Cover Caption
Lunar topographic map derived from KAGUYA laser altimeter LALT (NAOJ/JAXA/SELENE).
South Pole-Aitken basin is spread over the lunar far side.

Postscript
EditorPublisher

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Publications Committee
MIYOSHI, Makoto
IMANISHI, Masatoshi
UEDA, Akitoshi
OE, Masafumi
KUDO, TakahiroSÔMA, Mitsuru
HANAOKA, Yoichiro
National Institutes of Natural Sciences

National Astronomical Observatory of Japan
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Annual Report of the
National Astronomical Observatory of Japan

Fiscal 2008

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Shoken MIYAMA
Director General
National Astronomical Observatory of Japan

Preface

I Scientific Highlights April 2008 – March 2009

001

II Publications, Presentations
1

Refereed Publications

056

2

Publications of the National Astronomical Observatory of Japan

069

3

Report of the National Astronomical Observatory of Japan

069

4

Conference Proceedings

069

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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 2008

P R E F A C E

Shoken MIYAMA
Director General of NAOJ

We are pleased to present the Annual Report of the
National Astronomical Observatory of Japan (NAOJ) for
fiscal 2008.
This year marked the 20th anniversary of theestablishment of NAOJ, and we held a commemorative
ceremony in November 2008. For the last 20 years, manyobservation facilities (such as Subaru Telescope) havebeen completed and they are now achieving remarkable
results.
Over the last two decades, there were various findings
in astronomy that brought us new insights and contributed
to astronomical advancement. In 1995, researchers of
Switzerland discovered a planet circling a star outside thesolar system incidentally when observing a primary star.
It turned out that this planet is orbiting around Pegasus 51
in an about four-day period and has a mass roughly a halfof Jupiter’s mass. Though the observed planetary system
is quite different from our solar system, this discovery
marked the beginning of similar observations which led
to discoveries of more than 300 planets.
After this discovery, astronomers began to focus on
three major targets:(1) Direct imaging of planets outside the solar system;(2) Exploration of the origin of diverse solar systems andreconstruction of conventional planet formation theory;and(3) Search for life in planets outside the solar system.
In connection with the target (1), a Canada-US

research team announced that they identified threepotential planets around a primary star using the Gemini
telescope and W.M. Keck Observatory in Hawaii, andfound out that these potential planets are undoubtedly
orbiting around the primary star by comparing two
images taken this time and a few years ago. However, it
seems to be difficult to estimate the mass of the potential
planets from pictures and thus it is still controversial
whether the mass of the potential planet is less than 13
times the Jupiter’s mass, which is regarded as an essential
qualification for a “planet” (the definition of planet
defined by AIU does not apply to planets outside the solar
system). Subaru Telescope will also start observation
with advanced AO (Adaptive Optics) and HiCIAO (HighContrast Instrument for the Subaru next generation
Adaptive Optics: a new stellar coronagraph) aiming for
direct observation of planets outside the solar system.
For the target (2), researchers are actively working
on theoretical studies to investigate the diversity of planetsand their formation process. In theoretical simulation,
more detailed calculation has become possible. The
GRAPE system was a special-purpose computer system
for astrophysical many-body simulations at the beginning,but it has evolved to a new general-purpose system called
GRAPE-DR. It is expected that this new system will
enable us to study planet formation under a wide range ofinitial conditions by performing calculation of N bodies
around the Sun.

Meanwhile, initial conditions of planetary formation
may be clearly defined by ALMA (Atacama Large
Millimeter/submillimeter Array) under construction in
Chile. ALMA is capable of analyzing details of a gas disk
(primordial solar system disk) formed around a youngstar in a nearby star- forming region. By performing
numerical simulation using the initial conditions derived
from the structure of a gas disk, we may be able to figureout the formation process of planets in our solar systemand the diversity of planetary systems.
It has been five years since the start of the ALMA
Project, which will be completed over eight years. At
the construction site in Chile, test observations havebeen conducted with antennas delivered from Japan, andthe Japanese antennas proved their high performanceand capability. As for other ALMA subsystems, we
successfully developed a submillimeter receiver called“Band 10” covering the highest frequency band in
ALMA, and confirmed that it meets extremely highrequirements of ALMA. This achievement proved thatthe receiver developed by NAOJ has the world’s highest
capability in this frequency band.
The target (3) “Search for life in planets outside thesolar system” is a medium-term objective in the future.
Even if Subaru Telescope could obtain direct images ofsome planets outside the solar system with its advanced
equipment, such images would be limited to those ofgas-giant planets with the size of Jupiter because small
rocky stars like the earth are difficult to be observed due
to its darkness. On the other hand, indirect observationof habitable planets may become possible by introducing
a high-resolution spectroscope. Generally speaking, incase of a Sun-like star, habitable planets (where a large
amount of liquid water exists) are supposed to have orbits
in a distance equivalent to the distance from the Sun to
the Earth. If they are in such a distant region, current
spectroscopes are unable to detect oscillations of thecentral star. In case of an M-type star (whose mass is lessthan a half of the Sun) with surface temperature much
lower than that of the Sun, its habitable zone would bemuch closer to the central star. If there is an Earth-likeplanet within such a close habitable zone, oscillations of
the central star would be larger due to closer distance andsmaller mass ratio between the central star and the planet.
Given this, if there is a habitable planet around an M-typestar, it may be indirectly observed by Subaru Telescope.

Furthermore, if any future 30-meter telescope (suchas TMT) can successfully observe a habitable planet
blocking the front of the central star, we may be able toanalyze atmospheric components of the planet: oxygen
molecules suggest the existence of plants, and methane
suggests the existence of animals. We expect that great
mysteries of mankind will be solved within the next 10
years.
To address these big challenges, there is nothing more
important than nurturing young researchers. NAOJ is
opening positions to researchers every year. Researches
are employed through open recruitment from the public or
through recommendation from each project, and currently
about 50 researchers are working at NAOJ. And we arealso providing research guidance for many graduate
students (currently 50 students are accepted) mainly fromthe Graduate University for Advanced Studies. We hopesome of these students will be astronomers who work on
the astronomical hottest themes that are now earnestly
explored by researchers all over the world, such asplanetary formation, planetary exploration, and search forlife in the universe.
Compared to last year, this year’s report contains
a lot more achievements in observational astronomy,
theoretical astronomy, equipment development, andengineering development focused on research targets
other than those listed above. Astronomy has continuously
made enormous and rapid progress. We appreciate yourcontinued support for the growth of astronomy and ouractivities.

Shoken MIYAMA
Director General of NAOJ

I Scientific Highlights(April 2008 – March 2009)

01 Vega's Rotational Velocity Determined from Spectral Line Profiles

TAKEDA, et al.

003

02 Observations of 1999 YC and the Breakup of the Geminid Stream Parent

KASUGA, JEWITT

004

Systematic infrared 2.5 – 5 μm spectroscopy of nearby ultraluminous
03 infrared galaxies: Buried AGNs as a function of galaxy infrared
luminosity

IMANISHI, et al.

005

Nobeyama Millimeter A r ray HCN(J = 1 – 0) and HCO + (J = 1 – 0)
observations of luminous infrared galaxies: The final sample

IMANISHI, et al.

006

05 Same-Beam VLBI Observations in SELENE (Kaguya)

LIU, et al.

007

06 Formation Scenario for Wide and Close Binary Systems

MACHIDA, et al.

008

04

07

Magnetic Field Configuration at the Galactic Center Investigated by
Wide Field Near-Infrared Polarimetry

NISHIYAMA, et al.

009

08

Interstellar Extinction Law toward the Galactic Center: V, J, H, and KS
Bands

NISHIYAMA, et al.

010

09

Evolution of the Anemone Active Region NOAA 10798 and the Related
Geo-Effective Flares and CMEs

ASAI, et al.

011

10

Strongly Blueshifted Phenomena Observed with Hinode/EIS in the 2006
December 13 Solar Flare

ASAI, et al.

012

ISHII, et al.

013

HANAOKA014

ARAI, et al.

015

Theoretical and Observational Studies Using Hinode of the MagneticField Emergence into the Solar Atmosphere

MAGARA016

15 Young Brown Dwarfs in the Core of the W3 Main Star-Forming Region

OJHA, et al.

017

16 Exoplanet Detection with Polarimetry

TAMURA, et al.

018

17 Achievement of the CLIO target sensitivity at room temperature

TATSUMI, et al.

019

HONDA, et al.

020

YANO, et al.

021

HATSUTORI, et al.

022

YOSHIDA, et al.

023

KUNO, et al.

024

KUSAKABE, et al.

025

SAITO, et al.

026

SAITO, et al.

027

MURAKAMI, et al.

028

11 Exploring the substellar temperature regime down to ~550 K
12High-Precision Correction of the Instrumental Polarization for HighLevel Polarimetry of the Sun

13 Sensitivity improvement of gravitational wave detector TAMA300
1418

Detection of water ice grains on the surface of the circumstellar disk
around HD 142527

19 Small-JASMINE (Small Satellite with 30 cm-class telescope)
20 Development of Very Small Astrometry Satellite: Nano-JASMINE
21

Neutrino-Nucleus Reaction Cross Sections for Light Element Synthesis
in Supernova Explosions

22 Central Spiral Structure of Molecular Gas in Maffei 2
23

Near-Infrared Imaging Polarimetry of M42: Aperture Polarimetry of
Point-like Sources

24 Infrared Imaging Polarimetry of S106 in Cygnus
25

Discovery of the Multiple-Core Systems toward Cluster-Forming
Regions

26 Four-Quadrant Phase Mask Coronagraph with a Jacquinot-Lyot Stop001

27 An Eight-Octant Phase-Mask Coronagraph
28 Variation of the Subhalo Abundance in Dark Matter Halos

029

ISHIYAMA, et al.

030

29

Tycho's Supernova is of Type Ia ~ Super explosion in 16th century caught
by Subaru in 21st century ~USUDA, et al.

031

30

Supernova Remnant Cassiopeia A: Decoding Light to Uncover the
Mystery of its Birth

USUDA, et al.

032

31 Detections of Strong Ionizing Radiation from High-redshift Galaxies

IWATA, et al.

033

32 Okayama Astrophysical Observatory has discovered ten exoplanets

SATO, et al.

034

WATANABE, et al.

035

NIWA, et al.

036

33 Fe XIII Density Diagnostics in the EIS Observing Wavelengths
34 Laser interferometric high-precision geometry monitor for JASMINE
35

Three-dimensional Simulation of Magnetized Cloud Fragmentation
Induced by Nonlinear Flows and Ambipolar Diffusion

KUDOH, BASU

037

36

How was the mushroom-shaped GW 123.4 – 1.5 formed in the Galactic
disk?

BAEK, et al.

038

37

Development of a hybrid N-body simulation code for planet formation
process that can handle number of large particles

OSHINO, MAKINO

039

38

Wide-Field Infrared Imaging Polarimetry of the NGC 6334 Region: A
Nest of Infrared Reflection Nebulae

HASHIMOTO, et al.

040

39

New Constraint on Radiative Decay of Long-lived Particles with New
4He Photodisintegration Data and Primordial 6Li Problem

KUSAKABE, et al.

041

40

Production mechanism of circular polarization in the ORION BN/KL
region: Near-infrared circular polarimetry by SIRPOLFUKUE, et al.

042

HAYAKAWA, et al.

043

42 Necessary conditions for super-integrability of Hamiltonian systems

YOSHIDA044

43 Trojan Stars near the Galactic Center

FUJII, et al.

045

41 New nuclear cosmochronometer for supernova neutrino process44

Detection of Fluorine in the Halo Planetary Nebula BoBn1: Evidence Fora Binary Progenitor StarOTSUKA, et al.

046

45

Project Milkyway: Shock-Induced Starburst at a Collision Interface
during the First Encounter of Interacting Galaxies

SAITOH, et al.

047

YAMAZAKI, et al.

048

47 Coronal Plasma Motions near Footpoints of Solar Active Region Loops

HARA, et al.

049

48 Subaru Witnesses the Assembly of Distant Clusters 8 Billion Years Ago

TANAKA, KODAMA050

IZUMIURA, et al.

051

YOSHIDA, et al.

052

ARAKI, et al.

053

NISHIKAWA, et al.

054

TAVROV, et al.

055

46 Limit of primordial magnetic field from the matter power spectra

49 Evidence for a Companion to BM~Gem, a Silicate Carbon Star
50

Discovery of strange filamentary structures (“fireballs”) around a merger
galaxy in the Coma cluster of galaxies

51 Lunar Global Topographic Map by the KAGUYA Laser Altimetry
52

Precise wavefront correction with an unbalanced nulling interferometerfor exo-planet imaging coronagraphs

53 TCP-AIC: Tandem common-path achromatic interfero-coronagraph

002

MURAKAMI, et al.

Vega’s Rotational Velocity Determined from Spectral Line Profiles
TAKEDA, Yoichi, KAWANOMOTO, Satoshi, OHISHI, Naoko(NAOJ)

spectroscopic result (~160 km s −1 ; [3]), while it issignificantly discrepant from the conclusions of recent
interferometric determinations (~270 km s−1; [4, 5]).
The complete procedures of our analysis and in-depth
discussions of the results are described in [7].
1.005
Ca I 6162.173
Normalized flux

Although Vega (A0V) has long been well known
for its sharp-line nature with a low projected rotational
velocity (ve sin i ~ 20 km s−1), we now believe that it is a
rapidly rotating star seen nearly pole-on. This evidencecame from studying the characteristic flat-bottom profilesof spectral lines, which were first discovered by [1] basedon the ultra-high S/N spectrum and successively analyzed
in detail by [2] and [3] to determine (ve, i) separately,
since they may contain information on rotation-induced
gravity darkening. Furthermore, this fact has recently
been confirmed also by interferometric observations ([4],[5]), by which the rotation-induced darkening on thestellar disk may be directly studied.
Unfortunately, from a quantitative point of view,
consensus has not yet been reached regarding how
fast Vega is actually rotating, since the (v e, i) results
derived so far do not necessarily agree, which diverge
into low scale ve (~160 – 170 km s−1; [3]) and high scaleve (~250 – 270 km s−1; [4, 5]). In order to shed light on
this confusing situation while establishing its absoluterotational velocity independently by ourselves, we
decided to carry out an extensive line profile study basedon the very high- S/N (~1000 – 3000) and high-resolution(R ~ 100000) spectrum data we have recently published([6]).
Regarding the modeling of a rapidly-rotating star, we
made the following assumptions:(1) Point-mass potential (Roche model).
(2) Axially-symmetric uniform rotation.
(3) Stellar shape of equipotential surface.
(4) Local Teff depends upon geff as Teff ∝ gβeff , (β ~_ 0.25).
A total of six model parameters are involved in ourmodeling: M (mass), [X/H] (metallicity), ve (equatorial
rotation velocity), i (inclination angle), Rp (polar radius),
and T eff,p (polar effective temperature). However, we
could reduce the number of degrees of freedom to one(only ve) by adequately assuming M (2.3 M) and [X/H](−0.5 dex), by the constraint of v e sin i = 22 km s −1 (areasonable value seen from recent determinations) and by
the requirement of absolute spectral energy distribution(SED), resulting in a sequence of candidate models [i(ve),Rp(ve), Teff,p(ve)] parameterized by ve.
Then, by comparing the observed profiles of carefully
selected sufficiently weak lines with the theoreticalprofiles (computed for various ve; see, e.g., Figure 1),
we determined the best-fit ve value for each line. Finally,
the best solution was concluded to be ve = 175 km s−1,
which further gives i = 7 °. 2, Rp = 2.52 R, and Teff,p =9867 K. Comparing these with the results of the previous
studies, we see that our ve solution is near to Hill et al.’s

1ve = 275 km s-1
ve = 225 km s-1

0.995

0.99

0.985

ve = 125 km s-1

ve = 175 km s-1-1
rigid rotation (vesin i = 22 km s )-0.50Δλ (Å)

0.5

Figure 1: Example of line-profile fitting. Symbols: observed
profile; lines: computed profiles with different ve.

References[1] Gulliver, A.F., et al.: 1991, ApJ, 380, 223.
[2] Gulliver, A.F., et al.: 1994, ApJL, 429, L81.
[3] Hill, G., et al.: 2004, in The A-Star Puzzle (Proc. IAU Symp.
224), ed. J. Zverko, J. Žižňovský, S. J. Adelman, W. W. Weiss(Cambridge: Cambridge University Press), 35.
[4] Peterson, D.M., et al.: 2006, Nature, 440, 896.
[5] Aufdenberg, J.P., et al.: 2006, ApJ, 645, 664 (erratum: 651,
617).
[6] Takeda, Y., et al.: 2007, PASJ, 59, 245.
[7] Takeda, Y., et al.: 2008, ApJ, 678, 446. 1.

I Scientific Highlights

003

Observations of 1999 YC and the Breakup of the Geminid Stream Parent
KASUGA, Toshihiro
				(NAOJ)		

Apollo asteroid 1999 YC may share a dynamical
association with the Phaethon-Geminid stream complex.
Here, we present photometric observations taken to
determine the physical properties of 1999 YC.
The object shows a nearly neutral reflection spectrum,
similar to but slightly redder than related objects 3200
Phaethon and 2005 UD (Fig. 1). Assuming an albedo
equal to 3200 Phaethon’s we find that the diameter is 1.4+/−0.1 km. Time-resolved broad-band photometry yields a
double-peaked rotational period of 4.4950+/− 0.0010 hr
while the range of the lightcurve indicates an elongatedshape having a projected axis ratio near 1.9:1 (Fig. 2).
Surface brightness models provide no evidence of lasting
mass loss of the kind seen in active short period cometary
nuclei [1].
An upper limit to the mass loss is set at about 0.001
kg/s, corresponding to an upper limit on the fraction of
the surface that could be sublimating water ice of 0.001.
If sustained over the 1000 yr age of the Geminid stream,
the total mass loss from 1999 YC (3e7 kg) would be small
compared to the reported stream mass (1e12 – 1e13 kg),suggesting that the stream is the product of catastrophic,
rather than steady-state, breakup of the parent object [1].

JEWITT, Dave
(IfA/University of Hawaii)

Figure 1: Color plots of V − R vs. B − V for PGC and near-Earthasteroids within various Tholen taxonomic classes.

Figure 2: Rotational phase vs. absolute red magnitude variation of1999 YC observed on UT 2007 October 4, 18, and 19.
mR(1, 1, 0) is phased to the double-peaked rotational
period of Prot = 4.4950 ± 0.0010 h.

Reference[1] Kasuga, T., Jewitt, D.: 2008, AJ, 136, 881.

004

I Scientific Highlights

Systematic infrared 2.5 – 5 μm spectroscopy of nearby ultraluminous
infrared galaxies: Buried AGNs as a function of galaxy infrared luminosity
IMANISHI, Masatoshi
			(NAOJ) 		

ONAKA, Takashi

OI, Nagisa(University of Tokyo)(GUAS/NAOJ)

NAKAGAWA, Takao, OHYAMA, Yoichi, SHIRAHATA, Mai, WADA, Takehiko(ISAS/JAXA)

Ultraluminous infrared galaxies (ULIRGs) radiate
the bulk of their large luminosities (>1012 L) 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
portion of the universe.
Since AGN activity is spatially very compact, it caneasily be buried (= obscured in virtually all directions)in dusty ULIRG’s cores. Unlike an AGN surrounded bytorus-shaped dusty medium, which is easily detectablethrough optical spectroscopy, such buried AGNs are very
difficult to find. However, detecting buried AGNs andestimating their energetic role are the most important
issue in the current ULIRG study. For this purpose,observations at wavelengths of low dust extinction arenecessary, and infrared 3 – 4 µm (rest-frame) spectroscopy
is an effective means. First, PAH (polycyclic aromatichydrocarbon) emission features, found at 3.3 µm (restframe), are detected in starburst galaxies, but not in
AGNs, because of the destruction of PAHs. Hence, thepresence or 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 spatiallywell mixed, there is an upper limit for the optical depthof dust absorption features found at 3 – 4 µm, while
it can be arbitrarily large in a buried AGN, where theenergy source is more centrally concentrated than thesurrounding dust [1].
Using the Subaru telescope, we have so far performed
systematic infrared 2.8 – 4.1 µm spectroscopy of ULIRGs
at z < 0.15, and found luminous buried AGN signaturesin a significant fraction of the observed ULIRGs[1]. AKARI satellite has spectroscopic capability at
2.5 – 5 µm, unaffected by Earth atmosphere, as well as
sufficient sensitivity to obtain high quality spectra of
ULIRGs at z < 0.3 in a short exposure time. By extending
our study to more distant ULIRGs at z > 0.15 (Figure1), many ULIRGs with higher infrared luminosities areincluded. We can thus investigate the detected buried
AGN fraction as a function of galaxy infrared luminosity.
We found that with increasing galaxy infrared luminosity,buried AGNs become relatively important energetically,
but the remaining star-formation-originating luminosities
are also higher (i.e., a star formation rate is higher andmore stars will be formed). Buried AGNs can have aparticularly strong feedback to the surrounding gas anddust in host galaxies. Our results may observationally
support the widely-proposed AGN feedback scenario as
the origin of the galaxy downsizing phenomenon [2],where more massive galaxies with currently larger stellar
masses have finished their major star-formation in an
early cosmic age on a shorter time scale.

Figure 1: Examples of AKARI 2.5 – 5 μm spectra of ULIRGs at
z = 0.15 – 0.3. All ULIRGs show low-equivalent-width
PAH emission and/or strong dust absorption features,
suggesting that buried AGNs are energetically important.
The 3.05 μm absorption feature is due to ice-covered
dust grains. Dashed lines mean continuum levels.
Dotted lines indicate the wavelength range where the3.05 µm ice absorption feature is strong. HII, LI meanULIRGs optically classified as HII-regions and LINERs,
respectively.

References[1] Imanishi, M., et al.: 2006, ApJ, 637, 114.
[2] Imanishi, M., et al.: 2008, PASJ, 60, S489.

I Scientific Highlights005

Nobeyama Millimeter Array HCN(J =1–0) and HCO+(J =1–0)
observations of luminous infrared galaxies: The final sample
IMANISHI, Masatoshi, NAKANISHI, Kouichiro,
			(NAOJ) 			

Luminous infrared galaxies radiate veryl a rg e l u m i n o s i t i e s ( > 1 0 11 L  ) a s i n f r a r e d d u s temission, suggesting that powerful energy sources(starburst and/or AGN) are present, surroundedby dust. Unlike AGNs obscured by torusshaped dusty medium, putative AGNs in LIRG’s
nuclei are likely to be obscured by a large amount of
dust and gas in all directions (= buried), making theidentification of AGNs difficult.
In an AGN, X-ray emission (E > 2 keV) is strong
and an emission surface brightness is high, compared
to a starburst. In the case of a buried AGN at a LIRG’s
nucleus, we may be able to detect these AGN signatures,
through the effects to the surrounding gas and dust. In
fact, observationally, the brightness-temperature ratiosof HCN(J =1 – 0) and HCO +(J =1 – 0) emission lines at
λ ~ 3.4 mm (ν ~ 89 GHz) are different between weaklyobscured AGN-dominated galaxy nuclei and starburst
galaxies. Through the systematic observations of
LIRGs, using the Nobeyama Millimeter Array (NMA),
we have found that LIRGs with luminous buried
AGN signatures in infrared spectra tend to show highHCN(J =1 – 0)/HCO + (J =1 – 0) brightness-temperature
ratios, as seen in weakly-obscured AGNs. However, oursample of buried AGN candidates has been limited tosources with very high infrared luminosities (>1012 L),so that a scenario without invoking an AGN (e.g.,different molecular gas properties in galaxies withdifferent luminosities) has been proposed to explain thehigh ratios.
In this paper, we have observed four LIRGs (fivenuclei) of moderate infrared luminosities (<1012 L), withor without buried AGN signatures at other wavelengths(Figure 1), and confirmed that those with AGN signatures
still show high ratios (Figure 2), reinforcing that theburied AGN scenario (not different molecular gas
properties scenario) is at work [1]. The high ratios could
be explained by an HCN abundance enhancement in an
AGN, due to strong X-rays, or infrared radiative pumpingof HCN molecules by hot dust heated by an AGN (=a high emission surface brightness energy source).
Sophisticated theoretical models are needed to properlyinterpret our observational results.
Reference[1] Imanishi, M., et al.: 2009, AJ, 137, 3581.

006

I Scientific Highlights

TAMURA, Yoichi

PENG, Chih-Han(Univ. of Tokyo/NAOJ)(GUAS/NAOJ)

Figure 1: Example spectra of LIRGs around HCN(J =1–0) andHCO+(J =1–0) lines, obtained with NMA.

Figure 2: Filled squares: weakly-obscured AGN-dominated galaxy
nuclei. Open circles: starburst galaxies. AGNs distributeat the upper part, compared to starbursts. Filled stars:
LIRGs. Large filled stars with objects name: LIRGs
observed this time. LIRGs with luminous buried AGN
signatures at other wavelengths tend to distribute at theupper part occupied by AGN-dominated galaxy nuclei.

Same-Beam VLBI Observations in SELENE (Kaguya)
LIU, Q., KIKUCHI, Fuyuhiko, GOOSSENS, S., MATSUMOTO, Koji, HANADA, Hideo, PING, J, SHI, X.
TAMURA, Yoshiaki, HARADA, Yuji, ASARI, Kazuyoshi, TSURUTA, Seiichi, ISHIKAWA, Toshiaki
KAWANO, Nobuyuki, ISHIHARA, Yoshiaki, NODA, Hirotomo, SASAKI, Sho, IWATA, Takahiro, NAMIKI, Noriyuki(NAOJ)m (1 ps) RMS. In addition, the DPD for each baseline
was estimated separately before and after 11 UT, thefluctuations have no jump at 11 UT as shown in Fig. 2(b).
The closure DPD among the three baselines, i.e., the sumof DPD of (IS-MZ)+ (MZ-IR)+ (IR-IS) shown in Fig.
2(a) was also calculated. As shown in Fig. 2(c), it wasvery small, less than 0.001 m (3 ps). Considering one
ambiguity at S-band corresponds to 0.136 m in DPD, it isconfirmed that the DPD has been successfully estimated.
We also performed the orbit determination of Rstar
and Vstar using the GEODYN II software. The orbit
errors were evaluated by overlap analysis, where orbit
differences were computed between two overlapping arcs.
Orbit consistency was greatly improved by including
the VLBI data. Without VLBI data, orbit consistency
for Rstar is 18.01 m, and that for Vstar is 75.26 m. WithVLBI data, the consistency was 2.79 m for Rstar and10.48 m for Vstar. In addition, the precise VLBI data havebeen used to improve the lunar gravity field model.

Figure 1: Correlation phase fluctuations of Rstar and Vstar at S1,
S2, S3 and difference between Rstar and Vstar.


IS-MZ

Closure DPD
MZ-IR

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IR-IS

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

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





IS-MZ
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

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2008-0513

(b) Fluctuation of DPD

Closure DPD (m)(a) DPD

Separation angle (deg)DPD (m)

Fluctuation of DPD (m)SELENE (Kaguya) was successfully launched on
Sep.14, 2007. It consists of a three-axis stabilized Mainsatellite and two small spin stabilized satellites, called
Rstar and Vstar. Rstar relays the Doppler signal between
the main satellite and ground station (4-way Doppler)
for the world’s first direct measurement of the gravity
field on the far side of the Moon. The differential VLBI
between Rstar and Vstar are used to determine the gravity
field of the Moon precisely, especially near the limb
region and for the low degree coefficients of the sphericalharmonics.
Rstar and Vstar only transmit three carriers (S1:2212, S2: 2218, S3: 2287 MHz) in S-band and one carrier(8456 MHz) in X-band; the differential phase delay(DPD) between Rstar and Vstar was obtained from therelation between correlation phase and frequency of thefour carriers. In this case, the differential correlation
phase at each frequency has to be estimated without the
2π ambiguity. This imposes strict conditions such as theerror of the correlation phase must be lower than 4.3 deg
rms. To resolve the 2π ambiguity, we have mainly usedsamebeam differential VLBI, in which Rstar and Vstar
are observed simultaneously with the main beam of thereceiving antennas.
Figure 1 shows the correlation phase fluctuations ofRstar and Vstar and their differences at S1, S2 and S3.
The separation angle was between 0.04 to 0.052 deg.
The integral time is 30 seconds and long-time trends,
which were mainly attributed to the error of the a priori
orbit, were removed by fitting 9th order polynomials.
The correlation phase fluctuations of Rstar and Vstar
with amplitude of about 10 deg are mainly caused by theatmosphere and ionosphere, they are very similar because
the propagation paths from Rstar and Vstar to the groundstations are nearly the same. In addition, the profiles ofphase fluctuations at S1, S2 and S3 are also very similar
because the difference in receiving frequencies is notlarge. These fluctuations were reduced to a low level bydifferencing the correlation phases of Rstar and Vstar
as shown in Fig. 1. The differences between correlation
phase fluctuations of Rstar and Vstar at S1, S2 and S3
were 0.99, 1.00, 0.83 deg RMS, respectively, which
satisfied the condition for obtaining DPD.
Figure 2(a) shows S-band DPD for three baselines,
Ishigaki-Mizusawa, Mizusawa-Iriki and Iriki-Ishigaki.
The separation angle is between 0.04 to 0.09 deg. The
fluctuations of DPD for the three baselines after removing
long-time trends by fitting 9th order polynomials areshown in Fig. 2(b). They were very small, about 0.0003









(d) Separation angle

















Time (hour)

Figure 2: (a) Differential phase delay, (b) their fluctuations, (c)closure phase delay, and (d) separation angle.
Reference[1] Liu, Q., et al.: 2009, J. Geod. Soc. of Japan, 55, 243.

I Scientific Highlights

007Formation Scenario for Wide and Close Binary Systems(Kyoto University)(i.e., the epoch of first core formation) evolve to a widebinary system, while the model showing fragmentation
at the higher density (i.e., the epoch of the second coreformation) evolve to a close binary system.
= 5 [km s-1]

= 3 [km s-1]
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25

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Figure 1: Density distributions (color and contours) withdifference scales. Arrows indicate the velocity vector.

16

nmax=2.1x1015 [cm-3]

log n

I Scientific Highlights

INUTSUKA, Shu-ichiro(Hosei University)		

15

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1415

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AU
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ω

Observations indicate that stars are born as binary
or multiple systems. The star formation occurs in thecollapsing cloud core. When fragmentation occurs in
the collapsing cloud, fragments evolve into binary or
multiple stellar systems. However, we cannot directly
observe fragmentation process, because it is embedded
in a dense cloud core. Thus, we need to investigate thestar and binary formation using numerical simulation. In
the collapsing cloud, two adiabatic cores hierarchicallyappear. The gas density increases as the cloud collapses.
When the central number density exceeds n = 1011 cm−3,
the first adiabatic core (hereafter the first core) is formed.
Then, further collapse begins inside the first core, andthe second core (i.e., the protostar) is formed when thegas density reaches n = 1021 cm−3. The evolution of suchcollapsing cloud was investigated in some past studies.
When the molecular cloud has a certain amount of theangular momentum and unmagnetized, fragmentation ispossible to occur just after the first core formation [1].
However, only a few studies focused on the evolution ofmagnetized clouds. In this study, using resistive MHD
nested grid simulations, we investigated the evolutionof the magnetized disk, and found the condition forfragmentation and binary formation [2]. Figure 1
shows the cloud evolution for a typical model withdifferent scales. In this model, fragmentation occurs
twice. The first fragmentation occurs just after the firstcore formation. After the first core formation, the gas
collapsing timescale shortens and the perturbation to
induce fragmentation grows. The second fragmentation
occurs just before the protostar formation. This is because(i) further collapse is initiated without the formation of
spiral arms owing to the removal of the magnetic field,and (ii) the transportation of the angular momentum
by the magnetic braking becomes ineffective. Figure
2 shows results of parameter survey, in which themagnetic field and angular velocity of the cloud coreis parameterized. In the figure, fragmentation occurs
at the epoch of the first core formation in models withblue background, while at the epoch of the second coreformation in models with red background. On the other
hand, models with gray background evolve to a single
star without fragmentation. The figure indicates that therotation promotes fragmentation, while the magnetic field
suppresses it. In addition, fragmentation is possible evenin the high-density gas region. The binary separation
depends on both the magnetic field and rotation of thecloud. Models showing fragmentation at lower density

008(NAOJ)y [AU]

MATSUMOTO, Tomoaki
			

TOMISAKA, Kohji(Kyoto University) 			

17

0.044 AU

nmax=3.0x1015 [cm-3] 15

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2744.7 AU11

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0.087

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0.01

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1719

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160.70 AU22-3[cm ] 2227

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-3

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[cm ]

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26

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nmax=9.5x1021 [cm-3]

28

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20

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0.001

19

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nmax=3.7x1022 [cm-3]

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~
~

MACHIDA, Masahiro
			

0.1

17

0.022 AU

0.011 AU

1

4

18

Figure 2: Results of parameter survey. The density distribution at
fragmentation epoch for each model is plotted against
the strength of the magnetic field (x−axis) and degree ofthe rotation (y−axis).
Reference[1] Matsumoto T., Hanawa T., 2003b, ApJ, 595, 913.
[2] Machida, M. N., et al.: 2008, ApJ, 677, 327.

Magnetic Field Configuration at the Galactic Center
Investigated by Wide Field Near-Infrared Polarimetry
NISHIYAMA, Shogo, MATSUNAGA, Noriyuki, NAGATA, Tetsuya, NAGAYAMA, Takahiro(Kyoto University)

TAMURA, Motohide, KANDORI, Ryo, NAKAJIMA, Yasushi, KUSAKABE, Nobuhiko(NAOJ)HATANO, Hirofumi, KANAI, Saori, KURITA, Mikio, SATO, Shuji

HOUGH, James H.

(Nagoya University)			

SATO, Yaeko(Graduate University for Advanced Studies)

SUGITANI, Koji

(University of Hertfordshire)

OKUDA, Haruyuki(Nagoya City University)		

The magnetic field (MF) configuration at the Galactic
center (GC) has been investigated with a wide variety ofmethods [1]. The discovery of polarized radio emission
extending perpendicular to the Galactic plane, suchas non-thermal radio filaments and polarized plumes,
has provided early evidence for a substantial poloidal
component of the MF at the GC. However, recent farinfrared (FIR) and sub-millimeter (sub-mm) polarimetricobservations point out that the MF is generally parallel to
the Galactic plane.
Previous near-infrared (NIR) polarization measurements of the GC were discussed in terms of selective
absorption by the intervening interstellar dust grains in
the Galactic disk. To our knowledge, no one has studied
the MF configuration at the GC with NIR polarimetry. In
this work, we conducted NIR polarimetric observations
toward the GC, and demonstrate that NIR polarizationof point sources can provide information on the MF
structure at GC [2].
We carried out NIR polarimetric observations with
the NIR polarimeter SIRPOL on the IRSF telescope.
Comparing the Stokes parameters between highextinction stars and relatively low extinction ones, we
obtained a polarization originating from magneticallyaligned dust grains at the GC (Fig. 1). The distributionof the position angles shows a peak at ~20°, nearlyparallel to the Galactic plane, suggesting a toroidal MF
configuration. The derived direction of the MF is ingood agreement with that obtained from FIR/sub-mm
observations, which detect polarized thermal emission
from dust in the molecular clouds at the GC [3, 4, 5]. Our
results show that by subtracting foreground components,
NIR polarimetry allows investigation of the MF structure
at the GC.

(ISAS)

Northern Thread(G0.08+0.15)

5.0 %
2.5 %

Radio Arc

l=0

10

o

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5∆δ [arcmin]

				

0

-5

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o

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10

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0
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Figure 1: K S band polarization map for the GC from ourobservation (red bars). The polarization map at the
GC derived from FIR/sub-mm observations (bluebars) is also shown [3, 4, 5]. The length of the bars is
proportional to the measured degree of polarization,and their orientation is drawn parallel to the inferredmagnetic field direction. Some prominent radio filaments
are shown as heavy dark lines.

References[1] Morris, M.: 2006, J. Phys. Conf. Ser., 54, 1.
[2] Nishiyama, S., et al.: 2009, ApJ, 690, 1648.
[3] Dotson, J. D., et al.: 2000, ApJS, 128, 335.
[4] Novak, G., et al.: 2000, ApJ, 529, 241.
[5] Chuss, D. T., et al.: 2000, ApJ, 599, 1116.

I Scientific Highlights009

Interstellar Extinction Law toward the Galactic Center:
V, J, H, and KS Bands
NISHIYAMA, Shogo, NAGATA, Tetsuya
			

TAMURA, Motohide, KANDORI, Ryo(Kyoto University) 				HATANO, Hirofumi, SATO, Shuji

The wavelength dependence of interstellar extinction
provides important diagnostic information about the dust
grain properties. Interstellar extinction law shows a large
range of variability from one line of sight to another,
especially in the ultraviolet and optical wavelengths. In
comparing the wavelength dependence among different
lines of sight, the normalization of the extinction curves
by the total extinction A V, instead of the usual color
excess EB–V , is vitally important. Toward the Galactic
center (GC), assuming only that the center of stellar
distribution in the lines of sight is at the same distancefrom us and that the foreground extinction is patchy,
we can directly derive the ratio of the total to selective
extinction (e.g., AV /EV–J ), from which we can obtain theextinction ratio normalized by the total extinction (e.g.,
AJ /AV ). By plotting the apparent magnitude versus thecolor excess of a group of stars, one obtains a straightline with the slope equal to the ratio of total to selective
extinction ratio.
In this work, we have determined the ratios of total
to selective extinction directly from observations in the
optical V band and near-infrared J band toward the GC [1].
The OGLE Galactic bulge fields were observed with the
SIRIUS camera on the IRSF telescope. We constructedcolor-magnitude diagrams, and measured the regressionof the mean color of red clump stars in the GC on theirmean magnitude. We obtain AV /EV–J = 1.251 ± 0.014 (seeFig. 1) and AV /EV–J = 0.225 ± 0.007. From these ratios,
we have derived AJ /AV = 0.188 ± 0.005; if we combine
AJ /AV with the near-infrared extinction ratios obtainedby Nishiyama et al. [2] for more reddened fields near theGC, we get AV : AJ : AH : AKS = 1 : 0.188 : 0.108 : 0.062,
which implies steeply declining extinction toward thelonger wavelengths.
The resultant Aλ /AV in the JHKS wavelength range is asteeply declining function. The frequently used extinction
curve derived by Cardelli et al. (1989 [3]) (for RV = 3.1,
AV /EV–J = 1.393, see Fig. 1), which is based on Rieke &Lebofsky (1985 [4]), decreases much more slowly toward
the longer wavelengths. In particular, it is striking that the
KS band extinction is ≈ 1/16 of the visual extinction AV ,much smaller than one tenth of AV so far employed ([3, 4]).

010

I Scientific Highlights

SUGITANI, Koji

(University of Tokyo)		

(Nagoya City University)
16
AV/EV-J =1.393

17

1.251

18

V

				

(NAOJ)

19
20
21
22

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3

V−J

4

5

6

Figure 1: V versus V–J color magnitude diagram of the OGLE
bulge fields. The solid and dashed lines show thedirection of the interstellar extinction with A V /E V–J= 1.251 (this work [1]), and 1.393 (R V = 3.1 [3],respectively. It is clear that the solid line is along theridge of bulge red clump stars.

References[1] Nishiyama, S., et al.: 2008, ApJ, 680, 1174.
[2] Nishiyama, S., et al.: 2006, ApJ, 638, 839.
[3] Cardelli, J. A., et al.: 1989, ApJ, 345, 245.
[4] Rieke, G. H., Lebofsky, M. J.: 1985, ApJ, 288, 618.

Evolution of the Anemone Active Region NOAA 10798
and the Related Geo-Effective Flares and CMEs
ASAI, Ayumi

		

SHIBATA, Kazunari, ISHII, T. Takako

OKA, Mitsuo(Kyoto University)		

(University of Alabama)(NAOJ) 		

KATAOKA, Ryuho

FUJIKI, Ken’ichi

GOPALSWAMY, Nat(RIKEN) 		

(Nagoya University)		

(NASA GSFC)

Space weather has attracted a lot of attention inrecent times. Space weather research involves various
related fields. Therefore, in order to understand whatkind of events on the solar surface can generate a large
geomagnetic storm, it is necessary to study active
phenomena on the solar surface and the propagation in
the interplanetary space, in relation to the surrounding
magnetic structure. We investigated the evolution of
the Active Region (AR) NOAA 10798 and the features
on/near the sun and in the interplanetary space, since
it generated flares/coronal mass ejections (CMEs) thatcaused a large geomagnetic storm on 2005 August 24
with the minimum Dst index of −216 nT [1].
The AR emerged in the middle of a small coronal hole(CH), and formed a sea anemone like configuration [2](Fig. 1). Hα filaments were formed in the AR, which havesouthward axial field. Two halo CMEs associated with
M-class flares occurred on 2005 August 22. The speedsof the CMEs were extremely fast, and recorded about1200 and 2400 km s−1, respectively. The second CME wasespecially fast, and probably caught up and interactedwith the first (slower) CME during their travelings toward
the earth (Fig. 1). The interplanetary disturbances withstrong southward magnetic field of about −50 nT andstrong compression of plasma were produced.
The reasons why the CMEs were particularly geoeffective were the high speeds of the two CMEs andtheir interaction as well as the CMEs traveled directly
toward the earth. The high speeds of the CMEs are morenotable. We suggest that the fast CMEs are probably
a consequence of the eruption inside a CH from ananemone AR. Eruptive activities of anemone ARs areusually low [3]. However, the relation between anemone
ARs and fast solar winds have been paid attentions
to, and recent papers (e.g. [4]) have also reported theassociation between fast Halo CMEs and CHs. Our
results indicate that flares/CMEs from anemone ARs arealso important for space weather researches.

SOHO EIT

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-400

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Figure 1: Coronal feature of the AR NOAA 10798. (a): An EUV(195 Å) image obtained with SOHO/EIT. The brightregion near the center of the image is the AR. The
surrounding dark region is a CH. (b): A magnetogram
taken with SOHO/MDI.

East

West
CH
sun

earth
Figure 2: Schematic cartoon of AR NOAA 10798 and related
flares/CMEs. The ejected plasma is bent eastward by
the surrounding magnetic field with positive magnetic
polarity. The ejecta from the anemone AR becomesa magnetic cloud (shown as a cylinder) that has asouthward axial magnetic field and is approaching to theearth.

References[1] Asai, A., et al.: 2009, JGR, 114, A00A21.
[2] Shibata, K., et al.: 1994, ApJ, 431, L51.
[3] Asai, A., et al.: 2008, ApJ, 673, 1188.
[4] Liu, Y., Hayashi, K.: 2006, ApJ, 640, 1135.

I Scientific Highlights

011

Strongly Blueshifted Phenomena Observed with Hinode/EIS
in the 2006 December 13 Solar Flare
ASAI, Ayumi, HARA, Hirohisa, WATANABE, Tetsuya, IMADA, Shinsuke(NAOJ)SAKAO, Taro, NARUKAGE, Noriyuki

CULHANE, J. L.

(JAXA)				

Solar flares are very spectacular, and are accompanied
by a variety of plasma motions. These plasma motions
can be observed as phenomena accompanied by line
shifts (Doppler shifts) in spectroscopic observations. We
examined in detail strongly blueshifted emission lines
observed with the EUV Imaging Spectrometer (EIS)on board the Hinode satellite that were observed to be
associated with the 2006 December 13 solar flare [1]. We
found two kinds of blueshifted phenomenon associatedwith the X3.4 flare.
One was related to a plasmoid ejection seen in soft
X-rays (SXRs), and we call it BS1. It was very brightin all the lines used for the observations (Fig. 1). The
Doppler velocity is about 250 km s −1. Although they
are associated with the plasmoid ejection, there are nocorresponding flare ribbons. Therefore, we concluded
that this blueshift is the ejected plasma, and is not an
evaporation flow.
02:24:39 UT(a)Normalized Intensity

SOT(BS2; Fig. 2). The center of the blueshifted component
recorded a Doppler velocity of about 100 km s −1, thedrift velocity is about 450 km s −1. These components
are observed only in the hottest lines of the raster
observation, and therefore, the plasma must be heated tomore than 2 MK. The blueshift region corresponds to the
propagation of the coronal wavelike (arc-shaped) ejection
seen in the SXR images. The SXR ejection is thought
to be an MHD fast-mode shock wave with the Alfvén
Mach number of about 1.4. This is, therefore, the first
spectroscopic observation of an MHD fast-mode shock
wave associated with a flare.

-100
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(Naval Research Laboratory)

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Figure 1: Top: Ca II (H-line) images taken with Hinode/SOT.
Bottom: Soft X-ray images obtained with the Hinode/
XRT (negative images). The cross signs (×) point to thepositions of the BS1. The arrows in the bottom rightpanel follows the plasmoid ejection seen in XRT. The
vertical line in the bottom right panel shows the positionof the EIS slit.

Figure 1: Top: Time sequenced spectra of Fe XV (left) andCa XVII (right) windows observed with Hinode/EIS.
Middle: Normalized spectra at BS2 in the windows.
The solid histograms show the spectra, and the dottedand solid black lines are the fitting results that represent
the main and the blueshift components of the line.
The peaks of each line are shown with thin and thickarrows. Bottom: SXR negative images taken with the
Hinode/XRT. The arrows show the front of the wavelike
ejection. Crosses (×) represent BS2 determined by the
Fe XV line. The vertical line in the bottom right panel
shows the position of the EIS slit.

The other, on the other hand, was very faint, andshowed spectra that broaden in the wavelength space

Reference[1] Asai, A., et al.: 2008, ApJ, 685, 622.

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DOSCHEK, G. A.

(MSSL)		

Normalized Intensity

		

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I Scientific Highlights

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Exploring the substellar temperature regime down to ~550 K
ISHII, Miki, TAMURA, Motohide			

KUZUHARA, Masayuki(NAOJ) 				BURNINGHAM, Ben, PINFIELD, David(University of Tokyo)

and the UKIDSS Cool Dwarf Science Working GroupULAS1335
Jupiter

3
2
H 2O

1

C H4

C H4
H2O

C H4

1.4

1.6

0
1

1.2

wavelength [micron]Figure 1: Near-infrared spectrum of the coolest brown dwarf
ever discovered (ULAS1335) (lower). For comparison
spectrum of the Jupiter is shown (above ULAS1335).
Broad absorption bands of H 2O and CH4 are seen in
their spectra.

Effective Temperature [K]Observations in the 1980–90s have established thatthe conventional spectral sequence from O to M stars isfollowed by even cooler dwarf stars — L and T dwarfs(effective temperature T eff = 2100 – 1300 K and T eff<~1300 K, respectively). Some L dwarfs and all T dwarfs
correspond to “brown dwarf” whose mass is below 0.075
solar masses.
Previous large area surveys (e.g., 2MASS, SDSS)
have discovered about 600 L dwarfs and 100 T dwarfs
so far. On the other hand, a deeper large area survey
is necessary to detect cooler (i.e., intrinsically fainter)brown dwarfs. Ongoing UKIDSS Large Area Survey(LAS) meets the requirement. The UKIDSS/LAS will
cover 4000 sq. degrees using the UKIRT Wide Field
Camera (WFCAM), with 4 mag deeper detection limit
than 2MASS. From the resultant data, the coolest T
dwarfs and, further more, a new class of dwarfs cooler
than T are expected to be found. Such ultra cool dwarfs
are referred to be “Y” dwarfs, and their spectra are
expected to be analogous to the spectrum of the Jupiter.
The Cool Dwarf Science Working group, aninternational collaboration including UK and Japanese
astronomers, has developed the selection method using
UKIDSS Y JHK colors and the combination of SDSSz-J, i-z to select L/T and Y dwarf candidates. Followup
spectroscopy using large telescopes such as Subaru
and Gemini is adopted to determine their spectral types
finally. As a result, we have discovered 72 T dwarfs fromthe UKIDSS early data so far, indicating that our method
is highly effective (e.g., [1, 2]). Six of them are classified
as T8.5–T9, coolest types among known T dwarfs. In
particular, ULAS J133553.45+113005.2 (ULAS335) has
been shown to be the coolest T dwarf ever known (Figures1, 2), with the effective temperature of 550 K and themass of about 20 Jupiter masses [3]. After the completionof UUKIDSS/LAS, we expect to discover Y dwarfs
together with hundreds of T dwarfs, which will shedlight on the formation processes of substellar objects, theInitial Mass Function (IMF) and the formation history.

relative flux

(University of Hertfordshire)

1500
1200
Gl229B

900
600
ULA S1335

1996

2000

2004

2008

Discovery year
Figure 2: History of the coolest brown dwarf discovered: T dwarfs
discovered by UKIDSS (◊) and previous surveys (○) areplotted against their discovery year.

References[1] Kendall, T. R., et al.: 2007, A&A, 466, 1059.
[2] Pinfield, D. J., et al.: 2008, MNRAS, 390, 304.
[3] Burningham, B., et al.: 2008, MNRAS, 391, 320.

I Scientific Highlights

013

High-Precision Correction of the Instrumental Polarizationfor High-Level Polarimetry of the Sun
HANAOKA, Yoichiro(NAOJ)The polarization of the light from the Sun shows thesurface magnetic field of the Sun. However, generally
it is not avoidable for big solar telescopes to have somefolding mirrors, which vary the polarization of theincident light. In such cases, the instrumental polarization
has to be corrected with a high precision to evaluate theincident polarization of the light from the Sun.
On the other hand, to carry out high precision
polarization measurements, it is also required to calibrate
the polarimeter itself with a high precision as well.
Generally unpolarized light (usually the continuum
from the Sun) is necessary for the calibration, but the
instrumental polarization changes the unpolarized
incident light into polarized light. Therefore, thecalibration with unpolarized light is difficult in the systemwith the instrumental polarization. This fact means thatthe evaluation of the parameters of the instrumental
polarization and that of the calibration parameters for thepolarimeter are coupled together.
We installed a polarimeter of NAOJ with ferroelectricliquid crystals into the Domeless Solar Telescope of
Hida Observatory, Kyoto University, and developed amethod to evaluate the parameters of the instrumental
polarization and those of the polarimeters simultaneously[1]. As shown in Figure 1, the Domeless Solar Telescope
has two folding mirrors, which produce the instrumental
polarization. However, the spectrograph rotationand the function of the turning-over of the telescope
attitude cancel the instrumental polarization virtually.
We evaluated the polarization parameters with a highprecision using these characteristics, and we succeeded toreproduce the measured instrumental polarization by thecalculated ones with RMS errors of 0.03 %, which meetsthe required error level to measure the weak polarizationin chromospheric lines. Figure 2 shows a sample setof the polarization spectra with the slit positioned on asunspot. The raw data show significant crosstalk, but the
spectra corrected for the instrumental polarization show
almost symmetric polarization profiles.
The method developed in this work is applicablefor various solar telescopes with oblique reflections.
Furthermore, it will become a guide to consider the
method to correct the instrumental polarization for thesolar telescope designed in future, where the obliquereflections cannot be avoided.
Reference[1] Hanaoka, Y.: 2009, PASJ, 62, 357-365.

014

I Scientific Highlights���������������

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�������������������������������

�����������

�����������������

���������������������

Figure 1: Layout of the light path in the Domeless Solar
Telescope. Mirrors S2 and S4 are folding mirrors. The
signs of Stokes Q and U signals into the polarimeter canbe reversed with a rotation of the spectrograph, and thatof Stokes V can be done so with the turning-over of thethe telescope.

(a)

(b)

I
Q/I
U/I
V/I
Figure 2: A sample set of Stokes Spectra of the Fe 6302.5 line
taken at a sunspot. The horizontal and vertical directions
are along the slit and the dispersion, respectively.
Panels (a) and (b) show the spectra before and after thecorrection of the instrumental polarization.

Sensitivity improvement of gravitational wave detector TAMA300
ARAI, Koji, TAKAHASHI, Ryutaro, TATSUMI, Daisuke, ISHIZAKI, Hideharu, YAMAZAKI, Toshitaka
FUKUSHIMA, Mitsuhiro, IZUMI, Kiwamu, WAKABAYASHI, Yaka, AGATSUMA, Kazuhiro
FUJIMOTO, Masa-Katsu, and the TAMA collaboration(NAOJ)

events should be detected than before. Particularly,
the distance for stellar mass binaries are remarkably
improved as the low frequency sensitivity contributes toit.
TAMA300 Strain Sensitivity

-13

10

-14

1/2

Strain sensitivity [1/Hz ]

10

-15

10

Previous
sensitivity

-16

10

-17

10

-18

10

-19

10

-20

10

Alignment
control noise

-21

10

Sensitivity with SAS

-22

10

10

1

10

2

3

4

10

10

Frequency [Hz]Figure 1: Current sensitivity of TAMA300 (red), being comperedwith the previous sensitivity (black). The blue line
indicates the estimation of the alignment control noise.

D istance ofdetecting inspirals w ith SN R =10
Observable Distance [kpc]

The TAMA project of NAOJ has been developinga laser interferometer gravitational wave detector
TAMA300. Here, we report a sensitivity improvement of
TAMA300.
We have been working on the new vibration isolation
system, called “Seismic Attenuation System (SAS)”,
since 2005. The sensitivity of TAMA300 at around 100
Hz was previously limited by alignment control noise.
In order to improve the sensitivity in the low frequency
band, we replaced the previous vibration isolation system
to the SAS for all of four test masses. As a result of theinstallation and tuning works, we could decrease thecontrol bandwidth of the alignment servo system. It leads
an update of the sensitivity.
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 so as torealize seismic filtration from the low frequency suchas 50 mHz. In order to suppress excited motions of the
low frequency resonances, the active local controls areapplied. All of the local control servos are realized bydigital control systems based on LabVIEW. With the
intrinsic vibration isolation performance of the SAS andthe local control systems, test mass motions are wellstabilized in all frequency band. It was confirmed by the
optical path length measurement of the 300-m arm cavity
that the RMS motion of the cavity length is improved
from 0.84 μm to 1.4 μm [1].
After the shaking down and tuning of the SAS, thepower recycled operation of the 300-m Fabry–Perot
Michelson interferometer has been recovered. The current
sensitivity of TAMA300 is shown in Figure ??. The
revised wave front sensing technique for the alignment
control helps to keep the stability of the sensitivity in the
kHz band, while the improved sensitivity at the frequency
band below 100 Hz is not compromised. As a result, thesensitivity between 0.1 Hz to 400 Hz was improved. The
Hz at around 1 kHz.
floor sensitivity is h = 1.3×10−21 m/√¯
The contribution of the alignment control noise is also
shown in the figure. It indicates that this noise is not
limiting the current sensitivity. This was owing to the
reduction of the alignment control bandwidth down to 3
Hz.
Figure 2 shows how distant compact binaries
TAMA300 should be able to detect. Each curve means theevent at the indicated distance is detected with S/N of 10,
assuming the direction of the event and the polarization
are optimal for the detector. For all binary masses farther

160
150
140
130
120
110
100
90
80
70
60
50
40
30
20
10
0
10

5.0Msolar - 145.7kpc

Current sensitivity

1.4Msolar - 82.4kpc
10Msolar - 56.7kpc

0.5Msolar - 37.2kpc

Previous sensitivity
-1

2

3

4

5 6 7 8

10

0

2

3

4

5 6 7 810

1

2

mass [Msolar]

Figure 2: “Observable distance” indicates how distant comact
binaries TAMA300 should be able to detect. This showsthe event at this distance is detected with S/N of 10,
assuming the direction of the event and the polarization
are optimal for the detector.

Reference[1] Arai, K., et al.: 2008, J. Phys.: Conf. Ser., 120, 032010.

I Scientific Highlights

015

Theoretical and Observational Studies Using Hinodeof the Magnetic-Field Emergence into the Solar Atmosphere
MAGARA, Tetsuya(NAOJ)We have performed a three-dimensional MHD
simulation for the emergence of a partially split flux
tube into the solar atmosphere, which is focused on
the mechanism of the activity observed on the Sunsuch as the merging of magnetic polarity regions in
the photosphere and the formation of multiple flux
domains in the corona. The simulation reproduces thata small polarity region associated with a rotational flow
merges into a main polarity region, and later in this mainpolarity region is developed a rotational flow in the same
direction as the small polarity region. In accordance withthe photospheric merging process, multiple flux domains
form in the corona and a current layer separating theseflux domains travels outward as the flux domains expand.
We also investigated the nature of helicity injection in a
multi-pole system.
We reported a result of investigating the structure of
subsurface magnetic field in an emerging flux region on
the Sun, using the data obtained by Hinode. We derived
several statistical quantities characterizing the distributionof surface magnetic field. These quantities were thenused to investigate the structure of invisible subsurface
magnetic field, such as the twist of field lines, bycomparing the observations with numerical simulations.
The result suggests a possible way of investigating
the structure of subsurface magnetic field by using
observational information on surface magnetic field.
We used Hinode’s observational data of photosphericmagnetic field to study the evolution of a flare-producing
active region. Hinode can provide the temporaldevelopment of the photospheric field as a vector quantity,
which shows that magnetic shear initially developed inan active region (AR10930), then it decreased toward
the onset of an X-class flare. The magnetic helicity inthis active region first increased rapidly, while it became
saturated in the late phase. We explained the physicalorigin of these features in terms of the emergence of atwisted flux tube into the solar atmosphere. We showed
how helicity evolution relates to the occurrence of aflare, suggesting that the helicity evolution obtained frommeasurements of the photospheric field can be used forflare prediction [1, 2, 3].

References[1] Magara, T.: 2008, PASJ, 60, 809.
[2] Magara, T.: 2008, ApJL, 685, L91.
[3] Magara, T., Tsuneta, S.: 2008, PASJ, 60, 1181.

016

I Scientific Highlights

Figure 1: Emergence of a partially split flux tube. The horizontal
plane indicates the photosphere.

ObservationySimulation (WT)ySimulation (HT)

y

x

x

x

Distance

Distance

Distance

Figure 2: Scattered diagrams of positive (triangles) and negative(diamonds) polarity regions. Left: Data from Hinode.
Middle: Simulation of a weakly twisted flux tube. Right:
Simulation of a highly twisted flux tube. Note thatthe observational result has mirror symmetry with thesimulations.

Figure 1: Left: Relative sunspot motions obtained from an elliptic
approximation applied to the boundary of the travellingsunspot. Right: Time variation of the injection rate ofmagnetic helicity. The vertical dashed line indicates theoccurrence time of a flare.

Young Brown Dwarfs in the Core of the W3 Main Star-Forming Region
OJHA, Devendra K., GHOSH, Swarna Kanti(Tata Institute of Fundamental Research, Mumbai)

TAMURA, Motohide, NAKAJIMA, Yasushi, SAITO, Hiro, AOKI, Kentaro(NAOJ)PANDEY, Anil. K.
(Aryabhatta Research Institute of Observational Sciences, Nainital)

We present the results of deep and high-resolution(FWHM ~0.35”) JHK near-infrared (NIR) observations
with the Subaru telescope, to search for very low mass
young stellar objects in the W3 Main star-forming region.
The NIR survey covers an area of ~2.6 arcmin2 with 10σ
limiting magnitude exceeding 20 mag in the JHK bands.
The survey is sensitive enough to provide unprecedented
details in W3 IRS 5 and IRS 3a regions and reveals acensus of the stellar population down to objects below thehydrogen-burning limit.
We construct JHK color-color and J–H/J and H–K/K
color-magnitude diagrams to identify very low luminosity
young stellar objects and to estimate their masses (see forexample Figure 1). Based on these color-color and colormagnitude diagrams, we identified a rich population ofembedded YSO candidates with infrared excesses (ClassI and Class II), associated with the W3 Main region. A
large number of red sources (H–K > 2) have also been
detected around W3 Main, which are arranged from thenorthwest toward the southeast regions. Most of these areconcentrated around W3 IRS 5. We argue that these redstars are most probably pre-main-sequence (PMS) stars
with intrinsic color excesses.
We find that the slope of the K-band luminosity
function of W3 Main is lower than the typical values
reported for young embedded clusters. Based on thecomparison between theoretical evolutionary models ofvery low-mass PMS objects with the observed colormagnitude diagram, we find there exists a substantial
substellar population in the observed region.
The mass function does not show the presence of
cutoff and sharp turnover around the substellar limit, atleast at the hydrogen-burning limit. Furthermore, themass function slope indicates that the number ratio ofyoung brown dwarfs and hydrogen-burning stars in theW3 Main is probably higher than those in Trapezium andIC 348.
The presence of mass segregation, in the sense that
relatively massive YSOs lie near the cluster center, isseen. The estimated dynamical evolution time indicatesthat the observed mass segregation in the W3 Main may
be the imprint of the star formation process [4].

Figure 1: Color-magnitude diagram for the YSO candidates in W3
Main. Class II candidates are indicated by blue stars,
filled green triangles represent Class I candidates, andthe filled red circles show red sources with H–K > 2 with
J band counterparts. Known IRS sources are shown withboxes. The solid and dotted curves denote the loci of 1
Myr old PMS stars; derived from the models of [1], [2]and [3].

References[1] Palla, F., Stahler, S.: 1999, ApJ, 525, 772.
[2] Baraffe, I., et al.: 1998, A&A, 337, 403.
[3] Baraffe, I., et al.: 2003, A&A, 402, 701.
[4] Ojha, D., et al.: 2009, ApJ, 693, 634.

I Scientific Highlights

017

Exoplanet Detection with Polarimetry
TAMURA, Motohide
		(NAOJ)			

HOUGH, James H., LUCAS, Philip W.

BAILEY, Jeremy(University of Hertfordshire)(University of New South Wales)

Since the discovery of planets orbiting around normalstars other than the Sun, exoplanet detection is one of
the hottest topics in astronomy. Most (>80%) of the
exoplanet candidates have been detected via the radial
velocity method. The transit method is detecting many
candidates (especially with the Kepler and the Corot
missions). However, the other successful methods are still
limited. Therefore, an independent approach is importantto reveal various physical parameters of exoplanets.
Aged planets shine by reflected light at optical andnear-IR wavelengths. Thus, exoplanet detection withreflected light is a promissing technique [1, 2].
In paerticular, high precision polarimetry is considered
to be direct detection if the waekly polarized light is
extracted from the highly diluted (unpolarized) lightfrom the central star. Close-in planets are expected show
as much as a few 10−6 polarization. In order to achievethis, a high precision (<10−6) polarimeter is necessary.
The Planetpol is an optical polarimeter composed of
PEM (photoelastic modulator) and APD (avalanche
photodiode) that can attain a polarization accuracy of<10−6 [3].
The PlanetPol observations were made during a
Saharan dust event over the La Palma observatory thatshow excess linear polarization in the horizontal direction
due to the passage of the starlight through the dust [4].
The polarization reached a maximum value of 4.8×10−5.
These results imply that some fraction of the dust grain
population aligns with a preferred orientation. We suggest
a possible mechanism for vertical orientation resulting
from the electric field in the atmosphere.
The PlanetPol observations were also made for
55 Cnc and τ Boo in an attempt to detect the partiallypolarized reflected light from the planets orbiting these
two stars [5]. The polarization of this system is very
stable, showing no sign of the periodic variations thatwould be expected if a short-period planet were detected.
The measured standard deviation of the nightly averaged
Stokes Q/I and U/I parameters is 2.2×10−6 (Figure 1).
These results contrast markedly with the recent claimof detection of a periodic polarization signal from
HD189733 with amplitude 2×10 −4, attributed to theplanet HD189733b [6]. Our multiple scattering model
atmosphere calculations indicate that the large amplitude
periodic polarization signal from the HD189733 systemcannot be explained in terms of reflected light from theplanet HD189733b. If the observations are confirmed it
would be important to consider the possible contributionof star spots to the polarization of the system, given that
HD189733 is an active star with much larger photometric018

I Scientific Highlights

variations than τ Boo or 55 Cnc.

Figure 1: Polarization vs. orbital angle of 55 Cnc e (period=
2.817d). 180 degrees correspond to the minimum
illumination. Polarization due to telescope and instument
is subtracted. Different symbols correspond different
nights.

References[1] Collier Cameron, A., et al.: 1999, Nature, 402, 751.
[2] Leigh, C., et al.: 2003, MNRAS, 344, 1271.
[3] Hough, J. H., et al.: 2006, PASP, 118, 1302.
[4] Bailey, J., et al.: 2008, MNRAS, 386, 1016.
[5] Lucas, P. W., et al.: 2009, MNRAS, 393, 229.
[6] Berdyugina, S. V., et al.: 2008, ApJ, 673, L83.

Achievement of the CLIO target sensitivity at room temperature
TATSUMI, Daisuke, KAWAMURA, Seiji, ARAI, Koji
(NAOJ)TELADA, Souichi(National Institute of Advanced Industrial Science and Technology)

MIYOKI, Shinji, UCHIYAMA, Takashi, AKUTSU, Tomomi, MIYAKAWA, Osamu
AGATSUMA, Kazuhiro, YAMAMOTO, Kazuhiro, OHASHI, Masatake(Institute of Cosmic Ray Research, University of Tokyo)

TOMARU, Takayuki, SUZUKI, Toshikazu, YAMAMOTO, Akira

SHINTOMI, Takakazu(High Energy Accelerator Research Organization)			

CLIO (Cryogenic Laser Interferometer Observatory)
is the first cryogenic interferometric gravitational wave
detector in the world. It has 100-m baseline length andis located in an underground mine at Kamioka. It is a
prototype interferometer for the future LCGT project
as well as TAMA300 detector in Mitaka campus. To
demonstrate advantages of the cryogenic interferometerand the Kamioka mine as a quiet site is the purpose.
The project started to excavate the center room andtwo tunnels in 2002. The vacuum and the cryogenic
systems were prepared by 2005. After the installation of
the interferometer optics and the suspension systems, theoperation of CLIO started in 2006. Test of the cryogenic
systems and the interferometer operation with cryogenic
mirrors were demonstrated in 2006.
After the demonstration of cryogenic operations, ouractivities have been focused on the noise investigation
at room temperature. At the time of 2007, the strain
sensitivity below 20 Hz is comparable to that of the
LIGO detector, which is a couple of 4-km detectors in
United State. Because the baseline length is fourty times
shorter than that of LIGO, it means that CLIO achived
fourty times smaller noise level [1]. This is due to a
big advantage of underground site. In February 2007,
a 57-hours observation data was obtained to search forgravitational wave signal at 22.38 Hz from the pulsar
J0835-4510 (Vela pulsar) [2].
To demonstrate the reduction of the noise level by
mirror cooling, the detector noise should be limited bythermal noises at room temperature. In the summer of
2008, the sensitivity of CLIO at room temperature was
improved in a wide frequency range above 20 Hz. This
improvement was obtained by elimination of thermal
noise from dissipation caused by eddy current induced
to the coil support made of aluminum, as well as tuningof beam spot positions on the mirror surfaces, whichindicates possible noise coupling from any kind of
mirror rotation noise. Current best floor sensitivity is
2.5×10−19 m/√ H̄z at 250 Hz as shown in Figure 1. We
estimated the fundamental noises of the CLIO as follows.
Seismic noise was estimated by the ground motion andtransfer function of the vibration isolation systems. The(Nihon University)

suspension thermal noise was estimated from the quality
factor of the violin mode resonances. The mirror thermal
noise at room temperature was supposed to be dominatedby thermoelastic damping. Shot noise was estimatedfrom incident optical power to the photodetector andits response. From these estimations, we concluded thatthe noise level is enough close to the fundamental limit
at room temperature and the cooling of the mirrors isnecessary for further noise investigations.
The next step is to realize noise reduction by mirror
cooling. Now we are preparing noise hunting with thecryogenic mirrors including works to refine the cryogenic
suspensions and the interferometer systems.

-12

CLIO displacement sensitivity at T=300K

10

2008/11/05 CLIO sensitivity-13

Displacement noise [m/Hz1/2]		

10

Seismic noise estimation
Suspension thermal noise

-14

10

Mirror thermal noise
Shot noise

-15

10

-16

10

-17

10

-18

10

-19

10

10

1

10

2

10

3

10

4

Frequency [Hz]Figure 1: Current displacement sensitivity of CLIO (black). Noiseestimations of seismic noise (red), suspension thermal
noise (yellow), mirror thermal noise (green), and shotnoise (purple) are also shown.

References[1] Yamamoto, K., et al.: 2008, J. Phys. Conf. Ser., 122, 12002.
[2] Akutsu, T., et al.: 2008, Class. Quantum Grav., 25, 225011.

I Scientific Highlights

019

Detection of water ice grains on the surfaceof the circumstellar disk around HD 142527
		

HONDA, Mitsuhiko

INOUE, Akio

FUKAGAWA, Misato(Kanagawa University)(Osaka Sangyo University)		

(Osaka University)

OKA, Akinori, NAKAMOTO, Taishi

ISHII, Miki, TERADA, Hiroshi, TAKATO, Naruhisa(Tokyo Institute of Technology) 				
		(NAOJ)KAWAKITA, Hideyo

OKAMOTO, Yoshiko

SHIBAI, Hirosi(Kyoto Sangyo University)(Ibaraki University)(Osaka University)

TAMURA, Motohide, KUDO, Tomoyuki
					(NAOJ) 			

Water ice grains theoretically play a number ofimportant roles in protoplanetary and debris disks. Ice
enhances the solid material in the cold outer part of a
protoplanetary disk, which promotes the formation ofcores of gaseous planets [1]. [2] show that ice absorption
can also be found in the light scattered by icy grains
and that multi-wavelength imaging in NIR wavebands,
including in the H2O band at 3.1 µm, is a useful tool toconstrain the ice distribution in the disk.
We have applied this method to the circumstellar
disk around a Herbig Ae star, HD142527, which is an
ideal target for imaging in the H2O band for a numberof reasons. Coronagraphic imaging observations for
the HD142527 using a L′ band (3.77 µm) and a narrowband H2O ice filter (3.08 µm) were performed using theCoronagraphic Imager with Adaptive Optics (CIAO) on
the Subaru Telescope. Figure 1 shows the PSF-subtracted
images of the circumstellar disk around HD 142527 in
the H2O ice filter with the 0.6″ mask and in the L′ bandwithout a mask, respectively. The eastern and westernarcs discovered by [3] in the H and K bands were also
detected in the H2O and L′ band. The spectrum for the
total flux densities is also presented for comparison in theleft panel of Figure 2, which shows few or no features inthe H2O band. The contribution from the scattered light tothe total flux density in the H and K bands is estimated tobe 3.1–3.2% [3], indicating that most of the flux density
in the total spectrum is attributed to the emission fromthe star itself and thermal emission from hot grains in
the vicinity of the star where icy grains cannot survive.
Therefore, the absence of a 3 µm ice feature is a naturalconsequence. In contrast, the spectra of the scattered lightshow a clear reduction in the H2O ice band (3.08 µm),
suggesting the presence of a 3 µm absorption feature. This
result can be explained by the water ice grains in the disk
surface where the light scattering occurs. Comparing themodel predictions [2] with the observed color diffrence,the size of the scattering grains is ~1 µm or more.
Our results successfully demonstrate that multiwaveband (K/H2O/L′ imaging is useful to detect water ice
grains in a (face-on) disk. The application of this method
for other face-on disks will enhance our knowledge020

I Scientific Highlights

ITOH, Yoichi(Kobe University)on the presence and spatial distribution of water ice incircumstellar disks [4].

Figure 1: PSF-subtracted 3.08 μm (left) and L′ band (right) imageof the disk around HD142527. The unit of intensity
is mJy arcsec −2. North is up; east is to the left. The
three enclosed regions (regions A, B, and C from inner
to outer regions) on the southwest structure are thepositions from which the spectra shown in Figure 2 are
extracted.

Figure 2: Left panel shows NIR photometry and a spectrum of
the entire HD 142527 system, which is used as therepresentative of the illuminating source spectrum.
Right panel represents the spectra of the scattered lightfrom regions A, B, and C shown in Figure 1. The dip in
3 μm, probably due to H2O ice grains, is present in all
the scattered light spectra, while it is not seen in the total
spectrum, which is dominated by thermal emission fromhot dust near the central star.
References[1] Hayashi, C., et al.: 1985, in Protostars and Planets II, ed. D.C.
Black & M. S. Matthews (Tucson, AZ: Univ. Arizona Press),
1100.
[2] Inoue, A., et al.: 2008, PASJ, 60, 557.
[3] Fukagawa, M., et al.: 2006, ApJ, 636, L153.
[4] Honda, M., et al.: 2009, ApJ, 690, L110.

Small-JASMINE (Small Satellite with 30cm-class telescope)
YANO, Taihei, GOUDA, Naoteru, KOBAYASHI, Yukiyasu, TUJIMOTO, Takuji, HATSUTORI, Youichi(NAOJ)YAMADA, Yoshiyuki
		

KAWAKATSU, Yasuhiro, MATSUHARA, Hideo(Kyoto University)				

NIWA Yoshito			(ISAS/JAXA)JASMINE Working Group(Kyoto University/NAOJ)

JASMINE is the acronym of the Japan Astrometry
Satellite Mission for INfrared Exploration. The main
objective of JASMINE is to study the fundamental
structure and evolution of the Milky Way bulge
components. In order to accomplish these objectives,
JASMINE will measure trigonometric parallaxes,
positions and proper motions of stars in the Galactic bulge
with a precision of 10 microarcsec. Before the launch of
JASMINE, we plan a launch of Small-JASMINE mission
which is a downsized version of JASMINE.
The primary mirror for the telescope of SmallJASMINE has a diameter of 30cm with a focal lengthof about 5m. The wavelength to be observed is around
2 μm with the HgCdTe detectors. A target accuracy of themission is the same with JASMINE, 10μas. The size ofthe field of view is about 0.87deg × 0.87deg by using 2 ×
2 detectors on the focal plane. The telescope is designed
to have only one field of view, which is different from thedesigns of other astrometric satellites (but the same withJASMINE). JASMINE will observe overlapping fields
without gaps to survey a total area of about a few square
degrees around the Galactic bulge. Accordingly wemake a “large frame” of a square degrees by linking thesmall frames using stars in overlapping regions. SmallJASMINE will observe the region of Galactic bulge
repeatedly during the mission life.

Optical Design

3 mirrors (Improved Korsch)

Wave length

1.5 μm ≤ λ ≤ 2.5 μm

Aperture

30 cm

Focal length

4.86 mField size

0.87º × 0.87º

Size of Focal Plane

6 cm × 6 cm

Detector

HgCdTeNumber of pixels

2K × 2K

Number of detectors

4 (2 × 2)

Pixel size

15 μm

Pixel on sky

138 masTable 1: Summary of JASMINE Optics.

Number of Small Frames

4×4

Observing Magnitude

K=11 mag

Integration time

3sec

Time for making a Large Frame

0.25 hMission Life

1.5 year

Table 2: Parameters.

Pointing Stability

280 mas/3 sec

Thermal Stability

0.4 K/0.25 h

Orbit

600 Km Earth Orbit

Ponting Accuracy

0.1 deg

Data Transfer Rate

2 MbpsTable 3: Requirements.

Figure 1: Overview of JASMINE Optics.

Reference[1] Yano, T., et al.: 2008, Proceedings of the IAU, IAU Symp. 248,
296-297.

I Scientific Highlights

021

Development of Very Small Astrometry Satellite: Nano-JASMINEHATSUTORI, Yoichi, KOBAYASHI, Yukiyasu, GOUDA, Naoteru, YANO, Taihei(NAOJ)YAMADA, Yoshiyuki

NIWA, Yoshito

USHIYAMA, Takao(Kyoto University)(Kyoto University/NAOJ)(Tokai University)

		

NAKASUKA, Shinichi, SAKO, Nobutada
			(University of Tokyo)

JASMINE Project Office of National Astronomical
Observatory of Japan, Kyoto University, University ofTokyo and Tokyo University of Marine Science andTechnology develop a very small astrometry satellite:
Nano- JASMINE. Nano-JASMINE is mounted a 5 cm
effective diameter telescope and aims to measurepositions and motions of stars with the accuracy of a few
milliarcseconds in z – band (λ ~ 0.9 μm). The satellite
weighs about 25 kg and is developed aiming at the launch
in 2010 [1]. JASMINE Project Office contributes todevelop a small reflecting telescope and a driver circuit
for a CCD detector. In 2008, we developed and evaluatedthese instruments and conducted the integration test
and environmental test. This paper reports the results ofdevelopment.
First, the small reflecting telescope was made ofaluminum alloy because of the suppression of effects ofstrain induced by thermal changes. The reflecting surfaces
were polished with a single-crystal diamond cutting tools
and deposited with Cr and Au vapor. Developed telescope
weighs 1.7 kg and occupies a volume of only 17×12×
12 cm [2]. Wavefront errors of developed telescope were
measured by an interferometer. As a result, the RSS
wavefront error is λ/14 (λ = 800 nm). Then it is confirmedthat developed telescope can achieve a diffractionlimitted
performance.
Second, new driver circuit for a CCD detector wasdeveloped. Developed circuit can be operated in TDI(Time Delay Integration) mode. In TDI mode, the rate ofcharge transfer is synchronized with the scan velocity ofthe spinning satellite. Developed circuit was evaluatedthrough the measurement of system gain, dark current andCTE. Fig. 1 shows the relationship between accumulated
charges and linearity error of CCD.
Next, Structure and Thermal Model (STM) of satellite
was developed for the thermal test and the vibration
test. Using STM, mechanical interfaces of satellite wereconfirmed and thermal vacuum test was conducted.
Fig. 2 shows the overview of STM before the thermal
vacuum test. Moreover, electric integration test was
conducted and the electric interface, each function andpower consumption were confirmed. These results werereflected to engineering model.
Over the next year, engineering model is to be
developed and examined, and flight model is to be022

I Scientific Highlights

EBINUMA, Takuji(Tokyo University of Marine Science and Technology)

developed. About the launch, NAOJ, University of Tokyo,
Alcantara Cyclone Space and SDO Yuzhnoye agreed thememorandum of understanding (MOU) to launch NanoJASMINE by Cyclone-4 rocket in the Federal Republicof Brazil.

Figure 1: The relationship between accumulated charges andlinearity error of CCD. The linearity error is increased at
115ke- where accumulated charge is saturated.

Figure 2: Nano-JASMINE STM at the NAOJ space chamber
just before the thermal vacuum test. Test heaters which
control outer temperature are equipped around STM.

References[1] Kobayashi, Y., et al.: 2006, SPIE, 6265, 6265544.
[2] Suganuma, M.,et al.: 2006, SPIE, 6265, 6265545.

Neutrino-Nucleus Reaction Cross Sections
for Light Element Synthesis in Supernova Explosions
YOSHIDA, Takashi
			(NAOJ) 		

SUZUKI, Toshio

CHIBA, Satoshi(Nihon University)(Japan Atomic Energy Agency)

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

TAKAMURA, Akira

HARTMANN, Dieter, H.

(Toyota National College of Technology)(Clemson University)

101
2

Neutrino nucleosynthesis (the ν-process) insupernovae is one of main synthesis processes for rare
light elements such as Li and B. In order to evaluate thelight element yields, cross sections of neutrino-nucleus
reactions should be precisely calculated. Recently, a
new shell model Hamiltonian (the SFO Hamiltonian)
reproduces well many characteristics of p-shell nuclei [1].
We evaluate cross sections of ν-12C and ν-4He reactions
using the SFO and WBP Hamiltonians, respectively.
Then, we discuss light element synthesis through the
ν-process in supernovae using the new cross sections [2].
Cross sections of ν- 12 C reactions are calculatedusing the SFO Hamiltonian [1]. Both of neutraland chargedcurrent reactions are taken into account.
Branching ratios for multiple particle emissions areevaluated using Hauser-Fechbach calculations. Cross
sections of ν-4He reactions are also calculated using the
WBP Hamiltonian. Figure 1 shows the cross sections ofneutral-current ν-12C reactions as a function of neutrino
temperature. Neutrino energy distribution is assumed toobey Fermi distributions with zero chemical potential.
Only large branches are shown in this figure. Tables of
the cross sections for ν-12C and ν-4He are listed in [2].
We evaluate the yields of light elements in a 16.2 Msupernova with the new cross sections. The yields of 7Li
and 11B are 2.67 × 10.7 M and 7.14 × 10.7 M, respectively. These yields are larger than the corresponding ones
with conventional cross sections by a factor of 1.1. The
yields of 6Li, 9Be, and a radioactive nucleus 10Be are alevel of 10−11 M and increase compared to the ones withthe conventional rates. The temperature range of νμ,τ andν̄μ,τ in supernovae appropriate for the Galactic chemical
evolution of 11B is reevaluated to be 4.3–6.5 MeV. This
range is slightly shifted to lower energy compared to thecase with the conventional rates. The increase in the 7Li
and 11B yields due to neutrino oscillations is also shownin [2]. This result is important in the determination of
unknown neutrino oscillation parameters.

cm )(Nagoya University) 		

-42

		

σν (10YOKOMAKURA, Hidekazu, KIMURA, Keiichi

100

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Be

9

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10-4

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7

B

Be

Li

Tν (MeV)8910Figure 1: Calculation neutrino- 12C reaction cross sections as
a function of neutrino temperature T ν for the SFO
Hamiltonian.

References[1] Suzuki, T., et al.: 2003, PRC, 67, 0444302.
[2] Yoshida, T., et al.: 2008, ApJ, 686, 448.

I Scientific Highlights

023

Central Spiral Structure of Molecular Gas in Maffei 2
SORAI, Kazuo

SHIBATSUKA, Toshihito(Hokkaido University) 		

(University of Tokyo)

We made CO(1 – 0), CO(2 – 1), CS(2 – 1) lines and
103 GHz continuum observations of the nearby barredspiral galaxy Maffei 2 with Nobeyama Millimeter Array(NMA) [1]. The CO integrated intensity maps show two
peaks in the central region (Figure 1). By investigating
the velocity structure, however, we found the spiralstructure of molecular gas in the central region (Figures2, 3). The offset ridges of molecular gas along theleading side of the bar continue to the spiral structure
embedded in the weak oval structure which is regarded
as an x2 orbit. The size of these structure is less than R ~100 pc. The mass within R ~ 35 pc is estimated to be 2 ×
108 M from the rotation velocity of molecular gas. The
high mass concentration is consistent with theoreticalpredictions concerning the creation of such a nuclear
spiral structure [2]. A comparison with tracers of dense
gas and star-forming region suggests that the dense
molecular gas traced by the CS(2–1) line is formed at thecrossing points of the x1 and x2 orbits and that the starforming region appears downstream of the peak of thedense gas.
(a)

D eclination (J2000.0)

D eclination (J2000.0)(b)

59 36 30

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(a)

(b)

(c)
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100

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VLSR (km s-1 )100-150 -100-50
050
VLSR (km s-1 )100

Figure 2: P-V diagrams of CO(2–1) along major axis of Maffei
2 and parallel to the major axis. (a) 0.9′′ eastern side of
the major axis. (b) along the major axis. (c) 0.9′′ westernside of the major axis. Two parallel components that
correspond to the spiral structure are seen.

D eclination (J2000.0)

KUNO, Nario, NAKANISHI, Koichiro		Rightascension (J2000.0)

Rightascension (J2000.0)

Figure 1: (a) CO(1–0) and ( b) CO(2–1) integrated intensity maps.
The cross indicates the galactic center. The circles
indicate the field of view of NMA. The arrow indicatesthe position angle of the major axis of Maffei 2.

Rightascension (J2000.0)
Figure 3: Contour) Integrated intensity map of CO(1–0) of thetwo components seen in Fig. 2. Color) The HST image(F814W).

References[1] Kuno, N., et al.: 2008, PASJ, 60, 475.
[2] Ann, H. B., Thakur, P.: 2005, ApJ, 620, 197.

024

I Scientific Highlights

Near-Infrared Imaging Polarimetry of M42:
Aperture Polarimetry of Point-like Sources
KUSAKABE, Nobuhiko, TAMURA, Motohide, KANDORI, Ryo(NAOJ)HASHIMOTO, Jun

NAKAJIMA, Yasushi(Graduate University for Advanced Studies)		

(NAOJ)NAGATA, Tetsuya, NAGAYAMA, Takahiro
			

HOUGH, James H., LUCAS, Philip W.

(Kyoto University) 			

We have conducted aperture polarimetry of ~500 starsof the Orion Nebula Cluster (ONC) in M42 based on our
wide-field (~8′ × ~8′) JHKs band polarimetry (Figure 1)[1]. Most of the near-infrared (NIR) polarizations are
dichroic, with position angles of polarization agreeing,both globally and locally, with previous far-infrared (FIR)
and submillimeter observations [2], having taken into
account the 90º difference in angles between dichroic
absorption and emission. This is consistent with theidea that both NIR dichroic polarizations and FIR/
submillimeter thermal polarizations trace the magnetic
fields in the OMC-1 region. The magnetic fields inferredfrom these observations show a pinch at scales less than
0.5 pc with a centroid near IRc2. The hourglass-shaped
magnetic field pattern is explained by the models inwhich the magnetic field lines are dragged along withthe contracting gas and then wound up by rotation ina disk. The highly polarized region to the northwest ofIRc2 and the low-polarized region near the bright bar are
also common among NIR and FIR/submillimeter data,
although a few regions of discrepancy exist.
We have also discerned 51 possible highly polarized
sources whose polarizations are more likely to be intrinsic
rather than dichroic. Their polarization efficiencies (P(H)/
A(H)) are too large to be explained by the interstellar
polarization. These include nine young brown dwarfs thatsuggest a higher polarization efficiency (see Figure 2),
which may present geometrical evidence for (unresolved)
circumstellar structures around young brown dwarfs.

References[1] Kusakabe, N., et al.: 2008, AJ, 136, 621.
[2] Schleuning, D. A.: 1998, ApJ, 493, 811.
[3] Slesnick, C. L., et al.: 2004, ApJ, 610, 1045.
[4] Riddick, F. C., et al.: 2007, MNRAS, 381, 1077.

(University of Hertfordshire)

Figure 1: H band (shown in blue) polarization vectors and 350 μm(shown in red, rotated by 90°) polarization vectors
overlaid on the 350 μm contours. 10% polarization
vectors for both wavelengths are shown at the bottomleft.
35
P(H)/A(H) (%/mag)

		

30
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0.3

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Mass

Figure 2: P(H)/A(H) for the 28 sources cross-identified with
Slesnik et al. (2004) [3] (filled circle) and Riddick etal. (2007) [4] (open circle). The horizontal dotted line
indicates P(H)/A(H) = 2.9, which corresponds to theassumed maximum value for interstellar polarization.
The vertical dotted line indicates 0.08 M  , whichcorresponds to the brown dwarf mass limit.

I Scientific Highlights

025

Infrared Imaging Polarimetry of S106 in Cygnus
SAITO, Hiro, TAMURA, Motohide, KANDORI, Ryo, KUSAKABE, Nobuhiko, NAKAJIMA, Yasushi(NAOJ)HASHIMOTO, Jun, SATO, Yaeko

026

NAGATA, Tetsuya, NAGAYAMA, Takahiro

KATO, Daisuke(Graduate University for Advanced Studies)			

(Kyoto University)			

SIRPOL [1] is the polarization mode of the three-band
simultaneous camera SIRIUS [2] on the 1.4-m telescope,
IRSF, at the South African Astronomical Observatory(SAAO). Now, SIRPOL has two polarization modes,
linear polarization and circular polarization modes.
The polarization happens when dust reflects the lightfrom the illuminating stars or absorb the light from thebackground stars. Thus, the imaging polarimetry canreveal the distribution of the reflection nebula and thecharacteristic of the dust in the region, and discover
the illuminating stars. In addition, we can reveal thestructure of the magnetic fields in the observing area
using polarimetry of the background stars because dust
grains are aligned by the magnetic fields. In particular,
near infrared polarimetry makes it possible to reveal thestructure of reflection nebulae and magnetic fields in starforming regions because infrared observations can detect
the objects in high dusty regions.
However, in spite of its usefulness for understanding
the physical characteristics, “wide-field” infrared
polarimetry has been scarcely carried out because of thelack of an appropriate polarimeter. Thus, the study withpolarimetry toward even nearby star-forming regions wasvery limited.
Figure 1 shows JHKs composite images of the S106
cluster forming region. Fig. 1(a) is the image in intensity
and Fig. 1(b) is the same image but in only polarized
intensity. We could easily find the clear difference
between these two images. The distribution of thepolarized intensity has the characteristic structures on theeastern and western edges of the S106 nebula and aroundthe exciting star, IRS 4. Compared with the distributionof the molecular gas, the ridges of the polarized intensity
are corresponding to the boundary of the molecular cloud,and we suggest that the polarized components originate
in the light reflected by the dust grain in the dense gas. In
addition, we found two small infrared reflection nebulae(SIRNe). Two SIRNe in Fig. 1(b) have the polarizedcomponent with a small size, and in particular, SIRN 1 isassociated with an early B protostar.
Figure 2 shows the aperture polarization vector
map of point-like sources in the H-band. We found thedifference between the polarization angle and the axis of
the S106 nebula because the overall polarization angle
distribution of the area outside the cluster is ~120°.
However, corresponding to the results of sub-millimeter
observations, we revealed that the magnetic field was
drawn into the center of the cluster. We suggested that

this feature was caused by the clear difference between
the rotation axis and the position angle of the magnetic
field.

I Scientific Highlights(Univ. of Tokyo)

Figure 1: NIR three-color composite images of the S106 nebula inintensity (a) and in polarized intensity (b).

Figure 2: Polarization vector of each point-like source on the
H-band image.

References[1] Kandori, R., et al.: 2006, SPIE, 6269, 159.
[2] Nagayama, T., et al.: 2003, SPIE, 484, 459.
[3] Saito, H., et al.: 2008, AJ, 137, 3149.

Discovery of the Multiple-Core Systems toward Cluster-Forming Regions
YONEKURA, Yoshinori

NAKAMURA, Fumitaka(Osaka Prefecture University) 		

Most stars in the galactic disk are formed as a cluster
in dense gas within giant molecular clouds as membersof clusters [1]. The cluster consists of stars of various
masses, and massive stars exist at the centers of clusters.
Thus, clusters must play a critical role in the origins ofsome of the most fundamental properties of the galactic
stellar population. Recently, observational results
suggested that clusters are formed in the clumps with acluster size scale [2] and that a few hot cores (0.03 pc)
exist in cluster-forming regions. On the other hand, many
cores must be formed in one clump to create a clusterwith a large number of stars. Therefore, we carried out
to reveal the inner structure of the clump with cluster
formation.
We identified 171 cores in six clumps with cluster
formation using Nobeyama Millimeter Array. The left
panel of Figure 1 shows the relationship between theline width and the radius of the cores and 18 clumps
identified by [2]. Although the line width of the clumps isin a narrow range, the line width of the cores is in a muchwider range. Such features are seen even in the individual
regions in the right panels of Figure 1. This indicatesthat the degree of the dissipation of the turbulent motion
varies even within a single clump.
Figure 2 shows that the mass of the cores increases
in proportion to the square of the line width, although
the dispersion of the plot is large. Considering that theinternal kinetic motion basically decreases with time,from this tendency, dense gas with a large kinetic motion
in a clump seems to be necessary to form massive cores.
The stellar number density of the cluster is mentioned
as an important characteristic of a cluster. The stellar
number density of the cluster is generally much higher
than that of typical low-mass star-forming regions. The
recent results found a good relationship between thenumber density of YSOs with the clump and the H 2density of the clump [2]. Figure 3 shows the relationshipbetween the number density of the cores in the clump andthe H2 density of the clump. A good correlation exists
between the core number density and the H2 density of
the clump. This indicates that the stellar number density
in the clump is controlled the core-formation mechanism.
We determined that the mechanism of cluster
formation would strongly depend on the mechanismof core formation and that the mechanism of coreformation would be controlled by both the H2 density
structure and the kinetic motion in a clump. Moreover,the characteristics of the cluster would be determined by
the distribution of the physical parameters of cores in theclump [3].

0.8
0.6

(Nigata University)

all

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log (R core/clump (pc))

0.0log (∆V core/clump (km s-1)) log (∆V core/clump (km s-1))(NAOJ)		

log (∆V core/clump (km s-1))

SAITO, Hiro, SAITO, Masao
		

0.8
0.6

GL 5162

GL 6366s

GL 5182

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GL 2455

0.4
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0.0

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0.0

-1.5

-1.0

-0.5

log (R core/clump (pc))

0.0

Figure 1: The correlation between the radius and the line widthof cores/clumps. The circles and squares indicate coresand clumps, respectively. The white, gray, and black
symbols indicate the objects without, with YSOs, andwith massive stars, respectively. The long- and shortdashed lines indicate the relationships of ΔV ~ R0.06 and~ R0.89, respectively.

∆

Figure 2: The LTE mass plotted against the line width of the cores.
The symbols are the same as in Figure 1.

Figure 3: The number density of the cores in each clump plottedagainst the average H2 density of the clump.

References[1] Lada, C. J., Lada, E. A.: 2003, ARA&A, 41, 57.
[2] Saito, H., Saito, M., et al.: 2008, ApJ, 659, 459.
[3] Saito, H., Saito, M., et al.: 2009, ApJS, 178, 302.

I Scientific Highlights

027

Four-Quadrant Phase Mask Coronagraph with a Jacquinot-Lyot Stop
MURAKAMI, Naoshi*
		

UEMURA, Ryosuke, BABA, Naoshi, SATO, Yoichiro(NAOJ)					(Hokkaido University)

NISHIKAWA, Jun, TAMURA, Motohide(NAOJ)For direct detection of Earth-like extrasolar
planets, extremely high dynamic range is required forcoronagraphs. A four-quadrant phase-mask (FQPM)
coronagraph is one of the most promising methods inthat it has a relatively small inner working angle, large
discovery space, and high optical throughput withtechnically simple instrumentation [1]. The FQPM isput on a focal plane to divide a stellar image into fourquadrant regions and provide π-phase difference between
the adjacent quadrants (Fig. 1). This causes destructive
interference inside the pupil area on a following reimaged
pupil plane, where a Lyot-stop is put to block stellar lightdiffracted outside the pupil. Theoretically, the FQPM
coronagraph can realize perfect stellar elimination forpoint-like stars. However, the FQPM coronagraph isvery sensitive to tip-tilt errors and finite stellar angularsizes. Thus residual stellar noise would prevent us fromdetecting faint companions around partially resolved
nearby stars.
To solve this problem, we propose to use a Jacquinot
pupil as a Lyot stop of the FQPM coronagraph [2]. The
Jacquinot pupil has a Gaussian-like shaped edge, as
shown in Figure 1, to suppress a stellar diffraction haloin specified regions of the focal plane (so-called working
region) where planetary signals can be detected. We
manufactured the Jacquinot pupil by means of a chemical
etching process on a nickel substrate (diameter of 1.125mm and thickness of about 20 μm), and conductedlaboratory experiments of the FQPM coronagraph. As
the FQPM, we used a four-quadrant polarization mask
(FQPoM) utilizing polarization interferometry [3].
Figure 2 shows coronagraphic images, acquiredwith a He-Ne laser (λ = 633 nm), for the circular- andJacquinot-Lyot stops for tip-tilt errors from 0.1 to 0.3
λ/D. Dotted lines and an arrow in the image (top left)show boundaries of the FQPoM and a tip-tilt direction,
respectively. As can be seen in the results, the residual
halo for the circular-Lyot stop increases rapidly with the
tip-tilt error, while that for the Jacquinot-Lyot stop canbe well suppressed (1.4 × 10−6 at 7.5 λ/D) in the working
regions (dashed circles) even for the large tip-tilt errorof 0.3 λ/D. Consequently, the laboratory experiments
demonstrate that the Jacquinot-Lyot stop would enhance
the FQPM-coronagraphic performance effectively.

* Present address: Hokkaido University028

I Scientific Highlights

Figure 1: A schematic optical setup of a FQPM coronagraphequipped with a Jacquinot-Lyot stop.

Circular-Lyots top

tip-tilt
10-4

Jacquinot-Lyot stop

10-7
0.1

0.2

0.3 [λ /D]
Tip-tilt error

Figure 2: Results of laboratory experiments of a FQPM
coronagraph with circular- and Jacquinot-Lyot stops forvarious tip-tilt errors.

References[1] Rouan, D., et al.: 2000, PASP, 112, 1479.
[2] Murakami, N., et al.: 2008, ApJ, 677, 1425.
[3] Baba, N., et al.: 2002, Opt. Lett., 27, 1373.

An Eight-Octant Phase-Mask Coronagraph
MURAKAMI, Naoshi*
			

NISHIKAWA, Jun, TAMURA, Motohide			

UEMURA, Ryosuke, BABA, Naoshi(NAOJ)			

(Hokkaido University)

HASHIMOTO, Nobuyuki

ABE, Lyu(CITIZEN Holdings Corp.)(Universit´e de Nice-Sophia Antipolis)(NAOJ)			

For direct detection and characterization of extrasolar
planets, light from their parent stars must be strongly
suppressed by coronagraphs. We propose an eight-octant
phase-mask (EOPM) coronagraph [1], which is analogous
to a previously proposed four-quadrant phase-mask(FQPM) one [2] (Fig. 1). It is expected that the EOPM
coronagraph has fourth-order sensitivity to tiptilt errors
while the sensitivity of the FQPM one is second-order.
This higher order behavior of the EOPM coronagraphwill be advantageous for observations of partiallyresolved nearby stars.
Figure 2: A manufactured liquid-crystal phase-mask, and acquired
and numerically simulated Lyot-stop images of FQPMand EOPM-mode.

0.16

Figure 1: Principles of FQPM and EOPM coronagraphs.

We manufactured an eight-segmented phase-mask
utilizing a nematic liquid-crystal (LC) device (Fig. 2). A
phase retardation of each segment can be adjusted by anapplied voltage to the device via flexible printed circuits(FPC). The LC phase-mask can be switched between
FQPM- and EOPM-mode by applying voltages toappropriate segments (e.g., segments L1, L3, R2, and R4
for the EOPM-mode).
We carried out laboratory experiments of thephasemask coronagraphs by using a He-Ne laser (λ =633 nm). In Figure 2, acquired Lyot-stop images for theboth coronagraphic modes are also shown together withthose of numerical simulations. Figure 3 shows residual
intensity of acquired coronagraphic images as a functionof a tip-tilt error. The coronagraphic images for 0.4 λ/D
tip-tilt error are also shown. Note that we subtract a zerotip-tilt coronagraphic image from each one to eliminate
speckle noise in order to evaluate residual intensity due
to only the tip-tilt error. As can be seen in the results, theresidual intensity can be well suppressed by the EOPM
coronagraph because of its fourth-order behavior.

Normalized integrated intensity

0.14
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FQPM
(Second-order)

0.06
0.04

EOPM
(Fourth-order)

0.02
0
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0.2

0.4

0.6

0.8

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Tip-tilt [lambda/D]

Figure 3: Residual intensity of FQPM and EOPM coronagraphs asa function of a tip-tilt error. Coronagraphic images for 0.4
λ/D tip-tilt error are also shown.

References[1] Murakami, N., et al.: 2008, PASP, 120, 1112.
[2] Rouan, D., et al.: 2000, PASP, 112, 1479.

* Present address: Hokkaido University

I Scientific Highlights

029

Variation of the Subhalo Abundance in Dark Matter Halos
FUKUSHIGE, Toshiyuki

MAKINO, Junichiro(K&F Computing Research Co.) 		
1000

100

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0.2

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Figure 2: Cumulative numbers of subhalos as a function of theirmaximum rotation velocities Vc normalized by thoseof the parent halos Vp for 68 galaxy-sized halos with
1.5 × 10 12 M  ≤ M < 3 × 10 12 M  . Three thick solid
curves show the average (middle) and ±1σ values (topand bottom). Red line are the result of [2] for a galaxysized halo. The thin dashed curve with open triangles
denotes the number of dwarf galaxies in our galaxy. The
open circles with error bars show the number of dwarf
galaxies in the Local Group.

100

50
N>0.10

Moore et al. (1999) and Klypin et al. (1999) calculated
the evolution of galaxy-scale dark mater halos using highresolution cosmological N-body simulations. They foundthat dark matter halos of the mass comparable to the
Local Group contained far too many subhalos comparedto the number of known dwarf galaxies in the Local
Group. In the case of dark matter halos of the size oftypical clusters of galaxies, thetheoretical prediction andobservation agreed pretty well. The theoretical prediction
for galaxy-sized and cluster-sized halos are similar, andobservations of clusters of galaxies and that of Local
Group are very different [1, 2]. This discrepancy is now
called “the missing dwarf problem”.
We analyzed the statistics of subhalo abundance ofgalaxy-sized and giant-galaxy-sized halos formed in ahigh-resolution cosmological simulation of a 46.5 Mpc
cube with the uniform mass resolution of 106M. We
analyzed all halos with mass more than 1.5 × 1012M
formed in this simulation box. The total number of halos
was 125. We found that the subhalo abundance shows
large halo-to-halo variations. The results of recent ultrahigh-resolution runs fall within the variation of oursamples. We found that the concentration parameter andthe radius at the moment of the maximum expansion
show fairly tight correlations with the subhalo abundance.
This correlation suggests that the variation of the subhalo
abundance is at least partly due to the difference in theformation history. Halos formed earlier have smaller
number of subhalos at present [3, 4].

(NAOJ)

Nc(Vc)ISHIYAMA, Tomoaki(NAOJ/University of Tokyo)

30

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c
Figure 3: Dependence on the concentration parameter c of thesubhalo abundance. More centrally concentrated halos
are generally formed earlier.

Figure 1: Snapshot (z = 0).

030

I Scientific Highlights

References[1] Klypin, A., et al.: 1999, ApJ, 522, 82.
[2] Moore, B., et al.: 1999, ApJL, 524, L19.
[3] Ishiyama, T., et al.: 2008, PASJ, 60, L13.
[4] Ishiyama, T., et al.: 2009, ApJ, 696, 2115.

Tycho’s Supernova is of Type Ia~Super explosion in 16th century caught by Subaru in 21st century~
USUDA, Tomonori, HATTORI, Takashi
		

KRAUSE, Oliver, BIRKMANN, Stephan M., GOTO, Miwa

(NAOJ)					(Max-Planck-Institut for Astronomy)

TANAKA, Masaomi, NOMOTO, Ken’ichi(University of Tokyo)

On the evening of 11 November 1572, Tycho
Brahe, a Danish astronomer observed a bright star in
the constellation Cassiopeia, outshining even Venus.
He studied the brightness and color of the “new star”
until March 1574 when it faded from view. On thebasis of historical records of the light curve and colour
evolution, it has been interpreted as a type Ia supernova
of either a normal or somewhat overluminous type or ofa subluminous type. Core-collapse supernovae of typeIb or II-L have also been suggested to be compatible
with the light curve, however the determination of theexact supernova type has not been possible without
spectroscopic information.
We started to observe the identified light-echo fieldsof SN 1572 using the 2.2-m and 3.5-m telescopes at the
Calar Alto Astronomical Observatory, on 23 August 2008
and 2 September 2008, and found a bright and extended
nebulosity with a peak surface brightness of R = 23.6 ± 0.2
mag arcsec−2 (Figure 1a).
The region was re-observed using the Faint Object
Camera And Spectrograph (FOCAS) at the Subaru 8.2m telescope on Mauna Kea, Hawaii, on 24 September
2008 (Figure 1b). The peak of the emission, with asurface brightness of R = 23.5 ± 0.2 mag arcsec−2 hasagain shifted away from SN 1572. A long-slit spectrumof the brightness peak of the echo structure was obtainedwith FOCAS on the same night, covering the wavelength
range from 3,800 to 9,200 Å with a spectral resolution of
24 Å. The acquired echo spectrum unambiguously shows
light of a supernova origin (Figure 2), a number of broad
absorption and emission features from neutral and singly
ionized intermediate mass elements. Type I supernovae
are distinguished from those of type II by the absence ofhydrogen, and type Ia supernovae are further distinguishedfrom types Ib and Ic by a prominent Silicon 6,355 Å
absorption feature at maximum light. We have compared
the spectrum of SN 1572 with thermonuclear supernovaeof different luminosity. Both sub- and overluminous
type Ia supernovae, such as SN 1991bg and SN 1991T,
respectively, showed peculiarities in their spectra near
maximum light. We concluded that SN 1572 belongs to
the majority class of normal type Ia supernovae [1].

Figure 1: (a) Optical R-band images of the Tycho ’s supernova
light echo taken by Calar Alto 3.5 m telescope (blackmeans bright). The rectangle shown in a indicates thelocation of a previous light-echo detection in 2006. The
vector towards Tycho’s supernova remnant is indicated(arrow). (b) R-band images taken by FOCAS on Subaru
Telescope.

Figure 2: Spectrum of Tycho’s supernova obtained by FOCAS.
Black solid lines show the spectrum of Tycho’s SN.
Comparison with templates of subluminous (red),
normal (orange) and overluminous (blue) type Ia
supernova.

Reference[1] Krause, O., et al.: 2008, Nature, 320, 1195.

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031

Supernova Remnant Cassiopeia A:
Decoding Light to Uncover the Mystery of its Birth
USUDA, Tomonori, HATTORI, Takashi
		

KRAUSE, Oliver, BIRKMANN, Stephan M., GOTO, Miwa

(NAOJ)					(Max-Planck-Institut for Astronomy)

RIEKE, George H., MISSELT, Karl A.
(Steward Observatory)

The supernova remnant Cassiopeia A (Cas A) is oneof the most-studied objects in the sky, with observations
from the longest radio waves to gamma rays. The lack ofa definitive sighting means that there is almost no direct
information about the type of the explosion, and the true
nature of its progenitor star has been a puzzle since thediscovery of the remnant. There is no chance to see theprecise date when it happened, or how it looked like at thetime of the outburst. The outburst supposedly happened
in approximately 1680, judging from the current
expansion rate. It is a mystery, however, why there is no
widely recorded sighting of such an extravagant outburst
in the 17th century, happened just 11,000 light years
away form the earth. The light echo is a phenomenon thatthe wave of light is reflected or re-emitted by the material
located away from its origin, and arrives to the observerwith a delay. The light echo of Cas A we see today istherefore the light of the outburst that arrived on the earth
300 yrs after the direct light sweeps out the planet. No
need to say, this light echo hides the secret of the birth of
Cas A within. We started regular patrols of the region by
Spitzer Space Telescope in the infrared wavelength, andwide field monitoring observation by MPIA Calar Alto
2.2 m telescope in Spain. The candidates were found in
September 2007.
On the night of 9 October 2007, the light echo (R =23.5 mag) was confirmed with FOCAS (Fig. 1), and we
started the spectroscopy. After 5.5 hours exposure, we
got a spectrum showing the clear spectral lines, the finger
prints of a very young SN (Fig. 2). Comparing with thedata in the spectral database of various supernovae, we
found that the spectra of the light echo is almost identicalwith that of SN 1993J (Fig. 2). The progenitor of Cas
A must be the same with that of SN1993J: a red super
giant more massive than 10 times of the solar mass.
And they went through the same type of outburst: Type
IIb. A supernova outburst of the type IIb is relatively
faint (M V = −17.5) and fades away fast. Unfortunate
weather of mere several days, that somehow overlappedwith the maximum of the light curve, would be enoughto let this young supernova escaped away from thehistory. At a relatively faint brightness, the light of theCas A supernova event would have been extinguishedrelatively quickly by the dust grains in the foregroundof the expanding supernova remnant along with thecharacteristically fast decay of light from a Type IIb

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I Scientific Highlights

outburst. With these findings, the answer to our historical
puzzle seems to be finally obtained.

Figure 1: Optical image of the echo region. It is a color compositeof I-band (red), R-band (green), and V-band (blue) by
FOCAS at Subaru Telescope. The faint white features in
the middle of the image are the light echoes.

Figure 2: Spectrum of the Cas A supernova (upper) taken by
FOCAS on 9 October 2007 and SN 1993J for a reference(bottom).

Reference[1] Krause, O., et al.: 2008, Science, 320, 1195.

Detections of Strong Ionizing Radiation from High-redshift Galaxies
IWATA, Ikuru, FURUSAWA, Hisanori
			(NAOJ)			

INOUE, Akio K.

MATSUDA, Yuichi(Osaka Sangyo University)(Durham University)

HAYASHINO, Tomoki, KOUSAI, Katsuki, AKIYAMA, Masayuki, YAMADA, Toru
(Tohoku University)

BURGARELLA, Denis, DEHARVENG, Jean-Michel(Laboratoire d’Astrophysique de Marseille, France)

Ionizing radiation from star-forming galaxies is alikely primary source of cosmic reionization. Although
the emissivity of Lyman continuum (LyC) from galaxies
is a key to evaluate the contribution of galaxies to cosmic
reionization, it has been poorly constrained due to the factthat LyC photons are easily absorbed by the intergalactic
medium (IGM). Since direct observation of LyC at z >4 is virtually impossible because of a rapid increase in
the number density of Lyman limit systems toward highredshifts, we must focus on z ~ 3 where the IGM opticaldepth is still about unity on average. So far the numberof galaxies with direct observation of LyC was too small
to reveal the typical LyC emissivity. It is because thespectroscopy for LyC search requires much observing
time for each target galaxy, and the number of galaxies
observed was limited.
In order to confront this issue, we adopted a novel
technique: imaging observation with a narrow-band
filter to trace the LyC from galaxies at a specific redshiftenables us to examine LyC from a large number ofgalaxies simultaneously. The target field of the present
study is the SSA22 field where the prominent protocluster of galaxies at z = 3.09 has been discovered, andthere are 198 galaxies with spectroscopic redshifts in
one Subaru / Suprime-Cam field. We fabricated a special
narrow-band filter NB359 (central λ = 359 nm with
_ 3.1
FWHM = 15 nm) to examine LyC from these z ~galaxies, and executed observation in Sep. 2007.
We detected 7 Lyman break galaxies (LBGs) and 10
Lyman α emitters (LAEs) in NB359 among 198 galaxies
with spectroscopic redshifts ([1]; Fig. 1). There are some
objects with significant spatial offsets between LyC andnon-ionizing UV radiation.
In Figure 2 colors of the detected galaxies areplotted. NB359-R color stands for the ratio of LyC andnonionizing UV radiation, while V–i′ color represents
UV slope. Most LAEs have NB359-R color bluer than
LBGs. We also show predicted colors of model spectralenergy distribution generated by the population synthesis
code with Salpeter initial mass function, low metallicity
and zero age. The colors which can be reproduced byconsidering dust and IGM attenuation are indicated withthe shaded area. Because increasing age or metallicity
make NB359-R color redder, the colors of detectedgalaxies (especially LAEs) cannot be explained with suchstandard stellar populations. This result would indicate
the existence of strong sources of ionizing radiations
among high redshift star-forming galaxies, which might
be a counterpart of galaxies in the cosmic reionization
epoch. Further investigation including deep spectroscopy
is required to clarify the nature of such strong LyC
emitters.

Figure 1: Examples of galaxies with LyC detection. In UV(R-band) images contours of NB359 images are overplotted.

Figure 2: NB359-R and V−i′ colors of galaxies with LyC
detection.

Reference[1] Iwata, I., et al.: 2009, ApJ, 692, 1287.

I Scientific Highlights

033

Okayama Astrophysical Observatory has discovered ten exoplanets		

SATO, Bun’ei

OMIYA, Masashi

TOYOTA, Eri(Tokyo Institute of Technology)(Tokai University)(Kobe University)

IZUMIURA, Hideyuki, KAMBE, Eiji, YOSHIDA, Michitoshi
				(NAOJ/OAO)			

MASUDA, Seiji(Asutamu Land Tokushima)

TAKEDA, Yoichi, ANDO, Hiroyasu, KOKUBO, Eiichiro(NAOJ)

ITOH, Yoichi, MURATA, Daisuke			(Kobe University)		

Since the first discovery of the extrasolar planet
in 1995, more than 300 extrasolar planets have been
discovered so far. While most of them orbits around FGK
dwarfs (0.7–1.5 M), so-called solar-type stars, about 20
planets orbit around GK-type giants (1.5–4 M). Suchintermediate-mass stars are unsuitable for Doppler planet
searches when they are on the main sequence (early-typestars) because they have few absorption lines in theirspectra, which are often rotationally broadened, and thus
it is difficult to attain high precision in radial velocity
measurements. On the other hand, late-G to early-K typegiants, which are evolved from early-type dwarfs, have
many sharp absorption lines in their spectra appropriate
for precise radial velocity measurements due to low
surface temperature and small rotational velocity. Thus,
giant stars are now regarded as ideal targets for planet
searches around intermediate-mass stars.
Since 2001 we have been carrying out a Doppler
planet search program targeting about 300 GK giants
using the 1.88 m telescope and HIgh Dispersion Echelle
Spectrograph at Okayama Astrophysical Observatory. We
discovered seven new planets in 2008 from the program[1, 2]. The planets have minimum masses of 1.6–10 MJUP
, semimajor-axes of 0.7–2.6 AU, and eccentricities of 0–0.2. Their host stars have masses of 1.6–2.7 M. The
number of our discoveries reached at 10, which is about ahalf of the currently known planets around giant stars.
One of the interesting properties of planets aroundgiants is paucity of inner planets. All of the known
planetary companions to giant stars orbit beyond 0.7 AU
and no planets have been found within the limit. Two
scenarios can account for the orbital distribution; oneis that inner planets are primordially deficient aroundintermediate-mass stars and the other is that they havebeen engulfed by the expanding central stars due tostellar evolution. When we assume that many of clump
giants are post-RGB stars (core-helium-burning stars),planets in orbits with <~ 0.5 AU could have been engulfed
by the central stars at the tip of RGB (Rstar ~ 25–40 R fora 2–3 M star) due to tidal force from the central stars. It
means that we can not reject the possibility that planets
had originally existed in short orbital distances aroundprogenitors of clump giants. Other interesting properties

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IKOMA, Masahiro, IDA, Shigeru(Tokyo Institute of Technology)of planets to giants, such as higher frequency of supermassive planets with ~> 5 MJUP compared to the case ofsolar-type stars and lack of metal-rich tendency in planethost giants, have begun to emerge [3]. We try to increase
the number of targets and detected planets further in order
to confirm their statistical properties.

Figure 1: Planet mass plotted against semimajor axis. Planets
around low-mass (< 1.6 M  ) giants, intermediatemass subgiants (1.6–1.9 M), and clump giants (1.7–
3.9 M), are plotted by red, green, and blue triangles,
respectively. Planets around solar-type dwarfs are plottedby open circles. Dashed lines express detection limits
with velocity semiamplitude of 10 m s−1 and 40 m s−1
around a 2 M star. Since giants have intrinsic variability
in radial velocity of 10–20 m s−1 due to stellar activity,
it is difficult to detect planets which impart velocity
variations less than 40 m s−1 to central stars.

References[1] Sato, B., et al.: 2008, PASJ, 60, 539.
[2] Sato, B., et al.: 2008, PASJ, 60, 1317.
[3] Takeda, Y., Sato, B., Murata, D.: 2008, PASJ, 60, 781.

Fe XIII Density Diagnostics in the EIS Observing Wavelengths
WATANABE, Tetsuya, HARA, Hirohisa
				(NAOJ)			

YAMAMOTO, Norimasa(Osaka University)

KATO, Daiji, SAKAUE, Hiroyuki A., MURAKAMI, Izumi, KATO, Takako(NIFS)NAKAMURA, Nobuyuki
					(UEC)			The EUV Imaging Spectrometer (EIS) on board the
Hinode satellite observes solar emission lines at EUV
wavelengths with high spatial and spectral resolution [1].
The two wavelength bands observed with EIS are 170–210 Å and 250–290 Å, and include emission lines ofHeii and a wide range of iron ions from Feviii through to
Fe XXIV, formed in the temperature range 4.7 ≤ log Te ≤ 7.2.
Among the emission lines of the various iron species,
the Fe XIII lines found in the EIS short wavelength band
(170–210 Å) are particularly important, as they provide
several line pairs sensitive to the density of the coronalplasma. As an independent parameter to the emission
measure, the density is crucial to determining the plasma
filling factor, i.e., the fraction of the observed plasma
volume that is emitting radiation.
The diagnostic capability of Fe XIII line features seenin the EIS observing wavelengths has been studied. Full
CCD slit spectra of the EIS first-light active region AR
10921 observed in the short wavelength band (170 Å–
210 Å) are used to provide a dataset of Fe XIII emission
lines, and their intensities are compared with twotheoretical models for density diagnostics: The first isa modification of the CHIANTI v5.2 model [2] that is
modified to use the Gupta-Tayal (1998) [3] electron
collision file, and the second is the model of Yamamoto
et al. (2008) [4] (hereafter Y08) that uses the electron
collision data of Aggarwal and Keenan (2005) [5].
Derived electron densities are plotted against theposition along the slit in Figure 1. In the density range
from 108.5 to 109.5 cm−3 the four density diagnostic line
pairs; λ96.5 Å, λ200.0 Å, λ203.2 Å, and λ203.8 Å vsλ202.0 Å give consistent densities. These are all stronglines appearing in the EIS waveband except λ203.2 Å.
The Y08 model gives slightly better consistency between
the ratios than the modified CHIANTI model for thesestrong line pairs.
For other Fexiii lines we find problems with both of
the theoretical models: from the Y08 model, λ204.3 Åand λ209.6 Å are not well predicted; while for themodified CHIANTI model λ204.3 Å and λ204.9 Å areinconsistent with observations. They are generally weaklines seen in the EIS waveband, and the problems withthe λ209.6 Å and λ209.9 Å may be partly due to the
instrument calibration, as they lie very close to end of the
EIS waveband.

Young, P. R.
(NRL)The accuracy of the high density limit of theimportant λ203.8 Å/λ202.0 Å density sensitive ratio has
also been investigated, using an EIS observation of a
C-class flare from on 2007 January 16. The measured
ratio is consistent with the theoretical predictions bothfrom the Y08 and modified CHIANTI models.
Watanabe et al. (2009) [6] describe the detail of theanalysis.

Figure 1: Densities derived from observed line ratios at thepositions (pixel numbers: 200–300) along the slit. Total
intensity of Fe XIII λ202.0 Å is plotted in the top-leftpanel. Solid lines are for the model of Y08 and dottedlines are for the CHIANTI.

References[1] Culhane, J. L., et al.: 2007, Sol. Phys., 243, 19.
[2] Landi, E., et al.: 2006, ApJ, 162, 261.
[3] Gupta, G. P., Tayal, S. S.: 1998, ApJ, 506, 464.
[4] Yamamoto, N., et al.: 2008, ApJ, 689, 646.
[5] Aggarwal, K. M., Keenan, F. P.: 2005, ApJ, 429, 1117.
[6] Watanabe, T., et al.: 2009, ApJ, 692, 1294.

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035

Laser interferometric high-precision geometry monitor for JASMINE
NIWA, Yoshito(NAOJ/Kyoto University)		

ARAI, Koji, UEDA, Akitoshi

SAKAGAMI, Masaaki(NAOJ)			

(Kyoto University)

GOUDA, Naoteru, KOBAYASHI, Yukiyasu, YANO, Taihei

A heterodyne metrology interferometer was
stabilized down to a noise level of 20 picometers (pm)as a rootmean- square (RMS) value integrated between
0.3 mHz and 1 Hz. This interferometer can be used inprecise metrology applications, such as characterizationof deformation for satellite optical components against
thermal exposure.
JASMINE (Japan Astrometry Satellite Mission
for Infrared Exploration) [1] is one of next-generation
astrometry satellite missions and aims to measure
parallaxes, positions and proper motion with theprecision of 10 microarcsec for ten million stars in thebulge of the Milky Way. Now, we are developing smallJASMINE, which is a downsized version of JASMINE
and planed to be launched around 2015. In order torealize high-precision astrometric observation, geometryof a small-JASMINE telescope with the structure size of
approximately 1 m should be stabilized with an accuracyof 100 pm in RMS value for a frequency range from
1 mHz to 1 Hz. In order to ensure such requirement byground experiments, thermal deformation properties oftelescope materials should be measured with the sameaccuracy under the similar environment to space. A
heterodyne metrology interferometer can be used as ahigh-precision displacement sensor for such a laboratory
test. Then, we had begun to develope a heterodyne
metrology interferometer [2] and stabilized it so as toverify that a noise level satisfies the requirement forsmall-JASMINE.
A conceptual design of our heterodyne metrology
interferometer is shown in Fig. 1. The heterodyne
interferometer was built on a 50 mm square ultra-low
expansion glass plate (OHARA, CLEARCERAM® -Z)
in order to reduce an optical path length change causedby temperature variation. Optical components are bonded
to the glass plate by hydroxide-catalysis bonding so as
to make the whole structure virtually monolithic. An
optical configuration of the interferometer is a MachZehnder interferometer with a design as symmetric as
possible so that a detection signal can be insensitive tohomogeneous thermal expansion of the glass plate. The
heterodyne frequency is actively controlled in order tosuppress residual noises that are caused by optical path
length changes outside of the glass plate as well as phasefluctuations of the heterodyne frequency source. Thisconfiguration allowed us to concentrate our effort forstabilization only at a 50 mm square optical base plate.
Figure 2 shows the power spectrum density and the036

I Scientific Highlights

YAMADA, Yoshiyuki(NAOJ)			

(Kyoto University)

RMS of the displacement measured by the stabilizedinterferometer. The displacement RMS noise level is
20 pm for the frequency range from 1 Hz to 1 mHz. This
meets the requirement for small-JASMINE.
NP B S

N d : YAGla s er

AO M2

O p ti c a l ba s e pl at e

f2

f1
M

PD2

AO M1

f he tPD1

f he tVa c uum c ha m be r

LO 1
To AO M1

PD1

f1

f he t = f 1 - f 2
f he tf2

To AO M2

LO 2

PD2

VC O

f he tR efe re nc es ign a l

Loop filter

DB M

Me a s ur em en ts ign a l
Di gi ta llo c k -in a m p.

Di gi ta llo c k -in a m p.
DA Q
PCFigure 1: Schematic drawing of a heterodyne interferometer.

Displacement (m/rtHz)

				

10

-7

10

-8

10

-9

10

-10

10

-11

10

-12

(a)

(b)

10

-4

10

-3

-2

10
Frequency (Hz)

10

-1

10

0

Figure 2: The displacement noise level of the stabilized interferometer: (a) the power spectrum density, (b) the RMS.

References[1] Gouda, N., et al.: 2008, Proc. of IAU Symp., 248, 248–251.
[2] Niwa, Y., et al.: 2008, SPIE, 7018, 70183D-1–70183D-12.

Three-dimensional Simulation of Magnetized Cloud Fragmentation
Induced by Nonlinear Flows and Ambipolar Diffusion
				

KUDOH, Takahiro

BASU, Shantanu(NAOJ)(University of Western Ontario)
Time = 20.5
1.5
1.0
0.5
0.0
-0.5
-1.0
-1.5
-2.0

= 3.00

20

10

0

y

We demonstrate that the formation of collapsingcores in subcritical clouds is accelerated by nonlinear
flows, by performing three-dimensional non-ideal MHD
simulations [1]. (In the subcritical clouds, magnetic force
suppress the gravitational collapse unless the magnetic
diffusion works.) This is the first 3D simulation thatwould alter the previous estimation of the starformation
time scale.

-10

-20

z

-20

Figure 1: The time evolution of maximum densities at z = 0. The
solid line shows the evolution for an initially nonlinear
supersonic perturbation and β0 = 0.25 (see Fig. 2). The
dashed line (β0 = 0.25) and the dash-dotted line (β0 =4) show the evolution for models with a linear initial
perturbation as calculated by Kudoh et al. (2007) [2].
The dotted line shows the evolution for an initiallynonlinear supersonic perturbation and β0 = 0.25, but
without ambipolar diffusion. The time unit t0 is about 2.5
× 105 years in this model.

An initial random supersonic (and trans-Alfvénic)turbulent-like flow is input into a self-gravitating gas
layer that is threaded by a uniform magnetic field(perpendicular to the layer) such that the initial massto-flux ratio is subcritical. (In this model, the subcriticalmeans β 0 < 1, where β 0 is the initial ratio of gas tomagnetic pressure at z = 0.) Magnetic ambipolar diffusion
occurs very rapidly initially due to the sharp gradients
introduced by the turbulent flow. It subsequently occurs
more slowly in the traditional near-quasistatic manner,
but in regions of greater mean density than present in theinitial state. The overall timescale for runaway growth of
the first core(s) is several ×106 yr, even though previous
studies have found a timescale of several ×107 yr whenstarting with linear perturbations and similar physicalparameters (Fig. 1, 2).

2
0
-2

-10

0
x

10

20
= 3.00

-20

-10

0
x

10

20

Figure 2: Logarithmic density image at t = 20.5 t0 for the nonlinear
perturbation case of the subcritical cloud (β0 = 0.25).
The top panel shows the cross section at z = 0, and thebottom panel shows the x–z cross section at y = −5.9 H0,
where H 0 is the scale height of the gas layer (H 0 ~0.05 pc). A collapsing core is formed in the vicinity of x
= −20 H0 and y = −6H0.

Large-scale supersonic flows exist in the cloudand provide an observationally testable distinguishing
characteristic from core formation due to linear initial
perturbations. However, the nonlinear flows have decayedsufficiently that the relative infall motions onto the firstcore are subsonic, as in the case of starting from linear
initial perturbations. The ion infall motions are very
similar to those of neutrals; however, they lag the neutral
infall in directions perpendicular to the mean magnetic
field direction and lead the neutral infall in the direction
parallel to the mean magnetic field.

References[1] Kudoh, T., Basu, S.: 2008, ApJ, 679, L97.
[2] Kudoh, T., et al.: 2007, MNRAS, 380, 499.

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037

How was the mushroom-shaped GW 123.4–1.5 formedin the Galactic disk?
BAEK, Chang Hyun*(Jeju Starlight World Park & Planetarium)

KUDOH, Takahiro, TOMISAKA, Kohji
		

GW 123.4–1.5 is a mushroom-shaped HI structurecomposed of a stem and a cap and is dissimilar to any
common shells or chimneys in our Galactic disk. To
understand the origin and velocity structure of GW
123.4 – 1.5, we extend the previous two-dimensionalhydrodynamical simulation [1] of the collision of a highvelocity cloud (HVC) with the Galactic disk to three
dimensions [2].
Figure 1 shows the evolution of column-density on
the x–z plane (integrating along the y-axis) for model O3(the angle from the vertical axis of the Galactic disk is 3°,
the number density is 0.1 cm−3, and the incident speed is
100 km s−1). We can find the mushroom-shaped structures
between t = 56 Myr (or t/t0 = 4.0) and t = 67 Myr (ort/t0 = 4.8). The height of the mushroom at the age of t =67 Myr is about 350 pc, which is the same size as that of
GW 123.4–1.5. The lifetime of the mushroom structure is~107 yr and the width ratio of the cap to the stem is about
3:1. The mass of the cap is about twice that of the stem,and the total mass is estimated to be ~105 M. The mean
column-density contrast between the mushroom andambient medium is about 2:1. Although the mass ratio isa little smaller than the observed one 4:1, most physicalparameters of the mushroom-shaped structure in modelO3 coincide with those of GW 123.4–1.5.
Figure 2 shows the column-density and the positionvelocity maps, which are equivalent to the observational
longitude-velocity (l–v) maps, for model O3. The velocity
gradient in Figure 2b is very similar to the observed valueof GW 123.4–1.5.
GW 123.4–1.5 is expected to be formed by the almost
head-on collision of a HVC with velocity ~100 km s−1 andmass ~105 M about 5×107 yr ago. A mushroomshaped
structure like GW 123.4–1.5 must be infrequent on the
Galactic plane, because the head-on collision which
explains the mushroom structure seems rare for observed
HVCs. HVC-disk collision explains not only the originof the mushroom-shaped structure but also the formationof a variety of structures like shells, loops, and verticalstructures in our Galaxy.
References[1] Kudoh, T., Basu, S.: 2004, A&A, 423, 183.
[2] Baek, C. H., Kudoh, T., Tomisaka, K.: 2008, ApJ, 682, 434.

* Chang Hyun Baek was invited to NAOJ as a Post-Doctoral Fellow by Korea Research
Foundation from October 2006 to September 2007.

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Figure 1: Time evolution of column-density of cool gas on the x–
z plane (integrating along the y-axis). The snapshots are
made at t/t0 = 0, 0.8, 1.6, 2.4 (top: left to right), 3.2, 4.0,
4.8, and 5.6 (bottom: left to right) for model O3.

Figure 2: Column-density (left panels) and position-velocity (rightpanels) at t/t0 = 4.8 in model O3. Position-velocity ismeasured for the lower (z = 2.4 H0) and upper (z = 3.2 H0)regions of the caps on (a) the x–z plane (along the y-axis)
and on (b) the y–z plane (along the x-axis).

Development of a hybrid N-body simulation codefor planet formation process that can handle number of large particles
OSHINO, Shoichi

MAKINO, Junichiro(Graduate University for Advanced Studies)

In the standard model of planet formation scenario
proposed by Hayashi et al., planetesimals evolve
to protoplanets through mutual collisions. N-bodysimulations have been used for the study of this process,and the formation mechanisms such as the runaway
growth and the oligarchic growth have been found. In
previous studies, the number of particles have been
limited to around 104, and therefore minimum particle
mass used was around 10 23 g. However, we need to
examine the behavior of small planetesimal, since it isbelieved that planetesimals of the mass 1016–1019 g are
first formed from dust. Moreover, because there is alimitation in the number of particles that can be handled,
in almost all N-body simulations the assumption of
perfect accretion has been used. This assumption is not
appropriate for the process of the planet growth in thelate stage. Thus a simulation code that can handle a large
number of particles is necessary to study these problems.
It can also handle fragmentation that increases thenumber of planetesimals.
In N-body simulations, the calculation cost increases
as the second power of the number of particles. Moreover,in planet formation simulations, since the formation time(106–107 years) is far longer than the orbital timescale ofplanetesimals, very long calculations are necessary. We
developed a high speed simulation code that can handle
a large number of particles. Since gravity decrease as
the inverse square of the distance, distant particles areorganized to calculate gravity with keeping calculation
cost lower. In addition, it can integrate with long time
steps, because gravity of distant particles have smaller
time variation than that of near particles. Hence, we
can calculate with high accuracy while keeping low
calculation cost and time.
Specifically, we split the mutual gravity of particles
as the distance [1]. The gravity can be divided into
gravity of near particles with rapid variation and thatof distant particles with slow variation. Moreover, thedistant particle gravity is calculated by the tree method[2], because it is relatively small compered to the solar
gravity and forces from nearby particles gravity. They
are calculated by the fourth Hermite scheme with small
and individually variable time steps. It can integrate athigh speed while keeping high accuracy by combining
these methods [3]. Figure 1 shows the relative energy
error as a function of time. The energy error changes
randomly, so this code can integrate the system withsmall error for long calculations. The calculation cost of
this code is about factor 60 smaller than conventional(NAOJ)

direct calculating code for 104 particles. Therefore, for
106 particles our code is 6000 times faster than the direct
calculation. Then we can calculate over 106 particles.

Relative Energy Error

		

5e-08
0
-5e-08-1e-07-1.5e-07-2e-07

0200

400 600
Time [yr]800 1000

Figure 1: Relative energy error as a function of time.

References[1] Chambers, J. E.: 1999, MNRAS, 304, 793.
[2] Barnes, J., Hut, P.: 1986, Nature, 324, 446.
[3] Fujii, M., et al.: 2007, PASJ, 59, 1095.

I Scientific Highlights

039

Wide-Field Infrared Imaging Polarimetry of the NGC 6334 Region:
A Nest of Infrared Reflection Nebulae
HASHIMOTO, Jun

TAMURA, Motohide(Graduate University for Advanced Studies)(Graduate University for Advanced Studies/NAOJ)

KANDORI, Ryo, KUSAKABE, Nobuhiko, NAKAJIMA, Yasushi

HOUGH, Jim, CHRYSOSTOMOU, Antonio(Nagoya University) 				(University of Hertfordshire)Ks band(A) NGC 6334 I

20%
10″

5 ″ 20%40″

IRN I-5

50″

NGC 6334 F

0″-35 °47′ 20″ 10″

IRN I-4

h

m

s

s

55

s

s

54

53

s

s

s

52

s

51

50

H bandI Scientific Highlights

Ks band(D) NGC 6334 IV
5″

2″ 10%

10%

20″

IRS IV-54

IRN IV-1
1″ 10%IRN IV-3

IRN IV-4
IRN IV-2

20 ″49′ 30″5″49′ 00″IRS II-23 IRN II-2

54 ′50 ″ 35 ″48′ 30 ″IRS II-22

IRN IV-6 3″ 10%
IRN IV-5

55 ′50 ″ 35″

50 ′ 00″

IRS II-22
IRS II-24

3″ 5%

5″

-35° 51′ ″00

IRN II-1

17 h20m 58s 56 s

54s

52s

50s

48 s

46s

44 s

H band(C) NGC 6334 III

42 s

IRN III-2

m

s

22

s

21

s

20

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18

s

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s

16

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Ks band(E) NGC 6334 V
10 ″51 ′ 00″ 45 ″h

17 20 23

s

14

s

13

s

10%

30″

15 ″

IRN I-1

IRN I-3

5%2″ 1%

48′ 00″47′ 30 ″17 20 57 56(B) NGC 6334 II

50′ 30″DECLINATION (J2000)

IRN I-2

3″ 20%IRS III-13

50%

3″ 20%IRN V-3

30 ″
40 ″

15 ″

50 ″

30 ″

IRN V-2

IRN III-1hms

17 20 37 36

s

35

s

s

34

33

s

32

s

31

s

30

s

29

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28

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27

s

IRN V-1hms

17 20 00

s

59

58

s

57

s

56

s

s

55

s

54

RIGHT ASCENSION (J2000)

Figure 1: Polarization vectors are superposed on the intensity
images in the H or Ks band. In the magnifications,
except for IRN IV-6, the vectors are superposed on thepolarized intensity images in the same band. The whitesquare indicates each IRN, and the circle shows eachposition of the illuminating sources with 1σ error. Bluecrosses represent the positions of Spitzer 8.0 μm sources,
green crosses represent the MIR sources for IRN I-2 and3, and purple cross represents the radio source for IRN
IV-6. For IRN I-1, I-5, IV-4, and V-3, since illuminating
sources are identified with NIR sources, the error circles
are not marked.

References[1] Hashimoto, J., et al.: 2008, ApJL, 677, L39.
[2] Loughran, L., et al.: 1986, ApJ, 303, 629.

040

50%

30″

20 ″

2″ 10%-35° 52′ 00″ 45″

We report the detection of eighteen infrared reflection
nebulae (IRNe) in the J, H, & Ks linear polarimetricobservations of the NGC 6334 massive star-formation
complex [1], a total bolometric luminosity ~ 1.9 × 106 L
[2], of which 16 IRNe are new discoveries. Our images
cover ~180 square arcminutes, one of the widest nearinfrared polarization data in star-formation regions so far.
These IRNe are most likely associated with embedded
young OB stars at different evolutionary phases, showing
a variety of sizes, morphologies, and polarization
properties, which can be divided into four categories ofType A to D. We argue the above classification can beplaced along the approximate evolutionary sequence, i.e.,Type A is the youngest and evolve into D through B and C.
We suggest that the difference of the polarized
patterns reflects the evolutionary sequence of IRNe;
the youngest IRNe with well aligned polarization (TypeA) evolve into monopolar/bipolar IRNe with roughly
centrosymmetric polarization (Type B). When IRNe
have concentric polarizations (Type C), the illuminating
sources create HII regions, and then, IRNe become lessdistinct near the central sources with a centrosymmetriccircular pattern at the region of the ionization boundary(Type D). We note, however, that care must be taken toinfer above conclusions from the polarization patternalone. Further high resolution radio observations forkinematical information should be undertaken to verify
our IRN evolutionary hypothesis.
This research was partly supported by Grants-inAid for Scientific Research on Priority Areas from the
Ministry of Education, Culture, Sports, Science andTechnology (MEXT) and No.16340061, 16077204, and16340061.

(Nagoya University)-35 °56 ′ 20 ″NAGATA, Tetsuya, NAGAYAMA, Takahiro
		

KURITA, Mikio

			

20 ″

(NAOJ)		

-35 °58 ′ 10 ″ 0 ″				New Constraint on Radiative Decay of Long-lived Particles
with New 4He Photodisintegration Data and Primordial 6Li Problem
KUSAKABE, Motohiko, KAJINO, Toshitaka
			(NAOJ/University of Tokyo)			

SHIMA, Tatsushi, NAGAI, Yasuki
				(Osaka University)		

Spectroscopic observations of metal-poor halo stars(MPHSs) indicate that abundances of 6Li and 7Li on thestellar surface are independent of the metallicity. The
observed value of 7Li is a factor of 2–4 smaller and thatof 6Li a factor of ~103 higher than predictions by standard
big bang nucleosynthesis (BBN) model. The radiative
decay of long-lived particles in the early universe could
trigger through nonthermal processes production of 6Li
up to about ten times more than observed in MPHSs[1]. The photodisintegration of 4He, which is involvedin the nonthermal nucleosynthesis triggered by theradiative decay, was newly measured with precise
quasimonochromatic laser-Compton photon beam [2].
They show smaller cross sections than deduced fromprevious experiments. We then calculate the decayinduced nonthermal nucleosynthesis with new crosssections fitted to the new experiment (Fig. 1) and derived
a new constraint on the radiative decay (Fig. 2) [3].

(NAOJ)

KII, Toshiteru(Kyoto University)

long-lived particles X, a lifetime τX and ζX =(nX0/n0γ)Eγ0. (nX0/n0γ) which is the number ratio of X to photon
before X-decay and Eγ0 is the photon energy emitted in
the radiative decay. The change in cross sections of 4He
photodisintegration affects the yields of D, 3He and 4He,
which are related to the 4He photodisintegration at low
energy (~30 MeV). The upper limit of allowed region ofζX for these nuclides shifts upward by ~ 300–30 % for τX= 106–1010 s accordingly. The nonthermal yield of 6Li isnot sensitive to the change in cross sections at low energy,
since the 6Li production is mainly through secondary
processes which need energetic photons of Eγ ≥ 50 MeV.
We study a possible uncertainty in the cross sections athigh energies associated with sum rules, and found thatit causes a factor of ≤ 3 change in the constraint on theparameter ζX.

(a)2
Cross Section [mb]

YOSHIDA, Takashi

1
0
(b)

2
1
0

20

25

30
35
40
E [MeV]

45

50

Figure 1: The cross sections of the 4He(γ,p)3H (a) and 4He(γ,n)3He(b) reactions as a function of the photon excitationenergy Eγ. The open circles correspond to the new datafrom experiments with quasi-monochromatic laserCompton photon beams [2]. The solid curves are themost probable excitation functions [3] while the dashdotted curves the previous fitting functions [4]. This
figure is reprinted from [3].

We calculate the non-thermal nucleosynthesis,
and constrain the allowed parameter region for

Figure 2: Contours corresponding to constraints on the primordial
light element abundances for calculations with new crosssections of 4He photodisintegration [3] (solid lines) andwith the previous ones [4] (dotted lines). Overabundance(over) and underabundance (low) regions of D, 3,4He and
7Li are excluded from a comparison with observations.
The region above the thick solid line is excluded by theconsistency requirement of the background radiation
with a black body. The grey region is the allowed region
where 6Li is produced more than observed in MPHSs.
This figure is reprinted from [3].
References[1] Kusakabe, M., et al.: 2006, PRD, 74, 023526.
[2] Shima, T., et al.: 2005, PRC, 72, 044004.
[3] Kusakabe, M., et al.: 2008, PRD, 79, 123513.
[4] Cyburt, R. H., et al.: 2003, PRD, 67, 103521.

I Scientific Highlights

041

Production mechanism of circular polarization in the ORION
BN/KL region: Near-infrared circular polarimetry by SIRPOLFUKUE, Tsubasa*
		

TAMURA, Motohide(Kyoto University)(Graduate University for Advanced Studies/NAOJ)

KANDORI, Ryo, KUSAKABE, Nobuhiko			

(NAOJ)		

BAILEY, Jeremy(University of New South Wales)		

HOUGH, James H., LUCAS, Philip W.
		

WHITTET, Douglas C. B.

HASHIMOTO, Jun

NAGATA, Tetsuya(Graduate University for Advanced Studies)(Kyoto University)

References[1] Fukue, T., et al.: 2009, ApJL, 692, 88.
[2] Fukue, T.: 2009, Polarimetric Study of Star/Planet-Forming
Regions, Ph.D thesis, Kyoto University.
[3] Tamura, M., et al.: 2006, ApJ, 649, 29.

* T. F. was supported by Research Fellowships of the Japan Society for the Promotionof Science for Young Scientists.

I Scientific Highlights

NAKAJIMA, Yasushi(Rensselaer Polytechnic Institute) 		

We reported a deep Ks band circular polarization (CP)image of the Orion BN/KL region, a massive star-forming
region [1, 2]. Further observations of CP from starforming regions were necessary to reveal the production
mechanism of CP.
This study is the first result of circular polarimetry
by a polarimeter SIRPOL mounted on the IRSF 1.4 m
telescope in South Africa. SIRPOL in CP mode saw
first light in the end of 2006, after SIRPOL in linear
polarization (LP) mode saw first light in the end of 2005.
Figure 1 shows the distribution of CP around the most
massive star in this region, IRc2. This distribution has aquadrupolar structure of right- and left-handed CP. Figure
2 shows, for the first time, correlations of CP, linear
polarization (LP), and H–Ks color representing extinction.
These quality correlations were yielded from CP and LP[3] data which were obtained by the same instrument andtelescope.
We theoretically derived a simple relation between
dichroic extinction, color excess, CP, and LP. This
derivation for a young stellar object was yielded byanalysis of the basic equation of vector radiative transfer.
This derived relation agreed with the observed correlation
between the Stokes parameters and the color excess. This
result suggests a major contribution of dichroic extinction
to the production of CP in this region.

042(University of Hertfordshire)(NAOJ)

Figure 1: Image of the degree of CP (%) in the Ks band (2.14 μm)of the BN/KL region. The field of view is 2 .′7 square. A
positive sign for CP indicates that the electric vector isrotated counterclockwise in a fixed plane relative to theobserver. The embedded massive star IRc2, which has
about 25 solar masses, is indicated by arrows.

Figure 2: Pixel-by-pixel correlation using logarithmic color: (a)between Stokes V and Q; (b) between Stokes V and U;(c) between Stokes V and the product of Stokes U and H–Ks color. Stokes Q and U express linear polarization,
and V expresses circular polarization.

New nuclear cosmochronometer for supernova neutrino process
HAYAKAWA, Takehito, SHIZUMA, Toshiyuki
				
				

KAJINO, Toshitaka(JAEA)				

(NAOJ)

OGAWA, Kengo

NAKADA, Hitoshi(RIKEN)(Chiba University)

Long-lived radioactivities are celestial nuclear
cosmochronometers to date when stellar nucleosynthesis
occurred, which have been widely used for estimationof ages of early generations of stars and the Milky way.
Since the number of the long-lived radioactivities islimited, there exist only six cosmochronometers, 40K,
87
Rb, 176Lu, 187Re, 232Th, and 238U, whose half-lives are of
the cosmological time scale 1–100 Gyr. However, there is
no chronometer for neutrino reaction nucleosynthesis insupernovae (ν-process).
We have proposed a 138La (T 1/2=102 Gyr) - 138Ce
136- Ce system as a chronometer to measure the time
elapsed from a single ν-process [1]. These three nuclei
are classfied to the p-nuclei and 138La is considered tobe synthesized dominantly by the ν-process [2]. This
chronometer is applied to samples affected by a single
nucleosynthesis episode, for example, presolar grains inprimitive meteorites. Recent studies of the presolar grains
suggest that such samples are available. If the abundancesof 136,138Ce and 138La in a sample affected strongly by asingle supernova are known, an age T elapsed from thesupernova episode is calculated by,(1)

where N is the observed abundance in the sample, Rppis the initial N(138Ce)/N(136Ce) ratio at the freezeout andb is the branching ratio of the β− decay of 138La. The
Rpp(Ce) ratio can be calculated by an empirical scaling
law between two p-nuclei with the same atomic number,which was found in the solar system abundances. The
detailed mechanism of the empirical scaling law waspresented in our previous paper [3]. The Rpp(Ce) ratio is
estimated to be 1.2.
In addition, we have pointed out that the nuclear
structure of 138La is crucial for the performance of thechronometer and the ν process origin of 138La. The lowest
1+ state has not been established experimentally. If this 1+
excited state exists at energy lower than 72 keV that is theenergy of the first excited state, the 1+ state may be a β
unstable isomer. If so, 138La synthesized by the ν-process
is destroyed via the isomer (see Fig. 1).
Neumann-Cosel et al., commented to us that a
recent nuclear experiment on 138La [4] indicates that theexistence of a low-energy 1+ state in 138La is extremely
unlikely [5]. This is consistent with our shell model
calculation in a relatively large model space [1]. We
conclude that there is no evidence that suggests theexistence of the 1 + isomer in 138La and our proposed
cosmochronometer is robust from this viewpoint [6].
Low spin

Excited statesν processBa(υe,e-)138La
reaction

138

1+(Isomer) T1/2 = min ~ days

5+

La

138

EC decay

Ground stateT1/2 = 102 Gyrβ− decay

0+

0+

Ce

138

0+
138

γ process

Ce

136

Ba

Figure 1: Schematic view of nucleosynthesis of 138La.

References[1] Hayakawa, T., et al.: 2008, PRC, 77, 065802.
[2] Heger, A., et al.: 2005, Phys. Lett. B, 606, 258.
[3] Hayakawa, T., et al.: 2008, ApJ, 685, 1089.
[4] Byelikov, A., et al.: 2007, Phys. Rev. Lett., 98, 082501.
[5] Neumann-Cosel, et al.: 2009, PRC, 79, 059801.
[6] Hayakawa, T., et al.: 2009, PRC, 79, 059802.

I Scientific Highlights

043

Necessary conditions for super-integrability of Hamiltonian systems
YOSHIDA, Haruo(NAOJ)A super-integrable system is defined to be a systemhaving maximum number of first integrals among
integrable Hamiltonian systems. The Kepler problem is asuper-integrable system. In a super-integrable system, allbounded orbits are closed (periodic) like the elliptic orbits
in the Kepler problem (Fig. 1).
A particle motion in a centrifugal potential V = V(r)is always integrable. It is known that among them,potentials in which bounded orbits are always periodic
are limited to only two cases; the Kepler problem with
V(r) = −1/r, and the isotropic harmonic oscillator with
V(r) = r2. This is known as Bertrand’s theorem (1873).
Since periodicity of all bounded orbits is a consequenceof super-integrability of the system, the classicalBertrand’s theorem is considered to have listed up allsuper-integrable centrifugal potentials. In the present
work, a necessary conditions for super-integrability ofHamiltonian systems with homogeneous potential isgiven, which is based on a theorem of Morales-Ramis(2001) on necessary conditions for integrability.
For a potential system q̈ = −∇V(q) with a 2-dim.
homogeneous potential V(q) of degree k, fix a solution
q = c of the simultaneous algebraic equation ∇V(q) = q.
Then compute the quantity

rifugal potentials V = ± rk always gives the value λ = 1.
This value of λ is compatible with super-integrability
only when k = −1 and k = 2. This means that system canbe super-integrable only in the case of Kepler problem(k = −1) and isotropic harmonic oscillator (k = 2). Thus,
it turns out that the classical Bertrand’s theorem is just a
simple example of a wide applicable theorem.
When this new condition is applied to known
sequences of integrable homogeneous polynomial
potentials of arbitrary degree k, it is shown that thesystem cannot be super-integrable whenever k ≥ 3. Thissuggests that there are no more super-integrable systems
besides known ones; harmonic oscillators with rationalfrequency ratios.
q2

q2
1

1
0.5

0.5

0

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-0.5

0

q1

-0.5

-1
-1

-1

-0.5

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-1

-0.5

0

0.5

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q2
1.5

The Morales-Ramis theorem says that if the system underconsideration is integrable, then the λ must be one of thediscrete values (two spectrums)

1
0.5
0

q1

-0.5

-1
-1.5
-1.5

Furthermore, λ can be arbitrary when k = ±2, andadditional spectrums are permitted when k = ±3, ±4, ±5.
Since super-integrable system is integrable, λ mustsatisfy at least the necessary condition for integrability
in order to be super-integrable. Only some subsets of λvalues are compatible with super-integrability. Below is
the main result [1].
• when k ≥ 3 or k ≤ −3 :and additional spectrums when k = ±3, ±4, ±5.
• k = 2 : λ = (n/m)2, a square of non-zero rationals•k=1:λ=0• k = −1 : λ = 1• k = −2 : λ = 1 − (n/m)2
Application of this theorem to homogeneous cent-044

I Scientific Highlights

-1

-0.5

0

0.5

1

1.5

Figure 1: Typical orbits in a super-integrable system (upperleft), in an integrable system (upper-right), and in anonintegrable system (lower-left).

Reference[1] Maciejewski, A., Przybylska, M., Yoshida, H.: 2008, Phys. Lett.
A, 372, 5581.

Trojan Stars near the Galactic Center		

FUJII, Michiko, IWASAWA, Masaki

FUNATO, Yoko

MAKINO, Junichiro(University of Tokyo/NAOJ)		

(University of Tokyo)(University of Tokyo/NAOJ)

Young and massive stars have been found within
one parsec from the Galactic center (GC) [1]. How
these massive stars were brought to the vicinity of thesupermassive black hole (SMBH) has been a mystery.
One possible scenario is the in-situ formation in an
accretion disk. Giant molecular clouds fall into the GC
and form massive gaseous disks around the central
BH. Stars form in the disk if it becomes gravitationallyunstable and results in fragmentation [2]. Anotherpossible scenario is the following. A star cluster formed
at a few tens of pc from the GC, and then spiraled in due
to the dynamical friction [3].
We performed a fully self-consistent N-bodysimulation in which the internal dynamics of the cluster,that of the parent galaxy, and interactions between clusterstars and galaxy stars are correctly handled. We used theBridge code [4] to handle the interaction between theparent galaxy and the star cluster fully self-consistently.
The Bridge scheme is a tree-direct hybrid scheme. In our
simulation, we adopted collisions of stars in a star cluster
and formation of an intermediate-mass black hole (IMBH)
in the cluster.
Figure 1 shows the projected distribution of stars
at the end of the run. This figure looks very similar to
K-band images of the GC [5].
We found that an IMBH is formed in the star clusterand stars escaped from the cluster are captured into a 1:1
mean motion resonance with the IMBH. These “Trojan”
stars are brought close to the SMBH by the IMBH,
which spirals into the GC due to the dynamical friction.
Furthermore, star clusters selectively carry massive stars
close to the GC. Massive stars sink to the center of theirparent star clusters due to the mass segregation. As aresult, massive stars tend to remain in star clusters andare carried to a few parsec from the GC.

Figure 1: Projected distribution of stars at T = 7.26 Myr.

Figure 2: Orbit of a star in a rotational frame, where the IMBH isfixed at (1.0, 0.0).

References[1] Paumard, T., et al.: 2006, ApJ, 643, 1011.
[2] Levin, Y., Beloborodov, M.: 2003, ApJ, 590, L33.
[3] Gerhard, O.: 2001, ApJL, 546, L39.
[4] Fujii, M., et al.: 2007, PASJ, 59, 1095.
[5] Lu, J. R., et al.: 2006, J. Phys. Conf. Ser., 54, 279.

I Scientific Highlights

045Detection of Fluorine in the Halo Planetary Nebula BoBn1:
Evidence For a Binary Progenitor StarOTSUKA, Masaaki(NAOJ/STScI)IZUMIURA, Hideyuki, TAJITSU, Akito			

Currently, over 1,000 objects are regarded asplanetary nebulae (PNe) in the Galaxy, while 14 of them
have been identified as halo members from their locationand kinematics. Halo PNe are interesting objects as they
provide direct insight into the final evolution of old, lowmass halo stars, and they are able to convey important
information for the study of low-mass star evolution andthe early chemical conditions of the Galaxy.
Five objects are known as C- and N-rich ([C,N/O] >~ 0)halo PNe with [Ar/H] <~ −1.7. The progenitors of halo PNe
are thought to be ~0.8 M stars, which is the typical massof a halo star. These C- and N-rich halo PNe, however,show signatures that they have evolved from massive
progenitors. For example, these halo PNe can become
N-rich, but not C-rich, if they have evolved from ~0.8 Msingle stars, according to the current stellar evolution
models. To become C-rich PNe, the third dredgeup (TDU)
must take place in the late AGB phase. However, theTDU takes place in stars with initial masses >~ 1.2–1.5 M.
Also, current stellar evolutionary models predict that the
post-AGB evolution of a star with an initial mass ~0.8 M
proceeds too slowly for a visible PN to be formed.
Resolving these issues would offer important results tobuild realistic stellar evolution and Galactic chemical
evolution models. Chemical abundance analysis should
help solve these issues, by revealing the signatures ofinternal nucleosynthesis and mixing taking place inprogenitor stars. In this paper, we report the results ofchemical abundance analysis of BoBn1 using VLT/UVES
archive spectra [1]. BoBn1 is an extremely metal-poor([Ar/H] ~ −2.1) and C- and N-rich halo PN ([C/O] ~ +1.5,[N/O] ~ +1.0).
Our analysis reveals that the [C/Fe] and [N/Fe]
abundances of BoBn1 are compatible with those ofcarbonenhanced metal-poor (CEMP) stars (Fig. 1). C
and N overabundances of CEMP can be explained bytheoretical binary interaction models. We have detected
two fluorine (F) lines (Fig. 2). The [F/H] of this object
is +1.1 ± 0.1, which makes BoBn1 the most F-enhanced
and metal-poor PN among F-detected PNe and provides
new evidence that F is enhanced by nucleosynthesis
in low mass metal-poor stars (Fig. 2 in [1]). We havefound that the C, N, and F overabundances of BoBn1
are comparable to those of the CEMP HE1305+0132(HE1305, hereafter).
The chemical similarities between BoBn1 and
CEMP stars suggest that this PN shares a similar origin
and evolutionary history. The theoretical model by [2]demonstrated that HE1305 consists of ~2 M (primary)
046

I Scientific Highlights(NAOJ)			

HYUNG, Siek
(Chungbuk National University)and ~0.8 M (secondary) stars, and the enhanced C andF can be explained by binary mass transfer from theprimary star. The C and F abundances of BoBn 1 can be
explained by the ~2 M and ~0.8 M binary model of [2].
Also, the issue of evolutionary time scale can be resolved
if BoBn 1 has evolved from a binary and experienced
mass transfer in the mid-course of its evolution.

Figure 1: Location of BoBn1 on the diagrams of [C/Fe] (left)and [N/Fe] (right) vs. [Fe/H]. For BoBn1, we used Ar
instead of Fe.

Figure 2: Emission line-profiles of [F IV] λ3996.92 Å (left) and[F IV] λ4059.90 Å (right) of BoBn 1.

References[1] Otsuka, M., et al.: 2008, ApJ, 682, L105.
[2] Lugaro, M., et al.: 2008, A&A, 484, L27.

Project Milkyway: Shock-Induced Starburst at a Collision Interface
during the First Encounter of Interacting Galaxies
SAITOH, Takayuki, KOKUBO, Eiichiro, WADA, Keiichi, TOMISAKA, Kohji, MAKINO, Junichiro(NAOJ)
		

OKAMOTO, Takashi

DAISAKA, Hiroshi

YOSHIDA, Naoki(Tsukuba University)(Hitotsubashi University)(Univ. of Tokyo)

The goal 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 computer, GRAPEs, which
accelerates the calculation of gravity, and (ii) a special
code for parallel simulations with GRAPEs, ASURA. The
latest version of ASURA employs a Phantom-GRAPE
library, which is a software emulator of GRAPE tuned
with SIMD operations.
We performed high resolution simulations of galaxygalaxy collisions with ASURA on Cray XT4 at CfCA [1].
In this simulation, we resolved a multiphase nature of theinterstellar medium and adopted a realistic conditions forstar formation [2]. Previous simulations of galaxy-galaxy
merging, on the contrary, did not employ a lower part ofa cooling function (< 104 K) and considered relatively
diffuse regions (nH > 0.1 cm−3) as star forming regions.
These simulations could not resolve neither wide spreadstarbursts nor star cluster formation during the firstencounter.
Our simulations successfully resolved not only awide spread starburst during the first encounter but
also the formation of star clusters. The starburst took
place along a filamentary region, which was induced byhydrodynamical shocks. This starburst rapidly quenchedbecause of the effect of supernovae. After 3×107 yr later,
we found about ten self-bound star clusters along thefilament. Interestingly, these star clusters have no dark
matter. Our results are consistent with the observational
properties of colliding galaxies.

Figure 1: The evolution of gas density during the first encounter.
A large and dense filament appears at the collisioninterface.

Figure 2: The evolution of gas mass as a function of density during
the first encounter. Gas, which was compressed by thelarge scale shock, satisfies star formation conditions anda burst-like star formation took place.

References[1] Saitoh, T. R., et al.:2009, PASJ, 61, 481.
[2] Saitoh, T. R., et al.:2008, PASJ, 60, 667.

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Limit of primordial magnetic field from the matter power spectra
YAMAZAKI, Dai G.
				
			

(NAOJ)		

I Scientific Highlights(University of Tokyo)

KAJINO, Toshitaka

MATHEWS, Grant J.

(NAOJ/University of Tokyo)(Chiba University)

Recent observations show that magnetic fields inclusters of galaxies are 0.1–1.0 μG. Many authors alsosuggest the existence of a primordial magnetic field (PMF)from this fact, and study effects of PMF in the early
univeses, such as the cosmic microwave background(CMB) [1, 2, 3], or the matter density field [4, 5]. In thisarticle we introduce effects of PMF on a matter power
spectra of density fluctuations in early universe, andshow that the observational constraints on cosmologicaldensity fluctuations, as parameterized by σ 8, lead tostrong constraints on the amplitude and spectral index of
the PMF [4, 5].
Pressure and tension of the PMF affect the evolutionof density fluctuations of ionized baryons. Since baryon
and cold dark matter (CDM) interact with each otherthorough gravitational force, the PMF also affects theevolution of density fluctuations of the CDM. Eventually,
the total matter density fluctuations are affected by the
PMF [4, 5].
The alternative normalization parameter σ8 is the rootmean-square matter density fluctuation in a comoving
sphere of radius 8h −1 Mpc. It is given by a weighted
integral of the matter power spectrum. We can study
the physical processes of density field fluctuations on
cosmological scales within the linear regime to determine
σ 8. From this we can obtain strong constraint on the
PMF parameters by numerically calculating σ8 under the
influence of PMF effects.
Since σ8 is affected by other cosmological parameters,
we should consider the degeneracy between the PMF
and other cosmological parameters as mentioned
above. Fortunately, these cosmological parameters areconstrained by recent CMB observations on larger scales(l < 1000), while it was shown in our previous work
[1] that the effect of the PMF mainly affects the CMB
anisotropies on smaller scales (l > 1000). Hence, we
expect that the degeneracy between the PMF parameters
and the other cosmological parameters is small. For thisreason in the present analysis we are justified to fix theother cosmological parameters at their best fit values.
We adopt the constraint that PMF parameters giving
σ8 > 1 are excluded by observations. Figure. 1 shows thata PMF amplitude of Bλ >~ 1 nG is excluded when nB > −0.9.
Furthermore, PMF amplitudes of Bλ >~ 0.1 nG are excluded
when nB > 0.2. The magnetic field strength in galaxy
clusters is ~1 μG. Therefore, if isotropic collapse is the
only process which amplifies the magnetic field strength,
the lower limit to the PMF is ~1 nG at z ~ 0. Hence, we

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ICHIKI, Kiyotomo

can obtain a strong constraint on this PMF evolution
model for a PMF spectral index in the range nB < −0.9.
It is very important to constrain the PMF as precisely
as possible since a magnetic field affects the formationof large scale structure, for example, magnetic pressure
delays the gravitational collapse. Recently, several
observations of the CMB anisotropies and polarizations
for higher multipoles l, e.g. via the Planck, QUIET, andPolarBear, are progressing as planned. If we combine
these future plans and our works, we will be able to limit
parameters of the PMF more accurately and develop
studies of evolution and formation of large scale structurewith the PMF.

Figure 1: Curves of constant values for σ8 in the parameter planeof PMF amplitude Bλ vs. spectral index nB. All curves
are as indicated in the legend box in the figure.

References[1] Yamazaki, D. G., et al.: 2005, ApJ. 625, L1.
[2] Kajino, T., Mathews, G. J.: 2006, ApJ, 646, 719.
[3] Yamazaki, D. G., et al.: 2008, PRD, 77, 043005.
[4] Yamazaki, D. G., et al.: 2006, PRD, 74, 123518.
[5] Yamazaki, D. G., et al.: 2008, PRD, 78, 123001.

Coronal Plasma Motions near Footpoints of Solar Active Region Loops
HARA, Hirohisa, WATANABE, Tetsuya

HARRA, L. K., CULHANE, J. L.

(NAOJ)			

MARISKA, J. T., DOSCHEK, G. A.

(STFC, Rutherford Appleton Lab.)		

Figure 1: Solar active region located at the disk center of the Sun
observed with Hinode EUV imaging spectrometer in theemission line Fe XIV at 27.4 nm. Line intensity I, Doppler
velocity V, and the line width in full width at half
maximum W are shown. Red (blue) shift is indicated inplus (minus) sign for the Dopplergram.

60

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The Sun has a tenuous 106 K corona located above thephotosphere of 6000 K. We try to fully understand how it
is heated to such a hot temperature. We are investigating
the heating mechanism of the solar activeregion coronafrom observations with the Hinode EUV imaging
spectrometer (EIS) [1]. Initial results of this study [2] arepresented here.
Figure 1 shows an observation of a solar active
region, located at the disk center, with EIS in the Fe XIV
emission line at 27.4 nm. The formation temperature of
the emission line is about 1.8 × 106 K. In this figure asingle Gaussian function is applied for fitting the emission
line profile to evaluate the spatial distribution of the line
intensity I, Doppler velocity V, and line width W. The
enhanced line width is wider than the thermal Doppler
width and the enhanced component is called nonthermalvelocity VNT. Subsonic upflow motions of 10 – 20 km s−1and enhanced nonthermal velocities have been found near
the footpoints of the active region loops. When the active
region is observed near the west limb, both Doppler
velocity and nonthermal velocity at the same footpoint
region essentially decrease. There is a strong correlation
between the upflow velocity and the nonthermal velocity(Fig. 2a). Significant deviations from a single Gaussian
profile with a weak emission enhancement are found in
the blue wing of the line profiles for the upflows (Fig. 2band 2c). These suggest that there are unresolved highspeed upflow components. Bluewing enhanced profiles
show fast upflow components of heated plasmas whose
velocities along the loop strucutre are nearly the coronalsound speed. The Hinode EIS has been revealing thecharacteristic motion of heated coronal plasmas.

(NRL)

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YOUNG, P. R.

(University College London, Mullard Space Science Lab.)

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Figure 2: (a) Correlation between Doppler velocity V andnonthermal velocity VNT in Fe XIV at 274 Å. (b) Blueside enhanced line profiles at a footpoint of a coronalloop and (c) residual from a single Gaussian fit. C (L)in black (gray) shows the line profile in the disk-center(limb) observation.

References[1] Culhane, J. L., et al.: 2007, Solar Phys., 243, 19.
[2] Hara, H., et al.: 2008, ApJ, 678, L67.

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Subaru Witnesses the Assembly of Distant Clusters 8 Billion Years Ago
TANAKA, Masayuki				(ESO)				Galaxies are dynamic star systems that have enormous numbers(millions to billions) of stars in wide varieties of colors and shapes.
Some galaxies have blue beautifully knotted spiral arms, whileothers are red diffuse light without arms. As most celestial objects,
galaxies are NOT uniformly distributed throughout the Universe.
They tend to flock together and form a “cosmic web”, which
represents the large-scale structure of the Universe. At intersections
within this webwork, astronomers observe massive concentrationsof galaxies called Galaxy Clusters.
Astronomers have observed that the colors and shapes ofgalaxies change depending on their location. In clusters, where somany galaxies live together, galaxies tend to be red and elliptical.
On the other hand, galaxies living alone are predisposed to beblue and spiral shaped. Astronomers do not yet have a clear idea
why galaxies change their colors and shapes contingent on theirlocation and their surrounding environments. Nonetheless, one
way to explain this phenomenon is to observe galaxies at great
distances that represent periods long ago in the past. Simply stated,
the Universe is like a time machine - as we look deeper into the
Universe, we go further back in time. Using the Subaru Telescope,
astronomers explored answering the question, “How do galaxies
change their colors and shapes over time?”
Recently, an international team of astronomers used Subaru toobserve two huge groups of galaxies, galaxy clusters, in the distant
Universe. One cluster (RDCS0910) was 8 billion light years away
while another (RDCS1252) was 8.5 billion light years distance.
These two clusters are among the most distant clusters known
to date. Galaxies at such a long distance appear very faint, but
Subaru is sensitive enough to collect the dim light from such great
distances.
Galaxy shape, color, and distribution in these structures are
keys to solving the riddles of galactic evolution in the distantreaches of Universe. Using Suprime-Cam, the astronomers
discovered a lot of galaxies within the clusters and found that theclusters are surrounded by small groups of galaxies. Not all thesesmall groups were confirmed to lie at exactly the same distance as
the clusters, but this discovery of prominent large-scale structuresin the distant Universe is a seed to understanding overall galactic
evolution.
Small galaxy groups at this distance (z = 1.2) have previously
not been studied in detail, and, as such, are very interesting objects
for astronomers. The small galaxy groups may get closer to the
nearby larger cluster through gravity and eventually will collidea few hundred million to a few billion years from now. In fact,
collisions and mergers are considered primary factors in galactic
cluster growth. That is, clusters grow by accreting small galaxygroups around them. It should not be surprising if colors andshapes of galaxies in small groups change during these large-scalecollisions.
Looking at the small groups of galaxies in Figures 1, the firstthing noted is the fantastic scale. The large zoom-in boxes are 3
million light years across, indicating that the galaxy groups arehuge. Looking closely at the boxes, many reddish (well, orangeish) galaxies are observed. These galaxies are so far away fromus that it is impossible to spatially resolve their shapes. However,
it is clearly visible that the small groups of galaxies are alreadydominated by red galaxies at least 8 billion years ago.
The fundamental question for this study was “What do theseobservations mean?” As mentioned earlier, galaxies living alone
tend to have blue colors, while galaxies in clusters have red colors.
Galaxies likely change their colors from blue to red during thecourse of relocation and structural growth. Nearby galaxies pulled
together by gravity, form a group of galaxies, and eventually
collide with other groups and form large clusters. At some point inthis structural growth, blue galaxies become red. The team foundin their study that small groups are already dominated by red050

I Scientific Highlights

KODAMA, Tadayuki(NAOJ)
galaxies before they collide with big clusters. Astronomers havelong believed that large clusters are the key environment changing
colors and shapes of galaxies, but the findings at Subaru now
point astronomers at small groups. Galaxies become red in groups
before they get together in large clusters - small groups are the key
environment for these changes in shape and color.
Astronomers know several physical processes that can affectcolors and shapes of galaxies. Among them, collisions and mergers
between galaxies (not between groups) are the ones that work very
efficiently. Because groups have many galaxies in them, galaxies
can attract each other by gravity and eventually collide and merge.
In fact, a computer simulation has shown that a collision between
two blue galaxies leaves a single red galaxy. The Universe 8 billion
years ago shows us that collisions with other galaxies might be thereason why galaxies change their colors and shapes depending on
environment around them. While the astronomers observed just atiny fraction of the Universe, galaxy collisions alone cannot explain
everything and some mysteries remain. Subaru will continue toobserve at great distances and at various wavelengths to get a better
understanding of galactic transformation.
This work is published in two papers [1] and [2].

Figure 1: This image shows a cluster of galaxies 8.5 billion lightyears away in the constellation Hydra. The pseudo-color
picture is made with images taken with Suprime-Camon the Subaru and WFCAM on the United Kingdom
Infrared Telescope (UKIRT). The picture covers 35’ x
28’ of the sky. This area corresponds approximately to 60
million x 45 million light years. The contours show howdensely galaxies flock together 8.5 billion years ago. The
zoom-in views on the corners show small groups and a
big cluster of galaxies. The one on the bottom-right is aknown large cluster. The newly discovered small groups
shown in the other corners surround this massive cluster.
Each panel illustrates 3 million light years across. The
arrows point at cluster member candidates.

References[1] Tanaka, M., et al.: 2008, A&A, 489, 571.
[2] Tanaka, M., et al.: 2007, MNRAS, 377, 1206.

Evidence for a Companion to BM Gem, a Silicate Carbon StarIZUMIURA, Hideyuki, NOGUCHI, Kunio, AOKI, Wako		and other 12 Authors(NAOJ/Graduate University for Advanced Studies)

A small number of carbon stars among those identified
in the optical were found to show silicate dust emission
features in the IRAS Low Resolution Spectra in 1986 [1,2]. Silicate dust forms in oxygen-rich environment where
the oxygen abundance exceeds the carbon abundance,
while it does not in carbon-rich environment where theopposite is the case.
Contemporary stellar evolution theories tell us theoccurrence of repetitive runaways of the He shell burning(“thermal pulses”) in AGB stars, which are descendants
of low- or intermediate-mass stars. In every thermal pulse
synthesized carbon is carried to the outer layer, which
eventually causes an originally oxygen-rich M-type star
evolve into a carbon star.
Two explanations were proposed for the origin ofsilicate carbon stars. One was that silicate carbon stars
were those that had newly evolved from mass-losing,
M-type AGB stars so that we could see remnant silicate
dust around them in the infrared emission features [2].
The other was that silicate carbon stars were binary
systems, each with a mass-losing, M-type AGB starcompanion that was enshrouded in a thick silicate dust
shell that shone in the infrared features [3]. These two
propositions were, however, both rejected by follow-up
studies.
In more than ten years two new pictures were
proposed for the origin of silicate carbon stars. Bothpostulate a low mass, low luminosity companion andinvoke an unknown mechanism that is driven by thebinarry interaction and gives rise to either a circumbinary reservoir [4] or a circum-companion disk [5] thatretains silicate grains captured when the primary wasan M-type mass-losing star. However, there has been noobservational evidence for the presence of a companion
in silicate carbon stars.
We obtained high resolution, high sensitivity ultraviolet to visible spectra of the brightest silicate carbon
star BM Gem with the high dispersion spectrograph HDS
on the Subaru telescope. In the spectra we discovered
ultraviolet continuum emission that is unusual for carbon
stars (Fig. 1). The emission has spectral features typicalfor an ionized gas. Further, we detected the Balmer
series lines, each of which has a P Cygni-type profilethat indicates the presence of a high velocity outflow as
fast as 400 km s−1 and is time variable [6]. No carbon
star has been known that shows such spectral features.
It is difficult to imagine a new radiative mechanism that
produces the observed spectral features in a cool carbon
star. On the other hand, we have found that the continuum
luminosity is plausibly explained if we interpret the

spectral features as emission from an ionized gas that iscaused by the heat from the gravitational potential energy
release during the accretion of a part of the primary’s
mass-loss flow by the companion. Furthermore, we havenoticed that almost identical spectral features have been
observed in Mira B, the companion to the M-type AGB
star Mira A (o Cet). With these observational results wehave conluded the presence of a low-luminosity, lowmass companion to the silicate carbon star BM Gem.

Figure 1: Ultraviolet to visible spectra of BM Gem observed withHDS on Subaru telescope (top and middle, different
dates). A spectrum of Y CVn, which looks similar to
BM Gem in the visible region, taken with the samesetting for comparison (bottom). Small vertical ticks inthe bottom show the positions of artifacts that mimic
emission lines.

References[1] Little-Marenin, I. R.: 1986, ApJL, 307, L15.
[2] Willems, F. J., de Jong, T.: 1986, ApJL, 309, L39.
[3] Benson, P. J., Little-Marenin, I. R.: 1987, ApJL, 316, L37.
[4] Jura, M., Kahane, C.: 1999, ApJ, 521, 302.
[5] Yamamura, I., et al.: 2000, A&A, 363, 629.
[6] Izumiura, H., et al.: 2008, ApJ, 682, 499.

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Discovery of strange filamentary structures (“fireballs”)
around a merger galaxy in the Coma cluster of galaxies
YOSHIDA, Michitoshi, YAGI, Masafumi, KOMIYAMA, Yutaka, FURUSAWA, Hisanori
KASHIKAWA, Nobunari, HATTORI, Takashi(NAOJ)KOYAMA, Yusei, OKAMURA, Sadanori			(University of Tokyo)		

Clusters of galaxies are ideal experimentallaboratories for studying environmental effects on
evolution of galaxies. Several environmental effects
which explain the evolution of cluster galaxies havebeen proposed so far and many observational studies
have been made to identify the dominant environmental
processes in clusters. However, it is still not clear whatkinds of physical processes are dominant for rapid galaxy
evolution in clusters.
Recently, two peculiar galaxies were found near thecentral regions of two rich clusters at z ≈ 0.2 [1]. Thesegalaxies have disturbed morphology and are associatedwith many small blue blobs extending toward theonesides of galaxies. It is suggested that these phenomena
may be snapshots of transformation of spiral galaxies to
S0 galaxies and may give insights to the origin of faintend population of clusters [1].
Here we report a discovery of a strange complexof narrow blue filaments and knots (Figure 1; its
morphology resembles a complex of “fireballs (large
meteors)”) which extends up to 80 kpc to the south from a
disturbed E+A galaxy, RB199, in the Coma cluster using
Subaru Telescope [2]. The morphology of the structure
is very similar to that of the phenomena found in the twoz ≈ 0.2 clusters. This structure may be a nearby counterpart of the transition galaxies found in the clusters atz ≈ 0.2.
The narrow blue filaments extend in straight shapes
toward the south from the galaxy and several bright blue
knots are located at the south ends of the blue filaments(Figure 1). The RC band absolute magnitudes, half lightradii and estimated masses of the bright knots are ~ −12– −13 mag, ~100 – 200 pc and ~106–7 M, respectively.
Strong Hα emission is associated with the bright knots.
Long narrow Hα emitting filaments are connected at
the south edge of the knots. The average color of the“fireballs” is B − RC ≈ 0.5, which is bluer than RB199 (B− R = 0.99), suggesting that most of the stars of which
the “fireballs” is composed were formed within several
times 10 8 yr. There is no Hα emission in the narrow
blue filaments, whereas strong Hα and UV emission are
emitted at the bright knots. These characteristics indicatethat star formation has been recently ceased in the blue
filaments and is now in progress in the bright knots. The
gas stripped by some mechanism from the disk of RB199

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YAMANOI, Hitomi(Graduate University for Advanced Studies/NAOJ)

may be traveling in the intergalactic space, forming stars
and leaving the formed stars along its trajectories. Most
plausible mechanism of forming the “fireballs” is rampressure stripping by high speed collision between thegalaxy and the hot intra-cluster medium. The “fireballs”
may be a snapshot of a formation process of diffuse intracluster population or halo star population of a cluster
galaxy.

Figure 1: False color (B band: blue, RC band: green, Hα NB: red)
image of area around RB199. North is right and east
is top. RB199 is located at the right side of the image.
Several blue filaments extend from RB199 to the centerof this image and bright blue knots are located at the tipsof the filaments. Red Hα emission is associated with thebright knots.

References[1] Cortese, L., et al.: 2007, MNRAS, 376, 157.
[2] Yoshida, M., et al.: 2008, ApJ, 688, 918.

Lunar Global Topographic Map by the KAGUYA Laser Altimetry
ARAKI, Hiroshi, TAZAWA, Seiichi, NODA, Hirotomo, ISHIHARA, Yoshiaki, GOOSSENS, Sander
SASAKI, Sho, KAWANO, Nobuyuki(NAOJ)KAMIYA, Izumi

OHTAKE, Hisashi(GSI) 			OBERST, J.

(JAXA)		

SHUM, C. K.

(DLR) 		The main orbiter of Japanese Lunar probe KAGUYA(SELENE) which was launched on 14 September, 2007
(UT; the same hereafter) has successfully closed its
observation by the controlled impact onto the Lunar
surface on 10 June, 2009. We have constructed a global
and precise topographic map of the Moon for the
first time using the KAGUYA laser altimeter (LALT)
topographic data (Fig. 1) [1]. LALT has obtained about
10 million range data during the nominal observation
period from 30 December, 2007 to 27 October, 2008. The
along and cross track resolution of the geo-located points
in the equatorial region is 1.5 km and less than 10 km,
respectively. The mean number density of the geo-locatedpoints is about 1/(200 m)2 in both polar regions.
It has been derived that Lunar mean radius is1737.15 km and the offset between the center of mass(COM) and the center of figure (COF) is 1.93 km
by the spherical harmonic analysis of 6.67 million
lunar topographic data obtained by 31 March, 2008.
The maximum topographic difference is found to be
19.81 km, where height reference is a sphere whose
radius is 1737.4 km centered on the COM. The spherical(OSU)

harmonic analysis has also revealed that the amplitude of
the topography for the horizontal scale less than 180 km
shows 2 or 3 times larger spectrum than the previous
estimation. This may suggest that the small scale
topography is not compensated and more rigid than otherterrestrial planets [1].
In the Lunar polar regions, volatile materials such as
water ice are expected to be buried within the regolith in
the deep crater floor where the sun lit rate is zero due tothe low solar elevation; while the high place where thesun lit rate is high such as on the crater rim is promising
candidate site for the Lunar base. We have calculated
and mapped the solar illumination condition on the bothpolar regions for more than 85 degrees based on the
LALT data. The results are as follows; (i) the sun lit rate
is 89% and 86% at most for the north and south region
respectively, (ii) the permanent shadow area for morethan 87.5 degrees is 844 km2 and 2751 km2 for the Lunar
north and south polar region, respectively [2].
References[1] Araki, H., et al.: 2009, Science, 323, 897.
[2] Noda, H., et al.: 2008, GRL, 35, L2420.

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is 1737.4 km and origin is set to the center of mass.

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Precise wavefront correction with an unbalanced nulling interferometerfor exo-planet imaging coronagraphs
NISHIKAWA, Jun, MURAKAMI, Naoshi(NAOJ)

ABE, Lyu			(NAOJ/Univ. Nice)KOTANI, Takayuki(Max-PLanc Institute für Radioastronomie/Paris Observatory)

In 1995, an exoplanet was discovered by a Doppler
method for the first time. Since then, about 350 exoplanet
were detected almost by indirect methods while a few
very bright exoplanets were recently detected by direct
coronagraphic imaging in 2009. Spectroscopic analysisof exoplanet light is one of the most important theme inmodern astronomy.
The direct imaging and the spectroscopy of Earthlike exoplanets is disturbed by bright diffracted light andspeckle noise of a central star, and the required dynamical
range is 109 ~ 1010 on small angular separation of a few
λ/D. Here an input wavefront quality of approximately
ten thousandths of a wavelength rms is required to reduce
the speckle noise. We studied pre-optics with nullinginterferometer [1], and complex compensation after
interference [2], and, as a combied extension of them,developed a method presented in the following.
We propose a novel method based on a 4-stage
configuration of a coronagraph system (Figure 1) [3,4, 5], in which a very important role is achieved by amiddle-stage optics setup (UNI-PAC) that behaves partly
as a low-efficiency coronagraph, and partly as a highsensitivity wavefront aberration compensator (phase andamplitude).
A first adaptive optics (AO) system compensate forthe wavefront aberrations of mainly the primary mirrorof a telescope with a quality of λ/1000 rms. Second, an(intensity-) unbalanced nulling interferometer (UNI)
performs a rejection of part of the wavefront electricfield. Then, the input aberrations of the recombined
output wavefront are magnified to λ/100 rms. Becauseof the unbalanced recombination scheme, aberrations
can be free of phase singular (zero intensity) points andcan therefore be compensated by a downstream phaseand amplitude correction (PAC) AO system, using two
deformable mirrors with a quality of λ/1000 rms. In
the image plane, the central star’s peak intensity andthe noise level of its speckled halo are reduced by the
UNI-PAC combination: the output-corrected wavefront
aberrations from the UNI-PAC can be interpreted as an
improved compensation of the initial incident wavefront
aberrations, implying that the wavefront quality was“virtually” improved to λ/10000 rms beyond the AO
system capabilities.
Finally the residual star light is reduced by acoronagraph and the speckle level is kept as low as the054

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planet intensity even with a wavefront quality of λ/1000
rms. A significant advantage of using the UNI-PAC is
the relaxation of the specification for the entire opticsof the coronagraph system to λ/1000 rms surface error
quality, which is an important step towards developing aterrestrial-planet detection system in a cost-effective way.

Figure 1: Schematic of the 4-stage coronagraph optics including
the UNI-PAC method [3, 4, 5]. Wavefront corrections
are made twice at the first AO and the PAC AO system,and star light suppressions are also made twice at the
UNI and the coronagraph.

References[1] Nishikawa, J., et al.: 2005, A&A, 435, 379.
[2] Abe, L., et al.: 2006, A&A, 451, 363.
[3] Nishikawa, J., et al.: 2006, SPIE, 6265, 62653Q.
[4] Nishikawa, J., et al.: 2008, SPIE, 7010, 70102A.
[5] Nishikawa, J., et al.: 2008, A&A, 489, 1389.

TCP-AIC: Tandem common-path achromatic interfero-coronagraph
TAVROV, Alexander, NISHIKAWA, Jun, TAMURA, Motohide, ABE, Lyu(NAOJ)YOKOCHI, Kaito, KUROKAWA, Takashi

TAKEDA, Mitsuo(Tokyo University of Agricultural and Technology)(The University of Electro-Communications)

New scheme for an achromatic interfero-coronagraph,incorporating two common-path interferometers intandem (Figure 1), is proposed to attain a deeper nullingfor an extended incoherent stellar disk. The predictedperformance improvement, by using TCP-AIC has thepossibility to reach a 10 10 achromatic coronagraphic
contrast for an almost 10 −2 λ/D effective source size
(stellar disk size).
Direct imaging of extra-solar Earth-like planets, using
stellar coronagraphs and nulling interferometers, requires
the realization of star-to-planet intensity contrasts,
as high as ~10 10 in the visible wavelength range and~106 in the mid-IR range. For the detection of a faintplanet signal, such optical systems require an extremely
accurate wavefront control and a highly stable system
configuration. Currently an achromatic � shifter with
sufficient inner working angle remains a key device fornulling interferometers and an AIC coronagraph concepts.
The AIC realizes coronagraphic nulling by shifting
the geometric phase in a common-path interferometer.
This common-path configuration makes the detection
system highly immune to environmental disturbances.
The coronagraphic image is a centro-symmetrical pair ofcompanion images.
For a monochromatic laser point source of 633 nm,
single CPAIC has demonstrated light suppression witha stable coronagraphic contrast of 106 at a 1 λ/D off-axis
distance [1].
For a star-disk diameter of 10−2 λ/D and an off-axis
planet separation distance of 1 λ/D, nulling contrast of
only 104 can be achieved with an AIC, which condition
corresponds to a Sun-Earth system at 5 pc distanceusing a 1-meter-class diameter telescope operated at a
1 µm center wavelength. The resulting non-null residual
starlight remains at 2 orders greater than the target planet
contrast of 106, which is required for the mid infrared
range. Residual visible light remains 6 orders greater tothe 1010 contrast required.
To cope with the problem of insufficient spatial
coherence caused by an extended source, we proposed
the TCP-AIC which use two interferometers cascadedin tandem, effectively making four-beam interference(Figure 2). The TCP-AIC was started experimentally torealize a 1010 coronagraphic contrast [2].

Figure 1: Schematic of the tandem common-path achromaticinterferometer coronagraph.

1010Nullingc ontrast

		

10
10
10
10
10

0

-2

-4

-6

-8

-10

-12

10

-3

10

-2

-1

10
Source size, λ/D.

100Figure 2: Nulling contrast of the single and tandem CPAIC.

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II Publications, Presentations
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Abbott, B., et al. including Kawamura, S., Sakata, S.: 2008, First
joint search for gravitational-wave bursts in LIGO and GEO
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Abbott, B., et al. including Kawamura, S., Sakata, S.: 2008,
Search for Gravitational-Wave Bursts from Soft Gamma
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Abbott, B., et al. including Kawamura, S., Sakata, S.: 2008, Searchof S3 LIGO data for gravitational wave signals from spinningblack hole and neutron star binary inspirals, PhRvD, 78, 42002.
Abbott, B., et al. including Kawamura, S., Sakata, S.: 2008,
Implications for the Origin of GRB 070201 from LIGO
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Abbott, B., et al. including Kawamura, S., Sakata, S.: 2008,
Beating the Spin-Down Limit on Gravitational Wave Emission
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Abbott, B., et al. including Kawamura, S., Sakata, S.: 2008,
Astrophysically triggered searches for gravitational waves:status and prospects, CQGra, 25, 114051.
Abbott, B., et al. including Kawamura, S., Sakata, S.: 2009, AllSky LIGO Search for Periodic Gravitational Waves in the Early
Fifth-Science-Run Data, PRL, 102, 111102.
Abbott, B., et al. including Kawamura, S., Sakata, S.: 2009,
Einstein@Home search for periodic gravitational waves in
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Akutsu, T., et al. including Kawamura, S., Arai, K., Tatsumi,D., Fukushima, M., Yamazaki, T., Fujimoto, M.-K.: 2008,
Development of a detector pair for very high frequency
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Agatsuma, K., et al. including Takahashi, R., Arai, K., Tatsumi,D., Fukushima, M., Yamazaki, T., Fujimoto, M.-K.: 2008,
Control system for the seismic attenuation system (SAS) in
TAMA300, JPhCS, 122, 12013.
Akutsu, T., et al. including Kawamura, S., Arai, K., Yamamoto,K., Tatsumi, D., Sugiyama, N., Fukushima, M., Yamazaki,T., Fujimoto, M.-K.: 2008, Search for a Stochastic Backgroundof 100-MHz Gravitational Waves with Laser Interferometers,
PhRvL, 101, 101101.
Akutsu, T., et al. including Tatsumi, D.: 2008, Search forcontinuous gravitational waves from PSR J0835-4510 using
CLIO data, CQGra, 25, 184013.
Allende Prieto, C., et al. including Aoki, W.: 2008, The Segue
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Ando, M., et al. including Kawamura, S., Seto, N., Arai, K.,
Fujimoto, M.-K., Fukushima, M., Ishizaki, H., Kotake, K.,
Ohishi, N., Sakata, S., Takahashi, R., Yamazaki, T.: 2008,056

II Publications, Presentations

DECIGO pathfinder, JPhCS, 120, 32005.
Antolin, P., Shibata, K., Kudoh, T., Shiota, D., Brooks, D.: 2008,
Predicting Observational Signatures of Coronal Heating by
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Aoki, W., Beers, T. C., Sivarani, T., Marsteller, B., Lee, Y. S.,
Honda, S., Norris, J. E., Ryan, S. G., Carollo, D.: 2008, CarbonEnhanced Metal-Poor Stars. III. Main-Sequence Turnoff Stars
from the SDSS SEGUE Sample, ApJ, 678, 1351-1371.
Aoki, W., Honda, S.: 2008, Enrichment of Lead (Pb) in the
Galactic Halo, PASJ, 60, L7-L11.
Arai, K., on behalf of the TAMA collaboration: 2008, Recent
progress of TAMA300, JPhCS, 120, 32010.
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S., Sasaki,S., Kawano, N., Kamiya, I., Otake, H., Oberst, J., Shum, C. K.:
2009, Lunar Global Shape and Polar Topography Derived from
Kaguya-LALT Laser Altimetry, Science, 323, 897-900.
Araki, H., Tazawa, S., Noda, H., Tsubokawa, T., Kawano, N.,
Sasaki, S.: 2008, Observation of the lunar topography by
the laser altimeter LALT on board Japanese lunar explorer
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Arase, Y., Takahashi, R., Arai, K., Tatsumi, D., Fukushima, M.,
Yamazaki, T., Fujimoto, M.-K., Agatsuma, K., Nakagawa, N.:
2008, Damping system for torsion modes of mirror isolation
filters in TAMA300, JPhCS, 122, 12027.
Arentoft, A., et al. including Kambe, E., Ando, H., Izumiura, H.:
2008, A Multisite Campaign to Measure Solar-like Oscillationsin Procyon. I. Observations, Data Reduction, and Slow
Variations, ApJ, 687, 1180-1190.
Asada, K., Inoue, M., Nakamura, M., Kameno, S., Nagai, H.:
2008, Multifrequency Polarimetry of the NRAO 140 Jet:
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Asai, A., Hara, H., Watanabe, T., Imada, S., Sakao, T., Narukage,N., Culhane, J. L., Doschek, G. A.: 2008, Strongly Blueshifted
Phenomena Observed with Hinode EIS in the 2006 December
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Asai, A., Shibata, K., Ishii, T. T., Oka, M., Kataoka, R., Fujiki, K.,
Gopalswamy, N.: 2009, Evolution of the anemone AR NOAA
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Aso, Y., et al. including Kotake, K.: 2008, Search method forcoincident events from LIGO and IceCube detectors, CQGra,
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Aspin, C., et al. including Pyo, T.-S.: 2009, Near-Ir Spectroscopyof Young Stars in the Braid Nebula Star Formation Region in
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Baek, C. H., Kudoh, T., Tomisaka, K.: 2008, How was theMushroom-shaped GW 123.4-1.5 Formed in the Galactic Disk?,
ApJ, 682, 434-444.
Baggio, L., et al. including Kawamura, S., Sakata, S.: 2008, A
joint search for gravitational wave bursts with AURIGA and
LIGO, CQGra, 25, 95004.

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Barbary, K., et al. including Morokuma, T.: 2009, Discovery of
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Bekki, K., Tsujimoto, T., Chiba, M.: 2009, Role of Galactic Gaseous
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Bekki, K., Yahagi, H., Nagashima, M., Forbes, D. A.: 2008,
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Bernard, J. P., et al. including Mizuno, N.: 2008, Spitzer Survey of
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Blanc, M., et al. including Sasaki, S.: 2009, LAPLACE: A mission
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Bowler, B. P., Waller, W. H., Megeath, S. T., Patten, B. M.,
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Brown, C. M., Feldman, U., Seely, J. F., Korendyke, C. M., Hara,H.: 2008, Wavelengths and Intensities of Spectral Lines in
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Buat, V., Boissier, S., Burgarella, D., Takeuchi, T. T., Le Floc'h, E.,
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Burningham, B., et al. including Tamura, M., Ishii, M., Kuzuhara,
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Carter, D., et al. including Komiyama, Y.: 2008, The Hubble Space
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Chae, J., Litvinenko, Yu. E., Sakurai, T.: 2008, Determinationof Magnetic Diffusivity from High-Resolution Solar Magnetograms, ApJ, 683, 1153-1159.
Chae, J. C., Sakurai, T.: 2008, A Test of Three Optical Flow
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Chae, J. C., Ahn, K. S., Lim, Y. K., Choe, G. S., Sakurai, T.: 2008,
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Chaplin, W. J., et al. including Sekii, T.: 2008, AsteroFLAG – fromthe Sun to the stars, JPhCS, 118, 12048.
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Chifor, C., Isobe, H., Mason, H. E., Hannah, I. G., Young, P. R.,
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Chifor, C., Young, P. R., Isobe, H., Mason, H. E., Tripathi, D.,
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Choi, M., Hamaguchi, K., Lee, J.-E., Tatematsu, K.: 2008, Centimeter
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Choi, M., Tatematsu, K., Hamaguchi, K., Lee, J.-E.: 2009,
Centimeter Polarimetry of the R Coronae Australis Region, ApJ,
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Choi, Y. K., et al. including Iwadate, K., Jike, T., Kameya, O.,
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Kuji, S., Manabe, S., Matsumoto, N., Miyaji, T., Oh, C. S.,
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Clements, D. L., et al. including Furusawa, H., Sekiguchi,
K.: 2008, The SCUBA Half-Degree Extragalactic Survey(SHADES) – VIII. The nature of faint submillimetre galaxies in
SHADES, SWIRE and SXDF surveys, MNRAS, 387, 247-267.
Cockell, C. S., et al. including Tamura, M.: 2009, Darwin-A
Mission to Detect and Search for Life on Extrasolar Planets,
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Curdt, W., Wilhelm, K., Feng, L., Kamio, S.: 2008, Multi-spacecraft
observations of polar coronal plumes , A&A, 481, L61.
Danilovic, S., Gandorfer, A., Lagg, A., Schüssler, M., Solanki, S.
K., Vögler, A., Katsukawa, Y., Tsuneta, S.: 2008, The intensity
contrast of solar granulation: comparing Hinode SP results with
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Dawson, J. R., Kawamura, A., Mizuno, N., Onishi, T., Fukui, Y.:
2008, Catalogue of 12CO(J = 1–0) and 13CO(J = 1–0) Molecular
Clouds in the Carina Flare Supershell, PASJ, 60, 1297-1315.
Dawson, J. R., Mizuno, N., Onishi, T., McClure-Griffiths, N. M.,
Fukui, Y.: 2008, The 'Carina Flare' supershell: probing the atomic
and molecular ISM in a Galactic chimney, MNRAS, 387, 31-44.
de Wijn, A. G., Lites, B. W., Berger, T. E., Frank, Z. A., Tarbell,
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de Wit, W. J., et al. including Fujiyoshi, T., Yamashita, T.: 2009,
Resolved 24.5 micron emission from massive young stellar
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de Wit, W. J., et al. including Fujiyoshi, T., Yamashita, T.: 2008,
A Red Supergiant Nebula at 25 μm: Arcsecond-Scale Mass-Loss
Asymmetries of μ Cephei, ApJ, 685, L75-L78.
Deguchi, S., Koike, K.: 2008, Clustering of Mater-Wave Luminous
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Del Moro, A., Watson, M. G., Mateos, S., Akiyama, M., Hashimoto,Y., Tamura, N., Ohta, K., Carrera, F. J., Stewart, G.: 2009, An
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Doschek, G. A., Warren, H. P., Mariska, J. T., Muglach, K., Culhane,
J. L., Hara, H., Watanabe, T.: 2008, Flows and Nonthermal

II Publications, Presentations

057

Velocities in Solar Active Regions Observed with the EUV
Imaging Spectrometer on Hinode: A Tracer of Active Region
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Dudley, C. C., Imanishi, M., Maloney, P. R.: 2008, Ice Emission
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Dye, S., et al. including Takata, T.: 2008, The SCUBA HAlf Degree
Extragalactic Survey (SHADES) – VII. Optical/IR photometry
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1107-1130.
Ebisuzaki, T., et al. including Mizumoto, Y., Watanabe, J.: 2008,
The JEM-EUSO Project: Observing Extremely High Energy
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Enomoto, R., et al. including Mizumoto, Y.: 2008, CANGAROOIII Search for Gamma Rays from Kepler's Supernova Remnant,
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Famiano, M., Boyd, R., Kajino T., Otsuki, K., Terasawa, M.,
Mathews, G. J.: 2008, Effects of β-decays of excited-state nuclei
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Frebel, A., Collet, R., Eriksson, K., Christlieb, N., Aoki, W.: 2008,
HE 1327-2326, an Unevolved Star with [Fe/H]<−5.0. II. New
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Fujii, M., Iwasawa, M., Funato, Y., Makino, J.: 2008, Evolutionof Star Clusters near the Galactic Center: Fully Self-consistentN-body Simulations, ApJ, 686, 1082-1093.
Fujiwara, M., Nagata, H., Matsuo, H., Sasaki, M.: 2008, Optical
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Fukui, Y., et al. including Mizuno, N., Ogawa, H.: 2008, The Second
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Fukushima, T.: 2008, An Orbital Element Formulation without
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Fukushima, T.: 2008, Simple, Regular, and Efficient Numerical
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Fukushima, T.: 2008, Gaussian Element Formulation of ShortAxis-Mode Rotation of a Rigid Body, AJ, 136, 649-653.
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Furusawa, H., et al. including Kosugi, G., Takata, T., Sekiguchi, K.,
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The Subaru/XMM-Newton Deep Survey (SXDS). II. Optical
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058

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Furuya, R. S., Kitamura, Y., Shinnaga, H.: 2008, Low-Mass StarForming Cores in the GF9 Filament, PASJ, 60, 421-428.
Furuya, R. S., Kitamura, Y., Shinnaga, H.: 2009, Spectroscopic
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Gaskell, R. W., et al. including Ishiguro, M.: 2008, Characterizing
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Goto, M., Usuda, T., Nagata, T., Geballe, T. R., McCall, B. J.,
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Goto, T., Kawai, A., Shimono, A., Sugai, H., Yagi, M., Hattori,
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Goto, T., Yagi, M., Yamauchi, C.: 2008, Spatialy-Resolved
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Grechnev, V. V., Uralov, A. M., Slemzin, V. A., Chertok, I. M.,
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SoPh, 253, 263-290.
Greiner, J., et al. including Aoki, K., Pyo, T.-S., Terada, H.: 2009,
GRB 080913 at Redshift 6.7, ApJ, 693, 1610-1620.
Groen, D., Portegies Zwart, S., McMillan, S., Makino, J.: 2008,
Distributed N-body simulation on the grid using dedicatedhardware, NewA, 13, 348-358.
Gusev, A., Petrova, N.: 2008, Spin-orbit evolution, geophysics andSelenodesy of the Moon, AdSpR, 42, 289-293.
Guyon, O., Matsuo, T., Angel, R. J.: 2008, Coronagraphic Low
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Guyon, O., Blain, C., Takami, H., Hayano, Y., Hattori, M.,
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Hachisuka, K., Brunthaler, A., Menten, K. M., Reid, M. J.,
Hagiwara, Y., Mochizuki, N.: 2009, The Distance to a StarForming Region in the Outer Arm of the Galaxy, ApJ, 696, 1981.
Hajima, R., Hayakawa, T., Kikuzawa, N., Minehara, E.: 2008,
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Hamaguchi, K., Choi, M., Corcoran, M. F., Choi, C.-S., Tatematsu,
K., Petre, R.: 2008, Resolving a Class I Protostar Binary Systemwith Chandra, ApJ, 687, 425-432.
Hamana, T., Miyazaki, S.: 2008, Note on Artificial Deformationin Object Shapes Due to Pixelization, PASJ, 60, 1363-1370.
Hanada, H., et al. including Kawano, N., Asari, K., Ishikawa, T.,
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AdSpR, 42, 341-346.
Hanaoka, Y.: 2009, Spectropolarimetry with the Hida DomelessSolar Telescope, PASJ, 61, 357-365.
Hara, H., Watanabe, T., Harra, L. K., Culhane, J. L., Young, P. R.,
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Hara, H., Watanabe, T., Matsuzaki, K., Harra, L. K., Culhane,
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December 17 Long Duration Flare Observed with the Hinode
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Harra, L., Williams, D., Wallace, A., Magara, T., Hara, H.,
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Hasegawa, S., Müller, T. G., Kawakami, K., Kasuga, T., Wada, T.,
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Albedo, Size, and Surface Characteristics of Hayabusa-2
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Hashimoto, J., Tamura, M., Kandori, R., Kusakabe, N.,
Nakajima, Y., Kurita, M., Nagata, T., Nagayama, T., Hough,J., Chrysostomou, A.: 2008, Wide-Field Infrared Imaging
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Hashimoto, T., et al. including Kajino T.: 2009, A new mea-surementof the astrophysical 8Li(d,t)7Li reaction, PhLB, 674, 276-280.
Hayakawa, T., Iwamoto, N., Kajino, T., Shizuma, T., Umeda,
H., Nomoto, K.: 2008, Empirical Abundance Scaling Laws
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Hayakawa, T., Shizuma, T., Kajino, T., Ogawa, K., Nakada, H.:
2008, 138La-138Ce-136Ce nuclear cosmochronometer of supernova
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Hayakawa, T., Shizuma, T., Kajino, T., Ogawa, K., Nakada, H.:
2009, Reply to "Comment on 138La-138Ce-136Ce nuclear cosmochronometer of supernova neutrino process", PhRvC, 79, 59802.
Hayakawa, T., et al. including Kajino, T.: 2008, Half-life of164
Ho isomer populated by (g,n) reaction from Laser Compton
scattering g-rays at NewSUBARU, PhRvC, 77, 68801.
Hayama, K., Desai, S., Kotake, K., Mohanty, S. D., Rakhmanov,
M., Summerscales, T., Yoshida, S.: 2008, Determinationof the angular momentum distribution of supernovae fromgravitational wave observations, CQGra, 25, 184022.
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064

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Noda, H., Araki, H., Goossens, S., Ishihara, Y., Matsumoto,K., Tazawa, S., Kawano, N., Sasaki, S.: 2008, Illumination
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Shimizu, M., Nishida, K., Takasaki, H., Shiota, D., Magara, T.,
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Image Stabilization System for Hinode (Solar-B) Solar Optical
Telescope, SoPh, 249, 221.
Shimizu, T., Lites, B. W., Katsukawa, Y., Ichimoto, K., Suematsu,
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Shimonishi, T., Onaka, T., Kato, D., Sakon, I., Ita, Y., Kawamura
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Shin, J., Sakurai, T.: 2009, Optical Characteristics of the SoftX-Ray Telescope Aboard Yohkoh. I. Interpretation of theUndersampled Point Spread Function, SoPh, 254, 357-384.
Shinnaga, H., Phillips, T. G., Furuya, R. S., Cesaroni, R.: 2008,
Submillimeter Observations of the Isolated Massive Dense
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Shintani, M., et al. including Hirota, T., Kijima, M., Kobayashi,
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2008, Statistical Properties of Stellar H2O Masers – Resultsof Three-Year Single-Dish Observations with the VERA Iriki
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Shirai, K., Okada, T., Yamamoto, Y., Arai, T., Ogawa, K., Shiraishi,
H., Iwasaki, M., Arakawa, M., Grande, M., Kato, M.: 2008,
Instrumentation and performance evaluation of the XRS on
SELENE orbiter, EP&S, 60, 277-281.
Shirasaki, Y., et al. including Tanaka, M., Kawanomoto, S.,
Honda, S., Ohishi, M., Mizumoto, Y., Masunaga, Y.: 2008,
Data processing for ‘SUBARU’ telescope using GRID, Fusion
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Shizuma, T., Hayakawa, T., Ohgaki, H., Toyokawa, H., Komatsubara,T., Kikuzawa, N., Tamii, A., Nakada, H.: 2008, Fine structure of
the magnetic-dipole-strength distribution in 208Pb, PhRC, 78,
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Shizuma, T., Ishii T., Makii, H., Hayakawa, T., Matsuda, M.: 2009,
A 3-quasiparticle isomer in neutron-rich 183Ta, EPJA, 39, 263-266.
Shizuma, T., Ishii, T., Makii, H., Hayakawa, T., Matsuda, M.,
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Stonkute, R., Vansevicius, V., Arimoto, N., Hasegawa, T., Narbutis,D., Tamura, N., Jablonka, P., Ohta, K., Yamada, Y.: 2008, An
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Suematsu, Y., et al. including Tsuneta, S., Katsukawa, Y., Nakagiri,M., Noguchi, M., Tamura, T., Kato, Y., Hara, H., Kubo, M.:
2008, The Solar Optical Telescope of Solar-B (Hinode): The
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Sugiyama, K., Odaka, M., Nakajima, K., Hayashi, Y.-Y.: 2008,
Development of a Cloud Convection Model to Investigate theJupiter's Atmosphere, Nagare Multimedia, http://www.nagare.
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Sugiyama, K., Fujisawa, K., Doi, A., Honma, M., Isono, Y.,
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Suwa, Y., Takiwaki, T., Kotake, K., Sato, K.: 2009, Impact ofRotation on Neutrino Emission and Relic Neutrino Backgroundfrom Population III Stars, ApJ, 690, 913-922.
Suzuki, R., Tokoku, C., Ichikawa, T., Uchimoto, Y. K., Konishi, M.,
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Suzuki, T., Kaneda, H., Matsuura, S., Shirahata, M., Nakagawa,T., Doi, Y., Onaka, T., Hibi, Y., Kawada, M., Shibai H.: 2008,
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Takahashi, R., et al. including Arai, K., Tatsumi, D., Fukushima,M., Yamazaki, T., Fujimoto, M. K.: 2008, Operational status
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Takahashi, R., et al. including Sugiyama, N.: 2008, Simulationsof baryon acoustic oscillations - I. Growth of large-scale density
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Takahashi, S., Saito, M., Ohashi, N., Kusakabe, N., Takakuwa, S.,
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Takato, N.: 2008, Rotation-Resolved Spectroscopy of a Very
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Takechi, S., et al. including Sasaki, S.: 2008, Investigation on piezoelectric lead zirconate titanate detector bombarded obliquelywith hypervelocity iron particles, P&SS, 56, 1309-1313.
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Takeda, Y., Kawanomoto, S., Ohishi, N.: 2008, Rotational Featureof Vega Revealed from Spectral Line Profiles, ApJ, 678, 446-462.
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Takeda, Y.: 2008, Abundances of lithium, sodium and potassiumin Vega, MNRAS, 388, 913-920.
Takiwaki T., Kotake, K., Sato, K.: 2009, Special Relativistic Simulations of Magnetically-dominated Jets in Collapsing Massive
Stars, ApJ, 691, 1360-1379.

Tanabq, T., et al. including Ita, Y.: 2008, Absolute Photometric
Calibration of the Infrared Camera (IRC) aboard AKARI, PASJ,60, 375.
Tanaka, M., et al. including Yoshida, M.: 2009, Supernova 2008D
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Tanaka, M., Finoguenov, A., Kodama, T., Morokuma, T., Rosati,P., Stanford, S. A., Eisenhardt, P., Holden, B., Mei, S.: 2008,
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Tanaka, M., Kawabata, K. S., Maeda, K., Hattori, T., Nomoto, K.:
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Tashiro, H., Silk, J., Langer, M., Sugiyama, N.: 2009, The SunyaevZel'dovich effect and Faraday rotation contributions of galaxygroups to the CMB angular power spectrum, MNRAS, 392,
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Tashiro, H., Sugiyama, N.: 2008, Constraints on primordial black
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Tatematsu, K., Kandori, R., Umemoto, T., Sekimoto, Y.: 2008,
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Tatsumi, D.: 2008, TAMA300 interferometer development, JPhCS,
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Tokuno, H., et al. including Mizumoto, Y., Shirasaki, Y.: 2008, The
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Tokutani, M., Yoshida, N., Oh, P. S., Sugiyama, N.: 2009, The
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Totani, T., Morokuma, T., Oda, T., Doi, M., Yasuda, N.: 2008,
Delay Time Distribution Measurement of Type Ia Supernovae
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Toth, G., et al. including Goossens, S.: 2009, IAG Newsletter, J.
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Tsap, Y. T., Kopylova, Y. G., Stepanov, A. V., Melnikov, V. F.,
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Tsuboi, M., et al. including Tosaki, T., Kuno, N., Nakanishi, K.,
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Tsuneta, S., et al. including Katsukawa, Y., Shimojo, M.,
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Tsuneta, S., et al. including Katsukawa, Y., Suematsu, Y.: 2008,

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The Solar Optical Telescope (SOT) for the Solar-B Mission,
SoPh, 249, 167.
Uchimoto, Y. K., et al. including Suzuki, R., Omata, K.,
Nishimura, T., Tanaka, I.: 2008, Subaru/MOIRCS Near-Infrared
Imaging in the Proto-Cluster Region at z=3.1, PASJ, 60, 683-693.
Ueda, H., Nagashima, M., Yahagi, H.: 2008, Analysis of theSpatial Distribution of Galaxies in the Numerical Galaxy
Catalog, PASJ, 61, 85.
Ueda, K., Imai, H., Deguchi, S., Kamohara, R., Maeda, T.,
Matsumoto, N., Omodaka, T.: 2008, Japanese VLBI Network
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PASJ, 60, 1051-1056.
Ueda, Y., et al. including Sekiguchi, K.: 2008, The Subaru/XMMNewton Deep Survey (SXDS). III. X-Ray Data, ApJS, 179,
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Uehara, T., Sato, A., Maehara, S., Nimonji, T., Sato, T., Ohkawa,
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Uemura, M., et al. including Yamashita, T.: 2008, Discovery ofa WZ Sge-Type Dwarf Nova, SDSS J102146.44+234926.3:
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Ueta, T., Izumiura, H., Yamamura, I., Nakada, Y., Matsuura, M.,
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AKARI/FIS Mapping of the ISM-Wind Bow Shock around α
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Ujino, H., Vinet, L., Yajima, T., Yoshida, H.: 2008, Additional
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Vargas Dominguez, S., Rouppe van der Voort, L., Bonet, J. A.,
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Moat Flow in the Vicinity of Sunspots for Various Penumbral
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Warren, H. P., Winebarger, A. R., Mariska, J. T., Doschek, G. A.,
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Watabe, Y., Kawakatu, N., Imanishi, M.: 2008, Nuclear/Circumnuclear Starbursts and Active Galactic Nucleus Mass
Accretion in Seyfert Galaxies, ApJ, 677, 895-905.
Watanabe, H., Kitai, R., Ichimoto, K., Katsukawa, Y.: 2009,
Magnetic Structure of Umbral Dots Observed with the HinodeSolar Optical Telescope, PASJ, 61, 193.
Watanabe, T., Hara, H., Yamamoto, N., Kato, D., Sakaue, H.
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Fe XIII Density Diagnostics in the EIS Observing Wavelengths,
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Whitney, B. A., et al. including Mizuno, N.: 2008, Spitzer Sage
Survey of the Large Magellanic Cloud. III. Star Formation and~1000 New Candidate Young Stellar Objects, AJ, 136, 18-43.
Wilson, C. D., et al. including Iono, D.: 2008, Luminous Infrared
Galaxies with the Submillimeter Array: I. Survey Overview and
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Wilson, G. W., et al. including Ezawa, H., Kawabe, R., Kuboi,

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A., Matsuo, H., Murakoshi, Y., Oshima, T., Tanaka, K.,
Yamaguchi, N.: 2008, A Bright, Dust-Obscure, MillimeterSelected Galaxy Beyond the Bullet Cluster (1E0657-56),
MNRAS, 390, 1061-1070.
Winn, J. N., Johnson, J. A., Narita, N., Suto, Y., Turner, E. L.,
Fischer, D. A., Butler, R. P., Vogt, S. S., O'Donovan, F. T.,
Gaudi, B. S.: 2008, The Prograde Orbit of Exoplanet TrES-2b,
ApJ, 682, 1283-1288.
Yabe, K., Ohta, K., Iwata, I., Sawicki, M., Tamura, N., Akiyama,
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Galaxies at z~5, ApJ, 693, 507.
Yamamoto, H., et al. including Mizuno, N.: 2008, Aligned Molecular Clouds towards SS 433 and L = 348°.5: Possible Evidence
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Yamamoto, K., et al. including Tatsumi, D.: 2008, Current statusof the CLIO project, JPhCS, 122, 12002.
Yamamoto, K., Hayakawa, H., Okada, A., Uchiyama, T., Miyoki,
S., Ohashi, M., Kuroda, K., Kanda, N., Tatsumi, D., Tsunesada,Y.: 2008, Effect of energy deposited by cosmic-ray particles oninterferometric gravitational wave detectors, PhRvD, 78, 22004.
Yamamoto, N., Kinoshita, D., Fuse, T., Watanabe, J., Kawabata,K.: 2008, A Deep Sky Survey of Edgeworth Kuiper Belt Objects
with an Improved Shift-and-Add Method, PASJ, 60, 285-291.
Yamamoto, T. T., Sakurai, T.: 2009, Correlations between FlareParameters and Magnetic Parameters in Solar Flares, PASJ, 61,
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Yamamoto, Y., Okada, T., Shiraishi, H., Shirai, K., Arai, T.,
Ogawa, K., Hosono, K., Arakawa, M., Kato, M.: 2008, Current
status of X-ray spectrometer development in the SELENE
project, AdSpR, 42, 305-309.
Yamauchi, C., Yagi, M., Goto, T.: 2008, E+A and Companion
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Yamazaki, D. G., Ichiki, K., Kajino, T., Mathews, G. J.: 2008,
Effects of a primordial magnetic field on low and high multipolesof the cosmic microwave background, PhRvD, 77, 43005.
Yamazaki, D. G., Kajino, T., Ichiki, K., Mathews, G. J.: 2008,
Constraints on the Primordial Magnetic Field from σ8, PhRvD,
78, 1123001.
Yan, J., Li, F., Ping, J., Goossens, S.: 2009, Lunar gravity fieldrecovery based on LP Doppler data, Cehui Xuebao/Acta
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Yan, J., Ping, J., Matsumoto, K., Li, F.: 2008, The Simulation oflunar gravity field recovery from D-VLBI of Chang’E-1 andSELENE lunar orbiters, AdSpR, 42, 337-340.
Yasutake, N., Kashiwa, K.: 2009, Lepton effects on the protoneutron stars with the hadron-quark mixed phase in the NambuJona-Lasinio model, PhRvD, 79, 43012.
Yasutake, N., Noda, T., Yamada, S., Hashimoto, M. Kotake, K.:
2008, Effects of QCD Phase Pransition on Ejected Elementsfrom the Envelopes of Compact Stars, Physics of Self- Organization Systems, 1, 219.
Yoshida, F., Nakamura, T.: 2008, A Comparative Study of Size
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Yoshida, M., Shimasaku, K., Ouchi, M., Sekiguchi, K., Furusawa,

H., Okamura, S.: 2008, The Subaru/XMM-Newton Deep
Survey (SXDS). VII. Clustering Segregation with Ultraviolet
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ApJ, 679, 269-278.
Yoshida, M., Yagi, M., Komiyama, Y., Furusawa, H., Kashikawa,N., Koyama, Y., Yamanoi, H., Hattori, T., Okamura, S.: 2008,
Strange Filamentary Structures ("Fireballs'') around a Merger
Galaxy in the Coma Cluster of Galaxies, ApJ, 688, 918-930.
Yoshida, N., Omukai, K., Hernquist, L.: 2008, Protostar Formationin the Early Universe, Science, 321, 669-671.
Yoshida, T., Suzuki, T., Chiba, S., Kajino, T., Yokomakura, H.,
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in Supernova Explosions, ApJ, 686, 448-466.
Young, P. R., Watanabe, T., Hara, H., Mariska, J. T.: 2009, Highprecision density measurements in the solar corona - I. Analysis
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Younger, J. D., et al. including Iono, D.: 2008, Clarifying the
Nature of the Brightest Submillimeter Sources: Interferometric
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Younger, J. D., et al. including Iono, D.: 2008, The PhysicalScale of the Far-Infrared Emission in the Most Luminous
Submillimeter Galaxies, ApJ, 688, 59-66.

2. Publications of the National Astronomical Observatory of Japan
Ukita, N., Ikenoue, B., Saito, M.: 2008, Optical Seeing Measurements with an Optical Telescope on a Radio Antenna, Publ.
Nat. Astron. Obs. Japan, 11, 1-12.
Sôma, M.: 2008, List of Lunar Eclipses between 1500 BC and1000 BC, Publ. Nat. Astron. Obs. Japan, 11, 13-35.

3. Report of the National Astronomical Observatory ofJapan (in Japanese)
Ishizaki, H.: 2008, Frequency Characteristics of AtmosphericTurbulent Flow in the Troposphere and Disturbance of Boundary under the Ionosphere Observed with the Radio Seeing
Monitors. —To Realize Phase Compensation of the ALMA
Observations, Rep. Nat. Astron. Obs. Japan, 11, 15-30.
Sekiguchi, H., Kawashima, S., Shinohara, N., Houjyou, M.:
2008, Trouble Database and Availability of Nobeyama Radioheliograph System, Rep. Nat. Astron. Obs. Japan, 11, 1-13.
Katayama, M., Matsuda, K., Fukushima, T., Watanabe, J.-I.:
2008, Revising Plan of “Calendar and Ephemeris”, Rep. Nat.
Astron. Obs. Japan, 11, 57-67.
Tanikawa, K., Sôma, M.: 2008, Japanese Astronomy in the Seventh Century, Rep. Nat. Astron. Obs. Japan, 11, 31-55.

4. Conference ProceedingsAbe, L., Venet, M., Enya, K., Kataza, H., Nakagawa, T., Tamura,M.: 2008, Multi-stage apodized pupil Lyot coronagraphexperimental results, SPIE 7014, Eds. I. S. McLean, M. M.
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Abe, M., et al. including Takato, N., Fujiyoshi, T., Terada, H.:
2008, Ground-based Observational Campaign for 162173
1999JU3, the Target Asteroid of Sample Return Mission,
Hayabusa-2, Asteroids, Comets, Meteors 2008.
Abe, M., et al. including Takato, N., Fujiyoshi, T., Terada, H.:
2008, Ground-based observational campaign for asteroid
162173 1999 JU3, 37th COSPAR Scientific Assembly,
B04-0061-08, 12.
Abe, M., et al. including Takato, N., Fujiyoshi, T., Terada, H.:
2008, Ground-based Observational Campaign for Asteroid
162173 1999 JU3, 39th Lunar and Planetary Science Conf.
Abramov-Maximov, V. E., Gelfreikh, G. B., Kobanov, N. I.,
Shibasaki, K.: 2009, A comparison of parameters of 3-minuteand 5-minute oscillations in sunspots from synchronous
microwave and optical observations, Proc. of the IAU Symp.
257, Eds. N. Gopalswamy, D. F. Webb, 95-99.
Adams, M., Boffin, H. J., Garnier, W., Iono, D.: 2008, The Global
ALMA EPO Programme: Communicating Astronomy with the
Public at Millimetre and Submillimetre Wavelengths,, Proc.
of the IAU/NOA/ESA/ESO Conf., Eds. L. L. Christensen, M.
Zoulias, I. Robson, 288-293.
Agata, H.: 2008, Science as a Culture, and an Introduction to new
PUR experiments in Japan, Global Hands-On Universe 2007,
Eds. T. Handa, M. Okyudo, 119-121.
Akitaya, H., et al. including Iye, M., Okita, K., Sato, N., Matsuo,
H., Yamashita, T.: 2008, Application of zero-expansion porefree ceramics to a mirror of an astronomical telescope, SPIE
7018, 70183H.
Akiyama, M., Minowa, Y., Kobayashi, N., Ohta, K., Iwata, I.:
2008, Adaptive Optics Rest-frame V-band Imaging of Galaxies
at z˜3: High Surface Density Disk-Like Galaxies?, Panoramic
Views of Galaxy Formation and Evolution (ASP Conf. Ser.
399), Eds. T. Kodama, T. Yamada, K. Aoki, 247.
Akiyama, M., Minowa, Y., Kobayashi, N., Ohta, K., Iwata, I.:
2008, Adaptive optics imaging of Lyman break galaxies asprogenitors of spheroids in the local Universe, Proc. of the IAU
Symp. 245, Eds. M. Bureau, E. Athanassoula, B. Barbuy, 447.
Akiyama, M., Smedley, S., Gillingham, P., Brzeski, J., Farrell, T.,
Kimura, M., Muller, R., Tamura, N., Takato, N.: 2008,
Performance of Echidna fiber positioner for FMOS on Subaru,
SPIE 7018.
Antolin, P., Shibata, K., Kudoh, T., Shiota, D., Brooks, D.: 2008,
Predicting observational signatures of coronal heating by Alfvén
waves and nanoflares, Proc. of the IAU Symp. 247, Eds. R.
Erdelyi, C. A. Mendoza-Briceno, 279.
Aoki, K., Totani, T., Hattori, T., Ohta, K., Kawabata, K. S.,
Kobayashi, N., Iye, M., Nomoto, K., Kawai, N.: 2008, No
Evidence for Variability of Intervening Absorption Lines toward
GRB 060206: Implications for the Mg II Incidence Problem,
arXiv0808:4157.
Aoki, W., Barklem, P., Beers, T. C., Christlieb, N., Inoue, S.: 2008,
Lithium Abundances in Extremely Metal-Poor Turn-Off Stars,
AIP Conf. Proc. 1016, Eds. T. Suda, et al., 37-42.
Arlot, J.-E., et al. including Sôma, M.: 2008, Division I-III/Working Group Natural Planetary Satellites, Trans. IAU 27A,
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Asada, K., Inoue, M., Nakamura, M., Kameno, S., Nagai, H.:
2008, Rotation Measure Observation towards NRAO 140 Jet:
Constraints for the Pitch Angle of a Helical Magnetic Field,
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Simulations of the Quiet Sun Radio Emission at Millimeterand Submillimeter Wavelengths, Geofísica Internacional, 47,
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Deguchi, S., Matsunaga, N., Fukushi, H., Kaminski, T.: 2009,
Detection of the SiO J=2–1, v=1 Maser Emission at 86.2 GHz in
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Doi, M., et al. including Morokuma, T., Furusawa, H., Nakaya,
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Ebizuka, N., Yokota, H., Kajino, F., Kawabata, K. S., Iye, M., Sato,S.: 2008, Novel direct vision prism and Wollaston prism
assembly for diffraction limit applications, SPIE 7018, 70184S6.
Endo, A., Noguchi, T., Kroug, M., Shitov, S. V., Shan, W.,
Tamura, T., Kojima, T., Uzawa, Y., Sakai, T., Inoue, H.,
Muraoka, K., Kohno, K.: 2008, A Novel THz SIS Mixer with a
NbTiN-Ground Plane and SIS Micro-Trilayers Directly Grown
on a Quartz Substrate, Proc. of the 19th Int. Symp. on SpaceTHz Technology, Ed. W. Wild, 73-78.
Enya, K., et al. including Tamura, M., Nishikawa, J., Murakami,
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Ezawa, H., et al. including Kawabe, R., Iwashita, H., Matsuo, H.,
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2008, New Archevements of ASTE: the Atacama Submillimeter
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Fukushima, T.: 2008, Astrometry Course at University of Tokyo,
Proc. of the IAU Symp. 248, Eds. W. J. Jin, I. Platais, M. A. C.
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Furusawa, H., Kosugi, G., Akiyama, M., Takata, T., Sekiguchi,
K., Furusawa, J.: 2008, Subaru/XMM-Newton Deep Survey(SXDS) - Optical Imaging Survey and Photometric Catalogs,
Panoramic Views of Galaxy Formation and Evolution (ASP
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Furusawa, H., et al. including Komiyama, Y., Miyazaki, S.,
Utsumi, Y.: 2008, Hyper Suprime-Cam: data analysis andmanagement system, SPIE 7016, Eds. R. J. Brissenden, D. R.

Silva, 45.
García Pérez, A. E., et al. including Aoki, W.: 2008, A new sample
of extremely/ultra metal-poor stars, Physica Scripta 133, 14036.
Gomez, Y., et al. including Deguchi, S.: 2008, HCO+ Emission
Possibly Related with a Shielding Mechanism that Protects
Water Molecules in the Young PN K 3-35, Proc. of the IAU
Symp. 251, Eds. S. Kwok, S. Sandford, 173-174.
Goossens, S., Matsumoto, K., Ishihara, Y., Liu, Q., Iwata, T.,
Namiki, N., Noda, H., Hanada, H., Kikuchi, F., Kawano, N.,
Tsuruta, S., Asari, K., Ishikawa, T., Sasaki, S.: 2008, Initial
results of global lunar gravity field recovery from Kaguya
tracking data, Proc. 41th Lunar Planet. Symp.
Goossens, S., Matsumoto, K., Ishihara, Y., Liu, Q., Kikuchi,F., Noda, H.: 2008, Kaguya orbit determination and quality
assessment, Proc. 18th JAXA Workshop on Astrodynamics andFlight Mechanics, 298-306.
Gopalswamy, N., Yashiro, S., Shibasaki, K.: 2008, Heating andKinematics of an Eruptive Prominence Associated with a Fast
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Gordon, K. D., et al. including Mizuno, N.: 2009, Early resultsfrom the SAGE-SMC Spitzer legacy, Proc. of the IAU Symp.
256, Eds. J. Th. van Loon, J. M. Oliveira, 184-188.
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T.: 2008, Infrared
space astrometry project JASMINE, Proc. of the IAU Symp.
248, Eds. W. J. Jin, I. Platais, M. A. C. Perryman, 248-251.
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B. Barbuy, 355-358.
Guyon, O.: 2008, Ultra-high-sensitivity wavefront sensing for
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Guyon, O., et al. including Tamura, M.: 2008, Pupil mapping
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Hanada, H., et al. including Kawano, N., Asari, K., Ishihara,Y., Ishikawa, T., Kikuchi, F., Liu, Q., Matsumoto, K., Noda,
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VLBI Observation of SELENE (KAGUYA) by VERA andInternational Network, IVS.
Hara, H.: 2008, Overview of EIS performance, First Results from
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Hasegawa, S., Miyasaka, S., Tokimasa, N., Sogame, A., Ibrahimov,
M. A., Yoshida, F., Abe, M., Kuroda, D.: 2009 Mar 1 , BRz'
Phase Function of Asteroid 4 Vesta During the 2006 Opposition,
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Hayakawa, T., Iwamoto, N., Kajino, T., Shizuma, T., Umeda, H.,
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AIP Conf. Proc. 1016, Eds. T. Suda, et al., 111-116.
Hayakawa, T., Iwamoto, N., Kajino, T., Shizuma, T., Umeda, H.,
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Hayakawa, T., Iwamoto, N., Shimizu, T., Kajino, T., Umeda, H.,
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Hayano, Y., Takami, H., Guyon, O., Oya, S., Hattori, M., Saito,
Y., Watanabe, M., Murakami, N., Minowa, Y., Ito, M.,
Colley, S., Eldred, E., Golota, T., Dinkins, M., Kashikawa,N., Iye, M.: 2008, Current status of the laser guide star adaptive
optic system for Subaru telescope, SPIE 7015, Eds. N. Hubin, C.
E. Max, P. L. Wizinowich, 701510.
Hayashi, M., Motohara, K., Shimasaku, K., Onodera, M.,
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Hayashi, M., Nakajima, T., Usuda, T.: 2008, HiCIAO: theSubaru Telescope's new high-contrast coronographic imager foradaptive optics, SPIE 7014, Eds. I. S. McLean, M. M. Casali,
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Honma, M., et al. including Iwadate, K., Jike, T., Kameya, O.,
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Hosokawa, T., Omukai, K.: 2008, Evolution of Massive Protostars with High Accretion Rates, Massive Star Formation:
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2009, Studying the lunar ionosphere with the SELENE radio

II Publications, Presentations071

science experiment, ISTS.
Inoue, H., Muraoka, K., Sakai, T., Endo, A., Kohno, K., Asayama,S., Noguchi, T., Ogawa, H.: 2008, 350 GHz Sideband Separating
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Inoue, M., Asada, K., Nagai, H.: 2008, A New Method to Detect
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Inoue, M., Nagai, H., Asada, K., Saito, H., Tsuboi, M.: 2008, The
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Three-Dimensional Structure Analysis of Coronal Magnetic Field
in AR NOAA 10930 Based on Vector Magnetogram Observations
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Ishihara, D., et al. including Ita, Y.: 2008, Mid-infrared all-sky
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Ishihara, D., et al. including Ita, Y.: 2009, AKARI Mid-Infrared
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Ita Y.: 2009, Period-Mbol Relations of Variable Stars in the Large
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Iwata, I., Ohta, K., Sawicki, M., Tamura, N., Akiyama, M., Aoki,
K.: 2008, Differential Evolution of Lyman Break Galaxies fromz=5 to 3, Panoramic Views of Galaxy Formation and Evolution(ASP Conf. Ser. 399), Eds. T. Kodama, T. Yamada, K. Aoki, 127.
Iwata, T., et al. including Hanada, H., Noda, H., Kawano, N.,
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Iye, M.: 2008, High redshift galaxy surveys, SPIE 7016, Eds. R. J.
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Iye, M., Kashikawa, N., Furusawa, H., Ota, K., Ouchi, M.,

072

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Shimasaku, K.: 2008, Suprime-Cam LAE Survey at Redshift
7.3 – Ultimate Limit with New Red-Sensitve CCDs, Panoramic
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399), Eds. T. Kodama, T. Yamada, K. Aoki, 61-62.
Izumiura, H.: 2009, AKARI's View of the Extended Dust Shellsof Evolved Stars, AGB Stars and Related Phenomena, Eds. T.
Ueta, N. Matsunaga, Y. Ita, 14-18.
Jenniskens, P., Sato, M., Watanabe, J.: 2008, Orionid Meteors
2008, Central Bureau Electronic Telegrams, Ed. D. W. E. Green.
Jike, T., Manabe, S., Tamura, Y.: 2008, Result from K-band Geodetic
VLBI using VERA, Measuring the Future, Proc. of the 5th IVS
General Meetings, Eds. A. Finkelstein, D. Behrend, 293-296.
Jike, T., Manabe, S., Tamura, Y., Shizugami, M.: 2008, VERA
Geodetic Activities, IVS 2007 Annual Report, Eds. D. Behrend,
K. D. Baver, 69-71.
Kadono, T., Sugita, S., Sako, S., Ootsubo, T., Kawakita, H.,
Honda, M., Miyata, T., Furusho, R., Watanabe, J.: 2009, The
Subsurface Structure of Comet 9P/Tempel 1 Projected into
the Dust Plume, Deep Impact as a World Observatory Event:
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Symposia, Eds. H. U. Käufl, C. Sterken, 143.
Kajino, T., Kusakabe, M., Kojima, K., Yoshida, T., Yamazaki, D.
G., Ichiki, K., Mathews, G. J.: 2008, Neutrino Mass and Cold
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Kajino, T., Sasaqui, T., Yoshida, T., Aoki, W.: 2008, Neutrino
Oscillation in Supernova and GRB Nucleosynthesis, Modern
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Kajisawa, M., et al. including Suzuki, R., Omata, K., Tanaka,I., Nishimura, T.: 2008, Distant Red Galaxies in the MOIRCS
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Aoki, 296.
Kamata, Y., Miyazaki, S., Nakaya, H., Tsuru, T. G., Tsunemi,
H., Miyata, E., Muramatsu, M., Suzuki, H., Miyaguchi, K.:
2008, Evaluation of the fully-depleted back-illuminated CCD
for Subaru Suprime-Cam, SPIE 7021, Eds. D. A. Dorn, A. D.
Holland, 70211S.
Kamikura, M., Naruse, M., Asayama, S., Satou, N., Shan, W.,
Sekimoto, Y.: 2008, Development of a 385-500 GHz Orthomode Transducer (OMT), Proc. of the 19th Int. Symp. on SpaceTHz Technology, Ed. W. Wild, 557-562.
Kamio, S., Hara, H., Watanabe, T.: 2008, Velocity structure ofbright points in a coronal hole, First Results from Hinode (ASP
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Kaneda, H., Onaka, T., Sakon, I., Matsumoto, H., Suzuki, T.: 2008,
Polycyclic aromatic hydrocarbons in elliptical galaxies, Proc. of
the IAU Symp. 251, Eds. S. Kwok, S. Sandford, 247-248.
Kaneda, H., Suzuki, T., Haze, K., Okada, Y., Onaka, T., Sakon,
I.: 2008, ISM in nearby elliptical galaxies revealed by AKARIand Spitzer, EAS Publication Series 31, Far-Infrared Workshop
2007, Eds. C. Kramer, S. Aalto R. Simon, 181-182.
Kawabata, K. S., et al. including Nakaya, H., Kamata, Y., Miyazaki,
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Kawada, M., et al. including Matsuo, H.: 2008, Imaging Fourier

transform spectrometer with photoconductive detector arrays:
an application to the AKARI far-infrared instrument, SPIE
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Kawaguchi, T., Nakanishi, K., Kohno, K., Ohta, K., Aoki, K.:
2008, 12CO Observations on Narrow-Line Seyfert 1 Galaxies,
Proc. of the IAU Symp. 245, Eds. M. Bureau, E. Athanassoula,
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Kawaguchi, T., Nakanishi, K., Kohno, K., Ohta, K., Aoki, W.:
2008, Molecular Gas in Narrow-Line seyfert 1 Galaxy: A Search
for Coevolving Massive Black Holes and Galaxies, Panoramic
Views of Galaxy Formation and Evolution (ASP Conf. Ser.
399), Eds. T. Kodama, T. Yamada, K. Aoki, 427-428.
Kawakatu, N., Nagai, H., Kino, M.: 2009, Fate of baby radiogalaxies: Dead or alive?, Astronomische Nachrichten, 330,
283-286.
Kawamura, A., Minamidani, T., Mizuno, Y., Mizuno, N., Onishi,T., Mizuno, A., Fukui, Y.: 2009, Molecular Clouds and Star
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Kawanomoto, S., Kajino, T., Suzuki, T. K., Ando, H., Aoki, W.:
2008, 7Li/6Li Ratio in Distant Interstellar Media and Primordial 7LiImplementation in Big-Bang Cosmology and Galactic Chemical
Evolution, AIP Conf. Proc. 1016, Eds. T. Suda, et al., 21-26.
Keum, Y. Y., Ichiki, K., Kajino, T.: 2008, Neutrino Mass Bounds
from Neutrinoless Double Beta Decays and Large, AIP Conf.
Proc. 1016, Eds. T. Suda, et al., 343-349.
Kikuchi, F., et al. including Liu, Q., Hanada, H., Kawano, N.,
Matsumoto, K.: 2008, Pico-second Accuracy VLBI of the Two
Sub-satellites of SELENE (KAGUYA) using Multi-Frequency
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Kikuchi, F., et al. including Liu, Q., Matsumoto, K., Ishihara, Y.,
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Li, J., Shen, Z. Q., Miyazaki, A., Miyoshi, M., Tsutsumi, T.,
Tsuboi, M., Huang, L., Sault, B.: 2008, The 3-mm flux density
monitoring of Sagittarius A* with the ATCA, Proc. of the IAU
Symp. 248, Eds. W. J. Jin, I. Platais, M. A. C. Perryman, 204-205.
Lites, B. W., et al. including Katsukawa, Y., Tsuneta, S., Suematsu,
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Perspective From Hinode, First Results from Hinode (ASP Conf.
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Luzum, B. J., et al. including Fukushima, T.: 2008, Report on
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Luzum, B. J., et al. including Fukushima, T.: 2008, Current
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Machida, M., Matsumoto, R.: 2009, Magneto-hydrodynamic Simulations of Excitation of Low-Frequency QPOs in Black Hole
Candidates, Astrophysics with All-Sky X-Ray Observations,
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Magara, T., Katsukawa, Y., Ichimoto, K., Tsuneta, S., Yokoyama,T., Nagata, S., Inoue, S.: 2008, Evolution of Magnetic Field andFlow in NOAA 10930 Obtained by Hinode, First Results from
Hinode (ASP Conf. Ser. 397), Eds. S. A. Mattews, J. M. Davis, L.
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Martinache, F., Guyon, O., Lozi, J., Tamura, M., Hodapp, K.,
Suzuki, R., Hayano, Y., McElwain, M. W.: 2009, The Subaru
Coronagraphic Extreme AO Project, AAS 213, 398.
Mathews, G. J., Ichiki, K., Kajino, T., Lan, N. Q., Zhao, X.: 2008,
Alternative Unified Views on Dark Matter and Dark Energy,
Modern Physics Letters A, 23, 1372-1383.
Matsumoto, R., Machida, M., Oda, H.: 2009, Variability Sciencein Accretion Disc Theory, Astrophysics with All-Sky X-Ray
Observations, Proc. of the RIKEN Symp., 126.
Matsuo, H., Hibi, Y., Nagata, H., Ariyoshi, S., Otani, C.,
Ikeda, H., Fujiwara, M.: 2008, Design of Superconducting
Terahertz Digicam, Proc. of the 19th Int. Symp. on Space THz
Technology, Ed. W. Wild, 466-472.
Matsuo, H., Hibi, Y., Nagata, H., Nakahashi, M., Murakoshi, Y.,
Arai, H., Ariyoshi, S., Otani, C., Ikeda, H., Fujiwara, M.: 2008,
System design of submillimeter-wave imaging array SISCAM,SPIE 7020, Eds. W. D. Duncan, W. S. Holland, 702015.
Matsuo, T., Shibai, H., Kawada, M., Hattori, M., Ohta, S. I.,
Matsuo, H.: 2008, Novel spectral imaging method for Fizeau
interferometer, SPIE 7013, Eds. M. Schöller, W. C. Danchi, F.
Delplancke, 70132F.
Minamidani, T., Mizuno, N., Mizuno, Y., Kawamura, A.,
Onishi, T., Tatematsu, K., Hasegawa, T., Ikeda, M., Fukui, Y.:
2009, An observational study of GMCs in the Magellanic
Clouds with the ASTE telescope, Proc. of the IAU Symp. 256,
Eds. J. Th. van Loon, J. M. Oliveira, 256-260.
Minowa, Y., Takami, H., Watanabe, M., Hayano, Y., Miyake,M., Iye, M., Oya, S., Hattori, M., Murakami, N., Guyon,O., Saito, Y., Itoh, M., Colley, S., Dinkins, M., Eldred, M.,
Golota, T.: 2008, Development of a dichroic beam splitter for
Subaru AO188, SPIE 7015, Eds. N. Hubin, C. E. Max, P. L.
Wizinowich, 701561-1-8.

Misawa, T., Eracleous, M., Charlton, J. C., Chartas, G., Kashikawa,N.: 2008, Dramatically Variable C IV Mini-Broad Absorption
Line System in the Quasar HS 1603+3820, Panoramic Views ofGalaxy Formation and Evolution (ASP Conf. Ser. 399), Eds. T.
Kodama, T. Yamada, K. Aoki, 423.
Mitsui, K., Okada, N., Fukushima, M., Nishino, T., Okamoto,Y. K., Kataza, H., Onaka, T.: 2008, Fabrication of slicer optics
of mid-infrared spectrometer with an image slicer (MIRSIS) for
ground-based astronomy, SPIE 7014, Eds. I. S. McLean, M. M.
Casali, 701427.
Miura, N., Noto, Y., Kato, S., Kuwamura, S., Baba, N., Hanaoka,
Y., Nagata, S., Ueno, S., Kitai, R., Takami, H.: 2009, Solar
Adaptive Optic system at the Hida Observatory, SPIE 7015,
Eds. N. Hubin, C. E. Max, P. L. Wizinowich, 70156U-1-U-8.
Miyata, T., et al. including Ezawa, H.: 2008, Site Evaluations of
the Summit of Co. Chajnantor for Infrared Observations, SPIE
7012, Eds. L. M. Stepp, R. Gilmozzi, 701243-1-8.
Miyatake, H., Uchida, T., Fujimori, H., Mineo, S., Nakaya, H.,
Aihara, H., Miyazaki, S.: 2008, Prototype Readout Module forHyper Suprime-Cam, IEEE Nuclear Science Symp. N02-25, 737.
Mori, Y. A., Nakajima, H., Shimokawabe, T., Kawai, N., Kuroda,D., Yoshida, M., Yanagisawa, K., Shimizu, Y., Toda, H.,
Nagayama, S.: 2008, GRB081203A: MITSuME optical observation, GRB Coordinates Network, Circular Service, 8619, 1.
Mori, Y., Sekiguchi, T., Sugita, S., Matsunaga, N., Fukushi,
H., Kaneyasu, N., Kawadu, T., Kandori, R., Nakajima, Y.,
Tamura, M.: 2009, One Month of Near-IR Imaging Photometryof Comet 9P/Tempel 1, Deep Impact as a World Observatory
Event: Synergies in Space, Time, and Wavelength, Eso
Astrophysics Symposia, Eds. H. U. Käufl, C. Sterken, 323.
Morokuma, T., et al. including Sekiguchi, K., Furusawa, H.,
Kashikawa, N.: 2008, Wide-Field Optical Variability Survey
for Low-Luminosity AGN with Suprime-Cam, Panoramic
Views of Galaxy Formation and Evolution (ASP Conf. Ser.
399), Eds. T. Kodama, T. Yamada, K. Aoki, 417.
Morokuma, T., Komiyama, Y., Miyazaki, S., Nakaya, H.,
Furusawa, H., Tomono, D., Kawanomoto, S., Tanaka, Y.:
2008, Hyper Suprime-Cam: autoguider and Shack-Hartmannsystems, SPIE 7014, Eds. I. S. McLean, M. M. Casali, 161.
Motohara, K., et al. including Uraguchi, F., Takato, N.: 2008,
Seeing environment at a 5640m altitude of Co. Chajnantor innorthern Chile, SPIE 7012, Eds. L. M. Stepp, R. Gilmozzi.
Motohara, K., Hayashi, M., Shimasaku, K., Yoshida, M.,
Kashikawa, N., Kodama, T.: 2008, Deep- and Wide-field
K-band Imaging of the Subaru Deep Field: Implications for
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Murakami, N., Uemura, R., Baba, N., Shibuya, H., Nishikawa,J., Abe, L., Tamura, M., Hashimoto, N.: 2008, Laboratory
experiments on the 8-octant phase-mask coronagraph, SPIE
7010, Eds. Jr. J. M., Oschmann, M. W. M., de Graauw, H. A.
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Nagai, H., Asada, K., Doi, A., Kameno, S., Inoue, M.: 2008,
Kinematic and Synchrotron Ages of Compact Symmetric Objects,
Extragalactic Jets: Theory and Observation from Radio to Gamma

Ray (ASP Conf. Ser. 386), Eds. T. A. Rector, D. S. De Young, 290.
Nagashima, M., Okamoto, T.: 2008, Chemical Abundance Patterns
in the Local Dwarf Galaxies in the CDM Universe, Panoramic
Views of Galaxy Formation and Evolution (ASP Conf. Ser.
399), Eds. T. Kodama, T. Yamada, K. Aoki, 475.
Nagata, H., Kobayashi, J., Matsuo, H., Hibi, Y., Nakahashi, M.,
Ikeda, H., Fujiwara, M.: 2008, Development of a cryogenic
GaAs AC-coupled CTIA readout for far-infrared andsubmillimeter detectors, SPIE 7020, Eds. W. D. Duncan, W. S.
Holland, 70202Q.
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, Mapping the Galaxy and Nearby
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Nakagawa, A., Omodaka, T., Shibata, K. M., Kurayama, T., Imai,
H., Kameno, S., Tsushima, M., Matsumoto, N., Matsui, M.:
2008, Parallax measurement of the Galactic Mira variables with
VERA , Proc. of the IAU Symp. 248, Eds. W. J. Jin, I. Platais, M.
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Nakajima, K., Ebizuka, N., Iye, M., Kodate, K.: 2008, Optimal
fabrication of volume phase holographic grism with highefficiency and high dispersion, and its applications for
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Casali, 70741Q11.
Nakajima, T., Sakai, T., Asayama, S., Kimura, K., Kawamura, M.,
Yonekura, Y., Ogawa, H., Kuno, N., Noguchi, T., Tsuboi, M.,
Kawabe, R.: 2008, Development of a Waveguide-Type DualPolarization Sideband-Separating SIS Receiver System in 100
GHz Band for the NRO 45-m Radio Telescope, Proc. of the 19thInt. Symp. on Space THz Technology, Ed. W. Wild, 286-291.
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Nakashima, J., Deguchi, S., Imai, H., Kembell, A.: 2008, MolecularLine Observations of the SiO Maser Source IRAS 19312+1950,
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Naruse, M., Kamikura, M., Sekimoto, Y., Ito, T., Sugimoto, M.,
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Virtual wavefront compensation and speckle reduction incoronagraph by unbalanced nulling interferometer (UNI) andphase and amplitude correction (PAC), SPIE 7010, Eds. Jr. J. M.,

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Niwa, Y., Arai, K., Ueda, A., Sakagami, M., Gouda, N., Kobayashi,Y., Yamada, Y., Yano, T.: 2008, Laser interferometric highprecision geometry (angle and length) monitor for JASMINE,
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Noguchi, T., Suzuki, T., Endo, A., Tamura, T.: 2009, Effect of
the energy-gap broadening on subgap current of SIS junctions,
IEICE Technocal Report, 108, 11-16.
Noumaru, J., et al. including Kawai, J. A., Schubert, K., Yagi,
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Network III (STN-III): more effective, more operation-oriented,
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Ohishi, N., Yoshizawa, M., Nishikawa, J., Murakami, N.,
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2008, Recent progress at the MIRA: development of fringe
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Ohnishi, K., Hosokawa, M., Fukushima, T.: 2008, Macro Lens
Toward the Galactic Center , Mapping the Galaxy and Nearby
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Ohnishi, N., Iwakami, W., Sugai, K., Kotake, K., Yamada, S.:
2008, Roles of shock instability interacting with neutrino
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Ohta, K., Yabe, K., Iwata, I., Sawicki, M., Akiyama, M., Tamura,N., Aoki, K.: 2008, Evolution of Star-forming Galaxies seenfrom Lyman-break Galaxies at z ˜ 5, Panoramic Views ofGalaxy Formation and Evolution (ASP Conf. Ser. 399), Eds. T.
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Systematic study for the shell effect in the fission fragment
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Omiya, M., et al. including Izumiura, H., Yoshida, M., Kambe, E.:076

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2008, A Korea-Japan planet search program: Current status anddiscovery of a brown dwarf candidate, Proc. of the IAU Symp.
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Onaka, T., et al. including Ita, Y., Tamura, M.: 2009, AKARI
Large Area Survey of the Large Magellanic Cloud, The
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Sawada, T., Koda, J., Handa, T., Sugimoto, M., Hasegawa, T.:2008, NRO/CSO/ASTE Galactic Plane CO Survey, Mapping the
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Spurny, P., et al. including Watanabe, J.: 2008, Commission 22:
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Watanabe, M., Oya, S., Hayano, Y., Takami, H., Hattori,
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Yoshida, M., Yanagisawa, K., Kuroda, D., Shimizu, Y.,
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- Nuclei in the Cosmos - X, Eds. H. Schatz, et al., 22.
Yoshida, T., Umeda, H., Nomoto, K.: 2008, ν-Process in Population
III Core-Collapse Supernovae, Proc. of the Int. Symp. on
Nuclear Astrophysics - Nuclei in the Cosmos - X, Eds. H.
Schatz, et al., 127.
Yoshikawa, T., Akiyama, M., Ichikawa, T., Kajisawa, M.,
Konishi, M., Yamada, T., Suzuki, R., Tokoku, C., Uchimoto, Y.
K., Tanaka, I., Omata, K., Nishimura, T.: 2008, Rest-Optical
Spectroscopic Properties of Luminous Infrared Galaxies at z˜
2, Panoramic Views of Galaxy Formation and Evolution (ASP
Conf. Ser. 399), Eds. T. Kodama, T. Yamada, K. Aoki, 214.
Zubko, N., Baba, N., Murakami, N.: 2008, Polarization analysis asa means of detecting exoplanets and measuring their objective
spectra, SPIE 7010, Eds. Jr. J. M., Oschmann, M. W. M., deGraauw, H. A. MacEwen, 70101P-1.

5. Publications in English
Kato, D., et al. including Nakaya, H., Tamura, M., Ita, Y.: 2008,
IRSF Magellanic Clouds Point Source Catalog (Kato+ 2007),
VizieR Online Data Catalog.
Kodama, T., Yamada, T., Aoki, K.: 2008, Panoramic Views ofGalaxy Formation and Evolution, ASP Conf. Ser. 399, USA.
Meyer, M. R., et al. including Kandori, R.: 2008, Star Formationin NGC 2023, NGC 2024, and Southern L1630, in "Handbookof Star Forming Regions, Vol. I The Northern Sky", ASP, USA.
Mortier, A. M., et al. including Sekiguchi, K.: 2008, Short Title(Mortier+, 2005), VizieR Online Data Catalog.
Takeuchi, T., Wyatt, M., Nakamura, A. M., Michel, P., Abe, S., Li,
A., Mann, I., Ishiguro, M., Ueno, M., Jewitt, D., Itoh, Y.: 2008,
Small Bodies in Planetary Systems (Lecture Notes in Physics),
Springer, Berlin / Heidelberg.

6. Conference Presentations
Agata, H.: 2008, “You are also Galileo” Project, Int. Workshop on
New Astronomical Facilities in Peru, (Instituto Geofisico delPeru, Lima, Peru, July 1, 2008).
Agata, H.: 2008, “You are also Galileo” Project - Produced by
the IYA Japan, The 10th Asian-Pacific Regional IAU Meeting,(Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Agata, H.: 2008, Astronomical Education and Public Outreach inJapan, Int. Workshop on New Astronomical Facilities in Peru,(Instituto Geofisico del Peru, Lima, Peru, July 1st, 2008).
Agata, H.: 2008, Introduction to the New Public Understandingof Research Experiments in Japan, The 10th Asian-PacificRegional IAU Meeting, (Kunming, Yunnan, Nanjing, China,
Aug. 3-6, 2008).
Agata, H.: 2008, Science Education Goals:Japanese’s Perspective,
Building New Global Science Education Systems for a New World,(The University of Hong Kong, Hong Kong, May 7, 2008).
Agata, H.: 2008, Telescopes for children, Building New Global
Science Education Systems for a New World, (The Universityof Hong Kong, Hong Kong, May 7, 2008).
Agata, H.: 2009, “You are also Galileo” Project - Produced by the
IYA Japan, Meeting on Developing a Global Science Education

080

II Publications, Presentations

Network, (Institute of Astrophysics, Paris, France, Jan. 27, 2009).
Agata, H.: 2009, Introduction to the New Public Understandingof Research Experiments in Japan, Meeting on Developing a
Global Science Education Network, (Institute of Astrophysics,
Paris, France, Jan. 27, 2009).
Akitaya, H., Ikeda, Y., Kawabata, K. S., Matsuda, K., Okazaki, A.,
Seki, M.: 2008, Echelle spectro-polarimetry of T Tauri Star RY
Tauri, Astronomical Polarimetry 2008, (La Malbaie, Quebec,
Canada, Jul. 6-11, 2008).
Aoki, W.: 2009, High resolution optical spectroscopy with the
Subaru Telescope, SPECTRA 2009: Conf. on Spectroscopy andits Applications, (Lima, Peru, Mar 9-13, 2009).
Arai, K., Miyakawa, O.: 2009, Status of Japanese Projects, March
LSC-Virgo Meeting, (Arcadia, California, USA, Mar 16-19, 2009).
Arai, K.: 2009, Current status of Japanese gravitational wave
detectors, GWDAW 13, (San Juan, Puerto Rico, Jan. 19-22, 2009).
Arai, T., Yamamoto, Y., Okada, T., Kato, M.: 2009, Lessons
Learned in Onboard Software Processing of XRS-Kaguya, 40th
Lunar and Planetary Science Conf., (The Woodlands, Texas,
USA, Mar. 23-27, 2009).
Araki, H., Ishihara, Y., Noda, H., Goossens, S., Tazawa, S.,
Kawano, N., Sasaki, S., Oberst, J., Shum, C. K.: 2008, A New
Lunar Topographic Map of the Moon by KAGUYA-LALT: The
First Precise Topography of the Polar Regions, AGU 2008 Fall
Meeting, (San Francisco, CA, USA, Dec. 15-19, 2008).
Araki, H., Ishihara, Y., Noda, H., Goossens, S., Tazawa, S.,
Kawano, N., Sasaki, S., Oberst, J., Shum, C. K.: 2009, Lunar
Global Topographic Map Derived from the LALT Altimetry:
The first year’s results, The 3rd KAGUYA (SELENE) Science
Working Team Meeting, (Tamachi, Japan, Jan. 14-15, 2009).
Araki, H., Sasaki, S., Noda, H., Tazawa, S., Ishihara, Y., Migita,
E., Kawano, N., Kamiya, I., Oberst, J.: 2008, Global Lunar
Topography by LALT (Laser Altimeter) on Board Kaguya, 71nd
Annual Meeting of the Meteoritical Society, (Matsue, Japan,
Jul. 28-Apr. 1, 2008).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S.,
Kawano, N., Sasaki, S., Kamiya, I., Otake, H., Oberst, J.,
Shum, C. K.: 2009, The First Lunar Global Topography by
the Laser Altimeter (LALT) on the KAGUYA (SELENE)
Main Orbiter, 1st Int. Conf. on Space Optical Systems andApplications, (Tokyo, Japan, Feb. 4-6, 2009).
Araki, H., Tazawa, S., Noda, H., Ishihara, Y., Goossens, S.,
Kawano, N., Sasaki, S., Kamiya, I., Otake, H., Oberst, J.,
Shum, C. K.: 2009, The Lunar Global Topography by the Laser
Altimeter (LALT) onboard KAGUYA (SELENE): Results fromOne Year Observation, 40th Lunar and Planetary Science Conf.,(The Woodlands, Texas, USA, Mar. 23-27, 2009).
Araki, H., Tazawa, S., Noda, H., Migita, E., Ishihara, Y., Kawano,N., Sasaki, S., Tsubokawa, T., Kamiya I., Kunimori, H.,
Oberst, J., Shum, C. K.: 2008, Initial Results of the Lunar Laser
Topography by KAGUYA-LALT Mission, AOGS 5th Annual
Meeting, (Busan, Korea, June 16-20, 2008).
Araki, H., Tazawa, S., Noda, H., Migita, E., Kamiya, I., Kawano,N., Sasaki, S.: 2008, Preliminary results of the Lunar topography by Kaguya-LALT misssion, The 26th Int. Symp. on SpaceTechnology and Science, (Hamamatsu, Japan, June 1-8, 2008).

Asayama, S., Kawashima, S., Iwashita, H., Inata, M., Obuchi, Y.,
Suzuki, T., Wada, T.: 2008, Design and Development of ALMABand 4 Cartridge Receiver, 19th Int. Symp. on Space Terahertz
Technology, (Groningen, Netherlands, Apr. 28-30, 2008).
Bukovski, M. A., Shitov, S. V., Uvarov, A. V., Koryukin, O. V.,
Uzawa, Y.: 2008, SIS mixers for ALMA band-10: comparison of
epitaxial and hybrid circuits, 19th Int. Symp. on Space Terahertz
Technology, (Groningen, Netherlands, Apr. 28-30, 2008).
Candotti, M., et al.: 2008, Status of the ALMA band 10 frontend optics development, The 9th Workshop on SMW Rx
Technologies in Eastern Asia, (Taipei, Taiwan, Nov. 18-20, 2008).
Candotti, M., Uzawa, Y., Fujii, Y., Shitov, S., Kaneko, K.: 2008,
Electromagnetic characterization of direct machined corrugatedhorn for the ALMA band 10 receiver, 2008 Int. Symp. on
Antenna and Propagation, (Taipei, Taiwan, Oct. 27-30, 2008).
Candotti, M., Uzawa, Y., Shitov, S. V., Fujii, Y., Kaneko, K.:
2008, Tolerance analysis of the ALMA band 10 front-end optics,
19th Int. Symp. on Space Terahertz Technology, (Groningen,
Netherlands, Apr. 28-30, 2008).
Endo, A., Noguchi, T., Kroug, M., Shitov, S. V., Shan, W., Tamura,T., Kojima, T., Uzawa, Y., Sakai, T., Inoue, H., Kohno, K.:
2008, A novel THz SIS mixer with a NbTiN-ground plane and
SIS micro-trilayers directly grown on a quartz substrate, Applied
Superconductivity Conf., (Chicago, USA, Aug. 17-22, 2008).
Endo, A., Noguchi, T., Kroug, M., Shitov, S. V., Shan, W.,
Tamura, T., Kojima, T., Uzawa, Y., Sakai, T., Inoue, H.,
Muraoka, K., Kohno, K.: 2008, A novel THz SIS mixer witha NbTiN-groundplane and SIS micro-trilayers directly grown
on a quartz substrate, 19th Int. Symp. on Space Terahertz
Technology, (Groningen, Netherlands, Apr. 28-30, 2008).
Fujii, M.: 2008, Trojan Stars in the Galactic Center, Back to the
Galaxy II, (Santa Barbara, USA, Sep. 29-Oct. 3, 2008).
Fujii, M.: 2009, N-body Simulation of Star Clusters near the
Galactic Center using BRIDGE, Formation and Evolution of
Globular Clusters, (Santa Barbara, USA, Jan. 12-16, 2009).
Fujii, Y., et al.: 2008, Measurement system of ALMA/Band10
cartridge, The 9th Workshop on SMW Rx Technologies in
Eastern Asia, (Taipei, Taiwan, Nov. 18-20, 2008).
Fujimura, D.: 2008, Discovery of Magneto-Hydrodynamic Waves
at Solar Photosphere, The 2nd Hinode Science Meeting –Beyond Discovery Toward Understanding, (Boulder, Colorado,
USA, Sep. 29-Oct. 3, 2008).
Fujiwara, M., Sasaki, M., Nagata, H., Matsuo, H.: 2008, Opticalcontrol of low frequency noise behavior in cryogenic GaAs
junction field effect transistor, 8th Int. Workshop on Low
Temperature Electronics, (Jena/Gabelbach, Germany, Jun.
22-25, 2008).
Furusho, R., Arai, A., Uemura, M., Kawabata, K. S., Sasada, M.,
Yamashita, T., Ohsugi, S., Sato, S., Kino, M., Kato, H.,
Watanabe, J.: 2008, Polarimetry of 17P/Holmes, AOGS 5th
Annual Meeting, (Busan, Korea, June 16-20, 2008).
Goossens, S., Matsumoto, K., Ishihara, Y., Liu, Q., Kikuchi, F.,
Noda, H., Iwata, T., Namiki, N., Hanada, H.: 2008, Analysisof tracking data and results from Kaguya (SELENE) satellites
for lunar gravity field estimation, AGU 2008 Fall Meeting, (SanFrancisco, CA, USA, Dec. 15-19, 2008).

Goossens, S., Matsumoto, K., Ishihara, Y., Liu, Q., Kikuchi, F.,
Noda, H., Namiki, N., Iwata, T.: 2008, Orbit determination andquality assessment using SELENE tracking data and results,
37th COSPAR Scientific Assembly, (Montreal, Canada, Jul.
13-20, 2008).
Goossens, S., Matsumoto, K., Noda, H.: 2009, Precise orbit determination of the main satel; lite of Kaguya, The 3rd KAGUYA(SELENE) Science Working Team Meeting, (Tamachi, Japan,
Jan. 14-15, 2009).
Guyon, O.: 2008, Adaptive Optics System Design, CfAO summer
school, (Santa Cruz, CA, USA, Aug. 4-8, 2008).
Guyon, O.: 2008, The Pupil mapping Exoplanet Coronagraphic
Observer (PECO), AIAA meeting, (San Diego, CA, USA, Sept.
9-11, 2008).
Guyon, O.: 2009, Coronagraphy review, Exoplanets and Disks:
Their Formation and Diversity, (Kona, Hawaii, USA, Mar. 9-11,2009).
Guyon, O.: 2009, Imaging and Characterizing the Habitable Zonesof nearby Planetary Systems with the Pupil mapping Exoplanet
Coronagraphic Observer (PECO), AAS meeting, (Long Beach,
CA, USA, Jan. 5-8, 2009).
Guyon, O.: 2009, Key technologies for the Pupil mapping
Exoplanet Coronagraphic Observer (PECO), AAS meeting,(Long Beach, CA, USA, Jan. 5-8, 2009).
Guyon, O.: 2009, The Pupil mapping Exoplanet Coronagraphic
Observer (PECO), Beyond JWST, (Baltimore, Maryland, USA,
Mar. 26-27, 2009).
Hagiwara, Y.: 2008, AGN Maser, Scientific Symp.: Activity in
Extragalactic Objects, (MPIfR, Bonn, Germany, Oct. 16-17, 2008).
Hagiwara, Y.: 2008, Water Megamaser Observations with SpaceVLBI, Radio Universe at Ultimate Angular Resolution, (AstroSpace Center, Moscow, Russia, Oct. 20-24, 2008).
Hagiwara, Y.: 2009, VSOP-2 Key Science Proposal, Korean VLBI
Network Internal Workshop, (Ringberg, Germany, Feb. 13, 2009).
Hamana, T.: 2008, HSC weak lensing survey, Taiwan-Japan
Subaru-HSC Science/Survey Mini Workshop, (ASIAA, Taipei,
Taiwan, Dec. 22, 2008).
Hamana, T.: 2008, Subaru weak lensing survey and Hyper
SuprimeCam, DENET summer school: Dark Energy in the
Universe, (Aomori, Japan, Sep. 1-4, 2008).
Hamana, T.: 2009, Reports from activities so far ongoing in Japan,
Japan-Princeton-Taiwan HSC Workshop, (Mitaka, Japan, Jan.
17-20, 2009).
Hanada, H., et al. including Kawano, N., Sasaki, S., Matsumoto,K., Noda, H., Tsuruta, S., Asari, K., Ishikawa, T., Kikuchi, F.,
Liu, Q., Goossens, S., Ishihara, Y.: 2008, Exploration of Lunar
Gravity by VLBI Observations of SELENE (KAGUYA), The
26th Int. Symp. on Space Technology and Science, (Hamamatsu,
Japan, June 1-8, 2008).
Hanada, H., et al. including Liu, Q., Kikuchi, F., Matsumoto, K.,
Ishihara, Y., Kawano, N., Asari, K., Noda, H., Ishikawa, T.,
Tsuruta, S., Goossens, S., Sasaki, S.: 2008, VLBI Observation of
Okina and Ouna in Kaguya (SELENE) for Improvement of Orbit
Determination and Lunar Gravity Field Model, 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Hanada, H., Iwata, T., Sasaki, S., Kawano, N., Araki, H., Noda, H.:

II Publications, Presentations081

2008, Lunar Observatory in a future Lunar Mission, 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Hanada, H., VRAD team: 2009, VRAD: Scientific Results andCurrent Status, The 3rd KAGUYA (SELENE) Science Working
Team Meeting, (Tamachi, Japan, Jan. 14-15, 2009).
Hanaoka, Y.: 2008, Spectropolarimetry with the Hide DomelessSolar Telescope, 37th COSPAR Scientific Assembly, (Montreal,
Canada, Jul. 13-20, 2008).
Hanaoka, Y.: 2008, Spectropolarimetry with the Hide DomelessSolar Telescope, Int. Workshop of 2008 Solar Total Eclipse,(Jiuquan, Gansu, China, Jul. 28-Aug. 5, 2008).
Hanayama, H.: 2008, Biermann Mechanism and Seed Magnetic
Fields from Primordial Supernova Remnant, East Asian Young
Astronomers Meeting 2008, (Jiayuguan, China, Sep. 27-Aug. 1,
2008).
Hanayama, H.: 2008, Biermann Mechanism in Primordial Supernova Remnant and Seed Magnetic Fields, New Vision 400,
(Beijing, China, Oct. 12-15, 2008).
Hara, H.: 2008, Coronal Plasma Motions in Active Region Loops
Observed with Hinode EIS, The 2nd Hinode Science Meeting Beyond Discovery Toward Understanding, (Boulder, Colorado,
USA, Sep. 29-Oct. 3, 2008).
Hara, H.: 2008, Coronal Plasma Motions near Footpoints ofActive Region Loops, Int. Workshop of 2008 Solar Total
Eclipse, (Jiuquan, Gansu, China, Jul. 28-Aug. 5, 2008).
Hara, H.: 2008, Coronal Plasma Motions near Footpoints of Active
Region Loops Revealed from Spectroscopic Observations with
it Hinode EIS, 37th COSPAR Scientific Assembly, (Montreal,
Canada, Jul. 13-20, 2008).
Hara, H.: 2008, Differential Rotation Rate of the Solar Corona
Estimated From X-Ray Bright Points, 37th COSPAR Scientific
Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Hara, H.: 2008, Plan-A Mission description, Solar-C Science
Definition Meeting, (Sagamihara, Japan, Nov. 17-21, 2008).
Harada, Y.: 2008, True Polar Wander Due to Surface Mass Loading on Mars: Implication to Evolution of the Tharsis Province,
AOGS 5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Harada, Y.: 2008, True Polar Wander Due to Surface Mass
Loading on Mars: Implication to Evolution of the Tharsis
Province, AGU 2008 Fall Meeting, (San Francisco, CA, USA,
Dec. 15-19, 2008).
Harada, Y.: 2008, True Polar Wander Due to Surface Mass Loading: Interaction between Rotation and Deformation throughPole Tide, EGU, (Vienna, Austria, Apr. 13-18, 2008).
Hasegawa, T., Fukuda, Y., Yamamoto, K., Nakaegawa, T., Tamura,Y.: 2008, 2006 Australian drought detected by GRACE, IAG
Int. Symp. on Gravity, Geoid and Earth Observation 2008,(Technical University of Grete, Greece, June 23-27, 2008).
Hasegawa, T.: 2008, ALMA Construction Status and Operation
Planning, The 10th Asian-Pacific Regional IAU Meeting,(Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Hashimoto, J., Tamura, M., Kandori, R., Kusakabe, N.,
Nakajima, Y., Kurita, M., Nagata, T., Nagayama, T., Hough, J.,
Chrysostomou, A.: 2008, Wide-Field Near-Infrared Polarimetryof Star Forming Regions: A Nest of Infrared Reflection Nebulaein the NGC 6334 Region, Astronomical Polarimetry 2008, (La082

II Publications, Presentations

Malbaie, Quebec, Canada, Jul. 6-11, 2008).
Hashimoto, J.: 2009, Polarimetry for the Disks around Young
Brown Dwarfs, Exoplanets and Disks: Their Formation andDiversity, (Kona, Hawaii, USA, Mar. 9-11, 2009).
Hashimoto, T., Watanabe, J., Sato, M.: 2008, Optical Observationof Northern Toroidal Source, AOGS 5th Annual Meeting,(Busan, Korea, June 16-20, 2008).
Hatsutori, Y., Nakasuka, S.: 2008, A Study on Vibration Isolator
for Reaction Wheel Assembly, The 26th Int. Symp. on SpaceTechnology and Science, (Hamamatsu, Japan, June 1-8, 2008).
Hatsutori, Y., Suganuma, M., Kobayashi, Y., Gouda, N., Yano,
T., Yamada, Y., Yamauchi, M.: 2008, A Very Small Astrometry
Satellite, Nano-JASMINE: Its Telescope and Mission Goal, The
26th Int. Symp. on Space Technology and Science, (Hamamatsu,
Japan, June 1-8, 2008).
Hibi, Y., Matsuo, H., Arai, H., Nagata, H., Ikeda, H., Fujiwara,
M.: 2008, The cryogenic multiplexer and shift register for
submillimeter-wave digital camera, 8th Int. Workshop on Low
Temperature Electronics, (Jena/Gabelbach, Germany, Jun.
22-25, 2008).
Higuchi, A.: 2008, Evolution of the Oort cloud by stellar encounters,
AOGS 5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Higuchi, A.: 2008, Formation of the Oort cloud by stellar
encounters, EPSC 2008: European Planetary Science Congress,(Münster, Germany, Sep. 21-26, 2008).
Hirai, T., Ohashi, H., Sasaki, S., Shibata, H., Nogami, K., Iwai,
T.: 2008, Development of a Light-Weight, Large Area In-Situ
Impact Ionization Dust/Debris Detector, AOGS 5th Annual
Meeting, (Busan, Korea, June 16-20, 2008).
Hirata, N., Abe, S., Ishiguro, M., Kitazato, K., Nakamura, R.,
Miyamoto, H., Demura, H., Abe, M., Sasaki, S.: 2008, Geologic
Processes on the Surface of a Small Asteroid Itokawa, 71nd
Annual Meeting of the Meteoritical Society, (Matsue, Japan,
Jul. 28-Apr. 1, 2008).
Hara, H.: 2009, Magnetic Activity on the Sun Revealed byHinode, US Japan Mini-Workshop on Magnetic Reconnection,(Princeton, USA, Mar. 2, 2009).
Hiroi, T., Abe, M., Nimura, T., Kitazato, K., Abe, S., Takagi, Y.,
Sasaki, S., Ishiguro, M.: 2008, Danger in Interpreting the2-Micron Band of Reflectance Spectra of Small Asteroids: A
Lesson from Hayabusa/NIRS Data of Itokawa, 71nd Annual
Meeting of the Meteoritical Society, (Matsue, Japan, Jul.
28-Apr. 1, 2008).
Hirota, T.: 2008, Proposal Writing and Observation Planning, 2nd
Asian Radio Astronomy School, (ASIAA, Taipei, Taiwan, Aug.
18-22, 2008).
Hirota, T.: 2008, Relationship between the H 2O and CH 3OH
masers, East Asia VLBI Mini-Workshop; Science of themethanol maser, (Shanghai, China, Nov. 25-26, 2008).
Hirota, T.: 2009, Observational Studies on Dark Cloud Coresin the Early Evolutionary Stage, 2nd Tokyo-NRO Workshop
Chemical Diagnostics of Star and Planet Formation, (Univ. ofTokyo, Tokyo, Japan, Mar. 5-6, 2009).
Hirota, T.: 2009, Report on the Second Asian Radio Astronomy
School, 2009 East Asia VLBI Workshop, (Ewha Woman's
University, Seoul, Korea, Mar. 18-20, 2009).

Hong, S. S., Pyo, J., Ueno, M., Kwon, S. M., Ishiguro, M., Usui,
F., Ootsubo, T., Ishihara, D., Mukai, T.: 2009, Modeling of theInterplanetary Dust Cloud, AKARI Int. Conf., (Univ. of Tokyo,
Tokyo, Japan, Feb. 16-19, 2009).
Honma, M.: 2008, Methanol Maser Observations with VERA,
East Asia VLBI Mini-Workshop; Science of the methanol
maser, (Shanghai, China, Nov. 25-26, 2008).
Honma, M.: 2008, Observations of AGB stars with VERA, AGB
stars and related phenomena, (Mitaka, Japan, Nov. 12-14, 2009).
Hosokawa, T.: 2008, Evolution of Massive Protostars with HighAccretion Rates, Early Phase of Starformation 2008, (Ringberg,
Germany, July 28-Aug.1, 2008).
Imada, S.: 2008, Solar wind acceleration, Solar-C Science
Definition Meeting, (Sagamihara, Japan, Nov. 17-21, 2008).
Imada, S.: 2008, Non-Gaussian line profiles associated with flows
in a large solar flare, The 2nd Hinode Science Meeting - Beyond
Discovery Toward Understanding, (Boulder, Colorado, USA,
Sep. 29-Oct. 3, 2008).
Imamura, T., Iwata, T., Yamamoto, Z., Mochizuki, N., Kono,
Y., Matsumoto, K., Liu, Q., Noda, H., Hanada, H., Oyama,
K., Futaana, Y., Nabatov, A., Saitou, A., Ando, H.: 2009,
Observation of the Lunar Ionosphere with SELENE Radio
Science Experiment, The 3rd KAGUYA (SELENE) Science
Working Team Meeting, (Tamachi, Japan, Jan. 14-15, 2009).
Imamura, T., Iwata, T., Yamamoto, Z., Mochizuki, N., Kono, Y.,
Matsumoto, K., Liu, Q., Noda, H., Hanada, H., Oyama, K.,
Futaana, Y., Nabatov, A., Saitou, A., Andou, H.: 2008, Studying
the Lunar Ionosphere with SELENE Radio Science Experiment,
AGU 2008 Fall Meeting, (San Francisco, CA, USA, Dec.
15-19, 2008).
Imamura, T., Iwata, T., Yamamoto, Z., Oyama, K.-I., Nabatov,
A., Kono, Y., Matsumoto, K., Liu, Q., Noda, H., Hanada,
H., Futaana, Y., Saito, A.: 2008, Initial Results of the Lunar
Ionosphere Observation with SELENE Radio Science, AOGS
5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Imamura, T., Oyama, K., Iwata, T., Kono, Y., Matsumoto, K.,
Liu, Q., Noda, H., Futaana, Y., Nabatov, A.: 2008, Studying the
lunar ionosphere with the SELENE radio science experiment,
The 26th Int. Symp. on Space Technology and Science,(Hamamatsu, Japan, June 1-8, 2008).
Imanishi, M.: 2008, Luminous buried AGNs in luminous IR
galaxies and the origin of galaxy downsizing, The Central
Kiloparsec Active Galactic Nuclei and Their Hosts, (Ierapetra,
Crete, Greece, June 4-6, 2008).
Imanishi, M.: 2008, Luminous Buried AGNs in the local universe (Subaru, Spitzer, AKARI, NRO), The Starburst-AGN
Connection Conf., (Shanghai, China, Oct. 27-31, 2008).
Imanishi, M.: 2008, Molecular gas diagnostics of nearby LIRGs
with ASTE WHSF, ASTE Science Workshop, (Mitaka, Japan,
Dec. 11-12, 2008).
Imanishi, M.: 2008, Nobeyama millimeter interferometric 3D
observations of high density molecular gas in luminous infrared
galaxies, Gas and Stars in Galaxies - A Multi-Wavelength 3D
Perspective, (Garching, Germany, June 10-13, 2008).
Imanishi, M.: 2009, Astronomical Science Results of the Subaru
Telescope: Infrared Spectroscopy, SPECTRA 2009: Conf. on

Spectroscopy and its Applications, (Lima, Peru, Mar 9-13, 2009).
Imanishi, M.: 2009, Luminous buried AGNs in nearby ultraluminous infrared galaxies, AKARI Int. Conf., (Univ. of Tokyo,
Tokyo, Japan, Feb. 16-19, 2009).
Imanishi, Y., Tamura, Y., Ikeda, H., Okubo, S.: 2008, Permanent
gravity changes caused by The 2007 Noto Hantou Earthquake
and The 2007 Niigataken Chuetsu-oki Earthquake recorded bysuperconducting gravimeters, Earth Tides Symp. 2008, IAG,
(Jena, Germany, Sep. 1-5, 2008).
Inamori, T., Sako, N., Casey, L., Hatsutori, Y., Nakasuka, S.: 2008,
Method to control nano-satellite attitude using star blurred andskewed images, The 26th Int. Symp. on Space Technology and
Science, (Hamamatsu, Japan, June 1-8, 2008).
Inoue, H., Noguchi, T.: 2008, Noise source using SIS junction,
The 9th Workshop on SMW Rx Technologies in Eastern Asia,(Taipei, Taiwan, Nov. 18-20, 2008).
Inoue, S., Magara, T., Takahashi, K., Miyagoshi, T.: 2008, Numerical Reconstruction of Sigmoidal Structure Associated with
Flux Emergence of the Sun, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Inoue, T.: 2008, Turbulence and Magnetic Field Amplification inSupernova Remunant, Astrophysical Jet, (Nagoya, Japan, Oct. 4,2008).
Ishiguro, M., Sarugaku, Y., Ueno, M.: 2008, Interplanetary Dust
Particles from Jupiter-Family Comets, AOGS 5th Annual
Meeting, (Busan, Korea, June 16-20, 2008).
Ishiguro, M., Sarugaku, Y., Urakawa, S., Usui, F., Ueno, M.:
2008, Optical Observations of Dust Trails and the Meteoric
Connection, AOGS 5th Annual Meeting, (Busan, Korea, June
16-20, 2008).
Ishiguro, M., Usui, F., Sarugaku, Y., Ishihara, D., Ootsubo, T.,
Ueno, M.: 2009, Optical and Infrared Observations of Comet
4P/Faye in 2006 Return, AKARI Int. Conf., (Univ. of Tokyo,
Tokyo, Japan, Feb. 16-19, 2009).
Ishihara, Y., Araki, H., Noda, H., Tazawa, S., Migita, E., Kawano,N., Sasaki, S.: 2008, A preliminary lunar topographic model by
KAGUYA/LALT, AOGS 5th Annual Meeting, (Busan, Korea,
June 16-20, 2008).
Ishihara, Y., Goossens, S., Matsumoto, K., Namiki, N., Noda,
H., Araki, H., Hanada, H., Iwata, T., Tazawa, S., Sasaki, S.,
RSAT/VRAD Mission Team, LALT Mission Team: 2009, Developing the Lunar Moho Depth Model from Selenodetic Data
of SELENE (Kaguya), The 3rd KAGUYA (SELENE) Science
Working Team Meeting, (Tamachi, Japan, Jan. 14-15, 2009).
Ishihara, Y., Matsumoto, K., Goossens, S., Araki, H., Namiki, N.,
Hanada, H., Iwata, T., Noda, H., Sasaki, S.: 2008, Localized
gravity/topography correlation spectra on the moon, 71nd
Annual Meeting of the Meteoritical Society, (Matsue, Japan,
Jul. 28-Apr. 1, 2008).
Ishihara, Y., Namiki, N., Hanada, H., Araki, H., Iwata, T.,
Matsumoto, K., Noda, H., Goossens, S., Tazawa, S., Sasaki,S., Ogawa, M., RSAT/VRAD team, LALT team: 2008, Current
Results of Selenodetic Observation of KAGUYA, 7th General
Assemby of Asian Seismological Commission and Seismological Society of Japan, 2008 Fall meeting, (Tsukuba,
Japan, Nov. 24-27, 2008).

II Publications, Presentations083

Ishihara, Y., Namiki, N., Sugita, S., Matsumoto, K., Goossens, S.,
Araki, H., Noda, H., Sasaki, S., Iwata, T., Hanada, H.:
2009, Localized gravity/topography correlation and admittancespectra on the Moon, 40th Lunar and Planetary Science Conf.,(The Woodlands, Texas, USA, Mar. 23-27, 2009).
Ishihara, Y., Noda, H., Sasaki, S., Migita, E., Araki, H., Goossens,S., Tazawa, S., Kawano, N.: 2008, Measurement of Lunar
Impact Structures and Ridge Features from KAGUYA Altimetry(LALT) Data, AGU 2008 Fall Meeting, (San Francisco, CA,
USA, Dec. 15-19, 2008).
Ishikawa, R., Tsuneta, S.: 2008, Statistical properties of transienthorizontal magnetic fields, Magnetic Coupling between theInterior and Atmosphere of the Sun, (Bangalore, India, Dec.
2-5, 2008).
Ishikawa, R.: 2008, New insights from Hinode-VTT He10830
observations, Solar-C Science Definition Meeting, (Sagamihara,
Japan, Nov. 17-21, 2008).
Ishikawa, R.: 2008, Properties of transient horizontal magnetic
field and its implication to a local dynamo process, SPD/AGU
Meeting, (Fort Lauderdale, Florida, USA, May 27-30, 2008).
Ishikawa, R.: 2008, Statistical properties of transient horizontal
magnetic fields, The 2nd Hinode Science Meeting - Beyond
Discovery Toward Understanding, (Boulder, Colorado, USA,
Sep. 29-Oct. 3, 2008).
Ita, Y.: 2008, AKARI IRC survey of the Large Magellanic Clouds,
IAU Symp. 256, The Magellanic System: Stars, Gas, andGalaxies, (University of Keele, UK, Jul. 28-Aug. 1, 2008).
Ita, Y.: 2008, IRSF/SIRIUS variable star survey in the Magellanic
Clouds, AGB stars and related phenomena, (Mitaka, Japan,
Nov. 12-14, 2009).
Ito, T., Malhotra, R.: 2008, Asymmetric Impacts of the Near-EarthAsteroids on the Moon, Asteroids, Comets, Meteors - ACM
2008, (Baltimore, Maryland, USA, Jul. 13-18, 2008).
Ito, T., Malhotra, R.: 2008, Asymmetric Impacts of the Near-EarthAsteroids on the Moon, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Ito, T., Malhotra, R.: 2009, Asymmetric cratering on the Moon andvery slow NEAs, Subaru Users Meeting 2008, (Mitaka, Japan,
Jan. 14-16, 2009).
Itoh, S., Agata, H., Nagai, T., Nakayama, H., Naito, S., Hirai, A.:
2008, What We Are Aiming at on “Science Culture Promotion Unit
Through Astronomical Images”, 2008 Int. Planetarium Society
Conf., (The Adler Planetarium, Chicago, USA, July 1, 2008).
Itoh, S., Agata, H., Nagai, T., Nakayama, H., Naito, S., Hirai, A.:
2009, What is our “Science Culture Promotion Unit throughAstronomy Images?”, Int. Symp. for Immersive Science
Visualization 2009, (Mitaka, Japan, Mar. 22-23, 2009).
Iwata, I.: 2008, Ionizing Radiation from Galaxies at z=3 throughWide-field Narrow-band Imaging, Far Away: Light in the Young
Universe, 24th IAP Colloquim, (Paris, France, Jul. 7-11, 2008).
Iwata, T., Minamino, H., Namiki, N., Hanada, H., Noda, H.,
Matsumoto, K., Kawano, N., Tsuruta, S., Liu, Q., Kikuchi,F., Goossens, S., Ishihara, Y., Takano, T.: 2008, On-orbit
Properties and Initial Results of SELENE / KAGUYA Small
Sub-satellites OKINA & OUNA for Lunar Gravity Mapping,
IAC2008, (Glasgow, UK, Sep. 29-Oct. 3, 2008).

084

II Publications, Presentations

Iwata, T., Minamino, H., Sasaki, T., Satoh, A., Takano, T., Namiki,N., Hanada, H., Noda, H., Kawano, N., Matsumoto, K.,
Tsuruta, S., Kikuchi, F.: 2008, Properties of SELENE Small
Satellites; Rstar (Okina) and Vstar (Ouna), The 26th Int. Symp.
on Space Technology and Science, (Hamamatsu, Japan, June
1-8, 2008).
Iwata, T., Namiki, N., Hanada, H., Matsumoto, K., Noda, H.,
Ogawa, M., Kawano, N., Asari, K., Tsuruta, S., Goossens, S.,
Liu, Q., Kikuchi, F., Ishihara, Y., Ishikawa, T., Sasaki, S.:
2008, The Global Mapping of Lunar Gravity Field by
KAGUYA, OKINA, and OUNA, 29th URSI General Assembly,(Chicago, USA, Aug. 9-16, 2008).
Iwata, T., Namiki, N., 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.:
2008, Initial Results of Global Lunar Gravity Field Mapping by
KAGUYA, OKINA, and OUNA, AOGS 5th Annual Meeting,(Busan, Korea, June 16-20, 2008).
Iwata, T., Noda, H., Misawa, H., Tsuchiya, F., Imai, K., Kondo,T., Kawano, N., Ujihara, H., Inoue, M.: 2008, A study on the
Observation System for the Lunar Low Frequency Astronomical
Observatory, 29th URSI General Assembly, (Chicago, USA,
Aug. 9-16, 2008).
Iye, M.: 2008, High redshift galaxy surveys, SPIE 2008 Astronomical
Instrumentation, (Marseilles, France, June 23-28, 2008).
Izumiura, H., Kambe, E., Sato, B., Salem, S. O., Yilmaz, M.,
Keskin, K., Yakut, K., Ozisik, V. Bikmaev, M.: 2008, Planet Search
Program at RTT150, Workshop on Exoplanet search Program
between China and Japan, (Mitaka, Japan, Apr. 23-25, 2008).
Izumiura, H., Nakaya, H., Otsuka, M., Kambe, E., Koyano, H.,
Nagayama, S., Yanagisawa, K., Yoshida, M.: 2008, Current
Status of the HIDES Mosaicked CCD camera, 3rd Workshop of
Astronomy with Precise Radial Velocity: Exoplanet Search andAstroseismology, (Jeju, Korea, Aug. 31-Sep. 5, 2008).
Izumiura, H., Nakaya, H., Otsuka, M., Kambe, E., Koyano, H.,
Nagayama, S., Yanagisawa, K., Yoshida, M.: 2008, Recent
Progress on the HIDES Mosaic CCD Camera, Workshop on
Exoplanet search Program between China and Japan, (Mitaka,
Japan, Apr. 23-25, 2008).
Izumiura, H., Yamamura, I., Ueta, T., Nakada, Y., Matsunaga, N.,
Ita, Y., Matsuura, M., Fukushi, H., Mito, H., Tanabe, T.: 2009,
Far -IR Imaging Survey of the Extended Dust Shells of Evolved
Stars with AKARI, AKARI Int. Conf., (Univ. of Tokyo, Tokyo,
Japan, Feb. 16-19, 2009).
Izumiura, H.: 2008, AKARI's View of the Extended Dust Shellsof Evolved Stars, AGB stars and related phenomena, (Mitaka,
Japan, Nov. 12-14, 2009).
Jeschke, E.: 2008, A Framework for the Subaru Telescope Observation Control System Processing Based on the Command
Design Pattern, SPIE 2008 Astronomical Instrumentation,(Marseilles, France, June 23-28, 2008).
Jeschke, E.: 2008, A Lightweight, Fault-Tolerant Middleware fora Subaru Telescope Second Generation Observation Control
System, SPIE 2008 Astronomical Instrumentation, (Marseilles,
France, June 23-28, 2008).
Kadono, T., Sugita, S., Ootsubo, T., Kawakita, H., Sako, S., Miyata,

T., Honda, M., Furusho, R., Watanabe, J.: 2008, Interpretation
on Deep Impact results, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Kajino, T.: 2009, Neutrino mass in cosmology and oscillationin supernova-nucleosynthesis, Int. Workshop on Frontiersin Theoretical Neutrino Physics, (University of Paris, Paris,
France, Mar. 16-19, 2009).
Kambe, E.: 2008, A Fiber-Link between Oakayam 1.89-m Telescopeand HIDES: Toward Higher Throughput and Radial Velociry
Measurement Precision, 3rd Workshop of Astronomy with
Precise Radial Velocity: Exoplanet Search and Astroseismology,(Jeju, Korea, Aug. 31-Sep. 5, 2008).
Kambe, E.: 2008, Comments on LAMOST-ET, Workshop on
Exoplanet search Program between China and Japan, (Mitaka,
Japan, Apr. 23-25, 2008).
Kambe, E.: 2008, Current Status of Software Development for
Okayama, Workshop on Exoplanet search Program between
China and Japan, (Mitaka, Japan, Apr. 23-25, 2008).
Kameya, O.: 2009, New Observation System of Mizusawa 10m
Radio Telescope, 2009 East Asia VLBI Workshop, (Ewha
Woman's University, Seoul, Korea, Mar. 18-20, 2009).
Kamikura, M., Naruse, M., Asayama, S., Satou, N., Shan, W.,
Sekimoto, Y.: 2008, Development of a 385-500 GHz Orthomode
Transducer (OMT), 19th Int. Symp. on Space Terahertz
Technology, (Groningen, Netherlands, Apr. 28-30, 2008).
Kamio, S.: 2008, Dynamics of solar transition region, Solar-C Science
Definition Meeting, (Sagamihara, Japan, Nov. 17-21, 2008).
Kamio, S.: 2008, The relation between explosive events and photospheric magnetic fields, 37th COSPAR Scientific Assembly,(Montreal, Canada, Jul. 13-20, 2008).
Kamohara, R.: 2008, VERA observations of SiO masers in thesymbiotic star R Aquarii, AGB stars and related phenomena,(Mitaka, Japan, Nov. 12-14, 2009).
Kandori, R., et al.: 2008, Gravitational Distortion of Magnetic
Field Lines in Prestellar Cores, IAU Symp. 259, Cosmic
Magnetic Fields: from Planets, to Stars and Galaxies, (CanaryIslands, Spain, Nov. 3-7, 2008).
Kandori, R., et al.: 2008, SEEDS Target Selection in Nearby Stars
Category, SEEDS Science Workshop, (Mitaka, Japan, Sep. 3-4,
2008).
Kandori, R., et al.: 2008, Subaru Exoplanet Survey, Science
with AO-fed instruments on Large Telescopes, (Dunk Island,
Australia, Apr. 6-11, 2008).
Kandori, R., et al.: 2009, SEEDS NS Category Report, Science
Workshop on Subaru Strategic Exploration of Exoplanets andDisks (SEEDS) 2, (Mitaka, Japan, Jan. 17, 2009).
Kandori, R., et al.: 2009, Selection of Nearby Star Targets for
the Subaru Strategic Exploration of Exoplanets and Disks,
Exoplanets and Disks: Their Formation and Diversity, (Kona,
Hawaii, USA, Mar. 9-11, 2009).
Kasuga, T., Jewitt, D.: 2008, Observations of 1999 YC and theBreakup of the Geminid Stream Parent, Future Ground based
Solar System Research: Synergies with Space Probesand Space
Telescope, (Isola d'Elba, Italy, Sep. 8-12, 2008).
Kasuga, T., Tsuboi, M., Ogawa, H., Ujihara, H.: 2008, GFRP
Waveguide Assembly for the Cooled Receiver on board theRadio Astronomical Satellite ASTRO-G (VSOP-2), 29th URSI
General Assembly, , (Chicago, USA, Aug. 9-16, 2008).
Kato, H., Furusho, R., Watanabe, J.: 2008, CCD Imaging of 17P/
Holmes after its Outburst, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Katsukawa, Y.: 2008, Chromospheric Activity at the Smallest
Scales Obtained by Hinode, The 2nd Hinode Science Meeting Beyond Discovery Toward Understanding, (Boulder, Colorado,
USA, Sep. 29-Oct. 3, 2008).
Katsukawa, Y.: 2008, Photospheric activities inside sunspots and theirrelationship with heating of the upper atmosphere, 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Katsukawa, Y.: 2008, Photospheric Signature of Penumbral
Microjets, SPD/AGU Meeting, (Fort Lauderdale, Florida, USA,May 27-30, 2008).
Katsukawa, Y.: 2008, Plan-B Mission description, Solar-C Science
Definition Meeting, (Sagamihara, Japan, Nov. 17-21, 2008).
Kawaguchi, N.: 2009, Possible Enginineering Support for Dual
Polarization and Ultra Wide Band Obs ervation with EAVN,
2009 East Asia VLBI Workshop, (Ewha Woman's University,
Seoul, Korea, Mar. 18-20, 2009).
Kawakatsu, N., Nagai, H., Kino, M.: 2008, Fate of baby radiogalaxies: Dead or Survive?, The 4th Workshop on Compact
Steep Spectrum and GHz-Peaked Spectrum Radio Sources,(Riccione, Italy, May 26-29, 2008).
Kawakatsu, N., Wada, K.: 2008, Co-evolution model of AGNs
and nuclear starburst, The Starburst-AGN Connection Conf.,(Shanghai, China, Oct. 27-31, 2008).
Kawamura, S.: 2008, 100MHz gravitational wave detection, Gravitational Wave Advanced Detector Workshop, (Elba, Italy, May
12-18, 2008).
Kawamura, S.: 2008, DECIGO, Gravitational Wave Advanced
Detector Workshop, (Elba, Italy, May 12-18, 2008).
Kawamura, S.: 2008, DECIGO, 1st Int. LISA-DECIGO Workshop,(Kanagawa, Japan, Nov. 12-13, 2008).
Kawamura, S.: 2008, Juggling Interferometer, LSC-Virgo Joint
Meeting, (Amsterdam, Netherlands, Sep. 22-25, 2008).
Kawamura, S.: 2009, Japanese Space Gravitational Wave Antenna
DECIGO, 1st Int. Conf. on Space Optical Systems andApplications, (Tokyo, Japan, Feb. 4-6, 2009).
Kikuchi, F., et al. including Liu, Q., Matsumoto, K., Ishihara, Y.,
Hanada, H., Kawano, N., Sasaki, S.: 2008, Differential Phase
Delay Estimation in VRAD mission of SELENE (KAGUYA),The 26th Int. Symp. on Space Technology and Science,(Hamamatsu, Japan, June 1-8, 2008).
Kikuchi, F., Liu, Q., Petrova, N., Noda, H., Matsumoto, K.,
Ishihara, Y., Goossens, S., Asari, K., Tsuruta, S., Ishikawa,T., Hanada, H., Iwata, T., Namiki, N., Kawano, N., Sasaki,
S.: 2008, VLBI observations in VRAD mission of Kaguya(SELENE), 37th COSPAR Scientific Assembly, (Montreal,
Canada, Jul. 13-20, 2008).
Kim, M.: 2009, SiO maser observations towards Orion-KL with
VERA, 2009 East Asia VLBI Workshop, (Ewha Woman's
University, Seoul, Korea, Mar. 18-20, 2009).
Kimura, K., et al. including Ogawa, H., Ujihara, H.: 2008,
STRO-G/VSOP-2 Off-Set Cassegrain Telescope, The 2008

II Publications, Presentations

085

IEEE Int. Symp. on Antennas and Propagation and the 2008
USNC/URSI National Radio Science meeting, (San Diego, CA,
USA, Jul. 5-12, 2008).
Kimura, K., Ogawa, H., Ujihara, H., Murata, Y., Tsuboi, M.,
Saito, H., Kasuga, T.: 2008, Development of the Optical System
for VSOP-2 Offset Cassegrain Antenna, 29th URSI General
Assembly, , (Chicago, USA, Aug. 9-16, 2008).
Kiuchi, H., Kawanishi, T., Yamada, M., Sakamoto, T., Tsuchiya,
M., Amagai, J., Izutsu, M.: 2008, Photonic Millimeter-wave
generation and transmission system applicable to the ALMARadio Telescopes, URSI: Int. Union of Radio Science, (Chicago,
USA, Aug. 7-16, 2008).
Kobayashi, H., Kawaguchi, N., Shibata, K.-M., Honma, M.,
Manabe, S., Tamura, Y., Kameya, O., Hirota, T., Jike, T.,
Imai, H., Omodaka, T.: 2008, Recent Results and Progress of
VERA, URSI: Int. Union of Radio Science, (Chicago, USA,
Aug. 7-16, 2008).
Kobayashi, H.: 2008, Direct distance measurements of Milky
way stars with VERA, The 10th Asian-Pacific Regional IAU
Meeting, (Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Kobayashi, H.: 2008, Recent activities of VERA and East AsisVLBI Network, 9th European VLBI Symp., (Bologna, Italy,
Sep. 22-26, 2008).
Kobayashi, H.: 2008, VLBI activities in Japan and East Asia, The
23rd Int. Technical Conf. on Circuits/Systems, Computers andCommunications, (Shimonoseki, Japan, July 6-9, 2008).
Kobayashi, H.: 2009, Status and future plan of East Asia VLBI
network, 2009 East Asia VLBI Workshop, (Ewha Woman's
University, Seoul, Korea, Mar. 18-20, 2009).
Kobayashi, H.: 2009, URSI Noth American General Assembly,
Japanese VLBI activities VERA and VSOP-2, (University ofBoldeaur, USA, Jan. 5-8, 2009).
Kobayashi, H.: 2009, VLBI in Eastern Asia and Pacific, 10th
Anniversary meeting of Int. VLBI Service, (University of
Bordeaux, France, Mar. 24, 2009).
Kobayashi, M.: 2009, LAE in Hierarchical Galaxy Formation,
Understanding Lyman-alpha Emitters, (Heidelberg, Germany,
Oct. 6-10, 2008).
Kodama, T.: 2008, Ultimate Studies of Environmental Effects in
Cosmic Webs in the Distant Universe, Cosmology Near and Far:
Science with WFMOS, (Kona Hawaii, USA, May 19-21, 2008).
Kodama, T.: 2008, When and Where Did Early-Type Galaxies
Form?, Int. Lorenz Center Workshop, Galaxies in Real Life andSimulations, (Leiden, Netherland, Sep. 15-19, 2008).
Kojima, K., Ichiki, K., Kajino, T., Mathews, G. J., Yamazaki, D. G.:
2008, Neutrino mass effect on CMB polarization in the existenceof primordial magnetic field, Int. Symp. on Cosmology andParticle Astrophysicsk, (APCTP, Korea, Oct. 28-Nov. 1, 2008).
Kojima, K., Ichiki, K., Kajino, T., Mathews, G. J., Yamazaki, D.
G.: 2008, Neutrino mass effects on the CMB polarization with
PMF, The 6th Japan-Italy symposium on Heavy-Ion Physics,(Tokai, Ibaraki, Japan, Nov. 11-15, 2008).
Kojima, K., Ichiki, K., Kajino, T., Mathews, G. J.: 2008, A new
method to constrain the neutrino mass from CMB polarization
with PMF, The 7th RESCEU Int. Symp. on Astroparticle
Physics and Cosmology, (Tokyo, Japan, Nov. 11-14, 2008).

086

II Publications, Presentations

Kojima, K., Yamazaki, D. G., Kajino, T.: 2008, Neutrino effects
in Cosmology with the primordial magnetic field, 10th Symp.
on Nuclei in the Cosmos, (Mackinac Island, Michigan, USA,
July 27-Aug. 1, 2008).
Kojima, T., Kroug, M., Fujii, Y., Uzawa, Y., Takeda, M., Wang,
Z., Shi, S.-C., Shan, W.-L.: 2008, Performance of terahertz
waveguide SIS mixers employing epitaxial NbN films and Nb
junctions, Applied Superconductivity Conf., (Chicago, USA,
Aug. 17-22, 2008).
Kojima, T., Kroug, M., Takeda, M., Shan, W.-L., Fujii, Y.,
Uzawa, Y., Wang, Z., Shi, S.-C.: 2008, Performance of terahertz
waveguide SIS mixers employing epitaxial NbN films and Nb
junctions, The 9th Workshop on SMW Rx Technologies in
Eastern Asia, (Taipei, Taiwan, Nov. 18-20, 2008).
Kojima, T., Uzawa, Y., Shan, W.-L., Fujii, Y., Takeda, M., Kroug,
M., Shitov, S., Ogawa, H.: 2008, Characterization of waveguidecomponents for the ALMA band 10, 19th Int. Symp. on Space
Terahertz Technology, (Groningen, Netherlands, Apr. 28-30,
2008).
Kokubo, E.: 2008, Dynamics of Planetary Accretion , The 3rd
East-Asia Numerical Astrophysics Meeting, (Nanjing, China,
Nov. 10-13, 2008).
Kokubo, E.: 2008, Formation of Terrestrial Planets, Origin and
Evolution of Planets 2008, (Ascona, Switzerland, June 29-July 4,2008).
Kokubo, E.: 2008, Formation of Terrestrial Planets from Protoplanets, AGU 2008 Fall Meeting, (San Francisco, CA, USA,
Dec. 15-19, 2008).
Kokubo, E.: 2008, Formation of Terrestrial Planets from Protoplanets,
Exoplanets and Disks: Their Formation and Diversity, (Keauhou,
Hawaii, USA, Mar. 9-12, 2009).
Kokubo, E.: 2008, Formation of Terrestrial Planets under a Realistic
Accretion Condition, The 10th Asian-Pacific Regional IAU
Meeting, (Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Komiyama, Y.: 2008, HSC Camera Design, Cosmology Near andFar: Science with WFMOS, (Kona Hawaii, USA, May 19-21,
2008).
Komiyama, Y.: 2009, Hyper Suprime-Cam Camera Mechanics
Design and Status, Japan-Princeton-Taiwan HSC Workshop,(Mitaka, Japan, Jan. 17-20, 2009).
Kotake, K.: 2008, Gravitational Radiation from SASI-aided
Rotating Supernova Explosions in Three Dimensions,
Numerical Modeling of Astrophysical Sources of Gravitational
Waves, (Valencia, Spain, Sep. 8-12, 2008).
Kotake, K.: 2008, Gravitational waves from core-collapse supernovae: key to the explosion mechanism, 24th Texas Symp. on
Relativistic Astrophysics, (Vancouver, Canada, Dec. 8-12, 2008).
Kotake, K.: 2008, Multidimensional modeling of core-collapse
supernovae: new challenges and perspectives, The 7th RESCEU
Int. Symp. on Astroparticle Physics and Cosmology, (Tokyo,
Japan, Nov. 11-14, 2008).
Kotake, K.: 2008, Stochastic Nature of Gravitational-wave Signals
from 3D Supernova Explosions, Asymmetric instabilities instellar collapse, (Paris, France, June 30-Jul. 11).
Kotoku, J.: 2008, Long Time Observation of X-Ray Bright Point
with Hinode, The 2nd Hinode Science Meeting - Beyond

Discovery Toward Understanding, (Boulder, Colorado, USA,
Sep. 29-Oct. 3, 2008).
Kroug, M., Endo, A., Tamura, T., Noguchi, T., Uzawa, Y.,
Takeda, M., Wang, Z., Shan, W.: 2008, SIS Mixer Fabrication
for ALMA Band10, Applied Superconductivity Conf., (Chicago,
USA, Aug. 17-22, 2008).
Kroug, M., Kojima, T., Fujii, Y., Uzawa, Y., Endo, A., Tamura,T., Kiuchi, Y., Noguchi, T., Takeda, M., Wang, Z., Shan, W.:
2008, SIS mixers for ALMA band-10(787-950 GHz), The 9thWorkshop on SMW Rx Technologies in Eastern Asia, (Taipei,
Taiwan, Nov. 18-20, 2008).
Kusakabe, M., Kajino, T., Mathews, G. J.: 2008, Big Bang Production of 6,7Li via the SUSY NLSP, 18th Midwest Relativity
Meeting, (Notre Dame, Indiana, Oct. 24-25, 2008).
Kusakabe, N., et al.: 2008, Magnetic Fields in Massive Star Forming Regions: Wide-field NIR Polarimetry of M 42 and Mon
R2, IAU Symp. 259, Cosmic Magnetic Fields: from Planets, toStars and Galaxies, (Canary Islands, Spain, Nov. 3-7, 2008).
Liu, Q., et al. including Kikuchi, F., Goossens, S., Matsumoto, K.,
Harada, Y., Ishihara, Y., Hanada, H., Asari, K., Ishikawa, T.,
Tsuruta, S., Kawano, N., Sasaki, S., Noda, H.: 2008, Correcting atmospheric and ionospheric delay in KAGUYA VLBI
observations using GPS technique, Int. Symp. on GPS/GNSS
2008, (Tokyo, Japan, Nov. 11-14, 2008).
Liu, Q., et al. including Kikuchi, F., Matsumoto, K., Goossens,S., Hanada, H., Harada, Y., Asari, K., Ishikawa, T., Tsuruta,
S., Kawano, N., Ishihara, Y., Noda, H., Sasaki, S.: 2009,
Same-beam VLBI observations of SELENE for detecting lunar
gravity field, 2009 East Asia VLBI Workshop, (Ewha Woman's
University, Seoul, Korea, Mar. 18-20, 2009).
Liu, Q., et al. including Kikuchi, F., Matsumoto, K., Hanada, H.,
Ishihara, Y., Kawano, N., Asari, K., Noda, H., Ishikawa, T.,
Tsuruta, S., Goossens, S., Sasaki, S.: 2008, Studies on Doppler
and differential VLBI techniques using two sub-satellites
OKINA and OUNA of KAGUYA (SELENE), AOGS 5th
Annual Meeting, (Busan, Korea, June 16-20, 2008).
Liu, Q., et al. including Kikuchi, F., Matsumoto, K., Ishihara, Y.,
Hanada, H., Kawano, N., Asari, K., Ishikawa, T., Tsuruta,
S., Goossens, S., Noda, H., Sasaki, S.: 2008, Same-beam andswitching VLBI observations for SELENE(KAGUYA) usingeight VLBI stations, The 10th Asian-Pacific Regional IAU
Meeting, (Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Liu, Q., Kikuchi, F., Matsumoto, K., Goossens, S., Hanada,
H., Iwata, T., Namiki, N., Noda, H., Ishihara, Y., Asari, K.,
Ishikawa, T., Tsuruta, S., Harada, Y., Kawano, N., Sasaki,
S.: 2009, Studies on 4-way Doppler and differential VLBI
techniques of Kaguya (SELENE) for detecting lunar gravity
field, The 3rd KAGUYA (SELENE) Science Working Team
Meeting, (Tamachi, Japan, Jan. 14-15, 2009).
Machida, M., Matsumoto, R.: 2008, Magneto-hydrodynamic Simulations of Excitation of Low-Frequency QPOs in Black Hole
Candidates, Astrophysics with All-Sky X-ray Observations,(Saitama, Japan, Oct. 12, 2008).
Machida, M.: 2008, Formation of an Inner Torus in Black Hole
Accretion Flows, Turbulence and Oscillations in Accretion
Discs, (Stockholm, Sweden, Oct. 1-15, 2008).

Magara, T.: 2008, Emergence of a Partially Split Flux Tube in the
Solar Atmosphere, 2008 Huntsville Workshop, (Huntsville, AL,
USA, Oct. 29, 2008).
Magara, T.: 2008, Hinode's Observational Result on the Saturationof Magnetic Helicity Injected into the Solar Atmosphere andits Relation to the Occurrence of a Solar Flare, The 2nd Hinode
Science Meeting - Beyond Discovery Toward Understanding,(Boulder, Colorado, USA, Sep. 29-Oct. 3, 2008).
Magara, T.: 2008, New view of the Sun revealed by Hinode, The
East Asian Young Astronomers Meeting 2008, (Jiayuguan,
China, July 27-Aug. 1, 2008).
Magara, T.: 2008, Toward understanding 3D and dynamic natureof solar prominences, Solar Activity in Solar Cycle 24, (Napa,
CA, USA, Dec. 8-12, 2008).
Magara, T.: 2008, What do we learn from the flux emergencestudy based on a comparison between simulations andobservations? II, 2008 Flux Emergence Workshop, (Kyoto,
Japan, Oct. 6-9, 2008).
Makino, J.: 2008, GRAPE-DR: An accelerator for scientificcomputing , HAC2008, (Tsukuba, Japan, Oct 1, 2008).
Makino, J.: 2008, Numerical Simulation of Galaxy Formation, From
Genome to Snowball Earth, (Tokyo, Japan, Sep. 28-Oct. 3, 2008).
Mann, I., Ishiguro, M.: 2008, Optical Properties of Cometary
Coma and Trail Particles, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Matsumoto, K., Goossens, S., Ishihara, Y., Liu, Q., Iwata, T.,
Namiki, N., Noda, H., Hanada, H., Kikuchi, F., Kawano, N.,
Tsuruta, S., Asari, K., Ishikawa, T., Sasaki, S.: 2008, Initial
results of global lunar gravity field recovery from SELENE
tracking data, Earth Tides Symp. 2008, IAG, (Jena, Germany,
Sep. 1-5, 2008).
Matsumoto, K., Goossens, S., Ishihara, Y., Liu, Q., Iwata, T.,
Namiki, N., Noda, H., Hanada, H., Kikuchi, F., Kawano, N.,
Tsuruta, S., Asari, K., Ishikawa, T., Sasaki, S.: 2008, Initial
Results of Global Lunar Gravity Field Recovery from SELENE
tracking data, 37th COSPAR Scientific Assembly, (Montreal,
Canada, Jul. 13-20, 2008).
Matsumoto, K., Namiki, N., Goossens, S., Ishihara, Y., Liu, Q.,
Kikuchi, F., Iwata, T., Hanada, H., Noda, H., Kawano, N.,
Asari, K., Tsuruta, S., Ishikawa, T., Harada, Y., Sasaki, S.,
Kurosawa, K., Sugita, S., Imamura, T., RSAT/VRAD Mission
Team: 2009, Current Status of Gravity Field Estimation fromTracking Data of SELENE (Kaguya), The 3rd KAGUYA(SELENE) Science Working Team Meeting, (Tamachi, Japan,
Jan. 14-15, 2009).
Matsumoto, N.: 2008, Variable Asymmetry of the Circumstellar
Envelope in IK Tauri Traced by SiO Maser Emission, AGB stars
and related phenomena, (Mitaka, Japan, Nov. 12-14, 2009).
Matsuo, H., Aria, T., Nitta, T., Kosaka, A.: 2009, Far-infrared
spectroscopic imaging of interstellar material around etaCarinae, AKARI Int. Conf., (Univ. of Tokyo, Tokyo, Japan, Feb.
16-19, 2009).
Matsuo, H., Hibi, Y., Nagata, H., Arai, H., Ariyoshi, S., Otani,C., Ikeda, H., Fujiwara, M.: 2008, Design of Superconducting
Terahertz Digicam, 33rd Int. Conf. on Infrared, Millimeter, andTerahertz Waves, (Pasadena, USA, Sep. 15-19, 2008).

II Publications, Presentations

087

Matsuo, H., Hibi, Y., Nagata, H., Ariyoshi, S., Otani, C., Ikeda,
H., Fujiwara, M.: 2008, Design of Superconducting Terahertz
Digicam, 19th Int. Symp. on Space Terahertz Technology,(Groningen, Netherlands, Apr. 28-30, 2008).
Matsuo, H., Hibi, Y., Nagata, H., Ikeda, H., Fujiwara, M.: 2008,
Cryogenic Readout Electronics for Cryogenic Readout
Electronics for Superconductive Terahertz Superconductive
Terahertz Digicam Digicam, The 9th Workshop on SMW Rx
Technologies in Eastern Asia, (Taipei, Taiwan, Nov. 18-20, 2008).
Matsuo, H., Hibi, Y., Nagata, H., Nakahashi, M., Murakoshi, Y.,
Arai, H., Ariyoshi, S., Otani, C., Ikeda, H., Fujiwara, M.: 2008,
System design of submillimeter-wave imaging array SISCAM,SPIE 2008 Astronomical Instrumentation, (Marseilles, France,
June 23-28, 2008).
Matsuo, H.: 2008, High Sensitivity THz Imaging Technologies
for Astronomy and other Applications, 2008 Workshop for
Microwave and Millimeter-waves, (Seoul, Korea, Oct. 9, 2008).
Matsuo, H.: 2009, Interferometer and detector developments inJapan, European Workshop on Far-Infrared Interferometry
Technology Development, (Edinburgh, UK, Feb. 10-11, 2009).
Migita, E., Araki, H., Noda, H., Tazawa, S., Ishihara, Y., Iwata,T.: 2009, Measurement of Lunar Craters Size from SELENE/LALT, 40th Lunar and Planetary Science Conf., (The
Woodlands, Texas, USA, Mar. 23-27, 2009).
Miyazaki, A.: 2009, First phase of the East Asia VLBI network
using the K4/VSOP terminal, 2009 East Asia VLBI Workshop,(Ewha Woman's University, Seoul, Korea, Mar. 18-20, 2009).
Miyoshi, M.: 2008, Horizon Telescope in Andes. A Black Hole
Imager, Int. Workshop on New Astronomical Facilities in Peru,
in honor to Mutsumi Ishitsuka, (Lima, Peru, June 28- July 8,2008).
Miyoshi, M.: 2009, High Resolutions in Spectra and Space Unveil
the Existence of Black Holes in the Universe, SPECTRA 2009,
Conf. on Spectroscopy and its Applications, (Lima, Peru, Mar.
2-13, 2009).
Mizuno, N.: 2008, The properties of molecular clouds across the
Magellanic System, IAU Symp. 256, The Magellanic System:
Stars, Gas, and Galaxies, (University of Keele, UK, Jul.
28-Aug. 1, 2008).
Morimoto, N., Hanaoka, Y.: 2008, Ultraviolet Jets as the Energy
Release Events in the Chromosphere, 37th COSPAR Scientific
Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Moroz, L., Helbert, J., Maturilli, A., Sasaki, S., Bischoff, A.: 2008,
Laboratory studies of Mercury analogue materials: optical
spectroscopy and space weathering simulation experiments,
37th COSPAR Scientific Assembly, (Montreal, Canada, Jul.
13-20, 2008).
Murakami, N., Uemura, R., Baba, N., Shibuya, H., Nishikawa,J., Abe, L., Tamura, M., Hashimoto, N.: 2008, Laboratory
experiments on the 8-octant phase-mask coronagraph, SPIE
2008 Astronomical Instrumentation, (Marseilles, France, June
23-28, 2008).
Murakami, N., Yokochi, K., Nishikawa, J., Tamura, M., Baba, N.,
Uemura, R., Hashimoto, N., Abe, L., Tavrov, A. V., Kurokawa,T., Takeda, M.: 2009, Development of 4th-Order NullingCoronagraphs for Partially Resolved Stars, Exoplanets and088

II Publications, Presentations

Disks: Their Formation and Diversity, (Kona, Hawaii, USA,
Mar. 9-11, 2009).
Nagai, H.: 2008, Constraining the kinematic and spectral ages of
the recurrent CSO 3C84 , The 4th Workshop on Compact Steep
Spectrum and GHz-Peaked Spectrum Radio Sources, (Riccione,
Italy, May 26-29, 2008).
Nagai, T., Agata, H., Itoh, S., Nakayama, H., Naito, S., Hirai, A.:
2009, Challenge of “Science Culture Promotion Unit ThroughAstronomical Images”, IAU Symp. 260: The Rôle of Astronomy inSociety and Culture, (UNESCO, Paris, France, Jan. 19-23, 2009).
Nagashima, K.: 2008, Travel-time analyses of an emerging-flux
region, The 2nd Hinode Science Meeting - Beyond Discovery
Toward Understanding, (Boulder, Colorado, USA, Sep. 29-Oct.
3, 2008).
Nagashima, M., Okamoto, T.: 2008, The Metal Enrichment of the
Milky Way and its Satellites in a Hierarchical Galaxy Formation
Model, The 10th Asian-Pacific Regional IAU Meeting,(Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Nagata, H., Kobayashi, J., Matsuo, H., Hibi, Y., Nakahashi, M.,
Ikeda, H., Fujiwara, M.: 2008, Development of a cryogenic GaAs
AC-coupled CTIA readout for far-infrared and submillimeter
detectors, SPIE 2008 Astronomical Instrumentation, (Marseilles,
France, June 23-28, 2008).
Nagata, H., Matsuo, H., Hibi, Y., Kobayashi, J., Nakahashi, M.,
Ikeda, H., Fujiwara, M.: 2008, GaAs cryogenic readout
electronics for high impedance detector arrays for far-infraredand submillimeter wavelength region, 8th Int. Workshop on
Low Temperature Electronics, (Jena/Gabelbach, Germany, Jun.
22-25, 2008).
Nakajima, Y., Tamura, M., Sato, Y., ATLAS team: 2008, AKARIIRC Atlas and Catalog of Star Forming Regions, AKARI Int.
Conf., (Univ. of Tokyo, Tokyo, Japan, Feb. 16-19, 2009).
Nakamura, K.: 2008, Second-order gauge-invariant cosmologicalperturbation theory –3. Consistency of equations–, The 18th
Workshop on General Relativity and Gravitation in Japan,(Hiroshima, Japan, Nov. 17-21, 2008).
Nakamura, K.: 2008, Second-order gauge-invariant cosmologicalperturbation theory and its applications, Int. workshop: 11th
Capra meeting on radiation reaction problem in Generalrelativity, (Orleans, France, June 23-29, 2008).
Namiki, N., et al. including Matsumoto, K., Goossens, S.,
Ishihara, Y., Noda, H., Sasaki, S., Hanada, H., Araki, H.:
2009, Comparative study of compensation mechanism of
Lunar impact basins from new gravity field model of SELENE(Kaguya), 40th Lunar and Planetary Science Conf., (The
Woodlands, Texas, USA, Mar. 23-27, 2009).
Namiki, N., Hanada, H., Iwata, T., RSAT Team, VRAD Team,and LALT team: 2008, Lunar far Side Gravity From SELENE
Mission And Dichotomy of the Moon, AGU 2008 Fall Meeting,(San Francisco, CA, USA, Dec. 15-19, 2008).
Namiki, N., Hanada, H., Iwata, T., RSAT, VRAD, and LALT
teams: 2008, Lunar far side gravity from the KAGUYA(SELENE) mission and dichotomy of the moon., 71nd Annual
Meeting of the Meteoritical Society, (Matsue, Japan, Jul.
28-Apr. 1, 2008).
Narita, N.: 2008, Subaru HDS Ground-based Transmission

Spectroscopy for HD189733b, Molecules in the Atmospheres ofExtrasolar Planets, (Paris, France, Nov. 19, 2008).
Narita, N.: 2008, Subaru HDS Ground-based Transmission
Spectroscopy for the Transiting Exoplanet HD189733b,
RESCEU Summer School, (Aomori, Japan, Aug. 30, 2008).
Narita, N.: 2008, The Rossiter-McLaughlin Effect and a Possible
Spin-Orbit Misalignment in HD17156b, IAU Symp. 253,
Transiting Planets, (Boston, USA, May 20, 2008).
Narita, N.: 2009, Past and Future Studies of Transiting Extrasolar
Planets, Exoplanets and Disks: Their Formation and Diversity,(Kona, Hawaii, USA, Mar. 9-11, 2009).
Naruse, M., Kamikura, M., Sekimoto, Y., Ito, T., Sugimoto, M.,
Iizuka, Y., Satou, N., Kumagai, K.: 2008, Near-field beam
and cross-polarization pattern measurements of ALMA band
8 cartridges, 19th Int. Symp. on Space Terahertz Technology,(Groningen, Netherlands, Apr. 28-30, 2008).
Naruse, M., Sekimoto, Y., Kamikura, M., Sugimoto, M., Ito,
T., Satou, N., Kumagai, K., Iizuka, Y., Fujimoto, Y.: 2008,
Near-Field Beam Pattern Measurement of ALMA Band 8 (385–500GHz) First Cartridge, 3rd European Conf. on Antenna andPropagation, (Berlin, Germany, Mar. 23-27, 2009).
Nishikawa, J., Yokochi, K., Abe, L., Murakami, N., Kotani, T.,
Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.: 2008,
Virtual wavefront compensation and speckle reduction incoronagraph by unbalanced nulling interferometer (UNI) andphase and amplitude correction (PAC), SPIE 2008 Astronomical
Instrumentation, (Marseilles, France, June 23-28, 2008).
Nishikawa, J., Yokochi, Murakami, N., Abe, L., Kotani, T.,
Tamura, M., Kurokawa, T., Tavrov, A. V., Takeda, M.: 2009,
Coronagraph methods on precise wavefront compensation (UNIPAC) and deep achromatic nulling, Exoplanets and Disks: Their
Formation and Diversity, (Kona, Hawaii, USA, Mar. 9-11, 2009).
Nishiyama, S., Tamura, M., Hatano, H., Kanai, S., Kurita, M.,
Sato, S., Nagata, T., IRSF/SIRIUS team: 2008, Near-Infrared
Polarimetry toward the Galactic Center, Astronomical Polarimetry
2008, (La Malbaie, Quebec, Canada, Jul. 6-11, 2008).
Nishizawa, J.: 2008, Cross-correlation study of the Rees-Sciama
effect with the weak lensing and implications for dark energy,
3rd Biennial Leopoldina Conf. on dark energy, (Munich,Germany, Oct. 7-11, 2008).
Niwa, Y., Arai, K., Ueda, A., Sakagami, M., Gouda, N., Kobayashi,Y., Yamada, Y., Yano, T.: 2008, Development of laserinterferometric high-precision geometry monitor for JASMINE,SPIE 2008 Astronomical Instrumentation, (Marseilles, France,
June 23-28, 2008).
Noda, H., Araki, H., Tazawa, S., Ishihara, Y., Migita, E., Kawano,N., Sasaki, S., Tsubokawa, T., Kamiya, I., Oberst, J.: 2008,
The First Global Lunar Topography Mapping by KAGUYA(SELENE) Laser Altimeter (LALT), EGU, (Vienna, Austria,
Apr. 13-18, 2008).
Noda, H., Araki, H., Tazawa, S., Ishihara, Y., Migita, E., Kawano,N., Tsubokawa, T., Kamiya, I., Sasaki, S., Oberst, J.: 2008, The
first global lunar topography mapping by KAGUYA (SELENE)
laser altimeter (LALT), 37th COSPAR Scientific Assembly,(Montreal, Canada, Jul. 13-20, 2008).
Noda, H., Hanada, H., Iwata, T., Kawano, N., Sasaki, S., Araki,

H., Imamura, T.: 2008, Optical and low frequency radio
observatory on the Moon, ILC(LEAG-ICEUM-SRR), (CapeCanaberal, USA, Oct. 28-31, 2008).
Noguchi, T.: 2008, Effect of complex superconducting gap energies
on SIS tunneling current, The 9th Workshop on SMW Rx
Technologies in Eastern Asia, (Taipei, Taiwan, Nov. 18-20, 2008).
Oh, C.: 2009, Study of the Galactic rotation curve with VERA,
2009 East Asia VLBI Workshop, (Ewha Woman's University,
Seoul, Korea, Mar. 18-20, 2009).
Ohishi, M.: 2008, Astrobiology-related research activity in the
National Astronomical Observatory of Japan, SPIE, (San Diego,
CA, USA, Aug. 13, 2008).
Ohishi, M.: 2008, Astronomical Virtual Observatories throughInternational Collaborations, Fifty Years after IGY, (Tsukuba,
Japan, Nov. 12, 2008).
Ohishi, M.: 2008, Construction of Virtual Observatories in
the World, The 10th Asian-Pacific Regional IAU Meeting,(Kunming, Yunnan, Nanjing, China Aug. 3-6, 2008).
Ohishi, M.: 2008, Impact to the Radio Astronomy by theInterference caused by the Solar Power Satellite Systems, 29th
URSI General Assembly, (Chicago, USA, Aug. 9-16, 2008).
Ohishi, M.: 2008, JVO and NaReGi (Japanese Grid middleware
initiative), EURO-VO, Grid Workshop, (Garching, Germany,
Apr. 10, 2008).
Ohishi, M.: 2008, Protection of Space-based Observations and theInternational Telecommunication Union (ITU), 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Ohishi, M.: 2008, Special Item: ITU/Leap Second, IVOA
interoperability meeting 2008 Autumn, (Baltimore, Maryland,
USA, Oct. 28, 2008).
Ohishi, M.: 2008, The spectral line survey in TMC-1 – Progressof the data analysis, Workshop for Interstellar Matter 2008,(Sapporo, Japan, Sep. 4, 2008).
Ohishi, N., Yoshizawa, M., Nishikawa, J., Murakami, N., Torii,
Y., Suzuki, S., Kubo, K., Iwashita, H., Kondo, Y.: 2008,
Recent progress at the MIRA: development of fringe tracking
system, SPIE 2008 Astronomical Instrumentation, (Marseilles,
France, June 23-28, 2008).
Ohsuga, K.: 2008, Global Radiation Magneto-hydrodynamic
Simulations of Accretion Flows and Outflows around Black
Holes, The 3rd East-Asia Numerical Astrophysics Meeting,(Nanjing, China, Nov. 10-13, 2008).
Okada, T., Shiraishi, H., Kato, M., Grande, M., Shirai, K.,
Yamamoto, Y., Arai, T., Ogawa, K.: 2008, X-ray fluorescence
spectrometry of the Moon by the XRS onboard SELENEKAGUYA, 37th COSPAR Scientific Assembly, (Montreal,
Canada, Jul. 13-20, 2008).
Okada, T., Shiraishi, H., Shirai, K., Yamamoto, Y., Arai, T.,
Ogawa, K., Kato, M., Grande, M., Selene Xrs Team: 2009,
X-Ray Fluorescence Spectrometer (XRS) on Kaguya: Current
Status and Results, 40th Lunar and Planetary Science Conf., (The
Woodlands, Texas, USA, Mar. 23-27, 2009).
Okada, T., Yamamoto, Y., Ogawa, K., Arai, T., Shirai, K.: 2008,
X-ray fluorescence spectrometry for Hayabusa and Hayabusa-2
missions, 37th COSPAR Scientific Assembly, (Montreal,
Canada, Jul. 13-20, 2008).

II Publications, Presentations089

Okamoto, T. J.: 2008, Prominence and coronal magnetic fielda,
Solar-C Science Definition Meeting, (Sagamihara, Japan, Nov.
17-21, 2008).
Okamoto, T. J.: 2008, Emergence of a helical flux rope andprominence formation, SPD/AGU Meeting, (Fort Lauderdale,
Florida, USA, May 27-30, 2008).
Okamoto, T. J.: 2008, Emergence of a Helical Flux Rope andProminence Formation, The 2nd Hinode Science Meeting Beyond Discovery Toward Understanding, (Boulder, Colorado,
USA, Sep. 29-Oct. 3, 2008).
Okamoto, T. J.: 2008, Observation of helical flux emergence, 2008
Flux Emergence Workshop, (Kyoto, Japan, Oct. 6-9, 2008).
Okamoto, T. J.: 2008, Emergence of a helical flux rope andprominence formation, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Ootsubo, T., Ueno, M., Ishiguro, M., Usui, F., Pyo, J., Hong, S.
S., Mukai, T.: 2009, Mid-infrared spectrum of the zodiacal
light observed by AKARI, AKARI Int. Conf., (Univ. of Tokyo,
Tokyo, Japan, Feb. 16-19, 2009).
Ootsubo, T., Ueno, M., Ishiguro, M., Usui, F., Pyo, J., Kwon, S.
M., Mukai, T., Hong, S. S.: 2008, Spectroscopic Observationsof Zodiacal Emission by AKARI, AOGS 5th Annual Meeting,(Busan, Korea, June 16-20, 2008).
Ootsubo, T., Watanabe, J., Honda, M., Kawakita, H., Furusho, R.:
2008, Mid-infrared Observations of Cometary Dust by Subaru
Telescope, AOGS 5th Annual Meeting, (Busan, Korea, June
16-20, 2008).
Oshima, T., Yoshitake, H.: 2008, Optimization Method for TES
Microcalorimeters with Absorbers, Applied Superconductivity
Conf., (Chicago, USA, Aug. 17-22, 2008).
Oyama, K., Imamura, T., Iwata, T., Kono, Y., Matsumoto, K., Liu,
Q., Noda, H., Futaana, Y., Nabatov, A., Mochizuki, N., Andou,
H.: 2008, Initial results of the lunar ionosphere observation with
SELENE Radio Science, 37th COSPAR Scientific Assembly,(Montreal, Canada, Jul. 13-20, 2008).
Ozaki, S.: 2008, Optical Medium Resolution Spectroscopic
Observation of NGC 1068, The 10th Asian-Pacific Regional IAU
Meeting, (Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Petrova, N., Gusev, A., Hanada, H., Heki, K., Kawano, N.: 2008,
Interpretation of the Lunar physical libration for future observations
from the Lunar surface, EPSC 2008: European Planetary
Science Congress, (Münster, Germany, Sep. 21-26, 2008).
Pyo, J., Hong, S. S., Kwon, S. M., Ishiguro, M., Ueno, M., Usui,
F., Ootsubo, T., Mukai, T.: 2008, Vertical Structure of theInterplanetary Dust Cloud, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Pyo, J., Hong, S. S., Kwon, S. M., Ueno, M., Ishiguro, M., Usui, F.,
Ootsubo, T., Ishihara, D., Mukai, T.: 2009, The Zodiacal Dust
Cloud Revealed by the AKARI IRC All-Sky Survey, AKARI
Int. Conf., (Univ. of Tokyo, Tokyo, Japan, Feb. 16-19, 2009).
Pyo, T.-S., et al.: 2009, Transition Disks – Key of Disk Evolution
and Planet Formation, Exoplanets and Disks: Their Formation
and Diversity, (Kona, Hawaii, USA, Mar. 9-11, 2009).
Saigo, K.: 2008, Observational Characteristics of the Rotating First
Core, The 5th ALMA Japan-Taiwan science workshop, (National
Tsin Hua University, Taiwan, Dec. 4-6, 2008).

090

II Publications, Presentations

Saigo, K.: 2008, Observational Characteristics of the Rotating First
Core, ASTE Science Workshop, (Mitaka, Japan, Dec. 11-12, 2008).
Saigo, K.: 2008, The Formation and Evolution of the First Core,
ALMA-JT, (Ibaraki University, Japan, Apr. 4-6, 2008).
Saitoh, T. R.: 2008, A parallel N-body/SPH code ASURA and
its applications, Astrosim: Frontiers in Computational Astrophysics, (Ascona, Switzerland, July 13-18, 2008).
Saitoh, T. R.: 2008, Initial results of "Project Milkyway'', The 3rd
East-Asia Numerical Astrophysics Meeting, (Nanjing, China,
Nov. 10-13, 2008).
Saitoh, T. R.: 2009, Formation of Globular Clusters in Colliding
Galaxies, Formation and Evolution of Globular Clusters, (Santa
Barbara, USA, Jan. 12-16, 2009).
Sakata, S., et al. including Nishizawa, A., Yamazaki, T., Fukushima,M., Kawamura, S.: 2008, Development for observation andreduction of radiation pressure noise, Gravitational Wave
Advanced Detector Workshop, (Elba, Italy, May 12-18, 2008).
Sakata, S., Miyakawa, O., Nishizawa, A., Numata, N., Nishida, E.,
Ishizaki, H., Furusawa, A., Kawamura, S.: 2008, Development
for observation and reduction of radiation pressure noise, LSCVirgo Joint Meeting, (Amsterdam, Netherlands, Sep. 22-25, 2008).
Sakata, S., Rager, S., Nishida, E., Kawamura, S.: 2009, Measurement of quantum efficiency of photodiode by radiationpressure, March LSC-Virgo Meeting, (Arcadia, California,
USA, Mar 16-19, 2009).
Sako, N., Hatsutori ,Y., Inamori, T., Nakasuka, S.: 2008, Small
Infrared Astrometry Satellite Nano-JASMINE Bus System, The
26th Int. Symp. on Space Technology and Science, (Hamamatsu,
Japan, June 1-8, 2008).
Sakurai, T.: 2008, Solar wind problems and what will newly be
expected from Plan-A observations, Solar-C Science Definition
Meeting, (Sagamihara, Japan, Nov. 17-21, 2008).
Sakurai, T.: 2008, Interpretation of magnetic filling factor
observed with Hinode/SOT, Int. Workshop of 2008 Solar Total
Eclipse, (Jiuquan, Gansu, China, Jul. 28-Aug. 5, 2008).
Sarugaku, Y., Ishiguro, M., Ueno, M., Usui, F., Reach, W. T.: 2008,
Large dust emission from Comet 2P/Encke in 2003 return, AOGS
5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Sarugaku. Y., Ishiguro, M., Ueno, M., Usui, F.: 2008, Scattering
Phase Function of the Comet 2P/Encke Dust Trail, AOGS 5th
Annual Meeting, (Busan, Korea, June 16-20, 2008).
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., Noda, H., Tazawa, S.,
Tsuruta, S., Harada, Y., Petrova, N., Kurosawa, K., Sugita, S.:
2008, Global Topography and Gravity of the Moon Revealedby KAGUYA Mission, The 40th Annual Meeting of DPS-AAS,(Ithaca, USA, Oct. 10-15, 2008).
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., Noda, H., Tazawa, S.,
Tsuruta, S., Kurosawa, K., Seiji, S., Takano, T.: 2008, Global
topography and gravity field of the Moon by SELENE(KAGUYA), ILC(LEAG-ICEUM-SRR), (Cape Canaberal,
USA, Oct. 28-31, 2008).
Sasaki, S., et al.: 2008, Development of plane parallel impact-ionization dust/debris detector, 37th COSPAR Scientific
Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Sasaki, S., et al.: 2008, Investigation of Jovian satellites and theorigin of Jovian system by LAPLACE, 37th COSPAR Scientific
Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Sasaki, S., et al.: 2008, Satellites and the Origin of the Jovian
System: A New Page by Laplace, AOGS 5th Annual Meeting,(Busan, Korea, June 16-20, 2008).
Sasaki, S., Hiroi, T., Helbert, J.: 2008, Simulating Space
Weathering on Mercury, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Sasaki, S., Hiroi, T.: 2008, Difference of Space Weathering Degree
on Asteroids of Various Sizes, 71nd Annual Meeting of the
Meteoritical Society, (Matsue, Japan, Jul. 28-Apr. 1, 2008).
Sasaki, S., Ishihara, Y., Noda, H., Araki, H., Migita, E., Tazawa,
S.: 2008, KAGUYA laser altimeter (LALT) initial results on
lunar impact structures, 37th COSPAR Scientific Assembly,(Montreal, Canada, Jul. 13-20, 2008).
Sasaki, S., Namiki, N., Hanada, H., Iwata, T., Kawano, N.,
Matsumoto, K., Noda, H., RSAT/VRAD Group: 2008, New lunar
gravity field from SELENE (KAGUYA) gravity experiment using
two subsatellites, EGU, (Vienna, Austria, Apr. 13-18, 2008).
Sasaki, S., Ohashi, H., Hirai, T., Iwai, T., Shibata, H., Nogami,K., Fujii, M.: 2008, Development of Plane-Parallel ImpactIonization Dust Detectors with Large Aperture: A Candidate for
Kibo Exposed Facility Payload, The 26th Int. Symp. on SpaceTechnology and Science, (Hamamatsu, Japan, June 1-8, 2008).
Sasaki, S., Satoh, T.: 2009, Japan's Mars Exploration Plan: MELOS,
MEPAG Meeting, (Arlington, Virginia, USA, Mar. 3-4, 2009).
Sasaki, S.: 2008, Change of the space weathering rate on
Mercury: Effect of the surface mixing, 37th COSPAR Scientific
Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Sasaki, S.: 2008, Surface heterogeneity of small asteroids, 37th
COSPAR Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Sasaki, S.: 2009, Gravity and Topography of Lunar Basins:
Kaguya Results, Brown-Vernadsky Microsymposium 49, (The
Woodlands, Texas, USA, Mar. 23-27, 2009).
Sato, M., Watanabe, J.: 2008, Origin of the recent Orionid Outburst,
AOGS 5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Sawada, T.: 2009, On-The-Fly Observing System of the Nobeyama
45-m and ASTE 10-m Telescopes, Annual meeting of the Chilean
Astronomical Society, (Santiago, Chile, Jan. 14-16, 2009.
Sekiguchi, Y.: 2008, Stellar core collapse with microphysics in fullgeneral relativity, Numerical Modeling of Astrophysical Sourcesof Gravitational Waves, (Valencia, Spain, Sep. 8-12, 2008).
Sekiguchi, Y.: 2008, Towards clarifying the central engine of long
gamma-ray bursts, The 18th Workshop on General Relativity
and Gravitation in Japan, (Hiroshima, Japan, Nov. 17-21, 2008).
Sekii, T.: 2008, High-resolution Helioseismic Observations, The
2nd Hinode Science Meeting - Beyond Discovery Toward
Understanding, (Boulder, Colorado, USA, Sep. 29-Oct. 3, 2008).
Sekii, T.: 2008, Sensitivity of large-angle method to detect deepsheeted magnetic flux, Solar-C Science Definition Meeting,(Sagamihara, Japan, Nov. 17-21, 2008).
Sekimoto, Y., Iizuka, Y., Satou, N., Ito, T., Kumagai, K., Kamikura,M., Naruse, M., Shan, W. L.: 2008, Development of ALMA Band

8 (385-500 GHz) Cartridge, 19th Int. Symp. on Space Terahertz
Technology, (Groningen, Netherlands, Apr. 28-30, 2008).
Sekimoto, Y., Iizuka, Y., Satou, N., Ito, T., Kumgai, K., Niizeki, Y.,
Fujimoto, Y., Kamikura, M., Naruse, M., Shan, W. L.: 2008,
Evaluation of ALMA Band 8 (385–500 GHz) preproduction
Cartridge #1, East Asia Submillimeter Receiver Workshop,(Taipei, Taiwan, Nov. 18-20, 2008).
Sekimoto, Y., Matsuo, H., Noguchi, T., Uzawa, Y., Hibi, Y.,
Suzuki, T., Endo, A., Naruse, M.: 2008, Development Planof ATC SIS submm camera, East Asia Submillimeter Receiver
Workshop, (Taipei, Taiwan, Nov. 18-20, 2008).
Shan, W.-L., Takeda, M., Kojima, T., Uzawa, Y., Shi, S. -C., Wang,Z.: 2008, Design and Performance of Waveguide Mixers withAll NbN tunnel junctions on MgO substrates, 19th Int. Symp.
on Space Terahertz Technology, (Groningen, Netherlands, Apr.
28-30, 2008).
Shibasaki, K.: 2008, A Driving Mechanism of Temperature
Dependent Plasma Up-Flows in the Solar Corona, The
2nd Hinode Science Meeting - Beyond Discovery Toward
Understanding, (Boulder, Colorado, USA, Sep. 29-Oct. 3, 2008).
Shibasaki, K.: 2008, Leakage of Sub-photospheric Hot Plasma
throught Magnetic Flux Tube, AGU 2008 Fall Meeting, (SanFrancisco, CA, USA, Dec. 15-19, 2008).
Shimajiri, Y., Hiramatsu, M., Tsukakoshi, T., Ikeda, N., Momose,M., AzTEC team: 2008, AzTEC on ASTE: 1.1 mm Survey
toward Lup-I, II, and III, (Helshinki Univ., Finland, Aug. 2008).
Shimajiri, Y., Takahashi, T., Takakuwa, S., Saito, M., Kawabe,
R.: 2008, Observational Evidence for Outflow-Triggered
Star Formation in the OMC-2 FIR3/5 region, The Birth andFeedback of Massive Stars, Within and Beyond the Galaxy,(Charlottesville, USA, Sep. 25-27, 2008).
Shimajiri, Y., Takahashi, T., Takakuwa, S., Saito, M., Kawabe,
R.: 2008, Observational Evidence for Outflow-Triggered Star
Formation in the OMC-2 FIR3/5 region, The 4th Japan-Taiwan
ALMA Science Meeting, (Ibaragi, Japan, Apr. 5-6, 2008).
Shimajiri, Y., Takahashi, T., Takakuwa, S., Saito, M., Kawabe,
R.: 2008, On the triggered star formation in Orion Molecular
Cloud, (Helshinki Univ., Finland, Aug. 2008).
Shimajiri, Y., Takahashi, T., Takakuwa, S., Saito, M., Kawabe,
R.: 2009, Observational Evidence for Outflow-Triggered Star
Formation in the OMC-2 FIR3/4 region, 2nd Tokyo-NRO
Workshop Chemical Diagnostics of Star and Planet Formation,(Univ. of Tokyo, Tokyo, Japan, Mar. 5-6, 2009).
Shimajiri, Y., Yoshida, A., 45m Legacy project team: 2008,
Intermediate Mass Star Formation, ALMA Science WG ISM
Subgroup Meeting, (Univ. of Tokyo, Tokyo, Japan, Apr. 5-6, 2009).
Shimojo, M.: 2008, The relation between the magnetic fields andthe coronal activities in the solar polar region, AGU 2008 Fall
Meeting, (San Francisco, CA, USA, Dec. 15-19, 2008).
Shimojo, M.: 2008, The Relationship Between the Magnetic Field
and the Coronal Activities in the Polar Region, 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Shimojo, M.: 2008, The Relationship Between the Magnetic Field
and the Coronal Activities in the Polar Region, The 2nd Hinode
Science Meeting - Beyond Discovery Toward Understanding,(Boulder, Colorado, USA, Sep. 29-Oct. 3, 2008).

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Shirasaki, Y., et al. including Tanaka, M., Ohishi, M., Mizumoto,Y.: 2008, Application of Information Technologies on Astronomy:
Japanese Virtual Observatory (JVO) Portal, Fifty Years after
IGY, (Tsukuba, Japan, Nov. 12, 2008).
Shirasaki, Y., et al. including Tanaka, M., Ohishi, M., Mizumoto,Y.: 2008, The Japanese Virtual Observatory in action, Astronomical Data Analysis Software and Systems, (Quebec City,
Canada, Nov. 2-5, 2008).
Shitov, S. V., Inatani, J., Shan, W.-L., Takeda, M., Uvarov, A. V.,
Uzawa, Y., Vystavkin, A. N.: 2008, Measurement of emissivityof the ALMA antenna panel at 840 GHz using NbN-based
heterodyne SIS receiver, 19th Int. Symp. on Space Terahertz
Technology, (Groningen, Netherlands, Apr. 28-30, 2008).
Sôma, M., Tanikawa, K.: 2008, Japanese astronomy in the 7th
century, The 6th Int. Conf. on Oriental Astronomy, (Townsvile,
Australia, July 7-11, 2008).
Suematsu, Y.: 2008, Dynamical Nature of Solar ChromosphericFine Structures Revealed with HINODE/SOT, The 2nd Hinode
Science Meeting - Beyond Discovery Toward Understanding,(Boulder, Colorado, USA, Sep. 29-Oct. 3, 2008).
Suematsu, Y.: 2008, Dynamical Nature of Solar Spicules Revealedwith HINODE/SOT, Int. Workshop of 2008 Solar Total Eclipse,(Jiuquan, Gansu, China, Jul. 28-Aug. 5, 2008).
Suematsu, Y.: 2008, Instrument Design and On-Orbit Performanceof the solar Optical Telescope Aboard Hinode (Solar-B), Int.
Conf. on Space Optics 2008, (Médiathèque José-Cabanis,
Toulouse, France, Oct. 14-17, 2008).
Suematsu, Y.: 2008, Nature of Small-Scale Jets On the Solar
Chromosphere Revealed with Hinode, AGU 2008 Fall Meeting,(San Francisco, CA, USA, Dec. 15-19, 2008).
Suematsu, Y.: 2008, Review of Hinode Results, Int. Workshop of
2008 Solar Total Eclipse, (Jiuquan, Gansu, China, Jul. 28-Aug. 5,2008).
Suematsu, Y.: 2009, Evolution and kinematics of mottles – spicules.
Pro and after Hinode, ISSI Int. Research 1st Meeting; Solar
small-scale transient phenomena and their role in coronalheating, (ISSI, Bern, Switzerland, Jan. 19-22, 2008).
Sugitani, K., Tamura, M., Watanabe, M., IRSF/SIRPOL Team:2008, Near-Infrared Polarimetry of the Serpens core, Astronomical Polarimetry 2008, (La Malbaie, Quebec, Canada, Jul.
6-11, 2008).
Sugiyama, K., Sato, M., Nakajima, K., Takeuchi, S., Takahashi, Y.:
2008, Observation of Lightning on Jupiter by a Future Mission,
AGU 2008 Fall Meeting, (San Francisco, CA, USA, Dec.
15-19, 2008).
Sunada, K.: 2009, New maser candidate sources in the AKARIFIS Bright Source Catalogue, 2009 East Asia VLBI Workshop,(Ewha Woman's University, Seoul, Korea, Mar. 18-20, 2009).
Suzuki, R.: 2008, HiCIAO status, SEEDS Science Workshop,(Mitaka, Japan, Sep. 3-4, 2008).
Suzuki, R.: 2009, HiCIAO: High Contrast Instrument for the Subaru
Next Generation, Exoplanets and Disks: Their Formation andDiversity, (Kona, Hawaii, USA, Mar. 9-11, 2009).
Suzuki, T., Kaneda, H., Onaka, T., Shibai, H.: 2009, Power-law
relations between cold and warm dust emission intensities
within nearby galaxies obtained with AKARI Far-Infrared

092

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Surveyor (FIS), AKARI Int. Conf., (Univ. of Tokyo, Tokyo,
Japan, Feb. 16-19, 2009).
Tachihara, K.: 2008, ALMA status, ASTE Science Workshop,(Mitaka, Japan, Dec. 11-12, 2008).
Tachihara, K.: 2008, Early phase of molecular outflow traced
by high-J CO emission, The 5th ALMA Japan-Taiwan science
workshop, (National Tsing Hua University, Taiwan, Dec. 5-6,
2008).
Tachihara, K.: 2008, Near-IR and high-J CO emission from lowmass class 0 objects, Star-formation subworking group meetingfor ALMA of Japan and Taiwan, (Ibaragi, Japan, Apr. 4, 2008).
Tachihara, K.: 2009, East-Asian preparatory activities for ALMAon star formation, ALMA and ELTs: A Deeper, Finer View of
the Universe, (ESO, Garching, Germany, Mar. 24-27, 2009).
Takahashi, K.: 2008, Formation of Intense Flux Tubes by
Convective Collapse in the Emerging Flux Region, 2008 Flux
Emergence Workshop, (Kyoto, Japan, Oct. 6-9, 2008).
Takahashi, K.: 2008, Similarity between the Molecular Loops
in the Galactic Center and the Solar Chromospheric Arch
Filaments, 2008 Flux Emergence Workshop, (Kyoto, Japan,
Oct. 6-9, 2008).
Takahashi, R., Saito, Y.: 2008, Vacuum-system design for thelarge-scale cryogenic gravitational wave telescope (LCGT),
4th Vacuum and Surface Sciences Conf. of Asia and Australia,(Matsue, Japan, Oct. 28-31, 2008).
Takano, S.: 2008, Nobeyama 45m Legacy Project: Line Survey,
The 10th Asian-Pacific Regional IAU Meeting, (Kunming,
Yunnan, Nanjing, China, Aug. 3-6, 2008).
Takeda, M., Kojima, T., Shan, W.-L., Nakayama, S., Saito, A.,
Kroug, M., Uzawa, Y., Wang, Z.: 2008, Current status of NbNbased SIS mixers for ALMA Band 10 development, The 9thWorkshop on SMW Rx Technologies in Eastern Asia, (Taipei,
Taiwan, Nov. 18-20, 2008).
Takeda, M., Shan, W. L., Kojima, T., Uzawa, Y., Saito, S., Fujii,
Y., Li, J., Shi, S. C., Wang, Z.: 2008, Mixing properties
of NbN-based SIS mixers with NbTiN wirings, Applied
Superconductivity Conf., (Chicago, USA, Aug. 17-22, 2008).
Takeda, T.: 2009, About the 4D2U Theater of the National
Astronomical Observatory of Japan, Int. Symp. for Immersive
Science Visualization 2009, (Mitaka, Japan, Mar. 22-23, 2009).
Takeda, Y.: 2008, Precision radial-velocity measurement in thecontext of line-profile variation, 3rd Workshop of Astronomy
with Precise Radial Velocity: Exoplanet Search and Astroseismology, (Jeju, Korea, Aug. 31-Sep. 5, 2008).
Tamura, M., Hashimoto, J., Kandori, R., Kusakabe, N., Nakajima,Y., Saito, H., Sato, Y., Sato, S., Nagata, T., Hough, J.: 2008,
Wide-Field Near-Infrared Polarimetry of Star Forming Regions:
Magnetic Field Structures of the Rho Oph Core, Astronomical
Polarimetry 2008, (La Malbaie, Quebec, Canada, Jul. 6-11, 2008).
Tamura, M., Kandori, R., Kusakabe, N., Nakajima, Y., Hashimoto,J., Sato, Y., Saito, H., Nishimayama, S., Fukue, T.: 2008, Wide
Field Infrared Polarimetry: Dust and Magnetic Field in Star
Forming Regions, AOGS 5th Annual Meeting, (Busan, Korea,
June 16-20, 2008).
Tamura, M.: 2008, Exoplanet science in Japan, Exoplanet Forum,(Pasadena, USA, May 29-30, 2008).

Tamura, M.: 2008, SEEDS project, SEEDS Science Workshop,(Mitaka, Japan, Sep. 3-4, 2008).
Tamura, M.: 2008, YSO category, SEEDS Science Workshop,(Mitaka, Japan, Sep. 3-4, 2008).
Tamura, M.: 2008, Subaru strategic exploration of exoplanets anddisks with HiCIAO/AO188, The 10th Asian-Pacific Regional IAU
Meeting, (Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Tamura, M.: 2009, Concluding Remark, Exoplanets and Disks: Their
Formation and Diversity, (Kona, Hawaii, USA, Mar. 9-11, 2009).
Tamura, M.: 2009, Subaru Explorations of Disks and Exoplanets
so far and "SEEDS", Exoplanets and Disks: Their Formation
and Diversity, (Kona, Hawaii, USA, Mar. 9-11, 2009).
Tamura, Y., GGP Japan Group: 2008, Status of GGP Japan Data
Center, Earth Tides Symp. 2008, IAG, (Jena, Germany, Sep. 1-5,
2008).
Tamura, Y., Omang, O .C. D.: 2008, Long Period Tide Observedat Ny-Alesund, Svalbard, Earth Tides Symp. 2008, IAG, (Jena,
Germany, Sep. 1-5, 2008).
Tanaka, M., Shirasaki, Y., Ohishi, M., Mizumoto, Y., Kawanomoto,S., Yasuda, N., Honda, S.: 2008, Astronomical Researches using
Virtual Observatories, Fifty Years after IGY, (Tsukuba, Japan,
Nov. 12, 2008).
Tanikawa, K., Yamamoto, T., Sôma, M.: 2008, Solar eclipses atsunrise and sunset in the Chunqiu Era, The 6th Int. Conf. on
Oriental Astronomy, (Townsvile, Australia, July 7-11, 2008).
Terazono, J., Tanaka, S., Sakamoto, S., Watanabe, J., Wakabayashi,N.: 2009, Ten Years in Lunar and Planetary Exploration
Outreach: "The Moon Station" Challenge, 40th Lunar andPlanetary Science Conf., (The Woodlands, Texas, USA, Mar.
23-27, 2009).
Toda, M., Yamamoto, M., Abe, S., Shigeno, Y., Maeda, K., Suzuki,
S., Kasuga, T., Higa, Y., Watanabe, J.: 2008, Height Analysesof Short-duration Meteor Trains, AOGS 5th Annual Meeting,(Busan, Korea, June 16-20, 2008).
Tomisaka, K.: 2008, Effect of Magnetic Field in Star Formation,
TIARA Workshop on Radiative Transfer, Chemistry, andNumerical Simulation, (National Taiwan University, Taipei,
Taiwan, July 7-11).
Tomisaka, K.: 2008, Effect of Magnetic Field in Star Formation
Process, The 10th Asian-Pacific Regional IAU Meeting,(Kunming, Yunnan, Nanjing, China, Aug. 3-6, 2008).
Tomisaka, K.: 2008, Observational Visualization: How is a FirstCore Observed?, The 3rd East-Asia Numerical Astrophysics
Meeting, (Nanjing, China, Nov. 10-13, 2008).
Tonooka, H.: 2008, Hinode DVD for Public Outreach, The
2nd Hinode Science Meeting - Beyond Discovery Toward
Understanding, (Boulder, Colorado, USA, Sep. 29-Oct. 3, 2008).
Tsuboi, M., Saito, H., Murata, Y., Kasuga, T., Kimura, K., Ogawa,
H., Ujihara, H., Bushimata, T., Umemoto, T.: 2008, Space
MM-WAVE Telescope of ASTRO-G Satellite, 29th URSI
General Assembly, , (Chicago, USA, Aug. 9-16, 2008).
Tsujimoto, T.: 2008, Chemical Evolution of Omega Centauri fromHe to Ba, Chemical Evolution of Dwarf Galaxies and Stellar
Clusters, (Garching, Germany, Jul. 21-25, 2008).
Tsujimoto, T.: 2008, New insights into the first stars in the Galactic
halo and dwarf spheroidal galaxies, IAU Symp. 255, (Rapallo,

Italy, June 16-20, 2008).
Tsuneta, S.: 2008, Contribution of Yohkoh observations to ourcurrent understanding of solar flares, 37th COSPAR Scientific
Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Tsuneta, S.: 2008, Dynamics of the Solar Atmosphere Revealed,
Solar Variability, Earth's Climate, and Space Environment,(Bozmen, Montana, USA, June 1-6, 2008).
Tsuneta, S.: 2008, Hinode observations of polar fields, 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Tsuneta, S.: 2008, Hinode results on the solar magnetic fields, 37th
COSPAR Scientific Assembly, (Montreal, Canada, Jul. 13-20,
2008).
Tsuneta, S.: 2008, Polar Magnetic Flux and the High Speed Solar
Wind, The 2nd Hinode Science Meeting - Beyond Discovery
Toward Understanding, (Boulder, Colorado, USA, Sep. 29-Oct.
3, 2008).
Tsuneta, S.: 2008, Polar region, quiet Sun and Aflven waves as
observed with Hinode, Magnetic Coupling between the Interiorand Atmosphere of the Sun, (Bangalore, India, Dec. 2-5, 2008).
Tsuneta, S.: 2008, Recent results from Hinode, 37th COSPAR
Scientific Assembly, (Montreal, Canada, Jul. 13-20, 2008).
Tsuneta, S.: 2008, Solar-C mission outline, Solar-C Science
Definition Meeting, (Sagamihara, Japan, Nov. 17-21, 2008).
Tsuneta, S.: 2008, The SOLAR-C Mission, SPD/AGU Meeting,(Fort Lauderdale, Florida, USA, May 27-30, 2008).
Umemoto, T.: 2008, VSOP-2 observations of non-thermal radio
continuum from Young Stellar Objects (YSOs), Space VLBI
Science and the VSOP-2 Mission, (MPIfR, Bonn, Germany,
May 14-16, 2008).
Umemoto, T.: 2009, Concept of VSOP-2 Science Operation
Center (SOC, tentative), 2009 East Asia VLBI Workshop, (Ewha
Woman's University, Seoul, Korea, Mar. 18-20, 2009).
Uraguchi, F., Takato, N., Iwata, I., Koyano, H., Mikami, Y.:
2008, First results from turbulence profiling with SODAR at
Subaru Telescope, SPIE 2008 Astronomical Instrumentation,(Marseilles, France, June 23-28, 2008).
Usui, F., Ishiguro, M., Ishihara, D., Ootsubo, T., Sarugaku, Y.,
Ueno, M.: 2008, 2006 Fragmentation of 73P/SchwassmannWachmann 3, AOGS 5th Annual Meeting, (Busan, Korea, June
16-20, 2008).
Usui, F., Ishiguro, M., Ishihara, D., Ootsubo, T., Ueno, M.: 2009,AKARI observations of Broken Comet 73P/SchwassmannWachmann 3, AKARI Int. Conf., (Univ. of Tokyo, Tokyo,
Japan, Feb. 16-19, 2009).
Uzawa, Y., Kojima, T., Kroug, M., Fujii, Y., Candotti, M., Shan,
W. L., Takeda, M,. Kaneko, K., Shitov, S., Wang, M. J.: 2008,
Development of the 787-950 GHz ALMA Band 10 Cartidge,
33rd Int. Conf. on Infrared, Millimeter, and Terahertz Waves,(California, USA, Sep. 17-19, 2008).
Wada, K.: 2008, Models of ISM on sub-kpc scales: Galactic
central regions and disks, Astrosim: Frontiers in Computational
Astrophysics, (Ascona, Switzerland, July 13-18, 2008).
Watanabe, J., Honda, M., Ishiguro, M., Ootsubo, T., Kadono,T., Sakon, I., Furusho, R.: 2008, What happened in comet
17P/Holmes?, AOGS 5th Annual Meeting, (Busan, Korea, June
16-20, 2008).

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Watanabe, J., et al. including Ishiguro, M., Fujiyoshi, T., Fuse, T.,
Takato, N., Furusho, R.: 2008, Subaru/COMICS Mid-infrared
Observation of Near-nucleus Region of Comet 17P/Holmes at
the Early Phase of the Outburst, Asteroids, Comets, Meteors ACM 2008, (Baltimore, Maryland, USA, Jul. 13-18, 2008).
Watanabe, J., Sato, M.: 2008, Trial for relating meteor shower
activities to parent comet activities, AOGS 5th Annual Meeting,(Busan, Korea, June 16-20, 2008).
Watanabe, T.: 2008, FeXIII density diagnostics for solar coronaland flare plasmas, 37th COSPAR Scientific Assembly,(Montreal, Canada, Jul. 13-20, 2008).
Watanabe, T.: 2008, The Solar-C Mission, NASA Heliophysics
Town Hall Meeting Planning Our Strategy for the Future,(College Park, Maryland, USA, May 19-20, 2008).
Watanabe, T.: 2008, Production of high-temperature plasmas
at the initial phase of a C9.7 flare, The 2nd Hinode Science
Meeting - Beyond Discovery Toward Understanding, (Boulder,
Colorado, USA, Sep. 29-Oct. 3, 2008).
Yamada, Y., Shimokawa, T., Shinomoto, S., Yano, T., Gouda,N.: 2008, JASMINE –Japan Astrometry Satellite Mission for
Infrared Exploration– data analysis and accuracy assessmentwith Kalman filter, Astronomical Data Analysis Software andSystems, (Quebec City, Canada, Nov. 2-5, 2008).
Yamada, Y., Yamauchi, M., Gouda, N., Kobayashi, Y., Tsujimoto,T., Yano, T., Suganuma, M., Nakasuka, S., Sako, N., Inamori, T.:2008, A Star Image Extractor for Small Satellites, The 26th Int.
Symp. on Space Technology and Science, (Hamamatsu, Japan,
June 1-8, 2008).
Yamamoto, M., Toda, M., Higa, Y., Maeda, K., Abe, S., Suzuki, S.,
Watanabe, J.: 2008, Recent Progress of Meteor Train Studies:
Visualization of Upper Atmosphere by Injected Materials,
AOGS 5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Yamamoto, S., Kimura, H., Zubko, E., Kobayashi, H., Wada, K.,
Ishiguro, M., Matsui, T.: 2008, Comet 9P/Tempel 1: Applicationof the Comet Standard Model to Observations of Its Dust, AOGS
5th Annual Meeting, (Busan, Korea, June 16-20, 2008).
Yamazaki, D. G.: 2008, A Strong Constraint on the Neutrino Massfrom the Formation of Large Scale Structure in the Presence of the
Primordial Magnetic Field, 10th Symp. on Nuclei in the Cosmos,(Mackinac Island, Michigan, USA, July 27-Aug. 1, 2008).
Yamazaki, D. G.: 2008, Limiting the Neutrino Mass and thePrimordial Magnetic Field from the Large Scale Structure,
The 7th RESCEU Int. Symp. on Astroparticle Physics andCosmology, (Tokyo, Japan, Nov. 11-14, 2008).
Yasutake, N.: 2008, General Relativistic Compact Stars with
Exotic Matter: Effects of rotation and strong magnetic field,
The 6th Japan-Italy symposium on Heavy-Ion Physics, (Tokai,
Ibaraki, Japan, Nov. 11-15, 2008).
Yokochi, K., Tavrov, A. V., Nishikawa, J., Abe, L., Tamura, M.,
Takeda, M, Kurokawa, T.: 2008, Achromatic characteristics
in 3-D Sagnac interferometer based on geometric phase shift,Conf. on Lasers and Electro-Optics (CLEO), (San Jose, CA,
USA, May 4-9, 2008).
Yoshida, F.: 2008, An Insight into the Solar System History
through the Size Distribution of Jupiter Trojans, NCU seminar,(National Central University, Taiwan, May 27, 2008).

094

II Publications, Presentations

Yoshida, F.: 2008, An insight into the solar system history through thesize distribution of Jupiter’s Trojans, Asteroids, Comets, Meteors ACM 2008, (Baltimore, Maryland, USA, Jul. 13-18, 2008).
Yoshida, F.: 2008, HSC survey for Small Solar system Bodies,
Taiwan-Japan Subaru-HSC Science/Survey Mini Workshop,(ASIAA, Taipei, Taiwan, Dec. 8, 2008).
Yoshida, F.: 2008, Size distributions and total populations of L4and L5 Jovian Trojans, AOGS 5th Annual Meeting, (Busan,
Korea, June 16-20, 2008).
Yoshida, F.: 2009, Asteroid observations at the Maidanakobservatory, Infrared Working Group Winter Workshop and30th Meeting, (Yongpyong, Korea, Feb. 23-24, 2009).
Yoshida, F.: 2009, Photometric Observations of Young Asteroid
Families at Maidanak Observatory, UBAI seminar, (Ulugh Beg
Astronomical Institute, Uzbekistan, Feb. 19, 2009).
Yoshida, F.: 2009, Solar system, Japan-Princeton-Taiwan HSC
Workshop, (Mitaka, Japan, Jan. 17-20, 2009).
Yoshida, F.: 2009, Toward the construction of an Extended Asian
network for the Solar system body observation, East-AsianCore Observatory Association EACOA 2009 Meeting, (ASIAA,
Taipei, Taiwan, Mar. 16-18, 2009).
Yoshida, H.: 2008, Necessary conditions for super-integrability ofHamiltonian systems with homogeneous potential, Dynamics
Days Asia Pacific 5, (Nara, Japan, Sep. 9-12, 2008).
Yoshida, M.: 2008, Strange filamentary structures (“fireballs”)
around a merger galaxy in the Coma cluster of galaxies, The
10th Asian-Pacific Regional IAU Meeting, (Kunming, Yunnan,
Nanjing, China, Aug. 3-6, 2008).
Yoshida, M.: 2009, Extended ionized gas regions around theComa cluster galaxies, Subaru Users Meeting 2008, (Mitaka,
Japan, Jan. 14-16, 2009).
Yoshida, T.: 2008, Effects of Spin-Flavor Conversion in Supernova
Neutrino Signal, The 6th Japan-Italy symposium on Heavy-Ion
Physics, (Tokai, Ibaraki, Japan, Nov. 11-15, 2008).
Yoshida, T.: 2008, Electron Fraction Dependence of Neutrino
Spin-Flavor Conversion in Supernovae, The 7th RESCEU Int.
Symp. on Astroparticle Physics and Cosmology, (Tokyo, Japan,
Nov. 11-14, 2008).
Yoshida, T.: 2008, Neutrino Nucleosynthesis in Supernovae, The
6th Japan-Italy symposium on Heavy-Ion Physics, (Tokai,
Ibaraki, Japan, Nov. 11-15, 2008).
Yoshida, T.: 2008, n-Process in Population III Core-Collapse
Supernovae, 10th Symp. on Nuclei in the Cosmos, (Mackinac
Island, Michigan, USA, July 27-Aug. 1, 2008).
Yoshida, T.: 2008, Supernova Mixing to Reproduce Isotopic Ratios
of Presolar Grains, 10th Symp. on Nuclei in the Cosmos,,(Mackinac Island, Michigan, USA, July 27-Aug. 1, 2008).
Zubko, N., Baba, N., Murakami, N.: 2008, Polarization analysis asa means of detecting exoplanets and measuring their objective
spectra, SPIE 2008 Astronomical Instrumentation, (Marseilles,
France, June 23-28, 2008).