Cover Caption
Near-infrared (wavelength of 1.6 µm) image of young solar-type star PDS 70 (age of 10 million years) observed in the Subaru telescope.
One of the largest gap in the protoplanetary disk around PDS 70 was observed for the first time among solar-type stars.

Postscript
Editor Publications Committee
HANAOKA, Yoichiro
UEDA, Akitoshi
OE, Masafumi
SÔMA, Mitsuru
NISHIKAWA, Jun
MIYOSHI, Makoto
YOSHIDA, Haruo
Publisher National Institutes of Natural Sciences
National Astronomical Observatory of Japan
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TEL: +81-422-34-3600
FAX: +81-422-34-3960
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Annual Report of the
National Astronomical Observatory of Japan

Fiscal 2012

T A

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Masahiko HAYASHI
Director General
National Astronomical Observatory of Japan

Preface

I Scientific Highlights April 2012 – March 2013

001

II Publications, Presentations
1

Refereed Publications

065

2

Publications of the National Astronomical Observatory of Japan

077

3

Report of the National Astronomical Observatory of Japan

077

4

Conference Proceedings

077

5

Publications in English

092

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Conference Presentations

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Annual Report of the
National Astronomical Observatory of Japan
Fiscal 2012

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

It is my pleasure to present our Annual Report for the
fiscal year 2012.
FY 2012 celebrated the inauguration of ALMA,
which has almost finished the installation of the total 66
antennas, and acceptance/commissioning of the receivers
and correlators. The inauguration ceremony was held at
the Operations Support Facility (OSF) at an altitude of2900 meters on March 13, 2013 with the attendance ofover 400 guests including President Pinera of Chile. FromJapan, more than 50 people attended the ceremony. Teru
Fukui, Senior Vice Minister of Education, Culture, Sports,
Science and Technology, made a speech expressing
continued strong support of the Japanese government to
ALMA. On the following day, most of the guests visited
the Array Operations Site (AOS) at 5000 meters.
ALMA started its open-use early science observations(Cycle 0) with 16 antennas from 2011, and began todeliver its early results from the second half of FY 2012.
Although the current angular resolution of ALMA isonly 1 arcsec (1/3600 of one degree), ALMA has alreadyachieved overwhelmingly high sensitivity. ALMA
revealed a totally unexpected spiral structure of gas
around a low-mass star (similar to the Sun) which isemitted at the end of its life before evolving to a whitedwarf. This is a whole new picture of the universe that wehave never seen before. We are excited to see what will
be discovered by ALMA with further improved resolution
and sensitivity.
On the other hand, we had very sad news of theaccidental death of Professor Koh-Ichiro Morita
in Santiago, a leading scientist in the field of radio
interferometer who worked for the realization of Japan’s participation to ALMA by proposing the enhancementof the array with the Atacama Compact Array (ACA).
In honor of the late Professor Morita, the ALMA Board
gave the name of “Morita Array” to the ACA. We always
remember his achievement seeing the array with his
name, which brings us small comfort and relief. I believe
the only thing we can do is to devote ourselves toward theachievement of maximum scientific results with ALMA.
Meanwhile, Subaru Telescope started test observations
with new Hyper Suprime-Cam, a next-generation
prime-focus camera with a field of view about 10
times wider than the old one. This “hyper” camera has
newly-developed 116 wideband CCDs for astronomical
observations and 900 million pixels in total. It will be a
powerful tool not only in the search for distant unknown
objects where Subaru telescope demonstrates unparalleledstrength but also in the high-sensitivity survey of a wide
field to study the distribution of dark matter and darkenergy which is yet to be explored.
Remarkable scientific results on exoplanets with
Subaru Telescope should also be mentioned. Its improved
function enabled direct imaging of Jupiter-like gaseousplanets and revealed the existence of a giant gaseousplanet in a place far from the central star, equivalent
to the distance between the Sun and Pluto in the solar
system. Also, Subaru successfully imaged a number ofprotoplanetary disks, many of which have a spiral or ring
structure. It is expected that further study using ALMA
observation data as well will enhance the understandingof planetary formation.
The Thirty Meter Telescope (TMT) is making steadyprogress in the preparation for the construction. TMT isan optical-infrared telescope to be built on the summitof Mauna Kea in international partnership of National
Astronomical Observatory of Japan (NAOJ), California
Institute of Technology (Caltech), University of California(UC), Department of Science and Technology of India,
Association of Canadian Universities for Research in
Astronomy (ACURA), and National Astronomical
Observatories of the Chinese Academy of Sciences. We
still have a lot to discuss about the share of contribution
to the construction among partners and how to ensureeach partner’s budget acquisition as planned, etc. Thiskind of collaborative work is inevitable for a large-scaleinternational project. In spite of various difficulties toovercome, we are pleased to have the opportunity to leada global project and take the initiative in building a strongorganization for TMT construction.
FY 2012 celebrated the 30th anniversary of Nobeyama
Radio Observatory and we held a commemoration
ceremony in September. The NRO 45-m Telescope has
produced significant results such as the discovery ofmany kinds of new interstellar molecules and findingof evidence for the existence of a massive black hole inthe center of a galaxy. Although its aging deterioration is
not avoidable, it will still be a front-line telescope withoverwhelmingly improved receiver sensitivity.
Also, FY 2012 marks the 10th anniversary of thecompletion of VERA at the Mizusawa VLBI Observatory
for which a commemoration ceremony was held in Oshu,
Iwate. VERA provides accurate measurement of the
distance and the motion of astronomical objects thousandsof light years away from the Sun, thereby revealing
detailed kinematics and structure of the Galaxy. A recent
result shows that the Sun orbits the Galaxy at a rate 10 %faster than previously believed.
The Center for Computational Astrophysics relocatedthe supercomputer from Mitaka campus to Mizusawa
VLBI Observatory at the renewal of the lease. The newsupercomputer, named Aterui in tribute to a hero in the
Tohoku region where Iwate prefecture is situated, will
start operation from FY 2013.
In this time of dynamic change, rapid development
is required also in astronomy. While new telescopes areplanned and realized one after another, once the mostadvanced telescopes become soon out of date. In this
rapidly changing world, we reaffirm our mission to keep
up with global scientific advances and continuously
provide frontier facilities for world-wide researchers
in order to return the results of research to society as
an institute of the Inter-University Research InstituteCorporations.

Masahiko HAYASHI
Director General of NAOJ

I Scientific Highlights(April 2012 – March 2013)

01

Three-Dimensional Structure of Supernovae Studied by SpectropolarimetricObservations

TANAKA, M., et al.

003

02

Infrared Observations of “Middle-Aged” Supernovae Filling the Gap between
Supernovae and Supernova Remnants

TANAKA, M., et al.

004

KWON, J., et al.

005

TAKEDA, Y., et al.

006

YAMANOI, H., et al.

007

INOUE, S.

008

INOUE, S., GOUDA, N.

009

ZENITANI, S., et al.

010

HANAOKA, Y., et al.

011

SUZUKI, A., SHIGEYAMA, T.

012

YAGI, M., et al.

013

YAGI, M.

014

YANO, T., et al.

015

YANO, T.

016

15 AKARI/AcuA Physical Studies of the Cybele Asteroid Family

KASUGA, T., et al.

017

16 Measurements of Stellar Inclinations for Kepler Planet Candidates

HIRANO, T., et al.

018

HIRANO, T., et al.

019

SCOTT, K. S., et al.

020

MUTO, T., et al.

021

03 Near-Infrared Circular Polarization Images of NGC 6334-V
04

Detection of Low-Level Activities in Solar-Analog Stars from the Emission
Strengths of Ca II 3934 Line

05 The Galaxy Luminosity Functions down to MR = −10 in the Coma Cluster
06 Kinematic Imprint of Clumpy Disk Formation on Halo Objects
07 Astrometric Mock Observations for Determining the Local Dark Matter Density
08 Spacecraft Observation of a Central Engine of Magnetic Reconnection
09

Accurate Measurements of the Brightness of the White-Light Corona at the Total
Solar Eclipses on 1 August 2008 and 22 July 200910 Early Thermal X-Ray Emission from Long Gamma-Ray Bursts
11 Recalibration of the Photometric Zero Point of SDF/SXDS Catalogs
12 Crosstalk Analysis of New CCDs of Suprime-Cam
13 Astrometric Goal of Small-JASMINE
1417

Astrometric Error Caused by Gravitational Microlensing Effect in the Galactic
Bulge Stars

Planet-Planet Eclipse and the Rossiter-McLaughlin Effect of a Multiple
Transiting System

18 The Source Counts of Submillimetre Galaxies Detected at λ = 1.1 mm
19 Spiral Structures in the Protoplanetary Disk around SAO 206462
20

Outer Rotation Curve of the Galaxy with VERA I: Trigonometric Parallax of
IRAS 05168+3634

SAKAI, N., et al.

022

21

Polarimetric Imaging of Large Cavity Structures in the Pre-Transitional
Protoplanetary Disk around PDS 70: Observations of the Disk

HASHIMOTO, J., et al.

023

22

Molecular Gas Distributions of Interacting Galaxies in Early and Mid Stage
Using 12CO(J = 1–0) Mapping Observations

KANEKO, H., et al.

024

23 Detailed Density and Velocity Structures of the Protostellar Core B335

KURONO, Y., et al.

025

24 Explicit-Implicit Scheme for Relativistic Radiation Hydrodynamics

TAKAHASHI, H. R.

026

25 Effects of Power Law Primordial Magnetic Field on Big Bang Nucleosynthesis

YAMAZAKI, D. G.,
KUSAKABE, M.

027

A Starbursting Proto-Cluster in Making Associated with a Radio Galaxy at
z = 2.53 Discovered by Hα Imaging

HAYASHI, M., et al.

028

Mechanical Engineering Shop,
Advanced Technology Center

029

MIURA, R. E., et al.

031

29 Suzaku/WAM and RHESSI Observations of Non-Thermal Electrons in Solar Microflares

ISHIKAWA, S.-N., et al.

032

30 Magnetically Confined Interstellar Hot Plasma in the Nuclear Bulge of Our Galaxy

NISHIYAMA, S., et al.

033

26

27 In-House Manufacturing of ALMA Receiver Parts
28 Giant Molecular Cloud Evolutions in the nearby Spiral Galaxy M33

001

31

Young, Massive Star Candidates Detected throughout the Nuclear Star Clusterof the Milky Way

NISHIYAMA, S.,SCHÖDEL, R.

034

32

Asymmetric Dust Jets and Extended Structure of 22P/Kopff Observed During
2009 Appearance

HANAYAMA, H., et al.

035

33

Production of High Temperature Plasmas During the Early Phases of a C9.7 Flare. II.
Bi-Directional Flows Suggestive of Reconnection in a Preflare Brightening Region

WATANABE, T., et al.

036

TAJITSU, A., et al.

037

SEKIMOTO, Y., et al.

038

IMADA, A., et al.

039

YABE, K., et al.

040

38 Giant Molecular Clouds and Star Formation in the Tidal Molecular Arm of NGC 4039

ESPADA, D., et al.

041

39 Disentangling the Circumnuclear Environs of Centaurus A: Gaseous Spiral Arms

ESPADA, D., et al.

042

40 A large Scale Structure Traced by [O II] Emitters Hosting a Distant Cluster at z = 1.62

TADAKI, K.-I., et al.

043

TOSHIKAWA, J., et al.

044

CARSON, J., et al.

045

KUSAKABE, N., et al.

046

34 The Image Slicers for the Subaru Telescope High Dispersion Spectrograph
35 MKID 102 Pixel Millimeter-Wave Camera Development
36 Discovery of Superhumps during a Normal Outburst of SU Uma
37 NIR Spectroscopy of Star-Forming Galaxies at z ~ 1.4 with Subaru/FMOS

41 Discovery of a Protocluster at z ~ 6
42 Direct Imaging Discovery of a ‘Super-Jupiter’ around the Late B-Type Star κ And
43 High-Contrast Near-Infrared Polarization Imagin of MWC 480
44

Optics Design and Optimizations of the Multi-Color TES Bolometer Camera for
the ASTE Telescope

TAKEKOSHI, T., et al.

047

45

Three-Dimensional Hydrodynamic Core-Collapse Supernova Simulations for an
11.2 M Star with Spectral Neutrino Transport

TAKIWAKI, T.

048

HONMA, M., et al.

049

ONODERA, S., et al.

050

48 The Origin and Maintenance of a Retrograde Exoplanet

NARITA, N., et al.

051

49 3D Dissipation Mechanism in Fast Magnetic Reconnection

FUJIMOTO, K.

052

KATSUKAWA, Y.,
OROZCO SUÁREZ, D.

053

51 Astrophysical Impact of New β-decay Half-lives on r-process Nucleosynthesis

NISHIMURA, N., et al.

054

52 Solution to Big-Bang Nucleosynthesis in Hybrid Axion Dark Matter Model

KUSAKABE, M., et al.

055

Supernova-, Solar- and Reactor-Neutrino Detection and Precise Theoretical
Calculation of Neutrino Capture Cross Section on 13C

SUZUKI, T., et al.

056

54 Subaru Imaging of Asymmetric Features in a Transitional Disk in Upper Scorpius

MAYAMA, S., et al.

057

55 The Detection of C60 in the Well-Characterized Planetary Nebula M1-11

OTSUKA, M., et al.

058

MATHEWS, G. J., et al.

059

NAKAMURA, F., et al.

060

46 Fundamental Structure of the Galaxy Determined with VERA
47

50

53

56

NRO M33 All-Disk Survey of Giant Molecular Clouds (NRO MAGiC): II.
Dense Gas Formation within Giant Molecular Clouds in M33

Power Spectral Analysis of the Magneto-Convection on the Solar Surface with
HINODE SOT

Exploring the Neutrino Mass Hierarchy Probability with Meteoritic Supernova
Material, ν-Process Nucleosynthesis, and θ13 Mixing

57 Substellar-Mass Condensations in Prestellar Cores
58

Early Galactic Chemical Evolution and r-Process Nucleosynthesis in BlackHole Forming Supernovae

AOKI, W., et al.

061

59

High-Lying Excited States in Gamow Teller Strength and Their Roles on
Neutrino Reactions

CHEOUN, M.-K., et al.

062

60

Neutrino Induced Reactions Related to the ν-Process Nucleosynthesis of 92Nb
and 98Tc

CHEOUN, M.-K., et al.

063

MARUYAMA, T., et al.

064

61 Pulsar Kick Induced by Asymmetric Emission of Supernova Neutrinos

002

Three-Dimensional Structure of Supernovae
Studied by Spectropolarimetric Observations(NAOJ)		

KAWABATA, Koji

AOKI, Kentaro, IYE, Masanori			PIAN, ElenaHATTORI, Takashi(Hiroshima University)(NAOJ)(INAF-Trieste)		

(University of Tokyo)

SASAKI, Toshiyuki

YAMANAKA, Masayuki(NAOJ)			

Massive stars are thought to end their lives as
supernova explosion. However, the explosion mechanism
is not yet clear. Recent numerical simulations suggestthat multi-dimensional effects are critical for successful
explosions. In contrast, it is not easy to study the multidimensional shape of supernovae observationally,
since supernovae in external galaxies are point sources(Figure 1).
In this study, we focus on spectropolarimetricobservations, which are sensitive to multi-dimensional
shape of the sources. We have performed multidimensional radiative transfer simulations and foundfollowing. (1) If the supernova explosion is completely
axisymmetric, the spectropolarimetric data shouldalign in the Stokes QU diagram. (2) If the supernova
explosion has a 3D, clumpy structure, the data in the
QU diagram show a loop. Based on these expectations,
we have performed spectropolarimetric observations of
extragalactic supernovae using Subaru/FOCAS.

MAZZALI, Paolo A.

(Max-Planck Institut für Astrophysik)

MAEDA, Keiichi, NOMOTO, Ken'ichi(NAOJ)				

(Kyoto University)

show a similar pattern. This indicates that supernova
explosion generally has a 3D, clumpy structure. Sucha structure may be formed by the convection during
the explosion. Our results can be an important key
to understand the explosion mechanism from actual
observations.

−20
1.0

−15

−10

−5

Doppler Velocity (103 km s−1)0

SN 2009jf(+9.3 days)

0.5

U (%)

TANAKA, Masaomi

0.0

−0.5
−1.0
−1.0

OI

−0.5

Ca II

0.0

Q (%)

0.5

1.0

Figure 2: Spectropolarimetric data of SN 2009jf taken with
Subaru/FOCAS. The data are plotted in the Stokes QU
diagram. Different colors represent different wavelength(Doppler velocities). The observed data suggest 3D,clumpy structure of supernova ejecta.

Figure 1: Optical image of SN 2009mi in IC 2151 (the position of
the supernova is pointed by the lines).

As a result of spectropolarimetric observations [1],we found that the data show a loop in the QU diagram asshown in Figure 2. This is consistent with the expectationof a 3D, clumpy explosion. By combining our new resultswith our past observations [2,3] and the data taken byother groups, we found 5 supernovae out of 6 objects

References[1] Tanaka, M., et al.: 2012, ApJ, 754, 63.
[2] Tanaka, M., et al.: 2008, ApJ, 689, 1191.
[3] Tanaka, M., et al.: 2009, ApJ, 699, 1119.

I Scientific Highlights

003

Infrared Observations of “Middle-Aged” Supernovae
Filling the Gap between Supernovae and Supernova Remnants
TANAKA, Masaomi(NAOJ)NOZAWA, Takaya, SAKON, Itsuki, ONAKA, Takashi, ARIMATSU, Ko, OHSAWA, Rhou, MAEDA, Keiichi(University of Tokyo)

WADA, Takehiko, MATSUHARA, Hideo				(ISAS/JAXA)			

Observational studies of supernovae can be divided
into two categories: (1) young supernovae (within a
few years after the explosion) in external galaxies, and(2) supernova remnants in our Galaxy (older than a few
hundred years old). Extragalactic supernovae can beobserved only for a few years since they get fainter. On
the other hand, probability to have a young supernova in
our Galaxy is extremely low (about once in a century).
Therefore, we don't have any observational example
in the gap of these two phases, except for SN 1987A
in the Large Magellanic Cloud. Thus, it was basically
impossible to observationally study the long-term
evolution from supernova to supernova remnant.
In order to detect supernovae in this gap, so called“middle-aged” supernovae, we searched supernovae
in the images of nearby galaxies taken with AKARI
satellite. As a result, we discover infrared emission
from SN 1978K in NGC 1313 [1] (Figure 1). This is theemission at 28 years after the explosion, and the second
example of middle-aged supernovae after SN 1987A.
The spectral energy distribution (SED) is quite

KANEDA, Hidehiro(Nagoya University)

intriguing. It is similar to the SED of Galactic supernova
remnant Cassiopeia A (about 300 years old). In addition,from the analysis of the SED and model calculations,
we found that (1) SN 1978K is associated with 1 × 10−3M of silicate dust, and (2) the emission is caused by
the circumstellar dust heated by the shock wave of
the supernova. These results indicate that at least thissupernova already radiates by the interaction between
supernova ejecta and surrounding medium as insupernova remnants. This observation provides a uniqueexample to understand the long-term evolution fromsupernova to supernova remnant.

Figure 2: Infrared-to-radio SED of SN 1978K (black), comparedwith that of Cassiopeia A (gray). Both objects show
synchrotron emission at radio wavelengths and infraredexcess by the dust emission. The infrared emission fromSN 1978K is reproduced by 1 × 10−3 M of silicate dust.

Reference[1] Tanaka, M., et al.: 2012, ApJ, 749, 173.
Figure 1: Infrared image of SN 1978K in NGC 1313 at 28 yr after
the explosion (the position of the supernova is pointed
by the lines).

004

I Scientific Highlights

Near-Infrared Circular Polarization Images of NGC 6334-V
KWON, Jungmi, TAMURA, Motohide

				(NAOJ/GUAS)		

LUCAS, Phil W.

(University of Hertfordshire)

HASHIMOTO, Jun, KUSAKABE, Nobuhiko, KANDORI, Ryo(NAOJ)

NAKAJIMA, Yasushi(Hitotsubashi University)		

NAGAYAMA, Takahiro(Nagoya University)

NAGATA, Tetsuya(Kyoto University)

HOUGH, James H.

(University of Hertfordshire)

We present results from deep imaging linear andcircular polarimetry of the massive star-forming region
NGC 6334-V (Figure 1). These observations show highdegrees of circular polarization (CP), as much as 22 %in the Ks band, in the infrared nebula associated withthe out ow. The CP has an asymmetric positive/negative
pattern and is very extended (~80″ or 0.65 pc). Both thehigh CP and its extended size are larger than those seenin the Orion CP region (Figure 2). Three-dimensional
Monte Carlo light-scattering models are used to showthat the high CP may be produced by scattering fromthe infrared nebula followed by dichroic extinction by
an optically thick foreground cloud containing aligned
dust grains. Our results show not only the magnetic eldorientation of around young stellar objects, but also thestructure of circumstellar matter such as out ow regions
and their parent molecular cloud along the line of sight.
The detection of the large and extended CP in this source
and the Orion nebula may imply the CP origin of thebiological homochirality on Earth [1].

Figure 2: ((a) and (b)) Stokes V and I images of NGC 6334-V IRN
in the Ks band, respectively. The white cross shown in (a)is the location of the illuminating star. (c) Ks polarization
vector map of NGC 6334-V IRN superposed on the
LP image. (d) CP image in the Ks band and a plot line
indicated a white box and columns of the sub-CP image
smoothed by 3 pixels of NGC 6334-V IRN. For making
the CP image, I image was masked with a threshold of
2σ of approximate sky value. (e) CP image of OMC-1 inthe Ks band.

Reference[1] Kwon, J., et al.: 2013, ApJ, 765, L6.

Figure 1: Color composite Stokes I image of the NGC 6334-V
region in the J (blue), H (green), and Ks (red) bands
from the IRSF/SIRPOL (CP) observations.

I Scientific Highlights005Detection of Low-Level Activities in Solar-Analog Stars
from the Emission Strengths of Ca II 3934 Line
TAKEDA, Yoichi, TAJITSU, Akito, KAWANOMOTO, Satoshi, ANDO, Hiroyasu, SAKURAI, Takashi(NAOJ)

HONDA, Satoshi(Kyoto University)

There have been several arguments regarding the status
of solar activity among similar Sun-like stars. This beganwith the implication of Baliunas and Jastrow [1] based on
their Mt. Wilson HK survey that a considerable portion(~1/3) of solar-type stars have activities significantly lower
than the present-day Sun, which they called “Maunderminimum stars.” However, their conclusion could not be
confirmed by Hall and Lockwood’s follow-up study [2],and Wright [3] criticized the reality of such low-active
solar-type stars by pointing out that most of them are notso much dwarfs as evolved subgiants.
Given this controversial situation, we decided tocontend with this problem by ourselves based on carefully
selected sample of 118 solar-analogs sufficiently similar
to each other (which we already investigated their stellar
parameters as well as Li/Be abundances in a series of
papers; cf. [4,5,6]), with a special attention being paid toreliably evaluating their activities down to a considerably
low level.
Practically, we measured the emission strength at
the core of Ca II 3933.663 line (K line; cf. Figure 1) on
the high-dispersion spectrogram obtained by Subaru/
HDS, where we gave effort to correctly evaluating thepure emission component by removing the wing-fitted
photospheric profile calculated from the classical solarmodel atmosphere to obtain R′Kp (ratio of chromosphericcore emission flux to the bolometric flux). This enabled us
to detect low-level activities down to log R′Kp ~ −5.5.

From the distribution histogram of log R′Kp (Figure 2),
we could recognize a clear Vaughan–Preston gap between
two peaks at ~ −5.3 and ~ −4.3. Our result of log R′Kp,
= −5.33 manifestly suggests that the Sun belongs to
the group of the former peak and has a distinctly lowactive nature among solar analogs. Actually, the fractionof stars satisfying the condition of log R′Kp ≤ log R′Kp,
is only ~10 %. This consequence exclude the possibility
for the existence of a considerable portion (e.g., ~1/3)of “Maunder-minimum stars” such that having activities
significantly lower than the current solar-minimum level
as once suggested by Baliunas and Jastrow ([1]). Thisconsequence also implies that the Sun is a distinctly lowactive star even within the group of solar-analog stars. See[7] for more details of this study.

Figure 2: Distributions of log R′Kp. The arrow shows the position
for the Sun, and its expected minimum–maximum range
is also indicated.

Figure 1: Observed spectra at the Ca II K line core for the 118
program stars (blue) and Vesta/Sun (red).

006

I Scientific Highlights

References[1] Baliunas, S., Jastrow, R.: 1990, Nature, 348, 520.
[2] Hall, J. C., Lockwood, G. W.: 2004, ApJ, 614, 942.
[3] Wright, J. T.: 2004, AJ, 128, 1273.
[4] Takeda, Y., Kawanomoto, S., Honda, S., Ando, H., Sakurai, T.:2007, A&A, 468, 663.
[5] Takeda, Y., Honda, S., Kawanomoto, S., Ando, H., Sakurai, T.:2010, A&A, 515, A93.
[6] Takeda, Y., Tajitsu, A., Honda, S., Kawanomoto, S., Ando, H.,
Sakurai, T.: 2011, PASJ, 63, 697.
[7] Takeda, Y., Tajitsu, A., Honda, S., Kawanomoto, S., Ando, H.,
Sakurai, T.: 2012, PASJ, 64, 130.

The Galaxy Luminosity Functions down to MR = −10
in the Coma Cluster
YAMANOI, Hitomi(NAOJ)		

OKAMURA, Sadanori

KOMIYAMA, Yutaka(NAOJ/The Graduate University for Advanced Studies)		

(NAOJ)

IYE, Masanori, KASHIKAWA, Nobunari, TAKATA, Tadafumi(Hosei University)			

				

YAGI, Masafumi(NAOJ/The Graduate University for Advanced Studies)

FURUSAWA, Hisanori(NAOJ) 		

The galaxy luminosity function (LF) is a usefulmeasure to describe fundamental statistical propertiesof galaxy populations and serves as a clue to study thehistory of galaxy formation and evolution. However, ourknowledge of the faint part of the LF (MR > −19), which
is dominated by dwarf galaxies, is still very limited. The
aim of the present study is to investigate the propertiesof the very faint dwarf population and their possible
environmental dependence, if any, in terms of LF, color,and surface brightness.
We construct the LFs at three fields ocated at thecenter, intermediate, and outskirt in the Coma Cluster [1].
Deep and wide images are obtained with the SuprimeCam mounted on the Subaru Telescope. Contaminationfrom background galaxies is subtracted statistically using
the number counts of galaxies in a blank field, the Subaru
Deep Field.
The LF (−19 < M R < −10) shows no significant
differences among the different three fields in this cluster(Figure 1). It shows a clear dip at M R ~ −13, and iscomposed of two distinct components of different slopes;
the bright component with −19 < MR < −13 has a flatter
slope than the faint component with −13 < MR < −10which has a steep slope. The bright component (−19 < MR
< −13) consists of mostly red extended galaxies including
few blue galaxies whose colors are typical of late-typegalaxies. On the other hand, the faint component (−13 <MR < −10) consists of largely PSFlike compact galaxies(Figure 2). We found that both these compact galaxies
and some extended galaxies are present in the center
while only compact galaxies are seen in the outskirt. In
the faint component, the fraction of blue galaxies is larger
in the outskirt than in the center. We suggest that the
dwarf galaxies in the Coma Cluster, which make up thetwo components in the LF, are heterogeneous with somedifferent origins.

References[1] Yamanoi, H., et al.: 2012, AJ, 144, 40.
[2] Marn-Franch, A., Aparicio, A.: 2002, ApJ, 568, 174.
[3] Harris, W., et al.: 2009, AJ, 137, 3314.

YOSHIDA, Michitoshi(Hiroshima University)

Figure 1: The R-band LFs of the center (Coma 1), intermediate(Coma 2) and outskirt (Coma 3) fields, respectively. The
error bars are based on Poisson statistics. The broken
curve indicates the LF of globular clusters in the Coma 1
field calculated using the previous results of [2] and [3].

Figure 2: The color-coded number density contours of estimatedmember galaxies (all galaxies: top row, red galaxies:
middle row, blue galaxies: bottom row) in the R absolutemagnitude versus effective surface brightness plane. The
white solid line indicates the discrimination between theextended (upper) and the compact (lower) objects.

I Scientific Highlights

007

Kinematic Imprint of Clumpy Disk Formation on Halo Objects
INOUE, Shigeki(Mullard Space Science Laboratory/NAOJ)

R = 1- 4 kpc
R = 4-7 kpc
R = 7-10 kpc
R = 10 -13 kpc-1<Vrot > [km s ]

60
40
20
0
0.6
(rapo - rperi) / (rapo + rperi)

Clumpy disk galaxies in the distant universe, at redshift of z >~ 1, have been observed to host several giant
clumps in their disks [1]. They are thought to correspondto early formative stages of disk galaxies [2]. On theother hand, halo objects, such as old globular clusters
and halo stars, are likely to consist of the oldest stars in agalaxy (age >~ 10 Gyr), clumpy disk formation can thus bepresumed to take place in a pre-existing halo system.
Giant clumps orbit in the same direction in apremature disk and are so massive that they may be
expected to interact gravitationally with halo objects andexercise influence on the kinematic state of the halo.
Accordingly, I scrutinize the possibility that the clumps
leave a kinematic imprint of the clumpy disk formation
on a halo system.
I perform a restricted N-body calculation with a toy
model to study the kinematic influence on halo objects
by orbital motions of clumps and the dependence of theresults on masses (mass loss), number, and orbital radiiof the clumps. My result shows that halo objects can berotated by clump motions and acquire disky rotation in a
dynamical friction time scale of the clumps, ~0.5 Gyr (thetop panel of Figure 1). The influence of clumps is limited
within a region around the disk, while the halo systemshows vertical gradients of net rotation velocity andorbital eccentricity (the bottom panel of Figure 1). The
signicance of the kinematic influence strongly depends
on the clump masses; the lower limit of postulated clump
mass would be ~5 × 108 M. The result also depends onwhether the clumps are subjected to rapid mass loss ornot, which is an open question under debate in recent
studies. The existence of such massive clumps is notunrealistic. I therefore suggest that the imprints of past
clumpy disk formation could remain in current galactic
halos. This result has already been published in a refereed
journal [3].

0.5

0.4

0.3

0

1

2

3

4

5

z [kpc]Figure 1: Map of mean line-of-sight velocity from the edgeon view (top). The values are normalized by the lineof-sight velocity dispersion inside r0 = 4 kpc, which is
106 km s−1. The mean azimuthal velocity and orbital
eccentricity, e ≡ (rapo − rperi) / (rapo + rperi), of the halo
objects as functions of distance from the clump orbital
plane (bottom), where rapo and rperi are apo- and pericenter distances, respectively. Each line indicates a radial
range in cylindrical coordinate, R. In the bottom panel,
the halo objects rotating prograde and retrograde are
separately plotted; the thick and thin lines correspond toprograde and retrograde ones, respectively.

References[1] Elmegreen, D. M., Elmegreen, B. G., Marcus, M. T., Shahinyan,
K., Yau, A., Petersen, M.: 2009, ApJ, 701, 306.
[2] Noguchi, M.: 1998, Nature, 392, 253.
[3] Inoue, S.: 2013, A&A, 550, A11.

008

I Scientific Highlights

Astrometric Mock Observations
for Determining the Local Dark Matter Density
INOUE, Shigeki(NAOJ/Korea Astronomy and Space Science Institute)

To determine the local dark matter density (LDMD)
around the solar system is a classical problem inastronomy since [1]. In recent years, dedicated searches
for candidates of dark matter (DM) particles haveintensified. Experiments aiming at direct detection of theDM particles look for signals from recoil of DM particles
with nuclei inside the detector. Thus, the event rates ofthe direct detection are clearly proportional to the LDMD
around the solar system. This is why the problem ofdetermining the LDMD at the solar position has recently
been attracting a great deal of attention.
Recently, Garbari et al. [2,3] have devised a novel
method to determine the LDMD from stellar distribution
and vertical velocity dispersion profiles perpendicular
to the Galactic plane, which they named a minimal
assumption (MA) method. Their method has theadvantages of abolishing conventional approximations
and using only a few assumptions. Their determinations
preferred higher dark matter densities than conventional
values although the previous results are within theirquoted errors.
This study is aimed at carefully scrutinizing the
MA method and examining influence on the LDMD
determination with the MA method by observational
uncertainties. We discuss how the determinations of the
LDMD vary with observational precisions on parallax,
proper motion and line-of-sight velocity measurements.
For these aims, we create mock observation data for stars
being dynamical tracers based on an analytical galaxy
model and apply parametrized observational errors to themock data. We evaluate the accuracy of determining the
LDMD by applying the MA method to the mock data.
In addition, we estimate a sample size and observational
precision required to determine the dark matter densitywith accuracy.
We find that the MA method is capable of determining
the LDMD with accuracy if the sample size andobservational precisions are satisfactory. The sample size
required is approximately 6,000 stars. The random errorsof parallaxes and proper motions can cause systematic
overestimation of the dark matter density. We estimate
the required precisions of the parallax measurements tobe approximately 0.1–0.3 milliarcseconds at 1 kpc awayfrom the sun; the proper motion precisions do not seemto be as important as the parallaxes. Also, we find thatthe line-of-sight velocity errors can cause either underestimation or overestimation of the dark matter density,
which is contingent on distance-dependence of the errors.
From these results, we expect that use of the

GOUDA, Naoteru(NAOJ)

Hipparcos catalog would overestimate the LDMD
because of the imprecise parallax measurements if the
MA method is applied; however, we emphasize thecapability of their method. [2] was making use of the
Hipparcos catalog which might lead to their high LDMD.
We expect that Gaia will provide data precise enough todetermine the LDMD.

Figure 1: Influence of the astrometric distance errors on
determining the LDMD. The panels from the left toright indicate the results of adopting A = 0.1 0.3 and 0.5,
respectively, where A is parallax measurement precisionat 1 kpc away from the sun. In each case, we conduct
the same computation with different tracer samples
generated in the same conditions (ID = 1–6) with 24,000
sample stars. The horizontal dotted line indicates thetrue LDMD assumed in our model.

References[1] Oort, J. H.: 1932, Bull. Astron. Inst. Neth., 6, 249.
[2] Garbari, S., Read, J. I., Lake, G.: 2011, MNRAS, 416, 2318.
[3] Garbari, S., Liu, C., Read, J. I., Lake, G.: 2012, MNRAS, 425,
1445.

I Scientific Highlights009

Spacecraft Observation of a Central Engine of Magnetic Reconnection		

ZENITANI, Seiji(NAOJ)		

SHINOHARA, Iku(JAXA/ISAS)

Magnetic reconnection is a driver of explosive
events in space and astrophysical plasmas. It has beenthought that the reconnection process is controlled bymagnetic dissipation physics in a small-scale region
near the reconnection point (X-line). In other words,
the dissipation region plays a role as a central engineof magnetic reconnection. Although it was not clearly
defined before, recent theory suggests that the dissipation
region is best identified by a frame-independent dissipation
measure [1].
In the Earth’s magnetosphere, spacecrafts haveobserved reconnection events for many years. Such “insitu” measurements have provided key information forreconnection theories. So far, there has been no clear
observation of the dissipation region, mainly because thepresent instruments can hardly resolve the small dissipation
region whose typical size is 1000 km × 100 km.
The Geotail spacecraft, developed by JAXA/ISAS
in collaboration with NASA, has been observing the
Earth’s magnetosphere since 1992. On 15 May 2003, it
encountered a reconnection event in the night side of themagnetosphere [2]. This is the best reconnection event in
20 years of Geotail observation. The top panel in Figure 1
shows selected Geotail data during the event [3]. Bothan ion flow (blue) and an electron flow (red) reverse
their directions, and electrons are outrunning ions. Thisis a signature of reconnection jets from the X-line. The
gray histogram shows an approximate form of the energy
dissipation,(1)
which is useful in this specific configuration [3]. As
indicated by the arrow, there is a characteristic structurewith energy dissipation at the plasma jet reversals.
The picture is qualitatively similar to one in a kinetic
simulation, as shown in the bottom panel in Figure 1.
We extensively check our dataset, including raw
instrumental data of the electric field. We confirm thatseveral possible factors such as an offset in Ex do notchange the picture around the jet reversal. Therefore,
although our resolution is quite limited, we are convincedthat the Geotail encountered the dissipation region.
To our knowledge, this is the first clear detection of
the dissipation region of magnetic reconnection in theplanetary magnetotail.
In 2014, NASA will launch magnetospheric multiscale(MMS) satellites to directly probe reconnection sites withultra-high-resolution instruments on four spacecrafts.
When the spacecrafts will encounter the dissipation

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I Scientific Highlights

NAGAI, Tsugunobu(Tokyo Institute of Technology)

Figure 1: (Top) Geotail observation from 1054:00 UT to 1057:45
UT on 15 May 2003. The outflow component of theperpendicular ion (blue) and electron (red) velocities,
and the approximate dissipation measure D*e (Eq. 1) arepresented. (Bottom) The same quantities in a 2D kinetic
simulation. 1D cut along the outflow direction.

region, we will hopefully be able to identify it by using
our diagnosis. The high-resolution data of the dissipation
region will be transferred to the ground with the highest
priority, and then it will provide key information about
the breaking mechanism of magnetic field lines.

References[1] Zenitani, S., et al.: 2011, Phys. Rev. Lett., 106, 195003.
[2] Nagai, T., et al.: 2011, J. Geophys. Res., 116, A04222.
[3] Zenitani, S., et al.: 2012, Geophys. Res. Lett., 39, L11102.

Accurate Measurements of the Brightness of the White-Light Coronaat the Total Solar Eclipses on 1 August 2008 and 22 July 2009

		HANAOKA, Yoichiro(NAOJ)KIKUTA, Yoshihiro(Yamanashi Prefectural Science Center)

OHNISHI, Kouji(Nagano National College of Technology)

The total eclipses are good chances to observe thewhite-light corona from just above the solar limb to as
far as several solar radii. We measured the brightnessof the white light corona at the total solar eclipses on
1 August 2008 and 22 July 2009 during the deep solar
minimum, when solar activity was at its lowest in one
hundred years [1]. After careful calibration, the total
brightness of the corona in both eclipses was evaluated tobe approximately 0.4 × 10−6 of the total brightness of theSun. The measured value is lower than those measured
in the former minima [2]. The total brightness of thewhite-light corona corresponds to the total amount of thecoronal material. Therefore, the low brightness of thecorona shows that the amount of the coronal material wasparticularly small when the magnetic activity on the solar
surface became quite low.
Furthermore, we compared the total brightness of
the K + F-corona beyond 3 R in both eclipses to theformerly measured brightness of the F-corona only
(Figure 1). The measured results of the F-corona show
some scatter, because it is generally difficult to isolate theF-corona from the K+F-corona. Our results show that theK + F-corona brightness values at the two eclipses arelower than some of the F-corona only brightness values
previously measured. Due to the low solar activity, theK-corona brightness beyond 3 R is quite low at the two
eclipses, and our measurements give the reliable upper
limit of the F-corona brightness on the basis of the highaccuracy calibration.

References[1] Hanaoka, Y., Kikuta, Y., Nakazawa, J., Ohnishi, K., Shiota, K.:
2012, Solar Phys., 279, 75.
[2] Rušin, V.: 2000, Last Total Solar Eclipse of the Millennium,
Livingston, W., Özgüç, A. (eds.), ASP Conf. Ser., 205, 17.
[3] Morgan, H., Habbal, S. R.: 2007, A&A, 471, L47.
[4] Fainshtein, V. G., Tsivileva, D. M., Kashapova, L. K.: 2010,
Solar Phys., 267, 203.
[5] Dürst, J.: 1982, A&A, 112, 241.

NAKAZAWA, Jun(Yamanashi Cement Company)

SHIOTA, Kazuo(Solar Eclipse Information Center)(a) 2008

1.0(b) 2009

(c)

2.5 R

Brightness (10-8 Bsun)

		

3.0 R
3.5 R
4.0 R
0.1
4.5 R
0 (N)

90 (E)
180 (S)270 (W)
Position Angle (degree)360

Figure 1: (a) Stacked images of the white-light corona taken in the
1 August 2008 eclipse and (b) the 22 July 2009 eclipse.
To show the fine structures in the corona clearly, radial
brightness decrease is suppressed, and structures of thecoronal streamers are enhanced. The solar north is to
the top. (c) Tangential coronal brightness distributionsin the 2008 (dashed curves) and the 2009 (solid curves)
eclipses at radii of 2.5, 3.0, 3.5, 4.0, and 4.5 R  .
Formerly measured brightness values of the F-corona[3,4,5] for radii 2.5, 3.5, and 4.5 R are also shown by
triangles, plus signs, and stars. Our results for these radii
are shown in thick curves.

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011

Early Thermal X-Ray Emission from Long Gamma-Ray Bursts
				

SUZUKI, Akihiro(NAOJ)			

Gamma-ray bursts (GRBs) are sudden appearance of
gamma-ray point source on the celestial sphere. GRBs
are divided into two groups, short and long bursts.
Bursts with the duration longer (shorter) than 2 sec areclassified as long (short) GRBs. Short GRBs are currently
considered to originate from the merger of two neutronstars in a closed binary. Long GRBs are produced byan ultrarelativistic jet that launches as a result of thegravitational collapse of the iron core of massive stars,
which is observationally confirmed by temporal andspacial coincidence between a special class of type Ic
supernovae and long GRBs. Many problems, such as,radiation mechanisms of gamma-rays, jet injection,and so on, remain unsolved and discussed by a lot of
researchers.
In this research [1], the dynamical evolution of an
ultrarelativistic jet injected into the core of a massive
star is investigated by two-dimensional relativistichydrodynamic code developed by one of the authors(Figure 1). As a progenitor model, we adopted a WolfRayet star with the mass of 14 M and the radius of 4
× 10 10 cm. Especially, we focus on the circumstellar
medium (CSM) of the progenitor. Wolf-Rayet stars are
considered to experience violent mass losing process
prior to the gravitational collapse. Then, we calculate
models with steady wind with the mass-loss rates 10−7,
10−6, 10−5, 10−4, and 10−3 M yr−1 to investigate effectsof the presence of dense CSM on the dynamics of the jet.
In Figure 2, radial profiles of the velocity, the density,and the pressure along the inclination angle of 45° arecompared for models with the mass-loss rates of 10−7 and10−3 M yr−1. In the dense CSM model, the reverse shock
is formed and propagates in the ejecta. On the other hand,in the dilute CSM model, the rarefaction wave propagatesin the ejecta.

SHIGEYAMA, Toshikazu(University of Tokyo)

Figure 2: Radial profiles of the velocity (top), density (middle),
and pressure (bottom) of the ejecta along the inclination
angle of θ = 45°. Solid and dashed lines correspond todense and dilute CSM models.

Calculating the photospheric emission from the ejecta
for each model, we found that the photospheric emission
can explain properties of recently discovered thermal
Xray emission from GRBs [2]. It may be possible that thecircumstellar environment of massive stars that end theirlives as GRBs can be probed by observing thermal X-ray
emission.

References[1] Suzuki, A., Shigeyama, T.: 2013, APJ, 764, L12.
[2] Starling, R. L. C., Page, K. L., Pe'Er, A., Beardmore, A. P.,
Osborne, J. P.: 2012, MNRAS, 427, 2950.

Figure 1: Results of relativistic hydrodynamical simulation of an
ultrarelativistic jet emanating from a massive star.

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Recalibration of the Photometric Zero Point of SDF/SXDS Catalogs
YAGI, Masafumi, YAMANOI, Hitomi, FURUSAWA, Hisanori, NAKATA, Fumiaki, KOMIYAMA, Yutaka(NAOJ)SUZUKI, Nao(LBNL)As products from Subaru Observatory Projects,
Subaru Deep Field (SDF) and Subaru XMM-Newton
Deep Survey (SXDS) public catalogs [1,2] are publicly
available. Recently, [3] reported that B-R color distribution
was inconsistent between SDF and SXDS. We therefore
recalibrated the B, V, R, i, and z magnitudes of SDF andSXDS against the Sloan Digital Sky Survey (SDSS) [4].
We first constructed color conversions from theSDSS filter system [5] to the Suprime-Cam filter system.
The model calculation by ATLAS9 [6] and Yonsei-Yale
isochrone [7,8] was used to construct a set of spectralenergy distributions (SED) of stars. The transmittance ofSDSS and Suprime-Cam were multiplied to the SEDs to
calculate the magnitudes, and polynomial function was
fitted to the SDSS color vs SDSS-Suprime colors.
Then, possible error sources, such as the mass andtemperature of the star, metallicity, recession velocity,
Galactic extinction, and atmospheric absorption in theobservation were examined. The color constraint of
SDSS color in which the variation by these factors issmall enough (no more than 0.04 mag) was calculated.
The conversion was tested with empirical stellar spectral
libraries (BPGS [9], HILIB [10], STELIB [11], CFLIB[12]), and it also worked well within the error.
We selected r~20 mag stars in SDSS, converted
them into AB magnitude, converted to Suprime-Cammagnitude, and compared with the SDF/SXDS catalogs.
Some data showed an offset larger than 0.1 mag (Table1). If we correct the offset, the color distribution of R~24
objects in SDF and SXDS became consistent, which were

band

SDF

SXDS-CSXDS-NSXDS-S

B

−0.12

0.00

0.02

0.01

V

−0.03

−0.02

−0.02

−0.01

R

−0.05

−0.04

−0.05

−0.05

i

−0.11

−0.10

−0.11

−0.16

z

−0.06

−0.13

−0.14

−0.12

Table 1: Part of the offset of zero point between SDF/SDXS andSDSS. Significant difference is in red.

inconsistent if we used the original catalog values (Fig. 1).
Since the offset around 20 mag corrected the data around24 mag, it should be an offset of the zero point.
The origin of the offset was partly explained byrelatively higher metallicity of model stars which wereused for color calibration of SDF B-band. Also, thecalibration of the spectrophotometric standard starSA95-42 [13] which was used for i-band calibration was
doubtful. The origin of other offsets remained unclear.
References[1] Kashikawa, N., et al.: 2004, PASJ, 56, 1011.
[2] Furusawa, H., et al.: 2008, ApJS, 176, 1.
[3] Yamanoi, H., et al.: 2012, AJ, 144, 40.
[4] Yagi, M., et al.: 2013, PASJ, 65, 22.
[5] Doi, M., et al.: 2010, AJ, 139, 1628.
[6] http://wwwuser.oat.ts.astro.it/castelli/grids.html.
[7] Yi, S., et al.: 2001, ApJS, 136, 417.
[8] Demarque, P., et al.: 2004, ApJS, 155, 667.
[9] http://www.stsci.edu/hst/observatory/cdbs/bpgs.html.
[10] Pickles, A.: 1998, PASP, 110, 863.
[11] Le Borgne, J.-F., et al.: 2003, A&A, 402, 433.
[12] Valdes, F., et al.: 2004, ApJS, 152, 251.
[13] Oke, J. B.: 1990, AJ, 99, 1621.

Figure 1: Color distribution of faint objects in SDF (black) and SXDS (red). Top panel uses the catalog values, and bottom panel is after
zero point correction. Left panels show B-R color distribution of 24<R<25 magnitude, and right ones show i-z color distribution of
23<i<24 objects.

I Scientific Highlights013

Crosstalk Analysis of New CCDs of Suprime-Cam
YAGI, Masafumi(NAOJ)The detectors of Suprime-Cam were replaced in
2008/07 to full-depleted back illuminated CCDs [1].
The new CCDs show a crosstalk features between
channels (Figure 1 top). Such crosstalk was reported in
multichannel CCDs in other observatories [2,3,4,5,6].
In Suprime-Cam, one of the three crosstalk shadowsmoves parallel to the source. Default dithering sequenceof Suprime-Cam does not change the position angle,
and the shadow of the same parity gains S/N after coadd(Figure 2). It causes problem especially in two cases:
a narrow band imaging with low sky background, anddeep imaging with lots of exposures. In either case, thecrosstalk affects the result, it is important to formalize theeffect and correct it appropriately.
In this study, I used cosmic rays in dark frames(exposures with shutter closed). Detecting cosmic rays
and compare the data at corresponding pixels in otherchannels, the crosstalk can be formalized. Moreover,as the dark current is very low in the new CCDs, thedifficulties of background subtraction is avoided.
The results of the analysis are as follows; 1) The
crosstalk of the Suprime-Cam new CCDs is a decreaseof the bias level. It is proportional to the input signal in achannel (Fig. 3), and the coefficient is typically 10−4. It is
comparable to other observatories [2,3]. 2) No crosstalk
between chips is detected. 3) The strength of crosstalk
depends on the pair of channels. The central two channels
shows significantly weak crosstalk. This asymmetry
implies that the crosstalk is a phenomenon around on-chip
amplifiers (amps). 4) The strength shows no difference
among chips. It only depends on the distance between
the channels. 5) Crosstalk does not change by a changeof the gain of on-chip amp. It implies that the crosstalk is
not an interaction of charges but an interaction of signals.
6) Crosstalk is recognized not only at the corresponding
pixel but 2 pixels read after the pixel.
A correction formula is derived from the analysis of
the dark frames. The correction also works well for otherdata frames (Fig. 1 bottom) [7], and the tool is provided tothe public.

014

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Figure 1: Example of crosstalk. (Top) before correction. (Bottom)
after correction.

Figure 2: Schematic figure of coadd of dithered data.

Figure 3: Correlation between input signal and crosstalk signal in
chip0 ch-B and ch-D. The solid line shows the best-fit
regression.

References[1] Kamata, Y., et al.: 2008, SPIE, 7021, 70211S.
[2] Freyhammer, L. M., et al.: 2001, Exp. Astron., 12, 147.
[3] Giavalisco, M.: 2004a, STScI Instrument Science Report, ACSISR, 2004-12.
[4] Giavalisco, M.: 2004b, STScI Instrument Science Report, ACSISR, 2004-13.
[5] Suchkov, A., et al.: 2010, STScI Instrument Science Report,
ACS-ISR, 2010-10.
[6] Suchkov, A., Baggett, S.: 2012, STScI Instrument Science
Report, ACS-ISR, 2012-02.
[7] Yagi, M.: 2012, PASP, 65, 22.

Astrometric Goal of Small-JASMINEYANO, Taihei, GOUDA, Naoteru, KOBAYASHI, Yukiyasu, TSUJIMOTO, Takuji, NIWA, Yoshito(NAOJ)

			

YAMADA, Yoshiyuki(Kyoto University)

Small-JASMINE [1] is the astrometric satellite, which
will observe the central region of the Galactic bulge,
measuring the parallax and the proper motion with highaccuracy using the near infrared wavelength (1.1 μm ~1.7 μm). The mission time is required to continue foraround 1 ~ 3 years. Three-year observation will produce
the astrometric data of the parallax with an accuracyof about 10 micro-arcseconds and the proper motions
with that of about 10 micro-arcseconds per year at
Hw = 11.5 mag. The region with the above accuracies isat the center of the observing region of 0.3 × 0.3 square
degrees. On the other hand, observing region covers afield of about 3 × 3 square degrees. The parallax with anaccuracy of about 70 micro-arcseconds and the propermotion with that of about 70 micro-arcseconds/yr will
be obtained within the region of 3 × 3 square degrees.
These accuracies of the parallax and proper motion
are summarized in maps shown in Fig. 1 and Fig. 2,
respectively [2].
After the one year observation has passed, we obtain
the parallax with an accuracy of 28 μas and the propermotion with an accuracy of 55 μas/yr at Hw=11.5 mag. In
this case, we cannot derive the distance of the bulge stars
with high accuracy. However, in the case of Hw = 10 mag,we obtain the parallax with an accuracy of 14 μas andthe proper motion with an accuracy of 23 μas/yr by one
year observation. In this case, bulge stars can be obtained
distances with high accuracy.
Kinematical and dynamical information on the
Galactic bulge stars will be obtained after the observing
period of about 1 ~ 3 years. Accordingly it is expectedthat our understanding of the dynamical structure of the
Galactic bulge will be greatly improved. Furthermore,
we may have the chance to observe the different region
which has scientifically interesting target in winter orsummer seasons. For example, Cygnus X-1 is one ofthe observing candidates. If we successfully observe theobject during a few weeks, the orbital elements of the staraccompanying Cygnus X-1 can be resolved by SmallJASMINE.

JASMINE Working Group

Figure 1: Accuracy map of the parallax.

Figure 2: Accuracy map of the proper motion.

References[1] Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Hatsutori,Y., Murooka, J., Niwa, Y., Yamada, Y.: 2011, EAS Publications
Series, 45, 449.
[2] Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Niwa, Y.,
Yamada, Y.: 2012, Advancing the Physics of Cosmic Distances,
Proc. IAU, IAU Symp., 289, 433.

I Scientific Highlights

015

Astrometric Error Caused by Gravitational Microlensing Effectin the Galactic Bulge Stars
YANO, Taihei(NAOJ)We have investigated an expected deviation of thepositions or the proper motions of stars as the cosmic
error caused by the gravitational microlensing effect [1].
In observing stars in the Galactic bulge region, we obtainan expected deviation of a star positions by gravitational
microlensing effect of about 7 μas. We have also
estimated the expected deviation of the proper motionsof stars in the Galactic bulge caused by the gravitational
microlensing effect. The expected deviation of the propermotions is mainly caused by the lens object located at
the nearest angular distance from the source star. Eachdeviation of the proper motion has a value of less than
0.02 μas/yr for 99 % of the sources.
In estimating the the expected deviations of positionsof stars and those of proper motions of stars in the
Galactic bulge region, we assume that the optical depth,
τ, is about 1 × 10−6. The typical relative proper motion
between a bulge star and a lens object can be estimatedas several mas/yr using the Oort constants, solar motion,and velocity dispersion. Accordingly we assume that theproper motion is about 5 mas/yr.
We have investigated the correlation of the deviationof Galactic bulge stars caused by the gravitational
microlensing effect. In order to estimate the correlationsof these deviations of two sources, we define thecorrelation between deviations of source A and source B,
ρAB, as follows,(1)
where δA and δB are positional deviations of source A
and source B, respectively. The correlation ρ has a value
between −1 and 1. If the value is around 1, deviations of
two sources are strongly correlated. On the other hand, if
the value is 0, deviations are not correlated.
Here we define the dimensionless correlation angle atwhich the value of the correlation is equal to 0.5. Then we
can say that the deviations of two sources, separated withan angle smaller than correlation angle, are correlated.
And if not, uncorrelated.
The value of the correlation angle of the positional
deviation is estimated to be about 1 arcmin. In the sameway, we have estimated the correlation angle of thedeviation of the proper motions. The angle is estimated to
be about 1 arcsec. The following difference distinguishes
the deviation of the position and that of the proper motion.
The positional deviation is affected not only by lenses
near the source but also by the lenses far from the source.
On the other hand, the deviation of the proper motion by016

I Scientific Highlights

Figure 1: Schematic of the deviations and correlation angle.

microlensing is mainly only caused by the nearest lensfrom the source. This difference causes that of thecorrelation angle.
Upcoming observation by an astrometric satellite like
Gaia or JASMINE [2] will provide the catalogue with theaccuracy of about 10 μas. Then the typical deviation withthe value of 7 μas is less than the value of the observing
accuracy by the forthcoming astrometric satellites.
Therefore it is not a crucial problem for astrometry
missions such as Gaia or JASMINE. However it will bea serious problem for the next generation of astrometry
missions with the accuracy of 1 micro-arcsecond level.

References[1] Yano, T.: 2012, ApJ, 757, 189.
[2] Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Hatsutori,Y., Murooka, J., Niwa, Y., Yamada, Y.: 2011, EAS Publications
Series, 45, 449.

AKARI/AcuA Physical Studies of the Cybele Asteroid Family
KASUGA, Toshihiro

USUI, Fumihiko, HASEGAWA, Sunao(NAOJ)				

OOTSUBO, Takafumi(Tohoku University)(ISAS/JAXA)				

MÜLLER, Thomas G.

(Max-Planck-Institut für Extraterrestrische Physik)

KURODA, Daisuke(NAOJ)ISHIGURO, Masateru(Seoul National University)

We present a study of 107 Cybele asteroids based on
the archival data base “Asteroid Catalog Using AKARI(AcuA)” taken by the infrared astronomical satellite.
The data base provides diameters D > 10 km, geometricalbedos and taxonomic informations (75 %) of theCybeles. We find taxonomic diversity (mainly C-, D- andP-type) in the population of seventy-eight small Cybeles
with diameters 10 km < D < 80 km. Their cumulative
power-law size distribution index shows a shallow valueof 0.86 ± 0.03. By contrast, twenty-nine large Cybeles
with D > 80 km are mostly classified as C- or P- types(90 %), having a power-law index of 2.39 ± 0.18. The
total mass of Cybele asteroids is estimated to be ~10−5
MEarth. We also discuss the origin and formation processof Cybele asteroid family. See [1] for more details.

Figure 1: Cumulative size distribution of 107 Cybele asteroids.
The derived power-law indexes are b = 0.17 (10 km < D< 20 km), 0.86 ± 0.03 (20 km < D < 80 km) and 2.39 ±0.18 (D > 80 km).

Reference[1] Kasuga, T., et al.: 2012, AJ, 143, 141.

I Scientific Highlights

017

Measurements of Stellar Inclinations for Kepler Planet Candidates
HIRANO, Teruyuki(University of Tokyo)		

			

SANCHIS-OJEDA, Roberto

WINN, Joshua N.

(MIT)			I Scientific Highlights(NAOJ)TARUYA, Atsushi, SUTO, Yasushi

The origin of close-in giant planets (so-called “hotJupiters”) has been the most enduring problem since thediscovery of the first extrasolar planet. Measurementsof the spin-orbit angle (the relation between the stellar
spin axis and planetary orbital axis) are a promising
tool to uncover the formation and evolution (migration)
history of exoplanetary systems. This is because different
evolution models predict different distributions for the
spin-orbit angle and measurements of the angle provide
us an insight into the origin of exoplanets.
So far, the Rossiter-McLaughlin (hereafter RM)
effect for transiting exoplanets has been the major
channel to measure the spin-orbit angle. However, theRM effect is only applicable to giant planets orbiting at
the proximity of their host stars. When the size of planetis small, the RM signal becomes weaker, which makes
the measurement unreliable. In order to measure thespin-orbit angle for a smaller and distant exoplanet, we
focused on the measurements of stellar inclinations Is(see Figure 1). In a transiting exoplanetary system, where
the planetary orbit is edge-on from our direction, thestellar inclination Is is a useful indicator of the spin-orbitalignment/misalignment; when Is turns out to be deviatedfrom 90° through observations, it suggests a spin-orbit
misalignment along the line-of-sight. This method toconstrain the spin-orbit angle can be applied regardless ofthe size and orbital distance of the transiting planet.
In order to measure stellar inclinations for transiting
systems, we focused on the Kepler photometry. Amongthe planet-hosting stars detected by Kepler, some show
periodic flux variations due to starspots. A period
analysis of such a periodic flux variation will give us
the rotational period P r of the star. Meanwhile, theprojected rotational velocity V sin Is could be obtained via
spectroscopy. Combining these measurements along withthe stellar radius estimated from spectroscopy, one canput a constraint on the stellar inclination Is.
We picked up about 10 systems among the “Kepler
Object of Interest (KOI)” list, all of which show periodic
flux variations, and conducted spectroscopic observations
with Subaru/HDS. Figure 2 shows the projected rotational
velocity V sin Is as a function of the rotational velocity at
the stellar equator (Veq). The equatorial rotational velocity
were estimated by combining the rotational periods Ps
from the Kepler photometry with the stellar radii fromthe Subaru spectroscopy. While most of the systems
are along the solid line (Is = 90°), suggesting spin-orbitalignments, at least one system, KOI- 261, significantly

018

TAKEDA, Yoichi, NARITA, Norio(MIT)				(University of Tokyo)

deviates from the solid line. This most likely implies aspin-orbit misalignment along the line-of-sight. We notethat all the systems shown in Figure 2 have Earth-sized or
Neptune-sized exoplanets (no Jovian one), providing usa unique opportunity to discuss the evolution history ofsmaller exoplanets [1].

λI
IFigure 1: Schematic figure for the spin and orbital axes. The
stellar inclination Is is defined as the angle between thestellar spin axis (red) and line-of-sight.

Figure 2: The estimated Veq and V sin Is. The solid line indicatesthe case that our line-of-sight is vertical to the stellar
spin axis.

Reference[1] Hirano, T., Sanchis-Ojeda, R., Takeda, Y., Narita, N., Winn, J.
N., Taruya, A., Suto, Y.: 2012, ApJ, 756, 66.

Planet-Planet Eclipse and the Rossiter-McLaughlin Effectof a Multiple Transiting System
HIRANO, Teruyuki(University of Tokyo)

NARITA, Norio(NAOJ)

SATO, Bun'ei

TAKAHASHI, Yasuhiro, MASUDA, Kento(Tokyo Institute of Technology)

TAKEDA, Yoichi, AOKI, Wako, TAMURA, Motohide

					(NAOJ)				

Transiting exoplanetary systems provide us a unique
opportunity to measure the stellar obliquity with respect
to the planetary orbital plane. When we observe radial
velocities (hereafter RVs) during a planetary transit,
an anomalous RV variation is manifested in addition
to the normal sinusoidal RV variation inspired by the
Keplerian motion of the planet. This phenomenon,
called the Rossiter-McLaughlin (RM) effect, has been
exploited to measure the sky-projected angle between thestellar spin axis and planetary orbital axis (the spin-orbit
angle). Measurements of the spin-orbit angle provide animportant observational clue to distinguish among thepossible scenarios for the formation and evolution of
exoplanetary systems.
So far, the RM effect has been measured for single
transiting systems. Since the kepler space telescope waslaunched in 2009, however, many multiple transiting
systems are now available, and their origin and evolution
history are of primary interest. In order to discuss the
spin-orbit angle for multiple transiting systems, we
focused on “KOI-94,” one of the planet-hosting candidate
detected by Kepler. KOI-94 is comprised of four planetcandidates with relatively packed orbits. As a result ofconducting the measurement of the RM effect for KOI94.01 (the largest candidate among the four), we obtained
Figure 1 and the RV anomaly due to the RM effect showsthat the planetary orbital axis is well aligned with thestellar spin axis [1].
In addition to the measurement of the RM effect,
we discovered a very unique astronomical event forthis multiple transiting system, which we call a “planetplanet eclipse.” Figure 2 indicates the archived dataof the KOI-94 light-curve, delivered by Kepler. This
clearly shows a double transit event, in which thetwo planets (KOI-94.01 and 94.03) transit the hoststar simultaneously. Interestingly enough, there is abump around the bottom of the double transit. Thisbump most likely represents an overlapping event of
the two transiting planets on the stellar disk (“planetplanet eclipse”). The planet-planet eclipse is not only an
astronomically rare event, but also provides us a unique
opportunity to put a tight constraint on the “mutual
inclination” between the two planetary orbits. From thetiming and size of the bump in Figure 2, we showed thatthe two planetary orbits (of KOI-94.01 and 94.03) are
well aligned at least in the sky.

(University of Tokyo)

SUTO, Yasushi(University of Tokyo)

Figure 1: RV variation of KOI-94 during the transit of KOI-94.01.

Figure 2: A part of the public light-curve delivered by the Kepler
space telescope.

Reference[1] Hirano, T., Narita, N., Sato, B., Takahashi, Y. H., Masuda, K.,
Takeda, Y., Aoki, W., Tamura, M., Suto, Y.: 2012, ApJ, 759,
L36.

I Scientific Highlights

019

The Source Counts of Submillimetre Galaxies Detected at λ = 1.1 mm
SCOTT, Kimberly S.1, WILSON, Grant W.2, YUN, Min S.2, WELCH, D.2, ARETXAGA, Itziar3
HUGHES, David H.3, MONTANA, A.3, ZEBALLOS, Milagro3, AUSTERMANN, Jay E.4
KOHNO, Kotaro5, TAMURA, Yoichil5, HATSUKADE, Bunyo6, KAWABE, Ryohei7, OSHIMA, Tai7
EZAWA, Hajime7, NAKANISHI, Koichiro7, CHAPIN, E. L.8, HALPERN, M.8, SCOTT, Duglous8
DUNLOP, J. S.9, SANDERS, Dave10, SCOVILLE, Nick Z.11, KIM, S.12, LOWENTHAL, J. D.13
1: National Radio Astronomy Observatory, 2: University of Massachusetts, 3: INAOE, 4: University of Colorado, 5: University of Tokyo, 6:
Kyoto University, 7: NAOJ, 8: University of British Columbia, 9: University of Edinburgh, 10: University of Hawaii, 11: Caltech, 12: Sejong
University, 13: Smith College

The source counts of galaxies discovered at
submillimetre and millimetre wavelengths provide
important information on the evolution of infraredbright galaxies. We combine the data from six blank-fieldsurveys carried out at 1.1 mm with AzTEC (Table 1),
totalling 1.6 deg2 in area with root-mean-square depths
ranging from 0.4 to 1.7 mJy, and derive the strongest
constraints to date on the 1.1 mm source counts at flux
densities S1.1 mm = 1 – 12 mJy (Figure 1). Using additional
data from the AzTEC Cluster Environment Survey toextend the counts to S1.1 mm ~ 20 mJy, we see tentative
evidence for an enhancement relative to the exponential
drop in the counts at S 1.1 mm ~ 13 mJy and a smoothconnection to the bright source counts at > 20 mJy
measured by the South Pole Telescope; this excess may
be due to strong-lensing effects.
We compare these counts to predictions from several
semi-analytical and phenomenological models and findthat for most the agreement is quite good at flux densities≥ 4 mJy; however, we find significant discrepancies (≥ 3σ)
between the models and the observed 1.1 mm counts
at lower flux densities, and none of them is consistent
with the observed turnover in the Euclideannormalizedcounts at S 1.1 mm ≤ 2 mJy. Our new results therefore
may require modifications to existing evolutionarymodels for low-luminosity galaxies. Alternatively, thediscrepancy between the measured counts at the faint end
and predictions from phenomenological models could
arise from limited knowledge of the spectral energy
distributions of faint galaxies in the local Universe [1].

Figure 1: Differential source counts derived from six blank-fieldsurveys carried out with AzTEC on JCMT and ASTE.
The shaded region highlights the 68 % confidence range
on the combined counts from all six surveys.

Table 1: Summary of AzTEC blank-field surveys.

Field

020

I Scientific HighlightsArea(deg2 )

Num. ofsources

Ref.

GOODS-N

JCMT

0.08

50

[2]

LH

JCMT

0.30

180

[3]

GOODS-S

ASTE

0.08

66

[4]

ADF-S

ASTE

0.20

279

[5]

SXDF

ASTE

0.21

271

[5]

COSMOS

ASTE

0.72

230

[6]

1.60

1076

Total:
References[1] Scott, K. S., et al.: 2012, MNRAS, 423, 575.
[2] Perera, T. A., et al.: 2008, MNRAS, 391, 1227.
[3] Austermann, J. E., et al.: 2010, MNRAS, 401, 160.
[4] Scott, K. S., et al.: 2010, MNRAS, 405, 2260.
[5] Hatsukade, B., et al.: 2011, MNRAS, 411, 102.
[6] Aretxaga, I., et al.: 2011, MNRAS, 415, 3831.

TelescopeSpiral Structures in the Protoplanetary Disk around SAO 206462
MUTO, Takayuki1, GRADY, Carol A.2, HASHIMOTO, Jun3, FUKAGAWA, Misato4, HORNBECK, Jeremy B.5
SITKO, Michael6, RUSSELL, Ray7, WERREN, Chelsea6, CURE, Michel8, CURRIE, Thayne9, OHASHI, Nagayoshi10
OKAMOTO, Yoshiko11, MOMOSE, Munetake11, HONDA, Mitsuhiko12, INUTSUKA, Shu-Ichiro13, TAKEUCHI, Taku14
DONG, Ruobing15, ABE, Lyu16, BRANDNER, Wolfgang17, BRANDT, Timothy15, CARSON, Joseph18
EGNER, Sebastian10, FELDT, Markus17, FUKUE, Tsubasa10, GOTO, Miwa17, GUYON, Olivier10, HAYANO, Yutaka10
HAYASHI, Masahiko10, HAYASHI, Saeko10, HENNING, Thomas17, HODAPP, Klaus W.19, ISHII, Miki10
IYE, Masanori10, JANSON, Markus15, KANDORI, Ryo10, KNAPP, Gillian R.15, KUDO, Tomoyuki10
KUSAKABE, Nobuhiko10, KUZUHARA, Masayuki14, MATSUO, Taro20, MAYAMA, Satoshi21
MCELWAINE, Michael W.2, MIYAMA, Shoken22, MORINO, Jun-Ichi10, MORO-MARTIN, Amaya23
NISHIMURA, Tetsuro10, PYO, Tae-Soo10, SERABYN, Eugene24, SUTO, Hiroshi10, SUZUKI, Ryuji25
TAKAMI, Michihiro26, TAKATO, Naruhisa10, TERADA, Hiroshi10, THALMANN, Christian27, TOMONO, Daigo10
TURNER, Edwin L.15, WATANABE, Makoto28, WISNIEWSKI, John P.29, YAMADA, Toru30,
TAKAMI, Hideki10, USUDA, Tomonori10, TAMURA, Motohide3
1: Kogakuin University, 2: Goddard Space Flight Center, 3: The University of Tokyo, 4: Osaka University, 5: University of Louisville,
6: University of Cincinnati, 7: The Aerospace Corporation, 8: Universidad de Valparaso, 9: University of Toronto, 10: NAOJ, 11: Ibaraki
University, 12: Kanagawa University, 13: Nagoya University, 14: Tokyo Institute of Technology, 15: Princeton University, 16: Observatoirede la Côte d'Azur, 17: Max Planck Institute for Astronomy, 18: College of Charleston, 19: University of Hawaii, 20: Kyoto University, 21:
The Graduate University for Advanced Studies, 22: Hiroshima University, 23: Instituto Nacional de Técnica Aeroespacial, 24: Jet Propulsion
Laboratory, 25: TMT Observatory Corporation, 26: Academia Sinica, 27: University of Amsterdam, 28: Hokkaido University, 29: Universityof Oklahoma, 30: Tohoku University

Understanding physical properties of protoplanetarydisks is important in understanding planet formation
processes.
We report the results of observations, conductedunder SEEDS project, of the disk around SAO 206462(HD 135344B, F4V, d = 140 pc [1]). We clearly detected
the disk in scattered light at H-band. The most interesting
features were the spiral structures (Fig. 1).
Assuming that the spirals were a part of density
wave, we constructed the model equation for the spiralstructures using spiral density wave theory. As a result, it
was indicated that such spirals were able to exist in diskswith the temperature profiles that were consistent withother observations. It was also hinted that the launching
point (corotation radius) of the spirals might exist in theouter part of the disk.
It is expected that dynamically active disks
ubiquitously harbor small-scale spirals. Future observations
by large telescopes (ALMA, TMT, etc.) with better
spatial resolution will deepen our understanding of
protoplanetary disks and planet formation processes.

Figure 1: H-band polarized intensity map of the disk around SAO
206462. The central region (r ≤ 0.2 asec) is covered.
The red dashed and the red cross indicate the best-fit forthe spiral structure and the launching point. This figure
is adopted from the front page of Astronomical Herald
2013 March issue.

Reference[1] Muto, T., et al.: 2012, ApJ, 748, L22.

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021

Outer Rotation Curve of the Galaxy with VERA I :Trigonometric Parallax of IRAS 05168+3634
SAKAI, Nobuyuki

HONMA, Mareki, SHIBATA, M. Katsunori, SHIZUGAMI, Makoto(The Graduate University for Advanced Studies)			

(NAOJ)NAKANISHI, Hiroyuki, SAKANOUE, Hirofumi, KURAYAMA, Tomoharu(Kagoshima University)

Precise structure and dynamics of the Milky Way
Galaxy are still relatively ambiguous due to difficulties
of precise distance measurements. In particular, for theoutside of the solar circle region, distance measurements
have large uncertainties since the tangent velocity method
can not be used in the place (e.g., [1]). To overcome thedistance uncertainties, we have been using VERA (VLBI
Exploration of Radio Astrometry) to measure parallactic
distances and proper motions of starforming regions
located at the outer region (outside the solar circle).
Our results can be used to understand not only precise
structure of the Milky Way Galaxy (e.g., spiral arm
location), but also mass distribution of the Galaxy. In thispaper, we report one of our results for IRAS 05168+3634
as a high-mass star-forming region [2].
Eleven VLBI observations with VERA obtained
between October 2009 and May 2011 yielded thetrigonometric parallax and proper motion of IRAS
05168+3634. The parallax is 0.532±0.053 mas,corresponding to a distance of 1.88 ±0.21
0.17 kpc. The propermotion components are (µ α cos δ, μ δ ) = (0.23 ± 1.07,−3.14 ±0.28) mas yr−1. Our result places the source in the
Perseus arm. Combining the distance and proper motion
with the systemic velocity results in a rotation velocity−1−1
of 227 +9−11 km s at the source, assuming Θ0 = 240 km s .
The result corresponds to marginally slower rotation withrespect to the flat Galactic rotation curve, Θ(R) = Θ0. In
addition, the slower rotation is almost consistent withprevious VLBI results in the Perseus arm (see Fig. 1).
Fig. 1 shows the peculiar (non-circular) motions
based on VLBI observations of the Perseus arm after
subtractions of the Galactic rotation and the solar peculiar
motions. Note that a flat Galactic rotation curve —Θ(R)= Θ 0— was assumed to derive the peculiar motions.
Obviously, almost all sources in the Perseus arm are
moving systematically toward the Galactic Center,and lag behind the Galactic rotation. These motions
are consistent with the prediction of the density wave
theory which showed that large peculiar motions, toward
Galactic center and counter to the Galactic rotation, areoccurred at the inner edge of the spiral arm in the case of
inner co-rotation radius [3].
We have been observing Galactic star-forming regionswith VERA, which will allow us to understand not only
the mass distribution of the Galaxy (as part of the VERA
outer rotation curve project), but also whether the density-

022

I Scientific Highlights

wave theory is correct or not in the near future.

Figure 1: Peculiar motions in the Perseus arm. The arrows
represent peculiar motions for the sources located in the
Perseus arm based on VLBI observations. Note that a at
Galactic rotation curve —Θ(R) = Θ0— was assumed toderive the peculiar motions. Based on the figure, almost
all sources in the Perseus arm are moving systematicallytoward the Galactic Center and lag behind the Galacticrotation.

References[1] Sofue, Y., et al.: 2009, PASJ, 61, 227.
[2] Sakai, N., et al.: 2012, PASJ, 64, 108.
[3] Mel'nik, A. M., et al.: 1999, Astron. Lett., 25, 518.

Polarimetric Imaging of Large Cavity Structuresin the Pre-Transitional Protoplanetary Disk around PDS 70:
Observations of the Disk*
HASHIMOTO, Jun1, TAMURA, Motohide1, HAYASHI, Masahiko1, IYE, Masanori1, KANDORI, Ryo1
KUSAKABE, Nobuhiko1, KUZUHARA, Masayuki1, KWON, Jangmi1, MORINO, Jun-Ichi1, SUENAGA, Takuya1
SUZUKI, Ryuji1, SUTO, Hirohi1, TAKAHASHI, Yasuhiro1, DONG, Ruobing2, ZHU, Zhaohuan2, BRANDT, Timothy2
JANSON, Markus2, KNAPP, Gillian2, TURNER, Edwin2, KUDO, Tomoyuki1, USUDA, Tomonori1, EGNER, Sebastian1
TERADA, Hiroshi1, TOMONO, Daigo1, TAKAMI, Hideki1, GUYON, Olivier1, HAYANO, Yutaka1, HAYASHI, Saeko1
ISHII, Miki1, NISHIMURA, Tetsuo1, PYO, Tae-Soo1, TAKATO, Naruhisa1, HONDA, Mitsuhiko3, MCCLURE, Melissa4
MUTO Takayuki5, WISNIEWSKI, John6, ABE, Lyu7, HENNING, Thomas8, BRANDER, Wolfgang8, FELDT, Markus8
CARSON, Joseph9, FUKAGAWA, Misato10, GOTO, Miwa11, MCELWAIN, Michael12, GRADY, Carol12
HODDAP, Klaus13, MATSUO, Taro14, MAYAMA, Satoshi15, MIYAMA, Syoken16, MORO-MARTIN, Amaya17
SERABYN, Eugene18, TAKAMI, Michihiro19, THALMANN, Christian20, WATANABE, Makoto21, YAMADA, Toru22
1: NAOJ, 2: Princeton University, 3: Kanagawa University, 4: The University of Michigan, 5: Kogakuin University, 6: Universityof Washington, 7: University of Nice, 8: Max Planck Institute for Astronomy, 9: College of Charleston, 10: Osaka University, 11:
Universitatssternwerte Munchen, 12: Goddard Space Flight Center, 13: University of Hawaii, 14: Kyoto University, 15: The Graduate
University for Advanced Studies, 16: Hiroshima University, 17: CAB-CSIC/INTA, 18: Jet Propulsion Laboratory, 19: Institute of Astronomy
and Astrophysics, 20: University of Amsterdam, 21: Hokkaido University, 22: Tohoku University

Protoplanetary disks are believed to be the birthplacesof planets [1]. Among them, disks which have substantial
infrared excesses but reduced uxes at wavelengths < 20µm, i.e., transitional disks [2], could be related to theearly phases of planet formation [3] and are therefore
particularly important for understanding how, where, andwhen planets form. For many transitional disks, partial
inner holes or partial gaps have been directly resolved
by interferometry at (sub)millimeter wavelengths [4].
However, gap formation mechanism is still unclear.
One good candidate to investigate the inner hole/gap
region at tens AU is a weak-lined T Tauri star PDS 70 (K5type; 0.82 M; < 10 Myr; [5]; [6]; [7]). A scattered lightdisk with a radius at 14 to 140 AU was detected by Ksband imaging [6]. Thus, we have observed PDS 70 with
H-band polarized imaging and L'-band imaging [8].
As results of observations, a giant inner gap is clearly
resolved for the first time, and the radius of the gap is~70 AU. Our data show that the geometric center of thedisk shifts with ~6 AU toward the minor axis. We confirm
that the brown dwarf companion candidate to the north of
PDS 70 is a background star based on its proper motion.
As a result of SED fitting by Monte Carlo radiativetransfer modeling, we infer the existence of an opticallythick inner disk at a few AU. Combined with ourobservations and modeling, we classified the disk of PDS
70 as a pre-transitional disk. Furthermore, based on theanalysis of L′-band imaging data, we put an upper limit
mass of companions at ~30 to ~50 MJ within the gap.
Taking account of the presence of the large and sharp gap,
* Based on data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan.

we suggest that the gap could be formed by dynamicalinteractions of sub-stellar companions or multiple unseen
giant planets in the gap.

Figure 1: H-band polarized intensity image of PDS 70 with asoftware mask with 0.″ 4 diameter. The FOV is 3.″ 0 ×3.″ 0with a convolution of a spatial resolution.
References[1] Hayashi, C., et al.: 1985, Protostars and planets II, 1100.
[2] Strom, K. M., et al.: 1989, AJ, 97, 1451.
[3] Williams, J. P., et al.: 2011, Annu. Rev. A&A, 49, 67.
[4] Andrews, S. M., et al.: 2011, ApJ, 732, 42.
[5] Gregorio-Hetem, J., et al.: 2002, MNRAS, 336, 197.
[6] Riaud, P., et al.: 2006, A&A, 458, 317.
[7] Metchev, S. A., et al.: 2004, ApJ, 600, 435.
[8] Hashimoto, J., et al.: 2012, ApJ, 758, 19.

I Scientific Highlights

023

Molecular Gas Distributions of Interacting Galaxies
in Early and Mid Stage Using 12CO( J= 1–0) Mapping Observations
KANEKO, Hiroyuki1, KUNO, Nario2,3, IONO, Daisuke2,3, TAMURA, Yoichi4, TOSAKI, Tomoka5
NAKANISHI Koichiro2,3,6, SAWADA Tsuyoshi3,61: Tsukuba University, 2: The Graduate University for Advanced Studies, 3: NAOJ, 4: University of Tokyo, 5: Joetsu University of Education, 6:
Joint ALMA Observatory

024

I Scientific Highlights

complicated processes such as an off-centre and/or wide
distributions of molecular gas in the beginning of theinteraction.
5

15

10

20

25 [K km s-1]
20

37 28 00

26 30
00
25 30
00
24 30
13 58 42 40 38

36 34 32

30

RIGHT ASCENSION(J2000)
10

20

15 30
00
14 30
00
13 30

00
12 36 40 38 36 34 32 30 28
RIGHT ASCENSION(J2000)[K km s-1]
40
50

30

50
-18 51 30
45
52 00
15
30
45
53 00
15
30
45
54 00
12 02 00 01 58

100[K km s-1]
150

54

52

DECLINATION(J2000)

23 30 30
15
00
29 45
30
15
00
28 45
30
15
00 01 46

[K km s-1]
60
80

40

11 16 00

00

DECLINATION(J2000)

DECLINATION(J2000)

27 30

DECLINATION(J2000)

Galaxies frequently interact with other galaxies
and give an influence of strong gravity on eachother. Those celestial objects whose distributions andkinematics of stars and gas are changed by the gravity
are called as interacting galaxies. Interacting galaxies
have an important features of active star formation
which have known from about 30 years ago. Althoughmany studies have been done, a precise mechanism ofactive star formation in interacting galaxies is an open
question. Since stars are made from molecular gas, it isnecessary to understand the properties of molecular gas
in interacting galaxies for clarifying the mechanism of
bursts of star formation. Most of previous observations
aimed only at the centre of galaxies where emission
from molecular gas tends to be strong, distributions ofmolecular gas is unknown. Even more, the most targets ofobservational studies are interacting galaxies in late stage
whose star formation activity is already enhanced. Thus,
the properties of molecular gas in interacting galaxies inearly stage are scarcely investigated. Although interacting
galaxies in late stage can be used to investigate the“results” of an enhancement of star formation, its “cause”
can not be understood without observing interacting
galaxies in early stage.
In order to understand how star formation activity
is enhanced through galaxy interactions, we performed
12
CO(J=1–0), which is a good tracer of diffuse moleculargas, mapping observations using NRO 45-m radio
telescope and revealed the distributions of molecular gas
of four interacting galaxies in early and mid stage: Arp
84, VV 219, VV 254, Arp 244 (Fig. 1). The distributionsof molecular gas greatly differ from both atomic gas
and old stars whose data are already obtained with othertelescopes. These discrepancies imply that the effects by
the interaction on each medium are different and physicalproperties should be also changed from isolated galaxies.
We derived the degree of central concentration ofmolecular gas and found that molecular gas in interacting
galaxies in early and mid stage are less concentrated thanthat in isolated galaxies. This result is opposite to the factthat molecular gas in interacting galaxies in late stage
is highly concentrated toward the centre of the galaxy
and numerical simulations which suggest gas inflow
occurs when two galaxies collide. We obtained a picturethat the interaction does not proceed through a direct
infall of molecular gas to a galactic centre but through

44

42

40

38

36

RIGHT ASCENSION(J2000)

56

50

RIGHT ASCENSION(J2000)

Figure 1: Integrated intensity maps of 12CO( J = 1–0). Arp 84 (topleft), VV 219 (top-right), VV 254 (bottom-left), Arp 244(bottom-right).

Reference[1] Kaneko, H., Kuno, N., Iono, D., Tamura, Y., Tosaki, T.,
Nakanishi, K., Sawada, T.: 2013, PASJ, 65, 20.

Detailed Density and Velocity Structures of the Protostellar Core B335
KURONO, Yasutaka, SAITO, Masao, KAMAZAKI, Takeshi, MORITA, Koh-Ichiro, KAWABE, Ryohei(NAOJ)In order to understand physical processes of lowmass star formation, it is important to investigate theproperties of dense (~10 5 cm −3 ) cores in molecular
clouds. Such compact (~0.1 pc) cores supply material
to newly forming stars through dynamical gravitational
collapse, nevertheless detailed physical processes arestill uncertain. One of the investigative approaches is toderive the detailed density and velocity structures fromobservations of protostellar cores which are expected toretain information on the initial conditions of collapse.
The Bok Globule B335 is an isolated low-mass starforming region harboring a low-mass Class 0 source,which is a suitable target for the study of low-mass starformation. We carried out the observations with theNobeyama 45 m telescope and the Nobeyama Millimeter
Array (NMA) in the H 13 CO + (J = 1 – 0) line emission.
We performed combined imaging of interferometer andsingle-dish data in the Fourier domain (u–v domain), andapplied the data optimizations to sensitivities and relative
weights between 45 m and NMA data [1]. We finallyobtained a combined image of B335 in the H13CO+ line
emission with a synthesized beam size of 5.″6 ×4.″4.
Our analysis using a combining technique of
singledish and interferometer data revealed the structureof the inner dense envelope within the core with a highspatial resolution of ~750 AU. Using the 45 m andcombined data, we determined the radial column density
profile of the B335 core. We found a reliable differencein the power-law indices of density profile between theouter and inner regions of the core; n(r) ∝ r−2 for r ≥4000 AU and n(r) ∝ r−1.5 for r ≤ 4000 AU. Our derived
density profile is better explained, both qualitatively andquantitatively, in the picture of Shu’s self-similar solution
than in that of the Larson–Penston solution. Moreover, we
performed simple model calculations of position–velocity
diagrams to investigate the kinematics in the core. The
model calculations successfully reproduce observational
results, while suggesting a central stellar mass of ~0.1 M
and a small inward velocity of ~0 km s−1 in the outerregion of the core ≥ 4000 AU.
From quantitative comparisons of density and velocity
structures from the observational results with theoreticalmodels, we concluded that a picture of Shu’s solution or
an isothermal collapse of a marginally stable Bonnor–
Ebert sphere is suitable for the gravitational collapse of
the B335 core. This result is published in [2].

Figure 1: Total integrated intensity maps of B335 in the H13CO+(J= 1–0) line emission obtained with the 45 m telescope(left) and by combining the 45 m telescope and NMA
data (right). The open star in each map is the peak
position of the 87 GHz continuum emission observedwith the NMA. The beam size for each map is shown asa filled circle or filled ellipse at the bottom right corner.
Dotted circle in the combined image indicates the fieldof view, i.e., FWHM primary beam size of the NMA
observations.

References[1] Kurono, Y., Morita, K.-I., Kamazaki, T.: 2009, PASJ, 61, 873.
[2] Kurono, Y., Saito, M., Kamazaki, T., et al.: 2013, ApJ, 765, 85.

I Scientific Highlights

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Explicit-Implicit Scheme for Relativistic Radiation Hydrodynamics
TAKAHASHI, Hiroyuki R.
(NAOJ)

Relativistic flows appear in many high-energy
astrophysical phenomena in which the magnetic field
has a crucial role in dynamics. For example, magnetic
fields connecting an accretion disk with a central star,or, different points of accretion disks are twisted andamplified due to the differential rotation, launching jets.
Also magnetic fields play an important role in accretion
disks to transport the angular momentum outward,
leading to the mass accretion.
Not merely the observational point of view, but
the radiation field is also an important ingredient in
the dynamics of relativistic phenomena. The radiationpressure force would play a key role in jet acceleration.
Recently, Takeuchi, et al. [1] showed a formation ofradiatively accelerated and magnetically collimated jets
using non-relativistic radiation magnetohydrodynamic(RMHD) simulations. These magnetic and radiative
forces would accelerate jets and outflows to therelativistic speed. But, due to the lack of numerical
techniques, RMHD simulations consistently including
relativistic effects have not been performed.
The radiation field is described by the radiationtransfer equation, which represents time evolutions of
the intensity. But it is hard task to solve the transfer
equation coupling with the hydrodynamic code due toits complexity and high computational costs. Recently,
Farris, et al. [2] proposed numerical schemes to solve
general-relativistic radiation magnetohydrodynamic
equations. They solved radiation moment equations
instead of solving the radiative transfer equations

where Er, Fri and Prij are the radiation energy density, flux,
and stress, respectively.
The radiation and fluids interact each other throughabsorption and scattering processes. These processes aredescribed by radiation four force G µ. In their treatment,
G µ is numerically integrated using explicit scheme. Then,a numerical time step Δt should be restricted being shorter
than their typical timescales (Δt < min[tab, tsc]) to ensure
the numerical stability. Therefore, high computationalcosts prevent us from studying long term evolutions when
the gas is optically thick.
In this paper [3], we propose an numerical schemes
to overcome this problem. Governed equations areintegrated in time using both explicit and implicit
schemes. The former solves an hyperbolic term and026

I Scientific Highlights

Figure 1: Thermal evolution of radiation energy E r . Crosses
and squares respectively denote results of explicit andimplicit schemes, while solid curves do analyticalsolutions. Filled circles with dotted curves show theresults of the implicit scheme with a larger time step of
Δt = 10 tab.

latter one treats the gas-radiation interactions throughabsorption and scattering processes. This method allows
us to take a larger time step Δt > tab, tsc than that of the
explicit scheme.
In figure 1, we show numerical results that theradiation field approaches to the local thermodynamic
equilibrium (LTE) state. We can see that the implicit
scheme guarantees that the radiation field stably
approaches to LTE with a larger time step Δt. Thus,
our scheme drastically reduce computational costs.
We believe that our scheme can be applicable to more
realistic high-energy astrophysical phenomena.

References[1] Takeuchi, S., Ohsuga, K., Mineshige, S.: 2010, PASJ, 62, L43.
[2] Farris, B. D., Li, T. K., Liu, Y. T., Shapiro, S. L.: 2008, Phys.
Rev. D, 78, 024023.
[3] Takahashi, H. R., Osuga, K., Sekiguchi, Y., Inoue T., Tomida, K.:
2012, ApJ, 764, 122.

Effects of Power Law Primordial Magnetic Field
on Big Bang Nucleosynthesis
				

YAMAZAKI, Dai G.

(NAOJ)		

Big bang nucleosynthesis (BBN) is affected by theenergy density of a primordial magnetic field (PMF)[1,2]. For an easy derivation of constraints on models
for PMF generations, we assume a PMF with a powerlaw (PL) distribution in wave number defined with afield strength, a PL index, and maximum and minimum
scales at a generation epoch. We then show a relation
between PL-PMF parameters and the scale invariant (SI)strength of PMF for the first time. We perform a BBN
calculation including PMF effects, and show abundances
as a function of baryon to photon ratio η. The SI-PMF
strength is constrained from observational constraints
on 4He and D. The minimum abundance of 7Li/H as afunction of η slightly moves to a higher 7Li/H value at alarger η value when a PMF exists during BBN. We thendiscuss degeneracies between the PL-PMF parametersin the PMF effect. We also assume a general case inwhich both the existence and the dissipation of PMF are
possible. It is then found that an upper limit on the SIPMF strength can be derived from a constraint on 4He
abundance, and that a lower limit on the allowed 7Li
abundance is significantly higher than those observed inmetal-poor stars.
We investigated constraints on parameters of the
PL-PMF from the light elements abundance up to
Li produced in BBN [3]. We showed respective andcombined constraints on the parameters. As a result, we
obtained upper limits on the SI-PMF strength, i.e., B YSIp+D≤ 1.45 −1.95 µG from abundances of 4He and D for the2σ region of η values by the WMAP 7yr data (Fig. 1).
We assume a PMF characterized by the power
spectrum of a PL in wave number. Parameters of thisPL-PMF are a field amplitude Bλ, a PL index nB, andmaximum and minimum scales at a generation epochk [max] and k [min], respectively. We then show a relation
between PL-PMF parameters and the scale invariant (SI)strength of PMF for the first time as follows:

KUSAKABE, Motohiko(University of Tokyo)

existence and energy dissipation of the PMF are allowed.
Based on our result of the BBN calculation (Fig. 1), it
was found that an upper limit on the strength of the PMF
can be derived from a constraint on 4He abundance. A
lower limit on 7Li abundance is also derived, and it issignificantly higher than those observed in metal-poorstars. We then conclude that it is impossible to solve
the 7Li problem by the PMF energy density, even if we
consider that part of the PMF energy is dissipated andtransferred to the radiation energies.

Figure 1: Constraints on the field strength BSIX We use the following
upper limits on the abundances: Yp = 0.2667 (thick solidline) and 0.2777 (thin solid line), D/H = 2.88×10−5 (thickdot-dashed line) and 2.64×10−5 (thin dot-dashed line),and 7Li/H = 2.35×10−5 (dotted line). The vertical painted
band is the limit on the baryon to photon ratio from
WMAP 7yr data [4]. The white dashed line indicates thebest value. Painted regions in this figure are as indicatedin the legend box at the top.

(1)
Using this relation, we discuss the degeneracy of the PLPMF parameters in effects on BBN and showed somepossibility of constraining models of PMF generations by
combining constraints on the SI field strength from lightelement abundances to the relation between PL-PMF
parameters and the SI field strength.
In addition, we consider a general case in which theReferences[1] Grasso, D., Rubinstein, H. R.: 2001, Phys. Rept., 348, 163-266.
[2] Kawasaki, M., Kusakabe, M.: 2012, Phys. Rev. D, 86, 063003.
[3] Yamazaki, D. G., Kusakabe, M.: 2012, Phys. Rev. D, 86,
123006.
[4] Larson, D., et al.: 2011, ApJS, 192, 16.

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A Starbursting Proto-Cluster in Making Associatedwith a Radio Galaxy at z = 2.53 Discovered by Hα Imaging
HAYASHI, Masao*

KODAMA, Tadayuki, TADAKI, Ken-Ichi, KOYAMA, Yusei, TANAKA, Ichi

(University of Tokyo) 						Galaxy clusters in the local Universe are dominatedby early-type galaxies evolving passively, in contrast
to general fields where late-type galaxies with active
star formation are preferentially found [2]. However,it remains unknown when and how the environmental
dependence of galaxy properties appeared. Protoclusters at z ~> 2 are ideal targets to address the issues,
because approaching the formation epoch means that we
can directly witness present-day cluster galaxies being
vigorously growing.
Here, we show a discovery of a starbursting protocluster around a radio galaxy USS 1558-003 at z = 2.53
where there are a lot of cluster galaxies forming stars.
The field surveyed has been known as an over-dense
region of distant red galaxies (DRGs) [3]. Using NB2315
filter in MOIRCS on Subaru Telescope, which isperfectly matched to detect Hα emissions from galaxies
at z = 2.53, a panoramic survey of Hα emitters (HAEs) is
conducted in the proto-cluster. We have then succeededin mapping out the 2-dimensional structure of the protocluster, and investigating the star forming activities andthe stellar mass content of this forming cluster. The threemain results we have found are summarized below (seealso figure 1, and our paper [1] for more details).
(1) The proto-cluster is composed of three conspicuousgroups of galaxies. One of them is surrounding the radiogalaxy, and another is about 1.5 Mpc (physical scale)away from the radio galaxy to the south-west, and theother is in between the two clumps. These groups show
significant excess in the number densities of both HAEs
and DRGs. Their close separations suggest that theywould merge together in the near future and grow to asingle, more massive galaxy cluster at later times.
(2) A large fraction of the HAEs in this proto-cluster
have star formation rates (SFRs) higher than 100 M yr−1,
indicating that at z ~ 2.5, the progenitors of cluster earlytype galaxies are vigorously forming in the biased
high density regions. Star formation activity is higheverywhere irrespective of environment within the protocluster region, and the properties of individual HAEs
show little environmental dependence, except that the
HAEs in the densest clump may have slightly higher
SFRs compared to those in other regions.
(3) Most of the HAEs have blue colors, but someemitters have very red colors comparable to DRG. The
red HAEs tend to be clustered in the three highest density* belonged to NAOJ when the paper [1] was published.

028

I Scientific Highlights(NAOJ)

clumps in contrast to lower-z clusters where similar red
emitters are avoiding the cluster cores and preferentiallylocated in the medium density regions or the outskirts ofthe clusters. Since the red emitters are likely to be dusty
starburst galaxies in the transitional phase, this result may
indicate that some environmental effects, such as galaxygalaxy interaction, are at work on galaxies in the dense
proto-cluster core at z = 2.53 and they are just changing
their properties rapidly.

Figure 1: The spatial distribution of HAEs at z = 2.53 shown by
blue open circles with the size scaled with SFR, i.e.,larger symbols mean higher SFRs [1]. Gray open circles
show three clumps where HAEs are strongly clustered.
The red HAEs with J – Ks > 1.38 are also specified with
red open circles. The red filled dots show DRGs, while
the black dots show all galaxies detected in the field.

References[1] Hayashi, M., et al.: 2012, ApJ, 757, 15.
[2] Dressler, A., et al.: 1997, ApJ, 490, 577.
[3] Kodama, T., et al.: 2007, MNRAS, 377, 1717.

In-House Manufacturing of ALMA Receiver Parts
Mechanical Engineering Shop, Advanced Technology Center(NAOJ)At the Mechanical Engineering Shop (ME Shop) in
Advanced Technology Center, we have been working on
in-house manufacturing (mass production processing)of four critical parts for the ALMA receiver cartridges.
We are pleased to announce that we have successfullycompleted the target production volume (73 units) in
March 2013. Including prototyping, it took four years
period to complete manufacturing. The aims of in-housemanufacturing were twofold: in budgetary terms, we
wished to achieve cost savings, and in technologicalterms, to establish high-precision processing in 'mass
production'. We have mostly been successful to achieveboth of these. The products’ details and our approach to
making these are outlined below.
The following two points required particular attention
in mass production. (1) Until this project, the ME Shop
had been principally involved in manufacturing one-off
processing pieces such as in prototyping manufacturing,and the current project was the first attempt at mass
production over a relatively long period. (2) Responding
to machining request for upcoming common use
programs other than ALMA. After detailed discussion
with the ALMA receiver development team, dedicatedmachinery for mass production was selected, 50 % ofmachinist manpower was allocated, and the ME Shop
took charge of machining the following four parts formass production.
(a) Band 4 Cold Optics Support Structure(b) Band 4 Warm Optics Frame(c) Band 4 Warm Optics Elliptical Mirror(d) Band 8 Cold Optics
All these products were fully machined fromaluminum blocks. Each produce has strict tolerance on its
key geometries. The following plans were taken to meetthese demanding requirements.
- Dedicated processing staffs.
- Use of dedicated processing machinery and thoroughenvironmental control, such as air temperature.
- Use of materials with quality certificates attached.
- Final machining process after feedback to the machinery
setting from the precision measurement using a threedimensional profiler etc.
Including the prototyping manufacturing, Mr. Tetsuo
Nishino was in charge of all processing of (a) and (b),and Mr. Takeo Fukuda was in charge of (c) and (d).
The 73 final products all passed inspection for ALMA
specification.

Product Name(a) Band 4 Cold Optics Support Structure

Materials

A6061 (aluminum alloy)

Materials Block Size

100 × 113 × 130 (mm)Product Dimensions

90 × 109 × 121 (mm)Processing Machinery Used

Wire electrical discharge machine, milling machine

Accuracy Required

Height ± 0.05 (mm) Parallelism between upper andlower surface 0.015 (mm)Positional tolerance between base location holes
and upper surface pins Φ 0.05

Average Processing Period

2.5 months for 1 lot (10 units)

Product Name(b) Band 4 Warm Optics Frame

Materials

A5083 (aluminum alloy)

Materials Block Size

25 × 260 × 390 (mm) (1 pair)

Product Dimensions

25 × 135 × 320 (mm)Processing Machinery Used

Wire electrical discharge machine, milling machine

Accuracy Required

Angular accuracy in each of the three surfaces formirror attachment is ± 0.01 degrees

Average Processing Period

2.5 months for 1 lot (12 units)

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029

(a) Cold Optics
Support StructureBand 4 Cartridge

030

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Product Name(c) Band 4 Warm Optics Elliptical Mirror

Materials

A5083 (aluminum alloy) + gold plating after
processing

Materials Block Size

21.5 × 151 × 163 (mm) (6-surface milled)

Product Dimensions

21.5 × 151 × 163 (mm)Processing Machinery Used

Milling machine, machining center

Accuracy Required

Surface contour 0.02 (mm)Average Processing Period

1 month for 1 lot (10 units)

Product Name(d) Band 8 Cold Optics

Materials

A6061 (aluminum alloy)

Materials Block Size

55 × 115 × 130 (mm)Product Dimensions

52 × 112 × 122.654 (mm)Processing Machinery Used

Milling machine, machining center

Accuracy Required

Gradient of horn attachment surface 0.02 (mm)Reference point of horn attachment location ± 0.015(mm)

Average Processing Period

2 months for 1 lot (5 units)(c) Warm Optics
Elliptical Mirror

Band 4 Warm Optics Arrangement Diagram(b) Warm Optics Frame(d) Cold Optics

Band 8 Cartridge

Giant Molecular Cloud Evolutions in the nearby Spiral Galaxy M33
MIURA, Rie E.1,2, KOHNO, Kotaro2, TOSAKI ,Tomoka3, ESPADA, Daniel1, HWANG, Narae1, KUNO, Nario1
OKUMURA, Sachiko K.1,4, HIROTA, Akihiko1, MURAOKA, Kazuyuki5, ONODERA, Sachiko1,6
MINAMIDANI, Tetsuhiro7, KOMUGI, Shinya1,8, NAKANISHI, Kouichiro1,8,9, SAWADA, Tsuyoshi1,8
KANEKO, Hiroyuki1,9,10, KAWABE, Ryohei1,81: NAOJ, 2: University of Tokyo, 3: Joetsu University of Education, 4: Japan Woman's University, 5: Osaka Prefecture University, 6: Meisei
University, 7: Hokkaido University, 8: Joint ALMA Observatory, 9: Graduate University for Advanced Studies, 10: University of Tsukuba

We present a giant molecular cloud (GMC) catalogof the nearby spiral galaxy M33, containing 71 GMCs intotal, based on wide-field (121 arcmin2 in total) and highsensitivity (1σ =16–32 mK in Tmb for a velocity resolutionof 2.5 km s−1) CO(J = 3–2) observations with a spatial
resolution of 100 pc using the ASTE 10 m telescope(Fig. 1) [1]. Employing archival optical data, we also
generate a complementary new catalog of young stellar
groups (YSGs) from the excess of the surface stellar
density, and estimate their ages by comparing with stellar
evolution models. The physical parameters of YSGs arecomparable to those of typical OB associations.

Figure 1: CO(J = 3–2) integrated intensity map with 100 pc
resolution, overlaid on the Hα image. The rectangularboxes the eight observed regions with labels. The crosssymbol is the galaxy center.

A spatial comparison among the identified GMCs,
YSGs, and H II regions from a compilation in theliterature enable us to classify GMCs into four categories:
Type A, showing no sign of massive star formation (SF);Type B, being associated only with H II regions; TypeC, with both H II regions and < 10 Myr old YSGs; andType D, with both H II regions and 10–30 Myr YSGs
(Fig. 2a). Out of 65 GMCs (discarding those at the edgesof the observed fields), 1 (1 %), 13 (20 %), 29 (45 %),and 22 (34 %) are Types A, B, C, and D, respectively.
We interpret these categories as stages in a GMC
evolutionary sequence. Assuming that the timescale foreach evolutionary stage is proportional to the number ofGMCs, the lifetime of a GMC with a mass > 105 M isestimated to be 20–40 Myr. In addition, we find that thedense gas fraction as traced by the CO(J = 3–2)/CO(J = 1–0) ratio is enhanced around SF regions (Fig. 2c). Thisconfirms a scenario where dense gas is preferentiallyformed around previously generated stars, and will be thefuel for the next stellar generation.

Figure 1: An example of Type D GMC with (a) CO(J = 3–2), (b)CO(J = 1–0) integrated intensity map, (c) CO(J = 3–2)/CO(J = 1–0) ratio, and (d) Hα image. Color contours
indicate the surface density of young stars.

Reference[1] Miura, R. E., Kohno, K., Tosaki, T., et al.: 2012, ApJ, 761, 37.

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Suzaku/WAM and RHESSI Observationsof Non-Thermal Electrons in Solar Microflares

			

ISHIKAWA, Shin-nosuke(NAOJ)

OHNO, Masanori(Hiroshima University)

The maximum energy up to which electrons areaccelerated in microflares is not well understood. While
microflares frequently show softer/steeper spectra thanregular flares [1], some also show spectra comparable
to the hardest/flattest flare spectra. Because of the rather
short durations of non-thermal HXR microflares (typically< 1 minutes [2]), a large effective area is essential for thedetection of high-energy photons from microflares. The
Wide-band All-sky Monitor (WAM [3,4]), which is apart of the Hard X-ray Detector (HXD [5]) onboard theSuzaku satellite [6], is a HXR and γ-ray all-sky monitor
with the highest effective area among the instruments
presently observing the Sun. We reported on hard X-ray
spectroscopy of solar microflares observed by Suzaku/
WAM and by the Reuven Ramaty High Energy Solar
Spectroscopic Imager (RHESSI) [7].
The WAM solar flare list contains 6 GOES B-classmicroflares that were simultaneously observed by
RHESSI between the launch of Suzaku in July 2005
and March 2010. At 100 keV, the detected WAM fluxes
are more than ~20 times below the typical RHESSI
instrumental background count rates (An example of
WAM and RHESSI joint spectrum is shown in Fig.
1). The RHESSI and WAM non-thermal spectra are ingood agreement with a single power-law with photon
spectral indices between 3.3 and 4.5. In a second step,
we also searched the RHESSI microflare list for events
that should be detectable by WAM assuming the nonthermal power-law emission seen by RHESSI extends
to > 50 keV. From the 12 detectable events between July
2005 and February 2007, 11 were indeed seen by WAM.
This shows that microflares, similar to regular flares, canaccelerate electrons to energies up to at least 100 keV.

KRUCKER, Säm(University of California, Berkeley)

LIN, Robert P.

(University of California, Berkeley)2005-11-17 03:13:45-03:14:01

X-ray spectrum [photons s-1 cm-2 keV-1]

				

102

RHESSI detectors:
1, 3, 4, 5, 6, 7 and 9

100

10-2

10-4

10

energy [keV]

100

Figure 1: WAM and RHESSI joint spectrum of an example ofthe microflares in this research. The black line with theerrorbars and magenta points are RHESSI and WAM
data, respectively. The gray curve gives the RHESSI
background spectrum, and the brown line gives the
WAM background. The red curve and blue line arethermal bremsstrahlung and non-thermal power-law
components obtained by fitting the RHESSI data.

References[1] Battaglia, M., Grigis, P. C., Benz, A. O.: 2005, A&A, 439, 737.
[2] Benz, A. O., Grigis, P. C.: 2002, Sol. Phys., 210, 431.
[3] Yamaoka, K., et al.: 2005, IEEE Trans. Nucl. Sci., 52, 2765.
[4] Yamaoka, K., et al.: 2009, PASJ, 61, 35.
[5] Takahashi, T., et al.: 2007, PASJ, 59, S35.
[6] Mitsuda, K., et al.: 2007, PASJ, 59, 1.
[7] Ishikawa, S., Krucker, S., Ohno, M., Lin, R. P.: 2013, ApJ, 765,
143.

032

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Magnetically Confined Interstellar Hot Plasma
in the Nuclear Bulge of Our Galaxy
NISHIYAMA, Shogo, TAMURA, Motohide, KWON, Jungmi

UCHIYAMA, Hideki

YASUI, Kazuki, NAGATA, Tetsuya, YOSHIKAWA, Tatsuhito

SCHÖDEL, Rainer

				(NAOJ)				

(University of Tokyo)				(Kyoto University)				 (Instituto de Astrofsica de Andaluca)
		

HATANO, Hirofumi, SATO, Shuji(Nagoya University)

SUGITANI, Koji

SUENAGA, Takuya(Nagoya City University) (Graduate University for Advanced Studies)

The origin of the Galactic center diffuse X-ray
emission (GCDX) is still under intense investigation.
In particular, the interpretation of the hot (kT ≈ 7 keV)component of the GCDX, characterised by the strong Fe
6.7 keV line emission, is problematic. Two main ideas
have been suggested to account for it : a truly diffuse
plasma that bathes the emitting region (e.g., [1]); anda superposition of a large number of unresolved point
sources (e.g., [2]).
In Nishiyama et al. 2013 [3], we show that the spatial
distribution of the GCDX does not correlate with thenumber density distribution of an old stellar population
traced by near-infrared (NIR) light. The longitudinaland latitudinal profiles of the 6.7 keV line emission
measured by Suzaku clearly show an excess over thestellar number density profiles, strongly suggesting asignificant contribution of the diffuse interstellar plasma.
Contributions of the old stellar population to the GCDX
are estimated to be ~50 % and ~20 % in the nuclear stellar
disk and nuclear star cluster, respectively.
The most puzzling aspects of the GCDX is its hightemperature. Since the kT ≈ 7 keV plasma is too hot to be
gravitationally bound, it requires a huge energy source
without a confinement mechanism of the plasma. One
idea to address this energetics issue is the confinement of
the plasma by magnetic fields [4].
We have carried out NIR polarimetric observations forthe central | l | < 1°. 5 and | b | < 1°. 0 region, and we obtainpolarization originating from magnetically aligned dust
grains in the Galactic center (for more detail, see [5]). The
polarized angle traces the Galactic center’s MF direction
projected onto the sky. The obtained polarization map(Fig. 1) suggests that the GCDX region is permeated by alarge scale, toroidal magnetic field, indicating a magnetic
confinement of the hot plasma.
If the plasma were not confined, it would be rushingout of the Galactic plane vertically as a galactic wind.
Assuming the gas flows out from the X-ray emitting
region at the sound speed, the escape timescale is ~ 4 ×
104 yr. This requires a huge energy input to sustain the
hot plasma; e.g., an unreasonably high supernova rate of~ 5 × 10−3 yr−1. If the plasma is magnetically confined, andthere is no other cooling mechanism, the hot plasma only

cools by radiation with a timescale of 107–108 yr, several
orders of magnitude longer than the escape timescale.
This would reduce the required energy input by several
orders of magnitude and thus relax the energetics
problem.

Figure 1: Polarimetry results covering 3 °. 0 × 2 °. 0 in the Galactic
coordinate, together with an intensity map of 6.7 keVline emission [6]. The cyan vectors show the inferredmagnetic field direction, and the lengths are proportional
to polarization percentage.

References[1] Koyama, K., et al.: 1989, Nature, 339, 603.
[2] Wang, Q. D., et al.: 2002, Nature, 415, 148.
[3] Nishiyama, S., et al.: 2013, ApJ, 769, L28.
[4] Tanuma, S., et al.: 1999, PASJ, 51, 161.
[5] Nishiyama, S., et al.: 2009, ApJ, 690, 1648.
[6] Nobukawa, M., et al.: 2012, AIP Conf. Proc., 1427, 209.

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Young, Massive Star Candidates
Detected throughout the Nuclear Star Cluster of the Milky Way
NISHIYAMA, Shogo(NAOJ)

Nuclear star clusters (NSCs) are ubiquitous in galaxies
and appear as compact clusters at the dynamical centersof their host galaxies [1]. They show mixed stellar
populations and their spectra indicate recent events of starformation. However, it is impossible to resolve external
NSCs in order to examine the relevant processes. The
Milky Way NSC, on the other hand, is close enough to beresolved into its individual stars and presents therefore aunique template for NSCs in general.
Young, massive stars have been found by AO assisted,systematic spectroscopic studies at projected distances R< 0.5 pc from the supermassive black hole Sgr A* (e.g.,[2]). In recent years, increasing evidence has been found
for the presence of young, massive stars also at R > 0.5
pc (e.g., [3]). Our goal is a systematic search for young,massive star candidates throughout the entire region
within R ~ 2.5 pc of the black hole.
We present the results of a systematic search foryoung, massive stars within R ≈ 2.5 pc of Sgr A* via
nearinfrared (NIR) imaging observations with VLT/ISAAC [4]. Our method is a narrow-band seeing-limited
imaging, using the CO-band absorption of late-type stars
to distinguish between young, massive, early-type stars
and late-type giants in the central ~ 6 × 6 pc. Recurrence
to seeing-limited observations allow us to probe asignificantly larger FoV than what would be possible incomparable time with AO imaging.
We have found 63 early-type star candidates at R < 2.5
pc, with an estimated erroneous identification rate of only
about 20 %. Considering their K-band magnitudes andinterstellar extinction, they are candidates for Wolf-Rayetstars, supergiants, or early O-type stars. Of these, 31 stars
are so far unknown young, massive star candidates, allof which lie at R > 0.5 pc. The surface number density
profile of the young, massive star candidates can bewell fit by a single power-law (∝ R −Γ ), with Γ = 1.6 ±0.17 at R < 2.5 pc, which is significantly steeper thanthat of the late-type giants that make up the bulk of theobservable stars in the NSC. Intriguingly, this power-law
is consistent with the power-law that describes the surface
density of young, massive stars in the same brightness
range at R < 0.5 pc.
The finding of a significant number of newly identified
early-type star candidates at the Galactic center suggeststhat young, massive stars can be found throughout theentire cluster which may require us to modify existing
theories for star formation at the Galactic center. Followup studies are needed to improve the existing data and lay
the foundations for a unified theory of star formation in

034

I Scientific Highlights

SCHÖDEL, Rainer(Instituto de Astrofsica de Andaluca)

the Milky Way's NSC.

Foreground-28d59m30.0s-29d00m00.0s

Declination

				

30.0s

01m00.0s

46.0s

44.0s

42.0s

17h45m40.0s

38.0s

36.0s

Right ascension

Figure 1: Spatial distribution of the early-type star candidates(green circles). The candidates which have been
unknown so far are indicated by blue arrows. Red giants
identified by our analysis are marked by red circles. The
large blue circle delimits a region within 0.5 pc (12′.′9)in projection from Sgr A*. We have identified about 30
new candidates outside the 0.5 pc region.

References[1] Böker, T., et al.: 2010, IAU Symp., 226, 58.
[2] Do, T., et al.: 2009, ApJ, 703, 1323.
[3] Mauerhan, J. C., et al.: 2010, ApJ, 710, 706.
[4] Nishiyama, S., et al.: 2013, A&A, 549, A57.

Asymmetric Dust Jets and Extended Structure of 22P/Kopff
Observed during 2009 Appearance
HANAYAMA, Hidekazu(NAOJ)		

ISHIGURO, Masateru

WATANABE, Jun-Ichi(Seoul National University)		

(NAOJ)			

SARUGAKU, Yuki
(ISAS)FUKUSHIMA, Hideo, MIYAJI, Takeshi, YANAGISAWA, Kenshi, KURODA, Daisuke(NAOJ)

		

YOSHIDA, Michitoshi(Hiroshima University)

OHTA, Kouji(Kyoto University)

We observed the short-period comet 22P/Kopff
during the 2009 appearance with MITSuME 3-color
simultaneous imaging CCD cameras of Ishigakijima
astronomical observatory and a 2kCCD camera of Kiso
observatory from 2009 August to December after the
perihelion passage on 2009 May [1].
In the observation, we confirmed the diffuse coma
structure around the nucleus and the asymmetricfanshaped jet structure toward the south (Fig. 1). In
addition, the dust trail was detected on the project orbitof the comet, while the obvious neck-line structure could
not be confirmed.
With the observational data of the asymmetric jet, we
deduced the direction of the rotational axis. We analyzed
the time evolution for the position angle of the rotational
axis and obtained the pole orientation of (αpl, δpl) = (302°±30°, 62°±10°) or (αpl, δpl) = (122°±30°, −62°±10°).
Then, we modified the theoretical model of the dust
ejection [2] in order to explain the dust trail and theasymmetric jet, and performed the numerical simulation(Fig. 2). As a result, we found the observed dust structure
can be well reproduced by the dust emission near thesouth polar region (Fig. 3).
This means that the polar region of the comet is still
active, while most of the surface is becoming dormant.

KAWAI, Nobuyuki(Tokyo Institute of Technology)

(a)

(b)

N

1arcmin1arcminE

Figure 1: Images of 22P/Kopff on 2009 August. (a) shows the
diffuse dust structure, including a linear tail. (b) shows
the fan-shaped jet structure around the comet nucleus.
Reality

Model

w
Jet

Rotational axis
(˞jet, ˡjet)

Effective jet

Effective jet
direction (˞jet, ˡjet)

Figure 2: Image of the cone-shaped dust jet influenced by rotationof the comet nucleus.

(a)

(b)

1arcmin

References[1] Hanayama, H., et al.: 2012, PASJ, 64, 134.
[2] Ishiguro, M., et al.: 2007, Icarus, 189, 169.

1arcminFigure 3: Images of the numerical simulation of 22P/Kopff basedon the dust ejection model considering the asymmetricjet.

I Scientific Highlights

035

Production of High Temperature Plasmas
During the Early Phases of a C9.7 Flare. II. Bi-Directional Flows
Suggestive of Reconnection in a Preflare Brightening Region
WATANABE, Tetsuya, HARA, Hirohisa

		(NAOJ)				

The 2007 June 6 16:55 flare was well observedwith high time-cadence sparse raster scans by the EUV
Imaging Spectrometer (EIS) on board the Hinodespacecraft. The observation covers an active region areaof 240″× 240″ with the 1″ slit in about 160 seconds [1].
A preflare brightening to this flare, which started ~9minutes prior to flare-ribbon onset, looks like two smallloops apparently having a cusp-shape structure about 40″–50″ west of the main flaring loops. This interaction
shows dyanamic behavior in velocity during the earlyphases of the flare: The He II line at 256.32 Å shows theexistence of a bi-directional flow along the Earth-Sun lineof sight of about −70 and +100 km s−1. On the other hand,
the Fe XVI line at 262.98 Å formed at higher coronaltemperatures shows only a slight increase in intensity
at the location of these loops, and the Fe XXIII line at
263.76 Å barely appears. Electron density at the site
derived from the intensity ratios of the Fe XIV line pair at
264.78 Å and 274.20 Å is lower than the average of 109.3
cm−3 in other parts of the active-region outskirts.
The Fe IX images taken on Stereo-A/B reveal that twotiny loops may merge at first around 17:14:24 UT, andmove south- or southwest-wards. A bright point locatedat the junction of the loops seen in the images taken at
17:19:24 UT may be considered as a candidate location
where magnetic reconnection took place, triggered by
the preceding interaction of these two loops. The S-E
side loop exhibits more dynamic plasma motions via thisenergy deposition.
From these observations, the preflare-brightening
region may be heated via magnetic reconnection taking
place as a result of loop-loop interaction [2].
A similar type of transient phenomena is explosive
events constantly occurring in the quiet-sun network,
which are thought to be a manifestation of magnetic
reconnection [3]. These phenomena appear as bi-

STERLING, A. C.

(MSFC/NASA)		

HARRA, L. K.
(MSSL/UCL)

directional jets in transition-region (TR) lines. Although
the characteristics of flows in the event studied here areobserved to be similar to those of TR explosive events,
this event is associated to the occurrence of a major flare(C9.7), and plasmas are produced around the region
heated more than 10 MK. The length of brightening loops
are much larger than those of explosive events, and thelocations of up- and down-flows in the TR are better
spatially-resolved in these interacting coronal loops.

Figure 2: Line-center wavelengths of the two components in the
He II line window. Bars indicate the ranges of fitting
errors. Horizontal dotted lines indicated the wavelengths
of He II λ256.32, Si X λ256.37, and Fe X/XII λ256.405.

References[1] Watanabe, T., Hara, H., Sterling, A. C., Harra, L. K.: 2010, ApJ,
719, 213.
[2] Watanabe, T., Hara, H., Sterling, A. C., Harra, L. K.: 2012, Sol.
Phys., 281, 87.
[3] Innes, D. E., Inhester, B., Axford, W. I., Willhelm, K.: 1997,
Nature, 386, 811.

Figure 1: Coalignment among the EIS (He II and Fe XXIII), XRT (Ti-Poly), and EUVI-171 Å on STEREOB, and its difference of image to thatof STEREO-A (top panels).

036

I Scientific Highlights

The Image Slicers for the Subaru Telescope High Dispersion Spectrograph
TAJITSU, Akito, AOKI, Wako

				

(NAOJ)			

The High Dispersion Spectrograph (HDS) on Subaru
Telescope can achieve a very high resolving power, up
to 150000, by applying a very narrow slit. When a slitof 0″3. (150 µm) width is applied, the resolving power is
115000. The throughput at the slit is, however, as low as
45 % for the typical seeing size of the telescope at Mauna
Kea in Hawaii (~0″6).
. In order to improve the efficiencyof the spectrograph for observations with very highresolution, we installed a Bowen-Walraven type image
slicer [1]. This type of image slicer traps incident lightin a thin plate by total internal reflection, and slices theimage by sending the light at every second reflection to a
glass prism inclined with an appropriate angle (see figure1). After designing the instrument in late 2008, it wasconstructed in 2009 and installed in 2010. The instrument
was opened for common use of HDS from 2011 August.

YAMAMURO, Tomoyasu(OptCraft)spectrograph with the image slicer to that with the 0″. 3slit, is higher than unity for a seeing size larger than 0″. 3,and reaches two at 0 ″. 8 (see black lines in figure 2).
Hence, to obtain spectra with resolution as high as R
= 110000, a higher S/N is expected by using the image
slicer under any seeing condition at Mauna Kea. Science
results using this instrument on, e.g., metal-poor binarystars and an extrasolar planet have been published [2,3].

Figure 2: Efficiencies of image slicers and corresponding slits.
Figure 1: Optical design of IS#1.

The Bowen-Walraven type image slicer that we
installed is optimized for the two following prime
requirements. The first requirement is to maximize theenergy from point sources under the typical seeing of 0.″6
on Mauna Kea. Therefore, the clear aperture should be up
to 1″. 5 (corresponding to 0.75 mm on the focal plane ofSubaru Telescope). The second requirement is a spectral
resolving power as high as R ~110000. Therefore, thewidth of the sliced images should be 0″. 3 (0.15 mm). In
order to fill these two requirements, the image slicer isdesigned to transform a 1″. 5 × 1″. 5 field of view into fivesliced images of 0″. 3 width, as shown in figure 1. The fivesliced images (hereafter “slices”) are numbered from 1
to 5 along the optical path, as shown in the figure. We
note that since observing targets of this instrument are
assumed to be bright stars, no slice is dedicated to obtaina background-sky spectrum.
The gain of photons expected by using the image
slicer, that is, the ratio of the fraction of light entering theIn addition to this first image slicer (IS#1), we
developed two more similar ones. The second one (IS#2),
which achieves R = 85000 with the 0.″46×3 format, wasopened for common use of HDS from 2012 August. Its
spectral resolution is adjusted to the one used the mostfrequently in HDS observations. The third one (IS#3)
has the highest spectral resolution R = 165000 with the0.″2×3 format. Among the 8–10 meters telescopes in theworld, HDS with the IS#3 must be the unique instrument
to realize efficient observations with such highest spectral
resolution. This IS#3 is also going to be opened forcommon use in 2013.

References[1] Tajitsu, A., Aoki, W., Yamamuro, T.: 2012, PASJ, 64, 77.
[2] Aoki, W., Ito, H., Tajitsu, A.: 2012, ApJ, 751, L6.
[3] Hirano, T., et al.: 2012, ApJ, 759, L36.

I Scientific Highlights

037

MKID 102 Pixel Millimeter-Wave Camera Development
SEKIMOTO, Y., NOGUCHI, T., KARATSU, K., MATSUO, H., OKADA, N., MITSUI, K.
(NAOJ)NITTA, T.

(Tsukuba University/NAOJ)

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

A 1000 pixel millimeter and terahertz camera withsuperconducting MKID (Microwave Kinetic Inductance
Detector) is being developed for LiteBIRD which detects
CMB B-mode polarization and for Antarctica Dome
Fuji telescope which observes distant galaxies with wide
field of view, in collaboration with KEK, Riken, Tsukuba
University, Saitama University, and Okayama University[1]. We developed 220 and 440 GHz imaging array in2012 fiscal year.
The MKID was invented by Caltech/JPL group (P.
Day et al. 2003). Superconducting resonators in MKID
senses surface impedance determined by a number ofquasi-particles which incoming photons generate by
destroying cooper pairs. It has larger dynamic range thanTES (transition-edge sensors). The resonant frequencies
among 2–12 GHz are sensed by frequency comb generated
by DAC (Fig. 3). MKID has a simple structure named
CPW (co-planar waveguide), so a higher yield is expected.
To detect submillimeter-waves efficiently, the camera
combined lens array with superconducting planar antenna.
Although silicon is an ideal material for millimeter-wave
lens in the aspects of low loss and large refractive index,
it was not available for this lens, because it was difficult
to fabricate millimeter-wave lens array. Recently, ATC
ME shop succeeded in fabricating millimeter-wave Si
lens array by a sealing process with a high-speed spindle
and small diameter end-mills.
We have demonstrated symmetrical and low side-lobe
beam pattern of this camera with the Si lens array (Fig.
2) [2]. Although it is necessary to apply anti-reflection
coating on the lens surface due to a large refractive indexof Si, the anti-reflection coating was not applied at themeasurement.
T. Noguchi et al. have been developing high quality
superconducting film to reduce imaginary part of the gap
energy and to decreases the noise and the loss [3]. For
this purpose, an MBE instrument has been introduced. Al(111) epitaxial film was fabricated on Si (111) substrate[4]. This Al MKID achieved an extremely low noise ofelectrical NEP 6 × 10−18 W Hz−1/2 (Fig. 2) [4,5].
A test system for noise and beam measurements has
been developed with 0.1 K dilution refrigerator (Fig. 3)[6]. A readout circuit with a complex FFT has been also
developed for frequency multiplexed MKIDs (Fig. 3). It
has been demonstrated to read the 100 pixel Al-MKIDs
simultaneously [1].

038

I Scientific Highlights

NARUSE, M.

(Saitama University)

Figure 1: Antenna coupled Al-MKID 102 pixel camera [2]. (left)
102 pixel Si lens array fabricated by ATC ME shop.
(right) Al CPW pattern of 102 pixel camera. The size ofthe camera is 24 ×22 mm2.

Figure 2: (left) Dark NEP of Al MKID [5]. Amplitude noise of
NEP was 6×10−18 W Hz−1/2. Phase noise was larger byan order of magnitude. (right) Beam pattern of a pixel of
Al-MKID camera was measured at 220 GHz [2].

Figure 3: (left) Schematic drawing of MKID and its readout
electronics. (right) Al-MKID camera and 0.1 K
cryogenic system [6] .
References[1] Karatsu, K., et al.: 2012, SPIE, 8452, 84520Q.
[2] Nitta, T., et al.: 2013, IEEE TST, 3, 56.
[3] Noguchi, T., et al.: 2012, Physics Procedia, 36, 318.
[4] Naruse, M., et al.: 2012, JLTP, 167, 373.
[5] Naruse, M., et al.: 2013, IEEE TST, 3, 180.
[6] Naruse, M.: 2012, PhD thesis, University of Tokyo.

Discovery of Superhumps during a Normal Outburst of SU UMa
IMADA, Akira, IZUMIURA Hideyuki, YANAGISAWA, Kenshi, KURODA, Daisuke(NAOJ)

KAWAI, Nobuyuki

OMODAKA, Toshihiro, MIYANOSHITA, Ryo(Tokyo Institute of Technology)			

Here we report on simultaneous g’, Rc, and Ic
photometry of SU UMa (a prototype of SU UMa-type
dwarf novae) using OAO/MITSuME 50 cm telescope.
SU UMa-type dwarf novae are a subclass of dwarf
novae. Their orbital periods range 1–2 hours. SU UMatype dwarf novae show two types of outbursts. One isnormal outburst, whose duration is about a few days.
The other is superoutburst, whose duration is about two
weeks. During the superoutburst, a tooth-like modulations
called superhumps are observed. The superhump period isa few percent longer than the orbital period of the system.
This is understood by phase-dependent tidal dissipationof a precessing accretion disk.
Long-term behavior of SU UMa-type dwarf novae are
well explained within the framework of the thermal-tidal
instability model [1]. According to this model, the radiusof the accretion disk increases when a normal outburst
occurs. When the radius of the accretion disk reaches
the 3:1 resonance (at which the tidal instability sets in),a superoutburst is triggered. In other words, the radiusof the accretion disk is below the 3:1 resonance radius
outside the superoutburst.
Recently, [2] reported that superhumps are detectedsuperhumps during a normal outburst just before thesuperoutburst. [3] further reported that superhumps persist
during a normal outburst just after the superoutburst.
These observations suggest that a reform of the thermaltidal instability model is required.
In the present observations, we report on the detectionof superhumps during an isolated normal outburst of
SU UMa (see figure 1). Our result suggests that theradius of the accretion disk is already reaches the 3:1
resonance radius even in the middle of the cycle of thesuperoutbursts. Our result also raises a question why
a superoutburst is suppressed, despite the accretion
disk reaching the 3:1 resonance radius. This should be
elucidated in future observations of other SU UMa-type
dwarf novae.
More detailed discussion is given in the publishedletter [4].

(Kagoshima University)

Figure 1: Rc band light curves of SU UMa. During the normal
outburst marked with an arrow, we detected superhumps.
This is the first case that superhumps are observed
during an isolated normal outburst.

Figure 2: top: Phase-averaged Rc light curve folded with 0.07904
d. This periodicity is identical with that reported by[5]. bottom: g’-Ic color variations folded with the same
period. A phase discordance between the magnitude andcolor is often observed during superhumps.

References[1] Osaki, Y.: 1989, PASJ, 41, 1005.
[2] Kato, T., et al.: 2011, PASJ, 64, 21.
[3] Kato, T., et al.: 2013, PASJ, 65, 23.
[4] Imada, A., et al.: 2012, PASJ, 64, L5.
[5] Udalski, A.: 1990, AJ, 100, 226.

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039

NIR Spectroscopy of Star-Forming Galaxies
at z~1.4 with Subaru/FMOS		

YABE, Kiyoto

OHTA, Kouji, IWAMURO, Fumihide, YUMA, Suraphong(NAOJ)				

AKIYAMA, Masayuki(Kyoto University)

TAMURA, Naoyuki, KIMURA, Masahiko, TAKATO, Naruhisa(Tohoku University)					(NAOJ)MORITANI, Yuki, SUMIYOSHI, Masanao, MAIHARA, Toshinori				(Kyoto University)				

SILVERMAN, John

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

The gas-phase metallicity (hereafter metallicity) is
one of the important parameters in understanding thegalaxy evolution. It is known that the metallicity ofgalaxies correlates well with the stellar mass at the local
universe. The mass-metallicity relation at higher redshifts
still remains unclear because of the small sample size. We
carried out the NIR spectroscopic survey of star-forming
galaxies at z ~ 1.4 by using FMOS (Fibre Multi Object
Spectrograph) [1] on the Subaru Telescope.
We observed ~320 galaxies with K < 23.9 mag (AB),
1.2 < zph < 1.6 (zmed ~ 1.4), M∗ > 109.5 M, F(Hα)expected> 5 × 10 −17 erg s −1 cm −2 in the SXDS (Subaru XMMNewton Deep Survey) field during the FMOS/GTO. The
data reduction was done with the FMOS standard pipeline[2], and the spectral fitting including the effects of OHmasks was carried out. For 71 objects, Hα emission lines
are detected significantly.
The metallicity is derived from the obtained [N II]/Hαline ratio. The stacking analysis is also done by dividing
the sample into three stellar mass bins. The distributionof the metallicity and the stellar mass with the result
from the stacking analysis is presented in Figure 1. It
is shown that the mass-metallicity relation at z ~ 1.4 islocated between those at z ~ 2.2 and z ~ 0.8 with a smoothevolution from z~ 3 to z ~ 0.1.
It is known that there exists an intrinsic scatter
significantly larger than the observational error in the
mass-metallicity relation at z ~ 0.1. The origin of thescatter, in other words, the dependence of physicalparameters on the mass-metallicity relation, is a key
to understand the galaxy evolution. At higher redshift,
however, it is still unclear whether there is a scatter in the
mass-metallicity relation or not, again, partly due to thesmall sample size.
By using the large NIR spectroscopic sample atz ~ 1.4, we examined the scatter of the mass-metallicity
relation and the dependence of other physical parameters.
The resultant mass-metallicity relation at z ~ 1.4 shows
an intrinsic scatter of ~0.1 dex after subtracting theobservational error, which is similar to that at z~ 0.1. We040

I Scientific Highlights

find that the dependence of dust corrected SFR and thegalaxy size (half light radius) on the mass-metallicity
relation: At a fixed stellar mass, galaxies with lower
SFR (smaller size) tend to show larger metallicity [3].
The sample size, however, is still limited, and further
observations are desirable for more detailed discussions.

Figure 1: The mass-metallicity relation at z ~ 1.4. Objects withthe [NII] SN ratio of ≥ 3.0 and 1.5–3.0 are indicated byfilled and open circles, respectively. Objects with the
SN ratio of < 1.5 are shown by arrows as upper limits.
Results from the stacking analysis are shown by filledstars with error bars. Previous results at z ~ 0.1–3 in theliterature are also presented. The typical error for anindividual object is presented on the bottom-right corner.

References[1] Kimura, M., et al.: 2010, PASJ, 62, 1135.
[2] Iwamuro, F., et al.: 2012, PASJ, 64, 59.
[3] Yabe, K., et al.: 2012, PASJ, 64, 60.

Giant Molecular Clouds and Star Formationin the Tidal Molecular Arm of NGC 4039
ESPADA, Daniel1, KOMUGI, Shinya1/2, MULLER, Eric1, NAKANISHI, Kouichiro1/2/3, SAITO, Masao1/2
TATEMATSU, Kenichi1, IGUCHI, Satoru1, HASEGAWA, Tetsuo1/2, MIZUNO, Norikazu1/2, IONO, Daisuke1
MATSUSHITA, Satoki2/4, TREJO, Alfonso4, CHAPILLON, Edwige4, TAKAHASHI, Satoko4, SU, Yu Nung4
KAWAMURA, Akiko1, AKIYAMA, Eiji1, HIRAMATSU, Masaaki1, NAGAI, Hiroshi1, MIURA, Rie E.1
KURONO, Yasutaka1, SAWADA, Tsuyoshi1/2, HIGUCHI, Aya1/2, TACHIHARA, Kengo1/2
SAIGO, Kazuya1, KAMAZAKI, Takeshi1/2
1: NAOJ, 2: Joint ALMA Observatory, 3: Graduate University for Advanced Studies, 4: Academia Sinica Institute of Astronomy andAstrophysics

The properties of tidally induced arms provide a means
to study molecular cloud formation and the subsequent
star formation under environmental conditions which inprinciple are different from quasi stationary spiral arms.
We report the properties of a newly discovered molecular
gas arm of likely tidal origin at the south of NGC 4039
and the overlap region in the Antennae galaxies, witha resolution of 1 ″. 68 × 0 ″. 85, using the Atacama Large
Millimeter/submillimeter Array science verification
CO(2–1) data (Fig. 1) [1].

the morphology of beads on a string, with an almost
equidistant separation between the beads of about 350 pc,
which may represent a characteristic separation scale for
giant molecular associations.
We find that the star formation efficiency at a resolutionof 6″ (600 pc) is in general a factor of 10 higher than in
disk galaxies and other tidal arms and bridges. This arm
is linked, based on the distribution and kinematics, tothe base of the western spiral arm of NGC 4039, but
its morphology is different to that predicted by highresolution simulations of the Antennae galaxies.

Figure 2: Integrated intensity map, emphasizing the tidal molecular
arm to the South. The triangle signs show the location ofsuper stellar clusters along the molecular arm.

Figure 1: HST Optical composite image of Antennae galaxy indicating
the positions of the NGC 4038/9 nuclei, the overlap
region, NGC 4039's spiral arm, and the molecular arm oftidal origin that we study in [1]. The rectangle indicatesthe mosaic covered by ALMA observations.

Reference[1] Espada, D., et al.: 2012, ApJ, 760, L25.

The arm extends 3.4 kpc (34″) and is characterized bywidths of <~ 200 pc (2″) and velocity widths of typically∆V  10–20 km s−1 (Fig. 2). About 10 clumps are strungout along this structure, most of them unresolved, withaverage surface densities of Σ gas  10–100 M  pc −2,and masses of (1–8) × 106 M. These structures resemble
I Scientific Highlights

041

Disentangling the Circumnuclear Environs of Centaurus A:
Gaseous Spiral Arms
ESPADA, Daniel1/2/3, MATSUSHITA, Satoki3/4, PECK, Alison B.4/5, HENKEL, Christian6/7
ISRAEL, Frank8, IONO, Daisuke1
1: NAOJ, 2: Harvard-Smithsonian Center for Astrophysics, 3: Academia Sinica Institute of Astronomy and Astrophysics, 4: Joint ALMA
Observatory, 5: NRAO, 6: Max-Planck-Institut für Radioastronomie, 7: Astron. Dept., King Abdulaziz University, 8: Leiden University

We report the existence of spiral arms in the recently
formed gaseous and dusty disk of the closest giant
elliptical, NGC 5128 (Centaurus A), using high resolution
12
CO(2–1) observations of the central 3′ (3 kpc) obtainedwith the Submillimeter Array (SMA) [1]. This provides
evidence that spiral-like features can develop within
ellipticals if enough cold gas exists.
We elucidate the distribution and kinematics of themolecular gas in this region with a resolution of 4 ″. 4
× 1 ″. 9 (80 pc × 40 pc). From the 12 CO(2–1) emission
distribution in Fig. 1, we confirm that the molecular gas
is preferentially located along two filamentary structures
resembling spiral-arm-like features to the SE and NWof the circum-nuclear gas (< 200 pc). The larger fieldof view of our observations demonstrates that thesefilamentary structures extend at least 1″. 0, and they are
curved toward the NE and SW. The general properties of
the arms are similar to those in spiral galaxies: they aretrailing, their width is ~500 ± 200 pc, and the pitch angle
is ~20°.
A consequence of the compression produced by thesespiral arms is that it is expected to trigger star formation(SF) on the leading edge. This is consistent with abundant
SF traced by Paα, coincident at least with the southernmolecular spiral arm (nearest part and thus likely the least
obscured). The spiral features seen in the 12CO emissionis also associated with the distribution of certain tracers
observed in poorer angular/spectral resolution maps,
such as the SCUBA 450 µm emission map as well as thepure rotational line of molecular hydrogen H2 (J = 2–0)
S(0) (28.22 µm) emission observed with Spitzer/IRS[2]. The molecular hydrogen transition H2 (J = 2–0) S(0)indicates the presence of gas with T ~ 200 K, which islikely tracing photodissociation regions associated with
abundant SF.
A small perturbation could have triggered thisspirality, such as a non-axisymmetric weak potential[3] or a minor merger after the disk was relatively wellsettled. From the HI structure and kinematics [4] we inferthat the formation of spiral arms took place in less than
0.3 Gyr, which is likely the most accurate measure oftime at our disposal since H I is one of the most sensitive
components of interaction. Simulations of gas fuelingin the deep potentials of giant ellipticals are needed toinvestigate the response of the gas under these conditions.

042

I Scientific Highlights

Figure 1: Left) Optical image of Centaurus A, showing its
prominent dust lane. Right) The molecular gas as traced
by our SMA CO(2–1) observation (green), PAH and
dust emission at 8 μm observed by Spitzer (red, [5]), andthe Chandra X-ray observations of the jet (blue). Notethat the spiral and the 8 μm emission in this panel arewithin the optical dust lane visible in the left panel. The
most prominent features of the 12CO(2–1) emission are
consistent with those of the 8 μm emission, but the COshows the spiral arms.

References[1] Espada, D., et al.: 2012, ApJ, 756, 10.
[2] Quillen, A. C., et al.: 2008, MNRAS, 384, 1469.
[3] Espada, D., et al.: 2009, ApJ, 695, 116.
[4] Struve, C., et al.: 2010, A&A, 515, A67.
[5] Quillen, A. C., et al.: 2006, ApJ, 645, 1092.

A Large Scale Structure Traced by [O II] Emitters
Hosting a Distant Cluster at z = 1.62
TADAKI, Ken-ichi, KODAMA, Tadayuki

			
			

(NAOJ) 			

KOYAMA, Yusei(NAOJ)		

OTA, Kazuaki(Kyoto University)

PAPOVICH, Casey(Texas A&M University)

TANAKA Masayuki

HAYASHI, Masao(University of Tokyo)

BRODWIN, Mark

(University of Missouri)

IYE, Masanori					(NAOJ)		(University of Tokyo/NAOJ)

It is widely known that the formation and evolutionof galaxies strongly depend on their surrounding
environments [1]. Clusters and their surrounding regions
serve as ideal sites for studying the roles of galaxy
environment on galaxy formation and evolution. We haveconducted a narrow-band survey of [O II] emitters in andaround the ClG J0218.3–0510 cluster at z = 1.6, which isone of the most distant cluster, using Suprime-Cam on
Subaru. The observation with zR filter was newly carriedout to measure the continuum at the same wavelength as
the narrow-band filter (NB 973).
On the basis of narrow-band excesses and photometricredshifts, our survey provides a sample of 352 [O II]
emitters over a 830 arcmin2 area [2]. The FMOS nearinfrared spectroscopic observations have confirmed 31[O II] emitters at z ~ 1.6 by the presence of Hα or [O III]lines at the expected wavelengths. The [O II] emittersconstitute a large scale structure at z = 1.62 in which the
ClG J0218.3–0510 cluster is embedded (Figure 1). Also,
we find that many star-forming [O II] emitters are locatedeven in the cluster core (r < 0.4 Mpc in the physicalscale) and in the surrounding clumps, and show a very
high overdensity by a factor of 40 compared to the fieldregion. This trend is consistent with our previous studies
in the distant cluster at z = 1.47 [3,4], suggesting thatthe integrated star formation activity per unit volume isactivated in cluster regions.
Also, we obtain a large fraction of [O II] emitterseven in the cluster core, showing that the star forming
activity in the cluster core is elevated substantiallycompared to the local clusters where there are little starforming galaxies in their cores. There is no longer aenvironmental dependence in the relative fraction of [O II]
emitters in the all population, and the well known SFRdensity relation in the present-day Universe no longer
exists within errors. Furthermore, the properties of theindividual [O II] emitters, such as star formation rates,
stellar masses and specific star formation rates, do notdepend on the local density, either. These results suggestthat the [O II] emitters in the high density regions are justin the transition phase from a star-bursting mode to aquiescent mode due to some environmental effects andthe star formation rates in these systems may be rapidly
declining.

Figure 1: The 2-D distributions of 352 [O II] emitters. Blue and red
filled circles show star-forming and red [O II] emitters,
respectively. Squares indicate the spectroscopicallyconfirmed objects with 1.590 ≤ zspec < 1.620 (black),
1.620 ≤ zspec ≤ 1:630 (green) and 1.630 < zspec ≤ 1.644(red). Contours denote the local number density of [O II]
emitters. A gray filled circle is a masked region near abright star.

References[1] Kauffmann, G., et al.: 2004, MNRAS, 353, 713.
[2] Tadaki, K.,et al.: 2012, MNRAS, 423, 2617.
[3] Hayashi, M., et al.: 2010, MNRAS, 402, 1980.
[4] Hayashi, M., et al.: 2011, MNRAS, 415, 2670.

I Scientific Highlights

043

Discovery of a Protocluster at z ~ 6
TOSHIKAWA, Jun, SHIBUYA, Takatoshi, ISHIZAKI, Yoshifumi(Graduate University for Advanced Studies)

KASHIKAWA, Nobunari, HAYASHI, Masao			OTA, Kazuaki, NAGAO, Tohru(NAOJ)				

(Kyoto University)

MOROKUMA, Tomoki, SHIMASAKU, Kazuhiro, MOTOHARA, Kentaro(University of Tokyo)

			

JIANG, Linhua, EGAMI, Eiichi(University of Arizona)

Exploring the structure formation and evolutionary
history of the early universe is an issue of strong current
interest in astronomy. In the cold dark matter model,
clusters of galaxies form in the densest peaks of dark
matter in the early universe. These grow by merging
and by accreting material from surrounding low-density
regions [1]. Theoretical models predict that galaxies
lying inside these high-density regions may have formed
earlier and/or evolved more rapidly, compared with
their surroundings [2]. Clusters of galaxies are thus thenoteworthy site of dark matter structure formation andgalaxy evolution. Protoclusters in the early universe
would provide a great deal of information on theprimordial conditions of clusters at their birth.
We used the deep and wide field of the Subaru Deep
Field. These images were constructed by stacking all thedata taken from 2001 to 2008, containing almost 30 hours
worth of integration time in total. We selected 258 z ~ 6galaxy candidates using Lyman break technique. Figure
1 shows the sky distribution of the 258 z ~ 6 galaxy
candidates. We found an apparently overdense region,
centered in the southern part of the field. To determine theoverdensity significance quantitatively, we estimated the
local surface number density. We found that our region ofinterest appeared overdense at the 6σ significance level
beyond the mean surface number density at the peak.
We carried out follow-up spectroscopy on theoverdense region, using FOCAS on the Subaru telescope.
We spectroscopically confirmed 15 z ~ 6 galaxies in theoverdense region. Eight galaxies of them are apparently
concentrating at z ~ 6.01 (Δz < 0.05). The redshiftconcentration at z ~ 6.01 is about seven times higher than
the number density expected from a uniform distribution.
Thus, this region is almost certain to be a galaxy
protocluster at z ~ 6.01. If true, this protocluster would
be the highest redshift large scale structure probed by theunique wide-field imaging capability of SuprimeCam.
The velocity dispersion of the eight protocluster
members is 647 ± 124 km s −1 , which is about threetimes higher than that predicted by the standard
cold dark matter model. From the three-dimensional
distribution, we proposed two possible explanations forthis discrepancy: either the protocluster is already mature,044

I Scientific Highlights

MALKAN, Matthew A.
(University of California)

with old galaxies at the center, or it is still immatureand composed of three subgroups merging to become alarger cluster. Further deep spectroscopic observations or
multi-wavelength imaging to trace the rest-frame optical
wavelengths would provide a clearer picture of the
protocluster structure, as well as providing constraints forthe galaxy/stellar populations of protocluster members[3].

Figure 1: Sky distribution of 258 z ~ 6 galaxy candidates, withsurface number density contours. The z ~ 6 galaxy
candidates are represented by filled circles whose size
is proportional to the z′-band magnitudes. The lines
correspond to contours of surface overdense significancefrom 6σ to 0σ with a step of 2σ. The overdense region
can be clearly seen at the southern edge of the plot.

References[1] Springel, V., et al.: 2005, Nature, 435, 629.
[2] De Lucia, G., et al.: 2006, MNRAS, 366, 499.
[3] Toshikawa, J., et al.: 2012, ApJ, 750, 137.

Direct Imaging Discovery of a ‘Super-Jupiter’around the Late B-Type Star κ AndCARSON, J.1/2, THALMANN, C.2/3, JANSON, M.4, KOZAKIS, T.1, BONNEFOY, M.2, BILLER, B.2
SCHLIEDER, J.2, CURRIE, T.5, MCELWAIN, M.5, GOTO, M.6, HENNING, T.2, BRANDNER, W.2, FELDT, M.2
KANDORI, R.7, KUZUHARA, M.7/8, STEVENS, L.1, WONG, P.1, GAINEY, C.1, FUKAGAWA, M.9
KUWADA, Y.9, BRANDT, T.4, KWON, J.7, ABE, L.10, EGNER, S.11, GRADY, C.5, GUYON, O.11
HASHIMOTO, J.7, HAYANO, Y.11, HAYASHI, M.7, HAYASHI, S.11, HODAPP, K.12, ISHII, M.11, IYE, M.7
KNAPP, G.4, KUDO, T.11, KUSAKABE, N.7, MATSUO, T.13, MIYAMA, S.14, MORINO, J.7
MORO-MARTIN, A.15, NISHIMURA, T.11, PYO, T.11, SERABYN, E.16, SUTO, H.7, SUZUKI, R.7
TAKAMI, M.17, TAKATO, N.11, TERADA, H.11, TOMONO, D.11, TURNER, E.4/18, WATANABE, M.19
WISNIEWSKI, J.20, YAMADA, T.21, TAKAMI, H.7, USUDA, T.11, TAMURA, M.7
1: College of Charleston, 2: MPIA, 3: University of Amsterdam, 4: Princeton University, 5: Goddard Space Flight Center, MaximiliansUniversität, 7: NAOJ, 8: The University of Tokyo, 9: GUAS, 10: Université Le de Nice-Sophia Antipolis, 11: Subaru Telescope, 12: Universityof Hawaii, 13: Kyoto University, 14: Hiroshima University

Stellar mass is emerging as one of the most importantparameters in determining the properties of planetarysystems, along with stellar metallicity. Radial velocity
surveys have indicated that the frequency of giant planets
increases with the mass of the stellar host [1], and manyof the roughly dozen exoplanets that have been directly
imaged so far have had A-type stellar hosts [2,3], despite
such large stars being in the small minority of surveyed
targets. The increase in planet frequency with host starmass can be readily explained theoretically, through theconsideration that more massive stars are likely to havemore massive disks [4]. On the other hand, massive
stars also feature anl increased intensity of high-energy
radiation, which may significantly shorten the disk
lifetime due to photo evaporation, and thus decrease thetime window in which giant planets are allowed to form.
This raises the question whether there is a maximum
stellar mass above which giant planets are unable to form.
We present the direct imaging discovery of an
extrasolar planet, or possible low-mass brown dwarf, at
a projected separation of 55 ± 2 AU (1″. 058 ± 0″. 007) fromthe B9-type star κ And [5]. The planet was detected with
Subaru/HiCIAO during the SEEDS survey, and confirmed
as a bound companion via common proper motion
measurements. Observed near-infrared magnitudes of
J = 16.3 ± 0.3, H = 15.2 ± 0.2, KS = 14.6 ± 0.4, and L′ =13.12 ±0.09 indicate a temperature of ~1700 K. The hoststar is a member of the Columba association, implying
a corresponding age of 30 +20−10 Myr. The system age,
combined with the companion photometry, points to amodel-dependent companion mass ~12.8 MJup. The hoststar’s estimated mass of 2.4–2.5 M places it among themost massive stars ever known to harbor an extrasolar
planet or low-mass brown dwarf. While the mass ofthe companion is colse to the deuterium burning limit,
its mass ratio, orbital separation, and likely planet-likeformation scenario imply that it may be best defined as a‘Super-Jupiter’ with properties similar to other recently
discovered companions to massive stars radial velocity
surveys.

Figure 1: Signal-to-Nise map of κ And b after LOCI/ADI data
reduction. The S/N is calculated in concentric annuli
around the star.

References[1] Johnson, M., et al.: 2010, PASP, 122, 905.
[2] Marois, C., et al.: 2008, Science, 322, 1348.
[3] Lagrange, A.-M., et al.: 2009, A&A, 493, L21.
[4] Mordasini, C., et al.: 2012, A&A, 541, 97.
[5] Carson, J., et al.: 2013, ApJ, 763, L32.

I Scientific Highlights

045

High-Contrast Near-Infrared Polarization Imagin of MWC 480
KUSAKABE, N.1, GRADY, C.2, SITKO, M.3/4, HASHIMOTO, J.1, KUDO, T.1, FUKAGAWA, M.5, MUTO, T.6/7
WISNIEWSKI, J.8, MIN, M.9, MAYAMA, S.10, WERREN, C.3, DAY, A.3, BEERMAN, L.3, LYNCH, D.11
RUSSELL, R.11, BRAFFORD, S.12, KUZUHARA, M.13, BRANDT, T.14, ABE, L.15, BRANDNER, W.16
CARSON, J.17, EGNER, S.18, FELDT, M.16, GOTO, M.19, GUYON, O.18, HAYANO, Y.18, HAYASHI, M.20
HAYASHI, S.18, HENNING, T.16, HODAPP, K.21, ISHII, M.20, IYE, M.1, JANSON, M.14, KANDORI, R.1
KNAPP, G.14, MATSUO, T.22, MCELWAIN, M.23, MIYAMA, S.1, MORINO, J.1, MORO-MARTIN, A.14/24
NISHIMURA, T.18, PYO, T.18, SUTO, H.1, SUZUKI, R.1, TAKAMI, M.25, TAKATO, N.18, TERADA, H.18
THALMANN, C.26, TOMONO, D.18, TURNER, E.14/27, WATANABE, M.28, YAMADA, T.29, TAKAMI, H.18
USUDA, T.18, TAMURA, M.1
1:NAOJ, 2: Eureka Scientific, 3: University of Cincinnati, 4: Space Science Institute, 5: Osaka University, 6: Tokyo Institute of Technology, 7:
Kogakuin University, 8: University of Washington, 9: Astronomical Institute ‘Anton Pannekoek’, 10: The Graduate University for Advanced
Studies, 11: The Aerospace Corporation, 12: Brafford & Phillips, 13: Department of Earth and Planetary Science, The University of Tokyo, 14:
Princeton University, 15: Université Le de Nice-Sophia Antipolis, 16: MPIA, 17: College of Charleston, 18: Subaru Telescope, 19: LudwigMaximilians-Universität, 20: Institute for Astronomy, The University of Tokyo, 21: University of Hawaii, 22: Kyoto University, 23: Goddard
Space Flight Center, 24: Instituto Nacional de Técnica Aeroespacial, 25: Academia Sinica, 26: University of Amsterdam, 27: Kavri IPMU, 28:
Hokkaido University, 29: Tohoku University

For the vast majority of protoplanetary disks,modeling of the IR spectral energy distribution (SED) has
been the principal tool for characterizing the properties ofthe dust disk. Some higher mass analogs to T Tauri stars,
The Herbig Ae stars, exhibit striking variability in the IR
SED, which has been interpreted as reflecting changes inthe scale height of the dust disk at or near the sublimation
radius [1]. One of the key predictions of modeling fromthe IR excess of Herbig Ae stars is that for protoplanetarydisks, where significant grain growth and settling has
occurred, the dust disk has flattened to the point that it
can be partially or largely shadowed by the innermost
material at or near the dust sublimation radius. Whenthe self-shadowing has already started, the outer disk
is expected to be detected in scattered light only in the
exceptional cases when the scale height of the dust disk
at the sublimation radius is smaller than usual. Hightcontrast imaging combined with the IR spectral energy
distribution allow us to measure the degree of flatteningof the disk, as well as to determine the properties of theouter disk.
We present polarimetric differential imaging in the
H band obtained with Subaru/HiCIAO of MWC 480 [2].
The HiCIAO data were obtained at a historic minimumof the NIR excess. The disk is detected in scattered
light from 0″. 2 to 1″. 0 (27.4–137 au). Together with themarginal detection of the disk from 1998 February 24 by
Hubble Space Telescope/NICMOS [3], our data constrain
the opening half-angle for the disk to lie between 1 °. 3 ≤θ ≤ 2 °. 2. When compared with similar measures in CO
for the gas disk is a factor of 5–7 flatter than transitional
disks, which have structural signatures that giant planets
have formed.

046

I Scientific Highlights

1"=137AU1

2 3 4
mJy/arcsec2

Figure 1: H-band Polarization Intensity image of MWC 480.
Central black circle shown the occulting mask (r = 0.″15).

References[1] Sitkko, M. L., et al.: 2008, ApJ, 678, 1070.
[2] Kusakabe, N., et al.: 2012, ApJ, 753, 153.
[3] Grady, C. A., et al.: 2010, ApJ, 719, 1565.

Optics Design and Optimizationsof the Multi-Color TES Bolometer Camera for the ASTE Telescope
TAKEKOSHI, Tatsuya1/2, MINAMIDANI, Tetsuhiro1, NAKATSUBO, Shunichi1, OSHIMA, Tai2
KAWAMURA, Masayuki2/3, MATSUO, Hiroshi2, SATO, Tatsuhiro2, HALVERSON, Nils W.4
LEE, Adrian T.5, HOLZAPFEL, William L.5, TAMURA, Yoichi3, HIROTA, Akihiko2,
SUZUKI, Kenta3, IZUMI, Takuma3, SORAI, Kazuo1, KOHNO, Kotaro3, KAWABE, Ryohei2
1: Hokkaido University, 2: NAOJ, 3: University of Tokyo, 4: University of Colorado, Boulder, 5: University of California, Berkeley

Wideband mm/submm continuum observations
provide great opportunities to explore the cosmic historyof star-formation across the Hubble time via observations
toward submm galaxies and nearby galaxies, as well as
the clusters of galaxies through the Sunyaev-Zel’dovich
effect. To promote such studies, a new TES (Transition
Edge Sensor) bolometer camera for the ASTE 10-m
telescope has been developed. The observing bands arecarefully selected at 1100, 850, and 450 μm. In this study,
we design the re-imaging optics to realize multi-pixel,
wide field of view, and multi-color system under thelimitation of the Cassegrain system of ASTE.
The optics is designed using the ray-trace method.
Figure 1 and 2 show the designed cabin optics andcold optics. The optics has capabilities of the two-color
observation and the 7.5 arcmin field of view. The pixel
numbers are optimized to be 169, 271, and 919 for the
1100, 850, and 450 μm bands, respectively. The imaging
qualities of the designed optics is enough better toachieve diffraction limit at the shortest wavelength.
The designed optics is simulated by physical optics
to evaluate the influence of diffraction. The beam
properties are calculated by tracing the propagations of
the electro-magnetic wave radiated from conical horns.
Consequently, the aperture efficiencies are ~35 %, 35 %,and 32 %, and the beam sizes (FWHM) are ~28″, 22″, and12″ for the 1100, 850, and 450 μm bands, respectively.
Thus we demonstrate the designed optics can achievesufficient optical performance at the observing bands.
Based on the optics design, the bolometer camera were
fabricated and evaluated. The first on-site installation
was performed in May 2012. The upcoming scientificruns expected to create new scientific achievements forunderstandings of the formation history of the Universe.

Reference[1] Takekoshi, T., et al.: 2012, IEEE Trans. Terahertz Sci. Technol.,2, 584.

Figure 1: Receiver cabin optics. The rays reflected by the mainand sub-reflectors focus near the ceiling of the receivercabin, and go into the receiver cabin. A modified
ellipsoidal mirror optimized by adding fifth-orderedpolynomials to reduce aberration is located near thebottom of the cabin to refocus the outspreading rays into
the camera cryostat.

Figure 2: Cold optics. The rays reflected by the ellipsoidal mirror
go through a cryostat window. The dichroic filter divides
incoming rays into two bands. Each ray is focused at
the focal plane after a flat mirror and a high density
polyethylene lens, and couples with a conical horn.

I Scientific Highlights047

Three-Dimensional Hydrodynamic Core-Collapse Supernova Simulations
for an 11.2 M Star with Spectral Neutrino Transport
TAKIWAKI, Tomoya(NAOJ)

Core-collapse supernovae have long drawn theattention of astrophysicists because they have many
aspects playing important roles in astrophysics. They
are the mother of neutron stars and black holes; theyplay an important role for acceleration of cosmic rays;
they influence galactic dynamics triggering further
star formation; they are gigantic emitters of neutrinos
and gravitational waves. They are also a major site fornucleosynthesis, so, naturally, any attempt to addresshuman origins may need to begin with an understandingof core-collapse supernovae.
Ever since the first numerical simulation of Colgate &White (1996), the neutrino-heating mechanism, in whicha stalled bounce shock is revived by neutrino energy
deposition to trigger explosions, has been the working
hypothesis of supernova theorists for these ~50 years.
However, one important lesson we have learned from thepioneering simulations that implemented the best input
physics and numerics to date, is that the mechanism fails
to blow up canonical massive stars in spherical symmetric(1D) simulations. Pushed by mounting supernova
observations of the blast morphology, it is now almost
certain that the breaking of the spherical symmetry is the
key to solve the supernova problem.
In fact, the neutrino-driven explosions havebeen obtained in the following state-of-the-art twodimensional (2D) simulations. Using the MuDBaTH
code which includes one of the best available neutrinotransfer approximations, Buras et al. (2006) firstly
reported explosions for a non-rotating low-mass (11.2 M)progenitor of Woosley et al. (2002), and then for a
15 M progenitor of Woosley & Weaver (1995) with amoderately rapid rotation imposed by Marek & Janka(2009).
To go up the ladders beyond 2D simulations, we
explore in this study possible 3D effects in the supernova
mechanism by performing 3D, multigroup, radiationhydrodynamic core-collapse simulations. For themultigroup transport, the IDSA scheme (Liebendörfer etal. (2009)) is implemented, which can be done rather in astraightforward manner by extending our 2D modules to
3D.
We focus here on the evolution of the 11.2 M star.
By comparing with our 1D and 2D results, we study
how the increasing multi-dimensionality could affect the
postbounce supernova dynamics.
In agreement with previous study, our 1D model
does not produce explosions for the 11.2 M star, while048

I Scientific Highlights

the neutrino-driven revival of the stalled bounce shock
is obtained both in the 2D and 3D models. Their result
indicates that violent convective matter motions promote
the neutrino heating for successful explosions.
For detail, see the original paper of Takiwaki et al.
(2012).

Figure 1: Time snapshot of the 3D model. The surfaces of constantentropy are depicted in the center and cutted colour
contour of entropy is pasted on the side walls.

References[1] Takiwaki, T., Kotake, K., Suwa, Y.: 2012, ApJ, 749, 98.
[2] Buras, R., Janka, H.-T., Rampp, M., Kifonidis, K.: 2006, A&A,
457, 281.
[3] Marek, A., Janka, H.-T.: 2009, ApJ, 694, 664.
[4] Liebendörfer, M., Whitehouse, S. C., Fischer, T.: 2009, ApJ,
698, 1174.

Fundamental Structure of the Galaxy Determined with VERA
HONMA, Mareki, NAGAYAMA, Takumi, BUSHIMATA, Takeshi, HIROTA, Tomoya, JIKE, Takaaki
KIM, Mi Kyoung, KAMEYA, Osamu, KAWAGUCHI, Noriyuki, KOBAYASHI, Hideyuki, KUJI, Seisuke
MATSUMOTO, Naoko, MANABE, Seiji, MIYAJI, Takeshi, NIINUMA, Kotaro, OYAMA, Tomoaki
SAKAI, Nobuyuki, SATO, Katsuhisa, SHIBATA, Katsunori, SUNADA, Kazuyoshi
TAMURA, Yoshiaki, UENO, Yuji, YAMAUCHI, Aya(NAOJ)

ANDO, Kazuma, HANDA, Toshihiro, IMAI, Hiroshi, KURAYAMA, Tomoharu,
NAKAGAWA, Akiharu, NAKANISHI, Hiroyuki, OMODAKA, Toshihiro, SHIOZAKI, Satoshi(Kagoshima University)

CHOI, Yoon Kyung, SATO, Mayumi

		(MPIfR)			

We have determined fundamental structure of the
Milky Way Galaxy based on the results of highlyaccurate astrometry carried out by VERA and other VLBI
arrays. VERA (VLBI Exploration or Radio Astrometry),
being operated by NAOJ in collaboration with
Kagoshima University, has been conducting astrometryof Galactic maser sources with an aim to reveal the threedimensional structure of the Milky Way Galaxy based
phase-referencing VLBI technique, and similar projects
are also on-going using VLBA, EVN and so on.
In the present study, we have compiled astrometricresults (distances and 3-d motions) of 52 star-forming
regions obtained by VERA and other arrays, and usedthem to determine the fundamental structure of the
Milky Way Galaxy. Figure 1 shows the distribution of
the 52 sources in the Galaxy, with vectors showing theirmotions in the Galactic plane. Clearly Galactic rotation
can be seen, and from their motions even the position

MOTOGI, Kazuhito(Hokkaido University)		

OH, Chung Sik(KASI)of the rotation center can be estimated. In the present
study, we have utilized MCMC (Markov-chain Monte
Carlo) method to obtain the best model to reproduce thepositions and motions of the maser sources, with model
parameters such as the Galactic center distance, R0, andGalactic rotation velocity at the Sun, Θ0.
The Galaxy center distance is obtained to be R0 = 8.05
± 0.45 kpc. This is consistent with the recent results andthe IAU standard (R0 of 8~8.5 kpc). On the other hand,
the Galactic rotation velocity is determined as Θ0 = 238± 14 km s−1, which is roughly 10 % larger than the IAU
standard of 220 km s−1. This result indicates that the massof the Galaxy is higher than previously expected, which
impacts not only on the Galactic structure but also on
dark mater search in the Galaxy.
Reference[1] Honma, M., et al.: 2012, PASJ, 64, 136.

Galactic
centerFigure 1: Galaxy-scale distribution and motion of the 52 star-forming regions, for which accurate astrometric results have been obtained.

I Scientific Highlights

049

NRO M33 All-Disk Survey of Giant Molecular Clouds (NRO MAGiC): II.
Dense Gas Formation within Giant Molecular Clouds in M33
ONODERA, S.1/2, KUNO, N.2/3, TOSAKI, T.4, MURAOKA, K.5, MIURA, E. R.6, KOHNO, K.7/8
NAKANISHI, K.3/6, SAWADA, T. 9, KOMUGI, S.9, KANEKO, H.10, HIROTA, A.2, KAWABE, R.2/9
1: Meisei University, 2: NRO, 3: Graduate University for Advanced Studies (Sokendai), 4: Joetsu University of Education, 5: Osaka Prefecture
University, 6: ALMA Project Office, 7: IoA, University of Tokyo, 8: RESCEU, University of Tokyo, 9: Joint ALMA Office, 10: University ofTsukuba

We have conducted observations of the 12CO(J = 1–0)
and 12 CO(J = 3–2) line emission of 74 major giant
molecular clouds (GMCs) within the galactocentric
distance of 5.1 kpc in the Local Group galaxy M33[1]. The observations are part of the Nobeyama Radio
Observatory M33 All-disk survey of Giant Molecular
Clouds project (NRO MAGiC [2]). The spatial resolution
is 100 pc.
We detect 12 CO(J = 3–2) emission of 65 GMCs
successfully. The 12 CO(J = 1–0) and 12 CO(J = 3–2)
integrated intensity ratio R 3–2/1–0 is spread over a wide
range from less than 0.1 to 0.74, having a weighted meanof R 3–2/1–0 = 0.26. This weighted mean is slightly smaller
than that of the quiescent disk region of the Milky Way.
Furthermore, we find that the correlation between thesurface density of the star formation rate (Σ SFR), which
is derived from a linear combination of Hα and 24 μm
emissions, and the 12CO(J = 3–2) integrated intensity
still holds at the scale of 100 pc (Figure 1), although thecorrelation between I CO(1–0) and Σ SFR is not obvious,
as we have already shown in the preceding paper [3].
This result show that the star-forming activity is closely
associated with warm and dense gases that are traced
with the 12CO(J = 3–2) line, even in the scale of GMCs.
We also find that the GMCs with a high star-forming
activity tend to show a high value of R 3–2/1–0. Moreover,
we also observe a mass-dependent trend of R 3–2/1–0 for the
GMCs with a low star-forming activity (Figure 2). Fromthese results, we speculate that the R 3–2/1–0 values of the
GMCs with a low star-forming activity mainly depend

Figure 1: The surface density of SFR (Σ SFR) versus ICO(1–0) andI CO(3–2) at the TCO(1–0) peak position in each GMC. The
dashed lines indicate the sensitivity limits for each
CO line. Correlation coefficients are 0.22 and 0.68,
respectively.

050

I Scientific Highlights

on the dense gas fraction and not on the temperature, andtherefore, the dense gas fraction increases with the massof GMCs, at least in the GMCs with a low star-forming
activity.

Figure 2: GMC mass versus R 3–2/1–0. The area of the circles is set
proportionally to Σ SFR at the TCO(1–0) peak position ofeach GMC. The red circles represent GMCs with Σ SFR> 1 × 10−8 M pc−2, and the blue ones indicate those with
Σ SFR < 1 × 10−8 M pc−2. The dotted line indicates thecriterion of MH2 = 8.4 × 104 M. The black crosses andthe numbers next to them stand for the averaged R 3–2/1–0
values in each mass-bin, which are taken for GMCs withhigher and lower star-forming activity, respectively. The
numbers in the bracket are the numbers of the GMCs
used for averaging. For GMCs whose 12CO(J = 3–2)
emissions are not detected, R 3–2/1–0 is shown as the upper
limit, with an arrow whose length is the rms value of
R 3–2/1–0.

References[1] Onodera, S., et al.: 2012, PASJ, 64, 15.
[2] Tosaki, T., et al.: 2011, PASJ, 63, 1171.
[3] Onodera, S., et al.: 2010, ApJ, 722, L127.

The Origin and Maintenance of a Retrograde Exoplanet
NARITA, Norio1, TAKAHASHI, Yasuhiro, H.2/1, KUZUHARA, Masayuki2/1, HIRANO, Teruyuki2
SUENAGA, Takuya3, KANDORI, Ryo1, KUDO, Tomoyuki1, SATO, Bun'ei4, SUZUKI Ryuji1, IDA, Shigeru4
NAGASAWA, Makiko4, ABE Lyu5, BRANDNER, Wolfgang6, BRANDT, Timothy, D.7, CARSON, Joseph8
EGNER, Sebastian, E.1, FELDT, Markus6, GOTO, Miwa9, GRADY, Carol, A.10, GUYON, Olivier1
HASHIMOTO, Jun1, HAYANO, Yutaka1, HAYASHI, Masahiko1, HAYASHI, Saeko, S.1, HENNING, Thomas6
HODAPP, Klaus, W.11, ISHII, Miki1, IYE, Masanori1, JANSON, Markus7, KNAPP, Gillian, R.7
KUSAKABE, Nobuhiko1, KWON, Jungmi3, MATSUO, Taro12, MAYAMA Satoshi3, McELWAIN, Michael, W.10
MIYAMA, Shoken13, MORINO Jun-Ichi1, MORO-MARTIN, Amaya14, NISHIMURA, Tetsuo,1 PYO, Tae-Soo1
SERABYN Eugene15, SUTO, Hiroshi1, TAKAMI Michihiro16, TAKATO, Naruhisa1, TERADA, Hiroshi1
THALMANN, Christian17, TOMONO, Daigo1, TURNER, Edwin, L.7/18, WATANABE, Makoto19
WISNIEWSKI, John, P.20, YAMADA, Toru21, TAKAMI, Hideki1, USUDA, Tomonori1, TAMURA, Motohide1
1:NAOJ, 2: University of Tokyo, 3: Graduate University for Advanced Studies, 4: Tokyo Institute of Technology, 5: Université de Nice-Sophia
Antipolis, 6: Max Planck Institute for Astronomy, 7: Princeton University, 8: College of Charleston, 9: Ludwig-Maximilians-Universitét,
10: Goddard Space Flight Center, 11: University of Hawaii, 12: Kyoto University, 13: Hiroshima University, 14: Consejo Superior deInvestigaciones Científicas, 15: Jet Propulsion Laboratory, 16: Academia Sinica, 17: University of Amsterdam, 18: Kavli Institute for Physics
and Mathematics of the Universe, 19: Hokkaido University, 20: University of Oklahoma, 21: Tohoku University

We previously discovered the first evidence of a
retrograde orbit of an extrasolar planet, HAT-P-7b (Narita
et al. 2009) [1]. Although retrograde planets, which haveorbits that run counter to the spin of their central stars, areabsent in our Solar System, they occur in other planetarysystems in the Universe. However, astronomers andplanetary scientists did not know how such retrograde
planets formed.
Generally speaking, planetary orbits are considered
to be well aligned with the host star’s rotation, at least at
the initial stage. Thus in a retrograde planetary system, it
is expected that other bodies in the planetary system hadaltered the orbit of the retrograde planet.
We used the HiCIAO and HDS instruments of the
Subaru telescope to search for such other massive bodies
in the HAT-P-7 system. Consequently, we found a binary
low-mass stellar companion at over 1000 AU, and anothergiant planet at over 5 AU in this system.
Then, how did the retrograde orbit of the planet
develop? We consider that the existence of the companion
star (HAT-P-7B) and the newly confirmed outer planet(HAT-P-7c) are likely to play an important role informing and maintaining the retrograde orbit of the inner
planet (HAT-P-7b) via the Kozai mechanism, a longterm
process during which a more massive object has an effecton the orbit of another.
In the case of HAT-P-7b, we posited so-called “sequential
Kozai migration” as an explanation of this retrograde
planet. It suggests that the companion star (HAT-P- 7B)
first affected the orbit of the newly confirmed outerplanet (HAT-P-7c) through the Kozai mechanism, causing
it to tilt. When the orbit of that planet inclined enough,
HAT-P7c altered the orbit of the inner planet (HAT-P7b) through the Kozai mechanism, so that it became
retrograde. This sequential orbital evolution of the planet

is one of the scenarios that could explain the origin of
retrograde/tilted/eccentric planets.
We have demonstrated the importance of this kind offollow-up observations for retrograde planetary systems
to check for the presence of outer massive bodies, which
may play an important role in understanding the entire
picture of planetary migration. The findings provide
important clues for understanding the origin of a varietyof planetary systems, including those with highly tilted
and also eccentric orbits [2].

Figure 1: Artist's rendition of the HAT-P-7 system. We used theSubaru Telescope to discover the retrograde planet(nearest the central star), another giant planet (in theforeground), and a companion star (upper right) in thissystem.
References[1] Narita, N., et al.: 2009, PASJ, 61, L35.
[2] Narita, N., et al.: 2012, PASJ, 64, L7.

I Scientific Highlights051

3D Dissipation Mechanism in Fast Magnetic Reconnection
FUJIMOTO, Keizo(NAOJ)

Magnetic reconnection is a promising process
which provides efficient energy release in solar flaresand geomagnetospheric substorms. The process is also
considered be important in fusion devices because it
can disturb the plasma confinement due to the magnetic
field. The efficient energy release of the magnetic fieldrequires a locally intense electric resistivity. However,
the generation mechanism of the resistivity has beenpoorly understood in collisionless reconnection. The
difficulty in understanding the dissipation processes
is attributed to the nonlinear and multi-scale natureof magnetic reconnection. The dissipation takes place
in a microscopic region where the plasma kinetics
is significant, while it can have an impact on largescale processes in macroscopic region where the fluid
approximation is valid. On the other hand, large-scale
field line topology also affects the kinetic processes in
the microscopic region. Therefore, in order to reveal thedissipation mechanism in magnetic reconnection, it isnecessary to describe self-consistently both the kinetic
process in microscopic region and the fluid dynamics inmacroscopic region.
It has been demonstrated that 2D magnetic
reconnection is supported by an effective resistivity
termed the inertia resistivity which is caused dueto the electrons accelerated in a finite time near the
x-line. However, the in-situ observations in the geomagnetosphere and laboratory experiments have indicatedthat the current layer is not so thin as expected in the 2Dmodel, and have detected active electromagnetic (EM)waves, which implys the importance of the anomalous
dissipation (e.g., [1]).
The present study has investigated the 3D dissipation
mechanism in a fast magnetic reconnection by using
the large-scale particle-in-cell (PIC) simulations. The
PIC model in this study employs the adaptive meshrefinement (AMR) [2]. The ion-to-electron mass ratio is100. The number of the particles used reaches 1011 totally,
and the maximum spatial resolution is 4096 × 512 × 4096
= 1010 [3]. Figure 1 shows a 3D snapshot around thex-line during the fast reconnection. It is found that an EM
mode is excited around the x-line and kinks the electron
current layer. The linear analysis indicates that the mode
is a new-type shear mode excited due to the velocity
shear across the current layer rather than the classicaldrift mode driven by the ion-electron relative velocity.
Furthermore, it is confirmed that the mode is unstableeven for the realistic mass ratio.
Figure 2 shows the anomalous momentum transport ofthe electrons due to the EM turbulence. One can see that052

I Scientific Highlights

the anomalous transport due to the shear driven mode isdominant in the localized region around the x-line. Since
the reconnection electric field is Ey ≈ 0.1, the estimatedcontribution to the magnetic dissipation of the anomaloustransport is about 50 % in the fast magnetic reconnection.
In particular, it is found that the anomalous transport isenhanced in association with the plasmoid (flux rope)
formations.

Figure 1: 3D snapshot around the x-line during the fast magnetic
reconnection of an isosurface for |J|/en0VA = 0.4 coloredby Ey with the magnetic field lines in yellow curves and2D profiles of Jy.

Figure 2: Anomalous momentum transport of the electrons due→→to the EM turbulence δ ( neVe ) × δ B  / ne, where ·
indicates the average over y axis.

References[1] Zhou, M., et al.: 2009, J. Geophys. Res., 114, A02216.
[2] Fujimoto, K.: 2011, J. Comput. Phys., 230, 8508.
[3] Fujimoto, K., Sydora, R. D.: 2012, Phys. Rev. Lett., 109,
265004.

Power Spectral Analysis of the Magneto-Convection
on the Solar Surface with HINODE SOT				

KATSUKAWA, Yukio(NAOJ)

Interaction between the thermal convection andmagnetic fields creates structures over various spatial
scales, such as sunspots (104–105 km) and fine magnetic
flux tubes (~100 km). It is quite important to investigate
the transfer of kinetic and magnetic energies among
the convection and magnetic fields at various spatial
scales for understanding how the magnetic structures
are created on the solar surface. In order to quantify
it, we performed power spectral analysis of surface
temperatures, velocities, and magnetic fields, using
spectro-polarimetric data taken with the HINODE Solar
Optical Telescope (SOT). Because of the stable image
quality as well as accurate polarimetric measurements,
we could successfully obtain power spectra of the surface
convection at the spatial scale smaller than granules withenough reliability for the first time by characterizing
influence of the telescope’s angular resolution and noises.
The kinetic (temperatures’ and velocities’) power
spectra have a prominent peak at the granular scale (~1000
km, Fig. 1 top), which indicates injection of the kinetic
energy occurs at that scale. At the spatial scale smaller
than granules, the power spectra show power-law like
spectra whose power-law indices are −4 – −3. The spectra
are significantly steeper than the Kolmogorov’s −5/3 forisotropic turbulences. It has not been understood why theslope is so steep on the solar surface.
The magnetic power spectra are created in low
magnetic flux regions (Fig. 1 top) and high flux regions(Fig. 1 bottom), separately. In the low flux regions (< 10gauss), the magnetic spectra exhibit a peak at aroundthe granular scale (~800 km) and power-law like spectra
whose indices are about −1.3 at the sub-granular scale.
A MHD numerical simulation of the surface magnetoconvection suggests that small-scale magnetic fields are
created at the scale smaller than the HINODE resolution
by local dynamo action, and they have more impacts on
the overall magnetic energy budgets than the magnetic
fields resolved with HINODE. The power spectra basedon the Hinode observation imply, on the other hand,that magnetic energies coming from the granular-scale
structures are more important than the structures of theunresolved scale. The magnetic spectra are less steep than
the kinetic ones at the sub-granular scale, and the powerlaw indices differ by about 2, which can be interpreted
that magnetic structures are created by velocity shearof the surface convection. In the high flux regions (> 50
gauss), the power-law indices of the kinetic and magnetic
power spectra become similar. This is probably due to

OROZCO SUÁREZ, David(Instituto de Astrofsica de Canarias)

strong coupling of the convection and magnetic fields
at each spatial scale. Comparison with MHD numericalsimulations of the surface magneto-convection is
expected to provide deeper insights on how the magnetic
structures are created as a next step.

Figure 1: Kinetic and magnetic power spectra of the granularconvection on the solar surface derived with HINODE
SOT in low and high flux regions (top and bottom,
respectively).

Reference[1] Katsukawa, Y., Orozco Suárez, D.: 2012, ApJ, 758, 139.

I Scientific Highlights

053

Astrophysical Impact of New β-decay Half-lives
on r-process Nucleosynthesis [1]NISHIMURA, Nobuya(University of Basel)			

KAJINO, Toshitaka(NAOJ/University of Tokyo)

SUZUKI, Toshio(Nihon University)		

Rapid neutron capture process (r-process) is
responsible for the origin of approximately half of theelements heavier than iron. Despite of several decadesof theoretical studies and observational progress, theastrophysical sites for r-process nucleosynthesis are
unknown.
Physical conditions for the r-process are wellconstrained. It is evident that the r-process occurs via
a sequence of rapid neutron captures on neutron-richisotopes far from stability. The relative abundance of
r-process elements is then determined by the relative
β-decay rates along this r-process path, i.e., slower
β-decay lifetimes result in higher abundances.
In this context, it is of particular interest that β-decay
half-lives of 38 neutron-rich isotopes including 100Kr, 103–
105
Sr, 106–108Y, 108–110Zr, 111,112Nb, 112–115Mo, and 116,117Tc
have been measured at the recently commissioned
radioactive isotope beam factory (RIBF) facility at the
RIKEN Nishina Center [2]. Newly measured lifetimes are
an improvement on existing measurements and a numberof them were measured for the first time.
We performed nucleosynthesis calculations for ejecta
from the MHD supernova model [3] with the threedifferent reaction networks. These are extensions of thebasic network described in [3,4]. First, we adopt FRDM
theoretical rates [5] from the REACLIB compilation [6]as standard. The other two (RIBF and RIBF+) utilize thenew experimental β-decay half-lives and two versionsof the theoretical FRDM β-decay rates for the otherisotopes. The RIBF network replaces the FRDM rates
with the new measured ones where possible. The network(RIBF+) is based on the RIBF network and FRDM rates
with modified Q values for (n, γ) for A = 97–115 isotopes
based on the new suggested masses.
Figure 1 shows the final abundance distribution withthe solar system abundances [7]. The newly measured
β-decay rates in this mass region might shift the β-flow
equilibrium thereby filling in the low abundances nearA ~ 120. The abundances in the A = 110–120 region
however are only slightly enhanced. Although the
new rates provide a little assistance in enhancing theabundances near the valley, they do not alleviate thisproblem.
We note that the r-process ow moved farther awayfrom stability and proceeded faster in the RIBF+ networkin which the (n, γ) Q values were systematically enhanced054

I Scientific Highlights

MATHEWS, Grant J.

(University of Notre Dame)NISHIMURA, Shunji(RIKEN Nishina Center)

for isotopes with A = 104–115. This helped to fill in theabundances in the higher mass region with A ≥ 115. Thus,
it is important to measure the masses and/or neutron
separation energies in this region.
Furthermore, our results suggest that nucleosynthesisin the LEPP (light-element primary process) elementswith A ≤ 120 observed in some ultra-metal-poor stars [8],also is sensitive to the nuclear physics uncertainty fromβ-decay rates in this region. Hence, further studies onboth the nuclear physics and astrophysics of the synthesisof elements with A ~ 110–120 are warranted.

Figure 1: Total final abundance distributions of r-process elementsfrom the adopted MHD supernova model with observed
solar system abundances (black dots, taken from[7]). Red solid, green dotted, and blue dashed lines
correspond to results from using the FRDM (standard),
RIBF, and RIBF+ rates, respectively.

References[1] Nishimura, N., et al.: 2012, Phys. Rev. C, 85, 048801.
[2] Nishimura, S., et al.: 2011, Phys. Rev. Lett., 106, 052502.
[3] Nishimura, S., et al.: 2006, ApJ, 642, 410.
[4] Otsuki, K., Tagoshi, H., Kajino, T., Wanajo, S.: 2000, ApJ, 533,
424.
[5] Möller, P., et al.: 1995, ADNDT, 59, 185.
[6] Rauscher, T., Thielemann, F.-K.: 2000, ADNT, 75, 1.
[7] Arlandini, C., et al.: 1999, ApJ, 525, 886.
[8] Travaglio, C., et al.: 2004, ApJ, 601, 864.

Solution to Big-Bang Nucleosynthesis in Hybrid Axion Dark Matter Model						

KUSAKABE, Motohiko(University of Tokyo)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

The primordial 7Li abundance predicted in standard
big bang nucleosynthesis (BBN) model for the baryonto-photon number ratio η determined from the cosmic
microwave background observations is significantly morethan those observed in old halo stars [1,2]. Recently a
new solution to the lithium puzzle was proposed, which
is a mechanism for the cooling of photons in the epoch
between the end of BBN and the last photon scattering.
An axion, one of candidates for the dark matter could
form a Bose-Einstein condensate (BEC) and may havecooled the photons in the epoch [3]. The baryon-tophoton ratio would then be smaller in BBN epoch (η =4.6 × 10−10 [3]) than that measured by WMAP (η = 6.2 ×
10−10 [4]). In the cooling model, however, the deuterium(D) abundance and the effective number of neutrinos
are too high although the 7Li abundance agrees withobservations.
Nonthermal photons can be generated throughelectromagnetic energy injections by the radiative decayof long-lived particles after the BBN epoch. Longlived particles are motivated by particle physics beyond
the standard model. These nonthermal photons canphotodisintegrate background light elements. Effects ofenergy injection depend on two parameters. One is ζ X= (n0X / n0γ)E γ0 where (n0X / n0γ) is the number ratio of the
decaying particle X and the background radiation before
the decay of X, and E γ0 is the energy of photon emitted at
the radiative decay. The other is τ X, the lifetime of X.
We calculated BBN in a hybrid axion and decaying
exotic relic particle model in which the axion cools thephotons and the particle produces nonthermal photons
to eliminate the high D abundance in the original axion
BEC model. We compared results with observational
constraints on primordial nuclear abundances.
We also utilize a limit on the sum of primordial
abundances of D and 3He taken from an observational
abundance for the protosolar cloud, i.e., (D+3He)/H=(3.6±0.5)×10 −5 [5]. This abundance can be regarded as
constant at least within the standard cosmology since it is
not affected by stellar activities significantly despite aneffect of D burning into 3He via 2H(p, γ)3He would exist[6]. We thus showed that the constraint on (D+3He)/H
abundance excludes the original axion BEC model.
We found a narrow parameter region in whichcalculated abundances of all nuclides including D and
7Li are simultaneously in ranges of adopted observational
constraints. We conclude that the present model
eliminates the main drawback of the original axion BEC

BALANTEKIN, A. B.

(University of Wisconsin, Madison/NAOJ)PEHLIVAN, Y.

(Mimar Sinan Fine Arts University/NAOJ)

model by reducing primordial D abundance via 2H(γ, n)1H
reaction, where γ’s are nonthermal photons. We note thatthe decaying X particle model with the WMAP η value
cannot resolve the 7Li problem by itself [7].
Figure 1 shows a result of a BBN calculation in
our hybrid model [8]. The small difference at T9 >~ 0.06
observed between solid and dashed lines is caused by−3
difference between initial η values. At 0.06 >~ T9 >~ 7×10 ,2
1effects of H(γ, n) H are seen in the decrease of D and
the increase of n abundances. We find a slight decrease in
7
Be abundance caused through reactions 7Be(γ, 3He)4He,
7Be(γ, p)6Li, and 7Be(γ, 2pn)4He. The second reaction−3
increases the 6Li abundance. Finally, at T9 <~ 7×10 ,when the abundance of long-lived X particle is alreadyless than 3 % of the initial abundance, effect of 4He
photodisintegration is to increase 3H and n abundances.

Figure 1: Mass fractions of H and 4He (Xp and Yp, respectively)
and number ratios of other nuclides relative to H asa function of T 9 ≡ T / (10 9 K). Solid lines show theabundances in the hybrid model with the parameters(τX, ζ X) = (106 s, 2 × 10−10 GeV) which predict primordial
abundances consistent with all observations. The
dashed lines show the standard BBN prediction. This isreprinted from [8].

Reference[1] Spite, F., Spite, M.: 1982, A&A, 115, 357.
[2] Aoki, W., et al.: 2009, ApJ, 698, 1803.
[3] Erken, O., et al.: 2012, Phys. Rev. Lett., 108, 061304.
[4] Larson, D., et al.: 2011, ApJS, 192, 16.
[5] Geiss, J, Gloeckler, G.: 1998, Space Sci. Rev., 84, 239.
[6] Steigman, G., Tosi, M.: 1995, ApJ, 453, 173.
[7] Kusakabe, M., et al.: 2006, Phys. Rev. D, 74, 023526.
[8] Kusakabe, M., et al.: 2013, Phys. Lett. B, 718, 704.

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055

Supernova-, Solar- and Reactor-Neutrino Detection and Precise
Theoretical Calculation of Neutrino Capture Cross Section on 13C [1]
SUZUKI, Toshio(Nihon University/NAOJ)

BALANTEKIN, Akif B.

(University of Wisconsin/NAOJ)

The natural abundance of 13C is 1.07 % in carbon
isotopes. As the threshold for charged-current reactions
on 12C is slightly more than 13 MeV, 13C is an attractive
target to detect very low-energy neutrinos. The
background is from supernova and 8B solar neutrinos. In
scintillator-based experiments, 13C may be useful to sortout uxes of various avors from supernovae.
A new shell-model Hamiltonian for p-shell nuclei,
SFO [2], is used to evaluate neutrino cross sections on
13
C. With this new Hamiltonian the magnetic propertiesof p-shell nuclei are considerably improved compared
to conventional Hamiltonians such as Cohen-Kurath(CK) Hamiltonian [3]. Here, we study neutrino-nucleus
reactions, which are induced mainly by excitationsof Gamow-Teller and spin-dipole states as well as
isobaric analog states. The SFO Hamiltonian, which
was constructed for use in the p-sd shell configurations
including up to 2–3 ħω excitations, can describe well
the magnetic moments of p-shell nuclei systematicallyand Gamow-Teller (GT) transitions in 12C and 14C witha small quenching for spin g-factor and axial-vector
coupling constant: i.e., g Aeff/gA = g eff
s /gs = 0.95. In caseof CK, where configuration space is restricted to within
p-shell, a large quenching factor of g Aeff/gA = 0.69 is used.
The exclusive cross sections, 12C (ν e, e − ) 12N (1 +g.s.),obtained by shell-model calculations with SFO and CK
are are shown in Fig. 1 together with the experimental
values. The SFO is found to reproduce the experimental
values very well. The cross sections for SFO areenhanced compared with those for CK.
The charged-current cross sections leading to various
states in the daughter 13N and the neutral-current crosssections leading to various states in the daughter 13C are
obtained with the use of SFO [1]. Simple polynomial
fits to those cross sections are also provided for quick
estimates of the reaction rates (see Ref. [1]). In Fig. 2,
cross sections induced by Gamow-Teller and isobaric
analog transitions are compared between SFO and CK.
The SFO give larger cross sections compared with CK [4].
One possible application of these cross sections could
be to search for electron neutrino appearance in thereactor antineutrino ux and determine the mass hierarchy[5], being free from supernova and solar neutrino
background. Ideally one would like to be as close to thereactors as possible much like experiments searching forthe neutrino magnetic moment. However, in this casereactor neutrino ux uncertainties can be sizable. This isalso true for the energy-integrated count rate, which is
between 5.2 and 13.0 MeV. One possible way to reduce056

I Scientific Highlights

KAJINO, Toshitaka(NAOJ/University of Tokyo)

such uncertainties is to use much more abundant electron
antineutrinos to estimate the reactor flux. This can beachieved using neutral-current scattering.

Figure 1: The exclusive cross sections for 12C (νe, e−) 12N (1+g.s.) inshell-model calculations with SFO and CK.

Figure 2: Calculated charged-current cross sections for 13C (νe, e−)13N to the ground (1/2−) and 3/2− (3.502 MeV) states
and neutral-current cross sections for 13C (ν̄e, ν̄e’)13C to
3/2− (3.685 MeV) state with SFO. Calculations with CK
are indicated by circles anf triangles.
References[1] Suzuki, T., Balantekin, A. B., Kajino, T.: 2013, Phys. Rev. C,
86, 015502.
[2] Suzuki, T., et al.: 2003, Phys. Rev. C, 67, 044302.
[3] Cohen, S., et al.: 1965, Nucl. Phys., 73, 1.
[4] Fukugita, M., et al.: 1990, Phys. Rev. C, 41, 1359.
[5] Mathews, G. J., et al.: 2012, Phys. Rev. D, 85, 105023.

Subaru Imaging of Asymmetric Featuresin a Transitional Disk in Upper Scorpius
MAYAMA, S.

(The Graduate University for Advanced Studies)

MUTO, T.

(Kogakuin University)		

KUSAKABE, N., KUDO, T., SUTO, H.

		KUZUHARA, M.
(TITECH)

FUKAGAWA, M.
(Osaka University)

HASHIMOTO, J., WISNIEWSKI, J. P.
(University of Oklahoma)

We report high-resolution (0.07 arcsec) near-infrared
polarized intensity images of the circumstellar disk
around the star 2MASS J16042165-2130284 obtainedwith HiCIAO mounted on the Subaru 8.2 m telescope[1]. We present our H-band data, which clearly exhibits aresolved, face-on disk with a large inner hole for the firsttime at infrared wavelengths (Figure 1). We detect thecentrosymmetric polarization pattern in the circumstellar
material as has been observed in other disks. Ellipticalfitting gives the semimajor axis, semiminor axis, andposition angle of the disk as 63 AU, 62 AU, and −14°,
respectively. The disk is asymmetric, with one dip locatedat position angles of ~85°. Our observed disk size agrees
well with a previous study of dust and CO emission at
submm wavelength with SMA. Hence, the near-infrared
light is interpreted as scattered light reflected from theinner edge of the disk. We discuss the possibility that theasymmetric features which we have observed may berelated to the existence of unseen bodies within the disk.

(Ibaraki University)

TAKAHASHI, Y., TAMURA, M.

				(NAOJ)				
		

TSUKAGOSHI, T., MOMOSE, M.

(University of Tokyo/NAOJ)

DONG, R.

TAKAMI, M.

FOLLETTE, K.

SEEDS team(Princeton University)(The University of Arizona)(ASIAA)

Figure 1: H-band HiCIAO images of J1604-2130. The saturated
central area (radius = 0 .″2) is masked in black. (a): thePI image of J1604-2130. The field of view (FOV) is 2.″9× 2 .″9. The unit of the color bar is mJy/arcsec2. The light
blue ellipse and plus sign are the best fit result of ourelliptical disk model and the ellipse center. (b): H-bandpolarization vectors super-posed on the PI image. The
vector directions indicate angles of polarization. The
plotted vectors are based on 7 [pixel] × 7 [pixel] binningcorresponding to the spatial resolution. The FOV is 2 .″0× 2 .″ 0. The vector’s lengths are arbirtrary. (c): Red(r = 145 AU), brown (r = 63 AU), and yellow (r = 33
AU) circles superimposed on the PI image. (d): SMA
880 µm continuum map [2] superimposed on the PI
image. White color contours indicate 2, 3, 6, 9, and 12σ
intensity (1σ = 1.3 mJy/beam). The ~0 .″5 × 0 .″3 beam of
SMA is shown in the bottom right.

Reference[1] Mayama, S., et al.: 2012, ApJ, 760, L26.
[2] Mathews, G. J., et al.: 2012, ApJ, 753, 59.

I Scientific Highlights

057

The Detection of C60 in the Well-Characterized Planetary Nebula M1-11
OTSUKA, Masaaki(ASIAA/STScI)		

			

KEMPER, Francisca(ASIAA)MEIXNER, Margaret

We performed multiwavelength observations of
the planetary nebula (PN) M1-11 and we obtained its
elemental abundances, dust mass, and the evolutionary
status of the central star.
Using Subaru/HDS, OAO/ISLE, and Spitzer/IRS
spectra, we detected over 220 emission lines and we
detemined the eleven elemental abundances. Our
determined elemental abundances are in excellent
agreement with a nucleosynthesis model for initially 1.5
M stars with the metallicity Z = 0.004.
The AKARI/IRC, VLT/VISIR, and Spitzer/IRS spectra
show features due to carbon-rich dust, such as the 3.3,
8.6, and 11.3 μm features due to polycyclic aromatichydrocarbons (PAHs), a smooth continuum attributable toamorphous carbon, and the broad 11.5 and 30 μm featuresoften ascribed to SiC and MgS, respectively. We also
reported the presence of an unidentified broad feature
at 16–22 μm, similar to the feature found in Magellanic
Cloud PNe with either C-rich or O-rich gas-phasecompositions. We identified for the first time in M1-11
spectral lines at 8.5 (blended with PAH), 17.3, and 18.9
μm that we attribute to the C60 fullerene (Fig. 1). Using
the detected C60 lines, we determined the C60 mass (2.75
×10−8 M) and temperature (399 K) in M1-11.
Using the radiative transfer code Cloudy, combinedwith a modified blackbody, we have fitted the ~0.1–90
μm spectral energy distribution (SED) and determined
physical properties of the central star and the ionizedgas and dust masses (Fig. 2). Our chemical abundance
analysis and SED model suggest that M1-11 is perhaps
a very young C-rich PN (~1000 yrs), and that it evolved
from a ~1.5 M star.
The obtained values in M1-11, namely, the C60 massand temperature, the elemental composition of the gas
in the nebula, the mass of the progenitor star, and theevolutionary status, are very similar to those seen in otherC60 containing PNe.

058

I Scientific Highlights

SARGENT, Benjamin A.
(RIT/STScI)

TAJITSU, Akito, YANAGISAWA, Ken’shi(STScI)				

Reference[1] Otsuka, M., et al.: 2013, ApJ, 764, 78.

HYUNG, Siek

(Chungbuk National University)(NAOJ)

Figure 1: Detection of C60 bands in M1-11. Arrows indicate thepositions of the 17.3 μm and 18.9 μm C60 bands.

Figure 2: The fitted SED from the Cloudy modeling (dots) and themodified blackbody fitting (long dash) and the resultant
SED (thick black line). The gray circles and lines are
the observed data. In the Cloudy model, we considered
PAHs, amorphous carbon (AC), and SiC. The modified
blackbody fitting is performed for MgS only. The closeup feature of the observed and fitted SEDs around 10–
40 μm are presented in the inner box.

Exploring the Neutrino Mass Hierarchy Probability
with Meteoritic Supernova Material,ν-Process Nucleosynthesis, and θ13 Mixing [1]MATHEWS, Grant J.

(University of Notre Dame)				

KAJINO, Toshitaka(NAOJ/University of Tokyo)		

FUJIYA, Wataru(University of Tokyo)

Oscillations in the three-neutrino flavor mixing
scenario are described by three angles θ12, θ23, and θ13
plus a CP-violating phase δCP. Solar, atmospheric, andreactor neutrino oscillation measurements have provided
information on the neutrino mass differences, i.e Δm 212≡ |m21 – m22| = 0.000079 eV2 and Δm213 ≈ |Δm223| ≈ 2.4 ×
10 −3 eV 2. These measurements, however, are unable
to determine the mass hierarchy, i.e. whether Δm223 >0 (normal) or Δm223 < 0 (inverted) is the correct order.
Also, solar, atmospheric and reactor neutrino oscillation
experiments have determined θ12 and θ23 to reasonableprecision. However, only recently have measurementsof θ13 become available. The best current measurements[with δ CP = 0 and θ 23 = �/4] is from the the Daya
Bay experiment that has reported sin 2 2θ 13 = 0.092 ±0.016(stat) ± 0.005(syst) [2], This is also consistent withthe previously reported lower limit and upper limits to θ13from the T2K collaboration [2] of 0.03(0.04) < sin2 2θ13 <0.28(0.34). These results, however, do not yet determine
whether the normal or inverted hierarchy is the correct
ordering of mass eigenstates.
In this context it is noteworthy that the synthesisof ν-process elements 7 Li and 11 B in core collapse
supernovae is sensitive to the neutrino mass hierarchyand θ13. Previous studies [3] pointed out that for a finite
mixing angle θ13 > 0.001 the relative synthesis of 7Li and
11B in the ν-process is sensitive to the mass hierarchy.
Since θ13 > 0.001 is indeed implied by the Daya Bay+RENO + Double Chooz results to better than the 5σ C.L.,
we could reconsider the supernova ν-process as a means
to constrain the neutrino mass hierarchy. The width of theshaded region of Figure 1 shows the current constraints
on the θ13 mixing compared with the extended results of
7Li and 11B nucleosynthesis from [3].
Moreover, there has also been a recent possible
discovery [4] of ν-process 7Li and 11B supernova materialin SiC X grains from the Murchison meteorite. The topof the shaded region on Figure 1 shows the 1σ upper
limit to the 7Li/11B ratio from that study. The goal ofthis paper was to examine the likelihood of one neutrinomass hierarchy over another in a Bayesian statisticalanalysis that took proper account of all of the supernova
model uncertainties as well as the measurement
uncertainties of the SiC X grains and the θ13 limits. In
our five dimensional Bayesian analysis we found that

AOKI, Wako
(NAOJ)

PITTS, J. B.

(University of Notre Dame)

there is a preference for an inverted hierarchy at thelevel of 74 % / 26 % compared to a prior expectation of
50 %/50 %.

Figure 1: Produced 7Li/11B abundance [3] as a function of mixing
angle for both a normal and inverted neutrino mass
hierarchy. This ratio varies in models with different
neutrino temperatures in the range indicated by the lower
and upper solid lines. The width of the blue shaded
region indicates the 2σ confidence limits to sin2 (2θ13)from the Daya Bay result [2]. The red shaded region is
the 1σ upper limit on the observed ν-process 7Li/11B ratio
as deduced here from the SiC X grains. This is reprinted
from [1].

References[1] Mathews, G. J., et al.: 2012, Phys. Rev. D, 85, 105023.
[2] An, F. P., et al.: (Daya Bay Collaboration) archive: 1203.1669[hep-ex]; Abe, K., et al.: 2011, Phys. Rev. Lett., 107, 041801.
[3] Yoshida, T., et al.: 2008, ApJ, 686, 448.
[4] Fujiya, W., Hoppe, P., Ott, U.: 2011, ApJ, 730, L7.

I Scientific Highlights

059

Substellar-Mass Condensations in Prestellar Cores
TAKAKURA, Shigehisa(NAOJ/Joint-ALMA Observatory)

Jy/beam
0.4(a) SM1

1000 AUa3

23′50″

0.3

a2

0.2

a1

24′ 0″

26′50″DEC (J2000)

We present combined Submillimeter-Array (SMA) +single-dish images of the (sub)millimeter dust continuum
emission toward two prestellar cores SM1 and B2-N5 in
the nearest star cluster forming region, ρ Ophiuchus. Our
combined images indicate that SM1 and B2–N5 consistof three and four condensations, respectively, with massesof 10−2–10−1 M and sizes of a few hundred AU. The
individual condensations have mean densities of 10 8–109 cm−3 and the masses are comparable to or larger thanthe critical Bonner-Ebert mass, indicating that the selfgravity plays an important role in the dynamical evolutionof the condensations. The coalescence timescale of thesecondensations is estimated to be about 104 yr, which iscomparable to the local gravitational collapse timescale,suggesting that merging of the condensations, insteadof accretion, plays an essential role in the star formation
process.
These results challenge the standard theory of starformation, where a single, rather featureless prestellar
core collapses to form at most a couple of condensations,each of which potentially evolves into a protostar that issurrounded by a rotating disk where planets are created.

KAWABE, Ryohei(ASIAA)

0.1-24°24′10″26m28s16h26m27s
RA (J2000)

5000 AU
SM1N

24′10″
24′40″-24°25′10″

SM2

SM1

3
2

VLA16231

026m34s 2 26m30s 226m26s 16h26m22s
RA (J2000)

b4

14
12

27′ 0″

10
8

b3

27′10″

b1

6
4

27m29sRA (J2000)

16h27m28s

Jy/beam25′ (d) Oph B2

5
423′40″

1000 AUb2

27m30sJy/beam
622′40″ (c) Oph A
23′10″ S1

0.0

mJy/beam
16(b) B2N5-24 27′20″

DEC (J2000)(NAOJ)			

DEC (J2000)

NAKAMURA, Fumitaka

DEC (J2000)

		

5000 AU

1.5

EL32

26′

1.0
27′

-24°28′

B2N4
EL33

0.5

0.0
27m35s 27m30s 27m25s 16h27m20s
RA (J2000)

Figure 1: (a) Combined SCUBA and SMA image toward SM1.
The contour levels are −20, 60, 80, 100, 130, 160,
and 320 mJy/beam. The cross is the position of SM1
identified by Motte et al. (1998). The alphabets designate
the identified condensations. (b) Combined AzTEC/
ASTE and SMA image toward B2–N5. The contour
levels are −3, 8, 10, 12, 14, and 16 mJy/beam. The crossis the position of B2-N5 identified by Friesen et al.
(2010). (c) the SCUBA 850 μm continuum image toward
the Oph A region (Johnstone 2000). The white and black
filled circles are the B star, S1, and the prototypicalClass 0 YSO, VLA 1623, respectively. The positions ofsome submillimeter continuum sources are indicated by
the squares (Motte et al. 1998). (d) the AzTEC/ASTE 1.1
mm continuum image toward the Oph B2 region. The
black filled circles are the positions of Class I YSOs,
EL32 and EL33. In panels (a) and (b), the synthesised
beams are shown in the lower right of the panels.

Reference[1] Nakamura, F., Takakuwa, S., Kawabe, R.: 2012, ApJ, 758, 25.

060

I Scientific Highlights

Early Galactic Chemical Evolution and r-Process Nucleosynthesis
in Black-Hole Forming Supernovae [1]				

AOKI, W., SUDA, T.
(NAOJ)

BOYD, R. N.

(University of California, Lawrence Livermore National Laboratory)

Extremely metal-poor (EMP) halo stars are early
generations of stars whose elemental abundances reflect
the interstellar gas compositions of the early Galaxy.
Compilations of abundances of neutron-capture elements
in EMP stars indicate that Sr and Ba show a clear cutoff
in the distribution of [Sr/Ba] at [Fe/H] ~ −3.6 and an
upper bound as a function of [Fe/H] as well as a lower
bound at [Sr/Ba] ~ −0.5 as shown in the upper Fig. 1 [2].
Our recent model [3] was developed in which thecollapses of type II supernovae (SNe) are found toreproduce many of these features seen in the data. We
point out that the cutoff at [Fe/H] = −3.6 for [Sr/Ba] > 0.0
data can be explained by the truncated r-process, that is,by the collapses to black holes over a fairly wide mass
range of progenitor stars. Furthermore, the results of our
GCE calculations can predict the upper bound in [Sr/Ba]
in these data. Effects of turbulence in an explosive site
have also been simulated, and are found to be importantin explaining the large scatter observed in the [Sr/Ba]
data [1]. See the lower Fig. 1.
A fascinating aspect of this work is the possibility thatobserved minima in [Ba/Fe], [Sr/Fe], and [Sr/Ba] may
be directly related to the stiffness of the nuclear EOS.
The lower limit of [Ba/Fe] as a function of metallicity
predicted in our model can be reproduced in a GCE
model assuming a contribution to r-process elementsfrom black holes produced in fallback SNe. The softer theequation of state (EOS), the lower the calculated [Ba/Fe]
as a function of [Fe/H]. Thus the observed lower limit in[Ba/Fe] as a function of metallicity appears to constrain
the lower limit of the stiffness of the EOS.
While astronomical observations of neutron starmasses are able to predict a lower limit of the stiffnessof the EOS, this model suggests a new method ofdetermining the upper limit [4].

KAJINO, Toshitaka(NAOJ/University of Tokyo)

FAMIANO, M. A.

(Western Michigan University/NAOJ)

Figure 1: Upper: The calculated results for [Sr/Ba] assuming a
truncated black-hole forming r-process. The red dashedline corresponds to a GCE model without production
in a truncated r-process, while the blue dashed line
corresponds to a GCE model with a primary production
from this r-process for all stars with M ≥ 20 M. Lower:
The GCE results for single-site truncated rprocess
production for turbulent ejection of specific shells
assuming only those shells are ejected. From shell 0
toward shell 14, each colored line indicates calculated[Sr/Ba] with the mixing for deeper shell.

References[1] Aoki, W., et al.: 2013, ApJ, 766, L13.
[2] Aoki, W., et al.: 2005, ApJ, 623, 611.
[3] Boyd, R. N., et al.: 2011, ApJ, 744, L14.
[4] Famiano, M. A., et al.: 2013, in preparation.

I Scientific Highlights

061

High-Lying Excited States in Gamow Teller Strengthand Their Roles on Neutrino Reactions
			CHEOUN, Myung-Ki, HA, Eunja(Soongsil University)			

The Gamow Teller (GT) transition strengths deduced
from charge exchange reactions (CEXRs) are very
helpful for understanding the nuclear reaction induced by
the solar neutrino. For further study of supernovae (SNe)neutrinos in the cosmos, one needs to study high-lying
GT states around a few tens of MeV region as well asother multipole transitions because of the high energy tailin the neutrino spectra emitted from the neutrino sphere.
In this report, we address the importance of the high-lying
GT excited states, which data now become available fromvarious CEXR experiments. For example, the GT(±)
strength up to 70 MeV are successfully extracted by90
Zr (n, p) and 90Zr (p, n) reactions [1].
Our discussions are extended to investigate rolesof the high-lying states beyond a few low-lying states
known in the old experiment on the reaction induced by
SNe neutrinos particularly on 40Ar target. The nucleus
was originally exploited to identify the solar neutrino
emitted in the pp-chain, and now lots of applications formore energetic neutrino detection are under progress.
Expected large difference between the cross sectionsof νe and ν̄e reactions on 40Ar, which difference were
anticipated because of the large Q value in the ν̄e reaction,is significantly diminished compared to previous results.
Our calculations are carried out by the Quasiparticle
Random Phase Approximation (QRPA), which takes
the neutron-proton pairing into account to the standard
proton-neutron QRPA (pnQRPA) where only protonproton and neutron-neutron pairing correlations are
considered.
First, we compare our theoretical results to recent
experimental GT( ) strength distribution data [1] whichwere deduced by the multipole decomposition (MD)technique from 90Zr (p, n) at the bombarding energy 295
MeV and 90Zr (n, p) at 293 MeV reactions. In such a highenergy region, the ΔL = 0 contribution from the isovector
spin monopole (IVSM) can be included around 35 MeV
region in the GT strength. By extracting ΔL = 0 IVSM
contribution with the MD technique, they succeed toobtain the ISR value about 90 %.
In Fig. 1, we show the GT strength distributions andtheir running sums by the the QRPA. The GT strengths
are clearly redistributed by the np pairing in the QRPA.
If we compare to the experimental data [1], two peak
positions around 3(9) and 10(16) MeV regions w.r.t 90Nb
(90Zr) are well reproduced in the QRPA. This result isalso consistent with previous results by the Dressed RPA.
Also the quenching factor data related to total running

KAJINO, Toshitaka(NAOJ/University of Tokyo)

sums, Q = (S− − S+)/(3(N − Z)) = 0.90 ± 0.05 or 0.88 ± 0.06
[1], are almost reproduced by our results 0.96, althoughstrength shapes are a bit different from the experimental
data. Since only the GT states are considered in this work,
our results beyond 20 MeV are not presented in Fig. 1.
Detailed discussion are done at Ref. [2].

±062

I Scientific Highlights

Figure 1: GT(−) strength distributions and their running sums for
90Zr by the QRPA. Experimental data [1] are denoted
as red points by subtracting the experimental Q value
between 90Zr and 90Nb.

References[1] Cheoun, M.-K., Ha, E., Kajino, T.: 2012, Eur. Phys. J., 48, 137.
[2] Yako, K., et. al.: 2005, Phys. Lett. B, 615, 193.

Neutrino Induced Reactions Related to the ν-Process Nucleosynthesisof 92Nb and 98Tc [1]				

CHEOUN, Myung-Ki, HA, Eunja(Soongsil University)

HAYAKAWA, T.

(Japan Atomic Energy Agency)

MATHEWS, Grant J.

(University of Notre Dame)		

The neutrino (ν) process involves ν-induced reactions
on various nuclei during core collapse supernovae (SNe).
Huge numbers of neutrinos are emitted from a protoneutron star in early phase of the SN. Most neutrinos
escape into the space, but a small fraction of neutrinos
transfer their energy to materials in outer layer of starby neutrino-nucleus interactions. This process has been
proposed as the origin of some rare isotopes of light andheavy elements.
Among the many heavy elements, only the two
isotopes 138La and 180Ta are currently thought to besynthesized primarily by the ν-process [1]. These two
isotopes have similar features: they cannot be producedby either β +, EC, or β − decays because they are shieldedagainst these decays.
In principle, any nuclide can be synthesized by the
ν-process in SN explosions. The produced abundances,
however, are usually negligibly small because of the
weak interaction. Thus, the ν-process can only play adominant role in the case of very rare isotopes that cannot
be produced by other means.
In a recent work [2], we pointed out that the nuclear
chart around 92Nb and 98Tc is quite similar to that of 138La
and 180Ta. Although both nuclei are unstable, their halflives are long enough to be observed on stellar surfaces
or to be incorporated into meteorites.
The isotopic abundance ratio of 92Nb/93Nb is known
to be ~ 10−3–10−5. This is comparable to the isotopic
rations for 138La/139La and 180Ta/181Ta. An evidence of theextinct unstable isotopes of Tc has been investigated, but
it has not been found yet. This suggests the abundance of
98Tc is small compared with a detection limit. Therefore,
it has been proposed that the two nuclei 92Nb and 98Tc
may have a ν-process origin.
The nuclear structure of 92 Nb and 98 Tc are key
ingredients for this calculation. Our scheme for describing
such excited states makes use of the standard quasiparticle random phase approximation (QRPA). For the
NC reactions, we generate the ground and excited statesof the odd-even target nuclei, 93Nb and 99Ru, by applying
the quasi-particle operators to the even-even nuclei, 92Zr
and 98Ru, which are treated as the BCS ground state.
In table 1, we tabulated main relevant neutrino-induced
reactions and averaged cross sections for the typical(averaged) neutrino energy given by the ν temperatureused in our calculations of nucleosynthesis [2].

CHIBA, Satoshi(Tokyo Institute of Technology)

NAKAMURA, Ko, KAJINO, Toshitaka(NAOJ/University of Tokyo)< Ek > [MeV]

T [MeV]<σ>

98Mo(ν , e−)98Tc
e

10.08

3.2

7.77

98Mo(ν , e−p)97Mo
e

10.08

3.2

1.90

98Mo(ν , e−n)97Tc
e

10.08

3.2

0.09

99Ru( ν̄ , ν̄′ )99Ru
µ µ

18.90

6.0

78.5

99Ru( ν̄ , ν̄′ n)98Ru
µ µ

18.90

6.0

14.6

99Ru( ν̄ , ν̄′ p)98Tc
µ µ

18.90

6.0

1.70

99Ru( ν̄ , ν̄′ )99Ru
e e

15.75

5.0

52.1

99Ru( ν̄ , ν̄′ n)98Ru
e e

15.75

5.0

10.5

99Ru( ν̄ , ν̄′ p)98Tc
e e

15.75

5.0

0.92

92Zr(ν , e−)92Nb
e

10.08

3.2

8.92

92Zr(ν , e−p)91Zr
e

10.08

3.2

2.32

92Zr(ν , e−n)91Nb
e

10.08

3.2

0.42

Reactions93Nb( ν̄ , ν̄′ )93Nb
µ µ

18.90

6.0

46.8

93Nb( ν̄ , ν̄′ n)92Zr
µ µ

18.90

6.0

1.04

93Nb( ν̄ , ν̄′ p)92Nb
µ µ

18.90

6.0

4.90

93Nb(ν̄ , ν̄′ )93Nb
e e

15.75

5.0

30.0

93Nb(ν̄ , ν̄′ n)92Zr
e e

15.75

5.0

0.60

93Nb(ν̄ , ν̄′ p)92Nb
e e

15.75

5.0

3.92

Table 1: Averaged cross sections in units of 10−42 cm2 for 98Mo
via CC and 99Ru via NC, and 92Zr via CC and 93Nb via
NC with the particle emission.

References[1] Hayakawa, T. et al.: 2010, Phys. Rev. C, 81, 052801(R).
[2] Cheoun, M.-K., et al.: 2012, Phys. Rev. C, 85, 065807.

I Scientific Highlights

063

Pulsar Kick Induced by Asymmetric Emission of Supernova Neutrinos [1]MARUYAMA, Tomoyuki(Nihon University)

		

YASUTAKE, Nobutoshi(Chiba Institute of Technology)

CHEOUN, Myung-Ki(Soongsil University)

HIDAKA, Jun

MATHEWS, Grant J.

(University of Notre Dame)

We studied the supernova neutrino scattering andabsorption processes in strongly magnetized protoneutron stars at finite temperature and density. We useda fully relativistic mean field theory [2] for the hadronic
sector of the equation of state including hyperons. We
solved the Dirac equations for all constituent particles,p, n, Λ, e, and ν, for a poloidal magnetic field with
B ~ 1017 G. We then applied the solutions to obtain aquantitative estimate of the asymmetry that emerges fromthe neutrino-baryon collision processes. We included
the effects of distortion of the Fermi spheres madeby magnetic field that implies asymmetric neutrino
scattering and absorption cross-sections.
We found that the differential neutrino scatteringcross sections are slightly enhanced in the arctic direction
parallel to the poloidal magnetic field B in both caseswith and without Λ’s (Fig. 1a, c), while the differential
absorption cross-sections are suppressed (Fig. 1b, d).
The differential cross-sections were integrated overthe momenta of the final electrons for absorption, andover the momenta of initial neutrinos for the scattering,
respectively. Quantitatively, when B = 2 × 1017 G, thereduction for the absorption process results in about 2 %,and the enhancement for the scattering process about 1 %in the forward direction along the direction of B.
Using these cross-sections, we calculated the neutrino
mean-free-paths (MFPs), and then applied to a calculationof pulsar-kicks in core-collapse supernovae. We solved
the Boltzmann equation using a one-dimensional
attenuation method. Our estimated pulsar-kick velocities
are vkick = 610 km s−1 or 580 km s−1 with or without Λ’s,at T = 20 MeV. These values are in reasonable agreementwith the observed average pulsar-kick velocity of vkick =400 km s−1.
Realistic 3D simulation [3] of rotational magnetized
proto-neutron star suggests that not only poloidal but
toroidal magnetic fields are induced. We currently
study the effect of of neutrino-asymmetry in spin-down
phenomena of the proto-neutron star [4].

(NAOJ)

KAJINO, Toshitaka(NAOJ/University of Tokyo)

RYU, Chung-Yeol(Soongsil University)

Figure 1: Effects of magnetic fields on the differential crosssections dσ = dΩ = A for neutrino scattering νe → νe (aand c), and for neutrino absorption νe → e− (b and d).
Each line is for the different case as indicated.

Figure 1: Upper panels show the neutrino MFP for scattering (a)and absorption (c) without magnetic field. Lower panels(b) and (d) show the magnetic contribution to the MFP
for scattering (b) and absorption (d). Each line is for thedifferent case as indicated.

References[1] Maruyama, T., et al.: 2012, Phys. Rev. D, 86, 123003.
[2] Maruyama, T., et al.: 2011, Phys. Rev. D, 83, 081303(R).
[3] Takiwaki, T., Katake, K., Sato, K.: 2009, ApJ, 691, 1360.:
Kuroda, T., Umeda, H.: 2010, ApJS, 191, 439.
[4] Maruyama, T., et al.: 2013, submitted.

064

I Scientific Highlights

II Publications, Presentations
1. Refereed Publications
Abramowski, A., et al. including Kino, M., Nagai, H.: 2012, The
2010 Very High Energy γ-Ray Flare and 10 Years of Multiwavelength Observations of M 87, ApJ, 746, 151.
Abu-Zayyad, T., et al. Including Oshima, A.: 2012, Search
for Anisotropy of Ultrahigh Energy Cosmic Rays with theTelescope Array Experiment, ApJ, 757, 26.
Abu-Zayyad, T., et al. Including Oshima, A.: 2012, The surface
detector array of the Telescope Array Experiment, Nucl.
Instrum. Meth. A, 689, 87-97.
Ackermann, M., et al. including Fukui, A.: 2013, Multiwavelength
Observations of GRB 110731A: GeV Emission from Onset to
Afterglow, ApJ, 763, 71.
Adams, J. H., et al. including Inoue, N., Kajino, T., Mizumoto,Y., Takami, H., Watanabe, J.: 2013, An Evaluation of the
Exposure in Nadir Observation of the JEM-EUSO Mission,
Astropart. Phys., 44, 76-90.
Ando, H., Imamura, T., Nabatov, A., Futaana, Y., Iwata, T.,
Hanada, H., Matsumoto, K., Mochizuki, N., Kono, Y., Noda,
H., Liu, Q., Oyama, K.-I., Yamamoto, Z., Saito, A.: 2012, Dualspacecraft radio occultation measurement of the electron density
near the lunar surface on the SELENE mission, J. Geophys.
Res., 117, A08313.
Ando, M.: 2013, DECIGO Pathfinder, Int. J. Modern. Phys. D, 22,1341002.
Aoki, W., Beers, T. C., Lee, Y.-S., Honda, S., Ito, H., TakadaHidai, M., Frebel, A., Suda, T., Fujimoto, M. Y., Carollo, D.,
Sivarani, T.: 2013, High-Resolution Spectroscopy of Extremely
Metal-Poor Stars from SDSS/SEGUE: I. AtmosphericParameters and Chemical Compositions, AJ, 145, 13.
Aoki, W., Ito, H., Tajitsu, A.: 2012, Examination of the Massdependent Li Depletion Hypothesis by the Li Abundances of the
Very Metal-poor Double-lined Spectroscopic Binary G166-45,
ApJ, 751, L6.
Aoki, W., Suda, T., Boyd, R. N., Kajino, T., Famiano, M. A.: 2013,
New Insights into the Astrophysical r-Process, ApJ, 766, L13.
Araki, M., Takano, S., Yamabe, H., Tsukiyama, K., Kuze, N.: 2012,
Radio Search for H2CCC toward HD 183143 as a Candidate fora Diffuse Interstellar Band Carrier, ApJ, 753, L11.
Asai, A., Kiyohara, J., Takasaki, H., Narukage, N., Yokoyama, T.,
Masuda, S., Shimojo, M., Nakajima, H.: 2013, Temporal andSpatial Analyses of Spectral Indices of Nonthermal Emissions
Derived from Hard X-Rays and Microwaves, ApJ, 763, 87.
Asayama, S., Nakajima, T.: 2013, Development of a Smooth Taper
Double-Ridge Waveguide Orthomode Transducer for a New
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Toshikawa, J., Kashikawa, N., Ota, K., Morokuma, T., Shibuya,T., Hayashi, M., Nagao, T., Jiang, L., Malkan, M. A., Egami, E.,
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Watanabe, T., Hara, H., Sterling, A. C., Harra, L. K.: 2012, Productionof High-Temperature Plasmas During the Early Phases of aC9.7 Flare. II. Bi-directional Flows Suggestive of Reconnection
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Westbrook, B., Lee, A., Meng, X., Suzuki, A., Arnold, K.,
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Wheelwright, H. E., de Wit, W. J., Oudmaijer, R. D., Hoare, M.
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Yabe, K., Ohta, K., Iwamuro, F., Yuma, S., Akiyama, M., Tamura,N., Kimura, M., Takato, N., Moritani, Y., Sumiyoshi, M.,
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Yagi, M., Suzuki, N., Yamanoi, H., Furusawa, H., Nakata,F., Komiyama, Y.: 2013, Re-Calibration of SDF/SXDS
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Yamada, K., Kitayama, T., Takakuwa, S., Iono, D., Tsutsumi, T.,
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Yamada, T., Matsuda, Y., Kousai, K., Hayashino, T., Morimoto,N., Umemura, M.: 2012, Profiles of Lyα Emission Lines of the
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Yamaguchi, T., Takano, S., Watanabe, Y., Sakai, N., Sakai, T., Liu,
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Yamaki, H., Kameno, S., Beppu, H., Mizuno, I., Imai, H.: 2012,
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Yamanoi, H., Komiyama, Y., Yagi, M., Okamura, S., Iye, M.,
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The Galaxy Luminosity Functions down to MR = −10 in the
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Yamauchi, A., Nakai, N., Ishihara, Y., Diamond, P., Sato, N.: 2012,
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2. Publications of the National Astronomical Observatory of Japan
Not Published.

3. Report of the National Astronomical Observatory ofJapan (in Japanese)Sôma, M., Ueda, A., Tanikawa, K., Yasumoto, B.: Eclipse on
March 24, AD 247 and ΔT, Rep. Nat. Astron. Obs. Japan, 14,
15-34.
Noda, S., Furusho, R., Furusawa, J., Yamada, Y., Yamauchi, C.,
Ozawa, T., Takata, T., Ichikawa, S.-I.: Development of Public
Science Archive System of Subaru Telescope 6, Rep. Nat. Astron. Obs. Japan, 14, 35-61.
Sôma, M., Araki, H., Noda, H., Tazawa, S., Goossens, S.,
Hayamizu, T.: Northern Limit of the Annular Solar Eclipse on
2012 May 21 in Japan, Rep. Nat. Astron. Obs. Japan, 15, 1-11.
Ochiai, A., Watanabe, M., Sôma, M., Ueda, A., Tanikawa, K.:
The Lunar Eclipse Record on Day Yi-Chou of Kogyoku Reign
Period, 2nd Year, 5th Month and The YuanJia Li Calendar,
Rep. Nat. Astron. Obs. Japan, 15, 13-28.

4. Conference Proceedings
Akashi, T., Kitamura, Y., Yoshida, A., Tatei, H., Shimajiri, Y.,
Kawabe, R.: 2012, CO Line Observations in the L1551
Cloud with the Nobeyama 45 m Telescope, New Trends inRadio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 146.
Ammons, S. M., Bendek, E. A., Guyon, O., Macintosh, B.,
Savransky, D.: 2012, Theoretical limits on bright star astrometry
with multi-conjugate adaptive optics using a diffractive pupil,
Proc. SPIE 8447, Eds. B. L. Ellerbroek, E. Marchetti, J.-P.
Veran, 84470P.
Ando, H., Kambe, E., Sato, B.: 2012, Okayama Project: Solar-like
Oscillations in Sub-giants and Giants, ASP Conf. Ser., 462, Eds.
H. Shibahashi, M. Takata, A. E. Lynas-Gray, 220-223.
Aoki, W.: 2012, Neutron-capture elements in extremely metal-poorstars, AIP Conf. Proc. 1484, Eds. S. Kubono, T. Hayakawa, T.
Kajino, H. Miyatake, T. Motobayashi, K. Nomoto, 175-182
Aoki, W.: 2012, Extremely metal-poor stars in the Milky Way
Galaxy, AIP Conf. Proc. 1480, Eds. M. Umemura K. Omukai,
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Aoki, W.: 2012, Extremely Metal-Poor Stars in the Milky Way
Halo, ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 55-60.
Aoki, W.: 2012, Observational evidence for the first stars andconstraints on stellar models, 12th Int. Symp. on Nuclei in the
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Aoki, W.: 2013, Li abundances in very metal-poor, main-sequence
turn-off stars, Memorie della Societa Astronomica Italiana
Supplement, 22, 35-40.
Asai, A., Hara, H., Watanabe, T., Imada, S.: 2012, Flare Onset
Observed with Hinode in the 2006 December 13 Flare, ASP
Conf. Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 303
Asayama, S., Knee, L. B. G., Calisse, P. G., Cortés, P. C., Jager,
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J. P., Planesas, P.: 2012, ALMA array element astronomicalverification, Proc. SPIE 8444, Eds. L. M. Stepp, R. Gilmozzi, H.
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Asayama, S., Whyborn, N., Yagoubov, P.: 2012, ALMA SIS mixer
optimization for stable operation, Proc. SPIE 8452, Eds. W. S.
Holland, J. Zmuidzinas,
Belikov, R., Pluzhnik, E., Witteborn, F. C., Greene, T. P., Lynch, D.
H., Zell, P. T., Schneider, G., Guyon, O., Tenerelli, D.: 2012,
EXCEDE technology development I: first demonstrations ofhigh contrast at 1.2 l/D for an Explorer space telescope mission,
Proc. SPIE 8442, Eds. M. C. Clampin, G. G. Fazio, H. A.
MacEwen, J. M. Oschmann, Jr., 844209.
Bendek, E. A., Ammons, S. M., Belikov, R., Pluzhnik, E., Guyon,
O.: 2012, High precision astrometry laboratory demonstrationfor exoplanet detection using a diffractive pupil telescope, Proc.
SPIE 8442, Eds. M. C. Clampin, G. G. Fazio, H. A. MacEwen, J.
M. Oschmann, Jr., 844243.
Benz, A. O., Brasja, R., Shimojo, M., Karlicky, M., Testi, L.: 2012,
Observing the Sun with ALMA, Science with Large Solar
Telescopes, Proc. IAU Special Session 6, held 22-24 August, 2012,
Blain, C., Guyon, O., Martinache, F., Bradley, C., Clergeon, C.:2012, Open-loop control of SCExAO's MEMS deformablemirror using the Fast Iterative Algorithm: speckle control
performances, Proc. SPIE 8447, Eds. B. L. Ellerbroek, E.
Marchetti, J.-P. Veran, 844768.
Boyd, R. N., Famiano, M., Meyer, B., Motizuki, Y., Kajino, T.,
Roederer, I. U.: 2012, The r-Process in Metal Poor Stars andBlack Hole Formation, AIP Conf. Proc. 1484, Eds. S. Kubono,
T. Hayakawa, T. Kajino, H. Miyatake, T. Motobayashi, K.
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Carlotti, A., Kasdin, N. J., Martinache, F., Vanderbei, R. J., Young, E.
J., Che, G., Groff, T. D., Guyon, O.: 2012, Fully optimized shaped
pupils: preparation for a test at the Subaru Telescope, Proc. SPIE
8446, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 84463C.
Cesar, O., et al. including Takato, N., Ueda, A.: 2012, FOCCoS
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Ramsay, H. Takami, 84464R.
Cheoun, M. K., Ha, E., Kajino, T.: 2012, Charge Exchange
Reactions and Applications to Astrophysics, AIP Conf. Proc.
1484, Eds. S. Kubono, T. Hayakawa, T. Kajino, H. Miyatake, T.
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Cheoun, M. K., Ryu, C. Y., Kajino, T., Kusakabe, M., Mathews,
G. J.: 2012, Reinvestigation of Quark Masses Variations on Big
Bang Nucleosynthesis, Int. Conf. on Few Body Systems, FewBody Sys., 54, 495-499.
Chibueze, J. O., Imai, H., Tafoya, D., Omodaka, T., Kameya, O.,
Hirota, T., Chong, S. N., Torrelles, J. M.: 2012, A Highly-

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collimated Water Maser Bipolar Outflow in the Cepheus A
HW3d Massive Protostellar Object, Cosmic Masers - fromOH to H0, Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L.
Humphreys, W. H. T. Vilemmings, 141-145
Chibueze, J. O., Imura, K., Omodaka, T., Handa, T., Nagayama,T., Fujisawa, K., Sunada, K., Nakano, M., Kamezaki, T.,
Yamaguchi, Y.: 2013, Star Formation in the Molecular Cloud
Associated with the Monkey Head Nebula: Sequential or
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Chitsazzadeh, S., Di Francesco, J., Bourke, T., Friesen, R.,
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S., Tatematsu, K., Tobin, J.: 2012, Molecular Emission
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Crabtree, D. R., Christensen, L. L., Robson, I., Pomare, O. A.,
Neto, A. D., Fienberg, R. T., Green, A., Kembhavi, A. K.,
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Crossfield, J. M. I., Barman, T., Hansen, M. S. B., Tanaka, I.,
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Davies, R., Corbett, I., Ekers, R., Green, R., Iye, M., KraanKorteweg, R., Ruiz, M. T., Tacconi, L., Tarenghi, M., Wilson, C.,
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Davis, L., Muders, D., Humphreys, E., Stoehr, F., Leon Tanne, S.,
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Davis, T. A., Heiderman, A., Iono, D., the VIXENS team: 2013,
Chemical Complexity and Star-Formation in Merging Galaxies,
Molecular Gas, Dust, and Star Formation, Proc. IAU Symp.
292, Eds. T. Wong, J. Ott, 224-224.
Deguchi, S.: 2012, SiO Maser Surveys of Nearby Miras and their
Kinematics in the Galaxy, Cosmic Masers - from OH to H0,
Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L. Humphreys, W.
H. T. Vilemmings, 265-274.
Doi, Y., Komugi, S., Kawada, M., Takita, S., Arimatsu, K.,
Ikeda, N., Kato, D., Kitamura, Y., Nakagawa, T., Ootsubo, T.,
Morishima, T., Hattori, M., Tanaka, M., White, G., Etxaluze,
M., Shibai, H.: 2012, Akari Far-Infrared All-Sky Survey Maps,
Publ. Korean Astron. Soc., 27, 111-116.
Doi, Y., Matsuura, S., Ootsubo, T., Komugi, S., Ikeda, N., Tanaka,
M., Kitamura, Y., Kawada, M., Morishima, T., Hattori, M.,
White, G., Shibai, H., Nakagawa, T.: 2012, New Far-Infrared
All-Sky Maps using the AKARI/FIS Mission, 39th COSPAR
Assembly, 461.
Eguchi, S., Shirasak, Y., Komiya, Y., Ohishi, M., Mizumoto, Y.,
Ishihara, Y., Tsutsumi, J., Hiyama, T., Nakamoto, H., Sakamoto,M.: 2012, Improvement of Service Searching Algorithm in
the JVO Portal Site, ASP Conf. Ser., 461, Eds. P. Ballester, D.

Egret, N. P. F. Lorente, 343-344.
Fujii, Y., Gonzalez, A., Kroug, M., Kaneko, K., Miyachi, A.,
Kuroiwa, K., Yokoshima, T., Makise, K., Uzawa, Y., Wang,Z.: 2012, Performance of the first six ALMA Band 10 receivers,
ISSTT Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, C-14.
Fujisawa, K., Hachisuka, K., Sugiyama, K., Doi, A., Honma,
M., Yonekura, Y., Hirota, T., Sawada-Satoh, S., Murata, Y.,
Motogi, K., Ogawa, H., Chen, X., Kim, K.-T., Shen, Z.-Q.:
2012, The VLBI mapping survey of the 6.7 GHz methanol
masers with the JVN/EAVN, Cosmic Masers - from OH to H0,
Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L. Humphreys, W.
H. T. Vilemmings, 288-289.
Fuse, T., Kuroda, D.: 2012, Asteroidal Satellites Search using
Subaru Telescope's AO Systems, Asteroids, Comets, Meteors
2012, 6489.
Genova, F., Norris, R., Smith, M., Crabtree, D., Dluzhnevskaya, O.
B., Ohishi, M., Ros, R. M., Ruggles, C. L. N., Samus, N. N.,
Trimble, V. L., van Driel, W., Wahlgren, G. M.: 2012, Division
XII: Union-Wide Activities, Transactions IAU, Vol. 7, Issue
T28A, Ed. I. Corbet, 325-326.
Gil-Pons, P., Doherty, C. L., Suda, T., Campbell, S. W., Lau, H.,
Giulani, S. M., Lattanzio, J. C.: 2012, The evolution and C, N
and O yields of intermediate-mass Z = 10−5 stars in isolationand in close binary systems, AIP Conf. Proc. 1480, Eds. M.
Umemura K. Omukai, 358-360.
Gonzalez, A., Uzawa, Y., Kaneko, K., Fujii, Y.: 2012, Improvements
in ALMA band 10 optics: Influence of IR filters and solutions,
ISSTT Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, P-30.
Gonzalez, A., Uzawa, Y.: 2012, Cross-polarization in quasi-opticalreceivers: ALMA band 4 and 10, IRMMW-THz2012, Int. Conf.
IR. MM. THz Waves, Tue-B-5-4.
Goswami, A., Aoki, W.: 2012, Contribution of HdC Stars to the
Galactic Enrichment: The Sr-rich HdC Star HE 1015-2050,
ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 127-128.
Gouda, N.: 2012, Infrared Space Astrometry Missions ~JASMINE
Missions~, ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T.
Suda, T. Tsujimoto, N. Arimoto, 417-418.
Guyon, O., Bendek, E., Ammons, S. M., Shao, M., Shaklan, S.,
Woodruff, R. A., Belikov, R., Milster, T.: 2012, Characterizationof habitable exoplanets with simultaneous coronagraphy andastrometry with a single aperture telescope, Proc. SPIE 8442,
Eds. M. C. Clampin, G. G. Fazio, H. A. MacEwen, J. M.
Oschmann, Jr., 84420K.
Guyon, O., Kern, B., Belikov, R., Shaklan, S., Kuhnert, A.,
Give'on, A., Martinache, F.: 2012, Phase induced amplitude
apodization (PIAA) coronagraphy: recent results and future
prospects, Proc. SPIE 8442, Eds. M. C. Clampin, G. G. Fazio, H.
A. MacEwen, J. M. Oschmann, Jr., 84424V.
Guyon, O., Martinache, F., Cady, E. J., Belikov, R., Balasubramanian,K., Wilson, D., Clergeon, C. S., Mateen, M.: 2012, How ELTs
will acquire the first spectra of rocky habitable planets, Proc.
SPIE 8447, Eds. B. L. Ellerbroek, E. Marchetti, J.-P. Veran,
84471X.
Guyon, O., Martinache, F.: 2012, Achieving high precision
photometry for transiting exoplanets with a low cost robotic

DSLR-based imaging system, Proc. SPIE 8444, Eds. L. M.
Stepp, R. Gilmozzi, H. J. Hall, 84444A.
Guyon, O., Schneider, G., Belikov, R., Tenerelli, D. J.: 2012, The
EXoplanetary Circumstellar Environments and Disk Explorer(EXCEDE), Proc. SPIE 8442, Eds. M. C. Clampin, G. G. Fazio,
H. A. MacEwen, J. M. Oschmann, Jr., 84421S.
Hamano, S., Kobayashi, N., Kondo, S., Tsujimoto, T., Okoshi,
K., Shigeyama, T.: 2012, Type-Ia SNR-Shell at z = 3.5 Seen in
the Three Sightlines toward the Gravitationally Lensed QSO
B1422+231, ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T.
Suda, T. Tsujimoto, N. Arimoto, 129-130.
Hanaoka, Y.: 2012, Polarimeter with a high-speed rotating
waveplate for the solar observation, Proc. SPIE 8446, Eds. I. S.
McLean, S. K. Ramsay, H. Takami, 844670.
Handa, T., Yoda, T., Kohno, K., Morino, J.-i., Nakajima, T.,
Kuno, N., Ogawa, H., Kimura, K.: 2012, The AMANOGAWA2SB Surevey and the Gas Density Histogram of Milky Way
Galaxy to Address the Origin of the Density Structure of ISM,ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 221-221.
Handa, T., Yoda, T., Kohno, K., Nakajima, T., Morino, J.-i.,
Yonekura, Y., Ogawa, H., Kimura, K., Dobashi, K.: 2013,
AMANOGAWA-2SB survey: a northern galactic plane survey
in 12CO (J = 2–1) and 13CO (J = 2–1) with the Amanogawa
telescope, Molecular Gas, Dust, and Star Formation, Proc. IAU
Symp. 292, Eds. T. Wong, J. Ott, 102-102.
Hara, C., Kawabe, R., Shimajiri, Y., Ueda, J., Kurano, Y.,
Tsukagoshi, T., Nakamura, F., Saito, M., Wilner, D.: 2012,
Discovery of the Rotating Molecular Outflow and Disk in theClass-0/1 Protostar [BHB2007]#11 in Pipe, New Trends inRadio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 145.
Hasegawa, S., Miyasaka, S., Mito, H., Sarugaku, Y., Ozawa,T., Kuroda, D., Nishihara, S., Harada, A., Yoshida, M.,
Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda, H., Okita,K., Kawai, N., Mori, M., Sekiguchi, T., Ishiguro, M., Abe, M.:
2012, Lightcurve Survey of V-Type Asteroids. Observations
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Hasegawa, T., the ALMA Front End Integration Subproject Team:2012, Integration and verification of ALMA receiver front ends,
ISSTT Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, P-27.
Hashimoto, T., Watanabe, J., Sato, M., Ishiguro, M.: 2011,
Identification of Optical Component of North Toroidal Sourceof Sporadic Meteors and Its Origin, Meteoroids: The Smallest
Solar System Bodies, Eds. W. J. Cooke, D. E. Moser, B. F.
Hardin, D. Janches, 82.
Hattori, M., Shirahata, M., Minowa, Y., Oya, S., Hayano, Y.,
Takami, H., Iye, M.: 2012, Recent development in real time
control system of Subaru LGSAO-188, Proc. SPIE 8447, Eds. B.
L. Ellerbroek, E. Marchetti, J.-P. Veran, 84472P.
Hayakawa, S., Kubono, S., Kahl, D., Yamaguchi, H., Binh, D. N.,
Hashimoto, T., Wakabayashi, Y., He, J. J., Iwasa, N., Kato, S.,
Komatsubara, T., Kwon, Y. K., Teranishi, T., Wanajo, S.: 2012,
Direct measurement of the breakout reaction 11C(a, p)14N in
explosive hydrogen-burning process, AIP Conf. Proc. 1484,
Eds. S. Kubono, T. Hayakawa, T. Kajino, H. Miyatake, T.

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Motobayashi, K. Nomoto, 445-447.
Hayakawa, S., Kubono, S., Kahl, D., Yamaguchi, H., Binh, D. N.,
Hashimoto, T., Wakabayashi, Y., He, J. J., Iwasa, N., Kato, S.,
Komatsubara, T., Kwon, Y. K., Teranishi, T., Wanajo, S.: 2012,
Direct measurement of the 11C(a, p)14N reaction at CRIB: A
path from pp-chain to CNO, AIP Conf. Proc. 1498, 339-343.
Hayama, K., Niinuma, K., Oyama, T.: 2012, Proposal for MultiMessenger Observations of Radio Transients by Nasu and LigoVirgo, New Horizons in Time-Domain Astronomy, Proc. IAU
Symp. 285, Eds. R. E. M. Griffin, R. J. Hanisch, R. Seaman,
331-333
He, J. J., et al. including Kajino, T.: 2012, A surprise in the Li6(p,γ)Be7 reaction at low energies, 12th Int. Symp. on Nuclei in the
Cosmos (NIC12), Cairns, Proc. of Science (NIC XII), Eds. J.
Lattanzio, A. Karakas, M. Lugaro, G. Dracoulis, 5.
Hibi, Y., Matsuo, H., Ookawa, T., Sekiguchi, S., Torii, D., Watanabe,D., Ikeda, H., Fujiwara, M.: 2012, Cryogenic Multi-Channel
Readout System for Submillimeter/Terahertz Photon Detectors,
ISSTT Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, P-47.
Hinz, P., Codona, J., Guyon, O., Hoffmann, W., Skemer, A., Hora,J., Tolls, V., Boss, A., Weinberger, A., Arbo, P., Connors, T.,
Durney, O., McMahon, T., Montoya, M., Vaitheeswaran, V.:
2012, TIGER: a high contrast infrared imager for the Giant
Magellan Telescope, Proc. SPIE 8446, Eds. I. S. McLean, S. K.
Ramsay, H. Takami, 84461P.
Hirota, A., Kuno, N., Tanaka, A., Nakanishi, K., Kawabe,
R.: 2012, Wide-Field 12CO (J = 1–0) Imaging of the Nearby
Barred Galaxy M83 with the NMA and the 45 m Telescope,
New Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 111.
Hirota, T., Tsuboi, M., Fujisawa, K., Honma, M., Kawaguchi, N.,
Kim, M. K., Kobayashi, H., Imai, H., Omodaka, T., Shibata,K. M., Shimoikura, T., Yonekura, Y.: 2012, VERA Observationsof the H2O Maser Burst in Orion KL, Cosmic Masers - fromOH to H0, Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L.
Humphreys, W. H. T. Vilemmings, 103-107.
Honda, S., Aoki, W., Arimoto, N., Sadakane, K., Otsuki, K.,
Kajino, T., Mathews, G. J.: 2012, Heavy elements in globularclusters and dwarf galaxies as probes of the origin of r-processelements, AIP Conf. Proc. 1484, Eds. S. Kubono, T. Hayakawa,T. Kajino, H. Miyatake, T. Motobayashi, K. Nomoto, 99-104.
Honda, S., Aoki, W., Arimoto, N., Sadakane, K., Otsuki, K.,
Kajino, T., Mathews, G. J.: 2012, Heavy elements in globularclusters and dwarf galaxies as probes of the origin of r-processelements, AIP Conf. Proc. 1484, Eds. S. Kubono, T. Hayakawa,T. Kajino, H. Miyatake, T. Motobayashi, K. Nomoto, 99-104.
Honda, S., Aoki, W., Arimoto, N., Sadakane, K.: 2012, Heavy
Neutron-Capture Elements in Extremely Metal-Poor Stars
in Dwarf Galaxies, ASP Conf. Ser., 458, Eds. W. Aoki, M.
Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 307-310.
Honma, M., Nagayama, T., Hirota, T., Matsumoto, N., Sakai,N., Kawaguchi, N.: 2012, Maser astrometry with VERA andGalactic structure, Cosmic Masers - from OH to H0, Proc. IAU
Symp. 287, Eds. R. S. Booth, E. M. L. Humphreys, W. H. T.
Vilemmings, 386-390.
Horie, M., Nishikawa, J., Oya, M., Waki, R., Kumagai, S.,080

II Publications, Presentations

Tamura, M., Kurokawa, T., Murakami, N., Murakami, H.,
Abe, L.: 2012, Wavefront correction inside unbalanced nullinginterferometer, Proc. SPIE 8445, Eds. F. Delplancke, J. K.
Rajagopal, F. Malbet, 84452E.
Iguchi, S., Saito, M.: 2012, Very large millimeter/submillimeter
array toward search for 2nd Earth, Proc. SPIE 8444, Eds. L. M.
Stepp, R. Gilmozzi, H. J. Hall, 84443I.
Imanishi, M., Nakagawa, T., Shirahata, M., Ohyama, Y., Onaka,
T.: 2012, AKARI IRC infrared 2.5–5 micron spectroscopy ofnearby luminous infrared galaxies, Publ. Korean Astron. Soc.,
27, 271-274.
Imanishi, M.: 2013, Selecting, Scheduling and Carrying Out
Observing Programmes at the Subaru Telescope, Organizations,
People and Strategies in Astronomy, 2, 305-322.
Inoue, S.: 2012, Nature of Clump-Origin Bulges: Similarities tothe Milky Way Bulge, ASP Conf. Ser., 458, Eds. W. Aoki, M.
Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 227-228.
Ishigaki, M. N., Aoki, W., Chiba, M.: 2012, Chemical abundancesof the Milky Way thick disk and stellar halo, AIP Conf. Proc.
1480, Eds. M. Umemura K. Omukai, 379-381.
Ishigaki, M., Chiba, M., Aoki, W.: 2012, Chemical Abundancesof the Kinematically Selected Thick Disk and Halo Stars,
ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 157-160.
Ishiguro, M., Hanayama, H., Hasegawa, S., Sarugaku, Y.,
Watanabe, J., Fujiwara, H., Terada, H., Hsieh, H. H.,
Vaubaillon, J. J., Kawai, N., Yanagisawa, K., Kuroda, D.,
Miyaji, T., Ohta, K., Fukushima, H., Hamanowa, H., Kim, J.,
Pyo, J., Nakamura, A. M.: 2012, Ejecta Plume Resulting
from an Oblique Impact on (596) Scheila, Asteroids, Comets,
Meteors 2012, 6121.
Ishii, S., Seta, M., Nakai, N., Miyamoto, Y., Nagai, M., Arai,
H., Maezawa, H., Nagasaki, T., Miyagawa, N., Motoyama,
H., Sekimoto, Y., Bronfman, L.: 2012, Development of aTransportable Telescope for Galactic Survey at 500 GHz in
Antarctica, ISSTT Proceedings 2012, Eds. H. Matsuo, Y.
Sekimoto, P-14.
Ishizuka, C., Suda, T., Suzuki, H., Ohnishi, A., Sumiyoshi, K., Toki,
H.: 2012, Database for Nuclear EOS, Proc. of Science, 197, Eds. J.
C. Lattanzio, A. Karakas, M. Lugaro, G. Dracoulis, 1-6.
Itoh, R., et al. including Tanaka, M.: 2012, Supernova 2012cm,
Central Bureau Electronic Telegrams, 3126, 2.
Iwai, K., Misawa, H., Tsuchiya, F., Morioka, A., Masuda, S.,
Miyoshi, Y.: 2012, Survey of Accelerated Particles in a Solar
Active Region Using Hinode/XRT and Ground-Based Type-I
Radio Burst Observations, ASP Conf. Ser., 454, Eds. T. Sekii, T.
Watanabe, T. Sakurai, 249-252.
Iwata, T., Kitazato, K., Abe, M., Ohtake, M., Matsuura, S., Tsumura,K., Hirata, N., Honda, C., Takagi, Y., Nakauchi, Y., Hiroi, T.,
Senshu, H., Arai, T., Nakamura, T., Matsunaga, T., Komatsu, M.,
Takato, N., Watanabe, S.: 2013, Results of the Critical Design
for NIRS3: The Near Infrared Spectrometer on Hayabusa-2, 44th
Lunar and Planetary Science Conference, 1908.
Iwata, T., SELENE Science Team: 2012, A review of SELENE/
Kaguya and outline of Japanese future Lunar and Martian
mission plans, New Scientific Observations in Lunar andPlanetary Exploration, Macau University of Science andTechnology, 55-59.
Jeschke, E., Inagaki, T., Kackley, R.: 2012, A next generation
open-source toolkit for FITS file image viewing, Proc. SPIE
8451, Eds. N. Radziwill, G. Chiozzi, 845102.
Jike, T., Manabe, S., Tamura, Y., Shizugami, M., VERA Group:
2012, VERA Geodetic Activities, IVS 2011 Annual Report, Eds.
D. Behrend K. D. Baver, 72-75.
Jike, T., Manabe, S., Tamura, Y., Shizugami, M.: 2012, Movementof the 2011 the Pacific coast of Tohoku Earthquake detected by
VERA geophysical observations, IVS 2012 General Meeting
Proc. “Launching the Next-Generation IVS Network”, Eds. D.
Behrend K. D. Baver, 450-454.
Kajino, T., Aoki, W., Cheoun, M. K., Chiba, S., Fujiya, W.,
Hayakawa, T., Mathews, G. J., Nakamura, K., Shaku, K.,
Yoshida, T.: 2012, Supernova Nucleosynthesis and Neutrino
Oscillation, AIP Conf. Proc. 1441, Eds. S. G. Steadman, G. S. F.
Stephans, F. E. Taylor, 375-377.
Kajino, T., Aoki, W., Fujiya, W., Mathews, G. J., Yoshida, T.,
Shaku, K., Nakamura, K., Hayakawa, T.: 2012, Supernova
Neutrino-Process and Implication in Neutrino Oscillation,
ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 31-34.
Kajino, T., Nakamura, K., Sato, K., Shaku, K., Yoshida, T.,
Hayakawa, T., Chiba, S., Yamazaki, D. G., Cheoun, M. K.,
Mathews, G. J.: 2012, Supernova Nucleosynthesis, Neutrino
Mass and Oscillation, and Nuclear Weak Interactions, FrenchJapanese Symp. on Nuclear Structure Problems, Eds. H. Otsu, T.
Motobayashi, P. Roussel-Chomaz, T. Otsuka, 161-166.
Kajino, T.: 2012, Supernova Nucleosynthesis and the Physics of
Neutrino Oscillation, AIP Conf. Proc. 1498, 229-236.
Kajino, T.: 2012, Particle and Nuclear Physics Aspects of the BigBang Nucleosynthesis, 12th Int. Symp. on Nuclei in the Cosmos(NIC12), Cairns, Proc. of Science (NIC XII), Eds. J. Lattanzio,
A. Karakas, M. Lugaro, G. Dracoulis, 70.
Kajino, T., Aoki, W., Fujiya, W., Mathews, G. J., Yoshida, T.,
Shaku, K., Nakamura, K., Hayakawa, T.: 2012, Supernova
Neutrino-Process and Implication in Neutrino Oscillation,
ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 31-34.
Kamata, Y., Miyazaki, S., Nakaya, H., Komiyama, Y., Obuchi,
Y., Kawanomoto, S., Uraguchi, F., Utsumi, Y., Suzuki, H.,
Miyazaki, Y., Muramatsu, M.: 2012, Hyper Suprime-Cam:characteristics of 116 fully depleted back-illuminated CCDs,
Proc. SPIE 8453, Eds. A. D. Holland, J. W. Beletic, 84531X.
Kamegai, K., Sakai, T., Sakai, N., Hirota, T., Yamamoto, S.:
2013, Submillimeter-wave Observations of Complex Organic
Molecules in Southern Massive Star Forming Regions,
Molecular Gas, Dust, and Star Formation, Proc. IAU Symp.
292, Eds. T. Wong, J. Ott, 107-107.
Kameno, S., Yamaki, H., Mizuno, I., Beppu, H., Imai, H., Kuno,
N., Akashi, T.: 2012, Optimization by Smoothed Bandpass
Calibration in Radio Spectroscopy, New Trends in Radio
Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 166.
Kameya, O.: 2013, Distribution of ionized gas density measured

by differential VLBI Observations of pulsars, Neutron Stars andPulsars: Challenges and Opportunities after 80 years, Proc. IAU
Symp. 291, Eds. J. van Leeuwen, 417-417.
Kamezaki, T., Imura, K., Nagayama, T., Omodaka, T., Handa, T.,
Yamaguchi, Y., Chibueze, J. O., Sunada, K., Nakano, M.: 2013,
VLBI Observations and NH 3 Mapping of the Star-forming
Region NGC 2264, Molecular Gas, Dust, and Star Formation,
Proc. IAU Symp. 292, Eds. T. Wong, J. Ott, 45-45.
Kamezaki, T., Nakagawa, A., Omodaka, T. Handa, T., Imai, H.,
Tafoya, D., Matsui, M., Nishida, Y., Nagayama, T., Honma, M.,
Kobayashi, H., Miyaji, T., Takeuti, M.: 2013, VLBI astrometryof the semi-regular variable star RX Bootis, Advancing thePhysics of Cosmic Distances, Proc. IAU Symp. 289, Eds. R. de
Grijs, 91-94.
Kaneko, H., Kuno, N., Iono, D., Tamura, Y., Tosaki, T., Nakanishi,K., Sawada, T.: 2012, Molecular Gas Properties and Formationin Interacting Galaxies, New Trends in Radio Astronomy in
the ALMA Era: The 30th Anniversary of Nobeyama Radio
Observatory, 87.
Kano, R., Bando, T., Narukage, N., Ishikawa, R., Tsuneta, S.,
Katsukawa, Y., Kubo, M., Ishikawa, S., Hara, H., Shimizu,
T., Suematsu, Y., Ichimoto, K., Sakao, T., Goto, M., Kato, Y.,
Imada, S., Kobayashi, K., Holloway, T., Winebarger, A., Cirtain,
J., De Pontieu, B., Casini, R., Trujillo Bueno, J., Štepán, J.,
Manso Sainz, R., Belluzzi, L., Asensio Ramos, A., Auchère,F., Carlsson, M.: 2012, Chromospheric Lyman-alpha spectropolarimeter (CLASP), Proc. SPIE 8443, Eds. T. Takahashi, S. S.
Murray, J.-W. A. den Herder, 84434F.
Karatsu, K., Naruse, M., Nitta, T., Sekimoto, Y., Sekine, M., Noguchi,T., Uzawa, Y., Matsuo, H., Kiuchi, H.: 2012, Development of1000 arrays MKID Camera for the CMB Observation, ISSTT
Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, C-32.
Karatsu, K., Naruse, M., Nitta, T., Sekine, M., Sekimoto, Y., Noguchi,T., Uzawa, Y., Matsuo, H., Kiuchi, H.: 2012, Developmentof 1000 arrays MKID camera for the CMB observation, Proc.
SPIE 8452, Eds. W. S. Holland, J. Zmuidzinas, 84520Q.
Kasuga, T., Usui, F., Hasegawa, S., Kuroda, D., Ootsubo, T.,
Müller, T. G., Ishiguro, M.: 2012, Two Faces of Cybele Asteroid
Group Revealed by AKARI/AcuA, Asteroids, Comets, Meteors
2012, 6097.
Kato, Y., Steiner, O., Steffen, M., Suematsu, Y.: 2012, Excitationof Slow-Modes in Network Magnetic Elements, The 4th Hinode
Science Meeting: Unsolved Problems and Recent Insights,
Rubio, L. R., Reale, F., Carlsson, M., 237.
Katsukawa, Y., Kitai, R., Watanabe, H.: 2012, Persistent Circulating
Motion in a Sunspot Umbra, ASP Conf. Ser., 454, Eds. T. Sekii,
T. Watanabe, T. Sakurai, 213.
Katsukawa, Y., Watanabe, T., Hara, H., Ichimoto, K., Kubo, M.,
Kusano, K., Sakao, T., Shimizu, T., Suematsu, Y., Tsuneta, S.:
2012, Next space solar observatory SOLAR-C: mission instruments
and science objectives, Science with Large Solar Telescopes, Proc.
IAU Special Session 6, held 22-24 August, 2012, E2.07.
Kawabe, R., Kohno, K., Yamamoto, S., Tamura, Y., Oshima, T.:2012, The Large Millimeter and Sub-Millimeter Telescope
Project, "ALMA SPICA Synergy Telescope (ASTe)", New
Trends in Radio Astronomy in the ALMA Era: The 30th

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Anniversary of Nobeyama Radio Observatory, 72.
Kim, J. H., Im, M., Kim, D., Woo, J.-H., Imanishi, M., AMUSES
team, LQSONG team: 2012, The 3.3 micron PAH Feature asa SFR Indicator: Probing the Interplay Between SF and AGN
Activities, Publ. Korean Astron. Soc., 27, 281-284.
Kim, M. K., Hirota, T., Kobayashi, H., VERA project teammembers: 2012, 3-Dimensional kinematics of water/SiO
masers in Orion-KL, Cosmic Masers - from OH to H0, Proc.
IAU Symp. 287, Eds. R. S. Booth, E. M. L. Humphreys, W. H. T.
Vilemmings, 415-416.
Kim, M., Choi, Y., Moon, H., Ishiguro, M., Mottola, S., Kaplan, M.,
Kuroda, D., Warjurkar, D., Takahashi, J., Byun, Y: 2013, Optical
Observations of NEA 162173 (1999 JU3) During the 2011-2012,
44th Lunar and Planetary Science Conference, 3068.
Kiriyama, Y., Ishihara, D., Nagayama, T., Kaneda, H., Oyabu,
S., Onaka, T., Fujiwara, H.: 2012, Debris Disks Explored by
AKARI and IRSF, Publ. Korean Astron. Soc., 27, 181-182.
Kiuchi, H., Saito, M., Iguchi, S.: 2012, Photonic local oscillator
technics for large-scale interferometers, Proc. SPIE 8444, Eds. L.
M. Stepp, R. Gilmozzi, H. J. Hall, 84442O.
Kobayashi, H.: 2013, VERA status and results, Advancing thePhysics of Cosmic Distances, Proc. IAU Symp. 289, Eds. R. de
Grijs, 194-194.
Kobayashi, K., Kano, R., Trujillo-Bueno, J., Ramos, A. A., Bando,T., Belluzzi, L., Carlsson, M., De Pontieu, R. C. B., Hara,
H., Ichimoto, K., Ishikawa, R., Katsukawa, Y., Kubo, M.,
Sainz, R. M., Narukage, N., Sakao, T., Stepan, J., Suematsu,
Y., Tsuneta, S., Watanabe, H., Winebarger, A.: 2012, The
Chromospheric Lyman-Alpha SpectroPolarimeter: CLASP, The
Fifth Hinode Science Meeting: Exploring the Active Sun, Eds. L.
Golub, I. De Moortel, T. Shimizu, 233.
Kobayashi, K., Sakai, Y., Sasaki, M., Kakimoto, S., Takano, S.:
2012, A Study on the Excitation Mechanism of Methy1 Formate
in Orion KL by Using Transitions in the Vibrational Excited
States, New Trends in Radio Astronomy in the ALMA Era: The
30th Anniversary of Nobeyama Radio Observatory, 148.
Kobayashi, T., Nishikawa, J., Tanaka, Y., Kurokawa, T., Kashiwagi,K., Tamura, M., Murakami, N., Baba, N., Hashimoto, N.: 2012,
Unbalanced nulling interferometer with four-quadrant phasemask, Proc. SPIE 8421, Eds. Y. Liao, W. Jin, D. D. Sampson, R.
Yamauchi, Y. Chung, K. Nakamura, Y. Rao, 84213D.
Kobayashi, Y., Shimura, Y., Niwa, Y., Yano, T., Gouda, N.,
Yamada, Y.: 2012, Nano-JASMINE: cosmic radiation
degradation of CCD performance and centroid detection, Proc.
SPIE 8442, Eds. M. C. Clampin, G. G. Fazio, H. A. MacEwen, J.
M. Oschmann, Jr., 8442471-6.
Koda, J., Scoville, N., Hasegawa, T., Calzetti, D., Donovan, M. J.,
Egusa, F., Kennicutt, R. C., Kuno, N., Louie, M., Momose, R.,
Sawada, T., Sorai, K., Umei, M.: 2013, Systematic Variationsof the CO J = 2–1/1–0 Ratio Between the Arm and Interarm
Regions of M51, AAS Meeting #221, #235.05.
Komatsubara, T., et al. including Kajino, T.: 2012, Study of levelstructure on Si26 for the astrophysical interest in Al26 production,
12th Int. Symp. on Nuclei in the Cosmos (NIC12), Cairns, Proc.
of Science (NIC XII), Eds. J. Lattanzio, A. Karakas, M. Lugaro,
G. Dracoulis, 206.

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Komiya, Y., Shirasaki, Y., Ohishi, M., Eguchi, S., Mizumoto, Y.,
Ishihara, Y., Tsutsumi, J., Hiyama, T., Nakamoto, H., Sakamoto,M.: 2012, VO Crawler: A Crawling System for Virtual
Observatory Services, ASP Conf. Ser., 461, Eds. P. Ballester, D.
Egret, N. P. F. Lorente, 375-376.
Komiya, Y., Yamada, S., Suda, T., Fujimoto, M. Y.: 2012,
Hierarchical Chemical Evolution and R-process Elements ofExtremely Metal-Poor Stars, ASP Conf. Ser., 458, Eds. W. Aoki,
M. Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 131-132
Komiya, Y., Yamada, S., Suda, T., Fujimoto, M. Y.: 2012, A
hierarchical model for the galactic chemical evolution andr-process elements of extremely metal-poor stars, AIP Conf.
Proc. 1480, Eds. M. Umemura K. Omukai, 388-391.
Komiyama, Y., Tanaka, Y., Miyazaki, S., Kawanomoto, S.,
Kamata, Y., Nakaya, H., Obuchi, Y., Uraguchi, F., Utsumi, Y.:
2012, Hyper Suprime-Cam: conceptual design to introduce
spectroscopic mode, Proc. SPIE 8446, Eds. I. S. McLean, S. K.
Ramsay, H. Takami, 84465D.
Komugi, S., et al. including Miura, R., Kuno, N.: 2012, Towards
a Comprehensive Law of the Interstellar Medium, New Trends
in Radio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 89.
Komugi, S., Tateuchi, K., Motohara, K., Takagi, T., Iono, D.,
Kaneko, H., Ueda, J., Saito, T. R., the miniTAO team: 2013,
The Schmide-Kennicutt Law oa Matched-Age Star Formation
Regions, Molecular Gas, Dust, and Star Formation, Proc. IAU
Symp. 292, Eds. T. Wong, J. Ott, 331.
Komugi, S., Tateuchi, K., Motohara, K., Takagi, T., Iono, D.,
Kaneko, H., Ueda, J., Saitoh, T. R., TAO/ANIR proect team:2012, The Star Formation Law in Similar-Age Regions: Casestudy of the Early-Phase Interacting Galaxy Taffy I, New Trends
in Radio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 90.
Kotani, T., Enya, K., Nakagawa, T., Matsuhara, H., Kataza, H.,
Kawada, M., Mita, M., Komatsu, K., Uchida, H., Fujiwara, K.,
Mitani, S., Sakai, S., Haze, K., Kaneda, H., Oyabu, S., Ishihara,D., Miyata, T., Sako, S., Nakamura, T., Asano, K., Tamura,M., Nishikawa, J., Yamashita, T., Narita, N., Hayano, H., Oya,S., Kokubo, E., Itoh, Y., Matsuo, T., Fukagawa, M., Shibai, H.,
Honda, M., Baba, N., Murakami, N., Okamoto, Y. K., Ida, S.,
Takami, M., Abe, L., Guyon, O., Yamamuro, T.: 2012, SPICA
coronagraph instrument: characterization of atmospheres andphysical parameters of giant planets by direct imaging andspectroscopy, Proc. SPIE 8442, Eds. M. C. Clampin, G. G.
Fazio, H. A. MacEwen, J. M. Oschmann, Jr., 84420F.
Kroug, M., Kuroiwa, K., Uzawa, Y.: 2012, Al/SiO2/Al Micro
Strip Lines for THz SIS Mixers, ISSTT Proceedings 2012, Eds.
H. Matsuo, Y. Sekimoto, P-16.
Kubo, M., Low, B. C., Lites, B. W.: 2012, Granular-Scale
Magnetic Flux Cancellations in the Photosphere, ASP Conf.
Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 41-42.
Kubo, M.: 2012, Diffusion and Decay of Sunspots, The 4th Hinode
Science Meeting: Unsolved Problems and Recent Insights,
Rubio, L. R., Reale, F., Carlsson, M., 49-60.
Kubono, S., Binh, D. N., Hayakawa, S., Hashimoto, T., Kahl, D.
M., Yamaguchi, H., Wakabayashi, Y., Teranishi, T., Iwasa, N.,Komatsubara, T., Kato, S., Chen, A., Cherubini, S., Choi, S.
H., Hahn, I. S., He, J. J., Khiem, Le H., Lee, C. S., Kwon, Y.
K., Wanajo, S., Janka, H.-T.: 2012, Experimental challenge tonuclear physics problems in the np-process, AIP Conf. Proc.
1484, Eds. S. Kubono, T. Hayakawa, T. Kajino, H. Miyatake, T.
Motobayashi, K. Nomoto, 189-196.
Kulcsar, C., et al. including Guyon, O., Martinache, F.: 2012,
Vibrations in AO control: a short analysis of on-sky data aroundthe world, Proc. SPIE 8447, Eds. B. L. Ellerbroek, E. Marchetti,
J.-P. Veran, 84471C.
Kuncarayakti, H., Doi, M., Aldering, G., Arimoto, N., Maeda, K.,
Morokuma, T., Pereira, R., Usuda, T., Hashiba, Y.: 2012, Massand metallicity constraints on supernova progenitors derived from
integral field spectroscopy of the environment, The Death ofMassive Stars: Supernovae and Gamma-Ray Bursts, Proc. IAU
Symp. 279, Eds. P. W. A. Roming, N. Kawai, E. Pian, 343-344.
Kuncarayakti, H., Doi, M., Aldering, G., Arimoto, N., Maeda,
K., Morokuma, T., Pereira, R., Usuda, T., Hashiba, Y.: 2012,
Supernova Progenitor Mass and Metallicity from Integral Field
Spectroscopic Study of the Environment, ASP Conf. Ser., 458,
Eds. W. Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 43.
Kuno, N.: 2012, Giant Molecular Clouds in M33 and M83,
New Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 24.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120404A: Mitsume ishigakijima optical observation, GRB
Coordinates Network, Circular Service, 13225, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120422A: Mitsume ishigakijima upper limit, GRB
Coordinates Network, Circular Service, 13263, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013,
GRB 120711B: Mitsume ishigakijima upper limits, GRB
Coordinates Network, Circular Service, 13465, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 120819A: Mitsume ishigakijima upper limits, GRB
Coordinates Network, Circular Service, 13686, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 121024A: Mitsume ishigakijima upper limits, GRB
Coordinates Network, Circular Service, 13897, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2012,
GRB 121108A: Mitsume ishigakijima upper limits, GRB
Coordinates Network, Circular Service, 13956, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013,
GRB 130216A: Mitsume Ishigakijima Upper Limits, GRB
Coordinates Network, Circular Service, 14233, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2013,
GRB 130306A: Mitsume Ishigakijima Upper Limits, GRB
Coordinates Network, Circular Service, 14280, 1.

Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120404A:
Mitsume okayama optical observation, GRB Coordinates
Network, 13224, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120803A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13574, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120803B:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13575, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120804A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13584, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120819A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13685, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120911A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13753, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 120923A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13817, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 121011A:
Mitsume okayama optical observation, GRB Coordinates
Network, 13846, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 121024A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13896, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 121028A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 13915, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 121211A:
Mitsume okayama optical observation, GRB Coordinates
Network, 14062, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2012, GRB 121226A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 14108, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130131A:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 14166, 1.
Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130131B:
Mitsume okayama optical upper limits, GRB Coordinates
Network, 14167, 1.

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Kuroda, D., Yanagisawa, K., Shimizu, Y., Toda, H., Nagayama,S., Yoshida, M., Ohta, K., Kawai, N.: 2013, GRB 130215A:
Mitsume okayama optical observation, GRB Coordinates
Network, 14220, 1.
Lawson, P. R., et al. including Guyon, O.: 2012, On advanced estimation
techniques for exoplanet detection and characterization using
ground-based coronagraphs, Proc. SPIE 8447, Eds. B. L.
Ellerbroek, E. Marchetti, J.-P. Veran, 844722.
Li, J. J., Moscadelli, L., Cesaroni, R., Furuya, R. S., Xu, Y., Usuda,T., Menten, K. M., Pestalozzi, M., Eliav, D., Schisano, E.: 2012,
Massive star-formation toward G28.87+0.07, Cosmic Masers from OH to H0, Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L.
Humphreys, W. H. T. Vilemmings, 180-181.
Liu, S.-Y., Aikawa, Y., Chen, V., Hirano, N., Hirota, T., Kamegai, K.,
Kobayashi, K., Kohno, K., Kuan, Y.-J., Liu, S.-Y., Nakajima, T.,
Ohashi, N., Ohishi, M., Ozeki, H., Sakai, N., Sakai, T., Shiba, S.,
Su, Y.-N., Sugimura, M., Takakuwa, S., Takano, S., Umemoto,T., Wang, K.-S., Watanabe, Y., Yamada, M., Yamaguchi, T.,
Yamamoto, S., Zhang, Q.-Z.: 2012, Nobeyama 45m Telescope
Legacy Project: Line Survey of IRDC G28.34+0.06, New
Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 140.
Lundgren, A., et al. including Saito, M., Tatematsu, K.: 2012,
ALMA: the first year of observations, Proc. SPIE 8448, Eds. A.
B. Peck, R. L. Seaman, F. Comeron, 844802.
Maezawa, H., Moribe, N., Nishimura, A., Ikeda, Y., Osaki, S.,
Horiuchi, K., Ohnishi, T., Ogawa, H., Sagawa, H., Tanaka, K.,
Tokumaru, M., Mizuno, A., Kondo, S., Fukui, Y., Takahashi,S., Maekawa, J., Iwashita, H., Handa, K., Oya, M., Kawabe,R., SPARK Team: 2012, Millimeter-Wave Band Monitoring
Observations of Solar System Planetary Atmospheres with an
Exclusive Ground-Based 10m-Telescope for SPART Project,
New Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 151.
Makise, K., Terai, H., Yamashita, T., Miki, S., Wang, Z., Uzawa,
Y., Ezaki, S., Odou, T., Shinozaki, B.: 2012, Fluctuation
conductance and the Berezinskii-Kosterlitz-Thouless transistionin two dimensional epitaxial NbTiN ultra-thin films, J. Phys.:Conf. Ser., 400, 022064.
Martinache, F., Guyon, O., Clergeon, C., Garrel, V., Blain.,C.: 2012, The Subaru coronagraphic extreme AO project:
first observations, Proc. SPIE 8447, Eds. B. L. Ellerbroek, E.
Marchetti, J.-P. Veran, 84471Y.
Martinache, F.: 2012, Super resolution from diffraction limited
images with kernel-phases, Proc. SPIE 8445, Eds. F. Delplancke,
J. K. Rajagopal, F. Malbet, 844504.
Maruyama, T., Kajino, T., Yasutake, N., Cheoun, M. K., Ryu,
C. Y.: 2012, Asymmetric neutrino reaction and pulsar kick inmagnetized oroto-neutron stars in fully relativistic framework,
AIP Conf. Proc. 1441, Eds. S. G. Steadman, G. S. F. Stephans, F.
E. Taylor, 393-395.
Maruyama, T., Kajino, T., Yasutake, N., Cheoun, M. K., Ryu, C.
Y.: 2012, Asymmetric Neutrino Reaction in Magnetized ProtoNeutron Stars in Fully Relativistic Approach, Int. Conf. on
Hadron Nuclear Physics 2011 (HNP2011): Quarks in Hadrons,
Nuclei, and Hadronic Matter, Pohang, Korea, Eds. H.-C. Kim, S.

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Nam, EPJ Vol.20, id.04003.
Maruyama, T., Kajino, T., Yasutake, N., Hidaka, J., Cheoun, M.
K., Ryu, C. Y., Mathews, G. J.: 2012, Asymmetric Neutrino
Reaction and Pulsar Kick in Magnetized Proto-Neutron Stars
in Fully Relativistic Framework, AIP Conf. Proc. 1484, Eds. S.
Kubono, T. Hayakawa, T. Kajino, H. Miyatake, T. Motobayashi,
K. Nomoto, 333-338.
Mathews, G. J., Cheoun, M. K., Kajino, T., Kusakabe, M.,
Yamazaki, D. G.: 2012, Frontiers of Big-Bang Cosmology
and Primordial Nucleosynthesis, AIP Conf. Proc. 1484, Eds. S.
Kubono, T. Hayakawa, T. Kajino, H. Miyatake, T. Motobayashi,
K. Nomoto, 339-347.
Matsui, K., Sorai, K., Watanabe, Y., Kuno, N.: 2012, Detection of
CO(J = 1–0) Emission from Barred Spiral Galaxies at z ~ 0.1,
New Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 92.
Matsumoto, N., Honma, M.: 2012, The bar effect in the galactic gas
motions traced by 6.7 GHz methanol maser sources with VERA,
Cosmic Masers - from OH to H0, Proc. IAU Symp. 287, Eds. R. S.
Booth, E. M. L. Humphreys, W. H. T. Vilemmings, 419-420.
Matsuo, H.: 2012, Photon Counting Terahertz Interferometry,
ISSTT Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, C-24.
Matsuo, T., Kotani, T., Murakami, N., Kawahara, H., Fujii,Y., Oya, S., Kurita, M., Natsume, N., Narita, N., Takizawa,
K., Ikoma, M., Minagawa, J., Baba, N., Tamura, M.: 2012,
Second-Earth imager for TMT (SEIT): concept and its
numerical simulation, Proc. SPIE 8446, Eds. I. S. McLean, S. K.
Ramsay, H. Takami, 84461K.
Matumoto, N., Honma, M.: 2013, 3D motions of 6.7 GHz
methanol masers and effects of the Galactic bar, Advancing thePhysics of Cosmic Distances, Proc. IAU Symp. 289, Eds. R. de
Grijs, 410-413.
Mawet, D., et al. including Guyon, O.: 2012, Review of smallangle coronagraphic techniques in the wake of ground-based
second-generation adaptive optics systems, Proc. SPIE 8442,
Eds. M. C. Clampin, G. G. Fazio, H. A. MacEwen, J. M.
Oschmann, Jr., 844204.
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.: 2012, Direct
Imaging of Bridged Twin Protoplanetary Disks in a Young
Multiple Star, From Interacting Binaries to Exoplanets:
Essential Modeling Tools, Proc. IAU Symp. 282, Eds. M.
Richards, I. Hubeny, 425-428.
McElwain, M. W., Brandt, T. D., Janson, M., Knapp, G. R., Peters, M.
A., Burrows, A. S., Carlotti, A., Carr, M. A., Groff, T., Gunn, J. E.,
Guyon, O., Hayashi, M., Kasdin, N. J., Kuzuhara, M., Lupton,
R. H., Martinache, F., Spiegel, D., Takato, N., Tamura, M.,
Turner, E. L., Vanderbei, R. J.: 2012, Scientific design of a highcontrast integral field spectrograph for the Subaru Telescope,Proc. SPIE 8446, Eds. I. S. McLean, S. K. Ramsay, H. Takami,
84469C.
Meech, K., Valsecchi, G., Bowell, E L., Bockelee-Morvan, D., Boss, A.,
Cellino, A., Consolmagno, G., Fernandez, J., Irvine, W., Lazzaro,D., Michel, P., Noll, K., Schulz, R., Watanabe, J., Yoshikawa,
M., Zhu, J.: 2012, Division III: Planetary Systems Sciences,Transactions IAU, Vol. 7, Issue T28A, Ed. I. Corbet, 125-137.
Melnikov, V. F., Pyatakov, N. P., Shibasaki, K.: 2012, Constraints
for Electron Acceleration Models in Solar Flares fromMicrowave Observations with High Spatial Resolution, ASP
Conf. Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 321-324.
Méndez, R. H., Teodorescu, A. M., Hattori, T., Magrini, L.,
Johnson, L. C.: 2012, Planetary nebula spectra in M 60 and M 82,
Planetary Nebulae: An Eye to the Future, Proc. IAU Symp. 283,
Eds. A. Manchado, L Stanghellini, D Schönberner, 434-435.
Minowa, Y., Hayano, Y., Terada, H., Pyo, T.-S., Oya, S., Hattori,
M., Shirahata, M., Takami, H., Guyon, O., Garrel, V.,
Colley, S., Weber, M., Golota, T., Watanabe, M., Saito, Y., Ito,
M., Iye, M.: 2012, Subaru laser guide adaptive optics system:
performance and science operation, Proc. SPIE 8447, Eds. B. L.
Ellerbroek, E. Marchetti, J.-P. Veran, 84471F.
Miura, N., Miyazaki, J., Kuwamura, S., Baba, N., Hanaoka, Y.,
Yamaguchi, M., Ueno, S., Nakatani, Y., Nagata, S., Kitai, R.,
Ichimoto, K., Takami, H.: 2012, Solar adaptive optics at the
Hida Observatory: latest achievements of current system anddesign of new system, Proc. SPIE 8447, Eds. B. L. Ellerbroek, E.
Marchetti, J.-P. Veran, 84474D.
Miyamoto, Y., Nakai, N., Kuno, N.: 2012, Disruption of Giant
Molecular Associations by Shear Motion in the Spiral Galaxy
M51, New Trends in Radio Astronomy in the ALMA Era: The
30th Anniversary of Nobeyama Radio Observatory, 94.
Miyata, T., et al. including Takato, N.: 2012, Evaluations of
new atmospheric windows at thirty micron wavelengths for
astronomy, Proc. SPIE 8446, Eds. I. S. McLean, S. K. Ramsay,
H. Takami, 84446B.
Miyazaki, S., et al. including Komiyama, Y., Nakaya, H.,
Kamata, Y., Doi, Y., Hamana, T., Karoji, H., Furusawa, H.,
Kawanomoto, S., Nariai, K., Tanaka, Y., Uraguchi, F., Utsumi,Y., Obuchi, Y., Okura, Y., Takata, T., Tomono, D., Kurakami,T., Namikawa, K., Usuda, T., Yamanoi, H., Terai, T., Uekiyo, H.,
Yamada, Y., Koike, M.: 2012, Hyper Suprime-Cam, Proc. SPIE
8446, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 84460Z.
Momose, R., Koda, J., Kennicutt, R. C., Egusa, F., Okumura, S. K.,
Clazetti, D., Liu, G., Donovan Meyer, J., Scoville, N. Z., Sawada,T., Kuno, N.: 2013, The Resolved Kennicutt-Schmidt Law in
Nearby Galaxies, Molecular Gas, Dust, and Star Formation, Proc.
IAU Symp. 292, Eds. T. Wong, J. Ott, 335-335.
Morita, S., Shibata, K., Ueno, S., Ichimoto, K., Kitai, R., Otsuji,
K.: 2012, Chromospheric Anemone Jets Observed with Hinode/
SOT and Hida CaII Spectroheliograph, ASP Conf. Ser., 454,
Eds. T. Sekii, T. Watanabe, T. Sakurai, 95-98.
Moritani, Y., Nogami, D., Okazaki, A. T., Imada, A., Kambe, E.,
Honda, S., Hashimoto, O., Ichikawa, K.: 2012, The Be Disk
Structure in A 0535+262/V725 Tau During the X-Ray Giant
Outburst, ASP Conf. Ser., 464, Eds. A. Carciofi, Th. Rivinius,
285-291.
Moriya, T. J., Blinnikov, S. I., Tominaga, N., Yoshida, N., Tanaka,
M., Maeda, K., Nomoto, K.: 2012, Type IIn superluminous
supernovae from collision of supernova ejecta and dense
circumstellar medium, AIP Conf. Proc. 1480, Eds. M. Umemura
K. Omukai, 391-393.
Morokuma, T., et al. including Tominaga, N., Tanaka, M., Ukita, N.,

Sako, S., Matsunaga, N., Doi, M., Kobayashi, N., Miyata, T.,
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Telegrams, Ed. D. W. E. Green, 3126, 1.
Morokuma, T., et al. including Tominaga, N., Mori, K., Tanaka, M.,
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Bureau Electronic Telegrams, 3139, 2.
Morokuma, T., et al. including Tominaga, N., Mori, K., Tanaka, M.,
Ukita, N., Sako, S., Matsunaga, N., Doi, M., Kobayashi, N.,
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Telegrams, 3145, 2.
Morokuma, T., et al. including Tanaka, M.: 2013, Supernova
2013Y, Central Bureau Electronic Telegrams, Ed. D. W. E. Green,
3414, 1.
Motogi, K., Sorai, K., Fujisawa, K., Sugiyama, K., Honma, M.:
2012, Intermittent maser flare around the high-mass youngstellar object G353.273+0.641, Cosmic Masers - from OH
to H0, Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L.
Humphreys, W. H. T. Vilemmings, 98-102.
Murakami, N., Kida, M., Baba, N., Matsuo, T., Kotani, T.,
Kawahara, H., Fujii, Y., Tamura, M.: 2012, Development of theSavart-plate lateral-shearing interferometric nuller for exoplanet(SPLINE), Proc. SPIE 8446, Eds. I. S. McLean, S. K. Ramsay, H.
Takami, 84468H.
Murakami, N., Nishikawa, J., Traub, W. A., Mawet, D., Moody,
D. C., Kern, B. D., Trauger, J. T., Serabyn, E., Hamaguchi, S.,
Oshiyama, F., Sakamoto, M., Ise, A., Oka, K., Baba, N., Murakami,
H., Tamura, M.: 2012, Coronagraph focal-plane phase masks
based on photonic crystal technology: recent progress andobservational strategy, Proc. SPIE 8442, Eds. M. C. Clampin, G.
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Muraoka, K., Matsui, K., Akashi, T., Kuno, N., Iwashita, H.,
Miyazawa, C., Koyano, M., Baji, H., Maekawa, J., Nakajima,T., Onodera, S., Sakai, T., Kiura, K., Maezawa, H., Onishi,T., Ogawa, H.: 2012, Test Observations of a New 100 GHz
Wave-Band FOur-Beam REceiver System on the Nobeyama
45-m Telescope (FOREST), New Trends in Radio Astronomy
in the ALMA Era: The 30th Anniversary of Nobeyama Radio
Observatory, 177.
Nagashima, K., Parchevsky, K. V., Zhao, J., Duvall, T. L. Jr.,
Kosovichev, A. G., Sekii, T.: 2012, Effects of Spectral Line
Formation Height in Time-Distance Helioseismology, The Fifth
Hinode Science Meeting: Exploring the Active Sun, Eds. L.
Golub, I. De Moortel, T. Shimizu, 57.
Nagashima, K., Zhao, J., Kosovichev, A. G., Sekii, T.: 2012, LocalHelioseismology Study of Supergranulation in the Polar Region,
ASP Conf. Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 19.
Nagayama, T.: 2012, Astrometry of Galactic Star-Forming
Regions ON1 and ON2N with VERA, Cosmic Masers - fromOH to H0, Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L.
Humphreys, W. H. T. Vilemmings, 391-395.
Nagayama, T.: 2013, VERA observations of the Galactic star-forming
regions ON1 and ON2N, Advancing the Physics of Cosmic
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Nakajima, T., Kimura, K., Katase, T., Koyano, M., Inoue, H.,
Sakai, T., Iwashita, H., Miyazawa, C., Asayama, S., Kuno,

II Publications, Presentations085

N., Ogawa, H., Onishi, T., Kawabe, R., Noguchi, T.: 2012,
Development of a New Multi-Beam Array 2SB Receiver in
100 GHz Band for the NRO 45-m Radio Telescope, ISSTT
Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, P-12.
Nakajima, T., Takano, S., Kohno, K., the Line Survey Team: 2012,
Nobeyama 45 m Telescope Legacy Project: Line Survey of
Galaxies, New Trends in Radio Astronomy in the ALMA Era:
The 30th Anniversary of Nobeyama Radio Observatory, 104.
Nakamrua, K., Takiwaki, T., Kotake, K., Nishimura, N.: 2012,
Supernova shock revival by nuclear reactions, Origin of Matterand Evolution of Galaxies 2011, Eds. S. Kubono, T. Hayakawa, T.
Kajino, H. Miyatake, T. Motobayashi, K.-I. Nomoto, 439-441.
Nakamura F., Ogawa, H., Kameno, S., Kimura, K., Mizuno, I.,
Tokuda, K., Takatsu, M., Iono, D., Takano, S., Dobashi, K.,
Matsumoto, T., Kuno, N., Kawabe, R., Onishi, T., Momose,
M., Shinnaga, H., Tanaka, T., Yamamoto, S., Maezawa, H.,
Hirota, T.: 2012, The CCS 45 GHz Zeman Project: Magnetic
Field Measurements towards Prestellar Cores, New Trends inRadio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 75.
Nakamura, F., Li, Z.-Y.: 2012, Present-Day Star Formation:
Protostellar Outflows and Clustered Star Formation, AIP Conf.
Proc. 1480, Eds. M. Umemura K. Omukai, 30-37.
Nakamura, F., Li, Z.-Y.: 2012, The Roles of Protostellar Outflow
Feedback in Clustered Star Formation, Molecular Gas, Dust, andStar Formation, Proc. IAU Symp. 292, Eds. T. Wong, J. Ott, 54.
Nakamura, K., Harikae, S., Kajino, T., Mathews, G. J.: 2012,
r-process nucleosynthesis in the neutrino-heated relativisticcollapsar jet model for gamma-ray bursts, 12th Int. Symp. on
Nuclei in the Cosmos (NIC12), Cairns, Proc. of Science (NIC XII),
Eds. J. Lattanzio, A. Karakas, M. Lugaro, G. Dracoulis, 216.
Nakamura, K., Harikae, S., Kajino, T., Mathews, G. J.: 2012,
Long Gamma-ray burst as a Production Site of R-process
Elements, AIP Conf. Proc. 1484, Eds. S. Kubono, T. Hayakawa,T. Kajino, H. Miyatake, T. Motobayashi, K. Nomoto, 301-306.
Nakamura, K., Hayakawa, T., Cheoun, M. K., Chiba, S., Kajino,T., Mathews, G. J.: 2012, Radioactivities from Supernovae and
Its Application to Cosmochronology, ASP Conf. Ser., 458, Eds.
W. Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 17-20.
Nakamura, K., Takiwaki, T., Kotake, K., Nishimura, N.: 2012,
Neutrino-driven supernova explosions powered by nuclear
reactions, The Death of Massive Stars: Supernovae and GammaRay Bursts, Proc. IAU Symp. 279, Eds. P. W. A. Roming, N.
Kawai, E. Pian, 365-366.
Nakanishi, K., Sorai, K., Kuno, N., Tosaki, T., Kohno, K., Nakai,
N.: 2012, Star-Formation Types and Molecular Gas in Nearby
Spiral Galaxy NGC 253: Suggestion for High-Redshift StarFormation Activities, New Trends in Radio Astronomy in
the ALMA Era: The 30th Anniversary of Nobeyama Radio
Observatory, 105.
Nakaya, H., Miyatake, H., Uchida, T., Fujimori, H., Mineo, S.,
Aihara, H., Furusawa, H., Kamata, Y., Karoji, H., Kawanomoto,S., Komiyama, Y., Miyazaki, S., Morokuma, T., Obuchi, Y.,
Okura, Y., Tanaka, M., Tanaka, Y., Uraguchi, F., Utsumi, Y.:
2012, Hyper Suprime-Cam: performance of the CCD readout
electronics, Proc. SPIE 8453, Eds. A. D. Holland, J. W. Beletic,

086

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84532R.
Naruse, M., Sekimoto, Y., Miyachi, A., Uzawa, Y., Nitta, T.,
Karatsu, K., Sekine, M., Noguchi, T.: 2012, Developmentof a MKID camera with high-quality Al films for millimeterwave astronomy, ISSTT Proceedings 2012, Eds. H. Matsuo, Y.
Sekimoto, P-52.
Niino, Y.: 2012, Revisiting Metallicity of Long Gamma-Ray
Burst Host Galaxies: The Role of Chemical Inhomogeneities in
Galaxies, The Death of Massive Stars: Supernovae and GammaRay Bursts, Proc. IAU Symp. 279, Eds. P. W. A. Roming, N.
Kawai, E. Pian, 369-370.
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani,T., Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.,
Murakami, H.: 2012, A coronagraph system with unbalanced
nulling interferometer: progress of dynamic range, Proc. SPIE
8442, Eds. M. C. Clampin, G. G. Fazio, H. A. MacEwen, J. M.
Oschmann, Jr., 84425D.
Nishizuka, N., Hara, H.: 2012, Spectroscopic Observations ofContinuous Outflows and Propagating Waves in Active Region
NOAA 10942 with Hinode/EIS, The 4th Hinode Science
Meeting: Unsolved Problems and Recent Insights , Rubio, L. R.,
Reale, F., Carlsson, M., 219.
Nishizuka, N., Matsumoto, T., Morita, S., Hara, H., Shibata, K.:
2012, Propagating Slow Magnetoacoustic Waves along theContinuous Outflows Observed with EIS/Hinode, ASP Conf.
Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 157-161.
Nitta, T., Naruse, M., Sekimoto, Y., Mitsui, K., Okada, N., Karatsu,
K., Sekine, M., Matsuo, H., Noguchi, T., Uzawa, Y., Seta, M.,
Nakai, N.: 2012, Development of Direct Machined Silicon Lens
Array for Millimeter-wave Kinetic Inductance Detector Camera,
ISSTT Proceedings 2012, Eds. H. Matsuo, Y. Sekimoto, C-22.
Norris, B. R. M., Tuthill, P. G., Ireland, M. J., Lacour, S., Zijlstra, A.
A., Lykou, F., Evans, T. M., Stewart, P., Bedding, T. R., Guyon, O.,
Martinache, F.: 2012, Probing dusty circumstellar environmentswith polarimetric aperture-masking interferometry, Proc. SPIE
8445, Eds. F. Delplancke, J. K. Rajagopal, F. Malbet, 844503.
Obuchi, Y., Komiyama, Y., Kamata, Y., Kawanomoto, S.,
Miyazaki, S., Morokuma, T., Nakaya, H., Uraguchi, F.,
Utsumi, Y.: 2012, Hyper Suprime-Cam: implementation andperformance of the cryogenic dewar, Proc. SPIE 8446, Eds. I. S.
McLean, S. K. Ramsay, H. Takami, 84466Q.
Ohashi, S., Kitamura, Y., Akashi, T.: 2012, Mapping Observationsof the NH3 (1,1), (2,2) and (3,3) in the Horsehead Nebula andthe NGC 2023 Region with the Nobeyama 45 m Telescope,
New Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 130.
Ohishi, M., Hanisch, R. J., Norris, R. P., Andernach, H., Bishop,M., Griffin, E., Kembhavi, A., Murphy, T., Pasian, F.: 2012,
Commission 5: Documentation and Astronomical Data,
Transactions IAU, Vol. 7, Issue T28A, Ed. I. Corbet, 327-334.
Ohishi, M.: 2013, Annual Report for 2012 of IUCAF, Radio
Science Bulletin, 344, 11-12.
Ohta, K., Yabe, K., Iwamuro, F., Yuma, S., Akiyama, M., Tamura,N.: 2012, Stellar-Mass Metallicity Relation at z ~ 1.4, ASP Conf.
Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N.
Arimoto, 87.

Oi, N., Imanishi, M.: 2012, Evolution of Luminous Infrared
Galaxies by Near-Infrared Multi-Band Imaging of their Hosts,
Publ. Korean Astron. Soc., 27, 301-303.
Okamoto, T. J., Tsuneta, S., Berger, T. E., Lites, B. W.: 2012,
Emergence of Twisted Flux in Prominence Observations, The
4th Hinode Science Meeting: Unsolved Problems and Recent
Insights , Rubio, L. R., Reale, F., Carlsson, M., 123.
Olguin, R., Shen, T., Brito, R., Saez, A., Soto, R., Asayama, S.,
Follert, C., Knee, L., Quintana, A., Rabanus, D., Reynolds,
E., Saez, N., Sepulveda, J.: 2012, Development of the test
interferometer for ALMA, Proc. SPIE 8452, Eds. W. S. Holland,
J. Zmuidzinas.
Onodera, S., Kuno, N., Tosaki, T., Muraoka, K., Miura, R.,
Kohno, K., Nakanishi, K., Sawada, T., Komugi, S., Kaneko,
H., Hirota, A., Kawabe, R.: 2012, NRO M33 All-Disk Surveyof Giant Molecular Clouds (NRO MAGiC): Properties of Giant
Molecular Clouds in M33, New Trends in Radio Astronomy
in the ALMA Era: The 30th Anniversary of Nobeyama Radio
Observatory, 10.
Oota, T., Shinonaga, H., Akutsu, K., Hashimoto, Y., Otsuka, I.,
Iwasaki, Y., Iye, M., Yamashita, T., Akitaya, H., Suzuki,
R.: 2012, Test production of a mirror segment for the Thirty
Meter Telescope, Proc. SPIE 8450, Eds. R. Navarro, C. R.
Cunningham, E. Prieto, 2.
Orozco Suárez, D., Bellot Rubio, L. R., Katsukawa, Y.: 2012,
Requirements for the Analysis of Quiet-Sun Internetwork
Magnetic Elements with EST and ATST, ASP Conf. Ser., 463,
Eds. T. Rimmele, A. Tritschler, F. Wöger, V. Collados, H.
Socos-Navarro, R. Schlichenmaier, M. Carlsson, T. Berger, A.
Cadavid, P. Gilbert, P. Goode, M. Knölker, 57.
Otsuka, M., Kemper, F., Sargent, B., Hyung, S., Meixner, M.,
Tajitsu, A., Yanagisawa, K.: 2012, Dust and Chemical
Abundances of the Young Planetary Nebula M1-11; First
Detection of Fullerenes C60, ASP Conf. Ser., 458, Eds. W. Aoki,
M. Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 137.
Oya, M., Nishikawa, J., Horie, M., Murakami, N., Kotani, T., Abe,L., Kumagai, S., Tamura, M., Kurokawa, T., Murakami, H.:
2012, Adaptive optics operation with two wavefront sensors in acoronagraph for exoplanet observations, Proc. SPIE 8442, Eds.
M. C. Clampin, G. G. Fazio, H. A. MacEwen, J. M. Oschmann,
Jr., 844255.
Oya, S., Akiyama, M., Hayano, Y., Minowa, Y., Iwata, I., Terada,
H., Usuda T., Takami H., Nishimura, T., Kodama, T., Takato,N., Tomono, D., Ono, Y.: 2012, A preliminary simulation resultof the next-generation wide-field AO at Subaru Telescope, Proc.
SPIE 8447, Eds. B. L. Ellerbroek, E. Marchetti, J.-P. Veran,
84473V.
Ozaki, S., Kitagawa, Y., Motohara, K., Konishi, M., Takahashi,
H., Yoshikawa, T., Tateuchi, K., Kato, N.: 2012, Developmentof an integral field unit for a near-infrared multi-object imaging
spectrograph SWIMS, Proc. SPIE 8450, Eds. R. Navarro, C. R.
Cunningham, E. Prieto, 84503Y.
Ozaki, S., Tanaka, Y., Hattori, T., Mitsui, K., Fukusima, M.,
Okada, N., Obuchi, Y., Miyazaki, S., Yamashita, T.: 2012,
Development of a slicer integral field unit for the existing
optical imaging spectrograph FOCAS, Proc. SPIE 8450, Eds. R.

Navarro, C. R. Cunningham, E. Prieto, 84501L.
Pan, H.-A., Kuno, N., Hirota, A.: 2012, Kennicutt-Schmidt Law
from nearby Galactic Center to the Disk: On the Aspect of
13CO, New Trends in Radio Astronomy in the ALMA Era: The
30th Anniversary of Nobeyama Radio Observatory, 95.
Parthasarathy, M., Jasniewicz, G., Aoki, W., Takeda, Y.: 2012, UV
Bright Stars in Globular Clusters, ASP Conf. Ser., 458, Eds. W.
Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 237-239.
Peters, M. A., Groff, T., Kasdin, N. J., McElwain, M. W., Galvin, M.,
Carr, M. A., Lupton, R., Gunn, J. E., Knapp, G., Gong, Q., Carlotti,A., B., Janson, M., Guyon, O., Martinache, F., Hayashi, M.,
Takato, N.: 2012, Conceptual design of the Coronagraphic High
Angular Resolution Imaging Spectrograph (CHARIS) for the
Subaru telescope, Proc. SPIE 8446, Eds. I. S. McLean, S. K.
Ramsay, H. Takami, 84467U.
Reznikova, V. E., Melnikov, V. F., Shibasaki, K.: 2012, Microwave
Diagnostics of the Acceleration Site Position and Pitch-Angle
Anisotropy of Energetic Electrons in the Flare 24 Aug 2002,
ASP Conf. Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai,
325-328.
Saito, M., Inatani, J., Nakanishi, K., Saito, H., Iguchi, S.: 2012,
Atacama compact array antennas, Proc. SPIE 8444, Eds. L. M.
Stepp, R. Gilmozzi, H. J. Hall, 84443H.
Saito, Y., Yatsu, Y., Nakajima, H., Kawai, N., Asano, K., Aoki, Y.,
Hayashi, M., Song, S., Kawakami, K., Tokoyoda, K., Enomoto, T.,
Usui, R., Kuroda, D., Yanagisawa, K., Shimizu, H., Toda, H.,
Nagayama, S., Hanayama, H., Yoshida, M., Ohta, K.: 2012,
Study of very early phase GRB afterglows with MITSuME, The
Death of Massive Stars: Supernovae and Gamma-Ray Bursts,
Proc. IAU Symp. 279, Eds. P. W. A. Roming, N. Kawai, E.
Pian, 387-388.
Sakai, N., Honma, M., Nakanishi, H., Sakanoue, H., Kurayama,
T.: 2012, Mass distribution of the Galaxy with VERA, Cosmic
Masers - from OH to H0, Proc. IAU Symp. 287, Eds. R. S.
Booth, E. M. L. Humphreys, W. H. T. Vilemmings, 421-422.
Sakai, N., Honma, M., Nakanishi, H., Sakanoue, H., Kurayama, T.:2012, Measurement of a Rotation Velocity of the Outer Galaxy
with VERA: Mass Distribution of the Galaxy, ASP Conf. Ser.,458, Eds. W. Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N.
Arimoto, 243-243.
Sakai, N., Honma, M., Nakanishi, H., Sakanoue, H., Kurayama,
T.: 2013, The outer rotation curve project with VERA:
Trigonometric parallax of IRAS 05168+3634, Advancing thePhysics of Cosmic Distances, Proc. IAU Symp. 289, Eds. R. de
Grijs, 95-98.
Sakao, T., Narukage, N., Imada, S., Suematsu, Y., Shimojo, M.,
Tsuneta, S., DeLuca, E. E., Watanabe, K., Ishikawa, S.: 2012,
The x-ray/EUV telescope for the Solar-C mission: science anddevelopment activities, Proc. SPIE 8443, Eds. T. Takahashi, S. S.
Murray, J.-W. A. den Herder, 84430A.
Sakari, C. M., Venn, K. A., Irwin, M., Aoki, W., Arimoto, N.,
Dotter, A.: 2012, Detailed Chemical Abundances of Four Stars
in the Unusual Globular Cluster, Palomar 1, ASP Conf. Ser.,458, Eds. W. Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N.
Arimoto, 247-248.
Sako, N., Shimojo, M., Kitabayashi, T.: 2012, Statistical StudyII Publications, Presentations087

of X-ray Jets in the Polar Region, ASP Conf. Ser., 454, Eds. T.
Sekii, T. Watanabe, T. Sakurai, 153-156.
Sako, S., Aoki, T., Doi, M., Ienaka, N., Kobayashi, N., Matsunaga,N., Mito, H., Miyata, T., Morokuma, T., Nakada, Y., Soyano, T.,
Tarusawa, K., Miyazaki, S., Nakata, F., Okada, N., Sarugaku,
Y., Richmond, M. W.: 2012, KWFC: four square degrees
camera for the Kiso Schmidt Telescope, Proc. SPIE 8446, Eds. I.
S. McLean, S. K. Ramsay, H. Takami, 84466L.
Sakon, I., Kataza, H., Onaka, T., Ohsawa, R., Okada, Y., Ikeda, Y.,
Fujishiro, N., Mitsui, K., Okada, N.: 2012, Recent progressin the development of mid-infrared medium resolution
spectrometer (MRS) installed in SPICA/MCS, Proc. SPIE
8442, Eds. M. C. Clampin, G. G. Fazio, H. A. MacEwen, J. M.
Oschmann, Jr., 84423S.
Sakurai, T.: 2012, Sixty Years of Norikura Solar Observatory, ASP
Conf. Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 439.
Sakurai, T.: 2012, Helioseismology, Dynamo, and Magnetic
Helicity, ASP Conf. Ser., 462, Eds. H. Shibahashi, M. Takata, A.
E. Lynas-Gray, 247.
Sasaki, S., Ishihara, Y., Goossens, S., Araki, H., Matsumoto, K.,
Noda, H., Hanada, H., Kikuchi, F., Namiki, N., Iwata, T.,
Kunimori, H., Otsubo, T., Funazaki, K.: 2012, New Scientific
Observations in Lunar and Planetary Exploration, New
Scientific Observations in Lunar and Planetary Exploration,
Macau University of Science and Technology, 8-17.
Sato, M., Hirota. T., Honma, M., Kobayashi, H.: 2012, VERA
astrometry of the Galactic Superbubble NGC 281, The Roleof the Disk-Halo Interaction in Galaxy Evolution: Outflow vs.
Infall?, EAS Publ. Ser. 56, Ed. M. A. de Avillez, 151-154.
Sato, M., Watanabe, J., NAOJ Campaign Team: 2011, Meteor
Shower Activity Derived from "Meteor Watching PublicCampaign" in Japan, Meteoroids: The Smallest Solar System
Bodies, Eds. W. J. Cooke, D. E. Moser, B. F. Hardin, D.
Janches, 31.
Sawada-Satoh, S., Fujisawa, K., Sugiyama, K., Wajima, K.,
Honma, M.: 2012, Internal Proper Motion of 6.7 GHz Methanol
Masers in Ultra Compact HII Region S269, Cosmic Masers from OH to H0, Proc. IAU Symp. 287, Eds. R. S. Booth, E. M. L.
Humphreys, W. H. T. Vilemmings, 188-189.
Scott, K. S., Wilsson, G. W., Aretxaga, I., Austermann, J. E., Chapin,
E. L., Dunlop, J. S., Ezawa, H., Halpern, M., Hatsukade, B.,
Hughes, D. H., Kawabe, R., Kim, S., Kohno, K., Lowenthal, J.
D., Montana, A., Nakanishi, K., Oshima, T., Sanders, D., Scott,D., Scoville, N., Tamura, Y., Welch, D., Yun, M. A., Zeballos, M.:
2012, The Source Counts of Submillimeter Galaxies Detector at
λ=1.1 mm, AAS Meeting #220, #308.03.
Seta, M., Nakai, N., Ishii, S., Nagai, M., Miyamoto, Y., Ichikawa,T., Takato, N., Motoyama, H.: 2013, Dome Fuji in Antarctica
as a Site for Infrared and Terahertz Astronomy, Astrophysics
from Antarctica, Proc. IAU Symp. 288, Eds. T. Montmerle, I. F.
Corbett, U. Grothkopf, C. Sterken, 251-255.
Shibasaki, K.: 2012, The Flare on December 13, 2006 and theStandard Solar Flare Model, ASP Conf. Ser., 454, Eds. T. Sekii,
T. Watanabe, T. Sakurai, 315-320.
Shimajiri, Y., Kawabe, R., Sakai, T., Kitamura, Y., Momose, M.,
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Shimizu, T., Sakao, T., Katsukawa, Y., Group, J. S. W.: 2012, The
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Shimojo, M.: 2012, The Event Detection and the Apparent
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Shino, N., Fujisawa, K., Sugiyama, K., Honma, M., Deguchi,
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Shiota, D., Tsuneta, S., Ito, H., Kusano, K., Nishikawa, N., Suzuki,
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Shirahata, M., Usuda, T., Oyabu, S., Nakagawa, T., Yamamura,I.: 2012, Near-Infrared High-Resolution Spectroscopy of the
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Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto, Y., Ishihara,Y., Tsutsumi, J., Hiyama, T., Nakamoto, H., Sakamoto, M.:
2012, Current Status of VO Compliant Data Service in Japanese
Virtual Observatory, ASP Conf. Ser., 461, Eds. P. Ballester, D.
Egret, N. P. F. Lorente, 451-454.
Shoda, A., Ando M., Okada, K., Ishidoshiro, K., Kokuyama,
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Sivaramakrishnan, A., Lafreniere, D., Ford, K. E. S., McKernan,
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Suda, T., Hirschi, R., Fujimoto, M. Y.: 2012, Triple-alpha Reaction
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Suda, T.: 2012, SAGA: Stellar Abundances for Galactic Archaeology,
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Suematsu, Y., Katsukawa, Y., Shimizu, T., Ichimoto, K., Takeyama,
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Electron capture reactions and beta-decays in astrophysicalprocesses, 12th Int. Symp. on Nuclei in the Cosmos (NIC12),
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Takahashi, S., Deguchi, S., Kuno, N., Hamura, T., Pogrebenko, S.
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Takano, S., Aikawa, Y., Chen, V., Hirano, N., Hirota, T., Kamegai,
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Roming, N. Kawai, E. Pian, 409-410.
Takiwaki, T., Kotake, K., Suwa, Y.: 2012, Three-dimensionalhydrodynamic core-collapse supernova simulations for an 11.2
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Tanaka, M., Chiba, M., Komiyama, Y., Guhathakurta, P., Kalirai, J.
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Onishi, T., Ogawa, H., Nakamura, F., Kuno, N., Takano, S.,
Iono, D., Kawabe, R., Kameno, S.: 2012, A New 45 GHz Band
Receiver with Dual Polarization for NRO 45-m Telescope,
New Trends in Radio Astronomy in the ALMA Era: The 30th
Anniversary of Nobeyama Radio Observatory, 165.
Tokudome, T., Sakai, N., Sakai, T., Takano, S., Yamamoto, S.,
NRO Line Survey Project Members: 2012, Nobeyama 45m
Telescope Legacy Project: Line Survey of L1527, New Trends
in Radio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 136.
Tosaki, T., Miura, R., Kohno, K., Kuno, N., Onodera, S., MAGiC
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Era: The 30th Anniversary of Nobeyama Radio Observatory, 108.
Tóth, L. V., Zahorecz, S., Marton, G., Onishi, T., Balázs, L.
G., Fehér, O., Kawamura, A., Kitamura, Y., Lisztes, M.,
Nishimura, A., Pásztor, L., Pintér, S., Racz, I., Tamura, M.,
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292, Eds. T. Wong, J. Ott, 113.
Toujima, H., Handa, T., Omodaka, T., Nagayama, T., Kobayashi,
H., Koyama, Y.: 2013, Propagation of Highly EfficientStar Formation in the North American Nebula (NGC 7000),
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Tsuboi, M., Asaki, Y., Yonekura, Y., Kaneko, H., Miyamoto, Y.,
Seta, M., Nakai, N., Kameya, O., Miyoshi, M., Takaba, H.,
Wakamatsu, K., Fukuzaki, Y., Morimitsu, T., Sekido, M.,
Omodaka, T., Handa, T., Takumi, A.: 2013, Non-detection offlare at 22 GHz of Sgr A* induced by the approaching G2 cloudin February and March 2013, The Astronomer's Telegram, 4923.
Tsujimoto, T.: 2013, Galactic Chemical Evolution in the Context
of the Recently Revealed SNe Ia Delay Time Distribution,
Binary Paths to Type Ia Supernovea Explosions, Proc. IAU
Symp. 281, Eds. R. Di Stefano, M. Orio, M. Moe, 251-252.
Unwin, S., Traub, W., Bryden, G., Brugarolas, P., Chen, P., Guyon,
O., Hillenbrand, L., Krist, J., Macintosh, B., Mawet, D.,
Mennesson, B., Moody, D., Roberts, L. C., Stapelfeldt, K.,
Stuchlik, D., Trauger, J., Vasisht, G.: 2012, Coronagraphic
imaging of debris disks from a high altitude balloon platform,
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MacEwen, J. M. Oschmann, Jr., 84420G.
Uraguchi, F., Wang, S.-Y., Komiyama, Y., Liaw, Eric J. Y.,
Chiu, C.-F., Chen, H.-Y., Ho, C.-L., Lai, T.-C., Lee, Y.-C.,
Jeng, D.-Z., Iwamura, S., Kamata, Y., Kawanomoto, S.,
Miyazaki, S., Morokuma, T., Nakaya, H., Utsumi, Y.: 2012,
Hyper Suprime-Cam: filter exchange unit and shutter, Proc. SPIE
8446, Eds. I. S. McLean, S. K. Ramsay, H. Takami, 844663.
Urakawa, S., Okumura, 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.: 2012, Photometric Observationsof Comet-Asteroid Transition Object 107P/Wilson-Harrington,
Asteroids, Comets, Meteors 2012, 6088.
Usuda, T., Krause, O., Tanaka, M., Hattori, T., Goto, M., Birkmann,
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Stefano, M. Orio, M. Moe, 335-336.
Usui, F., Kuroda, D., Müller, T. G., Hasegawa, S., Ishiguro, M.,
Ootsubo, T., Kasuga, T.: 2012, AKARI/IRC Mid-Infrared
Asteroid Survey, Asteroids, Comets, Meteors 2012, 6119.
Usui, F., Kuroda, D., Müller, T. G., Hasegawa, S., Ishiguro,
M., Ootsubo, T., Ueno, M., AKARI SOSOS Team: 2012, A
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Utsumi, Y., Kawanomoto, S., Tait, P., Jeschke, E., Furusawa, H.,
Kamata, Y., Koike, M., Komiyama, Y., Miyazaki, S.,
Morokuma, T., Nakaya, H., Uraguchi, F., Nakata, F.: 2012,
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van Driel, W., Green, R., Wainscoat, R. J., Alvarez del Castillo,
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50 Protection of Existing and Potential Observatory Sites,
Transactions IAU, Vol. 7, Issue T28A, Ed. I. Corbet, 408-412.
Vargas, L. C., Aoki, W.: 2012, Chemical Abundances of Upper Red
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Walker, E. S., Mazzali, P. A., Pian, E., Tanaka, M., Morokuma,
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Walker, E. S., Mazzali, P. A., Pian, E., Tanaka, M., Morokuma,
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Wanajo, S., Tachibana, T., Goriely, S.: 2012, Physical Conditions
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T. Hayakawa, T. Kajino, H. Miyatake, T. Motobayashi, K.
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Wang, S.-Y., Hu, Y.-S., Yan, C.-H., Chang, Y.-C., Tamura, N.,
Takato, N., Shimono, A., Karr, J., Ohyama, Y., Chen, H.-Y.,
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Wang, Y. P., Yamada, T., Tanaka, I., Iye, M., Ji, T.: 2013, Adaptive
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White, G., Doi, Y., Komugi, S., Kawada, M., Takita, S., Arimatsu,
K., Ikeda, N., Kato, D., Kitamura, Y., Nakagawa, T., Ootsubo, T.,
Morishima, T., Hattori, M., Tanaka, M., Etxaluze, M., Shibai, H.:
2012, The Filamentary Web of Star Formation, Publ. Korean
Astron. Soc., 27, 201-207.

Yaji, K., Tokimasa, N., Shimojo, M., Tonooka, H., Nakamichi,
A., Suzuki, D.: 2012, Education and Public Outreach Activities
with Hinode Satellite Data, ASP Conf. Ser., 454, Eds. T. Sekii, T.
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Yamada, S., Suda, T., Komiya, Y., Katsuta, Fujimoto, M. Y.:
2012, Enrichment history of elements in the galactic stars
based on the SAGA database, AIP Conf. Proc. 1480, Eds. M.
Umemura K. Omukai, 445-447.
Yamada, T., Iwata, I., Ando, M., Doi, M., Goto, T., Ikeda, Y.,
Imanishi, M., Inoue, A. K., Iwamura, S., Kawai, N., Kobayashi,
M. A. R., Kodama, T., Komiyama, Y., Kubo, M., Matsuhara,
H., Mawatari, K., Matsuoka, Y., Morokuma, T., Nakaya, H.,
Ohta, K., Okamoto, A., Oyabu, S., Sato, Y., Sugita, H., Tsutsui,R., Tokoku, C., Toshikawa, J., Tsuneta, S., Wada, T., Yabe, K.,
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surveys, Proc. SPIE 8442, Eds. M. C. Clampin, G. G. Fazio, H.
A. MacEwen, J. M. Oschmann, Jr., 84421A.
Yamada, Y., Fujita, S., Gouda, N., Kobayashi, Y., Hara, T., Nishi,R., Yoshioka, S., Hozumi, S.: 2013, Scientific goals of NanoJASMINE, Advancing the Physics of Cosmic Distances, Proc.
IAU Symp. 289, Eds. R. de Grijs, 429-432.
Yamada, Y., Hara, T., Yoshioka, S., Kobayashi, Y., Gouda, N.,
Miyashita, H., Hatsutori, Y., Lammers, U., Michalik, D.: 2012,
Nano-JASMINE Data Analysis and publication, ASP Conf. Ser.,
461, Eds. P. Ballester, D. Egret, N. P. F. Lorente, 585-588.
Yamaguchi, T., Takano, S., Sakai, N., Watanabe, Y., Yamamoto,S., NRO Line Survey Team Members: 2012, The ShockChemistry in Low-Mass Star-Forming Regions, New Trends inRadio Astronomy in the ALMA Era: The 30th Anniversary ofNobeyama Radio Observatory, 118.
Yamanaka, M., Kawabata, K. S., Maeda, K., Tanaka, M., Yoshida,M., Hattori, T., Nomoto, K., Komatsu, T., Okushima, T.: 2012,
Late-Phase Observations of a Super-Chandrasekhar SN Ia,
Binary Paths to Type Ia Supernovea Explosions, Proc. IAU
Symp. 281, Eds. R. Di Stefano, M. Orio, M. Moe, 319-321
Yamanaka, M., Kawabata, K. S., Maeda, K., Tanaka, M., Yoshida,M., Hattori, T., Nomoto, K., Komatsu, T., Okushima, T.: 2012,
Late-Phase Observations of a Super-Chandrasekhar SN Ia,
ASP Conf. Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T.
Tsujimoto, N. Arimoto, 49-50.
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Niwa, Y.,
Yamada, Y.: 2013, The scientific goal of the Japanese small
astrometric satellite, Small-JASMINE, Advancing the Physics
of Cosmic Distances, Proc. IAU Symp. 289, Eds. R. de Grijs,
433-436.
Yoshida, F., Nozawa, Y., Ito, T., Takahashi, S., Okita, K.,
Ibrahimov, M., Ehgamberdiev, S., Marshalkina, A., Karimov,
R., Burhonov, O., Tillayev, Y., Hafizov, B., Yanagisawa, T.,
Kurosaki, H., Yoshikawa, M., Urakawa, S., Ohtani, H.: 2012,
Photometric Observation of Young Asteroid Families in
2006-2010 at Maidanak Observatory, LPICo 1667, 6418.
Yung, B. H.-K., Nakashima, J., Imai, H., Deguchi, S., DiamondP., Kwok, S.: 2012, Maser Kinematics and Infrared of theWater Fountain IRAS 18286-0959, Planetary Nebulae: An
Eye to the Future, Proc. IAU Symp. 283, Eds. A. Manchado, L
Stanghellini, D Schönberner, 524-525.

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Zahorecz, S., Tóth, L. V., Marton, G., Onishi, T., Balázs, L.
G., Fehér, O., Kawamura, A., Kitamura, Y., Lisztes, M.,
Nishimura, A., Pásztor, L., Pintér, S., Rácz, I., Tamura, M.,
Sese, R. M. D., Ueno, M.: 2013, YSOs in Taurus-AurigaPerseus and Orion, Molecular Gas, Dust, and Star Formation,
Proc. IAU Symp. 292, Eds. T. Wong, J. Ott, 64-64.
Zhao, Z., Okamoto, S., Arimoto, N., Aoki, W., Kodama, T.: 2012,
Blue Straggler Stars in Dwarf Spheroidal Galaxies, ASP Conf.
Ser., 458, Eds. W. Aoki, M. Ishigaki, T. Suda, T. Tsujimoto, N.
Arimoto, 349-350.
Zharkov, S., Harra, L. K., Sekii, T.: 2012, Helioseismic Investigationof Sub-Photospheric Properties of a Coronal Hole, ASP Conf.
Ser., 454, Eds. T. Sekii, T. Watanabe, T. Sakurai, 27.

5. Publications in English
Aoki, W., Ishigaki, M., Suda, T., Tsujimoto, T., Arimoto, N.:
2012, Galactic Archaeology: Near-Field Cosmology and theFormation of the Milky Way. ASP Conf. Ser. 458, ASP, San
Francisco.
Matsuo, H. (as a Guest Editor): 2012, IEEE Transactions on
Terahertz Science and Technology Vol.3, No1, Mini Special
Issue on 23rd international Symposium on Space Terahertz
Technology, IEEE, New York.
Sekii, T., Watanabe, T., Sakurai, T.: 2012, The 3rd Hinode
Science Meeting, ASP, San Francisco.

6. Conference Presentations
Agata, H.: 2012, Introduction to Astronomy & Astronomical
Education on National Astronomical Observatory of Japan(NAOJ), You are Galileo teachers workshop, (Songkhla,
Thaland, Nov. 26, 2012).
Akiyama, E., Espada, D., Chapillon, E., Takahashi, S., Kitamura, T.,
de Gregorio-Monsalvo, I., Klaassen, P., Testi, L., Rawlings, M.,
Menard, F., Dent, W., Pinte, C., Hales, A., Cortes, P., Lopez, C.,
Tachihara, K., Higuchi, A., Corder, S., Mathews, G., Juhasz, A.,
Nyman, L., Phillips, N. M., Rodon, J., Saito, M., van Kempen,
T.: 2012, An observational study of the temperature and surface
density structures of the protoplanetary disk around HD163296,
The First Year of ALMA Science, (Puerto Varas, Chile, Dec.
12-15, 2012).
Akiyama, E., Kitamura, Y., Momose, M., Tsukagoshi, T.: 2012,
The temperature and surface density structures of a typicalfull disk around MWC 480, New Trends in Radio Astronomy
in the ALMA Era -The 30th Anniversary of Nobeyama Radio
Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Akiyama, E., Momose, M., Tsukagoshi, T., Kitamura, Y.: 2012,
Radial Density Structure of Protoplanetary Disk: Power-Law
Disk Model vs. Similarity Solution Disk Model, Revealing
Evolution of Protoplanetary Disks in the ALMA Era, (Kyoto,
Japan, May 8-11, 2012).
Akutsu, T.: 2012, DECIGO and DECIGO Pathfinder, 9th LISA
Symposium, (Paris, Francs, May 21-25, 2012).

092

II Publications, Presentations

Akutsu, T.: 2012, DECIGO Pathfinder, 11th DECIGO Workshop,(Kyoto, Japan, Nov. 27, 2012).
Akutsu, T.: 2012, Baffles in cryostat, ELiTES First Collaboration
Meeting, (Tokyo, Japan, Oct. 3-4, 2012).
Ando, M., Akutsu, T.: 2012, Stray-Light Control in Interferometers,
3rd Korea-Japan Workshop on KAGRA, (Souel, Korea, Dec.
21-22, 2012).
Ando, M., Ishidoshiro, K., Shoda, A., Okada, K., Kokuyama,W., Yagi, K., Yamamoto, K., Takahash, H., Kanda, N., Aso,Y., Matsumoto, N., Tsubono, K., Takamori, A., Gondo, R.,
Takahashi, R.: 2013, TOBA: Torsion-Bar Antenna, Gravitational
Waves: New Frontier, (Seoul, Korea, Jan. 16-18, 2013).
Ando, M.: 2012, DECIGO, 11th DECIGO Workshop, (Kyoto,
Japan, Nov. 27, 2012).
Ando, M.: 2012, Recent News from KAGRA, The 33th Program
Advisory Committee Meeting, (Hanford, USA, Nov. 8, 2012).
Ando, M.: 2012, Commissioning of TAMA, ELiTES First
Collaboration Meeting, (Tokyo, Japan, Oct. 3-4, 2012).
Ando, M.: 2012, Space Gravitational-wave observatory: DECIGO,
The Fifth International ASTROD Symposium, (Raman
Research Institute, India, Jul. 12, 2012).
Ando, M.: 2012, TOBA: Torsion-Bar Antenna, GWADW2012,(Hawaii, USA, May 17, 2012).
Ando, M.: 2012, News from KAGRA, The 32nd Program
Advisory Committee Meeting, (Pasadena, USA, May 3, 2012).
Ando, M.: 2013, Gravity and Gravitational-Wave Physics, Global
COE Symposium 'Development of Emergent New Fields',(Kyoto, Japan, Feb. 13, 2013).
Ando, M.: 2013, DECIGO, Gravitational Waves: New Frontier,(Seoul, Korea, Jan. 16-18, 2013).
Aoki, K., Iwata, I., Hattori, T., Nagao, T., Oyabu, S.: 2012, MIR
Selected Quasars from WISE PDR, AGN workshop 2012 in
Jeju, (Jeju, South Korea, Sep. 12-14, 2012).
Aoki, K.: 2012, A Statistical Study of Chromosphric Evaporation
Flows in Solar Flares, The 6th Hinode Science Meeting, (U. St.
Andrews, UK, Aug. 12-15, 2012).
Aoki, W.: 2012, Extremely metal-poor stars in the Milky Way
Galaxy, First Stars IV - From Hayashi to the Future, (Kyoto,
Japan, May 21-25, 2012).
Aoki, W.: 2012, Observational evidence for the first stars andconstraints on stellar models, Nuclei in the Cosmos XII, (Cairns,
Queensland, Australia, Aug. 5-10, 2012).
Araki, H., Kashima, S., Noda, H., Kunimori, H., Mashiko,H., Ootsubo, T., Utsunomiya, M., Matsumoto, Y.: 2013,
Develpoment of the retro-reflector on the moon for the future
lunar laser ranging, SELENE Symposium, (ISAS, JAXA, Japan,
Jan. 23-25, 2013).
Araki, H., Noda, H., Kunimori, H., Kashima, S., Ootsubo,T., Murata, K., Matsumoto, Y.: 2012, Development of LLR
retro-reflector for SELENE-2 mission, Seminar on Lunar andPlanetary Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Araki, H.: 2012, Research activities in Japan for the precise
measurement of the lunar rotation and tide -LLR and ILOM,
3rd Lunar Laser Ranging Workshop, (Bern, Switzerland, Mar.
23-25, 2012).
Arimoto, T., Ohtake, M., Haruyama, J., Iwata, T.: 2013,

Composition and Crystallinity Analysis of Lunar Dark Mantle
Deposits, 44th Lunar and Planetary Science Conference,(Woodlands, TX, USA, Mar. 18-22, 2013).
Barkin, Y., Hanada, H., Matsumoto, K., Noda, H., Petrova, N.,
Sasaki, S.: 2012, The effects of the physical libration of theMoon, caused by a liquid core, and their possible detection
from the long-term laser observations and from lunar surface
telescope (the Japanese project ILOM), 3rd Moscow Solar
System Symposium (3M-S3), (Space Research Institute,
Moscow, Russia, Oct. 8-11, 2012).
Barkin, Y., Hanada, H., Sasaki, S., Barkin, M.: 2012, Aboutsome inner structures of the Earth, the Moon and Mars asgeodynamical conseguences of the action of mechanism of theforced relative oscillations of the core and mantle, 3rd Moscow
Solar System Symposium (3M-S3), (Space Research Institute,
Moscow, Russia, Oct. 8-11, 2012).
Barkin, Y., Hanada, H., Sasaki, S., Goossens, S., Matsumoto,K.: 2012, Current and future exploration of the Moon and Mars:
tidal and non-tidal variations in rotation, temporal variations of
the shapes, secular expanding, gravitational fields and changes
in locations of the center of mass, Japan Geoscience Union
Meeting 2012, (Chiba, Japan, May 20-24, 2012).
Barkin, Y., Hanada, H., Sasaki, S., Goossens, S., Matsumoto,K.: 2012, Current and future exploration of the Moon and Mars:variations of rotation, shapes, displacements of center of mass,
Japan Geoscience Union Meeting 2012, (Chiba, Japan, May
20-24, 2012).
Baudry, A., Lacasse, R., Escoffier, R., Webber, J., Greenberg,J., Platt, L., Treacy, R., Saez, A. F., Cais, P., Comoretto, G.,
Quertier, B., Okumura, S. K., Kamazaki, T., Chikada, Y.,
Watanabe, M., Okuda, T., Kurono, Y., Iguchi, S.: 2012,
Performance Highlights of the ALMA Correlators, SPIE
Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Bowler, B. P., Liu, M. C., Shkolnik, E., Mann, A., Tamura, M.:
2013, The Planets Around Low-Mass Stars (PALMS) Direct
Imaging Survey, American Astronomical Society, (Long Beach,
CA, USA, Jan. 6-10, 2013).
Cabezas, D., Asai, A., Ueno, S., Morita, S., Martinez, L., Buleje, Y.,
Ishitsuka, J., Takasao, S., Yoshinaga, Y., Shibata, K., Kitai, R.,
Ishitsuka, M., Ishii, T.: 2012, CHAIN-project: Invesitigationsof solar active phenomenon obtained with Flare Monitoring
Telescope (FMT), United Nations/Ecuador Workshop on theInternational Space Weather Initiative, (Quito, Ecador, Oct.
8-12, 2012).
Carson, J., Carson, J., Thalmann, C., Janson, M., Kozakis, T.,
Bonnefoy, M., Biller, B. A., Schlieder, J., Currie, T. M.,
McElwain, M. W., Goto, M., Henning, T., Brandner, W., Feldt,
M., Kandori, R., Kuzuhara, M., Stevens, L., Wong, P., Gainey,
K., Brandt, T.: 2013, Direct Imaging Discovery of a ‘SuperJupiter’ Around a Late B-Type Star, American Astronomical
Society, (Long Beach, CA, USA, Jan. 6-10, 2013).
Cesar, O., et al. including Takato, N., Ueda, A.: 2012, FOCCoS for
Subaru PFS, SPIE Astronomical Telescope and Instrumentation,(Amsterdam, Netherlands, Jul. 1-6, 2012).
Chapillon, E., Takahashi, S., Hirano, N., Liu, S. Y., Taiwan ARC

node members, Akiyama, E., Dent, W., Espada, D., Hales, A.,
de Gregorio, I., Klaassen, P., Mathews, G., Juhasz, A., Rawling,M., Leonardo Testi, L.: 2012, A close look at low-mass star
forming regions: first ALMA results from SV data, The First Yearof ALMA Science, (Puerto Varas, Chile, Dec. 12-15, 2012).
Chibueze, J. O., Imura, K., Omodaka, T., Handa, T., Nagayama,T., Fujisawa, K., Sunada, K., Nakano, M., Kamezaki, T.,
Yamaguchi, Y.: 2013, Star Formation in the Molecular Cloud
Associated with the Monkey Head Nebula: Sequential or
Spontaneous?, IAU Symp. 292: Molecular Gas, Dust, and Star
Formation in Galaxies, (Beijing, China, Aug. 20-24, 2012).
de Gregorio, I., Klaassen, P., Testi, L., Rawling, M., Menard,F., Dent, W., Pinte, C., Takahashi, S., Hales, A., Espada, D.,
Cortes, P., Lopez, C., Tachihara, K., Higuchi, A., Akiyama,
E., Corder, S., Chapilliion, E., Mathews, G., Juhasz, A., Nyman,
L., Phillips, N. M., Rodon, J., Saito, M., van Kempen, T.: 2012,
Unveiling the Gas and Dust Disk Structure in HD 163296 Using
ALMA Observations, The First Year of ALMA Science, (Puerto
Varas, Chile, Dec. 12-15, 2012).
Eguchi, S., Kawasaki, W., Shirasaki, Y., Komiya, Y., Kosugi, G.,
Ohishi, M., Mizumoto, Y.: 2012, Prototype Implementation of
Web and Desktop Applications for ALMA Science Verification
Data and the Lessons Learned, Astronomical Data Analysis
Software and Systems (ADASS) Conference XXII, (Champaign,
IL, USA, Nov. 4-8, 2012).
Eguchi, S., Shirasaki, Y., Komiya, Y., Ohishi, M., Mizumoto,Y.: 2012, Japanese Virtual Observatory III: Three Scientific Use
Cases utilizing Virtual Observatory, XXVIIIth IAU General
Assembly, (Beijing, China, Aug. 20-31, 2012).
Espada, D., Takahashi, S., Chapillon, E., Akiyama, E.: 2012, EA
Imaging Team Studies with ALMA Science Verification Data,
New Trends in Radio Astronomy in the ALMA Era -The 30th
Anniversary of Nobeyama Radio Observatory-, (Hakone, Japan,
Dec. 3-8, 2012).
Espada, D.: 2012, ALMA Science Verification, East Asian ALMA
Science Workshop in Korea, (Daejeon Korea, Sep. 12-13, 2012).
Famiano, M. A.: 2012, Neutrino Effects in r-Process Nucleosynthesis
and Black Hole Formation, The 2nd Dogae Nuclear Physics andNuclear Astrophysics Workshop, (Kangwon-do, Korea, Aug.
1-4, 2012.).
Famiano, M. A.: 2012, Constraints on Elemental Observations
from the r-Process in Black Hole Collapse Scenarios, 1st NAOJ
Visiting Fellow Workshop Program on Element Genesis andCosmic Chemical Evolution: r-process perspective, (Wako,
Saitama, Japan, Oct. 17-19, 2012).
Famiano, M. A.: 2012, The r-Process in Core Collapse Models andExplanation of Scatter in Sr and Ba Abundances in Metal-PoorStars, Invited Astronomy, Invited Nuclear Physics Colloquium,(Sendai, Japan, Dec. 11, 2012).
Famiano, M. A.: 2012, Experimental Investigations of the Nuclear
Equation-of-State, Invited Nuclear Physics Colloquium,(Miyagi, Japan, Dec. 12, 2012).
Famiano, M. A.: 2012, Model for Determining Amino Acid
Chirality in the Supernova Neutrino Processing Model, NAOJ
Astrobiology Workshop, (Mitaka, Japan, Nov. 23-24, 2012).
Famiano, M. A.: 2012, Heavy Element Production in r-Process

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093

Collapse Scenarios, Nuclear Physics Seminar, (The Universityof Tokyo, Japan, Nov. 4, 2012).
Famiano, M. A.: 2012, Black Hole Formation and Constraints
on the r-Process and Galactic Chemical Evolution, 1st NAOJ
Visiting Fellow Workshop Program on Element Genesis andCosmic Chemical Evolution: r-process perspective, (Wako,
Saitama, Japan, Oct. 17-19, 2012).
Famiano, M. A.: 2012, Observational Constraints of Computational
Nuclear Astrophysics, National Astronomical Observatory
Colloquium, (Mitaka, Japan, Jul. 4, 2012).
Famiano, M. A.: 2012, Cosmology, Science, and Religion, Public
Lecture at the Tokyo Chapter of the WMU Alumni Association,(Tokyo, Japan, Jun. 5, 2012).
Fujii, K., Minamidani, T., Kawamura, A., Mizuno, N., Muller, E.,
Onishi, T., Fukui, Y.: 2012, Dense Molecular Clumps associatedwith the LMC Supergiant Shell LMC4, ALMA Workshop Science
with Mopra for the ALMA, (Mitaka, Japan, Jun. 8-9, 2012).
Fujii, K., Minamidani, T., Kawamura, A., Mizuno, N., Muller, E.,
Onishi, T., Fukui, Y.: 2012, Dense Molecular Clumps associatedwith the LMC Supergiant Shell LMC4, The Magellanic System:
In Perspective, (Perth, WA, Austraria, Sep. 10-13, 2012).
Fujii, K.: 2012, Dense Molecular Clumps associated with the LMC
Supergiant Shell LMC4, ALMA Workshop Science with Mopra
for the ALMA, (Mitaka, Japan, Jun. 8-9, 2012).
Fujii, Y., Gonzalez, A., Kroug, M., Kaneko, K., Miyachi, A.,
Kuroiwa, K., Yokoshima, T., Makise, K., Uzawa, Y., Wang,
A.: 2012, Performance of the first six ALMA Band 10 receivers,
23rd International Symposium on Space Terahertz Technology(ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Fujimoto, K., Sydora, R. D.: 2012, Plasmoid-induced turbulencein 3D kinetic reconnection, 39th COSPAR Scientific Assembly,(Mysore, India, Jul. 14-22, 2012).
Fujimoto, K.: 2012, AMR-PIC simulation of collisionlessmagnetic reconnection, Conference on Computational Physics(CCP2012), (Kobe, Japan, Oct. 14-18, 2012).
Fujiwara, H.: 2012, Public Information and Outreach Activities at
Subaru Telescope, XXVIIIth IAU General Assembly, (Beijing,
China, Aug. 20-31, 2012).
Fujiwara, H.: 2012, AKARI and Spitzer Observations of Warm
Debris Disks, Planet Formation and Evolution 2012, (Munich,Germany, Sept. 19-24, 2012).
Fukagawa, M., Tsukagoshi, T., Saigo, K., Aso, Y., Ohashi, N.,
Momose, M., Kitamura, Y., Akiyama, E., Takeuchi, T., Kobayashi,
H., Muto, T., Honda, M., Fujiwara, H., Nomura, H., Shibai, H.:
2012, High-Sensitivity Observations of the Protoplanetary Disk
around HD 142527 in 13CO(3–2), The First Year of ALMA
Science, (Puerto Varas, Chile, Dec. 12-15, 2012).
Fukui, A.: 2012, NIR transit photometry with the Okayama 188
cm telescope/ISLE, Transiting Planets in the House of the Sun,
(Maui, HI, USA, Jun. 3-6, 2012).
Fukui, A.: 2013, Optical-to-Near-infrared Simultaneous Observations
for the Transiting Hot Uranus GJ3470b, 1st Doha International
Astronomy Conference on Gravitational Microlensing - 101
years from theory to practice, (Doha, Qatar, Feb. 10-13, 2013).
Furusawa, H.: 2012, Status of HSC Data Analysis Pipeline,
Supermassive Black Holes in the Universe: The Era of the HSC

094

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Surveys, (Ehime, Japan, Dec. 18-20, 2012).
Furusho, R., Shinoda, T., Watanabe, J.: 2012, Imaging Polarimetryof 103P/Hartley and 10 Comets/Nuclei, Asteroids, Comets,
Meteors 2012, (Niigata, Japan, May 16-20, 2012).
Gonzalez, A., Uzawa, Y., Kaneko, K., Fujii, Y.: 2012, Improvements
in ALMA band 10 optics: Influence of IR filters and solutions,23rd International Symposium on Space Terahertz Technology(ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Gonzalez, A., Uzawa, Y.: 2012, Cross-polarization in quasioptical receivers: ALMA band 4 and 10, IRMMW-THz2012,(Wollongong, Australia, Sep. 23-28, 2012).
Gouda, N.: 2012, Present status of JASMINE projects,
Commission 8 Science Meeting at IAU General Assembly 28,(Beijing, China, Aug. 29, 2012).
Grady, C. A., Wisniewski, J. P., McElwain, M. W., Currie, T. M.,
Carson, J., Fukagawa, M., Hashimoto, J., Muto, T., Tamura,M.: 2013, The SEEDS of Planet Formation: Spiral Arms in theDisks of Herbig Ae-Fe Stars, American Astronomical Society,(Long Beach, CA, USA, Jan. 6-10, 2013).
Groff, T. D., Peters, M., Kasdin, N. J., McElwain, M. W., Galvin,
M., Carr, M., Knapp, G. R., Janson, M., Brandt, T., Lupton, R.,
Gunn, J. E., Guyon, O., Martinache, F., Hayashi, M., Takato,
N.: 2013, Preliminary Design of the Coronagraphic High
Angular Resolution Imaging Spectrograph (CHARIS), American
Astronomical Society, (Long Beach, CA, USA, Jan. 6-10, 2013).
Gusev, A., Hanada, H., Kikuchi F., Kosov, A., Li, J., Matsumoto,K., Ping, J., Sasaki, S., Tretyakov, V.: 2012, Radio-beaconson the moon and lunar physical libration for selene–2, chang’e–3/4, luna–glob and luna–resource projects, 3rd Moscow
Solar System Symposium (3M-S3), (Space Research Institute,
Moscow, Russia, Oct. 8-11, 2012).
Gusev, A., Noda, H., Araki, H., Hanada, H., Ping, J., Kikuchi,
F., Li, J., Matsumoto, K., Sasaki, S., Tretyakov, V.: 2012, Big
size hollow ccr of llr and lunar physical librations for selene–2, chang’e–4,5,6 and luna–resource projects, 3rd Moscow
Solar System Symposium (3M-S3), (Space Research Institute,
Moscow, Russia, Oct. 8-11, 2012).
Gutierrez, M., Terrazas, R., Ishitsuka, M., Ishitsuka, J., Yoshinaga,Y., Nakamura, N., Hillier, A., Morita, S., Asai, A., Ishii, T.,
Ueno, S., Kitai, R., Shibata, K.: 2012, A 3-dimensional view ofthe filament eruption and coronal mass ejection associated withthe 2011 March 8 solar flare, United Nations/Ecuador Workshop
on the International Space Weather Initiative, (Quito, Ecador,
Oct. 8-12, 2012).
Guyon, O., Martinache, F.: 2013, How Extremely Large Telescopes(ELTs) will Acquire the First Spectra of Rocky Habitable
Planets, AAS Meeting #221, (Long Beach, USA, Jan 23, 2013).
Guyon, O.: 2012, Optical Tricks to image Habitable Planets
around nearby Starts, Frontiers in Optics 2012, (Rochester, NY,
Oct. 18, 2012).
Hada, K.: 2012, M87: core and HST-1, East Asia To Italy: Nearly
Global VLBI, (Bologna, Italy, Oct. 15-16, 2012).
Hagiwara, Y.: 2012, Search for extragalactic water masers from
AGN, ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22,
2012).
Hagiwara, Y.: 2012, Upgrade of the VERA telescopes for Dual-polarization Receiving, East Asia VLBI Workshop 2012, (Taipei,
Taiwan, May 30-Jun. 2, 2012).
Hagiwara, Y.: 2012, Upgrade of the VERA telescopes for Dualpolarization Receiving, The 3rd KVN & VERA Joint Science
WG Meeting, (Mizusawa, Japan, Jul. 25-26, 2012).
Hagiwara, Y.: 2012, Large/key science program policy, The 3rd
KVN & VERA Joint Science WG Meeting, (Mizusawa, Japan,
Jul. 25-26, 2012).
Hagiwara, Y.: 2012, Recent status of VLBI in Japan and east Asia,
East Asia To Italy: Nearly Global VLBI, (Bologna, Italy, Oct.
15-16, 2012).
Hagiwara, Y.: 2012, Search for Extragalactic Water Masers from
AGN, ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Hagiwara, Y.: 2012, Search for Extragalactic H2O Maser toward
Active Galaxies, New Trends in Radio Astronomy in the ALMA
Era -The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Hagiwara, Y.: 2013, Synergies between ALMA and KVN+VERA,The 4th KVN & VERA Joint Science WG Meeting, (Seoul,
Korea Jan. 29-30, 2013).
Hanada, H., Araki, H., Tsuruta, S., Kashima, S., Tazawa, 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., Iwata, T., Utsunomiya, S., Kamiya, T., Heki, K.: 2012,
Development of a small digital telescope, and its application
to Geodesy and Selenodesy, Seminar on Lunar and Planetary
Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Hanada, H., Tsuruta, S., Araki, H., Kashima, S., Asari, K.,
Tazawa, S., Noda, H., Matsumoto, K., Sasaki, S., Funazaki, K.,
Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Itou, Y., Chiba, K.,
Inaba, K., Gouda, N., Yano, T., Yamada, Y., Niwa, Y., Kunimori,
H., Petrova, N., Gusev, A., Ping, J., Iwata, T., Utsunomiya, S.,
Kamiya T., Heki, K.: 2012, Technical development of a small
digital telescope for in-situ lunar orientation measurements(ilom), 3rd Moscow Solar System Symposium (3M-S3), (Space
Research Institute, Moscow, Russia, Oct. 8-11, 2012).
Hanada, H.: 2013, Gravimetry and Rotation Measurements in
SELENE-2 and Future Space Missions, Russia-Japan Scientific
Meeting on some problems in the exploration of space and joint
projects, (Kazan Aviation University, Russia, Mar. 15, 2013).
Hanaoka, Y.: 2012, Polarimeter with a high-speed rotating
waveplate for the solar observation, SPIE Astronomical Telescopeand Instrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Hanaoka, Y.: 2012, Long-term synoptic observations of the Sunat the National Astronomical Observatory of Japan, Eclipse on
the Coral Sea: Cycle 24 Ascending, (Palm Cove, Queensland,
Australia, Nov. 12-16, 2012).
Hara, C., Kawabe, R., Shimajiri, Y., Ueda, J., Kurono, Y.,
Tsukagoshi, T., Nakamura, F., Saito, M., Wilner, D.: 2012,
Discovery of the rotating molecular outflow and disk in theClass-0/I protostar [BHB2007]#11 in Pipe, New Trends inRadio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Hara, H.: 2012, Spectroscopy of the site of magnetic reconnection

in solar flares, Spectroscopy of the Dynamic Sun, (London, UK,
Apr. 18-20, 2012).
Hara, H.: 2012, Hinode Observations: Dynamic Solar Corona,
Japan-Norway Symposium on Space Science in Polar Region,(Oslo, Norway, Jun. 5-6, 2012).
Hara, H.: 2012, Spectroscopy of Reconnection Outow in Solar
Flares, The 6th Hinode Science Meeting, (U. St. Andrews, UK,
Aug. 12-15, 2012).
Hara, H.: 2012, What can and cannot be measured with SUVITLEMUR-XIT I dynamic atmosphere?, The Solar-C science
meeting, (U. St. Andrews, UK, Aug. 11, 2012).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda,
H.: 2012, Dependence of the tidal response on the internal
structure of the Moon: Geodetic implication to the partial melt
layer, Japan Geoscience Union Meeting 2012, (Chiba, Japan,
May 20-24, 2012).
Hasegawa, T., the ALMA Front End Integration Subproject
Team: 2012, Integration and verification of ALMA receiver
front ends, 23rd International Symposium on Space Terahertz
Technology (ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Hayano, Y., Akiyama, M., Hattori, M., Hattori, T., Iwata, I., Iye,
M., Kodama, T., Minowa, Y., Motohara, K., Nishimura, T.,
Ohashi, N., Ono, Y., Oya, S., Takami, H., Takato, N., Takiura,
K., Tamura, N., Tanaka, I,, Terada H., Tomono, D., Usuda,T., Watanabe, M., Yamamuro, T., Arimoto, N.: 2012, Widefield adaptive optics for Subaru Telescope, SPIE Astronomical
Telescope and Instrumentation, (Amsterdam, Netherlands, Jul.
1-6, 2012).
He, J. J., et al. including Kajino, T.: 2012, A surprise in the
Li 6 (p,gamma)Be 7 reaction at low energies, Nuclei in the
Cosmos XII, (Cairns, Queensland, Australia, Aug. 5-10, 2012).
Hibi, Y., Matsuo, H., Ookawa, T., Sekiguchi, S., Torii, D.,
Watanabe, D., Ikeda, H., Fujiwara, M.: 2012, Cryogenic MultiChannel Readout System for Submillimeter/Terahertz Photon
Detectors, 23rd International Symposium on Space Terahertz
Technology (ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Hibi, Y., Qin, H., Matsuo, H., Kang L., Chen, J., Wu, P.: 2013, Comaking super- and semiconductor devices onto same substrate,
13th Workshop on Submm Wave Receiver Technologies in
Eastern Asia, (Nanjing, China, Jan. 10-12, 2013).
Hiramatsu, M.: 2012, ALMA public outreach report, ALMA Users
Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Hiramatsu, M.: 2012, Molecular line study of low-luminosity
protostars, ALMA Workshop Science with Mopra for the
ALMA, (Mitaka, Japan, Jun. 8-9, 2012).
Hiramatsu, M.: 2012, Communicating ALMA with the Public
in Japan, IAU General Assembly 2012 Special Session 14:
Communicating Astronomy with the Public for Scientists,(Beijing, China, Aug. 29-31, 2012).
Hirota, A., Kuno, N., Tanaka, A., Nakanishi, H., Kawabe, R.:
2012, Widw-Field 12CO (J = 1–0) Imaging of the Nearby Barred
Galaxy M83 with the NMA and the 45 m Telescope, New Trends
in Radio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Hirota, T.: 2012, Observations of the mm/submm H2O masers inOrion KL, ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22,

II Publications, Presentations095

2012).
Hirota, T.: 2012, VERA+ALMA observations of the H2O maser
burst in Orion KL, East Asia VLBI Workshop 2012, (Taipei,
Taiwan, May 30-Jun. 2, 2012).
Hirota, T.: 2012, Status report of SFRs sub-WG, The 3rd KVN& VERA Joint Science WG Meeting, (Mizusawa, Japan, Jul.
25-26, 2012).
Hirota, T.: 2012, VERA+ALMA Observations of the H2O Maser
Burst in Orion KL, EVN Symposium 2012, (Bordeaux, France,
Oct. 9-12, 2012).
Hirota, T.: 2012, Observations of the millimeter/submillimeter
H 2O masers in Orion KL, ALMA Users Meeting, (Mitaka,
Japan, Nov. 20-22, 2012).
Hirota, T.: 2012, Observational Studies of Chemically Young Dark
Cloud Cores, New Trends in Radio Astronomy in the ALMA
Era -The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Hirota, T.: 2012, High-resolution Observations of Centimeter/(Sub)millimeter H 2O masers in Orion KL with VERA and
ALMA, New Trends in Radio Astronomy in the ALMA Era-The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Hirota, T.: 2012, VLBI studies of nearby star-forming regions,
NRO workshop Star Formation 2012, (Mitaka, Japan, Dec.
10-12, 2012).
Hirota, T.: 2012, Observations of the centimeter/(sub)millimeter
H2O masers in Orion KL with ALMA and VERA, The First Yearof ALMA Science, (Puerto Varas, Chile, Dec. 12-15, 2012).
Hirota, T.: 2013, Report from the star forming regions SWG, The
4th KVN & VERA Joint Science WG Meeting, (Seoul, Korea
Jan. 29-30, 2013).
Hirota, T.: 2013, ALMA early science of H2O masers in Orion
KL, The 4th KVN & VERA Joint Science WG Meeting, (Seoul,
Korea Jan. 29-30, 2013).
Honma, M., Hirota, T.: 2012, KVN-VERA studies on starformation/late type stars, East Asia To Italy: Nearly Global
VLBI, (Bologna, Italy, Oct. 15-16, 2012).
Honma, M.: 2012, Maser astrometry and Galactic structure with
VERA, East Asia VLBI Workshop 2012, (Taipei, Taiwan, May
30-Jun. 2, 2012).
Honma, M.: 2012, Sub-mm VLBI in the world and the role ofJapan & East Asia, East Asia VLBI Workshop 2012, (Taipei,
Taiwan, May 30-Jun. 2, 2012).
Honma, M.: 2012, Key-science policy draft plan, The 3rd KVN& VERA Joint Science WG Meeting, (Mizusawa, Japan, Jul.
25-26, 2012).
Honma, M.: 2012, Galaxy-scale maser astrometry with VERA,EVN Symposium 2012, (Bordeaux, France, Oct. 9-12, 2012).
Honma, M.: 2012, AGN studies with EHT and EATING VLBI,VLBI Workshop - Relativistic Jets in AGNs, (Mitaka, Japan,
Nov. 29, 2012).
Honma, M.: 2012, Maser Astrometry with VERA and the Galaxy's
structure, New Trends in Radio Astronomy in the ALMA Era-The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Honma, M.: 2013, Status of EHT and ALMA phasing project, The

096

II Publications, Presentations

4th KVN & VERA Joint Science WG Meeting, (Seoul, Korea
Jan. 29-30, 2013).
Hori, Y., Ikoma, M., Lin, D. N. C.: 2012, On the Accretion of
Atmospheres Onto Super-Earths, Planet formation and evolution
2012, 8th Conference on Formation and Evolution of Planetarysystems, (Munich, Germany, Sep. 3-7, 2012).
Hori, Y.: 2012, On the Accretion of Atmospheres onto Super-Earths,
CPS 9th International School of Planetary Sciences Across the
Earth into Exoplanets, (Suma, Japan, Jun. 24-29, 2012).
Hori, Y.: 2012, Theories of Planet Formation, GUAS/SOKENDAI
Asian Winter School 2012, (Mitaka, Japan, Dec. 3-5, 2012).
Hori, Y.: 2013, Diversity of Low-Mass Planets with Atmospheres,
Nagoya University GCOE program: QFPU Final International
Forum, (Gifu, Japan, Mar. 7-10, 2013).
Horie, M., Nishikawa, J., Oya, M., Waki, R., Kumagai, S., Tamura,M., Kurokawa, T., Murakami, N., Murakami, H., Abe, L.: 2012,
Wavefront correction inside unbalanced nulling interferometer,
SPIE Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Iguchi S., Saito, M.: 2012, Very large millimeter, SPIE Astronomical
Telescope and Instrumentation, (Amsterdam, Netherlands, Jul.
1-6, 2012).
Iguchi, S.: 2012, ALMA Construction and Development Status,
ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Iguchi, S.: 2012, ALMA Construction and Development Status,
East Asian ALMA Science Workshop in Korea, (Daejeon Korea,
Sep. 12-13, 2012).
Iguchi, S.: 2012, ALMA Construction and Early Science Operations,
Shanghai Astronomical Observatory New Technologies in
Astronomy Symposium, (Shanghai, China, June 23-25, 2012).
Imada, S.: 2012, High-Speed Plasma Flows Observed By EIS
During X-class Limb Flare, The 6th Hinode Science Meeting,(U. St. Andrews, UK, Aug. 12-15, 2012).
Imada, S.: 2012, Self-Organization of Reconnecting Plasmas to a
Marginally Collisionless State in the Solar Corona, The 6th Hinode
Science Meeting, (U. St. Andrews, UK, Aug. 12-15, 2012).
Imaeda, R., Haruyama, J., Ohtake, M., Iwata, T., Arimoto, T., Ito,K., Kuriyama, Y.: 2013, Lunar Marius Hills Plateau Exhibiting
the Early Imbrian Model Age, 44th Lunar and Planetary Science
Conference, (Woodlands, TX, USA, Mar. 18-22, 2013).
Imanishi, M.: 2012, AGN study from z < 0.5 to z > 7, AGN
workshop 2012 in Jeju, (Jeju, South Korea, Sep. 12-14, 2012).
Imanishi, M.: 2012, Nuclear starbursts at the outer part of dusty
molecular tori of nearby AGNs, Torus workshop 2012, (San
Antonio, TX, USA, Dec. 5-7, 2012).
Imanishi, M.: 2012, z > 6 QSOs study using HSC wide survey
data, Supermassive Black Holes in the Universe: The Era of the
HSC Surveys, (Ehime, Japan, Dec. 18-20, 2012).
Imanishi, M.: 2013, Infrared and (sub)millimeter energy diagnosticsof nearby ultraluminous infrared galaxies, Dissecting Galaxies
with 2D Wide-field Spectroscopy, (Lijiang, China, Mar. 25-30,
2013).
Imanishi, Y., Nawa, K., Tamura, Y., Ikeda, H., Miyaji, T., Tanaka, Y.:
2012, Superconducting gravimeter observation for identifying
slow slip events at Ryukyu Trench, AGU Fall Meeing 2012, (SanFrancisco, CA, USA, Dec. 3-7, 2012).

Inoue, S., Nishikawa, J., Kotani, T., Kashiwagi, K., Suto, H.,
Tamura, M., Kurokawa, T.: 2012, Design and Test of Star light
Coupling to High Precision Doppler Spectrograph using Multimode Fiber, Frontiers in Optics 2012, (Rochester, NY, Oct. 18,
2012).
Iono, D., Hasegawa, T., Iguchi, S., Mizuno, N., Saito, M.: 2012,
ALMA EA Activities/Future Development of ALMA, New Trends
in Radio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Iono, D.: 2012, ALMA workshop report, ALMA Users Meeting,(Mitaka, Japan, Nov. 20-22, 2012).
Iono, D.: 2012, Mopra status report, ALMA Users Meeting,(Mitaka, Japan, Nov. 20-22, 2012).
Iono, D.: 2012, Observing Molecular Gas in External Galaxies
using Mopra, ALMA Workshop Science with Mopra for the
ALMA, (Mitaka, Japan, Jun. 8-9, 2012).
Iono, D.: 2012, ALMA Science Activities Toward Future Proposals
and Developments, East Asian ALMA Science Workshop in
Korea, (Daejeon Korea, Sep. 12-13, 2012).
Ishiguro, M., Hanayama, H., Hasegawa, S., Sarugaku, Y., Watanabe,J., Fujiwara, H., Terada, H., Hsieh, H. H., Vaubaillon, J. J.,
Kawai, N., Yanagisawa, K., Kuroda, D., Miyaji, T., Ohta, K.,
Fukushima, H., Hamanowa, H., Kim, J., Pyo, J., Nakamura,A. M.: 2012, Ejecta Plume Resulting from an Oblique Impact
on (596) Scheila, Asteroids, Comets, Meteors 2012, (Niigata,Japan, May 16-20, 2012).
Ishii, S., Seta, M., Nakai, N., Miyamoto, Y., Nagai, M., Arai,
H., Maezawa, H., Nagasaki, T., Miyagawa, N., Motoyama,
H., Sekimoto, Y., Bronfman, L.: 2012, Development of aTransportable Telescope for Galactic Survey at 500 GHz in
Antarctica, 23rd International Symposium on Space Terahertz
Technology (ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Ishikawa, R.: 2012, A new initiative of magnetic eld measurements
via the Hanle eect with a sounding rocket experiment CLASP,The 6th Hinode Science Meeting, (U. St. Andrews, UK, Aug.
12-15, 2012).
Ishitsuka, J., Asai, A., Morita, S., Terrazas, R., Cabezas, D.,
Gutierrez, M., Martinez, L., Buleje, Y., Nakamura, N., Takasao, S.,
Yoshinaga, Y., Hillier, A., Otsuji, K., Shibata, K., Ueno, S., Kitai,
R., Ishii, T., Ichimoto, K., Nagata, S., Ishitsuka, M., Narukage, N.:
2012, Within the international collaboration CHAIN: A summaryof events observed with Flare Monitoring Telescope (FMT) in
Peru, United Nations/Ecuador Workshop on the International
Space Weather Initiative, (Quito, Ecador, Oct. 8-12, 2012).
Ito, T., Higuchi, A., 2012, Dynamical evolution of the Oort cloud
new comets, XXVIIIth IAU General Assembly, (Beijing, China,
Aug. 20-31, 2012).
Ito, T., Higuchi, A.: 2012, Dynamical evolution of the Oort cloud
new comets, AOGS - AGU (WPGM) Joint Assembly, (Singapore,Aug. 13-17, 2012).
Ito, T., Higuchi, A.: 2012, Dynamical evolution of the Oort cloud
new comets, Asteroids, Comets, Meteors 2012, (Niigata, Japan,
May 16-20, 2012).
Iwai, A., Itoh, Y., Terai, T.: 2012, Optical Spectroscopy of Highly
Inclined Main-Belt Asteroids, Asteroids, Comets, Meteors 2012,(Niigata, Japan, May 16-20, 2012).
Iwai, K., Masuda, S., Miyoshi, Y., Tsuchiya, F., Morioka, A.,
Misawa, H.: 2012, Spectrum Fine Structures of Solar Radio
Type-I Burst Observed with AMATERAS, Solar Physics with
Radio Observations, (Aichi, Japan, Nov. 20-23, 2012).
Iwai, K., Misawa, H., Tsuchiya, F., Morioka, A., Miyoshi, Y.,
Masuda, S., Obara, T.: 2012, Spectrum Fine Structures of Solar
Radio Type-I Burst, AOGS - AGU (WPGM) Joint Assembly,(Singapore, Aug. 13-17, 2012).
Iwai, K., Shibasaki, K.: 2012, Measurements of the Chromospheric
Magnetic Field by the Polarization Observation of Nobeyama
Radioheliograph, Solar Physics with Radio Observations,(Aichi, Japan, Nov. 20-23, 2012).
Iwata, T., ILOM/LLFAST group: 2012, A road map for lunar
astronomical observatory, Seminar on Lunar and Planetary
Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Iwata, T., Kawakatsu, Y., DESTINY Working Group: 2012,
Mission outline of DESTINY: Demonstration and Experimentof Space Technology for Interplanetary Voyage, Symposium on
Planetary Science 2012, (Sendai, Japan, Apr. 3-5, 2012).
Iwata, T., Kitazato, K., Abe, M., Ohtake, M., Hirata, N., Honda, C.,
Takagi, Y., Matsuura, S., Tsumura, K., NIRS3 Mission Group:
2012, Results of the Critical Design for NIRS3: the Near
Infrared Spectrometer on Hayabusa-2, AOGS - AGU (WPGM)
Joint Assembly, (Singapore, Aug. 13-17, 2012).
Iwata, T., Kitazato, K., Abe, M., Ohtake, M., Hirata, N., Honda, C.,
Takagi, Y., Matsuura, S., Tsumura, K., NIRS3 Mission Group:
2012, NIRS3: the Near Infrared Spectrometer on Hayabusa-2,
International (CJMT 2012) Asteroid Science Workshop, (Macau,
China, Oct. 18, 2012).
Iwata, T., Kitazato, K., Abe, M., Ohtake, M., Matsuura, S.,
Tsumura, K., Hirata, N., Honda, C., Takagi, Y., Nakauchi, Y.,
Hiroi, T., Senshu, H., Arai, T., Nakamura, T., Matsunaga, T.,
Komatsu, M., Takato, N., Watanabe, S.: 2013, Results of the
Critical Design for NIRS3: The Near Infrared Spectrometer on
Hayabusa-2, 44th Lunar and Planetary Science Conference,(Woodlands, TX, USA, Mar. 18-22, 2013).
Iwata, T., Kitazato, K., Abe, M., Ohtake, M., Matsuura, S.,
Tsumura, K., Hirata, N., Honda, C., Takagi, Y., Nakauchi, Y.,
Hiroi, T., Senshu, H., Arai, T., Nakamura, T., Matsunaga, T.,
Komatsu, M., Takato, N., Watanabe, S.: 2013, Results of the
Critical Design for NIRS3: The Near Infrared Spectrometer on
Hayabusa-2, 44th Lunar and Planetary Science Conference,(Woodlands, TX, USA, Mar. 18-22, 2013).
Iwata, T., Matsumoto, K., Ishihara, Y., Kikuchi, F., Harada Y.:
Sasaki, S.: 2012, Measurements of Martian rotation variations
by space geodetic techniques, Seminar on Lunar and Planetary
Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Iwata, T., Murata, Y.: 2012, Status of Japanese Space Radio
Astronomy and Solar System Explorations, SHAO New
Technologies in Astronomy Symposium 2012, (SHAO, Shanghai,
China, Jun. 23-25, 2012).
Iwata, T., SELENE Science Team: 2012, A review of SELENE/
Kaguya and outline of Japanese future Lunar and Martian
mission plans, International Symposium on Lunar and Planetary

II Publications, Presentations

097

Science (ISLPS 2012), (Macau, China, Mar. 26-27, 2012).
Iwata, T., SELENE Science Team: 2012, A strategy for integrated
Science using the data of SELENE/Kaguya mission, AOGS AGU (WPGM) Joint Assembly, (Singapore, Aug. 13-17, 2012).
Izumiura, H., Fukui, A., Imada, A., Kambe, E., Koyano, H.,
Kuroda, D., Okita, K., Sakamoto, A., Shimizu, Y., Toda, H.,
Tsutsui, H., Ukita, N., Yanagisawa, K.: 2012, Refurbishingplan of the 188 cm reflector at OAO, East Asian RV-Workshop,(Beijing, China, Aug. 31-Sep. 2, 2012).
Jovanovic, N., Cvetojevic, N., Guyon, O., Martinache, F., Lawrence.
J.: 2013, Detecting exoplanets with extreme adaptive optics anda single-mode fibre fed spectrograph, European Conference on
Lasers and Electro-Optics, (Munich, Germany, May 12-16, 2012).
Jovanovic, N., Guyon, O., Martinache, F., Clergeon, C., Garrel.,V.: 2013, The Subaru Coronagraphic Extreme AO project:progress and upgrades, AAS Meeting #221, (Long Beach, USA,Jan 23, 2013).
Jovanovic. N., Gross, S., Arriola, A., Charles, N., Tuthill, N., Norris,
B., Stewart, P., Lawrence, J., Withford, M.: 2013, Improved
performance characteristics for the integrated photonic pupil
remapping interferometer Dragonfly, European Conference on
Lasers and Electro-Optics, (Munich, Germany, May 12-16, 2012).
Kaithakkal, A. J., Tsuneta, S., Suematsu, Y., Kubo, M., Shiota, D.,
Shimojo, M.: 2012, Association of Polar Faculae with the Polar
Magnetic Patches as Revealed by Hinode Observations, AGU
Fall Meeing 2012, (San Francisco, CA, USA, Dec. 3-7, 2012).
Kajino, T.: 2012, Cosmology and Nuclear Astrophysics, Korea
Isotope Accelerator (KoRIA) Workshop, Institute of Basic
Science, (Daejeon, Korea, May 11-12, 2012).
Kajino, T.: 2012, R-process in Astronomy and Nuclear Physics,
1st RIKEN-RIBF Workshop, (Wako, Japan, May 24, 2012).
Kajino, T.: 2012, Neutrino Oscillation and Mass Hierarchy fromSupernova Nucleosynthesis, 4th International Symposium on
Neutrinos and Dark Matter in Nuclear Physics (NDM12), (Nara,
Japan, Jun. 11-15, 2012).
Kajino, T.: 2012, Supernova Nucleosynthesis and Physics of
Neutrino Oscillation, 4th Carpathian Summer School of Physics
2012 on Exotic Nuclei and Nuclear and Particle Astrophysics:
From nuclei to stars, (Sinaia, Romania, Jun. 24-Jul. 7, 2012).
Kajino, T.: 2012, Nuclear and Particle Physics Aspects of BigBang Nucleosynthesis, Nuclei in the Cosmos XII, (Cairns,
Queensland, Australia, Aug. 5-10, 2012).
Kajino, T.: 2012, Dark Matter and Neutrino Oscillation in
Primordial and Supernova Nucleosynthesis, 1st International
Sung Kyun Kwan University (SKKU) Symposium on
Astrophysics and Cosmology: from Particles to Universe,(Suwon, Korea, Aug. 30-Sep. 1, 2012).
Kajino, T.: 2012, Nuclear Weak Interactions, Supernova Nucleosynthesis
and Neutrino Oscillation, International Symposium on Exotic
Nuclear Structure from Nucleons (ENSFN 2012), (Tokyo,
Japan, Oct. 10-12, 2012).
Kajino, T.: 2012, Element Genesis and Cosmic Chemical Evolution,
1st NAOJ Visiting Fellow Workshop Program on Element
Genesis and Cosmic Chemical Evolution: r-process perspective,(Wako, Saitama, Japan, Oct. 17-19, 2012).
Kajino, T.: 2012, Neutrino nucleosynthesis process in core-collapse098

II Publications, Presentations

supernovae and neutrino oscillation, The 8th International
Workshop on Neutrino-Nucleus Interactions in the Few-Gev
Region, (Rio de Janeiro, Brasil, Oct. 21-27, 2012).
Kajino, T.: 2012, Neutrino Physics Phenomenology: Cosmologicaland Astrophysical Constraints on Neutrino Mass and Hierarchy,
International Workshop on the Interconnection between Particle
Physics and Cosmology (PPC 2012), (Seoul, Korea, Nov. 5-9,2012).
Kajino, T.: 2013, Supernova nucleosynthesis and neutrino oscillation,
10th Russbach School on Nuclear Astrophysics, (Russbach,Salzburg, Austria, Mar. 10-15, 2013).
Kamata, S., Sugita, S., Abe, Y., Ishihara, Y., Harada, Y., Namiki,N., Iwata, T., Hanada, H., Araki, H., Matsumoto, K., Tajika,
E.: 2013, Highly degraded early pre-nectarian impact basins:
implications for the timing of the magma ocean solidification,
44th Lunar and Planetary Science Conference, (Woodlands, TX,
USA, Mar. 18-22, 2013).
Kambe, E., Sadakane, K., Hashimoto, O., Honda, S., Sato, B.:
2013, Line-profile Variations of the Primary of Epsilon Aurigae
Eclipsing Binary System, Progress in Physics of the Sun andStars: A New Era in Helio- and Asteroseismology, (Hakone,
Japan, Nov. 26-29, 2012).
Kambe, E.: 2012, A Suatus Report on HIDES Fiber-Links, East
Asian RV-Workshop, (Beijing, China, Aug. 31-Sep. 2, 2012).
Kamegai, K., Sakai, T., Sakai, N., Hirota, T., Yamamoto, S.:
2013, Submillimeter-wave Observations of Complex Organic
Molecules in Southern Massive Star Forming Regions, IAU
Symp. 292: Molecular Gas, Dust, and Star Formation in
Galaxies, (Beijing, China, Aug. 20-24, 2012).
Kameno, S., Nakai, N., Honma, M.: 2012, ALMA Extended
Array, East Asia VLBI Workshop 2012, (Taipei, Taiwan, May
30-Jun. 2, 2012).
Kameno, S., Nakai, N., Honma, M.: 2012, ALMA Extended Array,
New Trends in Radio Astronomy in the ALMA Era -The 30th
Anniversary of Nobeyama Radio Observatory-, (Hakone, Japan,
Dec. 3-8, 2012).
Kameno, S., Yamaki, H., Beppu, H., Mizuno, I., Imai, H.: 2012,
Optimization of Bandpas Calibration in Radio Spectroscopy, East
Asia VLBI Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Kameno, S., Yamaki, H., Beppu, H., Mizuno, I., Imai, H.: 2012,
Optimization by Smoothed Bandpass Calibration in Radio
Spectroscopy, New Trends in Radio Astronomy in the ALMA
Era -The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Kameno, S.: 2012, Digital signal processing for accurate calibration,
East Asia VLBI Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2,2012).
Kameya, O.: 2012, Possible differential VLBI Observationsof pulsars using east-Asia VLBI antennas, East Asia VLBI
Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Kameya, O.: 2012, Possible differential VLBI Observations ofpulsars using VLBI antennas, The 3rd KVN & VERA Joint
Science WG Meeting, (Mizusawa, Japan, Jul. 25-26, 2012).
Kameya, O.: 2012, Water Vapor Masers in the NGC 7538 Region,
New Trends in Radio Astronomy in the ALMA Era -The 30th
Anniversary of Nobeyama Radio Observatory-, (Hakone, Japan,

Dec. 3-8, 2012).
Kameya, O.: 2013, Distribution of ionized gas density measured
by differential VLBI Observations of pulsars, IAU Symp. 291:
Neutron Stars and Pulsars: Challenges and Opportunities after
80 years, (Beijing, China, Aug. 20-24, 2012).
Kameya, O.: 2013, On the possibility of pulsar observations, The
4th KVN & VERA Joint Science WG Meeting, (Seoul, Korea
Jan. 29-30, 2013).
Kamezaki, T., Imura, K., Nagayama, T., Omodaka, T., Handa, T.,
Yamaguchi, Y., Chibueze, J. O., Sunada, K., Nakano, M.: 2013,
VLBI Observations and NH 3 Mapping of the Star-forming
Region NGC 2264, IAU Symp. 292: Molecular Gas, Dust, andStar Formation in Galaxies, (Beijing, China, Aug. 20-24, 2012).
Kamezaki, T., Nakagawa, A., Omodaka, T., Handa, T., Imai, H.,
Tafoya, D., Matsui, M., Nishida, Y., Nagayama, T., Honma, M.,
Kobayashi, H., Miyaji, T., Takeuti, M.: 2012, VLBI astrometryof the semi-regular variable star RX Bootis, IAU Symp. 289:
Advancing the Physics of Cosmic Distances, (Beijing, China,
Aug. 27-31, 2012).
Kano, R., Bando, T., Narukage, N., Ishikawa, R., Tsuneta, S.,
Katsukawa, Y., Kubo, M., Ishikawa, S., Hara, H., Shimizu,
T., Suematsu, Y., Ichimoto, K., Sakao, T., Goto, M., Kato,
Y., Imada, S., Kobayashi, K., Holloway, T., Winebarger, A.,
Cirtain, J., De Pontieu, B., Casini, R., Trujillo Bueno, J., Stepan,J., Manso Sainz, R., Belluzzi, L., Asensio Ramos, A., Auchere,
F. Carlsson, M.: 2012, Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP), SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Kano, R.: 2012, Photospheric properties of hot and cool coronalloops, The 6th Hinode Science Meeting, (U. St. Andrews, UK,
Aug. 12-15, 2012).
Karatsu, K., Naruse, M., Nitta, T., Sekimoto, Y., Sekine, M.,
Noguchi, T., Uzawa, Y., Matsuo, H., Kiuchi, H.: 2012,
Development of 1000 arrays MKID Camera for the CMB
Observation, SPIE Astronomical Telescope and Instrumentation,(Amsterdam, Netherlands, Jul. 1-6, 2012).
Karatsu, K., Naruse, M., Nitta, T., Sekimoto, Y., Sekine, M.,
Noguchi, T., Uzawa, Y., Matsuo, H., Kiuchi, H.: 2012,
Development of 1000 arrays MKID Camera for the CMB
Observation, 23rd International Symposium on Space Terahertz
Technology (ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Kashikawa, N.: 2012, High-z Universe Probed by Wide-Field
Observations, 39th COSPAR Scientific Assembly, (Mysore,
India, Jul. 14-22, 2012).
Kashikawa, N.: 2012, High-z universe probed by Subaru, KoreaJapan Collaboration Workshop, (Seoul, Korea, Nov. 14-16, 2012).
Kashikawa, N.: 2012, HSC high-z qso survey, Supermassive
Black Holes in the Universe: The Era of the HSC Surveys,(Ehime, Japan, Dec. 18-20, 2012).
Kashikawa, N.: 2012, First galaxies and cosmic reionization, TMT
Science and Instrumentation Workshop, (Pune, India, Dec.
10-12, 2012).
Kashima, S., Araki, H., Noda, H., Hanada, H., Kunimori, H.,
Murata, K., SELENE2-LLR Team: 2012, Optical Response
Simulation of Corner Cube Mirror for SELENE-2 Mission,
Seminar on Lunar and Planetary Geodesy, (Mitaka, Japan, Jun.

19-20, 2012).
Kasuga, T., Usui, F., Hasegawa, S., Kuroda, D., Ootsubo, T.,
Müller, T. G., Ishiguro, M.: 2012, Two Faces of Cybele Asteroid
Group revealed by AKARI/AcuA, Asteroids, Comets, Meteors
2012, (Niigata, Japan, May 16-20, 2012).
Kataoka, A., Machida, M. N., Tomisaka, K.: 2012, Exploring
Magnetic Field Structure in Star-Forming Cores with
Polarization of Thermal Dust Emission, Star Formation 2012,(Mitaka, Japan, Dec. 10-12).
Kataoka, A., Tanaka, H., Okuzumi, S., Wada, K: 2012, Static
compression process of dust aggregates in protoplanetary disks,
The 5th East Asia Numerical Astrophysics Meeting, (Kyoto,
Japan, Oct. 29-Nov. 2, 2012).
Kato, Y., Carlsson, M., Hansteen, V., Steiner, O.: 2012, Simulationsof Chromospheric/Coronal Generation in the Network Magnetic
Elements, BUKS 2012 MHD waves and seismology of the solar
atmosphere, (Crete, Greece, Sep 29, 2012).
Kato, Y.: 2012, Searching for Missing Links between Photospheric
Downdrafts and Chromospheric Brightening in the Network
Magnetic Elements, The 6th Hinode Science Meeting, (U. St.
Andrews, UK, Aug. 12-15, 2012).
Kato, Y.: 2012 , Modeling of Accretion Flow around the Galactic
Center Black Hole and its Radiative Properties, Galactic Center
Mini-Workshop, (Mitaka, Japan, May 11, 2012).
Kato, Y.: 2012, Modeling of Hot Accretion Flows around theGalactic Center Black Hole, Conference on Computational
Physics (CCP2012), (Kobe, Japan, Oct. 14-18, 2012).
Katsukawa, Y.: 2012, Chromospheric dynamics observed arounda sunspot in a HINODE-IBIS coordinated observation, The 6th
Hinode Science Meeting, (U. St. Andrews, UK, Aug. 12-15, 2012).
Kawamura, A., Mintamidani, T., Onishi, T., Mizuno, N., Mizuno,
Y., Kizawa, J., Fukui, Y.: 2012, Physical Properties of Molecular
Clouds in the Magellanic Clouds Revealed by Observationsin Multi-Transition CO Molecular Lines, New Trends inRadio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Kawamura, A.: 2012, Millimeter and Submillimeter Observationsof Molecular Clouds in the Magellanic Clouds, IAU Symp. 292:
Molecular Gas, Dust, and Star Formation in Galaxies, (Beijing,
China, Aug. 20-24, 2012).
Kawasaki, W., Eguchi, S., Shirasaki, Y., Komiya, Y., Kosugi,G., Ohishi, M., Mizumoto, Y.: 2012, Vissage: an ALMA-VO
Desktop Application, Astronomical Data Analysis Software andSystems (ADASS) Conference XXII, (Champaign, IL, USA,
Nov. 4-8, 2012).
Kawate, T., Ishii, T., Nakatani, Y., Morita, S., Ichimoto, K.,
Masuda, S.: 2012, High speed imaging system for solar flare
research at Hida observatory, Solar in Sonoma Tracing theConnections in Solar Eruptive Events, (Petaluma, CA, USA,
Nov. 27-Dec. 2. 2012).
Kero, J., Nakamura, T., Nishimura, K., Meisel, D. D., Terasawa,T., Masayoshi, U., Fujiwara, Y., Szasz, C, Watanabe, J.: 2012,
The MU Radar Meteor Head Echo Observation Programme,
39th COSPAR Scientific Assembly, (Mysore, India, Jul. 14-22,
2012).
Kikuchi, F., Matsumoto, K., Hanada, H., Tsuruta, S., Asari

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099

K., Kono, Y., Yamada, R., Sasaki, S., Iwata, T., Iijima, Y.,
Ogawa, K., Kamata, S., Goossens, S.: 2012, Recent status of
SELENE-2/VLBI instrument, Seminar on Lunar and Planetary
Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Kikuchi, F., Matsumoto, K., Hanada, H., Tsuruta, S., Asari,K., Kono, Y., Yamada, R., Iwata, T., Sasaki, S.: 2013, VLBIRadio Source Mission Proposed For Moon Lander SELENE-2,
SELENE Symposium, (ISAS, JAXA, Japan, Jan. 23-25, 2013).
Kim, M. K.: 2012, VLBI observations toward water/SiO masersin Orion-KL, East Asia VLBI Workshop 2012, (Taipei, Taiwan,
May 30-Jun. 2, 2012).
Kim, M., Choi, Y., Moon, H., Mottola, S., Ishiguro, M., Kaplan,
M., Kuroda, D., Warjurkar, D. S., Takahashi, J., Byun, Y.:
2012, Observational Properties Of 1999 Ju3 - Hayabusa 2
Mission Primary Target, 44th annual meeting of the Division
for Planetary Sciences of the American Astronomical Society,(Reno, NV, USA, Oct. 14-19, 2012).
Kim, S., Masuda, S., Shibasaki, K.: 2012, Two Episodes ofMicrowave Source Motions along Neutral Line during Tworibbon Flare, AGU Fall Meeing 2012, (San Francisco, CA,
USA, Dec. 3-7, 2012).
Kim, S.: 2012, Two Episodes of Systematic Microwave Source
Motions Parallel to Neutral Line during Two-ribbon Flare, Solar
Physics with Radio Observations, (Aichi, Japan, Nov. 20-23,
2012).
Kim, S.: 2012, Microwave Emission on Hot Supra-arcade Structureassociated with M1.6 Limb Flare, Solar Physics with Radio
Observations, (Aichi, Japan, Nov. 20-23, 2012).
Kim, S.: 2013, Displacement of Particle Acceleration Site during
Strong Solar Flare, STEL-KASI workshop, (Nagoya, Japan,
Mar. 18-19, 2013).
Kino, M.: 2012, Initial report on AGN observations with
KVN+VERA: M87 and Sgr A*, East Asia VLBI Workshop
2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Kino, M.: 2012, AGN observation with KVN+VERA: M87 and
Sgr A*, The 3rd KVN & VERA Joint Science WG Meeting,(Mizusawa, Japan, Jul. 25-26, 2012).
Kiuchi, H., Saito, M., Iguchi, S.: 2012, Photonic local oscillator
technics for large-scale interferometers, SPIE Astronomical
Telescope and Instrumentation, (Amsterdam, Netherlands, Jul.
1-6, 2012).
Kiyokane, K., Morita, K.-I., Kurono, Y., Saito, M., Mizuno,
N.: 2012, Evaluate the imaging performance of ALMA bysimulation, East Asian ALMA Science Workshop in Korea,(Daejeon Korea, Sep. 12-13, 2012).
Kiyokane, K., Saito, M., Saigo, K., Kurono, Y., Momose, M.,
Tsukagoshi, T., NRO45M SF-LEGACY TEAM: 2012, Prospect
for revealing the problem of the angular momentum transport
in the star formation physics by observation, The First Year of
ALMA Science, (Puerto Varas, Chile, Dec. 12-15, 2012).
Kiyokane, K., Saito, M., Saigo, K., Kurono, Y., Momose, M.,
Tsukagoshi, T., NRO45M SF-LEGACY TEAM: 2012, Mapping
Observation toward Protostellar Core L1527, New Trends inRadio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Kiyokane, K.: 2012, Evaluate the imaging performance of ALMA100

II Publications, Presentations

by simulation, East Asian ALMA Science Workshop in Korea,(Daejeon Korea, Sep. 12-13, 2012).
Klaassen, P., de Gregorio, I., Takahashi, S., Akiyama, E., Chapillon,
E., Dent, W., Espada, D., Hales, A., Hogerheijde, M., Juhasz, A.,
Mathews, G., Mottram, J., Rawlings, M., Testi, L., van Dishoeck,
E.: 2012, Band 6 and 7 CO observations of the molecularcounterpart to HH409 coming from HD 163296, The First Yearof ALMA Science, (Puerto Varas, Chile, Dec. 12-15, 2012).
Kobayashi, H.: 2012, Progress of East Asian VLBI network, East
Asia VLBI Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2,2012).
Kobayashi, H.: 2012, VERA status and results, IAU Symp. 289:
Advancing the Physics of Cosmic Distances, (Beijing, China,
Aug. 27-31, 2012).
Kobayashi, T., Nishikawa, J., Tanaka, Y., Kurokawa, T., Kashiwagi,K., Tamura, M., Murakami, N., Baba, N., Hashimoto, N.: 2012,
Unbalanced nulling interferometer with four-quadrant phasemask, OFS2012 22nd International Conference on Optical Fiber
Sensors, (Beijing, China, Oct. 14, 2012).
Kobayashi, Y., Shimura, Y., Niwa, Y., Yano, T., Gouda, N.,
Yamada, Y.: 2012, Nano-JASMINE: cosmic radiation
degradation of CCD performance and centroid detection, SPIE
Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Kodama, T., Hayashi, M., Koyama, Y., Tadaki, K., Tanaka, I.,
Shimakawa, R.: 2012, Formation and Evolution of Galaxies
and Clusters, Korea-Japan Collaboration Workshop, (Seoul,
Korea, Nov. 14-16, 2012).
Kodama, T., Hayashi, M., Koyama, Y., Tadaki, K., Tanaka, I.,
Shimakawa, R.: 2012, MAHALO-Subaru: Mapping star formation
at the peak epoch of massive galaxy formation, The intriguinglife of massive galaxies, (Beijing, China, Aug. 27-31, 2012).
Kodama, T., Hayashi, M., Koyama, Y., Tadaki, K., Tanaka, I.:2012, MAHALO-Subaru: Mapping star formation at the peak
epoch of galaxy formation, IAP-Subaru Joint International
Conference: Stellar Populations across Cosmic Times, (Paris,
France, Jun. 25-29, 2012).
Kokubo, E.: 2012, Gravitational Relaxation of Particulate Disks,
Dust and Grains in Low Gravity and Space Environment,(Noordwijk, Netherland, Apr. 2-4, 2012).
Kokubo, E.: 2012, The Basic Dynamical Model of Terrestrial
Planet Formation, IAU Symp. 293: Formation, Detection, andCharacterization of Extrasolar Habitable Planets, (Beijing,
China, Aug. 27-31, 2012).
Kokubo, E.: 2012, The Final Stage of Terrestrial Planet Formation,
The 5th East Asia Numerical Astrophysics Meeting, (Kyoto,
Japan, Oct. 29-Nov. 2, 2012).
Komiya, Y., Shirasaki, Y., Eguchi, S., Ohishi, M., Mizumoto, Y.,
Ishihara, Y., Ohnishi, T., Tsutsumi, J., Hiyama, T., Nakamoto,
H., Sakamoto, M.: 2012, Japanese Virtual Observatory II: VO
crawling system, IAU General Assembly 2012 Special Session
15: Data intensive astronomy, (Beijing, China, Aug. 20-31, 2012).
Komiya, Y., Shirasaki, Y., Ohishi, M., Eguchi, S., Mizumoto,Y.: 2012, Study of AGN and Galaxy Clustering using Virtual
Observatory, Supermassive Black Holes in the Universe: The
Era of the HSC Surveys, (Ehime, Japan, Dec. 18-20, 2012).

Komiya, Y., Suda, T., Fujimoto, M. Y.: 2012, Hierarchical modelfor the Galactic chemical evolution and r-process elements of
EMP stars, First Stars IV - From Hayashi to the Future, (Kyoto,
Japan, May 21-25, 2012).
Komiya, Y., Yamada, S., Suda, T., Fujimoto, M. Y.: 2012,
Chemical evolution of r-process elements in the hierarchicalgalaxy formation model, 1st NAOJ Visiting Fellow Workshop
Program on Element Genesis and Cosmic Chemical Evolution:
r-process perspective, (Wako, Saitama, Japan, Oct. 17-19, 2012).
Komiyama, Y.: 2012, Subaru Wide-Field Imaging Survey of the
Local Universe: Recent Results and Future Prospect, IAPSubaru Joint International Conference: Stellar Populations
across Cosmic Times, (Paris, France, Jun. 25-29, 2012).
Kotake, K.: 2012, Current status of multi-D hydrodynamic
simulations, NIC XII Workshop on r-process nucleosynthesis,(Cairns, Australia, Aug. 4-10, 2012).
Kotake, K.: 2012, Brainstorming on core-collapse supernova
theory with perspectives toward multi-messenger astronomy,
Nuclear Theory program INT-12-2a, (Seattle, WA, USA, Jul.
13-23, 2012).
Kotake, K.: 2012, Gravitational Waves from Core-Collapse
Supernovae, 13th Marcel Grossmann Meeting, (Stockholm,
Sweden, Jul. 1-7, 2012).
Kotake, K.: 2012, From micro- to macrophyisical impacts on
the mechanism of core-collapse supernvoae, Modeling at theinterface between nuclear physics and nuclear astrophysics,(Beijing, China, Jun. 17-13, 2012).
Kotani, T., et al. including Tamura, M., Guyon, O.: 2012, SPICA
coronagraph instrument: characterization of atmospheres
and physical parameters of giant planets by direct imaging
and spectroscopy, SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Kozakis, T., Stevens, L., Carson, J., Thalmann, C., Janson, M.,
Goto, M., Henning, T., Feldt, M., McElwain, M. W., Brandner,
W., Bonnefoy, M., Biller, B. A., Wong, P., Kandori, R.,
Tamura, M.: 2013, The Subaru SEEDS Imaging Search for
Exoplanets Around High-Mass Stars, American Astronomical
Society, (Long Beach, CA, USA, Jan. 6-10, 2013).
Kroug, M., Kuroiwa, K., Uzawa, Y.: 2012, Al/SiO2/Al Micro
Strip Lines for THz SIS Mixers, 23rd International Symposiumon Space Terahertz Technology (ISSTT2012), (Tokyo, Japan,
Apr. 2-4, 2012).
Kroug, M., Kuroiwa, K., Uzawa, Y.: 2012, Tuning circuit for SIS
mixers in the 800–950 GHz range: Comparison between NbTiN/
SiO2/Al and Al/SiO2/Al strip lines, Applied Superconductivity
Conf., (Portland, OR, USA, Oct. 7-12, 2012).
Kubo, M.: 2012, Role of small-scale magnetic elements inmagnetic flux transportation on the solar surface, 39th COSPAR
Scientific Assembly, (Mysore, India, Jul. 14-22, 2012).
Kubo, M.: 2012, Instrument for the Chromospheric Lyman-Alpha
SpectroPolarimeter (CLASP), The 6th Hinode Science Meeting,(U. St. Andrews, UK, Aug. 12-15, 2012).
Kunimori, H., Ishizu M., Araki, H.: 2012, Laser and configurationof Laser Ranging station for Lunar and Planetarymission,
Seminar on Lunar and Planetary Geodesy, (Mitaka, Japan, Jun.
19-20, 2012).

Kunimori, H., Matsumoto, Y., Kashima, S., Araki, H., Noda, H.,
LLR_Selene2 PI team: 2012, A Thermal distribution simulationof Hollow Laser Retro-reflector for SELENE2, Seminar on Lunarand Planetary Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Kunimori, H., Noda, H., Araki, H., Fuse, T., Hanada, H.,
Katayama, M., Kashima, S., Otsubo, T., Sasaki, S., Tazawa,
S., Funazaki, K., Taniguchi, H.: 2012, Feasibility Study of the
Lunar Laser Ranging Instrumentation for SELENE-2, AOGS AGU (WPGM) Joint Assembly, (Singapore, Aug. 13-17, 2012).
Kuno, N.: 2012, Giant Molecular Clouds in M33 and M83, New
Trends in Radio Astronomy in the ALMA Era -The 30th
Anniversary of Nobeyama Radio Observatory-, (Hakone, Japan,
Dec. 3-8, 2012).
Kuriyama, Y., Ohtake M., Haruyama, J., Iwata, T., Hirata, N.:
2013, Implications for Timescale of Central Peak Formation
Estimated by Impact Melts on Central Peaks of Lunar Craters,
44th Lunar and Planetary Science Conference, (Woodlands, TX,
USA, Mar. 18-22, 2013).
Kurono, Y., Saito, M., Kamazaki, T., Morita, K.-I., Kawabe, R.:
2012, Unveiling the detailed density and velocity structures ofthe protostellar core B335, The First Year of ALMA Science,(Puerto Varas, Chile, Dec. 12-15, 2012).
Kurono, Y.: 2012, Combined Imaging with ACA, ALMA Users
Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Kurosaki, K., Ikoma, M., Hori, Y.: 2012, Thermal Evolution and
Mass Loss of Water-Rich Exoplanets, The Origins of Stars andTheir Planetary Systems, (Hamilton, Canada, Jun. 10-15, 2012).
Kwon, J., Tamura, M., Kandori, R., Kusakabe, N., Hashimoto,J., Nakajima, Y., Nakamura, F., Nagayama, T., Nagata, T.,
Hough, J. H., Werner, M. W., Teixeira, P. S.: 2012, Complex
Scattered Radiation Fields And Multiple Magnetic Fields In
The Protostellar Cluster In NGC 2264, American Astronomical
Society, (Long Beach, CA, USA, Jan. 6-10, 2013).
Lee, M., Hiwaki, H., Kameno, S.: 2012, Jet Kinematics andAbsorbing Matter in the Quasar 1413+135 , New Trends inRadio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
M. W. M. de Graauw, Iguchi, S., McKinnon, M. M., Wild, W.,
Kurz, R. J., Hills, R. E.: 2012, Atacama large millimeter, SPIE
Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Maruyama, T., Yasutake, N., Cheoun, M.-K., Hidaka, J., Kajino,T., Mathews, G. J., Ryu, C.-Y.: 2012, Asymmetric neutrinotransport in strong toroidal magnetic field, 4th International
Symposium on Neutrinos and Dark Matter in Nuclear Physics(NDM12), (Nara, Japan, Jun. 11-15, 2012).
Mathews, G. S., Klaassen, P., Juhasz, A., Harsono, D., Akiyama,
E., Chapillon, E., Dent, W., Espada, D., de Gregorio, I., Hales,A., Hogerheijde, M., Mottram, J., Rawlings, M., Takahashi,S., Testi, L., van Dishoeck, E.: 2012, Directly tracing the COsnowline of HD 163296 with DCO+, The First Year of ALMA
Science, (Puerto Varas, Chile, Dec. 12-15, 2012).
Matsuda, Y.: 2012, The nature of Lyman-alpha blobs (LABs),
European Week of Astronomy and Space 2012, (Rome, Italy,
Jul. 1-6, 2012).
Matsui, K., Sorai, K., Watanabe, Y., Kuno, N.: 2012, Detection

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101

of CO (J = 1–0) Emission from Barred Spiral Galaxies at
z ~ 0.1 Nobeyama 45 m telescope legacy project: Line survey,
New Trends in Radio Astronomy in the ALMA Era -The 30th
Anniversary of Nobeyama Radio Observatory-, (Hakone, Japan,
Dec. 3-8, 2012).
Matsumoto, J., Masada, Y., Shibata, K.: 2012, Effect of Interacting
Rarefaction Waves on Relativistic Jets, JSST2012 International
Conference on Simulation Technology, (Kobe, Japan, Sep.
27-28, 2012).
Matsumoto, J., Masada, Y., Shibata, K.: 2012, Effect of Interacting
Rarefaction Waves on Relativistically Hot Jets, The 5th East
Asia Numerical Astrophysics Meeting, (Kyoto, Japan, Oct.
29-Nov. 2, 2012).
Matsumoto, K., Kikuchi, F., Goossens, S., Kamata, S., Iwata,T., Hanada, H., Ishihara, Y., Yamada, R., Sasaki, S.: 2012,
VLBI mission proposed for SELENE-2 and its contribution to
constrain the lunar internal structure, Japan Geoscience Union
Meeting 2012, (Chiba, Japan, May 20-24, 2012).
Matsumoto, K., Kikuchi, F., Yamada, R., Iwata, T., Kono, Y.,
Tsuruta, S., Hanada, H., Goossens, S., Ishihara, Y., Kamata, S.,
Sasaki, S.: 2012, VLBI mission proposed for SELENE-2 andits contribution to constrain thelunar internal structure, Seminaron Lunar and Planetary Geodesy, (Mitaka, Japan, Jun. 19-20,
2012).
Matsumoto, K., Kikuchi, F., Yamada, R., Iwata, T., Kono, Y.,
Tsuruta, S., Hanada, H., Goossens, S., Ishihara, Y., Kamata,S., Sasaki, S.: 2012, Placing constraints on the lunar internal
structure by SELENE-2 geodetic measurements, 3rd Moscow
Solar System Symposium (3M-S3), (Space Research Institute,
Moscow, Russia, Oct. 8-11, 2012).
Matsumoto, K., Kikuchi, F., Yamada, R., Iwata, T., Kono, Y.,
Tsuruta, S., Hanada, H., Goossens, S., Ishihara, Y., Kamata,S., Sasaki, S.: 2012, Contribution of SELENE-2 geodetic
measurements to constrain the lunar internal structure, AGU
Fall Meeing 2012, (San Francisco, CA, USA, Dec. 3-7, 2012).
Matsumoto, K., Yamada, R., Kikuchi, F., Iwata, T., Kono, Y.,
Tsuruta, S., Hanada, H., Goossens, S., Ishihara, Y., Kamata,S., Sasaki, S.: 2013, Contribution of SELENE-2 Geodetic
Measurements to Constrain the Lunar Internal Structure,
SELENE Symposium, (ISAS, JAXA, Japan, Jan. 23-25, 2013).
Matsumoto, N., Honma, M., Hirota, T., Shibata, K. M., VERA
project members: 2012, The bar effect in the galactic gas motions
traced by 6.7 GHz methanol maser sources with VERA, East Asia
VLBI Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Matsumoto, N., Imai, H., KVN+VERA Evolved star sub-Science
WG: 2012, Maser detectability test with VLBA data, The 3rd
KVN & VERA Joint Science WG Meeting, (Mizusawa, Japan,
Jul. 25-26, 2012).
Matsumoto, N., Oyama, T., Miyazaki, A.: 2013, Fringe checkobservations of galactic center SiO maser sources, The 4th
KVN & VERA Joint Science WG Meeting, (Seoul, Korea Jan.
29-30, 2013).
Matsuo, H.: 2012, Photon Counting Terahertz Interferometry,
23rd International Symposium on Space Terahertz Technology(ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Matsuo, H.: 2012, Terahertz Interferometry from Antarctic

102

II Publications, Presentations

Plateaus, XXVIIIth IAU General Assembly, (Beijing, China,
Aug. 20-31, 2012).
Matsuo, H.: 2012, Photon Counting Terahertz Interferometryfor Exo-Planet Imaging, New Trends in Radio Astronomy in
the ALMA Era -The 30th Anniversary of Nobeyama Radio
Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Matsuo, H.: 2012, Proposal of Photon Counting VLBI Technology,
East-Asian sub-mm VLBI workshop, (Tokyo, Japan, Dec. 10, 2012).
Matsuo, H.: 2013, Design of SIS terahertz photon counters andapplication to astrophysics, 13th Workshop on Submm Wave
Receiver Technologies in Eastern Asia, (Nanjing, China, Jan.
10-12, 2013).
Matsuo, H.: 2013, High Sensitivity Astronomical Imaging Arrayswith Cryogenic Electronics for Terahertz-waves, International
Solid-Sate Circuits Conference, (San Fransisco, USA, Feb. 17-21,
2013).
Matsuo, T., Kotani, T., Murakami, N., Kawahara, H., Fujii,Y., Oya, S., Kurita, M., Natsume, N., Narita, N., Takizawa,
K., Ikoma, M., Minagawa, J., Baba, N., Tamura, M.: 2012,
Second-Earth imager for TMT (SEIT): concept and its
numerical simulation, SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Matumoto, N., Honma, M.: 2012, 3D motions of 6.7 GHz
methanol masers and effects of the Galactic bar, IAU Symp.
289: Advancing the Physics of Cosmic Distances, (Beijing,
China, Aug. 27-31, 2012).
McElwain, M. W., Brandt, T. D., Janson, M., Knapp, G. R., Peters, M.
A., Burrows, A. S., Carlotti, A., Carr, M. A., Groff, T., Gunn, J. E.,
Guyon, O., Hayashi, M., Kasdin, N. J., Kuzuhara, M., Lupton,
R. H., Martinache, F., Spiegel, D., Takato, N., Tamura, M.,
Turner, E. L., Vanderbei, R. J.: 2012, Scientific design of a highcontrast integral field spectrograph for the Subaru Telescope,
SPIE Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Min, C. H.: 2012, VERA observations of SiO masers in Symbiotic
star R Aquarii, The 3rd KVN & VERA Joint Science WG
Meeting, (Mizusawa, Japan, Jul. 25-26, 2012).
Min, C. H.: 2013, SiO masers in the symbiotic star R Aquarii, The
4th KVN & VERA Joint Science WG Meeting, (Seoul, Korea
Jan. 29-30, 2013).
Minowa, Y., Hayano, Y., Terada, H., Pyo, T.-S., Oya, S., Hattori,
M., Shirahata, M., Takami, H., Guyon, O., Garrel, V., Colley, S.,
Weber, M., Golota, T., Watanabe, M., Saito, Y., Ito, M., Iye, M.:
2012, Subaru laser guide adaptive optics system: performanceand science operation, SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Miura, N., Miyazaki, J., Kuwamura, S., Baba, N., Hanaoka, Y.,
Yamaguchi, M., Ueno, S., Nakatani, Y., Nagata, S., Kitai,
R., Ichimoto, K., Takami, H.: 2012, Solar adaptive optics atthe Hida Observatory: latest achievements of current systemand design of new system, SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Miyata, T., et al. including Takato, N.: 2012, Evaluations of
new atmospheric windows at thirty micron wavelengths for
astronomy, SPIE Astronomical Telescope and Instrumentation,(Amsterdam, Netherlands, Jul. 1-6, 2012).

Mizuno, N.: 2012, ALMA observations of the LMC/SMC, East
Asian ALMA Science Workshop in Korea, (Daejeon Korea,
Sep. 12-13, 2012).
Mizuno, Y., Kashiwagi, K., Isizu, H., Nishikawa, J., Suto, H.,
Tamura, M., Kurokawa, T.: 2012, Multi-Gigahertz-Spaced
Frequency Comb Generation Using Optical Pulse Synthesizer
for Extra-Solar Planet Finder, The Conference on Lasers andElectro-Optics: Applications and Technology (CLEO_AT), (SanJose, USA, May, 6-11, 2012).
Muller, E.: 2012, Mopra status report, ALMA Users Meeting,(Mitaka, Japan, Nov. 20-22, 2012).
Muller, E.: 2012, An exploration of the un-evolved extragalactic
ISM of the Magellanic System, with the Mopra Telescope,
ALMA Workshop Science with Mopra for the ALMA, (Mitaka,
Japan, Jun. 8-9, 2012).
Murakami, N., Kida, M., Baba, N., Matsuo, T., Kotani, T.,
Kawahara, H., Fujii, Y., Tamura, M.: 2012, Development of theSavart-plate lateral-shearing interferometric nuller for exoplanet(SPLINE), SPIE Astronomical Telescope and Instrumentation,(Amsterdam, Netherlands, Jul. 1-6, 2012).
Murakami, N., Nishikawa, J., Traub, W. A., Mawet, D., Moody,
D. C., Kern, B. D., Trauger, J. T., Serabyn, E., Hamaguchi,
S., Oshiyama, F., Sakamoto, M., Ise, A., Oka, K., Baba, N.,
Murakami, H., Tamura, M.: 2012, Coronagraph focal-plane
phase masks based on photonic crystal technology: recent
progress and observational strategy, SPIE Astronomical Telescopeand Instrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Nagai, H., Kino, M., Niinuma, K., Akiyama, K., Hada, K.,
Koyama, S., Hiura, K., GENJI PROGRAMME MEMBER:
2012, VLBI Monitoring Programme of AGN Jets in Japan and
Future Prospects for Mm/submm VLBI, New Trend in Radio
Astronomy in the ALMA era, (Hakone, Japan, Dec. 3-8, 2012).
Nagai, H., Nakanishi, K., George M., Ed, F., Edwige, C.,
Richard, H., Stuartt, C.: 2012, Commissioning Status of ALMA
Polarization Observations, The First Year of ALMA Science,(Puerto Varas, Chile, Dec. 12-15, 2012).
Nagai, H.: 2012, ALMA polariztion capabilities, ALMA Users
Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Nagayama, T.: 2012, Report of activity for Astrometry science
sub-WG, The 3rd KVN & VERA Joint Science WG Meeting,(Mizusawa, Japan, Jul. 25-26, 2012).
Nagayama, T.: 2012, VERA observations of the Galactic star-forming
regions ON1 and ON2N, IAU Symp. 289: Advancing the Physics
of Cosmic Distances, (Beijing, China, Aug. 27-31, 2012).
Nakajima, T., Kimura, K., Katase, T., Koyano, M., Inoue, H., Sakai,T., Iwashita, H., Miyazawa, C., Asayama, S., Kuno, N., Ogawa,
H., Onishi, T., Kawabe, R., Noguchi, T.: 2012, Development ofa New Multi-Beam Array 2SB Receiver in 100 GHz Band for the
NRO 45-m Radio Telescope, 23rd International Symposium onSpace Terahertz Technology (ISSTT2012), (Tokyo, Japan, Apr.
2-4, 2012).
Nakamura, F., Awazu, Y., Takakuwa, S., Shimajiri, Y., Tanaka,T., Kawabe, R., Sugitani, K., Yoshida, H., Hara, C., Akashi,T., Onishi, T.: 2012, A Burst of Molecular Outflows From theSerpens South Cluster, EPoS 2012 The Early Phase of Star
Formation - Assembling Pieces of the Missing Paradigm,(Ringberg, Germany, Jul. 1-6, 2012).
Nakamura, F., Li, Z.-Y.: 2012, The Roles of Protostellar Outflow
Feedback in Clustered Star Formation, IAU Symp. 292:
Molecular Gas, Dust, and Star Formation in Galaxies, (Beijing,
China, Aug. 20-24, 2012).
Nakamura, F., Takakuwa, S., Kawabe, R.: 2012, SubstellarMass Condensations in Prestellar Cores, Star Formation & theInterstellar Medium : Thirty Five Years Later, (Berkeley, CA,
USA, Sep. 10-12, 2012).
Nakamura, F.: 2012, Present Day Star Formation: Theory andObservation, First Stars IV - From Hayashi to the Future, (Kyoto,
Japan, May 21-25, 2012).
Nakamura, F.: 2012, Molecular line observations toward afilamentary, cluster-forming IRDC, Serpens South, Star
Formation 2012, (Mitaka, Japan, Dec. 10-12).
Nakamura, F.: 2012, Star Formation in Magnetized Molecular
Clouds, APCTP Workshop on Astrophysics: Magnetic Fields in
Astrophysics, (Pohang, Korea, Nov. 19-22, 2012).
Nakamura, F.: 2012, The CCS Zeeman Project: Magnetic Field
Measurements Towards Prestellar Cores, New Trend in Radio
Astronomy in the ALMA era, (Hakone, Japan, Dec. 3-8, 2012).
Nakamura, F.: 2013, Toward Understanding of the Initial
Conditions of Star Cluster Formation:The Case of Serpens South,
Florida Star Formation 2012, (Gainesville, USA, Feb. 15, 2013).
Nakamura, F.: 2013, Protostellar Outflow Feedback and Cluster
Formation, Florida Astronomy Colloquium, (Gainesville, USA,
Jan. 30, 2013).
Nakamura, K., Harikae, S., Kajino, T., Mathews, G. J.: 2012, The
r-process in the neutrino-induced relativistic jet of a gamma-ray
burst, Nuclei in the Cosmos XII, (Cairns, Queensland, Australia,
Aug. 5-10, 2012).
Nakamura, K., Hayakawa, T., Kajino, T., Mathews, G. J.: 2012,
Neutrino-induced nucleosynthesis in supernova explosions,
4th International Symposium on Neutrinos and Dark Matter in
Nuclear Physics (NDM12), (Nara, Japan, Jun. 11-15, 2012).
Nakamura, K., Nishizawa, A., Fujimoto, M.-K.: 2012, Evaluationof weak measurements to all order and its applications, The
Principles and Applications of Control in Quantum Systems,(Tokyo, Japan. Sep. 10-13, 2012).
Nakamura, K., Takiwaki, T., Kotake, K., Nishimura, N.: 2012,
Multi-dimensional Simulations of Core-collapse Supernovae,
Quarks to Universe in Computational Science, (Nara, Japan,
Dec. 13-16, 2012).
Nakamura, K.: 2012, Problems in n-th order extension of generalrelativistic gauge-invariant perturbation theory, The 22ndworkshop on General Relativity and Gravitation in Japan,(Tokyo, Japan. Nov. 12-16, 2012).
Nakamura, K.: 2012, Construction of gauge-invariant variables
for linear-order metric perturbations on an arbitrary backgroundspacetime, The 13th Marchel Grossmann Meeting, (Stockholm,
Sweden, Jul. 1-7, 2012).
Nakamura, K.: 2013, Problems in n-th order extension of generalrelativistic gauge-invariant perturbation theory, 1st Annual
Symposium on New Developments in Astrophysics ThroughMulti-Messenger Observations of Gravitational Wave Sources,(Osaka, Japan, Mar. 1-2, 2013).

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Nakamura, K.: 2013, Problems in n-th order extension of generalrelativistic gauge-invariant perturbation theory, NishinomiyaYukawa Symposium on Gravity and Cosmology 2012, (Kyoto,
Japan. Dec. 4-5, 2012).
Narita, N.: 2012, Searching and characterizing new transiting
exoplanets around cool stars with Japanese facilities, Transiting
Planets in the House of the Sun, (Maui, HI, USA, Jun. 3-6, 2012).
Narita, N.: 2012, Photometric Studies of Transiting Exoplanets,
GUAS/SOKENDAI Asian Winter School 2012, (Mitaka, Japan,
Dec. 3-5, 2012).
Narita, N.: 2012, Time-Resolved Photometry and Spectroscopyof Transiting Exoplanetary Systems, TMT Science andInstrumentation Workshop, (Pune, India, Dec. 10-12, 2012).
Narita, N.: 2013, Transmission Spectroscopy of a Transiting
Super-Earth GJ1214b, Subaru Users' Meeting 2012, (Mitaka,
Tokyo, Japan, Jan. 15-17, 2013).
Narita, N.: 2013, Candidate Stellar Companions around Transiting
Planets with High Obliquity, Exoplanets in Multi-body Systems
in the Kepler Era, (Aspen, CO, USA, Feb. 10-15, 2013).
Naruse, M., Sekimoto, Y., Miyachi, A., Uzawa, Y., Nitta, T.,
Karatsu, K., Sekine, M., Noguchi, T.: 2012, Development of
a MKID camera with high-quality Al films for millimeter-wave
astronomy, 23rd International Symposium on Space Terahertz
Technology (ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Niino, Y.: 2012, The Mass-SFR-Metallicity Relation of Star
Forming Galaxies and Its Evolution: Implications for GRB/SN
Host Galaxies, 15 years of Gamma-Ray Bursts afterglows,(Marbella, Spain, Oct. 8-12, 2012).
Nishikawa, J., Yokochi, K., Murakami, N., Abe, L., Kotani,T., Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.,
Murakami, H.: 2012, A coronagraph system with unbalanced
nulling interferometer: progress of dynamic range, SPIE
Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Nitta, T., Naruse, M., Sekimoto, Y., Karatsu, K., Sekine, M.,
Mitsui, K., Okada, N., Matsuo, H., Noguchi, T., Uzawa, Y.,
Seta, M., Nakai, N.: 2012, Beam Pattern Measurements ofMillimeter-wave MKIDs Camera with Direct Machined Silicon
Lens Array, 23rd International Symposium on Space Terahertz
Technology (ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Niwa, Y., Ueda, A., Yano, T., Gouda, N., Kobayashi, Y., Yamada, Y.:
2012, Sub-nanometer scale measurement of thermal deformation
for telescope components by a heterodyne laser interferometer,
SPIE Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Noda, H., Araki, H., Hanada, H., Iwata, T., Kikuchi, F.,
Kunimori, H., Matsumoto, K., Namiki, N., Sasaki, S.: 2012,
Geodetic experiments in Kaguya (SELENE) and SELENE-2,
AOGS - AGU (WPGM) Joint Assembly, (Singapore, Aug.
13-17, 2012).
Noda, H., Araki, H., Hanada, H., Kashima, S., Katayama, M.,
Sasaki, S., Tazawa, S., Tsuruta, S., Kunimori, H., Fuse, T.,
Otsubo, T., Funazaki, K., Sato, A., Taniguchi, H., Murata, K.,
Mashiko, H.: 2012, Lunar Laser Ranging (LLR) for SELENE-2:
science goal and developmentstatus, Seminar on Lunar andPlanetary Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).

104

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Noda, H., Kunimori, H., Araki, H., Funazaki, K., Fuse, T., Hanada,
H., Kashima, S., Katayama, M., Mashiko, H., Matsumoto,Y., Murata, K., Otsubo, T., Sasaki, S., Taniguchi, H., Tazawa,
S., Utsunomiya, S.: 2012, Development status of lunar laser
ranging experiment aboard japanese lunar lander selene-2, 3rd
Moscow Solar System Symposium (3M-S3), (Space ResearchInstitute, Moscow, Russia, Oct. 8-11, 2012).
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 Japanese SELENE-2 landing mission,
EGU General Assembly, (Vienna, Austria, Apr. 22-27, 2012).
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 experimentfor SELENE-2, 43rd Lunar and Planetary Science Conference(LPSC 2012), (Texas, 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., Funazaki, K.,
Taniguchi, H., Murata, K.: 2012, Development status of the Lunar
Laser Ranging Experiment for SELENE-2, European Lunar
Symposium (ELS2012), (Berlin, Germany, Apr. 19-20, 2012).
Noda, H.: 2013, Development Status of SELENE-2 LLR, Lunar
Laser Ranging, Russia-Japan Scientific Meeting on someproblems in the exploration of space and joint projects, (Kazan
Aviation University, Russia, Mar. 15, 2013).
Noguchi, T.: 2012, RF conductivity and surface impedance of asuperconductor taking into account the complex superconducting
gap energy, Applied Superconductivity Conf., (Portland, OR,
USA, Oct. 7-12, 2012).
Nomura, H., Walsh, C., Heinzeller, D., Millar, T. J.: 2012, Water
in Protoplanetary Disks, The Astrochemical Universe Unveiled
with Herschel, (Rome, Italy, Sep. 3, 2012).
Nomura, H., Walsh, C., Heinzeller, D., Millar, T. J.: 2012, Water
in Protoplanetary Disks, IAU Symp. 293: Formation, Detection,
and Characterization of Extrasolar Habitable Planets, (Beijing,
China, Aug. 27-31, 2012).
Nomura, H., Walsh, C., Millar, T. J., Aikawa, Y.: 2012, Diagnosing
Gas Dispersal Processes in Protoplanetary Disks, New Trends
in Radio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Ohashi, N.: 2012, Kepler Disks around Protostars: from NMA
to SMA and ALMA, New Trends in Radio Astronomy in
the ALMA Era -The 30th Anniversary of Nobeyama Radio
Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Ohashi, N.: 2012, Keplerian Disk Formation around Protostars,
The First Year of ALMA Science, (Puerto Varas, Chile, Dec.
12-15, 2012).
Ohishi, M.: 2012, Activities towards Data Intensive Astronomy
in Japan, CODATA 23 International Conference: Open Data &Information for a Changing Planet, (Taipei, Taiwan, Oct. 28-31,
2012).
Ohishi, M.: 2012, Radio Astronomy and the Future, ITU Regional
Seminar, (Manta, Ecuador, Sep. 20-21, 2012).
Ohishi, M.: 2013, Searching for Seeds of Life in the Universe,
NINS Astrobiology Workshop, (Tokyo, Japan, Mar. 3, 2013).

Ohsuga, K.: 2012, Radiation-MHD Simulations of Accretion
Flows and Outflows around Black Holes, ASTRONUM 2012,(Hawaii, USA, Jun. 24-29, 2012).
Ohsuga, K.: 2012, Overview of Recent Advances in Accretion
Disk Theory, 2012 X-ray Binaries, (Boston, MA, USA, Jul.
10-12, 2012).
Ohsuga, K.: 2012, Simulations of the radiation-pressure instabilityof disk and outflow, Accretion flow instabilities, (Warsaw,
Poland, Sep. 4-7, 2012).
Ohsuga, K.: 2012, Launching mechanisms, The Physics ofAccretion onto Black Holes, (Bern, Switzerland, Oct. 8-12,
2012).
Ohsuga, K.: 2012, Radiation Magnetohydrodynamics of Black Hole
Accretion Flows and Outflows, The 5th East Asia Numerical
Astrophysics Meeting, (Kyoto, Japan, Oct. 29-Nov. 2, 2012).
Okita, H., Takato, N., Ichikawa, T., Bonner, C. S., Ashley, M. C. B.,
Storey, J. W. V.: 2013, Dome Fuji Seeing -the Summer Results
and the Future Winter-over Observations, IAU Symp. 288:
Astrophysics from Antarctica, (Beijing, China, Aug. 20-24, 2012).
Onishi, K., Iguchi, S., Okuda, T.: 2012, Derivation of the Mass ofSuper-Massive Black Hole, The First Year of ALMA Science,(Puerto Varas, Chile, Dec. 12-15, 2012).
Onishi, K., Iguchi, S., Muller, E., Nagai H.: 2012, Rotating
Molecular Gases of 3C 31 with ALMA, East Asian ALMA
Science Workshop in Korea, (Daejeon Korea, Sep. 12-13, 2012).
Onishi, K., Iguchi, S., Okuda T.: 2012, Derivation of the Mass ofSuper-Massive Black Hole, New Trends in Radio Astronomy
in the ALMA Era -The 30th Anniversary of Nobeyama Radio
Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Onishi, K., Iguchi, S., Okuda, T.: 2012, Derivation of the Massof Super-Massive Black Hole, ALMA Users Meeting, (Mitaka,
Japan, Nov. 20-22, 2012).
Onishi, K., Iguchi, S., Okuda, T.: 2012, SMBH Mass Estimation
with Rotating Gas inside Nearby Galaxies, Supermassive Black
Holes in the Universe: The Era of the HSC Surveys, (Ehime,
Japan, Dec. 18-20, 2012).
Onishi, K., Iguchi, S.: 2012, Molecular Line Survey of Giant
Elliptical Galaxies, ALMA Workshop Science with Mopra for
the ALMA, (Mitaka, Japan, Jun. 8-9, 2012).
Ootsubo, T., Kawakita, H., Hamada, S., Kobayashi, H., Yamaguchi,
M., Usui, F., Nakagawa, T., Ueno, M., Ishiguro, M., Sekiguchi,T., Watanabe, J., Sakon, I., Shimonishi, T., Onaka, T.: 2012,AKARI Near-Infrared Spectroscopic Survey for Carbon
Dioxide in Comets, Asteroids, Comets, Meteors 2012, (Niigata,Japan, May 16-20, 2012).
Oshigami, S., Watanabe, S., Yamaguchi, Y., Yamaji, A., Kobayashi,T., Kumamoto, A., Ono, T.: 2012, Mare volcanism in thenearside of the Moon: Reinterpretation based on Kaguya LRS
data, Seminar on Lunar and Planetary Geodesy, (Mitaka, Japan,
Jun. 19-20, 2012).
Oshigami, S., Watanabe, S., Yamaguchi, Y., Yamaji, A., Kobayashi,T., Kumamoto, A., Ono, T.: 2012, Mare Volcanism in thenearside of the Moon: Reinterpretation based on Kaguya LRS
data, AGU Fall Meeing 2012, (San Francisco, CA, USA, Dec.
3-7, 2012).
Oshigami, S., Watanabe, S., Yamaguchi, Y., Yamaji, A., Kobayashi,T., Kumamoto, A., Ono, T.: 2013, Formation histories of multilayered maria, SELENE Symposium, (ISAS, JAXA, Japan, Jan.
23-25, 2013).
Oshino, S., Hori, Y., Kokubo, E., Ida, S.: 2012, Planet Formation
around M-Type Stars, Planet formation and evolution 2012, 8th
Conference on Formation and Evolution of Planetary systems,(Munich, Germany, Sep. 3-7, 2012).
Oshino, S.: 2012, Planet formation around M-type stars, Planet
formation and evolution 2012, 8th Conference on Formationand Evolution of Planetary systems, (Munich, Germany, Sep.
3-7, 2012).
Oshino, S.: 2012, Dynamics of stars with planetesimals using P3T,
MODEST-12, (Kobe, Japan, Aug. 15-17, 2012).
Otsuji, K.: 2012, Magnetic field evolution in emerging flux
regions observed by SOT/SP, The 6th Hinode Science Meeting,(U. St. Andrews, UK, Aug. 12-15, 2012).
Oya, M., Nishikawa, J., Horie, M., Murakami, N., Kotani, T.,
Abe, L., Kumagai, S., Tamura, M., Kurokawa, T., Murakami,
H.: 2012, Adaptive optics operation with two wavefront sensors
in a coronagraph for exoplanet observations, SPIE Astronomical
Telescope and Instrumentation, (Amsterdam, Netherlands, Jul.
1-6, 2012).
Oya, S., Akiyama, M., Hayano, Y., Minowa, Y., Iwata, I., Terada,
H., Usuda, T., Takami H., Nishimura, T., Kodama, T., Takato,N., Tomono, D., Ono, Y.: 2012, A preliminary simulation resultof the next-generation wide-field AO at Subaru Telescope, SPIE
Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Oyama, T.: 2012, New VLBI observing system OCTAVE-family
based on the VDIF speci cations for VERA, JVN and KJJVC,EVN Symposium 2012, (Bordeaux, France, Oct. 9-12, 2012).
Ozaki, S., Ishigaki, T., Hattori, T., Ohtani, H., Sugai, H., Hayashi,
T.: 2012, Indirect estimations of UV luminosity of LINERs with
optical narrow-band imaging, AGN workshop 2012 in Jeju,(Jeju, South Korea, Sep. 12-14, 2012).
Ozaki, S., Kitagawa, Y., Motohara, K., Konishi, M., Takahashi,
H., Yoshikawa, T., Tateuchi, K., Kato, N.: 2012, Developmentof an integral field unit for a near-infrared multi-object imaging
spectrograph SWIMS, Modern Technologies in Space- andGround-based Telescopes and Instrumentation II, (Amsteldam,
Nertherlands, July. 1-6, 2012).
Ozaki, S., Tanaka, Y., Hattori, T., Kenji, M., Fukushima, M.,
Okada, N., Obuchi, Y., Miyazaki, S., Yamashita, T.: 2012,
Development of a slicer integral ﬁeld unit for the existing
optical imaging spectrograph FOCAS, Modern Technologies inSpace- and Ground-based Telescopes and Instrumentation II,(Amsteldam, Nertherlands, July. 1-6, 2012).
Pan, H.-A., Kuno, N., Hirota, A.: 2012, Kennicutt-Schmidt Law
from Nearby Galactic Center to the Disk: On the Aspect of
13CO, New Trends in Radio Astronomy in the ALMA Era -The
30th Anniversary of Nobeyama Radio Observatory-, (Hakone,
Japan, Dec. 3-8, 2012).
Peters, M. A., Groff, T., Kasdin, N. J., McElwain, M. W., Galvin,
M., Carr, M. A., Lupton, R., Gunn, J. E., Knapp, G., Gong, Q.,
Carlotti, A. B., Janson, M., Guyon, O., Martinache, F., Hayashi,M., Takato, N.: 2012, Conceptual design of the Coronagraphic

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105

High Angular Resolution Imaging Spectrograph (CHARIS)
for the Subaru telescope, SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Petrova, N., Abdulmyanov T., Hanada, H.: 2012, Some preliminary
estimates of the possibility of determining the Lunar physicallibration in the project ILOM, Japan Geoscience Union Meeting
2012, (Chiba, Japan, May 20-24, 2012).
Ping, J., Gusev, A., Hanada, H., Li, J., et al.: 2012, May Small
Digital PZT And Radio Beacons Improve The LPhL For Future
Lunar Missions, XXVIIIth IAU General Assembly, (Beijing,
China, Aug. 20-31, 2012).
Saito, M., Inatani, J., Nakanishi, K., Saito, H., Iguchi, S.: 2012,
Atacama compact array antennas, SPIE Astronomical Telescopeand Instrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Saito, T., Iono, D., Kawabe, R.: 2012, ALMA observations of
the IR bright merger VV114, ALMA Users Meeting, (Mitaka,
Japan, Nov. 20-22, 2012).
Saito, T., Iono, D., Kawabe, R.: 2012, ALMA Cycle 0 observationsof a LIRG VV114, East Asian ALMA Science Workshop in
Korea, (Daejeon Korea, Sep. 12-13, 2012).
Saito, T., Iono, D., Yun, M., Ueda, J., Espada, D., Hagiwara, Y.,
Imanishi, M., Motohara, K., Nakanishi, K., Sugai, H., Tateuchi,
K., Kawabe, R.: 2012, ALMA Observations of the IR-brightMerger VV114, ALMA Users Meeting, (Mitaka, Japan, Nov.
20-22, 2012).
Saito, T., Iono, D., Yun, M., Ueda, J., Espada, D., Hagiwara, Y.,
Imanishi, M., Motohara, K., Nakanishi, K., Sugai, H., Tateuchi,
K., Kawabe, R.: 2012, ALMA Observations of the IR-brightMerger VV114, East Asian ALMA Science Workshop in Korea,(Daejeon Korea, Sep. 12-13, 2012).
Saito, T., Iono, D., Yun, M., Ueda, J., Espada. D., Hagiwara, Y.,
Imanishi, M., Motohara, K., Nakanishi, K., Sugai, H., Tateuchi,
K., Kawabe, R.: 2012, ALMA Observations of the IR-brightMerger VV114, New Trends in Radio Astronomy in the ALMA
Era -The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Saito, T., Iono., D., Yun, M., Ueda, J., Espada, D., Hagiwara, Y.,
Imanishi, M., Motohara, K., Nakanishi, K., Sugai, H., Tateuchi,
K., Kawabe, R.: 2012, ALMA Observations of the IR-brightMerger VV114, The First Year of ALMA Science, (Puerto
Varas, Chile, Dec. 12-15, 2012).
Sakai, N., Honma, M., Nakanishi, H., Sakanoue, H., Kurayama,
T.: 2012, The outer rotation curve project with VERA:
Trigonometric parallax of IRAS 05168+3634, IAU Symp. 289:
Advancing the Physics of Cosmic Distances, (Beijing, China,
Aug. 27-31, 2012).
Sakai, N.: 2012, Outer Rotation Curve project with VERA, East Asia
VLBI Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Sakai, N.: 2012, Outer Rotation Curve measurements with
KAVARRAY (Kvn And Vera ARRAY), The 3rd KVN & VERA
Joint Science WG Meeting, (Mizusawa, Japan, Jul. 25-26, 2012).
Sakai, N.: 2013, Absolute proper motions of IRAS 00259+5625,
The 4th KVN & VERA Joint Science WG Meeting, (Seoul,
Korea Jan. 29-30, 2013).
Sako, N., Shimojo, M.: 2012, The statistical study of the X-ray jet
and transient brightening around the north pole, The 6th Hinode106

II Publications, Presentations

Science Meeting, (U. St. Andrews, UK, Aug. 12-15, 2012).
Sako, N.: 2012, The relation of the activities and magnetic eld inpolar coronal hole, The 6th Hinode Science Meeting, (U. St.
Andrews, UK, Aug. 12-15, 2012).
Sakurai, T.: 2012, Magnetic Helicity as a Probe of Magnetic FluxTube Dynamics in the Solar Interior, IAU Symp. 294: Solar andAstrophysical Dynamos and Magnetic Activity, (Beijing, China,
Aug. 27-31, 2012).
Sasaki, S., et al.: 2012, Investigation of the lunar deep interior by
SELENE-2, 39th COSPAR Scientific Assembly, (Mysore, India,
Jul. 14-22, 2012).
Sasaki, S., et al.: 2012, Selenodesy results by KAGUYA mission,
39th COSPAR Scientific Assembly, (Mysore, India, Jul. 14-22,
2012).
Sasaki, S., Goossens, S., Ishihara, Y., Araki, H., Hanada, H.,
Matsumoto, K., Noda, H., Kikuchi, F., Iwata, T., Kawano,N.: 2013, Formation History of South Pole Aitken - from
Selenodesy and Other Kaguya data, SELENE Symposium,(ISAS, JAXA, Japan, Jan. 23-25, 2013).
Sasaki, S., Ishihara, Y., Goossens, S., Araki, H., Matsumoto, K.,
Noda, H., Hanada, H., Kikuchi, F., Namiki, N., Iwata, T.,
Kunimori, H., Otsubo, T., Funazaki, K.: 2012, New Scientific
Observations in Lunar and Planetary Exploration, International
Symposium on Lunar and Planetary Science (ISLPS 2012),(Macau, China, Mar. 26-27, 2012).
Sasaki, T., Yao, Y., Yoshida, M., Ohshima, N., Mikami, Y., Okada,N., Koyanao, H., Nagayama, S., Sekiguchi, K., Ando, H., Liu,
L.: 2012, China-Japan Collaborative Site Testing in West China,
EACOA: Site Survey Workshop, (Beijing, China, Apr. 3-4, 2012).
Sato, M., Watanabe, J., Ohkawa, T.: 2012, Observation of
October Draconids 2011 in Maidanak Observatory and Studyof its Peak Time, Asteroids, Comets, Meteors 2012, (Niigata,Japan, May 16-20, 2012).
Sato, S., Misawa, H., Tsuchiya, F., Iwai, K., Masuda, S., Miyoshi,
Y., Obara, T.: 2012, Fine spectral structures of a solar radio
type-II burst observed with AMATERAS, Solar Physics with
Radio Observations, (Aichi, Japan, Nov. 20-23, 2012).
Sawada, T., Hasegawa, T., Koda, J., Handa, T., Sugimoto, M.:
2012, Structured Molecular Gas Reveals Galactic Spiral Arms,
New Trends in Radio Astronomy in the ALMA Era -The 30th
Anniversary of Nobeyama Radio Observatory-, (Hakone, Japan,
Dec. 3-8, 2012).
Sawada, T.: 2012, ALMA Observation mode, calibration, and imaging,
ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Sawada-Satoh, S.: 2012, Introduction of AIPS, VERA+KVN SFR
Sub WG AIPS Tutorial, (Seoul, Korea, May 7-11, 2012).
Sawada-Satoh, S.: 2012, Internal Proper Motion of 6.7 GHz Methanol
Masers in an Ultra Compact HII Region S269, East Asia VLBI
Workshop 2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Sawada-Satoh, S.: 2012, Internal Proper Motion of 6.7 GHz
Methanol Masers in an Ultra Compact HII Region S269, EVN
Symposium 2012, (Bordeaux, France, Oct. 9-12, 2012).
Sawada-Satoh, S.: 2013, The AGN-Starburst Connection, The 4th
KVN & VERA Joint Science WG Meeting, (Seoul, Korea Jan.
29-30, 2013).
Schneider, G., Carson, J., Debes, J., Goto, M., Grady, C., Henning, T.,Hines, D., Hinz, P., Jang-Condell, H., Kuchner, M., Moro-Martin,A., Marshall, P., Serabyn, G., Silverstone, M., Stark, C., Tamura,M., Weinberger, A., Wisniewski, J., Woodgate, B.: 2012, Probingfor Exoplanets Hiding in Dusty Debris Disks II: Disk Imaging,
Characterization, and Exploration with HST/STIS Multi-Roll
Coronagraphy - Update, American Astronomical Society, (LongBeach, CA, USA, Jan. 6-10, 2013).
Sekii, T., Shibahashi, H.: 2012, Avoided crossing and synchronization,
Progress in Physics of the Sun and Stars: A New Era in Helioand Asteroseismology, (Hakone, Japan, Nov. 26-29, 2012).
Sekii, T.: 2012, Solar C/D, ISSI Workshop on Helioseismology andDynamics of the Solar Interior, (Bern, Switzerland, Sep. 24-28,
2012).
Sekimoto, Y.: 2013, Submillimeter Camera Development for
LiteBIRD and South Pole Dome-Fuji Telescope, 13th Workshop
on Submm Wave Receiver Technologies in Eastern Asia,(Nanjing, China, Jan. 10-12, 2013).
Seta, M., Nakai, N., Ishii, S., Nagai, M., Miyamoto, Y., Ichikawa,T., Takato, N., Motoyama, H.: 2013, Dome Fuji in Antarctica
as a Site for Infrared and Terahertz Astronomy, IAU Symp. 288:
Astrophysics from Antarctica, (Beijing, China, Aug. 20-24, 2012).
Shi, S. C., Paine, S., Yao, Q. J., Lin, Z. H., Li, X. X., Duan, W. Y.,
Matsuo, H., Zhang, Q., Yang, J., Ashley, M. C. B., Shang, Z.
H., Hu, Z. W.: 2012, THz atmospheric transmission measured at
antarctic Dome A, IRMMW-THz2012, (Wollongong, Australia,
Sep. 23-28, 2012).
Shi, S. C., Paine, S., Yao, Q. J., Lin, Z. H., Li, X. X., Duan, W.
Y., Matsuo, H., Zhang, Q., Yang, J., Ashley, M., Shang, Z. H.,
Hu, Z. W.: 2012, A Fourier Transform Spectrometer for the
Atmospheric Measurement at Dome A, XXVIIIth IAU General
Assembly, (Beijing, China, Aug. 20-31, 2012).
Shibagaki, S.: 2013, Nuclear fission in the r-process nucleosynthesis,
10th Russbach School on Nuclear Astrophysics, (Russbach,Salzburg, Austria, Mar. 10-15, 2013).
Shibasaki, K.: 2012, Quiet Sun, Active regions and Global Solar
Activity studied by Nobeyama Radioheliograph, Solar Physics
with Radio Observations, (Aichi, Japan, Nov. 20-23, 2012).
Shibasaki, K.: 2012, Coronal Magnetic Field in Post Flare Loops,
Workshop on Coronal Magnetism, (Boulder, USA, May 21-23,
2012).
Shibasaki, K.: 2012, Relation between Solar Activities at Low andHigh Latitudes Inferred from Microwave Observations, IAU
General Assembly JD3, (Beijing, China, Aug. 19-24, 2012).
Shibasaki, K.: 2012, Hot Plasma Flows in the Solar Corona, AGU
Fall Meeing 2012, (San Francisco, CA, USA, Dec. 3-7, 2012).
Shibasaki, K.: 2013, Highlights of Nobeyama Solar Results: From
Nobeyama To ALMA, Solar ALMA Workshop, (Glasgow, UK,
Jan. 14-17, 2013).
Shibasaki, K.: 2013, Long-term global solar activity observed by
Nobeyama Radioheliograph, STEL-KASI workshop, (Nagoya,Japan, Mar. 18-19, 2013).
Shibata, K. M.: 2013, Status of VERA, The 4th KVN & VERA
Joint Science WG Meeting, (Seoul, Korea Jan. 29-30, 2013).
Shimajiri, Y., Kawabe, R., Sakai, T., Kitamura, Y., Momose, M.,
Tsukagoshi, T., Nakamura, F.: 2012, Line-Survey Observationsat 82–106 GHz and 335–355 GHz toward Outflow-Interacting

Region, OMC-2/FIR 4, New Trend in Radio Astronomy in the
ALMA era, (Hakone, Japan, Dec. 3-8, 2012).
Shimoikura, T., Dobashi, K., Onishi, T., Ogawa, H., Kimura, K.,
Nishimura, A., Matsumoto, T., Nakamura, F., Saito, H.: 2012,
Cluster Formation in the Sh247/ Sh252/ BFS52 Regions, New
Trend in Radio Astronomy in the ALMA era, (Hakone, Japan,
Dec. 3-8, 2012).
Shimojo, M.: 2012, Polar eld reversal observed with Hinode, The 6th
Hinode Science Meeting, (U. St. Andrews, UK, Aug. 12-15, 2012).
Shimojo, M.: 2012, Database and Data Analysis in Solar Physics,
CODATA 23 International Conference: Open Data & Information
for a Changing Planet, (Taipei, Taiwan, Oct. 28-31, 2012).
Shimojo, M.: 2012, Prominence Activities Observed with NoRH,
Solar Physics with Radio Observations, (Aichi, Japan, Nov.
20-23, 2012).
Shimojo, M.: 2012, Solar Observations by ALMA, Solar Physics
with Radio Observations, (Aichi, Japan, Nov. 20-23, 2012).
Shimojo, M.: 2013, The ARC activities for solar ALMA observationsin Japan, Solar ALMA Workshop, (Glasgow, UK, Jan. 14-17,
2013).
Shino, N.: 2012, Testing the formation scenario of massive starby CH3OH maser, The 3rd KVN & VERA Joint Science WG
Meeting, (Mizusawa, Japan, Jul. 25-26, 2012).
Shino, N.: 2012, Testing the Formation Scenario of Massive Star by
CH3OH Maser, New Trends in Radio Astronomy in the ALMA
Era -The 30th Anniversary of Nobeyama Radio Observatory-,(Hakone, Japan, Dec. 3-8, 2012).
Shino, N.: 2013, VLBI observations of 6.7-GHz methanol masers
in massive SFRs, The 4th KVN & VERA Joint Science WG
Meeting, (Seoul, Korea Jan. 29-30, 2013).
Shirasaki, Y., Kawasaki, W., Eguchi, S., Komiya, Y., Kosugi, G.,
Ohishi, M., Mizumoto, Y.: 2012, Web and Desktop Applications
for ALMA Science Verification Data, Astronomical Data Analysis
Software and Systems (ADASS) Conference XXII, (Champaign,
IL, USA, Nov. 4-8, 2012).
Shirasaki, Y., Komiya, Y., Eguchi, S., Ohishi, M., Mizumoto, Y.,
Ishihara, Y., Ohnishi, T., Tsutsumi, J., Hiyama, T., Nakamoto,
H., Sakamoto, M.: 2012, Japanese Virtual Observatory I: An
On-line Astronomical Research Facility, IAU General Assembly2012 Special Session 15: Data intensive astronomy, (Beijing,
China, Aug. 20-31, 2012).
Shirasaki, Y., Komiya, Y., Eguchi, S., Ohishi, M., Mizumoto,Y., Takata, T., Yasuda, N.: 2012, Clustering of galaxies aroundbright QSOs at redshift ~1.5, IAU General Assembly 2012
Special Session 2: Cosmic evolution of groups and clusters ofgalaxies, (Beijing, China, Aug. 20-31, 2012).
Sôma, M.: 2012, Lunar Limb Profiles Predicted from the Lunar
Topographic Data of Kaguya and LRO, Spring Meeting of
Korean Astronomical Society, (Gyeongju, Korea, Apr. 5-6, 2012).
Sotani, H., Nakazato, K., Iida, K., Oyamatsu, K.: 2012, Probing
the nuclear EOS via neutron star asteroseismology, CompStar:
the physics and astrophysics of compact stars, (Tahiti, French
Polynesia, Jun. 4-8, 2012).
Sotani, H., Nakazato, K., Iida, K., Oyamatsu, K.: 2012, Constraints
on the nuclear symmetry energy via asteroseismology, NEB15,(Crete, Greece, Jun. 20-23, 2012).

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Suda, T., Komiya, Y., Yamada, S., Katsuta, Y., Aoki, W., Gil-Pons,P., Doherty, C. L., Campbell, S. W., Wood, P. R., Fujimoto, M. Y.:
2012, AGB Evolution and Nucleosynthesis at Low-Metallicity
Constrained by the Star Formation History of Our Galaxy,
Nuclei in the Cosmos XII, (Cairns, Queensland, Australia, Aug.
5-10, 2012).
Suda, T., Komiya, Y., Yamada, S., Katsuta, Y., Aoki, W., Gil-Pons,P., Doherty, C. L., Campbell, S. W., Wood, P. R., Fujimoto,
M. Y.: 2012, Transition of the Initial Mass Function Based on
Binary Population Synthesis, IAP-Subaru Joint International
Conference: Stellar Populations across Cosmic Times, (Paris,
France, Jun. 25-29, 2012).
Suda, T., Komiya, Y., Yamada, S., Katsuta, Y., Aoki, W., Gil-Pons,P., Doherty, C. L., Campbell, S. W., Wood, P. R., Fujimoto, M.
Y.: 2012, Transition of the Initial Mass Function in the Galaxy
Based on Binary Population Synthesis, First Stars IV - From
Hayashi to the Future, (Kyoto, Japan, May 21-25, 2012).
Suda, T.: 2012, Analysis of Element Enrichment History during
the Early Universe with the SAGA Database, 1st NAOJ Visiting
Fellow Workshop Program on Element Genesis and Cosmic
Chemical Evolution: r-process perspective, (Wako, Saitama,
Japan, Oct. 17-19, 2012).
Suda, T.: 2012, SAGA: Stellar Abundances for Galactic Archaeology,
Nuclei in the Cosmos XII, (Cairns, Queensland, Australia, Aug.
5-10, 2012).
Suematsu, Y.: 2012, Solar Spicules are all Twins?, The 6th Hinode
Science Meeting, (U. St. Andrews, UK, Aug. 12-15, 2012).
Suematsu, Y., Katsukawa, Y., Ichimoto, K., Shimizu, T.: 2012,
Science and Instrument Design of 1.5-m Aperture Solar Optical
Telescope for the SOLAR-C Mission, IAU General Assembly2012 Special Session 6: Science with large solar telescopes,(Beijin, China, Aug. 22-24, 2012).
Suematsu, Y., Katsukawa, Y., Shimizu, T., Ichimoto, K.: 2012,
Instrument Design of 1.5-m Aperture Solar Optical Telescope
for the SOLAR-C Mission, International Conference on Space
Optics, (Ajaccio, Corse, France, Oct. 9-12, 2012).
Sugai, H., et al. including Takato, N., Ueda, A.: 2012, Prime focus
spectrograph: Subaru's future, SPIE Astronomical Telescopeand Instrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Sugimoto, K.: 2012, CASA status report, ALMA Users Meeting,(Mitaka, Japan, Nov. 20-22, 2012).
Sugita, S., Kuroda, D., Kameda, S., Hasegawa, S., Kamata, S.,
Abe, M., Ishiguro, M., Takato, N., Yoshikawa, M.: 2012, Visible
Spectroscopic Observation Of Asteroid 162173 (1999 JU3)
With The Gemini-s Telescope, 44th annual meeting of theDivision for Planetary Sciences of the American Astronomical
Society, (Reno, NV, USA, Oct. 14-19, 2012).
Sugita, S., Kuroda, D., Kameda, S., Hasegawa, S., Kamata, S.,
Hiroi, T., Abe, M., Ishiguro, M., Takato, N., Yoshikawa, M.:
2013, Visible Spectroscopic Observations of Asteroid 162173(1999 JU3) with the Gemini-S Telescope, 44th Lunar andPlanetary Science Conference, (Woodlands, TX, USA, Mar.
18-22, 2013).
Suzuki, A., Shigeyama, T.: 2012, Early thermal X-ray emission
from GRB-SNe and their circumstellar environment, Supernovae
Illuminating the Universe: from Individuals to Populations ,108

II Publications, Presentations(Garching bei München, Germany, Sep. 10-14, 2012).
Suzuki, T., Honma, M., Yoshida, T., Kajino T., Otsuka, T.: 2012,
Electron capture reactions and beta-decays in astrophysicalprocesses, NIC XII Workshop on r-process nucleosynthesis,(Cairns, Australia, Aug. 4-10, 2012).
Suzuki, T., Horita, T., Ohishi, M.: 2012, Distribution of CCS and
HC3N in L1147, A Less Evolved Molecular Cloud, Workshop
in Interstellar Matter 2012, (Sapporo, Japan, Sep. 17-19, 2012).
Suzuki, T., Ohishi, M., Horita, T.: 2012, Distribution of CCS and
HC3N in L1147, A Less Evolved Molecular Cloud, New Trend
in Radio Astronomy in the ALMA era, (Hakone, Japan, Dec. 3-8,2012).
Suzuki, T., Otsuka, T., Honma, M.: 2012, Spin-dependent modes innuclei and nuclear forces, The 2nd Nuclear Physics Conferenceon Nuclear Structure and Dynamics, (Opatija, Croatia, Jul. 13,
2012).
Suzuki, T.: 2012, Roles of tensor and three-body forces on shellevolutions and spin degrees-of-freedom, The Extreme Matter
Physics of Nuclei: From Universal Properties to Neutron-Rich
Extremes, (Darmstadt, Germany, May 3, 2012).
Suzuki, T.: 2012, Nuclear Weak Proceeses in Stars, CompStar:
the physics and astrophysics of compact stars, (Tahiti, French
Polynesia, Jun. 4-8, 2012).
Suzuki, T.: 2012, Neutrino-nucleus reactions based on recent shellmodel interactions, 4th International Symposium on Neutrinos
and Dark Matter in Nuclear Physics (NDM12), (Nara, Japan,
Jun. 11-15, 2012).
Suzuki, T.: 2012, Spin structure of nuclei and nuclear weakprocesses in stars, The 2nd Dogye Workshop on Nuclear
Astrophysics, (Dogye, Korea, Aug. 2, 2012).
Suzuki, T.: 2012, Beta-decays of isotones with N=126 and nearby
and r-process nucleosynthesis, NIC XII Workshop on r-process
nucleosynthesis, (Cairns, Australia, Aug. 4-10, 2012).
Suzuki, T.: 2012, Nuclear structure, weak-induced reactions andnucleosynthesis, 1st NAOJ Visiting Fellow Workshop Programon Element Genesis and Cosmic Chemical Evolution: r-processperspective, (Wako, Saitama, Japan, Oct. 17-19, 2012).
Suzuki, T.: 2012, Neutrino nucleus reactions based on recent
structure studies, The 8th International Workshop on NeutrinoNucleus Interactions in the Few-Gev Region, (Rio de Janeiro,
Brasil, Oct. 21-27, 2012).
Suzuki, T.: 2012, Nuclear Structure and Nuclear AstrophysicalProcesses, Symposium Italy-Japan 2012 on Nuclear Physics ,(Milano, Italy, Nov. 20, 2012).
Takahashi, H. R.: 2012, Magnetic Reconnection in Relativistic
Plasmas, The 5th East Asia Numerical Astrophysics Meeting,(Kyoto, Japan, Oct. 29-Nov. 2, 2012).
Takahashi, H. R.: 2012, Numerical Study of Relativistic
Magnetohydrodynamic Reconnection and its Radiative Effects,
13th Marcel Grossmann Meeting, (Stockholm, Sweden, Jul.
1-7, 2012).
Takahashi, H. R.: 2012, Radiative MHD Simulation of Relativistic
Magnetic Reconnection, 2012 US-Japan Workshop on Magnetic
Reconnection (MR2012), (Princeton, NJ, USA, May 23-25,
2012).
Takahashi, R., Saito, Y.: 2012, A Large Seismic Attenuation System

in UHV, AVS 59th International Symposium & Exhibition,(Tampa, FL, USA, Oct. 28-Nov. 2, 2012).
Takahashi, R., Yamamoto, K., Uchiyama, T., Sekiguchi, T.,
Ishizaki, H., Takamori, A., DeSalvo, R., Majorana, E., van den
Brand, J., Hennes, E., Bertolini, A.: 2012, Seismic Attenuation
System (SAS) in the Kamioka mine, 13th Marcel Grossmann
Meeting, (Stockholm, Sweden, Jul. 1-7, 2012).
Takahashi, R.: 2012, Feed-forward vibration isolation andreduction of Newtonian noise, 2nd Korea-Japan Workshop on
KAGRA, (Kashiwa, Japan, May 28-29, 2012).
Takahashi, R.: 2012, Control strategy in the vibration isolation
system for KAGRA, 3rd Korea-Japan Workshop on KAGRA,(Souel, Korea, Dec. 21-22, 2012).
Takahashi, R.: 2013, Modal analysis of gravitational wave signals,
Symposium on gravitational wave astronomy, (Osaka, Japan,
Mar. 1-2, 2013).
Takahashi, S., Deguchi, S., Kuno, N., Iino, T., Hamura, T.,
Pogrebenko, S. V., Gurvits, L. I., Yoshida, F.: 2012, A Search
Water Masers in Icy Bodies of the Solar System, New Trends inRadio Astronomy in the ALMA Era -The 30th Anniversary ofNobeyama Radio Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Takano, S., Aikawa, Y., Chen, V., Hirano, N., Hirota, T., Kamegai,
K., Kobayashi, K., Kohno, K., Kuan, Y.-J., Liu, S.-Y., Nakajima,T., Ohashi, N., Ohishi, M., Ozeki, H., Sakai, N., Sakai, T.,
Shiba, S., Su, Y.-N., Sugimura, M., Takakuwa, S., Umemoto,T., Wang, K.-S., Watanabe, Y., Yamada, M., Yamaguchi, T.,
Yamamoto, S., Zhang, Q.-Z.: 2012, Nobeyama 45 m telescope
legacy project: Line survey, New Trends in Radio Astronomy
in the ALMA Era -The 30th Anniversary of Nobeyama Radio
Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Takano, S.: 2012, ALMA cycle 0 observations of NGC 1068 andNGC 253, ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22,
2012).
Takato, N., Iwata, I.: 2012, Instrumentation at the Subaru Telescope,
SPIE Astronomical Telescope and Instrumentation, (Amsterdam,
Netherlands, Jul. 1-6, 2012).
Takato, N.: 2012, Deployment of Astronomical Instruments at
Dome Fuji, XXXII Scientific Committee on Antarctic Research(SCAR), (Portland, OR, USA, Jul. 16-19, 2012).
Takekoshi, T., Minamidani, T., Nakatsubo, S., Oshima, T.,
Kawamura, M., Matsuo, H., Sato, T., Halverson, N. W., Lee, A.
T., Holzapfel, W. L., Tamura, Y., Hirota, A., Izumi, T., Suzuki,
K., Sorai, K., Kohno K., Kawabe, R.: 2012, Optics design ofthe multi-color TES bolometer camera for the ASTE telescope,
23rd International Symposium on Space Terahertz Technology(ISSTT2012), (Tokyo, Japan, Apr. 2-4, 2012).
Takiwaki, T.: 2012, Computing dynamics of supernovae with the
K computer, SC12, (Salt Lake City, UT, USA, Nov. 14, 2012).
Tamura, M., Suto, H., Nishikawa, J., Kotani, T., Sato, B., Aoki, W.,
Usuda, T., Kurokawa, T., Kashiwagi, K., Nishiyama, S., Ikeda,
Y., Hall, D., Hodapp, K., Hashimoto, J., Morino, J., Inoue,
S., Mizuno, Y., Washizaki, Y., Tanaka, Y., Suzuki, S., Kwon,
J., Suenaga, T., Oh, D., Narita, N., Kokubo, E., Hayano, Y.,
Izumiura, H., Kambe, E., Kudo, T., Kusakabe, N., Ikoma, M.,
Hori, Y., Omiya, M., Genda, H., Fukui, A., Fujii, Y., Guyon, O.,
Harakawa, H., Hayashi, M., Hidai, M., Hirano, T., Kuzuhara,M., Machida, M., Matsuo, T., Nagata, T., Ohnuki, H., Ogihara, M.,
Oshino, S., Suzuki, R., Takami, H., Takato, N., Takahashi, Y.,
Tachinami, C., Terada, H.: 2012, Infrared Doppler instrument for
the Subaru Telescope (IRD), SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Tamura, M.: 2012, SEEDS (Strategic Explorations of Exoplanets
and Disks with Subaru), New Trends in Radio Astronomy in
the ALMA Era -The 30th Anniversary of Nobeyama Radio
Observatory-, (Hakone, Japan, Dec. 3-8, 2012).
Tamura, M.: 2012, Strategic Explorations of Exoplanets and Disks
with Subaru (SEEDS), APCTP Workshop on Astrophysics:
Magnetic Fields in Astrophysics, (Pohang, Korea, Nov. 19-22,
2012).
Tamura, M.: 2012, SEEDS (Strategic Explorations of Exoplanets
and Disks with Subaru), Subaru-KASI workshop, (Seoul,
Korea, Nov. 15, 2012).
Tamura, M.: 2012, SEEDS: status report, SEEDS workshop, (Hakone,
Japan, Oct. 12, 2012).
Tamura, M.: 2012, Direct Imaging of Exoplanets and Their
Forming Disks with the Subaru Telescope, AOGS Distinguished
Lectures, (Sentosa, Singapore, Aug. 14, 2012).
Tamura, M.: 2012, Near-IR High-Contrast imaging polarimetryof protoplanetary disks - SEEDS Disk Results, AOGS-2012 PS,(Sentosa, Singapore, Aug. 14, 2012).
Tamura, M.: 2012, Direct imaging polarimetry of dust scattering in
protoplanetary disks, Cosmic Dust, (Kobe, Japan, Aug. 9, 2012).
Tamura, N., Takato, N., Iwamuro, F., Akiyama, M., Kimura, M.,
Tait, P., Dalton, G. B., Murray, G. J., Smedley, S., Maihara,
T., Ohta, K., Moritani, Y., Yabe, K., Sumiyoshi, M., Totani, T.,
Sugai, H., Karoji, H., Wang, S.-Y., Ohyama, Y.: 2012, Subaru
FMOS now and future, SPIE Astronomical Telescope andInstrumentation, (Amsterdam, Netherlands, Jul. 1-6, 2012).
Tamura, Y.: 2012, Geophysical Observations at Mizusawa, The
3rd KVN & VERA Joint Science WG Meeting, (Mizusawa,
Japan, Jul. 25-26, 2012).
Tanaka, M.: 2012, 3D Geometry of Supernovae: SpectropolarimetricObservations, Core-Collapse Supernovae: Models and Observable
Signals, (Seattle, WA, USA, Jul. 16-20, 2012).
Tanaka, M.: 2012, Spectropolarimetric Observations of Supernovae,
Tsinghua Transient Workshop, (Beijing, China, Nov. 5-9, 2012).
Tanaka, M.: 2012, High-Cadence Supernova Survey, Workshop on
Supernovae, Dark Energy, and Cosmology, (Chiba, Japan, Nov.
20-21, 2012).
Tanaka, M.: 2012, KISS: Kiso Supernova Survey, Kavli IPMU
Focus Week for Supernovae Near and Far, (Chiba, Japan, Dec
12-14, 2012).
Tanaka, T., Awazu, Y., Nakamura, F., Sugitani, K., Shimajiri,Y., Kawabe, R., Onishi, T., Yoshida, H.: 2012, The Dynamical
State of a Filamentary Infrared Dark Cloud, Serpens South,
New Trend in Radio Astronomy in the ALMA era, (Hakone,
Japan, Dec. 3-8, 2012).
Tanikawa, K., Sôma, M.: 2012, A list of historical comets observedat plural sites, IAU General Assembly JD5: From meteors andmeteorites to their parent bodies: Current status and future
developments, (Beijing, China, Aug. 20-31, 2012).
Tatematsu, K.: 2012, ALMA Cycle 0, cycle 1 report and cycle 2

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capabilities, ALMA Users Meeting, (Mitaka, Japan, Nov. 20-22,
2012).
Tatematsu, K.: 2012, ASTE status report, ALMA Users Meeting,(Mitaka, Japan, Nov. 20-22, 2012).
Tatematsu, K.: 2012, Prospect for Astrochemical Studies ofGalactic GMC Cores, ALMA Workshop Science with Mopra
for the ALMA, (Mitaka, Japan, Jun. 8-9, 2012).
Tatematsu, K.: 2012, Science Operation and Cycle 0/1 Status, East
Asian ALMA Science Workshop in Korea, (Daejeon Korea,
Sep. 12-13, 2012).
Terai, T., Itoh, Y.: 2012, Collisional Evolution of Main-Belt
Asteroids with High Inclination, Asteroids, Comets, Meteors
2012, (Niigata, Japan, May 16-20, 2012).
Toda, M., Yamamoto, M.-Y., Maeda, K., Shigeno, Y., Higa, Y.,
Watanabe, J.: 2012, Observation of Meteor Trains by HighSensitivity Digital Still Cameras, Asteroids, Comets, Meteors
2012, (Niigata, Japan, May 16-20, 2012).
Tokuda, K., Kuzu, M., Kimura, K., Muraoka, K., Maezawa, H.,
Onishi, T., Ogawa, H., Nakamura, F., Kuno, N., Takano, S.,
Iono, D., Kawabe, R., Kameno, S.: 2012, New 45 GHz Band
Receiver with Dual Polarization for NRO 45-m Telescope, New
Trend in Radio Astronomy in the ALMA era, (Hakone, Japan,
Dec. 3-8, 2012).
Tokuda, K., Kuzu, M., Kimura, K., Muraoka, K., Maezawa, H.,
Onishi, T., Ogawa, H., Nakamura, F., Kuno, N., Takano, S.,
Iono, D., Kawabe, R., Kameno, S.: 2013, Development of A
45 GHz Band Receiver with Dual Polarization for NRO 45-m
Telescope, International Winter School on the Interstellar Mediumand High-Energy Phenomena2013, (Ise, Japan, Mar. 3, 2013).
Tomida, K., Tomisaka, K., Matsumoto, T., Hori, Y., Okuzumi, S.,
Machida, M. N., Saigo, K.: 2012, Radiation Magnetohydrodynamic
Simulations of Protostellar Core Formation, The Labyrinthof Star Formation: A Conference Dedicated to Prof. Anthony
Whitworth, (Crete, Greece, Jun. 18-22, 2012).
Tomisaka, K., Kataoka, A., Machida, M. N., Tomida, K.: 2012,
Expected Observations of the Star Formation Process: from
Molecular Cloud Core to First Hydrostatic Core, EPoS 2012
The Early Phase of Star Formation - Assembling Pieces of theMissing Paradigm, (Ringberg, Germany, Jul. 1-6, 2012).
Tomisaka, K., Kataoka, A., Machida, M. N., Tomida, K.: 2012,
Expected Observations of the Star Formation Process: from
Molecular Cloud Core to First Hydrostatic Core, The Labyrinthof Star Formation: A Conference Dedicated to Prof. Anthony
Whitworth, (Crete, Greece, Jun. 18-22, 2012).
Tomisaka, K.: 2012, Expected Observations of Star Formation
Process: from Molecular Cloud Core to Protostar Phase, New
Trend in Radio Astronomy in the ALMA era, (Hakone, Japan,
Dec. 3-8, 2012).
Toshikawa, J., Kashikawa, N., Ota, K.: 2012, Discovery of a
protocluster at z ~ 6, First Stars IV - From Hayashi to the Future,(Kyoto, Japan, May 21-25, 2012).
Toujima, H., Handa, T., Omodaka, T., Nagayama, T., Kobayashi,
H., Koyama, Y.: 2013, Propagation of Highly Efficient Star
Formation in the North American Nebula (NGC 7000), IAU
Symp. 292: Molecular Gas, Dust, and Star Formation in
Galaxies, (Beijing, China, Aug. 20-24, 2012).

110

II Publications, Presentations

Tsujimoto, T., Bekki, K.: 2012, Globular Cluster Formation fromthe Ejecta of Type Ia Supernovae in the LMC, The Magellanic
System: In Perspective, (Perth, WA, Austraria, Sep. 10-13, 2012).
Tsujimoto, T., Bekki, K.: 2012, Globular Cluster Formation fromthe Ejecta of Type Ia Supernovae in the LMC, IAU Special
Session 1: Origin and Complexity of Massive Star Clusters,(Beijing, China, Aug. 20-24, 2012).
Tsujimoto, T.: 2012, Chemical Evolution of the Galactic
Bulge Formed through Two Stellar Disks, IAP-Subaru Joint
International Conference: Stellar Populations across Cosmic
Times, (Paris, France, Jun. 25-29, 2012).
Tsuneta, S.: 2012, Solar-C Mission, The Solar-C science meeting,(U. St. Andrews, UK, Aug. 11, 2012).
Ueda, J., Iono, D., Kawabe, R.: 2012, Reformtiion of Cold
Molecular Disks in Merger Remnants, East Asian ALMA Science
Workshop in Korea, (Daejeon Korea, Sep. 12-13, 2012).
Ueno, S., Shibata, K., Morita, S., Kimura, G., Asai, A., Kitai,
R., Ichimoto, K., Nagata, S., Ishii, T., Nakatani, Y.: 2012,
International collaboration and academic exchange of the
CHAIN project in this three years (ISWI period), United
Nations/Ecuador Workshop on the International Space Weather
Initiative, (Quito, Ecador, Oct. 8-12, 2012).
Umemoto, T.: 2012, A Radio Flare at Millimeter-wavelengths fromthe Young Stellar Object V773 Tau, East Asia VLBI Workshop
2012, (Taipei, Taiwan, May 30-Jun. 2, 2012).
Umemoto, T.: 2012, Radio Flares from the Young Stellar Objects,
The 3rd KVN & VERA Joint Science WG Meeting, (Mizusawa,
Japan, Jul. 25-26, 2012).
Usuda, T.: 2012, Science with TMT, TMT Science and Instrumentation
Workshop, (Pune, India, Dec. 10-12, 2012).
Uzawa, Y., Kroug, M., Fujii, Y., Kaneko, K., Kojima, T.,
Gonzalez, A., Kuroiwa, K., Miyachi, A., Makise, K., Wang,
Z., Shan, W.-L.: 2012, Development of receives for the ALMA
project, ISS2012, (Tokyo, Japan, Dec. 3-5, 2012).
Uzawa, Y., Qiu, W., Makise, K., Terai, H., Kroug, M., Wang,Z.: 2012, Characterization of the superconducting gap in theelectrodes of epitaxial NbN/AlN/NbN tunnel junctions, Applied
Superconductivity Conf., (Portland, OR, USA, Oct. 7-12, 2012).
Wada, T., Fujisawa, K.: 2012, Particle simulation for Rotating
White Dwarf magnetosphere, 13th Marcel Grossmann Meeting,(Stockholm, Sweden, Jul. 1-7, 2012).
Wada, T.: 2012, Particle Simulation for Axisymmetric Pulsar
Magnetosphere, XXVIIIth IAU General Assembly, (Beijing,
China, Aug. 20-31, 2012).
Wanajo, S.: 2012, Origin of r-process elements, 1st NAOJ Visiting
Fellow Workshop Program on Element Genesis and Cosmic
Chemical Evolution: r-process perspective, (Wako, Saitama,
Japan, Oct. 17-19, 2012).
Wanajo, S.: 2012, r-process from type-II supernovae, VIII Tours
symposium on nuclear physics and astrophysics, (LenzkirchSaig, Germany, Sep. 2-7, 2012).
Wanajo, S.: 2012, r-process: supernovae vs. neutron star mergers,
Quarks to Universe in Computational Science, (Nara, Japan,
Dec. 13-16, 2012).
Wanajo, S.: 2012, Role of neutrinos in SN nucleosynthesis, 6th
meeting of OMEG Institute, (Saitama, Japan, Apr. 25, 2012).

Wang, S.-Y., Hu, Y.-S., Yan, C.-H., Chang, Y.-C., Tamura, N.,
Takato, N., Shimono, A., Karr, J., Ohyama, Y., Chen, H.-Y., Ling,
H.-H., Karoji, H., Sugai, H., Ueda, A.: 2012, The metrology
cameras for Subaru PFS and FMOS, SPIE Astronomical
Telescope and Instrumentation, (Amsterdam, Netherlands, Jul.
1-6, 2012).
Wang, Z., Terai, H., Makise, K., Qiu, W., Uzawa, Y.: 2012,
Interface and tunneling properties of epitaxially grown NbN/
AlN/NbN tunnel junctions, Applied Superconductivity Conf.,(Portland, OR, USA, Oct. 7-12, 2012).
Washizaki, Y., Kashiwagi, K., Nishikawa, J., Kotani, T., Suto, H.,
Tamura, M., Kurokawa, T.: 2012, Highly Precise Calibrationof Spectrographs using Optical Frequency Shifer and Laser
Comb Generator, Frontiers in Optics 2012, (Rochester, NY, Oct.
18, 2012).
Watanabe, J., Tabe, I., Sugita, S., Yanagisawa, M., Terai, T., Ito,T.: 2012, Jovian Impact Flashes and its Implication to the Small
Bodies, Asteroids, Comets, Meteors 2012, (Niigata, Japan, May
16-20, 2012).
Watanabe, M.: 2012, ALMA computing report, ALMA Users
Meeting, (Mitaka, Japan, Nov. 20-22, 2012).
Watanabe, T.: 2012, FeXVII Emission Line Intensity Ratios Seen in
EIS and LHD - still the present continuous tense -, Spectroscopyof the Dynamic Sun, (London, UK, Apr. 18-20, 2012).
Watanabe, T.: 2012, Branching Ratio of FeXVII Emission Lines
Tested by Solar and Laboratory Plasmas, The 6th Hinode
Science Meeting, (U. St. Andrews, UK, Aug. 12-15, 2012).
Yamada, R., Matsumoto, K., Kikuchi, F., Noda, H., Kobayashi,N., Sasaki, S.: 2012, Investigation of lunar interior structure by
SELENE-2 geodetic and seismicobservations, Seminar on Lunarand Planetary Geodesy, (Mitaka, Japan, Jun. 19-20, 2012).
Yamada, Y., Fujita, S., Gouda, N., Kobayashi, Y., Hara, T., Nishi,R., Yoshioka, S., Hozumi, S.: 2012, Scientific goals of NanoJASMINE, IAU Symp. 289: Advancing the Physics of Cosmic
Distances, (Beijing, China, Aug. 27-31, 2012).
Yamagishi, A., Yoshimura, Y., Honda, H., Miyakawa, A., Naganuma,
A., Ohno, T., Ishimaru, R., Sasaki, S., Kubota, T., Satoh, T.,
Miyamoto, H.: 2012, MELOS life search proposal: search formicrobes on the mars surface with special interest in methaneoxdizing bacteria, Japan Geoscience Union Meeting 2012, (Chiba,
Japan, May 20-24, 2012).
Yamauchi, C.: 2012, 2MASS Catalog Server Kit version 2.1,
Astronomical Data Analysis Software and Systems (ADASS)
Conference XXII, (Champaign, IL, USA, Nov. 4-8, 2012).
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Niwa, Y.,
Yamada, Y.: 2012, The scientific goal of the Japanese small
astrometric satellite, Small-JASMINE, IAU Symp. 289:
Advancing the Physics of Cosmic Distances, (Beijing, China,
Aug. 27-31, 2012).
Yano, T., Gouda, N., Ueda, H.: 2012, Estimation for Dynamical
Structure of our Galaxy by the Future Astrometric Data, Gaia
and JASMINE, IAU General Assembly 2012 Special Session
3: Galaxy evolution through secular processes, (Beijing, China,
Aug. 20-24, 2012).
Yoshida, F.: 2012, Size distribution of asteroids, Asteroids,
Comets, Meteors 2012, (Niigata, Japan, May 16-20, 2012).

Yoshida, F.: 2012, Physical properties of Jovian Trojans and JAXA’s plan for a Jupiter Trojan mission, International (CJMT 2012)
Asteroid Science Workshop, (Macau, China, Oct. 18, 2012).
Zenitani, S., Hesse, M., Klimas, A., Black, C., Kuznetsova, M.:
2012, Identification of the dissipation region in collisionlessmagnetic reconnection: Theory and Simulations, AGU Fall
Meeing 2012, (San Francisco, CA, USA, Dec. 3-7, 2012).
Zenitani, S., Hesse, M., Klimas, A., Kuznetsova, M., Black, C.,
Nagai, T., Shinohara, I.: 2012, A new measure of the dissipation
region in collisionless magnetic reconnection, Computational
Methods in High Energy Density Plasmas - Workshop II:
Computational Challenges in Magnetized Plasma, (Los Angels,
CA, USA, Apr. 16-20, 2012).
Zenitani, S., Hesse, M., Klimas, A., Kuznetsova, M., Black, C.,
Shinohara, I., Nagai, T., Takahashi, H., Takamoto, M., Bessho,
N.: 2012, A new measure of the dissipation region in collisionlessmagnetic reconnection: Theory, simulation, and observation,2012 US-Japan Workshop on Magnetic Reconnection (MR2012),(Princeton, NJ, USA, May 23-25, 2012).
Zenitani, S., Miyoshi, T., Hesse, M., Klimas, M.: 2012, Magnetohydrodynamic structure of a plasmoid in fast reconnection
in low-beta plasmas, 2012 US-Japan Workshop on Magnetic
Reconnection (MR2012), (Princeton, NJ, USA, May 23-25, 2012).
Zenitani, S., Shinohara, I., Nagai, T.: 2012, Geotail observation of
the dissipation region in magnetotail reconnection, AGU Fall
Meeing 2012, (San Francisco, CA, USA, Dec. 3-7, 2012).
Zenitani, S., Shinohara, I., Nagai, T.: 2012, Geotail observation of
the dissipation region in collisionless magnetic reconnection,
AOGS - AGU (WPGM) Joint Assembly, (Singapore, Aug.
13-17, 2012).
Zenitani, S., Shinohara, I., Nagai, T.: 2012, Evidence for thedissipation region in magnetotail reconnection, International
Cambridge Workshop on Magnetic Reconnection 2012,(Copenhagen, Denmark, Aug. 27-30, 2012).
Zenitani, S.: 2012, Magnetohydrodynamic structure of a plasmoid
in fast reconnection in low-beta plasmas, GEOTAIL 20th
Anniversary Workshop, (Tokyo, Japan, Nov. 12-14, 2012).
Zenitani, S.: 2012, The structure of the dissipation region incollisionless magnetic reconnection: Theory, simulation, andobservation, GEOTAIL 20th Anniversary Workshop, (Tokyo,
Japan, Nov. 12-14, 2012).
Zenitani, S.: 2013, GEOTAIL observation of the dissipation
region and Particle dynamics in ion current layer, MMS Science
Working Team Meeting, (Boulder, CO, USA, Mar. 20-21, 2013).

II Publications, Presentations

111