Cover Caption
Most distant and ancient supernovae discovered by the Subaru Telescope. In the image, which show the Subaru Deep Field, numerous
supernovae related to white dwarfs were found, and ten of them had exploded more than ten billion years ago. This discovery gives an importantclue to study how the heavy elements created in the ancient universe (Graur et al. MNRAS, 417, 916, 2011).

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
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Annual Report of the
National Astronomical Observatory of Japan

Fiscal 2011

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Masahiko HAYASHI
Director General
National Astronomical Observatory of Japan

Preface

I Scientific Highlights April 2011 – March 2012

001

II Publications, Presentations
1

Refereed Publications

063

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Publications of the National Astronomical Observatory of Japan

073

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Report of the National Astronomical Observatory of Japan

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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 2011

P R E F A C E
Masahiko HAYASHI
Director General of NAOJ

It is my pleasure to present the Annual Report of the
National Astronomical Observatory of Japan (NAOJ) for
the fiscal year 2011 (FY2011).
The FY2011 began in the aftermath of the East
Japan Earthquake. Although the earthquake caused
significant damage to two antennas at the Mizusawa
VLBI Observatory in Tohoku – including a 20-metre
VLBI Earth Rotation Astrometry (VERA) antenna –and a further two VLBI antennas located in Takahagi

and Hitachi, they have all been restored and are fully
operational. It is also worth noting that the supercomputerat the Mitaka headquarters was in fallback operations
during the 2011 summer season in order to reduce energy
consumption.
On July 2, there was a coolant leak from the prime
focus of the Subaru Telescope. As a result, we were forced
to temporarily stop the operation of the telescope as theprimary mirror and observing instruments, includingSuprime-Cam, were inoperative. We apologize to Subaru
users and other persons concerned for the inconveniencecaused by this interruption. Corrective measures weretaken immediately, by cleaning the primary mirror andrepairing the damaged instruments. Furthermore, a special
committee was established to investigate the cause of theleak in order to prevent a future recurrence.
The ALMA project is making steady progress at the
Atacama plateau in Chile. Currently, 16 antennas outof 66 are available for observations. The Joint ALMA
Observatory announced the call for proposals for Cycle
0 – a preliminary open-use period, with 16 antennas thisyear. By the end of June 2011, more than 900 proposals
were submitted from all over the world, revealing
extraordinarily high levels of interest from the global
scientific community in ALMA. About 150 proposals
were submitted to Cycle 0 from Japan, the second
largest number of submissions among the ALMA member
countries. The Cycle 0 observation began in October
2011 and we expect some exciting results from ALMA
observations to be released to the public in the near future.
Meanwhile, the Subaru Telescope continues to be
productive, despite the accident mentioned above. Morethan 120 scientific papers are published per year, whichmeans about one research paper every three days. Manyof the papers published in the FY2011 are categorized into
two areas: the first is distant galaxies, clusters of galaxies
and dark matter; the second is exoplanets and disks
around young stars. These are the main streams of modern
astronomy, where the Subaru Telescope plays an importantrole. In fact, the Subaru Telescope has made remarkable
contribution to the advancement of evolutionary studies
of distant galaxies and clusters of galaxies.

planets is impossible. We need a larger light collecting
area, sharper imaging resolution, and higher contrast. This
will be achieved by the Thirty Meter Telescope (TMT),
which will be constructed on Mauna Kea, at a slightly
lower elevation than Subaru. Representatives from theprospective partners – Japan, USA (California and NSF),
Canada, India and China – are busy coordinating theconstruction of TMT, which is expected to begin in thespring of 2014. Japan plans to assume the construction of
the telescope structure and part of the primary mirror.
There are also growing aspirations for Solar-C, anext generation space-based solar observatory that will
succeed Hinode. Recently, the solar activity appears tobe slipping out of phase from its long sustained 11-year
period, which has been attracting global attention because
it might eventually cause significant environmental
changes. The NAOJ recognizes the importance of suchresearch and is always committed to fulfilling its societal
responsibilities.
The FY2012 will mark the completion of ALMA andthe 30th anniversary of the Nobeyama Radio Observatory,
which has produced some astounding scientificachievements. Astronomy is always rapidly changing,with new telescopes being planned and realized, while
those that were once at the frontier of science eventually
become obsolete. It is the mission of the NAOJ to respondto these changes and to provide advanced facilities that
attract top researchers from around the world so that we
can return important scientific results to society.

The most impressive feature of the Subaru Telescopeis its wide-field capability. Now we have developed
a 900-megapixel Hyper Suprime-Cam at the NAOJ
Advanced Technology Center in Mitaka. It will provide
a field of view several times larger than the current
Suprime-Cam. Furthermore, new corrector optics will
provide sharp and undistorted stellar images over theentire CCD area.
The Subaru Telescope has successfully imaged
gaseous giant exoplanets, but imaging Earth-like rocky

Masahiko HAYASHI
Director General of NAOJ

I Scientific Highlights(April 2011 – March 2012)

01

Complex Scattered Radiation Fields and Multiple Magnetic Fields in the
Protostellar Cluster in NGC 2264

02 Potential Members of Stellar Kinematic Groups within 30 pc of the Sun
03 Beryllium Abundances of Solar-Analog Stars
04

Infrared 18 μm High-Spatial-Resolution Imaging of nearby Luminous
Infrared Galaxies Using Subaru and Gemini South Telescopes

05 The Inner Structure of Collisionless Magnetic Reconnection
06

Clustered Star Formation in Magnetic Clouds: Properties of Dense Cores
Formed in Outflow-Driven Turbulence

07 Molecular Outflows From the Protocluster, Serpens South08

Evidence For Cloud-Cloud Collision and Parsec-Scale Stellar Feedback
within the L1641-N Region

09 Hα Emission from Magellanic Stream
Three Classical Cepheid Variable Stars in the Nuclear Bulge of the MilkyWay
Near-Infrared Imaging Polarimetry toward Serpens South: Revealing the11
Importance of the Magnetic Field
10

KWON, J., et al.

003

NAKAJIMA, T., MORINO, J.-I.

004

TAKEDA, Y., et al.

005

IMANISHI, M., et al.

006

ZENITANI, S.

007

NAKAMURA, F., LI, Z.-Y.

008

NAKAMURA, F., et al.

009

NAKAMURA, F., et al.

010

YAGI, M., et al.

011

MATSUNAGA, N., et al.

012

SUGITANI, K., et al.

013

Oscillation Phenomena in the Disk around the Massive Black HoleMIYOSHI, M., et al.
Sagittarius A*
Observational Identification of First Cores: Non-LTE Radiative Transfer
13
TOMISAKA, K., TOMIDA, K.
Simulation
12

014
015

14 A discovery of Red Star Forming Galaxies in Groups at z = 0.4

KOYAMA, Y., et al.

016

15 Subaru Measurements of Spin-Orbit Alignment Angles of Exoplanets

NARITA, N., et al.

017

KODA, J., et al.

018

URAKAWA, S., et al.

019

Images of the Extended Outer Regions of the Debris Ring around HR 4796
A

THALMANN, C., et al.

020

19 Development of the Ultra-Low Loss Mirrors for Gravitational Wave Detector

TATSUMI, D., UEDA, A.

021

Astrometry of 6.7 GHz Methanol Maser toward W3(OH) with Japanese
VLBI Network

MATSUMOTO, N., et al.

022

OTSUJI, K., et al.

023

HAYASHI, M., et al.

024

HANAOKA, Y., et al.

025

SCHOLZ, A., et al.

026

OJHA, D. K., et al.

027

TAKAHASHI, H., et al.

028

27 Size Distribution of Main-Belt Asteroids with High Inclination

TERAI, T., ITOH, Y.

029

28 Orion IRc2, Radiated by the Scattering of Emission from Source I

OKUMURA, S., et al.

030

NAKAMURA, K., et al.

031

16 The Standard IMF in the Outskirts of M83
17 Photometric Observations of 107P/Wilson-Harrington
1820

21 Statistical Study of Flux Emergences on the Sun
Properties of Star-Forming Galaxies in a Cluster and its Surrounding
Structure at z = 1.46
Practical Method to Derive Non-Linear Response Functions of Cameras for
23
Scientific Imaging
Substellar Objects in nearby Young Clusters (SONYC). IV. A Census of
24
Very Low Mass Objects in NGC 1333
22

25 Star Formation Activity in the Galactic HII Complex S255-S257
26 Scaling Law of Relativistic Sweet-Parker Type Magnetic Reconnection

29 Properties of Weak Measurements through Exact Evaluations

001

30

Efficient Parallel Computation of All-Pairs N-body Acceleration by Do
Loop Folding

FUKUSHIMA, T.

032

SUDOU, H., IGUCHI, S.

033

TAMURA, Y., et al.

034

33 SDSS J1334+3315: A Resolved Lensed Quasar with Separation 0.″8

RUSU, C. E., et al.

035

34 Completing the Census of Lyα Emitters at the Reionization EpochKASHIKAWA, N., et al.

036

35 Identification of the Bursting Water Maser Features in Orion KL

HIROTA, T., et al.

037

36 Detection of Chemically Young Dark Cloud Cores in the Aquila Rift

HIROTA, T., et al.

038

YANO, T., et al.

039

ONO, Y., et al.

040

TOSAKI, T., et al.

041

40 Formation of a Propeller Structure by a Moonlet in a Dense Planetary Ring MICHIKOSHI, S., KOKUBO, E.

042

41 Secular Gravitational Instability of a Dust Layer in Shear Turbulence

MICHIKOSHI, S., et al.

043

42 Stellar Populations and spatial distributions of ultra faint dwarf galaxies

OKAMOTO, S., et al.

044

KUZUHARA, M., et al.

045

NAGAYAMA, T., et al.

046

OSHINO, S., et al.

047

IKARASHI, S., et al.

048

YAMAZAKI, D.-G., et al.

049

HANAYAMA, H., et al.

050

HANAYAMA, H., et al.

051

WATANABE, J.-I., et al.

052

Global Structure of Three Distinct Accretion Flows and Outflows around
51 Black Holes from Two-Dimensional Radiation-Magnetohydrodynamic OHSUGA, K., MINESHIGE, S.
Simulations

053

31 Detection of Proper Motion of the Sub-Parsec-Scale Jet in 3C 66B
32 The Millimeter Sky Transparency Imager (MiSTI)

37 Small-JASMINE: Stray Light and Thermal Environment
Spectroscopic Confirmation of Galaxies at z = 6.844 –7.213: Demographics
of Lyα Emission in z ~ 7 Galaxies
NRO M33 All Disk Survey of Giant Molecular Clouds (NRO MAGiC): HI39
to H2 Transition
38

43

The Widest-Separation Substellar Companion Candidate to a Binary T
Tauri Star

44 Astrometry of Galactic Star-Forming Region G48.61+0.02 with VERA
Particle-Particle Particle-Tree: A Direct-Tree Hybrid Scheme for Collisional
N-Body Simulations
Detection of an Ultra-Bright Submillimeter Galaxy in the Subaru/XMM46
Newton Deep Field Using AzTEC/ASTE
47 Effects of Magnetic Fields with Log-Normal Distribution on the CMB
45

48

Observational Evidence for an Impact on the Main-Belt Asteroid (596)
Scheila49 Multiband Optical Observation of P/2010 A2 Dust Tail50

Expedition for Ground-Based Observation of HAYABUSA Spacecraft ReEntry

Gravitational Wave Signatures of Magnetohydrodynamically Driven CoreCollapse Supernova Explosions

TAKIWAKI, Tomoya

054

53 Cosmological Time-Dependent Quark Masses and Big Bang Nucleosynthesis

CHEOUN, M.-K., et al.

055

Gamow-Teller St reng ths in Ni Isotopes and Elect ron Capt u re in
Gravitational Core-Collapse of Massive StarsSUZUKI, T., et al.

056

55 Role of β-Decays of N=126 Isotones in Supernova R-Process Nucleosynthesis

SUZUKI, T., et al.

057

Asymmetric Neutrino Reaction from Magnetized Proto-Neutron Stars infully Relativistic Framework

MARUYAMA, T., et al.

058

PEHLIVAN, Y., et al.

059

RYU, C. Y., et al.

060

CHEOUN, M.-K., et al.

061

BOYD, R. N., et al.

062

52

54

56

57 Nonlinear Neutrino Oscillations in Astronomy
58 Properties of the Proto-Neutron Star with Smeared Trapped Neutrinos
59

40

Reactions on Ar Involving Solar Neutrinos and Neutrinos from CoreCollapsing Supernovae

60 The r-Process in Metal Poor Stars and Black Hole Formation

002

Complex Scattered Radiation Fields and Multiple Magnetic Fields
in the Protostellar Cluster in NGC 2264
KWON, Jungmi, TAMURA, Motohide(Graduate University for Advanced Studies / NAOJ)

KANDORI, Ryo, KUSAKABE, Nobuhiko, HASHIMOTO, Jun, NAKAJIMA, Yasushi(NAOJ)NAKAMURA, Fumitaka(Graduate University for Advanced Studies / NAOJ)

HOUGH, James H.

(University of Hertfordshire)

NAGAYAMA, Takahiro(Nagoya University)		

WERNER, Michael W.

(Jet Propulsion Laboratory)

Near-infrared imaging polarimetry in the J, H, andKs bands has been carried out for the protostellar cluster
region around NGC 2264 IRS 2 in the Monoceros OB1
molecular cloud. Various infrared reflection nebulaclusters (IRNCs) associated with NGC 2264 IRS 2 andthe IRAS 12 S1 core, as well as local infrared reflection
nebulae (IRNe), were detected. The illuminating sourcesof the IRNe were identified with known or new nearand mid-infrared sources. In addition, 314 point-likesources were detected in all three bands and their aperturepolarimetry was studied. Using a color-color diagram,
reddened field stars and diskless pre-main-sequence stars
were selected to trace the magnetic field (MF) structureof the molecular cloud. The mean polarization position

Figure 1: H polarization vector map superposed on the color
composite image in the IRSF/SIRPOL JHKs (blue),
Spitzer/IRAC 5.8 μm and Spitzer/MIPS 24 μm (red)bands. The length of the vectors is proportional to thedegree of polarization. Shown in the upper left corneris a 20 % vector. The vectors were made by 6 × 6 pixel
smoothing (twice the seeing size), and the vectors
were shown every 6 pixels with intensities greater than
3σ above the mean sky level, where is the standard
deviation of sky brightness. Three IRNCs are labeled.

NAGATA, Tetsuya(Kyoto University)

TEIXEIRA, Paula S.

(European Southern Observatory)

angle of the point-like sources is 81° ± 29° in the cluster
core, and 58° ± 24° in the perimeter of the cluster core,
which is interpreted as the projected direction on thesky of the MF in the observed region of the cloud. The
Chandrasekhar-Fermi method gives a rough estimate of
the MF strength to be about 100 μG. A comparison withrecent numerical simulations of the cluster formation
implies that the cloud dynamics is controlled by the
relatively strong MF. The local MF direction is wellassociated with that of CO outflow for IRAS 12 S1and consistent with that inferred from submillimeterpolarimetry. In contrast, the local MF direction runs
roughly perpendicular to the Galactic MF direction [1].

Figure 2: Stokes I image of the H band with contours of 870 μm
continuum emission [2]. Con- tours are at 0.5, 1.0, 1.5,
2.0, and 2.5 Jy beam−1. Red con- tours: dense cluster of
the IRS 1 region. Blue contours: dense cluster of the IRS
2 region.

References[1] Kwon, J., et al.: 2011, ApJ, 741, 35.
[2] Williams, J., Garland, C.: 2002, ApJ, 568, 259.

I Scientific Highlights

003

Potential Members of Stellar Kinematic Groups within 30 pc of the Sun
NAKAJIMA, Tadashi, MORINO, Jun-Ichi(NAOJ)

Age dating of individual stars in general is a very
difficult task. Usually groups of stars or stellar clusters
provide us with age-controlled sample of stars. For
instance, a globular cluster is considered to be the sourceof an old sample of coeval stars in the halo with rather
uniform metallicity. On the other hand, an open cluster
provides us with a relatively young sample of stars with asimilar age in the Galactic disk.
Some open clusters are located closer to the Sun than
the nearest-by star-forming regions, such as Taurus andChamaeleon dark clouds located at about 140 pc of theSun. Due to the proximity, spatial localization alone is
not a stringent criterion for the membership for theseclusters. At least the proper motion and mean radial
velocity have been used to define a kinematic group.
Nearby streams of stars identified this way are called“stellar kinematic groups (SKGs)”. At least eleven SKGs
are known to date [1]. Owing to the success of Hipparcos
in measuring parallaxes and proper motions of stars in thesolar neighborhood, and to ground-based observational
efforts to obtain radial velocities of nearby stars, threedimentional velocity information is available for a setof nearby stars brighter than about V = 11 measured by
Hipparcos within about 40 pc of the Sun.
A sample of age-controlled young stars in the very
solar neighborhood has a wide range of applications. For
instance, the direct detection of sub-stellar companions
and planets is possible only around these young stars
with the present-day technology, since brown dwarfs andplanets shine only by the release of their gravitationalenergy. For instance, Gl 229A, the main star of Gl 229B,
was selected as a target for the brown dwarf search,based on its kinematic youth as a young disk star [2,3].
However, the age of Gl 229AB system is not known
precisely enough to estimate the mass of Gl 229B. Since
the luminosity of a brown dwarf or a planet depends
on both its mass and age, the knowledge of the age
is essential in obtaining the mass from its luminosity.
Other than that, age controlled samples are useful for thestudies of stellar properties such as chromospheric andcoronal activities, magnetic field strength, rotation, andthe presence of circumstellar disks around them.
We analyze the kinematic histories of stars within
30 pc of the Sun, for which three-dimensional spatial
coordinates and three-dimensional velocity vectors, areavailable. From this sample, we extract members ofstellar kinematic groups (SKGs) in the following manner.
First, we consider in the three-dimensional velocity spacecentered on the local standard of rest, a sphere with aradius of 8 km s−1 centered on the mean velocity vector004

I Scientific Highlights

of a particular SKG. Around each SKG velocity center,
we have found significant excess of stars compared tobackground field stars. For each candidate, in the threedimensional spatial coordinate space, its trajectory is
traced back in time by the age of the relevant SKG, toobtain the estimated distance from the SKG center at thetime of the SKG’s birth by the epicyclic approximationand harmonic vertical motion. It often happens that a staris a candidate member of multiple SKGs. Then we rank
the candidacy to multiple SKGs based on the smallnessof distance separations. This way, we have kinematicallyselected 238 candidates. Then we further impose atleast one of the following qualitative criteria to be amember: spectral type A or B, variability, or EUV and
X-ray emission. We have finally selected 137 candidate
members of SKGs out of a sample of 966 stars [4].
SKG

Age (Myr)# of members

TW Hydra

8

13

η Cha

8

6

Cha-Near

10

7

β Pic

12

8

Tuc-Hor30

7

IC 2391

45

17

AB Dor50

18

Pleiades120

0Castor200

19

Ursa Major

300

33

Hyades600

9References[1] Zuckerman, B., Song, I.: 2004, ARA&A, 42, 685.
[2] Nakajima, T., Oppenheimer, B. R., Kulkarni, S. R., Golimowski,
D. A., Durrance, S. T.: 1995, Nature, 378, 463.
[3] Leggett, S. K.: 1992, ApJS, 82, 351.
[4] Nakajima, T., Morino, J-I.: 2012, AJ, 143, 2.

Beryllium Abundances of Solar-Analog Stars
TAKEDA, Yoichi, TAJITSU, Akito, KAWANOMOTO, Satoshi, ANDO, Hiroyasu, SAKURAI, Takashi(NAOJ)

HONDA, Satoshi(Kyoto University)

The surface Li abundances (ALi) in solar-analog stars(i,e., early G-type main-sequence stars like our Sun)show a remarkably large diversity amounting to morethan ~2 dex. Why such a large difference is produced
for stars with similar parameter values? We previously
found in statistical study on 118 selected solar-analogs
based on the OAO/HIDES spectra that A Li depends
upon the rotational velocity (see [1]). This finding was
further corroborated from the viewpoint of stellar activity(controlled by rotation via a dynamo) estimated from thecore flux of the Ca II 8542 line [2].
Then, why slow rotation leads to an efficient Li
depletion? Interestingly, according to Bouvier’s recent
theoretical simulation [3], slow rotators develop a highdegree of differential rotation between the radiative core
and the convective envelope, which eventually promotes
lithium depletion by enhanced mixing, while such core–envelope decoupling does not evolve in faster rotators.
Then, the key to understanding the mixing process lies in“the bottom of the convection zone” (i.e., “tachocline”),
where the condition may be probed by examining theabundance of Be along with Li (each having different
burning temperatures). (See Figure 1 showing thestructure of the solar envelope model taken from [4].)Accordingly, we conducted an extensive beryllium
abundance analysis for the same sample of 118 solar
analogs (based on the high-dispersion UV spectra
obtained with Subaru/HDS in 2009–2010) by applying
the spectrum synthesis technique to the near-UV region
comprising the Be II line at 3131.066 Å, in an attempt toinvestigate how and whether Be suffers any depletion
such as the case of Li showing a large diversity.
Our findings are as follows (cf. Figure 2):—In marked contrast to Li, most (~96%) of the solar
analogs are superficially similar in terms of their ABe.
—However, 4 out of 118 stars turned out strikingly Bedeficient (by > ~ 2 dex) and these 4 stars have the lowest
ve sin i, the lowest stellar activity, and depleted ALi.
—Moreover, even for the other majority showing anapparent similarity in Be, we can recognize a tendency
that A(Be) gradually increases with an increase in ve sin i.
These results suggest that any solar analog star(including the Sun) generally suffers some kind ofrotation-dependent Be depletion, for which we suspect
two kinds of mechanisms may operate: The “strong”
process should work only in limited cases under special
conditions but depletes surface Be very efficiently once
triggered, whereas the “weak” process acts on most stars

and slowly reduce Be in the outer envelope. Contributionsof theoreticians are awaited toward developing areasonable model accounting for these observational
facts.
See [5] for more details of this study.

Figure 1: Physical structure of the envelope of the Sun.

Figure 2: Be abundances plotted against the projected rotational
velocity.
References[1] Takeda, Y., Kawanomoto, S., Honda, S., Ando, H., Sakurai, T.:2007, A&A, 468, 663.
[2] Takeda, Y., Honda, S., Kawanomoto, S., Ando, H., Sakurai, T.:2010, A&A, 515, A93.
[3] Boubier, J.: 2008, A&A, 489, L53.
[4] Stix, M.: 2002, The Sun, 2nd ed. (Berlin: Springer), ch.6.
[5] Takeda, Y., Tajitsu, A., Honda, S., Kawanomoto, S., Ando, H.,
Sakurai, T.: 2011, PASJ, 63, 697.

I Scientific Highlights

005

Infrared 18μm High-Spatial-Resolution Imaging of nearby Luminous
Infrared Galaxies Using Subaru and Gemini South Telescopes
		

IMANISHI, Masatoshi(NAOJ)			

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

Luminous infrared galaxies (LIRGs) radiate verylarge infrared luminosities with LIR > 1011 L, and so mustpossess luminous energy sources hidden behind dust,
which absorbs the bulk of the primary energetic radiation,is heated, and produces strong thermal infrared radiation.
The dust-obscured hidden energy sources can be either
starburst (energy release by nuclear fusion reaction
inside stars) and/or AGN activity (release of gravitationalenergy by a mass accreting active supermassive blackhole). We have previously performed systematic infrared
2.5 – 40 μm low-resolution spectroscopy of LIRGs, toinvestigate the relative energetic roles of starburst and
AGN activity [1,2]. Based on the strengths of polycyclicaromatic hydrocarbon emission and dust absorption
features detected in infrared spectra, AGNs withhard primary energetic radiation and more centrallyconcentrated energy source geometry than dust, can bedifferentiated from normal starbursts which emit soft
energetic radiation and have mixed energy sources anddust geometry. Although AGNs and normal starbursts are
distinguishable, an extreme starburst, consisting of HIIregions only and showing an exceptionally centrallyconcentrated energy source geometry, can produce similar
infrared spectral shapes to AGNs, and so cannot be ruledout based on infrared spectroscopy alone.
It is shown, both theoretically and observationally,that there is an upper limit for the emission surface
brightness of starburst activity with ~1013 L kpc−2 [3,4],
because the radiative energy generation efficiency of
nuclear fusion inside stars is modest (0.7 % of Mc2). It isvery difficult even for an extreme starburst to exceed thisthreshold by a large factor, as long as the extreme starburst
is powered by nuclear fusion. On the other hand, an AGN
can produce much higher emission surface brightness,because the efficiency of a mass accreting supermassive
blackhole can be 6 – 42 % of Mc 2. Thus, a very highemission surface brightness energy source, if detected,
must be an AGN, rather than an extreme starburst.
We performed infrared 18 μm high-spatial-resolution
imaging of nearby luminous infrared galaxies using
Subaru 8.2 m and Gemini South 8.1 m telescopes (Figure1). Infrared 18 μm observations can probe the dominant
dust emission components of luminous infrared galaxies,
and the point spread function (PSF) is stable at 18 μm,
due to the reduction of Earth’s atmospheric turbulence,
making reliable discussion of intrinsic emission’s spatial
extent possible. Since we can constrain the emission
size more strongly, and obtain a more stringent lower
limit of emission surface brightness using ground-basedlarge 8–10 m telescopes than space-based satellites with

006

I Scientific Highlights

ICHIKAWA, Kohei(Kyoto University)

small apertures, our ground-based data play a crucialrole. We found that many LIRGs with AGN signatures inpreviously-taken infrared spectra show emission surface
brightnesses much higher than the maximum value set bya starburst phenomenon, supporting the AGN scenario forthese galaxies, rather than the extreme starburst picture [5].

Figure 1: Infrared 18 μm images taken with Subaru (Top andbottom; 5″×5″) and Gemini South telescope (Middle;
8″×8″). (Left) : galaxies. (Right) : corresponding PSF
reference stars. North and East directions are indicated.
(Top and middle): Infrared emission from galaxies iscompact and its spatial extent is indistinguishable from
PSF stars. The observed very high emission surface
brightnesses suggest AGNs. (Bottom): Galaxy infraredemission is spatially extended, and can be explained bya normal starburst.
References[1] Imanishi, M., et al.: 2007, ApJS, 171, 72.
[2] Imanishi, M., et al.: 2010, ApJ, 721, 1233.
[3] Thompson, T. A., et al.: 2005, ApJ, 630, 167.
[4] Soifer, B. T., et al.: 2000, AJ, 119, 509.
[5] Imanishi, M., et al.: 2011, AJ, 141, 156.

The Inner Structure of Collisionless Magnetic Reconnection
ZENITANI, Seiji(NAOJ)

Magnetic reconnection is a driving engine of solar
flares, stellar flares, and quite probably bursty eventsin high-energy astrophysical sites. The reconnection
process is driven by a small-scale “dissipation region”
surrounding the reconnection point (X-point), at whicha plasma ideal condition breaks down. Recently, kinetic
particle-in-cell (PIC) simulations have revealed that theelectron ideal condition is violated in many locations incollisionless reconnection: i.e., the nonidealness cannot
locate the dissipation region. To overcome this problem,
we have proposed an electron-frame dissipation measure
as a new marker of the dissipation region [1],(1)where γe = [1 − (ve /c)2]−1/2 is the Lorentz factor for theelectron bulk velocity and ρc is the charge density. This
stands for the nonideal energy conversion in the MHD
framework as well as the energy transfer in the moving
frame of electron’s bulk flow.
The measure gives us a new perspective to understandthe structure of magnetic reconnection. Figure 1 showsmagnetic field lines and key physical quantities in adimensional PIC simulation with antiparallel
symmetric fields [2]. Kinetic reconnection exhibits ahighly-modulated field-line structure due to Hall effects.
One can recognize a well-known quadruple pattern of theout-of-plane magnetic field By in the rear panel. In such acomplicated geometry, the previous measure (the electron
frozen-in) falsely detects an elongated nondissipative
region. In contrast, our new measure De successfully
distinguishes a compact and narrow dissipation region
around the X-point (the central red region in the front
panel). Series of PIC simulations suggest that the size ofthe dissipation region is controlled by electron physics.
The dissipation region is typically ~O(1)deloc thick and~O(10)deloc long, where deloc is a local electron inertial
length. More work is necessary for better prediction. We
have also discussed structures surrounding the dissipation
region, such as a narrow fast electron jet and a shock-likejet front. Our understanding is summarized in a unified
picture in Ref. [2].
It is important to verify the new theory in the realworld. Efforts are in progress to probe the dissipation
region by laboratory experiments or by satellite
observations in the terrestrial magnetosphere. HopefullyNASA’s upcoming magnetospheric multiscale (MMS)
mission [3] will observe reconnection sites at electronscale spatial and temporal resolutions after 2014. We
hope that MMS will find an unambiguous evidence forthe dissipation region.

Figure 1: Magnetic field lines, the dissipation measure De (Eq. 1),
and the out-of-plane magnetic field By from run 1A in
Ref. [2].

References[1] Zenitani, S., et al.: 2011, Phys. Rev. Lett., 106, 195003.
[2] Zenitani, S., et al.: 2011, Phys. Plasmas, 18, 122108.
[3] http://mms.gsfc.nasa.gov/.

I Scientific Highlights

007

Clustered Star Formation in Magnetic Clouds:
Properties of Dense Cores Formed in Outflow-Driven Turbulence
NAKAMURA, Fumitaka

					(NAOJ)		

Millimeter and submillimeter observations of dense
cores in nearby parsec-scale cluster-forming clumps haveshown that the core mass function (CMF) resembles thestellar initial mass function (IMF). This suggests thatthe observed dense cores may be the direct progenitorsof individual stars and the bulk of the stellar IMF may
be at least partly determined by cloud fragmentation in
the parsec-scale dense clumps. Thus, understanding theformation process of dense cores is a key step towards afull understanding of how stars form.
In this study, we investigate the physical propertiesof dense cores formed in turbulent, magnetized, parsecscale clumps of molecular clouds, using three-dimensional
numerical simulations that include protostellar outflow
feedback. In a cluster-forming clump, protostellar outflow feedback can play an important role in turbulence
regeneration. In our previous studies, we demonstrated
that protostellar outflows can resupply the supersonicturbulence, keeping the clumps near a quasi-virial
equilibrium state for a relatively long time [1,2].
Figure 1 compares the column density distributions
along the y-axis for the three models with different initial
magnetic field strengths, at a stage when the star formation
efficiency has reached 16 %. Figure 1 indicates that the
global density distribution depends on the initial magnetic
field strength. In the presence of a moderatelystrong
magnetic field, the cloud material condenses preferentiallyalong the magnetic field lines into a large-scale filamentary
structure that is nearly perpendicular to the initial magnetic
field direction. The dense cores are distributed primarily
along the main filament.
Then, we identified dense cores using the CLUMPFIND
algorithm and found the following.
1. Dense cores do not follow Larson’s linewidth-size
relation. We find that the velocity dispersions of dense
cores show little correlation with core radius, irrespectiveof the strength of the magnetic field and outflow feedback.
In the absence of a magnetic field, the majority of thecores have supersonic velocity dispersions, whereas in thepresence of a moderately-strong magnetic field, the cores
tend to be subsonic or at most transonic.
2. We find that most of the cores are out of virial
equilibrium, with the external pressure due to ambient
turbulence dominating the self-gravity. The coreformation and evolution is largely controlled by the
dynamical compression due to outflow-driven turbulence.
Such a situation is contrast to the strongly-magnetized(magnetically subcritical) case, where the self-gravity plays
a more important role in the core dynamics, particularly for008

I Scientific Highlights

LI, Zhi-Yun(University of Virginia)

Figure 1: Column density snapshots on the x-z plane for (a) modelN1 (t = 4.6tff,c ~ 0.9 Myr), (b) W1 (t = 6.5tff,c ~ 1.2 Myr),and (c) S1 (t = 7.4tff,c ~ 1.4 Myr) at the stage when 16% of the total mass has been converted into stars. The
positions of the formed stars are overlaid with the dots.
The units of length are the central Jeans length LJ = (�c2s/Gρ0)1/2 ~– 0.17(T/20K)1/2(nH2,0/2.69 × 104 cm−3)−1/2 pc.

massive cores.
3. Even an initially-weak magnetic field can retard
star formation significantly, because the field is amplified
by supersonic turbulence to an equipartition strength. In
such an initially weak field, the distorted field component
dominates the uniform one. In contrast, for a moderatelystrong field, the uniform component remains dominant.
Such a difference in the magnetic structure can be observedin simulated polarization maps of dust thermal emission.
Recent polarization measurements show that the fieldlines in nearby cluster-forming clumps are spatially wellordered, indicative of a moderately-strong, dynamicallyimportant, field.
Our simulations indicate that in clustered star formation
moderately strong magnetic field is needed to reproduce
the physical properties of dense cores [3].
References[1] Nakamura, F., Li, Z.-Y.: 2007, ApJ, 662, 395.
[2] Wang, P., Li, Z.-Y., Abel, T., Nakamura, F.: 2010, ApJ, 709, 27.
[3] Nakamura, F., Li, Z.-Y.: 2011, ApJ, 740, 36.

Molecular Outflows From the Protocluster, Serpens SouthNAKAMURA, Fumitaka1, SUGITANI, Koji2, SHIMAJIRI, Yoshito1, TSUKAGOSHI, Takashi3
HIGUCHI, Aya1, NISHIYAMA, Shogo4, KAWABE, Ryohei1, TAKAMI, Michiriro5
KARR, Jennifer L.5, GUTERMUTH, Robert A.6, WILSON, Grant6
1: NAOJ, 2: Nagoya City University, 3: University of Tokyo, 4: Kyoto University, 5: ASIAA, 6: University of Massachusetts

Most stars form in clusters. Therefore, understanding
the formation process of star clusters is a key step
towards a full understanding of how stars form. Recent
observations have revealed that star clusters form inturbulent, magnetized, parsec-scale dense clumps ofmolecular clouds. These clumps contain masses of
10 2 – 10 3 M  , fragmenting into an assembly of coresthat collapse to produce stars. In cluster-forming
clumps, stellar feedback such as protostellar outflows,
stellar winds, and radiation rapidly start to shape thesurroundings. Because of the short separations between
forming stars and cores, these feedback mechanisms are
expected to control subsequent star formation. However,
the roles of the stellar feedback on cluster formation
remain poorly understood observationally.
In this study, we carried out molecular outflow survey
toward a young embedded cluster, Serpens South, in CO(3–2) using the ASTE 10 m telescope, and attemped toreveal the role of molecular outflows in star formationin this cluster-forming region. Serpens South is a nearby
embedded cluster, recently discovered by Guthermuth etal. (2008) using the Spitzer Space telescope.
An interesting characteristic of the cluster is its
extremely-high fraction of protostars. In the central
region, the number fraction of protostars (Class I) relative
to the YSOs detected by the Spitzer telescope (Class I/II)
reaches about 80 %. This fraction is largest among thecluster-forming regions known within the nearest 400
pc. This suggests that Serpens South is in the very earlyphase of cluster formation.
The main results are summarized as follows.
1. We found that many outflow components
concentrate in the dense part where the protocluster
resides. Most of these outflow components appear tomove away from the dense part.
2. We estimated the global physical quantities of theoutflows. The total outflow mass, momentum, and energy
seem smaller than those of the Serpens Cloud Core,a nearby typical parsec-scale cluster-forming clump,
located about 3° north of Serpens South. However, thecharacteristic outflow speed appears somewhat larger
than that of the Serpens Cloud Core. This may imply that
the YSO populations of Serpens South are younger thanthose of the Serpens Cloud Core.
3. The outflow energy injection rate is likely to be
somewhat larger than the energy dissipation rate of
the supersonic turbulence, suggesting that the outflow

feedback can significantly contribute to the generation of
the supersonic turbulence in the dense clump. Assuming
the median stellar mass of 0.5 M , the mean outflow
momentum per unit stellar mass is estimated to be about
4 km s−1, under the assumption of optically-thin gas.
4. The total outflow energy appears significantly
smaller than the global gravitational energy of the densepart where the protocluster is located. In other words, it
may be difficult to destroy the cluster-forming clump by
the current outflow activity. This may be inconsistent withthe dynamical model of cluster formation, for which theoutflow feedback due to the initial star burst is envisioned
to disperse the dense gas from the cluster-forming clump[1].

Figure 1: Molecular outflow lobes identified from CO (J = 3–2)
emission toward the Serpens South protocluster. The
blue contours represent blueshifted 12CO gas and red
contours represent redshifted 12CO gas. The blue andred contour levels go up in 6 K km s−1 step, starting from3 K km s−1. The integration ranges are −9.75 to 3.75 km
s −1 for blueshifted gas and 11.25 to 29.25 km s−1 forredshifted gas.

Reference[1] Nakamura, F., Sugitani, K., Shimajiri, Y., et al.: 2011, ApJ, 737,
56.

I Scientific Highlights009

Evidence For Cloud-Cloud Collision and Parsec-Scale Stellar Feedback
Within the L1641-N Region
NAKAMURA, Fumitaka1, MIURA, Tomoya2, KITAMURA, Yoshimi3, SHIMAJIRI, Yoshito1
KAWABE, Ryohei1, AKASHI, Toshiya4, IKEDA, Norio3, TSUKAGOSHI, Takashi5
MOMOSE, Munetake6, NISHI, Ryoichi2, LI, Zhi-Yun7
1: NAOJ, 2: Niigata University, 3: JAXA, 4: Tokyo Tech. University, 5: University of Tokyo, 6: Ibaraki University, 7: University of Virginia

Most stars form in GMCs. In GMCs, various environmental effects such as large-scale flows, supernovae, andstellar feedback from young stars (winds, radiation, andoutflows) often shape the cloud structure and dynamics,
triggering and suppressing the formation of the nextgeneration stars. Fingerprints of these environmental
effects have been found in some star-forming regions,However, the roles of the environmental effects in starformation remain poorly understood observationally.
This is partly because wide-field, high spatial and/or
spectral resolution observations, which are needed toresolve the cloud structure and kinematics in detail, arestill limited. In particular, stellar feedbacks such as winds
or outflows are often extended to parsec-scale. Widefield observations of the cloud structure and kinematics
are needed to unveil such environmental effects. At thesame time, it is necessary to resolve the cloud structure
at a scale of “dense cores”, which are the basic units
of individual star formation (≈ 0.1 pc ~ one arcmin at a
distance of 400 pc), in order to uncover a link between
individual star formation and the environmental effects.
In this study, to understand how the environmental
effects influence the internal structure and kinematics instar-forming molecular clouds, we present the results ofwide-field 12CO (J = 1–0) mapping observations toward
the L1641-N region, a nearby active star-forming region
in the Orion A giant molecular cloud complex, using
the Nobeyama 45 m radio telescope. Our data have highangular (≈ 21″) resolution, allowing us to resolve spatial
structures at a scale of 0.04 pc at a distance of 400 pc.
The main results are summarized as follows.
The 12CO (J = 1–0) velocity channel maps suggestthat the blueshifted (V LSR < 6 km s −1) and redshifted(VLSR > 7 km s−1) components are interacting with eachother. Since the two components appear to overlap
toward the dust filaments identified by the AzTEC/ASTE
observations (Shimajri et al. 2010) on the plane of thesky, the collision between the two components may haveoccurred almost along the line of sight.
We found several parsec-scale shells in the 12CO
(J = 1 – 0) data cube. Some of the shells appear to bespatially well-ordered and homocentric. The centers of
the shells are close to either the L 1641-N or V 380 Ori
cluster centers, implying that the star formation activity
in the clusters may be responsible for the formation and010

I Scientific Highlights

evolution of the shells.
The molecular gas distribution and kinematicalstructure of this region led us to the following scenario.
On the large scale of at least about 1 –10 pc, a cloudcloud collision may have occurred almost along the lineof sight in this region, contributing to the formationof several dense filaments. The cloud-cloud collision
have triggered the formation of the L1641-N cluster.
Multiple protostellar winds and outflows from the cluster
member YSOs created large expanding bubbles that canbe recognized in the 12CO and 13CO maps. Here, wecall these YSO winds as “protocluster winds”. The shellsurrounding V 380 Ori also has two different velocity
components both in the 12CO and 13CO maps. Both thecloud-cloud collision and the protocluster winds arelikely to have created the complicated cloud morphology
and kinematics.

Figure 1: CO (1–0) peak intensity map twoard the L1641-N regionin Orion A. The image indicates that several prominentshells shape the cloud structure in this region. We
propose that these shells were created by protostellar
winds, stellar feedback from forming star clusters. See[1] for more detail.

Reference[1] Nakamura, F., Miura, T., Shimajiri, Y., et al.: 2012, ApJ, 746,25.

Hα Emission from Magellanic Stream
YAGI, Masafumi, KOMIYAMA, Yutaka

				(NAOJ)			

Magellanic Stream is a long and narrow filamentof neutral hydrogen gas which extends more than 180
degree around our Galaxy. It is thought to be a stripped
gas from both of or one of the Magellanic clouds by theirinteraction. Most of the stream is observed as a neutralhydrogen gas [1], and no stars have been detected in it.
Nevertheless, Hα emission is observed from some part ofthe stream [2,3], and the ionizing mechanism has been indebate.
We can expect that an optical intermediate-dispersion
spectroscopic observation with a wide spectral coverage
would be helpful to investigate the ionization sources.
For example, as one of the hyposethes for the ionization,“shock cascade” model predicted a high Hβ/Hα ratio [4].
If we could measure the ratio from an observation, themodels would be verified. The difficulty was, however,that the previous Hα observations used Fabry-Pérot
spectrographs and the spatial information were averaged
out. The spatial resolution was about 7 arcmin at most.
The resolution is not enough for long-slit spectroscopy or
multi object spectroscopy.
Aiming for breakthrough, we observed a 50 arcmin
square region around one of the previous Hα detection inHα narrowband and R-band filter using 2kCCD camera
at the Kiso Observatory of the University of Tokyo in
September and November in 2011 [5]. The exposure timecorrected for the weather dimming was about 5 hours
in total, and the limiting surface brightness was about
24 mag per square arcseconds as 1σ. We detected threeparallel filamentary structures of Hα excess which lie ashort distance away from a previous study (Fig. 1). The
filaments are 2 arcminutes wide and 6–30 arcminutes
long with 12 arcminutes intervals. Their position overlaps
the neutral hydrogen stucture of the Magellanic Stream,
but it also overlaps a nearby structure of hydrogen gas(Fig. 2).
If the Hα comes from a part of Magellanic Stream,
it is qualitatively consistent with the shock cascade
model; the surface of an upstream cloud is stripped by
the interaction with the halo gas and then heated up by
the collision with the following cloud at the downstream.
If it is a nearby object, on the otherhand, it is difficult
to make such a long, narrow and straight ionized gas
structure. A possible explanation would be that several
Fossil Strömgren Trails [6], a traveling white dwarf left
its Strömgren sphere, were somehow created at the same
direction from us. We will try to determine the recession
velocity of the emission by spectroscopy and to answer
whether they belong to Magellanic Stream (v ~ −200 km/s)
or near by gas (v ~ −40 km/s).

YOSHIDA, Michitoshi(Hiroshima University)

Figure 1: R-band subtracted N657 (Hα) image. Around the center,three parallel filamentary structures running from the top
right to the bottom left direction are recognized.

Figure 2: Hα emission overlaied on the contour of neutralhydrogen gas [7,8]. The left is the gas of Magellanic
Stream, and the right is nearby Galactic gas.

References[1] Mathewson, D. S., et al.: 1974, ApJ, 190, 291.
[2] Weiner, B. J., Williams, T. B.: 1996, AJ, 111, 1156.
[3] Putman, M. E., et al.: 2003, ApJ, 586, 170.
[4] Bland-Hawthorn, J., et al.: 2007, ApJ, 670, L109.
[5] Yagi, M., Komiyama, Y., Yoshida, M.: 2012, ApJ, 749, L2.
[6] McCullough, P. R., Benjamin, R. A.: 2001, AJ, 122, 1500.
[7] McClure-Griffiths, N. M., et al.: 2009, ApJS, 181, 398.
[8] Kalberla, P. M. W., et al.: 2010, A&A, 512, A14.

I Scientific Highlights011

Three Classical Cepheid Variable Stars
in the Nuclear Bulge of the Milky Way
MATSUNAGA, Noriyuki, KOBAYASHI, Naoto		

KAWADU, Takahiro, NAGATA, Tetsuya(University of Tokyo)				

NISHIYAMA, Shogo, TAMURA, Motohide

				
		

(NAOJ)				

BONO, Giuseppe(Universita di Roma Tor Vergata)

The star formation history and the triggering process
for star formation of the nuclear bulge of our Galaxy
remain to be resolved. Classical Cepheid variable stars
have pulsation periods that decrease with increasing age,so it is possible to probe the star-formation history. We
have reported the presence of three classical Cepheids inthe nuclear bulge with pulsation periods of approximately
20 days [1]. No Cepheids with longer or shorter periods
were found. We infer that there was a period about 25
Myr ago, and possibly lasting until recently, in which starformation increased relative to the period of 30–70 Myrago.
We conducted a near-infrared survey for the 0°. 33 by
0.°5 area around the Galactic center [2], where no classical
Cepheids were known before. The data were taken with
the Infrared Survey Facility (IRSF) 1.4-m telescope andthe SIRIUS near-infrared camera located at the South
African Astronomical Observatory. Approximately 90
time-series images were collected in each of the J, H andKS bands during eight years between 2001 and 2008, andthree classical Cepheids were discovered on the basis of
their light curves (Fig. 1).
All of our classical Cepheids have periods close to
20 days, suggesting their ages of 25 ± 5 Myr. We canestimate the star-formation rate at about 25 Myr ago byassuming an initial mass function and the lifetime spentby the Cepheid inside the instability strip, and find that
−1 in the entire
the star-formation rate was 0.075+0.15−0.05 M yr
nuclear bulge 20–30 Myr ago. On the other hand, theabsence of shorter-period Cepheids leads to 0.02 M yr−1
as a 1σ upper limit on the star-formation rate for 30–70
Myr ago. Thus we find the change in the star-formation
rate between 20 and 70 Myr ago in the nuclear bulge.
A recent investigation suggested that the starformation rate was low a few tens of millions of years
ago and then increased to a peak at about 0.1 Myr ago,followed by a decline in very recent times [3]. However,
the tracers used give only a rough timescale for therange 1–100 Myr ago. Our estimates have much higher
time resolution for the 20–70 Myr range and indicate anincrease in star-formation rate within this period.
It is of interest to consider how and why such time
variations in star formation occurred. Episodic starformation has been suggested in some of the so-called

012

I Scientific Highlights(Kyoto University)

NAGAYAMA, Takahiro(Nagoya University)

FEAST, Michael W.

(University of Cape Town)

pseudobulges, the central regions of a few barred spiralgalaxies, possibly growing with bar-driven gas inflow.
Our result suggests that episodic star formation on ashort timescale of about 25 Myr occurred in the nuclear
bulge, which some authors claim to be a pseudobulge [4].
The timescale is comparable with that of the cyclic gas
accumulation predicted for the central part of the Milky
Way [5].

Figure 1: The classical Cepheids discovered in the Nuclear Bulge.
The near-infrared false-color image (left), close-ups
around the Cepheids (middle), and the H-band light
curves are shown. The positions of the Cepheids areshown by blue circles.

References[1] Matsunaga, N., et al.: 2011, Nature, 477, 188.
[2] Matsunaga, N., et al.: 2009, MNRAS, 399, 1709.
[3] Yusef-Zadeh, F., et al.: 2009, ApJ, 702, 178.
[4] Binney, J., et al.: 2009, IAUS, 254, 145.
[5] Stark, A. A., et al.: 2004, ApJ, 614, L41.

Near-Infrared Imaging Polarimetry toward Serpens South:
Revealing the Importance of the Magnetic Field
SUGITANI, Koji

(Nagoya City University)

NAKAMURA, Fumitaka, TAMURA, Motohide, NISHIYAMA, Shogo, KANDORI, Ryo, KAWABE, Ryohei(NAOJ)				

WATANABE, Makoto(Hokkaido University) 		

NAGATA, Tetsuya

NAGAYAMA, Takahiro, SATO, Shuji(Nagoya University)

GUTERMUTH, Robert A., WILSON, Grant W.

(Kyoto University) 			

It is now widely accepted that stars form predominantly within clusters inside dense clumps
of molecular clouds (MCs) that are turbulent andmagnetized. However, how clusters form in such dense
clumps remains poorly understood. Recent numericalsimulations suggest that a moderately strong magnetic
field (MF) is needed to impede star formation in MCs
for the simulated star formation rates to match observed
values (e.g., [1]). In contrast, weak MF (a few μG) is
claimed in MCs where turbulent compression largely
controls the structural formation of MCs on scales ofa few to several parsecs [2]. In the later case, the MFs
associated with cluster-forming clumps are expected tobe distorted significantly by supersonic turbulent flows.
To characterize the MF structure of cluster-forming
clumps, it is important to uncover the global MF
structures associated with cluster-forming clumps. So
we carried out near-infrared polarization observationsof filamentary clouds in the Serpens South embeddedcluster [3], which is believed to be in a very early stage ofcluster formation. Although some small deviation is seen,
the MF is roughly perpendicular to the main filament
elongated toward the NW and SE direction (Fig. 1, here
the polarization vectors are assumed to be the directionsof the local MF). This ordered MF configuration suggeststhat the MF is strong enough to regulate the entire
structure of the main filament and, therefore, that theformation of the main filament has proceeded under the
influence of the MF.
In contrast to the main filament, sub-filaments thatconverge on the central part of the cluster or intersect
the main filament, appears to be nearly parallel to the
MF direction. They could be outflows from the cluster or
inflow toward the main filament. Recent CO observations
toward Serpens South suggest that CO outflow lobes are
anti-correlated with the sub-filaments [4], reinforcing the
inflow view of the sub-filaments.
In addition, the global MF appears to be curved in
the southern part of the observed region. This curved
morphology suggests that the global MF is distorted bygravitational contraction along the main filament toward(University of Massachusetts)

the northern part, where the mass of the cloud seems to
be mostly concentrated. Using the Chandrasekhar-Fermi
method, the MF strength is roughly estimated to be a few
×100 μG in two zones along the main filament.
All the above results show that the MF appears tosignificantly influence the dynamics of the Serpens Southcloud. This does not appear to support the weak MF
models of MC evolution/cluster formation, at least not for
the Serpens South cloud

Figure 1: H-band polarization vector map toward Serpens Southfor point sources, superposed on the 1.1-mm dustcontinuum image. YSOs are indicated by red (class 0/I)
and blue (class II) open circles.

References[1] Li, Z.-Y., Nakamura, F.: 2006, ApJ, 640, L187.
[2] Padoan, P., et al.: 2001, ApJ, 553, 227.
[3] Sugitani, K., et al.: 2011, ApJ, 734, 63.
[4] Nakamura, F., et al.: 2011, ApJ, 737, 56.

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013

Oscillation Phenomena in the Disk
around the Massive Black Hole Sagittarius A*						OYAMA, Tomoaki

MIYOSHI, Makoto(NAOJ)			

(NAOJ)			

I Scientific Highlights(SHAO)

TAKAHASHI, Rohta

The existence of black holes has been definitely
established while zooming-in the relativistic region is stillin difficulty though promising in near future. Sagittarius
A* (Sgr A*), the most convincing massive black holeat the Galactic center, shows short time flares withquasiperiodic oscillations (QPO) with P = 17, 22, & 33
min in near-infrared and X-ray regions originated fromnear the central black hole.
Here we report the detection of radio QPOs withstructure changes using the Very Long Baseline Array(VLBA) at 43 GHz [1]. We found conspicuous patternedchanges of the structure with P = 16.8, 22.2, 31.4, &56.4
min, roughly in a 3 : 4 : 6 : 10 ratio. The first two periods
show a rotating one-arm structure, while the P = 31.4 minshows a rotating 3-arm structure, as if viewed edgeon. At
the central 50 µas the P = 56.4 min period shows a double
amplitude variation of those in its surroundings. Spatial
distributions of the oscillation periods indicate that thedisk of Sgr A* is presumably almost edge-on, rotatingaround an axis with PA = −10°. The observed VLBI
images of Sgr A* remain several features of the blackhole accretion disk of Sgr A* in spite of being obscured
and broadened by scattering of surrounding plasma.
If the QPOs originate in a strong gravity field where
the relativistic effect plays an important role, the periods
of QPOs should depend on the mass and the spin of a
massive black hole. Recent theories of disk seismology
predict that peak frequencies of QPOs can be scaled bya mass of central black holes as an analogy to QPOs inblack hole X-ray binaries (BXB). For example, in GRO
J1655-40, a peak frequency of high frequency QPOs
is about 3 × 10 2(6.0 – 6.6 M  / M BH) Hz (where M  is asolar mass), with the result that a corresponding peakfrequency using the mass of Sgr A* derived from theorbital motions of surrounding stars (3.6 ± 0.3 × 106 M)is about 5.1 × 10 −4 Hz (P = 32 min), which is one of
our findings. Detailed analysis with the obtained four
QPO periods and wave-warp resonant oscillation model
predicts the spin of Sgr A* to be 0.44 ± 0.08 and the blackhole mass to be (4.2 ± 0.4) × 106 M   [2].

014SHEN, Zhi-Qiang(TNCT)			

KATO, Yoshiaki(NAOJ)

Figure 1: The slit-modulation-imaging (SMI) [3] maps with the 4
periods P = 16.8(a), 22.2(b), 31.4(c), and 56.4 min (d).
The 8 maps show the images in phase frame series withrespective periods. The white filled circles mark theintensity peak position in each map. In P = 31.4 & 56.4
min, second peaks are also marked with circles. Total
amplitudes of respective periods are 22 mJy (P = 16.8min), 24 mJy (P = 22.2 min), 24 mJy (P = 31.4 min),and 20 mJy (P = 56.4 min), which obtained by Fouriertransform.

References[1] Miyoshi, M., Shen, Z.-Q., Oyama, T., Takahashi, R., Kato, Y.:
2011, PASJ, 63, 1093-1116.
[2] Kato, Y., Miyoshi, M., Takahashi, R., Negoro, H., Matsumoto,R.: 2010, MNRAS, 402, L74-L78.
[3] Miyoshi, M.: 2008, PASJ, 60, 1371-1386.

Observational Identification of First Cores:
Non-LTE Radiative Transfer Simulation
TOMISAKA, Kohji, TOMIDA, Kengo(NAOJ)

A first core is a first hydrostatic object formed in thecourse of dynamical contraction of a molecular cloudcore. Since the inflow pattern changes drastically before
and after the first core formation, it is regarded as amilestone in the star formation process. Although the firstcore was predicted by Larson in 1969 [1], this has notbeen confirmed by observation yet. In order to identify
the first core from a mapping observation, the features
expected for the first core are studied for CS rotationtransitions at radio wavelengths [2]. The non-LTE
radiation transfer is calculated for the results of radiation
magnetohydrodynamical simulations of the contractionof the magnetized molecular cloud core in rotation [3].
Figure 1 indicates the structure at the age of τ = 6.45 ×
102 yr after the first core formation.

Figure 1: Density and velocity (left) and temperature (right)
distributions. This 140-AU scale map shows that a firstcore warms the surrounding gas and an outflow is ejectedvertically by the effect of rotation and magnetic field.
Inflowing gas is essentially isothermal with a temperatureof T  10 K, while the first core has higher temperature.

We use the Monte-Carlo method to solve the nonLTE radiation transfer in a nested grid hierarchy.
Balance equation between radiative excitaion, induced
emission, spontaneous deexcitaion, collisional excitationand deexcitation is solved, coupled with the radiationtransfer equation. Denoting the number density of the J
level (energy level E(J)) as nJ , we can write the balance
equation as nJ ∑ J' ≠ J RJJ' = ∑ J' ≠ J nJ' RJ'J (J = 0, 1, ···,Jmax), where RJJ' represents the transition probability fromJ to J'
aswhere AJJ' and BJJ' represent Einstein’s coefficients, theformer being the coefficient for spontaneous emission
and the latter the coefficient for absorption (J < J' ) and
induced emission (J > J'). CJJ' is the collisional transition
rate from J to J' for collisions with H2 molecules whose
density is denoted by n. The average intensity of radiation

with a frequency of ν = [E(J') − E(J)]/h is written as,
where h is the Plank constant.
In the first core phase, an outflow arises from thevicinity of the first core due to the twisted magnetic field
amplified by the rotation motion of the contracting gas
disk.
The disk and outflow system has several characteristic
observational features (Fig. 2): (i) relatively opaque lines
indicate asymmetry in the emission lines in which theblue side is stronger than the red side (an infall signatureof the envelope); (ii) in the edge-on view, the disk has
a signature of simultaneous rotation and infall, i.e., theintegrated intensity of the approaching side is brighter
than that of the receding side and the gradient in theintensity-weighted velocity is larger in the approachingside; (iii) the observed outflow indicates rotation aroundthe rotation axis. The size of the outflow gives theapproximate age after the first core is formed, since theoutflow is not expected for the earlier runaway isothermal
collapse phase.
The reason why the mirror symmetry is broken in
the rotating infall disk is understood as follows. Thisassymmetry arises due to the self-absorption. Since thetemperature decreases outwardly, the emission fromthe portion near the tangential point is absorbed byforeground rotating inflow gas. In this configuration,
velocity difference between gases which contributeemission and absorption is larger for approating siderather than receding side of rotation.

Figure 2: Expected distribution of the integrated intensity of the
CS J = 2–1 (left) and J = 7–6 (right) emissions. The
integrated intensities are shown with false color andintensityweighted mean velocity (first moment) is shownin white contour lines. This shows the edge-on view.
References[1] Larson, R. B.: 1969, MNRAS, 145, 271.
[2] Tomisaka, K., Tomida, K.: 2011, PASJ, 63, 1151.
[3] Tomida, K., Tomisaka, K., Matsumoto, T., Ohsuga, K.,
Machida, M. N., Saigo, K.: 2010, ApJ, 714, L58.

I Scientific Highlights

015

A discovery of Red Star Forming Galaxies in Groups at z = 0.4
		

KOYAMA, Yusei

KODAMA, Tadayuki, NAKATA, Fumiaki(NAOJ / University of Tokyo)			

(NAOJ)SHIMASAKU, Kazuhiro, OKAMURA, Sadanori(University of Tokyo)

In the present-day Universe, galaxy properties arestrongly correlated with the environment where thegalaxies reside. For example, high-density environment
such as clusters are dominated by red ellipticals andS0s, while general field environments are dominatedby blue star-forming spirals or irregulars [1]. In orderto study the origin of this environmental dependence ofgalaxy properties, the most direct and useful approachis to observe distant clusters of galaxies, because distantclusters are the young stage of present-day clusters
where we can see active assembly of galaxies in thepast Universe. In particular, wide-field observationsof distant clusters enable us to unveil filamentarylarge-scale structures around the clusters [2], and toinvestigate the galaxy properties in such intermediatedensity environment. Some previous studies with Subaru
Telescope have shown that galaxy colours are strongly
changing from blue to red in such cluster surrounding
environment, and suggested that the cluster surrounding
structures are key for understanding galaxy evolution(but not yet fully cultivated) [3,4,5]. Therefore, in orderto study galaxy activities in such key environment morein detail, we heve carried out an Hα-based star-forming
galaxy survey of the CL0939+4713 cluster (Abell 851) at
z = 0.41 [6].
The Abell 851 cluster was studied with the Prime
Focus Camera on Subaru (Suprime-Cam) [3], anda huge structure over ~ 10 Mpc has been identified
around the cluster. Fortunately, the Hα line (rest-frame
6563 Å) from this cluster can be neatly captured by thenarrowband filter NB921 (λ c =9180 Å) on SuprimeCam. Combining the available broad-band data (BVRIz'),
we have identified more than 400 Hα emitting galaxies
with star formation rates of >0.3 M / yr along the largescale structure (Fig. 1). An intriguing finding from thissurvey is the colours of the Hα emitters: the majorityof them show blue colours reflecting their young stellar
population (as expected), while we find a non-negligible
fraction of them show red colours with B – I > 2. Such
red Hα emitters are expected to be dust-reddened star
forming galaxies (dusty starbursts), and they are probably
in the transitional stage from blue star forming population
to red quiescent one. We find that the red Hα emittersare very rare in the cluster central region (within ~1 Mpc
from the cluster centre), while as can be seen in Fig. 1
they are most strongly concentrated in group-scale
environment which are located far from the cluster (wefind that ~30 % of star forming galaxies in groups show

016

I Scientific Highlights

red colours). This result shows that dusty starbursts are
triggered in the group-scale environment (rather thanhighest-density cluster core), and suggests that this strong
activity is related to the acceleration of galaxy evolution
in distant group environment. We finally stress that thisstudy provides us with an important clue on cluster
galaxy evolution, and this is a great achievement ofSubaru Telescope with wide-field of view.

Figure 1: The large-scale structure around the Abell 851 clusterat z = 0.41, revealed by Suprime-Cam imaging. The
grey dots show the photo-z selected members and thecontours are drawn based on the surface number densityof member galaxies. The red and blue squares indicate
the red and blue Hα emitters, respectively. It is clear thatthe “red emitters” are preferentially found in the groupscale environment located far away from the cluster
core.

References[1] Dressler, A.: 1980, ApJ, 236, 351.
[2] Kodama, T., et al.: 2005, PASJ, 57, 309.
[3] Kodama, T., et al.: 2001, ApJ, 562, 9.
[4] Tanaka, M., et al.: 2005, MNRAS, 362, 268.
[5] Koyama, Y., et al.: 2008, MNRAS, 391, 1758.
[6] Koyama, Y., et al.: 2011, ApJ, 734, 66.

Subaru Measurements of Spin-Orbit Alignment Angles of Exoplanets						

NARITA, NorioHIRANO, Teruyuki(NAOJ)

SATO, Bun’ei(MIT / University of Tokyo)

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

Since the discovery of the first exoplanet in 1995,
scientists have identified more than 700 exoplanets,
planets outside of our solar system, nearly all of which
are giant planets. Most of these giant exoplanets closely
orbit their host stars, unlike our solar system’s giant
planets, like Jupiter, that orbit the Sun from a distance.
Accepted theories propose that these giant planets
originally formed from abundant planet-forming materials
far from their host stars and then migrated to their current
close locations. Different migration processes have beensuggested to explain close-in giant exoplanets.
Disk-planet interaction models of migration focus
on interactions between the planet and its protoplanetarydisk, the disk from which it originally formed. Sometimes
these interactions between the protoplanetary disk andthe forming planet result in forces that make the planet
fall toward the central star. This model predicts that the
spin axis of the star and the orbital axis of the planet
will be in alignment with each other. Planet-planet
interaction models of migration have focused on mutual
scatterings among giant planets. Migration can occur
from planet scattering, when multiple planets scatter
during the creation of two or more giant planets within
the protoplanetary disk. While some of the planets scatterfrom the system, the innermost one may establish a final
orbit very close to the central star. Another planet-planet
interaction scenario, Kozai migration, postulates that thelong-term gravitational interaction between an inner giant
planet and another celestial object such as a companion
star or an outer giant planet over time may alter theplanet’s orbit, moving an inner planet closer to the central
star. Few-body interactions, including planetplanet
scattering and Kozai migration, could produce an inclined
orbit between the planet and the stellar axis.
Overall, the inclination of the orbital axes of closein planets relative to the host stars’ spin axes emerges asa very important observational basis for supporting or
refuting migration models upon which theories of orbital
evolution center. For this reason, we have conducted
observations with the Subaru Telescope to measure the
Rossiter-McLaughlin (hereafter, RM) effect of transiting
planetary systems so as to investigate these inclinations.
The RM effect refers to apparent irregularities in
the radial velocity or speed of a celestial object in theobserver’s line of sight during planetary transits. Unlike
the spectral lines that are generally symmetrical inmeasures of radial velocity, those with the RM effectdeviate into an asymmetrical pattern. Such apparent(NAOJ)

variation in radial velocity during a transit reveals
the sky-projected angle between the stellar spin axis
and planetary orbital axis [1]. Subaru Telescope has
participated in previous measurements of the RM effect,
which we have investigated for over ten exoplanetarysystems. In 2011, we newly found that XO-2b has a wellaligned orbit [2], whereas XO-3b has highly inclined
orbits (Figure 1) [3].
The latest observational results about the RM effect,
including those obtained independently of the findings
reported here, suggest that about one-third of the observed
hot Jupiter systems have highly inclined planetary orbits.
Also, it has now turned out that the latest distributionof the spin-orbit alignment angles have dependences onstellar temperature and age [4,5].
We plan to extend our targets to smaller planets in the
future aiming to uncover the whole picture of planetary
migration mechanisms.

Figure 1: The Rossiter-McLaughlin effect of XO-3b taken with
the Subaru HDS (purple and blue points). Also plotted
are the Keck HIRES data (green) which cover a partial
transit.
References[1] Hirano, T., et al.: 2011, PASJ, 63, S531-S536.
[2] Narita, N., et al.: 2011, PASJ, 63, L67-L71.
[3] Hirano, T., et al.: 2011, ApJ, 742, 69.
[4] Winn, J. N., et al.: 2010, ApJ, 718, L145-L149.
[5] Triaud, A. M. D., et al.: 2011, A&A, 534, L6.

I Scientific Highlights

017

The Standard IMF in the Outskirts of M83
KODA, Jin

(Stony Brook University)

GIL DE PAZ, Armando(Universidad Complutense de Madrid)		

YAGI, Masafumi(NAOJ)IMANISHI, Masatoshi(NAOJ)			

MADORE, Barry F.

(Carnegie Institution of Washington)

The initial mass function (IMF) is of crucial importance to developing models of star formation and galaxy
evolution. Most observations are consistent with auniversal IMF [1]; however, recently, a non-universal
IMF has been inferred [2]. The IMF in low-density
environments could be truncated (or steeper) at its highmass end. Fewer high-mass stars appear to form in dwarf
and low surface brightness galaxies [3].
The Galaxy Evolution Explorer (GALEX) ultraviolet(UV) satellite has revealed tantalizing evidence for starformation far beyond the optical edge of galactic disks.
These extended UV (XUV) disks are providing a newopportunity for studying the mode of star formation in
extremely low-density, low star-forming environments.
By capitalizing on the exceedingly high sensitivity andwide field-of-view of the Suprime-Cam, we observe
the whole extension of the large XUV disk of the
nearby galaxy M83 (Figure 1). GALEX UV images are
sensitive to both O and B stars but cannot distinguishbetween them, while Subaru Hα images are sensitive
almost exclusively to O stars since only O stars produce
appreciable HII regions. Therefore, the combination ofSubaru and GALEX can determine the high-mass end of
the IMF. Suprime-Cam with the Hα filter (i.e., NA659)
detects every HII region around a single O star at the
distance of M83.
Our new observations enable the first complete
census of very young stellar clusters over the entire
XUV disk. Combining Subaru and GALEX data with astellar population synthesis model, we find that (1) the
standard, but stochastically-sampled, IMF is preferredover the truncated (or steeper) IMF, because there are low
mass stellar clusters (102–3 M) that host massive O stars,
which should not exist under the truncated IMF; that(2) the standard Salpeter IMF and a simple aging effectexplain the counts of FUV-bright and Hα-bright clusters
with masses > 103 M; and that (3) the Hα to FUV flux
ratio over the XUV disk supports the standard IMF. To
reach conclusion (2), we assumed instantaneous cluster
formation and a constant cluster formation rate over the
XUV disk.
Suprime-Cam covers a large area even outside the
XUV disk – far beyond the detection limit of the HI gas.
This permits us to statistically separate the stellar clusters
in the disk from background contamination. The new018

I Scientific Highlights

BOISSIER, Samuel(Laboratoire d’Astrophysique de Marseille)

DONOVAN MEYER, Jennifer(Stony Brook University)

THILKER, David A.

(The Johns Hopkins University)

data, model, and previous spectroscopic studies provide
overall consistent results with respect to the internal dust
extinction (AV ~ 0.1 mag) and low metallicity (~ 0.2 Z)using the dust extinction curve of the Small Magellanic
Cloud. The background subtraction and extinction
correction have been the major issues in studies of the
IMF in external galaxies. This result is published in [4].

Figure 1: Suprime-Cam coverage of the XUV disk of M83. The
background is a GALEX far-UV (FUV) image. Solidoverlapping rectangles are two Suprime-Cam pointings.
The inner (yellow) contour is roughly at the traditionaledge of the optical disk. The outer (red) counter is at an
HI surface density of 1.5 × 1020 cm−2 [5]. The Hα-brightclusters (NA659 − Rc < −1 mag) are also plotted: green
for clusters with > 103 M and cyan for the ones with <103 M.
References[1] Kroupa, P.: 2002, Science, 295, 82.
[2] Bastian, N., Covey, K. R., Meyer, M. R.: 2010, ARA&A, 48,339.
[3] Meurer, G., Wong, O. I., Kim, J. H., et al.: 2009, ApJ, 695, 765.
[4] Koda, J., Yagi, M., Boissier, S., et al.: 2012, ApJ, 749, 20.
[5] Miller, E. D., Bregman, J. N., Wakker, B. P.: 2009, ApJ, 692,470.

Photometric Observations of 107P/Wilson-Harrington
URAKAWA, Seitaro, OKUMURA, Shin-ichiro, NISHIYAMA, Kota, SAKAMOTO, TsuyoshI, TAKAHASHI, Noritsugu(Japan Spaceguard Association)

ABE, Shiunsuke(National Central University)
			

ISHIGURO, Masateru

KITAZATO, Kohei(Seoul University)		

OHTA, Kouji(Aizu University)

KAWAI, Nobuyuki(Kyoto University)		

(Tokyo Institute of Technology)

KURODA, Daisuke, SHIMIZU, Yasuhiro, NAGAYAMA, Shogo, YANAGISAWA, Kenshi(NAOJ)

		

YOSHIDA, Michitoshi

HASEGAWA, Sunao, YOSHIKAWA, Makoto(Hiroshima University)				

Introduction: Main-belt comets (MBCs) are objects
that display cometary activities in the main-belt asteroid(MBA) region [1]. The mechanism of the cometaryactivity is controversial: i.e. impact collisions or
ice sublimations. The discovery of MBCs indicatesthat objects in the outer-MBA region have enoughvolatile materials, as suggested by the Nice model [2].
Furthermore, some outer-MBAs would migrate to theorbit of near-earth objects (NEOs). A part of such volatilerich objects would impact with the Earth in the earliest
stage of the Solar System. The study of objects in whichcometary activity is shown provides keys to the origin ofEarth’s water and life.
107P/Wilson-Harrington: 107P/Wilson-Harrington(also know as 4015 Wilson-Harrington, hereafter, 107P)
was discovered accompanied by a faint cometary tailin 1949 [3]. Despite a devoted search, no cometaryactivity has been detected since the initial observation[4]. A numerical simulation mentions that there is a 65 %chance that 107P has an origin in the outer-MBAs region[5]. Thus, 107P might include much volatile material
like MBCs. Moreover, if the cometary activity of 107P
is driven by impact collisions, the collision would affectthe rotation of 107P. In that case, the lightcurve of 107P
shows the multi-periodicity. Besides, 107P is a promisingtarget by an advanced asteroid probe. Clarification of therotational states of 107P is important to design the futuresample return mission.
Results: We had conducted the photometric observationsof 107P in 2009-2010 apparition. The lightcurve had
showed a periodicity of 0.2979 day (7.15 h) and 0.0993
day (2.38 h), which has a commensurability of 3:1 (Fig.
1) [6]. We suggest the following four possibilities for theinterpretation. 1) 107P is a tumbling object with a sidereal
rotation period of 0.2979 day and a precession periodof 0.0993 day. 2-A) 107P is not a tumbler. The sidereal
rotation period is 0.2979 day. The period of 0.0993 day
represents the roughly symmetrical hexagonal shape.
2-B) 107P is not a tumbler. The sidereal rotation period
is 0.2979 day. The period of 0.0993 day comes from the(JAXA)

binary eclipse. 2-C) The observations were conducted at
the phase angle of around 50 √¯? √ £̄. Therefore, the shadeby topography would provide the period of 0.0993 day.
In that case, 107P is not a tumbler. The sidereal rotation
period is 0.1490 day (a half period of 0.2970 day).
Tumbling, binary aster oid, and the topographical effect
imply that the cometary activity of 107P results from theimpact collisions.

Figure 1: Lightcurve of 107P.

References[1] Hsieh, H. H., Jewitt, D.: 2006, Science, 312, 561.
[2] Levison, H., et al.: 2009, Nature, 460, 364.
[3] Fernandez, Y. R., et al.: 1997, Icarus, 128, 114.
[4] Ishiguro, M., et al.: 2011, ApJ, 726, 101.
[5] Bottke, W. F., et al.: 2002, Icarus, 156, 399.
[6] Urakawa, S., et al.: 2011, Icarus, 215, 17.

I Scientific Highlights

019

Images of the Extended Outer Regions of the Debris Ring around HR 4796 A*
THALMANN, Christian1, DOMINIK, Carsten1, JANSON, Markus2, BUENZLI, Esther3, WISNIEWSKI, John4
BRANDT, Timothy5, KNAPP, Gillian5, TURNER, Edwin5, MORO-MARTIN, Amaya6, SCHNEIDER, Glenn7
USUDA, Tomonori8, EGNER, Sebastian8, TERADA, Hiroshi8, TOMONO, Daigo8, TAKAMI, Hideki8
GOLOTA, Taras8, GUYON, Olivier8, HAYANO, Yutaka8, HAYASHI, Masahiko8, HAYASHI, Saeko8, ISHII, Miki8
NISHIMURA, Tetsuo8, PYO, Tae-Soo8, TAKATO, Naruhisa8, KUDO, Tomoyuki8, CARSON, Joseph9
MCELWAIN, Michael10, GRADY, Carol10, ABE, Lyu11, GOTO, Miwa12, HENNING, Thomas12, BRANDER, Wolfgang12
FELDT, Markus12, HODDAP, Klaus13, SERABYN, Eugene14, TAKAMI, Michihiro15, FUKUE, Tsubasa8
HASHIMOTO, Jun8, IYE, Masanori8, KANDORI, Ryo8, KUSAKABE, Nobuhiko8, MATSUO, Taro8MIYAMA, Syoken8, MORINO, Jun-ichi8, SUZUKI, Ryuji8, SUTO, Hirohi8, TAMURA, Motohide8
KUZUHARA, Masayuki16, TAKAHASHI, Yasuhiro16, WATANABE, Makoto17, YAMADA, Toru18
1: University of Amsterdam, 2: University of Toronto, 3: Institute for Astronomy, 4: University of Washington, 5: Princeton University, 6:
CAB-CSIC/INTA, 7: The University of Arizona, 8: NAOJ, 9: College of Charleston, 10: Goddard Space Flight Center, 11: University of Nice,
12: Max Planck Institute for Astronomy, 13: University of Hawaii, 14: Jet Propulsion Laboratory, 15: Institute of Astronomy and Astrophysics,
16: Univesity of Tokyo, 17: Hokkaido University, 18: Tohoku University

Vega-type debris disks were first identified by infrared(IR) excesses around nearby main sequence stars [1]. The
dust content of these second-generation disk systems isbelieved to be continuously replenished via collisional
breakup of remnant planetesimals [2]. Since the imagingof the β Pic system [3], nearly two dozen nearby debris
disks have been spatially resoved. The morphologicalappearance of resolved debris disks is predicted byseveral mechanisms, e.g., interactions between dust in thedisk and nearby planets [4].
We present high-contrast images of HR 4796A takenwith Subaru/HiCIAO in H-band, resolving the debris
disk in scattered light[4]. HR 4796A is a young (~8–10 Myr; [5]), nearby (72.8 ± 1.7 pc; [6]), A0V-type starfirst identified as a debris disk system from an IR excess
observed with IRAS [7]. The application of specialized
angular differential imaging methods (ADI) allows us
to trace the inner edge of the disk with high precision,and reveals a pair of “streamers” extending radiallyoutwards from the ansae. Using a simple disk model witha power-law surface brightness profile, we demonstratethat the observed streamers can be understood as part ofthe smoothly tapered outer boundary of the debris disk,
which is most visible at the ansae. Our observations
are consistent with the expected result of a narrowplanetesimal ring being ground up in a collisional .Basedon data collected at the Subaru Telescope, which isoperated by the National Astronomical Observatory ofJapan. cascade, yielding dust with a wide range of grain
sizes. Radiation forces leave large grains in the ring andpush smaller grains onto elliptical, or even hyperbolic
trajectories. We measure and characterize the disks
surface brightness profile, and confirm the previously
suspected offset of the disks center from the stars position
along the rings major axis. Furthermore, we present firstevidence for an offset along the minor axis. Such offsets* Based on data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan.

020

I Scientific Highlights

are commonly viewed as signposts for the presence of
unseen planets within a disks cavity. Our images also offer
new constraints on the presence of companions down tothe planetary mass regime (~9 MJup at 0.″5, ~3 MJup at 1″).

Figure 1: High-contrast images of the HR 4796 A debris disk.
White plussigns mark the star’s location. The saturated
central area is masked in gray. (a) Subaru HiCIAO
H-band data after reduction with simple ADI (subtractionof a median background) and median smoothing on ascale of 5 pixels (=48 mas ~1 λ/D). Orange dotted lines
mark the mean of the spider diffraction pattern. The
stretch is linear between ± 3 × 10−5 times the stellar peak
flux. (b) The same after ADI reduction with the LOCI
algorithm, using conservative settings (optimization
region area of 10,000 PSF footprints). Note the“streamers” extending radially out from the ansae(yellow arrows). Linear stretch of ± 1.5 × 10−5.
References[1] Aumann, H. H., et al.: 1984, ApJ, 278, L23.
[2] Wyatt, M. C., et al.: 2008, ARA&A, 46, 339.
[3] Smith, B. A., et al.: 1984, Science, 226, 1421.
[4] Thalmann, C., et al.: 2011, ApJ, 743, L6.
[5] Stauffer, J. R., et al.: 1995, ApJ, 454, 910.
[6] van Leeuwen, F.: 2007, A&A, 474, 653.
[7] Jura, M.: 1991, ApJ, 383, L79.

Development of the Ultra-Low Loss Mirrors for Gravitational Wave Detector
TATSUMI, Daisuke, UEDA, Akitoshi(NAOJ)

represented by Eq. (1).
(1)
Here λ is the wavelength of the laser and δ is microroughness. In our case, the wavelength is at 1064 nm andmicro-roughness is 0.75 Å, and hence the scattering (Total
Integrated Scatter) is expected to be 1 ppm. This value isconsistent with our measured one [2].
By using this system, a lot of trial mirrors are being
evaluated to obtain high reflectivity and low loss mirrors.





    




 


 

     

 


Figure 1: An experimental setup for the scatter mater.






 

At long last construction of the next generation
gravitational wave (GW) detector KAGRA has begun.
Because the detector consists of a 100Watt class highpower laser and complex optical cavities, high quality
mirrors are key items to obtain its designed performance.
Not only optical properties but also mechanical one need
to be high quality. Therefore, the mirror developments for
KAGRA detector are very complex and difficult.
Our group is in charge of the ultra low loss and highreflectivity mirror developments and of the high damage
threshold mirror for the high power laser. The research iscollaborated with the University of Tokyo, the Universityof electro-communications, and several Japanese optics
companies. Storing large number of photons in an opticalcavity is effective to improve the sensitivity of not only
GW detectors but also of general precise measurements
using laser interferometers. To realize this situation,
the cavity should have high finesse which corresponds
to a number of bounces of photons in the cavity. Highreflection mirrors are necessary for this reason. If we needvery high reflectivity of more than 99.99 %, its opticalloss becomes important. In general easy-obtainablemirrors have a untolerable loss of 100 ppm level. Because
no transmitted light is available, such cavity cannot
be used for precise measurements. Therefore, it is our
immediate target to develop mirrors which are compatible
with high reflectivity of more than 99.99 % and low lossof less than 10 ppm. At the time TAMA detector wasconstructed, it was succeeded to achieve ultra low loss of
1.5 ppm [1]. Unfortunately the optics company which wascollaborated with our group withdrew. Now we collaborate
with several companies to recover the mirror quality. Finaltarget is to break our world lowest loss record.
As the first step, a scatter meter was constructed in
TAMA experimental hall which has been used for the GW
observation experiments. Figure 1 shows an experimental
setup on a table. To obtain extremely good sensitivity,
the following efforts are undertaken: 1) a pinhole filter
is applied to obtain ideal Gaussian beam profile, 2) the
lock-in detection method is applied to obtain good signalto-noise ratio for the scattering light power measurement,
3) an acousto-optical modulator is applied to reduce thescattering noises at the modulator such as the mechanicalchopper, and 4) a low-scattering beam dumper for thetransmitted light of the objective mirror is developed.
Figure 2 shows a histogram of two dimensional scan
results for a fused silica plate which is polished witha micro-roughness of less than 0.75 Å. An averaged
scattering of 1.5 ppm was obtained. Theoretically the
relationship between micro-roughness and scattering is  





































Figure 2: A histogram for a fused silica plate. An averaged
scattering of 1.5 ppm was obtained.

References[1] Ueda, A., et al.: 1996, Opt. Rev., 3, 369.
[2] Tatsumi, D.: 2012, Talk presented at annual meeting (spring) ofJapan Astronomical Society, V249a.

I Scientific Highlights

021

Astrometry of 6.7 GHz Methanol Maser toward W3(OH)with Japanese VLBI Network
MATSUMOTO, Naoko, HONMA, Mareki(The Graduate University for Advanced Studies / NAOJ)

ISONO, Yasuko

KIMURA, Kimihiro, MATSUMOTO, Kouhei

			
			

(Osaka Prefecture University)			

DOI, Akihiro(ISAS)FUJISAWA, Kenta(Yamaguchi Univerisity)

We present the results of multi-epoch VLBI observations for 6.7 GHz methanol maser emission toward the
UC HII region of W3(OH) with Japanese VLBI Network(JVN) [1]. Based on phase-referencing VLBI astrometry,
we derived the trigonometric annual parallax to be 0.598± 0.067 mas, corresponding to a distance of 1.67 +0.21−0.17
kpc. This is the first detection of parallax for a 6.7 GHz
methanol maser source with JVN, following European
VLBI Network [2], and demonstrates that JVN/VERA
is capable of conducting VLBI astrometry for 6.7 GHz
methanol maser sources within a few kpc from the Sun.
Based on in-beam mapping of the W3(OH) methanol
maser, we also measured the internal proper motions of
its 6.7 GHz methanol maser for the first time. The internal
proper motions basically show north-south expansion
with a velocity of few km s −1 , being similar to OH
masers. The spatial distribution and the internal propermotions of 6.7 GHz methanol masers suggest a rotatingand expanding torus structure surrounding the UC HII
region.

Figure 1: Results of positional offsets variation for the maser
components of v LSR = −43.10 (1), −43.80 (2), −45.91 (3a),−45.20 (3b), and −45.60 (3c) km s−1 after subtracting
the best-fit proper motions. The first day corresponds to
New Year’s day 2008.

022

I Scientific Highlights

UJIHARA, Hideki(Nagoya University)(NICT)SAWADA-SATOH, Satoko(NAOJ)

UENO, Yuji
(NAOJ)

Figure 2: Internal proper motion for 6.7 GHz methanol maser
components toward W3(OH). Color-codes represent the
LSR velocity. The colored vectors show the directions
and amplitudes of the relative proper motions on the sky
plane to the reference component with the −45.4 km s−1
LSR velocity. The thick black vectors show the averaged
relative proper motion at each cluster of A, B, and D-G
to the C cluster around the origin. The proper motion
vectors of 1665 MHz OH maser (gray vectors) and thecontour map of 15 GHz radio continuum emission of the
UCHII region (broken lines) are taken from Bloemhof,
Reid, and Moran [3].

References[1] Matsumoto, N., et al.: 2011, PASJ, 63, 1345.
[2] Rygl, K. L. J., et al.: 2010, A&A, 511, A2.
[3] Bloemhof, E. E., Reid, M. J., Moran, J. M.: 1992, ApJ, 397,
500.

Statistical Study of Flux Emergences on the Sun
		OTSUJI, Kenichi

KITAI, Reizaburo, ICHIMOTO, Kiyoshi, SHIBATA, Kazunari(NAOJ)				

Since Hinode has been launched in 2006, it hasrevealed new aspects of the sun. We carried out thestatistical study of flux emergences on the solar surface
observed with Hinode Solar Optical Telescope (SOT),
which clarified that the total flux of one emerging flux
region controls its spatial size and the timescale ofemergence [1].
The solar activities such as flares occur according
to the release of magnetic energy transported from theconvective zone. Emerging flux regions are where theflux tubes from the convective zone emerge onto the solar
surface, and take important role in the studies on the solar
activities like flares, coronal mass ejections and theireffects on the earth.
The result of this study showed the power-law relation
between the total flux and the mean flux growth rate of
emerging flux regions. This implies that one can estimate
the final emerged flux amount of a region from its mean
flux growth rate of the initial phase, which can be used
for the space weather forecasting.
Hinode SOT observed 101 flux emergence eventsin between November 2006 and August 2010 withmagnetogram. Figure 1 shows the example of a flux
emergence event observed on December 30, 2009. From
the observed data, physical parameters of emerging flux
regions were measured with respect to the spatial size
(dmax), emerged total flux amount (Φmax) and the mean
flux growth rate (dΦ/dt). As the result, we obtained thepower-law relations as shown in Figure 2.

(Kyoto University)

Figure 1: Magnetic field of the emerging flux region observed on
December 30, 2009 by Hinode SOT. Between the large
black and white area corresponding to sunspots, the flux
emergence occurs.

(1)(2)
These results give the observational support tothe flux tube evolution and emergence model at theconvective zone. Further investigation with comparing to
the simulation for revealing more realistic picture of thesolar interior is required.

Reference[1] Otsuji, K., Kitai, R., Ichimoto, K., Shibata, K.: 2011, PASJ, 63,
1047.

Figure 2: The scatterplots of the total flux (Φmax), spatial size (d)and mean flux growth rate (dΦ/dt) of the emerging
flux regions.

I Scientific Highlights

023

Properties of Star-Forming Galaxies in a Cluster and
Its Surrounding Structure at z = 1.46
HAYASHI, Masao, KODAMA, Tadayuki, KOYAMA, Yusei, TANAKA, Ichi				

(NAOJ)					Galaxies in the local Universe have properties
dependent on environments as galaxy clusters tend to
be dominated by massive, passively evolving galaxies
with an elliptical morphology [1]. Galaxy clusters at highredshift (z) provide important clues to understanding
galaxy formation and evolution, since going back to ashigh redshift as possible enables us to approach the epoch
when galaxy clusters were formed. Indeed, recent surveys
suggest that there are a lot of active, star-forming galaxies
even in clusters or proto-clusters at z >~ 1.5 and theprominent sequence of red galaxies in color–magnitude
diagram, which is peculiar to galaxy clusters at z <~ 1,seems to be formed during z ~ 1–3 [2].
XMMXCS J2215.9-1738 cluster at z = 1.46 is one of
the most massive galaxy clusters at z > 1 [3]. We conducted
a wide-field [O II] emission line survey in and aroundthis high-z cluster with Suprime-Cam on the Subaru
Telescope, and selected 380 [O II] emitting galaxies in theregion of 32 × 23 arcmin2. Among them, 16 [O II] emittersin the central region of the cluster were confirmed bynear-infrared spectroscopy with MOIRCS on the Subaru
Telescope. Thanks to the wide-field coverage, we foundthat [O II] emitters are distributed along filamentary largescale structures around the cluster for the first time (Figure1), which are among the largest structures of star-forming
galaxies ever identified at 1.3 <~z<~ 3.0. We defined
several environments such as cluster core, outskirts,
filament, and field as shown in Figure 1, and investigatedthe environmental dependence of properties of starforming galaxies at z = 1.46.
The colour–magnitude diagram of z' – K vs. K for the[O II] emitting galaxies shows that a significantly higher
fraction of [O II] emitters with red z' – K colours is seenin the cluster core than in other environments. It seems
that the environment which hosts such red star-forming
galaxies shifts from the core region at z = 1.46 to theoutskirts of clusters at lower redshifts. The multi-colour
analysis of the red emitters indicates that these galaxies
are more like nearly passively evolving galaxies whichhost [O II] emitting AGNs, rather than dust-reddened
star-forming [O II] emitters. We also find that the cluster
has experienced high star formation activities at rates
comparable to that in the field at z = 1.46 in contrast tolower redshift clusters, and that star formation activity ingalaxy clusters on average increases with redshift up to z
= 1.46. In addition, line ratios of [N II]/Hα and [O III]/Hβ
indicate that a mass–metallicity relation exists in thecluster at z = 1.46, which is similar to that of star-forming
galaxies in the field at z ~ 2.

024

I Scientific Highlights

TADAKI, Ken-ichi(University of Tokyo)

In summary, we have found that star formation activityof galaxies at z = 1.46 is not yet strongly dependenton environments, and that even the cluster core isexperiencing high star forming activity comparable tothose in other lower-density regions [4].

Figure 1: Distribution of 380 [O II] emitters at z = 1.46 in andaround the cluster. North is up, and east is to the left.
The axes show relative coordinates from the cluster
centre. Black dots show the [O II] emitters. Cluster core,outskirts, and filament regions are defined by a dottedline circle, broken-line circle, and long-dashed lines,
respectively. The rest of the area is defined as the field.
Blue, magenta and green contours show the local densityof [O II] emitters.

References[1] Dressler, A., et al.: 1997, ApJ, 490, 577.
[2] Kodama, T., et al.: 2007, MNRAS, 377, 1717.
[3] Stanford, S. A., et al.: 2006, ApJ, 646, L13.
[4] Hayashi, M., et al.: 2011, MNRAS, 415, 2670.

Practical Method to Derive Non-Linear Response Functionsof Cameras for Scientific Imaging
HANAOKA, Yoichiro, SUZUKI, Isao, SAKURAI, Takashi(NAOJ)We developed a practical method to derive response
functions which convert the amount of incident light to
the A/D counts of cameras for scientific imaging [1].
Some cameras do show non-linear responses, and wehave to know them to carry out photometric analysis
with the data taken by such cameras. We applied thismethod for an InGaAs near-infrared camera, XEVACL-640 (XENICS), and succeeded to derive a response
function, even though it was complicated non-linear one.
In principle, such response functions can be derived fromthe output A/D counts, S, measured at various incident
light levels, I, which are accurately controlled over thewhole dynamic range. However, it is not easy to actually
do such measurements with high accuracy. Then wedeveloped a new practical method to derive non-linear
response functions. In this method, we need a mechanism
to accurately control the amount of incident light intocameras just within a limited dynamic range and at alimited number of steps (relative light level T, which
may be exposure time, transparency, etc.). A variablebrightness light source (brightness B), which supplies theincident light into cameras, is also necessary, but we do
not need to know its accurate brightness.
Figure 1(a) shows the raw results measured undersuch conditions; output A/D values, S, are measured atseveral T’s under various unknown B’s (the brightnessof the incident light, I, is written as I = BT). It seems thatwithout knowing B’s, it is difficult to derive the relation
between I and S from the results shown in Figure 1(a).
However, we can derive IdS/dI, because the relation dI= BdT based on I = BT brings dS/dT = BdS/dI, and thismeans TdS/dT = TBdS/dI = IdS/dI. The value TdS/dT canbe derived from the known values, T and S, and therefore,
without knowing B, we can derive a unique relation
between T and TdS/dT (= IdS/dI) as shown in Figure1(b). The relation seen in Figure 1(b) can be converted
to the relation between I and S through the numericalintegration. Figure 1(c) shows the derived relation
between I and S, namely the response function of thecamera. Obviously the function is non-linear. Figure 1(d)shows a close-up of the low-light level portion of Figure1(c), and we can find a complex non-linear behavior.
We are using a XEVA camera for the polarimetry of
the infrared solar light, which requires high accuracy
measurements. Compensation of the non-linearity
based on the derived function works well, and we havequantitatively high-quality observational data.

Figure 1: (a) Measured A/D counts S at various values T are
shown with plus signs. Each line represents themeasurements carried out under the same brightness Bof the light source. (b) Relation between the measured
A/D count, S, and the TdS/dT value. All the measured
points are on a unique curve, regardless of the values ofB. (c) Calculated non-linear response function between
the amount of light input, I, and the output A/D count,
S, is shown with a solid grey line. The measured points
shown in Figure 1(a) are also plotted with plus signs. (d)Enlargement of the low-I range of panel (c).

Reference[1] Hanaoka, Y., Suzuki, I., Sakurai, T.: 2011, App. Opt., 50,
2401-2407.

I Scientific Highlights

025

Substellar Objects in nearby Young Clusters (SONYC). IV.
A Census of Very Low Mass Objects in NGC 1333
SCHOLZ, Alexander(Dublin Institute for Advanced Studies)

BONAVITA, Mariangela(University of Toronto)		

MUZIC, Koraljka(University of Toronto)

JAYAWARDHANA, Ray

GEERS, Vincent C.

(University of Toronto / NAOJ)		

SONYC (Substellar Objects in Nearby Young
Clusters) is a program to investigate the frequency
and properties of young substellar objects with masses
down to a few times that of Jupiter [1]. Here we present
a census of very low mass objects in the ~1 Myr oldcluster NGC 1333. We analyze nearinfrared spectra takenwith Fiber Multi-Object Spectrograph/ Subaru for 100
candidates from our deep, widefield survey and find 10
new likely brown dwarfs with spectral types of M6 orlater. Among them, there are three with later than M9 and
one with early L spectral type, corresponding to masses
of 0.006 to 0.02 M , so far the lowest mass objects
identified in this cluster.
The combination of survey depth, spatial coverage,
and extensive spectroscopic follow-up makes NGC 1333
one of the most comprehensively surveyed clusters for
substellar objects. In total, there are now 51 objects with
spectral type M5 or later and/or effective temperature of3200 K or cooler identified in NGC 1333; 30–40 of them
are likely to be substellar. NGC 1333 harbors about half as
many brown dwarfs as stars, which is significantly morethan in other well-studied star-forming regions (Fig. 1),
thus raising the possibility of environmental differencesin the formation of substellar objects. The brown dwarfs
in NGC 1333 are spatially strongly clustered within aradius of less than 1 pc (Fig. 2), mirroring the distributionof the stars. The disk fraction in the substellar regime
is 66 %, lower than for the total population (83 %) but
comparable to the brown dwarf disk fraction in other 2–3
Myr old regions [2].

(ETH Zurich)

TAMURA, Motohide(NAOJ)

Figure 1: Star vs. brown dwarf ratios for various starforming
regions. Squares are values with 0.08–1.0 M as stellar
and 0.03–0.08 M as brown dwarfs, while circles are 0.08
–10 M as stellar and 0.02–0.08 M as brown dwarfs.

Figure 2: Spatial distribution of NGC 1333 members. Crosses are
all 137 objects with Spitzer excess and squares are allconfirmed brown dwarfs. Objects with spectroscopy forwhich we can exclude that they are substellar members
are shown with dots.

References[1] Tamura, M., et al.: 1998, Science, 282, 1095.
[2] Scholz, A., et al.: 2012, ApJ, 744, 6.

026

I Scientific Highlights

Star Formation Activity in the Galactic HII Complex S255-S257
OJHA, D. K.1, SAMAL, M. R.2, PANDEY, A. K.2, BHATT, B. C.3, GHOSH, S. K.1, SHARMA, S.2
TAMURA, M.4, MOHAN, V.5, ZINCHENKO, I.6
1: Tata Institute of Fundamental Research, India, 2: Aryabhatta Research Institute, India, 3: Indian Institute of Astrophysics, 4: NAOJ, 5: InterUniversity Centre for Astronomy and Astrophysics, India, 6: Russian Academy of Sciences

We present results on the star formation activity of an
optically obscured region containing an embedded cluster(S255-IR) and molecular gas between two evolved HII
regions, S255 and S257. We have studied the complex
using optical and near-infrared (NIR) imaging, optical
spectroscopy, and radio continuum mapping at 15 GHz,
along with Spitzer-IRAC results. We found that the main
exciting sources of the evolved HII regions S255 andS257 and the compact HII regions associated with S255IR are of O9.5–B3 V nature, consistent with previous
observations. Our NIR observations reveal 109 likely
young stellar object (YSO) candidates in an area of
about 4.9 arcmin × 4.9 arcmin centered on S255-IR,
which include 69 new YSO candidates (see Fig. 1). To
see the global star formation, we constructed the V-I/V
diagram for 51 optically identified IRAC YSOs in anarea of about 13 arcmin × 13 armin centered on S255IR. We suggest that these YSOs have an approximate
age between 0.1 and 4 Myr, indicating a non-coeval starformation. Using spectral energy distribution models, weconstrained physical properties and evolutionary statusof 31 and 16 YSO candidates outside and inside the gas
ridge, respectively. The models suggest that the sources
associated with the gas ridge are younger (mean age about
1.2 Myr) than the sources outside the gas ridge (mean age
about 2.5 Myr). The positions of the young sources inside
the gas ridge at the interface of the HII regions S255 andS257 favor a site of induced star formation (Fig. 2) [1].

Figure 1: JHKs color-composite image of the S255-IR SFR (J,blue; H, green; and Ks, red). Only the central 1.5 arcmin
× 1.5 arcmin is shown here. The ionizing sources of thecompact and UC HII regions S255-2a, S255-2b, andS255-2c (marked with circles) are labeled IRS3, IRS2,
and IRS1b, respectively. North is up and east is to theleft.

Reference[1] Ojha, D. K., et al.: 2011, ApJ, 738, 156.

Figure 2: Spatial distributions of YSOs identified using the NIR
CC diagram (asterisks), sources detected only in the H
and Ks bands (filled circles), and sources detected onlyin the Ks band (plus symbols), overlaid on Ks-band
image. The white dashed line shows the outer peripheryof the dust continuum emission at 870 μm. The yellow
circles are the positions of 1.2 mm continuum cores in
the gas ridge. The red dashed lines are the demarcationof the outer boundaries of the S255 and S257. The large
crosses represent the positions of the radio continuum
sources. The YSO density contours are shown by blacklines.

I Scientific Highlights

027

Scaling Law of Relativistic Sweet-Parker Type Magnetic Reconnection
TAKAHASHI, Hiroyuki, KUDOH, Takahiro

			(NAOJ)				

Magnetic reconnection is one of the most important
subjects in the studies of space, laboratory, andastrophysical plasmas. It plays an essential role in theunderstanding of energy conversion processes in highenergy plasmas that characterize astrophysical compact
objects.
While issues concerning the physical mechanisms
and properties of magnetic reconnection remain unsettled
in the relativistic regime, a few theoretical studies ofrelativistic effects have been made. Lyutikov & Uzdensky
studied relativistic Sweet.Parker type reconnection within
the framework of magnetohydrodynamics (MHD).
They found that the reconnection-driven outflow canhave an ultra-relativistic speed (Lorentz factor γ  1)
when the magnetic energy is preferentially converted tokinetic energy [1]. They concluded that the reconnection
rate would be enhanced in the relativistic regime
due to Lorentz contraction. In contrast, Lyubarsky
concluded that the outflow cannot be accelerated to a_ 1) because the magnetic energy
relativistic speed (γ ~should be converted into thermal energy [2]. The effectof the Lorentz contraction is then negligible and thereconnection rate would not be enhanced.
We performed the two-dimensional Relativistic
Resistive Magnetohydrodynamic (R2MHD) simulations
to determine the energy conversion rate of the SweetParker type magnetic reconnection in the relativistic
regime [3]. Figure 1 shows the numerical results of theR2MHD simulations. At the initial state, we give a small
perturbation around the origin. Then, the magnetic fieldlines start to reconnect around the origin. The plasma
inflowing in to the current sheet is evacuated in the ± ydirection (formation of the reconnection outflow). We cansee that the plasma is heated up inside the current sheet.
The magnetic energy is liberated in the diffusion region
by the Ohmic dissipation. Most of the magnetic energy
is converted not into the kinetic, but into the thermalenergy. Then, the enhancement of the thermal energy
density, which is larger than the rest mass energy density,
contributes to the plasma inertia due to the relativistic
effects. The increase in the plasma inertia leads to the_ 1). This indicates theslow outflow (Lorentz factor ~relativistic effects such as the Lorentz contraction on theenergy conversion rate cannot be expected.
Next, we evaluate the reconnection rate R, whichcharacterizes the energy conversion rate. We confirmedthat the reconnection rate relates with the magnetic
Reynolds number RM = 4�Lv A /η, where L, vA, and η
are the length of the current sheet, Alfvén velocity andelectric resistivity, respectively. The reconnection rate in028

I Scientific Highlights

MASADA, Youhei

MATSUMOTO, Jin(Kobe University)(Kyoto University)

the relativistic reconnection is well fitted by R = R −0.5M
as well as that in the non-relativistic plasma. Also wefound that the reconnection rate is almost independentof the initial magnetic field strength. Thus, we conclude
that the Sweet-Parker type magnetic reconnection is theslow process for the energy conversion not only in thenonrelativistic regime but also in the relativistic regime.
-0.4

1.0
=0.5

0.0

8.0

0.0

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50

40

40

40

30

30

30

20

20

20

10

10

10

50

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-10

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Figure 1: Numerical results of R2MHD simulations. Color shows
the outflow (y-direction) four velocity, gas temperature,and the current density from left to right, respectively.
Curves and arrows denote for the magnetic field lines
and the velocity fields.

References[1] Lyubarsky, Y. E.: 2005, MNRAS, 358, 113.
[2] Lyutikov, M., Uzdensky, D.: 2003, ApJ, 589, 893.
[3] Takahashi, H. R., Kudoh, T., Masada, Y., Matsumoto, J.: 2011,
ApJ, 739, L53.

Size Distribution of Main-Belt Asteroids with High Inclination				

TERAI, Tsuyoshi(NAOJ)		

Asteroids in the main-belt region between the Marsand Jupiter orbits have been fractions of the remnant
planetesimals. Main-belt asteroids (MBAs) undergo
collisions and disruption with each other. Their size
distribution is primary determined by the impact strength(critical specic energy per unit mass required to catastrophically disrupt the target) [1]. The impact strength
increases with size, and the degree of the increase affects
a slope of the size distribution in the size of observable
asteroids (larger than sub km).
In the early Solar system, MBAs' orbital eccentricities
and inclinations are pumped up via dynamical excitation
due to the planetary perturbation [2]. They cause higher
relative velocities than the present. It has been indicatedthat the size-impact strength relation depends on impact
velocity [3]. MBAs possibly have a different collisional
evolution under collisions with impact velocities muchhigher than the present mean value (~4 km sec−1).
We investigate the size distribution of high-inclination
MBAs which collide with an asteroid at high velocity( ~ 10 km sec −1). The size distribution of small MBAs
around 1 km in diameter with high inclination remains
unknown. We performed a wide-field observation forthem using Subaru telescope with Suprime-Cam on highecliptic latitude region of β ~ +25°. The archival data ofSuprime-Cam was also used. We obtained the dataset of
9.0 square-degree in total.
As the result of data reduction for moving objects,
more than 600 candidates of MBAs were detected.
Using the sample of uniform detection probability, thecumulative size distributions (CSDs) are measured fromthe two groups: one includes asteroids with inclination
lower than 15° and the other includes asteroids higher
than 15°. We found that the latter has a shallower CSD.
Furthermore, we provided continuous CSD from 0.7 km
to 50 km in diameter using the Asteroid Orbital Elements
Database (ASTORB) and Sloan Digital Sky Survey
Moving Object Catalog (SDSS MOC). CSD is generally
written as a power-law of N (> D) ∝ D−b, where D isdiameter. The obtained CSDs show b = 1.79 ± 0.05 forthe low-inclination sample and b = 1.62 ± 0.07 for thehigh-inclination sample. We conrmed that CSD of highinclination MBAs has a shallower slope than that of lowinclination MBAs [4].
This result indicates the fact that large asteroids ismore resistant to destruction under hypervelocity collisions. Massive bodies could have been more dominant
in the main belt region during the dynamical excitation
phase at the early Solar system.

ITOH, Yoichi(University of Hyogo)

Figure 1: Cumulative size distributions of main-belt asteroid
populations with inclination lower than 15° (blue)and higher than 15° (red) using the data from Asteroid
Orbital Elements Database (solid lines), Sloan Digital
Sky Survey Moving Object Catalog (open circles), andthis study (diamonds).

References[1] O'Brien, D. P., Greenberg, R.: 2003, Icarus, 164, 334.
[2] Bottke, W. F., et al.: 2005, Icarus, 179, 63.
[3] Jutzi, M., Michel, P., Benz, W., Richardson, D. C.: 2010, Icarus,
207, 54.
[4] Terai, T., Itoh, Y.: 2011, PASJ, 63, 335.

I Scientific Highlights029

Orion IRc2, Radiated by the Scattering of Emission from Source I

I Scientific Highlights(University of Tokyo)

KATAZA, Hirokazu

OKAMOTO, Yoshiko K.

(JAXA/ISAS)		

(Ibaraki University)

10
5
-6

+ +
+

After the discovery of BN and KL in the Orion
Molec- ular Cloud, following infrared observations
revealed that the KL nebula splits up into a number ofcompact “ IRc ” sources. The most luminous of these,
IRc2, was thought to be the dominant energy source forthe KL complex. Then, radio continuum point source “ I ”
was found at 1″ south of IRc2 [1,2], and many radio
observations have showed evidence of the existenceof a young stellar object (YSO) embedded in source I.
However, the infrared counterpart of source I have notdetected at any wavelength, and the relationship of source
I to IRc2 also still remains ambiguous. A direct linkage
between IRc2 and source I was revealed with a detailed
analysis of the SUBARU/COMICS mid-infrared data [3].
It also shows what IRc2 really is.
Figure 1 shows the mid-infrared images of the BN/KL
region obtained with COMICS. The 9.7m optical depth
and the 7.8 μm/12.4 μm color temperature distribution
are presented in Figure 2. For IRc2, a morphologicalcorrelation is seen between the near-infrared image [4]and the optical depth distribution, and the optical depth
peak roughly coincides with the 3.8 μm peak position,
IRc2-A [4]. The color temperature peak coincides withthe position of source I, and no dominant temperaturepeak is seen at IRc2.
The spectral energy distribution (SED) of IRc2 canbe reproduced by a two-temperature model; a 400 K
component and a 150 K component. It resembles theSED of a YSO, BN. However, it is plausible that no
dominant energy source is embedded because there is notemperature peak in IRc2. It is surprising that the shorter
wavelength emission exhibits its intensity peak at the
local absorption peak position, when the 3.8 μm emission
arises from self-luminous objects embedded in IRc2-A.
In addition, considering the polarimetric results [4], thenear-infrared emission from IRc2 is most likely to be
scattered radiation. Whereas, the distribution of the 400K
component resembles with that of near-infrared emission,and the mid-infrared polarimetric study of IRc2 shows thepossibility of the mid-infrared emission to be scattered[5]. Therefore, the mid-infrared 400 K component
emission from IRc2 is due to the same source with nearinfrared emission. The near-infrared emission from IRc2
is reproduced by the scattering of radiation from source I,
and so is the mid-infrared emission.

030

SAKO, Shigeyuki, MIYATA, Takashi(NAOJ)			

0+

HONDA, Mitsuhiko(Kanagawa University)

YAMASHITA, Takuya

Dec Offset (arcsec)

OKUMURA, Shin-ichiro(Japan Spaceguard Association)		

-8

-5
-10

--10
-12

-15
6

4

2

-20
15

10

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5

0

-5

Figure 1: Mid-infrared images of the BN/KL region. Three-color
composite image (8.7 μm(blue), 12.4 μm(green), 18.5 μm(red)) (left), 12.4 μm image (center), and the close-up
around IRc2 (right). Coordinates are centered on the BN.
Crosses show the positions of the 3.8 μm peaks [4].

Figure 2: 9.7 μm color-coded optical depth image (left) and the
7.8 μm/12.4 μm color temperature distribution image(right) of the 7.5″ × 7.5″ field around IRc2. The overlaid
contour shows the 12.4 μm surface brightness. Crosses
show the positions of the 3.8 μm peaks [4], and a plus
shows the position of source I.

References[1] Garay, G., Moran, J. M., Reid, M. J.: 1987, ApJ, 314, 535.
[2] Churchwell, E., et al.: 1987, ApJ, 321, 516.
[3] Okumura, S., et al.: 2011, PASJ, 63, 823.
[4] Dougados, C., et al.: 1993, ApJ, 406, 112.
[5] Smith, C. H., et al.: 2000, MNRAS, 312, 327.

Properties of Weak Measurements through Exact Evaluations
		

NAKAMURA, Kouji(NAOJ)		

NISHIZAWA, Atsushi

FUJIMOTO, Masa-Katsu(Kyoto University)			

Current gravitational wave (GW) detectors have“standard quantum limit” (SQL) due to the uncertainty
in quantum mechanics and GW detectors in near futureneeds to beat this SQL. So, quantum non-demolition
measurements are researched in the GW researchcommunity and some techniques have been proposed tobeat SQL. On the other hand, in quantum information,“quantum measurement theory” is developing andits experiments are carried out. Unfortunately, thisdevelopment has been almost independent of GW
researches. For this reason, we have been exploring
applicabilities of techniques in quantum information to
GW detectors.
We focused on the “weak measurement” (WM) proposed by Aharonov et al. [1] in 1988. Many experimentsof WM are recently carried out and their properties look
similar to current GW detectors. Then, we expect that
WMs are applicable to GW detectors.
In the usual “measurement” in quantum mechanics,
we treat two quantum systems which are called“system” (S) and “detector” (D). We want to measure
the observable A associated with S and D measures A
interacting with S. As a model of D, an one-dimensional
quantum system is considered, whose canonicalvariables are (q, p) ([q, p] = i, ħ = 1), and the initialstate of D is assumed to be zero-mean Gaussian. Theinteraction is given by H = gδ (t − t0) pA. The state of S
before the measurement is |Si  = ∑ k αk|ak , where {|ak }are eigenstates of A with eigenvalues {ak }. After theinteraction at t = t0, the total system is entangled. The
measurement outcome of q in D of this state becomesgak with the probability |ak |2. If we know the coupling
constant g and if we perform this measurement for many
ensemble, we obtain the expectation value Si |A|Si .
On the other hand, in WM, after the interaction between S and D, we concentrate only on the subensemble
in which the final state S is |Sf . Then, the expectation
value of q in D becomes gReAw within the accuracy ofO(g). Here, Aw is called “weak value” defined by Aw : =Sf |A|Si /Sf |Si . From this definition, when Sf |Si  ~ 0,
Aw may become large. This result is within O(g) and it
implies that the interaction between S and D should be
sufficiently weak and g should be small enough. In otherwords, when we want to measure this small g, it can bemeasured as an amplified value gReAw. This is called
the “weak value amplification” (WVA). Aharonov et
al. applied this WVA to the sequence of Stern-Gerlach
experiments. They claimed that the neutron spin can bemeasured as 100.

(NAOJ)We re-examined the scenario of WMs and concentrated only on the case of measurements of A withthe property A2 = 1. This property is satisfied in many
experimental setups including GW detectors. Then, we
have derived the exact expectation value of q of D after
the WM as(1)
through the all-order evaluation of g [2]. Here, s : =2g 2p 2 is the measurement strength and p 2 is theinitial variance of p in D. According to Eq. (1), for a
fixed s, there is an optimal overlap Sf |Si  in which theamplification of the outcome is maximal. The applicationof Eq. (1) to the sequence of Stern-Gerlach experiments
proposed by Aharonov et al. is depicted in Fig. 1.
A recent experiment suggests that Eq. (1) is also
experimentally correct [3]. Based on the understanding of
WMs which we have obtained, we are now discussing theapplicability of WMs to GW detectors.

Figure 1: The application of Eq. (1) to the experiments proposedby Aharonov et al. α → π corresponds to Sf |Si  → 0.

References[1] Aharonov, Y., Albert, D. Z., Vaidman, L.: 1988, Phys. Rev. Lett.,
60, 1351.
[2] Nakamura, K., Nishizawa, A., Fujimoto, M.-K.: 2012, Phys.
Rev. A, 85, 012113.
[3] Iinuma, M., et al.: 2011, New J. Phys., 13, 033041.

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Efficient Parallel Computation of All-Pairs N-body Acceleration
by Do Loop Folding
FUKUSHIMA, Toshio(NAOJ)

Simple Parallelization
4

4C4T

Speed-Up

3.5

4C8T

2

2C2T
2C4T
1C2T

1.5
1
0.5
0

2

4

6

8

10

12

14

16

18

log 2N
Figure 1: Size Dependence of Speed-Up Factor: Simple Parallelization.

In fact, the observed value is 1.0 for a singlecore two-thread processor (1C2T), 1.7 for a dual-core
twothread processor (2C2T), 1.2 for a dual-core fourthread processor (2C4T), 3.5 a quad-core four-thread
processor (4C4T), and 2.4 for a quad-core 8-thread
processor (4C8T), respectively. Meanwhile the ideal
value is 1.0 for 1C2T, 2.0 for 2C2T and 2C4T, and 4.0 for
4C4T and 4C8T, respectively. In order to overcome thissituation, we apply the idea of folding the outer do loop [1]to the computation of N-body acceleration [2].
Consider a do loop of the form
do j=1,L {task(j)}where we assume that the task inside the loop is another
do loop the length of which is linearly changing with theouter loop index as
do k=j+1,L {subtask(j,k)}where the sub task is of an equal computational amountindependently on the indices.
Then, we transform this double do loop such that the032

I Scientific Highlights

Folded Parallelization
5
4C8T
4C4T

4
3

2C4T
2C2T
1C2T

2
1

3
2.5

inner loops contain an equally balanced load as
do j=1,(L+1)/2 {task(j);if(L+1-j!=j){task(L+1-j)}}
As a result, we mostly recover the speed loss in thesimple parallel computation of the all-pairs Newtonian
N-body acceleration vectors as shown in Fig. 2.

Speed-Up

In the Newtonian celestial mechanics, the all-pairs
Nbody acceleration vectors are expressed in the form of
double summation as aj = ∑ Nk= 1 , k ≠ j ajk where the index
j runs 1 ≤ j ≤ N. In the ordinary serial computation, theanti-symmetric nature of the mutual accelerations, μj ajk +μk akj = 0, is used to halve the total computational amountfrom N(N− 1 ) to N(N− 1 ) / 2.
In the parallel computation, however, this property is
not always utilized. This means that the total amount ofcomputation is almost doubled. Indeed Figure 1 showsthat the speed-up factor of the simple parallelization forvarious PCs suffers this defects.

0

2

4

6

8

10

12

14

16

18

log 2N
Figure 2: Size Dependence of Speed-Up Factor: Folded Parallelization.

At a consumer PC with a quad-core 8-thread processor for sufficiently large number of N, the new program
achieves an acceleration factor of 4.5 in the single,
4.2 in the double, and 4.9 in the quadruple precisionenvironments, respectively. This is an interesting result
if considering that 4 is the theoretical value for a quadcore processor. We consider that this is due to Intel’sHyper-Threading Technology, which tries to utilize
all available computational resource. In general, thepresent formulation will be applicable to many othercomputational problems.

References[1] Ito, T., Fukushima, T.: 1997, AJ, 114, 1260.
[2] Fukushima, T.: 2011, AJ, 142, 18.

Detection of Proper Motion of the Sub-Parsec-Scale Jet in 3C 66B				

SUDOU, Hiroshi(Gifu University)		

3C 66B, a giant elliptical galaxy with a redshift (z)of 0.0213, is known as an FR I radio galaxy and it has
a prominent core–jet structure that extend to about 100
kpc. High-resolution imaging using very long baseline
interferometry (VLBI) at 5 GHz has revealed the presenceof a faint counterjet within a distance of 2 mas from thecore [1]. The intensity ratio between the jet and counterjet
was estimated to be approximately 10, indicating possible
acceleration of the jet outflow on a sub-parsec scale. In
order to search for motion of the inner jet, we carried out
multi-epoch imaging of 3C 66B using VLBA [2].
From images of 3C 66B at 8.4 GHz, we found threeknots at 0.7, 1.5, and 2.5 mas (0.3, 0.7, and 1.1 pc) fromthe core (Fig. 1). Using weighted least-squares fitting,
we estimated the proper motion of the inner three knots
during 1.3 years to be 0.21 ± 0.03, 0.36 ± 0.04, and 0.63 ±0.18 mas year−1, which corresponds to βapp= 0.30 ± 0.04,
0.49 ± 0.06, and 0.87 ± 0.24 (Fig. 2).
3C 66B showed that the apparent jet speed increases
with a distance from the core within 3 mas (1.3 pc). This
result is consistent with the fact that the sub-parsec scalecounterjet was found within a distance of 2 mas from thecore.
According to the relativistic beaming model, assumingthat the jet accelerates with a constant viewing angle of 4.9
degrees [3], the jet speed accelerates from 0.78 c to 0.91 c,

IGUCHI, Satoru(NAOJ)

corresponding to the bulk Lorentz factor Γ from 1.60 to2.46. Assuming the other interpretation, that is, a change
in the viewing angle with a constant jet velocity of 0.78 c[3], the angle varies from 4.9 to 16.2 degrees. To reveal
the kinematics and geometry of the jet in 3C 66B, further
monitoring with higher dynamic-range is required over alonger period at 8.4 GHz or higher.

Figure 2: Linear fitting of the relative position shift of the threeknots (E1, E2, and E3) at 8.4 GHz. (a) time evolutionand (b) spatial distribution. A filled lozenge means the
R.A. direction (X), and an open lozenge means the Dec.
direction (Y). Dotted lines indicate the best fit.

Figure 1: An 8.4 GHz image of 3C 66B observed at 2001.20.
Contours are drawn at 3-σ × (1, √2̄, 2, 2√2̄, ...), the 3-σlevel in this image is 0.8 mJy beam−1. The synthesized
beam is shown at the bottom-left of the image. The crossmarks indicate the fitted position of knots using delta
functionin. The Gaussian component of the core positionis also shown.

References[1] Giovannini, G., et al.: 2001, ApJ, 552, 508.
[2] Sudou, H., Iguchi, S.: 2011, AJ, 142, 49.
[3] Iguchi, S., Okuda, T., Sudou, H.: 2010, ApJ, 724, L166.

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The Millimeter Sky Transparency Imager (MiSTI)TAMURA, Yoichi*, KOHNO, Kotaro, FUKUHARA, Masayuki, KUBOI, Akihito(University of Tokyo)

KAWABE, Ryohei, EZAWA, Hajime, KAMAZAKI, Takeshi, OKADA, Norio(NAOJ)MOMOSE, Munetake, NAKAGAWA, Yuki
(Ibaraki University)

SEKIGUCHI, Tomohiko(Hokkaido University of Education)

The Millimeter Sky Transparency Imager (MiSTI)[1] is a small millimeter-wave scanning telescope witha 25-cm diameter dish operating at 183 GHz (Figure 1).
MiSTI is installed at the ASTE site, Atacama, Chile, andit measures emission from atmospheric water vapor andits fluctuations to estimate atmospheric absorption in the
millimeter to submillimeter. MiSTI observes the water
vapor distribution at a spatial resolution of 0.5°, and it
is sensitive enough to detect an excess path length of ≥0.05 mm for an integration time of 1 s. By comparing the
MiSTI measurements with those by a 220 GHz tipper,
we validate that the 183 GHz measurements of MiSTI
are correct, down to the level of any residual systematic
errors in the 220 GHz measurements.
Since 2008, MiSTI has provided real-time (every
1 hr) monitoring of the all-sky opacity distribution(Figure 2) and atmospheric transmission curves in the(sub)millimeter through the internet, allowing to know
the (sub)millimeter sky conditions in Atacama.
The 183 GHz monitor is available at
http://www2.nao.ac.jp/~misti/opacity.html.

VILA-VILARÓ, Baltasar(Joint ALMA Observatory)

Figure 1: (left) A picture of the Millimeter Sky Transparent
Imager (MiSTI) installed at the ASTE site. (right)
Schematic drawing of MiSTI. The membrane and its
support structures are not shown. The positions of theazimuth and elevation axes are noted by “AZ” and “EL”,
respectively.

Figure 2: An example of the all-sky opacity image taken withMiSTI on 2010 July 1. (a) All-sky opacity map at 183
GHz in the fish-eye lens view. The sky hemisphere isorthographically projected to the plane of the paper.
The north is top and the east is left. The solid and dotted
circles indicate the horizon (El = 0°), El = 20, 40, 60,
and 80°. (b) The fluctuations of the all-sky opacity map,δτ (Az, El).

Reference[1] Tamura, Y., Kawabe, R., Kohno, K., et al.: 2011, PASJ, 63, 347.

* The author is at NAOJ when the paper [1] was submitted.

034

I Scientific Highlights

SDSS J1334+3315: A Resolved Lensed Quasar with Separation 0.″8
RUSU, Cristian E.1, OGURI, Masamune2,3, INADA, Naohisa4, KAYO, Issha5, IYE, Masanori1,3,6
HAYANO, Yutaka3, OYA, Shin3, HATTORI, Masayuki3, SAITO, Yoshihiko7, ITO, Meguru8, MINOWA, Yosuke3
PYO, Tae-Soo3, TERADA, Hiroshi3, TAKAMI, Hideki3, WATANABE, Makoto9
1: University of Tokyo, 2: IPMU, 3: NAOJ, 4: Nara National College of Technology, 5: Toho University, 6: The Graduate University for
Advanced Studies, 7: Tokyo Institute of Technology, 8: Victoria University, 9: Hokkaido University

We have observed the newly discovered SDSS Quasar
Lens Search (SQLS) [1,2,3,4,5,6] gravitationally lensed
quasar candidate pair SDSS J1334+3315 in the J, H andK' bands, using the Subaru Telescope adaptive optics
system with laser guide star (LGSAO188) [7,8]. The
quasar pair has a redshift of z = 2.426, and a separationof 0 ″. 833. We were successful in achieving a clear
detection of the lensing galaxy located in between thetwo quasars, thus proving that this is one gravitationallylensed quasar. In Figure 1, we show the improvement
obtained in resolution due to the use of AO. We estimate
the redshift of the lensing galaxy to be 0.557 based on
absorption lines in the quasar spectra as well as the colorof the galaxy. Our gravitational lens mass modelingwith improved astrometry implies that a nearby brightgalaxy ~ 4″ apart from the lensing galaxy is likely toaffect the lens potential (Figure 2). The bright nearby
galaxy is clearly revealed to be a spiral in the LGSAO188
observations.
This is the first in a campaign of Subaru Telescope
adaptive optics observations of the SQLS lensed quasars,
and demonstrates the usefulness of the LGSAO188 imaging for studying small-separation strong lens systems.

Figure 1: J, H, K′ band SDSS J1334+3315 imaged without (upper
left) and with adaptive optics (upper right). The lower
panel, enlarged five times, shows for the first time theresolved lensing galaxy located in between the two
quasar images.

References[1] Oguri, M., et al.: 2006, AJ, 132, 999.
[2] Oguri, M., et al.: 2008, AJ, 135, 512.
[3] Oguri, M., et al.: 2012, AJ, 143, 120.
[4] Inada, M., et al.: 2008, AJ, 135, 496.
[5] Inada, M., et al.: 2010, AJ, 140, 403.
[6] Inada, M., et al.: 2012, AJ, 143, 119.
[7] Hayano, Y., et al.: 2010, SPIE, 7736, 21.
[8] Minowa, Y., et al.: 2010, SPIE, 7736, 122.

Figure 2: Best-fit χ 2 for the mass model, as a function of theposition angle of the singular isothermal sphere withshear (SIS+γ) model (or alternatively, singular isothermal
ellipsoid). The horizontal line indicates the 1σ range ofthe measured position angle of the lensing galaxy G. The
vertical dotted lines show directions of the external shear
corresponding to the location of nearby galaxies G1 (thebright spiral) and G2, strongly suggesting the influenceof G1.

I Scientific Highlights

035

Completing the Census of Lyα Emitters at the Reionization EpochKASHIKAWA, Nobunari1,2, SHIMASAKU, Kazuhiro3, MATSUDA, Yuichi4, EGAMI, Eiichi5, JIANG, Linhua5
NAGAO, Tohru6, OUCHI, Masami7, MALKAN, Matthew A.8, HATTORI, Takashi1, OTA, Kazuaki7
TANIGUCHI, Yoshiaki6, OKAMURA, Sadanori3, LY, Chun9, IYE, Masanori1, FURUSAWA, Hisanori1
SHIOYA, Yasuhiro6, SHIBUYA, Takatoshi2, ISHIZAKI, Yoshifumi2, TOSHIKAWA, Jun2
1: NAOJ, 2: The Graduate University for Advanced Studies, 3: University of Tokyo, 4: Durham University, 5: University of Arizona, 6: Ehime
University, 7: ICRR, Tokyo University, 8: University of Calfornia, 9: STScI

We carried out extended spectroscopic confirmationsof Lyα emitters (LAEs) at z = 6.5 and 5.7 in the Subaru
Deep Field. Now, the total number of spectroscopicallyconfirmed LAEs is 45 and 54 at z = 6.5 and 5.7,
respectively, and at least 81 % (70 %) of our photometriccandidates at z = 6.5 (5.7) have been spectroscopically
identified as real LAEs. We made careful measurementsof the Lyα luminosity, both photometrically andspectroscopically, to accurately determine the Lyα andrest-UV luminosity functions (LFs), which can constrain
the cosmic reionization process. Given the large numberof spectroscopic confirmations in our LAE sample, the
Lyα LFs at both redshifts are more tightly constrained
than those in our previous studies. The substantially
improved evaluation of the Lyα LF at z = 6.5 shows anapparent deficit from z = 5.7 at least at the bright end,
and a possible decline even at the faint end, though small
uncertainties remain. The Lyα LF at z = 6.5 shows a
24 % decrease in the Lyα luminosity, or a 34 % decreasein the LF amplitude. The rest-UV LFs at z = 6.5 and
5.7 are in good agreement, at least at the bright end,
in clear contrast to the differences seen in the Lyα LF.
These results imply an increase in the neutral fraction of
the intergalactic medium from z = 5.7 to 6.5. The restframe equivalent width (EW 0) distribution at z = 6.5
seems to be systematically smaller than z = 5.7, and it
shows an extended tail toward larger EW0. The brightend of the rest-UV LF can be reproduced from theobserved Lyα LF and a reasonable EW0–UV luminosity
relation. Integrating this rest-UV LF provides the firstmeasurement of the contribution of LAEs to the photon
budget required for reionization. The derived UV LF
suggests that the fractional contribution of LAEs to thephoton budget among Lyman break galaxies significantly
increases toward faint magnitudes. Low-luminosity LAEs
could dominate the ionizing photon budget, though thisinference depends strongly on the uncertain faint-end
slope of the Lyα LF [1].

036

I Scientific Highlights

Figure 1: Comparison of the cumulative Lyα LFs of LAEs at z =6.5 (red-shaded region) and z = 5.7 (blue-shaded region).
We estimated the acceptable Lyα LF ranges as specified
by the upper and lower limits. The upper limit wasestimated assuming that all the uncertain photometriccandidates are really LAEs, and the lower limit wasestimated assuming that all the uncertain candidates are
not LAEs, i.e., using only the pure spectroscopically
identified LAE sample. In both the upper and lower limit
estimates, we corrected for the detection completenessby number weighting according to the NB magnitude.
Error bars evaluated by the Poisson errors are shownin some average data points between the upper limits
and lower limits. The short-dashed lines (red for z = 6.5
and blue for z = 5.7) show the fitted Schechter LFs in
the case of α = −1.5. As a comparison, the green longdashed line shows the Lyα LF at z = 6.5 from Ouchi etal. 2010, and the green dot-dashed line shows that of Hu
et al. 2010.

Reference[1] Kashikawa, N., et al.: 2011, ApJ, 734, 119.

Identification of the Bursting Water Maser Features in Orion KL
HIROTA, Tomoya1, TSUBOI, Masato2, FUJISAWA, Kenta3, HONMA, Mareki1, KAWAGUCHI, Noriyuki1
KIM, Mi Kyoung1, KOBAYASHI, Hideyuki1, IMAI, Hiroshi4, OMODAKA, Toshihiro4, SHIBATA, Katsunori M.1
SHIMOIKURA, Tomomi5, YONEKURA, Yoshinori6
1: Graduate University for Advanced Studies / NAOJ, 2: IRAS/JAXA, 3: Yamaguchi University, 4: Kagoshima University, 5: Tokyo Gakugei
University, 6: Ibaraki University

2000
3
Flux density [ 10 Jy]

30

1500

10
0

Flux density [Jy]6810LSR velocity [km s -1 ]2011 March 09

1000

500

2006 July 15

0
-10

0

10

20

30

40

LSR velocity [km s -1]
Figure 1: Cross-power spectra of the H 2O masers in the burst(upper) and the quiescent (lower) phases. Dashed lines
indicate the radial velocities of the burst features. An
inset shows the zoom-up of the bursting component.

15(a) 11/03/09(b) 11/05/01

Feature 1

10(c) 11/05/17

Feature 1

Feature 1

5
Feature 2

Feature 2

Feature 2

0
Feature 3

-5
10

5

0

RA offset [mas]Reference[1] Hirota, T., et al.: 2011, ApJ, 739, L59.

20

4

Dec offset [mas]In 2011 February, a burst event of the 22 GHz H2O
maser in Orion KL (Kleinmann-Low object) was
detected. This is the third time such phenomena has been
detected in Orion KL, followed by the events in 1979–
1985 and 1998–1999. In spite of extensive monitoring
observations with the Kagoshima 6 m single-dishtelescope and VLBA during the last time burst event in
1998–1999, the origin of this maser burst is still unclear.
If the current burst event would have a common origin as
in the case of previous burst events, the flux density of the
H2O maser in Orion KL is expected to be >106 Jy, which
will provide best opportunity to investigate the maser
burst phenomenon. With this in mind, we have started
monitoring observations of the bursting H 2O maser
features in Orion KL with VERA since 2011 March 09 [1].
In the monitoring observations, we found that theflux density of the H2O maser reached about 50000 Jy
at the beginning of the burst event, which was threeorders of magnitudes brighter than that in the quiescentphase (Figure 1), while it was still far below the previous
burst events. According to the astrometric observations,the bursting maser features consisted of two spatially
distinct components separated by about 5 AU at different
velocities, 6.95 km s−1 and 7.58 km s−1 (Figure 2). We
successfully determined the absolute positions of the
bursting features for the first time ever with a submilliarcsecond (mas) accuracy. Their positions are coincident
with the shocked molecular gas called the Orion Compact
Ridge. It is most likely that the protostellar outflow
interacting with the Compact Ridge is a possible origin of
the H2O maser burst.
We still continue monitoring observations with VERAof the bursting masers to achieve higher astrometricaccuracy. In addition, we will carry out follow-up
observations with the ALAM of the submillimeter H2O
masers in Orion KL. Detailed mechanisms of the maser
burst will be studied based on the multi-transition maser
data.

-5 10

5

Feature 30

RA offset [mas]

-5 10

5

0

-5

RA offset [mas]Figure 2: Channel maps of the bursting maser features on (a) 2011
March 9, (b) 2011 May 1, and (c) 2011 May 17. Red andblue contours represent the 7.58 km s−1 and 6.95 km s−1
features, respectively. The synthesized beam pattern isshown by a gray ellipse at the bottom left corner of eachpanel.

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Detection of Chemically Young Dark Cloud Cores in the Aquila Rift		

HIROTA, Tomoya

SAKAI, Takeshi, SAKAI, Nami, YAMAMOTO, Satoshi(Graduate University for Advanced Studies / NAOJ)			

29

Declination (J2000)

28

27

26

25

24
19 20 38

36

34

32

30

28

26

24

22

Right Ascension (J2000)
Figure 1: Distributions of CCS (thin contours) and NH 3 (boldcontours) superposed on the dust continuum (gray scale)in L673-SMM4. The position offset between the NH3(cross) and CCS (square) peaks suggests a chemicaldifferentiation in the core.

1000

100
N(NH3)/N(CCS)

In the last decade, we have carried out a survey ofradio spectral lines of NH3 and carbon-chain molecules
such as CCS and HC3N with the Nobeyama 45 m radio
telescope. Because carbon-chain molecules and NH 3
are expected to be abundant in the early and late stagesof chemical evolution, respectively, due to different
production timescales, the abundance ratio of NH3/CCS
can be used as one of the good indicators of chemical
evolutionary phase of dark cloud cores.
Recently, we extensively surveyed the NH3 and CCS
lines in the Aquila Rift region, for which observational
studies with molecular lines were still limited. As aresult, two dense cores, CB130-3 and L673-SMM4,
were detected which show remarkably intense spectraof carbon-chain molecules compared with the weak
NH3 lines [1]. According to their high NH3/CCS ratios,they could be chemically and dynamically less evolved
dense cores. Such chemically less-evolved dense cores
have been found only in the Taurus Molecular Cloud andthe Aquila Rift region. This implies a similarity in thephysical properties and/or chemical evolutionary phasesof these two molecular clouds.
We have also carried out detailed mapping observations of the CCS and NH3 lines with the Nobeyama 45 m
telescope and Effelsberg 100 m telescope of the Max
Planck Institute (Figure 1), as well as a survey of othermolecular lines such as DNC, HN13C, H13CO+, and N2H+.
Using these data, we compared the chemical abundancesof CB130-3 and L673-SMM4 with previously known
carbon-chain-rich cores in the Taurus region [1].
According to the NH3/CCS ratios as well as the DNC/
HN13C ratio, which is another good probe of chemical
evolutionary phase of dense cores, CB130-3 and L673SMM4 are found to be analogous to the previously
known chemically young cores while their chemical
evolutionary phases would be slightly older than thosein the Taurus region. These two sources could be goodtargets to study initial conditions of protostar formation
with future high-sensitivity/high-resolution studies with
ALMA.

(University of Tokyo)

10

L673-SMM4
L1495B

CB130-3
TMC-1(CP)L1521B

L1521E

1
Chemical evolution

Reference[1] Hirota, T., Sakai, T., Sakai, N., Yamamoto, S.: 2011, ApJ, 736, 4.

0.1

0.1

1

10

N(DNC)/N(HN 13C)
Figure 2: Relationship between NH3/CCS and DNC/HN13C ratios.
Filled and open symbols represent the starless and starforming cores, respectively. Dense cores evolve frombottom-left to top-right direction (gray arrow).

038

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Small-JASMINE: Stray Light and Thermal Environment
YANO, Taihei, GOUDA, Naoteru, KOBAYASHI, Yukiyasu, TSUJIMOTO, Takuji, NIWA, Yoshito(NAOJ)YAMADA, Yoshiyuki

YASUDA, Susumu, UTSUNOMIYA, Shin

(Kyoto University)				

(JAXA)

Small-JASMINE [1] is the astrometric satellite
measuring the parallax and the proper motion with theaccuracy of 10 μas level. Current status of the straylight and the thermal condition for small-JASMINE arereported.
1 Stray Light of Small-JASMINE
A lot of integration time is needed to accomplish
the aim of accuracy of about 10 μas level in the SmallJASMINE mission. Accordingly, we need to observe
the object until the albedo from the earth is close to thedirection of 23 degrees from the observing direction.
Therefore avoiding the stray light is very importanttask. We have investigated the baffle hood shown in Fig.
1. Inner baffle of the telescope shown in Fig. 2 is also
considered.
Inner coating of the telescope using the carbon fiber
developed by Energy Science Laboratories adopted by
JWST is the first candidate for Small-JASMINE.
The requirement of the stray light is under 13 photons/
pix/sec. It is achieved using the baffle hood and the inner
baffle with the carbon fiber coating.

JASMINE Working Groupcut off developed by Teledyne. We need to operate thedetector under 180 K. Accordingly the temperature of
the telescope must be 180 K ~ 200 K. The peltier coolingof the detector will be adopted. Then we calculate thethermal environment of the telescope under the attitude of
the satellite shown in Fig. 3. We obtain that the telescope
satisfies the temperature of under 190 K (See Fig. 4).

Figure 3: (Upper) attitude of the satellite in spring. (Lower) Same
as upper panel but in summer.

Figure 1: Baffle hood. We consider a few more baffle hoods.

Figure 4: Tempreture of the telescope (primary mirror) against thetime (season).
Figure 2: Inner baffle.

2 Attitude and the Thermal Condition for SmallJASMINE
The candidate of the detector of Small-JASMINE
is HgCdTe detector, HAWAII-4RG-10, with 1.7 μm

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

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Spectroscopic Confirmation of Galaxies at z = 6.844 – 7.213:
Demographics of Lyα Emission in z ~ 7 Galaxies
		ONO, Yoshiaki, OUCHI, Masami(University of Tokyo)		

PENNER, Kyle

(University of Arizona)		
				(UC Riverside)		

SHIMASAKU, Kazuhiro(University of Tokyo)		

KARTALTEPE, Jeyhan S.

NAKAJIMA, Kimihiko(NOAO) 		

STERN, Daniel

MOBASHER, Bahram

KASHIKAWA, Nobunari(NAOJ)		

One of the most outstanding questions in modern
astronomy is when and how the cosmic reionization
occurred. Since it requires a large number of ionizing
photons, the process of reionization is closely related
to an early phase of the cosmic structure formation
history. Understanding the reionization process canbe accomplished by studying the state of the IGM
through estimates of the Lyα fraction, the fraction of
Lyα emitters among dropout galaxies. Since neutralhydrogen in the IGM resonantly scatters Lyα photons,
the Lyα fraction is expected to decrease at the epochof reionization [1]. Searching for Lyα emission fromsamples of dropouts with available spectra at 4 < z < 6,
Stark et al. (2011) showed that the Lyα fraction does notdecrease with redshift [2]. However, it is not yet clear if
this trend continues at z > 6. To explore this, we require
spectroscopy of z ~ 7 dropouts.
We performed Keck/DEIMOS spectroscopic observations of 11 z-dropout galaxies found in the SDF andGOODS-N fields [3,4]. An emission line is detected at
9500–10000 Å in the spectra of three objects. Since all thedetected lines are singlet with a large positive weighted
skewness, we conclude that the three objects are Lyαemitting z-dropout galaxies at zspec = 7.213, 6.965, and6.844. The z = 7.213 galaxy is confirmed by observations
in two independent DEIMOS runs in 2010 and 2011 withthree different spectroscopic configurations.
We then measure the Lyα fraction at z ~ 7. To reduce
statistical uncertainties and possible effects of field-tofield variance, we combine our results with the z-dropout
spectroscopic studies by other groups [5,6,7,8]. We findthat the Lyα fraction drops from z ~ 6 to 7 in contrast to
the reported increasing trend from z ~ 4 to 6. We also findLyαthat X 25
drops more strongly in UV-faint galaxies thanin UV-bright galaxies. These findings would suggest thatthe neutral fraction of the IGM significantly increases
from z ~ 6 to 7, and that the increase is stronger aroundgalaxies with fainter UV luminosities, which is consistent
with inside-out reionization models where reionization
proceeds from high- to low-density environments.

040

I Scientific Highlights(NOAO)WEINER, Benjamin J.

(University of Tokyo) 		

(JPL) 			DICKINSON, Mark

(Steward Observatory)NAYYERI, Hooshang(UC Riverside)

SPINRAD, Hyron(UC Berkeley)

Figure 1: Evolution in the fraction of strong Lyα-emitting galaxies
with MUV ~_ −21.0 (top panels) and MUV ~_ −19.5 (bottom
panels) over 4 < z < 7. The left panels show the fractionof galaxies with EW larger than 25 Å, while the rightpanels show the fraction of those with EW larger than55 Å. The red filled circle is the composite result, andthe shaded area is derived by extrapolating the trend
seen in lower redshifts to z ~ 7. For details, see [4].

References[1] Dijkstra, M., et al.: 2011, MNRAS, 414, 2139.
[2] Stark, D. P., et al.: 2011, ApJ, 728, L2.
[3] Ouchi, M., et al.: 2009, ApJ, 706, 1136.
[4] Ono, Y., et al.: 2012, ApJ, 744, 83.
[5] Fontana, A., et al.: 2010, ApJ, 725, L205.
[6] Vanzella, E., et al. 2011, ApJ, 730, L35.
[7] Schenker, M. A., et al.: 2012, ApJ, 744, 179.
[8] Pentericci, L., et al.: 2011, ApJ, 743, 132.

NRO M33 All Disk Survey of Giant Molecular Clouds (NRO MAGiC):
HI to H2 Transition
TOSAKI, Tomoka1, KUNO, Nario2, ONODERA, Sachiko2, MIURA, Rie2,3, MURAOKA, Kazuyuki4
SAWADA, Tsuyoshi2, NAKANISHI, Kouichiro2, KOMUGI, Shinya2, HIROTA, Akihiko2, KAWABE, Ryohei2
KOHNO, Kotaro3, KANEKO, Hiroyuki2,5, NAKANISHI, Hiroyuki6
1: Joetsu University of Education, 2: NAOJ, 3: Unversity of Tokyo, 4: Osaka Prefecture University, 5: The Graduate University for Advanced
Studies, 6: Kagoshima University

We present the results of the Nobeyama Radio
Observatory (NRO) M33 All Disk (30′ × 30′, or 7.3 kpc
× 7.3 kpc) Survey of Giant Molecular Clouds (NRO
MAGiC) based on 12CO (J = 1 – 0) observations using
the NRO 45-m telescope [1]. M33 is the best target to
study the properties of the individual GMCs and theircorrelation with galactic structures such as spiral arms
due to its proximity ( ~840 kpc) and small inclination
angle. The spatial resolution of the resultant map is 19″.3 (= 81 pc) which is sufficient to identify each GMC.
We found clumpy structures with a typical spatial
scale of ~100 pc, corresponding to GMCs, and no diffuse,smoothly distributed component of molecular gas at
this sensitivity. The overall distribution of molecular
gas roughly agrees with that of H I. However, closer
inspection of the CO and H I maps suggests that not
every CO emission is associated with local HI peaks,
particularly in the inner portion of the disk (r < 2 kpc),
although most of CO emission is located at the local HI
peaks in the outer radii. We found that most uncovered
GMCs are accompanied by massive star-forming regions,although the star formation rates (SFRs) vary widelyfrom cloud to cloud.
We obtained a map of the molecular fraction, fmol =∑ H2 / (∑ HI + ∑ H2 ), at a 100-pc resolution. This is thefirst fmol map covering an entire galaxy with a GMCscale resolution. We find that fmol tends to be high near
the center. The correlation between fmol and gas surface
density shows two distinct sequences. The presenceof two correlation sequences can be explained bydifferences in metallicity, i.e., higher (~2-fold) metallicity
in the central region (r < 1.5 kpc) than in the outer parts.
Alternatively, differences in scale height can also accountfor the two sequences, i.e., increased scale height toward
the outer disk.

Reference[1] Tosaki, T., et al. : 2011, PASJ, 63, 1171.

Figure 1: CO(1-0) total integrated intensity map.

Figure 2: Correlation between gas surface density and fmol. Red,
blue, and green points represent data with ranges of r ≤1.5 kpc, 1.5 kpc ≤ r ≤ 3 kpc, and r ≥ 3 kpc. Pink dottedand cyan dashed lines indicate correlation for U = 10 U0
at Z = Z0 and Z = 0.5 Z0 (left), and for Z = 1.0 Z0 at U =10 U0 and U = 48 Z0 (right), respectively.

I Scientific Highlights041

Formation of a Propeller Structure
by a Moonlet in a Dense Planetary Ring
MICHIKOSHI, Shugo*

A moonlet embedded in a planetary ring tends to open
a gap, such as Keeler or Encke gap, due to gravitational
scattering [1]. Conversely, viscous diffusion of ringparticles tends to close a gap. If a moonlet is sufficiently
large, it will form a fully circular gap, whereas a small
moonlet will form only a partial gap that consists of two
azimuthally aligned lobes shaped like a propeller. Using
the viscous fluid model, the formation of propellers bysmall moonlets was predicted. The Cassini spacecraft
discovered propellers in Saturn’s A ring [2,3].
The optical depth of the A ring is as high as 0.3–0.5,
while that of the B ring is larger than unity. Distinct andlarge gravitational wakes form in rings with large opticaldepths [4]. Such large gravitational wakes can alter the
structures around an embedded moonlet. We investigatedthe condition for propeller formation in a dense ring inwhich gravitational wakes are prevalent.
Figure 1 shows snapshots of the low and highsurface density models [5]. In the low surface density
model, a propeller-shaped feature is clearly visible
in the weak gravitational wakes. The surface density
decreases considerably in the two lobes downstream ofthe moonlet. They are aligned in the orbital direction andare symmetric about the moonlet. In the high surface
density model, strong wake structures due to gravitational
instability formed but no propeller structures areobserved.

Figure 1: Snapshots of numerical simulations of low and highsurface density models.

The numerical simulation results indicate thatpropeller formation depends on the ring surface density.
The clumps in gravitational wakes typically have amass of ~ Σ λ2, where Σ is the surface density and λ isthe critical wavelength of the gravitational instability.
If the clump mass is greater than the moonlet mass, thegravitational wakes may not be affected by gravitational
scattering due to the moonlet. Accordingly we derived thecritical moonlet size that depends on the surface density* The author is at NAOJ when the paper [5] was submitted.

042

I Scientific Highlights

KOKUBO, Eiichiro(Doshisha University)			

(NAOJ)

around the moonlet.
We performed 25 simulations with different ring
surface densities and moonlet radii so as to confirm thecondition. As shown in Figure 2, we confirmed that apropeller-shaped structure is clearly observed when thiscondition is satisfied. If this condition is not satisfied, nodistinct steady propeller structure is observed although
the ring particles are affected by the moonlet to someextent.
700
600500
Σ (g/cm2)

			

400

0.98

0.61

0.63

0.45

0.32

0.94

0.85

0.43

0.29

0.27

0.97

0.61

0.42

0.15

0.10

0.57

0.21

0.10

0.07

0.05

0.25

0.12

0.08

0.08

0.09

50

100

150

200

250

300
200
100
0

0

300

R (m)
Figure 2: Condition for propeller formation in the R-Σ plane.
Filled squares denote models in which clear propellers
form and crosses denote models in which no propellers
form. We show the ratio of the time-averaged surface
density in the propeller region to the initial surface
density Σ̄ / Σ0 at each point. The solid line indicates thecondition for propeller formation.

References[1] Lissauer, J. J., Shu, F. H., Cuzzi, J. N.: 1981, Nature, 292, 707.
[2] Spahn, F., Sremčević, M.: 2000, A&A, 358, 368.
[3] Tiscareno, M. S., et al.: 2006, Nature, 440, 648.
[4] Salo, H.: 1995, Icarus, 117, 287.
[5] Michikoshi, S., Kokubo, E.: 2011, ApJ, 732, L23.

Secular Gravitational Instability of a Dust Layer in Shear Turbulence
MICHIKOSHI, Shugo*(Doshisha University)		

KOKUBO, Eiichiro(NAOJ)		

In the standard scenario of planet formation,planetesimals are the precursors of planets, the sizes ofwhich are on the order of kilometer. Their formation
process is one of the unsolved problems of the planet
formation theory. From micron-sized dust grains dust
particles grow to centimeter size in a protoplanetary
disk by collisional agglomeration. The least understood
growth phase is growth from centimeter-sized dust to
kilometersized planetesimals.
One of the possible models in this stage is thegravitational instability model. A very thin and dense
layer of settled dust aggregates in the mid-plane of the
protoplanetary disk may be gravitationally unstable. Thenthe gravitational collapse of the dust layer occurs, andkilometer-sized planetesimals are formed directly. This
scenario has the advantage of a very rapid formation
timescale, which is on the order of the Keplerian time.
However, the various hydrodynamic instabilities cause
the turbulence in the protoplanetary disk. In this case, thegravitational instability may be suppressed since the dust
layer can not become thin due to the turbulence [1].
We investigated the motion of dust particles inturbulent gas and derived the surface density evolution
using the stochastic model [2]. We derived the advection
diffusion equation with the strong coupling approximation. We solved the advection diffusion equation
coupled with the Poisson equation for gravity using thelinear approximation. As a result, we found that the dust
layer is always unstable regardless of the turbulence
strength, but its timescale becomes longer as theturbulence becomes stronger. The dust density increases
monotonically because of the instability.
The physical meaning of the secular gravitational
instability can be understood in terms of the responses
to the density perturbation. We suppose that the density
fluctuation exists. The gravitational potential is inducedby the density fluctuation. Due to the resultant potential
gradient, the matter moves to the local maximum point of
the surface density with the terminal velocity. Therefore,
the density fluctuation increases monotonically.
We applied this instability to the protoplanetary
disk. This instability always occurs, but its timescale istypically very long. If the radial drift of dust particles
due to gas drag is faster than the secular gravitational
instability, the secular instability seems to be inefficient.
In this case, the particle pileup mechanism due to theradial drift enhances the surface density of dust [3].
Thus, we should compare the timescales of the seculargravitational instability and the radial drift. Figure 1

INUTSUKA, Shu-Ichiro(Nagoya University)

shows the critical fg value, where fg is the enhancement
factor of the surface density of gas, as a function of
the distance from the Sun. The value Jc is the critical
Richardson number. Here we assume the quasiequilibrium shear turbulence model. If fg is larger than thecritical value, the secular gravitational instability is fasterthan the radial drift. When fg > 3 and Jc = 0.1, the seculargravitational instability is faster than the radial drift inthe entire disk. If this condition is satisfied, axisymmetrichigh-density patterns form. When the dust surface
density becomes large due to this instability, the classicalgravitational instability may occur finally [4]. We will
investigate this process by numerical simulations in the
future work.

Figure 1: The critical fg values as a function of the distance fromthe Sun a.

References[1] Weidenschilling, S. J.: 1980, Icarus, 44, 172.
[2] Michikoshi, S., Kokubo, E., Inutsuka, S.-i.: 2012, ApJ, 746, 35.
[3] Youdin, A. N., Shu, F. H.: 2002, ApJ, 580, 494.
[4] Sekiya, M.: 1998, Icarus, 133, 298.

* The author is at NAOJ when the paper [2] was submitted.

I Scientific Highlights

043

Stellar Populations and Spatial Distributions of Ultra Faint Dwarf Galaxies
OKAMOTO, Sakurako

ARIMOTO, Nobuo, YAMADA,Yoshihiko(Peking University)			

Dwarf spheroidal galaxies (dSphs) around the Milky
Way provide us a unique opportunity to investigate
galaxy formation and evolution through their resolvedstars. Since 2005, extremely faint dwarf (UFD) galaxies
and stellar streams are found around the Milky Way [1,2].
The newly discovered UFD galaxies are roughly 10 to
100 times fainter than the well-known “classical” dSphs,
having amorphous morphology, and yet are the most dark
matter (DM) dominated galaxies. Their star formation
histories and detailed structural properties provide a clue
to understanding of the galaxy formation at the faint-end
and the Galactic tidal effects for the satellite galaxies.
We take deep images of four UFD galaxies, Canes
Venatici I, II (CVn I, II), Boötes I (Boö I), and Leo
IV, using the Suprime-Cam on the Subaru Telescope[3]. Color-magnitude diagrams (CMDs) extend below
mainsequence turnoffs and yield measurements of theages of stellar populations. The stellar populations of
three faint UFD galaxies are estimated to be as old as the
Galactic globular cluster M92. We confirm that Boö I(NAOJ)		

ONODERA, Masato(Institute for Astronomy, ETH Zürich)dSph has no intrinsic color spread in the MSTO andno spatial difference in the CMD morphology, whichindicates that Boö I dSph is composed of an old single
stellar population. One of the brightest UFDs, CVn I
dSph, shows a relatively younger age (~12.6 Gyr) withrespect to fainter dSphs, and the distribution of red
horizontal branch (HB) stars is more concentrated toward
the center than that of blue HB stars, suggesting that thegalaxy contains complex stellar populations. CVn II dSph
has the smallest tidal radius of a Milky Way satellite
and has a distorted shape, while Leo IV dSph shows aless concentrated spherical shape. The simple stellar
population of faint UFDs indicates that the gases in theirprogenitors were removed more effectively than thoseof brighter dSphs at the occurrence of their initial starformation. This is reasonable if the progenitors of UFDs
belong to less massive halos than those of brighter dSphs.

Figure 2: Spatial distribution of the member candidates selectedfrom CMD and iso-density contour of the member
candidates of Boötes I dSph.

Figure 1: (V – IC)0 – V0 CMD of whole observed region of Boötes
I dSph. The theoretical Padova isochrone of Z = 0.0001
and 13.7 Gyr is overlaid.

044

I Scientific Highlights

References[1] Willman, B., et al.: 2005, ApJ, 626, 85.
[2] Belokurov, V., et al.: 2007, ApJ, 654, 897.
[3] Okamoto, S., et al.: 2012, ApJ, 744, 96.

The Widest-Separation Substellar Companion Candidate
to a Binary T Tauri StarKUZUHARA, Masayuki, TAMURA, Motohide, ISHII, Miki, KUDO, Tomoyuki, NISHIYAMA, Shogo, KANDORI, Ryo(NAOJ)

Direct imaging surveys are powerful tools to search
for Jupiter-mass planets around young stars, and thosesearchers are useful to study the theory of the formationof giant planets with wide orbits around their parent stars.
Recent direct imaging surveys show that the projected
separation of young planetary-mass companions(PMCs) are surprisingly wide compared with the orbital
separations of planets in our solar system, extra-solar
planets detected by indirect methods, and predictionsof the standard core accretion model [1]. These results
may suggest a diversity in the formation and evolution of
PMCs. (e.g., [2]).
We present the results of the direct imaging of a
PMC candidate around a binary T Tauri star, SR12AB(K4–M2.5), in the ρ Oph star-forming region [3]. The
rst discovery of the PMC candidate, SR12 C, was madethrough the imaging observations carried out on 2002
using the near-infrared camera SIRIUS mounted on the
1.4-m telescope IRSF. SR12C is separated by ~ 8.7″,
corresponding to 045 1100 AU at 125 pc (Fig. 1).
The associated members of a star-forming region
share a common proper motion, and thus can be
distinguished from background objects by investigating
their proper motions from images obtained at multiple
epochs. Two epoch images using Subaru (IRCS andCIAO), and three archive date sets (HST/NICMOS, VLT/
NACO, and Gemini/QUIRC+Hokupa'a) are used for
precise astrometry of the SR12 system. The separationof SR12C from SR12AB is constant from 1998 to 2008,
suggesting physical relation of them. In addition, the Hband spectra of SR12C shows a triangular shape, which
is a characteristic feature of young, late-ytpe dwarfs withlow surface gravity. Therefore we conclude that SR12C isa member of the ρ Oph star-forming region. In addition,
the probability of a chance alignment of objects in ρ Oph,physically associated with SR12AB is very low (~1 %),indicating that SR12C is a genuine companion to SR12
AB.
Using an age-luminosity diagram, we estimate themass of SR12 C. It has an J-band absolute brightness of
10.5 mag and infrared spectra suggesting a spectral typeof M9.0 ± 0.5 and Teff ≈ 2400. The bolometric luminosityof SR12C was estimated to be log(L = L) = −2.87 ± 0.20.
Assuming that the age of SR12C is the same as those of
YSOs in ρ Oph, the mass of SR12C was estimated as
0.013 ± 0.007 M (14 +7−8 MJup) by comparing with models.

Therefore SR12C is a strong PMC candidates, and the rst
PMC candidate directly imaged around a binary T Tauri
star. Considering the projected separation from SR12
AB, SR12C has the widest separation from its parent staramong PMC candidates imaged so far1. This discovery
spreads the range of distributions of the PMC candidates
from ~50 to 1100 AU.

Figure 1: Subaru/CIAO K-band coronagraphic image of a binary
T Tauri star SR12 AB and its planetary-mass companion
candidate SR12 C. The parent binary star is blocked
by the occulting mask. The companion (SR12 C) is
separated by ~8.7″, corresponding to ~1100 AU at 125 pc.

References[1] Pollack, J. B., et al.: 1996, Icarus, 124, 62.
[2] Lafreniere, D., et al.: 2007, ApJ, 670, 1367.
[3] Kuzuhara, M., et al.: 2011, AJ, 141, 119.
[4] Burgasser, A., et al.: 2010, ApJ, 725, 1405.

* When the manuscript was submitted, PMO candidates with the similar
separations with SR12 C were reported (e.g., [4] ).

I Scientific Highlights

045

Astrometry of Galactic Star-Forming Region G48.61+0.02 with VERANAGAYAMA, Takumi, HONMA, Mareki, KOBAYASHI, Hideyuki, KAWAGUCHI, Noriyuki, UENO, Yuji
(NAOJ)OMODAKA, Toshihiro, HANDA, Toshihiro(Kagoshima University)

We performed the astrometry of H2O masers in the
Galactic star-forming region G48.61 + 0.02 with the
VLBI Exploration of Radio Astrometry (VERA). We
derived a trigonometric parallax of 199 ± 7 μas, whichcorresponds to a distance of 5.03 ± 0.19 kpc. The distanceto G48.61 + 0.02 is about a half of its far kinematic
distance, which was often assumed previously. Thisdistance places G48.61 + 0.02 in the Sagittarius-Carina
arm and near the active star forming region and thesupernova remnant W51. The obtained distance is very
close to the parallactic distance of W51 Main/South,
which is measured to be 5.41+0.31−0.28 kpc by the H2O maser
astrometric observations with VLBA [1].
We also obtained the three dimensional motion of
G48.61 + 0.02, and found that it has a large peculiar
motion of 40 ± 5 km s −1 . The kinetic energy of thepeculiar motion is estimated to be (2 ± 1) × 10 51 erg.
What is the origin of this peculiar motion? This peculiar
motion would be originated with the multiple supernovae
explosions in W51, or the streaming motion across the
Sagittarius-Carina arm. W51 C is the nearest SN remnant
from G48.61 + 0.02. Figure 1(a) shows the position of
G48.61 + 0.02 superimposed on Fermi LAT counts map
in 2–10 GeV around W51 C [2]. The separation between
G48.61 + 0.02 and the center of W51 C is 0.70 deg (62pc). Figure 1(b) and (c) show the integrated intensity
and the position velocity maps in the 13CO J = 1–0 line
around W51 C [3]. The explosion kinetic energy of
W51 C is estimated to be ~ 5 × 1051 erg [2]. Considering
the energetics, the SN explosion is the possible origin.
G48.61 + 0.02 appears to be located on the SagittariusCarina arm. Therefore, the streaming motion across the
spiral arm is one possible origin for the large peculiar
motion of G48.61 + 0.02.
This study is published in Nagayama et al. (2011),
PASJ, 63, 719.

References[1] Sato, M., Reid, M. J., Brunthaler, A., Menten, K. M.: 2010,
ApJ, 720, 1055.
[2] Abdo, A. A., et al.: 2009, ApJ, 706, L1.
[3] Jackson, J. M., et al.: 2006, ApJS, 163, 145.

046

I Scientific Highlights

Figure 1: (a): Positions of G48.61+0.02, W51 Main/South(white circle), and OB stars in G49.5–0.4 (green cross)superimposed on Fermi LAT counts map in 2.10 GeV
around W51 C [2]. The crosses show the center of W51
C and the position of J1921+1419. The arrow shows
the motion of G48.61+0.02 relative to W51 Main/South
which is obtained to be −0.12 ± 0.16 mas yr−1 (−2.9 ±3.9 km s−1) in right ascension and −0.17 ± 0.19 mas yr−1(−4.1 ± 4.6 km s−1) in declination. (b): same as (a), but
the background shows the integrated intensity map in
the 13CO J = 1–0 line [3]. (c): Longitude-velocity map in
the 13CO J = 1–0 line [3].

Particle-Particle Particle-Tree: A Direct-Tree Hybrid Scheme
for Collisional N-Body Simulations
				

OSHINO, Shoichi(NAOJ) 		

FUNATO, Yoko

(University of Tokyo)

For the time integration of collisional -body systems,
such as star clusters and systems of planetesimals, thecombination of direct summation for force calculation andthe individual timestep algorithm has been the standard
method for nearly a half century. It is not impossible tocombine an individual timestep algorithm and a fast andapproximate force calculation. However, it was difficult
to achieve good performance on distributedmemory
parallel computers for such a scheme.
Figure 1 shows the long-term variation of the relative
energy error. In this case, the energy error reaches about
7.5 × 10−8 after the time integration for 10 yr (10 orbital
periods), while it is 9.8 × 10−9 for 10 yr (10 periods). In
other words, the energy error grows to be 10 times larger
as the integration time becomes 1000 times longer. Thisshows that the growth of the energy error is stochastic,
like a random walk. It means that the error is mainly
caused by the force error of the tree scheme. The growthof the energy error is, therefore, expected to be slow, andthe error is small enough even after long calculations.
Figure 2 shows the calculation time per one tree timestep
as a function of the total number of particles in system.
We used the Intel(R) Core(TM)2 Quad CPU Q6600 (2.4
GHz). It shows that the calculation time increases as O(Nlog N). Therefore, we reduce the calculation cost fromO(N 2) to (N log N).
We have developed a new hybrid N-body simulation
algorithm for simulating collisional N-body systems. This
new scheme is constructed by combining the tree anddirect schemes using a hybrid integrator. The results oftest simulations involving the evolution of a planetesimal
system show that our new scheme PPPT can drasticallyreduce the calculation cost, to a level comparable to thecost of a tree scheme with a constant timestep, while
keeping the accuracy sufficient for realistic simulations[1].
In principle, our scheme can be used for collisional
systems other than planetary systems, such as globularclusters and stars around a supermassive blackhole in thegalactic center.

MAKINO, Junichiro(Tokyo Institute of Technology)

Figure 1: The relative energy error.

Figure 2: The calculation time plotted against a function of
number of particles. The crosses and squares show
the results of PPPT and fourth-order Hermite scheme,
respectively.

Reference[1] Oshino, S., Funato, Y., Makino, J.: 2011, PASJ, 63, 881.

I Scientific Highlights

047Detection of an Ultra-Bright Submillimeter Galaxy
in the Subaru/XMM-Newton Deep Field Using AzTEC/ASTE
IKARASHI, Soh1, KOHNO, Kotaro1, MOTOHARA, Kentaro1, TAMURA, Yoichi1, NAKAJIMA, Kimihiko1
SHIMASAKU, Kazuhiro1, TSUKAGOSHI, Takashi1, IONO, Daisuke2, KAWABE, Ryohei2, EZAWA, Hajime2
NAKANISHI, Koichiro2, FURUSAWA, Hisanori2, FURUSAWA, Junko2, TAKATA, Tadafumi2
HATSUKADE, Bunyo3, MATSUHARA, Hideo4, TAKAGI, Toshinobu4, TANAKA, Tomohiko5
AGUIRRE, James E.6, LUPU, Roxana6, SCOTT, Kimberly S.6, ARETXAGA, Itziar7, HUGHES, David H.7
ARUMUGAM, Vinodiran8, CIRASUOLO, Michele8, IVISON, Rob J.8, AUSTERMANN, Jason9
EARLE, Lieko9, GLENN, Jason9, KAMENETZKY, Julia9, MALONEY, Philip9, BOCK, James J.10,11
BRADFORD, Charles M.10,11, ZMUIDZINAS, Jonas10,11, MURPHY, Eric J.11, NAYLOR, Bret J.10
NGUYEN, Hien10, JOHNSON, Seth12, WILSON, Grant W.12, YUN, Min S.12, MAUSKOPF, Philip D.13
PETERA, Thushara A.14, WILNER, David J.15
1: University of Tokyo, 2: NAOJ, 3: Kyoto University, 4: Institute of Space and Astronautical Science, 5: Keio University, 6: University ofPennsylvania, 7: INAOE, 8: University of Edinburgh, 9: University of Colorado, 10: Jet Propulsion Laboratory, 11: California Institute ofTechnology, 12: University of Massachusetts, 13: Cardiff University, 14: Illinois Wesleyan University, 15: Harvard-Smithsonian Center for
Astrophysics

We report the detection of an extremely bright (~37 mJy
at 1100 μm and ~ 91 mJy at 880 μm) submilli-meter
galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafterreferred to as SXDF1100.001 or Orochi), discovered in
1100 μm observations of the Subaru/XMM-Newton Deep
Field using AzTEC on ASTE[1]. Subsequent CARMA
1300 μm and SMA 880 μm observations successfully
pinpoint the location of Orochi (Fig. 1) and suggest thatit has two components, one extended (FWHM of ~4″)and one compact (unresolved). Z-Spec on CSO has also
been used to obtain a wide band spectrum from 190 to
308 GHz, although no significant emission/absorption
lines are found. The derived upper limit to the line-tocontinuum flux ratio is 0.1–0.3 (2σ) across the Z-Specband.
Based on the analysis of the derived spectral energy
distribution from optical to radio wavelengths of possible
counterparts near the SMA/CARMA peak position, wesuggest that Orochi is a lensed, optically dark SMG lying
at z ~ 3.4 behind a foreground, optically visible (but red)galaxy at z ~ 1.4 (Fig. 2). The deduced apparent (i.e., no

Figure 1: Multi-wavelength images of Orochi with SMA contours(3, 6, 9, 12, 15, 18, and 21 σ). The size of each image is
10″ × 10″; north is towards the top of the image and east
is towards the left side of the image. From left to rightand top to down: VLA 20 cm; CARMA 1300 μm; SMA
880 μm; MIPS 24 μm; rgb image of IRAC/ 3.6 μm (blue),
4.5 μm (green), 5.8 and 8 μm (red); rg image of WFCAM/
J (green) and K (red); rgb image of SuprimeCam/R, i′and z′; rgb image of SuprimeCam/uR, B and V.

048

I Scientific Highlights

correction for magnification) infrared luminosity (LIR)
and star formation rate (SFR) are 6 × 1013 L and 11000
M yr−1, respectively, assuming that the LIR is dominatedby star formation. These values suggest that Orochi willconsume its gas reservoir within a short time scale (3 ×
107 yr), which is indeed comparable to those in extreme
starbursts like the centres of local ULIRGs.

Figure 2: The left panel shows the colour-colour-redshif plot
for Orochi. The flux ratios of the mock galaxies are
represented as diamonds, and their redshifts are colourcoded according to the scale shown in the panel on theright. The cross represents the measured colours ofOrochi, and the dashed box shows the 1σ uncertanity
in each colour. The top right panel shows estimatedredshift probability distribution of Orochi. In the bottom
right panel, the observed SED of Orochi normalised to
the flux densities at 1000 μm is shown as squares andarrows. The arrow indicates 3σ upper limits. The squares
denote the detection at a level. 3σ, with 1σ error bars.
The template SEDs (lines) are redshifted to z = 3.4. The
template SEDs at this redshift compatible within 3σ error
bars with the SED of Orochi are displayed as blue lines.
The photometric data are shown at 1000, 1100, 1500 μm,
20 and 50 cm, and The upper limit is shown at 160 μm.
Reference[1] Ikarashi, S., et al.: 2011, MNRAS, 415, 3081.

Effects of Magnetic Fields with Log-Normal Distribution on the CMB		YAMAZAKI, Dai G.
(NAOJ)		

ICHIKI, Kiyotom(Nagoya University)

We research effects of a primordial magnetic field(PMF) on the temperature fluctuations and polarization
anisotropies of the cosmic microwave background (CMB)[1]. We assume that spectra of a primordial magnetic field(PMF) are described by log-normal distributions (LND)
to research the PMF which has a characteristic scale on
the temperature fluctuations and polarization anisotropiesof the CMB and constrain the parameters of the LNDPMF by the CMB observations.
Theoretical models of PMF generations on
cosmological scales have been proposed by many
researchers. Since such generation models are based on
causal physical processes, PMFs are expected to havethe model-dependent scale. If PMFs have been generated
from inflation the power law model would be a good
representation of the magnetic field power spectrum. On
the other hand, if the PMFs was created through othermechanisms than inflation the spectrum would have acharacteristic scale and may not be described as a simple
power law. Furthermore, we need to understand how
such PMFs cascade from smaller to larger scales to study
effects of the PMFs created in the early universe on thelarge scale structures. Actually, we can learn behaviors of
PMF cascading or inverse-cascading by simulations [2],which results, however, generally depend on cosmologicalparameters and models. Since such simulations generally
spend too long time and have the limited dynamical
range, it is not efficient to estimate distributions of the
PMF by some simulations when we study cosmology andastrophysics with the PMF quantitatively.
To avoid these problems, we use a log-normal
distribution (LND) in place of the power law defined as,

TAKAHASHI, Keitaro(Kumamoto University)of the CMB for smaller scale is dominated by the vector
modes. Because three parameters which characterize the
LND-PMF affect the CMB power spectra differently at
small and large scales we expect that tight constraints
can be placed on these parameters without degeneracy.
We f o u n d t h a t t h e L N D - P M F w h i c h g e n e r a t e s
CMB anisotropies among 1000 < ℓ < 2000 is mosteffectively constrainted by the current CMB data sets.
For example, B LND for 10 −3 Mpc −1 ≤ k/h ≤ 10 −2 Mpc −1
and σM = 1.0 is limited most strongly as shown in Fig. 1.
In the near future, the tigher constraints on BLND at
kM /h > 10−2 Mpc−1 will be expected from the observations,such as Planck, QUIET, and PolarBear missions.

Figure 1: Constraint on the strengths of LND-PMF for 10−5 < kM
< 10−1. Blue curve is the 2 σ (95 % CL) upper limits of
BLND [nG]. We fix the standard cosmological parameters
and use the best-fitted value from WMAP 7th + tensor
mode [2].

(1)
where kM is the characteristic scale depending on the
PMF generation model, and σM is the variance. The
variance σM in Eq.(1) expresses how this distribution
is expanded (or concentrated) around the characteristic
scale kM. Therefore, the variance σM may be related to thecascading of the PMFs.
We have revealed the features of the LND-PMF
effects on the CMB as follows: (1) For larger kM or/and
σM, the CMB spectra of TT, TE and EE from the LNDPMF are dominated by the vector mode. Meanwhile,in the opposite case, these spectra are dominatedby the scalar mode. (2) The CMB spectrum of the
BB polarization anisotropy for all scales and otherpolarization anisotropies and temperature fluctuations

References[1] Yamazaki, D. G., Ichiki K., Takahashi, K: 2011, Phys. Rev. D,
84, 123006.
[2] Larson D., et al.: 2011, ApJS, 192, 16.

I Scientific Highlights

049

Observational Evidence for an Impact
on the Main-Belt Asteroid (596) Scheila
HANAYAMA, Hidekazu

ISHIGURO, Masateru(NAOJ)		

HASEGAWA, Sunao, SARUGAKU, Yuki

(Seoul National University)			

WATANABE, Jun-Ichi, FUJIWARA, Hideaki, TERADA, Hiroshi

				
				

(NAOJ)					VAUBAILLON, Jeremie J.
(Observatoire de Paris)(ISAS)

HSIEH, Henry H.

(University of Hawaii)

KAWAI, Nobuyuki(Tokyo Institute of Technology)

YANAGISAWA, Kenshi, KURODA, Daisuke, MIYAJI, Takeshi, FUKUSHIMA, Hideo					

HAMANOWA, Hiromi(NAOJ)						KIM, Junhan(Hamanowa Astro. Obs.)				

We made imaging observations of the main-belt
asteroid (596) Scheila which was found to exhibit an
outburst and a comet-like activity, using Murikabushi
105 cm telescope at the Ishigakijima Astronomical
Observatory and Subaru 8.2 m telescope at the NAOJ
Hawaii observatory.
We restricted the amount and size distribution of
the dust particles with the analysis of the dust structure,and found when it exhibited the outburst, comparing theposition angle of the dust tail and synchrones [1].
Then, we constructed the numerical model based on
the laboratory experiment of the asteroid impact, andshowed that the model reproduced the morphology of thecomet-like dust structure [2].

PYO, Jeonghyun(KASI)		

NAKAMURA, Akiko M.
(Kobe University)

Figure 1: (596) Scheila which showed an outburst and cometlike
activity. Upper and middle panels, except the middle
center panel, show the dust tails observed with
Murikabushi 105 cm telescope at the Ishigakijima
Astronomical Observatory. The lower panel is the imageof the dust tail observed with Subaru 8.2 m telescope at
the NAOJ Hawaii observatory.

References[1] Ishiguro, M., et al.: 2011, ApJ, 740, L11.
[2] Ishiguro, M., et al.: 2011, ApJ, 741, L24.

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OHTA, Kouji(Kyoto University)

Multiband Optical Observation of P/2010 A2 Dust Tail			HANAYAMA, Hidekazu

KIM, Junhan(NAOJ)				

HASEGAWA, Sunao, USUI, Fumihiko		(ISAS)				

WATANABE, Jun-ichi(NAOJ) 		

ISHIGURO, Masateru(Seoul National University)

YANAGISAWA, Kenshi

YOSHIDA, Michitoshi(ISAS)FUKUSHIMA, Hideo, MIYAJI, Takeshi(Hiroshima University)				

We observed the main-belt asteroid P/2010 A2 dust
tail, using Murikabushi 105 cm telescope and MITSuME
three-channel simultaneous imaging system at the
Ishigakijima Astronomical Observatory.
The analysis of the relative reflectance of the dust tailand the type classification of the asteroid revealed that thereflectance of the P/2010 A2 dust tail resembled that ofan Sq-type or C-type asteroid and the spectrum was close
to ordinary chondrites [1].

SARUGAKU, Yuki

(NAOJ)			

(NAOJ)

(a)

(b)

(c)

Figure 1: Images of P/2010 A2 dust trail. These are composite
image in three different waveband of (a) g' -band, (b)Rc -band, and (c) Ic -band.

Reference[1] Kim, J., et al.: 2012, ApJ, 746, L11.

I Scientific Highlights

051

Expedition for Ground-Based Observationof HAYABUSA Spacecraft Re-Entry
WATANABE, Jun-ichi, OHKAWA, Takuya, SATO, Mikiya

				

IIJIMA, Yutaka

					(NAOJ)			

KAGAYA, Yutaka(Kagaya studio)

The HAYABUSA spacecraft re-entered the Earth's
atmosphere on June 13, 2010 UT., together with thecapsule for the sample return. This was the first trialof the re-entry experiment as a Japanese interplanetary
spacecraft. We organized an expedition to South Australia
for ground-based observations, and succeeded in
obtaining valuable data of various phenomena occurringat this re-entry by using 17 instruments. Our data were
widely used not only for scientific analysis, but also for
outreach purposes [1].
We succeeded to monitor fragmentation of the main
body of HAYABUSA spacecraft at the re-entry. The
fragmentation started at 13 h 52 m 5.2 s UT at 83 – 84
km above the sea level, and the number of fragments
increased with time. The maximum number is more than afew hundreds at around 13 h 52 m 20 s, and the fragments
dispersed with more than 14 km in length, and 1 km inwidth along the re-entry trajectory. The number decreased
after the maximum, and almost ended at 13 h 52 m 31.3 s
at around the height of 45 km. Under some assumptions,
we derived size distribution of the fragments, whichshows small power low index within a range of −1.2
and −1.4, which is similar to −1.5 of the intrinsic size
distribution of assembled parts of the spacecraft. Thisstrongly indicates that in the fragmentation phenomena
the size distribution of the fragments reflects the internal
structure of the parent bodies [2].
A low resolution spectroscopic observation of thecapsule were also performed. The altitude at the maximal
flux was ocuurred at around 56 km (13 h 52 m 19.8 s UT),
and thederived blackbody temperature was 3100 ± 300 K
at the altitude of 50 km, and 2400 ± 300 K at the altitude

OHNISHI, Kouji(Nagano National College of Technology)

TANABE, Tsutomu

of around 40 km, respectively [3].
The brightness variation of the main body during theablation was derived by using ghost images instead ofthe direct ones due to heavy saturation. Among several
peaks of flare up possibly due to the rapid increase of thetotal cross section of fragments, the maximum brightness
obtained was −13.1 ± 0.1 which is apparent magnitude
at 13 h 52 m 19.8 s UT, which corresponds to the heightof 57.4 km. The corresponding absolute magnitude is−13.7 ± 0.1 [4].

References[1] Watanabe, J.-I., et al.: 2011, PASJ, 63, 941-946.
[2] Watanabe, J.-I., et al.: 2011, PASJ, 63, 955-960.
[3] Ohnishi, K., et al.: 2011, PASJ, 63, 987-993.
[4] Ohkawa, T., et al.: 2012, PASJ, 64, 11-14.

Figure 1: Image of maximal phase of the fragmentation of the HAYABUSA spacecraft at 13 h 52 m 19.8 s. Hundreds of fragments are easily
recognized. Taken by OLYMPUS E-30 with a ZUIKO DIGITAL ED 35–100 mm (F 2.0) lens which was set up for sequential
shooting mode of 5 frames every second. The exposure time was 1/60 second. The focal length was fixed at 100 mm, which resulted
in 12.3 degrees in the diagonal field of view. The ISO was set at 3200 to achieve high sensitivity.

052

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Global Structure of Three Distinct Accretion Flows andOutflows around Black Holes from
Two-Dimensional Radiation-Magnetohydrodynamic Simulations
OHSUGA, Ken(Graduate University for Advanced Studies / NAOJ)

Wi t h a t w o - d i m e n s i o n a l g l o b a l R a d i a t i o n magnetohydrodynamic (RMHD) code [1], we could
reproduce three distinct inflow-outflow modes aroundblack holes. Our three models correspond to the twodimensional RMHD version of the slim disk (supercritical flow), the standard disk, and the RIAF, all with
substantial outflows (see Figure 1) [2].
We find the supercritical disk accretion flow, of which
the photon luminosity exceeds the Eddington luminosity.
The vertical component of the radiation force balancesthat of the gravity in the disk region but it largely exceeds
the gravity above the disk. Our RMHD simulations reveal
a new type of jet, i.e., the radiatively driven, magneticallycollimated outflow, which might account for the jets ofradio-loud NLS1s and microquasars [3,4]. The disk, thetemperature of which is around 107–8 K, is surroundedby hot outflowing matter, > 109 K, which would induce
Compton upscattering and obscuration of the inner partof the disk. Because of the mildly collimated radiative
flux, the apparent (isotropic) photon luminosity is ~22LE,
which is 1.5 × 1041 erg s−1 for the black hole of 50 M inthe face-on view. It implies that our supercritical model isable to explain the central engine of ULXs [5].
When the radiative cooling is effective, a cold (~106 K)
geometrically thin disk forms and enveloped by the
hot rarefied atmosphere with T gas > 10 9 K, Compton
upscattering the seed photons from the cold disk. The

MINESHIGE, Shin
(Kyoto University)

cold thermal component and the non-thermal hardcomponent of the spectra are observed in luminous AGNs
and in the high-soft state of BHBs [6,7]. The disk windappears above the disk, which was not predicted in theframework of the standard disk model. This result seems
to be consistent with the observations of the blueshifted
absorption lines [8].
The simulations with low accretion rate corresponds
to the RIAF. The magnetic-pressure force, together withthe gas-pressure force, drives the outflows. The flow
releases the energy via jets rather than via radiation.
The accretion flow as well as the outflows are hot andoptically thin. Thus, the spectra would resemble those of
the low-luminosity AGNs and of the BHBs in their lowhard state [9].

References[1] Ohsuga, K., et al.: 2009, PASJ, 61, L7.
[2] Ohsuga, K., Mineshige, S.: 2011, ApJ, 736, 2.
[3] Fender, R. P., et al.: 2004, MNRAS, 355, 1105.
[4] Doi, A., et al.: 2006, PASJ, 58, 829.
[5] Makishima, K., et al.: 2000, ApJ, 535, 632.
[6] Brunner, H., et al.: 1997, A&A, 326, 885.
[7] Kubota, A., Makishima, K.: 2004, ApJ, 601, 428.
[8] Miller, J. M., et al.: 2006, Nature, 441, 953.
[9] Markowitz, A., Uttley, P.: 2005, ApJ, 625, L39.

Figure 1: Simulated normalized density distributions (color) and streamlines near the black hole for three models, which correspond to thetwo-dimensional RMHD version of the slim disk (supercritical flow; left), the standard disk (center), and the RIAF (right).

I Scientific Highlights

053

Gravitational Wave Signatures ofMagnetohydrodynamically Driven Core-collapse Supernova Explosions
TAKIWAKI, Tomoya(NAOJ)

Core-collapse supernovae are now expected to be
opening a new branch of astronomy, gravitationalwave (GW) astronomy. Currently, long baseline laserinterferometers LIGO, VIRGO, GEO600, TAMA300,
AIGO and KAGRA with their international networks ofobservatories are beginning to take data at sensitivities
where astrophysical events are predicted. For thesedetectors, corecollapse supernovae have been proposed as
one of the most plausible sources of gravitational waves.
Although the explosion mechanism of core-collapse
supernovae has not been completely clarified yet,magnetohydrodynamic (MHD) explosion mechanism
gathers great attention for special explosions associatedwith birth of magnetars instead of ordinary pulsars.
By performing a series of two-dimensional, special
relativistic MHD simulations, we study signaturesof gravitational waves in the MHD mechanism. The
simulation code utilized here is developed at Takiwaki
et al 2009 [1]. We choose to take precollapse magnetic
fields less than 10 12 G and rapid rotation based on a
recent GRBoriented progenitor models. By this choice,the rotation of the central proto-neutron star amplifies
magnetic fields enough strong to overwhelm the rampressure of the accreting matter, leading to the MHD
explosions. Figure 1 shows the bipolar jet generated by
the magnetic field in our simulations.
We found that the total GW amplitudes show amonotonic increase after bounce for models with a strong
precollapse magnetic field (10 12 G) also with a rapid
rotation imposed. Figure 2 shows the time evolution of
the gravitational wave denoted above. We pointed outthat this trend stems both from the kinetic contributionof MHD outflows with large radial velocities andalso from the magnetic contribution dominated by thetoroidal magnetic fields that predominantly trigger MHD
explosions. The feature can be clearly understood witha careful analysis on the explosion dynamics. It waspointed out that the GW signals with an increasing trend,
possibly visible to the next-generation detectors for a
Galactic supernova, would be associated with MHD
explosions exceeding 1051 erg. For detail, see the original
paper of Takiwaki and Kotake 2011 [2].

Figure 2: Amplitude of the gravitational wave as a functionof time (Red line). Green and blue lines depict thecontributions of hydrodynamical part and magnetic part,respectively.

Figure 1: Time snapshot of MHD explosion: Entropy [kB]
and plasma β are shown in the left and right panel,
respectively.

054

I Scientific Highlights

References[1] Takiwaki, T., Kotake, K., Sato, K.: 2009, ApJ, 691, 1360.
[2] Takiwaki, T., Kotake, K.: 2011, ApJ, 743, 30.

Cosmological Time-Dependent Quark Masses and Big Bang Nucleosynthesis
CHEOUN, Myung-Ki.
(Soongsil University)

KAJINO, Toshitaka(NAOJ / University of Tokyo)

There has been considerable interest [1] in theuse of big bang nucleosynthesis (BBN) to constrain
any possible time variation of fundamental physicalconstants in the early universe. A time dependence offundamental constants in an expanding universe can bea generic result [2] of theories unifying gravity and otherinteractions. It can be argued [3] that BBN is much moresensitive to variations in the averaged quark mass, i.e.,mq ≡ (mu + md )/2, than other physical parameters suchas variations in the fine structure constant. Hence, mq
may be the best parameter to search for evidence of time
variation of fundamental constants.
We reinvestigate the constraints from BBN on a
possible time-dependent quark mass [4]. The limits onsuch quark-mass variations are particularly sensitive tothe adopted observational abundance constraints. Hence,
we have adopted updated light-element abundances anduncertainties deduced from observations.
Changing mq affects nuclear reaction rates throughthe dependence of the rates on nuclear binding energies
and the reaction Q values. Resonant reactions of BBN
were treated slightly differently than those in the previous
study [1]. There are two important resonant reactions:
3 He(d, p) 4 He and 3 H(d, n) 4 He. We adopt an analytic
reaction rate for variable nuclear binding energy [5].
For the 3He(d, p)4He reaction, the resonance is an
excited state of the compound nucleus 5Li*. For the3H(d, n)4He reaction the compound nucleus is 5He*. The
resonance energies are related to the excitation energy
in the compound nucleus and the net binding energiesof the reactants. We point out that there is a consistency
check on the δmq sensitivity of the forward 3He(d, p)4He
reaction from the reverse 4He(p, d)3He reaction [4]. Asa test on the robustness of the constraint on δmq /mq we
include the variations in the resonance energy based on
the parameters in this reverse channel.
In Fig. 1 we show primordial abundances as a functionof variations in the quark mass δmq /mq for a fixed valueof baryon-to-photon ratio η = 6.23 × 10−10 from WMAP 7
data for model ΛCDM+SZ+lens. The revised constraints
on 7Li and 4He do not confirm a concordance best fit fora positive value of δmq /mq = 0.016 ± 0.005 [1]. Rather,
the optimum concordance level is for much smaller
values consistent with δmq /mq = 0. Combining limits
from all nuclides (except 3He), we deduce conservative
concordance limits of −0.005 <~ δmq /mq <~ 0.007.
4
Since He and D abundances mainly determine theconcordance region, we present analytic formulas forthe dependence of the 4He and D abundances with quark
mass [4]. 6Li production in standard BBN occurs via the

KUSAKABE, Motohiko(University of Tokyo)

MATHEWS, Grant J.

(University of Notre Dame)

4He(d, γ)6Li reaction, and some consequence of a varying

quark mass on its abundance exists. Nevertheless, weshow that effects of a varying quark mass on the resonant
4He(d, γ)6Li reaction can be safely neglected [4].

Figure 1: Calculated light-element abundances as a function ofvariations in the quark mass δmq /mq. The blue solid lines
are for the case of no shifts in the resonance energies [1].
The dashed line corresponds to the resonances being
shifted the same energy as the ground state. The dotdashed line corresponds to an averaged value of theresonance sensitivity in the forward direction. The solid
green curve is new to the present study. It derives fromconsidering the reverse reaction for the determining thevariation of the resonance energy. The red boxes show
the allowed parameter regions for the case of the reverse
reaction determined using our adopted observational
constraints. Error bars at δmq /mq = 0 show theoreticaluncertainties in standard BBN [6]. This is reprinted from
[4].

References[1] Berengut, J. C., et al.: 2010, Phys. Lett. B, 683, 114.
[2] Flambaum, V. V.: 2008, Eur. Phys. JST, 163, 159.
[3] Flambaum, V. V., et al.: 2007, Phys. Rev. C, 76, 054002.
[4] Cheoun, M. K., et al.: 2011, Phys. Rev. D, 84, 043001.
[5] Cyburt, R. H.: 2004, Phys. Rev. D, 70, 023505.
[6] Cyburt, R. H., et al.: 2004, Phys. Rev. C, 78, 064614.

I Scientific Highlights

055

Gamow-Teller Strengths in Ni Isotopes and Electron Capture in
Gravitational Core-Collapse of Massive StarsSUZUKI, Toshio(Nihon University / NAOJ)

HONMA, Michio(University of Aizu)

Electron capture reactions play the most essential
roles in the core-collapse processes at the end of thelife-cycle of massive stars. Accurate evaluations of theelectron capture rates at high densities and temperatures
are important to determine the initial conditions for the
nucleosynthesis in supernova explosions [1].
Gamow-Teller (GT) transition strengths in Ni
isotopes are studied by shell model calculations withthe use of a new Hamiltonian in fp-shell, GXPF1J [2].
The GT strengths obtained are used to evaluate electron
capture rates at stellar environments [1]. Calculated GT
strength for 58Ni and 60Ni as well as the experimental
data[3,4] are shown in Fig. 1. Calculated sum of the GT
strengths obtained by GXPF1J is in fair agreement withobservation for both 58Ni and 60Ni. Calculated electron
capture rates for 58Ni and 60Ni are shown in Figs. 2.

KAJINO, Toshitaka(NAOJ / University of Tokyo)

OTSUKA, Takaharu(University of Tokyo)

calculations [3,4] as well as those by KB3G [5].
The capture rates for 56Ni, and neutron-rich 62Ni
and 64Ni isotopes as well as Co and Mn isotopes arealso investigated [6]. The GT strengths for GXPF1J
are generally more fragmented compared to those of
conventional Hamiltonians such as KB3G. The GT
distribution in 56Ni obtained by GXPF1 is found toreproduce the recent (p, n) reaction data [7].

Figure 2: Electron capture rates on 58Ni and 60Ni obtained for
GXPF1J and KB3G [5] as well as those obtained byexperimental GT strength [3,4].
Figure 1: The sum of GT strengths in (a) 58 Ni and (b) 60 Ni
up to the excitation energies (E x) of 58Co and 60Co.
Experimental data are taken from Refs. [3,4].

The calculated capture rates in 58Ni and 60Ni arefound to reproduce well the rates obtained by using theexperimental GT strengths [3,4]. Better evaluations of thecapture rates have been obtained compared with previous

056

I Scientific Highlights

References[1] Suzuki, et al.: 2011, Phys. Rev. C, 83, 044619.
[2] Honma, et al.: 2005, J. Phys. Conf. Ser., 20, 7; 2002, Phys. Rev.
C, 65, 061301(R); 2004, 69, 034335.
[3] Hagemann, et al.: 2004, Phys. Lett. B, 579, 251.
[4] Anantaraman, et al.: 2008, Phys. Rev. C, 78, 065803.
[5] Caurier, et al.: 2005, Rev. Mod. Phys., 77, 427.
[6] Suzuki, et al.: 2011, Prog. Part. Nucl. Phys., 66, 385.
[7] Sasano, et al.: 2011, Phys. Rev. Lett., 107, 202501.

Role of β-Decays of N = 126 Isotones in Supernova R-Process
Nucleosynthesis
SUZUKI, Toshio(Nihon University / NAOJ)YOSHIDA, Takashi(University of Tokyo)

The r-process is the promising nuclear process for thesynthesis of about a half of heavy elements beyond iron[1,2]. Study of the r-process element synthesis has been
done by considering neutrino-driven winds in supernova
explosions [3] as well as ONeMg supernovae [4] andneutron-star meregers [5].
The evaluation of β-decay rates, particularly at thewaiting point nuclei, is one of the important issues of thenucleosynthesis through the r-process. Investigations on
the β-decays of isotones with neutron magic number of
N= 82 have been done by various methods including shellmodel [6], QRPA/FRDM [7] as well as CQRPA [8] etc.,
which lead to results consistent to one another.
For the β-decays at N = 126 isotones, however, halflives obtained by various calculations differ to one
another [9]. First-forbidden (FF) transitions become
important for these nuclei in addition to the GamowTeller (GT) transitions in contrast to the case of N = 82.
Beta decays of the isotones with N = 126 are studied byshell model calculations taking into account both theGamow- Teller (GT) and first-forbidden (FF) transitions.
The FF transitions are found to be important to reduce thehalf-lives, by nearly twice to several times, from those by
the GT contributions only as shown in Fig. 1 [1].
The present half-lives of the shell model calculations
are shorter than those of the standard values of ref. [7]by 2.3 ~ 8.3 for even Z and by 1.4 ~ 2.0 for odd Z (except
for Z = 71), respectively. They increase monotonicallyas Z increases showing no odd-even staggering found in

KAJINO, Toshitaka(NAOJ / University of Tokyo)

OTSUKA, Takaharu(University of Tokyo)

FRDM’s. The present half-lives are longer than those ofRef. [8] by about 1.1 ~ 1.3 (1.5) for Z = 64 ~ 67 (68) andby twice for Z = 69 and 70, respectively.
Possible implications of the short half-lives of the
waiting point nuclei on the r-process nucleosynthesis
during the supernova explosions are investigated. We
use an analytic model for neutrino-driven winds [10] forthe time evolution of thermal profiles. The third peak of
the abundance of the elements in the r-process has beenfound to be shifted toward higher mass region as shownin Fig. 2. Although the magnitude of the shift is rather
modest, it is found to be a robust effect independent of
the present astrophysical conditions for the r-process aswell as the quenching factors of gA and gV adopted in theshell model calculations [1].

Figure 2: The abundances of elements in the r-process nucleosynthesis obtained by using the present β-decay halflives for the N=126 isotones (denoted as ‘modified’) andstandard half-lives of ref. [7] (denoted as ‘standard’).

Figure 1: (a) Calculated half-lives for the N = 126 isotones. Resultsof the present shell model calculations with GT andwith GT+FF transitions are denoted by dashed and solid
curves, respectively. Half-lives of Ref. [7] denoted as
FRDM are shown by a dotted curve.

References[1] Suzuki, T., et al.: 2012, Phys. Rev. C, 85, 015802.
[2] Burbridge, et al.: 1957, Rev. Mod. Phys., 29, 547; Cowan, et al.:1991, Phys. Rep., 208, 267; Kratz, et al.: 1993, ApJ, 216.
[3] Meyer, et al.: 1992, ApJ, 393, 656; Woosley, et al.: 1994, ApJ,
433, 229.
[4] Wanajo, et al.: 2006, Nucl. Phys. A, 777, 676.
[5] Freiburghaus, et al.: 1999, ApJ, 525, L121.
[6] Martinez-Pinedo, et al.: 2003, Phys. Rev. Lett., 75, 818.
[7] Moller, et al.: 1997, At. Data Nucl. Data Tables, 66, 131; 2003,
Phys. Rev. C, 67, 055802.
[8] Borzov, et al.: 2003, Phys. Rev. C, 67, 025802,[9] Langanke, et al.: 2003, Rev. Mod. Phys., 75, 818; Grawe, et al.:2007, Rev. Part. Phys., 70, 1525.
[10] Takahashi, et al.: 1997, Origin of Matter and Evolution of
Galaxies, eds. T. Kajino, S. Kubono, Y. Yoshii (Singapore:
World Scientific), 213.
[11] Nishimura, et al.: 2011, Phys. Rev. Lett., 106, 052501.

I Scientific Highlights

057

Asymmetric Neutrino Reaction from Magnetized Proto-Neutron Stars
in Fully Relativistic Framework
MARUYAMA, Tomoyuki(Nihon University)

KAJINO, Toshitaka

HIDAKA, Jun(NAOJ / University of Tokyo)		

(NAOJ)

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

Various phases of the hot and dense hadronic matterare interesting topics in nuclear, particle and astro
physics. The neutron star is the most possible target torealize these dense matter. Furthermore a new type ofneutron stars, called “magnetars”, with a super strong
magnetic field have been discovered [1]. In this study
only the neutrino emission is the observable information;it also gives us an interesting question as for the dense
matter. Neutrino emission as well as GW is the uniqueobservable that provides signals of the change of internal
structure of the neutron star [2]. Then, we have calculated
scattered and absorbed neutrinos in the hot and dense
hadrons with hyperons under strong magnetic field.
Here we assume that there is uniform magnetic fieldalong z-direction as B = Bẑ. Even astronomically strong→
magnetic field is still weaker than the strong interaction
order: √ ¯e B  μ a, where μ a is the chemical potentialof the particle a. We therefore treat the magnetic fieldin the perturbative way, ignore the contribution fromthe convective current, and thus consider only the spin
interaction. In this approximation the cross-section is
given as		σ = σ 0 + Δσ			(1)0where σ is independent of B, and Δσ is proportional to B.
Figure 1 shows Δσ of the neutrino scattering (νe → νe)
and absorption (νe → e−) in the upper and lower panels,
respectively, as a function of the incident neutrino angle
θi, where the magnetic field is set to be B = 2 × 1017 G,
and the initial neutrino energy is taken to be thechemical potential. We found that the scattering crosssections is maximum at θi = 0°, and that the absorption
cross section is minimum at θi = 0°. In addition theseresults are opposite at θi = 180°. These results lead to avery interesting phenomena that in the strong poloidal
magnetic field, the neutrinos are strongly absorpted in
the antarctic areas of the proto neutron-stars. This result
implies that the strong magnetic field could influence thepulser-kick of proto neutron stars.
As the next step, we applied the above results tocalculations of pulsar-kick in core-collapse supernovaeof the proto neutron-star. In these calculations wesolved the Boltzmann equation using a one-dimensional
attenuation method. Then, we obtain the kick velocity of
about 600 km/s for the MNS = 1.68 M isothermal modelwith T = 20 MeV when the magnetic field is uniformly
poloidal, with its strength B = 2 × 1017 G.

058

I Scientific Highlights

YASUTAKE, Nobutoshi(Chiba Institute of Technology)

MATHEWS, Grant J.

(University of Notre Dame)

Figure 1: (Color online) Ratios of the magnetic part of thescattering cross-sections ΔσS and those of the absorption
cross-sections Δσ A for B = 2 × 10 17 G, to the crosssections without a magnetic-field σ 0S,A at T = 20 MeV.
Dotted, dashed and solid lines represent the results fordensities of ρB = ρ0, 3ρ0 and 5ρ0, respectively.

References[1] Reddy, S., Prakash, M., Lattimer, J. M.: 1998, Phys. Rev. D, 58,
013009.
[2] Arras, P., Lai, D.: 1999, Phys. Rev. D, 60, 043001.
[3] Maruyama, T., et al.: 2011, Phys. Rev. D, 83, 081303(R).

Nonlinear Neutrino Oscillations in Astronomy
PEHLIVAN, Y.

BALANTEKIN, A. B.

KAJINO, Toshitaka(Mimar Sinan University) (University of Wisconsin, Madison) (NAOJ / University of Tokyo)

Nonlinear neutrino flavor conversion is investigatedby neutrino-neutrino scatterings in the presence of astrong neutrino background and plays an important rolein some astronomical sites such as the type II supernovae,
the early Universe, and possibly the sites of the gamma
ray bursts [1]. In particular, the forward scattering and theflavor exchange diagrams shown in Fig. 1 play a central
role because they undergo coherent superposition andtherefore have a dominant contribution [2]. These terms
also couple the evolutions of neutrinos with different
energies and turn the flavor conversion of neutrinos into a
nonlinear many-body problem.
We investigate the flavor evolution of neutrinos

(a)

(b)

Figure 1: ν − ν scattering diagrams corresponding to (a) forward
scattering (b) and flavor exchange.

undergoing vacuum oscillations and self interactionsin an isotropic and homogeneous environment in theabsence of a net leptonic background [3]. Assuming
a two neutrino mixing scenario, we point out that theresulting flavor evolution has the same dynamics and thesame symmetries as i) spins in a system with spin-spin
interactions and ii) pair occupation numbers in a systemwith BCS type pairing [3]. All three of these systems aredescribed by an effective Hamiltonian in the form
(1)
In the case of neutrinos, the fundamental
degree of→freedom is the neutrino isospin J which is defined interms of a multiplet of neutrino states [4]. Other relevant
quantities and the corresponding physical degrees of
freedom are summarized in the following table:

→

J

ω
μ

Neutrino Flavor
Evolution

Interacting Spin
SystemNeutrino isospin
Vacuum oscillation
frequency

Spin
Gyromagneticratio
Spin-spin
coupling

Neutrino density

BCS Pairing

YOSHIDA, Takashi(University of Tokyo)

neutrino flavor evolution possesses hidden dynamical
symmetries which manifest themselves in terms of thefollowing set of conserved quantities [3,5]:(2)
The existence of these conserved quantities make thesystem completely integrable and we can write the exact
eigenstates and eigenvalues using the method of Bethe
ansatz [3]. Such invariants always simplify the analysis ofcomplex systems. Here we neglected leptonic asymmetry
in comparison to the neutrino background which can
only be justified in the early Universe. But even when theassumptions which guarantee the existence of constantsof motion (including the homogeneity and isotropy of thespace) are broken, they can still provide a convenient setof variables which behave in a relatively simple mannerdepending on how drastic the symmetry breaking is.
The symmetries of the Hamiltonian lead tovarious collective flavor oscillation modes such as thesynchronized oscillations and spectral splits [1,3,6]
which may be manifest in a future supernova signal.
For example, the analogy between self interacting
neutrinos and the BCS pairing system offers an intuitive
description of neutrino spectral splits in terms of theconserved quantities. Namely, the method of Bogoliubovtransformation borrowed from BCS theory can describe
the neutrinos in terms of noninteracting quasi-particle
degrees of freedom whose adiabatic evolution from ahigh density region into the vacuum (like the neutrinos
emanated from a supernova) results in the splits ofneutrino spectra [3]. A full survey of the symmetries andthe associated constants of motion of self interacting
neutrinos from the point of view of the emergent
collective flavor oscillation modes remains to be an open
problem for future research.
References[1] Duan, H., et al.: 2010, Annu. Rev. Nucl. Part. Sci., 60, 569.
[2] Pantaleone, J. T.: 1992, Phys. Lett. B, 287, 128.
[3] Pehlivan, Y., et al.: 2011, Phys. Rev. D, 84, 065008.
[4] Balantekin, A. B., Pehlivan, Y.: 2007, J. Phys. G, 34, 47.
[5] Gaudin, M.: 1976, J. Physique, 37, 1087.
[6] Raffelt, G. G., Smirnov, A. Y.: 2007, Phys. Rev. D, 76, 125008.

Pair quasispin
Single particle
energy level
Pairing strength

Based on these observations, we point out that the

I Scientific Highlights

059

Properties of the Proto-Neutron Star with Smeared Trapped Neutrinos
RYU, Chung-Yeol, CHEOUN, Myung-Ki

KAJINO, Toshitaka(Soongsil University)		

(NAOJ / University of Tokyo)

We investigate the structure of a proto-neutronstar (PNS) with trapped neutrinos by using quantum
hadrodynamics (QHD). Ratios of the trapped neutrinos
and corresponding leptons to the baryons are usuallyassumed as a constant. But relevant reactions associatedto the beta equilibrium could be sensitive to the given
density and temperature. By adopting a phenomenologicallepton density which is smeared near the surface, we
calculate and discuss populations of baryons and leptons,
equations of state and the mass-radius relation of a PNS
in isentropic process (S = 2).
Calculation for a neutron star is usually constrainedby three conditions, baryon number conservation, charge
neutrality and beta equilibrium. But for a PNS withtrapped neutrinos, the beta equilibrium has to be modified
with trapped neutrinos μν,(2)where β = 0.05 and γ = 2 are used. When we ignore themass of a electron, x(ρ) is nearly x(ρ) ≈ 0.5 for μe = μν
because the degeneracy factor of neutrino is 1. Since thecondition, x(ρ) > 0.5, means proton rich matter, we takethe x(ρ) as x < 0.5 in all regions of a PNS. Thus, in thiswork, we use x0 = 0.3. This ratio function implies smoothsmearing of relevant leptons at the surface of a PNS.
With these formula and conditions, we obtained
populations of neutrinos in Fig. 1. When comparing our
results with the simple fixed lepton model [1], the ratioof neutrinos from our formula agrees with those fromthe simulation of transport theory [2,3]. We thus think
our assumptions can explain the results of the simulationand give a physical insight for a PNS. Although ourmodel does not have time evolution, it suggests a
phenomenological model about the trapped neutrino
which can be or might be reproduced by the realistic
dynamical model.

060

I Scientific Highlights(Nihon University)

0.1
0.08 ν
e
νµ
0.06
0.04
0.02
0

0

2

4

6

8

10

6

8

10

ρ/ρ0
0.1
0.08 ν
e
νµ
0.06
Yi

(1)
In the beta equilibrium, the matter becomes symmetricmatter if μ e = μ ν . By considering that the neutrino
propagation and the beta equilibrium may depend on
density and temperature, density of electron neutrinos, ρνe ,is assumed to be related as ρνe = x(ρ)ρe. The condition formuon production is also taken as ρνμ = x(ρ)ρμ by satisfying
the chemical equilibrium μe +μνe = μμ +μνμ . Here x(ρ) may
depend on baryon density and temperature. However, tomake the problem simple, we assume that x(ρ) depends
on baryon density by using a phenomenological formula,

MARUYAMA, T.

Yi

		

0.04
0.02
0

0

2

4
ρ/ρ0

Figure 1: Population of neutrinos in nucleonic phase (npν) (upper)and hyperonic one (npHν) (lower) for density dependent
YLe model in S = 2 isentropic process.

References[1] Prakash, M., et al.: 1997, Phys. Rep., 280, 1.
[2] Burrows, A., Lattimer, J. M.: 1986, ApJ, 307, 178.
[3] Ryu, C. Y., et al.: 2011, Phys. Rev. C, 83, 018802.

Reactions on 40Ar involving solar neutrinos and neutrinos
from core-collapsing supernovae
CHEOUN, Myung-Ki, HA, Eunja

KAJINO, Toshitaka(Soongsil University)		

800
σν (10-42 cm2 )Neutrino (ν) reactions on 40Ar were of astrophysicalimportance because the reactions are used to detect
the solar ν emitted from 8B via the pp-chains in thesun through the liquid argon time projection chamber(LArTPC) in the ICARUS (Imaging of Cosmic and Rare
Underground Signals) [1]. Since the maximum energy ofthe solar ν is thought to be about 17 MeV in the standard
solar model, the ν reactions are sensitive to discreteenergy states of 40Ar. The Q-value for the 40Ar(νe , e−)40K*
reaction is 1.50 MeV while it is 7.48 MeV for the 40Ar(ν̄e ,e+)40Cl* reaction. Therefore, 40Ar(ν̄e , e+)40Cl* reactions
might be kinematically disfavored in the low energy νsuch as solar ν’s. In this respect, 40Ar was claimed toeffectively distinguish the νe and ν̄e emitted from the sun.
Recently, Ref. [1] revised previous work by focusing
on the possible detection of ν oscillation of supernova(SN) ν’s. The ν’s from the SN explosion can give valuable
information about the ν properties, because they traverse
regions of dense matter in the exploding star where
matter enhanced oscillations take place.
Since ν energies from the SN explosion are expected
to be higher than the solar ν [2], one needs to consider
the contributions from higher multi-pole transitions.
Moreover ν(ν̄) energies and flux emitted from the corecollapsing SN explosion are believed to be peaked froma few to tens of MeV energy region [2]. Therefore, theν(ν̄)-induced reactions on 40Ar are sensitive to the higher
excited states of the nucleus beyond nucleon thresholds,
which eventually decay to lower energy states with theemission of some particles.
Here we report more advanced results [3] based on the
QRPA calculation for ν(ν̄)-40Ar reactions by solar and SN
ν’s, whose energy ranges are considered up to 30 and 80
MeV region, respectively. In particular, we focus on rolesof higher excited states around 20 MeV although they
are not verified at the experiments. Our results decrease
the cross sections of 40Ar(νe , e−)40K* reaction about 3.5
times and increase about twice those of 40Ar(ν̄e , e+)40Cl*
reaction compared to the previous calculations [1].
Consequently, the expected 12 times difference between
the reactions at Ev= 80 MeV is drastically reduced about
twice, as shown in Fig. 1 [3].
Other related ν-reactions on 40 Ar target throughcharged and neutral currents are shown in Fig. 2.

(NAOJ / University of Tokyo)

600
400

0

Ar40-CC-EN-CS

012340+
+
1
2+
3+
4+
total

200

0

10

20

30

40
50
E ν (MeV)

60

70

80

Figure 1: (Color online) Cross sections by CC current, 40Ar(νe,e−)40K*, for solar and SN ν’s.

Ar40-CS1000σν (10-42 cm2 )

			

100
10

Ar40-CC-AEN
Ar40-CC-EN
Ar40-NC-AEN
Ar40-NC-EN

1
0.1

0

10

20

30

40
50
Eν (MeV)

60

70

80

Figure 2: (Color online) Comparison of cross sections for relevantν reactions on 40Ar for SN ν’s.

References[1] Gil-Botella, I., Rubbia, A.: 2003, J. Cosmol. Astropart. Phys.,
10, 009.
[2] Yoshida, T., et al.: 2008, ApJ, 686, 448.
[3] Cheoun, M.-K., Ha, E., Kajino, T.: 2011, Phys. Rev. C, 83,028801.

I Scientific Highlights

061

The r-Process in Metal Poor Stars and Black Hole Formation
BOYD, R. N.

					(LLNL)MOTIZUKI, Y.

(RIKEN Nishina Center)

FAMIANO, M. A.

(Western Michigan University)

KAJINO, Toshitaka(NAOJ / University of Tokyo)

Historically r-process studies focused on the ubiquityof the r-process, i.e., the similarity of the r-process
abundances in extremely metal poor (EMP) stars to
those of the Solar system. In the past decade, however, anumber of EMP stars, which might have been thought toexhibit the r-process abundances, have been observed tohave abundances very different from those of the standard
r-process [1]. They have led to the suggestion that theirabundances are produced by two classes of progenitor
star r-processes.

Figure 1: EMP abundance data and r-process calculations [2]using the ref. [6] trajectories, but summing results fromtrajectory 24 to some later trajectory. The successive
curves include trajectory 24, 24–26, 24–28, 24–30, 24–31, 24–32, and 24–40. The sums to higher trajectories
make both the mass 130 and 195 r-process peaks. Data
are from [6].

Our papers [2,3] propose one primary site for the
r-process, i.e., core-collapse supernovae. Then the
r-process outliers result from progenitor stars that lie inthe 25-40 solar mass range; these stars are thought tobecome supernovae by first collapsing to a neutron star,then having fallback onto the nascent neutron star to
exceed the maximum mass for a neutron star, producing
a black hole [4]. Progenitor stars more massive than
40 solar masses would collapse directly to black holes,
adding no r-process material to the interstellar medium,
whereas stars less massive than 25 solar masses would
expel relatively large amounts to the ISM. In the 25–
40 solar mass range some r-process material would be
expelled to the ISM through hydrodynamic fluctuations
that would produce regions with radial velocities in062

I Scientific Highlights

MEYER, B. S.

(Clemson University)

ROEDERER, I. U.

(Carnegie Observatories)

excess of the black hole escape velocity. The amountof material expelled would vary with the mass of theprogenitor star, since the more (less) massive stars would
remain as neutron stars for times that approaches zero
(infinity).
We [2] applied the approach of [5], which described
the r-process as occurring in the neutrino driven windfrom a core-collapse supernova in 40 trajectories(thin shell wind elements), all originating within thestar, but having different initial density, temperature,
entropy, and electron fraction. Processing conditions forindividual trajectories evolved with time and trajectory
identity. Different trajectories were emitted from thestar successively, but ceased when the collapse to theblack hole occurred, consistent with [5] in which thetotal emissions of the trajectories generated a good
representation of the Solar r-process abundances. Our
calculations are described in more detail in [2].
Our results are shown in the Fig. 1. There it canbe seen that truncating the r-process at increasing
trajectory number terminates the r-process at increasingly
higher mass. Note that although the curve representing
trajectories 24 through 31 does reach the mass 195
u peak, the abundances in that region are nearly twoorders of magnitude below that of the full r-process,which would render the higher mass nuclides difficult
to observe. The abundances for that scenario would
therefore appear observationally to terminate at a massof about 140 u. The figure shows that the tr-process
predictions do produce a qualitative representation of theobserved abundances for the outlier stars, suggesting that
all of these stars can be represented by a single r-process,provided that the truncation possibility is allowed.
References[1] Roederer, I. U., et al.: 2010, ApJ, 724, 975.
[2] Boyd, R. N., et al.: 2012, ApJ, 744, L14.
[3] Boyd, R. N., et al.: 2011, Proc. OMEG, 11, to be published.
[4] Heger, A., et al.: 1992, ApJ, 591, 288.
[5] Woosley, et al.: 1994, ApJ, 433, 229.
[6] Käppeler, F., et al.: 1989, Rep. Prog. Phys., 52, 945.

II Publications, Presentations
1. Refereed Publications
Abadie, J., et al. including Hayama, K., Izumi, K., Mori, T.:2011, A gravitational wave observatory operating beyond thequantum shot-noise limit, Nature Phys., 7, 962-965.
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S5 LIGO data, Phys. Rev. D, 85, 022001.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2011,
Search for Gravitational Wave Bursts from Six Magnetars, ApJ,
734, L35.
Abadie, J., et al. including Hayama, K., Kawamura, S.: 2011,
Search for gravitational waves from binary black hole inspiral,merger, and ringdown, Phys. Rev. D, 83, 122005.
Abadie, J., et al. including Hayama, K.: 2011, Directional Limits
on Persistent Gravitational Waves Using LIGO S5 Science
Data, Phys. Rev. Lett., 107, 271102.
Abadie, J., et al. including Hayama, K.: 2011, Beating the Spindown Limit on Gravitational Wave Emission from the Vela
Pulsar, ApJ, 737, 93.
Abramov-Maximov, V. E., Gelfreikh, G. B., Kobanov, N. I.,
Shibasaki, K., Chupin, S. A.: 2011, Multilevel Analysis ofOscillation Motions in Active Regions of the Sun, Sol. Phys.,
270, 175-189.
Abramov-Maximov, V. E., Gelfreikh, G. B., Shibasaki, K.:
2011, Quasi-periodic Oscillations of Solar Active Regions inConnection with Their Flare Activity - NoRH Observations,Sol. Phys., 273, 403-412.
Abramowski, A., et al. including Hada, K., Kino, M., Nagai, H.:
2012, The 2010 Very High Energy γ-Ray Flare and 10 Years ofMulti-wavelength Observations of M 87, ApJ, 746, 151.
Aikawa, Y., Kamuro, D., Sakon, I., Itoh, Y., Terada, H., Noble, J.
A., Pontoppidan, K. M., Fraser, H. J., Tamura, M., Kandori, R.,
Kawamura, A., Ueno, M.: 2012, AKARI observations of ice
absorption bands towards edge-on young stellar objects, A&A,
538, 57-68.
Albrecht, S., Winn, J. N., Johnson, J. A., Butler, R. P., Crane, J. D.,
Shectman, S. A., Thompson, I. B., Narita, N., Sato, B., Hirano, T.,
Enya, K., Fischer, D.: 2011, Two Upper Limits on the RossiterMcLaughlin Effect, with Differing Implications: WASP-1 has aHigh Obliquity and WASP-2 is Indeterminate, ApJ, 738, 50.
Araki, M., Takano, S., Yamabe, N., Koshikawa, H., Tsukiyama, K.,
Nakane, A., Okabayashi, T., Kunimatsu, A., Kuze, N.: 2012, A
Search for Interstellar Carbon-Chain Alcohol HC4OH in StarForming Region L1527 and Dark Cloud TMC-1, ApJ, 744, 163.
Archinal, B. A., et al. including Fukushima, T.: 2011, Report of the
IAU Working Group on Cartographic Coordinates and Rotational
Elements: 2009, Celest. Mech. Dyn. Astron., 109, 101-135.
Aretxaga, I., Wilson, G. W., Aguilar, E., Alberts, S., Scott, K. S.,
Scoville, N., Yun, M. S., Austermann, J., Downes, T. P., Ezawa,
H., Hatsukade, B., Hughes, D. H., Kawabe, R., Kohno, K.,
Oshima, T., Perera, T. A., Tamura, Y., Zaballos, M.: 2011,

AzTEC Millimeter Survey of the COSMOS Field – III. Source
Catalog Over 0.72 sq. deg. and Plausible Boosting by LargeScale Structure, MNRAS, 415, 3831-3850.
Aspin, C., Beck, T. L., Davis, C. J., Froebrich, D., Khanzadyan,T., Magakian, T. Yu., Moriarty-Schieven, G. H., Movsessian, T.
A., Mitchison, S., Nikogossian, E. G., Pyo, T.-S., Smith, M. D.:
2011, CSO Bolocam 1.1 mm Continuum Mapping of the Braid
Nebula Star Formation Region in Cygnus OB7, AJ, 141, 139.
Barbary, K., et al. including Hattori, T., Kashikawa, N.: 2011,
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Barbary, K., et al. including Hattori, T., Kashikawa, N.: 2011,
The Hubble Space Telescope Cluster Supernova Survey. II. The
Type Ia Supernova Rate in High-redshift Galaxy Clusters, ApJ,
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Barker, M. K., Ferguson, A. M. N., Irwin, M. J., Arimoto, N.,
Jablonka, P.: 2012, Quantifying the faint structure of galaxies:
the late-type spiral NGC 2403, MNRAS, 419, 1489-1506.
Barro, G., Perez-Gonzalez, P. G., Gallego, J., Ashby, M. L. N,
Kajisawa, M., Miyazaki, S., Yamada, T., Zamorono, J.: 2011,
UV-to-FIR Analysis of Spitzer/IRAC Sources in the Extended
Groth Strip. II. Photometric Redshifts, Stellar Masses, and Star
Formation Rates, ApJS, 193, 30-64.
Batista, V., et al. including Fukui, A.: 2011, MOA-2009-BLG387Lb: a massive planet orbiting an M dwarf, A&A, 529, A102.
Bayo, A., Barrado, D., Stauffer, J., Morales-Calderón, M., Melo, C.,
Huélamo, N., Bouy, H., Stelzer, B., Tamura, M., Jayawardhana,R.: 2011, Spectroscopy of very low mass stars and browndwarfs in the Lambda Orionis star forming region. I. Enlarging
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Bekki, K., Tsujimoto, T.: 2011, Formation of the Galactic bulge
from a two-component stellar disc: explaining cylindrical rotation
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Bellagamba, F., Maturi, M., Hamana, T., Meneghetti, M.,
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to the COSMOS field, MNRAS, 413, 1145-1157.
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Boyd, R. N., Famiano, M., Meyer, B. S., Motizuki, Y., Kajino, T.,
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Boyd, R. N., Kajino, T., Onaka, T.: 2011, Supernovae, Neutrinos, andthe Chirality of the Amino Acids, Int. J. Mol. Sci., 12 , 3432-3444.
Burningham, B., Leggett, S. K., Homeier, D., Saumon, D., Lucas,
P. W., Pinfield, D. J., Tinney, C. G., Allard, F., Marley, M.

II Publications, Presentations

063

S., Jones, H. R. A., Murray, D. N., Ishii, M., Day-Jones, A.,
Gomes, J., Zhang, Z. H.: 2011, The properties of the T8.5p
dwarf Ross 458C, MNRAS, 414, 3590.
Carollo, D., Beers, T. C., Bovy, J., Sivarani, T., Norris, J. E.,
Freeman, K. C., Aoki, W., Lee, Y. S., Kennedy, C. R.: 2012,
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Cheoun, M. K., Ha, E., Kajino, T.: 2011, Neutrino reactions on
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Rev. C, 83, 028801.
Cheoun, M. K., Kajino, T., Kusakabe, M., Mathews, G. M.: 2011,
Time Dependent Quark Masses and Big Bang Nucleosynthesis
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Choi, M., Kang, M., Tatematsu, K., Lee, J.-E., Park, G.: 2011,
Radio Imaging of the NGC 1333 IRAS 4A Region: Envelope,
Disks, and Outflows of a Protostellar Binary System, PASJ, 63,
1281-1291.
Chorley, N., Foullon, C., Hnat, B., Nakariakov, V. M., Shibasaki, K.:
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A&A, 529, A123.
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074

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Katsukawa, Y., Suematsu, Y., Shimizu, T., Ichimoto, K., Takeyama,
N.: 2011, Focal plane instrument for the Solar UV-Vis-IR
Telescope aboard SOLAR-C, Proc. of the SPIE, 8148, Eds. S.
Fineschi, J. Fennelly, 81480E.
Kawabata, K. S., Nagae, O., Chiyonobu, S., Tanaka, H., Miyamoto,H., Nakaya, H., Suzuki, M., Kamata, Y., Miyazaki, S., Hiragi,K., Yamanaka, M., Arai, A., Yamashita, T., Uemura, M., Ohsugi,T., Isogai, M., Ishitobi, Y., Sato, S.: 2011, Wide-Field One-Shot
Optical Polarimeter: HOWPol, ASP Conf. Ser. 449, 83.
Kiuchi, H., Kawanishi, T.: 2011, Photonic millimeter-wave/
microwave signal generation and transmission techniques for ahigh-frequency Radio Interferometer and a very large anttena
array, XXX URSI General Assembly and Scientific Symp. ofInt. Union of Radio Science, 978-1-4244-6051-9/11/$26.00 ©
2011 IEEE.
Komugi, S., Tosaki, T., Kohno, K., Tsukagoshi, T., Tamura, Y.,
Miura, R., Onodera, S., Kuno, N., Kawabe, R., Nakanishi,K., Sawada, T., Ezawa, H., Wilson, G. W., Yun, M. S., Scott,
K. S., Hughes, D. H., Aretxaga, I., Perera, T. A., Austermann,
J. E., Tanaka, K., Muraoka, K., Egusa, F.: 2011, Cold Dust andits Heating Sources in M 33, Proc. IAU Symp. 277, Eds. C.
Carignan, F. Combes, K. C. Freeman, 26-29.
Kudo, N., Torii, K., Machida, M., Takahashi, K., Nozawa, S.,
Yamamoto, H., Okuda, T., Kawamura, A., Mizuno, N., Onishi,T., Matsumoto, R., Fukui, Y.: 2011, Molecular Loops in the
Galactic Center; The Physical Condition in the Whole Loops,
ASP Conf. Ser. 439, Eds. M. R. Morris, Q. D. Wang, F. Yuan, 69.
Kuno, N., Tosaki, T., Onodera, S., Miura, R., Muraoka, K.,
Komugi, S., Sawada, T., Nakanishi, K., Kohno, K., Kaneko,
H., Hirota, A., Arimoto, N., Nakanishi, H., Kawabe, R.: 2011,
NRO Legacy Project: M33 all Disk Survey of Giant Molecular
Clouds with NRO 45-m and ASTE 10-m telescopes, Proc. IAU
Symp. 277, Eds. C. Carignan, F. Combes, K. C. Freeman, 67-70.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110402A: MITSuME okayama and ishigakijima optical
upper limits, GRB Coordinates Network, Circular Service,
11873, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110414A: MITSuME Ishigakijima Optical upper limits,
GRB Coordinates Network, Circular Service, 11940, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110422A: MITSuME Ishigakijima Optical Observation,
GRB Coordinates Network, Circular Service, 11972, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110709A: MITSuME Ishigakijima Optical upper limits,
GRB Coordinates Network, Circular Service, 12139, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110726A: MITSuME Ishigakijima Optical Observation,
GRB Coordinates Network, Circular Service, 12204, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,

GRB 110731A: MITSuME Ishigakijima Optical Upper Limits,
GRB Coordinates Network, Circular Service, 12226, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110801A: MITSuME Ishigakijima Optical Observation,
GRB Coordinates Network, Circular Service, 12233, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110801A: MITSuME Ishigakijima Optical Observation
at 1 day after the burst, GRB Coordinates Network, CircularService, 12240, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 110820A: MITSuME Ishigakijima Optical upper limits,
GRB Coordinates Network, Circular Service, 12293, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2011,
GRB 111029A: MITSuME Ishigakijima Optical upper limits,
GRB Coordinates Network, Circular Service, 12511, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120212A: MITSuME Ishigakijima Optical Observation,
GRB Coordinates Network, Circular Service, 12947, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120308A: MITSuME Ishigakijima Optical Upper Limits,
GRB Coordinates Network, Circular Service, 13026, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120326A: MITSuME Ishigakijima Optical Observation
at 2 days afterthe burst, GRB Coordinates Network, CircularService, 13170, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120326A: MITSuME Ishigakijima Optical Observation
at 3 days afterthe burst, GRB Coordinates Network, CircularService, 13177, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120327A: MITSuME Ishigakijima Optical Observation,
GRB Coordinates Network, Circular Service, 13156, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120327A: MITSuME Ishigakijima Optical Upper Limits
at 1 day afterthe burst, GRB Coordinates Network, CircularService, 13169, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120328A: MITSuME Ishigakijima Optical Upper Limits,
GRB Coordinates Network, Circular Service, 13171, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120326A:
MITSuME Ishigakijima Optical Observation, GRB Coordinates
Network, Circular Service, 13155, 1.
Kuroda, D., Hanayama, H., Yanagisawa, K., Shimizu, Y., Toda,
H., Miyaji, T., Watanabe, J., Nagayama, S., Yoshida, M.,

Ohta, K., Kawai, N.: 2011, GRB 110407A: MITSuME okayama
and ishigakijima optical upper limits, GRB Coordinates
Network, Circular Service, 11905, 1.
Kuroda, D., Hanayama, H., Yanagisawa, K., Shimizu, Y., Toda,
H., Miyaji, T., Watanabe, J., Nagayama, S., Yoshida, M., Ohta,
K., Kawai, N.: 2011, GRB 110915A: MITSuME Okayama andIshigakijima Optical upper limits, GRB Coordinates Network,
Circular Service, 12344, 1.
Kuroda, D., Hanayama, H., Yanagisawa, K., Shimizu, Y., Toda,
H., Miyaji, T., Watanabe, J., Nagayama, S., Yoshida, M., Ohta,
K., Kawai, N.: 2012, GRB 120211A: MITSuME Okayama andIshigakijima Optical upper limits, GRB Coordinates Network,
Circular Service, 12929, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB 110414A:
MITSuME Okayama Optical Upper Limits, GRB Coordinates
Network, Circular Service, 11938, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB 110530A:
MITSuME Okayama Optical Observation, GRB Coordinates
Network, Circular Service, 12053, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB 111123A:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 12591, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2011, GRB 111210A:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 12659, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120106A:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 12814, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120215A:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 12960, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120219A:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 12969, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120311B:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 13046, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120320A:
MITSuME Okayama Optical upper limits, GRB Coordinates
Network, Circular Service, 13082, 1.
Kuroda, D., Yanagisawa, K., Yoshida, M., Shimizu, Y.,
Nagayama, S., Toda, H., Ohta, K., Yatsu, Y., Kawai, N.: 2011,
The development of an automatic reduction system for GammaRay Burst afterglow, Proc. of Telescopes from Afar Conf.
Kusakabe, M., Kajino, T., Mathews, G. M.: 2011, SUSY-catalyzed
big bang nucleosynthesis as a solution of lithium problems, J.
Phys.: Conf. Ser., 312, 42012.

II Publications, Presentations

075

Kusakabe, N., Tamura, M., Kandori, R., Kudo, T., Hashimoto,J.: 2011, Strategic Exploration of Exoplanets and Disks with
Subaru: SEEDS, Proc. IAU Symp. 276, Ed. A. Sozzetti.
Lee, M. G., Lim, S., Park, H. S., Hwang, H. S., Hwang, N.: 2011,
Wandering Globular Clusters: the First Dwarf Galaxies in the
Universe?, EAS Publ. Ser., 48, Eds. M. Koleva, Ph. Prugniel, I.
Vauglin, 243-248.
Li, J., Shen, Z.-Q., Miyazaki, A., Huang, L., Sault, R. J., Miyoshi,M., Tsuboi, M., Tsutsumi, T.: 2011, Flaring Emission from
Sagittarius A* at Millimeter Wavelengths, ASP Conf. Ser. 439,
Eds. M. R. Morris, Q. D. Wang, F. Yuan, 319.
Maruyama, T., Yasutake, N., Kajino, T., Cheoun, M. K., Ryu, C.
Y.: 2011, Asymmetric Neutrino Reactions from MagnetizedProto-Neutron Stars in fully Relativistic Framework including
Hyperons, AIP Conf. Proc. 1377, 389-391.
Matsuo, H., Matsuo, T., Ohta, I. S.: 2011, A Study on Photon
Counting Interferometry in Terahertz Frequencies, NRAO
ISSTT Proceedings, Eds. C. Walker, C. Groppi, 62.
Mawet, D., et al. including Nishikawa, J., Tamura, M.: 2011,
Taking the vector vortex coronagraph to the next level forground- and space-based exoplanet imaging instruments: reviewof technology developments in the USA, Japan, and Europe,
Proc. of the SPIE, 8151, Ed. S. Stuart.
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.: 2011, Direct
imaging of bridged twin protoplanetary disks in a young
multiple star, Proc. IAU Symp. 276, Ed. A. Sozzetti.
Miyoshi, M., et al. including Furuya, R.-S., Kawaguchi, N.,
Nakajima, J., Irimajiri, Y., Koyama, Y.: 2011, A First Black
Hole Imager, Caravan-sub at Andes, ASP Conf. Ser. 439, Eds. M.
R. Morris, Q. D. Wang, F. Yuan, 279-280.
Miyoshi, M., Oyama, T., Shen, Z., Takahashi, R., Kato, Y.: 2011,
Oscillation Phenomena in Sagittarius A*, ASP Conf. Ser. 439,
Eds. M. R. Morris, Q. D. Wang, F. Yuan, 336-339.
Miyoshi, M., Oyama, T., Shen, Z.: 2011, VLBA Synthesis
Imagings of SgrA* at 43 GHz, ASP Conf. Ser. 439, Eds. M. R.
Morris, Q. D. Wang, F. Yuan, 386-388.
Miyoshi, M.: 2011, Slit-Modulation Imaging Method for Detecting
Periodic Structural Change in SgrA*, ASP Conf. Ser. 439, Eds.
M. R. Morris, Q. D. Wang, F. Yuan, 384.
Moritani, Y., Nogami, D., Okazaki, A. T., Imada, A., Kambe,
E., Honda, S., Hashimoto, O., Ichikawa, K.: 2011, Optical
spectroscopic observations of the Be/X-Ray binary A0535+262/
V725 Tau during the giant outburst in 2009, Proc. IAU Symp.
272, Eds. C. Neiner, G. Wade, G. Meynet, G. Peters, 18-19.
Morota, T., Ishihara, Y., Sasaki, S., Goossens, S., Matsumoto,K., Noda, H., Araki, H., Hanada, H., Tazawa, S., Kikuchi,
F., Ishikawa, T., Tsuruta, S., Haruyama, J., Ohtake, M.: 2011,
Lunar mare volcanism: lateral heterogeneity in eruptional
activity and relationship with crustal structure, Proc. 44th ISAS
Lunar. Planet. Symp., Abstract #44-07.
Nakajima, T., Iwashita, H., Miyazawa, C., Yonezu, T., Kuno,
N., Kawabe, R., Inoue, H., Sakai, T., Kohno, K., Koyano, M.,
Katase, T., Nishimura, A., Kimura, K., Ogawa, H., Asayama,S., Noguchi, T.: 2011, Development of the Sideband-Separating

076

II Publications, Presentations(2SB) Receiver Systems for the NRO 45-m Millimeter Wave
Telescope, Proc. of the 12th Workshop on Submillimeter-wave
Receiver Technologies in Eastern Asia, 14.
Nakamura, K.: 2012, Construction of gauge-invariant variables
for linear-order metric perturbations on general backgroundspacetime, 21st Workshop on General Relativity and Gravitationin Japan, Eds. Y. Ito, T. Futamase, et al.
Narukage, N., et al. including Tsuneta, S., Bando, T., Kano, R.,
Kubo, M., Ishikawa, R., Hara, H., Suematsu, Y., Katsukawa,Y.: 2011, Overview of Chromospheric Lyman-Alpha
SpectroPolarimeter (CLASP), Proc. of the SPIE, 8148, Eds. S.
Fineschi, J. Fennelly, 81480T.
Niino, Y.: 2011, High-Metallicity Host Galaxies and The Metallicity
Dependence of Long Gamma-Ray Bursts, AIP Conf. Proc.
1358, Eds. J. E. McEnery, J. L. Racusin, N. Gehrels, 275-278.
Nishiyama, S., Hatano, H., Tamura, M., Nagata, T.: 2011, NearInfrared Polarimetry toward the Galactic Center - Magnetic
Field Configuration in the Central One Degree Region, ASP
Conf. Ser. 439, Eds. M. R. Morris, Q. D. Wang, F. Yuan.
Noda, H., Kunimori, H., Araki, H., Fuse, T., Hanada, H.,
Katayama, M., Otsubo, T., Sasaki, S., Tazawa, S., Tsuruta, S.,
Funazaki, K., Taniguchi, H., Murata, K.: 2012, Lunar Laser
Ranging Experiment for SELENE-2, 43rd Lunar and Planetary
Science Conference, #1855.
Oe, M., Onodera, Y., Murai, J.: 2011, Early survey report on ICT
disaster recovery activities in the Great East Japan Earthquake,
Int. Symp. on Disaster Simulation & Structural Safety in the
Next Generation, 2011, 443-447.
Ohishi, M., Hanisch, R. J., Norris, R. P., Andernach, H., Bishop,M., Griffin, E., Kembhavi, A., Murphy, T., Pasian, F.: 2011,
Commission 5: Documentation and Astronomical Data, Proc.
IAU Symp., Ed. I. Corbet, 327-334.
Ohishi, M.: 2011, Impact to the radio astronomy by the interference
caused by the solar power satellite systems, XXX URSI General
Assembly and Scientific Symp. of Int. Union of Radio Science,
10.1109/URSIGASS.2011.6050557.
Ohishi, M.: 2011, IUCAF activity in 2008–2011, XXX URSI
General Assembly and Scientific Symp. of Int. Union of Radio
Science, 10.1109/URSIGASS.2011.6051246.
Oka, T., Geballe, T. R., Goto, M., Usuda, T., Indriolo, N., McCall,
B. J.: 2011, H3+ in Warm, Diffuse Gas of the Central MolecularZone, ASP Conf. Ser. 439, Eds. M. R. Morris, Q. D. Wang, F.
Yuan, 18.
Oka, T., Morong, C. P., Geballe, T. R., Indriolo, N., McCall, B.
J., Goto, M., Usuda, T.: 2011, Warm and Diffuse Gas andHigh Ionization Rate Near the Galactic Center, Int. Symp. on
Molecular Spectroscopy, 66th meeting.
Oka, T., Tanaka, K., Matsumura, S. Nagai, M., Kamegai, K.,
Hasegawa, T.: 2011, The ASTE Galactic Center CO J = 3–2
Survey: Probing Shocked Molecular Gas in the CMZ, ASP
Conf. Ser. 439, Eds. M. R. Morris, Q. D. Wang, F. Yuan, 3-12.
Oshima, A., et al.: 2011, Cosmic ray anisotropy observed by
GRAPES-3 air shower array, 32nd Int. Cosmic Ray Conf., Eds.
A. Oshima, et. al., Vol. 1, 109-112.
Pinfield, D. J., et al. including Tamura, M.: 2011, Understanding
sub-stellar populations using wide-field infrared surveys, EPJ

Web of Conf., 16, Eds. E. L. Martin, J. Ge, W. Lin.
Saiki, K., Arai, T., Araki, H., Ishihara, Y., Ohtake, M., Karouji,
Y., Kobayashi, N., Sugihara, T., Haruyama, J., Honda, C., Sato,
H., Takeda, H.: 2011, SELENE-2 landing site research board
activity report, Proc. 44th ISAS Lunar. Planet. Symp., Abstract#44-10.
Saito, M., Kitamura, Y., Momose, M., Tsukagoshi, T., Kawabe, R.:
2012, Aperture Synthesis Observations Toward The Protostellar
Systems L1551 IRS 5 And Hl Tau: Rotation In The Infalling
Envelope, AAS Meeting #219, #437.02.
Sakai, N., Sakai, T., Hirota, T., Yamamoto, S.: 2011, Peculiar
Carbon-Chain Chemistry in Low-Mass Star Forming Regions,
EAS Publ. Ser., 52, Eds. M. Roellig, R. Simon, V. Ossenkopf, J.
Stutzki, 235-238.
Sakao, T., Narukage, N., Shimojo, M., Tsuneta, S., Suematsu, Y.,
Miyazaki, S., Imada, S., Nishizuka, N., Watanabe, K., Dotani, T.,
DeLuca, E. E., Ishikawa, S.: 2011, Photon-counting soft x-ray
telescope for the Solar-C mission, Proc. of the SPIE, 8148, Eds.
S. Fineschi, J. Fennelly, 81480C.
Sasaki, S., Goossens, S., Ishihara, Y., Araki, H., Hanada, H.,
Matsumoto, K., Noda, H., Kikuchi, F., Iwata, T.: 2012,
Kaguya Selenodesy and the South Pole Aitken Basin, 43rd
Lunar and Planetary Science Conference, #1838.
Sasaki, S., Ishihara, Y., Goossens, S., Matsumoto, K., Hanada,
H., Araki, H., Noda, H., Iwata, T., Namiki, N.: 2011, The
Shape and Interior Structure of the South Pole-Aitken Basinfrom KAGUYA Selenodesy Data, Proc. 44th ISAS Lunar.
Planet. Symp., #10.
Sekiguchi, K.: 2012, WWDA Visit to Kazakhstan, IAU
Information Bulletin, 109, 62-70.
Shibasaki, K., Narukage, N., Yoshimura, K.: 2011, Imaging
Observations of Coronal Magnetic Field by Nobeyama
Radioheliograph, Solar Polarization 6, Proc. of a conf. held in
Maui, Hawaii, USA, Eds. J. R. Kuhn, D. M. Harrington, H. Lin,S. V. Berdyugina, J. Trujillo-Bueno, S. L. Keil, T. Rimmele, 433.
Shimajiri, Y., Kawabe, R., Takakuwa, S., Saito, M., Tsukagoshi,T., Momose, M., Ikeda, N., Akiyama, E., Austermann, J. E.,
Ezawa, H., Fukue, K., Hiramatsu, M., Hughes, D., Kitamura,Y., Kohno, K., Kurono, Y., Acott, K. S., Wilson, G., Yoshida,A., Yun, M. S.: 2011, Star Formation in the Orion A Molecular
Cloud, EAS Publ. Ser., 52, Eds. M. Roellig, R. Simon, V.
Ossenkopf, J. Stutzki, 307-308.
Shimizu, T., Tsuneta, S., Hara, H., Ichimoto, K., Kusano, K.,
Sakao, T., Sekii, T., Suematsu, Y., Watanabe, T.: 2011, The
SOLAR-C mission: current status, Proc. of the SPIE, 8148, Eds.
S. Fineschi, J. Fennelly, 81480B.
Shimonishi, T., Onaka, T., Kato, D., Ita, Y., Sakon, I., Kawamura,A., Kaneda, H.: 2011, Effect of Metallicity on the Chemical
Properties of Ices around embedded Young Stellar Objects,
Proc. IAU Symp. 280, Eds. J. Cernicharo, R. Bachiller, 339.
Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto. Y., Ishihara, Y.,
Yanaka, H., Tsutsumi, J., Hiyama, T., Nakamoto, H., Sakamoto,M.: 2011, Current Status of the Japanese Virtual Observatory
Portal, ASP Conf. Proc. 442, Eds. I. N. Evans, A. Accomazzi, D.
J. Mink, A. H. Rots, 591-594.
Sôma, M., Tanikawa, K.: 2011, Investigation of the Earth's

Rotation using Ancient Chinese Occultation Records, Mapping
the Oriental Sky, Proc. of the Seventh Int. Conf. on Oriental
Astronomy (ICOA-7), Eds. T. Nakamura, W. Orchiston, M.
Sôma, R. Strom, 64-66.
Sôma, M., Tanikawa, K.: 2011, Japanese astronomy in the 7th
century, Highlighting the History of Astronomy in the AsiaPcific Region, Proc. of the ICOA-6 Conf., Eds. W. Orchiston, T.
Nakamura, R. Strom, 139-151.
Sotani, H., Kokkotas, K. D.: 2011, Non-axisymmetric Torsional
Oscillations of Relativistic Stars, J. Phys.: Conf. Ser., 314, 12081.
Sotani, H.: 2011, Slowly Rotating Relativistic Stars in TeVeS, J.
Phys.: Conf. Ser., 314, 12126.
Suematsu, Y., Katsukawa, Y., Shimizu, T., Ichimoto, K., Horiuchi,T., Matsumoto, Y., Takeyama, N.: 2011, Short telescope designof 1.5-m aperture solar UV visible and IR telescope aboard
Solar-C, Proc. of the SPIE, 8148, Eds. S. Fineschi, J. Fennelly,
81480D.
Suzuki, T., Mao, H., Honma, M., Yoshida, T., Kajino, T., Otsuka,
T.: 2011, Electron capture reactions and beta decays in stellar
environments, AIP Conf. Proc. 1377, 28-32.
Suzuki, T., Yoshida, T., Honma, M., Mao, H., Otsuka, T., Kajino, T.:2011, Gamow-Teller and First-Forbidden Transition Strengths
in Astrophysical Processes, J. Phys.: Conf. Ser., 312, 72008.
Takanashi, N., Hiramatsu, M.: 2011, The TENPLA project:
Communicating Astronomy with the Public in Japan, Proc. IAU
Symp. 260, Eds. D. Valls-Gabaud, A. Boksenberg, 44-47.
Tanikawa, K., Sôma, M.: 2011, How were solar eclipses remembered
when there were no astronomers?, Mapping the Oriental Sky,
Proc. of the Seventh Int. Conf. on Oriental Astronomy (ICOA-7),
Eds. T. Nakamura, W. Orchiston, M. Sôma, R. Strom, 67-69.
Tanikawa, K., Yamamoto, T., Sôma, M.: 2011, Solar Eclipses atSunrise and Sunset in the Chunqiu Period, Highlighting theHistory of Astronomy in the Asia-Pcific Region, Proc. of the
ICOA-6 Conf., Eds. W. Orchiston, T. Nakamura, R. Strom, 21-43.
Tholen, D. J., et al. including Yagi, M., Yoshida, F.: 2011, Minor
Planet Observations [568 Mauna Kea], Minor Planet Circulars,
7540.
Torii, K., Fukui, Y., Kudo, N., Yamamoto, H., Kawamura, A.,
Machida, M., Takahashi, K., Nozawa, S., Matsumoto, R.: 2011,
Molecular Loops in the Galactic Center: Detailed Observationsof the Footpoint of the Loops, ASP Conf. Ser. 439, Eds. M. R.
Morris, Q. D. Wang, F. Yuan, 71.
Tosaki, T., Kuno, N., Onodera, S., Miura, R., Muraoka, K.,
Sawada, T., Komugi, S., Nakanishi, K., Kohno, K., Kawabe,R., Nakanishi, H., Arimoto, N.: 2011, NRO Legacy Project: M
33 All Disk Survey of Giant Molecular Clouds (GMCs) with
NRO-45m and ASTE-10m Telescope, EAS Publ. Ser., 52, Eds.
M. Roellig, R. Simon, V. Ossenkopf, J. Stutzki, 125-128.
Tsujimoto, T., Bekki, K.: 2011, Diagnosis of the IMF in the
Universe using C, N Abundances, ASP Conf. Ser. 445, Eds. F.
Kerschbaum, T. Lebzelter, R. F. Wing, 549-550.
Uemoto, K., Ohtake, M., Haruyama, J., Matsunaga, T., Yokota,
Y., Yamamoto, S., Nakamura, R., Morota, T., Kobayashi, S.,
Iwata, T.: 2011, Geological structure of the lunar South PoleAitken basin based on data derived from SELENE, Proc. 44th
ISAS Lunar. Planet. Symp., Abstract #44-12.

II Publications, Presentations

077

Ueta, T., Izumiura, H., Yamamura, I., Matsunaga, N., Ita, Y.,
Matsuura, M., Nakada, Y., Fukushi, H., Mito, H., Tanabe,T., Hashimoto, O.: 2011, Extended Dust Shell of the Carbon
Star U Hya Revealed by AKARI, ASP Conf. Ser. 445, Eds. F.
Kerschbaum, T. Lebzelter, R. F. Wing, 627.
Vivian, U., Wang, Z., Sanders, D., Fazio, G., Chung, A., Petitpas,
G., Iono, D., Gao, Y., Kewley, L., Huang, J.-S., GOALS: 2011,
High-Resolution Mapping of CO(3 – 2) in NGC 6240, ASP
Conf. Ser. 446, Eds. W. Wang, J. Lu, Z. Luo, Z. Yang, H. Hua, Z.
Chen, 97-102.
Watanabe, H., Narukage, N., Kubo, M., Ishikawa, R., Bando, T.,Kano, R., Tsuneta, S., Kobayashi, K., Ichimoto, K., TrujilloBueno, J.: 2011, Ly-alpha polarimeter design for CLASP rocket
experiment, Proc. of the SPIE, 8148, Eds. S. Fineschi, J.
Fennelly, 81480E.
Yamada, Y., Lammers, U., Gouda, N.: 2011, Application of Gaia
Analysis Software AGIS to Nano-JASMINE, ASP Conf. Proc.
442, Eds. I. N. Evans, A. Accomazzi, D. J. Mink, A. H. Rots,
367-370.
Yamaguchi, T., Sugimura, M., Sakai, T., Sakai, N., Takano, S.,
Hirano, N., Liu, S.-L., Nomura, H., Su, Y.-N., Takakuwa, S.,
Yamamoto, S.: 2011, Line Survey of L1157 B1 Shocked Region,
EAS Publ. Ser., 52, Eds. M. Roellig, R. Simon, V. Ossenkopf, J.
Stutzki, 311-312.
Yamamoto, S., Nakamura, R., Matsunaga, T., Ogawa, Y., Ishihara,Y., Morota, T., Hirata, N., Ohtake, M., Hiroi, T., Yokota,
Y., Haruyama, J.: 2012, Global Distribution Trend of Purest
Anorthosite on the Moon Revealed by SELENE Spectral
Profiler, 43rd Lunar and Planetary Science Conference, #1356.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Okita, K., Yoshida, M.,
Ohta, K., Kawai, N.: 2011, GRB 110915A MITSuME Okayama
j-band upper-limit, GRB Coordinates Network, Circular Service,
12345, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Okita, K., Yoshida,M., Ohta, K., Kawai, N.: 2011, GRB 111210A: MITSuMEOkayama J-band upper-limit, GRB Coordinates Network,
Circular Service, 12655, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Okita, K., Yoshida, M.,
Ohta, K., Kawai, N.: 2012, GRB 120106A: Mitsume okayama
ks-band upper limit, GRB Coordinates Network, CircularService, 12819, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Okita, K., Yoshida, M.,
Ohta, K., Kawai, N.: 2012, GRB 120211A: Mitsume okayama
ks-band observation, GRB Coordinates Network, CircularService, 12936, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Okita, K., Yoshida, M.,
Ohta, K., Kawai, N.: 2012, GRB 120211A: Mitsume okayama
ks-band upper limit, GRB Coordinates Network, CircularService, 12923, 1.
Yanagisawa, K., Kuroda, D., Shimizu, Y., Okita, K., Yoshida,M., Ohta, K., Kawai, N.: 2012, GRB 120212A: errata of subject
in GCNC 12936, GRB Coordinates Network, Circular Service,
12938, 1.
Yasuda, N., Okura, Y., Takata, T., Furusawa, H.: 2011, A Method
for Measuring Distortion in Wide-Field Imaging with High
Order Polynomials, ASP Conf. Proc. 442, Eds. I. N. Evans, A.

078

II Publications, Presentations

Accomazzi, D. J. Mink, A. H. Rots, 537-540.
Yokota, Y., Gwinner, K., Oberst, J., Haruyama, J., Matsunaga, T.,
Morota, T., Noda, H., Araki, H., Ohtake, M., Yamamoto, S.:
2012, Lunar Surface Roughness at Baseline 0.15-100 km andthe Impact History of the Highlands, 43rd Lunar and Planetary
Science Conference, #2843.
Yoshida, F., Yagi, M., Tomatic, A. U.: 2011, 2010 LQ68, Minor
Planet Electronic Circulars.
Yung, B., Nakashima, J., Imai, H., Deguchi, S., Diamond, P. J.,
Kwok, S.: 2011, High Velocity Precessing Jet from the Water
Fountain IRAS 18286-0959 Revealed by VLBA Observations,AAS Meeting #218, #127.12.
Zamaninasab, M., Witzel, G., Eckart, A., Sabha, N., Dovciak,
M., Karas, V., Schödel, R., García-Marín, M., Kunneriath,D., Nishiyama, S., Straubmeier, C., Valencia-Schneider, M.,
Zensus, A.: 2011, Near Infrared Polarimetry as a Tool for
Testing the Properties of Radiation from Sagittarius A*, ASP
Conf. Ser. 439, Eds. M. R. Morris, Q. D. Wang, F. Yuan.
Zenitani, S., Hesse, M., Klimas, A.: 2011, Fluid and Magnetofluid
Modeling of Relativistic Magnetic Reconnection, AIP Conf.
Proc. 1366, Eds. V. Florinski, J. Heerikhuisen, G. P. Zank, D. L.
Gallagher, 138-144.
Zhu, M., Papadopoulos, P. P., Xilouris, M., Kuno, N., Lisenfeld, U.:
2011, Excess Submillimeter Emission in the Starburst Galaxy
NGC 3310?, ASP Conf. Ser. 446, Eds. W. Wang, J. Lu, Z. Luo, Z.
Yang, H. Hua, Z. Chen, 119-124.

5. Publications in English
Finoguenov, A., et al. including Sekiguchi, K.: 2012, SXDF X-ray
groups and galaxy clusters, VizieR Online Data Catalog Vol. 740.
Nakamura, T., Orchiston, W., Sôma, M., Strom, R.: 2011, Mapping
the Oriental Sky, Proceedings of the Seventh International
Conference on Oriental Astronomy (ICOA-7), NAOJ, Tokyo.

6. Conference Presentations
Agata, H.: 2011, “You are Galileo!” telescope workshop in Indnesia,
APRIM2011, (Chiang Mai, Thailand, Jul. 25-29, 2011).
Agata, H.: 2011, Report of “You are Galileo!” telescope workshop,
CAP2011, (Beijing, China, Oct. 10-14, 2011).
Agatsuma, K., Chen, D.: 2011, Folding PRC for bLCGT, 4th
LCGT face to face meeting, (Kashiwa, Japan, Aug. 3-5, 2011).
Agatsuma, K., Mori, T., Ballmer, S., Sakata, S., Nishida, E.,
Kawamura, S.: 2011, High accuracy measurement of thequantum efficiency using radiation pressure, 9th Edoardo
Amaldi Conference on Gravitational Waves, (Cardiff, UK, Jul.
10-15, 2011).
Agatsuma, K., Mori, T., Friedrich, D., Sakata, S., Ballmer, S.,
Miyakawa, O., Numata, K., Kawamura, S.: 2012, Radiationpressure noise measurement, 5th KAGRA face to face meeting,(Kashiwa, Japan, Feb. 2-4, 2012).
Akiyama, K.: 2011, Results of multi-epoch VERA observations of
Sgr A* and future prospects for VERA+KVN, 1st VERA-KVN
science working group, (Mitaka, Japan, Jun. 13-14, 2011).
Akiyama, K.: 2011, The results of multi-epoch VERA observations

toward the galactic center, Sgr A*, AGN jet 2011, (Mitaka,
Japan, Nov. 25, 2011).
Akutsu, T., Chen, D., Ejiri, Y., Suzuki, R., Sato, S., Araya, A.,
Ando, M., Tanaka, N., Torii, Y., Kawamura, S.: 2011, Groundtesting of inertial sensors for DECIGO Pathnder, 9th Edoardo
Amaldi Conference on Gravitational Waves, (Cardiff, UK, Jul.
10-15, 2011).
Akutsu, T., DECIGO Working Group: 2011, DECIGO andDECIGO Pathfiner, Gravitational Wave Advanced Detector
Workshop 2011, (Isola d'Elba, Italy, May 22-28, 2011).
Akutsu, T.: 2011, Status Report of Auxiliary Optics Subsystem, 4th
LCGT face to face meeting, (Kashiwa, Japan, Aug. 3-5, 2011).
Akutsu, T.: 2012, Status Report of Auxiliary Optics, 5th KAGRA
face to face meeting, (Kashiwa, Japan, Feb. 2-4, 2012).
Aoki, K., Hara, H.: 2011, A High-Velocity Motion of Active Region
Loops Triggered by a 2011 Feb 18 Flare, The 5th Hinode Science
Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Aoki, K., Iwata, I., Hattoti, T.: 2011, Mid-Infrared selected quasars
in WISE Preliminary Data Release, Through the Infrared Looking
Glass: A Dusty View of Galaxy and AGN Evolution, (Pasadena,
CA, USA, Oct. 2-5, 2011).
Aoki, K.: 2011, Rest optical spectroscopy of FeLoBALs and
LoBALs at intermideiate redshift, Narrow-line Seyfert1 galaxies
and their place in the universe, (Milano, Italy, Apr. 4-6, 2011).
Aoki, W.: 2011, Extremely Metal-Poor Stars in the Milky Way
Halo, 3rd Subaru Int. Conf., 1st NAOJ Symp., Galactic
Archaeology: Near-Field Cosmology and the Formation of the
Milky Way, (Shuzenji, Japan, Nov. 1-4, 2011).
Aoki, W.: 2011, Neutron-Capture Elements in Extremely MetalPoor Stars, 11th Int. Symp. on Origin of Matter and Evolutionof Galaxies, (Wako, Japan, Nov. 14-17, 2011).
Aoki, W.: 2011, The metallicity distribution of Sr-enhanced metalpoor stars, The Light Element Primary Process & the Originof Lighter Heavy Elements, (GSI, Darmstadt, Germany, Oct.
10-12, 2011).
Aoki, W.: 2012, Li abundances in very metal-poor, main-sequence
turn-off stars, Int. Workshop on Lithium in the Cosmos, (Paris,
France, Feb, 27-29, 2012).
Araki, H., Noda, H., Hanada, H., Katayama, M., Sasaki, S.,
Tazawa, S., Tsuruta, S., Kunimori, H., Fuse, T., Otsubo,T., Funazaki, K., Sato, A., Taniguchi, H., Murata, K.: 2012,
Research Activities in Japan for the Precise Measurement of the
Lunar Rotation and Tide -LLR and ILOM-, Theory and Model
For the New Generation of the Lunar Laser RANGING DATA;
3rd Work Shop, (ISSI, Bern, Switzerland, Mar. 23-25, 2012).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S.,
Sasaki, S.: 2012, The Status of Data Archive and Calibration/
Validation of LALT, The 6th KAGUYA (SELENE) Science
Working Team Meeting (SWTM6), (Nagoya, Japan, Jan. 10-12,2012).
Ariyoshi, S., Takahashi, K., Noguchi, T., Koga, K., Furukawa, N.,
Otani, C.: 2011, Terahertz detector with transmission-line typesuperconducting tunnel junctions, Superconductivity Centennial
Conf. (EUCAS-ISEC-ICMC 2011), (Hague, Netherlands, Sep.
18-23, 2011).
Black, C., Antiochos, S. K., Hesse, M., Karpen, J. T., DeVore, C.

R., Kuznetsova, M. M., Zenitani, S.: 2011, Kinetic Simulationsof Current-Sheet Formation and Reconnection at a Magnetic
X Line, 53rd Annual Meeting of the APS Division of Plasma
Physics, (Salt Lake City, UT, USA, Nov. 14-18, 2011).
Black, C., Antiochos, S. K., Hesse, M., Karpen, J. T., DeVore,
C. R., Zenitani, S., Kuznetsova, M. M.: 2011, Current-Sheet
Formation and Reconnection at a Magnetic X Line in Particlein-Cell Simulations, AGU Fall Meeting 2011, (San Francisco,
CA, USA, Dec. 5-9, 2011).
Bowler, B. P., Liu, M. C., Shkolnik, E. L., Tamura, M.: 2012,
A High-Contrast Adaptive Optics Imaging Search for Giant
Planets Around Young M Dwarfs, AAS Meeting #219, (Austin,
TX, USA, Jan. 8-12, 2012).
Carson, J., Thalmann, C., Janson, M., Kozakis, T., Wong, P., Goto,
M., Henning, T., Brandner, W., Biller, B., Bonnefoy, M., Feldt,M., McElwain, M., Kandori, R., Tamura, M., SEEDS Team:2012, A Subaru SEEDS Imaging Search for Extrasolar Planets
Around Early-Type Stars, AAS Meeting #219, (Austin, TX,
USA, Jan. 8-12, 2012).
Chen, D., Akutsu, T., Ejiri, Y., Suzuki, R., Ueda, A., Torii, Y.,
Tanaka, N., Araya, A., Sato, S., Ando, M., Gondo R., Obuchi,Y., Okada, N., Kawamura, S., Fujimoto, M.-K.: 2011,
Development of the inertial sensor for DECIGO Pathfinder, 9th
Edoardo Amaldi Conference on Gravitational Waves, (Cardiff,
UK, Jul. 10-15, 2011).
Eguchi, S., Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto, Y.,
Ishihara, Y., Yanaka, H., Tsutsumi, J., Hiyama, T., Nakamoto,
H., Sakamoto, M.: 2011, Improvement of Service Searching
Algorithm in the JVO Portal Site, Astronomical Data Analysis
Software and Systems XX, (Paris, France, Nov. 6-10, 2011).
Fukui, A., Homlan, M. J., Narita, N., Sumi, T.: 2011, Frequency
of Second Planet Occurrence in Mean Motion Resonances withHot Jupiters, Exsteme Solar Systems II, (Jackson, WY, USA,
Sep. 11-17, 2011).
Gonzalez, A., Fujii, Y., Kaneko, K., Uzawa, Y.: 2011, Quasioptical attenuators for ALMA band 10 receiver, Asia-PacificMicrowave Conf. 2011 (APMC 2011), (Melbourne, Australia,
Dec. 5-8, 2011).
Goossens, S., Matsumoto, K., Kikuchi, F., Liu, Q., Hanada,
H., Lemoine, F. G., Rowlands, D. D., Mazarico, E., Ishihara,Y., Noda, H., Araki, H., Namiki, N., Iwata, T., Sasaki, S.:
2012, Improved high-resolution lunar gravity field modelfrom SELENE and historical tracking data, The 6th KAGUYA(SELENE) Science Working Team Meeting (SWTM6),(Nagoya, Japan, Jan. 10-12, 2012).
Goossens, S., Matsumoto, K., Kikuchi, F., Liu, Q., Hanada, H.,
Lemoine, F. G., Rowlands, D. D., Ishihara, Y., Noda, H.,
Namiki, N., Iwata, T., Sasaki, S.: 2011, Improved HighResolution Lunar Gravity Field Model From SELENE andHistorical Tracking Data, AGU Fall Meeting 2011, (SanFrancisco, CA, USA, Dec. 5-9, 2011).
Gouda, N., JASMINE working group: 2011, Infrared Space
Astrometry Missions ~JASMINE missions~, 3rd Subaru Int.
Conf., 1st NAOJ Symp., Galactic Archaeology: Near-Field
Cosmology and the Formation of the Milky Way, (Shuzenji,
Japan, Nov. 1-4, 2011).

II Publications, Presentations079

Hada, K.: 2011, Measurement of the velocity field of the M87 jetwith VERA/GENJI, AGN jet 2011, (Mitaka, Japan, Nov. 25,
2011).
Hada, K.: 2012, M87 observations, 2nd VERA-KVN science
working group, (Seoul, Korea, Feb. 15-16, 2012).
Hanada, H., Araki, H., Tazawa, S., Tsuruta, S., Noda, H.,
Asari, K., Ishihara, Y., Matsumoto, K., Sasaki, S., Funazaki,
K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Murata,
K., Itou, Y., Chiba, K., Wakamatsu, H., Petrova, N., Gusev, A.,
Gouda, N., Yano, T., Yamada, Y., Niwa, Y., Ping, J., Kawano,N., Iwata, T., Heki, K.: 2011, Development of a Small Telescopefor Observations of Lunar Rotation, ASTROKAZAN 2011,(Kazan, Russia, Aug. 22-30, 2011).
Hanada, H., Tsuruta, S., Araki, H., Tazawa, S., Asari, K.,
Noda, H., Ishihara, Y., Matsumoto, K., Sasaki, S., Funazaki,
K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Murata,
K., Itou, Y., Chiba, K., Wakamatsu, H., Gouda, N., Yano,
T., Yamada, Y., Niwa, Y., Petrova, N., Gusev, A., Ping, J.,
Kawano, N., Iwata, T., Heki, K.: 2012, Development of a
Small Digital Telescope for Observations of Lunar Rotation,
The 6th KAGUYA (SELENE) Science Working Team Meeting(SWTM6), (Nagoya, Japan, Jan. 10-12, 2012).
Hanaoka, Y.: 2012, Long-Term Synoptic Observation of theSun by the Solar Observatory of the NAOJ, The 2nd Nagoya
Workshop on the Relationship between Solar Activity andClimate Changes, (Nagoya, Japan, Jan. 16-17, 2012).
Hara, C., Kawabe, R., Shimajiri, Y., Saito, M., Nakamura, F.,
Tsukagoshi, T., Wilner, D.: 2012, ASTE and SMA observationsof B59 in the Pipe nebula; Evidence for disk-driven rotating
molecular outflow from a protost, ALMA/NAASC 2012
Workshop: Outflows, Winds and Jets, (Charlottesville, Virginia,
USA, Mar. 3-6, 2012).
Hara, H., Watanabe, T., Harra, L. K., Culhane, J. L., Young, P.
R.: 2011, Observed Features of Magnetic Reconnection in 2007
May 19 Flare, The 5th Hinode Science Meeeting, (Boston, MA,
USA, Oct. 11-15, 2011).
Hara, H.: 2012, Photosphere -Corona Connection in ActiveRegion Plage, SDO-4/ IRIS/ Hinode Workshop, (Monterey,
USA, Mar. 12-16, 2012).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J.: 2012,
The Tidal Response of the Moon, The 6th KAGUYA (SELENE)
Science Working Team Meeting (SWTM6), (Nagoya, Japan,
Jan. 10-12, 2012).
Hashimoto, J., Tamura, M., Muto, T., SEEDS Project Team: 2011,
Implications of Giant Planet Formation in the Protoplanetary
Disk around AB Aurigae, Signposts of Planets Conf., (Goddard
Space Flight Center, USA, Oct. 18-20, 2011).
Hashimoto, J., Tamura, M., Muto, T., SEEDS Project Team: 2011,
Initial Result of the Subaru SEEDS Project: Fine Structuresof the Circumstellar Disk around AB Aur, Asia Oceania
Geosciences Society 2011, (Taipei, Taiwan, Aug. 8-12, 2011).
Hayama, K., Niinuma, K., Oyama, T.: 2011, Proposal for multimessenger observations of radio transients by Nasu and LIGOVirgo, New Horizons in Time Domain Astronomy, (Oxford,
UK, Sep. 19-23, 2011).
Hayama, K.: 2011, Multi-messenger observation using LCGT, 4th080

II Publications, Presentations

LCGT face to face meeting, (Kashiwa, Japan, Aug. 3-5, 2011).
Hayama, K.: 2012, Current status of Detector Characterization for
KAGRA, 5th KAGRA face to face meeting, (Kashiwa, Japan,
Feb. 2-4, 2012).
Hayano, Y., Akiyama, M., Hattori, T., Iwata, I., Kodama, T.,
Minowa, Y., Motohara, K., Nishimura, T., Ohashi, N., Ohno,
Y., Oya, S., Shirahata, M., Takami, H., Takato, N., Tamura,N., Tanaka, I., Terada, H., Tomono, D., Usuda, T.: 2011,
Next generation AO system of Subaru Telescope, 2nd Int. Conf.
on Adaptive Optics for Extremely Large Telescopes, (Victoria,
Canada, Sep. 25-30, 2011).
Hayano, Y., Oya, S., Hattori, M., Minowa, Y., Shirahata, M.,
Terada, H., Pyo, T.-S., Takami, H., Iye, M.: 2011, AO188/
LGS at Subaru Telescope, Mauna Kea AO meeting, (IfA Hilo,
HI, USA, Sep. 14, 2011).
Hayashi, M.: 2011, Star formation activities in a cluster and its
surrounding structure at z = 1.46, Galaxy Formation 2011,(Durham, UK, Jul. 18-22, 2011).
Hayashi, T.: 2011, Rejuvenated young radio source J1159+011 as
BAL quasar, 4th East Asia VLBI Workshop — Sciences andTechnology by now and future, (Lijiang, China, Apr. 18-20,
2011).
Hayashi, T.: 2011, Young radio sources and BAL quasars, AGN jet
2011, (Mitaka, Japan, Nov. 25, 2011).
Hayashi, T.: 2011, Young Radio Sources Associated with
Broad Absorption Line Quasars, Workshop on East-Asiancollaboration for SKA, (Daejeon, Korea, Nov. 30-Dec. 2, 2011).
Hibi, Y., Matsuo, H., Ikeda, H., Fujiwara, M.: 2011, 32-ch multichip module with GaAs-JFET cryo-ASICs, 12th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Seoul, Korea, Dec. 5-6, 2011).
Hibi, Y., Matsuo, H., Ikeda, H., Fujiwara, M.: 2011, The Cryogenic
Multi-Channel Readout System for Submillimeter/Terahertz
Cameras, 14th Int. Workshop on Low Temperature Detectors,(Heidelberg, Germany, Aug. 1-5, 2011).
Hibi, Y., Matsuo, H., Ookawa, T., Nagata, H., Ikeda, H., Fujiwara,
M.: 2011, "32-channel Multi-Chip-Module" The Cryogenic
Readout System for Submillimeter/Terahertz Cameras, 22ndInt. Symp. on Space Terahertz Technology, (Tucson, AZ, USA,
Apr. 26-28, 2011).
Higuchi, A., Kokubo, E., Ito, T.: 2012, Radial transport of small
solar system bodies - from 100 AU to 105 AU -, MISASA IV
Solar System Exploration and New Geosciences -Perspective
for the Next Decade-, (Tottori, Japan, Feb. 24-26, 2012).
Hirota, T.: 2011, Observational Studies on Star-formation with
VERA, Ishigaki International Workshop "Formation of Stars &Planets 2011(FSP2011)", (Ishigaki, Okinawa, Japan, Oct. 3-7,
2011).
Hirota, T.: 2011, Review of "VERA nearby SFRs project", 1st
VERA-KVN science working group, (Mitaka, Japan, Jun.
13-14, 2011).
Hirota, T.: 2012, Proposal of SFRs studies with VERA+KVN, 2nd
VERA-KVN science working group, (Seoul, Korea, Feb. 15-16,
2012).
Hirota, T.: 2012, Status report of SFRs sub-WG, 2nd VERA-KVN
science working group, (Seoul, Korea, Feb. 15-16, 2012).

Hirota, T.: 2012, VERA observations of the H2O maser burst inOrion KL, IAU Symp. 287, "Cosmic Masers - from OH to H0",
(Stellenbosch, South Africa, Jan. 30-Feb. 3, 2012).
Honma, M.: 2011, Maser astrometry and East-Asian VLBI, 11th
Asian-Pacific Regional IAU Meeting, (Chiang Mai, Thailand,
Jul. 26-29, 2011).
Honma, M.: 2011, mm/sub-mm VLBI, AGN jet 2011, (Mitaka,
Japan, Nov. 25, 2011).
Honma, M.: 2011, VLBI astrometry with VERA+KVN, 1st VERAKVN science working group, (Mitaka, Japan, Jun. 13-14, 2011).
Honma, M.: 2012, EHT and Chandra Sgr A* campaign, 2nd
VERA-KVN science working group, (Seoul, Korea, Feb. 15-16,
2012).
Honma, M.: 2012, Maser astrometry with VERA and Galactic
structure, IAU Symp. 287, "Cosmic Masers - from OH to H0",
(Stellenbosch, South Africa, Jan. 30-Feb. 3, 2012).
Hori, Y., Ikoma, M.: 2011, Gas Giant Formation with Small Cores
Triggered by Envelope Pollution by Icy Planetesimals, Extreme
Solar Systems II, (Moran, WY, USA, Sep. 11-17, 2011).
Hori, Y., Kokubo, E., Oshino, S., Ida, S.: 2011, Formation andDiversity of Planetary Systems around M-dwarfs: Toward the
Next-Generation Observations, The 1st Kepler Science Conf.,(NASA Ames Research Park, USA, Dec. 5-9, 2011).
Hwang, N.: 2011, Origin of Extended Star Clusters: New
Archaeological Tracers of Galaxy Evolution?, 3rd Subaru Int.
Conf., 1st NAOJ Symp., Galactic Archaeology: Near-Field
Cosmology and the Formation of the Milky Way, (Shuzenji,
Japan, Nov. 1-4, 2011).
Hwang, N.: 2011, The Nature of Extended Star Clusters in the
Dwarf Galaxy NGC 6822, Stellar Clusters & Associations: A
RIA Workshop on Gaia, (Granada, Spain, May 23-27, 2011).
Ichimoto, K., Suematsu, Y., Katsukawa, Y., Shimizu, T., SUVIT
Team: 2011, Science objective and design concept of the Large
Aperture Solar UV Visible and IR Observing Telescope for
Solar-C Mission, 2nd ATST-EAST Workshop in Solar Physics,(Washington, DC, USA, Oct. 9-11, 2011).
Iguchi, S.: 2011, ALMA and Key Technologies for Future Large
Single Dishes, Large Aperture Millimeter/Submillimeter
Telescopes in the ALMA Era, (Osaka, Japan, Sep. 12-13, 2011).
Iguchi, S.: 2011, ALMA Status and Development Policy, ALMA EA
Development Workshop 2011, (Mitaka, Japan, Sep. 8, 2011).
Iguchi, S.: 2011, ALMA Status, Science Operation, and EA Science
activities, The 5th East Asian Core Observatories Association
Meeting, (Kyoto, Japan, Nov. 7-8, 2011).
Iguchi, S.: 2011, Very Close Binary Black Hole in a Giant Elliptical
Galaxy 3C 66B and its Black Hole Merger, Gravitational Wave
Astrophysics, Binary Supermassive Black Holes, and Galaxy
Mergers, (Lijiang, Yunnan, China, Aug. 1-5, 2011).
Iguchi, S.: 2012, A Very Close Binary Black Hole in a Giant
Elliptical Galaxy 3C 66B and its Black Hole Merger, AAS
Meeting #219, (Austin, TX, USA, Jan. 8-12, 2012).
Ikoma, M., Hori, Y.: 2011, Accumulation of Hydrogen-richAtmospheres of Nebular Orgins on Short-Period Super-Earths:
Implications for Kepler-11 Systems, The 1st Kepler Science
Conf., (NASA Ames Research Park, USA, Dec. 5-9, 2011).
Imada, S., Hara, H., Watanabe, T., Shimizu, T., Harra, L. K.:

2011, Imaging Spectroscopic Observation of Filament Eruptions
by Hinode/EIS Flare Hunting Study, The 5th Hinode Science
Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Imamura, T., Iwata, T., Yamamoto, Z., Mochizuki, N., Kono,
Y., Matsumoto, K., Liu, Q., Noda, H., Hanada, H., Oyama,
K., Futaana, Y., Nabatov, A., Saitou, A., Ando, H.: 2012, The
status of data archive and calibration/validation of RS, The
6th KAGUYA (SELENE) Science Working Team Meeting(SWTM6), (Nagoya, Japan, Jan. 10-12, 2012).
Imanishi, M., Nakagawa, T., Ohyama, Y., Shirahata, M., Onaka,
T.: 2012, AKARI IRC systematic infrared spectroscopy ofluminous infrared galaxies, The 2nd AKARI Conf., Legacy of
AKARI: A Panoramic View of the Dusty Universe, (Jeji, Korea,
Feb. 27-29, 2012).
Ishigaki, M., Chiba, M., Aoki, W.: 2011, Chemical abundance
analyses of the kinematically selected thick disk/halo stars, 3rd
Subaru Int. Conf., 1st NAOJ Symp., Galactic Archaeology:
Near-Field Cosmology and the Formation of the Milky Way,
(Shuzenji, Japan, Nov. 1-4, 2011).
Ishihara, Y., Hiramatsu, Y., Yamamoto, M., Furumoto, M., Fujita,
K.: 2011, Infrasound and Seismic Observation of Hayabusa
Reentry as An Artificial Meteorite Fall, AGU Fall Meeting
2011, (San Francisco, CA, USA, Dec. 5-9, 2011).
Ishihara, Y., Hiramatsu, Y., Yamamoto, M., Furumoto, M., Fujita,
K.: 2012, Infrasound and Seismic Observation of Hayabusa
Reentry as An Artificial Meteorite Fall, MISASA IV Solar
System Exploration and New Geosciences -Perspective for the
Next Decade-, (Tottori, Japan, Feb. 24-26, 2012).
Ishikawa, R.: 2011, Properties of transient horizontal magnetic
fields; their implication to the origin of quiet-Sun magnetism,
The 5th Hinode Science Meeeting, (Boston, MA, USA, Oct.
11-15, 2011).
Ishikawa, R.: 2011, Properties of Transient Horizontal Magnetic
Fields and Their Implication to the Origin of the Quiet-Sun
Magnetism, Asia Oceania Geosciences Society 2011, (Taipei,
Taiwan, Aug. 8-12, 2011).
Ishisaki, Y., Henmi, K., Akamatsu, H., Enoki, T., Ohashi, T.,
Hoshino, A., Shinozaki, K., Matsuo, H., Okada, N., Oshima,T.: 2011, Development of active gas-gap heat switch for doublestage adiabatic demagnetization refrigerator, 14th Int. Workshop
on Low Temperature Detectors, (Heidelberg, Germany, Aug.
1-5, 2011).
Ishitsu, N.: 2011, Dust Settling in Turbulent Protoplanetary Disks,
Ishigaki International Workshop "Formation of Stars & Planets
2011 (FSP2011)", (Ishigaki, Okinawa, Japan, Oct. 3-7, 2011).
Ito, T., Higuchi, A.: 2011, Dynamical evolution of the Oort cloud
new comets, Asia-Oceania Geoscience Society 8th Annual
Meeting, (Taipei, Taiwan, Aug. 8-12, 2011).
Ito, T.: 2012, Asymmetric cratering on the Moon and its implication
to a hidden NEA population, 3rd Maidanak Observatory Users
Meeting, (Mitaka, Japan, Jan. 30-Feb. 1, 2012).
Iwata, I., Yamada, T., WISH Working Group: 2011, Our WISH:
Feeding z >10 Targets to ELTs, Feeding the Giants: ELTs in theera of Surveys, (Ischia, Italy, Aug. 29-Sep. 2, 2011).
Iwata, T., Matsumoto, K., Ishihara, Y., Kikuchi, F., Harada, Y.,
Sasaki, S.: 2011, Measurements of Martian rotational variations

II Publications, Presentations081

by space geodetic techniques, 28th Int. Symp. on SpaceTechnology and Science (28th ISTS), (Okinawa, Japan, Jun.
5-12, 2011).
Iwata, T., Matsumoto, K., Ishihara, Y., Kikuchi, F., Harada, Y.,
Sasaki, S.: 2011, A study of Mars’ rotation measurements using
four-way Doppler and inverse VLBI methods, EPSC-DPS Joint
Meeting 2011, (Nantes, France, Oct. 2-7, 2011).
Iwata, T., Matsumoto, K., Ishihara, Y., Kikuchi, F., Harada, Y.,
Sasaki, S.: 2011, A study on the four-way Doppler measurements
and inverse VLBI observations for Mars rotation, European
Geosciences Union General Assembly 2011, (Vienna, Austria,
Apr. 3-8, 2011).
Iwata, T., Matsumoto, K., Ishihara, Y., Kikuchi, F., Harada, Y.,
Sasaki, S.: 2011, A study on the Four-way Doppler Measurements
and Inverse VLBI Observations for Mars’ Rotation, Asia Oceania
Geosciences Society 2011, (Taipei, Taiwan, Aug. 8-12, 2011).
Iye, M.: 2011, From the early universe to the formation of galaxies,
German-Japan Round Table: From the Early Universe to the
Evolution of Life, (Heiderberg, Germary, Dec. 1-3, 2011).
Izumiura, H., Kambe, E., Kuroda, D., Yanagisawa, K., Fukui,A., Shimizu, Y., Okita, K., Koyano, H., Sakamoto, A.: 2011,
Refurbishing the 188cm reflector for exoplanet studies,
Workshop on Astronomy with Precise Radial Velocity Exoplanet Search and Asteroseismology, (Seoul, Korea, Sep.
26-28, 2011).
Izumiura, H., Ueta, T., Yamamura, I., Nakada, Y., Matsunaga,N., Ita, Y., Matsuura, M., Fukushi, H., Mito, H., Tanabe, T.,
Sorahana, T., Hashimoto, O., Arimatsu, K., Onaka, T.: 2012,AKARI observations of cool evolved stars, The 2nd AKARI
Conf., Legacy of AKARI: A Panoramic View of the Dusty
Universe, (Jeji, Korea, Feb. 27-29, 2012).
Jayawardhana, R., Muzic, K., Scholz, A., Geers, V., Tamura, M.: 2011,
Substellar Objects in Nearby Young Clusters (SONYC): Latest
Results, AAS Meeting #218, (Boston, USA, May 22-26, 2011).
Jike, T., Manabe, S., Tamura, Y., Shizugaki, M.: 2012, Movementof the 2011 off the Pacific coast of Tohoku Earthquake detected
by VERA geophysical observations, 6th IVS General Meeting,(Spain, Madrid, Mar. 4-9, 2012).
Kajino, T.: 2011, Big-Bang Models, 6th European Physical Society
Summer School of on Experimental Nuclear Astrophysics,(Catania, Italy, Sep. 18-27, 2011).
Kajino, T.: 2011, Cosmology and the Formation of Elementsin the Early Universe, 2nd Multidisciplinary Science Forum,(Kalamazoo, MI, USA, Oct. 27-28, 2011).
Kajino, T.: 2011, Neutrinos in Cosmology, Astronomy and Astrophysics, Korean Physical Society, Annual meeting, (Daejon,
Korea, Apr. 13-15, 2011).
Kajino, T.: 2011, Nuclear Weak Interactions, Supernova Nucleosynthesis and Neutrino Oscillation, Rutherford Centennial Conf.
on Nuclear Physics, (Manchester, UK, Aug. 24-29, 2011).
Kajino, T.: 2011, R-Process in Gamma-Ray Bursts, Int. Workshop
on Physics of Rare-Ring, (Wako, Japan, Nov. 10-12, 2011).
Kajino, T.: 2011, Supernova Neutrino-process Nucleosynthesis
and Implications in Neutrino Oscillation, 3rd Subaru Int. Conf.,
1st NAOJ Symp., Galactic Archaeology: Near-Field Cosmology
and the Formation of the Milky Way, (Shuzenji, Japan, Nov.

082

II Publications, Presentations

1-4, 2011).
Kajino, T.: 2011, Supernova Nucleosynthesis and Neutrino
Oscillation, 19th Particles and Nuclei International Conference(PANIC) , (MIT, Boston, USA, Jul. 25-30, 2011).
Kajino, T.: 2012, Quest for Particle Astrophysics Solution to
Lithium Problems, Int. Workshop on Lithium in the Cosmos,(Paris, France, Feb, 27-29, 2012).
Kameya, O.: 2011, Pulsar Study using SKA, Workshop on East-Asiancollaboration for SKA, (Daejeon, Korea, Nov. 30-Dec. 2, 2011).
Kameya, O.: 2012, Short commet on pulsar observations, 2nd VERAKVN science working group, (Seoul, Korea, Feb. 15-16, 2012).
Kaneko, H., Kuno, N., Iono, D., Tamura, Y., Tosaki, T., Nakanishi,K., Sawada, T.: 2011, Molecular Gas Properties and Star
Formation in Interacting Galaxies, Galaxy Mergers In An
Evolving Universe, (Hualien, Taiwan, Oct. 23-28, 2011).
Kano, R., Narukage, N., Ishikawa, R., Kubo, M., Katsukawa,Y., Suematsu, Y., Hara, H., Bando, T., Tsuneta, S., Watanabe,
H., Ichimoto, K., Kubo, M., Song, D., Kobayashi, K., Trujillo
Bueno, J.: 2011, Instrument for the Chromospheric LymanAlpha SpectroPolarimeter (CLASP) program, The 5th Hinode
Science Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Kano, R., Tsuneta, S., Ueda, K.: 2011, What determines coronalloop temperature?, The 5th Hinode Science Meeeting, (Boston,
MA, USA, Oct. 11-15, 2011).
Kato, Y., Carlsson, M., Hansteen, V., Steiner, O.: 2011, Propagationof Slow-Modes through the Transition Region in Network
Magnetic Elements, The 5th Hinode Science Meeeting, (Boston,
MA, USA, Oct. 11-15, 2011).
Kato, Y.: 2012, Generation of shock waves traveling from thephotosphere to the transition region within network magnetic
elements, SDO-4/ IRIS/ Hinode Workshop, (Monterey, USA,
Mar. 12-16, 2012).
Katsukawa, Y., Hinode SOT Team: 2011, Magnetic Field
Diagnostics with the HINODE Spectro-Polarimeter, AGU Fall
Meeting 2011, (San Francisco, CA, USA, Dec. 5-9, 2011).
Katsukawa, Y., Orozco Suarez, D.: 2011, Power spectra of thesolar surface convection and implication to local dynamo, The 5th
Hinode Science Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Katsukawa, Y., Suematsu, Y., Shimizu, T., Ichimoto, K., Takeyama,
N.: 2011, Focal Plane Instrument for the Solar UV-Vis-IR
Telescope aboard SOLAR-C, SPIE Optics + Photonics, (San
Diego, CA, USA, Aug. 21-25, 2011).
Katsukawa, Y., Suematsu, Y., Tsuneta, S., Ichimoto, K., Shimizu,
T.: 2011, Modeling and verification of the diffraction-limited visible
light telescope aboard the solar observing satellite HINODE,
Symp. on Integrated Modeling of Complex Optomechanical
Systems, (Kiruna, Sweden, Aug. 15-17, 2011).
Katsukawa, Y.: 2011, Spacecraft overview, Solar-C Meeting,(Boston, MA, USA, Oct. 16, 2011).
Kawaguchi, N.: 2011, Earthquake damage on Mizusawa VLBI
Observatory and Operation Plan in 2011, 4th East Asia VLBI
Workshop — Sciences and Technology by now and future,(Lijiang, China, Apr. 18-20, 2011).
Kikuchi, F., Matsumoto, K., Hanada, H., Tsuruta, S., Asari, K.,
Kono, Y., Yamada, R., Ishihara, Y., Sasaki, S., Iwata, T., Iijima,Y., Ogawa, K., Kamata, S., Goossens, S.: 2012, Recent status

of SELENE-2/VLBI instrument, The 6th KAGUYA (SELENE)
Science Working Team Meeting (SWTM6), (Nagoya, Japan,
Jan. 10-12, 2012).
Kim, M. K.: 2011, Dimensional Kinematics of H2O and SiO Masersin Orion­KL, 4th East Asia VLBI Workshop — Sciences andTechnology by now and future, (Lijiang, China, Apr. 18-20, 2011).
Kim, M. K.: 2011, The origin of outflows in Orion-KL, 1st VERAKVN science working group, (Mitaka, Japan, Jun. 13-14, 2011).
Kim, M. K.: 2012, 3-Dimensional Kinematics of water/SiO
Masers in Orion-KL, IAU Symp. 287, "Cosmic Masers - fromOH to H0", (Stellenbosch, South Africa, Jan. 30-Feb. 3, 2012).
Kim, M. K.: 2012, Water/SiO masers in Orion-KL, 2nd VERAKVN science working group, (Seoul, Korea, Feb. 15-16, 2012).
Kim, S., Bain, H. M., Shibasaki, K.: 2011, Hot Flare Plasma
Observed by Nobeyama Radioheliograph, RHESSI, and AIA/
SDO, LWS/SDO Workshop "Many Spectra of Solar Activity",(Tahoe, CA, USA, May 1-5, 2011).
Kim, S., Bain, H. M., Shibasaki, K.: 2011, Microwave Emissionof Supra-Arcade Structure Associated with M1.6 Limb Flare,
11th Asian-Pacific Regional IAU Meeting, (Chiang Mai,
Thailand, Jul. 26-29, 2011).
Kim, S., Bain, H. M., Shibasaki, K.: 2011, Multi-wavelength
Observations of Supra-Arcade Structure associated with M1.6
Limb Flare, Japan-Korea Space Weather Workshop 2011:
Current Status and Prospect of Space Weather Modeling andObervation, (Daejeon, Korea, Sep. 29- Oct. 1, 2011).
Kim, S., Bain, H. M., Shibasaki, K.: 2011, Multi-wavelength
Observations of Supra-Arcade Structure associated with M1.6
Limb Flare, 12th RHESSI Workshop and High Energy Solar
Physics Symp., (Nanjing, China, Oct. 17-21, 2011).
Kim, S., Bain, H. M., Shibasaki, K.: 2011, Multi-wavelength
Observations of Supra-Arcade Structure associated with M1.6
Limb Flare, AGU Fall Meeting 2011, (San Francisco, CA, USA,
Dec. 4-9, 2011).
Kino, M.: 2011, AGN jet Science with KVN+VERA, AGN jet
2011, (Mitaka, Japan, Nov. 25, 2011).
Kino, M.: 2011, Where is the gamma-ray emission region in
AGNs? Monthly monitoring of M87, 1st VERA-KVN science
working group, (Mitaka, Japan, Jun. 13-14, 2011).
Kino, M.: 2012, Initial report on AGN observations with
VERA+KVN: Overview, 2nd VERA-KVN science working
group, (Seoul, Korea, Feb. 15-16, 2012).
Kiuchi, H., Kawanishi, T.: 2011, Photonic millimeter-wave/
microwave signal generation and transmission techniques fora high-frequency Radio Interferometer and a very large anttena
array, XXX URSI General Assembly and Scientific Symp. of Int.
Union of Radio Science, (Istanbul, Turkey, Aug. 13-20, 2011).
Kiuchi, H.: 2011, Artificial calibration source on the ALMA highsite, ALMA EA Development Workshop 2011, (Mitaka, Japan,
Sep. 8, 2011).
Kiuchi, H.: 2011, Photonic LO signal generation and transmission
techniques, ALMA EA Development Workshop 2011, (Mitaka,
Japan, Sep. 8, 2011).
Kobayashi, H.: 2011, Japanese VLBI activities and East AsianVLBI Network, Advances in Asia and Oceania Toward
Very Long Baseline Interferometry in the Age of the Square

Kilometre Array, (Perth, Australia, May 4-6, 2011).
Kobayashi, H.: 2011, Japanese VLBI activities and East Asian VLBI
Network, Postgraduate Bursary Conf. Project 2011 Postgraduate
Bursary Conf., (Stellenbosch, South Africa, Nov. 21-25, 2011).
Kobayashi, H.: 2011, Status and future of EAVN, 4th East Asia
VLBI Workshop — Sciences and Technology by now andfuture, (Lijiang, China, Apr. 18-20, 2011).
Kobayashi, K., et al. including Tsuneta, S., Hara, H., Ishikawa, R.,
Kano, R., Katsukawa, Y., Kubo, M., Suematsu, Y.: 2011, The
Chromospheric Lyman-Alpha Spectro Polarimeter (CLASP),
The 5th Hinode Science Meeeting, (Boston, MA, USA, Oct.
11-15, 2011).
Kobayashi, M. A. R.: 2011, A Model Prediction to the Natureof High-z Lyman-Alpha Emitters, Galaxy Formation 2011,(Durham, UK, Jul. 18-22, 2011).
Kodama, T.: 2011, Mahalo-Subaru: Mapping Star Formation at
the Peak Epoch of Galaxuy Formation, Galaxy Formation 2011,(Durham, UK, Jul. 18-22, 2011).
Kokubo, E.: 2011, The Final Stage of Terrestrial Planet Formation,
The 1st Kepler Science Conf., (NASA Ames Research Park,
USA, Dec. 5-9, 2011).
Kokubo, E.: 2012, Formation of Terrestrial Planets: The Basic
Dynamical Model, MISASA IV Solar System Exploration and
New Geosciences -Perspective for the Next Decade-, (Tottori,
Japan, Feb. 24-26, 2012).
Komiya, Y., Eguchi, S., Shirasaki, Y., Ohishi, M., Mizumoto, Y.,
Ishihara, Y., Yanaka, H., Tsutsumi, J., Hiyama, T., Nakamoto, H.,
Sakamoto, M.: 2011, VO Crawler: a crawling system for Virtual
Observatory services, Astronomical Data Analysis Software andSystems XX, (Paris, France, Nov. 6-10, 2011).
Komiya, Y., Suda, T., Yamada, S., Fujimoto, M. Y.: 2011,
Hierarchical Chemical Evolution and R-process Elementsof EMP Stars, 3rd Subaru Int. Conf., Galactic Archaeology,(Shuzenji, Kyoto, Japan, Nov. 6-10, 2011).
Kotake, K.: 2011, 3D simulations of core-collapse supernovae
with spectral neutrino transport, Coconuts meeting 2011,(Meudon observatory, Paris, Nov. 17, 2011).
Kotake, K.: 2011, Multidimensional supernova simulations witha concentration of equation of state, Int. symp. of symmetryenergy, (Massachusetts, USA, Jun. 17-19, 2011).
Kotake, K.: 2011, Multimessenger from core-collapse supernovae:
multidimensionality as a key to bridge theory and observation,
Multi-messenger probe into nuclear physics, (Washington,
USA, Jul. 16, 2011).
Kotake, K.: 2011, Numerical recipes in microphysics to energize
core-collapse supernovae, Microphysics in Computational
Relativistic Astrophysics, (Perimeter institute, Ontario, Canada,Jun. 20, 2011).
Kotake, K.: 2012, 3D vs. GR: which one will help the onsetof neutrino-driven explosions, 16th Workshop on "Nuclear
Astrophysics", (Ringberg, Germany, Mar. 30, 2012).
Kotake, K.: 2012, Cutting-edge issues in core-collapse supernova
modeling, Formations of compact objects: from the cradle to thegrave, (Tokyo, Japan, Mar. 8, 2012).
Kotake, K.: 2012, Cutting-edge issues in the theory of corecollapse supernovae, IAU Symp. 279, "Death of Massive Stars:

II Publications, Presentations083

Supernovae and Gamma-Ray Bursts", (Nikko, Japan, Mar.
12-16, 2012).
Koyama, Y., Kodama, T., Hayashi, M., Tadaki, K., Nakata, F.,
Tanaka, I., Shimasaku K., Okamura, S.: 2011, Red Star
Forming Galaxies in Distant Cluster Outskirts A key population
for understanding environmental effects at z < 1, Galaxy
Formation 2011, (Durham, UK, Jul. 18-22, 2011).
Kroug, M., Gonzales, A., Kuroiwa, K., Miyachi, A., Uzawa, Y.,
Makise, K., Wang, Z.: 2011, Resonances in Superconducting
Circuits at THz Frequencies, Superconductivity Centennial
Conf. (EUCAS-ISEC-ICMC 2011), (Hague, Netherlands, Sept.
18-23, 2011).
Kroug, M., Uzawa, Y.: 2011, Plans for an SIS Based Heterodyne
Receiver above 1 THz, 12th Workshop on Submillimeter-Wave
Receiver Technologies in Eastern Asia, (Seoul, Korea, Dec. 5-6, 2011).
Kubo, M., Sekii, T., Gizon, L.: 2011, Comparing Photospheric
Magnetic Fields and Subsurface Flows in the Quiet Sun, The 5th
Hinode Science Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Kurosaki, K., Ikoma, M., Hori, Y.: 2011, Thermal Evolution and
Mass Loss of Water-rich Super-Earths, The 1st Kepler Science
Conf., (NASA Ames Research Park, USA, Dec. 5-9, 2011).
Leisawitz, D., et al. including Matsuo, H.: 2011, Is Space-basedInterferometry Dead?, AAS Meeting #218, (Boston, USA, May
22-26, 2011).
Masuda, S., Goto, T., Shimojo, M., Kawate, T.: 2011, An extremely
microwave-rich flare observed with Nobeyama Radio
Heliograph, AGU Fall Meeting 2011, (San Francisco, CA, USA,
Dec. 4-9, 2011).
Matsumoto, K., Kikuchi, F., Iwata, T., Kono, Y., Tsuruta, S.,
Hanada, H., Goossens, S., Ishihara, Y., Kamata, S., Sasaki,
S.: 2011, VLBI mission proposed for SELENE-2 and its
contribution to constrain the lunar internal structure, AGU Fall
Meeting 2011, (San Francisco, CA, USA, Dec. 5-9, 2011).
Matsumoto, K., Kikuchi, F., Iwata, T., Kono, Y., Tsuruta, S.,
Hanada, H., Goossens, S., Ishihara, Y., Kamata, S., Sasaki, S.:
2011, VLBI radio sources on a lander and an orbiter for studyof lunar internal structure proposed for SELENE-2 mission,
ASTROKAZAN 2011, (Kazan, Russia, Aug. 22-30, 2011).
Matsumoto, K., Kikuchi, F., Iwata, T., Kono, Y., Tsuruta, S.,
Hanada, H., Goossens, S., Ishihara, Y., Kamata, S., Sasaki, S.:
2011, VLBI radio sources on a lander and an orbiter for studyof lunar internal structure proposed for SELENE-2 mission,
European Geosciences Union General Assembly 2011, (Vienna,
Austria, Apr. 3-8, 2011).
Matsumoto, K., Kikuchi, F., Iwata, T., Kono, Y., Tsuruta, S.,
Hanada, H., Goossens, S., Ishihara, Y., Kamata, S., Sasaki, S.:
2012, VLBI mission proposed for SELENE-2 and its
contribution to constrain the lunar internal structure, The
6th KAGUYA (SELENE) Science Working Team Meeting(SWTM6), (Nagoya, Japan, Jan. 10-12, 2012).
Matsumoto, N., Honma, M., Isono, Y., Fujisawa, K.: 2011,
Astrometry observations of 6.7 GHz methanol maser sources
with VERA/JVN, Star Formation through Spectroimaging at
High Angular Resolution, (Taipei, Taiwan, Jun. 20-24, 2011).
Matsumoto, N.: 2011, Astrometry Observation of 6.7 GHz Methanol
Maser Sources with JVN/VERA, 4th East Asia VLBI Workshop

084

II Publications, Presentations— Sciences and Technology by now and future, (Lijiang, China,
Apr. 18-20, 2011).
Matsumoto, N.: 2011, Investigation of 3D Galactic Gas Dynamics
with 6.7 GHz Methanol Masers Sources, Workshop on East-Asiancollaboration for SKA, (Daejeon, Korea, Nov. 30-Dec. 2, 2011).
Matsumoto, N.: 2011, Proper motion measurements of sources
around the galactic bar structure, 1st VERA-KVN science
working group, (Mitaka, Japan, Jun. 13-14, 2011).
Matsumoto, N.: 2012, Investigation of 3-D galactic dynamics
with masers, 2nd VERA-KVN science working group, (Seoul,
Korea, Feb. 15-16, 2012).
Matsumoto, N.: 2012, The bar effect in the galactic gas motions
traced by 6.7 GHz methanol maser sources with VERA, IAU
Symp. 287, "Cosmic Masers - from OH to H0", (Stellenbosch,South Africa, Jan. 30-Feb. 3, 2012).
Matsuo, H., Hibi, Y., Matsuo, T., Ohta, I. S., Kawada, M.: 2011,
Technical Challenges in Photon Counting Terahertz Interferometry(PCTI), 12th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Seoul, Korea, Dec. 5-6, 2011).
Matsuo, H., Kosaka, A., Arai, T., Tanaka, M.: 2012, Far-Infrared
Spectroscopic Study of Interstellar Material around Eta Carinae,
The 2nd AKARI Conf., Legacy of AKARI: A Panoramic Viewof the Dusty Universe, (Jeji, Korea, Feb. 27-29, 2012).
Matsuo, H., Matsuo, T., Ohta, I. S.: 2011, A Study on Photon
Counting Interferometry in Terahertz Frequencies, 22nd Int.
Symp. on Space Terahertz Technology, (Tucson, AZ, USA, Apr.
26-28, 2011).
Matsuo, H., Shi, S.-C.: 2011, High-Angular Resolution Terahertz
Astronomy from Dome A, SCAR Astronomy and Astrophysics
from Antarctica 2011, (Sydney, Australia, Jun. 29-Jul. 1, 2011).
Matsuo, H.: 2011, Requirements on photon counting detectors interahertz frequencies, 14th Int. Workshop on Low Temperature
Detectors, (Heidelberg, Germany, Aug. 1-5, 2011).
Mauersberger, R., et al. including Asayama, S., Kamazaki, T.,
Komugi, S., Sawada, T., Tachihara, K.: 2011, Commissioning
and Science Verification of ALMA, IAU symp. 280, "The
Molecular Universe", (Toledo, Spain, May 30-Jun. 3, 2011).
Min, C. H.: 2011, Orbital determination for R Aquarii, 1st VERAKVN science working group, (Mitaka, Japan, Jun. 13-14, 2011).
Miyazaki, S.: 2011, Hyper Suprime-Cam, First eROSITA Int.
Conf., (Garmisch-Partenkirchen, Germany, Oct. 17-20, 2011).
Miyazaki, S.: 2011, Hyper Suprime-Cam, Very Wide Field Surveys
in Light of the Astro2010, (STScI, MD, USA, Jun. 13-16, 2011).
Miyoshi, M., Shen, Z.-Q., Oyama, T., Takahashi, R., Kato, Y.:
2011, Oscillation Phenomena in the Disk around the Massive
Black Hole Sagittarius A*, 21st Workshop on General Relativity
and Gravitation (JGRG21), (Sendai, Japan, Sep. 26-29, 2011).
Miyoshi, M.: 2011, ALMA EA Development WorkShop 2011, ALMAEA Development Workshop 2011, (Mitaka, Japan, Sep. 8, 2011).
Mizuno, N.: 2011, The CO View of the Milky Way by NANTEN,
IAU Symp. 284 "The Spectral Energy Distribution of the
Galaxies", (Preston, UK, Sep. 5-9, 2011).
Mori, T., Agatsuma, K., Ballmer, S., Sakata, S., Miyakawa, O.,
Numata, K., Kawamura, S., Mio, N.: 2011, Control of motionsof a suspended mirror through radiation pressure in a highpower optical cavity, 9th Edoardo Amaldi Conference on

Gravitational Waves, (Cardiff, UK, Jul. 10-15, 2011).
Mori, T., Agatsuma, K., Ballmer, S., Sakata, S., Miyakawa, O.,
Numata, K., Kawamura, S., Mio, N.: 2011, Ponderomotive
squeezing experiment for gravitational wave detectors, Gravity andquantum information workshop, (Seoul, Korea, Aug. 29-30, 2011).
Nagai, H., et al.: 2012, Status report of GENJI, KVN-VERA Science
Workshop 2012, (Yonsei University, Korea, Feb. 14-16, 2012).
Nagai, H.: 2011, Current status of GENJI projects and future
prospects for VERA+KVN, 1st VERA-KVN science working
group, (Mitaka, Japan, Jun. 13-14, 2011).
Nagai, H.: 2011, Preliminary Cycle 1 Capability of ALMA & Short
Comments for Jet Science, AGN jet 2011, (Mitaka, Japan, Nov.
25, 2011).
Nagai, H.: 2012, GENJI status report, 2nd VERA-KVN science
working group, (Seoul, Korea, Feb. 15-16, 2012).
Nagashima, K., Zhao, J., Duvall, Jr. T., Kosovichev, A. G.,
Parchevsky, K., Sekii, T.: 2011, Time-distance helioseismology
analyses of multi-wavelength datasets obtained with Hinode/
SOT and SDO/HMI, The 5th Hinode Science Meeeting, (Boston,
MA, USA, Oct. 11-15, 2011).
Nagayama, T.: 2011, Astrometry of Galactic Star-Forming Regions
ON1 and ON2N with VERA: Estimation of Angular Velocity of
Galactic Rotation at the Sun, 11th Asian-Pacific Regional IAU
Meeting, (Chiang Mai, Thailand, Jul. 26-29, 2011).
Nagayama, T.: 2012, Astrometry of Galactic star-forming regions
ON1 and ON2N with VERA, IAU Symp. 287, "Cosmic Masers from OH to H0", (Stellenbosch, South Africa, Jan. 30-Feb. 3, 2012).
Nagayama, T.: 2012, Reports from Astrometry sub WG, 2nd VERAKVN science working group, (Seoul, Korea, Feb. 15-16, 2012).
Nakajima, T., Iwashita, H., Miyazawa, C., Yonezu, T., Kuno,
N., Kawabe, R., Inoue, H., Sakai, T., Kohno, K., Koyano, M.,
Katase, T., Nishimura, A., Kimura, K., Ogawa, H., Asayama,S., Noguchi, T.: 2011, Development of the Sideband-Separating(2SB) Receiver Systems for the NRO 45-m Millimeter Wave
Telescope, 12th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Seoul, Korea, Dec. 5-6, 2011).
Nakajima, T., Sakai, T., Kimura, K., Iwashita, H., Miyazawa,C., Katase, T., Koyano, M., Inoue, H., Kuno, N., Kawabe, R.,
Ogawa, H., Asayama, S., Noguchi, T.: 2011, Development ofa New Multi-Beam Array 2SB Receiver and the Measurment
System of Image Rejection Ratio for 2SB Mixer, ALMA EA
Development Workshop 2011, (Mitaka, Japan, Sep. 8, 2011).
Nakajima, T., Sakai, T., Kimura, K., Nishimura, A., Katase, T.,
Koyano, M., Inoue, H., Iwashita, H., Miyazawa, C., Kuno, N.,
Kawabe, R., Ogawa, H., Kohno, K., Asayama, S., Tamura,T., Noguchi, T.: 2011, 100-GHz Band Sideband-Separating(2SB) Receivers for the NRO 45-m Telescope, Large Aperture
Millimeter/Submillimeter Telescopes in the ALMA Era, (Osaka,
Japan, Sep. 12-13, 2011).
Nakajima, T., Takano, S., Kohno, K., Inoue, H., the line survey
team: 2011, Line Survey Project of External Galaxies with NRO
45-m Telescope, IAU symp. 280, "The Molecular Universe",(Toledo, Spain, May 30-Jun. 3, 2011).
Nakajima, T.: 2011, Imaging of Molecular Abundances toward
Active Galactic Nucleus, IAU symp. 280, "The Molecular
Universe", (Toledo, Spain, May 30-Jun. 3, 2011).

Nakamura, F.: 2012, A Burst of Molecular Outflows From theSerpens South Protocluster, ALMA/NAASC 2012 Workshop:
Outflows, Winds and Jets, (Charlottesville, Virginia, USA, Mar.
3-6, 2012).
Nakamura, K., Harikae, S., Kajino, T., Mathews, G. J.: 2011,
Long Gamma-ray Burst as a Production Site of R-process
Elements, 11th Int. Symp. on Origin of Matter and Evolution of
Galaxies, (Wako, Japan, Nov. 14-17, 2011).
Nakamura, K., Hayakawa, T., Kajino, T., Chiba, S., Iwamoto,N., Cheoun, M.-K., Mathews, G. J.: 2011, Radioactivities
from Supernovae and Its Application to Cosmochronology, 3rd
Subaru Int. Conf., 1st NAOJ Symp., Galactic Archaeology:
Near-Field Cosmology and the Formation of the Milky Way,
(Shuzenji, Japan, Nov. 1-4, 2011).
Nakamura, K., Kajino, T., Hayakawa, T., Chiba, S., Iwamoto, N.,
Cheoun, M.-K., Mathews, G. J.: 2011, Radioactive Niobium-92
Production via Neutrino-induced Nucleosynthesis, 11th Int.
Symp. on Origin of Matter and Evolution of Galaxies, (Wako,
Japan, Nov. 14-17, 2011).
Nakamura, K., Takiwaki, T., Kotake, K., Nishimura, N.: 2011,
Supernova Shock Revival by Nuclear Reactions, 11th Int.
Symp. on Origin of Matter and Evolution of Galaxies, (Wako,
Japan, Nov. 14-17, 2011).
Nakamura, K.: 2011, Construction of gauge-invariant variables
for linear-order metric perturbations on general backgroundspacetime, 21st Workshop on General Relativity and Gravitation(JGRG21), (Sendai, Japan, Sep. 26-29, 2011).
Narita, N.: 2011, Subaru Observations of Spin-Orbit Angles andOuter Massive Bodies, Exploring Strange New Worlds: From
Giant Planets to Super Earths, (High Country ConferenceCenter, AZ, USA, May 2-6, 2011).
Narita, N., SEEDS/RV team: 2011, Companion Candidates around
Transiting Planetary Systems: SEEDS First/Second Year Results,
Extreme Solar Systems II, (Wyoming, USA, Sep. 11-17, 2011).
Narita, N.: 2011, Status of RV Sub-Category, SEEDS 2nd General
Workshop, (Heidelberg, Germany, Oct. 10-12, 2011).
Narita, N.: 2012, High Frequency of Candidate Companions around
Planetary Systems with High Obliquity, Subaru Users Meeting
2011, (Mitaka, Japan, Feb. 28-Mar. 1, 2012).
Narita, N.: 2012, JHKs Simultaneous Transit Photometry of GJ1214b,
Exoclimes 2012 The Diversity of Planetary Atmospheres,(Aspen Center for Physics, USA, Jan. 15-20, 2012).
Narukage, N., Sakao, T., Kano, R., Shimojo, M.: 2011, Diagnostics
of coronal temperature based on the calibration result of X-Ray
Telescope and further calibration, The 5th Hinode Science
Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Naruse, M., Sekimoto, Y., Miyachi, A., Uzawa, Y., Nitta, T.,
Karatsu, K., Sekine, M., Noguchi, T.: 2011, The properties of
MKID made of crystal Al films and amorphous-Al films, 4thMicroresonator Workshop, (Grnoble, France, Jul. 26-27, 2011).
Naruse, M., Sekimoto, Y., Miyachi, A., Uzawa, Y., Nitta, T.,
Noguchi, T.: 2011, Development of Crystal Al MKIDs by
Molecular Beam Epitaxy, 14th Int. Workshop on Low Temperature
Detectors, (Heidelberg, Germany, Aug. 1-5, 2011)
Niino, Y.: 2011, Revisiting Metallicity of Long GRB Host Galaxies:
the Chemical Inhomogeneities in Galaxies, "Chemical Evolution

II Publications, Presentations085

of GRB Host Galaxies", (Sexten, Italy, Jul. 18-22, 2011).
Niino, Y.: 2012, Revisiting Metallicity of Long GRB Host
Galaxies: the Chemical Inhomogeneities in Galaxies, IAU
Symp. 279, "Death of Massive Stars: Supernovae and GammaRay Bursts", (Nikko, Japan, Mar. 12-16. 2012).
Nishizawa, A., Nakamura, K., Fujimoto, M.-K.: 2012, Weakmeasurement for gravitational wave detectors, 5th KAGRA face
to face meeting, (Kashiwa, Japan, Feb. 2-4, 2012).
Nitta, T., Naruse, M., Sekimoto, Y., Matsuo, H., Noguchi, T.,
Uzawa, Y., Mitsui, K., Okada, N., Karatsu, K., Sekine, M.,
Seta, M., Nakai, N.: 2011, Development of silicon lens array for
MKID camera, 4th Workshop on the Physics and Applicationsof Superconducting Microresonators, (Grenoble, France, Jul.
28-29, 2011).
Niwa, Y., Kobayashi, Y., Gouda, N., Yano, T., Yamada, Y.,
Hatsutori, Y.: 2011, Performance Evaluation of Nano-JASMINE
Telescope Flight Model, 28th Int. Symp. on Space Technology
and Science (28th ISTS), (Okinawa, Japan, Jun. 5-12, 2011).
Noda, H., Kunimori, H., Araki, H., Funazaki, K., Fuse, T., Hanada,
H., Katayama, M., Murata, K., Morota, T., Otsubo, T., Sasaki,S., Taniguchi, H., Tazawa, S., Tsuruta, S.: 2011, Lunar Laser
Ranging Experiment in Japanese Lunar Lander SELENE-2,
ASTROKAZAN 2011, (Kazan, Russia, Aug. 22-30, 2011).
Noda, H., Kunimori, H., Araki, H., Funazaki, K., Fuse, T.,
Hanada, H., Katayama, M., Murata, K., Otsubo, T., Sasaki,S., Taniguchi, H., Tazawa, S., Tsuruta, S.: 2012, Development
status of the Lunar Laser Ranging Experiment for SELENE-2,
The 6th KAGUYA (SELENE) Science Working Team Meeting(SWTM6), (Nagoya, Japan, Jan. 10-12, 2012).
Noda, H., Kunimori, H., Araki, H., Funazaki, K., Fuse, T., Hanada,
H., Katayama, M., Otsubo, T., Sasaki, S., Taniguchi, H.,
Tazawa, S., Tsuruta, S.: 2011, Lunar Laser Ranging experimentin Japanese lunar lander SELENE-2, 4th annual NASA Lunar
Science Forum, (Ames/NASA, USA, Jul. 19-21, 2011).
Noda, H., Kunimori, H., Araki, H., Fuse, T., Hanada, H.,
Katayama, M., Otsubo, T., Sasaki, S., Tazawa, S., Tsuruta,
S., Funazaki, K., Taniguchi, H., Murata, K.: 2011, Lunar Laser
Ranging Experiment for SELENE-2, 43rd Lunar and Planetary
Science Conference, (Woodlands, TX, USA, Mar. 19-23, 2012).
Noda, H., Kunimori, H., Araki, H., Fuse, T., Hanada, H., Katayama,
M., Otsubo, T., Sasaki, S., Tazawa, S., Tsuruta, S.: 2011,
Lunar Laser Ranging Experiment in SELENE-2, Asia Oceania
Geosciences Society 2011, (Taipei, Taiwan, Aug. 8-12, 2011).
Noguchi, T., Naruse, M., Sekimoto, Y.: 2011, RF conductivity
and surface impedance of a superconductor taking into accountthe complex superconducting gap energy, Superconductivity
Centennial Conf. (EUCAS-ISEC-ICMC 2011), (Hague,
Netherlands, Sep. 18-23, 2011)
Noguchi, T., Naruse, M., Sekimoto, Y.: 2011, Surface Resistanceof a Superconductor Taking into Account the Quasiparticle
States Inside the Energy Gap, 12th Workshop on SubmillimeterWave Receiver Technologies in Eastern Asia, (Seoul, Korea,
Dec. 5-6, 2011).
Noguchi, T.: 2011, Rf conductivity of a superconductor taking
into account the complex Superconducting gap energy, East
Asia Symp. on Superconductor Electronics (EASSE 2011),

086

II Publications, Presentations(Yamagata, Japan, Oct. 27-29, 2011).
Noguchi, T.: 2012, Surface resistance of a NbN ﬁlm accounting
for the broadening of the qp DOS, 2nd Superconducting Nitride
Detector Workshop, (Pasadena, CA, USA, Feb. 21-22, 2012).
Oe, M., Onodera, Y., Murai, J.: 2011, Early survey report on ICT
disaster recovery activities in the Great East Japan Earthquake,
Int. Symp. Disaster Simulation & Structural Safety in the Next
Generation, 2011, (Kobe, Japan, Sep. 17-18, 2011).
Ohishi, M.: 2011, Case Study – PLT Impacts on Radio Astronomy,
ITU Forum on compatibility between Power Line Telecommunication systems and Radiocommunication Services,(Geneva, Switzerland, May 27, 2011).
Ohishi, M.: 2011, Data Discovery in and Science Results by meansof Vos, JSPS-DST Asia Academic Seminar, CPS 8th Int. Schoolof Planetary Sciences, Challenges in Astronomy: Observational
Advances, (Minamiawaji, Hyogo, Japan, Sep. 26-Oct. 1, 2011).
Ohishi, M.: 2011, Impact to the Astronomy by Interference causedby the Solar Power Satellite Systems, XXX URSI General
Assembly and Scientific Symp. of Int. Union of Radio Science,(Istanbul, Turkey, Aug. 13-20, 2011).
Ohishi, M.: 2011, IUCAF Activity Report between 2008 and 2011,
XXX URSI General Assembly and Scientific Symp. of Int.
Union of Radio Science, (Istanbul, Turkey, Aug. 13-20, 2011).
Ohishi, M.: 2011, IUCAF and its activities within ITU-R, XXXURSI General Assembly and Scientific Symp. of Int. Union ofRadio Science, (Istanbul, Turkey, Aug. 13-20, 2011).
Ohishi, M.: 2011, Search for Large Molecules and Spectral Line
Surveys, 11th Asian-Pacific Regional IAU Meeting, (Chiang
Mai, Thailand, Jul. 26-29, 2011).
Ohishi, M.: 2012, Towards Life in the Universe, Sokendai Asian
Winter School "Basics and Frontiers in Molecular Science",(Okazaki, Aichi, Japan, Jan. 10-13, 2012).
Ohsuga, K.: 2011, Radiation-HD/MHD simulations, Black HoleSlim Disk Workshop, (Warsaw, Poland, Jul. 1-8, 2011).
Ohsuga, K.: 2011, Radiation-MHD simulations of black holeaccretion flows and outflows, AGN Winds in Charleston,(Charleston, SC, USA, Oct. 15-18, 2011).
Ohtake, M., Mastunaga, T., Takeda, H., Yokota, Y., Yamamoto,S., Morota, T., Ishihara, Y., Ogawa, Y., Hirori, T., Nakamura,R., Haruyama, J.: 2011, Compositional trend within the lunar
highland crust, EPSC-DPS Joint Meeting 2011, (Nantes, France,
Oct. 2-7, 2011).
Okada, T., et al. including Arai, T.: 2012, Thermal Infrared Imager
TIR on Hayabusa 2 to Investigate Physical Properties of C-Class
Near-Earth Asteroid 1999JU3, 43rd Lunar and Planetary
Science Conference, (Woodlands, TX, USA, Mar. 19-23, 2012).
Okamoto, T. J., De Pontieu, B.: 2011, Propagating waves along
spicules, The 5th Hinode Science Meeeting, (Boston, MA,
USA, Oct. 11-15, 2011).
Okamoto, T. J., De Pontieu, B.: 2012, Propagating waves along
spicules, SDO-4/ IRIS/ Hinode Workshop, (Monterey, USA,
Mar. 12-16, 2012).
Okita, K., Ohtani, H., Yoshida, F., Ito, T.: 2012, Assemble andTest of New CCD Camera System for Kiev 60 cm Telescope,
3rd Maidanak Observatory Users Meeting, (Mitaka, Japan, Jan.
31-Feb. 1, 2012).

Oshima, A.: 2011, Cosmic ray anisotropy observed by GRAPES-3
air shower array, 32nd Int. Cosmic Ray Conf., (Beijing, China,
Aug. 11-18, 2011).
Oshima, A.: 2011, Estimation of 3D structures of cosmic-ray low
density region behind shock waves associated with solar flares,
32nd Int. Cosmic Ray Conf., (Beijing, China, Aug. 11-18, 2011).
Oshima, A.: 2011, Rigidity dependence of the solar-wind-effect on
cosmic-ray intensities associated with Solar activity, 32nd Int.
Cosmic Ray Conf., (Beijing, China, Aug. 11-18, 2011).
Oshima, A.: 2012, Contamination of radioactive caesium in soil inthe campus of NAOJ Mitaka, 3rd Maidanak Observatory Users
Meeting, (Mitaka, Japan, Jan. 30-Feb. 1, 2012).
Otsubo, T., Kunimori, H., Noda, H., Hanada, H., Araki, H.,
Katayama, M.: 2011, Optical design for next-generation singlereflector LLR targets, AGU Fall Meeting 2011, (San Francisco,
CA, USA, Dec. 5-9, 2011).
Otsubo, T., Noda, H., Araki, H., Kunimori, H., Hanada, H.:
2011, Simulation of optical response for next-generation singlereflector LLR targets: Asymmetric dihedral angle offsets, 17th
Int. Workshop on Laser Ranging, (Bad Kötzting, Germany, May
16-20, 2011).
Otsuji, K., Kitai, R., Ichimoto, K., Shibata, K.: 2011, Statistical
Study on the Nature of Solar Flux Emergence, The 5th Hinode
Science Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Oyama, T.: 2011, Astrometric observations toward the galactic
center region, 1st VERA-KVN science working group, (Mitaka,
Japan, Jun. 13-14, 2011).
Oyama, T.: 2012, Astrometric observations of maser sources in thegalactic center region with VERA and VLBA, IAU Symp. 287,
"Cosmic Masers - from OH to H0", (Stellenbosch, South Africa,
Jan. 30-Feb. 3, 2012).
Parthasarathy, M.: 2011, Chemical Composition of UV-BrightStars in Globular Clusters, 3rd Subaru Int. Conf., 1st NAOJ
Symp., Galactic Archaeology: Near-Field Cosmology and theFormation of the Milky Way, (Shuzenji, Japan, Nov. 1-4, 2011).
Reznikova, V., Shibasaki, K., Nakariakov, V., Sych, R.: 2011,
Three-minutes oscillations over sunspot umbra observed with
SDO and NoRH, 13th European solar Physics Meeting, (Rhodes,
Greece, Sep. 12-16, 2011).
Reznikova, V., Shibasaki, K., Nakariakov, V., Sych, R.: 2011,
Three-minutes oscillations over sunspot: SDO and NoRH
data analysis, LWS/SDO Workshop "Many Spectra of Solar
Activity", (Tahoe, CA, USA, May 1-5, 2011).
Reznikova, V., Shibasaki, K., Nakariakov, V., Sych, R.: 2011,
Three-minutes oscillations over sunspot: SDO/AIA and NoRH
data analysis, 11th Asian-Pacific Regional IAU Meeting,(Chiang Mai, Thailand, Jul. 26-29, 2011).
Reznikova, V., Shibasaki, K.: 2011, The slow magnetoacoustic
mode in the flaring loop, 11th Asian-Pacific Regional IAU
Meeting, (Chiang Mai, Thailand, Jul. 26-29, 2011).
Saiki, K., Arai, T., Araki, H., Ishihara, Y., Ohtake, M., Karouji, Y.,
Kobayashi, N., Sugihara, T., Haruyama, J., Honda, C., Sato, H.,
Takeda, H.: 2011, Landing Site Evaluation for the Nest Lunar
Exploration Project: SELENE-2, AGU Fall Meeting 2011, (SanFrancisco, CA, USA, Dec. 5-9, 2011).
Saiki, K., Arai, T., Araki, H., Ishihara, Y., Ohtake, M., Karouji,

Y., Kobayashi, N., Sugihara, T., Haruyama, J., Honda, C., Sato,
H., Takeda, H.: 2012, Report on Landing Site Evaluation for the
Next Lunar Exploration Project: SELENE-2, The 6th KAGUYA(SELENE) Science Working Team Meeting (SWTM6),(Nagoya, Japan, Jan. 10-12, 2012).
Saito, M., Kitamura, Y., Momose, M., Tsukagoshi, T., Kawabe, R.:
2012, Aperture Synthesis Observations Toward The Protostellar
Systems L1551 Irs 5 And Hl Tau: Rotation In The Infalling
Envelope, AAS Meeting #219, (Austin, TX, USA, Jan. 8-12, 2012).
Saito, M.: 2011, ALMA Antenna, XXX URSI General Assemblyand Scientific Symp. of Int. Union of Radio Science, (Istanbul,
Turkey, Aug. 13-20, 2011).
Sakai, N.: 2012, Galactic Outer Rotation Curve with VERA+KVN,
2nd VERA-KVN science working group, (Seoul, Korea, Feb.
15-16, 2012).
Sakai, N.: 2012, Mass distribution of the Galaxy using H2O maser
with VERA, IAU Symp. 287, "Cosmic Masers - from OH to
H0", (Stellenbosch, South Africa, Jan. 30-Feb. 3, 2012).
Sakurai, T.: 2012, Magnetic Helicity as a Probe of Magnetic FluxTube Dynamics in the Solar Interior, Plasma Astrophysics:
Acquired Knowledge and Future Perspectives, (Leuven,
Belgium, Feb. 22-24, 2012).
Sasaki, S., Araki, H., Hanada, H., Iwata, T., Namiki, N.,
Matsumoto, K., Noda, H., Ishihara, Y., Goossens, S., Kikuchi,F., Kawano, N., Tazawa, S., Tsuruta, S., Asari, K., Ishikawa, T.,
Morota, T., Liu, Q., Harada, Y.: 2011, The First Precise Gravity
and Topography of the Global Moon by KAGUYA (SELENE),
Astro Kazan 2011, (Kazan, Russia, Aug. 22-30, 2011).
Sasaki, S., Araki, H., Goossens, S., Hanada, H., Ishihara, Y.,
Kikuchi, F., Matsumoto, K., Noda, H., Kawano, N., Kono, Y.,
Yamada, R., Iwata, T., Namiki, N., Kunimori, H., Funazaki, K.:
2012, Selenodesy from KAGUYA to SELENE-2, MISASA IV
Solar System Exploration and New Geosciences -Perspective
for the Next Decade-, (Tottori, Japan, Feb. 24-26, 2012).
Sasaki, S., Fujimoto, M., Takashima, T., Yano, H., Kasaba, Y.,
Kimura, J., Takahashi, Y., Tsuda, Y., Funase, R., Mori, O.: 2011,
The Jupiter Magnetospheric Orbiter and the Trojan Asteroid
Explorer in EJSM (Europa Jupiter System Mission), 28th Int.
Symp. on Space Technology and Science (28th ISTS), (Okinawa,
Japan, Jun. 5-12, 2011).
Sasaki, S., Fujimoto, M., Yano, H., Takashima, T., Kasaba, Y.,
Takahashi, Y., Kimura, J., Funase, R., Mori, O., Tsuda, Y.,
Campagnola, S., Kawakatsu, Y.: 2011, Japanese mission planfor Jupiter system: The Jupiter magnetospheric orbiter andthe Trojan asteroid explorer, EPSC-DPS Joint Meeting 2011,(Nantes, France, Oct. 2-7, 2011).
Sasaki, S., Goossens, S., Ishihara, Y., Araki, H., Hanada, H.,
Matsumoto, K., Noda, H., Kikuchi, F., Iwata, T.: 2012,
KAGUYA Selenodesy and the South Pole Aitken basin, 43rd
Lunar and Planetary Science Conference, (Woodlands, TX,
USA, Mar. 19-23, 2012).
Sasaki, S., Hanada, H., Noda, H., Kikuchi, F., Araki, H., Matsumoto,K., Iwata, T., Goossens, S., Kunimori, H., Ootsubo, T.: 2011,
Lunar gravity and rotation measurements by Japanese lunar
landing missions, 28th Int. Symp. on Space Technology and
Science (28th ISTS), (Okinawa, Japan, Jun. 5-12, 2011).

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087

Sasaki, S., Hiroi, T., Yokota, Y., Matsunaga, T.: 2011, Possible
Variation of Space Weathering Degree on Mercury: Lessons
from the Moon, Asia Oceania Geosciences Society 2011, (Taipei,
Taiwan, Aug. 8-12, 2011).
Sasaki, S., Hiroi, T.: 2011, Difference of Space Weathering Degreeof Asteroids: Lessons from Itokawa, 28th Int. Symp. on SpaceTechnology and Science (28th ISTS), (Okinawa, Japan, Jun.
5-12, 2011).
Sasaki, S., Hiroi, T.: 2011, Space weathering of Itokawa, a small
rubble pile asteroid, EPSC-DPS Joint Meeting 2011, (Nantes,
France, Oct. 2-7, 2011).
Sasaki, S., Ishihara, Y., Araki, H., Matsumoto, K., Goossens, S.,
Hanada, H., Ohtake, M., Iwata, T.: 2011, Structure of the South
Pole Aitken basin from KAGUYA selenodesy data, 28th Int.
Symp. on Space Technology and Science (28th ISTS), (Okinawa,
Japan, Jun. 5-12, 2011).
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Goossens, S.,
Namiki, N., Iwata, T., Hanada, H., Matsumoto, K., SELENE
Topography/Gravity Team Group.: 2011, The first precise global
gravity and topography of the Moon by KAGUYA (SELENE),
28th Int. Symp. on Space Technology and Science (28th ISTS),(Okinawa, Japan, Jun. 5-12, 2011).
Sasaki, S., Ishihara, Y., Araki, H., Noda, H., Hanada, H.,
Matsumoto, K., Goossens, S., Kikuchi, F., Iwata, T., Namiki,N.: 2011, The First Accurate Global Gravity and Topography of
the MOON by KAGUYA (SELENE) and Implication for Lunar
Basin Evolution, Asia Oceania Geosciences Society 2011,(Taipei, Taiwan, Aug. 8-12, 2011).
Sasaki, S., Ishihara, Y., Goossens, S., Matsumoto, K., Araki, H.,
Hanada, H., Kikuchi, F., Noda, H., Iwata, T., Ohtake, M.: 2011,
Structure of lunar crust from KAGUYA selenodesy data, EPSCDPS Joint Meeting 2011, (Nantes, France, Oct. 2-7, 2011).
Sasaki, S., Noda, H., Kikuchi, F., Kumimori, H., Araki, H.,
Matsumoto, K., Goossens, S., Ishihara, Y., Hanada, H., Otsubo,
H., Iwata, T.: 2011, Lunar rotation and gravity measurements by
SELENE-2 and future landers, EPSC-DPS Joint Meeting 2011,(Nantes, France, Oct. 2-7, 2011).
Sasaki, S.: 2011, Science of Mercury Dust Monitor, BepiColombo
Science Working Group Meeting, (Ishikawa, Japan, Sep. 8-10, 2012).
Sasaki, S.: 2012, KAGUYA and Beyond: Summary of Selenodesy
Results and Future Plans, Int. Symp. on Lunar and Planetary
Science 2012, (Macau, China, Mar. 26-27, 2012).
Sasaki, S.: 2012, State of the core and lower mantle should
constrain the lunar origin, The 6th KAGUYA (SELENE)
Science Working Team Meeting (SWTM6), (Nagoya, Japan,
Jan. 10-12, 2012).
Sasaki, T., Yao, Y., Yoshida, M., Ohshima, N., Mikami, Y.,
Okada, N., Koyanao, H., Sekiguchi, K., Liu, L., Li, L.: 2011,
A China-Japan Collaborative Site Survey in west Tibet Sky
clearness at Oma, Tibet, 11th Asian-Pacific Regional IAU
Meeting, (Chiang Mai, Thailand, Jul. 26-29, 2011).
Sawada-Satoh, S.: 2011, Amplitude Calibration of the KVN+VERAArray, 4th East Asia VLBI Workshop — Sciences and Technology
by now and future, (Lijiang, China, Apr. 18-20, 2011).
Sawada-Satoh, S.: 2011, Early Phase Observations of the
KVN+VERA Joint Array, 11th Asian-Pacific Regional IAU

088

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Meeting, (Chiang Mai, Thailand, Jul. 26-29, 2011).
Sawada-Satoh, S.: 2011, Molecular absorption lines as new tracers
in circumnuclear region, 1st VERA-KVN science working
group, (Mitaka, Japan, Jun. 13-14, 2011).
Sawada-Satoh, S.: 2011, Recent results of VERA, KVN/TRAO
Users Meeting, (Busan, Korea, Aug. 25-26, 2011).
Sawada-Satoh, S.: 2012, Internal Proper Motion of 6.7 GHz
Methanol Masers in Ultra Compact HII Region S269, IAU
Symp. 287, "Cosmic Masers - from OH to H0", (Stellenbosch,South Africa, Jan. 30-Feb. 3, 2012).
Sawada-Satoh, S.: 2012, Search for Molecular Absorptions on
Acrive Galactic Nuclei, 2nd VERA-KVN science working
group, (Seoul, Korea, Feb. 15-16, 2012).
Sekiguchi, K.: 2011, Astronomy: "Then", "Now" and "Future", The
5th Annual Int. Workshop on Applications of Remote Sensing
and Space Science in Mongolia, (Ulaanbaatar, Mongolia, Jun.
6-7, 2011).
Sekiguchi, K.: 2011, Collaboration in Astronomy between Egypt
and Japan, 2nd Middle-East and Africa Regional IAU Meeting,(Cape Town, South Africa, Apr. 10-15, 2011).
Shibasaki, K.: 2011, Diamagnetic and Non-linear Nature of
Plasma as a Cause of Solar Activities, PROM2011 Workshop"Prominence Research: Observations and Models", (Pasadena,
CA, USA, Dec. 13-15, 2011).
Shibasaki, K.: 2011, Measurements of Total Radio Flux fromthe Sun for Sixty Years, The first ICSU World Data system
Conference "Global Data for Global Science", (Kyoto, Japan,
Sep. 3-6, 2011).
Shibasaki, K.: 2011, Radio Imaging Observations of Solar
Activity Cycle and Its Anomaly, AGU Fall Meeting 2011, (SanFrancisco, CA, USA, Dec. 4-9, 2011).
Shibasaki, K.: 2011, Radio Imaging Observations of Solar
Activity Cycle and Its Anomaly, The 2nd Nagoya Workshop on
the Relationship between Solar Activity and Climate Changes,(Nagoya, Japan, Jan. 16-17, 2012).
Shibata, K. M.: 2012, VERA status, 2nd VERA-KVN science
working group, (Seoul, Korea, Feb. 15-16, 2012).
Shimizu, T., Ichimoto, K., Suematsu, Y.: 2011, Precursor ofsunspot penumbral formation discovered with Hinode SOT
observations, The 5th Hinode Science Meeeting, (Boston, MA,
USA, Oct. 11-15, 2011).
Shimojo, M., ALMA project: 2012, Millimeter/sub-millimeter wave
observations for chromospheric science, SDO-4/ IRIS/ Hinode
Workshop, (Monterey, USA, Mar. 12-16, 2012).
Shimojo, M., Tsuneta, S., Shiota, D., Itoh, H.: 2011, The Solar Polar
Region Observed with Hinode, Sun-360: Stereo-4, SDO-2,
SOHO-25 Workshop, (Kiel, Germany, Jul. 25-29, 2011).
Shimojo, M.: 2011, Acceleration & Heating in Prominence Eruption
Observed in Radio & EUV, Japan-Korea Space Weather
Workshop 2011: Current Status and Prospect of Space Weather
Modeling and Obervation, (Daejeon, Korea, Sep. 29-Oct. 1, 2011).
Shimojo, M.: 2011, The Solar polar field from Hinode, Sun-360:
Stereo-4, SDO-2, SOHO-25 Workshop, (Kiel, Germany, Jul.
25-29, 2011).
Shiota, D., Tsuneta, S., Orozco Suarez, D., Shimojo, M., Sako, N.:
2011, Yearly Variation of Magnetic Field in the Polar Regions

Observed with Hinode, The 5th Hinode Science Meeeting,(Boston, MA, USA, Oct. 11-15, 2011).
Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto, Y., Ishihara, Y.,
Tsutsumi, J., Hiyama, T., Nakamoto, H., Sakamoto, M.: 2011,
Current status of VO compliant data service in Japanese Virtual
Observatory, ADASS XXI Conference, (Paris, France, Nov.
6-10, 2011).
Shirasaki, Y., Tanaka, M., Ohishi, M., Mizumoto, Y., Yasuda, N.,
Takata, T.: 2011, AGN and Galaxy Clustering at z = 0.3 to 3.0
measured by using the Japanese Virtual Observatory, Galaxy
Formation 2011, (Durham, UK, Jul. 18-22, 2011).
Shum, C, K., Fok, H, S., Yi, Y., Dai, C., Araki, H., Matsumoto,K., Sasaki, S., Bâki Iz, H., Ding, X., Ping, J.: 2012, Improved
Lunar Topography Model Using Laser Altimetry from Multiple
Orbiters!, The 6th KAGUYA (SELENE) Science Working Team
Meeting (SWTM6), (Nagoya, Japan, Jan. 10-12, 2012).
Sôma, M., Tanikawa, K.: 2011, Determination of ΔT and Lunar
Tidal Acceleration from Ancient Eclipses and Occultations,
StephensonFest, (Durham, UK, Apr. 13-16, 2011).
Sotani, H., Yasutake, N., Maruyama, T., Tatsumi, T.: 2011, Signaturesof hadron-quark mixed phase in gravitational waves, 20thStellar Pulsation Conf. Series, (Granada, Spain, Sep. 5-9, 2011).
Sotani, H.: 2011, Constraints on Pasta Structure of Neutron Stars, 20thStellar Pulsation Conf. Series, (Granada, Spain, Sep. 5-9, 2011).
Sotani, H.: 2011, Effect of Pasta Phase on Oscillations in NeutronStars, 21st Workshop on General Relativity and Gravitation(JGRG21), (Sendai, Japan, Sep. 26-29, 2011).
Sotani, H.: 2011, Imprint of Alternative Theories, Numerical
Relativity and High Energy Physics, (Madeira, Portugal, Aug.
31-Sep. 3, 2011).
Sotani, H.: 2011, Probing the Pasta Structure of Neutron Stars,
Frontier Issues in Physics of Exotic Nuclei (YKIS2011), (Kyoto,
Japan, Oct. 11-15, 2011).
Sotani, H.: 2011, Nonuniform nuclear structures and QPOs in
giant flares, 11th Int. Symp. on Origin of Matter and Evolutionof Galaxies, (Wako, Japan, Nov. 14-17, 2011).
Sotani, H.: 2011, Probing nuclear properties via asteroseismology
in neutron stars, YITP-KoRIA Workshop on Nuclear Symmetry
Energy, (Kyoto, Japan, Nov. 10-12, 2011).
Suda, T., Hirschi, R., Fujimoto, M. Y.: 2010, Triple-alpha Reaction
Rates Constrained by Stellar Evolution Models, 11th Int. Symp.
on Origin of Matter and Evolution of Galaxies, (Wako, Japan,
Nov. 14-17, 2011).
Suda, T., Yamada, S., Katsuta, Y., Komiya, Y., Fujimoto, M. Y.:
2010, Star Formation History of Our Galaxy Explored withAGB Star Evolution Models, 3rd Subaru Int. Conf., 1st NAOJ
Symp., Galactic Archaeology: Near-Field Cosmology and theFormation of the Milky Way, (Shuzenji, Japan, Nov. 1-4, 2011).
Suematsu, Y., Sano, I., Ueno, S.: Integral Field Spectroscopy of the
Sun with Microlens Array and Liquid Crystal Retarders, AGU
Fall Meeting 2011, (San Francisco, CA, USA, Dec. 5-9, 2011).
Suematsu, Y., Yatini, C. Y.: 2011, Study of Short-Term Sunspot
Motion toward Flare Onset Prediction, AGU Fall Meeting 2011,(San Francisco, CA, USA, Dec. 5-7, 2011).
Suematsu, Y., Yatini, C. Y.: 2011, Study of Sunspot Proper Motion
toward Flare Onset Prediction, Asia Oceania Geosciences

Society 2011, (Taipei, Taiwan, Aug. 8-12, 2011).
Suematsu, Y.: 2011, Study of Small-Scale Chromospheric
Plasmoid Ejections with Improved Hinode Ca II H Filtergrams,
The 5th Hinode Science Meeeting, (Boston, MA, USA, Oct.
11-15, 2011).
Suematsu, Y.: Instrument Design of Large Aperture Solar UVVisible and IR Observing Telescope for SOLAR-C Mission,
2nd ATST-EAST Workshop in Solar Physics, (Washington, DC,
USA, Oct. 9-11, 2011).
Tachihara, K., Saigo, K., Higuchi, A., Inoue, T., Inutsuka, S.:
2012, Small Scale Structures as Units of Dynamical MultiPhase Interstellar Medium, AAS Meeting #219, (Austin, TX,
USA, Jan. 8-12, 2012).
Takahashi, H. R., Ohsuga, K.: 2011, Magnetic Energy Release in
Relativistic Plasma, IAU Symp. 279, "Death of Massive Stars:
Supernovae and Gamma-Ray Bursts", (Nikko, Japan, Mar.
12-16. 2012).
Takahashi, H. R.: 2012, Numerical Study of Relativistic Magnetic
Reconnection with R3MHD Codes, Int. Workshop on Particles
and Radiation from Cosmic Accelerators (CA2012), (Chiba,
Japan, Feb. 20-22, 2012).
Takahashi, R.: 2011, Vibration Isolation, 4th LCGT face to facemeeting, (Kashiwa, Japan, Aug. 3-5, 2011).
Takahashi, R.: 2012, Seismic Attenuation System (SAS) for
LCGT, 1st Korea-Japan Workshop on LCGT, (Souel, Korea,
Jan. 12-13, 2012).
Takahashi, R.: 2012, Vibration Isolation, 5th KAGRA face to facemeeting, (Kashiwa, Japan, Feb. 2-4, 2012).
Takano, S., et al. including Hirota, T., Nakajima, T., Ohishi, M.,
Umemoto, T.: 2011, Nobeyama 45m telescope legacy project:
Line survey, IAU symp. 280, "The Molecular Universe",(Toledo, Spain, May 30-Jun. 3, 2011).
Takeda, Y.: 2011, Application of Iodine-Cell Technique to HighPrecision Radia-Velocity Studies of the Solar Disk, Workshop
on Astronomy with Precise Radial Velocity - Exoplanet Searchand Asteroseismology, (Seoul, Korea, Sep. 25-28, 2011).
Takiwaki, T.: 2012, Three-dimensional Hydrodynamic CoreCollapse Supernova Simulations for an 11.2 Ms Star with Spectral
Neutrino Transport, 11th Int. Symp. on Origin of Matter and
Evolution of Galaxies, (Wako, Japan, Nov. 14-17, 2011).
Takiwaki, T.: 2012, Three-dimensional simulations of corecollapse supernovae, Nuclear, Particle and Astrophysics
Seminar, (Basel, Switzerland, Mar. 22, 2012).
Takiwaki, T.: 2012, Three-dimensional simulations of corecollapse supernovae, Formations of compact objects: from thecradle to the grave, (Tokyo, Japan, Mar. 8, 2012).
Takiwaki, T.: 2012, Three-dimensional simulations of corecollapse supernovae, 16th Workshop on "Nuclear Astrophysics",(Ringberg, Germany, Mar. 30, 2012).
Tamura, M., SEEDS team: 2011, Direct imaging of exoplanetsand their formation sites with Subaru, "Germany-Japan
Round Table", (Heidelberg, Germany, Dec. 1-3, 2011).
Tamura, M., SEEDS team: 2011, Early Result from SEEDS and
The Subaru's Next Step, Exploring Strange New Worlds: From
Giant Planets to Super Earths, (High Country ConferenceCenter, AZ, USA, May 2-6, 2011).

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Tamura, M., SEEDS team: 2011, SEEDS Overview, SEEDS 2ndGeneral Workshop, (Heidelberg, Germany, Oct. 10-12, 2011).
Tamura, M., SEEDS team: 2011, Strategic Explorations of
Exoplanets and Disks with Subaru and its next step, Ishigaki
International Workshop "Formation of Stars & Planets 2011
(FSP2011)", (Ishigaki, Okinawa, Japan, Oct. 3-7, 2011).
Tamura, M., SEEDS team: 2012, SEEDS Status, Subaru Users
Meeting 2011, (Mitaka, Japan, Feb. 28-Mar. 1, 2012).
Tamura, Y.: 2012, Monitoring of coordinates and estimation of
wet zenith delay at VERA stations by GPS, 2nd VERA-KVN
science working group, (Seoul, Korea, Feb. 15-16, 2012).
Tanaka, M.: 2012, Spectropolarimetry of Type Ibc Supernovae,
IAU Symp. 279, "Death of Massive Stars: Supernovae andGamma-Ray Bursts", (Nikko, Japan, Mar. 12-16. 2012).
Tazawa, S., Noda, H., Araki, H., Ishihara, Y., Kawano, N., Sasaki,
S.: 2011, Behavior of return pulse intensity data obtained by thelaser altimeter onboard KAGUYA, 28th Int. Symp. on SpaceTechnology and Science (28th ISTS), (Okinawa, Japan, Jun.
5-12, 2011).
Terai, T., Itoh, Y., Jewitt, D.: 2011, Photometric Observations for
the Brightness Variations on the Irregular Satellites of Uranus
and Neptune, Asia Oceania Geosciences Society 2011, (Taipei,
Taiwan, Aug. 8-12, 2011).
Tomida, K., Machida, M. N., Saigo, K., Tomisaka, K., Matsumoto,T.: 2011, Exposed Long-lifetime First core: Star formation invery low-mass molecular cloud cores, Formation and Early
Evolution of Very Low Mass Stars and Brown Dwarfs, (ESO
Garching, Germany, Oct. 11-14, 2011)
Tomida, K., Tomisaka, K., Kawabe, R., Saigo, K., Machida,
M. N., Matsumoto, T., Hori, Y.: 2011, RMHD simulationsof protostellar collapse, Ishigaki International Workshop"Formation of Stars & Planets 2011 (FSP2011)", (Ishigaki,
Okinawa, Japan, Oct. 3-7, 2011).
Toyokuni, G., Ishihara, Y., Takenaka, H.: 2011, Global seismic
waveform modeling in the whole Mars -a preliminary study-,
EPSC-DPS Joint Meeting 2011, (Nantes, France, Oct. 2-7, 2011).
Tsujimoto, T.: 2011, Galactic Chemical Evolution in the context of
the recently revealed SN Ia delay time distribution, IAU Symp.
281, "Binary Paths to the Explosions of Type Ia Supernovae",(Padova, Italy, Jul. 4-8, 2011).
Tsujimoto, T.: 2012, The IMF variation and short-delayed SNe Ia
in the context of Galactic chemical evolution, The Chemical
Evolution of the Milky Way, (Sesto, Italy, Jan. 23-27, 2012).
Tsukamoto, Y., Machida, N. M.: 2011, The formation andevolution processes of circum stellar disk, Ishigaki International
Workshop "Formation of Stars & Planets 2011 (FSP2011)",(Ishigaki, Okinawa, Japan, Oct. 3-7, 2011).
Tsuneta, S., Solar-C Working Group: 2011, Solar-C mission
with Solar-D on the horizon, The 5th Hinode Science Meeeting,(Boston, MA, USA, Oct. 11-15, 2011).
Tsuneta, S., Ueda, K., Reardon, K., Cauzzi, G., Ishikawa, R.: 2011,
Evidence of magnetic heating of chromosphere, The 5th Hinode
Science Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Tsuneta, S.: 2011, Solar-C status and Science Goals overview,
Solar-C Meeting, (Boston, MA, USA, Oct. 16, 2011).
Umemoto, T., Saito, M., Nakanishi, K., Kuno, N., Tsuboi, M.:

090

II Publications, Presentations

2011, Radio Flare at Millimeter-wavelengths from Young
Stellar Objects, Star Formation through Spectroimaging at High
Angular Resolution, (Taipei, Taiwan, Jun. 20-24, 2011).
Urakawa, S., Okumrua, S., Nishiyama, K., Sakamoto, T., Takahashi,N., Abe, S., Ishiguro, M., Kitazato, K., Kuroda, D., Hasegawa, S.,
Ohta, K., Kawai, N., Shimizu, Y., Nagayama, S., Yanagisawa,
K., Yoshida, M., Yoshikawa, M.: 2011, Photometric Observationsof 107P/4015Wilson-Harrington, Asia Oceania Geosciences
Society 2011, (Taipei, Taiwan, Aug. 8-12, 2011).
Urakawa, S., Okumrua, S., Nishiyama, K., Sakamoto, T., Takahashi,N., Abe, S., Ishiguro, M., Kitazato, K., Kuroda, D., Hasegawa, S.,
Ohta, K., Kawai, N., Shimizu, Y., Nagayama, S., Yanagisawa,
K., Yoshida, M., Yoshikawa, M.: 2011, Photometric Observationsof 107P/Wilson-Harrington, EPSC-DPS Joint Meeting 2011,(Nantes, France, Oct. 2-7, 2011).
Usuda, T., Arimoto, N.: 2011, Status and Future view of Subaru
Telescope, Keck Science Meeting, (Pasadena, CA, USA, Sep.
23-24, 2011).
Uzawa, Y., Saito, S., Kuroiwa, K., Kroug, M., Fujii, Y., Takeda,M., Makise, K., Wang, Z., Hosako, I.: 2011, Direct Observationof Superconducting Gap Broadening in a Niobium Nitride filmby Terahertz Time Domain Spectroscopy, Superconductivity
Centennial Conf. (EUCAS-ISEC-ICMC 2011), (Hague,
Netherlands, Sep. 18-23, 2011)
Uzawa, Y.: 2011, Current status and future development of Band
10 cartridge, EA ALMA development workshop, (Mitaka,
Tokyo, Japan, Sep. 8, 2011).
Uzawa, Y.: 2011, Heterodyne receivers for submm and THz bands,
Large Aperture Millimeter/Submillimeter Telescopes in the
ALMA Era, (Osaka, Japan, Sep. 12-13, 2011).
Wada, T., Takata, J., Shibata, S.: 2011, Particle Simulation for
the Axisymmetric Pulsar Magnetosphere, 2nd Fermi Asian
Network (FAN) Workshop, (Hsinchu, Taiwan, Aug. 1-5, 2011).
Wada, T.: 2012, A Particle Simulation for the Axisymmetric Pulsar
Magnetosphere, Int. Workshop on Particles and Radiation from
Cosmic Accelerators (CA2012), (Chiba, Japan, Feb. 20-22, 2012).
Watanabe, T., Hara, H., Imada, S., Watanabe, K., Shimizu, T.:2011, High-Temperature & High-Speed Downflows in an
Impulsive Flare of 2011 March 12, The 5th Hinode Science
Meeeting, (Boston, MA, USA, Oct. 11-15, 2011).
Watanabe, T., Sterling, A. C., Harra, L. K., Hara, H.: 2011,
Small Loop-loop Interaction in the Initial Phases of A C9.7
Flare, Sun-360: Stereo-4, SDO-2, SOHO-25 Workshop, (Kiel,
Germany, Jul. 25-29, 2011).
Wisniewski, J. P., Fukagawa, M., Goto, M., Grady, C., Hashimoto,J., Henning, T., Hodapp, K., Honda, M., Janson, M., Kudo, T.,
Thalmann, C., Whitney, B., Tamura, M., SEEDS Team: 2012,
SEEDS Polarimetric Differential Imaging of LkCa 15, AAS
Meeting #219, (Austin, TX, USA, Jan. 8-12, 2012).
Yagi, M.: 2012, Crosstalk in Suprime-Cam, Subaru Users Meeting
2011, (Mitaka, Japan, Feb. 28-Mar. 1, 2012).
Yamada, R., Shiraishi, H., Kobayashi, N., Takeuchi, N., Murakami,
H., Tanaka, S., Okamoto, T., Ishihara, Y., Hayakawa, M.,
Hayakawa, H., Garcia, R., Lognonne, P.: 2012, Exploration of
the Materials in Lunar Deep Region using the Seismological
Method, MISASA IV Solar System Exploration and New

Geosciences -Perspective for the Next Decade-, (Tottori, Japan,
Feb. 24-26, 2012).
Yamada, R., Yamamoto, Y., Nakamura, Y., Kuwamura, J.: 2012,
A New Retrieval System of Apollo Lunar Seismic Data with
Data Correction, 43rd Lunar and Planetary Science Conference,(Woodlands, TX, USA, Mar. 19-23, 2012).
Yamada, Y., Hara, T., Yoshioka, S., Kobayashi, Y., Gouda, N.,
Miyashita, H., Hatsutori, Y., Lammers, U., Michalik, D.: 2011,
Nano-JASMINE data analysis and publication, Astronomical
Data Analysis Software and Systems XX, (Paris, France, Nov.
6-10, 2011).
Yao, Y., Wang, Y., Liu, L., Zhou, Y., Li, L., Sasaki, T., Yoshida, M.,
Ohshima, N., Mikami, Y., Sekiguchi, K.: 2011, The NAOC Ali
Observatory, Tibet, 11th Asian-Pacific Regional IAU Meeting,(Chiang Mai, Thailand, Jul. 26-29, 2011).
Yasui, C., Kobayashi, N., Tokunaga, A. T., Saito, M.: 2011, The
Lifetime of Protoplanetary Disks Surrounding Intermediate-massstars, AAS Meeting #219, (Austin, TX, USA, Jan. 8-12, 2012).
Zenitani, S., Hesse, M., Klimas, A., Black, C., Kuznetsov, M.:
2011, The electron-frame dissipation measure in collisionlessmagnetic reconnection, AGU Fall Meeting 2011, (SanFrancisco, CA, USA, Dec. 3-7, 2011).

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