Annual Report of the
National Astronomical Observatory of Japan

Fiscal 2007

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Shoken MIYAMA
Director General
National Astronomical Observatory of Japan

Preface

I Scientific Highlights April 2007 – March 2008

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II Publications, Presentations
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Refereed Publications

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Publications of the National Astronomical Observatory of Japan

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Report of the National Astronomical Observatory of Japan

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Conference Proceedings

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Publications in English

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Conference Presentations

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Annual Report of the
National Astronomical Observatory of Japan
Fiscal 2007

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Shoken MIYAMA
Director General of NAOJ

I am pleased to present the Annual Report of the
National Astronomical Observatory of Japan (NAOJ)
for fiscal 2007. In the preface, I would like to focus on
the activities and achievements related to one of the
key topics of today’s astronomy as the status of NAOJ
activities are provided in each section of this report.
Using numerous telescopes, NAOJ has been observing
astronomical phenomena in the universe including stars,
planet systems, galaxies, clusters of galaxies, and cosmic
large-scale structure (the entire structure of the universe).
Recent studies have revealed that these astronomicalmaterials which are visible with telescopes (starts andgalaxies) account for only 4% of the total mass in theuniverse, indicating that most of the universe mass ismade up of invisible materials named “dark matter” and“dark energy”, 20% and 75% respectively. The presenceof these invisible materials became known because of thegravitational effects they have on visible objects.
The dark matter was suggested as a gravitationalsource (not a gravity of a regular material like fixed stars)
by a phenomenon called flat rotation where the orbital
velocity of stars is maintained evenly regardless of the
distance between the stars and the center of our galaxy.
In addition, nothing seems more persuasive than the dark
matter when it comes to explaining why high temperature
gas in galaxy clusters can remain bound to the cluster andwhy lights are inflected more greatly than by the gravityof the galaxy (gravitational lens effect).
It gradually became known that the dark energy must
exist, as universal repulsion, three times the mass of thegravitational sources in the universe. This is derived
from the fact that the expansion velocity of the universe
is increasing at an accelerated pace, while gravitationalsources are present in the universe (materials and dark

matter).
The dark matter and dark energy have not yet been
identified exactly but posed an enormous challenge tobasic science (elementary particles theory and highenergy physics) with the findings obtained in the fields ofastrophysics and astronomy (observational and theoreticalastronomy). A fundamental concept of astrophysics has
been, so far, to grasp a reasonable picture of the universe
based on basic science. However, it may be changed by
new emerging forces like the dark energy which can be a
trigger requiring a new approach to the science of the 21st
century.
In the new phase of cosmology, NAOJ’s observational
instruments are playing a significant role, including
VERA (VLBI Exploration of Radio Astrometry) of
Mizusawa VERA Observatory which has succeeded indetermining the distance of the farthest star ever observedin our galaxy by the triangulation. This achievement
allowed NAOJ to investigate in detail stars moving at aconstantly high velocity in our galaxy. NAOJ will observe
the distance and orbital velocity of more stars, trying todetermine the distribution of the dark matter.
The 8-m Subaru Telescope remarkably contributes
to development of observational cosmology, with its
spectrograph and wide-field imager that is the only camera
mounted among similar-sized telescopes to Subaru. To
investigate the dark energy and dark matter more closely,
we started a project to fabricate Hyper Suprime-Cam, acamera with an even wider view filed than the current
imager. This project, in collaboration with Princeton
University of the United States and Academia Sinica
Institute of Astronomy and Astrophysics of Taiwan, is socomprehensive that it requires the upgrade of the Subaru
Telescope itself as well. This camera is expected todramatically accelerate the advancement of observationalcosmology. In addition to the implementation of the
project, we successfully completed a new adaptive optics
with near-diffraction-limit resolution for images obtainedby ground-based telescopes as well as a laser-guidestar system which artificially creates reference objects
for the adaptive optics. The both satisfied the projected
performance.
Computation simulation, which is of significancefor the studies of cosmology, revealed what type ofdark matter is necessary to form the cosmic largescale structure. To analyze observational data, softwareand hardware for data analysis need to be regularly
maintained and upgraded. Thanks to the support frommany people concerned, the computer system andinstruments of NAOJ have been fully replaced, which areused for shared use, advance theoretical study, analyze
and establish database.
Atacama Large Millimeter/submillimeter Array(ALMA), an international project with Europe andNorth America, is expected to benefit the advancementof the astronomical studies. ALMA is an arrayconsisted of eighty antennas (7-m and 12-m antennas)
including sixteen Japanese antennas and has been underconstruction in Chile. NAOJ has delivered four 12-m
antennas to the site in Chile ahead of the other two
partners and took images of the moon in radio spectrumwith one of the antennas. The Japanese correlator was
installed at the site and will combine signals transmitted
from the Japanese sixteen antennas. The development andfabrication of the receivers for the antennas are steadily
going on.
On top of the subjects mentioned above, there are
more challenging subjects of today’s astronomy: thediscovery of extrasolar planets; the exploration of
extraterrestrial life; the advancement of solar science; theexplanation of undefined celestial materials like black
hole; the ascertainment of the structure of galaxies; andthe unravelment of the forming process of galaxies, stars
and planets. To explore these unanswered mysteries, thefollowing activities have been continuously conducted:
the development of the Subaru Telescope and its new
device; Hinode, the observational satellite to study
the sun; Kaguya, the moon exploration satellite which
provides the new information on the moon; VSOP-2(VLBI Space Observatory Programme-2) whose operation

has actually started; Nobeyama Millimeter Array; andOkayama Astrophysical Observatory.
MIRA Project which was ranked as “A project”(projects in the early developmental stage) ended at
the end of fiscal 2007 as the external review committee
decided the continuous study by MIRA in Mitaka was not
feasible. The other “A project,” 4-Dementional Digital
Universe (4D2U) Project also ended in fiscal 2007, while
the development of its contents and public outreachactivities will be continued, by Center for Computational
Astrophysics and by Public Relations Center respectively.
Our public outreach activities have intensely beenpromoted to provide the public with the information on
the astronomical achievements. The official website of
NAOJ has been successful with 50 million hit counts ayear. Astronomy-related questions asked of NAOJ wereanswered in a more effective way, and the special open
day events at the observatories attracted more visitors
than previous years.
Following the adoption of adjusting cost for thepromotion of science and technology from Ministry of
Education, Culture, Sports, Science and Technology,
Scientific Culture Formation Unit was established incollaboration with Mitaka City in fiscal 2007. The
Unit provides educational programs for those whohave been recruited and will promote scientific culture
taking advantage of NAOJ’s scientific resources andachievements. Scientific Culture Formation Unit has
started to support the students who try to establish new
business on their own.
In terms of education, great efforts have been
made to provide excellent graduate education, nurture
young researchers, and improve academic research
environments. In such environments of NAOJ, 50 andmore graduate students and researchers engaged inresearch activities. We will continuously make further
efforts to educate and support young researchers.

Shoken MIYAMA
Director General of NAOJ

I Scientific Highlights(April 2007 – March 2008)

01 Detection of coronal Alfvén waves in a solar prominence with Hinode

OKAMOTO et al.

003

KATSUKAWA et al.

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TAKEDA et al.

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SHIMOJO et al.

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NAGASHIMA et al.

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06 Dynamic formation of the magnetic structure of a solar prominence

MAGARA008

07 Supernova Mixtures Reproducing Isotopic Ratios of Presolar Grains

YOSHIDA

009

YOSHIDA et al.

010

KASHIKAWA et al.

011

IYE et al.

012

02 Small-Scale Jetlike Features in Penumbral Chromospheres
03 Behavior of Lithium Abundances in Solar-Analog Stars
04

Fine Structures of Solar X-Ray Jets Observed with protect the X-Ray
Telescope aboard Hinode05 First Results from the Hinode/SOT Helioseismology Programme

08 ν-Process Nucleosynthesis in Population III Core-Collapse Supernovae
09

The Habitat Segregation between Lyman Break Galaxies and Lyman α
Emitters around a QSO at z ~ 5

10 First Measurement of Meteoroid Tunnel Size in Earth's Atmosphere
11

Active supermassive blackholes buried in ultraluminous infrared galaxies,
unveiled through Spitzer infrared spectroscopy

IMANISHI et al.

013

12

Nobeyama Millimeter Array HCN(1–0) and HCO+(1–0) observations ofluminous infrared galaxies

IMANISHI et al.

014

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Observations of Circumstellar Disks around Massive Protostars by the
Subaru Telescope

JIANG et al.

015

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Infrared Imaging Polarimetry of the NGC 2071 Star-Forming Region withSIRPOLTAMURA et al.

016

TAMURA et al.

017

KAMIO et al.

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KOTOKU et al.

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OKAMOTO et al.

020

YAGI et al.

021

ARAI et al.

022

SAITOH et al.

023

MURAKAMI et al.

024

23 Wide-Field Survey of the Local Group Dwarf Spheroidal Galaxy Leo II

KOMIYAMA et al.

025

24 Activities of parent comets and related meteor showers

WATANABE, SATO

026

15 UKIDSS searches of ultracool dwarfs: 1
16 Velocity of coronal jets measured by EIS/Hinode17

Magnetic Feature and Morphological Study of X-Ray Bright Points with
Hinode18 Emergence of a helical flux rope associated with prominence formation
19 Discovery of long, narrow, and straight HII gas in the Coma Cluster
20

Performance improvement of gravitational wave detector TAMA300 witha low frequency vibration isolation system

21 Project Milkyway
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Common-Path Spectropolarimetric Differential Imager Using Variable
Channeled Spectrum

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Three-dimensional simulations of molecular cloud fragmentation
regulated by magnetic fields and ambipolar diffusion

KUDOH

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Vertical Temperature Structures of the Solar Corona derived with the
Hinode X-Ray Telescope

KANO et al.

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Radial Velocity Variations of Procyon: Detection of Oscillations andLong-Term Variations

KAMBE et al.

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Physical and Chemical Properties of Massive Clumps in the AFGL 333
Cloud

SAKAI et al.

030

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Three Dimensional Line Transfer Study of Molecular Gas at the Centersof Active Galaxies

YAMADA et al.

031

30

Subaru Near-Infrared Multicolor Images of Class II Young Stellar Object,
RNO 91

MAYAMA et al.

032

31 Parallax measurement of star-forming region S 269 with VERA

HONMA et al.

033

32 Dense molecular gas arc in supergiant HII region NGC 604

TOSAKI et al.

034

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Near-Infrared Imaging Polarimetry of the Star Forming Region NGC
2024

KANDORI et al.

035

34

Water Maser and Ammonia Survey toward IRAS Sources in the Galaxy:
H2O Maser Data

SUNADA et al.

036

35

Characteristics of Anemone Active Regions Appearing in Coronal Holes
Observed with the Yohkoh Soft X-Ray Telescope

ASAI et al.

037

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Discovery of a Scattering Disk around the Low-Mass T Tauri Star FN
Tauri

KUDO et al.

038

37

Supernova Nucleosynthesis and Neutrino Oscillation with Improved
Reaction Rates

SUZUKI et al.

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ISHIKAWA et al.

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38 Transient horizontal magnetic fields in solar plage regions

002

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Direct and semi-direct neutron capture of neutron-rich Tin isotopes and its
implications for the r-process nucleosynthesis

CHIBA et al.

041

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Effects of primordial magnetic field and background gravitational wave
on low and high multipoles of the cosmic microwave background

YAMAZAKI et al.

042

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Simultaneous Solution to the Big-Bang Li Problems from a Long-lived
Negatively Charged Particle

KUSAKABE et al.

043

Detection of coronal Alfvén waves in a solar prominence with Hinode
OKAMOTO, Takenori J., TSUNETA, Saku, KATSUKAWA, Yukio, ICHIMOTO, Kiyoshi, SUEMATSU, Yoshinori(NAOJ)		

SHIMIZU, Toshifumi(ISAS / JAXA)NAGATA, Shin’ichi, SHIBATA, Kazunari(Kyoto University)

TARBELL, Theodore D., SHINE, Richard A., BERGER, Thomas E., TITLE, Alan M.

		(Lockheed Martin Solar and Astrophysics Laboratory)

It is well known that a bright structure is often seenin Hα line above the solar limb. It is called prominence(or filament if seen on the disk), which is cool plasma(~10,000 K) supported by coronal magnetic fields in thehotter corona (~1 MK). Detailed properties of prominence
have remained unclear.
The new Japan/US/UK solar physics satellite Hinodeenables the highest resolution imaging of prominences
as yet seen with a temporal uniformity that allows
long hours of diffraction-limited movies, a feat that is
impossible by ground-based observations. We investigate
fine structures of active region prominences with HinodeSolar Optical Telescope (SOT) observations.
To investigate fine structures and coronal magnetic
property of an active region prominence, we obtained over
1 hour of continuous SOT images of active region NOAA
AR 10921 on the west solar limb on 2006 November 9.
The prominence is located 10,000–20,000 km above
the visible limb (Fig. 1), and exhibits a very complex
fine structure with predominant horizontal thread-likefeatures. These threads have continuous horizontal flows
with a typical speed of about 40 km s−1, and also verticaloscillations in the plane of the sky with periods of several
minutes (Fig. 2). The oscillatory motion is most likely
due to propagating or standing Alfvén waves on thehorizontal magnetic field lines that form the prominence.
This represents the first direct detection of Alfvén waves
along coronal magnetic field lines [1].

		

LITES, Bruce W.
(HAO / NCAR)

because the wavelength of the Alfvén waves seems to
be much longer than that of the threads. From the fact,
we estimate the wavelength and speed to be more than
250,000 km and 1,050 km s−1, respectively. If we assume
that the plasma density is 1010 cm−3, the implied magnetic
field strength is ~50 Gauss for the propagating Alfvénwave, in agreement with measurements and models ofactive region prominence magnetic fields. The Poynting
flux of the observed Alfvén waves is sufficient to heatcoronal loops, so the Alfvén waves may play an importantrole in the coronal heating.

Figure 2: Example of a vertical oscillation of a single prominence
thread. A small field of view is extracted from the larger
field shown in Figure 1 and shown in negative contrast.
The dashed line in each panel indicates an approximately
constant height above the photosphere.

Figure 1: A prominence over the solar limb with the Hinode Solar
Optical Telescope (SOT). The prominence consistsof fine thread structures. We can also see a sunspot,
spicules, and so on.

Reference[1] Okamoto, T. J., et al.: 2007, Science, 318, 1577.

We cannot distinguish the time difference at theminimum and maximum amplitudes all along the thread

I Scientific Highlights003

Small-Scale Jetlike Features in Penumbral Chromospheres
KATSUKAWA, Yukio, ICHIMOTO, Kiyoshi, SUEMATSU, Yoshinori, TSUNETA, Saku
(NAOJ)BERGER, T. E., SHINE, R. A., TARBELL, T. D., TITLE, A. M.
(Lockheed Martin Solar and Astrophysics Laboratory)			

SHIMIZU, Toshifumi(JAXA / ISAS) 		

NAGATA, Shinichi(Kyoto University)

The Solar Optical Telescope (SOT) on HINODE,
which was successfully launched in September 2006,
has provided dynamic nature of the solar chromosphereby unprecedented high resolutional observations fromspace. It is discovered that small-scale jetlike activities
frequently happen in penumbral chromospheres (Fig. 1)[1]. The jet-like features newly discovered with SOT havelength of 1000–3000 km and width of 300–400 km. It isremarkable that their duration is mostly shorter than
1min. The spatial and temporal scales are much smaller
than chromospheric activities ever known, and existing
ground-based observations could not resolve them.
An apparent velocity of the jetlike activities is 50–100
km/s, but sometimes reaches over than 100 km/s. The
velocities are much faster than the acoustic velocity
in the chromosphere that is about 10 km/s. The jetlike
activities in penumbral chromospheres are referred to as“penumbral microjets” according to their small scales.
Penumbral microjets are a ubiquitous phenomenon
in the penumbral chromosphere. But there is a tendency
about the occurrence site of penumbral microjets.
The footpoints are always located between two dark
penumbral filaments. There are nearly horizontal
magnetic fields along the dark filaments, and relatively
vertical fields are there between the dark filaments. The
penumbral microjets are structures brightened along thevertical field lines. In addition, the penumbral microjets
are found to occur frequently near penumbral grains
moving inward with velocities of about 0.7 km/s.
There are complex magnetic configuration, called
uncombed magnetic structure, in a penumbra as
mentioned above. A penumbra consists of two magnetic
components, one is nearly horizontal flux tubes and theother is relatively vertical background fields. The twomagnetic field components are interlaced each other withspatial scale of about 1000 km. Strong discontinuities
and electric currents are naturally generated between thetwo different magnetic fields, and magnetic energies aresupposed to be sporadically released through magnetic
reconnection. The energy release most probably causes
brightening in the chromosphere, and is observed as apenumbral microjet. It is expected to have an outflow
with Alfvén velocity when magnetic reconnection
happens. The observed apparent velocity of penumbral
microjets is roughly consistent with the Alfvén velocity in

004

I Scientific Highlights

LITES, B. W.

(High Altitude Observatory)

the chromosphere, which strongly supports the possibilityof magnetic reconnection.
We can make rough estimation of an energy content
of each penumbral microjet by assuming its temperatureand density in the chromosphere. The estimated energy is
about 1023 erg per each microjet, which are comparable
to an energy of a microflare (or nanoflare) in coronae.
Because the penumbral microjets are a ubiquitous activity
in a sunspot penumbra, they might contribute to heatingof chromospheres and coronae.

Figure 1: Penumbral microjets in the sunspot chromospherediscovered with HINODE SOT. (A) A sunspot image
taken through the Ca II H filter of SOT, and (B) its
brightness difference from a previous frame 30 sec
before. Penumbral microjets are clearly identified in the
difference image.
Reference[1] Katsukawa, Y., et al.: 2007, Science, 318, 1594.

Behavior of Lithium Abundances in Solar-Analog Stars
TAKEDA, Yoichi, KAWANOMOTO, Satoshi, HONDA, Satoshi
ANDO, Hiroyasu, SAKURAI, Takashi(NAOJ)

speculate from this fact that the decrease in the stellar
angular mumentum caused by the existence/formation ofplanets may have lowered the surface Li abundance via
the enhanced mixing.

Teff (K)

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Since lithium atoms are destroyed when they areconveyed into the hot stellar interior (T > 2.4 × 106 K),
the surface Li abundance (ALi) can be used as a probe
for diagnosing the past history of envelope mixing.
For example, the fact that the current solar ALi value isconsiderably reduced (by a factor of ~100) as comparedto the solar system composition (primordial value) may
be interpreted as a result of long-proceeding gradualdepletion caused by mixing due to the deep convection
zone. Curiously, however, when we pay attention to othersolar type stars (early G-type main-sequence stars), we
see a remarkably large diversity of ALi amounting to morethan ~2 dex (among which the Sun’s ALi is definitelylow). Why such a large difference is produced for stars
with similar parameter values?
In order to contend with this problem, we carried out
a comprehensive statistical study on 118 selected solar
analogs based on the high-dispersion spectra obtainedwith the 188 cm reflector and the HIDES spectrograph at
Okayama Astrophysical Observatory. The atmosphericparameters were determined spectroscopically from Fe I
and Fe II lines, the mass and age were evaluated fromthe positions on the HR diagram with the help of stellar
evolutionary tracks, the macrobroadening velocity (vr+m)
was established by spectrum-fitting analyses in the 6080–
6089 Å region, and the Li abundance (ALi) was evaluatedfrom the Li I 6708 line feature. The resulting ALi vs. Teffand ALi vs. vr+m plots are depicted in Figures 1a and 1b,
respectively, from which we can draw the following
conclusions (see [1] for more details).
— (1) A close connection exists between the macrobroadening velocity (vr+m; a combination of the projectedrotational velocity v e sin i, and the macroturbulencevmacro) and the surface Li abundance, in the sense that ALi
progressively grows with an increase in vr+m (Fig. 1b).
Since the macroturbulence (essentially the granularmotion of stellar convection origin) is unlikely to varymuch among stars of similar parameters, we may regard
that the diversity of vr+m simply reflects the differencein ve sin i. Accordingly, we may state that “a loweringof stellar rotation leads to an enhanced envelope mixing(i.e., decrease in ALi)”. (This kind of mechanism wasonce proposed from the theoretical side; e.g., [2]).
— (2) The ALi values of five planet-host stars situate in
the lower envelope of the distribution (Fig. 1a), which
confirms the recent argument that the photospheric Li
abundances in planet-host stars tend to be lower thanthose in non-planet-host stars (e.g., [3, 4]). Considering
the ve sin i-dependence of ALi mentioned above, we may

2
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0

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4
6 -1 8vr+m (km s )10

Figure 1: (a) Relation between the surface lithium abundance (ALi)and the effective temperature (Teff). Filled circles (blue):reliable ALi values. Dianmonds (purple): unreliable ALi
values at the detection limit. Inverse triangles (green):
upper limit ALi values (for the case of invisible Li line).
The double circle (red) represents the solar value. The
five planet-host stars are indicated by their HIP numbers.
(b) Relation between the surface lithium abundance (ALi)and the macrobroadening velocity (vr+m).
References[1] Takeda, Y., et al.: 2007, A&A, 468, 663.
[2] Martín, E. L., Claret, A.: 1996, A&A, 306, 408.
[3] Israelian, G., et al.: 2004, A&A, 414, 601.
[4] Takeda, Y., Kawanomoto, S.: 2005, PASJ, 57, 45.

I Scientific Highlights005

Fine Structures of Solar X-Ray Jets Observed with
the X-Ray Telescope aboard Hinode
SHIMOJO, Masumi, KANO, Ryohei, TSUNETA, Saku, SHIBASAKI, Kiyoto(NAOJ)NARUKAGE, Noriyuki, SAKAO, Taro
(ISAS / JAXA)CIRTAIN, Jonathan W.
(NASA)

LUNDQUIST, Loraine, REEVES, Katherine, SAVCHEVA, Antonia(SAO)

The X-Ray Telescope (XRT) aboard Hinode hasrevealed the fine structure of solar X-ray jets [1]. One of
the fine structures observed by XRT is an expanding loop.
The loop appears near the footpoint of the jet when thefootpoint brightening is observed. Additionally, we havefound that the X-ray jets begin just after the expanding
loop ‘breaks’. Other fine structures discovered by XRT
are thread-like features along the axis of the jets. XRT
has shown that these thread structures compose the crosssection of jets. The fine structures and their motions
strongly support the X-ray jet model based on magnetic
reconnection, and also suggest that we must consider
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the threedimensional configuration of magnetic field tounderstand jet phenomenon.
We investigated also the reverse jet associated with
the Xray jet in the quiet sun, and propose that the reverse
jet is produced by heat conduction or a MHD wave subsequent to the main jet.
Reference[1] Shimojo, M., et al.: 2007, PASJ, 59, S745.

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Figure 1: A solar X-ray jet in quiet sun. Upper row: The X-ray intensity maps with the wide field of view (Negative images). Middle row: The
X-ray intensity maps around the foorpoint (Negative images). The triangle symbols indicate expanding loops. Lower row: Running
difference images are shown for the jet (Positive Images). The black circles indicate the thread-pattern movement for the jet.

006

I Scientific Highlights

First Results from the Hinode/SOT Helioseismology Programme
NAGASHIMA, Kaori, SEKII, Takashi(Graduate University for Advanced Studies / NAOJ)MITRA-KRAEV, Urmila(University of Sheffield)

Results from initial helioseismic observations by the
Solar Optical Telescope (SOT) on Hinode are reported.
SOT has been providing us with excellent stable highresolution images of the Sun in various wavelengths since
it was launched in September, 2006. As an attempt to
exploit this capability for helioseismology, we examined
intensity oscillation data in Ca II H line and the G bandfrom the Broadband Filter Imager (BFI).
The power spectra (k–ω diagrams) and the corresponding time-distance cross-correlation diagrams
were obtained for data from a 12-hour observation ofa quiet region [1]. In these basic diagnostic diagrams,
we saw components of much higher frequencies andwavenumbers than had been observed before, indicating
great potential for high-resolution helioseismic
observation by Hinode/SOT. In our initial time-distanceanalysis, we observed subsurface supergranular patterns
clearly (see Fig. 1), which were found to be coherent overthe depth range of a few Mm.
In [2] we reported a cross-spectral analysis of solar oscillations observed in intensity signals from two different
layers. We found that below the acoustic cutoff frequency
there is no phase shift in the cross phase spectrum along
the f-mode ridge, but along the p-mode ridges the phaseshift has strong peaks. If the absence of the phase shift isdue to the standing wave nature, the phase shift along thep-mode ridges must also be zero. Why the p modes andthe f modes behave differently is still a puzzle.
Oscillations within sunspots have been observed by
SOT [3, 4]. In local-helioseismological techniques, we
examine how acoustic waves propagate so that we canstudy subsurface structures. Furthermore, to reveal themechanism of how sunspots evolve and dissipate by
local helioseismology, we need to know how the acoustic
waves interact with magnetic fields in detail. Therefore,
sunspot oscillations are important scientific targets.
We investigated the spatial distribution of the power
spectral density of the oscillatory signal in and arounda sunspot [3]. In Ca II H intenstiy 5.5-mHz oscillationsin the umbra were prominent. These are due to so-called‘umbral flash’, patchy transient brightening seen in thechromosphere of the sunspot umbra. The Ca II H poweris enhanced throughout most of the umbra, but in theregion within about 3 arcsec from the center of the umbra
the power was suppressed (See Fig. 2). This kind of finestructure cannot easily be explained by the field-guided
upward-propagating shock-wave model for the umbral
flash proposed so far.

KOSOVICHEV, Alexander, ZHAO, Junwei(Stanford University)

TSUNETA, Saku, Hinode/SOT Team(NAOJ)We also reported observations of sunspot oscillations
excited by a solar flare [4]. Since these oscillations
appeared in the sunspot umbra and inner penumbra, theymight represent magnetohydrodynamic oscillatory modes
and may provide us with useful information about theflare mechanism.

Figure 1: An outward-inward travel time difference map from
12-hr Ca II H data over the surface distance of 14.86Mm,
indicating flow divergence due to supergranulation [1].

Figure 2: Intensity map (left) and power map (right) from the Ca II
H data of the active region NOAA 10935 [3].

References[1] Sekii, T., et al.: 2007, PASJ, 59, S637.
[2] Mitra-Kraev, U., Kosovichev, A. G., Sekii T.: 2008, A&A, 481,
L1.
[3] Nagashima, K., et al.: 2007, PASJ, 59, S631.
[4] Kosovichev, A. G., Sekii, T.: 2007, ApJ, 670, L147.

I Scientific Highlights

007

Dynamic formation of the magnetic structure of a solar prominence
MAGARA, Tetsuya(NAOJ)

Solar filaments, or prominences observed at the solarlimb, are one of the prominent objects showing floatedstructure on the Sun. The gas density in a filament issignificantly higher than its surroundings, and now
it is widely believed that the mass of a filament ismagnetically supported against gravity (Fig. 1; see [1],[2]). The magnetic field has a significant effect on the
dynamic and thermodynamic states of filaments via theLorentz force and thermal conduction along magnetic
field lines, so the structure of magnetic field in filaments
has been an important issue for the study of the nature offilaments [3].
a)

a)

b)

b)

c)
foot

Figure 1: a) A solar prominence, b) A two-dimensional, static
model of a prominence.

We reported a result that the emergence of subsurface
magnetic field naturally reproduces the feature of the
global magnetic configuration observed in solar filaments.
This is obtained by performing three-dimensional
simulation of a twisted flux tube that emerges in the
shape of multi-loop in a highly stratified solar atmosphere
extending from the subsurface layer to corona (Fig. 2.
from [4]). A key finding is that a kinking of the twisted
flux tube occurs at the site of a linkage between adjacent-loops. This develops a magnetic structure that has
remarkable similarities to the structure of a filament inthat the inner part of the twisted flux tube can be applied
to the main body of a filament while the outer part isreminiscent of observations of filament feet and a coronalarcade overlying the main body of a filament. Basedon the result we concluded that geometric features offilaments observed on the Sun may have the origin in
the handedness of twisted magnetic field below the solar
surface, i.e., a flux tube with a left- (right-) handed twist
produces a dextral (sinistral) filament. This research was
supported by a Grant-in-Aid (19740101, PI: T. Magara)from the Ministry of Education, Culture, Sports, Scienceand Technology.

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I Scientific Highlights

main bodyfootdextral filament
footmain bodyfootsinistral filament

Figure 2: a) Magnetic structure of a solar prominence obtained by
a 3D MHD simulation b) Distribution of photosphericmagnetic field and the field lines formed above thephotospheric field. c) Geometric features of dextral andsinistral filaments.
References[1] Kippenhahn, R., Schlüter, A.: 1957, Zeitschrift fur Astrophysik,
43, 36.
[2] Kuperus, M., Raadu, M. A.: 1974, A&A, 31, 189.
[3] Tandberg-Hanssen, E.: 1995, Astrophysics and Space Science
Library, 199.
[4] Magara, T.: 2007, PASJ, 59, L51.

Supernova Mixtures Reproducing Isotopic Ratios of Presolar Grains
YOSHIDA, Takashi(NAOJ)

Primitive meteorites contain very small (nm ~ μm
sized) grains indicating huge isotopic anomalies. These
isotopic anomalies are not explained by physical andchemical processing in the solar-system formation, andare considered to indicate evidence for nucleosynthesis
in stars and the Galactic chemical evolution. Therefore,
these grains are called as presolar grains (e.g., [1]).
Silicon carbide type X (SiC X) and low density
graphite are considered to originate from supernovae. The
excesses of 28Si and the original presence of short lived
nuclei 44Ti are strong evidence for their origin. However,their isotopic and elemental features are different fromthose of bulk composition of supernova ejecta. Therefore,
their features are considered to be evidence for large
heterogeneous mixing of supernova ejecta.
In this study, heterogeneous supernova mixtures
reproducing isotopic ratios of individual single grains
as many as possible are sought. The isotopic featuresand mixing ratios of the mixtures are also investigated.
From the obtained mixtures, the elemental compositions
and the formation condition of the presolar grains fromsupernovae are discussed [2].
The isotopic ratios 12 C/ 13 C, 14 N/ 15 N, 26 Al/ 27 Al,
29
Si/ 28Si, 30Si/ 28Si, 44Ti/ 48Ti of 18 SiC X and 26 low
density graphite (and 16O/17O and 16O/18O for low density
graphites) are adopted for comparison. The abundance
distributions of the supernova ejecta of 3.3, 4, 6, and 8 MHe star models corresponding to the advanced stagesof 13, 15, 20, and 25 M ZAMS stars [3] are used toinvestigate supernova mixtures. The supernova ejecta are
divided into seven layers; the Ni, Si/S, O/Si, O/Ne, C/O
or O/C, He/C, and He/N layers in accordance with theirmain compositions.
Figure 1 shows six isotopic ratios of SiC X KJGM2243-9 and three supernova mixtures. These mixtures
reproduce five isotopic ratios except 14N/ 15N. In thisstudy, the mixtures reproducing isotopic ratios of individual grains are classified into three groups. The above
mixtures are classified into group C. The ones reproducing except 12C/13C are classified into group N. The ones
reproducing both C and N isotopic ratios but except one
ratio are classified into group CN. In the case of low density graphites in which 44Ti/48Ti was not measured, themixtures reproducing six isotopic ratios in seven ratios
are found. They are also classified into the three groups.
The mixing ratios of the mixtures depend on reproduced isotopic ratios. In group C, the main component
is the He/N layer. The C/O, He/C, and Ni layers areadded with small fractions. In group N, the main component is the He/C layer. The C/O, He/N, and Ni layers

are additionally contained. In group CN, the innermost
Ni layer is the main component and the He/N layer is thesecond main component.
The elemental composition of the supernova mixtures
is important from the viewpoint of the grain formation.
Silicon carbide and low density graphite are formed incarbon-enriched material rather than oxygen. In thisstudy, most of the mixtures indicate the C/O ratio in therange of 1 ~ 2. On the other hand, the mixtures of group
CN for SiC X indicate very small C/O ratio (~ O(10−3)).
TiC subgrains in some graphite suggest that graphite
grains are formed in Fe-enriched environment rather than
Si. The mixtures obtained in this study have a correlation
between Fe/Si and Fe/C. The mixtures in group CN for
low density graphite show Fe/Si ~104, which is favorable
for the formation of TiC subgrains.

Figure 1: Isotopic ratios of SiC X grain KJGM2-243-9 and supernova mixtures. Circles indicate the isotopic ratios of
KJGM 2-243-9. Solid, dotted, and dash-dotted lines
correspond to the supernova mixtures for 3.3, 6, and 8 Mmodels.

References[1] Lodders, K., Amari, S.: 2005, Chem. Erde Geochem., 65, 93.
[2] Yoshida, T.: 2007, ApJ, 666, 1048.
[3] Yoshida, T., Umeda, H., Nomoto, K.: 2005, ApJ, 631, 1039.

I Scientific Highlights009

ν-Process Nucleosynthesis in Population III Core-Collapse Supernovae
YOSHIDA, Takashi(NAOJ)

UMEDA, Hideyuki, NOMOTO, Ken'ichi

Recent observations of metal-poor stars with −4 <[Fe/H] < −2 indicated that the average abundance ratios
to Fe [X/Fe] are in the range ±0.5 dex for most observed
elements [1] ([X/Y] ≡ log(NX/NY) − log(NX/NY) where
NX and NY are the abundances of elements X and Y). The
abundance ratios observed in extremely metal-poor (EMP)
stars and those in very metal-poor stars are in agreementwith the yields produced in Population III hypernovae
and both contributions from Population III supernovae
and hypernovae [1]. On the other hand, the supernova
and hypernova yields for N, K, Sc, Ti, Mn, and Co are
too small to explain the observed abundance ratios.
We investigate the contribution of the ν-process in the
nucleosynthesis of Population III supernovae and hypernovae. We focus on the production of odd-Z iron-peakelements. We investigate the dependence of the yields ofSc, Mn, and Co on the neutrino irradiation of the supernova ejecta. Then, we indicate whether the abundance
ratios of these elements observed in EMP stars are reproduced by supernovae and hypernovae with the effectsof the ν-process [2].
In the case without the ν-process, most of Sc and Mn
are produced during incomplete Si burning. Most of Co
is produced in complete Si burning region. On the other
hand, when the ν-process is considered, the Sc amountproduced in complete Si burning region increases. In theregions of complete and incomplete Si burning, 55Co as
well as neutrons and protons are produced from 56Ni,
which has been produced in NSE and QSE, throughthe ν-process. The produced 55Co decays to 55Mn. The
neutrons and protons are captured by 44Ti and 58Ni to
produce 45V, 59Cu, and 59Ni. They change to 45Sc and 59Co
through β+-decays and electron captures.
Figure 1 indicates the abundance ratios of Population
III 15 M  supernova and 25 M  hypernova with therelation of the total energy released by neutrinos Eν . The
abundance ratios of the 25 M supernova are similar to
those of the 15 M supernova. The abundance ratios ofSc, Mn, and Co in the supernovae increase owing to thecontribution from the ν-process. The abundance ratios
of Sc and Mn in the hypernova are also enhanced by the
ν-process but the Co abundance ratio is not.
Supernova models with the ν-process well reproduce
the Mn/Fe ratio observed in EMP stars. The neutrinoenergy released from the supernovae should be (3–9) ×
1053 erg to reproduce the Mn/Fe ratio of the EMP stars.
On the other hand, in order to reproduce the Sc/Fe and
Co/Fe ratios observed in the EMP stars, stronger neutrino
irradiation is necessary for the supernova and hypernova
models.

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I Scientific Highlights(University of Tokyo)

Figure 1: Abundance ratios [X/Fe] for Population III 15 M supernova (upper panel) and 25 M hypernova (lower
panel). Black, red, blue, and green lines correspondto the case without the ν-process, the cases with the
ν-process and Eν = 3 × 1053, 9 × 1053, 3 × 1054 ergs.
Circles indicate the abundance ratios of averaged over
22 EMP stars [3].

References[1] Tominaga, N., Umeda, H., Nomoto, K.: 2007, ApJ, 660, 516.
[2] Yoshida, T., Umeda, H., Nomoto, K.: 2008, ApJ, 672, 1043.
[3] Cayrel, R., et al.: 2004, A&A, 416, 1117.

The Habitat Segregation between Lyman Break Galaxies andLyman α Emitters around a QSO at z ~ 5
KASHIKAWA, Nobunari(NAOJ / Graduate University for Advanced Studies)

MISAWA, Toru
(RIKEN)KITAYAMA, Tetsu(Toho University)

KOMIYAMA, Yutaka

We carried out a target survey for Lyman breakgalaxies (LBGs) and Lyman α emitters (LAEs) aroundQSO SDSS J0211-0009 at z = 4.87. The deep and wide
broadband and narrowband imaging simultaneously
revealed the perspective structure of these two high-z
populations. The LBGs without Lyα emission form
a filamentary structure including the QSO, while theLAEs are distributed around the QSO but avoid it within
a distance of ~4.5 Mpc (Fig. 1). On the other hand,
we serendipitously discovered a protocluster with asignificant concentration of LBGs and LAEs where nostrongly UV ionizing source such as a QSO or radiogalaxy is known to exist (Fig. 2). In this cluster field, twopopulations are spatially crosscorrelated with each other.
The relative spatial distribution of LAEs to LBGs is instark contrast between the QSO and the cluster fields.
We also found a weak trend showing that the number
counts based on Lyα and UV continuum fluxes of LAEs
in the QSO field are slightly lower than in the cluster
field, whereas the number counts of LBGs are almost
consistent with each other. The LAEs avoid the nearby
region around the QSO where the local UV backgroundradiation could be ~100 times stronger than the averagefor the epoch. The clustering segregation between
LBGs and LAEs seen in the QSO field could be due toeither enhanced early galaxy formation in an overdense
environment having caused all the LAEs to evolve into
LBGs, or local photoionization due to the strong UVradiation from the QSO effectively causing a deficit in
low-mass galaxies like LAEs [1].

(NAOJ)

DOI, Mamoru(IoA, University of Tokyo)

OTA, Kazuaki(RIKEN)

Figure 1: The LBG (blue circle)/LAE (red triangle) distribution
and its surface number density contours (blue for LBGs
and red for LAEs) in the QSO field around SDSS
J0211-0009 (central orange square). The thin and thickcontours denote 1σ and 3σ excess from the mean local
density.

Reference[1] Kashikawa, N., et al.: 2007, ApJ, 663, 765.

Figure 2: Same as Figure 1 but for the cluster field.

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First Measurement of Meteoroid Tunnel Size in Earth’s Atmosphere
IYE, Masanori, KOMIYAMA, Yutaka, FURUSAWA, Hisanori(NAOJ)			TANAKA, Mikihito, ASAMI, Naoko

OHNISHI, Koji

(University of Tokyo)			

(Nagano National College of Technology)

YANAGISAWA, Masahisa

EBIZUKA, Noboru(University Electro-Communication)

Subaru Telescope, focused to infinity, records
defocused images of nearby meteors and artificial
satellites (Fig. 1). Meteors and artificial satellites can be
distinguished by their angular width of defocused images(Fig. 2). Imaging observations of Andromeda galaxy for
19 hours during August 12-15, 2004, recorded 57 tracks,of which 44 were artificial satellites and 13 were meteors.
Although the observing run was just after the peak of
Perseids meteor shower, most were sporadic meteors andonly one was confirmed to be Perseids. Among the 44
tracks of artificial satellites, 17 were identified to specificsatellites catalogued in the public data base.

(RIKEN)HIROSE, Chikako(JAXA)of the collision column from the following equation
S = N[OI] / (nOIL).

(1)

Analysis of four meteors observed through the V-band
filter covering the 558nm forbidden line photons yielded
the column diameter in the range 2–10 mm. This size
turned out to be about 10 times the size of a few–few
tens of μg meteoroids, that were estimated from theirluminosity. This paper eventually yielded scientific results
for the nearest object ever studied by Subaru Telescope[1].

Figure 2: Typical images of a meteor (left) and an artificial
satellite (right). Meteors at 110 km altitude are much
more defocused than satellites at 500–20,000 km
altitude. Arrows indicate 5 arcmin span. Images areshown in negative prints.

Figure 1: Calculated angular size of an object with diameter D [m]at a distance of d [km] as seen by Subaru Telescope.

The main scientific achievement of the present
paper was the first measurement of the size of shiningcolumn of meteors based on a physical assessment. The
width of meteor tracks were unresolved so far and thesize of the shining column was known to be smaller
than about 1m, corresponding to the size spanning 0.5
arcsecond at 110 km height. The current team used thefact that the forbidden line photons emitted at 558 nm
by neutral oxygen atoms are produced by collisional
excitation (Fig. 3). If one can evaluate the total numberof this forbidden line photons N [OI] emitted in a unit
time, it should be equal to the total number of collisional
excitation events that took place in the same time. As thenumber density of neutral oxygen atoms nOI at 110 km
altitude and the track length L traversed by the meteor ina unit time are known, one can derive the cross section S

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Figure 3: Neutral oxygen atoms directly hit by the meteoroid or byaccelerated nitrogen or oxygen atoms are collisionallyexcited. Excited atoms return to ordinary state byemitting a 558-nm forbidden line photon. By counting
the number of these special photons, one can calculate
the width of the collision tunnel bored by the meteoroid.
(Illustration by N. Ishikawa)
Reference[1] Iye, M., et al.: 2007, PASJ, 59, 841.

Active supermassive blackholes buried in ultraluminous
infrared galaxies, unveiled through Spitzer infrared spectroscopy
IMANISHI, Masatoshi(NAOJ)MALONEY, P. R.

(University of Colorado)

DUDLEY, C. C.

(George Mason University)

NAKAGAWA, Takao(ISAS / JAXA)

Ultraluminous infrared galaxies (ULIRGs) radiate
the bulk of their large luminosities (>1012L) as infraredemission. This means that (1) very luminous energy
sources are present hidden behind dust, (2) the bulk of
the energetic radiation from the hidden energy sources
is once absorbed by the surrounding dust, and (2) the
heated dust emits strong infrared radiation. The energy
source can be nuclear fusion inside rapidly formedstars (starburst) and/or active mass accretion onto acentral supermassive blackhole (AGN). Distinguishing
the hidden energy sources of ULIRGs is indispensable
not only to understand the true nature of the ULIRG
population, but also to unveil the history of star-formationand supermassive blackhole growth in the dust-obscured
side of the universe.
Identifying the hidden energy sources of ULIRGs
is difficult because highly-concentrated nuclear dust
can easily bury (= obscure in all directions) the putative
AGNs. Unlike an AGN surrounded by torus-shaped dust,
which is easily detectable through optical spectroscopy,
such buried AGNs are very difficult to find. However,detecting buried AGNs and estimating their energeticrole are the most important issue in the current ULIRG
study. For this purpose, observations at wavelengths oflow dust extinction are necessary, and infrared 5–35 μm
spectroscopy is an effective means. First, PAH (polycyclicaromatic hydrocarbon) emission features, found at 3–25
μm, are detected in starburst galaxies, but not in AGNs,
because of the destruction of PAHs. Hence, the presenceor absence of the PAH emission can be used to identify
the energy sources. Next, in a normal starburst, where
the stellar energy sources and dust are spatially well
mixed (Fig. 1, left), there is an upper limit for the opticaldepth of the 9.7 μm silicate dust absorption feature, while
it can be arbitrarily large in a buried AGN, where theenergy source is more centrally concentrated than thesurrounding dust (Fig. 1, right) [1].
Using the IRS spectrograph onboard the Spitzer
infrared satellite, we observed 48 ULIRGs with no
obvious AGN signatures in the optical, by combining
data taken through our Cycle-1 program and archival
data. We have obtained low resolution (R < 100) infrared
5–35 μm spectra of the complete sample of optically nonAGN ULIRGs at z < 0.15 (Fig. 2), and found signaturesof luminous buried AGNs in roughly half of the observed
ULIRGs [1]. Our results strengthen our previous
argument, based on Subaru infrared 3–4 μm spectroscopy

MAIOLINO, R.

(Rome Observatory)RISALITI, G.

(Arcetri Observatory)[2], that luminous buried AGNs are common in the
ULIRG population.

Figure 1: Geometry of energy sources and dust. (Left): Normal
starburst. Stellar energy sources (open stars) and dust are
spatially well mixed. (Right): Buried AGN. The energy
source (= a mass accreting supermassive blackhole;filled circle) is spatially very compact and is more
centrally concentrated than the surrounding dust.

Figure 2: Examples of Spitzer infrared 5–35 μm spectra of ULIRGs.
(Upper left): Starburst-dominated ULIRG. PAH emission
is strong. (Upper right): ULIRG dominated by a buried
AGN. No PAH emission and strong silicate dust
absorption are detected. (Lower): ULIRG with starburst
and buried AGN composite. PAH emission is seen, but
its strength is weak.

References[1] Imanishi, M., et al.: 2007, ApJS, 171, 72.
[2] Imanishi, M., et al.: 2006, ApJ, 637, 114.

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Nobeyama Millimeter Array HCN(1– 0) and HCO+(1– 0)
observations of luminous infrared galaxies
IMANISHI, Masatoshi, NAKANISHI, Kouichiro(NAOJ)				OI, Nagisa(GUAS)

Luminous infrared galaxies radiate very large luminosities (>1011 L) as infrared dust emission, suggestingthat powerful energy sources are present, surroundedby dust. The energy sources are star-formation (nuclear
fusion inside stars) and/or active galactic nuclei (AGNs;
active mass accretion onto a central supermassive
blackhole with mass >106 M). Unlike AGNs obscured
by torus-shaped dust, putative AGNs in LIRG's nuclei
are likely to be obscured by a large amount of nuclear
dust and gas in all directions (= buried), making theidentification of AGNs difficult.
An AGN has the following remarkable properties,
compared to star-formation. First, strong X-ray (E > 2 keV)emission is produced in the close vicinity of the accretion
disk around a central supermassive blackhole, throughthe inverse Compton process. Second, emission surface
brightness of an AGN is so high that the surrounding
dust can be heated to high temperature and the hot dust
can produce strong mid-infrared (5–20 μm) emission.
In the case of a buried AGN at a LIRG's nucleus, direct
detection of these AGN's properties is not easy, becauseof large extinction/absorption. However, we may be able
to detect buried AGN signatures, through the effects of
the AGN to the surrounding gas.
HCN(1–0) and HCO+(1–0) emission are proposed to
be a useful tool to probe such AGN effects. Observationally, AGN-dominated galaxy nuclei show high HCN(1–0)
to HCO+(1–0) ratios in brightness temperature (∝ flux ×λ2), while starburst galaxies display low ratios. We havesystematically investigated the HCN(1–0)/HCO+(1–0)
brightness-temperature ratios in a large number of LIRGs[1]. Our main results are that LIRGs with luminous buried
AGN signatures in our previously taken infrared spectra
tend to show large HCN(1–0)/HCO +(1–0) brightnesstemperature ratios, as seen in AGNs, while LIRGs
without luminous AGN signatures in the infrared tend toshow low ratios (Fig. 1 and 2). Namely, in many LIRGs,
this HCN(1–0)/HCO + (1–0) method agrees with our
infrared energy diagnostic, confirming the effectivenessof this HCN/HCO+ method.
The high H CN (1–0)/H CO + (1–0) brightnesstemperature ratios found in AGNs could be explained by
the following scenarios. First, if the HCN abundance inthe gas close to the AGN is enhanced, relative to HCO+,
due to AGN's chemical effects, then the HCN brightnesstemperature can be high. Some theoretical calculations
also predict that HCN abundance can be high, compared014

I Scientific Highlights

TAMURA, Yoichi(University of Tokyo)

KOHNO, Kotaro(University of Tokyo)

to HCO+, in some reasonable parameter range for gas
around buried AGNs in LIRG's nuclei. Alternatively,
HCN molecule can be excited by absorbing mid-infrared
photons, because HCN has a line at 14 μm. Since midinfrared 14 μm emission is strong in an AGN, thisradiative excitation can work effectively in an AGN, andcan produce strong HCN(1–0) emission in the millimeter
wavelength range, through a cascade process. We needdetailed comparison with sophisticated theoretical models
which realistically incorporate the structure of gas at
LIRG's nuclei.

Figure 1: Example spectra of LIRGs obtained with Nobeyama
Millimeter Array. HCN(1–0) emission is strong.

Figure 2: Filled squares: AGN-dominated galaxy nuclei. Opencircles: starburst galaxies. AGNs distribute at the upper
part, compared to starbursts. Filled stars: LIRGs. Large
filled stars with objects name: LIRGs observed thistime. LIRGs with luminous AGN signatures at otherwavelengths tend to distribute at the upper part occupied
by AGN-dominated galaxy nuclei.
Reference[1] Imanishi, M., et al.: 2007, AJ, 134, 2366.

Observations of Circumstellar Disks around Massive Protostars
by the Subaru Telescope
JIANG, Z.

(Purple Mountain Observatory)		

YAO, Y.
(NAOC)TAMURA, Motohide(NAOJ) 		

ISHII, Miki
(NAOJ)

HOARE, M. G.

(University of Leeds)

FANG, M., YANG, J.

(Purple Mountain Observatory)

The formation process for stars with masses several
times that of the Sun is still unclear. The two main
theories are mergers of several low-mass young stellar
objects, which requires a high stellar density, or massaccretion from circumstellar disks in the same way as
low-mass stars are formed, accompanied by outflows
during the process of gravitational infall. Although anumber of disks have been discovered around low- andintermediate-mass young stellar objects, the presenceof disks around massive young stellar objects is still
uncertain. One of the best methods for distinguishingthese two hypothesis is to directly detect a compact
circumstellar disk around a massive YSO. However,massive stars are rarer than low-mass stars, and massive
YSOs are distant in general. Since the expected accretion
disk has a scale of a few 100 AU, a spatial resolution of 0.1
arcsec is necessary.
We have conducted high resolution (~0.1 arcsec)
near-infrared imaging polarimetry with the adaptive
optics, an IR camera (CIAO), and its polarimeter on the
Subaru telescope. High resolution polarimetry is thus
proven to be a powerful tool to detect circumstellar
disks around massive YSOs and can be used to test theaccretion hypothesis for more massive (>10 solar masses)
stars. We have detected such a disk around BN andreported in Nature in 2005. We also observed 4 additional
objects (S140 IRS1, S255 IRS1, NGC7538 IRS1,
IRAS23033+5951) and found evidence for disks around3 objects (Fig. 1) [1]. These are considered to be 10–30
solar mass objects.
These results strongly support the theory that stars
with masses up to 30 solar masses form in the same way
as lower mass stars. We could not detect such evidencein NGC 7538, however. We hope to study more massive
stars with the new instrument HiCIAO, to test theaccretion hypothesis for more massive stars.
Figure 1: (left) Polarization vector (yellow) and polarization
degree (gray-scale) maps. Blue contours show surface
brightness. (right) surface brightness. (red) and polarized
intensity (blue) maps. Contours in (a) show ionized disk.
Reference[1] Jiang, J., et al.: 2008, ApJ, 673, L175.

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Infrared Imaging Polarimetry of the NGC 2071
Star-Forming Region with SIRPOLTAMURA, Motohide, KANDORI, Ryo, HASHIMOTO, Jun, KUSAKABE, Nobuhiko, NAKAJIMA, Yasushi(NAOJ)

HOUGH, J., CHRYSOSTOMOU, A.

Reference[1] Tamura, M., et al.: 2007, PASJ, 59, 467.

MATSUMOTO, Tomoaki(Hosei University)(a) Intensity (JHKs)
SSV 40

IRS 4
IRS 7

IRN 6

IRS 6

IRS 3

IRS 2

IRN 8

IRS 1
IRS 8
IRS 5

IRS 8aSSV 37

NGC 2071(b) Polarized Intensity (JHKs)
IRN 9

IRN 3
IRN 2
IRN 1

IRN 4
IRN 5

IRN 7

Figure 1: JHKs color composite images of intensity (a) andpolarized intensity (b) of the NGC 2071 region. Fieldof-view is 7.′7 × 7.′7 in the left images, while it is 40′′ ×40′′ in the right images.

DECLINATION ( J2000 )22′ 00″23′ 00″24′ 00″25 ′00 ″10 %21′ 00″SIRPOL is the polarimetry mode of the JHKs band
simultaneous infrared (IR) camera SIRIUS mounted
on the 1.4 m IRSF survey-dedicated telescope in South
Africa, which has been available since 2005 December.
The instrument is the first to provide deep and widefield infrared polarimetric images, and can in principle
measure polarizations of all 2MASS-detected sources
within a field-of-view of 7.′7 × 7.′7 in the JHKs bands
simultaneously with 1% polarization accuracy. Sucha capability is unique and has broad applications inmany fields of astronomy, including efficient detectionof circumstellar material that produces scattering, anddelineating magnetic field structures in molecular clouds
and in galaxies, through dichroic polarization.
We conducted deep JHKs imaging polarimetryof the NGC 2071 star-forming region (Fig. 1). Ourpolarization data revealed various infrared reflection
nebulae (IRNe) associated with the central IR young starcluster NGC 2071IR and identified their illuminating
sources. There are at least 4 IRNe in NGC 2071IR, andseveral additional IRNe were identified around nearby
young stars. Each illuminating source coincides with aknown near-IR source, except for IRS 3, which is only
a part of IRN 2 and is illuminated by the radio source
1c. Aperture polarimetry of the other point-like sources
within the field was conducted in this region for the firsttime. The magnetic field structures (from 1 pc down to
0.1 pc) were derived using both aperture polarimetry of
the pointlike sources (Fig. 2) and imaging polarimetryof the shocked H2 emission; both are of dichroic origin
and the derived field directions are consistent with eachother. The magnetic field direction projected on the sky
is running roughly perpendicular to the direction of thelargescale outflow. We argue that the field strength is too
weak to align the outflow in the large-scale field direction
via magnetic braking [1].

(University of Hertfordshire)

20′ 00″(Nagoya University)		

00°19 ′00 ″SATO, Syuji, NAGASHIMA, Chie, KURITA, Mikio

		JOU

5 47 20

OU

47 10

OU

47 00

RIGHT ASCENSION ( J2000 )Figure 2: Ks band polarization map of point-like sources
superposed on the intensity image. Note that thepolarization of the central source of IRN 6 seen in thenorthwest has a clear intrinsic polarization.

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UKIDSS searches of ultracool dwarfs: 1
TAMURA, Motohide, ISHII, Miki, KUZUHARA, Masayuki, NAKAJIMA, Tadashi(NAOJ)

LUCAS, P., KENDALL, T., BURNINGHAM, B., PINFIELD, D.

			(University of Hertfordshire)

It has been established that the dwarf temperature
sequence goes beyond the M stars from the observationsin 1980–90s, and they are now recognied as L stars andT stars. The temperatures for M stars are 3800–2100K,
corresponding to young brown dwarfs and low-massstars. Those for L stars are 2100–1300K, while they areless than 1300K for T stars. L/T stars are brown dwarfs
whose masses are less than 0.075 M.
In retrospect, the first L dwarf was discovered in 1988,
and the first T dwarf was discovered in 1995. About 500
L dwarfs and about 60 T dwarfs have been known before
2007. These numbers can be significantly increased
by recent deep and wide-area surveys. It is expectedthat UKIDSS survey using UKIRT 3.8 m telescope
and WFCAM IR camera can detect many faint objects
that cannot be observed with 2MASS/SDSS surveys.
Furthermore, ultracool dwarfs, too cool to be detectedwith previous surveys, can be detected. Such ultracool
dwarfs are called Y dwarfs; its spectra are expected to bevery similar to that of Jupiter.
Our UKIDSS consortium has first used Early Data
Release (EDR) and developed a method to select goodcandidates for ultracool dwarfs with UKIDSS/SDSS
colors (Fig. 1). We then made extensive follow up
observations such as methane imaging and spectroscopy
with Subaru/Gemini telescopes (Fig. 2).
As a result, from the EDR and First Data Release 1,
we have discovered 13 T dwarfs down to T8.5 [1, 2]. We
are close to the first Y dwarf detection and its statistical
discussion.

UKIDSS Cool Star Consortium

Figure 1: J–H, Y–J 2-color diagram for sources we expect in the
UKIDSS. The location of A-M (III-V) stars, late M, L,
and T dwarfs and z = 2 QSOs have been determinedusing colors synthesized from variable spectroscopy.
Expected Y dwarf colors have been synthesized from thelatest theoretical model spectra.

References[1] Kendall, T. R., et al.: 2007, A&A, 466, 1059.
[2] Lodieu, N., et al.: 2007, MNRAS, 379, 1423.

Figure 2: Example of spectroscopic library of UKIDSS T dwarfs(T4.5–T7.5). The spectra are from Gemini/GNIRS.

I Scientific Highlights

017

Velocity of coronal jets measured by EIS/Hinode
KAMIO, Suguru, HARA, Hirohisa, WATANABE, Tetsuya(NAOJ)

Hinode spacecraft [1] has found a lot of jets in a polar
coronal hole, where used to be thought quiescent. Theseubiquitous phenomena are essential for understanding thecoronal heating and solar wind acceleration in coronalholes. The X-Ray Telescope (XRT; [2]) allowed to
examine the evolution of fine structures in jets. Detailed
analysis indicates that the movements of thread in a jet
is consistent with the X-ray jet model based on magnetic
reconnection [3]. In addition to the apparent motion of
the jets, line-of-sight velocity must be measured to study
their dynamics.
Thanks to the high throughput and resolution of the
EUV Imaging Spectrometer (EIS; [4]), Doppler shiftof Fe XII λ195.12 emission line has been measured ina polar coronal hole [5]. Figure 1 shows radiance andvelocity maps in the Fe XII λ195.12. Elongated jets
are found above bright tiny loops in the coronal hole.
Assuming one component plasma flow, Doppler shiftof −30 km s−1 was derived in the most prominent jet.
Blueshifts in jets are interpreted as upward flow in thecorona. The actual upflow velocity could exceed 200
km s −1 if projection effect is taken into account. The
observation implies that these jets are persistent flows
rather than transient events, since it took about two hours
to complete the raster scan. It is interesting to note thatthese jets are much weaker in radiance than bright loops
in corona and they may not be clearly detected by aimaging telescope. Spectroscopic observations provide
essential data for studying coronal dynamics, which arecomplementary to imaging observation.
It is important to understand the role of magnetic
fields in view of energy release in the corona. Anotherobservations including Solar Optical Telescope (SOT) arebeing investigated to examine magnetic fields in coronalholes.

References[1] Kosugi, T., et al.: 2007, Sol. Phys., 243, 3.
[2] Golub, L., et al.: 2007, Sol. Phys., 243, 63.
[3] Shimojo, M., et al.: 2007, PASJ, 59, 745.
[4] Culhane, L., et al.: 2007, Sol. Phys., 243, 19.
[5] Kamio, S., et al.: 2007, PASJ, 59, 757.

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I Scientific Highlights

Figure 1: Top: Radiance map in Fe XII λ195.12. Coordinates
indicate positions with respect to the Sun center. Bottom:
Doppler velocity in the range of −40 to +40 km s−1.
Positive and negative velocities correspond to blue andred shifts, respectively.

Magnetic Feature and Morphological Study of
X-Ray Bright Points with Hinode
KOTOKU, Jun’ichi, KANO, Ryohei, TSUNETA, Saku, KATSUKAWA, Yukio, SHIBASAKI, Kiyoto(NAOJ)SHIMIZU, Toshifumi, SAKAO, Taro
(ISAS / JAXA)DELUCA, Edward E., KORRECK, Kelly E., GOLUB, Leon, BOBRA, Monica(Smithsonian Astrophysical Observatory)

We observed X-ray bright points in a quiet regionof the Sun with the X-ray Telescope (XRT) aboard the
Hinode satellite from 11 UT to 24 UT on 19 December
2006.
There are two primary results of our investigation:
first we identify four distinct shapes of XBP in the
XRT observations; second we identify several XBPs
that appear to be inconsistent with the flux cancellation
model based on simultaneous SOT/NFI line-of-sightmagentograms and XRT images.

1994 [1], cancelling magnetic features at the photosphereare correlated with their accompanying XBPs in thecorona. However, X-ray intensity changes of XBPs did
not seem to depend on their magnetic footpoint behavior.
In other words, foot-point magnetic field does not directly
affect the upper coronal behavior [2].

Figure 2: Typical morphologies of XBPs. Raw images (top) andunsharp masked images (bottom). From left to right,
images represent loop, multiple loop, cusp and point-likestructures.

Figure 1: A snap shot of the quiet region of the Sun taken with
the XRT on 19 Dec 2006. Small white squares withreference numbers represent areas of identified XBPs.
The large dashed rectangle shows the field of view of
SOT NFI.

High resolution X-ray images revealed that many
XBPs have complicated structure and vary dramaticallywith time. Almost all of the dynamic eruptions in thequiet region were composed of XBPs and they have
either loop or multiloop shapes, as is observed in larger
flares. We classified the morphology of the XBPs into
four types as shown in Figure 2.
In this observation sequence, the brightening XBPs
have strong magnetic fields with opposite polarities near
their footpoints. Several theoretical models of XBPs haverecently been proposed, most of which include magnetic
reconnection for generating the X-ray sources. While wehave found a possible example of associated magnetic
cancellation, at least for some XBPs, their Xray variation
did not seem to be associated with magnetic cancellation.
According to converging flux model proposed by Priest

Figure 3: X-ray images taken with XRT are overlaid with thecontours of the line-of-sight magnetograms taken with
SOT. The contour levels correspond to the polarized
degrees for both plus (red) and minus (cyan).
References[1] Priest, E. R., et al.: 1994, ApJ, 427, 459.
[2] Kotoku, J., et al.: 2007, PASJ, 59 735.

I Scientific Highlights

019

Emergence of a helical flux rope associated with prominence formation
OKAMOTO, Takenori J., TSUNETA, Saku, KATSUKAWA, Yukio, ICHIMOTO, Kiyoshi, SUEMATSU, Yoshinori(NAOJ)SHIMIZU, Toshifumi(ISAS / JAXA)YOKOYAMA, Takaaki(University of Tokyo)

NAGATA, Shin’ichi, SHIBATA, Kazunari		(Kyoto University)

KUBO, Masahito, LITES, Bruce W.
(High Altitude Observatory / NCAR)TARBELL, Theodore D., SHINE, Richard A., BERGER, Thomas E., TITLE, Alan M.
(Lockheed Martin Solar and Astrophysics Laboratory)

Solar prominences are cool material (104 K) floatingin the corona (106 K). It is known that prominences aresupported by coronal magnetic fields against gravity andlocated along polarity inversion lines (PILs). Moreover,based on previous quantitative studies, it is often
thought that magnetic fields in prominences have helicalstructures.
How is such a helical magnetic field created inassociation with prominences in the corona? Two theories
have been discussed: flux rope models and sheared
arcade models. In the former model, an originally twisted
flux rope emerges from below the photosphere into thecorona. In the latter one, potential fields in the corona
are sheared by the photospheric motion along PILs.
As a result, magnetic reconnection occurs among thesheared fields, and then helical fields are constructed in
the corona. However, we have no clear observational
evidence to support either model. To clarify the formation
process of magnetic fields in a prominence, we have toinvestigate the relationship between the evolution of its
associated magnetic fields on the photosphere and theoverlying prominence.
The Hinode satellite was tracking a sunspot in
active region NOAA 10953 from 2007 April 28 to
May 9. Figure 1 shows an Hα filtergram, and a vector
magnetogram of the active region taken or scanned. At
the beginning of this observation, the prominence was so
unstable that it disappeared and reappeared repeatedly.
However, at some point, the prominence became stable.
Focusing on this change, we analyze the time evolutionof photospheric vector magnetic fields. As a result, wefound four features:
1. The abutting opposite-polarity regions on the twosides along the PIL first grew laterally in size and thennarrowed.
2. These abutting regions contained vertically-weak, buthorizontally-strong magnetic fields.
3. The orientations of the horizontal magnetic fields along
the PIL on the photosphere gradually changed withtime from a normal-polarity configuration to a inversepolarity one.
4. The horizontal-magnetic field region was blueshifted.

020

I Scientific Highlights

These indicate that helical flux rope was emerging
from below the photosphere into the corona under thepreexisting prominence [1]. We suggest that this supply ofa helical magnetic flux into the corona is associated withformation and evolution of active-region prominences.

Figure 1: (a) Hα image. (b) Magnetogram. Color contour indicatesthe strength of vertical magnetic fields; red is positiveand blue is negative. Arrows show the strength ofhorizontal magnetic fields. The yellow line is PIL.
Reference[1] Okamoto, T. J., et al.: 2008, ApJ, 673, L215.

Discovery of long, narrow, and straight HII gas in the Coma Cluster
YAGI, Masafumi, KOMIYAMA, Yutaka, YOSHIDA, Michitoshi, FURUSAWA, Hisanori, KASHIKAWA, Nobunari(NAOJ)KOYAMA, Yusei, OKAMURA, Sadanori(University of Tokyo)

We observed the Coma Cluster in broadband andHα narrowband with the Suprime-Cam mounted on the
Subaru Telescope. In the data, we discovered a long,narrow and straight ionized hydrogen structure fromthe center of a poststarburst galaxy, D100 (Fig. 1) [1].
The follow-up spectroscopy confirmed that the structure
has almost the same redshift as D100, and is emittingstrong Hα (Fig. 2). If we assume the distance to the Coma
Cluster to be 100 Mpc and the structure is observed asedge-on, the size of the structure is 60 × 2 kpc.
If we assume that the morphology of the gas is homogeneous cylinder, the mass of the ionized gas is ~2 ×
108 M. The mass is comparable to a whole gas mass ofa dwarf galaxy. Since the structure was not detected inprevious HI observation, the gas is almost fully ionized.
The questions are the origin of the gas, the mechanism
to form the long, narrow, and straight structure, and theionizing source. Such long, narrow and straight ionizedgas features were discovered in other clusters by previous
studies, and they were jets from AGN. D100, however,shows no AGN. Neither X-ray nor radio, which often
associate with jets, was detected around the region.
Moreover, the emission line ratio implies that the ionizing
source is not an AGN, but rather UV photon from HII
regions or shock excitation. We presented two possible
hypotheses to explain these results;
1. A gas rich dwarf is elongated by tidal force during
infall to D100
2. The disk of D100 is stripped by ram pressure of thecluster gas.
Each hypothesis has problems, though. The former cannot
explain the large dispersion of recession velocity in the
structure. Also, the latter hypothesis requires special
configuration that the edge of the tidal structure should beon at the line of sight to D100, and the orbit of the dwarf
should be edge on, which is very rare. The latter, on theother hand, cannot explain why the structure is so narrowand straight. It is a future task to construct a consistentmodel.
Regarding the ionizing source, we proposed threepossible ideas, since there are no AGN nearby;
1. interaction with cluster gas,
2. ionizing photon from star-forming region of D100,
3. the UV from hot cluster gas,
We now have data showing that the current star-formationof D100 is too weak to excite the structure, and 2. isdenied.

Figure 1: B(B), G(Hα), R(i) pseudo-color image. Ionized gas isseen as green.

Figure 2: Spectrun of the gas near the center of D100.

Reference[1] Yagi, M., et al.: 2007, ApJ, 660, 1209.

I Scientific Highlights021

Performance improvement of gravitational wave detector TAMA300
with a low frequency vibration isolation system
ARAI, Koji, TAKAHASHI, Ryutaro, TATSUMI, Daisuke, YAMAZAKI, Toshitaka, FUKUSHIMA, Mitsuhiro
ISHIZUKA, Hideharu, AGATSUMA, Kazuhiro, ARASE, Yuta, IZUMI, Kiwamu
WAKABAYASHI, Yaka, FUJIMOTO, Masa-Katsu, and the TAMA collaboration(NAOJ)We have been working on the new vibration isolation
system, called “Seismic Attenuation System” (SAS),
since 2005. The sensitivity of gravitational wave detector
TAMA300 at around 100 Hz was previously limited bycoupling of alignment sensing noise. In order to improve
the sensitivity of TAMA300 in the low frequency band,the control bandwidth of the alignment control shouldhave been reduced. For this purpose, we replaced theprevious vibration isolation system to the SAS for all offour test masses. The installation and the tuning werecompleted in the summer of 2007.
The vibration isolation performance of the SAS
essentially relies on low resonant frequencies of themechanical systems. The SAS has a multiple-stage
structure with a total height of about 2.5 meters, torealize seismic filtration from the low frequency such as
50 mHz. In order to suppress the excited motion of the
low frequency resonances, three active local controls,
an inverted pendulum control, a torsion mode control,
and a test mass control, are applied. All of these control
servos are realized by digital control systems basedon LabVIEW. With the intrinsic vibration isolation
performance of the SAS and these local control systems,
test mass motions are well stabilized in all frequency
band [1]. The longitudinal fluctuation of the 300-m FabryPerot cavity was measured by a cavity length correction
signal. The displacement spectrum below 10 Hz is shownin Figure 1. By comparison with the spectrum with theprevious suspension system, significant improvement of
the length fluctuation with the SAS above 0.2 Hz was
confirmed.
After the shaking down and tuning of the SAS, thepower recycled operation of the 300-m Fabry-Perot
Michelson interferometer has been recovered [1]. For thelock acquisition of the arm cavity, a digital control with
TMS320C6713 DSP based system with a sampling rateof 200 kHz is newly employed. This achieves control
bandwidth of about 800 Hz. Increasing use of digital
filters makes the interferometer operation flexible andeasier. Digital filters, however, have 100 to 1000 times
worse noise levels compared to well-designed analog
circuits. In order to avoid coupling of these noises to theinterferometer sensitivity, analog frontend system before
and after the digital filters were carefully designed.
The current sensitivity of TAMA300 is shown in
Figure 2. Sensitivity improvement up to 200 Hz was
confirmed although further tuning of the interferometer022

I Scientific Highlights

system is needed for the higher frequency band. Further
improvement is expected by employing fast wave front
sensing servos for mirror angular control.

Figure 1: Length fluctuation of the 300-m cavity with the SAS andwith the previous suspension system.

Figure 2: Current strain sensitivity of TAMA300 (red). The
previous best sensitivity (black) is also shown.

Reference[1] Takahashi, R., et al: 2008, Class. Quamtum Grav., 25, 114036.

Project Milkyway
SAITOH, Takayuki, KOKUBO, Eiichiro, WADA, Keiichi, TOMISAKA, Kohji, MAKINO, Junichiro(NAOJ)

		

OKAMOTO, Takashi(Durham University)

DAISAKA, Hiroshi(Hitotsubashi University)

The aim of “Project Milkyway” is to reveal theformation process of galaxies, especially that of the
Milkyway galaxy, by the state-of-the-art simulations. For
this purpose, we have developed (i) PC-clusters whose
computational nodes consist of ordinary CPUs (AMDOpteron) and special purpose computers, GRAPEs, which
accelerate the calculation of gravity, and (ii) a parallel
tree SPH code ASURA that utilizes GRAPEs.
We first performed high-resolution simulationsof the ISM in order to investigate feasible modellingof star formation in high-resolution simulations [1].
From our simulations, we found that simulations which
adopt a high-n th model, where stars are formed fromdense regions (nH > 100 cm−3), reproduce observational
properties of global star formation such as star formation
histories and surface gas density-surface star formation
rate relations. Previous low-resolution simulations
which adopt the isothermal ISM with a low-nth model(nth = 0.1 cm−3), which is usually used in cosmologicalsimulations of galaxy formation, also reproduce theseproperties. However, only high-nth models can reproduce
the inhomogeneous structure of the ISM and the verticalstructure of gas and stars. It is remarkable that the use ofa high-nth criterion for star formation in high-resolution
simulations makes numerical models fairy insensitive tothe assumed values of the local star formation efficiency.
We next applied the high-nth model to the evolutionof interacting galaxies. We simply considered a collisionof an equal mass, gas rich galaxies with a parabolic orbit.

YOSHIDA, Naoki(Nagoya University)

Figure 2: “Starburst” occurs in the “giant filament” during the firstencounter. A number of star clusters are formed in thegiant filament at the starburst phase. Brown, white andgreen points indicate gas, disk stars, and young stars,
respectively. Red circles represent the star clusters which
is self-bound. We thank Takaaki Takeda, who createdthis beautiful picture.

We use a total of 1.5 × 107 particles to represent twoprogenitor galaxies. From our simulations, we found that(I) a “giant filament” is formed at the collision interface
and the burst of star formation occurs in the filament (seeFig. 1), and (II) a number of star clusters are formed in thegiant filament at the starburst phase (see Fig. 2). These
are consistent with observed properties of interacting
galaxies and none of previous simulations reproduce
these properties.
High-resolution with a realistic star formation model,such as our high-n th model, allows us to study bothquiescent star formation and starburst modes in N-body/
SPH simulations. We are now tackling cosmologicalsimulations of galaxy formation.

Reference[1] Saitoh, T. R., et al.: 2008, PASJ, 60, 667-681.

Figure 1: Star formation rate as the function of time (Myr). Blacksolid and red-dotted lines indicate global star formation
rate for two different mass resolution runs. Blue-solidline indicates the separation distance of galactic cores.

I Scientific Highlights

023

Common-Path Spectropolarimetric Differential Imager
Using Variable Channeled Spectrum
MURAKAMI, Naoshi, ABE, Lyu, TAMURA, Motohide(NAOJ)

BABA, Naoshi(Hokkaido University)

Various concepts of a high-contrast imager have been
proposed for direct detection of exoplanets. In particular,
a four-quadrant phase mask (FQPM) coronagraph caneliminate stellar light efficiently [1]. However, stellar
speckle noise due to imperfections of optical surfaces
prevents from observing the exoplanets. For suppressing
the residual speckle noise, a spectral differential imager(SDI) or a polarization differential imager (PDI) has
been proposed [2, 3]. The differential imagers acquire
two images of different wavelengths or two orthogonal
polarizations, and subtract one image from another one tocancel out the speckle noise. However, non-common-pathaberration will be a serious problem because it causes
remnant speckle noise in the differential images.
We propose a novel common-path differential
imager, which can obtain both spectral and polarizationdifferential images. Figure 1 shows the principle. The
SDI-part is composed of two polarizers (P1 and P2), avariable retarder (VR1), and an interference filter (IF). By
adjusting the retardation of VR1 and transmittance of IF
properly (Δ0 and T0, respectively), a spectral transmittanceof the optical system can be written as T0 cos2(Δ0/2),
which acts as a bandpass filter with a central wavelengthof λ1, as described in Figure 1a. When the retardation is
set to Δ0 + π, the transmittance becomes T0 sin2(Δ0/2) andalso acts as a bandpass filter of λ2, (Fig. 1b). A spectral
differential image can be obtained by subtracting two
images acquired by these bandpass filters. The PDI-part iseasily realized by inserting an additional variable retarder(VR2). Two images of 0°- and 90°- linearly polarizations
can be obtained when the retardation of VR2 is set to
2π and π, respectively. Thus, a polarization differential
image can be obtained by subtracting these two images.
We carry out numerical simulations of the proposed
method (only the SDI-mode) equipped with an achromatic
FQPM coronagraph. We simulate observations of amethane absorption feature in the H band. Note that, inpractice, the variable retarder VR1 must be separated
into a fixed retarder with large retardation and a variable
retarder with small one, because it is difficult to reachlarge enough retardation with a single variable retarder.
As the fixed and variable retarders, we assume a quartz
retarder with a thickness of 1.8mm and an achromatic
variable retarder, respectively. The central wavelengthand bandwidth of the assumed interference filter are λ0= 1610 nm and Δλ = 85 nm, respectively. As a result,the simulated optical system has two specific central024

I Scientific Highlights

wavelengths (λ1 = 1580 nm, λ2 = 1635 nm). Figure 2
shows the simulated FQPM-coronagraphic images withand without the SDI. As a result, a model exoplanet,
which is 2 × 10−8 times fainter than a model star can beclearly observed at 5.0 λ/D (a white arrow).
PDI
SDI
VR2

VR1

IF

P1

Detector

P2
Interference Filter

Channeled Spectracos 2 δ 0T0(a) ∆V 1 (λ ) = ∆ 0 (λ )Resultant Spectra

T0 cos 2 δ 0

=

λ

λ1

sin δ 02T0(b) ∆V 1 (λ ) = ∆ 0 (λ ) + π

T0 sin 2 δ 0

=
λ2

λ

Figure 1: Principle of a common-path spectropolarimetricdifferential imager.

(a)

0.0

(b)

1e-6

-5e-9

5e-9

Figure 2: Numerical simulations of FQPM-coronagraphic images(a) without and (b) with the SDI.
References[1] Rouan, D., et al.: 2000, PASP, 112, 1479.
[2] Racine, R., et al.: 1999, PASP, 111, 587.
[3] Baba, N., Murakami, N.: 2003, PASP, 115, 1363.

Wide-Field Survey of the Local Group Dwarf Spheroidal Galaxy Leo II
KOMIYAMA, Yutaka, FURUSAWA, Hisanori, MIYAZAKI, Satoshi
NAKATA, Fumiaki, OKADA, Norio, YAGI, Masafumi(NAOJ)

DOI, Mamoru, OKAMURA, Sadanori, SHIMASAKU, Kazuhiro, YASUDA, Naoki(University of Tokyo)

		

HAMABE, Masaru(Japan Women’s University)

KIMURA, Masahiko(Kyoto University)

We carried out a wide-field imaging survey of the
Local Group dwarf spheroidal galaxy Leo II using Subaru
Prime Focus Camera (Suprime-Cam) (Fig. 1). The
extensive field coverage of Suprime-Cam enabled us toinvestigate the extent of Leo II and the variation of theproperties of stars within the galaxy. In particular, since
Leo II is located so close (230 kpc), we can measure theposition and the brightness of each star in the galaxy very
accurately. By comparing these measurements and theevolution theory of stars, we can investigate the evolutionof the galaxy, as an assembly of stars in the galaxy, indetail.
We first investigated the extent of Leo II by counting
the number of red giant stars, which were selected fromthe color-magnitude diagram of Leo II, as a function of
the radius; over a dozen red giant stars were found toexist beyond the tidal radius. To investigate how these
extra-tidal stars are distributed, we made the surface
brightness map determined by the stars that belong to
Leo II (Fig. 2). As seen in this picture, a knotty structure,
whose surface brightness is as faint as about 31 mag/arcsec2, was discovered on the east (left) side of Leo II.
The stars belonging to the structure are relatively old
and their properties are similar to that of the stars locatedwithin the main body of the galaxy. We suggest that thisstructure could be a small globular cluster being disrupted
by the tidal force of the galaxy; however, further observation is required to give a definite answer.
We also investigated distributions of red giant stars,
horizontal branch stars and sub-giant branch stars locatedin the inner part of the galaxy. We showed that theproperty of the stars is different throughout the galaxy;
the younger stars are found in the inner portions while
old stars are found all through the galaxy. We conclude
that star-forming activity occurred more than 8 Gyr
ago throughout the galaxy, and the star-forming region
gradually shrank from the outside toward the center [1].
The formation of stars ceased approximately 4 Gyr ago,
except for the galactic center, where a small population
younger than 4 Gyr is present.

References[1] Komiyama, Y., et al.: 2007, AJ, 134, 835.

OUCHI, Masami(Carnegie Observatory)

Figure 1: False-color image of Leo II (composed from V andIc band images). The field of view is 26.67 arcmin,covering much wider area than the tidal radius of Leo II(8.6 arcmin).

Figure 2: The surface brightness map of Leo II. From this figure,very faint knotty structure (shown in green to the east
(left) of Leo II) was discovered.

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025

Activities of parent comets and related meteor showers
WATANABE, Jun-ichi, SATO, Mikiya(NAOJ)

The activity of a meteor shower is thought to be
proportional to the activities through time of the parent
comet. Recent applications of the dust trail theory provide
us not only with a new method to forecast the occurrences
and intensities of shower activities, but it is also offers a
new approach to explore the history of past activities ofthe parent comet by retro-tracking its associated meteor
showers. We introduce the result of an effort for relating
meteor shower activities to the parent comet activities forwhich we chose the Draconids and comet P/GiacobiniZinner in this paper [1].

ZHR
16000
14000

1933

12000

1946

10000
Expected ZHR

8000

Obs. ZHR(MIN)

6000

Obs.ZHR(MAX)

4000
1998

2000
0
0

0.5

1

1.5

2

Σ fM

Figure 2: The relation between the ZHR and fM value. The solidline is the expected relation when normalized to the 1998
outburst. The vertical lines are the range of the observed
ZHR. Both the 1946 and 1933 storms are higher than
expected.

ZHR
16000
14000
12000

1933

10000

Expected ZHR

8000

Obs. ZHR(MAX)

1946

6000
4000

Obs. ZHR(MIN)

1998

2000
0
0

Figure 1: Comet 21P/Giacobini-Zinner taken on October 2 with the
50cm telescope at the Mitaka of National Astronomical
Observatory of Japan. The image is a composite ofseparate exposures of three filters ofdifferent color
bands.

1

2

3

4

5

Σ (f M × ΔQ(H10))

Figure 3: Same as figure 1, but the "corrected" fM value by theabsolute magnitude of the parent comet. The 1933 and1946 storm activities are well within the expected levelof the 1998 activity case.
Reference[1] Watanabe, J., Sato, M.: 2008, Earth, Moon, and Planets, 102,
111.

026

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Three-dimensional simulations of molecular cloud fragmentation regulated
by magnetic fields and ambipolar diffusion
KUDOH, Takahiro(NAOJ)

Time = 150.
1.5
1.0
0.5
0.0
-0.5
-1.0
-1.5
-2.0

= 1.00

20

10

y

0

-10

-20

-20

z

We employ the first fully three-dimensional
simulation to study the role of magnetic fields and ionneutral friction in regulating gravitationally-driven
fragmentation of molecular clouds [1]. The cores in an
initially subcritical cloud develop gradually over an
ambipolar diffusion time while the cores in an initiallysupercritical cloud develop in a dynamical time (Fig. 1).
The infall speeds on to cores are subsonic in the case of
an initially subcritical cloud (Fig. 2), while an extended (≥0.1 pc) region of supersonic infall exists in the case of an
initially supercritical cloud. These results are consistent
with previous twodimensional simulations. We also foundthat a snapshot of the relation between density (ρ) andthe strength of the magnetic field (B) at different spatial
points of the cloud coincides with the evolutionary trackof an individual core (Fig. 3). When the density becomeslarge, both relations tend to B ∝ ρ0.5.

-10

0

x

10

20

= 1.00

2
1
0
-1
-2
-20

-10

0

x

10

20

Figure 2: The logarithmic density contours for β0 = 0.25 at t = 150.
Arrows show velocity vectors on each cross section. The
unit of the velocity vector is the sound speed (~0.2 km/s)
at z = 0. Upper panel shows the cross section at z = 0,
and the lower panel shows the cross section at y = 4.3.

Figure 1: The time evolution of the density at the location
where the density reaches its maximum value in eachsimulation. Each line shows a case of different initialplasma β (β0). When β0 < 1, the cloud is subcritical. The
unit of time is ~ 2.5 × 105 yr.
Reference[1] Kudoh, T., et al.: 2007, MNRAS, 380, 499.

Figure 3: Open circles show the magnetic field strength as afunction of density along z = 0 at t = 150 for the modelwith β0 = 0.25. Filled circles are the same for β0 = 4, at t
= 15.3. The blue line shows the evolutionary track of thepoint at which the density achieves its maximum value
for the model with β0 = 0.25. The red line is the same forβ0 = 4. The dashed line shows B ∝ ρ0.5. The unit of themagnetic field strength is ~10 µG.

I Scientific Highlights

027

Vertical Temperature Structures of the Solar Corona derived
with the Hinode X-Ray Telescope
KANO, Ryohei, TSUNETA, Saku, KOTOKU, Jun’ichi, BANDO, Takamasa
HARA, Hirohisa, SHIMOJO, Masumi, SHIBASAKI, Kiyoto(NAOJ)SAKAO, Taro, NARUGAGE, Noriyuki, MATSUZAKI, Keiichi
SHIMIZU, Toshifumi, NAKATANI, Ichiro(JAXA / ISAS)

DELUCA, Edward, LUNDQUIST, Loraine, GOLUB, Leon
(SAO)

Reference[1] Kano, R., et al.: 2008, PASJ, 60, 827.

(a) Temperature
0.1 RSUN

1.0

1.5

2.0

2.5

MK

(b) Log EM
0.1 RSUN

24.5 25.0 25.5 26.0 26.5 27.0 27.5

cm-5

Figure 1: (a) Temperature and emission measure maps derived
with the filter-ratio method of Hinode/XRT. We
accurately estimated scatterred X-rays from surrounding
corona in lunar shades, and analyzed the coronaltemperature in it.
2007 Feb 17

2.4

2.2

Temperature (MK)We obtain temperature structures in faint coronalfeatures above and near the solar limb with the X-ray
Telescope (XRT) on board the Hinode satellite byaccurately correcting the scattered X-rays fromsurrounding bright regions with occulted images during
the solar eclipses [1]. Figure 1 shows the temperature andemission measure maps taken at the eclipse on February
17, 2007, in which the Moon passed the southern part ofthe solar corona and occulted a polar coronal hole. Our
analysis yields the polar coronal hole temperature ofabout 1.0 MK and emission measure in the range of 1025.5–1026.0 cm−5. The derived temperature is almost consistent
with past studies by emission lines, but inconsistent with
the SXT result. It is probably because SXT has almost no
response to 1 MK plasma. Above the coronal hole someradial plume-like structures were seen. The temperature
profiles along them as a function of height are shown in
Figure 2. They appear to have increasing temperature
with height during the first 100 Mm and constanttemperatures above 100 Mm. We discussed the possibilityof heating by Alfvén waves with periods of 3–5 minutes,
and ruled out such the heating at last.
In addtion, we analyzed diffuse quiet Sun region
at mid-latitudes by the eclipse on March 19, 2007, andfound for the diffuse quiet-Sun region the temperatures
are the highest just above the limb and appear to decrease
with height. The difference with the temperature along
plume-like structures may be due to different magnetic
configurations.

2.0

1.8

1.6

1.4
0

Height (RSUN)
0.05

0.10
50

0.15
100
Height (Mm)

0.20

0.25
150

200

Figure 2: Temperature profiles along some plume-like structures
which were seen above the southern coronal hole (thindot lines in Figure 1).

028

I Scientific Highlights

Radial Velocity Variations of Procyon:
Detection of Oscillations and Long-Term Variations
			

KAMBE, Eiji, ANDO, Hiroyasu(NAOJ)		

SATO, Bun’ei(Tokyo Institute of Technology)

Small uncertainties in physical processes in stars, suchas convection, rotation, and material diffusion, have often
large consequences for the evolution of stars. The goal ofasteroseismology is to improve the description of interior
physics of stars to such a level that cannot be reachedwith conventional observations. The asteroseismology ofsolar-type stars become active than ever, as an applicationof helioseismology, as a probe of planet-harboringstars, and stimulated by developments of sophisticatedobserving methods.
After Bedding et al.’s convincing detection of solartype oscillations in β Hyi in 2001, asteroseismology is
now applied to several main-sequence stars like α Cen A.
Despite formidable challenges by many researchers forthe past few decades, however, features of oscillationsin Procyon have not been uncovered yet. One of reasonsof this inability is that the star, almost departing its mainsequence phase, has already lost its simple oscillation
pattern in the periodogram. Therefore, to firmly obtainits oscillation frequencies, we conducted a big observing
campaign of Procyon in Jan. 2007 (P.I. Tim Bedding),
connecting 10 observatories around the globe.
We, Japanese group, developed an iodine cell for the
HIDES at Okayama Astrophysical Observatory in 2000,
and have tried to improve our radial-velocity extraction
software since then. In fact, for iodine cell observations,
it is crucial to remove influences of temporally variable
instrumental profile of the spectrograph on the stellar
radial velocity. In the 2007 campaign, we can reach theprecision of 2 m s−1 [1].
Owing to such high precision, we could see theoscillation signal in real temporal domain at Okayama(Fig. 1). More interestingly, in comparison to simultaneous
observations with AAT we can clearly detect slow
variations on time scale of hours to weeks in the star.
These are probably due to granules and spots in the star,
indicating similar activities occurring in Procyon to thoseseen in our sun. We are now examining properties of theoscillations and the slow variations by combining all
campaign data.

and 14 authors

Figure 1: Radial velocity variations in Procyon during 2007
campaign. Not only oscillation signals, but also slow
variations are clearly seen both in OAO and AAT data.

Reference[1] Kambe, E., et al.: 2008, PASJ, 60, 45.

I Scientific Highlights

029

Physical and Chemical Properties of Massive Clumps
in the AFGL 333 Cloud
SAKAI, Takeshi

OKA, Tomoharu, YAMAMOTO, Satoshi(NAOJ)			

A far-infrared source, AFGL 333, is located in the
W 3 giant molecular cloud at a distance of 1.95 kpc [1].
AFGL 333 itself is a compact HII region generated by a
B0.5 type star [2]. Recently, we have mapped the AFGL
333 region in the C0 3P1–3P0 line and the CO J = 1–0
isotopomer lines ([3]; Paper I). From the C18O J = 1–0
observation, we have found two massive clumps in the
AFGL 333 cloud: Clump A (2.3 × 103 M) and B (1.4 ×
103 M) (Fig. 1a). Although their masses are comparable
to those for on-going massive star-forming clumps, no
IRAS and NVSS sources are associated with Clump A
and B. In addition, we have found in Paper I that the[C 0]/[CO] and [CCS]/[N 2H +] ratios are higher in the
AFGL 333 cloud than in the W 3(OH) cloud. From theseresults, we have suggested that these massive clumps are
in an early stage of massive star formation. In this paper,
we have further investigated their physical and chemical
properties in detail.
We have mapped the N2H+ J = 1–0, CCS JN = 43–32,
HC3N J = 5–4 toward two massive clumps in the AFGL
333 cloud by using the Nobeyama Radio Observatory 45
m telescope (Fig. 1b–d). The distributions are found to bedifferent from molecule to molecule. The N2H+ emission
comes from the both clumps, whereas the CCS and HC3N
emissions mainly come from Clump B. We found that the[CCS]/[N2H+] and [HC3N]/[N2H+] ratios tend to be higher
in Clump B than Clump A. These results may indicatethat Clump B is chemically younger than Clump A.
In Fig. 1e, we plot 2MASS sources as diamonds.
Several 2MASS sources with H–K > 2, which are expected to be YSO candidates, are associated with Clump
A. In contrast, such sources are not found in the central
part of Clump B. These results indicate that Clump B isin an earlier evolutionary stage than Clump A.
Figure 1f shows the 1.3 mm continuum contour map
observed by [4]. It appears that each clump contains
four cores (MMS 1a–d in Clump A and MMS 2a–c and
3 in Clump B). In the Spitzer 24 µm image (Fig. 1g),
dark patches correspond to MMS 2a–c, implying thatMMS 2a–c are still starless or in a very early stage ofstar formation. We suggest that MMS 2a, which is themost massive core in Clump B, might be a starless corein which high- or intermediate mass stars will be formed
there in the near future. Such a core is an important
target to understand the initial condition of high- orintermediate-mass star formation. Details of this study
are described in [5].

030

I Scientific Highlights(University of Tokyo)
(a)

(e)

0 47

C 18O J=1-0 (b)effective
beam size

H -K > 2
H -K < 244(c) C C S J =4 -3
N

3

2

(d)

H C 3N J=5-4

beam size

beam sizem m continuum(K lein etal.2005)

1a

1b

45

N 2H + J=1-0

effective
beam size

(f)

46
b

			

1c
1d

2a

43

3

42
134 13

12
l

2b
2c

11

Figure 1: Integrated intensity maps of C18O J = 1–0 (a), N2H+ J= 1–0 (b), CCS JN = 43–32 (c), HC3N J = 5–4 (d). (e)Distribution of the 2 MASS point sources. (f) 1.3 mm
continuum contour map observed by [4]. (g) Spitzer 24
μm image.
References[1] Xu, Y., et al.: 2006, Science, 311, 54.
[2] Hughes, V. A., Viner, M. R.: 1982, AJ, 87, 685.
[3] Sakai, T., Oka, T., Yamamoto, S.: 2006, ApJ, 649, 268.
[4] Klein, R., et al.: 2005, ApJS, 161, 361.
[5] Sakai, T., Oka, T., Yamamoto, S.: 2007, ApJ, 662, 1043.

Three Dimensional Line Transfer Study of Molecular Gas
at the Centers of Active Galaxies
YAMADA, Masako, WADA, Keiichi, TOMISAKA, Kohji(NAOJ)

Molecular gas in external galaxies is a subject of
crucial importance for observational and theoreticalstudies of galaxy formation. Among the interstellar
medium (ISM) in external galaxies, compact molecular
gas around an active galactic nuclei (AGN) is expected
to be an energy budget from AGN and/or the central
starburst. Recent observations suggest line ratios inmillimeter and submillimeter band may be a good tool toreveal the longstanding question on the origin of activity– AGN or nuclear starburst [1]. In spite of numerous
observational studies towards the compact molecular gas
or AGN torus at the center of external galaxies, current
instruments have not succeeded in resolving internalhydrodynamical and/or thermal structures [2, 3].

ISM is subthermally excited and marginally thick (τ0 ≈1), interpretation of observational results should be done
carefully. Figure 2 shows the density and optical depth
increment distributions along two lines of sight labelled
as (a) and (b) in Figure 1. At the point (a) the stimulated
emission dominates the intensity due to weak inverted
population, though, such an amplification does not appear
at the point (b). These results emphasize the ability andapplicability of our approach, that is, the compilationof hydrodynamic simulations and three-dimensionalradiative transfer calculations.
(a)

(b)

Figure 2: Density and optical depth increment distribution
along two lines of sight at the points labeled (a) and(b) in Figure 1. Red lines denote density, and blacklines do optical thickness increment, respectively.
These correspond different circumstances, due toinhomogeneous torus structure and excitation condition.

Figure 1: The integrated intensity distribution of HCN(1–0) lineof our simulation in face-on view.

In order to study the internal structures of compact
molecular gas at the center of an active galaxy, we
performed line transfer calculations of HCN, and HCO+
rotational lines along with high resolution hydrodynamic
simulation [2]. Figure 1 shows an integrated intensity
distribution of HCN(1–0) line. It presents inhomogeneous
intensity distribution caused by highly clumpy density
and temperature structures of the molecular gas. The
typical size of bright spots appearing in Figure 1 is about
10 pc, or 0′.′1 if the galaxy is located at distance of 20
Mpc. The forthcoming high resolution observation with
Atacama Millimeter/submillimeter Array (ALMA) can
resolve such tiny structures. In this mean, our line transfer
simulation method is capable of direct simulation of highquality mm./submm. observations in ALMA era.
These results demonstrates that when inhomogeneous

Our results of excitation temperatures show that line
ratio RHCN/HCO+ > 1 is quite difficult to achieve unlessfractional abundance of HCN is much greater than thatof HCO+, namely yHCN ≥ 10 × yHCO+ or more (where y ismolecular abundance compared with hydrogen molecule).
Realistic simulation with chemical evolution models will
reveal the validity of HCN/HCO+ diagnostics of active
galaxies.
References[1] Kohno, K.: 2005, API Conf. Proc., 783, 203.
[2] Yamada, M., Wada, K., Tomisaka, K.: 2007, ApJ, 671, 73.
[3] Wada, K., Tomisaka, K.: 2005, ApJ, 619, 93.

I Scientific Highlights

031

Subaru Near-Infrared Multicolor Images ofClass II Young Stellar Object, RNO 91
MAYAMA, Satoshi(Graduate University for Advanced Studies)

TAMURA, Motohide, HAYASHI, Masahiko, ISHII, Miki, HAYASHI, S., Saeko, KUDO, Tomoyuki(NAOJ)

ITOH, Yoichi, OASA, Yumiko				(Kobe University)			

RNO91 is known as a source of complex molecular
outflows. Previous studies suggested that RNO91 was
associated with a reflection nebula [1, 2, 3], a CO outflow[4], shock-excited H 2 emission [5], and a disk typestructure [3]. However, geometry of RNO91, especially
its inner region, is not well confirmed yet. High resolution
imaging is needed to understand the nature of RNO91
and its interaction with outflow.
Thus, we conducted sub-arcsecond near-infrared
imaging observations of RNO91 with CIAO mounted on
the Subaru 8.2 m telescope. We present our JHK banddata along with optical images, which are the highest
resolution images of RNO91 ever taken (Fig. 1) [6]. We
examined the colors of associated nebula and compared
the geometry of the outflow/disk system suggested by ourdata with that already proposed on the basis of previous
studies. The main conlusions are as follows [6]:1. Our K-band image shows bright circumstellar
nebulosity detected within ~2″ around the central source
while it is less conspicuous at shorter wavelengths. At
all wavelengths, radial profile of the surface brightness
showed a change of slope at ~2″(300AU) from the central
peak, suggesting a morphological difference beyond thispoint. P.A. and size of this red color nebulosity agree withthose of the previously detected polarization disk. These
data agreement indicates that this bright nebulosity region
which follows the reddening law might be attributed to a
disk-like structure.
2. At J and optical wavelengths, several blue knot-likestructures are detected. Each of these structures has a
few of 10 AU scales and randomly distributed aroundand beyond the bright circumstellar disk. We suggestthat these knotty reflection nebulae may represent
disintegrating fragments of an infalling envelope. The
complex distribution of reflection nebulosity seen around
RNO91 appears to confirm the interpretation of thissource as an object dispersing its molecular envelope
while transitioning from protostar to T Tauri star.
3. Our image has the appearance of arc-shaped nebulosity.
We interpret these structures as being roots of a bipolar
cavity opening toward the northeast and the southwest.

032

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FUKAGAWA, Misato(Nagoya University)

Figure 1: J, H and K band images of RNO91 with an HST opticalimage (F606W). Field of View (FOV) is 17″ × 17″.

References[1] Schild, R., Weir, N., Mathieu, R. D.: 1989, AJ, 97, 1110.
[2] Hodapp, K.-W.: 1994, ApJS, 94, 615.
[3] Weintraub, D. A., et al.: 1994, ApJ, 423, 674.
[4] Arce, H. G., Sargent, A. I.: 2006, ApJ, 646, 1070.
[5] Kumar, M. S. N., et al.: 1999, A&A, 344, L9.
[6] Mayama, S., et al.: 2007, PASJ, 59, 1153.

Parallax measurement of star-forming region S269 with VERA
HONMA, Mareki, BUSHIMATA, Takeshi, HIROTA, Tomoya, IWADATE, Kenzaburo, JIKE, Takaaki
KAMEYA, Osamu, KAMOHARA, Ryu-ichi, KAN-YA, Yukitoshi, KAWAGUCHI, Noriyuki
KOBAYASHI, Hideyuki, KUJI, Seisuke, KURAYAMA, Tomoharu, MANABE, Seiji, MIYAJI, Takeshi
OYAMA, Tomoaki, SAKAI, Satoshi, SATO, Katsuhisa, SHIBATA, M. Katsunori, TAMURA, Yoshiaki(NAOJ)

CHOI, Yoon Kyung, OH, Chung Sik, SUDA, Hiroshi(University of Tokyo)

		

SASAO, Tetsuo(Ajou University)		

KIJIMA, Masachika, YAMASHITA, Kazuyoshi(Graduate University for Advanced Study)

IMAI, Hiroshi, NAGAYAMA, Takumi, NAKAGAWA, Akiharu, OMODAKA, Toshihiro
SHINTANI, Motonobu, TSUSHIMA, Miyuki

Reference[1] Honma, M., et al.: 2007, PASJ, 59, 889.

time(day)Figure 1: East-West motion of the maser source in S269 observedwith VERA. The annual modulation caused by theparallax (π = 189 ± 8 μas) is clearly seen.

Measurementswith HI 21cm line

S269

Rotation velocity (km/s)

S269 (Sharpless 269) is a massive star forming region
toward constellation Orion, and a bright H 2O maser
source is associated with S269. We have performed
highprecision astrometry of the H 2O maser in S269
with VERA, and detected the annual modulation in theeastwest position offset as shown in Figure 1. From theamplitude of the position modulation, the trigonometricparallax of S269 is determined to be 189 ± 8 μas. This
corresponds to the source distance of 17250 light-year,
being one of the largest ditances ever measured by meansof trigonometric parallax.
The proper motions of S269 have also been measured
based on the VERA observations. The relative motion of
S269 with respect to the LSR (the Local Standard of Rest)
is found to be 0.2 mas yr−1. Such a small proper motion
can be explained if the velocity vectors of S269 and the
Sun are similar to each other and cancelled out in therelative measurements. Based on this fact combined withthe parallax measurement of S269, the Galactic rotation
velocity at the position of S269 is also determined
precisely. The result indicates that the difference ofrotation velocities at the Sun and at S269 (which is 13.1
kpc away from the Galaxy’s center) is less than 3 %. This
gives the strongest constraint on the flatness of the outerrotation curve as shown in Figure 2, and provides a directconfirmation on the existence of large amount of dark
matter in the Galaxy’s outer disk.

East-West offser㸦mas㸧(Kagoshima University)

Uncertainty inprevious studies

Sun

Rota
witho tion cur
ve
ut da
rk m
atter










Distance from the Galaxy Center (in 10000 light year)

Figure 2: Rotation curve of the Galaxy obtained by previous
studies as well as the rotation velocity at S269 obtainedwith VERA. Our observations suggest that the rotation
curve is likely to be flat out to ~40000 light year fromthe Galaxy’s center.

I Scientific Highlights

033

Dense molecular gas arc in supergiant HII region NGC 604
TOSAKI, Tomoka1, MIURA, Rie1,2, SAWADA, Tsuyoshi1, KUNO, Nario1
NAKANISSHI, Kohichiro1, KOHNO, Kotaro2, OKUMURA, Sachiko1, KAWABE, Ryohei1(1 NAOJ, 2 University of Tokyo)

2

Declination (J2000.0)

30˚49’

4

6

1

2

+

47’

3

4

30s

25s

CO(3-2) ASTE

CO(1-0) 45m

48’(K km s -1)

gas compressed by the stellar wind and/or supernova of
the first-generation stars of NGC 604, i.e., the central starcluster of NGC 604. Thus, NGC 604 is an example of alarge-scale sequential star formation.
0.4

30˚48’00"

Declination (J2000.0)

Giant or supergiant HII regions (hereafter referred toas GHRs) are one of the most prominent objects in starforming galaxies at the optical wavelength (Kennicut
1984). Central star clusters in GHRs appear to haveformed during the initial stages of the formation of
GHRs, and are expected to have a strong impact on theirnatal molecular clouds due to their strong UV radiation,
stellar wind, and supernova explosion. Therefore, GHRs
provide us with an ideal environment to understand theclustered OB star formation process, and their impact on
the ambient interstellar medium (ISM). These physicalprocesses are also crucial in the evolution of starburst in
galaxies.
To address this issue, we present the 12CO(3–2) and
12
CO(1–0) observations of NGC 604 in the nearest faceon
spiral galaxy M 33 using the Atacama Submillimeter
Telescope Experiment (ASTE) 10-m and the Nobeyama
Radio Observatory (NRO) 45-m telescopes [1].

0.6

0.8

1.0

CO(3-2)/CO(1-0) ratio

100 pcCO(3-2)/CO(1-0) ratio (contour)
Ha (grey)30"
47’00"
30"
46’00"
01h 34m 38s

36s

34s

32s

30s 01h 34m 38s+
200 pc

45’
40s

35s

30s

25s 01h 34m 45s

40s

Right Ascention (J2000.0)

35s

Figure 1: Total integrated intensity maps of 12CO(1–0) (left panel)and 12CO(3–2) (right panel). the position of the central
star cluster of NGC 604 indicated as cross.

We found a high 12CO(3–2)/12CO(1–0) ratio gas withan arc-like distribution (“high-ratio gas arc”) surrounding
the central star cluster of the supergiant HII region NGC
604. The discovered “high-ratio gas arc” extends to thesouth-east to north-west direction with a size of ~ 200
pc. The western part of the high-ratio gas arc closely
coincides well with the shells of the HII regions traced by
Hα and radio continuum peaks. The CO(3–2)/CO(1–0)
ratio, R3–2/1–0, ranges between 0.3 and 1.2 in the observed
region, and the R3–2/1–0 values of the high-ratio gas arc arearound or higher than unity, indicating very warm (Tkin ≥60 K) and dense (nH2 ≥ 103–4 cm−3) conditions of the highratio gas arc. We suggest that the dense gas formation andsecond-generation star formation occur in the surrounding

034

I Scientific Highlights

34s

32s

30s

Figure 2: Maps of the ratio of 12CO(3–2) to 12CO(1–0) (left panel)and the Hα emission by HST (right panel; from the HST
archive). The contour levels are 0.4, 0.6, 0.8, and 1.0.
The crosshairs in the center indicate the position of thecentral star cluster of NGC 604, while the stars represent
the peak positions of the HII regions detected by λ 3.6-cm
radio continuum emission.

46’

01h 34m 45s

36s

Right Ascention (J2000.0)

Figure 3: Scematic view of NGC 604.

Reference[1] Tosaki, T., et al.: 2007, ApJL, 664, L27.

Near-Infrared Imaging Polarimetry of the Star Forming Region NGC 2024
KANDORI, Ryo, TAMURA, Motohide, KUSAKABE, Nobuhiko, NAKAJIMA, Yasushi
HASHIMOTO, Jun, ISHIHARA, Akika(NAOJ)(Nagoya University)

HOUGH, James H.

(University of Hertfordshire)

NGC 2024 through dichroic polarization. The average
position angle of projected magnetic fields acrossNGC 2024 is 110°. We found a good consistency inmagnetic field structures obtained using near-infrareddichroic polarization and sub-mm/far-infrared dust
emission polarization [5, 6], indicating that the dichroic
polarizations at near-infrared wavelengths trace magnetic
field structures inside dense molecular clouds.

55-1° 58′57

56

Dec. (J2000)

54

53

52

51

NGC 2024: Intensity (JHKs)

5h 42m 00

41m 55

50

45

40

35

30

R.A. (J2000)

Figure 1: Three color composite of JHKs intensity (I) images
toward NGC 2024. The image is in logarithmic scale.

55

Dec. (J2000)

54

53

52

51

Polarized Intensity (JHKs)

56

We present near-infrared polarimetric studies of NGC
2024, a massive star-forming region in the Orion B giant
molecular cloud [1]. Observations were made using thenear-infrared imaging polarimeter SIRPOL (polarimeter:[2], camera: [3]) on the IRSF 1.4-m telescope in South
Africa. IRSF/SIRPOL is the first instrument to provide
deep (J = 19.2 mag, S/N = 5) and wide-field (7.′7 × 7.′7)
polarization images at JHKs simultaneously. Suchcapability is particularly useful to trace extended
polarized emission by dust scattering, i.e., infrared
reflection nebulae (IRNe), and to delineate magnetic fieldstructure through dichroic polarization.
In Figs. 1 and 2, we show composite JHKs intensity(I) and polarized intensity (PI) images, respectively. On
the largest scale, we found an extensive IRN extending
over the entire FoV in Fig. 2. Though the IRN can be
responsible for massive star(s) exciting the HII region,
source identification studies reported so far are still
unclear because of heavy obscuration of the nebula byforeground dust lane. We directly constrained the positionof illuminating source through the analysis of polarization
vectors; a massive O8–B2 type star IRS 2b, located in thecenter of centrosymmetric polarization vector pattern, is
most likely to be the source illuminating the nebula.
For smaller-scale nebulae, we discovered five IRNe
associated with YSOs in our polarization images (Fig.
2). The pattern of polarization vector around the YSOs
appears centrosymmetric, indicating that these IRNe
are illuminated by each central star and are responsible
for the structure of circumstellar material that produces
strongly polarized light through dust scattering. The
polarized intensity of each IRN shows a butterfly-shaped
emission pattern extending over 5000–10000 AU, which
agrees well with the picture of disk/envelope system
around young stars.
We performed software aperture polarimetry of the
211 point-like sources detected on the JHKs intensity
images. We found 64 highly polarized sources (HPS),
which show larger polarizations than estimated fromdichroic extinction. The large polarization of HPSs
indicates that they are accompanied by unresolved IRNe.
By comparing our polarimetry with recent spectrophotometric results [4], we found five brown dwarfs withhighly polarized integrated emission. These sources serve
as direct evidence of (compact) circumstellar structurearound young brown dwarfs.
We investigated the magnetic field structure of

NAGASHIMA, Chie

57

(Kyoto University)-1° 58′NAGAYAMA, Takahiro, NAGATA, Tetsuya		

5h 42m 00s

41m 55s

50

45

40

35

30

R.A. (J2000)

Figure 2: Three color composite of JHKs polarized intensity (PI)images. Newly found five small IRNe are enclosed
by circles. A nebula enclosed by broken line is thepreviously known IRN associated with the source FIR 4.
The image is in logarithmic scale.
References[1] Kandori, R., et al.: 2007, PASJ, 59, 487.
[2] Kandori, R., et al.: 2006, SPIE, 6269, 159.
[3] Nagayama, T., et al.: 2003, SPIE, 4841, 459.
[4] Levine, J., et al.: 2006, ApJ, 646, 1215.
[5] Dotson, J. L., et al.: 2000, ApJS, 128, 335.
[6] Matthews, B. C., et al.: 2002, ApJ, 569, 304.

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Water Maser and Ammonia Survey toward IRAS Sourcesin the Galaxy. : H2O Maser Data
SUNADA, Kazuyoshi, NAKAZATO, Takeshi(NAOJ)								(Tokyo Institute of Technology)		

HONGO, Satoshi

I Scientific Highlights(ISAS / JAXA)YANG, Ji

(PMO, China)

and 06053-0622, we succeeded in spatially separating
multiple velocity components.
Details of the obsered sources, the maser spectraof the new sources, and the line parameters of all thedetected sources are described in [6].

Flux Density [Jy]We have completed a sensitive survey of IRAS
sources in the H2O maser and NH3 emission with theNobeyama 45 m telescope.
The H2O masers are believed to be one of the best
tracers to investigate the earliest phases of low- tohighmass star formation. In addition, the NH3 emission
is another good tracer to investigate the earliest phases oflow- to high-mass star formation. They often trace dense
cores with sizes of ~0.1 pc, which are thought to be thesites of star formation [1]. Consequently, our combined
survey of H2O maser and NH3 emission is most likely
to provide a useful database to reveal the earliest phasesof star formation. The other goal of our study is toinvestigate the excitation conditions of the H2O masers
and its relation to the evolution phase of the YSOs. An
additional goal of our survey is to detect new H2O maser
sources and to increase the number of known masers.
Our target sources mainly consist of the cold IRAS
point sources with strong CO emission cataloguedby [2]. They selected the YSO candidates with color
indices of log(F12/F25) ≤ −0.4, and log(F25/F60) ≤ −0.4 or log(F12/F60) ≤ −0.4 from the IRAS point source
catalogue, and carried out a CO(1–0) survey toward them.
They made a catalogue of 1331 YSOs with the significant
CO emission. Furthermore, we picked up other YSO
candidates from the catalogues of outflow sources [3],embedded clusters [4], and low-mass stars [5]. Finally,
we selected 1563 sources for our survey.
This survey has a 1σ noise level as small as 0.24
Jy, resulting in one of the most sensitive water maser
surveys. The maximum distance of the masers to be
detected by our survey is estimated to be 3 kpc for thesources with Fν,1kpc < 10 Jy and 10 kpc for 10 Jy ≤ Fν,1kpc< 100 Jy, where Fν,1kpc is the maser flux density converted
at the distance of 1 kpc. For the strong masers with Fν,1kpc≥ 100 Jy, our survey can detect all the sources in the
Galaxy.
We carried out a total of 2229 observations toward
1563 sources and detected water maser emission toward
222 sources. Our survey newly found the masers from75 of the 222 sources. Among these 75 masers, two areassociated with the low-mass stars L1551 IRS 5 (Fig.1)
and IRS 43. Furthermore, we discovered an extreme highvelocity component with VLSR = −146 km s−1 toward thewell known source, NGC 7538 IRS 11. For the threesources of NGC 1333 IRAS 4A/B, IRAS 05329-0512,

036

IKEDA, Norio, KITAMURA, Yoshimi

			

60
40
20
0
-20

-10

0
10
Velocity [km s-1]

20

Figure 1: New H2O maser emission from L1551 IRS 5.

References[1] Myers, P. C., Benson, P. J.: 1983, ApJ, 266, 309.
[2] Yang, J., et al.: 2002, ApJS, 141, 157.
[3] Wu, Y., et al.: 1996, A&AS, 115, 283.
[4] Lada, C. J., Lada, E. A.: 2003, ARA&A, 41, 57.
[5] Furuya, R., et al.: 2003, ApJS, 144, 71.
[6] Sunada, K., et al.: 2007, PASJ, 59, 1185.

30

Characteristics of Anemone Active Regions Appearing in Coronal Holes
Observed with the Yohkoh Soft X-Ray Telescope
ASAI, Ayumi(NAOJ)SHIBATA, Kazunari(Kyoto University)

HARA, Hirohisa

Among many findings achieved by the Soft X-ray
Telescope (SXT) aboard Yohkoh, one of the interesting
discoveries is “sea-anemone” like structure. This phenomenon is characterized by radially aligned coronalloops as shown in Fig. 1a. These active regions (ARs)are thought to often appear in coronal holes (CHs) thatconsist of global open magnetic field, and they arecalled anemone ARs [1]. The situation of the magnetic
reconnection between the emerging flux and thesurrounding field in forming an anemone AR is suitableto generate Xray jets, and indeed, many associatedjets have been observed. Attentions to the relation
between anemone ARs and fast solar winds have also
been paid, and therefore, the understandings physicaland morphological characteristics of anemone ARs areimportant for space weather studies. However, howfrequently such an asymmetric magnetic configuration
occurs in CHs, and the features have not been wellunderstood.
We statistically examined the features of anemone
ARs observed by Yohkoh/SXT [2]. First, we surveyed
49 ARs whose births were observed with SXT from1991 November to 1992 May, and found; (1) About oneforth of all newly emerged ARs were anemone ARs.
Moreover, almost all anemone ARs appeared withinCHs, and the ARs that appeared in quiet regions did
not show anemone structure. We also confirmed that
anemone ARs usually generate X-ray jets. Next, we
examined 28 anemone ARs observed between 1991
November and 1993 March, and found the following
features; (2) About 71 % of all anemone ARs appeared in
the northern hemisphere, while the sunspot number waslarger in the southern hemisphere, in this period. Thismeans that the number of anemone ARs has a feature of
the anti-solar activity. Furthermore, almost all anemone
ARs were not located on or near the global neutral line
where active longitudes were situated, (3) Among theanemone ARs in the northern hemisphere, about 80% had the characteristics that magnetic polarity of thepreceding spots was negative, which is consistent with
the Hale-Nicholson’s polarity law. It is opposite to that ofsurrounding CHs, since almost all the surrounding CHs
in the northern hemisphere had the positive magnetic
polarity during this period. (4) Anemone ARs showed
more or less following-preceding (east-west) asymmetryin SXR intensity distribution. The features (1), (2),and (3) suggest that the anemone ARs have simpler(less sheared) magnetic structure than other ARs. The“anemone” shape itself shows a potential like magnetic(NAOJ)NITTA, Nariaki V.

(Lockheed Martin Solar and Astrophysics Lab.)

configuration, that is, the lowest energy state. This is also
consistent with the facts that α- β-type spots, which areless active ARs, are observed at the center of anemone
ARs. Moreover, the observed anemone ARs showed thepreceding-spotdominant magnetic structure clearer thanthose appearing in other regions. The feature (4) showedthat the following-preceding asymmetry in SXR intensity
distribution depends on the order of the magnetic
polarities of anemone ARs and CH.
More detailed examinations of anemone ARs andstructure of the emerging fluxes, by using data that havehigher spatial resolution and sensitivity are required toanswer these questions. For example X-Ray Telescope on
board Hinode have observed many similar (and smaller)
features, and analyzing them will be appropriate.

SXT X-Ray 1992-Jan-10 21:43 UT(nega)

Kitt Peak 1992-Jan-09 18:38 UT
-300

(a)

150"

-150

0

150

300 [G](b)

Figure 1: Typical example of the anemone AR observed on 1992
January 10 (NOAA AR 7001). (a) SXR image takenwith the Yohkoh SXT. (b) Magnetogram taken at Kitt
Peak.

References[1] Shibata, K., et al.: 1994, ApJ, 431, L51.
[2] Asai, A., et al.: 2008, ApJ, 673, 1188.

I Scientific Highlights

037

Discovery of a Scattering Disk around the Low-Mass T Tauri StarFN Tauri
KUDO, Tomoyuki(Graduate University for Advanced Studies)

TAMURA, Motohide(NAOJ)			

HAYASHI, Masahiko, KOKUBO, Eiichiro		(NAOJ)			

ITOH, Yoichi(Kobe University)
		

FUKAGAWA, Misato

MAYAMA, Satoshi(NAOJ)		

OASA, Yumiko

References[1] Muzerolle, J., et al.: 2003, ApJ, 592, 266.
[2] Kudo, T., et al.: 2008, ApJ, 673, L67.
[3] Kokubo, E., Ida, S.: 2002, ApJ, 581, 666.

038

I Scientific Highlights

HAYASHI, Saeko, ISHII, Miki
(NAOJ)MOMOSE, Munetake(Ibaraki University)

PYO, Tae-Soo, SUTO, Hiroshi(Kobe University)		

Investigation of protoplanetary disks is importantto understand the origin of the Earth and our solar
system. In particular, direct imaging of circumstellar
disks provides hard-and-fast proof of its existence andenables us to derive properties such as radius, inclination,and the surface brightness distribution. However, thenumber of resolved disks around T Tauri star is notlarge enough to discuss the morphological diversity andevolutionary sequence. Therefore, we have conducted
deep coronagraphic imaging of T Tauri stars using theCoronagraphic Imager (CIAO) with the adaptive optics
system (AO) on the Subaru telescope.
FN Tau is classified as a single, classical T Tauri starwith a spectral type of M5. This star is associated with
the Taurus molecular cloud at a distance of ~140 pc. The
stellar mass is estimated to be ~0.1 M [1].
We have discovered an optically thick disk as far as~260 AU from the central star (Fig. 1) [2]. The surface
brightness of disk decreases as a power-law of r −2.5,
suggesting that the disk is flared. The disk morphology
appears to be relatively featureless except for anazimuthal asymmetry in the surface brightness, indicatingthat the disk is not perfectly face-on but is slightly tilted.
The disk mass, derived from a simple disk emission
model with previous photometry at optical to millimeter
wavelengths, is ~0.007 M, 6 % of the mass of the central
star (Fig. 2).
FN Tau disk has sufficient mass to produce several
Jupiter-mass planet. However, the predicted surface
density distribution seems to be too small [3]. The final
mass of possible proto-planet is estimated to be ~1 Earthmass. Our result is a first direct imaging of disks aroundM type T Tauri stars. . The FN Tau disk is one of the best
targets for disk and planet formation studies around M
stars.

(JAXA)(Nagoya University)			

(Graduate University for Advanced Studies)

MORINO, Jun-ichi

KITAMURA, Yoshimi(NAOJ)

Figure 1: H-band (1.65 μm) coronagraphic image of FN Tau disk.
Diameter of the occulting mask is 0.8 arcsec. The crossmark indicates the stellar position. The directions of the
spider patterns are indicated by white dash lines.

Figure 2: Spectral energy distribution (circles) and its disk model
for FN Tau. The dashed line is a blackbody for thecentral star (3240 K). The solid line is sum of the stellar
and disk fluxes.

Supernova Nucleosynthesis and Neutrino Oscillation
with Improved Reaction Rates
YOSHIDA, Takashi

HIGASHIYAMA, Koji

(NAOJ)(Chiba Institute of Technology)

KAJINO, Toshitaka

OTSUKA, Takaharu(NAOJ / University of Tokyo)

true for the calculated results for the 56Ni (νe, e−) 56Cu
reaction cross sections.
Branching ratios to neutron, proton and α-particle
knock-out reactions were calculated in the HauserFeshbach theory. Protons are mainly emitted after the(νe, e−) processes while neutron emission is the dominantchannel for the 56Fe (ν–e, e+) 56Mn reaction. For the (ν–e,e+) reaction, calculated B(GT) value, 2.9 for the GXPF1J
Hamiltonian, is close to the experimental value of 2.8± 0.3 [8]. We find that neutron emission cross sections
increase as the neutron excess gets larger for the (νe, e−)reactions. We expect more neutrons emitted from theneutron-rich nuclei for the improved new Hamiltonian,
GXPF1, compared to conventional ones. Extended study
on the roles of these neutrons in the SN nucleosysnthesis
is now underway.
56

dσ/dE (x10-41cm 2 /MeV)

8

Fe (ν, e- ) Co
56

DAR

GXPF1J

6

GT
IAS

4

2

0

0

5

10

15

20

E x(MeV)Figure 1: Calculated reaction cross sections for 56Fe (νe, e−) 56Co
induced by DAR neutrinos.
10

2

10

1

10

0

56

2

Quantum states of three-flavor neutrinos admix
with one another, which induces flavor oscillation.
Mixing angle θ13 and mass hierarchy are still unknown
among neutrino oscillation parameters. Our proposed
astronomical method to determine these unknown
parameters is to make use of the neutrino matter effect(MSW effect) on the abundance ratio of the elements like7
Li/11B produced in supernova (SN) nucleosynthesis [1,2].
Absolute yields however depend strongly on the
Hamiltonians which were used in the theoretical
calculations of the neutrino-induced reaction crosssections in this method. Based on the recent advances innuclear shell model calculations in p-shell and fp-shell
nuclei, we studied neutrino reactions on 12C and 4He as
well as Fe and Ni isotopes quantum mechanically [1].
The charge-exchange reaction cross sections based on
new shell model Hamiltonians are found to be enhanced
compared with previous calculations. It was also foundthat more neutrons are knocked-out by SN neutrinos
from more neutron-rich Ni isotopes. We clarified thatthe Hamiltonian dependence of the cross sections offsets
each other by taking the abundance ratio 7Li/11B. Our
proposed astronomical method to determine the unknown
neutrino oscillation parameters thus turns out to be a very
precise one [1, 3].
In the fp-shell, recently proposed shell model Hamiltonian (GXPF1 [4]) leads to a good description of heavy
mass nuclei. We show calculated results of the DAR(decay-at-rest) neutrino-induced reaction 56Fe (νe, e−)56
Co in Fig. 1. They include both GT (Gamow-Tellar)
and IAS (isobaric analog state) transitions. The GT
strength distribution in 58Ni is very well reproduced with
the GXPF1J Hamiltonian. Calculated cross section for
the GT and IAS transitions for GXPF1J is σ = 2.29 ×
10−40 cm2 while the experimental value obtained by the
KARMEN collaborations [5] is σ = 2.56 ± 1.08 ± 0.43 ×
10−40 cm2 [6], that includes also the contributions fromthe spin-dipole transitions.
We also investigated the 56Fe (νe, e−) 56Co reaction
induced by the SN neutrinos. Calculated results of the
GT transitions for the GXPF1J Hamiltonian are shownin Fig. 2 for the neutrino temperature of T = 2~12 MeV,
comparing with previous calculations [6, 7]. The present
results, which include contributions other than the GTtransition, would get larger than those of ref. [6] for T ≤8 MeV but still smaller than those of ref. [7]. This is also

(University of Tokyo)

cm )(University of Aizu)		

(JAEA)		

-41

HONMA, Michio

CHIBA, Satoshi

σ (10SUZUKI, Toshio(Nihon University / NAOJ)

10

Fe (ν, e- ) 56Co

present(GT : Honma et al.)Wooskey et al.
Kolbe-Langanke

-1

2

4

6

8

10

T (MeV)

12

Figure 2: The same as in Fig. 1 for supernova neutrinos withtemperature T.
References[1] Suzuki, T., et al.: 2007, PPNP, 59, 486.
[2] Yoshida, T., et al.: 2008, ApJ, 686, 448.
[3] Suzuki, T., et al.: 2006, PRC, 74, 034307.
[4] Honma, M., et al.: 2002, PRC, 65, 061301.
[5] Rapaport, J., et al.: 1981, PRC, 24, 335.
[6] Woosley, S. E., et al.: 1990, ApJ, 356, 272.
[7] Kolbe, E., et al.: 2000, PRC, 63, 025802.
[8] Caurier, E., et al.: 1999, NPA, 653, 439.

I Scientific Highlights

039

Transient horizontal magnetic fields in solar plage regions
ISHIKAWA, Ryohko(University of Tokyo / NAOJ)TSUNETA, Saku, ICHIMOTO, Kiyoshi, KATSUKAWA, Yukio, SUEMATSU, Yoshinori(NAOJ)

		

ISOBE, Hiroaki(University of Tokyo)		

NAGATA, Shin’ichi(Kwasan and Hida Observatories, Kyoto University)
		

I Scientific Highlights

SHIMIZU, Toshifumi(Institute of Space and Astronautical Science, JAXA)SHINE, Richard A., TARBELL, Theodore D., TITLE, Alan M.
(Lockheed Martin Solar and Astrophysics Laboratory)

Magnetic fields on the Sun appear to be essentiallyvertical in the quiet Sun and in active regions due tobuoyancy, (Exceptions are penumbra and emerging flux
region.), and the classical concept about solar magnetic
fields was dominated by sub-arcsecond vertical kG
magnetic flux tubes as well as sunspots and pores.
However, the Solar Optical Telescope aboard Hinodecompletely change the paradigm that the quiet Sun isdominated by vertical magnetic fields; Hinode discovered
prevalent existence of small-scale horizontal hG magnetic
fields in the quiet Sun at unprecedented small scales [1, 2,
3].
Our Spectro-polarimetric observations reveal
widespread occurrence of transient, spatially isolated
horizontal magnetic fields in a plage region as well as in
the quiet Sun [4]. Figure 1 shows an example of them.
These events are not associated with existing long-lived
magnetic fields forming the active region, and appear
in a region of insignificant vertical fields. A remarkablefeature is that the horizontal magnetic structure first
appears inside the (bright) granule, subsequently moves
to the (dark) inter-granular lane, and finally disappears in
the inter-granular lane. The horizontal magnetic structure
continues to be smaller than or at most as large as the sizeof the granule where it appears. These transient horizontal
magnetic fields which we detect are granular-sized (~1″),
and transient with a lifetime less than ~10 minutes,
which are comparable to the lifetime of granules. The
lifetime, the size, and the Stokes profiles show that thesehorizontal magnetic fields are tossed about by granularmotion. These properties are in contrast to those of
the more well-known emergence driven by magnetic
buoyancy, which we also report in this paper (See [4]for more details.). Our finding suggests that the granularconvection in the plage regions is characterized by a highrate of occurrence of granular-sized transient horizontal
fields.
These ubiquitous transient horizontal fields raise two
curious questions. One is about their origin; they may
come from the local vertical fields and/or the global
magnetic fields or they may be generated by a local

040

LITES, Bruce W.

(High Altitude Observatory)

dynamo process. Another one is about their influenceon chromosphere and corona; do horizontal magnetic
fields which dominate the Sun on the photosphere haveany consequence on upper atmosphere? These transienthorizontal fields would provide new insights on solar
daynamo process and chromospheric and/or coronalheating.
Δt= 0 s

68 s

136 s

204 s

272 s 340 s

408 s

476 s

1.0

2.5 arcsec

(a)
(b)
(c)
(a)

-1.5

0
(%)

1.5

(b)

0

0.3
(%)

0.6

(c)

0.7

Figure 1: The evolution of physical quantities of transienthorizontal fields for the plage region: (a) CP (verticalmagnetic field), (b) LP (horizontal magnetic field), (c)Ic. The region where LP is larger than 0.3% is enclosed
by red lines.
References[1] Centeno, R., et al.: 2007, ApJ, 666, L137.
[2] Lites, B. W., et al.: 2008, ApJ, 672, 1237.
[3] Orozco Suárez, D., et al.: 2007, ApJ, 670, L61.
[4] Ishikawa, R., et al.: 2008, A&A, 481, L25.

Direct and semi-direct neutron capture of neutron-rich Tin isotopes
and its implications for the r-process nucleosynthesis
CHIBA, Satoshi, KOURA, Hiroyuki, HAYAKAWA, Taketo, MARUYAMA, Toshiki(JAEA)KAWANO, Toshihiko

KAJINO, Toshitaka(LANL)			

The neutron capture reaction rates on neutronrich unstable isotopes far from the β-stability line are
essential for understanding the rapid neutron capture
nucleosynthesis (r-process), considered to occur insupernova explosions. The neutron magic numbers
N = 50, 82, 126 etc. affect the final mass distributionof products in the r-process, where the capture crosssections have minima. As a matter of fact, astronomical
observations of metal-deficient stars reported a“universal” abundance distribution of the r-nuclei in acertain mass region but that relative abundances between
different mass regions separated by the neutron magic
number N = 82 are different [1]. Therefore, an unstabledouble-magic nucleus 132Sn (N = 82) takes the key forunderstanding the r-process.
We carry out a systematic calculation of both direct
and semi-direct (DSD) cross sections to improve theprediction of the neutron capture reaction rates of
the Tin isotopes. A single-particle potential (SPP) is
adopted which gives a good reproduction of the known
singleparticle energies over a wide mass region, namely
the Koura-Yamada potential (KY-SPP) [2]. We also
perform Hauser-Feshbach (HF) model calculations andinvestigate whether the inversion of the HF and directcross sections occurs or not at the neutron-rich isotopes[3].
The levels calculated by KY-SPP exhibit somewhat
narrow gap at N = 82 compared to an experimental value,
but the single-particle energies of the unfilled levels are
reproduced with an accuracy of about 300 keV on the
average. It is especially important to predict the energy
and presence of 3p3/2 and 3p1/2 states that can couple tothe s-wave of the incoming scattering wave, that gives adominant contribution to the low-energy direct capture
cross section relevant to the r-process.
The DSD and HF neutron capture cross sections
are calculated for a series of even-even Tin isotopes at
30 keV, which are shown in the Figure 1. The HF crosssection decreases as the mass number increases, andshows a drastic decrease when going from 130Sn to 132Sn.
This trend is correlated with a change in the neutron
separation energies. On the other hand, the DSD crosssection decreases only modestly, and it exceeds the HF
cross section at 132Sn and beyond. Therefore, we see thatthe inversion of the HF and DSD cross section indeed
occurs at the border of the N = 82 magic for the neutronrich Tin isotopes (and probably its vicinity). The gradual(NAOJ)

decrease of the DSD cross sections in our calculation isdifferent from a more-rapid mass-number dependence ofthe direct capture cross section calculated by Rauscher et
al. [4] due, probably, to the stability of the single-particle
energies calculated with KY-SPP. The cross symbol
denotes a result calculated by Rauscher et al. [4] by using
experimental level energies as their best estimate of thedirect (n, γ) cross section of 132Sn. Our result, without
adjustment, is in a fair agreement with this value.
The r-process abundance of 132Sn isotope is calculatedwith the HF (n, γ) rate alone and both the HF + DSD
rates. We notice that the difference in these reaction rate
gives rise to a difference of more than a factor of 3 in theinitial abundance of 132Sn, but the difference diminishes
as time passes, indicating a presence of unknown mechanism that brings about universality.

Cross section (mb)				(n,γ ) cross sections of Sn isotopes

101

at 30 keV

100
10−1
10−2

DSD
HF
Rauscher et al.

125

130
A

135

Figure 1: Calculated DSD and HF cross sections for a series ofeven-even Tin isotopes at 30 keV.
References[1] Sneden, C., et al: 2000, AJ, 533, L139.
[2] Koura, H., Yamada, Y.: 2000, Nucl. Phys. A, 671, 96.
[3] Chiba, S., et al: 2008, Phys. Rev. C, 77, 015809.
[4] Rauscher, T., et al: 1998, Phys. Rev. C, 57, 2031.

I Scientific Highlights041

Effects of primordial magnetic field and background gravitational wave
on low and high multipoles of the cosmic microwave background
				
			

YAMAZAKI, Dai G.

(NAOJ)		

KAJINO, Toshitaka(NAOJ / University of Tokyo)

Magnetic fields in clusters of galaxies have been
observed with a strength of 0.1–1.0 μG. The existenceof a primordial magnetic field (PMF) of order 1 nG
whose field lines collapse as structure forms is one
possible explanation for such magnetic fields ingalactic clusters. The origin and detection of the PMF
is, hence, a subject of considerable interest in modern
cosmology. Moreover, the PMF could influence avariety of phenomena in the early universe such as thecosmic microwave background (CMB) [1, 2, 3], or thematter density field [4]. Temperature and polarization
anisotropies in the CMB provide very precise informationon the physical processes in operation during the early
universe. Recent experiments, however, has indicateda potential discrepancy between these observations at
higher multipoles l ≥ 2000 and the best-fit cosmologicalmodel. This discrepancy is difficult to account for by asimple retuning of cosmological parameters or by the
Sunyev-Zeldovich effect. The PMF provides a plausible
explanation for such the possible disparity between
observations and theoretical fits to the CMB power
spectrum [1, 2, 3]. Here we report on calculations of thenumerical CMB polarization anisotropies from the PMF.
We then deduce a precise estimate of the PMF effect on a
BB mode of perturbations.
The introduction of the PMF leads to a better fit to
the CMB power spectrum for the higher multipoles, andthe fit at lowest multipoles can be used to constrain thecorrelation of the PMF with the density fluctuations forlarge negative values of the spectral index. Our prediction
for the BB mode for the PMF average field strength |Bλ|
= 4.0 nG is consistent with the upper limit on the BB
mode deduced from the latest CMB observations. We
find that the BB mode is dominated by the vector modeof the PMF for higher multipoles and by a gravitationalwave background (GWB) for lower muotipoles (Fig. 1).
We also show that by fitting the complete power
spectrum one can break the degeneracy between the PMF
amplitude and its power spectral index. Furthermore,
there is no discrepancy at higher l between observations
and theories of the CMB polarization for models with the
PMF. We also show clearly that the power spectral index
of the PMF, nB, is effectively constrained from CMB
observations for higher l. The models with higher nB give
better fits to the observations than those with lower nB for
the lower l regions of the BB modes [3].
The PMF affects the formation of large scale structure.

042

I Scientific Highlights

ICHIKI, Kiyotomo(University of Tokyo)

MATHEWS, Grant J.

(University of Notre Dame)

For example, magnetic pressure delays the gravitational
collapse. It is thus very important to constrain the PMF as
precisely as possible. If we combine our study and futureplans to observe the CMB anisotropies and polarizations
for higher multipoles l, e.g. via the Planck, QUIET, andPolarBear we will be able to constrain the PMF moreaccurately, and explain the evolution and generation of
the magnetic field on galaxy cluster scales along with theformation of the LSS.

Figure 1: CMB polarization anisotropies (BB mode) from the
PMF . This figure shows a comparison of the computed
total power spectrum with the observed CMB spectrum
for models with Bλ = 4.0 nG and nB = −2.5. All Lines in
the figure are plotted in the absolute value. Downward
arrows for the error bars indicate that the data points are
positive and the lower error negative. Green and grayareas show the PMF and the GWB dominant areas.
References[1] Yamazaki, D. G., Ichiki, K., Kajino, T.: 2005, ApJ, 625, L1.
[2] Yamazaki, D. G., et al.: 2006, ApJ, 646, 719.
[3] Yamazaki, D. G., et al.: 2008, Phys. Rev. D, 77, 043005.
[4] Yamazaki, D. G., et al.: 2006, Phys. Rev. D, 74, 123518.

Simultaneous Solution to the Big-Bang Li Problems
from a Long-lived Negatively Charged Particle
			

KUSAKABE, Motohiko(University of Tokyo / NAOJ)

BOYD, Richard N.

(Lawrence Livermore National Laboratory / NAOJ)YOSHIDA, Takashi

Recent spectroscopic observations of metal poor
halo stars (MPHSs) have indicated that both 7Li and 6Li
have abundance plateaus with respect to the metallicity.
Abundances of 7Li are about a factor of three lower
and those of 6Li are about 1000 times higher than theprimordial abundances predicted by standard big-bang
nucleosynthesis (SBBN). 6Li, therefore, might haveanother cosmological or Galactic origin than the SBBN.
We calculated big-bang nucleosynthesis (BBN)
assuming existence of a negatively-charged massive
particle X − in the early universe that binds to the lightnuclei A produced in BBN and makes bound states AX,
but would have decayed long before it could be detected[1, 2]. We found that the 7BeX (p, γ) reaction throughthe atomic ground state 8BX between a X − particle anda 1+, E* = 0.770 MeV nuclear excited state of 8B could
possibly contribute to destruction of 7BeX [1]. But weconcluded that this channel would not be important fromthe estimate of realistic binding energies of AX [2]. We
integrated Boltzmann equations including terms for therecombination and ionization of X − particles by normal
and X-bound nuclides as well as many possible nuclear
reactions among them. Parameters are the life time τX andthe abundance ratio of X − to baryon YX ≡ nX /nb.
We perform the BBN calculation in which X −particles are included at 10 % of the total baryon number,i.e., YX = 0.1 (Fig. 1). The decay of X − is not considered,corresponding to the case of τX = ∞. The recombinations
occur at temperature of T9 ≡ T/(109K) ~ 0.3 for 7Li andT9 ~ 0.5 for 7Be. 7BeX abundance increases accordingly.
At T 9 ~ 0.1, the X − particles are captured onto 4He.
The reaction 4HeX(d, X −) [3], then, produces 6Li. 7Be is
destroyed by the nuclear reaction after the recombination(T 9 ~ 0.3), i.e., 7Be(X −, γ) 7Be X(p, γ) 8B X [4]. Figure 2
shows Li abundances relative to the observed values, i.e.,d(ALi) = ALiCalc/ALiObs in the YX vs. τX plane. We find asimultaneous solution to both of the 7Li overproduction
problem and the 6Li underproduction problem in theparameter region of YX ≥ 0.2 and τX ~ (1–3) × 103 s.

References[1] Kusakabe, M., et al.: 2007, PRD, 76, 121302.
[2] Kusakabe, M., et al.: 2008, ApJ, 680, 846.
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KAJINO, Toshitaka(NAOJ / University of Tokyo)(NAOJ)		

MATHEWS, Grant J.

(University of Notre Dame)

Figure 1: Abundances of normal nuclides (a) and X-boundnuclides (b) as a function of T9. The parameters are set
to be YX = 0.1 and τX = ∞. This figure is reprinted from[2].

Figure 2: Contours of constant lithium abundances relative to thevalues observed in MPHSs, i.e., d(6Li) = 6LiCalc/6LiObs(solid curves) and d(7Li) =7LiCalc/7LiObs (dashed curves).
In the gray region, the condition d( 6Li) > d( 7Li) is
satisfied. This figure is reprinted from [2].

I Scientific Highlights

043

II Publications, Presentations
1. Refereed Publications
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2007, Upper limits on gravitational wave emission
from 78 radio pulsars, PhReD, 76, 042001.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2007, Search for gravitational wave radiation associated with the pulsating tail of the SGR 1806-20 hyperflare of 27
December 2004 using LIGO, PhReD, 76, 062003.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2007, First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds, PhReD, 76, 022001.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2007, Searches for periodic gravitational waves fromunknown isolated sources and Scorpius X-1: Results from thesecond LIGO science run, PhReD, 76, 082001.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2007, Upper limit map of a background of gravitational waves, PhReD, 76, 082003.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2007, Search for gravitational-wave bursts in LIGO
data from the fourth science run, CQGra, 24, 5343–5369.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2008, All-sky search for periodic gravitational waves
in LIGO S4 data, PhReD, 77, 022001.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2008, Search for gravitational waves from binary inspirals in S3 and S4 LIGO data, PhReD, 77, 062002.
Abbott, B., et al. including Kawamura, S., Kawazoe, F.,
Kokeyama, K., Leonhardt, V., Nishizawa, A., Sakata, S.,
Sato, S.: 2008, Search for gravitational waves associated with
39 gamma-ray bursts using data from the second, third, andfourth LIGO runs, PhReD, 77, 062004.
Abe, S., Ebizuka, N., Yano, H., Watanabe, J., Borovička, J.: 2007,
Search for OH(A X) and detection of N2+(B X) in ultraviolet
meteor spectrum, AdSpR, 39, 538–543.
Adelman-McCarthy, J. K., et al. including Ichikawa, S.-I.: 2007,
The Fifth Data Release of the Sloan Digital Sky Survey, ApJS,
172, 634–644.
Akiyama, M., Minowa, Y., Kobayashi, N., Ohta, K., Ando, M.,
Iwata, I.: 2008, Adaptive Optics Rest-Frame V-Band Imagingof Lyman Break Galaxies at z~3: High Surface Density Disklike
Galaxies?, ApJS, 673, 1–28.

044

II Publications, Presentations

Ando, H., Tan, K., Kambe, E., Sato, B., Zhao, G.: 2008, Detection of Small-Amplitude Oscillations in the G-Giant HD76294(ζHydrae), PASJ, 60, 219–222.
Ando, M., Ohta, K., Iwata, I., Akiyama, M., Aoki, K., Tamura,N.: 2007, Lyman Break Galaxies at z~5: Rest-Frame UV Spectra. II, PASJ, 59, 717.
Aoki, W., Honda, S., Beers, T. C., Takada-Hidai, M., Iwamoto, N.,
Tominaga, N., Umeda, H., Nomoto, K., Norris, J. E.,
Ryan, S. G.: 2007, Spectroscopic Studies of Extremely Metalpoor Stars with the Subaru High-Dispersion Spectrograph. IV.
The α-Element-Enhanced Metal-poor Star BS 16934-002, ApJ,
660, 747–761.
Aoki, W., Honda, S., Sadakane, K., Arimoto, N.: 2007, First Determination of the Actinide Thorium Abundance for a Red Giantof the Ursa Minor Dwarf Galaxy, PASJ, 59, L15–L19.
Arimoto, M., et al. including Shirasaki, Y.: 2007, HETE-2 Observations of the X-Ray Flash XRF 040916, PASJ, 59, 695–702.
Arnaboldi, M., Gerhard, O., Okamura, S., Kashikawa, N., Yasuda,N., Freeman, K. C.: 2007, Multi-Slit Imaging Spectroscopy
Technique: Catalog of Intracluster Planetary Nebulae in the
Coma Cluster, PASJ, 59, 419–425.
Asada, K., Inoue, M., Kameno, S., Nagai, H.: 2008, Time Variation of the Rotation Measure Gradient in the 3C 273 Jet, ApJ,
675, 79.
Asai, A., Nakajima, H., Oka, M., Nishida, K., Tanaka, Y.: 2007,
Loop top nonthermal emission sources associated with an overthe-limb flare observed with NoRH and RHESSI, AdSpR, 39,
1398–1401.
Asai, A., Shibata, K., Hara, H., Nitta, N. V.: 2008, Characteristics of Anemone Active Regions Appearing in Coronal Holes
Observed with Yohkoh Soft X-Ray Telescope, ApJ, 673, 1188–
1193.
Asaki, Y., Sudou, H., Kono, Y., Doi, A., Dodson, R., Pradel, N.,
Murata, Y., Mochizuki, N., Edwards, P. G., Sasao, T., Fomalont,E. B.: 2007, Verification of the Effectiveness of VSOP-2 Phase
Referencing with a Newly Developed Simulation Tool, ARIS,
PASJ, 59, 397.
Asano, K., Inoue, S.: 2007, Prompt GeV-TeV Emission ofGamma-Ray Bursts Due to High-Energy Protons, Muons, andElectron-Positron Pairs, ApJ, 671, 645–655.
Aulanier, G., Golub, L., DeLuca, E. E., Cirtain, J. W., Kano, R.,
Lundquist, L. L., Narukage, N., Sakao, T., Weber, M. A.: 2007,
Slipping Reconnection in Coronal Loops, Science, 318, 1588–
1591.
Bekki, K., Yahagi, H., Forbes, D.: 2007, On the origin of mass?
metallicity relations, blue tilts and scaling relations for metalpoor globular cluster systems, MNRAS, 377, 215–228.
Bekki, K., Yahagi, H., Nagashima, M., Forbes, D. A.: 2007,
Formation of the Galactic globular clusters with Herich stars in low-mass haloes virialized at high redshift,
MNRAS, 382, L87–L91.
Bellot Rubio, L. R., Tsuneta, S., Ichimoto, K., Katsukawa, Y.,

Lites, B. W., Nagata, S., Shimizu, T., Shine, R. A., Suematsu, Y.,
Tarbell, T. D., Title, A. M., del Toro Iniesta, J. C.: 2007, Vector
Spectropolarimetry of Dark-Cored Penumbral Filaments with
Hinode, ApJ, 668, L91–L94.
Berger, T. E., Shine, R. A., Slater, G. L., Tarbell, T. D., Title,
A. M., Okamoto, T. J., Ichimoto, K., Katsukawa, Y.,
Suematsu, Y., Tsuneta, S., Lites, B. W., Shimizu, T.: 2008,
Hinode SOT Observations of Solar Quiescent Prominence Dynamics, ApJL, 676, L89–L92.
Brown, C. M., Hara, H., Kamio, S., Feldman, U., Seely, J. F.,
Doschek, G. A., Mariska, J. T., Korendyke, C. M., Lang, J.,
Dere, K. P., Culhane, L., Thomas, R. J., Davila, J. M.: 2007,
Wavelength Determination for Solar Features Observed by the
EUV Imaging Spectrometer on Hinode, PASJ, 59, S865–S869.
Cai, H.-B., Shen, Z.-Q., Sudou, H., Shang, L.-L., Iguchi, S.,
Murata, Y., Taniguchi, Y., Wakamatsu, K., Takaba, H.: 2007,
Multi-epoch VLBA observations of 3C 66A, A&A, 468, 963.
Campbell, M. F., Sridharan, T. K., Beuther, H., Lacy, J. H., Hora, J.
L., Zhu, Q., Kassis, M., Saito, M., De Buizer, J. M., Fung, S. H.,
Johnson, L. C.: 2008, Mid-Infrared Photometry and Spectra ofThree High-Mass Protostellar Candidates at IRAS 18151-1208
and IRAS 20343+4129, ApJ, 673, 954.
Capak, P., et al. including Komiyama, Y., Miyazaki, S., Nagao,
T.: 2007, The First Release COSMOS Optical and Near-IR Data
and Catalog, ApJS, 172, 99–116.
Carlsson, M., Hansteen, V. H., De Pontieu, B., McIntosh, S.,
Tarbell, T., Shine, D. D., Tsuneta, S., Katsukawa, Y.,
Ichimoto, K., Suematsu, Y., Shimizu, T., Nagata, S.: 2007, Can
High Frequency Acoustic Waves Heat the Quiet Sun Chromosphere?, PASJ, 59, S663–S668.
Centeno, R., Socas-Navarro, H., Lites, B., Kubo, M., Frank, Z.,
Shine, R., Tarbell, T., Title, A., Ichimoto, K., Tsuneta, S.,
Katsukawa, Y., Suematsu, Y., Shimizu, T., Nagata, S. 2007,
Emergence of Small-Scale Magnetic Loops in the Quiet-Sun
Internetwork, ApJ, 666, L137.
Chae, J., Moon, Y.-J., Park, Y.-D., Ichimoto, K., Sakurai, T.,
Suematsu, Y., Tsuneta, S., Katsukawa, Y., Shimizu, T., Shine,
R. A., Tarbell, T. D., Title, A. M., Lites, B., Kubo, M., Nagata,
S., Yokoyama, T.: 2007, Initial Results on Line-of-Sight Field
Calibrations of SP/NFI Data Taken by SOT/Hinode, PASJ, 59,
S619–S624.
Chen, L.-J., Bhattacharjee, A., Puhl-Quinn, P. A., Yang, H., Bessho,N., Imada, S., Mühlbachler, S., Daly, P. W., Lefebvre, B.,
Khotyaintsev, Y., Vaivads, A., Fazakerley, A., Georgescu, E.:
2008, Observation of energetic electrons within magnetic islands, Nature Phys., 4, 19–23.
Chiba, S., Koura, H., Hayakawa, T., Maruyama, T., Kawano,T., Kajino, T.: 2008, Direct and semi-direct capture in low energy (n, γ) reactions of neutron-rich Tin isotopes and its implications for the r-process ucleosynthesis, PhReC, 77, 15809.
Choi, M., Tatematsu, K., Park, G., Kang, M.: 2007, Ammonia
Imaging of the Disks in the NGC 1333 IRAS 4A Protobinary
System, ApJ, 667, L183–L186.
Cirtain, J., Golub, L., Lundquist, L., van Ballegooijen, A.,
Savcheva, A., Shimojo, M., Shibata, K., DeLuca, E., Tsuneta,
S., Sakao, T., Reeves, K., Weber, M., Kano, R., Narukage,N., Shibasaki, K.: 2007, Evidence for Alfvén Waves in Solar
X-Ray Jets, Science, 318, 1580–1582.
Culhane, L., Harra, L. K., Baker, D., van Driel-Gesztelyi, L., Sun,
J., Doschek, G. A., Brooks, D. H., Lundquist, L. L., Kamio, S.,
Young, P. R., Hansteen, V. H.: 2007, Hinode EUV Study of Jets
in the Sun's South Polar Corona, PASJ, 59, S751–S756.
Culhane, J. L., et al. including Hara, H., Watanabe, T.: 2007, The
EUV Imaging Spectrometer for Hinode, SoPh, 243, 19–61.
De Pontieu, B., McIntosh, S. W., Carlsson, M., Hansteen, V.
H., Tarbell, T. D., Schrijver, C. J., Title, A. M., Shine, R. A.,
Tsuneta, S., Katsukawa, Y., Ichimoto, K., Suematsu, Y.,
Shimizu, T., Nagata, S.: 2007, Chromospheric Alfvénic Waves
Strong Enough to Power the Solar Wind, Science, 318, 1574–
1577.
Deguchi, S., Fujii, T., Ita, Y., Imai, H., Izumiura, H., Kameya,O., Matsunaga, N., Miyazaki, A., Mizutani, A., Nakada, Y.,
Nakashima, J., Winnberg, A.: 2007, An SiO Maser Search off
the Galactic Plane, PASJ, 59, 559–587.
Deguchi, S., Nakashima, J., Kwok, S., Koning, N.: 2007, Identification of Very Red Counterparts of SiO Maser and OH/IR Objects in the GLIMPSE Survey, ApJ, 664, 1130–1143.
Doi, A., et al. including Inoue, M., Nagai, H.: 2007, Japanese
VLBI Network Observations of Radio-Loud Narrow-Line Seyfert 1 Galaxies, PASJ, 59, 703.
Doschek, G. A., Mariska, J. T., Warren, H. P., Culhane, L.,
Watanabe, T., Young, P. R., Mason, H. E,. Dere, K. P.: 2007,
The Temperature and Density Structure of an Active Region
Observed with the Extreme-Ultraviolet Imaging Spectrometeron Hinode, PASJ, 59, S707–S712.
Doschek, G. A., Mariska, J. T., Warren, H. P., Brown, C. M.,
Culhane, J. L., Hara, H., Watanabe, T., Young, P. R., Mason,
H. E.: 2007, Nonthermal Velocities in Solar Active Regions Observed with the Extreme-Ultraviolet Imaging Spectrometer on
Hinode, ApJL, 667, L109.
Ebisuzaki, T., et al. including Mizumoto, Y., Inoue, S., Asano, K.,
Sugiyama, T., Watanabe, J.: 2008, The JEM-EUSO Project:
Observing Extremely High Energy Cosmic Rays and Neutrinos
from the International Space Station, NuPhS, 175, 237–240.
Endo, A., Kohno, K., Hatsukade, B., Ohta, K., Kawai, N., Sofue,
Y., Nakanishi, K., Tosaki, T., Vila-Vilaro, B., Kuno, N., Okuda, T., Muraoka, K.: 2007, A Revised Estimated of the CO(J=1–0) Emission from the Host Galaxy of GRB 030329 Using theNobeyama Millimeter Array, ApJ, 659, 1431–1437.
Endo, A., Noguchi, T., Matsunaga, T., Tamura, T.: 2007, Development of Nb/Al-AlNx/Nb SIS Tunnel Junctions for Submillimeter-Wave Mixers, EA&S, 17, 367–370.
Enya, K., Abe, L., Tanaka, S., Nakagawa, T., Haze, K., Sato, T.,
Wakayama, T.: 2008, High contrast experiment of an AO-freecoronagraph with a checkerboard pupil mask, A&A, 480, 899–
903.
Famiano, M., Boyd, R., Kajino, T., Otsuki, K., Terasawa, M.,
Mathews, G. J.: 2008, Shell model calculation of excited betadecays for r-process nucleosynthesis, J. Phys., G35, 252203.
Frebel, A., Norris, J. E., Aoki, W., Honda, S., Bessell, M. S.,
Takada-Hidai, M., Beers, T. C., Christlieb, N.: 2007, Chemical Abundance Analysis of the Extremely Metal-poor Star HE

II Publications, Presentations045

1300+0157, ApJ, 658, 534–552.
Fu, J.-N., et al. including Zhang, X.-B.: 2007, Asteroseismology of
the PG 1159 star PG 0122+200, A&A, 467, 237.
Fujii, M., Iwasawa, M., Funato, Y., Makino, J.: 2007, BRIDGE:
A Direct-tree Hybrid N-body Algorithm for Fully Self-consistent Simulations of Star Clusters and their Parent Galaxies,
PASJ, 59, 1095.
Fujita, Y., Suzuki, T., Kudoh, T., Yokoyama, T.: 2007, The Originof Ripples in Cool Cores of Galaxy Clusters: Heating by Magnetohydrodynamic Waves?, ApJ, 659, L1–L4.
Fukui, A., Abe, F., Ayani, K., Fujii, M., Iizuka, R., Itow, Y.,
Kabumoto, K., Kamiya, K., Kawabata, T., Kawanomoto, S.,
Kinugasa, K., Koff, R. A., Krajci, T., Naito, H., Nogami, D.,
Narusawa, S., Ohishi, N., Ohnishi, K., Sumi, T., Tsumuraya, F.:
2007, Observation of the First Gravitational Microlensing Eventin a Sparse Stellar Field: The Tago Event, ApJ, 670, 423–427.
Fukushima, T.: 2007, New Two-Body Regularization, AJ, 133, 1–
10.
Furusho, R., Ikeda, Y., Kinoshita, D., Ip, W.-H., Kawakita, H.,
Kasuga, T., Sato, Y., Lin, H.-C., Chang, M.-S., Lin, Z.-Y.,
Watanabe, J.: 2007, Imaging polarimetry of Comet 9P/Tempel
before and after the Deep Impact, Icarus, 190, 454–458.
Furuya, R. S., Cesaroni, R., Takahashi, S., Codella, S., Momose,M.: 2008, Candidate Rotating Toroids around High-Mass (Proto)
Stars, ApJ, 673, 363.
Fuse, T., Yamamoto, N., Kinoshita, D., Furusawa, H., Watanabe,J.: 2007, Observations of Fragments Split from Nucleus B of
Comet 73P/Schwassmann-Wachmann 3 with Subaru Telescope,
PASJ, 59, 381–386.
Fuse, T., Yoshida, F., Tholen, D., Ishiguro, M., Saito, J.: 2008,
Searching satellites of asteroid Itokawa by imaging observation
with Hayabusa spacecraft, EP&S, 60, 33–37.
Gao, L., Yoshida, N., Abel, T., Frenk, C. S., Jenkins, A., Springel,V.: 2007, The First Generation of Stars in the Λ CDM Cosmology, MNRAS, 378, 449–468.
Garavini, G., et al. including Kashikawa, N.: 2007, Quantitative
comparison between type Ia supernova spectra at low and highredshifts: a case study, A&A, 470, 411.
Gerhard, O., Arnaboldi, M., Freeman, K. C., Okamura, S.,
Kashikawa, N., Yasuda, N.: 2007, The kinematics of intracluster planetary nebulae and the on-going subcluster merger in the
Coma cluster core, A&A, 468, 815–822.
Golub, L., Deluca, E., Austin, G., Bookbinder, J., Caldwell, D.,
Cheimets, P., Cirtain, J., Cosmo, M., Reid, P., Sette, A.,
Weber, M., Sakao, T., Kano, R., Shibasaki, K., Hara, H.,
Tsuneta, S., Kumagai, K., Tamura, T., Shimojo, M.,
McCracken, J., Carpenter, J., Haight, H., Siler, R., Wright, E.,
Tucker, J., Rutledge, H., Barbera, M., Peres, G., Varisco, S.:
2007, The X-Ray Telescope (XRT) for the Hinode Mission,
SoPh, 243, 63–86.
Goossens, S., Matsumoto, K.: 2007, Lunar satellite orbit determination analysis and quality assessment from Lunar Prospector
tracking data and SELENE simulations, AdSpR, 40, 43–50.
Goossens, S., Matsumoto, K.: 2008, Lunar degree 2 potential
Love number determination from satellite tracking data, GRL,
35, L02204.

046

II Publications, Presentations

Goto, M., Kwok, S., Takami, H., Hayashi, M., Gaessler, W.,
Hayano, Y., Iye, M., Kamata, Y., Kanzawa, T., Kobayashi, N.,
Minowa, Y., Nedachi, K., Oya, S., Pyo, T.-S., SaintJacques, D., Takato, N., Terada, H., Henning, Th.: 2007,
Diffraction-Limited 3 μm Spectroscopy of IRAS 04296+3429
and IRAS 05341+0852: Spatial Extent of Hydrocarbon Dust
Emission and Dust Evolutionary Sequence, ApJ, 662, 389–394.
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T., JASMINE
Working Group: 2007, Space astrometry project JASMINE, AdSpR, 40, 664–671.
Groen, D., Portegies Zwart, S., McMillan, S., Makino, J.: 2008,
Distributed N-body simulation on the grid using dedicated hardware, NewA, 13, 348–358.
Groenewegen, M. A. T., et al. including Matsuura, M.: 2007, Luminosities and mass-loss rates of carbon stars in the Magellanic
Clouds, MNRAS, 376, 313.
Hagiwara, Y., Baan, W., Hofner, P.: 2007, HI and OH absorption
toward NGC 6240, NewAR, 51, 58.
Hagiwara, Y.: 2007, Low-Luminosity Extragalactic Water Masers
toward M82, M51, and NGC 4051, AJ, 133, 1176.
Hanaoka, Y.: 2007, A new magnetograph system for the observation of the multi-height vector magnetic field of the Sun, AdSpR,
39, 1730–1733.
Hansteen, V. H., De Pontieu, B., Carlsson, M., McIntosh, S.,
Watanabe, T., Warren, H. P., Harra, L. K., Hara, H., Tarbell,
T. D., Shine, D., Title, A. M., Schrijver, C. J., Tsuneta, S.,
Katsukawa, Y., Ichimoto, K., Suematsu, Y., Shimizu, T.:2007, On Connecting the Dynamics of the Chromosphere andTransition Region with Hinode SOT and EIS, PASJ, 59, S699–
S706.
Hara, H., Watanabe, T., Harra, L. K., Culhane, J. L., Young, P. R.,
Mariska, J. T., Doschek, G. A.: 2008, Coronal Plasma Motions
near Footpoints of Active Region Loops Revealed from Spectroscopic Observations with Hinode EIS, ApJL, 678, L67–L70.
Harra, L. K., Hara, H., Imada, S., Young, P. R., Williams, D. R.,
Sterling, A. C., Korendyke, C., Attrill, G. D. R.: 2007, Coronal
Dimming Observed with Hinode: Outflows Related to a Coronal Mass Ejection, PASJ, 59, S801–S806.
Harra, L. K., Sakao, T., Mandrini, C. H., Hara, H., Imada, S.,
Young, P. R., van Driel-Gesztelyi, L., Baker, D.: 2008, Outflows
at the Edges of Active Regions: Contribution to Solar Wind
Formation?, ApJL, 676, L147–L150.
Hasegawa, T., Arai, T., Yamaguchi, N., Sato, F.: 2008, ASTE Observations of the Massive-Star Forming Region Sgr B2: a Giant
Impact Scenario, Ap&SS, 313, 91–94.
Hashimoto, J., Tamura, M., Kandori, R., Kusakabe, N.,
Nakajima, Y., Sato, S., Nagashima, C., Kurita, M., Nagata, T.,
Nagayama, T., Hough, J. H.: 2007, Near-Infrared Polarization
Images of the Orion Molecular Cloud 1 South Region, PASJ,59, 481–486.
Hayashi, M., Shimasaku, K., Motohara, K., Yoshida, M.,
Okamura, S., Kashikawa, N.: 2007, Luminosity-Dependent
Clustering of Star-forming BzK Galaxies at Redshift 2, ApJ,
660, 72–80.
Heggie, D. C., Hut, P., Mineshige, S., Makino, J., Baumgardt, H.:
2007, The Core Radius of a Star Cluster Containing a MassiveBlack Hole, PASJ, 59, L11–14.
Higuchi, A., Kokubo, E., Kinoshita, H., Mukai, T.: 2007, Orbital
Evolution of Planetesimals due to the Galactic Tide: Formationof the Comet Cloud, AJ, 134, 1693–1706.
Hioki, T., Itoh, Y., Oasa, Y., Fukagawa, M., Kudo, T., Mayama, S.,
Funayama, H., Hayashi, M., Hayashi, S. S., Pyo, T.-S., Ishii,M., Nishikawa, T., Tamura, M.: 2007, Near-Infrared Coronagraphic Observations of the T Tauri Binary System UY Aur, AJ,
134, 880–885.
Hiramatsu, M., Hayakawa, T., Tatematsu, K., Kamegai, K.,
Onishi, T., Mizuno, A., Yamaguchi, N., Hasegawa, T.: 2007,
ASTE Submillimeter Observations of a Young Stellar Object
Condensation in Cederblad 110, ApJ, 664, 964–974.
Hirota, T., Bushimata, T., Choi, Y. K., Honma, M., Imai, H.,
Iwadate, K., Jike, T., Kameno, S., Kameya, O., Kamohara,R., Kan-Ya, Y., Kawaguchi, N., Kijima, M., Kim, M. K.,
Kobayashi, H., Kuji, S., Kurayama, T., Manabe, S.,
Maruyama, K., Matsui, M., Matsumoto, N., Miyaji, T.,
Nagayama, T., Nakagawa, A., Nakamura, K., Oh, C. S.,
Omodaka, T., Oyama, T., Sakai, S., Sasao, T., Sato, K., Sato,
M., Shibata, K. M., Shintani, M., Tamura, Y., Tsushima, M.,
Yamashita, K.: 2007, Distance to Orion KL Measured with
VERA, PASJ, 59, 897.
Hirota, T., Bushimata, T., Choi, Y. K., Honma, M., Imai, H.,
Iwadate, K., Jike, T., Kameya, O., Kamohara, R., KanYa, Y., Kawaguchi, N., Kijima, M., Kobayashi, H., Kuji, S.,
Kurayama, T., Manabe, S., Miyaji, T., Nagayama, T.,
Nakagawa, A., Oh, C. S., Omodaka, T., Oyama, T., Sakai, S.,
Sasao, T., Sato, K., Shibata, K. M., Tamura, Y., Yamashita,
K.: 2008, Astrometry of H2O Masers in Nearby Star-Forming
Regions with VERA II SVS13 in NGC1333, PASJ, 60, 37.
Honda, S., Aoki, W., Ishimaru, Y., Wanajo, S.: 2007, Neutron-Capture Elements in the Very Metal-poor Star HD 88609: AnotherStar with Excesses of Light Neutron-Capture Elements, ApJ,
666, 1189–1197.
Honma, M., Bushimata, T., Choi, Y. K., Hirota, T., Imai, H.,
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2007, Hinode Calibration for Precise Image Co-Alignment between SOT and XRT (2006 November-2007 April), PASJ, 59,
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Shimojo, M., Narukage, N., Kano, R., Sakao, T., Tsuneta, S.,
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Shiota, D., Kusano, K., Miyoshi, T., Nishikawa, N., Shibata, K.:
2008, A quantitative MHD study of the relation among arcade
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Evolution of the Sheared Magnetic Fields of Two X-Class
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Near-Infrared Polarimetry of the Eagle Nebula (M 16), PASJ,59, 507–517.
Sugiyama, K., Fujisawa, K., Doi, A., Honma, M., Kobayashi,
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Sunada, K., Nakazato, T., Ikeda, N., Hongo, S., Kitamura, Y.,
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Suzuki, T., Chiba, S., Yoshida, T., Kajino, T., Otsuka, T.: 2007,
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Takagi, T., Mortier, A. M. J., Shimasaku, K., Coppin, K., Pope, A.,
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Tanaka, M., Letip, A., Nishimaki, Y., Yamamuro, T., Motohara, K.,
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Taniguchi, Y., et al. including Nagao, T., Karoji, H., Arimoto, N.:
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Tavrov, A., Nishikawa, J., Tamura, M., Abe, L., Yokochi, K.,
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Warren, H. P., Ugarte-Urra, I., Brooks, D. H., Cirtain, J. W.,
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Yagi, M., Komiyama, Y., Yoshida, M., Furusawa, H.,
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Yamada Y., Gouda, N., Yano, T., Kobayashi, Y., Sako, N.,
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Yamamoto, K., Parkinson, D., Hamana, T., Nichol, R. C., Suto, Y.:
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Yamamuro, T., Kawabata, H., Nedachi, Ko., Nishimaki, Y.,
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Yamanoi, H., et al. including Yagi, M., Iye, M., Komiyama, Y.,
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Yamazaki, D. G., Ichiki, K., Kajino, T., Mathews, G. J.: 2008,
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Young, P. R., Del Zanna, G., Mason, H. E., Dere, K. P., Landi, E.,
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2. Publications of the National Astronomical Observatory of Japan
Ito, T., Tanikawa, K.: 2007, Trends in 20th century celestialmechanics, Publ. Nat. Astron. Obs. Japan, 9, 55–122.
Mito, H., Nakada, Y., Karoji, H., Noumaru, J., Okita, K.,
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Miyoshi, M., Kameno, S., Ishitsuka, J. K., Shen, Z.-Q., Takahashi,R., Horiuchi, S.: 2007, An Approach Detecting the Event
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Ukita, N., Ezawa, H., Ikenoue, B., Saito, M.: 2007, Thermaland Wind Effects on the Azimuth Axis Tilt of the ASTE 10-m
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3. Report of the National Astronomical Observatory ofJapan (in Japanese)
Yamada, Y., Sako, N., Hatsutori, Y., Katagishi, H., Tanaka, T.,
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Ishizaki, H.: 2007, Theoretical Consideration about the Observational Modeling of the Fast Phenomena Found with the Radio
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Yoshino, A., Yamada, Y., Nakata, F., Enoki, M., Takata, T.,
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4. Conference ProceedingsAbe, L., Guyon, O., Tamura, M., Enya, K., Tanaka, S., Matsuo, T.:2007, Status of PIAA-related Experiments and Projects, Proc.
of the Conf., In the Spirit of Bernard Lyot: The Direct Detectionof Planets and Circumstellar Disks in the 21st Century, Ed. P.
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Abe, M., et al. including Takato, N., Fujiyoshi, T., Terada, H.,
Wada, T., Ita, Y.: 2008, Ground-based Observational Campaign
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Science Conf., 1594.
Akiyama, M., Minowa, Y., Ohta, K., Ando, M., Iwata, I.,
Kobayashi, N.: 2007, Adaptive Optics Imaging Survey of
Lyman Break Galaxies at z~3, AAS Meeting 210.
Andre, P., Basu, S., Inutsuka, S.: 2008, The Formation and
Evolution of Prestellar Cores Invited review, Structure
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Aoki, K., Iwata, I., Ohta, K., Tamura, N., Ando, M., Akiyama, M.,
Kiuchi, G., Nakanishi, K.: 2007, Balmer Absorption Lines in
FeLoBALs, The Central Engine of Active Galactic Nuclei, ASP
Conf. Ser. 373, Eds. L. C. Ho, J. Wang, 337–338.
Asada, K., Inoue, M., Nagai, H., Kameno, S.: 2007, Further
Evidence of Helical Magnetic Field, The Central Engine of
Active Galactic Nuclei, ASP Conf. Ser. 373, Eds. L. C. Ho, J.
Wang, 211.
Asai, A., Yokoyama, T., Shimojo, M., Masuda, S., Shibata, K.:
2007, Evolution of Hα Kernels and Energy Release in an
X-Class Flare, New Solar Physics with Solar-B Mission, ASP
Conf. Ser. 369, Eds. K. Shibata, S. Nagata, T. Sakurai, 461–468.
Asaki, Y., Deguchi, S., Imai, H., Hachisuka, K., Miyoshi, M.,
Honma, M.: 2008, Measurements of Annual Parallaxes andProper Motions of the Red Supergiant S Per, IAU Symp. 242,
Astrophysical Masers and their Environments, Eds. J. M.
Chapman, W. A. Baan, 378–380.
Buehler, S., Ferguson, A. M. N., Irwin, M., Arimoto, N., Jablonka,
P.: 2007, Probing Stellar Populations in the Outskirts of
NGC4244, IAU Symp. 241, Stellar Populations as Building
Blocks of Galaxies, Eds. A. Vazdekis, R. F. Peletier, 321–322.
Choi, M., Tatematsu, K., Park, G., Kang, M.: 2007, NGC 1333
IRAS 4A: Twin Protostellar Disks with Vastly Dissimilar
Characters, AAS Meeting 210, #87.11.
Cirtain, J. W., Lundquist, L. L., DeLuca, E. E., Savcheva, A.,
Shimojo, M., Tsuneta, S.: 2007, The Statistics of Polar Coronal
Jets using XRT/Hinode, AAS Bulletin Vol. 39, No. 1 (AAS
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Deguchi, S., Fujii, T., Ita, Y., Izumiura, H., Kameya, O.,
Miyazaki, A., Nakada, Y., Ideta, M.: 2008, Dynamics of Stars
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Wada, F. Combes, 33–38.
Deguchi, S., Matsunaga, N., Fukushi, H.: 2007, SiO Maser
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Deguchi, S.: 2008, SiO Maser Survey of Evolved Stars in the
Galaxy: Various Environments of Maser Sources, IAU Symp.
242, Astrophysical Masers and their Environments, Eds. J. M.
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Doi, A., Fujisawa, K., Honma, M., Sugiyama, K., Murata,Y., Mochizuki, N., Isono, Y.: 2007, Japanese VLBI network
observations of 6.7-GHz methanol masers I. Array, IAU Symp.
242, Astrophysical Masers and their Environments, Eds. J. M.
Chapman, W. A. Baan, 148.
Egusa, F., Sofue, Y., Nakanishi, H., Komugi, S.: 2008,
Determination of Pattern Speed and Star Formation Timescalein Nearby Spiral Galaxies, ASS Proc. “Mapping the Galaxy and
Nearby Galaxies”, Eds. K. Wada, F. Combes, 320.
Enoki, M., Nakata, F., Yoshino, A., Yamada, Y., Yagi, M.,
Takata, T., Ichikawa, S., Ozawa, T., Horaguchi, T.: 2007, New
Features of the Subaru Telescope Science Archive System,
SMOKA, Astronomical Data Analysis Software & Systems
XVI, ASP Conf. Ser. 376, Eds. R. A. Shaw, F. Hill, D. J. Bell,213.
Enya, K., Abe, L., Tanaka, S., Nakagawa, T., Tamura, M., Kataza,H., Guyon, O.: 2007, The SPICA Coronagraph Project, Proc.
of the Conf., In the Spirit of Bernard Lyot: The Direct Detectionof Planets and Circumstellar Disks in the 21st Century, Ed. P.
Kalas.
Fukagawa, M., Itoh, Y., Oasa, Y., Kudo, T., Fujiwara, H., Tamura,M., Hayashi, M., Hayashi, S.: 2007, Near-Infrared Images of
the Disk around HD 142527, Proc. of the Conf., In the Spirit ofBernard Lyot: The Direct Detection of Planets and Circumstellar
Disks in the 21st Century, Ed. P. Kalas.
Fukushi, H., Matsunaga, N., Tanabe, T., Nakada, Y., Deguchi,
S., Ishihara, A., Kusakabe, N., Tamura, M., IRSF/SIRPOL
team: 2007, Near-IR Scattered Light in V838 Monocerotis, The
Nature of V838 Mon and its Light Echo, ASP Conf. Ser. 363,
Eds, R. L. M. Corradi, U. Munari, 181–183.
García Pérez, A. E., Inoue, S., Aoki, W., Ryan, S.: 2008, Lithium
Isotopic Abundances in Old Stars, Proc. of the ESO/Lisbon/
Aveiro Conf., Precision Spectroscopy in Astrophysics, Eds. N. C.
Santos, et al., 9–12.
Guyon, O., et al. including Iye, M., Tamura, M.: 2007, Direct
Imaging of Nearby Exoplanets with a Small Size Space
Telescope: Telescope to Observe Planetary System (TOPS),
Proc. of the Conf., In the Spirit of Bernard Lyot: The Direct
Detection of Planets and Circumstellar Disks in the 21stCentury, Ed. P. Kalas.
Hachisuka, K., Mochizuki, N., Umemoto, T.: 2008, Water Maser
Sources in the Outer Galaxy, ASS Proc. “Mapping the Galaxy
and Nearby Galaxies”, Eds. K. Wada, F. Combes, 328.
Hagino, M., Moon, Y.-J., Sakurai, T.: 2007, Skew Angle andMagnetic Helicity in Solar Active Regions, New Solar Physics
with Solar-B Mission, ASP Conf. Ser. 369, Eds. K. Shibata, S.
Nagata, T. Sakurai, 163–166.

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Hanami, H., Takagi, T., Fujishiro, N., Nakanishi, K.: 2008,
Unveiling Hidden Connection between high-z Starbursts andPresent Spheroids with Multi-Wavelength Studies, At the Edgeof the Universe: Latest Results from the Deepest Astronomical
Surveys, ASP Conf. Ser. 380, Eds. J. Afonso, H. C. Ferguson, B.
Mobasher, R. Norris, 413–416.
Handa, T., Sakano, M., Naito, S., Hiramatsu, M., Tsuboi, M.:
2008, H13CO+ and Thermal SiO Observations of G0.11-0.11; anExtremely Large Colum Density Cloud, ASS Proc. “Mapping
the Galaxy and Nearby Galaxies”, Eds. K. Wada, F. Combes,
330.
Hara, H.: 2007, Hinode: A New Solar Observatory in Space,
Plasma and Fusion Research vol. 2, 2007, Eds. K. Ida et al.,
S1008.
Hayamizu, T., Sôma, M., Herald, D.: 2008, Occultations by (90)
Antiope and by S/2000 (90) 1, CBET 1263, IAU.
Hirabayashi, H., Murata, Y., Edwards, P. G., Asaki, Y., Mochizuki,N., Inoue, M., Umemoto, T., Kameno, S., Gurvits, L. I.,
Lobanov, A. P.: 2007, Design of the Near-term Next Generation
Space-VLBI Mission VSOP-2, ESO AP Symp., 37.
Hirota, A., Kuno, N., Sato, N., Tosaki, T., Nakanishi, H., Sorai, K.:
2008, GMCs in the Nearby Galaxy IC 342, ASS Proc. “Mapping
the Galaxy and Nearby Galaxies”, Eds. K. Wada, F. Combes,
334.
Hirota, T.: 2008, Observations of H2O Maser Sources in Nearby
Molecular Clouds with VERA, ASS Proc. “Mapping the Galaxy
and Nearby Galaxies”, Eds. K. Wada, F. Combes, 335.
Hirota, T., et al.: 2007, Astrometry of H2O maser sources in nearby
molecular clouds with VERA, IAU Symp. 242, Astrophysical
Masers and their Environments, Eds. J. M. Chapman, W. A.
Baan, 158.
Honma, M., et al.: 2008, VERA Project, ASS Proc. “Mapping the
Galaxy and Nearby Galaxies”, Eds. K. Wada, F. Combes, 28.
Hori, K., Ichimoto, K., Sakurai, T.: 2007, Flare-AssociatedOscillations in Coronal Multiple-Loops Observed with the
Norikura Green-Line Imaging System, New Solar Physics
with Solar-B Mission, ASP Conf. Ser. 369, Eds. K. Shibata, S.
Nagata, T. Sakurai, 213–220.
Hough, J. H., Lucas, P. W., Bailey, J. A., Tamura, M.: 2007,
Low Polarization Standards, The Future of Photometric,
Spectrophotometric and Polarimetric Standardization, ASP
Conf. Ser. 364, Ed. C. Sterken, 523.
Huang, J., Fazio, G., Younger, J., Wilner, D., Yun, M., Wilson, G.,
Webb, T., Gurwell, M., Lai, K., Peck, A., Petitpas, G., Iono, D.,
Kohno, K., Kawabe, R., Sanders, D., Hughes, D., MartinezSansiger, A., Kim, S.: 2007, SMA/AzTEC Observations ofSubmillimeter Galaxies in the Cosmos Field,, AAS Meeting
210, #39.1.
Ichimoto, K., SOT Team: 2007, Solar Optical Telescope onboard
Hinode for Diagnosing the Solar Magnetic Fields, Plasma andFusion Research vol. 2, 2007, Eds. K. Ida et al., S1009.
Ichimoto, K., Suematsu, Y., Shimizu, T., Katsukawa, Y., Noguchi,M., Nakagiri, M., Miyashita, M., Tsuneta, S., Tarbell T. D.,
Shine, R. A., Hoffmann, C. M., Cruz, T., Lites, B. W., Elmore, D.
F., SOT Team: 2007, Calibration of the SOT Polarization, New
Solar Physics with Solar-B Mission, ASP Conf. Ser. 369, Eds. K.

058

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Shibata, S. Nagata, T. Sakurai, 39–42.
Ichimoto, K., Suematsu, Y., Tsuneta, S., Katsukawa, Y.,
Shimojo, M., Kubo, M., Shimizu, T., Shine, R., Tarbell, T.,
Title, A., Lites, B., Elmore, D., Yokoyama, T., Nagaka, S.: 2007,
Hinode/SOT Observation of Fine Structure of the Evershed
Flow, AAS Bulletin Vol. 39, No. 1 (AAS Meeting 210), Ed. K. B.
Marvel, #94.08.
Imaeda, Y., Tsuribe, T., Inutsuka, S.: 2007, SPH for Cold and
Low Viscous Shear Flow. SPHERIC – Smoothed Particle
Hydrodynamics European Research, Interest Community, 87.
Imai, H., Omodaka, T., Hirota, T., Umemoto, T., Sorai, K.,
Kondo, T., the VERA collaboration: 2008, A Collimated Jet
and an Infalling-Rotating Disk in G192.16-3.84 Traced by H2O
Maser Emission, IAU Symp. 242, Astrophysical Masers andtheir Environments, Eds. J. M. Chapman, W. A. Baan, 340–341.
Imanishi, M.: 2008, Buried AGNs in Nearby Ultraluminous
Infrared Galaxies, The Second Spitzer Science Center Conf.:
Infrared Diagnostics of Galaxy Evolusion, Eds. R.-R. Chary, H.
I. Teplitz, K. Sheth, 478–481.
Imanishi, M.: 2008, Comparison of Nuclear Starburst Luminosities
Between Seyfert 1 and 2 Galaxies, Based on Infrared 3–4
micron Spectroscopy, The Second Spitzer Science Center Conf.:
Infrared Diagnostics of Galaxy Evolusion, Eds. R.-R. Chary, H.
I. Teplitz, K. Sheth, 474–478.
Imanishi, M.: 2007, A systematic infrared spectroscopic study of
nuclear starbursts in Seyfert galaxies –Implications for an AGN
fueling mechanism–, ASS Proc. “Mapping the Galaxy and
Nearby Galaxies”, Eds. K. Wada, F. Combes, 336–336.
Imanishi, M.: 2007, Luminous buried AGNs in the local universe,
The Central Engine of Active Galactic Nuclei, ASP Conf. Ser.
373, Eds. L. C. Ho, J. Wang, 612–613.
Imanishi, M.: 2007, Millimeter interferometric observationsof nearby luminous infrared galaxies, The Central Engine of
Active Galactic Nuclei, ASP Conf. Ser. 373, Eds. L. C. Ho, J.
Wang, 614–615.
Imanishi, M.: 2007, Nuclear starbursts in the dusty tori of Seyfert
1 and 2 galaxies, The Central Engine of Active Galactic Nuclei,
ASP Conf. Ser. 373, Eds. L. C. Ho, J. Wang, 608–611.
Inoue, M., Asada, K., Nagai, H.: 2007, Possible Detection ofFaraday Screen, The Central Engine of Active Galactic Nuclei,
ASP Conf. Ser. 373, Eds. L. C. Ho, J. Wang, 209.
Inoue, M., Haba, A., Asada, K., Nagai, H., Murata, Y., Edwards,
P.: 2007, Kinematic Aging and Spectral Aging in YoungRadio Galaxies, ASS Proc. “Mapping the Galaxy and Nearby
Galaxies”, Eds. K. Wada, F. Combes, 338.
Inoue, M., Murata, Y.: 2007, The Next-generation Space VLBI
Project: VSOP-2, The Central Engine of Active Galactic Nuclei,
ASP Conf. Ser. 373, Eds. L. C. Ho, J. Wang, 715.
Inoue, T., Inutsuka, S., Koyama, H.: 2007, Transition Layers in
the Interstellar Medium SINS – Small Ionized and Neutral
Structures in the Diffuse Interstellar Medium, ASP Conf. Ser.
365, 127.
Inutsuka, S., Koyama, H.: 2007, Dynamics of a Multi-Phase
Interstellar Medium SINS – Small Ionized and Neutral
Structures in the Diffuse Interstellar Medium, ASP Conf. Ser.
365, 162.

Iono, D., Takakuwa, S., Kawabe, R., Vila-Vilaro, B., Saito, M.,
Tamura, Y.: 2007, ALMA Imaging Simulations of Nearby
and Distant Colliding Galaxies, From Z-Machines to ALMA:(Sub)Millimeter Spectroscopy of Galaxies, ASP Conf. Ser. 375,
Eds. A. J. Baker, J. Glenn, A. I. Harris, J. G. Mangum, M. S.
Yun, 242–245.
Ishimura, T., Yatsu, Y., Shimokawabe, T., Kawai, N., Yoshida, M.:
2007, GRB 071020: MITSuME Akeno optical observations,
GCN Circular 7026, 1.
Ishitsuka, J. K., Ishitsuka, M. Kaifu, N., Inoue, M., Tsuboi, M.,
Ohishi, M., Kondo, T., Koyama, Y., Kasuga, T., Fujisawa, K.,
Miyazawa, K., Miyoshi, M., Umemoto, T., Bushimata, T.,
Horiuchi, S., Vidal, E. D.: 2007, A New Astronomical Facility
for Peru: Converting a Telecommunication's 32 Meter Parabolic
Antenna into a Radio Telescope, Proc. of the “Astronomy for
the Developing World: IAU 26th General Assembly in Pragua”,
Eds. J. B. Hearnshaw, P. Martinez, 77–82.
Ito, H., Kino, M., Kawakatu, N., Isobe, N., Yamada, S.: 2007,
Large kinetic power in FRII radio jets, ASS 311, 335–339.
Ito, T., Malhotra, R.: 2007, Dynamical transport and collision
probability of asteroid fragments from ν6, Proc. of the “N-bodyDynamics Symposium”, Ed. M. Sekiguchi, 214–213.
Ito, T., Yoshida, F.: 2007, Surface Color Variation of a NewBorn Family Asteroid, Karin, Proc. of the “N-body Dynamics
Symposium”, Ed. M. Sekiguchi, 232–244.
Iye, M.: 2007, Japan's optical/infrared astronomy plan, Highlights
of Astronomy, 14, 532.
Izumiura, H., Nakada, Y., Hashimoto, O., Mito, H., Hayashi, T.:2007, Detection of an 0.1 pc Dust Shell of the Carbon Star U
Hydrae in Optical Light, Why Galaxies Care About AGB Stars:
Their Importance as Actors and Probes, ASP Conf. Ser. 378,
Eds. F. Kerschbaum, C. Charbonnel, R. F. Wing.
Kambe, E., Sato, B., Izumiura, H., Takeda, Y.: 2007, Test
Observation of EN Lac with Iodine Cell at Okayama, ASP
Conf. Ser. 361, Eds. S. Stefl, S. P. Owocki, A. T. Okazaki, 445.
Kamio, S., Kurokawa, H., Brooks, D. H.: 2007, The Relationshipbetween EUV Brightenings and Dark Mottles in the Quiet Sun,
New Solar Physics with Solar-B Mission, ASP Conf. Ser. 369,
Eds. K. Shibata, S. Nagata, T. Sakurai, 257–260.
Kamohara, R.: 2007, VLBI phase-referencing observations of
SiO masers towards R Aquarii, IAU Symp. 242, Astrophysical
Masers and their Environments, Eds. J. M. Chapman, W. A.
Baan, 322.
Kano, R., XRT Team: 2007, Multiplicity of Solar X-Ray Corona inTime and Space, Plasma and Fusion Research vol. 2, 2007, Eds.
K. Ida et al., S1010.
Kano, R., Sakao, T., Narukage, N., Kotoku, J., Bando, T.,
DeLuca, E. E., Lundquist, L., Golub, L., Tsuneta, S., Hara,
H., Shibasaki, K., Shimojo, M.: 2007, Temperature Structures
Above Coronal Hole and Quiet Sun, AAS Bulletin Vol. 39, No.
1 (AAS Meeting 210), Ed. K. B. Marvel, #94.36.
Kashikawa, N.: 2007, The End of the Reionization Epoch Probed
by Lyα Emitters at z=6.5, At the Edge of the Universe: Latest
Results from the Deepest Astronomical Surveys, ASP Conf. Ser.
380, Eds. J. Afonso, H. C. Ferguson, B. Mobasher, R. Norris,
11.

Katsukawa, Y.: 2007, Observational Analysis of the Relation
between Coronal Loop Heating and Photospheric Magnetic
Fields, New Solar Physics with Solar-B Mission, ASP Conf.
Ser. 369, Eds. K. Shibata, S. Nagata, T. Sakurai, 287–298.
Katsukawa, Y., Ichimoto, K., Sekii, T., Suematsu, Y., Tsuneta,
S., Shine, R. A., Tarbell, T. D.: 2007, Calibration of SOT
Dopplergrams, New Solar Physics with Solar-B Mission, ASP
Conf. Ser. 369, Eds. K. Shibata, S. Nagata, T. Sakurai, 43–46.
Kawakatu, N., Kino, M.: 2007, Dynamical Evolution of Hot Spotsin Radio-loud AGNs, The Central Engine of Active Galactic
Nuclei, ASP Conf. Ser. 373, Eds. L. C. Ho, J. Wang, 215.
Kawakatu, N., Kino, M.: 2007, The Velocity of Large-Scale Jets
in a Declining Density Medium, Triggering Relativistic Jets:
Revista Mexicana de Astronomía y Astrofísica (Serie de Conf.),
Eds. W. H. Lee, E. Ramírez-Ruiz, 192.
Kawazoe, F., Morioka, T., Sugamoto, A., Nishizawa, A., Sato, S.,
Leonheardt, V., Yamazaki, T., Fukushima, M., Kawamura,S.: 2007, Experimental Investigation of a Control Scheme for a
Tuned Resonant Sideband Extraction Interferometer for NextGeneration Gravitational Wave Detectors, Proc. of the XLIInd
Moriond Workshop, The Gioi Publishers, Vietnam, 191–196.
Kino, M., Kawakatu, N.: 2007, Cocoon Dynamics in AGN Jets as
a Probe of Their Power and Age, Triggering Relativistic Jets:
Revista Mexicana de Astronomía y Astrofísica (Serie de Conf.),
Eds. W. H. Lee, E. Ramírez-Ruiz, 198.
Kiuchi, K., Nakazato, K.-I., Kotake, K., Sumiyoshi, K. E.,
Yamada, S.: 2008, Gravitational Wave from Realistic Stellar
Collapse: Odd Parity Perturbation, Relativistic Astrophysics
Legacy and Cosmology – Einstein's, ESO Astrophysics
Symposia, Eds. B. Aschenback et al., 79.
Kobayashi, H., Kawakita, H., Mumma, M. J., Bonev, B. P., Fuse,
T., Watanabe, J.: 2007, Organic Volatiles in Comet 73P-B/
Schwassmann-Wachmann 3 Observed during Its Outburst: A
Clue to the Formation Region of the Jupiter-Family Comets,
AAS.
Kohno, K., Muraoka, K., Nakanishi, K., Tosaki, T., Kuno, N.,
Miura, R., Sawada, T., Sorai, K., Okuda, T., Kamegai, K.,
Tanaka, K., Endo, A., Hatsukade, B., Ezawa, H., Sakamoto,
S., Cortes, J., Yamaguchi, N., Matsuo, H., Kawabe, R.: 2007,
ASTE Observations of Dense Molecular Gas in Galaxies, IAU
Symp, 237, Triggered Star Formation in a Turbulent Interstellar
Medium, Eds. B. G. Elmegreen, J. Palous, 436.
Kohno, K., Nakanishi, K., Imanishi, M.: 2007, Compact Starburst
in the Central Regions of Seyfert Galaxies, The Central Engineof Active Galactic Nuclei, ASP Conf. Ser. 373, Eds. L. C. Ho, J.
Wang, 647–650.
Komugi, S., Sofue, Y., Nakanishi, H., Onodera, S., Egusa, F.,
Muraoka, K., Young, J. S.: 2008, Molecular Gas and Star
Formation in Nearby Galaxies, ASS Proc. “Mapping the Galaxy
and Nearby Galaxies”, Eds. K. Wada, F. Combes, 231–236.
Kotake, K.: 2008, Gravitational Radiation and Equations of Stateof Superdense Cores of Supernovae, Int. symp. on Exotic Statesof Nuclear Matter, Eds. U. Lombardo et al., 160–164.
Kotani, T., Abe, L., Tamura, M., Kurokawa, T., Tavrov, A.,
Takeda, M.: 2007, Low Speckle Noise Coronagraph with
UNI+PAC, Proc. of the Conf., In the Spirit of Bernard Lyot:

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The Direct Detection of Planets and Circumstellar Disks in the
21st Century, Ed. P. Kalas.
Koubsky, P., Harmanec, P., Skoda, P., Slechta, M., Yang, S.,
Bohlender, D., Kambe, E., Hashimoto, O.: 2007, Study of theLine-Profile Variations in the Spectrum of ζ Oph during the
May/June 2004 MOST Satellite Campaign, ASP Conf. Ser. 361,
Eds. S. Stefl, S. P. Owocki, A. T. Okazaki, 451.
Kudoh, T., Basu, S.: 2007, Three-dimensional MHD simulations ofmagnetized molecular cloud fragmentation with turbulence andion-neutral friction, IAU Symp, 237, Triggered Star Formation
in a Turbulent Interstellar Medium, Eds. B. G. Elmegreen, J.
Palous, 437–437.
Kuno, N., Sato, N., Nakanishi, H., Hirota, A., Tosaki, T., Shioya,
Y., Sorai, K., Nakai, N., Nishiyama, K., Vila-Vilaro, B.: 2007,
Distribution of Molecular Gas in Barred Spiral Galaxies, IAU
Symp. 235, Galaxy evolution across the Hubble Time, Eds. F.
Combes, J. Palous, 116.
Kuno, N., Sato, N., Nakanishi, H., Hirota, A., Tosaki, T., Shioya,
Y., Sorai, K., Nakai, N., Nishiyama, K., Vila-Vilaro, B.: 2008,
Nobeyama CO Atlas of Nearby Spiral Galaxies, ASS Proc.
“Mapping the Galaxy and Nearby Galaxies”, Eds. K. Wada, F.
Combes, 170–177.
Kuroda, D., Yanagisawa, K., Yoshida, M., Ishimura, T., Kawai,N.: 2007, GRB 071011: MITSuME Optical Observations, GCN
Circular 6922, 1.
Le Bertre, T., Tanaka, M., Yamamura, I., Murakami, H.,
MacConnell, D. J., Guertin, A.: 2007, Near-infrared Spectrophotometry of Carbon Stars, EAS Publ. Ser. 25, Eds. N.
Epchtein, M. Candidi, 175–178.
Lites, B. W., Elmore, D. F., Streander, K. V., Hoffmann, C.
M., Tarbell, T. D., Title, A. M., Shine, R. A., Ichimoto, K.,
Tsuneta, S., Shimizu, T., Suematsu, Y.: 2007, Performance
Characteristics of the Solar-B Spectro-Polarimeter, New Solar
Physics with Solar-B Mission, ASP Conf. Ser. 369, Eds. K.
Shibata, S. Nagata, T. Sakurai, 55–58.
Machida, M., Matsumoto, R.: 2007, Low-frequency, one-armed
oscillations in black hole accretion flows obtained from direct
3D MHD simulations, IAUS 2008, Eds. V. Karas, G. Matt, 405–406.
Manabe, S., Jike, T., Tamura, Y., VERA Group: 2007, VERA
Geodetic Activities, IVS 2006 Annual Report, NASA/
TP-2007-214151, Eds. D. Behrend, K. D. Baver, 69.
Matsui, H., Habe, A., Saitoh, T. R.: 2008, Effects of aSupermassive Black Hole Binary on a Nuclear Gas Disk, ASS
Proc. “Mapping the Galaxy and Nearby Galaxies”, Eds. K.
Wada, F. Combes, 350.
Matsumoto, R., Yahagi, H., Isobe, H., Yokoyama, T., Shiota,
D., Shibata, K., Miyagoshi, T., Kato, Y., Machida,M.: 2007, Cosmic Structure Formation and Dynamics:
Cosmological N-Body Simulations and Magnetohydrodynamic
Simulations, Annual Report of the Earth Simulator Center, 187–
192.
Matsumoto, R., Machida, M.: 2007, Sawtooth-like oscillations ofblack hole accretion disks, IAUS 2008, Eds. V. Karas, G. Matt,
37–42.
Matsumoto, R., Nishikori, H., Tanaka, M., Machida, M.: 2008,

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Global MHD Simulations of Galactic Gas Disks, ASS Proc.
“Mapping the Galaxy and Nearby Galaxies”, Eds. K. Wada, F.
Combes, 71.
Matsuo, H., Nagata, H., Kobayashi, J., Ariyoshi, S., Fujiwara,
M., Mori, Y., Murakoshi, Y., Nakahashi, M., Otani, C.: 2007,
Focal plane array technologies for SISCAM, IRMMW-THz,
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Matsuo, T., Shibai, H., Ootsubo, T., Tamura, M.: 2007, Planetary
Formation Scenarios Revisited: Core Accretion Versus Disk
Instability, Proc. of the Conf., In the Spirit of Bernard Lyot: The
Direct Detection of Planets and Circumstellar Disks in the 21stCentury, Ed. P. Kalas.
Matsushita, S., Tsai, A. L., Kawabe, R., Nakanishi, K., VilaVilaro, B., Kohno, K., Inui, T., Matsumoto, H., Tsuru, T. G.,
Peck, A. B.: 2008, Molecular Bubbles and Outflows in the
Edge-on Starburst Galaxies M82 and NGC 2146, ASS Proc.
“Mapping the Galaxy and Nearby Galaxies”, Eds. K. Wada, F.
Combes, 352.
McConnachie, A. W., Arimoto, N., Irwin, M.: 2007, The structuralcomplexity of the dwarf galaxies of the Local Group, IAU
Symp. 241, Stellar Populations as Building Blocks of Galaxies,
Eds. A. Vazdekis, R. F. Peletier, 361–362.
Miura, R., Tamura, Y., Okumura, S. K., Kawabe, R., Tosaki, T.,
Kuno, N., Nakanishi, K., Sakamoto, S., Hasegawa, T.: 2008,
Dense Clouds and Star Formation on Spiral Arm in M33 –deep
CO and HCN Observation in NGC604–, ASS Proc. “Mapping
the Galaxy and Nearby Galaxies”, Eds. K. Wada, F. Combes,
354.
Miyazaki, A., Shen, Z.-Q., Miyoshi, M., Tsuboi, M., Tsutsumi,
T.: 2008, Flux variability of Sgr A* at Short Millimeter
Wavelengths, ASS Proc. “Mapping the Galaxy and Nearby
Galaxies”, Eds. K. Wada, F. Combes, 355.
Motoyama, K., Umemoto, T., Shang, H.: 2007, Radiation Driven
Implosion Model for Star Formation Near an H II Region, IAU
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Medium, Eds. B. G. Elmegreen, J. Palous, 450.
Muraoka, K., Kohno, K., Tosaki, T., Kuno, N., Nakanishi, K.,
Sorai, K., Sakamoto, S.: 2007, ASTE CO(3–2) Observationsof M83: Correlation between CO(3–2)/(1–0) Ratios andStar Formation Efficiencies, IAU Symp, 237, Triggered Star
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Muraoka, K., Kohno, K., Tosaki, T., Kuno, N., Nakanishi, K.,
Sorai, K., Sakamoto, S.: 2008, CO(3–2) Wide Area Imaging of
M83 with ASTE: Correlation between CO(3–2)/CO(1–0) Ratios
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Galaxy and Nearby Galaxies”, Eds. K. Wada, F. Combes, 357.
Murata, Y., Mochizuki, N., Saito, H., Hirabayashi, H., Inoue, M.,
Kobayashi, H., Edwards, P. G.: 2007, The next generation
space VLBI project, VSOP-2, IAU Symp. 242, Astrophysical
Masers and their Environments, Eds. J. M. Chapman, W. A.
Baan, 517.
Nagai, H., Inoue, M., Asada, K., Kameno, S., Doi, A.: 2008,
Kinematic Aging and Spectral Aging in Young Radio Galaxies,
ASS Proc. “Mapping the Galaxy and Nearby Galaxies”, Eds. K.
Wada, F. Combes, 358.

Nagashima, M., Inutsuka, S., Koyama, H.: 2007, Evaporation
Timescales of HI Clouds SINS – Small Ionized and Neutral
Structures in the Diffuse Interstellar Medium, ASP Conf. Ser.
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Nagashima, M., Koyama, H., Inutsuka, S.: 2008, Evaporationof Tiny HI Clouds: Possible Probes of Physical State of the
Galactic Gas Di, ASS Proc. “Mapping the Galaxy and Nearby
Galaxies”, Eds. K. Wada, F. Combes, 360.
Nagayama, T., Omodaka, T., Handa, T., Sawada, T., Iahak, H.
B., Matsuyama, N.: 2008, A Wide Survey in NH3 Lines of theCentral 200 pc Around the Galactic Center with Kagoshima 6
Meter Radio Telescope, ASS Proc. “Mapping the Galaxy and
Nearby Galaxies”, Eds. K. Wada, F. Combes, 361.
Nakagawa, A., et al. including Shibata, K. M., Kurayama, T.,
the VERA project: 2007, VLBI monitoring of Mira variables
with VERA, IAU Symp. 242, Astrophysical Masers and their
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Nakamura, K.: 2008, “Gauge” in General Relativity: –Secondorder gauge-invariant perturbation theory–, Lie Theory and Its
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Nakamura, K.: 2008, Second-order gauge-invariant cosmologicalperturbation theory, The VIII Asia- Pacific International
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Nakamura, K.: 2008, Inclusion of first-order vector- and tensormodes in the second-order gauge-invariant cosmologicalperturbation theory, The 17th Workshop on General Relativity
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H., Kawai, N.: 2007, GRB 071021: MITSuME Okayama
Optical Upper Limits, GCN Circular 6975, 1.
Yoshida, M., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Kawai, N.: 2007, GRB 071112C MITSuME Okayama
optical observation, GCN Circular 7082, 1.
Yoshida, M., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Kawai, N.: 2007, GRB 071118 MITSuME OAO opticalobservation, GCN Circular 7119, 1.
Yoshida, M., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Kawai, N.: 2008, GRB 080229: possible optical afterglow,
GCN Circular 7341, 1.
Yoshida, M., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Kawai, N.: 2008, GRB 080307: optical upper limits, GCN
Circular 7370, 1.
Yoshida, M., Yanagisawa, K., Shimizu, Y., Nagayama, S., Toda,
H., Kawai, N.: 2008, GRB 080310: optical observation by
MITSuME telescope, GCN Circular 7410, 1.
Yoshida, N.: 2008, Structure of Galactic Dark Halos andObservational Prospects for Identifying the Nature of Dark
Matter, ASS Proc. “Mapping the Galaxy and Nearby Galaxies”,
Eds. K. Wada, F. Combes, 302–307.
Yoshida, T., Suzuki, T., Chiba, S., Kajino, T., Yokomakura,
H., Kimura, K., Takamura, A., Hartmann, D. H.: 2007,
Can supernova neutrino nucleosynthesis constrain neutrino
oscillation parameters?, Proc. of the Int. Symp. on Nuclear
Astrophysics – Nuclein in the Cosmos – IX, Ed. A. Mengoni etal., 196.

5. Publications in English
Kokubo, E.: 2007, Limites et Lobes de Roche (Brahic et al.),Vuibert, Paris.
Shibata, K., Nagata, S., Sakurai, T.: 2007, New Solar Physics with
Solar-B Mission, The Sixth Solar-B Science Meeting, ASP, San
Francisco.

6. Conference Presentations
Abe, L., Tamura, M., Nishikawa, J., Murakami, N., Enya, K.,
Tanaka, S., Nakagawa, T., Kataza, H.: 2007, High contrast
imaging activities in Japan, Navigator Program Forum – 2007,(Pasadena, USA, May 17-18).
Agata, H.: 2007, 4D2U theater; 3D movie theater at NAOJ, Global
Hands-On Universe Conference 2007, (Mitaka, Japan, Sept.
13-17).
Agata, H.: 2007, Introduction to new PUR experiments in Japan,
7th East Asian Astronomy Meeting Symposium, (Fukuoka,
Japan, Oct. 8-12).
Agatsuma, K.: 2007, Control system for the Seismic Attenuation
System (SAS) in TAMA300, 7th Edoardo Amaldi Conferenceon Gravitational Waves, (Sydney, Australia, July 8-14).
Akisawa, H., Sugawara, K., Watanabe, J.: 2007, The Dust Tail
Structure of C/2006 P1 (McNaught), Asia Oceania Geosciences
Society 4th Annual Meeting, (Bangkok, Thailand, Sept. 30-Aug.
4).
Akutsu, T., Kawamura, S., Arai, K., Tatsumi, D., Nagano, S.,
Sugiyama, N., Chiba, T., Takahashi, R., Yamamoto, K.,
Nishizawa, A., Nishida, E., Fukushima, M., Yamazaki, T.,
Fujimoto, M.-K.: 2007, Development of a detector pair forvery high frequency gravitational waves, 7th Edoardo Amaldi
Conference on Gravitational Waves, (Sydney, Australia, July8-14).
Ando, M., et al. including Kawamura, S., Seto, N., Arai, K.,
Fujimoto, M., Fukushima, M., Ishizaki, H., Miyakawa, O.,
Ohishi, N., Takahashi, R., Yamamoto, K., Yamazaki, T.:2007, DECIGO pathfinder, 10th International Conference on
Topics in Astroparticle and Underground Physics (TAUP 2007),(Sendai, Japan, Sept. 11-15).
Aoki, W., Barklem, P., Beers, T. C., Christlieb, N., Inoue, S.: 2007,
Lithium abundances in extremely metal-poor turn-off stars, 10th
Origin of Matter and Evolution fo Galaxies, (Sapporo, Japan,
Dec. 4-7).
Aoki, W.: 2007, Current and future spectroscopy capabilities ofSubaru, 2nd Sino-German Workshop on Galactic Astronomy
with LAMOST, (Hamburg, Germany, Sept. 16-22).
Arai, K.: 2007, Recent progress of TAMA300, 10th International
Conference on Topics in Astroparticle and Underground Physics(TAUP 2007), (Sendai, Japan, Sept. 11-15).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Migita, E., Kamiya,I., Kawano, N., Sasaki, S., Oberst, J.: 2008, Status andPreliminary Results of the Lunar Topography by KAGUYALALT Mission, The 2nd KAGUYA(SELENE) Science Working
Team Meeting, (Tokyo, Japan, Jan. 15-17).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Migita, E., Kamiya,I., Kawano, N., Sasaki, S., Oberst, J.: 2008, Present Status andPreliminary Results of the Lunar Topography by KAGUYALALT Mission, 39th Lunar and Planetary Science Conference,(League City, Texas, USA, Mar. 10-14).
Araki, H., Tazawa, S., Noda, H., Tsubokawa, T., Kawano, N.,
Sasaki, S.: 2007, Final status report of the Laser Altimeter(LALT) on board SELENE, Asia Oceania Geosciences Society
4th Annual Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).

Araki, H., Tazawa, S., Noda, H., Tsubokawa, T., Kawano, N.,
Sasaki, S.: 2007, Topographic Exploration of the Moon by laser
altimeter onboard SELENE (LALT), European Geosciences
Union General Assembly 2007, (Vienna, Austria, Apr. 15-20).
Arase, Y., Takahashi, R., Arai, K., Tatsumi, D., Fukushima, M.,
Yamazaki, T., Fujimoto, M-K., Agatsuma, K.: 2007, Damping
system for torsion modes of mirror isolation filter in TAMA300,
7th Edoardo Amaldi Conference on Gravitational Waves,(Sydney, Australia, July 8-14).
Arimoto, N.: 2007, Integrated Stellar Populations of Bulges,
Formation and Evolution of Galactic Bulges IAU Symposium
245, (Oxford, UK, July 16-20).
Asai, A., Hara, H., Watanabe, T., Imada, S., Narukage, N.,
Sakao, T.: 2007, Strongly Blueshifted Phenomena Observed in a
Flare with Hinode/EIS, Initial Results from Hinode: Workshop
in Memory of Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Asaki, Y., Miyoshi, M.: 2007, An Idea of Future Sub-millimeterWave Space-VLBI, Approaching Micro-Arcsecond Resolution
with VSOP-2: Astrophysics and Technology, (Sagamihara,
Japan, Dec. 3-7).
Asayama, S., Kawashima, S., Iwashita, H., Takahashi, T., Inata,
M., Obuchi, Y., Suzuki, T., Wada, T.: 2007, Progress andStatus of the ALMA Band 4 Cartridge Receiver, 7th Workshop
on Submillimeter-wave Receiver Technologies in Eastern Asia,(Osaka, Japan, Jan. 17-19).
Asayama, S.: 2008, Current Status of ALMA band 4 Cartridge
Receiver, 8th Workshop on Submillimter-wave ReceiverTechnology in Eastern Asia, (Seoul, Korea, Jan. 17-18).
Baba, N., Furuta, H., Murakami, N.: 2007, Geometric phasemodulator for IR nulling interferometer, Advanced Infrared
Technology and Applications 9, (Leon, Mexico, Oct. 7-12).
Candotti, M.: 2008, Vector near-field beam pattern measurement
facility for the characterisation of the ALMA band 10 frontend optics, 8th Workshop on Submillimter-wave ReceiverTechnology in Eastern Asia, (Seoul, Korea, Jan. 17-18).
Chiba, M., Tanaka, M., Komiyama, Y.: 2007, Subaru / SuprimeCam photometric data, Spectroscopic and PhotometricLandscape of Andromeda's Stellar Halo (SPLASH): Team
Meeting, (Santa Cruz, CA, USA, Sept. 20-22).
Choi, Y. K., et al.: 2007, Astrometry of red supergiant star VY
Canis Majoris with VERA, Approaching Micro-Arcsecond
Resolution with VSOP-2: Astrophysics and Technology,(Sagamihara, Japan, Dec. 3-7).
Choi, Y. K., et al.: 2007, Astrometry of red supergiant VY Canis
Majoris with VERA, IAU Symp. 248, A Giant Step: From Millito Micro-arcsecond Astrometry, (Shanghai, China, Oct. 15-19).
Endo, A., Inoue, H., Asayama, S., Noguchi, T., Kroug, M.,
Tamura, T.: 2007, Fabrication of aluminium nitride barrier
SIS mixer devices using plasma diluted by noble gases, 8thEuropean Conference on Applied Superconductivity, (Brussels,
Belgium, Sept. 16-20).
Endo, A.: 2007, Logarithmic growth of AlNx barriers in Nb/AlAlNx/Nb SIS tunnel junctions, 18th International Symposiumon Space Terahertz Technology, (Pasadena, USA, Mar. 21-23).
Endo, A.: 2007, Novel Techniques for Controlling the RnA of RF
Plasma Nitridized AlN Barriers for SIS Tunnel Junctions, 7th

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Workshop on Submillimeter-wave Receiver Technologies in
Eastern Asia, (Osaka, Japan, Jan. 17-19).
Endo, A.: 2008, A novel THz SIS mixer with a NbTiN-groundplaneand SIS micro-trylayers directly grown on a quartz substrate,
8th Workshop on Submillimter-wave Receiver Technology inEastern Asia, (Seoul, Korea, Jan. 17-18).
Fujii, M., Iwasawa, M., Funato, Y., Makino, J.: 2007, Fully selfconsistent N-body simulation of star cluster in the Galactic
center, IAU Symp. 246, Dynamical Evolution of Dense Stellar
Systems, (Capri, Italy, Sep 5-9).
Fukagawa, M., Itoh, Y., Oasa, Y., Kudo, T., Fujiwara, H., Tamura,M., Hayashi, M., Hayashi, S.: 2007, Near-Infrared Imagesof the Disk around HD 142527, Spirit of Bernard Lyot: The
Direct Detection of Planets and Circumstellar Disks in the 21stCentury, (Berkeley, CA, USA, June 4-8).
Fuse, T.: 2007, Observations of Fragments Split from Nucleus B of
Comet 73P/Schwassmann-Wachmann 3 by Subaru Telescope,2007 Asia Oceania Geosciences Society 4-th Annual General
Assembly, (Bangkok, Thailand, Sept. 30-Aug. 4).
Fuse, T.: 2007, Subaru Search for Neptunian L5 Trojans, New
Horizons Science Team Meeting 15, (Boulder, USA, May
30-31).
Fuse, T.: 2007, Understanding Outer Solar System –Past, Now,
and Future–, Asia Oceania Geosciences Society 4th Annual
Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Fuse, T.: 2008, Subaru Telescope's Collaboration with Space
Missions, The First Meeting of The International Primitive
Body Exploration Working Group, (Okinawa, Japan, Jan.
13-16).
Goossens, S., Matsumoto, K., Liu, Q., Noda, H., Namiki,N., Iwata, T.: 2008, On the procissing of tracking data fromthe SELENE satellites for orbit and lunar gravity field
determination, The 2nd KAGUYA(SELENE) Science Working
Team Meeting, (Tokyo, Japan, Jan. 15-17).
Goossens, S., Matsumoto, K.: 2008, Lunar degree 2 potential
Love number determination from satellite tracking data, 39th
Lunar and Planetary Science Conference, (League City, Texas,
USA, Mar. 10-14).
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T., JASMINE
Working Group: 2007, Infrared space astrometry project
JASMINE, IAU Symp. 248, A Giant Step: From Milli- to
Micro-arcsecond Astrometry, (Shanghai, China, Oct. 15-19).
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T., Tsujimoto, T.,
Suganuma, M., Niwa, Y., Yamauchi, M., JASMINE Working
Group: 2007, JASMINE-Consructor of the dynamical structureof the Galactic bulge, Formation and Evolution of Galactic
Bulges IAU Symposium 245, (Oxford, UK, July 16-20).
Guyon, O., Angel, R., Bowers, C., Burge, J., Burrows, A., Codona,J., Greene, T., Iye, M., Kasting, J., Martin, H., McCarthy,D., Meadows, V., Meyer, M., Pluzhnik, E., Sleep, N., Spears,
A., Tamura, M., Tenerelli, D., Vanderbei, R., Woodgate, B.,
Woodruff, R., Woolf, N.: 2007, Direct Imaging Of Nearby
Exoplanets With A Small Size Space Telescope: Telescope To
Observe Planetary System (TOPS), AAS Meeting 210, (Hawaii,
USA, May 27-31).
Hamana, T.: 2007, Subaru weak lensing cluster survey, XXIIIrd

066

II Publications, Presentations

IAP Conference “From giant arcs to CMB lensing: 20 yearsof gravitational distortion” in Honour of Bernard Fort, (Paris,
France, July 2-6).
Hamana, T.: 2007, Weak lensing cluster search, JSPS Core-tocore Program Seminar “Cosmology with Wide-field Imaging
Surveys of Galaxies”, (Tokyo, Japan, June 7-8).
Hanada, H., et al. including Tsuruta, S.: 2008, VLBI observationof SELENE(KAGUYA) by VERA and International Network,
IVS 5th General Meeting, (St. Petersburg, Russia, Mar. 3-8).
Hanada, H., et al. including Tsuruta, S.: 2008, Present status of
VRAD, The 2nd KAGUYA(SELENE) Science Working Team
Meeting, (Tokyo, Japan, Jan. 15-17).
Hanaoka, Y.: 2007, Expanding Applications of the Polarimeterswith Ferroelectric Liquid Crystals, 5th Solar Polarization
Workshop, (Ascona, Switzerland, Sept. 17-21).
Hara, H.: 2007, 2006 Dec 17 Long-Duration Flare Observed with
Hinode EIS, Initial Results from Hinode: Workshop in Memoryof Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Hara, H.: 2007, A Long-duration Flare Observed With Hinode
EIS, SPD/AAS Meeting, (Honolulu, Hawaii, USA, May 27-31).
Hara, H.: 2007, Enhanced Heating near the Footpoints of Coronal
Loops in Solar Active Regions, International CAWSES
Symposium, (Kyoto, Japan, Oct. 23-27).
Hara, H.: 2007, High-Velocity Nonthermal Plasma Motion
Concentrated at Footpoints of Coronal Loops, Initial Resultsfrom Hinode: Workshop in Memory of Takeo Kosugi, (Mitaka,
Japan, Apr. 24-27).
Hara, H.: 2007, Hinode/EIS: Current Status, Initial Results from
Hinode: Workshop in Memory of Takeo Kosugi, (Mitaka, Japan,
Apr. 24-27).
Hara, H.: 2007, Hinode: A New Solar Observatory in Space,
Hinode Workshop in China, (Beijin, China, Dec. 7-10).
Hara, H.: 2007, Non-thermal velocities at footpoints of active
regions and implications for coronal heating, Hinode Science
Meeting 7, (Dublin, Ireland, Aug. 21-24).
Hara, H.: 2007, Overview of EIS performance, Hinode Science
Meeting 7, (Dublin, Ireland, Aug. 21-24).
Hara, H.: 2007, Plasma Flows and Motions in Active Region
Loops observed with HINODE EUV Imaging Spectrometer, 3rdCoronal Loop Workshop, (Santorini, Greece, June 18-21).
Hayakawa, T., Iwamoto, N., Shimizu, T., Kajino, T., Umeda, H.,
Nomoto, K.: 2007, Universality of Photodisintegration Reaction
Nucleosynthesis in Supernovae, 23rd International Nuclear
Physics Conference 2007, (Tokyo, Japan, June 3-8).
Hayano, Y., Saito, Y., Ito, M., Saito, N., Akagawa, K., Takazawa,
A., Ito, M., Wada, S., Takami, H., Iye, M.: 2007, The Laser
Guide Star System for Adaptive Optics at Subaru Telescope,
Advanced Maui Optical and Space Surveillance Technologies
Conference, (Wailea, Hawaii, USA, Sept. 12-15).
Hayashi, S. S., Fuse, T., Ishida, C. M., Usuda-Sato, K.: 2007,
Interaction with Public at Subaru Telescope, AAS Meeting 210,
(Hawaii, USA, May 27-31).
Higuchi, A., Kokubo, E., Kinoshita, H., Mukai, T.: 2007,
Formation of the Oort Cloud and New Comets due to the
Galactic Tide, Extreme Solar Systems, (Santorini, Greece, June
24-29).

Hiroi, T., Nimura, T., Ueda, Y., Sasaki, S., Pieters, C. M.: 2008,
Deriving the Distribution of Ordinary Chondrite (H, L, LL)like Materials in Asteroids from Their Visible and Near-Infrared
Reflectance Spectroscopy, 39th Lunar and Planetary Science
Conference, (League City, Texas, USA, Mar. 10-14).
Hirota, T., et al.: 2007, Astrometry of H2O maser sources in Orion
KL with VERA, Massive Star Formation: Observations confront
theory, (Heidelberg, Germany, Sept. 10-14).
Hirota, T., Kawabe, R., Hagiwara, Y., Iono, D., Kurayama, T.,
Nakanishi, K., Takakuwa, S., Murata, Y., Kameno, S.: 2007,
Report of Asian Radio Astronomy Winter School, 7th East
Asian Astronomy Meeting Symposium, (Fukuoka, Japan, Oct.
8-12).
Hirota, T., VERA project team: 2007, Astrometry of H2O maser
sources in nearby molecular clouds with VERA, Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnology, (Sagamihara, Japan, Dec. 3-7).
Hirota, T.: 2007, Chemical Evolution of Dark Cloud Cores: A
View from Carbon-Chain and Deuterium Chemistry, NRO
Workshop, Workshop on Carbon-Chain Chemistry – 20th
Anniversary of CCS, (Tokyo, Japan, Dec. 7-8).
Hirota, T.: 2008, Report on the First Asian Radio Astronomy
Winter School 2007, East Asia VLBI Workshop, (Shanghai,
China, Mar. 20-22).
Honma, M., et al.: 2007, Astrometry of Galactic star forming
regions with VERA, IAU Symp. 248, A Giant Step: From Millito Micro-arcsecond Astrometry, (Shanghai, China, Oct. 15-19).
Honma, M.: 2007, Maser Astrometry with VERA, Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnology, (Sagamihara, Japan, Dec. 3-7).
Honma, M.: 2007, VERA, 7th East Asian Astronomy Meeting
Symposium, (Fukuoka, Japan, Oct. 8-12).
Honma, M.: 2008, Recent results from VERA, East Asia VLBI
Workshop, (Shanghai, China, Mar. 20-22).
Horaguchi, T, H., Goshima, M., Hara, T., Agata, H.: 2007,
Development of Makali`i and Teaching Materials using
Authentic Resources of Scientific Observation, 7th East Asian
Astronomy Meeting Symposium, (Fukuoka, Japan, Oct. 8-12).
Hori, K., Ichimoto, K., Sakurai, T.: 2007, Temperature
Diagnosis of Coronal Loop Oscillations Using Hinode EIS andNorikura NOGIS Coronagraph, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Hori, K.: 2007, Temperature Diagnosis of Coronal Loop
Oscillations using Hinode EIS andNorikura NOGIS coronagraph, Initial Results from Hinode: Workshop in Memory of
Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Horii, S., Watanabe, J., Sato, M.: 2007, Meteors brought from
73P/Schwassmann-Wachmann 3, Meteoroids 2007, (Barcelona,
Spain, June 11-15).
Hosokawa, T.: 2007, Evolution of the massive protostar with thehigh accretion rate, Massive Star Formation: Observations
confront theory, (Heidelberg, Germany, Sept. 10-14).
Ichimoto, K.: 2007, A new view of fine scale dynamics andmagnetism of sunspots revealed by Hinode/SOT, 5th Solar
Polarization Workshop, (Ascona, Switzerland, Sept. 17-21).

Ichimoto, K.: 2007, Convections in Sunspots Observed by SOT/
Hinode, International CAWSES Symposium, (Kyoto, Japan,
Oct. 23-27).
Ichimoto, K.: 2007, Diagnostic capability of FG/SP, Hinode
Workshop in China, (Beijin, China, Dec. 7-10).
Ichimoto, K.: 2007, Early results of the Solar-B (Hinode)spacecraft program, SuperDARN Workshop 2007, (Abashiri,
Japan, June 4-7).
Ichimoto, K.: 2007, Fine Structures of the Evershed Flow
Observed by SOT aboard Hinode, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Ichimoto, K.: 2007, First results and on-going researches in
Hinode team, Hinode Workshop in China, (Beijin, China, Dec.
7-10).
Ichimoto, K.: 2007, Hinode/SOT Observation of Fine Structureof the Evershed Flow, SPD/AAS Meeting, (Honolulu, Hawaii,
USA, May 27-31).
Ichimoto, K.: 2007, On-orbit performance of instrument, Hinode
Workshop in China, (Beijin, China, Dec. 7-10).
Ichimoto, K.: 2007, Overview of SOT performance, Hinode
Science Meeting 7, (Dublin, Ireland, Aug. 21-24).
Ichimoto, K.: 2007, SOT instrument introduction, Hinode
Workshop in China, (Beijin, China, Dec. 7-10).
Ichimoto, K.: 2007, Status of data analysis softwares and an
introduction, Hinode Workshop in China, (Beijin, China, Dec.
7-10).
Ichimoto, K.: 2007, Vertical components of mass motions insunspot penumbrae as observed by Hinode/SOT, Hinode
Science Meeting 7, (Dublin, Ireland, Aug. 21-24).
Imada, S.: 2007, Characteristics of the Upflow in the Plage Region
During the Gradual Phase of the X3.2 Flare on December 13,
2006, JPGU meeting – International Session, (Chiba, Japan,
May 19-24).
Imada, S.: 2007, Comparison Study of Different Mass Emission
Lines on Active Region, International CAWSES Symposium,(Kyoto, Japan, Oct. 23-27).
Imada, S.: 2007, Gradual Phase of teh X3.2 Flare on December
13, 2006, IUGG, (Perugia, Italy, July 2-13).
Imada, S.: 2007, Initial Results of the Extreme-ultraviolet Imaging
Spectrometer, Asia Oceania Geosciences Society 4th Annual
Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Imada, S.: 2007, Temperature-Dependent Upflow in the Plage
Associated with an X3.2 Flare on December 13, 2006, Initial
Results from Hinode: Workshop in Memory of Takeo Kosugi,(Mitaka, Japan, Apr. 24-27).
Imada, S.: 2007, Upflow in the plage region associated with an
X-class flare, Hinode Science Meeting 7, (Dublin, Ireland, Aug.
21-24).
Imamura, T., Iwata, T., Yamamoto, Z., Kono, Y., Matsumoto,K., Liu, Q., Noda, H., Hanada, H., Oyama, K.-I., Futaana,
Y., Saito, A., Nabatov, A.: 2008, Initial results of the lunar
ionosphere observation by RS, The 2nd KAGUYA(SELENE)
Science Working Team Meeting, (Tokyo, Japan, Jan. 15-17).
Imamura, T., Iwata, T., Yamamoto, Z., Oyama, K.-I., Nabatov, A.,
Kono, Y., Matsumoto, K., Liu, Q., Noda, H., Hanada, H.,

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Futaana, Y., Namaki, N., Saito, A.: 2008, Initial Results of thelunar ionosphere observation with SELENE radio scienece, 39th
Lunar and Planetary Science Conference, (League City, Texas,
USA, Mar. 10-14).
Imanishi, M.: 2007, Luminous buried AGNs at z>1 – Understanding the dust obscured AGN-starburst connections in the
distant universe, SPICA Science workshop, (Sagamihara, Japan,
May 24).
Imanishi, M.: 2007, Luminous buried AGNs in the local universe,
Obscured AGN across cosmic time, (Kloster Seeon, Bavaria,
Germeny, June 5-8).
Imanishi, M.: 2007, Millimeter interferometric HCN and HCO+
observations of luminous infrared galaxies, Radiative transfermini-workshop in Hakone, (Hakone, Japan, Oct. 16-17).
Imanishi, M.: 2007, NMA observations of luminous infrared
galaxies, Far-infrared and submillimeter emission of theinterstellar medium: models meet extragalactic and Galactic
observations, (Bad Honnef, Germany, Nov 5-7).
Inoue, A. K., Iwata, I.: 2007, Evolution of Escape Fraction of
Lyman Continumm from z=0 to 6, Galaxy Growth in the Dark
Universe, (Heidelberg, Germany, July 16-20).
Inoue, S.: 2007, Astrophysical Origin of Ultra-High Energy
Cosmic Rays, Future Prospects of Ultra-High Energy Cosmic
Rays, (Paris, France, May 22-23).
Inoue, S.: 2007, High Energy Emission from GRBs, High Energy
Phenomena in Relativistic Outflows, (Dublin, Ireland, Sept.
24-28).
Inoue, S.: 2007, Origin of Ultra High Energy Cosmic Rays,
10th International Conference on Topics in Astroparticle andUnderground Physics (TAUP 2007), (Sendai, Japan, Sept.
11-15).
Inoue, S.: 2007, Ultrahigh Energy Cosmic Rays as Heavy Nuclei
from Cluster Accretion Shocks, 30th International Cosmic Ray
Conference, (Merida, Mexico, Mar. 11).
Inoue, S.: 2008, Astrophysical Accelerators of Ultra-High Energy
Cosmic Rays, Accelerators in the Universe, (Tsukuba, Japan,
Mar. 12-14).
Ishikawa, R.: 2007, Discovery of Small-Scale Horizontal
Magnetic Structures in the Photosphere, Initial Results from
Hinode: Workshop in Memory of Takeo Kosugi, (Mitaka, Japan,
Apr. 24-27).
Ishikawa, R.: 2007, Discovery of Small-scale Horizontal Magnetic
Structures on The Solar Photosphere, SPD/AAS Meeting,(Honolulu, Hawaii, USA, May 27-31).
Ishikawa, R.: 2007, Ubiquitous Sporadic Horizontal Magnetic
Fields on the Photosphere with HINODE/SOT, International
CAWSES Symposium, (Kyoto, Japan, Oct. 23-27).
Ishiyama, T.: 2007, Statistical Study of Substructure Pair Histories,
Elizabeth and Frederick White Conference on the Magellanic
System, (Sydney, Australia, July 16-17).
Ito, T., Malhotra, R.: 2007, Collision probability of asteroid
fragments from the nu6 resonance, Asia Oceania Geosciences
Society 4th Annual Meeting, (Bangkok, Thailand, Sept. 30-Aug.
4).
Ito, T., Yoshida, F.: 2008, Boundary condition in collisional
evolution given by size frequency distribution observation of068

II Publications, Presentations

astronoids, 2007 Subaru Users Meeting, (Mitaka, Japan, Jan.
29-31).
Iwata, I., Ohta, K., Sawicki, M., Tamura, N., Akiyama, M., Aoki,
K.: 2007, Differential Evolution of Lyman Break Galaxies fromz=5 to 3, The 1st Subaru International Conference, Panoramic
Views of Galaxy Formation and Evolution, (Hayama, Japan,
Dec. 11-16).
Iwata, I., Ohta, K., Sawicki, M., Yabe, K., Tamura, N., Akiyama,
M., Aoki, K., Ando, M., Kiuchi, G.: 2007, Evolution of Lyman
Break Galaxies from Redshift 5 to 2: Implications for the First 2
Gyr of Galaxy Formation, Galaxy Growth in the Dark Universe,(Heidelberg, Germany, July 16-20).
Iwata, T., Namiki, N., Hanada, H., Noda, H., Kawano, N.,
Matsumoto, K., Tsuruta, S., Liu, Q., Kikuchi, F., Minamino,
H., Sasaki, T.: 2008, Properties of SELENE Small Satellites
for Selenodetic Measurements: Okina (Relay Satellite) andOuna (VRAD Satellite), The 2nd KAGUYA(SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 15-17).
Iye, M., et al. including Takami, H., Hayano, Y.: 2007, Subaru
LGSAO, Astronomy with Laser Guide Star Adaptive optics,(Ringberg, Germany, Oct. 29-11).
Iye, M., Kashikawa, N., Furusawa, H., Ota, K., Ouchi, M.,
Shimasaku, K.: 2007, SuprimeCam LAE Survey at redshift
7.3 – Ultimate limit with new red-sensitve CCDs, The 1st
Subaru International Conference, Panoramic Views of Galaxy
Formation and Evolution, (Hayama, Japan, Dec. 11-16).
Iye, M.: 2007, From Subaru to TMT, Extremely Distant Galaxies,
Science in the Era of TMT, (Irvine, CA, USA, July 23-25).
Izumiura, H.: 2007, HIDES upgrade: Current status of themosaiced CCD camera, The 2nd Annual Workshop on
Extrasolar Panet Survey, (Lijiang, China, May 14-20).
Jike, T., Manabe, S., Tamura, Y.: 2008, Result from K-band
Geodetic VLBI using VERA, IVS 5th General Meeting, (St.
Petersburg, Russia, Mar. 3-8).
Jurcak, J.: 2007, Penumbral models in the light of Hinode
spectropolarimetric observations, Hinode Science Meeting 7,(Dublin, Ireland, Aug. 21-24).
Jurcak, J.: 2007, Plasma Properties of Penumbral Fine Structures,
Initial Results from Hinode: Workshop in Memory of Takeo
Kosugi, (Mitaka, Japan, Apr. 24-27).
Kajino, T.: 2007, Baryons and Nucleosynthesis in Big-Bang
Cosmology and Spernovae, 11th international Baryons
Conference, (Seoul, Korea, June 11-15).
Kajino, T.: 2007, Big-Bang Cosmology, Nucleosynthesis andNeutrino Oscillation, 13th Lomonosov Conf. on Elementary
Particle Physics, (Moscow, Russia, Aug. 23-29).
Kajino, T.: 2007, Neutrino Oscillation in Supernova and GRB
Nucleosynthesis, Int. Symp. on Cosmology and Particle
Astrophysics, (Taipei, Taiwan, Nov. 13-15).
Kajino, T.: 2007, Nuclear Physics in Explosive Processes:
Nucleosynthesis in Big-Bang Cosmology and Supernova
Neutrino R-Process, 23rd International Nuclear Physics
Conference 2007, (Tokyo, Japan, June 3-8).
Kajino, T.: 2007, Nucleosynthesis and Cosmology, 19th
Rencontres de Blois on Matter and Energy in the Universe:
from nucleosynthesis to cosmology, (Blois, France, May 20-25).

Kajino, T.: 2007, R-process nuclei as nucleosynthetic signature
o GRBs, 3rd German-Japanese Int. Workshop on Nuclear
Structure and Astrophysics, (Munich, Germany, Sept. 29-Oct. 2).
Kambe, E.: 2007, Stellar Oscillations in Procyon A, Astronomy
with Precise Radial Velocity Measurements –Current Status and
its Future in East Asia–, (Lijiang, China, May 14-20).
Kambe, E.: 2007, Tuning of the multiple Gaussian IP fitting
technique through stellar oscillation observations with HIDES,
Astronomy with Precise Radial Velocity Measurements –Current Status and its Future in East Asia–, (Lijiang, China,
May 14-20).
Kameya, O., et al.: 2007, Star Formation in the NGC7538
region, Massive Star Formation: Observations confront theory,(Heidelberg, Germany, Sept. 10-14).
Kameya, O., VERA Team: 2007, Water Vapor Masers in the
NGC7538 Region, Approaching Micro-Arcsecond Resolution
with VSOP-2: Astrophysics and Technology, (Sagamihara,
Japan, Dec. 3-7).
Kameya, O.: 2008, Protection from Interference and Outreach
Activity of VERA, East Asia VLBI Workshop, (Shanghai,
China, Mar. 20-22).
Kamikura, M.: 2008, Design and Evaluations of a 385-500GHz
Orthomode Transducer(OMT), 8th Workshop on Submillimterwave Receiver Technology in Eastern Asia, (Seoul, Korea, Jan.
17-18).
Kamio, S.: 2007, Derivation of dBz/dz from Stokes Profiles and its
Application to Azimuth Ambiguity Resolution, Initial Resultsfrom Hinode: Workshop in Memory of Takeo Kosugi, (Mitaka,
Japan, Apr. 24-27).
Kamio, S.: 2007, Initial Results from EIS, JPGU meeting –International Session, (Chiba, Japan, May 19-24).
Kamio, S.: 2007, Velocity structure of bright points in a coronalhole, Hinode Science Meeting 7, (Dublin, Ireland, Aug. 21-24).
Kamio, S.: 2007, Velocity Structure of Jets in Coronal Holes,
Initial Results from Hinode: Workshop in Memory of Takeo
Kosugi, (Mitaka, Japan, Apr. 24-27).
Kano, R.: 2007, Data Archive & Distribution, Hinode Workshop in
China, (Beijin, China, Dec. 7-10).
Kano, R.: 2007, First Results & On-going Topics with XRT,
Hinode Workshop in China, (Beijin, China, Dec. 7-10).
Kano, R.: 2007, HINODE/X-Ray Telescope, Hinode Workshop in
China, (Beijin, China, Dec. 7-10).
Kano, R.: 2007, Hinode/XRT: Current Status, Initial Results from
Hinode: Workshop in Memory of Takeo Kosugi, (Mitaka, Japan,
Apr. 24-27).
Kano, R.: 2007, Micro-Flares Observed with Hinode/XRT, JPGU
meeting – International Session, (Chiba, Japan, May 19-24).
Kano, R.: 2007, Micro-Flares Observed with Hinode/XRT, Initial
Results from Hinode: Workshop in Memory of Takeo Kosugi,(Mitaka, Japan, Apr. 24-27).
Kano, R.: 2007, Temperature Structures Above Coronal Hole andQuiet Sun, SPD/AAS Meeting, (Honolulu, Hawaii, USA, May
27-31).
Kano, R.: 2007, Temperature Structures above Coronal Hole
Boundary and Quiet Sun, International CAWSES Symposium,(Kyoto, Japan, Oct. 23-27).

Kano, R.: 2007, Temperature Structures and Micro-Flares
Observed with Hinode/XRT, 3rd Coronal Loop Workshop,(Santorini, Greece, June 18-21).
Kano, R.: 2007, Vertical temperature structures above coronal holeboundary and quiet Sun, Hinode Science Meeting 7, (Dublin,
Ireland, Aug. 21-24).
Kano, R.: 2007, XRT Analysis Software, Hinode Workshop in
China, (Beijin, China, Dec. 7-10).
Kano, R.: 2007, XRT Observation Planning, Hinode Workshop in
China, (Beijin, China, Dec. 7-10).
Kano, R.: 2007, XRT On-orbit Performance, Hinode Workshop in
China, (Beijin, China, Dec. 7-10).
Kashikawa, N.: 2007, Lyman Alpha Galaxies from z=5.7 to 6.96
with Subaru, AAS Meeting 210, (Hawaii, USA, May 27-31).
Katsukawa, Y.: 2007, Chromospheric Micro-Jets Discovered
above Sunspot Penumbrae, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Katsukawa, Y.: 2007, Chromospheric Micro-jets Discovered
Above Sunspot Penumbrae, SPD/AAS Meeting, (Honolulu,
Hawaii, USA, May 27-31).
Katsukawa, Y.: 2007, Formation Process of a Light Bridge
Observed with Hinode/SOT, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Katsukawa, Y.: 2007, Hinode A New Solar Observatory in Space- Initial Results from Solar Optical Telescope, IUGG, (Perugia,
Italy, July 2-13).
Katsukawa, Y.: 2007, HINODE SOT observation of fine magnetic
structures, SOHO 19/GONG: Seismology of Magnetic Activity,(Melbourne, Australia, July 9-13).
Katsukawa, Y.: 2007, Properties of penumbral micro-jets
discovered by HINODE SOT, Hinode Science Meeting 7,(Dublin, Ireland, Aug. 21-24).
Katsukawa, Y.: 2007, Ubiquitous Jet-Like Activities in Sunspot
Chromospheres, International CAWSES Symposium, (Kyoto,
Japan, Oct. 23-27).
Katsukawa, Y.: 2008, Magnetic Reconnection in Sunspot
Penumbrae Observed with HINODE, The US-Japan Workshop
on Magnetic Reconnection 2008, (Okinawa, Japan, Mar. 3-6).
Kawagoe, S.: 2007, Constraints of oscillation parameters through
MSW effect of Supernova neutrino, 10th International
Conference on Topics in Astroparticle and Underground Physics(TAUP 2007), (Sendai, Japan, Sept. 11-15).
Kawagoe, S.: 2007, Modeling of Supernova Shock Propagation,
and Neutrino Oscillation, 23rd International Nuclear Physics
Conference 2007, (Tokyo, Japan, June 3-8).
Kawaguchi, N.: 2007, Current Status of eVLBI development
activities in NAOJ, 6th International e-VLBI Workshop, (Bonn,
Germany, Sept. 17-18).
Kawaguchi, N.: 2007, Highly Sensitive Radio Inter-ferometer
Observation with High Speed Data Transmission throughOptical Fiber Communication Network, iPOP2007, (Tokyo,
Japan, June 7-8).
Kawaguchi, N.: 2007, Phase Transfer and Science Data Acquisition
at Usuda, Approaching Micro-Arcsecond Resolution with

II Publications, Presentations

069

VSOP-2: Astrophysics and Technology, (Sagamihara, Japan,
Dec. 3-7).
Kawaguchi, N.: 2008, eVLBI activities in Japan, East Asia VLBI
Workshop, (Shanghai, China, Mar. 20-22).
Kawakatu, N., Nagai, H., Kino, M.: 2007, A New Evolution
scenario of compact symmetric objects, Approaching MicroArcsecond Resolution with VSOP-2: Astrophysics andTechnology, (Sagamihara, Japan, Dec. 3-7).
Kawakatu, N., Wada, K.: 2007, Coevolution of Super-massive
Black Holes and Circumnuclear Disks, Active Galactic Nuclei
at the highest angular resolution: theory and observations,(Torun, Poland, Aug. 27-Sept. 7).
Kawakatu, N., Wada, K.: 2007, Growth of supermassive black
holes and physical states of AGN obscuring tori, X-ray Surveys:
Evolution of Accretion, Star-Formation and the Large Scale
Structure, (Rodos Island, Greece, July 2-6).
Kawakatu, N., Wada, K.: 2008, Growth of supermassive black
holes and role of circumnuclear disk, Accretion and Outflow in
Astrophysics 2008 and Second Korea-Japan Young Astronomers
Meeting, (Kyoto, Japan, Jan. 8-11).
Kawamura, S., et al. including Seto, N., Sato, S., Arai, K.,
Fujimoto, M., Fukushima, M., Ishizaki, H., Miyakawa,O., Ohishi, N., Takahashi, R., Yamamoto, K., Yamazaki,
T.: 2007, The Japanese Space Gravitational Wave Antenna –DECIGO, 7th Edoardo Amaldi Conference on Gravitational
Waves, (Sydney, Australia, July 8-14).
Kawamura, S., et al. including Seto, N., Sato, S., Arai, K.,
Fujimoto, M., Fukushima, M., Ishizaki, H., Miyakawa,O., Ohishi, N., Takahashi, R., Yamamoto, K., Yamazaki,
T.: 2007, The Japanese Space Gravitational Wave Antenna
DECIGO, 10th International Conference on Topics in
Astroparticle and Underground Physics (TAUP 2007), (Sendai,
Japan, Sept. 11-15).
Kawazoe, F., Leonhardt, V., Sato, S., Miyakawa, O., Morioka, T.,
Nishizawa, A., Yamazaki, T., Fukushima, M., Kawamura,S., Sugamoto, A.: 2007, Experimental Investigation of aControl Scheme for a Tuned Resonant Sideband Extraction
Interferometer for Next-Generation Gravitational -Wave
Detectors, 7th Edoardo Amaldi Conference on Gravitational
Waves, (Sydney, Australia, July 8-14).
Kawazoe, F., Sato, S., Leonhardt, V., Miyakawa, O., Morioka, T.,
Nishizawa, A., Yamazaki, T., Fukushima, M., Kawamura, S.,
Sugamoto, A.: 2007, Experimental Demonstration of a control
scheme for next-generation gravitational-wave detectors, LSCVIRGO Meeting, (Hannover, Germany, Oct. 22-25).
Kikuchi, F., Liu, Q., Petrova, N., Matsumoto, K., Ishihara, Y.,
Goossens, S., Asari, K., Tsuruta, S., Ishikawa, T., Noda, H.,
Hanada, H., Iwata, T., Namiki, N., Kawano, N., Sasaki, S.:
2008, Differential phase delay estimation in VRAD missionof SELENE(KAGUYA), 39th Lunar and Planetary Science
Conference, (League City, Texas, USA, Mar. 10-14).
Kikuchi, K., Petrova, N., Liu, Q., Ishihara, Y., Mastumoto, K.,
Ishikawa, T., Asari, K., Tsuruta, S., Hanada, H., Iwata,T., Namiki, N., Kawano, N., RISE Project office, Mizusawa
VERA Observatory, RSAT/VRAD/RS mission team: 2008,
Differential phase delay estimation in VRAD mission of070

II Publications, Presentations

SELENE(KAGUYA), The 2nd KAGUYA(SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 15-17).
Kim, M. K., et al.: 2007, SiO maser observation towards Orion KL
with VERA, Massive Star Formation: Observations confront
theory, (Heidelberg, Germany, Sept. 10-14).
Kim, M. K., et al.: 2007, SiO Maser Observations towards OrionKL with VERA, Approaching Micro-Arcsecond Resolution
with VSOP-2: Astrophysics and Technology, (Sagamihara,
Japan, Dec. 3-7).
Kiuchi, H., Kawanishi, T., Yamada, M., Sakamoto, T.,
Tsuchiya, M., Amagai, J., Izutsu, M.: 2007, Photonic
Millimeter-wave generation Developments for the ALMA Radio
Telescope, 20th annual meeting of the IEEE Lasers and ElectroOptics society, (Florida, USA, Oct. 21-25).
Kiuchi, H., Kawanishi, T., Yamada, M., Sakamoto, T., Tsuchiya,
M., Amagai, J., Izutsu, M.: 2008, Photonic millimeter-wave
generation and distribution system applicable to the ALMA
radio telescopes, Progress in Electromagnetics research
symposium 2008, (Hangzhou, China, Mar. 24-28).
Kobayashi, H., Cho, S. H.: 2007, Progress of the East Asia VLBI
Consortium, 7th East Asian Astronomy Meeting Symposium,(Fukuoka, Japan, Oct. 8-12).
Kobayashi, H.: 2007, Phase referencing VLBI astrometry
observation system: VERA, IAU Symp. 248, A Giant Step:
From Milli- to Micro-arcsecond Astrometry, (Shanghai, China,
Oct. 15-19).
Kobayashi, H.: 2007, VSOP/HALCA Preparation and Launch,
Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technology, (Sagamihara, Japan, Dec. 3-7).
Kobayashi, H.: 2008, Status and future of East Asia VLBI
network, East Asia VLBI Workshop, (Shanghai, China, Mar.
20-22).
Kobayashi, Y., Gouda, N., Yano, T., Suganuma, M., Tsujimoto,T., Yamada, Y., Sako, N., Nakasuka, S.: 2007, The current statusof the Nano-JASMINE project, IAU Symp. 248, A Giant Step:
From Milli- to Micro-arcsecond Astrometry, (Shanghai, China,
Oct. 15-19).
Kohjiro, S., Shi, S.-C., Inatani, J., Maezawa, M., Uzawa, Y.,
Wang, Z., Shoji, A.: 2007, An Octave Bandwidth SIS Mixer for
Compact Spectrometers, 7th Workshop on Submillimeter-wave
Receiver Technologies in Eastern Asia, (Osaka, Japan, Jan.
17-19).
Kojima, K., Yamazaki, D. G., Kajino, T.: 2007, Neutrino-Mass
Effect on CMB anisotropies in A Cosmological Model with
Primordial Magnetic Field, 10th Origin of Matter and Evolution
fo Galaxies, (Sapporo, Japan, Dec. 4-7).
Kojima, K.: 2007, Cosmological constraint on “neutrino mass”
from CMB anisotropies with primordial magnetic field, DARK
2007, (Sydney, Australia, Sept. 24-28).
Kojima, T.: 2008, Preliminary design of the ALMA band 10
cartridge, 8th Workshop on Submillimter-wave ReceiverTechnology in Eastern Asia, (Seoul, Korea, Jan. 17-18).
Kokeyama, K.: 2007, The experimental plan of dis-placementand
and frequency-noise free laser inter-ferometer, 7th Edoardo
Amaldi Conference on Gravitational Waves, (Sydney, Australia,
July 8-14).

Kokubo, E.: 2007, Formation of Terrestrial Planets fromProtoplanets: Effects of Conditional Accretion, IAU Symposium
249, Exoplanets: Detection, Formation and Dynamics, (Suzhou,
China, Oct. 22-27).
Kokubo, E.: 2007, Formation of Terrestrial Planets from Protoplanets: Statistics of Planetary Spin, Extreme Solar Systems,(Santorini, Greece, June 24-29).
Kokubo, E.: 2008, Formation of Planetary Systems, Accretion and
Outflow in Astrophysics 2008 and Second Korea-Japan Young
Astronomers Meeting, (Kyoto, Japan, Jan. 8-11).
Komiyama, Y.: 2007, Galaxies in the Local Universe: Viewed
at the Subaru Prime Focus, The 1st Subaru International
Conference, Panoramic Views of Galaxy Formation and
Evolution, (Hayama, Japan, Dec. 11-16).
Komiyama, Y.: 2007, Technical Challenges for Constructing HSC,JSPS Core-to-core Program Seminar “Cosmology with Widefield Imaging Surveys of Galaxies”, (Tokyo, Japan, June 7-8).
Komiyama, Y.: 2007, Wide-field imaging survey of Leo II dwarf
spheroidal galaxy: stellar content and distribution, Galaxies inthe Local Volume, (Sydney, Australia, July 8-13).
Koryukin, V., Shitov. S. V., Bukovski, M. A., Uvarov, A. V., Uzawa,Y., Noguchi, T., Wang, Z., Kroug. M.: 2007, Balanced
waveguide mixer for ALMA band 10: HFSS simulation, 7thWorkshop on Submillimeter-wave Receiver Technologies in
Eastern Asia, (Osaka, Japan, Jan. 17-19).
Kotake, K.: 2007, Gravitational Radiation and Equations of Stateof Super-dense Cores of Supernovae, International Symposium
on Exotic States of Nuclear matter, (Catania, Italy, June 11-15).
Kotake, K.: 2007, Gravitational Wave Signals from typeII
Supernovae and Strongly Magnetized Neutron Stars, School ofMathematics, (Southampton, UK, Nov. 22).
Kotake, K.: 2007, Gravitational waves as a probe of the explosion
mechanism, Spanish Relativity Meeting, (Tenerife, Spain, Sept.
10-14).
Kotake, K.: 2007, Multidimensional modeling of core-collapse
supernovae, Seminar, (Niels Bohr Institute, Copenhagen,Denmark).
Kotake, K.: 2008, Features of Gravitational Wave-Signals from
Explosion of Massive Stars, MPA institute-seminar, (Garching,
Germany, Feb. 25).
Kotani, T., Nishikawa, J., Yokochi, K., Murakami, N., Abe, L.,
Tamura, M., Kurokawa, T., Tavrov, A., Takeda, M.: 2007, Low
speckle noise coronagraph with UNI+PAC, Spirit of Bernard
Lyot: The Direct Detection of Planets and Circumstellar Disks
in the 21st Century, (Berkeley, CA, USA, June 4-8).
Kotoku, J.: 2007, Magnetic feature and morphological studyof X-ray bright points, Hinode Science Meeting 7, (Dublin,
Ireland, Aug. 21-24).
Kotoku, J.: 2007, Observation of XBP, Hinode/SUMER Workshop, (Tokyo, Japan, Oct. 9).
Kotoku, J.: 2007, X-ray Bright Points Observed with Hinode/XRT,
Initial Results from Hinode: Workshop in Memory of Takeo
Kosugi, (Mitaka, Japan, Apr. 24-27).
Kroug, M.: 2008, SIS Mixer Fabrication for ALMA Band10,
8th Workshop on Submillimter-wave Receiver Technology inEastern Asia, (Seoul, Korea, Jan. 17-18).

Kudoh, T., Basu, S.: 2007, Three-dimensional simulations ofmolecular cloud fragmentation induced by ambipolar diffusion
and nonlinear flows, Magnetic Fields in the Universe II: From
Laboratory and Stars to the Primordial Universe, (Cozumel,
Mexico, Jan. 28-Feb. 1).
Kudoh, T.: 2007, Nonlinear Alfven wave model of spicules andcoronal heating, IAU Symposium 247, Waves & Oscillationsin the Solar Atmosphere: Heating and Magneto-Seismology,(Porlamar, Isla de Margarita, Venezuela, Sept. 17-21).
Kurayama, T., et al.: 2007, VERA observation of the massive star
forming region G34.4+0.23, IAU Symp. 248, A Giant Step:
From Milli- to Micro-arcsecond Astrometry, (Shanghai, China,
Oct. 15-19).
Kurayama, T.: 2007, VERA Observation of G34.4+0.23 andMatters That Require attention for VSOP-2 Phase Referencing,
Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technology, (Sagamihara, Japan, Dec. 3-7).
Kusakabe, M.: 2007, Big-Bang Nucleosynthesis with NegativelyCharged Massive Particles as a Cosmological Solution to the
6Li and 7Li Problems, 10th Origin of Matter and Evolution fo
Galaxies, (Sapporo, Japan, Dec. 4-7).
Kusakabe, M.: 2007, Cosmological Non-thermal Nuclear
Processes of 6Li Synthesis Induced by Radiative Decay of Relic
Particles, 23rd International Nuclear Physics Conference 2007,(Tokyo, Japan, June 3-8).
Kusakabe, M.: 2007, Effect of Negatively-Charged Massive
Particles on Big-Bang Nucleosynthesis and a Solution to the
Lithium Problems, Int. Symp. on Cosmology and Particle
Astrophysics, (Taipei, Taiwan, Nov. 13-15).
Kusakabe, M.: 2007, Negatively-Charged Massive Particles
as a Solution to the 6Li and 7Li Problems, VIII Asia-PacificInternational Conference on Gravitation and Astrophysics,(Nara, Japan, Aug. 29-Sept. 1).
Kusakabe, M.: 2007, Negatively-Charged Massive Particles as
Progenitors for CDM, and Solution to the 6Li and 7Li Problem
in Big Bang Nucleosynthesis, DARK 2007, (Sydney, Australia,
Sept. 24-28).
Li, J., Shen, Z.-Q., Miyazaki, A., Miyoshi, M.: 2007, The 3-mm
Flux Density Monitoring of Sagittarius A* with the ATCA,
IAU Symp. 248, A Giant Step: From Milli- to Micro-arcsecond
Astrometry, (Shanghai, China, Oct. 15-19).
Liu, Q., Kikuchi, F., Matsumoto, K., Hanada, H., Iwata, T.,
Kawano, N., Namiki, N., Asari, K., Ishihara, Y., Noda, H.,
Ishikawa, T., Tsuruta, S., Goossens, S., Petrova, N., Sasaki,
S.: 2008, Studies on Doppler and differential VLBI techniques
using two sub-satellites Rstar (OKINA) and Vstar (OUNA) of
KAGUYA (SELENE), The 2nd KAGUYA(SELENE) Science
Working Team Meeting, (Tokyo, Japan, Jan. 15-17).
Ly, C., Malkan, M. A., Treu, T., Woo, J., Kashikawa, N.,
Shimasaku, K.: Lyman Break Galaxies in the Redshift Desert:
Deep Galex Nuv Imaging Of The Subaru Deep Field, AAS
Meeting 210, (Hawaii, USA, May 27-31).
Machida, M.: 2007, High frequency QPOs excited by lowfrequency disk oscillation, YITP Workshop on Quasi-Periodic
Oscillations and Time Variabilities of Accretion Flows, (Kyoto,
Japan, Nov. 20-22).

II Publications, Presentations071

Machida, M.: 2008, MHD simulations of the Coronal Loop-like
Structrues in our Galactic Center, International winter school on
the Interstellar Medium 2008, (Ise-Shima, Japan, Feb. 18-22).
Machida, M.: 2008, Quasi-periodic ejection of outflows from theinnermost region of an accretion disk, Accretion and Outflow in
Astrophysics 2008 and Second Korea-Japan Young Astronomers
Meeting, (Kyoto, Japan, Jan. 8-11).
Machida, M.: 2008, Quasi-periodic oscillation of an inner torus by
the magnetic activities, The US-Japan Workshop on Magnetic
Reconnection 2008, (Okinawa, Japan, Mar. 3-6).
Magara, T.: 2007, An Investigation into the Initiation Mechanismof a Solar Flare Based on the Observed Nature of Photospheric
Magnetic Field, International CAWSES Symposium, (Kyoto,
Japan, Oct. 23-27).
Makino, J.: 2007, Current status of GRAPE Project PDF
Dynamical Evolution of Dense Stellar Systems, IAU Symp.
246, Dynamical Evolution of Dense Stellar Systems, (Capri,
Italy, Sep 5-9).
Makino, J.: 2007, Do-it-yourself Computational Astronomy –Hardwares, Algorithms, Softwares, and Sciences, The third
Takagi Lectures, (Tokyo, Japan, Nov. 23).
Makino, J.: 2007, Evolution of Multiple Blackhole Systems
in Galactic Centers, N-body dynamics in near-Keplerianpotentials, (Leiden, Netherlands, May 29-June 1).
Makino, J.: 2007, GRAPE-DR, AstroGPU, (Princeton, NJ, USA,
Nov. 9-10).
Makino, J.: 2007, GRAPE-DR: 2-Pflops massively-parallel
computer with 512-core, 512-Gflops processor chips forscientific computing, SC07, (Reno, NV, USA, Nov. 10-17).
Makino, J.: 2007, Gravitational Many-Body Problem, International
Symposium on New Facet of Three Nucleon Force, (Tokyo,
Japan, Oct. 29-31).
Matsumoto, K., Goossens, S., Liu, Q., Iwata, T., Namiki, N.,
Noda, H., Hanada, H., Kikuchi, F., Ishihara, Y., Kawano,N., Tsuruta, S., Asari, K., Ishikawa, T., Sasaki, S.: 2008,
Current status of acquisition and processing of tracking datafrom SELENE (KAGUYA) satellites for Lunar gravity field
estimation, 39th Lunar and Planetary Science Conference,(League City, Texas, USA, Mar. 10-14).
Matsumoto, K., Hanada, H., Goossens, S., Sasaki, S., Kawano,N., Namiki, N.: 2007, A simulation study for anticipatedaccuracy of lunar gravity field model by SELENE tracking
data, Asia Oceania Geosciences Society 4th Annual Meeting,(Bangkok, Thailand, Sept. 30-Aug. 4).
Matsumoto, K., Sasaki, S., Hanada, H., Goossens, S., Tsuruta,
S., Kawano, N., Namiki, N., Iwata, T., Rowlands, D.: 2007, A
simulation study for anticipated accuracy of lunar gravity fieldmodel by SELENE tracking data, European Geosciences Union
General Assembly 2007, (Vienna, Austria, Apr. 15-20).
Matsuo, H., Mori, Y., Murakoshi, Y., Ariyoshi, S., Ezawa, H.,
Hibi, Y., Kobayashi, J., Nagata, H., Nakahashi, M., Otani,C.: 2007, Realization of submillimeter-wave imaging array withsupercondeucting direct detectors, 12th international workshop
on Low Temperature Detectors, (Paris, France, July 22-27).
Matsuo, H., Nagata, H., Kobayashi, J., Ariyoshi, S., Fujiwara,
M., Mori, Y., Murakoshi, Y., Nakahashi, M., Otani, C.:072

II Publications, Presentations

2007, Focal plane array technologies for SISCAM, IRMMWTHz2007, (Cardiff, UK, Sept. 3-7).
Matsuo, H.: 2007, Wideband Imaging Techniques in Terahertz
Frequencies, 7th Workshop on Submillimeter-wave ReceiverTechnologies in Eastern Asia, (Osaka, Japan, Jan. 17-19).
Matsuo, H.: 2008, System design of superconducting submilimeterwave digicam, 8th Workshop on Submillimter-wave ReceiverTechnology in Eastern Asia, (Seoul, Korea, Jan. 17-18).
Miyakawa, O.: 2007, Lock Acquisition Studies for Advanced
Interferometers, 7th Edoardo Amaldi Conference on
Gravitational Waves, (Sydney, Australia, July 8-14).
Miyazaki, A., Shen, Z.-Q., Miyoshi, M., Tsutsumi, T., Tsuboi,
M.: 2007, Flux variability of Sagittarius A* at short mmwavelengths, Approaching Micro-Arcsecond Resolution with
VSOP-2: Astrophysics and Technology, (Sagamihara, Japan,
Dec. 3-7).
Miyazaki, S.: 2007, ROE JSPS Workshop, Hyper Suprime-Cam,(Edinburgh, UK, Oct. 24-26).
Miyoshi, M.: 2007, Several Problems on VERA System to besolved, IAU Symp. 248, A Giant Step: From Milli- to Microarcsecond Astrometry, (Shanghai, China, Oct. 15-19).
Miyoshi, M., Kameno, S., Ishitsuka, J. K., Shen, Z.-Q., Takahashi,R., Horiuchi, S.: 2007, An Approach to Detect the Event
Horizon in SgrA* using ground based submillimetre VLBI
array, Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technology, (Sagamihara, Japan, Dec. 3-7).
Miyoshi, M.: 2008, Radio QPO from Sagittarius A* with a new
method investigating black hole, Observational Evidence forBlack Holes in the Universe II, (Kolkota, India, Feb. 10-15).
Miyoshi, M.: 2007, QPO from Sagittarius A*, YITP Workshop on
Quasi-Periodic Oscillations and Time Variabilities of Accretion
Flows, (Kyoto, Japan, Nov. 20-22).
Morinaga, S., Sakurai, T., Tsuneta, S., Suematsu, Y., Ichimoto,K., Jurcak, J., Nagata, S., Lites, B. W.: 2007, Center-to-Limb
Variation in Stokes Profiles of Magnetic Fluxtubes Observedwith Hinode Spectropolarimeter, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Morinaga, S.: 2007, Center-to-Limb Variation in Stokes Profiles ofMagnetic Fluxtubes Observedwith Hinode Spectropolarimeter,
Initial Results from Hinode: Workshop in Memory of Takeo
Kosugi, (Mitaka, Japan, Apr. 24-27).
Nagashima, K.: 2007, Distribution of Acoustic Power in NOAA
AR 10935 Seen by HINODE/SOT, SOHO 19/GONG: Seismology of Magnetic Activity, (Melbourne, Australia, July 9-13).
Nagashima, K.: 2007, Observations of Sunspot Oscillations fromHINODE, Workshop on Time-Distance Helioseismology andHelioseismic Holography, (Stanford, CA, USA, Aug. 7).
Nagashima, K.: 2008, Initial analyses of non-magnetic
Dopplergrams obtained by Hinode/SOT, SDO - HMI/EVE/AIA
Science Teams Meeting - 2008, (Napa, CA, USA, Mar. 25-28).
Nagata, H., Kobayashi, J., Matsuo, H., Nakahashi, M.,
Kobayashi, K., Ikeda, H., Fujiwara, M.: 2007, Astronomical
testing observation in Multi-Fourier transform interferometer:
Aperture synthesis technique and CMB, 12th international
workshop on Low Temperature Detectors, (Paris, France, July

22-27).
Nakajima, T., Kaiden, M., Korogi, J., Kimura, K., Yonekura, Y.,
Ogawa, H., Nishiura, S., Dobashi, K., Yoda, T., Handa, T.,
Kohno, K., Morino, J., Asayama, S., Noguchi, T.: 2007,
New 60-cm Radio Survey Telescope with the SidebandSeparating SIS Receiver for the 200 GHz Band, 7th Workshop
on Submillimeter-wave Receiver Technologies in Eastern Asia,(Osaka, Japan, Jan. 17-19).
Nakamura, K.: 2007, Gauges in general relativity –Second
order gauge invariant cosmological perturbation theory–, 7thInternational Conference on ''Lie Theory and Its Application in
Physics", (Varna, Bulgaria, June 18-24).
Nakamura, K.: 2007, Second-order gauge-invariant cosmologicalperturbation theory, VIII Asia-Pacific International Conferenceon Gravitation and Astrophysics, (Nara, Japan, Aug. 29-Sept. 1).
Nakamura, K.: 2007, Second-order gauge-invariant perturbation
theory and its application to cosmology, Invited Seminar,(Academia Sinica, Taiwan, May 31).
Nakamura, K.: 2007, Second-order gauge-invariant cosmologicalperturbation theory – 2. Extension to include the first-order
vector- and tensor-modes, 17th Workshop on General Relativity
and Gravitation in JAPAN, (Nagoya, Japan, Dec. 3-7).
Nakata, F., Kodama, T., Tanaka, M.: 2007, Spectroscopic studyof galaxies within the structure around Cl 0939+4713, The 1st
Subaru International Conference, Panoramic Views of Galaxy
Formation and Evolution, (Hayama, Japan, Dec. 11-16).
Nakayama, Y., Okamoto, A., Takayama, Y., Hayano, Y.: 2007,
Splice of photonic crystal fibres by use of double phaseconjugate mirror, SPIE Europe: Optics and Optoelectronics:
Photonic Crystal Fibers, (Prague, Czech Republic, Apr. 16-19).
Namiki, N., Iwata, T., Matsumoto, K., Hanada, H., Noda, H.,
Ogawa, M., Kawano, N., Asari, K., Tsuruta, S., Goossens,
S., Liu, Q., Kikuchi, F., Ishihara, Y., Ishikawa, T., Sasaki,S., Aoshima, C., Sugita, S., Kurosawa, K., Matsumura, M.,
Yokoyama, M., Kamata, S., Kubo, N.: 2008, Initial results ofgravity experiment by four-way Doppler measurement, The 2nd
KAGUYA(SELENE) Science Working Team Meeting, (Tokyo,
Japan, Jan. 15-17).
Namiki, N., Iwata, T., Matsumoto, K., Hanada, H., Noda, H.,
Ogawa, M., Kawano, N., Asari, K., Tsuruta, S., Goossens,
S., Liu, Q., Kikuchi, F., Ishihara, Y., Ishikawa, T., Sasaki,S., Aoshima, C.: 2008, Initial Results of Gravity Experiment
By Four-Way Doppler Measurement Of KAGUYA (SELENE),
39th Lunar and Planetary Science Conference, (League City,
Texas, USA, Mar. 10-14).
Nishiyama, S.: 2007, Pre-main sequence stars in the Magellanic
Bridge, Elizabeth and Frederick White Conference on the
Magellanic System, (Sydney, Australia, July 16-17).
Nishizawa, A.: 2007, Laser-interferometric detectors forgravitational-wave background at 100 MHz, The 1st Subaru
International Conference, Panoramic Views of Galaxy
Formation and Evolution, (Hayama, Japan, Dec. 11-16).
Nishizawa, A.: 2007, Quantum noise in differential-type GWinterferometer and signal recycling, 7th Edoardo Amaldi
Conference on Gravitational Waves, (Sydney, Australia, July8-14).

Nishizawa, A.: 2008, Displacement noise-free inter-ferometers forgravitational waves at ultra high frequencies, LIGO-VIRGO
meeting, (Caltech, USA, Mar. 17-20).
Nitadori, K.: 2007, 6th and 8th order Hermite Integrator Using
Snap and Crackle, IAU Symp. 246, Dynamical Evolution ofDense Stellar Systems, (Capri, Italy, Sep 5-9).
Nitadori, K.: 2007, High-Accuracy N-body Simulasions on GPU(poster award), AstroGPU, (Princeton, NJ, USA, Nov. 9-10).
Nitta, S.: 2007, Continuous Transition from Fast to Slow Regimeof Magnetic Reconnection and Application to Solar Flares,
International CAWSES Symposium, (Kyoto, Japan, Oct. 23-27).
Niwa, Y., Arai, K., Ueda, A., Sakagami, M., Gouda, N.,
Kobayashi, Y., Yamada, Y., Yano, T.: 2007, Laser interferometric high-precision angle monitor, IAU Symp. 248,
A Giant Step: From Milli- to Micro-arcsecond Astrometry,(Shanghai, China, Oct. 15-19).
Nogami, K., et al. including Sasaki, S.: 2007, Present Status of
the Mercury Dust Monitor Onboard Bepicolombo Spacecraft
MMO, Asia Oceania Geosciences Society 4th Annual Meeting,(Bangkok, Thailand, Sept. 30-Aug. 4).
Noguchi, T.: 2007, Status of SIS device development at NAOJ,
7th Workshop on Submillimeter-wave Receiver Technologies in
Eastern Asia, (Osaka, Japan, Jan. 17-19).
Noguchi, T.: 2008, SIS Devices Development at NAOJ, 8thWorkshop on Submillimter-wave Receiver Technology inEastern Asia, (Seoul, Korea, Jan. 17-18).
Noumaru, J.: 2007, Subaru East Asia Youth Astronomers Seminar,
7th East Asian Astronomy Meeting Symposium, (Fukuoka,
Japan, Oct. 8-12).
Oh, C., Kobayashi, H., VERA group: 2007, VLBI Observationsof H2O Masers in IRAS 06058+2138 with VERA, Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnology, (Sagamihara, Japan, Dec. 3-7).
Ohashi, H., Shibata, H., Ngami, K, Iwai, T., Sasaki, S.: 2007,
Development of a Curved Potential Time-Of-Flight Mass
Spectrometer with Micro- Piezoelectric Element as a Target
Material, Asia Oceania Geosciences Society 4th Annual
Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Ohishi, M., et al.: 2007, Construction of Virtual Observatories
through Global Collaboration and Standardization, UN/ESA/
NASA Workshop on Basic Space Science and the International
Heliophysical Year 2007, (Tokyo, Japan, June 18-22).
Ohishi, M.: 2007, Virtual Observatories in the East Asia - Japan,
China, Taiwan and Korea, Joint European and National
Astronomy Meeting 2007, (Yerevan, Armenia, Aig. 20-25).
Ohishi, M.: 2008, Molecular spectral line surveys and the organic
molecules in the interstellar molecular clouds, IAU Symposium
251, Organic Matter in Space, (Hong Kong, China, Feb. 18-2).
Ohta, I. S., Hattori, M., Chinone, Y., Luo, Y., Hamaji, Y.,
Takahashi, J., Matsuo, H., Kuno, N.: 2007, Astronomical
testing observation in Multi-Fourier transform interferometer:
Aperture synthesis technique and CMB, IRMMW-THz2007,(Cardiff, UK, Sept. 3-7).
Ohta, K., Yabe, K., Iwata, I., Sawicki, M., Akiyama, M., Tamura,N., Aoki, K.: 2007, Evolution of Star-forming Galaxies seenfrom Lyman Break Galaxies at z~5, The 1st Subaru International

II Publications, Presentations073

Conference, Panoramic Views of Galaxy Formation and
Evolution, (Hayama, Japan, Dec. 11-16).
Ohta, M., Tatsuda, S., Hashizume, K., Wada, T., Sumiyoshi, K.,
Otsuki, K., Kajino, T., Koura, H., Chiba, S., Aritomo, Y.: 2007,
Systematic study for the shell effect in the fission fragment
mass distribution ruptured from neutron rich nuclei, 23rd
International Nuclear Physics Conference 2007, (Tokyo, Japan,
June 3-8).
Ohtsuka, K., Yoshikawa, M., Watanabe, J., Hidaka, E.,
Maruyama, H., Kasuga, T.: 2007, Jovian impulses acting upon
the Quadrantids meteor stream, Meteoroids 2007, (Barcelona,
Spain, June 11-15).
Okamoto, T. J.: 2007, Ultra-fine structure of a solar prominenceand discovery of Alfvén wave with Hinode Solar Optical
Telescope, IAU Symposium 247, Waves & Oscillations in
the Solar Atmosphere: Heating and Magneto-Seismology,(Porlamar, Isla de Margarita, Venezuela, Sept. 17-21).
Okamoto, T. J.: 2007, Discovery of Cool Cloud-Like Structuresin the Corona with Hinode/SOT, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Okamoto, T. J.: 2007, Discovery Of Cool Cloud-like Structures In
The Corona With Hinode Solar Optical Telescope, SPD/AAS
Meeting, (Honolulu, Hawaii, USA, May 27-31).
Okamoto, T. J.: 2007, Detection of Coronal Alfvén Waves in a
Solar Prominence with the Hinode Solar Optical Telescope,International CAWSES Symposium, (Kyoto, Japan, Oct. 23-27).
Omukai, K.: 2007, Formation of zero- and low-metallicity stars,
Star Formation, Then and Now, (Santa Barbara, USA, Aug. 13).
Omukai, K.: 2007, Radiative feedback from the first stars and theformation of the second-generation stars, HI Survival throughCosmic Times, (Siena, Italy, June 11).
Omukai, K.: 2007, The formation of stars at very low metallicities,
First Stars III, (Santa Fe, NM, USA, July 16).
Oshima, T., Yamakawa, Y., Kurabayashi, H., Hoshino, A.,
Ishisaki, Y., Ohashi, T., Mitsuda, K., Tanaka, K.: 2007, A HighEnergy Resolution Gamma-Ray TES Microcalorimeter with
Fast Response Time, 12th international workshop on Low
Temperature Detectors, (Paris, France, July 22-27).
Oshima, T.: 2007, ASTE and High Energy Astrophysics, NUSO
Conference on High-Energy vs. Cold Universe, (Nagoya, Japan,
Nov. 14).
Otsuka, M., Tajitsu, A., Hyung, S., Izumiura, H.: 2007, The
Origin and Evolution of the Extreme Metal-Poor Halo Planetary
Nebulae, 10th Origin of Matter and Evolution fo Galaxies,(Sapporo, Japan, Dec. 4-7).
Packham, C. C., Axon, D. J., Hough, J. H., Jones, T. J., Roche, P. F.,
Tamura, M., Telesco, C. M.: 2008, Mid-IR Polarimetry: New
Vistas For SOFIA, AAS Meeting 211, (Austin, TX, USA, Jan.
7-11).
Pyo, T.-S.: 2007, SUBARU Wide Field Imaging Of Near-infrared [Fe II ] And H2 Toward L1551 And XZ / HL Tau Regions, AAS
Meeting 210, (Hawaii, USA, May 27-31).
Rodriguez, J. A. P., Zimbelman, J. R., Kargel, J. S., Tanaka, K.
L., Yamamoto, A., Sasaki, S.: 2008, The Pali Aike Windstreak
Field, Southern Patagonia, Argentina, 39th Lunar and Planetary074

II Publications, Presentations

Science Conference, (League City, Texas, USA, Mar. 10-14).
Saigo, K., Tomisaka, K., Wada, K., Omukai, K.: 2007, The
observational possibility of the rotating first core, Radiativetransfer mini-workshop in Hakone, (Hakone, Japan, Oct.
16-17).
Sakata, S., et al.: 2007, Toward suppression of radiation pressure
nosie in resonant cavities with suspended small mirrors, 7th
Edoardo Amaldi Conference on Gravitational Waves, (Sydney,
Australia, July 8-14).
Sakurai, T., Li, H., Ichimoto, K.: 2007, Response of the Chromosphere and Corona to Emerging Flux, Hinode Science Meeting 7,(Dublin, Ireland, Aug. 21-24).
Sakurai, T.: 2007, Initial Results from Hinode: Optical and X-ray
Observations, Norway-Japan Symposium on Space and Polar
Research, (Tokyo, Japan, May 29-30).
Sakurai, T.: 2007, Response of the chromosphere and corona toemerging flux, Hinode Science Meeting 7, (Dublin, Ireland,Aug. 21-24).
Sakurai, T.: 2008, Large and Small Scale Dynamics in the
Magnetic Activities of the Sun, International Symposium on
Hierarchy and Holism: Bridging Across Different Hierarchies in
Natural Sciences, (Okazaki, Japan, Feb. 21-23).
Sasaki, S., Araki, H., Hanada, H., Namiki, N., Iwata, T., Asari,K., Goossens, S., Ishihara, Y., Ishikawa, T., Kawano, N.,
Kikuchi, F., Liu, Q., Matsumoto, K., Migita, E., Noda,
H., Tazawa, S., Tsubokawa, T., Tsuruta, S.: 2008, Global
topography and gravity field of the moon by SELENE (Kaguya),COE-21 International Symposium, MISASA-III “Origin,
Evolution and Dynamics of the Earth”, (Okayama, Japan, Mar.
22-23).
Sasaki, S., et al.: 2007, Exploration of Lunar Gravity and
Selenodesy by KAGUYA and the Role of VLBI Observation,
7th East Asian Astronomy Meeting Symposium, (Fukuoka,
Japan, Oct. 8-12).
Sasaki, S., et al.: 2007, Simulating the Albedo Heterogeneity of
Rocky Surface of Itokawa, Asia Oceania Geosciences Society
4th Annual Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Sasaki, S., Hiroi, T.: 2008, How Does Space Weathering Dependon the Surface Condition of Airless Bodies (Asteroids, theMoon, and Mercury)?, 39th Lunar and Planetary Science
Conference, (League City, Texas, USA, Mar. 10-14).
Sasaki, S., Ishiguro, M., Hirata, N., Hiroi, T., Abe, M., Abe, S.,
Miyamoto, H., Saito, J.: 2007, Albedo/color heterogeneity
on the surface of rubble pile asteroid Itokawa: evidence forthe space weathering, European Geosciences Union General
Assembly 2007, (Vienna, Austria, Apr. 15-20).
Sasaki, S., Nogami, K., Shibata, H., Iwai, T., Hirai, T., Ohashi,
H.: 2007, Development of a Light-Weight, Large-Area insitu Impact Ionization Dust/Debris Detector, Asia Oceania
Geosciences Society 4th Annual Meeting, (Bangkok, Thailand,
Sept. 30-Aug. 4).
Sasaki, S., Ohashi, H., Hirai, T., Muranaga, K., Iwai, T., Shoji, S.,
Shibata, H., Nogami, K.: 2007, Development of plane-parallel
impact-ionization dust detectors with large aperture, European
Geosciences Union General Assembly 2007, (Vienna, Austria,
Apr. 15-20).

Sasaki, S.: 2007, Origin/Satellite: Discussion in Japanese Group,
Europa - Jupiter Graz Meeting, (Graz, Austria, Apr. 23-24).
Sasaki, S.: 2007, Space Weathering of Mercury in Comparison
with the Moon and asteroids, Asia Oceania Geosciences Society
4th Annual Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Sasaki, T., Yoshida, M., Ohshima, N., Mikami, Y., Okada,N., Koyanao, H., Nagayama, S., Takato, N., Sekiguchi, K.,
Miyashita, A., Uraguchi, F., Yao, Y., Yang, G., Wang, J.-J.:
2007, Collaborative Site Testing in West China, 7th East Asian
Astronomy Meeting Symposium, (Fukuoka, Japan, Oct. 8-12).
Sato, K., Tsuchiya, A., Oshima, T., Yamasaki, N. Y., Morooka, T.:2007, Development of Low Temperature SQUID Gradiometer
Array for Metallic Magnetic Microcalorimeters, 12th
international workshop on Low Temperature Detectors, (Paris,
France, July 22-27).
Sato, M., et al.: 2007, Superbubble Motion Away from the Galactic
Plane Traced by Water Masers in NGC 281 Observed with
VERA, Massive Star Formation: Observations confront theory,(Heidelberg, Germany, Sept. 10-14).
Sato, M., et al.: 2007, Superbubble Motion away from the Galactic
Plane: Astrometry of Water Masers in NGC 281 with VERA,Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technology, (Sagamihara, Japan, Dec. 3-7).
Sato, M., Watanebe, J.: 2007, Exploring Comet-Asteroid
Transition (CAT) Objects from Meteor Showers, Asia Oceania
Geosciences Society 4th Annual Meeting, (Bangkok, Thailand,
Sept. 30-Aug. 4).
Sato, M., Watanebe, J.: 2007, Origin of the outburst of Orionids
2006, Meteoroids 2007, (Barcelona, Spain, June 11-15).
Sato, M.: 2008, Distances and Motions of Galactic Superbubbles
via Water Maser Parallaxes with VERA, International winterschool on the Interstellar Medium 2008, (Ise-Shima, Japan, Feb.
18-22).
Sato, S., Kawamura, S.: 2007, Alignment signal extraction of
the optically degenerated RSE interferometer using wave
front sensing technique, 7th Edoardo Amaldi Conference on
Gravitational Waves, (Sydney, Australia, July 8-14).
Sato, S., Kokeyama, K., Kawamura, S., Ward, R. L., Nishizawa,
A., Chen, Y., Pai, A., Somiya, K.: 2007, Demonstration of
displacement noise free interferometory using bi-directional
Mach-Zehnder interferometer, 7th Edoardo Amaldi Conferenceon Gravitational Waves, (Sydney, Australia, July 8-14).
Sato, S., Kokeyama, K., Kawamura, S., Ward, R. L., Nishizawa,
A., Chen, Y., Pai, A., Somiya, K.: 2007, Displacement noise
free interferometory for gravitational wave detection, 10th
International Conference on Topics in Astroparticle andUnderground Physics (TAUP 2007), (Sendai, Japan, Sept.
11-15).
Sekii, T.: 2007, Early results from Hinode/SOT helioseismology,
SOHO 19/GONG: Seismology of Magnetic Activity,(Melbourne, Australia, July 9-13).
Sekii, T.: 2007, Helioseismology from Hinode, Workshop on
Time-Distance Helioseismology and Helioseismic Holography,(Stanford, CA, USA, Aug. 7).
Sekii, T.: 2007, Hinode Observations, HELAS II International
Conference: Helioseismology, Asteroseismology and MHD

Connections, (Goettingen, Germany, Aug. 20-24).
Sekii, T.: 2007, Initial Analysis of Hinode/SOT Helioseismology
Data, Initial Results from Hinode: Workshop in Memory of
Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Sekii, T.: 2008, First results from the Hinode/SOT helioseismology
programme SDO – HMI/EVE/AIA Science Teams Meeting –2008, (Napa, CA, USA, Mar. 25-28).
Sekimoto, Y.: 2008, Progress of ALMA Band 8(385–500 GHz)
Cartridge, 8th Workshop on Submillimter-wave ReceiverTechnology in Eastern Asia, (Seoul, Korea, Jan. 17-18).
Serizawa, Y.: 2008, A 400–500 GHz Balanced SIS Mixer witha Waveguide Quadrature Hybrid Coupler 8th Workshop on
Submillimter-wave Receiver Technology in Eastern Asia,(Seoul, Korea, Jan. 17-18).
Shibasaki, K., Koshiishi, H., Shimojo, M., Minoshima, S.,
Imada, S., Sakao, T., Hinode team: 2007, Particle Accelerationin the X3 Event on Dec. 13, 2007, AAS Meeting 210, (Hawaii,
USA, May 27-31).
Shibasaki, K.: 2007, Kosugi-san and Nobeyama Solar Radio
Observatory, Initial Results from Hinode: Workshop in Memoryof Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Shibasaki, K.: 2007, Nobeyama Radioheliograph and Radiopolarimeters –Open Data Use–, UN/ESA/NASA Workshop on
Basic Space Science and the International Heliophysical Year2007, (Tokyo, Japan, June 18-22).
Shibasaki, K.: 2007, Particle Acceleration in the X3 Event on Dec.
13, 2007, SPD/AAS Meeting, (Honolulu, Hawaii, USA, May
27-31).
Shimojo, M., Narukage, N., Kano, R., Sakao, T., Tsuneta, S.,
Cirtain, J. W., Lundquist, L. L., Deluca, E. E., Goulub, L.: 2007,
Fine Structures of Solar X-ray Jets, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Shimojo, M., Tsuneta, S., Suematsu, Y., Ichimoto, K.,
Katsukawa, Y., Shimizu, T., Nagata, S.: 2007, The Propertiesof the Ca II/G-band Bright Point around the Penumbra, Hinode
Science Meeting 7, (Dublin, Ireland, Aug. 21-24).
Shimojo, M., Tsuneta, S., Suematsu, Y., Ichimoto, K.,
Katsukawa, Y., Shimizu, T., Nagata, S.: 2007, The Propertiesof the Ca II/G-band Bright Points around the Penumbra,
International CAWSES Symposium, (Kyoto, Japan, Oct. 23-27).
Shimojo, M.: 2007, Fine Structures of Solar X-ray Jets, Initial
Results from Hinode: Workshop in Memory of Takeo Kosugi,(Mitaka, Japan, Apr. 24-27).
Shimojo, M.: 2007, Particle acceleration in the X3.4 event on
December 13, 2006, Hinode Science Meeting 7, (Dublin,
Ireland, Aug. 21-24).
Shimojo, M.: 2007, The Dynamics Of Fine Structures In Solar
X-ray Jets, SPD/AAS Meeting, (Honolulu, Hawaii, USA, May
27-31).
Shimojo, M.: 2007, The Properties of the Ca II/G-band Bright
Points around the Penumbra, International CAWSES
Symposium, (Kyoto, Japan, Oct. 23-27).
Shimojo, M., Narukage, N., Kano, R., Sakao, T., Tsuneta, T.,
Cirtain, J. W., Lundquist, L. L., Deluca, E. E., Golub, L.: 2007,
The Dynamics and Magnteic Enviroments of Solar X-ray Jets

II Publications, Presentations075

observed with Hinode, AGU Fall Meeting, (San Francisco,USA, Dec. 10-15).
Shimojo, M., Narukage, N., Kano, R., Sakao, T., Tsuneta, T.,
Cirtain, J. W., Lundquist, L. L., Deluca, E. E., Golub, L.: 2007,
The Dynamics of Fine Structures in Solar X-ray Jets, AAS
Meeting 210, (Hawaii, USA, May 27-31).
Shiota, D., Kusano, K., Kataoka, R., Asano, E., Inoue, S., Ogino, T.,
Shibata, K.: 2007, Interlocked MHD modeling of the Launching
and Propagation of Coronal Mass Ejections, AGU Fall Meeting,(San Francisco, USA, Dec. 10-15).
Shiota, D., Kusano, K., Miyoshi, T., Nishikawa, N., Shibata, K.:
2007, Three Dimensional Magnetohydrodynamic Simulation ofCoronal Mass Ejections, International CAWSES Symposium,(Kyoto, Japan, Oct. 23-27).
Shirasaki, Y., et al.: 2007, Spectrum Feature of the Underlying
Soft Component of GRB041006, Gamma Ray Burst 2007,(Santa Fe, NM, USA, Nov. 5-9).
Shirasaki, Y., et al.: 2007, Subaru Data Analysis on Japanese
Virtual Observatory, UN/ESA/NASA Workshop on Basic Space
Science and the International Heliophysical Year 2007, (Tokyo,
Japan, June 18-22).
Shirasaki, Y.: 2007, Data Processing for 'SUBARU' Telescopeusing GRID, The 6th IAEA Technical Meeting on Control, Data
Acquisition, and Remote Participation for Fusion Research,(Inuyama, Japan, June 4-8).
Shitov, S. V., Uvarov, A. V., Koryukin, O. V., Bukovski, M.
A., Takeda, M., Wang, Z., Kroug, M., Uzawa, Y., Noguchi,
T.: 2007, Tolerance analysis of THz-range lens-antenna andbalanced SIS mixer, 18th International Symposium on Space
Terahertz Technology, (Caltech, USA, Mar. 21-23).
Shum, C. K., Araki, H., Matsumoto, K., Sasaki, S., Bâki Iz, H.,
Chen, Y. Q., Potts, L.: 2008, Research in Selenodesy Using the
KAGUYA/SELENE Laser Altimeter and Other Data, The 2nd
KAGUYA (SELENE) Science Working Team Meeting, (Tokyo,
Japan, Jan. 15-17).
Sôma, M.: 2007, Occultation by (22) Kalliope and its satellite
Linus, IAU Symp. 248, A Giant Step: From Milli- to Microarcsecond Astrometry, (Shanghai, China, Oct. 15-19).
Suematsu, Y.: 2007, First Results from Solar Optical Telescopeaboard Hinode, Asia Oceania Geosciences Society 4th Annual
Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Suematsu, Y.: 2007, High Resolution Observation of Spiculesin Ca II H with Hinode/SOT, SPD/AAS Meeting, (Honolulu,
Hawaii, USA, May 27-31).
Suematsu, Y.: 2007, High Resolution Observation of Spicules withCa II H Filtergraph, Initial Results from Hinode: Workshop in
Memory of Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Suematsu, Y.: 2007, High resolution observations of spicules with
Hinode/SOT, Hinode Science Meeting 7, (Dublin, Ireland, Aug.
21-24).
Suematsu, Y.: 2007, In-Orbit Optical Performance of Hinode/SOT
in G-band (430 nm) Estimated with Phase Diversity Method,
Initial Results from Hinode: Workshop in Memory of Takeo
Kosugi, (Mitaka, Japan, Apr. 24-27).
Suematsu, Y.: 2007, Optical Performance of the Solar Optical
Telescope aboard HINODE, SPD/AAS Meeting, (Honolulu,

076

II Publications, Presentations

Hawaii, USA, May 27-31).
Suganuma, M., Kobayashi, Y., Gouda, N., Yano, T., Yamada,Y., Takato, N., Yamauchi, M.: 2007, Development of a verysmall telescope for a milli-arcsec space astrometry, IAU Symp.
248, A Giant Step: From Milli- to Micro-arcsecond Astrometry,(Shanghai, China, Oct. 15-19).
Suzuki, T., Chiba, S., Honma, M., Higashiyama, M., Yoshida,T., Umeda, H., Nomoto, K., Kajino, T., Otsuka, T.: 2007,
Spin-Dependent Transitions in Nuclei and Neutrino-Nucleus
Reactions, 2nd FINUSTAR International Conference, (Crete
Island, Greece, Sept. 10-14).
Suzuki, T., Chiba, S., Yoshida, T., Kajino, T., Otsuka, T.: 2007,
Neutrino-nucleus reactions based on recent advances inshell-model calculations, 23rd International Nuclear Physics
Conference 2007, (Tokyo, Japan, June 3-8).
Takahashi, R.: 2007, Operational Status of TAMA300 with
the Seismic Attenuation System (SAS), 7th Edoardo Amaldi
Conference on Gravitational Waves, (Sydney, Australia, July8-14).
Takeda, M., Shan, W., Kojima, T., Uzawa, Y., Fujii, Y., Krong, M.,
Li, J., Shi, S.-C., Wang, Z.: 2008, Development of SIS mixers
using NbN techniques for ALMA Band 10, 8th Workshop
on Submillimter-wave Receiver Technology in Eastern Asia,(Seoul, Korea, Jan. 17-18).
Takeda, M., Shoji, A., Saito, S., Shan, W., Uzawa, Y., Li, J., Shi,
S.-C., Wang, Z.: 2007, Measurement of complex dielectric
constant of MgO substrate in the THz region, 7th Workshop on
Submillimeter-wave Receiver Technologies in Eastern Asia,(Osaka, Japan, Jan. 17-19).
Takeda, M., Shan, W., Uzawa, Y., Li, J., Shi, S. C., Wang, Z.: 2007,
Low-noise waveguide mixers using NbN/AlN/NbN junctions on
MgO substrates for ALMA band 10, 8th European Conference
on Applied Superconductivity, (Brussels, Belgium, Sept. 16-20).
Takeda, T.: 2007, Visualization of Astronomical Many-Particle
Simulation Data in 4-Dimensional Digital Universe Project(4D2U Project), SIGGRAPH 2007, (SanDiego, CA, USA, Aug.
5-9).
Takeda, T., Takahei, T.: 2007, Visualizing Many-Particle
Astronomical Simulations, SIGGRAPH 2007, (SanDiego, CA,
USA, Aug. 5-9).
Takeda, Y.: 2007, Rotational feature of Vega and its impact onabundance determinations, CP#AP Workshop, (Vienna, Austria,
Sept. 10-14).
Tamura, M., Hodapp, K., Suzuki, R., Abe, L., Takami, H., Suto,
H., Guyon, O., Kandori, R., Morino, J., Hashimoto, J.,
Stahlberger, V., Jacobson, S., Yamada, H., Shelton, R., Tavrov,
A., Murakami, N., Nishikawa, J., Hayashi, M., Usuda, T.,
Yamada, T., Nishmura, T.: 2007, HiCIAO and Exoplanet/
Disk Searches on Subaru, Spirit of Bernard Lyot: The Direct
Detection of Planets and Circumstellar Disks in the 21stCentury, (Berkeley, CA, USA, June 4-8).
Tamura, T.: 2007, Fabrication of submicron SIS junction using
i-line stepper, 7th Workshop on Submillimeter-wave ReceiverTechnologies in Eastern Asia, (Osaka, Japan, Jan. 17-19).
Tamura, T.: 2008, Fabrication of ALMA Band8 SIS mixer device
using a new fabrication system and method, 8th Workshop

on Submillimter-wave Receiver Technology in Eastern Asia,(Seoul, Korea, Jan. 17-18).
Tamura, Y.: 2008, The Earth Tide and Measurements of Earth's
Deformation, International Workshop on Accelerator Alignment,(Tsukuba, Japan, Feb. 11-15).
Tanaka, M.: 2008, Japanese Virtual Observatory and Workflow,
OGF22, (Cambridge, USA, Feb. 25-28).
Tanaka, M., Shirasaki, Y., Ohishi, M., Mizumoto, Y., Ishihara,Y., Tsutsumi, J., Machida, Y., Nakamoto, H., Kobayashi,Y., Sakamoto, M.: 2007, Construction of Multiple-Catalog
Database for JVO, Astronomical Data Analysis Software &Systems XVII, (London, UK, Sept. 24-26).
Tanikawa, A.: 2007, Effects of Hardness of Primordial Binaries
on Evolution of Star Clusters, IAU Symp. 246, Dynamical
Evolution of Dense Stellar Systems, (Capri, Italy, Sep 5-9).
Tatematsu, K.: 2007, ALMA and East Asian Research Center, 7th
East Asian Astronomy Meeting Symposium, (Fukuoka, Japan,
Oct. 8-12).
Tatematsu, K.: 2007, East Asia ALMA Regional Center, ALMA
Community Meeting, (Garching, Germany, Sept. 3-4).
Tatsumi, D.: 2007, TAMA300 interferometer development,
10th International Conference on Topics in Astroparticle andUnderground Physics (TAUP 2007), (Sendai, Japan, Sept.
11-15).
Toda, M., Yamamoto, M., Shigeno, Y., Kasuga, T., Abe, S., Higa,
Y., Watanebe, J.: 2007, Invisible persistent trains generated byGeminids, Meteoroids 2007, (Barcelona, Spain, June 11-15).
Tsujimoto, T.: 2007, A New Picture of the Bulge-Disk Connection
Imprinted in Elemental Abundances of Metal-Rich Disk Stars,
Formation and Evolution of Galaxy Disks, (Rome, Italy, Oct.
1-5).
Tsujimoto, T., Kobayashi, N., Yasui, C., Kondo, S., Minami, A.,
Motohara, K., Ikeda, Y., Gouda, N.: 2007, A near-infrared highresolution spectroscopic survey of bulge stars by WINERED,IAU Symp. 248, A Giant Step: From Milli- to Micro-arcsecond
Astrometry, (Shanghai, China, Oct. 15-19).
Tsujimoto, T.: 2007, Evidence of outflow from the Galactic bulge
imprinted in stellar elemental abundances, Formation and
Evolution of Galactic Bulges IAU Symposium 245, (Oxford,
UK, July 16-20).
Tsuneta, S.: 2007, Attempt to Detect Alfvén Waves with Hinode/
SOT, Initial Results from Hinode: Workshop in Memory of
Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Tsuneta, S.: 2007, High-Sensitivity Observations of Quiet Sun
Magnetic Fields by Using both Extreme-Limb and SunCenter Spectro-Polarimetric Data, Initial Results from Hinode:
Workshop in Memory of Takeo Kosugi, (Mitaka, Japan, Apr.
24-27).
Tsuneta, S.: 2007, Hinode A New Solar Observatory in Space,International CAWSES Symposium, (Kyoto, Japan, Oct. 23-27).
Tsuneta, S.: 2007, Hinode/SOT: Current Status, Initial Resultsfrom Hinode: Workshop in Memory of Takeo Kosugi, (Mitaka,
Japan, Apr. 24-27).
Tsuneta, S.: 2007, Initial results from HINODE, IAU Symposium
247, Waves & Oscillations in the Solar Atmosphere: Heatingand Magneto-Seismology, (Porlamar, Isla de Margarita,

Venezuela, Sept. 17-21).
Tsuneta, S.: 2007, Magnetic Landscape of Solar Polar Region Fast
solar wind and flux transport dynamo, Hinode Science Meeting
7, (Dublin, Ireland, Aug. 21-24).
Tsuneta, S.: 2007, Magnetic Landscape of Solar Polar Region with
Solar Optical Telescope Aboard Hinode, SPD/AAS Meeting,(Honolulu, Hawaii, USA, May 27-31).
Tsuneta, S.: 2007, New View of the Sun with Hinode Satellite,
UN/ESA/NASA Workshop on Basic Space Science and theInternational Heliophysical Year 2007, (Tokyo, Japan, June
18-22).
Tsuneta, S.: 2007, New views of the solar surface, Living With aStar Science Workshop, (Boulder, USA, Sept. 10-13).
Tsuneta, S.: 2007, Overview of Hinode mission, Hinode Science
Meeting 7, (Dublin, Ireland, Aug. 21-24).
Ustinov, A. V., Batov, I. E., Jin, X. Y., Shitov, S. V., Koval,
Y., Müller, P.: 2007, Detection of 0.5 THz radiation from
Bi2Sr2CaCu2O8 single crystals, 18th International Symposiumon Space Terahertz Technology, (Caltech, USA, Mar. 21-23).
Uvarov, A. V., Shitov, S. V., Uzawa, Y., Vystavkin, A. N.: 2007,
Tolerance Analysis of THz-range Integrated Lens Antennas,
2007 International Symposium on Antennas and Propagation,(Niigata, Japan, Aug. 20-24).
Uzawa, Y., Sugimoto, M., Kimura, K, Nohara, R., Tanabe, T.,
Ogawa, H., Fujii, Y., Shan, W.-L., Kaneko, K., Kroug, M.,
Shitov, S.: 2007, Near-Field beam measurements of corrugatedhorns for ALMA band 10, 18th International Symposium onSpace Terahertz Technology, (Caltech, USA, Mar. 21-23).
Uzawa, Y.: 2007, Status of band 10 development, 7th Workshop
on Submillimeter-wave Receiver Technologies in Eastern Asia,(Osaka, Japan, Jan. 17-19).
Venn, K., Chutter, A., Irwin, M., Arimoto, N., Aoki, W., Sadakane,
K.: 2007, Does the Globular Cluster Pal 1 have an Extragalactic
Origin?, AAS Meeting 210, (Hawaii, USA, May 27-31).
Wang, Z., Takeda, M., Terai, H., Uzawa, Y.: 2007, Interface
properties of NbN/AlN/NbN tunnel junctions fabricated byreactive dc-magnetron sputtering, 8th European Conference on
Applied Superconductivity, (Brussels, Belgium, Sept. 16-20).
Watanabe, J.: 2007, Activities of parent comets and related meteor
showers, Meteoroids 2007, (Barcelona, Spain, June 11-15).
Watanabe, T.: 2007, Iron Line Ratio Analysis in an Active Region,
SPD/AAS Meeting, (Honolulu, Hawaii, USA, May 27-31).
Watanabe, T.: 2007, Temperature and Desinsity Structures of Solar
Corona –A Test ofDiagnostic Capability of the EIS Instrument
on board Hinode–, Initial Results from Hinode: Workshop in
Memory of Takeo Kosugi, (Mitaka, Japan, Apr. 24-27).
Watanabe, T.: 2007, Fine structures of flaring loops seen in Fe
XIII 263.76 A line, Hinode Science Meeting 7, (Dublin, Ireland,Aug. 21-24).
Watanabe, T.: 2007, New Sunrise of Solar Physics Galvanizedby the Hinode Mission, Asia Oceania Geosciences Society 4th
Annual Meeting, (Bangkok, Thailand, Sept. 30-Aug. 4).
Yabe, K., Ohta, K., Iwata, I., Sawicki, M., Tamura, N., Akiyama,
M., Aoki, K.: 2007, The Stellar Populations of Lyman Break
Galaxies at z~5, The 1st Subaru International Conference,
Panoramic Views of Galaxy Formation and Evolution, (Hayama,

II Publications, Presentations

077

Japan, Dec. 11-16).
Yamada, M.: 2007, 3D Molecular Line Transfer Study ofExtragalactic ISM towards ALMA, Durham Radiative Transfer
Workshop 2007, (Durham, NC, USA, Sept. 14).
Yamada, M.: 2007, Carbon Lines and Chemistry in Multi-Phase
Diffuse Clouds, 3rd ALMA-JT Science Workshop, (Chungli,
Taiwan, Apr. 13-14).
Yamada, M.: 2007, Miilimeter and Submillimeter Line Diagnostics
of AGN Molecular Torus: 3D Radiative Transfer Approach, 3rd
ALMA-JT Science Workshop, (Chungli, Taiwan, Apr. 13-14).
Yamada, M.: 2007, Radiative Transfer and ISM (review), Durham
Radiative Transfer Workshop 2007, (Durham, NC, USA, Sept.
14).
Yamada, M.: 2007, Radiative Transfer Approach to Millimeter andSubmillimeter Molecular Line Dia-gnostics of AGN Molecular
Torus, SPICA Science workshop, (Sagamihara, Japan, May 24).
Yamada, Y., Gouda, N., Yano, T., Kobayashi, Y., Niwa, Y.,
JASMINE Working Group: 2007, JASMINE data analysis,
IAU Symp. 248, A Giant Step: From Milli- to Micro-arcsecond
Astrometry, (Shanghai, China, Oct. 15-19).
Yamada, Y., Gouda, N., Yano, T., Kobayashi, Y., Niwa, Y.,
JASMINE Working Group: 2007, JASMINE –Design andmethod of data reduction–, Formation and Evolution of Galactic
Bulges IAU Symposium 245, (Oxford, UK, July 16-20).
Yamamoto, K.: 2007, Parametric instability of LCGT interferometer, 7th Edoardo Amaldi Conference on Gravitational
Waves, (Sydney, Australia, July 8-14).
Yamamoto, K.: 2007, The current status of the CLIO project, 7th
Edoardo Amaldi Conference on Gravitational Waves, (Sydney,
Australia, July 8-14).
Yamamoto, M., Suzuki, S., Maeda, K., Higa, Y., Toda, M.,
Watanebe, J.: 2007, Invisible persistent trains generated byGeminids, Meteoroids 2007, (Barcelona, Spain, June 11-15).
Yamamoto, T. T., Ichimoto, K., Shinoda, K., Hagino, M.: 2007,
Universal spectropolarimeter, Norikura Henkou Kansokusouti(NHK), 5th Solar Polarization Workshop, (Ascona, Switzerland,
Sept. 17-21).
Yamamoto, T. T., Sakurai, T., Yokoyama, T., Kusano, K.: 2007,
Forecast of the Solar Flare Magnitude from the Photospheric
Magnetic Field Properties, International CAWSES Symposium,(Kyoto, Japan, Oct. 23-27).
Yamauchi, M., Gouda, N., Kobayashi. Y., Tsujimoto, T., Yano,
T., Suganuma, M., Yamada, Y., Nakasuka, S., Sako, N.: 2007,
A Star Image Extractor for the Nano-JASMINE satellite, IAU
Symp. 248, A Giant Step: From Milli- to Micro-arcsecond
Astrometry, (Shanghai, China, Oct. 15-19).
Yamazaki, D. G.: 2007, Effects of a Primordial Magnetic Field on
Low and High Multipoles of, PASCOS 07, (London, UK, July
2-7).
Yamazaki, D. G.: 2007, Effects of Primordial Magnetic Field on
CMB and Density Field, DARK 2007, (Sydney, Australia, Sept.
24-28).
Yamazaki, D. G.: 2007, Effects of Primordial Magnetic Field
on Early Universe, Int. Symp. on Cosmology and Particle
Astrophysics, (Taipei, Taiwan, Nov. 13-15).
Yamazaki, D., Ichiki, K., Kajino, T., Mathews, G. J.: 2007,

078

II Publications, Presentations

Constraint on Cosmological Magnetic Field from Likelihood
Analysis, PASCOS 07, (London, UK, July 2-7).
Yano, T., Gouda, N., Kobayashi, Y., Yamada, Y., Tsujimoto,T., Suganuma, M., Niwa, Y., Yamauchi, M.: 2007, Space
Astrometry –JASMINE–, IAU Symp. 248, A Giant Step: FromMilli- to Micro-arcsecond Astrometry, (Shanghai, China, Oct.
15-19).
Yano, T., Gouda, N., Ueda, H. Koyama, H., Kan-ya, Y., Taruya,
A.: 2007, Kinematical and Dynamical Structure of the Galactic
Bulge, Formation and Evolution of Galactic Bulges IAU
Symposium 245, (Oxford, UK, July 16-20).
Yokochi, K., Nishikawa, J., Murakami, N., Abe, L., Kotani, T.,
Tamura, M., Kurokawa, T., Tavrov, A., Takeda, M.: 2007,
Precise wavefront correction with unbalanced nulling interferometer for direct detection of exo-planet, The 7th Pacific Rim
Conference on Lasers and Electro-Optics, (Seoul, Korea, Aug.
26-31).
Yoshida, M., Yanagisawa, K., Shimizu, Y., Okita, K., Nagayama,S., Toda, H., Ohta, K., Kawai, N.: 2007, OAOWFC: Okayama
Astrophysical Observatory NIR Wide-Field Camera, Gamma
Ray Burst 2007, (Santa Fe, NM, USA, Nov. 5-9).
Yoshida, M.: 2007, Progress Report of East Asian 2m Class
Telescope Collaboration, 7th East Asian Astronomy Meeting
Symposium, (Fukuoka, Japan, Oct. 8-12).
Yoshida, M.: 2007, Progress Report of the Kyoto University 3.8m
Telescope, The 2nd Annual Workshop on Extrasolar Panet
Survey, (Lijiang, China, May 14-20).
Yoshida, N.: 2007, Formation of primordial protostars, First Stars
III, (Santa Fe, NM, USA, July 16).
Yoshida, N.: 2007, Formation of the First Stars in the Universe,
10th Origin of Matter and Evolution fo Galaxies, (Sapporo,
Japan, Dec. 4-7).
Yoshida, N.: 2007, Second-Generation Star Formation in ProtoGalaxies, Star Formation Through Cosmic Time, (Santa Baraba,
USA, Aug. 17).
Yoshida, T.: 2007, Constraint on neutrino energy spectra fromsupernova light-element synthesis, 23rd International Nuclear
Physics Conference 2007, (Tokyo, Japan, June 3-8).
Yoshida, T.: 2007, Neutrino fravor mixing in supernova
nucleosynthesis, 23rd International Nuclear Physics Conference
2007, (Tokyo, Japan, June 3-8).
Yoshida, T.: 2007, Supernova Neutrino Nucleosynthesis, GDR
Neutrino, (Bordeaux, France, Oct. 25-26).
Yoshizumi, C., Mizutani, A., Okyudo, M., Watanabe, K., Tanaka,
H., Otani, M., Ozawa, T., Ono, T., Agata, H., Nakane, M.,
Hirai, A., Horaguchi, T.: 2007, New prospects for Public
Astronomical Observatory Network (PAONET), 7th East Asian
Astronomy Meeting Symposium, (Fukuoka, Japan, Oct. 8-12).