Cover Caption
The total solar eclipse on July 22, 2009, observed on the pacific ocean near Kita-Iwo Jima by H. Fukushima, A. Miyachi, and M. Katayama.
It became topical because the path of totality covered a part of the land of Japan for the first time in 46 years.

Postscript
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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
http://www.nao.ac.jp/
Hobunsha Co., Ltd.
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TEX: +81-42-792-3100
FAX: +81-42-792-3162

Annual Report of the
National Astronomical Observatory of Japan

Fiscal 2009

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Shoken MIYAMA
Director General
National Astronomical Observatory of Japan

Preface

I Scientific Highlights April 2009 – March 2010

001

II Publications, Presentations
1

Refereed Publications

047

2

Publications of the National Astronomical Observatory of Japan

058

3

Report of the National Astronomical Observatory of Japan

059

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Conference Proceedings

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Publications in English

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Conference Presentations

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Annual Report of the
National Astronomical Observatory of Japan
Fiscal 2009

P R E F A C E

Shoken MIYAMA
Director General of NAOJ

I am pleased to present the Annual Report of the
National Astronomical Observatory of Japan (NAOJ) for
fiscal 2009.
The year 2009 was a year full of exciting events
that drummed up the national interest in science. Thisis because of the International Year of Astronomy 2009
(IYA2009) that was declared by the United Nations tocelebrate the 400th anniversary of the first use of anastronomical telescope by Galileo Galilei in 1609. A
variety of IYA2009 events were held on a local level inJapan and throughout the world, raising great interestin astronomy and astrophysics. In the year of IYA2009,
Japan was blessed with an opportunity of the total eclipse,
which came to national attention. Unfortunately, badweather on the day of the eclipse prevented people withhigh expectation for the astronomical event from seeing
it in the main land. On the other hand, a spectacular
eclipse was fully observed on the ocean of the Ogasawara
Islands’ area, about 1,000 km south of Tokyo. For thisevent, NAOJ sent a group of researchers to one of the
Ogasawara Islands, Iwo Island to successfully conduct
a spectrum observation of the Sun’s corona. The sundrew attention in 2009 for another reason: the numberof sunspots on its surface. The sun has an active phaseand a quiet phase in turn in its 11-year activity cycle.
The phase is identified by the number of sunspots, which
are observed more in the active phase and less in thequiet phase. The sun was expected to enter the active

phase from the quiet phase in 2009, but it had been quiet
without increasing the number of sunspots. Experts
suspected the sun might be in the maunder minimum
where the number of sunspots was abnormally low forseveral decades in the 1600s. It is said that, back then in
Europe, the temperature became so low the Thames Rivergot frozen. The quiet sun this time seems not as abnormal
as in the maunder minimum in the 1600s because thenumber of sunspots has been on the rise since around theend of 2009. Solar physicists are studying this unusual
solar event as an intriguing phenomenon to figure out
what is behind it.
In Mitaka Campus of NAOJ, Mitaka Picture Book
House in the Astronomical Observatory Forest was
opened to the public on July 7, 2009. The house wasone of more than 40 wooden, one-story Japanese-style
houses built in the Campus during the period from 1915
through 1951 for researchers and their families. Thosehouses were demolished a few years ago, except thefirst house constructed before the others, as considered
too dangerous to live in due to their old age and poor
earthquake resistance. The first house was a luxurious
historical structure built in 1915 for professors andtheir families, having a study, living room, kitchen, an
apprentice room, and even a maid room. The house cameto be known to Mitaka City, which proposed an idea to
NAOJ to collaboratively renovate and transform it intoa facility where children can enjoy picture book story

sessions. Located next to the cutting-edge space research
center and surrounded by lush forest, Mitaka PictureBook House in the Astronomical Observatory Forest has
been attracting many children and their parents since its
opening, thanks to proactive efforts by the municipal
office staff of Mitaka City dedicated to the operation ofthis House.
In addition to those described above, we steadily
make best efforts through public outreach and educational
activities by Public Relations Center of NAOJ in order
to be an institute open to and introduce up-to-datescientific information and astronomical findings to the
public. Mizusawa Campus of NAOJ, Nobeyama Radio
Observatory, Okayama Astrophysical Observatory, andthe Subaru Telescope are also making the same efforts byregularly opening the facilities to the public and having
a special open house day where visitors can have close
contacts with researchers.
NAOJ continuously released research findings in 2009that intrigued interest from scientific communities andthe public. The year 2009 marked the 10th anniversary of
the reception of the first light with the Subaru Telescopethat keeps achieving amazing scientific results. In the
exploration of extrasolar planets, it discovered a planet
orbiting counter to the direction of a fixed star’s rotationand succeeded in taking the world’s first, direct picture ofa star that is considered a planet of a sunlike central star.
The direct picture taking itself is the second success inthe world following the first by a North American teamof astronomers in 2008, but taking a direct picture of aplanet with a sunlike host star is the first success in theworld. The discovery of these planets poses challenges tothe current view of planet formation theory. The Subaru
Telescope also produced world-acclaimed results for the
study of cosmology and in the field of galaxy physics.
In October, a symposium to introduce the results by the
Subaru Telescope was held in Tokyo, followed by a party
where persons involved were invited.
The ALMA Project, an international project among
East Asian, North American and European countries andregions, marked its 6th year of construction. Japan has
started the construction of 7-meter-diameter antennas
following that of 12-meter-diameter antennas. At the
ALMA’s high site of 5,000 meters asl, interferometry
experiments were conducted with three antennas
constructed by Japan and the United States to confirm theappropriate operability of the antennas. As to the antenna

receivers, a Band-10 cartridge assembly with highest
frequencies among the ALMA bands was successfully
fabricated. This significant milestone proves that the
NAOJ’s capability of cartridge development is the world’s highest level as the cartridge fabrication requires
ultraprecision machining at a level never before achieved.
The ALMA Project is steadily advancing the process tothe completion of the ALMA Observatory, making further
efforts necessary for the inception of the early and fullscale operation.
Each Observatory of NAOJ is also producing
remarkable scientific results. Okayama AstrophysicalObservatory made a world record by successfully
spotting the gamma-ray burst that detonated 13.1 billion
light years from Earth and is the most distant burst in
the universe overall. Nobeyama Radio Observatory
successfully observed ”monster galaxy” that is actively
forming stars and obtained data suggesting the presence
and distribution of “dark matters” around the galaxy. The
lunar explorer Kaguya, in which the RISE Project Teamof Mizusawa Campus of NAOJ participated, completed
its mission when it fell onto the moon in May 2009.
NAOJ released the groundbreaking study results obtainedwith the explorer such as the gravity map and detailed
topographic map of the moon. Of all the results, theprecise data of the nearside and farside of the moon drewa great deal of attention.
NAOJ is an inter-university research instituteoperating an array of the researches described above.
These researches are conducted in response to requests
from researchers of universities throughout Japan, andmost of the research results are shared by NAOJ andthe researchers of these universities participated in the
research. For further development, education of andprovision of research guidance to young researchers areindispensable elements. NAOJ is continuously making
significant efforts in postgraduate education at theGraduate University for Advanced Studies and throughcollaboration with other universities. Your continued
support will be greatly appreciated.

Shoken MIYAMA
Director General of NAOJ

I Scientific Highlights(April 2009 – March 2010)

01 Potassium Abundances in Red Giants of Globular Clusters

TAKEDA, Y., et al.

003

02

The Circumbinary Outf low: A Protostellar Outf low Driven by a
Circumbinary Disk

MACHIDA, M. N., et al.

004

03

Buried active supermassive blackholes as a function of galaxy infrared
luminosity revealed through Spitzer infrared spectroscopy

IMANISHI, M., et al.

005

04

Direct Imaging of Bridged Twin Protoplanetary Disks in a Young
Multiple Star

MAYAMA, S., et al.

006

OKOSHI, K., et al.

007

05 HI-selected galaxies and quasar absorption systems
06

Global Radiation-Magnetohydrodynamic Simulations of Black Hole
Accretion Flow and Outflow: Unified Model of Three States

OHSUGA, K., et al.

008

07

GreeM: Massively Parallel TreePM Code for Large CosmologicalN-body Simulations

ISHIYAMA, T., et al.

009

08

Magnetic Field Structure of the HH 1–2 Region: Near-Infrared
Polarimetry of Point-Like Sources

KWON, J., et al.

010

09

Stochastic Nature of Gravitational Waves from Supernova Explosions
with Standing Accretion Shock Instability

KOTAKE, K.

011

10

Centroid Experiment for 10 −4 Pixel Order Determination of the
Positions of Stars

YANO, T., et al.

012

11

Ach romat ic de e p nu l l i ng w it h a t h ree - d i me n sional Sag na cinterferometer

YOKOCHI, K., et al.

013

12

Interstellar Extinction Law toward the Galactic Center: J, H, KS bands,
and 3.6, 4.5, 5.8, 8.0 µm

NISHIYAMA, S., et al.

014

NISHIYAMA, S., et al.

015

14 A Necessary Condition for Individual Time-steps in SPH Simulations

SAITOH, T., MAKINO, J.

016

15 Chemical composition of extremely metal-poor stars in a dwarf galaxy

AOKI, W., et al.

017

HATSUTORI, Y., et al.

018

SHIMOJO, M.,
TSUNETA, S.

019

TAKAHASHI, R., et al.

020

OKAMOTO, T., et al.

021

SCHOLZ, A., et al.

022

21 Constructing a Theoretical Model for High-z Lyman α Emitters

KOBAYASHI, M., et al.

023

22 A Cluster of Starburst Galaxies 11.5 Billion Light-years Away

TAMURA, Y., et al.

024

23 Fiber-link between Okayama 1.88-m reflector and HIDESKAMBE, E., et al.

025

24 Observations of transient objects using OAO/ISLEIMADA, A., et al.

026

KUSAKABE, M., et al.

027

13 Near-infrared Polarized Flares from Sgr A*

16 Performance Evaluation of Nano-JASMINE
17The Relation between the Magnetic Fields and the Coronal Activities
in the Polar Coronal Hole18 Sensitivity improvement of CLIO with cooling the mirrors
19 Prominence formation associated with an emerging helical flux rope
20

25

Substellar Objects in Nearby Young Clusters (SONYC): The Bottom of
the Initial Mass Function in NGC 1333

Effect of Long-lived Strongly Interacting Particles on Big Bang
Nucleosynthesis

001

26

Subaru/COMICS Mid-Infrared Observation of the Near-Nucleus
Region of Comet 17P/Holmes at the Early Phase of an Outburst

WATANABE, J.-I., et al.

028

27

BD+44º493: A Ninth Magnitude Messenger from the Early Universe;
Carbon Enhanced and Beryllium Poor

ITO, H., et al.

029

28

Entire Topography of Lunar Surface: A Movie Created from KAGUYA(SELENE) Data

NAKAYAMA, H., et al.

030

UEDA, K., et al.

031

THALMANN, C., et al.

032

29 Orientation of X-Ray Bright Points in the Quiet Sun
30 Discovery of the Coldest Imaged Companion of a Sun-like Star
31

Development of Cryogenic Integration Circuits with GaAs JFETs for
Sub-millimeter Camera

HIBI, Y., et al.

033

32

Detection of the most distant explosion ever known (Near-infraredobservation of GRB 090423@z = 8.2)

YOSHIDA, M., et al.

034

33

Neutrino-Induced Reactions on 56Ni and Production of 55Mn in
Population III StarsSUZUKI, T., KAJINO, T.

035

34 Search for Remnant Clouds Associated with the TW Hya Association

TACHIHARA, K., et al.

036

35 Polarimetric mode of stellar interferometer using birefringent retarders

MURAKAMI, N., et al.

037

36

Emission Signature of a Young Protostellar Object: Line Transfer Studyof an Embedded Young Molecular Outflow

YAMADA, M., et al.

038

37

An improved lunar gravity field model from SELENE and historical
tracking data

MATSUMOTO, K., et al.

039

38

Development of the Lunar Crustal Thickness Model by SELENE(Kaguya) Selenodetic Data

ISHIHARA, Y., et al.

040

39 The new detections of 7Li/6Li isotopic ratio in the interstellar media

KAWANOMOTO, S., et al.

041

40 The interstellar rubidium isotope ratio toward HD169454

KAWANOMOTO, S., et al.

042

HAYAKAWA, T., et al.

043

41 s-Process contribution to Sn-115 [1]

002

42

Neutrino-nucleus reactions via neutral and charged currents by the
Quasi-particle Random Phase Approximation(QRPA)CHEOUN, M.-K., et al.

044

43

Imaging Spectroscopy on Pref lare Coronal Nonthermal Sources
Associated with the 2002 July 23 Flare

ASAI, A., et al.

045

44

Multiple Plasmoid Ejections and Associated Hard X-ray Bursts in the2000 November 24 FlareNISHIZUKA, N., et al.

046

Potassium Abundances in Red Giants of Globular Clusters
TAKEDA, Yoichi(NAOJ / GUAS)KANEKO, Hiroyuki, MATSUMOTO, Naoko, OSHINO, Shoichi, ITO, Hiroko, SHIBUYA, Takatoshi(GUAS)

KI 7698.98

KI 7664.91

Fe I 7664.29

Given the confusing situation regarding the [K/Fe]
ratio of metal-poor stars in the halo, where some worksuggests a fairly tight tendency (such like disk stars)
while others report a considerably large diversity
amounting to ~1 dex, we carried out a spectroscopic
study on 15 red giants of three mildly to very metal-poor
globular clusters (M 4, M 13, and M 15) along with two
reference stars (ρ Boo and α Boo) based on the highdispersion spectra obtained with Subaru/HDS (cf. Figure1), with a purpose of clarifying the behavior of [K/Fe] at
the relevant metallicity range of −2.5 <~ [Fe/H] <
~ −1.

ρ Boo
α Boo
M4 L2406
M4 L2617

analysis.
This result is quite consistent (i.e., smoothly connecting) with the [K/Fe] trend of disk stars (−1 <~ [Fe/H])
and that of extremely metal-poor stars (−4 <~ [Fe/H] <~−2.5). That is, [K/Fe] appears to continue a gradualincrease from [Fe/H] ~ 0 toward a lower metallicity
regime down to [Fe/H] ~ −3 (cf. Figure 2), where a broad
maximum of [K/Fe] ~ +0.3 – 0.4 is attained, possibly
followed by a slight downturn toward a further lower
metallicity at [Fe/H] <~ −3.
This investigation is based on the data obtained by
the observation with the Subaru Telescope, which was
carried out during the practical training of observational
astronomy for graduate students as a coursework of The
Graduate University for Advanced Studies (SOKENDAI).
More detailed results of this study are described in [1].

M4 L3209

1

M4 L3624
M4 L4511
M13I -130.5

M13 II-76

0.5[K/Fe]

M13 III-52
M13 III-59
M13 III-73
M15K 144

III-73

L2406

G

0

M15K 341
M15K 431-0.5 (a)M15K 634
M15K 825

7665

7666 7698 7699
Wavelength (Å)

7700

Figure 1: Spectra of 17 stars in the neighborhood of the K I 7665
line and the K I 7699 line.

The atmospheric parameters (Teff, log g, vt, and [Fe/H])
were spectroscopically determined by using Fe I and Fe II
lines, and the abundance of K was derived from the K I
resonance lines at 7664.91 and 7698.97 Å while taking
the non-LTE effect into account.
We confirmed that [K/H] (as well as [Fe/H]) isalmost homogeneous within each of the three clusters
to a precision of <~ 0.1 dex, though superficially large
deviations are exceptionally seen for two peculiar stars
which show signs of considerably increased turbulence inthe upper atmosphere.
The [K/Fe] ratios of these cluster stars turned out
mildly supersolar by a few tenths of dex, tending togradually increase from ~ +0.1–0.2 at [Fe/H] ~ −1 to~ +0.3 at [Fe/H] ~ −2.5, which is a fairly tight and clean
trend. We thus consider that the previously reported
large diversity of [K/Fe] in halo stars is not real, which
we suspect to be due to some improper treatment in the

∆NLTE

7664

0
-0.2
-0.4
-0.6 (b)
-4

S

T

-3

-2
[Fe/H]-1

0

Figure 2: (a) The [K/Fe] vs. [Fe/H] plots constructed from themetallicity and the NLTE potassium abundances
determined by us. The results for the 17 program stars
are shown in large open symbols (diamonds for ρ Boo
and α Boo, squares for M 4 stars, circles for M 13 stars,
and triangles for M 15 stars). The two stars (M 13 III-73
and M 4 L2406) showing exceptionally large deviations
from the main trend are also indicated. Meanwhile,the smaller filled symbols represent the results for diskstars and extremely metal poor stars presented here forcomparison. Lines show the three kinds of theoreticalpredictions (b) The NLTE corrections for K abundance
NLTE
determinations (ΔNLTE is the average of ΔNLTE
7665 and Δ 7699 incase that both lines are available), plotted against [Fe/H].

Reference[1] Takeda, Y., et al.: 2009, PASJ, 61, 563.

I Scientific Highlights

003

The Circumbinary Outflow: A Protostellar Outflow Driven by
a Circumbinary Disk
MACHIDA, Masahiro N.

			

INUTSUKA, Shu-ichiro, MATSUMOTO, Tomoaki(NAOJ) 			

Outflow(vout>3cs)

Magnetic Field Strength

36 AU

Circumbinary disk
Proto-binary-1.5

log Bz [G]I Scientific Highlights

Magnetic Field lines

280 AU004

is verified by future observations such as ALMA.

280 AUThe protostellar outflow is star’s first cry at the
moment of birth. Since Snell discovered an outflow
from a protostar in 1980, over 300 outflows have been
observed in many star-forming regions. The protostellar
outflow is believed to be driven from the circumstellar
disk by release of the gravitational energy mediated by
the Lorentz and centrifugal forces [1]. In general, thestar is formed in gravitationally collapsing cloud cores.
The binary frequently appears through the fragmentationof the collapsing cloud core [2]. With the proto-binary
formation, the collapsing gas forms a circumbinary diskthat is frequently observed. Thus, outflow may be driven
also by the circumbinary disk.
In this study, the evolution of a magnetized rotating
cloud is investigated using three-dimensional resistive
MHD nested-grid code that covers over five orders ofmagnitude of spatial scale [3]. After the adiabatic coreformation in the collapsing cloud core, the magnetic flux
is significantly removed from the center of the cloudby the Ohmic dissipation. Since this removal makes
the magnetic braking ineffective, the adiabatic corecontinuously acquires the angular momentum to induce
fragmentation and subsequent binary formation. The
magnetic field accumulates in the circumbinary disk
where the removal and accretion of magnetic field arebalanced. The outflow is driven by the circumbinary disk,
while no outflow appears in the proximity of the protobinary because of the deficit of strong field.
Figure 1 left panel shows the configuration of theoutflow, which indicates that the outflow driven by thecircumbinary disk, not by the protostar (or proto-binary).
Figure 1 upper right panel shows the configuration ofmagnetic field lines that are strongly twisted by therotation of the circumbinary disk. The outer region of
circumbinary disk has a density of n < 1012 cm−3 and iswell coupled with the magnetic field that can drive theoutflow. On the other hand, the magnetic field is too
weak to drive outflow in the region around protobinary.
Figure 1 right lower panel shows Bz on the z = 0 planewith the same scale of left panel, and indicates that themagnetic field is weak around protobinary but strong in
the circumbinary disk.
This result explains the morphology of some specificyoung stellar objects such as L1551 IRS5. We can inferthat most of the bipolar molecular outflows observed
by low density tracers (i.e., CO) would correspond tocircumbinary or circum-multiple outflows found in thisletter, since most of the young stellar objects are supposed
to be multiples. We expect that the circumbinary outflows(Nagoya-University)

z=0 plane-3.0

Figure 1: Large-scale structure of l = 10 grid in three dimension.
Left panel: The configuration of circumbinary outflow isshown by red-volume, in which color means the outflow
speed. The density contours (colors) and velocity
vectors (arrows) are projected in each wall surface.
The square at lower right corner shows the close-up
view around the protobinary, in which color means thedensity distribution, and the high-density region (i.e.,
the protobinary) is represented by the red iso-density
surface. Right upper panel: The magnetic field lines
integrated from the circumbinary disk are plotted. The
bottom panel indicates the strength of Bz by the color.
Right lower panel: The strength of Bz on z = 0 plane isrepresented by the color.

References[1] Machida, M. N., Inutsuka, S.-i., Matsumoto, T.: 2008a, ApJ,
676, 1088.
[2] Machida, M. N., Tomisaka, K., Matsumoto, T., Inutsuka, S.-i.:
2008b, ApJ, 677, 327.
[3] Machida, M. N., Inutsuka, S.-i., Matsumoto, T.: 2007, ApJ, 670,
1198.

Buried active supermassive blackholes as a function of galaxy
infrared luminosity revealed through Spitzer infrared spectroscopy		

IMANISHI, Masatoshi(NAOJ) 		

MAIOLINO, Roberto.

(Rome Observatory) 		

Ultraluminous infrared galaxies (ULIRGs) radiatehuge infrared luminosities (LIR > 1012L), originatingfrom thermal emission from dust heated by energy
sources hidden behind dust. The energy sources can beenergy generation by nuclear fusion reaction inside stars(star-formation) and/or the conversion from gravitationalenergy produced by accreted material onto a compact
supermassive blackhole, to radiative energy (AGN
activity). Since the ULIRG population contributes
importantly to the cosmic infrared radiation density at z >1, distinguishing the energy sources of ULIRGs is closely
coupled to clarifying the connections between starformation and supermassive blackhole mass growth in
the dust obscured galaxy formation of the early universe.
Since a large amount of dust and gas concentrates tothe nuclear regions of ULIRGs, spatially-compact AGNs
can easily be buried (= obscured by dust in virtually all
directions) and become very difficult to find throughoptical spectroscopy, because of large dust extinction.
Infrared 5 – 35 µm spectroscopy is a powerful tool tostudy such optically elusive buried AGNs in ULIRGs,
because of much reduced effects of dust extinction.
Furthermore, PAH (Polycyclic Aromatic Hydrocarbons)emission features, found in this wavelength range, aredetected in starbursts, but not in pure AGNs, making thefeatures a good tool to distinguish the energy sources.
Finally, the optical depths of rest-frame 9.7 µm silicate
dust absorption features can also be used to differentiate
between normal star-formation (stellar energy sourcesand dust are spatially well mixed) and buried AGNs (theenergy source, a compact mass-accreting supermassive
blackhole, is more centrally concentrated than dust) [1].
We have extended Spitzer 5 – 35 µm infrared
spectroscopy to ULIRGs at z > 0.15 (Figure 1), and foundthat (1) optically-elusive, bur intrinsically luminousburied AGNs are common in ULIRGs, and (2) the
importance of buried AGNs increases with increasinggalaxy infrared luminosity (Figure 2), suggesting that theAGN-starburst connections are luminosity dependent[2,3]. We quantitatively estimated that the relative
energetic importance of buried AGNs is higher in more
infrared luminous galaxies, and these galaxies havecurrently higher star formation rates, and will evolve into
more massive galaxies with larger stellar masses in the
future. Our results may be observationally related to thewidely-proposed AGN feedback scenario as the possible
origin of the galaxy down-sizing phenomenon, where
currently more massive galaxies have finished their major
star-formation in an early cosmic age.

NAKAGAWA, Takao(ISAS)

Figure 1: (Left): Spitzer infrared 5–35 μm spectrum of a starburstdominated ULIRG, with strong PAH emission features.
(Right): Buried AGN, with non-detectable PAH emission
and strong silicate dust absorption features.

Figure 2: Detected buried AGN fraction as a function of galaxy
infrared luminosity. The abscissa is the decimallogarithm of infrared luminosity in units of solar
luminosity.

References[1] Imanishi, M., Dudley, C. C., Maiolino, R., Maloney, P. R.,
Nakagawa, T., Risaliti, G.: 2007, ApJS, 171, 72.
[2] Imanishi, M.: 2009, ApJ, 694, 751.
[3] Imanishi, M., Maiolino, R., Nakagawa, T.: 2010, ApJ, 709, 801.

I Scientific Highlights

005

Direct Imaging of Bridged Twin Protoplanetary Disks
in a Young Multiple Star
MAYAMA, Satoshi(The Graduate University for Advanced Studies [SOKENDAI])TAMURA, Motohide, HAYASHI, Masahiko, ISHII, Miki, PYO, Tae-Soo
SUTO, Hiroshi, NAOI, Takahiro, KUDO, Tomoyuki, HASHIMOTO, Jun(NAOJ)

MATSUMOTO, Tomoaki

NISHIYAMA, Shogo

KUZUHARA, Masayuki

006

I Scientific Highlights

A

-1.5

B

L2

L2

Secondary
Disk

Secondary
SR24N

L1

05

L1

PrimaryDisk

0

Primary
SR24S

N

L3

E
500 AU
3.1 arcsec

L3

-0.5

Studies of protoplanetary disks in multiple systems
are essential for describing the general processes of starand planet formation because most stars form as multiples[1]. However, such circummultiple disks and spiral arms
in multiple systems have rarely been directly resolved todate. Here, we present the direct image of an interacting
binary protoplanetary system [2]. We investigate thegeometry of a young (a stellar age of 4 million years)
multiple circumstellar disk system, SR24, to understandits nature based on observations and numericalsimulations. SR24 is a hierarchical multiple, located 160
pc away in the Ophiuchus star-forming region.
We obtained an infrared image of SR24 with CIAO
[3] mounted on the Subaru 8.2-m Telescope. (Fig. 1,left). The emission arises from dust particles mixed
with gas in the circumstellar structures scattering thestellar light. Both circumprimary and circumsecondarydisks are clearly resolved. Both disks overflow the inner
Roche lobes (dotted contours in Fig. 1), suggesting thatthe material outside the lobes can fall into either ofthe inner lobes. There is a bridge of infrared emission
connecting the two disks and a long spiral arm extending
from the circumprimary disk. A spiral arm would suggestthat the SR24 system rotates counter clockwise. The
orbital period of the binary is 15,000 yr. The arm would
also imply replenishment of the twin disk gas from thecircumbinary disk.
We performed 2D numerical simulations of accretionfrom a circumbinary disk to identify the features seenin the coronagraphic image(Fig. 1, right). Although thegas flow was not stationary, especially inside the Roche
lobes, the stage of the 2D simulations shown in Fig. 1
shared common features with the observed image. These
agreements between observation and simulation suggestthat the bridge corresponds to gas flow and a shock wave
caused by the collision of gas rotating around the primaryand secondary stars. The arm corresponds to a spiralwave excited in the circumbinary disk.

(University of Tokyo)-1(Kyoto University)		

(Hosei University)-1(Chiba University)			

-0

			

HANAWA, Tomoyuki

0

			

x

1

[mJy/arcsec ]
2

2

3

4

-2

-1

log

0

1

Figure 1: Observed and simulated images of the young multiple
star, SR24. (a) H-band (1.6 μm) coronagraphic imageof SR24. The total integration time was 1008 s. The
PSFs of the final images have sizes of 0.1 arcsecond(FWHM) for the H-band. The inner and outer Roche
Lobes are overlaid on the Subaru image as dotted anddashed lines, respectively. L1, L2, and L3 represent
the inner Lagrangian point, outer Lagrangian pointon the secondary side, and outer Lagrangian pointon the primary side, respectively. (b) Snapshot of
accretion onto the binary system SR24 based on 2D
numerical simulations. The color and arrows denote thesurface density distribution and velocity distribution,
respectively.

References[1] Ghez, A. M., Neugebauer, G., Matthews, K.: 1993, AJ, 106,
2005.
[2] Mayama, S., et al.: 2010, Science, 327, 306.
[3] Tamura, M., et al.: 2000, Proc. SPIE, 4008, 1153.

HI-selected galaxies and quasar absorption systems
		

OKOSHI, Katsuya

NAGASHIMA, Masahiro(Tokyo University of Science) 		

(Nagasaki University)

GOUDA, Naoteru, MINOWA, Yousuke(NAOJ)The quasar/GRB absorption systems provide us
with a unique probe of galaxy formation and evolution
processes. In particular, the HI absorption systems havebeen investigated extensively to place stringent constraint
on the physical condition of the galactic gas. However,
the origin of the absorption systems (e.g., damped
Lyα absorption system; DLA) are still unclear because
the optical counterparts are handful. For a purpose
to revealing the origin of DLAs, we focus on the HI
emission galaxies detected in blind radio surveys (e.g.,the HI Parkes All Sky Survey; HIPASS), and investigate
a link between the HI-selected galaxies and DLAs.
We employ a semi-analytic model for galaxy
formation [1, 2] which incorporates basic processesof galaxy formation (e.g., merging process and SN
feedback). The models, where the star formation rates(SFR) are high (the HS model) and low (the LS model),reproduce the HI mass functions (HIMFs) of the galaxy
population based on the radio observations (Figure 1(a)).
We find that the number fractions of DLAs relative
to galaxies are almost unity at MHI > 108M at redshift
z = 0 [3], which suggests a trend that gaseous disks ofgalaxies have HI column densities as high as those in
DLA systems. The HI-selected galaxies at MHI > 108M
correspond to DLA hosts. By contrast, in the lowmass range MHI < 108M, the number fractions begin to
decrease toward the low-mass end. This indicates that asmall amount of HI gas of the less massive systems does
not produce high enough HI column densities to detectas DLAs. More specifically, at the low-mass end, anotherpopulation, sub-DLAs, becomes dominant instead of
DLAs. The predicted number fractions of sub-DLAs
reaches 30% – 80% for MHI ~ 107M (Figure 1(b)).
The study of HI-selected galaxies (e.g., the SFRs
(Figure 2)) can offer statistically valuable information
about quasar absorption systems and opportunities forrevealing the origins that place stringent constraints ongalaxy formation and evolution.

Figure 1: (a) The HI mass functions of galaxies for models. The
shaded region represents the region of HIMFs given byvarious blind surveys. The points are the observational
data provided by the HIPASS (circles) and the Arecibo
Dual-Beam Survey (squares). The observations are
consistent with the HIMFs for the models. (b) The
histogram of number fractions of sub-DLAs. In the
low-mass range MHI < 108M, the number fractions are
obviously higher than those at MHI > 109M.
2

0

-2

-4

7

8

9

10

Figure 2: The contour map for the SFR vs the HI mass MHI ingalaxies for the LS model. The SFRs of optical/infrared
counterparts of HI-selected galaxies are shown as points
and boxes. A star formation rate in an optical counterpartof a DLA system is also plotted as cross (for details, [3]).
References[1] Okoshi, K., Nagashima, M., Gouda, N., Yoshioka, S.: 2004,
ApJ, 603, 12.
[2] Okoshi, K., Nagashima, M.: 2005, ApJ, 623, 99.
[3] Okoshi, K., Nagashima, M., Gouda, N., Minowa, Y.: 2010, ApJ,
710, 1295.

I Scientific Highlights

007

Global Radiation-Magnetohydrodynamic Simulations of Black Hole
Accretion Flow and Outflow: Unified Model of Three States
OHSUGA, Ken(Graduate University for Advanced Studies / NAOJ)
			

MORI, Masao(University of Tsukuba)		

Black-hole accretion, the most powerful energyproduction mechanism in the Universe, is known to
exhibit several distinct modes (or spectral states), such as
low-hard state, high-soft state, and so on. Onedimensionalmodels for each mode were proposed. However, theα-viscosity is assumed, although its physical basis is
not clear (for a review, see [1]). Since the disk viscosity
is likely to be of magnetic origin [2], dynamics ofmagnetized accretion disks has been extensively
studied via multi-dimensional MHD simulations [3, 4].
Nevertheless, our understanding of the accretion disk
today is far from being satisfactory, since the radiative
processes were neglected or restrictively treated in theprevious simulations.
Here, we report the results of our new simulations
that would open a new era of the accretion disk research.
We performed global, two-dimensional radiation-MHD(RMHD) simulations, in which radiation processes
as well as MHD processes are fully considered, we
demonstrate three distinct modes of accretion with thesame code by varying mass density normalizations.
When the density is large, a thick, very luminous (superEddington) disk forms (model A). When the density is

MINESHIGE, Shin
(Kyoto University)

KATO, Yoshiaki(JAXA)

moderate, the accreting gas can effectively cool byemitting radiation, thus generating a thin disk, i.e., thehighsoft state disk (model B). When the density is too
low for radiative cooling to be important, a disk becomes
hot, thick, and faint; i.e., the low-hard state disk (model
C). The magnetic energy is amplified within the disk
up to about twice, 30%, and 20% of the gas energy incases described above, respectively. Notably, the disk
outflows with helical magnetic fields, which are driven
either by radiation pressure force or magnetic pressure
force, are ubiquitous in any accretion modes. Finally, our
RMHD simulations first showed that the disk viscosity
is proportional to the pressure; this is hitherto the key
assumption of the phenomenological standard disk
theory.
References[1] Kato, S., Fukue, J., Mineshige, S.: 2008, Black-Hole Accretion
Disks - Towards a New Paradigm (Kyoto University Press).
[2] Balbus, S. A., Hawley, J. F.: 1991, ApJ, 376, 214.
[3] Machida, M., Hayashi, M. R., Matsumoto, R.: 2000, ApJ, 532,
L67.
[4] Hawley, J. F., Krolik, J. H.: 2001, ApJ, 548, 348.

Figure 1: Perspective view of inflow and outflow patterns near the black hole for models A, B, and C, from left to right, respectively. Upper
panels: Normalized density distributions (color) are overlaid with isosurfaces, at which the outward velocity equals to the escapevelocity. Lower panels: The distributions of the normalized radiation energy density (color) is overlaid with the magnetic field lines.

008

I Scientific Highlights

GreeM: Massively Parallel TreePM Codefor Large Cosmological N-body Simulations
FUKUSHIGE, Toshiyuki(K&F Computing Research Co.)		

MAKINO, Junichiro(NAOJ)

100
Time(sec/step)

We developed GreeM, a massively parallel TreePM
code for large-scale cosmological N-body simulations.
GreeM uses a recursive multi-section algorithm fordomain decomposition [1]. The size of the domains areadjusted so that the total calculation time of the force
becomes the same for all processes. Figure 1 shows thedomain decomposition for a simulation of a LCDM
universe.
Figure 2 shows the CPU times per step as a functionof the number of CPU cores. The loss of performancedue to non-optimal load balancing is around 4%, evenfor more than 103 CPU cores whereas those of existing
TreePM codes are more than 10% even for less than 256
CPU cores[2, 3] (Figure 3 shows the speed-up factors ofGreeM and GADGET-2). GreeM runs efficiently on PC
clusters and massively-parallel computers, such as a Cray
XT4. The measured calculation speed on Cray XT4 is 7
× 104 particles per second per CPU core, for the case ofan opening angle of θ = 0.5, if the number of particles per
CPU core is larger than 106 [4].
GreeM is extended for simulations on a planet-wide
distributed supercomputer [5]. We acheieved to run
simulations over a variety of supercomputers in Tokyo(Japan), Amsterdam (Netherlands), Edinburgh (UK), andEspoo (Finland). We are able to achieve ~87 % of theperformance compared to an equal number of cores on asingle supercomputer.

1014096 3 HECToR
2048 3 HECToR
31000 CfCA
512 3 CfCA
3
256 CfCA
10

10

102
103
number of CPU cores

104

105

Figure 2: Calculation time per step of our code as a function of
the number of CPU cores on Cray-XT4 and HECToR(Edinburgh).

100

Speed up

ISHIYAMA, Tomoaki(NAOJ / University of Tokyo)

10

GreeM
GADGET-2
1

1

10

100

1000

number of CPU cores
Figure 3: Speed up of our code and GADGET-2 plotted against
the number of CPU cores. The filled circles andopen squares show the result of GreeM and that of
GADGET-2, respectively.

References[1] Makino, J.: 2004, PASJ, 56, 521.
[2] Dubinski, J., et al.: 2004, New Astronomy, 9, 111.
[3] Springel, V.: 2005, MNRAS, 364, 1105.
[4] Ishiyama, T., et al.: 2009, PASJ, 61, 1319.
[5] Portegies Zwart, S., et al.: 2010, IEEE Computer Society, inpress.

Figure 1: Decomposition in the LCDM universe at z = 0. It shows
8 × 8 division in two dimensions.

I Scientific Highlights009

Magnetic Field Structure of the HH 1–2 Region:
Near-Infrared Polarimetry of Point-Like Sources
KWON, Jungmi(Kyung Hee University / Korea Astronomy and Space Science Institute)

CHOI, Minho

PAK, Soojong(Korea Astronomy and Space Science Institute)

KANDORI, Ryo, TAMURA, Motohide

			(NAOJ) 			

The HH 1–2 region in the L1641 molecular cloud wasobserved in the near-infrared (IR) J, H, and Ks bands,
and imaging polarimetry was performed. Seventy-six
point-like sources were detected in all three bands. The
near-IR polarizations of these sources seem to be caused
mostly by the dichroic extinction [1]. Using a colorcolor diagram, reddened sources with little IR excess
were selected to trace the magnetic field structure of themolecular cloud. The mean polarization position angleof these sources is about 111°, which is interpreted as the
projected direction of the magnetic field in the observed
region of the cloud. The distribution of the polarization
angle has a dispersion of about 11°, which is smaller
than what was measured in previous studies. This small
dispersion gives a rough estimate of the strength of themagnetic field to be about 130 μG and suggests thatthe global magnetic field in this region is quite regularand straight. In contrast, the outflows driven by youngstellar objects in this region seem to have no preferred(Kyung Hee University)

NAGATA, Tetsuya

SATO, Shuji(Kyoto University)(Nagoya University)orientation. This discrepancy suggests that the magnetic
field in the L1641 molecular cloud does not dictate theorientation of the protostars forming inside[2].
HH
15
Number

		

10

4

1

2

1

7

5

0

7

6

1

0

7

1

0

5

0
0

30

60
90
120
Position Angle

150

010

I Scientific Highlights

0

Figure 2: Left: Histogram of polarization position angles for thegroup Ar sources in the H band (either background stars
or pre-main-sequence stars with little IR excess andwith substantial reddening in the L1641 cloud). The
peak angle is 111°, and the dispersion is 11°. Dot-dashedcurve: Gaussian fit. Right: Average polarization position
angle of group Ar sources in 2′ × 2′ subregions of theHH 1–2 field. The number of sources in each subregionis labeled.

References[1] Tamura, M., et al.: 2007, PASJ, 59, 467.
[2] Kwon, J., et al.: 2010, ApJ, 708, 758.

Figure 1: Finding chart of the HH 1–2 field (color-negative imageof Color composite Stokes I image in the J(blue),H(green), and Ks(red) bands from the IRSF/SIRPOL
observations). Detected point-like sources are labeled.
Bright stars and some extended sources are also labeled.

2

Stochastic Nature of Gravitational Waves from Supernova Explosions
with Standing Accretion Shock Instability
KOTAKE, Kei(NAOJ)

Traditionally, most of the model calculations ofgravitational waves (GWs) have focused on the bounce
signals in the context of rotational and magneotrotational
corecollapse (see collective references in [1]). However,most of them have been based on the two-dimensional(2D) simulations that assume axisymmetry. Then, thegrowth of standing accretion shock instability (SASI)[2] and the large-scale convection, both of which are
now considered to generically develop in the postbounce
phase and to help the neutrino-driven explosions, develop
along the symmetry axis preferentially, thus suppressing
the anisotropies in explosions.
These situations motivated us to study the properties
of GW based on the 3D simulations, which demonstrate
the neutrino-driven explosions aided by SASI [3]. Figure 1
shows the 3D hydrodynamical features of SASI fromthe early phase of the non-linear regime of SASI (topleft) until the shock break-out (bottom right) with thegravitational waveform from neutrinos inserted in eachpanel. After about 100 ms, the deformation of the standing
shock becomes remarkable marking the epoch when the
SASI enters the non-linear regime (top left of Figure 1).
At the same time, the gravitational amplitudes begin todeviate from zero. As seen from the top right throughbottom left to right panels of Figure 1, the major axisof the growth of SASI is shown to be not aligned withthe symmetric axis (:Z axis in the figure) and the flow
inside the standing shock wave is not symmetric withrespect to this major axis (see the first and third quadrantin Figure 1). This is a generic feature in the computed
3D models, which is in contrast to the axisymmetriccase. The GW amplitudes from SASI in 2D showed anincreasing trend with time due to the symmetry axis,
along which SASI can develop preferentially [2, 4].
Free from such a restriction, a variety of the waveforms
is shown to appear (see waveforms inserted in Fig.).
Such signals from a Galactic supernova are probably
within the detection limits of the LIGO-class detectors,
and seem surely visible to the next-generation detectors
such as the advanced LIGO and LCGT. This means thatthe successful detection of the GW signals will supply
us a powerful tool to probe the explosion mechanism.
Recently the next-generation detectors, by which theGWs studied here could be surely visible for a Galactic
source, are planned to be on line soon (2014!). It is anurgent task for theorists to make precise predictions of theGW signals based on more sophisticated 3D supernova
modeling.
We have also studied the equilibrium configurationsof magnetized neutron stars in the framework of generalrelativity.

Figure 1: Four snapshots of the entropy distributions of arepresentative 3D supernova explosion model. The
second and fourth quadrant of each panel shows thesurface of the standing shock wave. In the first andthird quadrant, the profiles of the high entropy bubbles(colored by red) inside the section cut by the ZX plane
are shown. The side length of each plot is 1000 km.
The insets show the gravitational waveforms fromanisotropic neutrino emissions, with ‘+’ on each curves
representing the time of the snapshot.

References[1] Kotake, K., Sato, K., Takahashi, K.: 2006, Reports of Progress
in Physics, 69, 971.
[2] Kotake, K., Ohnishi, N., Yamada, S.: 2007, ApJ, 655, 406.
[3] Kotake, K., Iwakami, W., Ohnishi, N., Yamada, S.: 2009, ApJL,
697, L133.
[4] Kotake, K., Iwakami, W., Ohnishi, N., Yamada, S.: 2009, ApJ,
704, 951.

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011

Centroid Experiment for 10−4 Pixel Order Determinationof the Positions of Stars
YANO, Taihei, ARAKI, Hiroshi, HANADA, Hideo, TAZAWA, Seiichi,
GOUDA, Naoteru, KOBAYASHI, Yukiyasu(NAOJ)YAMADA, Yoshiyuki(Kyoto University)

NIWA Yoshito(Kyoto University / NAOJ)

We have experimented with the determination of thepositions of star images on a detector with high precisionsuch as 10 microarcseconds, required by a spaceastrometry satellite, JASMINE. In order to accomplish
such a precision, we take the following two procedures.
(1) We determine the positions of star images on thedetector with the precision of about 0.01 pixel for one
measurement, using an algorithm for estimating themfrom photon weighted means of the star images. (2) We
determine the positions of star images with the precisionof about 0.0001–0.00001 pixel, which corresponds to thatof 10 microarcseconds, using a large amount of data over
10000 measurements, that is, the error of the positions
decreases according to the amount of data. Here, wenote that the procedure 2 is not accomplished when thesystematic error in our data is not excluded adequately
even if we use a large amount of data. We show the resultsin the laboratory experiment for precision of determining
the positions of star images. We obtain that the precisionof estimation of positions of star images on the detector
is under a variance of 0.01 pixel for one measurement(procedure 1). We also obtain that the precision of thepositions of star images becomes a variance of about
0.0001 pixel using about 10000 measurements (procedure
2).
1 Results of Experiment 1
We obtain that the variance of the estimated distancesof two stars is less than 0.01 pixel from several image
frames using the algorithm shown in [1].
2 Results of Experiment 2
We finally need to determine the positions of star
images with the precision of about 0.0001–0.00001 pixel,
which corresponds to that of 10 microarcseconds, usinga large amount of data over 10000 measurements, thatis, the error of the positions decreases according to theamount of data. The above procedure is not necessarily
accomplished when the systematic error in our data is
not excluded adequately even if we use a large amountof data. In our experiment, we ascertain that the errorof the positions of stars decreases according to theamount of data. The result is shown in the figure 1. The
abscissa indicates the number of images in deriving
the variance. The ordinate indicates the variance of the012

I Scientific Highlights

JASMINE Working Groupestimated distance of stars. As shown in the figure 1, thevariance decrease according to the slope of random error.
Therefore, we obtain that the precision of the positionsof star images becomes a variance of about 0.0001 pixel
using about 10000 measurements [2].

Figure 1: Variance against the number of images.

References[1] Yano, T., et al.: 2004, A&A, 116, 667.
[2] Yano, T., et al.: Proceedings of the Astronomical Data Analysis
Software and Systems(ADASS) XIX, Oct 4-8 2009, Sapporo,
Japan.

Achromatic deep nulling with a three-dimensional Sagnac interferometer		

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

TAVROV, Alexander(Space Research Institute)

NISHIKAWA, Jun, MURAKAMI, Naoshi, TAMURA, Motohide(NAOJ)

		

ABE, Lyu

TAKEDA, Mitsuo(Universite de Nice-Sophia Antipolis)(The University of Electro-Communications)

Not only for the detection but also the spectroscopic
characterization of faint extra-solar planets, bright stellar
light should be suppressed over a broad wavelength bandto carry out investigations.
A 3-D Sagnac interferometer, which we have alreadyproposed, introduces an achromatic nulling interferencewith geometrical π phase shift and a stable optical path
length because of its common path architecture [1]. So
far, to our knowledge the achromaticity of the practical
3-D Sagnac interferometer has never been evaluatedtheoretically. Here we show the achromaticity of the 3D Sagnac interferometer based on the Jones matrix andlaboratory experiments by using two laser lights (λ = 532
nm and 633 nm)[2].
Figure 1 shows the schematic of the 3-D Sagnac
interferometer. The anticlockwise and clockwise opticalpaths (1, PBS-BS-M1-M2-M3-M4-M5-M6-BS-PBS and2, PBS-BS-M6-M5-M4-M3-M2-M1-BS-PBS) in thenulled output rotate the electric field vectors ± 90 deg,
respectively.
Nulled Output
Bright Output
Input
BS
M1
PBS( 45 deg.)
M2

A nulling condition
can be obtained only
when X = Y, which corresponds to the azimuth angle θ= π/4. On this condition, the two output electric vectors
through the 3-D Sagnac interferometer have the same
amplitude and achromatic π-phase difference for arbitrary
input electric vector. This optical system can makeeffective nulling observations for linearly polarized light,
so that two Sagnac systems can take all of the unpolarizedstar light divided into two linear polarizations.
Four pictures shown in Fig. 3 are CCD images inconstructive and destructive conditions exposed by the
twowavelengths laser light. The pictures are normalized
by the peak value of the bright output, and the lower
graph is their mean radial intensity profiles. The
nulling contrasts of 4.16 × 106 (for 532 nm) and 1.17 ×
105 (for 633 nm) at the central position were obtained
simultaneously.
532nm(Bright) 532nm(Null)

671nm(Bright) 671nm(Null)

1e-2

M6
1e-8

M3

M4

532nm
Bright
671nm
BrightM5

Figure 1: Schematic of the 3-D Sagnac interferometer consistingof a polarized beam splitter (PBS), a beam splitter (BS),and six plane mirrors (M1-M6).

532nm
Null
671nm
Null

The transformed Jones matrices of the two opticalpaths can be calculated as(1)

Figure 2: (Upper) Interferometric images and (lower) intensity
profiles with the simulated one, assuming wavefront
errors of about λ/200 rms. Theoretical transmittance ofoffaxis light is also plotted.

(2)

References[1] Tavrov, A., et al.: 2005, Opt. Lett., 30, 2224.
[2] Yokochi, K., et al.: 2009, Opt. Lett., 34, 1985.

here

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013

Interstellar Extinction Law toward the Galactic Center:
J, H, KS bands, and 3.6, 4.5, 5.8, 8.0 μm
NISHIYAMA, Shogo, NAGATA, Tetsuya(Kyoto University)

				

TAMURA, Motohide

HATANO, Hirofumi(NAOJ) 				(Nagoya University)

KATO, Daisuke, TANABÉ, Toshihiko

The wavelength dependence of interstellar extinction
is not only important information to understand the natureof interstellar dust grains, but an essential ingredientin recovering the intrinsic properties of reddened
objects. The absolute value of interstellar extinction to
an individual star is difficult to determine, and so is its
wavelength dependence. Toward the Galactic center(GC), however, we can directly derive the wavelength
dependence of interstellar extinction, assuming onlythat the center of stellar distribution in the lines of sightis at the same distance from us and that the foregroundextinction is patchy. By plotting the apparent magnitude
versus the color excess of a group of stars, one obtains astraight line with the slope equal to the total to selective
extinction ratio, e.g., AKS / EH–KS.
We have determined the interstellar extinction law
toward the GC at the wavelength from 1.2 to 8.0 μm,
using point sources detected in the IRSF/SIRIUS nearinfrared survey and those in the Spitzer/IRAC/GLIMPSE
II catalog [1]. We made KS versus KS − λ color-magnitude
diagrams where λ = 3.6, 4.5, 5.8, and 8.0 μm. The KS
magnitudes of bulge red clump stars and the KS − λ colorsof red giant branches are used as a tracer of the reddening
vector in the color-magnitude diagrams. From thesemagnitudes and colors, we have obtained the ratios of
total to selective extinction AKS / EKS – λ for the four IRAC
bands. Combined with A λ / A KS for the J and H bands
derived by Nishiyama et al. (2006 [2]), we obtain AJ : AH
: AKS : A[3.6] : A[4.5] : A[5.8] : A[8.0] = 3.02 : 1.73 : 1 : 0.50 :0.39 : 0.36 : 0.43 for the line of sight toward the GC (Fig.
1). This confirms the flattening of the extinction curve at
λ > 3 μm from a simple extrapolation of the power-law
extinction at shorter wavelengths.

014

I Scientific Highlights

SUGITANI, Koji

(University of Tokyo) 		

(Nagoya City University)
3.0This work
Rieke & Lebofsky 1985
Lutz et al. 1999
Indebetouw et al. 2005

1.0

Aλ/ AKs

				

0.5

0.2
1

5

10

Wavelength[µm]Figure 1: Wavelength dependence of interstellar extinction Aλ /AKS toward the Galactic center. The ratios derived bythis study [1] (filled blue circles), Lutz (1999 [3], open
diamonds), and Rieke & Lebofsky (1985 [4], filledsquares) are represented. A simple power law, Aλ ∝ λ−1.75
is shown by the dashed line. Although it is not toward
the Galactic center, the extinction curve for diffuse
interstellar medium [5] is shown by thin red smooth line
for reference.

References[1] Nishiyama, S., et al.: 2009, ApJ, 696, 1407.
[2] Nishiyama, S., et al.: 2006, ApJ, 638, 839.
[3] Lutz, D.: 1999, in The Universe as Seen by ISO, ed. P. Cox & M.
F. Kessler (ESA SP-427; Noordwijk: ESA), 623.
[4] Rieke, G. H., Lebofsky, M. J.: 1985, ApJ, 288, 618.
[5] Indebetouw, R., et al.: 2005, ApJ, 619, 931.

Near-infrared Polarized Flares from Sgr A*
NISHIYAMA, Shogo, NAGATA, Tetsuya(Kyoto University)

TAMURA, Motohide, KUDO, Tomoyuki, ISHII, Miki

				
		

(NAOJ)				

SCHÖDEL, Rainer(Instituto de Astrofisica(IAA)-CSIC))

Although the theory of general relativity has passed
experimental tests in a weak gravitational field, it has notbeen well tested in a strong gravitational field. Testing thetheory in the strong field generated by collapsed objects
such as a neutron star and a black hole has been proposed
as a possible mean for such investigation.
Periodicity of ~20 min claimed in NIR monitoring
observations of Sgr A*, a supermassive black hole
(SMBH) at the center of our Galaxy, would place
the corresponding emission region at roughly three
Schwarzschild radii for a BH mass of 4 × 106 M [1]. If
this picture is correct, the NIR flares from Sgr A* should
be significantly influenced by general relativistic effects,
and thus are powerful tools that allows us to probe withina few gravitational radii of the event horizon.
Sgr A* was observed continuously for ~4 hours on
28 May 2008, using the near-infrared camera CIAO andAO36 on the Subaru telescope [2]. We detected threeflares (Fig. 1). The rise and decay timescales of ~6.5 minin the third flare are consistent with the light crossing
timescale for the inner part of the accretion disk, less than
10 Schwarzschild radii, around 4 × 106 M BH.
Clear variations in the degree and position angle ofpolarization were also detected. The first and second
flares consist of a weakly or non- polarized main flare anda highly polarized sub-flare. The degree of polarization
rises slowly up to ~20%, and decays sharply. The rises
occur after the bright flare phase, when flux of Sgr A* isdecaying. We found swings of the position angle of ~60º–
70º in the declining phase of the flares.
The correlation between the flux and the degreeof polarization suggests that the flare emission comesfrom hotspot(s) orbiting Sgr A*. In the hotspot model,
observed flares correspond to synchrotron emission
from a hot blob orbiting Sgr A* near its innermost
stable circular orbit. Recent calculation [3] show thatthe primary feature of the light curves from the orbiting
hotspot with a large orbital inclination angle i (close to
the edge-on view) is a narrow and higher peak followed
by a broad lower peak/bump. The first peak is formed
by a gravitational lensing effect which is strongest when
the hotspot is right behind the black hole. Doppler effectand beaming due to the relativistic motion of the hotspot
in the approaching regime make the second peak/bump.
The time evolutions of the degree of polarization show

HATANO, Hirofumi(Nagoya University)

ECKART, Andreas(Universit¨at zu Köln)

a doublepeak profile with a higher second peak than thefirst one, or a slow-rise and sharp-decay profile (with alower time resolution).
The similarities between the second flare we detected
and the calculations [3] suggest that the second flare
could be explained with a single orbital motion of a
hotspot. In the light curve of the second flare, we can see
the “first peak and second peak/bump” profile. It is clearlyseen that the degree of polarization increases in the decay
phase of the flare, and its profiles is asymmetric, showing
slow rise and sharp decay. These comparison with thecalculations gives a constraint to the inclination angle iof the orbit of the hotspot around Sgr A*, as 45º ≤ i < 90º(close to edge-on).
0.1"

0.1"

Figure 1: KS-band images of the central 1.3′′ × 1.3′′ region of our
Galaxy. The time from the beginning of the observation
is 145.1 (left) and 158.4 min (right). In each image, thelocation of Sgr A* is marked by a circle.

References[1] Genzel, R., et al.: 2003, Nature, 425, 934.
[2] Nishiyama, S., et al.: 2009, ApJL, 702, L56.
[3] Broderick, A. E., Loeb, A.: 2006, MNRAS, 367, 905.

I Scientific Highlights

015

A Necessary Condition for Individual Time-steps in SPH Simulations
SAITOH, Takyuki, MAKINO, Junichiro(NAOJ)

Individual time-step method is widely used insimulation of galaxy formation. This method allows
particles to have different time-steps, and integrates
these particles with their own time-steps. Almost all
implementation of individual time-steps used for particle
systems violates Newton’s third law. However, as long as
physical quantities are integrated with sufficient accuracy,
the violation is not so serious in simulations.
It is, however, not always possible to maintain theaccuracy. Since time-steps are usually evaluated at theend of previous time-steps, particles can not follow
an event during the time-step. Simulations involving
supernova explosions are one of such examples. Whensupernova explosion occurs, a little amount of very hot
gas generates in a compact region. The time-steps in theregion rapidly shrink about 1/1000 of the previous steps.
Therefore, hot gas particles step forward about 1000 steps
or more time-steps before neighboring cold gas particle
respond to the SN event, resulting in a large integration
error. In principle, we can avoid the integration error,
for instance, by adopting an implicit method [1], butthere are no implementations of such methods for SPH
simulations.
Here, we propose a simple limiter for hydrodynamical
time-steps in individual time-step method which solves
this problem [2]. We denote the time-step of an i-th
particle as dti and that of a neighbor particle, with index
j, as dtj . The basic idea of our limiter is to enforce thefollowing conditions:dti ≤ f dtj and dtj ≤ f dti,

I Scientific Highlights

Figure 1: The projected particle distributions in |z| < 0.01 (upperrow) and the density profiles (bottom row) at T = 0.02.
Left, middle and right columns show the evolutionof particles integrated with (a)global time-steps, (b)traditional individual time-steps, (c) individual timesteps with the limiter. Crosses indicate positions of theinitially heated particles. Solid lines are the analytic
solution of Sedov problem.

(1)

where f is an adjustable parameter. We found f = 4 to give
good results. By introducing this limiter, particles canfollow events which occur during the time-steps.
In order to verify the effect of the limiter, we
performed a Sedov problem [3]. We set that there is sixorders of magnitude in temperature between the hot
gas and cold, ambient gas. We performed three runs:(a) integrated with global time-steps, (b) traditional
individual timesteps, and (c) individual time-steps withthe limiter.
Figure 1 shows the results of the test. Run (a) shows aclear spherical structure and its density profile traces theanalytic solution very well. Run (b), however, displays
penetrations of the hot gas particles into the ambient
medium and fails to reproduce the analytic solution. Thisis because the time-steps of the ambient gas particles arequite long compared with those of the initially heatedparticles. Thus the ambient gas particles can not follow

016

the explosion. Run (c) does not show this problem, andthe result of Run (c) is very close to that of Run (a). Thisis because the short time-steps propagate to surrounding
particles quickly enough. As a result, cold gas particles
can respond to the pressure of the hot gas particles. Hence
we conclude that this limiter (or a similar criterion fortime-steps) is necessary for the simulations of SPH withindividual time-steps involving strong shocks.

References[1] Makino, J., Hut, P., Kaplan, M., Saygın, H.: 2006, New
Astronomy, 12, 124.
[2] Saitoh, T. R., Makino, J.: 2009, ApJL, 697, L99.
[3] Sedov, L. I.: 1959, Similarity and Dimensional Methods in
Mechanics New York: Academic Press.

Chemical composition of extremely metal-poor stars in a dwarf galaxy
AOKI, Wako, ARIMOTO, Nobuo

			(NAOJ)		

Dwarf galaxies in the local group have been
investigated from a variety of view points including theirroles in the Milky Way formation. Some of them, likethe Sagittarius dwarf galaxy, are currently interactingwith the Milky Way, indicating that the merging ofsuch galaxies should have played important roles in the
Galaxy formation. However, significant differences in thechemical nature are known between Milky Way halo anddwarf galaxies observed at present.
A remarkable difference is found in chemical
abundances of individual stars measured for nearby
dwarf galaxies based on high resolution spectroscopy.
Chemical abundance studies for several dwarf galaxies
in the past decade revealed that the abundance ratios
between α elements (e.g., Mg, Ca) and Fe are lower, ingeneral, in dwarf galaxy stars than in field stars. This
trend is clear particularly in relatively luminous, metalrich dwarf galaxies. Moreover, the metallicity distributionfunction of dwarf galaxies, which was estimated frommedium resolution spectroscopy, suggests a deficiency of
extremely metal-poor stars in dwarf galaxies [1].
We have started chemical abundance measurementsof extremely metal-poor stars in dwarf galaxies, whichhave not been well covered by previous work. Medium
resolution spectroscopy suggested that the Sextans dwarf
galaxy includes relatively large number of candidates ofextremely metal-poor stars. We applied high resolution
spectroscopy with the Subaru Telescope High Dispersion
Spectrograph (HDS) to six objects in Sextans [2].
We first confirmed the existence of extremely metalpoor stars in this galaxy. Since the calibration for the
metallicity estimate from medium resolution spectroscopy(using Ca triplet at ~8500 Å) is still insufficient atvery low metallicity ([Fe/H] < −2.5), high resolution
spectroscopy for Fe absorption lines is required. Our
measurements result in even lower metallicity than theestimates from medium-resolution spectroscopy.
The α elements in such extremely metal-poor stars
are expected to be over-abundant as found in the bulkof field halo stars. However, surprisingly, most of the
Sextans objects show low α/Fe ratios. Figure 1 depicts
the Mg/Fe ratio as an example. The Mg/Fe ratios ofmost objects are as low as the solar ratio, while only afew shows overabundance of Mg as in the field stars. A
similar result is also obtained for Ca abundance ratios.
Over-abundances of α elements are expected fromthe nucleosynthesis of usual core-collapse (type II)supernovae. The Sextans dwarf galaxy includes objects
that cannot be explained by the yields of usual type IIsupernovae alone.

SADAKANE, Kozo

(Osaka Kyoiku University)

DART team

One possible explanation is to include the contributions of type Ia supernovae, as the origins of ironin the Solar-System. However, because of the longer
time-scale of type Ia supernovae, large contributions ofthem are not expected at such low metallicity. Anotherpossibility is to assume that less massive stars, fromwhich only small amount of α elements provided throughsupernovae, are dominant among the progenitors of typeII supernovae in this galaxy.
Rapid progresses are recently found in chemical
abundance studies for dwarf galaxies that have similar
luminosity and metallicity to Sextans. These studies show
significant differences in the chemical abundance ratios
between galaxies, indicating that we need to investigate
the formation and evolution of individual galaxies.
Studies of ultra-faint dwarf galaxies recently discovered
might be particularly important as more primitive objects.

Figure 1: [Mg/Fe] as a function of metallicity for Sextans stars(filled circles: our study; diamonds: previous studies)and field stars (smaller symbols from literature). Thisgalaxy includes extremely metal-poor stars that havequite low α elements.

References[1] Helmi, A., et al.: 2006, ApJ, 651, L121.
[2] Aoki, W., et al.: 2009, A&A, 502, 569.

I Scientific Highlights017

Performance Evaluation of Nano-JASMINEHATSUTORI, Yoichi, KOBAYASHI, Yukiyasu, GOUDA, Naoteru, YANO, Taihei(NAOJ)

		

YAMADA, Yoshiyuki(Kyoto University)

NIWA, Yoshito(NAOJ / Kyoto University)

Nano-JASMINE is mounted a 5 cm effective diametertelescope and aims to measure positions and motions ofstars with the accuracy of a few milli-arcseconds in z–band(λ ~ 0.8 µm). The satellite weighs about 35 kg andit is developed by National Astronomical Observatoryof Japan, Kyoto University and University of Tokyo.
Nano-JASMINE will be launched at August 2011 from
Alcantara Launch Center at Brazil by Cyclon-4 rocket.
JASMINE Project Office contributes to develop a smallreflecting telescope and a driver circuit for a CCD
detector. In 2009, we developed and evaluated these
instruments [1]. This paper reports the results of theperformance evaluation.
First, the small reflecting telescope was made ofaluminum alloy because of the suppression of effects ofstrain induced by thermal changes. The reflecting surfaces
were polished with a single-crystal diamond cutting tools
and deposited with Cr and Au vapor. Developed telescope
weighs 1.7 kg and occupies a volume of only 17x12x12
cm. The telscope will be operated below 220 K on orbit.
The thermal vacuum test was conducted to evaluate
the performance at orbital condition. The telescope
was cooled down by LN2 and the wavefront errors ofdeveloped telescope were measured by an interferometer.
As a result, the RSS wavefront error is λ/14(λ = 800 nm).
Therefore, it is confirmed that developed telescope canachieve a diffraction-limitted performance. Moreover,numerical analysis was conducted to calculate therelatonship between the thermal change and thedeformation of telescope. Fig. 1 shows the result of thenumerical analysis.
Second, the radiation test of a CCD detector was
conducted to evaluate the performance degradation.
Gamma ray and proton were irradiated. As a result, it
was confirmed that although noise will be increased andCharge Transfer Efficiency(CTE) will be degraded, theseeffects can be corrected in analysis.
Finally, the engineering model of Nano-JASMINE
was assembled. Fig. 2 shows the outlook of the satellite.
Using this engineering model, comprehensive tests wereconducted to analyse the total noise of observations.
Moreover, the Critical Design Review(CDR) wasconvened to judge the satellite design. As a result, we
obtained the consensus for the flight model of NanoJASMINE. In 2010, the flight model of Nano-JASMINE
is to be developed018

I Scientific Highlights

MUROOKA, Jumpei(University of Tokyo)

Figure 1: Numerical Result of thermal analysis. The change in therelative angle is required to be below 1mas(p-v). It is
confirmed that the result satisfies the requirement.

Figure 2: Enginnering Model of Nano-JASMINE. Telescope
and CCD are equipped inside the satellite. A series of
performance evaluation are conducted.

Reference[1] Hatsutori, Y., et al.: 2009, Trans. JSASS Space Tech. Japan, 7,
Tm19-Tm23.

The Relation between the Magnetic Fields and the Coronal Activities
in the Polar Coronal HoleSHIMOJO, Masumi, TSUNETA, Saku
(NAOJ)

References[1] Shimojo, M., Tsuneta, S.: 2009, ApJ, 706, L145.
[2] Tsuneta, S.: 2008, ApJ, 688, 1374.

1000 SOT-SP Fe I Stokes-Q 10-Sep-2007 17:00 - 21:26UTY (arcsecs)

Transverse Magnetic Field (White: East/West, Black: North/South)
Saturates at the degree of polarization 0.2%

950

900

850
SOT-FG Na I Stokes-V 10-Sep-2007 21:01:19UT

Y (arcsecs)

Line-of-sight Magnetic Field
Saturates at the degree of polarizaton 1%

950

900

850

Y (arcsecs)

XRT Al_poly 10-Sep-2007 21:00:46UT

950

900

850
EIT 195A 10-Sep-2007 21:12:42UT

Y (arcsecs)

We obtain the spatial relation between the polar
magnetic fields and the polar coronal activities/structureswith careful co-alignment among the Stokes maps ofthe lower atmosphere, the X-ray images and the EUV
images. These images are taken with Hinode and SOHO.
We found that the coronal structures and activities appear
when the relatively large magnetic concentrations withminority polarity appear near the KG-patches, and we
also verified that the increases of the minority signalsthat associated with the polar X-ray jets in the Na I
Stokes-V indicate the emerging flux regions. Since therelation between the coronal structures and the magnetic
concentrations with minority polarity can be easily foundfrom other dataset of the polar region, the relation is very
rigid. The result suggests that the coronal structures andactivities in the polar coronal hole are produced by theinteractions of the kG-patches with the emerging minority
polarities near the kG-patches [1].
We show that the emerging flux appears even in thepolar region. It may not be conceivable that the magnetic
flux located in the middle latitude of the convection
zone emerges at the polar region. The emerging flux inthe polar region may be generated by the local dynamo
process due to the granular/super-granular motion.
We discuss the relation between the kG-patches, theXray jets and the fast solar wind. The kG-patches provide
all the open magnetic fields that serves as the channels of
the fast solar wind [2]. If the X-ray jets provide the energy
for the acceleration of the fast solar wind, the X-ray
jets have to occur at around almost all the kG-patches.
However, most of the kG-patches are not associated with
the X-ray jets. Thus, it is unlikely that the polar X-ray jets
provide sufficient energy for the acceleration of the fastsolar wind. The energy may be provided

950

900

850
-50

0

50
X (arcsecs)

100

150

Figure 1: The north pole images around 21:00 UT on September
10, 2007. The yellow dash circles indicate the relatively
large minority poles identified in the Na I Stokes-V map.
The green and the red lines in the lower panels are thecontours of the degree of the polarization (1 %) of the Fe
I Stokes-Q map.

I Scientific Highlights

019

Sensitivity improvement of CLIO with cooling the mirrors
TAKAHASHI, Ryutaro, ARAI, Koji, TATSUMI, Daisuke, OHISHI, Naoko
KAWAMURA, Seiji, FUJIMOTO, Masa-Katsu(NAOJ)MIYOKI, Shinji, UCHIYAMA, Takashi, MIYAKAWA, Osamu, AGATSUMA, Kazuhiro
SAITIO, Takanori, OHASHI, Masatake, KURODA, Kazuaki, NAKATANI, Ichirou(Institute of Cosmic Ray Research, University of Tokyo)

TOMARU, Takayuki, SUZUKI, Toshikazu, YAMAMOTO, Akira(High Energy Accelerator Research Organization)

ASO, Yoichi

I Scientific Highlights(Nihon University)

improve the sensitivity further, we continue to upgrade
the detector.
     
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CLIO (Cryogenic Laser Interferometer Observatory)
is the first cryogenic interferometric gravitational wave
detector in the world. It has 100 meters baseline lengthand is located in an underground mine at Kamioka. It isa prototype interferometer for the future LCGT project
as well as TAMA300 detector in Mitaka campus. It has
the purpose to demonstrate advantages of the cryogenic
interferometer and the Kamioka mine as a quiet site.
The detector construction started in 2002. The vacuum
and the cryogenic systems were prepared by 2005. Afterthe installation of the interferometer optics and thesuspension systems, the interferometer operation withcooling mirrors were demonstrated in 2006. Due to thenoise investigations and reductions in room temperature[1], we concluded that the noise level is enough close
to the fundamental limit at room temperature andthe cooling of the mirrors is necessary for further
noise investigations. It was one of the most importantmilestones in gravitational wave detector developments.
At the beginning of 2009, we made a decision thatsensitivity improvement of CLIO by cooling the mirrors
is the highest priority issue. In this cooling experiment
only two mirrors were cooled among four mirrors ofwhich consist of the main interferometer, because weshould get rid of various problems associated with thecooling. In fact, hundreds of hours are spent to address
technical issues such as variation of eddy current
damping, variation of coil impedance and reduction of
scattered lights at the radiation shield.
In March of 2010, we succeed to exceed the fundamental limit at room temperature by cooling the mirrors
in a frequency region between 120 and 200 Hz. Figure
1 shows a displacement noise spectrum of CLIO (red)together with the limited sensitivity at room temperature(black). Both purple and aqua dashed lines are mirror
thermal noise spectrum without and with two mirrors
cooling, respectively. The current noise spectrum islimited by (1) shot noise and RF intensity noise above
500 Hz, (2) seismic originated noises below 40 Hz and(3) thermal noise of the suspension and various underinvestigating noises such as coil actuator noise. To

020

SHINTOMI, Takakazu(University of Tokyo)TELADA, Souichi(Advanced Industrial Science and Technology)





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Figure 1: Displacement sensitivity of CLIO (red) and limiting
sensitivity at room temperature (black). The current
noise spectrum is limited by (1) shot noise and RF
intensity noise above 500 Hz, (2) seismic originatednoises below 40 Hz and (3) thermal noise of thesuspension and various under investigating noises suchas coil actuator noise.

References[1] Agatsuma, K., et al.: 2010, Phys. Rev. Lett, 104, 040602.
[2] Miyoki, S., et al.: 2010, J. Phys. Conf. Ser, 203, 012075.

Prominence formation associated with an emerging helical flux rope
OKAMOTO, Takenori J., TSUNETA, Saku, KATSUKAWA, Yukio
ICHIMOTO, Kiyoshi, SUEMATSU, Yoshinori(NAOJ)SHIMIZU, Toshifumi(ISAS / JAXA)		

YOKOYAMA, Takaaki

NAGATA, Shin’ichi, SHIBATA, Kazunari(University of Tokyo)			

(Kyoto University)

KUBO, Masahito, LITES, Bruce W.
(HAO / NCAR)TARBELL, Theodore D., SHINE, Richard A., BERGER, Thomas E., TITLE, Alan M.
(LMSAL)

Prominences are relatively cool objects embedded in
the hotter corona. Although it is known that prominences
are supported by coronal magnetic fields against gravity,
the structure and formation process of magnetic fields inand around a prominence remains unclear.
A recent study of a series of vector magnetograms
obtained by the Spectro-Polarimeter (SP) of the HinodeSolar Optical Telescope (SOT) was interpreted as the
emergence of a helical flux rope under a prominence inan active region [1]. This is the first observational study
to detail the evolution of the photospheric magnetic fieldsuggesting the emergence of a helical flux rope that may
be associated with the formation and maintenance processof an active region prominence. Here, we report the moredetailed features of the emerging helical flux rope and therelationship between the flux rope and the prominence.
The results are listed below [2].
(1) We can see a similar phenomenon in Ca H-line
filtergrams, which is indicated as the emergence of thehelical flux rope. However, using only the filtergraphobservations, we cannot determine the existence of a flux
emergence with confidence. Observations comprising
only line-of-sight magnetograms suffer from the same
limitation. Observations of vector magnetic fields arenecessary to detect a possible flux rope emergence.
(2) We take a closer look at the interaction between
the emerging flux rope and granular convection. The
horizontal magnetic fields are roughly independent of the
granular patterns, but we can find some local modulations
caused by granules (see figure). This result is useful forsolving 180-degree ambiguity of azimuth of magnetic
fields.
(3) We examine the relationship of magnetic fields
to photospheric motions. No shear motion or converging
flows are detected, but we find diverging flows such as
mesogranules along the polarity inversion line under
the prominence. The presence of mesogranules may berelated to the emergence of the helical flux rope.
(4) The emerging helical flux rope reconnectswith magnetic fields of the pre-existing prominence tostabilize the prominence for the next several days. We
thus conjecture that prominence coronal magnetic fields

emerge in the form of helical flux ropes that contribute to
the formation and maintenance of the prominence.

Figure 1: Close-up maps of the helical emerging flux region. (a)Continuum intensity map. White lines indicate brightcontours of granules. (b) Inclination map of magnetic
fields. Red indicates positive polarity (toward us) andblue indicates negative polarity (away from us) in thelocal frame. The color table saturates at ±10º withrespect to the solar surface.
References[1] Okamoto, T. J., et al.: 2008, ApJ, 673, L215.
[2] Okamoto, T. J., et al.: 2009, ApJ, 697, 913.

I Scientific Highlights

021

Substellar Objects in Nearby Young Clusters (SONYC):
The Bottom of the Initial Mass Function in NGC 1333
SCHOLZ, A.

(University of St. Andrews)

GEERS, V., JAYAWARDHANA, R., FISSEL, L., LEE, L., LAFRENIERE, D.
(University of Torontoa)

TAMURA, Motohide(NAOJ)The origin of the stellar initial mass function (IMF)
is one of the major issues in astrophysics. The lowestmass end of the IMF, in particular, has been the subjectof numerous studies in star forming regions over the past
decade [1, 2].
SONYC - Substellar Objects in Nearby Young
Clusters - is a survey program to investigate the frequency
and properties of substellar objects with masses down toa few times that of Jupiter in nearby star-forming regions.
We present the first results from SONYC observationsof NGC 1333, a ~1 Myr old cluster in the Perseus
starforming complex [3]. We have carried out extremely
deep optical and near-infrared imaging in four bands (i,z, J, K) using Subaru Prime Focus Camera and MultiObject InfraRed Camera and Spectrograph (MOIRCS)
instruments at the Subaru telescope. The survey covers
0.25 square degrees and reaches completeness limitsof 24.7 mag in the i band and 20.8 mag in the J band.
We select 196 candidates with colors as expected foryoung, very low-mass objects. Follow-up multi-object
spectroscopy with MOIRCS is presented for 53 objects.
We confirm 19 objects as likely brown dwarfs (BDs)in NGC 1333, seven of them previously known. Nine
additional objects are classified as possible stellar cluster
members, likely with early to mid-M spectral types.
The confirmed objects are strongly clustered aroundthe peak in the gas distribution and the core of the clusterof known stellar members. For 11 of them, we confirm
the presence of disks based on Spitzer/Infrared Array
Camera photometry.
The effective temperatures for the BD sample range
from 2500 K to 3000 K, which translates to masses of~0.015 – 0.1 M , based on model evolutionary tracks.
For comparison, the completeness limit of our survey
translates to mass limits of 0.004 M for Av ≤ 5 mag or
0.008 M or Av ≤ 10 mag.
Compared with other star-forming regions, NGC
1333 shows an overabundance of BDs relative to lowmass stars, by a factor of 2-5. On the other hand, NGC
1333 has a deficit of planetary-mass objects: based on
the surveys in σ Orionis, the Orion Nebula Cluster andChamaeleon I, the expected number of planetary-mass
objects in NGC 1333 is 8-10, but we find none (seeFig. 1). It is plausible that our survey has detected the022

I Scientific Highlights

minimum mass limit for star formation in this particularcluster, at around 0.012 – 0.02 M . If confirmed, ourfindings point to significant regional/environmental
differences in the number of BDs and the minimum massof the initial mass function.

Figure 1: Mass distribution of BDs in NGC 1333 (hatchedhistogram) and the deficit of planetary-mass objects. The
three labeled data points show the predicted number ofplanemos in NGC 1333 based on the surveys in σ Ori,
the ONC, and in ChaI. The non-detection of planetarymass objects points to a deficit of objects in this massregime compared with other clusters. The dotted lines
refer to our detection limit for Av = 5 and 10 mag.

References[1] Tamura, M., et al.: 1998, Science, 282, 1095.
[2] Lucas, P. W., Roche, P. F.: 2000, MNRAS, 314, 858.
[3] Scholz, A., et al.: 2009, ApJ, 702, 805.

Constructing a Theoretical Model for High-z Lyman α Emitters
		

KOBAYASHI, Masakazu A.R.
(NAOJ)		

TOTANI, Tomonori(Kyoto University)

We have constructed a new theoretical modelfor high-z Lyα emitters (LAEs) in the framework ofhierarchical galaxy formation, which is based on one of
the latest semi-analytic model for galaxy formation. It
is unique one in the theoretical model for LAEs because
the two following physical effects are incorporated in
calculating the escape probability of Lyα photons fromtheir host galaxy: extinction by interstellar dust, which
is not necessarily the same for that of continuum, andgalaxy-scale outflows induced as supernova feedback.
Our previous study has confirmed the model reproduces
the observational Lyα luminosity functions (LFs) of theLAEs at z ~ 3–6 [1].
We performed a further comparison of the modelwith the other available observations for the LAEs,
i.e., the rest-frame ultraviolet (UV) continuum LFs,
the distribution of Lyα equivalent width (EW), andthe distribution in UV continuum luminosity vs. EW
plane. The model parameters were kept unchanged fromour previous study; there is no more free parameters
adjustable to fit the observations. We paid carefulattention to the selection conditions of the model LAEs
(i.e., the threshold Lyα line luminosity and EW: L thLyα
thand EWLyα) and applied the same conditions with thoseadopted in each observation.
As shown in Figs. 1 and 2, our model nicely
reproduced all of the available observations of the LAEs
at z ~ 3–6.
It should be emphasized that the number fractions of
the LAEs with EW > 240 Å were naturally reproduced,
without introducing PopIII stars nor top-heavy IMF. We
showed that both the stallar population (young age andlow metallicity) and the selective extinction to continuum
by clumpy dust geometry are the keys to reproducing
large EW LAEs. Our model predicts a positive correlation
between EW and extinction. The observed trend thatbrighter LAEs in UV continuum tend to have smaller
mean EW is also reproduced, and the clumpy dust plays
an important role again for this trend [2].
Our model would be helpful in planning an LAE
survey at even higher redshifts and interpreting suchdata sets in future studies. The numerical data on thesequantities of LAEs are available on request to the authors

NAGASHIMA, Masahiro(Nagasaki University)

Figure 1: Rest-frame UV continuum LFs for LAEs at z = 3–6.
The curves are the model predictions, while the solid
symbols with error bars are the observed data of theLAEs at various redshifts. The numerical quantities of
th
th
LLyα
(in the unit of ergs/s/h−2) and EWLyα
are shown ineach panel.

Figure 2: Rest-frame EW distribution for LAEs at z = 3–6. The
curves are the model predictions, while the histogramswith error bars are the observations. Arrows represent
the 1σ upper limits of the Poissonian statistics for small
sample number.

References[1] Kobayashi, M. A. R., Totani, T., Nagashima, M.: 2007, ApJ,
670, 919.
[2] Kobayashi, M. A. R., Totani, T., Nagashima, M.: 2010, ApJ,
708, 1119.

I Scientific Highlights

023

A Cluster of Starburst Galaxies 11.5 Billion Light-years Away
TAMURA, Yoichi , KAWABE, Ryohei, NAKANISHI, Kouichiro, HATSUKADE, Bunyo(NAOJ)

KOHNO, Kotaro(University of Tokyo)

In 2009, the Atacama Submillimeter Telescope
Experiment (ASTE) reported a discovery of a dozen ofsubmillimeter-selected galaxies (SMGs) that clusters
towards a protocluster at redshift z = 3.1 (11.5 billion
light-years away) [1]. In this report, we are highlighting
one of the most significant results from our large
campaign of SMG survey.
The concordance standard theory of galaxy formation
is successfully accounted for introducing the idea inwhich large galaxies are constructed through merger
and accretion of small building blocks of galaxies. The
problem is that this idea requires a special condition orenvironments in which formation of massive galaxies
preferentially occurs.
One of the key clue breaking the problem is to takea large submillimeter-wavelength image which covers
the sky several 10 Mpc across. One of the reasons is that
submm-selected galaxies are now believed to be huge
starburst galaxies at high-z and progenitors of presentday
massive ellipticals. The other is that large-scale distribution of galaxies (baryons) has a typical spacial scaleof ~10 Mpc.
The advantage of AzTEC/ASTE is a survey speed
which is 20 times higher than the SCUBA camera,
allowing us to investigate the environment in which
SMGs are formed. Figure 1 shows the 1.1-mm image
taken with ASTE. The target is the SSA22 field, a partof the sky having a proto-cluster of galaxies — Subaru
has discovered a hundred of Lyα-emitting galaxies at z
= 3.1 in this field, which are thought to be young small
galaxies.
Our ASTE observations reveal (1) a spacial correlation
between the positions of SMGs and Lyα galaxies (Fig.
2), and (2) that averaged mass of Lyα emitters is muchsmaller (< 1%) than that of a typical SMG, suggestingthat the two populations of galaxies reside in the same
volume of the protocluster although they exhibit different
properties in their dust content.
These results provide evidence for the preferential
formation of SMGs in a high-density environment[1]. The current standard model of galaxy-formation
predicts previrialized dark matter halos with 10 14M — protoclusters — in the early Universe at z ≥ 2. Insuch environments, a lot of small galaxies can merge toform massive galaxies with intense starburst activities.
This picture predicts that clustering strength (a degreeof nonuniformity of spacial distribution) of the SMG
population is higher than coeval normal galaxies, and024

I Scientific Highlights

the AzTEC/ASTE teamthat SMGs are selectively (preferentially) located in
the cosmic largescale structure at high-z. This selective
distribution (i.e., clustering) of SMGs are actuallyobserved as the positive signals in the spacial crosscorrelation between SMGs and Lyα emitters (Fig. 2)

0.4°

Figure 1: (left)The AzTEC/ASTE 1.1-mm image towards the
SSA22 protocluster. The field of view is 0.4 degree
across, roughly corresponding to the diameter of thefull Moon. The open circles indicate the positions of 30
submillimeter galaxies detected with AzTEC/ASTE.
(right) A false color closeup image near the core of
the SSA22 protocluster (red: the AzTEC/ASTE 1.1
mm image, green: Spitzer/IRAC 3.6-μm image, blue:
Hubble/ACS i-band image.

1
CCF (bright SMG-LAE)
Angular cross-correlation function

			

0.8

ACF (LAE-LAE)

0.6
0.4
0.2
0
-0.2
0

2

4

6

8

10

12

14

16

Angular distance (arcmin)

Figure 2: Two point angular cross-correlation function between
the positions of AzTEC sources and Lyα emitters (circles)
and auto-correlation function of Lyα emitters (squares).

Reference[1] Tamura, Y., et al.: 2009, Nature, 459, 61–63.

Fiber-link between Okayama 1.88-m reflector and HIDES				KAMBE, Eiji

YOSHIDA, Michitoshi(NAOJ)		

(Hiroshima University NAOJ)IZUMIURA, Hideyuki, KOYANO, Hisashi, SHIMIZU, Yasuhiro, NAGAYAMA, Shogo
OKITA, Ki’ichi, SAKAMOTO, Akihiro, OKADA, Norio(NAOJ)

		

SATO, Bun’ei(Tokyo Institute of Technology)		

In December 2009, we successfully had the scientificfirst-light of our new fiber-link system between OAO
1.88-m reflector and the HIgh Dispersion Echelle
Spectrograph (HIDES). Here we report purposes of the
project, designs of the fiber-link, and some preliminary
results of our commissioning-phase observations.
The HIDES has been the most frequently used
openuse instrument at Okayama since its installation in
1999. But recently it became less attractive because of
its rather low throughput (typically, 2 % or less) and notsohigh radial velocity (rv) measurement precision (severalms−1). There is in fact growing need for developing new
fiber-fed and more stable spectrographs in near future.
Naturally, we started the fiber-link project in 2007 as thefirst step toward such goals.
The optical design of the fiber-link is as follows;
stellar light within 2″.7 FOV is collected into the opticalfiber at the Cassegrain focus of the telescope (typicalseeing size at OAO is 1″.4); the light is guided to its coude
focus through a 11-m length fiber; and then, the output
image, sliced into three by an image slicer, is injected
into the HIDES (Figure 1). With this design, we expect
to improve its throughput by about one magnitude, while
maintaining good wavelength resolution (R=52,000).
We also pursuit for rv measurement precision with theiodine cell technique. Once completed, the fiber-link will
improve the efficiency of various observations, including
the on-going planet search projects in which we will beable to monitor several times as many targets as before.
In October 2009, we installed the complete system
to the telescope, and checked its basic performance suchas the echelle format of sliced image and the wavelength
resolution (Figure 2). Then, in December 2009, we had
its scientific first-light and confirmed that its throughput
was better than that of previous observations.
In Figure 3 we compare the photon count statistics
between two observations (blue dash line: slit mode, redsolid line: fiber mode), in both of which we monitored thesame star over a week. It is clearly seen that the typicalthroughput is already doubled. We also confirmed that the
short-term rv measurement precision is much better than
2 ms−1 in this fiber-mode observation.
We currently make further adjustments/improvementsof the system toward its open-use in early 2011.

YAMAMURO, Tomoyasu(Optcraft)

Figure 1: Optical drawings at the output of the fiber (left), image
slicer (top-right), and the sliced stellar image (bottomright).

Figure 2: Spectra of Th-Ar (left) and of Procyon (right).

Figure 3: Comparison of the photon count statistics between slit
mode and fiber mode observations. See text in detail.
(courtesy to Prof. Hiroyasu Ando).

I Scientific Highlights

025

Observations of transient objects using OAO/ISLEIMADA, Akira, YANAGISAWA, Kenshi, KURODA, Daisuke(OAO / NAOJ)

YAMANAKA, Masayuki, KAWABATA Koji, YOSHIDA Michitoshi(Hiroshima University)

KINUGASA, Kenzo

TANAKA, Masaomi

KATO, Taichi

OMODATA, Toshihiro(Gunma Observatory)(Kyoto University)(Kagoshima University)

Here we report on observations of transient objects
using OAO/ISLE [1] in 2009.
First, we succeeded in obtaining multiband light
curves of a type Ia supernova SN 2009dc. The supernova
was discovered on 2009 April 9 near the outer edge of
UGC 10064. On 2009 April 26, the maximum magnitude
reached B = 15.2. Extensive observations were performed
by Hiroshima Univ., Tokyo Univ., OAO/NAOJ, andmany other institutes in Japan. As a result, the absolute V
magnitude was estimated to be MV = −20.19 ± 0.19 basedon the known distance to the host galaxy. Assuming thatthe host extinction of AV = 0.29, we estimated the ejected
56
Ni mass of 1.6 ± 0.4 M[2]. These results raise a newquestion about the maximum mass of white dwarf. Nearinfrared observations using ISLE revealed that MJ = −19.20 ± 0.16 mag, MH = −19.00 ± 0.17 mag, and MKs =−19.19 ± 0.17 mag. This suggests that SN 2009dc was
exceptionally luminous even in near infrared range.
ISLE also detected an afterglow of GRB 090423,
which holds the highest record of redshift among GRBs (z= 8.2). Detailed discussion is given by YOSHIDA, M.
Dwarf novae are one of the main targets for
ISLE. We performed quiescent photometry of SDSS
J080434.20+510349.2 and derived J = 17.29(0.05), H= 16.97(0.05), and Ks = 16.41(0.06). This suggests that
J0804 has a brown dwarf-like secondary [3]. Quiescentphotometry under high S/N was also performed for SU
UMa-type dwarf novae, 1RXS J053234+624755 andNSV 4838 [4, 5]. In future, high precision photometry innear infrared range will shed light on understanding theperiod minimum problem1 in dwarf novae.

*1 There are big differences between theory and observation with respect to theorbital period minimum (Pmin) of dwarf novae. Theory suggests Pmin = 65 min, whileobservation shows Pmin = 75 min. Futher, theory suggests than more than 70 % of dwarf
novae should exist around Pmin. However, observation shows that about 80 % of dwarf
novae are off the period minimum.

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MAEDA, Keiichi, NOMOTO, Ken’ichi(Tokyo University)				

(IPMU)

KAWAI, Nobuyuki(Tokyo Institute of Technology)

et al.

Figure 1: Light curves of SN 2009dc. compared with a superChandrasekhar SNe Ia 2006gz and 2003fg, anoverluminous SN Ia 1991T, and a normal SN 2005ef.
The magnitudes were arbitrarily shifted for display
purpose.

References[1] Yanagisawa, K., et al.: 2006, SPIE, 226, 1421.
[2] Yamanaka, M., et al.: 2009, ApJ, 707L, 118.
[3] Kato, T., et al.: 2009, PASJ, 61, 601.
[4] Imada, A., et al.: 2009, PASJ, 61, 535.
[5] Imada, A., et al.: 2009, PASJ, 61L, 47.

Effect of Long-lived Strongly Interacting Particles
on Big Bang Nucleosynthesis						

KUSAKABE, Motohiko(University of Tokyo)

YOSHIDA, Takashi(University of Tokyo)		

Some particle models beyond the standard one include
long-lived heavy colored particles [1] which are scientifictargets of the Large Hadron Collider experiment. Ifsuch particle exists in the early universe, it would be
confined in exotic hadrons, i.e., X, at T < 180 MeV. If
the strongly interacting X particle exists in the epoch of
Big Bang nucleosynthesis (BBN), it binds to nuclei andmakes exotic nuclei. We then study a new BBN scenario
including long-lived strongly interacting particles X.
The mass of X is assumed to be much larger than thatof nucleon, i.e., O(1 GeV). The strength of interaction
between an X and nuclei is supposed to be similar to thatbetween a nucleon and the nuclei. We estimate binding
energies between an X and nuclides and thermonuclear
reaction rates and β-decay rates of X-bound nuclei (i.e.,
AX or X-nuclei) using available cross sections for normal
nuclei. We integrated rate equations including terms forradiative captures of X by normal nuclides and nuclear
reactions of X-nuclei. Parameters are the life time τX andthe abundance ratio of X to baryon YX ≡ nX/nb.
Figure 1 shows a result of BBN calculation in which
the abundance and the life time of X are YX = 10−8 and τX= ∞. When the temperature decreases to T9 ≡ T/(109 K) ~ 5,
X particles capture nucleons. At T9 ~ 1, the d abundance
increases, and consecutive nonradiative d-captures lead tothe production of heavy X-nuclei.
Strongly interacting particles have a greater impact
on BBN [2] than leptonic particles [3] for the following
reasons. 1) Both of binding energies between an X andnuclides, and cross sections of nucleon captures by X arelarge, so that an early and rapid formation of bound states
is possible. 2) 5He and 5Li which are unstable to particle
emissions can be stabilized when bound to Xs, so thatheavy X-nuclides can form through the states.
Figure 2 shows the contours of calculated abundancesin the (τX, YX) plane. In this scenario 9Be and B can beproduced in amounts more than in standard BBN. Future
observations of Be [4] and B abundances in metalpoor
stars may show primordial plateaus. In addition, thepredicted isotopic ratio 10B/11B is very high. A solution to
the 6,7Li problems [5, 6] was not found. A constraint on
the life time, i.e., τX < 200 s is derived using an estimationof relic abundance of X : YX ~ 10−8 [1].

KAJINO, Toshitaka(NAOJ / University of Tokyo)

MATHEWS, Grant J.

(University of Notre Dame)

Figure 1: Abundances of normal (a) and X-nuclides (b) as afunction of temperature T9. The parameters are set to be
YX = 10.8 and τX = ∞. This figure is reprinted from [2].

Figure 2: Contours of adopted observational constraints on
primordial abundances. Upper right regions surroundedby the contours are excluded. This figure is reprinted
from [2].
References[1] Kang, J., et al.: 2008, JHEP, 09, 086.
[2] Kusakabe, M., et al.: 2009, PRD, 80, 103501.
[3] Kusakabe, M., et al.: 2010, PRD, 81, 083521.
[4] Ito, H., et al.: 2009, ApJ, 698, L37.
[5] Perez, A. E. G., et al.: 2009, A&A, 504, 213.
[6] Aoki, W., et al.: 2009, ApJ, 698, 1803.

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Subaru/COMICS Mid-Infrared Observation of the Near-Nucleus Regionof Comet 17P/Holmes at the Early Phase of an Outburst
		

WATANABE, Jun-Ichi

HONDA, Mitsuhiko

ISHIGURO, Masateru

OOTSUBO, Takafumi

SARUGAKU, Yuki

KADONO, Toshihiko(NAOJ)		(Kanagawa University)		

(ISAS/JAXA)		

(University of Tokyo)		

SAKON, Itsuki(NAOJ)(Osaka University)

FUSE, Tetsuharu, TAKATO, Naruhisa, FURUSHO, Reiko(University of Tokyo) 			

(NAOJ)

Magnitude

A Mid-infrared imaging and spectroscopic
observations of comet 17P/Holmes in the early phase of
its outburst in brightness were performed on 2007 October
25–28 UT using the Cooled Mid-Infrared Camera andSpectrometer (COMICS) on the 8.2-m Subaru Telescope.
We detected an isolated dust cloud that moved toward thesouth-west direction from the nucleus at 8.7 ± 0.3 (″/day)(fig. 1). The 11.2 µm peak of a crystalline silicate feature
onto a broad amorphous silicate feature was detectedboth in the central condensation of the nucleus and theisolated dust cloud. The color temperature of the cloudis estimated to be ~200 K. Our analysis of the motion
indicates the isolated cloud moved anti-sunward (fig. 2).
We propose several possibilities for the motion of thecloud; fluffy dust particles in the isolated cloud started
to depart from the nucleus by radiation pressure almost
as soon as the main outburst occurred, or dust particles
moved by some other forces such as rocket effect andphotophoresis when the surrounding dust coma became
optically thin.
0
5
10

Separation (arcsec.)

40

observed peak position
constant acceleration model
constant velocity model

30
20
10
0

23

24

25

26

27

28

29

30

Date (2007 October )Figure 1: (Top) Light curve of comet 17P/Holmes. (Bottom)
Motion of the isolated dust cloud to the central
condensation. The dashed and the solid lines denotethe first-order (a constant velocity model) and secondorder fits (a constant acceleration model), respectively.
The estimated onset time of the outburst is indicated byarrows.

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Figure 2: N8.8 images of 17P on Oct. 25, 26, 27, and 28, 2007 UT.
The flux unit is in Jy/pixel. The pixel scale is 0.13”. The
cross indicates the center of cloud and the rectangularregion is the aperture for photometry (31 pix × 31 pix).
The isolated cloud was moving toward the anti-sun
direction.
Reference[1] Watanabe, J., et al.: 2009, PASJ, 61, 67.

BD+44º493: A Ninth Magnitude Messenger from the Early Universe;
Carbon Enhanced and Beryllium Poor
ITO, Hiroko, AOKI, Wako

HONDA, Satoshi(The Graduate University for Advanced Studies / NAOJ)(Gunma Astronomical Observatory)

BEERS, Timothy, C.

(Michigan State University)
6

V [mag]8

BD +44 493

10
12
14
16
-6

-5

-4
[Fe/H]-3-2

Figure 1: Apparent magnitudes of metal-poor stars in the Milky
Way as a function of [Fe/H]. Data are taken from the
SAGA database (http://saga.sci.hokudai.ac.jp/).

1

A(Be)

The chemical composition of the early universe
is essentially recorded in the atmospheres of metalpoor stars. Therefore, chemical abundance studies ofmetal-poor stars have been playing an important role in
our understanding of the nucleosynthesis of the early
generations of stars as well as the chemical enrichment in
the Galaxy.
We present a one-dimensional LTE chemical
abundance analysis of the very bright (V = 9.1) carbonenhanced metal-poor (CEMP) star BD+44º493, basedon high-resolution, high signal-to-noise spectra obtainedwith Subaru/HDS [1]. The star is shown to be a subgiantwith an extremely low iron abundance ([Fe/H] = −3.7).
Although astronomers have been searching for extremely
metal-poor stars for decades, this is the first star foundwith [Fe/H] < −3.5 and an apparent magnitude V < 12
(Fig. 1).
The low metallicity of this object suggests thatits chemical composition record the yields of firstgeneration stars. The most important feature of the staris the large excess of carbon ([C/Fe] = +1.3) and oxygen([O/Fe] = +1.6), as also found in the most iron-poor([Fe/H] < −5) stars yet discovered. Based on its low
abundances of neutron-capture elements (e.g., [Ba/Fe]= −0.6), BD+44º493 is classified as a “CEMP-no” star.
Its abundance pattern implies that a first-generation faintsupernova is the most likely origin of its carbon excess,while scenarios related to mass loss from rapidly rotating
massive stars or mass transfer from an asymptotic giant
branch companion star are not favored.
From a high-quality spectrum in the near-UV region,
we set a very low upper limit on this star’s beryllium
abundance (A(Be) = log (Be/H)+12 < −2.0), whichindicates that the decreasing trend of Be abundances withlower [Fe/H] still holds at [Fe/H] < −3.5 (Fig. 2). This is
the first attempt to measure a Be abundance for a CEMP
star, and demonstrates that high C and O abundances do
not necessarily imply high Be abundances. Taking theevolutionary status of the star into account, however, theBe at its surface might have been depleted during thestellar evolution and not means the initial abundance.

0

-1

-2
-4

-3

-2
[Fe/H]-1

0

Figure 2: A(Be) vs. [Fe/H]. Our resultant upper limit is the filled
circle. The open symbols represent results of previous
studies (see [1] for details).

Reference[1] Ito, H., Aoki, W., Honda, S., Beers, T. C.: 2009, ApJ, 698, L37.

I Scientific Highlights

029

Entire Topography of Lunar Surface:
A Movie Created from KAGUYA(SELENE) Data
NAKAYAMA, Hirotaka, KOKUBO, Eiichiro, ARAKI, Hiroshi(NAOJ)

We make various movies by visualization of scientificobserved or simulated data at Four Dimentional Digital
Universe Project(4D2U Project). The most recent movie“Entire Topography of Lunar Surface” was made by the
lunar topographic data which was observed by Japanese
lunar orbiter spacecraft “KAGUYA(SELENE)”, and it
was accepted to the SIGGRAPH Asia 2009 Computer
Animation Festival[1].
There are many visualization software which areshareware or freeware. Naturally, the purpose of thesesoftware are scientific visualization, so there is a limit inimage quality and camerawork. On the other hand, we
created lunar movie by using Autodesk Maya[2] which
is high-end 3-D CG software instead of visualization
software in this work. Autodesk Maya has no function
for scientific visualization. But we can append various
functions to Maya by using scripting language or
programming language, and we developed special tool for
import the data to Maya. Figure 1 shows surface(left) andcube(right) models of lunar topographic data in Maya.
We made this movie at full high-vision size and we
prepared stereoscopic vision, too. The low resolution
version(640×360) is able to download from the 4D2U
website[3]. In the near future, we convert this movie into
dome master.

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Figure 1: Surface(left) and cube(right) models of lunar topographic data.

References[1] Nakayama, H., Kokubo, E., Araki, H.: 2009, SIGGRAPH Asia
2009, Animation Theater, 0575.
[2] http://www.autodesk.co.jp[3] http://4d2u.nao.ac.jp/t/var/download

Orientation of X-Ray Bright Points in the Quiet Sun
KANO, Ryouhei, TSUNETA, Saku

(NAOJ)				

In the Solar corona, there are many small structures
which are bright in soft X-rays and have size of less than
60″ in diameter. They are called “X-ray Bright Points(XBP)”. Two processes are considered for formationof XBPs; chance encounters of opposite polarities andemergence of magnetic bipoles
XBPs have been, as the name suggests, observed
as point-like features with the previous-generation
grazing incidence X-ray telescopes. The soft X-ray
telescope (XRT) aboard the Hinode satellite has resolved
their complex loop-like structures with its high spatial
resolution. This enables us to perform a detailed research
about shapes of XBPs. As a first step for understanding
the magnetic structures to form XBPs, we measured
the orientation angle of many XBPs found in snapshot
Xray images[1] and compared its distribution with thatof emerging magnetic bipolar regions investigated by
Harvey (1993) [2].
We used 26 snapshot XRT images of the quiet Sunnear the disk center taken between 2006 December and2008 November. The field of view is 526″ × 526″. We had
488 valid XBPs in total, and their size ranges between 8″
and 75″. Orientation angles are defined as the angle
between the line connecting the two footpoints and thelatitudinal east-west line of the Sun.
Figure 1 is the orientation distribution of XBPs
identified in this research. The magnitude of orientation
angles is defined as 0º for east-west direction, and ± 90º
for north-south direction. The shape of this histogramshows that the distribution is not uniform and there ispreference toward east-west direction. (The random
distribution is rejected with a significance level of 1% by
the χ2-test). This bias of orientation angle is, however,much smaller than that of emerging bipolar regions
investigated by Harvey (1993) [2]. The fact that theorientation distribution of XBPs is much more uniform
than that of emerging bipolar regions suggests that
XBPs come from not only emerging bipoles. However,
it is unlikely that the slight preference toward east-west
direction appeares through random chance encounters of
opposite polarities. This leads us to the concept that bothchance encounters and emerging bipoles contribute to theformation of XBPs.
We discuss the origin of XBPs in terms of solar
dynamo mechanism. There are two types of dynamo
processes; one is the global dynamo system driven by
the differential rotation of the Sun, and the other is the
local dynamo system with the granular convection flows
around the photoshere. Although large-scale magnetic
fields made by the global dynamo tend to have east-west

SHIBAHASHI, Hiromoto(University of Tokyo)

direction, transient horizontal magnetic fields, which arethought to come from the local dynamo process, shows
uniform orientation distribution [3]. This suggests thatthe preference toward east-west direction seen in theorientation distribution of XBPs is a hint for the influenceof the global dynamo on the formation of emerging
bipoles with size of XBPs.

100
number of XBPs

UEDA, Kohei(NAOJ / University of Tokyo)			

80
60
40
20
0

0-15 15-30 30-45 45-60 60-75 75-90
orientation angle (absolute value)

Figure 1: The distribution of the orientation of XBPs. 0ºcorresponds to the east-west direction, and 90ºcorresponds to the north-south direction. The dashed line
shows the expected distribution in the case of a perfectly
uniform distribution, and the dotted lines represent ± 1σ
statistical error.

References[1] Ueda, K., Kano, R., Tsuneta, S., Shibahashi, H.: 2010, Sol.
Phys., 261, 77.
[2] Harvey, K. L.: 1993, Ph.D.thesis, Univ.Utrecht.
[3] Ishikawa, R. Tsuneta, S.: 2009, A&A, 495, 607.

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Discovery of the Coldest Imaged Companion of a Sun-like StarTHALMANN, C.

		CARSON, J.

(Max Planck Institute for Astronomy) (Max Planck Institute for Astronomy / College of Charleston)

JANSON, M.

(University of Toronto)

EGNER, S.

FELDT, M.

(NAOJ)

McELWAIN, M.

(Princeton University)

HASHIMOTO, J., HAYANO, Y.

(Max Planck Institute for Astronomy)			

HENNING, T.

(Max Planck Institute for Astronomy)KLAHR, H.

GOTO, M.

(Max Planck Institute for Astronomy)(Max Planck Institute for Astronomy)

HODAPP, K.W.

(University of Hawaii)			

KUDO, T., KUSAKABE, N.
(NAOJ)		

(NAOJ)KANDORI, R.
(NAOJ)

MORDASINI, C.

(Max Planck Institute for Astronomy)

MORINO, J.-I., SUTO, H., SUZUKI, R., TAMURA, M.
(NAOJ)

We present the discovery of a brown dwarf or possible
planet to the nearby sun-like star GJ 758 based on direct
imaging in the H band using the high contrast imaging
instrument HiCIAO on the Subaru telescope[1,2]. The
imaged substellar companion, GJ 758 B, was found tohave a mass of 10–40MJup, a temperature of 550–640 K,
and a projected separations of 1.9″ = 29 AU. This makes
GJ 758 B one of the few known T-type companions, andthe coldest ever to be imaged around a sun-like star.
GJ 758 is a G9-type star with a mass of 0.97 M ,
located at a distance of 15.5 pc. We first detected GJ
758 B with HiCIAO in angular differential imaging(ADI) mode on Subaru telescope on May 3, 2009, witha field of view of 20″ In addition to the known nine fieldobjects around the host star, we have detected unknown
tenth object in close separation with 5σ confidence. Ina follow-up observations on August 6, 2009, the object
was rediscovered with 8.5σ confidence. We used a locally
optimized combination of images algorithm (LOCI, [3])in ADI data reduction. The discovery image of GJ 758 B
is shown in Fig. 1.
Located only 15.5 pc away from the Sun, GJ 758
B exhibits strong proper motion. On the basis of two
epoch data, GJ 758 B is found to share common propermotion with its host star, confirming that they form agravitationally bound system. Their motion deviates fromthe proper motion for the background stars by 10σ. thus achance alignment can be excluded. GJ 758 B is measured
to move by (−7.6 ± 9.5, 23.4 ± 9.5) mas along the (RA,Dec) axes relative to GJ 758. This represents the orbital
motion of the companion around its host. Future longterm observations are desirable in order to cover the longorbital period of GJ 758 B.
The mass and effective temperature of GJ 758 B
are derived based on the COND models[4] and thephotometries in the H band. We found 10 –40 MJup forthe mass and 549–637 K for the temperature. The large
uncertainty in the mass measurements comes from theambiguity of the estimated system age (0.7 to 8.7 Gyr),032

I Scientific Highlights

because GJ 758 is a nearby field star with no known
connection to any co-moving stellar association. If weemploy the photometric age (0.7 Gyr), a typically usedmethod for age estimation, we expect the companion tobe high-mass (10 MJup) planet with T9 spectral type. This
makes GJ 758 B the coolest substellar companion to a
sun-like star ever imaged in thermal light.
Though there is large uncertainty in measured orbital
motion of GJ 758 B, its orbit can be estimated basedon the observations and Monte Carlo simulation. The
orbit of GJ 758 B is likely eccentric (e = 0.50–0.87) andof a size comparable to Pluto's orbit (33.9–118.0 AU).
The separation occupies intermediate position at which
companions are expected to form by core accretion ( <~ 5AU) or gravitational collapse (typicaly >~ 100 AU). The
search of planets around G-type stars with direct imaging
is essentially important to reveal whether the giant planetswith large orbit are common or not.

Figure 1: The discovery image of GJ 758 B taken in theobservations in August 2009. For the two point sources
enclosed by circles, lower source represents GJ 758 B,
and upper source is a possible second object detected
only in the August image. The host star is located inimage center.
References[1] Thalmann, C., et al.: 2009, ApJL, 707, 123.
[2] Hodapp, K. W., et al.: 2008, SPIE, 7014, 42.
[3] Lafreni`ere, D., et al.: 2007, ApJ, 660, 770.
[4] Baraffe, I., et al.: 2003, A&A, 402, 701.

Development of Cryogenic Integration Circuitswith GaAs JFETs for Sub-millimeter Camera
HIBI, Yasunori, MATSUO, Hiroshi(NAOJ)NAGATA, Hirohisa, IKEDA, Hirokazu

				(JAXA/ISAS)				

In NAOJ ATC, we have been developing torealize the sub-millimeter/terahertz camera with morethan 10 k pixel. As its detectors, we suppose the SIS(Superconductor-Insulator-Superconductor) photon
detectors [4]. Since these detectors must be cooled below
1 K for their best performance, a cryogenic readout
system is need for precise and effective readout. To
realize such many channel cryogenic readout system, it isvery important to suppress the system power dissipation.
From cooling power of the cryogenic cooler, current
power dissipation target is below 1 µW/ch.
We have developed several kinds of integration
circuits with n-type GaAs JFETs until 2009 spring.
The reason to select the n-type GaAs JFETs is that thecryogenic static characteristics in low power dissipation(≤ 0.1 µW) are very similar to those in room temperature.
From 2007 to 2009, we have done three times trial
manufactures and cryogenic demonstrations. Thesedemonstration results are reported in those papers[1-7]. We show some concrete results of cryogenic ICs(integration circuits). We have realized the amplifier
which integrate photo current signal and exchange thisto voltage at power dissipation 2 ~ 3 µW/ch (Fig. 1a) [2,6]. We also have realized multiplexers with sample-andholds (Fig. 1b) [1], the shift registers to control the abovementioned multiplexers which are able to work fasterthan 100 kHz at cryogenic temperature (Fig. 1c) [5], andthe 32 channels voltage distributer to cancel input offset
voltages of the 16 channels AC coupled CTIA (Fig. 1d).
We have been planning a cryogenic readout system withthese cryogenic circuits. In 2010 spring, we designed andmanufactured 32 channel multi-chip modules by using
these GaAs ICs to realize the cryogenic readout system.
To increase possible number of readout channel by thiscryogenic system, power dissipations of each circuit haveto be suppressed by redesigning or newly investigations.
These demonstration results are useful not only forour sub-millimeter/terahertz camera but also for every
kinds of cryogenic multi-pixel camera which detectors
have high impedance.

FUJIWARA, Mikio(NiCT)

Figure 1: Trial manufactures of ICs with GaAs JFETs in 2008’s.
The sizes of these ICs are 1.8 mm × 7.6 mm. a):
16 channels AC coupled CTIA (Capacitive TransImpedance Amplifier). b): 32 channels multiplexer withsample-and-holds. c): 32 channels shift register. d): 32
channels voltage distributer.

References[1] Hibi, Y., et al.: 2009, Cryogenics, 49, 672.
[2] Nagata, H., et al.: 2009, Cryogenics, 49, 676.
[3] Fujiwara, M., et al.: 2009, Cryogenics, 49, 626.
[4] Matsuo, H., et al.: 2009, AIP Conf. Proc., 1185, 393.
[5] Hibi, Y., et al.: 2009, AIP Conf. Proc., 1185, 290.
[6] Nagata, H., et al.: 2009, AIP Conf. Proc., 1185, 115.
[7] Fujiwara, M., et al.: 2009, AIP Conf. Proc., 1185, 267.

I Scientific Highlights

033

Detection of the most distant explosion ever known(Near-infrared observation of GRB 090423@z = 8.2)
YOSHIDA, Michitoshi(Hiroshima University / NAOJ)YANAGISAWA, Kenshi, KURODA, Daisuke, SHIMIZU, Yasuhiro, NAGAYAMA, Shogo, TODA, Hiroyuki(NAOJ)

			

OHTA, Koji

(Kyoto University)

Gamma ray burst (GRB) is one of the most promisingprobes currently available for investigating early
universe. It has been revealed that significant fraction(~50 %) of GRBs emits optical - infrared afterglow. By
observing optical - infrared afterglows, we can obtainvarious pieces of information about GRB progenitors,
circumstance around GRBs, and redshifts, as well as
explosion and emission mechanisms of GRBs.
GRB 090423 is a long duration GRB detected by the
Swift satellite at 07:55:19 UT on April 23 in 2009 [1].
Deep near-infrared (NIR) spectroscopic observations
revealed that the redshift of GRB 090423 is ~8.2 [2],indicating that this is the most distant astronomical object
ever known.
We performed NIR observations of this burstwith a NIR camera, ISLE [3] attached to the 188 cm
telescope of Okayama Astrophysical Observatory. We
started the observation at 10:32:27 UT, i.e the timedelay from the trigger t d was 9,428 s. We made J, H,
and Ks band imaging observations in a 4′ × 4′ fieldaround the afterglow position reported by other infraredobservations. Total exposure times for J, H, and Ks bands
were 720 s, 960 s, and 480 s, respectively. Sky was clear
and typical seeing is around 1.5″.
We clearly detected the afterglow emission of GRB
090423 in combined J band image (Figure 1) [4]. The
J-band AB magnitude of the afterglow was 20.16 ± 0.14
at td = 10,694 s. The afterglow was marginally detected(2σ detection) in our H band image, but it was too faint tomake reliable photometry. There was no corresponding
source in our Ks band image.
Together with other NIR photometric data [2] of GRB
090423, our data revealed that the light curve (LC) of theafterglow is quite shallow ( f ∝ t d−0.01 ) in the early epoch
and this shallow phase continues to td ~ 3,000 s in the rest
frame. Such long, shallow decay of optical afterglow
is very rare. The fraction of optical afterglow showing
such shallow decay is only 9 %. Similar shallow decay
was observed for GRB 050801, but its duration is much
shorter than GRB 090423.
The afterglow LC of GRB 090423 shows much
rapid decay in later epoch (td > 10,000 s) [2]. In order toestimate the break time of the NIR LC, tb,NIR, we tried to
fit the late epoch NIR LC by two models of power law

034

I Scientific Highlights

KAWAI, Nobuyuki(Tokyo Institute of Technology)

decay, a rapid decay model and a shallow decay model.
The power-law decay index α ( f ∝ t d−α) and break time forthe both models are (α, tb,NIR) ≈ (−1.5, 24,000 s) and ≈ (−0.9, 9,800 s), respectively. Unfortunately, there is no dataaround td ~ 20,000–30,000 s, definite break time cannot
be determined. Nevertheless, adding our data to the NIR
LC made it clear that td,NIR is much later than the X-ray
break time (tb,X ≈ 4,800 s). The time delay Δt = tb,NIR − tb,X
is ~ 5,000–17,000 s. The Δt of GRB 090423 is one of thelongest ones ever observed in GRB LCs.

Star 2

Star 1Figure 1: The J band image of the afterglow of GRB 090423.
“Star1” and “Star2” are photometric reference stars.

References[1] Krimm, H. A., et al.: 2009, GCN Circular, 9198, 1.
[2] Tanvir, N. R., et al.: 2009, Nature, 461, 1254.
[3] Yanagisawa, K., et al.: 2006, SPIE, 6269, 118.
[4] Yoshida, M., et al.: 2009, GCN Circular, 9218, 1.

Neutrino-Induced Reactions on 56Ni and Production of 55Mn
in Population III Stars

Figure 1: (a) GT strength in 56Ni. (b) Neutral current reaction
cross sections for 56Ni at supernova temperatutes Tν.

102

(c)

p+55Coγ+56Ni

100

5
e
α+ F
2

n+55Nipp+ 54
Fe

We study neutrino nucleus reactions on 56Ni as well as
its astrophysical implications [1]. GT transitions in 56Ni
are studied by shell model calculations with the use of a
new shell model Hamiltonian for the pf-shell, GXPF1J[2], which describes well the spin transitions in fp-shell
nuclei,The neutral current proton knock out reaction 56Ni (ν,ν′p) 55Co is quite interesting as it leads to production of
Mn through electron capture twice; 55Co (e−, νe) 55Fe (e−,νe) 55Mn. The GT transition strengths in 56Ni (B(GT0))
are shown in Fig. 1(a). We find that the strength isfragmented into two peaks for GXPF1J, while it has only
one peak for KB3G [3]. This difference in the distributionof the strength leads to different (ν, ν′p) cross sections.
Calculated cross sections for 56Ni (ν, ν′) 56Ni inducedby supernova neutrinos are shown in Fig. 1(b), wherecontributions from multipoles besides 1+ are evaluatedby the RPA method and the universal quenching, gAeff /gA= 0.74, is adopted for all multipoles. The present results
are close to those of ref. [4] but small compared to thoseof ref. [5].
Cross sections for particle knock out channels as wellas γ emission channels are obtained by using branchingratios calculated by the Hauser-Feshbach theory. We
find that the (ν, ν′p) cross section becomes large for
GXPF1J compared to the previous calculation using thecross sections of HW92 [6] as shown in Fig. 2. This isdue to large branching ratios for the proton knock-out
channels for GXPF1J caused by the spreading of the GT
distribution.
We now discuss the production yields of elements
during supernova explosion for a Population III star withmass 15 M. The production yields of Mn are found to beenhanced for the GXPF1J Hamiltonian. The logarithmicvalues of the yield ratio over Fe relative to the solar
abundances, [ Mn/Fe ], are −0.19, −0.29 and −0.53 for
GXPF1J, HW92 and no ν-processes, respectively. The
calculated values are consistent with the abundances
observed in extremely metal-poor stars with [Fe/H] ≤ −3
−0.43 +0.31/−0.17 [7]. The proton knocked out from
56Ni by the neutrino-induced reaction enhances also the
production yield of 59Co (see ref. [1] for details). Theseenhancement shows the importanct roles of the neutrino
processes in nucleosynthesis in stars.

KAJINO, Toshitaka(NAOJ / University of Tokyo)

10-2

αα+48Cr
51 Fe

10-4
10-6

αn+
αp+ 5
1
M
pn+ 5 n4
Co

SUZUKI, Toshio(Nihon University / NAOJ)

σ (10 -42 cm2 )			2nn+54Ni

46Tν (MeV)810Figure 2: Reaction cross sections on 56 Ni for γ and particle
emission channbels at supernova temperatures T ν .
Results obtained by using cross sections of HW92 [6]are denoted by triangles, filled circles and hollow circles.

References[1] Suzuki, T., et al.: 2009, PRC, 79, 061603(R).
[2] Honma, M., et al.: 2002, PRC, 65, 061301; ibid.: 2004, C 69,
034335.
[3] Caurier, E., et al.: 2005, Rev. Mod. Phys., 77, 427.
[4] Kolbe, E., Langanke, K.: 2001, PRC, 63, 025802.
[5] Woosley, S. E., et al.: 1990, ApJ, 356, 272.
[6] Hoffman, R. D., Woosley, S. E.: 1992, Neutrino Interaction
Cross Sections and Branching Ratios.
[7] Cayrel, R., et al.: 2004, A&A, 416, 1117.

I Scientific Highlights

035

Search for Remnant Clouds Associated with the TW Hya Association
TACHIHARA, Kengo(NAOJ)

NEUHÄUSER, Ralph

FUKUI, Yasuo(Astrophysikalisches Institut und Universit¨ats-Sternwarte Jena, Germany)

036

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HIP 64837

21

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HIP 65178

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HIP 64925

C1

Tr* (K)

Galactic latitude

We surveyed for natal molecular clouds that formed
the most nearby young cluster TW Hya association in
12CO emission line and estimated their distance from the
NaI absorption lines. The TW Hya association (TWA; d~ 50 pc) consist of 20 member stars [1] including a typicalclassical T Tauri star, TW Hya, and the cluster age isestimated to be ~ 2 Myr. While almost all similarly young
associations such as those in Taurus are known to beembedded in or located close to molecular clouds, TWA
is isolated from any molecular gas and its natal cloud has
not been discovered. Taking advantage of its proximity,
proto-planetary disks [2] and young exoplanets have been
actively surveyed for the member stars, while due to its
large extent, sensitive and extensive survey for molecular
cloud has not been well attempted.
We have carried out 12CO (J =1–0) survey for remnant
clouds with the NANTEN telescope at Las Companas
Observatory, Chile. The survey areas are chosen fromcold dust clouds with strong 100 m emission by IRAS
where entire TWA member are distributed. As a result,faint CO emission is detected from some of the observed
positions (Fig. 1).
In order to investigate the association of those
CO clouds with TWA, the distances to the clouds are
estimated as follows. Expected background stars withknown distances are picked up from the Hipparcos
catalog, and their optical spectra are obtained with the
FEROS spectrograph on the ESO 2.2 m telescope. Theinterstellar absorption lines of NaI doublet at 5890 Å
are extracted from the spectra (Fig. 2). Because ofnon- detection from nearby Hipparcos stars, the largest
molecular cloud is revealed to be background with adistance of > 200 pc. Distances to the other two small
clouds are estimated to be < 100 pc, and thus they arevery low-mass possible remnant clouds associated withTWA.
We conclude that despite the extensive survey, theestimated mass of the remnant molecular cloud is ~3 M
at the most. Assuming the star formation efficiency to be
3%, the TWA natal cloud of ~540 M molecular gas has
been dissipated away within only 1 Myr. This implies
past disturbance such as nearby supernova explosion.

(Nagoya University)

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306

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VLSR (km/s)

Galactic longitude

Figure 1: One of the dust cirrus cloud where CO emission isdetected. The gray scale represents dust extinction with
contours of 0.15 mag. The detected CO emission lines (4arcmin grid spacing) are illustrated aside. The circles andcross show Hipparcos stars with and without detectionsof NaI absorption lines, respectively. From the distanceto HIP 64837, distance to this cloud is estimated to be <81 pc.

HIP 57809
5880

5885

HIP 64837
5890

5895

Wavelength (Å)

5900

5880

5885

HIP 64925
5890

5895

Wavelength (Å)

5900

5880

5885

5890

5895

5900

5905

Wavelength (Å)

Figure 2: Spectra around the detected Na I doublet lines. The
narrower lines than those of the stellar photospheres are
by interstellar absorption.

References[1] Tachihara, K., Neuhäuser, R., Frink, S., Guenther, E.: 2003,
Astronomische Nachrichten, 324, 543.
[2] Kastner, J. H., Zuckerman, B., Weintraub, D. A., Forveille, T.:1997, Science, 277, 67.

Polarimetric mode of stellar interferometer using birefringent retarders
MURAKAMI, Naoshi(NAOJ / Hokkaido University)

OHISHI, Naoko, NISHIKAWA, Jun

YOSHIZAWA, Masanori(NAOJ)				

A stellar interferometer uses two or more telescopes
to measure interferometric fringe visibilities, andprovides astronomical observations with very highangular resolution. It is expected that a polarimetricstellar interferometer, which measures fringe visibilitiesof two orthogonal polarized lights, will be a powerfultool for investigating many astronomical targets, suchas magnetism of chemical peculiar stars, mass loss andcircumstellar disks of hot stars, extrasolar planets, and soon.
For building a polarimetric stellar interferometer,polarizers or polarizing beam splitters (PBS) areneeded to separate the two polarized fringes. When thepolarizers are used, one component of polarizations is
discarded, which would result in a large time lag between
acquisitions of the two polarized fringes. In addition, it
is required to rotate the polarizers to measure the two
fringes. When the PBSs are used, on the other hand, twodetectors or a two-dimensional detector will be needed
for acquiring the polarized fringes.
We proposed a novel technique for a polarimetricobservational mode, which can be readily installed
into existing stellar interferometers [1]. Figure 1 showsa principle of the proposed technique, in which twobirefringent retarders R1 and R2 (thickness of l) are
inserted into each arm of an interferometer. A birefringent
retarder has two different refractive indices (n e andno) along two orthogonal (p- and s-) polarizations. By
setting axes of the retarders 0º and 90º, centers of the twopolarized fringes shift in opposite directions ± βl (β = ne− no) along an optical-path deference (OPD). Thus thepolarized fringes can be isolated and detected by a single
detector for measuring their visibilities separately.
We manufactured quartz retarders of l = 1.124 mm (apicture in Fig. 1). The thickness l corresponds to a fringe
isolation of ±10.3 μm in visible. We carried out laboratory
demonstration of the proposed technique using a whitelight source. Figure 2 shows interferometric fringes
acquired (a) without and (b) with the fringe isolation. We
can see in the result that the two polarized fringes areclearly isolated.
We also proposed to install this technique into the
Mitaka optical Infra-Red Array (MIRA-I.2). Assuming
the retarders with l = 0.4 mm, the MIRA-I.2 can detect thetwo polarized fringes with a time lag of about 18 msec,
which is greater than atmospheric coherent time (typicallyof the order of a few msec). Thus an effect of atmosphericturbulence will not be identical for acquisitions of the two(formerly NAOJ)

fringes. Nevertheless, precise polarimetric observations
will be feasible by averaging a large number of fringe
visibilities measured within short time (e.g., 187 fringes/
minute for the MIRA-I.2).
From
telescope2+β

R 2 (90o)

From
telescope1−βDetectors-pol.
R 1 (0o)

Beam combinerp-pol.

Figure 1: Principle of a novel polarimetric stellar interferometerusing birefringent retarders.

(a)I (δ )

2

Intensity [arb. unit]

				

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5

10

15

20

O ptical Path Difference [micron](b)

1i' (δ )
0

-20

-10

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OPD δ [micron]Figure 2: Reslt of laboratory demonstration; interferometricfringes (a) without and (b) with the fringe isolation.

Reference[1] Murakami, N., Ohishi, N., Nishikawa, J., Yoshizawa, M.: 2009,
Appl. Opt., 48, 5774.

I Scientific Highlights

037

Emission Signature of a Young Protostellar Object: Line Transfer Studyof an Embedded Young Molecular Outflow
YAMADA, Masako(ASIAA)MACHIDA, Masahiro,TOMISAKA, Kohji

I Scientific Highlights(Nagoya University)

the early stage examined in this article, different kindsof velocities take the similar speed (vinfall ~_ voutflow ~_ vrot).
It complicates the emission distributions compared tothe more evolved objects (voutflow  vinfall) observed withcurrent instruments.
Our simulation demonstrated how the characteristics
of a specific MHD model appear in the line emission.
The relation between the emission feature and thephysical processes generating them is quite complicated,and should be pursued more with further line transfer
experiments in the future.

10.5
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1000

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1000

11.5

(a)

log10(n[cm-3])

1000

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x[AU]

1000

Figure 1: Panel(a) shows the density structure (in color), andwhite arrows describe the flows directions. Panel(b)exhibits the integrated intensity map of SiO(7–6) line for
an inclination angle 30º. Red and blue contours indicate
redand blue-shifted components integrated separately.

Tb [K]

Pre-main sequence stars exhibit ubiquitously bipolar
outflows of molecular gas of the speed about 10 km s−1.
Recent magneto-hydrodynamic (MHD) simulations haveachieved a significant progress in the studies of lowmass star formation and launching mechanisms of theoutflows. Formation of stars begins with gravitational
collapse of a cold (~_ 10 K) molecular core. We performed
non-LTE (non-thermodynamic equilibrium) line transfer
simulation with MHD simulation of a young outflow
embedded in its parent collapsing core (“envelope”),
seeking for characteristic features of the model in thesynthesized emission, which will be observed with the
ALMA telescope.
In the snapshot data used in the line transfer
6−3
simulation, the density is as high as n >~ 10 cm . The high_ 10 for lines ofdensity thermalizes the population up to J ~low critical densities such as 12CO and its isotopologues,
and their huge optical thicknesses make them inadequate
for probing the central region. Contrarily, the populationof higher critical density lines such as SiO (ncrit (J) ~_ 105
× J 3 cm−3) deflects from LTE for high-J transitions inthe sub-mm band. The optical thicknesses of these lines
fall below 1% of CO lines, proving their effectivenessin examination of the dynamics of the central launchingregion of the young outflow.
Figure 1 shows the density structure of the snapshot
data of MHD simulation, and the integrated intensity mapof SiO(7–6) line for the inclination angle of the outflow
axis 30º. In this model, the interplay of the core rotationand magnetic field drives the outflow. The magnetocentrifugal force (MCF) moves away the matter close to
the first core (Figure 1(a), R ~ 50 AU). The distribution ofred- and blue-shifted intensity components in Figure 1(b)reflects the rotation.
One of the most characteristic features of the
MCFdriven flow is the rotation of the formed outflow
in the same direction of the launching region. It appears
most clearly in the line-of-sight velocity (v r) related
diagrams such as velocity channel maps (see [1] fordetails). In Figure 2, we plot the distribution of line
profiles of the SiO(7–6) line for 30. inclination (Figure1(b)). Figure 2 exhibits a double-horn profile skewed
to the blue-ward in most of the region. This is known
as a signature of the collapse of the cloud [2]. Our linetransfer simulation caputures the global feature of theobject embedded in the contracting envelope. Local
profiles reflect the rotation and birth of the outflow. In

038

INUTSUKA, Shu-ichiro(NAOJ)			

z[AU]

				

6
4
2
0
-4 -2 0 2 4
Vlos[km sec-1]

Figure 2: SiO(7–6) line profile distribution of Figure 1(b).
References[1] Yamada, M., et al.: 2009, ApJ, 703, 1141.
[2] Evans, N.: 1999, Annual Review of A&A, 37, 311.

An improved lunar gravity field model from SELENE
and historical tracking data
MATSUMOTO, Koji, GOOSSENS, Sander, ISHIHARA, Yoshiaki
KIKUCHI, Fuyuhiko, NODA, Hirotomo, HANADA, Hideo(NAOJ)

LIU, Quinghui, KAWANO, Nobuyuki

				
		

(SHAO)				

NAMIKI, Noriyuki(JAXA)LEMOINE, Frank, ROWLANDS, David(Chiba Inst. of Tech.) 		

The direct satellite tracking data over the lunar
farside were for the first time collected by SELENE(Kaguya) mission using a relay sub-satellite. The first 5
months of 4-way Doppler data so obtained by the relay
subsatellite greatly improved our knowledge of thefarside gravity field [1, 2]. A new spherical harmonic
solution of the lunar gravity field to degree and order 100,
called SGM100h, has been developed using historical
tracking data and longer span (14.2 months) of SELENE
tracking data including all usable 4-way Doppler data [3].
Figure 1 shows free-air gravity anomaly maps which arecalculated from SGM100h model.
The new model successfully reveals farside featuresin free-air gravity anomalies which are characterizedby ring-shaped structures for large impact basins andnegative spots for large craters. SGM100h produces acorrelation with SELENE-derived topography as highas about 0.9, through degree 70. Comparison between
SGM100h and LP100K (one of the pre-SELENE models)
shows that the large gravity errors which existed in
LP100K are drastically reduced and the asymmetric error
distribution between the nearside and the farside almost
disappears. The gravity anomaly errors predicted fromthe error covariance, through degree and order 100, are
26 mGal and 35 mGal for the nearside and the farside,
respectively. Owing to the 4-way Doppler measurements
the gravity coefficients below degree and order 70 are
now determined by real observations with contribution
factors larger than 80 percent. With the SELENE farside
data coverage, it is possible to estimate the gravity field
to degree and order 70 without applying any a priori
constraint or regularization. SGM100h can be used for
global geophysical interpretation through degree andorder 70.

References[1] Namiki, N., et al.: 2009, Science, 323, 900.
[2] Matsumoto, K., et al.: 2009, J. Geod. Soc. Jpn., 55, 269.
[3] Matsumoto, K., et al.: 2010, JGR, 115, E06007.

IWATA, Takahiro(NASA GSFC)

Nearside

Farside−400 −300 −200 −1000mGal
100 200 300 400

Figure 1: Free-air gravity anomalies from SGM100h model for
lunar nearside (top) and farside (bottom).

I Scientific Highlights039

Development of the Lunar Crustal Thickness Modelby SELENE (Kaguya) Selenodetic Data
ISHIHARA, Yoshiaki, GOOSSENS, Sander, MATSUMOTO, Koji
NODA, Hirotomo, ARAKI, Hiroshi, HANADA, Hideo, TAZAWA, Seiichi, SASAKI, Sho(NAOJ)				

NAMIKI, Noriyuki(Chiba Inst. of Tech.)

The SELENE (Kaguya) were launched on September
14, 2007. The main orbiter of the SELENE was directly
tracked, even when that was over the lunar farside using
relay subsatelite (4-WAY Doppler measurements).
SELENE gravity models [1], those constructed using
SELENE and previous tracking data, drastically improve
the farside gravity anomaly. Accurate and high resolution
lunar shape models were also developed using laser
altimeter data of the SELENE [2]. These SELENE
selenodetic data enable us to conduct various kinds ofselenodetic analysis not only for the nearside but also for
the farside.
Free-air gravity anomaly indicate effect of both
topography and subsurface density anomalies. Bouguer
gravity anomaly, that express internal density anomalies,
can compute by subtracting topography contribution fromfree-air gravity anomaly using lunar shape model. For
the lunar case, a main cause of Bouguer gravity anomaly
is undulation of the Moho (crust / mantle interface).
The Moho relief can compute by assuming the value of
density difference of interface, and at least one reference
depth of interface. In this model, we have used crustal
density of 2800 kg/m3, mantle density of 3360 kg/m3,
and we assume that the mantle materials are not exposed
anywhere. Mare basalts are higher density than that ofcrustal materials. Therefore moho relief modeling are
affected by thick basalt fills. So we extract effects ofsome thick mare basalt fills by assuming mare basalt
density of 3200 kg/m3.
Figure 1 shows total crustal thickness (thicknessof crustal materials plus mare basalt) variations over
the whole Moon [3]. Crustal thickness ranges from theminimum of nearly zero beneath the Moscoviense basin
to a maximum of 110 km on the southern rim of the
Dirichlet- Jackson basin, and mean thickness is about
53 km. Nearside crust is thinner than that of farside. At
inside area of impact basins have thinner crust than thatof surrounding area. Our result agrees well with previous
analyses of general features of crustal thickness. On theother hand, locations of the minimum and maximum
crustal thickness are quite different from those ofprevious analyses. The shift of the thinnest crust is dueto the low resolution and inaccuracy of previous gravity
models over the farside. Shifting of the thickest crust
position is mainly due to the inaccuracy of previous

040

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IWATA, Takahiro(ISAS / JAXA)

topographic models.
For farside baisins, we classified the lunar impact
basins into two types (type I, and type II) by spatial
pattern and ratio of free-air and Bouguer gravity
anomalies. The crustal thickness map indicates that thedifferences between type I and type II basins are probably
controlled by the ratio between pre-impact crustal
thickness and impact scale.
This research was supported by a Grant-in-Aid for
Scientific Research (A) (20244073, PI: S. Sasaki).

km
0

10 20 30 40 50 60 70 80 90 100 110

Figure 1: Total lunar crustal thickness (crustal materials and marebasalt fills) map for a simple one-layer crust model. Thismap is centered on 180ºE longitude.

References[1] Namiki, N., et al.: 2009, Science, 323, 900.
[2] Araki, H., et al.: 2009, Science, 323, 897.
[3] Ishihara,Y., et al.: 2009, Geophys. Res. Lett., 36, L19202.

The new detections of 7Li/6Li isotopic ratio in the interstellar media
KAWANOMOTO, Satoshi, KAJINO, Toshitaka, AOKI, Wako, ANDO, Hiroyasu
NOGUCHI, Kunio, IZUMIURA, Hideyuki, KAMBE, Eiji, OKITA, Kiichi, TAJITSU, Akito
TANAKA, Wataru, WATANABE, Etsuji, YOSHIDA, Michitoshi(NAOJ)BESSELL,M.

(Mount Stromlo Observatory)

SADAKANE, Kozo

(Osaka-Kyoiku University)

SUZUKI, Ken, Takeru(University of Tokyo)

HONDA, Satoshi(Gunma Astronomical Observatory)

SATO, Bun’ei

TAKADA-HIDAI, Masahide(Tokyo Institute of Technology)		

The elemental abundance of lithium preserves richinformation from the early Big-Bang Universe to thepresent Milky Way Galaxy. Lithium has two stable
isotopes, 6Li and 7Li. Within the framework of a wellestablished theory of standard BBN, significant amountsof the light elements, 2H (D), 3He, 4He and 7Li, weresynthesized during the first three minutes of the hot
Big- Bang Universe. At later times, 7Li is continuously
produced by stellar nucleosynthesis, as well as byspallation and α + α fusion reactions of Galactic Cosmic
Rays interacting with the interstellar medium, while 6Li isalmost purely synthesized by the GCR-ISM interactions.
We have determined the isotopic abundance ratioof 7Li/6Li in the interstellar media (ISMs) along linesof sight to HD169454 and HD250290 using the High
Dispersion Spectrograph on the Subaru Telescope. We
also observed ζ Oph for comparison with previous data.
The observed abundance ratios were 7Li/6Li = 8.1+3.6−1.7
and 6.3+3.0−1.8 for HD169454 and HD250290, respectively.
These values are in reasonable agreement with thoseobserved previously in the solar neighborhood ISMs
within ±2σ error bars and are also consistent with ourmeasurement of 7Li/6Li = 7.1+2.9−1.6 for a cloud along the lineof sight to ζ Oph. This is good evidence for homogeneous
mixing and instantaneous recycling of the gas component
in the Galactic disk. We also discuss several sourcecompositions of 7Li, Galactic cosmic-ray interactions,stellar nucleosynthesis, and Big-Bang nucleosynthesis [1].
Although we cannot find a clear RG-dependence of
7Li/6Li, we expect that more precise determination of thelithium isotopic ratio (7Li/6Li)obs over the wider rangeof RG than the present study may exhibit the gradientas suggested theoretically. This would serve to infera more reliable value of the primordial 7Li abundance
independently of stellar depletion effects that confront
the identification of the primordial value from the Spite
plateau in population II stars. A primordial 7Li abundance
that is totally free from the stellar depletion process
should directly test the cosmological models for the BigBang nucleosynthesis and the particle theory of weakinteractions and dark matter.

(Tokai University)

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0
10
VLSR (km/s)

20

30

40

Figure 1: An example of observation of neutral lithium absorption.
Histogram : Observational data toward ζ Oph. Solid line
: The model fitting of absorption line of 7Li. Dashedline: The model fitting of absorption line of 6Li. Dots:
Residuals.

Reference[1] Kawanomoto, S.: 2009, ApJ, 701, 1506.

I Scientific Highlights

041

The interstellar rubidium isotope ratio toward HD169454
KAWANOMOTO, Satoshi, AOKI, Wako, KAJINO, Toshitaka(NAOJ)

MATHEWS, Grant J.

(University of Notre Dame)

lar
M s-p
r
ai
n oce
spr ss
oc
es
s

ess

So

We

Sola

r To

r-procetal

4.0e+09
0.995

roc

1.000

s-p

1.005

ak

1.010

This new value differs significantly from the only
other reported local interstellar value of 1.21 ± 0.30(1σ)
along a different line of sight [2], and is marginallyconsistent with the Solar value of 2.43. We discuss theimplications of this new isotopic ratio in the context ofthe various relevant models for the nucleosynthesis ofheavy elements. We suggest that material in this cloud
may be depleted in the main s-process component.
A pure r-process, a pure main s-process, and a pure
weak s-process produce Rb isotopes in the ratio of 5.9, 2.0,
and 1.1, respectively. The difference between our results
and that of Federman et al.[2] suggests that variations
in neutron-capture nucleosynthesis may have indeed
occurred in the local Solar neighborhood.
ss

We report here on a new determination of theinterstellar 85Rb/87Rb isotopic ratio for diffuse gas along
the line of sight toward HD169454 [1]. We have detected
no contribution of 87Rb in the Rb I absorption line at
7800 Å in this cloud. We deduce a lower limit of 85Rb/
87Rb > 2.4(95%C.L.).

1.010

2.0e+09

85

1.005

1

1

-2

N( Rb I ) (cm )3.0e+09

2

2
3

3

1.000

1.0e+09
0.995

0.0e+00
0.0e+00

1.010

1.000

0.995

3.0e+09

References[1] Kawanomoto, S., et al.: 2009, ApJ, 698, 509.
[2] Federman, S. R., et al.: 2004, ApJL, 603, L105.
7800.17800.27800.37800.47800.57800.67800.7

Figure 1: The absorption line of neutral rubidium toward
HD169454. Three panels show the best fit to theabsorption feature in which 85Rb/87Rb = ∞, 2.59, 1.21,
respectively.

042

2.0e+09
N(87Rb I ) (cm-2 )

4.0e+09

Figure 1: Contours of constant χ2 confidence levels in the 85Rb I
vs. 87Rb I plane. Contours are drawn for the 1, 2, and 3σ
confidence levels as labeled. Our data for HD169454 areshown in solid lines. For illustration, the dotted lines are
extracted from Federman et al.[2].

1.005

0.990
7800

1.0e+09

I Scientific Highlights

s-Process contribution to Sn-115 [1]
HAYAKAWA, Takehito, SHIZUMA, Toshiyuki, CHIBA, Satoshi, HATSUKAWA, Yuichi
IWAMOTO, Nobuyuki, SHINOHARA, Nobuo, HARADA, Hideo(JAEA)

KAJINO, Toshitaka(NAOJ / University of Tokyo)

The astrophysical origin of rare isotopes 115Sn has
been a long-standing puzzle [2]. It was suggested that βunstable isomers in stable isotopes may have importantrole for nucleosynthesis of this neutron-deficient isotope
as shown in Fig. 1 [3]. The isotope 115Sn may be produced
by a weak branch of the s-process through an isomerin 113Cd. However, a neutron capture cross-section for
the 112Cd(n, γ)113Cdm reaction has not beem emassured
yet. We have measured this cross section by using thecadmium-difference method with neutrons provided froma nuclear reactor, and discuss the s-process contribution
to the solar abundance of 115Sn.
The isomer in 113 Cd β-decays dominantly to theground state of the daughter nucleus 113 In with abranching ratio of 99.86 % (see Fig. 2). This isomer also
decays to its ground state through an internal 263.59-keV
γ- transition with a branching ratio of 0.14 %. Thus, we
obtain the neutron capture cross-section by measuringof the internal 263.59-keV γ-ray. Two sets of a 112Cd foilenriched to 98.27 % and an Al-Co wire were irradiatedwith neutrons provided from a nuclear reactor JRR-3
at the Japan Atomic Energy Agency (JAEA). One setof the samples was irradiated with a cover of natural
cadmium of 1-mm thickness, the other was irradiatedwithout Cd covers. After the neutron irradiation of aperiod of two hours, the samples were cooled in a waterpool in order to reduce background γ-rays emitted fromshort-lived radioactivities. The γ-rays from the activatedsamples were measured by a HPGe detector with a lowbackground environment 8 and 14 months after theneutron irradiation.
We obtain the thermal neutron capture cross-sectionof 0.028 ± 0.009 [b] and the resonance integral of 1.1 ±0.3 [b] using a cadmium difference method. The crosssection ratio of the isomer to the ground state has been
calculated as a function of the incident neutron energy,
E, by using a statistical model. The calculated ratios arealmost constant over a wide range of E < 100 keV. We
have evaluated the s-process contribution to the solar
abundance of 115Sn using the classical steady-flow modelwith various astrophysical parameters. This calculated
results have shown that the production through 113Cdm
may give minor contribution to the solar abundance of115Sn.

112

Sn

114

Sn

115

Sn

113

In

113

In

Sn

117

In m

116

115

In

116

114

Cd

116

115

s-process
111
110

Cd

Cd

111

m

113
112

Cd

Cd

Cd

113

m

115

Inm
In

Cdm

115

Cd

Sn

Cd

r-processFigure 1: Schematic view of nucleosynthesis of 115Sn.

Neutron Capture

0+

112 Cd11/2 Beta decay
99.86 %

9/2+

1/2+

264

T =14.1 yr

0.14 % 1/2

0

113 Cd113 InFigure 2: Partical decay scheme of 113Cd.

References[1] Hayakawa, et al.: 2009, ApJ, 707, 859.
[2] N´emeth, Zs., et al.: 1994, ApJ, 426, 357.
[3] Ward, R.A., et al.: 1976, ApJ, 31, 33.

I Scientific Highlights

043

Neutrino-nucleus reactions via neutral and charged currents
by the Quasi-particle Random Phase Approximation(QRPA)CHEOUN, Myung-Ki

KIM, Kyungsik(1)where F(α) is a nomalization factor. T and α can bechosen for neutrino types. Cross sections via CC aremuch larger, about 3 times, than those by NC, irrespectiveof nuclear species. Applications to the ν-process forrelevant nuclear abundances are in progress.
The QRPA is a very efficient method to consider
multiparticle and multi-hole interactions and theirconfiguration mixing. It successfully described nuclear
reactions sensitive on the nuclear structure, such as
the nuclear β ±, 2ν2β and 0ν2β decays. Therefore theuncertainties due to the nuclear structure in ν(ν̄) − Areactions can be pinned down to some extent byreproducing the data related to the β and ββ decays.
Since the present discussions are based on the

I Scientific Highlights(Kangwon University)

nondeformed spherical QRPA, one needs to exploit
the deformed QRPA [3, 4] for the nucleosynthesis ofdeformed nuclei, which are expected to be synthesized
frequently in core collapsing SN explosions. Suchextension of the QRPA calculation for ν − A reactions isin progress. It also enables us to perform various nuclear
weak reactions for unstable exotic nuclei.
200
Ni56-NC-AEN
2

We applied the QRPA to ν( ν̄) − A reactions by
including multipole transitions up to Jπ = 4± state withfinite momentum transfers and evaluated cross sectionsof ν- reactions on 12C, 56Ni and 56Fe target nucleus. Our
results for ν(ν̄) − A reactions show quite consistent resultswith available experimental data and other theoretical
calculations [1].
Remarkable points from our results are summarized
as follows. Firstly, not only GT, IAS and spin dipole
transitions but also other multipole transitions could
play roles for ν(ν̄) − A reactions via CC. However, NC
reactions are dominated by the GT transition.
Secondly, np pairing as well as nn and pp pairingcorrelations, which act as important ingredients fordescribing the BCS ground state and the QRPA excitedstates, may contribute to large extent to cross sections ofν(ν̄) − A reactions. In particular, we showed that it affects
results for medium heavy nuclei such as 56Ni and 56Fe,
which was already expected from our previous results for2ν2β and 0ν2β decays.
Finally, for more exact evaluations within a few %for the flux averaged cross section expected from thewould-be experiment, more deliberate calculations of the
Coulomb correction are of importance [2]. In particular,
experimental data via NC reactions are highly desirable
to pin down the ambiguities on the Coulomb correction,
because they are not subject to the Coulomb distortion.
For the application to the SN explosions, in Fig. 1,
we summarize the cross sections averaged by the SN
neutrino spectrum.

044

SO, W.Y(Korea Aerospace University)

cm )KAJINO, Toshitaka(NAOJ / University of Tokyo)(Soongsil University)

Ni56-NC-EN

20

Fe56-CC-EN

-42

		

HA, Eunja, LEE, Su Youn

(NAOJ / Soongsil University)		

σν (10		

C12-NC-EN
C12-NC-MN

2

C12-NC-AMN
C12-CC-EN

0.2

4

6

8

10
Tν (MeV)12

14

Figure 1: Temperature dependence of the energy weighted crosssection for ν− 12C, - 56Ni and - 56Fe reactions, where
neutrino spectrum for the SN, Eq.(1), is exploited.

References[1] Cheoun, M.-K., et al.: 2010, J. of Phys. G, 37, 055101.
[2] Cheoun, M.-K., et al.: 2010, PRC, 81, 028501.
[3] Simkovic, F., et al.: 2003, PRC, 68, 054319.
[4] Simkovic, F., et al.: 2004, Nuc. Phys. A, 733, 321.

Imaging Spectroscopy on Preflare Coronal Nonthermal Sources
Associated with the 2002 July 23 Flare
ASAI, Ayumi, NAKAJIMA, Hiroshi, SHIMOJO, Masumi(NAOJ)YOKOYAMA, Takaaki(University of Tokyo)		

MASUDA, Satoshi

Nonthermal emissions from accelerated particles
are often observed in hard X-rays (HXRs), γ-rays, andmicrowaves at the beginning of a solar flare. Althoughthese nonthermal emissions are undoubtedly associatedwith intense energy release processes, the mechanisms toaccelerate particles are still unclear. The HXR nonthermal
emission is explained with the bremsstrahlung emission,
which is emitted by the nonthermal electrons withenergies E > 20 keV. In the microwave range, on the other
hand, the gyrosynchrotron emission is the most promisingfor nonthermal emission. The microwave-emitting
electrons have relatively higher energies (~1 MeV).
Although HXR and microwave emissions have showna lot of similarities, it has been also reported that anelectron spectral index derived from HXR emissions isoften larger (softer) than that derived from microwave
emissions, and the temporal behaviors of the spectral
indices are totally different between HXR and microwave.
In order to study such similarities/dissimilarities on
the nonthermal emissions, we examined in detail thecoronal nonthermal emissions during the preflare phaseof the X4.8 flare that occurred on 2002 July 23, spatially,
temporally and spectroscopically [1]. In the previous
paper [2], we reported that nontheral emission sources
are clearly seen in microwaves and in HXRs during thepreflare phase (Fig. 1). By using the microwave dataobtained by Nobeyama Radioheliograph (NoRH), we
derived a spectral index for the microwave emission
source. By following the gyrosynchrotron emission
model, we further derived the spectral index of theaccelerated electron. Although the gyrosynchrotron
emission strongly depends on the magnetic field strength
in the corona, which is very difficult to measure, we
can roughly assume that B 0 = 150 gauss from other
TRACE 00:24:31UT
-200

NoRH

(University of California)

observational results. Finally, we got the spectral index
of about 4.7, and the number density of nonthermal
electrons as N20keV ~ 4.8 × 108 electrons cm−3 with thelow energy cut-off of 20 keV.
Then, we investigate the spectral index of the HXR
emission source by using the Reuven Ramaty HighEnergy Solar Spectroscopic Imager (RHESSI) data.
The intensity of the core region clearly shows thepower-law distribution. We could adopt the thin-target
bremsstrahlung model to derive an electron power-law
index, since the HXR source is located on the loop-top,where is almost the same location as the nonthermal
emission source seen in microwaves. Assuming the thintarget model for the HXR emission, the spectral index
of the accelerated electrons is derived as 4.7, whichis almost the same as that from the NoRH microwave
data. This implies that the distribution of the accelerated
electrons follows a single power-law. We can further
estimate the number density of the HXR-emitting electronin the core region to be N20keV = 5.1×106 electrons cm−3with the lower energy cut-off of 20 keV. These resultson the accelerated electrons are, however, about twoorders of magnitude less than those from the microwave
emission.
The gap of the number density is reduced if we
assume low ambient plasma density for the HXR-emitting
region. If we adopt the thick-target model for the HXR
emission source, however, the electron spectral index(~6.7) is much different, while the gap of the number
density of the accelerated electrons is somewhat reduced.
References[1] Asai, A., et al.: 2009, ApJ, 695, 1623.
[2] Asai, A., et al.: 2006, PASJ, 58, L1.

00:23:00-00:23:40UT NoRH -map

RHESSI 00:22:30-00:24:06UT

flare ribbons

KRUCKER, Säm(Nagoya University)

-4

-2

-900

-880

0

2

flare ribbons

-220
-240
-260

flare loops

-900

-880

(a)
-860

(b)
-900

-880

-860

(c)

flare loops

(d)

-860

Figure 1: Images for the preflare phase of the flare. (a) the EUV image taken with TRACE 195 Å at 00:24:31 UT. (b) (c) show the microwave
image of NoRH 34 GHz and the map of NoRH α index. (d) shows the positions of the flare ribbons (dark gray regions) and the flare
loops (light gray). We overlaid the contour images of NoRH 34 GHz and of the RHESSI 30–40 keV with the white dashed and withblack solid lines, respectively.

I Scientific Highlights

045

Multiple Plasmoid Ejections and Associated Hard X-ray Bursts
in the 2000 November 24 FlareNISHIZUKA, Naoto, TAKASAKI, Hiroyuki, SHIBATA, Kazunari				(Kyoto University)			

046

I Scientific Highlights

ASAI, Ayumi(NAOJ)

Figure 1: The snapshot images of multiple plasmoid ejectionsasociated with a flare on 2000 November 24 taken with
Yohkoh/SXT. Each plasmoid ejection is marked with acolored circle.

(a)

10 -3

(b)
o

GOES 1.0-8.0 A

X 10
Yohkoh/HXT
H-band[W m-2 ]We present an examination of the GOES X2.3 classflare that occurred at 14:51 UT on 2000 November 24 [1].
The Soft X-ray Telescope (SXT) on board Yohkoh
revealed that the a soft X-ray emitting plasma ejection, or
plasmoid ejection, is sometimes observed in solar flares.
It was also found that the plasmoids show blob-like orloop-like shapes and that the strong acceleration of theplasmoid ejection occurs during the peak time of the hard
X-ray emission. Their ejection velocities are typicallyseveral hundred km s−1 and the ejected plasma is heatedto more than 10 MK before the onset of the ejection.
The standard CSHKP flare model, which includes
a filament/ plasmoid ejection, was extended, to unify
reconnection and plasmoid ejection. The modelstresses the importance of the plasmoid ejection ina reconnection process, and is called the “plasmoidinduced reconnection” model. The plasmoid, in thatmodel, inhibits reconnection and stores magnetic energy
in a current sheet. However, once it is ejected, inflow is
induced because of the mass conservation, resulting in
the enhancement of reconnection rate and the accelerationof the plasmoid due to the faster reconnection outflow.
Reconnection theories, furthermore, predict several
plasmoids of various scales are generated. The dynamics
of plasmoid formation in the solar flare and theirsubsequent plasmoid ejection affect the reconnection ratein the nonlinear evolution. Therefore, plasmoid ejections
are observational evidence of magnetic reconnection ofsolar flares.
In the SXT images we found “multiple” plasmoid
ejections with velocities in the range of 250–1500 km/s
(Fig. 1). Furthermore, we also found that each plasmoid
ejection is associated with an impulsive burst of hard
X-ray emission (Fig. 2). Although some correlation
between plasmoid ejection and hard X-ray emission has
been discussed previously, our observation shows similar
behavior for multiple plasmoid ejection such that eachplasmoid ejection occurs during the strong energy releaseof the solar flare. As a result of temperature- emission
measure analysis of such plasmoids, it was revealed
that the apparent velocities and kinetic energies of theplasmoid ejections show a correlation with the peakintensities in the hard X-ray emissions.

		

M 10

Figure 2: (a) Apparent height of the ejected plasmoids. Timeslice image is obtained with Yohkoh/SXT. The signs areplotted over the time slice image in figure. (b) Counting
rates of hard X-ray emission observed with the H-band(52.7–92.8 keV channel) of Yohkoh/HXT and thecorresponding GOES soft X-ray light curve.

Reference[1] Nishizuka, N., Takasaki, H., Asai, A., Shibata, K.: 2010, ApJ,
711, 1062.

II Publications, Presentations
1. Refereed Publications
Abazajian, K. N., et al. including Ichikawa, S.: 2009, The Seventh
Data Release of the Sloan Digital Sky Survey, ApJS, 182,
543-558.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, An upper limit on thestochastic gravitational-wave background of cosmologicalorigin, Nature, 460, 990-994.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Einstein@Home searchfor periodic gravitational waves in early S5 LIGO data, Phys.
Rev. D, 80, 42003.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, First LIGO search forgravitational wave bursts from cosmic(super) strings, Phys. Rev.
D, 80, 62002.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, LIGO: the Laser Interferometer Gravitational-Wave Observatory, Rep. Prog. Phys.,
72, 76901.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Observation of a kilogramscale oscillator near its quantum ground state, New J. Phys., 11,73032.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Search for gravitational
wave ringdowns from perturbed black holes in LIGO S4 data,
Phys. Rev. D, 80, 62001.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Search for gravitational
waves from low mass binary coalescences in the first year of
LIGO’s S5 data, Phys. Rev. D, 79, 122001.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Search for gravitational
waves from low mass compact binary coalescence in 186 daysof LIGO’s fifth science run, Phys. Rev. D, 80, 47101.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Search for gravitationalwave bursts in the first year of the fifth LIGO science run, Phys.
Rev. D, 80, 102001.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Search for high frequency
gravitational-wave bursts in the first calendar year of LIGO's
fifth science run, Phys. Rev. D, 80, 102002.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2009, Stacked Search for
Gravitational Waves from the 2006 SGR 1900+14 Storm, ApJ,
701, L68-L74.
Abbott, B. P., et al. including Ballmer, S., Kawamura, S., Majorana,E., Nishizawa, A., Sakata, S.: 2010, Searches for Gravitational
Waves from Known Pulsars with Science Run 5 Ligo Data, ApJ,

713, 671-685.
Abdo, A. A., et al. including Kino, M., Nagai, H.: 2009, Multiwavelength Monitoring of the Enigmatic Narrow-Line Seyfert 1
PMN J0948+0022 in 2009 March-July, ApJ, 707, 727-737.
Abdo, A. A., et al. including Yamashita, T.: 2010, PKS 1502+106:
A New and Distant Gamma-ray Blazar in Outburst Discoveredby the Fermi Large Area Telescope, ApJ, 710, 810.
Agatsuma, K., Uchiyama, T., Yamamoto, K., Ohashi, M.,
Kawamura, S., Miyoki, S., Miyakawa, O., Telada, S., Kuroda,
K.: 2010, Direct measurement of thermal fluctuation of high-Q
pendulum, Phys. Rev. Lett., 104, 40602.
Akitaya, H., Ikeda, Y., Kawabata, K. S., Matsuda, K., Okazaki, A.,
Seki, M.: 2009, Linear polarization in forbidden lines of the T
Tauri star RY Tauri, A&A, 499, 163.
Amaro-Seoane, P., Sesana, A., Hoffman, L., Benacquista, M., Eichhorn,C., Makino, J., Spurzem, R.: 2010, Triplets of supermassive
black holes: astrophysics, gravitational waves and detection,
MNRAS, 402, 2308-2320.
Ando, M., et al. including Kawamura, S., Fujimoto, M.,
Fukushima, M., Ishizaki, H., Kotake, K., Nakamura, K.,
Nishizawa, A., Obuchi, Y., Okada, N., Takahashi, R., Torii,
Y., Ueda, A., Yamazaki, T.: 2009, DECIGO pathfinder, Class.
Quantum Grav., 26, 94019.
Aoki, W., Arimoto, N., Sadakane, K., Tolstoy, E., Battaglia,
G., Jablonka, P., Shetrone, M., Letarte, B., Irwin, M., Hill,
V., Francois, P., Venn, K., Primas, F., Helmi, A., Kaufer, A.,
Tafelmeyer, M., Szeifert, T., Babusiaux, C.: 2009, Chemicalcomposition of extremely metal-poor stars in the Sextans dwarf
spheroidal galaxy, A&A, 502, 569.
Aoki, W., Barklem, P. S., Beers, T. C., Christlieb, N., Inoue, S.,
García Pérez, A. E., Norris, J. E., Carollo, D.: 2009, Lithium
Abundances of Extremely Metal-Poor Turnoff Stars, ApJ, 698,
1803.
Arai, A., et al. including Okita, K., Yoshida, M., Yanagisawa, K.:
2009, Anti-Correlation of Near-Infrared and X-Ray Variationsof the Microquasar GRS 1915+105 in the Soft State, PASJ, 61,
L1-L5.
Arai, K., et al. including Takahashi, R., Tatsumi, D., Izumi, K.,
Wakabayashi, Y., Ishizaki, H., Fukushima, M., Yamazaki, T.,
Fujimoto, M.-K.: 2009, Status of Japanese gravitational wave
detectors, Class. Quantum Grav., 26, 204020.
Araki, H., Tazawa, S., Noda, H., Migita, E., Kamiya, I., Kawano,N., Sasaki, S.: 2009, Preliminary Results of the Lunar
Topography by KAGUYA-LALT Mission, Transaction ofJapan Society for Aeronautical and Space Sciences, Aerospace
Technology Japan, 7, Tk_23-Tk_25.
Ariyoshi, S., Taino, T., Dobroiu, A., Sato, H., Matsuo, H., Otani,C.: 2009, Terahertz detector based on a superconducting tunnel
junction coupled to a thin superconductor film, Appl. Phys.
Lett., 95, 193504.
Asai, A., Nakajima, H., Shimojo, M., Yokoyama, T., Masuda, S.,
Krucker, Säm: 2009, Imaging Spectroscopy on Preflare Coronal

II Publications, Presentations047

Nonthermal Sources Associated with the 2002 July 23 Flare,
ApJ, 695, 1623-1630.
Asayama, S., Kamikura, M.: 2009, Development of DoubleRidged Wavegide Orthomode Transducer for the 2 MM Band,
Int. J. Infrared Millimeter Waves, 30, 573-579.
Baba, J., Asaki, Y., Makino, J., Miyoshi, M., Saitoh, T. R.,
Wada, K.: 2009, The origin of large peculiar motions of starforming regions and spiral, ApJ, 706, 471-481.
Barker, M. K., Ferguson, A. M. N., Irwin, M., Arimoto, N.,
Jablonka, P.: 2009, Resolving the Stellar Outskirts of M81:
Evidence for a Faint, Extended Sgtructural Components, AJ,
138, 1469-1484.
Bedding, T. R., et al. including Kambe, E., Ando, H., Izumiura, H.:
2010, A Multi-Site Campaign to Measure Solar-Like Oscillationsin Procyon. II. Mode Frequencies, ApJ, 713, 935-949.
Bisterzo, S., Gallino, R., Straniero, O., Aoki, W.: 2009, Interpretation of CEMP(s) and CEMP(s + r) Stars with AGB Models,
PASA, 26, 314.
Bouy, H., Huélamo, N., Barrado Y Navascués, D., Martín, E. L.,
Petr-Gotzens, M. G., Kolb, J., Marchetti, E., Morales-Calderón,M., Bayo, A., Artigau, E., Hartung, M., Marchis, F., Tamura,
M., Sterzik, M., Köhler, R., Ivanov, V. D., Nürnberger, D.:2009, A deep look into the core of young clusters. II. λ-Orionis,
A&A, 504, 199-209.
Brooks, D. H., Warren, H. P., Williams, D. R., Watanabe, T.:2009, Hinode/Extreme-Ultraviolet Imaging Spectrometer
Observations of the Temperature Structure of the Quiet Corona,
ApJ, 705, 1522-1532.
Burningham, B., et al. including Tamura, M.: 2009, The discoveryof an M4+T8.5 binary system, MNRAS, 395, 1237-1248.
Campisi, M. A., Vignali, C., Brusa, M., Daddi, E., Comastri,A., Possetti, L., Alexandre, D. M., Renzini, A., Arimoto, N.,
Kong, X.: 2009, On the nature of red galaxies: the Chandra
perspective, A&A, 501, 485-494.
Chassefiere, E., et al. including Sasaki, S.: 2010, PHEBUS: A
double ultraviolet spectrometer to observe Mercury’s exosphere,
Planet. Space Sci., 58, 201-223.
Cheoun, M. K., Ha, E., Kim, K. M., 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. M., So, W. Y., Kajino,
T.: 2010, Neutrino reactions on C 12 by the quasiparticle
random-phase approximation, Phys. Rev. C, 81, 28501.
Codella, C., Cesaroni, R., López-Sepulcre, A., Beltrán, M. T.,
Furuya, R., Testi, L.: 2010, Looking for high-mass youngstellar objects: H2O and OH masers in ammonia cores, A&A,
510, A86.
Dawson, K. S., et al. including Hattori, T., Kashikawa, N.,
Morokuma, T., Takanashi, N.: 2009, An Intensive Hubble
Space Telescope Survey for z>1 Type Ia Supernovae byTargeting Galaxy Clusters, AJ, 138, 1271.
Desmet, M., Briquet, M., Thoul, A., Zima, M., De Cat, P., Handler,G., Ilyin, I., Kambe, E., Krzesinski, J., Lehmann, H., Masuda,S., Mathias, P., Mkrtichian, D. E., Telting, J., Uytterhoeven,K., Yang, S. L. S., Aerts, C.: 2009, An asteroseismic studyof the beta Cephei star 12 Lacertae: multisite spectroscopic048

II Publications, Presentations

observations, mode identification and seismic modelling,
MNRAS, 396, 1460.
Doherty, M., et al. including Kodama, T.: 2009, Optical and nearIR spectroscopy of candidate red galaxies in two z~2.5 protoclusters, A&A, 509, 83.
Doi, A., et al. including Kawaguchi, N., Kono, Y., Oyama,T., Yamauchi, A.: 2009, VLBI Detections of Parsec-Scale
Nonthermal Jets in Radio-Loud Broad Absorption Line Quasars,
PASJ, 61, 1389-1398.
Endo, A., Noguchi, T., Kroug, M., Shitov, S. V., Shan, W., Tamura,T., Kojima, T., Uzawa, Y., Sakai, T., Inoue, H., Kohno, K.:
2009, A THz SIS Mixer with a NbTiN-Ground Plane and SIS
Microtrilayers Directly Grown on a Quartz Substrate, IEEE
Trans. Appl. Supercond., 19, 400-404.
Enomoto, R., et al. including Mizumoto, Y.: 2009, CANGAROOIII Observation of TeV Gamma Rays from the Vicinity of PSR
B1706-44, ApJ, 703, 1725-1733.
Espada, D., Matsushita, S., Peck, A., Henkel, C., Iono, D., Israel, F.
P., Muller, S., Petitpas, G., Pihlstroem, Y., Taylor, G. B., DinhV-Trug: 2009, Disentangling the Circumnuclear Environs ofCentaurus A: I. High Resolution Molecular Gas Imaging, ApJ,
695, 116-134.
Förster, S., et al. including Arimoto, N.: 2009, The SINS Survey:
SINFONI Integral Field Spectroscopy of z~2 Star-forming
Galaxies, ApJ, 706, 1364-1428.
Freyhammer, L. M., Kurtz, D. W., Elkin, V. G., Mathys, G.,
Savanov, I., Zima, W., Shibahashi, H., Sekiguchi, K.: 2009, A
3D study of the photosphere of HD99563 - I. Pulsation analysis,
MNRAS, 396, 325-342.
Friesen, R. K., Di Franesco, J., Shimajiri, Y., Takakuwa, S.: 2010,
The Initial Conditions of Clusteres Star Formation II: N 2H+
Observations of the Ophiuchus B Core, ApJ, 708, 1002-1024.
Fujii, M., Iwasawa, M., Funato, Y., Makino, J.: 2009, Trojan
Stars in the Galactic Center, ApJ, 695, 1421-1429.
Fujimura, D., Tsuneta, S.: 2009, Properties of Magnetohydrodynamic Waves in the Solar Photosphere Obtained with
Hinode, ApJ, 702, 1443-1457.
Fujishita, M., Torii, K., Kudo, N., Kawase, T., Yamamoto, H.,
Kawamura, A., Mizuno, N., Onishi, T., Mizuno, A., Machida,M., Takahashi, K., Nozawa, S., Matsumoto, R., Fukui, Y.:
2009, Discovery of Molecular Loop 3 in the Galactic Center:
Evidence for a Positive-Velocity Magnetically Floated Loop
towards L = 355°–359°, PASJ, 61, 1039-1053.
Fujiwara, H., Yamashita, T., Ishihara, D., Onaka, T., Kataza, H.,
Ootsubo, T., Fukagawa, M., Marshall, J. P., Murakami, H.,
Nakagawa, T., Hirao, T., Enya, K., White, G. J.: 2009, Hot
Debris Dust Around HD 106797, ApJ, 695, L88.
Fujiwara, M., Sasaki, M., Nagata, H., Matsuo, H.: 2009, Opticalcontrol of low frequency noise behavior in cryogenic GaAs
junction field effect transistor, Cryogenics, 49, 626-629.
Fukagawa, M., Itoh, Y., Tamura, M., Oasa, Y., Hayashi, S. S.,
Fujita, Y., Shibai, H., Hayashi, M.: 2009, H-Band Image ofa Planetary Companion Around HR 8799 in 2002, ApJ, 696,
L1-L5.
Fukui, Y., Furukawa, N., Dame, T. M., Dawson, Joanne R.,
Yamamoto, H., Rowell, G. P., Aharonian, F., Hofmann, W., deOña Wilhelmi, E., Minamidani, T., Kawamura, A., Mizuno,N., Onishi, T., Mizuno, A., Nagataki, S.: 2009, A Peculiar Jet
and Arc of Molecular Gas toward the Rich and Young Stellar
Cluster Westerlund 2 and a TeV Gamma Ray Source, PASJ, 61,
L23-L27.
Fukui, Y., Kawamura, A., Wong, T., Murai, M., Iritani, H.,
Mizuno, N., Mizuno, Y., Onishi, T., Hughes, A., Ott, J., Muller,
E., Staveley-Smith, L., Kim, S.: 2009, Molecular and Atomic
Gas in the Large Magellanic Cloud. II. Three-dimensional
Correlation Between CO and HI, ApJ, 705, 144-155.
Fukushima, T.: 2009, Efficient Solution of Initial-Value Problem
of Torque-Free Rotation, AJ, 138, 210-218.
Fukushima, T.: 2009, Fast Computation of Jacobian Elliptic
Functions and Incomplete Elliptic Integrals for Constant Valuesof Elliptic Parameter and Elliptic Characteristic, Celest. Mech.
Dyn. Astron., 105, 245-260.
Fukushima, T.: 2009, Fast Computation of Complete Elliptic
Integrlals and Jacobian Elliptic Functions, Celest. Mech. Dyn.
Astron., 105, 305-328.
Furukawa, N., Dawson, J. R., Ohama, A., Kawamura, A., Mizuno,N., Onishi, T., Fukui, Y.: 2009, Molecular Clouds Toward
RCW49 and Westerlund 2: Evidence for Cluster Formation
Triggered by Cloud-Cloud Collision, ApJ, 696, L115-L119.
Furuya, R. S., Shinnaga, H.: 2009, High-velocity Molecular
Outflow in CO J = 7–6 Emission from the Orion Hot Core, ApJ,
703, 1198.
García Pérez, A. E., Aoki, W., Inoue, S., Ryan, S. G., Suzuki, T. K.,
Chiba, M.: 2009, 6Li/7Li estimates for metal-poor stars, A&A,
504, 213.
Goossens, S., Matsumoto, K., Ishihara, Y., Liu, Q., Kikuchi, F.,
Noda, H.: 2009, Results for Orbit Determination of the Three
Satellites of Kaguya, J. Geodetic Soc. Jpn., 55, 255-268.
Goto, T., Utsumi, Y., Furusawa, H., Miyazaki, S., Komiyama,
Y.: 2009, A QSO host galaxy and its Lyα emission at z = 6.43,
MNRAS, 400, 843.
Guyon, O., Pluzhnik, E., Martinache, F., Totems, J., Tanaka, S.,
Matsuo, T., Blain, C., Belikov, R.: 2010, High-Contrast
Imaging and Wavefront Control with a PIAA Coronagraph:
Laboratory System Validation, PASP, 122, 71-84.
Hachisuka, K., Brunthaler, A., Menten, K. M., Reid, M. J.,
Hagiwara, Y., Mochizuki, N.: 2009, The Distance to a StarForming Region in the Outer Arm of the Galaxy, AJ, 696,
1981-1986.
Hamana, T., Miyazaki, S., Kashikawa, N., Ellis, R. S., Massey,
R. J., Refregier, A., Taylor, J. E.: 2009, Subaru Weak-Lensing
Survey II: Multi-Object Spectroscopy and Cluster Masses,
PASJ, 61, 833.
Hanada, H., Iwata, T., Namiki, N., Kawano, N., Sasaki, S.,
Matsumoto, K., Noda, H., Tsuruta, S., Asari, K., Ishikawa,T., Kikuchi, F., Liu, Q., Goossens, S., Ishihara, Y., Petrova,N., Harada, Y., Shibata, K., Iwadate, K., Kameya, O., Tamura,Y., Hong, X., Ping, J., Aili, Y., Ellingsen, S., Schlueter, W.:2009, Exploration of Lunar Gravity by VLBI Observationsof SELENE (KAGUYA), Transaction of Japan Society for
Aeronautical and Space Sciences, Aerospace Technology Japan,
7, Tk_1-Tk_5.

Hanawa, T., Ochi, Y., Ando, K.: 2010, Gas Accretion from a
Circumbinary Disk, ApJ, 708, 485-497.
Hara, H.: 2009, Differential Rotation Rate of X-ray Bright
Points and Source Region of Their Magnetic Fields, ApJ, 697,
980-984.
Harikae, S., Takiwaki, T., Kotake, K.: 2009, Long-Term
Evolution of Slowly Rotating Collapsar in Special Relativistic
Magnetohydrodynamics, ApJ, 704, 354-371.
Hasegawa, K., Umemura, M., Susa, H.: 2009, Radiative Regulationof Population III Star Formation, MNRAS, 395, 1280-1286.
Hashimoto, S., Ogata, K., Chiba, S., Yahiro, M.: 2009, New
Approach for Evaluating Incomplete and Complete Fusion
Cross Sections with Continuum-Discretized Coupled-Channels
Method, Prog. Theo. Phys., 122, 1291-1300.
Hashimoto, T., et al. including Kajino, T.: 2009, A new measurementof the astrophysical Li8(d,t)Li7 reaction, Phys. Lett. B, 674,
276-280.
Hatsukade, B., et al. including Iono, D., Ezawa, H., Kawabe, R.,
Nakanishi, K.: 2010, Unveiling the Nature of Submillimeter
Galaxy SXDF 850.6, ApJ, 711, 974-979.
Hatsukade, B., Iono, D., Motohara, K., Nakanishi, K., Hayashi,
M., Shimasaku, K., Nagao, T., Tamura, Y., Malkan, M., Ly, C.,
Kohno, K.: 2009, A Search for Molecular Gas toward a BzKSelected Star-Forming Galaxy at z = 2.044, PASJ, 61, 487-491.
Hatsutori, Y., Shinichi, N.: 2009, A Study on Vibration Isolator for
Reaction Wheel Assembly, Transactions of the Japan Society
for Aeronautical and Space Sciences, Space Technology Japan,
7, Pd_69-Pd_73.
Hatsutori, Y., Suganuma, M., Kobayashi, Y., Gouda, N., Yano,
T., Yamada, Y., Yamauchi, M.: 2009, A Very Small Astrometry
Satellite, Nano-JASMINE: Its Telescope and Mission Goals,
Transactions of the Japan Society for Aeronautical and Space
Sciences, Space Technology Japan, 7, Tm_19-Tm_23.
Hayakawa, T., Shizuma, T., Chiba, S., Kajino, T., Hatsukawa, Y.,
Iwamoto, N., Shinohara, N., Harada, H.: 2009, Neutron capture
cross-section to Cd113 isomer and s-process contribution to rare
p-nuclide Sn115, ApJ, 707, 859-865.
Hayakawa, T., Shizuma, T., Kajino, T., Ogawa, K., Nakada,N.: 2009, Reply to Comment on La 138-Ce 138-Ce 136 nuclear
cosmochronometer of supernova neutrino process, Phys. Rev. C,
79, 59802.
Hayashi, M., Kodama, T., Koyama, Y., Tanaka, I., Shimasaku, K.,
Okamura, S.: 2010, High star formation activity in the central
region of a distant cluster at z=1.46, MNRAS, 402, 1980-1990.
Hayashi, Sei., et al. including Mizumoto, Y.: 2009, Search for
VHE gamma rays from SS433/W50 with the CANGAROO-II
telescope, Astropart. Phys., 32, 112-119.
Hibi, Y., Matsuo, H., Arai, H., Nagata, H., Ikeda, H., Fujiwara,
M.: 2009, The cryogenic multiplexer and shift register for
submillimeter-wave digital camera, Cryogenics, 49, 672-675.
Higuchi, A. E., Kurono, Y., Saito, M., Kawabe, R.: 2009, A
Mapping Survey of Dense Clumps Associated with Embedded
Clusters: Evolutionary Stages of Cluster-Forming Clumps, ApJ,
705, 468-482.
Hioki, T., Itoh, Y., Oasa, Y., Fukagawa, M., Kudo, T., Mayama, S.,
Pyo, T.-S., Hayashi, M., Hayashi, S. S., Ishii, M., Tamura,

II Publications, Presentations049

M.: 2009, High-Resolution Near-Infrared Images of the T Tauri
Binary System XZ Tauri, PASJ, 61, 1271-1279.
Hirashita, H., Omukai, K.: 2009, Dust coagulation in starformation with different metallicities, MNRAS, 399, 1795-1801.
Hirota, A., Kuno, N., Sato, N., Nakanishi, H., Tosaki, T., Matsui, H.,
Habe, A., Sorai, K.: 2009, Determination of the Pattern Speedof Barred Spiral Galaxies, PASJ, 61, 441-450.
Hirota, T., Ohishi, M., Yamamoto, S.: 2009, A Search for CarbonChain-rich Cores in Dark Clouds, ApJ, 699, 585-602.
Hosokawa, T., Omukai, K.: 2009, Low-Metallicity Protostars andthe Maximum Stellar Mass Resulting from Radiative Feedback:Spherically Symmetric Calculations, ApJ, 703, 1810-1818.
Huang, G., Nakajima, H.: 2009, Statistical Analysis of Flaring
Loops Observed by Nobeyama Radioheliograph. I. Comparisonof Looptop and Footpoints, ApJ, 696, 136-142.
Huang, G., Nakajima, H.: 2009, Statistics of Flaring Loops
Observed by Nobeyama Radioheliograph. II. Spectral Evolution,
ApJ, 702, 19-26.
Hwang, N., Lee, M. G.: 2010, Vestige of the Star Cluster Burst in
M51, ApJ, 709, 411-423.
Ichihashi, Y., Masuda, N., Tsuge, M., Nakayama, H., Shiraki, A.,
Shimobaba, T., Ito, T.: 2009, One-unit system to reconstruct a
3-D movie at a video-rate via electroholography, Opt. Express,
17(22), 13895-13903.
Ichihashi, Y., Nakayama, H., Ito, T., Masuda, N., Shimobaba, T.,
Shiraki, A., Sugie, T.: 2009, HORN-6 special-purpose clusteredcomputing system for electroholography, Opt. Express, 17(16),13895-13903.
Iliev, I. T., et al. including Susa, H.: 2009, Cosmological radiativetransfer comparison project - II. The radiation-hydrodynamic
tests, MNRAS, 400, 1283-1316.
Imada, A., Henden, A., Kato, T., Moritani, Y., Sumiyoshi, M.,
Tanada, S., Omodaka, T., Ishioka, R., Uemura, M., Yanagisawa, K.,
Nogami, D.: 2009, Superhump Development during the 2005
Superoutburst of 1RXS J053234+624755, PASJ, 61, L17-L21.
Imada, A., Yasuda, T., Omodaka, T., Oizumi, S., Yamamoto, H.,
Tanada, S., Arao, Y., Kodama, K., Suzuki, M., Matsuo, T.,
Maehara, H., Kato, T., Sugiyasu, K., Moritani, Y., Sumiyoshi,M., Nakajima, K., Pietz, J., Yanagisawa, K., Nogami, D.: 2009,
CCD Photometry of a Newly Confirmed SU UMa-Type Dwarf
Nova, NSV 4838, PASJ, 61, 535-541.
Imada, S., Hara, H., Watanabe, T.: 2009, Ion Temperature and NonThermal Velocity in a Solar Active Region: Using Emission
Lines of Different Atomic Species, ApJ, 705, L208-L212.
Imai, H., He, J.-H., Nakashima, J., Ukita, N., Deguchi, S., Koning,N.: 2009, CO J=3–2 Emission from the "Water Fountain"
Sources IRAS 16342-3814 and IRAS 18286-0959, PASJ, 61,
1365-1372.
Imanishi, M., Maiolino, R., Nakagawa, T.: 2010, Spitzer Infrared
Low-Resolution Spectroscopic Study of Buried Active Galactic
Nuclei in a Complete Sample of Nearby Ultraluminous Infrared
Galaxies, ApJ, 709, 801-815.
Imaishi, M., Nakanishi, K., Yamada, M., Tamura, Y., Kohno,
K.: 2010, ASTE Simultaneous HCN(4–3) and HCO +(4–3)
Observations of the Two Luminous Infrared Galaxies NGC
4418 and Arp 220, PASJ, 62, 201-209.

050

II Publications, Presentations

Imanishi, M.: 2009, Luminous Buried Active Galactic Nuclei asa Function of Galaxy Infrared Luminosity Revealed throughSpitzer Low-resolution Infrared Spectroscopy, ApJ, 694,751-764.
Imanishi, Y., Tamura, Y., Ikeda, H., Okubo, S.: 2009, Permanent
gravity changes recorded on superconducting gravimeters fromearthquakes in central Japan–The Noto Hantou and Niigataken
Chuetsu-oki events in 2007, J. Geodyn., 48, 260-268.
Inoue, T., Inutsuka, S.-I.: 2009, Two-fluid MHD Simulationsof Converging HI Flows in the Interstellar Medium. II: Are
Molecular Clouds Generated Directly From Warm Neutral
Medium?, ApJ, 704, 161-169.
Iono, D., Wilson, C. D., Yun, M. S., Baker, A. J., Petitpas, G. R.,
Peck, A. B., Krips, M., Cox, T. J., Matsushita, S., Mihos, J.
C., Pihistrom, Y.: 2009, Luminous Infrared Galaxies with theSubmillimeter Array: II. Comparing the CO(3–2) Size andLuminosities of Local and High-Redshift Luminous Infrared
Galaxies, ApJ, 695, 1537-1549.
Ishigaki, M., Chiba, M., Aoki, W.: 2010, Chemical Abundances ofOuter Halo Stars in the Milky Way, PASJ, 62, 143.
Ishiguro, M., Usui, F., Sarugaku, Y., Ueno, M.: 2009, 2006
Fragmentation of Comet 73P/Schwassmann-Wachmann 3B
Observed with Subaru/Suprime-Cam, Icarus, 203, 560.
Ishihara, Y., Goossens, S., Matsumoto, K., Noda, H., Araki,
H., Namiki, N., Hanada, H., Iwata, T., Tazawa, S., Sasaki, S.:
2009, Crustal thickness of the Moon: Implications for farsidebasin structures, Geophys. Res. Lett., 36, L19202.
Ishii, S., Seta, M., Nakai, N., Nagai, S., Miyagawa, N., Yamauchi,A., Motoyama, H., Taguchi, M.: 2010, Site testing at Dome
Fuji for submillimeter and terahertz astronomy: 220 GHz
atomospheric-transparency, Polar Sci., 3, 213-221.
Ishiyama, T., Fukushige, T., Makino, J.: 2009, GreeM: Massively
Parallel TreePM Code for Large Cosmological N-body
Simulations, PASJ, 61, 1319-1330.
Ishiyama, T., Fukushige, T., Makino, J.: 2009, Variation of the
Subhalo Abundance in Dark Matter Halos, ApJ, 696, 2115-2125.
Isobe, N., Tashiro, M. S., Gandhi, P., Hayato, A., Nagai, H., Hada,
K., Seta, H., Matsuta, K.: 2009, Suzaku Observation of theGiant Radio Galaxy 3C 326, ApJ, 706, 454-463.
Ito, H., Aoki, W., Honda, S., Beers. T. C.: 2009, BD+44°493: A
Ninth Magnitude Messenger from the Early Universe; Carbon
Enhanced and Beryllium Poor, ApJ, 698, L37-L41.
Ito, M., Hayano, Y., Saito, Y., Takami, H., Saito, N., Akagawa,
K., Takazawa, A., Ito, M., Wada, S., Iye, M.: 2009, High-Power
Laser Beam Transfer through Optical Relay Fibers for a Laser
Guide Adaptive Optics System, PASJ, 61, 763-768.
Ito, T.: 2009, Asymmetric impacts of near-Earth asteroids on theMoon, Adv. Geosci., 15, 107-118.
Iwakami, W., Kotake, K., Ohnishi, N., Yamada, S., Sawada, K.:
2009, Spiral mode of standing accretion shock instability incore-collapse supernovae, ApJ, 700, 232-242.
Iwakami, W., Ohnishi, N., Kotake, K., Yamada, S., Sawada, K.:
2009, Spiral mode of standing accretion shock instability incore-collapse supernovae, Astrophys. Space Sci., 322, 43-47.
Iwata, T., Namiki, N., Hanada, H., Noda, H., Kawano, N.,
Matsumoto, K., Tsuruta, S., Liu, Q., Kikuchi, F., Minamino,

H., Sasaki, T.: 2009, Properties of SELENE Small Satellites for
Selenodetic Measurements: Rstar(OKINA) and Vstar(OUNA),
Transaction of Japan Society for Aeronautical and Space
Sciences, Aerospace Technology Japan, 7, Tk_33-Tk_37.
Jike, T., Manabe, S., Tamura, Y.: 2009, Result of VERA Internal
Geodetic VLBI with 1Giga-bps Recording in the First Three
Years, J. Geodetic Soc. Jpn., 55, 369-384.
Kadono, T., Sugita, S., Ootsubo, T., Sako, S., Miyata, T.,
Furusho, R., Honda, M., Kawakita, H., Watanabe, J.: 2010,
Interpretation on Deep Impact results: Radial Distribution of
Ejecta and the Size Distribution of Large-sized Grains, Earth,Planets and Space, 62, 13-16.
Kajino, H., Ohta, K. Iwata, I., Yabe, K., Yuma, S., Akiyama, M.,
Tamura, N., Aoki, K., Sawicki, M.: 2009, Lyman Break
Galaxies at z ~ 5: Rest-Frame UV Spectra. III, ApJ, 704, 117.
Kajino, T., Kojima, K., Yamazaki, D, Ichiki, K., Mathews, G.
J.: 2010, An alternative to inflation? Critical role of neutrino
anisotropic stress in CMB, Prog. Part. Nucl. Phys., 64, 378-380.
Kajisawa, M., Ichikawa, T., Tanaka, I., Konishi, M., Yamada,T., Akiyama, M., Suzuki, R., Tokoku, C., Uchimoto, Y. K.,
Yoshikawa, T., Ouchi, M., Iwata, I., Hamana, T., Onodera, M.:
2009, MOIRCS Deep Survey. IV. Evolution of Galaxy Stellar
Mass Function Back to z ~ 3, ApJ, 702, 1393.
Kamikura, M., Naruse, M., Asayama, S., Satou, N., Shan, W.,
Sekimoto, Y.: 2010, Development of a 385–500 GHz Orthomode
Transducer(OMT), J. Infrared, Millimeter, and Terahertz Waves,31, 697-707.
Kamio, S., Hara, H., Watanabe, T., Curdt, W.: 2009, Distributionof jets and magnetic fields in a coronal hole, A&A, 502, 345-353.
Kamohara, R., Bujarrabal, V., Honma, M., Nakagawa, A., Matsumoto,N., Oyama, T., Hirota, T., Imai, H., Shibata, K. M., Kobayashi,
H., Sato, K., Ueno, Y.: 2010, VERA observations of SiO maser
emission from R Aquarii, A&A, 510, A69.
Kaneda, H., Fouks, B., Yasuda, A., Murakami, N., Okada, Y.,
Coulais, A., Doi, Y., Fujiwara, M., Kawada, M., Matsuo, H.,
Takahashi, H.: 2009, Application of Photoconductor PhysicalTransient Model to Fourier Transform Spectrometer Data of
AKARI/Far-Infrared Surveyor(FIS), PASP, 121, 549-557.
Karr, J. L., Ohashi, N., Kudo, T., Tamura, M.: 2010, Candidate
Coronagraphic Detections of Protoplanetary Disks Around Four
Young Stars, AJ, 139, 1015-1027.
Kato, T., Pavlenko, E. P., Maehara, H., Nakajima, K., Andreev,
M., Shugarov, S. Y., de Ponthiere, P., Brady, S., Klingenberg,G., Shears, J., Imada, A., Yanagisawa, K.: 2009, SDSS
J080434.20+510349.2: Eclipsing WZ Sge-Type Dwarf Nova
with Multiple Rebrightenings, PASJ, 61, 601-613.
Kato, Y., Miyoshi, M., Takahashi, R., Negoro, H., Matsumoto,R.: 2010, Measuring spin of a supermassive black hole at the
Galactic centre, MNRAS, 403, L74-L78.
Kato, Y., Umemura, M., Ohsuga, K.: 2009, Three-dimensional
Radiative Properties of Hot Accretion Flows onto the Galactic
Centre Black Hole, MNRAS, 400, 1742-1748.
Kawabata, K. S., Tanaka, M., Maeda, K., Hattori, T., Nomoto,K., Tominaga, N., Yamanaka, M.: 2009, Extremely Luminous
Supernova 2006gy at Late Phase: Detection of Optical Emission
from Supernova, ApJ, 697, 747.

Kawagoe, S., Takiwaki, T., Kotake, K.: 2009, Neutrino oscillations
in magnetically driven supernova explosions, J. Cosmol.
Astropart. Phys., 9, 33.
Kawakatu, N., Kino, M., Nagai, H.: 2009, On the Origin ofFanaroff-Riley Classification of Radio Galaxies: Decelerationof Supersonic Radio Lobes, ApJ, 679, L173-L176.
Kawakatu, N., Wada, K.: 2009, Formation of High-redshift (z>6)
Quasars Driven by Nuclear Starbursts, ApJ, 706, 676-686.
Kawamura, A., Mizuno, Y., Minamidani, T., Filipović, M. D.,
Staveley-Smith, L., Kim, S., Mizuno, N., Onishi, T., Mizuno, A.,
Fukui, Y.: 2009, The Second Survey of the Molecular Clouds inthe Large Magellanic Cloud by NANTEN. II. Star Formation,
ApJS, 184, 1-17.
Kawanomoto, S., Aoki, W., Kajino, T., Mathews, G. J.: 2009,
The interstellar rubidium isotope ratio toward HD169454, ApJ,
698, 509-513.
Kawanomoto, S., Kajino, T., Aoki, W., Bessell, M., Suzuki, T. K.,
Ando, H., Noguchi, K., Honda, S., Izumiura, H., Kambe, E.,
Okita, K., Sadakane, K., Sato, B., Tajitsu, A., Takada-Hidai,M., Tanaka, W., Watanabe, E., Yoshida, M.: 2009, The New
Detections of 7Li/6Li Isotopic Ratio in the Interstellar Media,
ApJ, 701, 1506-1518.
Kawashima, T., Ohsuga, K., Mineshige, S., Heinzeller, D., Takabe,
H., Matsumoto, R.: 2009, New Spectral State of Supercritical
Accretion Flow with Comptonizing Outflow, PASJ, 61, 769-776.
Kida, S., et al. including Niinuma, K.: 2010, Radio Variabilityof a Fermi Large Area Telescope Bright Source 0FGL
J1847.8+3223, ApJ, 711, L36-L40.
Kim, M., Kim, E., Hwang, N., Lee, M. G., Im, M., Karoji, H.,
Noumaru, J., Tanaka, I.: 2009, Reddening and Distance of the
Local Group Starburst Galaxy IC 10, ApJ, 703, 816-828.
Kimura, H., Fukagawa, M., Tamura, M., Kobayashi, H., Yamamoto,T., Ishii, M., Suto, H.: 2010, Planets in orbit around β Pictoris
formed the orbital architecture of planetesimal belts?, Earth,Planets and Space, 62, 111-116.
Kino, M., Ito, H., Kawakatu, N., Nagai, H.: 2009, New predictionof extragalactic GeV γ-ray emission from radio lobes of young
AGN jets, MNRAS, 395, L43-L47.
Kitamura, M., Sekiguchi, K., Yumoto, K., Haubold, H. J.: 2009, Third
UN/ESA/NASA Workshop on the International HeliophysicalYear 2007 and Basic Space Science, Earth Moon and Planets,
104, 141-159.
Kiuchi, K., Sekiguchi, Y., Shibata, M., Taniguchi, K.: 2009, Longterm general relativistic simulation of binary neutron stars
collapsing to a black hole, Phys. Rev. D, 80, 064037.
Kiuchi, K., Kotake, K., Yoshida, S.: 2009, Equilibrium Configurations of Relativistic Stars with Purely Toroidal Magnetic
Fields: Effects of Realistic Equations of State, ApJ, 698,
541-557.
Kiuchi, R., et al. including Mizumoto, Y.: 2009, CANGAROO-III
Search for TeV Gamma Rays from Two Clusters of Galaxies,
ApJ, 704, 240-246.
Ko, J., Im, M., Lee, H. M. Lee, M. G., Hopwood, R. H., Serjeant, S.,
Smail, I., Hwang, H. S., Hwang, N., Shim, H., Kim, S. J., Lee, J.
C., Lim, S., Seo, H., Goto, T., Hanami, H., Matsuhara, H., Takagi,T., Wada, T.: 2009, The Mid-infrared View of Red Sequence

II Publications, Presentations051

Galaxies in Abell 2218 with AKARI, ApJ, 695, L198-L202.
Kobayashi, M. A. R., Totani, T., Nagashima, M.: 2010, Lyman
Alpha Emitters in Hierarchical Galaxy Formation II. UVContinuum Luminosity Function and Equivalent Width
Distribution, ApJ, 708, 1119-1134.
Koda, J., et al. including Sawada, T.: 2009, Dynamically Driven
Evolution of the Interstellar Medium in M51, ApJ, 700, L132-L136.
Koike, C., Imai, Y., Chihara, H., Suto, H., Murata, K., Tsuchiyama,A., Tachibana, S., Ohara, S.: 2010, Effects of Forsterite Grain
Shape on Infrared Spectra, ApJ, 709, 983-992.
Kojima, K., Kajino, T., Mathews, G. J.: 2010, Growth of Cosmological Perturbation by Extra Anisotropic Stress, J. Cosmol.
Astropart. Phys., 2, 18.
Kojima, T., Kroug, M., Takeda, M., Shan, W., Fujii, Y., Uzawa, Y.,
Wang, Z., Shi, S.: 2009, Performance of Terahertz Waveguide
SIS Mixers Employing Epitaxial NbN Films and Nb Junctions,
IEEE Tran. Appl. Supercond., 19, 405.
Kojima, T., Kroug, M., Takeda, M., Uzawa, Y., Shan, W., Fujii,Y., Wang, Z., Ogawa, H.: 2009, Three Quanta Sensitivity Superconductor-Insulator-Superconductor Mixer for the 0.78-0.95
THz Band, Appl. Phys. Express, 2, 10220.
Kokeyama, K., Sato, S., Nishizawa, A., Kawamura, S.: 2009,
Development of displacement- and frequency-noise-freeinterferometer in 3-D configuration for gravitational wave
detection, Phys. Rev. Lett., 103, 171101.
Komiya, Y., Habe, A., Suda, T., Fujimoto, M.: 2009, HierarchicalFormation of the Galactic Halo and the Origin of Hyper MetalPoor Stars, ApJ, 696, L79.
Komiya, Y., Suda, T., Fujimoto, M.: 2009, Early-Age Evolutionof the Milky Way Related by Extremely Metal-Poor Stars, ApJ,
694, 1577.
Kong, X., Fang, G., Arimoto, N., Wang, M.: 2009, Classificationof Extremely Red Objetcs in the Cosmos Field, ApJ, 702,
1458-1471.
Korn, A. J., Richard, O., Mashonkina, L., Bessell, M. S., Frebel, A.,
Aoki, W.: 2009, HE 1327–2326, An Unevolved Star with [Fe/H]< −5.0. III. Does its Atmosphere Reflect its Natal Composition?,
A&A, 698, 410.
Koshida, S., Yoshii, Y., Kobayashi, Y., Minezaki, T., Sakata, Y.,
Sugawara, S., Enya, K., Suganuma, M., Tomita, H., Aoki, T.,Peterson, B. A.: 2009, Variation of Inner Radius of Dust Torus
in NGC4151, ApJ, 700, L109-L113.
Kotake, K., Iwakami, W., Ohnishi, N., Yamada, S.: 2009, RayTracing Analysis of Anisotropic Neutrino Radiation for
Estimating Gravitational Waves in Core-Collapse Supernova,
ApJ, 704, 951-963.
Kotake, K., Iwakami, W., Ohnishi, N., Yamada, S.: 2009, Stochastic
Nature of Gravitational Waves from Supernova Explosions withStanding Accretion Shock Instability, ApJ, 697, L133-L136.
Kroug, M., Endo, A., Tamura, T., Noguchi, T., Kojima, T.,
Uzawa, Y., Takeda, M., Wang, Z., Shan, W.: 2009, SIS Mixer
Fabrication for ALMA Band10, IEEE Tran. Appl. Supercond.,
19, 171.
Kuinieda, S., Chiba, S., Shibata, K., Ichihara, A., Iwamoto, O.,
Iwamoto, N., Fukahori, T., Soukhovitski, E. Sh.: 2009, An
Extensive Study of the Soft-rotator Model Hamiltonian052

II Publications, Presentations

Parameters for Medium and Heavy Even-even Nuclei, J. Nucl.
Sci. Technol., 46, 914-924.
Kurono, Y., Morita, K.-I., Kamazaki, T.: 2009, A Study ofCombining Technique of Single-Dish and Interferometer Data:
Imaging Simulations and Analysis, PASJ, 61, 873-894.
Kusakabe, M., Kajino, T., Yoshida, T., Mathews, G. J.: 2009,
Effect of Long-lived Strongly Interacting Relic Particles on BigBang Nucleosynthesis, Phys. Rev. D, 80, 103501.
Kusakabe, M., Kajino, T., Yoshida, T., Shima, T., Nagai, Y., Kii,
T.: 2009, New Constraints on Radiative Decay of Long-LivedX Particles in Big Bang Nucleosynthesis with New Rates of
Photodisintegration Reactions of He4, Phys. Rev. C, 79, 23513.
Kwon, J., Choi, M., Pak, S., Kandori, R., Tamura, M., Nagata, T.,
Sato, S.: 2010, Magnetic Field Structure of the HH 1-2 Region:
Near-Infrared Polarimetry of Point-Like Sources, ApJ, 708,
758-769.
Landi, E., Miralles, M. P., Curdt, W., Hara, H.: 2009, Physical
Properties of Cooling Plasma in Quiescent Active Region
Loops, ApJ, 695, 221-237.
Landi, E., Raymond, J. C., Miralles, M. P., Hara, H.: 2010,
Physical Conditions in a Coronal Mass Ejection from Hinode,
Stereo, and SOHO Observations, ApJ, 711, 75-98.
Lee, J.-Y., Hahn, I., Kim, Y., Hong, S.-W., Chiba, S., Soukhovitskii,
E. Sh.: 2009, Optical potentials for nuclear level structuresand nucleon interactions data of tin isotopes based on the softrotator model, Phys. Rev. C, 79, 064612.
Lee, M. G., Park, H. S., Hwang, H. S., Arimoto, N., Tamura,N., Onodera, M.: 2010, The Globular Cluster System of theVirgo Giant Elliptical Galaxy NGC 4636. II. Kinematics of the
Globular Cluster System, ApJ, 709, 1083.
Leggett, S. K., Burningham, B., Saumon, D., Marley, M. S.,
Warren, S. J., Smart, R. L., Jones, H. R. A., Lucas, P. W.,
Pinfield, D. J., Tamura, M.: 2010, Mid-Infrared Photometry ofCold Brown Dwarfs: Diversity in Age, Mass, and Metallicity,
ApJ, 710, 1627-1640.
Leggett, S. K., et al. including Tamura, M.: 2009, The Physical
Properties of Four ~600 K T Dwarfs, ApJ, 695, 1517-1526.
Li, J., Shen, Z. Q., Miyazaki, A., Huang, L., Sault, R. J., Miyoshi,M., Tsuboi, M., Tsutsumi, T.: 2009, The Variability of Sagittarius
A* at 3 Millimeter, ApJ, 700, 417-425.
Liszt, H. S., Pety, J., Tachihara, K.: 2009, Imaging galactic diffuse
clouds: CO emission, reddening and turbulent flow in the gas
around ζ Ophiuchi, A&A, 499, 503.
Liu, G., Calzetti, D., Yun, M. S., Wilson, G. W., Draine, B. T.,
Scott, K., Austerman, J., Perera, T., Hughes, D., Aretxaga, I.,
Kohno, K., Kawabe, R., Ezawa, H.: 2010, An Investigationof the Dust Content in the Galaxy Pair NGC 1512/1510 from
Near-Infrared to Millimeter Wavelengths, AJ, 139, 1190-1198.
Liu, Q., Kikuchi, F., Goossens, S., Matsumoto, K., Hanada, H.,
Ping, J., Shi, X., Tamura, Y., Harada, Y., Asari, K., Tsuruta,
S., Ishikawa, T., Kawano, N., Ishihara, Y., Noda, H., Sasaki,S., Iwata, T., Namiki, N.: 2009, S-band Same-Beam VLBI
Observations in SELENE (kaguya) and Correction of Atmosphericand Ionospheric Delay, J. Geodetic Soc. Jpn., 55, 243-254.
Liu, Q., et al. including Kikuchi, F., Matsumoto, K., Goossens,S., Hanada, H., Harada, Y., Ishikawa, T., Tsuruta, S., Asari,K., Ishihara, Y., Iwata, T., Noda, H., Sasaki,S., Shibata, K.,
Tamura, Y., Jike, T., Iwadate, K., Kameya, O.: 2010, Samebeam VLBI Observations of SELENE for Improving Lunar
Gravity Field Model, Radio Sci., 45, RS2004.
Liu, Q., Shi, X., Kikuchi, F., Huang, Q., Kamata, S., Matsumoto,K., Hanada, H., Hong, X., Yu, A., Ping, J., Fan, Q., Xia, B., An,
T., Qian, Z., Yang, W., Zhang, H., Wang, Z., Wang, N.: 2009,
High-accuracy same-beam VLBI observations using Shanghai
and Urumqi telescopes, Sci. China, Ser. G, 52, 1858-1866.
Lundock, R., Ichikawa, T., Okita, H., Kurita, K., Kawabata, K. S.,
Uemura, M., Yamashita, T., Ohsugi, T., Sato, S., Kino, M.:
2009, Tohoku-Hiroshima-Nagoya planetary spectra library: amethod for characterizing planets in the visible to near infrared,
A&A, 507, 1649.
Ly, C., Malkan, M. A., Treu, T., Woo, J.-H., Currie, T., Hayashi,M., Kashikawa, N., Motohara, K., Shimasaku, K., Yoshida,M.: 2009, Lyman Break Galaxies at z ≈ 1.8–2.8: GALEX/NUVImaging of the Subaru Deep Field, ApJ, 697, 1410.
Machida, M. N., Inutsuka, S., Matsumoto, T.: 2009, First Direct
Simulation of Brown Dwarf Formation in a Compact Cloud
Core, ApJ, 699, 157-160.
Machida, M. N., Inutsuka, S., Matsumoto, T.: 2009, The Circumbinary Outflow: A Protostellar Outflow Driven by a
Circumbinary Disk, ApJ, 704, 10-14.
Machida, M. N., Omukai, K., Matsumoto, T., Inutsuka, S.-i.:
2009, Binary formation with different metallicities: dependence
on initial conditions, MNRAS, 399, 1255-1263.
Machida, M. N., Omukai, K., Matsumoto, T.: 2009, Star
Formation in Relic H II Regions of the First Stars: Binarity and
Outflow Driving, ApJ, 705, 64-67.
Machida, M., Matsumoto, R., Nozawa, S., Takahashi, K., Fukui, Y.,
Kudo, N., Tomisaka, K.: 2009, Formation of Galactic Center
Magnetic Loops, PASJ, 61, 411-420.
Magakian, T. Y., Nikogossian, E. H., Aspin, C., Pyo, T.-S.,
Khanzadyan, T., Movessian, T., Smith, M. D., Mitchison, S.,
Davis, C. J., Beck, T. L., Moriarty-Schieven, G. H.: 2010, A
Wide-Field Narrowband Optical Survey of the Braid NebulaStar Formation Region in Cygnus OB7, AJ, 139, 969-983.
Magara, T.: 2009, Characteristic Development of Magnetic Shearin a Flare-producing Sunspot Obtained from Vector Magnetic
Field Measurements by Hinode, ApJ, 702, 386-391.
Mamyoda, K., Nakai, N., Yamauchi, A., Diamond, P., Huré, J.
M.: 2009, Detection of a Sub-Keplerian Water Maser Disk at
the Active Galactic Nucleus of the Galaxy IC 1481, PASJ, 61,
1143-1151.
Martínez-Pillet, P. V., Katsukawa, Y., Puschmann, K. G., RuizCobo, B.: 2009, Supersonic Continuation of the Evershed Flow
Outside a Sunspot as Observed with Hinode, ApJ, 701, L79-L82.
Matsubayashi, K., Sugai, H., Hattori, T., Kawai, A., Ozaki, S.,
Kosugi, G., Ishigaki, T., Shimono, A.: 2009, Galactic Windin the Nearby Starburst Galaxy NGC 253 Observed with the
Kyoto3DII Fabry-Perot Mode, ApJ, 701, 1636.
Matsuda, Y., Richard, J., Smail, Ian, Kashikawa, N., Shimasaku,
K., Frye, B. L., Yamada, T., Nakamura, Y., Hayashino, T., Fujii,
T.: 2010, A search for galaxies in and around an H I overdense
region at z = 5, MNRAS, 403, L54.

Matsui, H., Habe, A.: 2009, Effects of Minor Mergers on the
Coalescence of a Supermassive Black Hole Binary, PASJ, 61,
421-428.
Matsui, R., Uemura, M., Arai, A., Sasada, A., Ohsugi, T.,
Yamashita, T., Kawabata, K., Fukazawa, Y., Mizuno, T.,
Katagiri, H., Takahashi, H., Sato, S., Kino, M., Yoshida, M.,
Shimizu, Y., Nagayama, S., Yanagisawa, K., Toda, H., Okita,K., Kawai, N.: 2009, Optical and Near-Infrared PhotometricObservation during the Superoutburst of the WZ Sge-Type
Dwarf Nova, V455 Andromedae, PASJ, 61, 1081-1092.
Matsumura, N., Niinuma, K., Kuniyoshi, M., Takefuji, K., Asuma,
K., Daishido, T., Kida, S., Tanaka, T., Aoki, T., Ishikawa, S.,
Hirano, K., Nakagawa, S.: 2009, The Closely Positioned ThreeRadio Transients in the Nasu 1.4 GHz Wide-Field Survey, AJ,
138, 787-795.
Matsunaga, N., Kawadu, T., Nishiyama, S., Nagayama, T., Hatano,
H., Tamura, M., Glass, I. S., Nagata, T.: 2009, A near-infrared
survey of Miras and the distance to the Galactic Centre,
MNRAS, 399, 1709-1729.
Mayama, S., Tamura, M., Hanawa, T., Matsumoto, T., Ishii, M., Pyo,
T.-S., Suto, H., Naoi, T., Kudo, T., Hashimoto, J., Nishiyama,S., Kuzuhara, M., Hayashi, M.: 2010, Direct Imaging ofBridged Twin Protoplanetary Disks in a Young Multiple Star,
Science, 327, 306-308.
Michikoshi, S., Kokubo, E., Inutsuka, S.: 2009, N-Body Simulationof Planetesimal Formation through Gravitational Instability and
Coagulation. II. Accretion Model, ApJ, 703, 1363-1373.
Miki, S., Takeda, M., Fujiwara, M., Sasaki, M., Wang, Z.: 2009,
Compactly packaged superconducting nanowire single-photon
detector with an optical cavity for multichannel system, Opt.
Express, 17, 23557.
Minato, F., Chiba, S., Hagino, K.: 2009, Fission of heavy Λhypernuclei with the Skyrme-Hartree-Fock approach, Nucl. Phys. A,
831, 150-162.
Minezaki, T., Chiba, M., Kashikawa, N., Inoue, K. T., Kataza, H.:
2009, Subaru Mid-Infrared Imaging of the Quadruple Lenses.
II. Unveiling Lens Structure of MG0414+0534 and Q2237+030,
ApJ, 697, 610.
Miura, N., Noto, Y., Kato, S., Yokoyama, F., Kuwamura, S., Baba,
N., Hanaoka, Y., Nagata, S., Ueno, S., Kitai, R., Ichimoto, K.,
Takami, H.: 2009, Solar Adaptive Optics System Using an
Electromagnetic Deformable Mirror, Opt. Rev., 16, 558-561.
Mizuno, Y., et al. including Mizuno, N., Ezawa, H., Yamaguchi,N., Hasegawa, T., Tatematsu, K.: 2010, Warm and dense
Molecular Gas in the N159 Region: 12CO J=4–3 and 13CO J=3–2
Observations with NANTEN2 and ASTE, PASJ, 62, 51-67.
Mizuta, A., Kino, M., Nagakura, H.: 2010, Hysteresis of Backflow
Imprinted in Collimated Jets, ApJ, 709, L83-L87.
Momose, M., Ohashi, N., Kudo, T., Tamura, M., Kitamura, Y.: 2010,
High-resolution Observations of Dust Continuum Emission at
340 GHz from the Low-Mass T Tauri Star FN Tauri, ApJ, 712,
397-404.
Moon, D.-S., Koo, B.-C., Lee, H.-G., Matthews, K., Lee, J.-J., Pyo,
T.-S., Seok, Ji Yeon, Hayashi, M.: 2009, Dense Iron Ejecta andCore-Collapse Supernova Explosion in the Young Supernova
Remnant G11.2-0.3, ApJ, 703, L81-L85.

II Publications, Presentations

053

Morokuma, T., et al. including Hattori, T., Furusawa, H., Kashikawa,N., Takanashi, N.: 2010, Subaru FOCAS Spectroscopic
Observations of High-Redshift Supernovae, PASJ, 62, 19.
Morota, T., Haruyama, J., Honda, C., Ohtake, M., Yokota, Y.,
Kumura, J., Matsunaga, T., Ogawa, Y., Hirata, N., Demura, H.,
Iwasaki, A., Miyamoto, H., Nakamura, R., Takeda, H., Ishihara,Y., Sasaki, S.: 2009, Mare volcanism in the lunar farside
Moscoviense region: Implication for lateral variation in magma
production of the Moon, Geophys. Res. Lett., 36, L21202.
Muller, E., Ott, J., Hughes, A., Pineda, J. L., Wong, T., Mizuno,N., Kawamura, A., Mizuno, Y., Fukui, Y., Onishi, T., Rubio, M.:
2010, Characterizing the Low-Mass Molecular Component in
the Northern Small Magellanic Cloud, ApJ, 712, 1248-1258.
Murakami, N., Ohishi, N., Nishikawa, J., Yoshizawa, M.:
2009, Polarimetric stellar interferometry by use of birefringent
retarders, Appl. Opt., 48, 5774-5781.
Muraoka, K., Kohno, K., Tosaki, T., Kuno, N., Nakanishi, K.,
Sorai, K., Ishizuki, S., Handa, T., Okuda, T.: 2009, Nobeyama
Millimeter Array Observations of the Nuclear Starburst of M83:
A GMA Scale Correlation between Dense Gas Fraction and Star
Formation Efficiency, PASJ, 61, 163-176.
Muraoka, K., Kohno, K., Tosaki, T., Kuno, N., Nakanishi, K.,
Sorai, K., Sawada, T., Tanaka, K., Handa, T., Fukuhara, M.,
Ezawa, H., Kawabe, R.: 2009, ASTE CO(3–2) Mapping
toward the Whole Optical Disk of M 83: Properties of Inter-arm
Giant Molecular-Cloud Associations, ApJ, 706, 1213-1225.
Nagakura, T., Hosokawa, T., Omukai, K.: 2009, Star formation
triggered by supernova explosions in young galaxies, MNRAS,
399, 2183-2194.
Nagashima, K., Sekii, T., Kosovichev, A. G., Zhao, J., Tarbell, T.
D.: 2009, Helioseismic Signature of Chromospheric Downflows
in Acoustic Travel-Time Measurements From Hinode, ApJ, 694,
L115-L119.
Nagata, H., Matsuo, H., Hibi, Y., Kobayashi, J., Nakahashi,
M., Ikeda, H., Fujiwara, M.: 2009, GaAs cryogenic readout
electronics for high impedance detector arrays for far-infraredand submillimeter wavelength region, Cryogenics, 49, 676-680.
Nagayama, T., Omodaka, T., Handa, T., Toujima, H., Sofue, Y.,
Sawada, T., Kobayashi, H., Koyama, Y.: 2009, NH3 in the
Galactic Center is Formed under Cool Conditio, PASJ, 61,
1023-1037.
Nakagawa, H., Kasaba, Y., Maezawa, H., Hashimoto, A., Sagawa,
H., Murata, I., Okano, S., Aoki, S., Moribe, N., Mizuno, A.,
Momose, M., Ohnishi, T., Mizuno, N., Nagahama, T.: 2009,
Search of SO 2 in the Martian atmosphere by ground-based
submillimeter observation, Planet. Space Sci., 57, 2123-2127.
Nakajima, T., Sakai, T., Kuno, N., Ogawa, H.: 2010, Developmentof the Measurement System of Image Rejection Ratio for the
Sideband-Separating Receiver, J. Infrared, Millimeter, andTerahertz Waves, 31, 143-150.
Nakamura, K.: 2009, Consistency of Equations in the Secondorder Gauge-invariant Cosmological Perturbation Theory, Prog.
Theor. Phys., 121, 1321.
Nakamura, K.: 2009, Perturbations of Matter Fields in the Secondorder Gauge-invariant Cosmological Perturbation Theory, Phys.
Rev. D, 80, 124021.

054

II Publications, Presentations

Nakariakov, V. M., Melnikov, V. F.: 2009, Quasi-Periodic
Pulsations in Solar Flares, Space Sci. Rev., 149, 119-151.
Narita, N., Hirano, T., Sato, B., Winn, J. N., Suto, Y., Turner,
E. L., Aoki, W., Tamura, M., Yamada, T.: 2009, Improved
Measurement of the Rossiter-McLaughlin Effect in the
Exoplanetary System HD 17156, PASJ, 61, 991-997.
Narita, N., Sato, B., Hirano, T., Tamura, M.: 2009, First Evidenceof a Retrograde Orbit of a Transiting Exoplanet HAT-P-7b,
PASJ, 61, L35-L40.
Naruse, M., Ito, T., Sekimoto, Y., Toba, H., Satou, N., Sugimoto,
M., Shan, W., Iizuka, Y., Kamba, T., Kamikura, M.,
Serizawa, Y.: 2009, Near-Field Beam Pattern Measurement of
Qualification Model of ALMA Band 8(385–500 GHz) Cartridge
Receiver, Exp. Astron., 24, 89-107.
Niino, Y., Totani, T., Kobayashi, M.: 2009, Probing the Long
Gamma-Ray Burst Progenitor by Lyα Emission of Host
Galaxies, ApJ, 707, 1634.
Niinuma, K., Daishido, T., Matsumura, N., Takefuji, K., Kuniyoshi,
M., Asuma, K., Kida, S., Tanaka, T., Aoki, T., Ishikawa, S.,
Hirano, K., Uehara, H., Nakagawa, S.: 2009, Discovery of Two
Radio Transients at a High Galactic Latitude in A 1.4 GHz DriftScan Survey, ApJ, 704, 652-660.
Nishimura, T., Aikawa, M., Suda, T., Fujimoto, M.: 2009, Oxygenand Light-Element Synthesis by Neutron-Capture Reactions in
Metal-Free and Extremely Metal-Poor AGB Stars, PASJ, 61,
909-929.
Ning, Z., Cao, W., Okamoto, T. J., Ichimoto, K., Qu, Z.: 2009,
Small-scale oscillations in a quiescent prominence observed by
HINODE/SOT - Prominence oscillations, A&A, 499, 595-600.
Nishiyama, S., Tamura, M., Hatano, H., Kato, D., Tanabé, T.,
Sugitani, K., Nagata, T.: 2009, Interstellar Extinction Law
Toward the Galactic Center III: J, H, KS Bands in the 2MASS
and the MKO Systems, and 3.6, 4.5, 5.8, 8.0 μm in the Spitzer/
IRAC System, ApJ, 696, 1407-1417.
Nishiyama, S., Tamura, M., Hatano, H., Nagata, T., Kudo, T., Ishii,
M., Schödel, R., Eckart, A.: 2009, Near-Infrared Polarimetry of
Flares from Sgr A* with Subaru/CIAO, ApJ, 702, L56-L60.
Nishizawa, A., Taruya, A., Hayama, K., Kawamura, S., Sakagami,
M.: 2009, Probing nontensorial polarizations of stochastic
gravitational-wave backgrounds with ground-based laserinterferometers, Phys. Rev. D, 79, 82002.
Nishizuka, N., Takasaki, H., Asai, A., Shibata, K.: 2010, Multiple
Plasmoid Ejections and Associated Hard X-ray Bursts in the2000 November 24 Flare, ApJ, 711, 1062-1072.
Niwa, T., Tachihara, K., Itoh, Y., Oasa, Y., Sunada, K., Sugitani, K.,
Mukai, T.: 2009, Millimeter-wave survey of molecular clouds
around the W5-East triggered star-forming region, A&A, 500,
1119-1129.
Niwa, Y., Arai, K., Ueda, A., Sakagami, M., Gouda, N., Kobayashi,Y., Yamada, Y., Yano, T.: 2009, Long-term stabilization of aheterodyne metrology interferometer down to a noise level of
20 pm over an hour, Appl. Opt., 48, 6105-6110.
Nogami, K., Fujii, M., Ohashi, H., Miyachi, T., Sasaki, S., Hasegawa,S., Yano, H., Shibata, H., Iwai, T., Minami, S., Takechi, S.,
Gruen, E., Srama, R.: 2010, Development of the Mercury dust
monitor(MDM) onboard the BepiColombo mission, Planet.

Space Sci., 58, 108-115.
Noguchi, T., Suzuki, T., Endo A., Tamura, T.: 2009, Contributionof the Imaginary Part of the Superconducting Gap Energy on
the SIS Tunneling Current, Physica C, 469, 1585-1588.
Noguchi, T., Tsuchiyama, A., Hirata, N., Demura, H., Nakamura,R., Miyamoto, H., Yano, H., Nakamura, T., Saito, J., Sasaki, S.,
Hashimoto, T., Kubota, T., Ishiguro, M., Zolensky, M. E.: 2010,
Surface morphological features of boulders on Asteroid 25143
Itokawa, Icarus, 206, 319-326.
Oh, C. S., Kobayashi, H., Honma, M., Hirota, T., Sato, K.,
Ueno, Y.: 2010, VERA Observations of H2O Maser Sourcesin Three Massive Star-Forming Regions and Galactic Rotation
Measurements, PASJ, 62, 101-114.
Ohama, A., Dawson, J. R., Furukawa, N., Kawamura, A., Moribe, N.,
Yamamoto, H., Okuda, T., Mizuno, N., Onishi, T., Maezawa, H.,
Minamidani, T., Mizuno, A., Fukui, Y.: 2010, Temperature andDensity Distribution in the Molecular Gas Toward Westerlund 2:
Further Evidence for Physical Association, ApJ, 709, 975-982.
Ohishi M.: 2009, JVO and NaReGi(Japanese Grid middleware
initiative), Memorie della Societa Astronomica Italiana, 80,
554-558.
Ohishi, M.: 2010, Astronomical Virtual Observatories throughInternational Collaboration, Data Sci. J., 8, S128-S134.
Ohsuga, K., Mineshige, S., Mori, M., Kato, Y.: 2009, Global
Radiation-Magnetohydrodynamic Simulations of Black Hole
Accretion Flow and Outflow: Unified Model of Three States,
PASJ Lett., 61, 7-11.
Ohtake, M., et al. including Sasaki, S.: 2009, The global distributionof pure anorthosite on the Moon, Nature, 461, 236-240.
Ohtsuka, K., Nakato, A., Nakamura, T., Kinoshita, D., Ito, T.,
Yoshikawa, M., Hasegawa, S.: 2009, Solar radiation heating
effects on 3200 Phaethon, Publ. Soc. Astron. Japan, 61, 1375-1387.
Okabe, N., Okura, Y., Futamase, T.: 2009, Weak-lensing Mass
Measurements of Substructures in Coma Cluster with Subaru/
Suprime-cam, ApJ, 713, 291-303.
Okamoto, T. J., Tsuneta, S., Lites, B. W., Kubo, M., Yokoyama, T.,
Berger, T. E., Ichimoto, K., Katsukawa, Y., Nagata, S., Shibata,K., Shimizu, T., Shine, R. A., Suematsu, Y., Tarbell, T. D.,
Title, A. M.: 2009, Prominence Formation Associated with an
Emerging Helical Flux Rope, ApJ, 697, 913-922.
Okamoto, Y. K., Kataza, H., Honda, M., Fujiwara, H., Momose, M.,
Ohashi, N., Fujiyoshi, T., Sakon, I., Sako, S., Yamashita, T.,
Miyata, T., Onaka, T.: 2009, Direct Detection of a Flared Disk
Around a Young Massive Star HD200775 and its 10 to 1000 AU
Scale Properties, ApJ, 706, 665.
Okoshi, K., Nagashima, M., Gouda, N., Minowa, Y.: 2010, H
I-Selected Galaxies as a Probe of Quasar Absorption Systems,
ApJ, 710, 1295-1309.
Okura, Y., Futamase, T.: 2009, A New Method for Measuring Weak
Gravitational Lensing Shear using Higher, ApJ, 699, 143-149.
Omiya, M., Izumiura, H., Han, I., Lee, B.-C., Sato, B., Kambe,
E., Kim, K.-M., Yoon, T. S., Yoshida, M., Masuda, S., Toyota,
E., Urakawa, S., Takada-Hidai, M.: 2009, A Massive Substellar
Companion to the Massive Giant HD 119445, PASJ, 61, 825-831.
Ono, M., Hashimoto, M., Fujimoto, S., Kotake, K., Yamada, S.:
2009, Explosive Nucleosynthesis in Magnetohydrodynamical

Jets from Collapsars, Prog. Theor. Phys., 122, 755-777.
Onodera, M., Arimoto, N., Daddi, E., Renzini, A., Kong, X.,
Cimatti, A., Broadhurst, T., Alexander, D. M.: 2010, A WideArea Survey or High-redshift Massive Galaxies. II. NearInfrared Spectroscopy of BzK-selected Massive Star-forming
Galaxies, ApJ, 715, 385.
Oshima, T., Yoshitake, H.: 2009, Optimization Method for
TES Microcalorimeters with Absorbers, IEEE Trans. Appl.
Supercond., 19, 465-468.
Otsubo, T., Kunimori, H., Noda, H., Hanada, H.: 2010, Simulationof optical response of retroreflectors for future lunar laser
ranging, Adv. Space Res., 45, 733-740.
Otsuka, M., Hyung, S., Lee, S.-J., Izumiura, H., Tajitsu, A.: 2009,
High-dispersion Spectrum of the Halo Planetary Nebula DdDm
1, ApJ, 705, 509-528.
Ouchi, M., Mobasher, B., Shimasaku, K., Ferguson, H. C., Fall,
S. M., Ono, Y., Kashikawa, N., Morokuma, T., Nakajima, K.,
Okamura, S., Dickinson, M., Giavalisco, M., Ohta, K.: 2009,
Large Area Survey for z = 7 Galaxies in SDF and GOODS-N:
Implications for Galaxy Formation and Cosmic Reionization,
ApJ, 706, 1136.
Ouchi, M., et al. including Oguri, M., Kashikawa, N., Furusawa,
H., Hayashi, M., Iye, M., Kodama, T., Yoshida, M.: 2009,
Discovery of a Giant Lya Emitter Near the Reionization Epoch,
ApJ, 696, 1164-1175.
Ozaki, S.: 2009, Kinematic and Excitation Structure of the NGC
1068 Narrow-Line Region, PASJ, 61, 259.
Park, H. S., Lee, M. G., Hwang, H. S., Arimoto, N., Tamura, N.,
Onodera, M.: 2010, The Globular Cluster System of the Virgo
Giant Elliptical Galaxy NGC 4636. I. Subaru/Faint Objects
Camera and Spetrograph Specgtroscopy and Database, ApJ,
709, 377-385.
Reach, W. T., Vaubaillon, J., Kelley, M. S., Lisse, C. M., Sykes,
M. V.: 2009, Distribution and Properties of Fragments andDebris from the Split Comet 73P/Schwassmann-Wachmann 3
as Revealed by Spitzer Space Telescope, Icarus, 203, 571.
Reid, M. J., Menten, K. M., Zheng, X. W., Brunthaler, A.,
Moscadelli, L., Xu, Y., Zhang, B., Sato, M., Honma, M.,
Hirota, T., Hachisuka, K., Choi, Y. K., Moellenbrock, G. A.,
Bartkiewicz, A.: 2009, Trigonometric Parallaxes of Massive
Star-Forming Regions. VI. Galactic Structure, Fundamental
Parameters, and Noncircular Motions, ApJ, 700, 137-148.
Reznikova, V. E., Melnikov, V. F., Shibasaki, K., Gorbikov, S.
P., Pyatakov, N. P., Myagkova, I. N., Ji, H.: 2009, 2002 August
24 Limb Flare Loop: Dynamics of Microwave Brightness
Distribution, ApJ, 697, 735-746.
Risaliti, G., Imanishi, M., Sani, E.: 2010, A quantitative determinationof the AGN content in local ULIRGs through L-band spectroscopy,
MNRAS, 401, 197-203.
Rusu, C. E.: 2009, Simple considerations on the deflection angleof light in General Relativity, Creative Math. Inf., 18, 200-207.
Saito, Y.-J., Takada-Hidai, M., Honda, S., Takeda, Y.: 2009, Chemical
Evolution of Zinc in the Galaxy, PASJ, 61, 549-561.
Saitoh, T. R., Makino, J.: 2009, A Necessary Condition for
Individual Time Steps in SPH Simulations, ApJ, 697, L99-L102.
Saitoh, T. R., Daisaka, H., Kokubo, E., Makino, J., Okamoto,

II Publications, Presentations055

T., Tomisaka, K., Wada, K., Yoshida, N.: 2009, Toward FirstPrinciple Simulations of Galaxy Formation: II. Shock-Induced
Starburst at a Collision Interface during the First Encounter ofInteracting Galaxies, PASJ, 61, 481-486.
Sajina, A., Spoon, H., Yan, L., Imanishi, M., Fadda, D., Elitzur, M.:
2009, Detections of Water Ice, Hydrocarbons, and 3.3 μm PAH
in z ~ 2 ULIRGs, ApJ, 703, 270-284.
Sakai, N., Sakai, T., Hirota, T., Burton, M., Yamamoto, S.: 2009,
Discovery of the Second Warm Carbon-Chain-Chemistry
Source, IRAS15398 - 3359 in Lupus, ApJ, 697, 769-786.
Sakai, N., Sakai, T., Hirota, T., Yamamoto, S.: 2009, Deuterated
Molecules in Warm Carbon Chain Chemistry: The L1527 Case,
ApJ, 702, 1025-1035.
Sakamoto, Y., Tsuneta, S., Vekstein, G.: 2009, A Nanoflare Heating
Model and Comparison with Observations, ApJ, 703, 2118-2130.
Sakata, S., Miyakawa, O., Nishizawa, A., Ishizaki, H., Kawamura,S.: 2010, Measurement of angular anti-spring effect in opticalcavity by radiation pressure, Phys. Rev. D, 81, 64023.
Sakata, Y., Minezaki, T., Yoshii, Y., Kobayashi, Y., Koshida, S.,
Aoki, T., Enya, K., Tomita, H., Suganuma, M., Katsuno, U.
Y., Sugawara, S.: 2010, Long-Term Optical Continuum Color
Variability of Nearby Active Galactic Nuclei, ApJ, 711, 461-483.
Sakuma, M., Susa, H.: 2009, Feedback Effects of First Supernovae
on the Neighboring Dark Matter Halos, ApJ, 698, 155-162.
Sasaki, S., Ohashi, H., Hirai, T., Iwai, T., Shibata, H., Nogami,K., Fujii, M.: 2010, Development of Plane-parallel Impactionization Dust Detectors with Large Aperture: A Candidate for
Kibo Exposed Facility Payload, Transaction of Japan Society
for Aeronautical and Space Sciences, Aerospace Technology
Japan, 7, Tr_2_71-Tr_2_74.
Schneider, R., Omukai, K.: 2010, Metals, dust and the cosmic
microwave background: fragmentation of high-redshift starforming clouds, MNRAS, 403, 429-435.
Scholz, A., Geers, V., Jayawardhana, R., Fissel, L., Lee, E.,
Lafreniere, D., Tamura, M.: 2009, Substellar Objects in Nearby
Young Clusters(SONYC): The Bottom of the Initial Mass
Function in NGC 1333, ApJ, 702, 805-822.
Seta, H., et al. including Fukuhara, M., Nakanishi, K., Shimajiri,
Y.: 2009, Suzaku and Multi-Wavelength Observations of
OJ287 During the Periodic Optical Outburst in 2007, PASJ, 61,
1011-1022.
Shan, W., Takeda, M., Kojima, T., Uzawa, Y., Shi, S.-C.,
Noguchi, T., Wang, Z.: 2009, Low-Noise Waveguide-Type
NbN/AlN/NbN SIS Mixers Approaching Terahertz Frequencies,
IEEE Trans. Microwave Theory Tech., 58, 841-848.
Shiino, T., Shiba, S., Sakai, N., Yamakura, T., Jiang, L., Uzawa, Y.,
Maezawa, H., Yamamoto, S.: 2010, Improvement of the criticaltemperature of superconducting NbTiN and NbN thin films
using the AlN buffer layer, Supercond. Sci. Technol., 23, 45004.
Shimajiri, Y., Takahashi, S., Takakuwa, S., Saito, M., Kawabe,
R.: 2009, Millimeter- and Submillimeter-Wave Observations of
the OMC-2/3 Region. IV Interaction between the Outflow andthe Dense Gas in the Cluster Forming Region of OMC-2 FIR 6,
PASJ, 61, 1055-1063.
Shimizu, T., Katsukawa, Y., Kubo, M., Lites, B. W., Ichimoto, K.,
Suematsu, Y., Tsuneta, S., Nagata, S., Shine, R. A., Tarbell,

056

II Publications, Presentations

T. D.: 2009, Hinode Observation of the Magnetic Fields
in a Sunspot Light Bridge Accompanied by Long-Lasting
Chromospheric Plasma Ejections, ApJ, 696, L66-L69.
Shimojo, M., Tsuneta, S.: 2009, The Relation Between Magnetic
Fields and Coronal Activities in the Polar Coronal Hole, ApJ,
706, L145-L149.
Shimono, A., Sugai, H., Kawai, A., Matsubayashi, K., Ohtani,
H., Ozaki, S., Hattori, T., Kosugi, G.: 2010, A study of threedimensional kinematics of the narrow-line region of the Seyfert
galaxy NGC 4151 based on integral field spectroscopy, PASJ,62, 225.
Shinnaga, H., Phillips, T. G., Furuya, R. S., Kitamura, Y.: 2009,
Warm Extended Dense Gas at the Heart of a Cold Collapsing
Dense Core, ApJ, 706, 226.
Shirasaki, Y., Ohishi, M., Mizumoto, Y., Kawanomoto, S.,
Yasuda, N., Honda, S.: 2010, Astronomical Research Using
Virtual Observatories, Data Sci. J., 8, S113-S121.
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Kawanomoto,S., Honda, S., Yasuda, N., Masunaga, Y.: 2010, Applicationof Information Technologies on Astronomy: Japanese Virtual
Observatory(JVO) Portal, Data Sci. J., 8, S122-S127.
Sobue, S., et al. including Sasaki, S., Iwata, T., Araki., H., Hanada,
H.: 2009, The Result of SELENE (KAGUYA) Development
and Operation, Recent Patents on Space Technology, 1, 12-23.
Stalin, C. S., Kawabata, K. S., Uemura, M., Yoshida, M., Kawai,N., Yanagisawa, K., Shimizu, Y., Kuroda, D., Nagayama, S.,
Toda, H.: 2009, Simultaneous MITSuME g'RCIC monitoringof S5 0716+714, MNRAS, 399, 1357-1366.
Su, J., Sakurai, T., Suematsu, Y., Hagino, M., Liu, Y.: 2009,
Local Twist and Current Helicity Distributions of Active Region
NOAA 10930, ApJ, 697, L103-L107.
Sugai, H., Hattori, T., Kawai, A., Ozaki, S., Hayashi, T., Ishigaki,T., Ishii, M., Ohtani, H., Shimono, A., Okita, Y., Matsubayashi,K., Kosugi, G., Sasaki, M., Takeyama, N.: 2010, The Kyoto
Tridimensional Spectrograph II on Subaru and the University of
Hawaii 88 in Telescopes, PASP, 122, 103.
Sugimoto, M., Carter, M., Inatani, J., Sekimoto, Y., Iguchi, S.:
2009, Design of Corrective Beam Waveguide System for the
ALMA/ACA 7-m Antenna, PASJ, 61, 1065-1080.
Sugimoto, M., Iguchi, S., Inatani, J., Sekimoto, Y., Asayama,
S.: 2010, Sensitivity Analysis of Optical Systems in Radio
Telescopes, PASJ, 62, 39-50.
Sugimoto, M., Kosugi, G., Iguchi, S., Iwashita, H., Saito, M.,
Inatani, J., Tasaki, M., Takahashi, T., Nakanishi, K., McMullin,
J. P., Puga, J. P., Hoff, B., Notambuena, J., Kamazaki, T., VilaVolaro, B., Ikenoue, B., Morita, K.-I., Asayama, S., Yamada,M., Kiuchi, H.: 2009, Beam Pattern Measurements andObservational Evaluations of the ALMA/ACA 12-m Antenna,
PASJ, 61, 451-459.
Susa, H., Hasegawa, K., Umemura, M.: 2009, Formation Criteria
and the Mass of Secondary Population III Stars, ApJ, 702,
480-488.
Suzuki, T., Honma, H., Higashiyama, K., Yoshida, T., Kajino,T., Otsuka, T., Umeda, H., Nomoto, K.: 2009, NeutrinoInduced Reactions on Fe56 and Ni56 and Production of Mn55 inPopulation III Stars, Phys. Rev. C, 79, 061603®.

Swinyard, B., et al. including Arimoto, N., Furusho, R., Hayashi,
M., Imanishi, M., Izumiura, H., Kodama, T., Kokubo, E.,
Omukai, K., Tamura, M., Watanabe, J.: 2009, The Space
Infrared Telescope for Cosmology and Astrophysics: SPICA
A Joint Mission between JAXA and ESA, Exp. Astron., 23,
193-219.
Tachihara, K., Neuhäuser, R., Fukui, Y.: 2009, Search for Remnant
Clouds Associated with the TW Hya Association, PASJ, 61, 585.
Takahashi, R. H., Hanawa, T., Matsumoto, R.: 2009, Extensionof the Sweet-Parker Magnetic Reconection to the Relativistic
Plasma, Journal of Plasma and Fusion Research Series, 8, 246.
Takahashi, R., Saito, Y.: 2010, Vacuum-system design for the largescale cryogenic gravitational wave telescope, Vacuum, 84, 709-712.
Takahashi, S., Ho, P. T. P., Tang, Y.-W., Kawabe, R., Saito, M.:
2009, Evolutionary Status of Brightest and Youngest Sources in
the Orion Molecular Cloud -3 Region, ApJ, 704, 1459-1470.
Takahashi, S., Yoshida, F., Shinokawa, K., Mukai, T., Kawabata,K. S.: 2009, Simultaneous Photometric and PolarimetricObservations of Asteroid 3 Juno, AJ, 138, 951-955.
Takami, H., Goto, M., Gaessler, W., Hayano, Y., Iye, M., Kamata,Y., Kanzawa, T., Kobayashi, N., Minowa, Y., Oya, S., Pyo,
T.-S., Saint-Jacques, D., Takato, N., Teradea, H., Tokunaga,
A. T., Tsuji, T.: 2009, Direct Observation of the Extended
Molecular Atmosphere of Ceti by Differential Spectral Imaging
with an Adaptive Optics System, PASJ, 61, 623-627.
Takeda, M., Shan, W., Kojima, T., Saito, S., Kroug, M., Uzawa,Y., Wang, Z.: 2009, Low-noise waveguide SIS mixer with
NbN/AlN/NbN tunnel junctions tuned by an NbN/MgO/NbTiN
microstrip circuit, Supercond. Sci. Technol., 22, 75015.
Takeda, M., Shan, W., Kojima, T., Uzawa, Y., Kroug, M., Li, J.,
Shi, S., Wang, Z.: 2009, Mixing Properties of NbN-Based SIS
Mixers With NbTiN, IEEE Tran. Appl. Supercond., 19, 436.
Takeda, Y., Kaneko, H., Matsumoto, N., Oshino, S., Ito, H., Shibuya,
T.: 2009, Potassium Abundances in Red Giants of Mildly to
Very Metal-Poor Globular Clusters, PASJ, 61, 563-576.
Takeda, Y., Kang, D.-I., Han, I., Lee, B.-C., Kim, K.-M.: 2009,
Can Sodium Abundances of A-Type Stars Be Reliably
Determined from Na I 5890/5896 Lines?, PASJ, 61, 1165-1178.
Takeda, Y., Tajitsu, A.: 2009, High-Dispersion Spectroscopic
Study of Solar Twins: HIP 56948, HIP 79672, and HIP 100963,
PASJ, 61, 471-480.
Takeuchi, S., Mineshige, S., Ohsuga, K.: 2009, Modified Slim-Disk
Model Based on Radiation-Hydrodynamic Simulation Data:
The Conflict Between Outflow and Photon Trapping, PASJ, 61,
783-790.
Tamura, Y., Kohno, K., Nakanishi, K., Hatsukade, B., Iono, D.,
Wilson, G. W., Yun, M. S., Takada, T., Matsuda, Y., Tosaki, T.,
Ezawa, H., Perera, T. A., Acott, K. S., Austermann, J. E., Hughes,
D. H., Aretxaga, I., Chung, A., Oshima, T., Yamaguchi, N.,
Tanaka, K., Kawabe, R.: 2009, Spatial Correlation between
Submillimeter and Lyman-Alpha Galaxies in the SSA 22
Protocluster, Nature, 459, 61-63.
Tanabe, N., Ichihashi,Y., Nakayama, H., Masuda, N., Ito, T.: 2009,
Speed-up of hologram generation using ClearSpeed Accelerator
board, Comput. Phys. Commun., 180, 1870-1873.
Tanaka, M., Chiba, M., Komiyama, Y., Guhathakurta, P., Kalirai,

J. S., Iye, M.: 2010, Structure and Population of the Andromeda
Stellar Halo from a Subaru/Suprime-Cam Survey, ApJ, 708,
1168-1203.
Tanaka, M., Finoguenov, A., Kodama, T., Koyama, Y., Maughan,B., Nakata, F.: 2009, The spectroscopically confirmed hugecosmic structure at z=0.55, A&A, 505, L9-L12.
Tanaka, M., Kawabata, K. S., Maeda, K., Iye, M., Hattori, T., Pian, E.,
Nomoto, K., Mazzali, P., Tominaga, N.: 2009, Spectropolarimetryof the Unique Type Ib Supernova 2005bf: Larger Asymmetry
Revealed by Later-Phase Data, ApJ, 699, 1119-1125.
Tanaka, M., Yamanaka, M., Maeda, K., Kawabata, K. S., Hattori,T., Minezaki, T., Valenti, S., Della Valle, M., Sahu, D. K.,
Anupama, G. C., Tominaga, N., Nomoto, K., Mazzali, P. A.,
Pian, E.: 2009, Nebular Phase Observations of the Type Ib
Supernova 2008D/X-ray Transient 080109: Side-viewed Bipolar
Explosion, ApJ, 700, 1680.
Tanigawa, T., Abe, S., Ishiguro, M., Mukai, T.: 2010, Models for
the Origin of the Quadrantids, Earth, Moon, and Planets, 106, 55.
Thalmann, C., Carson, J., Janson, M., Goto, M., McElwain, M., Egner,
S., Feldt, M., Hashimoto, J., Hayano, Y., Henning, T., Hodapp,
K. W., Kandori, R., Klahr, H., Kudo, T., Kusakabe, N.,
Mordasini, C., Morino, J.-I., Suto, H., Suzuki, R., Tamura,M.: 2009, Discovery of the Coldest Imaged Companion of aSun-like Star, ApJ, 707, L123-L127.
Tomida, K., Tomisaka, K., Matsumoto, T., Ohsuga, K., Masahiro,
M. N., Saigo, K.: 2010, Radiation Magnetohydrodynamics
Simulation of Proto-stellar Collapse: Two-component Molecular
Outflow, ApJ, 714, L58-L63.
Tsai, A. L., Matsushita, S., Nakanishi, K., Kohno, K., Kawabe,R., Inui, T., Matsumoto, H., Tsuru, T. G., Peck, A. B., Tarchi, A.:
2009, Molecular Superbubbles and Outflows from the Starburst
Galaxy NGC 2146, PASJ, 61, 237-250.
Tsuboi, M., Miyazaki, A., Okumura, S. K.: 2009, A Galactic Center
50-km s−1 Molecular Cloud with an Expanding Shell, PASJ, 61,
29-37.
Tsujimoto, T., Bekki, K.: 2009, Chemical Signature of a Major
Merger in the Early Formation of the Small Magellanic Cloud,
ApJ, 700, L69-L72.
Tsujimoto, T., Bland-Hawthorn, J., Freeman, K. C.: 2010, Evidenceof Early Enrichment of the Galactic Disk by Large-Scale Winds,
PASJ, 62, 447-456.
Ueda, K., Kano, R., Tsuneta, S., Shibahashi, H.: 2010, Orientationof X-Ray Bright Points in the Quiet Sun, Sol. Phys., 261, 77-85.
Uehara, T., Sato, A., Maehara, S., Nimonji, T., Sato, T., Ohkawa,M., Maruyama, T., Kawamura, S.: 2009, Comparison of threesemiconductor laser systems for gravitational wave detection,
Opt. Eng., 48, 34302.
Uemura, M., et al. including Yamashita, T.: 2010, Dwarf Novae in
the Shortest Orbital Period Regime. I A New Short Superhump
Period Dwarf Nova, OT J055717+683226, PASJ, 62, 187.
Uzawa, Y., Kroug, M., Kojima, T., Takeda, M., Candotti, M.,
Fujii, Y., Kaneko, K., Shan, W., Noguchi, T., Wang, Z.: 2009,
A sensitive ALMA Band 10 SIS receiver engineering model,
Supercond. Sci. Technol., 22, 114002.
Wada, K., Papadopoulos, P. P., Spaans, M.: 2009, Molecular Gas
Disk Structures Around Active Galactic Nuclei, ApJ, 702, 63-74.

II Publications, Presentations057

Wang, Y., Yamada, T., Tanaka, I., Iye, M.: 2009, A Massive Disk
Galaxy at z > 3 along the Line of Sight of QSO 1508+5714,
PASJ, 61, 1179-1184.
Watabe, Y., Kawakatu, N., Imanishi, M., Takeuchi, T. T.: 2009,
Supermassive Black Hole Mass Regulated by Host Galaxy
Morphology, MNRAS, 400, 1803-1807.
Watanabe, H., Kitai, R., Ichimoto, K., Katsukawa, Y.: 2009,
Magnetic Structure of Umbral Dots Observed with the HinodeSolar Optical Telescope, PASJ, 61, 193-200.
Watanabe, J., Honda, M., Ishiguro, M., Ootsubo, Y., Sarugaku,
Y., Kadono, T., Sakon, I., Fuse, T., Takato, N., Furusho, R.:
2009, Subaru/COMICS Mid-Infrared Observation of the NearNucleus Region of Comet 17P/Holmes at the Early Phase of an
Outburst, PASJ, 61, 679-685.
Whitelock, P. A., Menzies, J. W., Feast, M. W., Matsunaga, N.,
Tanabé, T., Ita, Y.: 2009, Asymptotic giant branch stars in the
Fornax dwarf spheroidal galaxy, MNRAS, 394, 795-809.
Wiegert, P., Vaubaillon, J., Campbell-Brown, M.: 2009, A Dynamical
Model of the Sporadic Meteoroid Complex, Icarus, 201, 295.
Winnberg, A., Deguchi, S., Reid, M. J., Nakashima, J., Olofsson, H.,
Habing, H. J.: 2009, CO in OH/IR Stars to the Galactic Centre,
A&A, 497, 177-181.
Wong, T., Hughes, A., Fukui, Y., Kawamura, A., Mizuno, N., Ott,J., Muller, E., Pineda, J. L., Welty, D. E., Kim, S., Mizuno, Y.,
Murai, M., Onishi, T.: 2009, Molecular and Atomic Gas in the
Large Magellanic Cloud. I. Conditions for CO Detection, ApJ,
696, 370-384.
Yaji, Y., Tashiro, M. S., Isobe, N., Kino, M., Asada, K., Nagai, H.,
Koyama, S., Kusunose, M.: 2009, Evidence of Non-thermal
X-ray Emission from Radio Lobes of Cygnus A, ApJ, 714, 37-44.
Yamada, M., Machida, M. N., Inutsuka, S., Tomisaka, K.: 2009,
Emission from a Young Protostellar Object. I. Signatures ofYoung Embedded Outflows, ApJ, 703, 1141-1158.
Yamada, T., Kajisawa, M., Akiyama, M., Ichikawa, T., Konishi, M.,
Nishimura, T., Omata, K., Suzuki, R., Tanaka, I., Tokoku,
C., Uchimoto, Y. K., Yoshikawa, T.: 2009, Moircs Deep Survey.
III. Active Galactic Nuclei in Massive Galaxies at z = 2–4, ApJ,
699, 1354-1364.
Yamada, Y., Yamauchi, M., Gouda, N., Kobayashi, Y., Tsujimoto,T., Yano, T., Suganuma, M., Nakasuka, S., Sako, N., Inamori, T.:2009, A Star Image Extractor for Small Satellites, Transactionsof the Japan Society for Aeronautical and Space Sciences, SpaceTechnology Japan, 7, Tm_25-Tm_29.
Yamamoto, S., Wada, K., Kobayashi, H., Kimura, H., Ishiguro, M.,
Matsui, T.: 2010, Collisional Process on Comet 9/P Tempel 1:
Mass Loss of its Dust and Ice by Impacts of Asteroidal Objects
and its Collisional History, Earth, Planets and Space, 62, 5.
Yamamoto, T. T., Sakurai, T.: 2009, Forecasting Maximum Solar
Flare Magnitudes from Photospheric Magnetograms, Space
Weather, 7, 04007.
Yamamoto, T. T., Sakurai, T.: 2009, Time Variation and Statistical
Studies of Magnetic Helicity Injection in Solar Magnetic
Regions, ApJ, 698, 928-937.
Yamanaka, M., et al. including Imada, A., Kuroda, D., Miyazaki,S., Nakaya, H., Yamashita, T., Yanagisawa, K., Yoshida, M.:
2009, Early Phase Observations of Extremely Luminous Type

058

II Publications, Presentations

Ia Supernova 2009dc, ApJ, 707, L118.
Yamanaka, M., Naito, H., Kinugasa, K., Takanashi, N., Tanaka, M.,
Kawabata, K. S., Ozaki, S., Narusawa, S., Sadakane, K.: 2009,
Early Spectral Evolution of the Rapidly Expanding Type Ia
Supernova 2006X, PASJ, 61, 713.
Yamazaki, D. G., Ichiki, K., Kajino, T., Mathews, G. J.: 2010, Newconstraint on the Primordial Magnetic Field, Phys. Rev. D, 81,
23008.
Yasui, C., Kobayashi, N., Tokunaga, A. T., Saito, M., Tokoku, C.:
2009, The Lifetime of Protoplanetary Disks in a Low-metallicity
Environment, ApJ, 705, 54.
Yasutake, N., Maruyama, T., Tatsumi, T.: 2009, Hot hadron-quark
mixed Phase transition including hyperons, Phys. Rev. D, 80,
123009.
Yasutake, N., Kiuchi, K., Kotake, K.: 2010, Relativistic hybrid
stars with super-strong toroidal magnetic fields: an evolutionary
track with QCD phase transition, MNRAS, 401, 2101-2112.
Yokochi, K., Tavrov, V., A., Nishikawa, J., Murakami, N., Abe,
L., Tamura, M., Takeda, M., Kurokawa, T.: 2009, Achromatic
deep nulling with a three-dimensional Sagnac interferometer,
Opt. Lett., 34, 1985-1987.
Yoshida, F., Ito, T., Takahashi, S., Ibrahimov, M. A., Marchalkina,
A. L.: 2009, Photometric observations of young asteroid
families at Maidanak observatory, Adv. Geosci., 15, 119-132.
Yoshida, T., Takamura, A., Kimura, K., Yokomakura, H., Kawagoe,
S., Kajino, T.: 2009, Resonant spin-flavor conversion ofsupernova neutrinos: Dependence on electron mole fraction,
Phys. Rev. D, 80, 12.
Yoshikoshi, T., Mori, M., Edwards, P. G., Gunji, S., Hara, S.,
Hara, T., Kawachi, A., Mizumoto, Y., Naito, T., Nishijima, K.,
Tanimori, T., Thornton, G. J., Yoshida, T.: 2009, Reanalysis of
Data Taken by the Cangaroo 3.8 Meter Imaging Atmospheric
Cherenkov Telescope: PSR B1706-44, SN 1006, and Vela, ApJ,
702, 631-648.
Yusef-Zadeh, F., et al. including Miyazaki, A.: 2009, SimultaneousMulti-Wavelength Observations of Sgr A* During 2007 April
1-11, ApJ, 706, 348-375.
Zhang, H., Sakurai, T., Pevtsov, A., Gao, Y., Xu, H., Sokoloff, D.
D., Kuzanyan, K.: 2010, A New Dynamo Pattern Revealed bySolar Helical Magnetic Fields, MNRAS, 402, L30-L33.
Zhang, L., Ishigaki, M., Aoki, W., Zhao, G., Chiba, M.: 2009,
Chemical Compositions of Kinematically Selected Outer HaloStars, ApJ, 706, 1095.
Zhao, J., Kosovichev, A. G., Sekii, T.: 2010, High-Resolution
Helioseismic Imaging of Subsurface Structures and Flows of a
Solar Active Region Observed by Hinode, ApJ, 708, 304-313.
Zhu, M., Papadopoulos, P. P., Xilouris, E. M., Kuno, N., Lisenfeld,
U.: 2009, Tracing Molecular Gas Mass in Extreme Extragalactic
Environments: An Observational Study, ApJ, 706, 941-959.

2. Publications of the National Astronomical Observatory of Japan
Miyashita, A., Tanaka, K., Watanabe, H., Tanabe, H., Sato, M.,
Watanabe. J.: 2009, Fireball Monitoring Observation at the
Kiso Observatory, Publ. Nat. Astron. Obs. Japan, 12, 11-80.

Miyoshi, M.: 2009, Re-analysis of the First Fringe with 2-Beam in
the VERA System from Archive Data, Publ. Nat. Astron. Obs.
Japan, 12, 1-10.

3. Report of the National Astronomical Observatory ofJapan (in Japanese)Sôma, M.: 2009, Problems in Using the Revised “Calendar andEphemeris”, Rep. Nat. Astron. Obs. Japan, 12, 1-11.
Ishizaki, H., Fukuda, T., Nishino, T., Arai, K.: 2009, Development and Experiments of a Pendulum with Suppressed
Rotational Motion, Rep. Nat. Astron. Obs. Japan, Rep. Nat.
Astron. Obs. Japan, 12, 13-22.
Tonooka, H., Gan, H., Shimojo, M., PAONET Working Groupfor Public Use of Hinode Data: 2009, Making of the DVD “TheSun Captured by Hinode” for Public Outreach, Rep. Nat. Astron. Obs. Japan, 12, 23-37.
Shimoikura, T., Nakamichi, A., Tonooka, H.: 2009, Surveys on
the Program Hinode DVD for Public Outreach, Rep. Nat. Astron. Obs. Japan, 12, 39-51.
Yamada, Y., Ozawa, T., Nishizawa, A., Furusho, R., Nishimura,T., Enoki, M., Yoshino, A., Furusawa, J., Takata, T.,
Ichikawa, S.-I.: 2009, Development of Public Science Archive
System of Subaru Telescope 5, Rep. Nat. Astron. Obs. Japan,
12, 53-78.
Tamura, T., Noguchi, T., Endo, A., Krong, M., Shan, W., Ito, T.,
Niizeki, Y., Iizuka, Y.: 2009, The Establishment of SIS Mixer
Device Fabrication System and the Development of SIS Mixer
Device for the ALMA Band 8 Cartridge Receivers, Rep. Nat.
Astron. Obs. Japan, 12, 79-91.
Onoma, F., Itoh, A., Harada, Y., Fukushima, H., Kosai, H.: 2009,
A Proposal of Photometric Technique for Evaluating the NightSky Brightness Using Commercially Available Digital Single
Lens Reflex Camera, Rep. Nat. Astron. Obs. Japan, 12, 93.

4. Conference Proceedings
Abramov-Maximov, V. E., Gelfreikh, G. B., Kobanov, N. I.,
Shibasaki, K.: 2009, A Possible Scenario of Energy Transport
in the 17th May 2002 Flare, Central European Astrophysical
Bulletin 33, 207-215.
Akamatsu, H., Ishisaki, Y., Hoshino, A., Ezoe, Y., Ohashi, T., Takei,
Y., Yamasaki, N. Y., Mitsuda, K., Oshima, T., Tanaka, K.: 2009,
Impedance Measurement of a Gamma-Ray TES Calorimeterwith a Bulk Sn Absorber, AIP Conf. Proc. 1185, 191-194.
Aoki, K., Totani, T., Hattori, T., Ohta, K., Kawabata, K. S.,
Kobayashi, N., Iye, M., Nomoto, K., Kawai, N.: 2009, No
Evidence for Variability of Intervening Absorption Lines toward
GRB 060206: Implications for the Mg II Incidence Problem,AIP Conf. Proc. 1133, 467-472.
Aoki, W.: 2010, Carbon-Enhanced Metal-Poor (CEMP) stars, IAU
Symp. 265, Eds. K. Cunha, M. Spite, B. Barbuy, 111-116.
Aoki, W., Honda, S.: 2010, Enrichment of Thorium (Th) and Lead
(Pb) in the early Galaxy, IAU Symp. 265, Eds. K. Cunha, M.
Spite, B. Barbuy, 61-62.
Ariyoshi, S., Taino, T., Dobroiu, A., Sato, H., Matsuo, H., Otani, C.:

2009, Design of Terahertz Detector based on a Superconducting
Tunnel Junction Coupled to a Thin Superconductor Film, Proc.
34th Int. Conf. on Infrared, Millimeter, and Terahertz Waves,
T5E06.0372.
Asada, K., Doi, A., Kino, M., Nagai, H., Nakamura, M., Kameno, S.,
VSOP-2 Science Working Group: 2009, VSOP-2 Observationsof M 87: A Proposal for a VSOP-2 Key Science Program, ASP
Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y.
Murata, 262.
Asaki, Y., Miyoshi, M.: 2009, A Future Submillimeter-Wave Space
VLBI, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M.
Tsuboi, Y. Murata, 431.
Barker, M., Ferguson, A., Irwin, M., Arimoto, N., Jablonka, P.:
2009, Hunting the Halos of M81 and NGC2403 with Subaru,
Bulletin of AAS 41, 689.
Buehler, S., Ferguson, A., Irwin, M., Arimoto, N., Jablonka, P.,
Macjkey, D.: 2009, The stellar outskirts of the disk galaxy NGC
4244, IAU Symp. 254, Eds. J. Andersen et al., 12.
Choi, Y. K., Hirota, T., Honma, M., Kobayashi, H.: 2009,
Astrometry of the Red Supergiant Star VY Canis Majoris with
VERA, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M.
Tsuboi, Y. Murata, 363.
De Cat, P., Wright, D. J., Pollard, K. R., Maisonneuve, F.,
Kilmartin, P. M., Lehmann, H., Yang, S., Kambe, E., Saesen, S.,
Carrier, F., Mkrtichian, D., Mantegazza, L., Rainer, M., Poretti,
E., Laney, D., Fu, J. N.: 2009, Towards asteroseismology ofmain-sequence g-mode pulsators: spectroscopic multi-site
campaigns for slowly pulsating B stars and γ Doradus stars, AIP
Conf. Proc. 1170, Eds. J. A. Guzik, P. A. Bradley, 480.
de Wijn, A. G., Stenflo, J. O., Solanki, S. K., Tsuneta, S.: 2009,
Small-Scale Solar Magnetic Fields, Space Science series of
ISSI 32, Eds. M. J. Thompson, A. Balogh, J. L. Culhane, Å.
Nordlund, S. K. Solanki, J.-P. Zahn, 275-315.
Deguchi, S., Koike, K., Balasubramanyam, R.: 2009, Natureof Meterwave Luminous Objects and Search for ElectronCyclotron Maser Emission, ASP Conf. Ser. 407, Eds. D. J.
Saikia, D. A. Green, Y. Gupta, T. Venturi, 260-263.
Deguchi, S., Matsunaga, N., Takahashi, S., Kuno, N., Nakashima,J.: 2010, Dying SiO Maser in the V407 Cyg System, The
Astronomer's Telegram, #2519.
Doeleman, S., et al. including Honma, M.: 2009, Imaging an
Event Horizon: submm-VLBI of a Super Massive Black Hole,Astro2010: The Astronomy and Astrophysics Decadal Survey,
Science White Papers, 68.
Enya, K., et al. including Yamashita, T., Narita, N., Tamura, M.,
Nishikawa, J., Hayano, H., Oya, S., Murakami, N., Matsuo,T., Guyon, O., Spica Coronagraph Team: 2009, SPICA
Coronagraph Instrument (SCI) for the Direct Imaging andSpectroscopy of Exo-Planets, SPICA joint European/JapaneseWorkshop, Eds. A. M. Heras, B. M. Swinyard, K. G. Isaak, J. R.
Goicoechea, 01004.
Fomalont, E. B., Kopeikin, S., Titov, O., Honma, M.: 2009, VLBA/VERA Test of General Relativity, IAU Symp. 261, Bulletin of
the AAS, 41, 890.
Fomalont, E., Kopeikin, S., Jones, D., Honma, M., Titov, O.:2010, Recent VLBA/VERA/IVS tests of general relativity, IAU

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Symp. 261, Bulletin of the AAS, 41, 291-295.
Friesen, R., Di, F., Shirley, Y., Myers, P. C., Shimajiri, Y.,
Takakuwa, S., Belloche, A., Andre, P., Bourke, T.: 2010,
Probing the Initial Conditions of Star Formation: Dense Gas in
the Ophiuchus Molecular Cloud, AAS Meeting #215, Bulletinof AAS 41, 257.
Fujimoto, M.-K.: 2009, Searching for Gravitational Waves with
Laser Interferometers, Proc. of the 28th Symp. on Materials
Science and Engineering, Ed. K. Kuriyama, 1.
Fujiwara, M., Nagata, H., Hibi, Y., Matsuo, H., Sasaki, M.: 2009,
Cryogenic Low Noise Amplifier with GaAs JFETs, AIP Conf.
Proc. 1185, 267-270.
Geise, K. M., Ueta, T., Speck, A. K., Izumiura, H., Stencel, R. E.:
2010, Spitzer Reveals New Insights into Mass Loss History of
Evolved Stars, Bulletin of AAS 41, 41.
Gopalswamy, N., Yashiro, S., Makela, P. A., Shibasaki, K.: 2009,
The subdued solar cycle 23/24 minimum revealed by microwave
butterfly diagram, AGU Fall Meeting 2009, SH13C-02.
Guhathakurta, P., et al. including Iye, M.: 2010, The SPLASH
Survey: Spectroscopy of Newly Discovered Tidal Streams in
the Outer Halo of the Andromeda Galaxy, AAS Meeting #215,
Bulletin of AAS 42, 537.
Hagino, M., Nakatani, Y., Ishii, T. T., Hanaoka, Y., Sakurai,
T., Hiei, E., Suzuki, D.: 2009, Comparison of the Vector
Magnetograms taken with the SFT/MTK and the SST/KSW,
ASP. Conf. Ser. 405, Eds. S. V. Berdyugina, K. N. Nagendra, R.
Ramelli, 393-396.
Hagiwara, Y., VSOP-2 Science Working Group: 2009, Extragalactic
Water Maser Observations with VSOP-2, ASP Conf. Ser. 402,
Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 266.
Hanaoka, Y.: 2009, Expanding Applications of the Polarimeterswith Ferroelectric Liquid Crystals and their Calibration, ASP.
Conf. Ser. 405, Eds. S. V. Berdyugina, K. N. Nagendra, R.
Ramelli, 401-405.
Hara, H., Watanabe, T., Bone, L. A., Culhane, J. L., van DrielGesztelyi, L., Young, P. R.: 2009, Characteristics of theNonthermal Velocity Signature Observed in the Impulsive Phaseof the 2007 May 19 Flare, ASP Conf. Ser. 415, Eds. B. Lites, M.
Cheung, T. Magara, J. Mariska, K. Reeves, 459-462.
Hara, H.: 2009, Coronal Plasma Motions in Active Region Loops
Observed with Hinode EIS, ASP Conf. Ser. 415, Eds. B. Lites,
M. Cheung, T. Magara, J. Mariska, K. Reeves, 252-255.
Harada, Y., Iwata, T., Kikuchi, F., Araki, H., Ishihara, Y.,
Sasaki, S., Noda, H., Hanada, H., Goossens, S., Matsumoto,K.: 2010, What do we know from Mars’ rotation?, Proc. of the42th ISAS Lunar and Planetary Symp., 22-25.
Harikae, S., Takiwaki, T., Kotake, K.: 2009, Long-Term Evolutionof Collapsar: Mechanism of Outflow Production, eConf Proc.
C091122, 2009 Fermi Symp., November 2-5.
Hashimoto, J., Tamura, M., Kandori, R., Nakajima, Y.,
Kusakabe, N., Sato, Y.: 2009, Polarimetry for the Disks around
Young Brown Dwarfs, AIP Conf. Proc. 1158, Eds. T. Usuda, M.
Tamura, M. Ishii, 111-114.
Hibi, Y., Matsuo, H., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
The Cryogenic Digital Readout Module with GaAs JFET Ics,
AIP Conf. Proc.,1185, 290-293.

060

II Publications, Presentations

Hirota, T., Bushimata, T., Choi, Y. K., Honma, M., Imai, H.,
Iwadate, K., Jike, T., Kameno, S., Kameya, O., Kamohara,R., Kan-Ya, Y., Kawaguchi, N., Kijima, M., Kim, M. K.,
Kobayashi, H., Kuji, S., Kurayama, T., Manabe, S., Maruyama,K., Matsui, M., Matsumoto, N., Miyaji, T., Nagayama, T.,
Nakagawa, A., Nakamura, K., Oh, C. S., Omodaka, T., Oyama,T., Sakai, S., Sasao, T., Sato, K., Sato, M., Shibata, K. M.,
Shintani, M., Tamura, Y., Tsushima, M., Yamashita, K.:
2009, Astrometry of H2O Maser Sources in Nearby Molecular
Clouds with VERA, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E.
Fomalont, M. Tsuboi, Y. Murata, 456.
Honma, M., Bushimata, T., Choi, Y. K., Hirota, T., Imai, H.,
Iwadate, K., Jike, T., Kameno, S., Kameya, O., Kamohara, R.,
Kawaguchi, N., Kijima, M., Kim, M., Kobayashi, H., Kuji,
S., Kurayama, T., Manabe, S., Matsui, M., Matsumoto, N.,
Miyaji, T., Nagayama, T., Nakagawa, A., Nakamura, K., Oh,
C. S., Omodaka, T., Oyama, T., Sakai, S., Sato, K., Sato, M.,
Sasao, T., Shibata, K. M., Tamura, Y., Yamashita, K.: 2009,
Maser Astrometry with VERA and VSOP-2, ASP Conf. Ser.
402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 460.
Hwang, N., Lee, M. G.: 2010, Tracing star cluster formation in theinteracting galaxy M51, IAU Symp. 266, Eds. R. de Grijs, J. R.
D. Lépine, 423-426.
Ichimoto, K., Suematsu, Y., Katsukawa, Y., Tsuneta, S., Shimojo,
M., Shimizu, T., Shine, R. A., Tarbell, T. D., Berger, T., Title, A.
M., Lites, B. W., Kubo, M., Yokoyama, T., Nagata, S.: 2009, A
New View of Fine Scale Dynamics and Magnetism of Sunspots
Revealed by Hinode/SOT, ASP. Conf. Ser. 405, Eds. S. V.
Berdyugina, K. N. Nagendra, R. Ramelli, 167.
Imamura, T., Iwata, T., Yamamoto, Z., Mochizuki, N., Kono, Y.,
Matsumoto, K., Liu, Q., Noda, H., Hanada, H., Oyama, K.,
Nabatov, A., Futaana, Y., Saito, A., Ando, H.: 2010, Studying
the Lunar Ionosphere with SELENE Radio Science Experiment,
Proc. of the 42th ISAS Lunar and Planetary Symp., 80-83.
Imanishi, M.: 2009, Luminous Buried AGNs in Nearby ULIRGs,
ASP Conf. Ser. 408, Eds. W. Wang, Z. Yang, Z. Luo, Z. Chen,
41-45.
Imanishi, M.: 2009, Luminous Buried AGNs in Ultraluminous
Infrared Galaxies and the Origin of Galaxy Downsizing, SPICA
joint European/Japanese Workshop, Eds. A. M. Heras, B. M.
Swinyard, K. G. Isaak, J. R. Goicoechea, 04011-04014.
Ishihara, D., et al. including Ita, Y.: 2009, AKARI Mid-Infrared
All-sky Survey, AIP Conf. Proc. 1158, Eds. T. Usuda, M.
Tamura, M. Ishii, 127-128.
Ishihara, Y., Morota, T., Iwata, T., Namiki, N., Goossens, S.,
Matsumoto, K., Noda, H., Araki, H., Hanada, H., Tazawa,
S., Sasaki, S.: 2010, Lunar Crustal Thickness and Impact Basin
Structures Based on Kaguya Gravity and Topography Data,
Proc. of the 42th ISAS Lunar and Planetary Symp., 59-62.
Ishikawa, R., Tsuneta, S.: 2009, Propeties of Transient Horizontal
Magnetic Fields, ASP Conf. Ser. 415, Eds. B. Lites, M. Cheung,
T. Magara, J. Mariska, K. Reeves, 132-139.
Ishiyama, H., et al. including Kajino, T.: 2009, A Systematic Studyof Astrophysical Reaction Rates through Li8, AIP Conf. Proc.
1120, Eds. S. C. Jeong, Y. Utsuno, T. Motobayashi, A. Bracco,177-182.

Ita, Y., IRSF Variable Star Survey Team, SIRIUS Variable Star
Survey Team: 2009, IRSF/SIRIUS JHKs Near-Infrared Variable
Star Survey in the Magellanic Clouds, AIP Conf. Proc. 1170,
Eds. J. A. Guzik, P. A. Bradley, 321-323.
Ito, H., Aoki, W., Honda, S., Beers, T. C., Tominaga, N.: 2010, The
9th Magnitude CEMP star BD+44°493: Origin of its Carbon
Excess and Beryllium Abundance, IAU Symp. 265, Eds. K.
Cunha, M. Spite, B. Barbuy, 124-125.
Ito, T.: 2009, NIR lightcurve of (832) Karin and its rotation, Proc.
of the N-body Dynamics Symposium, March 13-14, 2009,
National Astronomical Observatory, Mitaka, Tokyo, Japan, Ed.
M. Sekiguchi, 14-23.
Iye, M.: 2009, National Astronomical Observatory, AAPPS
Bulletin, 19(3), 5-10.
Jenniskens, P., Genovese, L., Barentsen, G., Vaubaillon, J.,
Watson, W., Godley, W., Lunsford, R., Kozich, P., Stone,
W.: 2009, Perseid Meteors 2009, Central Bureau Electronic
Telegrams 2009, Ed. D. W. E. Green, 1921, 1.
Jenniskens, P., Sato, M., Watanabe, J.: 2009, Orionid Meteors
2009, Central Bureau Electronic Telegrams 2009, Ed. D. W. E.
Green, 1976, 1.
Kameya, O., Vera Team: 2009, Water Vapor Masers in the
NGC7538 Region, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E.
Fomalont, M. Tsuboi, Y. Murata, 369.
Kandori, R., Tamura, M., Morino, J., Ishii, M., Suzuki, R.,
Hashimoto, J., Kusakabe, N., Narita, N., Sato, B., Yamada,T., Enya, K., Goto, M., Carson, J., Thalmann, C., McElwain,
M., Moro-Martin, A., Knapp, J., Turner, E. L.: 2009, Selectionof Nearby Star Targets for the Subaru Strategic Exploration of
Exoplanets and Disks, AIP Conf. Proc. 1158, Eds. T. Usuda, M.
Tamura, M. Ishii, 251-252.
Kandori, R., Tamura, M., Tatematsu, K., Kusakabe, N., Nakajima,
Y.: 2009, Distortion of magnetic fields in the pre-stellar core
Barnard 68, IAU Symp. 259, Eds. K. G. Strassmeier, A. G.
Kosovichev, J. E. Beckman, 107-108.
Kanoh, T., Shibai, H., Fukagawa, M., Matsuo, T., Kato, E.,
Itoh, Y., Kawada, M., Watabe, T., Kohyama, T., Matsumoto,Y., Morishita, H., Yamamoto, K., Kanoh, R., Nakashima, A.,
Tanabe, M., Narita, M.: 2009, Development of the Far-Infrared
Interferometric Telescope Experiment, AIP Conf. Proc. 1158,
Eds. T. Usuda, M. Tamura, M. Ishii, 389-390.
Kato, Y., Magara, T., Shimizu, T.: 2009, Radiation Transfer
Analysis on Heating Mechanism of Magnetohydrodynamic
Emerging Magnetic Flux Tube, ASP Conf. Ser. 415, Eds. B.
Lites, M. Cheung, T. Magara, J. Mariska, K. Reeves, 272-274.
Katsukawa, Y., Jurcak, J.: 2009, Donwflow Patches in a Penumbra
Observed with the Hinode Spectropolarimeter, ASP Conf.
Ser. 415, Eds. B. Lites, M. Cheung, T. Magara, J. Mariska, K.
Reeves, 117-120.
Kawagoe, S., Takiwaki, T., Kotake, K.: 2010, Neutrino oscillationsin MHD supernova explosions, J. Phys.: Conf. Ser., 203, Eds. E.
Coccia, L. Pandola, N. Fornengo, R. Aloisio, 12128.
Kawaguchi, N.: 2009, HALCA Data Recording and ASTRO-G,ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi,
Y. Murata, 18.
Kawakami, A., Takeda, M., Uzawa, Y., Wang, Z.: 2009, Design

and Fabrication of Epitaxial NbN/MgO/NbN SIS Mixers, Int.
Superconductive Electronics Conf. 2009 (ISEC2009), MD-P18.
Kawakatu, N., Nagai, H., Kino, M.: 2009, A New Evolution
Scenario of Compact Symmetric Objects, ASP Conf. Ser. 402,
Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 299.
Kawakatu, N., Wada, K.: 2009, Co-Evolution Model of AGNs
and Nuclear Starbursts, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E.
Fomalont, M. Tsuboi, Y. Murata, 148153.
Kikuchi, F., Matsumoto, K., Goossens, S., Ishihara, Y., Liu,
Q., Iwata, T., Namiki, N., Noda, H., Hanada, H., Sasaki, S.,
RSAT/VRAD mission team: 2010, On the latest lunar gravity
field model from SELENE and historical tracking data, Proc. of
the 42th ISAS Lunar and Planetary Symp., 76-79.
Kim, M. K., Hirota, T., Honma, M., Kobayashi, H.: 2009, SiO
Maser Observations toward Orion-KL with VERA, ASP Conf. Ser.
402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 469.
Kino, M., Asada, K., Hagiwara, Y., Edwards, P. G., VSOP-2
Science Working Group: 2009, Direct Observations of the
Dynamics and Variability at High Energy Emission Regionsin TeV Blazars, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E.
Fomalont, M. Tsuboi, Y. Murata, 270.
Kino, M., Takahara, F.: 2009, Invisible Plasma Content in Blazars?
—: The Case of Markarian 421, ASP Conf. Ser. 402, Eds. Y.
Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 303.
Kitamura, M., Yamada, T., Tamura, M., Kudo, T.: 2009, Direct
Imaging of the Pre-outburst FU Ori Candidate V1331 Cyg, AIP
Conf. Proc. 1158, Eds. T. Usuda, M. Tamura, M. Ishii, 135-136.
Kiuchi, H., Kawanishi, T.: 2009, Photonic millimeter-wave
generation and transmission system applicable to the highfrequency Radio Interferometers, EFTF-IFCS 2009, 880-885.
Kiuchi, H., Kawanishi, T.: 2009, Photonic millimeter-wave
generation and transmission techniques for the high-frequency
Radio Interferometers, LEOS 2009, 591-592.
Kojima, K., Kajino, T., Mathews, G. J.: 2009, Neutrino masseffects on the CMB polarization with PMF, AIP Conf. Proc.
1120, Eds. S. C. Jeong, Y. Utsuno, T. Motobayashi, A. Bracco,303-307.
Kojima, T., Kroug, M., Takeda, M., Shitov, S., Uzawa, Y., Shan,
W., Fujii, Y., Wang, Z.: 2009, A low noise NbTiN-based SIS
mixer for terahertz band, Int. Superconductive Electronics Conf.
2009 (ISEC2009), MD-P32.
Kokubo, E.: 2009, Formation of Terrestrial Planets from Protoplanets, AIP Conf. Proc. 1158, Eds. T. Usuda, M. Tamura, M.
Ishii, 235-238.
Kudo, Y., Kawai, N., Shimokawabe, T., Vasquez, N., Mori, Y. A.,
Yoshida, M., Yanagisawa, K., Nagayama, S., Toda, H., Shimizu,
Y., Kuroda, D., Watanabe, J., Fukushima, H., Mori, M.:
2009, The State of Development and Observation of MITSuME
Telescope, Proc. of the RIKEN Symp., held 10-12 June, 2008.
Kudoh, T., Basu, S.: 2009, Molecular cloud fragmentation driven
by gravity, ambipolar diffusion and nonlinear flows: threedimensional simulations, Revista Mexicana de Astronomía
Astrofísica, 36, Eds. A. Esquivel, et al., CD278.
Kudoh, T., Basu, S.: 2009, Three-dimensional MHD simulationsof molecular cloud fragmentation regulated by gravity,
ambipolar diffusion, and turbulence, IAU Symp. 259, Eds. K. G.

II Publications, Presentations

061

Strassmeier, A. G. Kosovichev, J. E. Beckman, 115.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2010, GRB100305A:
Optical upper limits at IAO, GRB Coordinates Network,
Circular Service, 10482, Ed. B. Scott, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Yoshida, M., Kawai, N.: 2010, GRB100206: MITSuME
optical upper limits, GRB Coordinates Network, CircularService, 10388, Ed. B. Scott, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nakajima, H.,
Yatsu, Y., Mori, Y. A., Endo, A., Shimokawabe, T., Kawai, N.,
Nagayama, S., Yoshida, M., Ohta, K.: 2010, GRB 100219A
Akeno and Okayama MITSuME Optical Observation, GRB
Coordinates Network, Circular Service, 10430, Ed. B. Scott, 1.
Kuroda, D., Yoshida, M., Isogai, M., Yanagisawa, K., Shimizu,
Y., Nagayama, S., Toda, H., Kawai, N.: 2009, GRB 090418:
optical observations with Mitsume Okayama and Ishigaki 1mtelescope, GRB Coordinates Network, Circular Service, 9168,
Ed. B. Scott, 1.
Kuroda, D., Yoshida, M., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090401B: upper limitsof Mitsume optical observation, GRB Coordinates Network,
Circular Service, 9080, Ed. B. Scott, 1.
Kuroda, D., Yoshida, M., Yanagisawa, K., Shimizu, Y.,
Nagayama, S., Toda, H., Kawai, N.: 2009, GRB 090417B:
Mitsume Okayama optical upper limits, GRB Coordinates
Network, Circular Service, 9143, Ed. B. Scott, 1.
Kusakabe, N., Tamura, M., Kandori, R.: 2009, Magnetic fields
in massive star forming regions: wide-field NIR polarimetry of
M42 and Mon R2, IAU Symp. 259, Eds. K. G. Strassmeier, A. G.
Kosovichev, J. E. Beckman, 97-98.
Kuznetsov, S. A., Melnikov V. F.: 2009, Roles of the selfabsorption and Razin effect on formation of the frequency
spectrum of microwave emission of solar flares, Proc. of AllRussian Conf., The Year of Astronomy: Solar and SolarTerrestrial Physics - 2009, 261-264.
Kuzuhara, M., Tamura, M., Kudo, T., Kandori, R., Ishii, M.,
Nishiyama, S.: 2009, A Substellar Companion with a Very Wide
Separation from a Binary T Tauri Star, AIP Conf. Proc. 1158,
Eds. T. Usuda, M. Tamura, M. Ishii, 253-254.
Lagg, A., Ishikawa, R., Merenda, L., Wiegelmann, T., Tsuneta, S.,
Solanki, S. K.: 2009, Internetwork Horizontal Magnetic Fields
in the Quiet Sun Chromosphere: Results from a Joint Hinode/
VTT Study, ASP Conf. Ser. 415, Eds. B. Lites, M. Cheung, T.
Magara, J. Mariska, K. Reeves, 327-331.
Li, J., Cao, X., Takeda, M., Matsuo, H., Wang, Z., Shi, S.: 2009,
Shot-Noise Characteristics of NbN Superconducting Tunnel
Junctions, Proc. of the 20th Int. Symp. on Space Terahertz
Technology, Eds. E. Bryerton, A. Kerr, A. Lichtenberger, 262.
Li, X.-X., Paine, S., Yao, Q.-J., Shi, S.-C., Matsuo, H., Yang, J.,
Zhang, Q.-Z.: 2009, A Fourier transform spectrometer for site
testing at Dome A, Proc. SPIE 7385, Eds. X.-C. Zhang, J. M.
Ryan,C.-L. Zhang, C.-X. Tang, 73851D-73851D-10.
Lim, S., Hwang, N., Lee, M. G.: 2010, Star clusters in the starburst
galaxy M82, IAU Symp. 266, Eds. R. de Grijs, J. R. D. Lépine,454-457.

062

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Lites, B. W., Kubo, M., Socas-Navarro, H., Berger, T., Frank, Z.,
Shine, R., Tarbell, T., Title, A. M., Ichimoto, K., Katsukawa, Y.,
Tsuneta, S., Suematsu, Y., Shimizu, T., Nagata, S.: 2009, Has
Hinode Revealed the Missing Turbulent Flux of the Quiet Sun?,
ASP. Conf. Ser. 405, Eds. S. V. Berdyugina, K. N. Nagendra, R.
Ramelli, 173-181.
Liu, G., Calzetti, D., Yun, M. S., Wilson, G. W., Draine, B. T.,
Scott, K., Austermann, J., Perera, T., Hughes, D., Aretxaga, I.,
Kohno, K., Kawabe, R., Ezawa, H.: 2010, From Near-Infraredto Millimeter: An Investigation of the Content in the NGC
1512/1510 Pair, AAS Meeting #215, Bulletin of AAS 41, 369.
Liu, Q., Goossens, S., Hanada, H., Kikuchi, F., Matsumoto,K., Iwata, T.: 2010, Same-beam VLBI technique and its
applications, Proc. of the 31st Solar System Science Symp.
Machida, M. N., Inutsuka, S., Matsumoto, T.: 2009, Protostellar
Jet and Outflow in the Collapsing Cloud Core, Protostellar Jetsin Context, Eds. K. Tsinganos, T. Ray, M. Stute, 405-410.
Machida, M. N., Omukai, K., Matsumoto, T., Inutsuka, S.: 2009,
Influence of the Magnetic Field on the Formation of Population
III Stars, Magnetic Fields in the Universe II: From Laboratory
and Stars to the Primordial Universe, Eds. A. Esquivel, J.
Franco, G. García-Segura, E. M. de Gouveia Dal Pino, A.
Lazarian, S. Lizano, A. Raga, 272-277.
Magara, T.: 2009, Saturation of Magnetic Helicity as an Indicatorof the Possible Occurrence of a Solar Flare, ASP Conf. Ser. 415,
Eds. B. Lites, M. Cheung, T. Magara, J. Mariska, K. Reeves,439-442.
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
Cryogenic Integrated Circuits for Superconducting Terahertz
Camera, Proc. of The 9th Japan-Taiwan Microelectronics Int.
Symp., 4-1.
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
GaAs-JFET Cryogenic Readout Electronics for the Superconducting Terahertz Digital Camera, Proc. 34th Int. Conf. on
Infrared, Millimeter, and Terahertz Waves, R5E35.0434.
Matsuo, H., Hibi, Y., Suzuki, T., Naruse, M., Noguchi, T.,
Sekimoto, Y., Uzawa, Y., Nagata, H., Ikeda, H., Ariyoshi,
S., Otani, C., Nitta, T., Yao, Q.-J., Fujiwara, M.: 2009, Superconducting THz Camera with GaAs-JFET Cryogenic Readout
Electronics, AIP Conf. Proc. 1185, 393-396.
Melnikov, V. F., Pyatakov, N. P., Gorbikov, S. P.: 2009, Microwave
diagnostics of the position of an acceleration site and pitchangle anisotropy of accelerated electrons in flaring loops, Proc.
of All-Russian Conf., The Year of Astronomy: Solar and SolarTerrestrial Physics - 2009, 293-298.
Miki, S., Takeda, M., Fujiwara, M., Sasaki, M., Otomo, A., Wang,Z.: 2009, Compact Packaging of Superconducting Nanowire
Single Photon Detectors with Optical Cavity, Int. Superconductive Electronics Conf. 2009 (ISEC2009), MD-P23.
Miki, S., Takeda, M., Fujiwara, M., Sasaki, M., Otomo, A., Wang,Z.: 2009, Superconducting Nanowire Single Photon Detectors
with NbTiN Thin Films, Int. Superconductive Electronics Conf.
2009 (ISEC2009), MD-P06.
Miura, N., Noto, Y., Kato, S., Kuwamura, S., Baba, N., Hanaoka, Y.,
Nagata, S., Ueno, S., Kitai, R., Takami, H.: 2009, Solar Adaptive
Optic system at the Hida Observatory, Proc. SPIE 7015, Eds. N.

Hubin, C. E. Max, P. L. Wizinowich, 70156U-1-U-8.
Miyazaki, A., Shen, Z.-Q., Li, J., Miyoshi, M., Tsuboi, M.,
Tsutsumi, T.: 2009, Flux variability of Sagittarius A* at short
mm-wavelengths, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E.
Fomalont, M. Tsuboi, Y. Murata, 379.
Miyoshi, M., Kameno, S., Ishitsuka, J.: 2009, An Approach to Detect
the Event Horizon in SgrA* Using Ground, ASP Conf. Ser. 402,
Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 380.
Mochizuki, N., Hachisuka, K., Umemoto, T.: 2009, Survey ofOuter Galaxy Molecular Lines Associated with Water Masers,
ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi,
Y. Murata, 384.
Momose, M., Hiramatsu, M., Tsukagoshi, T., Shimajiri, Y., Ikeda,N., Kitamura, Y., Kamegai, K., Ezawa, H., Kawabe, R., Saito,
M.: 2009, Wide-field Imaging Survey of Dust Continuum
Emissions at λ = 1.1 mm toward the Chamaeleon and Lupus
Regions with AzTEC on ASTE, AIP Conf. Proc. 1158, Eds. T.
Usuda, M. Tamura, M. Ishii, 141-142.
Moon, Dae-Sik, Koo, B., Lee, H., Matthews, K., Lee, J., Pyo, T.-S.,
Seok, J., Hayashi, M.: 2009, Dense Iron-predominant Ejecta
and Core-collapse Supernova Explosion in the Young Supernova
Remnant G11.2-0.3, AAS Meeting #214, Bulletin of AAS 41, 762.
Mori, Y. A., Kawai, N., Arimoto, M., Yoshida, M., Ohta, K.: 2009,
MITSuME Telescope Observation of GRB080506, AIP Conf.
Proc. 1133, 232.
Moritani, Y., Nogami, D., Okazaki, A. T., Imada, A., Kambe, E.,
Honda, A. S., Ishino, Y., Suzuki, Y.: 2009, High-Dispersion
Spectroscopy of a Be/X-Ray Binary A0535+26/V725 Tau, ASP
Conf. Ser. 404, Eds. B. Soonthornthum, S. Komonjinda, K. S.
Cheng, K. C. Leung, 154.
Murakami, N., Yokochi, K., Nishikawa, J., Tamura, M., Baba, N.,
Uemura, R., Hashimoto, N., Abe, L., Tavrov, A. V., Kurokawa,T., Takeda, M.: 2009, Development of Fourth-order NullingCoronagraphs for Partially Resolved Stars, AIP Conf. Proc.
1158, Eds. T. Usuda, M. Tamura, M. Ishii, 397-398.
Nagai, H., Asada, K., Doi, A., Kameno, S., Inoue, M.: 2009,
Constraining the Synchrotron Age of 3C 84, ASP Conf. Ser.
402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 106.
Nagai, H., Asada, K., Doi, A., Kino, M., Kameno, S., VSOP-2
Science Working Group: 2009, Disk-Jet Connection in the
Nearby Low Luminosity AGN M 81: A Proposal for VSOP-2
Key Science Program, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E.
Fomalont, M. Tsuboi, Y. Murata, 110.
Nagashima, K., Sekii, T., Kosovichev, A. G., Zhao, J., Tarbell, T.
D.: 2009, Travel-Time Analyses of an Emerging-Flux Region,
ASP Conf. Ser. 415, Eds. B. Lites, M. Cheung, T. Magara, J.
Mariska, K. Reeves, 417-420.
Nagata, H., Matsuo, H., Hibi, Y., Ikeda, H., Fujiwara, M.: 2009,
Development of cryogenic analog amplifiers based on GaAsJFET technology for high impedance array sensors, AIP Conf.
Proc. 1185, 115-118.
Nakamura, K.: 2009, Consistency of Equations for the Single
Scalar Field Case in Secondorder Gauge-invariant Cosmological
Perturbation Theory, Proc. of the 19th Workshop on General
Relativity and Gravitation in Japan, Eds. M. Harada, et al.
Namiki, N., Ishihara, Y., Sasaki, S., Sugita, S., Iwata, T., Kamata, S.,

Mori, A., Sato, M.: 2010, Comparative Study of Compensation
Mechanism of Lunar Impact Basins, Proc. of the 42th ISAS
Lunar and Planetary Symp., 71-75.
Naruse, M., Sekimoto, Y., Suzuki, T., Hibi, Y., Matsuo, H.,
Uzawa, Y., Noguchi, T.: 2009, Design of SIS Imaging Array
for Terahertz Astronomy, Proc. 34th Int. Conf. on Infrared,
Millimeter, and Terahertz Waves, M1B04.0318.
Niino, Y., Totani, T., Kobayashi, M.: 2009, Lyα Emission ofLong GRB Host Galaxies at High Redshift and the Metallicity
Dependence of Long GRB Production, AIP Conf. Proc. 1133, 273.
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani, T.,
Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.: 2009,
Coronagraph Methods on Precise Wavefront Compensation(UNI-PAC) and Deep Achromatic Nulling, AIP Conf. Proc.
1158, Eds. T. Usuda, M. Tamura, M. Ishii, 365-368.
Nishiyama, S., Hatano, H., Tamura, M., Nagata, T.: 2010, Nearinfrared Polarimetry toward the Galactic Center - Magnetic
Field Configuration in the Central One Degree Region -, Proc.
Article for the Galactic Center Workshop 2009.
Nishizawa, A., Taruya, A., Hayama, K., Kawamura, S., Sakagami,
M.: 2009, Searching for nontensorial polarizations of stochastic
gravitational waves with laser interferometers, Proc. of the
19th Workshop on General Relativity and Gravitation in Japan(JGRG19), 271-274.
Noguchi, T., Suzuki, T., Endo, A., Naruse, M., Hibi, Y., Matsuo,
H., Sekimoto, Y.: 2009, Effect of lifetime broadening of superconducting energy gap on quasiparticle tunneling current, Proc.
of the 20th Int. Symp. on Space Terahertz Technology, Eds. E.
Bryerton, A. Kerr, A. Lichtenberger, 74-79.
Okoshi, K., Nagashima, M., Gouda, N., Minowa, Y.: 2010, H
I-Selected Galaxies as a Probe of Galactic Disks, IAU Symp.
262, 402-403.
Orozco-Suarez, D.: 2009, Simulation and Analysis of Hinode
Spectropolarimteric Observations, ASP Conf. Ser. 415, Eds. B.
Lites, M. Cheung, T. Magara, J. Mariska, K. Reeves, 57-62.
Otsuka, M., Tajitsu, A., Izumiura, H., Hyung, S.: 2010, A search fors-process elements in extremely metal-poor halo planetary nebulae,
IAU Symp. 265, Eds. K. Cunha, M. Spite, B. Barbuy, 77-78.
Pyo, T.-S., Kudo, T., Hashimoto, J., Tamura, M.: 2009, Transition
Disks-Key to Disk Evolution and Planet Formation, AIP Conf.
Proc. 1158, Eds. T. Usuda, M. Tamura, M. Ishii, 151-152.
Qiu, W., Wang, Z., Takeda, M., Miki, S., Terai, H., Shimakage,H., Kawakami, A.: 2009, Fabrication and Characterization ofHigh Quality Low Critical Current Density NbN/AlN/NbN
tunnel junctions, Int. Superconductive Electronics Conf. 2009(ISEC2009), TD-P11.
Readon, K. P., Rimmele, T., Tritschler, A., Cauzzi, G., Woeger,
F., Uitenboroek, H., Tsuneta, S., Berger, T.: 2009, ServiceMode Obsevations for Ground-Based Solar Physics, ASP Conf.
Ser. 415, Eds. B. Lites, M. Cheung, T. Magara, J. Mariska, K.
Reeves, 332-336.
Reznikova, V. E., Melnikov, V. F., Ji, H.: 2009, Spatial dynamics offlaring loop footpoints, Proc. of All-Russian Conf., The Year of
Astronomy: Solar and Solar-Terrestrial Physics - 2009, 377-378.
Ross, N., Ly, C., Ota, K., Malkan, M., Sekiguchi, K., SXDS Team:2010, Tracing Star Formation Using Narrowband-Emitters in

II Publications, Presentations

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the SXDS, Bulletin of AAS 42, 259.
Rottler, L., Rau, A., Koda, J., Kirkpatrick, D., Deguchi, S.,
Kaminski, T.: 2010, CARMA Observations of the Mysterious
Galactic Transient V838 Monocerotis, AAS Meeting #215,
Bulletin of AAS 41, 269.
Saito, S., Takeda, M., Shimakage, H., Uzawa, Y., Wang, A., Sekine,N., Hosako, I., Sakai, K.: 2009, Observation of phase transitionin niobium nitride with THz time-domain spectroscopy, Proc.
34th Int. Conf. on Infrared, Millimeter, and Terahertz Waves, 234.
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Hanada, H.,
Matsumoto, K., Goossens, S., Namiki, N., Iwata, T., Sugita,
S.: 2010, Shape and Structure of the Lunar South Pole-Aitken
Basin from KAGUYA (SELENE) Gravity/Topography, Proc. of
the 42th ISAS Lunar and Planetary Symp., 63-66.
Sato, M., Hirota, T., Honma, M., Kobayashi, H., Vera Project
Team: 2009, Superbubble Motion Away from the Galactic
Plane: Astrometry of Water Masers in NGC 281 with VERA,ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi,
Y. Murata, 476.
Sato, S., et al. including Kawamura, S., Fujimoto, M., Fukushima,M., Hayama, K., Ishizaki, H., Kotake, K., Nakamura, K.,
Nishida, E., Nishizawa, A., Obuchi, Y., Okada, N., Takahashi,R., Torii, Y., Ueda, A., Yamazaki, T.: 2009, DECIGO: The
Japanese space gravitational wave antenna, J. Phys.: Conf. Ser.,
154, 12040.
Sawada-Satoh, S., Kameno, S., Nakamura, K., Namikawa, D.,
Shibata, K. M., Inoue, M.: 2009, Positional Coincidence of
H2O Maser and a Plasma Obscuring Torus in the Radio Galaxy
NGC 1052, ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont,
M. Tsuboi, Y. Murata, 127.
Sekido, M., Kawaguchi, N., Koyama, Y., Kimura, M., Kondo, T.,
Takiguchi, H., Hobiger, T., Takefuji, K., Ikeda, T., Shimojo, S.,
Oyama, T., Harai, H., Hara, T., Kono, Y., Kurihara, S., Kokado,
K., Tanimoto, D., Nozawa, K., Takeuchi, H., Uose, H., Fujisawa,
K., Takaba, H.: 2009, e-VLBI Activities in Japan, Proc. of the 8thInt. e-VLBI Workshop. 22-26 June 2009. Madrid, Spain , 24.
Sekiguchi, Y.: 2009, Towards clarlying the central engine of long
gamma-ray bursts, Proc. of the 18th Workshop on General
Relativity and Gravitation in Japan (JGRG18), Ed. Y. Kojima.
Sekii, T.: 2009, Hinode/SOT Helioseismic Observations, ASP Conf.
Ser. 415, Eds. B. Lites, M. Cheung, T. Magara, J. Mariska, K.
Reeves, 405-410.
Shibasaki, K.: 2009, Nonlinear and Diamagnetic Nature of Plasma
and Activities in the Solar Atmosphere, Bulletin of AAS 41, 864.
Shih, Y. H., Chen, W. P., Hsiao, W. S., Tamura, M.: 2009,
Near Infrared Polarimetric Imaging of the Giant H II region
NGC 3576, ASP Conf. Ser. 404, Eds. B. Soonthornthum, S.
Komonjinda, K. S. Cheng, K. C. Leung, 27.
Shiino, T., Todoroki, K., Minh, N., Jiang, L., Shiba, S., Uzawa,Y., Maezawa, H., Sakai, N., Yamamoto, S.: 2009, Improvementof critical temperature of superconducting NbN and NbTiN
thin films using an AlN buffer layer, Int. Superconductive
Electronics Conf. 2009 (ISEC2009), MD-P04.
Shimokawabe, T., Kawai, N., Mori, Y. A., Kudo, Y., Nakajima,
H., Yoshida, M., Yanagisawa, K., Nagayama, S., Toda, H.,
Shimizu, Y., Kuroda, D., Watanabe, J., Fukushima, H.,

064

II Publications, Presentations

Mori, M.: 2009, MITSuME-multicolor optical/NIR telescopes
for GRB afterglows, AIP Conf. Proc. 1133, Eds. M. Charles, K.
Chryssa, G. Neil, 79-81.
Shimonishi, T., Onaka, T., Kat, D., Sakon, I., Ita, Y., Kawamura,A., Kaneda, H.: 2009, Near-infrared Spectroscopic Observationof Ices around Extragalactic Young Stellar Objects, AIP Conf.
Proc. 1158, Eds. T. Usuda, M. Tamura, M. Ishii, 155-156.
Shirasaki, Y., et al. including Ohishi, M., Mizumoto, Y.,
Kawanomoto, S., Yasuda, N., Masunaga, Y.: 2009, Design
and Implementation of the Japanese Virtual Observatory (JVO)
system, Proc. of the 10th Asian-Pacific Regional IAU Meeting(APRIM 2008).
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Kawanomoto,S., Honda, S., Yasuda, N., Masunaga, Y., Ishihara, Y., Machida,Y., Nakamoto, H., Sakamoto, M.: 2009, The Japanese Virtual
Observatory in Action, ASP Conf. Ser. 411, Eds. D. A. Bohlender,
D. Durand, P. Dowler, 396.
Suda, T., Yamada, S., Katsuta, Y., Ishizuka, C., Komiya, Y.,
Nishimura, T., Aoki, W., Fujimoto, M. Y.: 2010, An overall
picture of EMP stars using the stellar abundances for galacticarchaeology(SAGA) database, IAU Symp. 265, Eds. K. Cunha,
M. Spite, B. Barbuy, 90-93.
Sugiyama, K., Fujisawa, K., Wajima, K., Sawada-Satoh, S., Isono,Y., Honma, M., Murata, Y., Mochizuki, N., Doi, A.: 2009, The
Kinematics of the Methanol Maser at 6.7 GHz in Cepheus A,
ASP Conf. Ser. 402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi,
Y. Murata, 392.
Suzuki, R., Tamura, M., Suto, H., Morino, J., Hashimoto, J.,
Kudo, T., Kandori, R., Murakami, N., Nishikawa, J., Ukita, N.,
Takami, H., Guyon, O., Nishimura, T., Hayashi, M., Izumiura,
H., Abe, L., Tavrov, A., Jacobson, S., Stahlberger, V., Yamada,H., Shelton, R., Hodapp, K.: 2009, HiCIAO: A High-contrast
Instrument for the Next Generation Subaru Adaptive Optics, AIP
Conf. Proc. 1158, Eds. T. Usuda, M. Tamura, M. Ishii, 293-298.
Suzuki, T., Noguchi, T., Matsuo, H.: 2009, Origin of subgap
current in an SIS junction, AIP Conf. Proc. 1185, 405-408.
Takeda, M., Nakayama, S., Saito, A., Shimakage, H., Uzawa, Y.,
Ohshima, S., Wang, Z.: 2009, Measurements of Microwave
Surface Resistances of NbN and NbTiN Thin Films, Int.
Superconductive Electronics Conf. 2009 (ISEC2009), HF-P25.
Tamura, M., Takami, M., Enya, K., Ootsubo, T., Fukagawa, M.,
Honda, M., Okamoto, Y. K., Sako, S., Yamashita, T., Hasegawa,
S., Kataza, H., Doi, Y., Matsuhara, H., Nakagawa, T.: 2009, Key
Sciences of SPICA Mission: Planetary Formation, Exoplanets,
and our Solar System, SPICA joint European/JapaneseWorkshop, Eds. A. M. Heras, B. M. Swinyard, K. G. Isaak, J. R.
Goicoechea, 02001.
Tamura, M.: 2009, Subaru Strategic Exploration of Exoplanets
and Disks with HiCIAO/AO188 (SEEDS), AIP Conf. Proc.
1158, Eds. T. Usuda, M. Tamura, M. Ishii, 11-16.
Tamura, N., Sharples, R. M., Arimoto, N., Onodera, M., Ohta, K.,
Yamada, Y.: 2009, A Subaru/Suprime-Cam Wide-Field Surveyof Globular Cluster Populations around M87, ESO Astrophysics
Symposia "Globular Clusters - Guide to the Galaxy", 287-291.
Tanaka, M., Maeda, K., Nomoto, K., Mazzali, P. A., Tominaga,N., Kawabata, K. S., Hattori, T.: 2009, Optical Emission fromAspherical Core-Collapse Supernovae, AIP Conf. Proc. 1111,
Eds. G. Giobbi, et al., 413.
Thalmann, C., Goto, M., Carson, J., Feldt, M., Henning, T., Itoh, Y.,
Janson, M., Kandori, R., Knapp, G. R., Mayama, S., McElwain,
M., Moro-Martín, A., Suzuki, R., Tamura, M., Turner, E. L.,
Usuda, T., Wisniewski, J.: 2009, SPOTS: Search for Planets Of
Two Stars-A Direct Imaging Survey for Exoplanets in Binary
Systems, AIP Conf. Proc. 1158, Eds. T. Usuda, M. Tamura, M.
Ishii, 271-272.
Tsang, E.: 2010, Digitizing newspaper clippings on the Mauna Kea
Astronomy Community, ASP Conf. Ser. 433, 232.
Tsuboi, M., Miyazaki, A., Nakanishi, K., Kamegai, K., Kotani,T.: 2009, A mm-wave Flare from Cyg X-3, The Astronomer's
Telegram, #2053.
Tsujimoto, T., Bekki, K.: 2010, Metal-rich infall onto the inner disk
through the interaction between bulge winds and gaseous halos,
IAU Symp. 265, Eds. K. Cunha, M. Spite, B. Barbuy, 384-385.
Tsujimoto, T., Bland-Hawthorn J., Freeman, K. C.: 2009, Chemical
evolution of the Galaxy disk in connection with large-scale
winds, IAU Symp. 254, Eds. J. Andersen et al., 393-398.
Tsuneta, S., Harra, L. K., Masuda, S.: 2009, Hinode "A New Solar
Observatory in Space", Climate and Weather of the Sun-Earth
System(CAWSES): Selected Papers from the 2007 Kyoto
Symp., Eds. T. Tsuda, R. Fujii, K. Shibata, M. Geller, 63-75.
Uemura, M., Arai, A., Matsui, R., Sasada, M., Ohsugi, T.,
Yamashita, T., Kawabata, K. S., Sato, S., Kino, M., Yoshida, M.,
Kawai, N.: 2009, New Aspects of WZ Sge-Type Dwarf Novae
through Simultaneous Optical-Infrared Observations during
Superoutbursts, ASP Conf. Ser. 404, Eds. B. Soonthornthum, S.
Komonjinda, K. S. Cheng, K. C. Leung, 64.
Ujihara, H., Bushimata, T.: 2009, Measurement of the Antenna
Mesh: Characteeristics for VSOP-2/ASTRO-G, ASP Conf. Ser.
402, Eds. Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 66.
Umemoto, T., Saito, M., Nakanishi, K., Kuno, N., Tsuboi, M.:
2009, Detection of a Radio Flare at Millimeter-Wavelengths
from the X-ray T Tauri Star V773 Tau, ASP Conf. Ser. 402, Eds.
Y. Hagiwara, E. Fomalont, M. Tsuboi, Y. Murata, 400.
Uzawa, Y., Kojima, T., Kroug, M., Takeda, M., Candotti, M.,
Fujii, Y., Kaneko, K., Shan, W., Noguchi, T., Wang, Z.: 2009,
Development of the 787-950 GHz ALMA Band 10 Cartridge,
Int. Superconductive Electronics Conf. 2009 (ISEC2009),
MD-O1.
Vaubaillon, J., Atreya, P., Watanabe, J., Sato, M., Maslov, M.,
Moser, D., Cooke, B., Lyytinen, E., Nissinen, M., Asher, D.,
Jenniskens, P.: 2009, Leonid Meteors 2009, Central Bureau
Electronic Telegrams 2009, Ed. D. W. E. Green, 2019, 2.
Watanabe, H., Kitai, R., Ichimoto, K., Katsukawa, Y.: 2009,
Magnetic Structure of Umbral Dots with SOT SP, ASP Conf.
Ser. 415, Eds. B. Lites, M. Cheung, T. Magara, J. Mariska, K.
Reeves, 378-382.
Wright, D. J., De Cat, P., Pollard, K. R., Maisonneuve, F.,
Kilmartin, P. M., Telting, J. H., Kambe, E., Poretti, E.,
Lehmann, H., Yang, S., Mkrtichian, D., Laney, D., Fu, J. N.:
2009, Results from Classification Observations and a Multi-siteCampaign on γ Doradus and SPB Type Stars, AIP Conf. Proc.
1170, Eds. J. A. Guzik, P. A. Bradley, 467.

Yamada, Y., Shimokawa, T., Shinomoto, S., Yano, T., Gouda,N.: 2009, JASMINE – Japan Astrometry Satellite Mission forINfrared Exploration: Data Analysis and Accuracy Assessmentwith a Kalman Filter, ASP Conf. Ser. 411, Eds. D. A. Bohlender,
D. Durand, P. Dowler, 39.
Yamamoto, K., Matsuo, T., McElwain, M., Tamura, M., Morishita,
H., Nakashima, A., Shibai, H., Fukagawa, M., Kato, E., Kanoh,T., Itoh, Y., Kaneko, Y., Shimoura, M., Itoh, Y., Funayama,
H., Hashiguchi, T.: 2009, SEEDS: Target Selection for OpenClusters and Moving Groups, AIP Conf. Proc. 1158, Eds. T.
Usuda, M. Tamura, M. Ishii, 273-274.
Yasui, C., Kobayashi, N., Tokunaga, A. T., Saito, M., Tokoku, C.:
2009, Disk Fraction in a Low-Metallicity Environment, AIP
Conf. Proc. 1158, Eds. T. Usuda, M. Tamura, M. Ishii, 171.
Yasutake, N., Maruyama, T., Tatsumi, T.: 2009, General Relativistic
Compact Stars with Exotic Matter: Effects of rotation andstrong magnetic field, The 6th Japan-Italy symp. on Heavy-Ion
Physics, Eds. S.-C. Jeong, H. Miyatake, Y. Utsuno, H. Ikezono,
T. Motobayashi, A. Bracco, 146-150.
Yoshida, F., Yagi, M., Komiyama, Y., Nakata, F., Furusawa, H.,
Ohno, T., Okamura, S., Nakamura, T.: 2010, Slitless Spectroscopyof Small Solar System Bodies on a Dark Cloud Curtain, LPI
Contribution No. 1533 (41st Lunar and Planetary Science Conf.,
held March 1-5, 2010 in The Woodlands, Texas), 1290.
Yoshida, F., Ito, T.: 2009, Asteroids: are they dangerous?, Science& Life of Uzbekistan, 73.
Yoshida, F.: 2009, 従特洛依群小行星 探討 太陽系行星形成史 ,台北市立天文教育科学館季刊誌「台北星空」, 46, 6.
Yoshida, M., Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090410: Mitsume optical
upper limits, GRB Coordinates Network, Circular Service, 9126,
Ed. B. Scott, 1.
Yoshida, M., Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090426: Okayama
Mitsume optical observation, GRB Coordinates Network,
Circular Service, 9266, Ed. B. Scott, 1.
Yoshida, M., Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090529: Mitsume opticalobservation, GRB Coordinates Network, Circular Service, 9467,
Ed. B. Scott, 1.
Yoshida, M., Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090807: Mitsume optical
upper limit, GRB Coordinates Network, Circular Service, 9752,
Ed. B. Scott, 1.
Yoshida, M., Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090831B: Mitsume optical
upper limits, GRB Coordinates Network, Circular Service,
9858, Ed. B. Scott, 1.
Yoshida, M., Kuroda, D., Yanagisawa, K., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 091208B: MITSuMEOkayama Optical Observation, GRB Coordinates Network,
Circular Service, 10258, Ed. B. Scott, 1.
Yoshida, M., Yanagisawa, K., Kuroda, D., Shimizu, Y., Nagayama,S., Toda, H., Kawai, N.: 2009, GRB 090423: near infraredobservation at Okayama observatory, GRB Coordinates
Network, Circular Service, 9218, Ed. B. Scott, 1.

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Yoshida, T., Suzuki, T., Chiba, S., Kajino, T., Yokomakura, H.,
Kimura, K., Takamura, A., Hartmann, D. H.: 2009, Neutrino
Nucleosynthesis in Supernovae, AIP Conf. Proc. 1120, Eds. S. C.
Jeong, Y. Utsuno, T. Motobayashi, A. Bracco, 165-170.
Yoshida, T., Takamura, A., Kimura, K., Yokomakura, H., Kawagoe,
S., Kajino, T.: 2009, Effects of Spin-Flavor Conversion inSupernova Neutrino Signal, AIP Conf. Proc. 1120, Eds. S. C.
Jeong, Y. Utsuno, T. Motobayashi, A. Bracco, 298.
Younger, J. D., Fazio, G. G., Wilner, D. J., Ashby, M. L. N.,
Blundell, R., Gurwell, M. A., Huang, J.-S., Iono, D., Peck,A. B., Scott, K. S., Wilson, G. W., Yun, M. S.: 2009, Are theMost Luminous Submillimeter Galaxies Eddington Limited
Starburst?, ASP Conf. Ser. 408, Eds. W. Wang, Z. Yang, Z. Luo,Z. Chen, 405-409.
Zhu, M., Papadopoulos, P. P., Xilouris, M., Kuno, N., Lisenfeld, U.:
2009, Is the Gas and Dust Mass Over-Estimated in the Starburst
Galaxy NGC 3310?, ASP Conf. Ser. 408, Eds. W. Wang, Z.
Yang, Z. Luo, Z. Chen, 76-79.

5. Publications in English
Hagiwara, Y., Fomalont, E., Tsuboi, M., Yasuhiro, M.: 2009,
Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technologies, ASP.
Nakata, F., Yagi, M., Yoshida, F., Marsden, B. G.: 2009, 2009
KK30, 2009 KL30, 2009 KM30, 2009 KN30, 2009 KO30,
Minor Planet Electronic Circ., 2009-P22.
Usuda, T., Ishii, M., Tamura, M.: 2010, Proceedings of theInternational Conference "Exoplanets and Disks: Their
Formation and Diviersity", AIP, New York.

6. Conference Presentations
Agata, H.: 2009, “You are also Galileo” Project - Produced by the
IYA Japan, Global Hands-On Universe Workshop 2009, (Porto
Alegre, Brazil, Jul. 23-27, 2009).
Agata, H.: 2009, The You are also Galileo! Telescopes, IAU XXVII
General Assembly, (Rio De Janeiro, Brazil, Aug. 03-14, 2009).
Agata, H.: 2010, Evaluation of You are also Galileo! Project,
Communicating Astronomy with the Public 2010, (Cape Town,
South Africa, Mar. 15-19, 2010).
Ando, H., Tsuboi, Y., Kambe, E., Sato, B.: 2009, Characteristics ofOscillations in G-type Giants, The 4th Workshop on Extra-Solar
Planet Search with Accurate Radial Velocity Measurements,(Sapporo, Japan, Oct. 7-9, 2009).
Aoki, W.: 2009, Alpha-elements in dwarf spheroidal galaxies andthe Galactic halo, Workshop on using the [alpha/Fe] as a tracerof formation and evolution of the Galaxy, (Beijing, China, Sep.
28-30, 2009).
Aoki, W.: 2009, Carbon-Enhanced Metal-Poor (CEMP) stars, IAU
symp. 265 "Chemical Abundances in the Universe: Connecting
First Stars to Planets", (Rio de Janeiro, Brazil, Aug. 10-14, 2009).
Aoki, W.: 2009, Enrichment of the heaviest elements Th and Pb
in the Galaxy, Third Joint Meeting of the Nuclear Physics
Divisions of the APS and JPS, (Hawaii, Oct. 13-17, 2009).
Aoki, W.: 2010, Extremely metal-poor stars in dwarf galaxies

066

II Publications, Presentations

around the Milky Way, Origin of Matter and Evolution of
Galaxies, (Osaka, Japan, Mar. 8-10, 2010).
Araki, H., et al.: 2009, Results from the One Year Topographic
Observation by the Laser Altimeter (LALT) aboard KAGUYA(SELENE), Asia-Oceania Geoscience Society 6th Annual
Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S.,
Sasaki, S., Kawano, N., Kamiya, I., Ohtake, H., Obserst, J.,
Shum, C. K.: 2009, Lunar global topographic map by the
Kaguya laser altimeter (LALT), The Moon, moons & Planets,(Kazan, Russia, Aug. 24-26, 2009).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S.,
Sasaki, S., Oberst, J., Shum, C. K.: 2010, Operation summary
and accuracy of the lunar topography by KAGUYA–LALT, 4th
KAGUYA (SELENE) Science Working Team Meeting, (Tokyo,
Japan, Jan. 31-Feb. 2, 2010).
Ariyoshi, S., Otani, C., Dobroiu, A., Sato, H., Taino, T., Matsuo,
H., Shimizu, H. M.: 2009, Two-dimensional Superconducting
Detector Array for Terahertz Imaging Applications, Int.
Superconductive Electronics Conf. 2009, (Fukuoka, Japan, Jun.
16-19, 2009).
Ariyoshi, S., Taino, T., Dobroiu, A., Sato, H., Matsuo, H., Otani, C.:
2009, Design of Terahertz Detector based on a Superconducting
Tunnel Junction Coupled to a Thin Superconductor Film, The
34th Int. Conf. on Infrared, Millimeter, and Terahertz Waves,(Busan, Korea, Sep. 21-25, 2009).
Asai, A., Hara, H., Watanabe, T., Imada, S.: 2009, Flare onset
observed with Hinode in the 2006 December 13 flare, Hinode-3:
The 3rd Hinode Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Asai, A.: 2009, Flare Dynamics and Geoeffectiveness: Observationsof Solar Active Regions that Generate Geoeffective Flares/
CMEs, Asia-Oceania Geoscience Society 6th Annual Meeting,(Suntech, Singapore, Aug. 11-15, 2009).
Asai, A.: 2009, Flare onset observed with Hinode in the 2006
December 13 flare, Hinode-3: The 3rd Hinode Science Meeting,(Tokyo, Japan, Dec. 1-4, 2009).
Bando, T.: 2010, UV telescope Contamination Control, The 2nd
SOLAR-C Science Definition Meeting, (Sagamihara, Japan,
Mar. 9-12, 2010).
Barinov, A. V., Melnikov, V. F., Ji, H.: 2009, A comparative analysisof the microwave spectral evolution from the flaring loop top
and foot points, The Pulkovo conf. "The Year of Astronomy:
Solar and Solar-Terrestrial Physics – 2009", (Saint-Peterbug,
GAO RAS, Russia, Jul. 5-11, 2009).
Bussey, D. B. J., McGovern, J. A., Spudis, P. D., Neish, C., Sorensen,
S., Noda, H., Ishihara, Y.: 2010, Lunar Polar Illumination
Conditions Derived Using Kaguya Laser Data, 41st Lunar andPlanetary Science Conf. (LPSC 2010), (Woodlands, Texas,
USA, Mar. 1-5, 2010).
Candotti, M., Uzawa, Y., Fujii, Y., Kojima, T.: 2009, Design
study for the local oscillator injection scheme for the ALMA
band 10 receiver, Int. Symp. on Space THz Technology 2009,(Virginia, USA, Apr. 20-22, 2009).
Fujii, M., Iwasawa, M., Funato, Y., Makino, J.: 2009, Star Cluster
Migration near the Galactic Center, IAU Symp. 267 "Evolutionof Galaxies and Central Black Holes: Feeding and Feedback",

(Rio de Janeiro, Brazil, Aug. 10-14, 2009).
Fujii, M.: 2009, Self-consistent N-body simulation of star clusters
within their parent galaxies, Star Formation and Star Clusters,(Seoul, Korea, Apr. 9, 2009).
Fujiwara, M., Nagata, H., Hibi, Y., Matsuo, H., Sasaki, M.: 2009,
Cryogenic Low Noise Amplifier with GaAs JFETs, 13th Int.
Workshop on Low Temperature Detectors LTD-13, (Stanford,
USA, Jul. 20-24, 2009).
Goossens, S., et al.: 2009, Updated Lunar Gravity Results From
Kaguya (SELENE) and Historical Tracking Data, AGU Fall
Meeting, (San Francisco, USA, Dec. 14-18, 2009).
Goossens, S., Matsumoto, K., Liu, Q., Kikuchi, F., Ishihara,Y., Noda, H., Hanada, H., Kawano, N., Iwata, T., Namiki,N., Lemoine, F. G., Rowlands, D. D.: 2010, Lunar gravity fieldmodelling with VLBI data and orbit determination using altimetry
crossovers, 4th KAGUYA (SELENE) Science Working Team
Meeting, (Tokyo, Japan, Jan. 31-Feb. 2, 2010).
Goossens, S., Matsumoto, K., Liu, Q., Kikuchi, F., Noda,
H., Namiki, N., Iwata, T., Hanada, H., Ishihara, Y.: 2009,
Lunar Gravity Results from Kaguya (SELENE) and Historical
Tracking Data, Asia-Oceania Geoscience Society 6th Annual
Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Goossens, S.: 2009, Lunar Orbit Determination with Kaguya:
Models and Data, NASA/GSFC Seminar, (GSFC, NASA, USA,
Sep. 16, 2009).
Gouda, N., JASMINE working group: 2009, JASMINE projects:
Series of Infrared Space Astrometry Missions, The Milky Way
and the Local Group - Now and in the Gaia Era, (The University
of Heidelberg, Germany, Aug. 31-Sep. 4. 2009).
Gouda, N., JASMINE working group: 2009, JASMINE: Infrared
Space Astrometry Mission, 27th Int. Symp. on Space Technology
and Science, (Tsukuba, Japan, Jul. 5-12, 2009).
Gouda, N., JASMINE working group: 2009, Series of JASMINE
projects -Exploration of the Galactic bulge-, Commission 8
Science meeting at IAU Gneral Assembly 27, (Rio de Janeiro,
Brazil, Aug. 10, 2009).
Gusev, A., Noda, H.: 2010, Prospects for Lunar Laser Ranging inJapan and in Russia, First Workshop: Theory and Model for the
New Generation of the Lunar Laser Ransing Data, (ISSI, Bern,
Switzerland, Feb. 16-19, 2010).
Hada, K.: 2010, Strong gradient of the spectral index in the compact
jet of the low-luminosity active galactic nucleus M 81, Galactic
Center Workshop 2009, (Shanghai, China, Oct. 19-23, 2009).
Hamana, T.: 2009, Prospects and issues of HSC weak lensing
survey, Science Opportunities with Wide-Field Imaging andSpectroscopy of the Distant Universe, (Princeton, New Jersey,
USA, Nov. 9-11, 2009).
Hanada, H., Gusev, A., Petrova, N.: 2010, Physical Librations
and Interior of the multi-layered Moon in Japanese andRussian space programs of 2010-2014 yrs, Int. Astron. Forum"ASTROKAZAN – 2010", (Kazan, Russia, Feb. 9-10, 2010).
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,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 in SELENE (Kaguya) for precise
orbit determination and lunar gravity field study, 4th KAGUYA(SELENE) Science Working Team Meeting, (Tokyo, Japan, Jan.
31-Feb. 2, 2010).
Hanada, H., Noda, H., Kikuchi, F., Tazawa, S., Kunimori, H.,
Matsumoto, K., Araki, H., Iwata, T., Funazaki, K., Sasaki,
S.: 2009, Different kinds of Observation of Lunar Rotation andGravity for SELENE-2, The Moon, moons & Planets, (Kazan,
Russia, Aug. 24-26, 2009).
Hanada, H., Sasaki, S., Kikuchi, F., Noda, H., Iwata, T., Funazaki,
K., Kawano, N., Kunimori, H., RISE Project Team: 2009,
Observation of Lunar Rotation by Future Landing Missions,
European Geosciences Union General Assembly 2009, (Vienna,
Austria, Apr. 19-24, 2009).
Hanada, H., Sasaki, S., Kikuchi, F., Noda, H., Matsumoto,K., Araki, H., Iwata, T., Funazaki, K., Kunimori, H., RISE
Project Team: 2009, Lunar Rotation and Gravity by SELENE-2,
The 2nd Annual NLSI Lunar Science Forum, (Moffett Field,
California, USA, Jul. 21-23, 2009).
Hanada, H., Sasaki, S., Kikuchi, F., Noda, H., Matsumoto, K.,
Araki, H., Iwata, T., Funazaki, K., Kunimori, H., RISE Project
Team: 2009, Observation of lunar rotation in SELENE-2, JPL
Seminar, (JPL, NASA, USA, Jul. 16, 2009).
Hanaoka, Y.: 2009, Professional-Amateur Collaborative Networkof Japan for White-light Imaging Observations of the July2009 Eclipse, The Dynamic Solar Corona, (Suzhou, China, Jul.
23-26, 2009).
Hanawa, T.: 2009, A New Scheme to Solve Gas Disks aroundStars, 4th Int. Conf. on Numerical Modeling of Space Plasma
Flows, (Chamonix, France, Jun. 30, 2009)
Hara, H., JAXA SOLAR-C WG: 2009, JAXA SOLAR-C Mission,
SPD 2009 meeting in American Astronomical Society, (Boulder,
CO, USA, Jun. 14-18, 2009).
Hara, H., JAXA SOLAR-C WG: 2009, The SOLAR-C Plan-A,
Hinode-3: The 3rd Hinode Science Meeting, (Tokyo, Japan,
Dec. 1-4, 2009).
Hara, H.: 2009, Coronal Heating Mechanisms Resticted from
Coronal Plasma Motions in Active region Loops, Asia-Oceania
Geoscience Society 6th Annual Meeting, (Suntech, Singapore,Aug. 11-15, 2009).
Hara, H.: 2009, Plasma motions and heating by magnetic
reconnection in 2007 May 19 flare, Hinode-3: The 3rd Hinode
Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Hara, H.: 2009, SOLAR-C out-of-ecliptic mission orbit andspacecraft systems, 3rd Solar Orbiter Workshop, (Sorrent, Italy,
May 25-29, 2009).
Hara, H.: 2009, The SOLAR-C Mission, Asia-Oceania Geoscience
Society 6th Annual Meeting, (Suntech, Singapore, Aug. 11-15,
2009).
Hara, H.: 2009, The SOLAR-C Plan-A, Hinode-3: The 3rd Hinode
Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Hara, H.: 2010, Instrumentation & Data rates, The 2nd SOLAR-C
Science Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Hara, H.: 2010, Plan A Mission description, The 2nd SOLAR-C

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067

Science Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Harada, Y.: 2009, Long-Term Polar Motion on a Quasi-Fluid Planetwith an Elastic Lithosphere: Semi-Analytic Solutions of theTime-Dependent Equation, Asia-Oceania Geoscience Society
6th Annual Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Harada, Y.: 2009, Long-Term Polar Motion on a Quasi-Fluid
Planet with an Elastic Lithosphere: Semi-Analytic Solutionsof the Time-Dependent Equation, AGU Fall Meeting, (SanFrancisco, USA, Dec. 14-18, 2009).
Harada, Y.: 2009, True Polar Wander Due to Surface Mass
Loading on Mars: Implication to Evolution of the Tharsis
Province, European Geosciences Union General Assembly
2009, (Vienna, Austria, Apr. 19-24, 2009).
Hatsutori, Y., Gouda, N., Kobayashi, Y., Yano, T., Yamada, Y.,
Nano-JASMINE Project Team: 2009, A very small satellite
for space astrometry: Nano-JASMINE, Commission 8 Science
meeting at IAU Gneral Assembly 27, (Rio de Janeiro, Brazil,
Aug. 10, 2009).
Hatsutori, Y., Kobayashi, Y., Gouda, N., Yano, T., Yamada, Y.,
Niwa, Y.: 2009, Development of 5cm Reflecting Telescope for
Nano-JASMINE, 27th Int. Symp. on Space Technology and
Science, (Tsukuba, Japan, Jul. 5-12, 2009).
Hayano, Y., Takami, H., Oya, S., Hattori, M., Saito, Y., Watanabe,M., Minowa, Y., Egner, S., Guyon, O., Ito, M., Garrel, V.,
Colley, S., Dinkins, M., Golota, T., Kurakami, T., Nabeshima,Y., Saito, N., Wada, S., Shibuya, T., Iye, M.: 2009, A Laser
Guide Star Adaptive Optics System of Subaru Telescope, OSA
topical meeting on Nonlinear Optics, (Honolulu, HI, USA, Jul.
12-17, 2009).
Hayashi, M., Takeda, T., Nakayama, H.: 2009, 4D2U demonstration,
Astronomical Data Analysis Software and Systems XIX,
(Sapporo, Japan, Oct. 4-8, 2009).
Hibi, Y., Matsuo, H., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
The Cryogenic Digital Readout Module with GaAs JFET Ics,
13th Int. Workshop on Low Temperature Detectors LTD-13,(Stanford, USA, Jul. 20-24, 2009).
Hibi, Y.: 2009, Cyogenic digital readout system with GaAs JFETs,
10th Workshop on Submillimeter-Wave Receiver Technologies
in Eastern Asia, (Wuxi, China, Nov. 15-18, 2009).
Hibi,Y., Matsuo, H., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
The cryogenic digital readout system with GaAs JFETs, The Int.
Workshop on Terahertz Technology 2009, (Osaka, Japan, Nov.
30-Dec. 3, 2010).
Hirota, T.: 2010, Detailed studies on newly found chemically young
cores in the Aquila region, The Third Tokyo-NRO Workshop
Submillimeter and THz Astrochemistry, (Tokyo, Japan, Mar.
17-18, 2010).
Hong, P. K., Sugita, S., Okamura, N., Sekine, Y., Terada, H., Takato,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 and Planetary
Science Conf. (LPSC 2010), (Woodlands, Texas, USA, Mar.
1-5, 2010).
Honma, M.: 2009, Galactic Structure Seen with VLBI Astrometry,068

II Publications, Presentations

New Science Enabled by Microarcsecond Astronmetry,(Socorro, NM, USA, Jul. 21-23, 2009).
Hosokawa, T.: 2010, Evolution of Massive Protostars andFormation of Massive Stars, Multi-Phase Interstellar Medium
and Dynamics of Star Formation, (Nagoya, Japan, Feb. 28-Mar.
2, 2010).
Hwang, N.: Nov-09, Extended Star Clusters and Galaxy Evolution,
The 2nd Japan-Korea Joint Workshop: Galaxy Build-Up AcrossCosmic Ages and Environments, (Hiraizumi, Japan, Nov. 25-28,
2009).
Ikeda, H., Ogawa, M., Hirota, M., Mori, S., Aoshima, C., Ohnishi,T., Ishibashi, S., Noda, H., Ishihara, Y., Iwata, T., Namiki, N.:
2009, Lunar Gravity Field Estimation Results of SELENE(KAGUYA), Asia-Oceania Geoscience Society 6th Annual
Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Imanishi, M.: 2009, Buried AGNs in luminous infrared galaxies
and the origin of galaxy down-sizing, Huntinh for the Dark: The
Hidden Side of Galaxy Formation, (Malta, Oct, 19-23, 2009).
Imanishi, M.: 2009, Luminous buried AGNs in the local universe,
Joint Subaru/Gemini Science Conf., (Kyoto, Japan, May 18-21,
2009).
Imanishi, M.: 2009, Luminous buried AGNs in the local universe
and the origin of galaxy downsizing, TIARA Workshop on AGN
and Star Formation, (Taipei, Taiwan, Nov. 16-20, 2009).
Imanishi, M.: 2009, Nobeyama millimeter interferometric observations of high density molecular gas in luminous infrared
galaxies, Millimeter and Submillimeter Astronomy at High
Angular Resolution, (Taipei, Taiwan, Jun. 8-12, 2009).
Imanishi, M.: 2009, The AGN-starburst connections and originof galaxy downsizing in the distant universe, SPICA Joint
European - Japanese Workshop, (Oxford, UK, Jul. 6-8, 2009).
Inoue, H., Noguchi, T., Kohno, K.: 2009, SIS junction using asa microwave noise source, 9th European Conf. on Applied
Superconductivity, (Dresden, Germany, Sep. 15, 2009).
Inoue., T.: 2009, Turbulence and Magnetic Field Amplificationin SNRs, Shock Waves, Turbulence, and Particle Acceleration,(Pohang, Korea, Nov. 18-21, 2009).
Inoue., T.: 2010, Nonlinear Evolution of Thermal Instability
Behind Shock Wave and Formation of Molecular Cloud, MultiPhase Interstellar Medium and Dynamics of Star Formation,(Nagoya, Japan, Feb. 28-Mar. 2, 2010).
Ishihara, Y., Morota, T., Iwata, T., Matsumoto, K., Goossens,S., Sasaki, S.: 2010, Lunar large impact basin structures andimplications for thermal history, 41st Lunar and Planetary Science
Conf. (LPSC 2010), (Woodlands, Texas, USA, Mar. 1-5, 2010).
Ishihara, Y., Namiki, N., Sugita, S., Matsumoto, K., Goossens,S., Araki, H., Noda, H., Sasaki, S., Iwata, T., Hanada, H.:
2009, Localized gravity/topography correlation and admittancespectra on the Moon, European Geosciences Union General
Assembly 2009, (Vienna, Austria, Apr. 19-24, 2009).
Ishihara, Y., Yamamoto, M.-Y., Kanao, M.: 2009, Current Status of
Infrasound Pilot Observation at Japanese Islands and SYOWA
Antarctica, and Development of New Infrasound Sensor using
Optical Sensing Method, AGU Fall Meeting, (San Francisco,USA, Dec. 14-18, 2009).
Ishihara, Y.: 2009, results by RSAT/VRAD and LALT: new insighton the crustal thickness, SELENE-2 LBBS (Seismology) Team
int. meeting on lunar interior, (Tokyo, Japan, Nov. 24, 2009).
Ishikawa, R.: 2009, 3D view of transient horizontal magnetic
fields in the convection zone with Hinode, Hinode-3: The 3rd
Hinode Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Ito, H., Aoki, W., Honda, S., Beers, T. C., Tominaga, N.: 2009, A very
low upper limit for a Beryllium abundance of a carbon-enhanced
metal-poor star BD+44°493, IAU Symp. 268 "Light Elements in
the Universe", (Geneva, Switzerland, Nov. 9-13, 2009).
Ito, H., Aoki, W., Honda, S., Beers, T. C., Tominaga, N.: 2009, The
9th Magnitude CEMP Star BD+44°493: Origin of its Carbon
Excess and Beryllium Abundance, IAU symp. 265 "Chemical
Abundances in the Universe: Connecting First Stars to Planets",(Rio de Janeiro, Brazil, Aug. 10-14, 2009).
Ito, H., Aoki, W., Honda, S., Beers, T. C.: 2009, The Exceptionally
Bright Carbon-Enhanced Metal-Poor Star BD+44°493, Joint
Subaru/Gemini Science Conf., (Kyoto, Japan, May 18-21, 2009).
Ito, H., Kino, M., Kawakatu, N., Yamada, S.: 2009, Non-Thermal
emissions from shocked shells driven by powerful AGN jets,
HEPRO II conf., (Buenos Aires, Argentina, Oct. 26, 2009).
Ito, T., Higuchi, A.: 2009, Impact probability of the Oort cloudcomets on planets, Asia-Oceania Geoscience Society 6th Annual
Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Ito, T., Yoshida, F., Ibrahimov, M.: 2009, Photometric observationsof young asteroid families at Maidanak Observatory, AsiaOceania Geoscience Society 6th Annual Meeting, (Suntech,Singapore, Aug. 11-15, 2009).
Ito, T.: 2010, JSPS Asia-Africa science platform program, 2010
Asian asteroid observation network workshop, (Lijiang, China,
Mar. 11-13, 2010).
Iwata, I.: 2009, Detections of ionizing radiation from high-z galaxies,
Reionization with Multi-frequency Datasets, (Stockholm,
Sweden, Jul. 17-21, 2009).
Iwata, I.: 2009, Observations of Forming Galaxies at z>4 andCosmic Reionization, Joint Subaru/Gemini Science Conf.,(Kyoto, Japan, May 18-21, 2009).
Iwata, I.: 2009, Observing the Dark Universe with Euclid, WISH
- Wide-field Imaging Surveyor for High-redshift, (Noordwijk,
Nederlanden, Nov. 17-18, 2009).
Iwata, T., Hanada, H., Noda, H., Kikuchi, F., Tazawa, S., Kunimori,
H., Matsumoto, K., Imai, K., Ishihara, Y., Harada, Y., Sasaki,
S.: 2010, Lunar, Martian, and Jovian Geodesy and Science
Mission using VLBI and Astrometrical Technology, IVS
GM2010, (Hobart, Australia, Feb. 7-14, 2010).
Iwata, T., Namiki, N., Hanada, H., Matsumoto, K., Noda, H.,
Ishihara, Y., Goossens, S., Liu, Q., Kikuchi, F., Ogawa, M.,
Asari, K., Tsuruta, S., Ishikawa, T., Harada, Y., Kawano, N.,
Sasaki, S., Takano, T.: 2010, Results of the Global Mapping of
Lunar Gravity Field by KAGUYA, OKINA, and OUNA, Int.
Symp. on Lunar Science, (Macau, China, Mar. 25-26, 2010).
Iwata,T., Noda, H., Misawa, H., Imai, K., Kondo, T., Takeuchi,
H., Tsuchiya, F., Kumamoto, A., Nakajo, T., Nariyuki, Y., Inoue,
M., Kawano, N.: 2009, A study on the Observation System for
LLFAST: the Lunar Low Frequency Astronomical Telescope,Asia-Oceania Geoscience Society 6th Annual Meeting,(Suntech, Singapore, Aug. 11-15, 2009).

Iye, M.: 2009, Adaptive Optics in Astronomy, OSA topical meetingon Nonlinear Optics, (Honolulu, HI, USA, Jul. 12-17, 2009).
Kajino, T.: 2009, An Alternative to Inflation?: Critical Role ofNeutrino Anisotropic Stress in CMB, Erice Int. School of
Nuclear Physics 31st Course on Neutrinos in Cosmology, in
Astro-, Particle- and Nuclear-Physics, (Erice, Sicily, Italy, Sep.
16-20, 2009).
Kajino, T.: 2009, Neutrinos in Nuclear Physics and Astrophysics
and US-Japan Collaboration, Third Joint Meeting of the Nuclear
Physics Divisions of the APS and JPS, (Hawaii, USA, Oct.
13-17, 2009).
Kajino, T.: 2009, Nuclear Astrophysics in Japan: Understanding
the Universe with the Origin and Evolution of Elements,
Elizabeth and Frederick White Conference on Nuclear Astrophysics in Australia, (Canberra, Australia, Aug. 24-26, 2009).
Kajino, T.: 2009, Nucleosynthetic Signature of Supernovae andCollapsars (Gamma Ray Bursts), JUSTIPEN-EFES Workshop
on Unstable Nuclei, (Wako, Japan, Dec. 7-9, 2009).
Kajino, T.: 2009, R-process in Supernovae and Gamma-Ray
Bursts, 7th Japan-China Joint Nuclear Physics Symp., (Tsukuba,
Japan, Nov. 9-13, 2009).
Kajino, T.: 2009, The Big-Bang Cosmology and Nucleosynthesis,
5th European Summer School on Nuclear Astrophysics, (Santa
Tecla, Sicily, Italy, Sep. 21-27, 2009).
Kajino, T.: 2010, Effects of primordial magnetic field and neutrino
on CMB, The First APCosPA (Asia Pacific Center for Cosmology
and Particle Astrophysics) Winter School on Cosmology andParticle Astrophysics, (Taipei, Taiwan, Jan. 18-19, 2010).
Kajino, T.: 2010, Observational constraints on brane world cosmology,
The First APCosPA (Asia Pacific Center for Cosmology andParticle Astrophysics) Winter School on Cosmology and Particle
Astrophysics, (Taipei, Taiwan, Jan. 18-19, 2010).
Kajino, T.: 2010, Supernova nucleosynthesis and neutrino oscillation,
The First APCosPA (Asia Pacific Center for Cosmology andParticle Astrophysics) Winter School on Cosmology and Particle
Astrophysics, (Taipei, Taiwan, Jan. 18-19, 2010).
Kajino, T.: 2010, SUSY-particle catalized Big-Bang Nucleosynthesis
and DM, The First APCosPA (Asia Pacific Center for Cosmology
and Particle Astrophysics) Winter School on Cosmology andParticle Astrophysics, (Taipei, Taiwan, Jan. 18-19, 2010).
Kamata, S., Sugita, S., Abe, Y., Ishihara, Y., Harada, Y., Namiki, N.,
Iwata, T., Hanada, H., Araki, H.: 2010, The thermal evolutionof the lunar farside inferred from viscoelastic deformation of
impact basins, 4th KAGUYA (SELENE) Science Working Team
Meeting, (Tokyo, Japan, Jan. 31-Feb. 2, 2010).
Kamata, S., Sugita, S., Abe, Y., Ishihara, Y., Harada, Y., Namiki, N.,
Iwata, T., Hanada, H., Araki, H.: 2010, Viscoelastic deformationof lunar basins : implications for lunar farside thermal history basedon selenodetic data of Kaguya, 41st Lunar and Planetary Science
Conf. (LPSC 2010), (Woodlands, Texas, USA, Mar. 1-5, 2010).
Kambe, E.: 2009, Progress in Developing the Fiber-Link of 188-cm
Telescope and HIDES, The 4th Workshop on Extra-Solar Planet
Search with Accurate Radial Velocity Measurements, (Sapporo,
Japan, Oct. 7-9, 2009).
Kameya, O.: 2009, Water Vapor Masers in the NGC 7538 Region,
New Science Enabled by Microarcsecond Astronmetry, (Socorro,

II Publications, Presentations

069

NM, USA, Jul. 21-23, 2009).
Kandori, R., Tamura, M., Kusakabe, N., Nakajima, Y.: 2009,
Wide-field NIR Imaging Polarimetry of Brown Dwarfs in NGC
2024, New Technologies for Probing the Diversity of Brown
Dwarfs and Exoplanets, (Shanghai, China, Jul. 19-24, 2009).
Kano, R.: 2009, Connectivities between Corona and Photosphereviewed from Microflares, 2009 XRT Team Meeting, (Boston,
USA, Jun. 22-24, 2009).
Kano, R.: 2009, Multi-thermal structures above a polar region
observed with XRT and EIS, Hinode-3: The 3rd Hinode Science
Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Kano, R.: 2010, Coronal heating, The 2nd SOLAR-C Science
Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Kashikawa, N.: 2009, High-z Galaxies at the epoch of reionization,
Reionization with Multi-frequency Datasets, (Stockholm,
Sweden, Jul. 17-21, 2009).
Kashikawa, N.: 2009, High-z Galaxies at the epoch of reionization,
Focus week of the Epoch of the reionization, (IPMU, Japan,
Nov. 30-Dec. 2, 2009).
Kato, Y., Takahashi, R., Miyoshi, M.: 2009, 3-D Radiative Properties
of Hot Accretion Flows onto the Galactic Center Black Hole,
Galactic Center Workshop 2009, (Shanghai, China, Oct. 19-23,
2009).
Katsukawa, Y., Jurcak, J.: 2009, Photosphere-Chromosphere
Coupling as Observed with HINODE, Asia-Oceania Geoscience
Society 6th Annual Meeting, (Suntech, Singapore, Aug. 11-15,
2009).
Katsukawa, Y.: 2009, Persistent circulating motion of umbral
dots observed with HINODE SOT, Hinode-3: The 3rd Hinode
Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Katsukawa, Y.: 2009, Photospheric Dynamics around Sunspots
Observed from HINODE, Asia-Oceania Geoscience Society 6th
Annual Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Katsukawa, Y.: 2010, Basic requirements to the instrument
including priority of chromospheric lines, The 2nd SOLAR-C
Science Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Katsukawa, Y.: 2010, Hinode – Space Mission to Investigate theSun, The First Asia-Europe Physics Summit, (Tsukuba, Japan,
Mar. 24-26, 2010).
Katsukawa, Y.: 2010, Plan B Mission description, The 2nd SOLAR-C
Science Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Kawabe, R.: 2009, Recent Activity at NRO: Observational Resultsand Upgrading of NRO 45m and ASTE Telescopes, 10th
Workshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Wuxi, China, Nov. 15-18, 2009).
Kawagoe, S., Takiwaki, T., Kotake, K.: 2009, Neutrino oscillationsin MHD supernova explosions, Int. Conf. on Topics in
Astroparticle and Underground Physics 2009 (TAUP2009),(Rome, Italy, Jul. 1-5, 2009).
Kawakami, A., Takeda, M., Uzawa, Y., Wang, Z.: 2009, Design
and Fabrication of Epitaxial NbN/MgO/NbN SIS Mixers, Int.
Superconductive Electronics Conf. 2009, (Fukuoka, Japan, Jun.
16-19, 2009).
Kawakatu, N., Wada, K.: 2009, Formation of High-redshift (z>6)
Quasars Driven by Nuclear Starbursts, Max Planck Institute forExtraterrestrial Physics (MPE) seminar, (Munich, Germany,

070

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Nov. 13, 2009).
Kawamura, S.: 2009, Ground-based Interferometers and their Science
Reach, 8th Edoardo Amaldi Conf. on Gravitational Waves, (NewYork, USA, Jun. 21-26, 2009).
Kawamura, S.: 2009, Japanese Gravitational Wave Detectors:
LCGT and DECIGO, Frontiers in Optics 2009/Laser Science
XXV, (San Jose, USA, Oct. 11-15, 2009).
Kikuchi, F., et al.: 2010, Lunar gravimetry by inverse VLBI method/iVLBI mission of SELENE‐2, 4th KAGUYA (SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 31-Feb. 2, 2010).
Kikuchi, F., Iwata, T., Kawano, N., Sasaki, S., Liu, Q.: 2009,
Application of VLBI technique for lunar and planetary
exploration, European Geosciences Union General Assembly
2009, (Vienna, Austria, Apr. 19-24, 2009).
Kim, M. K.: 2009, The Outflows Traced by Water Masers in OrionKL, New Science Enabled by Microarcsecond Astronmetry,(Socorro, NM, USA, Jul. 21-23, 2009).
Kino, M.: 2010, Blazars: Progress, Problems, Prospects, Variabilityof blazars on diverse timescales, (Hiroshima, Japan, Mar. 4-5,
2010).
Kitazato, K., Abe, M., Kuroda, D., Yoshikawa, M.: Photometricobservations of Hayabusa follow-on mission targets, European
Planetary Science Congress 2009, (Potsdam, Germany, Sep.
13-18, 2009).
Kiuchi, H.: 2010, Photonic Millimeter-wave generation andtransmission techniques for the ALMA high-frequency RadioInterferometer, Symp. on Innovative Lightwave, MillimeterWave and THz Technologies for Future Sustainable Network,(San Diego, CA, USA, Mar. 26, 2010).
Kobayashi, H.: 2009, Status and Future Plan of VERA Project,
New Science Enabled by Microarcsecond Astronmetry,(Socorro, NM, USA, Jul. 21-23, 2009).
Kobayashi, H.: 2010, VLBI activities in Eastern Asia and Pacific,
Siam Physics Conf. 2010, (Kanchanaburi, Thailand, Mar. 25-27,
2010).
Kobayashi, M.: 2009, A Theoretical Model for LAE in HierarchicalGalaxy Formation: Comparison with the LAEs at z=4.86 in the
COSMOS 2-sq. degree Field, 2009 COSMOS Team Meeting,(Ehime, Japan, Jun. 15-18, 2009).
Kobayashi, M.: 2009, Semi-Analytic Model for high-z LAEs,
25th IAP Annual Colloq. "The Lyman Alpha Universe", (Paris,
France, Jul. 6-10, 2009).
Kobayashi, N., Araya, A., Shiraishi, H., Kakuma, H., Satoh, T.,
Okada, T., Tanaka, S., Kurita, K., Takeuchi, N., Okamoto, T.,
Ishihara, Y., Sasaki, S., Miyamoto, H.: 2009, Seismology
in MELOS, Asia-Oceania Geoscience Society 6th Annual
Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Kodama, T.: 2009, Inside-out propagation of star forming activity
in clusters, Galaxies Evolution and Environment, (Kuala
Lumpur, Malaysia, Apr. 3, 2009).
Kodama, T.: 2009, Panoramic Views of Cluster Evolution sincez=3 with Subaru, Galaxy Clusters in the Early Universe, (Pucón,
Chile, Nov. 12, 2009).
Kodama, T.: 2009, Panoramic Views of Cluster Formation and
Evolution, The 2nd Japan-Korea Joint Workshop: Galaxy BuildUp Across Cosmic Ages and Environments, (Hiraizumi, Japan,

Nov. 25-28, 2009).
Kojima, T., Kroug, M., Takeda, M., Shan, W., Fujii, Y., Uzawa, Y.,
Wang, Z.: 2009, Terahertz waveguide SIS mixers with epitaxial
NbTiN films and Nb junctions, 9th European Conf. on Applied
Superconductivity, (Dresden, Germany, Sep. 15, 2009).
Kojima, T., Kroug, M., Takeda, M., Shitov, S., Uzawa, Y., Shan,
W., Fujii, Y., Wang, Z.: 2009, A low noise NbTiN-based SIS
mixer for terahertz band, Int. Superconductive Electronics Conf.
2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Kokubo, E.: 2009, Formation of Terrestrial Planets: The Basic
Dynamical Model, The Dynamics of Discs and Planets,(Cambridge, UK, Aug. 17-21, 2009).
Kokubo, E.: 2009, Planetesimal Dynamics, Winter Workshop on
Planetary Astrophysics, (Beijing, China, Dec. 12-19, 2009).
Komiya, Y.: 2009, Near field cosmology with binary, high mass
IMF, and hierarchical galaxy formation, Tours 2009: Tours
Symp. on Nuclear Physics and Astrophysics VII, (Kobe, Japan,
Nov. 16-20, 2009).
Komiya, Y.: 2010, Extremely metal-poor stars and hierarchicalmodels of the Galactic chemical evolution, Origin of Matter and
Evolution of Galaxies, (Osaka, Japan, Mar. 8-10, 2010).
Kotake, K.: 2009, Magnetically-driven explosion of massive stars:
a possible route to collapsar and beyond, Shocking universe,(Venice, Itary, Sep. 14-18, 2009).
Kotake, K.: 2009, Neutrino-driven explosion of massive stars,
New frontiers in QCD, (Kyoto, Japan, Feb. 2, 2010).
Kotake, K.: 2009, Probing supernova mechanisms throughgravitational waves, Spanish relativity meeting, (Valencia,
Spain, Sep. 5-11, 2009).
Kotake, K.: 2009, Probing the central engine of core-collapse
supernovae through gravitational-wave and neutrino emissions,
Gravitational Wave + High-Energy Neutrino Workshop, (Paris,
France, May 18-21, 2009).
Kotake, K.: 2010, 2D and 3D modeling of core-collapse supenova
explosion, 15th workshop on nuclear astrophysics, (Tegernsee,
Germany, Mar. 22-27, 2010).
Kroug, M., Kojima, T., Takeda, M., Fujii, Y., Miyachi, A.,
Noguchi, T., Uzawa, Y., Wang, Z.: 2009, Low noise SIS mixer
for the 790-950 GHz band, 10th Workshop on SubmillimeterWave Receiver Technologies in Eastern Asia, (Wuxi, China,
Nov. 15-18, 2009).
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.: 2009, NRO Legacy
Project: Survey of Giant Molecular Clouds in M33, FIR2009:
the ISM of Galaxies in the Far-Infrared and Sub-MillimetreJoint Discussion at the 2009 XXVII IAU General Assembly(IAU-JD 14), (Reo de Janero, Brasil, Aug. 12-14, 2009).
Kusakabe, M., Kajino, T., Yoshida, T., Mathews, G. J.: 2009, Big
Bang nucleosynthesis with long-lived strongly interacting relicparticles, IAU Symp. 268 "Light Elements in the Universe",(Geneva, Switzerland, Nov. 9-13, 2009).
Kusakabe, M., Kajino, T., Yoshida, T., Mathews, G. J.: 2009, Effectof Long-lived Strongly Interacting Relic Particles on Big Bang
Nucleosynthesis, Third Joint Meeting of the Nuclear Physics
Divisions of the APS and JPS, (Hawaii, USA, Oct. 13-17, 2009).

Kusakabe, N.: 2009, Wide-Field NIR Imaging Polarimetry ofBrown Dwarfs in M42, New Technologies for Probing theDiversity of Brown Dwarfs and Exoplanets, (Shanghai, China,
Jul. 19-24, 2009).
Kuznetsov, S. A., Melnikov, V. F.: 2009, The role of the selfabsorption and Razin effect in formation of the frequency
spectrum of solar flare microwave emission, The Pulkovo conf.
"The Year of Astronomy: Solar and Solar-Terrestrial Physics –2009", (Saint-Peterbug, GAO RAS, Russia, Jul. 5-11, 2009).
Li, J., Cao, X., Takeda, M., Matsuo, H., Wang, Z., Shi, S.: 2009,
Shot-Noise Characteristics of NbN Superconducting Tunnel
Junctions, 20th Int. Symp. on Space Terahertz Technology,(Charlottesville, VA, USA, Apr. 22-24, 2009).
Liu, Q., Goossens, S., Hanada, H., Kikuchi, F., Matsumoto, K.,
Chen, M., Ping, J., Iwata, T.: 2010, Same-beam VLBI techniqueand its applications, 4th KAGUYA (SELENE) Science Working
Team Meeting, (Tokyo, Japan, Jan. 31-Feb. 2, 2010).
Liu, Q., Kikuchi, F., Matsumoto, K., Goossens, S., Hanada, H.,
Iwata, T., Namiki, N., Noda., H., Ishihara, Y., Ping, J., Asari,K., Ishikawa, T., Tsuruta, S., Harada, Y., Sasaki, S.: 2009,
Studies on same-beam VLBI and 4-way Doppler techniquesof SELENE for improving lunar gravity field model, Lunar/
Planetary Meeting & Forum, (Beijing/Wuhan, China, Jun.
15-27, 2009).
Machida, M. N.: 2009, Circumplanetary disk formation aroundproto-gas giant planets and implication of the satellite
formation, Icy Moons and Origin of Jupiter and other Giant
Planets, (Sapporo, Japan, Nov. 9-10, 2009).
Machida, M. N.: 2009, Gas Giant Planet Formation in Magnetized
Disks, Magneto-Rotational Instability in Protoplanetary Disks,(Kobe, Japan, Jun. 2-3, 2009).
Magara, T.: 2009, Characteristic Development of Magnetic Shearin a Flare-producing Sunspot obtained from Vector Magneticfield Measurements by Hinode, 2009 UN BSS and IHYWorkshop, (Daejeon, Korea, Sep. 24, 2009).
Magara, T.: 2009, Characteristic Development of Magnetic Shearin a Flare-productive Sunspot obtained by Hinode, Asia-Oceania
Geoscience Society 6th Annual Meeting, (Suntech, Singapore,Aug. 11-15, 2009).
Magara, T.: 2009, Dynamics of Coronal Mass Ejections, Hinode-3:
The 3rd Hinode Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Makino, J.: 2010, GRAPE-DR and Next-Generation GRAPE,
Accelerated Computing, (Tokyo, Jan. 28, 2010).
Makino, J.: 2009, Cosmogrid Project, GLIF 2009, (Daejeon, Korea,
Oct. 27, 2009).
Makino, J.: 2009, Gamma-rays from Earth-Size dark-matter halos,
Seminar at Ebisuzaki Lab, RIKEN, (Wako, Japan, Nov. 20, 2009).
Makino, J.: 2009, GRAPE-DR and Next-Generation GRAPE,
Accelerator-based Computing and Manycore Manycore andAccelerator-based Computing for Physics and Astronomy
Applications, (Menlo Park, CA, USA, Dec. 2, 2009).
Makino, J.: 2009, Stellar Dynamics of Massive Blackhole
Binaries, Workshop on Massive Black Hole Binaries and Their
Coalescence in Galactic Nuclei, (Beijing, China, Jul. 21, 2009).
Maruyama, T., Yasutake, N., Kajino, T., Cheoun, M.-K., Ryu,
C.-Y.: 2010, Asymmetric Neutrino Reaaction from Magnetized

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Proto-Neutron Stars in fully Relativisitc Framework including
Hyperons, Origin of Matter and Evolution of Galaxies, (Osaka,
Japan, Mar. 8-10, 2010).
Masada, Y.: 2009, A possible roles of Magneto-Rotational
Instability in the solar, Hinode-3: The 3rd Hinode Science
Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Masada, Y.: 2010, Pointing stability of Hinode and requirements
for Solar-C, The 2nd SOLAR-C Science Definition Meeting,(Sagamihara, Japan, Mar. 9-12, 2010).
Matsumoto, K., et al.: 2009, Gravity field of the Moon derived
from SELENE (Kaguya), JPL Seminar, (JPL, NASA, USA, Jul.
16, 2009).
Matsumoto, K., Goossens, S., Ishihara, Y., Liu, Q., Kikuchi,
F., Iwata, T., Namiki, N., Hanada, H., Noda, H., Kawano,N., Lemoine, F. G., Rowlands, D. D.: 2010, Lunar gravity fieldmodeling with 4-way Doppler data obtained during whole
RSAT mission period, 4th KAGUYA (SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 31-Feb. 2, 2010).
Matsumoto, K., Goossens, S., Ishihara, Y., Liu, Q., Kikuchi,
F., Iwata, T., Namiki, N., Noda, H., Hanada, H., Kawano, N.,
RSAT/VRAD Mission Team: 2010, An Improved Lunar Gravity
Field Model from SELENE and Historical Tracking Data, IVS
GM2010, (Hobart, Australia, Feb. 7-14, 2010).
Matsumoto, K., Goossens, S., Namiki, N., Ishihara, Y., Liu, Q.,
Kikuchi, F., Iwata, T., Noda, H., Hanada, H., RSAT/VRAD:
2009, A new lunar garvity field model from SELENE andhistorical tracking data, European Geosciences Union General
Assembly 2009, (Vienna, Austria, Apr. 19-24, 2009).
Matsumoto, K.: 2009, An Improved Lunar Gravity Field Modelfrom SELENE and Historical Tracking Data, NASA/GSFC
Seminar, (GSFC, NASA, USA, Sep. 16, 2009).
Matsumoto, N.: 2009, Astrometric Observations of Methanol
Masers toward W3(OH) with JVN, New Science Enabled byMicroarcsecond Astronmetry, (Socorro, NM, USA, Jul. 21-23,
2009).
Matsuo, H., Arai, T., Nitta, T., Kosaka, A.: 2009, Far-infrared
spectroscopic imaging of interstellar material around etaCarinae, IAU XXVII General Assembly, (Rio De Janeiro,
Brazil, Aug. 03-14, 2009).
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
Cryogenics Integrated Circuits for Superconducting Terahertz
Camera, The 9th Japan-Taiwan Microelectronics Int. Symp.,(Tokyo, Japan, Oct. 28-29, 2009).
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2009,
GaAs-JFET Cryogenic Readout Electronics for the Superconducting Terahertz Digital Camera, The 34th Int. Conf. on
Infrared, Millimeter, and Terahertz Waves, (Busan, Korea, Sep.
21-25, 2009).
Matsuo, H., Hibi, Y., Suzuki, T., Naruse, M., Noguchi, T.,
Sekimoto, Y., Uzawa, Y., Nagata, H., Ikeda, H., Ariyoshi,
S., Otani, C., Nitta, T., Yao, Q.-J., Fujiwara, M.: 2009, Superconducting THz Camera with GaAs-JFET Cryogenic Readout
Electronics, 13th Int. Workshop on Low Temperature Detectors
LTD-13, (Stanford, USA, Jul. 20-24, 2009).
Matsuo, H.: 2009, Far-Infrared Interferometry from Antarctica,
10th Workshop on Submillimeter-Wave Receiver Technologies

072

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in Eastern Asia, (Wuxi, China, Nov. 15-18, 2009).
Matsuo, H.: 2010, AKARI FIR spectroscopic imaging of interstellar
material around Eta Carinae, Global-COE Workshop on Eta
Carinae and its Surrounding Media, (Nagoya, Japan, Jan. 10,2010).
Matsuo, H.: 2010, Far-Infrared Interferometry from Antarctica,
21th Int. Symp. on Space Terahertz Technology, (Oxford, UK,
Mar. 23-25, 2010).
Melnikov, V. F.: 2009, Microwave diagnostics of the positionof acceleration site and pitch-angle anisotropy of energetic
electrons in flaring loops, The Pulkovo conf. "The Year of
Astronomy: Solar and Solar-Terrestrial Physics – 2009", (SaintPeterbug, GAO RAS, Russia, Jul. 5-11, 2009).
Melnikov, V. F., Reznikova, V. E., Shibasaki, K., Pyatakov, N.
P., Myagkova, I., Ji, H.: 2009, Microwave diagnostic of theposition of an acceleration site and pitch-angle anisotropyof energetic electrons, The 9th RHESSI general Workshop,(Genova, Italy, Sep. 1-5, 2009).
Melnikov, V. F.: 2009, Possibilities for constraining acceleration
models from microwave observations, The 9th RHESSI general
Workshop, (Genova, Italy, Sep. 1-5, 2009).
Michikoshi, S.: 2009, N-body simulation of planetesimal formation
through gravitational instability, Magneto-Rotational Instability
in Protoplanetary Disks, (Kobe, Japan, Jun. 2-3, 2009).
Michikoshi, S.: 2009, N-body simulation of planetesimal formation
through gravitational instability, The Dynamics of Discs andPlanets, (Cambridge, UK, Sep. 17-21, 2009).
Miki, S., Takeda, M., Fujiwara, M., Sasaki, M., Otomo, A., Wang, Z.:
2009, Compact Packaging of Superconducting Nanowire Single
Photon Detectors with Optical Cavity, Int. Superconductive
Electronics Conf. 2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Miki, S., Takeda, M., Fujiwara, M., Sasaki, M., Otomo, A., Wang,Z.: 2009, Superconducting Nanowire Single Photon Detectors
with NbTiN Thin Films, Int. Superconductive Electronics Conf.
2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Miki, S., Takeda, M., Fujiwara, M., Sasaki, M., Wang, Z.: 2009,
Compact packaging of optical cavity structured SNSPDs withhigh optical coupling efficiency, 9th European Conf. on Applied
Superconductivity, (Dresden, Germany, Sep. 15, 2009).
Miyazaki, A.: 2009, First Phase of the East Asia VLBI Network,
New Science Enabled by Microarcsecond Astronmetry,(Socorro, NM, USA, Jul. 21-23, 2009).
Miyazaki, A.: 2009, NMA monitoring observations of Sagittarius
A* at short mm-wavelengths, Galactic Center Workshop 2009,(Shanghai, China, Oct. 19-23, 2009).
Miyazaki, A.: 2009, Wide-field mapping observations of multiammonia emission lines in the Galactic center region, Galactic
Center Workshop 2009, (Shanghai, China, Oct. 19-23, 2009).
Miyazaki, A.: 2010, Present status of the first phase East Asia
VLBI Network, ミニワークショップ「KVN −山口アレイで狙うサイエンス」, (Yamaguchi, Japan, Mar. 16, 2010).
Miyoshi, M., Furuya, R., Kawaguchi, N., Nakajima, J., Irimajiri, Y.,
Koyama, Y., Sekido, M., Ujihara, H., Ishitsuka, K. J. I., Asaki, Y.,
Kato, Y., Takeuchi, H., Tsuboi, M., Kasuga, T., Tomimatsu, A.,
Takahashi, M., Eriguchi, Y., Yoshida, S., Koide, S., Takahashi,R., Oka, T.: 2009, An Earliest Black Hole Imager at Andes, The

19th Workshop on General Relativity and Gravitation in Japan(JGRG19), (Tokyo, Japan, Nov. 30-Dec. 4, 2009).
Miyoshi, M., Furuya, R.-S., Kawaguchi, N., Nakajima, J.,
Irimajiri, Y., Koyama, Y., Sekido, M., Ujihara, H., Ishitsuka,
K. J. I., Asaki, Y., Kato, Y., Takeuchi, H., Tsuboi, M., Kasuga,
T., Tomimatsu, A., Takahashi, M., Eriguchi, Y., Yoshida, S.,
Koide, S., Takahashi, R., Oka, T.: 2009, A First Black Hole
Imager, Caravan-sub at Andes, Galactic Center Workshop 2009,(Shanghai, China, Oct. 19-23, 2009).
Miyoshi, M., Furuya, R.-S., Kawaguchi, N., Nakajima, J.,
Irimajiri, Y., Koyama, Y., Sekido, M., Ujihara, H., Ishitsuka, K.,
J., I., Asaki, Y., Kato, Y., Takeuchi, H., Tsuboi, M., Kasuga, T.,
Tomimatsu, A., Takahashi, M., Eriguchi, Y., Yoshida, Si., Koide,S., Takahashi, R., Oka, T.: 2010, An Earliest Black Hole Imager
at Andes, Probing Strong Gravity near Black Holes, (Prague,
Cheko, Feb. 15-18, 2010).
Miyoshi, M., Oyama, T., Shen, Z.-Q.: 2009, VLBA Synthesis
Imagings of SgrA* at 43 GHz, Galactic Center Workshop 2009,(Shanghai, China, Oct. 19-23, 2009).
Miyoshi, M., Shen, Z.-Q., Oyama, T., Takahashi, R., Kato Y.:
2009, Oscillation phenomena in Sagittarius A*, Galactic Center
Workshop 2009, (Shanghai, China, Oct. 19-23, 2009).
Miyoshi, M.: 2009, Slit-Modulation Imaging Method for Detecting
Periodic Structural Change in SgrA*, Galactic Center Workshop
2009, (Shanghai, China, Oct. 19-23, 2009).
Morota, T., Haruyama, J., Ohtake, M., Matsunaga, T., Yokota, Y.,
Honda, C., Sugihara, T., Kimura, J., Ishihara, Y., Kawamura,T., Iwasaki, A., Saiki, K., Takeda, H.: 2010, Mare Volcanism on
the Farside and in the Orientale Region of the Moon, 41st Lunarand Planetary Science Conf. (LPSC 2010), (Woodlands, Texas,
USA, Mar. 1-5, 2010).
Motoyama, K., Shang, H., Hasegawa, T., Umemoto, T.: 2010,
Test of radiation-driven implosion model by comparison
between hydrodynamic simulation and molecular line
observations, Multi-Phase Interstellar Medium and Dynamics ofStar Formation, (Nagoya, Japan, Feb. 28-Mar. 2, 2010).
Murakami, N., Baba, N., Nishikawa, J., Yokochi, K., Tamura,M., Hashimoto, N., Abe, L.: 2009, Eight-Octant Phase-Mask
Coronagraph by Using Liquid Crystal and Photonic Crystal
Devices, OIE '09 The Eighth Japan-Finland Joint Symp. on Optics
in Engineering, (Tokyo, Japan, Sep. 3-4, 2009).
Murakami, N., Nishikawa, J., Yokochi, K., Tamura, M., Baba,
N., Hashimoto, N., Abe, L.: 2009, Eight-octant phase-mask
coronagraph for detecting Earth-like exoplanets around partiallyresolved stars, Pathways towards habitable planets, (Barcelona,
Spain, Sep. 14-18, 2009).
Murakami, N., Inabe, T., Komatsu, T., Nishikawa, J., Hashimoto,N., Kurihara, M., Baba, N., Tamura, M.: 2010, Laboratory
demonstrations of liquid-crystal eight-octant phase-mask
coronagraph, The 6th Exoplanet Conf., (Mitaka, Japan, Jan.
18-20, 2010).
Muraoka, K., Tosaki, T., Kuno, N., Kohno, K., Nakanishi, K.,
Sorai, K.: 2009, ASTE CO(3–2) Mapping of the Spiral Galaxy
M 83: GMA Properties in the Whole Optical Disk, Millimeterand Submillimeter Astronomy at High Angular Resolution,(Taipei, Taiwan, Jun. 8-12, 2009).

Muraoka, K., Tosaki, T., Kuno, N., Kohno, K., Nakanishi, K.,
Sorai, K.: 2009, ASTE CO(3–2) Mapping of the Spiral Galaxy
M 83: GMA Properties in the Whole Optical Disk, FIR2009: theISM of Galaxies in the Far-Infrared and Sub-Millimetre-Joint
Discussion at the 2009 XXVII IAU General Assembly (IAU-JD14), (Reo de Janero, Brasil, Aug. 12-14, 2009).
Nagashima, K.: 2009, Local helioseismology of the polar region
dynamics by Hinode/SOT, Hinode-3: The 3rd Hinode Science
Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Nagata, H., Matsuo, H., Hibi, Y., Ikeda, H., Fujiwara, M.: 2009,
Development of cryogenic analog amplifiers based on GaAsJFET technology for high impedance array sensors, 13th Int.
Workshop on Low Temperature Detectors LTD-13, (Stanford,
USA, Jul. 20-24, 2009).
Nakajima, T., Miyazawa, C., Iwashita, H., Kuno, N., Kawabe,R., Sakai, T., Kohno, K., Nishimura, A., Kimura, K., Ogawa, H.,
Asayama, S., Noguchi, T.: 2009, Development of the 100-GHz
Band 2SB SIS Receiver Systems for the NRO 45-m Telescope,
10th Workshop on Submillimeter-Wave Receiver Technologies
in Eastern Asia, (Wuxi, China, Nov. 15-18, 2009).
Nakamura, K., Yoshida, T., Shigeyama, T., Kajino, T.: 2009,
Lithium, beryllium, and boron production in core-collapse
supernovae, IAU Symp. 268 "Light Elements in the Universe",(Geneva, Switzerland, Nov. 9-13, 2009).
Nakamura, K., Yoshida, T., Shigeyama, T., Kajino, T.: 2010, Lightelements from core-collapse supernovae: the neutrino-process
and spallation reactions, Origin of Matter and Evolution of
Galaxies, (Osaka, Japan, Mar. 8-10, 2010).
Nakamura, K.: 2009, Consistency of Equations for the Single Scalar
Field Case in Second-order Gauge-invariant Cosmological
Perturbation Theory, The 19th Workshop on General Relativity
and Gravitation in Japan (JGRG19), (Tokyo, Japan, Nov.
30-Dec. 4, 2009).
Nakamura, K.: 2009, Gauge-invariant formulation of the secondorder cosmological perturbations: -Single scalar field case-,
Workshop in YITP on "Non-linear cosmological perturbations",(Kyoto, Japan, Apr. 13-24, 2010).
Nakamura, K.: 2009, Lithium, Beryllium, and Boron Productionin Core-collapse Supernovae, IAU Symp. 268 "Light Elementsin the Universe", (Geneva, Switzerland, Nov. 9-13, 2009).
Nakamura, K.: 2009, The neutrino-process and spallation reactions
in core-collapse supernovae, Japan-US Theory Institute forPhysics with Exotic Nuclei Workshop, (Wako, Japan, Dec. 7,2009).
Nakayama, H.: 2009, Entire topography of lunar surface, SIGGRAPH
Asia 2009, (Yokohama, Japan, Dec. 16-19, 2009).
Nakazato, T.: 2009, Current Status of Single-dish Data Analysis
Software for ALMA, Astronomical Data Analysis Software andSystems XIX, (Sapporo, Japan, Oct. 4-8, 2009).
Namiki, N., Iwata, T., Hanada, H., Matsumoto, K., Goossens, S.,
Ishihara, Y., Sugita, S., Noda, H., Sasaki, S., Araki, H.: 2009,
Study of Compensation Mechanism of Lunar Impact Basins
From New Gravity and Topographic Data of Kaguya, 41st annual
meeting of the Division for Planetary Sciences of the American
Astronomical Society, (Fajardo, Puerto Rico, Oct. 5-9, 2009).
Namiki, N., Sugita, S., Matsumoto, K., Goossens, S., Ishihara, Y.,

II Publications, Presentations073

Noda, H., Sasaki, S., Iwata, T., Hanada, H., Araki, H., Kubo,
N., Mori, A., Sato, M.: 2009, Comparative study of compensation
mechanism of lunar impact basin from new gravity field modelof SELENE (Kaguya), The Moon, moons & Planets, (Kazan,
Russia, Aug. 24-26, 2009).
Namiki, N., Sugita, S., Matsumoto, K., Goossens, S., Ishihara,Y., Noda, H., Sasaki, S., Iwata, T., Hanada, H., Araki, H.,
Kurosawa, K., Matsumura, M., Yokoyama, M., Kamata, S.,
Kubo, N., Mori, A., Sato, M.: 2009, Comparative Study ofCompensation Mechanism of Lunar Impact Basins, AsiaOceania Geoscience Society 6th Annual Meeting, (Suntech,Singapore, Aug. 11-15, 2009).
Namiki, N., Sugita, S., Matsumoto, K., Goossens, S., Ishihara,Y., Noda, H., Sasaki, S., Iwata, T., Hanada, H., Araki, H.,
Kurosawa, K., Matsumura, M., Yokoyama, M., Kamata,S., Kubo, N., Mori, A., Sato, M.: 2009, Comparative studyof compensation mechanism of lunar impact basins fromnew gravity filed model of SELENE (Kaguya), European
Geosciences Union General Assembly 2009, (Vienna, Austria,
Apr. 19-24, 2009).
Narukage, N.: 2009, The Thermal Structures of Solar Corona,
Asia-Oceania Geoscience Society 6th Annual Meeting,(Suntech, Singapore, Aug. 11-15, 2009).
Narukage, N.: 2009, Time evolution of coronal structure in T-EM
diagram examined with calibrated XRT responses, Hinode-3:
The 3rd Hinode Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Naruse, M., Sekimoto, Y., Suzuki, T., Hibi, Y., Matsuo, H.,
Uzawa, Y., Noguchi, T.: 2009, Design of SIS Imaging Array for
Terahertz Astronomy, The 34th Int. Conf. on Infrared, Millimeter,
and Terahertz Waves, (Busan, Korea, Sep. 21-25, 2009).
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani, T.,
Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.: 2009,
A Coronagraph with an Unbalanced Nulling Interferometerand Adaptive Optics, Pathways towards habitable planets,(Barcelona, Spain, Sep. 14-18, 2009).
Nishizawa, A., Taruya, A., Hayama, K., Kawamura, S., Sakagami,
M.: 2009, Searching for nontensorial polarizations of stochastic
gravitational waves with laser interferometers, The 19th
Workshop on General Relativity and Gravitation in Japan(JGRG19), (Tokyo, Japan, Nov. 30-Dec. 4, 2009).
Nishizawa, A.: 2009, Probing non-tensorial polarizations of
stochastic gravitational-wave background, 8th Edoardo Amaldi
Conf. on Gravitational Waves, (New York, USA, Jun. 21-26, 2009).
Noda, H., Araki, H., Goossens, S., Ishihara, Y., Matsumoto,K., Haruyama, J., Ohtake, M., Matsunaga, T.: 2009, Lunar
global topographic model by Laser Altimeter (LALT) aboard
KAGUYA (SELENE), Asia-Oceania Geoscience Society 6th
Annual Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Noda, H., Araki, H., Tazawa, S., Goossens, S., Ishihara, Y.,
Matsumoto, K., Kawano, N., Sasaki, S., Kamiya, I., Oberst, J.,
Shum, C. K.: 2009, KAGUYA (SELENE) Laser Altimeter (LALT):
one year in orbit, European Geosciences Union General
Assembly 2009, (Vienna, Austria, Apr. 19-24, 2009).
Noda, H., et al.: 2009, Lunar Global shape and polar topographyderived from SELENE (Kaguya), JPL Seminar, (JPL, NASA,
USA, Jul. 16, 2009).

074

II Publications, Presentations

Noda, H., et al.: 2009, Lunar surface reflectance by LALT aboard
KAGUYA, AGU Fall Meeting, (San Francisco, USA, Dec.
14-18, 2009).
Noda, H., Kunimori, H., Araki, H., Oya, S., Okita, K., Katayama,
M., Sasaki, S., Takato, N., Tazawa, S., Tsuruta, S., Hanada,
H., Harada, Y., Watanabe. J., Otsubo, T.: 2010, Proposed Lunar
Laser Ranging experiment for SELENE-2, Int. Astron. Forum"ASTROKAZAN – 2010", (Kazan, Russia, Feb. 9-10, 2010).
Noda, T., Hashimoto, M., Yasutake, N., Maruyama, T., Tatsumi,T., Fujimoto, M.: 2010, Cooling of Exotic Stars with QuarkHadron Mixed Phase in the Color Superconductive State, Origin
of Matter and Evolution of Galaxies, (Osaka, Japan, Mar. 8-10,
2010).
Noguchi, T., Suzuki, T., Endo, A., Naruse, M., Hibi, Y., Matsuo,
H., Sekimoto, Y.: 2009, Effect of Lifetime Broadening ofSuperconducting Energy Gap on Quasiparticle Tunneling
Current, 20th Int. Symp. on Space Terahertz Technology,(Charlottesville, VA, USA, Apr. 22-24, 2009).
Noguchi, T., Suzuki, T., Endo, A., Tamura, T.: 2009, Investigationof subgap current at low temperature in Nb/Al SIS junctions,
9th European Conf. on Applied Superconductivity, (Dresden,
Germany, Sep. 15, 2009).
Noguchi, T.: 2009, A proposal of a new type of pair-breaking
detector using a SIS transmission line, 10th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Wuxi, China, Nov. 15-18, 2009).
Noguchi, T.: 2009, Contribution of imaginary part of the gap
energy on superconducting films and devices, 10th Workshop
on Submillimeter-Wave Receiver Technologies in Eastern Asia,(Wuxi, China, Nov. 15-18, 2009).
Noguchi, T.: 2009, Energy-gap Broadening Effect on the SIS
Tunneling Current, Int. Superconductive Electronics Conf.
2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Noguchi, T.: 2009, Superconducting tunnel junction detectors
for submillimeter-wave astronomy, Int. Superconductive
Electronics Conf. 2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Oe, M.: 2009, Proposal from the HOTARU project, ETSI Plugtest 3,(Lannion, France, Oct. 16-23, 2009).
Oguri, M.: 2009, ALMA and Virtual Observatory, ALMA Users
Meeting, (Mitaka, Japan, Dec. 21-23, 2009).
Oguri, M.: 2009, Astrobiology Network in Japan, 9th European
Workshop on Astrobiology, (Brussels, Belgium, Oct. 12-14,
2009).
Oguri, M.: 2009, Cluster strong lensing, Science Opportunities
with Wide-Field Imaging and Spectroscopy of the Distant
Universe, (Princeton, New Jersey, USA, Nov. 9-11, 2009).
Oguri, M.: 2009, Cosmology with clusters of galaxies, NIMSAPCTP workshop: String theory and cosmology, (Daejeon,
Korea, Sep. 24-26, 2009).
Oguri, M.: 2009, Current Developments in Virtual Observatories
for Astronomy, First Meeting of the ICSU Strategic
Coordination Committee on Information and data, (Paris,
France, Octl. 15-16, 2009).
Oguri, M.: 2009, Finding bright high-z galaxies through gravitational lensing, The 2nd Japan-Korea Joint Workshop:
Galaxy Build-Up Across Cosmic Ages and Environments,

(Hiraizumi, Japan, Nov. 25-28, 2009).
Oguri, M.: 2009, Gravitational lens time delays: Past, present andfuture, Dark universe: from cosmology to planets, (Hakone,
Japan, Oct. 14-16, 2009).
Oguri, M.: 2009, WG on Astrophysically Important Spectral Lines,
IAU XXVII General Assembly, (Rio De Janeiro, Brazil, Aug.
03-14, 2009).
Oguri, M.: 2009, Lessons Learned during the Development andOperation of Virtual Observatory, Astronomical Data Analysis
Software and Systems XIX, (Sapporo, Japan, Oct. 4-8, 2009).
Ohsuga, K.: 2009, Global Radiation-Magnetohydrodynamic Simulations of Black Hole Accretion Flow and Outflow: Unified
Model of Three States, Accretion and Ejection in AGN: A
Global New, (Como, Italy, Jun. 22-26, 2009).
Okamoto, T. J.: 2009, Cool material from the lower atmospherein a quiescent prominence, Hinode-3: The 3rd Hinode Science
Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Okamoto, T. J.: 2010, Topology and dynamics of magnetic solar
atmosphere, The 2nd SOLAR-C Science Definition Meeting,(Sagamihara, Japan, Mar. 9-12, 2010).
Okamura, N., Sugita, S., Hong, P. K., Kawakita, H., Sekine,Y., Terada, H., Takato, N., Hayano, Y., Fuse, T., Wooden,
D. H., Young, E. F., Lucey, P. G., Furusho, R., Watanabe,J., Haruyama, J., Nakamura, R., Kurosawa, K., Hamura, T.,
Kadono, T.: 2010, The Estimate of the Amount of Ejecta in
LCROSS Mission, 41st Lunar and Planetary Science Conf.
(LPSC 2010), (Woodlands, Texas, USA, Mar. 1-5, 2010).
Omukai, K.: 2009, Low-metallicity star formation, Tours 2009:
Tours Symp. on Nuclear Physics and Astrophysics VII, (Kobe,
Japan, Nov. 16-20, 2009).
Omukai, K.: 2010, Low-metallicity star formation: the Pop III-IItransition, The First Stars and Galaxies: Challenges for the Next
Decade, (Austin, USA, Mar. 10, 2010).
Onodera, S., Kuno, N., Tosaki, T., Muraoka, K., Kaneko, H.,
Sawada, T., Nakanishi, K., Komugi, S., Tamura, Y., Kohno,
K., Kawabe, R., Arimoto, N., Okamoto, S.: 2009, NRO Legacy
Project: GMC Survey in M33 – First Year Results, Millimeterand Submillimeter Astronomy at High Angular Resolution,(Taipei, Taiwan, Jun. 8-12, 2009).
Ootsubo, T., Watanabe, J., Honda, M., Ishiguro, M., Sarugaku,Y., Sakon, I.: 2009, Mid-infrared Spectroscopic Observations ofComet 17P/Holmes, IAU Symp. 263 "Icy Bodies in the Solar
System,", (Rio de Janeiro, Brazil, Aug. 3-7, 2009).
Orozco Suarez, D.: 2009, Emergence of vertical magnetic fields
in quiet Sun granules: statistical properties, Hinode-3: The 3rd
Hinode Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Orozco Suarez, D.: 2009, Center-to-limb variation of the internetwork magnetic field vector distribution derived from Hinodeobservations, Hinode-3: The 3rd Hinode Science Meeting,(Tokyo, Japan, Dec. 1-4, 2009).
Oshima, A.: 2009, Study of an angular resolution of the GRAPES-3
array, 31th Int. Cosmic Ray Conf., (Lodz, Poland, Jul. 7-15, 2009).
Oyama, T.: 2009, The Astrometric Feasibility and Accuracy of
VERA, New Science Enabled by Microarcsecond Astronmetry,(Socorro, NM, USA, Jul. 21-23, 2009).
Petrova, N., Hanada, H., Akutina, M.: 2009, Computer simulationof star transition across the prime meridian for the future
observations by the Lunar polar telescope in the Japanese
project ILOM, European Planetary Science Congress 2009,(Potsdam, Germany, Sep. 13-18, 2009).
Pyatakov, N. P., Gorbikov, S. P., Melnikov, V. F.: 2009, Modelingof the dynamics of gyrosynchrotron emission from flaring
loops, The Pulkovo conf. "The Year of Astronomy: Solar andSolar-Terrestrial Physics – 2009", (Saint-Peterbug, GAO RAS,
Russia, Jul. 5-11, 2009).
Pyo, T.-S.: 2009, Studying the Origin of Outflows from YSOs with
SUBARU and GEMINI, Joint Subaru/Gemini Science Conf.,(Kyoto, Japan, May 18-21, 2009).
Qiu, W., Wang, Z., Takeda, M., Miki, S., Terai, H., Shimakage,H., Kawakami, A.: 2009, Fabrication and Characterization ofHigh Quality Low Critical Current Density NbN/AlN/NbN
tunnel junctions, Int. Superconductive Electronics Conf. 2009,(Fukuoka, Japan, Jun. 16-19, 2009).
Reznikova, V. E., Melnikov, V. F., Ji, H.: 2009, Spatial dynamics
of flaring loop footpoints, The Pulkovo conf. "The Year of
Astronomy: Solar and Solar-Terrestrial Physics – 2009", (SaintPeterbug, GAO RAS, Russia, Jul. 5-11, 2009).
Reznikova, V. E., Melnikov, V. F., Shibasaki, K.: 2009, Microwave
diagnostics of the position of an acceleration site and pich-angle
anisotropy of energetic electrons in the flare of 24 Aug 2002,
Hinode-3: The 3rd Hinode Science Meeting, (Tokyo, Japan,
Dec. 1-4, 2009).
Saito, S., Takeda, M., Shimakage, H., Uzawa, Y., Wang, A., Sekine,N., Hosako, I., Sakai, K.: 2009, Observation of phase transitionin niobium nitride with THz time-domain spectroscopy, The
34th Int. Conf. on Infrared, Millimeter, and Terahertz Waves,(Busan, Korea, Sep. 21-25, 2009).
Saitoh, T. R.: 2009, How Should we Choose Star Formation
criteria in High-Resolution Simulations, Monthly meeting on
GRAPE in Korea, (Seoul, Korea, Apr. 10, 2009).
Saitoh, T. R.: 2009, Shock-Induced Starburst and Star Cluster
Formation in Colliding Galaxies, Galaxy Wars: Stellar
Populations and Star Formation in Interacting Galaxies,(Johnson City, TN, USA, Jul. 19-22, 2009).
Saitoh, T. R.: 2009, Star Cluster Formation in Interacting Galaxies,
Star Formation and Star Clusters, (Seoul, Korea, Apr. 9, 2009).
Sako, S., Shimojo, M., Kitabayashi, T.: 2009, Statistical study
for X-ray jets occurred in the polar region, Hinode-3: The 3rd
Hinode Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Sakurai, T.: 2009, Sixty Years of Norikura Solar Observatory,
Hinode-3: The 3rd Hinode Science Meeting, (Tokyo, Japan,
Dec. 1-4, 2009).
Sakurai, T.: 2010, Hinode Sciences: Achievements and Prospects,
The 2nd SOLAR-C Science Definition Meeting, (Sagamihara,
Japan, Mar. 9-12, 2010).
Sasaki, S., Fujimoto, M., Takashima, T., Yano, H., Kasaba, Y.,
Takahashi, Y., Kimura, J., Tsuda, Y., Funase, R., Mori, O.: 2009,
Exploration of Jovian Magnetosphere and Trojan Asteroids
by a Solar Power Sail Mission, European Geosciences Union
General Assembly 2009, (Vienna, Austria, Apr. 19-24, 2009).
Sasaki, S., Fujimoto, M., Yano, H., Kimura, J.: 2009, Explorationof the Jovian System by EJSM, Asia-Oceania Geoscience Society

II Publications, Presentations075

6th Annual Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Sasaki, S., Fujimoto, M., Yano, H., Takashima, T., Kasaba, Y.,
Takahashi, Y., Kimura, J., Kawaguchi, J., Kawakatsu, Y., Tsuda,
Y.: 2009, Exploration of Jupiter System and Trojan Asteroids,
European Planetary Science Congress 2009, (Potsdam, Germany,
Sep. 13-18, 2009).
Sasaki, S., Hanada, H., Kikuchi, F., Noda, H., Araki, H.,
Matsumoto, K., Funazaki, K., Iwata, T., Kunimori, H., RISE
Project Team: 2009, Lunar Rotation and Gravity Measurements
by SELENE-2, European Planetary Science Congress 2009,(Potsdam, Germany, Sep. 13-18, 2009).
Sasaki, S., Hiroi, T., Arai, T., Helbert, J.: 2009, Space Weatheringon Mercury: Simulation of Plagioclase Weathering, European
Planetary Science Congress 2009, (Potsdam, Germany, Sep.
13-18, 2009).
Sasaki, S., Hiroi, T., Helbert, J.: 2009, Space Weathering on Mercury:
Effect of Impact Mixing and Weathering of Anorthite, AsiaOceania Geoscience Society 6th Annual Meeting, (Suntech,Singapore, Aug. 11-15, 2009).
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Goossens, S.,
Namiki, N., Iwata, T., Hanada, H., Matsumoto, K., Kawano, N.,
Kikuchi, F., Liu, Q., Harada, Y., SELENE Gravity/Topography
Group: 2009, Lunar Topography and Crustal Thickness by
KAGUYA (SELENE) Selenodesy Observation, 41st annual
meeting of the Division for Planetary Sciences of the American
Astronomical Society, (Fajardo, Puerto Rico, Oct. 5-9, 2009).
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Goossens, S., Namiki,N., Iwata, T., Hanada, H., Matsumoto, K.: 2009, Topography
and Crustal Thickness of the Moon by KAGUYA (SELENE)
Selenodesy Observation, European Geosciences Union General
Assembly 2009, (Vienna, Austria, Apr. 19-24, 2009).
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Hanada, H.,
Matsumoto, K., Goossens, S., Namiki, N., Iwata, T., Ohtake,M.: 2010, Structure of the lunar South Pole-Aitken basin fromKAGUYA (SELENE) gravity/topography, 41st Lunar andPlanetary Science Conf. (LPSC 2010), (Woodlands, Texas,
USA, Mar. 1-5, 2010).
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Hanada, H.,
Matsumoto, K., Goossens, S., Namiki, N., Iwata, T., Ohtake, M.:
2010, Structure of the South Pole-Aitken basin from KAGUYA
gravity/topography, 4th KAGUYA (SELENE) Science Working
Team Meeting, (Tokyo, Japan, Jan. 31-Feb. 2, 2010).
Sasaki, S., Ishihara, Y.: 2010, Crustal Thickness and Structureof Impact Basins from Kaguya Data, Brown-Vernadsky
Microsymposium 51: Compositional Structure of the Lunar
Crust: The New View from the Moon, (Woodlands, Texas,
USA, Feb. 27-28, 2010).
Sasaki, S., Namiki, N., Hanada, H., Araki, H., Iwata, T., Ishihara,Y., Matsumoto, K., Noda, H., Goossens, S., KAGUYA
topography/gravity team: 2009, Global Topography and Gravityof the Moon Observed by KAGUYA, European Planetary
Science Congress 2009, (Potsdam, Germany, Sep. 13-18, 2009).
Sasaki, S., Namiki, N., Hanada, H., Araki, H., Iwata, T., Ishihara,Y., Noda, H., Matsumoto, K., Goossens, S., KAGUYA
topography/gravity team: 2009, Global Topography and Gravityof the Moon Observed by KAGUYA, The 2nd Annual NLSI

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Lunar Science Forum, (Moffett Field, California, USA, Jul.
21-23, 2009).
Sasaki, S.: 2009, Keynote Speech: Icy Moons and Origin of Jupiterand other Giant Planets, Icy Moons and Origin of Jupiter andother Giant Planets, (Sapporo, Japan, Nov. 9-10, 2009).
Sasaki, S.: 2010, Mars Dust Counter on board NOZOMI, CPS
Cosmic Dust Workshop, (Kobe, Japan, Mar. 11, 2010).
Sekiguchi, K.: 2009, IYA2009, NUM-ITC-UNESCO Remote
Sensing and Space Science Laboratory, (National University ofMongolia, Ulaanbaatar, Jun. 29, 2009).
Sekiguchi, K.: 2010, Evaluations and future plans of IYA2009
activities in Japan, Communicating Astronomy with the Public
2010, (Cape Town, South Africa, Mar. 15-19, 2010).
Sekiguchi, Y.: 2009, Full GR Simulations with Microphysics,
Microphysics in Computational Relativistic Astrophysics:
MICRA2009, (Copenhagen, Denmark, Aug. 24-28, 2009).
Sekiguchi, Y.: 2009, Rotating PopIII core collapse in Full generalrelativity, The 19th Workshop on General Relativity andGravitation in Japan (JGRG19), (Tokyo, Japan, Nov. 30-Dec. 4,2009).
Sekiguchi, Y.: 2009, Stellar core collapse in general relativity,
2009 Int. School on Numerical Relativity and Gravitation,(Seoul, Korea, Dec. 7-11, 2009).
Sekiguchi, Y.: 2009, Towards constrainging nuclear EOS using
gravitational waves from binary, Numerical Relativity and Data
Analysis Meeting, (Potsdam, Germany, Jul. 6-9, 2009).
Sekiguchi, Y.: 2010, Formulation and application of generalrelativistic neutrino leakagw scheme, New Frontiers in QCD
2010, (Kyoto, Japan, Jan. 18-Mar. 19, 2010).
Sekii, T.: 2009, Eigenfrequencies of solar high-degree f modes,
Hinode-3: The 3rd Hinode Science Meeting, (Tokyo, Japan,
Dec. 1-4, 2009).
Sekii, T.: 2009, Solar-C and solar dynamo, 3rd Solar Orbiter
Workshop, (Sorrent, Italy, May 25-29, 2009).
Sekii, T.: 2010, Helioseismology and dynamo science, The 2nd
SOLAR-C Science Definition Meeting, (Sagamihara, Japan,
Mar. 9-12, 2010).
Sekimoto, Y., Iizuka, Y., Satou, N., Ito, T., Kumagai, K.,
Kamikura, M., Naruse, M., Shan, W. L.: 2009, Developmentof ALMA Band 8 Cartridge, 20th Int. Symp. on Space Terahertz
Technology, (Charlottesville, VA, USA, Apr. 22-24, 2009).
Shi, S. C., Paine, S., Yao, Q. J., Li, X. X., Zhang, X. G., Lin, Z. H.,
Zhou, K. M., Huang, Q. G., Matsuo, H., Yang, J., Zhang, Q. Z.:
2010, A THz FTS for Site Testing at Dome A, 21th Int. Symp.
on Space Terahertz Technology, (Oxford, UK, Mar. 23-25,
2010).
Shibasaki, K.: 2009, Nonlinear and Diamagnetic Nature of Plasma
and Activities in the Solar Atmosphere, SPD 2009 meetingin American Astronomical Society, (Boulder, CO, USA, Jun.
14-18, 2009).
Shibasaki, K.: 2009, Temperature dependent plasma upflows in
the solar atmosphere and the coronal temperature, IAGA2009,(Sopron, Hungary, Aug. 23-30, 2009).
Shibasaki, K.: 2009, The flare on December 13, 2006 and thestandard solar flare model, Hinode-3: The 3rd Hinode Science
Meeting, (Tokyo, Japan, Dec. 1-4, 2009).

Shiino, T., Todoroki, K., Minh, N., Jiang, L., Shiba, S., Uzawa,Y., Maezawa, H., Sakai, N., Yamamoto, S.: 2009, Improvementof critical temperature of superconducting NbN and NbTiN
thin films using an AlN buffer layer, Int. Superconductive
Electronics Conf. 2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Shimakage, H., Miki, S., Takeda, M., Wang, Z.: 2009, Fabricationof Superconducting MgB2 Nanowires for Hot Electron Type
Detectors, Int. Superconductive Electronics Conf. 2009,(Fukuoka, Japan, Jun. 16-19, 2009).
Shimojo, M.: 2009, The statistical study of polar X-ray jets basedon a thousand events, 2009 XRT Team Meeting, (Boston, USA,
Jun. 22-24, 2009).
Shimojo, M.: 2010, Polar region activity, The 2nd SOLAR-C Science
Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Shimojo, M.: 2010, Science and possible instrumentation with
Normal Incidence Imager, The 2nd SOLAR-C Science
Definition Meeting, (Sagamihara, Japan, Mar. 9-12, 2010).
Shimojo, M.: 2009, The event detection and the apparent velocity
estimation based on computer vision, Hinode-3: The 3rd Hinode
Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Yasuda, N.,
Takata, T.: 2009, AGN and Galaxy Clustering at z = 0.3–3.0
using the Japanese Virtual Observatory, IAU XXVII General
Assembly, (Rio De Janeiro, Brazil, Aug. 03-14, 2009).
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Yasuda, N.,
Takata, T.: 2009, AGN and Galaxy Clustering at z = 0.3 to 3.0
using the Japanese Virtual Observatory, Joint Subaru/Gemini
Science Conf., (Kyoto, Japan, May 18-21, 2009).
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Yasuda, N.,
Takata, T.: 2009, Environment Study of AGNs at z = 0.3 to 3.0
using the Japanese Virtual Observatory, Astronomical Data
Analysis Software and Systems XIX, (Sapporo, Japan, Oct. 4-8,2009).
Sôma, M., Tanikawa, K.: 2009, The Investigation of the Earth
Rotation from Ancient Occultation Records, IAU XXVII
General Assembly, (Rio De Janeiro, Brazil, Aug. 03-14, 2009).
Suematsu, Y.: 2009, Comments on Hinode Operation, ATST
Science Working Group Meeting, (Boulder, CO, USA, Sep.
9-11, 2009).
Suematsu, Y.: 2009, Hinode Results and on possible JapaneseContribution to ATST project, Open House Discussion on
Coordinating International Solar Astronomy Programs, AURA
Solar Observatory Council-International Participants, (Freiburg,
Germany, Oct. 7, 2009).
Suematsu, Y.: 2009, On magnetic origin and evolution of smallscale jets in the solar chromosphere, Hinode-3: The 3rd Hinode
Science Meeting, (Tokyo, Japan, Dec. 1-4, 2009).
Suematsu, Y.: 2009, On the evaluation of image quality of HinodeSolar Optical Telescope, AGU Fall Meeting, (San Francisco,USA, Dec. 14-18, 2009).
Suematsu, Y.: 2009, Review of Hinode Results, First EAST &ATST Workshop in Solar Physics, (Freiburg, Germany, Oct.
14-16, 2009).
Suematsu, Y.: 2009, Small-Scale Jets in the Solar Chromosphere:
T h e i r d y n a m i c s a n d E v o l u t i o n , N S O Wo r k s h o p # 2 5 ,Chromospheric Structure and Dynamics, From Old Wisdom to

New Insights, (NSO - Sunspot, NM, USA, Aug. 31-Sep. 4, 2009).
Suematsu, Y.: 2010, 1.5m telescope and focal plane instruments,
The 2nd SOLAR-C Science Definition Meeting, (Sagamihara,
Japan, Mar. 9-12, 2010).
Suematsu, Y.: 2010, Magnetic origin of chromospheric small-scale
jets, 2nd Meeting of Solar Small-Scale Transient Phenomena
and Their Role in Coronal Heating, (ISSI, Bern, Switzerland,Jan. 25-28, 2010).
Suematsu, Y.: 2010, On science with next solar mission Solar-C
plan-B, 2nd Meeting of Solar Small-Scale Transient Phenomena
and Their Role in Coronal Heating, (ISSI, Bern, Switzerland,Jan. 25-28, 2010).
Sugimoto, K.: 2009, Single dish observation simulator in CASA,
Astronomical Data Analysis Software and Systems XIX,
(Sapporo, Japan, Oct. 4-8, 2009).
Suzuki, T., Honma, M., Higashiyama, K., Yoshida, T., Kajino, T.,
Otsuka, T., Umeda, H., Nomoto, K.: 2009, Neutrino-Induced
Reactions on Ni and Fe Isotopes and Nucleosynthesis in Stars,
Third Joint Meeting of the Nuclear Physics Divisions of the
APS and JPS, (Hawaii, Oct. 13-17, 2009).
Suzuki, T., Noguchi, T., Endo, A., Matsuo, H.: 2009, Origin
of Subgap Current in an SIS Junction, Int. Superconductive
Electronics Conf. 2009, (Fukuoka, Japan, Jun. 16-19, 2009).
Suzuki, T., Noguchi, T., Matsuo, H.: 2009, Origin of subgap current
in an SIS junction, 13th Int. Workshop on Low Temperature
Detectors LTD-13, (Stanford, USA, Jul. 20-24, 2009).
Tachihara, K.: 2009, Small scale structure of cloud surface
perturbed by nearby H II region, Millimeter and Submillimeter
Astronomy at High Angular Resolution, (Taipei, Taiwan, Jun.
8-12, 2009).
Takahashi, R., Arai, K., Tatsumi, D., Izumi, K., Ishizaki, H.,
Fukushima, M., Yamazaki, T., Fujimoto, M.-K., Tsubono, K.,
Takamori, A., DeSalvo, R., Sannibale, V., Bertolini, A., Márka,S., Wakabayashi, Y., Miyakawa, O., Agatsuma, K., TAMA
collaboration: 2009, Development of TAMA300 for LCGT, 8th
Edoardo Amaldi Conf. on Gravitational Waves, (New York,USA, Jun. 21-26, 2009).
Takahashi, R., Kato, Y., Miyoshi M.: 2009, Imaging Simulationsof Quasi-periodic Oscillation of Accretion Discs around Black
Holes, Galactic Center Workshop 2009, (Shanghai, China, Oct.
19-23, 2009).
Takeda, M., Kroug, M., Kojima, T., Fujii, Y., Miyachi, A., Kaneko,
K., Uzawa, Y., Wang, Z.: 2009, Superconducting properties of
NbTiN films, 10th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Wuxi, China, Nov. 15-18, 2009).
Takeda, M., Nakayama, S., Saito, A., Shimakage, H., Uzawa, Y.,
Ohshima, S., Wang, Z.: 2009, Measurements of Microwave
Surface Resistances of NbN and NbTiN Thin Films, Int.
Superconductive Electronics Conf. 2009, (Fukuoka, Japan, Jun.
16-19, 2009).
Tamura, M., Nakajima, Y., Kandori, R., Kusakabe, N., Hashimoto,J., Sato, Y., Saito, H., Nishiyama, S., Fukue, T.: 2009, Infrared
Polarimetry of Star Forming Regions: IRSF and Subaru, An Int.
Workshop on Interstellar Matter and Star Formation – A MultiWavelength Perspective, (Hyderabad, India, Oct. 5-7, 2009).
Tamura, M.: 2009, Direct Explorations of Exoplanets and Disks

II Publications, Presentations077

with Subaru, Joint Subaru/Gemini Science Conf., (Kyoto,
Japan, May 18-21, 2009).
Tamura, M.: 2009, Possible Key Sciences of SPICA Mission:
Planetary Formation, Exoplanets, and our Solar System, SPICA
Joint European-Japanese Workshop, (Oxford, UK, Jul. 6-8, 2009).
Tamura, M.: 2009, Subaru Explorations of Exoplanets and Disks
with its IR Coronagraph, New Technologies for Probing theDiversity of Brown Dwarfs and Exoplanets, (Shanghai, China,
Jul. 19-24, 2009).
Tamura, M.: 2009, Subaru Explorations of Exoplanets and Steps
toward JTPF for Habitable Planets, Pathways towards habitable
planets, (Barcelona, Spain, Sep. 14-18, 2009).
Tamura, M.: 2009, Subaru, SPICA, and Future Japanese Space
Missions, Missions for Exoplanets: 2010-2020, (Pasadena,USA, Apr. 21-23, 2009).
Tamura, M.: 2010, Status Report of the SEEDS Project, The 6th
Exoplanet Conf., (Mitaka, Japan, Jan. 18-20, 2010).
Tamura, Y., Kohno, K., Hatsukade, B., Kawabe, R., Iono, D.,
Ezawa, H., Tosaki, T., Oshima, T., Nakanishi, K., Takada,T., Wilson, G. W., Yun, M. S., Scott, K. S., Austermann, J. E.,
Hughes, D. H., Aretxaga, I., Perera, T. A., Matsuda, Y., Tanaka,
K., Chung, A., Wilner, D.: 2009, The AzTEC/ASTE Survey for
Submillimeter Galaxies in the SSA 22 Proto-Cluster at z = 3.1,
Millimeter and Submillimeter Astronomy at High Angular
Resolution, (Taipei, Taiwan, Jun. 8-12, 2009).
Tamura, Y.: 2009, SG Observations for 20 years, Specialist
meeting for establishing gravity observation network, (Hsinchu,
Taiwan, Dec. 7, 2009).
Tomida, K.: 2010, High-resolution RMHD simulation of Protostellar Collapse, Multi-Phase Interstellar Medium and Dynamics
of Star Formation, (Nagoya, Japan, Feb. 28-Mar. 2, 2010).
Tonooka, H.: 2009, The education and public outreach activity ofHinode in Japan, Hinode-3: The 3rd Hinode Science Meeting,(Tokyo, Japan, Dec. 1-4, 2009).
Tsujimoto, T., Bekki, K.: 2009, Evidence of a Major Merger in
the Small Magellanic Cloud Imprinted in the Age-Metallicity
Relation, The Milky Way and the Local Group – Now and in
the Gaia Era, (The University of Heidelberg, Germany, Aug.
31-Sep. 4. 2009).
Tsujimto, T., Bland-Hawthorn, J., Freeman, K. C.: 2009, Galactic
winds and the evolution of the Galactic abundance gradient, JD
5: Modelling the Milky Way in the Era of Gaia at IAU Gneral
Assembly 27, (Rio de Janeiro, Brazil, Aug. 6-7, 2009).
Tsujimto, T., Bland-Hawthorn, J.: 2009, Chemical Evolution of
D in the Local Disk, IAU Symp. 268 "Light Elements in the
Universe", (Geneva, Switzerland, Nov. 9-13, 2009).
Tsujimto, T.: 2009, Galaxy Formation through Winds, Infall, andMerger: Learning from Galactic Archaeology, Huntinh for
the Dark: The Hidden Side of Galaxy Formation, (Malta, Oct,19-23, 2009).
Tsuneta, S.: 2009, JAXA's Solar-C Mission Opitons and Science
Goals, 3rd Solar Orbiter Workshop, (Sorrent, Italy, May 25-29,
2009).
Tsuneta, S.: 2010, Future prospects for Solar-C, The 2nd SOLAR-C
Science Definition Meeting, (Sagamihara, Japan, Mar. 9-12,
2010).

078

II Publications, Presentations

Ueda, H., Gouda, N., Yano, Y., Koyama, H.: 2009, A New Approachto the Construction of Dynamical Structure of our Galaxy, JD
5: Modelling the Milky Way in the Era of Gaia at IAU Gneral
Assembly 27, (Rio de Janeiro, Brazil, Aug. 6-7, 2009).
Ueda, K.: 2009, Orientation of X-ray bright points in the quiet
Sun, Hinode-3: The 3rd Hinode Science Meeting, (Tokyo,
Japan, Dec. 1-4, 2009).
Umemoto, T.: 2009, Concept of VSOP-2 Science Operation Center(SOC: tentative), Astronomical Data Analysis Software andSystems XIX, (Sapporo, Japan, Oct. 4-8, 2009).
Umemoto, T.: 2010, Overview of VSOP-2 (ASTRO-G) Project,
The First Asia-Europe Physics Summit, (Tsukuba, Japan, Mar.
24-26, 2010).
Uzawa, Y., Kojima, T., Kroug, M., Takeda, M., Candotti, M.,
Fujii, Y., Kaneko, K., Shan, W., Noguchi, T., Wang, Z.: 2009,
Sensitive Terahertz SIS Receiver for the ALMA Telescope, Int.
Superconductive Electronics Conf. 2009, (Fukuoka, Japan, Jun.
16-19, 2009).
Uzawa, Y., Kojima, T., Kroug, M., Takeda, M., Candotti, M.,
Fujii, Y., Shan, W., Kaneko, K., Shitov, S., Wang, M.: 2009,
Development of the 787-950 GHz ALMA Band 10 Cartridge,
Int. Symp. on Space THz Technology 2009, (Virginia, USA,
Apr. 20-22, 2009).
Wada, K.: 2009, Feedback on the dark domain, IAU Symp. 267"Evolution of Galaxies and Central Black Holes: Feeding andFeedback", (Rio de Janeiro, Brazil, Aug. 10-14, 2009).
Wang, Z., Miki, S., Takeda, M., Fujiwara, M., Sasaki, M.: 2009,
Superconducting nanowire single photon detectors withepitaxial NbTiN thin films, 9th European Conf. on Applied
Superconductivity, (Dresden, Germany, Sep. 15, 2009).
Watanabe, J., Honda, M., Ishiguro, M., Ootsubo, T., Sarugaku, Y.:
2009, Early Phase of the Outburst of Comet 17P/Holmes, IAU
Symp. 263 "Icy Bodies in the Solar System", (Rio de Janeiro,
Brazil, Aug. 3-7, 2009).
Watanabe, J.: 2009, Star Week -A Successful Campaign in Japan-,
Astronomy Education between Past and Future, Specail session
SpS4, SpS-p:46, (Rio de Janeiro, Brazil, Aug. 3-14, 2009).
Watanabe, J.: 2010, The number is the matter: Great Success of
IYA Activities in Japan, Communicating Astronomy with the
Public 2010, (Cape Town, South Africa, Mar. 15-19, 2010).
Watanabe, T.: 2009, FeXVII Emission Lines Seen in the Hinode/
EIS Observing Wavelengths, AGU Fall Meeting, (San Francisco,USA, Dec. 14-18, 2009).
Watanabe, T.: 2010, Particle acceleration – Non-equilibrium plasma
diagnostics, The 2nd SOLAR-C Science Definition Meeting,(Sagamihara, Japan, Mar. 9-12, 2010).
Yagi, M.: 2009, An algorithm of refinement of image alignment forimage subtraction, Astronomical Data Analysis Software andSystems XIX, (Sapporo, Japan, Oct. 4-8, 2009).
Yamada, Y., Gouda, N., Yano, T., Hatsutori, Y., Kobayashi, Y.,
Tsuiki, A., Kamiyoshi, S.: 2009, JASMINE as small satellite, JD
5: Modelling the Milky Way in the Era of Gaia at IAU Gneral
Assembly 27, (Rio de Janeiro, Brazil, Aug. 6-7, 2009).
Yamada, Y., Hatsutori, Y., Ushiyama, T., Kobayashi, Y., Gouda,N., Yano, T.: 2009, Design and Implementation of Mission OnBoard Computer for Nano-JASMINE, 27th Int. Symp. on SpaceTechnology and Science, (Tsukuba, Japan, Jul. 5-12, 2009).
Yamada, Y., JASMINE WG: 2009, Nano-JASMINE –mission
status and data analysis–, The Milky Way and the Local Group– Now and in the Gaia Era, (The University of Heidelberg,
Germany, Aug. 31-Sep. 4. 2009).
Yamamoto, S., Nakamura, R., Matsunaga, T., Ogawa, Y., Ishihara,Y., Morota, T., Hirata, N., Ohtake, M., Hiroi, T., Yokota, Y.,
Haruyama, J.: 2010, Global Distribution of Olivine Exposureson the Moon Revealed by SELENE Spectral Profiler, 41st
Lunar and Planetary Science Conf. (LPSC 2010), (Woodlands,
Texas, USA, Mar. 1-5, 2010).
Yamashita, T.: 2009, SPICA observations of transiting extra-solar
planets, SPICA Joint European - Japanese Workshop, (Oxford,
UK, Jul. 6-8, 2009).
Yano, T., Araki, H., Hanada, H., Tazawa, S., Asari, K., Gouda,N., Kobayashi, Y., Yamada, Y., Niwa, Y.: 2009, Centroiding
experiment for determining the positions of stars with highprecision, Astronomical Data Analysis Software and Systems
XIX, (Sapporo, Japan, Oct. 4-8, 2009).
Yano, T., Gouda, N., Ueda, H., Koyama, H.: 2009, A Methodof the Estimation of Dynamical Structure of our Galaxy fromAstrometric Data, JD 5: Modelling the Milky Way in the Era ofGaia at IAU Gneral Assembly 27, (Rio de Janeiro, Brazil, Aug.
6-7, 2009).
Yasutake, N., Maruyama, T., Tatsumi, T.: 2009, Hot hadron-quark
mixed phase including hyperons, APS&APS joint meetings on
Nuclear Physics 4th, (Hawaii, USA, Oct. 20, 2009).
Yasutake, N., Maruyama, T., Tatsumi, T.: 2009, The pasta structurein the hadron-quark phase transition and the effects onmagnetized compact stars, Compact stars in the QCD phase
diagram II, (Beijin, China, Jun. 19, 2009).
Yasutake, N., Maruyama, T., Tatsumi, T.: 2010, Finite size effects
on hot hadron-quark mixed phase including hyperons, Origin
of Matter and Evolution of Galaxies, (Osaka, Japan, Mar. 8-10,
2010).
Yasutake, N., Maruyama, T., Tatsumi, T.: 2010, Quark-hadron phasetransition and the effects on the structures of compact stars, New
Frontiers in QCD 2010, (Kyoto, Japan, Jun.19, 2010).
Yokochi, K., Nishikawa, J., Murakami, N., Abe, L., Kotani, T.,
Tamura, M., Tavrov, V. A., Takeda, M., Kurokawa, T.: 2009,
High dynamic range optical system for direct detection of exoplanets by unbalanced nulling interferometer and adaptive
optics, Conf. on Lasers and Electro-Optics (CLEO), (Baltimore,
USA, May 31-Jun. 5, 2009).
Yoshida, F., Ito, T., Takahashi, S., Nozawa, Y., Ibrahimov, M.
A., Marshalkina, A. L.: 2009, Photometric observations ofYoung asteroid families at Maidanak Observatory, UBAI
Seminar, (UBAI, Uzbekistan, Nov. 21, 2009).
Yoshida, F., The HSC Solar System Science Group: 2009, Survey
Design for the Small Solar System Objects with the Hyper
Suprime-Cam (HSC), Asia-Oceania Geoscience Society 6th
Annual Meeting, (Suntech, Singapore, Aug. 11-15, 2009).
Yoshida, F., Yagi, M., Komiyama, Y., Nakata, F., Furusawa,
H., Ohno, T., Okamura, S., Nakamura, T.: 2010, A possible
collaboration with the Slitless Spectroscopic survey of Small
Solar System Bodies by Subaru Telescope, 2010 Asian asteroid

observation network workshop, (Lijiang, China, Mar. 11-13,
2010).
Yoshida, F.: 2009, 君もガリレオプロジェクト , 世界天文年イベン, (Uzbekistan,ト「君もガリレオプロジェクトinウズベキスタン」
Oct. 22, 2009).
Yoshida, F.: 2009, An Insight into the Solar System History
through the Size Distribution of Jupiter Trojans, CPS Workshop
on Icy Moons and Origin of Jupiter and other Giant Planets,(Sapporo, Japan, Nov. 9-10, 2009).
Yoshida, F.: 2009, Asia-wide observational network for NEO
observation, Asian Asteroid Observation Network Workshop,(Purple Mountain Observatory, China, Jul. 25-26, 2009).
Yoshida, F.: 2009, Asia-wide observational network for NEO
observation, Maidanak User’s Meeting, (Seoul, Korea, Jun. 30,2009).
Yoshida, F.: 2009, Collaborations between NCU and NAOJ 1. Improvements of the Maidanak observatory 2. The HSC
survey for small solar system bodies, NCU-CPS Japan-Taiwan
Planetary Science Workshop, (NCU, Taiwan, Dec. 8-9, 2009).
Yoshida, F.: 2009, Photometric observations of young asteroids
families at Maidanak Observatory, Asian Asteroid Observation
Network Workshop, (Purple Mountain Observatory, China, Jul.
25-26, 2009).
Yoshida, F.: 2009, Photometric observations of young asteroids
families at Maidanak Observatory, Maidanak User’s Meeting,(Seoul, Korea, Jun. 30, 2009).
Yoshida, F., Yagi, M., Komiyama, Y., Nakata, F., Furusawa, H.,
Ohno, T., Okamura, S., Nakamura, T.: 2010, Slitless Spectroscopyof Small Solar System Bodies on a Dark Cloud Curtain, 41st
Lunar and Planetary Science Conf. (LPSC 2010), (Woodlands,
Texas, USA, Mar. 1-5, 2010).
Yoshida, H.: 2009, Necessary conditions for super-integrability ofHamiltonian systems with homogeneous potential, CELMEC 5,(Viterbo, Italy, Sep. 6-11, 2009).
Yoshida, H.: 2010, Criteria for integrability of Hamiltoniansystems based on differential Galois theory vs singular point
analysis, China-Japan Joint workshop on Integrable Systems,(Shaoxing, China, Jan. 7-10, 2010).

II Publications, Presentations079