Table of Contents

PrefaceI

Scientific Highlights April 2003

Norio KAIFU
Director General
National Astronomical Observatory of Japan

March 2004 ………………………………………1

II Publications, Presentations ……………………………………………………………46
1. Refereed publications ………………………………………………………………46
2. Publications of the National Astronomical Observatory of Japan …………………59
3. Report of the National Astronomical Observatory of Japan ………………………59
4. Other Publications …………………………………………………………………59
5. Presentations ………………………………………………………………………68

PREFACE
We present the annual report of achievements by NAOJ
through the FY 2003.
Since its successful completion in 2000, the 8.2m aperture
Subaru telescope at Mauna Kea, Hawaii has been released anumber of remarkable observing results such as continuous
renewal of record of the most distant galaxies ever observed,
and detailed structure of proto-planetary disks, etc., as one of
the leading ground-based optical/IR telescopes. The VERA(VLBI Experiment of Radio Astrometry) is accumulating
observational test to achieve super-high spatial resolution forthe long-term program which aims to map the whole our
Galaxy by means of three-dimensional distance measurements of maser sources. The development of SOT, on-board SOLAR-B, a 50-cm aperture space optical telescope for observationsof detailed solar surface structure which will be launched in 2006 by collaboration with JAXA,
is approaching its final stage. The “Four-Dimensional Digital Universe” project which aims toopen a novel means for education, PR and research is attracting a strong public interest. The
NAOJ, a core national institute for astronomy in Japan, has been developing activities in wide
areas based on its unique character as an inter-university research institute including all fieldsof ground based astronomy and related sciences : Details are presented in the text.
A big news in the FY 2003 is the allocation of the 8-year ALMA construction budget for
NAOJ by the Government. From the FY 2004 Japan will join the world-scale cooperative construction of ALMA with Europe and North America toward the full operation from 2011 toopen the unknown part of the universe. One of the important concepts of ALMA is a big jumpin spatial resolution to achieve 0.01 arc-sec in sub-millimeter wavelength region which had
been proposed and developed by Japanese radio astronomers’ community for many years. The
ALMA will conduct cutting-edge observations to reveal the process of planetary formation
around a number of stars shining in the night sky, to develop our understanding of the material
evolution throughout the history of expanding universe, and to find objects and phenomena
which we never know without ALMA.
In 1982 NAOJ (the then Tokyo Astronomical Observatory, University of Tokyo) started theworld-level mm-wave astronomy by establishing of the Nobeyama Radio Observatory
equipped with the 45-m mm-wave telescope and the mm-wave interferometer. At the sametime we started the discussion and development toward the next generation radio telescopes.
The plan firstly based on the idea of large mm-wave interferometer with 30 element antennas(LMA), then had been developed to LMSA (Large MM- and Submm-wave Array) by emphasizing the astronomical importance of the sub-mm wave capability. Now the plan is going to berealized as a huge “world telescope” ALMA by global cooperation . We NAOJ will do our bestfor the successful completion and operation of this exciting project.
The NAOJ started its new history as a member institute of an inter-university research
agency NINS (National Institutes of Natural Sciences) from April 2004. The NINS is a newresearch organization covering wide area of natural sciences; universe, energy, material, lifeand human physiology, and it aims to develop novel fields and activities in the science. Also
such reorganization of research institutes in Japan to independent agencies from organizations

directly belonging to the government aims to add more freedom to operational activities inthose institutes for their scientific research of world level. Based on this viewpoint the NAOJ
started serious discussion from 2001 aiming to construct new internal structure and operation
system for our better activities as a research agency. After two years examination phase theproposal was accepted in September 2003 by the community through the comprehensive discussions, and the NAOJ started its new internal structure and operation system from April 1,
2004. The outlines of the new system are as follows.
1) Adoption of the project system. All observatories, facilities and groups in NAOJ except
the theoretical astrophysics group are defined as “project” with various scales in size and term.
Each project should make its mission, life and leadership clear, and all projects are reviewed
yearly. This is to strengthen and heighten the moral, motives and efficiency for scientificachievements in each project under the limited resources of NAOJ. All the project should bebuilt under the leadership of scientists(bottom-up). Small scale projects to develop novel methods/fields are also encouraged.
2) To ensure the above direction we strengthen the management structure to support director general, renew the personnel management system for research and engineering employee,
and widen the acceptable position of the contracting staff members to make possible to invite avariety of talented people for projects, management, and support.
The NAOJ had achieved a number of successful developments and science in the past two
decades, and had extended cooperative scientific activities with domestic and overseas communities widely. We continue our best efforts to reveal the universe we live, and to serve
humankind in the field of science, technology, education and intellectual adventure.

Director General of NAOJ

I Scientific Highlights(April 2003-March 2004)

1. Interferometer Gravitational Wave Detector TAMA300
Automatic Operation and International Collaboration Run ……………………………………… FUJIMOTO et al. 3
2. Solar-B/Optical Telescope Flight Model is Coming Up …………………………………………… SUEMATSU et al. 4
3. Discovery of a Planetary Companion to the G-type Giant Star HD 104985 ……………………………… SATO et al. 5
4. Discovery of a Large-Scale Structure at Redshift - 5 …………………………………………… SHIMASAKU et al. 6
5. Buried AGNs in Ultraluminous Infrared Galaxies …………………………………………………… IMANISHI et al. 7
6. Compact Nuclear Starbursts in the CfA and 12 nm Seyfert 2 Galaxies …………………………………… IMANISHI 8
7. X-ray Underluminous AGNs in Ultraluminous Infrared Galaxies ………………………… IMANISHI, TERASHIMA 9
8. Ha Impact Polarization Observed in a Gradual Flare……………………………………………………… HANAOKA 10
9. Correlation Tracking Image Stabilizer for Ground-Base Solar Observations …………………………… HANAOKA 11
10. Detection of a Warm Molecular Wind in DG Tauri:a Milestone for Understanding the Mechanism of Mass Accretion and Ejection…………………… TAKAMI et al. 12
11. Universality in the Distribution of Caustics ……………………………………………………………… YANO et al. 13
12. r-Process Abundance Universality and Actinide Cosmochronology …………………………………… OTSUKI et al. 14
13. Subaru/FOCAS Spectropolarimetry of Type Ic Hypernova SN 2003dh/GRB 030329 …………… KAWABATA et al. 15
14. Late-time Spectroscopy of the Interacting Type Ia SN 2002ic:Evidence of a H-rich, Asymmetric CSM… DENG et al. 16
15. SUBARU Deep Spectroscopy of the Very Extended Emission-Line Regionof the Seyfert Galaxy NGC 4388 ………………………………………………………………… YOSHIDA et al. 17
16. VERA Observations of the W49N H 2 O Maser Outburst ……………………………………………… HONMA et al. 18
17. Meteoroid Clusters in Leonids: Evidence of Fragmentation in Space …………………………… WATANABE et al. 19
18. The Distribution of Star-Forming Regions in Luminous Infrared Galaxies ………………………… HATTORI et al. 20
19. Near-Infrared Coronagraphic Imaging of Herbig Ae Star HD 150193A ………………………… FUKAGAWA et al. 21
20. The Collapse and Fragmentation of Magnetized Molecular Cloud– MHD Nested Grid Simulation – ………………………………………………………………… MACHIDA et al. 22
21. An Optical and NIR Search for Brown Dwarfs in the Pleiades Cluster ………………………… NAGASHIMA et al. 23
22. Evolution of DLA Systems From Hierarchical Galaxy Formation Models …………………………… OKOSHI et al. 24
23. Toward General Relativistic Gauge Invariant Nonlinear Perturbation ………………………………… NAKAMURA 25
24. Discovery of Star Formation in Extended HI Gas around NGC 6822 …………………………… KOMIYAMA et al. 26
25. Magnetic Properties at the Footpoints of Hot and Cool Loops ………………………… KATSUKAWA, TSUNETA 27
26. High Resolution Lunar Gravity Anomaly Maps …………………………………………………… SUGANO, HEKI 28
27. Observational Impact of Scattered Light from the Laser Beam of a Laser Guide Star Adaptive Optics…… HAYANO et al. 29
28. The Discovery of Two Lyman a Emitters beyond Redshift 6 in the Subaru Deep Field …………… KODAIRA et al. 30
29. New Methods to Monitor a Satellite-to-Satellite 4-way Link …………………………………………… ASARI et al. 31
30. Development of Ultra Light Weight Mirror for Space and Ground Based Telescopes ……………… KOHARA et al. 32
31. Observation of Solar Flare Hard x-ray Spectra Using CdTe Detectors …………………………… KOBAYASHI et al. 33
32. Hard X-ray Surveys of AGNs :Revealing Formation History of Massive Black Holes in Galaxies ……………………………… AKIYAMA et al. 34
33. Nucleosynthesis of Light Elements and Heavy r-Process Elements throughthe o-Process in Supernova Explosions …………………………………………………………… YOSHIDA et al. 35
34. Oscillations in the Coronal Green-Line Intensity
ˇ ´ and Norikura Nearly Simultaneously ………………………… MINAROVJECH et al. 36
Observed at Lomnicky´ Stit
35. New Clean Room for Space Instrumentation ………………………………………………………… NOGUCHI et al. 37

1

36. Oscillatory Orbits in the Standard Mapping …………………………………………… YAMAGUCHI, TANIKAWA 39
37. Subaru/HDS Studies of Eu Isotope Abundances in Metal-Deficient Stars ………………………………… AOKI et al. 40
38. A New Precession Formula……………………………………………………………………………… FUKUSHIMA 41
39. Formation of the First Stars by Accretion ………………………………………………………… OMUKAI, PALLA 42
40. The Mass Spectrum of Metal-free Stars Resulting from Photodissociation Feedback:
A Scenario for the Formation of Low-mass Population III Stars ……………………………… OMUKAI, YOSHII 43
41. An S0-like Galaxy Found at Redshift 1.5………………………………………………………………………IYE et al. 44
42. Disappearing Dark Matter in Brane World Cosmology:
New Limits on Noncompact Extra Dimensions…………………………………………………………ICHIKI et al. 45

2Interferometer Gravitational Wave Detector TAMA300
Automatic Operation and International Collaboration Run
FUJIMOTO, Masa-Katsu, KAWAMURA, Seiji, YAMAZAKI, Toshitaka
TAKAHASHI, Ryutaro, ARAI, Koji, TATSUMI, Daisuke, FUKUSHIMA, Mitsuhiro
SATO, Shuichi, TSUNESADA, Yoshiki, and the TAMA Collaboration(Division of Astrometry and Celestial Mechanics, NAOJ)

A laser interferometer gravitational wave detector
TAMA300 has performed nine times of data takings (DT)from 1999 up to now. In August 2000, the world's best sensitivity (5 # 10 21 / Hz in strain) was achieved (M. Andoet al. 2001, Phys. Rev. Lett., 86, 3950). The shot noise levelhas been reduced after the implementation of the power
recycling in December 2001, according to which the total
sensitivity of the detector is improved up to
2 # 10 21 / Hz. The observable distance, at which neutronstar binaries with 1.4M9 yield S/N=10, was extended from33kpc to 73kpc. The strain sensitivity of the interferometeris shown in Figure 1. The sensitivity reached the shot noise
limit at the frequencies higher than 1kHz.

with the S3 run of LIGO in USA and GEO600 in Germany.
Green lines indicate the period when the interferometer was
operated and the analyzable data was taken. Total observation time was 558 hours.

Figure2: Operational status of the interferometer in DT9.

Figure1: Strain sensitivity of the interferometer.

Since gravitational wave signals are detectable through24 hours, we had developed an automatic and crew-lessoperation system. The auto lock system recovers the servo
loops to control the interferometer automatically. The programming language has been changed from C to National
Instruments LabVIEW, which enabled to code a complicated sequence with multi-thread easily.
Figure 2 shows the operational status of the interferometer in DT9. This observation was placed as an international collaboration run. The period of the run was coordinatedIn the first half of the run (Nov. 28–Dec. 19, 2003), theinterferometer was operated only in the nighttime except
weekends because of terrible vibrations caused by constructions around the site. The run was interrupted during
Dec. 20–24 due to the power failure. In the latter half (Dec.
25, 2003–Jan. 10, 2004), three times of continuous operations longer than 24 hours were achieved (the longest timewas 28 hours) owing to good environments in the New
Year's holidays. The sensitivity was better than that in thefirst half, and such a sensitivity was kept up. As for the stability and the duty rate of the detector, the automatic operation system shows its ability with the newly complemented
functions such as the automatic adjustment system for theinterferometer, the emergency-call system to expert people
via the mobile phone, the remote operation system, etc. In
the case that the interferometer was not recovered automatically, the expert people called by the mobile phone confirmed the status of the interferometer through the internet
and recovered the interferometer with the remote operation
soon.

3

Solar-B/Optical Telescope Flight Model is Coming Up
SUEMATSU, Yoshinori, ICHIMOTO, Kiyoshi, SHIMIZU, Toshifumi, OTSUBO, Masashi
NAKAGIRI, Masao, NOGUCHI, Motokazu, TAMURA, Tomonori, KATO, Yoshihiro
HARA, Hirohisa, MIYASHITA, Masakuni, TSUNETA, Saku
(NAOJ)KATSUKAWA, Yukio, KUBO, Masahito, SAKAMOTO Yasushi(Univ. of Tokyo)

Integration of flight model Solar Optical Telescope(SOT) is nearly completing, which is to be carried aboard
the JAXA/NAO solar observing satellite SOLAR-B (thelaunch is scheduled in the summer of 2006). The SOT isaiming at observing the solar atmospheric structures, especially solar magnetic structures, with a diffraction-limited
resolution of 0.2 to 0.3 arcsec and polarization accuracy
better than 10- 3 which are difficult to keep during observation with ground-based instruments. The SOT consists of
two separate optical structures: the Optical Telescope
Assembly (OTA) being manufactured in Japan and the
Focal Plane Package (FPP) by NASA, USA. The OTA is
made of an aplanatic Gregorian telescope of 50 cm effective aperture and other indispensable auxiliary optical components such as a heat dump mirror, a secondary field stopmirror, a collimataing lens unit, a polarization modulation
unit and a tip-tilt mirror for image stabilization.
The integration of OTA-FM started in November, 2003,
in a newly-built clean room of NAOJ. The framework of
OTA was a truss of CFRP which had been used and provedin a proto-model OTA. Flight model optical components
were individually examined and demonstrated optical performance better than allocated optical error budgets. Then,assembly and fine alignment of optical components on thetruss were carried out by using the method well-establishedin the proto-model integration. As a result, the opticalassembly was successful; OTA has small optical (coma anddefocus) aberration enough to be acceptable for diffractionlimited performance in zero-gravity condition, which wasestimated by the average of both measurements in OTA
pointing upward and downward.
In the next, we are performing opto-thermal test inwhich OTA is put in a vacuum chamber and given temperature distributions expected on orbit. The purpose of thistest is to confirm that additional wavefront error and defocus due to thermal deformation of structure are in acceptable ranges. Furthermore, end-to-end optical tests for OTA
combined with FPP is planned in the summer of 2004 by
actual sun observations. The sunlight can be fed to SOT in
the clean room of NAOJ by a 90 cm heliostat installed on
the roof in October, 2003.
Upon the integration, we have been much cautious in
all the contaminant doubtful materials and spent considerable time in selection of low outgassing material, grease4

removing cleanings and baking out of most structure materials except for optical components, because contaminationof optical surfaces and resulted degradation of photon
through-put are one of the most crucial for the success ofthe telescope. Since assembly of deployment mechanisms
for two doors (top-door at telescope entrance and side-doorat heat dump window) and installation of heaters and temperature sensors are progressing satisfactorilly, final integration will be completed in the summer of 2004.

Figure1:OTA-FM is being hoisted out of an integration tower intoanother support frame for installation of heaters, temperature
sensors, cables, and envelopes after the initial optical assembly
and test (in the clean room of NAOJ).

Figure2:Upside-down OTA-FM is being hoisted down to lower part ofa vacuum chamber for opto-thermal test (in the clean room ofNAOJ).
References[1] Suematsu, Y.: 2003, Solar-B: Status of Project, The Proc. of the IAU
8th Asian-Pacific Regional Meeting, ASP Conf. Proc., 289, 37–44.

Discovery of a Planetary Companion to the G-type Giant StarHD 104985
SATO, Bun'ei, ANDO, Hiroyasu, TAKEDA, Yoichi, NOGUCHI, Kunio(Division of Optical and Infrared Astronomy, NAOJ)

KAMBE, Eiji
(National Defense Academy)IZUMIURA, Hideyuki, MASUDA, Seiji, WATANABE, Etsuji, KOYANO, Hisashi
MAEHARA, Hideo, NORIMOTO, Yuji, OKADA, Takafumi, SHIMIZU, Yasuhiro
YANAGISAWA, Kenshi, YOSHIDA, Michitoshi(Okayama Astrophysical Observatory, NAOJ)

WADA, Setsuko(The University of Electro-Communications)

OKADA, Norio

URAGUCHI, Fumihiro(Advanced Technology Center, NAOJ)(Subaru Telescope, NAOJ)

We have carried out a precise Doppler survey of G-type
giants in order to search for planets around intermediatemass stars (1.5 + 5M 9) and to understand the formationand evolution of planetary systems around them. G-type
giants are slow-rotators and have many sharp lines in theirspectra and their surface activities are relatively low in contrast to their younger counterparts on the main-sequence,
which would allow us to detect planets around them by precise radial velocity measurements. We are now monitoring
about 300 G–K giants using HIgh Dispersion Echelle
Spectrograph (HIDES) and an iodine absorption cell at
Okayama Astrophysical Observatory. In this article, wereport the first result from our survey, the discovery of aplanetary companion around G-type giant star HD 104985(G9III). This is the first planetary candidate around G-type
giants and the third one around evolved giants.
The radial velocity of HD 104985 has been monitored
since 2001 March, and it is found to show a large variation
with a significant periodicity. The variability can be wellfitted by a nearly circular orbit with a period
P = 198.2 ! 0.3 days, a velocity semiamplitude
K 1 = 161 ! 2 m s 1, and an eccentricity e = 0.03 ! 0.02
(Fig.1). Since HD 104985 is identified as a photometricallystable star from the Hipparcos measurements and theobserved period is at least 2 orders of magnitude larger
than expected in the case of radial pulsation, it is unlikelythat rotational modulation or pulsation is the cause of thevariability. Adopting a stellar mass of 1.6M 9, we obtain forthe companion a mass m 2 sin i = 6.3M J and a semimajor
axis a = 0.78 AU (Fig.2). A probable upper limit of 3 M 9
to the stellar mass yields m 2 sin i = 9.6 M J, which still falls
within the planetary mass regime. The estimated primary
mass of 1.6 M 9 for HD 104985 corresponds to a progenitor
with spectral type from early F to late A on the main

sequence. The surrounding disks of such massive stars may
have lifetimes shorter than those of lower mass stars, andthe existence of gas giant planets around such stars would
constrain the time scale and mechanism of giant planet formation.

Figure1:Observed radial velocities of HD 104985 (dots). The Keplerian
orbital fit is shown by the solid line. The rms deviation to thefit is 23.5 m s 1.

Figure2:Artist’s concept of the planetary system around HD 104985
compared with the solar system.

References[1] Kambe, E. et al.: 2002, PASJ, 54, 865.
[2] Sato, B. et al.: 2003, ApJ, 597, L157.

5

Discovery of a Large-Scale Structure at Redshift - 5
SHIMASAKU, Kazuhiro, OUCHI, Masami, OKAMURA, Sadanori, DOI, Mamoru,
KIMURA, Masahiko, MIYAZAKI, Masayuki, SEKIGUCHI, Maki
(University of Tokyo)

KASHIKAWA, Nobunari,KAWABATA, Koji,YAGI, Masafumi, YAMADA, Toru, YASUDA, Naoki(NAOJ)

FURUSAWA, Hisanori, KOMIYAMA, Yutaka, MIYAZAKI, Satoshi, OHYAMA, Yoichi(Subaru Telescope, NAOJ)

HAMABE, Masaru(Japan Women's University)

HAYASHINO, Tomoki, MATSUDA, Yuichi, SHIOYA, Yasuhiro, TAMURA, Hajime,TANIGUCHI, Yoshiaki(Tohoku University)

KODAIRA, Keiichi

NAKATA, Fumiaki

OHTA, Kouji(SOKENDAI)(University of Durham)(Kyoto University)

Figure1:Two-color diagrams for continuum color (R-i) and narrowband
excess color (Ri-NB711), where Ri / (R + i)/ 2 is a continuum magnitude. Left panel: Tracks of model galaxies at different redshifts. The red lines indicate model LAEs, while theother lines are for foreground galaxies (z # 2). The yellow starmarks show Galactic stars. Right panel: Colors of the detected
objects. The large circles indicate 43 LAE candidates, among
which the red ones have spectroscopic observations while thesmall dots are for the other objects. Our LAE selection criteria
are outlined by a pink line.

The formation and evolution of the large-scale clustering of galaxies, as seen in the present-day universe, arecentral issues in cosmology. Observations of galaxy clustering in the distant universe give us great clues to thisissue, including how galaxies were formed in the underlying dark matter.
Here we report the discovery of a large-scale structureof Lyman a emitting galaxies (LAEs [1]) at z = 4.86 basedon wide-field imaging with Suprime-Cam on Subaru [2].
We observed a 30l# 45l area of the Subaru Deep Field in anarrow band (NB711, m C =7126Å and FWHM=73Å)together with the R and il bands. We isolate from these data
43 LAE candidates down to NB711 = 25.5 mag using color
criteria (Fig.1). Follow-up spectroscopy of five of the 43
candidates suggests that the contamination by low-z objects
is + 20%.
We find that the LAE candidates are clustered in an
elongated region on the sky of 20Mpc in width and 50 Mpc

6

Figure2:Sky distribution of 43 LAE candidates. Areas of relatively
poor quality have been trimmed. Brighter candidates areshown by larger circles. The dotted, dashed, and solid lines
correspond to contours of a surface overdensity of 0, 1, and 2,
respectively.Five objects with spectroscopic redshifts aremarked with A - E.

in length at z=4.86 (Fig.2), which is comparable in size topresent-day large-scale structures (we adopt). This elongated region includes a circular region of 12Mpc radius of ahigher surface overdensity (d v = 2), which may be theprogenitor of a present-day cluster of galaxies.
Assuming this circular region to be a sphere with a spatial overdensity of 2, we compare our observation with predictions by Cold Dark Matter models. We find that an
X 0 = 0.3 flat model with v 8 = 0.9 predicts the number ofsuch spheres consistent with the observed number if thebias parameter of LAEs is as high as b - 6. This value suggests that the typical mass of dark haloes hosting LAEs at
z - 5 is of the order of 1012 M 9. Such a large mass poses aninteresting question about the nature of LAEs.
References[1] Hu, E. et al.: 1998, ApJ, 502, L99.
[2] Shimasaku, K. et al.: 2003, ApJ, 586, L111.

Buried AGNs in Ultraluminous Infrared Galaxies
IMANISHI, Masatoshi

MALONEY, Philip(Division of Optical and Infrared Astronomy, NAOJ)(University of Colorado)

TERASHIMA, Yuichi, ANABUKI, Naohisa, NAKAGAWA, Takao(ISAS)

Ultraluminous infrared galaxies (ULIRGs), discovered
with the IRAS all sky survey, radiate very large luminosities (L > 1012 L 9) as infrared dust emission, and thus possessextremely powerful energy sources hidden behind dust.
High-redshift ULIRGs dominate the cosmic infrared background emission, and so have been used to trace the dustobscured star formation rate, dust content, and metallicity
in the early universe, by assuming that these ULIRGs are
powered by starburst activity. However, the most important
issue, namely, whether the dominant energy sources of
ULIRGs are starbursts or dust-obscured AGNs, is still
unclear.
If powerful AGNs are present and obscured by dust in a
torus geometry, their signatures are easily detectable,
because a large amount of AGN's radiation escapes along
the torus axis. However, since nuclear regions of ULIRGs
are very dusty, AGNs resident in the majority of ULIRGs
may be deeply embedded in dust along all sightlines. It isfundamental to detect such buried AGNs and quantitatively
determine their energetic importance. For these purposes,
observations at wavelengths of low dust extinction are
clearly a powerful way. One of such wavelengths is thermal infrared 3–4 nm. Extinction at 3–4 nm is as low as thatat 5–13 nm. Furthermore, starburst and AGN emission are
clearly distinguishable based on the spectral shapes; A starburst always shows strong 3.3 nm Polycyclic Aromatic
Hydrocarbons (PAH) emission, while if the equivalent
width of the 3.3 nm PAH emission is substantially smaller
than that of a starburst, and strong dust absorption features
are also detected, then a powerful buried AGN is required.
Finally, in a starburst, the energy sources and dust shouldbe spatially well mixed, while the energy source is more
centrally concentrated than the dust in a buried AGN. In theformer case (starburst), there are upper limits to the opticaldepths of dust absorption features at 3–4 nm, but they canbe large in the latter case (buried AGN) [1].
Using these methods, we have succeeded in providing
strong evidence for buried AGNs, which had previously
been undetected with other methods, in several ULIRGs,
and in quantitatively determining the energetic importanceof buried AGNs (Figure 1). The presence of a powerful
AGN in a bright ULIRG, UGC 5101, has been confirmedwith subsequent X-ray observations (Figure 2), clearlydemonstrating the reliability of our 3–4 nm spectroscopic
energy diagnostic method [2].

Figure1:3-4 nm spectra of two ULIRGs that show strong evidence ofburied AGNs (UGC 5101 and IRAS 00188–0856). The equivalent widths of the 3.3 nm PAH emission is significantly weaker than those of starbursts, and 3.1 nm absorption by ice-covered dust (below the dashed continuum line) as well as 3.4 nm
absorption by bare dust (below the solid continuum) are detected. The large optical depths of these absorption features areincompatible with a starburst, but favors a buried AGN. Since
3–4 nm continuum is dominated by hot dust with T + 1000K
at the innermost part of the surrounding dust, these opticaldepths probe dust column toward the buried AGNs.We foundthat the dereddened AGN luminosities could account for thebulk of the infrared luminosities of these ULIRGs.

Figure2:X-ray spectrum of UGC 5101 obtained with XMM. In theupper panel, the higher and lower plots are EPIC PN and MOS
spectra, respectively. Soft X-ray emission at 0.5–2 keV is dominated by thermal emission from starbursts. At >3 keV, a clear
excess above the thermal emission is recognizable, which isinterpreted as emission from a buried AGN. The absorptioncorrected AGN luminosity is sufficiently large, as was estimated from the thermal infrared 3–4 nm spectrum.

References[1] Imanishi, M., and Maloney, P. R.: 2003, ApJ, 588, 165.
[2] Imanishi, M. et al.: 2003, ApJ, 596, L167.

7

Compact Nuclear Starbursts in the CfA and
12 nm Seyfert 2 Galaxies
IMANISHI, Masatoshi(Division of Optical and Infrared Astronomy, NAOJ)

According to the current unification paradigm of active
galactic nuclei (AGNs), Seyfert 2 galaxies (which do notshow broad optical emission lines) are believed to contain
AGNs obscured behind dusty tori. Since the dusty tori arerich in molecular gas, they are plausible sites for starbursts
to occur. However, the true nature of these starbursts is still
unclear. To understand the properties of the compact (<300pc in size) nuclear starbursts, by disentangling from extended star-formation activity in host galaxies, slit spectroscopy
is effective.
In particular, 3–4nm slit spectroscopy can provide an
excellent tool not only for detecting the compact nuclear
starbursts, but also for making quantitative estimates of
their luminosities. First, the 3.3 nm polycyclic aromatichydrocarbon (PAH) emission feature is detected only in
starbursts and not in AGNs, making its luminosity a goodmeasure of starburst activity. Second, the 3.3 nm PAH
emission from starbursts is intrinsically so strong that thesignatures of even weak compact nuclear starbursts aredetectable in normal (S/N + 20) spectra. Third, the effectsof dust extinction are much lower than at shorter wavelengths, and in a few selected Seyfert 2 galaxies, it has
actually been confirmed that the magnitudes of the compact
nuclear starbursts are reasonably quantifiable from theobserved (not extinction-corrected) 3.3nm PAH luminosities [1].
We have applied this successful 3–4 n m slit spectroscopy to 32 Seyfert 2 galaxies in the CfA and 12nm
samples (Figure 1), and found the following main conclusions, based on this statistically meaningful sample number[2].
(1) The signatures of the nuclear starbursts were detected in one-third of the observed Seyfert 2 galaxies.
However, in the majority of them, the equivalent widths ofthe 3.3nm PAH emission feature were much smaller thanthose observed in starburst galaxies, suggesting that the
3–4 nm fluxes are dominated by AGNs and not by the
nuclear starbursts.
(2) The 3.3nm PAH to infrared dust emission luminosity ratios were so small that the compact nuclear starbursts
contribute only insignificantly to the infrared luminosities
of Seyfert 2 galaxies.
(3) The 3.3nm PAH emission luminosities were statistically correlated with some indicators of AGN powers;
IRAS 12nm and 25nm luminosities, and nuclear N -band (m= 10.6nm) luminosities (Figure 2). These correlations are
consistent with some theoretical models predicting that thepresence of the nuclear starbursts in the torus can enhance8

the mass accretion rate onto a central supermassive blackhole, and thereby increase the AGN luminosity.
(4) Dust absorption features at 3.1nm (by ice-covereddust) and 3.4nm (by bare dust) were generally weak, suggesting that dust extinction toward the 3–4nm continuum
emitting hot (1000K) dust at the innermost part of the torus
is relatively modest, AV <50-60 mag.

Figure1:Examples of 3–4nm spectra of Seyfert 2 nuclei. The abscissa isobserved wavelength in nm, and the ordinate is Fm in 10 15 W
m 2 nm 1. The left source shows a clear 3.3nm PAH emission
feature, while the spectrum of the right source is nearly featureless, with no detectable 3.3nm PAH emission.

Figure2:The ordinate is the 3.3nm PAH emission luminosities measured in our slit spectra and reflects the absolute magnitudes of
the compact nuclear starbursts. The abscissa is some luminosities that are thought to trace AGN powers. (a) IRAS 12nm
luminosities. (b) IRAS 25nm luminosities. (c) Nuclear N-band
luminosities measured with ground-based aperture (<10 arcsec)
photometry. In all the plots, statistical correlations are found,suggesting that AGN and nuclear starbursts are physicallyclosely related.
References[1] Imanishi, M.: 2002, ApJ, 569, 44.
[2] Imanishi, M.: 2003, ApJ, 599, 918.

X-ray Underluminous AGNs in Ultraluminous Infrared Galaxies
IMANISHI, Masatoshi

TERASHIMA, Yuichi(Division of Optical and Infrared Astronomy, NAOJ)(ISAS)

Ultraluminous infrared galaxies (ULIRGs) radiate
quasar-like luminosities (> 1012 L 9) as infrared dust emission, and thus possess extremely powerful energy sources
hidden behind dust. Estimating what fraction of theinfrared luminosities are powered by starburst and AGN
activity individually is important to understand the dustobscured AGN–starburst connections.
To estimate an AGN contribution, an indicator which
can trace AGN power, by disentangling from star-formation activity, is required. Two useful indicators currently
known are (1) broad hydrogen emission lines in the opticaland near-infrared domains and (2) X-ray emission at E >2keV. First, broad emission lines whose line widths arelarger than 1500km s 1 in full-width at half maximum(FWHM) are believed to originate in high-velocity gas
around an AGN, but are difficult to be produced with phenomena related to star formation. Next, 2–10 keV emission
from an AGN is much stronger than star-formation. In
many optically-selected dust-unobscured type-1 AGNs, theluminosities between 2–10 keV and broad line emission are
correlated. If this correlation holds also for ULIRGs, thenboth of these indicators can be used to estimate the contributions from AGNs to the infrared luminosities of ULIRGs.
Although putative AGNs in the majority of ULIRGs are
deeply buried in dust and gas, some fraction of ULIRGs
happen to possess modestly dust obscured AGNs along ourline-of-sight and show detectable near-infrared broad emission lines. If X-ray absorption is also modest(N H < 10 24 cm 2) toward the AGNs in these ULIRGs, thenwe can detect direct 2–10keV X-ray emission from theAGNs and thus estimate absorption-corrected X-ray luminosities with sufficient accuracy. We have performed X-ray
observations of ULIRGs with such modestly-dust-obscured
AGNs (Figure 1) and compared their 2–10keV to broadline luminosity ratios with optically-selected type-1 AGNs
[1]. We found that in ULIRGs the absorption-corrected
2–10keV luminosities are underluminous by an order ofmagnitude, with respect to the broad line luminosities(Figure 2). Based on some independent energy diagnostic
methods, it is more likely that the AGNs in ULIRGs areunderluminous in X-rays with respect to their overall spectral energy distributions, than that their broad lines areoverluminous.
Possible reasons for the X-ray underluminosity include(1) at the dusty nuclear regions of ULIRGs, X-ray emission
from AGNs is significantly suppressed for some reasons,(2) the detected 2–10 keV emission suffer from partial

absorption by foreground compact (smaller than the X-ray
emitting regions), clumpy, and Compton-thick(N H > 10 24 cm 2) material, and (3) the 2–10 keV emission
we detected is not directly transmitted components fromthe AGNs, but is scattered components by ionized gas. In
any case, estimated AGN contribution from the observed
2–10keV spectra will substantially underestimate the actual
AGN luminosities in ULIRGs. There are some ULIRGs,
which are consistently suggested to be AGN-powered bysome independent methods, but are argued to be starburstpowered from X-ray observations due to weak X-ray emission. This contradiction may come from the X-ray underluminosity from AGNs in ULIRGs.

Figure1:X-ray spectra of two ULIRGs with detectable broad emission
lines (Mrk463 and IRAS 05189-2524), obtained with XMM.
In the upper panel, the upper and lower plots are EPIC PN and
MOS data, respectively. In both sources, spectral excess at E L
2 keV is attributed to the X-ray emission from the AGNs, andabsorption is estimated to be N H < 3 # 10 23 cm 2.

Figure2:Comparison between absorption-corrected 2–10keV X-ray
luminosity (ordinate) and extinction- uncorrected broad optical
Ha emission line luminosity (abscissa). Open circles are optically-selected type-1 AGNs. Filled squares are ULIRGs, whose
locations are systematically at the lower-right side of the type1 AGNs. For ULIRGs, the optical Ha luminosities are estimated with a conservative case-B theory, so that the actual positions should be even righter than the current plots.
Additionally, while dust extinction of broad lines are negligible
in type-1 AGNs, that may be significant in ULIRGs. If we correct for this dust extinction correction, the plots of ULIRGs
will move even to the right, increasing their deviations fromthe type-1 AGNs.
References[1] Imanishi, M., and Terashima, Y.: 2004, AJ, 127, 758.

9

H Impact Polarization Observed in a Gradual FlareHANAOKA, Yoichiro(Division of Radio Astronomy, NAOJ)

Figure1:The Solar Flare Telescope and the layout of the H
ter including the rotating waveplate modulator.

polarime-

Linear polarization of chromospheric lines including
the H line observed in solar flares is interpreted as impact
polarization. The impact polarization is produced by accelerated high-energy particles, which precipitate into thechromosphere. Protons are preferable to produce the impact
polarization, because they have heavy mass and easily penetrate into the chromosphere. Therefore, observations ofimpact polarization gives a rare chance to detect protons insolar flares, and have been considered to be very importantfor studying protons in solar flares.
There are some former observations of impact polarization. However, compared with the abundance of hard X-ray
observations, polarization observations are few, and the
behavior of protons in flares is not yet clear. Therefore, we
installed a polarimeter into the H imager of the Solar
Flare Telescope at Mitaka, which is operated by theDivision of Solar Physics. As shown in Figure 1, a rotating/2 waveplate is placed just before the H Lyot filter. The
images taken with the CCD camera are integrated in realtime, and polarization image sets are taken every 4s.
Therefore, high-cadence imaging polarimetry in the H line
became possible with this polarimeter. We started a regularobservation with this polarimeter to obtain a number ofsamples of impact polarization observations in 2002 July.
We carry out not only the polarimetry, but also the highcadence imaging at the H center and the H off-band
imaging for the Doppler velocity analysis.
Among the flares observed so far, a C5.8 flare on 2002
October 14 showed a particularly significant linear polarization [1]. This flare is a gradual one, which was accompanied by a filament eruption [Figures 2(a) and 2(b)]. The
maximum degree of polarization of this flare exceeds 1%,
and the orientation of the polarization is approximately per-10

Figure2:Images of the flare on 2002 October 14 and a polarization map
and a Dopplergram. (a) A pre-flare image showing the filament before the eruption. (b) The two-ribbon flare occurring
after the filament eruption. The contours show the hard X-ray
source observed with the RHESSI. (c) A polarization map(left-side) and a Dopplergram (right-side) of the region indicated by a rectangle in panel (b). Ticks in the polarization maps
show the orientation and the degree of the polarization. In the
Dopplergram, white patches in the flare ribbon correspond to
the red shift.

pendicular to the flare ribbons, as shown in Figure 2(c).
These results can be explained with the assumption that theobserved polarization is impact polarization produced byaccelerated protons. Downward motion of the H emitting
layer of the flare kernels, which is generally accepted as thereaction to the chromospheric evaporation, was also
observed. Both the polarization and the downward motion
show the tendency that they exhibit a significant signal during the rise phase of kernel brightenings. This fact suggeststhat not only the downward motion but also the polarization is closely related to the heating agent of the chromosphere. The hard X-rays observed by the Reuven Ramaty
High Energy Solar Spectroscopic Imager (RHESSI) show athermal component, which corresponds to the loop-top
high-temperature source shown in Figure 2(b), but there isno detectable power-law component due to accelerated
electrons. Therefore, protons are presumed to be not only
the cause of the polarization, but also a possible candidateof the principal heating agent in this flare, which lacks
high-energy electrons.
Reference[1] Hanaoka, Y.: 2003, ApJ, 596, 1347.

Correlation Tracking Image Stabilizer for
Ground-Base Solar Observations
HANAOKA, Yoichiro(Division of Radio Astronomy, NAOJ)
X-Spectrum
1.0000

X-Amplitude

0.10000.01000.00100.0001
1

10
X-Frequency (Hz)100

Y-Spectrum
1.0000

Y-Amplitude

0.10000.01000.00100.00011

Figure1:Red line: Motion of the stabilized sunspot image (residual errorof the correlation tracking) for 1000 frames, which corresponds
to about 1s. Black lines: Motions of non-stabilized sunspot
images. Two cases are shown with solid and dotted lines.
Upper and lower panels show the motion along the x- and yaxes, respectively. The sunspot image used for the experimentis shown in the inset.

Image stabilizers and adaptive optics systems are now
under operation in many ground-base solar telescopes toremove the seeing effect. In both types of the systems,
optical components are actively controlled on the basis of
the image displacement signals.
In the solar observation, the image displacement should
be calculated by the correlation calculation between the reference image and the live image. The live image is shifted
step by step, and the displacement which gives the maximum correlation is searched. The huge amount of the correlation calculation was the biggest problem in the correlation tracking of the solar observation. However, personal
computers (PCs) nowadays have enough performance tocarry out the correlation calculation with a sufficiently highrate. Therefore, the combination of a PC and our real time
software system for solar observation can realize the correlation tracking system.
We have developed a image stabilizing system based on
the real-time correlation tracking with a high-speed CCD
camera, of which the frame rate is 955 frames s 1. In thissystem, the image displacement is calculated in every
frame and a plane mirror attached on a piezo tilt-mount is
controlled to cancel the displacement. An example of thecomparison between the motion of the non-stabilized
image for 1s and the (residual) motion of the stabilized
image is shown in Figure 1. The striking effect of the10
Y-Frequency (Hz)100

Figure2:Spectra of the motion of the sunspot in the stabilized (red lines)
and the non-stabilized cases (black lines). The spectra of the xand y-motions are shown in the upper and the lower panels.

image stabilization can be seen. The residual RMS fluctuation of the stabilized image is only 0.08 pixel (1pixel corresponds to 1 square-arcsec), while the non-stabilized image
wobbles within several arcseconds. The spectra of theimage motions are shown in Figure 2. The image motions
up to several tens of hertz are suppressed by the image stabilization. Figures 1 and 2 show the behavior of the image
stabilizer for only 1s, but our image stabilizing software
can be used for the long-duration automatic tracking. The
reference image is renewed every 10s, and in the case oftroubles such as the cloud passing and the piezo mountreaching the limit, the mirror automatically returns to theorigin and the tracking is resumed.
As mentioned above, the correlation tracking technique
is common in the image stabilizer and the adaptive optics.
Then we construct an experimental Shack-Hartmann sensor
with the same CCD camera with 955 frames s 1 to evaluate
the performance of a PC as the controller for the adaptive
optics. Even though the PC used for the evaluation is not a
new one (Pentium III 1.2 GHz), it can carry out the correlation tracking calculation for 4#4 subapertures of the ShackHartmann image with the rate of 955 frames s 1. In thecase of the half frame rate, the number of subapertures
increases to 6#6. This result indicates that a low-orderadaptive optics systems, which is under operation in someof the solar observatories, can be easily realized with oursoftware system and a faster PC. Now we are developing
an adaptive optics system for solar observations.

11Detection of a Warm Molecular Wind in DG Tauri: a Milestone for
Understanding the Mechanism of Mass Accretion and Ejection
TAKAMI, Michihiro, CHRYSOSTOMOU, Antonio

RAY, P. Thomas(University of Hertfordshire)(Dublin Insitute for Advanced Studies)

DAVIS, Christopher

DENT, R. F. William(Joint Astronomy Centre)(Royal Observatory of Edinburgh)

BAILEY, Jeremy

TAMURA, Motohide, TERADA, Hiroshi(Anglo-Australian Observatory)(National Astronomical Observatory of Japan)

Jets/outflows in a variety of objects are associated withaccretion disks. Among such objects ranging from X-ray
binaries to quasars, young stellar objects (YSOs) provide
the most easily observable examples. Indeed, many YSOs
exhibit beautiful collimated jets at optical-IR wavelengths,
and energetic molecular outflows at radio wavelengths.
Understanding the mechanism of mass accretion and ejection in these systems is one of the fundamental open problems in contemporary astrophysics.
Accretion cannot proceed unless excess angularmomentum is removed from surrounding materials, andthere is growing evidence that the jet/outflow plays animportant role for this process. Popular magneto-hydrodynamic models (magneto-centrifugal wind models) explain
this physical link as follows; Magnetic and centrifugal
forces act together to launch the jet/wind along magnetic
field lines from the accretion disk, or interface between
stellar magnetosphere and circumstellar disk. The magnetic
field lines act as solid wires close to the star, and rotate
together with the circumstellar disk. These accelerate theflow particles outwards and upwards in a `bead-on-a-wire'fashion. In this way angular momentum is channeled awayfrom the disk through the outflow. This fascinating picture
cannot easily be tested, since the process should occur onvery small scales, which neither the Hubble Space
Telescope (HST) nor adaptive optics on Subaru can resolve
directly.

Figure1:Near-IR H 2 emission in DG Tauri observed at 8.2-m Subaru[1]. The emission features are blueshifted by 15 km s 1 fromthe systemic velocity, indicating that the observed emission isassociated with outflowing gas. The asterisks indicate photospheric absorption features. Our seeing-limited observations
show that the 1-0 S(1) emission is offset by 0 .2 from the star
towards the extended jet, and a typical width of +0 .6 perpendicular to the jet. Correcting the inclination to the line of sight,
these indicate a flow length and width of +40 and +80AU,
respectively. The line flux ratios indicate an excitation temperature of +2000K.

˝

12

˝

Figure2:Centroidal velocities of emission features observed across the
DG Tau outflow. The data for forbidden line emission wereobtained with the Hubble Space Telescope by Bacciotti etal.[2]. The dots for molecular hydrogen are based on ourSubaru data. The figure suggests that the H2 and forbidden line
emission originate from different components of the same
flow, i.e., a fast and partially ionised component near the axis
and a slow molecular component surrounding it.

These models predict the presence of poorly collimatedstreamlines surrounding a well-collimated jet. In otherwords, a collimated jet observed at optical-IR wavelengths
may be only a limited portion of the entire flow close to theoutflow axis. The presence of an ''unseen'' wide-angled
component has been suggested by the presence of a cavity
in the molecular envelope, shock-heated molecular hydrogen along a cavity wall, a broad range of morphology ofmolecular bipolar outflows, and so on. Direct detection ofsuch a flow component is desired to test the validity of theabove models, and also understand the nature of molecularbipolar outflows.
The large diameter of Subaru and the high sensitivity of
its infrared spectrograph (IRCS) allowed us to detect molecular hydrogen emission associated with a missing wideangled wind. Fig. 1 shows the spectra of H 2 emission
observed in DG Tauri, one of the most active T Tauri stars
known. These emission lines exhibit a blueshifted line profile and spatial extension towards the extended jet, indicating that the emission is associated with outflowing gas.
(Absence of redshifted emission is explained by obscuration of the counterflow by a circumstellar disk.) As shownin Fig. 2, the observed velocity and spatial scale are well
explained if we regard this flow component as an outerextension of the kinematic structure observed in forbiddenline outflow. This indeed agrees with model predictions of
the magneto-centrifugal wind scenario.
References[1] Takami, M. et al.: 2003, A&A, 416, 213.
[2] Bacciotti, F. et al.: 2002, ApJ, 576, 222.

Universality in the Distribution of Caustics
YANO, Taihei, KOYAMA, Hiroko, BUCHERT, Thomas, GOUDA, Naoteru(NAOJ)

We numerically investigate the long–time evolution ofdensity perturbations after the first appearance of caustics
in an expanding cosmological model with one–dimensional‘single–wave’ initial conditions. Focusing on thetime–intervals of caustic appearances and the spatial distribution of caustics at subsequent times, we find that thetime–intervals of caustic appearances approach a constant,i.e., their time–subsequent ratio converges to 1; it is also
found that the spatial distribution of caustics at a given timefeatures some universality rules, e.g., the ratio between theposition of the nearest caustic from the center and that of
the second nearest caustic from the center approaches aconstant. Furthermore we find some rules for the mass distribution for each caustic. Using these universality constants we are in the position to predict the spatial distribution of caustics at an arbitrary time in order to give an estimate for the power spectral index in the fully–developed
non–dissipative turbulent (‘virialized’) regime.
We have argued that the system of caustics displays
some universality, after some time, with respect to regularity of time–intervals in the appearances of caustics, and thespatial distribution of caustics at subsequent times.
First, we have noticed the existence of a rule for thetime–intervals of the appearances of caustics: the ratio ofintervals quickly approaches 1, a fact that we have madeplausible.
Second, we have found some rules hidden in the spatial
distribution of caustics: the ratio between a position of thenearest caustic from the center and that of the second nearest caustic from the center R1 = X (N - 1, N)/ X (N - 2, N)
approaches a value of around 0.15, where X (i, j) is the
position of a caustic, as the i–th position of a caustic at thetime when the j–th caustic appears.
Furthermore, the ratio between the nearest caustic fromthe center at the (N–1)th appearance of a caustic and that at
the Nth appearance of a caustic R 2 = X (N - 1, N)/ X(N - 2, N - 1) attains a value of around 0.3.
Third, we have found a rule for the mass distribution
for each caustic, that is, we have derived the density distribution of a cluster. The mass distribution for each caustic
can be fit to a line with the geometric progression of ratio
0.5.
Furthermore, using the above constants, we have foundFigure1:Spatial positions of caustics at the N–th appearance of caustics.

the smoothed density profile, and finally have evaluated thepower index of the power spectrum in the ‘virialized’
regime to be - 0.73. This value is different from - 1 that isdetermined by the density profile around one singularpoint.
The discovery presented in this research note, namelythat there exist remarkable rules for the distribution of
caustics, points towards several interesting theoretical
implications for long–term properties of self–gravitating
systems. As in studies of dynamical systems we here deal
with a hierarchy of bifurcations. A fruitful way to explore
universality properties further is to use renormalizationgroup techniques similar to those developed for the
Feigenbaum scenario of pitchfork bifurcations. With thisnote we have just provided a hint to the existence of universal constants. A detailed renormalization group andfixed point analysis is needed to support these findings. In
this context an interesting question remains open: the existence of chaotic regimes.
Besides this theoretical interest we think that our results
may be useful to check the accuracy of numerical simulations concerning their stability under long–time integration.
References[1]Yano, T., Koyama, H., Buchert, T., & Gouda, N.: 2004, ApJS, 151,
185.

13

r-Process Abundance Universality and Actinide Cosmochronology
OTSUKI, Kaori, MATHEWS, G. J.

KAJINO, Toshitaka(University of Notre Dame)(Division of Theoretical Astrophysics, NAOJ)

The heavy radioactive actinide nuclei, U and Th are
generated by rapid neutron capture process (i.e., r-process).
These
nuclide
have
half
lives

[t 1/2 ( 238 U) = 4.47 # 10 9 yr, t 1/2 ( 232 Th) = 1.40 # 1010 yr]
which are comparable to the cosmic age. The inferredabundance of U and/or Th can be used to estimate stellar
ages. The stellar ages are given by;

DT = 46.7 ( log (Th/Eu) 0 - log (Th/Eu) T ) Gyr,DT = 21.8 ( log (U/Th) 0 - log (U/Th) T ) Gyr,where the index 0 denotes the initial production ratio, while
the index T refers to the presently observed value.
Metal-deficient stars are believed to be the oldest stars
in the Galaxy.Their age can be regarded as the Galactic age
and a lower limit to the cosmic age. Dozens of observationsof r-process elements in metal-deficient halo stars havebeen reported which show a Z > 56 abundance distribution
pattern similar to the Solar-system r-process distribution(e.g.,[1]). This feature is called ''the universality of the rprocess''. Because of this universality, it is believed that rprocess elements for Z > 56 formed in the same ratio andtheir astrophysical origin is unique. The Th/Eu chronometer has applied for these metal-deficient stars and indicatesreasonable ages(e.g.,[1]). However, the extremely r-processenhanced, metal-deficient star CS31082-001was reported
to show quite high Th/Eu ratio [2]. Although it shows asimilar abundance distribution for 56 < Z < 80 elements,
the Th/Eu ratio is higher than in the Sun. The Th/Eu
chronometer shows this star is younger than the Sun inspite of its low metallicity ([Fe/H]+ –2.9). HDS group
found two other metal-deficient stars which also show highTh/Eu ratio[3]. These observations imply that the heaviest
r-process elements in these stars were generated with different production ratios and these elements could beformed in different nucleosynthesis environments.
We investigated r-process nucleosynthesis in various
environments. For this study, we assume steady-state flow
as a general model for the r-process nucleosynthesis environment. We calculated r-process nucleosynthesis in various combinations of the dynamical timescale x dyn, theentropy S, the electron fraction Ye, and boundary temperature T b. Differences in these parameters mean different
density and temperature profiles, which results in different
neutron-seed ratios and/or different paths of the rprocess[4][5]. For details of our calculation, see [6].
The results are shown in Fig.1. Our results show thatthe abundance distribution for the 56 < Z < 80 elements isalmost independent of the nucleosynthesis environment aslong as there are enough neutrinos to form 3rd peak elements. However, Th/Eu production ratio strongly depends

14

upon the nucleosynthesis environment. In these calculations, the beta-decay flow into stable nuclei occurs afteralmost all neutrons have been depleted. Hence, the final
abundance distribution was controlled by beta-delayed neutron emission rather than neutron-capture path. This seems
to be the main reason of the universality between the peakelements which hold in theoretical calculations.
The observed universality does not mean a unique
Th/Eu production ratio. This introduces an uncertainty into
the use of the Th/Eu chronometer as a means to estimate
the ages of the metal-deficient stars. On the other hand, theU/Th chronometer seems to be a good chronometer. We
found the U/Th production ratio is almost independent of
the nucleosynthesis environment if there were enough neutrons to reproduce the observed abundance distribution
when they formed. Unfortunately, there are several uncertainties in the nuclear physics models. It is also difficult to
detect U in metal-deficient stars. More experimental, observational, and theoretical studies for r-process nucleosynthesis are desired.

Figure1:Dependence of the nucleosynthesis yields upon various parameters of the astrophysical environment. Closed circles show
observed elemental abundances in CS22892-052 [1].

References[1] Sneden, C. et al.: 2000, ApJ, 533, L139.
[2] Cayrel, R. et al.: 2001, Nature, 409, 691.
[3] Honda, S. et al.: 2004, ApJS, 152, 113.
[4] Otsuki, K. et al.: 2000, ApJ, 533, 424.
[5] Terasawa, M. et al.: 2002, ApJ, 578, 137.
[6] Otsuki, K. et al.: 2003, New Astronomy, 8, 767.

Subaru/FOCAS Spectropolarimetry of Type Ic
Hypernova SN 2003dh/GRB 030329
KAWABATA, S. Koji
(Hiroshima University)

DENG, Jinsong, MAZZALI, Paolo, NOMOTO, Ken'ichi, MAEDA, Keiichi, TOMINAGA, Nozomu
UMEDA, Hideyuki, KOBAYASHI, Naoto(Tokyo University)

WANG, Lifan(Lawrence Berkeley National Laboratory)

IYE, Masanori, KOSUGI, George, OHYAMA, Youichi, SASAKI, Toshiyuki, AOKI, Kentaro
KASHIKAWA, Nobunari, TAKATA, Tadafumi, AOKI, Wako, KOMIYAMA, Yutaka
MIZUMOTO, Yoshihiko, NOUMARU, Junichi, OGASAWARA, Ryusuke
SEKIGUCHI, Kazuhiro, SHIRASAKI, Yuji, WATANABE, Jun-ichi, YAMADA, Toru
(NAOJ)HÖFLICH, Peter, WHEELER, J. Craig

JEFFERY, J. David(University of Texas)(University of Nevada)

KAWAI, Nobuyuki, SAKAMOTO, Takanori, URATA, Yuji

YOSHIDA, Atsumasa(Tokyo Institute of Technology)(Aoyama Gakuin University)

TAMAGAWA, Toru, TORII, Ken'ichi

TOTANI, Tomonori(RIKEN)(Kyoto University)

We carried out spectropolarimetric observationsof SN 2003dh/GRB 030329 in 2003 May and its properties
are investigated through a comparison with spectra of theType Ic hypernovae SNe 1997ef and 1998bw [1].
(Hypernovae being a tentatively defined class of SNe withvery broad absorption features: these features suggest alarge velocity of the ejected material and possibly a large
explosion kinetic energy.)
It is shown that the spectrum of SN 2003dh obtained on
2003 May 8 and 9, i.e., 34–35 rest-frame days after the
GRB (for z = 0.1685), are similar to those of SN 1997ef
obtained 34 - 42 days after the fiducial time of explosionof that SN. The match with SN 1998bw spectra is not as
good (at rest 7300–8000Å), but again spectra obtained
33 - 43 days after GRB 980425 are preferred. This indicates that the SN may have intermediate properties between
SNe 1997ef and 1998bw. The time of explosion of SN
2003dh is then constrained to be between - 8 and + 2 daysof the GRB, making this the first case to link the identity of
GRB and hypernova both in space and in time. The Si andO P-Cygni lines of SN 2003dh seem comparable to thoseof SN 1997ef, which suggests that the ejected mass in SN
2003dh may match that in SN 1997ef. More recently,
Mazzali et al. reported that the ejecta mass of SN 2003dh isfound to be + 8M 9 which is somewhat less than in othertwo hypernovae [2].

Figure1:Comparison of spectra of SNe 2003dh (black), 1997ef (green)and 1998bw (red).

Polarization was marginally detected at optical wavelengths and it is consistent with measurements of the lateafterglow, implying that it mostly originated in the interstellar medium of the host galaxy. However, further spectropolarimetric observation of bright SNe of similar class isrequired to confim the interpretation.
References[1] Kawabata, K. S. et al.: 2003, ApJ, 593, L19–L22.
[2] Mazzali, P. A. et al.: 2003, ApJ, 599, L95–L98.

15

Late-time Spectroscopy of the Interacting Type Ia SN 2002ic:
Evidence of a H-rich, Asymmetric CSM
DENG, Jinsong

KAWABATA, Koji S.

OHYAMA, Youichi(Tokyo University)(Hiroshima University)(Subaru Telescope, NAOJ)NOMOTO, Ken'ichi

IYE, Masanori

MAZZALI, Paolo A.

(Tokyo University)(Optical & IR Astronomy Division, NAOJ)(INAF-Trieste Osservatorio)

JEFFERY, David J.

TOMITA, Hiroyuki, YOSHII, Yuzuru(LBNL)(Univ. of Nevada at Las Vegas)(Tokyo University)

References[1] Deng, J. et al.: 2004, ApJ, 605, L37–L40.
[2] Hamuy, M. et al.: 2003, Nature, 424, 651–654.
[3] Turatto, M. et al.: 2000, ApJ, 534, L57–61.
[4] Rigon, L. et al.: 2003, MNRAS, 304, 191–196.
[5] Filippenko, A. V.: 1989, AJ, 97, 726–734.
[6] Wang, L. et al.: 2004, ApJ, 604, L53–L56.

16

OI[Ca II] / [O II]

OI

Hα
He I

[O I]

He I

Fe II

Fe II
Hβ
[O III]

Ca II

Fe II

SN 1997cy, 1997 Aug 24

SN 2002ic day 222

Flux scaled + constant

We obtained late-time optical spectroscopy of the TypeIa SN2002ic on 2003 June 27.6 UT [1] with the Faint
Object Camera and Spectrograph on the Subaru Telescope.
The spectrum has an epoch of + 222 rest-frame days after
explosion[2].
The spectrum is shown in Figure 1 with line-identifications and compared with those of SNe 1997cy [3] and1999E[4]. Strong H emission indicates an interaction
between the expanding SN ejecta and an H-rich CSM (see[2] for early-time observations). The late-time spectrum of
SN 2002ic resembles those of SNe 1997cy and 1999E,
though the latter were originally classified as Type IIn SNe.
The three SNe also have similar luminosities, suggestingthat they are the same phenomenon and that the CSM isalso similar. We proposed a new classification, Type IIa
SNe, for these events.
The observed line profiles and line ratios were analyzed
within the ejecta-CSM interaction scenario. The emissionin H Balmer, [O III], and He I lines, and in permitted Fe II
blends, resembles the spectra of the Type IIn SN 1987F [5]and of Seyfert 1 galaxies. A high-density, clumpy CSM isinferred. Strong, very broad [CaII]/Ca II and [O I]/O I
emissions imply that not all the outer SN ejecta were decelerated in the interaction, suggesting that the CSM is aspherical. This asymmetric scenario is consistent with spectropolarimetical observations [6].

Ca II / O I

WANG, Lifan

SN 1997cy 1998 Jun 26

SN 2002ic day 222

SN 1999E, 1999 Apr 12
SN 2002ic day 222

SN 1997cy, 1998 Aug 30

4000

5000

6000
7000
Rest wavelength

8000

9000

Figure1:Spectrum of SNe 2002ic (red thick lines;+ 222 days) compared with those of SNe 1997cy (blue thinlines) and 1999E(green dashed line)

SUBARU Deep Spectroscopy of the Very Extended Emission-Line
Region of the Seyfert Galaxy NGC 4388
YOSHIDA, Michitoshi, OHYAMA, Youichi, IYE, Masanori, AOKI, Kentaro,
KASHIKAWA, Nobunari, SASAKI, Toshiyuki, YAGI, Masafumi, FURUSAWA, Hisanori,
KOMIYAMA, Yutaka, MIYAZAKI, Satoshi, YASUDA, Naoki (NAOJ)SHIMASAKU, Kazuhiro, OKAMURA, Sadanori, DOI, Mamoru, NAKATA, Fumiaki,
OUCHI, Masami, SEKIGUCHI, Maki (Tokyo University)
HAMABE, Masaru (Japan Women's University)
KIMURA, Masahiko (Kyoto University)

Recently, Yoshida et al.[1] found a very large region ofionized gas extending around a Seyfert 2 galaxy in the
Virgo Cluster, NGC 4388. This very extended emissionline region (VEELR) has a size of 35 kpc and is locatedpreferentially toward the northeastern side of the galaxy.
Here we report the results of deep optical spectroscopy of
the VEELR of NGC 4388 using FOCAS of the Subaru
Telescope[2].
The Ha radial velocities of most of the filaments of theregion are highly blueshifted with respect to the systemic
velocity of NGC 4388. The velocity field is complicated,
and from the kinematic and morphological points of view,
there seems to be several streams of filaments: low-velocity
filaments, with radial velocities v relative to the systemic
velocity of the galaxy of roughly - 100 km/s; high-velocity(v + -300 km/s) filaments; and a very high velocity (v + 500 km/s) cloud complex (Fig.1).

tributes to the ionization of the gas. In particular, the filaments outside the ionization cone of the Seyfert nucleus aremainly excited by shocks. The predicted shock velocity is
200 - 300 km/s, which is comparable to the velocities ofthe filaments.
We conclude that the VEELR was formerly the disk gasof NGC 4388, which has been stripped by ram pressure dueto the high-speed (+ 2000 km/s) collision between the hot
intracluster medium (ICM) and the galaxy. The velocity
field and the morphology of the VEELR closely resemble
snapshots from some numerical simulations of this process.
In the case of NGC 4388, the ram pressure stripped gas,
which is normally seen as extended HI filaments, happens
to be exposed and ionized by the power-law radiation fromthe Seyfert nucleus, and so can be seen as optical emissionline gas (Fig.2). The ram pressure probably caused active
star-formation in the disk of the galaxy, also. Interaction
between the outflow induced by the disk star-formation andthe ram pressure stripped gas stream well explains theproperties of extended radio emission and the morphology
of faint Ha filaments.

Figure1:Velocity field of the VEELR of NGC 4388 overplotted on the
Ha+[N II] image. Schematic lines indicating individual groupsof filaments/clouds are overlaid.

The emission-line intensity ratios of the VEELR filaments are well explained by power-law photoionization
models with solar metal abundances, suggesting that the
Seyfert nucleus of NGC 4388 is the dominant ionization
source and that the VEELR gas has moderate metallicity.
In addition to photoinozation, shock heating probably con-Figure2:Schematic draw of the structure of the emission-line regions
around NGC 4388.

Refernces[1] Yoshida, M. et al.: 2002, ApJ, 567, 118.
[2] Yoshida, M. et al.: 2004, AJ, 127, 90.

17

VERA Observations of the W49N H2O Maser Outburst
HONMA, Mareki, BUSHIMATA, Takeshi, FUJII, Takahiro, HIROTA, Tomoya, HORIAI, Kouji
ISHITSUKA, Jose, IWADATE, Kenzaburo, JIKE, Takaaki, KAMEYA, Osamu, KAN-YA, Yukitoshi
KAWAGUCHI, Noriyuki, KOBAYASHI, Hideyuki, KUJI, Seisuke, MANABE, Seiji
MIYAJI, Takeshi, RIOJA, Maria, SAKAI, Satoshi, SATO, Katsuhisa, SHIBATA, M. Katsunori
TAMURA, Yoshiaki(VERA Project, NAOJ)

CHOI, Yoon Kyung, KURAYAMA, Tomoharu, OYAMA, Tomoaki, SUDA, Hiroshi(University of Tokyo)

SASAO, Tetsuo(Ajou University)

IMAI, Hiroshi, INOMATA, Noritomo, KAMOHARA, Ryuichi, NAKAGAWA, Akiharu
NAKASHIMA, Kouichirou, NAGAYOSHI, Riiko, OMODAKA, Toshihiro
SAKAKIBARA, Sei-ichirou, SHIMIZU, Rie, SORA, Kasumi, YAMASHITA, Kazuyoshi(Kagoshima University)

We report on a strong outburst of the W 49N H 2 O
maser observed with VERA in 2003 October[1].
As a part of VERA's phase-referencing performance
test [2], observations of the W 49N and OH43.8-0.1 H 2 O
maser pair were performed with an interval of about one
month. During the course of the observations, a strong
maser outburst has occurred in W49N, and we have successfully detected this outburst with VERA. Figure 1
shows the spectral evolution of W49N H 2 O maser at 22
GHz, with a strong outburst around day of year 281 and294 at V LSR =- 30.7 km/s. The peak intensity was
7.9 # 10 4 Jy, being one of the strongest outbursts observedin W49N so far.
We have also mapped the W49N H 2 O maser using
VERA array on the day of year 294, and successfully identified the outburst maser spot. Figure 2 shows the maser
spot distribution in W49N, and the arrow on the right map
shows the location of the outburst spot. Interestingly, thespot is on the arc-like structure, which is likely to be ashock front powered by forming stars, indicating possible
link between the maser outburst and shock phenomenon.
Further monitoring observations of the spot motions in
the arc-like structure will allow us to understand moredeeply the mechanism of maser outburst. Also, we are performing astrometric measurements of the separation of thetwo sources (W49N and OH43.8-0.1), and further observations will allow us to evaluate astrometric capability of the
VERA system.
References[1] Honma, M., et al.: 2004, PASJ, 56, in press.
[2] Honma, M., et al.: 2003, PASJ, 55, L57.

18

Figure1:Spectral evolution of W49N H 2 O maser. Vertical arrow corre4
sponds to 10 Jy. Dates of observations (day of year) are also
indicated.

Figure2:Maser spot distribution in W49N on day of year 294 in 2003.
Right panel shows the extended map of the central maser cluster, and the arrow indicates the position of outburst spot.

Meteoroid Clusters in Leonids: Evidence ofFragmentation in SpaceWATANABE, Jun-ichi

TABE, Isshi(Public Relations Center, NAOJ)(Libra Co. Ltd.)HASEGAWA, Hitoshi

HASHIMOTO, Takema(ASTEC, Inc.)(Nippon Meteor Society)

FUSE, Tetsuharu

YOSHIKAWA, Makoto, ABE, Shinsuke(Subaru Telescope, NAOJ)(Inst. Sp. Astron. Sci.)SUZUKI, Bunji(Misato Tech. HS)

During the recent Leonids storm, several short-duration“outbursts” in which more than 20–40 meteors appeared ina few seconds, have been reported[1][2]. The meteors inthese events were extremely localized within a few hundredkm, which should be caused by clusters of meteoroids. The
existence of such clusters indicates the fragmentation of
meteoroids during orbital motion in interplanetary space.
Considering the extent of the spatial distribution, the fragmentation should have occurred at around the perihelion
passage of the meteoroids just before encountering the
Earth. This may cause a possible enhancement of smaller
meteoroids, even in old dust trails. A possible example ofsimilar clusters in the past meteor storm of Giacobinids isalso noted. Such phenomena may be generally observed instrong meteor storms.
References[1] Watanabe, J., Tabe, I., Hasegawa, H., Hashimoto, T., Fuse. T.,
Yoshikawa, M., Abe, S., Suzuki, B.: 2003, Pub. Astron. Soc. Japan,
55, L23–L26.
[2] Kinoshita, M., Maruyama, T., Sagayama, T.: 1999, Geophys. Res.
Lett., 26, 1, 41–44.

Figure1:The Leonid meteor storm in 2001 over Japan. Photo by M.
Tsumura.

19

The Distribution of Star-Forming Regions in Luminous
Infrared Galaxies
HATTORI, Takashi, YOSHIDA, Michitoshi

OHTANI, Hiroshi(Okayama Astrophysical Observatory, NAOJ)(Ryukoku University)

SUGAI, Hajime

ISHIGAKI, Tsuyoshi(Faculty of Science, Kyoto University) (Graduate School of Engineering, Hokkaido University)

SASAKI, Minoru

HAYASHI, Tadashi

OZAKI, Shinobu(Shimonoseki City University)(Toyama Science Museum)(Nishi-Harima Astronomical Observatory)

ISHII, Motomi

KAWAI, Atsushi(Kurashiki Science Center)(Faculty of Science, Kyoto University)

We performed Ha imaging observations of 22 luminous
infrared galaxies (LIRGs) to investigate how the distribution of star-forming regions in these galaxies is related togalaxy interactions and global star-forming properties[1].
Observations were made with the Kyoto tridimensional
spectrograph I attached at the Cassegrain focus of the
Okayama Astrophysical Observatory 188cm telescope.

These classes of star-forming region were found to bestrongly related to global star-forming properties such as
star-formation efficiency, far-infrared color, and dust
extinction (e.g., figure 3). There was a clear tendency forthe objects with more compact distributions of star-forming
regions to show a higher star-formation efficiency and hotter far-infrared color.

Figure1:Examples of Ha and continuum images. The scale bar represents 5 kpc.

Based on correlation diagrams between Ha flux andcontinuum emission for individual galaxies (figure 2), a
sequence for the distribution of star-forming regions wasfound: very compact (+ 100pc) nuclear starbursts withalmost no star-forming activity in the outer regions (type1), dominant nuclear starbursts K 1kpc in size and a smallcontribution from the outer regions (type 2), nuclear starbursts L 1kpc in size and a significant contribution from theouter regions (type 3), and extended starbursts with relatively faint nuclei (type 4).

Figure2:The ordinate represents log Ha surface brightness(ergs 1 cm 2 arc sec 2 ) and the abscissa log continuum surface brightness (ergs 1 cm 2 Å 1 arc sec 2 ). The continuum
surface brightness increases leftward, so the galaxy nucleus
corresponds to the left edge of the diagram. The small dots represent Ha and continuum surface brightness measured at eachposition. In the top panel of each diagram, the distribution of
integrated Ha flux from each continuum surface brightness bin
is shown.

20

Figure3:IRAS color-color diagram for the sample objects. The different
types of objects show different flux ratios.

We also found that the distribution of star-forming
regions was weakly but clearly related to galaxy morphology: severely disturbed objects had a more concentrated distribution. The sequence of the distribution of star-forming
regions and its relation to morphological properties suggest
that, as the interaction proceeds, star formation in outerregions fades out and nuclear starburst becomes dominant.
It is also notable that an appreciable fraction of the sample
objects were dominated by extended starbursts (type 4),
which is unexpected in the standard scenario of interactioninduced starburst galaxies. Therefore, it may be crucial todetermine the triggering mechanism of star-formation inthese objects in order to better understand star-forming
activity in LIRGs.
References[1] Hattori, T. et al.: 2004, AJ, 127, 736.

Near-Infrared Coronagraphic Imaging of
Herbig Ae Star HD 150193A
FUKAGAWA, Misato

TAMURA, Motohide(The University of Tokyo/NAOJ)(Division of Optical and Infrared Astronomy, NAOJ)

HAYASHI, Saeko

ITOH, Yoichi, OASA, Yumiko(Subaru Telescope, NAOJ)(Kobe University)

Figure1:Circumstellar disk around HD 150193A. The scattered light by
dust grains was detected in the H-band. The occulting mask
has a diameter of 0 .5 but inner 0 .8 region (black circle) is photometrically unusable. A gray filled circle represents the T
Tauri companion star located at 1 .1 from the primary. The contours are overplotted starting from 64 to 6.4 mJy arcsec 2 insteps of 0.5 magnitude. Dotted lines indicate the directions ofsecondary spider pattern.

Figure2:Azimuthally averaged radial profile of the circumprimary disk
around HD 150193A (filled circles). The profile is averaged
along the elliptical path with P.A. = 358 % and ellipticity = 0.79,
assuming that the disk is circular. The profile is well fitted by apower-law with the index of - 4.6 (dashed line). Profile aroundthe companion is also shown (open circles), azimuthally averaged in the southern half region.

We report the near-infrared imaging of pre-mainsequence (PMS) star HD 150193A with the stellar coronagraphic camera and the adaptive optics (AO) on the Subaru
8.2-m Telescope [1].
The disk structure is now ubiquitous around low-mass
T Tauri stars and intermediate-mass Herbig Ae stars. In
order to understand the formation process of extra-solar
planetary systems, it is important to study the spatial structure of disks where planets are most likely formed as a byproduct of star formation process. However, few disks havebeen spatially resolved so far because of the observationaldifficulty: both high-resolution and high-contrast are
required to image the small and faint structure in the vicinity of the central bright star. Therefore, we have initiated
AO imaging of PMS stars with the coronagraphic camera
CIAO on the Subaru Telescope, which is one of the mostsuitable instruments for direct imaging of disks.
HD 150193A is a relatively old Herbig Ae star with its
mass of + 2M 9 and its age of 6 Myr. Previous observations
suggest the presence of abundant circumstellar dust aroundHD 150193 which led us to observe this nearby (d = 150pc) source: the circumstellar dust mass was estimated to be
0.01 M 9 in the submilliter observations [2], and [3] marginally resolved HD 150193A with 2 nm speckle holography.
It is also notable that HD 150193 is a binary with a T Tauricompanion star HD 150193B, which enables us to investigate the disk properties in the multiple system.

The H -band (1.65 nm) observations were carried out in2002 July. The AO was utilized, giving the spatial resolution of 0.̋1. We occulted HD 150193A with a mask whose
diameter was 0.̋5. In order to detect the faint structure, we
observed the reference star without any circumstellar material using the same AO and coronagraphic configurations,then subtracted the reference star image from each of HD
150193A and B.
We detected the disk around HD 150193A extending
from the edge of the coronagraphic mask at 50 AU to about
190 AU. The surface brightness and size of the disk aresimilar to those of other resolved disks around Herbig Aestars. While, no circumstellar matter was detected aroundthe companion star. This is consistent with the observational trends that the circumprimary disk have larger mass thanthat of the circumsecondary disk, and that the properties ofcircumprimary disks in wide binary systems are comparable to those of the disks around single stars [4]. Further
detailed study of this typical binary HD 150193 could contribute the understanding of disk evolution and planet formation in binary systems.

˝

˝

˝

References[1] Fukagawa, M. et al.: 2003, ApJ, 590, L49.
[2] Mannings, V., and Sargent, A. I.: 1997, ApJ, 490, 792.
[3] Koresko, C. D.: 2002, AJ, 124, 1082.
[4] Jensen, E. L. N. et al.: 2003, ApJ, 584, 875.

21

The Collapse and Fragmentation of Magnetized Molecular Cloud– MHD Nested Grid Simulation –MACHIDA, N. Masahiro

MATSUMOTO, Tomoaki

TOMISAKA, Kohji(Chiba University)(Hosei University)(Division of Theoretical Astrophysics, NAOJ)

Bar fragmentation

Ring fragmentationt = 1.0521e+7 (yr)t = 1.1519e+7 (yr)

L=13

L=11
L=14

L=12
L=15

L=13

L=11

L=12

L=14
L=15

Figure1:Two typical models of the adiabatic core are plotted (bar:left,ring:right). Density (contour and false color) and velocity vectors (arrows) are plotted on x=0 plane (lower panels) and on thez=0 plane (upper panels). The elapsed time, the maximum density, grid level and scale length are also plotted. Thick lines in
the upper panels denote the contour line of the adiabatic core,
while those in the lower panels mean the isovelocity curves representing the outflow region.

Collapse and fragmentation of the rotating magnetizedmolecular cloud is studied by using 3D MHD Nested Grid
simulations[1].
To study the evolutional processes of the molecular
cloud, we assume a cylindrical gas cloud with rotation axis
and magnetic field being parallel to the cylindrical axis andadd the axisymmetric and non-axisymmetric perturbation
for collapse and fragmentation of cloud. For adopting the
Nested Grid method, we calculate the cloud evolution with
15 orders of magnitude for density (10 2 - 1017 cm 3) and 5orders of magnitude for spatial scale(10 6 - 10 AU). We
parameterize the magnetic field strength, rotation speed andthe amount of initial non-axisymmetric perturbation. We
calculated 51 different models by vector parallel supercomputer VPP5000 at Astronomical Data Analysis Center,
National Astronomical Observatory of Japan.
As a result, the cloud evolutions are classified into thefollowing three types: (1)Core, (2)Bar Fragmentation, and(3)Ring Fragmentation. Figure 1 shows the final state of
the typical Bar Fragmentation (left panels) and Ring
Fragmentation (right panels) models. When the elongatedbar is formed in the isothermal collapse phase, fragmentation occurs in the adiabatic accretion phase. In Bar
Fragmentation models, the fragments are easy to merge
owing to their small orbital angular momenta, while strong
outflows are driven by their large spin angular momenta.

22

Figure2:The axis ratio and oblateness are plotted when the gas at thecloud center becomes adiabatic. The abscissa indicates the axis
ratio and the ordinate is the oblateness. Fragmentation occurs
above the horizontal dashed line (oblateness> 4). The domains
in large circles mean that fragmented cores survive to form
binary or multiple stars. The solid(dotted) lines represent theevolutional tracks for some typical parameters. The symbols
denote the shape of the adiabatic core when the fragmentation
occurs or the calculation ends. Thick-line and filled symbols
represent the cores which experience fragmentation.

On the other hand, when the axisymmetric disk is formed
and the non-axisymmetry does not grow sufficiently in theisothermal collapse phase, the disk deforms into a ring andfragments in the adiabatic accretion phase. The fragments
formed by Ring Fragmentation have large orbital angularmomenta but small spin one. For this reason, they seem tobecome a binary system, although the weak outflows are
driven.
Figure 2 shows the axis ratio (x-axis:degree of the bar
at z=0 plane), oblateness (y-axis:degree of the disk) andcore shape at the final state. Four thick (dotted) lines indicate the evolutions of the cloud shape in the isothermal collapse (adiabatic accretion) phase. From these lines, wefound that (i)disk forms early in the model with initial large
rotation speed and strong magnetic field, (ii)the nonaxisymmetry evolves only after the disk formation. From
distribution of symbols in Figure 2, we found that the binary formation conditions are (i) the sufficiently thin disk isformed (oblateness >4) and (ii) the central region has thesmall axis ratio (<1) or sufficiently large axis ratio (>10) in
the isothermal collapse phase.
References[1] Machida, M. N., Tomisaka, K., & Matsumoto, T.: 2004, MNRAS,
348, L1.

An Optical and NIR Search for Brown Dwarfs
in the Pleiades Cluster
NAGASHIMA, Chie, NAKAJIMA, Yasushi, TAMURA, Motohide, NAKAJIMA, Tadashi,
NAKAYA, Hidehiko (NAOJ), NAGAYAMA, Takahiro, NAGATA, Tetsuya, SATO, Shuji(Nagoya Univ.)

SUGITANI, Koji

DOBBIE, P.D.

(Nagoya City Univ.)(Univ. of Leicester)HODGKIN, S.T.

PICKLES, A.J.

(Univ. of Cambridge)(Univ. of Hawaii)

We report discovery of four new brown dwarf (BD)candidates including three L-type from a brown dwarf
search in the Pleiades open cluster in five optical and nearinfrared (NIR) bands [1].
In the Pleiades cluster which is one of the best clusters
for a BD search, about 20 M-type BDs have been identified
by optical surveys, however, there is only one known Ltype BD (Roque25; [2]). L-type BDs are too cool to detectin optical wavelengths. So we have carried out a BD survey
in both the optical and NIR of an area of 14l # 23l of thecentral region of the Pleiades cluster, which has not yet
been surveyed because of the existence of large extinction.
The NIR survey was made with SIRIUS on the UH 2.2 m
telescope and the optical survey was made with Wide Field
Camera on the Isaac Newton Telescope.

the reddening band, 12 objects (c01 + 12) in this region
are selected as candidates. Among them, four objects lie on
the theoretical isochrones in the colour-magnitude diagram(In Fig. 2), so we identified them as Pleiades BD candidates (PL-1+ 4). The estimated mass of faintest one, PL-4,
is around 0.028 M 9 , which is maybe the lowest mass object
found so far in the Pleiades cluster.
The SED of PL-1 is consistent with a mid to late-M
spectral type, PL-2 and PL-3 with late-M to early L types,
and PL-4 with an early-mid L type (fig. 3). The result of
this work shows that the combination of optical and NIR
survey is effective for a L-type BD search.

Figure2:The J, i l - K colour-magnitude diagram. Filled circles are BD
candidates and dotted arrows are estimated maximum reddening vectors. Other symbols are as in Fig. 1.

Figure1:The J - Ks, i l - J colour-colour diagram for all detected
objects. Small dots are point sources and open circles areextended sources. The thick solid and dashed curves are theloci of main sequence and red giant stars. The thin dashed anddot-dashed lines are the 125 and 120 Myr isochrones of the
NextGen model (inappropriate for L-type) and Dusty model(inappropriate for early M-type), respectively. Numbers withtick marks denote masses in solar mass units.

In Fig. 1, most objects are concentrated in the region ofreddened main sequence (reddening band), and a number ofextended sources spread upward and some point sources
exist on the right hand of the reddening band. Objects
spread upward are likely to be galaxies reddened withextinction and K-corrections (dotted lines). Because thetheoretical isochrones for BDs extend toward right hand of

Figure3:The SEDs for four BD candidates. Solid and dashed lines represent the SEDs with no extinction and with possible maximum extinction, respectively. Dotted lines are SED templates
made from field BDs.
References[1] Nagashima, C. et al.: 2003, MNRAS, 343, 1263.
[2] Martín, E. L. et al.: 1998, ApJ, 507, L41.

23

Evolution of DLA Systems From Hierarchical Galaxy
Formation Models
OKOSHI, Katsuya

NAGASHIMA, Masahiro(NAOJ)(University of Durham)

GOUDA, Naoteru

YOSHIOKA, Satoshi(Astronomical Data Analysis Center, NAOJ)(Tokyo University of Mercantile Marine)

We investigate evolution of Damped Lyman a(DLA)
systems in the hierarchical structure formation scenario[1].
DLA systems, which have been associated with cold gas(HI column densities N HI > 2 # 10 20 cm 2 ) in protogalactic
disks, provide some advantages in the investigation of various characteristics of primordial galaxies. Recent measurements of metal abundance unaffected by dust depletion can
provide good evidence for understanding the processes ofmetal pollution and revealing the connection between DLA
systems and galaxies. For example, the metallicities is typically Z 9 /10 and it exhibits milder evolution at redshift
1 < z < 4. Furthermore, DLA systems have other observational properties that the HI column density distributions
follow a single-power law.
We here investigate the evolution of DLA systems inour semi-analytic model taking into account merging
processes of dark halos, star formation processes and so on.
We can consistently show the metallicity evolution andthe column density distribution for reasonable models
which also reproduce fundamental properties of local
galaxy population[2]. This result suggests that the chemical
evolution of DLA systems can be consistently reconciledwith the observational features of typical galaxies. We
conclude that DLA systems primarily consist of sub- L*
and/or dwarf galaxies (e.g., B-band magnitude M + - 17
mag, HI-gas mass + 10 9 M 9 , circular velocity V c + 90km/s). This picture shows strong conflict with the classicalone in which DLA systems are relatively massive galaxies
like our Galaxy. We also compare our results with othertheoretical studies and discuss some advantages in theinvestigation of DLA systems[1].
Based on this study, we proceed to investigate the evolution of DLA systems as follows.
(1) DLA systems at low redshifts. Recently, groundbased and HST images have revealed various properties ofhost galaxies of DLA systems (DLA galaxies) especially at
redshift z < 1. We focus on the low-redshift DLA systems.
As a result, DLA galaxies primarily comprise low surface
brightness (LSB) dwarf galaxies(surface brightness
22 - 27 mag arcsec 2, size + 3 kpc, star formation rate
+ 10 2 M 9 /yr)[3].
(2) Radio observations of DLA systems. Recent radio
observations reveal new properties of DLA systems such as
abundance of hydrogen molecules. We explore some possi-

24bilities for studying DLA systems by radio observations
based on radio properties which agree well with our
results[3].
(3) DLA-galaxy surveys at high redshift. Recent surveys of DLA galaxies at redshift z > 3 presented that DLA
galaxies exhibit fundamental properties of Lyman-breakgalaxies[4]. In autumn 2004, we have a plan to observe
DLA galaxies at high redshifts with ESO investigators andto clarify the connection between DLA galaxies andLyman-break galaxies.

Figure1:Metallicity of cold gas in DLA systems as a function of redshift (soild line: best model)

Figure2:DLA column density distribution (solid line:best model)
References[1] Okoshi, K. et al.: 2004, ApJ, 603, 12.
[2] Nagashima, M. et al.: 2001, ApJ, 557, 505.
[3] Okoshi, K., & Nagashima, M.: 2004, submitted to ApJ.
[4] Mzller, P. et al.: 2002, ApJ, 574, 51.

Toward General Relativistic Gauge Invariant Nonlinear Perturbation
NAKAMURA, Kouji(Graduate Univiversity for Advanced Studies/NAOJ)

This research is concerning about general framework ofgeneral relativistic nonlinear perturbation theory, which
will have many physical applications. We report the part[1]of this research.
General relativity is based on the concept of generalcovariance. Intuitively, general covariance states that there
is no preferred coordinate system in nature. This is basedon the philosophy that the choice of coordinate systemhave nothing to do with natural phenomena. If we choose
one coordinate system, we can observe the natural phenomena in terms of this coordinate system, and if we choose
another coordinate system, we observe the same phenomena by different way.
On the other hand, the Einstein equation in general relativity is a set of nonlinear equations, but many exact solutions to this equation are known[2]. However, these exact
solutions are most often too idealized to properly represent
the realm of natural phenomena. In such situations, the perturbative approach is one of the powerful techniques toinvestigate physical systems and is one of the popular techniques in any theory of physics. In general relativistic perturbations, gauge freedom, which is unphysical degree of
freedom, arises due to general covariance. To obtain physically meaningful results, we have to fix these gauge freedom or to extract gauge invariant part of perturbations.
In linear perturbation theory, this “gauge freedom” isregarded as the freedom of the infinitesimal coordinatetransformation. This understanding of “gauge freedom” iscorrect when we concentrate only on the linear order.
However, it is known that this understanding of gauge freedom is not enough in nonlinear perturbations.
To explain the notion of “gauge freedom”, we have toremind what we are doing in the perturbation theory. In perturbation theory, we always treat two spacetime manifold.
One is the “physical spacetime” which we try to describe by
perturbation theory and another is the “background” which
is prepared for perturbations. Further, in perturbation theory,
we always write the equation in the form

Q (“p”) = Q0 (p) + dQ (p).

(1)

This gives the relation between the variable Q on the physical spacetime and its background value Q 0 and the variable
dQ on the background. dQ is called the perturbation of Q
from Q 0.
However, through Eq. (1), we are implicitly assumingthat there exists a point identification map between thephysical spacetime and the background. This is called a“gauge choice” in perturbation theory [3]. Namely, Q in
Eq. (1) is a field on the physical spacetime and the point“p” is on this spacetime. On the other hand, the backgroundvalue Q 0 of Q and its deviation dQ from Q 0 in Eq. (1) are

Figure1:The “physical spacetime” M e is described by the perturbation
on a “background” M 0 with an infinitesimal parameter e. The
correspondence of the points of these two spacetime manifold
is arbitrary and this is “gauge freedom”.

fields on the background and the point p is on this background. Since we regard that Eq. (1) is for fields, the points“p” and p should be same.
If there is a preferred coordinate system on both thesespacetimes, we can accomplish this identification using thispreferred coordinate system. However, there is no such
coordinate system due to general covariance and the gauge
choice is not unique when we consider theories in which
general covariance is imposed. This arbitrariness is just“gauge freedom” of perturbations. This freedom is arisenby the relation between the physical spacetime and the artificial background. Hence, this gauge freedom should havenothing to do with physical quantities which appear inobservations or in experiments. Actually, some linear ordervariables which is independent of this gauge freedom relatevariables in observations. These are called gauge invariant
variables.
Based on this understanding of “gauge freedom”, we
propose the systematic procedure to find gauge invariant
variables for gravitational field in nonlinear perturbation
theory with two infinitesimal parameters. Further, we haveshown that we can always find the gauge invariant quantities for nonlinear perturbations of an arbitrary physicalvariables by using gauge variant part of the spacetime metric. In our proposal, we do not specify anything about thebackground nor physical meaning of parameters for perturbations. This implies that our proposal is applicable to any
theory in which general covariance is imposed and has
many applications. One of applications is already publishedin literature[4].
References[1] Nakamura, K.: 2003, Prog. Theor. Phys., 110, 723.
[2] Kramer, D., Stephani, H., MacCallum, M. A. H., and Herlt, E.:
1980, Exact Solutions of Einstein's Field Equations (Cambridge:
Cambridge University Press).
[3] Stewart, J. M., and Walker, M.: 1974, Proc. R. Soc. London A, 341,
49.
[4] Nakamura, K.: 2003, Prog. Theor. Phys., 110, 201.

25

Discovery of Star Formation in Extended HI Gas around NGC 6822
KOMIYAMA, Yutaka, YAGI, Masafumi, FURUSAWA, Hisanori, MIYAZAKI, Satoshi,
OKADA, Norio, YASUDA, Naoki, ARIMOTO, Nobuo, IKUTA, Chisato(NAOJ)OKAMURA, Sadanori, DOI, Mamoru, OUCHI, Masami, SEKIGUCHI, Maki, SHIMASAKU, Kazuhiro(Univ. of Tokyo)

HAMABE, Masaru

KIMURA, Masahiko

NAKATA, Fumiaki(JWU)(Kyoto Univ.)(Univ. of Durham)

The Local Group dwarf irregular galaxy NGC 6822 islocated at about 500 kpc from our Galaxy and is a wellstudied galaxy in an isolated environment. Similar to many
dwarf irregular galaxies, it is also embedded in an HI gas
envelope which is more extended than the main stellar
body of the galaxy observed in the optical wavelength [1](see Fig. 1). However, the star formation activity in the gas
envelope has not been studied extensively so far. We
therefore carried out an observation with Subaru Prime
Focus Camera (Suprime-Cam) to cover the entire gas envelope down to unprecedented depth [2].
Since stars are well resolved by Suprime-Cam beyond
the limiting magnitude of existing surveys, the data enable
us to investigate the spatial distribution of each stellar population over a very wide field of view. The old stellar population is distributed in a nearly circular area out to + 15l
and comprises the main stellar body of the galaxy as seenin Fig. 1. On the other hand, blue young stellar population
traces the HI gas envelope very well, suggesting that thestar formation activity had also occurred in the gas envelope (Fig. 2). The age of the blue stellar population is estimated to be + 180 Myr from the color-magnitude diagramsfor SR-1,2 regions (shown in Fig. 2). The age is consistent
with the time of the onset of the recent star formation
observed in the central region of the galaxy.
Since the surface brightness of the blue stellar population in the gas envelope is 27 mag arcsec 2 even at thebrightest region, it is first discovered by Suprime-Cam
which has wide and deep observation capability. To makeuse of the capability of Suprime-Cam, we are planning toobserve several nearby dwarf irregular galaxies, aiming toreveal; whether the star formation activity in the extended
gas envelope is universal for all dwarf irregular galaxies ornot, how the star formation activity in the extended gas
envelope affects the evolution of dwarf irregular galaxies,
what the origin of the gas envelope around dwarf irregulargalaxies is.
References[1] de Blok, W. J. G., & Walter, F.: 2000, ApJ, 537, L95.
[2] Komiyama, Y. et al.: 2003, ApJ, 590, L17.

26

Figure1:The HI density map taken from de Blok & Walter (2000) overlaid on the Digitized Sky Survey image. The HI gas envelope
is more extended than the stellar body of the galaxy and hascomplicated structures such as arm, hole and cloud. Our survey
fields are represented by red lines.

Figure2:Distributionofblue
stellarpopulation( B - R C < 0.5, - 3.5 < M B < 0.5; mainly B- to A-type main
sequence stars). The area is the same as Fig. 1. Note that thecentral part of the galaxy, where stars are crowded, is excluded
from present analysis (hence the center of the figure is blank).

Magnetic Properties at the Footpoints of Hot and Cool Loops
KATSUKAWA, Yukio

TSUNETA, Saku

(University of Tokyo/NAOJ)(Solar Physics Division, NAOJ)

The solar corona consists of ubiquitous loops representing magnetic fieldlines. Recent observations with Yohkoh,
SOHO, and TRACE have revealed that individual coronalloops have different temperatures ranging from 1 to 5 MK.
Hot (T = 2 - 5 MK) loops seen in Yohkoh/SXT images
and cool (T + 1 MK) loops seen in SOHO/EIT and TRACE
images have different appearances and do not coincide inposition. We investigate what kind of magnetic properties
in the photosphere makes such a difference in the coronaltemperature.
Since the heating energy is supplied from the footpointsof the coronal loops along magnetic field lines, it is critically important to investigate magnetic properties at andaround the footpoints of the coronal loops. However, it isdifficult to identify footpoint positions unambiguously with
the SXT because the hot SXT loops are diffuse and darknear their footpoints. We overcome the difficulty by using
moss structure observed with the TRACE, which is lowlying EUV structure located at the base of the hot loops. It
is necessary to use measurement of photospheric magnetic
fields as precise as possible because the heating of thecorona does not depend on the magnetic flux alone (e.g.
sunspot umbrae). We employ the Advanced Stokes
Polarimeter (ASP) at the National Solar Observatory(NSO).
The photospheric magnetic parameters (field strength,
inclination, and magnetic filling factor) in the moss regions(i.e. footpoints of the hot SXT loops) are compared withthose in the footpoint regions of the cool TRACE loops.
The footpoints of the both loops have magnetic fields
whose strength is 1 – 1.5 kG and the orientation is nearlyvertical to the surface. The most significant difference isdiscovered in the magnetic filling factor, which is definedby the fraction of an ASP pixel filled with a magnetizedatmosphere. The moss regions, i.e. the footpoints of the hotloops, have significantly lower filling factor than the footpoints of the cool loops.
Magnetic fields are not uniformly distributed in thephotosphere, but are clusters of strong and fine magnetic
elements. If we assume that the magnetic elements havethe same field strength and spatial size, the observed magnetic filling factor can be interpreted to be proportional to
the surface number density of the magnetic elements. Low
filling factor observed in the moss regions corresponds to a
low number density of the magnetic elements. The lower
number density with larger photospheric motion would
provide enhanced coronal heating by efficient braiding ofcoronal magnetic fields, and leading to the hot loops. On

the other hand, concentrated magnetic elements with smaller velocity fields may not allow efficient braiding, resulting
in less heating for the cool loops.
References[1] Katsukawa, Y., Tsuneta, S.: 2004, ApJ, submitted.

Figure1:(a)Cool (1MK) corona observed with TRACE,
and (b) the hot (>2MK) corona observed with
Yohkoh/SXT.

Figure2:Percentage of the area covered by (a) the moss
(hot loops)and (b) the footpoints of the cool loops
as a function of the magnetic filling factor.

27

High Resolution Lunar Gravity Anomaly Maps
SUGANO, Takayuki*,

HEKI, Kosuke†(Graduate University for Advanced Studies/NAOJ)

Gravity data of the planets and satellites are provided
by radio tracking of spacecraft. In the case of the Moon,
however, the gravity studies have a difficulty, that is, direct
tracking data are unavailable at farside because of the lunar
synchronous rotation. The Lunar Prospector (LP) carriedout detailed gravity measurement in average altitude of 30
km at the end of the mission. Though the gravity data havea potential of deriving high resolution gravity map, previous works such as LP165 gravity model [1], which adopted
spherical harmonic expansion, could not achieve it becauseof the farside gravity data gap.
In this study, we have made lunar nearside free-air
gravity anomaly map through direct inversion of LP LOS(Line-of-Sight) acceleration data (Fig. 1a) [2]. We also perform terrain correction directly for the LOS data using
Clementine grid topography data, and the corrected data areprocessed with same procedure as the free-air gravity
anomaly in order to obtain Bouguer gravity anomaly map(Fig. 1b). These two maps achieve 24 km resolution at
lunar surface, and are the highest resolution lunar gravity
maps at present.
To take advantage of the high-resolution, we investigate
compensation state of craters and mascons in detail.
Among these gravity anomaly maps, the Bouguer gravity
anomaly is useful to study relatively shallow interior since
it is supposed to be free from gravity signals of the surface
topography. The compensation state mainly controlled by
two factors, (1) size of the crater, and (2) elastic thicknessof lithosphere. Thus, the compensation state inferred fromthe Bouguer gravity anomaly map enable us to estimate thethickness of lithosphere at the time of crater formation.
The compensation states of craters and mascons areevaluated as a mass deficit. Figure 2a shows mass deficits
of medium-sized craters, 60 – 300km in diameter. It represents the mass deficits are almost zero; the lithosphere wasenough rigid to support these medium-sized craters. Next,
we calculate mass deficits of large impact basins, 200–1,000 km in diameter, and compared the results with
Moho topography model for the purpose of estimating
lithospheric thickness beneath them. It is found from Fig.
2b that the lunar lithosphere was as thick as 20 – 60 km at
the time of the mascon formation.
These results will be an important constraint for thermal
history of the Moon, because the thickness of lithospherenotably depends on the temperature.
References[1] Konopliv, A. S. et al.: 2001, Icarus, 150, 1–18.
[2] Sugano, T. and Heki, K.: 2002, Earth, Planets and Space, 56, 81–86.

*Present affiliation: Kyoto University †Present affiliation: Hokkaido University

28

Figure1:The free-air (a) and Bouguer (b) gravity anomaly maps fromdirect inversion of the LP LOS data. Resolution of these maps
are 24km.

Figure2:Observed (circles) and calculated (curves) mass deficits associated with medium-sized craters (a) and mascons (b) from
Bouguer anomaly. Thickness of the lithosphere, Te, was 20 –60 km at the time of mascon formation.

Observational Impact of Scattered Light from the Laser
Beam of a Laser Guide Star Adaptive Optics
HAYANO, Yutaka, GAESSLER, Wolfgang, TAKATO, Naruhisa, TAKAMI, Hideki(Subaru Telescope, NAOJ)

IYE, Masanori

MINOWA, Yosuke(Division of Optical and Infrared Astronomy, NAOJ)(Institute for Astronomy, University of Tokyo)

WIZINOWICH, Peter, SUMMERS, Douglas(Keck Observatory)

Figure1:Measured surface brightness profiles of the scattered light during three observed transits of the Keck II laser beam. We estimated the surface brightness of the scattered light by calculating the total flux at the pupil plane normalized by the area sizeof field stop. This is equivalent to the surface brightness at thetelescope focal plane. While the sky background is to 20.4
mag/arcsec2, the surface brightness increases to 19.5 mag/arcsec2 when the laser beam collides with Subaru Telescope beam.
The dip in the middle of the light curve is due to the vignettingof secondary mirror.

We report our measurement whose purpose was to evaluate the observational impact of the scattered light from thelaser beam on other telescopes whose field of view happens
to cross the laser beam[1].
The scattered light from the sodium laser beam at the
wavelength of 589 nm (D2 line) projected from the Keck II
telescope towards 70 arcsecond north of the star,
SAO99809, was measured using the wavefront sensor ofSubaru Adaptive Optics[2] on December 24, 2001 (Hawaii
Standard Time). The projected laser power was 17 W andbeam diameter was 48 cm. The actual flux level measured
when the Subaru Telescope was pointing at elevation
angles of 45 and 60 degrees was roughly equivalent to 19.5
magnitude per square arcsecond calibrated by a standard
star magnitude in R band (See figure 1).
The results of measurements were shown to be consistent within a factor of 2 with theoretical estimation basedon the laser beam flux and the efficiency of Rayleigh scattering due to molecules and Mie scattering of aerosols in

Figure2:Calculated surface brightness of other telescopes at Mauna Kea
in the case of the first collision of our measurement. The surface brightness becomes larger when the telescope diameter issmaller. This is because that the surface brightness increases
linearly with the telescope diameter while the sky backgroundincreases by the square of telescope diameter. Also the surface
brightness becomes larger for the closer telescope from KeckII, because the overlapped laser beam with the telescope beam
is getting longer.

the atmosphere, which was evaluated by the combinationof AERONET database[3] of Mauna Loa Observatory andour measured data of dust counter at the Subaru Telescope.
We also found that about 90 % of the scattered light wasdue to Rayleigh scatter, since the number density of aerosol
is quite stable and small. Our measurement, for which thescattered height is about several hundred meters, shows thatthe surface brightness of the laser beam is no brighter than
the sky background 45 degrees away from the fullmoon[4]. Although the impact of this scattered lightdepends on the type of observation, many observations
could be performed without significant deterioration.
We also estimate the effect of scattered light for othertelescopes at Mauna Kea (See figure 2). The disturbance toastronomical observations could be most significant, when
the optical axis of the telescope and the center of the laser
beam collide at an altitude of around 8 kilometers.
References[1] Hayano, Y. et al.: 2003, PASP, 115, 1419.
[2] Takami, H. et al.: 2004, PASJ, 56, 225.
[3] Holben, B. N. et al.: 2001, J. Geophys. Res. 106, 12067.
[4] Krisciunas, K., & Schaefer, B. E.: 1991, PASP 103, 1033.

29

The Discovery of Two Lyman a Emitters beyond Redshift 6in the Subaru Deep Field
KODAIRA, Keiichi

TANIGUCHI, Yoshiaki(Graduate University for Advanced Studies/NAOJ)(University of Tohoku)

KASHIKAWA, Nobunari and Subaru Deep Field team(Division of Optical and Infrared Astronomy, NAOJ)

Probing the star-formation activity in galactic or subgalactic systems in the early universe is important forunderstanding both the history of galaxies and the origin ofcosmic reionization. Recent advances in deep optical imaging capability with 8-10m class telescopes enabled new
searches for star-forming galaxies beyond redshift 5. The
surveys for emission-line galaxies with narrow-band filters
have an intrinsic limitation in redshift coverage, and hence
the survey volumes are often not large enough to ensuresufficient robustness for success. In order to increase thesurvey volumes and to reach the faint limiting magnitude,
we need wide-field CCD cameras on 8-10m class telescopes. Suprime-Cam mounted at the prime focus of the
8.2m Subaru Telescope, provides a unique opportunity for
wide-field (a 34 l # 27 l field of view), narrow-band imaging
surveys for emission-line objects at high redshift.
We performed a deep optical imaging survey using anarrow-band filter (NB921) centered at m = 9196 Å
together with i l and z l broadband filters covering an
814 arc min 2 area of the Subaru Deep Field. Although thehelp of any gravitational lensing is highly useful for investigating faint high-z objects, it is also important to searchfor high-z LAEs in a so-called blank field for an unbiased
study.
We obtained a sample of 73 strong NB921-excess
objects based on the following two color criteria:z l - NB921 > 1 and i l - z l > 1.3. We then obtained optical
spectroscopy of nine objects in our NB921-excess sample,
and identified at least two Ly a emitters at
z = 6.541 ! 0.002 and z = 6.578 ! 0.002, each of whichshows the characteristic sharp cutoff together with continuum depression at wavelengths shortward of the line peak.
The latter object is more distant than HCM-6A at z = 6.56,
which is the most distant known object that has been foundso far.
These new data allow us to estimate the first meaningful lower limit of the star-formation rate density beyond
4redshift 6; tSFR + 5.2 # 10 M 9 yr 1 Mpc 3 . Since it isexpected that the actual density is several times higher than
this value, our new observation reveals that a moderately
high level of star formation activity already occurred at
z + 6.6.
References[1] Kodaira, K. et al.: 2003, PASJ, 55, L17.

30

Figure1:Thumbnail images of the two well-defined LAEs, (a) SDF
J132415.7 + 273058 and (b) SDF J132418.3 +271455. The
size of each image is 10 ll # 10 ll, and north is up and east is tothe left.

Figure2:Rest-frame UV spectra of two LAE candidates between 1200Å
and 1230Å. The spectra of SDF J132415.7 + 273058 and SDF
J132418.3 + 271455 are shown in panels (a) and (b), respectively. The combined spectrum of these two LAEs is shown inpanel (c). A trial of the profile fitting with a combination
between emission and absorption is shown by the red line.

New Methods to Monitor a Satellite-to-Satellite 4-way Link
ASARI, Kazuyoshi1, KONO, Yusuke1, IWATA, Takahiro2, YONEKURA, Katsuhide2
TAKANO, Tadashi2, KAWANO, Nobuyuki1
1:National Astronomical Observatoy, 2:Japan Aerospace Exploration Agency

Figure1:4-way Doppler measurement system.

Figure2:Allan standard deviation.

We proposed new methods to monitor a satellite-tosatellite 4-way link to make the first direct measurement of
Doppler frequency above the lunar far-side [1].
The Japanese lunar explorer SELENE will be launchedin 2006. It consists of 15 mission instruments, and will
make various observations all over the Moon. The lunar
gravity field in the far-side will be directly measured forthe first time. It is achieved by relaying a stable frequency
signal between a ground station and the main orbiter by arelay satellite when the main orbiter is above the far-side.
This method is called “4-way Doppler method” since
the stable frequency signal travels on four paths between
the ground station and the main orbiter via the relay satellite [2]. The relay satellite has the high orbit with peri-luneheight of 2,400 km, while the height of the main orbiter is
100 km. The orbit of the main satellite is affected by thesmall irregularity of the lunar gravity field. On the contrary,
the irregularity changes the orbit of the relay satellite little
because of its high orbit. Thus, the high order and degree
gravity coefficients are estimated by 4-way Doppler measurements.
In order to perform a 4-way measurement, the frequency signal transmitted from every satellite has to be coherent
with the transmitted stable frequency signal from theground station. For this reason, all the satellite has a PLL(phase locked loop). However, the relay satellite cannot
relay telemetry signals since the weight and electric consumption of the satellite is quite limited.
We can not know directly the PLL status onboard themain orbiter from the telemetry signal when the main
orbiter is above the far-side. Thus, the new methods tomonitor a satellite to satellite 4-way link are required.

There are some methods other than telemetry to know the
PLL status from the down-link signal. We noticed that thefrequency stability of the down-link signal depends on the
PLL status. The down-link signal is highly stable when the
PLL is locked. On the other hand, its stability is two orders
worse than that of the locked down-link signal when the
PLL is unlocked. We compared the advantages of thesemethods mutually by the simulation of Doppler frequencies
when the PLL is locked or un-locked. We propose the following new methods to monitor a satellite-to-satellite 4way link.
(1) To calculate Doppler frequency variation of the
returned signal. When the variation exceeds a certain level,
the PLL is decided to be un-locked.
(2) To calculate Doppler rate variations of the returned
signal. When the variation exceeds a certain level, the PLL
is decided to be un-locked.
(3) The grand station periodically sweeps the frequencyof the transmitting signal. When the spectrum at the sweep
period exceeds a certain level, the PLL is decided to belocked. These three method can be easily performed for a
few tens seconds without any prediction of Doppler frequency and its rate.
References[1] Asari, K. et al.: 2003, IEICE, J86, 2328-2335.
[2] Sasaki, S. et al.: 1998, SELENE Mission: Scientific Objectives(abstract), Proc. 21st Inter. Space Tech Sci.
[3] Iwata, T. et al.: 1998, Technical Report of IEICE, SANE98-4,
17–22.
[4] Matsumoto, K. et al.: 1999, Adv. Space Res., 23, 1809–1812.

31

Development of Ultra Light Weight Mirror
for Space and Ground Based Telescopes
KOHARA, Naoki

OTSUBO, Masashi(University of Tokyo/Solar Physics Division, NAOJ)(Advanced Technology Center, NAOJ)TSUNETA, Saku
(Solar Physics Division, NAOJ)OZAKI, Tsuyoshi, TAKEYA, Hajime, KUME, Masami(Mitsubishi Electric Corporation)

We report on the development of the light weight mirror by employing the Carbon-fiber-reinforced Carbon composite material (hereafter referred to as C/C). Future large
aperture optical-IR telescopes require very light-weight primary mirror. While the lightweight mirrors are being developed around the world, the technology appears not to bemature enough for the optical and near infrared wavelengths.
We choose C/C, which has such attractive properties ashigh specific rigidity, almost zero-CTE thermal expansion,and no dimensional change due to moisture-absorption. We
stress that the light-weight honeycomb sandwich panel has
been already developed for C/C. Our finite element analysis indicates that a 3.5m diameter C/C mirror for the opticaltelescope can be built with total weight under 200kg.
Reflective surface with optical quality is developed on
the C/C surface by depositing a thick (about 100 micrometer) electroless nickel plating layer (Kanizen) with highprecision cutting and polishing. Figure 1 shows the 15cm
aperture C/C spherical mirror, which is made to establish
the fabrication process of the curved C/C mirror. The figure
error (deviation from sphere) of the substrate before plating
reaches 7 micron rms.

Given the complex structure of the C/C mirror, we measure the figure change with temperature. The mirror is
located in the temperature oven for measurement with aninterferometer located outside. Figure 2 shows the thermal
deformation. Top panel is the wavefront error (WFE) map
with 50 degree C subtracted by that with 23.6 degree C.
This WFE map is then divided into three components withdifferent spatial frequency (bottom panels).
Two significant improvements are made based on themaps. First, we succeed to reduce the thermal deformationof the high spatial frequency (period+ 2mm), which is dueto the braiding of the carbon-fiber bundles by employing
thinner fiber bundles. Second, the thermal deformation of
the middle spatial frequency (honeycomb pattern, period +6mm) is also reduced by adopting the thicker (3mm) substrate [1].
We believe that this is the first attempt to make the ultra
light weight mirror with C/C. Further improvement is being
pursued.
References[1] Kohara, N.: 2004, master’s thesis, University of Tokyo.

Figure1:C/C spherical mirror (15cm aperture).
Figure2:Thermal deformation of C/C spherical mirror (evaluation area is 5.6cm aperture,=633nm).

32

Observation of Solar Flare Hard X-ray Spectra Using CdTe Detectors
KOBAYASHI, Ken

TSUNETA, Saku, TAMURA, Tomonori, KUMAGAI, Kazuyoshi(U. of Tokyo)(NAOJ)KATSUKAWA, Yukio, KUBO, Masahito, SAKAMOTO, Yasushi, KOHARA, Naoki(U. of Tokyo)

YAMAGAMI, Takamasa, SAITO, Yoshitaka(ISAS)

MORI, Kunishiro

KATO, Genzo(ClearPulse Co.)

(Mitsubishi Heavy Industries)

Most solar flares are accompanied by signatures ofhighly accelerated electrons, yet the acceleration process
and its role in flares remains a mystery. In many flares
these nonthermal electrons are shown to contain enoughenergy to drive the entire flare. Yet a significant minorityof flares show little or no evidence for nonthermal electrons, suggesting the existence of alternative energy releaseand transport mechanisms. We report an observation of asolar flare where neither hard X-ray nor radio emission
shows any sign of accelerated electrons [1].
The flare was observed by a balloon-borne hard X-ray
spectrometer [2,3] newly developed at NAOJ. This instrument is composed of sixteen 10 # 10 # 0.5 mm cadmium
telluride (CdTe) semiconductor detectors, and has an energy range of 15 - 120 keV with an energy resolution of
3 keV at 60 keV.
The flare occured at 06:41 UT on 24 May 2002 in the
on-disk active region NOAA 9963. It was also observed by
the Nobeyama Radio Polarimeters (NORP), and partiallyby the RHESSI satellite. The observed light curves areshown in figure 1.
The observed HXR spectra was fitted to two models, a
single-temeprature thermal model and a pure power law
spectrum (figure 2). While both models are consistent withthe data, the best fit spectral index of the nonthermal(power law) model is an unusually high values, e.g. 8.3 forthe 06:41:50––06:43:30 time interval. The temperature of

the best-fit thermal models are in a more reasonable range,e.g. 37.8 MK for the same time range. The RHESSI spectrum for the same time period was also analyzed, and theresult was shown to be inconsistent with the nonthermal
model and consistent with the thermal model.
The NORP data shows two features, the impulsive
emission in the 3.75 GHz band and more gradual emission
in 9.4 and 17 GHz bands. The impulsive feature was successfully modeled as thermal gyrosynchrotron from thethermal component seen in the HXR data. The gradualcomponent was also successfully modeled from GOESSXT data, using the source size obtained by SOHO EIT.
Therefore the radio and X-ray data are consistent if allobserved emission are assumed to be thermal. Furthermore,
we calculated the energy of an unseen nonthermal component assuming it just below the detection threshold
throughout the flare. This was found to be less than thepeak thermal energy content of the SXR source. Thisshows the nonthermal electrons cannot be the sole energy
source for creating the SXR source.

Figure1:Top: GOES soft X-ray light curve. Middle: Nobeyama
Radio Polarimeters (NORP) lightcurves. Bottom: balloon HXR light curve.

Figure2:Balloon HXR spectrum integrated over 06:41:50––
06:43:30 (size of crosses indicate 1v error bars), and fit
results to purely thermal spectrum (solid line) andpower law spectrum (dashed line).

References[1] Kobayashi, K. et al.: ApJ, submitted.
[2] Kobayashi, K. et al.: 2003, Proc. SPIE, 4851, 1009.
[3] Kobayashi, K. et al.: Sol. Phys., submitted.

33

Hard X-ray Surveys of AGNs : Revealing Formation Historyof Massive Black Holes in Galaxies
AKIYAMA, Masayuki

UEDA, Yoshihiro

OHTA, Kouji(Subaru Telescope, NAOJ)(ISAS, JAXA)(Department of Astronomy, Kyoto University)

Figure1:Cosmological evolution of number density of AGNs in eachluminosity bin. The points with error bars represent the results,
and the lines indicate results of fitting for the data points withthe luminosity-dependent density evolution model.

Understanding the evolution of the Active Galactic
Nuclei (AGN) population is a crucial key to reveal the formation history of massive black holes found at the centersof nearby galaxies. Hard X-ray survey of AGNs is lessaffected by absorption to the nucleus, thus useful to reveal
the whole population of AGNs and examine their cosmological evolution.
We conducted optical follow-up observations of hard
X-ray sources found by X-ray satellite, ASCA, mostly using
University of Hawaii 2.2m telescope and Kitt Peak 2.1m
telescope, and with Subaru telescope for faintest objects.
We revealed natures and redshifts of optical counterparts ofalmost all of the hard X-ray sources [1][2]. Combining thehigh-completeness hard X-ray AGN sample with an AGN
sample obtained by the Chandra deep survey, we examined
the fraction of obscured AGN as a function of luminosity
and the cosmological evolution of the AGN luminosity
function [3]. The fraction of obscured AGN decreases withincreasing luminosity. For AGNs with luminosity comparable to Seyfert galaxies, the fraction of the obscured AGNs
is about 60%, but for more luminous AGNs, i.e. QSOs, thefration is 30%. If we explain the results based on the unified scheme of Seyfert galaxies, the opening angle of thedust torus of QSOs is larger than that of Seyfert galaxies on
average. The AGN number density in each luminosity bin
which derived from cosmological evolution of AGN luminosity function shows that the number density of QSOs
peaks at redshift of 2, which is consistent with the results

34

Figure2:X-ray spectrum of an obscured QSO, AXJ08494+4454,
obtained with Chandra (Upper). Optical and near-infrared
spectra of the QSO taken with Subaru/FOCAS and IRCS
(Lower). The near-infrared observation revealed strong broad
Ha emission line.

from optical QSO surveys, but that of Seyfert galaxies
peaks at lower redshift, +1 (Figure 1). This may indicatethat larger black holes are formed at higher redshift.
We also conducted near-infrared spectroscopic observation of an obscured QSO found in the ASCA surveys with
Subaru/IRCS. Although the amount of X-ray aborption islarge, the near-infrared spectrum shows strong broad Ha
emission line [4] (Figure 2). Near-infrared imaging observations of ASCA AGNs with UH 2.2m telescope also
revealed that the optical to near-infrared colors of X-ray
obscured AGNs are not so red [5]. These results indicate
the dust extinction observed in the optical is not as large asthat expected from the amount of the X-ray absorption. The
gas and dust composition around the nucleus can be different from that of inter-stellar matter in the Galaxy.
References[1] Akiyama, M. et al.: 2000 ApJ, 532, 700.
[2] Akiyama, M. et al.: 2003, ApJS, 148, 275.
[3] Ueda, Y. et al.: 2003, ApJ, 598, 886.
[4] Akiyama, M. et al.: 2002, ApJ, 567, 42.
[5] Watanabe, C. et al.: 2004, ApJ, in press.

Nucleosynthesis of Light Elements and Heavy r-Process
Elements through the o-Process in Supernova Explosions
YOSHIDA, Takashi

TERASAWA, Mariko(Astronomical Data Analysis Center, NAOJ)(Univ. of Tokyo)

KAJINO, Toshitaka

SUMIYOSHI, Kohsuke(Division of Theoretical Astrophysics, NAOJ)(Numazu College of Technology)

Figure1:The dependence of neutrino parameters on the ejected 11 B
mass. Horizontal and vertical axes indicate the total neutrinoenergy and the ejected 11 B mass. The energy (MeV) and ther n, x and thetime (s) in parenthesis are the temperature of o n, x, odecay time of the neutrino flux. The horizontal shaded regionis the range evaluated from Galactic chemical evolution models of the light elements. The vertical shaded region is therange evaluated from the gravitational energy of a neutron star.

We investigate the dependence of the supernova neutrinos emitted during supernova explosions on the ejectedmasses of the light elements such as 7 Li and 11 B and theheavy r-process elements[1]. We adopte a common neutrino luminosity model for the light element and r-processelement synthesis. The total neutrino energy E o and the
decay time of the neutrino flux x o are adopted as parameters. The energy spectra of the supernova neutrinos are
assumed to obey Fermi distribution. The temperature ofo n, x and or n, x, T o , o is set to be 8 MeV and the temperatures of o e and or e are set to be 3.2 MeV and 5.0 MeV.
We used the supernova explosion model of a 16.2 M 9star corresponding to SN 1987A [2]. The obtained ejectedmasses of 7 Li and 11 B are roughly proportional to the total
neutrino energy and scarcely depend on the decay time of
the neutrino flux (see Fig. 1). The r-process nucleosynthesis was calculated using the neutrino driven wind models of
a 1.4 M 9 neutron star [3]. The obtained r-process abundance pattern mainly depends on the peak neutrino luminosity which is proportional to E o /x o. A small peak neutrino luminosity is favorable for the reproduction of the rprocess abundance pattern of the solar system composition.
There is an overproduction problem of 11 B in the
Galactic chemical evolution: the supernova contribution ofn, xFigure2:The r-process abundance pattern in the case of53
MeV and E o = 3 # 10 ergs, x o = 9s. Stars indicate theobserved abundance pattern of the r-process elements[4]11 B evaluated from the supernova nucleosynthesis theory is

overproduced by a factor of 2.5 to 5.6 compared to the
Galactic chemical evolution models [5][6]. On the other
hand, the total neutrino energy is almost equal to the gravitational energy of a typical neutron star, i.e., about 3 # 10 53
ergs. We reproduce the ejected mass of 11 B evaluated fromthe Galactic chemical evolution models when we decrease
the neutrino temperature T o , o from 8MeV to 6MeV and
set the decay time of the neutrino flux x o as 9s. The r process abundance pattern has been also well reproducedwith the same supernova neutrino model. Small neutrino
temperature about 6MeV can reproduce the Galactic chemical evolution of both of the light element and the r-processelement synthesis.
n, x

n, x

n, x

References[1] Yoshida, T., Terasawa, M., Kajino, T., and Sumiyoshi, M.: 2004,
ApJ, 600, 204.
[2] Shigeyama, T., and Nomoto, K.: 1990, ApJ, 360, 242.
[3] Terasawa, M., Sumiyoshi, K., Yamada, S., Suzuki, H., and Kajino,
T.: 2002, ApJ, 578. L137.
[4] Käppeler, F., Beer, H., Wisshak, K.: 1989, Rep. Prog. Phys., 52,
945.
[5] Fields, B. D., Olive, K. A., Vangioni-Flam, E., and Cassè, M.: 2000,
ApJ, 540, 930.
[6] Ramaty, R., Lingenfelter, R. E., and Kozlovsky, B.: IAU Symp., 198,
51.

35

Oscillations in the Coronal Green-Line Intensity Observed atˇ and Norikura Nearly Simultaneously
Lomnicky´ Stítˇ
´ Milan
MINAROVJECH, Milan, RUSIN,
Vojtech, RYBANSKY,(Astronomical Institute, Slovak Academy of Sciences)

SAKURAI, Takashi, ICHIMOTO, Kiyoshi(Solar Physics Division, NAOJ)

The heating mechanism of the solar corona is not yet
fully understood, but so far two competing models havebeen proposed. One is the microflare hypothesis, and theother is the wave hypothesis. In the framework of the wave
model, it is crucially important to know what kind of waves
exist in the solar corona.
The observations of waves in the corona have been
made in two ways. One is to observe the Doppler shift incoronal emission lines, and the other is to observe theintensity of either the emission lines or of the electron scattering continuum. Although it is easier to measure theintensity than the Doppler shift, the intensity observation is
subject to variations in sky conditions. So far many reports
appeared claiming the detection of oscillations in line orcontinuum intensities, but they are not truly believed.
In the present analysis, we combined the data of thecoronal emission line at 5303Å (the so-called coronal green
ˇ observatory in Slovakia (altiline) from the Lomnicky´ Stít
tude 2632m) and from the Norikura Solar Observatory
ˇ data were(altitude 2876m), NAOJ. The Lomnicy´ Stít

obtained with a 20cm aperture coronagraph with a photoelectric photometer. The 25cm aperture coronagraph with aspectrograph at Norikura was used to obtain the spectra(and therefore the Doppler shift and line intensity) of thegreen line. The joint observation was carried out on 2000
October 24, with a time difference of two hours.
The background sky intensities from Slovakia and from
Norikura showed different power spectra, indicating differing sky conditions at the two sites. The line intensity datafrom the two observatories, however, showed a similar
peak in power spectra, centered around a period of 3–5
minutes. The Doppler shift data from Norikura also showeda similar behavior. Therefore, the existence of intensity
oscillation was of no doubt. However, the intensity variations showed coherence over a large spatial scale which is
hard to interpret.
References[1] Minarovjech, M., Rusin,
V., Rybansky,ˇ´ M., Sakurai, T., andIchimoto, K.: 2003, Solar Phys., 213, 269.

Spatial position along the slit

0

50

100

150

200

250
0

500

1000

1500

2000

2500

3000

3500

4000

4500

Time (sec)Figure1:The intensity variation of the coronal green line observed at Norikura. The abscissa is time and the ordinate is the coordinate along the slit of thespectrograph. The left-hand-side panel is the raw data, and the right-hand-side panel shows low-pass filtered data in which short time-scale phenomena are enhanced.

36

New Clean Room for Space Instrumentation
NOGUCHI, Motokazu, NAKAGIRI, Masao, SUEMATSU, Yoshinori, TSUNETA, Saku
(Solar Physics Division, NAOJ)

KUBO, Masahito(University of Tokyo/Solar Physics Division, NAOJ)

1. Introduction
New clean room (192m 2 ) was completed in the
Advanced Environment Test building on the spring of2003. The clean room is equipped with the checkout roomon the second floor looking over the clean room to generally support the activities in the clean room. The nominal
cleanliness is 100,000. The class indicates the number ofparticles with size larger than 0.5
per cubic feet. We
extensively clean up the clean room and equipment to bebrought into the clean room immediately after its completion. The clean room turns out to have performance ofapproximately class 100 with 10 personnel working in theclean room.
On February 2003, the heliostat (Fig. 6) was completed
on the roof top of the building, and we can introduce thelight from the sun and stars into the clean room through theglass window on the ceiling without breaking the cleanliness. Since May 2003, this clean room has been heavily
used to construct and test the Optical Telescope Assembly
to be aboard the Solar-B satellite. The beam size is approximately 50 cm. This is a unique feature of the NAO clean
room.

Figure1: Clean Room.

2. Environmental maintenance of the clean room
Needless to say, dusts and organic materials (gas) are
extremely hazardous for space optical hardware. We aretaking the following precautions to maintain the clean environment:(1) continuous monitoring of number of floating particles

in air (particle contamination),(2) regular monitoring of molecular contamination withwitness glass located on the walls of the clean room,(3) control of the temperature and humidity (20±0.2℃,
45±2%),(4) folding (accordion) booth for carrying-in equipment andunpacking,(5) maintenance of air condition system including the addition of the high-performance particle filters for air comingfrom outside to maintain the positive pressure of the cleanroom,(6) cleaning and dust check of equipment carried into theclean room with black light,(7) regular cleaning of the floor and prompt exchange ofthe filled garbage boxes in the clean room.
Regarding (4), the clean room is unfortunately not
equipped with a dedicated room for unpacking. Thus, wedeveloped the foldable booth located inside of the entrance
door, and the carry-in procedure is as follows: We open theentrance door, and bring containers inside. The area connected to the door is separated from the clean room withthe unfolded booth with curtain. We clean the hardware
after closing the door in the booth. The booth is then folded
to the width of 1m not to dominate the area of clean room,
and instruments are moved into the clean room. Thissequence enables us to completely separate the dirty outside from the clean room.
Regarding (5), when the air condition system had to beturned off for the critical measurement such as the measurement with an interferometer to eliminate the effect ofvibration, cleanliness class more than 100,000 was recorded. This was due to the air that was introduced from outside
through the built-in filter, whose performance is apparently
not acceptable. In order to improve the quality of the air,
we installed the HEPA filter, resulting in a significant
improvement with cleanliness class<200 (0.3 m particles).
With these efforts, we can usually achieve class 100(0.3 m particles). Furthermore, Optical Telescope
Assembly has been kept in the clean booth (27m2) locatedin the clean room. The cleanliness class in the clean boothis less than 50 when there are several workers inside thebooth and 0 when there are no personnel inside.

37

3. Monitoring the cleanliness
The number of floating particles is being measured byparticle counters. Fig. 2 shows the time variation of number
density of >0.3 m particles in the clean booth, and Fig. 3
shows that of >0.5 m particles for the period when opticalalignment of Solar-B optical telescope assembly is done
from 6 May to 26 May 2004. From these data, periodic
day-night variation can be read. Sometimes over 1,000 wasrecorded, because the air conditions of the clean booth was
turned off to remove the effect of vibration during interferometer measurement. Some of these peaks corresponds tothe timing when containers were brought from outside. Fig.
4 shows the histogram of 0.5 m particles, and indicatesthat for 90% of the time cleanliness class was less than 5.
Even when approximately 10 persons were working in theclean room, the class was almost less than 10. Fig. 5 shows
the long-term monitoring on the number of 0.3 m particles. Although the cleanliness factor was sometimes close
to 100,000 for short duration as mentioned previously, it isusually about 100. (From the end of January to the beginning of February 2004, the particle counter was out of orderso there is no data for the period.)

Figure4: Histogram of the number density (0.5 m particles).

Figure5: Long-time variation of the number density (0.3 m particles).

Figure2: Time variation of the number density (0.3 m particles).

Figure6: Heliostat

Figure3: Time variation of the number density (0.5 m particles).

38

Oscillatory Orbits in the Standard Mapping
Yoshihiro YAMAGUCHI

Kiyotaka TANIKAWA(Teikyo Heisei Univesity)(Division of Theoretical Astrophysics, NAOJ)

Chazy introduced oscillatory solutions of the gravitational three–body problem as a logical consequence in theclassification of final motions. Sitnikov proved the existence of this type of motion in the three-dimensional
restricted three–body problem with masses m1 = m 2 ! 0 and
m3 = 0. The demonstration of this existence was named the
Sitnikov problem.
Sitnikov considered the situation in which two bodies
with equal mass move in elliptic orbits in the x-y plane. The
center of mass is located at the origin. The third bodymoves along the z axis. Sitnikov proved that there is a setof initial conditions whose orbits survive the first ejection
after the first syzygy (the line connecting two primaries)
crossing (that is, the orbits do not escape), there is a subset
of initial conditions whose orbits survive the second ejection, and so on, and that there are orbits whose ejection distances grow indefinitely. He proved that there exist initialconditions such that the distance r (t) of the third body fromthe origin does not grow monotonically although its supremum increases without bound. These conditions are thoseof an oscillatory orbit. The Sitnikov problem has been
extended by Alekseev, Easton and McGehee. The existenceof oscillatory orbits in other three-body systems was verified with the aid of numerical integration. Many references
are in Ref[1].
The orbits of the accelerator mode[2] in the standard
mapping corresponds to escape orbits in three–body problems. The accelerator mode appears as soon as the last
Kolmogorov–Arnold–Moser curve disintegrates. In thevicinity of an orbital point of the accelerator mode, there
exist points of non–Birkhoff periodic orbits which, in thelanguage of the three–body problem, are ejected to various
distances. Therefore we hypothesize the existence of oscillatory orbits if orbits of the accelerator mode exist. We
prove that this hypothesis is correct. The detailed proof iscontained in Ref[3].
The standard mapping we consider is defined on acylinder:take any accelerator mode from the dynamical order relation obtained in Ref[2]. Next we prove the existence of the
non–Birkhoff type doubly symmetric periodic orbits in thevicinity of this accelerator mode. These orbits go together
with the accelerator mode but return back. The initial pointof the oscillartoy orbit is obtained as the accumulation
point of these orbits.
The system containing oscillatory orbits seems to havethe following characteristic property. There is a point z 0such that the orbit starting at this point goes to infinity as t
goes to infinity; that is, an escape orbit exists. Further there
exists an initial point z l0 in a neighborhood of z 0 such thatthe orbit starting from z l0 goes far from z l0 but eventuallycomes back to z l0. The initial point of an oscillatory orbit islocated in the vicinity of z 0 and z l0. It is important to makeclear the necessary and sufficient conditions for the existence of oscillatory orbits. This is a future problem.
Rerferences[1] Tanikawa, K., and Umehara, H.: 1997, Celest. Mech. Dynam.
Astron., 70, 167.
[2] Yamaguchi, Y., and Tanikawa, K.: 2002, Prog. Theor. Phys., 108,669.
[3] Yamaguchi, Y., and Tanikawa, K.: 2004, Prog. Theor. Phys., 111,
689.

y n + 1 = y n + a sin x n , x n + 1 = x n + y n + 1 ( mod 2r),
where a is a positive parameter.
Here we show briefly the procedure of our proof. We

39

Subaru/HDS Studies of Eu Isotope Abundances in
Metal-Deficient Stars
AOKI, Wako

RYAN, S. G.

(Division of Optical and Infrared Astronomy, NAOJ)(Open University)

IWAMOTO, Nobuyuki

NORRIS, J. E.

BEERS, T. C.

(University of Tokyo)(Australian National University)(Michigan State University)

ANDO, Hiroyasu

KAJINO, Toshitaka(Division of Optical and Infrared Astronomy, NAOJ)(Division of theoretial Astronomy, NAOJ)

MATHEWS, G. J.

FUJIMOTO, Masayuki(University of Notre Dame)(Hokkaido University)

Chemical composition of metal-deficient stars provide
with a unique opportunity to study the nucleosynthesis
processes in the early Galaxy. Analyses of isotope abundances, in addition to elemental abundances, in these stars
are expected to make a significant progress in the understanding of details of the processes. As the first step of thischallenge, we have obtained high-resolution (R + 10 5)
spectra of several metal-deficient stars with Subaru/HDS,
and made analysis of the Eu II lines, which show relatively
large isotope (151 Eu and 153 Eu) splittings.
(1)The 151 Eu fraction in r-process-enhanced stars is slightly
smaller than 50% (left figure), in agreement with that insolar system material. The elemental abundance pattern ofheavy nuclei in these stars are well known to agree withthat of the solar-system r-process component, and theagreement has been confirmed in isotopic level for Eu [1].
(2)The 151 Eu fractions in two stars with s-process elementexcesses are 55-60% (left figure)[2]. While more than 90%
of Eu in solar-system material originates from the rprocess, the majority of Eu in these stars is estimated to beyielded by the s-process from the abundance patterns ofheavy elements. The present analysis derived, for the firsttime, an observational constraint on the Eu isotope ratio
produced by the s-process. Since the Eu isotope is signifi-

cantly affected by the branching at 151 Sm, the isotope ratio
can be a probe to investigate the temperature and neutron
density in the s-process site. Our model calculation of thes-process, adopting the recent nuclear reaction rate showsthat the observed Eu isotope ratio can be well explained byneutron density of 10 7 9 cm 3 and temperature ofkT = 10 - 30 keV (right figure). Future progress in thequality of the observational data and nuclear reaction rates
will enable us to study the condition of the s-process inevolved intermediate-mass stars (AGB stars), i.e., to estimate the contribution of the process during the thermal
pulse (high temperature and high neutron density) and thatbetween the pulses (low temperature and low neutron density). The present study shows that detailed analyses of Eu
isotope ratio will provide a new observational constraint on
the recent complicated s-process and AGB models.
References[1] Aoki, W., Honda, S., Beers, T. C., and Sneden, C.: 2003, ApJ, 586,
506-511.
[2] Aoki, W., Ryan, S. G., Iwamoto, N., Beers, T. C., Norris, J. E.,
Ando, H., Kajino, T., Mathews, G. J., Fujimoto, M. Y.: 2003, ApJ,
592, L67.

Figure1: left: A Eu II line of the r-process-enhanced star HD6268 (upper panel) and those of the s-process-enhanced stars LP625-44 and CS31062-050.
Solid lines show synthetic spectra calculated assuming the best-fit Eu isotope ratios, and dotted and dashed lines indicate the ones assuming
10% differences of 151 Eu fraction. right: 151 Eu fraction as a function of neutron density calculated by the s-process model for 30keV(squares),
20keV(triangles), 15keV(circles), and 10keV(asterisks). The observational result for LP625-44 is shown by the hatched area.

40

A New Precession Formula
FUKUSHIMA, Toshio(Public Relations Center, NAOJ)

Modifying J. G. Williams' formulation [1], we developed a new scheme to express the precession and nutationin an arbitrary inertial frame of reference. It gives the precession-nutation matrix as the product of four rotation
matrices asr ) R 3 (cr )NP = R1 (- e) R 3 (- }) R1 ({and the precession one similarly asr ) R1 ({r ) R 3 (cr ).
P = R1 (- er ) R 3 (- }r and cr are the angles to specify the location
Here (1) {of the ecliptic pole of date in the given inertial frame, (2) }r are the true and mean ecliptic angles of precessionand }Xr 0 =- (17.12 ! 0.01) mas, Yr 0 =- (5.06 ! 0.02) mas.
By shifting the base reference frame from the ICRF to
the mean equator and equinox at J2000.0, we derived thebest-fit polynomials of the classic precession quantities,
sin r A sin P A, sin r A cos P A, r A, P A, p A, } A, ~ A, | A, e A,
g A, z A, and i A. They are provided in Table 1 of Fukushima(2003) as well as all the existing formulas given in the literature.
As a by-product, we estimated the speed of general precession in longitude at J2000.0 as˝

p = (5028.7955 ! 0.0003) /Julian century,

around the ecliptic pole of date and counted clock-wisefrom the direction to the z-axis of the given inertial frame,
respectively, and (3) e and er are the true and mean obliquities of the ecliptic with respect to the x- y plane of thegiven inertial frame, respectively. Note thatr + D}ande / er + De, whereD}andDe are the}/}usual nutations in longitude and in obliquity, respectively.
As a result, reference frames referred to the true ormean equator and equinox of date are explicitly describedin the ICRF by using the newly introduced precession
angles and the usual nutation angles. Although the expression of nutation matrix is unchanged as

we determined the dynamical flattening of the Earth fromthe precession constant as

N = R1 (- e) R 3 (- D}) R1 (er ),H d = (3.2737804 ! 0.0000003) # 10 3.

we recommend the usage of the above form of NP insteadof preparing P and N separately because of faster evaluation. The formulation is robust in the sense it avoids a singularity caused by finite pole offsets near the epoch. Facing
the singularity is inevitable in the pre-2003 IAU formulation.
By using the new formulation, we created a new set ofprecession formulas [2]. First, we adopted a numericaldetermination of the motion of ecliptic in DE405 [3] tor in the inerspecify the polynomial expressions of cr and {tial sense. Next, we selected a recent theory of the forced
nutation of the non-rigid Earth, SF2001, [4], to express D}
and De in a compact and precise trigonometric series
expansion. Then we converted the true pole offsets
observed by VLBI for 1979-2000 to the offests in the twor and er . As their first approximation,
precession angles, }we used h A and f A of Williams (1994). From the converted
offsets, we determined the best-fit polynomial expressionsof the corrections to the approximations as well as theequinox correction. We judged from a weighted leastsquare method that linear corrections are sufficient. Thusr and er as
we determined the polynomial expressions of }well as the equinox correction E to the IAU 1976 formulation. Combining these with the above formulas of planetary
precession, we determined the mean celestial pole offset at
J2000.0 as

From the classic polynomial expressions derived in theabove, we evaluated the effect of the sense in defining theecliptic. The resulting polynomial forms of the new precession angles in both the rotational and inertial senses are, as
well as the derived classic precession quantities, summarized in [4]. These constitute a new set of the fundamental
expressions of the precession quantities.
If the concern is the minimization of modification of
the pre-2003 IAU formulation, the readers may use theupdated classic quantities as well as the frame adjustment
at the epoch.
r and er the luniNote that, although we have called }solar precession in this article, they are meant to include theeffect of the geodesic precession. In spite of our presentation of precession quantities in both senses, one should
understand that those in the inertial sense are of primarynature and the expressions in the rotational one were
derived from them.

the mean obliquity at J2000.0 in the inertial sense as( e 0 )I = (84381.40621 ! 0.00001) ,˝and that in the rotational sense as( e 0 )R = (84381.40955 ! 0.00001) .

˝

Also, by adopting a best estimate of the theoretical value ofthe geodesic precession,p g = (1.9196 ! 0.0003)˝/Julian century,

Refrences[1] Williams, J. G.: 1994, Astron. J., 108, 711.
[2] Fukushima, T.: 2003, Astron. J., 126, 494.
[3] Harada, W., and Fukushima, T.: 2004, Astron. J., 127, 531.
[4] Shirai, T., and Fukushima, T.: 2001, Astron. J., 121, 3270.

41

Formation of the First Stars by Accretion
OMUKAI, Kazuyuki

PALLA, Francesco(Division of Theoretical Astrophysics, NAOJ)(Arcetri)

The process of star formation from metal-free gas isinvestigated by following the evolution of accreting protostars with emphasis on the properties of massive objects.
The main aim is to establish the physical processes that
determine the upper mass limit of the first stars. Although
the consensus is that massive stars were commonly formedin the first cosmic structures, our calculations show that
their actual formation depends sensitively on the massaccretion rate and its time variation. Even in the rather idealized case in which starformation is mainly determined by
Mo acc, the characteristic mass scale of the first stars is rather
uncertain. We find that there is a critical mass accretion
rate Mo crit - 4 # 10 3 M 9 yr 1 that separates solutions with
Mo acc < Mo crit in which objects with mass & 100M 9 can form,
provided there is sufficient matter in the parent clouds,
from others (Mo acc > Mo crit) where the maximum mass limit
decreases as Mo acc increases. In the latter case, the protostellar luminosity reaches the Eddington limit before the onsetof hydrogen burning at the center via the CN-cycle. This
phase is followed by a rapid and dramatic expansion of theradius, possibly leading to reversal of the accretion flow
when the stellar mass is about 100 M 9.
Under a realistic time dependent accretion rate thatstarts at high values (+ 10 2 M 9 yr 1) and decreases rapidly
in the high mass regime (M ) > 90M 9), the evolution follows the case of Mo acc < Mo crit and accretion can continue
unimpeded by radiation forces. Thus, the maximum mass is
set by consideration of stellar lifetimes rather than by protostellar evolution. In this case, the upper limit can be as
high as + 600M 9.
We consider also the sensitivity of the results to thepresence of heavy elements with abundances in the range
Z = 5 # 10 5 Z 9 to 5 # 10 3 Z 9. The main evolutionary
features of protostars are similar to those of metal-freeobjects, except that the value of Mo crit increases for metalenriched protostars. Since the accretion rate is lower in aslightly polluted environment, the condition Mo acc < Mo crit isexpected to be more easily met. We find that for metallicities below + 10 2 Z 9, where radiation forces onto dust
grains in the flow are negligible, a slightly metal-rich gas
favors continued accretion and the formation of very massive stars.
References[1] Omukai, K. & Palla, F.: 2003, ApJ, 589, 677.
[2] Bromm, V., Kudritzki, R. P., & Loeb, A.: 2001, ApJ, 552, 464.
[3] Marigo, P., Girardi, L., Chiosi, C., & Wood, P.: 2001, A&A, 371,
152.

42

Figure1:Mass-radius relations for metal-free protostars evolving withan accretion rate Mo acc = 1/4, 1/2, 1, 2Mo fid (from top to bottom).
The dashed line is for Mo acc = Mo fid, where the fiducial value is3
Mo fid = 4.4 # 10 M 9 yr 1. The filled circles indicate theonset of H-burning via the CN-cycle.

Figure2:HR diagram for primordial protostars. For comparison, we also
show the locus of the metal-free ZAMS stars as computed by
Marigo et al. [3] for M ) < 100M 9 and by Bromm et al. [2] forhigher masses. The dotted lines show the temperature andluminosity at the stellar surface.

The Mass Spectrum of Metal-free Stars
Resulting from Photodissociation Feedback:
A Scenario for the Formation of Low-mass Population III StarsOMUKAI, Kazuyuki(Division of Theoretical Astrophysics, NAOJ)YOSHII, Yuzuru(IoA, Tokyo)

The initial mass function (IMF) of metal-free stars thatform in the initial starburst of massive (virial temperatures>10 4K) metal-free protogalaxies is studied. In particular,
we focus on the effect of H 2 photodissociation by pre-existing stars on the fragmentation mass scale, presumedly
determined by the Jeans mass at the end of the initial freefall phase, i.e., at the so-called “loitering phase,” characterized by the local temperature minimum. Photodissociation
diminishes the Jeans mass at the loitering phase, thereby
reducing the fragmentation mass scale of primordial
clouds. Thus, in a given cloud, far ultraviolet (FUV) radiation from the first star, which is supposedly very massive(+ 10 3 M 9), reduces the mass scale for subsequent fragmentation. Through a series of similar processes the IMF
for metal-free stars is established. If FUV radiation exceeds
a threshold level, the star-forming clumps collapse solely
through atomic cooling. Correspondingly, the fragmentation scale drops discontinuously from a few times 10M 9 to
sub-solar scales. In compact clouds (< 1.6 kpc for clouds ofgas mass 10 8 M 9), this level of radiation field is attained,
and sub-solar mass stars are formed even in a metal-freeenvironment. Consequently, the IMF becomes bi-modal,
with peaks at a few tenths of M 9 and a few times 10M 9.
The high-mass portion of the IMF, p high (m) ), is found to bea very steep function of the stellar mass m),
5
p high (m ) ) " m ) . Therefore, the typical mass scale ofmetal-free stars is significantly smaller than that of the very
first stars. In the Appendix we study the thermal instability
in collapsing primordial prestellar clumps, and discuss why
the thermal instability occuring during the three-body H 2
formation does not appear to manifest itself in causing further fragmentation of such clumps.
References[1] Omukai, K. & Yoshii, Y.: 2003, ApJ, 599, 746.

Figure1:The fragmentation mass scale as a function of the dilution factor W, which parametrizes the FUV radiation density.

Figure2:The initial mass function of metal-free stars in clouds of
8
M cl = 10 M 9. Shown are the results for the cloud lengthscale of 300pc (solid line), 500pc (dotted line), 1000pc (shortdashed line), and 3000pc (long-dashed line).

[2] Yoshii, Y.: 1981, A&A, 97, 280.
[3] Yoshii, Y., & Sabano, Y.: 1979, PASJ, 31, 505.
[4] Yoshii, Y., & Saio, H.: 1985, ApJ, 295, 521.
[5] Yoshii, Y., & Saio, H.: 1986, ApJ, 301, 587.

43

An S0-like Galaxy Found at Redshift 1.5
IYE, Masanori, KASHIKAWA, Nobunari, IMANISHI, Masatoshi, SAITO, Yoshihiko(NAOJ, Optical & Infrared Astronomy Division)

MIYAZAKI, Satoshi, SIMPSON, Chris(NAOJ, Subaru Telescope)

CHIBA, Masashi(NAOJ, Astrometry and Celestial Mechanics Division)

SHIMASAKU, Kazuhiro(Univ. Tokyo) and others

The first light imaging observation of a cluster of galaxies A851(CL0939+4713) at redshift 0.4 with the Subaru
SuprimeCam revealed its superb imaging capability withlimiting magnitude R=28 in 1 hour exposure [1]. A remarkable ERO (Extremely Red Object) found in this observation, ERO J094258+4659.2 with R–K=7.5, was originallyconsidered to be a gravitationally lens stretched image of abackground elliptical galaxy as the major axis of this imageis aligned with the equipotential surface of the lensing cluster.
However, following detailed imaging and spectroscopic
studies have shown that this is an S0-like galaxy with exponential luminosity profile, rather than a lensed ellipticalwith de Vaucouleurs' law, without recent star forming
activity and located in a field environment at redshift 1.5[2].
Although this is a single case of finding an S0-likegalaxy at such a high redshift, this finding places an important constraint on the galaxy formation scenario as ERO
J094258+4659.2 is likely to be a galaxy with dynamicallyrelaxed disk component of evolved stars without a conspic-

uous young population. The ordinary scenario of tidal stripping of disk galaxy to form an S0 in a cluster environment
cannot explain the origin of ERO J094258+4659.2, as it isin a field environment at redshift 1.5. Usual CDM scenario
shows the formation of massive galaxies takes place at redshift < 1 by successive merging of tiny galaxies. However,the lack of spectroscopic evidence of recent star forming
activity in this galaxy and the very well relaxed luminosity
profile of this galaxy imply that such a major merger event,if any, should have taken place long ago in this galaxy,meaning the epoch of formation of this galaxy much earlier
than redshift 1.5.
HST proposal to observe this galaxy was granted forcycle 13.
References[1] Iye, M. , Iwamuro,F., Maihara,T., et al.: 2000, Publ.Astron.Soc.
Japan, 52, 9.
[2] Iye, M., Shimasaku, K., Miyazaki, S. et al.: 2003, Astrophy. J., 590,
770.

Figure1: Multi band images of ERO J094258+4659.2(left) and its exponential luminosity profile(right)

44

Disappearing Dark Matter in Brane World Cosmology:
New Limits on Noncompact Extra Dimensions
ICHIKI, Kiyotomo, KAJINO, Toshiki(NAOJ/University of Tokyo)

YAHIRO, Masanobu

P. M. Garnavich, G. J. Mathews(University of Kyushu)(University of Notre Dame)figure1: Illustration of the energy densities with scale factor in models
with dark-matter decay into the extra dimension.

-1

figure2: Contours of constant | 2 in the C vs. X K plane. Lines drawn
correspond to 1, 2, and 3v confidence limits for fits to the magnituderedshift relation for Type Ia supernovae, the mass-to-light ratios ofgalaxy clusters, and constraints from the CMB. The dashed lines indicate contours of constant X as labeled. The dark radiation contribution
can be deduced from the figure, via X = 1 - X K - X - X B

We consider a brane-world cosmology whereby theuniverse is described as a three-brane embedded in a fivedimensional anti-de Sitter (AdS 5) bulk spacetime, andexplore cosmological implications of dark matter as massive particles trapped on a brane. It is an unavoidable consequence of this cosmology that massive particles aremetastable and can disappear into the bulk dimension.
Here, we assume that a massive dark matter particle (e.g.
the lightest supersymmetric particle) has the shortest lifetime C 1 for disappearing into the bulk. The energy flow ofdark matter particles into the bulk induces a back reaction
from the background gravitational field in the bulk andgenerates the ''dark radiation'' on the brane. As an example,
Figure 1 illustrates the evolution of a a simple flat,, disappearing dark matter cosmology with

Gyr. This cosmology separates into four characteristic
regimes identified on Figure 1. These are: I) The usual
early radiation dominated era; II) a dark-matter dominatedera; III) a late dark radiation dominated era ; and IV)
Eventually, a baryon-dominated regime also exists.
This new paradigm will change the standard thermal
history of the universe mainly in two ways. First, moredark matter particles in the past change the expansion history of the universe and lead the stronger decelerating expansion in the early universe. Second, the disappearance ofdark matter particles results in the increasing ratio of dark
matter density to that of baryon with look back time to thepast. We examine cosmological constraints on this newparadigm and show that disappearing dark matter is consistent (at the 95% confidence level) with all cosmologicalconstraints, i.e. present observations of Type Ia supernovae
at the highest redshift, trends in the mass-to-light ratios ofgalaxy clusters with redshift, the fraction of X-ray emitting
gas in rich clusters, and the spectrum of power fluctuationsin the cosmic microwave background. The result of ourstandard | 2 goodness of fit to the data sets are depicted in
Figure 2. In this figure, X K means the energy density incosmological constant (K) in critical density units, forexample. We find a minimum | 2 per degree of freedom of| 2r = 0.61 for C 1 = 34 Gyr for Cluster M/L data, which is an
improvement over the fit with a fixed M/L (assumed instandard cosmology) for which | 2r = 0.67. The Type Ia SN
implies | 2r = 0.94 for C 1 = 0.3 Gyr, which is to be compared | 2r = 0.96 for a standard KCDM cosmology.
Combining recent cosmic microwave background measurements by WMAP, a best 2v concordance region is identified corresponding to a mean lifetime for dark matter disappearance of 15 # C 1 # 80 Gyr. Should the dark-mattermass m0 ever be known, this would give a new limit on thefivedimensional
Planck
mass
to
1/2
1
1/6
(M 5 /M 4 ) . 4 (m0 /TeV) (C /15~Gyr) .
References[1] Dubovsky, S. L. et al.: 2000, PRD, 62, 105011.
[2] Ichiki, K. et al.: 2003, PRD, 68, 083518.

45

II Publications, Presentations
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46

Cook, K. H., Furuta, Y., Gal-Yam, A., Glicenstein, J.-F.,
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Matsubara, Y., Mizumoto, Y., Mori, M., Moro, H.,
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Astron. Obs. Japan, 7, 37−52.
3. Report of the National Astronomical Observatory ofJapan (in Japanese)
山本直孝，野田祥代，多賀正敏，小澤友彦，洞口俊博，奥村真一郎，古荘玲子，馬場 肇，八木雅文，安田直樹，高田唯史，
市川伸一：2003，すばる望遠鏡公開データアーカイブシステ
ムの開発2，国立天文台報，6，79−100．
山口喜助，桜井 隆，入江 誠，熊谷收可，萩野正興，宮下正邦，塩見靖彦，日江井榮二郎：2003，1991年６月４日の重要度3Bフレアとモートン波，国立天文台報，6，101−115．

田村友範，小林 研，常田佐久，久保雅仁, 勝川行雄：2003, 気
球観測用太陽姿勢センサーの開発と飛翔結果, 国立天文台報，
6, 117−127．

4. Other Publications
Akabane, K., and Kuno, N.: 2003, Dust Content in
Compact HⅡ Regions (NGC 7538 - IRS 1, IRS 2, andIRS 3), Proc. of the IAU 8th Asian-Pacific Regional
Meeting, V. II, eds. S. Ikeuchi, J. Hearnshaw, and T.
Hanawa, ASP Conf. Ser., 289, 121−122.
Arimoto, N., Ikuta, C., Jablonka, P.: 2004, Star Formation
Histories of Dwarf Galaxies in the Local Group, Proc.
Japan-German Seminar, eds. N. Arimoto, W. Duschl,
147−155.
Ariyoshi, S., Matsuo, H., Otani, C., Sato, H., Shimizu, H.,
Matsunaga, T., Noguchi, T.: 2003, Nb-Based
Superconducting Tunnel Junctions as SubmillimeterWave Direct Detectors, IEEE Trans. Applied Supercond.
13, 1128−1131.
Asada, K., Inoue, M., Kameno, S., and Uchida, Y.: 2003, A
Helical Magnetic Field in the Jet of 3C 273, Proc. of
Active galactic nuclei: from central engine to hostgalaxy, eds. S. Collin, F. Combes, and I. Shlosman, ASP
Conf. Ser., 290, 335−336.
Asai, A., Masuda, S., Yokoyama, T., Shimojo, M., Ishii, T.
T., Isobe, H., Shibata, K., and Kurokawa, H.: 2003,
Evolution of Flare Ribbons and Energy Release, Proc. of
the IAU 8th Asian-Pacific Regional Meeting, V. II, eds.
S. Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf.
Ser., 289, 415−416.
Asai, A., Yokoyama, T., Shimojo, M., Masuda, S.,
Kurokawa, H., and Shibata, K.: 2003, Evolution of Flare
Ribbons and Energy Release, 28th Int. Cosmic Ray Conf.
v. 6, eds. T. Kajita, Y. Asaoka, A. Kawachi, Y.
Matsubara, and M. Sasaki, 3367−3370.
Barraud, C., Atteia, J. L., Olive, J. F., Dezalay, J. P., Lamb,
D. Q., Kawai, N., Yoshida, A., Shirasaki, Y., Sakamoto,T., Tamagawa, T., Torii, K., Matsuoka, M., Fenimore, E.
E., Galassi, M., Tavenner, T., Donaghy, T. Q., Graziani,C.: 2003, The E-Peak Distribution of the GRBs Detected
by HETE FREGATE Instrument, Gamma-Ray Burst andAfterglow Astronomy 2001: A Workshop Celebrating theFirst Year of the HETE Mission. AIP Conf. Proc., 662,
59−62.
Boehnhardt, H., Barucci, A., Delsanti, A., Dotto, E.,
Lazzarin, M., Tozzi, G. P., Romon, J., Doressoundiram,
A., Peixinho, N., Davies, J. K., Hainaut, O., de Bergh, C.,
Barrera, L., Birkle, K., Meech, K., Ortiz, J. L., Rousselot,
P., Sekiguchi, T., Thomas, N., Watanabe, J., West, R. M.,
Fulchignoni, M.: 2003, Physical studies of KuiperBelt
objects: an ESO VLT large program, Discoveries andResearch Prospects from 6- to 10-Meter-Class
Telescopes II, ed. Guhathakurta, Puragra. Proc. SPIE,
4834, 383−394.
Boku, T., Sato, M., Onuma, K., Makino, J., Susa, H.,
Takahashi, D., Umemura, M., and Ukawa, A.: 2003,
HMCS-G: Grid Enabled Hybrid Computing System for
Computational Astrophysics, Proc. of Grid and59

Advanced Network (GAN'03) in CCGrid2003, 558−565.
Byun, D.-Y., Koo, B.-C., Tatematsu, K., and Sunada, K.:
2003, Interaction between the Supernova Remnant HB21
and Molecular Clouds, Proc. of the IAU 8th AsianPacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 131−
132.
Deguchi, S.: 2003, SiO Maser Sources Near the Galactic
Center, Workshop on Mass-Losing Pulsating Stars andtheir Circumstellar Matter, eds. Y. Nakada, M. Honma,
and M. Seki, ASSL, 283, 347−354.
Dermawan, B., Nakamura, T., Yoshida, F., Sato, Y.: 2003,
Application of CLEAN Algorithm to Detection ofAsteroids with Multi-period Rotations, Proc. of the 36th
ISAS Lunar and Planetary Symp., 196−199.
Dobashi, K., Uehara, H., Kandori, R., Umemoto, T., andSato, F.: 2003, A Catalogue of Dark Clouds Using theDigitized Sky Survey I, Proc. of the IAU 8th AsianPacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 67−68.
Doi, M., Fadeyev, V., Lee, B., Stanishev, V., Vogel, R.,
Yasuda, N., Kashikawa, N., Motohara, K., Morokuma,
T., Sekiguchi, K.., Kosugi, G., Furusawa, H., Komiyama,Y., Takata, T., Ouchi, M., and Ohyama, Y.: 2003,
Supernovae 2002km-2002ky, IAU Circ., 8119, 1.
Ebizuka, N., Oka, K., Yamada, A., Watanabe, M., Shimizu,
K., Kotate, K., Kawabata, M., Teranishi, T., Kawabata,K. S., and Iye, M.: 2003, Development of Volume Phase
Holographic (VPH) Grism for Visible to Near Infrared
Instruments of the 8.2m Subaru Telescope, Proc. SPIE,
4842, 319−328.
Ellis, R. S., Tren, T., Conselice, C., van Dokkum, P.,
Fukugita, M., Kodama, T.: 2003, Mass Assembly of
Galaxies Through Detailed Studies at z=1, Maps of the
Cosmos, Proc. of IAU symp., 216. 20.
Enoki, M., Takahara, F., and Fujita, Y.: 2004, A model prediction of X-ray luminosity and temperature function ofgalaxy clusters considering the formation epoch distribution, Studies of Galaxies in the Young Universe with New
Generation Telescope, Proc. of Japan-German Seminar,
139−142.
Fujita, Y., and Suzuki, T.-K.: 2004, Heating of Cluster
Cores by Acoustic Waves, Proc. of The Riddle ofCooling Flows in Galaxies and Clusters of Galaxies,
published electronically at http://www.astro.virginia.edu/
coolflow/.
Gaessler, W., Takami, H., Takato, N., Hayano, Y., Kamata,Y., Iye, M.: 2003, Software and algorithms of Subaru
AO, Proc. SPIE, 4839, 954−963.
Goto, M., Hayano, Y., Kobayashi, N., Terada, H., Pyo, T.-S.,
Tokunaga, A. T., Takami, H., Takato, N., Minowa, Y.,
Gaessler, W., Iye, M.: 2003, Spectroscopy with Adaptive
Optics : Spectroral Slope Variations, Proc. SPIE, 4839,
1117−1123.
Goto, M., McCall, B. J., Geballe, T. R., Usuda, T.,
Kobayashi, N., Terada, H., and Oka, T.: 2003, The Proc.
of the IAU 8th Asian-Pacific Regional Meeting, Volume
I, eds. I. Satoru, H. John, and H. Tomoyuki, ASP Conf.
Ser., 289, 189−193.

60

Goto, M., Tokunaga, A. T., Cushing, M., Potter, D.,
Kobayashi, N., Takami, H., Takato, N., Terada, H.,
Hayano, Y., Iye, M., Gaessler, W., and Saint-Jacques, D.
J.: 2003, Brown Dwarfs, ed. M. Eduardo, Proc. of IAU
Symp., 211, 263.
Gouda, N., Tsujimoto, T., Kobayashi, Y., Nakajima, T.,
Matsuhara, H., Yano, T., Yasuda, N., Kan-ya, Y.,
Yamada, Y., Ueno, M.: 2003, Introduction of Japanese
astrometry satellite mission for infrared exploration(JASMINE), IR Space Telescope and Instruments, ed. J.
C. Mather, Proc. SPIE, 4850, 1161−1168.
Gouda, N., Tsujimoto, T., Kobayashi, Y., Nakajima, T.,
Yasuda, N., Kan-Ya, Y., Matsuhara, H., Yano, T.,
Yamada, Y., Ueno, M.: 2003, IR space astrometry - JASMINE project, Mass-losing pulsating stars and their circumstellar matter, ed. Y. Nakada, M. Honma and M.
Seki, Astrophysics and Space Science Library., 283,
397−404.
Gouda, N., Yano, T., Kobayashi, Y., Yamada, Y.,
Tsujimoto, T., Ueda, S., and JASMINE working group:
2003, Exploration of Near-Field Cosmology by theInfrared Space Astrometry (JASMINE), The Proc. of
Frontier in Astroparticle Physics and Cosmology(RESCEU Int. Symp.), 373−374.
Graziani, C., Shirasaki, Y., Donaghy, T., Fenimore, E.,
Galassi, M., Kawai, N., Lamb, D. Q., Sakamoto, T.,
Takahashi, D., Tamagawa, T., Tavenner, T., Torii, K.,
Yoshida, A., Vanderspek, R.: 2003, Astrometric
Calibration and Estimate of the Systematic Error in
WXM Localizations Obtained by the Chicago Bayesian
Method, Gamma-Ray Burst and Afterglow Astronomy
2001: A Workshop Celebrating the First Year of the
HETE Mission. AIP Conf. Proc., 662, 114−116.
Guyon, O., Ridgway, S., Pupil Remapping Apodization
Study Group Collaboration: 2003, Pupil Remapping
Apodization: A 2m Terrestrial Planet Finder?, American
Astronomical Society Meeting, 203, 03.01.
Hanada, H., Iwata, T., Namiki, N., Matsumoto, K., Tsuruta,
S., Ishikawa, T., Asari, K., Noda, H., Kono, Y., Ping, J.,
Liu, Q., Kikuchi, F., Heki, K., Kawano, N., and
RSAT/VRAD group: 2003, Present status of gravimetricmissions in SELENE/RISE, IVS CRL-TDC News, 23,
43−45.
Hasegawa, S., Hiroi, T., Ishiguro, M., Nonaka, H., Takato,N., Davis, C. J., Ueno, M., and Murakawa, K.: 2004,
Spectroscopic Observations of Asteroid 4 Vesta from 1.9
to 3.5 micron: Evidence of Hydrated and/or
Hydroxylated Minerals, 35th Lunar and Planetary
Science Conf., 35, 1458.
Hayano, Y., Takami, H., Gaessler, W., Takato, N., Kamata,Y., Minowa, Y., Kobayashi, N., Iye, M.: 2003, Upgradeplans for the Subaru AO system, Proc. SPIE, 4839, 32−
43.
Hirabayashi, H., Edwards, P. G., Murata, Y., Asaki, Y.,
Murphy, D. W., Kobayashi, H., Inoue, M., Kameno, S.,
and Umemoto, T.: 2003, Highlight from the First Five
Years of the VSOP Mission, Proc. of the IAU 8th AsianPacific Regional Meeting, V. I, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 375−

378.
Hiroi, K., Umemura, M., and Nakamoto, T.: 2003,
Constraints on Cosmic Reionization from High-Z QSO
Spectra, Maps of the Cosmos, Proc. of IAU symp., 216,
208−209.
Ichikawa, T., Matsumoto, D., Yanagisawa, K., Katsuno, Y.,
Suzuki, R., Tokoku, C., Asai, K., Nishimura, T.: 2003,
Tohoku University Focal Plane Array Controller (TUFPAC), Proc. SPIE, 4841, 376.
Ichiki, K., Garnavich, P., Kajino, T., Mathews, G. J., andYahiro, M.: 2004, 6th RESCEU Int. Symp. on Frontier in
Astroparticle Physics and Cosmology, eds. K. Sato and S.
Nagataki (Universal Academy Press), 307−311.
Iguchi, S., Kawaguchi, N., Okumura, S. K., and Sunada, K.:
2003, The Gigabit Digital Filter and the High-Speed
ADC (Analog-to-Digital Converter) for Radio
Astronomy, Proc. of the New Technologies in VLBI, ed.
Y. C. Mihn, ASP Conf. Ser., 306, 161−176.
Ikuta, C., Arimoto, N.: 2003, Stellar Populations in
Globular Clusters and Dwarf Galaxies, New Horizona in
Globular Clusters Astronomy, ASP Conf. Ser., 296, 587.
Imai, H., Deguchi, S., Nakashima, J., Miyazaki, A., Kameya,O., Fujii, T., Ita, Y., Nakada, Y., Izumiura, H., and Glass,
I. S.: 2003, SiO Maser Survey towards the Stellar Cluster
at the Galactic Center, Mass-Losing Pulsating Stars andtheir Circumstellar Matter, eds. Y. Nakada, M. Honma,
and M. Seki, Astrophysics and Space Science Library,
283, 373−376.
Imanishi, M.: 2003, 3-4 Micron Spectroscopy of 17 Seyfert
2 Nuclei: Quantification of the Compact Starburst
Contribution, The Proc. of the IAU 8th Asian-PacificRegional Meeting, ASP Conf. Proc. Volume I, 289, 345−
348.
Inoue, M., Asada, K., and Uchida, Y.: 2003, Thermal
Electrons in the Helical Magnetic Field of 3C 273, Proc.
of the Radio Astronomy Fringe, eds. J. A. Zensus, M. H.
Cohen, and E. Ros, ASP Conf. Ser., 300, 141−142.
Ishii, M., Tamura, M., Nagata, T., Sato, S., Yao, Y., Jiang,Z., and Yanagisawa, K.: 2003, K band spectroscopy of
Herbig Ae/Be stars, American Astronomical Society
Meeting, 202, 28.03.
Isobe, H., Shibata, K., Yokoyama, T., and Imanishi, K.:
2003, Hydrodynamic Modeling of a Protostellar Flare
Loop Connecting a Central Star with its Accretion Disk,
Proc. of the IAU 8th Asian-Pacific Regional Meeting, V.
II, eds. S. Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP
Conf. Ser., 289, 433−434.
Itoh, Y., Tamura, M., Hayashi, S. S., Oasa, Y., Fukagawa,
M., Suto, H., Murakawa, K., Naoi, T.: 2003, Subaru
Coronagraphic Search for Companion Brown Dwarfs,
Brown Dwarfs, ed. M. Eduardo, IAU Symp., 211, 293−
294.
Iye, M.: 2003, Scientific results with the Subaru Telescope,Proc. SPIE, 4834, 288−301.
Iye, M.: 2004, ERO R1 in CL0939+4713 - An Evidence for
an S0 Galaxy at Redshift 1.5, Studies of Galaxies in the
Young Universe with New Generation Telescope, Proc.
Japan-German Seminar, eds. N. Arimoto and W. Duschl,
9.

Iye. M., Kashikawa, N., Imanishi,M., Kodama, T.,
Chiba, M., Shimasaku, K., Okamura, S., Miyazaki, S.,
Simpson, C., Kobayashi, N., Terada, H., Goto, M.,
Iwamuro, F.: 2003, Evidence for an S0-Like Galaxy at
z=1.5, Dark Matter in Galaxies, Proc. of IAU symp., 220,
181.
Izumiura, H.: 2003, Violet spectra of carbon stars associated with silicate features, Mass-losing pulsating stars andtheir circumstellar matter, eds. Y. Nakada, M. Honma,
and M. Seki, Astrophysics and Space Science Library,
283, 189.
Kajino, T., Sasaqui, T., Orito, M., Otsuki, K., Mathews, G.
J., Honda, S., Aoki, W., and Chiba, S.: 2004,
Nucleosynthesis in Supernovae and the Early Universe,
5th Tours Int. Conf. on Nuclear Physics, AIP Conf.
Proc., 704, 488−497.
Kameya, O., Kobayashi, H., Sato, K., Miyaji, T., Iwadate,K., Horiai, K., Sasao, T., Omodaka, T., and the VERA
team: 2003, Construction and Current Status of The
VERA Stations, Proc. of the IAU 8th Asian-PacificRegional Meeting, V. II, eds. S. Ikeuchi, J. Hearnshaw,
and T. Hanawa, ASP Conf. Ser., 289, 15, 2003.
Kameya, O.: 2003, Mizusawa 10m Antenna System forStudy of Pulsating Stars, Mass-losing Pulsating Stars andtheir Circumstellar Matter -Observations and Theory-,
Mass-losing Pulsating Stars and their Circumstellar
Matter -Newest Results of Observations and Theory-,
eds. Y. Nakada, M. Honma, and M. Seki (Kluwer
Academic), 409−410.
Kandori, R., Dobashi, K., Uehara, H., Sato, F., andYanagisawa, K.: 2003, Extensive Extinction Maps ofDark Clouds at Multiple Wavelengths, Proc. of the IAU
8th Asian-Pacific Regional Meeting, V. II, eds. S.
Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf. Ser.,
289, 153−154.
Kasuga, T., Tsuboi, M., Miyahara, H., Miyazaki, A., andShinnaga, H.: 2003, Search for Polarization towards
Sagittarius A* at 100 GHz, Proc. of the IAU 8th AsianPacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 383.
Kasuga, T., Yamamoto, T., Watanabe, J., Abe, S., Ebizuka,N., Sugimoto, M., Yano, H.: 2003, Metallic abundancesof the 2002 Leonid meteor, Proc. 36th ISAS Lunar andPlanetary Symp., 36, 192−195.
Kawabata, K. S., Ebizuka, N., Sasaki, T., Sekiguchi, K., Iye,
M., Aoki, K., Asai, R., Inata, M., Kashikawa, N., Kosugi,G., Misawa, T., Ohyama, Y., Okita, K., Ozawa, T., Saito,
Y., Shimizu, Y., Taguchi, H., Takata, T., Yadoumaru, Y.,
and Yoshida, M.: 2003, Properties of FOCAS Optical
Components, Instrument Design and Performance for
Optical/Infrared Ground-based Telescopes, eds. M. Iya
and A. F. M. Moorwood, Proc. SPIE, 4841, 1219.
Kawabata, K. S., Kosugi, G., Iye, M., Sasaki, T., Ohyama,Y., Deng, J., Nomoto, K., Mazzali, P.: 2003, GRB
030329 and Supernova 2003dh, IAU Circ., 8133, 2.
Kawabata, K. S., Ohyama, Y., Nomoto, K., Mazzali, P., andWang, L.: 2003, Supernova 2002ic, IAU Circ., 8161, 3.
Kawabata, K., Tanikawa, K., Sôma, M.: 2004, TT–UT in
the seventh century derived from astronomical records in61

the Nihongi, the Suishu, and the Jiu- and Xin-Tangshu,
Astronomical Instruments and Archives from the AsiaPacific Region, eds. W. Orchiston, R. Stephenson, S.
Débarbat, I.-S. Nha (Yonsei University Press), 113−118.
Kawai, N., Yoshida, A., Matsuoka, M., Shirasaki, Y.,
Tamagawa, T., Torii, K., Sakamoto, T., Takahashi, D.,
Fenimore, E., Galassi, M., Tavenner, T., Lamb, D. Q.,
Graziani, C., Donaghy, T., Vanderspek, R., Yamauchi,M., Takagishi, K., Hatsukade, I.: 2003, In-Orbit
Performance of WXM (Wide-Field X-Ray Monitor),
Gamma-Ray Burst and Afterglow Astronomy 2001: A
Workshop Celebrating the First Year of the HETE
Mission. AIP Conf. Proc., 662, 25−32.
Kawakatu, N., and Umemura, M.: 2003, Quasar Formation;
Coevolution of Bulge to Nucleus, Maps of the Cosmos,
Proc. of IAU symp., 216, 55−56.
Kawakatu, N., and Umemura, M.: 2003, RadiationHydrodynamic Formation of Massive Black Hole,Dynamics and Evolution of Dense Stellar Systems, IAU
Joint Discussion, 11, 19−20.
Kawakita, H., Watanabe, J.-I., Furusho, R., and Fuse, T.:
2003, Relationship Between Spin Temperatures andChemical Compositions in Comets, American
Astronomical Society, DPS meeting, 35, #38.06.
Kawakita, H., Watanabe, J., Sasaki, S., Sasaki, T., Takato,N., and Fuse, T.: 2003, Comet C/2002 T7 (LINEAR),
IAU Circ., 8206, 3.
Kawamura, S.: 2003, Laser Interferometric GravitationalWave Detectors in Future, Proc. of 12th Workshop on
General Relativity and Gravitation, eds. M. Shibata, Y.
Eriguchi, K. Taniguchi, T. Nakamura, K. Tomita, 55.
Kikuchi, F., Kono, Y., Ping, J., Liu, Q., Asari, K.,
Matsumoto, K., Tsuruta, S., Hanada, H., Kawano, N., andNOZOMI VLBI group: 2003, VLBI observation byreceiving narrow bandwidth signal from NOZOMI, IVS
CRL-TDC News, 23, 36−38.
Kitayama, T., Susa, H., Umemura, M., and Ikeuchi, S.:
2003, Radiation-Hydrodynamical Simulations of
Primordial Galaxy Formation in the UV Background,Astrophysical Supercomputing using Particle
Simulations, IAU Symp., 208, 417−418.
Kobayashi, H., Sasao, T., Kawaguchi, N., Manabe, S.,
Omodaka, T., Kameya, O., Shibata, K. M., Miyaji, T.,
Honma, M., Tamura, Y., Hirota, T., Kuji, S., Horiai, K.,
Sakai, S., Sato, K., Iwadate, K., Kanya, Y., Ujihara, H.,
Jike, T., Fujii, T., Motiduki, N., Oyama, T., Kurayama,
H., Kamohara, R., Suda, H., and Kasuga, T.: 2003,
VERA: A New VLBI Instrument Free from theAtmosphere, Proc. of the New Technologies in VLBI, ed.
Y. C. Mihn, ASP Conf. Ser., 306, 367−371.
Kobayashi, K., Tsuneta, S., Tamura, T., Kumagai, K.,
Katsukawa, Y., Kubo, M., Yamagami, T., and Saito, Y.:
2003, Balloon-Borne Hard X-Ray Spectrometer for Flare
Observations, Proc. SPIE, 4851, 1009−1018.
Kobayashi, Y., Yoshii, Y., Minezaki, T., Enya, K., Aoki, T.,
Suganuma, M., Tomita, H., Doi, M., Motohara, K.,
Peterson, B. A., Smith, C. H., Little, J. K., Greene, B.:
2003, Automated observatory for multicolor active galactic nuclei monitoring (MAGNUM), Large Ground-based

62

Telescopes, eds. J. M. Oschmann, L. M. Stepp, Proc.
SPIE, 4837, 954−964.
Koda, J., Sofue, Y., Kohno, K., Okumura, S. K., and Irwin,
J. A.: 2003, A Weak Bar Potential and Massive Core in
the Seyfert 2 Galaxy NGC 3079: CO(1-0) Observations
Using the Nobeyama Millimeter Array, Proc. of the IAU
8th Asian-Pacific Regional Meeting, V. II, eds. S.
Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf. Ser.,
289, 387−388.
Kodama, T., Smail, I., Nakata, F., Okamura, S., Bower, R.
G.: 2004, History of Mass Assembly and Star Formationin Galaxy Cluster, Proc. of Japan-German Seminar,
Studies of Galaxies in the Young Universe with New
Generation Telescope, 23−31.
Koyama, H., and Yano, T.: 2003, The relation between the
two-point and the three-point correlation functions in the
non-linear gravitational clustering regime, Proc. of the
6th RESCEU Int. Symp., 421−422.
Kuno, N., Nakai, N., Sorai, K., Sato, N., Yamauchi, A.,
Tosaki, T., Shioya, Y., Vila-Vilaro, B., Nishiyama, K.,
Ishihara, Y., and Cepa, J.: 2003, Nobeyama CO Atlas of
Nearby Spiral Galaxies, Proc. of the IAU 8th AsianPacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 71−72.
Makino, J., Kokubo, E., and Fukushige, T.: 2003,
Evaluation and Tuning of GRAPE-6 - Toward 40 Real
Tflops, Proc. of SC2003, CD-ROM.
Mariska, J. T., Brown, C. M., Dere, K. P., Doschek, G. A.,
Korendyke, C. M., Myers, S. H., Seely, J. F., Culhane, J.
L., and Watanabe, T.: 2003, Expected Performance of theExtreme Ultraviolet Imaging Spectrometer on Solar-B,
American Astronomical Society, SPD meeting, 34, 20.06.
Matsuo, H., Ariyoshi, S., Otani, C., Shimizu, H.: 2003, SIS
Photon Detectors in Submillimeter-wave: optical andelectrical performance, The 28th Int. Conf. on Infrared
and Millimeter Waves, 2003,115−116.
Matsushita, M., Takata, T., Ikeda, Y., Hirao, N., Saito, M.,
Chiba, Y., and Takeyama, Y.: 2004, Development of
Ground-based Lunar VIS/NEAR IR Spectral Imager,
35th Lunar and Planetary Science Conf., 35, 1595.
Misawa, T., Kashikawa, N., Ohyama, Y., Iye, M.: 2004,
QSO Metal Absorption Systems at High Redshift,Studies of Galaxies in the Young Universe with New
Generation Telescope, Proc. Japan-German Seminar,eds. N. Arimoto and W. Duschl, 142−146.
Miyagoshi, T., and Yokoyama, T.: 2003, Formation ofCoronal Magnetic Structures by Emergence of a Twisted
Flux Tube studied by Three-Dimensional MHD
Numerical Simulations, Proc. of the IAU 8th AsianPacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 447−
448.
Miyawaki, R., Hasegawa, T., and Hayashi, M.: 2003,
Cluster of Massive Stars and Hot Cores in W49A, Proc.
of the IAU 8th Asian-Pacific Regional Meeting, V. II,
eds. S. Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf.
Ser., 289, 171−172.
Miyazaki, A., Sunada, K., Kitamura, Y., Kawamura, A.,
Inutsuka, S.-I., Sawada, T., Koyama, H., Morino, J.-I.:2003, Properties of Molecular Clumps in the TaurusAuriga Region, IAU Symp., 221, 235.
Miyoshi, M., Kameno, S., and Falcke, H.: 2003, A Proposal
for Constructing a New VLBI Array, Horizon Telescope,Proc. of the IAU 8th Asian-Pacific Regional Meeting, V.
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Sakamoto, S.: 2003, Detailed Structure and Kinematics of
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Clusters, Proc. of the IAU 8th Asian-Pacific Regional
Meeting, V. I, eds. S. Ikeuchi, J. Hearnshaw, and T.
Hanawa, ASP Conf. Ser., 289, 255−258.
Tsujimoto, M., Koyama, K., Imanishi, K., Kobayashi, N.,
Saito, M., and Tsuboi, Y.: 2003, Radio Centimeter
Emissions at a Protostellar Core in OMC-3 and its
Association with X-ray and NIR, Proc. of the IAU 8th
Asian-Pacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 223−
224.
Tsujimoto, T., and Shigeyama, T.: 2004, Histories of the
Milky Way Dwarf Spheroidal Galaxies and w Centauri,
Origin and Evolution of the Elements, from the Carnegie
Observatories Centennial Symposia. Carnegie
Observatories Astrophysics Series, 57−66.
Tsunesada, Y., and the TAMA Collaboration: 2003, Search
for Gravitational Waves from Ringing-down Black
Holes, The 28th Int. Cosmic Ray Conf. Proc., OG3.2,
3055.
Uehara, H., Dobashi, K., Kandori, R., and Sato, F.: 2003, A
Museum of Dark Clouds on the Internet, Proc. of the
IAU 8th Asian-Pacific Regional Meeting, V. II, eds. S.
Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf. Ser.,
289, 109−110.
Ujihara, H., Chikada, Y., and Nakahira, K.: 2003, Aperture
Efficiency of 90-cm Film Lens Antennas, Proc. of the
IAU 8th Asian-Pacific Regional Meeting, V. II, eds. S.
Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf. Ser.,
289, 33−34.
Umemoto, T., Kamazaki, T., Sunada, K., Kitamura, Y., andHasegawa, T.: 2003, Fragmentation in the r Ophiuchi
Cluster Forming Region, Proc. of the IAU 8th Asian-Pacific Regional Meeting, V. II, eds. S. Ikeuchi, J.
Hearnshaw, and T. Hanawa, ASP Conf. Ser., 289, 229−
230.
Umemura, M., and Kawakatu, N.: 2003, A New Picture of
QSO Formation, The 8th IAU Asian-Pacific Regional
Meeting, 363−366.
Umemura, M., Nakamoto, T., and Susa, H.: 2004, The
Epoch of Cosmic Reionization, Studies of Galaxies in the
Young Universe with New Generation Telescopes,
Japan-German Seminor 2002, 77−82.
Uraguchi, F., Takato, N., Miyashita, A., Yanagisawa, K.,
Okada, N.: 2003, DIMM with large aperture separationand simultaneous seeing measurements at Mauna Kea,
Large Ground-based Telescopes, eds. J. M. Oschmann,
L. M. Stepp, Proc. SPIE, 4837, 864−871.
Wada, K., Norman, C. A.: 2003, The Starburst-AGN
Connection: 3-D Structure of the Massive Gas Disk
around the Nucleus, IAU Symp. 208: AstrophysicalSupercomputing using Particle Simulations, ASP conf.
Ser., 463−464.
Wada, K.: 2003, Computer Center at NAOJ:
Supercomputing Facilities and Products, Numerical
Simulations in Astronomy 2002, 1−6.
Wada, K.: 2003, Obscuring Material around the Central
Engine with Starbursts, Active Galactic Nuclei: fromCentral Engine to Host Galaxy, ASP Conf. Ser., 290,
261−262.
Yahagi, H., Nagashima, M., Enoki, M., Gouda, N., andYoshii, Y.: 2003, Numerical Galaxy Catalog: a High
Resolution Galaxy Catalog, The Proc. of the IAU symp.,
216, 65.
Yamaguchi, Y., and Tanikawa, K.: 2003, A zone void ofmonotone points in the standard map, Proc. of the 35th
Symp. on Celestial Mechanics, eds. E. Kokubo, H.
Arakida, and T. Yamamoto, 385−395.
Yamamoto, F., Hasegawa, T., Sawada, T., Sugimoto, M.,
Naitoh, S., Handa, T., and Sofue, Y.: 2003, Survey of
Molecular Clouds around Galactic SNRs, Proc. of the
IAU 8th Asian-Pacific Regional Meeting, V. II, eds. S.
Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf. Ser.,
289, 235−236.
Yamauchi, Y., Suess, S., and Sakurai, T.: 2003, Relation
between Polar Plumes and Fine Structure in the Solar
Wind from Ulysses High-Latitude Observations, Proc. of
the Tenth Int. Solar Wind Conf., AIP Conf. Proc., 679,
255−258.
Yanagisawa, T., Nakamura, T., Yoshida, F., Dermawan, B.,
Sato, Y., Nakajima, A.: 2003, Detection of Small MainBelt Asteroids on the SUBARU Images using the
Stacking Method, Proc. of the 36th ISAS Lunar andPlanetary Symp., 169−172.
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Yamada,Y., Kan-Ya, Y., Araki, H., Tazawa, S., Asari, K., Tsuruta,
S., Hanada, H., and Kawano, N.: 2003, Japanese
Astrometry Satellite Mission - Jasmine Project, The
Proc. of the 25th meeting of the IAU, Joint Discussion,
16, 55−58.
Yano, T., Koyama, H., Buchert, T., and Gouda, N.: 2003,
Distribution of Caustics in the Expanding Universe, The

Proc. of Frontier in Astroparticle Physics andCosmology (RESCEU Int. Symp.), 519−520.
Yokogawa, S., Kitamura, Y., Momose, M., and Kawabe, R.:
2003, Deep 13CO (J=1-0) Imaging of the Protostar Haro
6-5B: Discovery of Rotational Motion in the Protostellar
Disk, Proc. of the IAU 8th Asian-Pacific Regional
Meeting, V. II, eds. S. Ikeuchi, J. Hearnshaw, and T.
Hanawa, ASP Conf. Ser., 289, 239−240.
Yokoyama, T., Nakajima, H., Shibasaki, K., Melnikov, V.
F., and Stepanov, A. V.: 2003, A Microwave Imaging
Observation of an Electron Stream in a Solar Flare by
Nobeyama Radioheliograph, 28th Int. Cosmic Ray Conf.,
v. 6, eds. T. Kajita, Y. Asaoka, A. Kawachi, Y.
Matsubara, and M. Sasaki, 3359−3362.
Yokoyama, T.: 2003, MHD Simulation of a Solar Flare
Based on the Magnetic Reconnection Model, Proc. of the
IAU 8th Asian-Pacific Regional Meeting, V. II, eds. S.
Ikeuchi, J. Hearnshaw, and T. Hanawa, ASP Conf. Ser.,
289, 473−474.
Yonehara, A., Umemura, M., and Susa, H.: 2003, Quasar
Mesolensing as a Probe of CDM Substructures, Dark
Matter in Galaxies, IAU Symp., 220, 106−107.
Yonehara, A., Umemura, M., and Susa, H.: 2003, Towards
Direct Detection of Substructure around Galaxies −Quasar Mesolensing, The 8th IAU Asian-PacificRegional Meeting, 469−472.
Yoshida, F.: 2003, Size and Distribution of Faint Jovian L4Trojan Asteroids, Annual progress report to NSC,
Taiwan.
Yoshida, M., Yagi, M., Okamura, S., Aoki, K., Ohyama, Y.,
Komiyama, Y., Yasuda, N., Iye, M., Kashiawa, N., Doi,
M., Furusawa, H., Hamabe, M., Kimura, M., Miyazaki,M., Miyazaki, S., Nakata, F., Ouchi, M., Sekiguchi, M.,
Shimasaku, K., and Ohtani, H.: 2003, Very Extended
Emission-Line Region around the Seyfert 2 Galaxy NGC
4388, The Proc. of the IAU 8th Asian-Pacific Regional
Meeting, Volume II, eds. S. Ikeuchi, J. Hearnshaw, and T.
Hanawa, ASP Conf. Ser. 289, 337−340.
Yoshida, M., Yagi, M., Okamura, S., Ohyama, Y., Miyazaki,
S., Yasuda, N., Aoki, K., and Iye, M.: 2003, Deep
Spectroscopy of Very Extended Ionized Gas of NGC
4388, Recycling Intergalactic and Interstellar Matter,
IAU Symp. 217, 142.
Yoshida, N.: 2003, Structure formation in the early universe, Proc. 6th RESCEU Symp., 217−224.
Yoshida, T., and Hashimoto, M.: 2003, Supernova
Nucleosynthesis and C, N, Al, Si, and Ti Isotopic Ratios
of Presolar Grains from Supernovae, Proc. of the 36th
ISAS Lunar and Planetary Symp., 113−116.
Yoshii, Y., Kobayashi, Y., Minezaki, T.: 2003, The MAGNUM (Multicolor Active Galactic NUclei Monitoring)
Project, American Astronomical Society Meeting, 202,
38.03.
5. Presentations
Aoki, W.: 2003, Measurements of Li and Eu abundances inmetal-defecient stars, Origin of Matter and Evolution of
the Galaxies, (Saitama, Nov. 17−19).

67

Aoki, W.: 2003, Subaru/HDS Studies of Carbon-Rich Very
Metal-Poor Stars, Elemental Abundances in Old Stars
and Damped Lyman-α Systems, 25th meeting of the
IAU, Joint Discussion 15, (Sydney, Australia, July 22).
Arai, K., and the TAMA Collaboration: 2003, Operation of
TAMA300 Detector, 10th Marcel Grossmann Meetingon General Relativity, (Rio de Janeiro, Brazil, July 2026).
Arai, K., and the TAMA Collaboration: 2003, Report on
the Observation Run of TAMA300 in the Spring of 2003,
The 28th Int. Cosmic Ray Conf., (Tsukuba, July 31-Aug.
7).
Arai, K.: 2003, Observation runs of an interferometric gravitational wave detector TAMA300, 10th Marcel
Grossmann Meeting on General Relativity, (Rio deJaneiro, Brazil, July 20−26).
Arimoto, N.: 2003, Spectroscopic Ages of EllipticalsSubaru Observation, ESO Workshop “Multiwavelength
Mapping of Galaxy Formation and Evolution”, (Venice,
Italy, Oct. 13−16).
Arimoto, N.: 2003, Submm Galaxies-Star Forming ProtoEllipticals at z>2?, Stellar Populations 2003, (Garching,
Germany, Oct. 6−10).
Beers, T. C., Chiba, M., et al.: 2003, The Mass of the
Galaxy from Large Samples of FHB Stars, in Dark
Matter in Galaxies, IAU Symp. 220, (Sydney, Australia,
July 22−25).
Chiba, M., Mizutani, A.: 2003, On the kinematics of tidal
debris from Omega Cen's progenitor galaxy, in Galactic
Chemodynamics, (Melbourne, Australia, July 9−11).
Enoki, M., Inoue, K. T., Sugiyama, N., and Nagashima, M.:
2003, Gravitational Background Radiation from Super
Massive Black Hole Coalescence, Workshop on StellarMass, Intermediate-Mass, and Supermassive Black
Holes, (Japan, Oct. 28−31)."
Fujimoto, H., Sato, T., Mochizuki, M., Mitsuzawa, K., andTamaki, T.: 2003, Ocean bottom pressure variations inthe southern Pacific following the 1997-98 El Nino
event, EGS/AGU/EUG Joint Assembly, (Nice, France,
Apr. 6).
Fujita, Y.: 2003, Heating of Cluster Cores By Acoustic
Waves, The Riddle of Cooling Flows in Galaxies andClusters of Galaxies, (Charlottesville, May. 31 - Jun. 4).
Furusho, R., Kawakita, H., Watanabe, J., Fujii, M.: 2003,
Sodium Emission in Cometary Comae, Formation of
Cometary Material, 25th meeting of the IAU, Joint
Discussion 14, (Sydney, Australia, July 22).
Gouda, N., Yano, T., Kobayashi, Y., Yamada, Y.,
Tsujimoto, T., Ueda, S., and JASMINE working group:
2003, Exploration of Near-Field Cosmology by theInfrared Space Astrometry (JASMINE), Frontier in
Astroparticle Physics and Cosmology (RESCEU Int.
Symp.), (Tokyo, Nov. 4−7).
Guyon, O., Ridgway, S., Otsubo, M.: 2003, Phase-induced
pupil apodization: a new concept for a simplier DARWIN/TPF, Proc. of the Conference on Towards Other
Earths: DARWIN/TPF and the Search for Extrasolar
Terrestrial Planets, (Heidelberg, Germany, Apr. 22−25).
Hamana, T.: 2003, Searching for massive clusters in weak68

lensing surveys, the 6th RESCEU International
Symposium, (Tokyo, Nov. 4−7).
Hamana, T.: 2004, Suprime-33: Suprime-Cam weak lensing survey, IAU symp. 208, (Torino, Mar. 12−16).
Hanada, H., Heki, K., Araki, H., Matsumoto, K., Noda, H.,
Kawano, N., Tsubokawa, T., Tsuruta, S., Tazawa, S.,
Asari, K., Kono, Y., Yano, T., Gouda, N., Iwata, T.,
Yokoyama, T., Kanamori, H., Funazaki, K., Miyazaki,
T.: 2003, Application of PZT telescope to In-situ Lunar
Orientation Measurement(ILOM), the XXIII General
Assembly of the Int. Union of Geodesy and Geophysics,
IUGG2003, (Sapporo, June 30 - July 11).
Hanaoka, Y.: 2003, Ha Impact Polarization Observed in a
Gradual Flare, 5th Solar-B Science Meeting, (Tokyo,
Nov. 12−14).
Hayakawa, T., Iwamoto, N., Shizuma, T., Kajino, T.:
2003, Universal scaling of p- and s-process nuclides,
Universal scaling of p- and s-process nuclides, The 8thInt. Conf. on Clustering Aspects of Nuclear Structure andDynamics, (Nara, Nov. 24−29).
Hayakawa, T., Shimizu, T., Arima, T., Kajino, T., Chiba,S., Shinohara, N., and Utsunomiya, H.: 2003, 186Re isomer contribution to 187Re−187Os Cosmochronometer,
Proc. Int. Symp. on Origin of Matter and Evolution of
Galaxies, (Saitama, Nov. 17−19).
Hayakawa, T., Shizuma, T., Arima, T., Kajino, T., Chiba,S., Shinohara, S., Utsunomiya, H.: 2003, s-Process contamination to 187Re−187Os nuclear cosmochronometer of rprocess, The 8th Int. Conf. on Clustering Aspects of
Nuclear Structure and Dynamics, (Nara, Nov. 24−29).
Heki, K.: 2003, Dense GPS array: A new versatile sensor of
the Earth, IUGG2003, Union Symp. U6, (Sapporo, June
30 - July 11).
Heki, K.: 2003, Seasonal crustal deformation: final synthesis, IUGG2003, Symp. JSG01, (Sapporo, June 30 - July
11).
Heki, K.: 2003, Seasonal crustal deformation in Japan andits interannual variation, AGU Fall Meeting, (SanFrancisco, Dec. 8−12).
Heki, K.: 2003, Secular subsidence and deep basal subduction erosion at the northeastern Japan forearc, AGU Fall
Meeting, (San Francisco, Dec. 8−12).
Heki, K.: 2004, Enigma of forearc subsidence in NE Japan:
deep basal subduction erosion or deep coupling?, Int.
Symp. on Slow Slip Events at Plate Subduction Zones,(Nagoya, Mar. 16−18).
Heki, K.: 2004, Monitoring crustal deformation in an island
arc: IGS contribution to crustal deformation studies, IGS
10th anniversary symp., (Bern, Switzerland, Mar. 4).
Honda, S., Aoki, W., Kajino, T., Ando, H., Beers, T. C.:
2003, Spectroscopic Studies of Extremely Metal-PoorStars with Subaru/HDS, The First Stars II, (USA, May
29−31).
Honda, S., Aoki, W., Kajino, T., Ando, H., Beers, T. C.:
2003, Spectroscopic Studies of r-Process Elements in
Very Metal-Poor Stars with Subaru/HDS, Origin of
Matter and Evolution of Galaxies 2003, (Japan, Nov.
17−19).
Honda, S., Aoki, W., Kajino, T., Ando, H., Beers, T. C.:

2003, Subaru/HDS Studies of r-Process Elements in
Metal-Poor Stars, IAU General Assembly, (Australia,
July 13−26).
Ibukiyama, A.: 2003, A Chemodynamical Galaxy
Formation Model with UV and Dust Physics, East AsianYoung Astronomers Meeting 2003, (Tienrai, Taiwan,
Nov. 9−12).
Ibukiyama, A.: 2003, Hipparcos Age-Metallicity Relationof the Solar Neighbourhood Disc Stars, Galactic
Chemodynamics V , (Swinburne Univ., Australia, July8−12).
Ichiki, K., Garnavich, P. M., Kajino, T., Mathews, G. J.,
and Yahiro, M.: 2003, Observational Evidence for
Disappearing Dark Matter in Brane World Cosmology,
RESCEU, (Tokyo, Nov. 4−7).
Ichiki, K., Garnavich, P. M., Kajino, T., Mathews, G. J.,
and Yahiro, M.: 2003, Decaying Cold Dark Matter andCosmological Microwave Background Anisotropies,
Origin of Matter and Evolution of Galaxies, (Saitama,
Nov. 17−19).
Imanishi, M.: 2003, Buried AGNs in LINER Ultraluminous
Infrared Galaxies, The Neutral ISM in Starburst
Galaxies, (Sweden, June 24−27).
Imanishi, M.: 2003, Compact Nuclear Starbursts in the CfA
and 12 Micron Seyfert 2 Galaxies, The Neutral ISM in
Starburst Galaxies, (Sweden, June 24−27).
Inoue, K. T.: 2003, Direct Mapping of Massive Compact
Objects in Extragalactic Dark Halos, PhysicalCosmology, (Blois, France, June 15−20).
Inoue, K. T., Chiba, M.: 2003, Detecting Dark Matter in
Compact Objects with VSOP-2 in Dark Matter in
Galaxies, IAU Symp. 220, (Sydney, Australia, July 22−
25).
Ishii, M., Tamura, M., Nagata, T., Sato, S., Yao, Y., Jiang,Z., and Yanagisawa, K.: 2003, K band spectroscopy of
Herbig Ae/Be stars, American Astronomical Society
Meeting 202.
Ito, T., and Malhotra, R.: 2003, Near-Earth orbital distribution of asteroid fragments coming from the ν6 resonance zone, 35th Annual Meeting of the Division ofPlanetary Sciences, the American Astronomical Society,(Monterey, California, USA, Sep. 1−6).
Ito, T., and Malhotra, R.: 2003, Near-Earth orbital distribution of asteroid fragments coming from the ν6 resonance zone, 6th Lunar & Planetary Laboratory Conf.,(Tucson, Arizona, USA, Sep. 18−19).
Ito, T., Yoshida, F., Malhotra, R., Takahashi, S.,
Nakamura, T., Dermawan, B., Ibrahimov, M. A.: 2004,
Lightcurves of the Karin family asteroids, 6th Lunar &Planetary Laboratory Conf., (Tucson, Arizona, USA,
Sep. 18−19).
Iwata, T., Sasaki, T., Izumi, T., Kono, Y., Hanada, H.,
Kawano, N., and Kikuchi, F.: 2003, Results of the criticaldesign of RSAT/VRAD mission instruments on
SELENE sub-satellites Rstar/Vstar for selenodesy,IUGG2003, (Sapporo, June 30 - July 11).
Kajino, T., Ichiki, K., Garnavich, P. M., Mathews, G. J.,
and Yahiro, M.: 2003, Dark Matter Dark Energy, andDark Radiation in the Universe and Cosmological

Nucleosynthesis, Proc. 1st Yamada Symp. on Neutrino
and Dark Matter, (Nara, Japan, June 9−14).
Kajino, T., Sasaqui, T., Orito, M., Otsuki, K., Mathews, G.
J., Honda, S., Aoki, W., and Chiba, S.: 2004,
Nucleosynthesis in Supernovae and the Early Universe,
5th Tours Int. Conf. on Nuclear Physics, (Tours, France,
Aug. 26−29).
Kajino, T.: 2003, Cosmological Nucleosynthesis in the BigBang and Supernovae, Invited lecture, (Seoul, Korea,
June 5−6).
Kajino, T.: 2003, Disappearing dark matter in the branecosmology, Invited Lecture, (Korea, June 5−6).
Kajino, T.: 2003, Quest for the Origin of Dark Matter, Dark
Energy, and Dark Radiation; QCD-Driven Cosmological
Nucleosynthesis and Supernova Nucleosynthesis, CERN
Advanced Studies Institute Symp. on Symmetries andSpin, (Prague, Czech Republic, July 12−19).
Kameya, O., Kobayashi, H., Kawaguchi, N., Sasao, T.,
Honma, M., Hirota, T., Omodaka, T., Miyaji, T., Suda,
H., and the VERA team: 2003, Study on Star Forming
Regions by using the VERA, IAU Symp. 221, (Australia,
July 22−25).
Kamimura, M., Matsumoto, T., Hiyama, E., Ogata, K.,
Iseri, Y., and Yahiro, M.: 2003, Four-Body CDCC calculation of elastic scattering of 6 He from 12 C, Direct
Reactions with Exotic Beams, (Surrey, July 10−12).
Kashikawa, N.: 2003, The Current Status of the Subaru
Deep Field Project, The Formation and Early Evolutionof Galaxies, (Irsee, June 30- Sep. 4).
Katsukawa, Y., and Tsuneta, S.: 2004, What Determines
the Coronal Heating Rate in the Photosphere? , Int.
Workshop "Explosive Phenomena in Magnetized
Plasmas - New Development in Reconnection Research",(Kyoto, Mar. 17−19).
Kawabata, K. S., Ikeda, Y., Akitaya, H., Matsuda, K., Seki,
M., Matsumura, M.: 2003, Another Implication for Dust
Formation Close to The Photosphere in R Coronae
Borealis, Astrophysics of Dust, (Colorado, May 26−30).
Kawabata, K., Tanikawa, K., Sôma, M.: 2003, Time variation of the moment of inertia of the Earth derived from
Chinese and Japanese records of ancient solar eclipses,
Meeting of IAU Comm. 41, (Sydney, Australia, July 21).
Kawakita, H., Watanabe, J., Furusho, R., Fuse, T.: 2003,
Ortho-To Ratios of Cometary Water and Ammonia,
Formation of Cometary Material, 25th meeting of the
IAU, Joint Discussion 14, (Sydney, Australia, July 22).
Kawakita, H., Watanabe, J., Furusho, R., Fuse, T.: 2003,
Relationship Between Spin Temperatures and ChemicalCompositions in Comets, American Astronomical
Society, DPS meeting, 35, #38.06.
Kawakita, H., Watanabe, J., Kinoshita, D., Ishiguro, M.,
Nakamura, R.: 2003, Saturated Hydrocarbons in Comet
Ikeya-Zhang, Formation of Cometary Material, 25th
meeting of the IAU, Joint Discussion 14, (Sydney,
Australia, July 22).
Kawano, N., Hanada, H., Namiki, N., and RISE project
team: 2003, Research In SElenodesy (RISE) by
SELENE, IAU, (Australia, July 13−26).
Kingsley, J. S., Stanghellini, S., and Ukita, N.: 2003,

69

ALMA Prototype Antennas, 2003 IEEE Int. Symp. on
Antennas and Propagation; URSI North American Radio
Science Meeting Columbus, (Ohio, USA, June 23−27).
Kinoshita, D., Watanabe, J., Yamamoto, N., Fuse, T.,
Miyasaka, S., Muroi, K.: 2003, Deep TNO Search Near
Invariable Plane Using SUBARU Telescope, Tsai, AnLi, Physical Properties and Morphology of Small Solar
System Bodies, 25th meeting of the IAU, Joint
Discussion 19, (Sydney, Australia, July 23).
Kodama, T., Bower, R. G., Best, P. N., & Hall, P.: 2003,
The KS-band Luminosity and Stellar Mass Functions ofGalaxies in z~1 and z~1.5 Clusters, Int. conf. Stellar
Populations 2003, (Garching, Germany, Oct 6−10).
Kodama, T.: 2003, Panoramic Imaging Survey of Cluster
Evolution with Subaru (PISCES) Int. workshop on
Multiwavelength Mapping of Galaxy Formation and
Evolution, (Venice, Italy, Oct 16).
Kodama, T.: 2004, The Mass Asssembly History of
Galaxies and Clusters of Galaxies, Int. conf. On Outskirts
of Galaxy Clusters: Intense Life in the Suburbs, (Torino,
Italy, Mar. 15).
Kokubo, E.: 2004, Oligarchic Growth of Protoplanets andDiversity of Planetary Systems, Planet Formation:
Terrestrial and Extra Solar, (Santa Barbara, Mar. 15−19).
Kono, Y., Hanada, H., Ping, J., Koyama, Y., Fukuzaki, Y.,
Kawano, N.: 2003, Precise positioning of spacecrafts bymulti-frequency VLBI, IUGG2003, (Sapporo, June 30 July 11).
Koyama, H., and Yano, T.: 2003, The relation between the
two-point and the three-point correlation functions in the
non-linear gravitational clustering regime, The 6th
RESCEU Int. Symp., (Tokyo, Nov. 4−7).
Machida, M. N., Tomisaka, K., and Matsumoto, T.: 2003,
Fragmentation of molecular cloud and binary star formation, IAU General Assembly, (Australia, July 13−26).
Machida, M., Nakamura, K. N., Matsumoto, R.: 2003,
Time Variabilities of Optically Thin Black Hole
Accretion Disks Reproduced by 3D MHD Simulations,
Stellar-Mass, Intermediate-Mass, and SupermassiceBlack Holes, (Kyoto, Oct. 28−31).
Manabe, S., Tamura, Y., Jike, T., Horiai, K., VERA Team:
2004, Status and Plan of Geodetic and AstrometricObservations with VERA, 3rd IVS General Meeting,(Ottawa, Feb. 9−11).
Matsumoto, T., Hiyama, E., Yahiro, M., Ogata, K, Iseri ,Y., and Kamimura, M.: 2003, Four-body CDCC analysisof 6He+12C Scattering, Clustering Aspects of Nuclear
Structure and Dynamics, (Nara, Nov. 24−29).
Matsumoto, T.: 2003, Fragmentation of a Molecular CloudCore versus Fragmentation of the Massive
Protoplanetary Disk in the Main Accretion Phase,
Magnetic fields and star formation: theory versus observations, (Madrid, Spain, Apr 21−25).
Matsumoto, T.: 2003, Self-gravitational Collapse of aMagnetized Cloud Core: High Resolution Simulations
with Three-dimensional MHD Nested Grid, The 18th Int.
Conf. on Numerical Simulation of Plasmas, (Cape Cod,
Massachusetts, USA, Sep. 7−10).
Matsuo, H., Ariyoshi, S., Otani, C., Shimizu, H. M.: 2003,

70

Development of Superconducting Direct Detectors using
Nb Junctions, New Perspectives for Post-Herschel FarInfrared Astronomy from Space Madrid, (Sept. 1−4).
Matumoto, K., Heki, K., Hanada, H., Tsuruta, S., Kono, Y.,
Kawano, N., Iwata, T., Namiki, N., and Rowlands, D. D.:
2003, Anticipated accuracy of lunar gravity field modelfrom RSAT/VRAD mission, IUGG2003, (Sapporo, June
30 - July 11).
Miyauchi-Isobe, N., Nakajima, K.: 2003, Astronomical Data
Analysis Software and Systems XIII, Int. Conf.,(Strasbourg, Oct. 12−15).
Nakai, N., Yamauchi, A., Sato, N., and Ishihara, Y.: 2003,
Two Types of H 2O Maser Disks in Active Galactic
Nuclei, Future Directions in High Resolution Astronomy:
A Celebration of the 10th Anniversary of the VLBA,(Socorro, New Mexico, USA, June 10).
Nakamura, K.: 2003, Treatments of oscillatory behaviors ofa gravitating Nambu-Goto string, Int. workshop: 6th
Capra meeting on radiationa reaction problem in General
Relativity, (Kyoto, June 23-July 2).
Nakanishi, K., Okumura, S. K., Kohno, K., Kawabe, R., andNakagawa, T.: 2003, Dense and Warm Molecular Gas in
Luminous IR Galaxy NGC 6240, The Neutral ISM in
Starburst Galaxies, Marstrand, (Sweden, June 23−27).
Nakao, K., Nakamura, K., and Mishima, T.: 2004, The
Hoop Conjecture and Cylindrically Symmetric Initialvalue Data in the Brane-World, 4th Australasian conf. on
General Relativity and Gravitation, (Melbourne,
Australia, Jan. 7−9).
Nishikori, H., Machida, M., Matsumoto, R.: 2003,
Magnetic Activity Following Re-Accretion onto
Galaxies, Recycling Intergalactic and Interstellar Matter,
IAU Symp. 217, (Sydney, Jul. 14−17).
Noda, H., Asari, K., Kono, Y., Iwata, T., Namiki, N.,
Hanada, H., Kawano, N., and Yamamoto, Z.: 2003,
Ground-base verification of four-way Doppler measurement for the SELENE mission, IUGG2003, (Sapporo,
June 30 - July 11).
Numata, K.: 2003, Direct Measurement of Mirror Thermal
Noise, The Edoardo Amaldi 5th Conf., (Pisa, Itary, July.
11).
Ogata, K., Yahiro, M., Iseri, Y., Matsumoto, T., Yamashita,N., and Kamimura, M.: 2003, Determination of S 17
based on CDCC analysis of 8B Dissociation Origin of
Matter and Evolution of Galaxies, (Saitama, Nov. 17−19).
Ogata, K., Yahiro, M., Iseri, Y., Matsumoto, T., Yamashita,N., and Kamimura, M.: 2003, Determination of S17 from8
B Dissociation, Clustering Aspects of Nuclear Structure
and Dynamics, (Nara, Nov. 24−29).
Ogata, K., Yahiro, M., Iseri, Y., Matsumoto, T., Yamashita,N., and Kamimura, M.: 2003, Determination of S17 fromsystematic analyses on 8B Coulomb breakup with the
Eikonal-CDCC method, Nuclear reaction mechanism,(Varenna, June 9−13).
Ogata, K., Yahiro, M., Iseri, Y., Matsumoto, T., Yamashita,N., and Kamimura, M.: 2003, Determination of S17 from
Systematic Analyses on 8B Coulomb Breakup with the
Eikonal-CDCC Method, Nuclear Theory, (Bulgaria, June
16−22).

Ogata, K., Yahiro, M., Iseri, Y., Matsumoto, T., Yamashita,N., and Kamimura, M.: 2003, Hybrid calculation of 8B
Coulomb dissociation with standard- and eikonal-CDCC
methods, Direct Reactions with Exotic Beams, (Surrey,
July 10−12).
Ohishi, M., Mizumoto, Y., Yasuda, N., Shirasaki, Y.,
Tanaka, M., and Masunaga, Y.: 2003, Japanese Virtual
Observatory Project, 25th meeting of the IAU, Joint
Discussion 8, (Sydney, Australia, July 17−19).
Ohishi, M., Mizumoto, Y., Yasuda, N., Shirasaki, Y.,
Tanaka, M., Honda, S., Masunaga, Y., Miura, K.,
Monzen, H., Kawarai, K., Ishihara, Y., Yamaguchi, Y.,
and Yanaka, H.: 2003, A Prototype toward Japanese
Virtual Observatory (JVO), Astronomical Data Analysis
Software and Systems XIII, (Strasbourg, France, Oct.
12−15).
Ohishi, M.: 2003, Current Status of Japanese Virtual
Observatory, IVOA Small Projects Meeting 2003,(Beijing, Nov. 27).
Ohishi, M.: 2004, A Prototype toward Japanese Virtual
Observatory (JVO), SAINT2004, (Tokyo, Jan. 27).
Ohishi, M.: 2004, Japanese Virtual Observatory Project,
Japan-France Grid Computing Workshop in Paris, (Paris,
Mar. 8).
Ohta, I. S., Hattori, M., Matsuo, H.: 2003, Development ofSuper Broadband Intererometer in FIR, New
Perspectives for Post-Herschel Far-Infrared Astronomy
from Space Madrid, (Sept. 1−4).
Okamura, N., Watanabe, J.: 2003, Reproduction of Cassini
Telescope, Effective Teaching and Learning of
Astronomy, 25th meeting of the IAU, Special Session 4,(Sydney, Australia, July 24−25).
Omukai, K.: 2003, Formation of the First Stars by
Accretion, (State College, May. 29−31).
Otsuki, K., Mathews, G. J., and Ashenfelter, T.: 2003,
Constraints in globular cluster formation and evolution
from Magnesium isotope ratios and r-process elemental
abundances, Origin of Matter and Evolution of galaxies
2003, (Saitama, Nov. 17−19).
Ping, J., and Matsumoto, K.: 2003, To improve a regional
ionospheric TEC model over Japan Islands, IUGG2003,(Sapporo, June 30-July 11).
Saigo, K., Tomisaka, K., and Matsumoto, T.: 2003,
Collapse of Rotating Gas Cloud: Formation and
Evolution of Hydrostatic Object, Japan-Italy Seminar,(Niigata, Japan, Dec. 1−5).
Saigo, K., Tomisaka, K., Matsumoto, T.: 2003, Collapseof First Core and The possibility of Binary Formation,
CFD-MHD Workshop in Astrophysics: Numerical
Methods and Astrophysical Turbulence, (Taipei, Dec.
10−12).
Saito, M. M., and Tanikawa, K.: 2003, Survey of one
dimensional three-body problem through the symbol
sequence, Order and Chaos in Stellar and Planetary
Systems, (St. Petersberg, Aug. 17−24).
Saito, Y., Iye, M., Ohyama, Y., Kashikawa, N., Yoshida, M.,
Sasaki, T., Takata, T., Kosugi, G., Aoki, K., andKawabata, K. S.: 2003, Subaru/focas Globular Clusters
Survey around M82, in Extragalactic Globular Clusters

and their Host Galaxies, 25th meeting of the IAU, Joint
Discussion 6, (Sydney, Australia, July 17).
Sasaki, T., Sasaki, S., Watanabe, J., Kawakita, H., Fuse, T.,
Takato, N., Sekiguchi, T.: 2004, SUBARU Spectroscopyof Asteroid (832)Karin; Determining Time, Scale ofSpace Weathering, 35th Lunar and Planetary Science
Conf., (League City, Texas, USA, March 15−19).
Sasaqui, T., Kajino, T., Otsuki, K., Mathews, G. J., andNakamura, T.: 2004, Supernova Nucleosynthesis andRadioactive Nuclei, Proc. 5th Japan-China Joint Nuclear
Physics Symp., (Fukuoka, Mar. 7).
Sasaqui, T., Otsuki, K., Kajino, T., Mathews, G. J., andNakamura, T.: 2004, Theoretical study of supernova rprocess: Dependence on the light neutron-rich nuclear
reactions, Proc. Int. Symp. on Origin of Matter and
Evolution of Galaxies 2003, (Saitama, Nov. 11−19).
Sato, S., for the TAMA Collaboration: 2003, Current Status
of TAMA300, The 28th Int. Cosmic Ray Conf.,(Tsukuba, July 31 - Aug. 7).
Sato, S.: 2004, Status of TAMA and Data Taking Run,
Aspen 2004, (Aspen, Feb. 4).
Sato, T., Fujimoto, H., Matsumoto, K., Tamura, Y.,
Higashi, T., Nishino, M., Hino, R., and Kanazawa, T.:
2003, Ocean Bottom Pressure Measurements Off
Sanriku,Japan, AGU Fall Meeting, (San Francisco, Dec.
8−12).
Sato, T., Hinderer, J., van Dam, T., Francis, O., Falk, R.,
Plag, H.-P., Kierulf, H., MacMilian, D., and Fukuda, Y.:
2003, Observed displacement and gravity changes at NyAlesund, svalbard and the effects of sea level changes
and the present-day ice melting, EGS/AGU/EUG Joint
Assembly, (Nice, France, Apr. 6).
Sato, T., Tamura, Y., Matsumoto, K., Plag, H.-P., andFrancis, O.: 2003, Seasonal gravity variation at NyAlesund, Svalbard observed from a super conducting
gravimeter, EGS/AGU/EUG Joint Assembly, (Nice,
France, Apr. 7).
Sekii, T.: 2003, Anticorrelated p modes?, The Second Far
Eastern Workshop on Helio- and Asteroseismology,(Tokyo, Oct. 18−19).
Sekii, T.: 2003, Seismology of Solar Internal Rotation, IAU
XXV General Assembly/Joint Discussion 12: Solar andSolar-like Oscillations: Insights and Challenges for the
Sun and Stars, (Sydney, Australia, July 18−19).
Sekii, T.: 2003, Time-distance analysis of high-frequency
acoustic waves, The Second Far Eastern Workshop on
Helio- and Asteroseismology, (Tokyo, Oct. 18−19).
Shibasaki, K.: 2003, A New Solar Flare Scenario: Highbeta Plasma Disruption, IUGG2003, (Sapporo, June 30July 11).
Shibasaki, K.: 2003, A Pumping-Up Mechanism of Massand Energy from the Photoshere into the Upper
Atmosphere, 5th Solar-B Science Meeting, (Tokyo, Nov.
12−14).
Shimojo, M.: 2003, Derivation of DEM Distribution Using
YOHKOH/Soft X-ray Telescope, 5th Solar-B Science
Meeting, (Tokyo, Nov. 12−14).
Shirasaki, Y., Matsuzaki, E., Mizumoto, Y., Kakimoto, F.,
Ogio, S., Yasuda, N., Tanaka, M., Yahagi, H.,

71

Nagashima, M., Kosugi, G.: 2003, Searching for a Long
Cosmic String Through the Gravitational Lensing Effect,
The 28th Int. Cosmic Ray Conf., (Japan, July 31 - Aug.
7).
Shirasaki, Y., Mizumoto, Y., Matsuzaki, E., Oishi, M.,
Yasuda, N., Tanaka, M., Honda, S., Yahagi, H.,
Nagashima, M., Kosugi, G., Kashikawa, N., Kakimoto,F., Ogio, S.: 2003, Searching for a cosmic string throughthe graviational lens effect: Japanese Virtual Observatory
science use case, Astronomical Data Analysis Softwareand Systems XIII, (Strasbourg, France, Oct. 12−15).
Shirasaki, Y.: 2003, Current status of Japanese Virtual
Observatory, Australian Virtual Observatory Workshop
2003, (Sydney, Australia, Nov. 17−18).
Sôma, M., Tanikawa, K., and Kawabata, K.: 2003, Tidal
term of the lunar longitude in the past 2,700 years
derived from Chinese and Japanese records of ancientsolar eclipses, IAU G.A. Comm. 41, (Sydney, Australia,
July 21).
Sôma, M., Tanikawa, K., Kawabata, K.: 2003, Earth's Rateof Rotation Between 700 BC and 1000 AD Derived from
Ancient Solar Eclipses, JOURNÉES 2003, Astrometry,
Geodynamics and Solar System Dynamics: from
Milliarcseconds to Microarcseconds, (St. Pertersburg,
Russia, Sept. 22−25).
Sôma, M., Hayamizu, T., Setoguchi, T., Hirose, T.: 2003,
Precise Position of Saturn Obtained from a Stellar
Occultation by Tethys, JOURNÉES 2003, Astrometry,
Geodynamics and Solar System Dynamics: from
Milliseconds to Microarcseconds, (St. Petersburg, Sept.
22−25).
Somiya, K., Beyersdorf, P., and Kawamura, S.: 2003, RSE
Experiment,Int. Cosmic Ray Conf., (Tsukuba, July 31Aug. 7).
Somiya, K., Miyakawa, O., and Kawamura, S.: 2003, Japan
4m RSE Experiment, LIGO Science Collaboration
August 2003 Meeting, (Hannover, Germany, Aug. 18−
21).
Sugano, T., and Heki, K.: 2004, Lunar Interior Studies
Using Lunar Prospector Line of Sight Acceleration Data,
Lunar and Planetary Science Conf., (Houston, Mar. 15−
19).
Sugiyama, N.: 2003, WMAP and Cosmic Microwave
Background Radiation, 13th workshop on General
Relativity and Gravity in Japan, (Osaka, Dec. 1−4).
Sugiyama, N.: 2003, Cosmic Microwave Background: What
did we learn from WMAP?, The Summer Institute 2003,(Fuji-Yoshida, Aug. 12−19).
Suzuki, B., Watanabe, J.: 2003, Astro-Classroom for HighSchool Students of the World, Astro-HS Committee,
Effective Teaching and Learning of Astronomy, 25th
meeting of the IAU, Special Session 4, (Sydney,
Australia, July 24−25).
Tajitsu, A., and Otsuka, M.: 2003, The Multiple Outflows
in the Galactic Halo PN H 4-1, Asymmetric Planetary
Nebula III (""APN3"") Wind, Structure & theThunderbird, (Mt. Rainier, USA, July 28 - Aug. 1).
Takahashi, R., and the TAMA collaboration: 2003, Status
of TAMA300, 5th Edoardo Amaldi Conf. on

72

Gravitational Waves, (Pisa, July 6−11).
Takahashi, R., Arai, K., Kawamura, S., and Smith, M.:
2003, Direct Measurement of Scattered Light Effect on
the sensitivity in TAMA300, 28th Int. Cosmic Ray
Conf., (Tsukuba, July 31-Aug. 7).
Takahashi, R., Saito, Y., Kubo, T., Tomaru, T., Tokunari,M., Sumiya, T., Takasugi, K., and Naito, Y.: 2003,
Application of Diamond-Like Carbon (DLC) coatings forgravitational wave detector, 8th European Vacuum
Conf., (Berlin, June 23−26).
Takano, S.: 2003, Systematically Peculiar MolecularComposition in M82, IAU XXV General Assembly Joint
Discussion 21: The Astrochemistry of External Galaxies
Wednesday, (Sydney, July 23).
Takemoto, S., Araya, A., Akamatsu, J., Morii, W., Ohashi,
M., Higashi, T., Fukuda Y., Momose, H., Kawasaki, I.,
Naito, I., and Hanada, H.: 2003, 100m Laser strainmeters
installed in a deep tunnel at Kamioka, Gifu, Japan,
IUGG2003, (Sapporo, June 30 - July 11).
Tamura, M. et al.: 2003, Luminosity Functions of YSO
Clusters in SFRs: NIR and MIR Surveys, The Formationand Evolution of Massive Young Clusters, (Cancun,
Nov. 17−21).
Tamura, M., Fukagawa, M., Hayashi, M., Itoh, Y., SDPS
team: 2003, Subaru AO Coronagraphic and Direct
Imaging of YSOs, IAU Symp. 221, Star Formation atHigh Angular Resolution, (Sydney, July 22−25).
Tamura, M., Fukagawa, M.: 2004, Circumstellar Disks in
PMS and T Tauri Stars, Astronomical Polarimetry,(Kona, March 15−19).
Tamura, Y., Sato, T., Fukuda, Y., and Higashi, T.: 2003,
Collocated Observations with a Superconducting
Gravimeter and an Absolute Gravimeter FG5 at Esashi
Station, AGU Fall Meeting, (San Francisco, USA, Dec.
8−12).
Tatsumi D., Tsunesada Y., and the TAMA Collaboration:
2003, Current Status of TAMA300 Online Search for
Inspiraling Binaries, The 28th Int. Cosmic Ray Conf.,(Tsukuba, July 31 - Aug. 7).
Tatsumi, D., and the TAMA collaboration: 2003, Online
Calibration and Preprocesses in TAMA300, 5th Edoardo
Amaldi Conf. on Gravitational Waves, (Pisa, July 6−11).
Tatsumi, D., and the TAMA collaboration: 2003, Online
Veto Analysis of TAMA300, 8th Annual Gravitational
Wave Data Analysis Workshop, (Milwaukee, WI, US,
Dec. 17−20).
Terasawa, T., Langanke, K.-H., Kajino, T., and Mathews,
G. J.: 2004, Neutrino effects before, during and after thefreezeout of the r-process, Proc. Int. Symp. on Origin of
Matter and Evolution of Galaxies 2003, (Saitama, Nov.
11−19).
Tsujimoto, T., and Shigeyama, T.: 2003, Mass Stripping in
Dwarf Spheroidal Galaxies and Omega Cen, Recycling
Intergalactic and Interstellar Matter, IAU Symp. 217,
(Sydney, Australia, July 14−17).
Tsujimoto, T., and Shigeyama, T.: 2003, Observed
Abundance Features and their Implication for Chemical
Evolution, Galactic Chemodynamics V, (Melbourne,
Australia, July 9−11).

Tsujimoto, T., and Shigeyama, T.: 2003, The origin of lowa stars, Stellar Populations, (Garching, Germany, Oct.
6−10).
Tsunesada, Y., and the TAMA collaboration: 2003, Current
Status of TAMA300 Online Search for Inspiraling
Binaries, 28th Int. Cosmic Ray Conf., (Tsukuba, July 31- Aug. 7).
Tsunesada, Y., and the TAMA collaboration: 2003, Searchfor black hole ringdown gravitational waves in
TAMA300 data, 8th Annual Gravitational Wave Data
Analysis Workshop, (Milwaukee, WI, US, Dec. 17−20).
Tsunesada, Y., and the TAMA collaboration: 2003, Search
for Gravitational Waves from Black Hole Ringdowns,
5th Edoardo Amaldi Conf. on Gravitational Waves,(Italy, July 6−11).
Tsunesada, Y., and the TAMA collaboration: 2003, Search
for Gravitational Waves from Ringing-down Black
Holes, The 28th Int. Cosmic Ray Conf., (Tsukuba, July
31-Aug. 7).
Tsuneta, S.: 2004, Gene Parker and Revolutionary
Development in Solar Physics, 第19回京都賞記念ワークシ
ョップ, 宇宙電磁流体力学と太陽活動, (Kyoto, Nov. 12).
Tsuneta, S.: 2004, Solar-B Mission, International
Workshop "Explosive Phenomena in Magnetized
Plasmas - New Development in Reconnection Research",(Kyoto, Mar. 17−19).
Umemura, M.: 2003, A Coevolution Scheme forSupermassive Black Holes and Galactic Bulges, StellarMass, Intermediate-Mass, and Supermassive Black
Holes, (Kyoto, Oct. 28−31).
Umemura, M.: 2003, Indicators for GRBs at z>10, New
Horizon of Gamma-Ray Burst Astronomy, (Tokyo, Dec.
8−10).
Wada, K.: 2003, Gas dynamics in the galactic central 100
pc region, Neutral gas in starburst galaxies, (Mastrand,
Sweden, June 26).
Wada, K.: 2003, Gravity-driven and spiral-shock driven
turbulence in galactic disks, CFD-MHD workshop,(Taipei, Taiwan, Dec. 10−11).
Wada, K.: 2004, Dynamics and Structure of the ISM
around the AGN and a Nuclear Starburst, IAU Symp.
222: The interplay among Black Holes, Stars and ISM in
Galactic Nuclei, (Gramado, Brasil, Mar. 1−5).
Watanabe, J., Honda, M., Yamashita, T., Kataza, H.,
Miyata, T., Okamoto, Y., Sako, S., Fujiyoshi, T., Onaka,T., Kinoshita, D.: 2003, 10 Micron Feature of Comets
Observed by Subaru Telescope, Formation of Cometary
Material, 25th meeting of the IAU, Joint Discussion 14,(Sydney, Australia, July 22).
Watanabe, J., Ono, T.: 2003, Star Week - a Successful
Campaign in Japan, Star Week Committee, Effective
Teaching and Learning of Astronomy, 25th meeting of
the IAU, Special Session 4, (Sydney, Australia, July
24−25).
Watanabe, J.: 2003, Jaasc Cooperation League for
Education and Public Outreach, JAASC Committee,
Effective Teaching and Learning of Astronomy, 25th
meeting of the IAU, Special Session 4, (Sydney,
Australia, July 24−25).

Watanabe, T.: 2003, Electron Densities of HighTemperature Coronal Loops, 5th Solar-B Science
Meeting, (Tokyo, Nov. 12−14).
Yamauchi, A., Nakai, N., Sato, N., and Diamond, P.: 2003,
Water-Vapor Maser Emission from the Seyfert 2/LINER
NGC 3079, Future Directions in High Resolution
Astronomy: A Celebration of the 10th Anniversary of the
VLBA, (Socorro, New Mexico, USA, June 9−12).
Yanagisawa, K., Kawai, N., Ohta, K., Watanabe, J.,
Yoshida, A., Shimizu, Y., Nagayama, S., Inata, M.,
Hattori, T., Okita, K., Watanabe, E., and Yoshida, M.:
2003, Development of the Optical-Infrared Wide Field
Imaging System at Okaya Astrophysical Observatory,
RIKEN-Symp., (Wako, Dec. 8−9).
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Yamada,Y., Kan-Ya, Y., Araki, H., Tazawa, S., Asari, K., Tsuruta,
S., Hanada, H., Kawano, N.: 2003, Japanese Astrometry
Satellite Mission - Jasmine Project, The International
Celestial Reference System: Maintenance and Future
Realization, 25th meeting of the IAU, Joint Discussion16, (Sydney, Australia, July 22).
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Yamada,Y., Kan-Ya, Y., Araki, K., Tazawa, S., Asari, K., Tsuruta,
S.: 2003, Japanese Astrometry Satellite Mission Jasmine Project ,The Int. Celestial Reference System:
Maintenance and Future Realization, 25th meeting of the
IAU, Joint Discussion, (Sydney, Australia, July 16−22).
Yano, T., Koyama, H., Buchert, T., and Gouda, N.: 2003,
Distribution of caustics in the expanding Universe, The
6th RESCEU Int. Symp., (Tokyo, Nov. 4−7).
Yasuda, N., Mizumoto, Y., Ohishi, M., O'Mullane, W.,
Budavari, T., Haridas, V., Li, N., Malik, T., Szalay, A.,
Hill, M., Linde, T., Mann, B., and Page, C.: 2003,
Astronomical Data Query Language :Simple Query
Protocol for the Virtual Observaroty, Astronomical Data
Analysis Software and Systems XIII, (Strasbourg,
France, Oct. 12−15).
Yoshida, F., Ito, T., Dermawan, B., Malhotra, R.,
Nakamura, T., Takahashi, S., Ibrahimov, M. A., Sawabe,S., Haji, M., Saito, R., Hirai, M., Miyasaka, S., Sato, Y.,
Fukushima, H., Sato, H., Ip, W. H., Chen, W. P., andYanagisawa, T.: 2003, Lightcurves of the Karin family
asteroids, Asteroids Dynamics Workshop, (USA, Feb.
2−4).
Yoshida, F., Ito, T., Malhotra, R., Dermawan, B.,
Nakamura, T., Takahashi, S., Ibrahimov, M. A., Sawabe,S., Haji, M., Saito, R., Hirai, M., Miyasaka, S., Sato, Y.,
Fukushima, H., Sato, H., Ip, W. H., Chen, W. P., andYanagisawa, T.: 2003, Lightcurves of the Karin family
asteroids, The 6th Lunar and Planetary Laboratory Conf.,(USA, Sep. 18−19).
Yoshida, F., Nakamura, T.: 2003, Size and Spatial
Distributions of Sub-km Main-Belt Asteroids,
CAST2003, (Taiwan, Apr.18−19).
Yoshida, F., Nakamura, T.: 2003, Size Distributions ofFaint Jovian L4-Trojan Asteroids, the 35th Annual
Meeting of the Division for Planetary Sciences of theAmerican Astronomical Society, (USA, Sep. 1−6).
Yoshida, M., Yagi, M., Okamura, M., Ohyama, Y.,73

Miyazaki, S., Yasuda, N., Aoki, K., and Iye, M.: 2003,
Deep Spectroscopy of Very Extended Ionized Gas of
NGC 4388, in Recycling Intergalactic and Interstellar
Matter, IAU Symp. 217, (Sydney, Australia, July 14−17).
Yoshida, N.: 2003, Early structure formation and reionization of the universe, The First Stars II, (State College,
USA, May. 23−26).
Yoshida, N.: 2003, Reionization by Population III stars,
First generation stars and galaxies, (Niigata, Dec. 9−11).
Yoshida, N.: 2003, Structure formation in the early universe, Frontier in Astroparticle Physics and Cosmology,(Tokyo, Nov. 4−7).
Yoshida, T., and Hashimoto, M.: 2003, Supernova Mixing
Models for Isotopic Ratios of Presolar Grains, Origin of
Matter and Evolution of the Galaxies, (Japan, Nov. 17−19).
Yoshida, T., and Kajino, T.: 2003, 7Li and 11B Synthesis inSupernovae through the ν-Process and the Role of
Nuclear Cluster Reactions, The 8th Int. Conf. on
Clustering Aspects of Nuclear Structure and Dynamics,(Japan, Nov. 24−29).
Yoshida, T., and Kajino, T.: 2003, Light element synthesis
through the n-process in supernova explosions, Proc. Int.
Symp. on Origin of Matter and Evolution of Galaxies,(Saitama, Nov. 11−19).
Yoshida, T., Terasawa, M., Kajino, T., and Sumiyoshi, K.:
2003, Light Element and r-Process Element Syntheses
through the ν-Process in Supernova Explosions, Origin
of Matter and Evolution of the Galaxies, (Japan, Nov.
17−19).
Yoshida, T.: 2003, 7Li and 11B Synthesis through the νProcess in Type II Supernova Explosions, 6th RESCEU
International Symposium, Frontier in Astroparticle
Physics and Cosmology, (Japan, Nov. 4−7).
Yoshino, T., Kunimori, H., Hosokawa, M., Kawamura, S.,
Nagano, S., Naito, I., Sato, T., and Ohkawa, M.: 2003,
Ground Simulator Development for Inter-Satellite Laser
Interferometer, IUGG 2003, (Sapporo, June 30 - July
11).

74