infrared
luminosity functions of galaxies in the AKARI NEP-deep field.
Revealing the cosmic star formation history hidden by dust,
A&A, 514, A6-17.
Gouda, N., JASMINE working group: 2010, JASMINE: Infrared
Space Astrometry Mission, Transcations of the Japan Society
for Aeronautical and Space Science, Aerospace Technology
Japan, 8(No.ists27), To.4.7-To.4.12.
Groen, D., Portegies Zwart, S., Ishiyama, T., Makino, J.: 2011,
High-performance gravitational N-body simulations on a planetwide-distributed supercomputer, Computational Science andDiscovery, 4, 015001.
Guyon, O., Martinache, F., Belikov. R., Soummer, R.: 2010, High
Performance PIAA Coronagraphy with Complex Amplitude
Focal Plane Masks, ApJS, 190, 220-232.
Hagiwara, Y.: 2010, Two Epochs of Very Large Array Observationsof Water Maser Emission in the Active Galaxy NGC 6240, AJ,
140, 1905-1910.
Hanada, H., Iwata, T., Liu, Q., Kikuchi, F., Matsumoto, K.,
Goossens, S., Harada, Y., Asari, K., Ishikawa, T., Ishihara,Y., Noda, H., Tsuruta, S., Petrova, N., Kawano, N., Sasaki,

070

II Publications, Presentations

S., Sato, K., Namiki, N., Kono, Y., Iwadate, K., Kameya, O.,
Shibata, K., Tamura, Y., Kamata, S., Yahagi, Y., Masui, W.,
Tanaka, K., Maejima, H., Hong, X., Ping, J., Shi, X., Huang,
Q., Aili, Y., Ellingsen, S., Schlüter, W.: 2010, Overview ofdifferential VLBI observations of lunar orbiters in SELENE(Kaguya) for precise orbit determination and lunar gravity fieldstudy, Space Sci. Rev., 154, 123-144.
Harikae, S., Kotake, K., Takiwaki, T.: 2010, Neutrino Pair
Annihilation in Collapsars: A Ray-tracing Method in Special
Relativity, ApJ, 713, 304-317.
Harikae, S., Kotake, K., Takiwaki, T., Sekiguchi Y.: 2010,
A General Relativistic Ray-tracing Method for Estimating
the Energy and Momentum Deposition by Neutrino Pair
Annihilation in Collapsars, ApJ, 720, 614-625.
Harra, L. K., Magara, T., Hara, H., Tsuneta, S., Okamoto, T. J.,
Wallace, A. J.: 2010, Response of the Solar Atmosphere to theEmergence of ‘Serpentine’ Magnetic Field, Solar Phys., 263,
105-119.
Hashimoto, J., et al. including Tamura, M., Kudo, T., Fukue, T.,
Kokubo, E., Egner, S., Golota, T., Hayano, Y., Hayashi, M.,
Hayashi, S., Ishii, M., Kandori, R., Kusakabe, N., Matsuo, T.,
Miyama, S., Morino, J.-I., Nishimura, T., Pyo, T.-S., Suto, H.,
Takato, N., Terada, H., Tomono, D., Takami, H., Usuda, T.:2011, Direct Imaging of Fine Structures in Giant Planet-forming
Regions of the Protoplanetary Disk Around AB Aurigae, ApJ,
729, L17-L21.
Hashimoto, T., Nagao, T., Yanagisawa, K., Matsuoka, K., Araki,N.: 2011, Spatially Extended [P II] 1.188 μm and [Fe II] 1.257 μm
Emission Lines in a Nearby Seyfert Galaxy NGC 1068
Observed with OAO/ISLE, PASJ, 63, L7-L11.
Hashimoto, T., Ohta, K., Aoki, K., Tanaka, I., Yabe, K., Kawai, N.,
Aoki, W., Furusawa, H., Hattori, T., Iye, M., Kawabata, K.
S., Kobayashi, N., Komiyama, Y., Kosugi, G., Minowa, Y.,
Mizumoto, Y., Niino, Y., Nomoto, K., Noumaru, J., Ogasawara,
R., Pyo, T.-S., Sakamoto, T., Sekiguchi, K., Shirasaki, Y., Suzuki,M., Tajitsu, A., Takata, T., Tamagawa, T., Terada, H., Totani,T., Watanabe, J., Yamada, T., Yoshida, A.: 2010, "Dark" GRB
080325 in a Dusty Massive Galaxy at z ~ 2, ApJ, 719, 378-384.
Hatsukade, B., Kohno, K., Aretxaga, I., Austermann, J. E., Ezawa,
H., Hughes, D. H., Ikarashi, S., Iono, D., Kawabe, R., Khan,
S., Matsuo, H., Matsuura, S., Nakanishi, K., Oshima, T.,
Perera, T., Scott, K. S., Shirahata, M., Takeuchi, T. T., Tamura,Y., Tanaka, K., Tosaki, T., Wilson, G. W., Yun, M. S.: 2011,
AzTEC/ASTE 1.1-mm Survey of the AKARI Deep Field South:
Source Catalogue and Number Counts, MNRAS, 411, 102-116.
Hayakawa, T., Kajno, T., Chiba, S., Mathews, G. J.: 2010, New
Estimate for the Time-Dependent Thermal Nucleosynthesisof 180Tam in Supernova Nucleosynthesis, Phys. Rev. C, 81,
52801.
Hayakawa, T., Mohr, P., Kajno, T., Chiba, S., Mathews, G. J.:
2010, Reanalysis of the (J = 5) state at 592 keV 180Ta and its rolein the ν-process nucleosynthesis of 180Ta in supernova, Phys.
Rev. C, 82, 58801.
Higuchi, A. E., Kurono, Y., Saito, M., Kawabe, R.: 2010, A
Mapping Survey of Dense Associated with Embedded Clusters
II: Can Clump-Climp Collisions Induce Stellar Clusters?, ApJ,

719, 1813-1827.
Hikage, C., Takada, M., Hamana, T., Spergel, D.: 2011, Shear
power spectrum reconstruction using the pseudo-spectrum
method, MNRAS, 412, 65-74.
Hinkley, S., et al. including Martinache, F.: 2011, Establishingalpha Oph as a Prototype Rotator: Improved Astrometric Orbit,
ApJ, 726, 104-110.
Hirano, T., Narita, N., Shporer, A., Sato, B., Aoki, W., Tamura,M.: 2011, A Possible Tilted Orbit of the Super-Neptune HAT-P11b, PASJ, 63, S531-S536.
Hirota, A., Kuno, N., Sato, N., Nakanishi, H., Tosaki, T., Sorai, K.:
2010, Variation of Molecular Gas Properties Across the SpiralArms in IC 342: Large-Scale 13CO(1–0) Emission, PASJ, 62,
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II Publications, Presentations075

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II Publications, Presentations

Submillimeter Image of a Rotating First Core, ApJ, 728, 78-87.
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Samal, M. R., Pandey, A. K., Ojha, D. K., Ghosh, S. K., Kulkarni, V. K.,
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Sato, B., Omiya, M., Liu, Y., Harakawa, H., Izumiura, H., Kambe,
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K.-I. Morita, M. Ohishi, 297-300.
Ikeda, Y., Kobayashi, N., Kuzmenko, P. J., Little, S. L.,Yasui,C., Kondo, S., Mito, H., Nakanishi, K., Sarugaku, Y.: 2010,
Fabrication and current optical performance of a large diamondmachined ZnSe immersion grating, Proc. SPIE 7739, Eds. E.
Atad-Ettedgui, D. Lemke, 4G.
Imanishi, M.: 2010, Luminous Buried AGNs in Ultraluminous
Infrared Galaxies, AIP Conf. Proc. 1240, Eds. V. P. Debattista, C,
C. Popescu, 72-75.
Ito, H., Aoki, W., Satoshi, H., Beers, T. C., Tominaga, N.: 2010, A
very low upper limit for a Be abundance of a carbon-enhanced
metal-poor star, Proc. IAU Symp. 268, Eds. C. Charbonnel, M.
Tosi, F. Primas, C. Chiappini, 337-338.
Ito, H., Kino, M., Kawakatu, K., Yamada, S.: 2010, Non-thermal
emission shocked shell driven by powerful AGN jets, Int. J. of
Modern Phys. D, 19, 893-899.
Ito, M., Hayano, Y., Saito, Y., Takami, H., Iye, M., Hattori, M.,
Oya, S., Watanabe, M., Akagawa, K., Colley, S. A., Golota, T. I.,
Guyon, O.: 2010, The characteristics of laser-transmission andguide star's brightness for Subaru LGS/AO188 system, Proc.
SPIE 7736, Eds. B. L. Ellerbroek, M. Hart, N. Hubin, P. L.
Wizinowich, 169.
Itoh, S., Agata, H., Nagai, T., Nakayama, H., Naito, S., Hirai, A.:
2010, What is our "Science Culture Promotion Unit ThroughAstronomical Images"?, Immersive Scientific Visualization,
Eds. M. Okyudo, T. Ebisuzaki, 15-17.
Jenniskens, P., Sato, M., Watanabe, J., Trigo-Rodriguez, J.
M., Madiedo, J. M., Pujols, P., de, J. A., Alonso-Azcarate, J.,
Zamorano, J.: 2010, Orionid Meteors 2010, Central Bureau
Electronic Telegrams.
Jeschke, E., Inagaki, T.: 2010, Lessons Learned Deploying a
Second Generation Observation Control System for Subaru
Telescope, Proc. SPIE 7740, Eds. N. M. Radziwill, A. Bridger.
Jeschke, E., Inagaki, T.: 2010, Designing a High-Availability
Cluster for the Subaru Telescope Second Generation
Observation Control System, Proc. SPIE 7740, Eds. N. M.
Radziwill, A. Bridger.
Kajino, T., Harikae, S., Yoshida, T., Nakamura, K., Aoki, W.:2010, R-process in Supernovae and Gamma-Ray Bursts, AIP
Conf. Proc. 1235, 242-246.
Kamata, Y., et al. including Nakaya, H., Miyazaki, S., Uraguchi,
F.: 2010, Characterization and performance of hyper SuprimeCam CCD, Proc. SPIE 7742, Eds. A. Holland, D. Dorn, 62.
Kaneko, H., Kuno, N., Iono, D., Tosaki, T., Sawada, T.,
Nakanishi, H., Hirota, A.: 2010, Molecular Gas in the Early

Stage of Interacting Galaxies: The NGC 4567/8 Pair, ASP Conf.
Ser. 423, Eds. B. J. Smith, N. Bastian, S. J. U. Higdon, J. L.
Higdon, 26-31.
Katsukawa, Y., Masada, Y., Shimizu, T., Sakai, S., Ichimoto, K.:
2010, Pointing stability of Hinode and requirements for the next
solar mission Solar-C, Proc. of Int. Conf. on Space Optics 2010,
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Katsukawa, Y., SOLAR-C Working Group: 2011, ChromosphericDiagnostics in the Next Japanese Solar Mission SOLAR-C,
ASP Conf. Ser. 437, Eds. J. R. Kuhn, S. V. Berdyugina, D. M.
Harrington, S. Keil, H. Lin, T. Rimmele, B. J. Trujillo, 281-286.
Kobayashi, Y., Yano, T., Gouda, N., Niwa, Y., Murooka, J.,
Yamada, Y., Sako, N., Nakasuka, S.: 2010, Nano-JASMINE:
current status and data output, Proc. SPIE 7731, Eds. J. M.
Oschmann Jr., M. C. Clampin, H. A. MacEwen, 3Z.
Kobayashi, Y., Yano, T., Hatsutori, Y., Gouda, N., Murooka, J.,
Niwa, Y., Yamada, Y.: 2011, Nano-JASMINE: Simulation of
Data Outputs, EAS Publications Series, 45, Eds. C. Turon, F.
Meynadier, F. Arenou, 401-404.
Komiya, Y., Suda, T., Fujimoto, M. Y.: 2010, Near field cosmology
with binary, high mass IMF, and hierarchical galaxy formation,
AIP Conf. Ser. 1238, Eds. H. Susa, M. Arnould, S. Gales, T.
Motobayashi, C. Scheidenberger, H. Utsunomiya, 126-129.
Komiya, Y., Suda, T., Fujimoto, M. Y.: 2010, EMP Stars andHierarchical Model of the Galactic Chemical Evolution, AIP
Conf. Proc. 1269, Eds. I. Tanihata, T. Shima, H. J. Ong, A.
Tamii, T. Kishimoto, H. Toki, T. Kajino, S. Kubono, 360-362.
Komiyama, Y., Aihara, H., Fujimori, H., Furusawa, H., Kamata,Y., Karoji, H., Kawanomoto, S., Mineo, S., Miyatake, H.,
Miyazaki, S., Morokuma, T., Nakaya, H., Nariai, K., Obuchi,Y., Okura, Y., Tanaka, Y., Uchida, T., Uraguchi, F., Utsumi, Y.,
Endo, M., Ezaki, Y., Matsuda, T., Miwa, Y., Yokota, H., Wang,
S.-Y., Liaw, E. J., Chen, H.-Y., Chiu, C.-F., Jeng, D.-Z.: 2010,
Hyper Suprime-Cam: camera design, Proc. SPIE 7735, Eds. I. S.
McLean, S. K. Ramsay, H. Takami.
Kotani, T., Miyazaki, A., Tsuboi, M., Endo, W., Fujisawa, K.,
Kawai, N., Kuno, N., Nakanishi, K., Yamaoka, K., Yonekura,Y.: 2011, Cyg X-3 is Flaring in Radio, The Astronomer's
Telegram, #32130.
Kuno, N., Tosaki, T., Onodera, S., Muraoka, K., Kaneko, H.,
Sawada, T., Nakanishi, K., Komugi, S., Tamura, Y., Kohno,
K., Kawabe, R., Arimoto, N., Okamoto, S.: 2010, NRO Legacy
Project: Survey of Giant Molecular Clouds in M33, Highlights
of Astronomy, 15, Ed. I. Corbett, 416-416.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100504A:
optical upper limits at IAO, GRB Coordinates Network,
Circular Service 10740.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100901A:
optical observations at IAO, GRB Coordinates Network,
Circular Service 11205.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB10901A:
murikabushi telescope observation at 3 days after the burst,

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GRB Coordinates Network, Circular Service 11212.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100901A: IAO
optical upper limits at 4 days after the burst, GRB Coordinates
Network, Circular Service 11258.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100902A:
optical upper limits at IAO, GRB Coordinates Network,
Circular Service 11206.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100905A:
optical upper limits at IAO, GRB Coordinates Network,
Circular Service 11225.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100906A:
optical observations at IAO, GRB Coordinates Network,
Circular Service 11249.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100909A:
Mitsume ishigakijima optical upper limits, GRB Coordinates
Network, Circular Service 11273.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100915A:
Mitsume ishigakijima optical upper limits, GRB Coordinates
Network, Circular Service 11287.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB101219A:
MITSuME Ishigakijima Optical upper limits, GRB Coordinates
Network, Circular Service 11479.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110205A:
MITSuME Ishigakijima Optical Observation, GRB Coordinates
Network, Circular Service 11652.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110305A:
MITSuME Ishigakijima Optical upper limits, GRB Coordinates
Network, Circular Service 11780.
Kuroda, D., Hanayama, H., Miyaji, T., Yanaisawa, K., Shimizu,
Y., Toda, H., Nagayama, S., Watanabe, J., Ali, G. B., Haroon,A., Essam, A., Ismal, M., Kawabata, K. S., Yoshida, M., Ohta,
K., Yatsu, Y., Nakajima, H., Enomoto, T., Kawakami, K.,
Tokoyoda, K., Kawai, N.: 2010, Multi-band optical monitoringof GRB100925A/MAXI J1659-152, The First Year of MAXI:
Monitoring Variable X-ray Sources, Eds. K. Ebisawa, N. Kawai.
Kuroda, D., Hanayama, H., Yanagisawa, K., Shimizu, Y., Toda,
H., Nagayama, S., Miyaji, T., Watanabe, J., Yoshida, M.,
Ohta, K., Kawai, N.: 2010, GRB100925A/MAXI J1659-152
Mitsume ishigakijima and okayama optical observation, GRB
Coordinates Network, Circular Service 11306.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Yoshida, M., Kawai, N.: 2010, GRB100420A: Mitsume
optical upper limits, GRB Coordinates Network, CircularService 10642.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB101224A:
Mitsume okayama optical upper limits, GRB Coordinates

082

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Network, Circular Service 11487.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB101017A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11351.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100906A:
errata of Mitsume okayama about observation time, GRB
Coordinates Network, Circular Service 11241.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100906A:
Mitsume okayama optical observation, GRB Coordinates
Network, Circular Service 11240.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100905A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11224.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100901A:
Mitsume okayama optical observation at 1 day after the burst,
GRB Coordinates Network, Circular Service 11189.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100901A:
errata of Mitsume okayama about reference catalog, GRB
Coordinates Network, Circular Service 11186.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100901A:
Mitsume okayama optical observation, GRB Coordinates
Network, Circular Service 11172.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100816A:
Mitsume optical upper limits, GRB Coordinates Network,
Circular Service 11126.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100807A:
Mitsume optical upper limits, GRB Coordinates Network,
Circular Service 11075.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100802A:
Mitsume optical upper limits, GRB Coordinates Network,
Circular Service 11041.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100725B:
Mitsume optical upper limits, GRB Coordinates Network,
Circular Service 10997.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100424A:
Mitsume optical upper limits, GRB Coordinates Network,
Circular Service 10679.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100423A:
Mitsume optical upper limits, GRB Coordinates Network,
Circular Service 10678.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110312A:
Mitsume okayama optical upper limits, GRB CoordinatesNetwork, Circular Service 11789.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110213A:
Mitsume okayama optical observation, GRB Coordinates
Network, Circular Service 11719.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110212A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11711.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110205A:
Mitsume okayama optical observation, GRB Coordinates
Network, Circular Service 11651.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110201A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11626.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110128A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11618.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110119A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11585.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB 110106A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, Circular Service 11535.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB110102A:
Mitsume okayama optical observation, GRB Coordinates
Network, Circular Service 11513.
Kuroda, K., LCGT Collaboration: 2010, Cryogenic Advanced
Gravitational Wave Detector (LCGT), Proc. of the 9th Asia-PacificInt. Conf., Eds. J. Luo, Z.-B. Zhou, H.-C. Yeh, J.-P. Hsu, 48-67.
Kusakabe, M., Kajino, T., Yoshida, T., Mathews, G. J.: 2010,
Signature of Long-lived Relic Particles on Primordial Light
Element Abundances in Big Bang Nucleosynthesis, AIP Conf.
Proc. 1269, Eds. I. Tanihata, T. Shima, H. J. Ong, A. Tamii, T.
Kishimoto, H. Toki, T. Kajino, S. Kubono, 63-68.
Landi, E., J. C. Raymond, J. C., Miralles, M. P., Hara, H.: 2010,
Physical Conditions in a CME from Hinode, STEREO, and
SOHO Observations, ASP Conf. Ser. 428, Eds. S. R. Cranmer, T.
Hoeksema, J. L. Kohl, 201-205.
Larkin, J. E., Moore, A. M., Barton, E. J., Bauman, B., Bui, K.,
Canfield, J., Cramton, D., Delacroix, A., Fletcher, M., Hale, D.,
Loop, D., Niehaus, C., Phillips, A. C., Reshetov, V., Simard, L.,
Smith, R., Suzuki, R., Usuda, T., Wright, S. A.: 2010, The infrared
imaging and spectrograph (IRIS) for TMT: instrument overview,Proc. SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 29.
Lee, S., et al. including Pyo, T.-S.: 2010, GMTNIRS (Giant Magellan
Telescope near-infrared spectrograph): design concept, Proc.
SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 87-95.
Lee, S., Itoh, R., Katayama, N., Furusawa, H., Aihara, H., Mineo,
S.: 2010, A common real time framework for SuperKEKB andHyper Suprime-Cam at Subaru telescope, J. Phys.: Conf. Ser.,
219, 22012-22020.
Lisenfeld, U., Espada, D., Leon, S., Lerdes-Montenegro, L.,
Kuno, N., Sato, N.: 2010, Molecular Gas Properties in the
Most Isolated Galaxies, ASP Conf. Ser. 421, Eds. L. VerdesMontenegro, A. del Olmo, J. W. Sulentic, 262.
Machida, M. N., Omukai, K., Matsumoto, T.: 2010, Magnetohydrodynamics of Population III Star Formation, AIP Conf.
Proc. 1294, Eds. D. Whalen., V. Bromm., N. Yoshida, 56-61.
Martinache, F., Guyon, O.: 2010, The Subaru Coronagraphic
Extreme AO Project, Pathways Towards Habitable Planets, Eds.
V. Coude du Foresto, D. Gelino, I. Ribas, 497-498.
Maruyama, T., Yasutake, N., Kajino, T., Cheoun, M. K., Ryu,
C. Y.: 2010, Asymmetric Neutrino Reaction from MagnetizedProto-Neutron Stars in fully Relativistic Framework including
Hyperons, AIP Conf. Proc. 1269, Eds. I. Tanihata, T. Shima, H.
J. Ong, A. Tamii, T. Kishimoto, H. Toki, T. Kajino, S. Kubono,
406-408.
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2010,
SISCAM 32-ch Cryogenic Readout Module with GaAs-JFET
ASICs, Proc. SPIE 7741, Eds. W. S. Holland, J. Zmuidzinas, 2V.
Matsuo, H., Shi, S.-C., Yao, Q.-J., Luo, Y., Matsuo, T., Ohta, I. S.:
2010, A design study on terahertz interferometry in Antarctica,
Proc. SPIE 7854, Eds. C. Zhang, X.-C. Zhang, P. H. Siegel, L.
He, S.-C. Shi, 10.
Matsuo, T., Tamura, M.: 2010, Second-earth imager for TMT(SEIT): a proposal and concept Description, Proc. SPIE 7735,
Eds. I. S. McLean, S. K. Ramsay, H. Takami, 84.
Matsuo, T., Traub, W. A., Hattori, M., Tamura, M., Shao, M.: 2010,
New concept for direct detection and spectra of exoplanets,
Proc. SPIE 7734, Eds. W. C. Danchi, F. Delplancke, J. K.
Rajagopal, 2K.
Matsuo, T., Traub, W. A., Hattori, M., Tamura, M., Shao, M.: 2010,
New Concept for Direct Detection and Spectra of Exoplanets,
Proc. Conf. in the Spirit of Lyot 2010, Ed. A. Boccaletti, 78.
Matsuo, T., Traub, W. A., Tamura, M., Hattori, M.: 2010, Spectral
Imaging with Nulling Interferometer, ASP Conf. Ser. 430, Eds.
V. Coudé du Foresto, M. G. Dawn, R. Ignasi, 499.
Matsuo, T., Traub, W. A., Tamura, M., Hattori, M.: 2010, Multiple
Aperture Imaging and its Application to Exo-Earth Imager,
ASP Conf. Ser. 430, Eds. V. Coudé du Foresto, M. G. Dawn, R.
Ignasi, 501.
Mineo, S., Aihara, H., Itoh, R., Katayama, N., Yasuda, N., Furusawa,
H., Okura, Y., Miyazaki, S., Loomis, C., Lupton, R. H.: 2010,
Development of an analysis framework for HSC and Belle II,
Proc. SPIE 7740, Eds. N. M. Radziwill, A. Bridger., 1P.
Minowa, Y., Hayano, Y., Oya, S., Watanabe, M., Hattori, M.,
Guyon, O., Egner, S., Saito, Y., Ito, M., Takami, H., Garrel, V.,
Colley, S., Golota, T., Iye, M.: 2010, Performance of Subaru
adaptive optics system AO188, Proc. SPIE 7736, Eds. B. L.
Ellerbroek, M. Hart, N. Hubin, P. L. Wizinowich, 122.
Miura, N., Yokoyama, F., Nefu, M., Kuwamura, S., Baba, N.,
Hanaoka, Y., Ueno, S., Nakatani, Y., Nagata, S., Kitai, R.,
Ichimoto, K., Takami, H.: 2010, Optical setup and wavefront
sensor for solar adaptive optics at the Domeless Solar Telescope,
Hida Observatory, Proc. SPIE 7736, Eds. B. L. Ellerbroek, M.

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Hart, N. Hubin, P. L. Wizinowich, 54.
Morita, K.-I., Kurono, Y., Kamazaki, T.: 2010, Optimizing
Spatial Frequency Data Weights for High Precision Imaging
with ALMA, ASP Conf. Ser. 434, Eds. Y. Mizumoto, K.-I.
Morita, M. Ohishi, 337-340.
Murakami, N., Guyon, O., Martinache, F., Matsuo., T., Yokochi,
K., Nishikawa, J., Tamura, M., Kurokawa, T., Baba, N., Vogt,
F., Garrel, V., Yoshikawa, T.: 2010, An eight-octant phasemask coronagraph for the Subaru coronagraphic extreme AO(SCExAO) system: system design and expected performance, Proc.
SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 33.
Murakami, N., Inabe, T., Komatsu, T., Nishikawa, J., Hashimoto,N., Kurihara, M., Baba, N., Tamura, M.: 2010, Polarizationinterferometric eight-octant phase-mask coronagraph using
ferroelectric liquid crystal for exoplanet detection, Proc. SPIE 7731,
Eds. J. M. Oschmann Jr., M. C. Clampin, H. A. MacEwen, 4E.
Murakami, N., Nishikawa, J., Yokochi, K., Tamura, M., Baba,
N., Hashimoto, N., Abe, L.: 2010, An eight-octant phasemask coronagraph for the Subaru coronagraphic extreme AO(SCExAO) system: system design and expected performance,
ASP Conf. Ser. 430, Eds. V. Coudé du Foresto, M. G. Dawn, R.
Ignasi, 510-512.
Nakajima, H., Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda,
H., Nagayama, S., Yoshida, M., Ohta, K., Yatsu, Y., Enomoto,T., Kawakami K., Tokoyoda, K., Ohkawa, T., Kawai, N.: 2011,
GRB 110112A: Mitsume akeno and okayama optical upper
limits, GRB Coordinates Network, Circular Service 11566.
Nakamura, K., Yoshida, T., Shigeyama, T., Kajino, T.: 2010,
Lithium, beryllium, and boron production in core-collapse
supernovae, Proc. IAU Symp. 268, Eds. C. Charbonnel, M.
Tosi, F. Primas, C. Chiappini, 463-468.
Nakamura, K., Yoshida, T., Shigeyama, T., Kajino, T.: 2010,
Light elements from core-collapse supernovae: the neutrinoprocess and spallation reactions, AIP Conf. Proc. 1269, Eds. I.
Tanihata, T. Shima, H. J. Ong, A. Tamii, T. Kishimoto, H. Toki, T.
Kajino, S. Kubono, 309-314.
Nakamura, R., Hashimoto, M., Fujimoto, S., Nishimura, N., Sato,K.: 2010, Constraints on the heavy elements production in
inhomogeneous Big-Bang nucleosynthesis from light-element
observations, AIP Conf. Proc. 1269, Eds. I. Tanihata, T. Shima,
H. J. Ong, A. Tamii, T. Kishimoto, H. Toki, T. Kajino, S.
Kubono, 378-380.
Nakaya, H., Uchida, T., Miyatake, H., Fujimori, H., Mineo, S., Aihara,
H., Furusawa, H., Kamata, Y., Karoji, H., Kawanomoto, S.,
Komiyama, Y., Miyazaki, S., Morokuma, T., Obuchi, Y.,
Okura, Y., Tanaka, M., Tanaka, Y., Uraguchi, F., Utsumi, Y.:
2010, Hyper Suprime-Cam: development of the CCD readout
electronics, Proc. SPIE 7735, Eds. I. S. McLean, S. K. Ramsay,
H. Takami, 52.
Nakazato, T., Sugimoto, K., Kawasaki, W., Kosugi, G., Tsutsumi, T.:2010, Current Status of Single-Dish Data Analysis Software for
ALMA, ASP Conf. Ser., 434, Eds. Y. Mizumoto, K.-I. Morita, M.
Ohishi, 83.
Narita. N.: 2011, Good Combination of the Rossiter-McLaughlin
Measurements and Direct Imaging Observations, EPJ Web ofConf. Col. 11, Eds. F. Bouchy, R. Diaz, C. Moutou, id.05004.

084

II Publications, Presentations

Niino, Y., Choi, J.-H., Kobayashi, M. A. R., Nagamine, K.,
Totani, T., Zhang, B.: 2010, Metallicity of Gamma-Ray Burst
Progenitors: Connection between Star Formation and GammaRay Burst Production, AIP Conf. Proc. 1269, Eds. I. Tanihata, T.
Shima, H. J. Ong, A. Tamii, T. Kishimoto, H. Toki, T. Kajino, S.
Kubono, 345-347.
Niino, Y., Choi, J.-H., Kobayashi, M. A.R., Nagamine, K., Totani,T., Zhang B.: 2010, Luminosity Distribution of Gamma-ray Burst
Host Galaxies at Redshift z = 1 in Cosmological Simulation, AIP
Conf. Proc. 1279, Eds. N. Kawai, S. Nagataki, 231-233.
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani, T.,
Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.: 2010,
A coronagraph system with unbalanced nulling interferometer:
progress of wavefront correction, ASP Conf. Ser. 430, Eds. V.
Coudé du Foresto, M. G. Dawn, R. Ignasi, 513-514.
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani,T., Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.,
Murakami, H.: 2010, A coronagraph system with unbalanced
nulling interferometer: progress of wavefront correction, Proc.
SPIE 7731, Eds. J. M. Oschmann Jr., M. C. Clampin, H. A.
MacEwen, 4O.
Nishimura, N., Takiwaki, T., Hashimoto, M., Sato, K.: 2010,
R-process Nucleosynthesis in Magnetically Dominated CoreCollapse Supernovae, AIP Conf. Proc. 1269, Eds. I. Tanihata, T.
Shima, H. J. Ong, A. Tamii, T. Kishimoto, H. Toki, T. Kajino, S.
Kubono, 131-136.
Niwa, Y., Yano, T., Araki, H., Gouda, N., Kobayashi, Y.,
Tazawa, S., Hanada H., Yamada, Y.: 2010, CCD centroiding
analysis for Nano-JASMINE observation data, Proc. SPIE 7731,
Eds. J. M. Oschmann Jr., M. C. Clampin, H. A. MacEwen, 41.
Noda, T., Hashimoto, M. Yasutake, N., Maruyama, T., Tatsumi,T., Fujimoto, M.: 2010, Cooling of Compact Stars with QuarkHadron Mixed Phase in the Colour Superconductive State,
AIP Conf. Proc. 1269, Eds. I. Tanihata, T. Shima, H. J. Ong, A.
Tamii, T. Kishimoto, H. Toki, T. Kajino, S. Kubono, 384-386.
Ohishi, M., Shirasaki, Y., Komiya, Y., Mizumoto, Y., Yasuda, N.,
Tanaka, M.: 2010, Lessons Learned during the Development
and Operation of Virtual Observatory, ASP Conf. Ser. 434, Eds.
Y. Mizumoto, K.-I. Morita, M. Ohishi, 73-80.
Okamoto, Y. K., et al. including Fujiyoshi, T., Imanishi, M.,
Yamashita, T.: 2010, The science driver for a mid-infrared
instrument for the TMT, Proc. SPIE 7735, Eds. I. S. McLean, S.
K. Ramsay, H. Takami, 5O.
Okoshi, K., Nagashima, M., Gouda, N., Minowa, Y.: 2010, HIselected Galaxies As a Probe of Quasar Absorption Systems,
Proc. IAU Symp. 262, Eds. G. R. Bruzual, S. Charlot, 402-403.
Omiya, M., Han, I., Izumiura, H., Lee, B.-C., Sato, B., Kim, K.-M.,
Yoon., T. S., Kambe, E., Yoshida, M., Masuda, S., Toyota, E.,
Urakawa, S., Takada-Hidai, M.: 2011, Korean-Japanese Planet
Search Program: Substellar Companions around IntermediateMass Giants, AIP Conf. Proc. 1331, Eds. S. Schuh, H., Drechsel,
U. Heber, 122-129.
Oya, S., Hattori, M., Minowa, Y., Negishi, S., Tomono, D., Terada,
H., Pyo, T.-S., Watanabe, M., Ito, M., Saito, Y., Egner, S., Hayano,Y., Takami, H., Iye, M., Guyon, O., Garrel, V., Colley, S.,
Golota, T.: 2010, Tip/tilt offload of Subaru AO188 by telescopesecondary mirror, Proc. SPIE 7736, Eds. B. L. Ellerbroek, M.
Hart, N. Hubin, P. L. Wizinowich, 128-136.
Ozaki, S., Iwata, I., Kambe, E., Yoshida, M., Okita, K., Iwamuro,F., Sugai, H. Ohta, K.: 2010, Development of the prototype
integral field unit for prompt follow-up spectroscopy of gammaray bursts, Proc. SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H.
Takami, 50.
Packham, C. C., et al. including Imanishi, M., Izumiura, H.,
Yamashita, T.: 2011, Michi: A MIR Instrument Concept for the
TMT, Bulletin of AAS, 43, #217, #157.03.
Pehlivan, Y., Kajino, T., Balantekin, A. B., Yoshida, T., Maruyama,
T.: 2010, On the Neutrino Self Refraction Problem from a
Many-Body Perspective, AIP Conf. Proc. 1269, Eds. I. Tanihata,
T. Shima, H. J. Ong, A. Tamii, T. Kishimoto, H. Toki, T. Kajino,
S. Kubono, 189-194.
Pehlivan, Y., Kajino, T., Balantekin, A. B., Mathews, G. J.,
Kusakabe, M.: 2010, Photodisintegration at High Temperature,
AIP Conf. Proc. 1269, Eds. I. Tanihata, T. Shima, H. J. Ong, A.
Tamii, T. Kishimoto, H. Toki, T. Kajino, S. Kubono, 397-399.
Robson, I. E., et al. including Sekiguchi, K.: 2010, Commission
55: Communicating Astronomy with the Public, Transactions of
the IAU, XXVII B, 274-277.
Saito, R., et al. including Tamura, M.: 2010, VISTA Variables inthe Vía Láctea (VVV): Current Status and First Results, The
Messenger, 141, 24-28.
Saito, Y., Hayano, Y., Ito, M., Minowa, Y., Egner, S., Oya, S.,
Watanabe, M., Hattori, M., Garrel, V., Akagawa, K.,
Guyon, O., Colley, S., Golota, T., Saito, N., Takazawa, A.,
Ito, M., Takami, H., Wada, S., Iye, M.: 2010, The performanceof the laser guide star system for the Subaru Telescope, Proc.
SPIE 7736, Eds. B. L. Ellerbroek, M. Hart, N. Hubin, P. L.
Wizinowich, 171.
Sato, S., Kawamura, S., Nishizawa, A., Chen, Y.: 2010, Noisecancellation properties of displacement noise free interferometer, J. Phys.: Conf. Ser., 228, 012026.
Sato, S., Torii, Y., Wakabayashi, Y., Ejiri, Y., Suzuki, R., Ueda,
A., Kawamura, S., Araya, A., Ando, M., Obuchi, Y., Okada,N.: 2010, Test-mass module for DECIGO Pathfinder, J. Phys.:Conf. Ser., 228, 012046.
Sekiguchi, Y.: 2010, Formation of Black hole-Disk System via
PopIII stellar core collapse in full general relativity, AIP Conf.
Proc. 1279, Eds. N. Kawai, S. Nagataki, 93-96.
Sekiguchi, Y.: 2010, Fully General Relativistic Simulations ofFormation of Black Hole-Accretion Disk System in Collapsar,
Proc. of the workshop on Physics of Compact Objects, Eds.
K. Uryu, S. Yoshida, S. Yoshida, N. Masuda, K. Taniguchi, S.
Karino, 140-149.
Sekiguchi, Y.: 2011, Black hole and accretion disk formation in
the collapsar model, Proc. of the 20th workshop on General
Relativity and Gravitation in Japan, Eds. M. Shibata, M.,
Sasaki, T. Tanaka, J. Soda, T. Shiromizu, N. Seto, 63.
Selam, S. O., Yilmaz, M., Izumiura, H., Bikmaev, I., Sato, B.,
Kambe, E., Keskin, V.: 2010, Precise Radial Velocity Measurements:
Key to Discover Low-mass Companions and Exoplanets AroundStars, ASP Conf. Ser. 435, Eds. A., Prša, M. Zejda, 413.
Shibasaki, K., Narukage, N., Yoshimura, K.: 2011, Imaging

Observations of Coronal Magnetic Field by Nobeyama
Radioheliograph, ASP Conf. Ser. 437, Eds. J. R. Kuhn, S. V.
Berdyugina, D. M. Harrington, S. Keil, H. Lin, T. Rimmele, B. J.
Trujillo, 433-435.
Shigeyama, T., Nakamura, K., Tsujimoto, T., Moriya, T.: 2010,
GRB Nucleosynthesis in Dwarf Galaxies, AIP Conf. Proc. 1279,
Eds. N. Kawai, S. Nagataki, 415-417.
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Takata, T.,
Yasuda, N.: 2010, AGN and Galaxy Clustering at z = 0.3–3.0
Using the Japanese Virtual Observatory, Proc. IAU Symp. 267,
Eds. B. M. Peterson, R. S. Somerville, T. Storchi-Bergmann, 267.
Shirasaki, Y., Ohishi, M., Mizumoto, Y., Takata, T., Tanaka, M.,
Yasuda, N.: 2010, Environment Study of AGNs at z = 0.3 to 3.0
Using the Japanese Virtual Observatory, ASP Conf. Ser. 434,
Eds. Y. Mizumoto, K.-I. Morita, M. Ohishi, 402-405.
Sivaramakrishnan, A., et al. including Martinache, F.: 2010,
Planetary system and star formation science with non-redundantmasking on JWST, Proc. SPIE 7731, Eds. J. M. Oschmann Jr., M.
C. Clampin, H. A. MacEwen, 3W.
Sôma, M., Tanikawa, K.: 2011, ΔT around AD 520 from Chinese
Records of Eclipses and Occultations, Proc. of the 4th Symp. on"History of Astronomy", Eds. M. Sôma, K. Tanikawa, 1-4.
Sotani, H.: 2010, Stellar oscillations in TeVeS, J. Phys.: Conf. Ser.,
229, Eds. R. Lazkoz, R. Vera, 012069.
Sotani, H., Kokkotas, K. D.: 2010, Polar oscillations in magnetars,
J. Phys.: Conf. Ser., 229, Eds. R. Lazkoz, R. Vera, 012079.
Suda, T., Komiya, Y., Habe, A., Yamada, S., Katsuta, Y., Nishimura,T., Ishizuka, C., Fujimoto, M. Y.: 2010, Pan Binary Scenario for
the Origin of Extremely Metal-Poor Stars in the Galactic Halo,ASP Conf. Ser. 435, Eds. A. Prša, M. Zejda, 360-362.
Suematsu, Y., Katsukawa, Y., Shimizu, T., Ichimoto, K., Horiuchi,T., Matsumoto, Y., Takeyama, N.: 2010, Optical and Thermal
Design of 1.5-m Aperture Solar UV Visible and IR Observing
Telescope for Solar-C Mission, Proc. of Int. Conf. of Space
Optics 2010, Eds. N. Karafolas, C. Kalamida, Session 4b, pp. 1-4.
Suzuki, R., Kudo, T., Hashimoto, J., Carson, J., Egner, S., Goto, M.,
Hattori, M., Hayano, Y., Hodapp, K., Ito, M., Iye, M., Jacobson,
S., Kandori, R., Kusakabe, N., Kuzuhara, M., Matsuo, T.,
McElwain, M., Morino, J.-I., Oya, S., Saito, Y., Shelton, R.,
Stahlberger, V., Suto, H., Takami, H., Thalmann, C., Watanabe, M.,
Yamada, H., Tamura, M.: 2010, Performance characterization of
the HiCIAO instrument for the Subaru Telescope, Proc. SPIE 7735,
Eds. I. S. McLean, S. K. Ramsay, H. Takami, 30.
Suzuki, R., Usuda, T., Crampton, D., Larkin, J., Moore, A., Phillips,
A., Simard, L.: 2010, The infrared imaging spectrograph (IRIS)
for TMT: imager design, Proc. SPIE 7735, Eds. I. S. McLean, S.
K. Ramsay, H. Takami, 5S.
Takahashi H. R., Kotake K., Yasutake N.: 2011, Stability MRITurbulent Accretion Disks, The First Year of MAXI: Monitoring
Variable X-ray Sources, Eds. K. Ebisawa, N. Kawai, online
available at http://maxi.riken.jp/FirstYear, id.9.
Takahashi, H. R., Matsumoto, J., Masada, Y., Kudoh, T.: 2010,
Numerical Study of Relativistic Magnetic Reconnections, AIP
Conf. Proc. 1279, 427-429.
Takahashi, H., Matsuo, H., Nakanishi, K.: 2010, Spectroscopic
Imaging Study of Nearby Spiral Galaxies: Introduction of

II Publications, Presentations

085

Observations with AKARI, NRO and ASTE, ASP Conf. Ser., 418,
Eds. T. Onaka, G. J. White, T. Nakagawa, I. Yamamura, 491-494.
Takahashi, S., Takano, S., Iono, D., Kuno, N.: 2010, Doppler
shift Correction for 2SB Receiver of the 45m Telescope at the
Nobeyama Radio Observatory, ASP Conf. Ser. 434, Eds. Y.
Mizumoto, K.-I. Morita, M. Ohishi, 425-428.
Takato, N., Usuda, T.: 2010, Instrumentation at the Subaru Telescope,Proc. SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 4.
Takiwaki, T., Harikae, S., Kotake K.: 2010, Neutrino Pair
Annihilation in Collapsars, AIP Conf. Proc. 1279, Eds. N.
Kawai, S. Nagataki, 430-432.
Tamura, M., SEEDS Team: 2010, First results from SEEDS,
Proc. Conf. in the Spirit of Lyot 2010, Ed. A. Boccaletti, 15.
Tanaka, M., Kawabata, K. S., Hattori, T., Aoki, K., Iye, M.,
Maeda, K., Mazzali, P. A., Nomoto, K., Pian, E., Sasaki, T.,
Yamanaka, M.: 2010, Multi-Dimensional Explosion Geometryof Supernovae: Spectropolarimetric Study with Subaru, AIP
Conf. Proc. 1279, Eds. N. Kawai, S. Nagataki, 433-435.
Tavrov, A., Korablev, O., Ksanfomaliti, L., Gnedykh, V., Rodin, A.,
Nishikawa, J., Tamura, M., Takeda, M., Kurokawa, T.: 2010,
A 400-3500 nm spectroscopy through a common-path interfero
coronagraph instrument on 600 mm telescope on RS ISS, Proc.
Conf. in the Spirit of Lyot 2010, Ed. A. Boccaletti, 82.
Thalmann, C., Grady, C. A., Goto, M., Wisniewski, J. P., Janson,
M., Henning, T., Fukagawa, M., Honda, M., Mulders, G. D.,
Min, M., Moro-Martin, A., McElwain, M. W., Hodapp, K. W.,
Carson, J., Tamura, M., SEEDS Team: 2010, Ongoing planet
formation around LkCa 15?, Proc. Conf. in the Spirit of Lyot
2010, Ed. A. Boccaletti, 33.
Tokunaga, A. T., Packham, C., Okamoto, Y. K., Kataza, H.,
Richter, M., Carr, J., Chun, M., Telesco, C., Honda, M., Najita, J.,
Onaka, T., Sakon, I., Yamashita, T.: 2010, Design concepts fora mid-infrared instrument for the Thirty-Meter Telescope, Proc.
SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 2C.
Tsujimoto, T.: 2010, Galaxy Formation through Winds, Infall, andMerger: Learning from Galactic Archaeology, AIP Conf. Proc.
1240, Eds. V. P. Debattista, C, C. Popescu, 175-176.
Tsujimoto, T.: 2011, Science brought by JASMINE data, EAS
Publications Series, 45, Eds. C. Turon, F. Meynadier, F. Arenou,
445-448
Tsujimoto, T., Bland-Hawthorn, J.: 2010, Chemical Evolution of
D in the Local Disk, Proc. IAU Symp. 268, Eds. C. Charbonnel,
M. Tosi, F. Primas, C. Chiappini, 499-500.
Ueda, H., Gouda, N., Yano, T., Koyama, H., Sakagami, M.: 2010,
A New Approach to the Construction of Dynamical Structure of
our Galaxy, Highlights of Astronomy, 15, Ed. I. Corbett, 202.
Ukita, N., Ezawa, H., Onodera, S., Saito, M.: 2010, Wind-induced
pointing errors and surface deformation of a 10-m submillimeter
antenna, Proc. SPIE 7733, Eds. L. M. Stepp, R. Gilmozzi, H. J.
Hall, 1D.
Vogt, F., Martinache, F., Guyon, O., Yoshikawa, T., Yokochi,
K., Garrel, V., Matsuo, T.: 2010, The Subaru Coronagraphic
Extreme AO (SCExAO) system: implementation andperformance of the Coronagraphic Low Order Wavefront
Sensor, Proc. SPIE 7736, Eds. E. Hart, H. Wizinowich, 12.
Wakabayashi, Y., Obuchi, Y., Okada, N., Torii, Y., Ejiri, Y., Suzuki,

086

II Publications, Presentations

R., Ueda, A., Kawamura, S., Araya, A., Ando, M., Sato, S.,
Sugamoto, A.: 2010, Structural design and analysis of test mass
module for DECIGO Pathfinder, J. Phys.: Conf. Ser., 228, 012047.
Watanabe, J., Jenniskens, P., Spurny, P., Borovi'ka, J., CampbellBrown, M., Consolmagno, G., Jopek, T., Vaubaillon, J., Williams,
I P., Zhu, J.: 2010, Commission 22: Meters, Meteorites andInterplanetary Dust, Transactions of the IAU, XXVII A, Ed. K.
A. van der Hucht.
Watanabe, M., Ito, M., Oya, S., Hayano, Y., Minowa, Y.,
Hattori, M., Saito, Y., Egner, S., Takami, H., Iye, M., Guyon, O.,
Garrel, V., Colley, S., Golota, T.: 2010, Visible low-orderwavefront sensor for the Subaru LGSAO system, Proc. SPIE 7736,
Eds. B. L. Ellerbroek, M. Hart, N. Hubin, P. L. Wizinowich, 183.
Wisniewski, J., Fukagawa, M., Grady, C., Hashimoto, J., Kudo, T.,
Munetake, M., Okamoto, Y., Tamura, M., Hodapp, K., SEEDS
Team: 2010, SEEDS J-band Polarimetric Imagery of the AB
Aur Protoplanetary Disk, Proc. Conf. in the Spirit of Lyot 2010,
Ed. A. Boccaletti, 36.
Yamada, T., et al. including Imanishi, M., Iwata, I., Kobayashi, M.
A. R., Kodama, T., Komiyama, Y., Tsuneta, S.: 2010, WISH:
wide-field imaging surveyor at high redshift, Proc. SPIE 7731,
Eds. J. M. Oschmann Jr., M. C. Clampin, H. A. MacEwen, 1Q.
Yamada, Y., Gouda, N., Lammers, U.: 2011, Nano-JASMINE: useof AGIS for the next astrometric satellite, EAS Publications
Series, 45, Eds. C. Turon, F. Meynadier, F. Arenou, 135-140.
Yamazaki, D., Ichiki, K., Kajino, T., Mathews, G. J.: 2011,
Primordial Magnetic Field Effects on the CMB and Large Scale
Structure, Advances in Astronomy, 586590.
Yanagisawa, K., Kuroda, D., Yoshida, M., Shimizu, Y., Nagayama,S., Toda, H., Ohta, K., Kawai, N.: 2010, Six years of GRB
follow up with MITSuME Okayama Telescope, AIP Conf. Proc.
1279, Eds. N. Kawai, S. Nagataki, 466-468.
Yano, T., Araki, H., Hanada, H., Tazawa, S., Gouda, N., Kobayashi,Y., Yamada, Y., Niwa, Y.: 2010, Centroiding Experiment for
Determining the Positions of Stars with High Precision, ASP
Conf. Ser. 434, Eds. Y. Mizumoto, K.-I. Morita, M. Ohishi, 151.
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Hatsutori, Y.,
Murooka, J., Niwa, Y., Yamada, Y.: 2011, Current Status of
Astrometry Satellite missions in Japan: JASMINE project series,
EAS Publications Series, 45, Eds. C. Turon, F. Meynadier, F.
Arenou, 449-452.
Yasutake, N., Maruyama, T., Tatsumi, T.: 2010, Finite-size effects
on hot hadron-quark mixed phase including hyperons, AIP
Conf. Proc. 1269, Eds. I. Tanihata, T. Shima, H. J. Ong, A.
Tamii, T. Kishimoto, H. Toki, T. Kajino, S. Kubono, 381-383.
Yatsu, Y., Nakajima, H., Enomoo, T., Tokoyoda, K., Kawakami,K., Kawai, N., Asano, K., Shimokawabe, T., Mori, Y. A., Endo,
H., Kuroda, D., Yanagisawa, K., Nagayama, S., Shimizu, Y.,
Toda, H., Hanayama, H., Yoshida, M., Ohta, K.: 2010, Opticalobservations of the very early phase GRB afterglows with
MITSuME, The First Year of MAXI: Monitoring Variable X-ray
Sources, Eds. K. Ebisawa, N. Kawai.
Yoshida, F.: 2011, The project “Stars of Asia”: Asian Myths andLegends of Stars and the Universe, Proc. of the 8th East Asian
Meeting on Astron. Symp., 86.
Yoshida, M., Yanagisawa, K., Kuroda, D., Ohta, K., Kawai, N.:2010, Near-Infrared Photometry of the afterglow of GRB 090423,
AIP Conf. Proc. 1279, Eds. N. Kawai, S. Nagataki, 469-471.
Yuk, I.-S., et al. including Pyo, T.-S.: 2010, Preliminary design of
IGRINS (Immersion GRating INfrared Spectrograph), Proc.
SPIE 7735, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 54-43.

5. Publications in English
Nakagawa, A., Takahashi, K., Hagiwara, Y., Nakanishi, H.: 2011,
Proceedings book "SKA-JAPAN 2010 WORKSHOP", SKAJapan Workshop Organizing Members, Kagoshima, Japan.
Nakata, F., Yagi, M., Komiyama, Y., Shinogi, S., Yoshida, F.,
Marsden, B. G.: 2010, 2009 KO30, 2009 KN30, 2009 KL30,
2009 KK30, Minor Planet Electronic Circ.
Tanihata, I., et al. including Kajino, T.: 2010, Origin of Matter and
Evolution of Galaxies, AIP , New York.

6. Conference Presentations
Agata, H.: 2010, Report of IYA2009 in Japan, 8th EAMA (East
Asian Meeting on Astronomy) Symp., (Shanghai, China, Oct.
10-15, 2010).
Agata, H.: 2011, Introduction to Astronomy on NAOJ, You are
Galileo!' workshop, (Mataram, Indonesia, Feb. 27, 2011).
Agata, H.: 2011, Introduction to Astronomy & Astronomical
Education on NAOJ, You are Galileo!' workshop, (Tomohon,
Indonesia, Mar. 2, 2011).
Agatsuma, K., Mori, T., Ballmer, S., Sakata, S., Reid, S., Miyakawa,O., Numata, K., Furusawa, A., Kawamura, S.: 2010, Status of
QND experiment in NAOJ, LSC (LIGO Scientific Collaboration)Virgo Meeting, (Cracow, Poland, Sep. 20-24, 2010).
Aikawa, Y.: 2010, Hydrocarbon chemistry in star-forming regions
and protoplanetary disks, The Methane Balance - Formation
and Destruction Processes on Planets, their Satellites and in theInterstellar Medium, (Bern, Switzerland, Nov. 16-18, 2010).
Akiyama, K.: 2010, Multi-Epoch VERA observations of Sagittarius
A*, Towards a root of AGN jets: Recent progress, (Mitaka,
Japan, Dec. 14-15, 2010).
Akutsu, T., DECIGO Working Group: 2010, DECIGO andDECIGO Pathfinder, 19th Int. Conf. on General Relativity andGravitation (GR19), (Mexico City, Mexico, Jul. 5-9, 2010).
Anan, T., Ichimoto, K., Ueno, S., Kimura, G., Nakatani, Y.,
Kaneda, N., Hagino, M., Suzuki, I.: 2010, Developments of theMulti-Wavelength Polarimeter of the Domeless Solar Telescopeat the Hida Observatory, 6th Solar Polarization Workshop,(Maui, HI, USA, May 31-June 4, 2010).
Aoki, W.: 2010, Galactic Archaeology with SuMIRe PFS, The
observational pursuit of dark energy after Astro2010, (Pasadena,
CA, USA, Oct. 7-8, 2010).
Aoki, W., Beers, T.C., Honda, S., Carollo, S., Ito, H., Lee, Y. S.:
2010, A systematic study of extremely metal-poor stars with
SDSS/Subaru, Nuclei in the Cosmos XI, (Heidlberg, Germany,
Jul. 19-23, 2010).
Aoki, W., Honda, S.: 2010, Enrichment of heavy elements in the
Sextans dwarf Spheroidal Galaxy, Nuclei in the Cosmos XI,(Heidlberg, Germany, Jul. 19-23, 2010).

Araki, H., Sasaki, S., Hanada, H., Noda, H., Kunimori, H.,
Kikuchi, F., Matsumoto, K., Iwata, T., Kawano, N., Funazaki,
K., RISE Group.: 2010, Investigations of In Situ Lunar Geodetic
Experiments in Japan for the Study of the Interior of the Moon,
EPSC (European Planetary Sciences Conf.), (Roma, Italy, Sep.
20-24, 2010).
Araki, H., Sasaki, S., Ishihara, Y., Noda, H., Hanada, H.,
Matsumoto, K., Kikuchi, F., Goossens, S., Namiki, N., Iwata,T.: 2010, The First Global Topography and Gravimetry of theMoon by KAGUYA, EPSC (European Planetary Sciences
Conf.), (Roma, Italy, Sep. 20-24, 2010).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S., Sasaki,
S.: 2011, The second version of the Lunar topographic data sets
by KAGUYA-LALT, The 5th KAGUYA (SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 17-19, 2011).
Araki, M., Koshikawa, N., Yamabe, H., Umeki, H., Tsukiyama, K.,
Takano, S., Kuze, N.: 2010, Spectral Lines of Carbon Chain
Molecule in a Star Forming Region L1527 between 29 and 90
GHz, Workshop on Interstellar Matter 2010, (Sapporo, Japan,
Sept. 13-15, 2010).
Ballmer, S.: 2010, Thoughts on optimizing coating thermal
noise, Gravitational-Wave Advanced Detector Workshop
2010(GWADW2010), (Kyoto, Japan, May 16-21, 2010).
Berger, T., Okamoto, J., Labrosse, N.: 2010, Diagnostics ofprominence structure, dynamics, and radiation with Hinode
SOT & EIS, Hinode-IV: unsolved problems and recent insights,(Mondello, Palermo, Italy, Oct. 11-15, 2010).
Deguchi, S.: 2010, HOCO+ toward Sgr B2 Complex, Workshop on
Interstellar Matter 2010, (Sapporo, Japan, Sept. 13-15, 2010).
Enya, K., et al. including Yamashita, T., Narita, N., Tamura, M.,
Nishikawa, J., Hayano, Y., Oya, S., Kokubo, E., Guyon, O.:2010, SPICA Capability for Studying Transiting Exoplanets,
38th COSPAR Scientific Assembly, (Bremen, Germany, Jul.
18-25, 2010).
Fujii, Y., Uzawa, Y., Kaneko, K., Kroug, M., Gonzalez, A.,
Kuroiwa, K., Miyachi, A., Ogawa, H., Makise, K., Wang,
Z., Wang, M., Shan, W.: 2010, Development of the 787–
950 GHz ALMA Band 10 Cartridge, The 11th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Nagoya, Japan, Nov. 14-16, 2010).
Fujiwara, K., Tsuiki, A., Kamiyoshi, S., Utsunomiya, S., Yasuda,S., Sato, Y., Gouda, N., Kobayashi, Y., Yano, T., Hatsutori,Y., Niwa, Y., Yamada, Y.: 2010, Preliminary Design of High
Precision Tip-Tilt Mirror Control System for the small
JASMINE satellite, 11th Annual Summer School on Adaptive
Optics, (CA, USA, Aug. 8-13, 2010).
Fukue, T., Tamura, M., Kandori, R., Kusakabe, N., Hough,J. H., Lucas, P. W., Bailey, J., Whittet, D. C. B., Nakajima,Y., Hashimoto, J., Nagata, T.: 2010, Near-Infrared Imageof Circular Polarization in the Orion Nebula, Workshop on
Interstellar Matter 2010, (Sapporo, Japan, Sept. 13-15, 2010).
Fukue, T., Tamura, M., Kandori, R., Kusakabe, N., Hough, J.
H., Lucas, P. W., Bailey, J., Whittet, D. C. B., Nakajima, Y.,
Hashimoto, J., Nagata, T.: 2010, Circular Polarimetry of theOrion Nebula by SIRPOL, AOGS 2010, (Hyderabad, India, Jul.
5-9, 2010）.

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087

Furuya, K., Aikawa, Y., Sakai, N., Yamamoto, S.: 2010, Carbon
Isotope and Isotopomer Fractionation in Cold Dense Cloud
Cores, Workshop on Interstellar Matter 2010, (Sapporo, Japan,
Sept. 13-15, 2010).
Gao, Yu., Zhang, H., Kuzanyan, K., Xu, H., Sokoloff, D.:2010, Polarity Rule for Vector Magnetic Fields in the Solar
Photosphere, 38th COSPAR Scientific Assembly, (Bremen,
Germany, Jul. 18-25, 2010).
Giroletti, M., Paragi, Z., Bignall, H., Foschini, L., Blanchard, J.,
Colomer, F., Doi, A., Hong, X., Kadler, M., Kino, M., vanLangevelde, H. J., Nagai, H., Phillips, C., Sekido, M., Szomoru,A., Tzioumis, A. K.: 2010, The rst scienti c experiment using
Global eVLBI observations: a multiwavelength campaign on
the gamma-ray Narrow-Line Seyfert 1 PMN J0948+0022, The
10th European VLBI Network Symposium: VLBI and the New
Generation of Radio Arrays, (Manchester, UK, Sep. 20-24, 2010).
Gonzalez, A., Uzawa, Y., Fujii, Y., Kaneko, K., Kroug, M.,
Kuroiwa, K., Miyachi, A.: 2010, Beam Performance
Characterization of ALMA Band 10 Cartridge, The 11th
Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Goossens, S., Matsumoto, K., Ishihara, Y., Liu, Q., Kikuchi, F.,
Hanada, H., Noda, H., Namiki, N., Iwata, T.: 2010, SELENE
Orbit Determination And Gravity Field Model Evaluation, 38th
COSPAR Scientific Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Goossens, S., Matsumoto, K., Kikuchi, F., Liu, Q., Hanada,
H., Lemoine, F. G., Rowlands, D. D., Ishihara, Y., Yan, J.,
Araki, H., Noda, H., Namiki, N., Iwata, T.: 2010, Analysis ofMulti-Satellite Tracking Data of the Kaguya Satellites for Orbit
and Gravity Field Determination, AGU Fall Meeting, (SanFrancisco, CA, USA, Dec. 13-17, 2010).
Goossens, S., Matsumoto, K., Liu, Q., Kikuchi, F., Hanada, H.,
Ishihara, Y., Noda, H., Kawano, N., Lemoine, F. G., Rowlands,
D. D., Namiki, N., Iwata, T., Sasaki, S., Yan, J.: 2011, Overview
of Kaguya lunar gravity field determination results, The 5th
KAGUYA (SELENE) Science Working Team Meeting, (Tokyo,
Japan, Jan. 17-19, 2011).
Gouda, N., JASMINE working group: 2010, Series of JASMINE
Missions, ELSA conference 2010 GAIA: At the Frontiers of
Astrometry, (Sèvres, France, Jun. 7-11, 2010).
Hada, K.: 2010, Nailing down the black hole location in M87,
Towards a root of AGN jets: Recent progress, (Mitaka, Japan,
Dec. 14-15, 2010).
Hagino, M., Hanaoka, Y., Sakurai, T., Ichimoto, K.: 2010,
Quantitative Comparison between the Polarization Data Taken
with the Solar Flare Telescope and with the Hinode SOTSpectro-Polarimeter, 6th Solar Polarization Workshop, (Maui,
HI, USA, May 31-June 4, 2010).
Hagiwara, Y.: 2010, Ground radio telescope support for VSOP-2:
An overview, East Asia VLBI Workshop 2010, (Kagoshima,
Japan, Apr. 22-24, 2010).
Hagiwara, Y.: 2010, EVN Observations of active galaxy NGC
6240, The 10th European VLBI Network Symposium: VLBI
and the New Generation of Radio Arrays, (Manchester, UK,
Sep. 20-24, 2010).
Hagiwara, Y.: 2010, VLBI observations of double nuclei of an088

II Publications, Presentations

active galaxy NGC 6240, Towards a root of AGN jets: Recent
progress, (Mitaka, Japan, Dec. 14-15, 2010).
Hagiwara, Y.: 2011, Science: VLBI (Extragalactic), East-Asia
Interferometry Winter School, (Mitaka, Japan, Feb. 7-11, 2011).
Hamana, T.: 2010, Searching for clusters with weak lensing and
HSC survey, CL J2010: from Massive Galaxy Formation to
Dark Energy, (Kashiwa, Japan, Jun. 28-Jul. 2, 2010).
Hanada, H., Noda, H., Kikuchi, F., Sasaki, S., Iwata, T., Kunimori,
H., Funazaki, K., Araki, H., Matsumoto, K., Tazawa, S.,
Tsuruta, S.: 2010, Development of selenodetic instruments forJapanese lunar explorer SELENE-2, The first Moscow Solar
System Symp. (1MS3), (Moscow, Russia, Oct. 11-15, 2010).
Hanada, H., Ping, J., Funazaki, K., Kawano, N., Petrova, N., Araki,
H., Tazawa, S., Tsuruta, S., Noda, H., Asari, K., Sasaki, S., Li,
Z., Su, X., Satoh, A., Taniguchi, H., Kikuchi, M., Takahashi,T., Yamazaki, A., Murata, K., Iwata, T.: 2010, Development ofa photographic zenith tube for observation of the lunar rotationand the deflection of the vertical, IAG symp. on terrestrial
gravimetry, (Saint Petersburg, Russia, Jun. 22-25, 2010).
Hanaoka, Y.: 2010, Scientific and Educational Applications of a
Small Coelostat/Spectrograph System, 1st Latin American FMT
Workshop, (Ica, Peru, Nov. 22-26, 2010).
Hanaoka, Y., Kikuta, Y., Nakazawa, J., Ohnishi, K., Shiota, K.:
2010, Brightness of the white light corona measured at the
total solar eclipses in 2008 and 2009, 38th COSPAR Scientific
Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Hanayama, H.: 2010, Generation Process of Seed Magnetic Fields
with Biermann Mechanism in Primordial Supernova Remnants,
Japan SKA Int. Workshop 2010, (Mitaka, Japan, Nov. 4-5,
2010).
Hanayama, H., Miyaji, T.: 2010, Ishigakijima Astronomical
Observatory and Murikabushi 105cm Telescope, An Ishigaki
Int. Conf. on Evolving Theory for Planet Formation, (Ishigaki,
Japan, Jun. 20-26, 2010).
Hara, H.: 2010, Coronal Plasma Motions at the Site of Coronal
Heating in Active Region Loops, AGU, 2010 Meeting of theAmericas, (Iguassu, Brazil, Aug. 9-12, 2010).
Hara, H.: 2010, Spectroscopic Observations of Magnetic Reconnection in the Solar Corona, Mgnetic Reconnection 2010,(Nara, Japan, Dec. 6-9, 2010).
Hara, H.: 2010, Flows in active regions revealed from Hinode EIS
Observations, 38th COSPAR Scientific Assembly, (Bremen,
Germany, Jul. 18-25, 2010).
Hara, H.: 2010, Plasma Heating and Velocity Fields nearby
Magnetic Reconnection Site Revealed from an EUV Emissionline Spectroscopy, 38th COSPAR Scientific Assembly, (Bremen,
Germany, Jul. 18-25, 2010).
Hara, H.: 2010, Magnetic Structures Associated with Unresolved
Fast Coronal Upflows in Plage Regions, Hinode-IV: unsolved
problems and recent insights, (Mondello, Palermo, Italy, Oct.
11-15, 2010).
Hashimoto, K., Watanabe, J., Sato, M.: 2010, Identification of
optical component of North Toroidal Source of sporadic meteors
and its origin, Meteoroids 2010, An Int. Conf. on Minor Bodies
in the Solar System, (Breckenridge, CO, USA, May 24-28,
2010).

Hashimoto, T., Ohta, K., Aoki, K., Tanaka, I., Yabe, K., Kawai,N., Aoki, W., Furusawa, H., Hattori, T., Iye, M., Kawabata,K. S., Kobayashi, N., Komiyama, Y., Kosugi, G., Minowa, Y.,
Mizumoto, Y., Niino, Y., Nomoto, K., Noumaru, J., Ogasawara,
R., Pyo, T.-S., Sakamoto, T., Sekiguchi, K., Shirasaki, Y.,
Suzuki, M., Tajitsu, A., Takata, T., Tamagawa, T., Terada,
H., Totani, T., Watanabe, J., Yamada, T., Yoshida, A.: 2010,"Dark'' GRB 080325 in a dusty massive galaxy at z~2, 26th IAP
Annual Colloquium "Progenitors and environments of stellar
explosions", (Paris, France, Jun. 28-Jul. 2, 2010).
Hashimoto, T., Ohta, K., Aoki, K., Tanaka, I., Yabe, K., Kawai,N., Aoki, W., Furusawa, H., Hattori, T., Iye, M., Kawabata,K. S., Kobayashi, N., Komiyama, Y., Kosugi, G., Minowa, Y.,
Mizumoto, Y., Niino, Y., Nomoto, K., Noumaru, J., Ogasawara,
R., Pyo, T.-S., Sakamoto, T., Sekiguchi, K., Shirasaki, Y., Suzuki,M., Tajitsu, A., Takata, T., Tamagawa, T., Terada, H., Totani,T., Watanabe, J., Yamada, T., Yoshida, A.: 2010, "Dark" GRB
080325 in a Dusty Massive Galaxy at z ~ 2, Deciphering theAncient Universe with Gamma-Ray Bursts, (Kyoto, Japan, Apr.
19-23, 2010).
Hatsutori, Y., Kobayashi, Y., Gouda, N., Yano, T., Murooka, J.,
Niwa, Y., Yamada, Y.: 2010, Performance Evaluation of NanoJASMINE, ELSA conference 2010 GAIA: At the Frontiers of
Astrometry, (Sèvres, France, Jun. 7-11, 2010).
Hayashi, M., Kodama, T., Koyama, Y., Tadaki, K.: 2010, A
wide-field survey for [OII] emission in and around a cluster at
z = 1.46, CL J2010: from Massive Galaxy Formation to Dark
Energy, (Kashiwa, Japan, Jun. 28-Jul. 2, 2010).
Hayashi, T.: 2010, Multi-frequency polarimetry of radio-loudbroad absorption quasars, Towards a root of AGN jets: Recent
progress, (Mitaka, Japan, Dec. 14-15, 2010).
Hayashi, T.: 2010, Multi-wavelength polarimetry of radio-loudbroad absorption quasars, Japan SKA Int. Workshop 2010,(Mitaka, Japan, Nov. 4-5, 2010).
Hibi, Y., Matsuo, H., Nagata. H., Ikeda, H., Fujiwara, M.: 2010,
The Cryogenic Readout System with GaAs JFETs for Multipixel Cameras, SPIE Conf., Infrared, Millimeter Wave, andTerahertz Technologies, (Beijing, China, Oct. 18-20, 2010).
Hibi, Y.: 2010, The Cryogenic Readout System and the
Cryogenic OP-Amp With GaAs-JFETs, The 11th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Nagoya, Japan, Nov. 14-16, 2010).
Hirota, T.: 2010, Development of astrometry analysis software;
VEDA, East Asia VLBI Workshop 2010, (Kagoshima, Japan,
Apr. 22-24, 2010).
Hirota, T.: 2010, Astrometry of H2O maser sources in nearby
star-forming regions with VERA, The 10th European VLBI
Network Symposium: VLBI and the New Generation of Radio
Arrays, (Manchester, UK, Sep. 20-24, 2010).
Hirota, T.: 2010, VLBI Observations of Galactic radio sources,
Japan SKA Int. Workshop 2010, (Mitaka, Japan, Nov. 4-5, 2010).
Hirota, T.: 2011, Proposal preparation, East-Asia Interferometry
Winter School, (Mitaka, Japan, Feb. 7-11, 2011).
Hong, P. K., Sugita, S., Okamura, N., Sekine, Y., Terada, H.,
Takatoh, N., Hayano, Y., Fuse, T., Kawakita, H., Wooden,
D. H., Young, E. F., Lucey, P. G., Furusho, R., Watanabe, J.,

Haruyama, J., Nakamura, R., Kurosawa, K., Hamura, T., Kadono,T.: 2010, Hot Bands Observation of Water in Ejecta Plume of
LCROSS Impact Using the Subaru Telescope, 41st Lunar andPlanetary Science Conf., (Woodlands, TX, USA, Mar. 1-5, 2010).
Honma, M.: 2010, The structure of the Milky Way Galaxy traced
with VERA, Spiral Structure in the Milky Way: Confronting
Observations and Theory, (Bahia Inglesa, Chile, Nov. 7-10, 2010).
Honma, M.: 2010, sub-mm VLBI observations of super massive
black holes and East Asian VLBI Network, East Asia VLBI
Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Honma, M.: 2010, mm/sub-mm VLBI toward the BH event
horizon, Towards a root of AGN jets: Recent progress, (Mitaka,
Japan, Dec. 14-15, 2010).
Honma, M.: 2010, VERA Key Science Projects (original title in
Korea), 2010 KVN and TRAO Radio Workshop, (Seoul, Korea,
Aug. 16-18, 2010).
Honma, M.: 2011, VERA and the Japan – Korea collaboration,
Future of the VLBA, (Charlottesville, USA, Jan. 27-28, 2011).
Honma, M.: 2011, Interferometry, East-Asia Interferometry WinterSchool, (Mitaka, Japan, Feb. 7-11, 2011).
Ichihashi, Y., Nakayama, H., Awazu, S., Shimobaba, T., Masuda,N., Ito, T.: 2010, Real-Time Reconstruction System Using
Multi Graphics Processing Units for 3D holographic display,
SISA2010, (Manila, Philipine, Sep. 8, 2010).
Ichihashi, Y., Nakayama, H., Awazu, S., Shimobaba, T., Masuda,N., Ito, T.: 2010, Real-Time Reconstruction System Using
High-Performance Computer for Electroholography, ICIS2010,(Yamagata, Japan, Aug. 20, 2010).
Iguchi, S., Saito, M.: 2010, Next Generation Millimeter/Submillimeter Array to Search for 2nd Earh, Asia-Pacific Radio
Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Ikeda, Y., Kobayashi, N., Kuzmenko, P. J., Little, S. L.,Yasui,C., Kondo, S., Mito, H., Nakanishi, K., Sarugaku, Y.: 2010,
Fabrication and current optical performance of a large diamondmachined ZnSe immersion grating, SPIE Astronomical
Instrumentation, (San Diego, CA, USA, Jun. 27-Jul. 2, 2010).
Imanishi, M.: 2010, The AGN-starburst connections in nearby
luminous infrared galaxies, Extrene starbursts in the local
universe, (Granada, Spain, Jun. 21-25, 2010).
Imanishi, M.: 2011, High-redshift QSO study with HSC/PFS,DENET 2011 Subaru HSC workshop, (Taipei, Taiwan, Mar.
7-8, 2011).
Inoue, H., Noguchi, T., Kohno, K.: 2010, SIS junction using asa microwave noise source, Applied Superconductivity Conf.,(Washington DC, USA, Aug. 1-6, 2010).
Ishihara, Y., et al.: 2011, Did the Moscoviense Basin Has Been
Formed by Souble-Impact?, The 5th KAGUYA (SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 17-19, 2011).
Ishihara, Y., Morota, T., Nakamura, R., Goossens, S., Sasaki, S.:
2011, Was the Moscoviense Basin Formed by Double-Impact?,
42nd Lunar and Planetary Science Conf., (Woodsland, TX,
USA, Mar. 7-11, 2011).
Ishikawa, R.: 2010, Ultra deep exposure observations of quiet
Sun magnetic fields, Hinode-IV: unsolved problems and recent
insights, (Mondello, Palermo, Italy, Oct. 11 - 15, 2010).
Ishikawa, R., et al.: 2010, A Sounding rocket experiment for

II Publications, Presentations089

spectropolrimetric observation with Ly-alpha line at 121.6 nm(CLASP), 6th Solar Polarization Workshop, (Maui, HI, USA,May 31-June 4, 2010).
Ishikawa, R.: 2010, The properties and origin of transienthorizontal magnetic fields, 6th Solar Polarization Workshop,(Maui, HI, USA, May 31-June 4, 2010).
Ishitsu, N., Inutsuka, S., Sekiya, M.: 2010, Dust diffusion by thestreaming instability in a protoplanetary disk, An Ishigaki Int.
Conf. on Evolving Theory for Planet Formation, (Ishigaki,
Japan, Jun. 20-26, 2010).
Ishiyama, T.: 2010, Variation of the Subhalo Abundance in Dark
Matter Halos, CL J2010: from Massive Galaxy Formation to
Dark Energy, (Kashiwa, Japan, Jun. 28-Jul. 2, 2010).
Ishiyama, T.: 2010, Bias-free survey of subhalos in dark matter
halos, Evolution of galaxies, their central black holes and theirlarge-scale environment, (Potsdam, Germany, Sep. 20-24, 2010).
Ishiyama, T.: 2010, High Resolution Simulations of Small Scale
Structures of Dark Matter Halos, The 4th East Asian Numerical
Astrophysics Meeting, (Taipei, Taiwan, Nov. 2-5, 2010).
Ito, T.: 2010, Comparison of seeing between Maidanak andNyukasa, Maidanak Users Meeting 2010, (Tashkent,
Uzbekistan, June 21-25, 2010).
Ito, T., Higuchi, A.: 2010, Impact probability of the Oort cloudcomets on planets, AOGS 2010, (Hyderabad, India, Jul. 5-9,2010）.
Ito, T., Malhotra, R.: 2010, Asymmetric cratering due to a steadystate NEA flux on the Moon, AOGS 2010, (Hyderabad, India,
Jul. 5-9, 2010).
Iwai, K., Masuda, S., Miyoshi, Y., Shimojo, M., Misawa, H.,
Tsuchiya, F., Morioka, A.: 2010, Relationship between solar
radio type-I noise storm and Coronal Mass Ejection, AGU Fall
Meeting, (San Francisco, CA, USA, Dec. 13-17, 2010).
Iwata, T., Hanada, H., Noda, H., Kikuchi, F., Harada, Y.: 2010,
Lunar, Martian, and Jovian geodesy, and science observation
using VLBI and astrometrical technology, The first Moscow Solar
System Symp. (1MS3), (Moscow, Russia, Oct. 11-15, 2010).
Izumiura, H., Ueta, T., Yamamura, I., Nakada, Y., Matsunagata,N., Ita, Y., Matsuura, M., Fukushi, H., Mito, H., Tanabe, T.,
Sorahana, T., Hashimoto, O.: 2010, Symmetric and asymmetriccircumstellar dust shells in evolved stars revealed by AKARI,
Asymmetric Planetary Nebulae 5, (Bowness-on-Windermere,
England, Jun. 20-25, 2010).
Kajino, T.: 2010, Nuclear Weak Interactions and Supernova
Neutrino- and R-Processes, 3rd Int. Conf. on Frontiers In
Nuclear Structure, Astrophysics and Reactions, (Rhodos,
Greece, Aug. 23-27, 2010).
Kajino, T.: 2010, Supernova neutrinos, nucleosynthesis, andneutrino oscillation, Symp. at Joint Institute for Nuclear
Astrophysics, (East Lansing, USA, Apr. 18-20, 2010).
Kajino, T.: 2010, Supernova neutrino process and nuclear
structure, Workshop on Nuclear Astrophysics, (Tokyo, Japan,
Jun. 26, 2010).
Kajino, T.: 2010, Nuclear astrophysics - theory, Workshop on the
Nuclear Physics and Nuclear Astrophysics, (Seoul, Korea, Oct.
26-27, 2010).
Kajino, T.: 2010, Nucleosynthesis and neutrinos, Int. Symp. on090

II Publications, Presentations

New Faces of Atomic Nuclei, (Okinawa, Japan, Nov. 15-17, 2010).
Kajino, T.: 2010, Similarity between 3a→C12+g and 2a+n→Be9+g
rates and their implication in SN r-process, RNC Workshop on
Impact of Triple-Alpha Reaction Rate on Stellar Evolution and
Nucleosynthesis, (Nishina, Japan, Dec. 17-18, 2010).
Kajino, T.: 2010, C12(a,g)O16 reaction in massive stars - Implicationin gamma-ray line astronomy of Al26 and Fe60, 3rd Instituteof Origin of Matter and Evolution of Galaxies, (Tokyo, Japan,
Nov. 1, 2010).
Kajino, T.: 2010, Nucleosynthesis in Gamma-Ray Bursts andExtremely Metal-Deficient Halo Stars, 24th Int. Nuclear Physics
Conf., (Vancouver, Canada, Jul. 7 - 9, 2010).
Kajino, T.: 2011, Supernova Nucleosynthesis, Neutrino Oscillation,
and Nuclear Weak Interactions, French-Japanese Symposium on
Nuclear Structure Problems, (Wako, Japan, Jan. 5-8, 2011).
Kajino, T.: 2011, Origin and Evolution of the Universe; fromthe Big-Bang to the Element Genesis, Sokendai Asian WinterSchool on Science of Structure Formation - Light, Energy,
Material, and Space, (Toki, Japan, Feb. 15-18, 2011).
Kambe, E.: 2010, Status Report on Commissioning Observations
with the Fiber-link of 188-cm Telescope and HIDES, China-Japan
collaboration project meeting, (Xinglong, China, Nov. 25, 2010).
Kameya, O.: 2010, Pulsar study using the SKA, Japan SKA Int.
Workshop 2010, (Mitaka, Japan, Nov. 4-5, 2010).
Kameya, O., Tatsuzawa, K., Okayasu, R., Chikada, Y., Kawabe,R., Yamamoto, S., Kawaguchi, N.: 2010, Interference Caused
by 79GHz High Resolution Radars for Automotive Applications–an estimation of co-existence between Radio Astronomy and
79GHz SRRs– NOBEYAMA 45m Radio Telescope, Asia-PacificRadio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Kano, R.: 2010, Multi-thermal Structures Above a Polar Region
Observed with XRT and EIS, 2010 XRT Team Meeting,(Bozeman, MT, USA, Jun. 16-18, 2010).
Kano, R.: 2010, Super-hot component in non-flaring active
regions, Hinode-IV: unsolved problems and recent insights,(Mondello, Palermo, Italy, Oct. 11-15, 2010).
Kashikawa, N.: 2010, Probing EoRwith LAE surveys, The firstgalaxies, QSOs & GRBs, (Penn State University, PA, USA, Jun.
7-11, 2010).
Kashikawa, N.: 2011, Concluding the census of LAEs at thereionization epoch w/Subaru+Keck, Subaru Users Meeting,(Mitaka, Japan, Jan. 19-20, 2011).
Kashikawa, N.: 2011, Current status and activities in Japan: Future
Instrument Plan, TMT Science and Instrument WS, (Victoria,
Canada, Mar. 28-30).
Katase, T., Kimura, K., Muraoka, K., Onishi, T., Ogawa, H.,
Nakajima, T., Kuno, N., Kawabe, R.: 2010, Development ofa New 2×2 Multi Beams Receiver for Nobeyama 45m Radio
Telescope, The 11th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Kato, Y., Steiner, O., Steffen, M., Suematsu, Y.: 2010, Excitation of
acoustic waves in network magnetic elements, IAU Symp. 273,
(Ventura, CA, USA, Aug. 22­26, 2010).
Kato, Y., Steiner, O., Steffen, M., Suematsu, Y.: 2010, Excitationof Slow-Mode Waves in Network Magnetic Element, HinodeIV: unsolved problems and recent insights, (Mondello, Palermo,

Italy, Oct. 11-15, 2010).
Katsukawa, Y., Asensio Ramos, A., Trujillo Bueno J.: 2010,
Hanle-Zeeman Diagnostics of Active Region Filaments in He
I 10830A, Hinode-IV: unsolved problems and recent insights,(Mondello, Palermo, Italy, Oct. 11-15, 2010).
Katsukawa, Y., Masada, Y., Shimizu, T., Sakai, S., Ichimoto, K.:
2010, Pointing stability of Hinode and requirements for the next
solar mission Solar-C, Int. Conf. on Space Optics, (Rhodes,
Greece, Oct. 4-8, 2010).
Katsukawa, Y., Orozco Suarez, D.: 2010, Power spectral analysis
of magnetized turbulence on the solar surface, Mgnetic
Reconnection 2010, (Nara, Japan, Dec. 6-9, 2010).
Katsukawa, Y., SOLAR-C WG: 2010, Chromospheric Diagnostics
in the Next Japanese Solar Mission SOLAR-C, 6th Solar
Polarization Workshop, (Maui, HI, USA, May 31-June 4, 2010).
Katsukawa, Y.: 2010, Prospects for High-Resolution Solar
Observations, 太陽フレア望遠鏡 20 周年記念研究会「太陽観測装置の新展開」, (Mitaka, Japan, Jul. 26-27, 2010).
Kawaguchi, N.: 2010, Raw Vlbi Data Buffer in use for efficientcorrelation processing by KJJVC, East Asia VLBI Workshop
2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Kawaguchi, N.: 2010, Ultra wideband VLBI technologies for
precise astrometry and geodesy, East Asia VLBI Workshop
2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Kawaguchi, N.: 2010, Technical Interests on the SKA, Japan SKA
Int. Workshop 2010, (Mitaka, Japan, Nov. 4-5, 2010).
Kawaguchi, N.: 2010, Report from Mizusawa VLBI Observatory,
8th EAMA (East Asian Meeting on Astronomy) Symp.,(Shanghai, China, Oct. 10-15, 2010).
Kawaguchi, N., Kono, Y., Oyama, T.: 2010, High Speed A/DConverter for Homodyne Detection of a Wideband Signal, AsiaPacific Radio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Kawamura, S., et al. including Agatsuma, K., Akutsu, T., Chen,
D., Ejiri, Y., Fujimoto, M., Fukushima, M., Hayama, K.,
Ishizaki, H., Izumi, K., Kotake, K., Nakamura, K., Nishida,E., Obuchi, Y., Ohishi, N., Okada, N., Suzuki, R., Takahashi,R., Torii, Y., Ueda, A., Yamazaki, T.: 2010, The JapaneseSpace Gravitational Wave Antenna DECIGO, 8th int. LISA
Symp., (Stanford, CA, USA, Jun. 28-Jul. 2, 2010).
Kawamura, S.: 2011, Design of LCGT, Workshop between
KGWG and LCGT, (Seoul, Korea, Jan. 22, 2011).
Kawata, D., et al.: 2010, Transient spiral arms and chemodynamics
of the Galactic disk, GCDS survey science, (Nice, France, Nov.
2-4, 2010).
Kida, S., Daishido, T., Tanaka, T., Aoki, T., Asuma, K., Niinuma, K.,
Akamatsu, H., Imai, A., Miyata, H.: 2010, Radio Variability of
Fermi Large Area Telescope Bright Source 0FGL J1847.8+3223,
Asia-Pacific Radio Science Conf., (Toyama, Japan, Sep. 22-26,
2010).
Kijima, M.: 2010, Application of geodetic-VLBI data to obtain
longterm light-curves, East Asia VLBI Workshop 2010,(Kagoshima, Japan, Apr. 22-24, 2010).
Kijima, M.: 2010, The application of the VLBI archive data to
drawing light curves for AGN sciences, Towards a root of AGN
jets: Recent progress, (Mitaka, Japan, Dec. 14-15, 2010).
Kikuchi, F., Hanada, H., Noda, H., Sasaki, S., Iwata, T.: 2010,

The study of lunar rotation by Japanese lunar landing missions,
European Geosciences Union General Assembly, (Vienna,
Austria, May 2-7, 2010).
Kikuchi, F., Matsumoto, K., Iwata, T., Hanada, H., Asari, K.,
Liu, Q., Goossens, S., Kono, Y., Takeuchi, H., Kawano, N.,
Sasaki, S.: 2010, Application of VLBI Technique for Lunar andPlanetary Mission, Asia-Pacific Radio Science Conf., (Toyama,
Japan, Sep. 22-26, 2010).
Kim, M. K.: 2010, Water masers associated with outflows inOrion-KL, East Asia VLBI Workshop 2010, (Kagoshima, Japan,
Apr. 22-24, 2010).
Kimura, K., Katase, T. Muraoka, K., Onishi, T., Ogawa, H., Nakajima,T., Kuno, N., Kawabe, R.: 2010, Optical Design of a New 4 MultiBeam 100-GHz Band Receiver for The NRO 45-m Radio Telescope,
The 11th Workshop on Submillimeter-Wave Receiver Technologies
in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Kino, M.: 2010, Hadronic emission from mini radio lobes, Towards
a root of AGN jets: Recent progress, (Mitaka, Japan, Dec.
14-15, 2010).
Kino, M.: 2010, AGN science with SKA, Japan SKA Int. Workshop
2010, (Mitaka, Japan, Nov. 4-5, 2010).
Kino, M., Asano, K.: 2010, Hadronic gamma-ray emission fromextragalactic mini radio lobes, Fermi meets Jansky-AGN at
Radio and Gamma-rays, (Bonn, Germany, Jun. 21-23, 2010).
Kobayashi, H.: 2010, Recent results of VERA, East Asia VLBI
Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Kobayashi, H.: 2010, Operation plan of EAVN, East Asia VLBI
Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Kobayashi, H.: 2011, Japanese VLBI Programs, the East Asia
VLBI Network and Space VLBI:VSOP-2, Future of the VLBA,(Charlottesville, USA, Jan. 27-28, 2011).
Kobayashi, H., Kim, B.-G., Shen, Z.-G.: 2010, EAST-ASIANVLBI NETWORK, Asia-Pacific Radio Science Conf., (Toyama,
Japan, Sep. 22-26, 2010).
Kobayashi, H., Miyazaki, A., Kawaguchi, N., Sawada-Satoh,S., East Asia VLBI consortium: 2010, Activities of East AsianVLBI network, 8th EAMA (East Asian Meeting on Astronomy)
Symp., (Shanghai, China, Oct. 10-15, 2010).
Kobayashi, K., Tsuneta, S., Trujillo Bueno, J., Cirtain, J. W.,
Bando, T., Kano, R., Hara, H., Fujimura, D., Ueda, K.,
Ishikawa, R., Watanabe, H., Ichimoto, K., Sakao, T., dePontieu, B., Carlsson, M., Casini, R.: 2010, The Chromospheric
Lyman Alpha SpectroPolarimeter (CLASP), AGU Fall Meeting,(San Francisco, CA, USA, Dec. 13-17, 2010).
Kobayashi, M. A. R.: 2010, A model prediction to the physicalquantities of high-z Lyman-alpha emitters, Evolution ofgalaxies, their central black holes and their large-scale
environment, (Potsdam, Germany, Sep. 20-24, 2010).
Kobayashi, Y., Yano, T., Gouda, N., Niwa, Y., Murooka, J., Yamada,Y., Sako, N., Nakasuka, S.: 2010, Nano-JASMINE: current status
and data output, SPIE Astronomical Instrumentation, (San
Diego, CA, USA, Jun. 27-Jul. 2, 2010).
Kobayashi, Y., Yano, T., Hatsutori, Y., Gouda, N., Murooka, J.,
Niwa, Y., Yamada, Y.: 2011, Nano-JASMINE: Simulation of
Data Outputs, ELSA conference 2010 GAIA: At the Frontiersof Astrometry, (Sèvres, France, Jun. 7-11, 2010).

II Publications, Presentations

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Kodama, T.: 2010, Panoramic Views of Cluster Evolution with
Subaru, CL J2010: from Massive Galaxy Formation to Dark
Energy, (Kashiwa, Japan, Jun. 28-Jul. 2, 2010).
Kodama, T.: 2010, Star Formation History and its Environmental
Dependence, FMOS science meeting, (Oxford, UK, Jul. 30,2010).
Kodama, T.: 2010, Panoramic Views of Galaxy Cluster Evolution,
Galaxy Formation Forum , (Seoul, Korea, Jun. 2, 2010).
Kokubo, E.: 2010, Planetesimal Dynamics and Accretion, An
Ishigaki Int. Conf. on Evolving Theory for Planet Formation,(Ishigaki, Japan, Jun. 20-26, 2010).
Komiya, Y., Suda, T., Fujimoto, M. Y.: 2011, IMF of Extremely
Metal-Poor Starsand Formation of the Milky Way, CPS 7th Int.
School of Planetary Sciences: Theory of Stellar Evolution and
Its Applications, (Kobe, Japan, Jan. 10-15, 2010).
Komugi, S.: 2010, The AKARI Far-Infrared Surveyor (FIS): AllSky Diffuse Map, Tracing the Ancestry of Galaxies on the Land of
our Ancestors, (Ouagadougou, Burkina Faso, Dec. 13-17, 2010).
Komugi, S.: 2010, Cold Dust and its Heating Sources in M33,
Tracing the Ancestry of Galaxies on the Land of our Ancestors,(Ouagadougou, Burkina Faso, Dec. 13-17, 2010).
Kotake, K.: 2010, Gravitational waves from successful vs. failed
supernova explosions, Korean Physical Society Meeting (special
session on compact objects), (Pyonchong, Korea, Oct. 20-22, 2010).
Kotake, K.: 2010, Multidimensional modeliing of core-collapse
supernovae, 35th Workshop on Gravitation and Numerical
Relativity, (Seoul, Korea, Oct. 22, 2010).
Kotake, K.: 2010, Topics in Failed Supernovae, Spanish relativity
meeting, (Granada, Spain, Sep. 6-10, 2010).
Kotake, K.: 2010, Gravitational waves from core-collapse
supernovae, Lecture at summer school on numerical relativity
and gravitation, (Pohang, Korea, Sep. 26-30, 2010).
Kouzuma, S., Nakagawa, A., Nakanishi, H., Kawaguchi, N.,
Ujihara, H., Ohta, I.: 2010, Experimental Text on a Tapered
Slot Antenna Used in an Ultra Wideband Receiver, Asia-PacificRadio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Koyama, S.: 2010, Discovery of Parsec Scale Structure in Kiloparsec Size Knot of 3C 380, Towards a root of AGN jets:
Recent progress, (Mitaka, Japan, Dec. 14-15, 2010).
Kroug, M., Kuroiwa, K., Fujii, Y., Miyachi, A., Gonzalez, A.,
Noguchi, T., Uzawa, Y., Makise, K., Wang, Z., Shan, W., Shi,
S.: 2010, SIS Mixers for the 790–950 GHz Band, The 11th
Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Kubo, M.: 2010, Diffusion and decay of sunspots, Hinode-IV:
unsolved problems and recent insights, (Mondello, Palermo,
Italy, Oct. 11-15, 2010).
Kubo, M., Low, B. C., Lites, B. W.: 2010, Unresolved Magnetic
Flux Removal Process in the Photosphere, 38th COSPAR
Scientific Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Kudoh, T., Basu, S.: 2010, Formation of collapsing cores inmagnetically subcritical clouds : three-dimensional simulations,
Magnetic Fields: Core Collapse to Young Stellar Objects,(London, ON, Canada, May 17-19, 2010).
Kudoh, T., Basu, S.: 2011, Formation of Collapsing Cores
in Subcritical Magnetic Clouds: Three-dimensional MHD

092

II Publications, Presentations

Simulations with Ambipolar Diffusion, Winter School andWorkshop on Star Formation, (Mitaka, Japan, Feb. 21-25, 2011).
Kuroda, D., et al. including Hanayama, H., Miyaji, T., Yanagisawa,
K.: 2010, Multi-band optical monitoring of GRB100925A/
MAXI J1659-152, The First Year of MAXI: Monitoring
Variable X-ray Sources, (Tokyo, Japan, Nov. 30-Dec. 2).
Kuroda, D., Yanagisawa, K., Yoshida, M., Shimizu, Y., Nagayama,S., Toda, H., Ohta, K., Yatsu, Y., Kawai, N.: 2011, The development of an automatic reduction system for Gamma-Ray
Burst afterglow, An int. conf. on remotely operated, automated,or robotic ground based telescopes, (Waikoloa, HI, USA, Feb.
28-Mar. 3, 2011).
Kuroiwa, K., Makise, K., Kojima, T., Fujii, Y., Kroug, M., Miyachi,
A., Uzawa, Y., Wang, Z., Ogawa, H.: 2010, Development ofSuperconducting NbTiN Waveguides for the Terahertz SIS
Mixers, Applied Superconductivity Conf., (Washington DC,
USA, Aug. 1-6, 2010).
Kuroiwa, K., Makise, K., Kojima, T., Fujii, Y., Kroug, M., Miyachi,
A., Uzawa, Y., Wang, Z., Ogawa, H.: 2010, Performance ofSuperconducting NbTiN Waveguide for Terahertz SIS Mixer, The
11th Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Kusakabe, M., Kajino, T., Yoshida, T., Mathews, G. J.: 2010,
SUSY-Catalyzed Big-Bang Nucleosynthesis as a Solution of
Lithium Problems, 24th Int. Nuclear Physics Conf., (Vancouver,
Canada, Jul. 7-9, 2010).
Kuzuhara, M.: 2011, The Widest-Separation Substellar Companion
Candidate to a Binary T Tauri Star, Star Formation AcrossSpace and Time Frontier Science with the LBT and Other Large
Telescopes, (Tucson, AZ, USA, Mar 31-Apr 2, 2011).
Lee, M. G., Lim, S., Park, H. S., Hwang, H. S., Hwang, N.: 2010,
Wandering Globular Clusters: the First Dwarf Galaxies in the
Universe?, A Universe of Dwarf Galaxies, (Lyon, France, Jun.
14-18, 2010).
Lim, S., Hwang, N., Lee, M. G.: 2010, Old Halo Star Clusters in
Nearby Starburst Galaxy M82, A Universe of Dwarf Galaxies,(Lyon, France, Jun. 14-18, 2010).
Ly, C., Malkan, M. A., Ross, N., Ota, K., Kashikawa, N., Iye, M.:
2011, The Stellar Population Completeness of Narrow-band
Emission-line Surveys, 217th AAS Meeting, (Seattle, WA,
USA, Jan. 9-13, 2011).
Machida, M. N.: 2010, Recent Developments in Simulations of
Low-mass Star Formation, IAU Symp. 270: Computational starformation, (Barcelona, Spain, May 31-Jun. 4, 2010).
Machida, M. N.: 2010, The Origin of the Circumstellar Disk andFormation of Gaseous Disk by Gravitational Instability, The 4th
East Asian Numerical Astrophysics Meeting, (Taipei, Taiwan,
Nov. 2-5, 2010).
Makino, J.: 2010, GRAPE and GRAPE-DR, MODEST-10, (Beijing,
China, Aug. 30-Sep. 3, 2010).
Makino, J.: 2010, GRAPE and GRAPE-DR, GPU Solutions toMultiscale Problems in Science and Engineering Workshop,(Harbin, China, Jul. 27-29, 2010).
Makino, J.: 2010, GRAPE-accelerators, IAU Symp. 270: Computational star formation, (Barcelona, Spain, May 31-Jun. 4, 2010).
Makise, K., Takeda, M., Terai, H., Uzawa, Y., Wang, Z.: 2010,

Characterization of NbTiN thin films deposited on various
substrates, Applied Superconductivity Conf., (Washington DC,
USA, Aug. 1-6, 2010).
Manabe, S.: 2010, Requirement on antenna positions accuracy forannual parallax determination with VERA and KVN, East Asia
VLBI Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Martinache, F.: 2010, Behind the coronagraphic mask, Lyot Conf.
2010, (Paris, France, Oct. 25-29, 2010).
Maruyama, T., Kajino, T., Yasutake, N., Cheoun, M. K., Ryu,
C. Y.: 2010, Asymmetric Neutrino Reaction from MagnetizedProto-Neutron Stars in Fully Relativisitc Framework Including
Hyperons, Int. Nuclear Physics Conf. (INPC10), (University of
British Columbia, USA, Jul. 4-9, 2010).
Maruyama, T., Kajino, T., Yasutake, N., Cheoun, M. K., Ryu,
C. Y.: 2010, Asymmetric Neutrino Reaction from MagnetizedProto-Neutron Stars in fully Relativisitc Framework including
Hyperons, The 11th Asia Pacific Physics Conf. (APPC11) ,(Shanghai, China, Nov. 16, 2010).
Maruyama, T., Kajino, T., Yasutake, N., Cheoun, M. K., Ryu,
C. Y.: 2010, Asymmetric Neutrino Reaction from MagnetizedProto-Neutron Stars in fully Relativisitc Framework including
Hyperons, 3rd Int. Conf. on Frontiers In Nuclear Structure,
Astrophysics and Reactions, (Rhodos, Greece, Aug. 23-27, 2010).
Maruyama, T., Kajino, T., Yasutake, N., Cheoun, M. K., Ryu, C. Y.:
2011, Asymmetric Neutrino Reaction in Magnetized Proto-NeutronStars in Fully Relativistic Approach, Workshop on Hadron
Nuclear Physics 2011, (Pohang, Korea, Feb. 21-24, 2011).
Masuda, S., Shimojo, M., Watanabe, K., Minoshima, T., Yaji, K.:
2010, Hard X-ray and microwave sources located around theapex of a solar flare loop, AGU Fall Meeting, (San Francisco,
CA, USA, Dec. 13-17, 2010).
Matsui, H., Saitoh, T. R., Makino, J., Wada, K., Tomisaka, K.,
Kokubo, E., Daisaka, H., Okamoto, T., Yoshida, N.: 2010,
Formation of Hypermassive Star Clusters and Mass Supply to
Galactic Center in Merging Galaxies, Central Massive Objects:
The Stellar Nuclei - Black Hole Connection, (Garching, Germany,
Jun. 22-25, 2010).
Matsumoto, K., Goossens, S., Kikuchi, F., Liu, Q., Ishihara, Y.,
Hanada, H.: 2010, An Improved Lunar Gravity Field Model
Using Same-Beam VLBI Data, 38th COSPAR Scientific
Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Matsumoto, K., Noda, H., Kikuchi, F., Kono, Y., Tsuruta, S.,
Hanada, H., Goossens, S., Ishihara, Y., Sasaki, S., Iwata, T.,
Araki, H., Katayama, M., Tazawa, S., Kunimori, H., Otsubo,T., Funazaki, K., Sato, A., Taniguchi, H., Yamazaki A.: 2011,
Selenodetic mission instruments proposed for SELENE-2:
VLBI and LLR, The 5th KAGUYA (SELENE) Science Working
Team Meeting, (Tokyo, Japan, Jan. 17-19, 2011).
Matsumoto, N.: 2010, Astrometric observations of 6.7GHz
methanol masers toward W3(OH) with JVN, East Asia VLBI
Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.:
2010, Development of Cryogenics Integrated Circuits forSuper-conducting Terahertz Camera, The 10th Taiwan-Japan
Microelectronics Int. Symp., (Hsinchu, Taiwan, Oct. 27-28, 2010).
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2010,

SISCAM 32-ch cryogenic readout module with GaAs-JFET
ASICs, SPIE Astronomical Instrumentation, (San Diego, CA,
USA, Jun. 27-Jul. 2, 2010).
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2010,
GaAs-JFET cryogenic readout module for superconducting
THz imaging arrays, Ninth International Workshop in Low
Temperature Electronics, (Guaruja, Brazil, Jun. 21-23, 2010).
Matsuo, H., Shi, S.-C., Yao, Q.-J., Luo, Y., Matsuo, T., Ohta, I. S.:
2010, A design study on terahertz interferometry in Antarctica,
SPIE Conf., Infrared, Millimeter Wave, and Terahertz
Technologies, (Beijing, China, Oct. 18-20, 2010).
Matsuo, H.: 2010, A Study on Antarctica Terahertz Interferometer,
The 11th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Matsuo, H.: 2010, Technical Challenges in Terahertz Astronomy,
4th Korean Workshop on Astronomical Instrumentations,(Daejeon, Korea, Sep. 8, 2010).
Matsuo, H.: 2010, Measurements of atmospheric transmission
using Fourier transform spectrometers in far-infrared andsubmillimeter waves, Comprehensive characterization ofastronomical sites, (Kislovodsk, Russia, Oct. 4-9, 2010).
Matsuo, H.: 2010, Far-infrared Interferometry for Atomic FineStructure Line Observations, Astronomy & Astrophysics in
Antarctica, (Xi'an, China, Aug. 18-21, 2010).
Matsuo, T., Kotani, T., Murakami, N., Tamura, M.: 2010, SecondEarth Imager for TMT (SEIT), TMT Science and Instrument
WS, (Victoria, Canada, Mar. 28-30).
Matsuo, T., Fukagawa, M., Kotani, T., Itoh, Y., Tamura, M.,
Nakagawa, T., Enya, K.: 2010, Direct Detection and Spectral
Characterization of Outer Planets with SPICA Coronagraph
Instrument, 38th COSPAR Scientific Assembly, (Bremen,
Germany, Jul. 18-25, 2010).
Matsuo, T., Tamura, M.: 2010, Second-Earth Imager for TMT(SEIT), SPIE Astronomical Instrumentation, (San Diego, CA,
USA, Jun. 27-Jul. 2, 2010).
Matsuo, T., Traub, W. A., Hattori, M. Tamura, M.: 2010, New
Concept for Direct Detection and Spectra of Exoplanets, SPIE
Astronomical Instrumentation, (San Diego, CA, USA, Jun.
27-Jul. 2, 2010).
Matsuo, T., Traub, W. A., Hattori, M. Tamura, M.: 2010, New
Concept for Direct Detection and Spectra of Exoplanets, Lyot
Conf. 2010, (Paris, France, Oct. 25-29, 2010).
Meyer, B. S.: 2010, Presolar Grains and Galactic Mergers,
Workshop on Nuclear Astrophysics at the University of Tokyo,(Tokyo, Japan, Jun. 15, 2010).
Meyer, B. S.: 2010, Nuclear Physics in Type Ia Supernovae
and FUN Calcium-Aluminum-rich Inclusions in Meteorites,
Workshop on Nuclear Astrophysics, (Tokyo, Japan, Jun. 26,
2010).
Meyer, B. S.: 2010, Presolar Grains and Galactic Mergers,
Workshop on Presolar Grains and Supernovae, (Sapporo, Japan,
Jul. 6, 2010).
Meyer, B. S.: 2010, Dense Type Ia Supernovae and Isotopic
Anomalies in FUN Inclusions and Hibonite Grains in
Meteorites, Workshop on Presolar Grains and Supernovae,(Sapporo, Japan, Jul. 6, 2011).

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Meyer, B. S.: 2010, Nuclear Dynamics of the r-Process of
Nucleosythesis: From the Ground Up, OMEG Institute,(Saitama, Japan, Jul. 15, 2010).
Meyer, B. S.: 2010, Nuclear Dynamics of the r-Process of
Nucleosynthesis and Production of the Third Abundance Peak ,Symp. on Nuclear Astrophysics, (Ibaraki, Japan, Jul. 20, 2010).
Minezaki, T., Sakata, Y., Yoshii, Y., Morokuma, T., Koshida, S.,
Sameshima, H., Aoki, T., Kobayashi, Y.: 2010, The spectral
variability of UV-optical continuum emission of Active Galactic
Nuclei, The First Year of MAXI: Monitoring Variable X-ray
Sources, (Tokyo, Japan, Nov. 30-Dec. 2).
Miura, R., Okumura, S. K., Tosaki, T., Tamura, Y., Kurono, Y.,
Kuno, N., Nakanishi, K., Sakamoto, S., Hasegawa, T., Kawabe,
R.: 2010, Sequential Star Formation in the Giant H II Region
NGC 604, Molecules in Galaxies, (Oxford, UK, Jul. 26-30,
2010).
Miyazaki, A.: 2010, Ammonia multi-transition survey in the
Galactic center region with the Nobeyama, Star formation under
extreme conditions: the Galactic center, (Besancon, France,
Dec. 6-9, 2010).
Miyazaki, A.: 2010, First phase of the East Asia VLBI Network,
East Asia VLBI Workshop 2010, (Kagoshima, Japan, Apr.
22-24, 2010).
Miyazaki, A., Sawada-Satoh, S., Kobayashi, H., Kawaguchi,N., Lee, S.-S., Sohn, B. W., KVN group, Shen, Z.-Q., Ling,
Q.-B., SHAO VLBI group: 2010, Present Status of First Phase
East Asia VLBI Network, 8th EAMA (East Asian Meeting on
Astronomy) Symp., (Shanghai, China, Oct. 10-15, 2010).
Miyazaki, S.: 2010, Subaru Wide Field Survey to Probe Dark
Matter Distribution and Nature of Dark Energy, COSMO/CosPA, (Tokyo, Japan, Sep. 27-Oct. 1, 2010).
Miyazaki, S.: 2010, Hyper Suprime-Cam, COSMOS Meeting,(Honolulu, HI, USA, Jun. 7-10, 2010).
Miyoshi, M., et al. including Furuya, R. S., Niinuma, K., Hagiwara,Y., Kawaguchi, N.: 2010, A First Black Hole Imager at Andes,
Asia-Pacific Radio Science Conf., (Toyama, Japan, Sep. 22-26,
2010).
Miyoshi, M., et al. including Furuya, R. S., Kawaguchi, N.,
Niinuma, K.: 2010, A first black hole imager at Andes, East Asia
VLBI Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Mizuno, N.: 2010, New Views of the Molecular Clouds and Star
Formation in the Magellanic System, "Magellanic Clouds"
splinter meeting of the Annual Meeting of Astronomische
Gesellschaft, (Bonn, Germany, Sep. 14-15, 2010).
Moritani, Y., Nogami, D., Okazaki, A. T., Imada, A., Kambe,
E., Honda, S., Hashimoto, O., Ichikawa, K.: 2010, Optical
Spectroscopic observations of the Be/X-Ray binary A0535+262/
V725 Tau during the giant outburst in 2009, The First Year of
MAXI: Monitoring Variable X-ray Sources, (Tokyo, Japan,
Nov. 30-Dec. 2).
Murakami, N., Guyon, O., Martinache, F., Matsuo, T., Yokochi,
K., Nishikawa, J., Tamura, M., Kurokawa, T., Baba, N., Vogt,
F., Garrel, V., Yoshikawa, T.: 2010, An eight-octant phasemask coronagraph for the Subaru coronagraphic extreme AO(SCExAO) system: system design and expected performance,
SPIE Astronomical Instrumentation, (San Diego, CA, USA,094

II Publications, Presentations

Jun. 27-Jul. 2, 2010).
Murakami, N., Inabe, T., Komatsu, T., Nishikawa, J., Hashimoto,N., Kurihara, M., Baba, N., Tamura, M.: 2010, Polarizationinterferometric eight-octant phase-mask coronagraph using
ferroelectric liquid crystal for exoplanet detection, SPIE
Astronomical Instrumentation, (San Diego, CA, USA, Jun.
27-Jul. 2, 2010).
Nagai, H., Suzuki, K., Asada, K., Kino, M., Kameno, S., Doi,
A., Inoue, M., Bach, U.: 2010, VLBI Monitoring of 3C 84 in
Gamma-ray Active Phase, Fermi meets Jansky-AGN at Radioand Gamma-rays, (Bonn, Germany, Jun. 21-23, 2010).
Nagashima, K., Zhao, J., Kosovichev, A. G., Sekii, T.: 2010,
Helioseismology Study of Subsurface Dynamics in the Polar
Regions of the Sun, AGU Fall Meeting, (San Francisco, CA,
USA, Dec. 13-17, 2010).
Naito, S.: 2011, Tokyo International Science Festival, The Int. Public
Science Events Conf., (Washington DC, USA, Feb. 16-17, 2011).
Nakajima, T., Iwashita, H., Miyazawa, C., Kuno, N., Kawabe,R., Katase, T., Nishimura, A., Kimura, K., Ogawa, H., Sakai,T., Asayama. S., Noguchi, T., 45-m members: 2010, The
New Observation System for the NRO 45-m Millimeter
Wave Telescope, The 11th Workshop on Submillimeter-Wave
Receiver Technologies in Eastern Asia, (Nagoya, Japan, Nov.
14-16, 2010).
Nakajima, T., Iwashita, H., Miyazawa, C., Kuno, N., Kawabe,R., Sakai, T., Kohno, K., Katase, T., Nishimura, A., Kimura,K., Ogawa, H., Asayma, S., Tamura, T., Noguchi, T.: 2010,
100-GHz Band Sideband-Separating Receivers for NRO 45-m
Telescope, Asia-Pacific Radio Science Conf., (Toyama, Japan,
Sep. 22-26, 2010).
Nakajima, T., Takano, S., Kohno, K., Inoue, H., the line survey
team: 2010, Line Survey Project of External Galaxies with
NRO 45-m Telescope, Workshop on Interstellar Matter 2010,(Sapporo, Japan, Sept. 13-15, 2010).
Nakamura, F.: 2010, Theory of Cluster Formation: Effectsof Magnetic Fields, IAU Symp. 270: Computational starformation, (Barcelona, Spain, May 31-Jun. 4, 2010).
Nakamura, F.: 2010, A Significant Role of Magnetic Field andProtostellar Turbulence on the Formation and Evolution ofDense Cores in Clustered vs. Distributed Star Formation,
MPIA Conference Series at Ringberg, The Early Phase of Star
Formation III, (Tegernge, Germany, Jun. 14-18, 2010).
Nakamura, F.: 2010, Effects of Magnetic Fields and Protostellar
Outflow Feedback on the Characteristic Mass of the IMF, The
Origin of Stellar Masses, (Tenerife, Spain, Oct. 18-22, 2010).
Nakamura, F.: 2010, Outflow Feedback Regulated Massive Star
Formation in Parsec-Scale Cluster Forming Clumps, The 4th
East Asian Numerical Astrophysics Meeting, (Taipei, Taiwan,
Nov. 2-5, 2010).
Nakamura, F., Li, Z.-Y.: 2011, Clustered Star Formation in
Magnetic Clouds, Winter School and Workshop on Star
Formation, (Mitaka, Japan, Feb. 21-25, 2011).
Nakamura, F., Li, Z.-Y., Wang, P., Abel, T.: 2010, Outflowregulated Massive Star Formation in PC-Scale Cluster
Forming Clumps, Great Barriers in High Mass Star Formation,(Townsville, Australia, Sep. 13-17, 2010).

Nakamura, K., Hayakawa, T., Cheoun, M. K., Kajino, T.,
Mathews, G. J.: 2011, The neutrino process in core-collapse
supernovae, From quarks to supernovae, (Izuatagawa, Japan,
Nov. 28-30, 2010).
Nakamura, K., Hayakawa, T., Cheoun, M. K., Kajino, T., Mathews,
G. J.: 2011, Radioactive Nuclei in Core-collapse Supernovae,
Astronomy with Radioactivities, (Victoria, Australia, Mar. 1-3,
2011).
Nakamura, K., Yoshida, T., Shigeyama, T., Kajino, T.: 2010, The
neutrino-process and light element production, Nuclei in the
Csomos -11, (Heidelberg, Germany, Jul. 19-23, 2010).
Nakanishi, H., Hagiwara, Y., Takahashi, K.: 2010, Summary of
Discussion, Japan SKA Int. Workshop 2010, (Mitaka, Japan,
Nov. 4-5, 2010).
Nakanishi, H., Takahashi, K., Yamamoto, S., Kawakatsu, N.,
Kameya, O., Hirashita, H., Imai, H.: 2010, Observation of the
Universe with Ultra Wideband Receiver and SKA, Asia-PacificRadio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Namekata, D., Habe. A.: 2010, Evolution of a Circumnuclear Diskand Gas Supply to the Galactic Center, The Fourth East Asia
Numerical Astrophysical Meeting, (Taipei, Taiwan, Nov. 2-5, 2010).
Narita, N.: 2010, SPICA for Transiting Exoplanets: Which SPICA
instruments are useful?, SPICA Science Workshop, (Mitaka,
Tokyo, Dec. 16-17, 2010).
Narita, N.: 2010, Good Combination of Rossiter-McLaughlin
Measurements and Direct Imaging Observations, Detection
and dynamics of transiting exoplanets, (Observatoire de HauteProvence, France, Aug. 23-27, 2010).
Narita, N.: 2010, Subaru Measurements of Spin-Orbit Alignment
Angles of Transiting Exoplanets, End-of-Term Hawaii Open
Meeting on Exoplanets, (Honolulu, HI, USA, May 27-28, 2010).
Narita, N.: 2010, Subaru Measurements of the Rossiter-McLaughlin
Effect and Direct Imaging Observations for Transiting Planetary
Systems, IAU Symp. 276: The Astrophysics of Planetary
Systems: Formation, Structure, and Dynamical Evolution,(Torino, Italy, Oct. 11-15, 2010).
Narita, N.: 2011, Japanese Research Plan for Exploring New
Worlds with TMT, TMT Science and Instrument WS, (Victoria,
Canada, Mar. 28-30).
Narita, N., et al. including Yamashita, T., Tamura, M., Nishikawa,J., Hayano, Y., Oya, S., Kokubo, E., Guyon, O.: 2010, SPICA
coronagraph for the detection and characterization of exoplanets, 38th COSPAR Scientific Assembly, (Bremen, Germany,
Jul. 18-25, 2010).
Narukage, N., Kano, R., Sakao, T.: 2010, Temperature andEmission Measure Properties of Coronal Structures across theWhole Sun Observed with Hinode/X-Ray Telescope, HinodeIV: unsolved problems and recent insights, (Mondello, Palermo,
Italy, Oct. 11-15, 2010).
Narukage, N.: 2010, Property of solar coronal structures based on
temperature and emission measure derived with Hinode/X-Ray
Telescope, 2010 XRT Team Meeting, (Bozeman, MT, USA,
Jun. 16-18, 2010).
Naruse, M., Sekimoto, Y., Noguchi, T., Uzawa, Y., Nitta, T.: 2010,
Development of a sub-millimeter camera with superconducting
resonators, The 11th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Niinuma, K.: 2010, The Quick Follow-up Observation of theLargest X-ray Flare from the TeV blazar Mrk 421, Towards a rootof AGN jets: Recent progress, (Mitaka, Japan, Dec. 14-15, 2010).
Niinuma, K., Kino, M., Hada, K., Asada, K., Koyama, S., Oyama,T., Kawaguchi, N., Nagai, H., Isobe, N., Hara, T.: 2010, Quick
Follow-up Observation of the Largest X-ray Flare from the TeV
blazar Mrk 421, The First Year of MAXI: Monitoring Variable
X-ray Sources, (Tokyo, Japan, Nov. 30-Dec. 2).
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani,T., Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.,
Murakami, H.: 2010, A coronagraph system with unbalanced
nulling interferometer: progress of wavefront correction, SPIE
Astronomical Instrumentation, (San Diego, CA, USA, Jun.
27-Jul. 2, 2010).
Nishimura, A., Sakaguchi, T., Tsuji, H., Kunizane, M., Minowa,
M., Katase, T., Kizawa, J., Matsumoto, K., Abe, Y., Kimura,K., Muraoka, K., Onishi, T., Ogawa, H., Dobashi, K., Handa,
T., Nakajima, T., Kuno, N.: 2010, The 1.85 m Mm-Submm
Telescope for Large Scale Molecular Cloud Survey, The 11th
Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Nishimura, A., Tsuji, H., Sakaguchi, T., Yashima, S., Kunizane,M., Minowa, M., Kimura, K., Abe, Y., Muraoka, K., Onishi,T., Ogawa, H., Dobashi, K., Handa, T., Nakajima, T.: 2010,
The 1.85 m mm-submm Telescope for Large Molecular Cloud
Survey, Asia-Pacific Radio Science Conf., (Toyama, Japan, Sep.
22-26, 2010).
Nishimura, N.: 2010, R-process Nucleosynthesis in the LongTerm Simulation of Magnetically Dominated Core-Collapse
Supernovae, EMMI workshop: Neutron Matter in Astrophysics:
From Neutron Stars to the r-Process, (Darmstadt, Germany, Jul.
15-18, 2010).
Nishimura, N., Sekiguchi, Y.: 2010, NSE Weak Interaction Rates
for Core-Collapse Simulations, From Quarks to Supernovae,(Shizuoka, Japan, Nov. 28-30, 2010).
Nishimura, N., Takiwaki, T., Hashimoto, M., Sato, K.: 2010,
R-process Nucleosynthesis in Magnetically Dominated CoreCollapse Supernovae, Nuclei in the Csomos -11, (Heidelberg,
Germany, Jul. 19-23, 2010).
Niwa, Y., Yano, T., Araki, H., Gouda, N., Kobayashi, Y., Tazawa,
S., Hanada H., Yamada, Y.: 2010, CCD centroiding analysis
for Nano-JASMINE observation data, SPIE Astronomical
Instrumentation, (San Diego, CA, USA, Jun. 27-Jul. 2, 2010).
Noguchi, T., Suzuki, T., Tamura, T.: 2010, Subgap tunnelingcurrent at low temperature in Nb/Al-AlN/Nb SIS junctions,Applied Superconductivity Conf., (Washington DC, USA, Aug.
1-6, 2010).
Noguchi, T.: 2010, Imaginary Part of the Superconducting Gap
Energy and Its Influence on Low-Temperature Devices, The
11th Workshop on Submillimeter-Wave Receiver Technologies
in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Oe, M.: 2010, RXFR: enhancement architecture for astronomical
observation systems, 2010 Northeastern Asian Symp. on ICT,
(Xian, China, Sep. 15-17, 2010).
Oe, M.: 2010, IOT activities in Japan, ETSI INT10, (Sophia

II Publications, Presentations

095

Antipolis, France, Sep. 7-9, 2010).
Oguri, M.: 2010, The shape of massive dark matter halos fromgravitational lensing, CL J2010+0628: from Massive Galaxy
Formation to Dark Energy, (Chiba, Japan, Jun. 28-Jul. 2, 2010).
Oguri, M.: 2010, Quasar lensing as a cosmological probe, String
Theory and Cosmology, (Daejeon, Korea, Sep. 30-Oct. 2, 2010).
Oguri, M.: 2010, Stacked weak lensing as a dark energy probe,
The observational pursuit of dark energy after Astro2010,(Pasadena, CA, USA, Oct. 7-8, 2010).
Oguri, M.: 2011, Weak lensing cosmology, DENET 2011 Subaru
HSC workshop, (Taipei, Taiwan, Mar. 7-8, 2011).
Oh, S.-J., Roh, D.-G., Yeom, J.-H., Chung, H.-S., Park, S.-Y.,
Kobayashi, H., Kawaguchi, N., Oyama, T., Kawakami, K.:
2010, FX-Based VLBI Correlator Development by KOREAJAPAN Joint Collaboration for East-Asian VLBI Network, AsiaPacific Radio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Ohishi, M.: 2010, Impact to the Radio Astronomy by theInterference Caused by the Solar Power Satellite Systems, AsiaPacific Radio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Ohishi, M.: 2010, Data Intensive Astronomy by means of Virtual
Observatories, 8th EAMA (East Asian Meeting on Astronomy)
Symp., (Shanghai, China, Oct. 10-15, 2010).
Ohishi, M.: 2010, Evolution of Life-Related Matter in the
Universe, Japan Geoscience Union 2010, (Chiba, Japan, May
23-28, 2010).
Ohishi, M., Kitagawa M., Misawa H., Tsuchiya F.: 2010, Impact of the
PLT Disturbance against Radio Astronomy in the HF Band, AsiaPacific Radio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Ohsuga, K.: 2010, Radiation-magnetohydrodynamic simulationsof black hole accretion flow and outflow, Accretion and Outflow
in Black Hole Systems, (Kathmandu, Nepal, Oct. 11-15, 2010).
Ohsuga, K.: 2010, Radiation MHD Simulations of Black Hole
Accretion Flow and Outflow, Relativistic Whirlwind, (Trieste,
Italy, May 31-Jun. 4, 2010).
Ohsuga, K.: 2010, Two-dimensional Global RadiationMagnetohydrodynamic Simulations of Black Hole Accretion
Flow and Outflow, The 4th East Asian Numerical Astrophysics
Meeting, (Taipei, Taiwan, Nov. 2-5, 2010).
Okamoto, T. J.: 2010, Emergence of twisted flux in prominence
observations, Hinode-IV: unsolved problems and recent
insights, (Mondello, Palermo, Italy, Oct. 11 - 15, 2010).
Okamoto, T. J., Tsuneta, S., Berger, T. E.: 2010, A rising coolcolumn associated with formation of prominence and coronalcavity, AGU Fall Meeting, (San Francisco, CA, USA, Dec.
13-17, 2010).
Okumura, S. K.: 2010, Radio Science & Technology— II,
Backends, 3rd Summer School in Spectrum Management forRadio Astronomy, (Mitaka, Japan, May 31-Jun. 4, 2010).
Okumura, S. K.: 2011, Correlator, backend, digital process, EastAsia Interefometry Winter School 2011, (Mitaka, Japan, Feb.
7-11, 2011).
Okumura, S. K., Chikada, Y., Kamazaki, K., Okuda, T., Kurono,Y., Iguchi, S.: 2010, Atacama Compact Array Correlator for
Atacama Large Millimeter/submillimeter Array, Asia-PacificRadio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Oshima, A., GRAPES-3 collaboration: 2010, Angular resolution

096

II Publications, Presentationsof GRAPES-3 experiment, Workshop on cosmic ray physics
2010, (Tamil Nadu, India, Dec. 14-16, 2010).
Oshima, A.: 2010, Visualization of CORSIKA EAS (Development
of EAS in the atmosphere), CORSIKA school 2010, (Tamil
Nadu, India, Dec. 17-20, 2010).
Oshino, S., Makino, J.: 2010, The effect of initial mass ofplanetesimals to the planet formation process, 2010 Western
Pacific Geophysics Meeting, (Taipei, Taiwan, Jun. 22-25, 2010).
Oshino, S., Makino, J.: 2010, The effect of initial mass ofplanetesimals to the planet formation process, AOGS 2010,(Hyderabad, India, Jul. 5-9, 2010).
Oyama, T.: 2010, Development of software correlator, East Asia
VLBI Workshop 2010, (Kagoshima, Japan, Apr. 22-24, 2010).
Petrova, N., Hanada, H., Abdulmyanov, T., Petrova, A.:
2010, Determination of Lunar physical libration from polar
observations in the project ILOM (Japan), EPSC (European
Planetary Sciences Conf.), (Roma, Italy, Sep. 20-24, 2010).
Reznikova, V. E.: 2010, Observation of the slow magnetoacoustic
mode in the flaring loop, CESRA2010, (La Roche en Ardenne,
Belgium, Jun. 15-19, 2010).
Reznikova, V. E.: 2010, Observation and interpretation of QPP
with a drift of period, All-Russian Conf. "Solar and SolarTerrestrial Physics – 2010", (Saint-Petersburg, GAO RAS,
Russia, Oct. 3-9, 2010).
Reznikova, V. E., Melnikov, V. F.: 2010, Dynamics of the systemof microwave flaring loops in the two-ribbon flare, All-RussianConf. "Solar and Solar-Terrestrial Physics – 2010", (SaintPetersburg, GAO RAS, Russia, Oct. 3-9, 2010).
Reznikova, V. E., Melnikov, V. F., Pyatakov, N. P., Shibasaki, K.:
2010, Diagnostics of an acceleration site location and pitchangle anisotropy of energetic electrons in the flare observed in
microwaves, CESRA2010, (La Roche en Ardenne, Belgium,Jun. 15-19, 2010).
Reznikova, V. E., Melnikov, V. F., Shibasaki, K., Ji, H.: 2010,
Topology dynamics of the flaring loop system on 2005 August
22 observed in microwaves and hard X-rays, 38th COSPAR
Scientific Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Reznikova, V. E., Melnikov, V. F., Shibasaki, K., Ji, H.: 2010,
Dynamics of the flaring loop system, CESRA2010, (La Rocheen Ardenne, Belgium, Jun. 15-19, 2010).
Saito, M., Inatani, J., Nakanishi, K., Naoi, T., Yamada, M.,
Saito, H., Ikenoue, B., Kato, Y., Morita, K.-I., Mizuno, N.,
Iguchi, S.: 2010, Atacama Compact Array Antenna, Asia-PacificRadio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Saito, M.: 2010, ALMA for Interstellar Matter, Workshop on
Interstellar Matter 2010, (Sapporo, Japan, Sept. 13-15, 2010).
Saitoh, T. R., Daisaka, H., Kokubo, E., Makino, J., Okamoto, T.,
Tomisaka, K., Wada, K., Yoshida, N.: 2010, Shock-induced
star cluster formation in colliding galaxies, IAU Symp. 270:
Computational star formation, (Barcelona, Spain, May 31-Jun. 4,2010).
Sakaguchi, T., Nishimura, A., Katase, T., Tsuji, H., Kunizane, K.,
Minowa, M., Kizawa, J., Matsumoto, K., Abe, Y., Kimura, K.,
Muraoka, K., Onishi, T., Ogawa, H., Dobashi, K., Handa, T.,
Nakajima, T., Kuno, N.: 2010, Performance of 1.85m Radio
Telescope, The 11th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Sakao, T., Kano, R., Narukage, N., Shimojo, M., Sako, N.:2010, Eruptive events observed with Hinode XRT, Hinode-IV:
unsolved problems and recent insights, (Mondello, Palermo,
Italy, Oct. 11-15, 2010).
Sako, N., Shimojo, M., Kitabayashi, T.: 2010, Statistical studyof the polar X-ray jets, 38th COSPAR Scientific Assembly,(Bremen, Germany, Jul. 18-25, 2010).
Sakurai, T., Hanaoka, Y., Shinoda, K., Noguchi, M., Miyashita,M., Fukuda, T., Suzuki, I., Hagino, M., Arai, T., Yamasaki,T., Takeyama, N.: 2010, Infrared Stokes Spectro-Polarimeterat the National Astronomical Observatory of Japan, 6th Solar
Polarization Workshop, (Maui, HI, USA, May 31-June 4, 2010).
Sakurai, T.: 2010, Studies of the Solar Corona by Relocating
the Coronagraph of Norkura Observatory to a High Mountain
Site in East Asia, The 4th EACOA Meeting, (Jeju, Korea, May
10-12, 2010).
Sakurai, T.: 2010, Twenty Years of Solar Flare Telescope, 太 陽
フレア望遠鏡 20 周年記念研究会「太陽観測装置の新展開」,(Mitaka, Japan, Jul. 26-27, 2010).
Sakurai, T.: 2011, Helioseismology, Solar Dynamo, and Magnetic
Helicity, Progress in Solar/Stellar Physics with Helio- andAstero-Seismology, (Hakone, Japan, Mar. 14-17, 2011).
Sakurai, T.: 2011, The First Four Years of Hinode, The First AsiaPacific Solar Physics Meeting, (Bangalore, India, Mar. 21-24,
2011).
Sasada, M., et al., including Kuroda, D., Yanagisawa, K., Imada, A.:
2010, Multi-wavelength photometric and polarimetric observationsof the outburst of 3C 454.3 in Dec. 2009, 38th COSPAR
Scientific Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Sasaki, S., KAGUYA Gravity/Topography Team.: 2010, The
first precise global gravity and topography of the Moon by
KAGUYA (SELENE) mission, 38th COSPAR Scientific
Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Sasaki, S., et al.: 2010, Topography and Crustal Thickness of
the Moon by KAGUYA (SELENE) Selenodesy Observation,
European Geosciences Union General Assembly, (Vienna,
Austria, May. 2-7, 2010).
Sasaki, S., et al.: 2010, Jupiter Magnetospheric Orbiter and Trojan
Asteroid Explorer in EJSM (Europa Jupiter System Mission),
European Geosciences Union General Assembly, (Vienna,
Austria, May. 2-7, 2010).
Sasaki, S., et al.: 2010, Summary of KAGUYA laser altimeter
LALT, BepiColombo Geodesy/Geophysics WG Workshop,(DLR Berlin, Germany, Jul. 1-2, 2010).
Sasaki, S., et al.: 2010, The First Accurate Global Gravity
and Topography of the MOON by KAGUYA (SELENE)
and Implication for Lunar Basin Evolution, AOGS 2010,(Hyderabad, India, Jul. 5-9, 2010）.
Sasaki, S., et al.: 2010, In situ measurements of lunar rotation andgravity for the study of the interior of the Moon, 38th COSPAR
Scientific Assembly, (Bremen, Germany, Jul. 18-25, 2010).
Sasaki, S., et al.: 2010, Jupiter Magnetospheric Orbiter and Trojan
Asteroid Explorer in EJSM, 38th COSPAR Scientific Assembly,(Bremen, Germany, Jul. 18-25, 2010).
Sasaki, S., et al.: 2010, Space weathering on Mercury: Simulationof plagioclase weathering, 38th COSPAR Scientific Assembly,(Bremen, Germany, Jul. 18-25, 2010).
Sasaki, S., et al.: 2010, The First Precise Global Gravity, Topography
and Crustal Thickness of the Moon by Kaguya (SELENE),
Int. Symp. of the Science and Utilization of the Moon, (Tokyo,
Japan, Sep. 7-9, 2010).
Sasaki, S., et al.: 2011, Structure of South-Pole Aitken Basin of theMoon from KAGUYA (SELENE) Gravity/Topography, The 5th
KAGUYA (SELENE) Science Working Team Meeting, (Tokyo,
Japan, Jan. 17-19, 2011).
Sasaki, S., Hiroi, T., Helbert, J.: 2010, Space Weathering on
Mercury: Laboratory Simulation of Plagioclase Weathering,
AOGS 2010, (Hyderabad, India, Jul. 5-9, 2010).
Sasaki, S., Ishihara, Y., Goossens, S., Matsumoto, K., Araki,
H., Hanada, H., Kikuchi, F., Noda, H., Iwata, T., Ohtake, M.:
2011, Lunar South Pole-Aitken Basin from Kaguya (SELENE)
Gravity/Topography, 42nd Lunar and Planetary Science Conf.,(Woodsland, TX, USA, Mar. 7-11, 2011).
Sasaki, S., MDM Team.: 2010, Measurement of Dust Environment
around Mercury by MDM (Mercury Dust Monitor) on Board
MMO Bepi Colombo Exploring Magnetosphere-Exospshere
Coupling at Mercury, A Joint MESSENGER-BepiColombo
Workshop, (Boulder, USA, Nov. 3, 2010).
Sasaki, S., Namiki, N., Hanada, H., Araki, H., Imamura, T., Iwata,T., RSAT/VRAD/RS Group.: 2010, Multi-satellite mission
KAGUYA (SELENE), EPSC (European Planetary Sciences
Conf.), (Roma, Italy, Sep. 20-24, 2010).
Sato, M.: 2010, Distance and location of the Sagittarius arm traced
by trigonometric parallaxes of massive star-forming regions,
Spiral Structure in the Milky Way: Confronting Observations
and Theory, (Bahia Inglesa, Chile, Nov. 7-10, 2010).
Sato, M., Watanabe, J.: 2010, Orionids in recent years:Simulations
and observed activities, Meteoroids 2010, An Int. Conf. on
Minor Bodies in the Solar System, (Breckenridge, CO, USA,May 24-28, 2010).
Sato, M., Watanabe, J., NAOJ Campagin Team: 2010, Meteor
shower activity derived from "Meteor Watching PublicCampagin" in Japan, Meteoroids 2010, An Int. Conf. on Minor
Bodies in the Solar System, (Breckenridge, CO, USA, May
24-28, 2010).
Sawada-Satoh, S.: 2010, JVN Analysis and Display for Effects ofSource Structure (JADESS), East Asia VLBI Workshop 2010,(Kagoshima, Japan, Apr. 22-24, 2010).
Sawada-Satoh, S.: 2010, Progress Reports of KVN+VERA Test
Observations, 2010 KVN and TRAO Radio Workshop, (Seoul,
Korea, Aug. 16-18, 2010).
Sawada-Satoh, S.: 2010, Preliminary Imaging of KVN+VERA test
observations, 8th EAMA (East Asian Meeting on Astronomy)
Symp., (Shanghai, China, Oct. 10-15, 2010).
Sawada-Satoh, S.: 2010, Methanol Maser Outflows of UCHII
Region S269, Great Barriers in High Mass Star Formation,(Townsville, Australia, Sep. 13-17, 2010).
Sekiguchi, K., Kaifu, N.: 2010, Strategy of Future Regional
Cooperation in Astronomy, 8th EAMA (East Asian Meeting on
Astronomy) Symp., (Shanghai, China, Oct. 10-15, 2010).
Sekiguchi, K.: 2010, Report from EACOA, 8th EAMA (East Asian

II Publications, Presentations097

Meeting on Astronomy) Symp., (Shanghai, China, Oct. 10-15,
2010).
Sekiguchi, Y.: 2010, Formation of Black hole-Disk System via
PopIII stellar core collapse in full general relativity, Deciphering
the Ancient Universe with Gamma-Ray Bursts, (Kyoto, Japan,
Apr. 19-23, 2010).
Sekiguchi, Y.: 2010, Collapse of rotating very massive stellar core
to a black hole and a disk, Spanish relativity meeting, (Granada,
Spain, Sep. 6-10, 2010).
Sekiguchi, Y.: 2010, Black hole and accretion disk formation in thecollapsar model, The 20th workshop on General relativity andGravitation, (Kyoto, Japan, Sep. 21-25, 2010).
Sekiguchi, Y.: 2010, Formation and evolution of black hole andaccretion disk in collapsar, Accretion and Outflow in Black
Hole Systems, (Kathmandu, Nepal, Oct. 11-15, 2010).
Sekiguchi, Y.: 2010, Formation and evolution of black hole anddisk in collapsar, The Fourth East Asia Numerical Astrophysical
Meeting, (Taipei, Taiwan, Nov. 2-5, 2010).
Sekiguchi, Y.: 2010, Formation and evolution of black holeand accretion disk in collapsar, From Quarks to Supernovae,(Shizuoka, Japan, Nov. 28-30, 2010).
Sekiguchi, Y.: 2011, Formation and evolution of a black hole andan accretion disk in Type III collapsars, The Prompt Activity ofGamma-Ray Bursts: their Progenitors, Engines, and Radiation
Mechanisms, (Nothr Carolina, USA, Mar. 5-7, 2011).
Sekii, T.: 2010, High-latitude solar dynamics/Helioseismology inhigh latitude regions, Hinode-IV: unsolved problems and recent
insights, (Mondello, Palermo, Italy, Oct. 11-15, 2010).
Sekii, T., Hartlep, T., Zhao, J., Nagashima, K., Kosovichev, A.
G.: 2010, Initial study of stereo-helioseismology, AGU Fall
Meeting, (San Francisco, CA, USA, Dec. 13-17, 2010).
Shibasaki, K.: 2010, The quiet sun at radio wavelengths,
CESRA2010, (La Roche en Ardenne, Belgium, Jun. 15-19, 2010).
Shibasaki, K., Narukage, N., Yoshimura, K.: 2010, Imaging
observations of coronal magnetic field by the Nobeyama
Radioheliograph, 6th Solar Polarization Workshop, (Maui, HI,
USA, May 31-June 4, 2010).
Shibasaki, K.: 2010, Imaging observations of coronal magnetic
field by Nobeyama Radioheliograph, 6th Solar Polarization
Workshop, (Maui, HI, USA, May 31-June 4, 2010).
Shibasaki, K.: 2010, Long-Term Radio Imaging Observations of
the Sun by Nobeyama Radioheliograph, 太陽フレア望遠鏡 20 周年記念研究会「太陽観測装置の新展開」, (Mitaka, Japan, Jul.
26-27, 2010).
Shimobaba, T., Nakayama, H., Masuda, N., Takada, N., Ito, T.: 2010,
24 mega pixels phase electroholography, IDW'10, (Fukuoka,
Japan, Dec. 1-3, 2010).
Shimojo, M.: 2010, The variations of prominence activities duringsolar cycle, 38th COSPAR Scientific Assembly, (Bremen,
Germany, Jul. 18-25, 2010).
Shimojo, M.: 2010, The Evolution of the Magnetic Field
Distribution Investigated Based on the Prominence Activities,XRT Team Meeting, (Montana, USA, Jun. 17-18, 2010).
Shimojo, M.: 2010, Prospects for Solar Data Analysis -The Sun
Seen by Computer Vision-, 太陽フレア望遠鏡20周年記念研究会「太陽観測装置の新展開」, (Mitaka, Japan, Jul. 26-27, 2010).

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Shirasaki, Y.: 2010, Study of QSO environment using the Japanese
Virtual Observatory of Japan (JVO), 8th EAMA (East Asian
Meeting on Astronomy) Symp., (Shanghai, China, Oct. 10-15, 2010).
Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto, Y., Ishihara, Y.,
Yanaka, Y., Tsutsumi, J., Hiyama, T., Nakamoto, H., Sakamoto,M.: 2010, Current Status of the Japanese Virtual Observatory
Portal, Astronomical Data Analysis Software and Systems XX,(Boston, MA, USA, Nov. 7-11, 2010).
Sofue, Y., Machida, M., Kudoh, T.: 2010, Primordial Origin ofComposite Magnetic Configurations in Spiral Galaxies, JapanSKA Int. Workshop 2010, (Mitaka, Japan, Nov. 4-5, 2010).
Sôma, M., Tanikawa, K.: 2010, Investigation of the Earth's Rotation
using Ancient Chinese Occultation Records, 7th Int. Conf. on
Oriental Astronomy (ICOA-7), (Tokyo, Japan, Sep. 6-10, 2010).
Sotani, H.: 2010, Slowly Rotating Relativistic Stars in TeVeS,
Spanish relativity meeting, (Granada, Spain, Sep. 6-10, 2010).
Sotani, H., Kokkotas, K. D.: 2010, Non-axisymmetric Torsional
Oscillations of Relativistic Stars, Spanish relativity meeting,(Granada, Spain, Sep. 6-10, 2010).
Suematsu, Y.: 2010, On the Relation of Bright Point Appearancewith Small-Scale Jets Formation in the Chromosphere, HinodeIV: unsolved problems and recent insights, (Mondello, Palermo,
Italy, Oct. 11-15, 2010).
Suematsu, Y.: 2010, Data Analysis of H-alpha Full Disk and
Hinode Observations, 1st Latin American FMT Workshop, (Ica,
Peru, Nov. 22-26, 2010).
Suematsu, Y.: 2010, Recent Progresses in Two-Dimensional
Spectroscopy, 太陽フレア望遠鏡 20 周年記念研究会「太陽観測装置の新展開」, (Mitaka, Japan, Jul. 26-27, 2010).
Suematsu, Y., Yatini, C. Y.: 2010, Sunspot Motions and Flare
Activity, 太陽フレア望遠鏡 20 周年記念研究会「太陽観測装置の新展開」, (Mitaka, Japan, Jul. 26-27, 2010).
Suematsu, Y., Yatini, C. Y.: 2010, Sunspot Proper Motion and
Flare Onset Prediction, AGU Fall Meeting, (San Francisco, CA,
USA, Dec. 13-17, 2010).
Suematsu, Y., Katsukawa, Y., Shimizu, T., Ichimoto, K.,
Horiuchi, T., Matsumoto, Y., Takeyama, N.: 2010, Optical and
Thermal Design of 1.5-m Aperture Solar UV Visible and IR
Observing Telescope for Solar-C Mission, Int. Conf. on Space
Optics, (Rhodes, Greece, Oct. 4-8, 2010).
Sugiyama, K., Fujisawa, K., Wajima, K., Honma, M., SawadaSatoh, S., Murata, Y., Mochizuki, N., Doi, A.: 2010, Infall
Motions of the 6.7 GHz Methanol Masers in the High-Mass
Star-forming Region Cepheus A, Great Barriers in High MassStar Formation, (Townsville, Australia, Sep. 13-17, 2010).
Tachihara, K.: 2010, Origin of the Interstellar Turbulence and
Its Role in Star Formation, The impact of Herschel Surveys on
ALMA Early Science, (Garching, Germany, Nov. 16-19, 2010).
Tachihara, K., Takahashi, H.: 2010, Introduction of instruments
in Gunma Astronomical Observatory and transit observation at
GAO, YETI/TTV/Mammut f2f workshop on "Young Planetary
Systems", (Jena, Germany, Nov. 15-17, 2010).
Takada, N., Nakayama, H., Awazu, S., Ichihashi, Y., Shimobaba, T.,
Masuda, N., Ito, T.: 2010, A real-time color electrohorographic
reconstruction system using multi graphics processing unit,
IDW'10, (Fukuoka, Japan, Dec. 1-3, 2010).

Takahashi H. R.: 2011, Relativistic Magnetohydrodynamic
Simulation of Magnetic Reconnection, Mgnetic Reconnection
2010, (Nara, Japan, Dec. 6-9, 2010).
Takahashi H. R., Masada Y.: 2011, Stability MRI-Turbulent
Accretion Disks, The First Year of MAXI: Monitoring Variable
X-ray Sources, (Tokyo, Japan, Nov. 30-Dec. 2).
Takahashi H. R., Matsumoto J., Masada Y., Kudoh T.: 2010,
Numerical Study of Relativistic Magnetic Reconnection,
Deciphering the Ancient Universe with Gamma-Ray Bursts,(Kyoto, Japan, Apr. 19-23, 2010).
Takahashi H. R., Matsumoto J., Masada Y., Kudoh T.: 2010,
Relativistic Magnetohydrodynamic Simulation of Sweet-Parker
type Magnetic Reconnection, The Fourth East Asia Numerical
Astrophysical Meeting, (Taipei, Taiwan, Nov. 2-5, 2010).
Takahashi, R.: 2010, Behavior of an inverted pendulum in the
Kamioka mine, Gravitational-Wave Advanced Detector Workshop
2010 (GWADW2010), (Kyoto, Japan, May 16-21, 2010).
Takahashi. R., Saito, Y., Suzuki, T.: 2010, Vacuum System for theLarge-Scale Cryogenic Gravitational Wave Telescope (LCGT),
AVS 57th Int. Symp. & Exhibition, (Albuquerque, NM, USA,
Oct. 17-22, 2010).
Takano, S., et al. including Hirota, T., Nakajima, T., Ohishi,
M., Umemoto, T.: 2010, Nobeyama 45 m Telescope Legacy
Project: Line Survey (II), Workshop on Interstellar Matter 2010,(Sapporo, Japan, Sept. 13-15, 2010).
Takiwaki T.: 2010, Special Relativistic Simulrations ofMagnetically-dominatyed Jets in Collapsing Massive Star,
The 4th East Asian Numerical Astrophysics Meeting, (Taipei,
Taiwan, Nov. 2-5, 2010).
Takiwaki T.: 2010, Neutrino Pair Annihilation in Collapsars,
Deciphering the Ancient Universe with Gamma-Ray Bursts,(Kyoto, Japan, Apr. 19-23, 2010).
Tamura, M.: 2010, Strategic Exploration of Exoplanets and Disks
with Subaru (SEEDS), An Ishigaki Int. Conf. on Evolving Theory
for Planet Formation, (Ishigaki, Japan, Jun. 20-26, 2010).
Tamura, M.: 2010, Strategic Exploration of Exoplanets and Disks
with Subaru (SEEDS), Princeton SEEDS Workshop, (Princeton,
USA, Jul. 5-9, 2010).
Tamura, M.: 2010, First Results from SEEDS, Lyot Conf. 2010,(Paris, France, Oct. 25-29, 2010).
Tamura, M.: 2010, SIRPOL: Wide-Field NIR Polarimetry ofStar Forming Regions, IRSF Workshop, (Nagoya, Japan, Nov.
16-18, 2010).
Tamura, Y., Kazama, T., Jike, T., Manabe, S., Asari, K.: 2010,
Collocated Geodetic Observations with a Superconducting
Gravimeter, VLBI and GPS in NAOJ Mizusawa, Second Asian
SG Workshop, (Taipei, Taiwan, Jun. 21-22, 2010).
Tanikawa, K., Sôma, M.: 2010, How were eclipses memorized
when there were no astronomers?, 7th Int. Conf. on Oriental
Astronomy (ICOA-7), (Tokyo, Japan, Sep. 6-10, 2010).
Tatsumi, D.: 2010, TAMA300, Gravitational-Wave Advanced
Detector Workshop 2010(GWADW2010), (Kyoto, Japan, May
16-21, 2010).
Tomida, K., Machida, M. N., Saigo, K., Tomisaka, K., Matsumoto,T.: 2011, First Cores in Very Low-Mass Molecular Cloud Cores,
Winter School and Workshop on Star Formation, (Mitaka,

Japan, Feb. 21-25, 2011).
Tomida, K., Tomisaka, K., Matsumoto, T., Kawabe, R.,
Machida, M. N., Saigo, K.: 2010, Numerical Models of theFirst Cores: Comparison with Observed Candidates, The Originof Stellar Masses, (Tenerife, Spain, Oct. 18-22, 2010).
Tomida, K., Tomisaka, K., Matsumoto, T., Machida, M. N., Saigo,
K.: 2010, Formation, Evolution and Observability of low-massFirst cores, Frontiers in Computational Astrophysics: Particle
and Flames in Radiative and Magnetic Flows, (Lyon, France,
Oct. 11-15, 2010).
Tomida, K., Tomisaka, K., Matsumoto, T., Machida, M. N., Saigo,
K., Ohsuga, K.: 2010, RMHD simulations of low-mass starformation, The 4th East Asian Numerical Astrophysics Meeting,(Taipei, Taiwan, Nov. 2-5, 2010).
Tomida, K., Tomisaka, K., Matsumoto, T., Ohsuga, K., Machida,
M. N., Saigo, K.: 2010, RMHD simulation of Proto-stellar
Collapse, IAU Symp. 270: Computational star formation,(Barcelona, Spain, May 31-Jun. 4, 2010).
Tomida, K., Tomisaka, K., Matsumoto, T., Ohsuga, K., Machida,
M. N., Saigo, K.: 2010, Nested-Grid RMHD Simulation ofProto-stellar Collapse, The Early Phase of Star Formation 2010
(EPoS 2010), (Schloss Ringberg, Germany, Jun. 14-18, 2010).
Tomisaka, K.: 2011, Origin of Molecular Outflow Determinedfrom Thermal Dust Polarization, Winter School and Workshop
on Star Formation, (Mitaka, Japan, Feb. 21-25, 2011).
Tsuji, H., Nishimura, A., Sakaguchi, T., Katase, T., Kizawa, J.,
Kunizane, M., Matsumoto, K., Minowa, M., Kimura, K., Abe,Y., Muraoka, K., Onishi, T., Ogawa, H., Dobashi, K., Handa,
T., Nakajima, T., Kuno, N.: 2010, Status of 1.85m Radio
Telescope, The 11th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Nagoya, Japan, Nov. 14-16, 2010).
Tsujimoto, T.: 2010, Science brought by JASMINE data, ELSA
conference 2010 GAIA: At the Frontiers of Astrometry, (Sèvres,France, Jun. 7-11, 2010).
Tsujimoto, T., Bekki, K.: 2010, Diagnosis of the IMF in the
Universe Using the C, N Abundances, Why Galaxies Care
About AGB Stars II, (Wien, Austria, Aug. 16-20, 2010).
Tsukamoto, Y.: 2010, The self gravity effect on the orbital stabilityof Twotinos, WPGM2010, (Taipei, Taiwan, Jun. 21-25, 2010).
Tsukamoto, Y.: 2010, The self gravity effect on the orbital stabilityof Twotinos, AOGS 2010, (Hyderabad, India, Jul. 5-9, 2010）.
Tsuneta, S.: 2010, Polar fields: are they today well determined?,
Hinode-IV: unsolved problems and recent insights, (Mondello,
Palermo, Italy, Oct. 11-15, 2010).
Tsuneta, S.: 2010, Solar Magnetism as revealed by Hinodesatellite, IAU Symp. 271: Astrophysical Dynamics: From Stars
to Galaxies, (Nice, France Jun. 21-25, 2010).
Ujihara, H., Kimura, K., Ogawa, H., Matsumoto, K., Kuroiwa, K.,
Tsuboi, M., Kamegai, K., Kawahara, K., Murata, Y., Kasuga, T.,
Homma, M.: 2010, Development of Multimode Horns forRadio Telescopes, Asia-Pacific Radio Science Conf., (Toyama,
Japan, Sep. 22-26, 2010).
Ujihara, H., Kouzuma, S., Nakagawa, A., Nakanishi, H., Kawaguchi,N., Ohta, I.: 2010, Numerical Simulations of Tapterd Slot
Anttenas for SKA, Asia-Pacific Radio Science Conf., (Toyama,
Japan, Sep. 22-26, 2010).

II Publications, Presentations099

Usuda, T.: 2010, Future Instrument Plan of JAPAN, SPIE Astronomical
Instrumentation, (San Diego, CA, USA, Jun. 27-Jul. 2, 2010).
Usuda, T.: 2011, Near-Infrared High Resolution Spectrograph, TMT
Science and Instrument WS, (Victoria, Canada, Mar. 28-30).
Usuda, T., Terada, H.: 2010, Subaru Telescope: The view 2010-2020,
W.M. Keck Observatory in the post Astro2010 Era, (Oxnard,
USA, Sep. 2010).
Uzawa, Y., Fujii, Y., Kaneko, K., Kroug, M., Gonzalez, A.,
Kojima, T., Kuroiwa, K., Miyachi, A., Makise, K., Wang,
Z., Shan, W.: 2010, Development of the 787-950 GHz ALMABand 10 Cartridge, Asia-Pacific Radio Science Conf., (Toyama,
Japan, Sep. 22-26, 2010).
Uzawa, Y., Fujii, Y., Kaneko, K., Kroug, M., Kojima, T., Kuroiwa,
K., Miyachi, A., Makise, K., Wang, Z., Shan, W.: 2010,
Performance of the ALMA Band 10 SIS Receiver Prototype
Model, Applied Superconductivity Conf., (Washington DC,
USA, Aug. 1-6, 2010).
Vaubaillon, J., Watanabe, J., Sato, M.: 2010, 2011 Draconids:
Meteor Storm Or Just An Outburst?, DPS 42nd Annual Meeting
Pasadena, (Pasadena, CA, USA, Oct. 3-8, 2010).
Wada, T., Takata, J., Shibata, S.: 2010, A three dimensional
particle simulation for axisymmetric pulsar magnetospherewith GRAPE-DR, The 4th East Asian Numerical Astrophysics
Meeting, (Taipei, Taiwan, Nov. 2-5, 2010).
Watanabe, T., Hara, H., Sterling, A. C., Harra, L. K.: 2010,
Production of high-temperature plasmas during the early phasesof C9.7 flare II, Hinode-IV: unsolved problems and recent
insights, (Mondello, Palermo, Italy, Oct. 11-15, 2010).
Watanabe, T., Yamamoto, N., Kato, D., Sakaue, H. A., Murakami,
I.: 2010, Fe XVII Emission Lines Seen in A Solar Active Region
and the Large Helical Device, 38th COSPAR Scientific Assembly,(Bremen, Germany, Jul. 18-25, 2010).
Watnabe, T.: 2010, Iron Line Diagnostics of Non-Equilibrium Plasma
in Solar and Laboratory Plasmas, Solar Plasma Spectroscopy:
Achievements And Future Challenges, Celebrating the Career of
Dr Helen Mason, Cambridge, UK, Sep. 13-15, 2010).
Yamada, Y., Gouda, N., Lammers, U.: 2010, Nano-JASMINE: useof AGIS for the next astrometric satellite, ELSA conference2010 GAIA: At the Frontiers of Astrometry, (Sèvres, France,
Jun. 7-11, 2010).
Yamada, Y., Gouda, N., Lammers, U.: 2010, Application of Gaia
analysis software AGIS to Nano-JASMINE, Astronomical Data
Analysis Software and Systems XX, (Boston, MA, USA, Nov.
7-11, 2010).
Yamaguchi, M., Ootsubo, T., Watanabe, J., Honda, M., Sakon,
I., Ishiguro, M., Sarugaku, Y., Shinnaka, Y., Kobayashi, H.,
Kawakita, H.: 2010, Crystalline Silicate Grains Of Comet
17P/Holmes Ejected At Its Outburst Observed With Subaru/
COMICS, DPS 42nd Annual Meeting Pasadena, (Pasadena, CA,
USA, Oct. 3-8, 2010).
Yamashita, K.: 2010, The young star cluster on the accretion flowin G10.6-0.4, East Asia VLBI Workshop 2010, (Kagoshima,
Japan, Apr. 22-24, 2010).
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Hatsutori,Y., Murooka, J., Niwa, Y., Yamada, Y.: 2010, Current Statusof Astrometry Satellite missions in Japan: JASMINE project100

II Publications, Presentations

series, ELSA conference 2010 GAIA: At the Frontiers of
Astrometry, (Sèvres, France, Jun. 7-11, 2010).
Yasutake. N., Maruyama, T., Tatsumi, T.: 2010, Finite size effectsof quark-hadron phase transition in supernovae, From quark tosupernovae, (Shizuoka, Japan, Nov. 28, 2010).
Yasutake. N., Maruyama, T., Tatsumi, T.: 2010, Quark-hadron
mixed phase with hyperons in proto-neutron stars, Nuclei in the
Cosmos XI, (Heidlberg, Germany, Jul. 19-23, 2010).
Yasutake. N., Maruyama, T., Tatsumi, T.: 2011, Pasta Structuresof Quark-Hadron Phase Transition in Proto-Neutron Stars, 24thInt. Nuclear Physics Conf., (Vancouver, Canada, Jul. 7-9, 2010).
Yonekura, Y., Momose, M., Yokosawa, M., Ogawa, H., Fujisawa,
K., Takaba, H., Sorai, K., Nakai, N., Kameno, S., Kobayashi, H.,
Kawaguchi, N.: 2010, Present Status and the Future Prospect of
the Takahagi and Hitachi 32-M Radio Telescopes, Asia-PacificRadio Science Conf., (Toyama, Japan, Sep. 22-26, 2010).
Yonezu, T.: 2010, THz High-Resolution TuFIR Spectroscopy ofPure Rotational Transitions of Molecular Ions H2D+, Workshop
on Interstellar Matter 2010, (Sapporo, Japan, Sept. 13-15, 2010).
Yonezu, T.: 2010, THz high-resolution high-precision spectroscopyof pure rotational transitions of gas phase OH– and OD– molecular anions and analysis, Int.l Symp. on Frontier ofTerahertz Spectroscopy IV: Innovation in THz Spectroscopy
and THz – Wave Wireless Communications, (Matsumoto,Japan, Oct. 20-22, 2010).
Yoshida, F., Ito, T., Takahashi, S., Okita, K., Karoji, H., Ozaki,
S., Yanagisawa, T., Kurosaki, H., Yoshikawa, M., Yamaguchi,T., Takahashi, N., Urakawa, S., Ohtani, H., Nozawa, Y.: 2010,
Japanese activities concerning Maidanak, Maidanak Users
Meeting 2010, (Tashkent, Uzbekistan, June 21-25, 2010).
Yoshida, F., Yagi, M., Komiyama, Y., Nakata, F., Furusawa,
H., Ohno, T., Okamura, S., Nakamura, T.: 2010, Slitless
Spectroscopy of Small Solar System Bodies on a Dark Cloud
Curtain, AOGS 2010, (Hyderabad, India, Jul. 5-9, 2010).
Yoshida, F.: 2010, Stars of Asia, 8th EAMA (East Asian Meetingon Astronomy) Symp., (Shanghai, China, Oct. 10-15, 2010).
Yoshida, F.: 2010, Stars of Asia, 11thPCST, (New Delhi, India,
Dec. 6-10, 2010).
Yoshida, F.: 2011, History of the solar system derived from therecord on the Moon surface What happened on the Moon 3.8
billion years ago?, You are Galileo! Workshop in Indonesia,(Jakarta, Indonesia, Feb. 22, 2011)
Yoshida, F.: 2011, History of the solar system derived from therecord on the Moon surface What happened on the Moon 3.8
billion years ago?, You are Galileo! Workshop in Indonesia,(Yogyakarta, Indonesia, Feb. 24, 2011).
Yoshida, H.: 2010, Super-integrable 2D homogeneous potentials
of degree -2, The 13th Slovenia-Japan seminar on nonlinear
science, (Tokyo, Japan, Nov. 4-6, 2010).
Yoshida, H.: 2010, Necessary conditions for integrability andsuper-integrability of Hamiltonian systems with homogeneous
potential, 7th Int. Conf. on Differential Equations andDynamical Systems, (Tampa, FL, USA, Dec. 15-18, 2010).
Yoshida, H.: 2010, A family of super-integrable homogeneous
potentials of degree -2, UPC Int. Integrability Seminar 2010,(Barcelona, Spain, Jun. 7-8, 2010).